FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Shrestha, AK Kato, S Wong, T Rutan, DA Miller, WF Rose, FG Smith, GL Bedka, KM Minnis, P Fernandez, JR AF Shrestha, Alok K. Kato, Seiji Wong, Takmeng Rutan, David A. Miller, Walter F. Rose, Fred G. Smith, G. Louis Bedka, Kristopher M. Minnis, Patrick Fernandez, Jose R. TI Unfiltering Earth Radiation Budget Experiment (ERBE) Scanner Radiances Using the CERES Algorithm and Its Evaluation with Nonscanner Observations SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article DE Satellite observations; Climate records; Filtering techniques; Remote sensing ID ENERGY SYSTEM INSTRUMENT; ANGULAR-DISTRIBUTION MODELS; DECADAL VARIABILITY; FLUX ESTIMATION; MODIS DATA; CLOUDS; SATELLITE; IDENTIFICATION; VALIDATION; MISSION AB The NOAA-9 Earth Radiation Budget Experiment (ERBE) scanner measured broadband shortwave, longwave, and total radiances from February 1985 through January 1987. These scanner radiances are reprocessed using the more recent Clouds and the Earth's Radiant Energy System (CERES) unfiltering algorithm. The scene information, including cloud properties, required for reprocessing is derived using Advanced Very High Resolution Radiometer (AVHRR) data on board NOAA-9, while no imager data were used in the original ERBE unfiltering. The reprocessing increases the NOAA-9 ERBE scanner unfiltered longwave radiances by 1.4%-2.0% during daytime and 0.2%-0.3% during nighttime relative to those derived from the ERBE unfiltering algorithm. Similarly, the scanner unfiltered shortwave radiances increase by similar to 1% for clear ocean and land and decrease for all-sky ocean, land, and snow/ice by similar to 1%. The resulting NOAA-9 ERBE scanner unfiltered radiances are then compared with NOAA-9 nonscanner irradiances by integrating the ERBE scanner radiance over the nonscanner field of view. The comparison indicates that the integrated scanner radiances are larger by 0.9% for shortwave and 0.7% smaller for longwave. A sensitivity study shows that the one-standard-deviation uncertainties in the agreement are +/- 2.5%, +/- 1.2%, and +/- 1.8% for the shortwave, nighttime longwave, and daytime longwave irradiances, respectively. The NOAA-9 and ERBS nonscanner irradiances are also compared using 2 years of data. The comparison indicates that the NOAA-9 nonscanner shortwave, nighttime longwave, and daytime longwave irradiances are 0.3% larger, 0.6% smaller, and 0.4% larger, respectively. The longer observational record provided by the ERBS nonscanner plays a critical role in tying the CERES-like NOAA-9 ERBE scanner dataset from the mid-1980s to the present-day CERES scanner data record. C1 [Shrestha, Alok K.; Rutan, David A.; Miller, Walter F.; Rose, Fred G.; Smith, G. Louis; Bedka, Kristopher M.; Fernandez, Jose R.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Shrestha, Alok K.; Kato, Seiji; Wong, Takmeng; Rutan, David A.; Miller, Walter F.; Rose, Fred G.; Smith, G. Louis; Bedka, Kristopher M.; Minnis, Patrick; Fernandez, Jose R.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Shrestha, AK (reprint author), Sci Syst & Applicat Inc, 1 Enterprise Pkwy,Suite 200, Hampton, VA 23666 USA. EM alok.k.shrestha@nasa.gov RI Minnis, Patrick/G-1902-2010; OI Minnis, Patrick/0000-0002-4733-6148; Rose, Fred G/0000-0003-0769-0772 FU NOAA Climate Data Record program FX We thank Drs. Bruce Wielicki, Norman G. Loeb, and David Johnson, and Mr. David Doelling for useful discussions. This work was supported by the NOAA Climate Data Record program (http://www.ncdc.noaa.gov/cdr). NR 35 TC 0 Z9 0 U1 0 U2 8 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD APR PY 2014 VL 31 IS 4 BP 843 EP 859 DI 10.1175/JTECH-D-13-00072.1 PG 17 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA AE6XX UT WOS:000334142400006 ER PT J AU Roithmayr, CM Lukashin, C Speth, PW Young, DF Wielicki, BA Thome, KJ Kopp, G AF Roithmayr, C. M. Lukashin, C. Speth, P. W. Young, D. F. Wielicki, B. A. Thome, K. J. Kopp, G. TI Opportunities to Intercalibrate Radiometric Sensors from International Space Station SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article DE Satellite observations; Remote sensing; Sampling; Shortwave radiation; Radiances; Instrumentation/sensors ID CLIMATE; SYSTEM; TERRA; MODIS AB Highly accurate measurements of Earth's thermal infrared and reflected solar radiation are required for detecting and predicting long-term climate change. Consideration is given to the concept of using the International Space Station to test instruments and techniques that would eventually be used on a dedicated mission, such as the Climate Absolute Radiance and Refractivity Observatory (CLARREO). In particular, a quantitative investigation is performed to determine whether it is possible to use measurements obtained with a highly accurate (0.3%, with 95% confidence) reflected solar radiation spectrometer to calibrate similar, less accurate instruments in other low Earth orbits. Estimates of numbers of samples useful for intercalibration are made with the aid of yearlong simulations of orbital motion. Results of this study support the conclusion that the International Space Station orbit is ideally suited for the purpose of intercalibration between spaceborne sensors. C1 [Roithmayr, C. M.; Lukashin, C.; Speth, P. W.; Young, D. F.; Wielicki, B. A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Thome, K. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kopp, G.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. RP Lukashin, C (reprint author), NASA, Langley Res Ctr, MS 420, Hampton, VA 23681 USA. EM constantine.lukashin-1@nasa.gov RI Thome, Kurtis/D-7251-2012; Richards, Amber/K-8203-2015 NR 22 TC 0 Z9 0 U1 2 U2 11 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD APR PY 2014 VL 31 IS 4 BP 890 EP 902 DI 10.1175/JTECH-D-13-00163.1 PG 13 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA AE6XX UT WOS:000334142400009 ER PT J AU Devi, VM Kleiner, I Sams, RL Brown, LR Benner, DC Fletcher, LN AF Devi, V. Malathy Kleiner, Isabelle Sams, Robert L. Brown, Linda R. Benner, D. Chris Fletcher, Leigh N. TI Line positions and intensities of the phosphine (PH3) Pentad near 4.5 mu m SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE PH3 Line positions; Intensities Infrared fundamentals; Pentad ID SPECTROSCOPIC PARAMETERS; SPECTRUM; BANDS; ATMOSPHERE; JUPITER; GAS; NH3; ASSIGNMENTS; STRENGTHS; MOLECULE AB In order to improve the spectroscopic database for remote sensing of the giant planets, line positions and intensities are determined for the five bands (2v(2), v(2) + v(4), 2v(4), v(1) and v(3)) that comprise the Pentad of PH3 between 1950 and 2450 cm(-1). Knowledge of PH3 spectral line parameters in this region is important for the exploration of dynamics and chemistry on Saturn, (using existing Cassini/VIMS observations) and future near-IR data of Jupiter from Juno and ESA's Jupiter Icy Moons Explorer (JUICE). For this study, spectra of pure PH3 from two Fourier transform spectrometers were obtained: (a) five high-resolution (0.00223 cm(-1)), high signal-to-noise (similar to 1800) spectra recorded at room temperature (298.2 K) with the Bruker IFS 125HR Fourier transform spectrometer (FTS) at the Pacific Northwest National Laboratory (PNNL), Richland, Washington and(b) four high-resolution (at 0.0115 cm(-1) resolution), high signal-to-noise (similar to 700) spectra recorded at room temperature in the region 1800-5200 cm(-1) using the McMath-Pierce Fourier transform spectrometer located at the National Solar Observatory (NSO) on Kitt Peak. Individual line parameters above 2150 cm(-1) were retrieved by simultaneous multispectrum fittings of all five Bruker spectra, while retrievals with the four Kitt Peak spectra were done in the 1938-2168 cm(-1) range spectrum by spectrum and averaged. In all, positions and intensities were obtained for more than 4400 lines. These included 53 A+A-split pairs of transitions (arising due to vibration-rotation interactions (Coriolis-type interaction) between the v3 and v(1) fundamental bands) for K" = 3, 6, and 9. Over 3400 positions and 1750 intensities of these lines were ultimately identified as relatively unblended and modeled up to J = 14 and K= 12 with rms values of 0.00133 cm(-1) and 7.7%, respectively. The PH3 line parameters (observed positions and measured intensities with known quantum assignments) and Hamiltonian constants are reported. Comparisons with other recent studies are discussed. (C) 2014 Elsevier Inc. All rights reserved. C1 [Devi, V. Malathy; Benner, D. Chris] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. [Kleiner, Isabelle] Univ Paris Est & Diderot, Lab Interuniv Syst Atmospher, CNRS, IPSL,UMR 7583, F-94010 Creteil, France. [Sams, Robert L.] Pacific NW Natl Lab, Richland, WA 99352 USA. [Brown, Linda R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Fletcher, Leigh N.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. RP Devi, VM (reprint author), Coll William & Mary, Dept Phys, Box 8795, Williamsburg, VA 23187 USA. EM malathy.d.venkataraman@nasa.gov RI Fletcher, Leigh/D-6093-2011 OI Fletcher, Leigh/0000-0001-5834-9588 FU College of William and Mary. Research at the Jet propulsion Laboratory (JPL), California Institute of Technology; Department of Energy's Office of Biological and Environmental Research; United States Department of Energy by the Battelle Memorial Institute [DE-ACO5-76RLO 1830] FX NASA's Outer Planetary Research Program supported the work performed at the College of William and Mary. Research at the Jet propulsion Laboratory (JPL), California Institute of Technology, was performed under contract with the National Aeronautics and Space Administration. The United States Department of Energy supported part of this research and was conducted at the W.R. Wiley Environmental Molecular Sciences laboratory, a national scientific user facility sponsored by the Department of Energy's Office of Biological and Environmental Research and located at the Pacific Northwest National Laboratory (PNNL). PNNL is operated for the United States Department of Energy by the Battelle Memorial Institute under Contract DE-ACO5-76RLO 1830. L.N. Fletcher was supported by a Royal Society Research Fellowship at the University of Oxford. NR 38 TC 5 Z9 5 U1 1 U2 12 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 EI 1096-083X J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD APR PY 2014 VL 298 BP 11 EP 23 DI 10.1016/j.jms.2014.01.0130022-2852 PG 13 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA AE8MT UT WOS:000334256700003 ER PT J AU Lau, W AF Lau, William TI ATMOSPHERIC SCIENCE Desert dust and monsoon rain SO NATURE GEOSCIENCE LA English DT News Item ID ARABIAN SEA C1 NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA. RP Lau, W (reprint author), NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA. EM William.K.Lau@nasa.gov NR 12 TC 6 Z9 6 U1 0 U2 12 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD APR PY 2014 VL 7 IS 4 BP 255 EP 256 DI 10.1038/ngeo2115 PG 2 WC Geosciences, Multidisciplinary SC Geology GA AE2PP UT WOS:000333815700009 ER PT J AU Curry, B Lee, CM Petrie, B Moritz, RE Kwok, R AF Curry, B. Lee, C. M. Petrie, B. Moritz, R. E. Kwok, R. TI Multiyear Volume, Liquid Freshwater, and Sea Ice Transports through Davis Strait, 2004-10* SO JOURNAL OF PHYSICAL OCEANOGRAPHY LA English DT Article DE Geographic location/entity; Sea ice; Circulation/ Dynamics; Arctic; Transport; Ocean circulation; In situ oceanic observations; Observational techniques and algorithms; Glaciers ID CANADIAN ARCTIC ARCHIPELAGO; NORTH-ATLANTIC; LABRADOR SEA; EAST GREENLAND; NARES STRAIT; BAFFIN-BAY; CIRCULATION; OCEAN; VARIABILITY; GLACIERS AB Davis Strait is a primary gateway for freshwater exchange between the Arctic and North Atlantic Oceans including freshwater contributions from west Greenland and Canadian Arctic Archipelago glacial melt. Data from six years (2004-10) of continuous measurements collected by a full-strait moored array and concurrent high-resolution Seaglider surveys are used to estimate volume and liquid freshwater transports through Davis Strait, with respective annual averages of -1.6 +/- 0.5 Sverdrups (Sv; 1 Sv equivalent to 10(6) m(3) s(-1)) and -93 +/- 6 mSv (negative sign indicates southward transport). Sea ice export contributes an additional -10 +/- 1 mSv of freshwater transport, estimated using satellite ice area transport and moored upward-looking sonar ice thickness measurements. Interannual and annual variability of the net transports are large, with average annual volume and liquid freshwater transport standard deviations of 0.7 Sv and 17 mSv and with interannual standard deviations of 0.3 Sv and 15 mSv. Moreover, there are no clear trends in the net transports over the 6-yr period. However, salinity in the upper 250 m between Baffin Island and midstrait decreases starting in September 2009 and remains below average through August 2010, but appears to return to normal by the end of 2010. This freshening event, likely caused by changes in arctic freshwater storage, is not apparent in the liquid freshwater transport time series due to a reduction in southward volume transport in 2009-10. Reanalysis of Davis Strait mooring data from the period 1987-90, compared to the 2004-10 measurements, reveals less arctic outflow and warmer, more saline North Atlantic inflow during the most recent period. C1 [Curry, B.; Lee, C. M.; Moritz, R. E.] Univ Washington, Appl Phys Lab, Seattle, WA 98105 USA. [Petrie, B.] Bedford Inst Oceanog, Ocean Sci Div, Dartmouth, NS, Canada. [Kwok, R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Curry, B (reprint author), Univ Washington, Appl Phys Lab, 1013 NE 40th St, Seattle, WA 98105 USA. EM beth4cu@uw.edu RI Kwok, Ron/A-9762-2008 OI Kwok, Ron/0000-0003-4051-5896 FU U.S. National Science Foundation Freshwater Initiative program; International Polar Year and Arctic Observing Network program [OPP0230381, OPP0632231] FX We thank the reviewers for helpful suggestions that improved this manuscript. This study is part of U.S. National Science Foundation Freshwater Initiative (2004-07) and the International Polar Year and Arctic Observing Network (2007-10) programs under Grants OPP0230381 and OPP0632231. Additional support was provided by the Department of Fisheries and Oceans, Canada. Knut Aagaard, Jerome Cuny, Humfrey Melling, Peter Rhines, and Charles Tang contributed to the array design. Jason Gobat, Eric Boget, James Johnson, Keith VanThiel, Murray Scotney, Victor Soukhovstev, Adam Huxtable, and James Abriel were essential to the measurement program. We thank Yongsheng Wu for conducting the principal component analysis of the current data (presented in appendix C of the online supplemental material). NR 57 TC 28 Z9 28 U1 3 U2 24 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-3670 EI 1520-0485 J9 J PHYS OCEANOGR JI J. Phys. Oceanogr. PD APR PY 2014 VL 44 IS 4 BP 1244 EP 1266 DI 10.1175/JPO-D-13-0177.1 PG 23 WC Oceanography SC Oceanography GA AE6TD UT WOS:000334128200011 ER PT J AU Yamakov, VI Warner, DH Zamora, RJ Saether, E Curtin, WA Glaessgen, EH AF Yamakov, V. I. Warner, D. H. Zamora, R. J. Saether, E. Curtin, W. A. Glaessgen, E. H. TI Investigation of crack tip dislocation emission in aluminum using multiscale molecular dynamics simulation and continuum modeling SO JOURNAL OF THE MECHANICS AND PHYSICS OF SOLIDS LA English DT Article DE Crack tip plasticity; Twinning; Slip; Aluminum; Molecular dynamics simulation ID SINGLE-CRYSTALS; DEFORMATION; NUCLEATION; METALS; FRACTURE; SOLIDS; ENERGY; AL AB This work investigates the dislocation nucleation processes that occur at the tip of a crack in aluminum under a broad range of crystallographic orientations and temperatures. A concurrent multiscale molecular dynamics - continuum simulation framework is employed. The results are then interpreted using a Peierls continuum model that uses finite temperature material properties derived from molecular dynamics simulation. Under ramped loading, partial dislocation nucleation at the crack tip is found to lead to both full dislocation emission and twinning, depending upon the orientation, temperature, and magnitude of the applied load in the simulation. The origins of the dependencies are made apparent by the Peierls continuum model. The continuum model suggests that in many instances dislocation nucleation from the crack tip can be considered to be a strain rate independent process, yet still temperature dependent through the temperature dependence of the stacking fault energies and elastic constants. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Yamakov, V. I.] Natl Inst Aerosp, Hampton, VA 23666 USA. [Warner, D. H.; Zamora, R. J.] Cornell Univ, Sch Civil & Environm Engn, Ithaca, NY 14853 USA. [Saether, E.; Glaessgen, E. H.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Curtin, W. A.] Ecole Polytech Fed Lausanne, Inst Engn Mech, CH-1015 Lausanne, Switzerland. RP Yamakov, VI (reprint author), Natl Inst Aerosp, Hampton, VA 23666 USA. EM yamakov@nianet.org RI Warner, Derek/A-2303-2012 FU National Institute of Aerospace [NCC-1-02043]; NASA [NNX08BA39A, NNX07AU56A]; Office of Naval Research [N00014-08-1-0862, N00014-10-1-0323, N00014-07-1-0528] FX V. Yamakov is sponsored through cooperative agreement NCC-1-02043 with the National Institute of Aerospace. D.H. Warner acknowledges support from NASA (Grant no. NNX08BA39A) and Paul Hess at the Office of Naval Research (Grant nos. N00014-08-1-0862 and N00014-10-1-0323). W.A. Curtin acknowledges support for this work from NASA through Grant NNX07AU56A and from the Office of Naval Research through Grant N00014-07-1-0528. NR 36 TC 15 Z9 15 U1 5 U2 64 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-5096 EI 1873-4782 J9 J MECH PHYS SOLIDS JI J. Mech. Phys. Solids PD APR PY 2014 VL 65 BP 35 EP 53 DI 10.1016/j.jmps.2013.12.009 PG 19 WC Materials Science, Multidisciplinary; Mechanics; Physics, Condensed Matter SC Materials Science; Mechanics; Physics GA AE6UB UT WOS:000334132300003 ER PT J AU Hoffmayer, ER Franks, JS Driggers, WB McKinney, JA Hendon, JM Quattro, JM AF Hoffmayer, Eric R. Franks, James S. Driggers, William B. McKinney, Jennifer A. Hendon, Jill M. Quattro, Joseph M. TI Habitat, movements and environmental preferences of dusky sharks, Carcharhinus obscurus, in the northern Gulf of Mexico SO MARINE BIOLOGY LA English DT Article ID SATELLITE ARCHIVAL TAGS; TUNA THUNNUS-ALBACARES; ATLANTIC BLUEFIN TUNA; SCALLOPED HAMMERHEAD; NORTHWEST ATLANTIC; SPHYRNA-LEWINI; SEXUAL SEGREGATION; GALEOCERDO-CUVIER; FISH ASSEMBLAGES; PELAGIC SHARKS AB The dusky shark (Carcharhinus obscurus) is the largest member of the genus Carcharhinus and inhabits coastal and pelagic ecosystems circumglobally in temperate, subtropical and tropical marine waters. In the western North Atlantic Ocean (WNA), dusky sharks are overfished and considered vulnerable by the International Union for the Conservation of Nature. As a result, retention of dusky sharks in commercial and recreational fisheries off the east coast of the United States (US) and in the northern Gulf of Mexico is prohibited. Despite the concerns regarding the status of dusky sharks in the WNA, little is known about their habitat utilization. During the summers of 2008-2009, pop-up satellite archival tags were attached to ten dusky sharks (one male, nine females) at a location where they have been observed to aggregate in the north central Gulf of Mexico southwest of the Mississippi River Delta to examine their movement patterns and habitat utilization. All tags successfully transmitted data with deployment durations ranging from 6 to 124 days. Tag data revealed shark movements in excess of 200 km from initial tagging locations, with sharks primarily utilizing offshore waters associated with the continental shelf edge from Desoto Canyon to the Texas/Mexican border. While most sharks remained in US waters, one individual moved from the northern Gulf of Mexico into the Bay of Campeche off the coast of Mexico. Sharks spent 87 % of their time between 20 and 125 m and 83 % of their time in waters between 23 and 30 A degrees C. Since dusky sharks are among the most vulnerable shark species to fishing mortality, there is a recovery plan in place for US waters; however, since they have been shown to make long-distance migrations, a multi-national management plan within the WNA may be needed to ensure the successful recovery of this population. C1 [Hoffmayer, Eric R.; Franks, James S.; Hendon, Jill M.] Univ So Mississippi, Gulf Coast Res Lab, Ctr Fisheries Res & Dev, Ocean Springs, MS 39564 USA. [McKinney, Jennifer A.] Louisiana Dept Wildlife & Fisheries, Fisheries Management Div, Baton Rouge, LA 70808 USA. [Quattro, Joseph M.] Univ S Carolina, Dept Biol Sci, Marine Sci Program, Columbia, SC 29208 USA. RP Hoffmayer, ER (reprint author), Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, 3209 Freder St,PO Drawer 1207, Pascagoula, MS 39567 USA. EM eric.hoffmayer@noaa.gov FU National Marine Fisheries Service, Cooperative Research Program [NA08NMF4540389]; US law under scientific research permits [HMS-EFP-08-07, SHK-EFP-09-03] FX We thank the Gulf Coast Research Laboratory Shark Research Program team members, including G. Gray, J. Shelley, S. Curran, B. Dempster, D. Hildebrandt and E. Hildebrandt for their field assistance. We thank Captain K. Beach of the sport fishing vessel "Pale Horse," Captain B. Delabar and deck-hand B. C. Bobby of the sport fishing vessel "Frenzy" (Venice, Louisiana) for their expertise, professionalism and spirit of cooperation. We are also indebted to B. Galuardi and A. Carlson for their assistance with filtering our movement data. Funding for this project was provided by the National Marine Fisheries Service, Cooperative Research Program (Grant #NA08NMF4540389) to E. Hoffmayer and J. Franks. This research was conducted in compliance with US law under scientific research permits HMS-EFP-08-07 and SHK-EFP-09-03, issued by the Highly Migratory Species Division of the Office of Sustainable Fisheries, National Marine Fisheries Service, Silver Spring, MD 20910, USA, and the Institutional Animal Care and Use Committee of the University of Southern Mississippi (protocol 09031204). The opinions expressed herein, are those of the author(s) and do not necessarily reflect the views of NOAA or the Department of Commerce. NR 83 TC 2 Z9 2 U1 2 U2 36 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0025-3162 EI 1432-1793 J9 MAR BIOL JI Mar. Biol. PD APR PY 2014 VL 161 IS 4 BP 911 EP 924 DI 10.1007/s00227-014-2391-0 PG 14 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AE3TD UT WOS:000333899500015 ER PT J AU Numata, K Alalusi, M Stolpner, L Margaritis, G Camp, J Krainak, M AF Numata, Kenji Alalusi, Mazin Stolpner, Lew Margaritis, Georgios Camp, Jordan Krainak, Michael TI Characteristics of the single-longitudinal-mode planar-waveguide external cavity diode laser at 1064 nm SO OPTICS LETTERS LA English DT Article ID STABILIZATION AB We describe the characteristics of the planar-waveguide external cavity diode laser (PW-ECL). To the best of our knowledge, it is the first butterfly-packaged 1064 nm semiconductor laser that is stable enough to be locked to an external frequency reference. We evaluated its performance from the viewpoint of precision experiments. Using a hyperfine absorption line of iodine, we suppressed its frequency noise by a factor of up to 10(4) at 10 mHz. The PW-ECL's compactness and low cost make it a candidate to replace traditional Nd:YAG nonplanar ring oscillators and fiber lasers in applications that require a single longitudinal mode. (C) 2014 Optical Society of America C1 [Numata, Kenji] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Numata, Kenji; Camp, Jordan; Krainak, Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Alalusi, Mazin; Stolpner, Lew; Margaritis, Georgios] Redfern Integrated Opt Inc, Santa Clara, CA 95054 USA. RP Numata, K (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM kenji.numata@nasa.gov FU NASA Small Business Innovation Research (SBIR) program FX This research was funded by the NASA Small Business Innovation Research (SBIR) program. NR 17 TC 9 Z9 9 U1 1 U2 22 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 EI 1539-4794 J9 OPT LETT JI Opt. Lett. PD APR 1 PY 2014 VL 39 IS 7 BP 2101 EP 2104 DI 10.1364/OL.39.002101 PG 4 WC Optics SC Optics GA AE3PG UT WOS:000333887800101 PM 24686685 ER PT J AU Ryasnyanskiy, A Vorobiev, N Smirnov, V Lumeau, J Glebova, L Mokhun, O Spiegelberg, C Krainak, M Glebov, A Glebov, L AF Ryasnyanskiy, A. Vorobiev, N. Smirnov, V. Lumeau, J. Glebova, L. Mokhun, O. Spiegelberg, Ch. Krainak, Michael Glebov, A. Glebov, L. TI DBR and DFB lasers in neodymium- and ytterbium-doped photothermorefractive glasses SO OPTICS LETTERS LA English DT Article ID THERMO-REFRACTIVE GLASS; HIGH-POWER; FEEDBACK AB The first demonstration, to the best of our knowledge, of distributed Bragg reflector (DBR) and monolithic distributed feedback (DFB) lasers in photothermorefractive glass doped with rare-earth ions is reported. The lasers were produced by incorporation of the volume Bragg gratings into the laser gain elements. A monolithic single-frequency solid-state laser with a linewidth of 250 kHz and output power of 150 mW at 1066 nm is demonstrated. (C) 2014 Optical Society of America C1 [Ryasnyanskiy, A.; Smirnov, V.; Glebova, L.; Mokhun, O.; Spiegelberg, Ch.; Glebov, A.] OptiGrate Corp, Oviedo, FL 32765 USA. [Vorobiev, N.; Lumeau, J.; Glebov, L.] Univ Cent Florida, CREOL Coll Opt & Photon, Orlando, FL 32816 USA. [Lumeau, J.] Aix Marseille Univ, CNRS, Inst Fresnel, UMR 7249, F-13013 Marseille, France. [Krainak, Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ryasnyanskiy, A (reprint author), OptiGrate Corp, 562 South Econ Circle, Oviedo, FL 32765 USA. EM aryasnyanskiy@optigrate.com RI Lumeau, Julien/P-6704-2015 OI Lumeau, Julien/0000-0001-9800-4189 FU NASA; DARPA [NNX11CA87C, W31P4Q-12-C-0215] FX This work was partially supported by NASA and DARPA contracts NNX11CA87C and W31P4Q-12-C-0215. NR 13 TC 1 Z9 1 U1 0 U2 11 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 EI 1539-4794 J9 OPT LETT JI Opt. Lett. PD APR 1 PY 2014 VL 39 IS 7 BP 2156 EP 2159 DI 10.1364/OL.39.002156 PG 4 WC Optics SC Optics GA AE3PG UT WOS:000333887800115 PM 24686699 ER PT J AU DeGloria, SD Beaudette, DE Irons, JR Libohova, Z O'Neill, PE Owens, PR Schoeneberger, PJ West, LT Wysocki, DA AF DeGloria, Stephen D. Beaudette, Dylan E. Irons, James R. Libohova, Zamir O'Neill, Peggy E. Owens, Philip R. Schoeneberger, Philip J. West, Larry T. Wysocki, Douglas A. TI Emergent Imaging and Geospatial Technologies for Soil Investigations SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING LA English DT Editorial Material ID PASSIVE SMAP MISSION C1 [DeGloria, Stephen D.] Cornell Univ, Ithaca, NY 14853 USA. [Beaudette, Dylan E.] USDA, NRCS, Washington, DC USA. [Irons, James R.; O'Neill, Peggy E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Libohova, Zamir; Schoeneberger, Philip J.; Wysocki, Douglas A.] USDA, NRCS Natl Soil Survey Ctr, Washington, DC USA. [Owens, Philip R.] Purdue Univ, W Lafayette, IN 47907 USA. [West, Larry T.] Formerly USDA, NRCS Natl Soil Survey Ctr, Washington, DC USA. RP DeGloria, SD (reprint author), Cornell Univ, Ithaca, NY 14853 USA. EM sdd4@cornell.edu; debeaudette@ucdavis.edu; james.r.irons@nasa.gov; zamir.libohova@lin.usda.gov; peggy.e.oneill@nasa.gov; prowens@purdue.edu; Philip.Schoeneberger@lin.usda.gov; larrywestar@gmail.com; doug.wysocki@lin.usda.gov RI DeGloria, Stephen/B-8513-2015 OI DeGloria, Stephen/0000-0002-3343-6607 NR 26 TC 0 Z9 0 U1 1 U2 16 PU AMER SOC PHOTOGRAMMETRY PI BETHESDA PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA SN 0099-1112 J9 PHOTOGRAMM ENG REM S JI Photogramm. Eng. Remote Sens. PD APR PY 2014 VL 80 IS 4 BP 289 EP 294 PG 6 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA AE3HK UT WOS:000333867400002 ER PT J AU DeGloria, SD Irons, JR West, LT AF DeGloria, Stephen D. Irons, James R. West, Larry T. TI Remote Sensing of Soils for Environmental Assessment and Management Foreword SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING LA English DT Editorial Material C1 [DeGloria, Stephen D.] Cornell Univ, Dept Crop & Sci, Ithaca, NY 14853 USA. [Irons, James R.] NASA Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD USA. RP DeGloria, SD (reprint author), Cornell Univ, Dept Crop & Sci, Ithaca, NY 14853 USA. EM sdd4@cornell.edu; james.r.irons@nasa.gov; larrywestar@gmail.com RI DeGloria, Stephen/B-8513-2015 OI DeGloria, Stephen/0000-0002-3343-6607 NR 0 TC 0 Z9 0 U1 0 U2 2 PU AMER SOC PHOTOGRAMMETRY PI BETHESDA PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA SN 0099-1112 J9 PHOTOGRAMM ENG REM S JI Photogramm. Eng. Remote Sens. PD APR PY 2014 VL 80 IS 4 BP 309 EP 310 PG 2 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA AE3HK UT WOS:000333867400005 ER PT J AU Cody, AM Stauffer, J Baglin, A Micela, G Rebull, LM Flaccomio, E Morales-Calderon, M Aigrain, S Bouvier, J Hillenbrand, LA Gutermuth, R Song, I Turner, N Alencar, SHP Zwintz, K Plavchan, P Carpenter, J Findeisen, K Carey, S Terebey, S Hartmann, L Calvet, N Teixeira, P Vrba, FJ Wolk, S Covey, K Poppenhaeger, K Gunther, HM Forbrich, J Whitney, B Affer, L Herbst, W Hora, J Barrado, D Holtzman, J Marchis, F Wood, K Guimaraes, MM Box, JL Gillen, E McQuillan, A Espaillat, C Allen, L D'Alessio, P Favata, F AF Cody, Ann Marie Stauffer, John Baglin, Annie Micela, Giuseppina Rebull, Luisa M. Flaccomio, Ettore Morales-Calderon, Maria Aigrain, Suzanne Bouvier, Jerome Hillenbrand, Lynne A. Gutermuth, Robert Song, Inseok Turner, Neal Alencar, Silvia H. P. Zwintz, Konstanze Plavchan, Peter Carpenter, John Findeisen, Krzysztof Carey, Sean Terebey, Susan Hartmann, Lee Calvet, Nuria Teixeira, Paula Vrba, Frederick J. Wolk, Scott Covey, Kevin Poppenhaeger, Katja Guenther, Hans Moritz Forbrich, Jan Whitney, Barbara Affer, Laura Herbst, William Hora, Joseph Barrado, David Holtzman, Jon Marchis, Franck Wood, Kenneth Guimaraes, Marcelo Medeiros Lillo Box, Jorge Gillen, Ed McQuillan, Amy Espaillat, Catherine Allen, Lori D'Alessio, Paola Favata, Fabio TI CSI 2264: SIMULTANEOUS OPTICAL AND INFRARED LIGHT CURVES OF YOUNG DISK-BEARING STARS IN NGC 2264 WITH CoRoT and SPITZER-EVIDENCE FOR MULTIPLE ORIGINS OF VARIABILITY SO ASTRONOMICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; protoplanetary disks; stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be; techniques: photometric ID T-TAURI STARS; MAIN-SEQUENCE STARS; ORION NEBULA CLUSTER; TERM PHOTOMETRIC VARIABILITY; ROTATION PERIOD DISTRIBUTION; INITIAL MASS FUNCTION; X-RAY OBSERVATIONS; MIDINFRARED VARIABILITY; MOLECULAR CLOUD; BROWN DWARFS AB We present the Coordinated Synoptic Investigation of NGC 2264, a continuous 30 day multi-wavelength photometric monitoring campaign on more than 1000 young cluster members using 16 telescopes. The unprecedented combination of multi-wavelength, high-precision, high-cadence, and long-duration data opens a new window into the time domain behavior of young stellar objects. Here we provide an overview of the observations, focusing on results from Spitzer and CoRoT. The highlight of this work is detailed analysis of 162 classical T Tauri stars for which we can probe optical and mid-infrared flux variations to 1% amplitudes and sub-hour timescales. We present a morphological variability census and then use metrics of periodicity, stochasticity, and symmetry to statistically separate the light curves into seven distinct classes, which we suggest represent different physical processes and geometric effects. We provide distributions of the characteristic timescales and amplitudes and assess the fractional representation within each class. The largest category (>20%) are optical "dippers" with discrete fading events lasting similar to 1-5 days. The degree of correlation between the optical and infrared light curves is positive but weak; notably, the independently assigned optical and infrared morphology classes tend to be different for the same object. Assessment of flux variation behavior with respect to (circum)stellar properties reveals correlations of variability parameters with Ha emission and with effective temperature. Overall, our results point to multiple origins of young star variability, including circumstellar obscuration events, hot spots on the star and/or disk, accretion bursts, and rapid structural changes in the inner disk. C1 [Cody, Ann Marie; Stauffer, John; Rebull, Luisa M.; Carey, Sean] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Baglin, Annie] Observ Paris, LESIA, F-92195 Meudon, France. [Micela, Giuseppina; Flaccomio, Ettore; Affer, Laura] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Morales-Calderon, Maria; Barrado, David; Lillo Box, Jorge] INTA CSIC, Ctr Astrobiol, Dpto Astrofis, E-28691 Madrid, Spain. [Aigrain, Suzanne; Gillen, Ed] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Bouvier, Jerome] UJF Grenoble 1 CNRS INSU, Inst Planetol & Astrophys Grenoble IPAG UMR 5274, F-38041 Grenoble, France. [Hillenbrand, Lynne A.; Carpenter, John; Findeisen, Krzysztof] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Gutermuth, Robert] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Song, Inseok] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. [Turner, Neal] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Alencar, Silvia H. P.] Dept Fis ICEx UFMG, BR-30270901 Belo Horizonte, MG, Brazil. [Zwintz, Konstanze] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Plavchan, Peter] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Terebey, Susan] Calif State Univ Los Angeles, Dept Phys & Astron, Los Angeles, CA 90032 USA. [Hartmann, Lee; Calvet, Nuria] Univ Michigan, Dept Astron, Ann Arbor, MI 48105 USA. [Teixeira, Paula; Forbrich, Jan] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Vrba, Frederick J.] US Naval Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA. [Wolk, Scott; Poppenhaeger, Katja; Guenther, Hans Moritz; Forbrich, Jan; Hora, Joseph] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Covey, Kevin] Lowell Observ, Flagstaff, AZ 86001 USA. [Whitney, Barbara] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Herbst, William] Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA. [Holtzman, Jon] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Marchis, Franck] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Wood, Kenneth] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9AD, Fife, Scotland. [Guimaraes, Marcelo Medeiros] Dept Fis & Matemat UFSJ, BR-36420000 Ouro Branco, MG, Brazil. [McQuillan, Amy] Tel Aviv Univ, Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Espaillat, Catherine] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Allen, Lori] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [D'Alessio, Paola] UNAM, Ctr Radioastron & Astrofs, Morelia 58089, Michoacan, Mexico. [Favata, Fabio] European Space Agcy, F-75738 Paris 15, France. RP Cody, AM (reprint author), CALTECH, Spitzer Sci Ctr, 1200 East Calif Blvd, Pasadena, CA 91125 USA. EM amc@ipac.caltech.edu RI Lillo-Box, Jorge/I-2841-2015; Alencar, Silvia/C-2803-2013; Teixeira, Paula Stella/O-2289-2013; Guimaraes, Marcelo/H-5897-2012; Barrado Navascues, David/C-1439-2017; Morales-Calderon, Maria/C-8384-2017; OI Lillo-Box, Jorge/0000-0003-3742-1987; Teixeira, Paula Stella/0000-0002-3665-5784; Guimaraes, Marcelo/0000-0002-0517-4507; Barrado Navascues, David/0000-0002-5971-9242; Morales-Calderon, Maria/0000-0001-9526-9499; Micela, Giuseppina/0000-0002-9900-4751; Findeisen, Krzysztof/0000-0003-1898-5760; Poppenhaeger, Katja/0000-0003-1231-2194; Gunther, Hans Moritz/0000-0003-4243-2840; Flaccomio, Ettore/0000-0002-3638-5788; Hora, Joseph/0000-0002-5599-4650; Zwintz, Konstanze/0000-0001-9229-8315; Rebull, Luisa/0000-0001-6381-515X; Covey, Kevin/0000-0001-6914-7797 FU NASA through JPL/Caltech.; JPL/Caltech [1373081, 1424329, 1440160]; CNpq; CAPES; Fapemig; NASA ADAP [NNX11AD14G, NNX13AF08G]; INCT-A/CNPq; Pegasus Marie Curie Fellowship of the Research Foundation Flanders (FWO); European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant [227224] FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. S.H.P.A. acknowledges support from CNpq, CAPES, and Fapemig. R.G. gratefully acknowledges funding support from NASA ADAP grants NNX11AD14G and NNX13AF08G and Caltech/JPL awards 1373081, 1424329, and 1440160 in support of Spitzer Space Telescope observing programs. M.M.G. acknowledges support from INCT-A/CNPq. K.Z. received a Pegasus Marie Curie Fellowship of the Research Foundation Flanders (FWO) during part of this work and received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 227224 (PROSPERITY). NR 109 TC 73 Z9 73 U1 0 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 APR PY 2014 VL 147 IS 4 DI 10.1088/0004-6256/147/4/82 PG 47 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE1KP UT WOS:000333728500014 ER PT J AU Sagiv, I Gal-Yam, A Ofek, EO Waxman, E Aharonson, O Kulkarni, SR Nakar, E Maoz, D Trakhtenbrot, B Phinney, ES Topaz, J Beichman, C Murthy, J Worden, SP AF Sagiv, I. Gal-Yam, A. Ofek, E. O. Waxman, E. Aharonson, O. Kulkarni, S. R. Nakar, E. Maoz, D. Trakhtenbrot, B. Phinney, E. S. Topaz, J. Beichman, C. Murthy, J. Worden, S. P. TI SCIENCE WITH A WIDE-FIELD UV TRANSIENT EXPLORER SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: eclipsing; methods: observational; supernovae: general; surveys; ultraviolet: general ID CORE-COLLAPSE SUPERNOVAE; GAMMA-RAY BURSTS; SUPERMASSIVE BLACK-HOLES; TIDAL DISRUPTION EVENTS; ACTIVE GALACTIC NUCLEI; HALO VELOCITY GROUPS; DIGITAL SKY SURVEY; SOLAR-TYPE STARS; II-P SUPERNOVAE; SHOCK BREAKOUT AB The time-variable electromagnetic sky has been well-explored at a wide range of wavelengths. In contrast, the ultra-violet (UV) variable sky is relatively poorly explored, even though it offers exciting scientific prospects. Here, we review the potential scientific impact of a wide-field UV survey on the study of explosive and other transient events, as well as known classes of variable objects, such as active galactic nuclei and variable stars. We quantify our predictions using a fiducial set of observational parameters which are similar to those envisaged for the proposed ULTRASAT mission. We show that such a mission would be able to revolutionize our knowledge about massive star explosions by measuring the early UV emission from hundreds of events, revealing key physical parameters of the exploding progenitor stars. Such a mission would also detect the UV emission from many tens of tidal-disruption events of stars by supermassive black holes at galactic nuclei and enable a measurement of the rate of such events. The overlap of such a wide-field UV mission with existing and planned gravitational-wave and high-energy neutrino telescopes makes it especially timely. C1 [Sagiv, I.; Gal-Yam, A.; Ofek, E. O.; Waxman, E.; Trakhtenbrot, B.; Topaz, J.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Aharonson, O.] Weizmann Inst Sci, Helen Kimmel Ctr Planetary Sci, IL-76100 Rehovot, Israel. [Kulkarni, S. R.; Phinney, E. S.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Nakar, E.; Maoz, D.] Tel Aviv Univ, Sch Phys & Astron, IL-93387 Tel Aviv, Israel. [Beichman, C.] CALTECH, Div Geophys & Planetary, Pasadena, CA 91105 USA. [Murthy, J.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Worden, S. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Sagiv, I (reprint author), Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. OI Murthy, Jayant/0000-0003-4034-5137 FU Israeli Space Agency; Keck Institute for Space Science (KISS) FX We thank M. Van Kerkwijk and B. E. Schaefer for useful discussions. This research has been supported by grants from the Israeli Space Agency and the Keck Institute for Space Science (KISS). NR 131 TC 13 Z9 13 U1 0 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 APR PY 2014 VL 147 IS 4 AR 79 DI 10.1088/0004-6256/147/4/79 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE1KP UT WOS:000333728500011 ER PT J AU Stauffer, J Cody, AM Baglin, A Alencar, S Rebull, L Hillenbrand, LA Venuti, L Turner, NJ Carpenter, J Plavchan, P Findeisen, K Carey, S Terebey, S Morales-Calderon, M Bouvier, J Micela, G Flaccomio, E Song, I Gutermuth, R Hartmann, L Calvet, N Whitney, B Barrado, D Vrba, FJ Covey, K Herbst, W Furesz, G Aigrain, S Favata, F AF Stauffer, John Cody, Ann Marie Baglin, Annie Alencar, Silvia Rebull, Luisa Hillenbrand, Lynne A. Venuti, Laura Turner, Neal J. Carpenter, John Plavchan, Peter Findeisen, Krzysztof Carey, Sean Terebey, Susan Morales-Calderon, Maria Bouvier, Jerome Micela, Giusi Flaccomio, Ettore Song, Inseok Gutermuth, Rob Hartmann, Lee Calvet, Nuria Whitney, Barbara Barrado, David Vrba, Frederick J. Covey, Kevin Herbst, William Furesz, Gabor Aigrain, Suzanne Favata, Fabio TI CSI 2264: CHARACTERIZING ACCRETION-BURST DOMINATED LIGHT CURVES FOR YOUNG STARS IN NGC 2264 SO ASTRONOMICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; stars: formation; stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be ID T-TAURI STARS; MAIN-SEQUENCE STARS; COROT PHOTOMETRIC-OBSERVATIONS; SPITZER-SPACE-TELESCOPE; INITIAL MASS FUNCTION; ARRAY CAMERA IRAC; MAGNETOSPHERIC ACCRETION; AA TAURI; MAGNETOHYDRODYNAMIC SIMULATIONS; MAGNETIZED STARS AB Based on more than four weeks of continuous high-cadence photometric monitoring of several hundred members of the young cluster NGC 2264 with two space telescopes, NASA's Spitzer and the CNES CoRoT (Convection, Rotation, and planetary Transits), we provide high-quality, multi-wavelength light curves for young stellar objects whose optical variability is dominated by short-duration flux bursts, which we infer are due to enhanced mass accretion rates. These light curves show many brief-several hours to one day-brightenings at optical and near-infrared wavelengths with amplitudes generally in the range of 5%-50% of the quiescent value. Typically, a dozen or more of these bursts occur in a 30 day period. We demonstrate that stars exhibiting this type of variability have large ultraviolet (UV) excesses and dominate the portion of the u - g versus g - r color-color diagram with the largest UV excesses. These stars also have large H alpha equivalent widths, and either centrally peaked, lumpy H alpha emission profiles or profiles with blueshifted absorption dips associated with disk or stellar winds. Light curves of this type have been predicted for stars whose accretion is dominated by Rayleigh-Taylor instabilities at the boundary between their magnetosphere and inner circumstellar disk, or where magneto-rotational instabilities modulate the accretion rate from the inner disk. Among the stars with the largest UV excesses or largest H alpha equivalent widths, light curves with this type of variability greatly outnumber light curves with relatively smooth sinusoidal variations associated with long-lived hot spots. We provide quantitative statistics for the average duration and strength of the accretion bursts and for the fraction of the accretion luminosity associated with these bursts. C1 [Stauffer, John; Cody, Ann Marie; Rebull, Luisa; Carey, Sean] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Baglin, Annie] LESIA, Observ Paris Meudon, F-92195 Meudon, France. [Alencar, Silvia] Univ Fed Minas Gerais, ICEx, Dept Fis, BR-30270901 Belo Horizonte, MG, Brazil. [Hillenbrand, Lynne A.; Carpenter, John; Findeisen, Krzysztof] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Venuti, Laura; Bouvier, Jerome] UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France. [Turner, Neal J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plavchan, Peter] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Terebey, Susan] Calif State Univ Los Angeles, Dept Phys & Astron, Los Angeles, CA 90032 USA. [Morales-Calderon, Maria; Barrado, David] CSIC, INTA, Dpto Astrofis, Ctr Astrobiol, E-28691 Madrid, Spain. [Micela, Giusi; Flaccomio, Ettore] INAF, Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Song, Inseok] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. [Gutermuth, Rob] Smith Coll, Coll Astron Dept 5, Northampton, MA 01063 USA. [Hartmann, Lee; Calvet, Nuria] Univ Michigan, Dept Astron, Ann Arbor, MI 48105 USA. [Whitney, Barbara] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Vrba, Frederick J.] US Naval Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA. [Covey, Kevin] Lowell Observ, Flagstaff, AZ 86001 USA. [Herbst, William] Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA. [Furesz, Gabor] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Aigrain, Suzanne] Univ Oxford, Dept Phys, Subdept Astrophys, Oxford OX1 3RH, England. [Favata, Fabio] European Space Agcy, F-75738 Paris 15, France. RP Stauffer, J (reprint author), CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. EM stauffer@ipac.caltech.edu RI Alencar, Silvia/C-2803-2013; Barrado Navascues, David/C-1439-2017; Morales-Calderon, Maria/C-8384-2017; OI Barrado Navascues, David/0000-0002-5971-9242; Morales-Calderon, Maria/0000-0001-9526-9499; Findeisen, Krzysztof/0000-0003-1898-5760; Micela, Giuseppina/0000-0002-9900-4751; Flaccomio, Ettore/0000-0002-3638-5788; Rebull, Luisa/0000-0001-6381-515X; Covey, Kevin/0000-0001-6914-7797 FU NASA; JPL/Caltech FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 60 TC 42 Z9 42 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD APR PY 2014 VL 147 IS 4 AR 83 DI 10.1088/0004-6256/147/4/83 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE1KP UT WOS:000333728500015 ER PT J AU Jolivet, R Duputel, Z Riel, B Simons, M Rivera, L Minson, SE Zhang, H Aivazis, MAG Ayoub, F Leprince, S Samsonov, S Motagh, M Fielding, EJ AF Jolivet, R. Duputel, Z. Riel, B. Simons, M. Rivera, L. Minson, S. E. Zhang, H. Aivazis, M. A. G. Ayoub, F. Leprince, S. Samsonov, S. Motagh, M. Fielding, E. J. TI The 2013 M-w 7.7 Balochistan Earthquake: Seismic Potential of an Accretionary Wedge SO BULLETIN OF THE SEISMOLOGICAL SOCIETY OF AMERICA LA English DT Article ID COSEISMIC DEFORMATION; IZMIT EARTHQUAKE; FAULT EARTHQUAKE; SOURCE INVERSION; SLIP; INTERFEROMETRY; ALGORITHM; PLATEAU; MODELS; IMAGES AB Great earthquakes rarely occur within active accretionary prisms, despite the intense long-term deformation associated with the formation of these geologic structures. This paucity of earthquakes is often attributed to partitioning of deformation across multiple structures as well as aseismic deformation within and at the base of the prism (Davis et al., 1983). We use teleseismic data and satellite optical and radar imaging of the 2013 M-w 7.7 earthquake that occurred on the southeastern edge of the Makran plate boundary zone to study this unexpected earthquake. We first compute a multiple point-source solution from W-phase waveforms to estimate fault geometry and rupture duration and timing. We then derive the distribution of subsurface fault slip from geodetic coseismic offsets. We sample for the slip posterior probability density function using a Bayesian approach, including a full description of the data covariance and accounting for errors in the elastic structure of the crust. The rupture nucleated on a subvertical segment, branching out of the Chaman fault system, and grew into a major earthquake along a 50 degrees north-dipping thrust fault with significant along-strike curvature. Fault slip propagated at an average speed of 3.0 km/s for about 180 km and is concentrated in the top 10 km with no displacement on the underlying decollement. This earthquake does not exhibit significant slip deficit near the surface, nor is there significant segmentation of the rupture. We propose that complex interaction between the subduction accommodating the Arabia-Eurasia convergence to the south and the Ornach Nal fault plate boundary between India and Eurasia resulted in the significant strain gradient observed prior to this earthquake. Convergence in this region is accommodated both along the subduction megathrust and as internal deformation of the accretionary wedge. C1 [Jolivet, R.; Duputel, Z.; Riel, B.; Simons, M.; Minson, S. E.; Zhang, H.; Aivazis, M. A. G.] CALTECH, Dept Geol & Planetary Sci, Seismol Lab, Pasadena, CA 91125 USA. [Ayoub, F.; Leprince, S.] CALTECH, Tecton Observ, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. [Rivera, L.] UdS, Inst Phys Globe Strasbourg, Strasbourg, France. [Rivera, L.] CNRS, EOST, UMR 7516, F-75700 Paris, France. [Samsonov, S.] Nat Resources Canada, Ottawa, ON K1A 0Y7, Canada. [Motagh, M.] GFZ, Helmholtz Ctr Potsdam, Dept Geodesy & Remote Sensing, D-14473 Potsdam, Germany. [Fielding, E. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Motagh, M.] Univ Tehran, Dept Surveying & Geomat Engn, Tehran, Iran. RP Jolivet, R (reprint author), CALTECH, Dept Geol & Planetary Sci, Seismol Lab, 1200 E Calif Blvd, Pasadena, CA 91125 USA. RI Duputel, Zacharie/C-2906-2016; OI Duputel, Zacharie/0000-0002-8809-451X; Jolivet, Romain/0000-0002-9896-3651; Samsonov, Sergey/0000-0002-6798-4847; Simons, Mark/0000-0003-1412-6395 FU Tectonics Observatory; National Science Foundation (NSF) [EAR-1118239, EAR-0529922]; Southern California Earthquake Center (SCEC); United States Geological Survey [07HQAG0008]; Gordon and Betty Moore Foundation; German Aerospace Agency (DLR) [Motagh-GEO1217]; National Aeronautics and Space Administration Earth Surface and Interior focus area FX Part of R. J. and L. R.'s funding were provided by the Tectonics Observatory. This research was supported by National Science Foundation (NSF) Grant EAR-1118239. This research was supported by the Southern California Earthquake Center (SCEC). SCEC is funded by NSF Cooperative Agreement EAR-0529922 and United States Geological Survey Cooperative Agreement 07HQAG0008. This is SCEC contribution 1899. This research was partly supported by the Gordon and Betty Moore Foundation. We thank the Canadian Space Agency for providing RADARSAT-2 data. TerraSAR-X original data are copyrighted by the German Aerospace Agency (DLR) and were provided under project Motagh-GEO1217. Part of this research was supported by the National Aeronautics and Space Administration Earth Surface and Interior focus area and performed by the Jet Propulsion Laboratory, California Institute of Technology. We thank J.-P. Avouac, J.-P. Ampuero, and H. Kanamori for their constructive comments and contributions. We thank the Associate Editor R. Burgmann, R. Bilham (reviewer), and an anonymous reviewer for their constructive comments, which helped improve this manuscript. NR 38 TC 26 Z9 26 U1 1 U2 14 PU SEISMOLOGICAL SOC AMER PI ALBANY PA 400 EVELYN AVE, SUITE 201, ALBANY, CA 94706-1375 USA SN 0037-1106 EI 1943-3573 J9 B SEISMOL SOC AM JI Bull. Seismol. Soc. Amer. PD APR PY 2014 VL 104 IS 2 BP 1020 EP 1030 DI 10.1785/0120130313 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AE0QU UT WOS:000333672000032 ER PT J AU Fletcher, LE Valdivia-Silva, JE Perez-Montano, S Condori-Apaza, RM Conley, CA Navarro-Gonzalez, R McKay, CP AF Fletcher, Lauren E. Valdivia-Silva, Julio E. Perez-Montano, Saul Condori-Apaza, Renee M. Conley, Catharine A. Navarro-Gonzalez, Rafael McKay, Christopher P. TI Field method for rapid quantification of labile organic carbon in hyper-arid desert soils validated by two thermal methods SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY LA English DT Article DE organic-variability; acid hydrolysis permanganate oxidation; hyper-arid extreme environments; thermal methods; labile soil organic carbon ID MARS-LIKE SOILS; ATACAMA DESERT; PERMANGANATE OXIDATIONS; MASS-SPECTROMETRY; MICROBIAL LIFE; SULFURIC-ACID; TAYLOR VALLEY; MINERAL SOILS; MATTER; HYDROLYSIS AB The objective of this work was to develop a field method for the determination of labile organic carbon in hyper-arid desert soils. Industry standard methods rely on expensive analytical equipment that are not possible to take into the field, while scientific challenges require fast turn-around of large numbers of samples in order to characterize the soils throughout this region. Here we present a method utilizing acid-hydrolysis extraction of the labile fraction of organic carbon followed by potassium permanganate oxidation, which provides a quick and inexpensive approach to investigate samples in the field. Strict reagent standardization and calibration steps within this method allowed the determination of very low levels of organic carbon in hyper-arid soils, in particular, with results similar to those determined by the alternative methods of Calcination and Pyrolysis-Gas Chromatography-Mass Spectrometry. Field testing of this protocol increased the understanding of the role of organic materials in hyper-arid environments and allowed real-time, strategic decision making for planning for more detailed laboratory-based analysis. C1 [Fletcher, Lauren E.] Univ Oxford, Clarendon Lab, AOPP, Oxford OX1 3PU, England. [Fletcher, Lauren E.; Valdivia-Silva, Julio E.; Perez-Montano, Saul; McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Valdivia-Silva, Julio E.; Navarro-Gonzalez, Rafael] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Lab Quim Plasmas & Estudios Planetarios, Mexico City 04510, DF, Mexico. [Perez-Montano, Saul] San Jose State Univ, Dept Chem, San Jose, CA 95192 USA. [Condori-Apaza, Renee M.] Univ Nacl San Agustin, Arequipa, Peru. [Conley, Catharine A.] NASA Headquarters, Sci Mission Directorate, Planetary Sci Div, Washington, DC USA. RP Fletcher, LE (reprint author), Univ Oxford, Clarendon Lab, AOPP, Parks Rd, Oxford OX1 3PU, England. EM Lauren@atm.ox.ac.uk RI Gonzalez, Rafael/D-1748-2009; OI CONDORI APAZA, RENEE/0000-0002-1097-5026 FU NASA ASTEP programme FX We would like to thank Dr Benito Gomez for many years of support and access to the Yungay Desert Research Station, Chile; to Antonio Ballon, for his help in the collection of samples, and to two anonymous reviewers whose suggestions greatly improved this manuscript. Acknowledgement is given to the NASA ASTEP programme for providing partial funds in support of this research work. NR 66 TC 1 Z9 1 U1 3 U2 14 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1473-5504 EI 1475-3006 J9 INT J ASTROBIOL JI Int. J. Astrobiol. PD APR PY 2014 VL 13 IS 2 SI SI BP 182 EP 189 DI 10.1017/S1473550414000019 PG 8 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AE1SJ UT WOS:000333749700011 ER PT J AU Smith, GL Daniels, JL Priestley, KJ Thomas, S AF Smith, G. Louis Daniels, Janet L. Priestley, Kory J. Thomas, Susan TI Point response function of the Clouds and Earth Radiant Energy System scanning radiometer SO JOURNAL OF APPLIED REMOTE SENSING LA English DT Article DE point response function; Clouds And Earth Radiant Energy System; Terra; Aqua; Suomi-NPP; image processing ID THERMISTOR BOLOMETER SENSORS; CERES; VALIDATION; ALGORITHM AB An overview of work related to the point response function (PRF) of the Clouds and Earth Radiant Energy System (CERES) scanning radiometer is presented. The aspects of the CERES design that affect the PRF are described, and then the design of the PRF is explained. The PRF was designed by shaping the field of view so as to minimize the blur plus alias errors of the radiance field reconstructed from the CERES measurements. The design is conducted in the Fourier domain. The PRF can then be computed by transforming the resulting transfer function to the physical domain. Alternatively, the PRF can be computed in the physical plane. The PRF of each model of the CERES instrument has been tested in the Radiation Calibration Facility by use of a PRF source and compared well with prediction. CERES instruments are aboard the Terra, Aqua, and Suomi-NPP spacecraft. In orbit, lunar observations are used to validate the PRF. These results showed nominal performance except for the longwave window channel of flight model 2, for which a region of anomalously high sensitivity was found. (c) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI. C1 [Smith, G. Louis; Daniels, Janet L.; Thomas, Susan] Sci Syst Applicat Inc, Hampton, VA 23666 USA. [Priestley, Kory J.] NASA, Sci Directorate, Langley Res Ctr, Hampton, VA 23681 USA. RP Smith, GL (reprint author), Sci Syst Applicat Inc, 1 Execut Dr, Hampton, VA 23666 USA. EM George.l.smith@nasa.gov FU Science Directorate of Langley Research Centre and to the Science Mission Directorate of the Earth Science Division of NASA FX The authors are grateful to the Science Directorate of Langley Research Centre and to the Science Mission Directorate of the Earth Science Division of NASA for the support of the CERES Project. We also thank the engineers and technicians at the Space Division of TRW (presently Northrop-Grumann) for their round-the-clock session with the RCF, the CERES Flight Operations Team at LaRC for collecting the data, and the CERES Instrument Working Group for analyzing all of the measurements. NR 23 TC 1 Z9 1 U1 1 U2 8 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1931-3195 J9 J APPL REMOTE SENS JI J. Appl. Remote Sens. PD APR 1 PY 2014 VL 8 AR 084991 DI 10.1117/1.JRS.8.084991 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AD9DM UT WOS:000333564900001 ER PT J AU Guo, YJ Jiang, XA Waliser, DE AF Guo, Yanjuan Jiang, Xianan Waliser, Duane E. TI Modulation of the Convectively Coupled Kelvin Waves over South America and the Tropical Atlantic Ocean in Association with the Madden-Julian Oscillation SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article DE Intraseasonal variability; Madden-Julian oscillation; Tropical variability ID TOGA-COARE IOP; INTRASEASONAL OSCILLATION; EQUATORIAL WAVES; WESTERN PACIFIC; VERTICAL STRUCTURE; DEEP CONVECTION; CLOUD CLUSTERS; WATER-VAPOR; MJO; MODEL AB In this study, evidence of the strong modulation of the convectively coupled Kelvin wave (CCKW) activity by the Madden-Julian oscillation (MJO) is presented, with a particular focus over the South America and tropical Atlantic region. The MJO impacts on CCKWs over this region, as noted in anomalous fields of rainfall as well as vertical profiles of wind, moisture, and temperature, are primarily through the modulation of Kelvin wave amplitude, with secondary effects on vertical structure, and little impact on wavenumber. CCKW activity is enhanced during MJO phases 8, 1, and 2 and damped during MJO phases 4, 5, and 6. Further analyses reveal that the strong modulation of the MJO on the CCKW activity could be largely through two factors: namely, the vertical zonal wind shear and the lower- to middle-tropospheric specific humidity. The CCKW activity tends to be enhanced during MJO phases when the easterly vertical wind shear and positive low- to midtroposphere moisture anomalies are present and vice versa. These two physical processes associated with the MJO are found to have positively (negatively) reinforcing influences on the CCKW activity in phase 1 (4 and 5), while counteracting influences in phases 2, 3, 6, 7, and 8, leading to the observed MJO cycle of the CCKW activity anomalies in the study region. The results presented in this study may have important implications for extended-range prediction of tropical wave activity and might suggest possible roles of the upstream CCKWs in the initiation of the MJO in the western Indian Ocean. C1 [Guo, Yanjuan; Jiang, Xianan; Waliser, Duane E.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. [Guo, Yanjuan; Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Guo, YJ (reprint author), CALTECH, Jet Prop Lab, M-S 233-304,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM yguo@jifresse.ucla.edu FU Marine Meteorology Program of the Office of Naval Research [ONRBAA12-001]; NSF Climate and Large-Scale Dynamics Program [AGS-1221013, AGS-1228302]; NOAA MAPP Program [NA12OAR4310075]; National Aeronautics and Space Administration FX This work was supported by the Marine Meteorology Program of the Office of Naval Research under Project ONRBAA12-001, NSF Climate and Large-Scale Dynamics Program under Awards AGS-1221013 and AGS-1228302, and NOAA MAPP Program under Award NA12OAR4310075. The contribution from D. Waliser to this study was performed on behalf of the Joint Institute for Regional Earth Science and Engineering (JIFRESSE) at the University of California, Los Angeles, and the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 56 TC 8 Z9 8 U1 1 U2 18 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 EI 1520-0469 J9 J ATMOS SCI JI J. Atmos. Sci. PD APR PY 2014 VL 71 IS 4 BP 1371 EP 1388 DI 10.1175/JAS-D-13-0215.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AD7KG UT WOS:000333442100009 ER PT J AU Potter, C AF Potter, Christopher TI Microclimate influences on vegetation water availability and net primary production in coastal ecosystems of Central California SO LANDSCAPE ECOLOGY LA English DT Article DE Plant production; Soil moisture; Remote sensing; MODIS; Big Sur; Central California Coast ID SUMMER FOG; SATELLITE; DROUGHT; BIOMASS; FOREST; MODEL; CLIMATE; CLASSIFICATION; VARIABILITY; GRASSLAND AB Field sampling and satellite remote sensing were used to test the hypothesis that site microclimate variability leading to divergent soil water use by vegetation types is closely associated with variability in annual net primary productivity (NPP) at the landscape scale. A simulation model based on satellite observations of seasonal phenology was used to estimate NPP of grassland, shrubland, and conifer forest vegetation types on the Central California coast near Big Sur. Daily microclimate at the soil surface was monitored over 4 years (2008-2011) for each vegetation type to infer soil moisture controls on plant production. Grassland soils were found to have lower soil organic matter content and were subjected to extreme radiation and wind events, and thereby dry-down faster with daily spring-summer warming than do shrubland or redwood forest soils. This reduced moisture microclimate affected the water stress on grassland plants to reduce NPP fluxes from April to October each year on the Central Coast far sooner than for shrubland or redwood stands. Results from this study suggested that the satellite-observed canopy greenness variations represented can be used to quantify plant production in coastal ecosystems at the landscape scale of defined microclimate variation. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Potter, C (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM chris.potter@nasa.gov RI Young, Kristina/M-3069-2014 FU NASA Ames Research FX This work was supported by grants from NASA Ames Research. The author acknowledges assistance from the US Forest Service, Los Padres National Forest (Ecosystem Manager Jeff Kwasny) for access to the Brazil Ranch property. The author thanks Shuang Li for assistance with the CASA Express model runs, and acknowledges assistance in field sample collections from Cyrus Hiatt, Lisa Mammel, Cole Potter, Enza Potter, and Stephen Rosenfield. CASA model data sets are available online at http://geo.arc.nasa.gov/sge/casa/, as part of the NASA Carbon Query and Evaluation Support Tools (CQUEST) project. NR 33 TC 5 Z9 5 U1 5 U2 72 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0921-2973 EI 1572-9761 J9 LANDSCAPE ECOL JI Landsc. Ecol. PD APR PY 2014 VL 29 IS 4 BP 677 EP 687 DI 10.1007/s10980-014-0002-6 PG 11 WC Ecology; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA AD8RR UT WOS:000333533800010 ER PT J AU Shindell, DT AF Shindell, Drew T. TI Inhomogeneous forcing and transient climate sensitivity SO NATURE CLIMATE CHANGE LA English DT Article ID FUTURE; MODEL; SIMULATIONS; SCENARIOS; SPREAD; CMIP5 AB Understanding climate sensitivity is critical to projecting climate change in response to a given forcing scenario. Recent analyses(1-3) have suggested that transient climate sensitivity is at the low end of the present model range taking into account the reduced warming rates during the past 10-15 years during which forcing has increased markedly(4). In contrast, comparisons of modelled feedback processes with observations indicate that the most realistic models have higher sensitivities(5,6). Here I analyse results from recent climate modelling intercomparison projects to demonstrate that transient climate sensitivity to historical aerosols and ozone is substantially greater than the transient climate sensitivity to CO2. This enhanced sensitivity is primarily caused by more of the forcing being located at Northern Hemisphere middle to high latitudes where it triggers more rapid land responses and stronger feedbacks. I find that accounting for this enhancement largely reconciles the two sets of results, and I conclude that the lowest end of the range of transient climate response to CO2 in present models and assessments(7) (<1.3 degrees C) is very unlikely. C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Shindell, DT (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM drew.t.shindell@nasa.gov RI Shindell, Drew/D-4636-2012 FU NASA's Modeling, Analysis and Prediction Program FX I acknowledge the World Climate Research Programme's Working Group on Coupled Modelling and the US Department of Energy's Program for Climate Model Diagnosis and Intercomparison, and I thank the climate modelling groups from CMIP and the Atmospheric Chemistry and Climate Model Intercomparison Project (listed in Supplementary Table 1) for making available their model output. I thank G. Faluvegi and G. Milly for assistance with data analysis and US taxpayers and D. Considine for their support through NASA's Modeling, Analysis and Prediction Program. NR 30 TC 47 Z9 47 U1 2 U2 48 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1758-678X EI 1758-6798 J9 NAT CLIM CHANGE JI Nat. Clim. Chang. PD APR PY 2014 VL 4 IS 4 BP 274 EP 277 DI 10.1038/NCLIMATE2136 PG 4 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AE0PY UT WOS:000333669600020 ER PT J AU Martucci, M Boezio, M Bravar, U Carbone, R Christian, ER De Nolfo, GA Merge, M Mocchiutti, E Munini, R Ricci, M Ryan, JM Sotgiu, A Stochaj, S Thakur, N Adriani, O Barbarino, GC Bazilevskaya, GA Bellotti, R Bogomolov, EA Bongi, M Bonvicini, V Bottai, S Bruno, A Cafagna, F Campana, D Carlson, P Casolino, M Castellini, G De Donato, C De Pascale, MP De Santis, C De Simone, N Di Felice, V Formato, V Galper, AM Karelin, AV Koldashov, SV Koldobskiy, S Krutkov, Y Kvashnin, AN Leonov, A Malakhov, V Marcelli, L Mayorov, AG Menn, W Mikhailov, VV Monaco, A Mori, N Osteria, G Palma, F Papini, P Pearce, M Picozza, P Pizzolotto, C Ricciarini, SB Sarkar, R Scotti, V Simon, M Sparvoli, R Spillantini, P Stozhkov, YI Vacchi, A Vannuccini, E Vasilyev, G Voronov, SA Yurkin, YT Zampa, G Zampa, N Zverev, VG AF Martucci, M. Boezio, M. Bravar, U. Carbone, R. Christian, E. R. De Nolfo, G. A. Merge, M. Mocchiutti, E. Munini, R. Ricci, M. Ryan, J. M. Sotgiu, A. Stochaj, S. Thakur, N. Adriani, O. Barbarino, G. C. Bazilevskaya, G. A. Bellotti, R. Bogomolov, E. A. Bongi, M. Bonvicini, V. Bottai, S. Bruno, A. Cafagna, F. Campana, D. Carlson, P. Casolino, M. Castellini, G. De Donato, C. De Pascale, M. P. De Santis, C. De Simone, N. Di Felice, V. Formato, V. Galper, A. M. Karelin, A. V. Koldashov, S. V. Koldobskiy, S. Krutkov, Y. Kvashnin, A. N. Leonov, A. Malakhov, V. Marcelli, L. Mayorov, A. G. Menn, W. Mikhailov, V. V. Monaco, A. Mori, N. Osteria, G. Palma, F. Papini, P. Pearce, M. Picozza, P. Pizzolotto, C. Ricciarini, S. B. Sarkar, R. Scotti, V. Simon, M. Sparvoli, R. Spillantini, P. Stozhkov, Y. I. Vacchi, A. Vannuccini, E. Vasilyev, G. Voronov, S. A. Yurkin, Y. T. Zampa, G. Zampa, N. Zverev, V. G. TI Analysis on H spectral shape during the early 2012 SEPs with the PAMELA experiment SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article; Proceedings Paper CT 4th Roma International Conference on Astroparticle Physics (RICAP) CY MAY 22-24, 2013 CL Roma, ITALY DE PAMELA; SEPs; Protons ID PARTICLE EVENTS; ACCELERATION; HELIOSPHERE AB The satellite-borne PAMELA experiment has been continuously collecting data since 2006. This apparatus is designed to study charged particles in the cosmic radiation. The combination of a permanent magnet, a silicon strip tracker and a silicon-tungsten imaging calorimeter, and the redundancy of instrumentation allow very precise studies on the physics of cosmic rays in a wide energy range and with high statistics. This makes PAMELA a very suitable instrument for Solar Energetic Particle (SEP) observations. Not only does it span the energy range between the ground-based neutron monitor data and the observations of SEPs from space, but PAMELA also carries out the first direct measurements of the composition for the highest energy SEP events, including those causing Ground Level Enhancements (GLEs). In particular, PAMELA has registered many SEP events during solar cycle 24, offering unique opportunities to address the question of high-energy SEP origin. A preliminary analysis on proton spectra behaviour during this event is presented in this work.(C) 2013 Elsevier B.V. All rights reserved. C1 [Adriani, O.; Bongi, M.; Spillantini, P.] Univ Florence, Dept Phys, I-50019 Florence, Italy. [Adriani, O.; Bongi, M.; Bottai, S.; Mori, N.; Papini, P.; Ricciarini, S. B.; Spillantini, P.; Vannuccini, E.] Ist Nazl Fis Nucl, Sez Florence, I-50019 Florence, Italy. [Barbarino, G. C.; Scotti, V.] Univ Naples Federico II, Dept Phys, I-80126 Naples, Italy. [Barbarino, G. C.; Campana, D.; Osteria, G.; Scotti, V.] Ist Nazl Fis Nucl, Sez Naples, I-80126 Naples, Italy. [Bazilevskaya, G. A.; Kvashnin, A. N.; Stozhkov, Y. I.] PN Lebedev Phys Inst, RU-119991 Moscow, Russia. [Bellotti, R.] Univ Bari, Dept Phys, I-70126 Bari, Italy. [Bellotti, R.; Bruno, A.; Cafagna, F.; Monaco, A.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Boezio, M.; Carbone, R.; Mocchiutti, E.; Munini, R.; Bonvicini, V.; Formato, V.; Pizzolotto, C.; Sarkar, R.; Vacchi, A.; Zampa, G.; Zampa, N.] Ist Nazl Fis Nucl, Sez Trieste, I-34149 Trieste, Italy. [Bogomolov, E. A.; Krutkov, Y.; Vasilyev, G.] AF Ioffe Phys Tech Inst, RU-194021 St Petersburg, Russia. [Carlson, P.; Pearce, M.] KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Carlson, P.; Pearce, M.] AlbaNova Univ Ctr, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Merge, M.; Casolino, M.; De Donato, C.; De Pascale, M. P.; De Santis, C.; De Simone, N.; Di Felice, V.; Palma, F.; Picozza, P.; Sparvoli, R.] Ist Nazl Fis Nucl, Sez Rome Tor Vergata, I-00133 Rome, Italy. [Casolino, M.] RIKEN, Adv Sci Inst, Wako, Saitama, Japan. [Castellini, G.] IFAC, I-50019 Florence, Italy. [Martucci, M.; Merge, M.; Sotgiu, A.; De Pascale, M. P.; De Santis, C.; Marcelli, L.; Palma, F.; Picozza, P.; Sparvoli, R.] Univ Roma Tor Vergata, Dept Phys, I-00133 Rome, Italy. [Munini, R.; Formato, V.] Univ Trieste, Dept Phys, I-34147 Trieste, Italy. [Galper, A. M.; Karelin, A. V.; Koldashov, S. V.; Koldobskiy, S.; Leonov, A.; Malakhov, V.; Mayorov, A. G.; Mikhailov, V. V.; Voronov, S. A.; Yurkin, Y. T.; Zverev, V. G.] NRNU MEPhI, RU-115409 Moscow, Russia. [Martucci, M.; Ricci, M.] Ist Nazl Fis Nucl, Lab Nazl Frascati, I-00044 Frascati, Italy. [Menn, W.; Simon, M.] Univ Siegen, Dept Phys, D-57068 Siegen, Germany. [Pizzolotto, C.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Pizzolotto, C.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Frascati, Italy. [Bravar, U.; Ryan, J. M.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Stochaj, S.] New Mexico State Univ, Las Cruces, NM 88003 USA. [Christian, E. R.; De Nolfo, G. A.; Thakur, N.] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD USA. RP Martucci, M (reprint author), Univ Roma Tor Vergata, Dept Phys, I-00133 Rome, Italy. EM matteo.martucci@roma2.infn.it RI de Nolfo, Georgia/E-1500-2012; Vasilyev, Gennady/E-4843-2014; Krutkov, Sergey/E-7561-2014; De Santis, Cristian/C-1210-2011; Mocchiutti, Emiliano/I-8049-2013; Cafagna, Francesco/A-9299-2010; Vacchi, Andrea/C-1291-2010; Mikhailov, Vladimir/B-5368-2014; De Donato, Cinzia/J-9132-2015; Palma, Francesco/K-3224-2015; Barbarino, Giancarlo/L-2559-2015; Bazilevskaya, Galina/M-6175-2015; Stozhkov, Yuri/M-7433-2015; Bongi, Massimo/L-9417-2015; Leonov, Alexey/E-4698-2016; Galper, Arkady/M-9610-2015; Koldobskiy, Sergey/K-6507-2015; marcelli, laura/K-8860-2016; Pizzolotto, Cecilia/G-5821-2013; Di Felice, Valeria/L-2989-2016; Mori, Nicola/D-9459-2016; Karelin, Alexander/O-6576-2016; Mayorov, Andrey/M-1207-2016; Voronov, Sergey/P-9654-2016; Malakhov, Vitaly/Q-6730-2016; Kvashnin, Aleksandr/M-8673-2015; OI Bellotti, Roberto/0000-0003-3198-2708; Papini, Paolo/0000-0003-4718-2895; Boezio, Mirko/0000-0002-8015-2981; De Santis, Cristian/0000-0002-7280-2446; Mocchiutti, Emiliano/0000-0001-7856-551X; Cafagna, Francesco/0000-0002-7450-4784; Vacchi, Andrea/0000-0003-3855-5856; Mikhailov, Vladimir/0000-0003-3851-2901; De Donato, Cinzia/0000-0002-9725-1281; Palma, Francesco/0000-0001-7076-8830; Barbarino, Giancarlo/0000-0001-9253-3397; Bongi, Massimo/0000-0002-6050-1937; Koldobskiy, Sergey/0000-0001-9187-0383; marcelli, laura/0000-0002-3180-1228; Pizzolotto, Cecilia/0000-0003-0200-2408; Mori, Nicola/0000-0003-2138-3787; Voronov, Sergey/0000-0002-9209-0618; casolino, marco/0000-0001-6067-5104; Ricciarini, Sergio Bruno/0000-0001-6176-3368; Kvashnin, Aleksandr/0000-0001-7218-6738; Castellini, Guido/0000-0002-0177-0643; Monaco, Alfonso/0000-0002-5968-8642; Sparvoli, Roberta/0000-0002-6314-6117; Picozza, Piergiorgio/0000-0002-7986-3321 NR 15 TC 2 Z9 2 U1 4 U2 23 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 APR 1 PY 2014 VL 742 BP 158 EP 161 DI 10.1016/j.nima.2013.11.078 PG 4 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA AE2BK UT WOS:000333778100027 ER PT J AU Bolmont, J Vasileiou, V Jacholkowska, A Piron, E Couturier, C Granot, J Stecker, FW Cohen-Tanugi, J Longo, F AF Bolmont, J. Vasileiou, V. Jacholkowska, A. Piron, E. Couturier, C. Granot, J. Stecker, F. W. Cohen-Tanugi, J. Longo, F. TI Lorentz invariance violation: The latest Fermi results and the GRB/AGN complementarity SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article; Proceedings Paper CT 4th Roma International Conference on Astroparticle Physics (RICAP) CY MAY 22-24, 2013 CL Roma, ITALY DE Quantum gravity; Lorentz invariance violation; Fermi-LAT; Gamma-ray burst ID HIGH-ENERGY; PHOTONS; LIGHT AB Because they are bright and distant, Gamma-ray Bursts (GRBs) have been used for more than a decade to test propagation of photons and to constrain relevant Quantum Gravity (QG) models in which the velocity of photons in vacuum can depend on their energy. With its unprecedented sensitivity and energy coverage, the Fermi satellite has provided the most constraining results on the QG energy scale so far. In this talk, the latest results obtained from the analysis of four bright GRBs observed by the Large Area Telescope will be reviewed: These robust results, cross-checked using three different analysis techniques set the limit on QG energy scale at E-QG,E-1 > 7.6 times the Planck energy for linear dispersion and E-QG,E-2 > 1.3 x 10(11) GeV for quadratic dispersion (95% CL). After describing the data and the analysis techniques in use, results will be discussed and confronted to latest constraints obtained with Active Galactic Nuclei. (C) 2013 Elsevier B.V. All rights reserved. C1 [Bolmont, J.; Jacholkowska, A.; Couturier, C.] Univ Paris 07, Univ Paris 06, LPNHE, CNRS,IN2P3, F-75221 Paris 05, France. [Vasileiou, V.; Piron, E.; Cohen-Tanugi, J.] Univ Montpellier 2, CNRS, LUPM, IN2P3, F-34095 Montpellier 5, France. [Granot, J.] Open Univ Israel, Dept Nat Sci, Raanana, Israel. [Stecker, F. W.] Univ Calif, NASA Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD USA. [Longo, F.] Univ Trieste, Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. RP Bolmont, J (reprint author), Univ Paris 07, Univ Paris 06, LPNHE, CNRS,IN2P3, F-75221 Paris 05, France. EM bolmont@in2p3.fr FU NASA, United States; DOE, United States; CEA/Irfu, France; IN2P3/CNRS, France; ASI, Italy; INFN, Italy; MEXT, Japan; KEK, Japan; JAXA, Japan; K.A. Wallenberg Foundation, Sweden; Swedish Research Council, Sweden; National Space Board, Sweden FX The Fermi LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K.A. Wallenberg Foundation, the Swedish Research Council and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged. NR 17 TC 1 Z9 1 U1 0 U2 3 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 APR 1 PY 2014 VL 742 BP 165 EP 168 DI 10.1016/j.nima.2013.10.088 PG 4 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA AE2BK UT WOS:000333778100029 ER PT J AU Mayer, CSJ Fasel, HF Choudhari, M Chang, CL AF Mayer, Christian S. J. Fasel, Hermann F. Choudhari, Meelan Chang, Chau-Lyan TI Transition Onset Predictions for Oblique Breakdown in a Mach 3 Boundary Layer SO AIAA JOURNAL LA English DT Article C1 [Mayer, Christian S. J.; Fasel, Hermann F.] Univ Arizona, Dept Aerosp & Mech Engn, Tucson, AZ 85721 USA. [Choudhari, Meelan; Chang, Chau-Lyan] NASA Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA. RP Mayer, CSJ (reprint author), ExxonMobil Upstream Res Co, Drilling & Subsurface, Houston, TX 77252 USA. RI Choudhari, Meelan/F-6080-2017 OI Choudhari, Meelan/0000-0001-9120-7362 FU U.S. Air Force Office for Scientific Research [FA9550-08-1-0211]; NASA [NNX07AC66A] FX This work was funded by the U.S. Air Force Office for Scientific Research under grant FA9550-08-1-0211 and by the Supersonics Project of NASA's Fundamental Aeronautics Program under cooperative agreement NNX07AC66A. The computer hours and the technical support provided by NASA Ames Research Center are gratefully acknowledged. NR 9 TC 1 Z9 1 U1 0 U2 1 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD APR PY 2014 VL 52 IS 4 BP 882 EP 885 DI 10.2514/1.J051966 PG 4 WC Engineering, Aerospace SC Engineering GA AD0YI UT WOS:000332960100020 ER PT J AU Weijerman, M Birkeland, C Piniak, GA Miller, MW Eakin, CM McElhany, P Dunlap, MJ Patterson, M Brainard, RE AF Weijerman, Mariska Birkeland, Charles Piniak, Gregory A. Miller, Margaret W. Eakin, C. Mark McElhany, Paul Dunlap, Matthew J. Patterson, Matt Brainard, Russell E. TI Endangered Species Act listing: three case studies of data deficiencies and consequences of ESA 'threatened' listing on research output SO CURRENT OPINION IN ENVIRONMENTAL SUSTAINABILITY LA English DT Article ID REGION-WIDE DECLINES; DEEP-SEA CORALS; CLIMATE-CHANGE; REEFS AB Determining whether a species warrants listing as threatened or endangered under the U.S. Endangered Species Act depends on the government's assessment of the species' extinction risk, usually in response to a petition. Deciding whether data are sufficient to make a listing determination is a challenging part of the process. We examined three case studies involving corals. A petition for deep-sea corals was rejected for full status review of the species, based on insufficient information on population trends and threats. Information on threats for 82 tropical corals was sufficient to propose listing of 66 species. Significant population declines and identified threats resulted in listing two Atlantic Acropora corals as 'Threatened'. There was no decrease in journal publication rate on the Acropora species after that listing, and no decrease in research permit applications in marine protected areas. However, the effects of listings on research that might help to sustain or recover species remains largely unknown. C1 [Weijerman, Mariska; Dunlap, Matthew J.] Univ Hawaii, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA. [Weijerman, Mariska] Wageningen Univ, Environm Syst Anal Grp, NL-6700 AA Wageningen, Netherlands. [Birkeland, Charles] Univ Hawaii, Dept Biol, Honolulu, HI 96822 USA. [Piniak, Gregory A.] Natl Ocean Serv, Natl Ctr Coastal Ocean Sci, Silver Spring, MD 20910 USA. [Miller, Margaret W.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Miami, FL 33149 USA. [Eakin, C. Mark] NOAA Coral Reef Watch, Ctr Satellite Applicat & Res, College Pk, MD 20740 USA. [McElhany, Paul] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Seattle, WA 98112 USA. [Patterson, Matt] Natl Pk Serv, Palmetto, FL 33157 USA. [Brainard, Russell E.] Natl Marine Fisheries Serv, Pacif Islands Fisheries Sci Ctr, Honolulu, HI 96814 USA. RP Weijerman, M (reprint author), Univ Hawaii, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA. EM mariska.weijerman@noaa.gov RI Eakin, C. Mark/F-5585-2010 NR 29 TC 2 Z9 2 U1 2 U2 24 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1877-3435 EI 1877-3443 J9 CURR OPIN ENV SUST JI Curr. Opin. Environ. Sustain. PD APR PY 2014 VL 7 BP 15 EP 21 DI 10.1016/j.cosust.2013.11.026 PG 7 WC GREEN & SUSTAINABLE SCIENCE & TECHNOLOGY; Environmental Sciences SC Science & Technology - Other Topics; Environmental Sciences & Ecology GA AE5HV UT WOS:000334019300004 ER PT J AU Simon, DL Borguet, S Leonard, O Zhang, XD AF Simon, Donald L. Borguet, Sebastien Leonard, Olivier Zhang, Xiaodong (Frank) TI Aircraft Engine Gas Path Diagnostic Methods: Public Benchmarking Results SO JOURNAL OF ENGINEERING FOR GAS TURBINES AND POWER-TRANSACTIONS OF THE ASME LA English DT Article AB Recent technology reviews have identified the need for objective assessments of aircraft engine health management (EHM) technologies. To help address this issue, a gas path diagnostic benchmark problem has been created and made publicly available. This software tool, referred to as the Propulsion Diagnostic Method Evaluation Strategy (ProDiMES), has been constructed based on feedback provided by the aircraft EHM community. It provides a standard benchmark problem enabling users to develop, evaluate, and compare diagnostic methods. This paper will present an overview of ProDiMES along with a description of four gas path diagnostic methods developed and applied to the problem. These methods, which include analytical and empirical diagnostic techniques, will be described and associated blind-test-case metric results will be presented and compared. Lessons learned along with recommendations for improving the public benchmarking processes will also be presented and discussed. C1 [Simon, Donald L.] NASA, Controls & Dynam Branch, Glenn Res Ctr, Cleveland, OH 44135 USA. [Borguet, Sebastien; Leonard, Olivier] Univ Liege, Turbomachinery Grp, B-4000 Liege, Belgium. [Zhang, Xiaodong (Frank)] Wright State Univ, Russ Engn Ctr 335, Dept Elect Engn, Dayton, OH 45435 USA. RP Simon, DL (reprint author), NASA, Controls & Dynam Branch, Glenn Res Ctr, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA. NR 13 TC 3 Z9 3 U1 1 U2 8 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 0742-4795 EI 1528-8919 J9 J ENG GAS TURB POWER JI J. Eng. Gas. Turbines Power-Trans. ASME PD APR PY 2014 VL 136 IS 4 AR 041201 DI 10.1115/1.4025482 PG 10 WC Engineering, Mechanical SC Engineering GA AD2CR UT WOS:000333041200001 ER PT J AU Rudin, C Wagstaff, KL AF Rudin, Cynthia Wagstaff, Kiri L. TI Machine learning for science and society SO MACHINE LEARNING LA English DT Editorial Material ID KNOWLEDGE DISCOVERY; DATABASES AB The special issue on "Machine Learning for Science and Society" showcases machine learning work with influence on our current and future society. These papers address several key problems such as how we perform repairs on critical infrastructure, how we predict severe weather and aviation turbulence, how we conduct tax audits, whether we can detect privacy breaches in access to healthcare data, and how we link individuals across census data sets for new insights into population changes. In this introduction, we discuss the need for such a special issue within the context of our field and its relationship to the broader world. In the era of "big data," there is a need for machine learning to address important large-scale applied problems, yet it is difficult to find top venues in machine learning where such work is encouraged. We discuss the ramifications of this contradictory situation and encourage further discussion on the best strategy that we as a field may adopt. We also summarize key lessons learned from individual papers in the special issue so that the community as a whole can benefit. C1 [Rudin, Cynthia] MIT, Sloan Sch Management, Cambridge, MA 02142 USA. [Wagstaff, Kiri L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Rudin, C (reprint author), MIT, Sloan Sch Management, 100 Main St, Cambridge, MA 02142 USA. EM rudin@mit.edu; wkiri@jpl.nasa.gov OI Wagstaff, Kiri/0000-0003-4401-5506 NR 32 TC 10 Z9 10 U1 2 U2 25 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0885-6125 EI 1573-0565 J9 MACH LEARN JI Mach. Learn. PD APR PY 2014 VL 95 IS 1 SI SI BP 1 EP 9 DI 10.1007/s10994-013-5425-9 PG 9 WC Computer Science, Artificial Intelligence SC Computer Science GA AD3PI UT WOS:000333157800001 ER PT J AU Ruff, SW Niles, PB Alfano, F Clarke, AB AF Ruff, Steven W. Niles, Paul B. Alfano, Fabrizio Clarke, Amanda B. TI Evidence for a Noachian-aged ephemeral lake in Gusev crater, Mars SO GEOLOGY LA English DT Article ID MARTIAN METEORITE; SPIRIT ROVER; CARBONATES; ALH84001; IDENTIFICATION; SURFACE; MODEL AB Gusev crater has long been considered the site of a lake early in Martian history, but the Mars Exploration Rover Spirit found no apparent evidence of lake deposits along its 7 km traverse from 2004 to 2010. Although outcrops rich in Mg-Fe carbonate, dubbed Comanche, were discovered in the Noachian-aged Columbia Hills, they were inferred to result from volcanic hydrothermal activity. We now find evidence that the alteration of the Comanche outcrops is consistent with evaporative precipitation of low-temperature, near-surface solutions derived from limited water-rock interaction with rocks equivalent to nearby outcrops called Algonquin. Additional observations show that the Algonquin outcrops are remnants of volcanic tephra that covered the Columbia Hills and adjacent plains well before emplacement or basalt flows onto the floor of Gusev crater. Water-limited leaching of formerly widespread Algonquin-like tephra deposits by ephemeral waters, followed by transport and evaporative precipitation of the fluids into the Comanche outcrops, can explain their chemical, mineralogical, and textural characteristics. C1 [Ruff, Steven W.; Alfano, Fabrizio; Clarke, Amanda B.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Niles, Paul B.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Ruff, SW (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. OI Alfano, Fabrizio/0000-0002-9819-4872 FU NASA Mars Data Analysis; Mars Fundamental Research Programs; Early Postdoc.Mobility grant from the Swiss National Science Foundation FX This work was supported in part through grants from the NASA Mars Data Analysis and Mars Fundamental Research Programs. Alfano was supported by an Early Postdoc.Mobility grant from the Swiss National Science Foundation. The comments and suggestions of two anonymous reviewers and the editor strengthened the manuscript. NR 23 TC 10 Z9 10 U1 2 U2 19 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 EI 1943-2682 J9 GEOLOGY JI Geology PD APR PY 2014 VL 42 IS 4 BP 359 EP 362 DI 10.1130/G35508.1 PG 4 WC Geology SC Geology GA AD4TT UT WOS:000333244300025 ER PT J AU Grazier, KR Castillo-Rogez, JC Sharp, PW AF Grazier, Kevin R. Castillo-Rogez, Julie C. Sharp, Philip W. TI Dynamical delivery of volatiles to the outer main belt SO ICARUS LA English DT Article DE Asteroids, composition; Asteroids, dynamics; Ices; Planetesimals; Origin, Solar System ID PRIMORDIAL SOLAR NEBULA; EMBEDDED STAR-CLUSTERS; SURFACE-DENSITY; OORT CLOUD; PLANETESIMALS; EVOLUTION; ICE; MIGRATION; ASTEROIDS; ORGANICS AB We quantify the relative contribution of volatiles supplied from outer Solar System planetesimal reservoirs to large wet asteroids during the first few My after the beginning of the Solar System. To that end, we simulate the fate of planetesimals originating within different regions of the Solar System - and thus characterized by different chemical inventories - using a highly accurate integrator tuned to handle close planet/planetesimal encounters. The fraction of icy planetesimals crossing the Asteroid Belt was relatively significant, and our simulations show that planetesimals originating from the Jupiter/Saturn region were orders of magnitude more abundant than those stemming from the Uranus and Neptune regions when the planets were just embryos. As the planets reached their full masses the Jupiter/Saturn and Saturn/Uranus regions contributed similar fractions of planetesimals for any material remaining in these reservoirs late in the stage of planetary formation, This implies that large asteroids like Ceres accreted very little material enriched in low-eutectic volatiles (e.g., methanol, nitrogen and methane ices, etc.) and clathrate hydrates expected to condense at the very low temperatures predicted for beyond Saturn's orbit in current early solar nebula models. Further, a large fraction of the content in organics of Ceres and neighboring ice-rich objects originates from the outer Solar System. (C) 2014 Published by Elsevier Inc. C1 [Grazier, Kevin R.; Castillo-Rogez, Julie C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sharp, Philip W.] Univ Auckland, Dept Math, Auckland 1, New Zealand. RP Grazier, KR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM kevin_grazier@yahoo.com OI Sharp, Philip/0000-0001-9550-0910 NR 37 TC 4 Z9 4 U1 0 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 APR PY 2014 VL 232 BP 13 EP 21 DI 10.1016/j.icarus.2013.12.011 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC8WJ UT WOS:000332815500002 ER PT J AU Uckert, K Chanover, NJ Olkin, CB Young, LA Hammel, HB Miller, C Bauer, JM AF Uckert, K. Chanover, N. J. Olkin, C. B. Young, L. A. Hammel, H. B. Miller, C. Bauer, J. M. TI An investigation of the temperature variations in Neptune's upper stratosphere including a July 2008 stellar occultation event SO ICARUS LA English DT Article DE Neptune, atmosphere; Occultations; Atmospheres, structure; Tides, atmospheric ID PLANETARY-ATMOSPHERES; ECLIPSING BINARIES; URANUS; TRITON; VOYAGER; RINGS; VARIABILITY; PHOTOMETRY; DISPERSION; EVOLUTION AB We extracted physical atmospheric parameters from a 23 July 2008 single-chord stellar occultation of the star USNO-B1.0 0759-0739128 (I-band magnitude of 12.60) by Neptune using a light curve model fitting technique. We observed the occultation using the Agile CCD camera mounted on the Astrophysical Research Consortium 3.5 m telescope at Apache Point Observatory. We found isothermal temperatures of 116.5 +/- 12.0 K and 154.0 +/- 13.0 K for the immersion and emersion light curve profiles, respectively. We compare the stratospheric temperatures derived from the 2008 occultation to published temperatures of Neptune at similar atmospheric pressures derived from previous stellar occultations observed in the 1980s, and from long-term photometric measurements made routinely since the 1983-1990 occultation campaign. No obvious long-term temporal variation in stratospheric isothermal temperature is present. Fluctuations in the fitted isothermal temperature values, on the order of 20 K, is evident. We explore several hypotheses to explain the observed temperature variability of Neptune's stratosphere, including seasonal variability, variations in the Lyman-alpha flux received at Neptune due to the 11-year solar cycle, diurnal variations, varying insolation due to heliocentric variability, IR and UV heating by hydrocarbons, aerosol precipitation, inertia-gravity wave dissipation, and effects due to atmospheric tidal perturbations by Triton. We investigate the effects of these mechanisms on the gradual temporal changes of Neptune's stratospheric temperature and conclude that local variations in stratospheric temperature during each event, on the order of 20 K, are dominated by viscous dissipation of inertia-gravity waves. (C) 2014 Elsevier Inc. All rights reserved. C1 [Uckert, K.; Chanover, N. J.; Miller, C.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Olkin, C. B.; Young, L. A.] Southwest Res Inst, Boulder, CO 80302 USA. [Hammel, H. B.] Assoc Univ Res Astron, Washington, DC 20005 USA. [Hammel, H. B.] Space Sci Inst, Boulder, CO 80301 USA. [Bauer, J. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Uckert, K (reprint author), New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. EM kuckert@astronomy.nmsu.edu FU NASA [NNX07AV25H] FX This work was supported by funds from NASA Grant NNX07AV25H. We thank Jeffrey Coughlin for the insightful discussions on light curve modeling and use of the JKTEBOP algorithm. We would also like to thank the anonymous reviewers for their helpful suggestions. NR 59 TC 0 Z9 0 U1 1 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD APR PY 2014 VL 232 BP 22 EP 33 DI 10.1016/j.icarus.2014.01.004 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC8WJ UT WOS:000332815500003 ER PT J AU Cuzzi, JN Whizin, AD Hogan, RC Dobrovolskis, AR Dones, L Showalter, MR Colwell, JE Scargle, JD AF Cuzzi, J. N. Whizin, A. D. Hogan, R. C. Dobrovolskis, A. R. Dones, L. Showalter, M. R. Colwell, J. E. Scargle, J. D. TI Saturn's F Ring core: Calm in the midst of chaos SO ICARUS LA English DT Article DE Planetary rings; Satum, rings; Resonances, orbital; Celestial Mechanics ID PLANETARY RINGS; NARROW RINGLETS; PROMETHEUS; SATELLITE; DYNAMICS; MOONLET; RESONANCES; KINEMATICS; EVOLUTION; ORBITS AB The long-term stability of the narrow F Ring core has been hard to understand. Instead of acting as "shepherds", Prometheus and Pandora together stir the vast preponderance of the region into a chaotic state, consistent with the orbits of newly discovered objects like S/2004 S 6. We show how a comb of very narrow radial locations of high stability in semimajor axis is embedded within this otherwise chaotic region. The stability of these semimajor axes relies fundamentally on the unusual combination of rapid apse precession and long synodic period which characterizes the region. This situation allows stable "antiresonances" to fall on or very close to traditional Lindblad resonances which, under more common circumstances, are destabilizing. We present numerical integrations of tens of thousands of test particles over tens of thousands of Prometheus orbits that map out the effect. The stable antiresonance zones are most stable in a subset of the region where Prometheus first-order resonances are least cluttered by Pandora resonances. This region of optimum stability is paradoxically closer to Prometheus than a location more representative of "torque balance", helping explain a longstanding paradox. One stable zone corresponds closely to the currently observed semimajor axis of the F Ring core. Corotation resonance may also play a role. While the model helps explain the stability of the narrow F Ring core, it does not explain why the F Ring material all shares a common apse longitude; we speculate that collisional damping at the preferred semimajor axis (not included in the current simulations) may provide that final step. Essentially, we find that the F Ring core is not confined by a combination of Prometheus and Pandora, but a combination of Prometheus and precession. Published by Elsevier Inc. C1 [Cuzzi, J. N.; Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Whizin, A. D.; Colwell, J. E.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. [Hogan, R. C.] BAERI Inc, Sonoma, CA 95476 USA. [Dobrovolskis, A. R.] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA. [Dones, L.] SWRI Inc, Boulder, CO 80302 USA. [Showalter, M. R.] SETI Inst, Mountain View, CA 94043 USA. RP Cuzzi, JN (reprint author), NASA, Ames Res Ctr, Div Space Sci, Mail Stop 245-3, Moffett Field, CA 94035 USA. EM jeffrey.cuzzi@nasa.gov; awhizin@yahoo.com; anthony.r.dobrovolskis@nasa.gov; luke@boulder.swri.edu; mshowalter@seti.org; jec@ucf.edu; jeffrey.d.scargle@nasa.gov NR 51 TC 3 Z9 3 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD APR PY 2014 VL 232 BP 157 EP 175 DI 10.1016/j.icarus.2013.12.027 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC8WJ UT WOS:000332815500013 ER PT J AU Kent, ST Kabagambe, EK Wadley, VG Howard, VJ Crosson, WL Al-Hamdan, MZ Judd, SE Peace, F McClure, LA AF Kent, Shia T. Kabagambe, Edmond K. Wadley, Virginia G. Howard, Virginia J. Crosson, William L. Al-Hamdan, Mohammad Z. Judd, Suzanne E. Peace, Fredrick McClure, Leslie A. TI The relationship between long-term sunlight radiation and cognitive decline in the REGARDS cohort study SO INTERNATIONAL JOURNAL OF BIOMETEOROLOGY LA English DT Article DE Sunlight; Temperature; Weather; Climate; Remote sensing technology; Cognition ID VITAMIN-D DEFICIENCY; BLOOD-PRESSURE; RACIAL-DIFFERENCES; SOLAR-RADIATION; MOOD DISORDERS; TEMPERATURE; PERFORMANCE; DEPRESSION; MORTALITY; DISEASE AB Sunlight may be related to cognitive function through vitamin D metabolism or circadian rhythm regulation. The analysis presented here sought to test whether ground and satellite measures of solar radiation are associated with cognitive decline. The study used a 15-year residential history merged with satellite and ground monitor data to determine sunlight (solar radiation) and air temperature exposure for a cohort of 19,896 cognitively intact black and white participants aged 45+ from the 48 contiguous United States. Exposures of 15, 10, 5, 2, and 1-year were used to predict cognitive status at the most recent assessment in logistic regression models; 1-year insolation and maximum temperatures were chosen as exposure measures. Solar radiation interacted with temperature, age, and gender in its relationships with incident cognitive impairment. After adjustment for covariates, the odds ratio (OR) of cognitive decline for solar radiation exposure below the median vs above the median in the 3rd tertile of maximum temperatures was 1.88 (95 % CI: 1.24, 2.85), that in the 2nd tertile was 1.33 (95 % CI: 1.09, 1.62), and that in the 1st tertile was 1.22 (95 % CI: 0.92, 1.60). We also found that participants under 60 years old had an OR = 1.63 (95 % CI: 1.20, 2.22), those 60-80 years old had an OR = 1.18 (95 % CI: 1.02, 1.36), and those over 80 years old had an OR = 1.05 (0.80, 1.37). Lastly, we found that males had an OR = 1.43 (95 % CI: 1.22, 1.69), and females had an OR = 1.02 (0.87, 1.20). We found that lower levels of solar radiation were associated with increased odds of incident cognitive impairment. C1 [Kent, Shia T.; Kabagambe, Edmond K.; Howard, Virginia J.] Univ Alabama Birmingham, Dept Epidemiol, Sch Publ Hlth, Birmingham, AL 35294 USA. [Kent, Shia T.; Judd, Suzanne E.; Peace, Fredrick; McClure, Leslie A.] Univ Alabama Birmingham, Dept Biostat, Sch Publ Hlth, Birmingham, AL 35294 USA. [Wadley, Virginia G.] Univ Alabama Birmingham, Dept Med, Birmingham, AL 35294 USA. [Crosson, William L.; Al-Hamdan, Mohammad Z.] NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville, AL 35812 USA. RP Kent, ST (reprint author), Univ Alabama Birmingham, Dept Environm Hlth Sci, Ryals 530,1665 Univ Blvd, Birmingham, AL 35294 USA. EM shia@uab.edu RI McClure, Leslie/P-2929-2015 FU National Institute of Neurological Disorders and Stroke [U01 NS041588]; National Aeronautics and Space Administration [NNX09AV81G] FX The authors thank the other investigators, the staff, and the participants of the REGARDS study for their valuable contributions. A full list of participating REGARDS investigators and institutions can be found at http://www.regardsstudy.org. This research project is supported by a cooperative agreement U01 NS041588 from the National Institute of Neurological Disorders and Stroke. Additional funding, data, data processing, and consultation were provided by an investigator-initiated grant from National Aeronautics and Space Administration (grant# NNX09AV81G). The NLDAS hourly data used in this study were acquired as part of the mission of National Aeronautics and Space Administration's Earth Science Division and archived and distributed by the Goddard Earth Sciences Data and Information Services Center. NR 42 TC 3 Z9 3 U1 5 U2 28 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0020-7128 EI 1432-1254 J9 INT J BIOMETEOROL JI Int. J. Biometeorol. PD APR PY 2014 VL 58 IS 3 BP 361 EP 370 DI 10.1007/s00484-013-0631-5 PG 10 WC Biophysics; Environmental Sciences; Meteorology & Atmospheric Sciences; Physiology SC Biophysics; Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences; Physiology GA AD3EC UT WOS:000333120100006 PM 23340910 ER PT J AU Gherlone, M Cerracchio, P Mattone, M Di Sciuva, M Tessler, A AF Gherlone, Marco Cerracchio, Priscilla Mattone, Massimiliano Di Sciuva, Marco Tessler, Alexander TI An inverse finite element method for beam shape sensing: theoretical framework and experimental validation SO SMART MATERIALS AND STRUCTURES LA English DT Article DE Timoshenko beam theory; shape sensing; frame structures; inverse finite element method; experimental strain ID BRAGG-GRATING SENSORS; STRAIN; SHEAR; RECONSTRUCTION; DISPLACEMENT AB Shape sensing, i.e., reconstruction of the displacement field of a structure from surface-measured strains, has relevant implications for the monitoring, control and actuation of smart structures. The inverse finite element method (iFEM) is a shape-sensing methodology shown to be fast, accurate and robust. This paper aims to demonstrate that the recently presented iFEM for beam and frame structures is reliable when experimentally measured strains are used as input data. The theoretical framework of the methodology is first reviewed. Timoshenko beam theory is adopted, including stretching, bending, transverse shear and torsion deformation modes. The variational statement and its discretization with C-0-continuous inverse elements are briefly recalled. The three-dimensional displacement field of the beam structure is reconstructed under the condition that least-squares compatibility is guaranteed between the measured strains and those interpolated within the inverse elements. The experimental setup is then described. A thin-walled cantilevered beam is subjected to different static and dynamic loads. Measured surface strains are used as input data for shape sensing at first with a single inverse element. For the same test cases, convergence is also investigated using an increasing number of inverse elements. The iFEM-recovered deflections and twist rotations are then compared with those measured experimentally. The accuracy, convergence and robustness of the iFEM with respect to unavoidable measurement errors, due to strain sensor locations, measurement systems and geometry imperfections, are demonstrated for both static and dynamic loadings. C1 [Gherlone, Marco; Cerracchio, Priscilla; Mattone, Massimiliano; Di Sciuva, Marco] Politecn Torino, Dept Mech & Aerosp Engn, I-10129 Turin, Italy. [Tessler, Alexander] NASA Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA. RP Gherlone, M (reprint author), Politecn Torino, Dept Mech & Aerosp Engn, Corso Duca Abruzzi 24, I-10129 Turin, Italy. EM marco.gherlone@polito.it; priscilla.cerracchio@polito.it; massimiliano.mattone@polito.it; marco.disciuva@polito.it; Alexander.Tessler-1@nasa.gov OI Gherlone, Marco/0000-0002-5711-0046 NR 33 TC 6 Z9 6 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0964-1726 EI 1361-665X J9 SMART MATER STRUCT JI Smart Mater. Struct. PD APR PY 2014 VL 23 IS 4 AR 045027 DI 10.1088/0964-1726/23/4/045027 PG 13 WC Instruments & Instrumentation; Materials Science, Multidisciplinary SC Instruments & Instrumentation; Materials Science GA AD0SC UT WOS:000332943400027 ER PT J AU Hruska, Z Yao, HB Kincaid, R Brown, R Cleveland, T Bhatnagar, D AF Hruska, Zuzana Yao, Haibo Kincaid, Russell Brown, Robert Cleveland, Thomas Bhatnagar, Deepak TI Fluorescence Excitation-Emission Features of Aflatoxin and Related Secondary Metabolites and Their Application for Rapid Detection of Mycotoxins SO FOOD AND BIOPROCESS TECHNOLOGY LA English DT Article DE Excitation-emission matrix; Fluorescence hyperspectral imaging; Aflatoxin; Secondary metabolites; Food and feed safety ID GREENISH-YELLOW-FLUORESCENCE; PERFORMANCE LIQUID-CHROMATOGRAPHY; ASPERGILLUS-FLAVUS; OCHRATOXIN-A; COTTON LINT; KOJIC ACID; CORN; CONTAMINATION; MATRIX; CLEANUP AB The persistent occurrence of aflatoxins in food and feed remains a problem for producers of commodities subject to colonization with toxigenic molds. Aflatoxins are secondary metabolites of fungi of the Aspergillus spp. associated with deleterious health effects. Because current screening methods for these toxins are lengthy, destructive, and costly, there is a continuous search for a more rapid, noninvasive, and cost-effective technology. The present study utilized a fluorescence excitation-emission matrix (EEM) of aflatoxin as well as two additional secondary metabolites (kojic acid and the bright greenish-yellow fluorescence (BGYF) compound) of Aspergillus flavus measured with a fluorescence spectrophotometer. The results were compared to image data acquired with a fluorescence hyperspectral sensor in order to evaluate the potential of image-based technology for detecting aflatoxin in grain. The excitation-emission matrix of aflatoxin B1 standard produced overlapping peaks in 340-400 nm of excitation range emitting in the blue range at around 450 nm. The spectral signature extracted from the hyperspectral image was also in the blue range, emitting blue fluorescence. Because the results from both systems were comparable, where all fluorescence peaks were in the blue range, the present study validates the feasibility of image-based technology for nondestructive detection of aflatoxin in corn. Additional peaks were revealed in the aflatoxin EEM in the 260-nm excitation range that were not present in the kojic acid and BGYF compound mixture. This new information allows for the separation of the aflatoxin signature from the potentially confounding overlap of other secondary metabolites occurring in the blue and blue-green spectral ranges. C1 [Hruska, Zuzana; Yao, Haibo; Kincaid, Russell] Mississippi State Univ, Geosyst Res Inst, MSU Sci & Technol Ctr, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. [Brown, Robert; Cleveland, Thomas; Bhatnagar, Deepak] Agr Res Serv, USDA, So Reg Res Ctr, New Orleans, LA 70124 USA. RP Hruska, Z (reprint author), Mississippi State Univ, Geosyst Res Inst, MSU Sci & Technol Ctr, Stennis Space Ctr, 1021 Balch Blvd, Stennis Space Ctr, MS 39529 USA. EM hruska@gri.msstate.edu FU USDA [58-6435-3-121]; MSU [58-6435-3-121] FX Funding for this study was provided by the cooperative agreement no. 58-6435-3-121 between USDA and MSU. The authors gratefully acknowledge the assistance provided by Professor Laodong Guo and his graduate student Zhengzhen Zhou from the University of Southern Mississippi for EEM data acquisition and instrumentation expertise, and Mr. Lee Hathcock (Mississippi State University) for radiometric calibration of the hyperspectral data. NR 32 TC 6 Z9 6 U1 3 U2 36 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1935-5130 EI 1935-5149 J9 FOOD BIOPROCESS TECH JI Food Bioprocess Technol. PD APR PY 2014 VL 7 IS 4 BP 1195 EP 1201 DI 10.1007/s11947-014-1265-2 PG 7 WC Food Science & Technology SC Food Science & Technology GA AC5CN UT WOS:000332538600024 ER PT J AU Li, ZH Driese, SG Cheng, H AF Li, Zheng-Hua Driese, Steven G. Cheng, Hai TI A multiple cave deposit assessment of suitability of speleothem isotopes for reconstructing palaeo-vegetation and palaeo-temperature SO SEDIMENTOLOGY LA English DT Article DE speleothem; vegetation; stable isotope; Cave deposit; southern Appalachians ID STABLE-ISOTOPE; DRIP WATER; TRACE-ELEMENT; NORTHWESTERN GEORGIA; LATE PLEISTOCENE; CLIMATE CHANGES; CARBON-DIOXIDE; OXYGEN-ISOTOPE; CALCITE; STALAGMITES AB The suitability of speleothems for interpreting palaeoclimate is typically determined by using either the Hendy Test, overlapping analysis or long-term cave environment monitoring. However, in many cases, these methods are not applicable, because a speleothem lacks clearly traceable layers for the Hendy Test, it is difficult to obtain an overlapping speleothem nearby, or long-term cave monitoring is impractical. The authors propose a multiple cave deposit approach to assess the suitability of speleothems for palaeoclimate study. Speleothems collected from two sites within Raccoon Mountain Cave, Tennessee (USA) exhibit remarkable spatial variation (delta C-13: -10 center dot 3 parts per thousand to -2 center dot 2 parts per thousand) over a relatively short distance (ca 260m). Drip water delta O-18 values exhibit a seasonal precipitation signal at Site 1 and an annual signal at Site 2. Combining field observations, water isotope analysis and trace-element data, the authors propose that the speleothem formation at Site 1 and Site 2 tapped distinct sources of CO2: (i) CO2 derived from overlying soils for Site 1; and (ii) limestone dissolved inorganic carbon induced by ground water dissolution for Site 2. Using fresh cave deposits (modern speleothem) delta C-13 (100% C3 vegetation) as an analogue, a simple model was developed to estimate land surface vegetation for speleothems. The speleothem formation temperature estimated using fresh cave deposit delta O-18 values generally reflects the mean annual temperature in this region. This study indicates that spatial variations in carbon isotopes could be caused by different carbon sources dominating in different parts of the cave, which should be taken into consideration by researchers when using speleothem delta C-13 values to reconstruct temporal palaeo-vegetation changes. This study demonstrates a practical sampling strategy for verifying suitability of speleothems for palaeo-vegetation and palaeo-temperature reconstructions by analysing multiple cave deposits, especially for cases in which the Hendy Test, parallel sampling and long-term monitoring of cave environment are not feasible. C1 [Li, Zheng-Hua] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Li, Zheng-Hua] Univ Alabama, Ctr Space Plasma & Aeronom Res, Huntsville, AL 35899 USA. [Driese, Steven G.] Baylor Univ, Dept Geol, Waco, TX 76798 USA. [Cheng, Hai] Xi An Jiao Tong Univ, Inst Global Environm Change, Xian 710049, Peoples R China. [Cheng, Hai] Univ Minnesota, Dept Geol Sci, Minneapolis, MN 55455 USA. RP Li, ZH (reprint author), NASA, George C Marshall Space Flight Ctr, 320 Sparkman Dr,NSSTC 2069, Huntsville, AL 35805 USA. EM zheng-hua.li@nasa.gov FU National Science Foundation (NSF) [EAR-0822824, EAR 0823131] FX The authors thank the Raccoon Mountain Cave manager Betty Perlaky for allowing them to collect speleothems, cave water and other cave sediments. The authors also thank Andrea H. Prichard, Mary Sue Pruitt, Deborah Caldwell, Amy Ladd, Yang Liu, Jim Kocis and Mathew Boehm for cave sediment sampling, B.J. Lindsay and Rebecca Finch for surface water sampling across East Tennessee, and Sharghi Rahmanian and Michelle Stern for speleothem sample preparation for stable isotope analysis. Gary Stinch-comb kindly read an earlier draft of the manuscript and provided helpful comments. This study is supported by National Science Foundation (NSF) EAR-0822824 awarded to Li and Horn, and EAR 0823131 awarded to Driese. Constructive reviews from Sedimentology Editors Peter Swart, Adrian Immenhauser and two anonymous reviewers helped to improve the manuscript. NR 65 TC 1 Z9 4 U1 1 U2 33 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0037-0746 EI 1365-3091 J9 SEDIMENTOLOGY JI Sedimentology PD APR PY 2014 VL 61 IS 3 BP 749 EP 766 DI 10.1111/sed.12078 PG 18 WC Geology SC Geology GA AC8IS UT WOS:000332777300006 ER PT J AU Jagermeyr, J Gerten, D Lucht, W Hostert, P Migliavacca, M Nemani, R AF Jaegermeyr, Jonas Gerten, Dieter Lucht, Wolfgang Hostert, Patrick Migliavacca, Mirco Nemani, Ramakrishna TI A high-resolution approach to estimating ecosystem respiration at continental scales using operational satellite data SO GLOBAL CHANGE BIOLOGY LA English DT Review DE FLUXNET; land surface temperature; LPJmL DGVM; MODIS; RECO; temperature sensitivity; terrestrial carbon flux; up-scaling ID LAND-SURFACE TEMPERATURE; ORGANIC-MATTER DECOMPOSITION; GLOBAL VEGETATION MODEL; GROSS PRIMARY PRODUCTION; CARBON-DIOXIDE EXCHANGE; SOIL-MOISTURE RETRIEVAL; EUROPEAN FORESTS; CLIMATE-CHANGE; CO2 EXCHANGE; TERRESTRIAL ECOSYSTEMS AB A better understanding of the local variability in land-atmosphere carbon fluxes is crucial to improving the accuracy of global carbon budgets. Operational satellite data backed by ground measurements at Fluxnet sites proved valuable in monitoring local variability of gross primary production at highly resolved spatio-temporal resolutions. Yet, we lack similar operational estimates of ecosystem respiration (Re) to calculate net carbon fluxes. If successful, carbon fluxes from such a remote sensing approach would form an independent and sought after measure to complement widely used dynamic global vegetation models (DGVMs). Here, we establish an operational semi-empirical Re model, based only on data from the Moderate Resolution Imaging Spectroradiometer (MODIS) with a resolution of 1km and 8days. Fluxnet measurements between 2000 and 2009 from 100 sites across North America and Europe are used for parameterization and validation. Our analysis shows that Re is closely tied to temperature and plant productivity. By separating temporal and intersite variation, we find that MODIS land surface temperature (LST) and enhanced vegetation index (EVI) are sufficient to explain observed Re across most major biomes with a negligible bias [R-2=0.62, RMSE=1.32 (gCm(-2)d(-1)), MBE=0.05 (gCm(-2)d(-1))]. A comparison of such satellite-derived Re with those simulated by the DGVM LPJmL reveals similar spatial patterns. However, LPJmL shows higher temperature sensitivities and consistently simulates higher Re values, in high-latitude and subtropical regions. These differences remain difficult to explain and they are likely associated either with LPJmL parameterization or with systematic errors in the Fluxnet sampling technique. While uncertainties remain with Re estimates, the model formulated in this study provides an operational, cross-validated and unbiased approach to scale Fluxnet Re to the continental scale and advances knowledge of spatio-temporal Re variability. C1 [Jaegermeyr, Jonas; Gerten, Dieter; Lucht, Wolfgang] Potsdam Inst Climate Impact Res, RD Earth Syst Anal 1, D-14412 Potsdam, Germany. [Jaegermeyr, Jonas; Lucht, Wolfgang; Hostert, Patrick] Humboldt Univ, Dept Geog, D-10099 Berlin, Germany. [Migliavacca, Mirco] Max Planck Inst Biogeochem, Dept Biogeochem Integrat, D-07745 Jena, Germany. [Migliavacca, Mirco] Univ Milano Bicocca, DISAT, Remote Sensing Environm Dynam Lab, I-20126 Milan, Italy. [Nemani, Ramakrishna] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Jagermeyr, J (reprint author), Potsdam Inst Climate Impact Res, RD Earth Syst Anal 1, POB 601203, D-14412 Potsdam, Germany. EM jonas.jaegermeyr@pik-potsdam.de RI Gerten, Dieter/B-2975-2013; Lucht, Wolfgang/G-2180-2011 OI Lucht, Wolfgang/0000-0002-3398-8575 FU European Communities [244240] FX We are thankful for the freely available Flux data at http://www.fluxnet.ornl.gov, which are subject to Fluxnet Data Fair Use Policies and we are grateful for the convenient and free provision of MODIS data at http://daac.ornl.gov/MODIS/modis.html. Sibyll Schaphoff, Steven W. Running and two anonymous reviewers are kindly acknowledged for additional comments. We also acknowledge the European Communities' Seventh Framework Program (Climafrica project, grant no. 244240). NR 116 TC 10 Z9 13 U1 3 U2 77 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1354-1013 EI 1365-2486 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD APR PY 2014 VL 20 IS 4 BP 1191 EP 1210 DI 10.1111/gcb.12443 PG 20 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AB8WA UT WOS:000332069500015 PM 24259306 ER PT J AU Jain, A AF Jain, Abhinandan TI Operational Space Inertia for Closed-Chain Robotic Systems SO JOURNAL OF COMPUTATIONAL AND NONLINEAR DYNAMICS LA English DT Article ID FORMULATION; DYNAMICS AB Operational space modeling and control are important techniques for robot manipulation. A key element of operational space control is the operational space inertia matrix (OSIM). The OSIM matrix represents a mapping between end-effector spatial forces and spatial accelerations and is configuration-dependent. In the case of multiple end-effectors, the OSIM also encapsulates the dynamics cross coupling between the end-effectors. The rich structure of the OSIM for tree systems has been exploited by researchers for analysis and the development of low-order computational algorithms. Extending such techniques to the OSIM for closed-chain robotic systems is the focus of this short paper. We derive explicit analytical expressions for the closed-chain OSIM that reveals its close relationship to an extended tree-system OSIM. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Jain, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Abhi.Jain@jpl.nasa.gov FU National Aeronautics and Space Administration; DARPA Autonomous Robotic Manipulation Software Track (ARM-S) program [20] FX The research described in this paper was performed at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under contract with the National Aeronautics and Space Administration. This project was also supported in part by the DARPA Autonomous Robotic Manipulation Software Track (ARM-S) program [20]. NR 20 TC 0 Z9 0 U1 0 U2 2 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 1555-1423 EI 1555-1415 J9 J COMPUT NONLIN DYN JI J. Comput. Nonlinear Dyn. PD APR PY 2014 VL 9 IS 2 AR 021015 DI 10.1115/1.4025893 PG 5 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA AB8TM UT WOS:000332062900015 ER PT J AU Das, NN Entekhabi, D Njoku, EG Shi, JCJC Johnson, JT Colliander, A AF Das, Narendra Narayan Entekhabi, Dara Njoku, Eni G. Shi, Jiancheng J. C. Johnson, Joel T. Colliander, Andreas TI Tests of the SMAP Combined Radar and Radiometer Algorithm Using Airborne Field Campaign Observations and Simulated Data SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Active-passive; L-band radiometer; L-band SAR; satellite; SMAP; soil moisture ID SOIL-MOISTURE RETRIEVAL; OCEAN SALINITY; L-BAND; MISSION AB A soil moisture retrieval algorithm is proposed that takes advantage of the simultaneous radar and radiometer measurements by the forthcoming NASA Soil Moisture Active Passive (SMAP) mission. The algorithm is designed to downscale SMAP L-band brightness temperature measurements at low resolution (similar to 40 km) to 9-km brightness temperature by using SMAP's L-band synthetic aperture radar (SAR) backscatter measurements at high resolution (1-3 km) in order to estimate soil moisture at 9-km resolution. The SMAP L-band SAR and radiometer instruments are designed to provide coincident observations at constant incidence angle, but at different spatial resolutions, across a wide swath. The algorithm described here takes advantage of the correlation between temporal fluctuations of brightness temperature and backscatter observed when viewing targets simultaneously at the same angle. Surface characteristics that affect the brightness temperature and backscatter measurements influence the signals at different time scales. This feature is applied in an approach in which fine-scale spatial heterogeneity detected by SAR observations is applied on coarser-scale radiometer measurements to produce an intermediate-resolution disaggregated brightness temperature field. These brightness temperatures are then used with established radiometer-based algorithms to retrieve soil moisture at the intermediate resolution. The capability of the overall algorithm is demonstrated using data acquired by the airborne passive and active L-band system from field campaigns and also by simulated global dataset. Results indicate that the algorithm has the potential to retrieve soil moisture at 9-km resolution, with the accuracy required for SMAP, over regions having vegetation up to 5-kg/m(2) vegetation water content. The results show a reduction in root mean square error of > 0.02 cm(3)/cm(3) volumetric soil moisture (40% improvement in the statistics) from the minimum performance defined as the soil moisture retrieved using radiometer measurements re-sampled to the intermediate scale. C1 [Das, Narendra Narayan; Njoku, Eni G.; Colliander, Andreas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Entekhabi, Dara] MIT, Dept Civil & Environm Engn, Cambridge, MA 02139 USA. [Shi, Jiancheng J. C.] Univ Calif Santa Barbara, ICESS, Santa Barbara, CA 93106 USA. [Johnson, Joel T.] Ohio State Univ, Electrosci Lab, Columbus, OH 43212 USA. RP Das, NN (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM nndas@jpl.nasa.gov; darae@mit.edu; eni.g.njoku@jpl.nasa.gov; shi@icess.ucsb.edu; johnson@ece.osu.edu; andreas.colliander@jpl.nasa.gov FU Jet Propulsion Laboratory, California Institute of Technology; National Aeronautics and Space Administration FX Manuscript received November 2, 2012; revised February 15, 2013; accepted April 15, 2013. Date of publication May 14, 2013; date of current version December 24, 2013. This work was supported in part by the Jet Propulsion Laboratory, California Institute of Technology, under Contract with the National Aeronautics and Space Administration. NR 16 TC 28 Z9 28 U1 4 U2 50 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD APR PY 2014 VL 52 IS 4 BP 2018 EP 2028 DI 10.1109/TGRS.2013.2257605 PG 11 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 287FK UT WOS:000329527000009 ER PT J AU Herzfeld, UC McDonald, BW Wallin, BF Neumann, TA Markus, T Brenner, A Field, C AF Herzfeld, Ute Christina McDonald, Brian W. Wallin, Bruce F. Neumann, Thomas A. Markus, Thorsten Brenner, Anita Field, Christopher TI Algorithm for Detection of Ground and Canopy Cover in Micropulse Photon-Counting Lidar Altimeter Data in Preparation for the ICESat-2 Mission SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Algorithms; altimetry; laser measurements; satellites ID LASER ALTIMETRY; FOREST STRUCTURE; ICE SHEETS; SEA-ICE; AIRBORNE; VALIDATION; ACCURACY; CLASSIFICATION; ICESAT/GLAS; PRECISION AB NASA's Ice, Cloud and Land Elevation Satellite-II (ICESat-2) mission is a decadal survey mission (2016 launch). The mission objectives are to measure land ice elevation, sea ice freeboard, and changes in these variables, as well as to collect measurements over vegetation to facilitate canopy height determination. Two innovative components will characterize the ICESat-2 lidar: 1) collection of elevation data by a multibeam system and 2) application of micropulse lidar (photon-counting) technology. A photon-counting altimeter yields clouds of discrete points, resulting from returns of individual photons, and hence new data analysis techniques are required for elevation determination and association of the returned points to reflectors of interest. The objective of this paper is to derive an algorithm that allows detection of ground under dense canopy and identification of ground and canopy levels in simulated ICESat-2 data, based on airborne observations with a Sigma Space micropulse lidar. The mathematical algorithm uses spatial statistical and discrete mathematical concepts, including radial basis functions, density measures, geometrical anisotropy, eigenvectors, and geostatistical classification parameters and hyperparameters. Validation shows that ground and canopy elevation, and hence canopy height, can be expected to be observable with high accuracy by ICESat-2 for all expected beam energies considered for instrument design (93.01%-99.57% correctly selected points for a beam with expected return of 0.93 mean signals per shot (msp), and 72.85%-98.68% for 0.48 msp). The algorithm derived here is generally applicable for elevation determination from photon-counting lidar altimeter data collected over forested areas, land ice, sea ice, and land surfaces, as well as for cloud detection. C1 [Herzfeld, Ute Christina; McDonald, Brian W.] Univ Colorado, Dept Elect Comp & Energy Engn, Boulder, CO 80523 USA. [Herzfeld, Ute Christina; Wallin, Bruce F.] Univ Colorado, Cooperat Inst Res Enviromental Sci, Boulder, CO 80309 USA. [Neumann, Thomas A.; Markus, Thorsten] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Brenner, Anita; Field, Christopher] Sigma Space Corp, Lanham, MD 20706 USA. RP Herzfeld, UC (reprint author), Univ Colorado, Dept Elect Comp & Energy Engn, Boulder, CO 80523 USA. EM ute.herzfeld@colorado.edu; brian.w.mcdonald@colorado.edu; bwallin@nmt.edu; thomas.neumann@nasa.gov; thorsten.markus-1@nasa.gov; Anita.Brenner@sigmaspace.com; Christopher.Field@sigmaspace.com RI Neumann, Thomas/D-5264-2012 FU ICESat-2 Project, NASA Goddard Space Flight Center [NNX10AR46G, NNX11AH43G S01]; Air Force Research Lab [PO FA8650-05C-1817] FX Manuscript received February 14, 2012; revised July 24, 2012, November 10, 2012, and March 18, 2013; accepted April 2, 2013. Date of publication May 31, 2013; date of current version December 24, 2013. The work of U.C. Herzfeld was supported in part by the ICESat-2 Project, NASA Goddard Space Flight Center under Award NNX10AR46G and Award NNX11AH43G S01 to U.C. The work presented here was conducted in collaboration and exchange with the ICESat-2 Project, the ICESat-2 Science Definition Team and Sigma Space Corporation. The Sigma Space Lidar was built under an SBIR under Contract PO FA8650-05C-1817 from the Air Force Research Lab, whom we thank for their permission to use data collected with the sensor for this work. NR 51 TC 18 Z9 19 U1 3 U2 33 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD APR PY 2014 VL 52 IS 4 BP 2109 EP 2125 DI 10.1109/TGRS.2013.2258350 PG 17 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 287FK UT WOS:000329527000017 ER PT J AU Pasolli, E Melgani, F Tuia, D Pacifici, F Emery, WJ AF Pasolli, Edoardo Melgani, Farid Tuia, Devis Pacifici, Fabio Emery, William J. TI SVM Active Learning Approach for Image Classification Using Spatial Information SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Active learning; image classification; spatial information; support vector machine (SVM); very high resolution (VHR) ID SUPPORT VECTOR MACHINES; REMOTE-SENSING IMAGES; COMPOSITE KERNELS; SEGMENTATION; CONFIDENCE; QUERIES AB In the last few years, active learning has been gaining growing interest in the remote sensing community in optimizing the process of training sample collection for supervised image classification. Current strategies formulate the active learning problem in the spectral domain only. However, remote sensing images are intrinsically defined both in the spectral and spatial domains. In this paper, we explore this fact by proposing a new active learning approach for support vector machine classification. In particular, we suggest combining spectral and spatial information directly in the iterative process of sample selection. For this purpose, three criteria are proposed to favor the selection of samples distant from the samples already composing the current training set. In the first strategy, the Euclidean distances in the spatial domain from the training samples are explicitly computed, whereas the second one is based on the Parzen window method in the spatial domain. Finally, the last criterion involves the concept of spatial entropy. Experiments on two very high resolution images show the effectiveness of regularization in spatial domain for active learning purposes. C1 [Pasolli, Edoardo] NASA, Goddard Space Flight Ctr, Computat & Informat Sci & Technol Off, Greenbelt, MD 20771 USA. [Melgani, Farid] Univ Trento, Dept Informat Engn & Comp Sci, I-38123 Trento, Italy. [Tuia, Devis] Ecole Polytech Fed Lausanne, Lab Syst Informat Geog, CH-1015 Lausanne, Switzerland. [Pacifici, Fabio] DigitalGlobe Inc, Longmont, CO 80503 USA. [Emery, William J.] Univ Colorado, Dept Aerosp Engn, Boulder, CO 80309 USA. RP Pasolli, E (reprint author), NASA, Goddard Space Flight Ctr, Computat & Informat Sci & Technol Off, Greenbelt, MD 20771 USA. EM edoardo.pasolli@nasa.gov RI Tuia, Devis/J-2239-2015; OI Tuia, Devis/0000-0003-0374-2459; Pasolli, Edoardo/0000-0003-0799-3490 NR 43 TC 39 Z9 39 U1 1 U2 37 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD APR PY 2014 VL 52 IS 4 BP 2217 EP 2233 DI 10.1109/TGRS.2013.2258676 PG 17 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 287FK UT WOS:000329527000025 ER PT J AU Williams, PE Pesnell, WD AF Williams, Peter E. Pesnell, W. Dean TI Time-Series Analysis of Supergranule Characteristics at Solar Minimum SO SOLAR PHYSICS LA English DT Article DE Sun: convection; Dopplergrams; Helioseismology; Sun: photosphere; SOHO/MDI; SDO/HMI; Solar cycle; Solar minimum; Solar dynamo; Sun: supergranulation ID MICHELSON DOPPLER IMAGER; STEADY PHOTOSPHERIC FLOWS; VELOCITY-FIELDS; ROTATION AB Sixty days of Doppler images from the Solar and Heliospheric Observatory (SOHO) / Michelson Doppler Imager (MDI) investigation during the 1996 and 2008 solar minima have been analyzed to show that certain supergranule characteristics (size, size range, and horizontal velocity) exhibit fluctuations of three to five days. Cross-correlating parameters showed a good, positive correlation between supergranulation size and size range, and a moderate, negative correlation between size range and velocity. The size and velocity do exhibit a moderate, negative correlation, but with a small time lag (less than 12 hours). Supergranule sizes during five days of co-temporal data from MDI and the Solar Dynamics Observatory (SDO) / Helioseismic Magnetic Imager (HMI) exhibit similar fluctuations with a high level of correlation between them. This verifies the solar origin of the fluctuations, which cannot be caused by instrumental artifacts according to these observations. Similar fluctuations are also observed in data simulations that model the evolution of the MDI Doppler pattern over a 60-day period. Correlations between the supergranule size and size range time-series derived from the simulated data are similar to those seen in MDI data. A simple toy-model using cumulative, uncorrelated exponential growth and decay patterns at random emergence times produces a time-series similar to the data simulations. The qualitative similarities between the simulated and the observed time-series suggest that the fluctuations arise from stochastic processes occurring within the solar convection zone. This behavior, propagating to surface manifestations of supergranulation, may assist our understanding of magnetic-field-line advection, evolution, and interaction. C1 [Williams, Peter E.] No Virginia Community Coll, Dept Phys, Annandale, VA 22003 USA. [Williams, Peter E.] Catholic Univ Amer, Washington, DC 20064 USA. [Williams, Peter E.; Pesnell, W. Dean] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Williams, PE (reprint author), No Virginia Community Coll, Dept Phys, Annandale, VA 22003 USA. EM pewilliams@nvcc.edu RI Pesnell, William/D-1062-2012 OI Pesnell, William/0000-0002-8306-2500 FU NASA Postdoctoral Program at NASA Goddard Space Flight Center FX This research was supported by an appointment to the NASA Postdoctoral Program at NASA Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA via the Solar Dynamics Observatory. SDO is part of NASA's LivingWith a Star (LWS) program. HMI was designed and assembled at Stanford University and Lockheed Martin Solar and Astrophysics Laboratory. SOHO is a project of international cooperation between ESA and NASA. The authors extend their gratitude to John Beck of Stanford University for producing the de-rotated Dopplergram datasets. We also thank the referee for the constructive comments that have improved the content of this article. NR 27 TC 1 Z9 1 U1 0 U2 11 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 APR PY 2014 VL 289 IS 4 BP 1101 EP 1113 DI 10.1007/s11207-013-0383-8 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268WB UT WOS:000328200300003 ER PT J AU Nitta, NV Aschwanden, MJ Freeland, SL Lemen, JR Wulser, JP Zarro, DM AF Nitta, N. V. Aschwanden, M. J. Freeland, S. L. Lemen, J. R. Wuelser, J. -P. Zarro, D. M. TI The Association of Solar Flares with Coronal Mass Ejections During the Extended Solar Minimum SO SOLAR PHYSICS LA English DT Article DE Flares; CMEs; STEREO ID EIT WAVES; QUADRATURE OBSERVATIONS; STEREO MISSION; CME; TRANSIENTS; CATALOG; RADIO; SPACECRAFT; SIGNATURES; REGIONS AB We study the association of solar flares with coronal mass ejections (CMEs) during the deep, extended solar minimum of 2007-2009, using extreme-ultraviolet (EUV) and white-light (coronagraph) images from the Solar Terrestrial Relations Observatory (STEREO). Although all of the fast (v > 900 kms(-1)), wide (theta > 100 degrees) CMEs are associated with a flare that is at least identified in GOES soft X-ray light curves, a majority of flares with relatively high X-ray intensity for the deep solar minimum (e.g. greater than or similar to 1 x 10(-6) W m(-2) or C1) are not associated with CMEs. Intense flares tend to occur in active regions with a strong and complex photospheric magnetic field, but the active regions that produce CME-associated flares tend to be small, including those that have no sunspots and therefore no NOAA active-region numbers. Other factors on scales similar to and larger than active regions seem to exist that contribute to the association of flares with CMEs. We find the possible low coronal signatures of CMEs, namely eruptions, dimmings, EUV waves, and Type III bursts, in 91 %, 74 %, 57 %, and 74 %, respectively, of the 35 flares that we associate with CMEs. None of these observables can fully replace direct observations of CMEs by coronagraphs. C1 [Nitta, N. V.; Aschwanden, M. J.; Freeland, S. L.; Lemen, J. R.; Wuelser, J. -P.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Zarro, D. M.] ADNET Syst Inc, Greenbelt, MD 20771 USA. [Zarro, D. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Nitta, NV (reprint author), Lockheed Martin Solar & Astrophys Lab, A021S,Bldg 252,3251 Hanover St, Palo Alto, CA 94304 USA. EM nitta@lmsal.com; aschwanden@lmsal.com; freeland@lmsal.com; lemen@lmsal.com; wuelser@lmsal.com; dominic.m.zarro@nasa.gov FU NASA STEREO mission under NRL [N00173-02-C-2035]; NASA; Science & Technology Facility Council; Deutsches Zentrum fur Luftund Raumfahrt e.V. (DLR); Belgian Science Policy Office; Centre National d'Etudes Spatiales (CNES); Centre National de la Recherche Scientifique (CNRS).; USAF Space Test Program; Office of Naval Research FX This work has been supported by the NASA STEREO mission under NRL Contract No. N00173-02-C-2035. We thank the referee for useful comments that are largely reflected in the revised manuscript. The STEREO/SECCHI data used here were produced by an international consortium of the Naval Research Laboratory (USA), Lockheed Martin Solar and Astrophysics Lab (USA), NASA Goddard Space Flight Center (USA), Rutherford Appleton Laboratory (UK), University of Birmingham (UK), Max-Planck-Institut for Solar System Research (Germany), Centre Spatiale de Liege (Belgium), Institut d'Optique Theorique et Appliquee (France), and Institut d'Astrophysique Spatiale (France). The USA institutions were funded by NASA, the UK institutions by the Science & Technology Facility Council (which used to be the Particle Physics and Astronomy Research Council, PPARC), the German institutions by Deutsches Zentrum fur Luftund Raumfahrt e.V. (DLR), the Belgian institutions by Belgian Science Policy Office, and the French institutions by Centre National d'Etudes Spatiales (CNES) and the Centre National de la Recherche Scientifique (CNRS). The NRL effort was also supported by the USAF Space Test Program and the Office of Naval Research. NR 60 TC 11 Z9 11 U1 0 U2 11 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 APR PY 2014 VL 289 IS 4 BP 1257 EP 1277 DI 10.1007/s11207-013-0388-3 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268WB UT WOS:000328200300013 ER PT J AU Susskind, J Blaisdell, JM Iredell, L AF Susskind, Joel Blaisdell, John M. Iredell, Lena TI Improved methodology for surface and atmospheric soundings, error estimates, and quality control procedures: the atmospheric infrared sounder science team version-6 retrieval algorithm SO JOURNAL OF APPLIED REMOTE SENSING LA English DT Article DE remote sensing; infrared; clouds; satellites; meteorology ID CLOUDY ATMOSPHERES AB The atmospheric infrared sounder (AIRS) science team version-6 AIRS/advanced microwave sounding unit (AMSU) retrieval algorithm is now operational at the Goddard Data and Information Services Center (DISC). AIRS version-6 level-2 products are generated near real time at the Goddard DISC and all level-2 and level-3 products are available starting from September 2002. Some of the significant improvements in retrieval methodology contained in the version-6 retrieval algorithm compared to that previously used in version-5 are described. In particular, the AIRS science team made major improvements with regard to the algorithms used to (1) derive surface skin temperature and surface spectral emissivity; (2) generate the initial state used to start the cloud clearing and retrieval procedures; and (3) derive error estimates and use them for quality control. Significant improvements have also been made in the generation of cloud parameters. In addition to the basic AIRS/AMSU mode, version-6 also operates in an AIRS only (AO) mode, which produces results almost as good as those of the full AIRS/AMSU mode. The improvements of some AIRS version-6 and version-6 AO products compared to those obtained using version-5 are also demonstrated. c The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI. C1 [Susskind, Joel; Blaisdell, John M.; Iredell, Lena] NASA, Goddard Space Flight Ctr, Earth Sci Div Atmospheres, Greenbelt, MD 20771 USA. [Blaisdell, John M.; Iredell, Lena] NASA, SAIC, Greenbelt, MD 20771 USA. RP Susskind, J (reprint author), NASA, Goddard Space Flight Ctr, Earth Sci Div Atmospheres, Greenbelt, MD 20771 USA. EM Joel.Susskind-1@nasa.gov FU NASA [09-TERRAQUA09-0099] FX This work was supported by NASA under the AIRS Science Team proposal "Improved AIRS/AMSU soundings, clear column radiances, error estimates and quality control for use in weather and climate studies (09-TERRAQUA09-0099). NR 17 TC 25 Z9 25 U1 1 U2 9 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1931-3195 J9 J APPL REMOTE SENS JI J. Appl. Remote Sens. PD MAR 31 PY 2014 VL 8 AR 084994 DI 10.1117/1.JRS.8.084994 PG 33 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AD9DK UT WOS:000333564700001 ER PT J AU Hajra, R Tsurutani, BT Echer, E Gonzalez, WD AF Hajra, Rajkumar Tsurutani, Bruce T. Echer, Ezequiel Gonzalez, Walter D. TI Relativistic electron acceleration during high- intensity, long- duration, continuous AE activity ( HILDCAA) events: Solar cycle phase dependences SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE HILDCAAs; magnetospheric relativistic electrons; chorus waves; high-speed streams; Alfven waves; solar cycle phases ID WHISTLER-MODE CHORUS; RESONANT DIFFUSION; ALFVEN WAVES; PRECIPITATION; MAGNETOSPHERE; SCATTERING; FLUXES; ZONE AB High-intensity, long-duration, continuous AE activity (HILDCAA) intervals during solar cycle 23 (1995-2008) have been studied by a superposed epoch analysis. It was found that HILDCAA intervals order the solar wind velocity, temperature and density (characteristic of high-speed solar wind intervals), the polar cap potential, and various other geomagnetic indices well. The interplanetary magnetic field B-z is generally negative, and the Newell solar wind coupling function is high during HILDCAA events. The HILDCAA intervals are well correlated with an enhancement of magnetospheric relativistic (E>2MeV) electron fluxes observed at geosynchronous orbit with a delay of similar to 1.5days from the onset of the HILDCAAs. The response of the energetic electrons to HILDCAAs is found to vary with solar cycle phase. The initial electron fluxes are lower for events occurring during the ascending and solar maximum (AMAX) phases than for events occurring during the descending and solar minimum (DMIN) phases. The flux increases for the DMIN phase events are >50% larger than for the AMAX phase events. Although the solar wind speeds during the DMIN phases were slightly higher and lasted longer than during the AMAX phases, no other significant solar wind differences were noted. It is concluded that electrons are accelerated to relativistic energies most often and most efficiently during the DMIN phases of the solar cycle. We propose two possible solar UV mechanisms to explain this solar cycle effect. Key Points Magnetospheric relativistic electron fluxes are enhanced during HILDCAAs Enhancements of relativistic electron fluxes vary with solar cycle phases Enhancements are higher in declining/minimum phases than rising/maximum phases C1 [Hajra, Rajkumar; Echer, Ezequiel; Gonzalez, Walter D.] Inst Nacl Pesquisas Espaciais, Sao Paulo, Brazil. [Tsurutani, Bruce T.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Hajra, R (reprint author), Inst Nacl Pesquisas Espaciais, Sao Paulo, Brazil. EM rajkumarhajra@yahoo.co.in RI Hajra, Rajkumar/C-1246-2011; OI Hajra, Rajkumar/0000-0003-1583-182X; Hajra, Rajkumar/0000-0003-0447-1531 FU Fundacao de Amparo a Pesquisa do Estado de Sao Paulo through postdoctoral research fellowship at INPE; Brazilian CNPq [301233/2011-0] FX The work of R.H. is financially supported by Fundacao de Amparo a Pesquisa do Estado de Sao Paulo through postdoctoral research fellowship at INPE. One of the authors (E.E.) would like to thank the Brazilian CNPq (301233/2011-0) agency for the financial support. Portions of this research were performed at the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. We thank the two referees for their helpful comments/suggestions that have helped improve this paper. NR 36 TC 16 Z9 16 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 28 PY 2014 VL 41 IS 6 BP 1876 EP 1881 DI 10.1002/2014GL059383 PG 6 WC Geosciences, Multidisciplinary SC Geology GA AE8PX UT WOS:000334264900009 ER PT J AU Han, SC Schmerr, N Neumann, G Holmes, S AF Han, Shin-Chan Schmerr, Nicholas Neumann, Gregory Holmes, Simon TI Global characteristics of porosity and density stratification within the lunar crust from GRAIL gravity and Lunar Orbiter Laser Altimeter topography data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE lunar crust; GRAIL gravity; LOLA topography; density; porosity ID MOON; MISSION; HISTORY; MANTLE; FIELD; MODEL AB The Gravity Recovery and Interior Laboratory (GRAIL) mission is providing unprecedentedly high-resolution gravity data. The gravity signal in relation to topography decreases from 100 km to 30 km wavelength, equivalent to a uniform crustal density of 2450 kg/m(3) that is 100 kg/m(3) smaller than the density required at 100 km. To explain such frequency-dependent behavior, we introduce rock compaction models under lithostatic pressure that yield radially stratified porosity (and thus density) and examine the depth extent of porosity. Our modeling and analysis support the assertion that the crustal density must vary from surface to deep crust by up to 500 kg/m(3). We found that the surface density of megaregolith is around 2400 kg/m(3) with an initial porosity of 10-20%, and this porosity is eliminated at 10-20 km depth due to lithostatic overburden pressure. Our stratified density models provide improved fits to both GRAIL primary and extended mission data. Key Points Density and porosity structure within the lunar crust was quantified The porosity is eliminated at 10-20 km depth due to lithostatic pressure Improved lunar crustal gravity models were constructed C1 [Han, Shin-Chan; Schmerr, Nicholas; Neumann, Gregory; Holmes, Simon] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Schmerr, Nicholas] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Holmes, Simon] SGT Inc, Greenbelt, MD USA. RP Han, SC (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. EM shin-chan.han@nasa.gov RI Neumann, Gregory/I-5591-2013; OI Neumann, Gregory/0000-0003-0644-9944; Schmerr, Nicholas/0000-0002-3256-1262 FU NASA FX This work was supported by NASA's LASER program and GRACE projects. We gratefully appreciate the GRAIL principal investigators and their team for releasing the L1B and L2 data within 6 months after the end of the primary mission. We thank Walter Kiefer and an anonymous reviewer for reviewing this paper. NR 28 TC 7 Z9 7 U1 5 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 28 PY 2014 VL 41 IS 6 BP 1882 EP 1889 DI 10.1002/2014GL059378 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AE8PX UT WOS:000334264900010 ER PT J AU Pan, L Ehlmann, BL AF Pan, L. Ehlmann, B. L. TI Phyllosilicate and hydrated silica detections in the knobby terrains of Acidalia Planitia, northern plains, Mars SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Mars mineralogy; phyllosilicates; hydrated silica; Northern Plains ID GLOBAL VIEW; MINERALS; SURFACE; WATER; DIVERSITY; LOWLANDS; DEPOSITS; SPECTRA; HISTORY; CRISM AB Here we report detections of Fe/Mg phyllosilicates and hydrated silica in discrete stratigraphic units within the knobby terrains of Acidalia Planitia made using data acquired by Compact Reconnaissance Imaging Spectrometer for Mars. Fe/Mg phyllosilicates are detected in knobs that were eroded during southward retreat of the dichotomy boundary. A second later unit, now eroded to steep-sided platforms embaying the knobs, contains hydrated silica, which may have formed via localized vapor weathering, thin-film leaching, or transient water that resulted in surface alteration. These are then overlain by smooth plains with small cones, hypothesized to be mud volcanoes which previous studies have shown to have no hydrated minerals. In spite of Acidalia's location within the putative northern ocean, collectively, the data record a history of aqueous processes much like that in the southern highlands with progressively less intensive aqueous chemical alteration from the Noachian to Amazonian. C1 [Pan, L.; Ehlmann, B. L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Ehlmann, B. L.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Pan, L (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM lpan@caltech.edu FU NASA Mars Data Analysis Program [NNX12AJ43G] FX Thanks to Jim Skinner for early discussions about northern plains evolution, Ara Oshagan for CTX mosaic and DEM processing, the MRO science operation teams for collecting the data set and the constructive comments of Nancy McKeown and one anonymous reviewer, which improved this manuscript. This work was supported by NASA Mars Data Analysis Program award NNX12AJ43G. NR 62 TC 2 Z9 3 U1 0 U2 13 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 MAR 28 PY 2014 VL 41 IS 6 BP 1890 EP 1898 DI 10.1002/2014GL059423 PG 9 WC Geosciences, Multidisciplinary SC Geology GA AE8PX UT WOS:000334264900011 ER PT J AU Argus, DF Fu, YN Landerer, FW AF Argus, Donald F. Fu, Yuning Landerer, Felix W. TI Seasonal variation in total water storage in California inferred from GPS observations of vertical land motion SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE California; GPS; hydrology; water; snow ID DATA ASSIMILATION SYSTEM; SPACE GEODESY; LOS-ANGELES; SURFACE; EARTH; VELOCITIES; GRAVITY; NLDAS; MODEL; GRACE AB GPS is accurately recording vertical motion of Earth's surface in elastic response to seasonal changes in surface water storage in California. California's mountains subside up to 12 mm in the fall and winter due to the load of snow and rain and then rise an identical amount in the spring and summer when the snow melts, the rain runs off, and soil moisture evaporates. We invert the GPS observations of seasonal vertical motions to infer changes in equivalent water thickness. GPS resolves the distribution of change in total water across California's physiographic provinces at a resolution of 50 km, compared to 200 km resolution from the Gravity Recovery and Climate Experiment. The seasonal surface water thickness change is 0.6 m in the Sierra Nevada, Klamath, and southern Cascade Mountains and decreases sharply to about 0.1 m east into the Great Basin and west toward the Pacific coast. GPS provides an independent inference of change in total surface water, indicating water storage to be on average 50% larger than in the NLDAS-Noah hydrology model, likely due to larger changes in snow and reservoir water than in the model. Seismicity and land uplift produced by groundwater loss in California's Central Valley is also being evaluated [Amos et al., 2014]. C1 [Argus, Donald F.; Fu, Yuning; Landerer, Felix W.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Argus, DF (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Donald.F.Argus@jpl.nasa.gov OI Landerer, Felix/0000-0003-2678-095X NR 40 TC 27 Z9 27 U1 2 U2 33 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 28 PY 2014 VL 41 IS 6 BP 1971 EP 1980 DI 10.1002/2014GL059570 PG 10 WC Geosciences, Multidisciplinary SC Geology GA AE8PX UT WOS:000334264900022 ER PT J AU Buermann, W Parida, B Jung, M MacDonald, GM Tucker, CJ Reichstein, M AF Buermann, Wolfgang Parida, Bikash Jung, Martin MacDonald, Glen M. Tucker, Compton J. Reichstein, Markus TI Recent shift in Eurasian boreal forest greening response may be associated with warmer and drier summers SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE climate change; boreal forests; heat and drought stress; vegetation remote sensing ID CARBON-DIOXIDE CONCENTRATIONS; WATER-USE EFFICIENCY; NORTH-AMERICA; WHITE SPRUCE; CLIMATE SYSTEM; NDVI DATA; GROWTH; TEMPERATURE; DROUGHT; PRODUCTIVITY AB Terrestrial ecosystems in the northern high latitudes are currently experiencing drastic warming, and recent studies suggest that boreal forests may be increasingly vulnerable to warming-related factors, including temperature-induced drought stress as well as shifts in fire regimes and insect outbreaks. Here we analyze interannual relationships in boreal forest greening and climate over the last three decades using newly available satellite vegetation data. Our results suggest that due to continued summer warming in the absence of sustained increases in precipitation, a turning point has been reached around the mid-1990s that shifted western central Eurasian boreal forests into a warmer and drier regime. This may be the leading cause for the emergence of large-scale negative correlations between summer temperatures and forest greenness. If such a regime shift would be sustained, the dieback of the boreal forest induced by heat and drought stress as predicted by vegetation models may proceed more rapidly than anticipated. Key Points Evidence for temperature plant growth divergence in boreal forests since mid-1990s Rising heat and drought stress due to sustained summer warming are key factors C1 [Buermann, Wolfgang] Univ Leeds, Inst Climate & Atmospher Sci, Sch Earth & Environm, Leeds, W Yorkshire, England. [Parida, Bikash] Shiv Nadar Univ, Dept Civil Engn, Dadri, Uttar Pradesh, India. [Jung, Martin; Reichstein, Markus] Max Planck Inst Biogeochem, D-07745 Jena, Germany. [MacDonald, Glen M.] Univ Calif Los Angeles, Inst Environm & Sustainabil, Los Angeles, CA USA. [Tucker, Compton J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Buermann, W (reprint author), Univ Leeds, Inst Climate & Atmospher Sci, Sch Earth & Environm, Leeds, W Yorkshire, England. EM w.buermann@leeds.ac.uk FU National Aeronautics and Space Administration Carbon Cycle Science Program [NNX11AD45G] FX W.B. and B. P. received funding for this study through the National Aeronautics and Space Administration Carbon Cycle Science Program (grant NNX11AD45G). We thank F. S. Chapin III and J. Fisher for their useful comments. NR 41 TC 18 Z9 18 U1 4 U2 32 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 MAR 28 PY 2014 VL 41 IS 6 BP 1995 EP 2002 DI 10.1002/2014GL059450 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AE8PX UT WOS:000334264900025 ER PT J AU Liu, JM Scheuer, E Dibb, J Ziemba, LD Thornhill, KL Anderson, BE Wisthaler, A Mikoviny, T Devi, JJ Bergin, M Weber, RJ AF Liu, Jiumeng Scheuer, Eric Dibb, Jack Ziemba, Luke D. Thornhill, Kenneth. L. Anderson, Bruce E. Wisthaler, Armin Mikoviny, Tomas Devi, J. Jai Bergin, Michael Weber, Rodney J. TI Brown carbon in the continental troposphere SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE brown carbon; aerosol light absorption; direct radiative forcing ID LIGHT-ABSORPTION; ORGANIC-CARBON; BLACK CARBON; AEROSOLS; COMBUSTION; DEPENDENCE; EXTRACTS AB Little is known about the optical significance of light absorbing particulate organic compounds (i.e., brown carbon, BrC), including the importance relative to black carbon (BC) and influence on direct radiative forcing by aerosols. The vertical profile of BrC affects its radiative forcing, yet the distribution of BrC in the free troposphere is largely unknown. In this study, BrC absorption was directly measured in solvent extracts of particulate filters obtained from aircraft sampling over the continental USA. Excluding biomass burning plumes, BrC was observed throughout the tropospheric column (<13km), and its prevalence increased relative to BC with increasing altitude, indicating contributions from secondary sources. Closure analysis showed good agreement between light absorption from BC plus BrC relative to measured total aerosol absorption. A radiative transfer model indicated that BrC absorption reduced top of atmosphere aerosol forcing by similar to 20%, suggesting that it is an important component of direct aerosol radiative forcing. Key Points BrC is prevalent in the troposphere and increases relative to BC with altitude Optical closure is obtained between BrC plus BC and total absorption at 365nm BrC contributes 20% to top of atmosphere absorbing aerosol forcing C1 [Liu, Jiumeng; Weber, Rodney J.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Scheuer, Eric; Dibb, Jack] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Ziemba, Luke D.; Thornhill, Kenneth. L.; Anderson, Bruce E.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Wisthaler, Armin] Inst Fuer Ionenphys & Angew Phys, Innsbruck, Austria. [Mikoviny, Tomas] Oak Ridge Associated Univ, Oak Ridge, TN USA. [Devi, J. Jai; Bergin, Michael] Georgia Inst Technol, Sch Civil & Environm Engn, Atlanta, GA 30332 USA. RP Weber, RJ (reprint author), Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. EM rodney.weber@eas.gatech.edu RI Liu, Jiumeng/K-2024-2012 OI Liu, Jiumeng/0000-0001-7238-593X FU GIT NASA [NNX12AB83G, NNX08AH80G]; EPA STAR [R83503901]; UNH NASA [NNX12AB80G] FX This project was funded by GIT NASA contracts NNX12AB83G and NNX08AH80G, EPA STAR grant R83503901, and UNH NASA contract NNX12AB80G. We thank Joshua Schwarz and Ru-shan Gao from NOAA, and Glenn Diskin from NASA, for data support. NR 23 TC 29 Z9 30 U1 2 U2 62 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 MAR 28 PY 2014 VL 41 IS 6 BP 2191 EP 2195 DI 10.1002/2013GL058976 PG 5 WC Geosciences, Multidisciplinary SC Geology GA AE8PX UT WOS:000334264900051 ER PT J AU Rostem, K Chuss, DT Colazo, FA Crowe, EJ Denis, KL Lourie, NP Moseley, SH Stevenson, TR Wollack, EJ AF Rostem, K. Chuss, D. T. Colazo, F. A. Crowe, E. J. Denis, K. L. Lourie, N. P. Moseley, S. H. Stevenson, T. R. Wollack, E. J. TI Precision control of thermal transport in cryogenic single-crystal silicon devices SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID PHONON-SCATTERING; HEAT; SURFACES; THERMOMETRY; CONDUCTION AB We report on the diffusive-ballistic thermal conductance of multi-moded single-crystal silicon beams measured below 1 K. It is shown that the phonon mean-free-path l is a strong function of the surface roughness characteristics of the beams. This effect is enhanced in diffuse beams with lengths much larger than l, even when the surface is fairly smooth, 5-10 nm rms, and the peak thermal wavelength is 0.6 mu m. Resonant phonon scattering has been observed in beams with a pitted surface morphology and characteristic pit depth of 30 nm. Hence, if the surface roughness is not adequately controlled, the thermal conductance can vary significantly for diffuse beams fabricated across a wafer. In contrast, when the beam length is of order, the conductance is dominated by ballistic transport and is effectively set by the beam cross-sectional area. We have demonstrated a uniformity of +/- 8% in fractional deviation for ballistic beams, and this deviation is largely set by the thermal conductance of diffuse beams that support the micro-electro-mechanical device and electrical leads. In addition, we have found no evidence for excess specific heat in single-crystal silicon membranes. This allows for the precise control of the device heat capacity with normal metal films. We discuss the results in the context of the design and fabrication of large-format arrays of far-infrared and millimeter wavelength cryogenic detectors. (C) 2014 AIP Publishing LLC. C1 [Rostem, K.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Rostem, K.; Chuss, D. T.; Colazo, F. A.; Crowe, E. J.; Denis, K. L.; Lourie, N. P.; Moseley, S. H.; Stevenson, T. R.; Wollack, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Rostem, K (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. EM karwan.rostem@nasa.gov RI Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 FU NASA ROSES/APRA program; NASA Postdoctoral Program at the Goddard Space Flight Center FX We gratefully acknowledge financial support from the NASA ROSES/APRA program. K. Rostem was supported by the NASA Postdoctoral Program at the Goddard Space Flight Center during the initial stages of this work. We thank Samelys Rodriguez for wirebonding and cryo-cable support. We thank our collaborators A. Ali, J. Appel, and T. A. Marriage for their contribution to the data acquisition. We thank the National Institute of Standards and Technology for providing the SQUID series array and time division multiplexer chips. NR 31 TC 9 Z9 9 U1 1 U2 10 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-8979 EI 1089-7550 J9 J APPL PHYS JI J. Appl. Phys. PD MAR 28 PY 2014 VL 115 IS 12 AR 124508 DI 10.1063/1.4869737 PG 10 WC Physics, Applied SC Physics GA AE3TP UT WOS:000333901100091 ER PT J AU Dent, WRF Wyatt, MC Roberge, A Augereau, JC Casassus, S Corder, S Greaves, JS de Gregorio-Monsalvo, I Hales, A Jackson, AP Hughes, AM Lagrange, AM Matthews, B Wilner, D AF Dent, W. R. F. Wyatt, M. C. Roberge, A. Augereau, J-C Casassus, S. Corder, S. Greaves, J. S. de Gregorio-Monsalvo, I. Hales, A. Jackson, A. P. Hughes, A. Meredith Lagrange, A-M Matthews, B. Wilner, D. TI Molecular Gas Clumps from the Destruction of Icy Bodies in the beta Pictoris Debris Disk SO SCIENCE LA English DT Article ID CIRCUMSTELLAR DISK; PLANET FORMATION; GIANT PLANET; COLLISIONS; DUST; CO; STARS; VEGA; MYR AB Many stars are surrounded by disks of dusty debris formed in the collisions of asteroids, comets, and dwarf planets, but is gas also released in such events? Observations at submillimeter wavelengths of the archetypal debris disk around beta Pictoris show that 0.3% of a Moon mass of carbon monoxide orbits in its debris belt. The gas distribution is highly asymmetric, with 30% found in a single clump 85 astronomical units from the star, in a plane closely aligned with the orbit of the inner planet, beta Pictoris b. This gas clump delineates a region of enhanced collisions, either from a mean motion resonance with an unseen giant planet or from the remnants of a collision of Mars-mass planets. C1 [Dent, W. R. F.; Corder, S.; de Gregorio-Monsalvo, I.; Hales, A.] Atacama Large Millimeter Submillimeter Array ALMA, Santiago Cent Off, Santiago, Chile. [Wyatt, M. C.; Jackson, A. P.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Roberge, A.] NASA, Exoplanets & Stellar Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Augereau, J-C; Lagrange, A-M] Univ Grenoble 1, CNRS, Inst Planetol & Astrophys Grenoble, Inst Natl Sci Univers,UMR 5274, F-38041 Grenoble, France. [Casassus, S.] Univ Chile, Dept Astron, Santiago, Chile. [Greaves, J. S.] Univ St Andrews, Dept Astron, St Andrews, Fife, Scotland. [de Gregorio-Monsalvo, I.] European So Observ, D-85748 Garching, Germany. [Jackson, A. P.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Hughes, A. Meredith] Wesleyan Univ, Dept Astron, Van Vleck Observ, Middletown, CT 06459 USA. [Matthews, B.] Natl Res Council Canada, Herzberg Astron Program, Victoria, BC V9E 2E7, Canada. [Matthews, B.] Natl Res Council Canada, Astrophys Program, Victoria, BC V9E 2E7, Canada. [Matthews, B.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. [Wilner, D.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Dent, WRF (reprint author), Atacama Large Millimeter Submillimeter Array ALMA, Santiago Cent Off, Alonso de Cordova 3107,Casilla 763 0355, Santiago, Chile. EM wdent@alma.cl RI Roberge, Aki/D-2782-2012; Casassus, Simon/I-8609-2016 OI Roberge, Aki/0000-0002-2989-3725; FU Millenium Nucleus (Chilean Ministry of Economy) [P10-022-F]; Goddard Center for Astrobiology, part of the NASA Astrobiology Institute; European Union through European Research Council [279973]; Ministerio de Ciencia e Innovacion (Spain) [AYA2011-30228-C03]; Science and Technology Facilities Council; French National Research Agency (ANR) [ANR-2010 BLAN-0505-01] FX This paper makes use of the following ALMA data: ADS/JAO. ALMA#2011.0.00087. S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and National Institute of Natural Sciences (Japan), together with National Research Council (Canada) and National Science Council and Academia Sinica Institute of Astronomy and Astrophysics (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, Associated Universities, Inc./National Radio Astronomy Observatory and National Astronomical Observatory of Japan. Partial financial support for S. Casassus, M. C. W. and A. H. was provided by Millenium Nucleus P10-022-F (Chilean Ministry of Economy). A. R. acknowledges support by the Goddard Center for Astrobiology, part of the NASA Astrobiology Institute. M. C. W. was supported by the European Union through European Research Council grant number 279973, I.d. G.-M. acknowledges support from Ministerio de Ciencia e Innovacion (Spain) grant number AYA2011-30228-C03 (including European Funds for Economic and Regional Development), A.P.J. was supported by a Science and Technology Facilities Council postgraduate studentship, and J.-C.A. acknowledges the French National Research Agency (ANR) for support through contract number ANR-2010 BLAN-0505-01 (EXOZODI). NR 28 TC 57 Z9 57 U1 2 U2 8 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 MAR 28 PY 2014 VL 343 IS 6178 BP 1490 EP 1492 DI 10.1126/science.1248726 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AD7TZ UT WOS:000333471000041 PM 24603151 ER PT J AU Hearty, TJ Savtchenko, A Tian, BJ Fetzer, E Yung, YL Theobald, M Vollmer, B Fishbein, E Won, YI AF Hearty, Thomas J. Savtchenko, Andrey Tian, Baijun Fetzer, Eric Yung, Yuk L. Theobald, Michael Vollmer, Bruce Fishbein, Evan Won, Young-In TI Estimating sampling biases and measurement uncertainties of AIRS/AMSU-A temperature and water vapor observations using MERRA reanalysis SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID DATA PRODUCTS; SATELLITES; PARAMETERS; ACCURACY; MISSION; IMPACT; ERRORS; MODEL; AIRS; AQUA AB We use MERRA (Modern Era Retrospective-Analysis for Research Applications) temperature and water vapor data to estimate the sampling biases of climatologies derived from the AIRS/AMSU-A (Atmospheric Infrared Sounder/Advanced Microwave Sounding Unit-A) suite of instruments. We separate the total sampling bias into temporal and instrumental components. The temporal component is caused by the AIRS/AMSU-A orbit and swath that are not able to sample all of time and space. The instrumental component is caused by scenes that prevent successful retrievals. The temporal sampling biases are generally smaller than the instrumental sampling biases except in regions with large diurnal variations, such as the boundary layer, where the temporal sampling biases of temperature can be +/- 2 K and water vapor can be 10% wet. The instrumental sampling biases are the main contributor to the total sampling biases and are mainly caused by clouds. They are up to 2 K cold and > 30% dry over midlatitude storm tracks and tropical deep convective cloudy regions and up to 20% wet over stratus regions. However, other factors such as surface emissivity and temperature can also influence the instrumental sampling bias over deserts where the biases can be up to 1 K cold and 10% wet. Some instrumental sampling biases can vary seasonally and/or diurnally. We also estimate the combined measurement uncertainties of temperature and water vapor from AIRS/AMSU-A and MERRA by comparing similarly sampled climatologies from both data sets. The measurement differences are often larger than the sampling biases and have longitudinal variations. C1 [Hearty, Thomas J.; Won, Young-In] Goddard Space Flight Ctr Wyle, Greenbelt, MD 20771 USA. [Savtchenko, Andrey; Theobald, Michael] NASA, Goddard Space Flight Ctr, ADNET, Greenbelt, MD 20771 USA. [Tian, Baijun; Fetzer, Eric; Fishbein, Evan] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Vollmer, Bruce] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hearty, TJ (reprint author), Goddard Space Flight Ctr Wyle, Greenbelt, MD 20771 USA. EM thomas.hearty@nasa.gov RI Tian, Baijun/A-1141-2007 OI Tian, Baijun/0000-0001-9369-2373 NR 31 TC 7 Z9 7 U1 1 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAR 27 PY 2014 VL 119 IS 6 BP 2725 EP 2741 DI 10.1002/2013JD021205 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH3SV UT WOS:000336046600003 ER PT J AU Bergman, JW Jensen, EJ Pfister, L Pan, LL Honomichl, S AF Bergman, John W. Jensen, Eric J. Pfister, Leonhard Pan, Laura L. Honomichl, Shawn TI Analyzing dynamical circulations in the tropical tropopause layer through empirical predictions of cirrus cloud distributions SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID LOWER STRATOSPHERE; WATER-VAPOR; TRANSPORT; TRAJECTORIES; BALANCE; OZONE AB We explore the use of nonlinear empirical predictions of thin cirrus for diagnosing transport through the tropical tropopause layer (TTL). Thirty day back trajectories are calculated from the locations of CALIPSO cloud observations to obtain Lagrangian dry and cold points associated with each observation. These historical values are combined with "local" (at the location of the CALIPSO observation) temperature and specific humidity to predict cloud probability using multivariate polynomial regression. We demonstrate that our statistical sample (seven seasons) is sufficient to retrieve the full nonlinear relationship between cloud probability and its predictors and that substantial information is lost in a purely linear analysis. The best cloud prediction is obtained by the two-variable combination of local temperature and humidity, which reflects the close relationship between clouds and relative humidity. However, single-variable predictions involving air parcel histories are better than those based solely on the individual local fields, indicating the existence of reliable dynamical information content within parcel trajectories. Thermal fields are better cirrus predictors during boreal winter than summer primarily due to poor predictions over the Asian summer monsoon region, revealing that the functional relationship over southern Asia differs from the rest of the tropics; in short, TTL cirrus formation over regions of active maritime convection, such as the West Pacific, is thermally dominated, indicating an environment in which in situ cirrus are readily formed, while TTL cirrus of southern Asia is moisture dominated, indicating a more direct connection between convective injection of moisture and thin cirrus. C1 [Bergman, John W.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Bergman, John W.; Pan, Laura L.; Honomichl, Shawn] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA. [Jensen, Eric J.; Pfister, Leonhard] NASA, Ames Res Ctr, Earth Sci Div, Moffett Field, CA 94035 USA. RP Bergman, JW (reprint author), Bay Area Environm Res Inst, Sonoma, CA 95476 USA. EM bergman@ucar.edu RI Pan, Laura/A-9296-2008 OI Pan, Laura/0000-0001-7377-2114 FU National Science Foundation FX This worked benefitted from helpful conversations with and comments on early versions of the manuscript from W. Randel and three anonymous reviewers. J. Bergman and E. Jensen were visitors at the Atmospheric Chemistry Division of NCAR during the execution of this study. The National Center for Atmospheric Research is operated by the University Corporation for Atmospheric Research, under sponsorship of the National Science Foundation. NR 40 TC 1 Z9 1 U1 1 U2 8 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 MAR 27 PY 2014 VL 119 IS 6 BP 2831 EP 2845 DI 10.1002/2013JD021295 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH3SV UT WOS:000336046600009 ER PT J AU McCormack, JP Coy, L Singer, W AF McCormack, J. P. Coy, L. Singer, W. TI Intraseasonal and interannual variability of the quasi 2 day wave in the Northern Hemisphere summer mesosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID 2-DAY WAVE; QUASI-2-DAY WAVE; MIDDLE ATMOSPHERE; BAROCLINIC INSTABILITY; STRATOSPHERIC ANALYSES; GENERAL-CIRCULATION; LOWER THERMOSPHERE; PLANETARY-WAVES; TEMPERATURE; STRATOPAUSE AB This study uses global synoptic meteorological fields from a high-altitude data assimilation system to investigate the quasi 2 day wave (Q2DW) and migrating diurnal tide during the Northern Hemisphere (NH) summers of 2007-2009. By applying a two-dimensional fast Fourier transform to meridional wind and temperature fields, we identify Q2DW source regions and diagnose propagation of Q2DW activity into the upper mesosphere and lower thermosphere. We find that the Q2DW in NH summer is composed primarily of westward propagating zonal wave number 3 and wave number 4 components that originate within baroclinically unstable regions along the equatorward flank of the summer midlatitude easterly jet. The amplitude of the wave number 3 Q2DW tends to peak in July while the amplitude of the wave number 4 Q2DW tends to peak in late June and again in early August. The seasonal mean Q2DW amplitudes are largest in 2009, when the amplitude of the migrating diurnal tide in the upper mesosphere near 30 degrees N was relatively weak. However, there is no evidence of rapid amplification of the Q2DW via nonlinear interaction with the diurnal tide. Instead, variations of Q2DW amplitudes during NH summer appear to be linked to variations in the strength and location of the mesospheric easterly jet from one summer to the next, with a stronger jet producing larger Q2DW amplitudes. Linear instability model calculations based on the assimilated wind fields indicate that the fastest-growing modes are zonal wave numbers 3 and 4 with periods near 2 days that originate in the vicinity of the easterly jet. C1 [McCormack, J. P.] Naval Res Lab, Space Sci Div, Washington, DC 20375 USA. [Coy, L.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Coy, L.] Sci Syst & Applicat Inc, Lanham, MD USA. [Singer, W.] Univ Rostock, Leibniz Inst Atmospher Phys, Kuhlungsborn, Germany. RP McCormack, JP (reprint author), Naval Res Lab, Space Sci Div, Washington, DC 20375 USA. EM john.mccormack@nrl.navy.mil OI McCormack, John/0000-0002-3674-0508 FU Office of Naval Research; NASA Heliophysics Guest Investigator Program [NNH09AK64I] FX We thank three anonymous reviewers for their constructive comments. We thank Michael Stevens at the Naval Research Laboratory for his assistance with comparisons between NOGAPS-ALPHA and meteor radar winds. This work was supported in part by the Office of Naval Research and by the NASA Heliophysics Guest Investigator Program under award NNH09AK64I. NR 55 TC 3 Z9 3 U1 0 U2 5 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 MAR 27 PY 2014 VL 119 IS 6 BP 2928 EP 2946 DI 10.1002/2013JD020199 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH3SV UT WOS:000336046600014 ER PT J AU Xia, YL Ek, MB Peters-Lidard, CD Mocko, D Svoboda, M Sheffield, J Wood, EF AF Xia, Youlong Ek, Michael B. Peters-Lidard, Christa D. Mocko, David Svoboda, Mark Sheffield, Justin Wood, Eric F. TI Application of USDM statistics in NLDAS-2: Optimal blended NLDAS drought index over the continental United States SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID UNCERTAINTY ESTIMATION; 20TH-CENTURY DROUGHT; SEVERITY INDEX; MODEL; INVERSION; MONITOR AB This study performs three experiments to calibrate the drought area percentages in the continental United States (CONUS), six U. S. Drought Monitor (USDM) regions, and 48 states downloaded from the USDM archive website. The corresponding three experiments are named CONUS, Region, and State, respectively. The data sets used in these experiments are from the North American Land Data Assimilation System Phase 2 (NLDAS-2). The main purpose is to develop an automated USDM-based approach to objectively generate and reconstruct USDM-style drought maps using NLDAS-2 data by mimicking 10 year (2000-2009) USDM statistics. The results show that State and Region have larger correlation coefficients and smaller root-mean-square error (RMSE) and bias than CONUS when compared to the drought area percentages derived from the USDM, indicating that State and Region perform better than CONUS. In general, State marginally outperforms Region in terms of RMSE, bias, and correlation. Analysis of normalized optimal weight coefficients shows that soil moisture percentiles (top 1m and total column) play the dominant role in most of the 48 states. The optimal blended NLDAS drought index (OBNDI) has higher simulation skills (correlation coefficient and Nash-Sutcliffe efficiency) in the South, Southeast, High Plains, and Midwest regions when compared to those in the West and Northeast. The highest simulation skills appear in TX and OK. By using optimal equations, we can reconstruct the long-term drought area percentages and OBNDI over the continental United States for the entire period of the NLDAS-2 data sets (January 1979 to present). C1 [Xia, Youlong; Ek, Michael B.] Natl Ctr Environm Predict, Environm Modeling Ctr, College Pk, MD USA. [Xia, Youlong] NCEP, EMC, IMSG, College Pk, MD USA. [Peters-Lidard, Christa D.; Mocko, David] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Mocko, David] SAIC, Greenbelt, MD USA. [Svoboda, Mark] Univ Nebraska, Natl Drought Mitigat Ctr, Lincoln, NE USA. [Sheffield, Justin; Wood, Eric F.] Princeton Univ, Dept Environm & Civil Engn, Princeton, NJ 08544 USA. RP Xia, YL (reprint author), Natl Ctr Environm Predict, Environm Modeling Ctr, College Pk, MD USA. EM Youlong.Xia@noaa.gov RI Peters-Lidard, Christa/E-1429-2012 OI Peters-Lidard, Christa/0000-0003-1255-2876 FU Modeling, Analysis, Predictions, and Projections (MAPP) Program within NOAA's Climate Program Office FX The NLDAS project is sponsored by the Modeling, Analysis, Predictions, and Projections (MAPP) Program within NOAA's Climate Program Office. The authors thank Weizheng Zhen, Helin Wei, and three anonymous reviewers whose edits and comments greatly improved the quality and readability of this manuscript. Y.X. also thanks Kingtse Mo from Climate Prediction Center who helped compute spi3 and spi6. NR 31 TC 13 Z9 13 U1 1 U2 11 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 MAR 27 PY 2014 VL 119 IS 6 BP 2947 EP 2965 DI 10.1002/2013JD020994 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH3SV UT WOS:000336046600015 ER PT J AU Zou, YH Yu, JY Lee, T Lu, MM Kim, ST AF Zou, Yuhao Yu, Jin-Yi Lee, Tong Lu, Mong-Ming Kim, Seon Tae TI CMIP5 model simulations of the impacts of the two types of El Nino on the US winter temperature SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OUTGOING LONGWAVE RADIATION; NORTH-AMERICAN PRECIPITATION; SEA-SURFACE TEMPERATURES; WESTERN UNITED-STATES; SOUTHERN-OSCILLATION; HEMISPHERE WINTER; SST ANOMALIES; PACIFIC; PATTERNS; TELECONNECTIONS AB Thirty Coupled Model Intercomparison Project phase 5 (CMIP5) preindustrial simulations are examined to contrast impacts of the two types of El Nino on the U. S. winter temperatures. The CMIP5 models are found more capable of simulating the observed eastern Pacific (EP) El Nino impacts (a warm northeast, cold southwest pattern over the U. S.) but less capable of simulating the observed central Pacific (CP) El Nino impacts (a warm northwest, cold southeast pattern). During EP El Nino, sea surface temperature (SST) anomalies influence the Walker circulation giving rise to a basin-wide pattern of outgoing longwave radiation (OLR) anomalies. The modeled atmospheric responses to the EP El Nino are thus less sensitive to the detailed structure of the simulated SST anomalies and can be well simulated by most of the CMIP5 models. In contrast, the SST anomalies during the CP El Nino affect the strength of the Walker circulation less effectively than the EP El Nino. OLR anomalies are local, rather than basin wide. The modeled atmospheric responses to the CP El Nino therefore depend more on how realistically the CP El Nino SST anomalies are simulated in the models. As a result, the CP El Nino's impact on the U. S. winter temperature, controlled by the atmospheric wave train response to the OLR forcing, is less well simulated by the CMIP5 models. This conclusion is supported by an examination of the Pacific North American and tropical/Northern Hemisphere patterns produced by the CMIP5 models in response to the two types of El Nino. C1 [Zou, Yuhao; Yu, Jin-Yi] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92717 USA. [Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Lu, Mong-Ming] Cent Weather Bur, Res & Dev Ctr, Taipei, Taiwan. [Kim, Seon Tae] CSIRO, Marine & Atmospher Res, Aspendale, Vic, Australia. RP Yu, JY (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92717 USA. EM jyyu@uci.edu OI Kim, Seon Tae/0000-0003-2628-0904 FU NOAA's MAPP Program [A11OAR4310102]; NSF [AGS-1233542] FX We would like to thank three anonymous reviewers and Editor Chidong Zhang for their comments that have helped improve this paper. We also benefited from the discussions with Gerry Bell at NOAA on the analysis of the PNA and TNH patterns. This research was supported by NOAA's MAPP Program (grant A11OAR4310102) and NSF (grant AGS-1233542). This work was conducted as part of the NOAA MAPP's CMIP5 Task Force. The NCEP-NCAR Reanalysis and the NOAA interpolated OLR data are downloaded from the NOAA/ESRL PSD data portal (http://www.esrl.noaa.gov/psd), and the CMIP5 preindustrial simulations are downloaded from the CMIP5 portal (http://pcmdi9.llnl.gov/). NR 40 TC 9 Z9 9 U1 2 U2 13 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 MAR 27 PY 2014 VL 119 IS 6 BP 3076 EP 3092 DI 10.1002/2013JD021064 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH3SV UT WOS:000336046600022 ER PT J AU Wang, AH Barlage, M Zeng, XB Draper, CS AF Wang, Aihui Barlage, Michael Zeng, Xubin Draper, Clara Sophie TI Comparison of land skin temperature from a land model, remote sensing, and in situ measurement SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SURFACE TEMPERATURE; ROUGHNESS LENGTH; ARID REGIONS; EMISSIVITY; MODIS; PARAMETERIZATION; VALIDATION; FLUXES; ASSIMILATION; VEGETATION AB Land skin temperature (Ts) is an important parameter in the energy exchange between the land surface and atmosphere. Here hourly Ts from the Community Land Model version 4.0, Moderate Resolution Imaging Spectroradiometer (MODIS) satellite observations, and in situ observations from the Coordinated Energy and Water Cycle Observation Project in 2003 were compared. Both modeled and MODIS Ts were interpolated to the 12 station locations, and comparisons were performed under MODIS clear-sky condition. Over four semiarid stations, both MODIS and modeled Ts show negative biases compared to in situ data, but MODIS shows an overall better performance. Global distribution of differences between MODIS and modeled Ts shows diurnal, seasonal, and spatial variations. Over sparsely vegetated areas, the model Ts is generally lower than the MODIS-observed Ts during the daytime, while the situation is opposite at nighttime. The revision of roughness length for heat and the constraint of minimum friction velocity from Zeng et al. (2012) bring the modeled Ts closer to MODIS during the day and have little effect on Ts at night. Five factors contributing to the Ts differences between the model and MODIS are identified, including the difficulty in properly accounting for cloud cover information at the appropriate temporal and spatial resolutions, and uncertainties in surface energy balance computation, atmospheric forcing data, surface emissivity, and MODIS Ts data. These findings have implications for the cross evaluation of modeled and remotely sensed Ts, as well as the data assimilation of Ts observations into Earth system models. C1 [Wang, Aihui] Chinese Acad Sci, Inst Atmospher Phys, Nansen Zhu Int Res Ctr, Beijing, Peoples R China. [Barlage, Michael] Natl Ctr Atmospher Res, Res Applicat Lab, Boulder, CO 80307 USA. [Zeng, Xubin] Univ Arizona, Dept Atmospher Sci, Tucson, AZ USA. [Draper, Clara Sophie] NASA GSFC, Global Modeling & Assimilat Off, Greenbelt, MD USA. [Draper, Clara Sophie] Univ Space Res Assoc, GESTAR, Columbia, MD USA. RP Wang, AH (reprint author), Chinese Acad Sci, Inst Atmospher Phys, Nansen Zhu Int Res Ctr, Beijing, Peoples R China. EM wangaihui@mail.iap.ac.cn RI Draper, Clara/P-6097-2016; OI Draper, Clara/0000-0002-8299-4939; Zeng, Xubin/0000-0001-7352-2764 FU Department of Science and Technology of China [2010CB428403]; National Science Foundation of China [41275110]; National Science Foundation [AGS-0944101]; NASA [NASA (NNX09A021G]; NOAA [NA13NES4400003]; NASA Modeling, Analysis, and Prediction Program; National Climate Assessment FX The work of A. W. was supported by the Department of Science and Technology of China under grant 2010CB428403 and the National Science Foundation of China under grant 41275110; the work of X.Z. was supported by the National Science Foundation (AGS-0944101) and NASA (NNX09A021G), while the work of M. B. was supported by NOAA (NA13NES4400003), and the work of C. S. D. was supported by the NASA Modeling, Analysis, and Prediction Program and the National Climate Assessment. Three anonymous reviewers are thanked for valuable comments and suggestions. The CEOP station observation data were obtained from http://www.ceop.net, the SURFRAD data were downloaded from http://www.srrb.noaa.gov, and the MODIS skin temperature was from https://lpdaac.usgs.gov/. NR 41 TC 10 Z9 10 U1 3 U2 21 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 MAR 27 PY 2014 VL 119 IS 6 BP 3093 EP 3106 DI 10.1002/2013JD021026 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH3SV UT WOS:000336046600023 ER PT J AU Kuba, N Hashino, T Satoh, M Suzuki, K AF Kuba, Naomi Hashino, Tempei Satoh, Masaki Suzuki, Kentaroh TI Relationships between layer-mean radar reflectivity and columnar effective radius of warm cloud: Numerical study using a cloud microphysical bin model SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MULTICOMPONENT FRAMEWORK; A-TRAIN; PART II; PRECIPITATION; ALGORITHM; EVOLUTION; SIMULATION; BREAKUP; CUMULUS; MISSION AB The relationship between the layer-mean radar reflectivity, Ze, and the columnar effective particle radius, Re, in evolving shallow warm clouds was investigated by numerical experiments using a hybrid cloud microphysical model and a forward simulator of satellite measurements. Changes in the cloud/rain droplet size distributions were traced in a kinematically driven warm cloud for various values of number concentration of cloud condensation nuclei (CCN) and maximum updraft velocity. In contrast to previous interpretations of the observed data, we found four paths for the relationships between Ze and Re during the lifetime of a warm cloud. In the first path, both Ze and Re increase with an approximate sixth-power dependency, indicating a stage of condensational growth of droplets without raindrops in the cloud. In the second path, only Ze increases rapidly, while Re remains almost constant (Re-second), indicating a stage in which few raindrops emerge in the cloud before appreciable precipitation occurs at the surface. This second path was newly identified in this study. In the third path, Re increases rapidly while Ze does not change greatly, indicating a stage of coalescence of droplets. Precipitation reaches the surface at the end of the third path. In the fourth path, both Ze and Re decrease, indicating a greater contribution of raindrop evaporation and weakening or termination of precipitation. The maximum values of Ze and Re and the constant value of Re-second for the second stage depend on the CCN number concentration and the updraft velocity. C1 [Kuba, Naomi; Hashino, Tempei; Satoh, Masaki] Univ Tokyo, Atmosphere & Ocean Res Inst, Kashiwa, Chiba, Japan. [Kuba, Naomi; Satoh, Masaki] Japan Agcy Marine Earth Sci & Technol, Res Inst Global Change, Yokohama, Kanagawa, Japan. [Hashino, Tempei] Acad Sinica, Res Ctr Environm Changes, Taipei 115, Taiwan. [Suzuki, Kentaroh] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Kuba, N (reprint author), Univ Tokyo, Atmosphere & Ocean Res Inst, Kashiwa, Chiba, Japan. EM kuba@aori.u-tokyo.ac.jp RI Satoh, Masaki/G-3325-2015; Suzuki, Kentaroh/C-3624-2011 OI Satoh, Masaki/0000-0003-3580-8897; FU MEXT Program for Risk Information on Climate Change and High Performance Computing Infrastructure (HPCI) Strategic Programs for Innovative Research (SPIRE) Field 3 Projection of Planet Earth Variations for Mitigating Natural Disasters; National Aeronautics and Space Administration of the U.S. FX The authors sincerely thank the Meteorological Research Institute (MRI) for offering the aircraft observational CCN data that they collected as part of the Special Coordination Funds for Promoting Science and Technology program, the "Japanese Cloud Seeding Experiments for Precipitation Augmentation (JCSEPA)," supported by the Ministry of Education, Culture, Sports, Science and Technology of Japan (MEXT). This study was supported by the MEXT Program for Risk Information on Climate Change and High Performance Computing Infrastructure (HPCI) Strategic Programs for Innovative Research (SPIRE) Field 3 Projection of Planet Earth Variations for Mitigating Natural Disasters. The Joint Simulator used in this study was developed under the Earth Clouds, Aerosols and Radiation Explorer (EarthCARE) project of the Japan Aerospace Exploration Agency (JAXA). Part of the research was performed at the Jet Propulsion Laboratory of the California Institute of Technology, under a contract with the National Aeronautics and Space Administration of the U.S. The authors also sincerely thank the anonymous referees for their useful comments. NR 29 TC 1 Z9 1 U1 0 U2 5 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 MAR 27 PY 2014 VL 119 IS 6 BP 3281 EP 3294 DI 10.1002/2013JD020276 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH3SV UT WOS:000336046600034 ER PT J AU Li, J Carlson, BE Lacis, AA AF Li, Jing Carlson, Barbara E. Lacis, Andrew A. TI Revisiting AVHRR tropospheric aerosol trends using principal component analysis SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID PINATUBO VOLCANIC AEROSOL; MOUNT-PINATUBO; STRATOSPHERIC AEROSOLS; EL-CHICHON; RETRIEVALS; OCEAN; VISIBILITY; RADIANCES; SURFACE; CLOUDS AB The advanced very high resolution radiometer (AVHRR) satellite instruments provide a nearly 25 year continuous record of global aerosol properties over the ocean. It offers valuable insights into the long-term change in global aerosol loading. However, the AVHRR data record is heavily influenced by two volcanic eruptions, El Chichon on March 1982 and Mount Pinatubo on June 1991. The gradual decay of volcanic aerosols may last years after the eruption, which potentially masks the estimation of aerosol trends in the lower troposphere, especially those of anthropogenic origin. In this study, we show that a principal component analysis approach effectively captures the bulk of the spatial and temporal variability of volcanic aerosols into a single mode. The spatial pattern and time series of this mode provide a good match to the global distribution and decay of volcanic aerosols. We further reconstruct the data set by removing the volcanic aerosol component and reestimate the global and regional aerosol trends. Globally, the reconstructed data set reveals an increase of aerosol optical depth from 1985 to 1990 and decreasing trend from 1994 to 2006. Regionally, in the 1980s, positive trends are observed over the North Atlantic and North Arabian Sea, while negative tendencies are present off the West African coast and North Pacific. During the 1994 to 2006 period, the Gulf of Mexico, North Atlantic close to Europe, and North Africa exhibit negative trends, while the coastal regions of East and South Asia, the Sahel region, and South America show positive trends. C1 [Li, Jing; Carlson, Barbara E.; Lacis, Andrew A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Li, Jing] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. RP Li, J (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM jl2862@columbia.edu FU NASA [509496.02.08.04.24] FX The AVHRR AOD data used in this study were provided by the GACP project team, downloaded from http://gacp.giss.nasa.gov/data/time_ser/. The SAGE II data were provided by the NASA Langley Research Center and the NASA Langley Radiation and Aerosols Branch for providing the SAGE II data, available at https://eosweb.larc.nasa.gov. Data set name: SAGE2_AEROSOL_O3_N2O_H2O_BINARY_V7.0. The MISR AOD data were provided by the NASA Langley Research Center Atmospheric Science Data Center, available at https://eosweb.larc.nasa.gov. Data set name: MISR_AEROOSL_CLIM. MODIS AOD data were downloaded by Goddard Space Flight Center Level 1 and Atmosphere Archive and Distribution System, at http://laadsweb.nascom.nasa.gov/. Data set name: MOD08_M3-Level 3 Monthly Joint Aerosol/Water Vapor/Cloud Product. This research was funded by the NASA climate grant 509496.02.08.04.24. Jing Li was also funded by the NASA Postdoctoral Program. NR 50 TC 4 Z9 4 U1 1 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 MAR 27 PY 2014 VL 119 IS 6 BP 3309 EP 3320 DI 10.1002/2013JD020789 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH3SV UT WOS:000336046600036 ER PT J AU Mlynczak, MG Hunt, LA Marshall, BT Mertens, CJ Marsh, DR Smith, AK Russell, JM Siskind, DE Gordley, LL AF Mlynczak, Martin G. Hunt, Linda A. Marshall, B. Thomas Mertens, Christopher J. Marsh, Daniel R. Smith, Anne K. Russell, James M. Siskind, David E. Gordley, Larry L. TI Atomic hydrogen in the mesopause region derived from SABER: Algorithm theoretical basis, measurement uncertainty, and results SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID UPPER MESOSPHERE; OXYGEN DENSITY; ATMOSPHERE; EMISSIONS; RATES AB Atomic hydrogen (H) is a fundamental component in the photochemistry and energy balance of the terrestrial mesopause region (80-100 km). H is generated primarily by photolysis of water vapor and participates in a highly exothermic reaction with ozone. This reaction is a significant source of heat in the mesopause region and also creates highly vibrationally excited hydroxyl (OH) from which the Meinel band radiative emission features originate. Concentrations (cm(-3)) and volume mixing ratios of H are derived from observations of infrared emission from the OH (upsilon = 9+8, Delta upsilon = 2) vibration-rotation bands near 2.0 mu m made by the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument on the NASA Thermosphere Ionosphere Mesosphere Energetics and Dynamics satellite. The algorithms for deriving day and night H are described herein. Day and night concentrations exhibit excellent agreement between 87 and 95 km. SABER H results also exhibit good agreement with observations from the Solar Mesosphere Explorer made nearly 30 years ago. An apparent inverse dependence on the solar cycle is observed in the SABER H concentrations, with the H increasing as solar activity decreases. This increase is shown to be primarily due to the temperature dependence of various reaction rate coefficients for H photochemistry. The SABER H data, coupled with SABER atomic oxygen, ozone, and temperature, enable tests of mesospheric photochemistry and energetics in atmospheric models, studies of formation of polar mesospheric clouds, and studies of atmospheric evolution via escape of hydrogen. These data and studies are made possible by the wide range of parameters measured simultaneously by the SABER instrument. C1 [Mlynczak, Martin G.; Mertens, Christopher J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Hunt, Linda A.] SSAI, Hampton, VA USA. [Marshall, B. Thomas; Gordley, Larry L.] GATS Inc, Newport News, VA USA. [Marsh, Daniel R.; Smith, Anne K.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Russell, James M.] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. [Siskind, David E.] Naval Res Lab, Washington, DC USA. RP Mlynczak, MG (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM m.g.mlynczak@nasa.gov RI Marsh, Daniel/A-8406-2008 OI Marsh, Daniel/0000-0001-6699-494X NR 22 TC 4 Z9 4 U1 2 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 MAR 27 PY 2014 VL 119 IS 6 BP 3516 EP 3526 DI 10.1002/2013JD021263 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH3SV UT WOS:000336046600048 ER PT J AU Pan, LL Paulik, LC Honomichl, SB Munchak, LA Bian, JC Selkirk, HB Vomel, H AF Pan, Laura L. Paulik, Laura C. Honomichl, Shawn B. Munchak, Leigh A. Bian, Jianchun Selkirk, Henry B. Voemel, Holger TI Identification of the tropical tropopause transition layer using the ozone-water vapor relationship SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID LOWERMOST STRATOSPHERE; TROPOSPHERE; TRANSPORT; CLIMATOLOGY; EXCHANGE; MONSOON; SUMMER; HEIGHT; MODEL AB We present a method of identifying the tropical tropopause transition layer (TTL) using chemical tracer-tracer relationships. Coincident ozone (O-3) and water vapor (H2O) measurements over Alajuela, Costa Rica (similar to 10 degrees N), in July and August 2007 are used to demonstrate the concept. In the tracer-tracer space, the O-3 and H2O relationship helps to separate the transition layer air mass from the background troposphere and stratosphere. This tracer relationship-based transition layer is found to span an approximately 40 K potential temperature range between 340 and 380 K and is largely confined between the level of minimum stability (LMS) and the cold point tropopause (CPT). This chemical composition-based transition layer is, therefore, consistent with a definition of the TTL based on the thermal structure, for which the LMS and CPT are the lower and upper boundaries of TTL, respectively. We also examine the transition layer over the region of Asian summer monsoon (ASM) anticyclone using the measurements over Kunming, China (similar to 25 degrees N), and compare its behavior with the TTL structure in the deep tropics. The comparison shows that the transition layer over the ASM is similar to the TTL, although the data suggest the ASM transition layer lies at higher potential temperature levels and is potentially prone to the influence of extratropical processes. C1 [Pan, Laura L.; Paulik, Laura C.; Honomichl, Shawn B.; Munchak, Leigh A.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Bian, Jianchun] Chinese Acad Sci, Inst Atmospher Phys, Key Lab Middle Atmosphere & Global Environm Obser, Beijing, Peoples R China. [Selkirk, Henry B.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Voemel, Holger] GRUAN Lead Ctr, Meteorol Observ, Lindenberg, Germany. RP Pan, LL (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. EM liwen@ucar.edu RI Pan, Laura/A-9296-2008 OI Pan, Laura/0000-0001-7377-2114 FU National Science Foundation; National Basic Research Program of China [2010CB428602]; National Natural Science Foundation of China [41175040] FX This work is supported by the National Science Foundation through its sponsorship to the National Center for Atmospheric Research. The SWOP campaign is supported by the National Basic Research Program of China (2010CB428602) and the National Natural Science Foundation of China (41175040). The authors thank Bill Randel, John Bergman, Cameron Homeyer, and three anonymous reviewers for helpful suggestions. NR 45 TC 7 Z9 7 U1 0 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 MAR 27 PY 2014 VL 119 IS 6 BP 3586 EP 3599 DI 10.1002/2013JD020558 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH3SV UT WOS:000336046600051 ER PT J AU Hoehler, TM Alperin, MJ AF Hoehler, Tori M. Alperin, Marc J. TI Methane minimalism SO NATURE LA English DT Editorial Material C1 [Hoehler, Tori M.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Alperin, Marc J.] Univ N Carolina, Dept Marine Sci, Chapel Hill, NC 27599 USA. RP Hoehler, TM (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. EM tori.m.hoehler@nasa.gov; alperin@email.unc.edu NR 7 TC 6 Z9 6 U1 7 U2 55 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 MAR 27 PY 2014 VL 507 IS 7493 BP 436 EP 437 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AD6WN UT WOS:000333402000025 PM 24670756 ER PT J AU Aartsen, MG Abbasi, R Ackermann, M Adams, J Aguilar, JA Ahlers, M Altmann, D Arguelles, C Arlen, TC Auffenberg, J Bai, X Baker, M Barwick, SW Baum, V Bay, R Beatty, JJ Tjus, JB Becker, KH BenZvi, S Berghaus, P Berley, D Bernardini, E Bernhard, A Besson, DZ Binder, G Bindig, D Bissok, M Blaufuss, E Blumenthal, J Boersma, DJ Bohm, C Bose, D Boser, S Botner, O Brayeur, L Bretz, HP Brown, AM Bruijn, R Casey, J Casier, M Chirkin, D Christov, A Christy, B Clark, K Classen, L Clevermann, F Coenders, S Cohen, S Cowen, DF Silva, AHC Danninger, M Daughhetee, J Davis, JC Day, M de Andre, JPAM De Clercq, C De Ridder, S Desiati, P de Vries, KD De With, M DeYoung, T Diaz-Velez, JC Dunkman, M Eagan, R Eberhardt, B Eichmann, B Eisch, J Euler, S Evenson, PA Fadiran, O Fazely, AR Fedynitch, A Feintzeig, J Feusels, T Filimonov, K Finley, C Fischer-Wasels, T Flis, S Franckowiak, A Frantzen, K Fuchs, T Gaisser, TK Gallagher, J Gerhardt, L Gladstone, L Glusenkamp, T Goldschmidt, A Golup, G Gonzalez, JG Goodman, JA Gora, D Grandmont, DT Grant, D Gretskov, P Groh, JC Gross, A Ha, C Ismail, AH Hallen, P Hallgren, A Halzen, F Hanson, K Hebecker, D Heereman, D Heinen, D Helbing, K Hellauer, R Hickford, S Hill, GC Hoffman, KD Hoffmann, R Homeier, A Hoshina, K Huang, F Huelsnitz, W Hulth, PO Hultqvist, K Hussain, S Ishihara, A Jacobi, E Jacobsen, J Jagielski, K Japaridze, GS Jero, K Jlelati, O Kaminsky, B Kappes, A Karg, T Karle, A Kauer, M Kelley, JL Kiryluk, J Klas, J Klein, SR Kohne, JH Kohnen, G Kolanoski, H Kopke, L Kopper, C Kopper, S Koskinen, DJ Kowalski, M Krasberg, M Kriesten, A Krings, K Kroll, G Kunnen, J Kurahashi, N Kuwabara, T Labare, M Landsman, H Larson, MJ Lesiak-Bzdak, M Leuermann, M Leute, J Lunemann, J Macias, O Madsen, J Maggi, G Maruyama, R Mase, K Matis, HS McNally, F Meagher, K Merck, M Meures, T Miarecki, S Middell, E Milke, N Miller, J Mohrmann, L Montaruli, T Morse, R Nahnhauer, R Naumann, U Niederhausen, H Nowicki, SC Nygren, DR Obertacke, A Odrowski, S Olivas, A Omairat, A O'Murchadha, A Palczewski, T Paul, L Pepper, JA de los Heros, CP Pfendner, C Pieloth, D Pinat, E Posselt, J Price, PB Przybylski, GT Quinnan, M Radel, L Rameez, M Rawlins, K Redl, P Reimann, R Resconi, E Rhode, W Ribordy, M Richman, M Riedel, B Robertson, S Rodrigues, JP Rott, C Ruhe, T Ruzybayev, B Ryckbosch, D Saba, SM Sander, HG Santander, M Sarkar, S Schatto, K Scheriau, F Schmidt, T Schmitz, M Schoenen, S Schoneberg, S Schonwald, A Schukraft, A Schulte, L Schulz, O Seckel, D Sestayo, Y Seunarine, S Shanidze, R Sheremata, C Smith, MWE Soldin, D Spiczak, GM Spiering, C Stamatikos, M Stanev, T Stanisha, NA Stasik, A Stezelberger, T Stokstad, RG Stossl, A Strahler, EA Strom, R Strotjohann, NL Sullivan, GW Taavola, H Taboada, I Tamburro, A Tepe, A Ter-Antonyan, S Tesic, G Tilav, S Toale, PA Tobin, MN Toscano, S Tselengidou, M Unger, E Usner, M Vallecorsa, S van Eijndhoven, N van Overloop, A van Santen, J Vehring, M Voge, M Vraeghe, M Walck, C Waldenmaier, T Wallraff, M Weaver, C Wellons, M Wendt, C Westerhoff, S Whelan, B Whitehorn, N Wiebe, K Wiebusch, CH Williams, DR Wissing, H Wolf, M Wood, TR Woschnagg, K Xu, DL Xu, XW Yanez, JP Yodh, G Yoshida, S Zarzhitsky, P Ziemann, J Zierke, S Zoll, M AF Aartsen, M. G. Abbasi, R. Ackermann, M. Adams, J. Aguilar, J. A. Ahlers, M. Altmann, D. Arguelles, C. Arlen, T. C. Auffenberg, J. Bai, X. Baker, M. Barwick, S. W. Baum, V. Bay, R. Beatty, J. J. Tjus, J. Becker Becker, K. -H. BenZvi, S. Berghaus, P. Berley, D. Bernardini, E. Bernhard, A. Besson, D. Z. Binder, G. Bindig, D. Bissok, M. Blaufuss, E. Blumenthal, J. Boersma, D. J. Bohm, C. Bose, D. Boeser, S. Botner, O. Brayeur, L. Bretz, H. -P. Brown, A. M. Bruijn, R. Casey, J. Casier, M. Chirkin, D. Christov, A. Christy, B. Clark, K. Classen, L. Clevermann, F. Coenders, S. Cohen, S. Cowen, D. F. Silva, A. H. Cruz Danninger, M. Daughhetee, J. Davis, J. C. Day, M. de Andre, J. P. A. M. De Clercq, C. De Ridder, S. Desiati, P. de Vries, K. D. De With, M. DeYoung, T. Diaz-Velez, J. C. Dunkman, M. Eagan, R. Eberhardt, B. Eichmann, B. Eisch, J. Euler, S. Evenson, P. A. Fadiran, O. Fazely, A. R. Fedynitch, A. Feintzeig, J. Feusels, T. Filimonov, K. Finley, C. Fischer-Wasels, T. Flis, S. Franckowiak, A. Frantzen, K. Fuchs, T. Gaisser, T. K. Gallagher, J. Gerhardt, L. Gladstone, L. Gluesenkamp, T. Goldschmidt, A. Golup, G. Gonzalez, J. G. Goodman, J. A. Gora, D. Grandmont, D. T. Grant, D. Gretskov, P. Groh, J. C. Gross, A. Ha, C. Ismail, A. Haj Hallen, P. Hallgren, A. Halzen, F. Hanson, K. Hebecker, D. Heereman, D. Heinen, D. Helbing, K. Hellauer, R. Hickford, S. Hill, G. C. Hoffman, K. D. Hoffmann, R. Homeier, A. Hoshina, K. Huang, F. Huelsnitz, W. Hulth, P. O. Hultqvist, K. Hussain, S. Ishihara, A. Jacobi, E. Jacobsen, J. Jagielski, K. Japaridze, G. S. Jero, K. Jlelati, O. Kaminsky, B. Kappes, A. Karg, T. Karle, A. Kauer, M. Kelley, J. L. Kiryluk, J. Klaes, J. Klein, S. R. Koehne, J. -H. Kohnen, G. Kolanoski, H. Koepke, L. Kopper, C. Kopper, S. Koskinen, D. J. Kowalski, M. Krasberg, M. Kriesten, A. Krings, K. Kroll, G. Kunnen, J. Kurahashi, N. Kuwabara, T. Labare, M. Landsman, H. Larson, M. J. Lesiak-Bzdak, M. Leuermann, M. Leute, J. Luenemann, J. Macias, O. Madsen, J. Maggi, G. Maruyama, R. Mase, K. Matis, H. S. McNally, F. Meagher, K. Merck, M. Meures, T. Miarecki, S. Middell, E. Milke, N. Miller, J. Mohrmann, L. Montaruli, T. Morse, R. Nahnhauer, R. Naumann, U. Niederhausen, H. Nowicki, S. C. Nygren, D. R. Obertacke, A. Odrowski, S. Olivas, A. Omairat, A. O'Murchadha, A. Palczewski, T. Paul, L. Pepper, J. A. de los Heros, C. Perez Pfendner, C. Pieloth, D. Pinat, E. Posselt, J. Price, P. B. Przybylski, G. T. Quinnan, M. Raedel, L. Rameez, M. Rawlins, K. Redl, P. Reimann, R. Resconi, E. Rhode, W. Ribordy, M. Richman, M. Riedel, B. Robertson, S. Rodrigues, J. P. Rott, C. Ruhe, T. Ruzybayev, B. Ryckbosch, D. Saba, S. M. Sander, H. -G. Santander, M. Sarkar, S. Schatto, K. Scheriau, F. Schmidt, T. Schmitz, M. Schoenen, S. Schoeneberg, S. Schoenwald, A. Schukraft, A. Schulte, L. Schulz, O. Seckel, D. Sestayo, Y. Seunarine, S. Shanidze, R. Sheremata, C. Smith, M. W. E. Soldin, D. Spiczak, G. M. Spiering, C. Stamatikos, M. Stanev, T. Stanisha, N. A. Stasik, A. Stezelberger, T. Stokstad, R. G. Stoessl, A. Strahler, E. A. Strom, R. Strotjohann, N. L. Sullivan, G. W. Taavola, H. Taboada, I. Tamburro, A. Tepe, A. Ter-Antonyan, S. Tesic, G. Tilav, S. Toale, P. A. Tobin, M. N. Toscano, S. Tselengidou, M. Unger, E. Usner, M. Vallecorsa, S. van Eijndhoven, N. van Overloop, A. van Santen, J. Vehring, M. Voge, M. Vraeghe, M. Walck, C. Waldenmaier, T. Wallraff, M. Weaver, Ch. Wellons, M. Wendt, C. Westerhoff, S. Whelan, B. Whitehorn, N. Wiebe, K. Wiebusch, C. H. Williams, D. R. Wissing, H. Wolf, M. Wood, T. R. Woschnagg, K. Xu, D. L. Xu, X. W. Yanez, J. P. Yodh, G. Yoshida, S. Zarzhitsky, P. Ziemann, J. Zierke, S. Zoll, M. CA IceCube Collaboration TI Search for a diffuse flux of astrophysical muon neutrinos with the IceCube 59-string configuration SO PHYSICAL REVIEW D LA English DT Article ID HIGH-ENERGY NEUTRINOS; RATIO; PERFORMANCE; TELESCOPE; DETECTORS; SELECTION; ICE AB A search for high-energy neutrinos was performed using data collected by the IceCube Neutrino Observatory from May 2009 to May 2010, when the array was running in its 59-string configuration. The data sample was optimized to contain muon neutrino induced events with a background contamination of atmospheric muons of less than 1%. These data, which are dominated by atmospheric neutrinos, are analyzed with a global likelihood fit to search for possible contributions of prompt atmospheric and astrophysical neutrinos, neither of which have yet been identified. Such signals are expected to follow a harder energy spectrum than conventional atmospheric neutrinos. In addition, the zenith angle distribution differs for astrophysical and atmospheric signals. A global fit of the reconstructed energies and directions of observed events is performed, including possible neutrino flux contributions for an astrophysical signal and atmospheric backgrounds as well as systematic uncertainties of the experiment and theoretical predictions. The best fit yields an astrophysical signal flux for nu(mu) + (nu) over bar (mu) of E-2. Phi(E) = 0.25 x 10(-8) GeV cm(-2) s(-1) sr(-1), and a zero prompt component. Although the sensitivity of this analysis for astrophysical neutrinos surpasses the Waxman and Bahcall upper bound, the experimental limit at 90% confidence level is a factor of 1.5 above at a flux of E-2 . Phi(E) = 1.44 x 10(-8) GeV cm(-2) s(-1) sr(-1). C1 [Bissok, M.; Blumenthal, J.; Coenders, S.; Euler, S.; Gretskov, P.; Hallen, P.; Heinen, D.; Jagielski, K.; Kriesten, A.; Krings, K.; Leuermann, M.; Paul, L.; Raedel, L.; Reimann, R.; Schoenen, S.; Schukraft, A.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.; Zierke, S.] Univ Aachen, RWTH, Inst Phys 3, D-52056 Aachen, Germany. [Aartsen, M. G.; Hill, G. C.; Robertson, S.; Whelan, B.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. [Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA. [Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA. [Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA. [Bay, R.; Binder, G.; Filimonov, K.; Gerhardt, L.; Ha, C.; Klein, S. R.; Miarecki, S.; Price, P. B.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Binder, G.; Gerhardt, L.; Goldschmidt, A.; Ha, C.; Klein, S. R.; Matis, H. S.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [De With, M.; Kolanoski, H.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. [Tjus, J. Becker; Eichmann, B.; Fedynitch, A.; Saba, S. M.; Schoeneberg, S.; Unger, E.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany. [Boeser, S.; Franckowiak, A.; Hebecker, D.; Homeier, A.; Kowalski, M.; Schulte, L.; Stasik, A.; Strotjohann, N. L.; Usner, M.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany. [Hanson, K.; Heereman, D.; Meures, T.; O'Murchadha, A.; Pinat, E.] Univ Libre Brussels, Sci Fac CP230, B-1050 Brussels, Belgium. [Brayeur, L.; Casier, M.; De Clercq, C.; de Vries, K. D.; Golup, G.; Kunnen, J.; Maggi, G.; Miller, J.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium. [Ishihara, A.; Mase, K.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan. [Adams, J.; Brown, A. M.; Hickford, S.; Macias, O.] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand. [Berley, D.; Blaufuss, E.; Christy, B.; Goodman, J. A.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Richman, M.; Schmidt, T.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Koskinen, D. J.; Sarkar, S.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Clevermann, F.; Frantzen, K.; Fuchs, T.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.; Scheriau, F.; Schmitz, M.; Ziemann, J.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany. [Grandmont, D. T.; Grant, D.; Nowicki, S. C.; Odrowski, S.; Sheremata, C.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Altmann, D.; Classen, L.; Gora, D.; Kappes, A.; Tselengidou, M.] Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany. [Aguilar, J. A.; Christov, A.; Montaruli, T.; Rameez, M.; Vallecorsa, S.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland. [De Ridder, S.; Feusels, T.; Ismail, A. Haj; Jlelati, O.; Labare, M.; Ryckbosch, D.; van Overloop, A.; Vraeghe, M.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium. [Barwick, S. W.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Bruijn, R.; Cohen, S.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland. [Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Abbasi, R.; Ahlers, M.; Arguelles, C.; Auffenberg, J.; Baker, M.; BenZvi, S.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kopper, C.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; McNally, F.; Merck, M.; Morse, R.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Tobin, M. N.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA. [Baum, V.; Eberhardt, B.; Koepke, L.; Kroll, G.; Luenemann, J.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany. [Kohnen, G.] Univ Mons, B-7000 Mons, Belgium. [Bernhard, A.; Gross, A.; Leute, J.; Resconi, E.; Schulz, O.; Sestayo, Y.] Tech Univ Munich, D-85748 Garching, Germany. [Bai, X.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.] Univ Delaware, Bartol Res Inst, Dept Phys & Astron, Newark, DE 19716 USA. [Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England. [Madsen, J.; Seunarine, S.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA. [Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.] Stockholm Univ, Dept Phys, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Bose, D.; Rott, C.] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea. [Clark, K.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Larson, M. J.; Palczewski, T.; Pepper, J. A.; Toale, P. A.; Williams, D. R.; Xu, D. L.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Cowen, D. F.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Arlen, T. C.; Cowen, D. F.; de Andre, J. P. A. M.; DeYoung, T.; Dunkman, M.; Eagan, R.; Groh, J. C.; Huang, F.; Quinnan, M.; Smith, M. W. E.; Stanisha, N. A.; Tesic, G.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Boersma, D. J.; Botner, O.; Hallgren, A.; de los Heros, C. Perez; Strom, R.; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. [Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Helbing, K.; Hoffmann, R.; Klaes, J.; Kopper, S.; Naumann, U.; Obertacke, A.; Omairat, A.; Posselt, J.; Soldin, D.; Tepe, A.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany. [Ackermann, M.; Berghaus, P.; Bernardini, E.; Bretz, H. -P.; Silva, A. H. Cruz; Gluesenkamp, T.; Jacobi, E.; Kaminsky, B.; Karg, T.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Schoenwald, A.; Shanidze, R.; Spiering, C.; Stoessl, A.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany. [Bai, X.; Schukraft, A.; Stamatikos, M.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA. [Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Schukraft, A (reprint author), Univ Aachen, RWTH, Inst Phys 3, D-52056 Aachen, Germany. EM schukraft@physik.rwth-aachen.de RI Sarkar, Subir/G-5978-2011; Beatty, James/D-9310-2011; Wiebusch, Christopher/G-6490-2012; Taavola, Henric/B-4497-2011; Tjus, Julia/G-8145-2012; Koskinen, David/G-3236-2014; Auffenberg, Jan/D-3954-2014; Aguilar Sanchez, Juan Antonio/H-4467-2015; Maruyama, Reina/A-1064-2013; OI Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952; Wiebusch, Christopher/0000-0002-6418-3008; Rott, Carsten/0000-0002-6958-6033; Taavola, Henric/0000-0002-2604-2810; Ter-Antonyan, Samvel/0000-0002-5788-1369; Groh, John/0000-0001-9880-3634; Koskinen, David/0000-0002-0514-5917; Auffenberg, Jan/0000-0002-1185-9094; Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X; Schukraft, Anne/0000-0002-9112-5479; Perez de los Heros, Carlos/0000-0002-2084-5866; Strotjohann, Nora Linn/0000-0002-4667-6730; Arguelles Delgado, Carlos/0000-0003-4186-4182 FU U.S. National Science Foundation-Office of Polar Programs; U.S. National Science Foundation-Physics Division; University of Wisconsin Alumni Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin-Madison; Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy; National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; Natural Sciences and Engineering Research Council of Canada; WestGrid and Compute/Calcul Canada; Swedish Research Council; Swedish Polar Research Secretariat; Swedish National Infrastructure for Computing (SNIC); Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Helmholtz Alliance for Astroparticle Physics (HAP); Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO Odysseus programme; Flanders Institute to encourage scientific and technological research in industry (IWT); Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, NewZealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF); Danish National Research Foundation, Denmark (DNRF) FX We acknowledge the support from the following agencies: the U.S. National Science Foundation-Office of Polar Programs, the U.S. National Science Foundation-Physics Division, the University of Wisconsin Alumni Research Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid infrastructure; the U.S. Department of Energy and the National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; the Natural Sciences and Engineering Research Council of Canada, WestGrid and Compute/Calcul Canada; the Swedish Research Council, the Swedish Polar Research Secretariat, the Swedish National Infrastructure for Computing (SNIC), and the Knut and Alice Wallenberg Foundation, Sweden; the German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), the Research Department of Plasmas with Complex Interactions (Bochum), Germany; the Fund for Scientific Research (FNRS-FWO), FWO Odysseus programme, the Flanders Institute to encourage scientific and technological research in industry (IWT), the Belgian Federal Science Policy Office (Belspo); the University of Oxford, United Kingdom; the Marsden Fund, NewZealand; the Australian Research Council; the Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; the National Research Foundation of Korea (NRF); and the Danish National Research Foundation, Denmark (DNRF). NR 57 TC 44 Z9 44 U1 1 U2 12 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD MAR 25 PY 2014 VL 89 IS 6 AR 062007 DI 10.1103/PhysRevD.89.062007 PG 19 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AE9EW UT WOS:000334309000003 ER PT J AU Gold, R Paschalidis, V Etienne, ZB Shapiro, SL Pfeiffer, HP AF Gold, Roman Paschalidis, Vasileios Etienne, Zachariah B. Shapiro, Stuart L. Pfeiffer, Harald P. TI Accretion disks around binary black holes of unequal mass: General relativistic magnetohydrodynamic simulations near decoupling SO PHYSICAL REVIEW D LA English DT Article ID ACTIVE GALACTIC NUCLEI; ANGULAR-MOMENTUM TRANSPORT; WAVE STANDARD SIRENS; FINAL PARSEC PROBLEM; BROAD-LINE QUASARS; GAS PILE-UP; EDDINGTON RATIOS; CIRCUMBINARY DISKS; 1.5 MIGRATION; DUAL JETS AB We report on simulations in general relativity of magnetized disks accreting onto black hole binaries. We vary the binary mass ratio from 1: 1 to 1: 10 and evolve the systems when they orbit near the binary-disk decoupling radius. We compare (surface) density profiles, accretion rates (relative to a single, nonspinning black hole), variability, effective a-stress levels and luminosities as functions of the mass ratio. We treat the disks in two limiting regimes: rapid radiative cooling and no radiative cooling. The magnetic field lines clearly reveal jets emerging from both black hole horizons and merging into one common jet at large distances. The magnetic fields give rise to much stronger shock heating than the pure hydrodynamic flows, completely alter the disk structure, and boost accretion rates and luminosities. Accretion streams near the horizons are among the densest structures; in fact, the 1: 10 no-cooling evolution results in a refilling of the cavity. The typical effective temperature in the bulk of the disk is similar to 10(5) (M/10(8)M(circle dot))(-1/4) (L/L-edd)(1/4) K yielding characteristic thermal frequencies similar to 10(15) (M/10(8)M(circle dot))(-1/4) (L/L-edd)(1/4) (1 + z)(-1) Hz. These systems are thus promising targets for many extragalactic optical surveys, such as the LSST, WFIRST, and PanSTARRS. C1 [Gold, Roman; Paschalidis, Vasileios; Etienne, Zachariah B.; Shapiro, Stuart L.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Etienne, Zachariah B.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Etienne, Zachariah B.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Etienne, Zachariah B.] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA. [Etienne, Zachariah B.] W Virginia Univ, Dept Math, Morgantown, WV 26506 USA. [Shapiro, Stuart L.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Shapiro, Stuart L.] Univ Illinois, NCSA, Urbana, IL 61801 USA. [Pfeiffer, Harald P.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Pfeiffer, Harald P.] Canadian Inst Adv Res, Toronto, ON M5G 1Z8, Canada. RP Gold, R (reprint author), Univ Illinois, Dept Phys, Urbana, IL 61801 USA. FU NSF [AST1002667, PHY-0963136, PHY-1300903, OCI-1053575]; NASA at the University of Illinois at Urbana-Champaign [NNX11AE11G, NNX13AH44G]; Fortner Fellowship at UIUC; NSERC of Canada; Canada Chairs Program; Canadian Institute for Advanced Research; Canada Foundation for Innovation under the auspices of Compute Canada; Government of Ontario; Ontario Research Fund-Research Excellence; University of Toronto; National Science Foundation [OCI 07-25070]; state of Illinois FX It is a pleasure to thank the Illinois Relativity group REU team (Albert Kim, Lingyi Kong, Brian R. Taylor, and Francis J. Walsh) for assistance in creating Figs. 1 and 23. We thank Brian Farris for useful discussions. This paper was supported in part by NSF Grants No. AST1002667, No. PHY-0963136 and No. PHY-1300903 as well as NASA Grants No. NNX11AE11G and No. NNX13AH44G at the University of Illinois at Urbana-Champaign. V. P. gratefully acknowledges support from a Fortner Fellowship at UIUC. H. P. P. acknowledges support by NSERC of Canada, the Canada Chairs Program, and the Canadian Institute for Advanced Research. The metric initial data were computed on the GPC supercomputer at the SciNet HPC Consortium [137]. SciNet is funded by: the Canada Foundation for Innovation under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund-Research Excellence; and the University of Toronto. This work used the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by NSF Grant No. OCI-1053575. This research is part of the Blue Waters sustained-petascale computing project, which is supported by the National Science Foundation (Grant No. OCI 07-25070) and the state of Illinois. Blue Waters is a joint effort of the University of Illinois at Urbana-Champaign and its National Center for Supercomputing Applications. NR 133 TC 22 Z9 22 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD MAR 25 PY 2014 VL 89 IS 6 AR 064060 DI 10.1103/PhysRevD.89.064060 PG 28 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AE9EW UT WOS:000334309000009 ER PT J AU Wu, TJ Shamsaddini, A Pan, Y Smith, K Crichton, DJ Simonyan, V Mazumder, R AF Wu, Tsung-Jung Shamsaddini, Amirhossein Pan, Yang Smith, Krista Crichton, Daniel J. Simonyan, Vahan Mazumder, Raja TI A framework for organizing cancer-related variations from existing databases, publications and NGS data using a High-performance Integrated Virtual Environment (HIVE) SO DATABASE-THE JOURNAL OF BIOLOGICAL DATABASES AND CURATION LA English DT Article ID PROTEIN INFORMATION RESOURCE; HUMAN GENOME; BIOTECHNOLOGY INFORMATION; CLASSIFICATION-SYSTEM; REFERENCE SEQUENCES; SOMATIC MUTATIONS; NATIONAL CENTER; READ ALIGNMENT; BIG DATA; ANNOTATION AB Years of sequence feature curation by UniProtKB/Swiss-Prot, PIR-PSD, NCBI-CDD, RefSeq and other database biocurators has led to a rich repository of information on functional sites of genes and proteins. This information along with variation-related annotation can be used to scan human short sequence reads from next-generation sequencing (NGS) pipelines for presence of non-synonymous single-nucleotide variations (nsSNVs) that affect functional sites. This and similar workflows are becoming more important because thousands of NGS data sets are being made available through projects such as The Cancer Genome Atlas (TCGA), and researchers want to evaluate their biomarkers in genomic data. BioMuta, an integrated sequence feature database, provides a framework for automated and manual curation and integration of cancer-related sequence features so that they can be used in NGS analysis pipelines. Sequence feature information in BioMuta is collected from the Catalogue of Somatic Mutations in Cancer (COSMIC), ClinVar, UniProtKB and through biocuration of information available from publications. Additionally, nsSNVs identified through automated analysis of NGS data from TCGA are also included in the database. Because of the petabytes of data and information present in NGS primary repositories, a platform HIVE (High-performance Integrated Virtual Environment) for storing, analyzing, computing and curating NGS data and associated metadata has been developed. Using HIVE, 31 979 nsSNVs were identified in TCGA-derived NGS data from breast cancer patients. All variations identified through this process are stored in a Curated Short Read archive, and the nsSNVs from the tumor samples are included in BioMuta. Currently, BioMuta has 26 cancer types with 13 896 small-scale and 308 986 large-scale study-derived variations. Integration of variation data allows identifications of novel or common nsSNVs that can be prioritized in validation studies. C1 [Wu, Tsung-Jung; Shamsaddini, Amirhossein; Pan, Yang; Smith, Krista; Mazumder, Raja] George Washington Univ, Dept Biochem & Mol Med, Washington, DC 20037 USA. [Crichton, Daniel J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Simonyan, Vahan] US FDA, Ctr Biol Evaluat & Res, Rockville, MD 20852 USA. [Mazumder, Raja] George Washington Univ, McCormick Genom & Prote Ctr, Washington, DC 20037 USA. RP Mazumder, R (reprint author), George Washington Univ, Dept Biochem & Mol Med, Washington, DC 20037 USA. EM mazumder@gwu.edu OI Pan, Yang/0000-0003-3487-7233 FU National Institutes of Health [U01 CA168926]; George Washington University FX U01 CA168926 (in part) National Institutes of Health and George Washington University funds. Funding for open access charge: George Washington University. NR 55 TC 15 Z9 16 U1 1 U2 8 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1758-0463 J9 DATABASE-OXFORD JI Database PD MAR 25 PY 2014 AR bau022 DI 10.1093/database/bau022 PG 11 WC Mathematical & Computational Biology SC Mathematical & Computational Biology GA AD8OV UT WOS:000333526400001 ER PT J AU Cao, F Fichot, CG Hooker, SB Miller, WL AF Cao, Fang Fichot, Cedric G. Hooker, Stanford B. Miller, William L. TI Improved algorithms for accurate retrieval of UV/visible diffuse attenuation coefficients in optically complex, inshore waters SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Diffuse attenuation coefficient; Remote sensing reflectance; Ocean color; Algorithms; Ultraviolet radiation; Inshore waters; Global scale ID OCEAN COLOR; ULTRAVIOLET-RADIATION; NATURAL-WATERS; COASTAL WATERS; UV; PENETRATION; PHYTOPLANKTON; ABSORPTION; IRRADIANCE; SPECTRA AB Photochemical processes driven by high-energy ultraviolet radiation (UVR) in inshore, estuarine, and coastal waters play an important role in global biogeochemical cycles and biological systems. A key to modeling photochemical processes in these optically complex waters is an accurate description of the vertical distribution of UVR in the water column which can be obtained using the diffuse attenuation coefficients of downwelling irradiance (K-d(lambda)). The SeaUV/SeaUVc algorithms (Fichot et al., 2008) can accurately retrieve K-d (lambda = 320, 340, 380, 412, 443 and 490 nm) in oceanic and coastal waters using multispectral remote sensing reflectances (R-rs(lambda), SeaWiFS bands). However, SeaUV/SeaUVc algorithms are currently not optimized for use in optically complex, inshore waters, where they tend to severely underestimate K-d(lambda). Here, a new training data set of optical properties collected in optically complex, inshore waters was used to re-parameterize the original SeaUV/SeaUVc algorithms, resulting in improved K-d(lambda) retrievals for turbid, estuarine waters. Although the updated SeaUV/SeaUVc algorithms perform best in optically complex waters, the original SeaUV/SeaUVc models still perform well in most coastal and oceanic waters. Therefore, we propose a composite set of SeaUV/SeaUVc algorithms, optimized for K-d(lambda) retrieval in almost all marine systems, ranging from oceanic to inshore waters. The composite algorithm set can retrieve K-d from ocean color with good accuracy across this wide range of water types (e.g., within a mean relative error of 13% for K-d(340)). A validation step using three independent, in situ data sets indicates that the composite SeaUV/SeaUVc can generate accurate K-d(lambda) values at lambda = 320-490 nm from ocean color on a global scale. Taking advantage of the inherent benefits of our statistical methods, we pooled the validation data with the training set, obtaining an optimized composite model for estimating K-d(lambda) in UV wavelengths for almost all marine waters. This "optimized composite" set of SeaUV/SeaUVc algorithms will provide the optical community with improved ability to quantify the role of solar UV radiation in photochemical and photobiological processes in the ocean. (C) 2014 Elsevier Inc. All rights reserved. C1 [Cao, Fang; Miller, William L.] Univ Georgia, Dept Marine Sci, Athens, GA 30602 USA. [Fichot, Cedric G.] Univ S Carolina, Marine Sci Program, Columbia, SC 29208 USA. [Hooker, Stanford B.] NASA, Ocean Ecol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Miller, WL (reprint author), Univ Georgia, Dept Marine Sci, Athens, GA 30602 USA. EM bmiller@uga.edu RI Hooker, Stanford/E-2162-2012 FU Office of Naval Research [N00140610219]; NASA [NNX07AD85G]; Georgia Sea Grant [R/SD-5]; NSF [OCE-0752254, OCE-0850677] FX This work was funded by grants from the Office of Naval Research (N00140610219), NASA (NNX07AD85G) and Georgia Sea Grant (R/SD-5) awarded to Dr. W. L. Miller. Validation data from the Gulf of Mexico were collected by C Fichot and S. Lohrenz during the GulfCarbon cruises (2009-2010), funded by the NSF (OCE-0752254), and an NSF award to Drs. R. Benner and W. L. Miller (OCE-0850677). We thank Leanne Powers and Joanna Green, as well as Ike Sellers, Mary Price, and Jason Johnson (UGA Marine Institute) for assistant with sampling aboard the RN Mud Minnow in coastal Georgia. We thank NASA for providing access to SeaWiFS data. SeaWiFS data were used in accordance with the Sea WiFS data access authorization policy. We also thank Dr. Adrian Burd for valuable suggestions on earlier versions of the draft. Finally, we thank three anonymous reviewers for careful reviews of this manuscript. NR 39 TC 3 Z9 3 U1 1 U2 16 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 MAR 25 PY 2014 VL 144 BP 11 EP 27 DI 10.1016/j.rse.2014.01.003 PG 17 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AD8BD UT WOS:000333490600002 ER PT J AU Mladenova, IE Jackson, TJ Njoku, E Bindlish, R Chan, S Cosh, MH Holmes, TRH de Jeu, RAM Jones, L Kimball, J Paloscia, S Santi, E AF Mladenova, I. E. Jackson, T. J. Njoku, E. Bindlish, R. Chan, S. Cosh, M. H. Holmes, T. R. H. de Jeu, R. A. M. Jones, L. Kimball, J. Paloscia, S. Santi, E. TI Remote monitoring of soil moisture using passive microwave-based techniques - Theoretical basis and overview of selected algorithms for AMSR-E SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Soil moisture; Algorithms; Passive microwave; Radiative transfer modeling; Forward/inverse modeling; AMSR-E ID VEGETATION OPTICAL DEPTH; POLARIZATION DIFFERENCE INDEX; LAND-SURFACE MODELS; NEURAL-NETWORKS; BRIGHTNESS TEMPERATURES; SATELLITE-OBSERVATIONS; SCANNING RADIOMETER; DIELECTRIC BEHAVIOR; WET SOIL; RETRIEVAL AB Satellite-based passive microwave remote sensing has been shown to be a valuable tool in mapping and monitoring global soil moisture. The Advanced Microwave Scanning Radiometer on the Aqua platform (AMSR-E) has made significant contributions to this application. As the result of agency and individual initiatives, several approaches for the retrieval of soil moisture from AMSR-E have been proposed and implemented. Although the majority of these are based on the same Radiative Transfer Equation, studies have shown that the resulting soil moisture estimates can differ significantly. A primary goal of this investigation is to understand these differences and develop a suitable approach to potentially improve the algorithm currently used by NASA in producing its operational soil moisture product In order to achieve this goal, the theoretical basis of several alternative soil moisture retrieval algorithms are examined. Analysis has focused on five established approaches: the operational algorithm adopted by NASA, which is referred to as the Normalized Polarization Difference algorithm, the Single Channel Algorithm, the Land Parameter Retrieval Model, the University of Montana soil moisture algorithm, and the HydroAlgo Artificial Neural Network algorithm. Previous comparisons of these algorithms in the literature have typically focused on the retrieved soil moisture products, and employed different metrics and data sets, and have resulted in differing conclusions. In this investigation we attempt to provide a more thorough understanding of the fundamental differences between the algorithms and how these differences affect their performance in terms of range of soil moisture provided. The comparative overview presented in the paper is based on the operating versions of the source codes of the individual algorithms. Analysis has indicated that the differences between algorithms lie in the specific parameterizations and assumptions of each algorithm. The comparative overview of the theoretical basis of the approaches is linked to differences found in the soil moisture retrievals, leading to suggestions for improvements and increased reliability in these algorithms. Published by Elsevier Inc. C1 [Mladenova, I. E.; Jackson, T. J.; Cosh, M. H.; Holmes, T. R. H.] USDA, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. [Njoku, E.; Chan, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bindlish, R.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [de Jeu, R. A. M.] Vrije Univ Amsterdam, Fac Earth & Life Sci, Amsterdam, Netherlands. [Jones, L.; Kimball, J.] Univ Montana, Flathead Lake Biol Stn, Polson, MT 59860 USA. [Jones, L.; Kimball, J.] Univ Montana, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA. [Paloscia, S.; Santi, E.] CNR, Inst Appl Phys, Florence, Italy. RP Mladenova, IE (reprint author), USDA ARS, Hydrol & Remote Sensing Lab, BARC West, B007,10300 Baltimore Ave, Beltsville, MD 20705 USA. EM Iliana.Mladenova@ARS.USDA.GOV RI Cosh, MIchael/A-8858-2015; Holmes, Thomas/F-4512-2010 OI Cosh, MIchael/0000-0003-4776-1918; Holmes, Thomas/0000-0002-4651-0079 NR 77 TC 37 Z9 39 U1 4 U2 52 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 MAR 25 PY 2014 VL 144 BP 197 EP 213 DI 10.1016/j.rse.2014.01.013 PG 17 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AD8BD UT WOS:000333490600016 ER PT J AU Kaufman, JP Miller, NJ Shimon, M Barkats, D Bischoff, C Buder, I Keating, BG Kovac, JM Ade, PAR Aikin, R Battle, JO Bierman, EM Bock, JJ Chiang, HC Dowell, CD Duband, L Filippini, J Hivon, EF Holzapfel, WL Hristov, VV Jones, WC Kernasovskiy, SS Kuo, CL Leitch, EM Mason, PV Matsumura, T Nguyen, HT Ponthieu, N Pryke, C Richter, S Rocha, G Sheehy, C Su, M Takahashi, YD Tolan, JE Yoon, KW AF Kaufman, J. P. Miller, N. J. Shimon, M. Barkats, D. Bischoff, C. Buder, I. Keating, B. G. Kovac, J. M. Ade, P. A. R. Aikin, R. Battle, J. O. Bierman, E. M. Bock, J. J. Chiang, H. C. Dowell, C. D. Duband, L. Filippini, J. Hivon, E. F. Holzapfel, W. L. Hristov, V. V. Jones, W. C. Kernasovskiy, S. S. Kuo, C. L. Leitch, E. M. Mason, P. V. Matsumura, T. Nguyen, H. T. Ponthieu, N. Pryke, C. Richter, S. Rocha, G. Sheehy, C. Su, M. Takahashi, Y. D. Tolan, J. E. Yoon, K. W. TI Self-calibration of BICEP1 three-year data and constraints on astrophysical polarization rotation SO PHYSICAL REVIEW D LA English DT Article ID MICROWAVE BACKGROUND POLARIZATION; ANISOTROPY AB Cosmic microwave background (CMB) polarimeters aspire to measure the faint B-mode signature predicted to arise from inflationary gravitational waves. They also have the potential to constrain cosmic birefringence, rotation of the polarization of the CMB arising from parity-violating physics, which would produce nonzero expectation values for the CMB's temperature to B-mode correlation (TB) and E-mode to B-mode correlation (EB) spectra. However, instrumental systematic effects can also cause these TB and EB correlations to be nonzero. In particular, an overall miscalibration of the polarization orientation of the detectors produces TB and EB spectra which are degenerate with isotropic cosmological birefringence, while also introducing a small but predictable bias on the BB spectrum. We find that BICEP1 three-year spectra, which use our standard calibration of detector polarization angles from a dielectric sheet, are consistent with a polarization rotation of alpha = -2.77 degrees +/- 0.86 degrees (statistical) +/- 1.3 degrees (systematic). We have revised the estimate of systematic error on the polarization rotation angle from the two-year analysis by comparing multiple calibration methods. We also account for the (negligible) impact of measured beam systematic effects. We investigate the polarization rotation for the BICEP1 100 GHz and 150 GHz bands separately to investigate theoretical models that produce frequency-dependent cosmic birefringence. We find no evidence in the data supporting either of these models or Faraday rotation of the CMB polarization by the Milky Way galaxy's magnetic field. If we assume that there is no cosmic birefringence, we can use the TB and EB spectra to calibrate detector polarization orientations, thus reducing bias of the cosmological B-mode spectrum from leaked E-modes due to possible polarization orientation miscalibration. After applying this "self-calibration" process, we find that the upper limit on the tensor-to-scalar ratio decreases slightly, from r < 0.70 to r < 0.65 at 95% confidence. C1 [Kaufman, J. P.; Shimon, M.; Keating, B. G.; Bierman, E. M.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Miller, N. J.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Shimon, M.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Barkats, D.] ESO, Joint ALMA Observ, Santiago 19001, Chile. [Bischoff, C.; Buder, I.; Kovac, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ade, P. A. R.] Univ Wales Coll Cardiff, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. [Aikin, R.; Bock, J. J.; Filippini, J.; Hristov, V. V.; Mason, P. V.; Richter, S.; Rocha, G.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [Battle, J. O.; Bock, J. J.; Dowell, C. D.; Nguyen, H. T.; Rocha, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chiang, H. C.] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Duband, L.] Commissariat Energie Atom, SBT, F-38054 Grenoble, France. [Hivon, E. F.] Inst Astrophys, F-75014 Paris, France. [Holzapfel, W. L.; Takahashi, Y. D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Kernasovskiy, S. S.; Kuo, C. L.; Tolan, J. E.; Yoon, K. W.] Stanford Univ, Palo Alto, CA 94305 USA. [Kernasovskiy, S. S.; Kuo, C. L.; Tolan, J. E.; Yoon, K. W.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Leitch, E. M.; Sheehy, C.] Univ Chicago, Chicago, IL 60637 USA. [Matsumura, T.] KEK, High Energy Accelerator Res Org, Tsukuba, Ibaraki 3050801, Japan. [Ponthieu, N.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Su, M.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Su, M.] MIT, Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA. RP Kaufman, JP (reprint author), Univ Calif San Diego, Dept Phys, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM jkaufman@physics.ucsd.edu RI Holzapfel, William/I-4836-2015; OI Barkats, Denis/0000-0002-8971-1954; Hivon, Eric/0000-0003-1880-2733 FU NSF [OPP-0230438, AST-1255358]; Caltech Presidents Discovery Fund; Caltech Presidents Fund [PF-471]; JPL Research and Technology Development Fund; Harvard College Observatory; Alfred P. Sloan Research Fellowship; NSF PECASE Award [AST-0548262]; NASA Postdoctoral Program at Goddard Space Flight Center; Joan and Irwin Jacobs FX BICEP1 was supported by NSF Grant No. OPP-0230438, Caltech Presidents Discovery Fund, Caltech Presidents Fund PF-471, JPL Research and Technology Development Fund, and the late J. Robinson. This analysis was supported in part by NSF CAREER Award No. AST-1255358 and the Harvard College Observatory, and J. M. K. acknowledges support from an Alfred P. Sloan Research Fellowship. B. G. K acknowledges support from NSF PECASE Award No. AST-0548262. N. J. M.' s research was supported by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. M. S. acknowledges support from a grant from Joan and Irwin Jacobs. We thank the South Pole Station staff for helping make our observing seasons a success. We also thank our colleagues in the ACBAR, BOOMERANG, QUAD, BOLOCAM, SPT, WMAP and Planck experiments, as well as Kim Griest, Amit Yadav, and Casey Conger for advice and helpful discussions, and Kathy Deniston and Irene Coyle for logistical and administrative support. We thank Patrick Shopbell for computational support at Caltech and the FAS Science Division Research Computing Group at Harvard University for providing support to run all the computations for this paper on the Odyssey cluster. NR 38 TC 28 Z9 28 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD MAR 24 PY 2014 VL 89 IS 6 AR 062006 DI 10.1103/PhysRevD.89.062006 PG 11 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AE9EU UT WOS:000334308800004 ER PT J AU Huang, XC Schwenke, DW Lee, TJ AF Huang, Xinchuan Schwenke, David W. Lee, Timothy J. TI Highly accurate potential energy surface, dipole moment surface, rovibrational energy levels, and infrared line list for (SO2)-S-32-O-16 up to 8000 cm(-1) SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID CORRELATED MOLECULAR CALCULATIONS; HIGH-RESOLUTION ANALYSIS; GAUSSIAN-BASIS SETS; EXCITED VIBRATIONAL-STATES; SULFUR-DIOXIDE; ATOMIZATION ENERGY; MICROWAVE SPECTRUM; ROTATIONAL LEVELS; COLOGNE DATABASE; ATOMS ALUMINUM AB A purely ab initio potential energy surface (PES) was refined with selected (SO2)-S-32-O-16 HITRAN data. Compared to HITRAN, the root- mean- squares error ( sRMS) for all J = 0-80 rovibrational energy levels computed on the refined PES (denoted Ames-1) is 0.013 cm(-1). Combined with a CCSD(T)/ aug-cc-pV(Q+d)Z dipole moment surface (DMS), an infrared (IR) line list (denoted Ames- 296K) has been computed at 296 K and covers up to 8000 cm(-1). Compared to the HITRAN and CDMS databases, the intensity agreement for most vibrational bands is better than 85%-90%. Our predictions for (SO2)-S-34-O-16 band origins, higher energy (SO2)-S-32-O-16 band origins and missing (SO2)-S-32-O-16 IR bands have been verified by most recent experiments and available HITRAN data. We conclude that the Ames-1 PES is able to predict (32/34)S(16)O2 band origins below 5500 cm(-1) with 0.01-0.03 cm(-1) uncertainties, and the Ames-296K line list provides continuous, reliable and accurate IR simulations. The Ka- dependence of both line position and line intensity errors is discussed. The line list will greatly facilitate SO2 IR spectral experimental analysis, as well as elimination of SO2 lines in high- resolution astronomical observations. (c) 2014 AIP Publishing LLC. C1 [Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA. [Schwenke, David W.] NASA, NAS Facil, Ames Res Ctr, Moffett Field, CA 94035 USA. [Lee, Timothy J.] NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Huang, XC (reprint author), SETI Inst, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA. EM Xinchuan.Huang-1@nasa.gov; David.W.Schwenke@nasa.gov; Timothy.J.Lee@nasa.gov RI Lee, Timothy/K-2838-2012; schwenke, david/I-3564-2013; HUANG, XINCHUAN/A-3266-2013 FU NASA [08-APRA08-0050, 10-APRA10-0096]; NASA/SETI Institute [NNX09AI49A, NNX12AG96A] FX We gratefully acknowledge funding support from the NASA Grants 08-APRA08-0050 and 10-APRA10-0096. X. H. also thanks the support from the NASA/SETI Institute Cooperative Agreements NNX09AI49A and NNX12AG96A. We sincerely appreciate the kind permission from Dr. Oleg Ulenikov (Tomsk State University) and Dr. Veli-Matti Horneman (University of Oulu) for sharing their published experimental spectra and the latest GS level set derived from their new Effective Hamiltonian Model published in 2013. Dr. Holger Muller (University of Cologne), Dr. Brian Drouin (Jet Propulsion Laboratory), and Professor Jonathan Tennyson (University College London) are thanked for helpful discussions. NR 62 TC 12 Z9 12 U1 0 U2 15 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD MAR 21 PY 2014 VL 140 IS 11 AR 114311 DI 10.1063/1.4868327 PG 17 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA AE7HP UT WOS:000334168400023 PM 24655184 ER PT J AU Jiang, YC Li, L Tian, ZB Ye, H Zhao, LH Yang, RQ Mishima, TD Santos, MB Johnson, MB Mansour, K AF Jiang, Yuchao Li, Lu Tian, Zhaobing Ye, Hao Zhao, Lihua Yang, Rui Q. Mishima, Tetsuya D. Santos, Michael B. Johnson, Matthew B. Mansour, Kamjou TI Electrically widely tunable interband cascade lasers SO JOURNAL OF APPLIED PHYSICS LA English DT Article DE laser tuning; optical design techniques; quantum cascade lasers; red shift; Stark effect ID COUPLED-QUANTUM-WELLS; ROOM-TEMPERATURE; TRANSITIONS; DIODES AB Electrically tunable interband cascade lasers are demonstrated with a wide tuning range of about 280 cm(-1) (34 meV in energy or 630 nm in wavelength) near 4.5 mu m and about 180 cm(-1) (22 meV or 900 nm) near 7 mu m wavelengths. The laser structures are designed such that the heating and Stark effects act together to enhance the red-shift of the lasing wavelength with current injection to achieve wide tunability. The control and manipulation of the tuning range and rate are discussed. C1 [Jiang, Yuchao; Li, Lu; Tian, Zhaobing; Ye, Hao; Zhao, Lihua; Yang, Rui Q.] Univ Oklahoma, Sch Elect & Comp Engn, Norman, OK 73019 USA. [Mishima, Tetsuya D.; Santos, Michael B.; Johnson, Matthew B.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Mansour, Kamjou] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Jiang, YC (reprint author), Univ Oklahoma, Sch Elect & Comp Engn, Norman, OK 73019 USA. RI li, lu/C-6965-2012; Santos, Michael/B-5836-2013 FU National Science Foundation [ECCS-1002202]; C-SPIN, the Oklahoma/Arkansas MRSEC [DMR-0520550]; NASA Planetary Instrument Definition & Developmen Program FX The authors thank J. C. Keay and C. Niu for technical assistance. This work was supported in part by the National Science Foundation (ECCS-1002202), and by C-SPIN, the Oklahoma/Arkansas MRSEC (DMR-0520550). K. Mansour was supported by NASA Planetary Instrument Definition & Developmen Program. NR 25 TC 11 Z9 12 U1 0 U2 12 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-8979 EI 1089-7550 J9 J APPL PHYS JI J. Appl. Phys. PD MAR 21 PY 2014 VL 115 IS 11 AR 113101 DI 10.1063/1.4865941 PG 17 WC Physics, Applied SC Physics GA AE3TM UT WOS:000333900600001 ER PT J AU Anyamba, A Small, JL Britch, SC Tucker, CJ Pak, EW Reynolds, CA Crutchfield, J Linthicum, KJ AF Anyamba, Assaf Small, Jennifer L. Britch, Seth C. Tucker, Compton J. Pak, Edwin W. Reynolds, Curt A. Crutchfield, James Linthicum, Kenneth J. TI Recent Weather Extremes and Impacts on Agricultural Production and Vector-Borne Disease Outbreak Patterns SO PLOS ONE LA English DT Article ID RIFT-VALLEY FEVER; WEST NILE VIRUS; CLIMATE-CHANGE; SOUTHERN-OSCILLATION; CROP YIELDS; EL-NINO; NOAA-AVHRR; VEGETATION; ENCEPHALITIS; TEMPERATURE AB We document significant worldwide weather anomalies that affected agriculture and vector-borne disease outbreaks during the 2010-2012 period. We utilized 2000-2012 vegetation index and land surface temperature data from NASA's satellite-based Moderate Resolution Imaging Spectroradiometer (MODIS) to map the magnitude and extent of these anomalies for diverse regions including the continental United States, Russia, East Africa, Southern Africa, and Australia. We demonstrate that shifts in temperature and/or precipitation have significant impacts on vegetation patterns with attendant consequences for agriculture and public health. Weather extremes resulted in excessive rainfall and flooding as well as severe drought, which caused similar to 10 to 80% variation in major agricultural commodity production (including wheat, corn, cotton, sorghum) and created exceptional conditions for extensive mosquito-borne disease outbreaks of dengue, Rift Valley fever, Murray Valley encephalitis, and West Nile virus disease. Analysis of MODIS data provided a standardized method for quantifying the extreme weather anomalies observed during this period. Assessments of land surface conditions from satellite-based systems such as MODIS can be a valuable tool in national, regional, and global weather impact determinations. C1 [Anyamba, Assaf; Small, Jennifer L.; Tucker, Compton J.; Pak, Edwin W.; Reynolds, Curt A.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Britch, Seth C.; Linthicum, Kenneth J.] USDA ARS, Ctr Med Agr & Vet Entomol, Gainesville, FL USA. [Crutchfield, James] USDA, Int Prod & Assessment Div, Foreign Agr Serv, Washington, DC 20250 USA. [Anyamba, Assaf] Univ Space Res Assoc, Columbia, MD USA. [Small, Jennifer L.; Pak, Edwin W.] Sci Syst & Applicat Inc, Lanham, MD USA. RP Anyamba, A (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. EM assaf.anyamba@nasa.gov FU USDA Foreign Agricultural Service; DoD Armed Forces Health Surveillance Center's Global Emerging Infections Surveillance and Response System (AFHSC/GEIS) under the Human Febrile and Vector -Borne Illnesses (FVBI) Program; USDA Agricultural Research Service FX This work was made possible by funding from USDA Foreign Agricultural Service towards the Global Agricultural Monitoring project, DoD Armed Forces Health Surveillance Center's Global Emerging Infections Surveillance and Response System (AFHSC/GEIS) under the Human Febrile and Vector -Borne Illnesses (FVBI) Program and USDA Agricultural Research Service. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 58 TC 14 Z9 15 U1 7 U2 86 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAR 21 PY 2014 VL 9 IS 3 AR e92538 DI 10.1371/journal.pone.0092538 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AD6GL UT WOS:000333355300095 PM 24658301 ER PT J AU Soria, R Long, KS Blair, WP Godfrey, L Kuntz, KD Lenc, E Stockdale, C Winkler, PF AF Soria, R. Long, K. S. Blair, W. P. Godfrey, L. Kuntz, K. D. Lenc, E. Stockdale, C. Winkler, P. F. TI Super-Eddington Mechanical Power of an Accreting Black Hole in M83 SO SCIENCE LA English DT Article ID X-RAY SOURCES; HIGH-RESOLUTION RADIO; GALAXY NGC 7793; FE-II EMISSION; INTERSTELLAR-MEDIUM; MICROQUASAR S26; REMNANTS; SS-433; LOBES; JETS AB Mass accretion onto black holes releases energy in the form of radiation and outflows. Although the radiative flux cannot substantially exceed the Eddington limit, at which the outgoing radiation pressure impedes the inflow of matter, it remains unclear whether the kinetic energy flux is bounded by this same limit. Here, we present the detection of a radio-optical structure, powered by outflows from a non-nuclear black hole. Its accretion disk properties indicate that this black hole is less than 100 solar masses. The optical-infrared line emission implies an average kinetic power of 3 x 10(40) erg second(-1), higher than the Eddington luminosity of the black hole. These results demonstrate kinetic power exceeding the Eddington limit over a sustained period, which implies greater ability to influence the evolution of the black hole's environment. C1 [Soria, R.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Long, K. S.; Blair, W. P.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Blair, W. P.; Kuntz, K. D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Godfrey, L.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Kuntz, K. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lenc, E.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia. [Lenc, E.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia. [Stockdale, C.] Marquette Univ, Dept Phys, Milwaukee, WI 53201 USA. [Winkler, P. F.] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. RP Soria, R (reprint author), Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia. EM roberto.soria@icrar.org OI Lenc, Emil/0000-0002-9994-1593 FU Australian Research Council [DP 120102393]; Space Telescope Science Institute [GO-12513-01]; NASA Wisconsin Space Grant Consortium; NSF [AST-0908566]; NASA by the Chandra X-ray Observatory Center [G01-12115]; NASA [NAS8-03060]; [CE110001020] FX We thank M. W. Pakull for his insightful lessons and comments on ULX bubbles, J. Miller-Jones and A. Moin for their help with the ATCA observations and data analysis, and P. P. Plucinsky for his helpful role in the Chandra study of M83. R. S. acknowledges an Australian Research Council's Discovery Projects funding scheme (project number DP 120102393). W. P. B. acknowledges Space Telescope Science Institute grant GO-12513-01 to Johns Hopkins University. C. S. acknowledges the NASA Wisconsin Space Grant Consortium research grant. P. F. W. acknowledges financial support from the NSF through grant AST-0908566. This work was supported by NASA through Chandra grant G01-12115, issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. The Centre for All-sky Astrophysics (CAASTRO) is an Australian Research Council Centre of Excellence, funded by grant CE110001020. NR 53 TC 13 Z9 13 U1 1 U2 10 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD MAR 21 PY 2014 VL 343 IS 6177 BP 1330 EP 1333 DI 10.1126/science.1248759 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AD3AI UT WOS:000333108500030 PM 24578533 ER PT J AU Whelan, JT Prix, R Cutler, CJ Willis, JL AF Whelan, John T. Prix, Reinhard Cutler, Curt J. Willis, Joshua L. TI New coordinates for the amplitude parameter space of continuous gravitational waves SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article DE gravitational waves; signal processing; Bayesian inference; neutron stars AB The parameter space for continuous gravitational waves (GWs) can be divided into amplitude parameters (signal amplitude, inclination and polarization angles describing the orientation of the source, and an initial phase) and phase-evolution parameters (signal frequency and frequency derivatives, and parameters such as sky position which determine the Doppler modulation of the signal). The division is useful in part because of the existence of a set of functions known as the Jaranowski-Krolak-Schutz (JKS) coordinates, which are a set of four coordinates on the amplitude parameter space such that the GW signal can be written as a linear combination of four template waveforms (which depend on the phase-evolution parameters) with the JKS coordinates as coefficients. We define a new set of coordinates on the amplitude parameter space, with the same properties, which can be more closely connected to the physical amplitude parameters. These naturally divide into two pairs of Cartesian-like coordinates on two-dimensional subspaces, one corresponding to left-and the other to right-circular polarization. We thus refer to these as circular polarization factored (CPF) coordinates. The corresponding two sets of polar coordinates (known as CPF-polar) can be related in a simple way to the physical parameters. A further coordinate transformation can be made, within each subspace, between CPF and so-called root-radius coordinates, whose radial coordinate is the fourth root of the radial coordinate in CPFpolar coordinates. We illustrate some simplifying applications for these various coordinate systems, such as a calculation of the Jacobian for the transformation between JKS or CPF coordinates and the physical amplitude parameters (amplitude, inclination, polarization and initial phase); a demonstration that the Jacobian between root-radius coordinates and the physical parameters is a constant; an illustration of the signal coordinate singularities associated with left-and right-circular polarization, which correspond to the origins of the two two-dimensional subspaces; and an elucidation of the form of the log-likelihood ratio between hypotheses of Gaussian noise with and without a continuous GW signal. These are used to illustrate some of the prospects for approximate evaluation of a Bayesian detection statistic defined by marginalization over the physical parameter space. Additionally, in the presence of simplifying assumptions about the observing geometry, we are able, using CPF-polar coordinates, to explicitly evaluate the integral for the Bayesian detection statistic, and compare it to the approximate results. C1 [Whelan, John T.] Rochester Inst Technol, Ctr Computat Relat & Gravitat, Rochester, NY 14623 USA. [Whelan, John T.] Rochester Inst Technol, Sch Math Sci, Rochester, NY 14623 USA. [Prix, Reinhard; Willis, Joshua L.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. [Cutler, Curt J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Willis, Joshua L.] Abilene Christian Univ, Dept Engn & Phys, Abilene, TX 79699 USA. RP Whelan, JT (reprint author), Rochester Inst Technol, Ctr Computat Relat & Gravitat, 85 Lomb Mem Dr, Rochester, NY 14623 USA. EM john.whelan@astro.rit.edu; reinhard.prix@aei.mpg.de; Curt.J.Cutler@jpl.nasa.gov; josh.willis@acu.edu OI Whelan, John/0000-0001-5710-6576; Prix, Reinhard/0000-0002-3789-6424 FU NSF [HY-0855494, PHY-1207010, PHY-106881]; Max Planck Society; Jet Propulsion Laboratory, California Institute of Technology FX The authors would like to thank Bruce Allen, Sanjeev Dhurandhar, Josh Faber, Steve Fairhurst and Andy Lundgren for helpful discussions and feedback. JTW was supported by NSF grants PHY-0855494 and PHY-1207010. RP and JLW were supported by the Max Planck Society. CJC's work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract to the National Aeronautics and Space Administration; he gratefully acknowledges support from NSF Grant PHY-106881. This paper has been assigned LIGO document number LIGO-P1300105-v5, and AEI-preprint number AEI-2013-250. NR 7 TC 4 Z9 4 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD MAR 21 PY 2014 VL 31 IS 6 AR 065002 DI 10.1088/0264-9381/31/6/065002 PG 27 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AC0TF UT WOS:000332207100004 ER PT J AU Akeson, RL Jensen, ELN AF Akeson, R. L. Jensen, E. L. N. TI CIRCUMSTELLAR DISKS AROUND BINARY STARS IN TAURUS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; protoplanetary disks; stars: formation ID STATISTICAL-METHODS; ASTRONOMICAL DATA; YOUNG BINARIES; UPPER LIMITS; UZ-TAURI; 5 MYR; MASS; EVOLUTION; ACCRETION; SYSTEMS AB We have conducted a survey of 17 wide (> 100 AU) young binary systems in Taurus with the Atacama Large Millimeter Array (ALMA) at two wavelengths. The observations were designed to measure the masses of circumstellar disks in these systems as an aid to understanding the role of multiplicity in star and planet formation. The ALMA observations had sufficient resolution to localize emission within the binary system. Disk emission was detected around all primaries and 10 secondaries, with disk masses as low as 10(-4)M(circle dot). We compare the properties of our sample to the population of known disks in Taurus and find that the disks from this binary sample match the scaling between stellar mass and millimeter flux of F-mm proportional to M-*(1.5-2.0) to within the scatter found in previous studies. We also compare the properties of the primaries to those of the secondaries and find that the secondary/primary stellar and disk mass ratios are not correlated; in three systems, the circumsecondary disk is more massive than the circumprimary disk, counter to some theoretical predictions. C1 [Akeson, R. L.] NASA, CALTECH, IPAC, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Jensen, E. L. N.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. RP Akeson, RL (reprint author), NASA, CALTECH, IPAC, Exoplanet Sci Inst, Pasadena, CA 91125 USA. OI Jensen, Eric/0000-0002-4625-7333 NR 35 TC 16 Z9 16 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 MAR 20 PY 2014 VL 784 IS 1 AR 62 DI 10.1088/0004-637X/784/1/62 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000062 ER PT J AU Burgess, JM Preece, RD Connaughton, V Briggs, MS Goldstein, A Bhat, PN Greiner, J Gruber, D Kienlin, A Kouveliotou, C McGlynn, S Meegan, CA Paciesas, WS Rau, A Xiong, S Axelsson, M Baring, MG Dermer, CD Iyyani, S Kocevski, D Omodei, N Ryde, F Vianello, G AF Burgess, J. M. Preece, R. D. Connaughton, V. Briggs, M. S. Goldstein, A. Bhat, P. N. Greiner, J. Gruber, D. Kienlin, A. Kouveliotou, C. McGlynn, S. Meegan, C. A. Paciesas, W. S. Rau, A. Xiong, S. Axelsson, M. Baring, M. G. Dermer, C. D. Iyyani, S. Kocevski, D. Omodei, N. Ryde, F. Vianello, G. TI TIME-RESOLVED ANALYSIS OF FERMI GAMMA-RAY BURSTS WITH FAST- AND SLOW-COOLED SYNCHROTRON PHOTON MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; gamma-ray burst: general; gamma rays: stars; methods: data analysis; radiation mechanisms: non-thermal; radiation mechanisms: thermal ID INTERNAL SHOCK MODEL; HIGH-ENERGY EMISSION; PARTICLE-ACCELERATION; PROMPT EMISSION; RELATIVISTIC SHOCKS; LUMINOSITY RELATION; SPECTRAL COMPONENT; OBLIQUE SHOCKS; CONSTRAINTS; PHOTOSPHERE AB Time-resolved spectroscopy is performed on eight bright, long gamma-ray bursts (GRBs) dominated by single emission pulses that were observed with the Fermi Gamma-Ray Space Telescope. Fitting the prompt radiation of GRBs by empirical spectral forms such as the Band function leads to ambiguous conclusions about the physical model for the prompt radiation. Moreover, the Band function is often inadequate to fit the data. The GRB spectrum is therefore modeled with two emission components consisting of optically thin non-thermal synchrotron radiation from relativistic electrons and, when significant, thermal emission from a jet photosphere, which is represented by a blackbody spectrum. To produce an acceptable fit, the addition of a blackbody component is required in five out of the eight cases. We also find that the low-energy spectral index a is consistent with a synchrotron component with a = -0.81 +/- 0.1. This value lies between the limiting values of a = -2/3 and a = -3/2 for electrons in the slow-and fast-cooling regimes, respectively, suggesting ongoing acceleration at the emission site. The blackbody component can be more significant when using a physical synchrotron model instead of the Band function, illustrating that the Band function does not serve as a good proxy for a non-thermal synchrotron emission component. The temperature and characteristic emission-region size of the blackbody component are found to, respectively, decrease and increase as power laws with time during the prompt phase. In addition, we find that the blackbody and non-thermal components have separate temporal behaviors as far as their respective flux and spectral evolutions. C1 [Burgess, J. M.; Preece, R. D.; Connaughton, V.; Briggs, M. S.; Goldstein, A.; Bhat, P. N.; Paciesas, W. S.; Xiong, S.] Univ Alabama, Huntsville, AL 35899 USA. [Greiner, J.; Gruber, D.; Kienlin, A.; Rau, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Kouveliotou, C.] NASA, Space Sci Off, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [McGlynn, S.] Tech Univ Munich, Exzellence Cluster Universe, D-85748 Garching, Germany. [Meegan, C. A.] Univ Space Res Assoc, Huntsville, AL 35899 USA. [Axelsson, M.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Axelsson, M.; Iyyani, S.; Ryde, F.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Axelsson, M.; Ryde, F.] AlbaNova, Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. [Dermer, C. D.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Kocevski, D.; Omodei, N.; Vianello, G.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Kocevski, D.; Omodei, N.; Vianello, G.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Vianello, G.] Consorzio Interuniv Fis Spaziale, I-10133 Turin, Italy. RP Burgess, JM (reprint author), Univ Alabama, 320 Sparkman Dr, Huntsville, AL 35899 USA. EM james.m.burgess@nasa.gov; Rob.Preece@nasa.gov; baring@rice.edu; shabuiyyani@gmail.com RI Iyyani, Shabnam/D-8736-2017; OI Iyyani, Shabnam/0000-0002-2525-3464; Burgess, James/0000-0003-3345-9515; Axelsson, Magnus/0000-0003-4378-8785 FU Office of Naval Research FX We would like to thank Frederic Daigne and Bing Zhang for helpful discussions concerning the nature of the non-thermal emission, and the referee for a constructive report. We would also like to thank Paz Beniamini and Tsvi Piran for extremely helpful comments clarifying the limitations of this model, now addressed in the Appendix. The work of C.D.D. is supported by the Office of Naval Research. NR 79 TC 26 Z9 26 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2014 VL 784 IS 1 AR 17 DI 10.1088/0004-637X/784/1/17 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000017 ER PT J AU Huang, JS Rigopoulou, D Magdis, G Rowan-Robinson, M Dai, Y Bock, JJ Burgarella, D Chapman, S Clements, DL Cooray, A Farrah, D Glenn, J Oliver, S Smith, AJ Wang, L Page, M Riechers, D Roseboom, I Symeonidis, M Fazio, GG Yun, M Webb, TMA Efstathiou, A AF Huang, J. -S. Rigopoulou, D. Magdis, G. Rowan-Robinson, M. Dai, Y. Bock, J. J. Burgarella, D. Chapman, S. Clements, D. L. Cooray, A. Farrah, D. Glenn, J. Oliver, S. Smith, A. J. Wang, L. Page, M. Riechers, D. Roseboom, I. Symeonidis, M. Fazio, G. G. Yun, M. Webb, T. M. A. Efstathiou, A. TI HerMES: SPECTRAL ENERGY DISTRIBUTIONS OF SUBMILLIMETER GALAXIES AT z > 4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: evolution; galaxies: formation; infrared: galaxies ID ULTRALUMINOUS INFRARED GALAXIES; SIMILAR-TO 2; HIGH-REDSHIFT GALAXIES; STAR-FORMING GALAXIES; MOLECULAR GAS; MIDINFRARED SPECTROSCOPY; STARBURST GALAXY; PHOTOMETRIC REDSHIFTS; LUMINOUS STARBURSTS; SPACE-TELESCOPE AB We present a study of the infrared properties for a sample of seven spectroscopically confirmed submillimeter galaxies (SMGs) at z > 4.0. By combining ground-based near-infrared, Spitzer IRAC and MIPS, Herschel SPIRE, and ground-based submillimeter/millimeter photometry, we construct their spectral energy distributions (SEDs) and a composite model to fit the SEDs. The model includes a stellar emission component at lambda(rest) < 3.5 mu m ot dust component peaking at lambda(rest) similar to 5 mu m and cold dust component which becomes significant for lambda(rest) > 50 mu m. Six objects in the sample are detected at 250 and 350 mu m. The dust temperatures for the sources in this sample are in the range of 40-80 K, and their LFIR similar to 10(13) L circle dot qualifies them as hyper-luminous infrared galaxies. The mean FIR-radio index for this sample is around q = 2.2 indicating no radio excess in their radio emission. Most sources in the sample have 24 mu m detections corresponding to a rest-frame 4.5 mu m luminosity of Log(10)(L-4.5/L circle dot) = 11 similar to 11.5. Their L4.5/L-FIR ratios are very similar to those of starburst-dominated SMGs at z similar to 2. The LCO -LFIR relation for this sample is consistent with that determined for local ULIRGs and SMGs at z similar to 2. We conclude that SMGs at z > 4 are hotter and more luminous in the FIR but otherwise very similar to those at z similar to 2. None of these sources show any sign of the strong QSO phase being triggered. C1 [Huang, J. -S.] Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China. [Huang, J. -S.] Chinese Acad Sci, China Chile Joint Ctr Astron, Santiago 1515, Chile. [Huang, J. -S.; Dai, Y.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rigopoulou, D.; Magdis, G.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Rigopoulou, D.] Rutherford Appleton Lab, RAL Space Sci & Technol Facil Council, Didcot OX11 0QX, Oxon, England. [Rowan-Robinson, M.; Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Dai, Y.] Boston Coll, Newton, MA USA. [Bock, J. J.] CALTECH, Pasadena, CA 91125 USA. [Burgarella, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Burgarella, D.] Univ Aix marseille, CNRS, OAMP, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Chapman, S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Oliver, S.; Smith, A. J.; Wang, L.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Page, M.; Symeonidis, M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Riechers, D.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Riechers, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Roseboom, I.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Yun, M.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Webb, T. M. A.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Efstathiou, A.] European Univ Cyprus, Sch Sci, CY-1516 Nicosia, Cyprus. RP Huang, JS (reprint author), Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China. RI Magdis, Georgios/C-7295-2014 OI Magdis, Georgios/0000-0002-4872-2294 FU NASA FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCLMSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). Facilities: Herschel (SPIRE), Spitzer (IRAC, MIPS) NR 80 TC 13 Z9 13 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 MAR 20 PY 2014 VL 784 IS 1 AR 52 DI 10.1088/0004-637X/784/1/52 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000052 ER PT J AU Hulsebus, A Marengo, M Carson, J Stapelfeldt, K AF Hulsebus, A. Marengo, M. Carson, J. Stapelfeldt, K. TI A MID-INFRARED SEARCH FOR SUBSTELLAR COMPANIONS OF NEARBY PLANET-HOST STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; infrared: stars; methods: data analysis; planetary systems; stars: low-mass ID SPITZER-SPACE-TELESCOPE; EXTRA-SOLAR PLANETS; INFRARED ARRAY CAMERA; T-DWARF COMPANIONS; 47 URSAE MAJORIS; BROWN DWARFS; MASS PLANET; UPSILON ANDROMEDAE; EPSILON-ERIDANI; IMAGING SURVEY AB Determining the presence of widely separated substellar-mass companion is crucial to understand the dynamics of inner planets in extrasolar planetary systems ( e. g., to explain their high mean eccentricity as inner planets are perturbed by the Kozai mechanism). We report the results of our Spitzer/Infrared Array Camera (IRAC) imaging search for widely separated (10 ''-25 '') substellar-mass companions for 14 planet-host stars within 15 pc of the Sun. Using deep 3.6 and 4.5 mu m observations in subarray mode, we found one object in the field of 47 UMa with [3.6]-[4.5] color similar to a T5 dwarf, which is, however, unlikely to share common proper motion with 47 UMa. We also found three objects with brown-dwarf-like [3.6]-[4.5] color limits in the fields of GJ 86, HD 160691, and GJ 581, as well as another in the field of HD 69830 for which we have excluded common proper motion. We provide model-based upper mass limits for unseen objects around all stars in our sample, with typical sensitivity to 10 M-J objects from a projected separation of 50-300 AU from the parent star. We also discuss our data analysis methods for point-spread-function subtraction, image co-alignment, and artifact subtraction of IRAC subarray images. C1 [Hulsebus, A.; Marengo, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50010 USA. [Carson, J.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA. [Stapelfeldt, K.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. RP Hulsebus, A (reprint author), Iowa State Univ, Dept Phys & Astron, 12 Phys Hall, Ames, IA 50010 USA. FU NASA; U.S. National Science Foundation [1009203]; South Carolina Space Grant Consortium; Research Corporation for Science Advancement [21026] FX Thanks to Brett Kail for helping to brainstorm ideas on image co-alignment. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. A.H., M.M., and J.C. were partially supported by the U.S. National Science Foundation under award No. 1009203. J.C. received support from the South Carolina Space Grant Consortium and the Research Corporation for Science Advancement (award No. 21026). NR 86 TC 0 Z9 0 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 MAR 20 PY 2014 VL 784 IS 1 AR 41 DI 10.1088/0004-637X/784/1/41 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000041 ER PT J AU Konstantopoulos, IS Appleton, PN Guillard, P Trancho, G Cluver, ME Bastian, N Charlton, JC Fedotov, K Gallagher, SC Smith, LJ Struck, CJ AF Konstantopoulos, I. S. Appleton, P. N. Guillard, P. Trancho, G. Cluver, M. E. Bastian, N. Charlton, J. C. Fedotov, K. Gallagher, S. C. Smith, L. J. Struck, C. J. TI SHOCKS AND STAR FORMATION IN STEPHAN'S QUINTET. I. GEMINI SPECTROSCOPY OF H alpha-BRIGHT KNOTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: groups: individual (HCG 92); galaxies: individual ( NGC 7317, NGC 7318A, NGC 7318B, NGC 7319); galaxies: interactions; galaxies: star formation; intergalactic medium; shock waves ID HICKSON COMPACT-GROUPS; MOLECULAR GAS; VELOCITY DISPERSION; DRIVEN TURBULENCE; INTRAGROUP MEDIUM; GALAXY PAIRS; EMISSION; STARBURST; MULTIWAVELENGTH; CLOUDS AB We present a Gemini-GMOS spectroscopic study of Hubble Space Telescope (HST)-selected H alpha-emitting regions in Stephan's Quintet (HCG 92), a nearby compact galaxy group, with the aim of disentangling the processes of shock-induced heating and star formation in its intra-group medium. The approximate to 40 sources are distributed across the system, but most densely concentrated in the similar to kiloparsec-long shock region. Their spectra neatly divide them into narrow-and broad-line emitters, and we decompose the latter into three or more emission peaks corresponding to spatial elements discernible in HST imaging. The emission-line ratios of the two populations of Ha-emitters confirm their nature as H II regions (90% of the sample) or molecular gas heated by a shock front propagating at less than or similar to 300 km s(-1). Their redshift distribution reveals interesting three-dimensional structure with respect to gas-phase baryons, with no H II regions associated with shocked gas, no shocked regions in the intruder galaxy NGC 7318B, and a sharp boundary between shocks and star formation. We conclude that star formation is inhibited substantially, if not entirely, in the shock region. Attributing those Hii regions projected against the shock to the intruder, we find a lopsided distribution of star formation in this galaxy, reminiscent of pileup regions in models of interacting galaxies. The H alpha luminosities imply mass outputs, star formation rates, and efficiencies similar to nearby star-forming regions. Two large knots are an exception to this, being comparable in stellar output to the prolific 30 Doradus region. We also examine Stephan's Quintet in the context of compact galaxy group evolution, as a paradigm for intermittent star formation histories in the presence of a rich, X-ray-emitting intra-group medium. All spectra are provided as supplemental materials. C1 [Konstantopoulos, I. S.; Cluver, M. E.] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Appleton, P. N.] CALTECH, NASA, Herschel Sci Ctr NHSC, Pasadena, CA 91125 USA. [Guillard, P.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Trancho, G.] Giant Magellan Telescope Org, Pasadena, CA 91101 USA. [Bastian, N.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Charlton, J. C.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Fedotov, K.; Gallagher, S. C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Fedotov, K.] Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Smith, L. J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Smith, L. J.] European Space Agcy, Baltimore, MD 21218 USA. [Struck, C. J.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. RP Konstantopoulos, IS (reprint author), Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia. EM iraklis@aao.gov.au OI Konstantopoulos, Iraklis/0000-0003-2177-0146 FU Jet Propulsion Laboratory [1439092]; Canadian Natural Science and Engineering Research Council; Ontario Early Researcher Award Program FX I.S.K. acknowledges support from grant no. 1439092 from the Jet Propulsion Laboratory. I.S.K. is also grateful for the hospitality of the staff at the NASA Herschel Science Center, the Giant Magellan Telescope Organisation, and Carnegie Observatories, all in Pasadena, CA, where much of this work was undertaken.; S.C.G. and K.F. thank the Canadian Natural Science and Engineering Research Council and the Ontario Early Researcher Award Program for support. NR 61 TC 6 Z9 6 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2014 VL 784 IS 1 AR 1 DI 10.1088/0004-637X/784/1/1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000001 ER PT J AU Lissauer, JJ Marcy, GW Bryson, ST Rowe, JF Jontof-Hutter, D Agol, E Borucki, WJ Carter, JA Ford, EB Gilliland, RL Kolbl, R Star, KM Steffen, JH Torres, G AF Lissauer, Jack J. Marcy, Geoffrey W. Bryson, Stephen T. Rowe, Jason F. Jontof-Hutter, Daniel Agol, Eric Borucki, William J. Carter, Joshua A. Ford, Eric B. Gilliland, Ronald L. Kolbl, Rea Star, Kimberly M. Steffen, Jason H. Torres, Guillermo TI VALIDATION OF KEPLER'S MULTIPLE PLANET CANDIDATES. II. REFINED STATISTICAL FRAMEWORK AND DESCRIPTIONS OF SYSTEMS OF SPECIAL INTEREST SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: statistical; planetary systems; stars: individual (Kepler-90=KOI-351, Kepler-102=KOI-82, Kepler-122=KOI-232, Kepler-132=KOI-284, Kepler-223=KOI-730, Kepler-238=KOI-834, Kepler-292=KOI-1364, Kepler-296=KOI-1422) ID LOW-MASS; TRANSITING PLANET; FALSE POSITIVES; STARS; RADII; CONFIRMATION; EVOLUTION; DWARFS; MODELS; PAIRS AB We extend the statistical analysis performed by Lissauer et al. in 2012, which demonstrates that the overwhelming majority of Kepler candidate multiple transiting systems (multis) represents true transiting planets, and we develop therefrom a procedure to validate large numbers of planet candidates in multis as bona fide exoplanets. We show that this statistical framework correctly estimates the abundance of false positives already identified around Kepler targets with multiple sets of transit-like signatures based on their abundance around targets with single sets of transit-like signatures. We estimate the number of multis that represent split systems of one or more planets orbiting each component of a binary star system. We use the high reliability rate for multis to validate more than one dozen particularly interesting multi-planet systems herein. Hundreds of additional multi-planet systems are validated in a companion paper by Rowe et al. We note that few very short period (P < 1.6 days) planets orbit within multiple transiting planet systems and discuss possible reasons for their absence. There also appears to be a shortage of planets with periods exceeding a few months in multis. C1 [Lissauer, Jack J.; Bryson, Stephen T.; Rowe, Jason F.; Jontof-Hutter, Daniel; Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Marcy, Geoffrey W.; Kolbl, Rea] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Carter, Joshua A.; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ford, Eric B.; Gilliland, Ronald L.; Star, Kimberly M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Ford, Eric B.; Gilliland, Ronald L.; Star, Kimberly M.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Steffen, Jason H.] Northwestern Univ, Dept Phys & Astron, CIERA, Evanston, IL 60208 USA. RP Lissauer, JJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Jack.Lissauer@nasa.gov OI /0000-0002-0802-9145; /0000-0001-6545-639X FU NASA's Science Mission Directorate FX Kepler was competitively selected as the tenth Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. We dedicate this paper to the memory of Kepler Deputy Principal Investigator David G. Koch (1945 August 6-2012 September 12), whose work over more than two decades was key to making the Kepler mission a success. We acknowledge Ruth Murray-Clay for stimulating and valuable conversations about FP modes. Tony Dobrovolskis, Mike Haas, Billy Quarles, Leslie Rogers, and Alexandre Santerne provided constructive comments on the manuscript. Elisabeth Adams assisted with the preparation of Figure 12. NR 51 TC 77 Z9 77 U1 1 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2014 VL 784 IS 1 AR 44 DI 10.1088/0004-637X/784/1/44 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000044 ER PT J AU Lupu, RE Zahnle, K Marley, MS Schaefer, L Fegley, B Morley, C Cahoy, K Freedman, R Fortney, JJ AF Lupu, R. E. Zahnle, Kevin Marley, Mark S. Schaefer, Laura Fegley, Bruce Morley, Caroline Cahoy, Kerri Freedman, Richard Fortney, Jonathan J. TI THE ATMOSPHERES OF EARTHLIKE PLANETS AFTER GIANT IMPACT EVENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; planetary systems; planets and satellites: general; radiative transfer; stars: low-mass ID MOLECULAR SPECTROSCOPIC DATABASE; DIRECT NUMERICAL DIAGONALIZATION; COOL STELLAR ATMOSPHERES; TERRESTRIAL MAGMA OCEAN; CONTINENTAL-CRUST; SYNTHETIC SPECTRA; BROWN DWARFS; MU-M; MULTIPLE-SCATTERING; MODEL ATMOSPHERES AB It is now understood that the accretion of terrestrial planets naturally involves giant collisions, the moon-forming impact being a well-known example. In the aftermath of such collisions, the surface of the surviving planet is very hot and potentially detectable. Here we explore the atmospheric chemistry, photochemistry, and spectral signatures of post-giant-impact terrestrial planets enveloped by thick atmospheres consisting predominantly of CO2 and H2O. The atmospheric chemistry and structure are computed self-consistently for atmospheres in equilibrium with hot surfaces with composition reflecting either the bulk silicate Earth (which includes the crust, mantle, atmosphere, and oceans) or Earth's continental crust. We account for all major molecular and atomic opacity sources including collision-induced absorption. We find that these atmospheres are dominated by H2O and CO2, while the formation of CH4 and NH3 is quenched because of short dynamical timescales. Other important constituents are HF, HCl, NaCl, and SO2. These are apparent in the emerging spectra and can be indicative that an impact has occurred. The use of comprehensive opacities results in spectra that are a factor of two lower brightness temperature in the spectral windows than predicted by previous models. The estimated luminosities show that the hottest post-giant-impact planets will be detectable with near-infrared coronagraphs on the planned 30m class telescopes. The 1-4 mu m will be most favorable for such detections, offering bright features and better contrast between the planet and a potential debris disk. We derive cooling timescales on the order of 10(5-6) yr on the basis of the modeled effective temperatures. This leads to the possibility of discovering tens of such planets in future surveys. C1 [Lupu, R. E.; Freedman, Richard] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Zahnle, Kevin; Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Schaefer, Laura] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fegley, Bruce] Washington Univ, Dept Earth & Planetary Sci, Planetary Chem Lab, St Louis, MO 63130 USA. [Fegley, Bruce] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. [Morley, Caroline; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Cahoy, Kerri] MIT, Cambridge, MA 02139 USA. RP Lupu, RE (reprint author), NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. EM Roxana.E.Lupu@nasa.gov RI Marley, Mark/I-4704-2013; Lupu, Roxana/P-9060-2014; OI Lupu, Roxana/0000-0003-3444-5908; Fortney, Jonathan/0000-0002-9843-4354; Marley, Mark/0000-0002-5251-2943; Schaefer, Laura/0000-0003-2915-5025 FU NASA; NSF Astronomy Program; NASA EPSCOR Program; NASA Cooperative Agreement [NNX09AG69A]; NASA Ames Research Center FX This work was supported by the NASA Origins program. B. F. was supported by the NSF Astronomy Program, the NASA EPSCOR Program, and by NASA Cooperative Agreement NNX09AG69A with the NASA Ames Research Center. NR 124 TC 18 Z9 18 U1 1 U2 24 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 MAR 20 PY 2014 VL 784 IS 1 AR 27 DI 10.1088/0004-637X/784/1/27 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000027 ER PT J AU MacDonald, RKD Bailyn, CD Buxton, M Cantrell, AG Chatterjee, R Kennedy-Shaffer, R Orosz, JA Markwardt, CB Swank, JH AF MacDonald, Rachel K. D. Bailyn, Charles D. Buxton, Michelle Cantrell, Andrew G. Chatterjee, Ritaban Kennedy-Shaffer, Ross Orosz, Jerome A. Markwardt, Craig B. Swank, Jean H. TI BLACK HOLE BINARY V4641 SAGITARII: ACTIVITY IN QUIESCENCE AND IMPROVED MASS DETERMINATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; stars: individual (V4641 Sgr); X-rays: binaries ID MODEL ATMOSPHERES; ULTRAVIOLET EXTINCTION; SAX J1819.3-2525; STANDARD STARS; NEUTRON-STAR; OUTBURST; SAGITTARII; A0620-00; GIANTS; EVENT AB We examine similar to 10 yr of photometric data and find that the black hole X-ray binary V4641 Sgr has two optical states, passive and active, during X-ray quiescence. The passive state is dominated by ellipsoidal variations and is stable in the shape and variability of the light curve. The active state is brighter and more variable. Emission during the active state varies over the course of the orbital period and is redder than the companion star. These optical/infrared states last for weeks or months. V4641 Sgr spends approximately 85% of X-ray quiescence in the passive state and 15% in the active. We analyze passive colors and spectroscopy of V4641 Sgr and show that they are consistent with a reddened B9III star (with E(B-V) = 0.37 +/- 0.19) with little or no contribution from the accretion disk. We use X-ray observations with an updated ephemeris to place an upper limit on the duration of an X-ray eclipse of <8 degrees.3 in phase (similar to 1.6 hr). High-resolution spectroscopy yields a greatly improved measurement of the rotational velocity of the companion star of V-rot sin i = 100.9 +/- 0.8 km s(-1). We fit ellipsoidal models to the passive state data and find an inclination angle of i = 72.3 +/- 4 degrees.1, a mass ratio of Q = 2.2 +/- 0.2, and component masses for the system of M-BH = 6.4 +/- 0.6 M circle dot and M-2 = 2.9 +/- 0.4M circle dot(.) Using these values we calculate an updated distance to V4641 Sgr of 6.2 +/- 0.7 kpc. C1 [MacDonald, Rachel K. D.; Bailyn, Charles D.; Buxton, Michelle; Cantrell, Andrew G.; Chatterjee, Ritaban; Kennedy-Shaffer, Ross] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Markwardt, Craig B.; Swank, Jean H.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP MacDonald, RKD (reprint author), Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA. EM rachel.macdonald@yale.edu RI MacDonald, Rachel/C-7412-2014 OI MacDonald, Rachel/0000-0002-2569-741X FU NSF [AST-0707627, 0407063, 070707]; National Aeronautics and Space Administration; National Science Foundation FX We thank the anonymous referee for many useful comments which improved the quality of this paper. R.K.D.M. and C.D.B. received support from NSF grant AST-0707627. This paper has made use of up-to-date SMARTS optical/near-infrared light curves that are available at www.astro.yale.edu/smarts/xrb/home.php. The Yale SMARTS XRB team is supported by NSF grants 0407063 and 070707 to Charles Bailyn. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the USNOFS Image and Catalogue Archive operated by the United States Naval Observatory, Flagstaff Station (http://www.nofs.navy.mil/data/fchpix/). This research has made use of data obtained through the High Energy Astrophysics Science Archive Research Center Online Service, provided by the NASA/Goddard Space Flight Center. NR 40 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2014 VL 784 IS 1 AR 2 DI 10.1088/0004-637X/784/1/2 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000002 ER PT J AU Rappaport, S Barclay, T DeVore, J Rowe, J Sanchis-Ojeda, R Still, M AF Rappaport, Saul Barclay, Thomas DeVore, John Rowe, Jason Sanchis-Ojeda, Roberto Still, Martin TI KOI-2700b-A PLANET CANDIDATE WITH DUSTY EFFLUENTS ON A 22 hr ORBIT SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: detection; planets and satellites: individual (KOI-2700b) ID EARTH-SIZED PLANET; SUPER-EARTHS; HOT JUPITERS; KEPLER DATA; MASS-LOSS; STAR; EVOLUTION; DYNAMICS; EVAPORATION; SIMULATION AB Kepler planet candidate KOI-2700b (KIC 8639908b), with an orbital period of 21.84 hr, exhibits a distinctly asymmetric transit profile, likely indicative of the emission of dusty effluents, and reminiscent of KIC 1255b. The host star has T-eff = 4435 K, M similar or equal to 0.63M circle dot , and R similar or equal to 0.57R circle dot, comparable to the parameters ascribed to KIC 12557548. The transit egress can be followed for similar to 25% of the orbital period and, if interpreted as extinction from a dusty comet-like tail, indicates a long lifetime for the dust grains of more than a day. We present a semiphysical model for the dust tail attenuation and fit for the physical parameters contained in that expression. The transit is not sufficiently deep to allow for a study of the transit-to-transit variations, as is the case for KIC 1255b; however, it is clear that the transit depth is slowly monotonically decreasing by a factor of similar to 2 over the duration of the Kepler mission. We infer a mass-loss rate in dust from the planet of similar to 2 lunar masses per Gyr. The existence of a second star hosting a planet with a dusty comet-like tail would help to show that such objects may be more common and less exotic than originally thought. According to current models, only quite small planets with Mp less than or similar to 0.03M circle plus are likely to release a detectable quantity of dust. Thus, any "normal-looking" transit that is inferred to arise from. a rocky planet of radius greater than similar to 1/2R circle plus should not exhibit any hint of a dusty tail. Conversely, if one detects an asymmetric transit due to a dusty tail, then it will be very difficult to detect the hard body of the planet within the transit because, by necessity, the planet must be quite small (i.e.,less than or similar to 0.3R circle plus). C1 [Rappaport, Saul; Sanchis-Ojeda, Roberto] MIT, Dept Phys, Cambridge, MA 02139 USA. [Rappaport, Saul; Sanchis-Ojeda, Roberto] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Barclay, Thomas; Still, Martin] NASA, Ames Res Ctr, BAER Inst, Mountain View, CA 94035 USA. [DeVore, John] Visidyne Inc, Burlington, MA 01803 USA. [Rowe, Jason] SETI Inst, Mountain View, CA 94043 USA. [Rowe, Jason] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. RP Rappaport, S (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. EM sar@mit.edu; thomas.barclay@nasa.gov; devore@visidyne.com; jasonfrowe@gmail.com; rsanchis86@gmail.com; martin.d.still@nasa.gov FU NASA support through the Kepler Participating Scientist Program; NASA Science Mission directorate; NASA Office of Space Science [NNX13AC07G] FX We thank Eugene Chiang and Josh Winn for helpful discussions. R.S.O. acknowledges NASA support through the Kepler Participating Scientist Program. This research has made use of data collected by the Kepler mission, which is funded by the NASA Science Mission directorate. Some of the analysis made use of PyKE (Still & Barclay 2012), a software package for the reduction and analysis of Kepler data. This open source software project is developed and distributed by the NASA Kepler Guest Observer Office. The J-band image of the KOI-2700 field was obtained with the United Kingdom Infrared Telescope (UKIRT) which is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the U. K. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS-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. NR 55 TC 34 Z9 34 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2014 VL 784 IS 1 AR 40 DI 10.1088/0004-637X/784/1/40 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000040 ER PT J AU Rowe, JF Bryson, ST Marcy, GW Lissauer, JJ Jontof-Hutter, D Mullally, F Gilliland, RL Issacson, H Ford, E Howell, SB Borucki, WJ Haas, M Huber, D Steffen, JH Thompson, SE Quintana, E Barclay, T Still, M Fortney, J Gautier, TN Hunter, R Caldwell, DA Ciardi, DR Devore, E Cochran, W Jenkins, J Agol, E Carter, JA Geary, J AF Rowe, Jason F. Bryson, Stephen T. Marcy, Geoffrey W. Lissauer, Jack J. Jontof-Hutter, Daniel Mullally, Fergal Gilliland, Ronald L. Issacson, Howard Ford, Eric Howell, Steve B. Borucki, William J. Haas, Michael Huber, Daniel Steffen, Jason H. Thompson, Susan E. Quintana, Elisa Barclay, Thomas Still, Martin Fortney, Jonathan Gautier, T. N., III Hunter, Roger Caldwell, Douglas A. Ciardi, David R. Devore, Edna Cochran, William Jenkins, Jon Agol, Eric Carter, Joshua A. Geary, John TI VALIDATION OF KEPLER'S MULTIPLE PLANET CANDIDATES. III. LIGHT CURVE ANALYSIS AND ANNOUNCEMENT OF HUNDREDS OF NEW MULTI-PLANET SYSTEMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: fundamental parameters ID TRANSIT TIMING OBSERVATIONS; MAIN-SEQUENCE STARS; 1ST 4 MONTHS; HABITABLE ZONES; INPUT CATALOG; EARTH; PARAMETERS; OBJECTS; RADII; SIZE AB The Kepler mission has discovered more than 2500 exoplanet candidates in the first two years of spacecraft data, with approximately 40% of those in candidate multi-planet systems. The high rate of multiplicity combined with the low rate of identified false positives indicates that the multiplanet systems contain very few false positive signals due to other systems not gravitationally bound to the target star. False positives in the multi-planet systems are identified and removed, leaving behind a residual population of candidate multi-planet transiting systems expected to have a false positive rate less than 1%. We present a sample of 340 planetary systems that contain 851 planets that are validated to substantially better than the 99% confidence level; the vast majority of these have not been previously verified as planets. We expect similar to two unidentified false positives making our sample of planet very reliable. We present fundamental planetary properties of our sample based on a comprehensive analysis of Kepler light curves, ground-based spectroscopy, and high-resolution imaging. Since we do not require spectroscopy or high-resolution imaging for validation, some of our derived parameters for a planetary system may be systematically incorrect due to dilution from light due to additional stars in the photometric aperture. Nonetheless, our result nearly doubles the number verified exoplanets. C1 [Rowe, Jason F.; Bryson, Stephen T.; Lissauer, Jack J.; Jontof-Hutter, Daniel; Mullally, Fergal; Howell, Steve B.; Borucki, William J.; Haas, Michael; Huber, Daniel; Thompson, Susan E.; Quintana, Elisa; Barclay, Thomas; Still, Martin; Hunter, Roger; Caldwell, Douglas A.; Jenkins, Jon] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rowe, Jason F.; Mullally, Fergal; Thompson, Susan E.; Quintana, Elisa; Caldwell, Douglas A.; Devore, Edna; Jenkins, Jon] SETI Inst, Mountain View, CA 94043 USA. [Marcy, Geoffrey W.; Issacson, Howard] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Gilliland, Ronald L.; Huber, Daniel] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Ford, Eric] Penn State Univ, State Coll, PA 16801 USA. [Steffen, Jason H.] Northwestern Univ, Dept Phys & Astron, CIERA, Evanston, IL 60208 USA. [Barclay, Thomas; Still, Martin] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Fortney, Jonathan] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Gautier, T. N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Cochran, William] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Cochran, William] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Carter, Joshua A.; Geary, John] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rowe, JF (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Jason.Rowe@nasa.gov RI Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Fortney, Jonathan/0000-0002-9843-4354; /0000-0002-0802-9145; Ciardi, David/0000-0002-5741-3047; /0000-0001-6545-639X FU NASA's Science Mission Directorate; Kepler Participating Scientist grant [NNX12AD21G] FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. We are indebted to the entire Kepler team for all the hard work and dedication that has made such discoveries possible. J.F.R. is partially supported by a Kepler Participating Scientist grant (NNX12AD21G). NR 57 TC 147 Z9 147 U1 12 U2 43 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 MAR 20 PY 2014 VL 784 IS 1 AR 45 DI 10.1088/0004-637X/784/1/45 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000045 ER PT J AU Smit, R Bouwens, RJ Labbe, I Zheng, W Bradley, L Donahue, M Lemze, D Moustakas, J Umetsu, K Zitrin, A Coe, D Postman, M Gonzalez, V Bartelmann, M Benitez, N Broadhurst, T Ford, H Grillo, C Infante, L Jimenez-Teja, Y Jouvel, S Kelson, DD Lahav, O Maoz, D Medezinski, E Melchior, P Meneghetti, M Merten, J Molino, A Moustakas, LA Nonino, M Rosati, P Seitz, S AF Smit, R. Bouwens, R. J. Labbe, I. Zheng, W. Bradley, L. Donahue, M. Lemze, D. Moustakas, J. Umetsu, K. Zitrin, A. Coe, D. Postman, M. Gonzalez, V. Bartelmann, M. Benitez, N. Broadhurst, T. Ford, H. Grillo, C. Infante, L. Jimenez-Teja, Y. Jouvel, S. Kelson, D. D. Lahav, O. Maoz, D. Medezinski, E. Melchior, P. Meneghetti, M. Merten, J. Molino, A. Moustakas, L. A. Nonino, M. Rosati, P. Seitz, S. TI EVIDENCE FOR UBIQUITOUS HIGH-EQUIVALENT-WIDTH NEBULAR EMISSION IN z similar to 7 GALAXIES: TOWARD A CLEAN MEASUREMENT OF THE SPECIFIC STAR-FORMATION RATE USING A SAMPLE OF BRIGHT, MAGNIFIED GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift ID LYMAN-BREAK GALAXIES; HIGH-REDSHIFT GALAXIES; STELLAR MASS DENSITY; ULTRA DEEP FIELD; ULTRAVIOLET LUMINOSITY DENSITY; SPECTRAL ENERGY-DISTRIBUTIONS; EARLY RELEASE SCIENCE; FORMING GALAXIES; FORMATION HISTORY; LENSING ANALYSIS AB Growing observational evidence indicates that nebular line emission has a significant impact on the rest-frame optical fluxes of z similar to 5-7 galaxies. This line emission makes z similar to 5-7 galaxies appear more massive, with lower specific star-formation rates (sSFRs). However, corrections for this line emission have been difficult to perform reliably because of huge uncertainties on the strength of such emission at z greater than or similar to 5.5. In this paper, we present the most direct observational evidence thus far for ubiquitous high-equivalent-width (EW) [O (III)]+ H beta line emission in Lyman-break galaxies at z similar to 7, and we present a strategy for an improved measurement of the sSFR at z similar to 7. We accomplish this through the selection of bright galaxies in the narrow redshift window z similar to 6.6-7.0 where the Spitzer/Infrared Array Camera (IRAC) 4.5 mu m flux provides a clean measurement of the stellar continuum light, in contrast with the 3.6 mu m flux, which is contaminated by the prominent [O III]+ H beta lines. To ensure a high signal-to-noise ratio for our IRAC flux measurements, we consider only the brightest (H-160 < 26 mag) magnified galaxies we have identified behind galaxy clusters. It is remarkable that the mean rest-frame optical color for our bright seven-source sample is very blue, [3.6]-[4.5] = - 0.9 +/- 0.3. Such blue colors cannot be explained by the stellar continuum light and require that the rest-frame EW of [O III]+ H beta is greater than 637 angstrom for the average source. The four bluest sources from our seven-source sample require an even more extreme EW of 1582 angstrom. We can also set a robust lower limit of greater than or similar to 4Gyr(-1) on the sSFR of our sample based on the mean spectral energy distribution. C1 [Smit, R.; Bouwens, R. J.; Labbe, I.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Zheng, W.; Lemze, D.; Ford, H.; Medezinski, E.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Bradley, L.; Coe, D.; Postman, M.] Space Telescope Sci Inst, Baltimore, MD 21208 USA. [Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Moustakas, J.] Siena Coll, Loudonville, NY 12211 USA. [Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Zitrin, A.; Bartelmann, M.] ZAH, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Zitrin, A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Gonzalez, V.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Benitez, N.; Jimenez-Teja, Y.; Molino, A.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Broadhurst, T.] Univ Basque Country, Dept Theoret Phys, Bilbao 48080, Spain. [Grillo, C.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Infante, L.] Pontificia Univ Catolica Chile, Dept Astronoia & Astrofis, Santiago 22, Chile. [Jouvel, S.] Inst Cincies Espai IEEC CSIC, Bellaterra, Barcelona, Spain. [Kelson, D. D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Lahav, O.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Maoz, D.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Melchior, P.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Melchior, P.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Meneghetti, M.] INAF, Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Meneghetti, M.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy. [Merten, J.; Moustakas, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nonino, M.] INAF, Osservatorio Astron Trieste, I-40131 Trieste, Italy. [Rosati, P.] ESO European Southern Observ, D-85748 Garching, Germany. [Seitz, S.] Univ Sternwarte, D-81679 Munich, Germany. RP Smit, R (reprint author), Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RI Jimenez-Teja, Yolanda/D-5933-2011; Grillo, Claudio/E-6223-2015; Gonzalez, Valentino/I-5279-2016; Gonzalez, Valentino/F-7021-2015; OI Benitez, Narciso/0000-0002-0403-7455; Meneghetti, Massimo/0000-0003-1225-7084; Grillo, Claudio/0000-0002-5926-7143; Gonzalez, Valentino/0000-0002-3120-0510; Nonino, Mario/0000-0001-6342-9662; Umetsu, Keiichi/0000-0002-7196-4822; Moustakas, Leonidas/0000-0003-3030-2360 FU ERC [227749]; NASA through Hubble Fellowship [HST-HF-51334.01-A] FX We thank Jeff Cooke, Rob Crain, Eichii Egami, Andrea Ferrara, Marijn Franx, Max Pettini, Norbert Pirzkal, and Vivienne Wild for interesting conversations. Eichii Egami independently discovered the same extreme [3.6]-[4.5] colors in at least one of the sources from the present sample. We thank Pascal Oesch for useful feedback on our manuscript. We acknowledge support from ERC grant HIGHZ No. 227749, an NWO Vrij Competitie grant, and the NASA grant for the CLASH MCT program. Support for A.Z. is provided by NASA through Hubble Fellowship grant no. HST-HF-51334.01-A awarded by STScI, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Part of this work was also supported by contract research "Internationale Spitzenforschung II/2-6" of the Baden W "urttemberg Stiftung. The work of L. A. M. was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 61 TC 55 Z9 55 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2014 VL 784 IS 1 AR 58 DI 10.1088/0004-637X/784/1/58 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000058 ER PT J AU Strohmayer, T Mahmoodifar, S AF Strohmayer, Tod Mahmoodifar, Simin TI A NON-RADIAL OSCILLATION MODE IN AN ACCRETING MILLISECOND PULSAR? SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; stars: neutron; stars: oscillations; stars: rotation; X-rays: binaries; X-rays: individual (XTE J1751 305, XTE J1814, 338, NGC 6440 X-2) ID X-RAY OSCILLATIONS; ROTATING RELATIVISTIC STARS; CLUSTER NGC 6440; NEUTRON-STARS; R-MODES; BURST OSCILLATIONS; XTE J1814-338; ISENTROPIC STARS; 2004 HYPERFLARE; LIGHT CURVES AB We present results of targeted searches for signatures of non-radial oscillation modes (such as r-and g-modes) in neutron stars using RXTE data from several accreting millisecond X-ray pulsars (AMXPs). We search for potentially coherent signals in the neutron star rest frame by first removing the phase delays associated with the star's binary motion and computing fast Fourier transform power spectra of continuous light curves with up to 230 time bins. We search a range of frequencies in which both r-and g-modes are theoretically expected to reside. Using data from the discovery outburst of the 435 Hz pulsar XTE J1751-305 we find a single candidate, coherent oscillation with a frequency of 0.5727597 nu(spin) = 249.332609 Hz, and a fractional Fourier amplitude of 7.46x10(-4). We estimate the significance of this feature at the 1.6 x 10(-3) level, slightly better than a 3 sigma detection. Based on the observed frequency we argue that possible mode identifications include rotationally modified g-modes associated with either a helium-rich surface layer or a density discontinuity due to electron captures on hydrogen in the accreted ocean. In the latter case the presence of sufficient hydrogen in this ultracompact system with a likely helium-rich donor would present an interesting puzzle. Alternatively, the frequency could be identified with that of an inertial mode or a core r-mode modified by the presence of a solid crust; however, the r-mode amplitude required to account for the observed modulation amplitude would induce a large spin-down rate inconsistent with the observed pulse timing measurements. For the AMXPs XTE J1814-338 and NGC 6440 X-2 we do not find any candidate oscillation signals, and we place upper limits on the fractional Fourier amplitude of any coherent oscillations in our frequency search range of 7.8x10(-4) and 5.6x10(-3), respectively. We briefly discuss the prospects and sensitivity for similar searches with future, larger X-ray collecting area missions. C1 [Strohmayer, Tod] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Strohmayer, Tod] NASA, Goddard Space Flight Ctr, Joint Space Sci Inst, Greenbelt, MD 20771 USA. [Mahmoodifar, Simin] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Mahmoodifar, Simin] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. RP Strohmayer, T (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. FU U.S. Department of Energy [DEFG02- 93ER-40762] FX We thank Tony Piro, Andrew Cumming, Jean in 't Zand, Cole Miller, and Diego Altamirano for many helpful comments and discussions. We thank the anonymous referee for valuable comments that helped us improve this paper. T.S. acknowledges NASA's support for high energy astrophysics. S.M. acknowledges the support of the U.S. Department of Energy through grant No. DEFG02- 93ER-40762. NR 60 TC 11 Z9 11 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 MAR 20 PY 2014 VL 784 IS 1 AR 72 DI 10.1088/0004-637X/784/1/72 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000072 ER PT J AU Zhang, S Hailey, CJ Baganoff, FK Bauer, FE Boggs, SE Craig, WW Christensen, FE Gotthelf, EV Harrison, FA Mori, K Nynka, M Stern, D Tomsick, JA Zhang, WW AF Zhang, Shuo Hailey, Charles J. Baganoff, Frederick K. Bauer, Franz E. Boggs, Steven E. Craig, William W. Christensen, Finn E. Gotthelf, Eric V. Harrison, Fiona A. Mori, Kaya Nynka, Melania Stern, Daniel Tomsick, John A. Zhang, William W. TI HIGH-ENERGY X-RAY DETECTION OF G359.89-0.08 (SGR A-E): MAGNETIC FLUX TUBE EMISSION POWERED BY COSMIC RAYS? SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; X-rays: individual (Sgr A-E, G359.89-0.08, XMM J17450-2904); X-rays: ISM ID GALACTIC-CENTER REGION; PULSAR WIND NEBULAE; NONTHERMAL EMISSION; SUPERNOVA-REMNANTS; MOLECULAR CLOUDS; RADIO FILAMENTS; GAMMA-RAYS; DISCOVERY; FIELD; ASTERISK AB We report the first detection of high-energy X-ray (E > 10 keV) emission from the Galactic center non-thermal filament G359.89-0.08 (Sgr A-E) using data acquired with the Nuclear Spectroscopic Telescope Array (NuSTAR). The bright filament was detected up to similar to 50 keV during a NuSTAR Galactic center monitoring campaign. The featureless power-law spectrum with a photon index G approximate to 2.3 confirms a non-thermal emission mechanism. The observed flux in the 3-79 keV band is F-X = (2.0 +/- 0.1) x 10(-12) erg cm(-2) s(-1), corresponding to an unabsorbed X-ray luminosity L-X = (2.6 +/- 0.8) x 10(34) erg s(-1) assuming a distance of 8.0 kpc. Based on theoretical predictions and observations, we conclude that Sgr A-E is unlikely to be a pulsar wind nebula (PWN) or supernova remnant-molecular cloud (SNR-MC) interaction, as previously hypothesized. Instead, the emission could be due to a magnetic flux tube which traps TeV electrons. We propose two possible TeV electron sources: old PWNe (up to similar to 100 kyr) with low surface brightness and radii up to similar to 30 pc or MCs illuminated by cosmic rays (CRs) from CR accelerators such as SNRs or Sgr A*. C1 [Zhang, Shuo; Hailey, Charles J.; Gotthelf, Eric V.; Mori, Kaya; Nynka, Melania] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Baganoff, Frederick K.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bauer, Franz E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, Franz E.] Space Sci Inst, Boulder, CO 80301 USA. [Boggs, Steven E.; Craig, William W.; Tomsick, John A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Christensen, Finn E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Zhang, S (reprint author), Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA. EM shuo@astro.columbia.edu RI Boggs, Steven/E-4170-2015 OI Boggs, Steven/0000-0001-9567-4224 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; NASA Headquarters under the NASA Earth and Space Science Fellowship Program-Grant [NNX13AM31] 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). S. Z. is partially supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program-Grant "NNX13AM31." The authors wish to thank Mark Morris for allowing them to view the recently acquired JVLA 6 cm continuum radio map of Sgr A-E. NR 35 TC 5 Z9 5 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2014 VL 784 IS 1 AR 6 DI 10.1088/0004-637X/784/1/6 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000006 ER PT J AU Koch, GJ Beyon, JY Cowen, LJ Kavaya, MJ Grant, MS AF Koch, Grady J. Beyon, Jeffrey Y. Cowen, Larry J. Kavaya, Michael J. Grant, Michael S. TI Three-dimensional wind profiling of offshore wind energy areas with airborne Doppler lidar SO JOURNAL OF APPLIED REMOTE SENSING LA English DT Article DE wind energy; Doppler lidar; airborne remote sensing; wind measurement; lasers AB A technique has been developed for imaging the wind field over offshore areas being considered for wind farming. This is accomplished with an eye-safe 2-mu m wavelength coherent Doppler lidar installed in an aircraft. By raster scanning the aircraft over the wind energy area (WEA), a three-dimensional map of the wind vector can be made. This technique was evaluated in 11 flights over the Virginia and Maryland offshore WEAs. Heights above the ocean surface planned for wind turbines are shown to be within the marine boundary layer, and the wind vector is seen to show variation across the geographical area of interest at turbine heights. c The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI. C1 [Koch, Grady J.; Beyon, Jeffrey Y.; Cowen, Larry J.; Kavaya, Michael J.; Grant, Michael S.] NASA Langley Res Ctr, Hampton, VA 23681 USA. RP Koch, GJ (reprint author), NASA Langley Res Ctr, Hampton, VA 23681 USA. EM grady.j.koch@nasa.gov FU NASA Earth Science Technology Office under the Laser Risk Reduction Program and Instrument Incubator Program; NASA Langley Research Center; George Hagerman of the Virginia Coastal Energy Research Consortium; Lynn Sparling of the University of Maryland Baltimore County FX DAWN instrument development was made possible by funding from the NASA Earth Science Technology Office under the Laser Risk Reduction Program and Instrument Incubator Program. Further development for flight implementation was provided by the NASA Airborne Instrument Technology Transition program. Flight campaigns aboard the UC-12B were funded by NASA Langley Research Center. A wide range of expertise to build the lidar was provided by Jirong Yu, Mulugeta Petros, Bo Trieu, Paul Petzar, Upendra Singh, Ed Modlin, Evan Horowitz, Mark Jones, Garfield Creary, and Farzin Amzajerdian of NASA Langley Research Center. Complex flight operations were provided at NASA Langley Research Center by pilots Gregory Slover, Leslie Kagey, and Richard Yasky; flight engineers Michael Wusk and Lucille Crittenden; and crew chiefs Andrew Haynes and Dean Riddick. Measurement needs of offshore WEAs were identified by collaboration with George Hagerman of the Virginia Coastal Energy Research Consortium and Lynn Sparling of the University of Maryland Baltimore County. NR 16 TC 3 Z9 4 U1 2 U2 14 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1931-3195 J9 J APPL REMOTE SENS JI J. Appl. Remote Sens. PD MAR 20 PY 2014 VL 8 AR 083662 DI 10.1117/1.JRS.8.083662 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AD9CV UT WOS:000333563200001 ER PT J AU Goobar, A Johansson, J Amanullah, R Cao, Y Perley, DA Kasliwal, MM Ferretti, R Nugent, PE Harris, C Gal-Yam, A Ofek, EO Tendulkar, SP Dennefeld, M Valenti, S Arcavi, I Banerjee, DPK Venkataraman, V Joshi, V Ashok, NM Cenko, SB Diaz, RF Fremling, C Horesh, A Howell, DA Kulkarni, SR Papadogiannakis, S Petrushevska, T Sand, D Sollerman, J Stanishev, V Bloom, JS Surace, J Dupuy, TJ Liu, MC AF Goobar, A. Johansson, J. Amanullah, R. Cao, Y. Perley, D. A. Kasliwal, M. M. Ferretti, R. Nugent, P. E. Harris, C. Gal-Yam, A. Ofek, E. O. Tendulkar, S. P. Dennefeld, M. Valenti, S. Arcavi, I. Banerjee, D. P. K. Venkataraman, V. Joshi, V. Ashok, N. M. Cenko, S. B. Diaz, R. F. Fremling, C. Horesh, A. Howell, D. A. Kulkarni, S. R. Papadogiannakis, S. Petrushevska, T. Sand, D. Sollerman, J. Stanishev, V. Bloom, J. S. Surace, J. Dupuy, T. J. Liu, M. C. TI THE RISE OF SN 2014J IN THE NEARBY GALAXY M82 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE dust, extinction; galaxies: individual (Messier 82); supernovae: individual (SN 2014J) ID HIGH-VELOCITY FEATURES; IA SUPERNOVA SPECTRA; OPTICAL PHOTOMETRY; CIRCUMSTELLAR GAS; TIME-SERIES; 2011FE; RADIO; SPECTROSCOPY; ENVIRONMENT; ULTRAVIOLET AB We report on the discovery of SN 2014J in the nearby galaxy M82. Given its proximity, it offers the best opportunity to date to study a thermonuclear supernova (SN) over a wide range of the electromagnetic spectrum. Optical, near-IR, and mid-IR observations on the rising light curve, orchestrated by the intermediate Palomar Transient Factory, show that SN 2014J is a spectroscopically normal Type Ia supernova (SN Ia), albeit exhibiting high-velocity features in its spectrum and heavily reddened by dust in the host galaxy. Our earliest detections start just hours after the fitted time of explosion. We use high-resolution optical spectroscopy to analyze the dense intervening material and do not detect any evolution in the resolved absorption features during the light curve rise. Similar to other highly reddened SNe Ia, a low value of total-to-selective extinction, R-V less than or similar to 2, provides the best match to our observations. We also study pre-explosion optical and near-IR images from Hubble Space Telescope with special emphasis on the sources nearest to the SN location. C1 [Goobar, A.; Johansson, J.; Amanullah, R.; Ferretti, R.; Papadogiannakis, S.; Petrushevska, T.] Stockholm Univ, Oskar Klein Ctr, Dept Phys, Albanova Univ Ctr, SE-10691 Stockholm, Sweden. [Cao, Y.; Perley, D. A.; Tendulkar, S. P.; Kulkarni, S. R.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Kasliwal, M. M.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Nugent, P. E.; Harris, C.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Computat Res Div, Berkeley, CA 94720 USA. [Nugent, P. E.; Harris, C.; Bloom, J. S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Gal-Yam, A.; Ofek, E. O.; Horesh, A.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Dennefeld, M.] IAP, CNRS, F-75014 Paris, France. [Dennefeld, M.] Univ Paris 06, F-75014 Paris, France. [Valenti, S.; Arcavi, I.; Howell, D. A.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Valenti, S.; Howell, D. A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Arcavi, I.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Banerjee, D. P. K.; Venkataraman, V.; Joshi, V.; Ashok, N. M.] Phys Res Lab, Ahmadabad 380009, Gujarat, India. [Cenko, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Cenko, S. B.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Diaz, R. F.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland. [Fremling, C.; Sollerman, J.] Stockholm Univ, Oskar Klein Ctr, Dept Astron, Albanova Univ Ctr, SE-10691 Stockholm, Sweden. [Sand, D.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Stanishev, V.] IST, CENTRA Ctr Multidisciplinar Astrofis, P-1049001 Lisbon, Portugal. [Surace, J.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Dupuy, T. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, M. C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Goobar, A (reprint author), Stockholm Univ, Oskar Klein Ctr, Dept Phys, Albanova Univ Ctr, SE-10691 Stockholm, Sweden. EM ariel@fysik.su.se RI Horesh, Assaf/O-9873-2016; Stanishev, Vallery/M-8930-2013; OI Horesh, Assaf/0000-0002-5936-1156; Ferretti, Raphael/0000-0001-7814-5814; Stanishev, Vallery/0000-0002-7626-1181; Sollerman, Jesper/0000-0003-1546-6615; Diaz, Rodrigo/0000-0001-9289-5160 FU Swedish Research Council; Swedish Space Board; Hubble Fellowship; Carnegie-Princeton Fellowship; National Energy Research Scientific Computing Center; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; ERC grant FX We thank S. Fossey for making the discovery R-band image of SN 2014J available to us. We are grateful to S. Fossey and M. Phillips for helpful comments on the manuscript. We acknowledge A. McKay, A. Bradley, N. Scoville, P.L. Capak, C. M. Carollo, S. Lilly, H. Sheth, V. Bhalerao, P. Donati, S. Geier, F. Saturni, G. Nowak, and A. Finoguenov for cooperating with ToO observations. A.G. and R.A. acknowledge support from the Swedish Research Council and the Swedish Space Board and A. G.-Y. an ERC grant. M.M.K. acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship. Based on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias, Faulkes Telescope North image observed by Gain Lee, the Mount Abu 1.2 m Infrared telescope, India, and the 1.93 m telescope of Haute-Provence Observatory, CNRS, France. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. NR 42 TC 60 Z9 60 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 20 PY 2014 VL 784 IS 1 AR L12 DI 10.1088/2041-8205/784/1/L12 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC8ME UT WOS:000332786300012 ER PT J AU King, AL Walton, DJ Miller, JM Barret, D Boggs, SE Christensen, FE Craig, WW Fabian, AC Furst, F Hailey, CJ Harrison, FA Krivonos, R Mori, K Natalucci, L Stern, D Tomsick, JA Zhang, WW AF King, Ashley L. Walton, Dominic J. Miller, Jon M. Barret, Didier Boggs, Steven E. Christensen, Finn E. Craig, William W. Fabian, Andy C. Fuerst, Felix Hailey, Charles J. Harrison, Fiona A. Krivonos, Roman Mori, Kaya Natalucci, Lorenzo Stern, Daniel Tomsick, John A. Zhang, William W. TI THE DISK WIND IN THE RAPIDLY SPINNING STELLAR-MASS BLACK HOLE 4U 1630-472 OBSERVED WITH NuSTAR SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; black hole physics; stars: winds, outflows; X-rays: binaries ID X-RAY REFLECTION; ACCRETION DISKS; EMISSION-LINES; GRO J1655-40; JET POWER; CANDIDATE 4U-1630-47; 1998 OUTBURST; 1H 0707-495; ABSORPTION; SUZAKU AB We present an analysis of a short NuSTAR observation of the stellar-mass black hole and low-mass X-ray binary 4U 1630-472. Reflection from the inner accretion disk is clearly detected for the first time in this source, owing to the sensitivity of NuSTAR. With fits to the reflection spectrum, we find evidence for a rapidly spinning black hole, alpha(*) = 0.985(-0.014)(+0.005) (1 sigma statistical errors). However, archival data show that the source has relatively low radio luminosity. Recently claimed relationships between jet power and black hole spin would predict either a lower spin or a higher peak radio luminosity. We also report the clear detection of an absorption feature at 7.03 +/- 0.03 keV, likely signaling a disk wind. If this line arises in dense, moderately ionized gas (log xi = 3.6(-0.3)(+0.2)) and is dominated by He-like Fe XXV, the wind has a velocity of v/c = 0.043(-0.007)(+0.002) (12900(-2100)(+600) km s(-1)). If the line is instead associated with a more highly ionized gas (log xi = 6.1(-0.6)(+0.7)), and is dominated by Fe XXVI, evidence of a blueshift is only marginal, after taking systematic errors into account. Our analysis suggests the ionized wind may be launched within 200-1100 Rg, and may be magnetically driven. C1 [King, Ashley L.; Miller, Jon M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Walton, Dominic J.; Fuerst, Felix; Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Barret, Didier] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Barret, Didier] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France. [Boggs, Steven E.; Craig, William W.; Krivonos, Roman; Tomsick, John A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Fabian, Andy C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Hailey, Charles J.; Mori, Kaya] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Natalucci, Lorenzo] INAF IAPS, Ist Nazl Astrofis, I-00133 Rome, Italy. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP King, AL (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM ashking@umich.edu RI Boggs, Steven/E-4170-2015 OI Boggs, Steven/0000-0001-9567-4224 FU NASA [NNG08FD60C]; NASA; ASI/INAF [I/037/12/0-011/13]; Italian Space Agency (ASI) FX We would like to thank Julia Lee for her invaluable comments. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. L.N. wishes to acknowledge the Italian Space Agency (ASI) for financial support by ASI/INAF grant I/037/12/0-011/13. NR 47 TC 20 Z9 20 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 20 PY 2014 VL 784 IS 1 AR L2 DI 10.1088/2041-8205/784/1/L2 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC8ME UT WOS:000332786300002 ER PT J AU Kirk, BS Stogner, RH Bauman, PT Oliver, TA AF Kirk, Benjamin S. Stogner, Roy H. Bauman, Paul T. Oliver, Todd A. TI Modeling hypersonic entry with the fully-implicit Navier-Stokes (FIN-s) stabilized finite element flow solver SO COMPUTERS & FLUIDS LA English DT Article DE Stabilized finite elements; Compressible flow; Hypersonic flow; Reentry; Surface ablation ID COMPUTATIONAL FLUID-DYNAMICS; EARTH ENTRY; ABLATION; RADIATION; FORMULATION; RELAXATION; FLOWFIELD; EQUATIONS AB In this paper, we present a novel scheme for modeling the hypersonic atmospheric entry of large vehicles with an ablative thermal protection system. The Favre-averaged thermochemical nonequilibrium Navier Stokes equations with Spalart Allmaras turbulence closure, thermodynamic, chemical kinetic, and quasi-steady ablation model are presented. The numerical method is based on a streamline upwind Petrov Galerkin (SUPG) stabilized finite element formulation. The formulation and implementation of the finite element approximation are discussed in detail. The performance of the scheme is investigated through a series of increasingly complex applications, culminating in the simulation of a three-dimensional ablating heatshield in transitioning flow. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Kirk, Benjamin S.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Stogner, Roy H.; Bauman, Paul T.; Oliver, Todd A.] Univ Texas Austin, Inst Computat Engn & Sci, Austin, TX 78712 USA. RP Kirk, BS (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM benjamin.kirk@nasa.gov; roystgnr@ices.utexas.edu; pbauman@ices.utexas.edu; oliver@ices.utexas.edu RI Bauman, Paul/G-1374-2014 OI Bauman, Paul/0000-0003-3513-8264 FU Department of Energy [National Nuclear Security Administration] [DE-FC52-08NA286151] FX The authors express their sincere gratitude for the many enjoyable collaborations with the late Graham Carey related to this work. The authors also acknowledge Steve Bova of Sandia National Labs for many fruitful discussions. This material is based upon work supported by the Department of Energy [National Nuclear Security Administration] under Award Number [DE-FC52-08NA286151; this support is gratefully acknowledged. NR 45 TC 2 Z9 2 U1 1 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0045-7930 EI 1879-0747 J9 COMPUT FLUIDS JI Comput. Fluids PD MAR 20 PY 2014 VL 92 BP 281 EP 292 DI 10.1016/j.compfluid.2013.10.003 PG 12 WC Computer Science, Interdisciplinary Applications; Mechanics SC Computer Science; Mechanics GA AC1OA UT WOS:000332264700025 ER PT J AU Behrangi, A Wong, S Mallick, K Fisher, JB AF Behrangi, Ali Wong, Sun Mallick, Kaniska Fisher, Joshua B. TI On the net surface water exchange rate estimated from remote-sensing observation and reanalysis SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID ATMOSPHERIC INFRARED SOUNDER; EVAPOTRANSPIRATION ALGORITHM; GLOBAL PRECIPITATION; GAUGE OBSERVATIONS; LAND; DATASET; ENERGY; VAPOR; TRMM; GPCP AB This study compares the net surface water exchange rates, or surface precipitation (P) minus evapotranspiration (ET), and atmospheric water vapour sinks calculated from various observations and reanalyses, and investigates whether they are physically consistent. We use the observed precipitation from the Global Precipitation Climatology Project (GPCP) and the Tropical Rainfall Measuring Mission (TRMM) 3B43, ocean evaporation from Goddard Satellite-based Surface Turbulent Fluxes Version 2c (GSSTF2c), and land ET from the Moderate Resolution Imaging Spectroradiometer (MODIS) global ET project (MOD16) and PT-JPL products to calculate observed P minus observed ET. P-ET is also obtained from atmospheric water vapour sink calculated using Atmospheric Infrared Sounder (AIRS)/Advanced Microwave Sounding Unit observation specific humidity observation and wind fields from the Modern-Era Retrospective Analysis for Research and Applications (MERRA) and ERA-interim, denoted as AIRS(M) and AIRS(E), respectively. MERRA and ERA-interim water vapour budgets are also calculated for cross-comparison and consistency check. The period of study is between 2003 and 2006 based on the availability of all of the data sets. Averaged water vapour sinks from AIRS and reanalysis are consistent over the global ocean and are close to zero (range: 0.02-0.06 mm day(-1)), but range between 0.14 and 0.23 mm day(-1) when land is included. Over ocean within 50 degrees S-50 degrees N, averaged observed P minus observed evaporation shows a much larger negative number than that obtained from AIRS and reanalysis. The differences mainly occur over subtropical oceans, especially in the southern hemisphere in summer and the northern hemisphere in winter. Over land, generally higher agreement between observed P minus observed ET and atmospheric water vapour sinks (calculated from AIRS and reanalysis) is found. However, large regional differences, often with strong seasonal dependence, are also observed over land. Estimates of atmospheric water vapour sinks are influenced by both winds and biases in water vapour data, especially over tropics and subtropical oceans, thereby calling for the need for further investigations and consistency checks of satellite-based and reanalysis water vapour, reanalysis winds, P observations, and surface evaporation estimates. In higher latitudes, atmospheric water vapour sinks calculated from AIRS(M), AIRS(E), MERRA, and ERA-interim are more consistent with each other. C1 [Behrangi, Ali; Wong, Sun; Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Mallick, Kaniska] Ctr Rech Publ Gabriel Lippmann, Dept Environm & Agrobiotechnol EVA, Belvaux, Luxembourg. RP Behrangi, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM ali.behrangi@jpl.nasa.gov OI Fisher, Joshua/0000-0003-4734-9085 FU JPL AIRS project; NASA; NASA's Terrestrial Hydrology Program FX This study was supported by the JPL AIRS project and a contract with NASA. Funding to JBF was provided by NASA's Terrestrial Hydrology Program. Government sponsorship is acknowledged. NR 53 TC 1 Z9 2 U1 0 U2 11 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0143-1161 EI 1366-5901 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PD MAR 19 PY 2014 VL 35 IS 6 BP 2170 EP 2185 DI 10.1080/01431161.2014.889866 PG 16 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA AE4YU UT WOS:000333995200009 ER PT J AU Hees, A Bertone, S Le Poncin-Lafitte, C AF Hees, A. Bertone, S. Le Poncin-Lafitte, C. TI Relativistic formulation of coordinate light time, Doppler, and astrometric observables up to the second post-Minkowskian order SO PHYSICAL REVIEW D LA English DT Article ID GENERAL-RELATIVITY; WORLD FUNCTION; PROPAGATION; CASSINI; FIELD; GRAVITATION; STATIONARY; SPACE; DELAY AB Given the extreme accuracy of modern space science, a precise relativistic modeling of observations is required. In particular, it is important to properly describe light propagation through the Solar System. For two decades, several modeling efforts based on the solution of the null geodesic equations have been proposed, but they are mainly valid only for the first-order post-Newtonian approximation. However, with the increasing precision of ongoing space missions such as Gaia, GAME, BepiColombo, JUNO, and JUICE, we know that some corrections up to the second order have to be taken into account for future experiments. We present a procedure to compute the relativistic coordinate time delay, Doppler, and astrometric observables avoiding the integration of the null geodesic equation. This is possible using the time transfer function formalism, a powerful tool providing key quantities such as the time of flight of a light signal between two point events and the tangent vector to its null geodesic. Indeed, we show how to compute the time transfer functions and their derivatives (and thus range, Doppler, and astrometric observables) up to the second post-Minkowskian order. We express these quantities as quadratures of some functions that depend only on the metric and its derivatives evaluated along a Minkowskian straight line. This method is particularly well adapted for numerical estimations. As an illustration, we provide explicit expressions in static and spherically symmetric space-time up to second post-Minkowskian order. Then we give the order of magnitude of these corrections for the range and Doppler on the BepiColombo mission and for astrometry in a GAME-like observation. C1 [Hees, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bertone, S.; Le Poncin-Lafitte, C.] UPMC, Observ Paris, SYRTE, CNRS UMR 8630, F-75014 Paris, France. [Bertone, S.] Univ Turin, Astrophys Observ Torino, INAF, I-10025 Turin, Italy. RP Hees, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM aurelien.hees@gmail.com; stefano.bertone@aiub.unibe.ch; christophe.leponcin@obspm.fr RI Bertone, Stefano/J-9263-2015 OI Bertone, Stefano/0000-0001-9885-8440 FU Belgian American Educational Foundation (BAEF); Gustave-Boel -Sofina "Plateforme pour l'Education et le Talent"; French-Italian University (UIF/UFI); CNRS/GRAM; CNES/Gaia FX The authors warmly thank P. Teyssandier for useful comments that helped to improve the readability of the manuscript. The research described in this paper was partially carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. A. H. acknowledges support from the Belgian American Educational Foundation (BAEF) and from the Gustave-Boel -Sofina "Plateforme pour l'Education et le Talent." S. B. thanks the French-Italian University (UIF/UFI) for financial support of this work. S. B. and C. L. P.-L. are grateful for the financial support of CNRS/GRAM and CNES/Gaia. NR 56 TC 13 Z9 13 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD MAR 19 PY 2014 VL 89 IS 6 AR 064045 DI 10.1103/PhysRevD.89.064045 PG 18 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AD3BB UT WOS:000333110600003 ER PT J AU Darr, S Hartwig, J AF Darr, Samuel Hartwig, Jason TI Optimal liquid acquisition device screen weave for a liquid hydrogen fuel depot SO INTERNATIONAL JOURNAL OF HYDROGEN ENERGY LA English DT Article DE Liquid hydrogen fuel depot; Liquid acquisition device; Cryogenic fluid management; Porous screen ID SUSTAINABLE ENERGY SYSTEM AB This paper presents the rationale for choosing the optimal screen type for a fully robust screen channel liquid acquisition device (LAD) to be implemented into future in-space liquid hydrogen (LH2) fuel depots. Typical Dutch Twill, Plain Dutch, Twilled Square, and Plain Square weaves are initially considered for comparison. From the set of influential performance parameters from Hartwig and Darr [1], bubble point pressure and flow-through-screen (FTS) pressure drop are combined to define a critical mass flux used to make general comparisons between screens. Based off the minimum bubble point pressure to maintain adequate phase separation against adverse depot acceleration levels, the five finest Dutch Twill screens are down selected for the depot. Along with secondary parameters such as wicking rate and screen compliance, a minimum screen area is defined to select the optimal mesh. Results here indicate that the 450 x 2750 Dutch Twill mesh may be the optimal screen weave for a future LH2 fuel depot. Copyright (C) 2014, Hydrogen Energy Publications, LLC. Published by Elsevier Ltd. All rights reserved. C1 [Darr, Samuel] Univ Florida, Gainesville, FL 32611 USA. [Hartwig, Jason] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Hartwig, J (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM Jason.W.Hartwig@nasa.gov OI Darr, Samuel/0000-0002-1891-405X NR 30 TC 9 Z9 10 U1 2 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0360-3199 EI 1879-3487 J9 INT J HYDROGEN ENERG JI Int. J. Hydrog. Energy PD MAR 18 PY 2014 VL 39 IS 9 BP 4356 EP 4366 DI 10.1016/j.ijhydene.2014.01.035 PG 11 WC Chemistry, Physical; Electrochemistry; Energy & Fuels SC Chemistry; Electrochemistry; Energy & Fuels GA AE3MV UT WOS:000333881500023 ER PT J AU Cyr-Racine, FY de Putter, R Raccanelli, A Sigurdson, K AF Cyr-Racine, Francis-Yan de Putter, Roland Raccanelli, Alvise Sigurdson, Kris TI Constraints on large-scale dark acoustic oscillations from cosmology SO PHYSICAL REVIEW D LA English DT Article ID DIGITAL SKY SURVEY; REDSHIFT-SPACE DISTORTIONS; GALAXY CLUSTER 1E-0657-56; INTERACTION CROSS-SECTION; SDSS-III; SPECTROSCOPIC SURVEY; HUBBLE CONSTANT; POWER-SPECTRUM; HALO MODEL; DATA RELEASE AB If all or a fraction of the dark matter (DM) were coupled to a bath of dark radiation (DR) in the early Universe, we expect the combined DM-DR system to give rise to acoustic oscillations of the dark matter until it decouples from the DR. Much like the standard baryon acoustic oscillations, these dark acoustic oscillations (DAO) imprint a characteristic scale, the sound horizon of dark matter, on the matter power spectrum. We compute in detail how the microphysics of the DM-DR interaction affects the clustering of matter in the Universe and show that the DAO physics also gives rise to unique signatures in the temperature and polarization spectra of the cosmic microwave background (CMB). We use cosmological data from the CMB, baryon acoustic oscillations, and large-scale structure to constrain the possible fraction of interacting DM as well as the strength of its interaction with DR. Like nearly all knowledge we have gleaned about DM since inferring its existence this constraint rests on the betrayal by gravity of the location of otherwise invisible DM. Although our results can be straightforwardly applied to a broad class of models that couple dark matter particles to various light relativistic species, in order to make quantitative predictions, we model the interacting component as dark atoms coupled to a bath of dark photons. We find that linear cosmological data and CMB lensing put strong constraints on the existence of DAO features in the CMB and the large-scale structure of the Universe. Interestingly, we find that at most similar to 5% of all DM can be very strongly interacting with DR. We show that our results are surprisingly constraining for the recently proposed double-disk DM model, a novel example of how large-scale precision cosmological data can be used to constrain galactic physics and subgalactic structure. C1 [Cyr-Racine, Francis-Yan; de Putter, Roland; Raccanelli, Alvise] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. [Cyr-Racine, Francis-Yan; de Putter, Roland; Raccanelli, Alvise] CALTECH, Pasadena, CA 91125 USA. [Sigurdson, Kris] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. RP Cyr-Racine, FY (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM francis-yan.cyr-racine@jpl.nasa.gov OI Raccanelli, Alvise/0000-0001-6726-0438; Cyr-Racine, Francis-Yan/0000-0002-7939-2988 FU W. M. Keck Foundation; W. M. Keck Institute for Space Studies Postdoctoral Fellow program; National Science and Engineering Research Council (NSERC) of Canada; National Science Foundation [NSF PHY11-25915]; NASA ATP Grant [11-ATP-090] FX We thank JiJi Fan, Andrey Katz, Lisa Randall, Matthew Reece, and Manoj Kaplinghat for useful discussions. We further thank Abhilash Mishra, Marius Millea, and Matthew Reece for insightful comments on an earlier version of this draft. We are also grateful to Olga Mena and Shun Saito for generously providing an initial version of the code for the BOSS galaxy power spectrum likelihood. This work was performed in part at the California Institute of Technology for the Keck Institute for Space Studies, which is funded by the W. M. Keck Foundation. F.-Y.C.-R. acknowledges support from the W. M. Keck Institute for Space Studies Postdoctoral Fellow program. The research of K. S. is supported in part by a National Science and Engineering Research Council (NSERC) of Canada Discovery Grant. F.-Y.C.-R. and K. S. thank the Aspen Center for Physics, where part of this work was completed, for their hospitality. This research was supported in part by the National Science Foundation under Grant No. NSF PHY11-25915. Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Part of this work is supported by NASA ATP Grant No. 11-ATP-090. NR 144 TC 47 Z9 47 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD MAR 17 PY 2014 VL 89 IS 6 AR 063517 DI 10.1103/PhysRevD.89.063517 PG 24 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AD3AT UT WOS:000333109700006 ER PT J AU Ammond, RF Ferrante, RF Hudson, RL AF Ammond, Rachelle F. Ferrante, Robert F. Hudson, Reggie L. TI Laboratory studies of ice mixtures of astrophysical interest SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc C1 [Ammond, Rachelle F.; Ferrante, Robert F.] US Naval Acad, Dept Chem, Annapolis, MD 21402 USA. [Hudson, Reggie L.] NASA, Astrochem Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM m140126@usna.edu; ferrante@usna.edu NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 308-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HZ UT WOS:000348457603701 ER PT J AU Brown, AT Hu, YF Bux, SK Kauzlarich, S AF Brown, Alexander T. Hu, Yufei Bux, Sabah K. Kauzlarich, Susan TI Synthesis and properties of Yb10Ca4-xBixMnSb11 SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc C1 [Hu, Yufei; Kauzlarich, Susan] Univ Calif Davis, Dept Chem, Davis, CA 95616 USA. [Brown, Alexander T.] Colorado Mesa Univ, Dept Phys & Environm Sci, Grand Junction, CO 81501 USA. [Bux, Sabah K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM abrowncitizen@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 320-INOR PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HZ UT WOS:000348457601409 ER PT J AU Denkins, PS AF Denkins, Pamela S. TI Pamela Denkins: NASA/Johnson Space Center SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc C1 [Denkins, Pamela S.] NASA Johnson Space Ctr, Houston, TX 77058 USA. EM pamela.s.denkins@nasa.gov NR 0 TC 0 Z9 0 U1 1 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 5-PROF PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HZ UT WOS:000348457605233 ER PT J AU Dodson, LG Shen, LH Savee, JD Eddingsaas, NC Welz, O Taatjes, CA Osborn, DL Sander, SP Okumura, M AF Dodson, Leah G. Shen, Linhan Savee, John D. Eddingsaas, Nathan C. Welz, Oliver Taatjes, Craig A. Osborn, David L. Sander, Stanley P. Okumura, Mitchio TI Kinetics and product yields of the acetyl peroxy + HO2 radical reaction studied by photoionization mass spectrometry SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc C1 [Dodson, Leah G.; Shen, Linhan; Eddingsaas, Nathan C.; Okumura, Mitchio] CALTECH, Dept Chem & Chem Engn, Pasadena, CA 91125 USA. [Savee, John D.; Welz, Oliver; Taatjes, Craig A.; Osborn, David L.] Sandia Natl Labs, Combust Resource Facil, Livermore, CA 94550 USA. [Sander, Stanley P.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Eddingsaas, Nathan C.] Rochester Inst Technol, Sch Chem & Mat Sci, Rochester, NY 14623 USA. EM lgdodson@caltech.edu NR 0 TC 0 Z9 0 U1 4 U2 9 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 98-ENVR PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HZ UT WOS:000348457600317 ER PT J AU Guo, HQ Meador, MAB Wilkewitz, B AF Guo, Haiquan Meador, Mary Ann B. Wilkewitz, Brittany TI Flexible polyimide aerogels cross-linked by poly(maleic anhydride-alt-alkylene) SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc C1 [Guo, Haiquan] Ohio Aerosp Inst, Cleveland, OH USA. [Meador, Mary Ann B.; Wilkewitz, Brittany] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM haiquanguo@oai.org NR 0 TC 0 Z9 0 U1 3 U2 7 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 83-PMSE PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HZ UT WOS:000348457604068 ER PT J AU Head-Gordon, M Peverati, R Bera, P Lee, TJ AF Head-Gordon, Martin Peverati, Roberto Bera, Partha Lee, Timothy J. TI Recent advances in electronic structure methods with applications to hydrocarbon association and growth mechanisms SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc C1 [Head-Gordon, Martin; Peverati, Roberto] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA. [Bera, Partha; Lee, Timothy J.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. EM mhg@cchem.berkeley.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 274-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HZ UT WOS:000348457603674 ER PT J AU Hudson, RL AF Hudson, Reggie L. TI Miroslaw Kernbaum and the curious case of planetary peroxide SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc C1 [Hudson, Reggie L.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. EM reggie.hudson@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 4-HIST PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HZ UT WOS:000348457600825 ER PT J AU Lee, TJ AF Lee, Timothy J. TI Applications of quantum chemistry to astrochemistry: Spectroscopic signatures, properties, and formation mechanisms SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc ID VIBRATIONAL FREQUENCIES; CONSTANTS C1 [Lee, Timothy J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. EM Timothy.J.Lee@nasa.gov NR 5 TC 0 Z9 0 U1 0 U2 2 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 275-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HZ UT WOS:000348457603675 ER PT J AU Lin, Y Kim, JW Connell, JW AF Lin, Yi Kim, Jae-Woo Connell, John W. TI Holey graphene supercapacitors SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc C1 [Lin, Yi; Kim, Jae-Woo] Natl Inst Aerosp, Hampton, VA 23666 USA. [Connell, John W.] NASA Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. EM yi.lin-1@nasa.gov RI Kim, Jae-Woo/A-8314-2008 NR 0 TC 0 Z9 0 U1 0 U2 4 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 421-ENFL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HZ UT WOS:000348457600155 ER PT J AU Mattioda, A Cook, A Quinn, R Elsaesser, A Ehrenfreund, P Ricca, A Jones, NC Hoffmann, S Ricco, A AF Mattioda, Andrew Cook, Amanda Quinn, Richard Elsaesser, Andreas Ehrenfreund, Pascale Ricca, Alessandra Jones, Nykola C. Hoffmann, Soren Ricco, Antonio TI Organism/organic exposure to orbital stresses (O/OREOS) satellite: Radiation exposure in LEO and supporting laboratory studies SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc C1 [Mattioda, Andrew; Cook, Amanda; Ricco, Antonio] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Quinn, Richard; Ricca, Alessandra] SETI Inst, Mountain View, CA USA. [Elsaesser, Andreas] Leiden Univ, Leiden, Netherlands. [Ehrenfreund, Pascale] George Washington Univ, Inst Space Policy, Washington, DC 20052 USA. [Jones, Nykola C.; Hoffmann, Soren] Aarhus Univ, Dept Phys & Astron, ISA, Aarhus, Denmark. EM andrew.mattioda@nasa.gov NR 0 TC 0 Z9 0 U1 1 U2 3 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 134-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HZ UT WOS:000348457603538 ER PT J AU Millar, TJ Cordiner, MA Charnley, SB Milam, SN Gull, TR AF Millar, T. J. Cordiner, M. A. Charnley, S. B. Milam, S. N. Gull, T. R. TI Eta Carinae: Astrochemistry in an extreme environment SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc C1 [Millar, T. J.] Queens Univ Belfast, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. [Cordiner, M. A.; Charnley, S. B.; Milam, S. N.; Gull, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM tom.millar@qub.ac.uk RI Milam, Stefanie/D-1092-2012 OI Milam, Stefanie/0000-0001-7694-4129 FU Science and Technology Facilities Council [ST/L000709/1, ST/M001970/1, ST/M003515/1] NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 174-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HZ UT WOS:000348457603577 ER PT J AU Netzer, NL Chen, B Jiang, CY AF Netzer, Nathan L. Chen, Bin Jiang, Chaoyang TI Tunable surface-enhanced Raman scattering of chemically modified silver nanowire thin films SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc C1 [Netzer, Nathan L.; Jiang, Chaoyang] Univ S Dakota, Dept Chem, Vermillion, SD 57069 USA. [Chen, Bin] NASA, Adv Studies Labs, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Nate.Netzer@coyotes.usd.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 416-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HZ UT WOS:000348457603797 ER PT J AU Nguyen, BN Meador, MAB Sandberg, A Cudjoe, E Rowan, SJ AF Nguyen, Boachau N. Meador, Mary Ann B. Sandberg, Anna Cudjoe, Elvis Rowan, Stuart J. TI Polyimide aerogels fabricated with cellulose nanocrystals SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc C1 [Nguyen, Boachau N.] Ohio Aerosp Inst, Brookpark, OH 44142 USA. [Meador, Mary Ann B.; Sandberg, Anna] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Cudjoe, Elvis; Rowan, Stuart J.] Case Western Reserve Univ, Cleveland, OH 44106 USA. EM baochau.n.nguyen@nasa.gov NR 0 TC 0 Z9 0 U1 2 U2 5 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 50-PMSE PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HZ UT WOS:000348457604035 ER PT J AU Theis, M Fortenberry, RC Lee, TJ Candian, A Tielens, XGGM AF Theis, Mallory Fortenberry, Ryan C. Lee, Timothy J. Candian, Alessandra Tielens, Xander G. G. M. TI Electronically excited states of PANH anions and application to interstellar spectra SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc C1 [Theis, Mallory; Fortenberry, Ryan C.] Georgia So Univ, Dept Chem, Statesboro, GA 30461 USA. [Lee, Timothy J.] NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA. [Candian, Alessandra; Tielens, Xander G. G. M.] Leiden Univ, Leiden Observ, Leiden, South Holland, Netherlands. EM rfortenberry@georgiasouthern.edu NR 0 TC 0 Z9 0 U1 1 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 307-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HZ UT WOS:000348457603700 ER PT J AU Baker, JS Williams, TS Miller, SG Meador, MA AF Baker, James S. Williams, Tiffany S. Miller, Sandi G. Meador, Michael A. TI Improved composites using crosslinked, surface-modified carbon nanotube materials SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc C1 [Baker, James S.; Williams, Tiffany S.; Miller, Sandi G.; Meador, Michael A.] NASA Glenn Res Ctr, Polymer Branch, Cleveland, OH 44135 USA. EM jsb39@zips.uakron.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 432-COLL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HD UT WOS:000348455204178 ER PT J AU Boucher, DS Barrett, HP Kennedy, WJ AF Boucher, David S. Barrett, Hayden P. Kennedy, William J. TI Spectroscopic characterization of P3HT/SWNT composites synthesized using in situ GRIM methods: Improved polymer ordering via nanoscaffolding SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc C1 [Boucher, David S.; Barrett, Hayden P.] Coll Charleston, Dept Chem & Biochem, Charleston, SC 29424 USA. [Kennedy, William J.] NASA, Lyndon B Johnson Space Ctr, Struct Engn Div, Houston, TX 77058 USA. EM boucherds@cofc.edu NR 0 TC 0 Z9 0 U1 1 U2 4 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 636-COLL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HD UT WOS:000348455204375 ER PT J AU Popa, A Li, J Samia, AC AF Popa, Adriana Li, Jing Samia, Anna C. TI Hybrid metal nanobox/carbon composites for environmental and biomedical sensing applications SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc C1 [Popa, Adriana; Samia, Anna C.] Case Western Reserve Univ, Dept Chem, Cleveland, OH 44106 USA. [Li, Jing] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM anp29@case.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 812-COLL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HD UT WOS:000348455204541 ER PT J AU Shultz, MJ Bisson, P Vu, T Wang, J AF Shultz, Mary Jane Bisson, Patrick Vu, Tuan Wang, Jing TI Aqueous interfaces: Localized and collective vibrations probed with nonlinear spectroscopy SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc C1 [Shultz, Mary Jane; Wang, Jing] Tufts Univ, Medford, MA 02155 USA. [Bisson, Patrick] Darmouth Coll, Thayer Sch Engn Dartmouth, Hanover, NH 03755 USA. [Vu, Tuan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM Mary.Shultz@Tufts.edu NR 0 TC 0 Z9 0 U1 0 U2 4 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 589-COLL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HD UT WOS:000348455204330 ER PT J AU Baker, DN Jaynes, AN Li, X Henderson, MG Kanekal, SG Reeves, GD Spence, HE Claudepierre, SG Fennell, JF Hudson, MK Thorne, RM Foster, JC Erickson, PJ Malaspina, DM Wygant, JR Boyd, A Kletzing, CA Drozdov, A Shprits, YY AF Baker, D. N. Jaynes, A. N. Li, X. Henderson, M. G. Kanekal, S. G. Reeves, G. D. Spence, H. E. Claudepierre, S. G. Fennell, J. F. Hudson, M. K. Thorne, R. M. Foster, J. C. Erickson, P. J. Malaspina, D. M. Wygant, J. R. Boyd, A. Kletzing, C. A. Drozdov, A. Shprits, Y. Y. TI Gradual diffusion and punctuated phase space density enhancements of highly relativistic electrons: Van Allen Probes observations SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE radiation belt acceleration ID RADIATION-BELT ELECTRONS; GEOMAGNETIC STORMS; INNER MAGNETOSPHERE; ACCELERATION; RING; ISTP AB The dual-spacecraft Van Allen Probes mission has provided a new window into mega electron volt (MeV) particle dynamics in the Earth's radiation belts. Observations (up to E similar to 10MeV) show clearly the behavior of the outer electron radiation belt at different timescales: months-long periods of gradual inward radial diffusive transport and weak loss being punctuated by dramatic flux changes driven by strong solar wind transient events. We present analysis of multi-MeV electron flux and phase space density (PSD) changes during March 2013 in the context of the first year of Van Allen Probes operation. This March period demonstrates the classic signatures both of inward radial diffusive energization and abrupt localized acceleration deep within the outer Van Allen zone (L similar to 4.00.5). This reveals graphically that both competing mechanisms of multi-MeV electron energization are at play in the radiation belts, often acting almost concurrently or at least in rapid succession. Key Points Clear observations to higher energy than ever before Precise detection of where and how acceleration takes place Provides new eyes on megaelectron Volt C1 [Baker, D. N.; Jaynes, A. N.; Li, X.; Malaspina, D. M.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Henderson, M. G.; Reeves, G. D.] Los Alamos Natl Lab, Los Alamos, NM USA. [Kanekal, S. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Spence, H. E.; Boyd, A.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Claudepierre, S. G.; Fennell, J. F.] Aerosp Corp, Dept Space Sci, El Segundo, CA 90245 USA. [Hudson, M. K.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Thorne, R. M.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. [Foster, J. C.; Erickson, P. J.] MIT, Haystack Observ, Westford, MA 01886 USA. [Wygant, J. R.] Univ Minnesota, Dept Phys & Astron, Minneapolis, MN 55455 USA. [Kletzing, C. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Drozdov, A.; Shprits, Y. Y.] Univ Calif Los Angeles, Dept Earth Space Sci, Los Angeles, CA USA. [Shprits, Y. Y.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. [Shprits, Y. Y.] Skolkovo Inst Sci & Technol, Skolkovo, Russia. RP Baker, DN (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA. EM Daniel.Baker@LASP.colorado.edu RI Reeves, Geoffrey/E-8101-2011; Henderson, Michael/A-3948-2011; OI Kletzing, Craig/0000-0002-4136-3348; Spence, Harlan/0000-0002-2526-2205; Reeves, Geoffrey/0000-0002-7985-8098; Henderson, Michael/0000-0003-4975-9029; Drozdov, Alexander/0000-0002-5334-2026; Boyd, Alexander/0000-0002-9725-508X FU JHU/APL under NASA [967399, NAS5-01072] FX This work was supported by JHU/APL contract 967399 under NASA's prime contract NAS5-01072. All Van Allen Probes data used are publicly available at (www.rbsp-ect.lanl.gov). NR 22 TC 37 Z9 37 U1 1 U2 15 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 MAR 16 PY 2014 VL 41 IS 5 BP 1351 EP 1358 DI 10.1002/2013GL058942 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AD9IO UT WOS:000333578800001 ER PT J AU Capria, MT Tosi, F De Sanctis, MC Capaccioni, F Ammannito, E Frigeri, A Zambon, F Fonte, S Palomba, E Turrini, D Titus, TN Schroder, SE Toplis, M Li, JY Combe, JP Raymond, CA Russell, CT AF Capria, M. T. Tosi, F. De Sanctis, M. C. Capaccioni, F. Ammannito, E. Frigeri, A. Zambon, F. Fonte, S. Palomba, E. Turrini, D. Titus, T. N. Schroeder, S. E. Toplis, M. Li, J. -Y. Combe, J. -P. Raymond, C. A. Russell, C. T. TI Vesta surface thermal properties map SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Vesta; Vesta thermal inertia; thermal properties; Vesta surface ID ASTEROID 21 LUTETIA; DAWN; SUBMILLIMETER; TEMPERATURE; REGOLITH; MARS AB The first ever regional thermal properties map of Vesta has been derived from the temperatures retrieved by infrared data by the mission Dawn. The low average value of thermal inertia, 3010 J m(-2)s(-0.5)K(-1), indicates a surface covered by a fine regolith. A range of thermal inertia values suggesting terrains with different physical properties has been determined. The lower thermal inertia of the regions north of the equator suggests that they are covered by an older, more processed surface. A few specific areas have higher than average thermal inertia values, indicative of a more compact material. The highest thermal inertia value has been determined on the Marcia crater, known for its pitted terrain and the presence of hydroxyl in the ejecta. Our results suggest that this type of terrain can be the result of soil compaction following the degassing of a local subsurface reservoir of volatiles. Key Points A thermophysical map of Vesta has been derived from spatially resolved data The average thermal inertia of the surface of Vesta is 30 +/- 10 Jm(-2)s(-0.5)K(-1) Pitted terrains in Marcia crater have the highest thermal inertia value C1 [Capria, M. T.; Tosi, F.; De Sanctis, M. C.; Capaccioni, F.; Ammannito, E.; Frigeri, A.; Zambon, F.; Fonte, S.; Palomba, E.; Turrini, D.] INAF, Ist Astrofis & Planetol Spaziali, Rome, Italy. [Titus, T. N.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Schroeder, S. E.] Deutsch Zentrum Luft & Raumfahrt, Berlin, Germany. [Toplis, M.] Observ Midi Pyrenees, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France. [Li, J. -Y.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Combe, J. -P.] Bear Fight Inst, Winthrop, WA USA. [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. RP Capria, MT (reprint author), INAF, Ist Astrofis & Planetol Spaziali, Rome, Italy. EM mariateresa.capria@iaps.inaf.it RI De Sanctis, Maria Cristina/G-5232-2013; Schroder, Stefan/D-9709-2013; Frigeri, Alessandro/F-2151-2010; OI Palomba, Ernesto/0000-0002-9101-6774; Tosi, Federico/0000-0003-4002-2434; Zambon, Francesca/0000-0002-4190-6592; De Sanctis, Maria Cristina/0000-0002-3463-4437; Schroder, Stefan/0000-0003-0323-8324; Frigeri, Alessandro/0000-0002-9140-3977; capria, maria teresa/0000-0002-9814-9588; Turrini, Diego/0000-0002-1923-7740; Capaccioni, Fabrizio/0000-0003-1631-4314 FU Italian Space Agency (ASI), ASI-INAF [I/004/12/0]; Dawn Science, Instrument, Operations Teams; Dawn at Vesta Participating Scientist program FX The VIR project is funded by the Italian Space Agency (ASI), ASI-INAF contract I/004/12/0. VIR was developed under the leadership of the Istituto di Astrofisica e Planetologia Spaziale (INAF-IAPS), Rome, Italy. The instrument was built by Selex-Galileo, Florence, Italy. Support of the Dawn Science, Instrument, Operations Teams, as well as of the Dawn at Vesta Participating Scientist program, is gratefully acknowledged. We also acknowledge the hard work carried out by Robert Gaskell in providing a detailed shape model that was used in this work to properly model the data. The data obtained by VIR are available at the Small Bodies Node of the Planetary Data System (http://sbn.pds.nasa.gov/). NR 31 TC 18 Z9 18 U1 0 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 MAR 16 PY 2014 VL 41 IS 5 BP 1438 EP 1443 DI 10.1002/2013GL059026 PG 6 WC Geosciences, Multidisciplinary SC Geology GA AD9IO UT WOS:000333578800013 ER PT J AU Konopliv, AS Park, RS Yuan, DN Asmar, SW Watkins, MM Williams, JG Fahnestock, E Kruizinga, G Paik, M Strekalov, D Harvey, N Smith, DE Zuber, MT AF Konopliv, Alex S. Park, Ryan S. Yuan, Dah-Ning Asmar, Sami W. Watkins, Michael M. Williams, James G. Fahnestock, Eugene Kruizinga, Gerhard Paik, Meegyeong Strekalov, Dmitry Harvey, Nate Smith, David E. Zuber, Maria T. TI High-resolution lunar gravity fields from the GRAIL Primary and Extended Missions SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE gravity; spherical harmonics ID MOON; CRUST AB The resolution and accuracy of the lunar spherical harmonic gravity field have been dramatically improved as a result of the Gravity Recovery and Interior Laboratory (GRAIL) mission. From the Primary Mission, previous harmonic gravity fields resulted in an average n=420 surface resolution and a Bouguer spectrum to n=330. The GRAIL Extended Mission improves the resolution due to a lower average 23 km altitude orbit. As a result, new harmonic degree 900 gravity fields (GL0900C and GL0900D) show nearly a factor of 2 improvement with an average surface resolution n=870 and the Bouguer spectrum extended to n=550. Since the minimum spacecraft altitude varies spatially between 3km and 23km, the surface resolution is variable from near n=680 for the central farside to near n=900 for the polar regions. These gravity fields with 0.8 million parameters are by far the highest-degree fields of any planet ever estimated with a fully dynamic least squares technique using spacecraft tracking data. Key Points A degree 900 gravity field from the GRAIL Primary and Extended Mission The GRAIL Extended Mission doubles the resolution of the gravity field The Bouguer spectrum is well determined to near harmonic degree 550 C1 [Konopliv, Alex S.; Park, Ryan S.; Yuan, Dah-Ning; Asmar, Sami W.; Watkins, Michael M.; Williams, James G.; Fahnestock, Eugene; Kruizinga, Gerhard; Paik, Meegyeong; Strekalov, Dmitry; Harvey, Nate] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. RP Konopliv, AS (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Alexander.S.Konopliv@jpl.nasa.gov FU National Aeronautics and Space Administration FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We gratefully acknowledge the use of the Ames Pleiades Supercomputer that was used to generate the gravity solutions of this paper. We thank Mark Wieczorek for providing the equivalent gravity from topography harmonic field that is used in this paper. We appreciate Terry Sabaka directing us on the techniques of generating gravity errors using clone fields from the covariance matrix. Data used to generate the results of this paper are available at http://pds-geosciences.wustl.edu. NR 20 TC 20 Z9 25 U1 0 U2 11 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 MAR 16 PY 2014 VL 41 IS 5 BP 1452 EP 1458 DI 10.1002/2013GL059066 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AD9IO UT WOS:000333578800015 ER PT J AU Thomas, AC Reager, JT Famiglietti, JS Rodell, M AF Thomas, Alys C. Reager, John T. Famiglietti, James S. Rodell, Matthew TI A GRACE- based water storage deficit approach for hydrological drought characterization SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE GRACE terrestrial water storage; water storage deficit; GRACE-identified hydrological drought; drought severity ID DEPLETION AB We present a quantitative approach for measuring hydrological drought occurrence and severity based on terrestrial water storage observations from NASA's Gravity Recovery and Climate Experiment (GRACE) satellite mission. GRACE measurements are applied by calculating the magnitude of the deviation of regional, monthly terrestrial water storage anomalies from the time series' monthly climatology, where negative deviations represent storage deficits. Monthly deficits explicitly quantify the volume of water required to return to normal water storage conditions. We combine storage deficits with event duration to calculate drought severity. Drought databases are referenced to identify meteorological drought events in the Amazon and Zambezi River basins and the southeastern United States and Texas regions. This storage deficit method clearly identifies hydrological drought onset, end, and duration; quantifies instantaneous severity and peak drought magnitude; and compares well with the meteorological drought databases. It also reveals information about the hydrological effects of meteorological drought on regional water storage. Key Point GRACE-based drought severity using water storage rather than just precipitation explicitly quantifies the volume of water needed to return to normal conditions and identifies hydrological drought onset, peak magnitude, duration, and severity C1 [Thomas, Alys C.; Reager, John T.; Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Reager, John T.; Famiglietti, James S.] Univ Calif Irvine, UC Ctr Hydrol Modeling, Irvine, CA USA. [Famiglietti, James S.] Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA USA. [Rodell, Matthew] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. RP Famiglietti, JS (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. EM jfamigli@uci.edu RI Rodell, Matthew/E-4946-2012 OI Rodell, Matthew/0000-0003-0106-7437 FU NASA GRACE Science Team; NASA Develop; NASA Graduate Student Researchers Program; University of California Office of the President, Multi-Campus Research Programs and Initiatives FX This work was supported by grants from the NASA GRACE Science Team, NASA Develop, NASA Graduate Student Researchers Program, and from the University of California Office of the President, Multi-Campus Research Programs and Initiatives. Special thanks to Caroline de Linage and Brian Thomas for offering their feedback as well as colleagues in the Hydrological Sciences Laboratory at NASA Goddard Space Flight Center. NR 24 TC 49 Z9 50 U1 3 U2 50 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 MAR 16 PY 2014 VL 41 IS 5 BP 1537 EP 1545 DI 10.1002/2014GL059323 PG 9 WC Geosciences, Multidisciplinary SC Geology GA AD9IO UT WOS:000333578800027 ER PT J AU Mouginot, J Rignot, E Scheuchl, B AF Mouginot, J. Rignot, E. Scheuchl, B. TI Sustained increase in ice discharge fromthe Amundsen Sea Embayment, West Antarctica, from1973 to 2013 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE ice dynamic; ice flux; West Antarctica ID PINE ISLAND GLACIER; MARIE-BYRD-LAND; RADAR INTERFEROMETRY; THWAITES GLACIER; MASS-BALANCE; SHEET; SHELF; RETREAT; ACCELERATION; FLOW AB We combine measurements of ice velocity from Landsat feature tracking and satellite radar interferometry, and ice thickness from existing compilations to document 41 years of mass flux from the Amundsen Sea Embayment (ASE) of West Antarctica. The total ice discharge has increased by 77% since 1973. Half of the increase occurred between 2003 and 2009. Grounding-line ice speeds of Pine Island Glacier stabilized between 2009 and 2013, following a decade of rapid acceleration, but that acceleration reached far inland and occurred at a rate faster than predicted by advective processes. Flow speeds across Thwaites Glacier increased rapidly after 2006, following a decade of near-stability, leading to a 33% increase in flux between 2006 and 2013. Haynes, Smith, Pope, and Kohler Glaciers all accelerated during the entire study period. The sustained increase in ice discharge is a possible indicator of the development of a marine ice sheet instability in this part of Antarctica. Key Points Sustained ASE mass flux increase: 77% since 1973 Thwaites accelerated by 33% during the last 6 years Speed changes are pervasive and rapid: major implications for ice flow modeling C1 [Mouginot, J.; Rignot, E.; Scheuchl, B.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Rignot, E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Mouginot, J (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. EM jmougino@uci.edu RI Mouginot, Jeremie/G-7045-2015; Rignot, Eric/A-4560-2014 OI Rignot, Eric/0000-0002-3366-0481 FU National Aeronautics and Space Administration's Cryospheric Science Program; National Aeronautics and Space Administration's MEaSUREs program FX This work was performed at the University of California, Irvine, and at the Jet Propulsion Laboratory, California Institute of Technology, under a grant from the National Aeronautics and Space Administration's Cryospheric Science Program and MEaSUREs program. The authors gratefully acknowledge the European Space Agency, the Canadian Space Agency, the Japan Aerospace Exploration Agency, and the Deutsches Zentrum fur Luft- und Raumfahrt for the use of ERS-1&-2, RADARSAT-1&-2, ALOS PALSAR, and TanDEM-X data, respectively. Data acquisition was coordinated by the Space Task Group (2006-2009) and the Polar Space Task Group (post 2009). NR 44 TC 65 Z9 69 U1 5 U2 54 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 MAR 16 PY 2014 VL 41 IS 5 BP 1576 EP 1584 DI 10.1002/2013GL059069 PG 9 WC Geosciences, Multidisciplinary SC Geology GA AD9IO UT WOS:000333578800032 ER PT J AU Hakkinen, S Hall, DK Shuman, CA Worthen, DL DiGirolamo, NE AF Haekkinen, Sirpa Hall, Dorothy K. Shuman, Christopher A. Worthen, Denise L. DiGirolamo, Nicolo E. TI Greenland ice sheet melt from MODIS and associated atmospheric variability SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Greenland ice sheet; melt; blocking ID SURFACE-TEMPERATURE; CIRCULATION; CLIMATOLOGY; BLOCKING; MODEL AB Daily June-July melt fraction variations over the Greenland ice sheet (GIS) derived from the Moderate Resolution Imaging Spectroradiometer (MODIS) (2000-2013) are associated with atmospheric blocking forming an omega-shape ridge over the GIS at 500hPa height. Blocking activity with a range of time scales, from synoptic waves breaking poleward (<5days) to full-fledged blocks (5days), brings warm subtropical air masses over the GIS controlling daily surface temperatures and melt. The temperature anomaly of these subtropical air mass intrusions is also important for melting. Based on the years with the greatest melt (2002 and 2012) during the MODIS era, the area-average temperature anomaly of 2 standard deviations above the 14 year June-July mean results in a melt fraction of 40% or more. Though the summer of 2007 had the most blocking days, atmospheric temperature anomalies were too small to instigate extreme melting. Key Points Short-term atmospheric blocking over Greenland contributes to melt episodes Associated temperature anomalies are equally important for the melt Duration and strength of blocking events contribute to surface melt intensity C1 [Haekkinen, Sirpa; Hall, Dorothy K.; Shuman, Christopher A.; Worthen, Denise L.; DiGirolamo, Nicolo E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Shuman, Christopher A.] Univ Maryland, Joint Ctr Earth Syst Technol JCET, Baltimore, MD 21201 USA. [Worthen, Denise L.] Wyle Informat Syst LLC, Lanham, MD USA. [DiGirolamo, Nicolo E.] Sci Syst & Applicat Inc, Lanham, MD USA. RP Hakkinen, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Sirpa.Hakkinen@nasa.gov FU NASA Cryospheric Sciences Program; NASA Physical Oceanography Program FX We thank the NASA Cryospheric Sciences Program and the NASA Physical Oceanography Program for support. We are grateful for the constructive comments by Son Nghiem and one anonymous reviewer and by the Editor, Julienne Stroeve. NR 22 TC 11 Z9 11 U1 2 U2 13 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 MAR 16 PY 2014 VL 41 IS 5 BP 1600 EP 1607 DI 10.1002/2013GL059185 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AD9IO UT WOS:000333578800035 ER PT J AU Aquila, V Garfinkel, CI Newman, PA Oman, LD Waugh, DW AF Aquila, V. Garfinkel, C. I. Newman, P. A. Oman, L. D. Waugh, D. W. TI Modifications of the quasi-biennial oscillation by a geoengineering perturbation of the stratospheric aerosol layer SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE geoengineering; QBO; stratospheric aerosol ID PINATUBO ERUPTION; OZONE; CIRCULATION; QBO AB This paper examines the impact of geoengineering via stratospheric sulfate aerosol on the quasi-biennial oscillation (QBO) using the NASA Goddard Earth Observing System version 5 Chemistry Climate Model. We performed four 30 year simulations with a continuous injection of sulfur dioxide on the equator at 0 degrees longitude. The four simulations differ by the amount of sulfur dioxide injected (5 Tg/yr and 2.5 Tg/yr) and the altitude of the injection (16km-25km and 22km-25km). We find that such an injection dramatically alters the quasi-biennial oscillation, prolonging the phase of easterly shear with respect to the control simulation. This is caused by the increased aerosol heating and associated warming in the tropical lower stratosphere and higher residual vertical velocity. In the case of maximum perturbation, i.e., highest stratospheric aerosol burden, the lower tropical stratosphere is locked into a permanent westerly QBO phase. Key Points Geoengineering aerosol would prolong the westerly phase of the QBO Large geoengineering stratospheric aerosol injections might interrupt the QBO QBO changes are due to aerosol warming and increased residual vertical velocity C1 [Aquila, V.] Goddard Earth Sci Technol & Res, Greenbelt, MD 20771 USA. [Aquila, V.; Waugh, D. W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Garfinkel, C. I.] Hebrew Univ Jerusalem, Fredy & Nadine Herrmann Inst Earth Sci, Jerusalem, Israel. [Newman, P. A.; Oman, L. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Aquila, V (reprint author), Goddard Earth Sci Technol & Res, Greenbelt, MD 20771 USA. EM valentina.aquila@jhu.edu RI Oman, Luke/C-2778-2009; Aquila, Valentina/D-7267-2012; garfinkel, chaim/H-6215-2012; Waugh, Darryn/K-3688-2016 OI Oman, Luke/0000-0002-5487-2598; Aquila, Valentina/0000-0003-2060-6694; garfinkel, chaim/0000-0001-7258-666X; Waugh, Darryn/0000-0001-7692-2798 NR 34 TC 21 Z9 21 U1 1 U2 16 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 MAR 16 PY 2014 VL 41 IS 5 BP 1738 EP 1744 DI 10.1002/2013GL058818 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AD9IO UT WOS:000333578800054 ER PT J AU Basu, S Krol, M Butz, A Clerbaux, C Sawa, Y Machida, T Matsueda, H Frankenberg, C Hasekamp, OP Aben, I AF Basu, S. Krol, M. Butz, A. Clerbaux, C. Sawa, Y. Machida, T. Matsueda, H. Frankenberg, C. Hasekamp, O. P. Aben, I. TI The seasonal variation of the CO2 flux over Tropical Asia estimated fromGOSAT, CONTRAIL, and IASI SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE inverse modeling; Tropical Asia; GOSAT; CONTRAIL; IASI ID ATMOSPHERIC CO2; CARBON BALANCE; EMISSIONS; GOSAT; RETRIEVALS; AEROSOL; FIRES AB We estimate the CO2 flux over Tropical Asia in 2009, 2010, and 2011 using Greenhouse Gases Observing Satellite (GOSAT) total column CO2(XCO2) and in situ measurements of CO2. Compared to flux estimates from assimilating surface measurements of CO2, GOSAT XCO2 estimates a more dynamic seasonal cycle and a large source in March-May 2010. The more dynamic seasonal cycle is consistent with earlier work by Patra et al. (2011), and the enhanced 2010 source is supported by independent upper air CO2 measurements from the Comprehensive Observation Network for Trace gases by Airliner (CONTRAIL) project. Using Infrared Atmospheric Sounding Interferometer (IASI) measurements of total column CO (XCO), we show that biomass burning CO2 can explain neither the dynamic seasonal cycle nor the 2010 source. We conclude that both features must come from the terrestrial biosphere. In particular, the 2010 source points to biosphere response to above-average temperatures that year. Key Points GOSAT estimates a dynamic seasonal cycle over Tropical Asia The GOSAT-estimated seasonal cycle is confirmed by CONTRAIL data IASI CO shows that the dynamism is not caused by biomass burning C1 [Basu, S.; Krol, M.; Hasekamp, O. P.; Aben, I.] SRON Netherlands Inst Space Res, Utrecht, Netherlands. [Basu, S.] NOAA, ESRL GMD, Boulder, CO USA. [Basu, S.; Krol, M.] Univ Utrecht, Inst Marine & Atmospher Res Utrecht, Utrecht, Netherlands. [Krol, M.] Univ Wageningen & Res Ctr, MAQ, Wageningen, Netherlands. [Butz, A.] Karlsruhe Inst Technol, IMK ASF, Eggenstein Leopoldshafen, Germany. [Clerbaux, C.] Univ Paris 06, Univ Versailles St Quentin En Yvelines, CNRS INSU, LATMOS IPSL, Paris, France. [Sawa, Y.; Matsueda, H.] Meteorol Res Inst, Tsukuba, Ibaraki 305, Japan. [Machida, T.] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan. [Frankenberg, C.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Basu, S (reprint author), SRON Netherlands Inst Space Res, Utrecht, Netherlands. EM sourish.basu@noaa.gov RI Butz, Andre/A-7024-2013; Krol, Maarten/E-3414-2013; clerbaux, cathy/I-5478-2013; Frankenberg, Christian/A-2944-2013 OI Butz, Andre/0000-0003-0593-1608; Frankenberg, Christian/0000-0002-0546-5857 FU ESA's Climate Change Initiative on Green House Gases; Emmy-Noether program of the Deutsche Forschungsgemeinschaft [BU2599/1-1]; Gebruikersondersteuning ruimteonderzoek program of the Nederlandse organisatie voor Wetenschappelijk Onderzoek [ALW-GO-AO/08-10]; SARA through NCF [SH-026-12] FX We would like to thank Thijs van Leeuwen for helpful discussions on CO:CO2 emission ratios. RemoTeC algorithm development was partly funded by ESA's Climate Change Initiative on Green House Gases. Andre Butz was supported by the Emmy-Noether program of the Deutsche Forschungsgemeinschaft through grant BU2599/1-1 (RemoteC). Sourish Basu was supported by the Gebruikersondersteuning ruimteonderzoek program of the Nederlandse organisatie voor Wetenschappelijk Onderzoek through project ALW-GO-AO/08-10. Computer resources for model runs were provided by SARA through NCF project SH-026-12. Access to GOSAT data was granted through the second GOSAT research announcement jointly issued by JAXA, NIES, and MOE. GPCP Precipitation data were provided by the NOAA/OAR/ESRL PSD, Boulder, Colorado, USA. The IASI spectra were received through the EUMETCast system, and the IASI CO data were retrieved from http://www.pole-ether.fr. Pierre Coheur and Daniel Hurtmans are acknowledged for developing the FORLI processing code. NR 26 TC 18 Z9 18 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 16 PY 2014 VL 41 IS 5 BP 1809 EP 1815 DI 10.1002/2013GL059105 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AD9IO UT WOS:000333578800064 ER PT J AU Ern, M Ploeger, F Preusse, P Gille, JC Gray, LJ Kalisch, S Mlynczak, MG Russell, JM Riese, M AF Ern, M. Ploeger, F. Preusse, P. Gille, J. C. Gray, L. J. Kalisch, S. Mlynczak, M. G. Russell, J. M., III Riese, M. TI Interaction of gravity waves with the QBO: A satellite perspective SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE quasi-biennial oscillation (QBO); gravity waves; satellite observations; ERA-Interim; momentum budget; atmospheric dynamics ID QUASI-BIENNIAL OSCILLATION; EQUATORIAL KELVIN WAVES; OFFICE UNIFIED MODEL; MOMENTUM FLUX; DRAG PARAMETERIZATION; LOWER THERMOSPHERE; SABER EXPERIMENT; CLIMATE MODELS; LIMB-SOUNDER; PART II AB One of the most important dynamical processes in the tropical stratosphere is the quasi-biennial oscillation (QBO) of the zonal wind. Still, the QBO is not well represented in weather and climate models. To improve the representation of the QBO in the models, a better understanding of the driving of the QBO by atmospheric waves is required. In particular, the contribution of gravity waves is highly uncertain because of the small horizontal scales involved, and there is still no direct estimation based on global observations. We derive gravity wave momentum fluxes from temperature observations of the satellite instruments HIRDLS and SABER. Momentum flux spectra observed show that particularly gravity waves with intrinsic phase speeds <30m/s (vertical wavelengths <10km) interact with the QBO. Gravity wave drag is estimated from vertical gradients of observed momentum fluxes and compared to the missing drag in the tropical momentum budget of ERA-Interim. We find reasonably good agreement between their variations with time and in their approximate magnitudes. Absolute values of observed and ERA-Interim missing drag are about equal during QBO eastward wind shear. During westward wind shear, however, observations are about 2 times lower than ERA-Interim missing drag. This could hint at uncertainties in the advection terms in ERA-Interim. The strong intermittency of gravity waves we find in the tropics might play an important role for the formation of the QBO and may have important implications for the parameterization of gravity waves in global models. Key Points Satellite observations of gravity waves (GWs) show QBO-related variations In the tropics observed GW drag agrees well with the missing drag in ERA-Interim GW observations hint at uncertainties in modeled advection terms C1 [Ern, M.; Ploeger, F.; Preusse, P.; Kalisch, S.; Riese, M.] Forschungszentrum Julich, Inst Energie & Klimaforsch Stratosphare IEK 7, D-52425 Julich, Germany. [Gille, J. C.] Univ Colorado, Ctr Limb Atmospher Sounding, Boulder, CO 80309 USA. [Gille, J. C.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Gray, L. J.] Univ Oxford, Dept Phys, Oxford, England. [Mlynczak, M. G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Russell, J. M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. RP Ern, M (reprint author), Forschungszentrum Julich, Inst Energie & Klimaforsch Stratosphare IEK 7, D-52425 Julich, Germany. EM m.ern@fz-juelich.de RI Riese, Martin/A-3927-2013; Ploeger, Felix/A-1393-2013; Ern, Manfred/I-8839-2016; Preusse, Peter/A-1193-2013; OI Riese, Martin/0000-0001-6398-6493; Ern, Manfred/0000-0002-8565-2125; Preusse, Peter/0000-0002-8997-4965; Ploeger, Felix/0000-0002-3427-6991 NR 72 TC 35 Z9 35 U1 4 U2 26 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 MAR 16 PY 2014 VL 119 IS 5 BP 2329 EP 2355 DI 10.1002/2013JD020731 PG 27 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AE3OL UT WOS:000333885700021 ER PT J AU Cheng, AN Xu, KM AF Cheng, Anning Xu, Kuan-Man TI An explicit representation of vertical momentum transport in a multiscale modeling framework through its 2-D cloud-resolving model component SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE explicit representation of vertical momentum transport; orientation of mesoscale convective system; multiscale modeling framework; precipitation ID ASIAN SUMMER MONSOON; MESOSCALE CONVECTIVE SYSTEMS; 3RD-ORDER TURBULENCE CLOSURES; GENERAL-CIRCULATION MODELS; MADDEN-JULIAN OSCILLATION; CLIMATE SIMULATIONS; RADIATION BUDGET; CUMULUS CLOUDS; PARAMETERIZATION; ORGANIZATION AB In this study, an explicit representation of vertical momentum transport by convective cloud systems, including mesoscale convective systems (MCSs), is proposed and tested in a multiscale modeling framework (MMF). The embedded cloud-resolving model (CRM) provides vertical momentum transport in one horizontal direction. The vertical momentum transport in the other direction is assumed to be proportional to the vertical mass flux diagnosed from the CRM in addition to the effects of entrainment and detrainment. In order to represent both upgradient and downgradient vertical momentum transports, the orientation of the embedded CRM must change with time instead of being stationary typically in MMFs. The orientation is determined by the stratification of the lower troposphere and environmental wind shear. Introducing the variation of the orientations of the embedded CRM is responsible for reducing the stationary anomalous precipitation and many improvements. Improvements are strengthened when the CRM simulated vertical momentum transport is allowed to modify the large-scale circulation simulated by the host general circulation model. These include an improved spatial distribution, amplitude, and intraseasonal variability of the surface precipitation in the tropics, more realistic zonal mean diabatic heating and drying patterns, more reasonable zonal mean large-scale circulations and the East Asian summer monsoon circulation, and an improved, annual mean implied meridional ocean transport in the Southern Hemisphere. Further tests of this convective momentum transport parameterization scheme will be performed with a higher-resolution MMF to further understand its roles in the intraseasonal oscillation and tropical waves, monsoon circulation, and zonal mean large-scale circulations. Key Points An explicit representation of vertical momentum transport by MCS in MMF Orientation of CRM changing with time to facilitate a realistic representation Anomalous precipitation biases reduced and numerous improvements produced C1 [Cheng, Anning] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Cheng, Anning; Xu, Kuan-Man] NASA, Climate Sci Branch, Langley Res Ctr, Hampton, VA USA. RP Cheng, AN (reprint author), Sci Syst & Applicat Inc, Hampton, VA 23666 USA. EM anning.cheng@nasa.gov RI Xu, Kuan-Man/B-7557-2013 OI Xu, Kuan-Man/0000-0001-7851-2629 FU NASA Modeling, Analysis, and Prediction program; DOE Atmospheric System Research Program [DE-SC0005450, DE-SC0008779]; NSF Science and Technology Center for Multiscale Modeling of Atmospheric Processes (CMMAP) [ATM-0425247] FX This work has been supported by NASA Modeling, Analysis, and Prediction program. This work was also partially supported by DOE Atmospheric System Research Program under Interagency agreements DE-SC0005450 and DE-SC0008779 and NSF Science and Technology Center for Multiscale Modeling of Atmospheric Processes (CMMAP), managed by Colorado State University under cooperative agreement ATM-0425247. Parts of the computational resources were provided by Argonne National Laboratory, DOE's Office of Science. NR 65 TC 3 Z9 3 U1 1 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAR 16 PY 2014 VL 119 IS 5 BP 2356 EP 2374 DI 10.1002/2013JD021078 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AE3OL UT WOS:000333885700022 ER PT J AU Rong, PP Russell, JM Randall, CE Bailey, SM Lambert, A AF Rong, P. P. Russell, J. M., III Randall, C. E. Bailey, S. M. Lambert, A. TI Northern PMC brightness zonal variability and its correlation with temperature and water vapor SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE PMCs; zonal variability; temperature; water vapor ID POLAR MESOSPHERIC CLOUDS; PARTICLE-SIZE EXPERIMENT; NITRIC-OXIDE EXPLORER; ICE; INSTRUMENT; CALIBRATION; SATELLITE; AERONOMY; MODEL AB Polar mesospheric clouds (PMCs) measured by the Cloud Imaging and Particle Size instrument on the AIM satellite show strong zonal asymmetries, with prominent planetary-scale variations. The correlations between zonal variations of cloud brightness and temperature or water vapor (H2O) are determined in different stages of the PMC season. Aura Microwave Limb Sounder measured temperature and water vapor are used in the analysis. A zero-dimensional (0-D) PMC model was used to interpret the observation. Analyses of all days of the five northern seasons from 2007 to 2011 indicate that temperature and albedo daily zonal variations are anticorrelated in the season start and end, whereas in the core of the season the correlation is relatively poor. The albedo and H2O correlation in the zonal direction is poor throughout the season. Zero-dimensional model physics indicates that when clouds are weaker, or the environment is warmer and drier, temperature plays an increasingly important role in determining the cloud ice mass variation, which explains the stronger correlation of temperature and albedo at the start and end of the season. Water vapor takes a strong role in determining the ice mass variation in the core of the season when the clouds are stronger and the environment is colder and wetter. However, on a daily basis the H2O depletion associated with the ice production will lead to significant shift of the ice maxima and post-ice H2O maxima in the zonal direction, which leads to the poor correlation between the observed H2O and albedo. Key Points PMC albedo and T zonal variations are anticorrelated in season start and end But in the core of the season albedo and T correlation is relatively poor Cloud albedo and water vapor are poorly correlated owing to vapor depletion C1 [Rong, P. P.; Russell, J. M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. [Randall, C. E.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Bailey, S. M.] Virginia Polytech Inst & State Univ, Bradley Dept Elect & Comp Engn, Blacksburg, VA 24061 USA. [Lambert, A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Rong, PP (reprint author), Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. EM ppr@jhu.edu RI Randall, Cora/L-8760-2014 OI Randall, Cora/0000-0002-4313-4397 FU NASA [NAS5-03132] FX Funding for this work was provided by NASA's Small Explorers Program under the AIM mission contract NAS5-03132. We thank the AIM CIPS team members for making CIPS data available online and providing invaluable advice on data screening and on other key aspects of the CIPS data set. We also appreciate many other AIM team members for their constant support and helpful comments. We thank the Aura MLS retrieval team for making the MLS level 2 data available online along with the most updated read routines. Work at the Jet Propulsion Laboratory, California Institute of Technology, was carried out under a contract with NASA. NR 34 TC 6 Z9 6 U1 0 U2 5 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 MAR 16 PY 2014 VL 119 IS 5 BP 2390 EP 2408 DI 10.1002/2013JD020513 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AE3OL UT WOS:000333885700024 ER PT J AU Ahn, C Torres, O Jethva, H AF Ahn, Changwoo Torres, Omar Jethva, Hiren TI Assessment of OMI near-UV aerosol optical depth over land SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Ozone Monitoring Instrument; UV aerosol remote sensing; aerosol optical depth; AERONET ID OZONE MONITORING INSTRUMENT; SOURCE REGIONS; AIR-QUALITY; SATELLITE; RETRIEVALS; MODIS; MISR; THICKNESS; AERONET; MISSION AB This is the first comprehensive assessment of the aerosol optical depth (AOD) product retrieved from the near-UV observations by the Ozone Monitoring Instrument (OMI) onboard the Aura satellite. The OMI-retrieved AOD by the UV aerosol algorithm (OMAERUV version 1.4.2) was evaluated using collocated Aerosol Robotic Network (AERONET) level 2.0 direct Sun AOD measurements over 8years (2005-2012). A time series analysis of collocated satellite and ground-based AOD observations over 8years shows no discernible drift in OMI's calibration. A rigorous validation analysis over 4years (2005-2008) was carried out at 44 globally distributed AERONET land sites. The chosen locations are representative of major aerosol types such as smoke from biomass burning or wildfires, desert mineral dust, and urban/industrial pollutants. Correlation coefficient () values of 0.75 or better were obtained at 50% of the sites with about 33% of the sites in the analysis reporting regression line slope values larger than 0.70 but always less than unity. The combined AERONET-OMAERUV analysis of the 44 sites yielded a of 0.81, slope of 0.79, y intercept of 0.10, and 65% OMAERUV AOD falling within the expected uncertainty range (largest of 30% or 0.1) at 440nm. The most accurate OMAERUV retrievals are reported over northern Africa locations where the predominant aerosol type is desert dust and cloud presence is less frequent. Reliable retrievals were documented at many sites characterized by urban-type aerosols with low to moderate AOD values, concentrated in the boundary layer. These results confirm that the near-UV observations are sensitive to the entire aerosol column. A simultaneous comparison of OMAERUV, Moderate Resolution Imaging Spectroradiometer (MODIS) Deep Blue, and Multiangle Imaging Spectroradiometer (MISR) AOD retrievals to AERONET measurements was also carried out to evaluate the OMAERUV accuracy in relation to those of the standard aerosol satellite products. The outcome of the comparison indicates that OMAERUV, MODIS Deep Blue, and MISR retrieval accuracies in arid and semiarid environments are statistically comparable. Key Points OMI AOD is comparable with AERONET, MODIS Deep Blue, and MISR AOD values Adequate sensitivity of UV remote sensing to aerosols in the boundary layer C1 [Ahn, Changwoo] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Torres, Omar] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Jethva, Hiren] Univ Space Res Assoc, Columbia, MD USA. RP Ahn, C (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA. EM Changwoo.Ahn@ssaihq.com RI Torres, Omar/G-4929-2013 FU NASA FX We thank the NASA data centers listed in section 2 for providing AOD data from OMI, MODIS, and MISR sensors. We also thank the AERONET principal investigators for their efforts in establishing and maintaining the sites that make it possible to evaluate satellite AOD values in this intercomparison study. Useful comments and suggestions from Lorraine Remer and the two anonymous reviewers to improve the quality of this paper are also acknowledged. This work was performed under contract with NASA. NR 34 TC 21 Z9 21 U1 0 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAR 16 PY 2014 VL 119 IS 5 BP 2457 EP 2473 DI 10.1002/2013JD020188 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AE3OL UT WOS:000333885700028 ER PT J AU Chipperfield, MP Liang, Q Strahan, SE Morgenstern, O Dhomse, SS Abraham, NL Archibald, AT Bekki, S Braesicke, P Di Genova, G Fleming, EL Hardiman, SC Iachetti, D Jackman, CH Kinnison, DE Marchand, M Pitari, G Pyle, JA Rozanov, E Stenke, A Tummon, F AF Chipperfield, M. P. Liang, Q. Strahan, S. E. Morgenstern, O. Dhomse, S. S. Abraham, N. L. Archibald, A. T. Bekki, S. Braesicke, P. Di Genova, G. Fleming, E. L. Hardiman, S. C. Iachetti, D. Jackman, C. H. Kinnison, D. E. Marchand, M. Pitari, G. Pyle, J. A. Rozanov, E. Stenke, A. Tummon, F. TI Multimodel estimates of atmospheric lifetimes of long-lived ozone-depleting substances: Present and future SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE lifetimes; ODS; CFC ID CHEMISTRY-CLIMATE MODELS; STRATOSPHERIC TRANSPORT; LMDZ-REPROBUS; PIPE MODEL; AIR; POTENTIALS; IMPACT; GASES; AGE AB We have diagnosed the lifetimes of long-lived source gases emitted at the surface and removed in the stratosphere using six three-dimensional chemistry-climate models and a two-dimensional model. The models all used the same standard photochemical data. We investigate the effect of different definitions of lifetimes, including running the models with both mixing ratio (MBC) and flux (FBC) boundary conditions. Within the same model, the lifetimes diagnosed by different methods agree very well. Using FBCs versus MBCs leads to a different tracer burden as the implied lifetime contained in the MBC value does not necessarily match a model's own calculated lifetime. In general, there are much larger differences in the lifetimes calculated by different models, the main causes of which are variations in the modeled rates of ascent and horizontal mixing in the tropical midlower stratosphere. The model runs have been used to compute instantaneous and steady state lifetimes. For chlorofluorocarbons (CFCs) their atmospheric distribution was far from steady state in their growth phase through to the 1980s, and the diagnosed instantaneous lifetime is accordingly much longer. Following the cessation of emissions, the resulting decay of CFCs is much closer to steady state. For 2100 conditions the model circulation speeds generally increase, but a thicker ozone layer due to recovery and climate change reduces photolysis rates. These effects compensate so the net impact on modeled lifetimes is small. For future assessments of stratospheric ozone, use of FBCs would allow a consistent balance between rate of CFC removal and model circulation rate. Key Points Modeled lifetimes diagnosed by different methods agree Model-model differences in lifteimes can be explained by transport variations Models suggest ODS lifetimes may not change much in the future C1 [Chipperfield, M. P.; Dhomse, S. S.] Univ Leeds, Sch Earth & Environm, Inst Climate & Atmospher Sci, Leeds, W Yorkshire, England. [Liang, Q.; Strahan, S. E.; Fleming, E. L.; Jackman, C. H.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA. [Liang, Q.; Strahan, S. E.] Univ Space Res Assoc, GESTAR, Columbia, MD USA. [Morgenstern, O.] NIWA, Lauder, New Zealand. [Abraham, N. L.; Archibald, A. T.; Braesicke, P.; Pyle, J. A.] Univ Cambridge, Dept Chem, Cambridge CB2 1EW, England. [Bekki, S.; Marchand, M.] IPSL, Paris, France. [Di Genova, G.; Iachetti, D.; Pitari, G.] Univ Aquila, Dept Phys & Chem Sci, I-67100 Laquila, Italy. [Fleming, E. L.] Sci Syst & Applicat Inc, Lanham, MD USA. [Hardiman, S. C.] Met Off Hadley Ctr, Exeter, Devon, England. [Kinnison, D. E.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Rozanov, E.] World Radiat Ctr, Phys Meteorol Observ, Davos, Switzerland. [Rozanov, E.; Stenke, A.; Tummon, F.] Swiss Fed Inst Technol, Inst Atmospher & Climate Sci, Zurich, Switzerland. RP Chipperfield, MP (reprint author), Univ Leeds, Sch Earth & Environm, Inst Climate & Atmospher Sci, Leeds, W Yorkshire, England. EM M.Chipperfield@leeds.ac.uk RI Liang, Qing/B-1276-2011; Jackman, Charles/D-4699-2012; Chipperfield, Martyn/H-6359-2013; Dhomse, Sandip/C-8198-2011; bekki, slimane/J-7221-2015; Braesicke, Peter/D-8330-2016; Pitari, Giovanni/O-7458-2016; Rozanov, Eugene/A-9857-2012; OI Morgenstern, Olaf/0000-0002-9967-9740; Chipperfield, Martyn/0000-0002-6803-4149; Dhomse, Sandip/0000-0003-3854-5383; bekki, slimane/0000-0002-5538-0800; Braesicke, Peter/0000-0003-1423-0619; Pitari, Giovanni/0000-0001-7051-9578; Rozanov, Eugene/0000-0003-0479-4488; Archibald, Alexander/0000-0001-9302-4180 FU NERC NCAS; MAPLE project [NE/J008621/1]; SNF grant FuMES [200021_138037/1]; NIWA; WCRP; NZ Ministry for the Environment; NASA Headquarters Atmospheric Composition Modeling and Analysis Program FX The UMUKCA modeling work was supported by NERC NCAS and the MAPLE project (NE/J008621/1). The UMUKCA team thanks Paul Telford and Olivier Dessens for help with the model. The SOCOL modeling work was supported by SNF grant FuMES (200021_138037/1). This work has been supported by NIWA as part of its government-funded, core research. OM acknowledges support by WCRP and by the NZ Ministry for the Environment. The GSFC2D modeling work was supported by the NASA Headquarters Atmospheric Composition Modeling and Analysis Program. We thank Charlotte Pascoe and the British Atmospheric Data Centre for archiving our model results. NR 42 TC 18 Z9 18 U1 4 U2 30 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAR 16 PY 2014 VL 119 IS 5 BP 2555 EP 2573 DI 10.1002/2013JD021097 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AE3OL UT WOS:000333885700034 ER PT J AU Segal-Rosenheimer, M Russell, PB Schmid, B Redemann, J Livingston, JM Flynn, CJ Johnson, RR Dunagan, SE Shinozuka, Y Herman, J Cede, A Abuhassan, N Comstock, JM Hubbe, JM Zelenyuk, A Wilson, J AF Segal-Rosenheimer, M. Russell, P. B. Schmid, B. Redemann, J. Livingston, J. M. Flynn, C. J. Johnson, R. R. Dunagan, S. E. Shinozuka, Y. Herman, J. Cede, A. Abuhassan, N. Comstock, J. M. Hubbe, J. M. Zelenyuk, A. Wilson, J. TI Tracking elevated pollution layers with a newly developed hyperspectral Sun/Sky spectrometer (4STAR): Results from the TCAP 2012 and 2013 campaigns SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE air-pollution; Biomass-burning; sunphotometery; hyperspectral; trace-gases ID AIRBORNE SUN PHOTOMETER; COLUMNAR WATER-VAPOR; SOLAR TRANSMITTANCE MEASUREMENTS; SPECTRAL-RESOLUTION LIDAR; ABSORPTION CROSS-SECTION; AEROSOL CLASSIFICATION; AIRCRAFT MEASUREMENTS; UNITED-STATES; SOLVE-II; ACE-ASIA AB Total columnar water vapor (CWV), nitrogen dioxide (NO2), and ozone (O-3) are derived from a newly developed, hyperspectral airborne Sun-sky spectrometer (4STAR) for the first time during the two intensive phases of the Two-Column Aerosol Project (TCAP) in summer 2012 and winter 2013 aboard the DOE G-1 aircraft. We compare results with coincident measurements. We find 0.045g/cm(2) (4.2%) negative bias and 0.28g/cm(2) (26.3%) root-mean-square difference (RMSD) in water vapor layer comparison with an in situ hygrometer and an overall RMSD of 1.28g/m(3) (38%) water vapor amount in profile by profile comparisons, with differences distributed evenly around zero. RMSD for O-3 columns average to 3%, with a 1% negative bias for 4STAR compared with the Ozone Measuring Instrument along aircraft flight tracks for 14 flights during both TCAP phases. Ground-based comparisons with Pandora spectrometers at the Goddard Space Flight Center, Greenbelt, Maryland, showed excellent agreement between the instruments for both O-3 (1% RMSD and 0.1% bias) and NO2 (17.5% RMSD and -8% bias). We apply clustering analysis of the retrieved products as a case study during the TCAP summer campaign to identify variations in atmospheric composition of elevated pollution layers and demonstrate that combined total column measurements of trace gas and aerosols can be used to define different pollution layer sources, by comparing our results with trajectory analysis and in situ airborne miniSPLAT (single-particle mass spectrometer) measurements. Our analysis represents a first step in linking sparse but intense in situ measurements from suborbital campaigns with total column observations from space. C1 [Segal-Rosenheimer, M.; Russell, P. B.; Redemann, J.; Johnson, R. R.; Dunagan, S. E.; Shinozuka, Y.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Segal-Rosenheimer, M.; Shinozuka, Y.] Bay Area Environm Res Inst, Sonoma, CA USA. [Schmid, B.; Flynn, C. J.; Comstock, J. M.; Hubbe, J. M.; Zelenyuk, A.; Wilson, J.] Pacific NW Natl Lab, Richland, WA 99352 USA. [Livingston, J. M.] SRI Int, Menlo Pk, CA 94025 USA. [Herman, J.] Univ Maryland Baltimore Cty, JCET Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. [Herman, J.; Cede, A.; Abuhassan, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Segal-Rosenheimer, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM michal.segalrozenhaimer@nasa.gov OI Herman, Jay/0000-0002-9146-1632 FU DOE ARM Program; Oak Ridge Associated Universities (ORAU) administered NASA Postdoctoral program (NPP); Weizmann Institute of Science in Israel FX TCAP was funded by the DOE ARM Program. We thank the ARM Aerial Facility staff for carrying out the TCAP research flights. We also thank the NASA Langley Research Center HSRL team and B200 flight crew for providing the HSRL measurements and classification products. 4STAR hardware and science algorithm development were funded by the NASA Radiation Science Program. Further maturation of 4STAR was funded by the DOE ARM program as well as the participation of 4STAR in TCAP and subsequent basic analyses. Michal Segal Rozenhaimer would like to thank the Oak Ridge Associated Universities (ORAU) administered NASA Postdoctoral program (NPP) for their financial support and the Weizmann Institute of Science in Israel for their financial support through the Women in Science Fellowship award. NR 49 TC 4 Z9 4 U1 0 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 MAR 16 PY 2014 VL 119 IS 5 BP 2611 EP 2628 DI 10.1002/2013JD020884 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AE3OL UT WOS:000333885700037 ER PT J AU Pitari, G Aquila, V Kravitz, B Robock, A Watanabe, S Cionni, I De Luca, N Di Genova, G Mancini, E Tilmes, S AF Pitari, Giovanni Aquila, Valentina Kravitz, Ben Robock, Alan Watanabe, Shingo Cionni, Irene De Luca, Natalia Di Genova, Glauco Mancini, Eva Tilmes, Simone TI Stratospheric ozone response to sulfate geoengineering: Results from the Geoengineering Model Intercomparison Project (GeoMIP) SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE geoengineering; intercomparison; ozone ID PINATUBO VOLCANIC-ERUPTION; AEROSOL-SIZE DISTRIBUTION; MT-PINATUBO; MOUNT-PINATUBO; ATMOSPHERIC CHEMISTRY; GLOBAL CLIMATOLOGY; SOLAR-RADIATION; II MEASUREMENTS; TROPICAL OZONE; GISS MODELE AB Geoengineering with stratospheric sulfate aerosols has been proposed as a means of temporarily cooling the planet, alleviating some of the side effects of anthropogenic CO2 emissions. However, one of the known side effects of stratospheric injections of sulfate aerosols under present-day conditions is a general decrease in ozone concentrations. Here we present the results from two general circulation models and two coupled chemistry-climate models within the experiments G3 and G4 of the Geoengineering Model Intercomparison Project. On average, the models simulate in G4 an increase in sulfate aerosol surface area density similar to conditions a year after the Mount Pinatubo eruption and a decrease in globally averaged ozone by 1.1-2.1 DU (Dobson unit, 1 DU = 0.001 atm cm) during the central decade of the experiment (2040-2049). Enhanced heterogeneous chemistry on sulfate aerosols leads to an ozone increase in low and middle latitudes, whereas enhanced heterogeneous reactions in polar regions and increased tropical upwelling lead to a reduction of stratospheric ozone. The increase in UV-B radiation at the surface due to ozone depletion is offset by the screening due to the aerosols in the tropics and midlatitudes, while in polar regions the UV-B radiation is increased by 5% on average, with 12% peak increases during springtime. The contribution of ozone changes to the tropopause radiative forcing during 2040-2049 is found to be less than -0.1 W m(-2). After 2050, because of decreasing ClOx concentrations, the suppression of the NOx cycle becomes more important than destruction of ozone by ClOx, causing an increase in total stratospheric ozone. Key Points Different processes affect ozone in stratospheric sulfate aerosol geoengineering Suppression of NOx cycle becomes more important than ClOx depleting cycle Polar UV-B increases by 5% annually and 12% in spring C1 [Pitari, Giovanni; De Luca, Natalia; Di Genova, Glauco; Mancini, Eva] Univ Aquila, Dept Phys & Chem Sci, I-67100 Laquila, Italy. [Pitari, Giovanni] Univ Aquila, Ctr Excellence CETEMPS, I-67100 Laquila, Italy. [Aquila, Valentina] Johns Hopkins Univ, GESTAR, NASA GSFC, Greenbelt, MD USA. [Kravitz, Ben] Pacific NW Natl Lab, Atmospher Sci & Global Change Div, Richland, WA 99352 USA. [Robock, Alan] Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08903 USA. [Watanabe, Shingo] Japan Agcy Marine Earth Sci & Technol, Yokohama, Kanagawa, Japan. [Cionni, Irene] ENEA, Ente Nuove Tecnol Energia & Ambiente, Rome, Italy. [Tilmes, Simone] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. RP Pitari, G (reprint author), Univ Aquila, Dept Phys & Chem Sci, I-67100 Laquila, Italy. EM gianni.pitari@aquila.infn.it RI Aquila, Valentina/D-7267-2012; Kravitz, Ben/P-7925-2014; Robock, Alan/B-6385-2016; Pitari, Giovanni/O-7458-2016; Watanabe, Shingo/L-9689-2014; OI Aquila, Valentina/0000-0003-2060-6694; Kravitz, Ben/0000-0001-6318-1150; Pitari, Giovanni/0000-0001-7051-9578; Watanabe, Shingo/0000-0002-2228-0088; Mancini, Eva/0000-0001-7071-0292 FU Fund for Innovative Climate and Energy Research (FICER); US Department of Energy by Battelle Memorial Institute [DE-AC05-76RL01830]; NASA High-End Computing (HEC) Program through the NASA Center for Climate Simulation (NCCS) at Goddard Space Flight Center; NASA Modeling, Analysis and Prediction (MAP) program [08-MAP-80]; SOUSEI program, MEXT, Japan; NSF [AGS-1157525, CBET-1240507] FX We thank all participants of the Geoengineering Model Intercomparison Project and their model development teams, CLIVAR/WCRP Working Group on Coupled Modeling for endorsing GeoMIP, and the scientists managing the Earth System Grid data nodes who have assisted with making GeoMIP output available. 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 for producing and making available their model output. For CMIP the US 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. Ben Kravitz is supported by the Fund for Innovative Climate and Energy Research (FICER). The Pacific Northwest National Laboratory is operated for the US Department of Energy by Battelle Memorial Institute under contract DE-AC05-76RL01830. Simulations performed by Ben Kravitz and Valentina Aquila were supported by the NASA High-End Computing (HEC) Program through the NASA Center for Climate Simulation (NCCS) at Goddard Space Flight Center. Valentina Aquila is supported by the NASA Modeling, Analysis and Prediction (MAP) program (David Considine, program manager) under the project 08-MAP-80. Shingo Watanabe was supported by the SOUSEI program, MEXT, Japan and the simulations were conducted using the Earth Simulator. Alan Robock was supported by NSF grants AGS-1157525 and CBET-1240507. We acknowledge use of SAGE-II data for stratospheric aerosols. NR 107 TC 35 Z9 36 U1 2 U2 41 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 MAR 16 PY 2014 VL 119 IS 5 BP 2629 EP 2653 DI 10.1002/2013JD020566 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AE3OL UT WOS:000333885700038 ER PT J AU Greenwood, RC Barrat, JA Yamaguchi, A Franchi, IA Scott, ERD Bottke, WF Gibson, JM AF Greenwood, Richard C. Barrat, Jean-Alix Yamaguchi, Akira Franchi, Ian A. Scott, Edward R. D. Bottke, William F. Gibson, Jenny M. TI The oxygen isotope composition of diogenites: Evidence for early global melting on a single, compositionally diverse, HED parent body SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Vesta; HEDs; diogenites; oxygen isotopes; magma oceans ID MAGMA OCEAN CRYSTALLIZATION; IRON-METEORITES; CORE FORMATION; BASALTIC ACHONDRITE; LATE ACCRETION; ORTHO-PYROXENE; 4 VESTA; ELEMENT CHEMISTRY; RAPID TIMESCALES; ASTEROID-4 VESTA AB Oxygen isotope measurements of a suite of 22 diogenites demonstrate that they have a restricted range of Delta O-17 values: -0.246 +/- 0.014 (2 sigma). These results indicate that the diogenites form a single population consistent with a single parent body source, rather than multiple sources as has recently been suggested. Our previously published analysis of eucrites and cumulate eucrites (n = 34) give very similar results to the diogenites, with Delta O-17 = -0.241 +/- 0.016% (2 sigma) and confirm that diogenites and eucrites are from the same parent asteroid. The isotopic homogeneity displayed by diogenites, eucrites and cumulate eucrites, provides strong evidence for an early large-scale melting event on the HED parent body, possibly resulting in the formation of a magma ocean. The paradox, whereby diogenites show isotopic evidence in favor of global melting, but also geochemical features indicative of late stage interaction with eucritic crust, may reflect a rapid transition from global to serial magmatism on their parent body. The fact that all the lithologically varied HED units have an isotopically homogeneous composition supports the proposal that they are derived from a single, large, diverse asteroid, most likely 4 Vesta. The recent suggestion that the HEDs are not from Vesta, but instead represent material from the same asteroidal source as the main-group pallasites and IIIAB irons can be excluded by our oxygen isotope data. (C) 2013 Elsevier B.V. All rights reserved. C1 [Greenwood, Richard C.; Franchi, Ian A.; Gibson, Jenny M.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Barrat, Jean-Alix] UBO IUEM, CNRS UMR Domaines Ocean 6538, F-29280 Plouzane, France. [Yamaguchi, Akira] Natl Inst Polar Res, Tokyo 1908518, Japan. [Scott, Edward R. D.] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Bottke, William F.] Southwest Res Inst, Boulder, CO 80302 USA. [Bottke, William F.] NASA, Lunar Sci Inst, Boulder, CO 80302 USA. RP Greenwood, RC (reprint author), Open Univ, Dept Phys Sci, Walton Hall, Milton Keynes MK7 6AA, Bucks, England. EM r.c.greenwood@open.ac.uk FU Science and Technology Funding Council Consolidated Grant FX This paper was considerably improved as a result of thorough, thought-provoking and detailed reviews by John Wasson, and James Day. We are also grateful for the comments and discussion provided by an anonymous reviewer. Bernard Marty is thanked both for his helpful comments and the very efficient manner in which he dealt with the manuscript. Oxygen isotope studies at the Open University are funded through a Science and Technology Funding Council Consolidated Grant to the Department of Physical Sciences. NR 85 TC 15 Z9 15 U1 4 U2 19 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 MAR 15 PY 2014 VL 390 BP 165 EP 174 DI 10.1016/j.epsl.2013.12.011 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AE4ZU UT WOS:000333998400017 ER PT J AU Tompson, SR AF Tompson, Sara R. TI Sally Ride: America's First Woman in Space SO LIBRARY JOURNAL LA English DT Book Review C1 [Tompson, Sara R.] Jet Prop Lab Lib, Pasadena, CA 91109 USA. RP Tompson, SR (reprint author), Jet Prop Lab Lib, Pasadena, CA 91109 USA. NR 1 TC 0 Z9 0 U1 2 U2 5 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAR 15 PY 2014 VL 139 IS 5 BP 125 EP 125 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA AD0KE UT WOS:000332922100169 ER PT J AU Huang, H Ren, Y Xie, G Yan, Y Yue, Y Ahmed, N Lavery, MPJ Padgett, MJ Dolinar, S Tur, M Willner, AE AF Huang, Hao Ren, Yongxiong Xie, Guodong Yan, Yan Yue, Yang Ahmed, Nisar Lavery, Martin P. J. Padgett, Miles J. Dolinar, Sam Tur, Moshe Willner, Alan E. TI Tunable orbital angular momentum mode filter based on optical geometric transformation SO OPTICS LETTERS LA English DT Article ID LIGHT; SCALE AB We present a tunable mode filter for spatially multiplexed laser beams carrying orbital angular momentum (OAM). The filter comprises an optical geometric transformation-based OAM mode sorter and a spatial light modulator (SLM). The programmable SLM can selectively control the passing/blocking of each input OAM beam. We experimentally demonstrate tunable filtering of one or multiple OAM modes from four multiplexed input OAM modes with vortex charge of l = -9, -4, +4, and +9. The measured output power suppression ratio of the propagated modes to the blocked modes exceeds 14.5 dB. (C) 2014 Optical Society of America C1 [Huang, Hao; Ren, Yongxiong; Xie, Guodong; Yan, Yan; Yue, Yang; Ahmed, Nisar; Willner, Alan E.] Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA. [Lavery, Martin P. J.; Padgett, Miles J.] Univ Glasgow, SUPA, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. [Dolinar, Sam] Jet Prop Lab, Pasadena, CA 91109 USA. [Tur, Moshe] Tel Aviv Univ, Sch Elect Engn, IL-69978 Tel Aviv, Israel. RP Huang, H (reprint author), Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA. EM haoh@usc.edu RI Padgett, Miles/B-7625-2008; Lavery, Martin/H-2265-2015 OI Padgett, Miles/0000-0001-6643-0618; FU DARPA under the Inpho program FX This work is supported by DARPA under the Inpho program. NR 16 TC 5 Z9 6 U1 1 U2 34 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 EI 1539-4794 J9 OPT LETT JI Opt. Lett. PD MAR 15 PY 2014 VL 39 IS 6 BP 1689 EP 1692 DI 10.1364/OL.39.001689 PG 4 WC Optics SC Optics GA AD0SG UT WOS:000332943800089 PM 24690870 ER PT J AU Mishchenko, MI Liu, L Mackowski, DW AF Mishchenko, Michael I. Liu, Li Mackowski, Daniel W. TI Morphology-dependent resonances of spherical droplets with numerous microscopic inclusions SO OPTICS LETTERS LA English DT Article ID LIGHT-SCATTERING; DIELECTRIC SPHERES; SOLAR-RADIATION; BLACK CARBON; MICRODROPLETS; ABSORPTION; PARTICLES AB We use the recently extended superposition T-matrix method to study the behavior of a sharp Lorenz-Mie resonance upon filling a spherical micrometer-sized droplet with tens and hundreds of randomly positioned microscopic inclusions. We show that as the number of inclusions increases, the extinction cross-section peak and the sharp asymmetry-parameter minimum become suppressed, widen, and move toward smaller droplet size parameters, while ratios of diagonal elements of the scattering matrix exhibit sharp angular features indicative of a distinctly nonspherical particle. Our results highlight the limitedness of the concept of an effective refractive index of an inhomogeneous spherical particle. (C) 2014 Optical Society of America C1 [Mishchenko, Michael I.; Liu, Li] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Liu, Li] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA. [Mackowski, Daniel W.] Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA. RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM michael.i.mishchenko@nasa.gov RI Mishchenko, Michael/D-4426-2012; Mackowski, Daniel/K-1917-2013 NR 24 TC 13 Z9 13 U1 0 U2 7 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 EI 1539-4794 J9 OPT LETT JI Opt. Lett. PD MAR 15 PY 2014 VL 39 IS 6 BP 1701 EP 1704 DI 10.1364/OL.39.001701 PG 4 WC Optics SC Optics GA AD0SG UT WOS:000332943800092 PM 24690873 ER PT J AU Latrubesse, EM Wilkinson, MJ Abad, JD AF Latrubesse, Edgardo M. Wilkinson, M. J. Abad, Jorge D. TI Large rivers and megafans SO SEDIMENTARY GEOLOGY LA English DT Editorial Material C1 [Latrubesse, Edgardo M.] Univ Texas Austin, Dept Geog & Environm, Austin, TX 78712 USA. [Wilkinson, M. J.] NASA, Jacobs Technol, Johnson Space Ctr, Houston, TX USA. [Abad, Jorge D.] Univ Pittsburgh, Dept Civil & Environm Engn, Pittsburgh, PA USA. RP Latrubesse, EM (reprint author), Univ Texas Austin, Dept Geog & Environm, Austin, TX 78712 USA. EM latrubesse@austin.utexas.edu NR 6 TC 0 Z9 0 U1 1 U2 4 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 MAR 15 PY 2014 VL 301 BP 91 EP 92 DI 10.1016/j.sedgeo.2014.01.004 PG 2 WC Geology SC Geology GA AB3ED UT WOS:000331673200007 ER PT J AU Karaca, HE Saghaian, SM Tobe, H Acar, E Basaran, B Nagasako, M Kainuma, R Noebe, RD AF Karaca, H. E. Saghaian, S. M. Tobe, H. Acar, E. Basaran, B. Nagasako, M. Kainuma, R. Noebe, R. D. TI Diffusionless phase transformation characteristics of Mn75.7Pt24.3 SO JOURNAL OF ALLOYS AND COMPOUNDS LA English DT Article DE MnPt; Phase transformations; Damping; X-ray diffraction ID SHAPE-MEMORY ALLOYS; MARTENSITIC-TRANSFORMATION; DAMPING CAPACITY; MAGNETIC TRANSFORMATION; SINGLE-CRYSTALS; BEHAVIOR; STRENGTH; TINI; MN3PT AB Phase transformation, damping, and magnetic properties of a Mn75.7Pt24.3 (at.%) alloy were characterized. It was observed that Mn75.7Pt24.3 exhibits a stable phase transformation in the temperature range of 180-200 degrees C with a small temperature hysteresis and maximum transformation strain of similar to 0.5%. The crystal structures and lattice parameters of the transforming phases were determined, where both the high and low temperature phases have a face-centered cubic structure but with different lattice parameters. Finally, it was revealed that the alloy possesses high damping capacity (average Tan Delta of 0.16) during phase transformation. (C) 2013 Elsevier B.V. All rights reserved. C1 [Karaca, H. E.; Saghaian, S. M.; Tobe, H.; Acar, E.; Basaran, B.] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA. [Basaran, B.] Univ Turkish Aeronaut Assoc, Ankara, Turkey. [Nagasako, M.; Kainuma, R.] Tohoku Univ, Grad Sch Engn, Dept Mat Sci, Sendai, Miyagi 980, Japan. [Noebe, R. D.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. RP Karaca, HE (reprint author), Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA. EM karaca@engr.uky.edu RI NAGASAKO, Makoto/D-8898-2015 OI NAGASAKO, Makoto/0000-0001-9010-2200 FU NASA Fundamental Aeronautics Program; Aeronautical Sciences Project; NASA EPSCOR [NNX11AQ31A]; National Science Foundation (NSF) CMMI [0954541] FX This work was supported by the NASA Fundamental Aeronautics Program, Aeronautical Sciences Project and the NASA EPSCOR program under Grant no: NNX11AQ31A and National Science Foundation (NSF) CMMI award #0954541. NR 27 TC 2 Z9 2 U1 1 U2 29 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0925-8388 EI 1873-4669 J9 J ALLOY COMPD JI J. Alloy. Compd. PD MAR 15 PY 2014 VL 589 BP 412 EP 415 DI 10.1016/j.jallcom.2013.11.174 PG 4 WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering GA 296JO UT WOS:000330181400063 ER PT J AU Ma, Q Boulet, C Tipping, RH AF Ma, Q. Boulet, C. Tipping, R. H. TI Two dimensional symmetric correlation functions of the (S)over-cap operator and two dimensional Fourier transforms: Considering the line coupling for P and R lines of linear molecules SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID SPECTRAL-LINES; COLLISIONAL INTERFERENCE; SEMICLASSICAL CALCULATIONS; RELAXATION PARAMETERS; HALF-WIDTHS; LINEWIDTHS; QUANTUM; SHIFTS; GASES; SHAPE AB The refinement of the Robert-Bonamy (RB) formalism by considering the line coupling for isotropic Raman Q lines of linear molecules developed in our previous study [Q. Ma, C. Boulet, and R. H. Tipping, J. Chem. Phys. 139, 034305 (2013)] has been extended to infrared P and R lines. In these calculations, the main task is to derive diagonal and off-diagonal matrix elements of the Liouville operator iS(1) - S-2 introduced in the formalism. When one considers the line coupling for isotropic Raman Q lines where their initial and final rotational quantum numbers are identical, the derivations of off-diagonal elements do not require extra correlation functions of the (S) over cap operator and their Fourier transforms except for those used in deriving diagonal elements. In contrast, the derivations for infrared P and R lines become more difficult because they require a lot of new correlation functions and their Fourier transforms. By introducing two dimensional correlation functions labeled by two tensor ranks and making variable changes to become even functions, the derivations only require the latters' two dimensional Fourier transforms evaluated at two modulation frequencies characterizing the averaged energy gap and the frequency detuning between the two coupled transitions. With the coordinate representation, it is easy to accurately derive these two dimensional correlation functions. Meanwhile, by using the sampling theory one is able to effectively evaluate their two dimensional Fourier transforms. Thus, the obstacles in considering the line coupling for P and R lines have been overcome. Numerical calculations have been carried out for the half-widths of both the isotropic Raman Q lines and the infrared P and R lines of C2H2 broadened by N-2. In comparison with values derived from the RB formalism, new calculated values are significantly reduced and become closer to measurements. (C) 2014 AIP Publishing LLC. C1 [Ma, Q.] Columbia Univ, NASA Goddard Inst Space Studies, New York, NY 10025 USA. [Ma, Q.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA. [Boulet, C.] CNRS, UMR8214, ISMO, F-91405 Orsay, France. [Boulet, C.] Univ Paris 11, F-91405 Orsay, France. [Tipping, R. H.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. RP Ma, Q (reprint author), Columbia Univ, NASA Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. FU NSF [1228861]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231] FX We would like to thank Dr. Thibault for helpful discussions and Professor Bermejo for having provided us experimental data prior to publication. Two of the authors (Q. Ma and R. H. Tipping) acknowledge financial support from NSF under Grant No. 1228861. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. NR 35 TC 4 Z9 4 U1 0 U2 4 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD MAR 14 PY 2014 VL 140 IS 10 AR 104304 DI 10.1063/1.4867417 PG 13 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA AE6RC UT WOS:000334120300022 PM 24628166 ER PT J AU Yang, R Gudipati, MS AF Yang, Rui Gudipati, Murthy S. TI Novel two-step laser ablation and ionization mass spectrometry (2S-LAIMS) of actor-spectator ice layers: Probing chemical composition of D2O ice beneath a H2O ice layer SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID POLYCYCLIC AROMATIC-HYDROCARBONS; WATER ICE; DESORPTION; WAVELENGTH; MALDI; UV; CRYSTALLINE; IRRADIATION; ORGANICS; STRESS AB In this work, we report for the first time successful analysis of organic aromatic analytes imbedded in D2O ices by novel infrared (IR) laser ablation of a layered non-absorbing D2O ice (spectator) containing the analytes and an ablation-active IR-absorbing H2O ice layer (actor) without the analyte. With these studies we have opened up a new method for the in situ analysis of solids containing analytes when covered with an IR laser-absorbing layer that can be resonantly ablated. This soft ejection method takes advantage of the tenability of two-step infrared laser ablation and ultraviolet laser ionization mass spectrometry, previously demonstrated in this lab to study chemical reactions of polycyclic aromatic hydrocarbons (PAHs) in cryogenic ices. The IR laser pulse tuned to resonantly excite only the upper H2O ice layer (actor) generates a shockwave upon impact. This shockwave penetrates the lower analyte-containing D2O ice layer (spectator, a non-absorbing ice that cannot be ablated directly with the wavelength of the IR laser employed) and is reflected back, ejecting the contents of the D2O layer into the vacuum where they are intersected by a UV laser for ionization and detection by a time-of-flight mass spectrometer. Thus, energy is transmitted from the laser-absorbing actor layer into the non-absorbing spectator layer resulting its ablation. We found that isotope cross-contamination between layers was negligible. We also did not see any evidence for thermal or collisional chemistry of PAH molecules with H2O molecules in the shockwave. We call this "shockwave mediated surface resonance enhanced subsurface ablation" technique as "two-step laser ablation and ionization mass spectrometry of actor-spectator ice layers." This method has its roots in the well-established MALDI (matrix assisted laser desorption and ionization) method. Our method offers more flexibility to optimize both the processes-ablation and ionization. This new technique can thus be potentially employed to undertake in situ analysis of materials imbedded in diverse media, such as cryogenic ices, biological samples, tissues, minerals, etc., by covered with an IR-absorbing laser ablation medium and study the chemical composition and reaction pathways of the analyte in its natural surroundings. (C) 2014 AIP Publishing LLC. C1 [Yang, Rui; Gudipati, Murthy S.] CALTECH, Div Sci, Jet Prop Lab, Pasadena, CA 91109 USA. [Yang, Rui] Univ Maryland, College Pk, MD 20742 USA. [Gudipati, Murthy S.] Univ Maryland, IPST, College Pk, MD 20742 USA. RP Gudipati, MS (reprint author), CALTECH, Div Sci, Jet Prop Lab, Mail Stop 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ryang73@ustc.edu; gudipati@jpl.nasa.gov RI Gudipati, Murthy/F-7575-2011 FU JPL's DRDF; JPL; NASA Spitzer Science Center; NASA; National Aeronautics and Space Administration FX This research was enabled through partial funding from JPL's DRDF and R&TD funding for infrastructure of the "Ice Spectroscopy Laboratory" at JPL, NASA Spitzer Science Center, NASA funding through Planetary Atmospheres and Cassini Data Analysis Programs. 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 29 TC 3 Z9 3 U1 3 U2 12 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD MAR 14 PY 2014 VL 140 IS 10 AR 104202 DI 10.1063/1.4867279 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA AE6RC UT WOS:000334120300018 PM 24628162 ER PT J AU Rieffel, EG Wiseman, HM AF Rieffel, Eleanor G. Wiseman, Howard M. TI Discord in relation to resource states for measurement-based quantum computation SO PHYSICAL REVIEW A LA English DT Article AB We consider the issue of what should count as a resource for measurement-based quantum computation (MBQC). While a state that supports universal quantum computation clearly should be considered a resource, universality should not be necessary given the existence of interesting, but less computationally powerful, classes of MBQCs. Here, we propose minimal criteria for a state to be considered a resource state for MBQC. Using these criteria, we explain why discord-free states cannot be resources for MBQC, contrary to recent claims [Hoban et al., arXiv: 1304.2667v1]. Independently of our criteria, we also show that the arguments of Hoban et al., if correct, would imply that Shor's algorithm (for example) can be implemented by measuring discord-free states. C1 [Rieffel, Eleanor G.] NASA, Ames Res Ctr, QuAIL, Moffett Field, CA 94035 USA. [Wiseman, Howard M.] Griffith Univ, Ctr Quantum Computat & Commun Technol, Australian Res Council, Ctr Quantum Dynam, Brisbane, Qld 4111, Australia. RP Rieffel, EG (reprint author), NASA, Ames Res Ctr, QuAIL, Moffett Field, CA 94035 USA. RI Wiseman, Howard/A-7266-2008 OI Wiseman, Howard/0000-0001-6815-854X NR 21 TC 1 Z9 1 U1 0 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD MAR 13 PY 2014 VL 89 IS 3 AR 032323 DI 10.1103/PhysRevA.89.032323 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AD3YT UT WOS:000333183100009 ER PT J AU Schumann, GJP Bates, PD Neal, JC Andreadis, KM AF Schumann, Guy J. -P. Bates, Paul D. Neal, Jeffrey C. Andreadis, Konstantinos M. TI Fight floods on a global scale SO NATURE LA English DT Letter C1 [Schumann, Guy J. -P.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Schumann, GJP (reprint author), NASA, Jet Prop Lab, Pasadena, CA 91109 USA. EM guy.j.schumann@jpl.nasa.gov RI Bates, Paul/C-8026-2012; Neal, Jeffrey/C-8723-2009; Schumann, Guy/F-9760-2011 OI Bates, Paul/0000-0001-9192-9963; Neal, Jeffrey/0000-0001-5793-9594; NR 1 TC 20 Z9 20 U1 2 U2 33 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 MAR 13 PY 2014 VL 507 IS 7491 BP 169 EP 169 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AC6RJ UT WOS:000332651800022 PM 24622194 ER PT J AU Amblard, A Riguccini, L Temi, P Im, S Fanelli, M Serra, P AF Amblard, A. Riguccini, L. Temi, P. Im, S. Fanelli, M. Serra, P. TI STAR FORMATION BIMODALITY IN EARLY-TYPE GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: ISM; infrared: galaxies; infrared: ISM ID ACTIVE GALACTIC NUCLEI; HERSCHEL REFERENCE SURVEY; ELLIPTIC GALAXIES; SAURON PROJECT; SPITZER OBSERVATIONS; MIDINFRARED SELECTION; ATLAS(3D) PROJECT; RED SEQUENCE; S0 GALAXIES; POPULATION SYNTHESIS AB We compute the properties of a sample of 221 local, early-type galaxies with a spectral energy distribution (SED) modeling software, CIGALEMC. Concentrating on the star-forming (SF) activity and dust contents, we derive parameters such as the specific star formation rate (sSFR), the dust luminosity, dust mass, and temperature. In our sample, 52% is composed of elliptical (E) galaxies and 48% of lenticular (SO) galaxies. We find a larger proportion of SO galaxies among galaxies with a large sSFR and large specific dust emission. The stronger activity of SO galaxies is confirmed by larger dust masses. We investigate the relative proportion of active galactic nuclei (AGNs) and SF galaxies in our sample using spectroscopic Sloan Digital Sky Survey data and near-infrared selection techniques, and find a larger proportion of AGN-dominated galaxies in the SO sample than the E one. This could corroborate a scenario where blue galaxies evolve into red ellipticals by passing through an SO AGN active period while quenching its star formation. Finally, we find a good agreement comparing our estimates with color indicators. C1 [Amblard, A.; Riguccini, L.; Temi, P.; Im, S.; Fanelli, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Amblard, A.; Riguccini, L.; Im, S.; Fanelli, M.] BAER Inst, Sonoma, CA USA. [Serra, P.] Univ Paris 11, CNRS, IAS, UMR8617, F-91400 Orsay, France. RP Amblard, A (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RI Serra, Paolo/G-9678-2014; amblard, alexandre/L-7694-2014 OI Serra, Paolo/0000-0002-7609-3931; amblard, alexandre/0000-0002-2212-5395 FU California Institute of Technology under NASA [NAS5-98034] FX This work is based in part on observations made with the NASA Galaxy Evolution Explorer. GALEX is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. NR 98 TC 11 Z9 11 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 MAR 10 PY 2014 VL 783 IS 2 AR 135 DI 10.1088/0004-637X/783/2/135 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5DQ UT WOS:000335439900071 ER PT J AU Barkats, D Aikin, R Bischoff, C Buder, I Kaufman, JP Keating, BG Kovac, JM Su, M Ade, PAR Battle, JO Bierman, EM Bock, JJ Chiang, HC Dowell, CD Duband, L Filippini, J Hivon, EF Holzapfel, WL Hristov, VV Jones, WC Kuo, CL Leitch, EM Mason, PV Matsumura, T Nguyen, HT Ponthieu, N Pryke, C Richter, S Rocha, G Sheehy, C Kernasovskiy, SS Takahashi, YD Tolan, JE Yoon, KW AF Barkats, D. Aikin, R. Bischoff, C. Buder, I. Kaufman, J. P. Keating, B. G. Kovac, J. M. Su, M. Ade, P. A. R. Battle, J. O. Bierman, E. M. Bock, J. J. Chiang, H. C. Dowell, C. D. Duband, L. Filippini, J. Hivon, E. F. Holzapfel, W. L. Hristov, V. V. Jones, W. C. Kuo, C. L. Leitch, E. M. Mason, P. V. Matsumura, T. Nguyen, H. T. Ponthieu, N. Pryke, C. Richter, S. Rocha, G. Sheehy, C. Kernasovskiy, S. S. Takahashi, Y. D. Tolan, J. E. Yoon, K. W. CA BICEP1 Collaboration TI DEGREE-SCALE COSMIC MICROWAVE BACKGROUND POLARIZATION MEASUREMENTS FROM THREE YEARS OF BICEP1 DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; gravitational waves; inflation; polarization ID PROBE WMAP OBSERVATIONS; POWER SPECTRA; GRAVITY-WAVES; EMISSION; TEMPERATURE; MODEL; DUST; QUAD; MAPS; GHZ AB BICEP1 is a millimeter-wavelength telescope designed specifically to measure the inflationary B-mode polarization of the cosmic microwave background at degree angular scales. We present results from an analysis of the data acquired during three seasons of observations at the South Pole (2006-2008). This work extends the two-year result published in Chiang et al., with additional data from the third season and relaxed detector-selection criteria. This analysis also introduces a more comprehensive estimation of band power window functions, improved likelihood estimation methods, and a new technique for deprojecting monopole temperature-to-polarization leakage that reduces this class of systematic uncertainty to a negligible level. We present maps of temperature, E-and B-mode polarization, and their associated angular power spectra. The improvement in the map noise level and polarization spectra error bars are consistent with the 52% increase in integration time relative to Chiang et al. We confirm both self-consistency of the polarization data and consistency with the two-year results. We measure the angular power spectra at 21 <= l <= 335 and find that the EE spectrum is consistent with Lambda cold dark matter cosmology, with the first acoustic peak of the EE spectrum now detected at 15 sigma. The BB spectrum remains consistent with zero. From B-modes only, we constrain the tensor-to-scalar ratio to r = 0.03(+) (0.27)(-0.23), or r < 0.70 at 95% confidence level. C1 [Barkats, D.] ESO, Joint ALMA Observ, Santiago, Chile. [Aikin, R.; Bock, J. J.; Filippini, J.; Hristov, V. V.; Mason, P. V.; Richter, S.; Rocha, G.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [Bischoff, C.; Buder, I.; Kovac, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kaufman, J. P.; Keating, B. G.; Bierman, E. M.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Su, M.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Su, M.] MIT, Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA. [Ade, P. A. R.] Univ Wales Coll Cardiff, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. [Battle, J. O.; Bock, J. J.; Dowell, C. D.; Nguyen, H. T.; Rocha, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chiang, H. C.] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Durban, South Africa. [Duband, L.] CEA Grenoble, SBT, F-38041 Grenoble, France. [Hivon, E. F.] Inst Astrophys, F-75014 Paris, France. [Holzapfel, W. L.; Takahashi, Y. D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Kuo, C. L.; Kernasovskiy, S. S.; Tolan, J. E.; Yoon, K. W.] Stanford Univ, Stanford, CA 94305 USA. [Kuo, C. L.; Kernasovskiy, S. S.; Tolan, J. E.; Yoon, K. W.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Leitch, E. M.; Sheehy, C.] Univ Chicago, Chicago, IL 60637 USA. [Matsumura, T.] KEK, High Energy Accelerator Org, Tsukuba, Ibaraki 3050801, Japan. [Ponthieu, N.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. RP Barkats, D (reprint author), ESO, Joint ALMA Observ, Santiago, Chile. EM dbarkats@alma.cl RI Holzapfel, William/I-4836-2015; OI Barkats, Denis/0000-0002-8971-1954; Hivon, Eric/0000-0003-1880-2733 FU NSF [OPP-0230438]; Caltech President's Fund [PF-471]; NSF CAREER [AST-1255358]; Harvard College Observatory; Alfred P.Sloan Research Fellowship; NSF PECASE [AST-0548262]; Caltech President's Fund; JPL Research and Technology Development Fund FX Bicep1 was supported by NSF grant No. OPP-0230438, Caltech President's Discovery Fund, Caltech President's Fund PF-471, JPL Research and Technology Development Fund, and the late J. Robinson. This analysis was supported in part by NSF CAREER award No. AST-1255358 and the Harvard College Observatory, and J.M.K. acknowledges support from an Alfred P. Sloan Research Fellowship. B.G.K acknowledges support from NSF PECASE Award No. AST-0548262. We thank the South Pole Station staff for helping make our observing seasons a success. We also thank our colleagues in ACBAR, Boomerang, QUAD, BOLOCAM, SPT, WMAP, and Planck for advice and helpful discussions, and Kathy Deniston and Irene Coyle for logistical and administrative support. We thank Patrick Shopbell for computational support at Caltech and the FAS Science Division Research Computing Group at Harvard University for providing support to run all the computations for this paper on the Odyssey cluster. NR 55 TC 24 Z9 24 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2014 VL 783 IS 2 AR 67 DI 10.1088/0004-637X/783/2/67 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5DQ UT WOS:000335439900003 ER PT J AU Beichman, C Gelino, CR Kirkpatrick, JD Cushing, MC Dodson-Robinson, S Marley, MS Morley, CV Wright, EL AF Beichman, C. Gelino, Christopher R. Kirkpatrick, J. Davy Cushing, Michael C. Dodson-Robinson, Sally Marley, Mark S. Morley, Caroline V. Wright, E. L. TI WISE Y DWARFS AS PROBES OF THE BROWN DWARF- EXOPLANET CONNECTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; brown dwarfs; parallaxes; proper motions; solar neighborhood ID EXTRASOLAR GIANT PLANETS; CIRCUMSTELLAR DUST DISKS; ADAPTIVE OPTICS SYSTEM; INITIAL MASS FUNCTION; SURVEY-EXPLORER WISE; SKY SURVEY 2MASS; SPECTRAL TYPE-L; PROPER MOTIONS; T DWARFS; SUBSTELLAR OBJECTS AB We have determined astrometric positions for 15 WISE-discovered late-type brown dwarfs ( six T8-9 and nine Y dwarfs) using the Keck-II telescope, the Spitzer Space Telescope, and the Hubble Space Telescope. Combining data from 8 to 20 epochs we derive parallactic and proper motions for these objects, which puts the majority within 15 pc. For ages greater than a few Gyr, as suggested from kinematic considerations, we find masses of 10-30 M-Jup based on standard models for the evolution of low-mass objects with a range of mass estimates for individual objects, depending on the model in question. Three of the coolest objects have effective temperatures similar to 350 K and inferred masses of 10-15 M-Jup. Our parallactic distances confirm earlier photometric estimates and direct measurements and suggest that the number of objects with masses below about 15MJup must be flat or declining, relative to higher mass objects. The masses of the coldest Y dwarfs may be similar to those inferred for recently imaged planet-mass companions to nearby young stars. Objects in this mass range, which appear to be rare in both the interstellar and protoplanetary environments, may both have formed via gravitational fragmentation-the brown dwarfs in interstellar clouds and companion objects in a protoplanetary disk. In both cases, however, the fact that objects in this mass range are relatively infrequent suggests that this mechanism must be inefficient in both environments. C1 [Beichman, C.; Gelino, Christopher R.; Kirkpatrick, J. Davy] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Beichman, C.] CALTECH, Jet Prop Lab, Pasadena, CA 91107 USA. [Beichman, C.; Gelino, Christopher R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Cushing, Michael C.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Dodson-Robinson, Sally] Univ Delaware, Dept Astron, Newark, DE 19716 USA. [Marley, Mark S.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. [Morley, Caroline V.] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA. [Wright, E. L.] Univ Calif Los Angeles, Dept Astron, Los Angeles, CA 90095 USA. RP Beichman, C (reprint author), CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. EM chas@ipac.caltech.edu RI Marley, Mark/I-4704-2013; OI Marley, Mark/0000-0002-5251-2943 NR 99 TC 22 Z9 22 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 MAR 10 PY 2014 VL 783 IS 2 AR 68 DI 10.1088/0004-637X/783/2/68 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5DQ UT WOS:000335439900004 ER PT J AU Campante, TL Chaplin, WJ Lund, MN Huber, D Hekker, S Garcia, RA Corsaro, E Handberg, R Miglio, A Arentoft, T Basu, S Bedding, TR Christensen-Dalsgaard, J Davies, GR Elsworth, YP Gilliland, RL Karoff, C Kawaler, SD Kjeldsen, H Lundkvist, M Metcalfe, TS Aguirre, VS Stello, D AF Campante, T. L. Chaplin, W. J. Lund, M. N. Huber, D. Hekker, S. Garcia, R. A. Corsaro, E. Handberg, R. Miglio, A. Arentoft, T. Basu, S. Bedding, T. R. Christensen-Dalsgaard, J. Davies, G. R. Elsworth, Y. P. Gilliland, R. L. Karoff, C. Kawaler, S. D. Kjeldsen, H. Lundkvist, M. Metcalfe, T. S. Aguirre, V. Silva Stello, D. TI LIMITS ON SURFACE GRAVITIES OF KEPLER PLANET-CANDIDATE HOST STARS FROM NON-DETECTION OF SOLAR-LIKE OSCILLATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: statistical; planetary systems; stars: late-type; stars: oscillations; techniques: photometric ID SUN-LIKE STAR; RED-GIANT STARS; SCALING RELATIONS; INPUT CATALOG; INITIAL CHARACTERISTICS; FUNDAMENTAL PROPERTIES; HABITABLE ZONE; MAIN-SEQUENCE; CADENCE DATA; ASTEROSEISMOLOGY AB We present a novel method for estimating lower-limit surface gravities (log g) of Kepler targets whose data do not allow the detection of solar-like oscillations. The method is tested using an ensemble of solar-type stars observed in the context of the Kepler Asteroseismic Science Consortium. We then proceed to estimate lower-limit log g for a cohort of Kepler solar-type planet-candidate host stars with no detected oscillations. Limits on fundamental stellar properties, as provided by this work, are likely to be useful in the characterization of the corresponding candidate planetary systems. Furthermore, an important byproduct of the current work is the confirmation that amplitudes of solar-like oscillations are suppressed in stars with increased levels of surface magnetic activity. C1 [Campante, T. L.; Chaplin, W. J.; Handberg, R.; Miglio, A.; Davies, G. R.; Elsworth, Y. P.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Lund, M. N.; Arentoft, T.; Christensen-Dalsgaard, J.; Karoff, C.; Kjeldsen, H.; Lundkvist, M.; Aguirre, V. Silva] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Huber, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Hekker, S.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Garcia, R. A.] Univ Paris Diderot, CNRS, CEA DSM, Lab AIM, F-91191 Gif Sur Yvette, France. [Garcia, R. A.] Ctr Saclay, IRFU SAp, F-91191 Gif Sur Yvette, France. [Corsaro, E.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Corsaro, E.] INAF Astrophys Observ Catania, I-95123 Catania, Italy. [Basu, S.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Bedding, T. R.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Gilliland, R. L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Metcalfe, T. S.] Space Sci Inst, Boulder, CO 80301 USA. RP Campante, TL (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. EM campante@bison.ph.bham.ac.uk OI Bedding, Tim/0000-0001-5222-4661; Bedding, Timothy/0000-0001-5943-1460; Davies, Guy/0000-0002-4290-7351; Metcalfe, Travis/0000-0003-4034-0416; Karoff, Christoffer/0000-0003-2009-7965; Garcia, Rafael/0000-0002-8854-3776; Lund, Mikkel Norup/0000-0001-9214-5642; Lundkvist, Mia Sloth/0000-0002-8661-2571; Handberg, Rasmus/0000-0001-8725-4502 FU NASA's Science Mission Directorate; UK Science and Technology Facilities Council (STFC); European Community's Seventh Framework Programme [FP7/2007-2013, 312844]; Danish National Research Foundation [DNRF106]; ASTERISK project; European Research Council [FP7/2007-2013, 267864, 227224]; Netherlands Organization for Scientific Research (NWO); Fund for Scientific Research of Flanders [G.0728.11]; Belgian federal science policy office [C90291 Gaia-DPAC]; ASK [PIRSESGA- 2010-269194]; NSF [AST-1105930]; NASA [NNX13AE70G, NNX13AE91G] FX Kepler was competitively selected as the tenth Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. The authors wish to thank the entire Kepler team, without whom these results would not be possible. T.L.C., W.J.C., R.H., A.M., G.R.D., and Y.P.E. acknowledge the support of the UK Science and Technology Facilities Council (STFC). The research leading to these results has received funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 312844 (SPACEINN). Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (Grant agreement No.: 267864). D.H. is supported by an appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. S.H. acknowledges financial support from the Netherlands Organization for Scientific Research (NWO). S.H. acknowledges support from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no. 338251 (StellarAges). E.C. acknowledges financial support from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 227224 (PROSPERITY), from the Fund for Scientific Research of Flanders (G.0728.11), from the Belgian federal science policy office (C90291 Gaia-DPAC), and from Project ASK under grant agreement no. PIRSESGA- 2010-269194. S.B. acknowledges support from NSF grant AST-1105930 and NASA grant NNX13AE70G. T.S.M. acknowledges NASA grant NNX13AE91G. NR 75 TC 13 Z9 13 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 MAR 10 PY 2014 VL 783 IS 2 AR 123 DI 10.1088/0004-637X/783/2/123 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5DQ UT WOS:000335439900059 ER PT J AU Kirkpatrick, JD Schneider, A Fajardo-Acosta, S Gelino, CR Mace, GN Wright, EL Logsdon, SE McLean, IS Cushing, MC Skrutskie, MF Eisenhardt, PR Stern, D Balokovic, M Burgasser, AJ Faherty, JK Lansbury, GB Rich, JA Skrzypek, N Fowler, JW Cutri, RM Masci, FJ Conrow, T Grillmair, CJ McCallon, HL Beichman, CA Marsh, KA AF Kirkpatrick, J. Davy Schneider, Adam Fajardo-Acosta, Sergio Gelino, Christopher R. Mace, Gregory N. Wright, Edward L. Logsdon, Sarah E. McLean, Ian S. Cushing, Michael C. Skrutskie, Michael F. Eisenhardt, Peter R. Stern, Daniel Balokovic, Mislav Burgasser, Adam J. Faherty, Jacqueline K. Lansbury, George B. Rich, J. A. Skrzypek, Nathalie Fowler, John W. Cutri, Roc M. Masci, Frank J. Conrow, Tim Grillmair, Carl J. McCallon, Howard L. Beichman, Charles A. Marsh, Kenneth A. TI THE ALLWISE MOTION SURVEY AND THE QUEST FOR COLD SUBDWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; catalogs; solar neighborhood; stars: fundamental parameters; stars: low-mass; subdwarfs ID HIGH PROPER MOTION; INFRARED-SURVEY-EXPLORER; KECK-II TELESCOPE; ALL-SKY SURVEY; BINARY BROWN DWARF; SPECTRAL TYPE-L; SPECTROSCOPIC SURVEY; M-STARS; ECHELLE SPECTROGRAPH; ULTRACOOL SUBDWARFS AB The AllWISE processing pipeline has measured motions for all objects detected on Wide-field Infrared Survey Explorer (WISE) images taken between 2010 January and 2011 February. In this paper, we discuss new capabilities made to the software pipeline in order to make motion measurements possible, and we characterize the resulting data products for use by future researchers. Using a stringent set of selection criteria, we find 22,445 objects that have significant AllWISE motions, of which 3525 have motions that can be independently confirmed from earlier Two Micron All Sky Survey (2MASS) images, yet lack any published motions in SIMBAD. Another 58 sources lack 2MASS counterparts and are presented as motion candidates only. Limited spectroscopic follow-up of this list has already revealed eight new L subdwarfs. These may provide the first hints of a "subdwarf gap" at mid-L types that would indicate the break between the stellar and substellar populations at low metallicities (i.e., old ages). Another object in the motion list-WISEA J154045.67-510139.3-is a bright (J approximate to 9mag) object of type M6; both the spectrophotometric distance and a crude preliminary parallax place it similar to 6 pc from the Sun. We also compare our list of motion objects to the recently published list of 762 WISE motion objects from Luhman. While these first large motion studies with WISE data have been very successful in revealing previously overlooked nearby dwarfs, both studies missed objects that the other found, demonstrating that many other nearby objects likely await discovery in the AllWISE data products. C1 [Kirkpatrick, J. Davy; Fajardo-Acosta, Sergio; Gelino, Christopher R.; Fowler, John W.; Cutri, Roc M.; Masci, Frank J.; Conrow, Tim; Grillmair, Carl J.; McCallon, Howard L.; Beichman, Charles A.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Schneider, Adam; Cushing, Michael C.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Gelino, Christopher R.; Beichman, Charles A.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Mace, Gregory N.; Wright, Edward L.; Logsdon, Sarah E.; McLean, Ian S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Skrutskie, Michael F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Eisenhardt, Peter R.; Stern, Daniel] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Balokovic, Mislav] CALTECH, Pasadena, CA 91125 USA. [Burgasser, Adam J.] Univ Calif San Diego, Dept Phys, San Diego, CA 92093 USA. [Faherty, Jacqueline K.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Lansbury, George B.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Rich, J. A.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Skrzypek, Nathalie] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astro Grp, London SW7 2AZ, England. [Marsh, Kenneth A.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. RP Kirkpatrick, JD (reprint author), CALTECH, Infrared Proc & Anal Ctr, MS 100-22, Pasadena, CA 91125 USA. EM davy@ipac.caltech.edu OI Rich, Jeffrey/0000-0002-5807-5078 FU National Aeronautics and Space Administration (NASA) FX This publication makes use of data products from WISE, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory (JPL)/California Institute of Technology (Caltech), funded by the National Aeronautics and Space Administration (NASA). This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by JPL/Caltech, under contract with NASA. We are indebted to the SIMBAD database and the VizieR catalog access tool, provided by CDS, Strasbourg, France, and we acknowledge use of the Database of Ultracool Parallaxes maintained by Trent Dupuy. We thank our referee, whose critique of the original draft resulted in a clearer, more complete paper. We thank Fiona Harrison, George Djorgovski, Brian Mazur, and Barry Madore for PI-ing telescope time used for spectroscopic follow-up and are grateful for the time allotted by Caltech, NASA/IRTF, and the Carnegie Observatories. We also thank Nicolas Lodieu, John Gizis, and Sebastien Lepine for providing published spectra of subdwarfs. NR 86 TC 33 Z9 33 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 MAR 10 PY 2014 VL 783 IS 2 AR 122 DI 10.1088/0004-637X/783/2/122 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5DQ UT WOS:000335439900058 ER PT J AU Maneva, YG Araneda, JA Marsch, E AF Maneva, Y. G. Araneda, J. A. Marsch, E. TI REGULATION OF ION DRIFTS AND ANISOTROPIES BY PARAMETRICALLY UNSTABLE FINITE-AMPLITUDE ALFVEN-CYCLOTRON WAVES IN THE FAST SOLAR WIND SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; instabilities; plasmas; solar wind; turbulence; waves ID HYBRID SIMULATIONS; ULYSSES OBSERVATIONS; CORONAL HOLES; HEAVY-IONS; HE++ IONS; 1 AU; INSTABILITIES; PLASMA; ACCELERATION; SIGNATURES AB We study the preferential heating and differential acceleration of minor ions by dissipation of ion-acoustic waves (IAWs) generated by parametric instabilities of a finite-amplitude monochromatic Alfven-cyclotron pump wave. We consider the associated kinetic effects of Landau damping and nonlinear pitch-angle scattering of protons and a particles in the tenuous plasma of coronal holes and the fast solar wind. Various data collected by Wind spacecraft show signatures for a local transverse heating of the minor ions, presumably by Alfven-cyclotron wave dissipation, and an unexpected parallel heating by a so far unknown mechanism. Here, we present the results from a set of 1.5 dimensional hybrid simulations in search for a plausible explanation for the observed field-aligned kinetic features in the fast solar wind minor ions. We investigate the origin and regulation of ion relative drifts and temperature anisotropies in low plasma beta, fast solar wind conditions. Depending on their initial drifts, both ion species can heat up not only transversely through cyclotron resonance and non-resonant wave-particle interactions, but also strongly in the parallel direction by Landau damping of the daughter IAWs. We discuss the dependence of the relative ion drifts and temperature anisotropies on the plasma beta of the individual species and we describe the effect of the pump wave amplitude on the ion heating and acceleration. C1 [Maneva, Y. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Maneva, Y. G.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Araneda, J. A.] Univ Concepcion, Dept Fis, Concepcion 4070386, Chile. [Marsch, E.] Univ Kiel, Inst Expt & Appl Phys, D-24118 Kiel, Germany. [Maneva, Y. G.; Marsch, E.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. RP Maneva, YG (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM yana.g.maneva@nasa.gov RI Araneda, Jaime/J-9245-2015 FU International Max Planck Research School (IMPRS) - MPS in Katlenburg-Lindau, Germany; FONDECYT [1110880]; NASA [NNX10AC56G] FX This work was initiated as part of a PhD thesis at the University of Gottingen and funded within the framework of the International Max Planck Research School (IMPRS) by the MPS in Katlenburg-Lindau, Germany. The research was finalized at the University of Concepcion and supported in part by FONDECYT grant No. 1110880. Partial support for this paper came from NASA grant NNX10AC56G. NR 47 TC 7 Z9 7 U1 1 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2014 VL 783 IS 2 AR 139 DI 10.1088/0004-637X/783/2/139 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5DQ UT WOS:000335439900075 ER PT J AU Remijan, AJ Snyder, LE McGuire, BA Kuo, HL Looney, LW Friedel, DN Golubiatnikov, GY Lovas, FJ Ilyushin, VV Alekseev, EA Dyubko, SF McCall, BJ Hollis, JM AF Remijan, Anthony J. Snyder, Lewis E. McGuire, Brett A. Kuo, Hsin-Lun Looney, Leslie W. Friedel, Douglas N. Golubiatnikov, G. Yu Lovas, Frank J. Ilyushin, V. V. Alekseev, E. A. Dyubko, S. F. McCall, Benjamin J. Hollis, Jan M. TI OBSERVATIONAL RESULTS OF A MULTI-TELESCOPE CAMPAIGN IN SEARCH OF INTERSTELLAR UREA [(NH2)(2)CO] SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: clouds; ISM: individual objects (SagISM: ittarius B2(N)); ISM: molecules ID SPECTRAL-LINE SURVEY; SAGITTARIUS B2(N); TENTATIVE IDENTIFICATION; MICROWAVE DETECTION; ETHYL FORMATE; PRIMOS SURVEY; ORION-KL; CHEMISTRY; GLYCINE; TELESCOPE AB In this paper, we present the results of an observational search for gas phase urea [(NH2)(2)CO] observed toward the Sgr B2(N-LMH) region. We show data covering urea transitions from similar to 100 GHz to 250 GHz from five different observational facilities: the Berkeley-Illinois-Maryland-Association (BIMA) Array, the Combined Array for Research in Millimeter-wave Astronomy (CARMA), the NRAO 12 m telescope, the IRAM 30 m telescope, and the Swedish-ESO Submillimeter Telescope (SEST). The results show that the features ascribed to urea can be reproduced across the entire observed bandwidth and all facilities by best-fit column density, temperature, and source size parameters which vary by less than a factor of two between observations merely by adjusting for telescope-specific parameters. Interferometric observations show that the emission arising from these transitions is cospatial and compact, consistent with the derived source sizes and emission from a single species. Despite this evidence, the spectral complexity of both (NH2)(2)CO and of Sgr B2(N) makes the definitive identification of this molecule challenging. We present observational spectra, laboratory data, and models, and discuss our results in the context of a possible molecular detection of urea. C1 [Remijan, Anthony J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Snyder, Lewis E.; Kuo, Hsin-Lun; Looney, Leslie W.; Friedel, Douglas N.] Univ Illinois, Dept Astron, Champaign, IL 61801 USA. [McGuire, Brett A.] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. [Golubiatnikov, G. Yu; Lovas, Frank J.] NIST, Sensor Sci Div, Gaithersburg, MD 20899 USA. [Ilyushin, V. V.; Alekseev, E. A.; Dyubko, S. F.] Inst Radio Astron NASU, UA-61002 Kharkov, Ukraine. [McCall, Benjamin J.] Univ Illinois, Dept Chem, Champaign, IL 61801 USA. [McCall, Benjamin J.] Univ Illinois, Dept Astron, Champaign, IL 61801 USA. [Hollis, Jan M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Remijan, AJ (reprint author), Natl Radio Astron Observ, Edgemont Rd, Charlottesville, VA 22903 USA. OI McGuire, Brett/0000-0003-1254-4817 FU NSF Graduate Research Fellowship; UIUC Critical Research Initiative; Laboratory for Astronomical Imaging at the University of Illinois; NSF [AST 99-81363, AST 02-28953]; states of California, Illinois, and Maryland; James S. McDonnell Foundation; Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris Foundation; University of Chicago; Associates of the California Institute of Technology; National Science Foundation; CARMA partner universities FX We thank the anonymous referee for very helpful comments which improved the quality of this manuscript. B.A.M. gratefully acknowledges G. A. Blake for his support, and funding by an NSF Graduate Research Fellowship. H.-L.K. and B.J.M. gratefully acknowledge funding by a UIUC Critical Research Initiative. We acknowledge support from the Laboratory for Astronomical Imaging at the University of Illinois and NSF AST 99-81363 and AST 02-28953. Support for CARMA construction was derived from the states of California, Illinois, and Maryland, the James S. McDonnell Foundation, the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the University of Chicago, the Associates of the California Institute of Technology, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 49 TC 4 Z9 4 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2014 VL 783 IS 2 AR 77 DI 10.1088/0004-637X/783/2/77 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5DQ UT WOS:000335439900013 ER PT J AU Roser, JE Ricca, A Allamandola, LJ AF Roser, J. E. Ricca, A. Allamandola, L. J. TI ANTHRACENE CLUSTERS AND THE INTERSTELLAR INFRARED EMISSION FEATURES SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; infrared: ISM; ISM: lines and bands; ISM: molecules; molecular data ID POLYCYCLIC AROMATIC-HYDROCARBONS; RED-RECTANGLE; ORION BAR; MU-M; SPECTROSCOPY; SPECTRA; BANDS; FLUORESCENCE; NAPHTHALENE; MOLECULES AB The unidentified infrared bands are ubiquitous in the interstellar medium and typically attributed to emission from neutral and ionized polycyclic aromatic hydrocarbons (or PAHs). The contribution of neutral PAH clusters to these bands has been impossible to determine due to a paucity of infrared spectral data. Here we investigated neutral clusters of the three-ring PAH anthracene using FTIR absorption spectroscopy of anthracene matrix-isolated at varying concentrations in solid argon. In order to determine likely cluster structures of the embedded molecules, we also calculated theoretical absorption spectra for the anthracene monomer through hexamer using density functional theory with a dispersion correction (DFT-D). The DFT-D calculations have been calibrated for the anthracene dimer using the second-order Moller-Plesset approach. Because there is some support for the hypothesis that three or four-ring PAHs are present in the Red Rectangle nebula, we discuss the application of our results to this nebula in particular as well as to the interstellar infrared emission in general. C1 [Roser, J. E.; Allamandola, L. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Roser, J. E.; Ricca, A.] SETI Inst, Mountain View, CA 94043 USA. RP Roser, JE (reprint author), NASA, Ames Res Ctr, Mail Stop 245-6,Bldg N245,Room 148,POB 1, Moffett Field, CA 94035 USA. EM Joseph.E.Roser@nasa.gov FU NASA's Laboratory [NNH09ZDA001N]; SETI Institute; NASA's Astrophysic [NNX09AD18G]; NASA's Laboratory Astrophysics [NNH10ZDA001N] FX Coauthors L. J. Allamandola and J. E. Roser acknowledge support from NASA's Laboratory Astrophysics Program ROSES Grant NNH09ZDA001N. Coauthors J. E. Roser and A. Ricca acknowledge institutional support from the SETI Institute and coauthor A. Ricca acknowledges support from NASA's Astrophysics Theory Program Grant NNX09AD18G. Additional support from NASA's Laboratory Astrophysics "Carbon in the Galaxy" Consortium Grant NNH10ZDA001N is gratefully acknowledged by all three coauthors. The authors thank Partha Bera, Scott Sandford, and Charles Bauschlicher for helpful criticisms of draft versions of this paper. NR 41 TC 4 Z9 4 U1 5 U2 17 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 MAR 10 PY 2014 VL 783 IS 2 AR 97 DI 10.1088/0004-637X/783/2/97 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5DQ UT WOS:000335439900033 ER PT J AU Scholz, P Archibald, RF Kaspi, VM Ng, CY Beardmore, AP Gehrels, N Kennea, JA AF Scholz, P. Archibald, R. F. Kaspi, V. M. Ng, C. -Y. Beardmore, A. P. Gehrels, N. Kennea, J. A. TI ON THE X-RAY VARIABILITY OF MAGNETAR 1RXS J170849.0-400910 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: individual (1RXS J170849.0-400910); stars: neutron; X-rays: general ID SOFT GAMMA REPEATER; NEUTRON-STARS; PULSAR 1E-1048.1-5937; CHANDRA OBSERVATIONS; SWIFT J1822.3-1606; XMM-NEWTON; OUTBURST; EMISSION; GLITCH; FLUX AB We present a long-term X-ray flux and spectral analysis for 1RXS J170849.0-400910 using the Swift/X-Ray Telescope spanning over eight years from 2005 to 2013. We also analyze two observations from Chandra and XMM in the period from 2003 to 2004. In this ten-year period, 1RXS J170849.0-400910 displayed several rotational glitches. Previous studies have claimed variations in the X-ray emission associated with some of the glitches. From our analysis we find no evidence for significant X-ray flux variations and evidence for only low-level spectral variations. We also present an updated timing solution for 1RXS J170849.0-400910, from Rossi X-ray Timing Explorer and Swift observations, which includes a previously unreported glitch at MJD 56019. We discuss the frequency and implications of radiatively quiet glitches in magnetars. C1 [Scholz, P.; Archibald, R. F.; Kaspi, V. M.; Ng, C. -Y.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Ng, C. -Y.] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Beardmore, A. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Kennea, J. A.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Scholz, P (reprint author), McGill Univ, Dept Phys, Rutherford Phys Bldg,3600 Univ St, Montreal, PQ H3A 2T8, Canada. EM pscholz@phsyics.mcgill.ca RI Ng, Chi Yung/A-7639-2013 OI Ng, Chi Yung/0000-0002-5847-2612 FU NSERC; FQRNT; Canadian Institute for Advanced Research FX We are grateful to the Swift team for their flexibility in the scheduling of the timing monitoring campaign of RXS J1708. We thank Marten van Kerkwijk, Andrew Cumming, Dave Tsang, and Kostas Gourgouliatos for helpful discussions. V. M. K. holds the Lorne Trottier Chair in Astrophysics and Cosmology and a Canadian Research Chair in Observational Astrophysics. R. F. A. receives support from a Walter C. Sumner Memorial Fellowship. This work is supported by NSERC via a Discovery Grant and an Accelerator Supplement, by FQRNT via the Centre de Recherche en Astrophysique du Quebec, and by the Canadian Institute for Advanced Research. NR 46 TC 4 Z9 4 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 MAR 10 PY 2014 VL 783 IS 2 AR 99 DI 10.1088/0004-637X/783/2/99 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5DQ UT WOS:000335439900035 ER PT J AU Tsukagoshi, T Momose, M Hashimoto, J Kudo, T Andrews, S Saito, M Kitamura, Y Ohashi, N Wilner, D Kawabe, R Abe, L Akiyama, E Brandner, W Brandt, TD Carson, J Currie, T Egner, SE Goto, M Grady, C Guyon, O Hayano, Y Hayashi, M Hayashi, S Henning, T Hodapp, KW Ishii, M Iye, M Janson, M Kandori, R Knapp, GR Kusakabe, N Kuzuhara, M Kwon, J McElwain, M Matsuo, T Mayama, S Miyama, S Morino, JI Moro-Martin, A Nishimura, T Pyo, TS Serabyn, E Suenaga, T Suto, H Suzuki, R Takahashi, Y Takami, H Takami, M Takato, N Terada, H Thalmann, C Tomono, D Turner, EL Usuda, T Watanabe, M Wisniewski, JP Yamada, T Tamura, M AF Tsukagoshi, Takashi Momose, Munetake Hashimoto, Jun Kudo, Tomoyuki Andrews, Sean Saito, Masao Kitamura, Yoshimi Ohashi, Nagayoshi Wilner, David Kawabe, Ryohei Abe, Lyu Akiyama, Eiji Brandner, Wolfgang Brandt, Timothy D. Carson, Joseph Currie, Thayne Egner, Sebastian E. Goto, Miwa Grady, Carol Guyon, Olivier Hayano, Yutaka Hayashi, Masahiko Hayashi, Saeko Henning, Thomas Hodapp, Klaus W. Ishii, Miki Iye, Masanori Janson, Markus Kandori, Ryo Knapp, Gillian R. Kusakabe, Nobuhiko Kuzuhara, Masayuki Kwon, Jungmi McElwain, Mike Matsuo, Taro Mayama, Satoshi Miyama, Shoken Morino, Jun-Ichi Moro-Martin, Amaya Nishimura, Tetsuro Pyo, Tae-Soo Serabyn, Eugene Suenaga, Takuya Suto, Hiroshi Suzuki, Ryuji Takahashi, Yasuhiro Takami, Hideki Takami, Michihiro Takato, Naruhisa Terada, Hiroshi Thalmann, Christian Tomono, Daigo Turner, Edwin L. Usuda, Tomonori Watanabe, Makoto Wisniewski, John P. Yamada, Toru Tamura, Motohide TI HIGH- RESOLUTION SUBMILLIMETER AND NEAR-INFRARED STUDIES OF THE TRANSITION DISK AROUND Sz 91 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; protoplanetary disks; stars:individual (Sz 91); stars:pre-main sequence ID T-TAURI STARS; CIRCUMSTELLAR DUST DISKS; MAIN-SEQUENCE STARS; PROTOPLANETARY-DISK; PLANET FORMATION; MILLIMETER EMISSION; UPPER SCORPIUS; MOLECULAR GAS; RHO-OPHIUCHI; LKCA 15 AB To reveal the structures of a transition disk around a young stellar object in Lupus, Sz 91, we have performed aperture synthesis 345 GHz continuum and CO(3-2) observations with the Submillimeter Array (similar to 1"-3" resolution) and high-resolution imaging of polarized intensity at the K-s-band using the HiCIAO instrument on the Subaru Telescope (0".25 resolution). Our observations successfully resolved the inner and outer radii of the dust disk to be 65 and 170 AU, respectively, which indicates that Sz 91 is a transition disk source with one of the largest known inner holes. The model fitting analysis of the spectral energy distribution reveals an H-2 mass of 2.4 Chi 10(-3) M-circle dot in the cold (T < 30 K) outer part at 65 AU < r < 170 AU by assuming a canonical gas-to-dust mass ratio of 100, although a small amount (> 3 Chi 10(-9)M(circle dot)) of hot (T similar to 180 K) dust possibly remains inside the inner hole of the disk. The structure of the hot component could be interpreted as either an unresolved self-luminous companion body (not directly detected in our observations) or a narrow ring inside the inner hole. Significant CO(3-2) emission with a velocity gradient along the major axis of the dust disk is concentrated on the Sz 91 position, suggesting a rotating gas disk with a radius of 420 AU. The Sz 91 disk is possibly a rare disk in an evolutionary stage immediately after the formation of protoplanets because of the large inner hole and the lower disk mass than other transition disks studied thus far. C1 [Tsukagoshi, Takashi; Momose, Munetake] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan. [Kudo, Tomoyuki; Saito, Masao; Ohashi, Nagayoshi; Kawabe, Ryohei; Akiyama, Eiji; Hayashi, Masahiko; Ishii, Miki; Iye, Masanori; Kandori, Ryo; Kusakabe, Nobuhiko; Kuzuhara, Masayuki; Morino, Jun-Ichi; Suto, Hiroshi; Suzuki, Ryuji; Takami, Hideki; Takami, Michihiro] Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. [Kitamura, Yoshimi] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Andrews, Sean; Wilner, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hashimoto, Jun] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Takahashi, Yasuhiro; Tamura, Motohide] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lboratoire Lagrange UMR 7293, F-06108 Nice 2, France. [Abe, Lyu] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Brandner, Wolfgang; Henning, Thomas; Janson, Markus; Knapp, Gillian R.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Brandt, Timothy D.; Turner, Edwin L.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA. [Carson, Joseph] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Egner, Sebastian E.; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko; Nishimura, Tetsuro; Pyo, Tae-Soo; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daigo; Usuda, Tomonori] Subaru Telescope, Hilo, HI 96720 USA. [Goto, Miwa] Univ Munich, Univ Sternwarte, D-81679 Munich, Germany. [Grady, Carol] Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Hodapp, Klaus W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [Kuzuhara, Masayuki] Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan. [McElwain, Mike] Grad Univ Adv Studies SOKENDAI, Hayama, Kanagawa 2400193, Japan. [Matsuo, Taro] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Miyama, Shoken] Hiroshima Univ, Higashihiroshima, Hiroshima 7398511, Japan. [Moro-Martin, Amaya] CSIC, CAB, INTA, Dept Astrophys, E-28850 Madrid, Spain. [Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Takami, Michihiro] Univ Tokyo, Sch Sci, Tokyo 1130033, Japan. [Thalmann, Christian] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Watanabe, Makoto] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Wisniewski, John P.] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan. [Yamada, Toru] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Kwon, Jungmi; Mayama, Satoshi; Suenaga, Takuya] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. RP Tsukagoshi, T (reprint author), Ibaraki Univ, Coll Sci, Bunkyo 2-1-1, Mito, Ibaraki 3108512, Japan. EM ttsuka@mx.ibaraki.ac.jp RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016 OI Watanabe, Makoto/0000-0002-3656-4081 FU MEXT; JSPS KAKENHI [24103504, 23103004]; NSF [T-1009203]; Academia Sinica Institute of Astronomy and Astrophysics; Smithsonian Institution; Academia Sinica FX We are grateful for the ASTE and AzTEC staff for the operation and maintenance of the observation instruments. A part of this work was conducted as the Observatory Project of "SEEDS: Strategic Explorations of Exoplanets and Disks with Subaru" supported by the MEXT Grant-in-Aid for Scientific Research on Priority Areas. This work is partially supported by JSPS KAKENHI grant numbers 24103504 (T.T.) and 23103004 (M.M.). J.C. gratefully acknowledges support from NSF grant AST-1009203. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. NR 65 TC 14 Z9 14 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 MAR 10 PY 2014 VL 783 IS 2 AR 90 DI 10.1088/0004-637X/783/2/90 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5DQ UT WOS:000335439900026 ER PT J AU Woillez, J Wizinowich, P Akeson, R Colavita, M Eisner, J Millan-Gabet, R Monnier, JD Pott, JU Ragland, S AF Woillez, J. Wizinowich, P. Akeson, R. Colavita, M. Eisner, J. Millan-Gabet, R. Monnier, J. D. Pott, J. -U. Ragland, S. TI FIRST FAINT DUAL-FIELD OFF-AXIS OBSERVATIONS IN OPTICAL LONG BASELINE INTERFEROMETRY SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation: high angular resolution; instrumentation: interferometers ID PALOMAR TESTBED INTERFEROMETER; KECK INTERFEROMETER; ADAPTIVE OPTICS; NARROW-ANGLE; ASTROMETRY; IMAGES AB Ground-based long baseline interferometers have long been limited in sensitivity in part by the short integration periods imposed by atmospheric turbulence. The first observation fainter than this limit was performed on 2011 January 22 when the Keck Interferometer observed a K = 11.5 target, about 1 mag fainter than its K = 10.3 atmospherically imposed limit; the currently demonstrated limit is K = 12.5. These observations were made possible by the Dual-Field Phase-Referencing (DFPR) instrument, part of the NSF-funded ASTrometry and phase-Referenced Astronomy project; integration times longer than the turbulence time scale are made possible by its ability to simultaneously measure the real-time effects of the atmosphere on a nearby bright guide star and correct for it on the faint target. We present the implementation of DFPR on the Keck Interferometer. Then, we detail its on-sky performance focusing on the accuracy of the turbulence correction and the resulting fringe contrast stability. C1 [Woillez, J.; Wizinowich, P.; Ragland, S.] WM Keck Observ, Kamuela, HI 96743 USA. [Woillez, J.] European So Observ, D-85748 Garching, Germany. [Akeson, R.; Millan-Gabet, R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Colavita, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Eisner, J.] Univ Arizona, Tucson, AZ 85721 USA. [Monnier, J. D.] Univ Michigan, Ann Arbor, MI 48109 USA. [Pott, J. -U.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Woillez, J (reprint author), WM Keck Observ, Kamuela, HI 96743 USA. FU National Science Foundation Major Research Instrumentation [AST- 0619965]; National Aeronautics and Space Administration FX The ASTRA project was supported by the National Science Foundation Major Research Instrumentation grant AST-0619965. The Keck Interferometer was funded by the National Aeronautics and Space Administration as part of its Exoplanet Exploration program. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 29 TC 2 Z9 2 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2014 VL 783 IS 2 DI 10.1088/0004-637X/783/2/104 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5DQ UT WOS:000335439900040 ER PT J AU Jin, B Lim, T Ju, S Latypov, MI Pi, DH Kim, HS Meyyappan, M Lee, JS AF Jin, Bo Lim, Taekyung Ju, Sanghyun Latypov, Marat I. Pi, Dong-Hai Kim, Hyoung Seop Meyyappan, M. Lee, Jeong-Soo TI Investigation of thermal resistance and power consumption in Ga-doped indium oxide (In2O3) nanowire phase change random access memory SO APPLIED PHYSICS LETTERS LA English DT Article ID NONVOLATILE AB The resistance stability and thermal resistance of phase change memory devices using similar to 40 nm diameter Ga-doped In2O3 nanowires (Ga:In2O3 NW) with different Ga-doping concentrations have been investigated. The estimated resistance stability (R(t)/R-0 ratio) improves with higher Ga concentration and is dependent on annealing temperature. The extracted thermal resistance (R-th) increases with higher Ga-concentration and thus the power consumption can be reduced by similar to 90% for the 11.5% Ga: In2O3 NW, compared to the 2.1% Ga: In2O3 NW. The excellent characteristics of Ga-doped In2O3 nanowire devices offer an avenue to develop low power and reliable phase change random access memory applications. (C) 2014 AIP Publishing LLC. C1 [Jin, Bo; Lee, Jeong-Soo] Pohang Univ Sci & Technol POSTECH, Div IT Convergence Engn, Pohang 790784, South Korea. [Lim, Taekyung; Ju, Sanghyun] Kyonggi Univ, Dept Phys, Suwon 443760, Gyeonggi Do, South Korea. [Latypov, Marat I.; Pi, Dong-Hai; Kim, Hyoung Seop] Pohang Univ Sci & Technol POSTECH, Dept Mat Sci & Engn, Pohang 790784, South Korea. [Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Meyyappan, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM m.meyyappan@nasa.gov; ljs6951@postech.ac.kr RI Kim, Hyoung Seop/C-2166-2009; OI Kim, Hyoung Seop/0000-0002-3155-583X; Latypov, Marat/0000-0003-4416-0877 FU National Research Foundation (NRF) [2012R1A2A2A02010432]; Basic Science Research Program through the Ministry of Science, ICT and Future Planning, Korea [2011-0023219]; Center for Advanced Soft Electronics under the Global Frontier Research Program of the Ministry of Education, Science and Technology, Korea [2011-0031638] FX This research was supported by National Research Foundation (NRF) (No. 2012R1A2A2A02010432); by the Basic Science Research Program (2011-0023219) through the Ministry of Science, ICT and Future Planning, Korea; and a grant (Code No. 2011-0031638) from the Center for Advanced Soft Electronics under the Global Frontier Research Program of the Ministry of Education, Science and Technology, Korea. NR 18 TC 2 Z9 2 U1 0 U2 29 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD MAR 10 PY 2014 VL 104 IS 10 AR 103510 DI 10.1063/1.4868537 PG 4 WC Physics, Applied SC Physics GA AD2RM UT WOS:000333082800084 ER PT J AU Marchis, F Durech, J Castillo-Rogez, J Vachier, F Cuk, M Berthier, J Wong, MH Kalas, P Duchene, G van Dam, MA Hamanowa, H Viikinkoski, M AF Marchis, F. Durech, J. Castillo-Rogez, J. Vachier, F. Cuk, M. Berthier, J. Wong, M. H. Kalas, P. Duchene, G. van Dam, M. A. Hamanowa, H. Viikinkoski, M. TI THE PUZZLING MUTUAL ORBIT OF THE BINARY TROJAN ASTEROID (624) HEKTOR SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE instrumentation: adaptive optics; minor planets, asteroids: general; minor planets, asteroids: individual (624 Hektor); planets and satellites: detection; planets and satellites: dynamical evolution and stability ID SPITZER-SPACE-TELESCOPE; MINOR PLANETS; SPECTROSCOPY; DYNAMICS; CAPTURE; DENSITY AB Asteroids with satellites are natural laboratories to constrain the formation and evolution of our solar system. The binary Trojan asteroid (624) Hektor is the only known Trojan asteroid to possess a small satellite. Based on W. M. Keck adaptive optics observations, we found a unique and stable orbital solution, which is uncommon in comparison to the orbits of other large multiple asteroid systems studied so far. From lightcurve observations recorded since 1957, we showed that because the large Req = 125 km primary may be made of two joint lobes, the moon could be ejecta of the low-velocity encounter, which formed the system. The inferred density of Hektor's system is comparable to the L5 Trojan doublet (617) Patroclus but due to their difference in physical properties and in reflectance spectra, both captured Trojan asteroids could have a different composition and origin. C1 [Marchis, F.; Cuk, M.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Marchis, F.; Vachier, F.; Berthier, J.] IMCCE Obs Paris, F-75014 Paris, France. [Durech, J.] Charles Univ Prague, Fac Math & Phys, Astron Inst, Prague, Czech Republic. [Castillo-Rogez, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wong, M. H.; Kalas, P.; Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Duchene, G.] Inst Planetol & Astrophys Grenoble, F-38041 Grenoble, France. [van Dam, M. A.] Flat Wavefronts, Christchurch 8140, New Zealand. [Hamanowa, H.] Hamanowa Observ, Motomiya, Fukushima 9691204, Japan. [Viikinkoski, M.] Tampere Univ Technol, FI-33101 Tampere, Finland. RP Marchis, F (reprint author), SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. EM fmarchis@seti.org RI Durech, Josef/C-5634-2017; OI Durech, Josef/0000-0003-4914-3646; Viikinkoski, Matti/0000-0001-8601-9164 FU NASA grant [NNX11AD62G]; Czech Science Foundation [P209/10/0537]; NASA OPR grant [NNX11AM48G] FX F.M. acknowledges the support of NASA grant NNX11AD62G. These data were obtained with the W. M. Keck Observatory, which is operated by the California Institute of Technology, the University of California, Berkeley, and the National Aeronautics and Space Administration. The work of J.D. was supported by grant P209/10/0537 of the Czech Science Foundation. We would like to thank A. W. Harris for his constructive and useful comments, which significantly improved this manuscript. We thank Helene Marchis for drawing Figures 3(D) and (E). M. Cuk's work was supported by NASA OPR grant NNX11AM48G. NR 33 TC 12 Z9 12 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 10 PY 2014 VL 783 IS 2 AR L37 DI 10.1088/2041-8205/783/2/L37 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC4UJ UT WOS:000332516300013 ER PT J AU Podio, L Kamp, I Codella, C Nisini, B Aresu, G Brittain, S Cabrit, S Dougados, C Grady, C Meijerink, R Sandell, G Spaans, M Thi, WF White, GJ Woitke, P AF Podio, L. Kamp, I. Codella, C. Nisini, B. Aresu, G. Brittain, S. Cabrit, S. Dougados, C. Grady, C. Meijerink, R. Sandell, G. Spaans, M. Thi, W. -F. White, G. J. Woitke, P. TI PROBING THE GASEOUS DISK OF T Tau N WITH CN 5-4 LINES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: molecules; protoplanetary disks; stars: individual (T Tau) ID HERBIG-AE STARS; PROTOPLANETARY DISKS; IMAGING SURVEY; BINARY-SYSTEM; DUST DISK; EMISSION; SUBMILLIMETER; CHEMISTRY; EVOLUTION; GAS AB We present spectrally resolved observations of the young multiple system T Tau in atomic and molecular lines obtained with the Heterodyne Instrument for the Far Infrared on board Herschel. While CO, H2O, [C II], and SO lines trace the envelope and the outflowing gas up to velocities of 33 km s(-1) with respect to systemic, the CN 5-4 hyperfine structure lines at 566.7, 566.9 GHz show a narrow double-peaked profile centered at systemic velocity, consistent with an origin in the outer region of the compact disk of T Tau N. Disk modeling of the T Tau N disk with the thermo-chemical code ProDiMo produces CN line fluxes and profiles consistent with the observed ones and constrain the size of the gaseous disk (R-out = 110(-20)(+10) AU) and its inclination (i = 25 degrees +/- 5 degrees). The model indicates that the CN lines originate in a disk upper layer at 40-110 AU from the star, which is irradiated by the stellar UV field and heated up to temperatures of 50-700 K. With respect to previously observed CN 2-1 millimeter lines, the CN 5-4 lines appear to be less affected by envelope emission, due to their larger critical density and excitation temperature. Hence, high-J CN lines are a unique confusion-free tracer of embedded disks, such as the disk of T Tau N. C1 [Podio, L.; Codella, C.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Podio, L.; Cabrit, S.; Dougados, C.; Thi, W. -F.] UJF Grenoble 1, CNRS INSU, IPAG, UMR 5274, F-38041 Grenoble, France. [Kamp, I.; Meijerink, R.; Spaans, M.] Univ Groningen, Kapteyn Astron Inst, NL-9747 AD Groningen, Netherlands. [Nisini, B.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Aresu, G.] INAF Osservatorio Astron Cagliari, I-09047 Selargius, Italy. [Brittain, S.] Clemson Univ, Dept Phys & Astron, Kinard Lab 118, Clemson, SC 29634 USA. [Cabrit, S.] UMR 8112 CNRS INSU, Observ Paris, LERMA, F-75014 Paris, France. [Dougados, C.] Univ Chile, CNRS, UMI 3386, LFCA, Santiago, Chile. [Dougados, C.] Univ Chile, Dept Astron, Santiago, Chile. [Grady, C.] Eureka Sci, Oakland, CA 96002 USA. [Grady, C.] NASA, Exoplanets & Stellar Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Meijerink, R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Sandell, G.] NASA, SOFIA USRA, Ames Res Ctr, Moffett Field, CA 94035 USA. [White, G. J.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [White, G. J.] Rutherford Appleton Lab, RALSpace, Chilton OX11 0QX, England. [Woitke, P.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. RP Podio, L (reprint author), INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy. OI Meijerink, Rowin/0000-0001-7584-9293; Codella, Claudio/0000-0003-1514-3074; , Brunella Nisini/0000-0002-9190-0113 FU European FP7 [PIEF-GA-2009-253896]; National Science Foundation [AST-0954811] FX L.P. and S.D.B. acknowledge funding from the European FP7 (PIEF-GA-2009-253896) and the National Science Foundation (AST-0954811). NR 44 TC 1 Z9 1 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 MAR 10 PY 2014 VL 783 IS 2 AR L26 DI 10.1088/2041-8205/783/2/L26 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC4UJ UT WOS:000332516300002 ER PT J AU Schilling, G Howell, S AF Schilling, Govert Howell, Steve TI Down but not out SO NEW SCIENTIST LA English DT Editorial Material C1 [Howell, Steve] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION LTD PI SUTTON PA QUADRANT HOUSE THE QUADRANT, SUTTON SM2 5AS, SURREY, ENGLAND SN 0262-4079 J9 NEW SCI JI New Sci. PD MAR 8 PY 2014 VL 221 IS 2959 BP 25 EP 25 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AC8AO UT WOS:000332755600019 ER PT J AU Callahan, MP Martin, MG Burton, AS Glavin, DP Dworkin, JP AF Callahan, Michael P. Martin, Mildred G. Burton, Aaron S. Glavin, Daniel P. Dworkin, Jason P. TI Amino acid analysis in micrograms of meteorite sample by nanoliquid chromatography-high-resolution mass spectrometry SO JOURNAL OF CHROMATOGRAPHY A LA English DT Article DE Amino Acids; astrobiology; high-resolution mass spectrometry; Murchison meteorite; nanoliquid Chromatography; orbitrap ID INTERPLANETARY DUST PARTICLES; CARBONACEOUS ANTARCTIC MICROMETEORITES; LIQUID-CHROMATOGRAPHY; MURCHISON METEORITE; AROMATIC-HYDROCARBONS; ORGANIC-COMPOUNDS; ACCRETION RATE; EARLY EARTH; ELECTROSPRAY; NUCLEOBASES AB Amino acids and their enantiomers in a 360 microgram sample of Murchison meteorite were unambiguously identified and quantified using chemical derivatization and nanoliquid chromatography coupled to nanoelectrospray ionization high resolution orbitrap mass spectrometry techniques. The distribution and abundance of amino acids were similar to past studies of Murchison meteorite but the samples used here were three orders of magnitude lower. The analytical method was also highly sensitive, and some amino acid reference standards were successfully detected at a level of similar to 200 attomoles (on column). These results may open up the possibility for investigating other less studied, sample-limited extraterrestrial samples (e.g., micrometeorites, interplanetary dust particles, and cometary particles) for biologically-relevant organic molecules Published by Elsevier B.V. C1 [Callahan, Michael P.; Glavin, Daniel P.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Martin, Mildred G.] Catholic Univ Amer, Washington, DC 20064 USA. [Burton, Aaron S.] NASA, Goddard Space Flight Ctr, Postdoctoral Program, Greenbelt, MD 20771 USA. RP Callahan, MP (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. EM michael.p.callahan@nasa.gov RI Burton, Aaron/H-2212-2011; Glavin, Daniel/D-6194-2012; Dworkin, Jason/C-9417-2012 OI Burton, Aaron/0000-0002-7137-1605; Glavin, Daniel/0000-0001-7779-7765; Dworkin, Jason/0000-0002-3961-8997 FU NASA Astrobiology Institute; Goddard Center for Astrobiology; NASA Cosmo-chemistry Program; NASA Postdoctoral Program FX The authors thank L. Welzenbach and T. McCoy (Smithsonian National Museum of Natural History, Washington, D.C.) for providing the Murchison meteorite sample. M.P.C., D.P.G., and J.P.D. acknowledge funding support from the NASA Astrobiology Institute and The Goddard Center for Astrobiology and the NASA Cosmo-chemistry Program. A.S.B. acknowledges support from the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. We thank K. Smith (Penn State University) as well as anonymous reviewers for valuable input regarding the writing of this manuscript. NR 35 TC 4 Z9 4 U1 4 U2 42 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0021-9673 EI 1873-3778 J9 J CHROMATOGR A JI J. Chromatogr. A PD MAR 7 PY 2014 VL 1332 BP 30 EP 34 DI 10.1016/j.chroma.2014.01.032 PG 5 WC Biochemical Research Methods; Chemistry, Analytical SC Biochemistry & Molecular Biology; Chemistry GA AC3NW UT WOS:000332429500005 PM 24529954 ER PT J AU Walsh, BM Foster, JC Erickson, PJ Sibeck, DG AF Walsh, B. M. Foster, J. C. Erickson, P. J. Sibeck, D. G. TI Simultaneous Ground- and Space-Based Observations of the Plasmaspheric Plume and Reconnection SO SCIENCE LA English DT Article ID EARTHS MAGNETOPAUSE; PATCHES AB Magnetic reconnection is the primary process through which energy couples from the solar wind into Earth's magnetosphere and ionosphere. Conditions both in the incident solar wind and in the magnetosphere are important in determining the efficiency of this energy transfer. In particular, the cold, dense plasmaspheric plume can substantially impact the coupling in the dayside reconnection region. Using ground-based total electron content (TEC) maps and measurements from the THEMIS spacecraft, we investigated simultaneous ionosphere and magnetosphere observations of the plasmaspheric plume and its involvement in an unsteady magnetic reconnection process. The observations show the full circulation pattern of the plasmaspheric plume and validate the connection between signatures of variability in the dense plume and reconnection at the magnetopause as measured in situ and through TEC measurements in the ionosphere. C1 [Walsh, B. M.; Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Walsh, B. M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Foster, J. C.; Erickson, P. J.] MIT, Haystack Observ, Westford, MA 01886 USA. RP Walsh, BM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM brian.walsh@nasa.gov RI Walsh, Brian/C-4899-2016 OI Walsh, Brian/0000-0001-7426-5413 FU NSF [AGS-1136827, AGS-1242204]; NASA [NAS5-02099] FX Supported by NSF grant AGS-1136827. We acknowledge NASA contract NAS5-02099 and instrument teams for use of the data from the THEMIS Mission, specifically the ESA, EFI, and FGM teams. Work at MIT Haystack Observatory was supported by NSF Cooperative Agreement AGS-1242204. NR 21 TC 30 Z9 30 U1 2 U2 12 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 MAR 7 PY 2014 VL 343 IS 6175 BP 1122 EP 1125 DI 10.1126/science.1247212 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AC2LB UT WOS:000332331500044 PM 24604196 ER PT J AU Osterbacka, R Han, JW AF Osterbacka, Ronald Han, Jin-Woo TI Nanotechnology in paper electronics SO NANOTECHNOLOGY LA English DT Editorial Material C1 [Osterbacka, Ronald] Abo Akad Univ, Dept Phys, FIN-20500 Turku, Finland. [Han, Jin-Woo] NASA, Ames Res Ctr, Ctr Nanotechnol, Dept Phys & Astron, Moffett Field, CA 94035 USA. RP Osterbacka, R (reprint author), Abo Akad Univ, Dept Phys, Porthansgaten 3, FIN-20500 Turku, Finland. EM rosterba@abo.fi; jin-woo.han@nasa.gov RI Osterbacka, Ronald/I-9161-2012 OI Osterbacka, Ronald/0000-0003-0656-2592 NR 15 TC 2 Z9 2 U1 1 U2 31 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0957-4484 EI 1361-6528 J9 NANOTECHNOLOGY JI Nanotechnology PD MAR 7 PY 2014 VL 25 IS 9 AR 090201 DI 10.1088/0957-4484/25/9/090201 PG 2 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Science & Technology - Other Topics; Materials Science; Physics GA AB1SI UT WOS:000331573500001 ER PT J AU Saitta, EKH Gittings, MJ Clausen, C Quinn, J Yestrebsky, CL AF Saitta, Erin K. H. Gittings, Michael J. Clausen, Christian Quinn, Jacqueline Yestrebsky, Cherie L. TI Laboratory evaluation of a prospective remediation method for PCB-contaminated paint SO JOURNAL OF ENVIRONMENTAL HEALTH SCIENCE AND ENGINEERING LA English DT Article DE Polychlorinated biphenyl (PCB); Remediation; Aroclor; Paint; Magnesium ID POLYCHLORINATED-BIPHENYLS; NORWAY; METAL AB Background: Paint laden with polychlorinated biphenyls (PCBs) often acts as a point source for environmental contamination. It is advantageous to address contaminated paint before the PCBs transport to surrounding media; however, current disposal methods of painted material introduce a variety of complications. Previous work demonstrates that PCBs can be broken down at ambient temperatures and pressures through a degradation process involving magnesium metal and acidified ethanol. This report is an extension of that work by describing the development of a delivery system for said reaction in preparation for a field test. Two treatment options including the Activated Metal Treatment System (AMTS) and the Non-Metal Treatment System (NMTS) remove and degrade PCBs from painted surfaces. Findings: AMTS decreased the Aroclor (R) concentration of a solution by more than 97% within 120 minutes and the Aroclor (R) concentration of industrial paint chips by up to 98% over three weeks. After removing up to 76% of PCBs on a painted surface after seven days, NMTS also removed trace amounts of PCBs in the paint's concrete substrate. The evaporation rate of the solvent (ethanol) from the treatment system was reduced when the application area was increased. The solvent system's ability to remove more than 90% of PCBs was maintained after losing 36% of its mass to solvent evaporation. Conclusions: The delivery systems, AMTS and NMTS, are able to support the hydrodechlorination reaction necessary for PCB degradation and are therefore attractive options for further studies regarding the remediation of contaminated painted surfaces. C1 [Saitta, Erin K. H.; Clausen, Christian; Yestrebsky, Cherie L.] Univ Cent Florida, Dept Chem, Orlando, FL 32816 USA. [Gittings, Michael J.] CUNY John Jay Coll Criminal Justice, New York, NY 10019 USA. [Quinn, Jacqueline] NASA, Kennedy Space Ctr, FL 32899 USA. RP Yestrebsky, CL (reprint author), Univ Cent Florida, Dept Chem, 4000 Cent Florida Blvd, Orlando, FL 32816 USA. EM cherie.yestrebsky@ucf.edu FU Environmental Security Technology Certification Program (ESTCP); Geosyntec FX The authors would like to thank the Environmental Security Technology Certification Program (ESTCP) for funding this research along with Geosyntec for their additional support. NR 20 TC 2 Z9 2 U1 1 U2 8 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 2052-336X J9 J ENVIRON HEALTH SCI JI J. Environ. Health Sci. Eng PD MAR 6 PY 2014 VL 12 AR 57 DI 10.1186/2052-336X-12-57 PG 5 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA AF6DK UT WOS:000334804400001 ER PT J AU Sakai, N Sakai, T Hirota, T Watanabe, Y Ceccarelli, C Kahane, C Bottinelli, S Caux, E Demyk, K Vastel, C Coutens, A Taquet, V Ohashi, N Takakuwa, S Yen, HW Aikawa, Y Yamamoto, S AF Sakai, Nami Sakai, Takeshi Hirota, Tomoya Watanabe, Yoshimasa Ceccarelli, Cecilia Kahane, Claudine Bottinelli, Sandrine Caux, Emmanuel Demyk, Karine Vastel, Charlotte Coutens, Audrey Taquet, Vianney Ohashi, Nagayoshi Takakuwa, Shigehisa Yen, Hsi-Wei Aikawa, Yuri Yamamoto, Satoshi TI Change in the chemical composition of infalling gas forming a disk around a protostar SO NATURE LA English DT Article ID CARBON-CHAIN MOLECULES; INTERSTELLAR-MOLECULES; STAR-FORMATION; L1527; PRESTELLAR; MASS; ENVELOPES; EMISSION; ROTATION; SYSTEM AB IRAS 04368+2557 is a solar-type (low-mass) protostar embedded in a protostellar core (L1527) in the Taurus molecular cloud(1,2), which is only 140 parsecs away from Earth, making it the closest large star-forming region. The protostellar envelope has a flattened shape with a diameter of a thousand astronomical units (1 AU is the distance from Earth to the Sun), and is infalling and rotating(3-5). It also has a protostellar disk with a radius of 90 AU (ref. 6), from which a planetary system is expected to form(7,8). The interstellar gas, mainly consisting of hydrogen molecules, undergoes a change in density of about three orders of magnitude as it collapses from the envelope into the disk, while being heated from 10 kelvin to over 100 kelvin in the mid-plane, but it has hitherto not been possible to explore changes in chemical composition associated with this collapse. Here we report that the unsaturated hydrocarbon molecule cyclic-C3H2 resides in the infalling rotating envelope, whereas sulphur monoxide (SO) is enhanced in the transition zone at the radius of the centrifugal barrier (100 +/- 20 AU), which is the radius at which the kinetic energy of the infalling gas is converted to rotational energy. Such a drastic change in chemistry at the centrifugal barrier was not anticipated, but is probably caused by the discontinuous infalling motion at the centrifugal barrier and local heating processes there. C1 [Sakai, Nami; Watanabe, Yoshimasa; Yamamoto, Satoshi] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Sakai, Takeshi] Univ Electrocommun, Dept Commun Engn & Informat, Chofu, Tokyo 1828585, Japan. [Hirota, Tomoya] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Ceccarelli, Cecilia; Kahane, Claudine] Inst Planetol & Astrophys Grenoble, F-38041 Grenoble 9, France. [Bottinelli, Sandrine; Caux, Emmanuel; Demyk, Karine; Vastel, Charlotte] Univ Toulouse 3, Observ Midi Pyrenees, Univ Toulouse, IRAP, F-31062 Toulouse, France. [Bottinelli, Sandrine; Caux, Emmanuel; Demyk, Karine; Vastel, Charlotte] CNRS, IRAP, F-31028 Toulouse 4, France. [Coutens, Audrey] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Osterbro, Denmark. [Coutens, Audrey] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Coutens, Audrey] Univ Copenhagen, Nat Hist Museum Denmark, DK-1350 Copenhagen K, Denmark. [Taquet, Vianney] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. [Ohashi, Nagayoshi; Yen, Hsi-Wei] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Ohashi, Nagayoshi] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Takakuwa, Shigehisa; Yen, Hsi-Wei] Natl Taiwan Univ, Inst Astrophys, Taipei 10617, Taiwan. [Aikawa, Yuri] Kobe Univ, Dept Earth & Planetary Sci, Kobe, Hyogo 6578501, Japan. RP Sakai, N (reprint author), Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. EM nami@taurus.phys.s.u-tokyo.ac.jp RI SAKAI, NAMI/G-4893-2014; Coutens, Audrey/M-4533-2014; OI SAKAI, NAMI/0000-0002-3297-4497; Coutens, Audrey/0000-0003-1805-3920; Watanabe, Yoshimasa/0000-0002-9668-3592 FU Ministry of Education, Culture, Sports, Science and Technologies of Japan [21224002, 25400223, 25108005, 24684011]; JSPS; MAEE under the Japan-France integrated action programme (SAKURA); French Agence Nationale pour la Recherche (ANR) project FORCOMS [ANR-08-BLAN-0225]; Partenariats Hubert Curien (PHC) Programme SAKURA [25765VC] FX We thank T. Hanawa and K. Furuya for discussions. This paper makes use of the ALMA dataset ADS/JAO.ALMA#2011.0.00604.S. ALMA is a partnership of the ESO (representing its member states), the NSF (USA) and NINS (Japan), together with the NRC (Canada) and the NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by the ESO, the AUI/NRAO and the NAOJ. We thank the ALMA staff for their support. N.S. and S.Y. acknowledge financial support from Grants-in-Aid from the Ministry of Education, Culture, Sports, Science and Technologies of Japan (21224002, 25400223 and 25108005), and by JSPS and MAEE under the Japan-France integrated action programme (SAKURA). T. H. acknowledges financial support from Grants-in-Aid from the Ministry of Education, Culture, Sports, Science, and Technologies of Japan (21224002, 24684011 and 25108005). C. C. and C. K. acknowledge financial support from the French Agence Nationale pour la Recherche (ANR) project FORCOMS (contract ANR-08-BLAN-0225) and from the Partenariats Hubert Curien (PHC) Programme SAKURA 25765VC. NR 28 TC 42 Z9 42 U1 1 U2 24 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 MAR 6 PY 2014 VL 507 IS 7490 BP 78 EP + DI 10.1038/nature13000 PG 14 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AC0ZQ UT WOS:000332224400045 PM 24522533 ER PT J AU Tang, H Brolly, M Zhao, F Strahler, AH Schaaf, CL Ganguly, S Zhang, G Dubayah, R AF Tang, Hao Brolly, Matthew Zhao, Feng Strahler, Alan H. Schaaf, Crystal L. Ganguly, Sangram Zhang, Gong Dubayah, Ralph TI Deriving and validating Leaf Area Index (LAI) at multiple spatial scales through lidar remote sensing: A case study in Sierra National Forest, CA SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Lidar; LAI; Sierra National Forest; LVIS; GLAS; Echidna ID WAVE-FORM LIDAR; GROUND-BASED LIDAR; HEMISPHERICAL PHOTOGRAPHY; LASER ALTIMETER; GLOBAL PRODUCTS; BOREAL FORESTS; CLUMPING INDEX; GAP FRACTION; PART 1; VEGETATION AB Increasing the accuracy and spatial coverage of Leaf Area Index (LAI) values is an important part of any attempt to successfully model global atmosphere/biosphere interactions. It is further a fundamental parameter in land surface processes and Earth system climate models. Remote sensing methods offer an opportunity to improve on each of these requirements but are typically limited by the necessity for validation using labor intensive and sparsely collected in situ measurements. In this paper we present the results of an intercomparative study of ground-based, airborne and spaceborne retrievals of total LAI over the conifer-dominated forests of Sierra Nevada in California. The efficacy of LVIS (Laser Vegetation Imaging Sensor) airborne waveform lidar LAI measurements (total and vertical profile) has previously been validated at the site specific level using destructive sampling. We also explore the efficacy of ground based measurements obtained from hemispherical photography, LAI-2000, and ground based lidar, acknowledging discrepancies existing between the systems and collected data. We highlight their use and role in validating the relationship between ground and airborne estimates of total LAI (LVIS LAI correlation with i) hemispherical photographs, r(2) = 0.80, ii) IAI-2000, r(2) = 0.85, and iii) terrestrial lidar, r(2) = 0.76. The existence of such relationships offers immediate implications for LAI estimation where LVIS data is available, creating the potential to obtain, not only total LAI values but also corresponding vertical LAI distributions from a ground validated source previously unobtainable at this spatial scale. The ability to validate airborne lidar LAI data collected at different spatial scales to the available ground measurements allows further upscaled validation using global lidar datasets provided by spacebome lidar, such as the Geoscience Laser Altimeter System (GLAS). In the absence of adequate ground validation plots coincident with GLAS footprints, GLAS LAI validation is examined using geographically limited but spatially continuous LVIS data. Under favorable conditions, significantly the absence of slopes greater than similar to 20 degrees, the comparison between LVIS and GLAS IAI values obtained using a recursive algorithm constrained by independently validated LAI limits exposes the capability of GLAS as an accurate standalone LAI sensor (r(2) = 0.69, bias = -0.05 and RMSE = 0.33). The correlation comparison between LVIS and GLAS LAI estimates not only significantly exceed those associated with equivalent space borne passive remote sensing datasets, such as MODIS (r(2) = 0.20, bias = -0.16 and RMSE = 0.67) but also offers significant advantages to future research including the prospective validation of regional and global L.Al products and data comparison with ecosystem model inputs. The encountered effectiveness of these relationships allows the implementation of a scaling-up strategy where ground-based LAI observations are related to aircraft observations of LAI, which in turn are used to validate GLAS LAI derived from coincident data. Successful implementation of this strategy paves the way for the future recovery of vertical LAI profiles on a global scale and opens up the potential for fusion studies to incorporate widely available and spatially abundant passive optical datasets. (C) 2014 Elsevier Inc. All rights reserved. C1 [Tang, Hao; Brolly, Matthew; Zhao, Feng; Dubayah, Ralph] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Zhao, Feng; Strahler, Alan H.; Schaaf, Crystal L.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA. [Schaaf, Crystal L.] Univ Massachusetts Boston, Sch Environm, Boston, MA 02125 USA. [Ganguly, Sangram; Zhang, Gong] Bay Area Environm Res Inst, West Sonoma, CA USA. [Ganguly, Sangram; Zhang, Gong] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Tang, H (reprint author), Univ Maryland, Dept Geog Sci, 2120 Lefrak Hall, College Pk, MD 20742 USA. RI ganguly, sangram/B-5108-2010; Beckley, Matthew/D-4547-2013; Tang, Hua/K-4948-2016; OI Tang, Hua/0000-0002-6685-6165; Brolly, Matthew/0000-0002-3576-9675 FU NASA [NNX08AP55G, NNG06GI92G, NNX08AE94A]; NSF [0923389]; Earth and Space Science graduate fellowship [NNX12AN43H] FX This work was funded by NASA under grant NNX08AP55G (Dubayah) and an Earth and Space Science graduate fellowship NNX12AN43H (Dubayah/cang). The ground based measurements were supported by NASA under grant NNG06GI92G and NNX08AE94A and NSF under grant 0923389. We thank Yong Pang for the original GLAS waveform processing, Ross Nelson for providing useful advice on GLAS data processing, Michelle Hofton for the advice regarding LVIS processing and Tao He for his help in processing MODIS data. We also thank the NSIDC (National Snow & Ice Data Center) User Services for the help on data acquisition. NR 55 TC 34 Z9 38 U1 8 U2 92 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 MAR 5 PY 2014 VL 143 BP 131 EP 141 DI 10.1016/j.rse.2013.12.007 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AB5WP UT WOS:000331859700012 ER PT J AU Piontek, F Muller, C Pugh, TAM Clark, DB Deryng, D Elliott, J Gonzalez, FDC Florke, M Folberth, C Franssen, W Frieler, K Friend, AD Gosling, SN Hemming, D Khabarov, N Kim, HJ Lomas, MR Masaki, Y Mengel, M Morse, A Neumann, K Nishina, K Ostberg, S Pavlick, R Ruane, AC Schewe, J Schmid, E Stacke, T Tang, QH Tessler, ZD Tompkins, AM Warszawski, L Wisser, D Schellnhuber, HJ AF Piontek, Franziska Mueller, Christoph Pugh, Thomas A. M. Clark, Douglas B. Deryng, Delphine Elliott, Joshua Gonzalez, Felipe de Jesus Colon Floerke, Martina Folberth, Christian Franssen, Wietse Frieler, Katja Friend, Andrew D. Gosling, Simon N. Hemming, Deborah Khabarov, Nikolay Kim, Hyungjun Lomas, Mark R. Masaki, Yoshimitsu Mengel, Matthias Morse, Andrew Neumann, Kathleen Nishina, Kazuya Ostberg, Sebastian Pavlick, Ryan Ruane, Alex C. Schewe, Jacob Schmid, Erwin Stacke, Tobias Tang, Qiuhong Tessler, Zachary D. Tompkins, Adrian M. Warszawski, Lila Wisser, Dominik Schellnhuber, Hans Joachim TI Multisectoral climate impact hotspots in a warming world SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE coinciding pressures; differential climate impacts; ISI-MIP ID GLOBAL CLIMATE; MALARIA; DROUGHT; MODELS AB The impacts of global climate change on different aspects of humanity's diverse life-support systems are complex and often difficult to predict. To facilitate policy decisions on mitigation and adaptation strategies, it is necessary to understand, quantify, and synthesize these climate-change impacts, taking into account their uncertainties. Crucial to these decisions is an understanding of how impacts in different sectors overlap, as overlapping impacts increase exposure, lead to interactions of impacts, and are likely to raise adaptation pressure. As a first step we develop herein a framework to study coinciding impacts and identify regional exposure hotspots. This framework can then be used as a starting point for regional case studies on vulnerability and multifaceted adaptation strategies. We consider impacts related to water, agriculture, ecosystems, and malaria at different levels of global warming. Multisectoral overlap starts to be seen robustly at a mean global warming of 3 degrees C above the 1980-2010 mean, with 11% of the world population subject to severe impacts in at least two of the four impact sectors at 4 degrees C. Despite these general conclusions, we find that uncertainty arising from the impact models is considerable, and larger than that from the climate models. In a low probability-high impact worst-case assessment, almost the whole inhabited world is at risk for multisectoral pressures. Hence, there is a pressing need for an increased research effort to develop a more comprehensive understanding of impacts, as well as for the development of policy measures under existing uncertainty. C1 [Piontek, Franziska; Mueller, Christoph; Frieler, Katja; Mengel, Matthias; Ostberg, Sebastian; Schewe, Jacob; Warszawski, Lila; Schellnhuber, Hans Joachim] Potsdam Inst Climate Impact Studies, D-14473 Potsdam, Germany. [Pugh, Thomas A. M.] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-82467 Garmisch Partenkirchen, Germany. [Clark, Douglas B.] Ctr Ecol & Hydrol, Wallingford OX1 08BB, Oxon, England. [Deryng, Delphine] Univ E Anglia, Sch Environm Sci, Tyndall Ctr, Norwich NR4 7TJ, Norfolk, England. [Elliott, Joshua] Univ Chicago, Computat Inst, Chicago, IL 60637 USA. [Gonzalez, Felipe de Jesus Colon; Tompkins, Adrian M.] Abdus Salam Int Ctr Theoret Phys, I-34151 Trieste, Italy. [Floerke, Martina] Univ Gesamthsch Kassel, Ctr Environm Syst Res, D-34109 Kassel, Germany. [Folberth, Christian] Swiss Fed Inst Aquat Sci & Technol EAWAG, CH-8600 Dubendorf, Switzerland. [Franssen, Wietse] Wageningen Univ, NL-6708 PB Wageningen, Netherlands. [Friend, Andrew D.] Univ Cambridge, Dept Geog, Cambridge CB2 1TN, England. [Gosling, Simon N.] Univ Nottingham, Sch Geog, Nottingham NG7 2RD, England. [Hemming, Deborah] Met Off Hadley Ctr, Exeter EX1 3PB, Devon, England. [Khabarov, Nikolay] Int Inst Appl Syst Anal, A-2361 Laxenburg, Austria. [Kim, Hyungjun] Univ Tokyo, Inst Ind Sci, Tokyo 1538505, Japan. [Lomas, Mark R.] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England. [Masaki, Yoshimitsu; Nishina, Kazuya] Natl Inst Environm Studies, Ctr Global Environm Res, Tsukuba, Ibaraki 3058506, Japan. [Morse, Andrew] Univ Liverpool, Sch Environm Sci, Liverpool L69 3GP, Merseyside, England. [Neumann, Kathleen] PBL Netherlands Environm Assessment Agcy, NL-3720 AH Bilthoven, Netherlands. [Neumann, Kathleen] Wageningen Univ, NL-6706 KN Wageningen, Netherlands. [Pavlick, Ryan] Max Planck Inst Biogeochem, D-07745 Jena, Germany. [Ruane, Alex C.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Schmid, Erwin] Univ Nat Resources & Life Sci, Dept Econ & Social Sci, A-1180 Vienna, Austria. [Stacke, Tobias] Max Planck Inst Meteorol, D-20146 Hamburg, Germany. [Tang, Qiuhong] Chinese Acad Sci, Inst Geog Sci & Nat Resources Res, Beijing 100101, Peoples R China. [Tessler, Zachary D.] CUNY, Environm Cross Rd Initiat, New York, NY 10031 USA. [Wisser, Dominik] Univ Utrecht, Dept Phys Geog, NL-3508 TC Utrecht, Netherlands. [Schellnhuber, Hans Joachim] Santa Fe Inst, Santa Fe, NM 87501 USA. RP Piontek, F (reprint author), Potsdam Inst Climate Impact Studies, D-14473 Potsdam, Germany. EM piontek@pik-potsdam.de RI Schellnhuber, Hans Joachim/B-2607-2012; Garmisch-Pa, Ifu/H-9902-2014; KIM, HYUNGJUN/I-5099-2014; Deryng, Delphine/F-7417-2010; Clark, Douglas/A-6102-2010; Tompkins, Adrian/N-6472-2013; Hermans, Kathleen/M-8564-2015; Mueller, Christoph/E-4812-2016; Osborne, Nicholas/N-4915-2015; Pugh, Thomas/A-3790-2010; OI Frieler, Katja/0000-0003-4869-3013; Nishina, Kazuya/0000-0002-8820-1282; Schmid, Erwin/0000-0003-4783-9666; Gosling, Simon/0000-0001-5973-6862; Ostberg, Sebastian/0000-0002-2368-7015; Schellnhuber, Hans Joachim/0000-0001-7453-4935; KIM, HYUNGJUN/0000-0003-1083-8416; Deryng, Delphine/0000-0001-6214-7241; Clark, Douglas/0000-0003-1348-7922; Tompkins, Adrian/0000-0003-0975-6691; Mueller, Christoph/0000-0002-9491-3550; Osborne, Nicholas/0000-0002-6700-2284; Pugh, Thomas/0000-0002-6242-7371; Colon-Gonzalez, Felipe de Jesus/0000-0002-9671-3405; Tang, Qiuhong/0000-0002-0886-6699 FU German Federal Ministry of Education and Research [01LS1201A]; Joint Department of Energy and Climate Change/Defra Met Office Hadley Centre Climate Programme [GA01101]; Federal Ministry for the Environment; Nature Conservation and Nuclear Safety [11_II_093_Global_A_SIDS_and_LDCs]; EUFP7 Quantifying Weather and Climate Impacts on Health in Developing Countries (QWeCI) and HEALTHY FUTURES project; Environment Research and Technology Development Fund of the Ministry of the Environment, Japan [S-10]; EU [282672]; [266992]; [238366] FX We thank the anonymous referees for detailed and valuable comments greatly improving this paper; the World Climate Research Programme's Working Group on Coupled Modelling, which is responsible for Coupled Model Intercomparison Project; and the climate modeling groups for producing and making available their model output. The Intersectoral Impact Model Intercomparison Project Fast Track project underlying the framework of this paper was funded by the German Federal Ministry of Education and Research (01LS1201A). For the Coupled Model Intercomparison Project, the US 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. This study was funded in part by the European Framework Programme FP7/20072013 under Grants 266992 (to F. P.) and 238366 (to A. F.); Joint Department of Energy and Climate Change/Defra Met Office Hadley Centre Climate Programme GA01101 (to D. H.); the Federal Ministry for the Environment (K. F.); the Nature Conservation and Nuclear Safety 11_II_093_Global_A_SIDS_and_LDCs (to K. F.); EUFP7 Quantifying Weather and Climate Impacts on Health in Developing Countries (QWeCI) and HEALTHY FUTURES projects (F. d. J. C. G.); and the Environment Research and Technology Development Fund (S-10) of the Ministry of the Environment, Japan (to Y. M. and K. Nishina). T. A. M. P. acknowledges support from EU FP7 project EMBRACE (Earth System Model Bias Reduction and Assessing Abrupt Climate Change) (Grant 282672). NR 37 TC 50 Z9 50 U1 8 U2 66 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 MAR 4 PY 2014 VL 111 IS 9 BP 3233 EP 3238 DI 10.1073/pnas.1222471110 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AC5KR UT WOS:000332560300023 PM 24344270 ER PT J AU Elliott, J Deryng, D Mueller, C Frieler, K Konzmann, M Gerten, D Glotter, M Florke, M Wada, Y Best, N Eisner, S Fekete, BM Folberth, C Foster, I Gosling, SN Haddeland, I Khabarov, N Ludwig, F Masaki, Y Olin, S Rosenzweig, C Ruane, AC Satoh, Y Schmid, E Stacke, T Tang, QH Wisser, D AF Elliott, Joshua Deryng, Delphine Mueller, Christoph Frieler, Katja Konzmann, Markus Gerten, Dieter Glotter, Michael Floerke, Martina Wada, Yoshihide Best, Neil Eisner, Stephanie Fekete, Balazs M. Folberth, Christian Foster, Ian Gosling, Simon N. Haddeland, Ingjerd Khabarov, Nikolay Ludwig, Fulco Masaki, Yoshimitsu Olin, Stefan Rosenzweig, Cynthia Ruane, Alex C. Satoh, Yusuke Schmid, Erwin Stacke, Tobias Tang, Qiuhong Wisser, Dominik TI Constraints and potentials of future irrigation water availability on agricultural production under climate change SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE adaptation; agriculture; hydrology; uncertainty ID MODEL DESCRIPTION; REQUIREMENTS; FOOD; SCARCITY; IMPACTS; PART AB We compare ensembles of water supply and demand projections from 10 global hydrological models and six global gridded crop models. These are produced as part of the Inter-Sectoral Impacts Model Intercomparison Project, with coordination from the Agricultural Model Intercomparison and Improvement Project, and driven by outputs of general circulation models run under representative concentration pathway 8.5 as part of the Fifth Coupled Model Intercomparison Project. Models project that direct climate impacts to maize, soybean, wheat, and rice involve losses of 4001,400 Pcal (8-24% of present-day total) when CO2 fertilization effects are accounted for or 1,400-2,600 Pcal (24-43%) otherwise. Freshwater limitations in some irrigated regions (western United States; China; and West, South, and Central Asia) could necessitate the reversion of 20-60 Mha of cropland from irrigated to rainfed management by end-of-century, and a further loss of 600-2,900 Pcal of food production. In other regions (northern/eastern United States, parts of South America, much of Europe, and South East Asia) surplus water supply could in principle support a net increase in irrigation, although substantial investments in irrigation infrastructure would be required. C1 [Elliott, Joshua; Mueller, Christoph; Frieler, Katja; Konzmann, Markus; Gerten, Dieter; Best, Neil; Foster, Ian] Univ Chicago, Computat Inst, Chicago, IL 60637 USA. [Elliott, Joshua; Foster, Ian] Argonne Natl Lab, Math & Comp Sci Div, Lemont, IL 60439 USA. [Elliott, Joshua; Rosenzweig, Cynthia; Ruane, Alex C.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. [Deryng, Delphine] Univ E Anglia, Tyndall Ctr Climate Change Res, Norwich NR4 7TJ, Norfolk, England. [Mueller, Christoph; Frieler, Katja; Konzmann, Markus; Gerten, Dieter] Potsdam Inst Climate Impact Res, D-14473 Potsdam, Germany. [Glotter, Michael] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Floerke, Martina; Eisner, Stephanie] Univ Kassel, Ctr Environm Syst Res, D-34109 Kassel, Germany. [Wada, Yoshihide] Univ Utrecht, Dept Phys Geog, NL-3584 CS Utrecht, Netherlands. [Fekete, Balazs M.] CUNY City Coll, New York, NY 10031 USA. [Folberth, Christian] Swiss Fed Inst Aquat Sci & Technol, CH-8600 Dubendorf, Switzerland. [Gosling, Simon N.] Univ Nottingham, Nottingham NG7 2RD, England. [Haddeland, Ingjerd] Norwegian Water Resources & Energy Directorate, N-0301 Oslo, Norway. [Khabarov, Nikolay] Int Inst Appl Syst Anal IIASA, Ecosyst Serv & Management Program ESM, A-2361 Laxenburg, Austria. [Ludwig, Fulco] Univ Wageningen & Res Ctr, NL-6708 PB Wageningen, Netherlands. [Masaki, Yoshimitsu] Natl Inst Environm Studies, Tsukuba, Ibaraki 3058506, Japan. [Olin, Stefan] Lund Univ, S-22362 Lund, Sweden. [Rosenzweig, Cynthia; Ruane, Alex C.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Satoh, Yusuke] Univ Tokyo, Tokyo 1538505, Japan. [Schmid, Erwin] Univ Nat Resources & Life Sci, A-1180 Vienna, Austria. [Stacke, Tobias] Max Planck Inst Meteorol, D-20146 Hamburg, Germany. [Tang, Qiuhong] Chinese Acad Sci, Inst Geog Sci & Nat Resources Res, Beijing 100101, Peoples R China. [Wisser, Dominik] Univ Bonn, Res Dev Ctr, D-53113 Bonn, Germany. RP Elliott, J (reprint author), Univ Chicago, Computat Inst, Chicago, IL 60637 USA. EM jelliott@ci.uchicago.edu RI Ludwig, Fulco/N-7732-2013; Gerten, Dieter/B-2975-2013; Wada, Yoshihide/F-3595-2012; Deryng, Delphine/F-7417-2010; Mueller, Christoph/E-4812-2016; OI Gosling, Simon/0000-0001-5973-6862; Wada, Yoshihide/0000-0003-4770-2539; Deryng, Delphine/0000-0001-6214-7241; Mueller, Christoph/0000-0002-9491-3550; Tang, Qiuhong/0000-0002-0886-6699; Frieler, Katja/0000-0003-4869-3013; Schmid, Erwin/0000-0003-4783-9666 FU German Federal Ministry of Education and Research (BMBF) [01LS1201A]; National Science Foundation (NSF) [SBE-0951576, GEO-1215910]; European Union [266992]; Argonne National Laboratory [S10 RR029030-01]; NSF [OCI-1148443]; Science, Technology, and Society Priority Group from the University of Nottingham; Environment Research and Technology Development Fund of the Ministry of the Environment, Japan [S-10]; 973 Program of China [2012CB955403]; Formas Strong Research Environment; Federal Ministry for the Environment Grant [11 II 093]; LDC FX 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 (SI Appendix, Table S2) for making their outputs available. For CMIP, the US Department of Energy's Program for Climate Model Diagnosis and Intercomparison provides coordinating support in partnership with the Global Organization for Earth System Science Portals. The ISI-MIP Fast Track project was funded by the German Federal Ministry of Education and Research (BMBF) with Project Funding Reference 01LS1201A. This work was also supported in part by the National Science Foundation (NSF) under Grants SBE-0951576 and GEO-1215910. The research leading to these results has received funding from the European Union's Seventh Framework Programme FP7/2007-2013 under Grant Agreement 266992. Computing was provided by a number of sources, including the University of Chicago Computing Cooperative, the University of Chicago Research Computing Center, and through the National Institutes of Health with resources provided by the Computation Institute and the Biological Sciences Division of the University of Chicago and Argonne National Laboratory, under Grant S10 RR029030-01. Part of the computing was facilitated using the Swift parallel scripting language, supported in part by NSF Grant OCI-1148443. S. N. G. was supported by a Science, Technology, and Society Priority Group grant from the University of Nottingham. Y. M. was supported by the Environment Research and Technology Development Fund (S-10) of the Ministry of the Environment, Japan. Q. T. is supported by the 973 Program of China (2012CB955403). S. O. acknowledges support by the Formas Strong Research Environment "Land Use Today and Tomorrow." This work has been conducted under the framework of ISI-MIP and in partnership with the AgMIP community. K. F. was supported by Federal Ministry for the Environment Grant 11 II 093 Global A SIDS and LDCs. NR 50 TC 97 Z9 100 U1 22 U2 147 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 MAR 4 PY 2014 VL 111 IS 9 BP 3239 EP 3244 DI 10.1073/pnas.1222474110 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AC5KR UT WOS:000332560300024 PM 24344283 ER PT J AU Rosenzweig, C Elliott, J Deryng, D Ruane, AC Muller, C Arneth, A Boote, KJ Folberth, C Glotter, M Khabarov, N Neumann, K Piontek, F Pugh, TAM Schmid, E Stehfest, E Yang, H Jones, JW AF Rosenzweig, Cynthia Elliott, Joshua Deryng, Delphine Ruane, Alex C. Mueller, Christoph Arneth, Almut Boote, Kenneth J. Folberth, Christian Glotter, Michael Khabarov, Nikolay Neumann, Kathleen Piontek, Franziska Pugh, Thomas A. M. Schmid, Erwin Stehfest, Elke Yang, Hong Jones, James W. TI Assessing agricultural risks of climate change in the 21st century in a global gridded crop model intercomparison SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE food security; AgMIP; ISI-MIP; climate impacts; agriculture ID IMPACTS; YIELD; DYNAMICS AB Here we present the results from an intercomparison of multiple global gridded crop models (GGCMs) within the framework of the Agricultural Model Intercomparison and Improvement Project and the Inter-Sectoral Impacts Model Intercomparison Project. Results indicate strong negative effects of climate change, especially at higher levels of warming and at low latitudes; models that include explicit nitrogen stress project more severe impacts. Across seven GGCMs, five global climate models, and four representative concentration pathways, model agreement on direction of yield changes is found in many major agricultural regions at both low and high latitudes; however, reducing uncertainty in sign of response in mid-latitude regions remains a challenge. Uncertainties related to the representation of carbon dioxide, nitrogen, and high temperature effects demonstrated here show that further research is urgently needed to better understand effects of climate change on agricultural production and to devise targeted adaptation strategies. C1 [Rosenzweig, Cynthia; Ruane, Alex C.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Rosenzweig, Cynthia; Elliott, Joshua; Ruane, Alex C.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. [Elliott, Joshua] Univ Chicago, Computat Inst, Chicago, IL 60637 USA. [Deryng, Delphine] Univ E Anglia, Tyndall Ctr, Norwich NR4 7TJ, Norfolk, England. [Deryng, Delphine] Univ E Anglia, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England. [Mueller, Christoph; Piontek, Franziska] Potsdam Inst Climate Impact Res, D-14473 Potsdam, Germany. [Arneth, Almut; Pugh, Thomas A. M.] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-82467 Garmisch Partenkirchen, Germany. [Boote, Kenneth J.; Jones, James W.] Univ Florida, Dept Agr & Biol Engn, Gainesville, FL 32611 USA. [Folberth, Christian; Yang, Hong] EAWAG Swiss Fed Inst Aquat Sci & Technol, CH-8600 Dubendorf, Switzerland. [Glotter, Michael] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Khabarov, Nikolay] Int Inst Appl Syst Anal, Ecosyst Serv & Management Program ESM, A-2361 Laxenburg, Austria. [Neumann, Kathleen] Netherlands Environm Assessment Agcy, Planbur Leefomgeving, NL-3720 AH Bilthoven, Netherlands. [Neumann, Kathleen] Wageningen Univ, NL-6700 AK Wageningen, Netherlands. [Schmid, Erwin] Univ Nat Resources & Life Sci, A-1180 Vienna, Austria. RP Rosenzweig, C (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM cynthia.rosenzweig@nasa.gov RI Deryng, Delphine/F-7417-2010; Hermans, Kathleen/M-8564-2015; Garmisch-Pa, Ifu/H-9902-2014; Mueller, Christoph/E-4812-2016; Pugh, Thomas/A-3790-2010; OI Deryng, Delphine/0000-0001-6214-7241; Mueller, Christoph/0000-0002-9491-3550; Pugh, Thomas/0000-0002-6242-7371; Boote, Kenneth/0000-0002-1358-5496; Schmid, Erwin/0000-0003-4783-9666 FU US Department of Agriculture; United Kingdom Department for International Development; European Union [266992] FX We thank the AgMIP research community and the ISI-MIP team for their contributions to this effort; the US Department of Agriculture and the United Kingdom Department for International Development for their support of AgMIP; the World Climate Research Programme's Working Group on Coupled Modelling, which is responsible for CMIP; the climate modeling groups for producing and making available their model output; and two anonymous reviewers for their helpful comments. At the Columbia Center for Climate Systems Research, we thank Erik Mencos-Contreras and Shari Lifson for research and graphics assistance. For CMIP the US 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. The research leading to these results has received funding from the European Union's Seventh Framework Programme FP7/2007-2013 under Grant Agreement 266992. NR 46 TC 195 Z9 197 U1 25 U2 182 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 MAR 4 PY 2014 VL 111 IS 9 BP 3268 EP 3273 DI 10.1073/pnas.1222463110 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AC5KR UT WOS:000332560300029 PM 24344314 ER PT J AU Roth, DJ Rouser, RW Bowman, RR Martin, RE Koshti, AM Morgan, DS AF Roth, D. J. Rouser, R. W. Bowman, R. R. Martin, R. E. Koshti, A. M. Morgan, David S. TI The Critical Role of High Resolution X-ray Micro-computed Tomography for Ultra-thin Wall Space Component Characterization SO MATERIALS EVALUATION LA English DT Article DE nondestructive testing; NDT; computed tomography; imaging; X-ray; metallic components; thin wall inspection AB A high-resolution micro-computed tomography system complemented by specialized hardware and software tools was used to provide quantitative characterization for a tapered ultra-thin wall space component at the National Aeronautics and Space Administration. The computed tomography data served two purposes: first, to assess whether an acceptable discontinuity condition based on component use requirements existed; and second, to provide comprehensive discontinuity measurements for life modeling. Regarding the latter, the measurements were used in a fracture mechanics based model to determine whether the components would be expected to survive (leak within) four service lives. This paper describes component acceptance criteria; the computed tomography system hardware and procedure; detectability and measurement error assessment of the computed tomography system; specialized software needed to aid the characterization process; example computed tomography results; correlation with optical/scanning electron microscope characterization; and an overview of the modeling technique utilizing the computed tomography data. C1 [Roth, D. J.; Bowman, R. R.; Morgan, David S.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Rouser, R. W.] Univ Toledo, Toledo, OH 43606 USA. [Martin, R. E.] Cleveland State Univ, Cleveland, OH 44115 USA. [Koshti, A. M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Roth, DJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 8 TC 0 Z9 0 U1 0 U2 1 PU AMER SOC NONDESTRUCTIVE TEST PI COLUMBUS PA 1711 ARLINGATE LANE PO BOX 28518, COLUMBUS, OH 43228-0518 USA SN 0025-5327 J9 MATER EVAL JI Mater. Eval. PD MAR PY 2014 VL 72 IS 3 BP 389 EP 397 PG 9 WC Materials Science, Characterization & Testing SC Materials Science GA AR1HB UT WOS:000343335200003 ER PT J AU Ricks, TM Lacy, TE Bednarcyk, BA Arnold, SM Hutchins, JW AF Ricks, Trenton M. Lacy, Thomas E., Jr. Bednarcyk, Brett A. Arnold, Steven M. Hutchins, John W. TI A Multiscale Progressive Failure Modeling Methodology for Composites That Includes Fiber Strength Stochastics SO CMC-COMPUTERS MATERIALS & CONTINUA LA English DT Article DE Generalized Method of Cells; Stochastic; Multiscale Modeling; Progressive Failure; Composites ID REINFORCED EPOXY COMPOSITE; TENSILE-STRENGTH; CARBON-FIBERS; LOAD-TRANSFER; MICROMECHANICAL ANALYSIS; GENERALIZED-METHOD; MATRIX COMPOSITES; FIBROUS MATERIALS; PREDICTION; DAMAGE AB A multiscale modeling methodology was developed for continuous fiber composites that incorporates a statistical distribution of fiber strengths into coupled multiscale micromechanics/finite element (FE) analyses. A modified two-parameter Weibull cumulative distribution function, which accounts for the effect of fiber length on the probability of failure, was used to characterize the statistical distribution of fiber strengths. A parametric study using the NASA Micromechanics Analysis Code with the Generalized Method of Cells (MAC/GMC) was performed to assess the effect of variable fiber strengths on local composite failure within a repeating unit. cell (RUC) and subsequent global failure. The NASA code FEAMAC and the ABAQUS finite element solver were used to analyze the progressive failure of a unidirectional SCS-6/TIMETAL 21S metal matrix composite tensile dogbone specimen at 650 degrees C. Multiscale progressive failure analyses were performed to quantify the effect of spatially varying fiber strengths on the RUC-averaged and global stress-strain responses and failure. The ultimate composite strengths and distribution of failure locations (predominately within the gage section) reasonably matched the experimentally observed failure behavior. The predicted composite failure behavior suggests that use of macroscale models that exploit global geometric symmetries are inappropriate for cases where the actual distribution of local fiber strengths displays no such symmetries. This issue has not received much attention in the literature. Moreover, the model discretization at a specific length scale can have a profound effect on the computational costs associated with multiscale simulations. C1 [Ricks, Trenton M.; Lacy, Thomas E., Jr.; Hutchins, John W.] Mississippi State Univ, Dept Aerosp Engn, Mississippi State, MS 39762 USA. [Bednarcyk, Brett A.; Arnold, Steven M.] NASA Glenn Res Ctr, Mech & Life Predict Branch, Cleveland, OH 44135 USA. RP Lacy, TE (reprint author), Mississippi State Univ, Dept Aerosp Engn, Mississippi State, MS 39762 USA. EM lacy@ae.msstate.edu NR 51 TC 1 Z9 1 U1 3 U2 6 PU TECH SCIENCE PRESS PI NORCROSS PA 6825 JIMMY CARTER BLVD, STE 1850, NORCROSS, GA 30071 USA SN 1546-2218 EI 1546-2226 J9 CMC-COMPUT MATER CON JI CMC-Comput. Mat. Contin. PD MAR PY 2014 VL 40 IS 2 BP 99 EP 129 PG 31 WC Engineering, Multidisciplinary; Materials Science, Multidisciplinary; Mathematics, Interdisciplinary Applications SC Engineering; Materials Science; Mathematics GA AQ2WU UT WOS:000342651500002 ER PT J AU Brown, AS Whitesides, G AF Brown, Alan S. Whitesides, George TI GEORGE WHITESIDES SO MECHANICAL ENGINEERING LA English DT Editorial Material C1 [Whitesides, George] NASA, Washington, DC USA. [Whitesides, George] Natl Space Soc, Washington, DC USA. [Whitesides, George] Blastoff Corp, Pasadena, CA USA. [Whitesides, George] Zero Grav Corp, Arlington, VA USA. [Whitesides, George] Orbital Sci, Dulles, VA USA. NR 0 TC 0 Z9 0 U1 2 U2 6 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 0025-6501 EI 1943-5649 J9 MECH ENG JI Mech. Eng. PD MAR PY 2014 VL 136 IS 3 BP 16 EP 16 PG 1 WC Engineering, Mechanical SC Engineering GA AQ0PQ UT WOS:000342485600010 ER PT J AU Sadovsky, AV AF Sadovsky, A. V. TI Application of the Shortest-Path Problem to Routing Terminal Airspace Air Traffic SO JOURNAL OF AEROSPACE INFORMATION SYSTEMS LA English DT Article ID FLOW MANAGEMENT; FLIGHT AB The flight navigation procedures envisioned under the Next Generation Transportation System will require a specification of the expected route of each flight. Once these specifications are provided, the flights must proceed along their routes with such speed profiles that every pair of aircraft complies with the minimal separation requirement imposed by the Federal Aviation Administration. The task of separation assurance is most challenging in terminal airspace, with many routes merging and crossing. This paper contributes a mathematical model and an algorithmic approach for routing flights strategically, with a foresight that potentially helps the subsequent computation of speed profiles compliant with the separation requirements and with each aircraft's feasible speed range. The approach consists of reducing a general routing problem to the shortest-path problem. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Sadovsky, AV (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM alexander.v.sadovsky@nasa.gov NR 34 TC 2 Z9 2 U1 0 U2 2 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 1940-3151 EI 2327-3097 J9 J AEROSP INFORM SYST JI J. Aerosp. Inf. Syst. PD MAR PY 2014 VL 11 IS 3 BP 118 EP 130 DI 10.2514/1.I010074 PG 13 WC Engineering, Aerospace SC Engineering GA AP4RK UT WOS:000342065800002 ER PT J AU Ponomarev, AL George, K Cucinotta, FA AF Ponomarev, Artem L. George, Kerry Cucinotta, Francis A. TI Generalized Time-Dependent Model of Radiation-Induced Chromosomal Aberrations in Normal and Repair-Deficient Human Cells SO RADIATION RESEARCH LA English DT Article ID DOUBLE-STRAND BREAKS; LINEAR-ENERGY-TRANSFER; HIGH-LET RADIATION; HEAT-LABILE SITES; HUMAN-LYMPHOCYTES; HUMAN FIBROBLASTS; BIOLOGICAL EFFECTIVENESS; INTERPHASE CHROMOSOMES; ACCELERATED PARTICLES; IONIZING-RADIATION AB We have developed a model that can simulate the yield of radiation-induced chromosomal aberrations (CAs) and un-rejoined chromosome breaks in normal and repair-deficient cells. The model predicts the kinetics of chromosomal aberration formation after exposure in the G(0)/G(1) phase of the cell cycle to either low-or high-LET radiation. A previously formulated model based on a stochastic Monte Carlo approach was updated to consider the time dependence of DNA double-strand break (DSB) repair (proper or improper), and different cell types were assigned different kinetics of DSB repair. The distribution of the DSB free ends was derived from a mechanistic model that takes into account the structure of chromatin and DSB clustering from high-LET radiation. The kinetics of chromosomal aberration formation were derived from experimental data on DSB repair kinetics in normal and repair-deficient cell lines. We assessed different types of chromosomal aberrations with the focus on simple and complex exchanges, and predicted the DSB rejoining kinetics and misrepair probabilities for different cell types. The results identify major cell-dependent factors, such as a greater yield of chromosome misrepair in ataxia telangiectasia (AT) cells and slower rejoining in Nijmegen (NBS) cells relative to the wild-type. The model's predictions suggest that two mechanisms could exist for the inefficiency of DSB repair in AT and NBS cells, one that depends on the overall speed of joining (either proper or improper) of DNA broken ends, and another that depends on geometric factors, such as the Euclidian distance between DNA broken ends, which influences the relative frequency of misrepair. (C) 2014 by Radiation Research Society C1 [Ponomarev, Artem L.] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA. [Ponomarev, Artem L.; Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Space Radiat Program, Houston, TX 77058 USA. [George, Kerry] Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA. RP Ponomarev, AL (reprint author), NASA, Lyndon B Johnson Space Ctr, ATTN Mail Code SK,2101 NASA Pkwy, Houston, TX 77058 USA. EM artem.l.ponomarev@nasa.gov FU NASA Space Radiation Risk Assessment Project FX Funding was provided through the NASA Space Radiation Risk Assessment Project. Special thanks to Dr. Michael Cornforth for useful discussions. NR 62 TC 3 Z9 4 U1 0 U2 3 PU RADIATION RESEARCH SOC PI LAWRENCE PA 810 E TENTH STREET, LAWRENCE, KS 66044 USA SN 0033-7587 EI 1938-5404 J9 RADIAT RES JI Radiat. Res. PD MAR PY 2014 VL 181 IS 3 BP 284 EP 292 DI 10.1667/RR13303.1 PG 9 WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology, Nuclear Medicine & Medical Imaging GA AO4KR UT WOS:000341307200006 PM 24611656 ER PT J AU Torres, A Ganley, J Maji, A Tucker, D Starodubov, D AF Torres, Anthony Ganley, Jeff Maji, Arup Tucker, Dennis Starodubov, Dmitry TI Increasing the working temperature range of ZrF4-BaF2-LaF3-AlF3-NaF glass through microgravity processing SO OPTICAL ENGINEERING LA English DT Article DE ZrF4-BaF2-LaF3-AlF3-NaF; microgravity; hyper-g; crystallization; working temperature; fluorozirconate glasses; optical microscopy; differential scanning calorimetry ID GRAVITY; CRYSTALLIZATION AB Fluorozirconate glasses, such as ZBLAN (ZrF4-BaF2-LaF3-AlF3-NaF), have the potential for optical transmission from 0.3 mu m in the ultraviolet to 7 mu m in the infrared regions. However, crystallites formed during the fiber-drawing process prevent this glass from achieving its desired transmission range. The temperature at which the glass can be drawn into a fiber is known as the working range, defined as (Tx-Tg), bounded by the glass transition temperature (Tg) and the crystallization temperature (Tx). In contrast to silica glasses, the working temperature range for ZBLAN glass is extremely narrow. Multiple ZBLAN samples were subjected to a heating and quenching test apparatus on the parabolic aircraft under a controlled mu-g and hyper-g environments and compared with 1-g ground tests. Optical microscopy examination elucidates that crystal growth in ZBLAN is suppressed and initiates at a later temperature when processed in a microgravity environment. Thus, the crystallization temperature, Tx, at which the crystals form has increased. The glass transition temperature, Tg, remains constant, as crystallization does not occur until approximately 360 degrees C for this composition of ZBLAN. Therefore, the working temperature range for ZBLAN has been broadened. (C) 2014 Society of Photo-Optical Instrumentation Engineers (SPIE) C1 [Torres, Anthony] Texas State Univ, Dept Engn Technol, San Marcos, TX 78666 USA. [Ganley, Jeff] Air Force Res Lab, Space Vehicles Directorate, Albuquerque, NM 87117 USA. [Maji, Arup] Univ New Mexico, Dept Civil Engn, Albuquerque, NM 87106 USA. [Tucker, Dennis] NASA MSFC, Huntsville, AL 35812 USA. [Starodubov, Dmitry] Phys Opt Corp, Torrance, CA 90501 USA. RP Torres, A (reprint author), Texas State Univ, Dept Engn Technol, San Marcos, TX 78666 USA. EM ast36@txstate.edu NR 9 TC 4 Z9 4 U1 0 U2 2 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 0091-3286 EI 1560-2303 J9 OPT ENG JI Opt. Eng. PD MAR PY 2014 VL 53 IS 3 AR 036103 DI 10.1117/1.OE.53.3.036103 PG 9 WC Optics SC Optics GA AM1QT UT WOS:000339623600033 ER PT J AU Gao, RS Rosenlof, KH Fahey, DW Wennberg, PO Hintsa, EJ Hanisco, TF AF Gao, R. S. Rosenlof, K. H. Fahey, D. W. Wennberg, P. O. Hintsa, E. J. Hanisco, T. F. TI OH in the tropical upper troposphere and its relationships to solar radiation and reactive nitrogen SO JOURNAL OF ATMOSPHERIC CHEMISTRY LA English DT Article DE OH; In situ; Tropical upper troposphere; STRAT ID AIRCRAFT EXHAUST PLUMES; IN-SITU OBSERVATIONS; LOWER STRATOSPHERE; HYDROGEN RADICALS; NASA ER-2; HYDROXYL; PACIFIC; HOX; O-3; INSTRUMENT AB In situ measurements of [OH], [HO2] (square brackets denote species concentrations), and other chemical species were made in the tropical upper troposphere (TUT). [OH] showed a robust correlation with solar zenith angle. Beyond this dependence, however, [OH] did not correlate to its primary source, the product of [O-3] and [H2O] ([O-3]aEuro cent[H2O]), or its sink [NOy]. This suggests that [OH] is heavily buffered in the TUT. One important exception to this result is found in regions with very low [O-3], [NO], and [NOy]. Under these conditions, [OH] is highly suppressed, pointing to the critical role of NO in sustaining OH in the TUT and the possibility of low [OH] over the western Pacific warm pool due to strong marine convections bringing NO-poor air to the TUT. In contrast to [OH], [HOx] ([OH] + [HO2]) correlated reasonably well with [O-3]aEuro cent[H2O]/[NOy], suggesting that [O-3]aEuro cent[H2O] and [NOy] are the significant source and sink, respectively, of [HOx]. C1 [Gao, R. S.; Rosenlof, K. H.; Fahey, D. W.] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA. [Fahey, D. W.; Hintsa, E. J.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Wennberg, P. O.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Wennberg, P. O.] CALTECH, Div Appl Sci, Pasadena, CA 91125 USA. [Hintsa, E. J.] NOAA, Global Monitoring Div, Earth Syst Res Lab, Boulder, CO 80305 USA. [Hanisco, T. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gao, RS (reprint author), NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA. EM RuShan.Gao@noaa.gov RI Rosenlof, Karen/B-5652-2008; Gao, Ru-Shan/H-7455-2013; Fahey, David/G-4499-2013; Manager, CSD Publications/B-2789-2015 OI Rosenlof, Karen/0000-0002-0903-8270; Fahey, David/0000-0003-1720-0634; FU NOAA Atmospheric Composition and Climate Program; NOAA Health of the Atmosphere Program; NASA Radiation Sciences Program; NASA Upper Atmosphere Research Program FX This work was supported by the NOAA Atmospheric Composition and Climate Program and the NOAA Health of the Atmosphere Program, the NASA Radiation Sciences Program, and the NASA Upper Atmosphere Research Program. We would like to thank the NASA ER-2 program for making the mission possible. We thank M. Rex and L. L. Pan for insightful discussions. NR 29 TC 5 Z9 5 U1 1 U2 14 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-7764 EI 1573-0662 J9 J ATMOS CHEM JI J. Atmos. Chem. PD MAR PY 2014 VL 71 IS 1 BP 55 EP 64 DI 10.1007/s10874-014-9280-2 PG 10 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AK8FA UT WOS:000338661500004 ER PT J AU Wolkovich, EM Cook, BI Davies, TJ AF Wolkovich, Elizabeth M. Cook, Benjamin I. Davies, T. Jonathan TI Progress towards an interdisciplinary science of plant phenology: building predictions across space, time and species diversity SO NEW PHYTOLOGIST LA English DT Review DE climate change; cues; investment; local adaptation; phenology; plant ecology; plasticity; risk ID CLIMATE-CHANGE; FLOWERING PHENOLOGY; PHENOTYPIC PLASTICITY; ADAPTIVE EVOLUTION; INVASIVE PLANT; GLOBAL CHANGE; RESPONSES; POLLINATORS; COMPETITION; EUROPE AB Climate change has brought renewed interest in the study of plant phenology - the timing of life history events. Data on shifting phenologies with warming have accumulated rapidly, yet research has been comparatively slow to explain the diversity of phenological responses observed across latitudes, growing seasons and species. Here, we outline recent efforts to synthesize perspectives on plant phenology across the fields of ecology, climate science and evolution. We highlight three major axes that vary among these disciplines: relative focus on abiotic versus biotic drivers of phenology, on plastic versus genetic drivers of intraspecific variation, and on cross-species versus autecological approaches. Recent interdisciplinary efforts, building on data covering diverse species and climate space, have found a greater role of temperature in controlling phenology at higher latitudes and for early-flowering species in temperate systems. These efforts have also made progress in understanding the tremendous diversity of responses across species by incorporating evolutionary relatedness, and linking phenological flexibility to invasions and plant performance. Future research with a focus on data collection in areas outside the temperate mid-latitudes and across species' ranges, alongside better integration of how risk and investment shape plant phenology, offers promise for further progress. C1 [Wolkovich, Elizabeth M.] Univ British Columbia, Biodivers Res Ctr, Vancouver, BC V6T 1Z4, Canada. [Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Cook, Benjamin I.] Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Davies, T. Jonathan] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. RP Wolkovich, EM (reprint author), Univ British Columbia, Biodivers Res Ctr, Vancouver, BC V6T 1Z4, Canada. EM lizzie@biodiversity.ubc.ca RI Cook, Benjamin/H-2265-2012 NR 52 TC 21 Z9 23 U1 10 U2 107 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0028-646X EI 1469-8137 J9 NEW PHYTOL JI New Phytol. PD MAR PY 2014 VL 201 IS 4 BP 1156 EP 1162 DI 10.1111/nph.12599 PG 7 WC Plant Sciences SC Plant Sciences GA AK6AS UT WOS:000338510200011 PM 24649487 ER PT J AU Drummond, JP AF Drummond, J. Philip TI Methods for Prediction of High-Speed Reacting Flows in Aerospace Propulsion SO AIAA JOURNAL LA English DT Article ID FILTERED DENSITY-FUNCTION; FLUX-CORRECTED TRANSPORT; NAVIER-STOKES EQUATIONS; SUPERSONIC CROSS-FLOW; LARGE-EDDY SIMULATION; TURBULENT FLOWS; PDF METHODS; COMBUSTION; INJECTION; MODEL C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Drummond, JP (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 175 TC 4 Z9 4 U1 0 U2 4 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 MAR PY 2014 VL 52 IS 3 BP 465 EP 485 DI 10.2514/1.J052283 PG 21 WC Engineering, Aerospace SC Engineering GA AJ6IQ UT WOS:000337796100001 ER PT J AU Glaze, LS Baloga, SM Fagents, SA Wright, R AF Glaze, Lori S. Baloga, Stephen M. Fagents, Sarah A. Wright, Robert TI The influence of slope breaks on lava flow surface disruption SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID EMPLACEMENT; PAHOEHOE; ERUPTION; HAWAII; VOLCANO; CHANNEL; SHEET; MODEL; AA AB Changes in the underlying slope of a lava flow impart a significant fraction of rotational energy beyond the slope break. The eddies, circulation, and vortices caused by this rotational energy can disrupt the flow surface, having a significant impact on heat loss and thus the distance the flow can travel. A basic mechanics model is used to compute the rotational energy caused by a slope change. The gain in rotational energy is deposited into an eddy of radius R whose energy is dissipated as it travels downstream. A model of eddy friction with the ambient lava is used to compute the time-rate of energy dissipation. The key parameter of the dissipation rate is shown to be rho R-2/mu, where rho is the lava density and mu is the viscosity, which can vary by orders of magnitude for different flows. The potential spatial disruption of the lava flow surface is investigated by introducing steady state models for the main flow beyond the steepening slope break. One model applies to slow-moving flows with both gravity and pressure as the driving forces. The other model applies to fast-moving, low-viscosity, turbulent flows. These models provide the flow velocity that establishes the downstream transport distance of disrupting eddies before they dissipate. The potential influence of slope breaks is discussed in connection with field studies of lava flows from the 1801 Hualalai and 1823 Keaiwa Kilauea, Hawaii, and 2004 Etna eruptions. C1 [Glaze, Lori S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Baloga, Stephen M.] Proxemy Res, Gaithersburg, MD USA. [Fagents, Sarah A.; Wright, Robert] Univ Hawaii Manoa, HIGP, Honolulu, HI 96822 USA. RP Glaze, LS (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Lori.S.Glaze@nasa.gov RI Glaze, Lori/D-1314-2012 FU NASA [NNX10AP63G, NNXAR10G, WBS 811073.02.01.05.80] FX Work performed by S. M. B., and L.S.G. was sponsored by NASA grants NNX10AP63G and NNXAR10G. L.S.G. also acknowledges partial support from the NASA Planetary Geology and Geophysics program (WBS 811073.02.01.05.80). NR 31 TC 1 Z9 1 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD MAR PY 2014 VL 119 IS 3 BP 1837 EP 1850 DI 10.1002/2013JB010696 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AI4OM UT WOS:000336844700018 ER PT J AU Jolivet, R Agram, PS Lin, NNY Simons, M Doin, MP Peltzer, G Li, ZH AF Jolivet, Romain Agram, Piyush Shanker Lin, Nina Y. Simons, Mark Doin, Marie-Pierre Peltzer, Gilles Li, Zhenghong TI Improving InSAR geodesy using Global Atmospheric Models SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID SATELLITE RADAR INTERFEROMETRY; 7.1 HECTOR MINE; MOUNT-ETNA; INTERSEISMIC STRAIN; SAR INTERFEROGRAMS; SUBDUCTION ZONE; GPS; FAULT; EARTHQUAKE; WATER AB Spatial and temporal variations of pressure, temperature, and water vapor content in the atmosphere introduce significant confounding delays in interferometric synthetic aperture radar (InSAR) observations of ground deformation and bias estimates of regional strain rates. Producing robust estimates of tropospheric delays remains one of the key challenges in increasing the accuracy of ground deformation measurements using InSAR. Recent studies revealed the efficiency of global atmospheric reanalysis to mitigate the impact of tropospheric delays, motivating further exploration of their potential. Here we explore the effectiveness of these models in several geographic and tectonic settings on both single interferograms and time series analysis products. Both hydrostatic and wet contributions to the phase delay are important to account for. We validate these path delay corrections by comparing with estimates of vertically integrated atmospheric water vapor content derived from the passive multispectral imager Medium-Resolution Imaging Spectrometer, onboard the Envisat satellite. Generally, the performance of the prediction depends on the vigor of atmospheric turbulence. We discuss (1) how separating atmospheric and orbital contributions allows one to better measure long-wavelength deformation and (2) how atmospheric delays affect measurements of surface deformation following earthquakes, and (3) how such a method allows us to reduce biases in multiyear strain rate estimates by reducing the influence of unevenly sampled seasonal oscillations of the tropospheric delay. C1 [Jolivet, Romain; Lin, Nina Y.; Simons, Mark] CALTECH, Dept Geol & Planetary Sci, Seismol Lab, Pasadena, CA 91125 USA. [Agram, Piyush Shanker; Peltzer, Gilles] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Doin, Marie-Pierre] Univ Grenoble Alpes, ISTerre, Grenoble, France. [Doin, Marie-Pierre] CNRS, ISTerre, Grenoble, France. [Peltzer, Gilles] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. [Li, Zhenghong] Univ Glasgow, Sch Geog & Earth Sci, COMET, Glasgow G12 8QQ, Lanark, Scotland. RP Jolivet, R (reprint author), CALTECH, Dept Geol & Planetary Sci, Seismol Lab, Pasadena, CA 91125 USA. EM rjolivet@caltech.edu RI Li, Zhenhong/F-8705-2010; Simons, Mark/N-4397-2015; OI Li, Zhenhong/0000-0002-8054-7449; Simons, Mark/0000-0003-1412-6395; Jolivet, Romain/0000-0002-9896-3651 FU NSF [EAR-1118239] FX We would like to thank two anonymous reviewers for their fruitful comments and suggestions and the Associate Editor for his help in evaluating this paper. We also would like to thank Simona Bordoni (Caltech) for all the discussions about the Global Atmospheric Models used in this study. Part of G. Peltzer's contribution was done at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Figures and maps were prepared using Generic Mapping Tools software [Wessel and Smith, 1995]. This study has been funded by NSF grant EAR-1118239. This is Caltech Seismo lab contribution 10096. This is TO contribution 252. NR 65 TC 35 Z9 36 U1 2 U2 26 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD MAR PY 2014 VL 119 IS 3 BP 2324 EP 2341 DI 10.1002/2013JB010588 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AI4OM UT WOS:000336844700043 ER PT J AU Chudnovsky, A Lyapustin, A Wang, Y Tang, C Schwartz, J Koutrakis, P AF Chudnovsky, A. Lyapustin, A. Wang, Y. Tang, C. Schwartz, J. Koutrakis, P. TI High resolution aerosol data from MODIS satellite for urban air quality studies SO CENTRAL EUROPEAN JOURNAL OF GEOSCIENCES LA English DT Article DE Remote Sensing; PM2.5 exposure assessment; urban air quality; Aerosol Optical Depth; MODIS; MAIAC; mixed effects model ID OPTICAL DEPTH; PARTICULATE; POLLUTION; PARTICLES; EXPOSURE; SPACE; PM2.5 AB The Moderate Resolution Imaging Spectroradiometer (MODIS) provides daily global coverage, but the 10 km resolution of its aerosol optical depth (AOD) product is not suitable for studying spatial variability of aerosols in urban areas. Recently, a new Multi-Angle Implementation of Atmospheric Correction (MAIAC) algorithm was developed for MODIS which provides AOD at 1 km resolution. Using MAIAC data, the relationship between MAIAC AOD and PM2.5 as measured by the 27 EPA ground monitoring stations was investigated. These results were also compared to conventional MODIS 10 km AOD retrievals (MOD04) for the same days and locations. The coefficients of determination for MOD04 and for MAIAC are R-2 =0.45 and 0.50 respectively, suggested that AOD is a reasonably good proxy for PM2.5 ground concentrations. Finally, we studied the relationship between PM2.5 and AOD at the intra-urban scale (a (c) 1/210 km) in Boston. The fine resolution results indicated spatial variability in particle concentration at a sub-10 kilometer scale. A local analysis for the Boston area showed that the AOD-PM2.5 relationship does not depend on relative humidity and air temperatures below similar to 7 A degrees C. The correlation improves for temperatures above 7-16 A degrees C. We found no dependence on the boundary layer height except when the former was in the range 250-500 m. Finally, we apply a mixed effects model approach to MAIAC aerosol optical depth (AOD) retrievals from MODIS to predict PM2.5 concentrations within the greater Boston area. With this approach we can control for the inherent day-to-day variability in the AOD-PM2.5 relationship, which depends on time-varying parameters such as particle optical properties, vertical and diurnal concentration profiles and ground surface reflectance. Our results show that the model-predicted PM2.5 mass concentrations are highly correlated with the actual observations (out-of-sample R-2 of 0.86). Therefore, adjustment for the daily variability in the AOD-PM2.5 relationship provides a means for obtaining spatially-resolved PM2.5 concentrations. C1 [Chudnovsky, A.; Tang, C.; Schwartz, J.; Koutrakis, P.] Harvard Univ, Sch Publ Hlth, Dept Environm Hlth, Boston, MA 02115 USA. [Chudnovsky, A.] Tel Aviv Univ, Dept Geog & Human Environm, IL-69978 Tel Aviv, Israel. [Lyapustin, A.] NASA, GEST, UMBC, Goddard Space Flight Ctr, Baltimore, MD USA. [Wang, Y.] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. RP Chudnovsky, A (reprint author), Harvard Univ, Sch Publ Hlth, Dept Environm Hlth, Boston, MA 02115 USA. EM achudnov@hsph.harvard.edu; alexei.i.lyapustin@nasa.gov; yujie.wang-1@nasa.gov; cht710@mail.harvard.edu; joel@hsph.harvard.edu; petros@hsph.harvard.edu RI Lyapustin, Alexei/H-9924-2014 OI Lyapustin, Alexei/0000-0003-1105-5739 FU USEPA [RD 83479801] FX This work was made possible by USEPA grant RD 83479801. Its contents are solely the responsibility of the grantee and do not necessarily represent the official views of the USEPA. Further, USEPA does not endorse the purchase of any commercial products or services mentioned in the publication. Authors greatly appreciate inspiring discussions with Prof. Alex Kostinski from Michigan Technological University, USA. Authors greatly appreciate important comments of Dr. Mike Wolfson. NR 19 TC 2 Z9 2 U1 2 U2 20 PU DE GRUYTER OPEN LTD PI WARSAW PA BOGUMILA ZUGA 32A ST, 01-811 WARSAW, POLAND SN 2081-9900 EI 1896-1517 J9 CENT EUR J GEOSCI JI Cent. Eur. J. Geosci. PD MAR PY 2014 VL 6 IS 1 BP 17 EP 26 DI 10.2478/s13533-012-0145-4 PG 10 WC Geosciences, Multidisciplinary SC Geology GA AI3AT UT WOS:000336731500003 ER PT J AU Christian, JA Robinson, SB D'Souza, CN Ruiz, JP AF Christian, John A. Robinson, Shane B. D'Souza, Christopher N. Ruiz, Jose P. TI Cooperative Relative Navigation of Spacecraft Using Flash Light Detection and Ranging Sensors SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID ANGLES-ONLY NAVIGATION; POSE ESTIMATION; ATTITUDE DETERMINATION; VECTOR OBSERVATIONS; SET UNION; ALGORITHMS; VISION; OPENINGS; IMAGES; OPTIMIZATION AB Autonomous rendezvous and docking of a spacecraft with a cooperative target vehicle is critical for a wide array of future mission applications, and flash light detection and ranging sensors are one of the most promising sensors for achieving this task. This paper presents an end-to-end assessment of how these sensors may be used for relative navigation. Within a unified framework, detailed discussions are provided on the topics of navigation architecture, flash light detection and ranging sensors measurements and image processing, reflector identification, and the estimation of relative position and attitude. C1 [Christian, John A.; Robinson, Shane B.; D'Souza, Christopher N.; Ruiz, Jose P.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Christian, JA (reprint author), W Virginia Univ, Dept Mech & Aerosp Engn, Morgantown, WV 26506 USA. EM john.christian@mail.wvu.edu NR 76 TC 6 Z9 7 U1 1 U2 9 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD MAR-APR PY 2014 VL 37 IS 2 BP 452 EP 465 DI 10.2514/1.61234 PG 14 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA AI3OX UT WOS:000336772900009 ER PT J AU Donnellan, A Parker, J Hensley, S Pierce, M Wang, J Rundle, J AF Donnellan, Andrea Parker, Jay Hensley, Scott Pierce, Marlon Wang, Jun Rundle, John TI UAVSAR observations of triggered slip on the Imperial, Superstition Hills, and East Elmore Ranch Faults associated with the 2010 M 7.2 El Mayor-Cucapah earthquake SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS LA English DT Article DE UAVSAR; crustal deformation; El Mayor-Cucapah earthquake; InSAR; fault slip ID SOUTHERN-CALIFORNIA; PATTERN INFORMATICS; THRESHOLD SYSTEMS; DYNAMICS AB The 4 April 2010 M 7.2 El Mayor-Cucapah earthquake that occurred in Baja California, Mexico and terminated near the U.S. Mexican border caused slip on the Imperial, Superstition Hills, and East Elmore Ranch Faults. The pattern of slip was observed using radar interferometry from NASA's Uninhabited Aerial Vehicle Synthetic Aperture Radar (UAVSAR) instrument collected on 20-21 October 2009 and 12-13 April 2010. Right-lateral slip of 369 and 142 mm occurred on the Imperial and Superstition Hills Faults, respectively. Left-lateral slip of 92 mm occurred on the East Elmore Ranch Fault. The widths of the zones of displacement increase northward suggesting successively more buried fault motion to the north. The observations show a decreasing pattern of slip northward on a series of faults in the Salton Trough stepping between the El Mayor-Cucapah rupture and San Andreas Fault. Most of the motion occurred at the time of the M 7.2 earthquake and the UAVSAR observations are consistent with field, creepmeter, GPS, and Envisat observations. An additional 281 mm of slip at the southern end of the Imperial Fault over a <1 km wide zone was observed over a 1 day span a week after the earthquake suggesting that the fault continued to slip at depth following the mainshock. The total moment release on the three faults is 2.3 x 10(23)-1.2 x 10(24) dyne cm equivalent to a moment magnitude release of 4.9-5.3, assuming shallow slip depths ranging from 1 to 5 km. C1 [Donnellan, Andrea; Parker, Jay; Hensley, Scott] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Donnellan, Andrea] Univ So Calif, Los Angeles, CA USA. [Pierce, Marlon; Wang, Jun] Indiana Univ, Res Technol Div, Bloomington, IN USA. [Rundle, John] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Rundle, John] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. RP Donnellan, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Andrea.Donnellan@jpl.nasa.gov OI Pierce, Marlon/0000-0002-9582-5712 NR 27 TC 3 Z9 3 U1 0 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1525-2027 J9 GEOCHEM GEOPHY GEOSY JI Geochem. Geophys. Geosyst. PD MAR PY 2014 VL 15 IS 3 BP 815 EP 829 DI 10.1002/2013GC005120 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AH6HZ UT WOS:000336232600018 ER PT J AU Firing, YL Chereskin, TK Watts, DR Tracey, KL Provost, C AF Firing, Y. L. Chereskin, T. K. Watts, D. R. Tracey, K. L. Provost, C. TI Computation of Geostrophic Streamfunction, Its Derivatives, and Error Estimates from an Array of CPIES in Drake Passage SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article DE Southern Ocean; Advection; Currents; Streamfunction; Acoustic measurements; effects; In situ oceanic observations ID INVERTED ECHO SOUNDERS; ANTARCTIC CIRCUMPOLAR CURRENT; DOPPLER CURRENT PROFILERS; GRAVEST EMPIRICAL MODE; GULF-STREAM; ABSOLUTE VELOCITY; SOUTHERN-OCEAN; TRANSPORT; ATLANTIC; FIELDS AB Current and pressure-recording inverted echo sounders (CPIES) were deployed in an eddy-resolving local dynamics array (LDA) in the eddy-rich polar frontal zone (PFZ) in Drake Passage as part of the cDrake experiment. Methods are described for calculating barotropic and baroclinic geostrophic streamfunction and its first, second, and third derivatives by objective mapping of current, pressure, or geopotential height anomaly data from a two-dimensional array of CPIES like the cDrake LDA.Modifications to previous methods result in improved dimensional error estimates on velocity and higher streamfunction derivatives. Simulations are used to test the reproduction of higher derivatives of streamfunction and to verify mapping error estimates. Three-day low-pass-filtered velocity in and around the cDrake LDA can be mapped with errors of 0.04 m s(-1) at 4000 dbar, increasing to 0.13 m s(-1) at the sea surface; these errors are small compared to typical speeds observed at these levels, 0.2 and 0.65 m s(-1), respectively. Errors on vorticity are 9 x 10(-6) s(-1) near the surface, decreasing with depth to 3 x 10(-6) s(-1) at 4000 dbar, whereas vorticities in the PFZ eddy field are 4 x 10(-5) s(-1) (surface) to 1.3 x 10(-5) s(-1) (4000 dbar). Vorticity gradient errors range from 4 x 10(-10) to 2 x 10(-10) m (-1) s(-1), just under half the size of typical PFZ vorticity gradients. Comparisons between cDrake mapped temperature and velocity fields and independent observations (moored current and temperature, lowered acoustic Doppler current profiler velocity, and satellite-derived surface currents) help validate the cDrake method and results. C1 [Firing, Y. L.; Chereskin, T. K.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Watts, D. R.; Tracey, K. L.] Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA. [Provost, C.] Univ Paris 06, CNRS, UMR 7159, LOCEAN,IRD,MNHN, Paris, France. RP Firing, YL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 233-305, Pasadena, CA 91109 USA. EM yfiring@caltech.edu OI Firing, Yvonne/0000-0002-3640-3974 FU National Science Foundation Office of Polar Programs under NSF [ANT-0636493, ANT-0635437]; NASA Earth Systems Science Fellowship [NNX09AN87H] FX We are particularly grateful to Kathleen Donohue for coleading the cDrake project and for providing extensive advice on numerous issues in this manuscript. The optimal interpolation codes developed for this work build on earlier codes developed by Xiaoshu Qian and Christopher Meinen. The LADCP data were processed using publicly available software, and we are grateful to the software developers and maintainers: E. Firing, M. Visbeck, A. Thurnherr, and G. Krahmann. XCTD data were provided by J. Sprintall. The National Science Foundation Office of Polar Programs supported this work under NSF Grants ANT-0636493 (SIO cDrake) and ANT-0635437 (URI cDrake). Y. Firing was supported by NASA Earth Systems Science Fellowship NNX09AN87H. We thank G. Chaplin, S. Escher, D. Holloway, E. Sousa, the captains and crew of the RVIB Nathaniel B. Palmer, and Raytheon Polar Services for technical and logistical support during the cDrake cruises. NR 36 TC 10 Z9 10 U1 0 U2 1 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD MAR PY 2014 VL 31 IS 3 BP 656 EP 680 DI 10.1175/JTECH-D-13-00142.1 PG 25 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA AH6EF UT WOS:000336222800008 ER PT J AU Omidi, N Isenberg, P Russell, CT Jian, LK Wei, HY AF Omidi, N. Isenberg, P. Russell, C. T. Jian, L. K. Wei, H. Y. TI Generation of ion cyclotron waves in the corona and solar wind SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MINOR IONS; PREFERENTIAL ACCELERATION; KINETIC DISSIPATION; INVERSE CORRELATION; MAGNETIC HELICITY; 1 AU; TURBULENCE; INSTABILITY; ANISOTROPY; VELOCITY AB To examine the generation and nonlinear evolution of ion cyclotron waves in the corona and solar wind, we perform electromagnetic simulations using a wide range of plasma conditions and ion velocity distribution functions. The source of the instability is temperature anisotropy of ions with temperature perpendicular to the magnetic field larger than parallel. For velocity distribution we use Maxwellian, bi-Maxwellian, and Fermi-accelerated functions with perpendicular temperature larger than parallel with the aim to understand the extent to which the details of the distribution function impact the general properties and the nonlinear evolution of the instability. The results show that in a proton-electron plasma, ion cyclotron waves are generated over a wide range of temperature anisotropies and plasma beta. Also, the general properties of the instability and the nonlinear evolution of the waves are not sensitive to the details of the velocity distribution functions. Allowing for the presence of minor ion species we show that these ions by themselves can drive the instability and generate waves with frequencies below the gyrofrequency of the minor ions. In the event that protons also have temperature anisotropy, waves on the proton branch are also generated. Results using bi-Maxwellian or Fermi-accelerated velocity distribution functions show similar properties for the instability and the nonlinear evolution of the waves. However, differences are found when allowing for relative drifts between the protons and minor ions in that when using Fermi-accelerated distribution functions oblique ion cyclotron waves are generated that are not observed in simulations using bi-Maxwellian distribution function. C1 [Omidi, N.] Solana Sci Inc, Solana Beach, CA 92075 USA. [Isenberg, P.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Russell, C. T.; Wei, H. Y.] Univ Calif Los Angeles, IGPP, Los Angeles, CA USA. [Jian, L. K.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Jian, L. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Omidi, N (reprint author), Solana Sci Inc, Solana Beach, CA 92075 USA. EM omidi@solanasci.com RI Jian, Lan/B-4053-2010 OI Jian, Lan/0000-0002-6849-5527 FU NASA [NNX12AB29G, NNX13AI65G, NNX11AJ37G, NNX13AF97G]; NSF SHINE [AGS0962506] FX Work for this project was supported by NASA grants NNX12AB29G, NNX13AI65G, NNX11AJ37G, and NNX13AF97G and NSF SHINE grant AGS0962506. NR 52 TC 10 Z9 10 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAR PY 2014 VL 119 IS 3 BP 1442 EP 1454 DI 10.1002/2013JA019474 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6CM UT WOS:000336218300003 ER PT J AU Lee, SH Zhang, H Zong, QG Otto, A Sibeck, DG Wang, Y Glassmeier, KH Daly, PW Reme, H AF Lee, S. H. Zhang, H. Zong, Q. -G. Otto, A. Sibeck, D. G. Wang, Y. Glassmeier, K. -H. Daly, P. W. Reme, H. TI Plasma and energetic particle behaviors during asymmetric magnetic reconnection at the magnetopause SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID LATITUDE BOUNDARY-LAYER; ACCELERATED FLOW EVENTS; EARTHS MAGNETOSPHERE; DAYSIDE MAGNETOSHEATH; OXYGEN IONS; CLUSTER; FIELD; CONVECTION; WAVES; EDGE AB The factors controlling asymmetric reconnection and the role of the cold plasma population in the reconnection process are two outstanding questions. We present a case study of multipoint Cluster observations demonstrating that the separatrix and flow boundary angles are greater on the magnetosheath than on the magnetospheric side of the magnetopause, probably due to the stronger density than magnetic field asymmetry at this boundary. The motion of cold plasmaspheric ions entering the reconnection region differs from that of warmer magnetosheath and magnetospheric ions. In contrast to the warmer ions, which are probably accelerated by reconnection in the diffusion region near the subsolar magnetopause, the colder ions are simply entrained by E x B drifts at high latitudes on the recently reconnected magnetic field lines. This indicates that plasmaspheric ions can sometimes play only a very limited role in asymmetric reconnection, in contrast to previous simulation studies. Three cold ion populations (probably H+, He+, and O+) appear in the energy spectrum, consistent with ion acceleration to a common velocity. C1 [Lee, S. H.; Zhang, H.; Otto, A.] Univ Alaska, Inst Geophys, Fairbanks, AK 99775 USA. [Zong, Q. -G.; Wang, Y.] Peking Univ, Inst Space Phys & Appl Technol, Sch Earth & Space Sci, Beijing 100871, Peoples R China. [Sibeck, D. G.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Glassmeier, K. -H.] Inst Geophys & Extraterr Phys, Braunschweig, Germany. [Daly, P. W.] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany. [Reme, H.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Reme, H.] CNRS, IRAP, Toulouse, France. RP Zhang, H (reprint author), Univ Alaska, Inst Geophys, Fairbanks, AK 99775 USA. EM hzhang@gi.alaska.edu FU German Bundesministerium fur Wirtschaft und Technologie [50OC1102, 50OC1001]; Deutsches Zentrum fur Luft- und Raumfahrt FX We thank all of those who have made the Cluster mission for the successful spacecraft operation and for the high-quality data. This work was carried out while S. H. Lee held a NASA Earth and Space Science Fellowship. K. H. G. was financially supported through grants 50OC1102 and 50OC1001 by the German Bundesministerium fur Wirtschaft und Technologie and the Deutsches Zentrum fur Luft- und Raumfahrt. NR 45 TC 13 Z9 13 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAR PY 2014 VL 119 IS 3 BP 1658 EP 1672 DI 10.1002/2013JA019168 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6CM UT WOS:000336218300022 ER PT J AU Chu, XN Hsu, TS McPherron, RL Angelopoulos, V Pu, ZY Weygand, JJ Khurana, K Connors, M Kissinger, J Zhang, H Amm, O AF Chu, Xiangning Hsu, Tung-Shin McPherron, Robert L. Angelopoulos, Vassilis Pu, Zuyin Weygand, James J. Khurana, Krishan Connors, Martin Kissinger, Jennifer Zhang, Hui Amm, Olaf TI Development and validation of inversion technique for substorm current wedge using ground magnetic field data SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ELEMENTARY CURRENT SYSTEMS; MAGNETOSPHERIC SUBSTORMS; CURRENT DISRUPTION; IMAGE-FUV; POLAR ELECTROJETS; TAIL RECONNECTION; ALIGNED CURRENT; CURRENT MODEL; ONSET; MAGNETOTAIL AB The classic substorm current wedge model represents ground and space magnetic perturbations measured during substorms. We have developed an inversion technique to calculate parameters determining the intensity and geometry of the current system using magnetic field data at midlatitudes. The current wedge consists of four segments: a sheet-like field-aligned current downward to the ionosphere postmidnight, a westward current across the auroral bulge, an upward sheet-like current from the westward surge premidnight, and an eastward current in the equatorial plane. The model has five parameters including the current strength, the locations, and breadths of the two field-aligned current sheets. Simultaneous changes in the ring current are represented by the superposition of a symmetric ring current and a partial ring current characterized by three additional parameters. Parameters of the model are determined as a function of time based on midlatitude ground magnetometers, using realistic field lines and accounting for Earth's induction. The model is validated by a variety of techniques. First, the model predicts more than 80% of the variance in the observations. Second, the intensity of the current wedge and the ring current follows the same trends of the westward electrojet and the ring current indices. Third, the intensity of the westward electrojet agrees extremely well with the intensity of the current wedge. Finally, spacecraft observations of the aurora correspond with the evolution deduced from the model. This model of the substorm current wedge provides a valuable tool for the study of substorm development and its relation to phenomena in space. C1 [Chu, Xiangning; Hsu, Tung-Shin; McPherron, Robert L.; Angelopoulos, Vassilis; Weygand, James J.; Khurana, Krishan] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. [Chu, Xiangning; Hsu, Tung-Shin; McPherron, Robert L.; Angelopoulos, Vassilis; Weygand, James J.; Khurana, Krishan] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Pu, Zuyin] Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China. [Connors, Martin] Athabasca Univ, Geophys Observ, Athabasca, AB, Canada. [Kissinger, Jennifer] NASA, Goddard Space Flight Ctr, College Pk, MD USA. [Zhang, Hui] Chinese Acad Sci, Inst Geol & Geophys, Beijing, Peoples R China. [Amm, Olaf] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. RP Chu, XN (reprint author), Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. EM xnchu@igpp.ucla.edu FU NASA [NNX10AE61G]; NSF [AGS-1003854] FX Support for this project was provided by NASA grant NNX10AE61G and NSF grant AGS-1003854. The authors would like to thank the NASA NSSDC and IMAGE FUV team and Harald Frey for data processing and advice. We gratefully acknowledge INTERMAGNET (www.intermagnet.org), SuperMAG (supermag.jhuapl.edu/), and their data providers. The IMAGE magnetometer network is an international project coordinated by the Finnish Meteorological Institute (www.geo.fmi.fi/image/). NR 71 TC 12 Z9 12 U1 2 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAR PY 2014 VL 119 IS 3 BP 1909 EP 1924 DI 10.1002/2013JA019185 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6CM UT WOS:000336218300041 ER PT J AU Santos, JC Sibeck, DG Buchner, J Gonzalez, WD Ferreira, JL AF Santos, J. C. Sibeck, D. G. Buechner, J. Gonzalez, W. D. Ferreira, J. L. TI Three-dimensional MHD simulation of FTEs produced by merging at an isolated point in a sheared magnetic field configuration SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID FLUX-TRANSFER EVENTS; SINGLE X LINE; RECONNECTION; FLOW; MAGNETOPAUSE; PLASMA; ONSET; MAGNETOSPHERE; GENERATION; VELOCITIES AB We present predictions for the evolution of FTEs generated by localized bursts of reconnection on a planar magnetopause that separates a magnetosheath region of high densities and weak magnetic field from a magnetospheric region of low densities and strong magnetic field. The magnetic fields present a shear angle of 105 degrees. Reconnection forms a pair of FTEs each crossing the magnetopause in the field reversal region and bulging into the magnetosphere and magnetosheath. At their initial stage they can be characterized as flux tubes since the newly reconnected magnetic field lines are not twisted. Reconnection launches Alfvenic perturbations that propagate along the FTEs generating high-speed jets, which move the pair of FTEs in opposite directions. As the FTE moves, it displaces the ambient magnetic field and plasma producing bipolar magnetic field and plasma velocity signatures normal to the nominal magnetopause in the regions surrounding the FTE. The combination of the ambient plasma with the FTE flows generates a vortical velocity pattern around the reconnected field lines. During its evolution the FTE evolves to a flux rope configuration due to the twist of the magnetic field lines. The alfvenic perturbations propagate faster along the part of the FTE bulging into the magnetosphere than in the magnetosheath, and due to the differences between the plasma and magnetic field properties the perturbations have slightly different signatures in the two regions. As a consequence, the FTEs have different signatures depending on whether the satellite encounters the part bulging into the magnetosphere or into the magnetosheath. C1 [Santos, J. C.; Ferreira, J. L.] Univ Brasilia, Inst Fis, Brasilia, DF, Brazil. [Santos, J. C.] Univ Tecnol Fed Parana, Dept Fis, Curitiba, Parana, Brazil. [Sibeck, D. G.] NASA GSFC, Greenbelt, MD USA. [Buechner, J.] Max Planck Inst Sonnensyst Forsch, Katlenburg Lindau, Germany. [Gonzalez, W. D.] Inst Nacl Pesquisas Espaciais, BR-12201 Sao Jose Dos Campos, Brazil. RP Santos, JC (reprint author), Univ Brasilia, Inst Fis, Brasilia, DF, Brazil. EM jeansantos@unb.br FU DPP/UnB; CNPq [482351/2012-8]; THEMIS Explorer Mission FX This work was supported by the DPP/UnB and CNPq under the project 482351/2012-8. Work at NASA/GSFC was supported by the THEMIS Explorer Mission. NR 34 TC 0 Z9 0 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAR PY 2014 VL 119 IS 3 BP 2009 EP 2023 DI 10.1002/2013JA018964 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6CM UT WOS:000336218300047 ER PT J AU Janches, D Hocking, W Pifko, S Hormaechea, JL Fritts, DC Brunini, C Michell, R Samara, M AF Janches, D. Hocking, W. Pifko, S. Hormaechea, J. L. Fritts, D. C. Brunini, C. Michell, R. Samara, M. TI Interferometric meteor head echo observations using the Southern Argentina Agile Meteor Radar SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID LARGE-APERTURE RADARS; 430 MHZ RADAR; HIGH-POWER; MU RADAR; VELOCITY DISTRIBUTION; RADIANT DISTRIBUTION; UPPER-ATMOSPHERE; HIGH-RESOLUTION; INPUT FUNCTION; SOLAR-SYSTEM AB A radar meteor echo is the radar scattering signature from the free electrons generated by the entry of extraterrestrial particles into the atmosphere. Three categories of scattering mechanisms exist: specular, nonspecular trails, and head echoes. Generally, there are two types of radars utilized to detect meteors. Traditional VHF all-sky meteor radars primarily detect the specular trails, while high-power, large-aperture (HPLA) radars efficiently detect meteor head echoes and, in some cases, nonspecular trails. The fact that head echo measurements can be performed only with HPLA radars limits these studies in several ways. HPLA radars are sensitive instruments constraining the studies to the lower masses, and these observations cannot be performed continuously because they take place at national observatories with limited allocated observing time. These drawbacks can be addressed by developing head echo observing techniques with modified all-sky meteor radars. Such systems would also permit simultaneous detection of all different scattering mechanisms using the same instrument, rather than requiring assorted different classes of radars, which can help clarify observed differences between the different methodologies. In this study, we demonstrate that such concurrent observations are now possible, enabled by the enhanced design of the Southern Argentina Agile Meteor Radar (SAAMER). The results presented here are derived from observations performed over a period of 12 days in August 2011 and include meteoroid dynamical parameter distributions, radiants, and estimated masses. Overall, the SAAMER's head echo detections appear to be produced by larger particles than those which have been studied thus far using this technique. C1 [Janches, D.] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hocking, W.] Univ Western Ontario, Dept Phys & Astron, London, ON, Canada. [Pifko, S.] Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA. [Hormaechea, J. L.] Estn Astron Rio Grande, Rio Grande, Tierra Fuego, Argentina. [Fritts, D. C.] Gats Inc, Boulder, CO USA. [Brunini, C.] Univ Nacl La Plata, Dept Ciencias Astron & Geofis, La Plata, Buenos Aires, Argentina. [Michell, R.; Samara, M.] SouthWest Res Inst, San Antonio, TX USA. RP Janches, D (reprint author), NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM diego.janches@nasa.gov RI Janches, Diego/D-4674-2012; OI Janches, Diego/0000-0001-8615-5166; Hormaechea, Jose Luis/0000-0003-4533-3282 FU NSF [AGS - 0634650, AGS - 0944104, AST - 0908118]; NASA [12-PAST12-0007, 12-PATM12-0006] FX This work was supported by NSF awards AGS - 0634650, AGS - 0944104, and AST - 0908118, as well as NASA awards 12-PAST12-0007 and 12-PATM12-0006. We wish to thank the EARG personnel for their invaluable help with the operation of SAAMER. The authors wishes to thank M. Nicolls, S. Close, and J. Chau for invaluable discussions. NR 73 TC 7 Z9 7 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAR PY 2014 VL 119 IS 3 BP 2269 EP 2287 DI 10.1002/2013JA019241 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6CM UT WOS:000336218300069 ER PT J AU Curry, SM Liemohn, M Fang, X Ma, Y Slavin, J Espley, J Bougher, S Dong, CF AF Curry, S. M. Liemohn, M. Fang, X. Ma, Y. Slavin, J. Espley, J. Bougher, S. Dong, C. F. TI Test particle comparison of heavy atomic and molecular ion distributions at Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SOLAR-WIND INTERACTION; PLASMA ENVIRONMENT; HYBRID MODEL; ATMOSPHERE; ESCAPE; EXPRESS; VARIABILITY; OXYGEN; VENUS; O+ AB This study uses the Mars Test Particle simulation to create virtual detections of O+, O-2(+), and CO2+ in an orbital configuration in the Mars space environment. These atomic and molecular planetary pickup ions are formed when the solar wind directly interacts with the neutral atmosphere, causing the ions to be accelerated by the background convective electric field. The subsequent ion escape is the subject of great interest, specifically with respect to which species dominates ion loss from Mars. O+ is found to be the dominant escaping ion because of the large sources of transported ions in the low-energy (<10 eV) and high-energy (>1 keV) range. O-2(+) and CO2+ are observed at these energy ranges but with much lower fluxes and are generally only found in the tail between 10 eV and 1 keV. Using individual particle traces, we reveal the origin and trajectories of the low-energy downtail O+ populations and high-energy polar O+ populations that contribute to the total escape. Comparing them against O-2(+) and CO2+ reveals that the extended hot oxygen corona contributes to source regions of high-and low-energy escaping ions. Additionally, we present results for solar minimum and maximum conditions with respect to ion fluxes and energies in order to robustly describe the physical processes controlling planetary ion distributions and atmospheric escape. C1 [Curry, S. M.; Liemohn, M.; Slavin, J.; Bougher, S.; Dong, C. F.] Univ Michigan, Dept Atmospher & Space Sci, Ann Arbor, MI 48109 USA. [Fang, X.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Ma, Y.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Espley, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Curry, SM (reprint author), Univ Michigan, Dept Atmospher & Space Sci, Ann Arbor, MI 48109 USA. EM smcurry@umich.edu RI Dong, Chuanfei/E-6485-2010; Liemohn, Michael/H-8703-2012; Bougher, Stephen/C-1913-2013; Fang, Xiaohua/C-2773-2008; Ma, Yingjuan/B-4895-2017 OI Dong, Chuanfei/0000-0002-8990-094X; Liemohn, Michael/0000-0002-7039-2631; Bougher, Stephen/0000-0002-4178-2729; Fang, Xiaohua/0000-0002-6584-2837; Ma, Yingjuan/0000-0003-2584-7091 FU NASA Goddard Space Flight Center under the Graduate Student Research Program [NNX10AL84H]; NASA [NNX11AD80G]; NSF [AST 0908311] FX This work was funded by the NASA Goddard Space Flight Center under the Graduate Student Research Program (grant NNX10AL84H), by NASA grant NNX11AD80G, and NSF grant AST 0908311. The authors would also like to acknowledge Yuni Lee for her technical support. NR 54 TC 7 Z9 7 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAR PY 2014 VL 119 IS 3 BP 2328 EP 2344 DI 10.1002/2013JA019221 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6CM UT WOS:000336218300073 ER PT J AU Jones, MC Wooller, M Peteet, DM AF Jones, Miriam C. Wooller, Matthew Peteet, Dorothy M. TI A deglacial and Holocene record of climate variability in south-central Alaska from stable oxygen isotopes and plant macrofossils in peat SO QUATERNARY SCIENCE REVIEWS LA English DT Article DE Holocene; Oxygen isotopes; Peat; Aleutian Low; Carbon ID NORTH PACIFIC; KENAI PENINSULA; INTERIOR ALASKA; YUKON-TERRITORY; WESTERN CANADA; ORGANIC-MATTER; CARBON; LAKE; CELLULOSE; HISTORY AB We used stable oxygen isotopes derived from bulk-peat (delta O-18(TOM)), in conjunction with plant macrofossils and previously published carbon accumulation records, in a 14,500 cal yr BP peat core (HT Fen) from the Kenai lowlands in south-central Alaska to reconstruct the climate history of the area. We find that patterns are broadly consistent with those from lacustrine records across the region, and agree with the interpretation that major shifts in delta O-18(TOM) values indicate changes in strength and position of the Aleutian Low (AL), a semi-permanent low-pressure cell that delivers winter moisture to the region. We find decreased strength or a more westerly position of the AL (relatively higher delta O-18(TOM) values) during the Bolling-Allerod, Holocene Thermal Maximum (HTM), and late Holocene, which also correspond to warmer climate regimes. These intervals coincide with greater peat preservation and enhanced carbon (C) accumulation rates at the HT Fen and with peatland expansion across Alaska. The HTM in particular may have experienced greater summer precipitation as a result of an enhanced Pacific subtropical high, a pattern consistent with modern delta O-18 values for summer precipitation. The combined warm summer temperatures and greater summer precipitation helped promote the observed rapid peat accumulation. A strengthened AL (relatively lower delta O-18(TOM) values) is most evident during the Younger Dryas, Neoglaciation, and the Little Ice Age, consistent with lower peat preservation and C accumulation at the HT Fen, suggesting less precipitation reaches the leeward side of the Kenai Mountains during periods of enhanced AL strength. The peatlands on the Kenai Peninsula thrive when the AL is weak and the contribution of summer precipitation is higher, highlighting the importance of precipitation seasonality in promoting peat accumulation. This study demonstrates that delta O-18(TOM) values in peat can be applied toward understand large-scale shifts in atmospheric circulation over millennial timescales. Published by Elsevier Ltd. C1 [Jones, Miriam C.] US Geol Survey, Natl Ctr, Reston, VA 20192 USA. [Jones, Miriam C.; Wooller, Matthew] Univ Alaska Fairbanks, Inst Northern Engn, Water & Environm Res Ctr, Fairbanks, AK 99775 USA. [Wooller, Matthew] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Alaska Stable Isotope Facil, Fairbanks, AK 99775 USA. [Wooller, Matthew] Univ Alaska Fairbanks, Alaska Quaternary Ctr, Fairbanks, AK 99775 USA. [Peteet, Dorothy M.] Goddard Inst Space Studies, New York, NY 20025 USA. [Peteet, Dorothy M.] Lamont Doherty Earth Observ, Palisades, NY 10964 USA. RP Jones, MC (reprint author), US Geol Survey, Natl Ctr, Reston, VA 20192 USA. EM miriamjones@usgs.gov OI Jones, Miriam/0000-0002-6650-7619; Wooller, Matthew/0000-0002-5065-4235 FU Columbia University LDEO Climate Center grant; NASA/GISS; National Science Foundation [ARC-1022979, ARC-1204233] FX This project was funded by a Columbia University LDEO Climate Center grant, NASA/GISS, and a grant from the National Science Foundation (Award #ARC-1022979). Matthew Wooller was supported by a grant from the National Science Foundation (Award #ARC-1204233). NR 84 TC 11 Z9 12 U1 0 U2 17 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 MAR 1 PY 2014 VL 87 BP 1 EP 11 DI 10.1016/j.quascirev.2013.12.025 PG 11 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA AH1JR UT WOS:000335876900001 ER PT J AU Morgan, JLL Ritchie, LE Crucian, BE Theriot, C Wu, HL Sams, C Smith, SM Turner, ND Zwart, SR AF Morgan, Jennifer L. L. Ritchie, Lauren E. Crucian, Brian E. Theriot, Corey Wu, Honglu Sams, Clarence Smith, Scott M. Turner, Nancy D. Zwart, Sara R. TI Increased dietary iron and radiation in rats promote oxidative stress, induce localized and systemic immune system responses, and alter colon mucosal environment SO FASEB JOURNAL LA English DT Article DE body iron stores; short-chain fatty acids; cytokines; injury repair; pathogen recognition ID TOLL-LIKE RECEPTORS; CHAIN FATTY-ACIDS; INFLAMMATORY-BOWEL-DISEASE; LONG-DURATION SPACEFLIGHT; HAMSTER OVARY CELLS; SPACE RADIATION; GUT MICROBIOTA; ELECTROLYTE TRANSPORT; PARTICLE RADIATION; GENE-EXPRESSION AB Astronauts are exposed to increased body iron stores and radiation, both of which can cause oxidative damage leading to negative health effects. The purpose of this study was to investigate combined effects of high dietary iron (650 mg/kg diet) and radiation exposure (0.375 Gy cesium-137 every other day for 16 d) on markers of oxidative stress, immune system function, and colon mucosal environment in male Sprague-Dawley rats (n=8/group). Control rats consumed adequate iron (45 mg/kg diet) and were not irradiated. Combined treatments increased liver glutathione peroxidase, serum catalase, and colon myeloperoxidase while decreasing total fecal short-chain fatty acid concentrations. The high-iron diet alone increased leukocyte count. Radiation decreased the T-cell CD4:CD8 ratio. Plasma iron was negatively correlated with cytokine production in activated monocytes. Genes involved in colon microbial signaling, immune response, and injury repair were altered by radiation. Genes involved with injury repair and pathogen recognition changed with dietary iron. These data demonstrate that dietary iron and radiation, alone and combined, contribute to oxidative stress that is related to immune system alterations in circulation and the colon. The model presented may help us better understand the changes to these systems that have been identified among astronauts.Morgan, J. L. L., Ritchie, L. E., Crucian, B. E., Theriot, C., Wu, H., Sams, C., Smith, S. M., Turner, N. D., Zwart, S. R. Increased dietary iron and radiation in rats promote oxidative stress, induce localized and systemic immune system responses, and alter colon mucosal environment. C1 [Morgan, Jennifer L. L.] Oak Ridge Associated Univ, NASA, Postdoctoral Fellowship Program, Houston, TX USA. [Crucian, Brian E.; Wu, Honglu; Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Biomed Res & Environm Sci Div, Houston, TX 77058 USA. [Sams, Clarence] NASA, Lyndon B Johnson Space Ctr, Space & Clin Operat Div, Human Hlth & Performance Directorate, Houston, TX 77058 USA. [Ritchie, Lauren E.; Turner, Nancy D.] Texas A&M Univ, Dept Nutr & Food Sci, College Stn, TX USA. [Theriot, Corey] Univ Texas Med Branch, Dept Prevent Med & Community Hlth, Galveston, TX 77555 USA. [Zwart, Sara R.] Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA. RP Zwart, SR (reprint author), Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA. EM sara.zwart-1@nasa.gov FU NASA Human Research Program's Human Health Countermeasures Element FX The authors thank the staff of the NASA Johnson Space Center Nutritional Biochemistry Laboratory for their assistance in processing and analyzing the samples, and in all aspects of carrying out this project. The authors thank Jane Krauhs for editorial assistance. This study was funded by the NASA Human Research Program's Human Health Countermeasures Element. NR 98 TC 3 Z9 3 U1 1 U2 6 PU FEDERATION AMER SOC EXP BIOL PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA SN 0892-6638 EI 1530-6860 J9 FASEB J JI Faseb J. PD MAR PY 2014 VL 28 IS 3 BP 1486 EP 1498 DI 10.1096/fj.13-239418 PG 13 WC Biochemistry & Molecular Biology; Biology; Cell Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Cell Biology GA AG3MY UT WOS:000335324800039 PM 24334706 ER PT J AU Wollack, EJ Chuss, DT Rostem, K U-Yen, K AF Wollack, E. J. Chuss, D. T. Rostem, K. U-Yen, K. TI Impedance matched absorptive thermal blocking filters SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID STEFAN-BOLTZMANN CONSTANT; N-DIMENSIONAL SPACE; SINGLE AB We have designed, fabricated, and characterized absorptive thermal blocking filters for cryogenic microwave applications. The transmission line filter's input characteristic impedance is designed to match 50 Omega and its response has been validated from 0 to 50 GHz. The observed return loss in the 0 to 20 GHz design band is greater than 20 dB and shows graceful degradation with frequency. Design considerations and equations are provided that enable this approach to be scaled and modified for use in other applications. C1 [Wollack, E. J.; Chuss, D. T.; Rostem, K.; U-Yen, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rostem, K.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Wollack, EJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM edward.j.wollack@nasa.gov RI Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 FU NASA ROSES/APRA program FX The authors gratefully acknowledge financial support from the NASA ROSES/APRA program and thank F. Colazo, A. J. Goulette, and M. Turvey for their contributions to the development of these structures. NR 27 TC 3 Z9 3 U1 1 U2 14 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0034-6748 EI 1089-7623 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD MAR PY 2014 VL 85 IS 3 AR 034702 DI 10.1063/1.4869038 PG 5 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA AH1ZL UT WOS:000335920400051 PM 24689607 ER PT J AU Mitrofanov, IG Litvak, ML Sanin, AB Lisov, DI Kuzmin, RO Behar, A Boynton, WV Hardgrove, C Harshman, K Jun, I Milliken, R Mischna, MA Moersch, JE Starr, R Tate, CG AF Mitrofanov, I. G. Litvak, M. L. Sanin, A. B. Lisov, D. I. Kuzmin, R. O. Behar, A. Boynton, W. V. Hardgrove, C. Harshman, K. Jun, I. Milliken, R. Mischna, M. A. Moersch, J. E. Starr, R. Tate, C. G. TI Studying of water consent in Mars' gale crater: The first results of the DAN experiment on the NASA curiosity rover SO DOKLADY PHYSICS LA English DT Article ID DYNAMIC ALBEDO; ONBOARD C1 [Mitrofanov, I. G.; Litvak, M. L.; Sanin, A. B.; Lisov, D. I.; Kuzmin, R. O.] Russian Acad Sci, Inst Space Res, Moscow V71, Russia. [Kuzmin, R. O.] Russian Acad Sci, VI Vernadsky Inst Geochem & Analyt Chem, Moscow, Russia. [Behar, A.; Jun, I.; Mischna, M. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Boynton, W. V.; Harshman, K.] Univ Arizona, Tucson, AZ USA. [Hardgrove, C.; Moersch, J. E.] Univ Tennessee, Knoxville, TN USA. [Milliken, R.; Tate, C. G.] Brown Univ, Providence, RI 02912 USA. [Starr, R.] Catholic Univ Amer, Washington, DC 20064 USA. RP Mitrofanov, IG (reprint author), Russian Acad Sci, Inst Space Res, Moscow V71, Russia. NR 8 TC 1 Z9 1 U1 0 U2 17 PU MAIK NAUKA/INTERPERIODICA/SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA SN 1028-3358 EI 1562-6903 J9 DOKL PHYS JI Dokl. Phys. PD MAR PY 2014 VL 59 IS 3 BP 126 EP 128 DI 10.1134/S1028335814030112 PG 3 WC Mechanics; Physics, Multidisciplinary SC Mechanics; Physics GA AG1IS UT WOS:000335169200005 ER PT J AU Allen, PA Wells, DN AF Allen, Phillip A. Wells, Douglas N. TI Interpolation methodology for elastic plastic J-integral solutions for surface cracked plates in tension SO ENGINEERING FRACTURE MECHANICS LA English DT Article DE J-pintegral; Surface crack; Elastic-plastic; Nonlinear fracture; Interpolation; Finite element analysis; Stress intensity factor AB No closed form solutions exist for the elastic-plastici-integral for surface cracks due to the nonlinear, three-dimensional (3-D) nature of the problem. Traditionally, each surface crack case must be analyzed with a unique and time-consuming nonlinear finite element analysis. To overcome this shortcoming, the authors have developed and analyzed an array of 600 3-D nonlinear finite element models for surface cracks in flat plates under tension loading. The solution space covers a wide range of crack shapes and depths (shape: 0.2 <= a/c <= 1.0, depth: 0.2 <= a/B <= 0.8) and material flow properties (elastic modulus to yield ratio: 100 <= E/sigma(ys) <= 1000, and hardening: 3 <= n <= 20). The authors have developed a methodology for interpolating between the geometric and material property variables that allows the user to reliably evaluate the full elastic-plastic J-integral and force versus CMOD solution; thus, a solution can be obtained very rapidly by users without elastic-plastic fracture mechanics modeling experience. Complete solutions for the 600 models and 25 additional benchmark models are provided in tabular format as well as a computer program for calculating the interpolated solutions. Published by Elsevier Ltd. C1 [Allen, Phillip A.; Wells, Douglas N.] NASA, George C Marshall Space Flight Ctr, MSFC, Huntsville, AL 35812 USA. RP Allen, PA (reprint author), NASA, George C Marshall Space Flight Ctr, MSFC, Huntsville, AL 35812 USA. EM phillip.a.allen@nasa.gov NR 19 TC 1 Z9 1 U1 3 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0013-7944 EI 1873-7315 J9 ENG FRACT MECH JI Eng. Fract. Mech. PD MAR PY 2014 VL 119 BP 173 EP 201 DI 10.1016/j.engfracmech.2014.02.021 PG 29 WC Mechanics SC Mechanics GA AG0JE UT WOS:000335101000014 ER PT J AU Toft, JE Burke, JL Carey, MP Kim, CK Marsik, M Sutherland, DA Arkema, KK Guerry, AD Levin, PS Minello, TJ Plummer, M Ruckelshaus, MH Townsend, HM AF Toft, J. E. Burke, J. L. Carey, M. P. Kim, C. K. Marsik, M. Sutherland, D. A. Arkema, K. K. Guerry, A. D. Levin, P. S. Minello, T. J. Plummer, M. Ruckelshaus, M. H. Townsend, H. M. TI From mountains to sound: modelling the sensitivity of Dungeness crab and Pacific oyster to landsea interactions in Hood Canal, WA SO ICES JOURNAL OF MARINE SCIENCE LA English DT Article DE climate change; Dungeness crab; future land use; land cover; landsea interactions; marine water quality; Pacific oyster; scenario analysis; watersheds ID ECOSYSTEM-BASED MANAGEMENT; CANCER-MAGISTER FISHERY; CLIMATE-CHANGE; MARINE ECOSYSTEMS; RED ALDER; COASTAL; CONSERVATION; SERVICES; WATERSHEDS; OREGON AB Many diagnoses of declining marine species and habitats along US coasts point to upland and freshwater sources of imperilment. Yet, little work has examined how and whether activities on land affect marine resources. Similarly, the impacts of climate change on coastal systems are among the most certain; yet, few studies have explored how alternative management and climate scenarios will affect the delivery of diverse benefits to people from coasts. We estimated how Dungeness crab (Metacarcinus magister) and Pacific oyster (Crassostrea gigas) harvest in Hood Canal, WA, may change given predictions of land uses and effects of climate change. These two marine species are critical components of local commercial and recreational fisheries and thus represent key ecosystem service endpoints. We found that Dungeness crab harvest responds strongly to effects of climate change, as mediated by increased ocean temperature, whereas Pacific oyster harvest is more responsive to projected change in land-use/land-cover due to increased nutrient loading to the marine system. These changes vary spatially throughout Hood Canal. These results can be used as a heuristic framework to help decision-makers, planners, and other stakeholders in the region as they work to target conservation and restoration activities and plan for future growth in a changing climate. C1 [Toft, J. E.; Kim, C. K.; Arkema, K. K.; Guerry, A. D.; Ruckelshaus, M. H.] Stanford Univ, Nat Capital Project, Stanford, CA 94305 USA. [Burke, J. L.; Carey, M. P.; Levin, P. S.; Plummer, M.] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Seattle, WA 98112 USA. [Kim, C. K.] Inha Univ, Ocean Sci & Technol Inst, Inchon, South Korea. [Marsik, M.] Nature Conservancy, Washington Field Off, Seattle, WA 98101 USA. [Sutherland, D. A.] Univ Oregon, Dept Geol Sci, Eugene, OR 97403 USA. [Minello, T. J.] NOAA, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Galveston Lab, Galveston, TX 77551 USA. [Townsend, H. M.] NOAA, Natl Marine Fisheries Serv, Chesapeake Bay Off, Annapolis, MD 21403 USA. RP Toft, JE (reprint author), Stanford Univ, Nat Capital Project, 371 Serra Mall, Stanford, CA 94305 USA. EM jetoft@stanford.edu OI Sutherland, David/0000-0002-2843-8608 FU CAMEO programme of NOAA/NSF FX We would like to thank the CAMEO programme of NOAA/NSF for funding. NR 96 TC 3 Z9 3 U1 4 U2 27 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1054-3139 EI 1095-9289 J9 ICES J MAR SCI JI ICES J. Mar. Sci. PD MAR-APR PY 2014 VL 71 IS 3 BP 725 EP 738 DI 10.1093/icesjms/fst072 PG 14 WC Fisheries; Marine & Freshwater Biology; Oceanography SC Fisheries; Marine & Freshwater Biology; Oceanography GA AF4OY UT WOS:000334694300029 ER PT J AU Gallaher, DW Campbell, GG Meier, WN AF Gallaher, David W. Campbell, G. Garrett Meier, Walter N. TI Anomalous Variability in Antarctic Sea Ice Extents During the 1960s With the Use of Nimbus Data SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article; Proceedings Paper CT 14th International Conference on Ground Penetrating Radar (GPR) CY JUN 04-08, 2012 CL Shanghai, PEOPLES R CHINA DE Antarctic sea ice; historic data; Nimbus AB The Nimbus I, II, and III satellites provide a new opportunity for climate studies in the 1960s. The rescue of the visible and infrared imager data resulted in the utilization of the early Nimbus data to determine sea ice extent. A qualitative analysis of the early NASA Nimbus missions has revealed Antarctic sea ice extents that are significant larger and smaller than the historic 1979-2012 passive microwave record. The September 1964 ice mean area is 19.7x10(6) km(2) +/- 0.3x10(6) km(2). This is more the 250,000 km(2) greater than the 19.44x10(6) km(2) seen in the new 2012 historic maximum. However, in August 1966 the maximum sea ice extent fell to 15.9x10(6) km(2) +/- 0.3x10(6) km(2). This is more than 1.5x10(6) km(2) below the passive microwave record of 17.5x10(6) km(2) set in September of 1986. This variation between 1964 and 1966 represents a change of maximum sea ice of over 3x10(6) km(2) in just two years. These inter-annual variations while large, are small when compared to the Antarctic seasonal cycle. C1 [Gallaher, David W.; Campbell, G. Garrett; Meier, Walter N.] Univ Colorado, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA. [Meier, Walter N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. OI Meier, Walter/0000-0003-2857-0550 FU NASA [NNG08HZ07C] FX This work was supported under NASA Sub-Contract NNG08HZ07C. NR 15 TC 5 Z9 5 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD MAR PY 2014 VL 7 IS 3 BP 881 EP 887 DI 10.1109/JSTARS.2013.2264391 PG 7 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA AG4KG UT WOS:000335387900018 ER PT J AU Greenwood, E Schmitz, FH AF Greenwood, Eric Schmitz, Fredric H. TI Separation of Main and Tail Rotor Noise from Ground-Based Acoustic Measurements SO JOURNAL OF AIRCRAFT LA English DT Article ID DE-DOPPLERIZATION AB A new method of characterizing the external noise radiation of rotorcraft is presented, making use of ground-based acoustic measurements. The method employs time-domain de-Dopplerization to transform the acoustic pressure time-history data collected from a fixed array of ground-based microphones to the equivalent time-history signals observed by an array of virtual in-flight microphones traveling with the helicopter. The now-stationary signals observed by the virtual microphones are then periodically averaged with the main and tail rotor blade passages, which are inferred from the acoustic signals using wavelet analysis. The averaging process suppresses noise that is not periodic with the respective rotor, allowing for the separation of main and tail rotor pressure time histories. The averaged measurements are then interpolated across the range of directivity angles captured by the microphone array in order to generate separate acoustic hemispheres for the main and tail rotor noise sources. This method facilitates a more direct comparison of ground-based noise measurements of rotorcraft with theoretical predictions and wind tunnel measurements of isolated rotors. The new method is successfully applied to ground-based microphone measurements of a Bell 206B3 helicopter and demonstrates the strong directivity characteristics of harmonic noise radiation from both the main and tail rotors of that helicopter. C1 [Greenwood, Eric] NASA Langley Res Ctr, Aeroacoust Branch, Hampton, VA 23681 USA. [Schmitz, Fredric H.] Univ Maryland, Dept Aerosp Engn, College Pk, MD 20742 USA. RP Greenwood, E (reprint author), NASA Langley Res Ctr, Aeroacoust Branch, Mail Stop 461, Hampton, VA 23681 USA. RI Greenwood, Eric/Q-7642-2016 OI Greenwood, Eric/0000-0002-0427-539X NR 11 TC 1 Z9 1 U1 2 U2 7 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD MAR-APR PY 2014 VL 51 IS 2 BP 464 EP 472 DI 10.2514/1.C032046 PG 9 WC Engineering, Aerospace SC Engineering GA AE2JD UT WOS:000333798200010 ER PT J AU Rallabhandi, SK Nielsen, EJ Diskin, B AF Rallabhandi, Sriram K. Nielsen, Eric J. Diskin, Boris TI Sonic-Boom Mitigation Through Aircraft Design and Adjoint Methodology SO JOURNAL OF AIRCRAFT LA English DT Article ID MINIMIZATION; PREDICTION; GRIDS AB This paper presents a novel approach to design of the supersonic aircraft outer mold line by optimizing a A-weighted loudness-based objective of the sonic-boom signature predicted on the ground. The optimization process uses the sensitivity information obtained by coupling the discrete adjoint formulations for the augmented Burgers equation and computational-fluid-dynamics equations. This coupled formulation links the loudness of the ground boom signature to the aircraft geometry, thus allowing efficient shape optimization for the purpose of minimizing the loudness. The accuracy of the adjoint-based sensitivities is verified against sensitivities obtained using an independent complex-variable approach. The adjoint-based optimization methodology is applied to a configuration previously optimized using alternative state-of-the-art optimization methods and produces additional loudness reduction. The results of the optimizations are reported and discussed. C1 [Rallabhandi, Sriram K.; Diskin, Boris] Natl Inst Aerosp, Hampton, VA 23666 USA. [Nielsen, Eric J.] NASA Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA. RP Rallabhandi, SK (reprint author), Natl Inst Aerosp, Hampton, VA 23666 USA. FU NASA [NNL08AA00B, NNL12AA55T] FX This work was supported by the NASA Project entitled "Sonic Boom Propagation Tools and Methods for Low Sonic Boom Design," under NASA contract number NNL08AA00B, task number NNL12AA55T, through the NASA Fundamental Aeronautics Supersonics Program. The first author wishes to thank Wu Li, Irian Ordaz, and Mike Park for some initial discussions of boom adjoints. The receipt of the time-domain A-weighted loudness calculation code from Gulfstream Aerospace is gratefully acknowledged. The time and effort put in by Scott Brynildsen, Jan-Renee Carlson, Norma Farr, and Dick Campbell for geometry generation and gridding for powered-on engine simulation in a short amount of time and Karl Geiselhart for engine boundary conditions is greatly appreciated. Help in several forms from Lori Ozoroski, Bill Jones, and Bill Kleb is also acknowledged. NR 33 TC 4 Z9 4 U1 2 U2 8 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD MAR-APR PY 2014 VL 51 IS 2 BP 502 EP 510 DI 10.2514/1.C032189 PG 9 WC Engineering, Aerospace SC Engineering GA AE2JD UT WOS:000333798200013 ER PT J AU Wu, H Adler, RF Tian, YD Huffman, GJ Li, HY Wang, JJ AF Wu, Huan Adler, Robert F. Tian, Yudong Huffman, George J. Li, Hongyi Wang, JianJian TI Real-time global flood estimation using satellite-based precipitation and a coupled land surface and routing model SO WATER RESOURCES RESEARCH LA English DT Article DE flood modeling; flood detection; VIC; DRT; DRIVE; TRMM ID COLORADO RIVER-BASIN; CLIMATE-CHANGE; DATA ASSIMILATION; HYDROLOGIC MODEL; WATER-RESOURCES; UNITED-STATES; UNCERTAINTY; RAINFALL; SYSTEMS; STORAGE AB A widely used land surface model, the Variable Infiltration Capacity (VIC) model, is coupled with a newly developed hierarchical dominant river tracing-based runoff-routing model to form the Dominant river tracing-Routing Integrated with VIC Environment (DRIVE) model, which serves as the new core of the real-time Global Flood Monitoring System (GFMS). The GFMS uses real-time satellite-based precipitation to derive flood monitoring parameters for the latitude band 50 degrees N-50 degrees S at relatively high spatial (approximate to 12 km) and temporal (3 hourly) resolution. Examples of model results for recent flood events are computed using the real-time GFMS (). To evaluate the accuracy of the new GFMS, the DRIVE model is run retrospectively for 15 years using both research-quality and real-time satellite precipitation products. Evaluation results are slightly better for the research-quality input and significantly better for longer duration events (3 day events versus 1 day events). Basins with fewer dams tend to provide lower false alarm ratios. For events longer than three days in areas with few dams, the probability of detection is approximate to 0.9 and the false alarm ratio is approximate to 0.6. In general, these statistical results are better than those of the previous system. Streamflow was evaluated at 1121 river gauges across the quasi-global domain. Validation using real-time precipitation across the tropics (30 degrees S-30 degrees N) gives positive daily Nash-Sutcliffe Coefficients for 107 out of 375 (28%) stations with a mean of 0.19 and 51% of the same gauges at monthly scale with a mean of 0.33. There were poorer results in higher latitudes, probably due to larger errors in the satellite precipitation input. C1 [Wu, Huan; Adler, Robert F.; Tian, Yudong; Wang, JianJian] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Wu, Huan; Adler, Robert F.; Tian, Yudong; Huffman, George J.; Wang, JianJian] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Li, Hongyi] Pacific NW Natl Lab, Richland, WA 99352 USA. RP Wu, H (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. EM huanwu@umd.edu RI Wu, Huan/K-1003-2013; Li, Hong-Yi/C-9143-2014; Huffman, George/F-4494-2014; Measurement, Global/C-4698-2015 OI Wu, Huan/0000-0003-2920-8860; Li, Hong-Yi/0000-0001-5690-3610; Huffman, George/0000-0003-3858-8308; FU NASA; Department of Energy Biological and Environmental Research (BER) FX This research was supported by NASA's Applied Sciences Program. TMPA data used in this study were provided by the NASA/Goddard Space Flight Center's laboratory for Atmospheres and PPS. The TMPA real-time product is from ftp://trmmopen.gsfc.nasa.gov and the research product is from ftp://disc2.nascom.nasa.gov/. H.-Y. Li is supported by the Department of Energy Biological and Environmental Research (BER) Earth System Modeling (ESM) and Integrated Assessment Modeling (IAM) Programs through the Integrated Earth System Modeling (iESM). We gratefully acknowledge the historic discharge measurement provision by the Global Runoff Data Centre. We also thank Justin Sheffield (University of Princeton) for sharing the VIC model setup data set. NR 53 TC 42 Z9 42 U1 4 U2 33 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 MAR PY 2014 VL 50 IS 3 BP 2693 EP 2717 DI 10.1002/2013WR014710 PG 25 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA AE6NV UT WOS:000334111600047 ER PT J AU Harpold, AA Guo, Q Molotch, N Brooks, PD Bales, R Fernandez-Diaz, JC Musselman, KN Swetnam, TL Kirchner, P Meadows, MW Flanagan, J Lucas, R AF Harpold, A. A. Guo, Q. Molotch, N. Brooks, P. D. Bales, R. Fernandez-Diaz, J. C. Musselman, K. N. Swetnam, T. L. Kirchner, P. Meadows, M. W. Flanagan, J. Lucas, R. TI LiDAR-derived snowpack data sets from mixed conifer forests across the Western United States SO WATER RESOURCES RESEARCH LA English DT Article DE snowpack; airborne LIDAR; snow-vegetation interactions; critical zone observatory ID STRUCTURE METRICS; DEPTH; TERRAIN AB Airborne-based Light Detection and Ranging (LiDAR) offers the potential to measure snow depth and vegetation structure at high spatial resolution over large extents and thereby increase our ability to quantify snow water resources. Here we present airborne LiDAR data products at four Critical Zone Observatories (CZO) in the Western United States: Jemez River Basin, NM, Boulder Creek Watershed, CO, Kings River Experimental Watershed, CA, and Wolverton Basin, CA. We make publicly available snow depth data products (1 m(2) resolution) derived from LiDAR with an estimated accuracy of <30 cm compared to limited in situ snow depth observations. Key Points LiDAR-derived snow depth from Western United States sites are publicly available Research catchments had variable forest properties and snow depths among sites LiDAR-derived snow depths were comparable to in situ measurements C1 [Harpold, A. A.; Molotch, N.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. [Guo, Q.; Bales, R.; Kirchner, P.; Meadows, M. W.; Flanagan, J.; Lucas, R.] Univ Calif Merced, Sierra Nevada Res Inst, Merced, CA USA. [Molotch, N.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Brooks, P. D.] Univ Arizona, Tucson, AZ USA. [Fernandez-Diaz, J. C.] Natl Ctr Airborne Laser Mapping, Houston, TX USA. [Musselman, K. N.] Univ Calif Los Angeles, Los Angeles, CA USA. [Swetnam, T. L.] Univ Arizona, Sch Nat Resources & Environm, Tucson, AZ USA. RP Harpold, AA (reprint author), Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. EM adrian.harpold@gmail.com RI Molotch, Noah/C-8576-2009; OI Harpold, Adrian/0000-0002-2566-9574 FU National Science Foundation [EAR 0922307]; CZO [EAR 724960, 725097, 724958]; EAR [1141764]; USDA [2012-67003-19802]; NSF EAR [EAR 1144894] FX This research was supported by the National Science Foundation to QG for the collection of the LiDARdata (EAR 0922307), to other coauthors in support of CZO sites (EAR 724960, 725097, 724958), and EAR 1141764 and USDA grant 2012-67003-19802. The first author was supported by an NSF EAR Postdoctoral Fellowship (EAR 1144894). NR 22 TC 12 Z9 12 U1 1 U2 24 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 MAR PY 2014 VL 50 IS 3 BP 2749 EP 2755 DI 10.1002/2013WR013935 PG 7 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA AE6NV UT WOS:000334111600050 ER PT J AU Adams, M Sterling, AC Moore, RL Gary, GA AF Adams, Mitzi Sterling, Alphonse C. Moore, Ronald L. Gary, G. Allen TI A SMALL-SCALE ERUPTION LEADING TO A BLOWOUT MACROSPICULE JET IN AN ON-DISK CORONAL HOLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: chromosphere; Sun: filaments, prominences; Sun: magnetic fields; Sun: transition region; Sun: UV radiation ID X-RAY JETS; QUIET SUN; H-ALPHA; MAGNETIC RECONNECTION; SOLAR SPICULES; MASS EJECTIONS; DYNAMICS; FLARES; SURGES; FLUX AB We examine the three-dimensional magnetic structure and dynamics of a solar EUV-macrospicule jet that occurred on 2011 February 27 in an on-disk coronal hole. The observations are from the Solar Dynamics Observatory (SDO) Atmospheric Imaging Assembly (AIA) and the SDO Helioseismic and Magnetic Imager (HMI). The observations reveal that in this event, closed-field-carrying cool absorbing plasma, as in an erupting mini-filament, erupted and opened, forming a blowout jet. Contrary to some jet models, there was no substantial recently emerged, closed, bipolar-magnetic field in the base of the jet. Instead, over several hours, flux convergence and cancellation at the polarity inversion line inside an evolved arcade in the base apparently destabilized the entire arcade, including its cool-plasma-carrying core field, to undergo a blowout eruption in the manner of many standard-sized, arcade-blowout eruptions that produce a flare and coronal mass ejection. Internal reconnection made bright "flare" loops over the polarity inversion line inside the blowing-out arcade field, and external reconnection of the blowing-out arcade field with an ambient open field made longer and dimmer EUV loops on the outside of the blowing-out arcade. That the loops made by the external reconnection were much larger than the loops made by the internal reconnection makes this event a new variety of blowout jet, a variety not recognized in previous observations and models of blowout jets. C1 [Adams, Mitzi; Sterling, Alphonse C.; Moore, Ronald L.; Gary, G. Allen] NASA, Space Sci Off, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Adams, M (reprint author), NASA, Space Sci Off, George C Marshall Space Flight Ctr, ZP13, Huntsville, AL 35812 USA. EM mitzi.adams@nasa.gov; alphonse.sterling@nasa.gov; ron.moore@nasa.gov; gag0002@uah.edu FU NASA's Office of Space Science through the Living With a Star Targeted Research & Technology Program FX A.C.S. and R. L. M. were supported by funding from NASA's Office of Space Science through the Living With a Star Targeted Research & Technology Program. NR 42 TC 14 Z9 14 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 MAR 1 PY 2014 VL 783 IS 1 AR 11 DI 10.1088/0004-637X/783/1/11 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600011 ER PT J AU Aliu, E Aune, T Behera, B Beilicke, M Benbow, W Berger, K Bird, R Buckley, JH Bugaev, V Cardenzana, JV Cerruti, M Chen, X Ciupik, L Connolly, MP Cui, W Duke, C Dumm, J Errando, M Falcone, A Federici, S Feng, Q Finley, JP Fortin, P Fortson, L Furniss, A Galante, N Gillanders, GH Griffin, S Griffiths, ST Grube, J Gyuk, G Hanna, D Holder, J Hughes, G Humensky, TB Kaaret, P Kargaltsev, O Kertzman, M Khassen, Y Kieda, D Krawczynski, H Lang, MJ Madhavan, AS Maier, G Majumdar, P McCann, A Moriarty, P Mukherjee, R Nieto, D de Bhroithe, AO Ong, RA Otte, AN Pandel, D Perkins, JS Pohl, M Popkow, A Prokoph, H Quinn, J Ragan, K Rajotte, J Reyes, LC Reynolds, PT Richards, GT Roache, E Sembroski, GH Skole, C Staszak, D Telezhinsky, I Theiling, M Tucci, JV Tyler, J Varlotta, A Vincent, S Wakely, SP Weekes, TC Weinstein, A Welsing, R Williams, DA Zitzer, B AF Aliu, E. Aune, T. Behera, B. Beilicke, M. Benbow, W. Berger, K. Bird, R. Buckley, J. H. Bugaev, V. Cardenzana, J. V. Cerruti, M. Chen, X. Ciupik, L. Connolly, M. P. Cui, W. Duke, C. Dumm, J. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fortin, P. Fortson, L. Furniss, A. Galante, N. Gillanders, G. H. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Hanna, D. Holder, J. Hughes, G. Humensky, T. B. Kaaret, P. Kargaltsev, Oleg Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Lang, M. J. Madhavan, A. S. Maier, G. Majumdar, P. McCann, A. Moriarty, P. Mukherjee, R. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Pohl, M. Popkow, A. Prokoph, H. Quinn, J. Ragan, K. Rajotte, J. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Sembroski, G. H. Skole, C. Staszak, D. Telezhinsky, I. Theiling, M. Tucci, J. V. Tyler, J. Varlotta, A. Vincent, S. Wakely, S. P. Weekes, T. C. Weinstein, A. Welsing, R. Williams, D. A. Zitzer, B. TI OBSERVATIONS OF THE UNIDENTIFIED GAMMA-RAY SOURCE TeV J2032+4130 BY VERITAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: general; pulsars: individual (PSR J2032+4127) ID CYGNUS REGION; SOURCE TEV-J2032+4130; FOLLOW-UP; ASTRONOMY; TELESCOPE; POPULATION; SEPARATION; DISCOVERY; EMISSION; GALAXY AB TeV J2032+4130 was the first unidentified source discovered at very high energies (VHEs; E > 100 GeV), with no obvious counterpart in any other wavelength. It is also the first extended source to be observed in VHE gamma rays. Following its discovery, intensive observational campaigns have been carried out in all wavelengths in order to understand the nature of the object, which have met with limited success. We report here on a deep observation of TeV J2032+4130 based on 48.2 hr of data taken from 2009 to 2012 by the Very Energetic Radiation Imaging Telescope Array System experiment. The source is detected at 8.7 standard deviations (sigma) and is found to be extended and asymmetric with a width of 9'.5 +/- 1'.2 along the major axis and 4'.0 +/- 0'.5 along the minor axis. The spectrum is well described by a differential power law with an index of 2.10 +/- 0.14(stat) +/- 0.21(sys) and a normalization of (9.5 +/- 1.6(stat) +/- 2.2(sys)) x 10(-13) TeV-1 cm(-2) s(-1) at 1 TeV. We interpret these results in the context of multiwavelength scenarios which particularly favor the pulsar wind nebula interpretation. C1 [Aliu, E.; Errando, M.; Mukherjee, R.; Nieto, D.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Aune, T.; Majumdar, P.; Ong, R. A.; Popkow, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Behera, B.; Chen, X.; Federici, S.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Skole, C.; Telezhinsky, I.; Vincent, S.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Cerruti, M.; Fortin, P.; Galante, N.; Roache, E.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Berger, K.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Berger, K.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bird, R.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cardenzana, J. V.; Madhavan, A. S.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Chen, X.; Federici, S.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Cui, W.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Tucci, J. V.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Dumm, J.; Fortson, L.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Griffin, S.; Hanna, D.; Ragan, K.; Rajotte, J.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Humensky, T. B.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kargaltsev, Oleg] George Washington Univ, Dept Phys, Washington, DC USA. [Kertzman, M.] DePauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Majumdar, P.] Saha Inst Nucl Phys, Kolkata 700064, India. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Pandel, D.] Grand Valley State Univ, Dept Phys, Allendale, MI 49401 USA. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. RP Aliu, E (reprint author), Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. EM gareth.hughes@desy.de; pratik.majumdar@saha.ac.in RI Khassen, Yerbol/I-3806-2015; Nieto, Daniel/J-7250-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Nieto, Daniel/0000-0003-3343-0755; Cui, Wei/0000-0002-6324-5772; Pandel, Dirk/0000-0003-2085-5586; Lang, Mark/0000-0003-4641-4201; Bird, Ralph/0000-0002-4596-8563 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U.K.; Young Investigators Program of the Helmholtz Association; NASA [NNX09AC84G, NNX09AC81G] FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748) and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. G. H. acknowledges support through the Young Investigators Program of the Helmholtz Association. The work by O.K. was supported by NASA grants NNX09AC84G and NNX09AC81G. NR 50 TC 10 Z9 10 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2014 VL 783 IS 1 AR 16 DI 10.1088/0004-637X/783/1/16 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600016 ER PT J AU Graur, O Rodney, SA Maoz, D Riess, AG Jha, SW Postman, M Dahlen, T Holoien, TWS McCully, C Patel, B Strolger, LG Benitez, N Coe, D Jouvel, S Medezinski, E Molino, A Nonino, M Bradley, L Koekemoer, A Balestra, I Cenko, SB Clubb, KI Dickinson, ME Filippenko, AV Frederiksen, TF Garnavich, P Hjorth, J Jones, DO Leibundgut, B Matheson, T Mobasher, B Rosati, P Silverman, JM U, V Jedruszczuk, K Li, C Lin, K Mirmelstein, M Neustadt, J Ovadia, A Rogers, EH AF Graur, O. Rodney, S. A. Maoz, D. Riess, A. G. Jha, S. W. Postman, M. Dahlen, T. Holoien, T. W. -S. McCully, C. Patel, B. Strolger, L. -G. Benitez, N. Coe, D. Jouvel, S. Medezinski, E. Molino, A. Nonino, M. Bradley, L. Koekemoer, A. Balestra, I. Cenko, S. B. Clubb, K. I. Dickinson, M. E. Filippenko, A. V. Frederiksen, T. F. Garnavich, P. Hjorth, J. Jones, D. O. Leibundgut, B. Matheson, T. Mobasher, B. Rosati, P. Silverman, J. M. U, V. Jedruszczuk, K. Li, C. Lin, K. Mirmelstein, M. Neustadt, J. Ovadia, A. Rogers, E. H. TI TYPE-Ia SUPERNOVA RATES TO REDSHIFT 2.4 FROM CLASH: THE CLUSTER LENSING AND SUPERNOVA SURVEY WITH HUBBLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general; surveys; white dwarfs ID DIGITAL SKY SURVEY; DELAY-TIME DISTRIBUTION; SUBARU DEEP FIELD; EXTRAGALACTIC LEGACY SURVEY; TELESCOPE ADVANCED CAMERA; STAR-FORMATION RATE; SPACE-TELESCOPE; PHOTOMETRIC REDSHIFTS; LUMINOSITY FUNCTIONS; RADIAL-DISTRIBUTION AB We present the supernova (SN) sample and Type-Ia SN (SN Ia) rates from the Cluster Lensing And Supernova survey with Hubble (CLASH). Using the Advanced Camera for Surveys and the Wide Field Camera 3 on the Hubble Space Telescope (HST), we have imaged 25 galaxy-cluster fields and parallel fields of non-cluster galaxies. We report a sample of 27 SNe discovered in the parallel fields. Of these SNe, similar to 13 are classified as SN Ia candidates, including four SN Ia candidates at redshifts z > 1.2. We measure volumetric SN Ia rates to redshift 1.8 and add the first upper limit on the SN Ia rate in the range 1.8 < z < 2.4. The results are consistent with the rates measured by the HST/GOODS and Subaru Deep Field SN surveys. We model these results together with previous measurements at z < 1 from the literature. The best-fitting SN Ia delay-time distribution (DTD; the distribution of times that elapse between a short burst of star formation and subsequent SN Ia explosions) is a power law with an index of -1.00(-0.06(0.10))(+0.06(0.09)) (statistical)(-0.08)(+0.12) (systematic), where the statistical uncertainty is a result of the 68% and 95% (in parentheses) statistical uncertainties reported for the various SN Ia rates (from this work and from the literature), and the systematic uncertainty reflects the range of possible cosmic star-formation histories. We also test DTD models produced by an assortment of published binary population synthesis (BPS) simulations. The shapes of all BPS double-degenerate DTDs are consistent with the volumetric SN Ia measurements, when the DTD models are scaled up by factors of 3-9. In contrast, all BPS single-degenerate DTDs are ruled out by the measurements at >99% significance level. C1 [Graur, O.; Rodney, S. A.; Riess, A. G.; Medezinski, E.; Jones, D. O.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Graur, O.; Maoz, D.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Graur, O.; Jedruszczuk, K.; Li, C.; Lin, K.; Neustadt, J.; Ovadia, A.; Rogers, E. H.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Graur, O.] New York Univ, CCPP, New York, NY 10003 USA. [Riess, A. G.; Postman, M.; Dahlen, T.; Strolger, L. -G.; Coe, D.; Bradley, L.; Koekemoer, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Jha, S. W.; Holoien, T. W. -S.; McCully, C.; Patel, B.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Benitez, N.; Molino, A.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Jouvel, S.] CSIC, Inst Ciencies Espai IEEC, E-08193 Bellaterra, Barcelonaa, Spain. [Nonino, M.; Balestra, I.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy. [Balestra, I.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Cenko, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Cenko, S. B.; Clubb, K. I.; Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Dickinson, M. E.; Matheson, T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Frederiksen, T. F.; Hjorth, J.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Garnavich, P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Leibundgut, B.; Rosati, P.] European So Observ, D-85748 Garching, Germany. [Leibundgut, B.] Tech Univ Munich, Excellence Cluster Univ, D-85748 Garching, Germany. [Mobasher, B.; U, V.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Silverman, J. M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Graur, O (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. EM orgraur@jhu.edu RI Hjorth, Jens/M-5787-2014; OI Hjorth, Jens/0000-0002-4571-2306; Nonino, Mario/0000-0001-6342-9662; Balestra, Italo/0000-0001-9660-894X; Graur, Or/0000-0002-4391-6137; Koekemoer, Anton/0000-0002-6610-2048; Benitez, Narciso/0000-0002-0403-7455 FU NASA from the Space Telescope Science Institute (STScI) [HST-GO-12060, HST-GO-12099]; NASA [NAS 5-26555, HF-51312.01]; I-CORE program of the PDC; ISF [1829/12]; Israel Science Foundation; STScI; NASA Exoplanet Science Institute; NSF CAREER award [AST-0847157]; Spanish Ministerio de Educacion y Ciencia [AYA2006-14056 BES-2007-16280]; PRIN INAF; NSF [AST-1211916, AST-9987045]; TABASGO Foundation; Christopher R. Redlich Fund; Danish National Research Foundation; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302771]; American Museum of Natural History's Science Research Mentoring Program under NASA [NNX09AL36G]; W.M. Keck Foundation; Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina) [GS-2011A-Q-16, GN-2011A-Q-14, GN-2012A-Q-32]; La Silla Paranal Observatory [086.A-0660, 088.A-0708, 089.A-0739]; European Southern Observatory, Chile (ESO Programmes) [086.A-0070, 087.A-0295, 089.A-0438, 091.A-0067]; NSF Telescope System Instrumentation Program (TSIP); Ohio Board of Regents; Ohio State University Office of Research; NASA; [AYA20102-2111-C03-01]; [PEX/10-CFQM-6444] FX We thank Gijs Nelemans for sharing the BPS DTD models with us, and Ori Fox, Patrick Kelly, Isaac Shivvers, Brad Tucker, and WeiKang Zheng for assistance with some of the Keck observations. Financial support for this work was provided by NASA through grants HST-GO-12060 and HST-GO-12099 from the Space Telescope Science Institute (STScI), which is operated by Associated Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. O.G. and D. M. acknowledge support by the I-CORE program of the PDC and the ISF, Grant 1829/12, and by a grant from the Israel Science Foundation. Support for S. R. was provided by NASA through Hubble Fellowship grant HF-51312.01 awarded by STScI. This work was supported by NASA Keck PI Data Awards (to Rutgers University, PI: S.W.J.), administered by the NASA Exoplanet Science Institute. Supernova research at Rutgers University is additionally supported by NSF CAREER award AST-0847157 to S.W.J. A. M. and N.B. acknowledge support from AYA20102-2111-C03-01 and PEX/10-CFQM-6444, and from the Spanish Ministerio de Educacion y Ciencia through grant AYA2006-14056 BES-2007-16280. M.N. is supported by PRIN INAF-2010. A. V. F. is also grateful for the support of NSF grant AST-1211916, the TABASGO Foundation, and the Christopher R. Redlich Fund. The Dark Cosmology Centre is funded by the Danish National Research Foundation. J.M.S. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. K.J., C. L., K. L., J.N., A.O., and H. E. R. were supported by the American Museum of Natural History's Science Research Mentoring Program under NASA grant award NNX09AL36G.; This work is based, in part, on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. Additional data presented here were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the Observatory was made possible by the generous financial support of the W.M. Keck Foundation. We wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.; Part of the research presented here is based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the NSF (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina) [ProgramsGS-2011A-Q-16, GN-2011A-Q-14, and GN-2012A-Q-32].; This research is based in part on observations made with ESO telescopes at the La Silla Paranal Observatory under program IDs 086.A-0660, 088.A-0708, and 089.A-0739; also, on observations collected at the European Southern Observatory, Chile (ESO Programmes 086.A-0070, 087.A-0295, 089.A-0438 and 091.A-0067).; We used data obtained with the MODS spectrographs built with funding from NSF grant AST-9987045 and the NSF Telescope System Instrumentation Program (TSIP), with additional funds from the Ohio Board of Regents and the Ohio State University Office of Research.; This research has made use of NASA's Astrophysics Data System (ADS) Bibliographic Services and of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 135 TC 40 Z9 40 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2014 VL 783 IS 1 AR 28 DI 10.1088/0004-637X/783/1/28 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600028 ER PT J AU Lane, BF Muterspaugh, MW Griffin, RF Scarfe, CD Fekel, FC Williamson, MH Eaton, JA Shao, M Colavita, MM Konacki, M AF Lane, Benjamin F. Muterspaugh, Matthew W. Griffin, R. F. Scarfe, C. D. Fekel, Francis C. Williamson, Michael H. Eaton, Joel A. Shao, M. Colavita, M. M. Konacki, Maciej TI THE ORBITS OF THE TRIPLE-STAR SYSTEM 1 GEMINORUM FROM PHASES DIFFERENTIAL ASTROMETRY AND SPECTROSCOPY SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: spectroscopic; stars: fundamental parameters; stars: individual (1 Gem); techniques: interferometric ID PALOMAR TESTBED INTERFEROMETER; RADIAL-VELOCITY SPECTROMETER; TIDAL FRICTION; BINARY ORBITS; TELESCOPE; CATALOG; INCLINATION; HERCULIS; DRACONIS; MASSES AB We have used precise differential astrometry from the Palomar High-precision Astrometric Search for Exoplanet Systems project and radial-velocity measurements covering a time span of 40 yr to determine the orbital parameters of the 1 Geminorum triple system. We present the first detection of the spectral lines of the third component of the system, together with precise mass (0.5%) and distance (0.15%) determinations for this system. In addition, our astrometry allows us to make the first determination of the mutual inclination of the orbits. C1 [Lane, Benjamin F.] Charles Stark Draper Lab Inc, Cambridge, MA 02139 USA. [Muterspaugh, Matthew W.] Tennessee State Univ, Coll Engn, Dept Math Sci, Nashville, TN 37209 USA. [Muterspaugh, Matthew W.; Fekel, Francis C.; Williamson, Michael H.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. [Griffin, R. F.] Univ Cambridge, Inst Astron, The Observatories, Cambridge CB3 0HA, England. [Scarfe, C. D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. [Shao, M.; Colavita, M. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Konacki, Maciej] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, PL-87100 Torun, Poland. RP Lane, BF (reprint author), Charles Stark Draper Lab Inc, 555 Technol Sq, Cambridge, MA 02139 USA. FU National Aeronautics and Space Administration; NASA; NSF; State of Tennessee's Centers of Excellence Program; Townes Postdoctoral Fellowship Program FX We wish to acknowledge the extraordinary observational efforts of K. Rykoski. He routinely put in extreme amounts of overtime to ensure successful operations and maintenance of an overwhelmingly complex instrument. He developed procedures and operations models that ensured the success of the observatory. The very low amount of lost time due to hardware failures at PTI is a result of his efforts and is unique in the field. Observations with PTI were made possible thanks to the efforts of the PTI Collaboration, which we acknowledge. We also thank the Dominion Astrophysical, Palomar, and Geneva observatories for allowing R. F. G. to obtain radial velocities of 1 Gem. We also thank Lou Boyd, Director of Fairborn Observatory, for dedication to robotic astronomy and excellent maintenance of a unique observatory. This research has made use of services from the Michelson Science Center, California Institute of Technology, http://msc.caltech.edu. Part of the work described in this paper was performed at the Jet Propulsion Laboratory under contract with the National Aeronautics and Space Administration. This research has made use of the Simbad database, operated at CDS, Strasbourg, France, and 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 NASA and the NSF. M.W.M. acknowledges support from State of Tennessee's Centers of Excellence Program and the Townes Postdoctoral Fellowship Program. NR 51 TC 1 Z9 1 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2014 VL 783 IS 1 AR 3 DI 10.1088/0004-637X/783/1/3 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600003 ER PT J AU Lien, A Sakamoto, T Gehrels, N Palmer, DM Barthelmy, SD Graziani, C Cannizzo, JK AF Lien, Amy Sakamoto, Takanori Gehrels, Neil Palmer, David M. Barthelmy, Scott D. Graziani, Carlo Cannizzo, John K. TI PROBING THE COSMIC GAMMA-RAY BURST RATE WITH TRIGGER SIMULATIONS OF THE SWIFT BURST ALERT TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: star formation; gamma-ray burst: general; stars: formation ID STAR-FORMATION HISTORY; LUMINOSITY FUNCTION; REDSHIFT DISTRIBUTION; SPECTRAL EVOLUTION; COMPLETE SAMPLE; RESOLUTION SPECTROSCOPY; PEAK ENERGY; GRB 091127; LONG; SUPERNOVA AB The gamma-ray burst (GRB) rate is essential for revealing the connection between GRBs, supernovae, and stellar evolution. Additionally, the GRB rate at high redshift provides a strong probe of star formation history in the early universe. While hundreds of GRBs are observed by Swift, it remains difficult to determine the intrinsic GRB rate due to the complex trigger algorithm of Swift. Current studies of the GRB rate usually approximate the Swift trigger algorithm by a single detection threshold. However, unlike the previously flown GRB instruments, Swift has over 500 trigger criteria based on photon count rate and an additional image threshold for localization. To investigate possible systematic biases and explore the intrinsic GRB properties, we develop a program that is capable of simulating all the rate trigger criteria and mimicking the image threshold. Our simulations show that adopting the complex trigger algorithm of Swift increases the detection rate of dim bursts. As a result, our simulations suggest that bursts need to be dimmer than previously expected to avoid overproducing the number of detections and to match with Swift observations. Moreover, our results indicate that these dim bursts are more likely to be high redshift events than low-luminosity GRBs. This would imply an even higher cosmic GRB rate at large redshifts than previous expectations based on star formation rate measurements, unless other factors, such as the luminosity evolution, are taken into account. The GRB rate from our best result gives a total number of 4568(-1429)(+825) GRBs per year that are beamed toward us in the whole universe. C1 [Lien, Amy; Cannizzo, John K.] CRESST, Greenbelt, MD 20771 USA. [Lien, Amy; Cannizzo, John K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lien, Amy; Cannizzo, John K.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. [Sakamoto, Takanori] Aoyama Gakuin Univ, Coll Sci & Engn, Dept Math & Phys, Chuo Ku, Sagamihara, Kanagawa 2525258, Japan. [Gehrels, Neil; Barthelmy, Scott D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Palmer, David M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Graziani, Carlo] Univ Chicago, Dept Astron, Chicago, IL 60637 USA. [Graziani, Carlo] Univ Chicago, Flash Ctr Computat Sci, Chicago, IL 60637 USA. RP Lien, A (reprint author), CRESST, Greenbelt, MD 20771 USA. FU NASA FX We are grateful for valuable discussions with Brian Fields, Brett Hayes, Daniel Kocevski, Judith Racusin, Jon Hakkila, Amir Shahmoradi, Lorenzo Amati, John Beacom, Jay Cummings, Antonino Cucchiara, and Dieter Hartmann. We also appreciate the helpful comments and suggestions from the anonymous referee. Amy Lien is supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 88 TC 22 Z9 22 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 MAR 1 PY 2014 VL 783 IS 1 AR 24 DI 10.1088/0004-637X/783/1/24 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600024 ER PT J AU Rawle, TD Egami, E Bussmann, RS Gurwell, M Ivison, RJ Boone, F Combes, F Danielson, ALR Rex, M Richard, J Smail, I Swinbank, AM Altieri, B Blain, AW Clement, B Dessauges-Zavadsky, M Edge, AC Fazio, GG Jones, T Kneib, JP Omont, A Perez-Gonzalez, PG Schaerer, D Valtchanov, I van der Werf, PP Walth, G Zamojski, M Zemcov, M AF Rawle, T. D. Egami, E. Bussmann, R. S. Gurwell, M. Ivison, R. J. Boone, F. Combes, F. Danielson, A. L. R. Rex, M. Richard, J. Smail, I. Swinbank, A. M. Altieri, B. Blain, A. W. Clement, B. Dessauges-Zavadsky, M. Edge, A. C. Fazio, G. G. Jones, T. Kneib, J. -P. Omont, A. Perez-Gonzalez, P. G. Schaerer, D. Valtchanov, I. van der Werf, P. P. Walth, G. Zamojski, M. Zemcov, M. TI [C II] AND (CO)-C-12(1-0) EMISSION MAPS IN HLSJ091828.6+514223: A STRONGLY LENSED INTERACTING SYSTEM AT z=5.24 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; galaxies: star formation; submillimeter: galaxies ID ULTRALUMINOUS INFRARED GALAXIES; STAR-FORMING GALAXIES; ACTIVE GALACTIC NUCLEI; LYMAN BREAK GALAXY; DEEP-FIELD-SOUTH; SUBMILLIMETER GALAXIES; MOLECULAR GAS; HIGH-REDSHIFT; INTERSTELLAR-MEDIUM; HERSCHEL-SPIRE AB We present Submillimeter Array [ C II] 158 mu m and Karl G. Jansky Very Large Array (CO)-C-12(1-0) line emission maps for the bright, lensed, submillimeter source at z = 5.2430 behind A 773: HLSJ091828.6+514223 (HLS0918). We combine these measurements with previously reported line profiles, including multiple 12CO rotational transitions, [C II], water, and [N II], providing some of the best constraints on the properties of the interstellarmedium in a galaxy at z > 5. HLS0918 has a total far-infrared (FIR) luminosity L-FIR(8-1000 mu m) = (1.6 +/- 0.1) x 1014 L-circle dot mu(-1), where the total magnification mu(total) = 8.9 +/- 1.9, via a new lens model from the [C II] and continuum maps. Despite a HyLIRG luminosity, the FIR continuum shape resembles that of a local LIRG. We simultaneously fit all of the observed spectral line profiles, finding four components that correspond cleanly to discrete spatial structures identified in the maps. The two most redshifted spectral components occupy the nucleus of a massive galaxy, with a source-plane separation < 1 kpc. The reddest dominates the continuum map (demagnified L-FIR,L- (component) = (1.1 +/- 0.2) x10(13) L-circle dot) and excites strong water emission in both nuclear components via a powerful FIR radiation field from the intense star formation. A third star-forming component is most likely a region of a merging companion (Delta V similar to 500 kms(-1)) exhibiting generally similar gas properties. The bluest component originates from a spatially distinct region and photodissociation region analysis suggests that it is lower density, cooler, and forming stars less vigorously than the other components. Strikingly, it has very strong [N II] emission, which may suggest an ionized, molecular outflow. This comprehensive view of gas properties and morphology in HLS0918 previews the science possible for a large sample of high-redshift galaxies once ALMA attains full sensitivity. C1 [Rawle, T. D.; Altieri, B.; Valtchanov, I.] ESA, ESAC, E-28691 Madrid, Spain. [Rawle, T. D.; Egami, E.; Rex, M.; Clement, B.; Perez-Gonzalez, P. G.; Walth, G.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Bussmann, R. S.; Gurwell, M.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ivison, R. J.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Boone, F.] Univ Toulouse, CNRS, UPS OMP, IRAP, F-310284 Toulouse, France. [Combes, F.] CNRS, LERMA, Observ Paris, F-75014 Paris, France. [Danielson, A. L. R.; Smail, I.; Swinbank, A. M.; Edge, A. C.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Richard, J.] Univ Lyon 1, CRAL, F-69561 St Genis Laval, France. [Blain, A. W.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Dessauges-Zavadsky, M.; Schaerer, D.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland. [Jones, T.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Kneib, J. -P.] Observ Sauverny, Lab Astrophys EPFL, CH-1290 Versoix, Switzerland. [Omont, A.] CNRS, Inst Astrophys Paris, F-75014 Paris, France. [Omont, A.] UPMC, UMR7095, F-75014 Paris, France. [Perez-Gonzalez, P. G.] Univ Complutense Madrid, Fac CC, Dept Astrofis, E-28040 Madrid, Spain. [Schaerer, D.] CNRS, IRAP, F-31400 Toulouse, France. [van der Werf, P. P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Rawle, TD (reprint author), ESA, ESAC, POB 78, E-28691 Madrid, Spain. EM tim.rawle@sciops.esa.int RI Kneib, Jean-Paul/A-7919-2015; Smail, Ian/M-5161-2013; Perez-Gonzalez, Pablo/J-2871-2016; Ivison, R./G-4450-2011; OI Kneib, Jean-Paul/0000-0002-4616-4989; Smail, Ian/0000-0003-3037-257X; Perez-Gonzalez, Pablo/0000-0003-4528-5639; Ivison, R./0000-0001-5118-1313; Edge, Alastair/0000-0002-3398-6916 FU European Space Agency (ESA) Research Fellowship at the European Space Astronomy Centre (ESAC), in Madrid, Spain; STFC; Leverhulme Fellowship; ERC Advanced Investigator program [DUSTYGAL 321334]; Royal Society/Wolfson Merit Award; Smithsonian Institution; Academia Sinica; INSU/CNRS (France); MPG (Germany); IGN (Spain); NASA through JPL/Caltech FX T.D.R. is supported by a European Space Agency (ESA) Research Fellowship at the European Space Astronomy Centre (ESAC), in Madrid, Spain. I. R. S. acknowledges support from STFC, a Leverhulme Fellowship, the ERC Advanced Investigator program DUSTYGAL 321334, and a Royal Society/Wolfson Merit Award.; The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. This work also includes observations carried out with the Karl G. Jansky Very Large Array (VLA): The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Additionally, based on observations carried out with the IRAM Plateau de Bure Interferometer and the IRAM 30 m Telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain).; This work follows on from observations made with the Herschel Space Observatory, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. We would also like to thank the HSC and NHSC consortia for support with data reduction. NR 96 TC 38 Z9 38 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2014 VL 783 IS 1 AR 59 DI 10.1088/0004-637X/783/1/59 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600059 ER PT J AU Turner, NJ Lee, MH Sano, T AF Turner, N. J. Lee, Man Hoi Sano, T. TI MAGNETIC COUPLING IN THE DISKS AROUND YOUNG GAS GIANT PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; astrochemistry; magnetohydrodynamics (MHD); planets and satellites: formation; turbulence ID PRIMORDIAL SOLAR NEBULA; WEAKLY IONIZED DISKS; HIGH-MASS PLANETS; PROTOPLANETARY DISKS; ACCRETION DISKS; MAGNETOROTATIONAL-INSTABILITY; PROTOSTELLAR DISKS; CIRCUMPLANETARY DISKS; REGULAR SATELLITES; DEAD ZONES AB conducting to experience turbulence driven by the magneto-rotational instability. By modeling the ionization and conductivity in the disk around proto-Jupiter, we find that turbulence is possible if the X-rays emitted near the Sun reach the planet's vicinity and either (1) the gas surface densities are in the range of the minimum-mass models constructed by augmenting Jupiter's satellites to solar composition, while dust is depleted from the disk atmosphere, or (2) the surface densities are much less, and in the range of gas-starved models fed with material from the solar nebula, but not so low that ambipolar diffusion decouples the neutral gas from the plasma. The results lend support to both minimum-mass and gas-starved models of the protojovian disk. (1) The dusty minimum-mass models have internal conductivities low enough to prevent angular momentum transfer by magnetic forces, as required for the material to remain in place while the satellites form. (2) The gas-starved models have magnetically active surface layers and a decoupled interior "dead zone." Similar active layers in the solar nebula yield accretion stresses in the range assumed in constructing the circumjovian gas-starved models. Our results also point to aspects of both classes of models that can be further developed. Non-turbulent minimum-mass models will lose dust from their atmospheres by settling, enabling gas to accrete through a thin surface layer. For the gas-starved models it is crucial to learn whether enough stellar X-ray and ultraviolet photons reach the circumjovian disk. Additionally, the stress-to-pressure ratio ought to increase with distance from the planet, likely leading to episodic accretion outbursts. C1 [Turner, N. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lee, Man Hoi] Univ Hong Kong, Dept Earth Sci, Hong Kong, Hong Kong, Peoples R China. [Lee, Man Hoi] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Sano, T.] Osaka Univ, Inst Laser Engn, Suita, Osaka 5650871, Japan. RP Turner, NJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM neal.turner@jpl.nasa.gov; mhlee@hku.hk; sano@ile.osaka-u.ac.jp RI Sano, Takayoshi/E-7860-2010 FU NASA [07-OPR07-0065]; Hong Kong Research Grants Council [HKU 7024/08P]; Center for Planetary Science at Kobe University under the auspices of the MEXT Global COE program titled "Foundation of International Center for Planetary Science" FX This work was supported by the NASA Outer Planets Research program through grant 07-OPR07-0065, by the Hong Kong Research Grants Council through grant HKU 7024/08P, and by the Center for Planetary Science at Kobe University under the auspices of the MEXT Global COE program titled "Foundation of International Center for Planetary Science." The work was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology. NR 89 TC 9 Z9 9 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2014 VL 783 IS 1 AR 14 DI 10.1088/0004-637X/783/1/14 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600014 ER PT J AU Velusamy, T Langer, WD Thompson, T AF Velusamy, T. Langer, W. D. Thompson, T. TI HiRes DECONVOLVED SPITZER IMAGES OF 89 PROTOSTELLAR JETS AND OUTFLOWS: NEW DATA ON THE EVOLUTION OF THE OUTFLOW MORPHOLOGY SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: ISM; ISM: jets and outflows; stars: formation; stars: protostars ID YOUNG STELLAR OBJECTS; WIDE-ANGLE OUTFLOWS; SCATTERED-LIGHT; CEPHEUS-E; MOLECULAR-HYDROGEN; ENVELOPE STRUCTURE; BIPOLAR OUTFLOWS; HIGH-VELOCITY; PROTOSTARS; SYSTEM AB To study the role of protosellar jets and outflows in the time evolution of the parent cores and the protostars, the astronomical community needs a large enough database of infrared images of protostars at the highest spatial resolution possible to reveal the details of their morphology. Spitzer provides unprecedented sensitivity in the infrared to study both the jet and outflow features, however, its spatial resolution is limited by its 0.85 m mirror. Here, we use a high-resolution deconvolution algorithm, "HiRes," to improve the visualization of spatial morphology by enhancing resolution (to subarcsecond levels in the IRAC bands) and removing the contaminating side lobes from bright sources in a sample of 89 protostellar objects. These reprocessed images are useful for detecting (1) wide-angle outflows seen in scattered light, (2) morphological details of H-2 emission in jets and bow shocks, and (3) compact features in MIPS 24 mu m images as protostar/disk and atomic/ionic line emission associated with the jets. The HiRes FITS image data of such a large homogeneous sample presented here will be useful to the community in studying these protostellar objects. To illustrate the utility of this HiRes sample, we show how the opening angle of the wide-angle outflows in 31 sources, all observed in the HiRes-processed Spitzer images, correlates with age. Our data suggest a power-law fit to opening angle versus age with an exponent of similar to 0.32 and 0.02, respectively, for ages <= 8000 yr and >= 8000 yr. C1 [Velusamy, T.; Langer, W. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Velusamy, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM velusamy@jpl.nasa.gov; William.D.Langer@jpl.nasa.gov; timthompson3@verizon.net FU National Aeronautics and Space Administration; National Science Foundation [AST-96-13717]; California Institute of Technology: USA Government FX We acknowledge Dr. C. A. Beichman for suggesting the development of the HiRes deconvolution tool for Spitzer images. We also thank the referee for helpful suggestions. This publication makes use of the Protostars webpage hosted by the University of Kent. This ADAP (ROSES 2009)-sponsored research was conducted at the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration. In 1997, the Owens Valley Radio Observatory millimeter array, which we used to observe CO, was supported by the National Science Foundation grant number AST-96-13717 (C) 2013. All rights reserved. California Institute of Technology: USA Government sponsorship acknowledged. NR 62 TC 10 Z9 10 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 MAR 1 PY 2014 VL 783 IS 1 AR 6 DI 10.1088/0004-637X/783/1/6 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600006 ER PT J AU Wang, J Xie, JW Barclay, T Fischer, DA AF Wang, Ji Xie, Ji-Wei Barclay, Thomas Fischer, Debra A. TI INFLUENCE OF STELLAR MULTIPLICITY ON PLANET FORMATION. I. EVIDENCE OF SUPPRESSED PLANET FORMATION DUE TO STELLAR COMPANIONS WITHIN 20 AU AND VALIDATION OF FOUR PLANETS FROM THE KEPLER MULTIPLE PLANET CANDIDATES SO ASTROPHYSICAL JOURNAL LA English DT Article DE astronomical databases: miscellaneous; methods: numerical; methods: observational; methods: statistical; planetary systems; planets and satellites: formation; techniques: radial velocities ID SOLAR-TYPE STARS; EXOPLANET HOST STARS; TRANSITING CIRCUMBINARY PLANET; SUN-LIKE STARS; BINARY-SYSTEMS; HABITABLE-ZONE; INPUT CATALOG; TIMING OBSERVATIONS; EXTRASOLAR PLANETS; FALSE POSITIVES AB The planet occurrence rate for multiple stars is important in two aspects. First, almost half of stellar systems in the solar neighborhood are multiple systems. Second, the comparison of the planet occurrence rate for multiple stars to that for single stars sheds light on the influence of stellar multiplicity on planet formation and evolution. We developed a method of distinguishing planet occurrence rates for single and multiple stars. From a sample of 138 bright (K-P < 13.5) Kepler multi-planet candidate systems, we compared the stellar multiplicity rate of these planet host stars to that of field stars. Using dynamical stability analyses and archival Doppler measurements, we find that the stellar multiplicity rate of planet host stars is significantly lower than field stars for semimajor axes less than 20 AU, suggesting that planet formation and evolution are suppressed by the presence of a close-in companion star at these separations. The influence of stellar multiplicity at larger separations is uncertain because of search incompleteness due to a limited Doppler observation time baseline and a lack of high-resolution imaging observation. We calculated the planet confidence for the sample of multi-planet candidates and find that the planet confidences for KOI 82.01, KOI 115.01, KOI 282.01, and KOI 1781.02 are higher than 99.7% and thus validate the planetary nature of these four planet candidates. This sample of bright Kepler multi-planet candidates with refined stellar and orbital parameters, planet confidence estimation, and nearby stellar companion identification offers a well-characterized sample for future theoretical and observational study. C1 [Wang, Ji; Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Xie, Ji-Wei] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Xie, Ji-Wei] Nanjing Univ, Dept Astron, Nanjing 210093, Jiangsu, Peoples R China. [Xie, Ji-Wei] Nanjing Univ, Key Lab Modern Astron & Astrophys, Minist Educ, Nanjing 210093, Jiangsu, Peoples R China. [Barclay, Thomas] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Barclay, Thomas] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA. RP Wang, J (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA. EM ji.wang@yale.edu OI Wang, Ji/0000-0002-4361-8885; Fischer, Debra/0000-0003-2221-0861 NR 88 TC 38 Z9 38 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2014 VL 783 IS 1 AR 4 DI 10.1088/0004-637X/783/1/4 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600004 ER PT J AU Schmidt, GA Kelley, M Nazarenko, L Ruedy, R Russell, GL Aleinov, I Bauer, M Bauer, SE Bhat, MK Bleck, R Canuto, V Chen, YH Cheng, Y Clune, TL Del Genio, A de Fainchtein, R Faluvegi, G Hansen, JE Healy, RJ Kiang, NY Koch, D Lacis, AA LeGrande, AN Lerner, J Lo, KK Matthews, EE Menon, S Miller, RL Oinas, V Oloso, AO Perlwitz, JP Puma, MJ Putman, WM Rind, D Romanou, A Sato, M Shindell, DT Sun, S Syed, RA Tausnev, N Tsigaridis, K Unger, N Voulgarakis, A Yao, MS Zhang, JL AF Schmidt, Gavin A. Kelley, Max Nazarenko, Larissa Ruedy, Reto Russell, Gary L. Aleinov, Igor Bauer, Mike Bauer, Susanne E. Bhat, Maharaj K. Bleck, Rainer Canuto, Vittorio Chen, Yong-Hua Cheng, Ye Clune, Thomas L. Del Genio, Anthony de Fainchtein, Rosalinda Faluvegi, Greg Hansen, James E. Healy, Richard J. Kiang, Nancy Y. Koch, Dorothy Lacis, Andy A. LeGrande, Allegra N. Lerner, Jean Lo, Ken K. Matthews, Elaine E. Menon, Surabi Miller, Ron L. Oinas, Valdar Oloso, Amidu O. Perlwitz, Jan P. Puma, Michael J. Putman, William M. Rind, David Romanou, Anastasia Sato, Makiko Shindell, Drew T. Sun, Shan Syed, Rahman A. Tausnev, Nick Tsigaridis, Kostas Unger, Nadine Voulgarakis, Apostolos Yao, Mao-Sung Zhang, Jinlun TI Configuration and assessment of the GISS ModelE2 contributions to the CMIP5 archive SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS LA English DT Review DE Climatology; Satellite Era; Climate model ID GENERAL-CIRCULATION MODEL; GLOBAL CLIMATE MODELS; ARCTIC SEA-ICE; RADIATION BUDGET; SURFACE-TEMPERATURE; TROPOSPHERIC OZONE; CLOUD MICROPHYSICS; OCEAN CIRCULATION; ATMOSPHERE MODEL; GREENHOUSE GASES AB We present a description of the ModelE2 version of the Goddard Institute for Space Studies (GISS) General Circulation Model (GCM) and the configurations used in the simulations performed for the Coupled Model Intercomparison Project Phase 5 (CMIP5). We use six variations related to the treatment of the atmospheric composition, the calculation of aerosol indirect effects, and ocean model component. Specifically, we test the difference between atmospheric models that have noninteractive composition, where radiatively important aerosols and ozone are prescribed from precomputed decadal averages, and interactive versions where atmospheric chemistry and aerosols are calculated given decadally varying emissions. The impact of the first aerosol indirect effect on clouds is either specified using a simple tuning, or parameterized using a cloud microphysics scheme. We also use two dynamic ocean components: the Russell and HYbrid Coordinate Ocean Model (HYCOM) which differ significantly in their basic formulations and grid. Results are presented for the climatological means over the satellite era (1980-2004) taken from transient simulations starting from the preindustrial (1850) driven by estimates of appropriate forcings over the 20th Century. Differences in base climate and variability related to the choice of ocean model are large, indicating an important structural uncertainty. The impact of interactive atmospheric composition on the climatology is relatively small except in regions such as the lower stratosphere, where ozone plays an important role, and the tropics, where aerosol changes affect the hydrological cycle and cloud cover. While key improvements over previous versions of the model are evident, these are not uniform across all metrics. C1 [Schmidt, Gavin A.; Kelley, Max; Nazarenko, Larissa; Ruedy, Reto; Russell, Gary L.; Aleinov, Igor; Bauer, Mike; Bauer, Susanne E.; Bleck, Rainer; Canuto, Vittorio; Chen, Yong-Hua; Cheng, Ye; Del Genio, Anthony; Faluvegi, Greg; Hansen, James E.; Healy, Richard J.; Kiang, Nancy Y.; Lacis, Andy A.; LeGrande, Allegra N.; Lerner, Jean; Lo, Ken K.; Matthews, Elaine E.; Miller, Ron L.; Oinas, Valdar; Perlwitz, Jan P.; Puma, Michael J.; Rind, David; Romanou, Anastasia; Sato, Makiko; Shindell, Drew T.; Sun, Shan; Tausnev, Nick; Tsigaridis, Kostas; Voulgarakis, Apostolos; Yao, Mao-Sung] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Schmidt, Gavin A.; Kelley, Max; Nazarenko, Larissa; Ruedy, Reto; Russell, Gary L.; Aleinov, Igor; Bauer, Mike; Bauer, Susanne E.; Bleck, Rainer; Canuto, Vittorio; Chen, Yong-Hua; Cheng, Ye; Del Genio, Anthony; Faluvegi, Greg; Hansen, James E.; Healy, Richard J.; Kiang, Nancy Y.; Koch, Dorothy; Lacis, Andy A.; LeGrande, Allegra N.; Lerner, Jean; Lo, Ken K.; Matthews, Elaine E.; Miller, Ron L.; Oinas, Valdar; Perlwitz, Jan P.; Puma, Michael J.; Rind, David; Romanou, Anastasia; Sato, Makiko; Shindell, Drew T.; Sun, Shan; Tausnev, Nick; Tsigaridis, Kostas; Voulgarakis, Apostolos; Yao, Mao-Sung] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Kelley, Max; Ruedy, Reto; Chen, Yong-Hua; Lo, Ken K.; Oinas, Valdar; Sato, Makiko; Sun, Shan; Tausnev, Nick; Yao, Mao-Sung] Trinnovim LLC, New York, NY USA. [Bauer, Mike; Bleck, Rainer; Perlwitz, Jan P.; Romanou, Anastasia] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. [de Fainchtein, Rosalinda; Oloso, Amidu O.; Putman, William M.; Syed, Rahman A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Menon, Surabi] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Unger, Nadine] Yale Univ, New Haven, CT USA. [Zhang, Jinlun] Univ Washington, Seattle, WA 98195 USA. RP Schmidt, GA (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM Gavin.A.Schmidt@nasa.gov RI Schmidt, Gavin/D-4427-2012; Miller, Ron/E-1902-2012; Bauer, Susanne/P-3082-2014; Healy, Richard/J-9214-2015; Sun, Shan/H-2318-2015; Shindell, Drew/D-4636-2012; Unger, Nadine/M-9360-2015 OI Schmidt, Gavin/0000-0002-2258-0486; Healy, Richard/0000-0002-5098-8921; FU NASA Modeling, Analysis, and Prediction program; NOAA Climate and Global Change Program FX Climate modeling at GISS is supported by the NASA Modeling, Analysis, and Prediction program, and 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. MSU data are produced by Remote Sensing Systems and sponsored by the NOAA Climate and Global Change Program and are available at www.remss.com. ERA-Interim data are available from the European Center for Medium Range Weather Forecasting (ECMWF) http://www.ecmwf.int/research/era. CERES data are available from http://ceres.larc.nasa.gov. The blended AIRS-SSMI column water vapor data were produced by W. Kovari. We thank two reviewers for constructive comments on an earlier draft. NR 161 TC 146 Z9 147 U1 5 U2 54 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1942-2466 J9 J ADV MODEL EARTH SY JI J. Adv. Model. Earth Syst. PD MAR PY 2014 VL 6 IS 1 BP 141 EP 184 DI 10.1002/2013MS000265 PG 44 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AF7AV UT WOS:000334866700010 ER PT J AU Ovchinnikov, M Ackerman, AS Avramov, A Cheng, AN Fan, JW Fridlind, AM Ghan, S Harrington, J Hoose, C Korolev, A McFarquhar, GM Morrison, H Paukert, M Savre, J Shipway, BJ Shupe, MD Solomon, A Sulia, K AF Ovchinnikov, Mikhail Ackerman, Andrew S. Avramov, Alexander Cheng, Anning Fan, Jiwen Fridlind, Ann M. Ghan, Steven Harrington, Jerry Hoose, Corinna Korolev, Alexei McFarquhar, Greg M. Morrison, Hugh Paukert, Marco Savre, Julien Shipway, Ben J. Shupe, Matthew D. Solomon, Amy Sulia, Kara TI Intercomparison of large-eddy simulations of Arctic mixed-phase clouds: Importance of ice size distribution assumptions SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS LA English DT Article DE ice size distribution; cloud microphysics; mixed-phase clouds; large-eddy simulations; Arctic clouds ID MICROPHYSICS PARAMETERIZATION; ATMOSPHERIC AEROSOLS; MODEL DESCRIPTION; PART I; STRATOCUMULUS; SCHEME; LAYER; VAPOR; FORMULATION; CRYSTALS AB Large-eddy simulations of mixed-phase Arctic clouds by 11 different models are analyzed with the goal of improving understanding and model representation of processes controlling the evolution of these clouds. In a case based on observations from the Indirect and Semi-Direct Aerosol Campaign (ISDAC), it is found that ice number concentration, N-i, exerts significant influence on the cloud structure. Increasing N-i leads to a substantial reduction in liquid water path (LWP), in agreement with earlier studies. In contrast to previous intercomparison studies, all models here use the same ice particle properties (i.e., mass-size, mass-fall speed, and mass-capacitance relationships) and a common radiation parameterization. The constrained setup exposes the importance of ice particle size distributions (PSDs) in influencing cloud evolution. A clear separation in LWP and IWP predicted by models with bin and bulk microphysical treatments is documented and attributed primarily to the assumed shape of ice PSD used in bulk schemes. Compared to the bin schemes that explicitly predict the PSD, schemes assuming exponential ice PSD underestimate ice growth by vapor deposition and overestimate mass-weighted fall speed leading to an underprediction of IWP by a factor of two in the considered case. Sensitivity tests indicate LWP and IWP are much closer to the bin model simulations when a modified shape factor which is similar to that predicted by bin model simulation is used in bulk scheme. These results demonstrate the importance of representation of ice PSD in determining the partitioning of liquid and ice and the longevity of mixed-phase clouds. C1 [Ovchinnikov, Mikhail; Fan, Jiwen; Ghan, Steven] Pacific NW Natl Lab, Richland, WA 99352 USA. [Ackerman, Andrew S.; Fridlind, Ann M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Avramov, Alexander] MIT, Ctr Global Change Sci, Cambridge, MA 02139 USA. [Cheng, Anning] Sci Syst & Applicat Inc, NASA LaRC, Hampton, VA USA. [Harrington, Jerry] Penn State Univ, Dept Meteorol, State Coll, PA USA. [Hoose, Corinna; Paukert, Marco] Karlsruhe Inst Technol, D-76021 Karlsruhe, Germany. [Korolev, Alexei] Environm Canada, Toronto, ON, Canada. [McFarquhar, Greg M.] Univ Illinois, Dept Atmospher Sci, Urbana, IL USA. [Morrison, Hugh] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Savre, Julien] Stockholm Univ, Dept Meteorol, S-10691 Stockholm, Sweden. [Shipway, Ben J.] Met Off, Exeter, Devon, England. [Shupe, Matthew D.; Solomon, Amy] Univ Colorado, NOAA, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Sulia, Kara] Princeton Univ, Geophys Fluid Dynam Lab, Princeton, NJ 08544 USA. RP Ovchinnikov, M (reprint author), Pacific NW Natl Lab, Richland, WA 99352 USA. EM mikhail@pnnl.gov RI Solomon, Amy/L-8988-2013; Hoose, Corinna/A-4295-2009; Fan, Jiwen/E-9138-2011; Shupe, Matthew/F-8754-2011; Ackerman, Andrew/D-4433-2012; Ghan, Steven/H-4301-2011; OI Hoose, Corinna/0000-0003-2827-5789; Shupe, Matthew/0000-0002-0973-9982; Ackerman, Andrew/0000-0003-0254-6253; Ghan, Steven/0000-0001-8355-8699; McFarquhar, Greg/0000-0003-0950-0135 FU Office of Biological and Environmental Research (OBER) of the U.S. Department of Energy (DOE) as part of the Atmospheric System Research Program (ASR); DOE, Office of Science, OBER; Battelle for the DOE [DE-AC06-76RLO 1830]; U.S. DOE, OBER; Office of Science of the U.S. DOE; DOE Office of Science, OBER; NASA Radiation Sciences Program; U.S. DOE [DE-SC0007005]; US DOE ASR [DE-SC0001279, DE-SC0008500]; U.S. DOE ASR [DE-SC0008648, DE-SC0005336]; NASA [NNX12AH90G]; National Science Foundation [AGS-0951807]; Department of Energy [DE-FG02-05ER64058]; Helmholtz Association through the Climate Initiative REKLIM; President's Initiative and Networking Fund; DOE Office of Science Graduate Fellowship Program (DOE SCGF); DOE [DE-AC05-06OR23100] FX This work was supported by the Office of Biological and Environmental Research (OBER) of the U.S. Department of Energy (DOE) as part of the Atmospheric System Research Program (ASR). Data were obtained from the ARM program archive, sponsored by DOE, Office of Science, OBER. The Pacific Northwest National Laboratory (PNNL) is operated by Battelle for the DOE under contract DE-AC06-76RLO 1830. This research was performed in part using the Molecular Science Computing Facility (MSCF) in the Environmental Molecular Sciences Laboratory (EMSL), a national scientific user facility sponsored by the U.S. DOE, OBER and located at PNNL. M.O. is grateful to Marat Khairoutdinov for providing the System for Atmospheric Modeling (SAM) and Alexander Khain for the microphysics code used in this study. We thank Michael Earle and Peter Liu of Environment Canada for providing aerosol size distributions and Peter Blossey for assistance with offline radiation calculations. ASA and AMF used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. DOE, and were supported by the DOE Office of Science, OBER, and the NASA Radiation Sciences Program. M.D.S. and A. S. were supported by U.S. DOE grant DE-SC0007005. G.M.M. was partially supported by US DOE ASR grants DE-SC0001279 and DE-SC0008500. H.M. was partially supported by U.S. DOE ASR grants DE-SC0008648 and DE-SC0005336, subawarded through NASA NNX12AH90G. J.H. was supported by the National Science Foundation for under grant AGS-0951807 and the Department of Energy under grant DE-FG02-05ER64058. C.H. and M.P. were funded by the Helmholtz Association through the Climate Initiative REKLIM and the President's Initiative and Networking Fund. K.S. was supported by an award from the DOE Office of Science Graduate Fellowship Program (DOE SCGF). The DOE SCGF Program was made possible in part by the American Recovery and Reinvestment Act of 2009. The DOE SCGF program is administered by the Oak Ridge Institute for Science and Education (ORISE) for the DOE. ORISE is managed by Oak Ridge Associated Universities (ORAU) under DOE contract DE-AC05-06OR23100. All opinions expressed in this paper are the author's and do not necessarily reflect the policies and views of DOE, ORAU, or ORISE. NR 48 TC 18 Z9 18 U1 3 U2 25 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1942-2466 J9 J ADV MODEL EARTH SY JI J. Adv. Model. Earth Syst. PD MAR PY 2014 VL 6 IS 1 BP 223 EP 248 DI 10.1002/2013MS000282 PG 26 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AF7AV UT WOS:000334866700013 ER PT J AU McGrath, D Steffen, K Holland, PR Scambos, T Rajaram, H Abdalati, W Rignot, E AF McGrath, Daniel Steffen, Konrad Holland, Paul R. Scambos, Ted Rajaram, Harihar Abdalati, Waleed Rignot, Eric TI The structure and effect of suture zones in the Larsen C Ice Shelf, Antarctica SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE LA English DT Article DE ice shelves; suture zone; fracture; GPR ID BASAL CREVASSES; PENINSULA; PROPAGATION; STABILITY; SHEET; MODEL; RIFT; FLOW AB Ice shelf fractures frequently terminate where they encounter suture zones, regions of material heterogeneity that form between meteoric inflows in ice shelves. This heterogeneity can consist of marine ice, meteoric ice with modified rheological properties, or the presence of fractures. Here, we use radar observations on the Larsen C Ice Shelf, Antarctica, to investigate (i) the termination of a 25km long rift in the Churchill Peninsula suture zone, which was found to contain similar to 60m of accreted marine ice, and (ii) the along-flow evolution of a suture zone originating at Cole Peninsula. We determine a steady state field of basal melting/freezing rates and apply it to a flowline model to delineate the along-flow evolution of layers within the ice shelf. The thickening surface wedge of locally accumulated meteoric ice, which likely has limited lateral variation in its mechanical properties, accounts for similar to 60% of the total ice thickness near the calving front. Thus, we infer that the lower similar to 40% of the ice column and the material heterogeneities present there are responsible for resisting fracture propagation and thereby delaying tabular calving events, as demonstrated in the >40year time series leading up to the 2004/2005 calving event for Larsen C. This likely represents a highly sensitive aspect of ice shelf stability, as changes in the oceanic forcing may lead to the loss of this heterogeneity. C1 [McGrath, Daniel; Abdalati, Waleed] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Steffen, Konrad] Swiss Fed Inst Forest Snow & Landscape Res, CH-8903 Birmensdorf, Switzerland. [Steffen, Konrad] Swiss Fed Inst Technol, Zurich, Switzerland. [Steffen, Konrad] Ecole Polytech Fed Lausanne, CH-1015 Lausanne, Switzerland. [Holland, Paul R.] British Antarctic Survey, Cambridge CB3 0ET, England. [Scambos, Ted] Univ Colorado, Natl Snow & Ice Data Ctr CIRES, Boulder, CO 80309 USA. [Rajaram, Harihar] Univ Colorado, Dept Civil Engn, Boulder, CO 80309 USA. [Rignot, Eric] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. [Rignot, Eric] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP McGrath, D (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. EM daniel.mcgrath@colorado.edu RI Holland, Paul/G-2796-2012; Steffen, Konrad/C-6027-2013; Rignot, Eric/A-4560-2014; OI Steffen, Konrad/0000-0001-8658-1026; Rignot, Eric/0000-0002-3366-0481; MCGRATH, DANIEL/0000-0002-9462-6842 FU NSF OPP [0732946]; Polar Geospatial Center under NSF OPP [ANT-1043681] FX This work is funded by NSF OPP research grant 0732946. The British Antarctic Survey and field assistant, Tom Weston, provided exceptional field support, without which this work would not have been possible. Geospatial support for this work was supported by the Polar Geospatial Center under NSF OPP agreement ANT-1043681. We thank Jan Lenaerts and Michael van den Broeke for the RACMO2.1/Ant surface mass balance data and Jenny Griggs for the surface elevation data. We thank the Editor Hubbard and three anonymous reviewers for their constructive insights that significantly improved the manuscript. NR 44 TC 4 Z9 4 U1 2 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9003 EI 2169-9011 J9 J GEOPHYS RES-EARTH JI J. Geophys. Res.-Earth Surf. PD MAR PY 2014 VL 119 IS 3 BP 588 EP 602 DI 10.1002/2013JF002935 PG 15 WC Geosciences, Multidisciplinary SC Geology GA AE9WR UT WOS:000334362800011 ER PT J AU Espirito-Santo, FDB Gloor, M Keller, M Malhi, Y Saatchi, S Nelson, B Oliveira, RC Pereira, C Lloyd, J Frolking, S Palace, M Shimabukuro, YE Duarte, V Mendoza, AM Lopez-Gonzalez, G Baker, TR Feldpausch, TR Brienen, RJW Asner, GP Boyd, DS Phillips, OL AF Espirito-Santo, Fernando D. B. Gloor, Manuel Keller, Michael Malhi, Yadvinder Saatchi, Sassan Nelson, Bruce Oliveira Junior, Raimundo C. Pereira, Cleuton Lloyd, Jon Frolking, Steve Palace, Michael Shimabukuro, Yosio E. Duarte, Valdete Mendoza, Abel Monteagudo Lopez-Gonzalez, Gabriela Baker, Tim R. Feldpausch, Ted R. Brienen, Roel J. W. Asner, Gregory P. Boyd, Doreen S. Phillips, Oliver L. TI Size and frequency of natural forest disturbances and the Amazon forest carbon balance SO NATURE COMMUNICATIONS LA English DT Article ID ABOVEGROUND LIVE BIOMASS; TROPICAL FORESTS; BRAZILIAN AMAZON; RAIN-FOREST; LARGE BLOWDOWNS; PLOTS; DYNAMICS; BASIN; STATE AB Forest inventory studies in the Amazon indicate a large terrestrial carbon sink. However, field plots may fail to represent forest mortality processes at landscape-scales of tropical forests. Here we characterize the frequency distribution of disturbance events in natural forests from 0.01 ha to 2,651 ha size throughout Amazonia using a novel combination of forest inventory, airborne lidar and satellite remote sensing data. We find that small-scale mortality events are responsible for aboveground biomass losses of similar to 1.7 Pg Cy-1 over the entire Amazon region. We also find that intermediate-scale disturbances account for losses of similar to 0.2 Pg Cy-1, and that the largest-scale disturbances as a result of blow-downs only account for losses of similar to 0.004 Pg Cy-1. Simulation of growth and mortality indicates that even when all carbon losses from intermediate and large-scale disturbances are considered, these are outweighed by the net biomass accumulation by tree growth, supporting the inference of an Amazon carbon sink. C1 [Espirito-Santo, Fernando D. B.; Saatchi, Sassan] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Espirito-Santo, Fernando D. B.; Keller, Michael; Frolking, Steve; Palace, Michael] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Gloor, Manuel; Lloyd, Jon; Lopez-Gonzalez, Gabriela; Baker, Tim R.; Feldpausch, Ted R.; Brienen, Roel J. W.; Phillips, Oliver L.] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. [Keller, Michael] USDA, Forest Serv, Int Inst Trop Forestry, San Juan, PR 00926 USA. [Keller, Michael] EMBRAPA Monitoramento Satelite, BR-13070115 Campinas, SP, Brazil. [Malhi, Yadvinder] Univ Oxford, Sch Geog & Environm, Environm Change Inst, Oxford OX1 3QY, England. [Nelson, Bruce] Natl Inst Res Amazonia INPA, BR-69011970 Manaus, Amazonas, Brazil. [Oliveira Junior, Raimundo C.] EMBRAPA Amazonia Oriental CPATU, BR-68035110 Santarem, Para, Brazil. [Lloyd, Jon] James Cook Univ, Sch Earth & Environm Sci, Ctr Trop Environm & Sustainabil Sci TESS, Cairns, Qld 4878, Australia. [Shimabukuro, Yosio E.; Duarte, Valdete] Natl Inst Space Res INPE, BR-12227010 Sao Jose Dos Campos, SP, Brazil. [Mendoza, Abel Monteagudo] Jardin Bot Missouri, Oxapampa 19231, Pasco, Peru. [Asner, Gregory P.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. [Boyd, Doreen S.] Univ Nottingham, Sch Geog, Nottingham NG7 2RD, England. RP Espirito-Santo, FDB (reprint author), CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91109 USA. EM f.delbon@gmail.com RI Phillips, Oliver/A-1523-2011; Lloyd, Jonathan/F-8893-2010; Feldpausch, Ted/D-3436-2009; James Cook University, TESS/B-8171-2012; Espirito-Santo, Fernando/O-4371-2014; Asner, Gregory/G-9268-2013; Keller, Michael/A-8976-2012 OI Phillips, Oliver/0000-0002-8993-6168; Lloyd, Jonathan/0000-0002-5458-9960; Feldpausch, Ted/0000-0002-6631-7962; Espirito-Santo, Fernando/0000-0001-7497-3639; Asner, Gregory/0000-0001-7893-6421; Keller, Michael/0000-0002-0253-3359 FU NASA Earth System Science Fellowship (NESSF) [NNX07AN84N]; NASA Terrestrial Ecology Program; CalTech Postdoctoral Fellowship at JPL; NERC [NE/F005806/1]; European Research Council; Brazilian Ministry of Science and Technology; National Institute for Research in Amazonia (INPA); Moore Foundation FX This research was supported by the NASA Earth System Science Fellowship (NESSF) Grant no. NNX07AN84N (F.D.B.E.-S. and M. K.), the NASA Terrestrial Ecology Program contribution to the Large Scale Biosphere-Atmosphere Experiment in the Amazon (LBA), CalTech Postdoctoral Fellowship at JPL (F.D.B.E.-S.), NERC consortia projects, AMAZONICA (NE/F005806/1, TROBIT) for support of RAINFOR and M. G., R.J.W.B., O.L.P., T. R. F., G. L-G., J.L. and Y.M., and two grants from the European Research Council (T-FORCES, O.L.P.; GEOCARBON, M. G., O.L.P. and Y.M. L.). We thank the Brazilian Ministry of Science and Technology for its support of the LBA program and the National Institute for Research in Amazonia (INPA) for implementation of this program. Development of the RAINFOR network including measurement of biomass dynamics has been supported by 34 different grants, especially the Moore Foundation. We thank the authorities in Bolivia, Brazil, Colombia, Ecuador, Guyana, Peru and Venezuela, and colleagues across the region for support. We are grateful to Dr Jeff Chambers who brought several of us together in an excellent meeting in 2006 at Tulane University where the idea for quantifying the disturbance spectrum was born. The Carnegie Airborne Observatory is made possible by Moore Foundation, the Grantham Foundation for the Protection of the Environment, the John D. and Catherine T. MacArthur Foundation, the Avatar Alliance Foundation, the W.M. Keck Foundation, the Margaret A. Cargill Foundation, Mary Anne Nyburg Baker and G. Leonard Baker Jr, and William R. Hearst III. NR 30 TC 33 Z9 34 U1 4 U2 62 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 MAR PY 2014 VL 5 AR 3434 DI 10.1038/ncomms4434 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AE9CA UT WOS:000334300400017 PM 24643258 ER PT J AU Jacobson, AR Holzworth, RH Pfaff, R Heelis, R Colestock, P AF Jacobson, Abram R. Holzworth, Robert H. Pfaff, Robert Heelis, Roderick Colestock, Patrick TI A method to estimate whistler wave vector from polarization using three-component electric field data SO RADIO SCIENCE LA English DT Article DE whistler polarization ID LIGHTNING LOCATION NETWORK; SATELLITE; PROPAGATION; IONOSPHERE; DEMETER; SIGNALS AB Satellites in the Earth's magnetosphere can be used to record the rich electromagnetic wave activity due to terrestrial lightning, typically up to several tens of kilohertz. With simultaneous recordings of the three components of wave electric field E and of the three components of wave magnetic field B, the entire wavefield, polarization, and wave vector can be specified without any appeal to a priori assumptions about the wave mode and without any reliance on the validity of a dispersion relation. However, some satellites lack such a complete suite of measurements. We develop a method which assumes the theoretical dispersion relation for whistler waves then uses recordings of the three components of wave electric field E but no magnetic components to derive the wave polarization and the wave vector (up to a sign ambiguity on the latter). The method can work only because the dispersion relation, which is assumed, already contains information from the full Maxwell's equations. We illustrate the method with 12s duration simultaneous recordings, at 32kilosample/s, of three orthogonal components of wave electric field E from the C/NOFS satellite in low-Earth orbit. Our particular example in this article is shown to contain two broadband whistler features in the range of 4-15kHz, whose wave vectors differ both according to their polar angles from the geomagnetic field B-0 and according to their azimuth around the geomagnetic field B-0. Key Points Wave vector obtained from 3-D wave electric field Allows satellite VLF data of three-component E to be interpreted C1 [Jacobson, Abram R.; Holzworth, Robert H.] Univ Washington, Earth & Space Sci Dept, Seattle, WA 98195 USA. [Pfaff, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Heelis, Roderick] Univ Texas Dallas, Ctr Space Sci, Richardson, TX 75083 USA. [Colestock, Patrick] Los Alamos Natl Lab, ISR 1, Los Alamos, NM USA. RP Jacobson, AR (reprint author), Univ Washington, Earth & Space Sci Dept, Seattle, WA 98195 USA. EM abramj@u.washington.edu FU DARPA Nimbus project FX Two authors (A.R.J. and R.H.H.) were supported in this work by the DARPA Nimbus project administered by Mathew Goodman. NR 27 TC 2 Z9 2 U1 1 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0048-6604 EI 1944-799X J9 RADIO SCI JI Radio Sci. PD MAR PY 2014 VL 49 IS 3 BP 131 EP 145 DI 10.1002/2013RS005335 PG 15 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA AE9XM UT WOS:000334365500001 ER PT J AU Helmboldt, JF Ellingson, SW Hartman, JM Lazio, TJW Taylor, GB Wilson, TL Wolfe, CN AF Helmboldt, J. F. Ellingson, S. W. Hartman, J. M. Lazio, T. J. W. Taylor, G. B. Wilson, T. L. Wolfe, C. N. TI All-sky imaging of meteor trails at 55.25 MHz with the first station of the LongWavelength Array SO RADIO SCIENCE LA English DT Article DE meteor trail; VHF; interferometry ID AMBIPOLAR DIFFUSION; ORBIT-RADAR; ECHOES; METHODOLOGY; ATMOSPHERE; DURATION; SPECTRUM; SYSTEM; ALTAIR; LIDAR AB A new capability for high-sensitivity, all-sky monitoring of VHF meteor trail reflections with the first station of the Long Wavelength Array, or "LWA1", is described. LWA1 is a similar to 100 m diameter HF/VHF array of 256 crossed-dipole antennas with a unique transient buffer mode that allows it to monitor for meteor trails via all-sky imaging with the same sensitivity as a single-dish antenna >= 40 m in diameter. To demonstrate this capability, we have used a 2 h observing run conducted in August 2012 aimed at detecting and characterizing meteor trail reflections of analog TV transmissions at 55.25 MHz. The analysis techniques described here allowed for a detection rate of similar to 9500 trails per hour, including the detection of two meteor streams with radiants in the Aries/Perseus and Aquila/Hercules regions that were not previously reported in the literature. In addition, we have found a population of relatively long-duration (similar to 1 to a few minutes), typically faint trails. These trails have implied horizontal speeds of 15-130 m s(-1), with a typical speed of similar to 30m s(-1). We have also used high-resolution time series of the brightest trails to characterize decay times over a relatively large geographical area (10 degrees x7 degrees in longitude and latitude) and on short (similar to 5 min) time scales. Potential enhancements that could be enabled by the addition of more LWA stations are discussed. C1 [Helmboldt, J. F.; Wilson, T. L.] US Naval Res Lab, Washington, DC USA. [Ellingson, S. W.; Wolfe, C. N.] Virginia Polytech Inst & State Univ, Bradley Dept Elect & Comp Engn, Blacksburg, VA 24061 USA. [Hartman, J. M.; Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Taylor, G. B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Taylor, G. B.] Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Helmboldt, JF (reprint author), US Naval Res Lab, Washington, DC USA. EM joe.helmboldt@nrl.navy.mil RI Helmboldt, Joseph/C-8105-2012 FU Office of Naval Research [N00014-07-C=0147]; National Science Foundation of the University Radio Observatory program [AST-1139963, AST-1139974] FX Basic research in astronomy at the Naval Research Laboratory is supported by 6.1 Base funding. Construction of the LWA has been supported by the Office of Naval Research under Contract N00014-07-C=0147. Support for operations and continuing development of the LWA1 is provided by the National Science Foundation under grants AST-1139963 and AST-1139974 of the University Radio Observatory program. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 47 TC 3 Z9 3 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0048-6604 EI 1944-799X J9 RADIO SCI JI Radio Sci. PD MAR PY 2014 VL 49 IS 3 BP 157 EP 180 DI 10.1002/2013RS005220 PG 24 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA AE9XM UT WOS:000334365500003 ER PT J AU Neigh, CSR Masek, JG Bourget, P Cook, B Huang, CQ Rishmawi, K Zhao, F AF Neigh, Christopher S. R. Masek, Jeffrey G. Bourget, Paul Cook, Bruce Huang, Chengquan Rishmawi, Khaldoun Zhao, Feng TI Deciphering the Precision of Stereo IKONOS Canopy Height Models for US Forests with G-LiHT Airborne LiDAR SO REMOTE SENSING LA English DT Article DE canopy height model; US; forest; G-LiHT; IKONOS; stereo ID RESOLUTION SATELLITE IMAGERY; DIGITAL ELEVATION MODELS; SENSOR ORIENTATION; DSM GENERATION; URBAN AREAS; BIOMASS; CARBON; COMBINATION; RECONSTRUCTION; EXTRACTION AB Few studies have evaluated the precision of IKONOS stereo data for measuring forest canopy height. The high cost of airborne light detection and ranging (LiDAR) data collection for large area studies and the present lack of a spaceborne instrument lead to the need to explore other low cost options. The US Government currently has access to a large archive of commercial high-resolution imagery, which could be quite valuable to forest structure studies. At 1 m resolution, we here compared canopy height models (CHMs) and height data derived from Goddard's airborne LiDAR Hyper-spectral and Thermal Imager (G-LiHT) with three types of IKONOS stereo derived digital surface models (DSMs) that estimate CHMs by subtracting National Elevation Data (NED) digital terrain models (DTMs). We found the following in three different forested regions of the US after excluding heterogeneous and disturbed forest samples: (1) G-LiHT DTMs were highly correlated with NED DTMs with R-2 > 0.98 and root mean square errors (RMSEs) < 2.96 m; (2) when using one visually identifiable ground control point (GCP) from NED, G-LiHT DSMs and IKONOS DSMs had R-2 > 0.84 and RMSEs of 2.7 to 4.1 m; and (3) one GCP CHMs for two study sites had R-2 > 0.7 and RMSEs of 2.6 to 3 m where data were collected less than four years apart. Our results suggest that IKONOS stereo data are a useful LiDAR alternative where high-quality DTMs are available. C1 [Neigh, Christopher S. R.; Masek, Jeffrey G.; Cook, Bruce] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Bourget, Paul] Univ So Maine, Muskie Sch Publ Serv, Geog Anthropol Program, Portland, ME 04104 USA. [Huang, Chengquan; Rishmawi, Khaldoun; Zhao, Feng] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. RP Neigh, CSR (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA. EM christopher.s.neigh@nasa.gov; jeffrey.g.masek@nasa.gov; paulbourget737@gmail.com; bruce.cook@nasa.gov; cqhuang@umd.edu; rishmawi@umd.edu; zhao26@umd.edu RI Neigh, Christopher/D-4700-2012; Masek, Jeffrey/D-7673-2012; OI Neigh, Christopher/0000-0002-5322-6340; Huang, Chengquan/0000-0003-0055-9798 FU NASA [NNH08ZDA001N-TE, NNH10ZDA001N-CARBON] FX This study was made possible by NASA's Terrestrial Ecology program under grants NNH08ZDA001N-TE and NNH10ZDA001N-CARBON. We would also like to thank three anonymous reviewers who enhanced the quality and clarity of our manuscript. NR 51 TC 8 Z9 8 U1 5 U2 22 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD MAR PY 2014 VL 6 IS 3 BP 1762 EP 1782 DI 10.3390/rs6031762 PG 21 WC Remote Sensing SC Remote Sensing GA AF6AO UT WOS:000334797000001 ER PT J AU Long, S Fatoyinbo, TE Policelli, F AF Long, Stephanie Fatoyinbo, Temilola E. Policelli, Frederick TI Flood extent mapping for Namibia using change detection and thresholding with SAR SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE flooding; SAR; remote sensing ID RADAR IMAGERY; RIVER; MODEL AB A new method for flood detection change detection and thresholding (CDAT) was used with synthetic aperture radar (SAR) imagery to delineate the extent of flooding for the Chobe floodplain in the Caprivi region of Namibia. This region experiences annual seasonal flooding and has seen a recent renewal of severe flooding after a long dry period in the 1990s. Flooding in this area has caused loss of life and livelihoods for the surrounding communities and has caught the attention of disaster relief agencies. There is a need for flood extent mapping techniques that can be used to process images quickly, providing near real-time flooding information to relief agencies. ENVISAT/ASAR and Radarsat-2 images were acquired for several flooding seasons from February 2008 to March 2013. The CDAT method was used to determine flooding from these images and includes the use of image subtraction, decision-based classification with threshold values, and segmentation of SAR images. The total extent of flooding determined for 2009, 2011 and 2012 was about 542 km(2), 720 km2, and 673 km2 respectively. Pixels determined to be flooded in vegetation were typically <0.5% of the entire scene, with the exception of 2009 where the detection of flooding in vegetation was much greater (almost one third of the total flooded area). The time to maximum flooding for the 2013 flood season was determined to be about 27 days. Landsat water classification was used to compare the results from the new CDAT with SAR method; the results show good spatial agreement with Landsat scenes. C1 [Long, Stephanie] Florida Int Univ, Dept Earth & Environm, Miami, FL 33199 USA. [Fatoyinbo, Temilola E.] NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD USA. [Policelli, Frederick] NASA, Off Appl Sci, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Long, S (reprint author), Florida Int Univ, Dept Earth & Environm, Miami, FL 33199 USA. EM stephanie.long@fiu.edu RI Fatoyinbo, Temilola/G-6104-2012 OI Fatoyinbo, Temilola/0000-0002-1130-6748 FU NASA [NNH09ZDA001N-TERRAQUA] FX This work is supported by the NASA Earth Science Research Program through the 'Science of Terra and Aqua' solicitation, NNH09ZDA001N-TERRAQUA. The authors wish to thank the Canadian Space Agency and the European Space Agency for providing RADARSAT and ASAR radar data. The authors also thank Stuart Frye (SGT, Inc.) for his tireless work coordinating data acquisitions and data access for this work. NR 29 TC 13 Z9 13 U1 10 U2 47 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 MAR PY 2014 VL 9 IS 3 AR 035002 DI 10.1088/1748-9326/9/3/035002 PG 9 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AE5ZO UT WOS:000334068000023 ER PT J AU Haberle, RM Gomez-Elvira, J Juarez, MD Harri, AM Hollingsworth, JL Kahanpaa, H Kahre, MA Lemmon, M Martin-Torres, FJ Mischna, M Moores, JE Newman, C Rafkin, SCR Renno, N Richardson, MI Rodriguez-Manfredi, JA Vasavada, AR Zorzano-Mier, MP AF Haberle, R. M. Gomez-Elvira, J. Juarez, M. de la Torre Harri, A-M Hollingsworth, J. L. Kahanpaa, H. Kahre, M. A. Lemmon, M. Martin-Torres, F. J. Mischna, M. Moores, J. E. Newman, C. Rafkin, S. C. R. Renno, N. Richardson, M. I. Rodriguez-Manfredi, J. A. Vasavada, A. R. Zorzano-Mier, M-P CA REMS Team MSL Sci Team TI Preliminary interpretation of the REMS pressure data from the first 100 sols of the MSL mission SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE MSL; REMS; pressure ID GREAT DUST STORMS; NUMERICAL-SIMULATION; MARTIAN ATMOSPHERE; THERMAL TIDES; MARS; DEVILS; MODEL; CIRCULATION; CYCLE AB We provide a preliminary interpretation of the Rover Environmental Monitoring Station (REMS) pressure data from the first 100 Martian solar days (sols) of the Mars Science Laboratory mission. The pressure sensor is performing well and has revealed the existence of phenomena undetected by previous missions that include possible gravity waves excited by evening downslope flows, relatively dust-free convective vortices analogous in structure to dust devils, and signatures indicative of the circulation induced by Gale Crater and its central mound. Other more familiar phenomena are also present including the thermal tides, generated by daily insolation variations, and the CO2 cycle, driven by the condensation and sublimation of CO2 in the polar regions. The amplitude of the thermal tides is several times larger than those seen by other landers primarily because Curiosity is located where eastward and westward tidal modes constructively interfere and also because the crater circulation amplifies the tides to some extent. During the first 100 sols tidal amplitudes generally decline, which we attribute to the waning influence of the Kelvin wave. Toward the end of the 100 sol period, tidal amplitudes abruptly increased in response to a nearby regional dust storm that did not expand to global scales. Tidal phases changed abruptly during the onset of this storm suggesting a change in the interaction between eastward and westward modes. When compared to Viking Lander 2 data, the REMS daily average pressures show no evidence yet for the 1-20Pa increase expected from the possible loss of CO2 from the south polar residual cap. Key Points REMS pressure sensor is operating nominally New phenomena have been discovered Familiar phenomena have been detected C1 [Haberle, R. M.; Hollingsworth, J. L.; Kahre, M. A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gomez-Elvira, J.; Martin-Torres, F. J.; Rodriguez-Manfredi, J. A.; Zorzano-Mier, M-P] Ctr Astrobiol INTA CSIC, Madrid, Spain. [Juarez, M. de la Torre; Mischna, M.; Vasavada, A. R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Harri, A-M; Kahanpaa, H.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. [Lemmon, M.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX USA. [Moores, J. E.] York Univ, Dept Earth & Space Sci & Engn, Toronto, ON M3J 2R7, Canada. [Newman, C.; Richardson, M. I.] Ashima Res, Pasadena, CA USA. [Rafkin, S. C. R.] SW Res Inst, Boulder, CO USA. [Renno, N.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP Haberle, RM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Robert.M.Haberle@nasa.gov RI Lemmon, Mark/E-9983-2010; Rodriguez-Manfredi, Jose/L-8001-2014; Ramos, Miguel/K-2230-2014; Gonzalez, Rafael/D-1748-2009; Zorzano, Maria-Paz/C-5784-2015; Martin-Torres, Francisco Javier/G-6329-2015; Harri, Ari-Matti/C-7142-2012; Zorzano, Maria-Paz/F-2184-2015 OI Kahanpaa, Henrik/0000-0001-9108-186X; Lemmon, Mark/0000-0002-4504-5136; Rodriguez-Manfredi, Jose/0000-0003-0461-9815; Ramos, Miguel/0000-0003-3648-6818; Zorzano, Maria-Paz/0000-0002-4492-9650; Martin-Torres, Francisco Javier/0000-0001-6479-2236; Harri, Ari-Matti/0000-0001-8541-2802; Zorzano, Maria-Paz/0000-0002-4492-9650 FU NASA's Mars Exploration Program and Planetary Science Division; Economy and Competitivity Ministry [AYA2011-25720] FX NASA's Mars Exploration Program and Planetary Science Division supported this work. J. G.-E., J. M.-T., J. A. R.-M., and M.-P. Z. are supported by Economy and Competitivity Ministry (AYA2011-25720). The reviews of A. Spiga and R. J. Wilson greatly improved the manuscript. R. M. H. acknowledges Dan Tyler and Jeff Barnes for their stimulating discussions about crater circulations. NR 34 TC 23 Z9 23 U1 4 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAR PY 2014 VL 119 IS 3 BP 440 EP 453 DI 10.1002/2013JE004488 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AF1AN UT WOS:000334446800004 ER PT J AU Ehresmann, B Zeitlin, C Hassler, DM Wimmer-Schweingruber, RF Bohm, E Bottcher, S Brinza, DE Burmeister, S Guo, JN Kohler, J Martin, C Posner, A Rafkin, S Reitz, G AF Ehresmann, Bent Zeitlin, Cary Hassler, Donald M. Wimmer-Schweingruber, Robert F. Boehm, Eckart Boettcher, Stephan Brinza, David E. Burmeister, Soenke Guo, Jingnan Koehler, Jan Martin, Cesar Posner, Arik Rafkin, Scot Reitz, Guenther TI Charged particle spectra obtained with the Mars Science Laboratory Radiation Assessment Detector (MSL/RAD) on the surface of Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; radiation; charged particles; galactic cosmic rays ID ENVIRONMENT; SIMULATION AB The Radiation Assessment Detector (RAD)situated inside the Mars Science Laboratory's Curiosity roveris the first ever instrument to measure the energetic particle radiation environment on the surface of Mars. To fully understand the influence of this surface radiation field in terms of potential hazard to life, a detailed knowledge of its composition is necessary. Charged particles are a major component of this environment, both galactic cosmic rays propagating to the Martian surface and secondary particles created by interactions of these cosmic rays with the atoms of the Martian atmosphere and soil. Here we present particle fluxes for a wide range of ion species, providing detailed energy spectra in the low-energy range (up to several hundred MeV/nucleon particle energy), and integral fluxes for higher energies. In addition to being crucial for the understanding of the hazards of this radiation to possible future manned missions to Mars, the data reported here provide valuable input for evaluating and validating particle transport models currently used to estimate the radiation environment on Mars and elsewhere in space. It is now possible for the first time to compare model results for expected surface particle fluxes with actual ground-based measurements. C1 [Ehresmann, Bent; Zeitlin, Cary; Hassler, Donald M.; Rafkin, Scot] SW Res Inst, Boulder, CO 80302 USA. [Wimmer-Schweingruber, Robert F.; Boehm, Eckart; Boettcher, Stephan; Burmeister, Soenke; Guo, Jingnan; Koehler, Jan; Martin, Cesar] Univ Kiel, Kiel, Germany. [Brinza, David E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Posner, Arik] NASA Headquarters, Sci Miss Directorate, Washington, DC USA. [Reitz, Guenther] Deutsch Zentrum Luft & Raumfahrt, Cologne, Germany. RP Ehresmann, B (reprint author), SW Res Inst, Boulder, CO 80302 USA. EM ehresmann@boulder.swri.edu OI Posner, Arik/0000-0003-1572-8734 FU NASA (HEOMD) under Jet Propulsion Laboratory (JPL) [1273039]; German Aerospace Center (DLR); DLR's Space Administration [50QM0501, 50QM1201]; NASA FX The authors would like to thank the reviewers for their efforts in evaluating this work and their helpful comments. RAD is supported by NASA (HEOMD) under Jet Propulsion Laboratory (JPL) subcontract 1273039 to Southwest Research Institute and in Germany by the German Aerospace Center (DLR) and DLR's Space Administration grants 50QM0501 and 50QM1201 to the Christian-Albrechts-Universitat zu Kiel. Part of this research was carried out at JPL, California Institute of Technology, under a contract with NASA. We thank Jeff Simmonds, John Grotzinger, Joy Crisp, Ashwin Vasvada, and Helen Mortensen at JPL, Gale Allen, Michael Meyer, Chris Moore, and Victoria Friedensen at NASA Headquarters, and Heiner Witte at DLR in Germany for their support of RAD. The data used in this paper are archived in the NASA Planetary Data System's Planetary Plasma Interactions Node at the University of California, Los Angeles. The archival volume includes the full binary raw data files, detailed descriptions of the structures therein, and higher-level data products in human-readable form. The PPI node is hosted at the following URL: http://ppi.pds.nasa.gov/. NR 27 TC 15 Z9 15 U1 2 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAR PY 2014 VL 119 IS 3 BP 468 EP 479 DI 10.1002/2013JE004547 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AF1AN UT WOS:000334446800006 ER PT J AU Guzewich, SD Wilson, RJ McConnochie, TH Toigo, AD Banfield, DJ Smith, MD AF Guzewich, Scott D. Wilson, R. John McConnochie, Timothy H. Toigo, Anthony D. Banfield, Donald J. Smith, Michael D. TI Thermal tides during the 2001 Martian global-scale dust storm SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; global dust storm; tides; waves ID RADIO OCCULTATION MEASUREMENTS; GENERAL-CIRCULATION MODEL; TES NADIR DATA; MGS TES; INTERANNUAL VARIABILITY; DATA ASSIMILATION; TRAVELING-WAVES; MARS; ATMOSPHERE; ACCELEROMETER AB The 2001 (Mars Year 25) global dust storm radically altered the dynamics of the Martian atmosphere. Using observations from the Thermal Emission Spectrometer onboard the Mars Global Surveyor spacecraft and MarsWRF general circulation model simulations, we examine the changes to thermal tides and planetary waves caused by the storm. We find that the extratropical diurnal migrating tide is dramatically enhanced during the storm, particularly in the southern hemisphere, reaching amplitudes of more than 20K. The tropical diurnal migrating tide is weakened to almost undetectable levels. The diurnal Kelvin waves are also significantly weakened, particularly during the period of global expansion at L-s=200 degrees-210 degrees. In contrast, the westward propagating diurnal wavenumber 2 tide strengthens to 4-8K at altitudes above 30km. The wavenumber 1 stationary wave reaches amplitudes of 10-12K at 50 degrees-70 degrees N, far larger than is typically seen during this time of year. The phase of this stationary wave and the enhancement of the diurnal wavenumber 2 tide appear to be responses to the high-altitude westward propagating equatorial wavenumber 1 structure in dust mixing ratio observed during the storm in previous works. This work provides a global picture of dust storm wave dynamics that reveals the coupling between the tropics and high-latitude wave responses. We conclude that the zonal distribution of thermotidal forcing from atmospheric aerosol concentration is as important to understanding the atmospheric wave response as the total global mean aerosol optical depth. Key Points The zonal distribution of dust forcing is key to understanding wave response The zonal wavenumber 1 pattern of dust forcing is the key mechanism High-latitude wave response is coupled to that of the tropics C1 [Guzewich, Scott D.; Smith, Michael D.] NASA, Goddard Spaceflight Ctr, Greenbelt, MD 20771 USA. [Wilson, R. John] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. [McConnochie, Timothy H.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Toigo, Anthony D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Banfield, Donald J.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. RP Guzewich, SD (reprint author), NASA, Goddard Spaceflight Ctr, Greenbelt, MD 20771 USA. EM scott.d.guzewich@nasa.gov OI Banfield, Don/0000-0003-2664-0164; Guzewich, Scott/0000-0003-1149-7385 FU NASA Postdoctoral Program fellowship FX Guzewich was supported by a NASA Postdoctoral Program fellowship. NR 48 TC 7 Z9 7 U1 3 U2 25 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAR PY 2014 VL 119 IS 3 BP 506 EP 519 DI 10.1002/2013JE004502 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AF1AN UT WOS:000334446800008 ER PT J AU Teodoro, LFA Eke, VR Elphic, RC Feldman, WC Lawrence, DJ AF Teodoro, L. F. A. Eke, V. R. Elphic, R. C. Feldman, W. C. Lawrence, D. J. TI How well do we know the polar hydrogen distribution on the Moon? SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE polar; distribution; hydrogen; lunar ID LUNAR RECONNAISSANCE ORBITER; IMAGE-RECONSTRUCTION; EXPERIMENT LEND; FAST-NEUTRONS; WATER ICE; PROSPECTOR; DEPOSITS; VOLATILES; MERCURY; FLUXES AB A detailed comparison is made of results from the Lunar Prospector Neutron Spectrometer (LPNS) and the Lunar Exploration Neutron Detector Collimated Sensors for Epithermal Neutrons (LEND CSETN). Using the autocorrelation function and power spectrum of the polar count rate maps produced by these experiments, it is shown that the LEND CSETN has a footprint that is at least as big as would be expected for an omnidirectional detector at an orbital altitude of 50 km. The collimated flux into the field of view of the collimator is negligible. A dip in the count rate in Shoemaker crater is found to be consistent with being a statistical fluctuation superimposed on a significant, larger-scale decrease in the count rate, providing no evidence for high spatial resolution of the LEND CSETN. The maps of lunar polar hydrogen with the highest contrast, i.e., spatial resolution, are those resulting from pixon image reconstructions of the LPNS data. These typically provide weight percentages of water-equivalent hydrogen that are accurate to 30% within the polar craters. Key Points How well do we know the polar hydrogen distribution C1 [Teodoro, L. F. A.] NASA, BAER, Ames Res Ctr, Mountain View, CA 94035 USA. [Eke, V. R.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham, England. [Elphic, R. C.] NASA, Planetary Syst Branch, Space Sci & Astrobiol Div, Ames Res Ctr, Mountain View, CA USA. [Feldman, W. C.] Planetary Sci Inst, Tucson, AZ USA. [Lawrence, D. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Teodoro, LFA (reprint author), NASA, BAER, Ames Res Ctr, Mountain View, CA 94035 USA. EM luis.f.teodoro@nasa.gov RI Lawrence, David/E-7463-2015 OI Lawrence, David/0000-0002-7696-6667 FU NASA Planetary Geology and Geophysics Program [07-PGG07-0007]; NASA Planetary Missions Data Analysis Program [07-DDAP07-0005]; STFC rolling grant [ST/F002289/1] FX L.T. and R. E. acknowledge the support of the NASA Planetary Geology and Geophysics Program Project #07-PGG07-0007 and NASA Planetary Missions Data Analysis Program Project #07-DDAP07-0005 for funding this research. V. R. E. was supported by the STFC rolling grant ST/F002289/1. L. T. acknowledges helpful discussions with J. Karcz. NR 46 TC 9 Z9 9 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAR PY 2014 VL 119 IS 3 BP 574 EP 593 DI 10.1002/2013JE004421 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AF1AN UT WOS:000334446800012 ER PT J AU Kohler, J Zeitlin, C Ehresmann, B Wimmer-Schweingruber, RF Hassler, DM Reitz, G Brinza, DE Weigle, G Appel, J Bottcher, S Bohm, E Burmeister, S Guo, J Martin, C Posner, A Rafkin, S Kortmann, O AF Koehler, J. Zeitlin, C. Ehresmann, B. Wimmer-Schweingruber, R. F. Hassler, D. M. Reitz, G. Brinza, D. E. Weigle, G. Appel, J. Boettcher, S. Boehm, E. Burmeister, S. Guo, J. Martin, C. Posner, A. Rafkin, S. Kortmann, O. TI Measurements of the neutron spectrum on the Martian surface with MSL/RAD SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; neutron; gamma; dose rate ID MARS; ENVIRONMENTS; EXPLORATION; SPACE AB The Radiation Assessment Detector (RAD), onboard the Mars Science Laboratory (MSL) rover Curiosity, measures the energetic charged and neutral particles and the radiation dose rate on the surface of Mars. An important factor for determining the biological impact of the Martian surface radiation is the specific contribution of neutrons, with their deeper penetration depth and ensuing high biological effectiveness. This is very difficult to measure quantitatively, resulting in considerable uncertainties in the total radiation dose. In contrast to charged particles, neutral particles (neutrons and gamma rays) are generally only measured indirectly. Measured spectra are a complex convolution of the incident particle spectrum with the detector response function and must be unfolded. We apply an inversion method (based on a maximum likelihood estimation) to calculate the neutron and gamma spectra from the RAD neutral particle measurements. Here we show the first spectra on the surface of Mars and compare them to theoretical predictions. The measured neutron spectrum (ranging from 8 to 740 MeV) translates into a radiation dose rate of 144Gy/d and a dose equivalent rate of 6115Sv/d. This corresponds to 7% of the measured total surface dose rate and 10% of the biologically relevant surface dose equivalent rate on Mars. Measuring the Martian neutron and gamma spectra is an essential step for determining the mutagenic influences to past or present life at or beneath the Martian surface as well as the radiation hazard for future human exploration, including the shielding design of a potential habitat. C1 [Koehler, J.; Wimmer-Schweingruber, R. F.; Appel, J.; Boettcher, S.; Boehm, E.; Burmeister, S.; Guo, J.; Martin, C.] Univ Kiel, Inst Expt & Appl Phys, Kiel, Germany. [Zeitlin, C.] SW Res Inst, Earth Oceans & Space Dept, Durham, NH USA. [Ehresmann, B.; Hassler, D. M.; Rafkin, S.] SW Res Inst, Space Sci & Engn Div, Boulder, CO USA. [Reitz, G.] Deutsch Zentrum Luft & Raumfahrt, Cologne, Germany. [Brinza, D. E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Weigle, G.] Big Head Endian LLC, Burden, KS USA. [Posner, A.] NASA Headquarters, Sci Miss Directorate, Washington, DE USA. [Kortmann, O.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Kohler, J (reprint author), Univ Kiel, Inst Expt & Appl Phys, Kiel, Germany. EM koehler@physik.uni-kiel.de OI Posner, Arik/0000-0003-1572-8734 FU NASA (HEOMD) under JPL [1273039]; DLR and DLR's Space Administration [50QM0501, 50 QM1201]; National Aeronautics and Space Administration FX RAD is supported by NASA (HEOMD) under JPL subcontract 1273039 to Southwest Research Institute and in Germany by DLR and DLR's Space Administration grants 50QM0501 and 50 QM1201 to the Christian Albrechts University, Kiel. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contact with the National Aeronautics and Space Administration. The data used in this paper are archived in the NASA Planetary Data System's Planetary Plasma Interactions Node at the University of California, Los Angeles. The archival volume includes the full binary raw data files, detailed descriptions of the structures therein, and higher-level data products in human-readable form. The PPI node is hosted at the following URL: http://ppi.pds.nasa.gov/. NR 22 TC 12 Z9 12 U1 1 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAR PY 2014 VL 119 IS 3 BP 594 EP 603 DI 10.1002/2013JE004539 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AF1AN UT WOS:000334446800013 ER PT J AU Goddard, K Warner, NH Gupta, S Kim, JR AF Goddard, Kate Warner, Nicholas H. Gupta, Sanjeev Kim, Jung-Rack TI Mechanisms and timescales of fluvial activity at Mojave and other young Martian craters SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE alluvial fans; Mojave Crater; Mars; Amazonian; precipitation ID GROUND ICE; IMPACT CRATERS; CLIMATE-CHANGE; ARES-VALLIS; MARS; SURFACE; WATER; HISTORY; REGION; MIDLATITUDES AB Mojave Crater, and five other relatively young Late Hesperian to Amazonian-age Martian craters exhibit channelized alluvial fans that are sourced from bedrock-eroded catchments. These catchments emerge from the crests of sloping surfaces, suggesting a formation mechanism that involved precipitation. The evidence for fluvial activity at all six craters is restricted to their interiors and the immediate surrounding regions. Detailed mapping at Mojave reveals the highest density of channels, catchments and fans interior to the crater. Similar landforms are identified outside of the crater, but not beyond similar to 200km from the rim. Irregular pits on the floor of Mojave, interpreted as degassing structures from hot impact melt, directly superpose several fan surfaces, and partly destroy the fan toes. This suggests that sediment was mobilized immediately after crater formation, while the crater was still hot. Based on the patterns and timing of channel-fan development at all six craters we favor several hypotheses for the precipitation mechanism: (1) snowfall and melt on young, hot impact craters, (2) impact plume precipitation, and (3) degassing of volatiles from impact melt terrain. Scenario (1) suggests a different global or regional climate relative to modern conditions, requiring equatorial and midlatitude snowfall accumulation. Scenarios (2) and (3) do not necessarily require unique climate conditions, as water may have been mobilized from the target or the impactor. Key Points Mojave Crater has alluvial fans suggesting recent precipitation on Mars Precipitation was localized around Mojave Crater suggesting a local mechanism Alluvial fans formed immediately after Mojave Crater formed C1 [Goddard, Kate; Gupta, Sanjeev] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London, England. [Warner, Nicholas H.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Kim, Jung-Rack] Univ Seoul, Dept Geoinformat, Seoul, South Korea. RP Warner, NH (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Nicholas.H.Warner@jpl.nasa.gov FU STFC doctoral studentship; UK Science and Technology Facilities Council (STFC) [ST/F003099/1]; NASA Postdoctoral Program at the Jet Propulsion Laboratory-California Institute of Technology; NASA FX We thank the CTX (Context Camera) and HiRISE (High Resolution Imaging Science Experiment) teams as well as the HRSC (High-Resolution Stereo Camera) team at Freie Universitat Berlin, the German Aerospace Centre (DLR), and the European Space Agency (ESA). Goddard was funded by an STFC doctoral studentship. Warner and Gupta were supported by the UK Science and Technology Facilities Council (STFC) under grant ST/F003099/1. Warner was partially supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory-California Institute of Technology, administered by Oak Ridge Associated Universities through a contract with NASA. We thank Edwin Kite and an anonymous reviewer for their helpful comments. NR 89 TC 2 Z9 2 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAR PY 2014 VL 119 IS 3 BP 604 EP 634 DI 10.1002/2013JE004564 PG 31 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AF1AN UT WOS:000334446800014 ER PT J AU Goudge, TA Head, JW Kerber, L Blewett, DT Denevi, BW Domingue, DL Gillis-Davis, JJ Gwinner, K Helbert, J Holsclaw, GM Izenberg, NR Klima, RL McClintock, WE Murchie, SL Neumann, GA Smith, DE Strom, RG Xiao, ZY Zuber, MT Solomon, SC AF Goudge, Timothy A. Head, James W. Kerber, Laura Blewett, David T. Denevi, Brett W. Domingue, Deborah L. Gillis-Davis, Jeffrey J. Gwinner, Klaus Helbert, Joern Holsclaw, Gregory M. Izenberg, Noam R. Klima, Rachel L. McClintock, William E. Murchie, Scott L. Neumann, Gregory A. Smith, David E. Strom, Robert G. Xiao, Zhiyong Zuber, Maria T. Solomon, Sean C. TI Global inventory and characterization of pyroclastic deposits on Mercury: New insights into pyroclastic activity from MESSENGER orbital data SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE pyroclastic deposits; volcanism; Mercury ID LUNAR RECONNAISSANCE ORBITER; DUAL IMAGING-SYSTEM; SPECTRAL REFLECTANCE; SPECTROPHOTOMETRIC PROPERTIES; ERUPTION CONDITIONS; VOLCANISM; SURFACE; FLYBY; MISSION; EVOLUTION AB We present new observations of pyroclastic deposits on the surface of Mercury from data acquired during the orbital phase of the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) mission. The global analysis of pyroclastic deposits brings the total number of such identified features from 40 to 51. Some 90% of pyroclastic deposits are found within impact craters. The locations of most pyroclastic deposits appear to be unrelated to regional smooth plains deposits, except some deposits cluster around the margins of smooth plains, similar to the relation between many lunar pyroclastic deposits and lunar maria. A survey of the degradation state of the impact craters that host pyroclastic deposits suggests that pyroclastic activity occurred on Mercury over a prolonged interval. Measurements of surface reflectance by MESSENGER indicate that the pyroclastic deposits are spectrally distinct from their surrounding terrain, with higher reflectance values, redder (i.e., steeper) spectral slopes, and a downturn at wavelengths shorter than similar to 400nm (i.e., in the near-ultraviolet region of the spectrum). Three possible causes for these distinctive characteristics include differences in transition metal content, physical properties (e.g., grain size), or degree of space weathering from average surface material on Mercury. The strength of the near-ultraviolet downturn varies among spectra of pyroclastic deposits and is correlated with reflectance at visible wavelengths. We suggest that this interdeposit variability in reflectance spectra is the result of either variable amounts of mixing of the pyroclastic deposits with underlying material or inherent differences in chemical and physical properties among pyroclastic deposits. Key Points We expand the catalog of pyroclastic deposits on Mercury from 40 to 51 Stratigraphic relationships suggest emplacement over a prolonged interval Deposits exhibit distinct spectral signatures with interdeposit variability C1 [Goudge, Timothy A.; Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Kerber, Laura] Univ Paris 06, Lab Meteorol Dynam, Ctr Natl Rech Sci, Inst Pierre Simon Laplace, Paris, France. [Blewett, David T.; Denevi, Brett W.; Izenberg, Noam R.; Klima, Rachel L.; Murchie, Scott L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Domingue, Deborah L.] Planetary Sci Inst, Tucson, AZ USA. [Gillis-Davis, Jeffrey J.] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Gwinner, Klaus; Helbert, Joern] Deutsch Zentrum Luft & Raumfahrt, Inst Planetary Res, Berlin, Germany. [Holsclaw, Gregory M.; McClintock, William E.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Neumann, Gregory A.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD USA. [Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. [Strom, Robert G.; Xiao, Zhiyong] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Xiao, Zhiyong] China Univ Geosci, Planetary Sci Inst, Wuhan 430074, Peoples R China. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. RP Goudge, TA (reprint author), Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. EM Tim_Goudge@brown.edu RI Neumann, Gregory/I-5591-2013; Blewett, David/I-4904-2012; Klima, Rachel/H-9383-2012; Murchie, Scott/E-8030-2015; Izenberg, Noam/F-3952-2015; Denevi, Brett/I-6502-2012; OI Neumann, Gregory/0000-0003-0644-9944; Blewett, David/0000-0002-9241-6358; Klima, Rachel/0000-0002-9151-6429; Murchie, Scott/0000-0002-1616-8751; Izenberg, Noam/0000-0003-1629-6478; Denevi, Brett/0000-0001-7837-6663; Helbert, Jorn/0000-0001-5346-9505 FU NASA Discovery Program [NAS5-97271, NASW-00002] FX We gratefully acknowledge the contributions of the engineers and managers of the MESSENGER mission that have made this work possible. The MESSENGER mission is supported by the NASA Discovery Program under contract NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of Washington. Sebastien Besse, Paul Byrne, Olaf Gustafson, and Catherine Weitz provided thorough and constructive reviews that improved this paper. We thank C. I. Fassett for assistance with topographic data, and J.L. Dickson and D. M. H. Baker for the help in processing image data. Thanks are also extended to D. M. H. Baker, M. Beach, D. M. Hurwitz, L. M. Jozwiak, K. E. Scanlon, W. M. Vaughan, and J. L. Whitten for assistance with the initial search for potential pyroclastic source vents and helpful discussions. NR 89 TC 16 Z9 16 U1 0 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAR PY 2014 VL 119 IS 3 BP 635 EP 658 DI 10.1002/2013JE004480 PG 24 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AF1AN UT WOS:000334446800015 ER PT J AU Mulder, E Frings-Meuthen, P von der Wiesche, M Clement, G Linnarsson, D Paloski, WH Wuyts, FL Zange, J Rittweger, J AF Mulder, E. Frings-Meuthen, P. von der Wiesche, M. Clement, G. Linnarsson, D. Paloski, W. H. Wuyts, F. L. Zange, J. Rittweger, J. TI Study protocol, implementation, and verification of a short versatile upright exercise regime during 5 days of bed rest SO JOURNAL OF MUSCULOSKELETAL & NEURONAL INTERACTIONS LA English DT Article DE Smith Machine; bed rest; standardization; squat; heel raise ID BODY NEGATIVE-PRESSURE; HEAD-DOWN TILT; CO-REBREATHING METHOD; SIMULATED MICROGRAVITY; ARTIFICIAL GRAVITY; COUNTERMEASURE; RESPONSES; BONE; SPACEFLIGHT; BEDREST AB Objectives: This work provides a reference for future papers originating from this study by providing basic results on body mass, urine volume, and hemodynamic changes to 5 days of bed rest (BR) and by describing acute cardio-respiratory/mechano-graphic responses to a short versatile upright exercise battery. Methods: Ten male subjects (mean +/- SEM age: 29.4 +/- 1.5 years; height: 178.8 +/- 1.5 cm; body mass: 77.7 +/- 1.5 kg) performed, in random order, 5 days of 6 head-down tilt (HDT) BR with no exercise (CON), or BR with daily 25 minutes of quiet upright standing (STA) or upright locomotion replacement training (LRT). Results: Plasma volume, exercise capacity and orthostatic tolerance decreased similarly between interventions following 5 days of BR. Upright heart rate during LRT and STA increased throughout BR; from 137 +/- 4 bpm to 146 +/- 4 bpm for LRT (P<0.01); and from 90 +/- 3 bpm to 102 +/- 6 bpm (P<0.001) for STA. Conclusion: the overall similarity in the response to BR, and increase in upright heart rate during the LRT sessions suggest early and advancing cardiovascular deconditioning during 5 days of BR bed rest, which was not prevented by the versatile exercise regime. C1 [Mulder, E.; Frings-Meuthen, P.; von der Wiesche, M.; Zange, J.; Rittweger, J.] DLR Inst Aerosp Med, D-51147 Cologne, Germany. [Clement, G.] Int Space Univ, Strasbourg, France. [Linnarsson, D.] Karolinska Inst, Dept Physiol & Pharmacol, Stockholm, Sweden. [Paloski, W. H.] NASA, Houston, TX USA. [Wuyts, F. L.] Univ Antwerp, Antwerp, Belgium. RP Mulder, E (reprint author), DLR Inst Aerosp Med, Dept Space Physiol, D-51147 Cologne, Germany. EM Edwin.Mulder@dlr.de RI Rittweger, Jorn/A-4308-2009 FU European Space Agency [22126/08/NL/VJ] FX We thank all test subjects for their participation in the study and the staff of the DLR operational study team for supervising. The study was funded by the European Space Agency (contract number 22126/08/NL/VJ). NR 36 TC 6 Z9 6 U1 1 U2 6 PU JMNI PI NAFPLION PA 7 SPILIADOU SQ, NAFPLION, 21 100, GREECE SN 1108-7161 J9 J MUSCULOSKEL NEURON JI J. Musculoskelet. Neuronal Interact. PD MAR PY 2014 VL 14 IS 1 BP 111 EP 123 PG 13 WC Neurosciences; Physiology SC Neurosciences & Neurology; Physiology GA AF2YV UT WOS:000334579300012 PM 24583546 ER PT J AU Lopez, RA Munoz, V Vinas, AF Valdivia, JA AF Lopez, Rodrigo A. Munoz, Victor Vinas, Adolfo F. Alejandro Valdivia, J. TI Particle-in-cell simulation for parametric decays of a circularly polarized Alfven wave in relativistic thermal electron-positron plasma SO PHYSICS OF PLASMAS LA English DT Article ID MAGNETIC RECONNECTION; PAIR PLASMA; ELECTROMAGNETIC-WAVES; CURRENT SHEETS; SOLAR-WIND; INSTABILITY; MAGNETOSPHERES; ACCELERATION; OUTFLOW AB Parametric decays of a left-handed circularly polarized Alfven wave propagating along a constant background magnetic field in a relativistic thermal electron-positron plasma are studied by means of a one dimensional relativistic particle-in-cell simulation. Relativistic effects are included in the Lorentz equation for the momentum of the particles and in their thermal motion, by considering a Maxwell-Juttner velocity distribution function for the initial condition. In the linear stage of the simulation, we find many instabilities that match the predictions of relativistic fluid theory. In general, the growth rates of the instabilities increase as the pump wave amplitude is increased, and decrease with a raise in the plasma temperatures. We have confirmed that for very high temperatures the Alfven branch is suppressed, consistent with analytical calculations. (C) 2014 AIP Publishing LLC. C1 [Lopez, Rodrigo A.; Munoz, Victor; Alejandro Valdivia, J.] Univ Chile, Fac Ciencias, Dept Fis, Santiago, Chile. [Vinas, Adolfo F.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Alejandro Valdivia, J.] CEDENNA, Ctr Desarrollo Nanociencia & Nanotecnol, Santiago, Chile. RP Lopez, RA (reprint author), Univ Chile, Fac Ciencias, Dept Fis, Casilla 653, Santiago, Chile. EM rlopez186@gmail.com RI Lopez, Rodrigo/H-7576-2013; Valdivia, Juan/A-3631-2008; Munoz, Victor/A-2255-2008 OI Valdivia, Juan/0000-0003-3381-9904; FU Conicyt through Fondecyt [1110135, 1110729, 1080658, 1121144]; Conicyt [21100839]; Becas Chile fellowship [75120086]; Cedenna FX We thank the support of Conicyt through Fondecyt Grant Nos. 1110135 (J.A.V.), 1110729 (J.A.V.), 1080658, and 1121144 (V. M.). R. A. L. thanks the award of a Doctoral Fellowship from Conicyt, Contract No. 21100839, and for a Becas Chile fellowship, Contract No. 75120086, for a doctoral internship at NASA/GSFC. We also thank the support of Cedenna. NR 46 TC 4 Z9 4 U1 1 U2 12 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD MAR PY 2014 VL 21 IS 3 AR 032102 DI 10.1063/1.4867255 PG 10 WC Physics, Fluids & Plasmas SC Physics GA AE7LU UT WOS:000334180200024 ER PT J AU Abbasi, R Abdou, Y Abu-Zayyad, T Ackermann, M Adams, J Aguilar, JA Ahlers, M Allen, MM Altmann, D Andeen, K Auffenberg, J Bai, X Baker, M Barwick, SW Baum, V Bay, R Alba, JLB Beattie, K Beatty, JJ Bechet, S Becker, JK Becker, KH Benabderrahmane, ML BenZvi, S Berdermann, J Berghaus, P Berley, D Bernardini, E Bertrand, D Besson, DZ Bindig, D Bissok, M Blaufuss, E Blumenthal, J Boersma, DJ Bohm, C Bose, D Boser, S Botner, O Brown, AM Buitink, S Caballero-Mora, KS Carson, M Chirkin, D Christy, B Clevermann, F Cohen, S Colnard, C Cowen, DF Silva, AHC D'Agostino, MV Danninger, M Daughhetee, J Davis, JC De Clercq, C Degner, T Demirors, L Descamps, F Desiati, P de Vries-Uiterweerd, G DeYoung, T Diaz-Velez, JC Dierckxsens, M Dreyer, J Dumm, JP Dunkman, M Eisch, J Ellsworth, RW Engdegard, O Euler, S Evenson, PA Fadiran, O Fazely, AR Fedynitch, A Feintzeig, J Feusels, T Filimonov, K Finley, C Fischer-Wasels, T Fox, BD Franckowiak, A Franke, R Gaisser, TK Gallagher, J Gerhardt, L Gladstone, L Glusenkamp, T Goldschmidt, A Goodman, JA Gora, D Grant, D Griesel, T Gross, A Grullon, S Gurtner, M Ha, C Ismail, AH Hallgren, A Halzen, F Han, K Hanson, K Heinen, D Helbing, K Hellauer, R Hickford, S Hill, GC Hoffman, KD Hofmann, B Homeier, A Hoshina, K Huelsnitz, W Hulss, JP Hulth, PO Hultqvist, K Hussain, S Ishihara, A Jakobi, E Jacobsen, J Japaridze, GS Johansson, H Kampert, KH Kappes, A Karg, T Karle, A Kenny, P Kiryluk, J Kislat, F Klein, SR Kohne, H Kohnen, G Kolanoski, H Kopke, L Kopper, S Koskinen, DJ Kowalski, M Kowarik, T Krasberg, M Kroll, G Kurahashi, N Kuwabara, T Labare, M Laihem, K Landsman, H Larson, MJ Lauer, R Lunemann, J Madsen, J Marotta, A Maruyama, R Mase, K Matis, HS Meagher, K Merck, M Meszaros, P Meures, T Miarecki, S Middell, E Milke, N Miller, J Montaruli, T Morse, R Movit, SM Nahnhauer, R Nam, JW Naumann, U Nygren, DR Odrowski, S Olivas, A Olivo, M O'Murchadha, A Panknin, S Paul, L de los Heros, CP Petrovic, J Piegsa, A Pieloth, D Porrata, R Posselt, J Price, PB Przybylski, GT Rawlins, K Redl, P Resconi, E Rhode, W Ribordy, M Richard, AS Richman, M Rodrigues, JP Rothmaier, F Rott, C Ruhe, T Rutledge, D Ruzybayev, B Ryckbosch, D Sander, HG Santander, M Sarkar, S Schatto, K Schmidt, T Schonwald, A Schukraft, A Schulte, L Schultes, A Schulz, O Schunck, M Seckel, D Semburg, B Seo, SH Sestayo, Y Seunarine, S Silvestri, A Singh, K Slipak, A Spiczak, GM Spiering, C Stamatikos, M Stanev, T Stezelberger, T Stokstad, RG Stossl, A Strahler, EA Strom, R Stuer, M Sullivan, GW Swillens, Q Taavola, H Taboada, I Tamburro, A Tepe, A Ter-Antonyan, S Tilav, S Toale, PA Toscano, S Tosi, D van Eijndhoven, N Vandenbroucke, J Van Overloop, A van Santen, J Vehring, M Voge, M Walck, C Waldenmaier, T Wallraff, M Walter, M Weaver, C Wendt, C Westerhoff, S Whitehorn, N Wiebe, K Wiebusch, CH Williams, DR Wischnewski, R Wissing, H Wolf, M Wood, TR Woschnagg, K Xu, C Xu, DL Xu, XW Yanez, JP Yodh, G Yoshida, S Zarzhitsky, P Zoll, M AF Abbasi, R. Abdou, Y. Abu-Zayyad, T. Ackermann, M. Adams, J. Aguilar, J. A. Ahlers, M. Allen, M. M. Altmann, D. Andeen, K. Auffenberg, J. Bai, X. Baker, M. Barwick, S. W. Baum, V. Bay, R. Alba, J. L. Bazo Beattie, K. Beatty, J. J. Bechet, S. Becker, J. K. Becker, K. -H. Benabderrahmane, M. L. BenZvi, S. Berdermann, J. Berghaus, P. Berley, D. Bernardini, E. Bertrand, D. Besson, D. Z. Bindig, D. Bissok, M. Blaufuss, E. Blumenthal, J. Boersma, D. J. Bohm, C. Bose, D. Boeser, S. Botner, O. Brown, A. M. Buitink, S. Caballero-Mora, K. S. Carson, M. Chirkin, D. Christy, B. Clevermann, F. Cohen, S. Colnard, C. Cowen, D. F. Silva, A. H. Cruz D'Agostino, M. V. Danninger, M. Daughhetee, J. Davis, J. C. De Clercq, C. Degner, T. Demiroers, L. Descamps, F. Desiati, P. de Vries-Uiterweerd, G. DeYoung, T. Diaz-Velez, J. C. Dierckxsens, M. Dreyer, J. Dumm, J. P. Dunkman, M. Eisch, J. Ellsworth, R. W. Engdegard, O. Euler, S. Evenson, P. A. Fadiran, O. Fazely, A. R. Fedynitch, A. Feintzeig, J. Feusels, T. Filimonov, K. Finley, C. Fischer-Wasels, T. Fox, B. D. Franckowiak, A. Franke, R. Gaisser, T. K. Gallagher, J. Gerhardt, L. Gladstone, L. Gluesenkamp, T. Goldschmidt, A. Goodman, J. A. Gora, D. Grant, D. Griesel, T. Gross, A. Grullon, S. Gurtner, M. Ha, C. Ismail, A. Haj Hallgren, A. Halzen, F. Han, K. Hanson, K. Heinen, D. Helbing, K. Hellauer, R. Hickford, S. Hill, G. C. Hoffman, K. D. Hofmann, B. Homeier, A. Hoshina, K. Huelsnitz, W. Huelss, J. -P. Hulth, P. O. Hultqvist, K. Hussain, S. Ishihara, A. Jakobi, E. Jacobsen, J. Japaridze, G. S. Johansson, H. Kampert, K. -H. Kappes, A. Karg, T. Karle, A. Kenny, P. Kiryluk, J. Kislat, F. Klein, S. R. Koehne, H. Kohnen, G. Kolanoski, H. Koepke, L. Kopper, S. Koskinen, D. J. Kowalski, M. Kowarik, T. Krasberg, M. Kroll, G. Kurahashi, N. Kuwabara, T. Labare, M. Laihem, K. Landsman, H. Larson, M. J. Lauer, R. Luenemann, J. Madsen, J. Marotta, A. Maruyama, R. Mase, K. Matis, H. S. Meagher, K. Merck, M. Meszaros, P. Meures, T. Miarecki, S. Middell, E. Milke, N. Miller, J. Montaruli, T. Morse, R. Movit, S. M. Nahnhauer, R. Nam, J. W. Naumann, U. Nygren, D. R. Odrowski, S. Olivas, A. Olivo, M. O'Murchadha, A. Panknin, S. Paul, L. de los Heros, C. Perez Petrovic, J. Piegsa, A. Pieloth, D. Porrata, R. Posselt, J. Price, P. B. Przybylski, G. T. Rawlins, K. Redl, P. Resconi, E. Rhode, W. Ribordy, M. Richard, A. S. Richman, M. Rodrigues, J. P. Rothmaier, F. Rott, C. Ruhe, T. Rutledge, D. Ruzybayev, B. Ryckbosch, D. Sander, H. -G. Santander, M. Sarkar, S. Schatto, K. Schmidt, T. Schoenwald, A. Schukraft, A. Schulte, L. Schultes, A. Schulz, O. Schunck, M. Seckel, D. Semburg, B. Seo, S. H. Sestayo, Y. Seunarine, S. Silvestri, A. Singh, K. Slipak, A. Spiczak, G. M. Spiering, C. Stamatikos, M. Stanev, T. Stezelberger, T. Stokstad, R. G. Stoessl, A. Strahler, E. A. Stroem, R. Stueer, M. Sullivan, G. W. Swillens, Q. Taavola, H. Taboada, I. Tamburro, A. Tepe, A. Ter-Antonyan, S. Tilav, S. Toale, P. A. Toscano, S. Tosi, D. van Eijndhoven, N. Vandenbroucke, J. Van Overloop, A. van Santen, J. Vehring, M. Voge, M. Walck, C. Waldenmaier, T. Wallraff, M. Walter, M. Weaver, Ch Wendt, C. Westerhoff, S. Whitehorn, N. Wiebe, K. Wiebusch, C. H. Williams, D. R. Wischnewski, R. Wissing, H. Wolf, M. Wood, T. R. Woschnagg, K. Xu, C. Xu, D. L. Xu, X. W. Yanez, J. P. Yodh, G. Yoshida, S. Zarzhitsky, P. Zoll, M. CA IceCube Collaboration TI IceCube sensitivity for low-energy neutrinos from nearby supernovae (vol 535, pg A109, 2011) SO ASTRONOMY & ASTROPHYSICS LA English DT Correction DE neutrinos; supernovae: general; instrumentation: detectors; errata, addenda C1 [Abbasi, R.; Aguilar, J. A.; Andeen, K.; Baker, M.; BenZvi, S.; Berghaus, P.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Feintzeig, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hanson, K.; Hill, G. C.; Hoshina, K.; Jacobsen, J.; Karle, A.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; Merck, M.; Montaruli, T.; Morse, R.; O'Murchadha, A.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Abdou, Y.; Carson, M.; Descamps, F.; de Vries-Uiterweerd, G.; Feusels, T.; Ismail, A. Haj; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Subat & Radiat Phys, B-9000 Ghent, Belgium. [Abu-Zayyad, T.; Madsen, J.; Spiczak, G. M.; Tamburro, A.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA. [Adams, J.; Brown, A. M.; Gross, A.; Han, K.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [Ahlers, M.; Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England. [Auffenberg, J.; Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Gurtner, M.; Helbing, K.; Kampert, K. -H.; Karg, T.; Kopper, S.; Naumann, U.; Posselt, J.; Schultes, A.; Semburg, B.] Berg Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany. [Bai, X.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bai, X.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Barwick, S. W.; Nam, J. W.; Silvestri, A.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Bay, R.; D'Agostino, M. V.; Filimonov, K.; Gerhardt, L.; Kiryluk, J.; Klein, S. R.; Miarecki, S.; Porrata, R.; Price, P. B.; Vandenbroucke, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Ackermann, M.; Alba, J. L. Bazo; Benabderrahmane, M. L.; Berdermann, J.; Bernardini, E.; Silva, A. H. Cruz; Franke, R.; Gora, D.; Jakobi, E.; Kislat, F.; Lauer, R.; Middell, E.; Nahnhauer, R.; Schoenwald, A.; Spiering, C.; Stoessl, A.; Tosi, D.; Walter, M.; Wischnewski, R.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany. [Beattie, K.; Buitink, S.; Gerhardt, L.; Goldschmidt, A.; Kiryluk, J.; Klein, S. R.; Matis, H. S.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Beatty, J. J.; Davis, J. C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Beatty, J. J.; Davis, J. C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Bechet, S.; Bertrand, D.; Dierckxsens, M.; Hanson, K.; Marotta, A.; Petrovic, J.; Swillens, Q.] Univ Libre Brussels, Sci Fac CP230, B-1050 Brussels, Belgium. [Altmann, D.; Becker, J. K.; Dreyer, J.; Fedynitch, A.; Olivo, M.; Richman, M.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany. [Berley, D.; Blaufuss, E.; Christy, B.; Ellsworth, R. W.; Goodman, J. A.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Schmidt, T.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Besson, D. Z.; Kenny, P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Gluesenkamp, T.; Heinen, D.; Hofmann, B.; Huelss, J. -P.; Laihem, K.; Meures, T.; Paul, L.; Schukraft, A.; Schunck, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany. [Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, S-10691 Stockholm, Sweden. [Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Zoll, M.] Stockholm Univ, Dept Phys, S-10691 Stockholm, Sweden. [Bose, D.; De Clercq, C.; Labare, M.; Singh, K.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium. [Boeser, S.; Degner, T.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.; Ribordy, M.; Stueer, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany. [Botner, O.; Engdegard, O.; Hallgren, A.; Miller, J.; Olivo, M.; de los Heros, C. Perez; Stroem, R.; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. [Clevermann, F.; Koehne, H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany. [Cohen, S.; Demiroers, L.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland. [Colnard, C.; Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.; Voge, M.; Wolf, M.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany. [Allen, M. M.; Caballero-Mora, K. S.; Cowen, D. F.; DeYoung, T.; Dunkman, M.; Fox, B. D.; Ha, C.; Koskinen, D. J.; Larson, M. J.; Meszaros, P.; Rutledge, D.; Slipak, A.; Toale, P. A.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Cowen, D. F.; Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Fadiran, O.; Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA. [Fazely, A. R.; Richard, A. S.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Grant, D.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Baum, V.; Griesel, T.; Koepke, L.; Kowarik, T.; Kroll, G.; Luenemann, J.; Piegsa, A.; Rothmaier, F.; Sander, H. -G.; Schatto, K.; Schulte, L.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany. [Kohnen, G.] Univ Mons, B-7000 Mons, Belgium. [Ishihara, A.; Mase, K.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan. [Kappes, A.; Kolanoski, H.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. [Montaruli, T.] Dipartimento Fis, Sez INFN, I-70126 Bari, Italy. [Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA. [Seunarine, S.] Univ W Indies, Dept Phys, Bridgetown, Barbados. [Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Huelsnitz, W.; Williams, D. R.; Xu, D. L.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Huelsnitz, W.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Abbasi, R (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA. EM lutz.koepke@uni-mainz.de RI Koskinen, David/G-3236-2014; Auffenberg, Jan/D-3954-2014; Aguilar Sanchez, Juan Antonio/H-4467-2015; Maruyama, Reina/A-1064-2013; Laihem, Karim/K-3835-2015; Sarkar, Subir/G-5978-2011; Beatty, James/D-9310-2011; Wiebusch, Christopher/G-6490-2012 OI Koskinen, David/0000-0002-0514-5917; Auffenberg, Jan/0000-0002-1185-9094; Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X; Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952; Wiebusch, Christopher/0000-0002-6418-3008 NR 2 TC 5 Z9 5 U1 0 U2 12 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2014 VL 563 AR C1 DI 10.1051/0004-6361/201117810e PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE2JB UT WOS:000333798000144 ER PT J AU Ellerbroek, LE Podio, L Dougados, C Cabrit, S Sitko, ML Sana, H Kaper, L de Koter, A Klaassen, PD Mulders, GD Mendigutia, I Grady, CA Grankin, K van Winckel, H Bacciotti, F Russell, RW Lynch, DK Hammel, HB Beerman, LC Day, AN Huelsman, DM Werren, C Henden, A Grindlay, J AF Ellerbroek, L. E. Podio, L. Dougados, C. Cabrit, S. Sitko, M. L. Sana, H. Kaper, L. de Koter, A. Klaassen, P. D. Mulders, G. D. Mendigutia, I. Grady, C. A. Grankin, K. van Winckel, H. Bacciotti, F. Russell, R. W. Lynch, D. K. Hammel, H. B. Beerman, L. C. Day, A. N. Huelsman, D. M. Werren, C. Henden, A. Grindlay, J. TI Relating jet structure to photometric variability: the Herbig Ae star HD 163296 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; circumstellar matter; stars: variables: T Tauri, Herbig Ae/Be; ISM: jets and outflows; Herbig-Haro objects; stars: individual: HD 163296 ID PRE-MAIN-SEQUENCE; T-TAURI STARS; HUBBLE-SPACE-TELESCOPE; YOUNG STELLAR OBJECTS; INTERMEDIATE-MASS STARS; NEAR-INFRARED EMISSION; SYSTEM Z CMA; AE/BE STARS; PROTOPLANETARY DISKS; ACCRETION RATES AB Herbig Ae/Be stars are intermediate-mass pre-main sequence stars surrounded by circumstellar dust disks. Some are observed to produce jets, whose appearance as a sequence of shock fronts (knots) suggests a past episodic outflow variability. This "jet fossil record" can be used to reconstruct the outflow history. We present the first optical to near-infrared (NIR) spectra of the jet from the Herbig Ae star HD 163296, obtained with VLT/X-shooter. We determine the physical conditions in the knots and also their kinematic "launch epochs". Knots are formed simultaneously on either side of the disk, with a regular interval of similar to 16 yr. The velocity dispersion versus jet velocity and the energy input are comparable between both lobes. However, the mass-loss rate, velocity, and shock conditions are asymmetric. We find. (M) over dot(jet)/(M) over dot(acc) similar to 0.01-0.1, which is consistent with magneto-centrifugal jet launching models. No evidence of any dust is found in the high-velocity jet, suggesting a launch region within the sublimation radius (<0.5 au). The jet inclination measured from proper motions and radial velocities confirms that it is perpendicular to the disk. A tentative relation is found between the structure of the jet and the photometric variability of the central source. Episodes of NIR brightening were previously detected and attributed to a dusty disk wind. We report for the first time significant optical fadings lasting from a few days up to a year, coinciding with the NIR brightenings. These are very likely caused by dust lifted high above the disk plane, and this supports the disk wind scenario. The disk wind is launched at a larger radius than the high-velocity atomic jet, although their outflow variability may have a common origin. No significant relation between outflow and accretion variability could be established. Our findings confirm that this source undergoes periodic ejection events, which may be coupled with dust ejections above the disk plane. C1 [Ellerbroek, L. E.; Kaper, L.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Podio, L.; Dougados, C.; Cabrit, S.] Inst Planetol & Astrophys Grenoble, F-38400 St Martin Dheres, France. [Podio, L.; Bacciotti, F.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Dougados, C.] CNRS Univ Chile, Lab Franco Chilien Astron LFCA, Santiago, Chile. [Cabrit, S.] Observ Paris, UMR CNRS 8112, LERMA, F-75014 Paris, France. [Sitko, M. L.] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA. [Sitko, M. L.] Space Sci Inst, Boulder, CO 80303 USA. [Sana, H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [de Koter, A.; van Winckel, H.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Leuven, Belgium. [Klaassen, P. D.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Mulders, G. D.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Mendigutia, I.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Grady, C. A.] Eureka Sci Inc, Oakland, CA 94602 USA. [Grady, C. A.] Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Grankin, K.] Sci Res Inst, Crimean Astrophys Observ, Nauchnyi, Ukraine. [Russell, R. W.; Lynch, D. K.] Aerosp Corp, Los Angeles, CA 90009 USA. [Russell, R. W.; Lynch, D. K.] Aerosp Corp, Los Angeles, CA 90009 USA. [Lynch, D. K.] Thule Sci, Topanga, CA 90290 USA. [Hammel, H. B.] Associated Univ Res Astron Inc, Washington, DC 20005 USA. [Beerman, L. C.] Univ Washington, Dept Astron, Seattle, WA 98105 USA. [Day, A. N.] Miami Univ, Dept Phys, Oxford, OH 45056 USA. [Huelsman, D. M.] Stanford Univ, Dept Management Sci & Engn, Stanford, CA 94305 USA. [Henden, A.] Amer Assoc Variable Star Observers, Cambridge, MA 02138 USA. [Grindlay, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ellerbroek, LE (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. EM lucas.ellerbroek@gmail.com RI Sana, Hugues/B-2664-2013; OI Sana, Hugues/0000-0001-6656-4130; Grankin, Konstantin/0000-0001-5707-8448; BACCIOTTI, FRANCESCA/0000-0001-5776-9476; Mendigutia, Ignacio/0000-0002-0233-5328 FU Netherlands Research School for Astronomy (NOVA); NASA ADP [NNH06CC28C, NNX09AC73G]; IR&D program at The Aerospace Corporation; FP7 Intra-European Marie Curie Fellowship [PIEF-GA-2009-253896] FX The referee, Dr. Tom Ray, is acknowledged for useful comments that helped improve the manuscript. The authors thank Myriam Benisty, Jerome Bouvier, Carsten Dominik, Patrick Hartigan, Henny Lamers, Koen Maaskant, Michiel Min, Brunella Nisini, Charlie Qi, Alex Raga, and Rens Waters for discussions about this work. Patrick Hartigan is also acknowledged for kindly providing the shock model results in tabular form. The ESO staff and Christophe Martayan in particular are acknowledged for their careful support of the VLT/X-shooter observations. Daryl Kim is acknowledged for his technical support of the BASS observing runs. The authors thank Bill Vacca, Mike Cushing, and John Rayner for useful discussions on the use of the SpeX instrument and the Spextool processing package. This work was supported by a grant from the Netherlands Research School for Astronomy (NOVA), NASA ADP grants NNH06CC28C and NNX09AC73G, and the IR&D program at The Aerospace Corporation. LP acknowledges the funding from the FP7 Intra-European Marie Curie Fellowship (PIEF-GA-2009-253896). NR 126 TC 18 Z9 18 U1 0 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2014 VL 563 AR A87 DI 10.1051/0004-6361/201323092 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE2JB UT WOS:000333798000087 ER PT J AU Faramaz, V Beust, H Thebault, P Augereau, JC Bonsor, A del Burgo, C Ertel, S Marshall, JP Milli, J Montesinos, B Mora, A Bryden, G Danchi, W Eiroa, C White, GJ Wolf, S AF Faramaz, V. Beust, H. Thebault, P. Augereau, J. -C. Bonsor, A. del Burgo, C. Ertel, S. Marshall, J. P. Milli, J. Montesinos, B. Mora, A. Bryden, G. Danchi, W. Eiroa, C. White, G. J. Wolf, S. TI Can eccentric debris disks be long-lived? A first numerical investigation and application to zeta(2) Reticuli SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE circumstellar matter; methods: numerical; planetary systems; stars: individual: zeta(2) Reticuli; celestial mechanics ID SPITZER-SPACE-TELESCOPE; SOLAR-TYPE STARS; PLANETARY SYSTEM; KUIPER-BELT; COLLISIONAL EVOLUTION; STELLAR COMPANIONS; PERICENTER GLOW; HIDDEN PLANETS; GIANT PLANETS; BROWN DWARFS AB Context. Imaging of debris disks has found evidence for both eccentric and offset disks. One hypothesis is that they provide evidence for massive perturbers, for example, planets or binary companions, which sculpt the observed structures. One such disk was recently observed in the far-IR by the Herschel Space Observatory around zeta(2) Reticuli. In contrast with previously reported systems, the disk is significantly eccentric, and the system is several Gyr old. Aims. We aim to investigate the long-term evolution of eccentric structures in debris disks caused by a perturber on an eccentric orbit around the star. We hypothesise that the observed eccentric disk around zeta(2) Reticuli might be evidence of such a scenario. If so, we are able to constrain the mass and orbit of a potential perturber, either a giant planet or a binary companion. Methods. Analytical techniques were used to predict the effects of a perturber on a debris disk. Numerical N-body simulations were used to verify these results and further investigate the observable structures that may be produced by eccentric perturbers. The long-term evolution of the disk geometry was examined, with particular application to the zeta(2) Reticuli system. In addition, synthetic images of the disk were produced for direct comparison with Herschel observations. Results. We show that an eccentric companion can produce both the observed offsets and eccentric disks. These effects are not immediate, and we characterise the timescale required for the disk to develop to an eccentric state (and any spirals to vanish). For zeta(2) Reticuli, we derive limits on the mass and orbit of the companion required to produce the observations. Synthetic images show that the pattern observed around zeta(2) Reticuli can be produced by an eccentric disk seen close to edge-on, and allow us to bring additional constraints on the disk parameters of our model (disk flux and extent). Conclusions. We conclude that eccentric planets or stellar companions can induce long-lived eccentric structures in debris disks. Observations of such eccentric structures thus provide potential evidence of the presence of such a companion in a planetary system. We considered the specific example of zeta(2) Reticuli, whose observed eccentric disk can be explained by a distant companion (at tens of AU) on an eccentric orbit (e(p) greater than or similar to 0.3). C1 [Faramaz, V.; Beust, H.; Augereau, J. -C.; Bonsor, A.; Ertel, S.; Milli, J.] UJF Grenoble 1, CNRS INSU, IPAG, UMR 5274, F-38041 Grenoble, France. [Thebault, P.] Observ Paris, LESIA, F-92195 Meudon, France. [del Burgo, C.] Inst Nacl Astrofis Opt & Electr, Puebla, Mexico. [Marshall, J. P.; Eiroa, C.] Univ Autonoma Madrid, Fac Ciencias, Dpto Fis Teor, E-28049 Madrid, Spain. [Milli, J.] European So Observ, Santiago 19, Chile. [Montesinos, B.] Ctr Astrobiol INTA CSIC, Dpt Astrofis, Madrid 28691, Spain. [Mora, A.] ESA ESAC, Aurora Technol BC, Madrid 28691, Spain. [Bryden, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Danchi, W.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [White, G. J.] Rutherford Appleton Lab, Chilton OX11 0QX, England. [White, G. J.] Open Univ, Dept Phys & Astrophys, Milton Keynes MK7 6AA, Bucks, England. [Wolf, S.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany. RP Faramaz, V (reprint author), UJF Grenoble 1, CNRS INSU, IPAG, UMR 5274, F-38041 Grenoble, France. EM Virginie.Faramaz@obs.ujf-grenoble.fr RI Montesinos, Benjamin/C-3493-2017 OI Montesinos, Benjamin/0000-0002-7982-2095 FU Agence Nationale pour la Recherche [ANR-07-BLAN-0221, ANR-2010-JCJC-0504-01, ANR-2010-JCJC-0501-01]; PNP/CNES; [AYA 2011-26202]; [ANR-2010 BLAN-0505-01] FX We thank the referee, A. Mustill, for very useful comments that contributed to the clarity of this paper. Computations presented in this paper were performed at the Service Commun de Calcul Intensif de l'Observatoire de Grenoble (SCCI), France, on the super-computer funded by the Agence Nationale pour la Recherche under contracts ANR-07-BLAN-0221, ANR-2010-JCJC-0504-01 and ANR-2010-JCJC-0501-01. B. Montesinos, C. Eiroa and J.P. Marshall are supported by Spanish grant AYA 2011-26202. A. Bonsor and S. Ertel acknowledge support from the ANR-2010 BLAN-0505-01 (EXOZODI). The authors wish to thank the PNP/CNES for their financial support. This work has also greatly benefited from the software resulting from Thomas Tintillier's training project. NR 78 TC 12 Z9 12 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2014 VL 563 AR A72 DI 10.1051/0004-6361/201322469 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE2JB UT WOS:000333798000072 ER PT J AU Motiyenko, RA Ilyushin, VV Drouin, BJ Yu, S Margules, L AF Motiyenko, R. A. Ilyushin, V. V. Drouin, B. J. Yu, S. Margules, L. TI Rotational spectroscopy of methylamine up to 2.6 THz SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: molecules; methods: laboratory: molecular; submillimeter: ISM; molecular data; line: identification ID MICROWAVE-SPECTRUM; GROUND-STATE; AMINO-ACIDS; LINE SURVEY; MOLECULES; GLYCINE; B2(N) AB Context. Methylamine (CH3NH2) is the simplest primary alkylamine that has been detected in the interstellar medium. The molecule is relatively light, with the 50 K Boltzmann peak appearing near 800 GHz. However, reliable predictions for its rotational spectrum are available only up to 500 GHz. Spectroscopic analyses have been complicated by the two large-amplitude motions: internal rotation of the methyl top and inversion of the amino group. Aims. To provide reliable predictions of the methylamine ground state rotational spectrum above 500 GHz, we studied its rotational spectrum in the frequency range from 500 to 2650 GHz. Methods. The spectra of methylamine were recorded using the spectrometers based on Schottky diode frequency multiplication chains in the Lille laboratory (500-945 GHz) and in JPL (1060-2660 GHz). The analysis of the rotational spectrum of methylamine in the ground vibrational state was performed on the basis of the group-theoretical high barrier tunneling Hamiltonian developed for methylamine by Ohashi and Hougen. Results. In the recorded spectra, we have assigned 1849 new rotational transitions of methylamine. They were fitted together with previously published data, to a Hamiltonian model that uses 76 parameters with an overall weighted rms deviation of 0.87. On the basis of the new spectroscopic results, predictions of transition frequencies in the frequency range up to 3 THz with J <= 50 and K-a <= 20 are presented. C1 [Motiyenko, R. A.; Margules, L.] Univ Lille 1, Lab Phys Lasers Atomes & Mol, UMR CNRS 8523, F-59655 Villeneuve Dascq, France. [Ilyushin, V. V.] NASU, Inst Radio Astron, UA-61002 Kharkov, Ukraine. [Drouin, B. J.; Yu, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Motiyenko, RA (reprint author), Univ Lille 1, Lab Phys Lasers Atomes & Mol, UMR CNRS 8523, F-59655 Villeneuve Dascq, France. EM roman.motienko@univ-lille1.fr RI Yu, Shanshan/D-8733-2016 FU Ukrainian-French CNRS-PICS [6051] FX The authors are indebted to Dr. N. Ohashi for providing his fitting program for methylamine. This work was done with the support of the Ukrainian-French CNRS-PICS 6051 project. Portions of this research were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 28 TC 4 Z9 4 U1 3 U2 16 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2014 VL 563 AR A137 DI 10.1051/0004-6361/201323190 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE2JB UT WOS:000333798000137 ER PT J AU Pires, AM Haberl, F Zavlin, VE Motch, C Zane, S Hohle, MM AF Pires, A. M. Haberl, F. Zavlin, V. E. Motch, C. Zane, S. Hohle, M. M. TI XMM-Newton reveals a candidate period for the spin of the "Magnificent Seven" neutron star RX J1605.3+3249 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: individuals: RX J1605.3+3249; stars: neutron; pulsars: general ID X-RAY-EMISSION; ROTATING RADIO TRANSIENTS; COHERENT TIMING SOLUTION; BROAD ABSORPTION FEATURE; PHOTON IMAGING CAMERA; MAGNETIC-FIELD; PROPER MOTION; MAGNETOTHERMAL EVOLUTION; 1RXS J130848.6+212708; SPECTRAL FEATURE AB Context. The group of seven thermally emitting isolated neutron stars (INSs) discovered by ROSAT and known as the "Magnificent Seven" (M7) is unique among the various neutron star populations. Crustal heating by means of magnetic field decay and an evolutionary link with magnetars may explain why these objects rotate more slowly and have higher thermal luminosities and magnetic field intensities than standard rotation-powered pulsars of similar age. Aims. The third brightest INS, RX J1605.3+3249, is the only object amidst the seven still lacking a detected periodicity. The source spectrum, while purely thermal with no significant magnetospheric emission, is complex and displays both narrow and broad absorption features that can potentially be used to constrain the surface component of the magnetic field, as well as the mass-to-radius ratio of the neutron star. Methods. We observed the source with the XMM-Newton Observatory for 60 ks aiming at unveiling the neutron star rotation rate and investigating its spectrum in detail. We confront our results with previous observations of the source and discuss its properties in the context of the M7 as a group and of the known population of Galactic INSs. Results. A periodic signal at P = 3.387864(16) s, most likely the neutron star spin period, is detected at the 4 sigma confidence level. The amplitude of the modulation was found to be energy dependent and is more significantly detected when the timing search is restricted to photons with energy higher than similar to 0.5 keV. The coherent combination of the new data with a past XMM-Newton EPIC-pn observation of the source constrains the pulsar spin-down rate at the 2 sigma confidence level, (nu) over dot similar to -1.39 x 10(-13) Hz s(-1), implying a dipolar magnetic field of B-dip similar to 7.4 x 10(13) G. If confirmed, RX J1605.3+3249 would be the neutron star with the highest dipolar field amongst the M7. The spectrum of the source shows evidence of a cool blackbody component, as well as for the presence of two broad absorption features. Furthermore, high-resolution spectroscopy with the RGS cameras confirms the presence of a narrow absorption feature at energy similar to 0.57 keV in the co-added spectrum of the source, also seen in other thermally emitting isolated neutron stars. Conclusions. Phase-resolved spectroscopy, as well as a dedicated observing campaign aimed at determining a timing solution, will give invaluable constraints on the neutron star geometry and will allow one to confirm the high value of spin down, which would place the source closer to a magnetar than any other M7 INS. C1 [Pires, A. M.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Haberl, F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Zavlin, V. E.] NASA, Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA. [Motch, C.] Univ Strasbourg, CNRS, Astron Observ, F-67000 Strasbourg, France. [Zane, S.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Hohle, M. M.] Inst Astrophys, D-07745 Jena, Germany. [Hohle, M. M.] Univ Sternwarte Jena, D-07745 Jena, Germany. RP Pires, AM (reprint author), Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany. EM apires@aip.de FU Deutsche Forschungsgemeinschaft [PI 983/1-1] FX The work of A. M. P. is supported by the Deutsche Forschungsgemeinschaft (grant PI 983/1-1). The authors acknowledge the use of the ATNF Pulsar Catalogue (http://www.atnf.csiro.au/research/pulsar/psrcat). We thank the anonymous referee for suggestions that helped improving the manuscript. NR 95 TC 5 Z9 5 U1 1 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2014 VL 563 AR A50 DI 10.1051/0004-6361/201423380 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE2JB UT WOS:000333798000050 ER PT J AU Soldi, S Beckmann, V Baumgartner, WH Ponti, G Shrader, CR Lubinski, P Krimm, HA Mattana, F Tueller, J AF Soldi, S. Beckmann, V. Baumgartner, W. H. Ponti, G. Shrader, C. R. Lubinski, P. Krimm, H. A. Mattana, F. Tueller, J. TI Long-term variability of AGN at hard X-rays SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; galaxies: Seyfert; X-rays: galaxies; surveys ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASS; SEYFERT 1 GALAXIES; SPECTRAL DENSITY-FUNCTION; XMM-NEWTON; MULTIWAVELENGTH CAMPAIGN; NGC 4051; CONTINUUM VARIABILITY; INTEGRAL OBSERVATIONS; OPTICAL VARIABILITY AB Aims. Variability at all observed wavelengths is a distinctive property of active galactic nuclei (AGN). Hard X-rays provide us with a view of the innermost regions of AGN, mostly unbiased by absorption along the line of sight. Characterizing the intrinsic hard X-ray variability of a large AGN sample and comparing it to the results obtained at lower X-ray energies can significantly contribute to our understanding of the mechanisms underlying the high-energy radiation. Methods. Swift/BAT provides us with the unique opportunity to follow, on time scales of days to years and with regular sampling, the 14-195 keV emission of the largest AGN sample available up to date for this kind of investigation. As a continuation of an early work using the first 9 months of BAT data, we study the amplitude of the variations and their dependence on subclass and on energy, for a sample of 110 radio quiet and radio loud AGN selected from the BAT 58-month survey. Results. About 80% of the AGN in the sample are found to exhibit significant variability on month-to-year time scales. In particular, radio loud sources are the most variable, and Seyfert 1.5-2 galaxies are slightly more variable than Seyfert 1, while absorbed and unabsorbed objects show similar timing properties. The amplitude of the variations and their energy dependence are incompatible with variability being driven at hard X-rays by changes in the absorption column density. In general, the variations in the 14-24 and 35-100 keV bands are correlated well, suggesting a common origin to the variability across the BAT energy band. However, radio quiet AGN display on average 10% larger variations at 14-24 keV than at 35-100 keV, and a softer-when-brighter behavior for most of the Seyfert galaxies with detectable spectral variability on a time scale of a month. In addition, sources with harder spectra are found to be more variable than softer ones, unlike what it is observed below 10 keV. These properties are generally consistent with a variable, in flux and shape, power law continuum, pivoting at energies greater than or similar to 50 keV, to which a constant reflection component is superposed. When the same time scales are considered, the timing properties of AGN at hard X-rays are comparable to those at lower energies, with at least some of the differences possibly ascribable to components contributing differently in the two energy domains (e. g., reflection, absorption). C1 [Soldi, S.] Univ Paris Diderot, Sorbonne Paris Cite, CEA Irfu, APC,CNRS IN2P3,Observ Paris, F-75205 Paris 13, France. [Beckmann, V.; Mattana, F.] Univ Paris Diderot, CNRS IN2P3, CEA Irfu, APC,Francois Arsgo Ctr,Sorbonne Paris Cite,Observ, F-75205 Paris 13, France. [Baumgartner, W. H.; Shrader, C. R.; Krimm, H. A.; Tueller, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Baumgartner, W. H.] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA. [Ponti, G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Shrader, C. R.; Krimm, H. A.] Univ Space Res Assoc, CRESST, Greenbelt, MD 20771 USA. [Shrader, C. R.; Krimm, H. A.] NASA GSFC, Greenbelt, MD 20771 USA. [Lubinski, P.] Univ Zielona Gora, Inst Phys, PL-65417 Zielona Gora, Poland. RP Soldi, S (reprint author), Univ Paris Diderot, Sorbonne Paris Cite, CEA Irfu, APC,CNRS IN2P3,Observ Paris, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France. EM soldi@apc.univ-paris7.fr FU Centre National d'Etudes Spatiales (CNES); EU Marie Curie Intra-European fellowship [FP-PEOPLE-2012-IEF-331095]; LabEx UnivEarthS project; Polish NCN [N N203 581240, 2012/04/M/ST9/00780] FX The authors thank Jerome Rodriguez for useful discussions of Galactic black holes, and the anonymous referee for the valuable suggestions that helped to improve this paper. S.S. acknowledges the Centre National d'Etudes Spatiales (CNES) for financial support. G.P. acknowledges support via an EU Marie Curie Intra-European fellowship under contract No. FP-PEOPLE-2012-IEF-331095. This work has been partly supported by the LabEx UnivEarthS project "Impact of black holes on their environment", and by the Polish NCN grants N N203 581240 and 2012/04/M/ST9/00780. This article commemorates our colleague Jack Tueller who passed away during the study. NR 135 TC 13 Z9 13 U1 1 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2014 VL 563 AR A57 DI 10.1051/0004-6361/201322653 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE2JB UT WOS:000333798000057 ER PT J AU Wiegert, J Liseau, R Thebault, P Olofsson, G Mora, A Bryden, G Marshall, JP Eiroa, C Montesinos, B Ardila, D Augereau, JC Aran, AB Danchi, WC del Burgo, C Ertel, S Fridlund, MCW Hajigholi, M Krivov, AV Pilbratt, GL Roberge, A White, GJ Wolf, S AF Wiegert, J. Liseau, R. Thebault, P. Olofsson, G. Mora, A. Bryden, G. Marshall, J. P. Eiroa, C. Montesinos, B. Ardila, D. Augereau, J. C. Aran, A. Bayo Danchi, W. C. del Burgo, C. Ertel, S. Fridlund, M. C. W. Hajigholi, M. Krivov, A. V. Pilbratt, G. L. Roberge, A. White, G. J. Wolf, S. TI How dusty is alpha Centauri? Excess or non-excess over the infrared photospheres of main-sequence stars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: individual: Alpha Centauri; binaries: general; circumstellar matter; infrared: stars; infrared: planetary systems; submillimeter: stars ID DEBRIS DISKS; SIZE DISTRIBUTION; BINARY-SYSTEMS; COLLISIONAL EVOLUTION; TEMPERATURE MINIMUM; SOLAR CHROMOSPHERE; PROTOSTELLAR CORES; RADIATION PRESSURE; MOLECULAR CLOUDS; PLANET FORMATION AB Context. Debris discs around main-sequence stars indicate the presence of larger rocky bodies. The components of the nearby, solar-type binary alpha Centauri have metallicities that are higher than solar, which is thought to promote giant planet formation. Aims. We aim to determine the level of emission from debris around the stars in the alpha Cen system. This requires knowledge of their photospheres. Having already detected the temperature minimum, T-min, of alpha Cen A at far-infrared wavelengths, we here attempt to do the same for the more active companion alpha Cen B. Using the alpha Cen stars as templates, we study the possible effects that T-min may have on the detectability of unresolved dust discs around other stars. Methods. We used Herschel-PACS, Herschel-SPIRE, and APEX-LABOCA photometry to determine the stellar spectral energy distributions in the far infrared and submillimetre. In addition, we used APEX-SHeFI observations for spectral line mapping to study the complex background around alpha Cen seen in the photometric images. Models of stellar atmospheres and of particulate discs, based on particle simulations and in conjunction with radiative transfer calculations, were used to estimate the amount of debris around these stars. Results. For solar-type stars more distant than alpha Cen, a fractional dust luminosity f(d) equivalent to L-dust/L-star similar to 2 x 10(-7) could account for SEDs that do not exhibit the T-min effect. This is comparable to estimates of f(d) for the Edgeworth-Kuiper belt of the solar system. In contrast to the far infrared, slight excesses at the 2.5 sigma level are observed at 24 mu m for both alpha Cen A and B, which, if interpreted as due to zodiacal-type dust emission, would correspond to f(d) similar to (1-3) x 10(-5), i.e. some 10(2) times that of the local zodiacal cloud. Assuming simple power-law size distributions of the dust grains, dynamical disc modelling leads to rough mass estimates of the putative Zodi belts around the alpha Cen stars, viz. less than or similar to 4 x 10(-6) M-(sic) of 4 to 1000 mu m size grains, distributed according to n(a) proportional to a(-3.5). Similarly, for filled-in T-min emission, corresponding Edgeworth-Kuiper belts could account for similar to 10(-3) M-(sic) of dust. Conclusions. Our far-infrared observations lead to estimates of upper limits to the amount of circumstellar dust around the stars alpha Cen A and B. Light scattered and/or thermally emitted by exo-Zodi discs will have profound implications for future spectroscopic missions designed to search for biomarkers in the atmospheres of Earth-like planets. The far-infrared spectral energy distribution of alpha Cen B is marginally consistent with the presence of a minimum temperature region in the upper atmosphere of the star. We also show that an alpha Cen A-like temperature minimum may result in an erroneous apprehension about the presence of dust around other, more distant stars. C1 [Wiegert, J.; Liseau, R.; Hajigholi, M.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Thebault, P.] Observ Paris, Sect Meudon, Lab Etud Spatials Instrumentat Astrophys, F-92195 Meudon, France. [Olofsson, G.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Mora, A.] ESA, ESAC Gaia SOC, Madrid 28691, Spain. [Bryden, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Marshall, J. P.; Eiroa, C.] Univ Autonoma Madrid, Fac Ciencias, E-28049 Madrid, Spain. [Montesinos, B.] CSIC, INTA, CAB, Ctr Astrobiol,Dept Astrofis, Madrid 28691, Spain. [Ardila, D.] CALTECH, NASA, Herschel Sci Ctr, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Ardila, D.] ESAC, European Space Agcy, Herschel Sci Ctr C11, Madrid 28691, Spain. [Augereau, J. C.; Ertel, S.] UJF Grenoble 1, IPAG, CNRS INSU, F-38041 Grenoble, France. [Aran, A. Bayo] European So Observ, Santiago 19, Chile. [Aran, A. Bayo] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Danchi, W. C.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [del Burgo, C.] Inst Nacl Astrofis Opt Elect, Puebla, Mexico. [Fridlund, M. C. W.] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany. [Fridlund, M. C. W.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Krivov, A. V.] Univ Jena, Astrophys Inst & Univ Sternwarte, D-07745 Jena, Germany. [Pilbratt, G. L.] ESTEC, Res & Sci Support Dept ESA, Astrophys Miss Div, NL-2200 AG Noordwijk, Netherlands. [Roberge, A.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [White, G. J.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [White, G. J.] Rutherford Appleton Lab, CCLRC, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. [Wolf, S.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany. RP Wiegert, J (reprint author), Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. EM wiegert@chalmers.se RI Roberge, Aki/D-2782-2012; Montesinos, Benjamin/C-3493-2017; OI Roberge, Aki/0000-0002-2989-3725; Montesinos, Benjamin/0000-0002-7982-2095; Marshall, Jonathan/0000-0001-6208-1801 FU Spanish grant [AYA 2011/26202]; Marie Curie Actions of the European Comission; French National Research Agency (ANR) [ANR2010 BLAN-0505-01] FX We thank the referee for the critical reading of the manuscript and the valuable suggestions that improved the quality of the paper. We are also grateful to H. Olofsson for granting his Director's Discretionary Time to this project. We also wish to thank P. Bergman for his help with the APEX observations on such short notice and the swift reduction of the data. We appreciate the continued support of the Swedish National Space Board (SNSB) for our Herschel projects. The Swedish authors appreciate the continued support from the Swedish National Space Board ( SNSB) for our Herschel projects. C. Eiroa, J. P. Marshall, and B. Montesinos are partially supported by Spanish grant AYA 2011/26202. A. Bayo was co-funded under the Marie Curie Actions of the European Comission (FP7-COFUND). S. Ertel thanks the French National Research Agency (ANR) for financial support through contract ANR2010 BLAN-0505-01 (EXOZODI). NR 98 TC 3 Z9 3 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2014 VL 563 AR A102 DI 10.1051/0004-6361/201321887 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE2JB UT WOS:000333798000102 ER PT J AU Plachta, DW Guzik, MC AF Plachta, David W. Guzik, Monica C. TI Cryogenic Boil-Off Reduction System SO CRYOGENICS LA English DT Article DE Self-supporting multi-layer insulation; Reverse turbo-Brayton cycle cryocooler; Zero boil-off; Cryogenic propellant storage AB A computational model of the cryogenic boil-off reduction system being developed by NASA as part of the Cryogenic Propellant Storage and Transfer technology maturation project has been applied to a range of propellant storage tanks sizes for high-performing in-space cryogenic propulsion applications. This effort focuses on the scaling of multi-layer insulation (MLI), cryocoolers, broad area cooling shields, radiators, solar arrays, and tanks for liquid hydrogen propellant storage tanks ranging from 2 to 10 m in diameter. Component scaling equations were incorporated into the Cryogenic Analysis Tool, a spreadsheet-based tool used to perform system-level parametric studies. The primary addition to the evolution of this updated tool is the integration of a scaling method for reverse turbo-Brayton cycle cryocoolers, as well as the development and inclusion of Self-Supporting Multi-Layer Insulation. Mass, power, and sizing relationships are traded parametrically to establish the appropriate loiter period beyond which this boil-off reduction system application reduces mass. The projected benefit compares passive thermal control to active thermal control, where active thermal control is evaluated for reduced boil-off with a 90 K shield, zero boil-off with a single heat interception stage at the tank wall, and zero boil-off with a second interception stage at a 90 K shield. Parametric studies show a benefit over passive storage at loiter durations under one month, in addition to showing a benefit for two-stage zero boil-off in terms of reducing power and mass as compared to single stage zero boil-off. Furthermore, active cooling reduces the effect of varied multi-layer insulation performance, which, historically, has been shown to be significant. Published by Elsevier Ltd. C1 [Plachta, David W.; Guzik, Monica C.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Plachta, DW (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM david.w.plachta@nasa.gov NR 10 TC 2 Z9 2 U1 5 U2 22 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0011-2275 EI 1879-2235 J9 CRYOGENICS JI Cryogenics PD MAR-APR PY 2014 VL 60 BP 62 EP 67 DI 10.1016/j.cryogenics.2013.12.006 PG 6 WC Thermodynamics; Physics, Applied SC Thermodynamics; Physics GA AE5AP UT WOS:000334000500009 ER PT J AU Nagihara, S Hedlund, M Zacny, K Taylor, PT AF Nagihara, Seiichi Hedlund, Magnus Zacny, Kris Taylor, Patrick T. TI Improved data reduction algorithm for the needle probe method applied to in-situ thermal conductivity measurements of lunar and planetary regoliths SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Heat flow; Thermal conductivity; JSC-1A; Needle probe ID PARTICULATE MATERIALS AB The needle probe method (also known as the 'hot wire' or 'line heat source' method) is widely used for in-situ thermal conductivity measurements on terrestrial soils and marine sediments. Variants of this method have also been used (or planned) for measuring regolith on the surfaces of extra-terrestrial bodies (e.g., the Moon, Mars, and comets). In the near-vacuum condition on the lunar and planetary surfaces, the measurement method used on the earth cannot be simply duplicated, because thermal conductivity of the regolith can be similar to 2 orders of magnitude lower. In addition, the planetary probes have much greater diameters, due to engineering requirements associated with the robotic deployment on extra-terrestrial bodies. All of these factors contribute to the planetary probes requiring a much longer time of measurement, several tens of (if not over a hundred) hours, while a conventional terrestrial needle probe needs only 1 to 2 min. The long measurement time complicates the surface operation logistics of the lander. It also negatively affects accuracy of the thermal conductivity measurement, because the cumulative heat loss along the probe is no longer negligible. The present study improves the data reduction algorithm of the needle probe method by shortening the measurement time on planetary surfaces by an order of magnitude. The main difference between the new scheme and the conventional one is that the former uses the exact mathematical solution to the thermal model on which the needle probe measurement theory is based, while the latter uses an approximate solution that is valid only for large times. The present study demonstrates the benefit of the new data reduction technique by applying it to data from a series of needle probe experiments carried out in a vacuum chamber on a lunar regolith simulant, JSC-1A. The use of the exact solution has some disadvantage, however, in requiring three additional parameters, but two of them (the diameter and the volumetric heat capacity of the probe) can be measured and the other (the volumetric heat capacity of the regolith/stimulant) may be estimated from the surface geologic observation and temperature measurements. Therefore, overall, the new data reduction scheme would make in-situ thermal conductivity measurement more practical on planetary missions. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Nagihara, Seiichi] Texas Tech Univ, Dept Geosci, Lubbock, TX 79409 USA. [Hedlund, Magnus; Zacny, Kris] Honeybee Robot, Pasadena, CA 91103 USA. [Taylor, Patrick T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Nagihara, S (reprint author), Texas Tech Univ, Dept Geosci, Lubbock, TX 79409 USA. EM seiichi.nagihara@ttu.edu FU NASA [10-PIDDP10-028] FX This work was supported by the NASA Planetary Instrument Definition and Development Program (10-PIDDP10-028). The authors thank Matthew Siegler and Walter Kiefer for constructive reviews and comments which helped improve this manuscript. NR 36 TC 0 Z9 0 U1 1 U2 12 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 MAR PY 2014 VL 92 BP 49 EP 56 DI 10.1016/j.pss.2013.12.012 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE2CF UT WOS:000333780200005 ER PT J AU Vasudev, R Mansour, K Webster, CR AF Vasudev, R. Mansour, K. Webster, C. R. TI Planetary laser spectrometer for sensitive in situ detection of water at 1881 nm SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Laser spectroscopy; Water; Isotopologues; Solar system applications ID ENHANCED ABSORPTION-SPECTROSCOPY; WAVELENGTH MODULATION; FREQUENCY-MODULATION; HIGH OBLIQUITY; MARS; ICE; ENCELADUS; SURFACE; ORGANICS; PLUME AB We describe the design and capabilities of a highly sensitive prototype tunable diode laser spectrometer for detecting water vapor and its isotopologues in the 1881 nm region. It is a compact instrument based on wavelength modulated cavity enhanced absorption spectroscopy and can measure a fractional optical absorption of similar to 10(-5) for a pathlength of similar to 4 km, corresponding to similar to 10(-8) mbar of water vapor (improvable to 10(-9) mbar). The spectrometer would be suitable for searching for fingerprints of ancient climates on Mars and potential habitats of life in the Solar system. It would be useful for appraising water deposits on the Moon and asteroids, and characterizing the isotopic composition. Lunar deployment could provide ground truth to the recent orbital measurements, and help to discover records of the early bombardment history of the inner Solar system buried at the poles and clarify the mechanism for the generation of water in the illuminated regions. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Vasudev, R.; Mansour, K.; Webster, C. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Vasudev, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM rvasudev@jpl.nasa.gov NR 58 TC 0 Z9 0 U1 1 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD MAR PY 2014 VL 92 BP 127 EP 135 DI 10.1016/j.pss.2014.01.009 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE2CF UT WOS:000333780200013 ER PT J AU Conrath, CL Tribuzio, CA Goldman, KJ AF Conrath, Christina L. Tribuzio, Cindy A. Goldman, Kenneth J. TI Notes on the Reproductive Biology of Female Salmon Sharks in the Eastern North Pacific Ocean SO TRANSACTIONS OF THE AMERICAN FISHERIES SOCIETY LA English DT Article ID LAMNA-DITROPIS; AUSTRALIA; GROWTH AB Little is known about the reproductive biology of the Salmon Shark Lamna ditropis from the eastern North Pacific Ocean. Female Salmon Shark specimens were collected from Alaskan waters in the summer, autumn, and winter to examine reproductive seasonality, the reproductive interval, fecundity, and embryonic development. Female Salmon Sharks were found to ovulate during the autumn months of September and October, and those captured in July were either in a resting or postpartum state, indicating a short gestation time of 9-10 months. The presence of two mature reproductive states in both the summer and autumn months indicates a biennial reproductive cycle and a resting period of at least 14 months between parturition and ovulation. This study found mean fecundity was 3.88 pups per litter (n = 8; SE = 0.13), with the majority of pregnant Salmon Sharks having a fecundity of four sharks per litter. These results provide new information on the reproductive biology of Salmon Sharks and will aid in the development of stock assessments for this species. Received June 26, 2013; accepted October 24, 2013 C1 [Conrath, Christina L.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Resource Assessment & Conservat Engn Div,Kodiak L, Kodiak, AK 99615 USA. [Tribuzio, Cindy A.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, Juneau, AK 99801 USA. [Goldman, Kenneth J.] Alaska Dept Fish & Game, Div Commercial Fisheries, Homer, AK 99603 USA. RP Conrath, CL (reprint author), NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Resource Assessment & Conservat Engn Div,Kodiak L, 301 Res Court, Kodiak, AK 99615 USA. EM christina.conrath@noaa.gov NR 22 TC 0 Z9 0 U1 3 U2 8 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 520 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0002-8487 EI 1548-8659 J9 T AM FISH SOC JI Trans. Am. Fish. Soc. PD MAR 1 PY 2014 VL 143 IS 2 BP 363 EP 368 DI 10.1080/00028487.2013.862179 PG 6 WC Fisheries SC Fisheries GA AE3NI UT WOS:000333882800005 ER PT J AU Berejikian, BA Bush, RA Campbell, LA AF Berejikian, Barry A. Bush, Richard A. Campbell, Lance A. TI Maternal Control over Offspring Life History in a Partially Anadromous Species, Oncorhynchus mykiss SO TRANSACTIONS OF THE AMERICAN FISHERIES SOCIETY LA English DT Article ID SALMON SALMO-SALAR; RESIDENT RAINBOW-TROUT; ATLANTIC SALMON; CHINOOK SALMON; SEXUAL-MATURATION; PARTIAL MIGRATION; STEELHEAD TROUT; POPULATION-STRUCTURE; GENETIC-DIVERGENCE; BROOK CHARR AB Environmental variability among freshwater habitats may influence migratory decisions in partially anadromous salmonids through (1) proximate effects on individual fish development and condition and (2) longer-term genetic adaptations of populations to the various environments. However, the relative importance of the two factors has been difficult to sort out. We used the gonadosomatic index as an indicator of maturation-and therefore residency-in age-1 and age-2 parr collected from eight partially anadromous Oncorhynchus mykiss (Rainbow Trout/steelhead) populations occupying a diversity of freshwater habitats. Substantial environmental variability among the eight Hood Canal (Washington) streams had little effect on life history pathways in male and female offspring of anadromous females (hereafter, ANAD parr), with the exception of significantly higher maturation rates in male ANAD parr from one population (Little Quilcene River). Between 0% and 8% of the female ANAD parr had initiated maturation, whereas 33% (Duckabush River) or 53% (Hamma Hamma River) maturation was observed among the female offspring of resident females (hereafter, RES parr) in the two populations with substantial resident components. The results indicate strong maternal control over offspring life history pathways in systems where resident and anadromous forms are sympatric. The RES parr that were collected above and below barriers to anadromy showed similar likelihoods of maturation. The expression of residency and anadromy in Hood Canal populations appears to reflect genetic adaptations to the diverse freshwater habitats (including the effects of O. mykiss sequestered above anadromy barriers) and, to some degree, the phenotypically plastic responses of male parr to the environmental variability among streams. Received July 26, 2013; accepted October 29, 2013 C1 [Berejikian, Barry A.] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Resource Enhancement & Utilizat Technol Div, Manchester, WA 98366 USA. [Bush, Richard A.] NOAA, Natl Marine Fisheries Serv, Southwest Reg Off, Protected Resources Div, Long Beach, CA 90802 USA. [Campbell, Lance A.] Washington Dept Fish & Wildlife, Olympia, WA 98501 USA. RP Berejikian, BA (reprint author), NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Resource Enhancement & Utilizat Technol Div, POB 130, Manchester, WA 98366 USA. EM barry.berejikian@noaa.gov NR 57 TC 3 Z9 3 U1 1 U2 34 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0002-8487 EI 1548-8659 J9 T AM FISH SOC JI Trans. Am. Fish. Soc. PD MAR 1 PY 2014 VL 143 IS 2 BP 369 EP 379 DI 10.1080/00028487.2013.862181 PG 11 WC Fisheries SC Fisheries GA AE3NI UT WOS:000333882800006 ER PT J AU Osborne, SJ Hanson, D Dore, O AF Osborne, Stephen J. Hanson, Duncan Dore, Olivier TI Extragalactic foreground contamination in temperature-based CMB lens reconstruction SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE non-gaussianity; gravitational waves and CMBR polarization; CMBR experiments; CMBR theory ID BIAS; SKY AB We discuss the effect of unresolved point source contamination on estimates of the CMB lensing potential, from components such as the thermal Sunyaev-Zel'dovich e ff ect, radio point sources, and the Cosmic Infrared Background. We classify the possible trispectra associated with such source populations, and construct estimators for the amplitude and scale-dependence of several of the major trispectra. We show how to propagate analytical models for these source trispectra to biases for lensing. We also construct a "source-hardened" lensing estimator which experiences signi fi cantly smaller biases when exposed to unresolved point sources than the standard quadratic lensing estimator. We demonstrate these ideas in practice using the sky simulations of Sehgal et al., for cosmic-variance limited experiments designed to mimic ACT, SPT, and Planck. We fi nd that for radio sources and SZ the bias is signi fi cantly reduced, but for CIB it is essentially unchanged. However, by using the high-frequency, all-sky CIB measurements from Planck and Her s c h e l it may be possible to suppress this contribution. C1 [Osborne, Stephen J.] Stanford Univ, Stanford, CA 94305 USA. [Osborne, Stephen J.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Hanson, Duncan] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Dore, Olivier] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Dore, Olivier] CALTECH, Dept Phys, Pasadena, CA 91125 USA. RP Osborne, SJ (reprint author), Stanford Univ, 382 Via Pueblo,Varian Bldg, Stanford, CA 94305 USA. EM steve.j.osborne@gmail.com; dhanson@physics.mcgill.ca; olivier.p.dore@jpl.nasa.gov FU US Planck Project; NASA Science Mission Directorate FX SJO acknowledges support from the US Planck Project, which is funded by the NASA Science Mission Directorate. Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Some of the results in this paper have been derived using the HEALPix [23] package. NR 24 TC 11 Z9 11 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD MAR PY 2014 IS 3 AR 024 DI 10.1088/1475-7516/2014/03/024 PG 18 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AE0PI UT WOS:000333667900024 ER PT J AU Paxson, DE Kaemming, T AF Paxson, Daniel E. Kaemming, Tom TI Influence of Unsteadiness on the Analysis of Pressure Gain Combustion Devices SO JOURNAL OF PROPULSION AND POWER LA English DT Article; Proceedings Paper CT 51st AIAA Aerospace Sciences Meeting Including the New Horizons Forum and Aerospace Exposition CY JAN 06-10, 2013 CL Grapevine, TX SP AIAA ID PULSE-DETONATION ENGINES AB Pressure gain combustion has been the subject of scientific study for over a century due to its promise of improved thermodynamic efficiency. In many recent application concepts, pressure gain combustion is used as a component in an otherwise continuous, normally steady flow system, such as a gas turbine or ramjet engine. However, pressure gain combustion is inherently unsteady. Failure to account for the effects of this periodic unsteadiness can lead to misunderstanding and errors in some performance calculations. This paper clarifies the accounting by presenting a consistent method of thermodynamic cycle analysis for a device using pressure gain combustion technology. The incorporation of the unsteady pressure gain combustion process into the conservation equations for a continuous flow device is presented. Most important, the appropriate method for computing the conservation of momentum is presented. It will be shown that proper, consistent analysis of cyclic conservation principles produces more realistic performance predictions. Specifically, for the ramjet example used, appropriate predictions of both the thermal efficiency (from energy conservation) and specific thrust (from momentum conservation) are developed. C1 [Paxson, Daniel E.] NASA, John H Glenn Res Ctr Lewis Field, Controls & Dynam Branch, Cleveland, OH 44130 USA. [Kaemming, Tom] Innovat Sci Solut Inc, Dayton, OH 45440 USA. RP Paxson, DE (reprint author), NASA, John H Glenn Res Ctr Lewis Field, Controls & Dynam Branch, 21000 Brookpk Rd,Mail Stop 77-1, Cleveland, OH 44130 USA. NR 11 TC 0 Z9 0 U1 3 U2 8 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 EI 1533-3876 J9 J PROPUL POWER JI J. Propul. Power PD MAR-APR PY 2014 VL 30 IS 2 BP 377 EP 383 DI 10.2514/1.B34913 PG 7 WC Engineering, Aerospace SC Engineering GA AD8ST UT WOS:000333536600014 ER PT J AU Datta, A Johnson, W AF Datta, Anubhav Johnson, Wayne TI Powerplant Design and Performance Analysis of a Manned All-Electric Helicopter SO JOURNAL OF PROPULSION AND POWER LA English DT Article; Proceedings Paper CT 12th AIAA Aviation Technology, Integration, and Operations (ATIO) Conference / 14th AIAA/ISSMO Multidisciplinary Analysis and Optimization Conference CY SEP 17-19, 2012 CL Indianapolis, IN SP AIAA, ISSMO AB This paper describes the conceptual design of three all-electric powerplants-a battery-only, a fuel-cell-only, and a battery-fuel cell hybrid powerplant-for a manned ultralight utility helicopter (Robinson R 22 Beta II-like) and carries out a comparative evaluation of performance delivered by each. The new powerplants consist of a combination of high-pressure proton exchange membrane fuel cells, 700bar type-4 hydrogen storage, a compressor-expander, lithium-ion batteries, and an alternating current synchronous permanent magnet motor. The key conclusion is that a hybrid powerplant that combines high specific power of batteries in hover and high calorific value of hydrogen in cruise delivers a superior performance compared to either system alone. The efficiency is higher than current rotorcraft piston engines but the key limitation is its low specific power, which is half of the current engines. Only 60% of the original payload can be flown (90kg solo pilot) for a duration of 35min (including 11min hover) over a range of 47km under high/hot (4000 ft/95 degrees F) conditions. The paper lays the foundations of performance analysis for all-electric rotorcraft, benchmarks the best performance achievable with current state of the art, and quantifies future technology targets to enable performance comparable to existing internal combustion engines. C1 [Datta, Anubhav] NASA, Ames Res Ctr, Sci & Technol Corp, Moffett Field, CA 94035 USA. [Johnson, Wayne] NASA, Ames Res Ctr, Aeromech Branch, Moffett Field, CA 94035 USA. RP Datta, A (reprint author), NASA, Ames Res Ctr, Sci & Technol Corp, Moffett Field, CA 94035 USA. NR 24 TC 0 Z9 0 U1 0 U2 6 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 EI 1533-3876 J9 J PROPUL POWER JI J. Propul. Power PD MAR-APR PY 2014 VL 30 IS 2 BP 490 EP 505 DI 10.2514/1.B34843 PG 16 WC Engineering, Aerospace SC Engineering GA AD8ST UT WOS:000333536600024 ER PT J AU Milos, FS Scott, CD Del Papa, SV AF Milos, Frank S. Scott, Carl D. Del Papa, Steven V. TI Arcjet Testing and Thermal Model Development for Multilayer Felt Reusable Surface Insulation SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article AB Felt reusable surface insulation was used extensively on leeward external surfaces of the shuttle Orbiter, where the material is reusable for temperatures up to 670K. For application on leeward surfaces of the Orion multipurpose crew vehicle, where predicted temperatures reach 1620K, the material functions as a pyrolyzing conformable ablator. An arcjet test series was conducted to assess the performance of multilayer felt reusable surface insulation at high temperatures, and a thermal-response, pyrolysis, and ablation model was developed. Model predictions compare favorably with the arcjet test data. C1 [Milos, Frank S.] NASA Ames Res Ctr, Thermal Protect Mat Branch, Moffett Field, CA 94035 USA. [Scott, Carl D.] LZ Technol Inc, Houston, TX 77058 USA. [Del Papa, Steven V.] NASA Johnson Space Ctr, Thermal Design Branch, Houston, TX 77058 USA. RP Milos, FS (reprint author), NASA Ames Res Ctr, Thermal Protect Mat Branch, Mail Stop 234-1, Moffett Field, CA 94035 USA. FU Orion Technology Development Project FX This work was supported by the Orion Technology Development Project. The authors greatly appreciate the assistance of T. Nguyen for arcjet test data, M. Stackpoole for laboratory data, and M. Rezin for helpful discussions of felt reusable surface insulation. The elemental composition and heat of combustion were measured at Galbraith Laboratories. NR 6 TC 3 Z9 3 U1 1 U2 5 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAR-APR PY 2014 VL 51 IS 2 BP 397 EP 411 DI 10.2514/1.A32460 PG 15 WC Engineering, Aerospace SC Engineering GA AE1VT UT WOS:000333759900002 ER PT J AU Rizvi, F AF Rizvi, Farheen TI Cassini Thruster Calibration Algorithm Using Reaction Wheel Biasing Data SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article AB Thrust force estimates for the reaction control thrusters onboard the Cassini spacecraft are presented in this paper. Cassini consists of two thruster branches, each with eight thrusters. The eight thrusters in each branch control the three body-fixed axes of the spacecraft. It is important to track the thrust force estimates in order to detect any thruster degradation and for supporting various activities in spacecraft operations (Titan flyby, spacecraft maneuvers, etc.). The Euler equation, which describes the rotational motion of the spacecraft during a reaction wheel bias event (wheel momentum change), is used to develop the algorithm. The thrust estimates are obtained from the pseudoinverse solution using flight telemetry during the bias. These results are similar to thrust estimates from the Kalman filtering algorithm. Cassini operations used the first thruster branch from launch until November2008. Results show that two thrusters in this branch exhibited degraded thrust in November2008. Because of the degraded thrust performance, the first branch usage was discontinued, and the prime branch was swapped to the second thruster branch in March2009. The thrust estimates from this branch do not show any degradation to date. The algorithm is used to trend the thruster branch thrust force estimates as the mission continues. C1 CALTECH, Jet Prop Lab, Autonomous Syst Div, Guidance & Control Operat Grp,Guidance & Control, Pasadena, CA 91109 USA. RP Rizvi, F (reprint author), CALTECH, Jet Prop Lab, Autonomous Syst Div, Guidance & Control Operat Grp,Guidance & Control, Mail Stop 230-104,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Farheen.Rizvi@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. The author would like to express great appreciation to Allan Y. Lee and Antonette Feldman for their invaluable input on the theoretical background of this work. The author would also like to thank Todd Barber from the Cassini Spacecraft Operations Team for providing the navigation team thrust estimates, Cassini spacecraft description documents, and hydrazine tank pressure data. The author would like to acknowledge the contributions of Thomas A. Burk, David Bates, and Todd Brown from the Cassini Spacecraft Operations Team. NR 4 TC 1 Z9 2 U1 0 U2 0 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAR-APR PY 2014 VL 51 IS 2 BP 563 EP 573 DI 10.2514/1.A32523 PG 11 WC Engineering, Aerospace SC Engineering GA AE1VT UT WOS:000333759900016 ER PT J AU Macala, GA Lee, AY Wang, EK AF Macala, Glenn A. Lee, Allan Y. Wang, Eric K. TI Feasibility Study of Two Cassini Reaction Wheel/Thruster Hybrid Controllers SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article AB As the first spacecraft to achieve orbit at Saturn in 2004, Cassini has collected science data throughout its four-year prime mission (2004-2008) and has since been approved for a first and second extended mission through September2017. Cassini carries a set of four reaction wheels for attitude control when stable pointing of a science instrument is required. In 2002-2003, a prime reaction wheel exhibited signs of bearing-cage instability and was replaced by the backup wheel. To date, all Cassini wheels have accumulated >3.5 billion revolutions each. As such, in spite of careful management of the wheel rates by the operation team, there are observed symptoms of anomalous wheel-bearing drag torque. To prepare for the contingency scenario in which two reaction wheels had degraded, the feasibility of controlling Cassini using the two remaining wheels and four thrusters to meet the spacecraft pointing requirements is evaluated. Our results indicate that the hybrid controllers can achieve better attitude-control performance and lower hydrazine consumption rate relative to those of an all-thruster control system. C1 [Macala, Glenn A.; Lee, Allan Y.] CALTECH, Jet Prop Lab, Div Autonomous Syst, Guidance & Control Sect, Pasadena, CA 91109 USA. [Wang, Eric K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Macala, GA (reprint author), CALTECH, Jet Prop Lab, Div Autonomous Syst, Guidance & Control Sect, Mail Stop 198-326,4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU NASA FX The work described in this paper was carried out by the Jet Propulsion Laboratory (JPL), California Institute of Technology, under contract with NASA. We are in debt to our JPL colleagues, David Bates, Tom Burk, Laura Burke, Cliff Lee, and Julie L. Webster, for helpful discussions. This paper is dedicated to the loving memory of William Breckenridge, our mentor, who has contributed to the design of the Cassini hybrid controllers. The authors also wish to thank the associate editor and three anonymous reviewers for their valuable and constructive comments on an earlier version of this paper. NR 3 TC 3 Z9 3 U1 0 U2 0 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAR-APR PY 2014 VL 51 IS 2 BP 574 EP 585 DI 10.2514/1.A32620 PG 12 WC Engineering, Aerospace SC Engineering GA AE1VT UT WOS:000333759900017 ER PT J AU Chan, V Clarke, R Squires, D AF Chan, Valerie Clarke, Raymond Squires, Dale TI Full retention in tuna fisheries: Benefits, costs and unintended consequences SO MARINE POLICY LA English DT Article DE Catch retention; Purse seine; Longline; Tuna; Western and central Pacific Ocean ID LONGLINE FISHERY; INDIAN-OCEAN; BYCATCH; DISCARDS; MORTALITY; SECURITY; PACIFIC; CATCHES AB Several tuna regional fisheries management organizations (t-RFMOs) have adopted retention requirements for skipjack, bigeye and yellowfin tunas caught by purse seine vessels to reduce discards, create disincentives to catch small fish, and incentivize the development and adoption of more selective technologies. Although retention policies in the t-RFMOs have been limited to target tunas in purse seine fisheries, some have advocated for an expansion of those policies, and t-RFMOs could consider expanding retention policies to a greater number of species and/or to other gear types. This paper discusses the benefits and costs of broader retention policies for purse seine and longline tuna fisheries in the western and central Pacific Ocean (WCPO). Using bycatch data from observers and logbooks from the U.S. purse seine and longline fleets operating in the WCPO, this paper documents the types and magnitude of fish discarded. For the purse seine fishery, this information was used to estimate direct impacts of having to off-load at the initial point of landing in key Pacific Island ports. For the longline fishery, estimates of direct impacts were limited to Honolulu and Pago Pago, American Samoa, the two primary ports where U.S. catch is landed. Expanding retention policies beyond the target tunas and to other gear types would further reduce discarding and possibly provide stronger incentives to develop and use more selective techniques. Beyond impacts to the ecosystem and fisher behavior, adopting broader retention policies may have other implications, and this paper explores those implications on vessels, processors, and communities. In general, as is the case with most direct interventions on fishing operations, there will be both benefits and costs, and the magnitude of those impacts will depend on the scope and extent of any expanded retention policy. Published by Elsevier Ltd. C1 [Chan, Valerie; Clarke, Raymond] Natl Marine Fisheries Serv, Pacific Isl Reg Off, Honolulu, HI 96814 USA. [Chan, Valerie] Univ Calif Los Angeles, Environm Sci & Engn Program, Los Angeles, CA 90095 USA. [Squires, Dale] Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, La Jolla, CA 92037 USA. RP Chan, V (reprint author), Natl Marine Fisheries Serv, Pacific Isl Reg Off, 1601 Kapiolani Blvd,Suite 1110, Honolulu, HI 96814 USA. EM valerie.chan@noaa.gov; raymond.clarke@noaa.gov; dale.squires@noaa.gov NR 34 TC 1 Z9 1 U1 4 U2 13 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0308-597X EI 1872-9460 J9 MAR POLICY JI Mar. Pol. PD MAR PY 2014 VL 45 BP 213 EP 221 DI 10.1016/j.marpol.2013.10.016 PG 9 WC Environmental Studies; International Relations SC Environmental Sciences & Ecology; International Relations GA AD8ER UT WOS:000333499800026 ER PT J AU Younes, B AF Younes, Badri TI Space lasers have bright future in communications SO PHOTONICS SPECTRA LA English DT Editorial Material C1 NASA, Pasadena, CA 91109 USA. RP Younes, B (reprint author), NASA, Pasadena, CA 91109 USA. NR 0 TC 0 Z9 0 U1 0 U2 3 PU LAURIN PUBL CO INC PI PITTSFIELD PA BERKSHIRE COMMON PO BOX 1146, PITTSFIELD, MA 01202 USA SN 0731-1230 J9 PHOTONIC SPECTRA JI Photon. Spect. PD MAR PY 2014 VL 48 IS 3 BP 26 EP 26 PG 1 WC Optics SC Optics GA AD8YK UT WOS:000333551400002 ER PT J AU Oshiyama, F Murakami, N Guyon, O Martinache, F Baba, N Matsuo, T Nishikawa, J Tamura, M AF Oshiyama, Fumika Murakami, Naoshi Guyon, Olivier Martinache, Frantz Baba, Naoshi Matsuo, Taro Nishikawa, Jun Tamura, Motohide TI Central-Obscuration Removal Plates for Focal-Plane Phase-Mask Coronagraphs with a Centrally-Obscured Telescope SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE Astronomical Instrumentation ID INDUCED AMPLITUDE APODIZATION; SUN-LIKE STAR; VORTEX CORONAGRAPH; LIGHT; COMPANIONS; APERTURE AB Focal-plane phase-mask coronagraphs, such as eight-octant phase-mask coronagraphs (8OPM), are one of the most promising tools for high contrast observations. However, coronagraphic performance would be degraded when combined with a centrally-obscured telescope. We propose pupil-remapping optics for removing the shade of a secondary mirror to generate a clear, circular pupil for the phase-mask coronagraph. First, we show the design of the pupil-remapping optics, called central-obscuration removal plates (CRPs). Next, we report laboratory experiments on the 8OPM coronagraph using manufactured CRPs. We also evaluate off-axis point-spread functions via both laboratory experiments and numerical simulations. Finally, we evaluate, via numerical simulations, limiting factors for coronagraphic performance, such as phase aberrations introduced by the CRPs, the effect of Fresnel diffraction, and chromatic behavior. The numerical simulations suggest that the phase aberrations could be a dominant limiting factor of the achievable contrast in the current laboratory experiments. C1 [Oshiyama, Fumika] Hokkaido Univ, Grad Sch Engn, Div Appl Phys, Sapporo, Hokkaido 0608628, Japan. [Murakami, Naoshi; Baba, Naoshi] Hokkaido Univ, Div Appl Phys, Fac Engn, Sapporo, Hokkaido 0608628, Japan. [Murakami, Naoshi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Guyon, Olivier] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Martinache, Frantz] CNRS UMR 7293, Lab Lagrange, Observ Cote Azur, F-06304 Nice, France. [Matsuo, Taro] Kyoto Univ, Grad Shool Sci, Kyoto 6068502, Japan. [Nishikawa, Jun; Tamura, Motohide] Natl Inst Nat Sci, Natl Astron Observ Japan, Div Opt & Infrared Astron, Mitaka, Tokyo 1818588, Japan. [Nishikawa, Jun] Grad Univ Adv Studies, Sch Phys Sci, Mitaka, Tokyo 1818588, Japan. [Tamura, Motohide] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. RP Oshiyama, F (reprint author), Hokkaido Univ, Grad Sch Engn, Div Appl Phys, Sapporo, Hokkaido 0608628, Japan. EM nmurakami@eng.hokudai.ac.jp FU NAOJ; Japan Society for the Promotion of Science (JSPS) through KAKENHI [23740139, 24103501, 25610038] FX We thank Nemanja Jovanovic and Garima Singh of the National Astronomical Observatory of Japan (NAOJ) for valuable discussions and support for the experiments on the CRPs. We are grateful to Moritsugu Sakamoto and Kazuhiko Oka of Hokkaido University for their helpful comments on numerical simulations of Fresnel diffaction. This research was partly supported by the NAOJ, and by the Japan Society for the Promotion of Science (JSPS) through KAKENHI (23740139, 24103501, and 25610038). NR 30 TC 2 Z9 2 U1 2 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD MAR 1 PY 2014 VL 126 IS 937 BP 270 EP 279 DI 10.1086/675807 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE1OO UT WOS:000333739000007 ER PT J AU Gaspari, M Brighenti, F Temi, P Ettori, S AF Gaspari, M. Brighenti, F. Temi, P. Ettori, S. TI CAN AGN FEEDBACK BREAK THE SELF-SIMILARITY OF GALAXIES, GROUPS, AND CLUSTERS? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: clusters: intracluster medium; galaxies: groups: general; galaxies: jets; hydrodynamics; methods: numerical ID ACTIVE GALACTIC NUCLEI; TEMPERATURE RELATION; INTRACLUSTER MEDIUM; SCALING RELATIONS; COOLING FLOWS; LOOSE GROUPS; EVOLUTION; SAMPLE; CORES; SIMULATIONS AB It is commonly thought that active galactic nucleus (AGN) feedback can break the self-similar scaling relations of galaxies, groups, and clusters. Using high-resolution three-dimensional hydrodynamic simulations, we isolate the impact of AGN feedback on the L-x-T-x relation, testing the two archetypal and common regimes, self-regulated mechanical feedback and a quasar thermal blast. We find that AGN feedback has severe difficulty in breaking the relation in a consistent way. The similarity breaking is directly linked to the gas evacuation within R-500, while the central cooling times are inversely proportional to the core density. Breaking self-similarity thus implies breaking the cool core, morphing all systems to non-cool-core objects, which is in clear contradiction with the observed data populated by several cool-core systems. Self-regulated feedback, which quenches cooling flows and preserves cool cores, prevents dramatic evacuation and similarity breaking at any scale; the relation scatter is also limited. The impulsive thermal blast can break the core-included L-x-T-x at T-500 less than or similar to 1 keV, but substantially empties and overheats the halo, generating a perennial non-cool-core group, as experienced by cosmological simulations. Even with partial evacuation, massive systems remain overheated. We show that the action of purely AGN feedback is to lower the luminosity and heat the gas, perpendicular to the fit. C1 [Gaspari, M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Gaspari, M.; Brighenti, F.] Univ Bologna, Dept Astron, I-40127 Bologna, Italy. [Gaspari, M.; Ettori, S.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Brighenti, F.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Temi, P.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. [Ettori, S.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy. RP Gaspari, M (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. EM mgaspari@mpa-garching.mpg.de RI Ettori, Stefano/N-5004-2015 OI Ettori, Stefano/0000-0003-4117-8617 FU Max Planck Fellowship; PRIN INAF; PRIN MIUR [2010LY5N2T]; [ASI-INAF I/009/10/0] FX The FLASH code was in part developed by the DOE NNSA-ASC OASCR Flash center at the University of Chicago. M.G. is grateful for the financial support provided by the Max Planck Fellowship. S. E. and F. B. acknowledge financial contribution from ASI-INAF I/009/10/0, PRIN INAF 2012, and PRIN MIUR 2010LY5N2T. High-performance computing resources were provided by the NASA/Ames HEC Program (SMD-13-3935, SMD-13-4373, SMD-13-4377; Pleiades). We thank M. Sun for providing data for the groups, and E. Churazov and the anonymous referee for interesting insights. NR 44 TC 13 Z9 13 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 MAR 1 PY 2014 VL 783 IS 1 AR L10 DI 10.1088/2041-8205/783/1/L10 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC4UB UT WOS:000332515500010 ER PT J AU Sartoris, B Biviano, A Rosati, P Borgani, S Umetsu, K Bartelmann, M Girardi, M Grillo, C Lemze, D Zitrin, A Balestra, I Mercurio, A Nonino, M Postman, M Czakon, N Bradley, L Broadhurst, T Coe, D Medezinski, E Melchior, P Meneghetti, M Merten, J Annunziatella, M Benitez, N Czoske, O Donahue, M Ettori, S Ford, H Fritz, A Kelson, D Koekemoer, A Kuchner, U Lombardi, M Maier, C Moustakas, LA Munari, E Presotto, V Scodeggio, M Seitz, S Tozzi, P Zheng, W Ziegler, B AF Sartoris, Barbara Biviano, Andrea Rosati, Piero Borgani, Stefano Umetsu, Keiichi Bartelmann, Matthias Girardi, Marisa Grillo, Claudio Lemze, Doron Zitrin, Adi Balestra, Italo Mercurio, Amata Nonino, Mario Postman, Marc Czakon, Nicole Bradley, Larry Broadhurst, Tom Coe, Dan Medezinski, Elinor Melchior, Peter Meneghetti, Massimo Merten, Julian Annunziatella, Marianna Benitez, Narciso Czoske, Oliver Donahue, Megan Ettori, Stefano Ford, Holland Fritz, Alexander Kelson, Dan Koekemoer, Anton Kuchner, Ulrike Lombardi, Marco Maier, Christian Moustakas, Leonidas A. Munari, Emiliano Presotto, Valentina Scodeggio, Marco Seitz, Stella Tozzi, Paolo Zheng, Wei Ziegler, Bodo TI CLASH-VLT: CONSTRAINTS ON THE DARK MATTER EQUATION OF STATE FROM ACCURATE MEASUREMENTS OF GALAXY CLUSTER MASS PROFILES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmology: theory; dark matter; equation of state; galaxies: clusters: general; galaxies: clusters: individual (1206.2-0847) ID SPECTROSCOPIC SURVEY; MACS J1206.2-0847; LENSING ANALYSIS; HALOS AB A pressureless scenario for the dark matter (DM) fluid is a widely adopted hypothesis, despite the absence of direct observational evidence. According to general relativity, the total mass-energy content of a system shapes the gravitational potential well, but different test particles perceive this potential in different ways depending on their properties. Cluster galaxy velocities, being << c, depend solely on the gravitational potential, whereas photon trajectories reflect the contributions from the gravitational potential plus a relativistic-pressure term that depends on the cluster mass. We exploit this phenomenon to constrain the equation of state (EoS) parameter of the fluid, primarily DM, contained in galaxy clusters. We use complementary information provided by the kinematic and lensing mass profiles of the galaxy cluster MACS 1206.2-0847 at z = 0.44, as obtained in an extensive imaging and spectroscopic campaign within the Cluster Lensing And Supernova survey with Hubble. The unprecedented high quality of our data set and the properties of this cluster are well suited to determine the EoS parameter of the cluster fluid. Since baryons contribute at most 15% to the total mass in clusters and their pressure is negligible, the EoS parameter we derive describes the behavior of the DM fluid. We obtain the most stringent constraint on the DM EoS parameter to date, w = (p(r) + 2p(t))/(3 c(2) rho) = 0.00 +/- 0.15 (stat) +/- 0.08 (syst), averaged over the radial range 0.5Mpc <= r <= r(200), where p(r) and p(t) are the radial and tangential pressure, and rho is the density. We plan to further improve our constraint by applying the same procedure to all clusters from the ongoing Cluster Lensing And Supernova Survey with Hubble-Very Large Telescope program. C1 [Sartoris, Barbara; Borgani, Stefano; Girardi, Marisa; Annunziatella, Marianna; Munari, Emiliano; Presotto, Valentina] Univ Trieste, Dipartimento Fis, Sez Astron, I-34143 Trieste, Italy. [Sartoris, Barbara; Biviano, Andrea; Borgani, Stefano; Girardi, Marisa; Balestra, Italo; Nonino, Mario; Annunziatella, Marianna; Munari, Emiliano; Presotto, Valentina] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy. [Sartoris, Barbara; Borgani, Stefano] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Rosati, Piero] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy. [Umetsu, Keiichi; Czakon, Nicole] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Bartelmann, Matthias] Heidelberg Univ, Zentrum Astron, D-69120 Heidelberg, Germany. [Grillo, Claudio] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Lemze, Doron; Medezinski, Elinor; Ford, Holland; Zheng, Wei] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Zitrin, Adi] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Balestra, Italo; Mercurio, Amata] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Postman, Marc; Bradley, Larry; Coe, Dan; Koekemoer, Anton] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Broadhurst, Tom] Univ Basque Country, Dept Theoret Phys, E-48080 Bilbao, Spain. [Melchior, Peter] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Meneghetti, Massimo; Ettori, Stefano] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Meneghetti, Massimo; Ettori, Stefano] INFN, Sez Bologna, I-40127 Bologna, Italy. [Merten, Julian; Moustakas, Leonidas A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Benitez, Narciso] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Czoske, Oliver; Kuchner, Ulrike; Maier, Christian; Ziegler, Bodo] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Donahue, Megan] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Fritz, Alexander; Scodeggio, Marco] INAF IASF Milano, I-20133 Milan, Italy. [Kelson, Dan] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Lombardi, Marco] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy. [Seitz, Stella] Univ Observ Munich, D-81679 Munich, Germany. [Seitz, Stella] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Tozzi, Paolo] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. RP Sartoris, B (reprint author), Univ Trieste, Dipartimento Fis, Sez Astron, Via Tiepolo 11, I-34143 Trieste, Italy. EM sartoris@oats.inaf.it RI Grillo, Claudio/E-6223-2015; Ettori, Stefano/N-5004-2015; Meneghetti, Massimo/O-8139-2015; OI LOMBARDI, MARCO/0000-0002-3336-4965; Moustakas, Leonidas/0000-0003-3030-2360; Koekemoer, Anton/0000-0002-6610-2048; Benitez, Narciso/0000-0002-0403-7455; Tozzi, Paolo/0000-0003-3096-9966; Grillo, Claudio/0000-0002-5926-7143; Ettori, Stefano/0000-0003-4117-8617; Meneghetti, Massimo/0000-0003-1225-7084; Maier, Christian/0000-0001-6405-2182; Nonino, Mario/0000-0001-6342-9662; Balestra, Italo/0000-0001-9660-894X; Scodeggio, Marco/0000-0002-2282-5850; Borgani, Stefano/0000-0001-6151-6439; Umetsu, Keiichi/0000-0002-7196-4822; Biviano, Andrea/0000-0002-0857-0732 FU PRIN-MIUR09; PD51 INFN grant; PRIN INAF; DFG Cluster of Excellence Origin and Structure of the Universe; NASA through Hubble Fellowship [HST-HF-51334.01-A]; INAF FX We thank the referee, Michael Strauss, for his constructive and thoughtful comments. B. S. thanks Marino Mezzetti and Pierluigi Monaco for useful discussions. This work has been partially supported by the PRIN-MIUR09 "Tracing the Growth of Structures in the Universe," by the PD51 INFN grant and by the PRIN INAF 2010 " Architecture and Tomography of Galaxy Clusters." P. R. acknowledges partial support by the DFG Cluster of Excellence Origin and Structure of the Universe (http://www.universe-cluster.de). Support for A.Z. was provided by NASA through Hubble Fellowship grant HST-HF-51334.01-A awarded by STScI. A.F. acknowledges the support by INAF through PRIN 2008 (VIPERS) and PRIN 2010 (VIPERS) grants. This research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 25 TC 8 Z9 8 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 1 PY 2014 VL 783 IS 1 AR L11 DI 10.1088/2041-8205/783/1/L11 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC4UB UT WOS:000332515500011 ER PT J AU Fiori, E Comellas, A Molini, L Rebora, N Siccardi, F Gochis, DJ Tanelli, S Parodi, A AF Fiori, E. Comellas, A. Molini, L. Rebora, N. Siccardi, F. Gochis, D. J. Tanelli, S. Parodi, A. TI Analysis and hindcast simulations of an extreme rainfall event in the Mediterranean area: The Genoa 2011 case SO ATMOSPHERIC RESEARCH LA English DT Article DE Deep convection; Numerical modeling; Flash flood ID CONVECTIVE ADJUSTMENT SCHEME; FLASH-FLOOD EVENT; EXPLICIT FORECASTS; WRF MODEL; BULK PARAMETERIZATION; PRECIPITATING EVENTS; HEAVY PRECIPITATION; RESOLUTION; WEATHER; SENSITIVITY AB The city of Genoa, which places between the Tyrrhenian Sea and the Apennine mountains (Liguria, Italy) was rocked by severe flash floods on the 4th of November, 2011. Nearly 500 mm of rain, a third of the average annual rainfall, fell in six hours. Six people perished and millions of Euros in damages occurred. The synoptic-scale meteorological system moved across the Atlantic Ocean and into the Mediterranean generating floods that killed 5 people in Southern France, before moving over the Ligurian Sea and Genoa producing the extreme event studied here. Cloud-permitting simulations (1 km) of the finger-like convective system responsible for the torrential event over Genoa have been performed using Advanced Research Weather and Forecasting Model (ARW-WRF, version 3.3). Two different microphysics (WSM6 and Thompson) as well as three different convection closures (explicit, Kain-Fritsch, and Betts-Miller-Janjic) were evaluated to gain a deeper understanding of the physical processes underlying the observed heavy rain event and the model's capability to predict, in hindcast mode, its structure and evolution. The impact of forecast initialization and of model vertical discretization on hindcast results is also examined. Comparison between model hindcasts and observed fields provided by raingauge data, satellite data, and radar data show that this particular event is strongly sensitive to the details of the mesoscale initialization despite being evolved from a relatively large scale weather system. Only meso-gamma details of the event were not well captured by the best setting of the ARW-WRF model and so peak hourly rainfalls were not exceptionally well reproduced. The results also show that specification of microphysical parameters suitable to these events have a positive impact on the prediction of heavy precipitation intensity values. (C) 2013 The Authors. Published by Elsevier B.V. All rights reserved. C1 [Fiori, E.; Comellas, A.; Molini, L.; Rebora, N.; Siccardi, F.; Parodi, A.] CIMA Res Fdn, Savona, Italy. [Tanelli, S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Comellas, A.; Siccardi, F.] Univ Genoa, I-16126 Genoa, Italy. [Gochis, D. J.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. RP Fiori, E (reprint author), CIMA Res Fdn, Savona, Italy. EM elisabetta.flori@cimafoundation.org FU Italian Civil Protection Department; Regione Liguria; National Aeronautics and Space Administration; Precipitation Measurement Mission program; FP7 DRIHM (Distributed Research Infrastructure for Hydro-Meteorology) project [283568]; National Center for Atmospheric Research (NCAR); U.S. National Science Foundation (NSF); NSF [OCI-1234742]; SuperMUC Petascale System of the LRZ Supercomputing Centre, Garching, Germany [pr45de] FX This work is supported by the Italian Civil Protection Department and by the Regione Liguria. We acknowledge Regione Liguria and Regione Piemonte for providing us with the data of the regional meteorological observation networks. We acknowledge the Italian Civil Protection Department for providing us with the Italian Radar Network data. We are very grateful to the meteorologists and the hydrologists of the Meteo-Hydrologic Centre of Liguria Region, as well as to Greg Thompson (NCAR) for many useful discussions. The portion of work carried out by Simone Tanelli was performed at Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration; likewise, support from the Precipitation Measurement Mission program is gratefully acknowledged. Elisabetta Fiori, Nicola Rebora and Antonio Parodi would like to acknowledge the support of the FP7 DRIHM (Distributed Research Infrastructure for Hydro-Meteorology, 2011-2015) project (contract number 283568). David J. Gochis is supported by the National Center for Atmospheric Research (NCAR). NCAR is supported by a cooperative grant from the U.S. National Science Foundation (NSF). Gochis also acknowledges support for this project from NSF Grant OCI-1234742. The numerical simulations were performed on the SuperMUC Petascale System of the LRZ Supercomputing Centre, Garching, Germany. Project-ID: pr45de. NR 51 TC 34 Z9 34 U1 3 U2 23 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0169-8095 EI 1873-2895 J9 ATMOS RES JI Atmos. Res. PD MAR 1 PY 2014 VL 138 BP 13 EP 29 DI 10.1016/j.atmosres.2013.10.007 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AD8GK UT WOS:000333504300002 ER PT J AU Lee, SMC Schneider, SM Feiveson, AH Macias, BR Smith, SM Watenpaugh, DE Hargens, AR AF Lee, Stuart M. C. Schneider, Suzanne M. Feiveson, Alan H. Macias, Brandon R. Smith, Scott M. Watenpaugh, Donald E. Hargens, Alan R. TI WISE-2005: Countermeasures to prevent muscle deconditioning during bed rest in women SO JOURNAL OF APPLIED PHYSIOLOGY LA English DT Article DE muscle strength; muscle endurance; treadmill exercise within LBNP; flywheel exercise; spaceflight; nutrition ID INTERNATIONAL-SPACE-STATION; BODY NEGATIVE-PRESSURE; LONG-DURATION SPACEFLIGHT; INDUCED BONE LOSS; RESISTANCE EXERCISE; PROTEIN-SYNTHESIS; NUTRITION COUNTERMEASURES; INSTRUMENTAL-VARIABLES; GENDER-DIFFERENCES; AEROBIC CAPACITY AB The objectives of this study were to evaluate the efficacy of two separate countermeasures, exercise and protein supplementation, to prevent muscle strength and lean tissue mass losses during 60 days of bed rest (BR) in women and whether countermeasure efficacy was influenced by pre-BR muscular fitness (strength, endurance, tissue mass). Twenty-four women were assigned to an exercise (EX, n = 8), a no-exercise control (CON, n = 8), or a no-exercise protein supplementation group (PROT, n = 8). EX performed supine treadmill exercise within lower body negative pressure 3-4 days/wk and maximal concentric and eccentric supine leg- and calf-press exercises 2-4 days/wk. PROT consumed a diet with elevated protein content compared with CON and EX (1.6 vs. 1.0 g.kg(-1).day(-1)). Knee and calf isokinetic strength and endurance, isotonic leg- press strength, and leg lean mass were measured before and after BR. Post-BR knee extensor strength and endurance, ankle strength, and leg lean mass were significantly greater and leg- press strength tended to be higher in EX than in CON and PROT. Post-BR measures in PROT were not different than those in CON. Exercise countermeasure efficacy was less, and strength, endurance, and leg lean mass losses in CON and PROT were greater, in subjects who were more fit pre-BR. An exercise protocol combining resistive and aerobic exercise training protects against losses in strength, endurance, and leg lean mass in women during BR, while a nutritional countermeasure without exercise was not effective. Exercise countermeasures may require individualization to protect higher levels of strength and endurance. C1 [Lee, Stuart M. C.] Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA. [Schneider, Suzanne M.] Univ New Mexico, Albuquerque, NM 87131 USA. [Feiveson, Alan H.; Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Macias, Brandon R.; Hargens, Alan R.] Sleep Associates Inc, Ft Worth, TX USA. [Watenpaugh, Donald E.] Univ Calif San Diego, San Diego, CA 92103 USA. RP Lee, SMC (reprint author), Wyle Sci Technol & Engn Grp, 1290 Hercules Blvd, Houston, TX 77058 USA. EM stuart.lee-1@nasa.gov OI Hargens, Alan/0000-0002-4722-1375 FU European Space Agency; US National Aeronautics and Space Administration (NASA); Canadian Space Agency; French "Centre National d'Etudes Spatiales"; NASA [NNJ04HF71G] FX The WISE-2005 study was sponsored by the European Space Agency, the US National Aeronautics and Space Administration (NASA), the Canadian Space Agency, and the French "Centre National d'Etudes Spatiales," which was the "Promoteur" of the study according to French law. The study was performed at MEDES, Institute for Space Physiology and Medicine in Toulouse, France. This work was supported by NASA Grant NNJ04HF71G to A.R. Hargens. NR 56 TC 4 Z9 4 U1 1 U2 9 PU AMER PHYSIOLOGICAL SOC PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA SN 8750-7587 EI 1522-1601 J9 J APPL PHYSIOL JI J. Appl. Physiol. PD MAR PY 2014 VL 116 IS 6 BP 654 EP 667 DI 10.1152/japplphysiol.00590.2013 PG 14 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA AD3YX UT WOS:000333183500009 PM 24458754 ER PT J AU Rojdev, K O'Rourke, MJE Hill, C Nutt, S Atwell, W AF Rojdev, Kristina O'Rourke, Mary Jane E. Hill, Charles Nutt, Steven Atwell, William TI Radiation effects on composites for long-duration lunar habitats SO JOURNAL OF COMPOSITE MATERIALS LA English DT Article DE proton radiation; Composite; scission; deep space; lunar habitat; aging ID ELECTRON-BEAM IRRADIATION; MECHANICAL-PROPERTIES; EPOXY-RESINS; NETWORK STRUCTURE; ION IRRADIATION; POLYMERS; DEGRADATION; BEHAVIOR; PES AB Fiber-reinforced composites are of great interest to NASA for deep-space habitation missions due to the specific strength, modulus and potential radiation shielding properties. However, the durability of these materials on long-duration missions has not been evaluated. Few studies have been conducted on the radiation effects of fiber-reinforced composites in space and even fewer have been conducted with high-energy protons, which replicate portions of the deep-space radiation environment. Furthermore, previous studies of carbon fiber-reinforced composites focused on pure epoxy composites, and aerospace composites in use today include toughening agents to increase the toughness of the material. These toughening agents are typically either rubber particles or thermoplastics, known to be susceptible to ionizing radiation, and could affect the overall composite durability when exposed to high-energy protons. Thus, NASA has undertaken a study to understand the long-term radiation effects on one such potential composite for use in deep-space habitats (boron fiber, carbon fiber and semi-toughened epoxy). Samples were irradiated with 200 MeV protons in air to different doses and evaluated via tensile tests, differential scanning calorimetry, Fourier transform infrared spectroscopy and scanning electron microscopy. The results showed evidence of a weakened matrix due to scission effects and interfacial failure as a result of resin debonding from the boron fibers. C1 [Rojdev, Kristina; O'Rourke, Mary Jane E.; Hill, Charles] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Rojdev, Kristina; Nutt, Steven] Univ So Calif, Mork Family Dept Chem Engn & Mat Sci, Los Angeles, CA USA. [Atwell, William] Boeing Co, Seattle, WA USA. RP Rojdev, K (reprint author), NASA, Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. EM kristina.rojdev-1@nasa.gov NR 42 TC 0 Z9 0 U1 3 U2 27 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0021-9983 EI 1530-793X J9 J COMPOS MATER JI J. Compos Mater. PD MAR PY 2014 VL 48 IS 7 BP 861 EP 878 DI 10.1177/0021998313479416 PG 18 WC Materials Science, Composites SC Materials Science GA AC7CV UT WOS:000332685700010 ER PT J AU Daly, AM Drouin, BJ Yu, SS AF Daly, Adam M. Drouin, Brian J. Yu, Shanshan TI Submillimeter measurements of the Criegee intermediate CH2OO, in the gas phase SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE Submillimeter; Criegee intermediate; Gas phase; Electric discharge ID PRIMARY OZONIDE; SPECTRUM; SPECTROSCOPY; TRANSITIONS; OZONOLYSIS; ETHYLENE; STATES; AIR AB High frequency pure rotational transitions of the simplest Criegee intermediate, methylene peroxide (CH2OO), have been measured up to 1 THz. The data provide the most accurate spectroscopic parameters for the ground vibrational state. The molecule was produced in a flow cell with a DC discharge of CH2I2, O-2 and Ar. Doppler limited measurements were made in the frequency ranges 220-320, 580-680 and 970-1080 GHz. A total of 211 transitions were measured and added to four transitions measured in the microwave to obtain a fit up to J(max) = 49 and K-a(max) = 14 of the a-dipole spectrum. (C) 2014 Elsevier Inc. All rights reserved. C1 [Daly, Adam M.; Drouin, Brian J.; Yu, Shanshan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Daly, AM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM adam.m.daly@jpl.nasa.gov RI Yu, Shanshan/D-8733-2016 NR 23 TC 16 Z9 16 U1 1 U2 22 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 MAR PY 2014 VL 297 BP 16 EP 20 DI 10.1016/j.jms.2014.01.002 PG 5 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA AC8WO UT WOS:000332816000004 ER PT J AU Graham, MJ Djorgovski, SG Drake, AJ Mahabal, AA Chang, M Stern, D Donalek, C Glikman, E AF Graham, Matthew J. Djorgovski, S. G. Drake, Andrew J. Mahabal, Ashish A. Chang, Melissa Stern, Daniel Donalek, Ciro Glikman, Eilat TI A novel variability-based method for quasar selection: evidence for a rest-frame similar to 54 d characteristic time-scale SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; techniques: photometric; surveys; quasars: general ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; DAMPED RANDOM-WALK; SURVEY STRIPE 82; OPTICAL VARIABILITY; PHOTOMETRIC VARIABILITY; MIDINFRARED SELECTION; MAGELLANIC-CLOUD; TRANSIENT SURVEY; LIGHT CURVES AB We compare quasar-selection techniques based on their optical variability using data from the Catalina Real-time Transient Survey (CRTS). We introduce a new technique based on Slepian wavelet variance (SWV) that shows comparable or better performance to structure functions and damped random walk models but with fewer assumptions. Combining these methods with Wide-field Infrared Survey Explorer mid-IR colours produces a highly efficient quasar-selection technique which we have validated spectroscopically. The SWV technique also identifies characteristic time-scales in a time series, and we find a characteristic rest-frame time-scale of similar to 54 d, confirmed in the light curves of similar to 18 000 quasars from CRTS, SDSS and MACHO data, and anticorrelated with absolute magnitude. This indicates a transition between a damped random walk and P(f) proportional to f(-1/3) behaviours and is the first strong indication that a damped random walk model may be too simplistic to describe optical quasar variability. C1 [Graham, Matthew J.; Djorgovski, S. G.; Drake, Andrew J.; Mahabal, Ashish A.; Chang, Melissa; Donalek, Ciro] CALTECH, Pasadena, CA 91125 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Glikman, Eilat] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. RP Graham, MJ (reprint author), CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM mjg@caltech.edu FU NSF [AST-0909182, IIS-1118041, AST-1313422, AST-0834235]; W. M. Keck Institute for Space Studies; US Virtual Astronomical Observatory; National Aeronautics and Space Administration; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science FX This work was supported in part by the NSF grants AST-0909182, IIS-1118041 and AST-1313422, by the W. M. Keck Institute for Space Studies, and by the US Virtual Astronomical Observatory, itself supported by the NSF grant AST-0834235.; This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the US Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/. NR 72 TC 25 Z9 25 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2014 VL 439 IS 1 BP 703 EP 718 DI 10.1093/mnras/stt2499 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AD5MR UT WOS:000333297700068 ER PT J AU Cohen, DH Wollman, EE Leutenegger, MA Sundqvist, JO Fullerton, AW Zsargo, J Owocki, SP AF Cohen, David H. Wollman, Emma E. Leutenegger, Maurice A. Sundqvist, Jon O. Fullerton, Alex W. Zsargo, Janos Owocki, Stanley P. TI Measuring mass-loss rates and constraining shock physics using X-ray line profiles of O stars from the Chandra archive SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: early-type; stars: mass-loss; stars: winds, outflows; X-rays: stars ID COLLIDING WIND BINARIES; ZETA-PUPPIS; DRIVEN INSTABILITY; SPECTRAL TYPES; STELLAR WIND; B-STARS; H-ALPHA; EMISSION; HOT; SPECTROSCOPY AB We quantitatively investigate the extent of wind absorption signatures in the X-ray grating spectra of all non-magnetic, effectively single O stars in the Chandra archive via line profile fitting. Under the usual assumption of a spherically symmetric wind with embedded shocks, we confirm previous claims that some objects show little or no wind absorption. However, many other objects do show asymmetric and blueshifted line profiles, indicative of wind absorption. For these stars, we are able to derive wind mass-loss rates from the ensemble of line profiles, and find values lower by an average factor of 3 than those predicted by current theoretical models, and consistent with Ha if clumping factors of f(cl) approximate to 20 are assumed. The same profile fitting indicates an onset radius of X-rays typically at r approximate to 1.5R(*), and terminal velocities for the X-ray emitting wind component that are consistent with that of the bulk wind. We explore the likelihood that the stars in the sample that do not show significant wind absorption signatures in their line profiles have at least some X-ray emission that arises from colliding wind shocks with a close binary companion. The one clear exception is zeta Oph, a weak-wind star that appears to simply have a very low mass-loss rate. We also reanalyse the results from the canonical O supergiant zeta Pup, using a solar-metallicity wind opacity model and find (M) over dot = 1.8 x 10(-6) M-circle dot yr(-1), consistent with recent multiwavelength determinations. C1 [Cohen, David H.; Wollman, Emma E.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [Wollman, Emma E.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [Leutenegger, Maurice A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Leutenegger, Maurice A.] CRESST, Baltimore, MD 21250 USA. [Leutenegger, Maurice A.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Sundqvist, Jon O.; Owocki, Stanley P.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Sundqvist, Jon O.] Univ Munich, Inst Astron & Astrophys, D-81679 Munich, Germany. [Fullerton, Alex W.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Zsargo, Janos] Inst Politecn Nacl, Escuela Super Fis & Matemat, Mexico City 07738, DF, Mexico. RP Cohen, DH (reprint author), Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. EM cohen@hven.astro.swarthmore.edu FU National Aeronautics and Space Administration through the ADAP award [NNX11AD26G]; National Aeronautics and Space Administration through the Chandra award [TM3-14001B, AR2-13001A, TM6-7003X]; Lotte Lazarsfeld Bailyn Summer Research Fellowship from the Provost's Office at Swarthmore College; NASA award [ATP NNX11AC40G]; DFG grant [Pu117/8-1] FX Support for this work was provided by the National Aeronautics and Space Administration through the ADAP award NNX11AD26G and Chandra award numbers TM3-14001B and AR2-13001A to Swarthmore College and award number TM6-7003X to University of Pittsburgh. EEW was supported by a Lotte Lazarsfeld Bailyn Summer Research Fellowship from the Provost's Office at Swarthmore College. JOS and SPO acknowledge support from NASA award ATP NNX11AC40G to the University of Delaware and JOS also acknowledges support from DFG grant Pu117/8-1. Special thanks to Veronique Petit for her careful reading of the manuscript and her numerous helpful suggestions. NR 94 TC 16 Z9 16 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 MAR PY 2014 VL 439 IS 1 BP 908 EP 923 DI 10.1093/mnras/stu008 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AD5MR UT WOS:000333297700081 ER PT J AU Mouroulis, P Van Gorp, B Green, RO Dierssen, H Wilson, DW Eastwood, M Boardman, J Gao, BC Cohen, D Franklin, B Loya, F Lundeen, S Mazer, A McCubbin, I Randall, D Richardson, B Rodriguez, JI Sarture, C Urquiza, E Vargas, R White, V Yee, K AF Mouroulis, Pantazis Van Gorp, Byron Green, Robert O. Dierssen, Heidi Wilson, Daniel W. Eastwood, Michael Boardman, Joseph Gao, Bo-Cai Cohen, David Franklin, Brian Loya, Frank Lundeen, Sarah Mazer, Alan McCubbin, Ian Randall, David Richardson, Brandon Rodriguez, Jose I. Sarture, Charles Urquiza, Eugenio Vargas, Rudolph White, Victor Yee, Karl TI Portable Remote Imaging Spectrometer coastal ocean sensor: design, characteristics, and first flight results SO APPLIED OPTICS LA English DT Article ID HYPERSPECTRAL IMAGER; CALIBRATION; AIRBORNE; SIMULATION; SEAGRASS; AVIRIS; MERIS AB The design, characteristics, and first test flight results are described of the Portable Remote Imaging Spectrometer, an airborne sensor specifically designed to address the challenges of coastal ocean remote sensing. The sensor incorporates several technologies that are demonstrated for the first time, to the best of our knowledge, in a working system in order to achieve a high performance level in terms of uniformity, signal-to-noise ratio, low polarization sensitivity, low stray light, and high spatial resolution. The instrument covers the 350-1050 nm spectral range with a 2.83 nm sampling per pixel, and a 0.88 mrad instantaneous field of view, with 608 cross-track pixels in a pushbroom configuration. Two additional infrared channels (1240 and 1610 nm) are measured by a spot radiometer housed in the same head. The spectrometer design is based on an optically fast (F/1.8) Dyson design form coupled to a wide angle two-mirror telescope in a configuration that minimizes polarization sensitivity without the use of a depolarizer. A grating with minimum polarization sensitivity and broadband efficiency was fabricated as well as a slit assembly with black (etched) silicon surface to minimize backscatter. First flight results over calibration sites as well as Monterey Bay in California have demonstrated good agreement between in situ and remotely sensed data, confirming the potential value of the sensor to the coastal ocean science community. (c) 2014 Optical Society of America C1 [Mouroulis, Pantazis; Van Gorp, Byron; Green, Robert O.; Wilson, Daniel W.; Eastwood, Michael; Cohen, David; Franklin, Brian; Loya, Frank; Lundeen, Sarah; Mazer, Alan; Randall, David; Richardson, Brandon; Rodriguez, Jose I.; Sarture, Charles; Urquiza, Eugenio; Vargas, Rudolph; White, Victor; Yee, Karl] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Dierssen, Heidi] Univ Connecticut, Dept Marine Sci, Groton, CT 06340 USA. [Boardman, Joseph] Analyt Imaging & Geophys LLC, Boulder, CO 80303 USA. [Gao, Bo-Cai] Naval Res Lab, Washington, DC 20375 USA. [McCubbin, Ian] Desert Res Inst, Reno, NV 89512 USA. RP Mouroulis, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM pantazis.mouroulis@jpl.nasa.gov NR 39 TC 18 Z9 18 U1 3 U2 19 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 MAR 1 PY 2014 VL 53 IS 7 BP 1363 EP 1380 DI 10.1364/AO.53.001363 PG 18 WC Optics SC Optics GA AC1AP UT WOS:000332226900017 PM 24663366 ER PT J AU Wilson, EL McLinden, ML Miller, JH Allan, GR Ott, LE Melroy, HR Clarke, GB AF Wilson, E. L. McLinden, M. L. Miller, J. H. Allan, G. R. Ott, L. E. Melroy, H. R. Clarke, G. B. TI Miniaturized laser heterodyne radiometer for measurements of CO2 in the atmospheric column SO APPLIED PHYSICS B-LASERS AND OPTICS LA English DT Article ID SOURCE INVERSIONS; INSTRUMENT; SPECTROSCOPY; NETWORK; AERONET; FLAME AB We have developed a low-cost, miniaturized laser heterodyne radiometer for highly sensitive measurements of carbon dioxide (CO2) in the atmospheric column. In this passive design, sunlight that has undergone absorption by CO2 in the atmosphere is collected and mixed with continuous wave laser light that is step-scanned across the absorption feature centered at 1,573.6 nm. The resulting radio frequency beat signal is collected as a function of laser wavelength, from which the total column mole fraction can be de-convolved. We are expanding this technique to include methane (CH4) and carbon monoxide (CO), and with minor modifications, this technique can be expanded to include species such as water vapor (H2O) and nitrous oxide (N2O). C1 [Wilson, E. L.; Allan, G. R.; Melroy, H. R.; Clarke, G. B.] NASA, Goddard Space Flight Ctr, Laser Remote Sensing Lab, Greenbelt, MD 20771 USA. [McLinden, M. L.] NASA, Goddard Space Flight Ctr, Microwave Instrument & Technol Branch, Greenbelt, MD 20771 USA. [Miller, J. H.; Melroy, H. R.] George Washington Univ, Dept Chem, Washington, DC 20052 USA. [Allan, G. R.] Sigma Space Corp, Lanham, MD 20706 USA. [Ott, L. E.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Clarke, G. B.] Amer Univ, Washington, DC 20016 USA. RP Wilson, EL (reprint author), NASA, Goddard Space Flight Ctr, Laser Remote Sensing Lab, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM Emily.L.Wilson@nasa.gov RI Ott, Lesley/E-2250-2012 FU NASA Goddard Space Flight Center's Internal Research and Development (IRAD); Science Innovation Fund (SIF) FX We would like to thank the NASA Goddard Space Flight Center's Internal Research and Development (IRAD) and Science Innovation Fund (SIF) programs for funding this effort. We would also like to thank Brent Holben and the entire AERONET team for their ongoing collaboration and support. NR 37 TC 7 Z9 7 U1 2 U2 16 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0946-2171 EI 1432-0649 J9 APPL PHYS B-LASERS O JI Appl. Phys. B-Lasers Opt. PD MAR PY 2014 VL 114 IS 3 BP 385 EP 393 DI 10.1007/s00340-013-5531-1 PG 9 WC Optics; Physics, Applied SC Optics; Physics GA AC9JW UT WOS:000332851700013 ER PT J AU Cure, D Weller, TM Price, T Miranda, FA Van Keuls, FW AF Cure, David Weller, Thomas M. Price, Tony Miranda, Felix A. Van Keuls, Frederick W. TI Low-Profile Tunable Dipole Antenna Using Barium Strontium Titanate Varactors SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION LA English DT Article DE Benzocyclobutene; BST; capacitors; ferroelectric; frequency-selective surfaces (FSS); low-profile antenna; varactor-tuned high impedance surfaces (HIS); varactors ID DESIGN AB In this paper, a 2.4 GHz low-profile dipole antenna that uses a frequency-selective surface (FSS) with interdigital barium strontium titanate (BST) varactor-tuned unit cells is presented. The tunable unit cell is a square patch with a small aperture on either side to accommodate the BST devices. The Ba0.6Sr0.4TiO3 varactors were fabricated on alumina substrates and demonstrate capacitance tuning of 1.5:1 (33%) at 90 V. The varactor chips were placed only along one dimension of the FSS to avoid the use of vias and simplify the dc-bias network. The measured data of the antenna demonstrate tunability from 2.23 to 2.55 GHz with a peak gain at broadside that ranges from 3 to 3.7 dBi, and instantaneous bandwidths of 50 to 160 MHz within the tuning range. The total antenna thickness is approximately lambda/47. C1 [Cure, David] Kymeta Corp, Redmond, WA 98052 USA. [Weller, Thomas M.] Univ S Florida, Tampa, FL 33620 USA. [Price, Tony] Intel Corp, Chandler, AZ 85226 USA. [Miranda, Felix A.] NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA. [Van Keuls, Frederick W.] NASA, John H Glenn Res Ctr, Vantage Partners LLC, Cleveland, OH 44135 USA. RP Cure, D (reprint author), Kymeta Corp, Redmond, WA 98052 USA. EM dcure@kymetacorp.com; weller@usf.edu; tony.price@intel.com; felix.a.miranda@nasa.gov; frederick.w.vankeuls@nasa.gov FU NASA Glenn Research Center's Graduate Student Researcher Program [NNX10AL41H]; NACME Alfred P. Sloan Fellowship; National Science Foundation [ECS-0901779] FX This work was supported by NASA Glenn Research Center's Graduate Student Researcher Program (Grant #NNX10AL41H), the NACME Alfred P. Sloan Fellowship and the National Science Foundation (Grant #ECS-0901779). NR 32 TC 2 Z9 2 U1 9 U2 34 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-926X EI 1558-2221 J9 IEEE T ANTENN PROPAG JI IEEE Trans. Antennas Propag. PD MAR PY 2014 VL 62 IS 3 BP 1185 EP 1193 DI 10.1109/TAP.2013.2294191 PG 9 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA AC7SH UT WOS:000332731700019 ER PT J AU Guraliuc, AR Zhadobov, M Valerio, G Chahat, N Sauleau, R AF Guraliuc, Anda R. Zhadobov, Maxim Valerio, Guido Chahat, Nacer Sauleau, Ronan TI Effect of Textile on the Propagation Along the Body at 60 GHz SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION LA English DT Article DE Body-centric communications; millimeter waves; on-body propagation; path gain; textile ID ANTENNAS; MEDIA AB The effect of textiles on propagation along the body at 60 GHz is studied. A Green's function representation is used to investigate analytically the field excited by an infinitesimal dipole over a multilayer structure representing a flat skin model and clothing. The propagation between two rectangular open-ended waveguides is studied numerically and analytically in terms of path gain. Furthermore, the effect of an air gap between the textile and phantom is considered. Results show that the presence of a textile over a skin-equivalent phantom, as well as an air gap between them, induces a typical decrease of the path gain by 2-5 dB, but it doesn't significantly affect the path gain exponent. In all considered scenarios the power decay exponent is around 3.6. C1 [Guraliuc, Anda R.; Zhadobov, Maxim; Valerio, Guido; Chahat, Nacer; Sauleau, Ronan] Univ Rennes 1, CNRS, UMR 6164, IETR, F-35042 Rennes, France. [Chahat, Nacer] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Guraliuc, AR (reprint author), Univ Rennes 1, CNRS, UMR 6164, IETR, F-35042 Rennes, France. EM anda.guraliuc@univ-rennes1.fr FU Labex CominLabs (French National Research Agency program "Investing for the Future") [ANR-10-LABX-07-01]; Brittany Region under ResCor/BoWi project; National Center for Scientific Research (CNRS), France FX This work was supported by Labex CominLabs (French National Research Agency program "Investing for the Future" ANR-10-LABX-07-01), by Brittany Region under ResCor/BoWi project, and by National Center for Scientific Research (CNRS), France. NR 32 TC 11 Z9 11 U1 1 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-926X EI 1558-2221 J9 IEEE T ANTENN PROPAG JI IEEE Trans. Antennas Propag. PD MAR PY 2014 VL 62 IS 3 BP 1489 EP 1494 DI 10.1109/TAP.2013.2295425 PG 6 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA AC7SH UT WOS:000332731700056 ER PT J AU Mehdi, I Baryshev, AM AF Mehdi, Imran Baryshev, Andrey M. TI Introduction to the Special Mini-Issue on the 24th International Symposium on Space Terahertz Technology (ISSTT) SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Editorial Material C1 [Mehdi, Imran] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Baryshev, Andrey M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. RP Mehdi, I (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD MAR PY 2014 VL 4 IS 2 SI SI BP 147 EP 148 DI 10.1109/TTHZ.2014.2305158 PG 2 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA AD0VB UT WOS:000332951100004 ER PT J AU Kooi, JW Chamberlin, RA Monje, RR Kovacs, A Rice, F Yoshida, H Force, B Cooper, K Miller, D Gould, M Lis, D Bumble, B LeDuc, R Stern, JA Phillips, TG AF Kooi, Jacob W. Chamberlin, Richard A. Monje, Raquel R. Kovacs, Attila Rice, Frank Yoshida, Hiroshige Force, Brian Cooper, Kevin Miller, David Gould, Marty Lis, Dariusz Bumble, Bruce LeDuc, R. Stern, Jeffrey A. Phillips, Tom G. TI Performance of the Caltech Submillimeter Observatory Dual-Color 180-720 GHz Balanced SIS Receivers SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Article DE Superconducting-insulating-superconducting (SIS) mixer; balanced mixers; amplitude noise rejection; Wilkinson in phase power combiner; AlN tunnel barrier; heterodyne receiver; high-current-density; multiple Andreev reflection (MAR); broadband waveguide transition; system stability; Allan variance; synthesized local oscillator (LO); quantum noise limit ID HETERODYNE INSTRUMENTATION UPGRADE; NB/ALOX/NB TUNNEL-JUNCTIONS; WAVE-GUIDE RECEIVER; SHOT-NOISE; DESIGN; MIXERS; STABILITY AB In this paper, we report on balanced SIS receivers covering the astronomical important 180-720 GHz submillimeter atmospheric window. To facilitate remote observations and automated spectral line surveys, fully synthesized local oscillators are employed. High-current-density Nb-AlN-Nb superconducting-insulating-superconducting (SIS) tunnel junctions are used as the mixing element. The measured double-sideband (DSB) 230 GHz receiver noise temperature, uncorrected for optics loss, ranges from 50 K at 185 GHz, 33 K at 246 GHz, to 51 K at 280 GHz. In this frequency range the mixer has a DSB conversion gain of 0 +/- 1.5 dB. The measured 460 GHz double-sideband receiver noise temperature, uncorrected for optics loss, is 32 K at 400 GHz, 34 K at 460 GHz, and 61 K at 520 GHz. Similar to the 230 GHz balanced mixer, the DSB mixer conversion gain 1 +/- 1 is dB. To help optimize performance, the mixer IF circuits and bias injection are entirely planar by design. Dual-frequency observation, by means of separating the incoming circular polarized electric field into two orthogonal components, is another important mode of operation offered by the new facility instrumentation. Instrumental stability is excellent supporting the LO noise cancellation properties of the balanced mixer configuration. In the spring of 2012 the dual-frequency 230/460 SIS receiver was successfully installed at Caltech Submillimeter Observatory (CSO), Mauna Kea, HI, USA. C1 [Kooi, Jacob W.; Chamberlin, Richard A.; Monje, Raquel R.; Kovacs, Attila; Rice, Frank; Yoshida, Hiroshige; Force, Brian; Cooper, Kevin; Miller, David; Lis, Dariusz; Phillips, Tom G.] CALTECH, Submillimeter Astron & Instrumentat Grp, Pasadena, CA 91125 USA. [Bumble, Bruce; LeDuc, R.; Stern, Jeffrey A.] JPL, Pasadena, CA 91109 USA. [Gould, Marty] Zen Machine & Sci Instruments, Lyons, CO 80540 USA. RP Kooi, JW (reprint author), CALTECH, Submillimeter Astron & Instrumentat Grp, Pasadena, CA 91125 USA. EM kooi@caltech.edu RI Kovacs, Attila/C-1171-2010 OI Kovacs, Attila/0000-0001-8991-9088 FU National Science Foundation (NSF) [AST-0838261] FX This work is supported in part by National Science Foundation (NSF)under Grant AST-0838261. NR 53 TC 2 Z9 3 U1 1 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD MAR PY 2014 VL 4 IS 2 SI SI BP 149 EP 164 DI 10.1109/TTHZ.2013.2293117 PG 16 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA AD0VB UT WOS:000332951100005 ER PT J AU Blazquez, B Cooper, KB Llombart, N AF Blazquez, Beatriz Cooper, Ken B. Llombart, Nuria TI Time-Delay Multiplexing With Linear Arrays of THz Radar Transceivers SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Article DE Multiplexing; quasi-optics; terahertz imaging ID IMAGING RADAR; SYSTEM; IMAGER AB The acquisition time of a terahertz imaging radar system with a single transceiver can be halved by using time-delay multiplexing of its beam. This is achieved by splitting a transmitted beam into two beams pointing towards different positions in the target plane. For near-video imaging frame rates, arrays of transceivers would be needed. Both techniques, time-delay multiplexing and the use of transceiver arrays, can be combined to achieve the fastest possible imaging speeds. In this contribution, the feasibility of using the multiplexing technique applied to linear arrays of transceivers is studied. A completely optical multiplexing system, that can work for relatively large arrays, is presented. The technique is demonstrated with measurements in a two-element array. C1 [Blazquez, Beatriz; Llombart, Nuria] Delft Univ Technol, Elect Engn Math & Comp Sci Fac, THz Sensing Grp, NL-2628 CD Delft, Netherlands. [Cooper, Ken B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Blazquez, B (reprint author), Delft Univ Technol, Elect Engn Math & Comp Sci Fac, THz Sensing Grp, NL-2628 CD Delft, Netherlands. EM B.Blazquez-Valles@tudelft.nl; Ken.B.Cooper@jpl.nasa.gov; n.llombartjuan@tudelft.nl FU National Aeronautics and Space Administration FX This work was supported in part under a contract with the National Aeronautics and Space Administration and carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA. NR 12 TC 2 Z9 2 U1 1 U2 13 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD MAR PY 2014 VL 4 IS 2 SI SI BP 232 EP 239 DI 10.1109/TTHZ.2013.2296146 PG 8 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA AD0VB UT WOS:000332951100014 ER PT J AU Hanna, E Fettweis, X Mernild, SH Cappelen, J Ribergaard, MH Shuman, CA Steffen, K Wood, L Mote, TL AF Hanna, Edward Fettweis, Xavier Mernild, Sebastian H. Cappelen, John Ribergaard, Mads H. Shuman, Christopher A. Steffen, Konrad Wood, Len Mote, Thomas L. TI Atmospheric and oceanic climate forcing of the exceptional Greenland ice sheet surface melt in summer 2012 SO INTERNATIONAL JOURNAL OF CLIMATOLOGY LA English DT Article DE climate change; global warming; Greenland; surface melt extent; temperature ID MODEL MAR; RUNOFF; SYSTEM; EXTENT AB The NASA announcement of record surface melting of the Greenland ice sheet in July 2012 led us to examine the atmospheric and oceanic climatic anomalies that are likely to have contributed to these exceptional conditions and also to ask the question of how unusual these anomalies were compared to available records. Our analysis allows us to assess the relative contributions of these two key influences to both the extreme melt event and ongoing climate change. In 2012, as in recent warm summers since 2007, a blocking high pressure feature, associated with negative NAO conditions, was present in the mid-troposphere over Greenland for much of the summer. This circulation pattern advected relatively warm southerly winds over the western flank of the ice sheet, forming a heat dome' over Greenland that led to the widespread surface melting. Both sea-surface temperature and sea-ice cover anomalies seem to have played a minimal role in this record melt, relative to atmospheric circulation. Two representative coastal climatological station averages and several individual stations in south, west and north-west Greenland set new surface air temperature records for May, June, July and the whole (JJA) summer. The unusually warm summer 2012 conditions extended to the top of the ice sheet at Summit, where our reanalysed (1994-2012) DMI Summit weather station summer (JJA) temperature series set new record high mean and extreme temperatures in 2012; 3-hourly instantaneous 2-m temperatures reached an exceptional value of 2.2 degrees C at Summit on 11 July 2012. These conditions translated into the record observed ice-sheet wide melt during summer 2012. However, 2012 seems not to be climatically representative of future average' summers projected this century. C1 [Hanna, Edward] Univ Sheffield, Dept Geog, Sheffield S10 2TN, S Yorkshire, England. [Fettweis, Xavier] Univ Liege, Dept Geog, Climatol Lab, Liege, Belgium. [Mernild, Sebastian H.] Los Alamos Natl Lab, Climate Ocean & Sea Ice Modelling Grp, Los Alamos, NM USA. [Mernild, Sebastian H.] Ctr Estudios Cient, Ctr Sci Studies, Glaciol & Climate Change Lab, Valdivia, Chile. [Cappelen, John] Danish Meteorol Inst, Copenhagen, Denmark. [Ribergaard, Mads H.] Danish Meteorol Inst, Ctr Ocean & Ice, Copenhagen, Denmark. [Shuman, Christopher A.] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21201 USA. [Shuman, Christopher A.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Steffen, Konrad] WSL, Swiss Fed Res Inst, Birmensdorf, Switzerland. [Steffen, Konrad] Swiss Fed Inst Technol, Inst Atmosphere & Climate, Zurich, Switzerland. [Steffen, Konrad] Ecole Polytech Fed Lausanne, Lausanne, Switzerland. [Wood, Len] Univ Plymouth, Sch Marine Sci & Engn, Plymouth PL4 8AA, Devon, England. [Mote, Thomas L.] Univ Georgia, Dept Geog, Athens, GA 30602 USA. RP Hanna, E (reprint author), Univ Sheffield, Dept Geog, Sheffield S10 2TN, S Yorkshire, England. EM ehanna@sheffield.ac.uk RI Steffen, Konrad/C-6027-2013; Hanna, Edward/H-2219-2016; OI Steffen, Konrad/0000-0001-8658-1026; Hanna, Edward/0000-0002-8683-182X; Fettweis, Xavier/0000-0002-4140-3813; Mote, Thomas/0000-0002-0021-0134 FU NASA MEaSUREs program; Climate Change Prediction Program; Scientific Discovery for Advanced Computing (SciDAC) program within the U.S. Department of Energy Office of Science, Los Alamos National Laboratory (LANL) Director's Fellowship; LANL Institute for Geophysics and Planetary Physics; NASA's Cryospheric Program; Danish Agency for Science, Technology and Innovation FX NASA MEaSUREs program supported the passive microwave surface melt product produced at the University of Georgia. The SnowModel work was supported by the Climate Change Prediction Program and Scientific Discovery for Advanced Computing (SciDAC) program within the U.S. Department of Energy Office of Science, Los Alamos National Laboratory (LANL) Director's Fellowship, and LANL Institute for Geophysics and Planetary Physics. Thanks to the Program for Monitoring of the Greenland Ice Sheet (PROMICE), Geological Survey of Denmark and Greenland, the Danish Meteorological Institute, the University of Utrecht, and the Greenland Climate Network (GC-Net) and the University of Colorado at Boulder for providing meteorological station observations. The GC-Net has been supported by NASA's Cryospheric Program with additional logistic support by the US-NSF Office of Polar Program. NOAA near-surface air temperature data are courtesy of Thomas Mefford (NOAA Earth System Research Laboratory Boulder, Colorado and Cooperative Institute for Research in Environmental Sciences, University of Colorado at Boulder) with additional processing by CAS and Michael J. Schnaubelt (University of Maryland, Baltimore County, Joint Center for Earth Systems Technology and Department of Physics, Baltimore, Maryland). The study received financial support from the Danish Agency for Science, Technology and Innovation and is a part of the Greenland Climate Research Centre. NCEP/NCAR Reanalysis data (Kalnay et al., 1996) plots were produced using the NOAA/ESRL Physical Sciences Division, Boulder Colorado website at . NAO Index data (Hurrell et al., 2012) were provided by the Climate Analysis Section, NCAR, Boulder, USA. SST data were provided by NOAA/ESRL and NCEP. EH thanks Grant Bigg and Tom Cropper for useful comments, and Paul Coles for help with drawing figures. NR 46 TC 49 Z9 50 U1 3 U2 49 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0899-8418 EI 1097-0088 J9 INT J CLIMATOL JI Int. J. Climatol. PD MAR PY 2014 VL 34 IS 4 BP 1022 EP 1037 DI 10.1002/joc.3743 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AC9DG UT WOS:000332833900007 ER PT J AU Sanghavi, S AF Sanghavi, Suniti TI Revisiting the Fourier expansion of Mie scattering matrices in generalized spherical functions SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Fourier expansion; Generalized spherical functions; Phase matrix; Wigner 3-j symbols; Aerosol; Cloud ID VECTOR RADIATIVE-TRANSFER; POLARIZED-LIGHT; MULTIPLE-SCATTERING; PHASE MATRIX; LINEARIZATION; RETRIEVAL; PARTICLES; MODEL AB Mie computations of the scattering properties of large particles are a time consuming step in the radiative transfer modeling of aerosol and clouds. Currently, there exist two methods based on the use of spherical functions for computing the Fourier moments of the phase matrix of a given spherical particle or particulate polydispersion: The first, developed over the years before being presented in a convenient form by Siewert [31], required an intermediate computation of the phase matrix over which numerical integration was performed to deliver the required Fourier components. The second, suggested by Domke [9], promised a direct computation of the Fourier moments using Wigner 3-j symbols. While the former was relatively easy to implement and is thus the most commonly used to date, its numerical implementation using an arbitrary user choice of angular quadrature (NAI-1) can produce inaccurate results. Numerical integration using quadrature points as recommended by de Rooij and van der Stap [5] (NAI-2) delivers accurate results with high computational efficiency. Domke's method enables a direct computation of the exact number of required Fourier components. However, the original manuscript contained several misprints, many of which were subsequently corrected by de Rooij and van der Stap [5]. Unfortunately, the main recurrence relationship used in Domke [9] remained uncorrected. In this paper, the corrected relationship is presented along with other minor corrections. de Rooij and van der Stap [5] had found the straightforward application of Domke's method viable only for size parameters smaller than similar to 120 due to issues involving computer storage. A means of implementing the corrected Domke formalism using precomputed tabulations of Wigner 3-j symbols (PCW) is presented here, making it more computationally economical and applicable over much broader particle size ranges. The accuracy of PCW is only limited by machine precision. For a single particle, NAI-2 is found to be faster than PCW for size parameters greater than about 228, whereas for polydispersions over a finite range of particle sizes, PCW is found to be at least 6-8 times faster for size parameters ranging from similar to 0 to beyond 900. PCW thus allows for significant reduction of the computational burden associated with Mie calculations for polydispersions. Published by Elsevier Ltd. C1 [Sanghavi, Suniti] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sanghavi, Suniti] Colorado State Univ, Ft Collins, CO 80523 USA. RP Sanghavi, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Suniti.V.Sanghavi@jpl.nasa.gov OI Sanghavi, Suniti/0000-0003-0754-9154 FU NASA Aerosol-Cloud-Ecosystem (ACE) mission project; NASA FX This work has been supported by the NASA Aerosol-Cloud-Ecosystem (ACE) mission project. This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. All rights reserved. NR 39 TC 4 Z9 4 U1 0 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD MAR PY 2014 VL 136 BP 16 EP 27 DI 10.1016/j.jqsrt.2013.12.015 PG 12 WC Optics; Spectroscopy SC Optics; Spectroscopy GA AC8VX UT WOS:000332814300002 ER PT J AU Lehnert, H Stone, RP Drumm, D AF Lehnert, Helmut Stone, Robert P. Drumm, David TI Geodia starki sp nov ( Porifera, Demospongiae, Astrophorida) from the Aleutian Islands, Alaska, USA SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article DE new species; Porifera; Demospongiae; Astrophorida; Geodia; Aleutian Islands; North Pacific; Alaska AB A new species of Geodia is described from the North Pacific, collected in the summer of 2012 in the western Aleutian Islands. Geodia starki sp. nov. differs from all known species of Geodia by the possession of two categories of sterrasters and exceptionally large megascleres. The new species is compared with congeners of the North Pacific Ocean, Bering Sea, Arctic and the North Atlantic Oceans. C1 [Stone, Robert P.] NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK 99801 USA. [Drumm, David] NOAA, Resource Assessment & Conservat Engn Div, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Seattle, WA 98115 USA. RP Lehnert, H (reprint author), Eichenstr 14, D-86507 Oberottmarshausen, Germany. EM Lehnert@spongetaxonomics.de FU North Pacific Research Board [1016]; Joint Institute for the Study of Atmosphere and Ocean, University of Washington, Seattle; Alaska Fisheries Science Center of NOAA/NMFS FX David Drumm was supported by the North Pacific Research Board (Grant number 1016) and the Joint Institute for the Study of Atmosphere and Ocean, University of Washington, Seattle. Helmut Lehnert was supported by a contract from the Alaska Fisheries Science Center of NOAA/NMFS. NR 30 TC 1 Z9 1 U1 0 U2 1 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0025-3154 EI 1469-7769 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD MAR PY 2014 VL 94 IS 2 BP 261 EP 265 DI 10.1017/S002531541300101X PG 5 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AC8JR UT WOS:000332779800005 ER PT J AU Krebs, JE Vaishampayan, P Probst, AJ Tom, LM Marteinsson, VT Andersen, GL Venkateswaran, K AF Krebs, Jordan E. Vaishampayan, Parag Probst, Alexander J. Tom, Lauren M. Marteinsson, Viggo Thor Andersen, Gary L. Venkateswaran, Kasthuri TI Microbial Community Structures of Novel Icelandic Hot Spring Systems Revealed by PhyloChip G3 Analysis SO ASTROBIOLOGY LA English DT Article ID 16S RIBOSOMAL-RNA; YELLOWSTONE-NATIONAL-PARK; AMMONIA OXIDIZING ARCHAEON; SULFOLOBUS-ACIDOCALDARIUS; BACTERIAL DIVERSITY; GEOTHERMAL AREAS; ELEMENTAL SULFUR; SP-NOV; TEMPERATURE; LIFE AB Microbial community profiles of recently formed hot spring systems ranging in temperatures from 57 degrees C to 100 degrees C and pH values from 2 to 4 in Hverageroi (Iceland) were analyzed with PhyloChip G3 technology. In total, 1173 bacterial operational taxonomic units (OTUs) spanning 576 subfamilies and 38 archaeal OTUs covering 32 subfamilies were observed. As expected, the hyperthermophilic (similar to 100 degrees C) spring system exhibited both low microbial biomass and diversity when compared to thermophilic (similar to 60 degrees C) springs. Ordination analysis revealed distinct bacterial and archaeal diversity in geographically distinct hot springs. Slight variations in temperature (from 57 degrees C to 64 degrees C) within the interconnected pools led to a marked fluctuation in microbial abundance and diversity. Correlation and PERMANOVA tests provided evidence that temperature was the key environmental factor responsible for microbial community dynamics, while pH, H2S, and SO2 influenced the abundance of specific microbial groups. When archaeal community composition was analyzed, the majority of detected OTUs correlated negatively with temperature, and few correlated positively with pH. Key Words: Microbial diversity-PhyloChip G3-Acidophilic-Thermophilic-Hot springs-Iceland. Astrobiology 14, 229-240. C1 [Krebs, Jordan E.; Vaishampayan, Parag; Venkateswaran, Kasthuri] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA. [Probst, Alexander J.] Univ Regensburg, Inst Microbiol, D-93053 Regensburg, Germany. [Probst, Alexander J.] Univ Regensburg, Archaea Ctr, D-93053 Regensburg, Germany. [Tom, Lauren M.; Andersen, Gary L.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Dept Ecol, Div Earth Sci, Berkeley, CA 94720 USA. [Marteinsson, Viggo Thor] Matis Ohf Food Safety Environm & Genet, Reykjavik, Iceland. RP Vaishampayan, P (reprint author), CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, M-S 89-108,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM vaishamp@jpl.nasa.gov RI Tom, Lauren/E-9739-2015; Andersen, Gary/G-2792-2015; Probst, Alexander/K-2813-2016 OI Andersen, Gary/0000-0002-1618-9827; FU National Aeronautics and Space Administration; German National Academic Foundation (Studienstiftung des deutschen Volkes); Caltech Amgen Scholars Fellowship; European Commission FX Part of the research described in this study was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. A. Probst's contribution was supported by the German National Academic Foundation (Studienstiftung des deutschen Volkes). J. Krebs's participation was funded by a Caltech Amgen Scholars Fellowship awarded in 2011. The authors are grateful to the Co-ordination Action for Research Activities on life in Extreme Environments (CAREX) project funded by the European Commission. A special thanks to N. Walter, European Science Federation, for supporting P. Vaishampayan's travel to Iceland. We are also thankful to all the participants for their assistance in the Icelandic CAREX fieldwork. NR 66 TC 0 Z9 0 U1 0 U2 20 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD MAR 1 PY 2014 VL 14 IS 3 BP 229 EP 240 DI 10.1089/ast.2013.1008 PG 12 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AC6GE UT WOS:000332618700003 PM 24588539 ER PT J AU Barge, LM Kee, TP Doloboff, IJ Hampton, JMP Ismail, M Pourkashanian, M Zeytounian, J Baum, MM Moss, JA Lin, CK Kidd, RD Kanik, I AF Barge, Laura M. Kee, Terence P. Doloboff, Ivria J. Hampton, Joshua M. P. Ismail, Mohammed Pourkashanian, Mohamed Zeytounian, John Baum, Marc M. Moss, John A. Lin, Chung-Kuang Kidd, Richard D. Kanik, Isik TI The Fuel Cell Model of Abiogenesis: A New Approach to Origin-of-Life Simulations SO ASTROBIOLOGY LA English DT Review ID CITY HYDROTHERMAL FIELD; RECENTLY DEVELOPED THEORY; RESPIRATORY COMPLEX I; FIXED CHARGE-DENSITY; PRECIPITATE MEMBRANES; IRON-METEORITES; EARLY EARTH; ELECTRON BIFURCATION; BIPOLAR MEMBRANES; CARBON FIXATION AB In this paper, we discuss how prebiotic geo-electrochemical systems can be modeled as a fuel cell and how laboratory simulations of the origin of life in general can benefit from this systems-led approach. As a specific example, the components of what we have termed the "prebiotic fuel cell" (PFC) that operates at a putative Hadean hydrothermal vent are detailed, and we used electrochemical analysis techniques and proton exchange membrane (PEM) fuel cell components to test the properties of this PFC and other geo-electrochemical systems, the results of which are reported here. The modular nature of fuel cells makes them ideal for creating geo-electrochemical reactors with which to simulate hydrothermal systems on wet rocky planets and characterize the energetic properties of the seafloor/hydrothermal interface. That electrochemical techniques should be applied to simulating the origin of life follows from the recognition of the fuel cell-like properties of prebiotic chemical systems and the earliest metabolisms. Conducting this type of laboratory simulation of the emergence of bioenergetics will not only be informative in the context of the origin of life on Earth but may help in understanding whether life might emerge in similar environments on other worlds. Key Words: Astrobiology-Bioenergetics-Iron sulfides-Origin of life-Prebiotic chemistry. Astrobiology 14, 254-270. C1 [Barge, Laura M.; Doloboff, Ivria J.; Lin, Chung-Kuang; Kidd, Richard D.; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Barge, Laura M.] Blue Marble Space Inst Sci, Seattle, WA USA. [Kee, Terence P.; Hampton, Joshua M. P.] Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England. [Ismail, Mohammed; Pourkashanian, Mohamed] Univ Leeds, Ctr Computat Fluid Dynam, Leeds, W Yorkshire, England. [Zeytounian, John] Univ So Calif, Mol & Computat Biol Program, Los Angeles, CA USA. [Baum, Marc M.; Moss, John A.] Oak Crest Inst Sci, Dept Chem, Pasadena, CA USA. RP Barge, LM (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-601,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM laura.m.barge@jpl.nasa.gov OI Pourkashanian, Mohammed/0000-0002-8399-5351 FU National Aeronautics and Space Administration; NASA Astrobiology Institute (Icy Worlds); University of Leeds; Centre for Computational Fluid Dynamics and Energy Leeds; NAI; NAI through the NASA; NASA FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration with support by the NASA Astrobiology Institute (Icy Worlds) and at the University of Leeds with support from the Centre for Computational Fluid Dynamics and Energy Leeds. We acknowledge useful discussions with members of the NAI-sponsored Thermodynamics Disequilibrium and Evolution Focus Group, and we thank two anonymous referees for their helpful suggestions. J.M.P.H. is a Nuffield Foundation Bursar (2013), and L. M. B. is supported by the NAI through the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. NR 140 TC 12 Z9 12 U1 9 U2 80 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD MAR 1 PY 2014 VL 14 IS 3 BP 254 EP 270 DI 10.1089/ast.2014.1140 PG 17 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AC6GE UT WOS:000332618700005 PM 24621309 ER PT J AU Venter, C Harding, AK AF Venter, C. Harding, A. K. TI High-energy pulsar models: Developments and new questions SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT XMM Newton Conference CY MAY 22-24, 2013 CL Madrid, SPAIN DE gamma rays: stars; magnetic fields; pulsars: general; radiation mechanism: non-thermal ID GAMMA-RAY PULSARS; LARGE-AREA TELESCOPE; ANNULAR GAP MODEL; CRAB PULSAR; MILLISECOND PULSARS; LIGHT CURVES; VELA PULSAR; SLOT GAPS; PARTICLE-ACCELERATION; OUTER MAGNETOSPHERE AB The past few years have seen a major advance in observational knowledge of high-energy (HE) pulsars. The Fermi Large Area Telescope (LAT) and AGILE have increased the number of known -ray pulsars by an order of magnitude, its members being divided roughly equally among millisecond pulsars (MSPs), young radio-loud pulsars, and young radio-quiet pulsars. Many new and diverse emission characteristics are being measured, while radio and X-ray follow-up observations increase the pulsar detection rate and enrich our multiwavelength picture of these extreme sources. The wealth of new data has provided impetus for further development and improvement of existing theoretical pulsar models. Geometric light curve (LC) modelling has uncovered three broad classes into which HE pulsars fall: those where the radio profile leads, is aligned with, or lags the -ray profile. For example, the original MSP and original black widow system are members of the second class, requiring co-located emission regions and thereby breaking with traditional notions of radio emission origin. These models imply narrow accelerator gaps in the outer magnetosphere, indicating copious pair production even in MSP magnetospheres that were previously thought to be pair-starved. The increased quality and variety of the LCs necessitate construction of ever more sophisticated models. We will review progress in global magnetosphere solutions which specify a finite conductivity on field lines above the stellar surface, filling the gap between the standard vacuum and force-free (FF; plasma-filled) models. The possibility of deriving phase-resolved spectra for the brightest pulsars, coupled with the fact that the HE pulsar population is sizable enough to allow sampling of various pulsar geometries, will enable much more stringent testing of future radiation models. Reproduction of the observed phase-resolved behavior of this disparate group will be one of the next frontiers in pulsar science, impacting on our understanding of particle acceleration, emission, and magnetosphere geometry. One may now also study evolutionary trends of the measured or inferred quantities, and probe pulsar visibility and population properties such as radiation beam sizes of different pulsar classes, as well as the distribution of spin-down power, -ray luminosity, conversion efficiency, spectral index, and cutoff energy across the population. Lastly, the recent detection of very-high-energy (VHE) pulsations from the Crab pulsar generated quite a few ideas to explain this emission, leading to an extension of standard models and possibly even a bridge between the physics of pulsars and pulsar wind nebulae (PWNe). ((c) 2014 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim) C1 [Venter, C.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa. [Harding, A. K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Venter, C (reprint author), North West Univ, Ctr Space Res, Potchefstroom Campus,Private Bag X6001, ZA-2520 Potchefstroom, South Africa. EM Christo.Venter@nwu.ac.za RI Venter, Christo/E-6884-2011 OI Venter, Christo/0000-0002-2666-4812 FU South African National Research Foundation; NASA Astrophysics Theory Program; Fermi Guest Investigator Program FX CV is supported by the South African National Research Foundation. AKH acknowledges support from the NASA Astrophysics Theory Program. CV and AKH acknowledge support from the Fermi Guest Investigator Program. NR 76 TC 1 Z9 1 U1 1 U2 5 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD MAR PY 2014 VL 335 IS 3 BP 268 EP 273 DI 10.1002/asna.201312030 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC2MG UT WOS:000332334600009 ER PT J AU An, H Kaspi, VM Archibald, R Bachetti, M Bhalerao, V Bellm, EC Beloborodov, AM Boggs, SE Chakrabarty, D Christensen, FE Craig, WW Dufour, F Forster, K Gotthelf, EV Grefenstette, BW Hailey, CJ Harrison, FA Hascoet, R Kitaguchi, T Kouveliotou, C Madsen, KK Mori, K Pivovaroff, MJ Rana, VR Stern, D Tendulkar, S Tomsick, JA Vogel, JK Zhang, WW AF An, H. Kaspi, V. M. Archibald, R. Bachetti, M. Bhalerao, V. Bellm, E. C. Beloborodov, A. M. Boggs, S. E. Chakrabarty, D. Christensen, F. E. Craig, W. W. Dufour, F. Forster, K. Gotthelf, E. V. Grefenstette, B. W. Hailey, C. J. Harrison, F. A. Hascoet, R. Kitaguchi, T. Kouveliotou, Ch. Madsen, K. K. Mori, K. Pivovaroff, M. J. Rana, V. R. Stern, D. Tendulkar, S. Tomsick, J. A. Vogel, J. K. Zhang, W. W. CA NuSTAR Team TI NuSTAR results and future plans for magnetar and rotation-powered pulsar observations SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT XMM Newton Conference CY MAY 22-24, 2013 CL Madrid, SPAIN DE space vehicles; stars: neutron; telescopes; X-rays: stars ID X-RAY PULSARS; SOFT GAMMA-REPEATERS; NEUTRON-STARS; WHITE-DWARF; 1E 1841-045; AE AQUARII; DISCOVERY; PULSATIONS; EMISSION AB The Nuclear Spectroscopic Telescope Array (NuSTAR) is the first focusing hard X-ray mission in orbit and operates in the 3-79 keV range. NuSTAR's sensitivity is roughly two orders of magnitude better than previous missions in this energy band thanks to its superb angular resolution. Since its launch in 2012 June, NuSTAR has performed excellently and observed many interesting sources including four magnetars, two rotation-powered pulsars and the cataclysmic variable AE Aquarii. NuSTAR also discovered 3.76-s pulsations from the transient source SGR J1745-29 recently found by Swift very close to the Galactic center, clearly identifying the source as a transient magnetar. For magnetar 1E 1841-045, we show that the spectrum is well fit by an absorbed blackbody plus broken power-law model with a hard power-law photon index of approximate to 1.3. This is consistent with previous results by INTEGRAL and RXTE. We also find an interesting double-peaked pulse profile in the 25-35 keV band. For AE Aquarii, we show that the spectrum can be described by a multi-temperature thermal model or a thermal plus non-thermal model; a multi-temperature thermal model without a non-thermal component cannot be ruled out. Furthermore, we do not see a spiky pulse profile in the hard X-ray band, as previously reported based on Suzaku observations. For other magnetars and rotation-powered pulsars observed with NuSTAR, data analysis results will be soon available. ((c) 2014 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim) C1 [An, H.; Kaspi, V. M.; Archibald, R.; Dufour, F.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Bachetti, M.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Bachetti, M.] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France. [Bhalerao, V.; Bellm, E. C.; Forster, K.; Grefenstette, B. W.; Harrison, F. A.; Madsen, K. K.; Rana, V. R.; Tendulkar, S.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Bhalerao, V.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Beloborodov, A. M.; Gotthelf, E. V.; Hailey, C. J.; Hascoet, R.; Mori, K.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Boggs, S. E.; Craig, W. W.; Tomsick, J. A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Chakrabarty, D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, W. W.; Pivovaroff, M. J.; Vogel, J. K.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Kitaguchi, T.] RIKEN, Wako, Saitama 3510198, Japan. [Kouveliotou, Ch.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, ZP12, Huntsville, AL 35812 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP An, H (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. EM hjan@physics.mcgill.ca RI Pivovaroff, Michael/M-7998-2014; Boggs, Steven/E-4170-2015; OI Pivovaroff, Michael/0000-0001-6780-6816; Boggs, Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337; Bhalerao, Varun/0000-0002-6112-7609 FU NASA [NNG08FD60C, NNX10AI72G, NNX13AI34G]; National Aeronautics and Space Administration; NSERC; FQRNT Centre de Recherche Astrophysique du Quebec; R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Research (CIFAR); Canada Research Chairs Program; Lorne Trottier Chair in Astrophysics and Cosmology; U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344] FX This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). V. M. K. acknowledges support from an NSERC Discovery Grant, the FQRNT Centre de Recherche Astrophysique du Quebec, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Research (CIFAR), the Canada Research Chairs Program and the Lorne Trottier Chair in Astrophysics and Cosmology. A. M. B. acknowledges the support by NASA grants NNX10AI72G and NNX13AI34G. 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. NR 29 TC 2 Z9 2 U1 0 U2 5 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD MAR PY 2014 VL 335 IS 3 BP 280 EP 284 DI 10.1002/asna.201312032 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC2MG UT WOS:000332334600011 ER PT J AU Gelfand, JD Slane, PO Temim, T AF Gelfand, J. D. Slane, P. O. Temim, T. TI The properties of the progenitor, neutron star, and pulsar wind in the supernova remnant Kes 75 SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT XMM Newton Conference CY MAY 22-24, 2013 CL Madrid, SPAIN DE ISM: (Kes 75); pulsars: individual (J1846-0258); supernova remnants ID HIGH MAGNETIC-FIELD; SPECTRAL EVOLUTION; PSR J1846-0258; BRAKING INDEX; NEBULAE; YOUNG; SPECTROSCOPY; KESTEVEN-75; OUTBURST; MODEL AB By studying composite supernova remnants (SNRs), remnants which contain a pulsar wind nebula (PWN), it is possible to estimate physical properties of the progenitor explosion, central neutron star, and its pulsar wind that are difficult to measure directly. This is best done by fitting the dynamical and broadband spectral properties of a PWN with an evolutionary model for a PWN inside an SNR. We apply such a model to the composite SNR Kes 75, whose associated pulsar PSR J1846-0258 is thought to have an extremely strong surface magnetic field. If approximate to 3 M of mass was ejected in the supernova, our model suggests a normal or slightly subenergetic supernova in a low density environment. Additionally, for the measured pre-outburst braking index of p = 2.65, our model prefers an age of approximate to 430 years and an initial spin period P-0 approximate to 0.2 s. Lastly, the magnetization of the pulsar wind and energy spectrum of particles injected at the termination shock are similar to those observed from other PWNe powered by less magnetized neutron stars. While further study is needed to verify these results, they are nominally inconsistent with strong neutron star magnetic fields resulting from very fast initial rotation. ((c) 2014 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim) C1 [Gelfand, J. D.] NYU Abu Dhabi, Abu Dhabi, U Arab Emirates. [Gelfand, J. D.] New York Univ, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Slane, P. O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Temim, T.] Goddard Space Flight Ctr, Greenbelt, MD USA. RP Gelfand, JD (reprint author), NYU Abu Dhabi, POB 129188, Abu Dhabi, U Arab Emirates. EM jg168@nyu.edu RI Gelfand, Joseph/F-1110-2015; OI Gelfand, Joseph/0000-0003-4679-1058; Temim, Tea/0000-0001-7380-3144 FU NASA through JPL/Caltech (RSA) [1479542] FX Support for this work was provided by NASA through an award issued by JPL/Caltech (RSA No. 1479542). NR 22 TC 4 Z9 4 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD MAR PY 2014 VL 335 IS 3 BP 318 EP 323 DI 10.1002/asna.201312039 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC2MG UT WOS:000332334600018 ER PT J AU Pernet-Fisher, JF Howarth, GH Liu, Y Barry, PH Carmody, L Valley, JW Bodnar, RJ Spetsius, ZV Taylor, LA AF Pernet-Fisher, John F. Howarth, Geoffrey H. Liu, Yang Barry, Peter H. Carmody, Laura Valley, John W. Bodnar, Robert J. Spetsius, Zdislav V. Taylor, Lawrence A. TI Komsomolskaya diamondiferous eclogites: evidence for oceanic crustal protoliths SO CONTRIBUTIONS TO MINERALOGY AND PETROLOGY LA English DT Article DE SCLM; Eclogites; Siberian craton; Mantle xenolith; TTG complex ID CRATONIC LITHOSPHERIC MANTLE; ARCHEAN SUBDUCTION ZONES; ROBERTS-VICTOR ECLOGITES; SOUTH-AFRICA; UDACHNAYA KIMBERLITE; SIBERIAN-CRATON; TRACE-ELEMENT; CLASSIFICATION SCHEME; PERIDOTITE XENOLITHS; OXYGEN ISOTOPES AB The Komsomolskaya kimberlite is one of numerous (>1,000) kimberlite pipes that host eclogite xenoliths on the Siberian craton. Eclogite xenoliths from the adjacent Udachnaya kimberlite pipe have previously been geochemically well characterized; however, data from surrounding diamond-bearing kimberlite pipes from the center of the craton are relatively sparse. Here, we report major-and trace-element data, as well as oxygen isotope systematics, for mineral separates of diamondiferous eclogite xenoliths from the Komsomolskaya kimberlite, suggesting two distinct subgroups of a metamorphosed, subducted oceanic crustal protolith. Using almandine contents, this suite can be divided into two subgroups: group B1, with a high almandine component (>20 mol%) and group B2, with a low almandine component (<20 mol%). Reconstructed REE profiles for B1 eclogites overlap with typical oceanic basalts and lack distinct Eu anomalies. In addition, elevated oxygen isotope values, which are interpreted to reflect isotopic exchange with seawater at low temperatures (<350 degrees C), are consistent with an upper-oceanic crustal protolith. Reconstructed REE profiles for B2 eclogites are consistent with oceanic gabbros and display distinct Eu anomalies, suggesting a plagioclase-rich cumulate protolith. In contrast to B1, B2 eclogites do not display elevated oxygen isotope values, suggesting an origin deep within the crustal pile, where little-to-no interaction with hydrothermal fluids has occurred. Major-element systematics were reconstructed based on mineral modes; group B1 eclogites have higher MgO wt% and lower SiO2 wt%, with respect to typical oceanic basalts, reflecting a partial melting event during slab subduction. Calculated residues from batch partial melt modeling of a range of Precambrian basalts overlap with group B1 trace-element chemistry. When taken together with the respective partial melt trajectories, these melting events are clearly linked to the formation of Tonalite-Trondhjemite-Granodiorite (TTG) complexes. As a result, we propose that many, if not all, diamondiferous eclogite xenoliths from Komsomolskaya represent mantle 'restites' that preserve chemical signatures of Precambrian oceanic crust. C1 [Pernet-Fisher, John F.; Howarth, Geoffrey H.; Liu, Yang; Barry, Peter H.; Carmody, Laura; Taylor, Lawrence A.] Univ Tennessee, Dept Earth & Planetary Sci, Planetary Geosci Inst, Knoxville, TN 37996 USA. [Liu, Yang] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Valley, John W.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Bodnar, Robert J.] Virginia Polytech & State Univ, Dept Geosci, Blacksburg, VA 24061 USA. [Spetsius, Zdislav V.] ALROSA Co Ltd, Inst Diamond Ind, Mirny, Yakutia, Russia. RP Pernet-Fisher, JF (reprint author), Univ Tennessee, Dept Earth & Planetary Sci, Planetary Geosci Inst, Knoxville, TN 37996 USA. EM jpf@utk.edu RI Valley, John/B-3466-2011; OI Valley, John/0000-0003-3530-2722; Barry, Peter/0000-0002-6960-1555 FU NSF [EAR-1144337, EAR-1144559, EAR-0838058] FX The authors thank Mike Spicuzza, Allan Patchen, and Luca Fedele for their assistance with data collection. This work was funded by NSF Grants EAR-1144337 (LAT), EAR-1144559 (PHB), and EAR-0838058 (JWV). YL is currently supported at Jet Propulsion Laboratory, which is managed by California Institute of Technology, under a contract with NASA. We would like to thank Katie Smart and Ryan Ickert for constructive reviews of an earlier version of this manuscript, in addition to two anonymous reviewers for their comments and suggestions that added significantly to the revision of this manuscript. NR 85 TC 7 Z9 7 U1 0 U2 18 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0010-7999 EI 1432-0967 J9 CONTRIB MINERAL PETR JI Contrib. Mineral. Petrol. PD MAR PY 2014 VL 167 IS 3 AR 981 DI 10.1007/s00410-014-0981-y PG 17 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA AC5UH UT WOS:000332585700004 ER PT J AU Liu, Z Owen, S Moore, A AF Liu, Zhen Owen, Susan Moore, Angelyn TI Rapid Estimate and Modeling of Permanent Coseismic Displacements for Large Earthquakes Using High-Rate Global Positioning System Data SO SEISMOLOGICAL RESEARCH LETTERS LA English DT Article ID TSUNAMI WARNING SYSTEMS; TOHOKU-OKI EARTHQUAKE; 1-HZ GPS DATA; FAULT; CALIFORNIA; ZONE C1 [Liu, Zhen; Owen, Susan; Moore, Angelyn] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Liu, Z (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM zhen.liu@jpl.nasa.gov RI Liu, Zhen/D-8334-2017 FU National Aeronautics and Space Administration; internal Research and Technology Development program; Earth Surface & Interior program FX The Japan Global Positioning System (GPS) time series is provided by the Advanced Rapid Imaging and Analysis (ARIA) team at Jet Propulsion Laboratory (JPL) and Caltech. Precise GPS orbit products used for time series analysis were provided by the JPL GPS Analysis Center. All original GEONET RINEX data were provided to Caltech by the Geospatial Information Authority (GSI) of Japan. The Costa Rica CGPS RINEX data were provided by University of South Florida, UNAVCO, and OVSICORI, a university group in Costa Rica charged with natural hazard research and mitigation. This research was carried out at JPL, California Institute of Technology, under a contract with the National Aeronautics and Space Administration and funded through the internal Research and Technology Development program and Earth Surface & Interior program. NR 28 TC 5 Z9 5 U1 0 U2 5 PU SEISMOLOGICAL SOC AMER PI ALBANY PA 400 EVELYN AVE, SUITE 201, ALBANY, CA 94706-1375 USA SN 0895-0695 J9 SEISMOL RES LETT JI Seismol. Res. Lett. PD MAR-APR PY 2014 VL 85 IS 2 BP 284 EP 294 DI 10.1785/0220130174 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AC8SF UT WOS:000332804400005 ER PT J AU Aasi, J Abadie, J Abbott, BP Abbott, R Abbott, T Abernathy, MR Accadia, T Acernese, F Adams, C Adams, T Adhikari, RX Affeldt, C Agathos, M Aggarwal, N Aguiar, OD Ajith, P Allen, B Allocca, A Ceron, EA Amariutei, D Anderson, RA Anderson, SB Anderson, WG Arai, K Araya, MC Arceneaux, C Areeda, J Ast, S Aston, SM Astone, P Aufmuth, P Aulbert, C Austin, L Aylott, BE Babak, S Baker, PT Ballardin, G Ballmer, SW Barayoga, JC Barker, D Barnum, SH Barone, F Barr, B Barsotti, L Barsuglia, M Barton, MA Bartos, I Bassiri, R Basti, A Batch, J Bauchrowitz, J Bauer, TS Bebronne, M Behnke, B Bejger, M Beker, MG Bell, AS Bell, C Belopolski, I Bergmann, G Berliner, JM Bertolini, A Bessis, D Betzwieser, J Beyersdorf, PT Beyersdorf, PT Bilenko, IA Billingsley, G Birch, J Bitossi, M Bizouard, MA Black, E Blackburn, JK Blackburn, L Blair, D Blom, M Bock, O Bodiya, TP Boer, M Bogan, C Bond, C Bondu, F Bonelli, L Bonnand, R Bork, R Born, M Bose, S Bosi, L Bowers, J Bradaschia, C Brady, PR Braginsky, VB Branchesi, M Brannen, CA Brau, JE Breyer, J Briant, T Bridges, DO Brillet, A Brinkmann, M Brisson, V Britzger, M Brooks, AF Brown, DA Brown, DD Bruckner, F Bulik, T Bulten, HJ Buonanno, A Buskulic, D Buy, C Byer, RL Cadonati, L Cagnoli, G Bustillo, JC Calloni, E Camp, JB Campsie, P Cannon, KC Canuel, B Cao, J Capano, CD Carbognani, F Carbone, L Caride, S Castiglia, A Caudill, S Cavaglia, M Cavalier, F Cavalieri, R Cella, G Cepeda, C Cesarini, E Chakraborty, R Chalermsongsak, T Chao, S Charlton, P Chassande-Mottin, E Chen, X Chen, Y Chincarini, A Chiummo, A Cho, HS Chow, J Christensen, N Chu, Q Chua, SSY Chung, S Ciani, G Clara, F Clark, DE Clark, JA Cleva, F Coccia, E Cohadon, PF Colla, A Colombini, M Constancio, M Conte, A Conte, R Cook, D Corbitt, TR Cordier, M Cornish, N Corsi, A Costa, CA Coughlin, MW Coulon, JP Countryman, S Couvares, P Coward, DM Cowart, M Coyne, DC Craig, K Creighton, JDE Creighton, TD Crowder, SG Cumming, A Cunningham, L Cuoco, E Dahl, K Dal Canton, T Damjanic, M Danilishin, SL D'Antonio, S Danzmann, K Dattilo, V Daudert, B Daveloza, H Davier, M Davies, GS Daw, EJ Day, R Dayanga, T De Rosa, R Debreczeni, G Degallaix, J Del Pozzo, W Deleeuw, E Deleglise, S Denker, T Dereli, H Dergachev, V DeRosa, R DeSalvo, R Dhurandhar, S Di Fiore, L Di Lieto, A Di Palma, I Di Virgilio, A Diaz, M Dietz, A Dmitry, K Donovan, F Dooley, KL Doravari, S Drago, M Drever, RWP Driggers, JC Du, Z Dumas, JC Dwyer, S Eberle, T Edwards, M Effler, A Ehrens, P Eichholz, J Eikenberry, SS Endroczi, G Essick, R Etzel, T Evans, K Evans, M Evans, T Factourovich, M Fafone, V Fairhurst, S Fang, Q Farr, B Farr, W Favata, M Fazi, D Fehrmann, H Feldbaum, D Ferrante, I Ferrini, F Fidecaro, F Finn, LS Fiori, I Fisher, R Flaminio, R Foley, E Foley, S Forsi, E Forte, LA Fotopoulos, N Fournier, JD Franco, S Frasca, S 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Huttner, SH Huynh, M Huynh-Dinh, T Iafrate, J Ingram, DR Inta, R Isogai, T Ivanov, A Iyer, BR Izumi, K Jacobson, M James, E Jang, H Jang, YJ Jaranowski, P Jimenez-Forteza, F Johnson, WW Jones, D Jones, DI Jones, R Jonker, RJG Ju, L Haris, K Kalmus, P Kalogera, V Kandhasamy, S Kang, G Kanner, JB Kasprzack, M Kasturi, R Katsavounidis, E Katzman, W Kaufer, H Kaufman, K Kawabe, K Kawamura, S Kawazoe, F Kefelian, F Keitel, D Kelley, DB Kells, W Keppel, DG Khalaidovski, A Khalili, FY Khazanov, EA Kim, BK Kim, C Kim, K Kim, N Kim, W Kim, YM King, EJ King, PJ Kinzel, DL Kissel, JS Klimenko, S Kline, J Koehlenbeck, S Kokeyama, K Kondrashov, V Koranda, S Korth, WZ Kowalska, I Kozak, D Kremin, A Kringel, V Krishnan, B Krolak, A Kucharczyk, C Kudla, S Kuehn, G Kumar, A Kumar, P Kumar, R Kurdyumov, R Kwee, P Landry, M Lantz, B Larson, S Lasky, PD Lawrie, C Lazzarini, A Le Roux, A Leaci, P Lebigot, EO Lee, CH Lee, HK Lee, HM Lee, J Lee, J Leonardi, M Leong, JR Leroy, N Letendre, N Levine, B Lewis, 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CA LIGO Sci Collaboration Virgo Collaboration TI FIRST SEARCHES FOR OPTICAL COUNTERPARTS TO GRAVITATIONAL-WAVE CANDIDATE EVENTS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE binaries: close; catalogs; gravitational waves; stars: neutron; surveys ID GAMMA-RAY BURSTS; COMPACT OBJECT MERGERS; FOLLOW-UP OBSERVATIONS; NEUTRON-STAR MERGERS; 28 FEBRUARY 1997; ELECTROMAGNETIC COUNTERPARTS; LIGHT CURVES; IMAGE SUBTRACTION; SWIFT-ERA; RADIO OBSERVATIONS AB During the Laser Interferometer Gravitational-wave Observatory and Virgo joint science runs in 2009-2010, gravitational wave (GW) data from three interferometer detectors were analyzed within minutes to select GW candidate events and infer their apparent sky positions. Target coordinates were transmitted to several telescopes for follow-up observations aimed at the detection of an associated optical transient. Images were obtained for eight such GW candidates. We present the methods used to analyze the image data as well as the transient search results. No optical transient was identified with a convincing association with any of these candidates, and none of the GW triggers showed strong evidence for being astrophysical in nature. We compare the sensitivities of these observations to several model light curves from possible sources of interest, and discuss prospects for future joint GW-optical observations of this type. C1 [Aasi, J.; Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M. R.; Adhikari, R. X.; Ajith, P.; Anderson, R. A.; Anderson, S. B.; Arai, K.; Araya, M. C.; Austin, L.; Barayoga, J. C.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cepeda, C.; Chakraborty, R.; Chalermsongsak, T.; Coyne, D. C.; Daudert, B.; Dergachev, V.; Driggers, J. C.; Ehrens, P.; Etzel, T.; Ferrante, I.; Fotopoulos, N.; Gushwa, K. E.; Gustafson, E. K.; Hall, E.; Harms, J.; Heefner, J.; Heptonstall, A. W.; Hodge, K. 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[Poznanski, D.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Schmidt, B.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Sokolowski, M.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Sokolowski, M.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia. [Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Sullivan, M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. RP Aasi, J (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA. RI Travasso, Flavio/J-9595-2016; Bartos, Imre/A-2592-2017; Punturo, Michele/I-3995-2012; Cella, Giancarlo/A-9946-2012; Cesarini, Elisabetta/C-4507-2017; Chow, Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Ciani, Giacomo/G-1036-2011; Siudek, Malgorzata/O-8727-2015; Di Virgilio, Angela Dora Vittoria/E-9078-2015; Sergeev, Alexander/F-3027-2017; Harms, Jan/J-4359-2012; Vicere, Andrea/J-1742-2012; Rocchi, Alessio/O-9499-2015; Martelli, Filippo/P-4041-2015; Branchesi, Marica/P-2296-2015; Gehring, Tobias/A-8596-2016; Strain, Kenneth/D-5236-2011; Miao, Haixing/O-1300-2013; Howell, Eric/H-5072-2014; Heidmann, Antoine/G-4295-2016; Zhu, Xingjiang/E-1501-2016; Frasconi, Franco/K-1068-2016; Pinto, Innocenzo/L-3520-2016; Ferrante, Isidoro/F-1017-2012; M, Manjunath/N-4000-2014; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Leonardi, Matteo/G-9694-2015; Sigg, Daniel/I-4308-2015; Puppo, Paola/J-4250-2012; Tacca, Matteo/J-1599-2015; Graef, Christian/J-3167-2015; Ottaway, David/J-5908-2015; Garufi, Fabio/K-3263-2015; Deleglise, Samuel/B-1599-2015; Neri, Igor/F-1482-2010; Shaddock, Daniel/A-7534-2011; Huerta, Eliu/J-5426-2014; Losurdo, Giovanni/K-1241-2014; Steinlechner, Sebastian/D-5781-2013; Hild, Stefan/A-3864-2010; Danilishin, Stefan/K-7262-2012; Gammaitoni, Luca/B-5375-2009; Iyer, Bala R./E-2894-2012; Canuel, Benjamin/C-7459-2014; Sokolowski, Marcin/B-5584-2013; Malek, Katarzyna/A-1254-2012; Lee, Chang-Hwan/B-3096-2015; Khalili, Farit/D-8113-2012; McClelland, David/E-6765-2010; prodi, giovanni/B-4398-2010; Costa, Cesar/G-7588-2012; Bell, Angus/E-7312-2011; Bilenko, Igor/D-5172-2012; Kumar, Prem/B-6691-2009; Marchesoni, Fabio/A-1920-2008; CONTE, ANDREA/J-6667-2012; Salemi, Francesco/F-6988-2014; Gemme, Gianluca/C-7233-2008; Prokhorov, Leonid/I-2953-2012; Gorodetsky, Michael/C-5938-2008; Strigin, Sergey/I-8337-2012; Mitrofanov, Valery/D-8501-2012; Ward, Robert/I-8032-2014; OI Travasso, Flavio/0000-0002-4653-6156; Punturo, Michele/0000-0001-8722-4485; Cella, Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167; Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Ciani, Giacomo/0000-0003-4258-9338; Siudek, Malgorzata/0000-0002-2949-2155; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Swinkels, Bas/0000-0002-3066-3601; Vicere, Andrea/0000-0003-0624-6231; Rocchi, Alessio/0000-0002-1382-9016; Martelli, Filippo/0000-0003-3761-8616; Gehring, Tobias/0000-0002-4311-2593; Strain, Kenneth/0000-0002-2066-5355; Miao, Haixing/0000-0003-4101-9958; Howell, Eric/0000-0001-7891-2817; Heidmann, Antoine/0000-0002-0784-5175; Zhu, Xingjiang/0000-0001-7049-6468; Frasconi, Franco/0000-0003-4204-6587; Ferrante, Isidoro/0000-0002-0083-7228; M, Manjunath/0000-0001-8710-0730; Vecchio, Alberto/0000-0002-6254-1617; Sigg, Daniel/0000-0003-4606-6526; Puppo, Paola/0000-0003-4677-5015; Tacca, Matteo/0000-0003-1353-0441; Graef, Christian/0000-0002-4535-2603; Garufi, Fabio/0000-0003-1391-6168; Deleglise, Samuel/0000-0002-8680-5170; Neri, Igor/0000-0002-9047-9822; 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Schmidt, Brian/0000-0001-6589-1287; Allen, Bruce/0000-0003-4285-6256; Granata, Massimo/0000-0003-3275-1186; Vitale, Salvatore/0000-0003-2700-0767; Vetrano, Flavio/0000-0002-7523-4296; Denker, Timo/0000-0003-1259-5315; Naticchioni, Luca/0000-0003-2918-0730; calloni, enrico/0000-0003-4819-3297; Scott, Jamie/0000-0001-6701-6515; Sorazu, Borja/0000-0002-6178-3198; Husa, Sascha/0000-0002-0445-1971; Papa, M.Alessandra/0000-0002-1007-5298; Vocca, Helios/0000-0002-1200-3917; Aulbert, Carsten/0000-0002-1481-8319; Pinto, Innocenzo M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200; Guidi, Gianluca/0000-0002-3061-9870; Drago, Marco/0000-0002-3738-2431; Pierro, Vincenzo/0000-0002-6020-5521; Coccia, Eugenio/0000-0002-6669-5787; Ward, Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447; Whelan, John/0000-0001-5710-6576; Vedovato, Gabriele/0000-0001-7226-1320; Fairhurst, Stephen/0000-0001-8480-1961; Matichard, Fabrice/0000-0001-8982-8418 FU United States National Science Foundation for the construction and operation of the LIGO Laboratory; Science and Technology Facilities Council of the United Kingdom; Max-Planck-Society; State of Niedersachsen/Germany; Italian Istituto Nazionale di Fisica Nucleare; French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector; Australian Research Council; International Science Linkages program of the Commonwealth of Australia; Council of Scientific and Industrial Research of India; Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de Economia y Competitividad; Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears; Foundation for Fundamental Research on Matter; Netherlands Organisation for Scientific Research; Polish Ministry of Science and Higher Education; FOCUS Programme of Foundation for Polish Science; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; National Aeronautics and Space Administration; OTKA of Hungary; Lyon Institute of Origins (LIO); National Research Foundation of Korea Industry Canada; Province of Ontario through the Ministry of Economic Development and Innovation; National Science and Engineering Research Council Canada; Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation, FIRB (Italian Ministry of Education, University and Research) [RBFR12PM1F]; Alfred P. Sloan Foundation; UK Science and Technology Facilities Council FX The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector, and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Economia y Competitividad, the Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, OTKA of Hungary, 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 National Science and Engineering Research Council Canada, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, FIRB 2012 Project RBFR12PM1F (Italian Ministry of Education, University and Research), and the Alfred P. Sloan Foundation. This work is based on results partially obtained at the ESO observatory, La Silla. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. This document has been assigned the identifier LIGO-P1200171-v19. NR 109 TC 34 Z9 32 U1 6 U2 93 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAR PY 2014 VL 211 IS 1 AR 7 DI 10.1088/0067-0049/211/1/7 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB9DN UT WOS:000332090200007 ER PT J AU Boersma, C Bauschlicher, CW Ricca, A Mattioda, AL Cami, J Peeters, E de Armas, FS Saborido, GP Hudgins, DM Allamandola, LJ AF Boersma, C. Bauschlicher, C. W., Jr. Ricca, A. Mattioda, A. L. Cami, J. Peeters, E. de Armas, F. Sanchez Saborido, G. Puerta Hudgins, D. M. Allamandola, L. J. TI THE NASA AMES PAH IR SPECTROSCOPIC DATABASE VERSION 2.00: UPDATED CONTENT, WEB SITE, AND ON(OFF)LINE TOOLS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE astrochemistry; ISM: lines and bands; methods: laboratory: molecular; methods: numerical; molecular data; techniques: spectroscopic ID POLYCYCLIC AROMATIC-HYDROCARBONS; THEORETICAL INFRARED-SPECTRA; PERDEUTERATED NAPHTHALENE; CATIONS; EMISSION; MODEL; IONS; IONIZATION; POLYACENES; PENTACENE AB A significantly updated version of the NASA Ames PAH IR Spectroscopic Database, the first major revision since its release in 2010, is presented. The current version, version 2.00, contains 700 computational and 75 experimental spectra compared, respectively, with 583 and 60 in the initial release. The spectra span the 2.5-4000 mu m (4000-2.5 cm(-1)) range. New tools are available on the site that allow one to analyze spectra in the database and compare them with imported astronomical spectra as well as a suite of IDL object classes (a collection of programs utilizing IDL's object-oriented programming capabilities) that permit offline analysis called the AmesPAHdbIDLSuite. Most noteworthy among the additions are the extension of the computational spectroscopic database to include a number of significantly larger polycyclic aromatic hydrocarbons (PAHs), the ability to visualize the molecular atomic motions corresponding to each vibrational mode, and a new tool that allows one to perform a non-negative least-squares fit of an imported astronomical spectrum with PAH spectra in the computational database. Finally, a methodology is described in the Appendix, and implemented using the AmesPAHdbIDLSuite, that allows the user to enforce charge balance during the fitting procedure. C1 [Boersma, C.; Bauschlicher, C. W., Jr.; Ricca, A.; Mattioda, A. L.; Allamandola, L. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ricca, A.; Mattioda, A. L.; Cami, J.; Peeters, E.; de Armas, F. Sanchez; Saborido, G. Puerta] SETI Inst, Mountain View, CA 94043 USA. [Cami, J.; Peeters, E.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Hudgins, D. M.] NASA Headquarters, Washington, DC 20546 USA. RP Boersma, C (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA. EM Christiaan.Boersma@nasa.gov RI Boersma, Christiaan/L-7696-2014 OI Boersma, Christiaan/0000-0002-4836-217X FU NASA's Astrophysics Data Analysis Program; NASA's Astrophysics Theory and Fundamental Physics Program; NASA's Long Term Space Astrophysics Program; NASA's Archival Research Program; NASA's Laboratory Astrophysics, "Carbon in the Galaxy" consortium grant [NNH10ZDA001N]; NASA Astrophysics Data Analysis program [NNX11AG11G]; INTEGRANTS program; Spanish Ministry of Science and Innovation; NASA Astrophysics Data Analysis Program FX An anonymous referee is thanked for carefully reading the manuscript and making very perceptive suggestions, improving the paper. This work was supported through NASA's Astrophysics Data Analysis, Astrophysics Theory and Fundamental Physics, Long Term Space Astrophysics, Laboratory Astrophysics, Astrobiology, The Spitzer Space Telescope Archival Research Programs and NASA's Laboratory Astrophysics, "Carbon in the Galaxy" consortium grant (NNH10ZDA001N). C. B. is grateful for an appointment at NASA's Ames Research Center through San Jose State University Research Foundation (NNX11AJ33A). A. R. thanks the NASA Astrophysics Data Analysis program (NNX11AG11G). Fernando Sanchez de Armas and Gerardo Puerta Saborido acknowledge support from the INTEGRANTS program, sponsored by the Spanish Ministry of Science and Innovation. Gerardo Puerta Saborido thanks additional financial support from the NASA Astrophysics Data Analysis Program. NR 44 TC 47 Z9 47 U1 3 U2 15 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAR PY 2014 VL 211 IS 1 AR 8 DI 10.1088/0067-0049/211/1/8 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB9DN UT WOS:000332090200008 ER PT J AU Gruber, D Goldstein, A von Ahlefeld, VW Bhat, PN Bissaldi, E Briggs, MS Byrne, D Cleveland, WH Connaughton, V Diehl, R Fishman, GJ Fitzpatrick, G Foley, S Gibby, M Giles, MM Greiner, J Guiriec, S van der Horst, AJ von Kienlin, A Kouveliotou, C Layden, E Lin, L Meegan, CA McGlynn, S Paciesas, WS Pelassa, V Preece, RD Rau, A Wilson-Hodge, CA Xiong, SL Younes, G Yu, HF AF Gruber, David Goldstein, Adam von Ahlefeld, Victoria Weller Bhat, P. Narayana Bissaldi, Elisabetta Briggs, Michael S. Byrne, Dave Cleveland, William H. Connaughton, Valerie Diehl, Roland Fishman, Gerald J. Fitzpatrick, Gerard Foley, Suzanne Gibby, Melissa Giles, Misty M. Greiner, Jochen Guiriec, Sylvain van der Horst, Alexander J. von Kienlin, Andreas Kouveliotou, Chryssa Layden, Emily Lin, Lin Meegan, Charles A. McGlynn, Sinead Paciesas, William S. Pelassa, Veronique Preece, Robert D. Rau, Arne Wilson-Hodge, Colleen A. Xiong, Shaolin Younes, George Yu, Hoi-Fung TI THE FERMI GBM GAMMA-RAY BURST SPECTRAL CATALOG: FOUR YEARS OF DATA SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE gamma-ray burst: general; methods: data analysis ID 1ST 2 YEARS; BATSE OBSERVATIONS; COMPONENT; EMISSION; MONITOR; PEAK; EVOLUTION; INDEXES; TIME AB In this catalog we present the updated set of spectral analyses of gamma-ray bursts (GRBs) detected by the Fermi Gamma-Ray Burst Monitor during its first four years of operation. It contains two types of spectra, time-integrated spectral fits and spectral fits at the brightest time bin, from 943 triggered GRBs. Four different spectral models were fitted to the data, resulting in a compendium of more than 7500 spectra. The analysis was performed similarly but not identically to Goldstein et al. All 487 GRBs from the first two years have been re-fitted using the same methodology as that of the 456 GRBs in years three and four. We describe, in detail, our procedure and criteria for the analysis and present the results in the form of parameter distributions both for the observer-frame and rest-frame quantities. The data files containing the complete results are available from the High-Energy Astrophysics Science Archive Research Center. C1 [Gruber, David; von Ahlefeld, Victoria Weller; Diehl, Roland; Greiner, Jochen; von Kienlin, Andreas; Rau, Arne; Yu, Hoi-Fung] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Gruber, David] Planetarium Sudtirol, I-39053 Karneid, Italy. [Goldstein, Adam; Bhat, P. Narayana; Briggs, Michael S.; Connaughton, Valerie; Layden, Emily; Lin, Lin; Meegan, Charles A.; Paciesas, William S.; Pelassa, Veronique; Preece, Robert D.; Xiong, Shaolin] Univ Alabama, Huntsville, AL 35805 USA. [von Ahlefeld, Victoria Weller] Univ Edinburgh, Sch Phys & Astron, Edinburgh EH9 3JZ, Midlothian, Scotland. [Bissaldi, Elisabetta] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy. [Byrne, Dave; Fitzpatrick, Gerard; Foley, Suzanne; McGlynn, Sinead] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cleveland, William H.; Younes, George] Univ Space Res Assoc, Huntsville, AL 35805 USA. [Fishman, Gerald J.; Kouveliotou, Chryssa; Wilson-Hodge, Colleen A.] NASA, George C Marshall Space Flight Ctr, VP62, Space Sci Off, Huntsville, AL 35812 USA. [Gibby, Melissa; Giles, Misty M.] Jacobs Technol Inc, Huntsville, AL USA. [Guiriec, Sylvain] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [van der Horst, Alexander J.] Univ Amsterdam, Inst Astron, NL-1098 XH Amsterdam, Netherlands. [Lin, Lin] Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey. [Bissaldi, Elisabetta] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. RP Gruber, D (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. RI Diehl, Roland/K-4496-2016; Bissaldi, Elisabetta/K-7911-2016 OI Diehl, Roland/0000-0002-8337-9022; Bissaldi, Elisabetta/0000-0001-9935-8106 FU German Bundesministeriums fur Wirtschaft und Technologie (BMWi) via the Deutsches Zentrum fur Luft und Raumfahrt (DLR) [50 QV 0301, 50 OG 0502] FX We thank the reviewer for his/her comments, which significantly contributed to improving the quality of the publication. The GBM project is supported by the German Bundesministeriums fur Wirtschaft und Technologie (BMWi) via the Deutsches Zentrum fur Luft und Raumfahrt (DLR) under the contract numbers 50 QV 0301 and 50 OG 0502. NR 38 TC 64 Z9 65 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAR PY 2014 VL 211 IS 1 AR 12 DI 10.1088/0067-0049/211/1/12 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB9DN UT WOS:000332090200012 ER PT J AU Huber, D Aguirre, VS Matthews, JM Pinsonneault, MH Gaidos, E Garcia, RA Hekker, S Mathur, S Mosser, B Torres, G Bastien, FA Basu, S Bedding, TR Chaplin, WJ Demory, BO Fleming, SW Guo, Z Mann, AW Rowe, JF Serenelli, AM Smith, MA Stello, D AF Huber, Daniel Aguirre, Victor Silva Matthews, Jaymie M. Pinsonneault, Marc H. Gaidos, Eric Garcia, Rafael A. Hekker, Saskia Mathur, Savita Mosser, Benoit Torres, Guillermo Bastien, Fabienne A. Basu, Sarbani Bedding, Timothy R. Chaplin, William J. Demory, Brice-Olivier Fleming, Scott W. Guo, Zhao Mann, Andrew W. Rowe, Jason F. Serenelli, Aldo M. Smith, Myron A. Stello, Dennis TI REVISED STELLAR PROPERTIES OF KEPLER TARGETS FOR THE QUARTER 1-16 TRANSIT DETECTION RUN SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; planetary systems; stars: fundamental parameters; stars: oscillations; techniques: photometric ID LOW-MASS STARS; SOLAR-LIKE OSCILLATIONS; SUN-LIKE STAR; CANDIDATE HOST STARS; R-CIRCLE-PLUS; GENEVA-COPENHAGEN SURVEY; MULTIPLE-PLANET SYSTEMS; RED GIANT STARS; 1ST 4 MONTHS; TIMING VARIATIONS AB We present revised properties for 196,468 stars observed by the NASA Kepler mission and used in the analysis of Quarter 1-16 (Q1-Q16) data to detect and characterize transiting planets. The catalog is based on a compilation of literature values for atmospheric properties (temperature, surface gravity, and metallicity) derived from different observational techniques (photometry, spectroscopy, asteroseismology, and exoplanet transits), which were then homogeneously fitted to a grid of Dartmouth stellar isochrones. We use broadband photometry and asteroseismology to characterize 11,532 Kepler targets which were previously unclassified in the Kepler Input Catalog (KIC). We report the detection of oscillations in 2762 of these targets, classifying them as giant stars and increasing the number of known oscillating giant stars observed by Kepler by similar to 20% to a total of similar to 15,500 stars. Typical uncertainties in derived radii and masses are similar to 40% and similar to 20%, respectively, for stars with photometric constraints only, and 5%-15% and similar to 10% for stars based on spectroscopy and/or asteroseismology, although these uncertainties vary strongly with spectral type and luminosity class. A comparison with the Q1-Q12 catalog shows a systematic decrease in radii of M dwarfs, while radii for K dwarfs decrease or increase depending on the Q1-Q12 provenance (KIC or Yonsei-Yale isochrones). Radii of F-G dwarfs are on average unchanged, with the exception of newly identified giants. The Q1-Q16 star properties catalog is a first step toward an improved characterization of all Kepler targets to support planet-occurrence studies. C1 [Huber, Daniel; Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huber, Daniel; Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA. [Aguirre, Victor Silva; Bedding, Timothy R.; Chaplin, William J.; Stello, Dennis] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Matthews, Jaymie M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Pinsonneault, Marc H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Gaidos, Eric] Univ Hawaii Manoa, Dept Geol & Geophys, Honolulu, HI 96822 USA. [Garcia, Rafael A.] Univ Paris 07, IRFU SAp, Ctr Saclay, Lab AIM,CEA DSM CNRS, F-91191 Gif Sur Yvette, France. [Hekker, Saskia] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany. [Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Mathur, Savita] Space Sci Inst, Boulder, CO 80301 USA. [Mosser, Benoit] Univ Paris 06, Univ Denis, Observ Paris, LESIA,CNRS, F-92195 Meudon, France. [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bastien, Fabienne A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Bedding, Timothy R.; Stello, Dennis] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Chaplin, William J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Demory, Brice-Olivier] MIT, Dept Phys, Cambridge, MA 02139 USA. [Fleming, Scott W.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Guo, Zhao] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA. [Mann, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Serenelli, Aldo M.] Inst Ciencias Espacio CSIC IEEC, Fac Ciencias, E-08193 Bellaterra, Spain. [Smith, Myron A.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Huber, D (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM daniel.huber@nasa.gov OI Fleming, Scott/0000-0003-0556-027X; Bedding, Timothy/0000-0001-5943-1460; Bedding, Tim/0000-0001-5222-4661; Demory, Brice-Olivier/0000-0002-9355-5165; Garcia, Rafael/0000-0002-8854-3776; Serenelli, Aldo/0000-0001-6359-2769 FU NASA [NNX13AE70G, NNX12AE17G]; Kepler Participating Scientist Program; NSF [AST-1105930]; Netherlands organisation for Scientific Research; ERC [338251]; NASA Harriet Jenkins Fellowship and a Vanderbilt Provost Graduate Fellowship; UK Science and Technology Facilities Council (STFC); MICINN [AYA2011-24704]; ESF EUROCORES Program EuroGENESIS (MICINN) [EUI2009-04170]; Danish National Research Foundation [DNRF106]; ASTERISK project (ASTERoseismic Investigations with SONG and Kepler); European Research Council [267864]; National Aeronautics and Space Administration; National Science Foundation FX We thank Lars Buchhave, Bill Cochran, Jonas Debosscher, Joris De Ridder, Mathieu Havel, Ulrich Kolb, Dave Latham, Mikkel Lund, Phil Muirhead, and Angie Wolfgang for helpful discussions and comments. Funding for the Kepler mission is provided by NASA's Science Mission Directorate. D. H. acknowledges support by an appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA and support by the Kepler Participating Scientist Program. S. B. acknowledges support from NSF grant AST-1105930 and NASA grant NNX13AE70 G. S. H. acknowledges financial support from the Netherlands organisation for Scientific Research and ERC starting grant No. 338251 (Stellar Ages). S. M. acknowledges support from the NASA grant NNX12AE17G. F. A. B. acknowledges support from a NASA Harriet Jenkins Fellowship and a Vanderbilt Provost Graduate Fellowship. W. J. C. acknowledges support from the UK Science and Technology Facilities Council (STFC). A. M. S. is supported by the MICINN grant AYA2011-24704 and by the ESF EUROCORES Program EuroGENESIS (MICINN grant EUI2009-04170). Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement no.: DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (grant agreement no.: 267864). This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. 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 172 TC 169 Z9 169 U1 7 U2 30 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAR PY 2014 VL 211 IS 1 AR 2 DI 10.1088/0067-0049/211/1/2 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB9DN UT WOS:000332090200002 ER PT J AU Tenenbaum, P Jenkins, J Seader, S Burke, CJ Christiansen, JL Rowe, JF Caldwell, DA Clarke, BD Coughlin, JL Li, J Quintana, EV Smith, JC Thompson, SE Twicken, JD Haas, MR Henze, CE Hunter, RC Sanderfer, DT Campbell, JR Girouard, FR Klaus, TC McCauliff, SD Middour, CK Sabale, A Uddin, AK Wohler, B Barclay, T Still, M AF Tenenbaum, Peter Jenkins, Jonm. Seader, Shawn Burke, Christopher J. Christiansen, Jessie L. Rowe, Jason F. Caldwell, Douglas A. Clarke, Bruce D. Coughlin, Jeffrey L. Li, Jie Quintana, Elisa V. Smith, Jeffrey C. Thompson, Susan E. Twicken, Joseph D. Haas, Michael R. Henze, Christopher E. Hunter, Roger C. Sanderfer, Dwight T. Campbell, Jennifer R. Girouard, Forrest R. Klaus, Todd C. McCauliff, Sean D. Middour, Christopher K. Sabale, Anima Uddin, Akm Kamal Wohler, Bill Barclay, Thomas Still, Martin TI DETECTION OF POTENTIAL TRANSIT SIGNALS IN 16 QUARTERS OF KEPLER MISSION DATA SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE planetary systems; planets and satellites: detection ID SYSTEMATIC-ERROR CORRECTION; PLANETS AB We present the results of a search for potential transit signals in 4 yr of photometry data acquired by the Kepler mission. The targets of the search include 111,800 stars which were observed for the entire interval and 85,522 stars which were observed for a subset of the interval. We found that 9743 targets contained at least one signal consistent with the signature of a transiting or eclipsing object where the criteria for detection are periodicity of the detected transits, adequate signal-to-noise ratio, and acceptance by a number of tests which reject false positive detections. When targets that had produced a signal were searched repeatedly, an additional 6542 signals were detected on 3223 target stars, for a total of 16,285 potential detections. Comparison of the set of detected signals with a set of known and vetted transit events in the Kepler field of view shows that the recovery rate for these signals is 96.9%. The ensemble properties of the detected signals are reviewed. C1 [Tenenbaum, Peter; Jenkins, Jonm.; Seader, Shawn; Burke, Christopher J.; Christiansen, Jessie L.; Rowe, Jason F.; Caldwell, Douglas A.; Clarke, Bruce D.; Coughlin, Jeffrey L.; Li, Jie; Quintana, Elisa V.; Smith, Jeffrey C.; Thompson, Susan E.; Twicken, Joseph D.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94305 USA. [Haas, Michael R.; Henze, Christopher E.; Hunter, Roger C.; Sanderfer, Dwight T.] NASA, Ames Res Ctr, Moffett Field, CA 94305 USA. [Campbell, Jennifer R.; Girouard, Forrest R.; Klaus, Todd C.; McCauliff, Sean D.; Middour, Christopher K.; Sabale, Anima; Uddin, Akm Kamal; Wohler, Bill] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94305 USA. [Barclay, Thomas; Still, Martin] NASA, BAER Inst, Ames Res Ctr, Moffett Field, CA 94305 USA. RP Tenenbaum, P (reprint author), NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94305 USA. EM peter.tenenbaum@nasa.gov RI Caldwell, Douglas/L-7911-2014 OI Caldwell, Douglas/0000-0003-1963-9616 FU NASA's Space Mission Directorate FX Funding for this mission is provided by NASA's Space Mission Directorate. The contributions of Hema Chandrasekaran continue to be essential in the studies documented here. NR 13 TC 21 Z9 21 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAR PY 2014 VL 211 IS 1 AR 6 DI 10.1088/0067-0049/211/1/6 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB9DN UT WOS:000332090200006 ER PT J AU von Kienlin, A Meegan, CA Paciesas, WS Bhat, PN Bissaldi, E Briggs, MS Burgess, JM Byrne, D Chaplin, V Cleveland, W Connaughton, V Collazzi, AC Fitzpatrick, G Foley, S Gibby, M Giles, M Goldstein, A Greiner, J Gruber, D Guiriec, S van der Horst, AJ Kouveliotou, C Layden, E McBreen, S McGlynn, S Pelassa, V Preece, RD Rau, A Tierney, D Wilson-Hodge, CA Xiong, SL Younes, G Yu, HF AF von Kienlin, Andreas Meegan, Charles A. Paciesas, William S. Bhat, P. N. Bissaldi, Elisabetta Briggs, Michael S. Burgess, J. Michael Byrne, David Chaplin, Vandiver Cleveland, William Connaughton, Valerie Collazzi, Andrew C. Fitzpatrick, Gerard Foley, Suzanne Gibby, Melissa Giles, Misty Goldstein, Adam Greiner, Jochen Gruber, David Guiriec, Sylvain van der Horst, Alexander J. Kouveliotou, Chryssa Layden, Emily McBreen, Sheila McGlynn, Sinead Pelassa, Veronique Preece, Robert D. Rau, Arne Tierney, Dave Wilson-Hodge, Colleen A. Xiong, Shaolin Younes, George Yu, Hoi-Fung TI THE SECOND FERMI GBM GAMMA-RAY BURST CATALOG: THE FIRST FOUR YEARS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; gamma-ray burst: general ID COMPREHENSIVE ANALYSIS; SPECTRAL PROPERTIES; MONITOR; EVOLUTION; SPECTROSCOPY; TELESCOPE; BRIGHTEST; TRIGGER; GRBS AB This is the second of a series of catalogs of gamma-ray bursts (GRBs) observed with the Fermi Gamma-ray Burst Monitor (GBM). It extends the first two-year catalog by two more years, resulting in an overall list of 953 GBM triggered GRBs. The intention of the GBM GRB catalog is to provide information to the community on the most important observables of the GBM detected GRBs. For each GRB the location and main characteristics of the prompt emission, the duration, peak flux and fluence are derived. The latter two quantities are calculated for the 50-300 keV energy band, where the maximum energy release of GRBs in the instrument reference system is observed and also for a broader energy band from 10-1000 keV, exploiting the full energy range of GBMs low-energy detectors. Furthermore, information is given on the settings and modifications of the triggering criteria and exceptional operational conditions during years three and four in the mission. This second catalog is an official product of the Fermi GBM science team, and the data files containing the complete results are available from the High-Energy Astrophysics Science Archive Research Center. C1 [von Kienlin, Andreas; Gruber, David; Rau, Arne; Yu, Hoi-Fung] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Meegan, Charles A.; Bhat, P. N.; Briggs, Michael S.; Burgess, J. Michael; Chaplin, Vandiver; Connaughton, Valerie; Goldstein, Adam; Layden, Emily; Pelassa, Veronique; Preece, Robert D.; Xiong, Shaolin] Univ Alabama, Huntsville, AL 35805 USA. [Paciesas, William S.; Cleveland, William; Younes, George] Univ Space Res Assoc, Huntsville, AL 35805 USA. [Bissaldi, Elisabetta] Ist Nazl Fis Nucl, I-34127 Trieste, Italy. [Bissaldi, Elisabetta] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy. [Byrne, David; Fitzpatrick, Gerard; Foley, Suzanne; McBreen, Sheila; McGlynn, Sinead; Tierney, Dave] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Collazzi, Andrew C.; Kouveliotou, Chryssa; Wilson-Hodge, Colleen A.] NASA, George C Marshall Space Flight Ctr, ZP 12, Astrophys Off, Huntsville, AL 35812 USA. [Gibby, Melissa; Giles, Misty] Jacobs Technol Inc, Huntsville, AL 35806 USA. [Gruber, David] Planetarium Sudtirol, I-39053 Karneid, Italy. [Guiriec, Sylvain] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [van der Horst, Alexander J.] Univ Amsterdam, Astron Inst, NL-1098 XH Amsterdam, Netherlands. [Yu, Hoi-Fung] Tech Univ Munich, Excellence Cluster Univ, D-85748 Garching, Germany. [Collazzi, Andrew C.] NASA, Postdoctoral Program, Washington, DC USA. RP von Kienlin, A (reprint author), Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RI Bissaldi, Elisabetta/K-7911-2016; OI Bissaldi, Elisabetta/0000-0001-9935-8106; Burgess, James/0000-0003-3345-9515; McBreen, Sheila/0000-0002-1477-618X FU Bundesministerium fur Bildung und Forschung (BMBF) via the Deutsches Zentrum fur Luft und Raumfahrt (DLR) [50 QV 0301]; Bundesministeriums fur Wirtschaft und Technologie (BMWi) through DLR grant [50 OG 1101]; Graduate Student Researchers Program; NASA; European Union [PERG04-GA-2008-239176]; Irish Research Council for Science, Engineering, and Technology; Marie Curie Actions under FP7; DFG FX Support for the German contribution to GBM was provided by the Bundesministerium fur Bildung und Forschung (BMBF) via the Deutsches Zentrum fur Luft und Raumfahrt (DLR) under contract number 50 QV 0301. A. v. K. was supported by the Bundesministeriums fur Wirtschaft und Technologie (BMWi) through DLR grant 50 OG 1101. A. G. acknowledges the support of the Graduate Student Researchers Program funded by NASA. SMB acknowledges support of the European Union Marie Curie Reintegration Grant within the 7th Program under contract number PERG04-GA-2008-239176. S. F. acknowledges the support of the Irish Research Council for Science, Engineering, and Technology, co-funded by Marie Curie Actions under FP7. H.F.Y. acknowledges support by the DFG cluster of excellence "Origin and Structure of the Universe." NR 32 TC 51 Z9 51 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAR PY 2014 VL 211 IS 1 AR 13 DI 10.1088/0067-0049/211/1/13 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB9DN UT WOS:000332090200013 ER PT J AU Plante, I Devroye, L Cucinotta, FA AF Plante, Ianik Devroye, Luc Cucinotta, Francis A. TI Calculations of distance distributions and probabilities of binding by ligands between parallel plane membranes comprising receptors SO COMPUTER PHYSICS COMMUNICATIONS LA English DT Article DE Green's functions; Diffusion equation; Brownian dynamics algorithm; Monte Carlo simulations; Cell signaling; Non-targeted effects of radiation ID TGF-BETA; RADIATION; AUTOCRINE; INDUCTION; DAMAGE; ACTIVATION; CULTURES; SIGNALS; TRACKS; CELLS AB Cell communication through biochemical signaling pathways is a key determinant of tissue responses to radiation. Several molecules, such as the transforming growth factor beta (TGF beta), are implicated in radiation-induced signaling between cells. Brownian Dynamics (BD) algorithms have recently been used to simulate the interaction of ligands with receptors and to elucidate signal transduction and autocrine loops in ligand receptors systems. In this paper, we discuss the simulation of particle diffusion and binding kinetics in a space bounded by two parallel plane membranes, using an exact algorithm to sample the propagator (Green's function) of a particle located between 2 membranes. We also show that the simulation results are independent of the number of time steps used, in accordance with time discretization equations. These simulations could be used to simulate the motion and binding of ligand molecules in a cell culture, and possibly in neuronal synapses. (C) 2013 Elsevier BM. All rights reserved. C1 [Plante, Ianik] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA. [Devroye, Luc] McGill Univ, Sch Comp Sci, Montreal, PQ H3A 0E9, Canada. [Cucinotta, Francis A.] Univ Nevada, Dept Hlth Phys & Med Diagnost, Las Vegas, NV 89154 USA. RP Plante, I (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. EM ianik.plante-1@nasa.gov; lucdevroye@gmail.com; Francis.Cucinotta@unlv.edu FU NASA Space Radiation Risk Assessment Project; DoE Low Dose Program [DE-AI02-09ER64843]; University of Nevada, Las Vegas FX This work was supported by the NASA Space Radiation Risk Assessment Project, the DoE Low Dose Program (DE-AI02-09ER64843), and the University of Nevada, Las Vegas. We also thank the reviewers for their valuable comments. NR 29 TC 0 Z9 0 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0010-4655 EI 1879-2944 J9 COMPUT PHYS COMMUN JI Comput. Phys. Commun. PD MAR PY 2014 VL 185 IS 3 BP 697 EP 707 DI 10.1016/j.cpc.2013.09.011 PG 11 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA AB6SF UT WOS:000331919100001 ER PT J AU Schwenke, DW AF Schwenke, David W. TI On the computation of high order Rys quadrature weights and nodes SO COMPUTER PHYSICS COMMUNICATIONS LA English DT Article DE Gaussian quadrature; Electron repulsion integrals ID POLYNOMIALS; SCHEME AB We develop and describe a new method for computing Gaussian quadrature weights and nodes for non-classical weight functions and apply it to the Rys quadrature used to accurately compute two-electron repulsion integrals over Gaussian type orbitals in molecular electronic structure theory. With the new method, using an ordinary 64 bit floating point representation, it is possible to compute weights and nodes to an accuracy of one part in 10(12) even for the absurdly high value of N = 101. Published by Elsevier B.V. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Schwenke, DW (reprint author), NASA, Ames Res Ctr, MS 258-2, Moffett Field, CA 94035 USA. EM david.w.schwenke@nasa.gov RI schwenke, david/I-3564-2013 NR 10 TC 3 Z9 3 U1 1 U2 11 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0010-4655 EI 1879-2944 J9 COMPUT PHYS COMMUN JI Comput. Phys. Commun. PD MAR PY 2014 VL 185 IS 3 BP 762 EP 763 DI 10.1016/j.cpc.2013.11.004 PG 2 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA AB6SF UT WOS:000331919100008 ER PT J AU Naud, CM Booth, JF Del Genio, AD AF Naud, Catherine M. Booth, James F. Del Genio, Anthony D. TI Evaluation of ERA-Interim and MERRA Cloudiness in the Southern Ocean SO JOURNAL OF CLIMATE LA English DT Article DE Cloud parameterizations; Extratropical cyclones; Reanalysis data; Climate models; Model evaluation/performance; Cloud cover ID SATELLITE-OBSERVATIONS; MIDLATITUDE CYCLONES; GLOBAL ENERGY; MODEL; SYSTEM; PARAMETERIZATION; PRECIPITATION; CLOUDSAT; SCHEME; MODIS AB The Southern Ocean cloud cover modeled by the Interim ECMWF Re-Analysis (ERA-Interim) and Modern-Era Retrospective Analysis for Research and Applications (MERRA) reanalyses are compared against Moderate Resolution Imaging Spectroradiometer (MODIS) and Multiangle Imaging Spectroradiometer (MISR) observations. ERA-Interim monthly mean cloud amounts match the observations within 5%, while MERRA significantly underestimates the cloud amount. For a compositing analysis of clouds in warm season extratropical cyclones, both reanalyses show a low bias in cloud cover. They display a larger bias to the west of the cyclones in the region of subsidence behind the cold fronts. This low bias is larger for MERRA than for ERA-Interim. Both MODIS and MISR retrievals indicate that the clouds in this sector are at a low altitude, often composed of liquid, and of a broken nature. The combined CloudSat-Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) cloud profiles confirm these passive observations, but they also reveal that low-level clouds in other parts of the cyclones are also not properly represented in the reanalyses. The two reanalyses are in fairly good agreement for the dynamic and thermodynamic characteristics of the cyclones, suggesting that the cloud, convection, or boundary layer schemes are the problem instead. An examination of the lower-tropospheric stability distribution in the cyclones from both reanalyses suggests that the parameterization of shallow cumulus clouds may contribute in a large part to the problem. However, the differences in the cloud schemes and in particular in the precipitation processes, which may also contribute, cannot be excluded. C1 [Naud, Catherine M.; Booth, James F.] Columbia Univ, New York, NY 10025 USA. [Del Genio, Anthony D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Naud, CM (reprint author), Columbia Univ, 2880 Broadway, New York, NY 10025 USA. EM cn2140@columbia.edu FU NASA [NNX10AM20G, NNX11AH22G] FX MODIS data were obtained from the Level 1 and Atmospheric Distribution System at the NASA Goddard Space Flight Center. MISR data files were obtained from the NASA Langley Atmospheric Sciences Data Center. CloudSat-CALIPSO GEOPROF-LIDAR data were obtained from the Cloudsat Data Processing Center. AMSR-E ocean products were obtained from the National Snow and Ice Data Center. AIRS level-2 files and MERRA files were obtained from the NASA Goddard Earth Sciences Data and Information Services Center. ERA-Interim files were obtained from the European Centre for Medium-Range Weather Forecasts Meteorological Archival and Retrieval System. This work was funded by NASA CloudSat Science team Grant NNX10AM20G to CMN and RTOP to ADD, and by NASA the Science of Terra and Aqua Grant NNX11AH22G to CMN. JFB was funded by a NASA Postdoctoral Program Fellowship. The authors thank the editor, Jay Mace, and two anonymous reviewers for their insightful comments that have helped significantly improve this manuscript. NR 44 TC 28 Z9 28 U1 2 U2 26 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD MAR PY 2014 VL 27 IS 5 BP 2109 EP 2124 DI 10.1175/JCLI-D-13-00432.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AB3KO UT WOS:000331689900011 ER PT J AU Nemmen, RS Storchi-Bergmann, T Eracleous, M AF Nemmen, Rodrigo S. Storchi-Bergmann, Thaisa Eracleous, Michael TI Spectral models for low-luminosity active galactic nuclei in LINERs: the role of advection-dominated accretion and jets SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; galaxies: active; galaxies: jets; galaxies: nuclei; galaxies: Seyfert ID RADIATIVELY INEFFICIENT ACCRETION; SUPERMASSIVE BLACK-HOLES; DWARF SEYFERT NUCLEI; SGR-A-ASTERISK; RAY BURST AFTERGLOWS; X-RAY; FUNDAMENTAL PLANE; NEARBY GALAXIES; RADIO-EMISSION; ENERGY-DISTRIBUTIONS AB We perform an exploratory study of the physical properties of accretion flows and jets in low-luminosity active galactic nuclei (LLAGNs) by modelling the spectral energy distributions (SEDs) of 12 LLAGNs in low-ionization nuclear emission-line regions (LINERs). These SEDs we constructed from high-resolution radio, X-ray and optical/ultraviolet (UV) observations of the immediate vicinity of the black hole. We adopt a coupled accretion-jet model comprising an inner advection-dominated accretion flow (ADAF) and an outer standard thin disc. We present best-fitting models in which either the ADAF or the jet dominates the X-ray emission. Six sources in our sample display an optical-UV excess with respect to ADAF and jet models; this excess can be explained as emission from the truncated disc with transition radii 30-225 R-S in four of them. In almost all sources the optical emission can also be attributed to unresolved, old stellar clusters with masses similar to 10(7)-10(8) M-circle dot. We find evidence for a correlation between the accretion rate and jet power and an anticorrelation between the radio loudness and the accretion rate. We confirm previous findings that the radio emission is severely underpredicted by ADAF models and explained by the relativistic jet. We find evidence for a non-linear relation between the X-ray and bolometric luminosities and a slight IR excess in the average model SED compared to that of quasars. We suggest that the hardness of the X-ray spectrum can be used to identify the X-ray emission mechanism and discuss directions for progress in understanding the origin of the X-rays. C1 [Nemmen, Rodrigo S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Storchi-Bergmann, Thaisa] Univ Fed Rio Grande do Sul, Inst Fis, Porto Alegre, RS, Brazil. [Eracleous, Michael] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. RP Nemmen, RS (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM rodrigo.nemmen@nasa.gov RI Nemmen, Rodrigo/O-6841-2014 FU NASA Postdoctoral Program at Goddard Space Flight Center; NASA; CNPq; CAPES; National Aeronautics and Space Administration FX We are grateful to Feng Yuan for useful discussions as well as help with the models and allowing us to use some of his codes; Renyi Ma and Hui Zhang for their help with setting up the models; Joao Steiner, Michael Brotherton, Rogerio Riffel, Francesco Tombezi, Judith Racusin, Rafael Eufrasio, Rachel Mason and Roman Shcherbakov for productive discussions; and to the referee for the useful comments and the suggestion of considering the contribution of stellar populations. RSN was supported by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. TSB acknowledges the financial support of the Brazilian institutions CNPq and CAPES. 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 170 TC 20 Z9 20 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 MAR PY 2014 VL 438 IS 4 BP 2804 EP 2827 DI 10.1093/mnras/stt2388 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB8KD UT WOS:000332038000007 ER PT J AU Schmidt, GA Shindell, DT Tsigaridis, K AF Schmidt, Gavin A. Shindell, Drew T. Tsigaridis, Kostas TI Reconciling warming trends SO NATURE GEOSCIENCE LA English DT Editorial Material ID AEROSOL C1 [Schmidt, Gavin A.; Shindell, Drew T.; Tsigaridis, Kostas] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Tsigaridis, Kostas] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. RP Schmidt, GA (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM gavin.a.schmidt@nasa.gov RI Schmidt, Gavin/D-4427-2012; Shindell, Drew/D-4636-2012 OI Schmidt, Gavin/0000-0002-2258-0486; NR 18 TC 82 Z9 86 U1 4 U2 48 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD MAR PY 2014 VL 7 IS 3 BP 158 EP 160 DI 10.1038/ngeo2105 PG 3 WC Geosciences, Multidisciplinary SC Geology GA AB9DB UT WOS:000332088800002 ER PT J AU Santer, BD Bonfils, C Painter, JF Zelinka, MD Mears, C Solomon, S Schmidt, GA Fyfe, JC Cole, JNS Nazarenko, L Taylor, KE Wentz, FJ AF Santer, Benjamin D. Bonfils, Celine Painter, Jeffrey F. Zelinka, Mark D. Mears, Carl Solomon, Susan Schmidt, Gavin A. Fyfe, John C. Cole, Jason N. S. Nazarenko, Larissa Taylor, Karl E. Wentz, Frank J. TI Volcanic contribution to decadal changes in tropospheric temperature SO NATURE GEOSCIENCE LA English DT Article ID CLIMATE; TRENDS; MODEL AB Despite continued growth in atmospheric levels of greenhouse gases, global mean surface and tropospheric temperatures have shown slower warming since 1998 than previously(1-5). Possible explanations for the slow-down include internal climate variability(3,4,6,7), external cooling influences(1,2,4,8-11) and observational errors(12,13). Several recent modelling studies have examined the contribution of early twenty-first-century volcanic eruptions(1,2,4,8) to the muted surface warming. Here we present a detailed analysis of the impact of recent volcanic forcing on tropospheric temperature, based on observations as well as climate model simulations. We identify statistically significant correlations between observations of stratospheric aerosol optical depth and satellite-based estimates of both tropospheric temperature and short-wave fluxes at the top of the atmosphere. We show that climate model simulations without the effects of early twenty-first-century volcanic eruptions overestimate the tropospheric warming observed since 1998. In two simulations with more realistic volcanic influences following the 1991 Pinatubo eruption, differences between simulated and observed tropospheric temperature trends over the period 1998 to 2012 are up to 15% smaller, with large uncertainties in the magnitude of the effect. To reduce these uncertainties, better observations of eruption-specific properties of volcanic aerosols are needed, as well as improved representation of these eruption-specific properties in climate model simulations. C1 [Santer, Benjamin D.; Bonfils, Celine; Painter, Jeffrey F.; Zelinka, Mark D.; Taylor, Karl E.] Lawrence Livermore Natl Lab, Program Climate Model Diag & Intercomparison, Livermore, CA 94550 USA. [Mears, Carl; Wentz, Frank J.] Remote Sensing Syst, Santa Rosa, CA 95401 USA. [Solomon, Susan] MIT, Cambridge, MA 02139 USA. [Schmidt, Gavin A.; Nazarenko, Larissa] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Fyfe, John C.; Cole, Jason N. S.] Environm Canada, Canadian Ctr Climate Modelling & Anal, Victoria, BC V8W 2Y2, Canada. RP Santer, BD (reprint author), Lawrence Livermore Natl Lab, Program Climate Model Diag & Intercomparison, Livermore, CA 94550 USA. EM santer1@llnl.gov RI Schmidt, Gavin/D-4427-2012; Taylor, Karl/F-7290-2011; Santer, Benjamin/F-9781-2011; Zelinka, Mark/C-4627-2011; OI Schmidt, Gavin/0000-0002-2258-0486; Taylor, Karl/0000-0002-6491-2135; Zelinka, Mark/0000-0002-6570-5445; Cole, Jason/0000-0003-0450-2748 FU U.S. Department of Energy [DE-AC52-07NA27344]; DOE/OBER Early Career Research Program Award [SCW1295] FX We acknowledge the World Climate Research Programme's Working Group on Coupled Modelling, which is responsible for CMIP, and we thank the climate modelling groups for producing and making available their model output. For CMIP, the US Department of Energy's Program for Climate Model Diagnosis and Intercomparison (PCMDI) provides coordinating support and led development of software infrastructure in partnership with the Global Organization for Earth System Science Portals. J-P. Vernier (NASA Langley) and M. Sato (GISS) supplied updated SAOD data. T. M. L. Wigley (University of Adelaide), N. Gillett (Canadian Centre for Climate Modelling and Analysis), A. Robock (Rutgers University), K. Trenberth (National Center for Atmospheric Research) and S. F. B. Tett (University of Edinburgh) provided helpful comments. At PCMDI, work by B. D. S., J.P., M.Z. and K. E. T. was performed under the auspices of the U.S. Department of Energy under contract DE-AC52-07NA27344; C. B. was supported by the DOE/OBER Early Career Research Program Award SCW1295. NR 28 TC 105 Z9 113 U1 13 U2 107 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD MAR PY 2014 VL 7 IS 3 BP 185 EP 189 DI 10.1038/NGEO2098 PG 5 WC Geosciences, Multidisciplinary SC Geology GA AB9DB UT WOS:000332088800011 ER PT J AU Valley, JW Cavosie, AJ Ushikubo, T Reinhard, DA Lawrence, DF Larson, DJ Clifton, PH Kelly, TF Wilde, SA Moser, DE Spicuzza, MJ AF Valley, John W. Cavosie, Aaron J. Ushikubo, Takayuki Reinhard, David A. Lawrence, Daniel F. Larson, David J. Clifton, Peter H. Kelly, Thomas F. Wilde, Simon A. Moser, Desmond E. Spicuzza, Michael J. TI Hadean age for a post-magma-ocean zircon confirmed by atom-probe tomography SO NATURE GEOSCIENCE LA English DT Article ID PB GEOCHRONOLOGY; JACK HILLS; AUSTRALIA; MINERALS; ORIGIN; CRUST; TIMS AB The only physical evidence from the earliest phases of Earth's evolution comes from zircons, ancient mineral grains that can be dated using the U-Th-Pb geochronometer(1). Oxygen isotope ratios from such zircons have been used to infer when the hydrosphere and conditions habitable to life were established(2,3). Chemical homogenization of Earth's crust and the existence of a magma ocean have not been dated directly, but must have occurred earlier(4). However, the accuracy of the U-Pb zircon ages can plausibly be biased by poorly understood processes of intracrystalline Pb mobility(5-7). Here we use atom-probe tomography(8) to identify and map individual atoms in the oldest concordant grain from Earth, a 4.4-Gyr-old Hadean zircon with a high-temperature overgrowth that formed about 1Gyr after the mineral's core. Isolated nanoclusters, measuring about 10nm and spaced 10-50nm apart, are enriched in incompatible elements including radiogenic Pb with unusually high Pb-207/Pb-206 ratios. We demonstrate that the length scales of these clusters make U-Pb age biasing impossible, and that they formed during the later reheating event. Our tomography data thereby confirm that any mixing event of the silicate Earth must have occurred before 4.4Gyr ago, consistent with magma ocean formation by an early moon-forming impact(4) about 4.5Gyr ago. C1 [Valley, John W.; Cavosie, Aaron J.; Ushikubo, Takayuki; Spicuzza, Michael J.] Univ Wisconsin, Dept Geosci, NASA, WiscSIMS,Astrobiol Inst, Madison, WI 53706 USA. [Cavosie, Aaron J.] Univ Puerto Rico, Mayaguez, PR 00681 USA. [Reinhard, David A.; Lawrence, Daniel F.; Larson, David J.; Clifton, Peter H.; Kelly, Thomas F.] CAMECA, Madison, WI 53711 USA. [Wilde, Simon A.] Curtin Univ, Perth, WA 6845, Australia. [Moser, Desmond E.] Univ Western Ontario, London, ON N6A 5B7, Canada. RP Valley, JW (reprint author), Univ Wisconsin, Dept Geosci, NASA, WiscSIMS,Astrobiol Inst, Madison, WI 53706 USA. EM valley@geology.wisc.edu OI Cavosie, Aaron/0000-0001-6819-6810 FU NASA Astrobiology Institute; [NSF-EAR0838058]; [DOE-93ER14389]; [NSF-EAR1053466] FX This research was supported by NSF-EAR0838058, DOE-93ER14389 and the NASA Astrobiology Institute. T.C., D.R., D.F.L., D.J.L. and P.C. thank their colleagues at CAMECA in Madison, Wisconsin, for their contribution to these efforts. WiscSIMS is partly supported by NSF-EAR1053466. NR 27 TC 82 Z9 85 U1 15 U2 114 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD MAR PY 2014 VL 7 IS 3 BP 219 EP 223 DI 10.1038/NGEO2075 PG 5 WC Geosciences, Multidisciplinary SC Geology GA AB9DB UT WOS:000332088800019 ER PT J AU Versteegh, EAA Black, S Hodson, ME AF Versteegh, Emma A. A. Black, Stuart Hodson, Mark E. TI Environmental controls on the production of calcium carbonate by earthworms SO SOIL BIOLOGY & BIOCHEMISTRY LA English DT Article DE Calcite; CO2; Experiment; Lumbricus terrestris; pH regulation; Temperature ID LUMBRICUS-TERRESTRIS; CALCIFEROUS GLANDS; GRANULES; SOIL AB Lumbricus terrestris earthworms produce calcium carbonate (CaCO3) granules with unknown physiological function. To investigate carbon sequestration potential, the influence of temperature and CO2 concentration ([CO2]) on CaCO3 production was investigated using three soils, five temperatures (3-20 degrees C) and four atmospheric [CO2] (439-3793 ppm). Granule production rates differed between soils, but could not be related to any soil characteristics measured. Production rates increased with temperature, probably because of higher metabolic rate, and with soil CO2 concentration. Implications for carbon sequestration are discussed. CaCO3 production in earthworms is probably related to pH regulation of blood and tissue fluid in the high CO2 environment of the soil. (C) 2013 The Authors. Published by Elsevier Ltd. All rights reserved. C1 [Versteegh, Emma A. A.] Univ Reading, Sch Archaeol Geog & Environm Sci, Dept Geog & Environm Sci, Reading RG6 6DW, Berks, England. [Black, Stuart] Univ Reading, Sch Archaeol Geog & Environm Sci, Dept Archaeol, Reading RG6 6AB, Berks, England. [Hodson, Mark E.] Univ York, Dept Environm, York YO10 5DD, N Yorkshire, England. RP Versteegh, EAA (reprint author), CALTECH, NASA Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM emma.versteegh@jpl.nasa.gov; s.black@reading.ac.uk; mark.hodson@york.ac.uk RI Black, Stuart/A-1099-2014; OI Black, Stuart/0000-0003-1396-4821; Hodson, Mark/0000-0002-8166-1526 FU NERC [NE/H021914/1] FX This research was funded by a NERC Standard Research Grant (MEH and SB; NE/H021914/1). We thank Jens Dyckmans (University of Gottingen) for the [CO2] analyses. The manuscript was greatly improved by the comments of two anonymous reviewers. NR 29 TC 5 Z9 5 U1 5 U2 28 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0038-0717 J9 SOIL BIOL BIOCHEM JI Soil Biol. Biochem. PD MAR PY 2014 VL 70 BP 159 EP 161 DI 10.1016/j.soilbio.2013.12.013 PG 3 WC Soil Science SC Agriculture GA AC3RV UT WOS:000332439800019 ER PT J AU Kim, J Waliser, DE Mattmann, CA Goodale, CE Hart, AF Zimdars, PA Crichton, DJ Jones, C Nikulin, G Hewitson, B Jack, C Lennard, C Favre, A AF Kim, J. Waliser, Duane E. Mattmann, Chris A. Goodale, Cameron E. Hart, Andrew F. Zimdars, Paul A. Crichton, Daniel J. Jones, Colin Nikulin, Grigory Hewitson, Bruce Jack, Chris Lennard, Christopher Favre, Alice TI Evaluation of the CORDEX-Africa multi-RCM hindcast: systematic model errors SO CLIMATE DYNAMICS LA English DT Article DE CORDEX; Africa; RCM evaluation; Regional climate; Impact assessments; Systematic model biases; IPCC ID REGIONAL CLIMATE MODELS; WESTERN UNITED-STATES; PRECIPITATION; TEMPERATURE; ENSEMBLE; PERFORMANCE; CIRCULATION; SIMULATION; WEATHER; TRENDS AB Monthly-mean precipitation, mean (T-AVG), maximum (T-MAX) and minimum (T-MIN) surface air temperatures, and cloudiness from the CORDEX-Africa regional climate model (RCM) hindcast experiment are evaluated for model skill and systematic biases. All RCMs simulate basic climatological features of these variables reasonably, but systematic biases also occur across these models. All RCMs show higher fidelity in simulating precipitation for the west part of Africa than for the east part, and for the tropics than for northern Sahara. Interannual variation in the wet season rainfall is better simulated for the western Sahel than for the Ethiopian Highlands. RCM skill is higher for T-AVG and T-MAX than for T-MIN, and regionally, for the subtropics than for the tropics. RCM skill in simulating cloudiness is generally lower than for precipitation or temperatures. For all variables, multi-model ensemble (ENS) generally outperforms individual models included in ENS. An overarching conclusion in this study is that some model biases vary systematically for regions, variables, and metrics, posing difficulties in defining a single representative index to measure model fidelity, especially for constructing ENS. This is an important concern in climate change impact assessment studies because most assessment models are run for specific regions/sectors with forcing data derived from model outputs. Thus, model evaluation and ENS construction must be performed separately for regions, variables, and metrics as required by specific analysis and/or assessments. Evaluations using multiple reference datasets reveal that cross-examination, quality control, and uncertainty estimates of reference data are crucial in model evaluations. C1 [Kim, J.; Waliser, Duane E.; Mattmann, Chris A.] Univ Calif Los Angeles, JIFRESSE, Los Angeles, CA 90095 USA. [Waliser, Duane E.; Mattmann, Chris A.; Goodale, Cameron E.; Hart, Andrew F.; Zimdars, Paul A.; Crichton, Daniel J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Jones, Colin; Nikulin, Grigory] Sveriges Meteorologiska Hydrologiska Inst, Norrkoping, Sweden. [Hewitson, Bruce; Jack, Chris; Lennard, Christopher; Favre, Alice] Univ Cape Town, ZA-7925 Cape Town, South Africa. [Favre, Alice] Univ Bourgogne, Ctr Rech Climatol, Biogeosci CNRS, UMR 6282, Dijon, France. RP Kim, J (reprint author), Univ Calif Los Angeles, JIFRESSE, Los Angeles, CA 90095 USA. EM jkim@atmos.ucla.edu RI Hewitson, Bruce/B-3295-2014; Jack, Christopher/B-7926-2014 OI Hewitson, Bruce/0000-0001-7546-4430; Jack, Christopher/0000-0002-0936-7277 FU American Recovery and Re-investment Act (ARRA); National Aeronautics and Space Administration (NASA) National Climate Assessment [11-NCA11-0028]; AIST [AIST-QRS-12-0002]; National Science Foundation (NSF) ExArch [1125798]; EaSM [2011-67004-30224] FX We thank Dr. Guan for the Taylor Diagrams used in this paper. This study is supported by American Recovery and Re-investment Act (ARRA), The National Aeronautics and Space Administration (NASA) National Climate Assessment (11-NCA11-0028) and AIST (AIST-QRS-12-0002) projects, and the National Science Foundation (NSF) ExArch (1125798) and EaSM (2011-67004-30224). The contribution from D. Waliser, C. Mattmann, C. Goodale, A. Hart, P. Zimdars, and D. Crichton to this study was performed on behalf of the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 56 TC 33 Z9 33 U1 0 U2 24 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 EI 1432-0894 J9 CLIM DYNAM JI Clim. Dyn. PD MAR PY 2014 VL 42 IS 5-6 BP 1189 EP 1202 DI 10.1007/s00382-013-1751-7 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AB7KV UT WOS:000331969800005 ER PT J AU Mattmann, CA Waliser, D Kim, J Goodale, C Hart, A Ramirez, P Crichton, D Zimdars, P Boustani, M Lee, K Loikith, P Whitehall, K Jack, C Hewitson, B AF Mattmann, Chris A. Waliser, Duane Kim, Jinwon Goodale, Cameron Hart, Andrew Ramirez, Paul Crichton, Dan Zimdars, Paul Boustani, Maziyar Lee, Kyo Loikith, Paul Whitehall, Kim Jack, Chris Hewitson, Bruce TI Cloud computing and virtualization within the regional climate model and evaluation system SO EARTH SCIENCE INFORMATICS LA English DT Article DE RCMES; Regional Climate Modeling; Apache; OODT; Hadoop; Sqoop; MongoDB; Hive AB The Regional Climate Model Evaluation System (RCMES) facilitates the rapid, flexible inclusion of NASA observations into climate model evaluations. RCMES provides two fundamental components. A database (RCMED) is a scalable point-oriented cloud database used to elastically store remote sensing observations and to make them available using a space time query interface. The analysis toolkit (RCMET) is a Python-based toolkit that can be delivered as a cloud virtual machine, or as an installer package deployed using Python Buildout to users in order to allow for temporal and spatial regridding, metrics calculation (RMSE, bias, PDFs, etc.) and end-user visualization. RCMET is available to users in an "offline", lone scientist mode based on a virtual machine dynamically constructed with model outputs and observations to evaluate; or on an institution's computational cluster seated close to the observations and model outputs. We have leveraged RCMES within the content of the Coordinated Regional Downscaling Experiment (CORDEX) project, working with the University of Cape Town and other institutions to compare the model output to NASA remote sensing data; in addition we are also working with the North American Regional Climate Change Assessment Program (NARCCAP). In this paper we explain the contribution of cloud computing to RCMES's specifically describing studies of various cloud databases we evaluated for RCMED, and virtualization toolkits for RCMET, and their potential strengths in delivering user-created dynamic regional climate model evaluation virtual machines for our users. C1 [Mattmann, Chris A.; Waliser, Duane; Goodale, Cameron; Hart, Andrew; Ramirez, Paul; Crichton, Dan; Zimdars, Paul; Boustani, Maziyar; Lee, Kyo; Loikith, Paul; Whitehall, Kim] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Mattmann, Chris A.; Waliser, Duane; Kim, Jinwon] UCLA JIFRESSE, Los Angeles, CA USA. [Whitehall, Kim] Howard Univ, Washington, DC 20059 USA. [Mattmann, Chris A.] Univ So Calif, Los Angeles, CA USA. [Jack, Chris; Hewitson, Bruce] Univ Cape Town, ZA-7925 Cape Town, South Africa. RP Mattmann, CA (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM chris.a.mattmann@nasa.gov RI Hewitson, Bruce/B-3295-2014; Jack, Christopher/B-7926-2014 OI Hewitson, Bruce/0000-0001-7546-4430; Jack, Christopher/0000-0002-0936-7277 FU NASA Advanced Information Systems (AIST) program [AIST-QRS-12-0002-T] FX This work was conducted at the Jet Propulsion Laboratory, managed by the California Institute of Technology, for the National Aeronautics and Space Administration. The research reported on herein was sponsored by the NASA Advanced Information Systems (AIST) program (AIST-QRS-12-0002-T). Thanks are due to the RCMES team including Duane Waliser, Jinwon Kim, Cameron Goodale, Andrew Hart, Paul Ramirez, Paul Zimdars, Kim Whitehall, Jesslyn Whittell and Dan Crichton. The author also wishes to thank Michael Seablom for his support in this effort. NR 19 TC 1 Z9 1 U1 2 U2 26 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1865-0473 EI 1865-0481 J9 EARTH SCI INFORM JI Earth Sci. Inform. PD MAR PY 2014 VL 7 IS 1 BP 1 EP 12 DI 10.1007/s12145-013-0126-2 PG 12 WC Computer Science, Interdisciplinary Applications; Geosciences, Multidisciplinary SC Computer Science; Geology GA AB8AT UT WOS:000332013200001 ER PT J AU Tappa, MJ Ayuso, RA Bodnar, RJ Aylor, JG Beard, J Henika, WS Vazquez, JA Wooden, JL AF Tappa, M. J. Ayuso, R. A. Bodnar, R. J. Aylor, J. G. Beard, J. Henika, W. S. Vazquez, J. A. Wooden, J. L. TI AGE OF HOST ROCKS AT THE COLES HILL URANIUM DEPOSIT, PITTSYLVANIA COUNTY, VIRGINIA, BASED ON ZIRCON U-Pb GEOCHRONOLOGY SO ECONOMIC GEOLOGY LA English DT Article ID SMITH RIVER ALLOCHTHON; HYDROTHERMAL CONDITIONS; SOUTHERN APPALACHIANS; METAMICT ZIRCON; ICP-MS; EVOLUTION; LEAD; ISOTOPE; TERRANE; SHRIMP AB New U-Pb zircon SHRIMP geochronology confirms that the Coles Hill uranium deposit in Pittsylvania County, Virginia, is hosted within the Late Ordovician to Silurian Martinsville Intrusive Complex. The meta-igneous host rocks at Coles Hill consist of two units of the Martinsville Intrusive Complex: the felsic Leatherwood Granite and the mafic Rich Acres Formation. Two samples of unmineralized Leatherwood Granite orthogneiss yield Pb-206/U-238 ages between 444.5 +/- 2.5 and 447.5 +/- 1.9 Ma. A third sample of unmineralized Leatherwood Granite orthogneiss shows a wider range in Pb-206/U-238 ages, possibly due to Pb loss, and a Pb-206/Pb-207 age of 452 +/- 18 Ma. Unmineralized Rich Acres Formation amphibolite that cuts the Leatherwood gives a mean Pb-206/U-238 age (426.2 +/- 7.0 Ma), slightly younger than the Leatherwood age. Samples of mineralized orthogneiss and mineralized amphibolite give similar Pb-206/Pb-207 ages of 419 +/- 19 and 426 +/- 21 Ma, respectively. A biotite gneiss unit that underlies the mineralized zone yields a Pb-206/Pb-207 age of 415 +/- 21 Ma, indicating that it is part of the Martinsville Intrusive Complex and not a member of the early Cambrian Fork Mountain Schist, as has been previously reported. A genetic model for the Coles Hill uranium deposit has not yet been developed, although age constraints indicate that mineralization is either late or postmagmatic, and this is consistent with the epigenetic, fracture-controlled nature of the mineralization. Results obtained here do not preclude either the igneous host rocks (or similar rocks at depth) or the sedimentary units in the adjacent Triassic basin as possible sources for the uranium. C1 [Tappa, M. J.; Bodnar, R. J.; Henika, W. S.] Virginia Tech, Dept Geosci, Blacksburg, VA 24061 USA. [Tappa, M. J.; Ayuso, R. A.] US Geol Survey, Natl Ctr, Reston, VA 20192 USA. [Aylor, J. G.] Virginia Uranium Inc, Chatham, VA 24351 USA. [Beard, J.] Virginia Museum Nat Hist, Martinsville, VA 24112 USA. [Vazquez, J. A.] US Geol Survey, Menlo Pk, CA 94025 USA. [Wooden, J. L.] Stanford Univ, Dept Geol & Environm Sci, Stanford, CA 94305 USA. RP Tappa, MJ (reprint author), NASA, Lyndon B Johnson Space Ctr, JETS, 2224 Bay Area Blvd, Houston, TX 77058 USA. EM rjb@vt.edu FU U.S. Geological Survey Mineral Resources External Research Program (MRERP) FX The authors thank Luca Fedele for his assistance with the LA-ICP-MS system at Virginia Tech. We also thank John Jackson and Drew Coleman for their assistance in the processing of samples, and Stewart East for assistance in sample collection. We thank Brad Ito for providing critical electronics support for the SHRIMP-RG ion microprobe. Reviews by F. Corfu and D. Selby improved the quality of this manuscript. Funding for this project was provided by a grant to RJB and RAA from the U.S. Geological Survey Mineral Resources External Research Program (MRERP). The curation staff at the Virginia Museum of Natural History generously provided access to drill core 41-90A from which samples (41-90A-1, 41-90A-2) were collected. Reviews of an earlier version of this manuscript by R. Tucker and G. Robinson significantly improved the presentation. NR 51 TC 4 Z9 4 U1 1 U2 10 PU SOC ECONOMIC GEOLOGISTS, INC PI LITTLETON PA 7811 SCHAFFER PARKWAY, LITTLETON, CO 80127 USA SN 0361-0128 EI 1554-0774 J9 ECON GEOL JI Econ. Geol. PD MAR-APR PY 2014 VL 109 IS 2 BP 513 EP 530 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AB3GQ UT WOS:000331679700012 ER PT J AU Norsk, P AF Norsk, Peter TI Blood pressure regulation IV: adaptive responses to weightlessness SO EUROPEAN JOURNAL OF APPLIED PHYSIOLOGY LA English DT Review DE Baroreflexes; Gravity; Pressure; Sympathetic; Vascular; Weightlessness; Spaceflight ID DOWN BED REST; OUT WATER IMMERSION; SYMPATHETIC-NERVE ACTIVITY; BODY-FLUID COMPARTMENTS; CENTRAL VENOUS-PRESSURE; HEART-RATE; NEGATIVE-PRESSURE; POSTURE CHANGE; PLASMA-VOLUME; CARDIOVASCULAR REGULATION AB During weightlessness, blood and fluids are immediately shifted from the lower to the upper body segments, and within the initial 2 weeks of spaceflight, brachial diastolic arterial pressure is reduced by 5 mmHg and even more so by some 10 mmHg from the first to the sixth month of flight. Blood pressure thus adapts in space to a level very similar to that of being supine on the ground. At the same time, stroke volume and cardiac output are increased and systemic vascular resistance decreased, whereas sympathetic nerve activity is kept surprisingly high and similar to when ground-based upright seated. This was not predicted from simulation models and indicates that dilatation of the arteriolar resistance vessels is caused by mechanisms other than a baroreflex-induced decrease in sympathetic nervous activity. Results of baroreflex studies in space indicate that compared to being ground-based supine, the carotid (vagal)-cardiac interaction is reduced and sympathetic nerve activity, heart rate and systemic vascular resistance response more pronounced during baroreflex inhibition by lower body negative pressure. The future challenge is to identify which spaceflight mechanism induces peripheral arteriolar dilatation, which could explain the decrease in blood pressure, the high sympathetic nerve activity and associated cardiovascular changes. It is also a challenge to determine the cardiovascular risk profile of astronauts during future long-duration deep space missions. C1 [Norsk, Peter] USRA, Div Space Life Sci, Houston, TX USA. [Norsk, Peter] NASA, Lyndon B Johnson Space Ctr, Biomed Res & Environm Sci Div, Houston, TX 77058 USA. RP Norsk, P (reprint author), NASA, Lyndon B Johnson Space Ctr, Biomed Res & Environm Sci Div, 2101 NASA Pkwy, Houston, TX 77058 USA. EM peter.norsk@nasa.gov NR 96 TC 8 Z9 9 U1 3 U2 13 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1439-6319 EI 1439-6327 J9 EUR J APPL PHYSIOL JI Eur. J. Appl. Physiol. PD MAR PY 2014 VL 114 IS 3 BP 481 EP 497 DI 10.1007/s00421-013-2797-2 PG 17 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA AB2VT UT WOS:000331650900005 PM 24390686 ER PT J AU Stenger, MB Lee, SMC Ribeiro, LC Phillips, TR Ploutz-Snyder, RJ Willig, MC Westby, CM Platts, SH AF Stenger, Michael B. Lee, Stuart M. C. Ribeiro, L. Christine Phillips, Tiffany R. Ploutz-Snyder, Robert J. Willig, Michael C. Westby, Christian M. Platts, Steven H. TI Gradient compression garments protect against orthostatic intolerance during recovery from bed rest SO EUROPEAN JOURNAL OF APPLIED PHYSIOLOGY LA English DT Article DE Spaceflight; Countermeasure; Anti-gravity suit; Tilt test; Presyncope ID HYPOTENSION; SPACEFLIGHT; VOLUME; ASTRONAUTS; RESPONSES; EXERCISE; FLIGHT; SUIT AB Abdomen-high, lower body graded compression garments (GCGs) may represent the next-generation of orthostatic intolerance protection with applications for exploration missions and commercial space flight. To evaluate the efficacy of the GCG to prevent orthostatic intolerance after a 14-day 6A degrees head-down tilt bed rest (BR) and to determine whether wearing thigh-high compression garments impairs recovery from BR. Sixteen (12 M, 4 F) subjects participated in a 15-min 80A degrees head-up tilt test 5 day before BR (BR-5), on the last morning of BR (BR+0), and on day 1 (BR+1) and 3 after BR (BR+3). No subjects wore the GCG on BR-5, and all subjects wore the GCG during testing on BR+0. Control subjects (n = 8) wore the GCG only through testing on BR+0. Treatment subjects (n = 8) wore the GCG on BR+0 and thigh-high garments on BR+1 and BR+2. No subjects were presyncopal during tilt on BR+0 while wearing the GCG. Despite lower plasma volume index (BR-5: 1.52 +/- A 0.06, BR+0: 1.32 +/- A 0.05 l/m(2)), the tilt-induced increase in heart rate (Delta HR, 17 +/- A 2 bpm) and decrease in stroke volume (Delta SV, -28 +/- A 3 ml) on BR+0 were less than on BR-5 (24 +/- A 2 bpm, -43 +/- A 4 ml). On BR+1 Delta HR in the control group (33 +/- A 4 bpm) was higher than in the treatment group (23 +/- A 2 bpm) but there were no group differences on BR+3. Wearing the GCG prevented the orthostatic intolerance that is normally present after BR. Thigh-high garments provided protection after BR, and wearing these garments did not impair recovery. C1 [Stenger, Michael B.; Lee, Stuart M. C.; Ribeiro, L. Christine; Phillips, Tiffany R.] Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA. [Ploutz-Snyder, Robert J.; Westby, Christian M.] Univ Space Res Assoc, Houston, TX USA. [Willig, Michael C.] JES Tech, Houston, TX USA. [Platts, Steven H.] NASA, Lyndon B Johnson Space Ctr, Biomed Res & Environm Sci Div, Houston, TX 77058 USA. RP Stenger, MB (reprint author), Wyle Sci Technol & Engn Grp, 1290 Hercules Ave, Houston, TX 77058 USA. EM michael.b.stenger@nasa.gov FU NASA; National Center for Advancing Translational Sciences, National Institutes of Health [1UL1RR029876-01] FX The authors would like to thank the subjects who participated in this study; Kevin Tucker and Mary Ann Hettich of BSN-medical, Inc. who collaborated in the design and constructed the GCG for this and our previous Space Shuttle study; the JSC Cardiovascular Laboratory personnel who were responsible for collecting and analyzing the cardiovascular data; the JSC Clinical Laboratory for analyzing the blood samples; the staff at the Flight Analogs Research Unit at UTMB-Galveston who supported the bed rest subjects and coordinated their efforts with ours for a successful project; and Jamie Guined and Jackie Reeves who provided editorial comments to this manuscript. This work was funded by the NASA Human Research Project and supported in part by grant 1UL1RR029876-01 from the National Center for Advancing Translational Sciences, National Institutes of Health. NR 33 TC 1 Z9 1 U1 1 U2 5 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1439-6319 EI 1439-6327 J9 EUR J APPL PHYSIOL JI Eur. J. Appl. Physiol. PD MAR PY 2014 VL 114 IS 3 BP 597 EP 608 DI 10.1007/s00421-013-2787-4 PG 12 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA AB2VT UT WOS:000331650900014 PM 24337701 ER PT J AU Moorhead, AV Wiegert, PA Cooke, WJ AF Moorhead, Althea V. Wiegert, Paul A. Cooke, William J. TI The meteoroid fluence at Mars due to Comet C/2013 A1 (Siding Spring) SO ICARUS LA English DT Article DE Comets, dust; Meteors; Mars ID FLUX MONITOR INSTRUMENT; MONTE-CARLO-SIMULATION; DUST MEASUREMENTS; BOWELL 1980B; DEEP-IMPACT; EVOLUTION; P/HALLEY; MODEL; APPARITIONS; ATMOSPHERES AB Long-period Comet C/2013 A1 (Siding Spring) will experience a close encounter with Mars on 2014 October 19. As of 2013 October 21, the distance of closest approach between the two is projected to be between 89,000 km and 173,000 km, with a nominal value of 131,000 km. Thus, a collision between the comet and the planet has been ruled out, but the comet's coma may very well envelop Mars and its man-made satellites. We present a simple analytic model of the dust component of cometary comae that describes the spatial distribution of cometary dust and meteoroids and their size distribution. We find that this model successfully reproduces, to within an order of magnitude, particle fluxes measured by spacecraft Giotto in the coma of 1P/Halley and by spacecraft Stardust in the coma of 81P/Wild 2. We apply our analytic model to C/2013 A1 (Siding Spring) and compute the expected total fluence of potentially damaging particles at Mars at the time of closest approach between the two bodies; we obtain a nominal fluence of 0.15 particles per square meter. We conduct numerical simulations of particle ejection from the comet's nucleus and compare the resulting spatial distribution with that of our analytic model, and conclude that our spherically symmetric analytic model is adequate for order-of-magnitude fluence estimates. (c) 2013 Elsevier Inc. All rights reserved. C1 [Moorhead, Althea V.] Geocent LLC, Jacobs ESSSA Grp, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Wiegert, Paul A.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Cooke, William J.] NASA Meteoroid Environm Off, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Moorhead, AV (reprint author), Geocent LLC, Jacobs ESSSA Grp, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM althea.moorhead@nasa.gov FU NASA [NNM12AA41C, NNX11AB76A]; Natural Sciences and Engineering Research Council of Canada FX This work was supported by NASA contract NNM12AA41C and NASA Cooperative Agreement NNX11AB76A. This work was also supported in part by the Natural Sciences and Engineering Research Council of Canada. NR 42 TC 14 Z9 14 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR 1 PY 2014 VL 231 BP 13 EP 21 DI 10.1016/j.icarus.2013.11.028 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB3CE UT WOS:000331668100002 ER PT J AU Smith, ML Claire, MW Catling, DC Zahnle, KJ AF Smith, Megan L. Claire, Mark W. Catling, David C. Zahnle, Kevin J. TI The formation of sulfate, nitrate and perchlorate salts in the martian atmosphere SO ICARUS LA English DT Article DE Mars; Mars, atmosphere; Photochemistry; Atmospheres, chemistry; Mars, surface ID PHOENIX LANDING SITE; GAS-PHASE REACTIONS; X-RAY SPECTROMETER; NATURAL PERCHLORATE; LOWER STRATOSPHERE; PHOTOCHEMICAL DATA; MERIDIANI-PLANUM; MARS; CHEMISTRY; CHLORINE AB In extremely arid regions on Earth, such as the Atacama Desert, nitrate, sulfate and perchlorate salts form in the atmosphere and accumulate on the surface from dry deposition according to diagnostic evidence in their oxygen isotopes. Salts of similar oxyanions should have formed in the atmosphere of Mars because of comparable photochemical reactions. We use a 1-D photochemical model to calculate the deposition rates of sulfate, nitrogen oxyanions, and perchlorate from Mars' atmosphere, given a plausible range of volcanic fluxes of sulfur- and chlorine-containing gases in the past. To calculate integrated fluxes over time, we assume that throughout the last 3 byr (the Amazonian eon), the typical background atmosphere would have been similar to today's cold and dry environment. If the soil has been mixed by impact perturbations to a characteristic depth of similar to 2 m during this time, given a time-average volcanic flux 0.1% of the modern terrestrial volcanic flux, the model suggests that the soil would have accumulated 1.0-1.7 wt.% SO42- and 0.2-0.4 wt.% N in the form of pernitrate (peroxynitrate) or nitrate. The calculated sulfate concentration is consistent with in situ observations of soils from rovers and landers and orbital gamma ray spectroscopy. However, nitrates or pernitrates are yet to be detected. The modeled formation of perchlorate via purely gas-phase oxidation of volcanically-derived chlorine is insufficient by orders of magnitude to explain 0.4-0.6 wt.% ClO4- measured by NASA's Phoenix Lander. The far smaller amount of ozone in the martian atmosphere compared to the terrestrial atmosphere and the colder, drier conditions are the cause of lower rates of gas phase oxidation of chlorine volatiles to perchloric acid. Our calculations imply that non-gas-phase processes not included in the photochemical model, such as heterogeneous reactions, are likely important for the formation of perchlorate and are yet to be identified. (c) 2013 The Authors. Published by Elsevier Inc. All rights reserved. C1 [Smith, Megan L.; Catling, David C.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. [Claire, Mark W.] Univ St Andrews, Dept Earth & Environm Sci, St Andrews KY16 9AL, Fife, Scotland. [Zahnle, Kevin J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Claire, Mark W.] Blue Marble Space Inst Sci, Seattle, WA 98145 USA. RP Smith, ML (reprint author), Univ Washington, Dept Earth & Space Sci, 4000 15th Ave NE, Seattle, WA 98195 USA. EM msmith25@u.washington.edu OI Catling, David/0000-0001-5646-120X FU NASA's Mars Fundamental Research Program [NNX10AN67G]; Mars Fundamental Research Program; National Science Foundation Integrative Graduate Education and Research Traineeship, under NSF-IGERT [DGE-9870713]; NAI Director's Discretionary Fund; NASA postdoctoral program FX This work was supported by NASA's Mars Fundamental Research Program through Grant NNX10AN67G awarded to DCC. KJZ also acknowledges support from Mars Fundamental Research Program. MLS acknowledges support from a National Science Foundation Integrative Graduate Education and Research Traineeship, under NSF-IGERT Grant DGE-9870713, Astrobiology: Life in and beyond Earth's Solar System. MWC acknowledges support from a 2011 NAI Director's Discretionary Fund award titled "Perchlorate, Water, and Life", along with a NASA postdoctoral program award to work at the Virtual Planetary Laboratory. MLS thanks Jim Kasting for helpful discussions about using the photochemical model. We also thank two anonymous reviewers for improving the scientific content and clarity of the paper. NR 114 TC 19 Z9 20 U1 7 U2 67 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 MAR 1 PY 2014 VL 231 BP 51 EP 64 DI 10.1016/j.icarus.2013.11.031 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB3CE UT WOS:000331668100005 ER PT J AU Poulet, F Carter, J Bishop, JL Loizeau, D Murchie, SM AF Poulet, F. Carter, J. Bishop, J. L. Loizeau, D. Murchie, S. M. TI Mineral abundances at the final four curiosity study sites and implications for their formation SO ICARUS LA English DT Article DE Mars, surface; Mineralogy ID MAWRTH VALLIS REGION; LANDING SITE; CLAY-MINERALS; HOLDEN CRATER; GALE CRATER; EARLY MARS; EVOLUTION; PHYLLOSILICATES; DEPOSITS; CRISM AB A component of the landing site selection process for the Mars Science Laboratory (MSL) involved the presence of phyllosilicates as the main astrobiological targets. Gale crater was selected as the MSL landing site from among 4 down selected study sites (Gale, Eberswalde and Holden craters, Mawrth Vallis) that addressed the primary scientific goal of assessing the past habitability of Mars. A key constraint on the formation process of these phyllosilicate-bearing deposits is in the precise mineralogical composition. We present a reassessment of the mineralogy of the sites combined with a determination of the modal mineralogy of the major phyllosilicate-bearing deposits of the four final study sites from the modeling of near-infrared spectra using a radiative transfer model. The largest abundance of phyllosilicates (30-70%) is found in Mawrth Vallis, the lowest one in Eberswalde (<25%). Except for Mawrth Vallis, the anhydrous phases (plagioclase, pyroxenes and martian dust) are the dominant phases, suggesting formation conditions with a lower alteration grade and/or a post-formation mixing with anhydrous phases. The composition of Holden layered deposits (mixture of saponite and micas with a total abundance in the range of 25-45%) suggests transport and deposition of altered basalts of the Noachian crust without major chemical transformation. For Eberswalde, the modal mineralogy is also consistent with detrital clays, but the presence of opaline silica indicates that an authigenic formation occurred during the deposition. The overall composition including approximately 20-30% smectite detected by MSL in the rocks of Yellow-knife Bay area interpreted to be material deposited on the floor of Gale crater by channels (http://www.nasa.gov/mission_pages/msl/news/ms120130312.html) is consistent with the compositions modeled for the Eberswalde and Holden deltaic rocks. At Gale, the paucity, the small diversity and the low abundance of nontronite do not favor a complex and long drainage system. Localized aqueous processes in space and time environments could have produced both nontronites and sulfates. However, most materials in Gale are unfortunately dust covered, so that orbital data are limited by spatial resolution and surficial fines that could dilute and obscure the spectral influence of phyllosilicates in the rocks. Potential formation processes of diverse and abundant Mawrth Vallis deposits include low temperature hydrothermal alteration in marine environments and/or pedogenesis. (c) 2013 Elsevier Inc. All rights reserved. C1 [Poulet, F.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France. [Carter, J.] European So Observ, Santiago 19, Chile. [Bishop, J. L.] SETI Inst, Mountain View, CA 94043 USA. [Bishop, J. L.] NASA, Ames Res Ctr, Mountain View, CA 94043 USA. [Loizeau, D.] Univ Lyon 1, LGLTPE, F-69622 Villeurbanne, France. [Murchie, S. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Poulet, F (reprint author), Univ Paris 11, CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France. EM francois.poulet@ias.u-psud.fr RI Murchie, Scott/E-8030-2015 OI Murchie, Scott/0000-0002-1616-8751 NR 62 TC 16 Z9 16 U1 6 U2 31 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 MAR 1 PY 2014 VL 231 BP 65 EP 76 DI 10.1016/j.icarus.2013.11.023 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB3CE UT WOS:000331668100006 ER PT J AU Gao, P Zhang, X Crisp, D Bardeen, CG Yung, YL AF Gao, Peter Zhang, Xi Crisp, David Bardeen, Charles G. Yung, Yuk L. TI Bimodal distribution of sulfuric acid aerosols in the upper haze of Venus SO ICARUS LA English DT Article DE Atmospheres, composition; Atmospheres, structure; Atmospheres, dynamics; Venus; Venus, atmosphere ID COMPRESSIBLE CONVECTION; PHYSICAL PROCESSES; MIDDLE ATMOSPHERE; TRANSPORT MODEL; METEORIC ORIGIN; CLOUD; STRATOSPHERE; MESOSPHERE; VAPOR; PARTICLES AB Observations by the SPICAV/SOIR instruments aboard Venus Express have revealed that the upper haze (UH) of Venus, between 70 and 90 km, is variable on the order of days and that it is populated by two particle modes. We use a one-dimensional microphysics and vertical transport model based on the Community Aerosol and Radiation Model for Atmospheres to evaluate whether interaction of upwelled cloud particles and sulfuric acid particles nucleated in situ on meteoric dust are able to generate the two observed modes, and whether their observed variability are due in part to the action of vertical transient winds at the cloud tops. Nucleation of photochemically produced sulfuric acid onto polysulfur condensation nuclei generates mode I cloud droplets, which then diffuse upwards into the UH. Droplets generated in the UH from nucleation of sulfuric acid onto meteoric dust coagulate with the upwelled cloud particles and therefore cannot reproduce the observed bimodal size distribution. By comparison, the mass transport enabled by transient winds at the cloud tops, possibly caused by sustained subsolar cloud top convection, are able to generate a bimodal size distribution in a time scale consistent with Venus Express observations. Below the altitude where the cloud particles are generated, sedimentation and vigorous convection causes the formation of large mode 2 and mode 3 particles in the middle and lower clouds. Evaporation of the particles below the clouds causes a local sulfuric acid vapor maximum that results in upwelling of sulfuric acid back into the clouds. In the case where the polysulfur condensation nuclei are small and their production rate is high, coagulation of small droplets onto larger droplets in the middle cloud may set up an oscillation in the size modes of the particles such that precipitation of sulfuric acid "rain" may be possible immediately below the clouds once every few Earth months. Reduction of the polysulfur condensation nuclei production rate destroys this oscillation and reduces the mode 1 particle abundance in the middle cloud by two orders of magnitude. However, it better reproduces the sulfur-to-sulfuric-acid mass ratio in the cloud and haze droplets as constrained by fits to UV reflectivity data. In general we find satisfactory agreement between our nominal and transient wind results and observations from Pioneer Venus, Venus Express, and Magellan, though improvements could be made by incorporating sulfur microphysics. (c) 2013 Elsevier Inc. All rights reserved. C1 [Gao, Peter; Zhang, Xi; Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Zhang, Xi] Univ Arizona, Lunar & Planetary Lab, Dept Planetary Sci, Tucson, AZ 85721 USA. [Crisp, David] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bardeen, Charles G.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. RP Gao, P (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM pgao@caltech.edu OI Gao, Peter/0000-0002-8518-9601 FU Venus Express program via NASA [NNX10AP80G]; NAI Virtual Planetary Laboratory grant from the University of Washington; California Institute of Technology; National Aeronautics and Space Administration FX We thank S. Garimella and R.L. Shia for assistance with the setting up and running of the CARMA code. We thank R.W. Carlson and C. Parkinson for their valuable inputs. We thank C. Li for his help in speeding up our model runs by more than a factor of 10. This research was supported in part by the Venus Express program via NASA NNX10AP80G grant to the California Institute of Technology, and in part by an NAI Virtual Planetary Laboratory grant from the University of Washington to the Jet Propulsion Laboratory and California Institute of Technology. Part of the research described here was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 70 TC 6 Z9 6 U1 1 U2 13 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 MAR 1 PY 2014 VL 231 BP 83 EP 98 DI 10.1016/j.icarus.2013.10.013 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB3CE UT WOS:000331668100008 ER PT J AU Hayne, PO Paige, DA Heavens, NG AF Hayne, Paul O. Paige, David A. Heavens, Nicholas G. CA Mars Climate Sounder Science Team TI The role of snowfall in forming the seasonal ice caps of Mars: Models and constraints from the Mars Climate Sounder SO ICARUS LA English DT Article DE Mars; Mars, polar caps; Mars, atmosphere; Mars, climate; Atmospheres, structure ID ORBITER LASER ALTIMETER; MARTIAN POLAR CAPS; GENERAL-CIRCULATION; VERTICAL STRUCTURE; SOUTH-POLE; ATMOSPHERE; CLOUDS; TEMPERATURES; ALBEDO; VENUS AB Wintertime observations of the martian polar regions by orbiting spacecraft have provided evidence for carbon dioxide clouds, which measurably alter the polar energy budget and the annual CO2 cycle. However, it has remained unclear whether snowfall contributes a substantial quantity to the accumulating seasonal ice caps. We develop models to constrain precipitation rates based on observations of south polar CO2 clouds by the Mars Climate Sounder (MCS), and show that snowfall contributes between 3% and 20% by mass to the seasonal deposits at latitudes 70-90 degrees S. The lower bound on this estimate depends on a minimum effective cloud particle size of similar to 50 mu m, derived by comparing the short lifetimes (less than a few hours) of some clouds with calculated sedimentation velocities. Separate constraints from infrared spectra measured by MCS suggest CO2 cloud particles in the size range 10-100 mu m. Snow particles are not likely to re-sublime before reaching the surface, because the lower atmosphere in this region remains near saturation with respect to CO2. Based on cooling rate calculations, snowfall originating below 4 km altitude likely contributes a comparable or greater amount to the seasonal deposits than the rest of the atmosphere. Due to the positive feedback between cloud particle number density and radiative cooling, CO2 snow clouds should propagate until they become limited by the availability of condensation nuclei or CO2 gas. Over the south polar residual cap, where cloud activity is greatest, atmospheric radiative cooling rates are high enough to offset heat advected into the polar regions and maintain consistent snowfall. At latitudes of 60-80 degrees S the lower atmosphere tends to be slightly sub-saturated and rapid cooling by mechanical lift driven by orography or convergent flow may be required to initiate a snowstorm, consistent with the more sporadic clouds observed by MCS in this region, and their correlation with topographic features. Snowfall and accumulation at the surface are found to be inevitable consequences of the polar energy budget, unless advection redistributes heat from lower latitudes in much greater quantities than expected. (c) 2013 Elsevier Inc. All rights reserved. C1 [Hayne, Paul O.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. [Paige, David A.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. [Heavens, Nicholas G.] Hampton Univ, Dept Atmospher & Planetary Sci, Hampton, VA 23668 USA. RP Hayne, PO (reprint author), CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. EM Paul.O.Hayne@jpl.nasa.gov OI Heavens, Nicholas/0000-0001-7654-503X FU National Aeronautics and Space Administration FX We gratefully acknowledge fruitful discussions with J. Shirley, D. Kass, J.T. Schofield, D. McCleese, and A. Colaprete. The paper also benefited from the criticism of two anonymous reviewers. Part of this research was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 43 TC 9 Z9 9 U1 1 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR 1 PY 2014 VL 231 BP 122 EP 130 DI 10.1016/j.icarus.2013.10.020 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB3CE UT WOS:000331668100011 ER PT J AU Fletcher, LN de Pater, I Orton, GS Hammel, HB Sitko, ML Irwin, PGJ AF Fletcher, Leigh N. de Pater, Imke Orton, Glenn S. Hammel, Heidi B. Sitko, Michael L. Irwin, Patrick G. J. TI Neptune at summer solstice: Zonal mean temperatures from ground-based observations, 2003-2007 SO ICARUS LA English DT Article DE Neptune; Atmospheres, composition; Atmospheres, structure ID ROTOTRANSLATIONAL ABSORPTION-SPECTRA; HERSCHEL-PACS OBSERVATIONS; CLOUD STRUCTURE; INFRARED OBSERVATIONS; VOYAGER MEASUREMENTS; THERMAL STRUCTURE; ADAPTIVE OPTICS; LONG-WAVELENGTH; KECK TELESCOPE; OUTER PLANETS AB Imaging and spectroscopy of Neptune's thermal infrared emission from Keck/LWS (2003), Gemini-N/MICHELLE (2005); VLT/VISIR (2006) and Gemini-S/TReCS (2007) is used to assess seasonal changes in Neptune's zonal mean temperatures between Voyager-2 observations (1989, heliocentric longitude L-s = 236 degrees) and southern summer solstice (2005, L-s = 270 degrees). Our aim was to analyse imaging and spectroscopy from multiple different sources using a single self-consistent radiative-transfer model to assess the magnitude of seasonal variability. Globally-averaged stratospheric temperatures measured from methane emission tend towards a quasi-isothermal structure (158-164 K) above the 0.1-mbar level, and are found to be consistent with spacecraft observations of AKARI. This remarkable consistency, despite very different observing conditions, suggests that stratospheric temporal variability, if present, is <+/- 5 K at 1 mbar and <+/- 3 K at 0.1 mbar during this solstice period. Conversely, ethane emission is highly variable, with abundance determinations varying by more than a factor of two (from 500 to 1200 ppb at 1 mbar). The retrieved C2H6 abundances are extremely sensitive to the details of the T(p) derivation, although the underlying cause of the variable ethane emission remains unidentified. Stratospheric temperatures and ethane are found to be latitudinally uniform away from the south pole (assuming a latitudinally-uniform distribution of stratospheric methane), with no large seasonal hemispheric asymmetries evident at solstice. At low and mid-latitudes, comparisons of synthetic Voyager-era images with solstice-era observations suggest that tropospheric zonal temperatures are unchanged since the Voyager 2 encounter, with cool mid-latitudes and a warm equator and pole. A re-analysis of Voyager/IRIS 25-50 mu m mapping of tropospheric temperatures and para-hydrogen disequilibrium (a tracer for vertical motions) suggests a symmetric meridional circulation with cold air rising at mid-latitudes (sub-equilibrium para-H-2 conditions) and warm air sinking at the equator and poles (super-equilibrium para-H-2 conditions). The most significant atmospheric changes have occurred at high southern latitudes, where zonal temperatures retrieved from 2003 images suggest a polar enhancement of 7-8 K above the tropopause, and an increase of 5-6 K throughout the 70-90 degrees S region between 0.1 and 200 mbar. Such a large perturbation, if present in 1989, would have been detectable by Voyager/IRIS in a single scan despite its long-wavelength sensitivity, and we conclude that Neptune's south polar cyclonic vortex increased in strength significantly from Voyager to solstice. (c) 2013 Elsevier Inc. All rights reserved. C1 [Fletcher, Leigh N.; Irwin, Patrick G. J.] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England. [de Pater, Imke] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Hammel, Heidi B.] Assoc Univ Res Astron, Washington, DC 20005 USA. [Hammel, Heidi B.] Space Sci Inst, Boulder, CO 80301 USA. [Sitko, Michael L.] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA. [Orton, Glenn S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Fletcher, LN (reprint author), Univ Oxford, Dept Phys, Clarendon Lab, Pk Rd, Oxford OX1 3PU, England. EM fletcher@atm.ox.ac.uk RI Fletcher, Leigh/D-6093-2011; OI Fletcher, Leigh/0000-0001-5834-9588; Irwin, Patrick/0000-0002-6772-384X FU Royal Society Research Fellowship at the University of Oxford; W.M. Keck Foundation; National Science Foundation Science and Technology Center for Adaptive Optics [AST 9876783]; NSF [AST-0908575]; NASA; Science and Technology Facilities Council (STFC) FX Fletcher was supported during this research by a Royal Society Research Fellowship at the University of Oxford. Some of the data presented here were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. This investigation was partially based on VLT/ VISIR observations acquired at the Paranal UT3/Melipal Observatory under ID 077.C-0571; and on Gemini MICHELLE and TReCS observations acquired under ID GN-2005A-DD-10 and ID GS2007B-Q-47 at the Gemini Observatory, which is operated by AURA, Inc., under an NSF cooperative agreement on behalf of the Gemini partnership.This work has been supported in part by the National Science Foundation Science and Technology Center for Adaptive Optics, managed by the University of California at Santa Cruz under cooperative agreement No. AST 9876783, and by NSF Grant AST-0908575 to UC Berkeley. Orton was supported by grants fro NASA to the Jet Propulsion Laboratory, California Institute of Technology. The UK authors acknowledge the support of the Science and Technology Facilities Council (STFC).We thank T. Greathouse for providing the Neptune T(p) structure derived for the October 2007 TEXES observations, and for interesting discussions about the nature of these results. We also thank R. Campbell at Keck user support for providing details of the historical filters on Keck/LWS; and M. Gustafsson for providing collision-induced absorption coefficients for a range of para-H2 fractions pertinent to Neptune's atmosphere. Finally, we thank two anonymous reviewers for helping to improve the quality of this manuscript. The UK authors acknowledge the support of the Science and Technology Facilities Council (STFC). NR 67 TC 9 Z9 9 U1 1 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 MAR 1 PY 2014 VL 231 BP 146 EP 167 DI 10.1016/j.icarus.2013.11.035 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB3CE UT WOS:000331668100014 ER PT J AU Mckay, AJ Chanoyer, NJ DiSanti, MA Morgenthaler, JP Cochran, AL Harris, WM Dello Russo, N AF Mckay, Adam J. Chanoyer, Nancy J. DiSanti, Michael A. Morgenthaler, Jeffrey P. Cochran, Anita L. Harris, Walter M. Dello Russo, Neil TI Rotational variation of daughter species production rates in Comet 103P/Hartley: Implications for the progeny of daughter species and the. degree of chemical heterogeneity SO ICARUS LA English DT Article DE Comets; Comets, coma; Comets, composition ID NARROW-BAND PHOTOMETRY; FORBIDDEN OXYGEN LINES; H2O PRODUCTION-RATES; HALE-BOPP; FLUORESCENCE EFFICIENCIES; OH; SPECTROPHOTOMETRY; PHOTOCHEMISTRY; ATMOSPHERES; CHEMISTRY AB We present analysis of high spectral resolution optical spectra of Comet 103P/Hartley taken during its Fall 2010 apparition. These spectra include transitions belonging to CN, C-2, CH, NH2, and OI. We measure production rates and mixing ratios from these spectra. We find evidence for large changes in production rates (factors of a few) over the course of a nucleus rotation, in agreement with other measurements. We also measure variability with rotational phase in the CN/H2O and C-2/CN ratios, which has not been previously reported for any comet. There may also be variability in the NH2/H2O ratio with rotational phase, but this trend is not as clear as for CN/H2O. We interpret the changing mixing ratios as due to H2O and C-2 being released primarily from the icy grain halo, while the CN parent molecule comes directly from the nucleus. There is evidence that the CH/CN ratio is higher pre-perihelion than post-perihelion. We conclude that the observed CN and NH2 abundances are consistent with HCN and NH3 being the dominant parent molecules for these species. The C-2 and CH abundances are higher than those of candidate parent molecules (C2H2 and CH4 respectively), so there must be another source for these molecules in 103P's coma. Carbonaceous dust grains could serve as this source. (c) 2013 Elsevier Inc. All rights reserved. C1 [Mckay, Adam J.; Chanoyer, Nancy J.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88001 USA. [DiSanti, Michael A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Morgenthaler, Jeffrey P.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Cochran, Anita L.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Harris, Walter M.] Univ Calif Davis, Dept Appl Sci, Davis, CA 95616 USA. [Dello Russo, Neil] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Mckay, AJ (reprint author), New Mexico State Univ, Dept Astron, 1320 Frenger Mall, Las Cruces, NM 88001 USA. EM amckay@nmsu.edu; nchanove@nmsu.edu; Michael.A.Disanti@nasa.gov; jpmorgen@psi.edu; anita@barolo.as.utexas.edu; wmharris@ucdavis.edu; neil.dello.russo@jhuapl.edu RI Dello Russo, Neil/G-2727-2015 OI Dello Russo, Neil/0000-0002-8379-7304 FU NASA GSRP Fellowship program [NNX11AO03H] FX We thank John Barentine, Jurek Krzesinski, Chris Churchill, Pey Lian Lim, Paul Strycker, and Doug Hoffman for developing and optimizing the ARCES IRAF reduction script used to reduce these data. We would also like to acknowledge the JPL Horizons System, which was used to generate ephemerides for nonsidereal tracking of the comets during the observations, and the SIMBAD database, which was used for selection of reference stars. We thank Hideyo Kawakita for providing us with the latest g-factors for NH2 and Dennis Bodewits for discussing results of the DIXI mission with us. This work is supported by the NASA GSRP Fellowship program through Grant No. NNX11AO03H. We appreciate the comments of two anonymous referees that improved the quality of this paper. NR 46 TC 6 Z9 6 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR 1 PY 2014 VL 231 BP 193 EP 205 DI 10.1016/j.icarus.2013.11.029 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB3CE UT WOS:000331668100017 ER PT J AU Bandfield, JL Song, E Hayne, PO Brand, BD Ghent, RR Vasavada, AR Paige, DA AF Bandfield, Joshua L. Song, Eugenie Hayne, Paul O. Brand, Brittany D. Ghent, Rebecca R. Vasavada, Ashwin R. Paige, David A. TI Lunar cold spots: Granular flow features and extensive insulating materials surrounding young craters SO ICARUS LA English DT Article DE Moon, surface; Impact processes; Infrared observations; Regoliths ID BASIN DEPOSITS; EMPLACEMENT; EJECTA; MOON; IMPACT AB Systematic temperature mapping and high resolution images reveal a previously unrecognized class of small, fresh lunar craters. These craters are distinguished by near-crater deposits with evidence for lateral, ground-hugging transport. More distal, highly insulating surfaces surround these craters and do not show evidence of either significant deposition of new material or erosion of the substrate. The near-crater deposits can be explained by a laterally propagating granular flow created by impact in the lunar vacuum environment. Further from the source crater, at distances of similar to 10-100 crater radii, the upper few to 10s of centimeters of regolith appear to have been "fluffed-up" without the accumulation of significant ejecta material. These properties appear to be common to all impacts, but quickly degrade in the lunar space weathering environment. Cratering in the vacuum environment involves a previously unrecognized set of processes that leave prominent, but ephemeral, features on the lunar surface. (c) 2013 Elsevier Inc. All rights reserved. C1 [Bandfield, Joshua L.] Space Sci Inst, Boulder, CO 80301 USA. [Song, Eugenie] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Hayne, Paul O.; Vasavada, Ashwin R.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Brand, Brittany D.] Boise State Univ, Dept Geosci, Boise, ID 83725 USA. [Ghent, Rebecca R.] Univ Toronto, Dept Geol, Toronto, ON M5S 1A1, Canada. [Paige, David A.] Univ Calif Los Angeles, Los Angeles, CA 90024 USA. RP Bandfield, JL (reprint author), Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA. EM jbandfield@spacescience.org NR 35 TC 7 Z9 7 U1 1 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR 1 PY 2014 VL 231 BP 221 EP 231 DI 10.1016/j.icarus.2013.12.017 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB3CE UT WOS:000331668100019 ER PT J AU Rathbun, JA Spencer, JR Lopes, RM Howell, RR AF Rathbun, J. A. Spencer, J. R. Lopes, R. M. Howell, R. R. TI Io's active volcanoes during the New Horizons era: Insights from New Horizons imaging SO ICARUS LA English DT Article DE IO; Satellites, surfaces; Volcanism ID JUPITERS MOON IO; GALILEO NIMS; ERUPTION; PELE; TEMPERATURES; VARIABILITY; ECLIPSE; CASSINI; MISSION; AURORAE AB In February 2007, the New Horizons spacecraft flew by the Jupiter system, obtaining images of Io, the most volcanically active body in the Solar System. The Multicolor Visible Imaging Camera (MVIC), a four-color (visible to near infrared) camera, obtained 17 sets of images. The Long-Range Reconnaissance Imager (LORRI), a high-resolution panchromatic camera, obtained 190 images, including many of Io eclipsed by Jupiter. We present a complete view of the discrete point-like emission sources in all images obtained by these two instruments. We located 54 emission sources and determined their brightnesses. These observations, the first that observed individual Ionian volcanoes on short timescales of seconds to minutes, demonstrate that the volcanoes have stable brightnesses on these timescales. The active volcanoes Tvashtar (63N, 124W) and E. Girru (22N, 245W) were observed by both LORRI and MVIC, both in the near-infrared (NIR) and methane (CH4) filters. Tvashtar was additionally observed in the red filter, which allowed us to calculate a color temperature of approximately 1200 K. We found that, with some exceptions, most of the volcanoes frequently active during the Galileo era continued to be active during the New Horizons flyby. We found that none of the seven volcanoes observed by New Horizons multiple times over short timescales showed substantial changes on the order of seconds and only one, E. Girru exhibited substantial variation over minutes to days, increasing by 25% in just over an hour and decreasing by a factor of 4 over 6 days. Observations of Tvashtar are consistent with a current eruption similar to previously observed eruptions and are more consistent with the thermal emission of a lava flow than the fire fountains inferred from the November 1999 observations. These data also present new puzzles regarding Ionian volcanism. Since there is no associated surface change or low albedo feature that could be identified nearby, the source of the emission from E. Girru is a mystery. Furthermore, the in-eclipse glows we observe over many paterae are likely to be gas emission from interaction with the magnetosphere, but the details of that process are not clear. (c) 2013 Elsevier Inc. All rights reserved. C1 [Rathbun, J. A.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Spencer, J. R.] SW Res Inst, Boulder, CO 80302 USA. [Lopes, R. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Howell, R. R.] Univ Wyoming, Laramie, WY 82071 USA. RP Rathbun, JA (reprint author), Planetary Sci Inst, 1700 E Ft Lowell, Tucson, AZ 85719 USA. EM rathbun@psi.edu RI Lopes, Rosaly/D-1608-2016 OI Lopes, Rosaly/0000-0002-7928-3167 FU NASA; NASA Jupiter Data Analysis Program; JPL summer faculty Fellowship program FX We would like to thank Lucas Kamp, who assisted with data reduction, Eric Bloss and Kyle McMillian, who assisted as summer undergraduate researchers, and two anonymous reviewers. Part of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. This project was supported by the NASA Jupiter Data Analysis Program and the JPL summer faculty Fellowship program. NR 26 TC 4 Z9 4 U1 2 U2 26 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 MAR 1 PY 2014 VL 231 BP 261 EP 272 DI 10.1016/j.icarus.2013.12.002 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB3CE UT WOS:000331668100022 ER PT J AU Lellouch, E Bezard, B Flasar, FM Vinatier, S Achterberg, R Nixon, CA Bjoraker, GL Gorius, N AF Lellouch, E. Bezard, B. Flasar, F. M. Vinatier, S. Achterberg, R. Nixon, C. A. Bjoraker, G. L. Gorius, N. TI The distribution of methane in Titan's stratosphere from Cassini/CIRS observations SO ICARUS LA English DT Article DE Titan, atmosphere; Atmospheres, composition; Atmospheres, structure; Atmospheres, dynamics; Spectroscopy ID MOLECULAR SPECTROSCOPIC DATABASE; COMPOSITE INFRARED SPECTROMETER; CM(-1) SPECTRAL RANGE; ATMOSPHERIC TEMPERATURES; SURFACE TEMPERATURES; RADIO OCCULTATIONS; HUYGENS PROBE; ABUNDANCE; PROFILES; DYNAMICS AB Cassini/CIRS spectra in the far- and mid-infrared region are used to determine the abundance of methane in Titan's lower stratosphere and investigate its distribution with latitude. The CIRS spectra include emission from both the CH4 v(4) band at 7.7 mu m and pure rotational lines longwards of 50 mu m, which show differential sensitivities to thermal profile and methane mole fraction. We analyze nadir and limb data taken over the first part of the Cassini mission (August 2005 to June 2010), including a selection of 12 latitudes that provides a reasonably complete and regular sampling of both hemispheres. Unexpectedly, but in a consistent manner for limb and nadir geometries, large variations of the methane mole fraction near 15 mbar (similar to 85 km) are found, with values ranging from similar to 1.0% (at low latitudes and near +/- 50-55 degrees) to similar to 1.5% (at +/- 30-35 degrees and polar latitudes). Error bars on the retrieved methane mole fraction are 0.07-0.12% at low latitudes in the Southern hemisphere and 0.14-0.21% northward of 40 degrees N. A 1.0% methane mole fraction at low latitudes permits us to reconcile the HASI-measured temperatures below 147 km altitude (2.7 mbar) with inferences from CIRS. The roughly hemispherically-symmetric distribution of methane gas is reminiscent of that observed or predicted for the tropospheric methane clouds, which on a yearly-averaged basis, show preferential occurrences at tropical and polar latitudes. We speculate that convective events at these latitudes result into local stratospheric methane enrichment, which may persist year-round due to dynamical mixing times in the lower stratosphere only moderately shorter than a Titan year. (C) 2013 Elsevier Inc. All rights reserved. C1 [Lellouch, E.; Bezard, B.; Vinatier, S.] UPMC, Univ Paris Diderot, Observ Paris, LESIA, F-92195 Meudon, France. [Flasar, F. M.; Achterberg, R.; Nixon, C. A.; Bjoraker, G. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gorius, N.] Catholic Univ Amer, IACS, Washington, DC 20064 USA. RP Lellouch, E (reprint author), UPMC, Univ Paris Diderot, Observ Paris, LESIA, F-92195 Meudon, France. EM emmanuel.lellouch@obspm.fr RI Flasar, F Michael/C-8509-2012; Nixon, Conor/A-8531-2009 OI Nixon, Conor/0000-0001-9540-9121 NR 58 TC 13 Z9 13 U1 0 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR 1 PY 2014 VL 231 BP 323 EP 337 DI 10.1016/j.icarus.2013.12.016 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB3CE UT WOS:000331668100027 ER PT J AU Han, JW Meyyappan, M AF Han, Jin-Woo Meyyappan, Meyya TI Trigger and Self-Latch Mechanisms of n-p-n Bistable Resistor SO IEEE ELECTRON DEVICE LETTERS LA English DT Article DE Self latch; n-p-n device; floating base; bistable resistor; biristor AB Trigger and self-latch mechanisms in n-p-n bistable resistor (biristor) were investigated. A two terminal vertical n-p-n biristor with floating p-type base was fabricated on a bulk silicon wafer. The temperature and current compliance effects on the current-voltage characteristics were analyzed to understand the underlying physical mechanism. The fact that the current compliance is temperature independent suggests that latch-up is triggered by band-to-band tunneling. In contrast, the high temperature and current compliance diminished the latch-down and hysteresis loop, which reveals that impact ionization is responsible for self-latching at bistable regime. C1 [Han, Jin-Woo; Meyyappan, Meyya] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Han, JW (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. EM jin-woo.han@nasa.gov NR 8 TC 1 Z9 1 U1 1 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0741-3106 EI 1558-0563 J9 IEEE ELECTR DEVICE L JI IEEE Electron Device Lett. PD MAR PY 2014 VL 35 IS 3 BP 387 EP 389 DI 10.1109/LED.2013.2297277 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA AB8GV UT WOS:000332029200032 ER PT J AU Boyce, BL Kramer, SLB Fang, HE Cordova, TE Neilsen, MK Dion, K Kaczmarowski, AK Karasz, E Xue, L Gross, AJ Ghahremaninezhad, A Ravi-Chandar, K Lin, SP Chi, SW Chen, JS Yreux, E Ruter, M Qian, D Zhou, Z Bhamare, S O'Connor, DT Tang, S Elkhodary, KI Zhao, J Hochhalter, JD Cerrone, AR Ingraffea, AR Wawrzynek, PA Carter, BJ Emery, JM Veilleux, MG Yang, P Gan, Y Zhang, X Chen, Z Madenci, E Kilic, B Zhang, T Fang, E Liu, P Lua, J Nahshon, K Miraglia, M Cruce, J DeFrese, R Moyer, ET Brinckmann, S Quinkert, L Pack, K Luo, M Wierzbicki, T AF Boyce, B. L. Kramer, S. L. B. Fang, H. E. Cordova, T. E. Neilsen, M. K. Dion, K. Kaczmarowski, A. K. Karasz, E. Xue, L. Gross, A. J. Ghahremaninezhad, A. Ravi-Chandar, K. Lin, S. -P. Chi, S. -W. Chen, J. S. Yreux, E. Ruter, M. Qian, D. Zhou, Z. Bhamare, S. O'Connor, D. T. Tang, S. Elkhodary, K. I. Zhao, J. Hochhalter, J. D. Cerrone, A. R. Ingraffea, A. R. Wawrzynek, P. A. Carter, B. J. Emery, J. M. Veilleux, M. G. Yang, P. Gan, Y. Zhang, X. Chen, Z. Madenci, E. Kilic, B. Zhang, T. Fang, E. Liu, P. Lua, J. Nahshon, K. Miraglia, M. Cruce, J. DeFrese, R. Moyer, E. T. Brinckmann, S. Quinkert, L. Pack, K. Luo, M. Wierzbicki, T. TI The Sandia Fracture Challenge: blind round robin predictions of ductile tearing SO INTERNATIONAL JOURNAL OF FRACTURE LA English DT Article DE Fracture; Tearing; Deformation; Ductility; Failure; Damage; Crack initiation ID POLYCRYSTALLINE AL 6061-T6; KERNEL PARTICLE METHODS; FATIGUE-CRACK GROWTH; LARGE-DEFORMATION; FAILURE BEHAVIOR; GURSON MODEL; SHEAR; DAMAGE; PROPAGATION; PLASTICITY AB Existing and emerging methods in computational mechanics are rarely validated against problems with an unknown outcome. For this reason, Sandia National Laboratories, in partnership with US National Science Foundation and Naval Surface Warfare Center Carderock Division, launched a computational challenge in mid-summer, 2012. Researchers and engineers were invited to predict crack initiation and propagation in a simple but novel geometry fabricated from a common off-the-shelf commercial engineering alloy. The goal of this international Sandia Fracture Challenge was to benchmark the capabilities for the prediction of deformation and damage evolution associated with ductile tearing in structural metals, including physics models, computational methods, and numerical implementations currently available in the computational fracture community. Thirteen teams participated, reporting blind predictions for the outcome of the Challenge. The simulations and experiments were performed independently and kept confidential. The methods for fracture prediction taken by the thirteen teams ranged from very simple engineering calculations to complicated multiscale simulations. The wide variation in modeling results showed a striking lack of consistency across research groups in addressing problems of ductile fracture. While some methods were more successful than others, it is clear that the problem of ductile fracture prediction continues to be challenging. Specific areas of deficiency have been identified through this effort. Also, the effort has underscored the need for additional blind prediction-based assessments. C1 [Boyce, B. L.; Kramer, S. L. B.; Fang, H. E.; Cordova, T. E.; Neilsen, M. K.; Dion, K.; Kaczmarowski, A. K.; Karasz, E.; Emery, J. M.; Veilleux, M. G.] Sandia Natl Labs, Albuquerque, NM 87185 USA. [Xue, L.] Schlumberger, Sugar Land, TX USA. [Gross, A. J.; Ravi-Chandar, K.] Univ Texas Austin, Austin, TX 78712 USA. [Ghahremaninezhad, A.] Univ Miami, Coral Gables, FL 33124 USA. [Lin, S. -P.; Chen, J. S.; Yreux, E.; Ruter, M.] Univ Calif Los Angeles, Los Angeles, CA USA. [Chi, S. -W.] Univ Illinois, Chicago, IL USA. [Qian, D.; Zhou, Z.] Univ Texas Dallas, Dallas, TX 75230 USA. [Bhamare, S.] Univ Cincinnati, Cincinnati, OH USA. [O'Connor, D. T.; Zhao, J.] Northwestern Univ, Evanston, IL USA. [Tang, S.] Chongqing Univ, Chongqing 630044, Peoples R China. [Elkhodary, K. I.] Amer Univ Cairo, Dept Mech Engn, Cairo, Egypt. [Hochhalter, J. D.] NASA Langley, Hampton, VA USA. [Cerrone, A. R.; Ingraffea, A. R.; Wawrzynek, P. A.; Carter, B. J.] Cornell Univ, Ithaca, NY USA. [Yang, P.; Zhang, X.] Tsinghua Univ, Beijing 100084, Peoples R China. [Gan, Y.] Zhejiang Univ, Hangzhou 310027, Peoples R China. [Chen, Z.] Univ Missouri, Columbia, MO USA. [Chen, Z.] Dalian Univ Technol, Dalian, Peoples R China. [Madenci, E.; Kilic, B.] Univ Arizona, Tucson, AZ USA. [Zhang, T.; Fang, E.; Liu, P.; Lua, J.] Global Engn & Mat Inc, Princeton, NJ USA. [Nahshon, K.; Miraglia, M.; Cruce, J.; DeFrese, R.; Moyer, E. T.] Naval Surface Warfare Ctr Carderock Div, Washington, DC USA. [Brinckmann, S.] Max Planck Inst Eisenforsch GmbH, D-40074 Dusseldorf, Germany. [Quinkert, L.] Ruhr Univ Bochum, Bochum, Germany. [Pack, K.; Luo, M.; Wierzbicki, T.] MIT, Cambridge, MA 02139 USA. RP Boyce, BL (reprint author), Sandia Natl Labs, POB 5800, Albuquerque, NM 87185 USA. EM blboyce@sandia.gov RI Xue, Liang/A-1266-2007; Qian, Dong/B-2326-2008; Luo, Meng/J-3829-2013; Brinckmann, Steffen/G-7075-2011; OI Xue, Liang/0000-0003-0468-0624; Qian, Dong/0000-0001-9367-0924; Brinckmann, Steffen/0000-0003-0930-082X; Elkhodary, Khalil/0000-0002-0249-5751; Emery, John /0000-0001-6671-4952 NR 71 TC 23 Z9 23 U1 1 U2 58 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0376-9429 EI 1573-2673 J9 INT J FRACTURE JI Int. J. Fract. PD MAR PY 2014 VL 186 IS 1-2 SI SI BP 5 EP 68 DI 10.1007/s10704-013-9904-6 PG 64 WC Materials Science, Multidisciplinary; Mechanics SC Materials Science; Mechanics GA AB2XB UT WOS:000331654300002 ER PT J AU Benafan, O Brown, J Calkins, FT Kumar, P Stebner, AP Turner, TL Vaidyanathan, R Webster, J Young, ML AF Benafan, O. Brown, J. Calkins, F. T. Kumar, P. Stebner, A. P. Turner, T. L. Vaidyanathan, R. Webster, J. Young, M. L. TI Shape memory alloy actuator design: CASMART collaborative best practices and case studies SO INTERNATIONAL JOURNAL OF MECHANICS AND MATERIALS IN DESIGN LA English DT Article DE CASMART; Shape memory alloy (SMA); Actuator design methodology; Adaptive/active structures; Smart materials, structures and systems ID MULTIVARIANT MICROMECHANICAL MODEL; 3-DIMENSIONAL CONSTITUTIVE MODEL; PRECISION TRACKING CONTROL; SEVERE PLASTIC-DEFORMATION; THERMAL CONDUCTION SWITCH; ACTIVE POSITION CONTROL; JET ENGINE CHEVRON; NICKEL-TITANIUM; STAINLESS-STEEL; MECHANICAL-PROPERTIES AB One goal of the Consortium for the Advancement of Shape Memory Alloy Research and Technology is to compile the collective design experiences of our member organizations into a single medium that researchers and engineers may use to make efficient and effective decisions when developing shape memory alloy (SMA) components and systems. Recent work toward this goal is presented through the framework of six fundamental design aspects we have identified, which include evaluation, alloy selection, processing and fabrication, testing and properties, modeling, and system integration considerations including control system design. Each aspect is documented in the light of enabling the design engineer to access the tools and information needed to successfully design and develop SMA systems. Application of these aspects is illustrated through case studies resulting from our own SMA designs. It is shown that there is not an obvious single, linear route a designer can adopt to navigate the path from concept to product. Each application brings unique challenges that demand a particular emphasis and priority for each engineering aspect involved in the development of a system actuated by SMAs. C1 [Benafan, O.] NASA Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. [Brown, J.] Dynalloy Inc, Tustin, CA 92780 USA. [Calkins, F. T.] Boeing Co, Seattle, WA 98124 USA. [Kumar, P.] Texas A&M Univ, Dept Aerosp Engn, College Stn, TX 77843 USA. [Stebner, A. P.] Northwestern Univ, Dept Mech Engn, Evanston, IL 60208 USA. [Turner, T. L.] NASA Langley Res Ctr, Struct Acoust Branch, Hampton, VA 23681 USA. [Vaidyanathan, R.] Univ Cent Florida, Adv Mat Proc & Anal Ctr AMPAC, Mech Mat & Aerosp Engn Dept, Orlando, FL 32816 USA. [Webster, J.] Rolls Royce PLC, Derby DE2 8BJ, England. [Young, M. L.] ATI Wah Chang, Albany, OR 97321 USA. [Young, M. L.] Univ N Texas, Dept Mat Sci & Engn, Denton, TX 76203 USA. RP Benafan, O (reprint author), NASA Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. EM othmane.benafan@nasa.gov RI Kumar, Prem/B-6691-2009; Stebner, Aaron/A-7685-2015 FU CASMART's member institutions FX This work documents many years of effort from multiple organizations, encompassing support from numerous programs and funding agencies, and we thank them all. We also acknowledge CASMART's member institutions for their support of our consortium. NR 230 TC 10 Z9 11 U1 1 U2 19 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1569-1713 EI 1573-8841 J9 INT J MECH MATER DES JI Int. J. Mech. Mater. Des. PD MAR PY 2014 VL 10 IS 1 BP 1 EP 42 DI 10.1007/s10999-013-9227-9 PG 42 WC Engineering, Civil; Engineering, Mechanical; Materials Science, Multidisciplinary; Mechanics SC Engineering; Materials Science; Mechanics GA AB3TP UT WOS:000331713400001 ER PT J AU Strizik, L Zhang, J Wagner, T Oswald, J Kohoutek, T Walsh, BM Prikryl, J Svoboda, R Liu, C Frumarova, B Frumar, M Pavlista, M Park, WJ Heo, J AF Strizik, L. Zhang, J. Wagner, T. Oswald, J. Kohoutek, T. Walsh, B. M. Prikryl, J. Svoboda, R. Liu, C. Frumarova, B. Frumar, M. Pavlista, M. Park, W. J. Heo, J. TI Green, red and near-infrared photon up-conversion in Ga-Ge-Sb-S:Er3+ amorphous chalcogenides SO JOURNAL OF LUMINESCENCE LA English DT Article DE Er3+; Ga-Ge-Sb-S; Chalcogenide glasses; Up-conversion; Upconversion; Judd-Ofelt analysis ID JUDD-OFELT PARAMETERS; SURFACE-PLASMON RESONANCE; ER3+ IONS; PHOSPHATE-GLASSES; SB-S; OPTICAL-TRANSITIONS; LASER; FIBERS; GA; DEPENDENCE AB We report on compositional tuning in Et3+ ions doped Ga-Ge-Sb-S glassy system allowing for effective H-2(11/2) -> I-4(15/2) (530 nm), S-4(3/2) -> I-4(15/2) (550 nm), F-4(9/2) -> I-4(15/2) (660 mm), I-4(9/2) -> I-4(15/2) ( 810 nm), I-4(11/2) -> I-4(15/2) (990 nm) intra-4f electronic transition emissions of Er3+ ions under 808 nm, 980 nm or 1550 nm laser pumping. We changed the composition of well-known Ge20Ga5Sb10S65 glass to Ge25Ga10-xSbxS65, where x=0.5 at%, 2.5 at% or 5.0 at% and doped it with 0.5 at% of Er3+ ions. The short-wavelength absorption edge of the studied glassy hosts is blue-shifted by substitution of Sb with Ga to similar to 500 nm making the green emission at 530 nm and 550 nm and even 495 nm (F-4(7/2)-> I-4(15/2)) observable, while the glass stability was kept high characterized with the difference of T-c-T-g>100 K and mean coordination numbers 2.67-2.71. Up-conversion emission decay times of all anti-Stokes emissions were in the range of 0.2-2.1 ms. The influence of Ga substitution with Sb on the structure and the optical properties was investigated. The spectroscopic parameters for Er3+ ions with local environment change were analyzed based on Judd-Ofelt theory. (C) 2013 Elsevier B.V. All rights reserved. C1 [Strizik, L.; Wagner, T.; Kohoutek, T.; Prikryl, J.; Frumar, M.] Univ Pardubice, Fac Chem Technol, Dept Gen & Inorgan Chem, Pardubice 53210, Czech Republic. [Zhang, J.; Park, W. J.; Heo, J.] Pohang Univ Sci & Technol POSTECH, Dept Mat Sci & Engn, Ctr Informat Mat, Div Adv Nucl Engn, Pohang 790784, Gyeongbuk, South Korea. [Oswald, J.] Acad Sci Czech Republic, Inst Phys, Vvi, CR-16200 Prague, Czech Republic. [Walsh, B. M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Svoboda, R.] Univ Pardubice, Fac Chem Technol, Dept Phys Chem, Pardubice 53210, Czech Republic. [Liu, C.] Wuhan Univ Technol, State Key Lab Silicate Mat Architectures, Wuhan 430070, Hubei, Peoples R China. [Frumarova, B.] Acad Sci Czech Republic, Inst Macromol Chem, Vvi, Prague, Czech Republic. [Pavlista, M.] Univ Pardubice, Fac Chem Technol, Dept Appl Phys & Math, Pardubice 53210, Czech Republic. RP Strizik, L (reprint author), Univ Pardubice, Fac Chem Technol, Dept Gen & Inorgan Chem, Studentska 573, Pardubice 53210, Czech Republic. EM lukas.strizik@centrum.cz RI Liu, Chao/B-4938-2008; Kohoutek, Tomas/F-2199-2014; Frumarova, Bozena/G-7819-2014; Oswald, Jiri/G-9721-2014 OI Liu, Chao/0000-0003-4324-6409; Oswald, Jiri/0000-0003-3332-2121 FU project "ReAdMat - Research Team for Advanced Non Crystalline Materials" [CZ.1.07/2.3.00/20.0254]; European Social Fund; state budget of the Czech Republic; Grant Agency of the Czech Republic [203/09/0827]; project KONTAKT II [LH11101] FX The authors gratefully acknowledge support from the project CZ.1.07/2.3.00/20.0254 "ReAdMat - Research Team for Advanced Non Crystalline Materials" co-financed by the European Social Fund and the state budget of the Czech Republic, Grant Agency of the Czech Republic grant 203/09/0827, project KONTAKT II no. LH11101. The authors thank Prof. Koichi Shimakawa (University of Pardubice, Czech Republic) and Prof. Takeshi Aoki (Tokyo Polytechnic University, Japan) for fruitful discussion. NR 67 TC 5 Z9 5 U1 5 U2 48 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-2313 EI 1872-7883 J9 J LUMIN JI J. Lumines. PD MAR PY 2014 VL 147 BP 209 EP 215 DI 10.1016/j.jlumin.2013.11.021 PG 7 WC Optics SC Optics GA AB3CC UT WOS:000331667900034 ER PT J AU He, H Loughner, CP Stehr, JW Arkinson, HL Brent, LC Follette-Cook, MB Tzortziou, MA Pickering, KE Thompson, AM Martins, DK Diskin, GS Anderson, BE Crawford, JH Weinheimer, AJ Lee, P Hains, JC Dickerson, RR AF He, Hao Loughner, Christopher P. Stehr, Jeffrey W. Arkinson, Heather L. Brent, Lacey C. Follette-Cook, Melanie B. Tzortziou, Maria A. Pickering, Kenneth E. Thompson, Anne M. Martins, Douglas K. Diskin, Glenn S. Anderson, Bruce E. Crawford, James H. Weinheimer, Andrew J. Lee, Pius Hains, Jennifer C. Dickerson, Russell R. TI An elevated reservoir of air pollutants over the Mid-Atlantic States during the 2011 DISCOVER-AQ campaign: Airborne measurements and numerical simulations SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Bay Breeze; CMAQ simulations; DISCOVER-AQ campaign ID 2003 HEAT-WAVE; UNITED-STATES; TROPOSPHERIC OZONE; MODELING SYSTEM; AASE-II; POLLUTION; SENSITIVITY; CHEMISTRY; PROFILES; EPISODE AB During a classic heat wave with record high temperatures and poor air quality from July 18 to 23, 2011, an elevated reservoir of air pollutants was observed over and downwind of Baltimore, MD, with relatively clean conditions near the surface. Aircraft and ozonesonde measurements detected similar to 120 ppbv ozone at 800 m altitude, but similar to 80 ppbv ozone near the surface. High concentrations of other pollutants were also observed around the ozone peak: similar to 300 ppbv CO at 1200 m, similar to 2 ppbv NO2 at 800 m, similar to 5 ppbv SO2 at 600 m, and strong aerosol optical scattering (2 x 10(-4) m(-1)) at 600 m. These results suggest that the elevated reservoir is a mixture of automobile exhaust (high concentrations of O-3, CO, and NO2) and power plant emissions (high SO2 and aerosols). Back trajectory calculations show a local stagnation event before the formation of this elevated reservoir. Forward trajectories suggest an influence on downwind air quality, supported by surface ozone observations on the next day over the downwind PA, NJ and NY area. Meteorological observations from aircraft and ozonesondes show a dramatic veering of wind direction from south to north within the lowest 5000 m, implying that the development of the elevated reservoir was caused in part by the Chesapeake Bay breeze. Based on in situ observations, CMAQ forecast simulations with 12 km resolution overestimated surface ozone concentrations and failed to predict this elevated reservoir; however, CMAQ research simulations with 4 km and 1.33 km resolution moresuccessfully reproduced this event. These results show that high resolution is essential for resolving coastal effects and predicting air quality for cities near major bodies of water such as Baltimore on the Chesapeake Bay and downwind areas in the Northeast. (C) 2013 Elsevier Ltd. All rights reserved. C1 [He, Hao; Loughner, Christopher P.; Tzortziou, Maria A.; Dickerson, Russell R.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [He, Hao; Stehr, Jeffrey W.; Arkinson, Heather L.; Dickerson, Russell R.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Loughner, Christopher P.; Tzortziou, Maria A.; Pickering, Kenneth E.; Thompson, Anne M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Brent, Lacey C.; Dickerson, Russell R.] Univ Maryland, Dept Chem & Biochem, College Pk, MD 20740 USA. [Follette-Cook, Melanie B.] Morgan State Univ, Baltimore, MD 21251 USA. [Follette-Cook, Melanie B.] Univ Space Res Assoc, Columbia, MD 21004 USA. [Thompson, Anne M.; Martins, Douglas K.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Diskin, Glenn S.; Anderson, Bruce E.; Crawford, James H.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Weinheimer, Andrew J.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Lee, Pius] NOAA, Air Resource Lab, College Pk, MD 20740 USA. [Hains, Jennifer C.] Maryland Dept Environm, Baltimore, MD 21230 USA. RP He, H (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. EM hhe@atmos.umd.edu RI Pickering, Kenneth/E-6274-2012; He, Hao/E-4771-2015; Lee, Pius/D-5201-2016; Dickerson, Russell/F-2857-2010; Thompson, Anne /C-3649-2014; OI Dickerson, Russell/0000-0003-0206-3083; Thompson, Anne /0000-0002-7829-0920; Loughner, Christopher/0000-0002-3833-2014 FU National Aeronautics and Space Administration (NASA); Maryland Department of the Environment; NASA Ozone Monitoring Instrument (OMI) Team; NASA Air Quality Applied Science Team (AQAST) [NNX11AK34G, NNX12AI18G, NNX10AQ79G] FX The DISCOVER-AQ campaign is supported by the National Aeronautics and Space Administration (NASA). We thank Maryland Department of the Environment for the support to the UMD RAMMPP program. We thank Dr. Ronald C. Cohen (University of California, Berkeley) for providing TD-LIF NO2 measurements. This research was supported by NASA Ozone Monitoring Instrument (OMI) Team and NASA Air Quality Applied Science Team (AQAST) grants NNX11AK34G, NNX12AI18G and NNX10AQ79G. NR 55 TC 14 Z9 14 U1 5 U2 52 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD MAR PY 2014 VL 85 BP 18 EP 30 DI 10.1016/j.atmosenv.2013.11.039 PG 13 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AA9MN UT WOS:000331417700003 ER PT J AU Yew, AG Atencia, J Hsieh, AH AF Yew, Alvin G. Atencia, Javier Hsieh, Adam H. TI Lab-on-Chip Clinorotation System for Live-Cell Microscopy Under Simulated Microgravity SO CELLULAR AND MOLECULAR BIOENGINEERING LA English DT Article DE Space biology; Clinostat; Real-time microscopy; Stem cell; Gravisensing ID MESENCHYMAL STEM-CELLS; MODELED MICROGRAVITY; US ASTRONAUTS; DIFFERENTIATION; ADIPOGENESIS; EXPOSURE AB Cells in microgravity are subject to mechanical unloading and changes to the surrounding chemical environment. How these factors jointly influence cellular function is not well understood. Ground-based analogues can be used to investigate their role in spaceflight, where mechanical unloading is simulated through the time-averaged nullification of gravity. The prevailing method for cellular microgravity simulation is to use devices called clinostats, or rotating wall vessel bioreactors. However, conventional clinostats are not designed for temporally tracking cell response, nor are they able to establish dynamic fluid environments. To address these needs, we developed a Clinorotation Time-lapse Microscopy (CTM) system, an experimental method that accommodates lab-on-chip cell culture devices for visualizing time-dependent alterations to cellular behavior. For the purpose of demonstrating CTM, we present preliminary results showing time-dependent differences in cell area between human mesenchymal stem cells (hMSCs) under modeled microgravity and normal gravity. C1 [Yew, Alvin G.] NASA GSFC, Greenbelt, MD 20771 USA. [Atencia, Javier; Hsieh, Adam H.] Univ Maryland, Dept Bioengn, College Pk, MD 20742 USA. RP Yew, AG (reprint author), NASA GSFC, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM Alvin.G.Yew@nasa.gov OI Hsieh, Adam/0000-0003-3162-1152 FU National Aeronautics and Space Administration [NNX13AM06G]; National Institute of Standards and Technology [70NANB11H191] FX We would like to thank Julianne Twomey for helping to maintain stem cell cultures, Ben Chinn for contributions to the CTM control system, Abby Iacangelo for fabricating cell culture microfluidic devices, and Kiran Bhadriraju for insightful discussions. This work was funded by the National Aeronautics and Space Administration (NNX13AM06G) and the National Institute of Standards and Technology (70NANB11H191). NR 20 TC 0 Z9 0 U1 1 U2 12 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1865-5025 EI 1865-5033 J9 CELL MOL BIOENG JI Cell. Mol. Bioeng. PD MAR PY 2014 VL 7 IS 1 BP 165 EP 170 DI 10.1007/s12195-013-0319-2 PG 6 WC Cell & Tissue Engineering; Biophysics; Cell Biology SC Cell Biology; Biophysics GA AB1JA UT WOS:000331546100015 ER PT J AU Barge, LM Doloboff, IJ Russell, MJ VanderVelde, D White, LM Stucky, GD Baum, MM Zeytounian, J Kidd, R Kanik, I AF Barge, Laura M. Doloboff, Ivria J. Russell, Michael J. VanderVelde, David White, Lauren M. Stucky, Galen D. Baum, Marc M. Zeytounian, John Kidd, Richard Kanik, Isik TI Pyrophosphate synthesis in iron mineral films and membranes simulating prebiotic submarine hydrothermal precipitates SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID GREEN RUST; INORGANIC PYROPHOSPHATE; MOLECULAR EVOLUTION; PHOSPHATE; LIFE; ORIGIN; PHOSPHORYLATION; ENERGY; ACID; POLYPHOSPHATE AB Cells use three main ways of generating energy currency to drive metabolism: (i) conversion of adenosine diphosphate (ADP) to adenosine triphosphate (ATP) by the proton motive force through the rotor-stator ATP synthase; (ii) the synthesis of inorganic phosphate similar to phosphate bonds via proton (or sodium) pyrophosphate synthase; or (iii) substrate-level phosphorylation through the direct donation from an active phosphoryl donor. A mechanism to produce a pyrophosphate bond as "energy currency" in prebiotic systems is one of the most important considerations for origin of life research. Baltscheffsky (1996) suggests that inorganic pyrophosphate (P2O74-; PPi) may have preceded ATP/ADP as an energy storage molecule in earliest life, produced by an H+ pyrophosphatase. Here we test the hypothesis that PPi could be synthesized in inorganic precipitates simulating hydrothermal chimney structures transected by thermal and/or ionic gradients. Appreciable yields of PPi were obtained via substrate phosphorylation by acetyl phosphate within the iron sulfide/silicate precipitates at temperatures expected for an alkaline hydrothermal system. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Barge, Laura M.; Doloboff, Ivria J.; Russell, Michael J.; White, Lauren M.; Kidd, Richard; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [VanderVelde, David] CALTECH, Dept Chem, Pasadena, CA 91125 USA. [White, Lauren M.; Stucky, Galen D.] Univ Calif Santa Barbara, Dept Chem & Biochem, Santa Barbara, CA 93106 USA. [Baum, Marc M.] Oak Crest Inst Sci, Dept Chem, Pasadena, CA 91107 USA. [Zeytounian, John] Univ So Calif, Mol & Computat Biol Program, Los Angeles, CA 90089 USA. RP Barge, LM (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-601,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM laura.m.barge@jpl.nasa.gov FU National Aeronautics and Space Administration; NASA Astrobiology Institute (Icy Worlds); NAI through the NASA Postdoctoral Program; NASA Harriett G. Jenkins Pre-doctoral Fellowship Program; Corning Foundation FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration with support by the NASA Astrobiology Institute (Icy Worlds). We thank Andy Pratt for helpful comments on this manuscript and acknowledge useful discussions with Shawn McGlynn, Elbert Branscomb and members of the NAI-sponsored Thermodynamics Disequilibrium and Evolution Focus Group. L.M.B. is supported by the NAI through the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. L.M.W. is supported by the NASA Harriett G. Jenkins Pre-doctoral Fellowship Program with additional support from the Corning Foundation. NR 58 TC 13 Z9 13 U1 3 U2 37 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 MAR 1 PY 2014 VL 128 BP 1 EP 12 DI 10.1016/j.gca.2013.12.006 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AA4ZR UT WOS:000331105700001 ER PT J AU Madni, AM Sievers, M AF Madni, Azad M. Sievers, Michael TI Systems Integration: Key Perspectives, Experiences, and Challenges SO SYSTEMS ENGINEERING LA English DT Article DE systems integration; legacy integration; human-systems integration; semantic integration ID ENTERPRISE INTEGRATION; SOFTWARE; PLATFORM; DESIGN AB As systems continue to grow in scale and complexity, systems integration (SI) has become a key concern. This is especially the case in defense and aerospace. SI involves interfacing and enabling the interactions of component elements to collectively provide the functionality needed by the system to accomplish its goals. SI is part of the overall system development life cycle. SI increases in complexity when there are legacy systems that need to be integrated, and when humans are an integral part of the system. An added layer of complexity is introduced when the system has to exhibit resilience and adaptability in the face of contingencies in the operational environment. This paper addresses key perspectives and challenges in SI. Specifically, it presents the integration continuum, ranging from loose to tight integration. It presents a SI ontology that captures the key issues and concerns in a standard language. It also presents various categories of integration and their unique challenges. This paper is intended to clarify various types of integration and to stimulate new ways of thinking about SI. C1 [Madni, Azad M.] Univ So Calif, Viterbi Sch Engn, Daniel J Epstein Dept Ind & Syst Engn, Los Angeles, CA 90089 USA. [Sievers, Michael] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Madni, AM (reprint author), Univ So Calif, Viterbi Sch Engn, Daniel J Epstein Dept Ind & Syst Engn, Los Angeles, CA 90089 USA. EM azad.madni@usc.edu NR 54 TC 5 Z9 5 U1 1 U2 12 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1098-1241 EI 1520-6858 J9 SYSTEMS ENG JI Syst. Eng. PD MAR PY 2014 VL 17 IS 1 BP 37 EP 51 DI 10.1002/sys.21249 PG 15 WC Engineering, Industrial; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA AA5YA UT WOS:000331174300004 ER PT J AU Pannuti, TG Rho, J Heinke, CO Moffitt, WP AF Pannuti, Thomas G. Rho, Jeonghee Heinke, Craig O. Moffitt, William P. TI THE X-RAY PROPERTIES OF FIVE GALACTIC SUPERNOVA REMNANTS DETECTED BY THE SPITZER GLIMPSE SURVEY SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM: individual objects (SNR 304.6+0.1, SNR 311.5-0.3, SNR 346.6-0.2, SNR 348.5+0.1, SNR 348.5-0.0); ISM: supernova remnants; X-rays: ISM ID LARGE-AREA TELESCOPE; MHZ MASER EMISSION; GAS IMAGING SPECTROMETER; OPTICALLY THIN PLASMAS; SPACE-TELESCOPE; RADIO-SOURCES; XMM-NEWTON; FERMI-LAT; RECOMBINING PLASMA; INNER GALAXY AB We present a study of the X-ray properties of five Galactic supernova remnants (SNRs)-Kes 17 (G304.6 + 0.1), G311.5-0.3, G346.6-0.2, CTB 37A (G348.5 + 0.1), and G348.5-0.0-that were detected in the infrared by Reach et al. in an analysis of data from the Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE) that was conducted by the Spitzer Space Telescope. We present and analyze archival ASCA observations of Kes 17, G311.5-0.3, and G346.6-0.2, archival XMM-Newton observations of Kes 17, CTB 37A, and G348.5-0.0, and an archival Chandra observation of CTB 37A. All of the SNRs are clearly detected in the X-ray except possibly G348.5-0.0. Our study reveals that the four detected SNRs all feature center-filled X-ray morphologies and that the observed emission from these sources is thermal in all cases. We argue that these SNRs should be classified as mixed-morphology SNRs (MM SNRs); our study strengthens the correlation between MM SNRs and SNRs interacting with molecular clouds and suggests that the origin of MM SNRs may be due to the interactions between these SNRs and adjacent clouds. Our ASCA analysis of G311.5-0.3 reveals for the first time X-ray emission from this SNR: the X-ray emission is center-filled within the radio and infrared shells and thermal in nature (kT similar to 0.98 keV), thus motivating its classification as an MM SNR. We find considerable spectral variations in the properties associated with the plasmas of the other X-ray-detected SNRs, such as a possible overabundance of magnesium in the plasma of Kes 17. Our new results also include the first detailed spatially resolved spectroscopic study of CTB 37A using Chandra as well as a spectroscopic study of the discrete X-ray source CXOU J171428.5-383601, which may be a neutron star associated with CTB 37A. Finally, we also estimate such properties as electron density n(e), radiative age t(rad) and swept-up mass M-X for each of the four X-ray-detected SNRs. Each of these values are comparable to archetypal MM SNRs like 3C 391 and W44. In an analysis of the spectrum of Kes 17, we did not find evidence of overionization unlike other archetypal MM SNRs like W44 and W49B. C1 [Pannuti, Thomas G.; Moffitt, William P.] Morehead State Univ, Dept Earth & Space Sci, Ctr Space Sci, Morehead, KY 40351 USA. [Rho, Jeonghee] NASA, Ames Res Ctr, SETI Inst, Mountain View, CA 94035 USA. [Rho, Jeonghee] NASA, Ames Res Ctr, SOFIA Sci Ctr, Mountain View, CA 94035 USA. [Heinke, Craig O.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. RP Pannuti, TG (reprint author), Morehead State Univ, Dept Earth & Space Sci, Ctr Space Sci, 235 Martindale Dr, Morehead, KY 40351 USA. EM t.pannuti@moreheadstate.edu; jrho@sofia.usra.edu; heinke@ualberta.ca; w.moffitt@moreheadstate.edu OI Heinke, Craig/0000-0003-3944-6109 NR 106 TC 5 Z9 5 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAR PY 2014 VL 147 IS 3 AR 55 DI 10.1088/0004-6256/147/3/55 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5HB UT WOS:000331125600010 ER PT J AU Smith, BJ Soria, R Struck, C Giroux, ML Swartz, DA Yukita, M AF Smith, Beverly J. Soria, Roberto Struck, Curtis Giroux, Mark L. Swartz, Douglas A. Yukita, Mihoko TI EXTRA-NUCLEAR STARBURSTS: YOUNG LUMINOUS HINGE CLUMPS IN INTERACTING GALAXIES SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: individual (Arp 82, Arp 240, Arp 244, Arp 256, Arp 270, NGC 2207, NGC 2403); galaxies: interactions; galaxies: starburst ID HUBBLE-SPACE-TELESCOPE; STAR-FORMING GALAXIES; X-RAY-EMISSION; TIDAL DWARF GALAXIES; GLOBULAR-CLUSTER FORMATION; FORMATION RATE INDICATOR; TO-LIGHT RATIOS; ANTENNAE GALAXIES; SPIRAL GALAXIES; CHANDRA OBSERVATIONS AB Hinge clumps are luminous knots of star formation near the base of tidal features in some interacting galaxies. We use archival Hubble Space Telescope (HST) UV/optical/IR images and Chandra X-ray maps along with Galaxy Evolution Explorer UV, Spitzer IR, and ground-based optical/near-IR images to investigate the star forming properties in a sample of 12 hinge clumps in five interacting galaxies. The most extreme of these hinge clumps have star formation rates of 1-9 M-circle dot yr(-1), comparable to or larger than the "overlap" region of intense star formation between the two disks of the colliding galaxy system the Antennae. In the HST images, we have found remarkably large and luminous sources at the centers of these hinge clumps. These objects are much larger and more luminous than typical "super star clusters" in interacting galaxies, and are sometimes embedded in a linear ridge of fainter star clusters, consistent with star formation along a narrow caustic. These central sources have FWHM diameters of similar to 70 pc, compared to similar to 3 pc in "ordinary" super star clusters. Their absolute I magnitudes range from M-I similar to -12.2 to -16.5; thus, if they are individual star clusters they would lie near the top of the "super star cluster" luminosity function of star clusters. These sources may not be individual star clusters, but instead may be tightly packed groups of clusters that are blended together in the HST images. Comparison to population synthesis modeling indicates that the hinge clumps contain a range of stellar ages. This is consistent with expectations based on models of galaxy interactions, which suggest that star formation may be prolonged in these regions. In the Chandra images, we have found strong X-ray emission from several of these hinge clumps. In most cases, this emission is well-resolved with Chandra and has a thermal X-ray spectrum, thus it is likely due to hot gas associated with the star formation. The ratio of the extinction-corrected diffuse X-ray luminosity to the mechanical energy rate (the X-ray production efficiency) for the hinge clumps is similar to that in the Antennae galaxies, but higher than those for regions in the normal spiral galaxy NGC 2403. Two of the hinge clumps have point-like X-ray emission much brighter than expected for hot gas; these sources are likely "ultra-luminous X-ray sources" due to accretion disks around black holes. The most extreme of these sources, in Arp 240, has a hard X-ray spectrum and an absorbed X-ray luminosity of similar to 2 x 10(41) erg s(-1); this is above the luminosity expected by single high mass X-ray binaries (HMXBs), thus it may be either a collection of HMXBs or an intermediate mass black hole (>= 80 M-circle dot). C1 [Smith, Beverly J.; Giroux, Mark L.] E Tennessee State Univ, Dept Phys & Astron, Johnson City, TN 37614 USA. [Soria, Roberto] Curtin Univ, Curtin Inst Radio Astron, Bentley, WA 6102, Australia. [Struck, Curtis] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Swartz, Douglas A.] NASA, Univ Space Res Assoc, George C Marshall Space Flight Ctr, Huntsville, AL USA. [Yukita, Mihoko] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Smith, BJ (reprint author), E Tennessee State Univ, Dept Phys & Astron, Johnson City, TN 37614 USA. EM smithbj@etsu.edu; rsoria@physics.usyd.edu.au; curt@iastate.edu; girouxm@etsu.edu; myukita1@pha.jhu.edu OI Struck, Curtis/0000-0002-6490-2156 FU NASA [ADAP10-0005, NAS5-98034]; National Science Foundation [AST-1311935]; NASA; National Aeronautics and Space Administration; National Science Foundation FX This research was supported by NASA Astrophysics Data Analysis Grant ADAP10-0005 and National Science Foundation Extragalactic Astronomy grant AST-1311935. We thank the anonymous referee for helpful suggestions. We also thank Michele Kaufman, Debra Elmegreen, Hongxin Zhang, Yu Gao, Howard Bushouse, Javier Zaragoza-Cardiel, Marcel Clemens, and Liese van Zee for providing copies of their data and helpful communications. We thank Mark Hancock for the use of his scripts to determine population ages. This research has made use of the NASA/IPAC Extragalatic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory (JPL), California Institute of Technology under a contract with NASA. This research is also based in part 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 (STSci/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA). This study also uses data from the NASA Galaxy Evolution Explorer (GALEX), which was operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. This research has also made use of data obtained from the Chandra Data Archive and software provided by the Chandra X-ray Center (CXC). This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by JPL, the California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 159 TC 10 Z9 10 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAR PY 2014 VL 147 IS 3 AR 60 DI 10.1088/0004-6256/147/3/60 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5HB UT WOS:000331125600015 ER PT J AU Wright, EL Kirkpatrick, JD Gelino, CR Fajardo-Acosta, S Mace, G Eisenhardt, PR Stern, D McLean, IS Skrutskie, MF Oza, A Nelson, MJ Cushing, MC Reid, IN Fumagalli, M Burgasser, AJ AF Wright, Edward L. Kirkpatrick, J. Davy Gelino, Christopher R. Fajardo-Acosta, Sergio Mace, Gregory Eisenhardt, Peter R. Stern, Daniel McLean, Ian S. Skrutskie, M. F. Oza, Apurva Nelson, M. J. Cushing, Michael C. Reid, I. Neill Fumagalli, Michele Burgasser, Adam J. TI THE FIRST ALLWISE PROPER MOTION DISCOVERY: WISEA J070720.50+170532.7 SO ASTRONOMICAL JOURNAL LA English DT Article DE brown dwarfs; infrared: stars; solar neighborhood; stars: individual (WISEA J070720.50+170532.7); stars: late-type; stars: low-mass ID INFRARED-SURVEY-EXPLORER; WHITE-DWARF; SKY SURVEY; FIELD; SUBDWARFS; CATALOG; STARS AB While quality checking a new motion-aware co-addition of all 12.5 months of Wide-field Infrared Survey Explorer (WISE) data, we found that the source WISE J070720.48+170533.0 moved 0".9 in six months. Backtracking this motion allowed us to identify this source as 2MASS J07071961+1705464, with several entries in the USNO B catalog. An astrometric fit to these archival data gives a proper motion of mu = 1793 +/- 2 mas yr(-1) and a parallax of pi = 35 +/- 42 mas. Photometry from WISE, 2MASS, and the POSS can be fit reasonably well by a blackbody with T = 3658 K and an angular radius of 4.36 x 10 (11) radians. No clear evidence of H-2 collision-induced absorption is seen in the near-infrared. An optical spectrum shows broad deep CaH bands at 638 and 690 nm, broad deep Na D at 598.2 nm, and weak or absent TiO, indicating that this source is an ultra-subdwarf M star with a radial velocity v(rad) approximate to -21 +/- 18 km s(-1) relative to the Sun. Given its apparent magnitude, the distance is about 39 +/- 9 pc and the tangential velocity is probably approximate to 330 km s(-1), but a more precise parallax is needed to be certain. C1 [Wright, Edward L.; Mace, Gregory; McLean, Ian S.] UCLA Astron, Los Angeles, CA 90095 USA. [Kirkpatrick, J. Davy; Gelino, Christopher R.; Fajardo-Acosta, Sergio] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Eisenhardt, Peter R.; Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Skrutskie, M. F.; Oza, Apurva; Nelson, M. J.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Cushing, Michael C.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Reid, I. Neill] STScI, Baltimore, MD 21218 USA. [Fumagalli, Michele] Carnegie Observ, Pasadena, CA 91101 USA. [Fumagalli, Michele] Princeton Univ, Dept Astrophys, Princeton, NJ 08544 USA. [Burgasser, Adam J.] Univ Calif San Diego, La Jolla, CA 92093 USA. RP Wright, EL (reprint author), UCLA Astron, POB 951547, Los Angeles, CA 90095 USA. EM wright@astro.ucla.edu RI Fumagalli, Michele/K-9510-2015 OI Fumagalli, Michele/0000-0001-6676-3842 FU National Aeronautics and Space Administration; NASA [HF-51305.01-A] FX This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.; Support for M.F. was provided by NASA through Hubble Fellowship grant HF-51305.01-A NR 29 TC 4 Z9 4 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAR PY 2014 VL 147 IS 3 AR 61 DI 10.1088/0004-6256/147/3/61 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5HB UT WOS:000331125600016 ER PT J AU Zhang, C Binienda, WK Goldberg, RK Kohlman, LW AF Zhang, Chao Binienda, Wieslaw K. Goldberg, Robert K. Kohlman, Lee W. TI Meso-scale failure modeling of single layer triaxial braided composite using finite element method SO COMPOSITES PART A-APPLIED SCIENCE AND MANUFACTURING LA English DT Article DE Polymer-matrix composites (PMCs); Mechanical properties; Finite element analysis (FEA); Damage mechanics ID UNIDIRECTIONAL FIBER COMPOSITES; TEXTILE COMPOSITES; MECHANICAL-BEHAVIOR; PROGRESSIVE DAMAGE; STRENGTH; PREDICTION; CELLS AB In this study, a meso-scale finite element (FE) model of a triaxial braided composite is generated based on realistic unit cell dimensions and fiber bundle geometry parameters. Micromechanical finite element models were developed to predict the elastic and strength properties of each fiber bundle. These details are then applied in a 14 unit cells meso-mechanical finite element model for a 0 degrees/+60 degrees/-60 degrees triaxially braided T700s/E862 carbon/epoxy composite. Simulations of the axial tension and transverse tension response of a straight-sided, single layer coupon are conducted using this meso-scale model, and the predictions are compared to experimental results. By applying a periodic boundary condition in the loading direction and an accurate number of unit cells perpendicular to the free edge, the meso-scale model captures the local damage initiation and global failure behavior, as well as the periodic free edge distortion effect. The failure mechanisms are studied using the field strain and stress contours. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Zhang, Chao; Binienda, Wieslaw K.] Univ Akron, Dept Civil Engn, Akron, OH 44325 USA. [Goldberg, Robert K.; Kohlman, Lee W.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Zhang, C (reprint author), Univ Akron, Dept Civil Engn, Akron, OH 44325 USA. EM cz14@zips.uakron.edu RI Zhang, Chao/H-3397-2013 NR 41 TC 17 Z9 20 U1 1 U2 39 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1359-835X EI 1878-5840 J9 COMPOS PART A-APPL S JI Compos. Pt. A-Appl. Sci. Manuf. PD MAR PY 2014 VL 58 BP 36 EP 46 DI 10.1016/j.compositesa.2013.11.009 PG 11 WC Engineering, Manufacturing; Materials Science, Composites SC Engineering; Materials Science GA AA5TG UT WOS:000331161900006 ER PT J AU Kaynak, Y Tobe, H Noebe, RD Karaca, HE Jawahir, IS AF Kaynak, Y. Tobe, H. Noebe, R. D. Karaca, H. E. Jawahir, I. S. TI The effects of machining on the microstructure and transformation behavior of NiTi Alloy SO SCRIPTA MATERIALIA LA English DT Article DE NiTi; Shape memory alloys; Cryogenic machining; Machining-induced layer; Twinning deformation ID SHAPE-MEMORY ALLOY; CHANNEL ANGULAR EXTRUSION; DEFORMATION; TI50NI47FE3; MARTENSITE AB This study presents evidence of a machining-induced deformation layer in a NiTi shape memory alloy and the subsequent effect of this layer on the underlying transformation behavior of the material. Severe twinning-induced deformation was observed in the substrate of samples pre-cooled and machined by orthogonal cutting under cryogenic conditions, while (1 1 4)(B2)-type deformation twinning and significant dislocation activity was observed after dry machining of the NiTi. In addition, cryogenic machining resulted in a much deeper affected zone than machining under dry conditions. (C) 2013 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved. C1 [Kaynak, Y.; Tobe, H.; Karaca, H. E.; Jawahir, I. S.] Univ Marmara, Mech & Machine Elements Div, TR-34722 Istanbul, Turkey. [Kaynak, Y.; Tobe, H.; Karaca, H. E.; Jawahir, I. S.] Univ Kentucky, Inst Sustainable Mfg, Lexington, KY 40506 USA. [Kaynak, Y.; Tobe, H.; Karaca, H. E.; Jawahir, I. S.] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA. [Noebe, R. D.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. RP Kaynak, Y (reprint author), Univ Marmara, Mech & Machine Elements Div, Goztepe Campus, TR-34722 Istanbul, Turkey. EM yusuf.kaynak@marmara.edu.tr RI Jawahir, I.S./E-8447-2014 FU NASA EPSCOR Program [NNX11AQ31A]; NASA FAP Aeronautical Sciences Project FX Support from the NASA EPSCOR Program under Grant no. NNX11AQ31A and the NASA FAP Aeronautical Sciences Project are greatly acknowledged. NR 19 TC 13 Z9 13 U1 2 U2 29 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-6462 J9 SCRIPTA MATER JI Scr. Mater. PD MAR PY 2014 VL 74 BP 60 EP 63 DI 10.1016/j.scriptamat.2013.10.023 PG 4 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA AA2HH UT WOS:000330915200013 ER PT J AU Meyyappan, M AF Meyyappan, Meyya TI Welcome to Materials Research Express SO MATERIALS RESEARCH EXPRESS LA English DT Editorial Material C1 [Meyyappan, Meyya] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Meyyappan, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM m.meyyappan@nasa.gov NR 0 TC 0 Z9 0 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2053-1591 J9 MATER RES EXPRESS JI Mater. Res. Express PD MAR PY 2014 VL 1 IS 1 AR 010201 DI 10.1088/2053-1591/01/1/015001 PG 2 WC Materials Science, Multidisciplinary SC Materials Science GA V43EQ UT WOS:000209665100001 ER PT J AU Lyman, TC Virgin, LN Davis, RB AF Lyman, Theodore C. Virgin, Lawrence N. Davis, R. Benjamin TI Application of Continuation Methods to Uniaxially Loaded Postbuckled Plates SO JOURNAL OF APPLIED MECHANICS-TRANSACTIONS OF THE ASME LA English DT Article ID THERMALLY BUCKLED PLATES; FINITE-ELEMENT-ANALYSIS; RECTANGULAR-PLATES; GEOMETRICALLY IMPERFECT; CYLINDRICAL-SHELLS; SNAP-THROUGH; FLAT-PLATE; COMPRESSION; BIFURCATION; VIBRATION AB Continuation methods are used to examine the static and dynamic postbuckled behavior of a uniaxially loaded, simply supported plate. Continuation methods have been extensively used to study problems in mathematics and physics; however, they have not been as widely applied to problems in engineering. When paired with a Galerkin approximation, continuation methods are shown to be well suited to solving nonlinear buckling problems. In addition to providing a robust solution method for nonlinear equations, the linearized Jacobians from the continuation steps will contain natural frequency and mode shape information for mechanical systems (provided inertia terms are included). Results for the primary buckling branch are compared to previously published results. Using the open-source continuation package AUTO, stable, remote secondary buckling branches were discovered. These secondary stable equilibrium persist even in the presence of geometric imperfections and their existence is confirmed by experiment. C1 [Lyman, Theodore C.; Virgin, Lawrence N.] Duke Univ, Dept Mech Engn & Mat Sci, Durham, NC 27708 USA. [Davis, R. Benjamin] NASA, Struct Dynam & Anal Branch ER41, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Lyman, TC (reprint author), Duke Univ, Dept Mech Engn & Mat Sci, Durham, NC 27708 USA. EM theodore.lyman@duke.edu; l.virgin@duke.edu; robert.b.davis@nasa.gov OI Davis, R Benjamin /0000-0003-4478-302X FU NASA Graduate Student Researchers Program (GSRP) Grant [NNX09AJ17H]; Air Force Office of Scientific Research Grant [FA9550-09-1-0204] FX The authors would like to acknowledge the NASA Graduate Student Researchers Program (GSRP) Grant No. NNX09AJ17H and the Air Force Office of Scientific Research Grant No. FA9550-09-1-0204 for support. NR 39 TC 0 Z9 0 U1 0 U2 6 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 0021-8936 EI 1528-9036 J9 J APPL MECH-T ASME JI J. Appl. Mech.-Trans. ASME PD MAR PY 2014 VL 81 IS 3 AR 031010 DI 10.1115/1.4024672 PG 10 WC Mechanics SC Mechanics GA 298UN UT WOS:000330350100010 ER PT J AU Sun, JQ Xiong, XX Madhavan, S Wenny, BN AF Sun, Junqiang Xiong, Xiaoxiong Madhavan, Sriharsha Wenny, Brian N. TI Terra MODIS Band 27 Electronic Crosstalk Effect and Its Removal SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Crosstalk; Moderate Resolution Imaging Spectroradiometer (MODIS); moon; striping; terra; thermal emissive bands (TEBs) ID REFLECTIVE SOLAR BANDS; ON-ORBIT CALIBRATION; PERFORMANCE AB gThe Moderate Resolution Imaging Spectroradiometer (MODIS) is one of the primary instruments in the National Aeronautics and Space Administration Earth observing system. The first MODIS instrument was launched in December, 1999 onboard the Terra spacecraft. MODIS has 36 bands, covering a wavelength range 0.4-14.4 mu m. MODIS band 27 (6.72 mu m) is a water vapor band, which is designed to be insensitive to Earth surface features. In recent Earth view images of Terra band 27, surface feature contamination is clearly seen with pronounced striping. In this paper, it is shown that these band-27 issues are caused by electronic crosstalk from bands 28-30. An algorithm using a linear approximation is developed to correct the crosstalk effect. The crosstalk coefficients are derived from Terra MODIS lunar observations. They show that the crosstalk is strongly detector-dependent and the crosstalk pattern has changed in a noticeable fashion since launch. The crosstalk contributions were positive to the instrument response of band 27 early in the mission but became negative and much larger in magnitude at later stages of the mission for most detectors of the band. The algorithms are applied to both the black body (BB) calibration and the MODIS L1B calibrated products. With the crosstalk effect significantly removed, the calibration coefficients of Terra MODIS band 27 derived from the BB show that the detector differences become smaller. With the algorithms applied to MODIS L1B products, the Earth surface features are significantly removed, thereby restoring the radiometric balance of the band and substantially reducing the striping features in the image. C1 [Sun, Junqiang; Wenny, Brian N.] Sigma Space Corp, Lanham, MD 20706 USA. [Xiong, Xiaoxiong] NASA, Sci & Explorat Directorate, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Madhavan, Sriharsha] Sci & Syst Applicat Inc, Lanham, MD 20706 USA. RP Sun, JQ (reprint author), Sigma Space Corp, Lanham, MD 20706 USA. EM junqiang.sun@sigmaspace.com; Xiaoxiong.Xiong-1@nasa.gov; sriharsha.madhavan@ssaihq.com; brian.wenny@sigmaspace.com NR 12 TC 21 Z9 23 U1 2 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD MAR PY 2014 VL 52 IS 3 BP 1551 EP 1561 DI 10.1109/TGRS.2013.2252180 PG 11 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 285PA UT WOS:000329404800002 ER PT J AU Smith, GL Priestley, KJ Loeb, NG AF Smith, George Louis Priestley, Kory J. Loeb, Norman G. TI Clouds and Earth Radiant Energy System: From Design to Data SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Aqua; Clouds and the Earth's Radiant Energy System (CERES); Earth Observing System; earth radiation budget; NPOESS Preparatory Project (NPP); Terra ID RAINFALL MEASURING MISSION; THERMISTOR BOLOMETER SENSORS; ANGULAR-DISTRIBUTION MODELS; RADIATION BUDGET EXPERIMENT; SCANNING RADIOMETER; TERRA SPACECRAFT; FLUX ESTIMATION; CERES; VALIDATION; SATELLITE AB The Clouds and the Earth's Radiant Energy System (CERES) project has instruments aboard the Terra and Aqua spacecraft that have provided a decade of radiation budget data. In October 2011, the CERES flight model 5 was placed in orbit on the NPOESS Preparatory Project spacecraft. Data from these instruments are being used to investigate the radiation balance of the Earth at various time and space scales and the role of clouds in this balance. The design and calibration, both on the ground and in-orbit, and operation of the instrument are discussed. C1 [Smith, George Louis] Sci Syst Applicat Inc, Lanham, MD 20706 USA. [Priestley, Kory J.; Loeb, Norman G.] Natl Aeronaut & Space Adm, Sci Directorate, Langley Res Ctr, Hampton, VA 23681 USA. RP Smith, GL (reprint author), Sci Syst Applicat Inc, Lanham, MD 20706 USA. EM g.louis.smith@cox.net FU Science Directorate of Langley Research Center of NASA; Science Mission Directorate of the Earth Science Division of NASA FX The authors would like to thank the Science Directorate of Langley Research Center and the Science Mission Directorate of the Earth Science Division of NASA for the support of the CERES Project. They would also like to thank the people of Northrop-Grumman Space Technology, under the leadership of Steve Carman and Tom Evert, for achieving the performance that was demonstrated by the CERES instruments. The authors' colleagues on the project at Langley Research Center have also made commendable contributions over the life of this project. Finally, the authors thank the reviewers for their time and effort to improve this paper. NR 52 TC 7 Z9 7 U1 1 U2 13 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD MAR PY 2014 VL 52 IS 3 BP 1729 EP 1738 DI 10.1109/TGRS.2013.2253782 PG 10 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 285PA UT WOS:000329404800017 ER PT J AU Rudiger, C Walker, JP Kerr, YH Kim, EJ Hacker, JM Gurney, RJ Barrett, D Le Marshall, J AF Ruediger, Christoph Walker, Jeffrey P. Kerr, Yann H. Kim, Edward J. Hacker, Joerg M. Gurney, Robert J. Barrett, Damian Le Marshall, John TI Toward Vicarious Calibration of Microwave Remote-Sensing Satellites in Arid Environments SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Calibration; environmental monitoring; passive microwave remote sensing; soil moisture ID SOIL-MOISTURE RETRIEVAL; L-BAND; AMSR-E; RADIOMETER; ASSIMILATION; TEMPERATURE; PERFORMANCE; SALINITY; SYSTEM; SPACE AB The Soil Moisture and Ocean Salinity (SMOS) satellite marks the commencement of dedicated global surface soil moisture missions, and the first mission to make passive microwave observations at L-band. On-orbit calibration is an essential part of the instrument calibration strategy, but on-board beam-filling targets are not practical for such large apertures. Therefore, areas to serve as vicarious calibration targets need to be identified. Such sites can only be identified through field experiments including both in situ and airborne measurements. For this purpose, two field experiments were performed in central Australia. Three areas are studied as follows: 1) Lake Eyre, a typically dry salt lake; 2) Wirrangula Hill, with sparse vegetation and a dense cover of surface rock; and 3) Simpson Desert, characterized by dry sand dunes. Of those sites, only Wirrangula Hill and the Simpson Desert are found to be potentially suitable targets, as they have a spatial variation in brightness temperatures of <4 K under normal conditions. However, some limitations are observed for the Simpson Desert, where a bias of 15 K in vertical and 20 K in horizontal polarization exists between model predictions and observations, suggesting a lack of understanding of the underlying physics in this environment. Subsequent comparison with model predictions indicates a SMOS bias of 5 K in vertical and 11 K in horizontal polarization, and an unbiased root mean square difference of 10 K in both polarizations for Wirrangula Hill. Most importantly, the SMOS observations show that the brightness temperature evolution is dominated by regular seasonal patterns and that precipitation events have only little impact. C1 [Ruediger, Christoph; Walker, Jeffrey P.] Univ Melbourne, Dept Civil & Environm Engn, Parkville, Vic 3010, Australia. [Kerr, Yann H.] CESBIO, Ctr Etud Spatiales Biosphere, F-31401 Toulouse, France. [Kim, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hacker, Joerg M.] Flinders Univ S Australia, Airborne Res Australia, Adelaide, SA 5106, Australia. [Gurney, Robert J.] Univ Reading, NERC Environm Syst Sci Ctr, Reading RG6 6UR, Berks, England. [Barrett, Damian] Commonwealth Sci & Ind Res Org, Land & Water, Canberra, ACT 2601, Australia. [Le Marshall, John] Bur Meteorol, Bur Meteorol Res Ctr, Melbourne, Vic 3000, Australia. RP Rudiger, C (reprint author), Monash Univ, Dept Civil Engn, Clayton, Vic 3800, Australia. EM chris.rudiger@monash.edu; jeff.walker@monash.edu; yann.kerr@cesbio.cnes.fr; ed.kim@nasa.gov; jorg@airborneresearch.com.au; rjg@mail.nerc-essc.ac.uk; d.barrett@smi.uq.edu.au; j.lemarshall@bom.gov.au RI Barrett, Damian/C-7972-2009; OI Barrett, Damian/0000-0002-8215-4892; Rudiger, Christoph/0000-0003-4375-4446 FU Australian Research Council Discovery Project [DP0879212] FX This work was supported by the Australian Research Council Discovery Project under Grant DP0879212. NR 21 TC 4 Z9 4 U1 0 U2 25 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD MAR PY 2014 VL 52 IS 3 BP 1749 EP 1760 DI 10.1109/TGRS.2013.2254121 PG 12 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 285PA UT WOS:000329404800019 ER PT J AU Case, JL LaFontaine, FJ Bell, JR Jedlovec, GJ Kumar, SV Peters-Lidard, CD AF Case, Jonathan L. LaFontaine, Frank J. Bell, Jordan R. Jedlovec, Gary J. Kumar, Sujay V. Peters-Lidard, Christa D. TI A Real-Time MODIS Vegetation Product for Land Surface and Numerical Weather Prediction Models SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Geoscience-Atmosphere-Atmospheric modeling; Geoscience-Land surface; Vegetation mapping ID GLOBAL FORECAST SYSTEM; COVER DATA; SENSITIVITY; FRACTION; INDEXES; INITIALIZATION; PRECIPITATION; INFORMATION; TEMPERATURE; CONVECTION AB A technique is presented to produce real-time, daily vegetation composites at 0.01 degrees resolution (similar to 1 km) over the Conterminous United States (CONUS) for use in the NASA Land Information System (LIS) and weather prediction models. Green vegetation fraction (GVF) is derived from direct-broadcast swaths of normalized difference vegetation index from the Moderate Resolution Imaging Spectroradiometer (MODIS) aboard the NASA Earth Observing System satellites. The real-time data and increased resolution compared to the 0.144 degrees (similar to 16 km) resolution monthly GVF climatology in community models result in an improved representation of vegetation in high-resolution models, especially in complex terrain. The MODIS GVF fields show seasonal variations that are similar to the community model climatology, and respond realistically to temperature and precipitation anomalies. The wet spring and summer 2010 over the U. S. Plains led to higher regional GVF than in the climatology. The GVF substantially decreased over the U.S. Southern Plains from 2010 to 2011, consistent with the transition to extreme drought in summer 2011. LIS simulations depict substantial sensitivity to the MODIS GVF, with regional changes in heat fluxes around 100 Wm(-2) over the northern U.S. in June 2010. CONUS LIS simulations during the 2010 warm season indicate that the larger MODIS GVF in the western U.S. led to higher latent heat fluxes and initially lower sensible heat fluxes, with a net drying effect on the soil. With time, the drier soil eventually lead to higher mean sensible heat fluxes such that the total surface energy output increased by late summer 2010 over the western U.S. A sensitivity simulation of a severe weather event using real-time MODIS GVF data results in systematic changes to low-level temperature, moisture, and instability fields, and improves the evolution of simulated precipitation. C1 [Case, Jonathan L.] NASA, Short Term Predict Res & Transit SPoRT Ctr, ENSCO Inc, Huntsville, AL 35805 USA. [LaFontaine, Frank J.] NASA, Short Term Predict Res & Transit SPoRT Ctr, Raytheon Co, Huntsville, AL 35824 USA. [Bell, Jordan R.] Univ Missouri, Dept Atmospher Sci, Columbia, MO 65211 USA. [Jedlovec, Gary J.] NASA, George C Marshall Space Flight Ctr, Short Term Predict Res & Transit SPoRT Ctr, Huntsville, AL 35805 USA. [Kumar, Sujay V.] NASA, Goddard Space Flight Ctr, Sci Applicat Int Corp, Greenbelt, MD 20771 USA. [Peters-Lidard, Christa D.] NASA, Dept HSB, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Case, JL (reprint author), NASA, Short Term Predict Res & Transit SPoRT Ctr, ENSCO Inc, Huntsville, AL 35805 USA. EM Jonathan.Case-1@nasa.gov; frank.j.lafontaine@nasa.gov; jrb42d@mail.missouri.edu; Gary.Jedlovec@nasa.gov; sujay.v.kumar@nasa.gov; christa.peters@nasa.gov RI Kumar, Sujay/B-8142-2015; Peters-Lidard, Christa/E-1429-2012 OI Peters-Lidard, Christa/0000-0003-1255-2876 FU National Aeronautics and Space Administration (NASA) Modeling Analysis and Prediction Solicitation [NNH08ZDA001N-MAP]; NASA Science Mission Directorate's Earth Science Division FX This work was supported in part by the National Aeronautics and Space Administration (NASA) Modeling Analysis and Prediction Solicitation under Grant NNH08ZDA001N-MAP (PI: Peters-Lidard/ Goddard Space Flight Center), and the NASA Science Mission Directorate's Earth Science Division in support of the Short-term Prediction Research and Transition Center at the NASA Marshall Space Flight Center. NR 46 TC 6 Z9 6 U1 0 U2 27 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD MAR PY 2014 VL 52 IS 3 BP 1772 EP 1786 DI 10.1109/TGRS.2013.2255059 PG 15 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 285PA UT WOS:000329404800021 ER PT J AU Wagner, W Brocca, L Naeimi, V Reichle, R Draper, C de Jeu, R Ryu, D Su, CH Western, A Calvet, JC Kerr, YH Leroux, DJ Drusch, M Jackson, TJ Hahn, S Dorigo, W Paulik, C AF Wagner, Wolfgang Brocca, Luca Naeimi, Vahid Reichle, Rolf Draper, Clara de Jeu, Richard Ryu, Dongryeol Su, Chun-Hsu Western, Andrew Calvet, Jean-Christophe Kerr, Yann H. Leroux, Delphine J. Drusch, Matthias Jackson, Thomas J. Hahn, Sebastian Dorigo, Wouter Paulik, Christoph TI Clarifications on the "Comparison Between SMOS, VUA, ASCAT, and ECMWF Soil Moisture Products Over Four Watersheds in US" SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Advanced Scatterometer (ASCAT); noise characterization; soil moisture; Soil Moisture and Ocean Salinity (SMOS); validation ID RETRIEVAL ALGORITHM; IN-SITU; VALIDATION AB In a recent paper, Leroux et al. compared three satellite soil moisture data sets (SMOS, AMSR-E, and ASCAT) and ECMWF forecast soil moisture data to in situ measurements over four watersheds located in the United States. Their conclusions stated that SMOS soil moisture retrievals represent "an improvement [in RMSE] by a factor of 2-3 compared with the other products" and that the ASCAT soil moisture data are "very noisy and unstable." In this clarification, the analysis of Leroux et al. is repeated using a newer version of the ASCAT data and additional metrics are provided. It is shown that the ASCAT retrievals are skillful, although they show some unexpected behavior during summer for two of the watersheds. It is also noted that the improvement of SMOS by a factor of 2-3 mentioned by Leroux et al. is driven by differences in bias and only applies relative to AMSR-E and the ECWMF data in the now obsolete version investigated by Leroux et al. C1 [Wagner, Wolfgang; Naeimi, Vahid; Hahn, Sebastian; Dorigo, Wouter; Paulik, Christoph] Vienna Univ Technol TU Wien, Dept Geodesy & Geoinformat, A-1040 Vienna, Austria. [Brocca, Luca] CNR, Res Inst Geohydrol Protect, I-06128 Perugia, Italy. [Reichle, Rolf; Draper, Clara] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [de Jeu, Richard] Free Univ Amsterdam, Dept Earth Sci, NL-1081 HV Amsterdam, Netherlands. [Ryu, Dongryeol; Su, Chun-Hsu; Western, Andrew] Univ Melbourne, Dept Infrastruct Engn, Melbourne, Vic 3010, Australia. [Calvet, Jean-Christophe] Meteo France, Ctr Natl Rech Meteorol, F-31057 Toulouse, France. [Kerr, Yann H.; Leroux, Delphine J.] Ctr Etud Spatiales Biosphere, F-31401 Toulouse, France. [Drusch, Matthias] European Space Agcy, European Space Res & Technol Ctr, NL-2201 AZ Noordwijk, Netherlands. [Jackson, Thomas J.] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA. RP Wagner, W (reprint author), Vienna Univ Technol TU Wien, Dept Geodesy & Geoinformat, A-1040 Vienna, Austria. EM wolfgang.wagner@geo.tuwien.ac.at; luca.brocca@irpi.cnr.it; rolf.reichle@nasa.gov; clara.draper@nasa.gov; r.a.m.de.jeu@vu.nl; dryu@unimelb.edu.au; csu@unimelb.edu.au; a.western@unimelb.edu.au; jean-christophe.calvet@meteo.fr; yann.kerr@cesbio.cnes.fr; delphine.leroux@cesbio.cnes.fr; matthias.drusch@esa.int; tom.jackson@ars.usda.gov RI Brocca, Luca/F-2854-2010; Western, Andrew/G-1730-2011; Reichle, Rolf/E-1419-2012; Su, Chun-Hsu/C-2076-2014; Ryu, Dongryeol/C-5903-2008; Draper, Clara/P-6097-2016; OI Wagner, Wolfgang/0000-0001-7704-6857; Brocca, Luca/0000-0002-9080-260X; Western, Andrew/0000-0003-4982-146X; Su, Chun-Hsu/0000-0003-2504-0466; Ryu, Dongryeol/0000-0002-5335-6209; Draper, Clara/0000-0002-8299-4939; Dorigo, Wouter/0000-0001-8054-7572; Paulik, Christoph/0000-0002-4231-7933 FU EUMETSAT through the H-SAF project; European Space Agency through the International Soil Moisture Network project FX This work was supported in part by EUMETSAT through the H-SAF project (hsaf.meteoam.it) and in part by the European Space Agency through the International Soil Moisture Network project. NR 20 TC 13 Z9 13 U1 2 U2 21 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD MAR PY 2014 VL 52 IS 3 BP 1901 EP 1906 DI 10.1109/TGRS.2013.2282172 PG 6 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 285PA UT WOS:000329404800032 ER PT J AU Tadesse, T Wiegelmann, T MacNeice, PJ Inhester, B Olson, K Pevtsov, A AF Tadesse, Tilaye Wiegelmann, T. MacNeice, P. J. Inhester, B. Olson, K. Pevtsov, A. TI A Comparison Between Nonlinear Force-Free Field and Potential Field Models Using Full-Disk SDO/HMI Magnetogram SO SOLAR PHYSICS LA English DT Article DE Active regions, magnetic fields; Active regions, models; Magnetic fields, corona; Magnetic fields, models; Magnetic fields, photosphere ID CORONAL MAGNETIC-FIELDS; SOLAR ACTIVE REGIONS; SPHERICAL GEOMETRY; GRAD-RUBIN; EXTRAPOLATION; RECONSTRUCTION; AMBIGUITY; ENERGY; CODE AB Measurements of magnetic fields and electric currents in the pre-eruptive corona are crucial to the study of solar eruptive phenomena, like flares and coronal mass ejections (CMEs). However, spectro-polarimetric measurements of certain photospheric lines permit a determination of the vector magnetic field only at the photosphere. Therefore, there is considerable interest in accurate modeling of the solar coronal magnetic field using photospheric vector magnetograms as boundary data. In this work, we model the coronal magnetic field above multiple active regions with the help of a potential field and a nonlinear force-free field (NLFFF) extrapolation code over the full solar disk using Helioseismic and Magnetic Imager (SDO/HMI) data as boundary conditions. We compare projections of the resulting magnetic field lines with full-disk coronal images from the Atmospheric Imaging Assembly (SDO/AIA) for both models. This study has found that the NLFFF model reconstructs the magnetic configuration closer to observation than the potential field model for full-disk magnetic field extrapolation. We conclude that many of the trans-equatorial loops connecting the two solar hemispheres are current-free. C1 [Tadesse, Tilaye; MacNeice, P. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wiegelmann, T.; Inhester, B.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Tadesse, Tilaye; Olson, K.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Pevtsov, A.] Natl Solar Observ, Sunspot, NM 88349 USA. RP Tadesse, T (reprint author), NASA, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20771 USA. EM tilaye.tadesse.asfaw@nasa.gov; wiegelmann@mps.mpg.de; peter.j.macneice@nasa.gov; inhester@mps.mpg.de; Kevin.M.Olson@drexel.edu; apevtsov@nso.edu OI Pevtsov, Alexei/0000-0003-0489-0920 FU NASA [NNX07AU64G]; NASA Postdoctoral Program at the Goddard Space Flight Center (GSFC) FX The authors thank the anonymous referee for helpful and detailed comments. Data are courtesy of NASA/SDO and the AIA and HMI science teams. SOLIS/VSM vector magnetograms are produced cooperatively by NSF/NSO and NASA/LWS. The National Solar Observatory (NSO) is operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. This research was partly supported by NASA grant NNX07AU64G and by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center (GSFC), administered by Oak Ridge Associated Universities through a contract with NASA. NR 47 TC 5 Z9 5 U1 0 U2 6 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 MAR PY 2014 VL 289 IS 3 BP 831 EP 845 DI 10.1007/s11207-013-0364-y PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268VV UT WOS:000328199700012 ER PT J AU Aschwanden, MJ Wulser, JP Nitta, NV Lemen, JR Freeland, S Thompson, WT AF Aschwanden, Markus J. Wuelser, Jean-Pierre Nitta, Nariaki V. Lemen, James R. Freeland, Sam Thompson, William T. TI STEREO/Extreme Ultraviolet Imager (EUVI) Event Catalog 2006-2012 SO SOLAR PHYSICS LA English DT Article DE Sun: corona; Sun: EUV; Sun: flares ID SELF-ORGANIZED CRITICALITY; SOLAR-FLARE; SYSTEM; SECCHI; SUN AB We generated an event catalog with an automated detection algorithm based on the entire EUVI image database observed with the two Solar Terrestrial Relations Observatory (STEREO)-A and -B spacecraft over the first six years of the mission (2006-2012). The event catalog includes the heliographic positions of some 20 000 EUV events, transformed from spacecraft coordinates to Earth-based coordinates, and information on associated GOES flare events (down to the level of GOES A5-class flares). The 304 angstrom wavelength turns out to be the most efficient channel for flare detection (79% of all EUVI event detections), while the 171 angstrom (4%), 195 angstrom (10 %), and the 284 angstrom channel (7%) retrieve substantially fewer flare events, partially due to the suppressing effect of EUV dimming, and partially due to the lower cadence in the later years of the mission. Due to the Sun-circling orbits of STEREO-A and -B, a large number of flares have been detected on the farside of the Sun, invisible from Earth, or seen as partially occulted events. The statistical size distributions of EUV peak fluxes (with a power-law slope of alpha(P) = 2.5 +/- 0.2) and event durations (with a power-law slope of alpha(T) = 2.4 +/- 0.3) are found to be consistent with the fractal-diffusive self-organized criticality model. The EUVI event catalog is available online at secchi.lmsal.com/EUVI/euvi_autodetection/euvi_events.txt and may serve as a comprehensive tool to identify stereoscopically observed flare events for 3D reconstruction and to study occulted flare events. C1 [Aschwanden, Markus J.; Wuelser, Jean-Pierre; Nitta, Nariaki V.; Lemen, James R.; Freeland, Sam] Lockheed Martin Adv Technol Ctr, Dept ADBS, Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Thompson, William T.] NASA, Goddard Space Flight Ctr, Adnet Syst Inc, Greenbelt, MD 20770 USA. RP Aschwanden, MJ (reprint author), Lockheed Martin Adv Technol Ctr, Dept ADBS, Solar & Astrophys Lab, Bldg 252,3251 Hanover St, Palo Alto, CA 94304 USA. EM aschwanden@lmsal.com FU NASA STEREO mission under NRL [N00173-02-C-2035] FX We thank Frederic Auchere, Lindsay Glesener, Nat Gopalswamy, Bala Poduval, Andreas Klassen, and David Long for helpful discussions and suggestions to create a mission-long STEREO/EUVI event catalog. Part of the work was supported by the NASA STEREO mission under NRL contract N00173-02-C-2035. The STEREO/SECCHI data used here were produced by an international consortium of the Naval Research Laboratory (USA), Lockheed Martin Solar and Astrophysics Lab (USA), NASA Goddard Space Flight Center (USA), Rutherford Appleton Laboratory (UK), University of Birmingham (UK), Max-Planck-Institut for Solar System Research (Germany), Centre Spatiale de Liege (Belgium), Institut d'Optique Theorique et Appliquee (France), and Institut d'Astrophysique Spatiale (France). The USA institutions were funded by NASA, the UK institutions by the Science & Technology Facility Council (which used to be the Particle Physics and Astronomy Research Council, PPARC), the German institutions by Deutsches Zentrum fur Luftund Raumfahrt e. V. (DLR), the Belgian institutions by Belgian Science Policy Office, and the French institutions by Centre National d'Etudes Spatiales (CNES) and the Centre National de la Recherche Scientifique (CNRS). The NRL effort was also supported by the USAF Space Test Program and the Office of Naval Research. NR 20 TC 5 Z9 5 U1 0 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD MAR PY 2014 VL 289 IS 3 BP 919 EP 938 DI 10.1007/s11207-013-0378-5 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268VV UT WOS:000328199700018 ER PT J AU Narukage, N Sakao, T Kano, R Shimojo, M Winebarger, A Weber, M Reeves, KK AF Narukage, N. Sakao, T. Kano, R. Shimojo, M. Winebarger, A. Weber, M. Reeves, K. K. TI Coronal-Temperature-Diagnostic Capability of the Hinode/X-Ray Telescope Based on Self-consistent Calibration. II. Calibration with On-Orbit Data SO SOLAR PHYSICS LA English DT Article DE Corona; Instrumentation and data management ID XRT; MISSION AB The X-Ray Telescope (XRT) onboard the Hinode satellite is an X-ray imager that observes the solar corona with the capability of diagnosing coronal temperatures from less than 1 MK to more than 10 MK. To make full use of this capability, Narukage et al. (Solar Phys. 269, 169, 2011) determined the thickness of each of the X-ray focal-plane analysis filters based on calibration measurements from the ground-based end-to-end test. However, in their paper, the calibration of the thicker filters for observations of active regions and flares, namely the med-Be, med-Al, thick-Al and thick-Be filters, was insufficient due to the insufficient X-ray flux used in the measurements. In this work, we recalibrate those thicker filters using quiescent active region data taken with multiple filters of XRT. On the basis of our updated calibration results, we present the revised coronal-temperature-diagnostic capability of XRT. C1 [Narukage, N.; Sakao, T.] Japan Aerosp Explorat Agcy ISAS JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Kano, R.; Shimojo, M.] NAOJ, Mitaka, Tokyo 1818588, Japan. [Winebarger, A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Weber, M.; Reeves, K. K.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Narukage, N (reprint author), Japan Aerosp Explorat Agcy ISAS JAXA, Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan. EM narukage@solar.isas.jaxa.jp RI Reeves, Katharine/P-9163-2014; Shimojo, Masumi/J-2605-2016 OI Shimojo, Masumi/0000-0002-2350-3749 FU NASA [NNM07AB07C] FX The authors thank members of the XRT team for useful discussions and comments. Hinode is a Japanese mission developed and launched by ISAS/JAXA, collaborating with NAOJ as a domestic partner, NASA and STFC (UK) as international partners. Scientific operation of the Hinode mission is conducted by the Hinode science team organized at ISAS/JAXA. This team mainly consists of scientists from institutes in the partner countries. Support for the post-launch operation is provided by JAXA and NAOJ (Japan), STFC (UK), NASA, ESA, and NSC (Norway). MW and KKR acknowledge support from contract NNM07AB07C through NASA to SAO. NR 7 TC 12 Z9 12 U1 0 U2 9 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 MAR PY 2014 VL 289 IS 3 BP 1029 EP 1042 DI 10.1007/s11207-013-0368-7 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268VV UT WOS:000328199700024 ER PT J AU Gencturk, B Araki, Y Kusama, T Omori, T Kainuma, R Medina, F AF Gencturk, Bora Araki, Yoshikazu Kusama, Tomoe Omori, Toshihiro Kainuma, Ryosuke Medina, Fernando TI Loading rate and temperature dependency of superelastic Cu-Al-Mn alloys SO CONSTRUCTION AND BUILDING MATERIALS LA English DT Article DE Cu-based; Cu-Al-Mn; Shape memory alloys; Superelastic effect; Loading rate; Temperature ID SHAPE-MEMORY ALLOYS; GRAIN-SIZE; SEISMIC APPLICATIONS; MECHANICAL-BEHAVIOR; CONSTITUTIVE MODEL; PSEUDOELASTICITY; WIRES; NITI; TRANSFORMATION; BARS AB This paper presents results from recent experiments performed on superelastic Cu-Al-Mn alloy bars (rods) with different diameters under various loading rates and temperatures. Previously, Araki et al. [2] tested the rate-dependent response of 8 mm bars up to 1 Hz loading rate. In this paper, loading rate (up to 15 Hz) and temperature (-40 to 50 degrees C) dependency of three different bar diameters (8, 12 and 16 mm) was investigated. In addition, the cyclic behavior under large tensile strains (up to 14%) was studied. The motivation for this study was to investigate test parameter ranges that were not explored before (i.e., loading rate, temperature and bar diameter) and to determine the suitability of superelastic Cu-Al-Mn alloys for use in full-scale structures subjected to earthquakes. The ranges for loading rate and temperature as well as the bar diameter were selected with these objectives in mind. It was observed that all Cu-Al-Mn bars show excellent superelastic behavior up to 12% strain under a wide range of loading rates and temperatures. Microstructural analysis of the Cu-Al-Mn alloy bars indicates that the control of texture as well as the relative grain size is important for obtaining stable superelasticity. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Gencturk, Bora] Univ Houston, Dept Civil & Environm Engn, Houston, TX 77204 USA. [Araki, Yoshikazu] Kyoto Univ, Dept Architecture & Architectural Engn, Katsura, Kyoto 6158540, Japan. [Kusama, Tomoe; Omori, Toshihiro; Kainuma, Ryosuke] Tohoku Univ, Dept Mat Sci, Aoba Ku, Sendai, Miyagi 9808579, Japan. [Medina, Fernando] NASA, Jacobs Technol Inc, Struct Test Lab, Johnson Space Ctr, Houston, TX 77058 USA. RP Gencturk, B (reprint author), Univ Houston, Dept Civil & Environm Engn, Houston, TX 77204 USA. EM bgencturk@uh.edu RI Araki, Yoshikazu/F-1894-2013; Omori, Toshihiro/A-4478-2017 OI Araki, Yoshikazu/0000-0001-9569-1753; FU NASA JSC; Jacobs Engineering Group Inc.; Japan Science and Technology Agency (JST); Grant for Excellent Graduate Schools, MEXT, Japan; Toray Science Foundation FX The superelastic tests on the bars were performed with support from National Aeronautics and Space Administration (NASA) Johnson Space Center (JSC) and Jacobs Engineering Group Inc. The authors are thankful to NASA JSC and Jacobs Engineering Group Inc. for their support. We also thank Furukawa Techno Material Co. Ltd. for sample preparation. Y.A., T.O. and R.K. acknowledge the support by the A-STEP program provided by the Japan Science and Technology Agency (JST), and R.K. thanks the support by a Grant for Excellent Graduate Schools, MEXT, Japan. Y.A. is grateful to the support from Toray Science Foundation. NR 20 TC 7 Z9 7 U1 5 U2 37 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0950-0618 EI 1879-0526 J9 CONSTR BUILD MATER JI Constr. Build. Mater. PD FEB 28 PY 2014 VL 53 BP 555 EP 560 DI 10.1016/j.conbuildmat.2013.12.002 PG 6 WC Construction & Building Technology; Engineering, Civil; Materials Science, Multidisciplinary SC Construction & Building Technology; Engineering; Materials Science GA AD8HI UT WOS:000333506700060 ER PT J AU Grant, JA Wilson, SA Mangold, N Calef, F Grotzinger, JP AF Grant, John A. Wilson, Sharon A. Mangold, Nicolas Calef, Fred, III Grotzinger, John P. TI The timing of alluvial activity in Gale crater, Mars SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Mars; Gale crater; alluvial fan; craters; Hesperian ID CONSTRAINTS; CHRONOLOGY; EVOLUTION; MOUND AB The Curiosity rover's discovery of rocks preserving evidence of past habitable conditions in Gale crater highlights the importance of constraining the timing of responsible depositional settings to understand the astrobiological implications for Mars. Crater statistics and mapping reveal the bulk of the alluvial deposits in Gale, including those interrogated by Curiosity, were likely emplaced during the Hesperian, thereby implying that habitable conditions persisted after the Noachian. Crater counting data sets and upper Peace Vallis fan morphology also suggest a possible younger period of fluvial activation that deposited similar to 10-20m of sediments on the upper fan after emplacement of the main body of the fan. If validated, water associated with later alluvial activity may have contributed to secondary diagenetic features in Yellowknife Bay. Key Points The bulk of alluvial deposits in Gale were likely emplaced during the Hesperian Habitable conditions persisted in Gale crater after the Noachian Limited evidence for possible younger fluvial activation on Peace Vallis fan C1 [Grant, John A.; Wilson, Sharon A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Mangold, Nicolas] Univ Nantes, LPGN CNRS UMR6112, Lab Planetol & Geodynam Nantes, Nantes, France. [Calef, Fred, III] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91125 USA. [Grotzinger, John P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Grant, JA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM grantj@si.edu FU NASA FX We thank the Jet Propulsion Laboratory, University of Arizona, Ball Aerospace, Malin Space Science Systems, and Lockheed Martin that built and operate the Curiosity rover, HiRISE and CTX cameras, and the Mars Reconnaissance Orbiter. Reviews by Devon Burr and David Crown improved this paper. This work was supported by NASA. NR 23 TC 18 Z9 18 U1 0 U2 23 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 FEB 28 PY 2014 VL 41 IS 4 BP 1142 EP 1148 DI 10.1002/2013GL058909 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AD1VV UT WOS:000333022700010 ER PT J AU Stroeve, JC Markus, T Boisvert, L Miller, J Barrett, A AF Stroeve, J. C. Markus, T. Boisvert, L. Miller, J. Barrett, A. TI Changes in Arctic melt season and implications for sea ice loss SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Arctic; sea ice AB The Arctic-wide melt season has lengthened at a rate of 5days decade(-1) from 1979 to 2013, dominated by later autumn freezeup within the Kara, Laptev, East Siberian, Chukchi, and Beaufort seas between 6 and 11days decade(-1). While melt onset trends are generally smaller, the timing of melt onset has a large influence on the total amount of solar energy absorbed during summer. The additional heat stored in the upper ocean of approximately 752MJm(-2) during the last decade increases sea surface temperatures by 0.5 to 1.5 degrees C and largely explains the observed delays in autumn freezeup within the Arctic Ocean's adjacent seas. Cumulative anomalies in total absorbed solar radiation from May through September for the most recent pentad locally exceed 300-400MJm(-2) in the Beaufort, Chukchi, and East Siberian seas. This extra solar energy is equivalent to melting 0.97 to 1.3m of ice during the summer. Key Points Melt season has lengthened Increased sea surface temperatures led to a delay in autumn freezeup Increased solar absorption melts an extra 1 m of ice C1 [Stroeve, J. C.; Barrett, A.] Univ Colorado, Cooperat Inst Res Environm Sci, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA. [Stroeve, J. C.] UCL, Ctr Polar Observat & Modelling, London, England. [Markus, T.; Miller, J.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Boisvert, L.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Miller, J.] Wyle Inc, Houston, TX USA. RP Stroeve, JC (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA. EM stroeve@nsidc.org OI Boisvert, Linette/0000-0003-4778-4765 FU NSF [PLR-1304246]; NASA's Cryospheric Sciences Program FX This work was funded in part by NSF award PLR-1304246 and by NASA's Cryospheric Sciences Program. The AVHRR extended Polar Pathfinder Data were provided courteously by J. Key. NR 17 TC 104 Z9 108 U1 15 U2 74 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 FEB 28 PY 2014 VL 41 IS 4 BP 1216 EP 1225 DI 10.1002/2013GL058951 PG 10 WC Geosciences, Multidisciplinary SC Geology GA AD1VV UT WOS:000333022700020 ER PT J AU Boulet, C Ma, QC Thibault, F AF Boulet, Christian Ma, Qiancheng Thibault, Franck TI Line interference effects using a refined Robert-Bonamy formalism: The test case of the isotropic Raman spectra of autoperturbed N-2 SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID PRESSURE-BROADENING THEORY; ROTATIONAL-EXCITATION; SEMICLASSICAL THEORY; RELAXATION; COLLISIONS; QUANTUM; SHAPES; ENERGY; GASES; N-2-H-2 AB A symmetrized version of the recently developed refined Robert-Bonamy formalism [Q. Ma, C. Boulet, and R. H. Tipping, J. Chem. Phys. 139, 034305 (2013)] is proposed. This model takes into account line coupling effects and hence allows the calculation of the off-diagonal elements of the relaxation matrix, without neglecting the rotational structure of the perturbing molecule. The formalism is applied to the isotropic Raman spectra of autoperturbed N-2 for which a benchmark quantum relaxation matrix has recently been proposed. The consequences of the classical path approximation are carefully analyzed. Methods correcting for effects of inelasticity are considered. While in the right direction, these corrections appear to be too crude to provide off diagonal elements which would yield, via the sum rule, diagonal elements in good agreement with the quantum results. In order to overcome this difficulty, a re-normalization procedure is applied, which ensures that the off-diagonal elements do lead to the exact quantum diagonal elements. The agreement between the (re-normalized) semi-classical and quantum relaxation matrices is excellent, at least for the Raman spectra of N-2, opening the way to the analysis of more complex molecular systems. (C) 2014 AIP Publishing LLC. C1 [Boulet, Christian] CNRS, Inst Sci Mol Orsay, UMR8214, F-91405 Orsay, France. [Boulet, Christian] Univ Paris 11, F-91405 Orsay, France. [Ma, Qiancheng] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Ma, Qiancheng] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA. [Thibault, Franck] Univ Rennes 1, CNRS, Inst Phys Rennes, UMR 6251, F-35042 Rennes, France. RP Boulet, C (reprint author), CNRS, Inst Sci Mol Orsay, UMR8214, Bat 350, F-91405 Orsay, France. EM Christian.boulet@u-psud.fr FU National Science Foundation [1228861]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231] FX Q. Ma acknowledges financial support from the National Science Foundation under Grant No. 1228861. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. The authors thank Dr. Kevin Dunseath (Rennes) for his careful reading of the paper. NR 29 TC 5 Z9 5 U1 0 U2 5 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD FEB 28 PY 2014 VL 140 IS 8 AR 084310 DI 10.1063/1.4865967 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA AC4IZ UT WOS:000332485900033 PM 24588172 ER PT J AU Bradford, AL Forney, KA Oleson, EM Barlow, J AF Bradford, Amanda L. Forney, Karin A. Oleson, Erin M. Barlow, Jay TI Accounting for Subgroup Structure in Line-Transect Abundance Estimates of False Killer Whales (Pseudorca crassidens) in Hawaiian Waters SO PLOS ONE LA English DT Article ID TROPICAL PACIFIC-OCEAN; RESPONSIVE MOVEMENT; SOCIAL UNITS; ISLANDS; POPULATION; CETACEANS; PATTERNS; BEHAVIOR; HABITAT; DESIGN AB For biological populations that form aggregations (or clusters) of individuals, cluster size is an important parameter in line-transect abundance estimation and should be accurately measured. Cluster size in cetaceans has traditionally been represented as the total number of individuals in a group, but group size may be underestimated if group members are spatially diffuse. Groups of false killer whales (Pseudorca crassidens) can comprise numerous subgroups that are dispersed over tens of kilometers, leading to a spatial mismatch between a detected group and the theoretical framework of line-transect analysis. Three stocks of false killer whales are found within the U. S. Exclusive Economic Zone of the Hawaiian Islands (Hawaiian EEZ): an insular main Hawaiian Islands stock, a pelagic stock, and a Northwestern Hawaiian Islands (NWHI) stock. A ship-based line-transect survey of the Hawaiian EEZ was conducted in the summer and fall of 2010, resulting in six systematic-effort visual sightings of pelagic (n = 5) and NWHI (n = 1) false killer whale groups. The maximum number and spatial extent of subgroups per sighting was 18 subgroups and 35 km, respectively. These sightings were combined with data from similar previous surveys and analyzed within the conventional line-transect estimation framework. The detection function, mean cluster size, and encounter rate were estimated separately to appropriately incorporate data collected using different methods. Unlike previous line-transect analyses of cetaceans, subgroups were treated as the analytical cluster instead of groups because subgroups better conform to the specifications of line-transect theory. Bootstrap values (n = 5,000) of the line-transect parameters were randomly combined to estimate the variance of stock-specific abundance estimates. Hawai'i pelagic and NWHI false killer whales were estimated to number 1,552 (CV = 0.66; 95% CI = 479-5,030) and 552 (CV = 1.09; 95% CI = 97-3,123) individuals, respectively. Subgroup structure is an important factor to consider in line-transect analyses of false killer whales and other species with complex grouping patterns. C1 [Bradford, Amanda L.; Oleson, Erin M.] Natl Ocean & Atmospher Adm, Protected Species Div, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96813 USA. [Forney, Karin A.] Natl Ocean & Atmospher Adm, Marine Mammal & Turtle Div, Southwest Fisheries Sci Ctr, Natl Marine Fisheries Serv, Santa Cruz, CA USA. [Barlow, Jay] Natl Ocean & Atmospher Adm, Marine Mammal & Turtle Div, Southwest Fisheries Sci Ctr, Natl Marine Fisheries Serv, La Jolla, CA USA. RP Bradford, AL (reprint author), Natl Ocean & Atmospher Adm, Protected Species Div, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96813 USA. EM amanda.bradford@noaa.gov FU National Marine Fisheries Service of the National Oceanic and Atmospheric Administration FX This study was supported by the National Marine Fisheries Service of the National Oceanic and Atmospheric Administration. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 40 TC 6 Z9 6 U1 2 U2 14 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD FEB 28 PY 2014 VL 9 IS 2 AR e90464 DI 10.1371/journal.pone.0090464 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AC3DW UT WOS:000332396200206 PM 24587372 ER PT J AU Schwadron, NA Adams, FC Christian, ER Desiati, P Frisch, P Funsten, HO Jokipii, JR McComas, DJ Moebius, E Zank, GP AF Schwadron, N. A. Adams, F. C. Christian, E. R. Desiati, P. Frisch, P. Funsten, H. O. Jokipii, J. R. McComas, D. J. Moebius, E. Zank, G. P. TI Global Anisotropies in TeV Cosmic Rays Related to the Sun's Local Galactic Environment from IBEX SO SCIENCE LA English DT Article ID INTERSTELLAR-BOUNDARY-EXPLORER; MAGNETIC-FIELD; OUTER HELIOSPHERE; LO OBSERVATIONS; ENA FLUX; RIBBON; PARAMETERS; SPECTRUM; ORIGIN; ORIENTATION AB Observations with the Interstellar Boundary Explorer (IBEX) have shown enhanced energetic neutral atom(ENA) emission from a narrow, circular ribbon likely centered on the direction of the local interstellar medium (LISM) magnetic field. Here, we show that recent determinations of the local interstellar velocity, based on interstellar atom measurements with IBEX, are consistent with the interstellar modulation of high-energy (tera-electron volts, TeV) cosmic rays and diffusive propagation from supernova sources revealed in global anisotropy maps of ground-based high-energy cosmic-ray observatories (Milagro, As gamma, and IceCube). Establishing a consistent local interstellar magnetic field direction using IBEX ENAs at hundreds to thousands of eV and galactic cosmic rays at tens of TeV has wide-ranging implications for the structure of our heliosphere and its interactions with the LISM, which is particularly important at the time when the Voyager spacecraft are leaving our heliosphere. C1 [Schwadron, N. A.; Moebius, E.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Schwadron, N. A.; McComas, D. J.] SW Res Inst, San Antonio, TX 78228 USA. [Adams, F. C.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Christian, E. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Desiati, P.] Univ Wisconsin, IceCube Observ, Madison, WI 53706 USA. [Desiati, P.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Frisch, P.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Funsten, H. O.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Jokipii, J. R.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [McComas, D. J.] Univ Texas San Antonio, San Antonio, TX 78249 USA. [Zank, G. P.] Univ Alabama, Huntsville, AL 35805 USA. RP Schwadron, NA (reprint author), Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. EM n.schwadron@unh.edu RI Funsten, Herbert/A-5702-2015; OI Funsten, Herbert/0000-0002-6817-1039; Moebius, Eberhard/0000-0002-2745-6978 FU NASA's Explorers Program [NNG05EC85C] FX We thank all those who made IBEX possible. IBEX is primarily funded by NASA's Explorers Program (Contract no. NNG05EC85C). IBEX data are available at http://ibex.swri.edu/researchers/publicdata.shtml. IceCube cosmic ray data are available from http://icecube.wisc.edu/science/data. NR 54 TC 31 Z9 31 U1 1 U2 8 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 FEB 28 PY 2014 VL 343 IS 6174 BP 988 EP 990 DI 10.1126/science.1245026 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AC2DZ UT WOS:000332309600036 PM 24526313 ER PT J AU Rollins, AW Thornberry, TD Gao, RS Smith, JB Sayres, DS Sargent, MR Schiller, C Kramer, M Spelten, N Hurst, DF Jordan, AF Hall, EG Vomel, H Diskin, GS Podolske, JR Christensen, LE Rosenlof, KH Jensen, EJ Fahey, DW AF Rollins, A. W. Thornberry, T. D. Gao, R. S. Smith, J. B. Sayres, D. S. Sargent, M. R. Schiller, C. Kraemer, M. Spelten, N. Hurst, D. F. Jordan, A. F. Hall, E. G. Voemel, H. Diskin, G. S. Podolske, J. R. Christensen, L. E. Rosenlof, K. H. Jensen, E. J. Fahey, D. W. TI Evaluation of UT/LS hygrometer accuracy by intercomparison during the NASA MACPEX mission SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE water vapor; UT; LS ID STRATOSPHERIC WATER-VAPOR; DIODE-LASER HYGROMETER; ICE SUPERSATURATIONS; TROPICAL TROPOPAUSE; CIRRUS CLOUDS; DATA PRODUCTS; OPEN-PATH; SPECTROMETER; CALIBRATION; TROPOSPHERE AB Acquiring accurate measurements of water vapor at the low mixing ratios (<10ppm) encountered in the upper troposphere and lower stratosphere (UT/LS) has proven to be a significant analytical challenge evidenced by persistent disagreements between high-precision hygrometers. These disagreements have caused uncertainties in the description of the physical processes controlling dehydration of air in the tropical tropopause layer and entry of water into the stratosphere and have hindered validation of satellite water vapor retrievals. A 2011 airborne intercomparison of a large group of in situ hygrometers onboard the NASA WB-57F high-altitude research aircraft and balloons has provided an excellent opportunity to evaluate progress in the scientific community toward improved measurement agreement. In this work we intercompare the measurements from the Midlatitude Airborne Cirrus Properties Experiment (MACPEX) and discuss the quality of agreement. Differences between values reported by the instruments were reduced in comparison to some prior campaigns but were nonnegligible and on the order of 20% (0.8ppm). Our analysis suggests that unrecognized errors in the quantification of instrumental background for some or all of the hygrometers are a likely cause. Until these errors are understood, differences at this level will continue to somewhat limit our understanding of cirrus microphysical processes and dehydration in the tropical tropopause layer. C1 [Rollins, A. W.; Thornberry, T. D.; Gao, R. S.; Rosenlof, K. H.; Fahey, D. W.] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA. [Rollins, A. W.; Thornberry, T. D.; Hurst, D. F.; Jordan, A. F.; Hall, E. G.; Fahey, D. W.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Smith, J. B.; Sayres, D. S.; Sargent, M. R.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. [Schiller, C.; Kraemer, M.; Spelten, N.] Forschungszentrum Julich, IEK 7, D-52425 Julich, Germany. [Hurst, D. F.; Jordan, A. F.; Hall, E. G.] NOAA, Global Monitoring Div, Earth Syst Res Lab, Boulder, CO USA. [Voemel, H.] GRUAN Deutsch Wetterdienst, Lindenberg, Germany. [Diskin, G. S.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Podolske, J. R.; Jensen, E. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Christensen, L. E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Rollins, AW (reprint author), NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA. EM andrew.rollins@noaa.gov RI Rollins, Andrew/G-7214-2012; Rosenlof, Karen/B-5652-2008; Gao, Ru-Shan/H-7455-2013; Thornberry, Troy/H-7106-2013; Kramer, Martina/A-7482-2013; Schiller, Cornelius/B-1004-2013; Fahey, David/G-4499-2013; Manager, CSD Publications/B-2789-2015 OI Rosenlof, Karen/0000-0002-0903-8270; Fahey, David/0000-0003-1720-0634; FU NASA; NOAA Climate Program Office; NASA Upper Atmosphere Research Program; NASA Radiation Sciences Program FX The authors thank NASA for MACPEX funding and the ground and aircrews of the NASA WB-57F for their support during the mission. We thank T. Peter for helpful discussions with regard to the manuscript. Support for NOAA and CIRES researchers was provided by the NOAA Climate Program Office, the NASA Upper Atmosphere Research Program, and the NASA Radiation Sciences Program. NR 45 TC 15 Z9 15 U1 7 U2 25 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 FEB 27 PY 2014 VL 119 IS 4 BP 1915 EP 1935 DI 10.1002/2013JD020817 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AD3KP UT WOS:000333138300018 ER PT J AU Vergados, P Luo, ZJ Emanuel, K Mannucci, AJ AF Vergados, Panagiotis Luo, Zhengzhao Johnny Emanuel, Kerry Mannucci, Anthony J. TI Observational tests of hurricane intensity estimations using GPS radio occultations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE GPS; radio occultation; remote sensing; hurricane intensity; natural hazards ID SURFACE WIND FIELDS; TROPICAL CYCLONES; WATER-VAPOR; PART I; STRATOSPHERE; TROPOPAUSE; AIR; TEMPERATURE; TRANSPORT; PROFILES AB This study presents a novel approach to estimating the intensity of hurricanes using temperature profiles from Global Positioning System radio occultation (GPSRO) measurements. Previous research has shown that the temperature difference between the ocean surface and the eyewall outflow region defines hurricanes' thermodynamic efficiency, which is directly proportional to the storm's intensity. Outflow temperatures in the eyewall region of 27 hurricanes in 2004-2011 were obtained from GPSRO observations. These observations, along with ocean surface temperatures from NASA Modern Era-Retrospective Analysis for Research and Applications, made it possible to estimate hurricane intensities using a simplified hurricane model. Our preliminary results are quantitatively consistent with best-track values from the National Hurricane Center within 9.4%. As a by-product of our study, we present for the first time GPSRO vertical temperature profiles in the vicinity of the eyewall region of hurricanes, which we compared with collocated temperature profiles from the European Centre for Medium-Range Weather Forecasts Reanalysis Interim (ERA-Interim). Some of the GPSRO data sets reveal a double tropopause in the vicinity of the eyewalla characteristic that we do not see in ERA-Interim. We conclude that GPSRO observations can be of supplementary assistance in augmenting existing data sets used in hurricane intensity estimation. GPSROs' cloud-penetrating capability and high vertical resolution can be useful in providing soundings in the area close to the eyewall region of hurricanes revealing detailed information about their thermal structure, potentially advancing our current knowledge of their dynamics, evolution, and physics. C1 [Vergados, Panagiotis; Mannucci, Anthony J.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA. [Luo, Zhengzhao Johnny] CUNY City Coll, Dept Earth & Atmospher Sci, New York, NY USA. [Luo, Zhengzhao Johnny] CUNY City Coll, CREST Inst, New York, NY USA. [Emanuel, Kerry] MIT, Program Atmospheres Oceans & Climate, Cambridge, MA 02139 USA. RP Vergados, P (reprint author), CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA. EM Panagiotis.Vergados@jpl.nasa.gov NR 60 TC 7 Z9 7 U1 0 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 27 PY 2014 VL 119 IS 4 BP 1936 EP 1948 DI 10.1002/2013JD020934 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AD3KP UT WOS:000333138300019 ER PT J AU Lee, JZ Burow, LC Woebken, D Everroad, RC Kubo, MD Spormann, AM Weber, PK Pett-Ridge, J Bebout, BM Hoehler, TM AF Lee, Jackson Z. Burow, Luke C. Woebken, Dagmar Everroad, R. Craig Kubo, Mike D. Spormann, Alfred M. Weber, Peter K. Pett-Ridge, Jennifer Bebout, Brad M. Hoehler, Tori M. TI Fermentation couples Chloroflexi and sulfate-reducing bacteria to cyanobacteria in hypersaline microbial mats SO FRONTIERS IN MICROBIOLOGY LA English DT Article DE microbial mats; hydrogen; fermentation; Guerrero Negro; NanoSIMS ID GUERRERO-NEGRO; MOLECULAR CHARACTERIZATION; MAXIMUM-LIKELIHOOD; LYNGBYA-SP; DIVERSITY; COMMUNITY; MARINE; BIOGEOCHEMISTRY; HYDROGEN; FIXATION AB Past studies of hydrogen cycling in hypersaline microbial mats have shown an active nighttime cycle, with production largely from cyanobacteria and consumption from sulfate-reducing bacteria (SRB). However, the mechanisms and magnitude of hydrogen cycling have not been extensively studied. Two mats types near Guerrero Negro, Mexico-permanently submerged Microcoleus microbial mat (GN-S), and intertidal Lyngbya microbial mat (GN-I)-were used in microcosm diel manipulation experiments with 3-(3,4-dichlorophenyl)-1,1-dimethylurea (DCMU), molybdate, ammonium addition, and physical disruption to understand the processes responsible for hydrogen cycling between mat microbes. Across microcosms, H-2 production occurred under dark anoxic conditions with simultaneous production of a suite of organic acids. H-2 production was not significantly affected by inhibition of nitrogen fixation, but rather appears to results from constitutive fermentation of photosynthetic storage products by oxygenic phototrophs. Comparison to accumulated glycogen and to CO2 flux indicated that, in the GN-I mat, fermentation released almost all of the carbon fixed via photosynthesis during the preceding day, primarily as organic acids. Across mats, although oxygenic and anoxygenic phototrophs were detected, cyanobacterial [NiFe]-hydrogenase transcripts predominated. Molybdate inhibition experiments indicated that SRBs from a wide distribution of DsrA phylotypes were responsible for H-2 consumption. Incubation with C-13-acetate and NanoSIMS (secondary ion mass-spectrometry) indicated higher uptake in both chloroflexi and SRBs relative to other filamentous bacteria. These manipulations and diel incubations confirm that cyanobacteria were the main fermenters in Guerrero Negro mats and that the net flux of nighttime fermentation byproducts (not only hydrogen) was largely regulated by the interplay between Cyanobacteria, SRBs, and Chloroflexi. C1 [Lee, Jackson Z.; Burow, Luke C.; Woebken, Dagmar; Everroad, R. Craig; Kubo, Mike D.; Bebout, Brad M.; Hoehler, Tori M.] NASA Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. [Lee, Jackson Z.] Bay Area Environm Res Inst, Sonoma, CA USA. [Burow, Luke C.; Woebken, Dagmar; Spormann, Alfred M.] Stanford Univ, Dept Civil & Environm Engn, Stanford, CA 94305 USA. [Burow, Luke C.; Woebken, Dagmar; Spormann, Alfred M.] Stanford Univ, Dept Chem Engn, Stanford, CA 94305 USA. [Kubo, Mike D.] SETI Inst, Mountain View, CA USA. [Weber, Peter K.; Pett-Ridge, Jennifer] Lawrence Livermore Natl Lab, Div Chem Sci, Livermore, CA USA. RP Lee, JZ (reprint author), NASA Ames Res Ctr, POB 1,MS 239-4, Moffett Field, CA 94035 USA. EM jackson.z.lee@nasa.gov RI Woebken, Dagmar/A-4447-2013; OI Woebken, Dagmar/0000-0002-1314-9926 FU US Department of Energy (DOE) Genomic Science Program [SCW1039]; U.S. Department of Energy at Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; NASA Postdoctoral Program FX We thank Erich Fleming, Angela Detweiler, Guillaume Lamarche-Gagnon, Daniel Albert, and Christina Ramon for technical support. We thank Jeff Cann, Associate Wildlife Biologist, Central Region, California Department of Fish and Game for coordinating our access to the Moss Landing Wildlife Area to collect Elkhorn Slough mats and Andrew McDowell at UCB for IRMS analyses. Funding was provided by the US Department of Energy (DOE) Genomic Science Program under contract SCW1039. Work at LLNL was performed under the auspices of the U.S. Department of Energy at Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. R. Craig Everroad acknowledges the support of the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. NR 64 TC 15 Z9 15 U1 6 U2 51 PU FRONTIERS RESEARCH FOUNDATION PI LAUSANNE PA PO BOX 110, LAUSANNE, 1015, SWITZERLAND SN 1664-302X J9 FRONT MICROBIOL JI Front. Microbiol. PD FEB 26 PY 2014 VL 5 AR 61 DI 10.3389/fmicb.2014.00061 PG 17 WC Microbiology SC Microbiology GA AB8WN UT WOS:000332070800001 PM 24616716 ER PT J AU Nobili, AM Pegna, R Shao, M Turyshev, SG Catastini, G Anselmi, A Spero, R Doravari, S Comandi, GL Lucchesi, DM De Michele, A AF Nobili, A. M. Pegna, R. Shao, M. Turyshev, S. G. Catastini, G. Anselmi, A. Spero, R. Doravari, S. Comandi, G. L. Lucchesi, D. M. De Michele, A. TI Integration time in space experiments to test the equivalence principle SO PHYSICAL REVIEW D LA English DT Article ID ENERGY AB The integration time required by space experiments to perform high accuracy tests of the universality of free fall and the weak equivalence principle is a crucial issue. It is inversely proportional to the square of the acceleration to be measured, which is extremely small; the duration of the mission is a severe limitation and experiments in space lack repeatability. An exceedingly long integration time can therefore rule out a mission target. We have evaluated the integration time due to thermal noise from gas damping, Johnson noise and eddy currents-which are independent of the signal frequency-and to internal damping, which is known to decrease with increasing frequency. It is found that at low frequencies thermal noise from internal damping dominates. In the "Galileo Galilei" proposed space experiment to test the equivalence principle to 10(-17) the rapid rotation of the satellite (1 Hz) up-converts the signal to a frequency region where thermal noise from internal damping is lower than gas damping and only a factor 2 higher than Johnson noise, with a total integration time of 2.4 to 3.5 hours even in a very conservative estimate. With an adequate readout and additional care in reducing systematics the test could be improved by another order of magnitude, close to 10(-18), requiring a hundred times longer-still affordable-integration time of 10 to 14.6 days. mu SCOPE, a similar room temperature mission under construction by the French space agency to be launched in 2015, aims at a 10(-15) test with an estimated integration time of 1.4 days. Space tests using cold atoms and atom interferometry have been proposed to be performed on the space station (Q-WEP, to 10(-14)) and on a dedicated mission (STE-QUEST, to 10(-15) like mu SCOPE). In this case integration is required in order to reduce single shot noise. European Space Agency funded studies report an integration time of several months and a few years respectively. C1 [Nobili, A. M.; De Michele, A.] Univ Pisa, Dept Phys E Fermi, I-56127 Pisa, Italy. [Nobili, A. M.; Pegna, R.; Comandi, G. L.; Lucchesi, D. M.] INFN Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Shao, M.; Turyshev, S. G.; Spero, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Catastini, G.; Anselmi, A.] Thales Alenia Space Italia, I-10146 Turin, Italy. [Doravari, S.] CALTECH, Pasadena, CA 91109 USA. [Lucchesi, D. M.] IAPS, INAF Ist Nazl Astrofis, I-00133 Rome, Italy. RP Nobili, AM (reprint author), Univ Pisa, Dept Phys E Fermi, Largo B Pontecorvo 3, I-56127 Pisa, Italy. EM nobili@dm.unipi.it FU ASI (Agenzia Spaziale Italiana); INFN; NASA FX This work has been supported by ASI (Agenzia Spaziale Italiana) and INFN and it was performed in part at JPL, Caltech under a contract with NASA. The contribution of one referee on the effects of eddy currents is gratefully acknowledged. NR 22 TC 3 Z9 3 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD FEB 25 PY 2014 VL 89 IS 4 AR 042005 DI 10.1103/PhysRevD.89.042005 PG 7 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AC0GG UT WOS:000332172200003 ER PT J AU Kwok, R AF Kwok, Ron TI Declassified high-resolution visible imagery for Arctic sea ice investigations: An overview SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Declassified visible imagery; Arctic sea ice; Remote sensing ID SYNTHETIC-APERTURE RADAR; FLOE SIZE DISTRIBUTION; THICKNESS DISTRIBUTION; COVER; OCEAN; MELT AB Since 2009, subsets of declassified satellite images of Arctic sea ice have been released as literal image derived products (LIDPs) with one-meter resolution for scientific use. The collections include imagery acquired over six fixed locations in the Arctic Basin since 1999. Targeted acquisitions over drifting ice parcels, from 2009 on, provide an added dimension to the LIDP archive. This mode of acquisition is especially useful for capturing time-varying processes during the melt season. In this paper, we describe the characteristics of LIDPs, the extent of the current archive, and highlight their uses for Arctic sea ice science. At this writing, the archive of LIDPs is still quite limited, and thus this paper illustrates the potential utility of the imagery. We provide an overview of the retrieval of five sea ice parameters that would benefit significantly from the surface details afforded by the higher resolution LIDPs. They include: melt pond coverage, open water fraction, ridge height, floe size, and, openings and closings. Two other uses are suggested: measurement of lateral melt and the interpretation of radar backscatter. The intent is to motivate geophysical uses of the LIDP and future acquisitions. Results here suggest that the effective observations of sea ice parameters and especially their changes require more focused sampling strategies to address specific spatial and temporal sampling needs. Presently, acquisitions of this type of imagery at fixed locations and drifting sites are being continued, and LIDPs are added to the archive as they are released. (C) 2013 Elsevier Inc All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ron.kwok@jpl.nasa.gov RI Kwok, Ron/A-9762-2008 OI Kwok, Ron/0000-0003-4051-5896 FU Medea; National Security Community on environmental issues FX I would like to thank Dr. Linda Zall, Medea program manager, for her support in this study. I also thank S. S. Pang for her software support during the preparation of this manuscript. The QuikSCAT data were provided by the Physical Oceanography DAAC at the Jet Propulsion Laboratory, Pasadena, CA. This work was conducted at the Jet Propulsion Laboratory, California Institute of Technology, under the auspices of Medea, a scientific advisory group working with the National Security Community on environmental issues. NR 44 TC 7 Z9 7 U1 2 U2 29 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD FEB 25 PY 2014 VL 142 BP 44 EP 56 DI 10.1016/j.rse.2013.11.015 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AA3VM UT WOS:000331023000005 ER PT J AU Kim, M Kim, J Wong, MS Yoon, J Lee, J Wu, D Chan, PW Nichol, JE Chung, CY Ou, ML AF Kim, Mijin Kim, Jhoon Wong, Man Sing Yoon, Jongmin Lee, Jaehwa Wu, Dong Chan, P. W. Nichol, Janet E. Chung, Chu-Yong Ou, Mi-Lim TI Improvement of aerosol optical depth retrieval over Hong Kong from a geostationary meteorological satellite using critical reflectance with background optical depth correction SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Remote sensing; Algorithm; Aerosol optical depth; Critical reflectance; Background aerosol optical depth; Geostationary ID SKY RADIANCE MEASUREMENTS; SURFACE REFLECTANCE; ALGORITHM; MODIS; URBAN; SUN; RADIATION; MTSAT-1R; CHANNELS; AVHRR AB Despite continuous efforts to retrieve aerosol optical depth (ADD) using a conventional 5-channel meteorological imager in geostationary orbit, the accuracy in urban areas has been poorer than other areas primarily due to complex urban surface properties and mixed aerosol types from different emission sources. The two largest error sources in aerosol retrieval have been aerosol type selection and surface reflectance. In selecting the aerosol type from a single visible channel, the season-dependent aerosol optical properties were adopted from long-term measurements of Aerosol Robotic Network (AERONET) sun-photometers. With the aerosol optical properties obtained from the AERONET inversion data, look-up tables were calculated by using a radiative transfer code: the Second Simulation of the Satellite Signal in the Solar Spectrum (6S). Surface reflectance was estimated using the clear sky composite method, a widely used technique for geostationary retrievals. Over East Asia, the AOD retrieved from the Meteorological Imager showed good agreement, although the values were affected by cloud contamination errors. However, the conventional retrieval of the AOD over Hong Kong was largely underestimated due to the lack of information on the aerosol type and surface properties. To detect spatial and temporal variation of aerosol type over the area, the critical reflectance method, a technique to retrieve single scattering albedo (SSA), was applied. Additionally, the background aerosol effect was corrected to improve the accuracy of the surface reflectance over Hong Kong. The AOD retrieved from a modified algorithm was compared to the collocated data measured by AERONET in Hong Kong. The comparison showed that the new aerosol type selection using the critical reflectance and the corrected surface reflectance significantly improved the accuracy of AODs in Hong Kong areas, with a correlation coefficient increase from 0.65 to 0.76 and a regression line change from T-MI [basic algorithm] = 0.41 tau (AERONET) + 0.16 to tau(MI [new algorithm]) = 0.70 tau(AERONET) + 0.01. (C) 2013 Elsevier Inc. All rights reserved. C1 [Kim, Mijin; Kim, Jhoon] Yonsei Univ, Dept Atmospher Sci, Dept Atmosphere Sci IEAA BK21, Seoul 120749, South Korea. [Wong, Man Sing; Nichol, Janet E.] Hong Kong Polytech Univ, Dept Land Surveying & Geoinformat, Kowloon, Hong Kong, Peoples R China. [Yoon, Jongmin] Otto Hahn Inst, Max Planck Inst Chem, Atmospher Chem Dept, D-55128 Mainz, Germany. [Lee, Jaehwa] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Lee, Jaehwa; Wu, Dong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Chan, P. W.] Hong Kong Observ, Hong Kong, Hong Kong, Peoples R China. [Chung, Chu-Yong] Natl Meteorol Satellite Ctr, Jincheon, South Korea. [Ou, Mi-Lim] Natl Inst Meteorol Res, Seoul, South Korea. RP Kim, J (reprint author), Yonsei Univ, Dept Atmospher Sci, Brain Korea Program 21, Inst Earth Astron & Atmosphere, Seoul 120749, South Korea. EM jkim2@yonsei.ac.kr RI Nichol, Janet/A-1442-2014; Chan, Pak Wai/C-8447-2011; Wu, Dong/D-5375-2012; Wong, Man Sing/A-2718-2014 OI Nichol, Janet/0000-0003-4015-893X; Chan, Pak Wai/0000-0003-2289-0609; Wong, Man Sing/0000-0002-6439-6775 FU GEMS program of the Ministry of Environment, Korea; Eco Innovation Program of KEITI [2012000160002]; Brain Korea 21 Plus FX We acknowledge the Korea Meteorological Administration (KMA) for the COMS dataset used in this work. This research was supported by the GEMS program of the Ministry of Environment, Korea and the Eco Innovation Program of KEITI (2012000160002). This research was partially supported by the Brain Korea 21 Plus for J. Kim, M. Kim. NR 42 TC 9 Z9 9 U1 1 U2 25 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 FEB 25 PY 2014 VL 142 BP 176 EP 187 DI 10.1016/j.rse.2013.12.003 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AA3VM UT WOS:000331023000016 ER PT J AU Bilitza, D Altadill, D Zhang, YL Mertens, C Truhlik, V Richards, P McKinnell, LA Reinisch, B AF Bilitza, Dieter Altadill, David Zhang, Yongliang Mertens, Chris Truhlik, Vladimir Richards, Phil McKinnell, Lee-Anne Reinisch, Bodo TI The International Reference Ionosphere 2012-a model of international collaboration SO JOURNAL OF SPACE WEATHER AND SPACE CLIMATE LA English DT Article ID AURORAL OVAL BOUNDARIES; SOLAR-CYCLE VARIATIONS; EMPIRICAL-MODEL; ELECTRON-TEMPERATURE; PROFILE PARAMETERS; COORDINATE SYSTEM; OUTER IONOSPHERE; ION COMPOSITION; B1 PARAMETERS; ENERGY FLUX AB The International Reference Ionosphere (IRI) project was established jointly by the Committee on Space Research (COSPAR) and the International Union of Radio Science (URSI) in the late sixties with the goal to develop an international standard for the specification of plasma parameters in the Earth's ionosphere. COSPAR needed such a specification for the evaluation of environmental effects on spacecraft and experiments in space, and URSI for radiowave propagation studies and applications. At the request of COSPAR and URSI, IRI was developed as a data-based model to avoid the uncertainty of theory-based models which are only as good as the evolving theoretical understanding. Being based on most of the available and reliable observations of the ionospheric plasma from the ground and from space, IRI describes monthly averages of electron density, electron temperature, ion temperature, ion composition, and several additional parameters in the altitude range from 60 km to 2000 km. A working group of about 50 international ionospheric experts is in charge of developing and improving the IRI model. Over time as new data became available and new modeling techniques emerged, steadily improved editions of the IRI model have been published. This paper gives a brief history of the IRI project and describes the latest version of the model, IRI-2012. It also briefly discusses efforts to develop a real-time IRI model. The IRI homepage is at http://IRImodel.org. C1 [Bilitza, Dieter; Richards, Phil] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA. [Bilitza, Dieter] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA. [Altadill, David] Uni Ramon Llull, CSIC, Observ Ebre, Roquetes, Spain. [Zhang, Yongliang] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Mertens, Chris] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. [Truhlik, Vladimir] ASCR, Inst Atmospher Phys, Prague 14131, Czech Republic. [McKinnell, Lee-Anne] SANSA Space Sci, ZA-7200 Hermanus, South Africa. [Reinisch, Bodo] Univ Massachusetts, Ctr Atmospher Res, Lowell, MA USA. RP Bilitza, D (reprint author), George Mason Univ, Sch Phys Astron & Computat Sci, 4400 Univ Dr, Fairfax, VA 22030 USA. EM dbilitza@gmu.edu RI Truhlik, Vladimir/H-6971-2014; Zhang, Yongliang/C-2180-2016; OI Truhlik, Vladimir/0000-0002-6624-4388; Zhang, Yongliang/0000-0003-4851-1662; Altadill, David/0000-0001-7730-385X NR 78 TC 60 Z9 64 U1 2 U2 18 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 FEB 20 PY 2014 VL 4 AR A07 DI 10.1051/swsc/2014004 PG 12 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AU8KX UT WOS:000345846500001 ER PT J AU Abdo, AA Abeysekara, AU Allen, BT Aune, T Barber, AS Berley, D Braun, J Chen, C Christopher, GE Delay, RS DeYoung, T Dingus, BL Ellsworth, RW Fraija, N Gonzalez, MM Goodman, JA Hays, E Hoffman, CM Huntemeyer, PH Imran, A Kolterman, BE Linnemann, JT Marinelli, A McEnery, JE Morgan, T Mincer, AI Nemethy, P Patricelli, B Pretz, J Ryan, JM Parkinson, PMS Schneider, M Shoup, A Sinnis, G Smith, AJ Vasileiou, V Walker, GP Williams, DA Yodh, GB AF Abdo, A. A. Abeysekara, A. U. Allen, B. T. Aune, T. Barber, A. S. Berley, D. Braun, J. Chen, C. Christopher, G. E. Delay, R. S. DeYoung, T. Dingus, B. L. Ellsworth, R. W. Fraija, N. Gonzalez, M. M. Goodman, J. A. Hays, E. Hoffman, C. M. Huentemeyer, P. H. Imran, A. Kolterman, B. E. Linnemann, J. T. Marinelli, A. McEnery, J. E. Morgan, T. Mincer, A. I. Nemethy, P. Patricelli, B. Pretz, J. Ryan, J. M. Parkinson, P. M. Saz Schneider, M. Shoup, A. Sinnis, G. Smith, A. J. Vasileiou, V. Walker, G. P. Williams, D. A. Yodh, G. B. TI THE STUDY OF TeV VARIABILITY AND THE DUTY CYCLE OF Mrk 421 FROM 3 Yr OF OBSERVATIONS WITH THE MILAGRO OBSERVATORY SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: individual (Markarian 421); gamma rays: general ID GAMMA-RAY FLARES; MULTIWAVELENGTH OBSERVATIONS; ENERGY-SPECTRUM; CORRELATED VARIABILITY; BLAZAR MARKARIAN-421; EMISSION; MKN-421; 1ES-1959+650; STATE; MODEL AB TeV-flaring activity with timescales as short as tens of minutes and an orphan TeV flare have been observed from the blazar Markarian 421 (Mrk 421). The TeV emission from Mrk 421 is believed to be produced by leptonic synchrotron self-Compton (SSC) emission. In this scenario, correlations between the X-ray and the TeV fluxes are expected, TeV orphan flares are hardly explained, and the activity (measured as duty cycle) of the source at TeV energies is expected to be equal to or less than that observed in X-rays if only SSC is considered. To estimate the TeV duty cycle of Mrk 421 and to establish limits on its variability at different timescales, we continuously observed Mrk 421 with the Milagro observatory. Mrk 421 was detected by Milagro with a statistical significance of 7.1 standard deviations between 2005 September 21 and 2008 March 15. The observed spectrum is consistent with previous observations by VERITAS. We estimate the duty cycle of Mrk 421 for energies above 1 TeV for different hypotheses of the baseline flux and for different flare selections and we compared our results with the X-ray duty cycle estimated by Resconi et al. The robustness of the results is discussed. C1 [Abdo, A. A.; Abeysekara, A. U.; Barber, A. S.; Linnemann, J. T.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Abdo, A. A.] Inst Def Anal, Operat Evaluat Div, Alexandria, VA 22311 USA. [Allen, B. T.; Chen, C.; Delay, R. S.; Yodh, G. B.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Aune, T.; Parkinson, P. M. Saz; Schneider, M.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Barber, A. S.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. [Berley, D.; Braun, J.; Goodman, J. A.; Smith, A. J.; Vasileiou, V.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Christopher, G. E.; Kolterman, B. E.; Mincer, A. I.; Nemethy, P.] NYU, Dept Phys, New York, NY 10003 USA. [DeYoung, T.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Dingus, B. L.; Hoffman, C. M.; Imran, A.; Pretz, J.; Sinnis, G.; Walker, G. P.] Los Alamos Natl Lab, Grp P23, Los Alamos, NM 87545 USA. [Ellsworth, R. W.] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA. [Fraija, N.; Gonzalez, M. M.; Patricelli, B.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Hays, E.; McEnery, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Huentemeyer, P. H.] Michigan Technol Univ, Dept Phys, Houghton, MI 49931 USA. [Marinelli, A.] Univ Nacl Autonoma Mexico, Inst Fis, Mexico City 04510, DF, Mexico. [Morgan, T.; Ryan, J. M.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Shoup, A.] Ohio State Univ, Lima, OH 45804 USA. [Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, F-34095 Montpellier 5, France. [Walker, G. P.] Natl Secur Technol, Las Vegas, NV 89102 USA. RP Abdo, AA (reprint author), Michigan State Univ, Dept Phys & Astron, 3245 BioMed Phys Sci Bldg, E Lansing, MI 48824 USA. RI Hays, Elizabeth/D-3257-2012; OI Mincer, Allen/0000-0002-6307-1418; Dingus, Brenda/0000-0001-8451-7450 FU National Science Foundation [PHY-0245234, -0302000, -0400424, -0504201, -0601080, ATM-0002744]; US Department of Energy (Office of High-Energy Physics); Los Alamos National Laboratory; University of California; Institute of Geophysics and Planetary Physics; Consejo Nacional de Ciencia y Tecnologia [Conacyt 105033, 103520]; Universidad Nacional Autonoma de Mexico [PAPIIT IN105211, IN108713, IG100413, IG100414]; DGAPA-UNAM; US Department of Energy (Office of Nuclear Physics) FX The Milagro project has been supported by the National Science Foundation (under grants PHY-0245234, -0302000, -0400424, -0504201, -0601080, and ATM-0002744), the US Department of Energy (Office of High-Energy Physics and Office of Nuclear Physics), Los Alamos National Laboratory, the University of California, the Institute of Geophysics and Planetary Physics. This work has been supported by the Consejo Nacional de Ciencia y Tecnologia (under grants Conacyt 105033 and 103520), Universidad Nacional Autonoma de Mexico (under grants PAPIIT IN105211, IN108713, IG100413, and IG100414), and DGAPA-UNAM. NR 31 TC 5 Z9 5 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2014 VL 782 IS 2 AR 110 DI 10.1088/0004-637X/782/2/110 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF3AV UT WOS:000334584700052 ER PT J AU Bennett, CJ Ennis, CP Kaiser, RI AF Bennett, Chris J. Ennis, Courtney P. Kaiser, Ralf I. TI EXPERIMENTAL STUDIES ON THE FORMATION OF D2O AND D2O2 BY IMPLANTATION OF ENERGETIC D+ IONS INTO OXYGEN ICES SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; cosmic rays; ISM: molecules; methods: laboratory: solid state; molecular processes; radiation mechanisms: non-thermal ID VIBRATIONAL INFRARED INTENSITIES; INTERSTELLAR HYDROGEN-PEROXIDE; COUPLED-CLUSTER SINGLES; AB-INITIO CALCULATION; WATER FORMATION; MOLECULAR-OXYGEN; RHO-OPHIUCHI; DUST GRAINS; ATMOSPHERIC-PRESSURE; ORGANIC-MOLECULES AB The formation of water (H2O) in the interstellar medium is intrinsically linked to grain-surface chemistry; thought to involve reactions between atomic (or molecular) hydrogen with atomic oxygen (O), molecular oxygen (O-2), and ozone (O-3). Laboratory precedent suggests that H2O is produced efficiently when O-2 ices are exposed to H atoms (similar to 100 K). This leads to the sequential generation of the hydroxyperoxyl radical (HO2), then hydrogen peroxide (H2O2), and finally H2O and a hydroxyl radical (OH); despite a barrier of similar to 2300K for the last step. Recent detection of the four involved species toward rho Oph A supports this general scenario; however, the precise formation mechanism remains undetermined. Here, solid O-2 ice held at 12K is exposed to a monoenergetic beam of 5 keV D+ ions. Products formed during the irradiation period are monitored through FTIR spectroscopy. O-3 is observed through seven archetypal absorptions. Three additional bands found at 2583, 2707, and 1195 cm(-1) correspond to matrix isolated DO2 (nu(1)) and D2O2 (nu(1),nu(5)), and D2O (nu(2)), respectively. During subsequent warming, the O-2 ice sublimates, revealing a broad band at 2472 cm(-1) characteristic of amorphous D2O (nu(1),nu(3)). Sublimating D-2, D2O, D2O2, and O-3 products were confirmed through their subsequent detection via quadrupole mass spectrometry. Reaction schemes based on both thermally accessible and suprathermally induced chemistries were developed to fit the observed temporal profiles are used to elucidate possible reaction pathways for the formation of D-2-water. Several alternative schemes to the hydrogenation pathway (O-2 -> HO2 -> H2O2 -> H2O) were identified; their astrophysical implications are briefly discussed. C1 [Bennett, Chris J.; Ennis, Courtney P.; Kaiser, Ralf I.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA. [Bennett, Chris J.; Kaiser, Ralf I.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Bennett, Chris J.; Kaiser, Ralf I.] Univ Hawaii, NASA Astrobiol Inst, Honolulu, HI 96822 USA. RP Bennett, CJ (reprint author), Georgia Inst Technol, 901 Atlantic Dr, Atlanta, GA 30332 USA. EM ralfk@hawaii.edu RI Ennis, Courtney/M-5050-2015; OI Ennis, Courtney/0000-0003-1774-8982; Bennett, Christopher/0000-0002-4181-6976 FU National Aeronautics and Space Administration (NASA) [NNA09DA77A] FX This material was based upon work supported by the National Aeronautics and Space Administration (NASA Astrobiology Institute under Cooperative Agreement No. NNA09DA77A issued through the Office of Space Science). NR 91 TC 3 Z9 3 U1 1 U2 19 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 FEB 20 PY 2014 VL 782 IS 2 AR 63 DI 10.1088/0004-637X/782/2/63 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF3AV UT WOS:000334584700005 ER PT J AU Garcia, J Dauser, T Lohfink, A Kallman, TR Steiner, JF McClintock, JE Brenneman, L Wilms, J Eikmann, W Reynolds, CS Tombesi, F AF Garcia, J. Dauser, T. Lohfink, A. Kallman, T. R. Steiner, J. F. McClintock, J. E. Brenneman, L. Wilms, J. Eikmann, W. Reynolds, C. S. Tombesi, F. TI IMPROVED REFLECTION MODELS OF BLACK HOLE ACCRETION DISKS: TREATING THE ANGULAR DISTRIBUTION OF X-RAYS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies: individual (Ark 120); line: formation; radiative transfer; X-rays: general ID ACTIVE GALACTIC NUCLEI; K-ALPHA LINE; FLUORESCENT IRON LINES; XMM-NEWTON; COLD MATTER; SPECTRAL VARIABILITY; COMPTON REFLECTION; SEYFERT-GALAXIES; LOW/HARD STATE; STRONG GRAVITY AB X-ray reflection models are used to constrain the properties of the accretion disk, such as the degree of ionization of the gas and the elemental abundances. In combination with general relativistic ray tracing codes, additional parameters like the spin of the black hole and the inclination to the system can be determined. However, current reflection models used for such studies only provide angle-averaged solutions for the flux reflected at the surface of the disk. Moreover, the emission angle of the photons changes over the disk due to relativistic light bending. To overcome this simplification, we have constructed an angle-dependent reflection model with the xillver code and self-consistently connected it with the relativistic blurring code RELLINE. The new model, relxill, calculates the proper emission angle of the radiation at each point on the accretion disk and then takes the corresponding reflection spectrum into account. We show that the reflected spectra from illuminated disks follow a limb-brightening law highly dependent on the ionization of disk and yet different from the commonly assumed form I alpha ln(1 + 1/mu). A detailed comparison with the angle-averaged model is carried out in order to determine the bias in the parameters obtained by fitting a typical relativistic reflection spectrum. These simulations reveal that although the spin and inclination are mildly affected, the Fe abundance can be overestimated by up to a factor of two when derived from angle-averaged models. The fit of the new model to the Suzaku observation of the Seyfert galaxy Ark 120 clearly shows a significant improvement in the constraint of the physical parameters, in particular by enhancing the accuracy in the inclination angle and the spin determinations. C1 [Garcia, J.; Steiner, J. F.; McClintock, J. E.; Brenneman, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dauser, T.; Wilms, J.; Eikmann, W.] Dr Karl Remeis Observ, D-96049 Bamberg, Germany. [Dauser, T.; Wilms, J.; Eikmann, W.] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany. [Lohfink, A.; Reynolds, C. S.; Tombesi, F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Lohfink, A.; Reynolds, C. S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Kallman, T. R.; Tombesi, F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. RP Garcia, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM javier@head.cfa.harvard.edu; thomas.dauser@sternwarte.uni-erlangen.de; alohfink@astro.umd.edu; timothy.r.kallman@nasa.gov; jsteiner@head.cfa.harvard.edu; jem@cfa.harvard.edu; lbrenneman@cfa.harvard.edu; joern.wilms@sternwarte.uni-erlangen.de; wiebke.eikmann@sternwarte.uni-erlangen.de; chris@astro.umd.edu; ftombesi@astro.umd.edu RI Wilms, Joern/C-8116-2013; XRAY, SUZAKU/A-1808-2009 OI Wilms, Joern/0000-0003-2065-5410; FU NASA [NNX11AD08G, HST-HF-51315.01, NNX10AE41G]; Elitenetzwerk Bayern FX The calculations presented here were performed in the Odyssey cluster of the Research Computing Facilities of Harvard University. J.G. and J.E.M. acknowledge the support of NASA grant NNX11AD08G. J.F.S. was supported by NASA Hubble Fellowship grant HST-HF-51315.01. C.S.R. thanks support from NASA under grant NNX10AE41G. T.D. acknowledges support by a fellowship from the Elitenetzwerk Bayern. We thank John E. Davis for the development of the SLxfig module used to prepare most figures in this paper. NR 74 TC 76 Z9 76 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 FEB 20 PY 2014 VL 782 IS 2 AR 76 DI 10.1088/0004-637X/782/2/76 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF3AV UT WOS:000334584700018 ER PT J AU Hou, Z Reichardt, CL Story, KT Follin, B Keisler, R Aird, KA Benson, BA Bleem, LE Carlstrom, JE Chang, CL Cho, HM Crawford, TM Crites, AT De Haan, T De Putter, R Dobbs, MA Dodelson, S Dudley, J George, EM Halverson, NW Holder, GP Holzapfel, WL Hoover, S Hrubes, JD Joy, M Knox, L Lee, AT Leitch, EM Lueker, M Luong-Van, D McMahon, JJ Mehl, J Meyer, SS Millea, M Mohr, JJ Montroy, TE Padin, S Plagge, T Pryke, C Ruhl, JE Sayre, JT Schaffer, KK Shaw, L Shirokoff, E Spieler, HG Staniszewski, Z Stark, AA Van Engelen, A Vanderlinde, K Vieira, JD Williamson, R Zahn, O AF Hou, Z. Reichardt, C. L. Story, K. T. Follin, B. Keisler, R. Aird, K. A. Benson, B. A. Bleem, L. E. Carlstrom, J. E. Chang, C. L. Cho, H. -M. Crawford, T. M. Crites, A. T. De Haan, T. De Putter, R. Dobbs, M. A. Dodelson, S. Dudley, J. George, E. M. Halverson, N. W. Holder, G. P. Holzapfel, W. L. Hoover, S. Hrubes, J. D. Joy, M. Knox, L. Lee, A. T. Leitch, E. M. Lueker, M. Luong-Van, D. McMahon, J. J. Mehl, J. Meyer, S. S. Millea, M. Mohr, J. J. Montroy, T. E. Padin, S. Plagge, T. Pryke, C. Ruhl, J. E. Sayre, J. T. Schaffer, K. K. Shaw, L. Shirokoff, E. Spieler, H. G. Staniszewski, Z. Stark, A. A. Van Engelen, A. Vanderlinde, K. Vieira, J. D. Williamson, R. Zahn, O. TI CONSTRAINTS ON COSMOLOGY FROM THE COSMIC MICROWAVE BACKGROUND POWER SPECTRUM OF THE 2500 deg(2) SPT-SZ SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmological parameters; early universe; inflation ID SOUTH-POLE TELESCOPE; BARYON ACOUSTIC-OSCILLATIONS; BIG-BANG NUCLEOSYNTHESIS; 720 SQUARE DEGREES; PRIMORDIAL NUCLEOSYNTHESIS; PRECISION COSMOLOGY; HELIUM ABUNDANCE; GALAXY CLUSTERS; HUBBLE CONSTANT; CENT DISTANCE AB We explore extensions to the Lambda CDM cosmology using measurements of the cosmic microwave background (CMB) from the recent SPT-SZ survey, along with data from WMAP7 and measurements of H-0 and baryon acoustic oscillation (BAO). We check for consistency within Lambda CDM between these data sets, and find some tension. The CMB alone gives weak support to physics beyond Lambda CDM, due to a slight trend relative to Lambda CDM of decreasing power toward smaller angular scales. While it may be due to statistical fluctuation, this trend could also be explained by several extensions. We consider running of the primordial spectral index (dn(s)/d ln k), as well as two extensions that modify the damping tail power (the primordial helium abundance Y-p and the effective number of neutrino species N-eff) and one that modifies the large-scale power due to the integrated Sachs-Wolfe effect (the sum of neutrino masses Sigma m(nu)). These extensions have similar observational consequences and are partially degenerate when considered simultaneously. Of the six one-parameter extensions considered, we find CMB to have the largest preference for dn(s)/d ln k with -0.046 < dn(s)/d lnk < -0.003 at 95% confidence, which strengthens to a 2.7 sigma indication of dn(s)/d lnk < 0 from CMB+BAO+H-0. Detectable dn(s)/d ln k not equal 0 is difficult to explain in the context of single-field, slow-roll inflation models. We find N-eff = 3.62 +/- 0.48 for the CMB, which tightens to N-eff = 3.71 +/- 0.35 from CMB+BAO+H-0. Larger values of N-eff relieve the mild tension between CMB, BAO, and H-0. When the Sunyaev-Zel'dovich selected galaxy cluster abundances (SPTCL) data are also included, we obtain N-eff = 3.29 +/- 0.31. Allowing for Sigma m(nu) gives a 3.0s detection of Sigma m(nu) > 0 from CMB+BAO+H-0 +SPTCL. The median value is (0.32+/-0.11) eV, a factor of six above the lower bound set by neutrino oscillation observations. All data sets except H-0 show some preference for massive neutrinos; data combinations including H-0 favor nonzero masses only if BAO data are also included. We also constrain the two-parameter extensions N-eff + Sigma m(nu) and N-eff + Y-p to explore constraints on additional light species and big bang nucleosynthesis, respectively. C1 [Hou, Z.; Follin, B.; Knox, L.; Millea, M.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Reichardt, C. L.; George, E. M.; Holzapfel, W. L.; Lee, A. T.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Story, K. T.; Keisler, R.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Dodelson, S.; Hoover, S.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Schaffer, K. K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Story, K. T.; Keisler, R.; Bleem, L. E.; Carlstrom, J. E.; Hoover, S.; Meyer, S. S.; Padin, S.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Dodelson, S.; Leitch, E. M.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Chang, C. L.; Mehl, J.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cho, H. -M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [De Haan, T.; Dobbs, M. A.; Dudley, J.; Holder, G. P.; Shaw, L.; Van Engelen, A.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [De Putter, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [De Putter, R.] CALTECH, Pasadena, CA 91125 USA. [Dodelson, S.; Lueker, M.; Vieira, J. D.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Joy, M.] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Mohr, J. J.] Excellence Cluster Univ, D-85748 Garching, Germany. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Schaffer, K. K.] Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. RP Hou, Z (reprint author), Univ Calif Davis, Dept Phys, 1 Shields Ave, Davis, CA 95616 USA. RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [ANT-0638937]; NSF [PHY-1125897, NSF PHY 1148698]; Kavli Foundation; Gordon and Betty Moore Foundation; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; NASA Hubble Fellowship [HF-51275.01]; KICP Fellowship; M. Dobbs an Alfred P. Sloan Research Fellowship; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; NASA Office of Space Science FX The SPT is supported by the National Science Foundation through grant ANT-0638937, with partial support provided by NSF grant PHY-1125897, the Kavli Foundation, and the Gordon and Betty Moore Foundation. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs program, and the Canadian Institute for Advanced Research. R. Keisler acknowledges support from NASA Hubble Fellowship grant HF-51275.01, B. A. Benson a KICP Fellowship, M. Dobbs an Alfred P. Sloan Research Fellowship, O. Zahn a BCCP fellowship. This research used resources of the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231, and the resources of the University of Chicago Computing Cooperative (UC3), supported in part by the Open Science Grid, NSF grant NSF PHY 1148698. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. NR 87 TC 117 Z9 117 U1 2 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2014 VL 782 IS 2 AR 74 DI 10.1088/0004-637X/782/2/74 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF3AV UT WOS:000334584700016 ER PT J AU Tsang, D Turner, NJ Cumming, A AF Tsang, David Turner, Neal J. Cumming, Andrew TI SHEDDING LIGHT ON THE ECCENTRICITY VALLEY: GAP HEATING AND ECCENTRICITY EXCITATION OF GIANT PLANETS IN PROTOPLANETARY DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; planet-disk interactions; planet-star interactions; protoplanetary disks; stars: variables: T Tauri, Herbig Ae/Be ID T-TAURI STARS; DENSITY WAVES; CIRCUMSTELLAR DISKS; EMBEDDED PLANETS; TORQUE FORMULA; SOLAR NEBULA; GASEOUS DISK; COROTATION; MIGRATION; LINDBLAD AB We show that the first order (non-co-orbital) corotation torques are significantly modified by entropy gradients in a non-barotropic protoplanetary disk. Such non-barotropic torques can dramatically alter the balance that, for barotropic cases, results in the net eccentricity damping for giant gap-clearing planets embedded in the disk. We demonstrate that stellar illumination can heat the gap enough for the planet's orbital eccentricity to instead be excited. We also discuss the "Eccentricity Valley" noted in the known exoplanet population, where low-metallicity stars have a deficit of eccentric planets between similar to 0.1 and similar to 1 AU compared to metal-rich systems. We show that this feature in the planet distribution may be due to the self-shadowing of the disk by a rim located at the dust sublimation radius similar to 0.1 AU, which is known to exist for several T Tauri systems. In the shadowed region between similar to 0.1 and similar to 1 AU, lack of gap insolation allows disk interactions to damp eccentricity. Outside such shadowed regions stellar illumination can heat the planetary gaps and drive eccentricity growth for giant planets. We suggest that the self-shadowing does not arise at higher metallicity due to the increased optical depth of the gas interior to the dust sublimation radius. C1 [Tsang, David; Cumming, Andrew] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Turner, Neal J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Tsang, D (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. EM dtsang@physics.mcgill.ca OI Tsang, David/0000-0002-1612-2585 FU Lorne Trottier Chair in Astrophysics and Cosmology; Canadian Institute for Advanced Research; National Aeronautics and Space Administration; NASA Origins of Solar Systems program [grant 11-OSS11-0074]; NSERC Discovery Grant FX D.T. was supported by funding from the Lorne Trottier Chair in Astrophysics and Cosmology, and the Canadian Institute for Advanced Research. D.T. thanks Kostas Gourgouliatos, Philip Muirhead, Jason Wright, John Johnson, and particularly Rebekah Dawson for helpful advice and useful discussions during the course of this work. N.J.T. carried out his part of the research at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration and with the support of the NASA Origins of Solar Systems program under grant 11-OSS11-0074. A.C. was supported by an NSERC Discovery Grant and is an Associate Member of the CIFAR Cosmology and Gravity program. NR 47 TC 14 Z9 14 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 FEB 20 PY 2014 VL 782 IS 2 AR 113 DI 10.1088/0004-637X/782/2/113 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF3AV UT WOS:000334584700055 ER PT J AU Wicks, RT Roberts, DA Mallet, A Schekochihin, AA Horbury, TS Chen, CHK AF Wicks, R. T. Roberts, D. A. Mallet, A. Schekochihin, A. A. Horbury, T. S. Chen, C. H. K. TI CORRELATIONS AT LARGE SCALES AND THE ONSET OF TURBULENCE IN THE FAST SOLAR WIND (vol 778, pg 177, 2013) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Wicks, R. T.; Roberts, D. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mallet, A.; Schekochihin, A. A.] Univ Oxford, Rudolf Peierls Ctr Theoret Phys, Oxford OX1 3NP, England. [Horbury, T. S.] Univ London Imperial Coll Sci Technol & Med, Space & Atmospher Phys Grp, London SW7 2AZ, England. [Chen, C. H. K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Wicks, RT (reprint author), NASA, Goddard Space Flight Ctr, Code 672, Greenbelt, MD 20771 USA. EM robert.t.wicks@nasa.gov RI Wicks, Robert/A-1180-2009 OI Wicks, Robert/0000-0002-0622-5302 NR 1 TC 0 Z9 0 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2014 VL 782 IS 2 AR 118 DI 10.1088/0004-637X/782/2/118 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF3AV UT WOS:000334584700061 ER PT J AU Cataldo, G Hsieh, WT Huang, WC Moseley, SH Stevenson, TR Wollack, EJ AF Cataldo, Giuseppe Hsieh, Wen-Ting Huang, Wei-Chung Moseley, S. Harvey Stevenson, Thomas R. Wollack, Edward J. TI Micro-Spec: an ultracompact, high-sensitivity spectrometer for far-infrared and submillimeter astronomy SO APPLIED OPTICS LA English DT Article ID DESIGN AB High-performance, integrated spectrometers operating in the far-infrared and submillimeter ranges promise to be powerful tools for the exploration of the epochs of reionization and initial galaxy formation. These devices, using high-efficiency superconducting transmission lines, can achieve the performance of a meter-scale grating spectrometer in an instrument implemented on a 4 inch silicon wafer. Such a device, when combined with a cryogenic telescope in space, provides an enabling capability for studies of the early universe. Here, the optical design process for Micro-Spec (mu-Spec) is presented, with particular attention given to its two-dimensional diffractive region, where the light of different wavelengths is focused on the different detectors. The method is based on the stigmatization and minimization of the light path function in this bounded region, which results in an optimized geometrical configuration. A point design with an efficiency of similar to 90% has been developed for initial demonstration and can serve as the basis for future instruments. Design variations on this implementation are also discussed, which can lead to lower efficiencies due to diffractive losses in the multimode region. (C) 2014 Optical Society of America C1 [Cataldo, Giuseppe; Hsieh, Wen-Ting; Huang, Wei-Chung; Moseley, S. Harvey; Stevenson, Thomas R.; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Cataldo, G (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM Giuseppe.Cataldo@nasa.gov RI Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 FU NASA ROSES/APRA program; Universities Space Research Association (USRA) FX Financial support received from the NASA ROSES/APRA program is gratefully acknowledged by the authors. GC would also like to acknowledge the support provided by Universities Space Research Association (USRA) in the administration of his appointment at the NASA Goddard Space Flight Center. NR 27 TC 7 Z9 7 U1 0 U2 11 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 FEB 20 PY 2014 VL 53 IS 6 BP 1094 EP 1102 DI 10.1364/AO.53.001094 PG 9 WC Optics SC Optics GA AB7DN UT WOS:000331949600012 PM 24663307 ER PT J AU Grefenstette, BW Harrison, FA Boggs, SE Reynolds, SP Fryer, CL Madsen, KK Wik, DR Zoglauer, A Ellinger, CI Alexander, DM An, H Barret, D Christensen, FE Craig, WW Forster, K Giommi, P Hailey, CJ Hornstrup, A Kaspi, VM Kitaguchi, T Koglin, JE Mao, PH Miyasaka, H Mori, K Perri, M Pivovaroff, MJ Puccetti, S Rana, V Stern, D Westergaard, NJ Zhang, WW AF Grefenstette, B. W. Harrison, F. A. Boggs, S. E. Reynolds, S. P. Fryer, C. L. Madsen, K. K. Wik, D. R. Zoglauer, A. Ellinger, C. I. Alexander, D. M. An, H. Barret, D. Christensen, F. E. Craig, W. W. Forster, K. Giommi, P. Hailey, C. J. Hornstrup, A. Kaspi, V. M. Kitaguchi, T. Koglin, J. E. Mao, P. H. Miyasaka, H. Mori, K. Perri, M. Pivovaroff, M. J. Puccetti, S. Rana, V. Stern, D. Westergaard, N. J. Zhang, W. W. TI Asymmetries in core-collapse supernovae from maps of radioactive Ti-44 in Cassiopeia A SO NATURE LA English DT Article ID GAMMA-RAY BURSTS; A SUPERNOVA; 3-DIMENSIONAL STRUCTURE; REMNANT CASSIOPEIA; CAS-A; EXPLOSION; EJECTA; STARS; IIB; HYDRODYNAMICS AB Asymmetry is required by most numerical simulations of stellar core-collapse explosions, but the form it takes differs significantly among models. The spatial distribution of radioactive Ti-44, synthesized in an exploding star near the boundary between material falling back onto the collapsing core and that ejected into the surrounding medium(1), directly probes the explosion asymmetries. Cassiopeia A is a young(2), nearby(3), core-collapse(4) remnant from which Ti-44 emission has previously been detected(5-8) but not imaged. Asymmetries in the explosion have been indirectly inferred from a high ratio of observed Ti-44 emission to estimated Ni-56 emission(9), from optical light echoes(10), and from jet-like features seen in the X-ray(11) and optical(12) ejecta. Here we report spatial maps and spectral properties of the Ti-44 in Cassiopeia A. This may explain the unexpected lack of correlation between the Ti-44 and iron X-ray emission, the latter being visible only in shock-heated material. The observed spatial distribution rules out symmetric explosions even with a high level of convective mixing, as well as highly asymmetric bipolar explosions resulting from a fast-rotating progenitor. Instead, these observations provide strong evidence for the development of low-mode convective instabilities in core-collapse supernovae. C1 [Grefenstette, B. W.; Harrison, F. A.; Madsen, K. K.; Forster, K.; Mao, P. H.; Miyasaka, H.; Rana, V.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Boggs, S. E.; Zoglauer, A.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Reynolds, S. P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. [Fryer, C. L.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Wik, D. R.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ellinger, C. I.] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA. [Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [An, H.; Kaspi, V. M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Barret, D.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Barret, D.] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France. [Christensen, F. E.; Hornstrup, A.; Westergaard, N. J.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, W. W.; Pivovaroff, M. J.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Giommi, P.; Perri, M.; Puccetti, S.] Agenzia Spaziale Italiana, Sci Data Ctr, I-00133 Rome, Italy. [Hailey, C. J.; Mori, K.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Kitaguchi, T.] RIKEN, Nishina Ctr, Wako, Saitama 3510198, Japan. [Koglin, J. E.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Perri, M.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Grefenstette, BW (reprint author), CALTECH, Cahill Ctr Astrophys, 1216 East Calif Blvd, Pasadena, CA 91125 USA. EM bwgref@srl.caltech.edu; fiona@srl.caltech.edu RI Pivovaroff, Michael/M-7998-2014; Boggs, Steven/E-4170-2015; OI Pivovaroff, Michael/0000-0001-6780-6816; Boggs, Steven/0000-0001-9567-4224; giommi, paolo/0000-0002-2265-5003; Perri, Matteo/0000-0003-3613-4409; Puccetti, Simonetta/0000-0002-2734-7835; Alexander, David/0000-0002-5896-6313 FU NASA [NNG08FD60C]; NASA FX This work was supported by NASA under grant no. NNG08FD60C, and made use of data from the Nuclear Spectroscopic Telescope Array (NuSTAR) mission, a project led by Caltech, managed by the Jet Propulsion Laboratory and funded by NASA. We thank the NuSTAR operations, software and calibration teams for support with execution and analysis of these observations. NR 40 TC 57 Z9 57 U1 0 U2 25 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 FEB 20 PY 2014 VL 506 IS 7488 BP 339 EP + DI 10.1038/nature12997 PG 14 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AB0JL UT WOS:000331477800035 PM 24553239 ER PT J AU Cheung, CC Larsson, S Scargle, JD Amin, MA Blandford, RD Bulmash, D Chiang, J Ciprini, S Corbet, RHD Falco, EE Marshall, PJ Wood, DL Ajello, M Bastieri, D Chekhtman, A D'Ammando, F Giroletti, M Grove, JE Lott, B Ojha, R Orienti, M Perkins, JS Razzano, M Smith, AW Thompson, DJ Wood, KS AF Cheung, C. C. Larsson, S. Scargle, J. D. Amin, M. A. Blandford, R. D. Bulmash, D. Chiang, J. Ciprini, S. Corbet, R. H. D. Falco, E. E. Marshall, P. J. Wood, D. L. Ajello, M. Bastieri, D. Chekhtman, A. D'Ammando, F. Giroletti, M. Grove, J. E. Lott, B. Ojha, R. Orienti, M. Perkins, J. S. Razzano, M. Smith, A. W. Thompson, D. J. Wood, K. S. TI FERMI LARGE AREA TELESCOPE DETECTION OF GRAVITATIONAL LENS DELAYED gamma-RAY FLARES FROM BLAZAR B0218+357 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; gamma rays: galaxies; gravitational lensing: strong; quasars: individual (B0218+357) ID ACTIVE GALACTIC NUCLEI; ALL-SKY SURVEY; TIME-DELAY; HUBBLE CONSTANT; EINSTEIN RING; RADIO-SOURCES; VARIABILITY; SYSTEM; CALIBRATION; REDSHIFT AB Using data from the Fermi Large Area Telescope (LAT), we report the first clear gamma-ray measurement of a delay between flares from the gravitationally lensed images of a blazar. The delay was detected in B0218+357, a known double-image lensed system, during a period of enhanced gamma-ray activity with peak fluxes consistently observed to reach >20-50x its previous average flux. An auto-correlation function analysis identified a delay in the gamma-ray data of 11.46 +/- 0.16 days (1 sigma) that is similar to 1 day greater than previous radio measurements. Considering that it is beyond the capabilities of the LAT to spatially resolve the two images, we nevertheless decomposed individual sequences of superposing gamma-ray flares/delayed emissions. In three such similar to 8-10 day-long sequences within a similar to 4 month span, considering confusion due to overlapping flaring emission and flux measurement uncertainties, we found flux ratios consistent with similar to 1, thus systematically smaller than those from radio observations. During the first, best-defined flare, the delayed emission was detailed with a Fermi pointing, and we observed flux doubling timescales of similar to 3-6 hr implying as well extremely compact gamma-ray emitting regions. C1 [Cheung, C. C.; Grove, J. E.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Larsson, S.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Larsson, S.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Amin, M. A.] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Amin, M. A.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Blandford, R. D.; Chiang, J.; Marshall, P. J.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Blandford, R. D.; Chiang, J.; Marshall, P. J.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Bulmash, D.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Ciprini, S.] ASI, Sci Data Ctr, I-00133 Rome, Italy. [Ciprini, S.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Monte Porzio Catone, Roma, Italy. [Corbet, R. H. D.] Ctr Res & Explorat Space Sci & Technol CRESST, Greenbelt, MD 20771 USA. [Corbet, R. H. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Corbet, R. H. D.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Falco, E. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marshall, P. J.] Univ Oxford, Dept Phys Astrophys, Oxford OX1 3RH, England. [Wood, D. L.] Praxis Inc, Alexandria, VA 22303 USA. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Bastieri, D.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Chekhtman, A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Lott, B.] Univ Bordeaux 1, IN2P3 CNRS, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Ojha, R.; Perkins, J. S.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Orienti, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. RP Cheung, CC (reprint author), Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. EM Teddy.Cheung@nrl.navy.mil; Jeffrey.D.Scargle@nasa.gov FU Royal Swedish Academy Crafoord Foundation; Italian Ministry of Education, University and Research (MIUR) [FIRB-2012-RBFR12PM1F] FX Supported by the Royal Swedish Academy Crafoord Foundation.; Funded by contract FIRB-2012-RBFR12PM1F from the Italian Ministry of Education, University and Research (MIUR). NR 50 TC 21 Z9 21 U1 1 U2 5 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 FEB 20 PY 2014 VL 782 IS 2 AR L14 DI 10.1088/2041-8205/782/2/L14 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5PV UT WOS:000331153000001 ER PT J AU Hjorth, J Gall, C Michallowski, MJ AF Hjorth, Jens Gall, Christa Michallowski, Michall J. TI SHAPING THE DUST MASS-STAR-FORMATION RATE RELATION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE dust, extinction; galaxies: evolution; galaxies: high-redshift; galaxies: ISM ID EARLY-TYPE GALAXIES; HIGH-REDSHIFT; FORMING GALAXIES; SDSS J1148+5251; NEARBY GALAXIES; SCHMIDT LAW; MULTIWAVELENGTH; EVOLUTION; STARBURST; QUASARS AB There is a remarkably tight relation between the observationally inferred dust masses and star-formation rates (SFRs) of Sloan Digital Sky Survey galaxies, M-dust alpha SFR1.11. Here we extend the M-dust-SFR relation to the high end and show that it bends over at very large SFRs (i.e., dust masses are lower than predicted for a given SFR). We identify several distinct evolutionary processes in the diagram: (1) a star-bursting phase in which dust builds up rapidly at early times. The maximum attainable dust mass in this process is the cause of the bend-over of the relation. A high dust-formation efficiency, a bottom-light initial mass function, and negligible supernova shock dust destruction are required to produce sufficiently high dust masses. (2) A quiescent star-forming phase in which the subsequent parallel decline in dust mass and SFR gives rise to the M-dust-SFR relation, through astration and dust destruction. The dust-to-gas ratio is approximately constant along the relation. We show that the power-law slope of the M-dust-SFR relation is inversely proportional to the global Schmidt-Kennicutt law exponent (i.e., similar to 0.9) in simple chemical evolution models. (3) A quenching phase which causes star formation to drop while the dust mass stays roughly constant or drops proportionally. Combined with merging, these processes, as well as the range in total baryonic mass, give rise to a complex population of the diagram which adds significant scatter to the original M-dust-SFR relation. (4) At very high redshifts, a population of galaxies located significantly below the local relation is predicted. C1 [Hjorth, Jens; Gall, Christa] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Gall, Christa] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Gall, Christa] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Michallowski, Michall J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium. [Michallowski, Michall J.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. RP Hjorth, J (reprint author), Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. EM jens@dark-cosmology.dk; cgall@phys.au.dk; mm@roe.ac.uk RI Hjorth, Jens/M-5787-2014; Gall, Christa/P-7630-2016 OI Hjorth, Jens/0000-0002-4571-2306; Gall, Christa/0000-0002-8526-3963 FU NASA Postdoctoral Program (NPP); Danish Agency for Science and Technology and Innovation; Danish National Research Foundation FX We thank Haley Gomez, Julie Wardlow, Sune Toft, Stefano Zibetti, Anna Gallazzi, and Darach Watson for discussions, and Elisabete da Cunha and Mark Swinbank for making their data points available in electronic form. The anonymous referee provided very insightful comments. C.G. was supported from the NASA Postdoctoral Program (NPP) and acknowledges funding provided by the Danish Agency for Science and Technology and Innovation. The Dark Cosmology Centre is funded by the Danish National Research Foundation. NR 33 TC 7 Z9 7 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 FEB 20 PY 2014 VL 782 IS 2 AR L23 DI 10.1088/2041-8205/782/2/L23 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5PV UT WOS:000331153000010 ER PT J AU Miceli, M Acero, F Dubner, G Decourchelle, A Orlando, S Bocchino, F AF Miceli, M. Acero, F. Dubner, G. Decourchelle, A. Orlando, S. Bocchino, F. TI SHOCK-CLOUD INTERACTION AND PARTICLE ACCELERATION IN THE SOUTHWESTERN LIMB OF SN 1006 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE acceleration of particles; ISM: clouds; ISM: individual objects (SN 1006); ISM: supernova remnants; X-rays: ISM ID SUPERNOVA-REMNANTS; PROPER MOTIONS; SN-1006; GAS; EMISSION; EJECTA; RAYS AB The supernova remnant SN 1006 is a powerful source of high-energy particles and evolves in a relatively tenuous and uniform environment despite interacting with an atomic cloud in its northwestern limb. The X-ray image of SN 1006 reveals an indentation in the southwestern part of the shock front and the H I maps show an isolated (southwestern) cloud, having the same velocity as the northwestern cloud, whose morphology fits perfectly in the indentation. We performed spatially resolved spectral analysis of a set of small regions in the southwestern nonthermal limb and studied the deep X-ray spectra obtained within the XMM-Newton SN 1006 Large Program. We also analyzed archive H I data, obtained by combining single-dish and interferometric observations. We found that the best-fit value of N-H derived from the X-ray spectra significantly increases in regions corresponding to the southwestern cloud, while the cutoff energy of the synchrotron emission decreases. The N-H variation corresponds perfectly with the H I column density of the southwestern cloud, as measured from the radio data. The decrease in the cutoff energy at the indentation clearly reveals that the back side of the cloud is actually interacting with the remnant. The southwestern limb therefore presents a unique combination of efficient particle acceleration and high ambient density, thus being the most promising region for gamma-ray hadronic emission in SN 1006. We estimate that such emission will be detectable with the Fermi telescope within a few years. C1 [Miceli, M.; Orlando, S.; Bocchino, F.] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Acero, F.] NASA, ORAU, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Dubner, G.] UBA CONICET, IAFE, RA-1428 Buenos Aires, DF, Argentina. [Decourchelle, A.] CEA DSM Irfu CNRS Univ Paris Diderot, CE Saclay, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. RP Miceli, M (reprint author), INAF Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy. EM miceli@astropa.unipa.it OI Bocchino, Fabrizio/0000-0002-2321-5616; Miceli, Marco/0000-0003-0876-8391; Orlando, Salvatore/0000-0003-2836-540X FU ASI-INAF [I/009/10/0]; CONICET; AN-PCYT (Argentina); CNES FX We thank the anonymous referee for important comments and suggestions. This Letter was partially funded by the ASI-INAF contract I/009/10/0. G. D. is funded by CONICET and AN-PCYT (Argentina) grants. A.D. acknowledges support from CNES. NR 16 TC 9 Z9 9 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2014 VL 782 IS 2 AR L33 DI 10.1088/2041-8205/782/2/L33 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5PV UT WOS:000331153000020 ER PT J AU Schmidt, KB Treu, T Brammer, GB Bradac, M Wang, X Dijkstra, M Dressler, A Fontana, A Gavazzi, R Henry, AL Hoag, A Jones, TA Kelly, PL Malkan, MA Mason, C Pentericci, L Poggianti, B Stiavelli, M Trenti, M von der Linden, A Vulcani, B AF Schmidt, K. B. Treu, T. Brammer, G. B. Bradac, M. Wang, X. Dijkstra, M. Dressler, A. Fontana, A. Gavazzi, R. Henry, A. L. Hoag, A. Jones, T. A. Kelly, P. L. Malkan, M. A. Mason, C. Pentericci, L. Poggianti, B. Stiavelli, M. Trenti, M. von der Linden, A. Vulcani, B. TI THROUGH THE LOOKING GLASS: HST SPECTROSCOPY OF FAINT GALAXIES LENSED BY THE FRONTIER FIELDS CLUSTER MACSJ0717.5+3745 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: clusters: individual (MACSJ0717.5+3745); galaxies: evolution; galaxies: high-redshift ID LYMAN BREAK GALAXIES; LY-ALPHA EMISSION; ULTRA DEEP FIELD; SIMILAR-TO 7; KECK SPECTROSCOPY; MACS J0717.5+3745; MOSFIRE SPECTROSCOPY; REIONIZATION; HUBBLE; FRACTION AB The Grism Lens-Amplified Survey from Space (GLASS) is a Hubble Space Telescope (HST) Large Program, which will obtain 140 orbits of grism spectroscopy of the core and infall regions of 10 galaxy clusters, selected to be among the very best cosmic telescopes. Extensive HST imaging is available from many sources including the CLASH and Frontier Fields programs. We introduce the survey by analyzing spectra of faint multiply-imaged galaxies and z greater than or similar to 6 galaxy candidates obtained from the first 7 orbits out of 14 targeting the core of the Frontier Fields cluster MACSJ0717.5+3745. Using the G102 and G141 grisms to cover the wavelength range 0.8-1.7 mu m, we confirm four strongly lensed systems by detecting emission lines in each of the images. For the 9 z greater than or similar to 6 galaxy candidates clear from contamination, we do not detect any emission lines down to a 7 orbit 1 sigma noise level of similar to 5x10(-18) erg s(-1) cm(-2). Taking lensing magnification into account, our flux sensitivity reaches similar to 0.2-5x10(-18) erg s(-1)cm(-2). These limits over an uninterrupted wavelength range rule out the possibility that the high-z galaxy candidates are instead strong line emitters at lower redshift. These results show that by means of careful modeling of the background-and with the assistance of lensing magnification-interesting flux limits can be reached for large numbers of objects, avoiding pre-selection and the wavelength restrictions inherent to ground-based multi-slit spectroscopy. These observations confirm the power of slitless HST spectroscopy even in fields as crowded as a cluster core. C1 [Schmidt, K. B.; Treu, T.; Wang, X.; Jones, T. A.; Mason, C.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Brammer, G. B.; Stiavelli, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Bradac, M.; Hoag, A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Dijkstra, M.] Univ Oslo, Inst Theoret Astrophys, N-0858 Oslo, Norway. [Dressler, A.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Fontana, A.; Pentericci, L.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Gavazzi, R.] CNRS, Inst Astrophys Paris, F-75014 Paris, France. [Henry, A. L.] Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kelly, P. L.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Malkan, M. A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Poggianti, B.] INAF Astron Observ Padova, Padua, Italy. [Trenti, M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Trenti, M.] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England. [von der Linden, A.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [von der Linden, A.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Vulcani, B.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Univ WPI, Kashiwa, Chiba 2778582, Japan. RP Schmidt, KB (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. EM kschmidt@physics.ucsb.edu OI Vulcani, Benedetta/0000-0003-0980-1499; Mason, Charlotte/0000-0002-3407-1785; Trenti, Michele/0000-0001-9391-305X; fontana, adriano/0000-0003-3820-2823 FU NASA [NAS 5-26555]; Danish National Research Foundation; [HST-13459]; [HST-GO13177]; [HST-AR13235] FX This Letter is based on observations made with the NASA/ESA Hubble Space Telescope, obtained at STScI. We acknowledge support through grants HST-13459, HST-GO13177, and HST-AR13235. This work utilizes gravitational lensing models produced by PIs Bradac, Ebeling, Merten, Zitrin, Sharon, and Williams funded as part of the HST Frontier Fields program conducted by STScI. STScI is operated by AURA, Inc. under NASA contract NAS 5-26555. The lens models were obtained from the Mikulski Archive for Space Telescopes (MAST). The Dark Cosmology Centre (DARK) is funded by the Danish National Research Foundation. Some of the data presented herein were obtained at the W. M. Keck Observatory. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. NR 39 TC 33 Z9 33 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2014 VL 782 IS 2 AR L36 DI 10.1088/2041-8205/782/2/L36 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5PV UT WOS:000331153000023 ER PT J AU Landgren, E Fritsches, K Brill, R Warrant, E AF Landgren, Eva Fritsches, Kerstin Brill, Richard Warrant, Eric TI The visual ecology of a deep-sea fish, the escolar Lepidocybium flavobrunneum (Smith, 1843)(+) SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE deep-sea vision; eye; escolar; visual ecology; visual sensitivity; visual resolution ID RETINAL TOPOGRAPHY; REEF TELEOSTS; FUSION FREQUENCY; EYES; VISION; LENS; PHOTORECEPTORS; SENSITIVITY; SWORDFISH; PIGMENTS AB Escolar (Lepidocybium flavobrunneum, family Gempylidae) are large and darkly coloured deep-sea predatory fish found in the cold depths (more than 200 m) during the day and in warm surface waters at night. They have large eyes and an overall low density of retinal ganglion cells that endow them with a very high optical sensitivity. Escolar have banked retinae comprising six to eight layers of rods to increase the optical path length for maximal absorption of the incoming light. Their retinae possess two main areae of higher ganglion cell density, one in the ventral retina viewing the dorsal world above (with a moderate acuity of 4.6 cycles deg(-1)), and the second in the temporal retina viewing the frontal world ahead. Electrophysiological recordings of the flicker fusion frequency (FFF) in isolated retinas indicate that escolar have slow vision, with maximal FFF at the highest light levels and temperatures (around 9 Hz at 23 degrees C) which fall to 1-2 Hz in dimlight or cooler temperatures. Our results suggest that escolar are slowly moving sit-and-wait predators. In dim, warm surface waters at night, their slow vision, moderate dorsal resolution and highly sensitive eyes may allow them to surprise prey from below that are silhouetted in the downwelling light. C1 [Landgren, Eva; Warrant, Eric] Lund Univ, Dept Biol, Lund Vis Grp, S-22362 Lund, Sweden. [Fritsches, Kerstin] Univ Queensland, Sch Biomed Sci, Brisbane, Qld 4072, Australia. [Brill, Richard] Northeast Fisheries Sci Ctr, James J Howard Marine Sci Lab, Natl Marine Fisheries Serv, Highlands, NJ 07732 USA. RP Warrant, E (reprint author), Lund Univ, Dept Biol, Lund Vis Grp, Solvegatan 35, S-22362 Lund, Sweden. EM eric.warrant@biol.lu.se NR 43 TC 6 Z9 6 U1 1 U2 18 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8436 EI 1471-2970 J9 PHILOS T R SOC B JI Philos. Trans. R. Soc. B-Biol. Sci. PD FEB 19 PY 2014 VL 369 IS 1636 SI SI AR 20130039 DI 10.1098/rstb.2013.0039 PG 12 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AC4BO UT WOS:000332465800008 PM 24395966 ER PT J AU Ting, DZ Soibel, A Keo, SA Rafol, SB Mumolo, JM Liu, JK Hill, CJ Khoshakhlagh, A Hoglund, L Luong, EM Gunapala, SD AF Ting, David Z. Soibel, Alexander Keo, Sam A. Rafol, Sir B. Mumolo, Jason M. Liu, John K. Hill, Cory J. Khoshakhlagh, Arezou Hoeglund, Linda Luong, Edward M. Gunapala, Sarath D. TI Development of quantum well, quantum dot, and type II superlattice infrared photodetectors SO JOURNAL OF APPLIED REMOTE SENSING LA English DT Article DE infrared detector; photodetector; quantum well; quantum dot; superlattice; heterostructure; unipolar barrier ID FOCAL-PLANE ARRAYS; BROAD-BAND; SUPER-LATTICE; MU-M; WAVELENGTH; QWIP; PHOTODIODES; PERFORMANCE; DETECTORS; SUBMONOLAYER AB We present an overview of III-V semiconductor-based infrared detector and focal plane array development at the NASA Jet Propulsion Laboratory in recent years. Topics discussed include: (1) the development of long-wavelength quantum well infrared photodetector for imaging spectrometer applications, (2) the concept and realization of the submonolayer quantum dot infrared photodetector (SML-QDIP) as an alternative to the standard QDIP-based on Stranski-Krastanov (SK) quantum dots, (3) the mid-wavelength infrared quantum dot barrier infrared detector with extended cutoff wavelength, and (4) high-performance type-II superlattice long-wavelength infrared detectors based on the complementary barrier infrared detector architecture. (C) 2014 Society of Photo-Optical Instrumentation Engineers (SPIE) C1 [Ting, David Z.; Soibel, Alexander; Keo, Sam A.; Rafol, Sir B.; Mumolo, Jason M.; Liu, John K.; Hill, Cory J.; Khoshakhlagh, Arezou; Hoeglund, Linda; Luong, Edward M.; Gunapala, Sarath D.] CALTECH, Jet Prop Lab, Ctr Infrared Photodetectors, Pasadena, CA 91109 USA. RP Ting, DZ (reprint author), CALTECH, Jet Prop Lab, Ctr Infrared Photodetectors, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM David.Z.Ting@jpl.nasa.gov RI Soibel, Alexander/A-1313-2007 FU National Aeronautics and Space Administration FX The authors thank S. Bandara, K. K. Choi, J. Nguyen, Y.-C. Chang, E. S. Daniel, E. R. Blazejewski, D. R. Rhiger, and J. N. Schulman for discussions and help. We thank R. Liang, M. Herman, E. Kolawa, S. Khanna, T. Cwik, and P. Dimotakis of JPL and M. Tidrow of the U.S. Army Night Vision Electronics Sensor Directorate for encouragement and support. The research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Government sponsorship is acknowledged. NR 97 TC 7 Z9 7 U1 4 U2 51 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1931-3195 J9 J APPL REMOTE SENS JI J. Appl. Remote Sens. PD FEB 19 PY 2014 VL 8 AR 084998 DI 10.1117/1.JRS.8.084998 PG 19 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AB3UA UT WOS:000331714500001 ER PT J AU Berninger, JP Martinovic-Weigelt, D Garcia-Reyero, N Escalon, L Perkins, EJ Ankley, GT Villeneuve, DL AF Berninger, Jason P. Martinovic-Weigelt, Dalma Garcia-Reyero, Natalia Escalon, Lynn Perkins, Edward J. Ankley, Gerald T. Villeneuve, Daniel L. TI Using Transcriptomic Tools to Evaluate Biological Effects Across Effluent Gradients at a Diverse Set of Study Sites in Minnesota, USA SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID LARGE GENE LISTS; RISK-ASSESSMENT; BISPHENOL-A; IMPACTS; ECOTOXICOLOGY; EXPRESSION; SYSTEM; MODEL; FISH AB The aim of this study was to explore the utility of "omics" approaches in monitoring aquatic environments where complex, often unknown stressors make chemical-specific risk assessment untenable. We examined changes in the fathead minnow (Pimephales promelas) ovarian transcriptome following 4-day exposures conducted at three sites in Minnesota (MN, USA). Within each site, fish were exposed to water from three locations along a spatial gradient relative to a wastewater treatment plant (WWTP) discharge. After exposure, site-specific impacts on gene expression in ovaries were assessed. Using an intragradient point of comparison, biological responses specifically associated with the WWTP effluent were identified using functional enrichment analyses. Fish exposed to water from locations downstream of the effluent discharges exhibited many transcriptomic responses in common with those exposed to the effluent, indicating that effects of the discharge do not fully dissipate downstream. Functional analyses showed a range of biological pathways impacted through effluent exposure at all three sites. Several of those impacted pathways at each site could be linked to potential adverse reproductive outcomes associated with the hypothalamic pituitary gonadal (HPG) axis in female fathead minnows, specifically signaling pathways associated with oocyte meiosis, TGF-beta signaling, gonadotropin-releasing hormone (GnRH) and epidermal growth factor receptor family (ErbB), and gene sets associated with cyclin B-1 and metalloproteinase. The utility of this approach comes from the ability to identify biological responses to pollutant exposure, particularly those that can be tied to adverse outcomes at the population level and those that identify molecular targets for future studies. C1 [Berninger, Jason P.] US EPA, Natl Res Council, Duluth, MN 55804 USA. [Martinovic-Weigelt, Dalma] Univ St Thomas, St Paul, MN 55105 USA. [Garcia-Reyero, Natalia] Mississippi State Univ, Inst Genom Biocomp & Biotechnol, Starkville, MS 39762 USA. [Escalon, Lynn; Perkins, Edward J.] US Army Engineer Res & Dev Ctr, Vicksburg, MS 39180 USA. [Ankley, Gerald T.; Villeneuve, Daniel L.] US EPA, Midcontinent Ecol Div, Duluth, MN 55804 USA. RP Berninger, JP (reprint author), US EPA, Natl Res Council, 6201 Congdon Blvd, Duluth, MN 55804 USA. EM Berninger.Jason@epa.gov RI Berninger, Jason/O-2401-2016; OI Berninger, Jason/0000-0003-3045-7899; Martinovic-Weigelt, Dalma/0000-0002-9973-4965 FU US Army Environmental Quality Research Program [BAA 11-4838] FX The views expressed in this paper are those of the authors and do not necessarily reflect the views or policies of the US Environmental Protection Agency. This work was partly funded by the US Army Environmental Quality Research Program (including BAA 11-4838). Permission for publishing this information has been granted by the Chief of Engineers. The authors thank Kathy Lee (USGS), Heiko Schoenfuss (St. Cloud State University), Leah Wehmas, and their co-workers for their efforts in collecting samples that were used in this study and Anthony Schroeder for helpful comments on the manuscript. NR 29 TC 12 Z9 12 U1 3 U2 36 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X EI 1520-5851 J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD FEB 18 PY 2014 VL 48 IS 4 BP 2404 EP 2412 DI 10.1021/es4040254 PG 9 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA AB4QD UT WOS:000331774100038 PM 24433150 ER PT J AU Cutler, C Burke-Spolaor, S Vallisneri, M Lazio, J Majid, W AF Cutler, Curt Burke-Spolaor, Sarah Vallisneri, Michele Lazio, Joseph Majid, Walid TI The gravitational-wave discovery space of pulsar timing arrays SO PHYSICAL REVIEW D LA English DT Article ID BLACK-HOLE BINARIES; MILLISECOND PULSARS; LIMITS; RADIATION; SYSTEMS; MEMORY AB Recent years have seen a burgeoning interest in using pulsar timing arrays (PTAs) as gravitational-wave (GW) detectors. To date, that interest has focused mainly on three particularly promising source types: supermassive black hole binaries, cosmic strings, and the stochastic background from early-Universe phase transitions. In this paper, by contrast, our aim is to investigate the PTA potential for discovering unanticipated sources. We derive significant constraints on the available discovery space based solely on energetic and statistical considerations: we show that a PTA detection of GWs at frequencies above similar to 10(-5) Hz would either be an extraordinary coincidence or violate "cherished beliefs;" we show that for PTAs GW memory can be more detectable than direct GWs, and that, as we consider events at ever higher redshift, the memory effect increasingly dominates an event's total signal-to-noise ratio. The paper includes also a simple analysis of the effects of pulsar red noise in PTA searches, and a demonstration that the effects of periodic GWs in the similar to 10(-7)-10(-4.5) Hz band would not be degenerate with small errors in standard pulsar parameters (except in a few narrow bands). C1 [Cutler, Curt; Burke-Spolaor, Sarah; Vallisneri, Michele; Lazio, Joseph; Majid, Walid] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cutler, Curt; Vallisneri, Michele] CALTECH, Pasadena, CA 91125 USA. RP Cutler, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU NSF [PHY-1068881]; JPL RTD program FX C. C. gratefully acknowledges support from NSF Grant No. PHY-1068881. M. V. is grateful for support from the JPL RTD program. This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract to the National Aeronautics and Space Administration. NR 51 TC 9 Z9 9 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD FEB 18 PY 2014 VL 89 IS 4 AR 042003 DI 10.1103/PhysRevD.89.042003 PG 12 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AC0FF UT WOS:000332169500002 ER PT J AU Varnai, T Marshak, A AF Varnai, Tamas Marshak, Alexander TI Near-cloud aerosol properties from the 1 km resolution MODIS ocean product SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE aerosol; cloud; MODIS; satellite; solar radiation ID ATMOSPHERIC CORRECTION; CALIPSO OBSERVATIONS; OPTICAL-THICKNESS; VALIDATION; RETRIEVAL; ALGORITHM; RADIANCE; SEAWIFS; SURFACE; REGIONS AB This study examines aerosol properties in the vicinity of clouds by analyzing high-resolution atmospheric correction parameters provided in the MODIS (Moderate Resolution Imaging Spectroradiometer) ocean color product. The study analyzes data from a 2 week long period of September in 10 years, covering a large area in the northeast Atlantic Ocean. The results indicate that on the one hand, the Quality Assessment (QA) flags of the ocean color product successfully eliminate cloud-related uncertainties in ocean parameters such as chlorophyll content, but on the other hand, using the flags introduces a sampling bias in atmospheric products such as aerosol optical thickness (AOT) and Angstrom exponent. Therefore, researchers need to select QA flags by balancing the risks of increased retrieval uncertainties and sampling biases. Using an optimal set of QA flags, the results reveal substantial increases in optical thickness near cloudson average the increase is 50% for the roughly half of pixels within 5km from clouds and is accompanied by a roughly matching increase in particle size. Theoretical simulations show that the 50% increase in 550nm AOT changes instantaneous direct aerosol radiative forcing by up to 8W/m(2) and that the radiative impact is significantly larger if observed near-cloud changes are attributed to aerosol particles as opposed to undetected cloud particles. These results underline that accounting for near-cloud areas and understanding the causes of near-cloud particle changes are critical for accurate calculations of direct aerosol radiative forcing. C1 [Varnai, Tamas] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. [Varnai, Tamas; Marshak, Alexander] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD 20771 USA. RP Varnai, T (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. EM tamas.varnai@nasa.gov RI Marshak, Alexander/D-5671-2012 FU NASA FX We gratefully acknowledge support for this research by the NASA Radiation Sciences Program managed by Hal Maring and by the NASA CALIPSO project supervised by Charles Trepte as the technical officer. We also thank Ziauddin Ahmad, Bryan Franz, Gerhard Meister, and other members of the MODIS ocean color team, as well as Bob Charlson, Guoyong Wen, Rob Wood, and Weidong Yang for insightful discussions and help. NR 31 TC 7 Z9 7 U1 0 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 FEB 16 PY 2014 VL 119 IS 3 BP 1546 EP 1554 DI 10.1002/2013JD020633 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AD1LD UT WOS:000332994600029 ER PT J AU Kishcha, P da Silva, AM Starobinets, B Alpert, P AF Kishcha, Pavel da Silva, Arlindo M. Starobinets, Boris Alpert, Pinhas TI Air pollution over the Ganges basin and northwest Bay of Bengal in the early postmonsoon season based on NASA MERRAero data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE aerosols; Bay of Bengal ID AEROSOL OPTICAL DEPTH; SATELLITE; MODIS; IMPACT; REGION; WINTER; MODEL; INDIA AB The MERRA Aerosol Reanalysis (MERRAero) has been recently developed at NASA's Global Modeling Assimilation Office. This reanalysis is based on a version of the Goddard Earth Observing System-5 (GEOS-5) model radiatively coupled with Goddard Chemistry, Aerosol, Radiation, and Transport aerosols, and it includes assimilation of bias-corrected aerosol optical thickness (AOT) from the Moderate Resolution Imaging Spectroradiometer (MODIS) sensor on both Terra and Aqua satellites. In October over the period 2002-2009, MERRAero showed that AOT was lower over the east of the Ganges basin than over the northwest of the Ganges basin: this was despite the fact that the east of the Ganges basin should have produced higher anthropogenic aerosol emissions because of higher population density, increased industrial output, and transportation. This is evidence that higher aerosol emissions do not always correspond to higher AOT over the areas where the effects of meteorological factors on AOT dominate those of aerosol emissions. MODIS AOT assimilation was essential for correcting modeled AOT mainly over the northwest of the Ganges basin, where AOT increments were maximal. Over the east of the Ganges basin and northwest Bay of Bengal (BoB), AOT increments were low and MODIS AOT assimilation did not contribute significantly to modeled AOT. Our analysis showed that increasing AOT trends over northwest BoB (exceeding those over the east of the Ganges basin) were reproduced by GEOS-5, not because of MODIS AOT assimilation but mainly because of the model capability of reproducing meteorological factors contributing to AOT trends. Moreover, vertically integrated aerosol mass flux was sensitive to wind convergence causing aerosol accumulation over northwest BoB. C1 [Kishcha, Pavel; Starobinets, Boris; Alpert, Pinhas] Tel Aviv Univ, Dept Geophys Atmospher & Planetary Sci, IL-69978 Tel Aviv, Israel. [da Silva, Arlindo M.] NASA GSFC, Global Modeling & Assimilat Off, Greenbelt, MD USA. RP Kishcha, P (reprint author), Tel Aviv Univ, Dept Geophys Atmospher & Planetary Sci, IL-69978 Tel Aviv, Israel. EM pavel@cyclone.tau.ac.il FU international Virtual Institute DESERVE (Dead Sea Research Venue); German Helmholtz Association FX This study was made with support from and in cooperation with the international Virtual Institute DESERVE (Dead Sea Research Venue), funded by the German Helmholtz Association. We also acknowledge the GES-DISC Interactive Online Visualization and Analysis Infrastructure (Giovanni) for providing us with TRMM data. NR 39 TC 9 Z9 9 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 16 PY 2014 VL 119 IS 3 BP 1555 EP 1570 DI 10.1002/2013JD020328 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AD1LD UT WOS:000332994600030 ER PT J AU Hurst, DF Lambert, A Read, WG Davis, SM Rosenlof, KH Hall, EG Jordan, AF Oltmans, SJ AF Hurst, Dale F. Lambert, Alyn Read, William G. Davis, Sean M. Rosenlof, Karen H. Hall, Emrys G. Jordan, Allen F. Oltmans, Samuel J. TI Validation of Aura Microwave Limb Sounder stratospheric water vapor measurements by the NOAA frost point hygrometer SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE water vapor; stratosphere; measurements ID BOULDER; VARIABILITY; WASHINGTON; INCREASE; TRENDS; DC AB Differences between stratospheric water vapor measurements by NOAA frost point hygrometers (FPHs) and the Aura Microwave Limb Sounder (MLS) are evaluated for the period August 2004 through December 2012 at Boulder, Colorado, Hilo, Hawaii, and Lauder, New Zealand. Two groups of MLS profiles coincident with the FPH soundings at each site are identified using unique sets of spatiotemporal criteria. Before evaluating the differences between coincident FPH and MLS profiles, each FPH profile is convolved with the MLS averaging kernels for eight pressure levels from 100 to 26 hPa (similar to 16 to 25 km) to reduce its vertical resolution to that of the MLS water vapor retrievals. The mean FPH-MLS differences at every pressure level (100 to 26 hPa) are well within the combined measurement uncertainties of the two instruments. However, the mean differences at 100 and 83 hPa are statistically significant and negative, ranging from -0.460.22 ppmv (-10.34.8%) to -0.100.05 ppmv (-2.21.2%). Mean differences at the six pressure levels from 68 to 26 hPa are on average 0.8% (0.04 ppmv), and only a few are statistically significant. The FPH-MLS differences at each site are examined for temporal trends using weighted linear regression analyses. The vast majority of trends determined here are not statistically significant, and most are smaller than the minimum trends detectable in this analysis. Except at 100 and 83 hPa, the average agreement between MLS retrievals and FPH measurements of stratospheric water vapor is better than 1%. C1 [Hurst, Dale F.; Davis, Sean M.; Hall, Emrys G.; Jordan, Allen F.; Oltmans, Samuel J.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Hurst, Dale F.; Hall, Emrys G.; Jordan, Allen F.; Oltmans, Samuel J.] NOAA, Global Monitoring Div, Earth Syst Res Lab, Boulder, CO USA. [Lambert, Alyn; Read, William G.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Davis, Sean M.; Rosenlof, Karen H.] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO USA. RP Hurst, DF (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. EM Dale.Hurst@noaa.gov RI Davis, Sean/C-9570-2011; Rosenlof, Karen/B-5652-2008; Hurst, Dale/D-1554-2016; Manager, CSD Publications/B-2789-2015 OI Davis, Sean/0000-0001-9276-6158; Rosenlof, Karen/0000-0002-0903-8270; Hurst, Dale/0000-0002-6315-2322; FU NOAA Climate Program Office; US Global Climate Observing System (GCOS) program; National Aeronautics and Space Administration Upper Atmosphere Research Program; National Aeronautics and Space Administration FX The authors thank the NOAA Climate Program Office, the US Global Climate Observing System (GCOS) program, and the National Aeronautics and Space Administration Upper Atmosphere Research Program for financial support of the NOAA ESRL GMD long-term UTLS water vapor monitoring programs at Hilo, Lauder, and Boulder. FPH soundings are carefully performed at Lauder by Hamish Chisholm and Alan Thomas of New Zealand's National Institute for Water and Atmospheric Research, and at Hilo by David Nardini and Darryl Kuniyuki of the NOAA ESRL GMD. Work at the Jet Propulsion Laboratory, California Institute of Technology, was carried out under a contract with the National Aeronautics and Space Administration. NR 20 TC 15 Z9 15 U1 0 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 16 PY 2014 VL 119 IS 3 BP 1612 EP 1625 DI 10.1002/2013JD020757 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AD1LD UT WOS:000332994600034 ER PT J AU Lange, H Casassa, G Ivins, ER Schroder, L Fritsche, M Richter, A Groh, A Dietrich, R AF Lange, H. Casassa, G. Ivins, E. R. Schroeder, L. Fritsche, M. Richter, A. Groh, A. Dietrich, R. TI Observed crustal uplift near the Southern Patagonian Icefield constrains improved viscoelastic Earth models SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE crustal uplift; Earth model; glacial isostatic adjustment; Southern Patagonian Icefield; GNSS Geodesy; ice loss ID SEA-LEVEL RISE; AMERICA; ALASKA; EVOLUTION; FLOW AB Thirtyone GPS geodetic measurements of crustal uplift in southernmost South America determined extraordinarily high trend rates (> 35 mm/yr) in the northcentral part of the Southern Patagonian Icefield. These trends have a coherent pattern, motivating a refined viscoelastic glacial isostatic adjustment model to explain the observations. Two endmember models provide good fits: both require a lithospheric thickness of 36.55.3 km. However, one endmember has a mantle viscosity near =1.6 x10(18)Pas and an ice collapse rate from the Little Ice Age (LIA) maximum comparable to a lowest recent estimate of 1995-2012 ice loss at about -11 Gt/yr. In contrast, the other endmember has much larger viscosity: = 8.0 x10(18)Pas, half the post-LIA collapse rate, and a steadily rising loss rate in the twentiethcentury after AD 1943, reaching -25.9 Gt/yr during 1995-2012. Key Points Post-Little Ice Age load changes cause viscoelastic GIA response GPS results improve knowledge of ice load history since LIA and Earth model Gravity changes from the load changes and GIA influence interpretations of GRACE C1 [Lange, H.; Schroeder, L.; Fritsche, M.; Richter, A.; Groh, A.; Dietrich, R.] Tech Univ Dresden, Inst Planetare Geodasie, D-01062 Dresden, Germany. [Casassa, G.] Ctr Estudios Cient, Valdivia, Chile. [Ivins, E. R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Richter, A.] Univ Nacl La Plata, Fac Ciencias Astron & Geofis, La Plata, Buenos Aires, Argentina. RP Lange, H (reprint author), Tech Univ Dresden, Inst Planetare Geodasie, D-01062 Dresden, Germany. EM heiner.lange@tu-dresden.de OI Groh, Andreas/0000-0003-0106-5802 FU German Research Foundation DFG [DI 473/40-1]; Centro de Estudios Cient ficos (CECs); Chilean Government through the Centers of Excellence Base Financing Program of CONICYT; FONDECYT [1090752]; Jet Propulsion Laboratory, California Institute of Technology; NASAs Earth Surface and Interior Focus Area; Cryosphere Program, Science Mission Directorate FX The German part of the project was funded by the German Research Foundation DFG (grant DI 473/40-1). Gino Casassa was partially funded via the Centro de Estudios Cient ficos (CECs) (which in turn is funded by the Chilean Government through the Centers of Excellence Base Financing Program of CONICYT) and FONDECYT Project 1090752. Erik Ivins was supported by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA, and funded through NASAs Earth Surface and Interior Focus Area and the Cryosphere Program, Science Mission Directorate. We express our thanks for the fieldwork support and permits granted by CONAF and DIFROL. Marcelo Arevalo (Punta Arenas), Rodrigo Traub (Puerto Natales) and Hans Silva (Villa O'Higgins) supported the fieldwork. Special thanks go to Michael J. Willis and Andres Rivera, who provided the gridded data of the "surface elevation change rates" for the Southern Patagonian Icefield [Willis et al., 2012]. Finally, the valuable comments of the reviewers Chris Larsen and Wouter van der Wal are gratefully acknowledged. NR 36 TC 3 Z9 3 U1 1 U2 10 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 FEB 16 PY 2014 VL 41 IS 3 BP 805 EP 812 DI 10.1002/2013GL058419 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AD1JO UT WOS:000332990500009 ER PT J AU Nghiem, SV Hall, DK Rigor, IG Li, P Neumann, G AF Nghiem, S. V. Hall, D. K. Rigor, I. G. Li, P. Neumann, G. TI Effects of Mackenzie River discharge and bathymetry on sea ice in the Beaufort Sea SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Arctic sea ice; Mackenzie River; Beaufort Sea; river discharge; bathymetry; Antarctic ID TRENDS; BASIN; DELTA AB Mackenzie River discharge and bathymetry effects on sea ice in the Beaufort Sea are examined in 2012 when Arctic sea ice extent hit a record low. Satellite-derived sea surface temperature revealed warmer waters closer to river mouths. By 5 July 2012, Mackenzie warm waters occupied most of an open water area about 316,000km(2). Surface temperature in a common open water area increased by 6.5 degrees C between 14 June and 5 July 2012, before and after the river waters broke through a recurrent landfast ice barrier formed over the shallow seafloor offshore the Mackenzie Delta. In 2012, melting by warm river waters was especially effective when the strong Beaufort Gyre fragmented sea ice into unconsolidated floes. The Mackenzie and other large rivers can transport an enormous amount of heat across immense continental watersheds into the Arctic Ocean, constituting a stark contrast to the Antarctic that has no such rivers to affect sea ice. Key Points Warm waters intrusion from the Mackenzie River discharge impacts sea ice melt Strong Beaufort Gyre fragmented sea ice to precondition andenhance melting Arctic rivers constitute the starkest contrast to Antarctic without such river C1 [Nghiem, S. V.; Li, P.; Neumann, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Hall, D. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rigor, I. G.] Univ Washington, Seattle, WA 98195 USA. RP Nghiem, SV (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Son.V.Nghiem@jpl.nasa.gov FU National Aeronautics and Space Administration (NASA) Cryospheric Sciences Program; NASA FX The research carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology, and at NASA Goddard Space Flight Center (GSFC) was supported by the National Aeronautics and Space Administration (NASA) Cryospheric Sciences Program. Rigor is funded by NASA and other contributors to the U.S. Interagency Arctic Buoy Program. We thank Jody Hoon-Starr and Nick DiGirolamo of Science Systems and Applications, Inc. (SSAI), and Lisa Nguyen of JPL for programming help. We thank Michael Dettinger of the U.S. Geological Survey for his help with additional river discharge data. NR 36 TC 20 Z9 22 U1 2 U2 21 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 FEB 16 PY 2014 VL 41 IS 3 BP 873 EP 879 DI 10.1002/2013GL058956 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AD1JO UT WOS:000332990500018 ER PT J AU Kolli, KK Helmy, TA Peelukhana, SV Arif, I Leesar, MA Back, LH Banerjee, RK Effat, MA AF Kolli, Kranthi K. Helmy, Tarek A. Peelukhana, Srikara V. Arif, Imran Leesar, Massoud A. Back, Lloyd H. Banerjee, Rupak K. Effat, Mohamed A. TI Functional Diagnosis of Coronary Stenoses Using Pressure Drop Coefficient: A Pilot Study in Humans SO CATHETERIZATION AND CARDIOVASCULAR INTERVENTIONS LA English DT Article DE coronary disease; stenosis; cardiac hemodynamics; catheterization ID FRACTIONAL FLOW RESERVE; LESION SEVERITY; PORCINE MODEL; TASK-FORCE; MICROVASCULAR DYSFUNCTION; EUROPEAN-SOCIETY; ARTERY STENOSES; END-POINTS; HEART-RATE; IN-VITRO AB Objectives and BackgroundMyocardial fractional flow reserve (FFR) in conjunction with coronary flow reserve (CFR) is used to evaluate the hemodynamic severity of coronary lesions. However, discordant results between FFR and CFR have been observed in intermediate coronary lesions. A functional parameter, pressure drop coefficient (CDP; ratio of pressure drop to distal dynamic pressure), was assessed using intracoronary pressure drop (dp) and average peak velocity (APV). The CDP is a nondimensional ratio, derived from fundamental fluid dynamic principles. We sought to evaluate the correlation of CDP with FFR, CFR, and hyperemic stenosis resistance (HSR: ratio of pressure drop to APV) in human subjects. MethodsTwenty-seven patients with reversible perfusion defects based on SPECT were consented for the study before cardiac catheterization. Distal coronary pressure and APV were measured simultaneously for each coronary lesion using a Combowire((c)) during cardiac catheterization. Reference diameter, minimal lumen diameter, and %AS were obtained by quantitative coronary angiography. Maximum hyperemia was induced by IV adenosine (140 mu g/kg/min). CDP was calculated as, (p)/(0.5 x x APV(2)). The density of blood () was assumed to be 1.05 gm/cm(3). ResultsThe functional index, CDP, when correlated simultaneously with FFR and CFR, was found to have a significant correlation (r=0.61; P<0.05). Similarly a significant correlation was achieved when CDP was correlated with HSR (r=0.91; P<0.001). This is consistent with the definition of CDP, which is a functional parameter that includes both pressure and flow information. ConclusionsCDP, a nondimensional parameter combining simultaneous measurements of pressure drop and velocity data, can accurately define the severity of coronary stenoses and could prove advantageous clinically. (c) 2013 Wiley Periodicals, Inc. C1 [Kolli, Kranthi K.; Peelukhana, Srikara V.; Banerjee, Rupak K.] Univ Cincinnati, Sch Dynam Syst, Mech Engn Program, Cincinnati, OH 45267 USA. [Kolli, Kranthi K.; Helmy, Tarek A.; Peelukhana, Srikara V.; Arif, Imran; Leesar, Massoud A.; Banerjee, Rupak K.; Effat, Mohamed A.] Vet Affairs Med Ctr, Cincinnati, OH 45267 USA. [Helmy, Tarek A.; Arif, Imran; Leesar, Massoud A.; Effat, Mohamed A.] Univ Cincinnati, Div Cardiovasc Dis, Cincinnati, OH 45267 USA. [Back, Lloyd H.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Effat, MA (reprint author), Univ Cincinnati, Div Cardiovasc Dis, Cincinnati, OH 45267 USA. EM effatma@ucmail.uc.edu FU VA Merit Review grant [I01CX000342-01] FX Contract grant sponsor: This work was partly supported by a VA Merit Review grant; Contract grant number: I01CX000342-01. NR 26 TC 7 Z9 8 U1 1 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1522-1946 EI 1522-726X J9 CATHETER CARDIO INTE JI Catheter. Cardiovasc. Interv. PD FEB 15 PY 2014 VL 83 IS 3 BP 377 EP 385 DI 10.1002/ccd.25085 PG 9 WC Cardiac & Cardiovascular Systems SC Cardiovascular System & Cardiology GA AA7DO UT WOS:000331257600010 PM 23785016 ER PT J AU Tompson, SR AF Tompson, Sara R. TI Faraday, Maxwell, and the Electromagnetic Field: How Two Men Revolutionized Physics SO LIBRARY JOURNAL LA English DT Book Review C1 [Tompson, Sara R.] Jet Prop Lab Lib, Pasadena, CA 91109 USA. RP Tompson, SR (reprint author), Jet Prop Lab Lib, Pasadena, CA 91109 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD FEB 15 PY 2014 VL 139 IS 3 BP 126 EP 126 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA AB0OO UT WOS:000331492200225 ER PT J AU Pellicer, XM Linares, R Gutierrez, F Comas, X Roque, C Carbonel, D Zarroca, M Rodriguez, JAP AF Pellicer, X. M. Linares, R. Gutierrez, F. Comas, X. Roque, C. Carbonel, D. Zarroca, M. Rodriguez, J. A. P. TI Morpho-stratigraphic characterization of a tufa mound complex in the Spanish Pyrenees using ground penetrating radar and trenching, implications for studies in Mars SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE tufa mound; GPR; ITMC; trenching; geochronology; Mars ID EYRE SOUTH REGION; NATIONAL-PARK; SPRINGS; LAKE; SPAIN; TRAVERTINES; AUSTRALIA; DEPOSITS; CLASSIFICATION; RECORD AB The Isona tufa mound complex (ITMC), associated with artesian springs of the Areny-Montsec aquifer, Spanish Pyrenees, is a potential analog for water constructed landforms on Mars. We used Ground Penetrating Radar (GPR), trenching, sedimentological description of exposures, and radiocarbon and U-series dating methods for the geological characterization of the ITMC. Preliminary geomorphological mapping combined with sedimentological analyses permitted the recognition of the different facies and their spatial distribution. GPR surveys conducted next to an outcrop and a trench provided electromagnetic wave velocity in tufas (0.09 and 0.11 m ns(-1)) and determined the correspondence of the radar signatures with fades types. This was used to reconstruct the tufas internal structure and the depositional stages for two different contexts: (1) an upper unit representing the morphostratigraphic record of paleosprings - Tufa 1 - composed of relict tufa mounds older than 350 ka BP; and (2) a lower unit - Tufa 3 - associated with groundwater aquifer outlets (Basturs Lakes). The GPR data allowed depicting the signatures for the vent, pool, rimstone, palustrine, dam, cascade and slope facies. A relationship was inferred between the age of the tufas and the radar signature, in terms of relative amplitude and signal attenuation. Older dry tufas with advanced diagenesis and karstification are characterized by well-defined GPR reflectors and lower attenuation than younger tufas, associated with aquifer discharge and shallower water tables. U-series and radiocarbon ages obtained from the Basturs Lakes tufas indicate that these have been active since 106 ka BP during both cold and mild Marine Isotopic Stages (MIS). We hypothesize that tufas related to the deep-seated Areny-Montsec confined karst aquifer were insensitive to climate variations. Landforms reminiscent of the ITMC have been detected during the last decade on Mars. Since GPR will be part of the ExoMars Rover of the European Space Agency (ESA) mission projected for 2018, we anticipate that our results may be able to constrain the interpretation of landforms possibly related to water on Mars. (C) 2013 Elsevier B.V. All rights reserved. C1 [Pellicer, X. M.] Geol Survey Ireland, Beggars Bush, Dublin 4, Ireland. [Linares, R.; Zarroca, M.] Univ Autonoma Barcelona, Dept Geol, E-08193 Barcelona, Spain. [Gutierrez, F.; Carbonel, D.] Univ Zaragoza, Dept Ciencias Tierra, Zaragoza, Spain. [Comas, X.] Florida Atlantic Univ, Dept Geosci, Davie, FL USA. [Roque, C.] Univ Girona, Area Geodinam Externa & Geomorfol, Girona, Spain. [Rodriguez, J. A. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Pellicer, XM (reprint author), Geol Survey Ireland, Beggars Bush, Haddington Rd, Dublin 4, Ireland. OI Pellicer, Xavier/0000-0002-1508-728X; Carbonel Portero, Domingo/0000-0001-6175-0364; Zarroca, Mario/0000-0001-6907-1892; Roque Pau, Carles/0000-0003-0650-160X FU Ministerio de Ciencia e Innovacion and Fondo Europeo de Desarrollo Regional [CGL2005-02404, CGL2010-16775]; Estacio Biologica del Pallars Jussa under AGAUR [2010-ACOM-00006] FX This research work was co-funded by the national projects CGL2005-02404 and CGL2010-16775 (Ministerio de Ciencia e Innovacion and Fondo Europeo de Desarrollo Regional) and by the Estacio Biologica del Pallars Jussa under the 2010-ACOM-00006 (AGAUR) grant scheme. The authors are very grateful to Oriol Roque and Veronica Rodriguez for their assistance during the geophysical campaigns. We also thank three anonymous reviewers for their thorough and constructive comments and suggestions on the review of this paper. NR 57 TC 4 Z9 4 U1 2 U2 16 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 FEB 15 PY 2014 VL 388 BP 197 EP 210 DI 10.1016/j.epsl.2013.11.052 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AB0SO UT WOS:000331502600020 ER PT J AU Fenton, LK Michaels, TI Beyer, RA AF Fenton, Lori K. Michaels, Timothy I. Beyer, Ross A. TI Inverse maximum gross bedform-normal transport 1: How to determine a dune-constructing wind regime using only imagery SO ICARUS LA English DT Article; Proceedings Paper CT 3rd International Planetary Dunes Workshop CY JUN 12-15, 2012 CL Lowell Observ, Flagstaff, AZ HO Lowell Observ DE Mars, Atmosphere; Geological processes; Meteorology; Image processing ID GREAT-SAND-DUNES; DIRECTIONALLY VARYING FLOWS; STAR DUNES; DYNAMIC PROCESSES; NATIONAL-PARK; AIR-FLOW; FIELD; PATTERNS; COLORADO; WATER AB It has been a goal of aeolian science to use bedforms as indicators of local and regional sediment transport and atmospheric circulation, but even with the application of the rule of maximum gross-bedform normal transport (MGBNT), the underdetermined nature of the problem has precluded its application in all but the most simple cases. We present a method to apply the rule of MGBNT and its inverse (IMGBNT) from analysis of aeolian dune crestlines derived from aerial imagery. Although the solutions to IMGBNT analysis are non-unique, the possible transport vectors influencing bedform morphology can often be constrained by making inferences regarding bedform type (e.g., transverse, oblique, or longitudinal), resultant drift direction, and the ratio of transport vector magnitudes. The technique is demonstrated on the Great Sand Dunes, located in Colorado, USA. This dune field has a wide array of dune morphologies; eight crestline sets were identified and mapped. IMGBNT analysis and the subsequent constraint of possible solutions suggests that transport vectors from the southeast and southwest, with a SE:SW transport ratio of similar to 1:2, produce oblique north-south oriented dunes that dominate the main dune field. These results compare favorably with MGBNT analysis of meteorologic measurements from three stations located adjacent to the Great Sand Dunes, which predict dune types and orientations similar to those observed in their vicinity. (C) 2013 Elsevier Inc. All rights reserved. C1 [Fenton, Lori K.; Michaels, Timothy I.; Beyer, Ross A.] SETI Inst, Mountain View, CA 94043 USA. [Beyer, Ross A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Fenton, LK (reprint author), SETI Inst, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA. EM lfenton@carlsagancenter.org NR 42 TC 9 Z9 11 U1 0 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 FEB 15 PY 2014 VL 230 SI SI BP 5 EP 14 DI 10.1016/j.icarus.2013.04.001 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 298OF UT WOS:000330333100002 ER PT J AU Hayward, RK Fenton, LK Titus, TN AF Hayward, R. K. Fenton, L. K. Titus, T. N. TI Mars Global Digital Dune Database (MGD(3)): Global dune distribution and wind pattern observations SO ICARUS LA English DT Article; Proceedings Paper CT 3rd International Planetary Dunes Workshop CY JUN 12-15, 2012 CL Lowell Observ, Flagstaff, AZ HO Lowell Observ DE Mars; Mars, Surface; Mars, Climate ID DIRECTIONALLY VARYING FLOWS; GENERAL-CIRCULATION MODEL; NORTH POLAR-REGION; AEOLIAN PROCESSES; MARTIAN SURFACE; SAND TRANSPORT; STRATIGRAPHY; ALIGNMENT; SURVEYOR; FIELDS AB The Mars Global Digital Dune Database (MGD(3)) is complete and now extends from 90 degrees N to 90 degrees S latitude. The recently released south pole (SP) portion (MC-30) of MGD(3) adds similar to 60,000 km(2) of medium to large-size dark dune fields and similar to 15,000 km(2) of sand deposits and smaller dune fields to the previously released equatorial (EQ similar to 70,000 km(2)), and north pole (NP, similar to 845,000 km(2)) portions of the database, bringing the global total to similar to 975,000 km(2). Nearly all NP dunes are part of large sand seas, while the majority of EQ and SP dune fields are individual dune fields located in craters. Despite the differences between Mars and Earth, their dune and dune field morphologies are strikingly similar. Bullseye dune fields, named for their concentric ring pattern, are the exception, possibly owing their distinctive appearance to winds that are unique to the crater environment. Ground-based wind directions are derived from slipface (SF) orientation and dune centroid azimuth (DCA), a measure of the relative location of a dune field inside a crater. SF and DCA often preserve evidence of different wind directions, suggesting the importance of local, topographically influenced winds. In general however, ground-based wind directions are broadly consistent with expected global patterns, such as polar easterlies. Intriguingly, between 40 S and 80 S latitude both SF and DCA preserve their strongest, though different, dominant wind direction, with transport toward the west and east for SF-derived winds and toward the north and west for DCA-derived winds. Published by Elsevier Inc. C1 [Hayward, R. K.; Titus, T. N.] US Geol Survey, Flagstaff, AZ 86001 USA. [Fenton, L. K.] NASA, Ames Res Ctr, Carl Sagan Ctr, Moffett Field, CA 94035 USA. RP Hayward, RK (reprint author), US Geol Survey, 2255 N Gemini Dr, Flagstaff, AZ 86001 USA. EM rhayward@usgs.gov NR 57 TC 14 Z9 14 U1 3 U2 22 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 FEB 15 PY 2014 VL 230 SI SI BP 38 EP 46 DI 10.1016/j.icarus.2013.04.011 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 298OF UT WOS:000330333100005 ER PT J AU Fenton, LK Michaels, TI Chojnacki, M Beyer, RA AF Fenton, Lori K. Michaels, Timothy I. Chojnacki, Matthew Beyer, Ross A. TI Inverse maximum gross bedform-normal transport 2: Application to a dune field in Ganges Chasma, Mars and comparison with HiRISE repeat imagery and MRAMS SO ICARUS LA English DT Article; Proceedings Paper CT 3rd International Planetary Dunes Workshop CY JUN 12-15, 2012 CL Lowell Observ, Flagstaff, AZ HO Lowell Observ DE Mars, Atmosphere; Mars, Surface; Mars, Climate; Titan; Mars ID DIRECTIONALLY VARYING FLOWS; LONGITUDINAL DUNES; AEOLIAN PROCESSES; VALLES-MARINERIS; FORMING WINDS; CASSINI RADAR; LINEAR DUNES; LANDING SITE; TITAN; CLIMATE AB Inverse maximum gross bedform-normal transport (IMGBNT) analysis has been applied to Context Camera (CTX) images of the largest dune field in Ganges Chasma on Mars. The dune field was selected for its position in a likely complex, multi-directional wind regime. Results indicate that four main winds are responsible for simultaneous construction of the dune field, including along-chasma winds from the ESE, winds blowing down a nearby re-entrant from the NE, winds blowing down the adjacent chasma wall from the NW, and chasma floor winds from the SW. Each wind represents a transport vector that dominates dune morphology at its respective edge of the dune field, such that the central axis of the dune field reflects the convergence of the three most prominent winds (ESE, NW, and SW). The Mars Regional Atmospheric Modeling System (MRAMS) was run at twelve times throughout the martian year to provide context for the local wind patterns. Potential sand fluxes calculated from MRAMS output show that three major air flows from the ENE-E, NNE-NE, and NNW-N converge near the location of the dune field. These flows likely correspond to the ESE, NE, and NW winds identified from IMGBNT analysis, respectively. MRAMS output shows that the flows with major northerly components are produced by larger-scale Hadley return flow constructively combining with nighttime downslope winds; the flow with a major easterly component is likely produced by equatorial easterly "trade" winds constructively combining with the diurnal tide and/or local topography. Although the model correctly predicts the major elements of the local wind pattern, some aspects are either over- or underrepresented, demonstrating the value of using aeolian morphological analysis to conclusively constrain the major sand-moving winds on Mars. Overlapping High Resolution Imaging Experiment (HiRISE) images of barchanoid dunes at the northernmost edge of the dune field indicate that these dunes are currently migrating southward at similar to 5 m/Mars year (similar to 2.6 m/Earth year); the direction of migration is consistent with both MRAMS predictions in this location and the NW/NE winds found from IMGBNT analysis. Dune morphology suggests that sand in the northwestern part of the dune field is likely to be derived from the adjacent chasma wall to the north and northwest, and sand in the southeastern part of the dune field was probably transported from farther east along the main chasma floor. (C) 2013 Elsevier Inc. All rights reserved. C1 [Fenton, Lori K.; Michaels, Timothy I.; Beyer, Ross A.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Chojnacki, Matthew] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Beyer, Ross A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Fenton, LK (reprint author), SETI Inst, Carl Sagan Ctr, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA. EM lfenton@carlsagancenter.org RI Chojnacki, Matthew/A-4245-2013 OI Chojnacki, Matthew/0000-0001-8497-8994 NR 82 TC 6 Z9 6 U1 0 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 FEB 15 PY 2014 VL 230 SI SI BP 47 EP 63 DI 10.1016/j.icarus.2013.07.009 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 298OF UT WOS:000330333100006 ER PT J AU Le Gall, A Janssen, MA Kirk, RL Lorenz, RD AF Le Gall, A. Janssen, M. A. Kirk, R. L. Lorenz, R. D. TI Modeling microwave backscatter and thermal emission from linear dune fields: Application to Titan SO ICARUS LA English DT Article; Proceedings Paper CT 3rd International Planetary Dunes Workshop CY JUN 12-15, 2012 CL Lowell Observ, Flagstaff, AZ HO Lowell Observ DE Radar observations; Radio observations; Satellites, Surfaces; Titan ID CASSINI RADAR; SAND DUNES; SAHARA DESERT; ERG SURFACES; IMAGES; SCATTEROMETRY; MORPHOMETRY; WAVELENGTH; SPACEBORNE; SAR AB We present an electromagnetic model that relates the microwave backscatter and thermal emission from linear dune fields to their compositional, physical (roughness, subsurface porosity/heterogeneity) and geometrical (slope, orientation) properties. This model shows the value of exploring these highly directional and geometrical features in light of both their backscattering cross-section and emissivity. Compared to Cassini concurrent radar and radiometry data acquired from October 2004 to June 2011 over Titan's dune fields, it provides clues to understand variations among dune regions on the largest Saturn's moon. In particular, it brings a formal support to the idea first advanced in Le Gall et al. (Le Gall, A., Janssen, M.A., Wye, LC., Hayes, A.G., Radebaugh, J., Savage, C., Zebker, H., Lorenz, R.D., Lunine, J.I., Kirk, R.L., Lopes, R.M.C., Wall, S., Callahan, P., Stofan, E.R., Farr, T. and the Cassini Radar Team [2011]. Icarus 213, 608-624) that the size of the interdune valleys (relative to that of the dunes) varies across Titan as well as the diffuse scattering properties of these interdune areas due to different thickness of sand cover (i.e. bedrock contribution) or degree of compaction/heterogeneity of the sand cover. The Fensal and Belet dune fields, in particular, are quite different in terms of these properties. The comparison between the model and Cassini data also reveals the potential presence of structures, possibly small-superposed dunes, oriented perpendicular to the dune crests in the Aztlan region. (C) 2013 Elsevier Inc. All rights reserved. C1 [Le Gall, A.] Univ Versailles St Quentin, Observat Spatiales LATMOS, Atmospheres Lab, F-78280 Guyancourt, France. [Janssen, M. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kirk, R. L.] US Geol Survey, Branch Astrogeol, Flagstaff, AZ 86001 USA. [Lorenz, R. D.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA. RP Le Gall, A (reprint author), Univ Versailles St Quentin, Observat Spatiales LATMOS, Atmospheres Lab, 11 Bd Alembert, F-78280 Guyancourt, France. EM Alice.Legall@latmos.ipsl.fr RI Lorenz, Ralph/B-8759-2016 OI Lorenz, Ralph/0000-0001-8528-4644 NR 38 TC 3 Z9 3 U1 1 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD FEB 15 PY 2014 VL 230 SI SI BP 198 EP 207 DI 10.1016/j.icarus.2013.06.009 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 298OF UT WOS:000330333100017 ER PT J AU Paillou, P Bernard, D Radebaugh, J Lorenz, R Le Gall, A Farr, T AF Paillou, Ph. Bernard, D. Radebaugh, J. Lorenz, R. Le Gall, A. Farr, T. TI Modeling the SAR backscatter of linear dunes on Earth and Titan SO ICARUS LA English DT Article; Proceedings Paper CT 3rd International Planetary Dunes Workshop CY JUN 12-15, 2012 CL Lowell Observ, Flagstaff, AZ HO Lowell Observ DE Titan; Titan surface; Radar observations; Earth ID CASSINI RADAR; IMAGING RADAR; SAND DUNES; SURFACE; SPACEBORNE; SCATTEROMETRY; DESERT; SAHARA; IMAGES; MAPPER AB We modeled the Synthetic Aperture Radar (SAR) response of linear dunes of the Great Sand Sea in Egypt using a single surface scattering term, based on Integral Equation and Physical Optics Models. Using multi-frequency SIR-C/X-SAR radar scenes and topography obtained from the Shuttle Radar Topography Mission (SRTM), we were able to estimate reasonable values for the parameters describing the surface roughness of the dunes. As the linear dunes of the Great Sand Sea are relevant analogs for the linear dunes observed on Titan by the Cassini Radar instrument, these results were thus used as a starting point to simulate the radar response of Titan's dunes, as imaged by the Radar instrument onboard the Cassini spacecraft during the T8 flyby in October 2005. We show that a single surface scattering term is not sufficient to simulate the radar signal backscattered by the dunes on Titan: one has to add a diffuse scattering term, indicating that Titan's dunes are likely to have somewhat inhomogeneous internal structures related to porosity and/or internal layering. Our results also indicate that the dunes on Titan should be close to perfectly smooth, possibly because of the formation of smaller ripples than on Earth, plus smoothing resulting from precipitation events. (C) 2013 Elsevier Inc. All rights reserved. C1 [Paillou, Ph.; Bernard, D.] Univ Bordeaux, UMR 5804, LAB, F-33270 Floirac, France. [Radebaugh, J.] Brigham Young Univ, Dept Geol Sci, Provo, UT 84602 USA. [Lorenz, R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Le Gall, A.] Univ Versailles, LATMOS, F-78280 Guyancourt, France. [Farr, T.] CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. RP Paillou, P (reprint author), Univ Bordeaux, UMR 5804, LAB, F-33270 Floirac, France. EM philippe.paillou@obs.u-bordeaux1.fr RI Lorenz, Ralph/B-8759-2016; OI Lorenz, Ralph/0000-0001-8528-4644; Farr, Thomas/0000-0001-5406-2096 NR 38 TC 4 Z9 4 U1 1 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 FEB 15 PY 2014 VL 230 SI SI BP 208 EP 214 DI 10.1016/j.icarus.2013.04.017 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 298OF UT WOS:000330333100018 ER PT J AU Williford, KH Grice, K Holman, A McElwain, JC AF Williford, Kenneth H. Grice, Kliti Holman, Alexander McElwain, Jennifer C. TI An organic record of terrestrial ecosystem collapse and recovery at the Triassic-Jurassic boundary in East Greenland SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID CARBON-ISOTOPE STRATIGRAPHY; ATLANTIC MAGMATIC PROVINCE; POLYCYCLIC AROMATIC-HYDROCARBONS; FLOOD-BASALT VOLCANISM; PHOTIC ZONE EUXINIA; TRIASSIC/JURASSIC BOUNDARY; MASS EXTINCTION; N-ALKANES; THERMAL MAXIMUM; INDIVIDUAL HYDROCARBONS AB Terrestrial ecosystem collapse at the end of the Triassic Period coincided with a major mass extinction in the marine realm and has been linked to increasing atmospheric carbon dioxide, global warming, and fire activity. Extractable hydrocarbons in samples from the fluvial Triassic-Jurassic boundary section at Astartekloft, East Greenland were analyzed to investigate the molecular and isotopic organic record of biotic and environmental change during this event. Carbon isotopic compositions of individual plant wax lipids show a >4 parts per thousand negative excursion coinciding with peak extinction and a further decrease of 2 parts per thousand coinciding with peak pCO(2) as estimated from the stomatal indices of fossil Gingkoales. An increase of similar to 30 parts per thousand in the hydrogen isotopic compositions of the same plant wax lipids coincides with ecosystem collapse, suggesting that the biotic crisis was accompanied by strong hydrologic change. Concentrations of polycyclic aromatic hydrocarbons related to combustion also increase together with abrupt plant diversity loss and peak with fossil charcoal abundance and maximum plant turnover, supporting the role of fire in terrestrial extinctions. Anomalously high concentrations of a monoaromatic diterpenoid related to gymnosperm resin derivatives (and similar to dehydroabietane) occur uniquely in samples from the boundary bed, indicating that environmental stress factors leading to peak plant extinction stimulated increased resin production, and that plant resin derivatives may be effective biomarkers of terrestrial ecosystem stress. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Williford, Kenneth H.; Grice, Kliti; Holman, Alexander] Curtin Univ Technol, Western Australian Organ & Isotope Geochem Ctr, Dept Chem, Perth, WA 6845, Australia. [McElwain, Jennifer C.] Univ Coll Dublin, Sch Biol & Environm Sci, Dublin 4, Ireland. RP Grice, K (reprint author), CALTECH, Jet Prop Lab, M-S 183-301, Pasadena, CA 91104 USA. EM kenneth.h.williford@jpl.nasa.gov; k.grice@curtin.edu.au OI McElwain, Jennifer/0000-0002-1729-6755 FU ARC Discovery grant of QEII Fellowship [DP0877167]; ARC Discovery DORA Fellowship; EU Marie Curie Excellence Grant [MEXT-CT-2006-042531]; National Geographic Society [7038-01]; ERC [StG 279962] FX We thank Geoff Chidlow and Sue Wang (Curtin University) for technical support. We acknowledge Dr. Lindsay Byrne (University of Western Australia) for providing NMR data. Comments by Associate Editor Jochen Brocks and three anonymous reviewers improved the quality of this manuscript. Funding was provided by ARC Discovery grant of QEII Fellowship (K. Grice DP0877167) and subsequent ARC Discovery DORA Fellowship (K. Grice), EU Marie Curie Excellence Grant MEXT-CT-2006-042531, National Geographic Society 7038-01, ERC StG 279962, NR 76 TC 10 Z9 10 U1 3 U2 40 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 FEB 15 PY 2014 VL 127 BP 251 EP 263 DI 10.1016/j.gca.2013.11.033 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 291QC UT WOS:000329842900016 ER PT J AU Yu, ML Wang, ZJ Liu, Y AF Yu, Meilin Wang, Z. J. Liu, Yen TI On the accuracy and efficiency of discontinuous Galerkin, spectral difference and correction procedure via reconstruction methods SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE Discontinuous Galerkin; Spectral difference; Correction procedure via reconstruction; High order accuracy; Computational efficiency; Curved element; Quadrature-free ID HIGH-ORDER ACCURATE; NAVIER-STOKES EQUATIONS; FINITE-ELEMENT-METHOD; CONSERVATION-LAWS; UNSTRUCTURED GRIDS; BASIC FORMULATION; VOLUME METHODS; IMPLEMENTATION; SYSTEMS; QUADRATURE AB Numerical accuracy and efficiency of several discontinuous high-order methods, including the quadrature-based discontinuous Galerkin (QDG), nodal discontinuous Galerkin (NDG), spectral difference (SD) and flux reconstruction/correction procedure via reconstruction (FR/CPR), for the conservation laws are analyzed and compared on both linear and curved quadrilateral elements. On linear elements, all the above schemes are one-dimensional in each natural coordinate direction. However, on curved elements, not all schemes can be reduced to a one-dimensional form, although the SD and CPR formulations remain one-dimensional by design. The efficiency and accuracy of various formulations are compared on highly skewed curved elements. Several benchmark problems are simulated to further evaluate the performance of these schemes. (C) 2013 Elsevier Inc. All rights reserved. C1 [Yu, Meilin; Wang, Z. J.] Univ Kansas, Lawrence, KS 66045 USA. [Liu, Yen] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Yu, ML (reprint author), Univ Kansas, Lawrence, KS 66045 USA. RI Wang, Z.J./A-9628-2010 OI Wang, Z.J./0000-0002-6203-6303 FU AFOSR [FA95501210286]; NASA [NNX12AK04A] FX Yu and Wang are partially funded by AFOSR grant FA95501210286 and NASA grant NNX12AK04A. The views and conclusions contained herein are those of the authors and should not be interpreted as necessarily representing the official policies or endorsements, either expressed or implied, of AFOSR, NASA, or the US Government. NR 51 TC 10 Z9 10 U1 1 U2 5 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 FEB 15 PY 2014 VL 259 BP 70 EP 95 DI 10.1016/j.jcp.2013.11.023 PG 26 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 286YZ UT WOS:000329506500006 ER PT J AU Barrett, HP Kennedy, WJ Boucher, DS AF Barrett, Hayden P. Kennedy, W. Joshua Boucher, David S. TI Spectroscopic Characterization of P3HT/SWNT Composites Synthesized Using In Situ GRIM Methods: Improved Polymer Ordering via Nanoscaffolding SO JOURNAL OF POLYMER SCIENCE PART B-POLYMER PHYSICS LA English DT Article DE carbon nanotubes; composites; Grignard metathesis; P3HT; photophysics; polystyrene; Raman spectroscopy; synthesis ID WALLED CARBON NANOTUBES; RESONANT RAMAN-SCATTERING; ORGANIC SOLAR-CELLS; REGIOREGULAR POLY(3-ALKYLTHIOPHENES); CONJUGATED POLYMERS; PHOTOVOLTAIC DEVICES; GRIGNARD METATHESIS; POLY(3-HEXYLTHIOPHENE); MORPHOLOGY; DISPERSION AB Poly(3-hexylthiophene)/single-walled carbon nanotube (P3HT/SWNT) materials are synthesized using an in-situ Grignard metathesis approach. The structural properties and photophysics of the materials are studied using a multitude of techniques, including H-1 NMR, FTIR, UV-vis absorption, Raman, photoluminescence (PL), and transient absorption spectroscopies. P3HT/SWNT composites with high P3HT regioregularity (rr>96%) are observed. Raman spectroscopic data on the solid samples reveals an increase in the dispersion rate parameter with increasing SWNT concentration, thereby indicating close overlap and strong interactions between P3HT and the carbon nanotubes. Changes in the solution-phase PL quantum yields and excited-state lifetimes relative to pure P3HT support these conclusions, and indicate that strong interactions persist even after the composites are dispersed in organic solvents. The high regioregularity and enhanced P3HT-SWNT interactions are promising attributes for improving the morphology and efficiency of functional P3HT/SWNT materials. (c) 2013 Wiley Periodicals, Inc. J. Polym. Sci. Part B: Polym. Phys. 2014, 52, 310-320 C1 [Barrett, Hayden P.; Boucher, David S.] Coll Charleston, Dept Chem & Biochem, Sch Sci & Math, Charleston, SC 29424 USA. [Kennedy, W. Joshua] NASA, Mat & Proc Branch, Struct Engn Div, Johnson Space Ctr, Houston, TX 77058 USA. RP Boucher, DS (reprint author), Coll Charleston, Dept Chem & Biochem, Sch Sci & Math, Charleston, SC 29424 USA. EM boucherds@cofc.edu FU College of Charleston, Faculty Research and Development Committee (Faculty R&D Starter Grant Fund); Howard Hughes Medical Institute, Pre-College and Undergraduate Science Education Program (HHMI Grant) [52006290, 52007537]; NASA Johnson Space Center's Engineering Directorate FX A special thanks to Richard Loomis (Department of Chemistry, Washington University in St. Louis). The authors acknowledge the financial support of the College of Charleston, Faculty Research and Development Committee (Faculty R&D Starter Grant Fund), the Howard Hughes Medical Institute, Pre-College and Undergraduate Science Education Program (HHMI Grant No. 52006290 and 52007537), and NASA Johnson Space Center's Engineering Directorate. NR 65 TC 4 Z9 4 U1 3 U2 30 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0887-6266 EI 1099-0488 J9 J POLYM SCI POL PHYS JI J. Polym. Sci. Pt. B-Polym. Phys. PD FEB 15 PY 2014 VL 52 IS 4 BP 310 EP 320 DI 10.1002/polb.23407 PG 11 WC Polymer Science SC Polymer Science GA 285CK UT WOS:000329370600004 ER PT J AU Kaul, AB AF Kaul, Anupama B. TI Two-dimensional layered materials: Structure, properties, and prospects for device applications SO JOURNAL OF MATERIALS RESEARCH LA English DT Article ID TRANSITION-METAL DICHALCOGENIDES; FIELD-EFFECT TRANSISTORS; ATOMICALLY THIN MOS2; ELECTRONIC-STRUCTURE; INTEGRATED-CIRCUITS; MAGNETIC-PROPERTIES; MONOLAYER MOS2; DIRECT-BANDGAP; HIGH-MOBILITY; BILAYER MOS2 AB Graphene's layered structure has opened new prospects for the exploration of properties of other monolayer-thick two-dimensional (2D) layered crystals. The emergence of these inorganic 2D atomic crystals beyond graphene promises a diverse spectrum of properties. For example, hexagonal-boron nitride (h-BN), a layered material closest in structure to graphene is an insulator, while niobium selenide (NbSe2), a transition metal dichalcogenide, is metallic, and monolayers of other transition metal dichalcogenides such as molybdenum disulfide (MoS2) and tungsten disulfide (WS2) are direct band gap semiconductors. The rich spectrum of properties exhibited by these 2D layered material systems can potentially be engineered on-demand and creates exciting prospects for using such systems in device applications ranging from electronics, photonics, energy harvesting, flexible electronics, transparent electrodes, and sensing. A review of the structure, properties, and the emerging device applications of these materials is presented in this paper. While the layered structure of these materials makes them amenable to mechanical exfoliation for quickly unveiling their novel properties and for fabricating proof-of-concept devices, an overview of the synthesis routes that can potentially enable scalable avenues for forming these 2D atomic crystals is also discussed. C1 [Kaul, Anupama B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kaul, Anupama B.] Natl Sci Fdn, Arlington, VA 22230 USA. RP Kaul, AB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM anu.kaul@jpl.nasa.gov FU NSF independent research and development (IRD) program FX ABK wishes to acknowledge support for this through the NSF independent research and development (IR&D) program. NR 87 TC 32 Z9 32 U1 21 U2 379 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0884-2914 EI 2044-5326 J9 J MATER RES JI J. Mater. Res. PD FEB 14 PY 2014 VL 29 IS 3 BP 348 EP 361 DI 10.1557/jmr.2014.6 PG 14 WC Materials Science, Multidisciplinary SC Materials Science GA AB7IJ UT WOS:000331962700005 ER PT J AU Sandoz-Rosado, E Page, W O'Brien, D Przepioski, J Mo, D Wang, B Ngo-Duc, TT Gacusan, J Winter, MW Meyyappan, M Cormia, RD Takahashi, S Oyea, MM AF Sandoz-Rosado, Emil Page, William O'Brien, David Przepioski, Joshua Mo, Dennis Wang, Benjamin Ngo-Duc, Tam-Triet Gacusan, Jovi Winter, Michael W. Meyyappan, M. Cormia, Robert D. Takahashi, Shuhei Oyea, Michael M. TI Vertical graphene by plasma-enhanced chemical vapor deposition: Correlation of plasma conditions and growth characteristics SO JOURNAL OF MATERIALS RESEARCH LA English DT Article DE vertical graphene; Raman spectroscopy; defects; plasma-enhanced CVD (PECVD) ID CARBON NANOTUBES; LAYER GRAPHENE; DC PLASMA; HYDROGEN; SINGLE; FABRICATION; NANOSHEETS AB Vertically aligned graphene was grown by plasma-enhanced chemical vapor deposition using methane feedstock. Optical emission spectroscopy (OES) was used to monitor the plasma species, and Raman spectroscopy was used for characterizing the properties of as-grown vertically aligned graphene. OES-derived information on plasma species, such as C, C-2, CH, and H, are correlated with the properties of the vertically aligned graphene. Graphene grown at 250 W and 15 sccm exhibited the lowest amount of defects. Although OES peak intensities occurred at the highest power and lowest flow conditions, the OES peak ratios of plasma species had a greater dependence on flow rate and exhibited a saddle point in the atomic C/H ratio corresponding to optimal growth involving the lowest amount of overall defects. Plasma diagnostics provides a valuable approach to optimize growth characteristics and material properties. C1 [Sandoz-Rosado, Emil; Page, William; O'Brien, David; Przepioski, Joshua; Mo, Dennis; Wang, Benjamin; Ngo-Duc, Tam-Triet; Gacusan, Jovi; Winter, Michael W.; Meyyappan, M.; Takahashi, Shuhei; Oyea, Michael M.] NASA Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. [Cormia, Robert D.] NASA Ames Res Ctr, Foothill Coll, Moffett Field, CA 94035 USA. [Cormia, Robert D.; Takahashi, Shuhei; Oyea, Michael M.] NASA Ames Res Ctr, UCSC NASA ARC Adv Studies Labs, Moffett Field, CA 94035 USA. [Takahashi, Shuhei; Oyea, Michael M.] Univ Calif Santa Cruz, Dept Elect Engn, Santa Cruz, CA 95064 USA. RP Oyea, MM (reprint author), NASA Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. EM Michael.M.Oye@nasa.gov FU Jenkins/NASA Fellowship; NASA [NNX09AQ44A] FX The authors acknowledge technical assistance and insightful discussions with Brett Cruden. Work by E. S.-R. was made possible through a Jenkins/NASA Fellowship. A NASA grant NNX09AQ44A to the University of California Santa Cruz is acknowledged for instruments in the UCSC MACS Facility within the UCSC/NASA-ARC ASL. W. P., D. O., J. P., D. M., B. W., S. T., and T-T. N-D. are student interns. M. W. now with University of Kentucky. T-T. N-D., J. G., and M. O. are employed by ELORET Corporation at NASA Ames. NR 42 TC 2 Z9 2 U1 7 U2 48 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0884-2914 EI 2044-5326 J9 J MATER RES JI J. Mater. Res. PD FEB 14 PY 2014 VL 29 IS 3 BP 417 EP 425 DI 10.1557/jmr.2013.293 PG 9 WC Materials Science, Multidisciplinary SC Materials Science GA AB7IJ UT WOS:000331962700012 ER PT J AU Miller, SAE AF Miller, Steven A. E. TI The prediction of jet noise ground effects using an acoustic analogy and a tailored Green's function SO JOURNAL OF SOUND AND VIBRATION LA English DT Article ID COMPUTATIONAL FLUID-DYNAMICS; AXISYMMETRIC SHEAR FLOWS; LOW-FREQUENCY SOUND; MULTIPOLE SOURCES; MEAN-FLOW; TURBULENCE; SHOCK AB An assessment of an acoustic analogy for the mixing noise component of jet noise in the presence of an infinite surface is presented. The reflection of jet noise by the ground changes the distribution of acoustic energy and is characterized by constructive and destructive interference patterns. The equivalent sources are modeled based on the two-point cross-correlation of the turbulent velocity fluctuations and a steady Reynolds-Averaged Navier-Stokes (RANS) solution. Propagation effects, due to reflection by the surface and refraction by the jet shear layer, are taken into account by calculating the vector Green's function of the linearized Euler equations (LEE). The vector Green's function of the LEE is written in relation to that of Lilley's equation; that is, it is approximated with matched asymptotic solutions and Green's function of the convective Helmholtz equation. The Green's function of the convective Helmholtz equation in the presence of an infinite flat plane with impedance is the Weyl-van der Pol equation. Predictions are compared with measurements from an unheated Mach 0.95 jet. Microphones are placed at various heights and distances from the nozzle exit in the peak jet noise direction above an acoustically hard and an asphalt surface. The predictions are shown to accurately capture jet noise ground effects that are characterized by constructive and destructive interference patterns in the mid- and far-field and capture overall trends in the near-field. Published by Elsevier Ltd. C1 Natl Aeronaut & Space Adm, Langley Res Ctr, Aeroacoust Branch, Hampton, VA 23681 USA. RP Miller, SAE (reprint author), Natl Aeronaut & Space Adm, Langley Res Ctr, Aeroacoust Branch, 2 N Dryden Sr MS 461, Hampton, VA 23681 USA. EM s.miller@nasa.gov NR 40 TC 3 Z9 3 U1 0 U2 13 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0022-460X EI 1095-8568 J9 J SOUND VIB JI J. Sound Vibr. PD FEB 14 PY 2014 VL 333 IS 4 BP 1193 EP 1207 DI 10.1016/j.jsv.2013.10.028 PG 15 WC Acoustics; Engineering, Mechanical; Mechanics SC Acoustics; Engineering; Mechanics GA 285GN UT WOS:000329381900007 ER PT J AU Morton, DC Nagol, J Carabajal, CC Rosette, J Palace, M Cook, BD Vermote, EF Harding, DJ North, PRJ AF Morton, Douglas C. Nagol, Jyoteshwar Carabajal, Claudia C. Rosette, Jacqueline Palace, Michael Cook, Bruce D. Vermote, Eric F. Harding, David J. North, Peter R. J. TI Amazon forests maintain consistent canopy structure and greenness during the dry season SO NATURE LA English DT Article ID RAIN-FOREST; TROPICAL FOREST; CARBON-DIOXIDE; DROUGHT; MODIS; ALLOMETRY; FLUXES; TREES; VARIABILITY; EMISSIONS AB The seasonality of sunlight and rainfall regulates net primary production in tropical forests(1). Previous studies have suggested that light is more limiting than water for tropical forest productivity(2), consistent with greening of Amazon forests during the dry season in satellite data(3-7). We evaluated four potential mechanisms for the seasonal green-up phenomenon, including increases in leaf area(5-7) or leaf reflectance(3,4,6), using a sophisticated radiative transfer model(8) and independent satellite observations from lidar and optical sensors. Here we show that the apparent green up of Amazon forests in optical remote sensing data resulted from seasonal changes in near-infrared reflectance, an artefact of variations in sun-sensor geometry. Correcting this bidirectional reflectance effect eliminated seasonal changes in surface reflectance, consistent with independent lidar observations and model simulations with unchanging canopy properties. The stability of Amazon forest structure and reflectance over seasonal timescales challenges the paradigm of light-limited net primary production in Amazon forests and enhanced forest growth during drought conditions. Correcting optical remote sensing data for artefacts of sun-sensor geometry is essential to isolate the response of global vegetation to seasonal and interannual climate variability. C1 [Morton, Douglas C.; Carabajal, Claudia C.; Rosette, Jacqueline; Cook, Bruce D.; Vermote, Eric F.; Harding, David J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nagol, Jyoteshwar; Rosette, Jacqueline] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Nagol, Jyoteshwar] Global Land Cover Facil, College Pk, MD 20740 USA. [Carabajal, Claudia C.] Sigma Space Corp, Lanham, MD 20706 USA. [Rosette, Jacqueline; North, Peter R. J.] Swansea Univ, Dept Geog, Swansea SA2 8PP, W Glam, Wales. [Palace, Michael] Univ New Hampshire, Earth Syst Res Ctr, Durham, NH 03824 USA. RP Morton, DC (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM douglas.morton@nasa.gov RI Morton, Douglas/D-5044-2012; North, Peter/A-1616-2009; Nagol, Jyoteshwar/P-2026-2015; Harding, David/F-5913-2012 OI North, Peter/0000-0001-9933-6935; Nagol, Jyoteshwar/0000-0003-0497-7874; FU NASA; NASA Postdoctoral Program; NERC National Centre for Earth Observation FX Funding for this research was provided by NASA, the NASA Postdoctoral Program and the NERC National Centre for Earth Observation. We thank G. P. Asner for providing Amazon leaf reflectance data. NR 49 TC 106 Z9 109 U1 17 U2 162 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 FEB 13 PY 2014 VL 506 IS 7487 BP 221 EP + DI 10.1038/nature13006 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AA5AK UT WOS:000331107700038 PM 24499816 ER PT J AU Ma, WP Jacobs, G Das, TK Masuku, CM Kang, JS Pendyala, VRR Davis, BH Klettlinger, JLS Yen, CH AF Ma, Wenping Jacobs, Gary Das, Tapan K. Masuku, Cornelius Mduduzi Kang, Jungshik Pendyala, Venkat Ramana Rao Davis, Burtron H. Klettlinger, Jennifer L. S. Yen, Chia H. TI Fischer-Tropsch Synthesis: Kinetics and Water Effect on Methane Formation over 25%Co/gamma-Al2O3 Catalyst SO INDUSTRIAL & ENGINEERING CHEMISTRY RESEARCH LA English DT Article ID SUPPORTED COBALT CATALYSTS; CO HYDROGENATION; PRODUCT DISTRIBUTIONS; CO/AL2O3 CATALYSTS; PARTIAL-PRESSURE; H2-CO MIXTURES; GROUP-8 METALS; TRANSIENT; HYDROCARBONS; MECHANISM AB The kinetics and the effect of indigenous and externally added water on methane formation during Fischer-Tropsch synthesis (FTS) was studied over Co based catalysts using a 1 L continuously stirred tank reactor (CSTR). The water cofeeding study (10% water) was conducted over a 0.27%Ru-25%Co/Al2O3 catalyst at a low CO conversion level of 19% at 220 degrees C in order to lessen the effect of catalyst aging during the addition of water, while the kinetic experiment was conducted over 25%Co/gamma-Al2O3 at the conditions of 205-230 degrees C, 1.4-2.5 MPa, H-2/CO = 1.0-2.5, and 3-16 (NL/g(cat))/h (X-CO < 60%). Indigenous and externally added water decreases methane formation by a kinetic effect. The addition of 10% water led to a decrease in the CH4 rate by 12% (3.5 -> 3.0 (mmol/g(cat))/h), while little catalyst deactivation was observed during water addition. Increases in indigenous water partial pressure also lowered the CH4 rate and its selectivity. Kinetic analysis was performed using a group of 220 degrees C data collected between 365 and 918 h when the deactivation rate was very low. An empirical CH4 kinetic model, with a water effect term (P-H2O/P-H2), (r(CH4) = kP(CO) P-a(H2)b/(1 + mP(H2O)/P-H2)) was used to fit kinetic data. The CH4 kinetic results suggest a negative water effect on CH4 formation during FTS on the unpromoted cobalt catalyst, consistent with the water effect results. The final methane kinetics (r(CH4)) equation obtained at 220 degrees C over 25%Co/gamma-Al2O3 is as follows: r(CH4)/[(mol/g(cat))/h] = 0.001053{(PCO-0.86PH21.32)/[1 + 0.46(P-H2O/P-H2)]}. Meanwhile, a methane selectivity model at 220 degrees C for the 25%CO/Al2O3 catalyst was also developed: S-CH4 = 0.0792P(CO)(-0.55)P(H2)(0.44)[1 - 0.24P(H2O)/P-H2)/(1 + 0.46P(H2O)/P-H2)]. The CH4 selectivity model provided a good prediction of CH4 selectivities under the experimental conditions used. Furthermore, our empirical CH4 kinetic results on the cobalt catalyst are consistent with literature kinetic models that were derived from carbide mechanisms; high CH4 selectivity from the cobalt catalyst is found to be mainly due to a high CH4 reaction rate constant. C1 [Ma, Wenping; Jacobs, Gary; Das, Tapan K.; Masuku, Cornelius Mduduzi; Kang, Jungshik; Pendyala, Venkat Ramana Rao; Davis, Burtron H.] Univ Kentucky, Ctr Appl Energy Res, Lexington, KY 40511 USA. [Klettlinger, Jennifer L. S.; Yen, Chia H.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Davis, BH (reprint author), Univ Kentucky, Ctr Appl Energy Res, 2540 Res Pk Dr, Lexington, KY 40511 USA. EM burtron.davis@uky.edu RI Jacobs, Gary/M-5349-2015 OI Jacobs, Gary/0000-0003-0691-6717 FU NASA [NNX07AB93A]; Commonwealth of Kentucky FX This work was supported by NASA Contract NNX07AB93A and the Commonwealth of Kentucky. NR 58 TC 13 Z9 13 U1 0 U2 27 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0888-5885 J9 IND ENG CHEM RES JI Ind. Eng. Chem. Res. PD FEB 12 PY 2014 VL 53 IS 6 BP 2157 EP 2166 DI 10.1021/ie402094b PG 10 WC Engineering, Chemical SC Engineering GA AA8KE UT WOS:000331343600009 ER PT J AU Ackermann, M Albert, A Anderson, B Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Bissaldi, E Bloom, ED Bonamente, E Bouvier, A Brandt, TJ Bregeon, J Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caragiulo, M Caraveo, PA Cecchi, C Charles, E Chekhtman, A Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J D'Ammando, F de Angelis, A Dermer, CD Digel, SW Silva, EDE Drell, PS Drlica-Wagner, A Essig, R Favuzzi, C Ferrara, EC Franckowiak, A Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Giglietto, N Giroletti, M Godfrey, G Gomez-Vargas, GA Grenier, IA Guiriec, S Gustafsson, M Hayashida, M Hays, E Hewitt, J Hughes, RE Jogler, T Kamae, T Knodlseder, J Kocevski, D Kuss, M Larsson, S Latronico, L Garde, ML Longo, F Loparco, F Lovellette, MN Lubrano, P Martinez, G Mayer, M Mazziotta, MN Michelson, PF Mitthumsiri, W Mizuno, T Moiseev, AA Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nemmen, R Nuss, E Ohsugi, T Orlando, E Ormes, JF Perkins, JS Piron, F Pivato, G Porter, TA Raino, S Rando, R Razzano, M Razzaque, S Reimer, A Reimer, O Ritz, S Sanchez-Conde, M Sehgal, N Sgro, C Siskind, EJ Spinelli, P Strigari, L Suson, DJ Tajima, H Takahashi, H Thayer, JB Tibaldo, L Tinivella, M Torres, DF Uchiyama, Y Usher, TL Vandenbroucke, J Vianello, G Vitale, V Werner, M Winer, BL Wood, KS Wood, M Zaharijas, G Zimmer, S AF Ackermann, M. Albert, A. Anderson, B. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Bissaldi, E. Bloom, E. D. Bonamente, E. Bouvier, A. Brandt, T. J. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caragiulo, M. Caraveo, P. A. Cecchi, C. Charles, E. Chekhtman, A. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. D'Ammando, F. de Angelis, A. Dermer, C. D. Digel, S. W. do Couto e Silva, E. Drell, P. S. Drlica-Wagner, A. Essig, R. Favuzzi, C. Ferrara, E. C. Franckowiak, A. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Giglietto, N. Giroletti, M. Godfrey, G. Gomez-Vargas, G. A. Grenier, I. A. Guiriec, S. Gustafsson, M. Hayashida, M. Hays, E. Hewitt, J. Hughes, R. E. Jogler, T. Kamae, T. Knoedlseder, J. Kocevski, D. Kuss, M. Larsson, S. Latronico, L. Garde, M. Llena Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Martinez, G. Mayer, M. Mazziotta, M. N. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nemmen, R. Nuss, E. Ohsugi, T. Orlando, E. Ormes, J. F. Perkins, J. S. Piron, F. Pivato, G. Porter, T. A. Raino, S. Rando, R. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Ritz, S. Sanchez-Conde, M. Sehgal, N. Sgro, C. Siskind, E. J. Spinelli, P. Strigari, L. Suson, D. J. Tajima, H. Takahashi, H. Thayer, J. B. Tibaldo, L. Tinivella, M. Torres, D. F. Uchiyama, Y. Usher, T. L. Vandenbroucke, J. Vianello, G. Vitale, V. Werner, M. Winer, B. L. Wood, K. S. Wood, M. Zaharijas, G. Zimmer, S. CA Fermi-LAT Collaboration TI Dark matter constraints from observations of 25 Milky Way satellite galaxies with the Fermi Large Area Telescope SO PHYSICAL REVIEW D LA English DT Article ID DWARF SPHEROIDAL GALAXIES; CONFIDENCE-INTERVALS; LUMINOSITY FUNCTION; GALACTIC HALO; LOCAL GROUP; SKY SURVEY; KINEMATICS; LAT; PROFILES; SUBSTRUCTURE AB The dwarf spheroidal satellite galaxies of the Milky Way are some of the most dark-matter-dominated objects known. Due to their proximity, high dark matter content, and lack of astrophysical backgrounds, dwarf spheroidal galaxies are widely considered to be among the most promising targets for the indirect detection of dark matter via gamma rays. Here we report on.-ray observations of 25 Milky Way dwarf spheroidal satellite galaxies based on 4 years of Fermi Large Area Telescope (LAT) data. None of the dwarf galaxies are significantly detected in. rays, and we present.-ray flux upper limits between 500 MeV and 500 GeV. We determine the dark matter content of 18 dwarf spheroidal galaxies from stellar kinematic data and combine LAT observations of 15 dwarf galaxies to constrain the dark matter annihilation cross section. We set some of the tightest constraints to date on the annihilation of dark matter particles with masses between 2 GeV and 10 TeV into prototypical standard model channels. We find these results to be robust against systematic uncertainties in the LAT instrument performance, diffuse.-ray background modeling, and assumed dark matter density profile. C1 [Ackermann, M.; Buehler, R.; Mayer, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Albert, A.; Bloom, E. D.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Franckowiak, A.; Funk, S.; Godfrey, G.; Jogler, T.; Kamae, T.; Kocevski, D.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Orlando, E.; Porter, T. A.; Reimer, A.; Reimer, O.; Sanchez-Conde, M.; Sehgal, N.; Strigari, L.; Tajima, H.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Albert, A.; Bloom, E. D.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Franckowiak, A.; Funk, S.; Godfrey, G.; Jogler, T.; Kamae, T.; Kocevski, D.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Orlando, E.; Porter, T. A.; Reimer, A.; Reimer, O.; Sanchez-Conde, M.; Sehgal, N.; Strigari, L.; Tajima, H.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Anderson, B.; Bechtol, K.; Conrad, J.; Larsson, S.; Garde, M. Llena; Martinez, G.; Zimmer, S.] Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden. [Anderson, B.; Conrad, J.; Larsson, S.; Garde, M. Llena; Zimmer, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Baldini, L.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Razzano, M.; Sgro, C.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Grenier, I. A.] Univ Paris Diderot, Serv Astrophys, Lab AIM, CEA Saclay,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Bissaldi, E.; Longo, F.; Zaharijas, G.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Pivato, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bissaldi, E.; Zaharijas, G.] Univ Trieste, I-34127 Trieste, Italy. [Bonamente, E.; Cecchi, C.; Lubrano, P.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Lubrano, P.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Bouvier, A.; Ritz, S.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Bouvier, A.; Ritz, S.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Brandt, T. J.; Ferrara, E. C.; Guiriec, S.; Hays, E.; Hewitt, J.; Nemmen, R.; Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Brigida, M.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Brigida, M.; Caragiulo, M.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Chekhtman, A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Ciprini, S.; Gasparrini, D.] ASI Sci Data Ctr, I-00044 Frascati, Roma, Italy. [Ciprini, S.; Gasparrini, D.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Monte Porzio Catone, Roma, Italy. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS, IN2P3, Montpellier, France. [D'Ammando, F.; Giroletti, M.] INAF Ist Radioastron, I-40129 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. [Dermer, C. D.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Space Sci Div, Washington, DC 20375 USA. [Drlica-Wagner, A.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA. [Essig, R.] SUNY Stony Brook, CN Yang Inst Theoret Phys, Stony Brook, NY 11794 USA. [Fukazawa, Y.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Gomez-Vargas, G. A.; Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Gomez-Vargas, G. A.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain. [Gomez-Vargas, G. A.] Univ Autonoma Madrid, Dept Fis Teor, CSIC, E-28049 Madrid, Spain. [Guiriec, S.] NASA, Postdoctoral Program, Washington, DC USA. [Gustafsson, M.] Univ Libre Bruxelles, Serv Phys Theor, B-1050 Brussels, Belgium. [Hayashida, M.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Knoedlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Moiseev, A. A.] CRESST, Greenbelt, MD 20771 USA. [Moiseev, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [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. [Razzaque, S.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa. [Reimer, A.; Reimer, O.; Werner, M.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.; Werner, M.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Torres, D. F.] CSIC, Inst Ciencies Espai IEEE, Barcelona 08193, Spain. [Torres, D. F.] ICREA, Barcelona, Spain. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. EM johann.cohen-tanugi@lupm.in2p3.fr; conrad@fysik.su.se; kadrlica@fnal.gov; maja.garde@fysik.su.se; mazziotta@ba.infn.it RI Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Reimer, Olaf/A-3117-2013; Funk, Stefan/B-7629-2015; Gomez-Vargas, German/C-7138-2015; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016; Bissaldi, Elisabetta/K-7911-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; OI Morselli, Aldo/0000-0002-7704-9553; Reimer, Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; Bissaldi, Elisabetta/0000-0001-9935-8106; Torres, Diego/0000-0002-1522-9065; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; Zaharijas, Gabrijela/0000-0001-8484-7791; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; Strigari, Louis/0000-0001-5672-6079; Bastieri, Denis/0000-0002-6954-8862; Giroletti, Marcello/0000-0002-8657-8852; Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726 FU Department of Energy Office of Science Graduate Fellowship Program (DOE SCGF) [DE-AC05-06OR23100]; Wenner-Gren Foundation; Italian Ministry of Education, University and Research (MIUR) [FIRB-2012-RBFR12PM1F]; National Aeronautics and Space Administration; Department of Energy in the U.S.; Commissariat a l'Energie Atomique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan; K. A. Wallenberg Foundation; Swedish Research Council; Swedish National Space Board in Sweden; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France FX The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the U.S., 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. Support was also provided by the Department of Energy Office of Science Graduate Fellowship Program (DOE SCGF) administered by ORISE-ORAU under Contract No. DE-AC05-06OR23100 and by the Wenner-Gren Foundation. J. C. is Wallenberg Academy Fellow, supported by the Knut & Alice Wallenberg foundation. M. R. received funds from Contract No. FIRB-2012-RBFR12PM1F from the Italian Ministry of Education, University and Research (MIUR). The authors would like to thank Joakim Edsjo, Torbjorn Sjostrand, and Peter Skands for helpful conversations concerning Pythia. The authors acknowledge the use of HEALPIX [97].12 NR 97 TC 227 Z9 229 U1 4 U2 21 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD FEB 11 PY 2014 VL 89 IS 4 AR 042001 DI 10.1103/PhysRevD.89.042001 PG 22 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AM1TE UT WOS:000339630400001 ER PT J AU Papastergiou, G Alexiadis, I Burleigh, S Tsaoussidis, V AF Papastergiou, Giorgos Alexiadis, Ioannis Burleigh, Scott Tsaoussidis, Vassilis TI Delay Tolerant Payload Conditioning protocol SO COMPUTER NETWORKS LA English DT Article DE Delay Tolerant Networking; Aggregation; End-to-end reliability; Transport protocol; In-order delivery; Duplicate suppression AB Delay Tolerant Networking (DTN) architecture is a new communication architecture developed to provide network connectivity in challenging environments. It forms a store-and-forward overlay network that employs persistent storage to deal with link disconnections. Consistent with its store-and-forward requirements, the design of the transport function of the DTN architecture was primarily based on hop-by-hop operations in preference to the traditional end-to-end communication model. As a result, pure end-to-end functionality is absent from the current DTN architecture and thus has been shifted towards applications. In this study, we highlight the benefits of having an additional layer of application-independent protocol offering transparent application data conditioning services end-to-end and we introduce Delay Tolerant Payload Conditioning (DTPC) protocol, a novel protocol that realizes this layer. DTPC protocol is an expandable, connectionless, reliable, sequenced transport protocol which extends the DTN architecture in a fashion that accords with the end-to-end principle, enabling the following services: (a) application data aggregation, (b) application-level reliability, (c) in-order delivery, and (d) duplicate suppression. DTPC was integrated into the JPL's Interplanetary Overlay Network (ION) DTN reference implementation, and its functionality was evaluated/validated through real-time experiments in a DTN testbed. (C) 2013 Elsevier B.V. All rights reserved. C1 [Papastergiou, Giorgos; Alexiadis, Ioannis; Tsaoussidis, Vassilis] Democritus Univ Thrace, Sch Engn, Dept Elect & Comp Engn, Space Internetworking Ctr, GR-67100 Xanthi, Greece. [Burleigh, Scott] CALTECH, Jet Prop Lab, La Canada Flintridge, CA 91011 USA. RP Papastergiou, G (reprint author), Democritus Univ Thrace, Dept Elect & Comp Engn, Bldg A,Off 1,Ground Floor, GR-67100 Xanthi, Greece. EM gpapaste@ee.duth.gr; ialex@ee.duth.gr; scott.c.burleigh@jpl.nasa.gov; vtsaousi@ee.duth.gr OI Burleigh, Scott/0000-0003-3768-5413 FU European Community [FP7/2007-2013_FP7-REGPOT-2010-1, 264226] FX The research leading to these results has received funding from the European Community's Seventh Framework Programme ([FP7/2007-2013_FP7-REGPOT-2010-1, SP4 Capacities, Coordination and Support Actions) under grant agreement no 264226 (project title: Space Internet-working Center-SPICE). This paper reflects only the authors' views and the Community is not liable for any use that may be made of the information contained therein. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 33 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1389-1286 EI 1872-7069 J9 COMPUT NETW JI Comput. Netw. PD FEB 11 PY 2014 VL 59 BP 244 EP 263 DI 10.1016/j.bjp.2013.11.003 PG 20 WC Computer Science, Hardware & Architecture; Computer Science, Information Systems; Engineering, Electrical & Electronic; Telecommunications SC Computer Science; Engineering; Telecommunications GA AB3BA UT WOS:000331665100017 ER PT J AU Che, H Goldstein, ML Vinas, AF AF Che, H. Goldstein, M. L. Vinas, A. F. TI Bidirectional Energy Cascades and the Origin of Kinetic Alfvenic and Whistler Turbulence in the Solar Wind SO PHYSICAL REVIEW LETTERS LA English DT Article ID DISSIPATION RANGE; SPECTRUM; DYNAMICS; CORONA; WAVES; AU AB The observed steep kinetic scale turbulence spectrum in the solar wind raises the question of how that turbulence originates. Observations of keV energetic electrons during solar quiet time suggest them as a possible source of free energy to drive kinetic turbulence. Using particle-in-cell simulations, we explore how the free energy released by an electron two-stream instability drives Weibel-like electromagnetic waves that excite wave-wave interactions. Consequently, both kinetic Alfvenic and whistler turbulence are excited that evolve through inverse and forward magnetic energy cascades. C1 [Che, H.; Goldstein, M. L.; Vinas, A. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Che, H (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. FU NASA Postdoctoral Program at NASA/GSFC administered by Oak Ridge Associated Universities [NNH11ZDA001N] FX This research was supported by the NASA Postdoctoral Program at NASA/GSFC administered by Oak Ridge Associated Universities through a contract with NASA and NASA Grant No. NNH11ZDA001N. The simulations and analysis were carried out at the NASA Advanced Supercomputing (NAS) facility at the NASA Ames Research Center, and on Kraken at the National Institute for Computation Sciences. The authors thank the anonymous referees whose comments have helped in making many improvements to this manuscript. H. C. is grateful for helpful discussions at the "7th Festival de Theorie" held in Aix-en-Provence, France. NR 23 TC 13 Z9 13 U1 0 U2 6 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD FEB 11 PY 2014 VL 112 IS 6 AR 061101 DI 10.1103/PhysRevLett.112.061101 PG 5 WC Physics, Multidisciplinary SC Physics GA AB7ED UT WOS:000331951200001 PM 24580684 ER PT J AU Aliu, E Archambault, S Arlen, T Aune, T Behera, B Beilicke, M Benbow, W Berger, K Bird, R Bouvier, A Buckley, JH Bugaev, V Byrum, K Cerruti, M Chen, X Ciupik, L Connolly, MP Cui, W Duke, C Dumm, J Errando, M Falcone, A Federici, S Feng, Q Finley, JP Fleischhack, H Fortin, P Fortson, L Furniss, A Galante, N Gillanders, GH Griffin, S Griffiths, ST Grube, J Gyuk, G Hanna, D Holder, J Hughes, G Humensky, TB Johnson, CA Kaaret, P Kertzman, M Khassen, Y Kieda, D Krawczynski, H Krennrich, F Lang, MJ Madhavan, AS Maier, G Majumdar, P McArthur, S McCann, A Meagher, K Millis, J Moriarty, P Mukherjee, R Nieto, D de Bhroithe, AO Ong, RA Otte, AN Park, N Perkins, JS Pohl, M Popkow, A Prokoph, H Quinn, J Ragan, K Reyes, LC Reynolds, PT Richards, GT Roache, E Sembroski, GH Smith, AW Staszak, D Telezhinsky, I Theiling, M Varlotta, A Vassiliev, VV Vincent, S Wakely, SP Weekes, TC Weinstein, A Welsing, R Williams, DA Zajczyk, A Zitzer, B AF Aliu, E. Archambault, S. Arlen, T. Aune, T. Behera, B. Beilicke, M. Benbow, W. Berger, K. Bird, R. Bouvier, A. Buckley, J. H. Bugaev, V. Byrum, K. Cerruti, M. Chen, X. Ciupik, L. Connolly, M. P. Cui, W. Duke, C. Dumm, J. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fleischhack, H. Fortin, P. Fortson, L. Furniss, A. Galante, N. Gillanders, G. H. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Hanna, D. Holder, J. Hughes, G. Humensky, T. B. Johnson, C. A. Kaaret, P. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Lang, M. J. Madhavan, A. S. Maier, G. Majumdar, P. McArthur, S. McCann, A. Meagher, K. Millis, J. Moriarty, P. Mukherjee, R. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Park, N. Perkins, J. S. Pohl, M. Popkow, A. Prokoph, H. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Sembroski, G. H. Smith, A. W. Staszak, D. Telezhinsky, I. Theiling, M. Varlotta, A. Vassiliev, V. V. Vincent, S. Wakely, S. P. Weekes, T. C. Weinstein, A. Welsing, R. Williams, D. A. Zajczyk, A. Zitzer, B. TI A THREE-YEAR MULTI-WAVELENGTH STUDY OF THE VERY-HIGH-ENERGY gamma-RAY BLAZAR 1ES 0229+200 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: general; BL Lacertae objects: individual (1ES 0229+200, VER J0232+202); diffuse radiation; galaxies: active; gamma rays: general; magnetic fields ID EXTRAGALACTIC BACKGROUND LIGHT; ACTIVE GALACTIC NUCLEI; BL LACERTAE OBJECTS; INTERGALACTIC MAGNETIC-FIELD; LARGE-AREA TELESCOPE; X-RAY; TEV BLAZARS; SPACE-TELESCOPE; DISTANT BLAZARS; LORENTZ FACTOR AB The high-frequency-peaked BL Lacertae object 1ES 0229+200 is a relatively distant (z = 0.1396), hard-spectrum (Gamma similar to 2.5), very-high-energy (VHE; E > 100 GeV) emitting gamma-ray blazar. VHE measurements of this active galactic nucleus have been used to place constraints on the intensity of the extragalactic background light and the intergalactic magnetic field (IGMF). A multi-wavelength study of this object centered around VHE observations by Very Energetic Radiation Imaging Telescope Array System (VERITAS) is presented. This study obtained, over a period of three years, an 11.7 standard deviation detection and an average integral flux F(E > 300 GeV) = (23.3 +/- 2.8(stat) +/- 5.8(sys)) x 10(-9) photons m(-2) s(-1), or 1.7% of the Crab Nebula's flux (assuming the Crab Nebula spectrum measured by H. E. S. S). Supporting observations from Swift and RXTE are analyzed. The Swift observations are combined with previously published Fermi observations and the VHE measurements to produce an overall spectral energy distributionwhich is then modeled assuming one-zone synchrotron-self-Compton emission. The chi(2) probability of the TeV flux being constant is 1.6%. This, when considered in combination with measured variability in the X-ray band, and the demonstrated variability of many TeV blazars, suggests that the use of blazars such as 1ES 0229+200 for IGMF studies may not be straightforward and challenges models that attribute hard TeV spectra to secondary gamma-ray production along the line of sight. C1 [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Staszak, D.] McGill Univ, Dept Phys, Montreal, PQ, Canada. [Arlen, T.; Aune, T.; Majumdar, P.; Ong, R. A.; Popkow, A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Behera, B.; Chen, X.; Federici, S.; Fleischhack, H.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Vincent, S.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Krawczynski, H.; Zajczyk, A.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Cerruti, M.; Fortin, P.; Galante, N.; Roache, E.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Berger, K.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Berger, K.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bird, R.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Bouvier, A.; Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Bouvier, A.; Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Byrum, K.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. [Chen, X.; Federici, S.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Dumm, J.; Fortson, L.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Humensky, T. B.; Nieto, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Krennrich, F.; Madhavan, A. S.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Majumdar, P.] Saha Inst Nucl Phys, Kolkata 700064, India. [McArthur, S.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Aliu, E (reprint author), Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. EM mcerruti@cfa.harvard.edu; jeremy.s.perkins@nasa.gov RI Khassen, Yerbol/I-3806-2015; Nieto, Daniel/J-7250-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Nieto, Daniel/0000-0003-3343-0755; Cui, Wei/0000-0002-6324-5772 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U.K; National Aeronautics and Space Administration FX VERITAS is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748) and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. 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 73 TC 14 Z9 14 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2014 VL 782 IS 1 AR 13 DI 10.1088/0004-637X/782/1/13 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB5SG UT WOS:000331848200013 ER PT J AU Blain, AW Assef, R Stern, D Tsai, CW Eisenhardt, P Bridge, C Benford, D Jarrett, T Cutri, R Petty, S Wu, JW Wright, EL AF Blain, Andrew W. Assef, Roberto Stern, Daniel Tsai, Chao-Wei Eisenhardt, Peter Bridge, Carrie Benford, Dominic Jarrett, Tom Cutri, Roc Petty, Sara Wu, Jingwen Wright, Edward L. TI WISE DETECTIONS OF KNOWN QSOs AT REDSHIFTS GREATER THAN SIX (vol 778, pg 113, 2013) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Blain, Andrew W.] Univ Leicester, Leicester LE1 7RH, Leics, England. [Assef, Roberto; Stern, Daniel; Tsai, Chao-Wei; Eisenhardt, Peter] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Assef, Roberto] Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile. [Bridge, Carrie] CALTECH, Pasadena, CA 91125 USA. [Benford, Dominic] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Jarrett, Tom] Univ Cape Town, Dept Astron, ZA-7700 Rondebosch, South Africa. [Cutri, Roc] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Petty, Sara] Virginia Tech, Dept Phys MC 0435, Blacksburg, VA 24061 USA. [Wu, Jingwen; Wright, Edward L.] Univ Calif Los Angeles, Div Astron & Astrophys, Los Angeles, CA 90095 USA. RP Blain, AW (reprint author), Univ Leicester, 1 Univ Rd, Leicester LE1 7RH, Leics, England. EM ab520@le.ac.uk RI Benford, Dominic/D-4760-2012 OI Benford, Dominic/0000-0002-9884-4206 NR 1 TC 1 Z9 1 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2014 VL 782 IS 1 AR 58 DI 10.1088/0004-637X/782/1/58 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB5SG UT WOS:000331848200058 ER PT J AU Corsi, A Ofek, EO Gal-Yam, A Frail, DA Kulkarni, SR Fox, DB Kasliwal, MM Sullivan, M Horesh, A Carpenter, J Maguire, K Arcavi, I Cenko, SB Cao, Y Mooley, K Pan, YC Sesar, B Sternberg, A Xu, D Bersier, D James, P Bloom, JS Nugent, PE AF Corsi, A. Ofek, E. O. Gal-Yam, A. Frail, D. A. Kulkarni, S. R. Fox, D. B. Kasliwal, M. M. Sullivan, M. Horesh, A. Carpenter, J. Maguire, K. Arcavi, I. Cenko, S. B. Cao, Y. Mooley, K. Pan, Y. -C. Sesar, B. Sternberg, A. Xu, D. Bersier, D. James, P. Bloom, J. S. Nugent, P. E. TI A MULTI-WAVELENGTH INVESTIGATION OF THE RADIO-LOUD SUPERNOVA PTF11qcj AND ITS CIRCUMSTELLAR ENVIRONMENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general; supernovae: individual (PTF11qcj) ID GAMMA-RAY BURST; DIGITAL SKY SURVEY; 25 APRIL 1998; X-RAY; IC SUPERNOVAE; IBC SUPERNOVA; LIGHT-CURVE; GRB 980425; SN 2009IP; SPACE-TELESCOPE AB We present the discovery, classification, and extensive panchromatic (from radio to X-ray) follow-up observations of PTF11qcj, a supernova (SN) discovered by the Palomar Transient Factory (PTF). Our observations with the Karl G. Jansky Very Large Array show that this event is radio-loud: PTF11qcj reached a radio peak luminosity comparable to that of the famous gamma-ray-burst-associated SN 1998bw (L-5 GHz approximate to 10(29) erg s(-1) Hz(-1)). PTF11qcj is also detected in X-rays with the Chandra Observatory, and in the infrared band with Spitzer. Our multi-wavelength analysis probes the SN interaction with circumstellar material. The radio observations suggest a progenitor mass-loss rate of similar to 10(-4) M-circle dot yr(-1) x (v(w)/1000 km s(-1)), and a velocity of approximate to 0.3-0.5 c for the fastest moving ejecta (at approximate to 10 days after explosion). However, these estimates are derived assuming the simplest model of SN ejecta interacting with a smooth circumstellar wind, and do not account for possible inhomogeneities in the medium and asphericity of the explosion. The radio data show deviations from such a simple model, as well as a late-time re-brightening. The X-ray flux from PTF11qcj is compatible with the high-frequency extrapolation of the radio synchrotron emission (within the large uncertainties). A light echo from pre-existing dust is in agreement with our infrared data. Our pre-explosion data from the PTF suggest that a precursor eruption of absolute magnitude M-r approximate to -13 mag may have occurred approximate to 2.5 yr prior to the SN explosion. Overall, PTF11qcj fits the expectations from the explosion of a Wolf-Rayet star. Precursor eruptions may be a feature characterizing the final pre-explosion evolution of such stars. C1 [Corsi, A.] George Washington Univ, Dept Phys, Washington, DC 20052 USA. [Corsi, A.] CALTECH, LIGO Lab, Pasadena, CA 91125 USA. [Ofek, E. O.; Gal-Yam, A.; Xu, D.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Frail, D. A.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Kulkarni, S. R.; Horesh, A.; Carpenter, J.; Arcavi, I.; Cao, Y.; Mooley, K.; Sesar, B.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Fox, D. B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Kasliwal, M. M.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Sullivan, M.; Maguire, K.; Pan, Y. -C.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Cenko, S. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cenko, S. B.; Bloom, J. S.; Nugent, P. E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Sternberg, A.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Xu, D.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Bersier, D.; James, P.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5UX, Merseyside, England. [Nugent, P. E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. RP Corsi, A (reprint author), George Washington Univ, Dept Phys, 725 21st St NW, Washington, DC 20052 USA. EM corsi@gwu.edu RI Horesh, Assaf/O-9873-2016; OI Horesh, Assaf/0000-0002-5936-1156; Sullivan, Mark/0000-0001-9053-4820; James, Philip/0000-0003-4131-5183 FU DOE Office of Science; UT/Austin; Pennsylvania State University; Stanford; Ludwig-Maximilians-Universitat Munchen; Georg-August-Universitat Gottingen; Instituto de Astronomia de la Universidad Nacional Autonoma de Mexico; W. M. Keck Foundation; UK Science and Technology Facilities Council; BSF; ISF; EU/FP7 via an ERC; GIF; Minerva; Kimmel Award; Israeli Ministry of Science; I-CORE Program of the Planning and Budgeting Committee; Israel Science Foundation [1829/12]; NSF-CDI [0941742]; Hubble Fellowship; Carnegie-Princeton Fellowship; Royal Society; Richard and Rhoda Goldman Fund; Christopher R. Redlich Fund; TABASGO Foundation; NSF [AST-1211916] FX PTF is a collaboration of Caltech, LCOGT, the Weizmann Institute, LBNL, Oxford, Columbia, IPAC, and Berkeley. Staff and computational resources were provided by NERSC, supported by the DOE Office of Science. HET/LRS are supported by UT/Austin, the Pennsylvania State University, Stanford, Ludwig-Maximilians-Universitat Munchen, Georg-August-Universitat Gottingen, and the Instituto de Astronomia de la Universidad Nacional Autonoma de Mexico. Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of California, Illinois, and Maryland, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. The K. Jansky Very Large Array is operated by NRAO, for the NSF under cooperative agreement by Associated Universities, Inc. The W. M. Keck Observatory, is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. The William Herschel Telescope is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. A.G. and S.R.K. acknowledge support from the BSF; A.G. further acknowledges support from the ISF, EU/FP7 via an ERC grant, GIF, Minerva, and a Kimmel Award; E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful to support by a grant from the Israeli Ministry of Science and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation (grant No 1829/12); J.S.B. acknowledges support of an NSF-CDI Grant 0941742, "Real-time Classification of Massive Time-series Data Streams"; M.M.K. acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship; M.S. acknowledges support from the Royal Society; S.B.C. acknowledges generous financial assistance from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. A.C. thanks the VLA staff for their support, and in particular: Miriam Krauss for very useful discussions on many aspects of the data reduction procedures; Heidi Medlin for support with the scheduling of the observations; and Drew Medlin for useful discussions on the VLA data reduction pipeline. A.C. also thanks E. Nakar for useful discussions. We thank the anonymous referee for useful comments. NR 90 TC 16 Z9 16 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 FEB 10 PY 2014 VL 782 IS 1 AR 42 DI 10.1088/0004-637X/782/1/42 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB5SG UT WOS:000331848200042 ER PT J AU Izidoro, A Haghighipour, N Winter, OC Tsuchida, M AF Izidoro, A. Haghighipour, N. Winter, O. C. Tsuchida, M. TI TERRESTRIAL PLANET FORMATION IN A PROTOPLANETARY DISK WITH A LOCAL MASS DEPLETION: A SUCCESSFUL SCENARIO FOR THE FORMATION OF MARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: numerical; planets and satellites: formation ID N-BODY SIMULATIONS; HIGH-RESOLUTION SIMULATIONS; LATE HEAVY BOMBARDMENT; EARTH-LIKE PLANETS; ASTEROID BELT; GIANT PLANETS; SOLAR-SYSTEM; OLIGARCHIC GROWTH; DYNAMICAL FRICTION; OUTWARD MIGRATION AB Models of terrestrial planet formation for our solar system have been successful in producing planets with masses and orbits similar to those of Venus and Earth. However, these models have generally failed to produce Mars-sized objects around 1.5 AU. The body that is usually formed around Mars' semimajor axis is, in general, much more massive than Mars. Only when Jupiter and Saturn are assumed to have initially very eccentric orbits (e similar to 0.1), which seems fairly unlikely for the solar system, or alternately, if the protoplanetary disk is truncated at 1.0 AU, simulations have been able to produce Mars-like bodies in the correct location. In this paper, we examine an alternative scenario for the formation of Mars in which a local depletion in the density of the protosolar nebula results in a non-uniform formation of planetary embryos and ultimately the formation ofMars-sized planets around 1.5 AU. We have carried out extensive numerical simulations of the formation of terrestrial planets in such a disk for different scales of the local density depletion, and for different orbital configurations of the giant planets. Our simulations point to the possibility of the formation of Mars-sized bodies around 1.5 AU, specifically when the scale of the disk local mass-depletion is moderately high (50%-75%) and Jupiter and Saturn are initially in their current orbits. In these systems, Mars-analogs are formed from the protoplanetary materials that originate in the regions of disk interior or exterior to the local mass-depletion. Results also indicate that Earth-sized planets can form around 1 AU with a substantial amount of water accreted via primitive water-rich planetesimals and planetary embryos. We present the results of our study and discuss their implications for the formation of terrestrial planets in our solar system. C1 [Izidoro, A.; Winter, O. C.] Univ Estadual Paulista, UNESP, Grp Dinamica Orbital & Planetol Guaratin, BR-12516410 Sao Paulo, Brazil. [Izidoro, A.] Capes Fdn, Minist Educ Brazil, BR-70040020 Brasilia, DF, Brazil. [Izidoro, A.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange, F-06304 Nice 4, France. [Haghighipour, N.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Haghighipour, N.] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA. [Haghighipour, N.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Tsuchida, M.] Univ Estadual Paulista, UNESP, DCCE IBILCE Sao Jos Rio Preto, BR-15054000 Sao Paulo, Brazil. RP Izidoro, A (reprint author), Univ Estadual Paulista, UNESP, Grp Dinamica Orbital & Planetol Guaratin, BR-12516410 Sao Paulo, Brazil. EM izidoro@feg.unesp.br; nader@ifa.hawaii.edu FU Brazilian National Research Council (CNPq); Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES); FAPESP - Sao Paulo State Funding Agency [proc. 2011/08171-3]; NASA Astrobiology Institute under the Institute for Astronomy, University of Hawaii [NNA09DA77A]; Alexander von Humboldt Foundation FX We thank the referee, Kevin Walsh, for his very constructive comments that greatly improved this manuscript. We are also grateful to Alessandro Morbidelli for his carefully reading of our paper and his helpful comments. A.I. and O.C.W. thank Rafael Sfair for his assistance with the computing cluster that was used to run part of these simulations. A.I. and O.C.W. acknowledge financial support from the Brazilian National Research Council (CNPq), Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES), and FAPESP - Sao Paulo State Funding Agency, proc. 2011/08171-3. A.I. thanks the Institute for Astronomy at the University of Hawaii for their kind hospitality during the course of this project. N.H. acknowledges support from the NASA Astrobiology Institute under Cooperative Agreement NNA09DA77A at the Institute for Astronomy, University of Hawaii, and the Alexander von Humboldt Foundation. N.H. is also grateful to the Computational Physics group at the Institute for Astronomy and Astrophysics, University of Tubingen for their kind hospitality during the course of this project. NR 71 TC 21 Z9 21 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2014 VL 782 IS 1 AR 31 DI 10.1088/0004-637X/782/1/31 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB5SG UT WOS:000331848200031 ER PT J AU Kitaguchi, T An, HJ Beloborodov, AM Gotthelf, EV Hayashi, T Kaspi, VM Rana, VR Boggs, SE Christensen, FE Craig, WW Hailey, CJ Harrison, FA Stern, D Zhang, WW AF Kitaguchi, Takao An, Hongjun Beloborodov, Andrei M. Gotthelf, Eric V. Hayashi, Takayuki Kaspi, Victoria M. Rana, Vikram R. Boggs, Steven E. Christensen, Finn E. Craig, William W. Hailey, Charles J. Harrison, Fiona A. Stern, Daniel Zhang, Will W. TI NuSTAR AND SWIFT OBSERVATIONS OF THE FAST ROTATING MAGNETIZED WHITE DWARF AE AQUARII SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; novae, cataclysmic variables; stars: individual (AE Aquarii); white dwarfs; X-rays: stars ID X-RAY PULSATIONS; CATACLYSMIC VARIABLES; INTERMEDIATE POLARS; LINE DIAGNOSTICS; ACCRETION FLOWS; HOT PLASMA; XMM-NEWTON; EMISSION; TELESCOPE; SPECTRA AB AE Aquarii is a cataclysmic variable with the fastest known rotating magnetized white dwarf (P-spin = 33.08 s). Compared to many intermediate polars, AE Aquarii shows a soft X-ray spectrum with a very low luminosity (L-X similar to 10(31) erg s(-1)). We have analyzed overlapping observations of this system with the NuSTAR and the Swift X-ray observatories in 2012 September. We find the 0.5-30 keV spectra to be well fitted by either an optically thin thermal plasma model with three temperatures of 0.75(-0.45)(+0.18), 2.29(-0.82)(+0.96), and 9.33(-2.18)(+6.07) keV, or an optically thin thermal plasma model with two temperatures of 1.00(-0.23)(+0.34) and 4.64(-0.84)(+1.58) keV plus a power-law component with photon index of 2.50(-0.23)(+0.17). The pulse profile in the 3-20 keV band is broad and approximately sinusoidal, with a pulsed fraction of 16.6% +/- 2.3%. We do not find any evidence for a previously reported sharp feature in the pulse profile. C1 [Kitaguchi, Takao] RIKEN Nishina Ctr, Wako, Saitama 3510198, Japan. [An, Hongjun; Kaspi, Victoria M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Beloborodov, Andrei M.; Gotthelf, Eric V.; Hailey, Charles J.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Beloborodov, Andrei M.; Gotthelf, Eric V.; Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Hayashi, Takayuki] Inst Space & Astronaut Sci JAXA, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Rana, Vikram R.; Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, Finn E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, Will W.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kitaguchi, T (reprint author), RIKEN Nishina Ctr, 2-1 Hirosawa, Wako, Saitama 3510198, Japan. RI Boggs, Steven/E-4170-2015 OI Rana, Vikram/0000-0003-1703-8796; Boggs, Steven/0000-0001-9567-4224 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; Japan Society for the Promotion of Science (JSPS) [24740185] 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 and the Swift Operations team 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 (Caltech, USA) and the XRT Data Analysis Software (XRTDAS) developed under the responsibility of ASDC. T. K. was supported by Japan Society for the Promotion of Science (JSPS) Grant-in-Aid for Young Scientists (B) (No. 24740185). NR 42 TC 3 Z9 3 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2014 VL 782 IS 1 AR 3 DI 10.1088/0004-637X/782/1/3 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB5SG UT WOS:000331848200003 ER PT J AU Mazumdar, A Monteiro, MJPFG Ballot, J Antia, HM Basu, S Houdek, G Mathur, S Cunha, MS Aguirre, VS Garcia, RA Salabert, D Verner, GA Christensen-Dalsgaard, J Metcalfe, TS Sanderfer, DT Seader, SE Smith, JC Chaplin, WJ AF Mazumdar, A. Monteiro, M. J. P. F. G. Ballot, J. Antia, H. M. Basu, S. Houdek, G. Mathur, S. Cunha, M. S. Aguirre, V. Silva Garcia, R. A. Salabert, D. Verner, G. A. Christensen-Dalsgaard, J. Metcalfe, T. S. Sanderfer, D. T. Seader, S. E. Smith, J. C. Chaplin, W. J. TI MEASUREMENT OF ACOUSTIC GLITCHES IN SOLAR-TYPE STARS FROM OSCILLATION FREQUENCIES OBSERVED BY KEPLER SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: interiors; stars: oscillations ID STELLAR EVOLUTION CODE; LOW-MASS STARS; CONVECTION ZONE; ASTEROSEISMIC ANALYSIS; LARGE SEPARATIONS; MODE FREQUENCIES; HELIUM ABUNDANCE; MAIN-SEQUENCE; PHASE-SHIFT; P-MODES AB For the very best and brightest asteroseismic solar-type targets observed by Kepler, the frequency precision is sufficient to determine the acoustic depths of the surface convective layer and the helium ionization zone. Such sharp features inside the acoustic cavity of the star, which we call acoustic glitches, create small oscillatory deviations from the uniform spacing of frequencies in a sequence of oscillation modes with the same spherical harmonic degree. We use these oscillatory signals to determine the acoustic locations of such features in 19 solar-type stars observed by the Kepler mission. Four independent groups of researchers utilized the oscillation frequencies themselves, the second differences of the frequencies and the ratio of the small and large separation to locate the base of the convection zone and the second helium ionization zone. Despite the significantly different methods of analysis, good agreement was found between the results of these four groups, barring a few cases. These results also agree reasonably well with the locations of these layers in representative models of the stars. These results firmly establish the presence of the oscillatory signals in the asteroseismic data and the viability of several techniques to determine the location of acoustic glitches inside stars. C1 [Mazumdar, A.] TIFR, Homi Bhabha Ctr Sci Educ, Bombay 400088, Maharashtra, India. [Monteiro, M. J. P. F. G.; Cunha, M. S.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Monteiro, M. J. P. F. G.] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4169007 Oporto, Portugal. [Ballot, J.] CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France. [Ballot, J.] Univ Toulouse, UPS OMP, IRAP, F-31400 Toulouse, France. [Antia, H. M.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. [Basu, S.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Houdek, G.; Aguirre, V. Silva; Christensen-Dalsgaard, J.; Metcalfe, T. S.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Houdek, G.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Mathur, S.] NCAR, High Altitude Observ, Boulder, CO 80307 USA. [Mathur, S.; Metcalfe, T. S.] Space Sci Inst, Boulder, CO 80301 USA. [Aguirre, V. Silva] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Garcia, R. A.] Univ Paris Diderot, IRFU SAp, Ctr Saclay, Lab AIM,CEA DSM,CNRS, F-91191 Gif Sur Yvette, France. [Salabert, D.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR7293, F-06304 Nice, France. [Verner, G. A.; Chaplin, W. J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Sanderfer, D. T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Seader, S. E.; Smith, J. C.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Mazumdar, A (reprint author), TIFR, Homi Bhabha Ctr Sci Educ, VN Purav Marg, Bombay 400088, Maharashtra, India. RI Monteiro, Mario J.P.F.G./B-4715-2008; OI Monteiro, Mario J.P.F.G./0000-0003-0513-8116; Cunha, Margarida/0000-0001-8237-7343; Antia, H. M./0000-0001-7549-9684; Metcalfe, Travis/0000-0003-4034-0416; Basu, Sarbani/0000-0002-6163-3472; Garcia, Rafael/0000-0002-8854-3776; Mazumdar, Anwesh/0000-0003-2409-2942 FU NASA's Science Mission Directorate; National Initiative on Undergraduate Science (NIUS) program of HBCSE (TIFR); NSF [AST-1105930]; Austrian Science Fund (FWF) [P21205-N16]; FCT/MCTES, Portugal [PTDC/CTE-AST/098754/2008]; POPH/FSE (EC); Excellence cluster "Origin and Structure of the Universe" (Garching); CNES; Danish National Research Foundation; ASTERISK project (ASTERoseismic Investigations with SONG and Kepler); European Research Council [267864]; National Science Foundation; NASA [NNX12AE17G]; European Commission under SPACEINN [FP7-SPACE-2012-312844] FX Funding for the Kepler Discovery mission is provided by NASA's Science Mission Directorate. A. M. acknowledges support from the National Initiative on Undergraduate Science (NIUS) program of HBCSE (TIFR). S. B. acknowledges support from NSF grant AST-1105930. G. H. acknowledges support from the Austrian Science Fund (FWF) project P21205-N16. M. C. and M.J.P.F.G.M. acknowledge financial support from FCT/MCTES, Portugal, through the project PTDC/CTE-AST/098754/2008. M. C. is partially funded by POPH/FSE (EC). V. S. A. received financial support from the Excellence cluster "Origin and Structure of the Universe" (Garching). D. S. acknowledges the financial support from CNES. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation. The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (grant agreement no.: 267864). N.C.A.R. is partially supported by the National Science Foundation. This work was partially supported by the NASA grant NNX12AE17G. This work has been supported, in part, by the European Commission under SPACEINN (grant agreement FP7-SPACE-2012-312844). J.B. acknowledges Othman Benomar for useful advice on MCMC methods. We thank Tim Bedding for suggesting improvements to the manuscript. We thank the anonymous referee for helping us to improve the paper. NR 73 TC 25 Z9 25 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2014 VL 782 IS 1 AR 18 DI 10.1088/0004-637X/782/1/18 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB5SG UT WOS:000331848200018 ER PT J AU Muller, TWA Haghighipour, N AF Mueller, Tobias W. A. Haghighipour, Nader TI CALCULATING THE HABITABLE ZONES OF MULTIPLE STAR SYSTEMS WITH A NEW INTERACTIVE WEB SITE SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; atmospheric effects; planetary systems ID MAIN-SEQUENCE STARS; PLANETARY ORBITS; SOLAR NEIGHBORHOOD; 3-BODY PROBLEM; BINARIES; STABILITY; EARTHS; 667C AB We have developed a comprehensive methodology and an interactive Web site for calculating the habitable zone (HZ) of multiple star systems. Using the concept of spectral weight factor, as introduced in our previous studies of the calculations of HZ in and around binary star systems, we calculate the contribution of each star (based on its spectral energy distribution) to the total flux received at the top of the atmosphere of an Earth-like planet, and use the models of the HZ of the Sun to determine the boundaries of the HZ in multiple star systems. Our interactive Web site for carrying out these calculations is publicly available at http://astro.twam.info/hz. We discuss the details of our methodology and present its application to some of the multiple star systems detected by the Kepler space telescope. We also present the instructions for using our interactive Web site, and demonstrate its capabilities by calculating the HZ for two interesting analytical solutions of the three-body problem. C1 [Mueller, Tobias W. A.; Haghighipour, Nader] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Haghighipour, Nader] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Haghighipour, Nader] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA. RP Muller, TWA (reprint author), Univ Tubingen, Inst Astron & Astrophys, Morgenstelle 10, D-72076 Tubingen, Germany. FU Carl-Zeiss-Stiftung; NASA ADAP [NNX13AF20G]; NASA Astrobiology Institute at the Institute for Astronomy, University of Hawaii [NNA09DA77]; HST [HST-GO-12548.06-A]; Alexander von Humboldt Foundation; NASA through the Space Telescope Science Institute [HST-GO-12548.06-A]; NASA [NAS5-26555] FX We thank the anonymous referee for constructive comments which have improved our manuscript. T.M. received financial support from the Carl-Zeiss-Stiftung. N.H. acknowledges support from the NASA ADAP grant NNX13AF20G, NASA Astrobiology Institute under Cooperative Agreement NNA09DA77 at the Institute for Astronomy, University of Hawaii, HST grant HST-GO-12548.06-A, and Alexander von Humboldt Foundation. Support for program HST-GO-12548.06-A 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. N.H. is also thankful to the Computational Physics group at the Institute for Astronomy and Astrophysics, University of Tubingen for their kind hospitality during the course of this project. NR 30 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2014 VL 782 IS 1 AR 26 DI 10.1088/0004-637X/782/1/26 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB5SG UT WOS:000331848200026 ER PT J AU Shao, M Nemati, B Zhai, CX Turyshev, SG Sandhu, J Hallinan, G Harding, LK AF Shao, Michael Nemati, Bijan Zhai, Chengxing Turyshev, Slava G. Sandhu, Jagmit Hallinan, Gregg Harding, Leon K. TI FINDING VERY SMALL NEAR-EARTH ASTEROIDS USING SYNTHETIC TRACKING SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; instrumentation: detectors; minor planets, asteroids: general; techniques: image processing ID KUIPER-BELT OBJECTS; TRANS-NEPTUNIAN OBJECTS; PENCIL-BEAM SURVEYS; SIZE DISTRIBUTION; MOVING TARGETS; SOLAR-SYSTEM; PAN-STARRS; TELESCOPE; ASTROMETRY AB We present an approach that significantly increases the sensitivity for finding and tracking small and fast near-Earth asteroids (NEAs). This approach relies on a combined use of a new generation of high-speed cameras which allow short, high frame-rate exposures of moving objects, effectively "freezing" their motion, and a computationally enhanced implementation of the "shift-and-add" data processing technique that helps to improve the signal-to-noise ratio (SNR) for detection of NEAs. The SNR of a single short exposure of a dim NEA is insufficient to detect it in one frame, but by computationally searching for an appropriate velocity vector, shifting successive frames relative to each other and then co-adding the shifted frames in post-processing, we synthetically create a long-exposure image as if the telescope were tracking the object. This approach, which we call "synthetic tracking," enhances the familiar shift-and-add technique with the ability to do a wide blind search, detect, and track dim and fast-moving NEAs in near real time. We discuss also how synthetic tracking improves the astrometry of fast-moving NEAs. We apply this technique to observations of two known asteroids conducted on the Palomar 200 inch telescope and demonstrate improved SNR and 10 fold improvement of astrometric precision over the traditional long-exposure approach. In the past 5 yr, about 150 NEAs with absolute magnitudes H = 28 (similar to 10 m in size) or fainter have been discovered. With an upgraded version of our camera and a field of view of (28 arcmin)(2) on the Palomar 200 inch telescope, synthetic tracking could allow detecting up to 180 such objects per night, including very small NEAs with sizes down to 7m. C1 [Shao, Michael; Nemati, Bijan; Zhai, Chengxing; Turyshev, Slava G.; Sandhu, Jagmit] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hallinan, Gregg; Harding, Leon K.] CALTECH, Pasadena, CA 91125 USA. RP Shao, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU National Aeronautics and Space Administration FX The authors wish to thank J. Giorgini of JPL for the simulation of what astrometric accuracy is needed to "not lose" an asteroid in a near-Earth orbit, and P. Chodas of JPL for supplying the estimates for the NEA population in the range of magnitudes H similar to 26-31. We thank V. E. Zharov of the Lomonosov Moscow State University, A. H. Parker of UCB, G. McKeegan of Chabot Observatory, and J. Scott Stuart of MIT for useful comments on the manuscript. We also thank the anonymous referee for a set of valuable comments that helped to improve the manuscript. The work described here was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 34 TC 9 Z9 9 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2014 VL 782 IS 1 AR 1 DI 10.1088/0004-637X/782/1/1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB5SG UT WOS:000331848200001 ER PT J AU Van Eylen, V Lund, MN Aguirre, VS Arentoft, T Kjeldsen, H Albrecht, S Chaplin, WJ Isaacson, H Pedersen, MG Jessen-Hansen, J Tingley, B Christensen-Dalsgaard, J Aerts, C Campante, TL Bryson, ST AF Van Eylen, V. Lund, M. N. Aguirre, V. Silva Arentoft, T. Kjeldsen, H. Albrecht, S. Chaplin, W. J. Isaacson, H. Pedersen, M. G. Jessen-Hansen, J. Tingley, B. Christensen-Dalsgaard, J. Aerts, C. Campante, T. L. Bryson, S. T. TI WHAT ASTEROSEISMOLOGY CAN DO FOR EXOPLANETS: KEPLER-410A b IS A SMALL NEPTUNE AROUND A BRIGHT STAR, IN AN ECCENTRIC ORBIT CONSISTENT WITH LOW OBLIQUITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: fundamental parameters; stars: individual (KOI-42, KIC 8866102, Kepler-410, Kepler-410A, HD 175289); stars: oscillations (including pulsations) ID SOLAR-TYPE STARS; TRANSIT TIMING OBSERVATIONS; SPITZER-SPACE-TELESCOPE; MAIN-SEQUENCE STARS; SUN-LIKE STAR; 1ST 4 MONTHS; SUPER-EARTH; STELLAR ROTATION; CCD PHOTOMETRY; LIGHT CURVES AB We confirm the Kepler planet candidate Kepler-410A b (KOI-42b) as a Neptune-sized exoplanet on a 17.8 day, eccentric orbit around the bright (K-p = 9.4) star Kepler-410A (KOI-42A). This is the third brightest confirmed planet host star in the Kepler field and one of the brightest hosts of all currently known transiting exoplanets. Kepler-410 consists of a blend between the fast rotating planet host star (Kepler-410A) and a fainter star (Kepler-410B), which has complicated the confirmation of the planetary candidate. Employing asteroseismology, using constraints from the transit light curve, adaptive optics and speckle images, and Spitzer transit observations, we demonstrate that the candidate can only be an exoplanet orbiting Kepler-410A. We determine via asteroseismology the following stellar and planetary parameters with high precision; M-star = 1.214 +/- 0.033M(circle dot), R-star = 1.352 +/- 0.010 R-circle dot, age = 2.76 +/- 0.54 Gyr, planetary radius (2.838 +/- 0.054 R-circle plus), and orbital eccentricity (0.17(-0.06)(+0.07)). In addition, rotational splitting of the pulsation modes allows for a measurement of Kepler-410A's inclination and rotation rate. Our measurement of an inclination of 82.5(-2.5)(+7.5) [degrees] indicates a low obliquity in this system. Transit timing variations indicate the presence of at least one additional (non-transiting) planet (Kepler-410A c) in the system. C1 [Van Eylen, V.; Lund, M. N.; Aguirre, V. Silva; Arentoft, T.; Kjeldsen, H.; Pedersen, M. G.; Jessen-Hansen, J.; Tingley, B.; Christensen-Dalsgaard, J.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Van Eylen, V.; Aerts, C.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium. [Lund, M. N.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Albrecht, S.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Albrecht, S.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Chaplin, W. J.; Campante, T. L.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Isaacson, H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94820 USA. [Bryson, S. T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Van Eylen, V (reprint author), Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. EM vincent@phys.au.dk RI Tingley, Brandon/E-5146-2014; OI Tingley, Brandon/0000-0003-4483-2661; Lund, Mikkel Norup/0000-0001-9214-5642 FU UK Science and Technology Facilities Council (STFC); Danish National Research Foundation [DNRF106]; ASTERISK project (ASTERoseismic Investigations with SONG and Kepler); European Research Council [267864]; NASA's Science Mission Directorate; NASA FX We thank Joanna Molenda-Zakowicz, Lars A. Buchhave and Christoffer Karoff for sharing stellar spectra. We thank Luca Casagrande for help with the InfraRed Flux Method to obtain the stellar distance and David Kipping for helpful comments in reviewing the manuscript. The referee's helpful comments and suggestions have led to significant improvements. M.N.L. thanks Dennis Stello and his colleagues at the Sydney Institute for Astronomy (SIfA) for their hospitality during a stay where some of the presented work was done. W.J.C. and T. L. C. acknowledge the support of the UK Science and Technology Facilities Council (STFC). Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (grant agreement No. DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (grant agreement No. 267864). Funding for the Kepler Discovery mission is provided by NASA's Science Mission Directorate. The Spitzer Space Telescope is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. We thank the entire Kepler team, without whom these results would not be possible. NR 90 TC 34 Z9 34 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2014 VL 782 IS 1 AR 14 DI 10.1088/0004-637X/782/1/14 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB5SG UT WOS:000331848200014 ER PT J AU Li, YF Reynolds, P O'Neill, P Cucinotta, FA AF Li, Yongfeng Reynolds, Pamela O'Neill, Peter Cucinotta, Francis A. TI Modeling Damage Complexity-Dependent Non-Homologous End-Joining Repair Pathway SO PLOS ONE LA English DT Article ID DOUBLE-STRAND BREAKS; KINASE CATALYTIC SUBUNIT; ULTRASOFT X-RAYS; DNA ENDS; PROTEIN-KINASE; IONIZING-RADIATION; GAMMA-H2AX FOCI; HUMAN-CELLS; MATHEMATICAL-MODEL; ATM AB Non-homologous end joining (NHEJ) is the dominant DNA double strand break (DSB) repair pathway and involves several repair proteins such as Ku, DNA-PKcs, and XRCC4. It has been experimentally shown that the choice of NHEJ proteins is determined by the complexity of DSB. In this paper, we built a mathematical model, based on published data, to study how NHEJ depends on the damage complexity. Under an appropriate set of parameters obtained by minimization technique, we can simulate the kinetics of foci track formation in fluorescently tagged mammalian cells, Ku80-EGFP and DNA-PKcs-YFP for simple and complex DSB repair, respectively, in good agreement with the published experimental data, supporting the notion that simple DSB undergo fast repair in a Ku-dependent, DNA-PKcs-independent manner, while complex DSB repair requires additional DNA-PKcs for end processing, resulting in its slow repair, additionally resulting in slower release rate of Ku and the joining rate of complex DNA ends. Based on the numerous experimental descriptions, we investigated several models to describe the kinetics for complex DSB repair. An important prediction of our model is that the rejoining of complex DSBs is through a process of synapsis formation, similar to a second order reaction between ends, rather than first order break filling/joining. The synapsis formation (SF) model allows for diffusion of ends before the synapsis formation, which is precluded in the first order model by the rapid coupling of ends. Therefore, the SF model also predicts the higher number of chromosomal aberrations observed with high linear energy transfer (LET) radiation due to the higher proportion of complex DSBs compared to low LET radiation, and an increased probability of misrejoin following diffusion before the synapsis is formed, while the first order model does not provide a mechanism for the increased effectiveness in chromosomal aberrations observed. C1 [Li, Yongfeng] Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA. [Reynolds, Pamela; O'Neill, Peter] Univ Oxford, Gray Inst Radiat Oncol & Biol, Dept Oncol, Oxford, England. [Cucinotta, Francis A.] Univ Nevada, Dept Hlth Phys & Diagnost Sci, Las Vegas, NV 89154 USA. [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Space Radiat Program, Houston, TX 77058 USA. RP Cucinotta, FA (reprint author), Univ Nevada, Dept Hlth Phys & Diagnost Sci, Las Vegas, NV 89154 USA. EM Francis.Cucinotta@unlv.edu FU DoE Low Dose Program; NASA Space Radiation Program FX The work was supported by DoE Low Dose Program and NASA Space Radiation Program. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 57 TC 8 Z9 8 U1 0 U2 3 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD FEB 10 PY 2014 VL 9 IS 2 AR e85816 DI 10.1371/journal.pone.0085816 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AA7CL UT WOS:000331254600008 PM 24520318 ER PT J AU Campbell, JF Lin, B Nehrir, AR AF Campbell, Joel F. Lin, Bing Nehrir, Amin R. TI Advanced sine wave modulation of continuous wave laser system for atmospheric CO2 differential absorption measurements SO APPLIED OPTICS LA English DT Article ID COLUMN MEASUREMENTS; LIDAR AB In this theoretical study, modulation techniques are developed to support the Active Sensing of CO2 Emissions over Nights, Days, and Seasons (ASCENDS) mission. A continuous wave (CW) lidar system using sine waves modulated by maximum length (ML) pseudo-noise (PN) codes is described for making simultaneous online/offline differential absorption measurements. Amplitude and phase-shift keying (PSK) modulated intensity modulation (IM) carriers, in addition to a hybrid-pulse technique are investigated, which exhibit optimal autocorrelation properties. A method is presented to bandwidth limit the ML sequence based on a filter implemented in terms of Jacobi theta functions, which does not significantly degrade the resolution or introduce sidelobes as a means of reducing aliasing and IM carrier bandwidth. C1 [Campbell, Joel F.; Lin, Bing; Nehrir, Amin R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Campbell, JF (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM joel.f.campbell@nasa.gov NR 27 TC 8 Z9 8 U1 0 U2 3 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 FEB 10 PY 2014 VL 53 IS 5 BP 816 EP 829 DI 10.1364/AO.53.000816 PG 14 WC Optics SC Optics GA AA8TQ UT WOS:000331368300004 PM 24663259 ER PT J AU Indebetouw, R Matsuura, M Dwek, E Zanardo, G Barlow, MJ Baes, M Bouchet, P Burrows, DN Chevalier, R Clayton, GC Fransson, C Gaensler, B Kirshner, R Lakicevic, M Long, KS Lundqvist, P Marti-Vidal, I Marcaide, J McCray, R Meixner, M Ng, CY Park, S Sonneborn, G Staveley-Smith, L Vlahakis, C van Loon, J AF Indebetouw, R. Matsuura, M. Dwek, E. Zanardo, G. Barlow, M. J. Baes, M. Bouchet, P. Burrows, D. N. Chevalier, R. Clayton, G. C. Fransson, C. Gaensler, B. Kirshner, R. Lakicevic, M. Long, K. S. Lundqvist, P. Marti-Vidal, I. Marcaide, J. McCray, R. Meixner, M. Ng, C. -Y. Park, S. Sonneborn, G. Staveley-Smith, L. Vlahakis, C. van Loon, J. TI DUST PRODUCTION AND PARTICLE ACCELERATION IN SUPERNOVA 1987A REVEALED WITH ALMA SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: ISM; ISM: supernova remnants; Magellanic Clouds; supernovae: individual (1987A) ID HUBBLE-SPACE-TELESCOPE; SN 1987A; EARLY UNIVERSE; OPTICAL-PROPERTIES; MASSIVE STARS; REVERSE SHOCK; EVOLUTION; REMNANT; EJECTA; EMISSION AB Supernova (SN) explosions are crucial engines driving the evolution of galaxies by shock heating gas, increasing the metallicity, creating dust, and accelerating energetic particles. In 2012 we used the Atacama Large Millimeter/Submillimeter Array to observe SN 1987A, one of the best-observed supernovae since the invention of the telescope. We present spatially resolved images at 450 mu m, 870 mu m, 1.4 mm, and 2.8 mm, an important transition wavelength range. Longer wavelength emission is dominated by synchrotron radiation from shock-accelerated particles, shorter wavelengths by emission from the largest mass of dust measured in a supernova remnant (>0.2 M-circle dot). For the first time we show unambiguously that this dust has formed in the inner ejecta (the cold remnants of the exploded star's core). The dust emission is concentrated at the center of the remnant, so the dust has not yet been affected by the shocks. If a significant fraction survives, and if SN 1987A is typical, supernovae are important cosmological dust producers. C1 [Indebetouw, R.; Chevalier, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Indebetouw, R.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Matsuura, M.; Barlow, M. J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Dwek, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zanardo, G.; Staveley-Smith, L.] Univ Western Australia, ICRAR, Crawley, WA 6009, Australia. [Baes, M.] Univ Ghent, Sterrenkundig Observat, B-9000 Ghent, Belgium. [Bouchet, P.] CEA Saclay, F-91191 Gif Sur Yvette, France. [Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Clayton, G. C.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Fransson, C.; Lundqvist, P.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Fransson, C.; Lundqvist, P.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Gaensler, B.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Kirshner, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lakicevic, M.; van Loon, J.] Keele Univ, Lennard Jones Labs, Keele ST5 5BG, Staffs, England. [Long, K. S.; Meixner, M.; Sonneborn, G.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Marti-Vidal, I.] Chalmers Univ, Dept Earth & Space Sci, Onsala Space Observ, SE-43992 Onsala, Sweden. [Marcaide, J.] Univ Valencia, E-46100 Burjassot, Spain. [McCray, R.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Meixner, M.] Johns Hopkins Univ, Dept Phys & Astron, Bloomberg Ctr 366, Baltimore, MD 21218 USA. [Ng, C. -Y.] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Park, S.] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA. [Vlahakis, C.] European So Observ, Joint ALMA Observ, Santiago 19, Chile. RP Indebetouw, R (reprint author), Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA. EM remy@virginia.edu RI Barlow, Michael/A-5638-2009; Ng, Chi Yung/A-7639-2013; Marti-Vidal, Ivan/A-8799-2017; Staveley-Smith, Lister/A-1683-2011; OI Barlow, Michael/0000-0002-3875-1171; Ng, Chi Yung/0000-0002-5847-2612; Marti-Vidal, Ivan/0000-0003-3708-9611; Staveley-Smith, Lister/0000-0002-8057-0294; Zanardo, Giovanna/0000-0003-2742-771X; Gaensler, Bryan/0000-0002-3382-9558; Baes, Maarten/0000-0002-3930-2757 FU NASA [NAG5-12595, NASA/ADAP NNX13AE36G] FX This Letter makes use of the following ALMA data: ADS/JAO. ALMA#2011.0.00273. S (PI: Indebetouw). ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. M. M. was supported by NASA NAG5-12595 and NASA/ADAP NNX13AE36G. NR 49 TC 59 Z9 60 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 10 PY 2014 VL 782 IS 1 AR L2 DI 10.1088/2041-8205/782/1/L2 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5OR UT WOS:000331149900002 ER PT J AU Milisavljevic, D Margutti, R Crabtree, KN Foster, JB Soderberg, AM Fesen, RA Parrent, JT Sanders, NE Drout, MR Kamble, A Chakraborti, S Pickering, TE Cenko, SB Silverman, JM Filippenko, AV Kirshner, RP Mazzali, P Maeda, K Marion, GHH Vinko, J Wheeler, JC AF Milisavljevic, Dan Margutti, Raffaella Crabtree, Kyle N. Foster, Jonathan B. Soderberg, Alicia M. Fesen, Robert A. Parrent, Jerod T. Sanders, Nathan E. Drout, Maria R. Kamble, Atish Chakraborti, Sayan Pickering, Timothy E. Cenko, S. Bradley Silverman, Jeffrey M. Filippenko, Alexei V. Kirshner, Robert P. Mazzali, Paolo Maeda, Keiichi Marion, G. H. Howie Vinko, Jozsef Wheeler, J. Craig TI INTERACTION BETWEEN THE BROAD-LINED TYPE Ic SUPERNOVA 2012ap AND CARRIERS OF DIFFUSE INTERSTELLAR BANDS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: lines and bands; ISM: molecules; molecular processes; supernovae: general; supernovae: individual (SN 2012ap) ID LUMINOUS BLUE VARIABLES; RAY TRANSIENT 080109; IA SUPERNOVA; CROSS-SECTIONS; IBC SUPERNOVA; MASS-LOSS; STARS; PHOTOIONIZATION; PHOTOABSORPTION; SPECTROSCOPY AB Diffuse interstellar bands (DIBs) are absorption features observed in optical and near-infrared spectra that are thought to be associated with carbon-rich polyatomic molecules in interstellar gas. However, because the central wavelengths of these bands do not correspond to electronic transitions of any known atomic or molecular species, their nature has remained uncertain since their discovery almost a century ago. Here we report on unusually strong DIBs in optical spectra of the broad-lined Type Ic supernova SN 2012ap that exhibit changes in equivalent width over short (less than or similar to 30 days) timescales. The 4428 angstrom and 6283 angstrom DIB features get weaker with time, whereas the 5780 angstrom feature shows a marginal increase. These nonuniform changes suggest that the supernova is interacting with a nearby source of DIBs and that the DIB carriers possess high ionization potentials, such as small cations or charged fullerenes. We conclude that moderate-resolution spectra of supernovae with DIB absorptions obtained within weeks of outburst could reveal unique information about the mass-loss environment of their progenitor systems and provide new constraints on the properties of DIB carriers. C1 [Milisavljevic, Dan; Margutti, Raffaella; Crabtree, Kyle N.; Soderberg, Alicia M.; Sanders, Nathan E.; Drout, Maria R.; Kamble, Atish; Chakraborti, Sayan; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Foster, Jonathan B.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Parrent, Jerod T.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Parrent, Jerod T.] Las Cumbres Observ Global Telescope Network, Goleta, CA USA. [Pickering, Timothy E.] Southern African Large Telescope, ZA-7935 Cape Town, South Africa. [Pickering, Timothy E.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Cenko, S. Bradley; Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Silverman, Jeffrey M.; Marion, G. H. Howie; Vinko, Jozsef; Wheeler, J. Craig] Univ Texas Austin, Austin, TX 78712 USA. [Mazzali, Paolo] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Mazzali, Paolo] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Mazzali, Paolo] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Maeda, Keiichi] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Maeda, Keiichi] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Univ WPI, Kashiwa, Chiba 2778583, Japan. [Vinko, Jozsef] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. RP Milisavljevic, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dmilisav@cfa.harvard.edu OI Crabtree, Kyle/0000-0001-5629-5192 FU W. M. Keck Foundation; David and Lucile Packard Foundation; NSF [AST-1302771, AST-1211196, AST-1109801, AST-1211916]; Richard and Rhoda Goldman Fund; Christopher R. Redlich Fund; TABASGO Foundation; CfA Postdoctoral Fellowship from the Smithsonian Astrophysical Observatory FX We thank an anonymous referee for a helpful, detailed, and critical reading of the Letter. T. Snow kindly provided comments on an early draft of the Letter. P. Massey provided insightful comments. G. Pignata, S. Valenti, D. Malesani, and G. Leloudas shared archival spectra that were examined. Many of the observations reported in this Letter were obtained with the Southern African Large Telescope. Additional data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. A. Miller, P. Nugent, and A. Morgan helped obtain the Keck observations. Some observations also came from the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. Support was provided by the David and Lucile Packard Foundation Fellowship for Science and Engineering awarded to A. M. S. J.M.S. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. T. E. P. thanks the National Research Foundation of South Africa. R. P. K. and J.C.W. are grateful for NSF grants AST-1211196 and AST-1109801, respectively. A. V. F. and S. B. C. acknowledge generous support from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. K.N.C. has been supported by a CfA Postdoctoral Fellowship from the Smithsonian Astrophysical Observatory. This Letter made extensive use of the SUSPECT database (http://www.nhn.ou.edu/similar to suspect/). NR 50 TC 9 Z9 9 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 10 PY 2014 VL 782 IS 1 AR L5 DI 10.1088/2041-8205/782/1/L5 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5OR UT WOS:000331149900005 ER PT J AU Mengshoel, OJ Galan, SF de Dios, A AF Mengshoel, Ole J. Galan, Severino F. de Dios, Antonio TI Adaptive generalized crowding for genetic algorithms SO INFORMATION SCIENCES LA English DT Article DE Genetic algorithms; Premature convergence; Generalized crowding; Scaling factor control ID OPTIMIZATION AB The genetic algorithm technique known as crowding preserves population diversity by pairing each offspring with a similar individual in the current population (pairing phase) and deciding which of the two will survive (replacement phase). The replacement phase of crowding is usually carried out through deterministic or probabilistic crowding, which have the limitations that they apply the same selective pressure regardless of the problem being solved and the stage of genetic algorithm search. The recently developed generalized crowding approach introduces a scaling factor in the replacement phase, thus generalizing and potentially overcoming the limitations of both deterministic and probabilistic crowding. A key problem not previously addressed, however, is how the scaling factor should be adapted during the search process in order to effectively obtain optimal or near-optimal solutions. The present work investigates this problem by developing and evaluating two methods for adapting, during search, the scaling factor. We call these two methods diversity-adaptive and self-adaptive generalized crowding respectively. Whereas the former method adapts the scaling factor according to the population's diversity, the latter method includes the scaling factor in the chromosome for self-adaptation. Our experiments with real function optimization, Bayesian network inference, and the Traveling Salesman Problem show that both diversity-adaptive and self-adaptive generalized crowding are consistent techniques that produce strong results, often outperforming traditional generalized crowding. (C) 2013 Elsevier Inc. All rights reserved. C1 [Mengshoel, Ole J.] Carnegie Mellon Univ, NASA Ames Res Pk, Moffett Field, CA 94035 USA. [Galan, Severino F.; de Dios, Antonio] UNED, Dept Artificial Intelligence, Madrid 28040, Spain. RP Galan, SF (reprint author), UNED, Dept Artificial Intelligence, Juan Rosal 16, Madrid 28040, Spain. EM ole.mengshoel@sv.cmu.edu; seve@dia.uned.es; adedios@dia.uned.es NR 44 TC 5 Z9 5 U1 0 U2 5 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0020-0255 EI 1872-6291 J9 INFORM SCIENCES JI Inf. Sci. PD FEB 10 PY 2014 VL 258 BP 140 EP 159 DI 10.1016/j.ins.2013.08.056 PG 20 WC Computer Science, Information Systems SC Computer Science GA 283QN UT WOS:000329262200008 ER PT J AU Bauschlicher, CW Ricca, A AF Bauschlicher, Charles W., Jr. Ricca, Alessandra TI The infrared spectra of C96H25 compared with that of C96H24 SO THEORETICAL CHEMISTRY ACCOUNTS LA English DT Article DE Astrochemistry; Molecular data; Infrared bands; Interstellar medium; DFT ID POLYCYCLIC AROMATIC-HYDROCARBONS; GAUSSIAN-BASIS SETS; ELECTRON CORRELATION; EMISSION; MOLECULES; APPROXIMATION; EXCHANGE; BANDS; FREQUENCIES; POSITION AB The addition of one H atom to C96H24 has been studied for the neutral, cation, and anion. Hydrogen atom binding at the solo site is the most favorable for all three charge states. The solo and duo sites are significantly more strongly bound than the endo positions. One extra hydrogen atom has very little effect on the infrared spectra. It is unlikely that species with one extra hydrogen could be identified from the astronomical emission spectra. C1 [Bauschlicher, Charles W., Jr.] NASA, Ames Res Ctr, Entry Syst & Technol Div Mail Stop 230 3, Moffett Field, CA 94035 USA. [Ricca, Alessandra] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. RP Bauschlicher, CW (reprint author), NASA, Ames Res Ctr, Entry Syst & Technol Div Mail Stop 230 3, Moffett Field, CA 94035 USA. EM Charles.W.Bauschlicher@nasa.gov; Alessandra.Ricca-1@nasa.gov FU NASA's Astrophysics Theory and Fundamental Physics (ATFP) [NNX09AD18G] FX AR thanks the NASA's Astrophysics Theory and Fundamental Physics (ATFP) (NNX09AD18G) program for its generous support of this work. NR 30 TC 1 Z9 1 U1 0 U2 1 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1432-881X EI 1432-2234 J9 THEOR CHEM ACC JI Theor. Chem. Acc. PD FEB 8 PY 2014 VL 133 IS 4 AR 1454 DI 10.1007/s00214-014-1454-0 PG 8 WC Chemistry, Physical SC Chemistry GA AA2ZA UT WOS:000330961500001 ER PT J AU Jin, B Lim, T Ju, S Latypov, MI Kim, HS Meyyappan, M Lee, JS AF Jin, Bo Lim, Taekyung Ju, Sanghyun Latypov, Marat I. Kim, Hyoung Seop Meyyappan, M. Lee, Jeong-Soo TI Ga-doped indium oxide nanowire phase change random access memory cells SO NANOTECHNOLOGY LA English DT Article DE phase change random access memory; Ga-doped In2O3 nanowire; crystalline; amorphous ID IN2O3 NANOWIRES; DRIVEN; NONVOLATILE; TECHNOLOGY; FILM AB Phase change random access memory (PCRAM) devices are usually constructed using tellurium based compounds, but efforts to seek other materials providing desirable memory characteristics have continued. We have fabricated PCRAM devices using Ga-doped In2O3 nanowires with three different Ga compositions (Ga/(In + Ga) atomic ratio: 2.1%, 11.5% and 13.0%), and investigated their phase switching properties. The nanowires (similar to 40 nm in diameter) can be repeatedly switched between crystalline and amorphous phases, and Ga concentration-dependent memory switching behavior in the nanowires was observed with ultra-fast set/reset rates of 80 ns/20 ns, which are faster than for other competitive phase change materials. The observations of fast set/reset rates and two distinct states with a difference in resistance of two to three orders of magnitude appear promising for nonvolatile information storage. Moreover, we found that increasing the Ga concentration can reduce the power consumption and resistance drift; however, too high a level of Ga doping may cause difficulty in achieving the phase transition. C1 [Jin, Bo; Lee, Jeong-Soo] Pohang Univ Sci & Technol, Div IT Convergence Engn, Pohang, South Korea. [Lim, Taekyung; Ju, Sanghyun] Kyonggi Univ, Dept Phys, Suwon 443760, Gyeonggi Do, South Korea. [Latypov, Marat I.; Kim, Hyoung Seop] Pohang Univ Sci & Technol, Dept Mat Sci & Engn, Pohang, South Korea. [Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Jin, B (reprint author), Pohang Univ Sci & Technol, Div IT Convergence Engn, Pohang, South Korea. EM ljs6951@postech.ac.kr RI Kim, Hyoung Seop/C-2166-2009; OI Kim, Hyoung Seop/0000-0002-3155-583X; Latypov, Marat/0000-0003-4416-0877 FU National Research Foundation (NRF) [2012R1A2A2A02010432]; Converging Research Center Program through the Ministry of Science, ICT and Future Planning, Korea [2013K000179]; Center for Advanced Soft Electronics under the Global Frontier Research Program of the Ministry of Education, Science and Technology, Korea [2011-0031638] FX This research was supported by the National Research Foundation (NRF; No. 2012R1A2A2A02010432); by the Converging Research Center Program through the Ministry of Science, ICT and Future Planning, Korea (2013K000179), and a grant (Code No. 2011-0031638) from the Center for Advanced Soft Electronics under the Global Frontier Research Program of the Ministry of Education, Science and Technology, Korea. NR 38 TC 3 Z9 3 U1 0 U2 44 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0957-4484 EI 1361-6528 J9 NANOTECHNOLOGY JI Nanotechnology PD FEB 7 PY 2014 VL 25 IS 5 AR 055205 DI 10.1088/0957-4484/25/5/055205 PG 7 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Science & Technology - Other Topics; Materials Science; Physics GA 296NI UT WOS:000330191400007 PM 24406901 ER PT J AU Moore, CW Obrist, D Steffen, A Staebler, RM Douglas, TA Richter, A Nghiem, SV AF Moore, Christopher W. Obrist, Daniel Steffen, Alexandra Staebler, Ralf M. Douglas, Thomas A. Richter, Andreas Nghiem, Son V. TI Convective forcing of mercury and ozone in the Arctic boundary layer induced by leads in sea ice SO NATURE LA English DT Article ID ATMOSPHERIC MERCURY; GASEOUS MERCURY; ELEMENTAL MERCURY; HEAT-TRANSFER; DEPLETION; OCEAN; TROPOSPHERE; CANADA; WATERS; WINTER AB The ongoing regime shift of Arctic sea ice from perennial to seasonal ice is associated with more dynamic patterns of opening and closing sea-ice leads (large transient channels of open water in the ice)(1-3), which may affect atmospheric and biogeochemical cycles in the Arctic(4). Mercury and ozone are rapidly removed from the atmospheric boundary layer during depletion events in the Arctic(5-7), caused by destruction of ozone along with oxidation of gaseous elemental mercury (Hg(0)) to oxidized mercury (Hg(II)) in the atmosphere and its subsequent deposition to snow and ice(5). Ozone depletion events can change the oxidative capacity of the air by affecting atmospheric hydroxyl radical chemistry(8), whereas atmospheric mercury depletion events can increase the deposition of mercury to the Arctic(6,9-11), some of which can enter ecosystems during snowmelt(12). Here we present near-surface measurements of atmospheric mercury and ozone from two Arctic field campaigns near Barrow, Alaska. We find that coastal depletion events are directly linked to sea-ice dynamics. A consolidated ice cover facilitates the depletion of Hg(0) and ozone, but these immediately recover to near-background concentrations in the upwind presence of open sea-ice leads. We attribute the rapid recoveries of Hg(0) and ozone to lead-initiated shallow convection in the stable Arctic boundary layer, which mixes Hg(0) and ozone from undepleted air masses aloft. This convective forcing provides additional Hg(0) to the surface layer at a time of active depletion chemistry, where it is subject to renewed oxidation. Future work will need to establish the degree to which large-scale changes in sea-ice dynamics across the Arctic alter ozone chemistry and mercury deposition in fragile Arctic ecosystems. C1 [Moore, Christopher W.; Obrist, Daniel] Desert Res Inst, Div Atmospher Sci, Reno, NV 89523 USA. [Steffen, Alexandra; Staebler, Ralf M.] Environm Canada, Air Qual Proc Res Sect, Toronto, ON M3H 5T4, Canada. [Douglas, Thomas A.] US Army Cold Reg Res & Engn Lab, Ft Wainwright, AK 99703 USA. [Richter, Andreas] Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany. [Nghiem, Son V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Moore, CW (reprint author), Desert Res Inst, Div Atmospher Sci, Reno, NV 89523 USA. EM chris.moore@dri.edu RI Moore, Christopher/E-8448-2012; OI Moore, Christopher/0000-0002-6042-5583; Richter, Andreas/0000-0003-3339-212X FU National Aeronautics and Space Administration (NASA); Desert Research Institute; Science and Technology Branch of Environment Canada; Canadian International Polar Year government programme; NASA CSP FX This research was supported in part by the National Aeronautics and Space Administration (NASA) Cryospheric Sciences Program (CSP) and by the Desert Research Institute. The Science and Technology Branch of Environment Canada helped fund Hg measurements in 2012 along with the Canadian International Polar Year government programme in 2009. The research at the Jet Propulsion Laboratory, California Institute of Technology, was supported by NASA CSP. We thank Umiaq for field logistic assistance, the Barrow whaling community for beneficial interactions, and the National Oceanic and Atmosphere Administration (NOAA), Global Monitoring Division for the Barrow Observatory data. We gratefully acknowledge the NOAA Air Resources Laboratory (ARL) for provision of the HYSPLIT transport and dispersion model and READY Website (http://www.ready.noaa.gov) used in this publication. We thank K. Pratt and R. Kreidberg for feedback on the manuscript, B. Hatchett and T. Malamakal for help with radiosonde and WRF data, D. Hall and J. Schmaltz for MODIS imagery support, and J. Deary for outstanding field technical support. NR 32 TC 27 Z9 28 U1 7 U2 73 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 FEB 6 PY 2014 VL 506 IS 7486 BP 81 EP + DI 10.1038/nature12924 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 303BA UT WOS:000330648100035 PM 24429521 ER PT J AU Mortin, J Howell, SEL Wang, LB Derksen, C Svensson, G Graversen, RG Schroder, TM AF Mortin, Jonas Howell, Stephen E. L. Wang, Libo Derksen, Chris Svensson, Gunilla Graversen, Rune G. Schroder, Thomas M. TI Extending the QuikSCAT record of seasonal melt-freeze transitions over Arctic sea ice using ASCAT SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Active microwave measurements; Satelliteborne scatterometry; Arctic sea ice and snow; Surface processes; Melt-freeze retrieval; Arctic climate ID SYNTHETIC-APERTURE-RADAR; INTERACTIVE MULTISENSOR SNOW; ERA-INTERIM REANALYSIS; C-BAND; BACKSCATTER SIGNATURES; SCATTEROMETER DATA; MAPPING SYSTEM; SURFACE; ONSET; VARIABILITY AB The seasonal melt-freeze transitions are important to continuously monitor over Arctic sea ice in order to better understand Arctic climate variability. The K-u-band scatterometer QuikSCAT (13.4 GHz), widely used to retrieve pan-Arctic seasonal transitions, discontinued its decadal long record in 2009. In this study, we show that the C-band scatterometer ASCAT (5.3 GHz), in orbit since 2006 and with an anticipated lifetime through 2021, can be used to extend the QuikSCAT record of seasonal melt-freeze transitions. This is done by (1) comparing backscatter measurements over multiyear and first-year ice, and by (2) retrieving seasonal transitions from resolution-enhanced ASCAT and QuikSCAT measurements and comparing the results with independent datasets. Despite operating in different frequencies, ASCAT and QuikSCAT respond similarly to surface transitions. However, QuikSCAT measurements respond slightly stronger to the early melt of first-year ice, making it less sensitive to sea-ice dynamics. To retrieve the transitions, we employed an improved edge-detector algorithm, which was iterated and constrained using sea-ice concentration data, efficiently alleviating unreasonable outliers. This gives melt-freeze transitions over all Arctic sea ice north of 60 degrees N at a 4.45 km resolution during 1999-2009 and 2009-2012 for QuikSCAT and ASCAT, respectively. Using the sensor overlap period, we show that the retrieved transitions retrieved from the different instruments are largely consistent across all regions in the Arctic sea-ice domain, indicating a robust consistency. (C) 2013 Elsevier Inc. All rights reserved. C1 [Mortin, Jonas; Svensson, Gunilla; Graversen, Rune G.] Stockholm Univ, Dept Meteorol, S-10691 Stockholm, Sweden. [Mortin, Jonas; Svensson, Gunilla; Graversen, Rune G.] Stockholm Univ, Bolin Ctr Climate Res, S-10691 Stockholm, Sweden. [Howell, Stephen E. L.; Wang, Libo; Derksen, Chris] Environm Canada, Div Climate Res, Toronto, ON, Canada. [Schroder, Thomas M.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Mortin, J (reprint author), Stockholm Univ, Dept Meteorol, Svante Arrhenius Vag 16C, S-10691 Stockholm, Sweden. EM mortin@misu.su.se RI Graversen, Rune/C-3956-2016 FU NASA FX The authors gratefully acknowledge the constructive remarks and valuable input by the three anonymous reviewers, as well as Ben Holt at Jet Propulsion Laboratory for fruitful discussion. Enhanced resolution QuikSCAT and ASCAT data were obtained from the NASA sponsored Scatterometer Climate Record Pathfinder at Brigham Young University (scp.byu.edu) through the courtesy of David G. Long. Furthermore, the authors thankfully acknowledge the following institutions for producing and providing essential data: National Snow and Ice Data Center (nsidc.org), NASA Cryosphere Science Research Portal (neptune.gsfc.nasa.gov/csb), U.S. National Ice Center (natice.noaa.gov), and European Centre for Medium-Range Weather Forecasts (ecmwf.int). NR 84 TC 10 Z9 11 U1 0 U2 16 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 FEB 5 PY 2014 VL 141 BP 214 EP 230 DI 10.1016/j.rse.2013.11.004 PG 17 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AB3AB UT WOS:000331662600018 ER PT J AU Mallick, K Jarvis, AJ Boegh, E Fisher, JB Drewry, DT Tu, KP Hook, SJ Hulley, G Ardo, J Beringer, J Arain, A Niyogi, D AF Mallick, Kaniska Jarvis, Andrew J. Boegh, Eva Fisher, Joshua B. Drewry, Darren T. Tu, Kevin P. Hook, Simon J. Hulley, Glynn Ardo, Jonas Beringer, Jason Arain, Altaf Niyogi, Dev TI A Surface Temperature Initiated Closure (STIC) for surface energy balance fluxes SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Surface energy balance; Penman-Monteith equation; Advection-aridity hypothesis; Boundary layer conductance; Surface conductance; MODIS; Land surface temperature; FLUXNET; Evapotranspiration ID CARBON-DIOXIDE EXCHANGE; PRIESTLEY-TAYLOR COEFFICIENT; PENMAN-MONTEITH EQUATION; SOIL-MOISTURE; HEAT-FLUX; WATER-VAPOR; EVAPOTRANSPIRATION RATES; RAINFALL INTERCEPTION; STOMATAL CONDUCTANCE; REGIONAL EVAPORATION AB The use of Penman-Monteith (PM) equation in thermal remote sensing based surface energy balance modeling is not prevalent due to the unavailability of any direct method to integrate thermal data into the PM equation and due to the lack of physical models expressing the surface (or stomatal) and boundary layer conductances (g(S) and g(B)) as a function of surface temperature. Here we demonstrate a new method that physically integrates the radiometric surface temperature (T-S) into the PM equation for estimating the terrestrial surface energy balance fluxes (sensible heat, H and latent heat, lambda E). The method combines satellite T-S data with standard energy balance closure models in order to derive a hybrid closure that does not require the specification of surface to atmosphere conductance terms. We call this the Surface Temperature Initiated Closure (STIC), which is formed by the simultaneous solution of four state equations. Taking advantage of the psychrometric relationship between temperature and vapor pressure, the present method also estimates the near surface moisture availability (M) from T-S, air temperature (T-A) and relative humidity (R-H), thereby being capable of decomposing lambda E into evaporation (lambda E-E) and transpiration (lambda E-T). STIC is driven with T-S, T-A, R-H, net radiation (R-N), and ground heat flux (G). T-S measurements from both MODIS Terra (MOD11A2) and Aqua (MYD11A2) were used in conjunction with FLUXNET R-N, G, T-A, R-H, lambda E and H measurements corresponding to the MODIS equatorial crossing time. The performance of STIC has been evaluated in comparison to the eddy covariance measurements of lambda E and H at 30 sites that cover a broad range of biomes and climates. We found a RMSE of 37.79 (11%) (with MODIS Terra T-S) and 44.27 W m(-2) (15%) (with MODIS Aqua T-S) in lambda E estimates, while the RMSE was 37.74(9%) (with Terra) and 44.72 W m(-2) (8%) (with Aqua) in H. STIC could efficiently capture the lambda E dynamics during the dry down period in the semi-arid landscapes where lambda E is strongly governed by the subsurface soil moisture and where the majority of other lambda E models generally show poor results. Sensitivity analysis revealed a high sensitivity of both the fluxes to the uncertainties in T-S. A realistic response and modest relationship was also found when partitioned lambda E components (lambda E-E and lambda E-T) were compared to the observed soil moisture and rainfall. This is the first study to report the physical integration of T-S into the PM equation and finding analytical solution of the physical (g(B)) and physiological conductances (g(S)). The performance of STIC over diverse biomes and climates points to its potential to benefit future NASA and NOAA missions having thermal sensors, such as HyspIRI, GeoSTAR and GOES-R for mapping multi-scale lambda E and drought. (C) 2013 Elsevier Inc. All rights reserved. C1 [Mallick, Kaniska; Fisher, Joshua B.; Drewry, Darren T.; Hook, Simon J.; Hulley, Glynn] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Jarvis, Andrew J.] Univ Lancaster, Lancaster Environm Ctr, Lancaster LA1 4YQ, England. [Boegh, Eva] Roskilde Univ, Dept Environm Social & Spatial Change, Roskilde, Denmark. [Tu, Kevin P.] Pioneer HiBred Int Inc, Woodland, CA USA. [Ardo, Jonas] Lund Univ, Dept Phys Geog & Ecosyst Sci, S-22100 Lund, Sweden. [Beringer, Jason] Monash Univ, Sch Geog & Environm Sci, Clayton, Vic 3800, Australia. [Arain, Altaf] McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON L8S 4L8, Canada. [Niyogi, Dev] Purdue Univ, Dept Agron & Earth Atmospher Planetary Sci, W Lafayette, IN 47907 USA. RP Mallick, K (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM kaniska.mallick@gmail.com RI Hook, Simon/D-5920-2016; Beringer, Jason/B-8528-2008; OI Hook, Simon/0000-0002-0953-6165; Beringer, Jason/0000-0002-4619-8361; Ardo, Jonas/0000-0002-9318-0973; Arain, M. Altaf/0000-0002-1433-5173; Fisher, Joshua/0000-0003-4734-9085 FU Jet Propulsion Laboratory, California Institute of Technology under the National Aeronautics and Space Administration; NERC [NEE0191531]; JPL Research and Technology Development Grant [01STCR-R.11.118.004]; Earth System Data Record (ESDR) grant [104772-547714.04.16.01.06]; NSF CAREER; NSF INTEROP; USDA NIFA/U2U FX K.M. acknowledges the postdoctoral fellowship from Jet Propulsion Laboratory, California Institute of Technology under the contract of National Aeronautics and Space Administration. K.M. and A.J. was earlier supported by NERC grant (NEE0191531) during the initial development of the work. The research was initiated at Lancaster University and completed at the Jet Propulsion Laboratory. J.B.F. was supported by JPL Research and Technology Development Grant (01STCR-R.11.118.004) and Earth System Data Record (ESDR) grant (104772-547714.04.16.01.06). We gratefully acknowledge entire FLUXNET site PIs for sharing the eddy covariance data and ORNL for maintaining the harmonized MODIS data. KM also acknowledges Dr. Junhak Lee for helping in GIS. The scientific discussions with Dr. Jozsef Szilagyi, University of Nebraska and Dr. Wilfred Brutsaert, Cornel University are also acknowledged. D.N. acknowledges partial support from NSF CAREER, NSF INTEROP, and USDA NIFA/U2U. All the copyrights of 2013 are reserved. K.M., A.J., and E.B. formulated idea, designed research and performed research; everyone contributed to writing the manuscript The authors declare no conflict of interest. NR 107 TC 17 Z9 17 U1 2 U2 60 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 FEB 5 PY 2014 VL 141 BP 243 EP 261 DI 10.1016/j.rse.2013.10.022 PG 19 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AB3AB UT WOS:000331662600020 ER PT J AU Fortenberry, RC Huang, XC Schwenke, DW Lee, TJ AF Fortenberry, Ryan C. Huang, Xinchuan Schwenke, David W. Lee, Timothy J. TI Limited rotational and rovibrational line lists computed with highly accurate quartic force fields and ab initio dipole surfaces SO SPECTROCHIMICA ACTA PART A-MOLECULAR AND BIOMOLECULAR SPECTROSCOPY LA English DT Article DE Rotational spectroscopy; Vibrational spectroscopy; Dipole surfaces; Coupled cluster theory; Moller-Plesset perturbation theory ID POTENTIAL-ENERGY SURFACE; CORRELATED MOLECULAR CALCULATIONS; COUPLED-CLUSTER THEORY; GAUSSIAN-BASIS SETS; VIBRATIONAL FREQUENCIES; SPECTROSCOPIC CONSTANTS; ELECTRON CORRELATION; APPROXIMATION; DIOXIDE; SYSTEMS AB In this work, computational procedures are employed to compute the rotational and rovibrational spectra and line lists for H2O, CO2, and SO2. Building on the established use of quartic force fields, MP2 and CCSD(T) Dipole Moment Surfaces (DMSs) are computed for each system of study in order to produce line intensities as well as the transition energies. The computed results exhibit a clear correlation to reference data available in the HITRAN database. Additionally, even though CCSD(T) DMSs produce more accurate intensities as compared to experiment, the use of MP2 DMSs results in reliable line lists that are still comparable to experiment. The use of the less computationally costly MP2 method is beneficial in the study of larger systems where use of CCSD(T) would be more costly. (C) 2013 Elsevier B.V. All rights reserved. C1 [Fortenberry, Ryan C.; Schwenke, David W.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA. RP Lee, TJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Timothy.J.Lee@nasa.gov RI Lee, Timothy/K-2838-2012; schwenke, david/I-3564-2013; HUANG, XINCHUAN/A-3266-2013 FU NASA Postdoctoral Program; NASA/SETI Institute [NNX09Al49A, NNX12AG96A]; NASA's Laboratory Astrophysics 'Carbon in the Galaxy' Consortium Grant [NNH10ZDA001N]; NASA [10-APRA10-0096] FX The NASA Postdoctoral Program administered through Oak Ridge Associated Universities is acknowledged for funding RCF. XH acknowledges financial support by NASA/SETI Institute Cooperative Agreements NNX09Al49A and NNX12AG96A. Support from NASA's Laboratory Astrophysics 'Carbon in the Galaxy' Consortium Grant (NNH10ZDA001N) is gratefully acknowledged. The authors also gratefully acknowledge support from NASA Grant 10-APRA10-0096. NR 57 TC 9 Z9 9 U1 0 U2 20 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1386-1425 J9 SPECTROCHIM ACTA A JI Spectroc. Acta Pt. A-Molec. Biomolec. Spectr. PD FEB 5 PY 2014 VL 119 BP 76 EP 83 DI 10.1016/j.saa.2013.03.092 PG 8 WC Spectroscopy SC Spectroscopy GA 277HN UT WOS:000328809700011 PM 23692860 ER PT J AU Verma, VB Horansky, R Marsili, F Stern, JA Shaw, MD Lita, AE Mirin, RP Nam, SW AF Verma, V. B. Horansky, R. Marsili, F. Stern, J. A. Shaw, M. D. Lita, A. E. Mirin, R. P. Nam, S. W. TI A four-pixel single-photon pulse-position array fabricated from WSi superconducting nanowire single-photon detectors SO APPLIED PHYSICS LETTERS LA English DT Article ID READOUT CIRCUIT; EFFICIENCY; TIME AB We demonstrate a scalable readout scheme for an infrared single-photon pulse-position camera consisting of WSi superconducting nanowire single-photon detectors. For an N x N array, only 2 x N wires are required to obtain the position of a detection event. As a proof-of-principle, we show results from a 2 x 2 array. (C) 2014 AIP Publishing LLC. C1 [Verma, V. B.; Horansky, R.; Lita, A. E.; Mirin, R. P.; Nam, S. W.] Natl Inst Stand & Technol, Boulder, CO 80305 USA. [Marsili, F.; Stern, J. A.; Shaw, M. D.] Jet Prop Lab, Pasadena, CA 91109 USA. RP Verma, VB (reprint author), Natl Inst Stand & Technol, 325 Broadway, Boulder, CO 80305 USA. EM verma@nist.gov OI Mirin, Richard/0000-0002-4472-4655 FU DARPA InPho program FX This work was supported by the DARPA InPho program. NR 22 TC 14 Z9 15 U1 2 U2 22 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD FEB 3 PY 2014 VL 104 IS 5 AR 051115 DI 10.1063/1.4864075 PG 4 WC Physics, Applied SC Physics GA AB2TD UT WOS:000331644100015 ER PT J AU Arumugam, DD Griffin, JD Stancil, DD Ricketts, DS AF Arumugam, Darmindra D. Griffin, Joshua D. Stancil, Daniel D. Ricketts, David S. TI Three-Dimensional Position and Orientation Measurements Using Magneto-Quasistatic Fields and Complex Image Theory SO IEEE ANTENNAS AND PROPAGATION MAGAZINE LA English DT Article DE Electromagnetic fields; magneto-quasistatics; radio position measurement; radio tracking ID TRACKING AB Traditional wireless position-location systems, operating using propagating waves, suffer reduced performance in non-line-of-sight (NLoS) applications. Traditional systems that use quasistatic fields have instead been limited to short ranges, progressive direction-finding applications, require RF fingerprinting, or do not provide complete immunity to dielectric obstacles (use of electric fields). These limitations impose severe restrictions in applications such as tracking an American football during game play, where position and orientation tracking may be required over long ranges, and when the line-of-sight (LoS) is blocked by groups of people. A technique using magneto-quasistatic fields and complex image theory was recently shown to circumvent these problems, and to enable accurate long-range one-dimensional and two-dimensional measurements. In this work, we present three-dimensional position and orientation measurements using the magneto- quasistatic system and complex image theory over an area of 27.43 m x 27.43 m. Inverting the theoretical expression for the voltage measured at the terminals of the receiving loops to determine three- dimensional position and orientation resulted in mean and median geometric position errors of 0.77 m and 0.71 m, respectively; inclination orientation mean and median errors of 9.67 degrees and 8.24 degrees, respectively; and azimuthal orientation mean and median errors of 2.84 degrees and 2.25 degrees, respectively. C1 [Arumugam, Darmindra D.] Carnegie Mellon Univ, Dept Elect & Comp Engn, Pittsburgh, PA 15213 USA. [Griffin, Joshua D.; Stancil, Daniel D.] Disney Res Pittsburgh, Pittsburgh, PA 15213 USA. [Stancil, Daniel D.; Ricketts, David S.] N Carolina State Univ, Dept Elect & Comp Engn, Raleigh, NC 27695 USA. RP Arumugam, DD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM darmindra.d.arumugam@jpl.nasa.gov; joshdgriffin@disneyresearch.com; ddstancil@ncsu.edu; david.ricketts@ncsu.edu FU Research and Technology Development fund at the Jet Propulsion Laboratory, California Institute of Technology; National Aeronautics and Space Administration FX The work described in this paper was supported in part using a Research and Technology Development fund at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 18 TC 10 Z9 10 U1 2 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1045-9243 EI 1558-4143 J9 IEEE ANTENN PROPAG M JI IEEE Antennas Propag. Mag. PD FEB PY 2014 VL 56 IS 1 BP 160 EP 173 PG 14 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA AP9KH UT WOS:000342398200011 ER PT J AU Takada, M Ellis, RS Chiba, M Greene, JE Aihara, H Arimoto, N Bundy, K Cohen, J Dore, O Graves, G Gunn, JE Heckman, T Hirata, CM Ho, P Kneib, JP Le Fevre, O Lin, L More, S Murayama, H Nagao, T Ouchi, M Seiffert, M Silverman, JD Sodre, L Spergel, DN Strauss, MA Sugai, H Suto, Y Takami, H Wyse, R AF Takada, Masahiro Ellis, Richard S. Chiba, Masashi Greene, Jenny E. Aihara, Hiroaki Arimoto, Nobuo Bundy, Kevin Cohen, Judith Dore, Olivier Graves, Genevieve Gunn, James E. Heckman, Timothy Hirata, Christopher M. Ho, Paul Kneib, Jean-Paul Le Fevre, Olivier Lin, Lihwai More, Surhud Murayama, Hitoshi Nagao, Tohru Ouchi, Masami Seiffert, Michael Silverman, John D. Sodre, Laerte, Jr. Spergel, David N. Strauss, Michael A. Sugai, Hajime Suto, Yasushi Takami, Hideki Wyse, Rosemary TI Extragalactic science, cosmology, and Galactic archaeology with the Subaru Prime Focus Spectrograph SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Review DE cosmology: dark energy; cosmology: large-scale structure of Universe; galaxies: formation; galaxies: kinematics and dynamics; instrumentation: spectographs ID GALAXY REDSHIFT SURVEY; LYMAN BREAK GALAXIES; DIGITAL SKY SURVEY; BARYON ACOUSTIC-OSCILLATIONS; LY-ALPHA EMITTERS; STAR-FORMATION HISTORIES; MULTIELEMENT ABUNDANCE MEASUREMENTS; LUMINOUS RED GALAXIES; PROBING DARK ENERGY; SPECTROSCOPIC SURVEY AB The Subaru Prime Focus Spectrograph (PFS) is a massively multiplexed fiber-fed optical and near-infrared three-arm spectrograph (N-fiber = 2400, 380 <= lambda <= 1260 nm, 1 degrees.3 diameter field of view). Here, we summarize the science cases in terms of provisional plans for a 300-night Subaru survey. We describe plans to constrain the nature of dark energy via a survey of emission line galaxies spanning a comoving volume of 9.3 h(-3) Gpc(3) in the redshift range 0.8 < z < 2.4. In each of six redshift bins, the cosmological distances will be measured to 3% precision via the baryonic acoustic oscillation scale, and redshift-space distortion measures will constrain structure growth to 6% precision. In the near-field cosmology program, radial velocities and chemical abundances of stars in the Milky Way and M 31 will be used to infer the past assembly histories of spiral galaxies and the structure of their dark matter halos. Data will be secured for 10(6) stars in the Galactic thick-disk, halo, and tidal streams as faint as V similar to 22, including stars with V < 20 to complement the goals of the Gaia mission. A medium-resolution mode with R = 5000 to be implemented in the red arm will allow the measurement of multiple alpha-element abundances and more precise velocities for Galactic stars. For the galaxy evolution program, our simulations suggest the wide wavelength range of PFS will be powerful in probing the galaxy population and its clustering over a wide redshift range. We plan to conduct a color-selected survey of 1 < z < 2 galaxies and AGN over 16 deg(2) to J similar or equal to 23.4, yielding a fair sample of galaxies with stellar masses above similar to 10(10) M-circle dot at z similar or equal to 2. A two-tiered survey of higher redshift Lyman break galaxies and Lyman alpha emitters will quantify the properties of early systems close to the reionization epoch. C1 [Takada, Masahiro; Aihara, Hiroaki; Bundy, Kevin; More, Surhud; Murayama, Hitoshi; Silverman, John D.; Spergel, David N.; Sugai, Hajime] Univ Tokyo, Kavli Inst Phys & Math Universe, Kavli IPMU, WPI, Kashiwa, Chiba 2778583, Japan. [Ellis, Richard S.; Cohen, Judith; Dore, Olivier; Hirata, Christopher M.] CALTECH, Pasadena, CA 91125 USA. [Chiba, Masashi] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Greene, Jenny E.; Graves, Genevieve; Gunn, James E.; Spergel, David N.; Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Aihara, Hiroaki; Suto, Yasushi] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Arimoto, Nobuo; Takami, Hideki] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Dore, Olivier; Seiffert, Michael] CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA. [Heckman, Timothy; Wyse, Rosemary] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Ho, Paul; Lin, Lihwai] Natl Taiwan Univ, Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Kneib, Jean-Paul; Le Fevre, Olivier] Lab Astrophys Marseille, Pole Etoile Site Chateau Gombert, F-13388 Marseille 13, France. [Murayama, Hitoshi] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Murayama, Hitoshi] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Nagao, Tohru] Kyoto Univ, Hakubi Ctr Adv Res, Sakyo Ku, Kyoto 6068501, Japan. [Ouchi, Masami] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Sodre, Laerte, Jr.] Inst Astron Geofis & Ciencias Atmosfer Sao Paulo, BR-05508090 Sao Paulo, Brazil. RP Takada, M (reprint author), Univ Tokyo, Kavli Inst Phys & Math Universe, Kavli IPMU, WPI, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778583, Japan. EM masahiro.takada@ipmu.jp RI More, Surhud/A-5049-2013; Aihara, Hiroaki/F-3854-2010; Kneib, Jean-Paul/A-7919-2015; Sodre, Laerte/P-6045-2016; OI More, Surhud/0000-0002-2986-2371; Aihara, Hiroaki/0000-0002-1907-5964; Kneib, Jean-Paul/0000-0002-4616-4989; Sodre, Laerte/0000-0002-3876-268X; Raccanelli, Alvise/0000-0001-6726-0438 FU JSPS Core-to-Core Program "International Research Network for Dark Energy,"; World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan; FIRST program "Subaru Measurements of Images and Redshifts (SuMIRe)," CSTP, Japan FX This work is supported in part by the JSPS Core-to-Core Program "International Research Network for Dark Energy," by the World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and by the FIRST program "Subaru Measurements of Images and Redshifts (SuMIRe)," CSTP, Japan. NR 121 TC 60 Z9 60 U1 1 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD FEB PY 2014 VL 66 IS 1 AR R1 DI 10.1093/pasj/pst019 PG 51 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL8YX UT WOS:000339426900019 ER PT J AU Katz, A Wissink, AM AF Katz, Aaron Wissink, Andrew M. TI Efficient Solution Methods for Strand Grid Applications SO AIAA JOURNAL LA English DT Article ID ARTIFICIAL DIFFUSION; NUMERICAL SCHEMES; GAS-DYNAMICS; ACCURACY; DESIGN AB The strand-Cartesian grid approach offers many advantages in terms of automation, efficiency, and accuracy for complex moving-body problems, such as rotorcraft. In this study, the solution procedures for strand grids are investigated by testing a variety of explicit, implicit, and hybrid methods on canonical aerodynamics test cases involving inviscid and viscous flows in three dimensions. A novel multigrid algorithm is formulated that acts at both the nonlinear pseudotime level and the linear level using line Gauss-Seidel sweeps. Various approximations are tested for the Jacobian, and the impacts on memory and convergence are quantified. The major result is that implicit schemes with first-order approximate Jacobians employing few Gauss-Seidel sweeps are most efficient for strand grids. The improvement by using the multigrid algorithm is significant for all cases tested and indicates O(n) convergence. C1 [Katz, Aaron] Utah State Univ, Logan, UT 84322 USA. [Wissink, Andrew M.] NASA, Ames Res Ctr, US Army Aeroflightdynam Directorate, Moffett Field, CA 94035 USA. RP Katz, A (reprint author), Utah State Univ, Logan, UT 84322 USA. RI Katz, Aaron/I-8244-2015 OI Katz, Aaron/0000-0003-2739-9384 FU Army Research Office Fluid Dynamics Program; U.S. Department of Defense High Performance Computing Modernization Office; U.S. Department of Defense HPC Modernization Program Office FX Development was performed with the support of the Army Research Office Fluid Dynamics Program directed by Frederick Ferguson as well as the HPC Institute for Advanced Rotorcraft Modeling and Simulation located at the U.S. Army Aeroflightdynamics Directorate at Moffett Field, CA, which is supported by the U.S. Department of Defense High Performance Computing Modernization Office. Material presented in this paper is a product of the CREATE-AV Element of the Computational Research and Engineering for Acquisition Tools and Environments Program sponsored by the U.S. Department of Defense HPC Modernization Program Office. NR 21 TC 0 Z9 0 U1 0 U2 1 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD FEB PY 2014 VL 52 IS 2 BP 267 EP 280 DI 10.2514/1.J052303 PG 14 WC Engineering, Aerospace SC Engineering GA AJ6KZ UT WOS:000337804700004 ER PT J AU Shupe, J Potter, C AF Shupe, John Potter, Christopher TI MODELING DISCHARGE RATES USING A COUPLED MODELED APPROACH FOR THE MERCED RIVER IN YOSEMITE NATIONAL PARK SO JOURNAL OF THE AMERICAN WATER RESOURCES ASSOCIATION LA English DT Article DE Merced River; Yosemite National Park; surface water hydrology; simulation; water discharge rates; snowmelt; flooding; drought ID WESTERN UNITED-STATES; CLIMATE-CHANGE; SNOWMELT RUNOFF; SIERRA-NEVADA; CALIFORNIA; SCALE; TEMPERATURE; UNCERTAINTY; SCENARIOS AB This study describes the application of the NASA version of the Carnegie-Ames-Stanford Approach (CASA) ecosystem model coupled with a surface hydrologic routing scheme previously called the Hydrological Routing Algorithm (HYDRA) to model monthly discharge rates from 2000 to 2007 on the Merced River drainage in Yosemite National Park, California. To assess CASA-HYDRA's capability to estimate actual water flows in extreme precipitation years, the focus of this study is the 2007 water year, which was very dry, and the 2005 water year, which was a moderately wet year in the historical record. Prior to comparisons to gauge records, CASA-HYDRA snowmelt algorithms were modified with equations from the U. S. Department of Agriculture Snowmelt-Runoff Model (SRM), which has been designed to predict daily streamflow in mountain basins where snowmelt is a major runoff factor. Results show that model predictions closely matched monthly flow rates at the Pohono Bridge gauge station (USGS#11266500), with R-2 = 0.67 and Nash-Sutcliffe (E) = 0.65. By subdividing the upper Merced River basin into subbasins with high spatial resolution in the gridded modeling approach, we were able to determine which biophysical characteristics in the Sierra differed to the largest degree in extreme low-flow and high-flow years. Average elevation and snowpack accumulation were found to be the most important explanatory variables to understand subbasin contributions to monthly discharge rates. C1 [Shupe, John] Calif State Univ, Div Sci & Environm Policy, Seaside, CA 93955 USA. [Potter, Christopher] NASA, Biospher Sci Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Shupe, J (reprint author), Calif State Univ, Div Sci & Environm Policy, Seaside, CA 93955 USA. EM chris.potter@nasa.gov FU Planetary Skin Institute FX This research was supported by a grant from the Planetary Skin Institute. We would also like to thank Dr. Robert Rice, research scientist at University of California at Merced, for providing degree-day factor data for the Sierra Nevada. NR 36 TC 0 Z9 0 U1 4 U2 9 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1093-474X EI 1752-1688 J9 J AM WATER RESOUR AS JI J. Am. Water Resour. Assoc. PD FEB PY 2014 VL 50 IS 1 BP 153 EP 162 DI 10.1111/jawr.12124 PG 10 WC Engineering, Environmental; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA AJ4IQ UT WOS:000337639100012 ER PT J AU Ploutz-Snyder, LL Downs, M Ryder, J Hackney, K Scott, J Buxton, R Goetchius, E Crowell, B AF Ploutz-Snyder, Lori L. Downs, Meghan Ryder, Jeffrey Hackney, Kyle Scott, Jessica Buxton, Roxanne Goetchius, Elizabeth Crowell, Brent TI Integrated Resistance and Aerobic Exercise Protects Fitness during Bed Rest SO MEDICINE AND SCIENCE IN SPORTS AND EXERCISE LA English DT Article DE SPACEFLIGHT; COUNTERMEASURES; DECONDITIONING; TRAINING; REHABILITATION ID HUMAN SKELETAL-MUSCLE; PROLONGED SPACE-FLIGHT; ANAEROBIC THRESHOLD; NUTRITION COUNTERMEASURES; KNEE EXTENSOR; CAPACITY; SIZE; SPACEFLIGHT; RESPONSES; STRENGTH AB Introduction: The current exercise countermeasures have not fully protected astronauts' preflight aerobic and muscular fitness levels during International Space Station (ISS) missions, prompting a need to optimize the exercise prescription to improve or maintain astronauts' ability to perform critical tasks and eventually extend the duration of missions. Purpose: To test the hypothesis that an integrated resistance and aerobic exercise prescription performed with exercise equipment similar to that on the ISS can be tolerated and maintain cardiovascular and muscular fitness during 14 d of exposure to a model of microgravity. Methods: Subjects (n = 9) participated in 14-21 d of pre-bed rest training and familiarization, 14 d of bed rest + iRAT exercise, and 7 d of ambulatory recovery. Peak aerobic capacity ((V) over dotO(2peak)), ventilatory threshold (VT), and isokinetic and leg press tests were performed before and after bed rest to evaluate cardiovascular and muscle functions. Muscle cross-sectional area (CSA) was determined before, during, and after bed rest using magnetic resonance imaging (MRI). Results: Improvements from before to after bed rest were observed in (V) over dotO(2peak) (2.8 perpendicular to 0.2 to 3.2 perpendicular to 0.2 L.min(-1)), VT (1.9 +/- 0.2 to 2.1 +/- 0.2 L.min(-1)), leg muscle power (1582 +/- 317 to 1740 +/- 359 W), and muscle CSA of the grouped vastus lateralis, vastus intermedius, and vastus medialis muscles (67.5 +/- 8.4 to 68.9 +/- 8.3 cm(2)). Muscle strength and total CSA of the upper and lower legs were not different from before to after bed rest. Conclusions: This is the first report of exercise being completely effective for the prevention of cardiovascular and skeletal muscle deconditioning during strict bed rest using exercise equipment similar to that on the ISS. This was accomplished with high subject compliance. C1 [Ploutz-Snyder, Lori L.; Ryder, Jeffrey; Scott, Jessica] Univ Space Res Assoc, Houston, TX USA. [Downs, Meghan; Buxton, Roxanne; Goetchius, Elizabeth] Univ Houston, Houston, TX USA. [Hackney, Kyle; Crowell, Brent] Wyle Sci Technol & Engn Grp, Houston, TX USA. RP Ploutz-Snyder, LL (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy,B261,SK3, Houston, TX 77058 USA. EM Lori.Ploutz-Snyder-1@nasa.gov FU NASA's Human Research Program FX The authors thank the research participants who provided considerable feedback on implementation logistics as well as Drs. Richard Simpson and William Paloski from the University of Houston for development of the MATLAB program to identify ventilatory threshold. The authors would also like to thank the entire staff of the Exercise Physiology and Countermeasures Lab and the Flight Analogs Project at Johnson Space Center for the implementation of the study. This work was funded by NASA's Human Research Program. NR 40 TC 10 Z9 11 U1 0 U2 8 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA TWO COMMERCE SQ, 2001 MARKET ST, PHILADELPHIA, PA 19103 USA SN 0195-9131 EI 1530-0315 J9 MED SCI SPORT EXER JI Med. Sci. Sports Exerc. PD FEB PY 2014 VL 46 IS 2 BP 358 EP 368 DI 10.1249/MSS.0b013e3182a62f85 PG 11 WC Sport Sciences SC Sport Sciences GA AJ4ZB UT WOS:000337688000019 PM 24441215 ER PT J AU Ness, JU Parmar, AN Valencic, LA Smith, R Loiseau, N Salama, A Ehle, M Schartel, N AF Ness, J. -U. Parmar, A. N. Valencic, L. A. Smith, R. Loiseau, N. Salama, A. Ehle, M. Schartel, N. TI XMM-Newton publication statistics SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE publications, bibliography; space vehicles; telescopes ID PHOTON IMAGING CAMERA; CATALOG AB We assessed the scientific productivity of XMM-Newton by examining XMM-Newton publications and data usage statistics. We analyse 3272 refereed papers, published until the end of 2012, that directly use XMM-Newton data. The SAO/NASA Astrophysics Data System (ADS) was used to provide additional information on each paper including the number of citations. For each paper, the XMM-Newton observation identifiers and instruments used to provide the scientific results were determined. The identifiers were used to access the XMM-Newton Science Archive (XSA) to provide detailed information on the observations themselves and on the original proposals. The information obtained from these sources was then combined to allow the scientific productivity of the mission to be assessed. Since around three years after the launch of XMM-Newton there have been around 300 refereed papers per year that directly use XMM-Newton data. After more than 13 years in operation, this rate shows no evidence that it is decreasing. Since 2002, around 100 scientists per year become lead authors for the first time on a refereed paper which directly uses XMM-Newton data. Each refereed XMM-Newton paper receives around four citations per year in the first few years with a long-term citation rate of three citations per year, more than five years after publication. About half of the articles citing XMM-Newton articles are not primarily X-ray observational papers. The distribution of elapsed time between observations taken under the Guest Observer programme and first article peaks at 2 years with a possible second peak at 3.25 years. Observations taken under the Target of Opportunity programme are published significantly faster, after one year on average. The fraction of science time taken until the end of 2009 that has been used in at least one article is similar to 90%. Most observations were used more than once, yielding on average a factor of two in usage on available observing time per year. About 20% of all slew observations have been used in publications. The scientific productivity of XMM-Newton measured by the publication rate, number of new authors and citation rate, remains extremely high with no evidence that it is decreasing after more than 13 years of operations. (C) 2014 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Ness, J. -U.; Loiseau, N.; Salama, A.; Ehle, M.] ESAC, Sci Operat Dept ESA, XMM Newton Sci Operat Ctr, Villanueva De La Canada 28691, Madrid, Spain. [Parmar, A. N.] Estec, Directorate Sci & Robot Explorat, Sci Support Off, NL-2200 AG Noordwijk, Netherlands. [Valencic, L. A.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Valencic, L. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Smith, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schartel, N.] ESAC, Res & Sci Support Dept ESA, Astrophys & Fundamental Phys Missions Div, Villanueva De La Canada 28691, Madrid, Spain. RP Ness, JU (reprint author), ESAC, Sci Operat Dept ESA, XMM Newton Sci Operat Ctr, Villanueva De La Canada 28691, Madrid, Spain. EM juness@sciops.esa.int OI Parmar, Arvind/0000-0002-3307-6517 NR 12 TC 0 Z9 0 U1 1 U2 4 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD FEB PY 2014 VL 335 IS 2 BP 210 EP 220 DI 10.1002/asna.201312001 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI1DM UT WOS:000336590200012 ER PT J AU Meehl, GA Goddard, L Boer, G Burgman, R Branstator, G Cassou, C Corti, S Danabasoglu, G Doblas-Reyes, F Hawkins, E Karspeck, A Kimoto, M Kumar, A Matei, D Mignot, J Msadek, R Navarra, A Pohlmann, H Rienecker, M Rosati, T Schneider, E Smith, D Sutton, R Teng, HY van Oldenborgh, GJ Vecchi, G Yeager, S AF Meehl, Gerald A. Goddard, Lisa Boer, George Burgman, Robert Branstator, Grant Cassou, Christophe Corti, Susanna Danabasoglu, Gokhan Doblas-Reyes, Francisco Hawkins, Ed Karspeck, Alicia Kimoto, Masahide Kumar, Arun Matei, Daniela Mignot, Juliette Msadek, Rym Navarra, Antonio Pohlmann, Holger Rienecker, Michele Rosati, Tony Schneider, Edwin Smith, Doug Sutton, Rowan Teng, Haiyan van Oldenborgh, Geert Jan Vecchi, Gabriel Yeager, Stephen TI DECADAL CLIMATE PREDICTION An Update from the Trenches SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Review ID SEA-SURFACE TEMPERATURES; NORTH-ATLANTIC OCEAN; MERIDIONAL OVERTURNING CIRCULATION; INTERDECADAL PACIFIC OSCILLATION; MULTIYEAR PREDICTABILITY; MULTIMODEL-ENSEMBLE; TROPICAL STORMS; CMIP5 MODELS; PART I; VARIABILITY AB This paper provides an update on research in the relatively new and fast-moving field of decadal climate prediction, and addresses the use of decadal climate predictions not only for potential users of such information but also for improving our understanding of processes in the climate system. External forcing influences the predictions throughout, but their contributions to predictive skill become dominant after most of the improved skill from initialization with observations vanishes after about 6-9 years. Recent multimodel results suggest that there is relatively more decadal predictive skill in the North Atlantic, western Pacific, and Indian Oceans than in other regions of the world oceans. Aspects of decadal variability of SSTs, like the mid-1970s shift in the Pacific, the mid-1990s shift in the northern North Atlantic and western Pacific, and the early-2000s hiatus, are better represented in initialized hindcasts compared to uninitialized simulations. There is evidence of higher skill in initialized multimodel ensemble decadal hindcasts than in single model results, with multimodel initialized predictions for near-term climate showing somewhat less global warming than uninitialized simulations. Some decadal hindcasts have shown statistically reliable predictions of surface temperature over various land and ocean regions for lead times of up to 6-9 years, but this needs to be investigated in a wider set of models. As in the early days of El Nino-Southern Oscillation (ENSO) prediction, improvements to models will reduce the need for bias adjustment, and increase the reliability, and thus usefulness, of decadal climate predictions in the future. C1 [Meehl, Gerald A.; Branstator, Grant; Danabasoglu, Gokhan; Karspeck, Alicia; Teng, Haiyan; Yeager, Stephen] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Goddard, Lisa] Int Res Inst Climate & Soc, Palisades, NY USA. [Boer, George] Canadian Ctr Climate Modeling & Anal, Victoria, BC, Canada. [Burgman, Robert] Florida Int Univ, Miami, FL 33199 USA. [Cassou, Christophe] Ctr Europeen Rech & Format Avancee Calcul Sci, Toulouse, France. [Corti, Susanna] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England. [Corti, Susanna] Italian Natl Res Council, Inst Atmospher Sci & Climate, Bologna, Italy. [Doblas-Reyes, Francisco] Catalan Inst Climate Sci, Barcelona, Spain. [Hawkins, Ed; Sutton, Rowan] Univ Reading, Natl Ctr Atmospher Sci, Reading, Berks, England. [Kimoto, Masahide] Univ Tokyo, Kashiwa, Chiba, Japan. [Kumar, Arun] Natl Ctr Environm Predict, Climate Predict Ctr, Natl Oceanog & Atmospher Adm, College Pk, MD USA. [Matei, Daniela; Pohlmann, Holger] Max Planck Inst Meteorol, D-20146 Hamburg, Germany. [Mignot, Juliette] Inst Pierre Simon Laplace Sci Environm, Paris, France. [Mignot, Juliette] Univ Bern, Bern, Switzerland. [Msadek, Rym; Rosati, Tony; Vecchi, Gabriel] Geophys Fluid Dynam Lab, Princeton, NJ USA. [Navarra, Antonio] Ctr Euromediterraneo Cambiamenti Climatici, Bologna, Italy. [Navarra, Antonio] Ist Nazl Geofis & Vulcanol, Bologna, Italy. [Rienecker, Michele] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Schneider, Edwin] George Mason Univ, Fairfax, VA 22030 USA. [Schneider, Edwin] COLA, Calverton, MD USA. [Smith, Doug] Met Off Hadley Ctr, Exeter, Devon, England. [van Oldenborgh, Geert Jan] Koninklijk Nederlands Meteorol Inst, De Bilt, Netherlands. RP Meehl, GA (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. EM meehl@ncar.ucar.edu RI Vecchi, Gabriel/A-2413-2008; kimoto, masahide/P-9077-2014; Mignot, Juliette/F-3138-2011; Corti, Susanna/B-8224-2015; Hawkins, Ed/B-7921-2011; Doblas-Reyes, Francisco/C-1228-2016; OI Vecchi, Gabriel/0000-0002-5085-224X; Mignot, Juliette/0000-0002-4894-898X; Corti, Susanna/0000-0003-4456-6682; Hawkins, Ed/0000-0001-9477-3677; Doblas-Reyes, Francisco/0000-0002-6622-4280; Sutton, Rowan/0000-0001-8345-8583 FU NASA; NSF; NOAA; DOE; AIMES; Office of Science (BER); U.S. Department of Energy; National Science Foundation; NOAA MAPP program; NOAA CPO program; DECC/Defra Met Office Hadley Centre Climate Programme [GA01101]; European Community; BMBF North Atlantic II project; NASA Modeling, Analysis, and Prediction program; French GICC EPIDOM Project; Spanish RUCSS project FX The authors acknowledge the Aspen Global Change Institute (AGCI) in Aspen, Colorado, Director John Katzenberger for hosting the workshop that laid the foundations for this paper, and particularly all the attendees who contributed to the workshop discussions that led to this paper. Funding for the AGCI workshop was provided by NASA, NSF, NOAA, DOE, and AIMES. The authors thank three anonymous reviewers for their constructive comments that helped considerably to improve and clarify points made in the manuscript. Portions of this study were supported by the Office of Science (BER); U.S. Department of Energy; the National Science Foundation; the NOAA MAPP and NOAA CPO programs; the DECC/Defra Met Office Hadley Centre Climate Programme (GA01101); the European Community's Seventh Framework Programme (FP7/2007-2013) THOR and COMBINE projects; the BMBF North Atlantic II project; the NASA Modeling, Analysis, and Prediction program; the French GICC EPIDOM Project; and the Spanish RUCSS project. NR 138 TC 108 Z9 108 U1 8 U2 99 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 FEB PY 2014 VL 95 IS 2 BP 243 EP 267 DI 10.1175/BAMS-D-12-00241.1 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AE1JK UT WOS:000333725400008 ER PT J AU Hoerling, M Eischeid, J Kumar, A Leung, R Mariotti, A Mo, K Schubert, S Seager, R AF Hoerling, M. Eischeid, J. Kumar, A. Leung, R. Mariotti, A. Mo, K. Schubert, S. Seager, R. TI CAUSES AND PREDICTABILITY OF THE 2012 GREAT PLAINS DROUGHT SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID UNITED-STATES; DUST-BOWL; PRECIPITATION; TEMPERATURE; VARIABILITY; SUMMER; OCEAN AB Central Great Plains precipitation deficits during May-August 2012 were the most severe since at least 1895, eclipsing the Dust Bowl summers of 1934 and 1936. Drought developed suddenly in May, following near-normal precipitation during winter and early spring. Its proximate causes were a reduction in atmospheric moisture transport into the Great Plains from the Gulf of Mexico. Processes that generally provide air mass lift and condensation were mostly absent, including a lack of frontal cyclones in late spring followed by suppressed deep convection in the summer owing to large-scale subsidence and atmospheric stabilization. Seasonal forecasts did not predict the summer 2012 central Great Plains drought development, which therefore arrived without early warning. Climate simulations and empirical analysis suggest that ocean surface temperatures together with changes in greenhouse gases did not induce a substantial reduction in sum mertime precipitation over the central Great Plains during 2012. Yet, diagnosis of the retrospective climate simulations also reveals a regime shift toward warmer and drier summertime Great Plains conditions during the recent decade, most probably due to natural decadal variability. As a consequence, the probability of the severe summer Great Plains drought occurring may have increased in the last decade compared to the 1980s and 1990s, and the so-called tail risk for severe drought may have been heightened in summer 2012. Such an extreme drought event was nonetheless still found to be a rare occurrence within the spread of 2012 climate model simulations. The implications of this study's findings for U.S. seasonal drought forecasting are discussed. C1 [Hoerling, M.] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA. [Eischeid, J.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Kumar, A.; Mo, K.] NOAA, Climate Predict Ctr, Camp Springs, MD USA. [Leung, R.] Pacific NW Natl Lab, Dept Energy, Richland, WA 99352 USA. [Mariotti, A.] NOAA, Climate Program Off, Silver Spring, MD USA. [Schubert, S.] NASA, Global Modeling & Assimilat Off, Greenbelt, MD USA. [Seager, R.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. RP Hoerling, M (reprint author), NOAA, Earth Syst Res Lab, 325 Broadway, Boulder, CO 80305 USA. EM martin.hoerling@noaa.gov FU MAPP; National Integrated Drought Information System (NIDIS) Program FX The authors acknowledge resources and organizational support for the Drought Task Force from the Modeling, Analysis, Predictions and Projections Program (MAPP) of NOAA's Climate Program Office; activities are supported by MAPP in partnership with the National Integrated Drought Information System (NIDIS) Program. The authors also gratefully acknowledge support from their home institutions and various funding agencies, which help sustain their work. NR 24 TC 66 Z9 66 U1 3 U2 34 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 FEB PY 2014 VL 95 IS 2 BP 269 EP 282 DI 10.1175/BAMS-D-13-00055.1 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AE1JK UT WOS:000333725400009 ER PT J AU Yonekura, E Hall, TM AF Yonekura, Emmi Hall, Timothy M. TI ENSO Effect on East Asian Tropical Cyclone Landfall via Changes in Tracks and Genesis in a Statistical Model SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID WESTERN NORTH PACIFIC; EL-NINO; CLUSTER-ANALYSIS; HURRICANE RISK; TYPHOON TRACKS; OSCILLATION; CLIMATE; EVENTS; IMPACTS; SURGE AB Improvements on a statistical tropical cyclone (TC) track model in the western North Pacific Ocean are described. The goal of the model is to study the effect of El Nino-Southern Oscillation (ENSO) on East Asian TC landfall. The model is based on the International Best-Track Archive for Climate Stewardship (IBTrACS) database of TC observations for 1945-2007 and employs local regression of TC formation rates and track increments on the Nino-3.4 index and seasonally varying climate parameters. The main improvements are the inclusion of ENSO dependence in the track propagation and accounting for seasonality in both genesis and tracks. A comparison of simulations of the 1945-2007 period with observations concludes that the model updates improve the skill of this model in simulating TCs. Changes in TC genesis and tracks are analyzed separately and cumulatively in simulations of stationary extreme ENSO states. ENSO effects on regional (100-km scale) landfall are attributed to changes in genesis and tracks. The effect of ENSO on genesis is predominantly a shift in genesis location from the southeast in El Nino years to the northwest in La Nina years, resulting in higher landfall rates for the East Asian coast during La Nina. The effect of ENSO on track propagation varies seasonally and spatially. In the peak activity season (July-October), there are significant changes in mean tracks with ENSO. Landfall-rate changes from genesis- and track-ENSO effects in the Philippines cancel out, while coastal segments of Vietnam, China, the Korean Peninsula, and Japan show enhanced La Nina-year increases. C1 [Yonekura, Emmi] Columbia Univ, Dept Earth & Environm Sci, New York, NY 10025 USA. [Hall, Timothy M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Yonekura, E (reprint author), Columbia Univ, Dept Earth & Environm Sci, 2880 Broadway, New York, NY 10025 USA. EM ey2111@columbia.edu FU NASA Applied Sciences program FX This work was supported in part by a grant from the NASA Applied Sciences program. We thank Phil Klotzbach and two anonymous reviewers for their helpful comments on this work. NR 48 TC 3 Z9 3 U1 2 U2 11 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD FEB PY 2014 VL 53 IS 2 BP 406 EP 420 DI 10.1175/JAMC-D-12-0240.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH9FU UT WOS:000336448000014 ER PT J AU Heymsfield, A Winker, D Avery, M Vaughan, M Diskin, G Deng, M Mitev, V Matthey, R AF Heymsfield, Andrew Winker, Dave Avery, Melody Vaughan, Mark Diskin, Glenn Deng, Min Mitev, Valentin Matthey, Renaud TI Relationships between Ice Water Content and Volume Extinction Coefficient from In Situ Observations for Temperatures from 0 degrees to-86 degrees C: Implications for Spaceborne Lidar Retrievals SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID PARTICLE-SIZE; CALIPSO; CLOUDS; ALGORITHMS; PROFILES; CIRRUS AB An examination of 2 yr of Cloud-Aerosol Lidar Infrared Pathfinder Satellite Observations (CALIPSO) lidar observations and CloudSat cloud radar observations shows that ice clouds at temperatures below about -45 degrees C frequently fall below the CloudSat radar's detection threshold yet are readily detectable by the lidar. The CALIPSO ice water content (IWC) detection threshold is about 0.1 versus 5 mg m(-3) for CloudSat. This comparison emphasizes the need for developing a lidar-only IWC retrieval method that is reliable for high-altitude ice clouds at these temperatures in this climatically important zone of the upper troposphere. Microphysical measurements from 10 aircraft field programs, spanning latitudes from the Arctic to the tropics and temperatures from -86 degrees to 0 degrees C, are used to develop relationships between the IWC and volume extinction coefficient sigma in visible wavelengths. Relationships used to derive a radiatively important ice cloud property, the ice effective diameter D-e, froms sigma are also developed. Particle size distributions (PSDs) and direct IWC measurements, together with evaluations of the ice particle shapes and comparisons with semidirect extinction measurements, are used in this analysis. Temperature-dependent D-e(sigma) and IWC-sigma relationships developed empirically facilitate the retrieval of IWC from lidar-derived sigma and D-e values and for comparison with other IWC observations. This suite of empirically derived relationships can be expressed analytically. These relationships can be used to derive IWC and D-e froms sigma and are developed for use in climate models to derive sigma from prognosed values of IWC and specified PSD properties. C1 [Heymsfield, Andrew] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Winker, Dave; Avery, Melody; Vaughan, Mark; Diskin, Glenn] NASA, Langley Res Ctr, Hampton Rd, VA USA. [Deng, Min] Univ Wyoming, Laramie, WY 82071 USA. [Mitev, Valentin] Ctr Suisse Elect & Microtech SA, Neuchatel, Switzerland. [Matthey, Renaud] Univ Neuchatel, Inst Phys, CH-2000 Neuchatel, Switzerland. RP Heymsfield, A (reprint author), NCAR, 3450 Mitchell Ln, Boulder, CO 80301 USA. EM heyms1@ucar.edu FU CALIPSO Project Office at NASA Langley Research Center; NASA [NNX08AH57G] FX The authors thank the CALIPSO Project Office at NASA Langley Research Center for their support throughout the course of this research. Funding was also provided through NASA Grant NNX08AH57G. We thank Carl Schmitt and Aaron Bansemer of NCAR for their help during the course of this study. NR 25 TC 11 Z9 11 U1 0 U2 9 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD FEB PY 2014 VL 53 IS 2 BP 479 EP 505 DI 10.1175/JAMC-D-13-087.1 PG 27 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH9FU UT WOS:000336448000019 ER PT J AU Campbell, BA Ray Hawke, B Morgan, GA Carter, LM Campbell, DB Nolan, M AF Campbell, Bruce A. Ray Hawke, B. Morgan, Gareth A. Carter, Lynn M. Campbell, Donald B. Nolan, Michael TI Improved discrimination of volcanic complexes, tectonic features, and regolith properties in Mare Serenitatis from Earth-based radar mapping SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Moon; volcanism; regolith; radar ID OCEANUS PROCELLARUM; ARISTARCHUS PLATEAU; WAVELENGTH RADAR; 70-CM WAVELENGTH; LUNAR NEARSIDE; MOON; THICKNESS; STRATIGRAPHY; CONSTRAINTS; DEPOSITS AB Radar images at 70 cm wavelength show 4-5dB variations in backscatter strength within regions of relatively uniform spectral reflectance properties in central and northern Mare Serenitatis, delineating features suggesting lava flow margins, channels, and superposition relationships. These backscatter differences are much less pronounced at 12.6 cm wavelength, consistent with a large component of the 70 cm echo arising from the rough or blocky transition zone between the mare regolith and the intact bedrock. Such deep probing is possible because the ilmenite content, which modulates microwave losses, of central Mare Serenitatis is generally low (2-3% by weight). Modeling of the radar returns from a buried interface shows that an average regolith thickness of 10m could lead to the observed shifts in 70 cm echo power with a change in TiO2 content from 2% to 3%. This thickness is consistent with estimates of regolith depth (10-15m) based on the smallest diameter for which fresh craters have obvious blocky ejecta. The 70 cm backscatter differences provide a view of mare flow-unit boundaries, channels, and lobes unseen by other remote sensing methods. A localized pyroclastic deposit associated with Rima Calippus is identified based on its low radar echo strength. Radar mapping also improves delineation of units for crater age dating and highlights a 250 km long, east-west trending feature in northern Mare Serenitatis that we suggest is a large graben flooded by late-stage mare flows. C1 [Campbell, Bruce A.; Morgan, Gareth A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Ray Hawke, B.] Univ Hawaii Manoa, HIGP SOEST, Honolulu, HI 96822 USA. [Carter, Lynn M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Campbell, Donald B.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Nolan, Michael] Natl Astron & Ionosphere Ctr, Arecibo Observ, Arecibo, PR 00613 USA. RP Campbell, BA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM campbellb@si.edu RI Carter, Lynn/D-2937-2012; OI Nolan, Michael/0000-0001-8316-0680 FU NASA's Planetary Astronomy and Planetary Geology and Geophysics Programs; National Science Foundation [AST-1100968]; National Aeronautics and Space Administration [NNX12AF24G] FX The authors thank J. Cahill and an anonymous reviewer for their thoughtful comments on the manuscript. This work was supported in part by grants from NASA's Planetary Astronomy and Planetary Geology and Geophysics Programs. The authors thank the staff at Arecibo Observatory and the Green Bank Telescope for invaluable assistance in collecting the lunar radar data. John Chandler of the Smithsonian Astrophysical Observatory provided the lunar ephemerides for our mapping. Mark Cintala offered helpful comments during our consideration of models for regolith structure. The Arecibo Observatory is operated by SRI International under a cooperative agreement with the National Science Foundation (AST-1100968), and in alliance with Ana G. Mendez-Universidad Metropolitana, and the Universities Space Research Association. The Arecibo Planetary Radar Program is supported by the National Aeronautics and Space Administration under grant NNX12AF24G issued through the Near Earth Object Observations program. The Green Bank Telescope is part of the National Radio Astronomy Observatory, a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. NR 53 TC 8 Z9 8 U1 1 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD FEB PY 2014 VL 119 IS 2 BP 313 EP 330 DI 10.1002/2013JE004486 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AH6EZ UT WOS:000336224800001 ER PT J AU McAdam, AC Franz, HB Sutter, B Archer, PD Freissinet, C Eigenbrode, JL Ming, DW Atreya, SK Bish, DL Blake, DF Bower, HE Brunner, A Buch, A Glavin, DP Grotzinger, JP Mahaffy, PR McLennan, SM Morris, RV Navarro-Gonzalez, R Rampe, EB Squyres, SW Steele, A Stern, JC Sumner, DY Wray, JJ AF McAdam, Amy C. Franz, Heather B. Sutter, Brad Archer, Paul D., Jr. Freissinet, Caroline Eigenbrode, Jennifer L. Ming, Douglas W. Atreya, Sushil K. Bish, David L. Blake, David F. Bower, Hannah E. Brunner, Anna Buch, Arnaud Glavin, Daniel P. Grotzinger, John P. Mahaffy, Paul R. McLennan, Scott M. Morris, Richard V. Navarro-Gonzalez, Rafael Rampe, Elizabeth B. Squyres, Steven W. Steele, Andrew Stern, Jennifer C. Sumner, Dawn Y. Wray, James J. TI Sulfur-bearing phases detected by evolved gas analysis of the Rocknest aeolian deposit, Gale Crater, Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; MSL; SAM; sulfur; mineralogy; evolved gas analysis ID THERMOCHEMICAL SULFATE REDUCTION; MERIDIANI-PLANUM; MARTIAN METEORITES; OMEGA/MARS EXPRESS; MAGNESIUM-SULFATE; CHEMICAL-COMPOSITION; HYDROTHERMAL FLUIDS; CARBONATE MINERALS; MASS-SPECTROMETRY; HYDROGEN-SULFIDE AB The Sample Analysis at Mars (SAM) instrument suite detected SO2, H2S, OCS, and CS2 from similar to 450 to 800 degrees C during evolved gas analysis (EGA) of materials from the Rocknest aeolian deposit in Gale Crater, Mars. This was the first detection of evolved sulfur species from a Martian surface sample during in situ EGA. SO2 (similar to 3-22 mu mol) is consistent with the thermal decomposition of Fe sulfates or Ca sulfites, or evolution/desorption from sulfur-bearing amorphous phases. Reactions between reduced sulfur phases such as sulfides and evolved O-2 or H2O in the SAM oven are another candidate SO2 source. H2S (similar to 41-109nmol) is consistent with interactions of H2O, H-2 and/or HCl with reduced sulfur phases and/or SO2 in the SAM oven. OCS (similar to 1-5nmol) and CS2 (similar to 0.2-1nmol) are likely derived from reactions between carbon-bearing compounds and reduced sulfur. Sulfates and sulfites indicate some aqueous interactions, although not necessarily at the Rocknest site; Fe sulfates imply interaction with acid solutions whereas Ca sulfites can form from acidic to near-neutral solutions. Sulfides in the Rocknest materials suggest input from materials originally deposited in a reducing environment or from detrital sulfides from an igneous source. The presence of sulfides also suggests that the materials have not been extensively altered by oxidative aqueous weathering. The possibility of both reduced and oxidized sulfur compounds in the deposit indicates a nonequilibrium assemblage. Understanding the sulfur mineralogy in Rocknest materials, which exhibit chemical similarities to basaltic fines analyzed elsewhere on Mars, can provide insight in to the origin and alteration history of Martian surface materials. C1 [McAdam, Amy C.; Franz, Heather B.; Freissinet, Caroline; Eigenbrode, Jennifer L.; Bower, Hannah E.; Brunner, Anna; Glavin, Daniel P.; Mahaffy, Paul R.; Stern, Jennifer C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Franz, Heather B.] Univ Maryland Baltimore Cty, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21228 USA. [Sutter, Brad; Archer, Paul D., Jr.] Jacobs, Houston, TX USA. [Sutter, Brad; Archer, Paul D., Jr.; Ming, Douglas W.; Morris, Richard V.; Rampe, Elizabeth B.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA. [Atreya, Sushil K.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Bish, David L.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA. [Blake, David F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Brunner, Anna] Univ Maryland, Ctr Res & Explorat Space Sci & Technol, College Pk, MD 20742 USA. [Brunner, Anna] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Buch, Arnaud] Ecole Cent Paris, LGPM, Chatenay Malabry, France. [Grotzinger, John P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [McLennan, Scott M.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. [Navarro-Gonzalez, Rafael] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Lab Quim Plasmas & Estudios Planetarios, Mexico City 04510, DF, Mexico. [Squyres, Steven W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Steele, Andrew] Carnegie Inst Sci, Geophys Lab, Washington, DC USA. [Sumner, Dawn Y.] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. [Wray, James J.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. RP McAdam, AC (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Amy.McAdam@nasa.gov RI Wray, James/B-8457-2008; Gonzalez, Rafael/D-1748-2009; Glavin, Daniel/D-6194-2012 OI Wray, James/0000-0001-5559-2179; Glavin, Daniel/0000-0001-7779-7765 FU NASA Postdoctoral Program; NASA FX NASA provided support for the development of SAM. Data from these SAM experiments will be archived in the Planetary Data System (pds.nasa.gov) in 2013. Essential contributions to the successful operation of SAM on Mars and the acquisition of SAM data were provided by the SAM development, operations, and test bed teams. P. D. A. and C. F. acknowledge support from the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. We thank members of the SAM and larger MSL team for insightful discussions and support. We also thank Melissa Lane and two anonymous reviewers for helpful comments. NR 136 TC 15 Z9 15 U1 3 U2 38 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD FEB PY 2014 VL 119 IS 2 BP 373 EP 393 DI 10.1002/2013JE004518 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AH6EZ UT WOS:000336224800004 ER PT J AU Mishra, N Helder, D Angal, A Choi, J Xiong, XX AF Mishra, Nischal Helder, Dennis Angal, Amit Choi, Jason Xiong, Xiaoxiong TI Absolute Calibration of Optical Satellite Sensors Using Libya 4 Pseudo Invariant Calibration Site SO REMOTE SENSING LA English DT Article DE radiometric calibration; absolute calibration; PICS; BRDF; Landsat; MODIS ID NEAR-INFRARED CHANNELS; CROSS-CALIBRATION; DESERT SITES; BRDF MODELS; REFLECTANCE; MODIS; BAND AB The objective of this paper is to report the improvements in an empirical absolute calibration model developed at South Dakota State University using Libya 4 (+28.55 degrees, +23.39 degrees)pseudo invariant calibration site (PICS). The approach was based on use of the Terra MODIS as the radiometer to develop an absolute calibration model for the spectral channels covered by this instrument from visible to shortwave infrared. Earth Observing One (EO-1) Hyperion, with a spectral resolution of 10 nm, was used to extend the model to cover visible and near-infrared regions. A simple Bidirectional Reflectance Distribution function (BRDF) model was generated using Terra Moderate Resolution Imaging Spectroradiometer (MODIS) observations over Libya 4 and the resulting model was validated with nadir data acquired from satellite sensors such as Aqua MODIS and Landsat 7 (L7) Enhanced Thematic Mapper (ETM+). The improvements in the absolute calibration model to account for the BRDF due to off-nadir measurements and annual variations in the atmosphere are summarized. BRDF models due to off-nadir viewing angles have been derived using the measurements from EO-1 Hyperion. In addition to L7 ETM+, measurements from other sensors such as Aqua MODIS, UK-2 Disaster Monitoring Constellation (DMC), ENVISAT Medium Resolution Imaging Spectrometer (MERIS) and Operational Land Imager (OLI) onboard Landsat 8 (L8), which was launched in February 2013, were employed to validate the model. These satellite sensors differ in terms of the width of their spectral bandpasses, overpass time, off-nadir-viewing capabilities, spatial resolution and temporal revisit time, etc. The results demonstrate that the proposed empirical calibration model has accuracy of the order of 3% with an uncertainty of about 2% for the sensors used in the study. C1 [Mishra, Nischal; Helder, Dennis] S Dakota State Univ, Dept Elect Engn & Comp Sci, Brookings, SD 57007 USA. [Mishra, Nischal] S Dakota State Univ, Image Proc Lab, Dept Elect Engn & Comp Sci, Brookings, SD 57007 USA. [Angal, Amit] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Choi, Jason] Sigma Space Corp, Lanham, MD 20706 USA. [Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Mishra, N (reprint author), S Dakota State Univ, Dept Elect Engn & Comp Sci, Brookings, SD 57007 USA. EM nischal.mishra@sdstate.edu; Dennis.helder@sdstate.edu; Amit.Angal@ssaihq.com; taeyoung.choi@sigmaspace.com; Xiaoxiong.Xiong.1@gsfc.nasa.gov NR 24 TC 19 Z9 20 U1 2 U2 11 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD FEB PY 2014 VL 6 IS 2 BP 1327 EP 1346 DI 10.3390/rs6021327 PG 20 WC Remote Sensing SC Remote Sensing GA AH4JB UT WOS:000336092100021 ER PT J AU Barichivich, J Briffa, KR Myneni, R van der Schrier, G Dorigo, W Tucker, CJ Osborn, TJ Melvin, TM AF Barichivich, Jonathan Briffa, Keith R. Myneni, Ranga van der Schrier, Gerard Dorigo, Wouter Tucker, Compton J. Osborn, Timothy J. Melvin, Thomas M. TI Temperature and Snow-Mediated Moisture Controls of Summer Photosynthetic Activity in Northern Terrestrial Ecosystems between 1982 and 2011 SO REMOTE SENSING LA English DT Article DE boreal forest; snowpack; drought; soil moisture; NDVI3g; scPDSI ID CANADA BOREAL FORESTS; TREE-GROWTH; VEGETATION INDEXES; WATER EQUIVALENT; INTERIOR ALASKA; ATMOSPHERIC CO2; HIGH-LATITUDES; WHITE SPRUCE; DROUGHT; CLIMATE AB Recent warming has stimulated the productivity of boreal and Arctic vegetation by reducing temperature limitations. However, several studies have hypothesized that warming may have also increased moisture limitations because of intensified summer drought severity. Establishing the connections between warming and drought stress has been difficult because soil moisture observations are scarce. Here we use recently developed gridded datasets of moisture variability to investigate the links between warming and changes in available soil moisture and summer vegetation photosynthetic activity at northern latitudes (>45 degrees N) based on the Normalized Difference Vegetation Index (NDVI) since 1982. Moisture and temperature exert a significant influence on the interannual variability of summer NDVI over about 29% (mean r(2) = 0.29 +/- 0.16) and 43% (mean r(2) = 0.25 +/- 0.12) of the northern vegetated land, respectively. Rapid summer warming since the late 1980s (similar to 0.7 degrees C) has increased evapotranspiration demand and consequently summer drought severity, but contrary to earlier suggestions it has not changed the dominant climate controls of NDVI over time. Furthermore, changes in snow dynamics (accumulation and melting) appear to be more important than increased evaporative demand in controlling changes in summer soil moisture availability and NDVI in moisture-sensitive regions of the boreal forest. In boreal North America, forest NDVI declines are more consistent with reduced snowpack rather than with temperature-induced increases in evaporative demand as suggested in earlier studies. Moreover, summer NDVI variability over about 28% of the northern vegetated land is not significantly associated with moisture or temperature variability, yet most of this land shows increasing NDVI trends. These results suggest that changes in snow accumulation and melt, together with other possibly non-climatic factors are likely to play a significant role in modulating regional ecosystem responses to the projected warming and increase in evapotranspiration demand during the coming decades. C1 [Barichivich, Jonathan; Briffa, Keith R.; Osborn, Timothy J.; Melvin, Thomas M.] Univ E Anglia, Sch Environm Sci, Climat Res Unit, Norwich NR4 7TJ, Norfolk, England. [Barichivich, Jonathan] CEA CNRS UVSQ, CE Orme Merisiers, Lab Sci Climat & Environm, F-91191 Gif Sur Yvette, France. [Myneni, Ranga] Boston Univ, Dept Geog, Boston, MA 02215 USA. [van der Schrier, Gerard] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands. [Dorigo, Wouter] Vienna Univ Technol, Dept Geodesy & Geoinfomat, A-1040 Vienna, Austria. [Tucker, Compton J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Barichivich, J (reprint author), Univ E Anglia, Sch Environm Sci, Climat Res Unit, Norwich NR4 7TJ, Norfolk, England. EM J.Barichivich@uea.ac.uk; k.briffa@uea.ac.uk; ranga.myneni@gmail.com; gerard.van.der.schrier@knmi.nl; wd@ipf.tuwien.ac.at; compton.j.tucker@nasa.gov; t.osborn@uea.ac.uk; t.m.melvin@uea.ac.uk RI Myneni, Ranga/F-5129-2012; Osborn, Timothy/E-9740-2011; OI Osborn, Timothy/0000-0001-8425-6799; Briffa, Keith/0000-0003-3323-3639 FU Chilean Government under the program Formacion de Capital Humano Avanzado of CONICYT; School of Environmental Sciences of the University of East Anglia; UK NERC [NE/G018863/1]; NASA Earth Science Division; ESA's Climate Change Initiative for Soil Moisture [4000104814/11/I-NB] FX We thank Ryan Teuling and Frank Janssen for sharing their Matlab code for bivariate color maps and multivariate statistics (MVSTAT toolbox), respectively. We also thank Ed Cook for sharing his Fortran routine for Kalman Filter Regression. Liang Xu and Jiang Bi (Boston University) kindly provided the land cover and continuous vegetation fields data at the spatial resolution of GIMMS NDVI3g. JB was supported by a doctoral scholarship from the Chilean Government under the program Formacion de Capital Humano Avanzado of CONICYT and recently by a grant from the School of Environmental Sciences of the University of East Anglia. KRB, TJO and TMM acknowledge support from UK NERC (under grant NE/G018863/1). RBM acknowledges support from the NASA Earth Science Division. The contribution of WD was supported by ESA's Climate Change Initiative for Soil Moisture (Contract No. 4000104814/11/I-NB). We thank Jorge Pinzon for technical discussions and three anonymous reviewers for their helpful comments. NR 98 TC 24 Z9 24 U1 10 U2 53 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD FEB PY 2014 VL 6 IS 2 BP 1390 EP 1431 DI 10.3390/rs6021390 PG 42 WC Remote Sensing SC Remote Sensing GA AH4JB UT WOS:000336092100024 ER PT J AU Ray, RD Erofeeva, SY AF Ray, Richard D. Erofeeva, Svetlana Y. TI Long-period tidal variations in the length of day SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE Earth rotation; tides; length of day ID OCEAN TIDES; HARMONIC DEVELOPMENT; MANTLE ANELASTICITY; EARTH ROTATION; EQUILIBRIUM AB A new model of long-period tidal variations in length of day is developed. The model comprises 80 spectral lines with periods between 18.6 years and 4.7 days, and it consistently includes effects of mantle anelasticity and dynamic ocean tides for all lines. The anelastic properties follow Wahr and Bergen; experimental confirmation for their results now exists at the fortnightly period, but there remains uncertainty when extrapolating to the longest periods. The ocean modeling builds on recent work with the fortnightly constituent, which suggests that oceanic tidal angular momentum can be reliably predicted at these periods without data assimilation. This is a critical property when modeling most long-period tides, for which little observational data exist. Dynamic ocean effects are quite pronounced at shortest periods as out-of-phase rotation components become nearly as large as in-phase components. The model is tested against a 20 year time series of space geodetic measurements of length of day. The current international standard model is shown to leave significant residual tidal energy, and the new model is found to mostly eliminate that energy, with especially large variance reduction for constituents Sa, Ssa, Mf, and Mt. C1 [Ray, Richard D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Erofeeva, Svetlana Y.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA. RP Ray, RD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM richard.ray@nasa.gov RI Ray, Richard/D-1034-2012 FU National Aeronautics and Space Administration FX We thank Gary Egbert, Duncan Agnew, and Shailen Desai for useful discussions and comments. This work was supported by the National Aeronautics and Space Administration's Ocean Surface Topography and Earth Surface/Interiors programs. NR 40 TC 8 Z9 8 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD FEB PY 2014 VL 119 IS 2 BP 1498 EP 1509 DI 10.1002/2013JB010830 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AD2AK UT WOS:000333034600037 ER PT J AU Contreras, MT Pasala, DTR Nagarajaiah, S AF Contreras, Michael T. Pasala, Dharma Theja Reddy Nagarajaiah, Satish TI Adaptive length SMA pendulum smart tuned mass damper performance in the presence of real time primary system stiffness change SO SMART STRUCTURES AND SYSTEMS LA English DT Article DE smart tuned mass damper; adaptive passive tuned mass damper; tuned vibration absorbers; shape memory alloy; adaptive length pendulum; observer based structural health monitoring ID STRUCTURAL CONTROL; RESPONSE CONTROL; IDENTIFICATION; TRANSFORM AB In a companion paper, Pasala and Nagarajaiah analytically and experimentally validate the Adaptive Length Pendulum Smart Tuned Mass Damper (ALP-STMD) on a primary structure (2 story steel structure) whose frequencies are time invariant (Pasala and Nagarajaiah 2012). In this paper, the ALP-STMD effectiveness on a primary structure whose frequencies are time varying is studied experimentally. This study experimentally validates the ability of an ALP-STMD to adequately control a structural system in the presence of real time changes in primary stiffness that are detected by a real time observer based system identification. The experiments implement the newly developed Adaptive Length Pendulum Smart Tuned Mass Damper (ALP-STMD) which was first introduced and developed by Nagarajaiah (2009), Nagarajaiah and Pasala (2010) and Nagarajaiah et al. (2010). The ALP-STMD employs a mass pendulum of variable length which can be tuned in real time to the parameters of the system using sensor feedback. The tuning action is made possible by applying a current to a shape memory alloy wire changing the effective length that supports the damper mass assembly in real time. Once a stiffness change in the structural system is detected by an open loop observer, the ALP-STMD is re-tuned to the modified system parameters which successfully reduce the response of the primary system. Significant performance improvement is illustrated for the stiffness modified system, which undergoes the re-tuning adaptation, when compared to the stiffness modified system without adaptive re-tuning. C1 [Contreras, Michael T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Pasala, Dharma Theja Reddy] Rice Univ, Dept Civil & Environm Engn, Houston, TX 77005 USA. [Nagarajaiah, Satish] Rice Univ, Dept Civil & Environm Engn & Mech Engn & Mat Sci, Houston, TX 77005 USA. RP Nagarajaiah, S (reprint author), Rice Univ, Dept Civil & Environm Engn & Mech Engn & Mat Sci, Houston, TX 77005 USA. EM Michael.T.Contreras@jpl.nasa.gov; drp1@rice.edu; Satish.Nagarajaiah@rice.edu RI PASALA, DHARMA THEJA/G-1358-2014; Nagarajaiah, Satish/E-6291-2012 OI PASALA, DHARMA THEJA/0000-0003-0689-2364; Nagarajaiah, Satish/0000-0003-0088-1656 FU National Science Foundation [CMMI-0830391, HRD-0450363] FX The authors would like to acknowledge support from the National Science Foundation through cooperative agreement no. CMMI-0830391. Additionally, the first author gratefully acknowledges the National Science Foundation for its support through the Alliance for Graduate Education and the Professoriate fellowship program, cooperative agreement no. HRD-0450363. NR 28 TC 4 Z9 4 U1 2 U2 13 PU TECHNO-PRESS PI DAEJEON PA PO BOX 33, YUSEONG, DAEJEON 305-600, SOUTH KOREA SN 1738-1584 J9 SMART STRUCT SYST JI Smart. Struct. Syst. PD FEB PY 2014 VL 13 IS 2 BP 219 EP 233 PG 15 WC Engineering, Civil; Engineering, Mechanical; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA AH9AX UT WOS:000336432200004 ER PT J AU Taylor, PC AF Taylor, Patrick C. TI Variability of Monthly Diurnal Cycle Composites of TOA Radiative Fluxes in the Tropics SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article DE Radiative fluxes; Cloud forcing; Tropics; Satellite observations; Shortwave radiation; Diurnal effects ID OUTGOING LONGWAVE RADIATION; BUDGET; CLOUD; CONVECTION; SATELLITE; LAYER; STRATOCUMULUS; PRECIPITATION; ENTRAINMENT; RAINFALL AB Earth system variability is generated by a number of different sources and time scales. Understanding sources of atmospheric variability is critical to reducing the uncertainty in climate models and to understanding the impacts of sampling on observational datasets. The diurnal cycle is a fundamental variability evident in many geophysical variables-including top-of-the-atmosphere (TOA) radiative fluxes. This study considers aspects of the TOA flux diurnal cycle not previously analyzed: namely, deseasonalized variations in the monthly diurnal cycle composites, termed monthly diurnal cycle variability. Significant variability in the monthly diurnal cycle composites is found in both outgoing longwave radiation (OLR) and reflected shortwave (RSW). OLR and RSW monthly diurnal cycle variability exhibits a regional structure that follows traditional, climatological diurnal cycle categorization by prevailing cloud and surface types. The results attribute monthly TOA flux diurnal cycle variability to variations in the diurnal cloud evolution, which is sensitive to monthly atmospheric dynamic- and thermodynamic-state anomalies. The results also suggest that monthly diurnal cycle variability can amplify or buffer monthly TOA flux anomalies, depending on the region. Considering the impact of monthly diurnal cycle variability on monthly TOA flux anomalies, the results suggest that monthly TOA flux diurnal cycle variability must be considered when constructing a TOA flux dataset from sun-synchronous orbit. The magnitude of monthly diurnal composite variability in OLR and RSW is regionally dependent-1-7 W m(-2) and 10%-80% relative to interannual TOA flux variability. The largest (4-7 W m(-2); 40%-80%) and smallest (1-3 W m(-2); 10%-30%) TOA flux uncertainties occur in convective and nonconvective regions, respectively, over both land and ocean. C1 [Taylor, Patrick C.] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. RP Taylor, PC (reprint author), NASA, Langley Res Ctr, 21 Langley Blvd,Mail Stop 420, Hampton, VA 23681 USA. EM patrick.c.taylor@nasa.gov RI Taylor, Patrick/D-8696-2015 OI Taylor, Patrick/0000-0002-8098-8447 FU NASA Energy and Water Cycle Studies program [NNH10ZDA001N] FX The author would like to thank the anonymous reviewers for their insightful comments. This work is supported by the NASA Energy and Water Cycle Studies program through Grant NNH10ZDA001N. The CERES data used in this study are stored at the Atmospheric Science Data Center at NASA Langley (https://eosweb.larc.nasa.gov). NR 28 TC 5 Z9 5 U1 0 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 EI 1520-0469 J9 J ATMOS SCI JI J. Atmos. Sci. PD FEB PY 2014 VL 71 IS 2 BP 754 EP 766 DI 10.1175/JAS-D-13-0112.1 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AG5XF UT WOS:000335491300001 ER PT J AU Yu, W Farrugia, CJ Lugaz, N Galvin, AB Kilpua, EKJ Kucharek, H Mostl, C Leitner, M Torbert, RB Simunac, KDC Luhmann, JG Szabo, A Wilson, LB Ogilvie, KW Sauvaud, JA AF Yu, W. Farrugia, C. J. Lugaz, N. Galvin, A. B. Kilpua, E. K. J. Kucharek, H. Mostl, C. Leitner, M. Torbert, R. B. Simunac, K. D. C. Luhmann, J. G. Szabo, A. Wilson, L. B., III Ogilvie, K. W. Sauvaud, J. -A. TI A statistical analysis of properties of small transients in the solar wind 2007-2009: STEREO andWind observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE small solar wind transients in 2007-2009 ID CORONAL MASS EJECTIONS; INTERPLANETARY MAGNETIC CLOUDS; ELECTRON-TEMPERATURE; PROTON TEMPERATURE; FLUX ROPES; 1 AU; EARTH; HELIOSPHERE; CONNECTION; SIGNATURES AB We present a comprehensive statistical analysis of small solar wind transients (STs) in 2007-2009. Extending work on STs by Kilpua et al. (2009) to a 3 year period, we arrive at the following identification criteria: (i) a duration < 12 h, (ii) a low proton temperature and/or a low proton beta, and (iii) enhanced field strength relative to the 3 year average. In addition, it must have at least one of the following: (a) decreased magnetic field variability, (b) large, coherent rotation of the field vector, (c) low Alfven Mach number, and (d) T-e/T-p higher than the 3 year average. These criteria include magnetic flux ropes. We searched for STs using Wind and STEREO data. We exclude Alfvenic fluctuations. Case studies illustrate features of these configurations. In total, we find 126 examples, approximate to 81% of which lie in the slow solar wind ( 450 km s(-1)). Many start or end with sharp field and flow gradients/discontinuities. Year 2009 had the largest number of STs. The average ST duration is approximate to 4.3 h, 75%<6 h. Comparing with interplanetary coronal mass ejections (ICMEs) in the same solar minimum, we find the major difference to be that T-p in STs is not significantly less than the expected T-p. Thus, whereas a low T-p is generally considered a very reliable signature of ICMEs, it is not a robust signature of STs. Finally, since plasma approximate to 1, force-free modeling of STs having a magnetic flux rope geometry may be inappropriate. Key Points Tp in small transients is not much less thanthe expected proton temperature Low Tp is not a robust signature of small transients Force-free modeling of flux rope small transients may be inappropriate C1 [Yu, W.; Farrugia, C. J.; Lugaz, N.; Galvin, A. B.; Kucharek, H.; Torbert, R. B.; Simunac, K. D. C.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Yu, W.; Farrugia, C. J.; Lugaz, N.; Galvin, A. B.; Kucharek, H.; Torbert, R. B.; Simunac, K. D. C.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Kilpua, E. K. J.] Univ Helsinki, Dept Phys, Div Geophys & Astron, Helsinki, Finland. [Mostl, C.; Leitner, M.] Graz Univ, Inst Phys, Graz, Austria. [Mostl, C.; Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Szabo, A.; Wilson, L. B., III; Ogilvie, K. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sauvaud, J. -A.] Univ Toulouse, Inst Rech Astrophys & Planetol CNRS UPS, Toulouse, France. RP Yu, W (reprint author), Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. EM charlie.farrugia@unh.edu RI Wilson III, Lynn/D-4425-2012; Lugaz, Noe/C-1284-2008; Kilpua, Emilia/G-8994-2012; OI Wilson III, Lynn/0000-0002-4313-1970; Lugaz, Noe/0000-0002-1890-6156; Moestl, Christian/0000-0001-6868-4152 FU NASA [NNX12AH45G, NNX13AP39G, NNX09AG28G, NNX13AP52G]; NSF [AGS-1140211]; STEREO/PLASTIC grant; Marie Curie International Outgoing Fellowship; European Community; COMESEP [263252] FX This work was supported by NASA grants NNX12AH45G, NNX13AP39G, and NNX09AG28G, NSF grant AGS-1140211, and STEREO/PLASTIC grant to UNH. This research was supported by a Marie Curie International Outgoing Fellowship with the 7th European Community Framework Programme. The work has received funding from the Seventh Framework Program (FP7/2007-2013) under grant 263252 [COMESEP]. Work supported also by NASA grant NNX13AP52G. NR 52 TC 7 Z9 7 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD FEB PY 2014 VL 119 IS 2 BP 689 EP 708 DI 10.1002/2013JA019115 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AD2CP UT WOS:000333041000005 ER PT J AU Uritsky, VM Slavin, JA Boardsen, SA Sundberg, T Raines, JM Gershman, DJ Collinson, G Sibeck, D Khazanov, GV Anderson, BJ Korth, H AF Uritsky, V. M. Slavin, J. A. Boardsen, S. A. Sundberg, T. Raines, J. M. Gershman, D. J. Collinson, G. Sibeck, D. Khazanov, G. V. Anderson, B. J. Korth, H. TI Active current sheets and candidate hot flow anomalies upstream of Mercury's bow shock SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE solar wind; MESSENGER mission; bow shock; hot flow anomaly; Mercury's magnetosphere ID DIAMAGNETIC CAVITIES UPSTREAM; MESSENGERS 1ST FLYBY; SOLAR-WIND; MAGNETIC-FIELD; FORESHOCK CAVITIES; TANGENTIAL DISCONTINUITY; PLASMA STRUCTURES; DENSITY HOLES; INTERPLANETARY; MAGNETOSPHERE AB Hot flow anomalies (HFAs) represent a subset of solar wind discontinuities interacting with collisionless bow shocks. They are typically formed when the normal component of the motional (convective) electric field points toward the embedded current sheet on at least one of its sides. The core region of an HFA contains hot and highly deflected ion flows and rather low and turbulent magnetic field. In this paper, we report observations of possible HFA-like events at Mercury identified over a course of two planetary years. Using data from the orbital phase of the MESSENGER mission, we identify a representative ensemble of active current sheets magnetically connected to Mercury's bow shock. We show that some of these events exhibit magnetic and particle signatures of HFAs similar to those observed at other planets, and present their key physical characteristics. Our analysis suggests that Mercury's bow shock does not only mediate the flow of supersonic solar wind plasma but also provides conditions for local particle acceleration and heating as predicted by previous numerical simulations. Together with earlier observations of HFA activity at Earth, Venus, Mars, and Saturn, our results confirm that hot flow anomalies could be a common property of planetary bow shocks and show that the characteristic size of these events is controlled by the bow shock standoff distance and/or local solar wind conditions. Key Points First observations of hot flow anomaly-like events at Mercury's bow shock New method for studying magnetic turbulence in kinetically active current sheets Comparative analysis of HFA events at different planets C1 [Uritsky, V. M.; Boardsen, S. A.; Sundberg, T.; Collinson, G.; Sibeck, D.; Khazanov, G. V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Uritsky, V. M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Slavin, J. A.; Raines, J. M.; Gershman, D. J.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Boardsen, S. A.] Univ Maryland, Goddard Planetary Heliophys Inst, Baltimore, MD 21201 USA. [Sundberg, T.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA. [Anderson, B. J.; Korth, H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Uritsky, VM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM vadim.uritsky@nasa.gov RI Slavin, James/H-3170-2012; feggans, john/F-5370-2012 OI Slavin, James/0000-0002-9206-724X; FU NASA through the CUA's Institute for Astrophysics and Computational Sciences [NNG11PL10A 670.002] FX The work of V.U. was supported by the NASA grant NNG11PL10A 670.002 through the CUA's Institute for Astrophysics and Computational Sciences. NR 79 TC 3 Z9 3 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD FEB PY 2014 VL 119 IS 2 BP 853 EP 876 DI 10.1002/2013JA019052 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AD2CP UT WOS:000333041000017 ER PT J AU Dmitriev, AV Suvorova, AV Chao, JK Wang, CB Rastaetter, L Panasyuk, MI Lazutin, LL Kovtyukh, AS Veselovsky, IS Myagkova, IN AF Dmitriev, A. V. Suvorova, A. V. Chao, J-K. Wang, C. B. Rastaetter, L. Panasyuk, M. I. Lazutin, L. L. Kovtyukh, A. S. Veselovsky, I. S. Myagkova, I. N. TI Anomalous dynamics of the extremely compressed magnetosphere during 21 January 2005 magnetic storm SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE erupting filament; geomagnetic storm; magnetosphere boundary layers; ring current decay ID EARTHS BOW SHOCK; SOLAR ENERGETIC PARTICLES; ART. NO. 1341; RING CURRENT; GEOMAGNETIC STORMS; DAYSIDE MAGNETOPAUSE; UNUSUAL LOCATIONS; WIND CONTROL; AUGUST 1972; D-ST AB The dayside magnetosphere and proton radiation belt were analyzed during unusual magnetic storm on 21 January 2005. We have found that from 1712 to 2400 UT, the subsolar magnetopause was continuously located inside geosynchronous orbit due to strong compression. The compression was extremely strong from 1846 to 2035 UT when the dense plasma of fast erupting filament produced the solar wind dynamic pressure that peaked up to >100 nPa, and during the first time, the upstream solar wind was observed at geosynchronous orbit for almost 2 h. Under the extreme compression, the outer magnetosphere at L>5 was pushed inward, and the outer radiation belt particles moved earthward, became adiabatically accelerated, and accumulated in the inner magnetosphere at L<4 that produced the intensified ring current with an exceptionally long lifetime. The observations were compared with predictions of various empirical and first-principles models. All the models failed to predict the magnetospheric dynamics under the extreme compression when the minimal magnetopause distance was estimated to be similar to 3 RE. The inconsistencies might result from distortions of plasma measurements by extreme heliospheric conditions consisting in very fast solar wind streams and intense fluxes of solar energetic particles. We speculated that anomalous dynamics of the magnetosphere could be well described by the models if the He abundance in the solar wind was assumed to be >20%, which is well appropriate for erupting filaments and which is in agreement with the upper 27% threshold for the He/H ratio obtained from Cluster measurements. Key Points Extreme compression pushes the bow shock inside geosynchronous orbit for 2 h Ring current moves to the inner magnetosphere (L similar to 3) with betatron energization High He abundance in the erupting filament allows predicting the observations C1 [Dmitriev, A. V.; Suvorova, A. V.; Chao, J-K.] Natl Cent Univ, Inst Space Sci, Chungli 32054, Taiwan. [Dmitriev, A. V.; Suvorova, A. V.; Panasyuk, M. I.; Lazutin, L. L.; Kovtyukh, A. S.; Veselovsky, I. S.; Myagkova, I. N.] Moscow MV Lomonosov State Univ, Skobeltsyn Inst Nucl Phys, Moscow, Russia. [Wang, C. B.] Univ Sci & Technol China, Dept Geophys & Planetary Sci, CAS Key Lab Geospace Environm, Hefei 230026, Peoples R China. [Rastaetter, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Veselovsky, I. S.] Russian Acad Sci, Space Res Inst IKI, Moscow, Russia. RP Dmitriev, AV (reprint author), Natl Cent Univ, Inst Space Sci, Chungli 32054, Taiwan. EM dalex@jupiter.ss.ncu.edu.tw RI Panasyuk, Mikhail/E-2005-2012; Rastaetter, Lutz/D-4715-2012; Suvorova, Alla/J-4174-2012; Dmitriev, Alexei/J-6161-2012 OI Rastaetter, Lutz/0000-0002-7343-4147; Suvorova, Alla/0000-0002-5146-0846; Dmitriev, Alexei/0000-0001-8038-251X FU National Science Council of Taiwan [NSC102-2111-M-008-023]; Ministry of Education under the Aim for Top University program [102G901-27]; RFBR [13-02-00461]; RAS Presidium [P22, P26] FX The authors thank NASA/GSFC ISTP for providing data from the ACE, GOES, LANL, and Cluster satellites. We are grateful to Cluster CIS and FGM instrument teams who have created the CIS (CODIF and HIA) and FGM instruments and made their data available to the community. In particular, we greatly appreciate the anonymous reviewer for providing the Cluster plasma data from the more recent calibrations of the CIS team. We thank C.W. Smith from the University of New Hampshire for providing the ACE magnetic data and R. Skoug from Los Alamos National Laboratory for providing the ACE plasma data. We also thank NASA and NOAA for providing the GOES magnetic data, Los Alamos National Laboratory for providing the LANL plasma data, and Kyoto World Data Center for Geomagnetism for providing the Dst and ASY/SYM indices. Simulation results of SWMF/BATS-R-US code have been provided by the Community Coordinated Modeling Center at Goddard Space Flight Center through their public Runs on Request system (http://ccmc.gsfc.nasa.gov). The CCMC is a multiagency partnership between NASA, AFMC, AFOSR, AFRL, AFWA, NOAA, NSF, and ONR. This work was supported by grants NSC102-2111-M-008-023 from the National Science Council of Taiwan and by Ministry of Education under the Aim for Top University program 102G901-27 at National Central University of Taiwan as well as by RFBR grant 13-02-00461 and Programs P22, P26 of the RAS Presidium at MSU SINP and IKI. NR 74 TC 4 Z9 4 U1 3 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD FEB PY 2014 VL 119 IS 2 BP 877 EP 896 DI 10.1002/2013JA019534 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AD2CP UT WOS:000333041000018 ER PT J AU Tsurutani, BT Falkowski, BJ Pickett, JS Verkhoglyadova, OP Santolik, O Lakhina, GS AF Tsurutani, Bruce T. Falkowski, Barbara J. Pickett, Jolene S. Verkhoglyadova, Olga P. Santolik, Ondrej Lakhina, Gurbax S. TI Extremely intense ELFmagnetosonicwaves: A survey of polar observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Magneotosonic waves; plasmaspheric hiss; plasmasphere; substorm protons; mode conversion ID EQUATORIAL NOISE; PLASMASPHERIC HISS; RING CURRENT; MAGNETIC DECREASES; CLUSTER SPACECRAFT; ALFVEN WAVES; PROPAGATION; CHORUS; PROTON; FREQUENCY AB A Polar magnetosonic wave (MSW) study was conducted using 1 year of 1996-1997 data (during solar minimum). Waves at and inside the plasmasphere were detected at all local times with a slight preference for occurrence in the midnight-postmidnight sector. Wave occurrence (and intensities) peaked within similar to 5 degrees of the magnetic equator, with half maxima at similar to 10 degrees. However, MSWs were also detected as far from the equator as +20 degrees and 60 degrees MLAT but with lower intensities. An extreme MSW intensity event of amplitude B-w=similar to 1 nT and E-w=similar to 25 mV/m was detected. This event occurred near local midnight, at the plasmapause, at the magnetic equator, during an intense substorm event, e.g., a perfect occurrence. These results support the idea of generation by protons injected from the plasma sheet into the midnight sector magnetosphere by substorm electric fields. MSWs were also detected near noon (1259 MLT) during relative geomagnetic quiet (low AE). A possible generation mechanism is a recovering/expanding plasmasphere engulfing preexisting energetic ions, in turn leading to ion instability. The wave magnetic field components are aligned along the ambient magnetic field direction, with the wave electric components orthogonal, indicating linear wave polarization. The MSW amplitudes decreased at locations further from the magnetic equator, while transverse whistler mode wave amplitudes (hiss) increased. We argue that intense MSWs are always present somewhere in the magnetosphere during strong substorm/convection events. We thus suggest that modelers use dynamic particle tracing codes and the maximum (rather than average) wave amplitudes to simulate wave-particle interactions. C1 [Tsurutani, Bruce T.; Falkowski, Barbara J.; Verkhoglyadova, Olga P.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Falkowski, Barbara J.] Glendale Community City Coll, Dept Phys, Glendale, CA USA. [Falkowski, Barbara J.] Glendale Community City Coll, Dept Astron, Glendale, CA USA. [Pickett, Jolene S.] Univ Iowa, Iowa City, IA USA. [Verkhoglyadova, Olga P.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Santolik, Ondrej] ASCR, Inst Atmospher Phys, Prague, Czech Republic. [Santolik, Ondrej] Charles Univ Prague, Fac Math & Phys, Prague, Czech Republic. [Lakhina, Gurbax S.] Indian Inst Geomagnetism, Navi Mumbai, India. RP Tsurutani, BT (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM bruce.t.tsurutani@jpl.nasa.gov RI Santolik, Ondrej/F-7766-2014; OI Lakhina, Gurbax /0000-0002-8956-486X; Verkhoglyadova, Olga/0000-0002-9295-9539 FU NASA; University of Iowa under JPL [1246597]; National Academy of Sciences, India under the NASI-Senior Scientist Platinum jubilee Fellowship; [GACR205-10/2279]; [LH11122] FX Portions of this research were performed at the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA, and at the University of Iowa under JPL subcontract 1246597. O.S. acknowledges support from GACR205-10/2279 and LH11122. G.L.S. thanks the National Academy of Sciences, India, for the support under the NASI-Senior Scientist Platinum Jubilee Fellowship. We acknowledge NASA's CDAWeb for providing the TIMAS data used in this study. We thank the two referees for helpful comments/suggestions that have helped improve this paper. NR 49 TC 25 Z9 25 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD FEB PY 2014 VL 119 IS 2 BP 964 EP 977 DI 10.1002/2013JA019284 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AD2CP UT WOS:000333041000023 ER PT J AU Collinson, GA Sibeck, DG Masters, A Shane, N Zhang, TL Fedorov, A Barabash, S Coates, AJ Moore, TE Slavin, JA Uritsky, VM Boardsen, S Sarantos, M AF Collinson, G. A. Sibeck, D. G. Masters, A. Shane, N. Zhang, T. L. Fedorov, A. Barabash, S. Coates, A. J. Moore, T. E. Slavin, J. A. Uritsky, V. M. Boardsen, S. Sarantos, M. TI A survey of hot flow anomalies at Venus SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Venus; hot flow anomaly; bow shock; Venus Express ID EARTHS BOW SHOCK; DIAMAGNETIC CAVITIES UPSTREAM; MULTI-SPACECRAFT MEASUREMENTS; CLUSTER OBSERVATIONS; CURRENT SHEET; SOLAR-WIND; EXPRESS; LOCATION; PLASMA; ASPERA-4 AB We present the first survey of hot flow anomalies (HFAs) at the bow shock of Venus, expanding on our recent initial case study. A 3.06 sol (774 Earth day) survey of Venus Express magnetometer, ion spectrometer, and electron spectrometer data was undertaken in order to identify Cytherian HFAs. Seven events were discovered, corresponding to a statistical frequency approximate to 1.20.8 per day, approximately the same rate as at the Earth. All seven HFAs were centered on a discontinuity in the solar wind, with inward pointing motional electric fields on at least one side, and exhibited electron and ion perturbations consistent with heating. For one event the calculation of continuous electron moments is possible, revealing that electron temperature increased from approximate to 2x10(5) K to 8x10(5) K in the HFA core (comparable to terrestrial and Kronian HFA observations), and density increased from approximate to 1cm(-3) to similar to 22.5cm(-3) in the bounding compression regions. Cytherian HFAs were found to be physically smaller (0.41.7Venus radii (R-V)) than their terrestrial or Kronian counterparts, although are much larger when compared to the overall size of the system (approximate to 130% of the subsolar bow shock distance), and occur very close (1.53.0R(V)) to the planet. Thus, we hypothesize that HFAs have a much more dominant role in the dynamics of the induced magnetosphere of Venus relative to the magnetospheres of magnetized planets. C1 [Collinson, G. A.; Sibeck, D. G.; Moore, T. E.; Uritsky, V. M.; Boardsen, S.; Sarantos, M.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Masters, A.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa, Japan. [Shane, N.; Coates, A. J.] Univ Coll London, Mullard Space Sci Lab, Holmbury, Surrey, England. [Shane, N.] UCL Birkbeck, Ctr Planetary Sci, London, England. [Zhang, T. L.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. [Fedorov, A.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Barabash, S.] Swedish Inst Space Phys, S-98128 Kiruna, Sweden. [Slavin, J. A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Uritsky, V. M.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Baltimore, MD USA. [Boardsen, S.; Sarantos, M.] Univ Maryland, Goddard Planetary & Heliophys Inst, Catonsville, MD 21228 USA. RP Collinson, GA (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. EM glyn.a.collinson@nasa.gov RI Slavin, James/H-3170-2012; Coates, Andrew/C-2396-2008; OI Slavin, James/0000-0002-9206-724X; Coates, Andrew/0000-0002-6185-3125; Shane, Neville/0000-0003-1024-7739 FU NASA; UK STFC FX This work was supported by an appointment to the NASA Postdoctoral Program at NASA Goddard Spaceflight Center, administered by Oak Ridge Associated Universities through a contract with NASA. This work was also supported by UK STFC through a rolling grant to MSSL/UCL. NR 49 TC 4 Z9 4 U1 3 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD FEB PY 2014 VL 119 IS 2 BP 978 EP 991 DI 10.1002/2013JA018863 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AD2CP UT WOS:000333041000024 ER PT J AU Sibeck, DG Lin, RQ AF Sibeck, D. G. Lin, R. -Q. TI Size and shape of the distant magnetotail SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE magnetotail; magnetopause; bow shock ID INTERPLANETARY MAGNETIC-FIELD; GLOBAL MAGNETOHYDRODYNAMIC SIMULATION; GEOMAGNETIC TAIL; BOUNDARY-LAYER; PLASMA SHEET; MAGNETOSPHERIC CONFIGURATION; MHD SIMULATIONS; IMF DEPENDENCE; NORTHWARD IMF; MAGNETOPAUSE AB We employ a global magnetohydrodynamic model to study the effects of the interplanetary magnetic field (IMF) strength and direction upon the cross section of the magnetotail at lunar distances. The anisotropic pressure of draped magnetosheath magnetic field lines and the inclusion of a reconnection-generated standing slow mode wave fan bounded by a rotational discontinuity within the definition of the magnetotail result in cross sections elongated in the direction parallel to the component of the IMF in the plane perpendicular to the Sun-Earth line. Tilted cross-tail plasma sheets separate the northern and southern lobes within these cross sections. Greater fast-mode speeds perpendicular than parallel to the draped magnetosheath magnetic field lines result in greater distances to the bow shock in the direction perpendicular than parallel to the component of the IMF in the plane transverse to the Sun-Earth line. The magnetotail cross section responds rapidly to variations in the IMF orientation. The rotational discontinuity associated with newly reconnected magnetic field lines requires no more than the magnetosheath convection time to appear at any distance downstream, and further adjustments of the cross section in response to the anisotropic pressures of the draped magnetic field lines require no more than 10-20min. Consequently, for typical ecliptic IMF orientations and strengths, the magnetotail cross section is oblate, while the bow shock is prolate. Key Points An ecliptic IMF causes prolate bow shock but oblate magnetotail cross sections The oblate lunar magnetotail cross sections include broad slow-mode fans Lunar magnetotail and bow shock cross sections respond rapidly to IMF variations C1 [Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NSWCCD, West Bethesda, MA USA. RP Sibeck, DG (reprint author), NASA, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20771 USA. EM david.g.sibeck@nasa.gov FU NASA's THEMIS project FX Research at GSFC was funded by NASA's THEMIS project. We would like to thank M. Kuznetsova for suggesting many of the topics in this paper and for her advice on the techniques used for the study, C. Kuang for performing the initial survey of the simulation results, and T. Gombosi for providing very helpful comments on the manuscript. Comments from both referees improved this paper. Simulation results have been provided by the Community Coordinated Modeling Center (CCMC) at Goddard Space Flight Center through their public Runs on Request system (http://ccmc.gsfc.nasa.gov). The CCMC is a multiagency partnership between NASA, AFMC, AFOSR, AFRL, AFWA, NOAA, NSF, and ONR. In particular, we have studied the runs "Claire_Kuang_071X11_X and David_Sibeck_013_X". The BATS-R-US Model was developed by the CSEM group at the University of Michigan. NR 49 TC 7 Z9 8 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD FEB PY 2014 VL 119 IS 2 BP 1028 EP 1043 DI 10.1002/2013JA019471 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AD2CP UT WOS:000333041000027 ER PT J AU Wang, X Malaspina, DM Ergun, RE Horanyi, M AF Wang, X. Malaspina, D. M. Ergun, R. E. Horanyi, M. TI Photoelectron- mediated spacecraft potential fluctuations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE spacecraft potential fluctuations; photoelectrons; electric field; chorus waves; magnetosphere; plasma density ID SURFACES AB Electric field fluctuations such as those due to plasma waves in Earth's magnetosphere may modulate photoelectrons emitted from spacecraft surface, causing fluctuations in spacecraft potential. We experimentally investigate such photoelectron-mediated spacecraft potential fluctuations. The photoelectric charge of a spacecraft model is found to increase with increasing applied electric field as more photoelectrons escape the spacecraft model surface and dissipates with a decrease in the electric field through collection of ambient plasma electrons. When the applied electric field is driven to oscillate at a frequency lower than the response frequency of the spacecraft model, the surface potential follows the electric field oscillations. The spacecraft model maintains an approximately constant potential if the electric field oscillations are driven at a much higher frequency. When a high-frequency electric field modulated by a low-frequency envelope is applied, rectified oscillations in the potential of the spacecraft model are observed. Our experimental results indicate that photoelectron-mediated wave rectifications must be taken into account when spacecraft potential fluctuations are used to infer plasma density structures. C1 [Wang, X.; Malaspina, D. M.; Ergun, R. E.; Horanyi, M.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Wang, X.; Horanyi, M.] NASA, SSERVIs Inst Modeling Plasma Atmospheres & Cosm D, Boulder, CO USA. RP Wang, X (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA. EM xu.wang@colorado.edu FU NASA's Van Allen Probes program [NAS5-01072]; NASA/SSERVI's Institute for Modeling Plasma, Atmospheres and Cosmic Dust (IMPACT) FX This work was supported by the NASA's Van Allen Probes program (award NAS5-01072) and by the NASA/SSERVI's Institute for Modeling Plasma, Atmospheres and Cosmic Dust (IMPACT). The authors thank Scott Robertson for helpful discussions. NR 18 TC 2 Z9 2 U1 3 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD FEB PY 2014 VL 119 IS 2 BP 1094 EP 1101 DI 10.1002/2013JA019502 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AD2CP UT WOS:000333041000031 ER PT J AU Huang, CS Le, G de La Beaujardiere, O Roddy, PA Hunton, DE Pfaff, RF Hairston, MR AF Huang, Chao-Song Le, G. de La Beaujardiere, O. Roddy, P. A. Hunton, D. E. Pfaff, R. F. Hairston, M. R. TI Relationship between plasma bubbles and density enhancements: Observations and interpretation SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Equatorial ionosphere; Plasma bubbles; Plasma enhancements; Plasma blobs ID EQUATORIAL-SPREAD-F; LOW LATITUDE IONOSPHERE; NONLINEAR EVOLUTION; HINOTORI SATELLITE; IMPEDANCE PROBE; IRREGULARITIES; BOARD AB Plasma bubbles are regions of depleted plasma density in the nighttime equatorial ionosphere. Plasma enhancements, also referred as plasma blobs, are regions where the plasma density is increased. It has not been well understood whether and how plasma enhancements are related to plasma bubbles. In this paper, we present the observations of plasma bubbles and enhancements by the Communication/Navigation Outage Forecasting System (C/NOFS) satellite during 2008 and 2009. In some cases, C/NOFS first detected plasma bubbles near the magnetic equator and then plasma enhancements at the same longitudes but at higher latitudes during subsequent orbits. In other cases, C/NOFS first detected plasma enhancements at off-equatorial locations and then plasma bubbles near the magnetic equator at the same longitudes. It is also found that plasma enhancements existed just above plasma depletions. We propose a unified scenario to describe the evolution of plasma bubbles and the formation of plasma enhancements. In the proposed scenario, plasma enhancements can occur at different latitudes and altitudes during the early, intermediate, and late stages of the bubble evolution. This scenario provides a reasonable explanation of the observations. Key Points New observations of plasma bubbles and enhancements are reported Relationship between plasma bubbles and enhancements are identified Physical mechanism for associated bubbles and enhancements is proposed C1 [Huang, Chao-Song; de La Beaujardiere, O.; Roddy, P. A.; Hunton, D. E.] Air Force Res Lab, Kirtland AFB, NM 87117 USA. [Le, G.; Pfaff, R. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hairston, M. R.] Univ Texas Dallas, Hanson Ctr Space Sci, Dallas, TX 75230 USA. RP Huang, CS (reprint author), Air Force Res Lab, Kirtland AFB, NM 87117 USA. EM chaosong.huang@kirtland.af.mil RI Le, Guan/C-9524-2012; OI Le, Guan/0000-0002-9504-5214; Hairston, Marc/0000-0003-4524-4837 FU Air Force Research Laboratory; SMC Defense Weather Systems Directorate; Department of Defense Space Test Program; National Aeronautics and Space Administration; Naval Research Laboratory; Aerospace Corporation FX The C/NOFS mission is supported by the Air Force Research Laboratory, the SMC Defense Weather Systems Directorate, the Department of Defense Space Test Program, the National Aeronautics and Space Administration, the Naval Research Laboratory, and The Aerospace Corporation. NR 31 TC 7 Z9 7 U1 2 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD FEB PY 2014 VL 119 IS 2 BP 1325 EP 1336 DI 10.1002/2013JA019579 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AD2CP UT WOS:000333041000047 ER PT J AU Soranno, PA Schimel, DS AF Soranno, Patricia A. Schimel, David S. TI Macrosystems ecology: big data, big ecology SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT LA English DT Editorial Material C1 [Soranno, Patricia A.] Michigan State Univ, Dept Fisheries & Wildlife, E Lansing, MI 48824 USA. [Schimel, David S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Soranno, PA (reprint author), Michigan State Univ, Dept Fisheries & Wildlife, E Lansing, MI 48824 USA. OI Soranno, Patricia/0000-0003-1668-9271 NR 1 TC 19 Z9 19 U1 9 U2 76 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1540-9295 EI 1540-9309 J9 FRONT ECOL ENVIRON JI Front. Ecol. Environ. PD FEB PY 2014 VL 12 IS 1 BP 3 EP 3 DI 10.1890/1540-9295-12.1.3 PG 1 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA AG4DX UT WOS:000335370600001 ER PT J AU Seidel, DJ Feingold, G Jacobson, AR Loeb, N AF Seidel, Dian J. Feingold, Graham Jacobson, Andrew R. Loeb, Norman TI Detection limits of albedo changes induced by climate engineering SO NATURE CLIMATE CHANGE LA English DT Article ID RADIATION BUDGET; ATMOSPHERE; TOP; DYNAMICS AB A key question surrounding proposals for climate engineering by increasing Earth's reflection of sunlight is the feasibility of detecting engineered albedo increases from short-duration experiments or prolonged implementation of solar-radiation management. We show that satellite observations permit detection of large increases, but interannual variability overwhelms the maximum conceivable albedo increases for some schemes. Detection of an abrupt global average albedo increase <0.002 (comparable to a similar to 0.7 W m(-2) reduction in radiative forcing) would be unlikely within a year, given a five-year prior record. A three-month experiment in the equatorial zone (5 degrees N-5 degrees S), a potential target for stratospheric aerosol injection, would need to cause an similar to 0.03 albedo increase, three times larger than that due to the Mount Pinatubo eruption, to be detected. Detection limits for three-month experiments in 1 degrees (latitude and longitude) regions of the subtropical Pacific, possible targets for cloud brightening, are similar to 0.2, which is larger than might be expected from some model simulations. C1 [Seidel, Dian J.] NOAA, Air Resources Lab, R ARL, NCWCP, College Pk, MD 20740 USA. [Feingold, Graham] NOAA, Earth Syst Res Lab, Chem Sci Div R CSD2, Boulder, CO 80305 USA. [Jacobson, Andrew R.] NOAA, Air Resources Lab, Boulder, CO 80305 USA. [Jacobson, Andrew R.] Univ Colorado, Global Monitoring Div, Boulder, CO 80305 USA. [Loeb, Norman] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Seidel, DJ (reprint author), NOAA, Air Resources Lab, R ARL, NCWCP, Room 4251,5830 Univ Res Court, College Pk, MD 20740 USA. EM dian.seidel@noaa.gov RI Feingold, Graham/B-6152-2009; Manager, CSD Publications/B-2789-2015 NR 24 TC 6 Z9 6 U1 1 U2 21 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1758-678X EI 1758-6798 J9 NAT CLIM CHANGE JI Nat. Clim. Chang. PD FEB PY 2014 VL 4 IS 2 BP 93 EP 98 DI 10.1038/NCLIMATE2076 PG 6 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AE0PD UT WOS:000333667300011 ER PT J AU Bockelee-Morvan, D Biver, N Crovisier, J Lis, DC Hartogh, P Moreno, R de Val-Borro, M Blake, GA Szutowicz, S Boissier, J Cernicharo, J Charnley, SB Combi, M Cordiner, MA de Graauw, T Encrenaz, P Jarchow, C Kidger, M Kuppers, M Milam, SN Muller, HSP Phillips, TG Rengel, M AF Bockelee-Morvan, D. Biver, N. Crovisier, J. Lis, D. C. Hartogh, P. Moreno, R. de Val-Borro, M. Blake, G. A. Szutowicz, S. Boissier, J. Cernicharo, J. Charnley, S. B. Combi, M. Cordiner, M. A. de Graauw, T. Encrenaz, P. Jarchow, C. Kidger, M. Kueppers, M. Milam, S. N. Mueller, H. S. P. Phillips, T. G. Rengel, M. TI Searches for HCl and HF in comets 103P/Hartley 2 and C/2009 P1 (Garradd) with the Herschel Space Observatory SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE comets: general; submillimeter: planetary systems; comets: individual: C/2009P1 (Garradd); comets: individual: 103P/Hartley 2 ID O1 HALE-BOPP; HYDROGEN-CHLORIDE; CHEMICAL-COMPOSITION; HYPERFINE-STRUCTURE; RADIO TELESCOPES; SUBMILLIMETER; WATER; EPOXI; ABUNDANCE; SPECTRA AB Context. Hydrogen chloride (HCl) and hydrogen fluoride (HE) are expected to be the main reservoirs of fluorine and chlorine over a wide range of conditions, wherever hydrogen is predominantly molecular. They are found to be strongly depleted in dense molecular clouds, suggesting freeze-out onto grains in such cold environments. We can then expect that HCl and HF were also the major carriers Cl of and F in the gas and icy phases of the outer solar nebula, and were incorporated into comets. Aims. We aimed to measure the HCl and 110 abundances in cometary ices as they can provide insights on the halogen chemistry in the early solar nebula. Methods. We searched for the J(1-0) lines of HCl and HF at 626 and 1232 GHz, respectively, using the Heterodyne Instrument for the Far-Infrared (HIFI) onboard the Herschel Space Observatory. HCl was searched for in comets 103P/Hartley 2 and C/2009 PI (Garradd), whereas observations of HF were conducted in comet C/2009 P1 (Garradd). In addition, observations of H2O and (H2O)-O-18 lines were performed in C/2009 PI (Garradd) to measure the 1420 production rate at the time of the HCl and HF observations. Three lines of CH3OH were serendipitously observed in the HCl receiver setting. Results. HCl is not detected, whereas a marginal (3.6-sigma) detection of HF is obtained. The upper limits for the HC1 abundance relative to water are 0.0114 and 0.022%, for comet 103P/Hartley 2 and C/2009 P1 (Garradd), respectively, showing that HC1 is depleted with respect to the solar Cl/O abundance by a factor more than 6(-3)(+6)., in 103P/Hartley 2, where the error is related to the uncertainty in the chlorine solar abundance. The marginal HF detection obtained in C/2009 P1 (Garradd) corresponds to an 110 abundance relative to water of (1.8 +/- 0.5) x 10(-4), which is approximately consistent with a solar photospheric F/O abundance. The inferred water production rate in comet C/2009 P1 (Garradd) is (1.1 +/- 0.3)x 10(29) s(-1) and (0.75 +/- 0.05)x 10(29) s(-1) on 17 and 23 February 2012, respectively. CH3OH abundances relative to water are 2.7 +/- 0.3% and 3.4 +/- 0.6%, for comets 103P/Hartley 2 and C/2009 P1 (Garradd), respectively. Conclusions. The observed depletion of HCl suggests that HCl was not the main reservoir of chlorine in the regions of the solar nebula where these comets formed. HF was possibly the main fluorine compound in the gas phase of the outer solar nebula. However, this needs to be confirmed by future measurements. C1 [Bockelee-Morvan, D.; Biver, N.; Crovisier, J.; Moreno, R.] UPMC, Univ Paris Diderot, CNRS, LESIA,Observ Paris, F-92195 Meudon, France. [Lis, D. C.; Blake, G. A.; Phillips, T. G.] CALTECH, Pasadena, CA 91125 USA. [Hartogh, P.; Rengel, M.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [de Val-Borro, M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Szutowicz, S.] Polish Acad Sci, Space Res Ctr, PL-00716 Warsaw, Poland. [Boissier, J.] Domaine Univ, Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Cernicharo, J.] CSIC, INTA, CAB, Dept Astrophys, Madrid 28850, Spain. [Charnley, S. B.; Cordiner, M. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. [Combi, M.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [de Graauw, T.] ALMA Observ, Santiago 7630000, Chile. [Encrenaz, P.] UPMC, CNRS, LERMA, Observ Paris, F-75014 Paris, France. [Kidger, M.; Kueppers, M.] ESAC, European Space Astron, Villanueva De Le Canada 28691, Spain. [Mueller, H. S. P.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. RP Bockelee-Morvan, D (reprint author), UPMC, Univ Paris Diderot, CNRS, LESIA,Observ Paris, 5 Pl Jules Janssen, F-92195 Meudon, France. EM dominique.bockelee@obspm.fr RI Milam, Stefanie/D-1092-2012; Combi, Michael/J-1697-2012 OI Milam, Stefanie/0000-0001-7694-4129; Combi, Michael/0000-0002-9805-0078 FU NASA [NNX12AH91H]; NSF [AST-1108686]; polish MNiSW [181/N-HSO/2008/0] FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States (NASA) under the leadership of SRON, Netherlands Institute for Space Research, Groningen, The Netherlands, and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U.Waterloo; France: CESR, LAB, LERMA, TRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON. TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomic Nacional (IGN), Centro de Astrobiologia (CSIC-INTA); Sweden: Chalmers University of Technology - MC2, RSS & GARD - Onsala Space Observatory, Swedish National Space Board, Stockholm University Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. M.d.V.B. acknowledges partial support from grants NSF AST-1108686 and NASA NNX12AH91H. S.S. was supported by polish MNiSW funds (181/N-HSO/2008/0). NR 72 TC 9 Z9 9 U1 0 U2 11 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2014 VL 562 AR A5 DI 10.1051/0004-6361/201322939 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC0CG UT WOS:000332161800135 ER PT J AU Bonnefoy, M Currie, T Marleau, GD Schlieder, JE Wisniewski, J Carson, J Covey, KR Henning, T Biller, B Hinz, P Klahr, H Boyer, ANM Zimmerman, N Janson, M McElwain, M Mordasini, C Skemer, A Bailey, V Defrere, D Thalmann, C Skrutskie, M Allard, F Homeier, D Tamura, M Feldt, M Cumming, A Grady, C Brandner, W Helling, C Witte, S Hauschildt, P Kandori, R Kuzuhara, M Fukagawa, M Kwon, J Kudo, T Hashimoto, J Kusakabe, N Abe, L Brandt, T Egner, S Guyon, O Hayano, Y Hayashi, M Hayashi, S Hodapp, K Ishii, M Iye, M Knapp, G Matsuo, T Mede, K Miyama, M Morino, JI Moro-Martin, A Nishimura, T Pyo, T Serabyn, E Suenaga, T Suto, H Suzuki, R Takahashi Takami, M Takato, N Terada, H Tomono, D Turner, E Watanabe, M Yamada, T Takami, H Usuda, T AF Bonnefoy, M. Currie, T. Marleau, G. -D. Schlieder, J. E. Wisniewski, J. Carson, J. Covey, K. R. Henning, T. Biller, B. Hinz, P. Klahr, H. Boyer, A. N. Marsh Zimmerman, N. Janson, M. McElwain, M. Mordasini, C. Skemer, A. Bailey, V. Defrere, D. Thalmann, C. Skrutskie, M. Allard, F. Homeier, D. Tamura, M. Feldt, M. Cumming, A. Grady, C. Brandner, W. Helling, C. Witte, S. Hauschildt, P. Kandori, R. Kuzuhara, M. Fukagawa, M. Kwon, J. Kudo, T. Hashimoto, J. Kusakabe, N. Abe, L. Brandt, T. Egner, S. Guyon, O. Hayano, Y. Hayashi, M. Hayashi, S. Hodapp, K. Ishii, M. Iye, M. Knapp, G. Matsuo, T. Mede, K. Miyama, M. Morino, J. -I. Moro-Martin, A. Nishimura, T. Pyo, T. Serabyn, E. Suenaga, T. Suto, H. Suzuki, R. Takahashi Takami, M. Takato, N. Terada, H. Tomono, D. Turner, E. Watanabe, M. Yamada, T. Takami, H. Usuda, T. TI Characterization of the gaseous companion kappa Andromedae b New Keck and LBTI high-contrast observations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE instrumentation: adaptive optics; techniques: photometric; planetary systems; stars: individual: kappa Andromedae ID LOW-MASS STARS; EXTRASOLAR GIANT PLANETS; BETA-PICTORIS B; FINDING CAMPAIGN DISCOVERY; DIRECT-IMAGING DISCOVERY; STELLAR KINEMATIC GROUPS; ADAPTIVE-OPTICS SYSTEM; DIRECTLY IMAGED PLANET; BROWN DWARF COMPANION; YOUNG SOLAR ANALOG AB Context. We previously reported the direct detection of a low-mass companion at a projected separation of 55 +/- 2 AU around the B9-type star kappa Andromedae. The properties of the system (mass ratio, separation) make it a benchmark for understanding the formation and evolution of gas giant planets and brown dwarfs on wide orbits. Aims. We present new angular differential imaging (ADI) images of the system at 2.146 (K-s), 3.776 (L'), 4.052 (NB_4.05), and 4.78 mu m (M') obtained with Keck/NIRC2 and LBTI/LMIRCam, as well as more accurate near-infrared photometry of the star with the MIMIR instrument. We aim to determine the near-infrared spectral energy distribution of the companion and use it to characterize the object. Methods. We used analysis methods adapted to ADI to extract the companion flux. We compared the photometry of the object to reference young, and old objects and to a set of seven PHOENIX-based atmospheric models of cool objects accounting for the formation of dust. We used evolutionary models to derive mass estimates considering a wide range of plausible initial conditions. Finally, we used dedicated formation models to discuss the possible origin of the companion. Results. We derive a more accurate J = 15.86 +/- 0.21, H = 14.95 +/- 0.13, K-s = 14.32 +/- 0.09 mag for kappa And b. We detect the companion in all our high-contrast observations. We confirm previous contrasts obtained at K-s and L' band. We derive NB_4.05 = 13.0 +/- 0.2, and M' = 13.3 +/- 0.3 mag and estimate log(10)(L/L-circle dot) = -3.76 +/- 0.06. Atmospheric models yield T-eff = 1900(-200)(+100) K. They do not set any constraint on the surface gravity. "Hot-start" evolutionary models predict masses of 14(-2)(+25) M-Jup based on the luminosity and temperature estimates, and when considering a conservative age range for the system (30(-10)(+120) Myr), "warm-start" evolutionary tracks constrain the mass to M >= 10 M-Jup. Conclusions. The mass of kappa Andromedae b mostly falls in the brown-dwarf regime, owing to remaining uncertainties in age and in mass-luminosity models. According to the formation models, disk instability in a primordial disk may account for the position and a wide range of plausible masses of kappa And b. C1 [Bonnefoy, M.; Marleau, G. -D.; Schlieder, J. E.; Carson, J.; Henning, T.; Biller, B.; Klahr, H.; Zimmerman, N.; Mordasini, C.; Thalmann, C.; Feldt, M.; Brandner, W.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Currie, T.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Wisniewski, J.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Carson, J.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA. [Covey, K. R.] Lowell Observ, Flagstaff, AZ 86001 USA. [Hinz, P.; Skemer, A.; Bailey, V.; Defrere, D.] Univ Arizona, Dept Astron, Steward Observ, Tucson, AZ 85721 USA. [Boyer, A. N. Marsh] Lehigh Univ, Dept Phys, Coll Art & Sci, Bethlehem, PA 18015 USA. [Janson, M.; Brandt, T.; Knapp, G.; Turner, E.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [McElwain, M.; Grady, C.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Thalmann, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Skrutskie, M.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Allard, F.; Homeier, D.] Univ Lyon, CNRS, CRAL, Ecole Normale Super Lyon,UMR 5574, F-69364 Lyon 07, France. [Tamura, M.; Kandori, R.; Kuzuhara, M.; Kwon, J.; Hashimoto, J.; Kusakabe, N.; Hayashi, M.; Iye, M.; Morino, J. -I.; Suto, H.; Suzuki, R.; Takami, H.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Tamura, M.; Mede, K.; Takahashi] Grad Sch Sci, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan. [Cumming, A.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Helling, C.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Witte, S.; Hauschildt, P.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Kuzuhara, M.; Hodapp, K.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [Fukagawa, M.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. [Kudo, T.; Egner, S.; Guyon, O.; Hayano, Y.; Hayashi, S.; Ishii, M.; Nishimura, T.; Pyo, T.; Takato, N.; Terada, H.; Tomono, D.; Usuda, T.] Subaru Telescope, Hilo, HI 96720 USA. [Abe, L.] Univ Nice Sophia Antipolis, CNRS, Lab Lagrange UMR 7293, Observ Cote Azur, F-06108 Nice 2, France. [Matsuo, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Miyama, M.] Hiroshima Univ, Higashihiroshima, Hiroshima 7398511, Japan. [Moro-Martin, A.] Inst Nacl Tecn Aeroespacial, Dept Astrofis, CAB INTA CSIC, Madrid 28850, Spain. [Serabyn, E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Suenaga, T.] Grad Univ Adv Studies Sokendai, Dept Astron Sci, Mitaka, Tokyo 1818858, Japan. [Takami, M.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Turner, E.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan. [Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan. [Yamada, T.] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. RP Bonnefoy, M (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM bonnefoy@mpia-hd.mpg.de RI WATANABE, Masahiko/A-4055-2012; Watanabe, Makoto/E-3667-2016; OI Watanabe, Makoto/0000-0002-3656-4081; Zimmerman, Neil/0000-0001-5484-1516 FU NASA; NSF [1009314, 1009203, 1008440]; W.M. Keck Foundation; NASA Origins of Solar Systems Program [NNX13AJ17G]; JSPS [PD: 24 110]; French "Agence Nationale de la Recherche" [ANR10-BLANC0504-01]; "Programme National de Physique Stellaire" (PNPS) of CNRS (INSU); European Research Council under the European Community [247060]; Lyon Institute of Origins [ANR-10-LABX-66] FX We are very grateful to our anonymous referee for reviewing this article. We thank the LMIRCam instrument team for operating the instrument during our observations. The authors recognize and acknowledge the significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We thank Ginny McSwain for her complementary analysis of the high-resolution spectrum of kappa And A. We thank Anne-Marie Lagrange for checking for past SOPHIE observations of kappa And A, Julien Rameau for providing the detection limit on HR7329B, Eric Nielsen and Michael Liu for discussion about their bayesian age-dating tool. We also thank Johan Olofsson for checking the spectral energy distribution of the star. This research was conducted in part using the MIMIR instrument, jointly developed at Boston University and Lowell Observatory and supported by NASA, NSF, and the W.M. Keck Foundation. J. Carson, J. Wisniewski, and C. Grady were supported by NSF awards 1009314, 1009203, and 1008440. Andrew Skemer was supported by the NASA Origins of Solar Systems Program, grant NNX13AJ17G. J. Kwon is supported by the JSPS Research Fellowships for Young Scientists (PD: 24 110). The research leading to these results has received funding from the French "Agence Nationale de la Recherche" through project grant ANR10-BLANC0504-01, the "Programme National de Physique Stellaire" (PNPS) of CNRS (INSU), and the European Research Council under the European Community's Seventh Framework Programs (FP7/2007-2013 Grant Agreement no. 247060). It was also conducted within the Lyon Institute of Origins under grant ANR-10-LABX-66. NR 223 TC 23 Z9 23 U1 0 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2014 VL 562 AR A111 DI 10.1051/0004-6361/201322119 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC0CG UT WOS:000332161800042 ER PT J AU Cavalie, T Moreno, R Lellouch, E Hartogh, P Venot, O Orton, GS Jarchow, C Encrenaz, T Selsis, F Hersant, F Fletcher, LN AF Cavalie, T. Moreno, R. Lellouch, E. Hartogh, P. Venot, O. Orton, G. S. Jarchow, C. Encrenaz, T. Selsis, F. Hersant, F. Fletcher, L. N. TI The first submillimeter observation of CO in the stratosphere of Uranus SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planets and satellites: individual: Uranus; planets and satellites: atmospheres; submillimeter: planetary systems ID ROTOTRANSLATIONAL ABSORPTION-SPECTRA; MILLIMETER-WAVE OBSERVATIONS; HERSCHEL-PACS OBSERVATIONS; NEPTUNES CARBON-MONOXIDE; ODIN SPACE TELESCOPE; WATER-VAPOR; TITANS ATMOSPHERE; COMET SHOEMAKER-LEVY-9; JUPITERS STRATOSPHERE; INFRARED-SPECTROSCOPY AB Context. Carbon monoxide (CO) has been detected in all giant planets and its origin is both internal and external in Jupiter and Neptune. Despite its first detection in Uranus a decade ago, the magnitude of its internal and external sources remains unconstrained. Aims. We targeted CO lines in Uranus in the submillimeter range to constrain its origin. Methods. We recorded the disk-averaged spectrum of Uranus with very high spectral resolution at the frequencies of CO rotational lines in the submillimeter range in 2011-2012. We used empirical and diffusion models of the atmosphere of Uranus to constrain the origin of CO. We also used a thermochemical model of its troposphere to derive an upper limit on the oxygen-to-hydrogen (O/H) ratio in the deep atmosphere of Uranus. Results. We have detected the CO(8-7) rotational line for the first time with Herschel-HIFI. Both empirical and diffusion models results show that CO has an external origin. An empirical profile in which CO is constant above the 100 mbar level with a mole fraction of 7.1-9.0 x 10(-9), depending on the adopted stratospheric thermal structure, reproduces the data. Sporadic and steady source models cannot be differentiated with our data. Taking the internal source model upper limit of a mole fraction of 2.1 x 10(-9) we find, based on our thermochemical computations, that the deep O/H ratio of Uranus is less than 500 times solar. Conclusions. Our work shows that the average mole fraction of CO decreases from the stratosphere to the troposphere and thus strongly advocates for an external source of CO in Uranus. Photochemical modeling of oxygen species in the atmosphere of Uranus and more sensitive observations are needed to reveal the nature of the external source. C1 [Cavalie, T.; Selsis, F.; Hersant, F.] Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France. [Cavalie, T.; Selsis, F.; Hersant, F.] CNRS, LAB, UMR 5804, F-33270 Floirac, France. [Moreno, R.; Lellouch, E.; Encrenaz, T.] Univ Paris Diderot, Univ Paris 06, CNRS, LESIA Observ Paris, Meudon, France. [Hartogh, P.; Jarchow, C.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Venot, O.] Katholieke Univ Leuven, Inst Sterrenkunde, Louvain, Belgium. [Orton, G. S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Fletcher, L. N.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. RP Cavalie, T (reprint author), Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France. EM cavalie@obs.u-bordeaux1.fr RI Fletcher, Leigh/D-6093-2011 OI Fletcher, Leigh/0000-0001-5834-9588 FU Centre National d'Etudes Spatiales (CNES); European Research Council [209622: E3ARTHs]; KU Leuven IDO project [IDO/10/2013]; FWO Post-doctoral Fellowship programme; National Aeronautics and Space Administration; Royal Society Research Fellowship at the University of Oxford FX T. Cavalie acknowledges funding from the Centre National d'Etudes Spatiales (CNES). T. Cavalie and F. Selsis acknowledge support from the European Research Council (Starting Grant 209622: E3ARTHs). O. Venot acknowledges support from the KU Leuven IDO project IDO/10/2013 and from the FWO Post-doctoral Fellowship programme. G. Orton acknowledges funding from the National Aeronautics and Space Administration to the Jet Propulsion Laboratory, California Institute of Technology. L. N. Fletcher was supported by a Royal Society Research Fellowship at the University of Oxford. The authors thank M. Hofstadter for his constructive review. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada, and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands, and with major contributions from Germany, France, and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiolog a (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. The James Clerk Maxwell Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK, the National Research Council of Canada, and the Netherlands Organisation for Scientific Research. NR 72 TC 15 Z9 15 U1 1 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2014 VL 562 AR A33 DI 10.1051/0004-6361/201322297 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC0CG UT WOS:000332161800053 ER PT J AU Ceccobello, C Farinelli, R Titarchuk, L AF Ceccobello, C. Farinelli, R. Titarchuk, L. TI Comptonization in ultra-strong magnetic fields: numerical solution to the radiative transfer problem SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE acceleration of particles; magnetic fields; radiative transfer; methods: numerical; X-rays: general; stars: magnetars ID RESONANT CYCLOTRON SCATTERING; RAY SPECTRAL FORMATION; CONVERGING FLUID-FLOW; SOFT GAMMA-REPEATERS; INTRINSIC SIGNATURE; VACUUM POLARIZATION; TRANSFER EQUATION; NEUTRON-STAR; BLACK-HOLES; ACCRETION AB Context. We consider the radiative transfer problem in a plane-parallel slab of thermal electrons in the presence of an ultra-strong magnetic field (B greater than or similar to B-c approximate to 4 : 4 x 10(13) G). Under these conditions, the magnetic field behaves like a birefringent medium for the propagating photons, and the electromagnetic radiation is split into two polarization modes, ordinary and extraordinary, that have different cross-sections. When the optical depth of the slab is large, the ordinary-mode photons are strongly Comptonized and the photon field is dominated by an isotropic component. Aims. The radiative transfer problem in strong magnetic fields presents many mathematical issues and analytical or numerical solutions can be obtained only under some given approximations. We investigate this problem both from the analytical and numerical point of view, provide a test of the previous analytical estimates, and extend these results with numerical techniques. Methods. We consider here the case of low temperature black-body photons propagating in a sub-relativistic temperature plasma, which allows us to deal with a semi-Fokker-Planck approximation of the radiative transfer equation. The problem can then be treated with the variable separation method, and we use a numerical technique to find solutions to the eigenvalue problem in the case of a singular kernel of the space operator. The singularity of the space kernel is the result of the strong angular dependence of the electron cross-section in the presence of a strong magnetic field. Results. We provide the numerical solution obtained for eigenvalues and eigenfunctions of the space operator, and the emerging Comptonization spectrum of the ordinary-mode photons for any eigenvalue of the space equation and for energies significantly lesser than the cyclotron energy, which is on the order of MeV for the intensity of the magnetic field here considered. Conclusions. We derived the specific intensity of the ordinary photons, under the approximation of large angle and large optical depth. These assumptions allow the equation to be treated using a diffusion-like approximation. C1 [Ceccobello, C.; Farinelli, R.; Titarchuk, L.] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy. [Ceccobello, C.] INFN, Sez Ferrara, I-44122 Ferrara, Italy. [Farinelli, R.] Univ Geneva, ISDC Data Ctr Astrophys, CH-1290 Versoix, Switzerland. [Titarchuk, L.] NASA GSFC, Greenbelt, MD 20771 USA. RP Ceccobello, C (reprint author), Univ Ferrara, Dipartimento Fis & Sci Terra, Via Saragat 1, I-44122 Ferrara, Italy. EM chiara.ceccobello@gmail.com NR 41 TC 0 Z9 0 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2014 VL 562 AR A99 DI 10.1051/0004-6361/201322668 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC0CG UT WOS:000332161800102 ER PT J AU Cuylle, SH Allamandola, LJ Linnartz, H AF Cuylle, Steven H. Allamandola, Louis J. Linnartz, Harold TI Photochemistry of PAHs in cosmic water ice The effect of concentration on UV-VIS spectroscopy and ionization efficiency SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; molecular processes; methods: laboratory: solid state; ISM: molecules ID POLYCYCLIC AROMATIC-HYDROCARBONS; MIDINFRARED LABORATORY SPECTRA; CHARGE-TRANSFER COMPLEXES; YOUNG STELLAR OBJECTS; INTERSTELLAR ICE; ASTROPHYSICAL ICES; INFRARED-SPECTROSCOPY; PROTOPLANETARY DISKS; EXCESS ELECTRONS; CLUSTER ANIONS AB Context. Observations and models show that polycyclic aromatic hydrocarbons (PAL ls) are ubiquitous in the interstellar medium. Like other molecules in dense clouds. PAEls accrete onto interstellar dust grains, where they are embedded in an ice matrix dominated by water. In the laboratory, mixed molecular ices (not containing PAHs) have been extensively studied using Fourier transform infrared absorption spectroscopy. Experiments including PAHs in ices have started, however, the concentrations used are typically much higher than the concentrations expected for interstellar ices. Optical spectroscopy oilers a sensitive alternative. Aims. We report an experimental study of the effect PAH concentration has on the electronic spectra and the vacuum UV (VILV) driven processes of PAHs in water-rich ices. The goal is to apply the outcome to cosmic ices. Methods. Optical spectroscopic studies allow us to obtain in-situ and quasi real-time electronic solid state spectra of two prototypical PAlls (pyrene and coronene) embedded in water ice under WV photoprocessing. The study is carried out on PAH:H2O concentrations in the range of 1:30 000 to pure PAH, covering the temperature range from 12 to 125 K. Results. PAH concentration strongly influences the efficiency of PAH cation formation. At low concentrations, ionization efficiencies are over 60% dropping to about 15% at 1:1000. Increasing the PAH concentration reveals spectral broadening in neutral and cation PAH spectra attributed to PAH clustering inside the ice. At the PAII concentrations expected for interstellar ices, some I() to 20% may be present as cations. The presence of PAlls in neutral and ion form will add distinctive absorption bands to cosmic ice optical spectra and this may serve as a tool to determine PAH concentrations. C1 [Cuylle, Steven H.; Linnartz, Harold] Leiden Univ, Sackler Lab Astrophys, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Allamandola, Louis J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. RP Cuylle, SH (reprint author), Leiden Univ, Sackler Lab Astrophys, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM Linnartz@strw.leidenuniv.nl FU Netherlands School for Astronomy; NWO-VICI; Dutch Organisation for Science; European Community [238258]; NASA's Laboratory Astrophysics and Astrobiology programs; NASA's Laboratory Astrophysics "Carbon in the Galaxy" Consortium; NASA Ames Research Center's Exchange program FX This research is financially supported by the Netherlands School for Astronomy, NWO-VICI, the Dutch Organisation for Science, and the European Communitys 7th Framework Programme (FP7/2007-2013) under grant agreement n.238258. L.J.A. gratefully acknowledges support from NASA's Laboratory Astrophysics and Astrobiology programs, NASA's Laboratory Astrophysics "Carbon in the Galaxy" Consortium and NASA Ames Research Center's Exchange program with the Netherlands. NR 68 TC 4 Z9 4 U1 1 U2 22 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2014 VL 562 AR A22 DI 10.1051/0004-6361/201322495 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC0CG UT WOS:000332161800078 ER PT J AU Elliou, J Yu, HF Schmidl, S Greiner, J Gruber, G Oates, S Kobayashi, S Zhang, B Cummings, JR Filgas, R Gehrels, N Grupe, D Kann, DA Klose, S Kruhler, T Guelbenzu, AN Rau, A Rossi, A Siegel, M Schady, P Sudilovsky, V Tanga, M Varela, K AF Elliou, J. Yu, H-F Schmidl, S. Greiner, J. Gruber, G. Oates, S. Kobayashi, S. Zhang, B. Cummings, J. R. Filgas, R. Gehrels, N. Grupe, D. Kann, D. A. Klose, S. Kruhler, T. Guelbenzu, A. Nicuesa Rau, A. Rossi, A. Siegel, M. Schady, P. Sudilovsky, V. Tanga, M. Varela, K. TI Prompt emission of GRB 121217A from gamma-rays to the near-infrared SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray burst: general; gamma-ray burst: individual: GRB 121217A; X-rays: individuals: GRB 121217A ID LIGHT CURVES; AFTERGLOW EMISSION; BURST AFTERGLOWS; OPTICAL-EMISSION; INTERNAL SHOCKS; OPEN QUESTIONS; DATA RELEASE; EARLY-TIME; SWIFT; TELESCOPE AB The mechanism that causes the prompt-emission episode of gamma-ray bursts (GRBs) is still widely debated despite there being thousands of prompt detections. The favoured internal shock model relates this emission to synchrotron radiation. However, it does not always explain the spectral indices of the shape of the spectrum, which is often fit with empirical functions, such as the Band function. Multi-wavelength observations are therefore required to help investigate the possible underlying mechanisms that causes the prompt emission. We present GRB 121217A, for which we were able to observe its near-infrared (NIR) emission during a secondary prompt-emission episode with the Gamma-Ray burst Optical Near-infrared Detector (GROND) in combination with the Swift and Fermi satellites, which cover an energy range of 5 orders of magnitude (10(-3) keV to 100 keV). We determine a photometric redshift of z = 3.1 +/- 0.1 with a line-of-sight with little or no extinction (A(v) similar to 0 mag) utilising the optical/NIR SED. From the afterglow, we determine a bulk Lorentz factor of Gamma(0) similar to 250 and an emission radius of R < 10(18) cm. The prompt-emission broadband spectral energy distribution is well fit with a broken power law with beta(1) = -0.3 +/- 0.1 and beta(2) = 0.6 +/- 0.1 that has a break at E = 6.6 +/- 0.9 keV, which can be interpreted as the maximum injection frequency. Self-absorption by the electron population below energies of E-a < 6 keV suggest a magnetic field strength of B similar to 10(5) G. However, all the best fit models underprcdict the flux observed in the NIR wavelengths, which also only rebrightens by a factor of similar to 2 during the second prompt emission episode, in stark contrast to the X-ray emission, which rebrightens by a factor of similar to 100. This suggests an afterglow component is dominating the emission. We present GRB 121217A, one of the few GRBs that has multi-wavelength observations of the prompt-emission period and shows that it can be understood with a synchrotron radiation model. However, due to the complexity of the GRB's emission, other mechanisms that result in Band-like spectra cannot be ruled out. C1 [Elliou, J.; Yu, H-F; Greiner, J.; Gruber, G.; Kann, D. A.; Rau, A.; Schady, P.; Sudilovsky, V.; Tanga, M.; Varela, K.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Schmidl, S.; Klose, S.; Guelbenzu, A. Nicuesa; Rossi, A.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Oates, S.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Kobayashi, S.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Zhang, B.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. [Cummings, J. R.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Cummings, J. R.] NASA, Ctr Res & Explorat Space Sci & Technol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Filgas, R.] Czech Tech Univ, Inst Expt & Appl Phys, Prague 12800, Czech Republic. [Gehrels, N.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Grupe, D.; Siegel, M.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Kruhler, T.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Kruhler, T.] European So Observ, Santiago 19, Chile. RP Elliou, J (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. EM jonnyelliott@mpe.mpg.de RI Rossi, Andrea/N-4674-2015; OI Rossi, Andrea/0000-0002-8860-6538; Kruehler, Thomas/0000-0002-8682-2384 FU Leibniz-Prize DFG grant [1850/28-1]; DFG cluster of excellence "Origin and Structure of the Universe"; Thuringer Ministerium fur Bildung, Wissenschaft und Kultur u [FKZ 12010-514]; DFG [SA 2001/1-1, K1 766/16-1]; Alexander von Humboldt Foundation of Germany; Thuringer Landessternwarte Tautenburg; PSU by NASA [NAS5-00136]; STFC; NASA [NAS5-00136]; European Commission; Danish National Research Foundation FX We thank the anonymous referee for their constructive comments. We thank A. Beloborodov, Z. Bosnjak, R. Mochkovitch, S. Xiong, and B. B. Zhang for their comments and suggestions. Part of the funding for GROND (both hardware as well as personnel) was generously granted from the Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. We thank Taka Sakamoto and Scott D. Barthelmy for the public BAT data. H.F.Y. acknowledges support by the DFG cluster of excellence "Origin and Structure of the Universe". S.S. acknowledges support by the Thuringer Ministerium fur Bildung, Wissenschaft und Kultur under FKZ 12010-514. P.S. acknowledges support by DFG grant SA 2001/1-1. P.S. and M.T. acknowledge support through the Sofja Kovalevskaja Award from the Alexander von Humboldt Foundation of Germany. S.K.l. and A.G.N. acknowledge support by DFG grant K1 766/16-1. A.R., A.G.N., and A.K. are grateful for travel funding support through MPE. A.R. acknowledges support by the Thuringer Landessternwarte Tautenburg. K.V. acknowledges support by DFG grant SA 2001/2-1. Swift is supported at PSU by NASA grant NAS5-00136. SKo acknowledges support from the STFC. MS is supported by NASA contract NAS5-00136. T.K. acknowledges support by the European Commission under the Marie Curie Intra-European Fellowship Programme in FP7. The Dark Cosmology Centre is funded by the Danish National Research Foundation. NR 77 TC 5 Z9 5 U1 0 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2014 VL 562 AR A100 DI 10.1051/0004-6361/201322600 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC0CG UT WOS:000332161800090 ER PT J AU Jouvel, S Host, O Lahav, O Seitz, S Molino, A Coe, D Postman, M Moustakas, L Benitez, N Rosati, P Balestra, I Grillo, C Bradley, L Fritz, A Kelson, D Koekemoer, AM Lemze, D Medezinski, E Mercurio, A Moustakas, J Nonino, M Scodeggio, M Zheng, W Zitrin, A Bartelmann, M Bouwens, R Broadhurst, T Donahue, M Ford, H Graves, G Infante, L Jimenez-Teja, Y Lazkoz, R Melchior, P Meneghetti, M Merten, J Ogaz, S Umetsu, K AF Jouvel, S. Host, O. Lahav, O. Seitz, S. Molino, A. Coe, D. Postman, M. Moustakas, L. Benitez, N. Rosati, P. Balestra, I. Grillo, C. Bradley, L. Fritz, A. Kelson, D. Koekemoer, A. M. Lemze, D. Medezinski, E. Mercurio, A. Moustakas, J. Nonino, M. Scodeggio, M. Zheng, W. Zitrin, A. Bartelmann, M. Bouwens, R. Broadhurst, T. Donahue, M. Ford, H. Graves, G. Infante, L. Jimenez-Teja, Y. Lazkoz, R. Melchior, P. Meneghetti, M. Merten, J. Ogaz, S. Umetsu, K. TI CLASH: Photometric redshifts with 16 HST bands in galaxy cluster fields SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: general; galaxies: distances and redshifts ID SPECTRAL ENERGY-DISTRIBUTIONS; MASSIVE CLUSTER; MACS J1206.2-0847; DEEP SURVEY; COMPLETE SAMPLE; FAINT GALAXIES; LEGACY SURVEY; RED GALAXIES; HUBBLE; EVOLUTION AB Context. The Cluster Lensing And Supernovae survey with Hubble (CLASH) is a Hubble Space Telescope (HST) Multi-Cycle Treasury programme that observes 25 massive galaxy clusters, 20 of which were X-ray-selected to preferably choose dynamically relaxed clusters, and 5 additional "high magnification" clusters, which were selected based on their optical lensing properties. CLASH aims to study the dark matter distribution of the clusters and find magnified high-redshift galaxies behind them. CLASH observations were carried out in 16 bands from UV to NIR to derive accurate and reliable estimates of photometric redshifts. Aims. We present the CLASH photometric redshifts using 16 HST bands and study the photometric redshift accuracy including a detailed comparison between photometric and spectroscopic redshifts for the strong lensing arcs using the measurements from the cluster MACSJ1206.2-0847. Methods. We used the publicly available Le Phare and BPZ photometric redshift estimation codes on 17 CLASH galaxy clusters for which the full photo-z data processing had been completed at the time of this analysis, and derive an estimate of the CLASH photo-z accuracy. Results. Using Le Phare code for objects with a S/N >= 10, we reach a precision of 3%(1 + z) for the strong lensing arcs, which is reduced to 2.4%(1 + z) after removing outliers. For galaxies in the cluster field, the corresponding values are 4%(1 + z) and 3%(1 + z). Using mock galaxy catalogues, we show that 3%(1 + z) precision is what is expected using the baseline sky substraction algorithm when taking into account extinction from dust, emission lines, and the finite range of SEDs included in the photo-z template library. An improved method for estimating galaxy colours that yields more accurate photometric redshifts will be explored in a forthcoming paper. We study photo-z results for different aperture photometry techniques and find that the SExtractor isophotal photometry works best. We check the robustness of the arcs photo-z results by rederiving the input photometry in the case of MACS1206. We describe and release a photometric redshift catalogue of the MACS1206 cluster we study. Conclusions. Our photo-z codes give similar results for the strong lensing arcs, as well as for galaxies of the cluster field. Results are improved when optimizing the photometric aperture shape that shows an optimal aperture size around 1 '' radius, giving results that are equivalent to isophotal photometry. Tailored photometry of the arcs improves the photo-z results by showing more consistency between the different arcs of the same strong lensing system. C1 [Jouvel, S.] Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain. [Jouvel, S.; Lahav, O.] UCL, London WC1E 6BT, England. [Host, O.; Grillo, C.] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Coe, D.; Postman, M.; Bradley, L.; Koekemoer, A. M.; Ogaz, S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Rosati, P.] ESO, D-85748 Garching, Germany. [Seitz, S.] Univ Munich, Inst Astron & Astrophys, D-81679 Munich, Germany. [Broadhurst, T.; Lazkoz, R.] Univ Basque Country, UPV EHU, Dept Theoret Phys, Bilbao 48080, Spain. [Broadhurst, T.] Basque Fdn Sci, Ikerbasque, Bilbao 48011, Spain. [Molino, A.; Benitez, N.; Jimenez-Teja, Y.] CSIC, IAA, E-18008 Granada, Spain. [Lemze, D.; Medezinski, E.; Zheng, W.; Ford, H.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Bartelmann, M.] Inst Theoret Astrophys, Zentrum Astron, D-29120 Heidelberg, Germany. [Bouwens, R.] Leiden Univ, Leiden Observ, NL-2333 Leiden, Netherlands. [Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Graves, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Infante, L.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 22, Chile. [Infante, L.] Pontificia Univ Catolica Chile, AIUC, Santiago 22, Chile. [Kelson, D.] Carnegie Inst Sci, Carnegie Observ, Pasadena, CA USA. [Melchior, P.] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA. [Meneghetti, M.] Ist Nazl Fis Nucl, INAF, Osservatorio Astron Bologna, Sez Bologna, I-40127 Bologna, Italy. [Moustakas, L.; Merten, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Balestra, I.; Mercurio, A.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Moustakas, J.] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. [Fritz, A.; Scodeggio, M.] Ist Astrofis Spaziale Fis Cosm IASF, INAF, I-20133 Milan, Italy. [Zitrin, A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Balestra, I.; Nonino, M.] Osserv Astron Trieste, INAF, I-40131 Trieste, Italy. RP Jouvel, S (reprint author), Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain. EM jouvel@ice.cat RI Molino Benito, Alberto/F-5298-2014; Lazkoz, Ruth/A-5642-2011; Jimenez-Teja, Yolanda/D-5933-2011; Grillo, Claudio/E-6223-2015; Meneghetti, Massimo/O-8139-2015; OI Koekemoer, Anton/0000-0002-6610-2048; Benitez, Narciso/0000-0002-0403-7455; Lazkoz, Ruth/0000-0001-5536-3130; Grillo, Claudio/0000-0002-5926-7143; Meneghetti, Massimo/0000-0003-1225-7084; Nonino, Mario/0000-0001-6342-9662; Balestra, Italo/0000-0001-9660-894X; Scodeggio, Marco/0000-0002-2282-5850; Umetsu, Keiichi/0000-0002-7196-4822; Moustakas, Leonidas/0000-0003-3030-2360 FU STFC; Royal Society; Leverhulme Senior Research Fellowship; Advanced ERC Grant; Spanish Science Ministry [AYA2009-13936 Consolider-Ingenio CSD2007-00060]; Generalitat de Catalunya [2009SGR1398]; European Commissions Marie Curie Initial Training Network CosmoComp [PITN- GA-2009-238356]; Danish National Research Foundation; Transregional Collaborative Research Centre TRR 33 "The Dark Universe"; DFG cluster of excellence "Origin and Structure of the Universe"; PRIN INAF : "Architecture and Tomography of Galaxy Clusters"; INAF grant; PRIN grant; NASA [HST-HF-51334.01-A]; STScI; Baden Wurttemberg Stiftung; [AYA2006-14056BES-2007-16280] FX S.J. and O.H. acknowledge STFC-supported Post-doctoral Felowships at UCL, O.L. acknowledges a Royal Society Wolfson Research Merit Award, a Leverhulme Senior Research Fellowship and an Advanced ERC Grant. S.J. is supported by the Spanish Science MinistryAYA2009-13936 Consolider-Ingenio CSD2007-00060, project2009SGR1398 from Generalitat de Catalunya and by the European Commissions Marie Curie Initial Training Network CosmoComp (PITN- GA-2009-238356). The Dark Cosmology Centre is funded by the Danish National Research Foundation. S. Seitz acknowledges support from the Transregional Collaborative Research Centre TRR 33 "The Dark Universe" and from the DFG cluster of excellence "Origin and Structure of the Universe". This research is partially supported by PRIN INAF 2010: "Architecture and Tomography of Galaxy Clusters". A. F. acknowledges support from INAF through PRIN 2008 and 2010 grants. Support for A.Z. is provided by NASA through Hubble Fellowship grant #HST-HF-51334.01-A awarded by STScI. Part of this work was also supported by contract research "Internationale Spitzenforschung II/2-6" of the Baden Wurttemberg Stiftung. A. M. acknowledges support from AYA2006-14056BES-2007-16280. NR 59 TC 18 Z9 18 U1 1 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2014 VL 562 AR A86 DI 10.1051/0004-6361/201322419 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC0CG UT WOS:000332161800066 ER PT J AU Lorenzi, V Pinilla-Alonso, N Licandro, J Ore, CMD Emery, JP AF Lorenzi, V. Pinilla-Alonso, N. Licandro, J. Ore, C. M. Dalle Emery, J. P. TI Rotationally resolved spectroscopy of (20000) Varuna in the near-infrared SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Kuiper belt objects: individual: (2000) Varuna; methods: observational; methods: numerical; techniques: spectroscopic; planets and satellites: composition ID TRANS-NEPTUNIAN OBJECTS; KUIPER-BELT OBJECTS; SURFACE-COMPOSITION; OPTICAL-PROPERTIES; ICE; CENTAURS; COLORS; PLUTO AB Context. Models of the escape and retention of volatiles by minor icy objects exclude any presence of volatile ices on the surface of trans-Neptunian objects (TNOs) smaller than similar to 1000 km in diameter at the typical temperature in this region of the solar system, whereas the same models show that water ice is stable on the surface of objects over a wide range of diameters. Collisions and cometary activity have been used to explain the process of surface refreshing of TNOs and Centaurs. These processes can produce surface heterogeneity that can be studied by collecting information at different rotational phases. Aims. The aims of this work are to study the surface composition of (20000) Varuna, a TNO with a diameter 668(-86)(+154) km and to search for indications of rotational variability. Methods. We observed (20000) Varuna during two consecutive nights in January 2011 with the near-infrared camera and spectrometer NICS at the Telescopio Nazionale Galileo, La Palma, Spain. We used the low resolution mode with the AMICI prism to obtain a set of spectra covering the whole rotation period of the Varuna (Pr = 6.34 h). We fit the resulting relative reflectance with radiative transfer models of the surface of atmosphereless bodies. Results. After studying the spectra corresponding to different rotational phases of Varuna, we did not find any indication of surface variability at 2 sigma level. In all the spectra, we detect an absorption at 2.0 mu m, suggesting the presence of water ice on the surface. We do not detect any other volatiles on the surface, although the signal-to-noise ratio is not high enough to discard their presence in small quantities. Based on scattering models, we present two possible compositions compatible with our set of data and discuss their implications in the framework of the collisional history of the trans-Neptunian belt. Conclusions. We find that the most probable composition for the surface of Varuna is a mixture of amorphous silicates, complex organics, and water ice. This composition is compatible with all the materials being primordial, so no replenishment mechanism is needed in the equation. However, our data can also be fitted by models containing up to a 10% of methane ice. For an object with the characteristics of Varuna, this volatile could not be primordial, so an event, such as an energetic impact, would be needed to explain its presence on the surface. C1 [Lorenzi, V.] Fdn Galileo Galilei INAF, Brena Baja 38712, TF, Spain. [Pinilla-Alonso, N.; Emery, J. P.] Univ Tennessee, Knoxville, TN 37996 USA. [Licandro, J.] IAC, Tenerife, Spain. [Ore, C. M. Dalle] SETI Inst, Carl Sagan Ctr, Mountain View, CA USA. [Ore, C. M. Dalle] NASA, Ames Res Ctr, Mountain View, CA USA. RP Lorenzi, V (reprint author), Fdn Galileo Galilei INAF, Rambla Jose Ana Fernandez Perez 7, Brena Baja 38712, TF, Spain. EM lorenzi@tng.iac.es FU Juan de la Cierva Fellowship Programme of MINECO (Spanish Ministry of Economy and Competitiveness); MINECO [AYA2012-39115-C03-03]; [AYA2011-30106-C02-01] FX N.P.A. acknowledges support from the project AYA2011-30106-C02-01 and the Juan de la Cierva Fellowship Programme of MINECO (Spanish Ministry of Economy and Competitiveness). J.L. acknowledges support from the project AYA2012-39115-C03-03 (MINECO). Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundacion Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. We want to thank the referee F. de Meo for her valuable comments that improved the manuscript. NR 34 TC 4 Z9 4 U1 0 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2014 VL 562 AR A85 DI 10.1051/0004-6361/201322251 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC0CG UT WOS:000332161800049 ER PT J AU Lowry, SC Weissman, PR Duddy, SR Rozitis, B Fitzsimmons, A Green, SF Hicks, MD Snodgrass, C Wolters, SD Chesley, SR Pittichova, J van Oers, P AF Lowry, S. C. Weissman, P. R. Duddy, S. R. Rozitis, B. Fitzsimmons, A. Green, S. F. Hicks, M. D. Snodgrass, C. Wolters, S. D. Chesley, S. R. Pittichova, J. van Oers, P. TI The internal structure of asteroid (25143) Itokawa as revealed by detection of YORP spin-up SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: observational; minor planets, asteroids: individual: (25143) Itokawa; techniques: photometric; radiation mechanisms: thermal ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; HAYABUSA SPACECRAFT; 1999 KW4; RADAR; 25143-ITOKAWA; TOPOGRAPHY; YARKOVSKY; RADIATION; DYNAMICS; ROTATION AB Context. Near-Earth asteroid (25143) Itokawa was visited by the Hayabusa spacecraft in 2005, resulting in a highly detailed shape and surface topography model. This model has led to several predictions for the expected radiative torques on this asteroid, suggesting that its spin rate should be decelerating. Aims. To detect changes in rotation rate that may be due to YORP-induced radiative torques, which in turn may be used to investigate the interior structure of the asteroid. Methods. Through an observational survey spanning 2001 to 2013 we obtained rotational lightcurve data at various times over the last five close Earth-approaches of the asteroid. We applied a polyhedron-shape-modelling technique to assess the spin-state of the asteroid and its long term evolution. We also applied a detailed thermophysical analysis to the shape model determined from the Hayabusa spacecraft. Results. We have successfully measured an acceleration in Itokawa's spin rate of d omega/dt = (3.54 +/- 0.38) x 10(-8) rad day(-2), equivalent to a decrease of its rotation period of similar to 45 ms year(-1) From the thermophysical analysis we find that the centre-of-mass for Itokawa must be shifted by similar to 21 m along the long-axis of the asteroid to reconcile the observed YORP strength with theory. Conclusions. This can be explained if Itokawa is composed of two separate bodies with very different bulk densities of 1750 +/- 110 kg m(-3) and 2850 +/- 500 kg m(-3), and was formed from the merger of two separate bodies, either in the aftermath of a catastrophic disruption of a larger differentiated body, or from the collapse of a binary system. We therefore demonstrate that an observational measurement of radiative torques, when combined with a detailed shape model, can provide insight into the interior structure of an asteroid. Futhermore, this is the first measurement of density inhomogeneity within an asteroidal body, that reveals significant internal structure variation. A specialised spacecraft is normally required for this. C1 [Lowry, S. C.; Duddy, S. R.] Univ Kent, Sch Phys Sci SEPnet, Ctr Astrophys & Planetary Sci, Canterbury CT2 7NH, Kent, England. [Weissman, P. R.; Hicks, M. D.; Chesley, S. R.; Pittichova, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rozitis, B.; Green, S. F.; Wolters, S. D.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Fitzsimmons, A.] Queens Univ Belfast, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg, Germany. [van Oers, P.] Isaac Newton Grp Telescopes, Santa Cruz De La Palma 38700, Canary Islands, Spain. RP Lowry, SC (reprint author), Univ Kent, Sch Phys Sci SEPnet, Ctr Astrophys & Planetary Sci, Canterbury CT2 7NH, Kent, England. EM s.c.lowry@kent.ac.uk RI Green, Simon/C-7408-2009; OI Snodgrass, Colin/0000-0001-9328-2905 FU UK Science and Technology Facilities Council; Southeast Physics Network (SEPnet); European Union [268421] FX We thank the anonymous referee for their helpful comments. We thank all the staff at the observatories involved in this study for their support. This work was based on observations at the following observatories: ESO, Chile (PID: 185.C-1033); The Liverpool Telescope, La Palma; Palomar Observatory, California; The Isaac Newton Group, La Palma; Steward Observatory, Arizona; Table Mountain Observatory, California. S.C.L., S.R.D., BR., and S.F.G. gratefully acknowledge support from the UK Science and Technology Facilities Council. S.C.L. acknowledges support from the Southeast Physics Network (SEPnet). CS received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 268421. This work was performed in part at the Jet Propulsion Laboratory under a contract with NASA. This work made use of the NASA/JPL HORIZONS ephemeris-generating programme. All image reduction and processing were performed using the Image Reduction and Analysis Facility (IRAF) (Tody 1986 & 1993). IRAF is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. NR 40 TC 12 Z9 12 U1 6 U2 11 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2014 VL 562 AR A48 DI 10.1051/0004-6361/201322602 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC0CG UT WOS:000332161800091 ER PT J AU Muller, C Kadler, M Ojha, R Bock, M Krauss, F Taylor, GB Wilms, J Blanchard, J Carpenter, B Dauser, T Dutka, M Edwards, PG Gehrels, N Grossberger, C Hase, H Horiuchi, S Kreikenbohm, A Lovell, JEJ McConville, W Phillips, C Plotz, C Pursimo, T Quick, J Ros, E Schulz, R Stevens, J Tingay, SJ Trustedt, J Tzioumis, AK Zensus, JA AF Mueller, Cornelia Kadler, M. Ojha, R. Boeck, M. Krauss, F. Taylor, G. B. Wilms, J. Blanchard, J. Carpenter, B. Dauser, T. Dutka, M. Edwards, P. G. Gehrels, N. Grossberger, C. Hase, H. Horiuchi, S. Kreikenbohm, A. Lovell, J. E. J. McConville, W. Phillips, C. Ploetz, C. Pursimo, T. Quick, J. Ros, E. Schulz, R. Stevens, J. Tingay, S. J. Truestedt, J. Tzioumis, A. K. Zensus, J. A. TI The unusual multiwavelength properties of the gamma-ray source PMN J1603-4904 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; galaxies: individual: PMNJ1603-4904; radio continuum: general; gamma rays: galaxies; techniques: interferometric; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; COMPACT SYMMETRIC OBJECTS; GHZ-PEAKED-SPECTRUM; EXTRAGALACTIC RADIO-SOURCES; BL LACERTAE OBJECTS; PULSAR WIND NEBULAE; ALL-SKY SURVEY; SOURCE CATALOG; STEEP-SPECTRUM AB Context. We investigate the nature and classification of PMN J1603-4904, a bright radio source close to the Galactic plane, which is associated with one of the brightest hard-spectrum gamma-ray sources detected by Fermi/LAT. It has previously been classified as a low-peaked BL Lac object based on its broadband emission and the absence of optical emission lines. Optical measurements, however, suffer strongly from extinction and the absence of pronounced short-time gamma-ray variability over years of monitoring is unusual for a blazar. Aims. In this paper, we are combining new and archival multiwavelength data of PMN J1603-4904 in order to reconsider the classification and nature of this unusual gamma-ray source. Methods. For the first time, we study the radio morphology of PMN J1603-4904 at 8.4 GHz and 22.3 GHz, and its spectral properties on milliarcsecond scales, based on VLBI observations from the TANAMI program. We combine the resulting images with multiwavelength data in the radio, IR, optical/UV, X-ray, and gamma-ray regimes. Results. PMN J1603-4904 shows a symmetric brightness distribution at 8.4 GHz on milliarcsecond scales, with the brightest, and most compact component in the center of the emission region. The morphology is reminiscent of a compact symmetric object (CSO). Such objects, thought to be young radio galaxies, have been predicted to produce gamma-ray emission but have not been detected as a class by the Fermi gamma-ray telescope so far. Sparse (u, v)-coverage at 22.3 GHz prevents an unambiguous modeling of the source morphology at this higher frequency. Moreover, infrared measurements reveal an excess in the spectral energy distribution (SED), which can be modeled with a blackbody with a temperature of about 1600 K, and which is usually not present in blazar SEDs. Conclusions. The TANAMI VLBI data and the shape of the broadband SED challenge the current blazar classification of one of the brightest gamma-ray sources in the sky. PMN J1603-4904 seems to be either a highly peculiar BL Lac object or a misaligned jet source. In the latter case, the intriguing VLBI structure opens room for a possible classification of PMN J1603-4904 as a gamma-ray bright CSO. C1 [Mueller, Cornelia; Krauss, F.; Wilms, J.; Dauser, T.; Grossberger, C.; Kreikenbohm, A.; Schulz, R.; Truestedt, J.] Univ Erlangen Nurnberg, Dr Remeis Sternwarte & ECAP, D-96049 Bamberg, Germany. [Mueller, Cornelia; Kadler, M.; Krauss, F.; Grossberger, C.; Kreikenbohm, A.; Schulz, R.; Truestedt, J.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [Ojha, R.; Gehrels, N.; McConville, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ojha, R.; Carpenter, B.; Dutka, M.] Catholic Univ Amer, Washington, DC 20064 USA. [Boeck, M.; Ros, E.; Zensus, J. A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Taylor, G. B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Blanchard, J.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Edwards, P. G.; Phillips, C.; Stevens, J.; Tzioumis, A. K.] CSIRO Astron & Space Sci, ATNF, Sydney, NSW 1710, Australia. [Hase, H.; Ploetz, C.] Bundesamt Kartog & Geodasie, D-93444 Bad Kotzting, Germany. [Horiuchi, S.] CSIRO Astron & Space Sci, Canberra Deep Space Commun Complex, Tuggeranong, ACT S, Australia. [Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Pursimo, T.] Nordic Opt Telescope, E-38700 Santa Cruz De La Palma, Spain. [Quick, J.] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdorp, South Africa. [Ros, E.] Univ Valencia, Observ Astron, Valencia 46980, Spain. [Ros, E.] Univ Valencia, Dept Astron & Astrofis, Valencia 46100, Spain. [Tingay, S. J.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6102, Australia. RP Muller, C (reprint author), Univ Erlangen Nurnberg, Dr Remeis Sternwarte & ECAP, Sternwartstr 7, D-96049 Bamberg, Germany. EM cornelia.mueller@sternwarte.uni-erlangen.de RI Wilms, Joern/C-8116-2013; OI Wilms, Joern/0000-0003-2065-5410; Krauss, Felicia/0000-0001-6191-1244; Ros, Eduardo/0000-0001-9503-4892; Kadler, Matthias/0000-0001-5606-6154 FU NASA [NNH09ZDA001N, NNH10ZDA001N]; NASA; Gemini Observatory [GS-2013A-Q-80]; Studienstiftung des Deutschen Volkes; Spanish MINECO [AYA2009-13036-C02-02, AYA2012-38491-C02-01]; Generalitat Valenciana project [PROMETEO/2009/104]; COST [MP0905]; Deutsche Forschungsgemeinschaft [DFG WI1860/10-1] FX The Australian Long Baseline Array and the Australia Telescope Compact Array are part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. This research was funded in part by NASA through Fermi Guest Investigator grants NNH09ZDA001N and NNH10ZDA001N. It was supported by an appointment to the NASA Post-doctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. It is based on observations obtained at the Gemini Observatory (Program ID: GS-2013A-Q-80), which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). This research has made use of data from the NASA/IPAC Extragalactic Database (NED), operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration; and the SIMBAD database (operated at the CDS, Strasbourg, France). C. M. acknowledges the support of the "Studienstiftung des Deutschen Volkes". E. R. was partially supported by Spanish MINECO projects AYA2009-13036-C02-02 and AYA2012-38491-C02-01 and by the Generalitat Valenciana project PROMETEO/2009/104, as well as by the COST MP0905 action "Black Holes in a Violent Universe". R. S. acknowledges support from Deutsche Forschungsgemeinschaft grant DFG WI1860/10-1. We thank I. Donnarumma for the useful discussion about star-burst SEDs, R. D'Abrusco for performing checks on the corrected WISE data, and J. E. Davis for the development of the slxfig module used to prepare all figures in this work. We thank the referee for helpful comments and suggestions. NR 100 TC 13 Z9 13 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2014 VL 562 AR A4 DI 10.1051/0004-6361/201322827 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC0CG UT WOS:000332161800121 ER PT J AU Parviainen, H Gandolfi, D Deleuil, M Moutou, C Deeg, HJ Ferraz-Mello, S Samuel, B Csizmadia, S Pasternacki, T Wuchterl, G Havel, M Fridlund, M Angus, R Tingley, B Grziwa, S Korth, J Aigrain, S Almenara, JM Alonso, R Baglin, A Barros, SCC Borde, P Bouchy, F Cabrera, J Diaz, RF Dvorak, R Erikson, A Guillot, T Hatzes, A Hebrard, G Mazeh, T Montagnier, G Ofir, A Ollivier, M Patzold, M Rauer, H Rouan, D Santerne, A Schneider, J AF Parviainen, H. Gandolfi, D. Deleuil, M. Moutou, C. Deeg, H. J. Ferraz-Mello, S. Samuel, B. Csizmadia, Sz. Pasternacki, T. Wuchterl, G. Havel, M. Fridlund, M. Angus, R. Tingley, B. Grziwa, S. Korth, J. Aigrain, S. Almenara, J. M. Alonso, R. Baglin, A. Barros, S. C. C. Borde, P. Bouchy, F. Cabrera, J. Diaz, R. F. Dvorak, R. Erikson, A. Guillot, T. Hatzes, A. Hebrard, G. Mazeh, T. Montagnier, G. Ofir, A. Ollivier, M. Paetzold, M. Rauer, H. Rouan, D. Santerne, A. Schneider, J. TI Transiting exoplanets from the CoRoT space mission XXV. C0R0T-27b: a massive and dense planet on a short-period orbit SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planets and satellites: detection; stars: individual: CoRoT-27; techniques: photometric; techniques: radial velocities; techniques: spectroscopic; methods: statistical ID ANGULAR-MOMENTUM EVOLUTION; GIANT PLANETS; BROWN DWARFS; LIGHT CURVES; SOLAR; JUPITER; MODEL; STARS; KEPLER; EQUILIBRIUM AB Aims. We report the discovery of a massive and dense transiting planet CoRoT-27b on a 3.58-day orbit around a 4.2 Gyr-old G2 star. The planet candidate was identified from the CoRoT photometry, and was confirmed as a planet with ground-based spectroscopy. Methods. The confirmation of the planet candidate is based on radial velocity observations combined with imaging to rule out blends. The characterisation of the planet and its host star was carried out using a Bayesian approach where all the data (CoRoT photometry, radial velocities, and spectroscopic characterisation of the star) are used jointly. The Bayesian analysis included a study whether the assumption of white normally distributed noise holds for the CoRoT photometry and whether the use of a non-normal noise distribution offers advantages in parameter estimation and model selection. Results. CoRoT-27b has a mass of 10.39 +/- 0.55 M-Jup, a radius of 1.01 +/- 0.04 R-Jup, a mean density of 12.6(-1.67)(+1.92) g cm(-3), and an effective temperature of 1500 +/- 130 K. The planet orbits around its host star, a 4.2 Gyr-old G2-star with a mass M-star = 1.06 M-circle dot and a radius R-star = 1.05 R-circle dot, on a 0.048 +/- 0.007 AU orbit of 3.58 days. The radial velocity observations allow us to exclude highly eccentric orbits, namely, e <0.065 with 99% confidence. Given its high mass and density, theoretical modelling of CoRoT-27b is demanding. We identify two solutions with heavy element mass fractions of 0.11 +/- 0.08 M-circle plus, and 0.07 +/- 0.06 M-circle plus, but even solutions void of heavy elements cannot be excluded. We carry out a secondary eclipse search from the CoRoT photometry using a method based on Bayesian model selection, but conclude that the noise level is too high to detect eclipses shallower than 9% of the transit depth. Using a non-normal noise model was shown not to affect the parameter estimation results, but led to significant improvement in the sensitivity of the model selection process. C1 [Parviainen, H.; Deeg, H. J.] IAC, San Cristobal la Laguna 38200, Tenerife, Spain. [Parviainen, H.; Deeg, H. J.; Alonso, R.] ULL, Dept Astrofis, San Cristobal la Laguna 38206, Tenerife, Spain. [Parviainen, H.; Angus, R.; Aigrain, S.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Gandolfi, D.] INAF, Catania Astrophys Observ, I-95123 Catania, Italy. [Deleuil, M.; Moutou, C.; Almenara, J. M.; Barros, S. C. C.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Ferraz-Mello, S.] Univ Sao Paulo, IAG, BR-05508090 Sao Paulo, Brazil. [Samuel, B.; Baglin, A.; Rouan, D.] Univ Paris Diderot, UVSQ, CNRS, LESIA,Observ Paris,UMR 8109, F-92195 Meudon, France. [Csizmadia, Sz.; Pasternacki, T.; Cabrera, J.; Erikson, A.; Rauer, H.] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany. [Wuchterl, G.] Thuringer Landessternwarte, CoRoT DLR, D-07778 Tautenburg, Germany. [Havel, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Fridlund, M.] ESTEC ESA, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. [Tingley, B.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Grziwa, S.; Korth, J.; Paetzold, M.] Univ Cologne, Rhein Inst Umweltforsch, Kolen, Germany. [Borde, P.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Bouchy, F.; Hebrard, G.; Montagnier, G.] Observa Haute Provence, F-04670 St Michel Lobservatoire, France. [Bouchy, F.; Hebrard, G.; Montagnier, G.] Inst Astrophys, F-75014 Paris, France. [Dvorak, R.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Guillot, T.] Observ Cote Azur, Lab Cassiopee, F-06304 Nice 4, France. [Mazeh, T.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Ofir, A.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Santerne, A.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Schneider, J.] Univ Paris Diderot, CNRS, LUTH, Observ Paris, F-92195 Meudon, France. RP Parviainen, H (reprint author), IAC, San Cristobal la Laguna 38200, Tenerife, Spain. EM hannu.parviainen@astro.ox.ac.uk RI Ferraz-Mello, Sylvio/B-7529-2013; Alonso, Roi/D-8799-2014; OI Alonso, Roi/0000-0001-8462-8126; Parviainen, Hannu/0000-0001-5519-1391; Gandolfi, Davide/0000-0001-8627-9628; Santerne, Alexandre/0000-0002-3586-1316; Diaz, Rodrigo/0000-0001-9289-5160 FU RoPACS; European Commission; Vaisala Foundation through the Finnish Academy of Science and Letters; Spanish Ministry of Economy and Competitiveness (MINECO) [AYA2012-39346-C02]; European Research Council/European Community [239953]; European Union [267251] FX First and foremost we would like to thank the anonymous referee for her/his prompt review. H.P. has received support from RoPACS during this research, a Marie Curie Initial Training Network funded by the European Commission's Seventh Framework Programme. H.P. has received funding from the Vaisala Foundation through the Finnish Academy of Science and Letters during this research. The team at the IAC acknowledges funding by grant AYA2012-39346-C02 of the Spanish Ministry of Economy and Competitiveness (MINECO). This research was supported by an appointment to the NASA Postdoctoral Program at the Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. A.S. acknowledges support from the European Research Council/European Community under the FP7 through Starting Grant agreement number 239953. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 267251. NR 60 TC 8 Z9 8 U1 0 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2014 VL 562 AR A140 DI 10.1051/0004-6361/201323049 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC0CG UT WOS:000332161800142 ER PT J AU Romano, P Krimm, HA Palmer, DM Ducci, L Esposito, P Vercellone, S Evans, PA Guidorzi, C Mangano, V Kennea, JA Barthelmy, SD Burrows, DN Gehrels, N AF Romano, P. y Krimm, H. A. Palmer, D. M. Ducci, L. Esposito, P. Vercellone, S. Evans, P. A. Guidorzi, C. Mangano, V. Kennea, J. A. Barthelmy, S. D. Burrows, D. N. Gehrels, N. TI The 100-month Swift catalogue of supergiant fast X-ray transients SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: binaries; catalogs; binaries: close; stars: neutron ID XMM-NEWTON OBSERVATIONS; BURST ALERT TELESCOPE; CLUMPY STELLAR WINDS; XTE J1739-302; IGR J17544-2619; ORBITAL PERIOD; SAX J1818.6-1703; MULTIWAVELENGTH OBSERVATIONS; INTEGRAL OBSERVATIONS; OPTICAL COUNTERPART AB Context. Supergiant fast X-ray transients (SFXTs) are high mass X-ray, binaries (HMXBs) that are defined by their hard X-ray flaring behaviour. During these flares they reach peak luminosities of 10(36)-10(37) erg s(-1) for a few hours On the hard X-ray), which are much shorter ti mescales than those characterizing Be/X-ray binaries. Aims. We investigate the characteristics of bright flares (detections in excess of 5 sigma.) for a sample of SFXTs and their relation to the orbital phase. Methods. We have retrieved all Swift/BAT Transient Monitor light curves and collected all detections in excess of 5 sigma from both dailyand orbital-averaged light curves in the time range of 2005 February 12 to 2013 May 31 (MID 53 413-56 443). We also considered all on-board detections as recorded in the same time span and selected those in excess of 5cr and within 4 arcmin of each source in our sample. Results. We present a catalogue of over a thousand BAT flares from 11 SIATs, down to 15-150 keV fluxes of similar to 6 x 10(-1) erg cm(-2) S-1 (daily timescale) and similar to 1.5 x 10(-9) erg cm(2) s(-1) (orbital timescale, averaging similar to 800 5); the great majority of these :flares are unpublished. The catalogue spans 100 months. This population is characterized by short (a few hundred seconds) and relatively bright (in excess of 100 mCrab, 15-50 keV) events. In the hard X-ray, these flares last generally much less than a day. Clustering of hard X-ray flares can be used to indirectly measure the length of an outburst, even when the low-level emission is not detected. We construct the distributions of.flares, of their significance (in terms of sigma), and of their flux as a function of orbital phase to infer the properties of these binary systems. In particular, we observe a trend of clustering of flares at some phases as P-orb increases, which is consistent with a progression from tight circular or mildly eccentric orbits at short periods to wider and more eccentric orbits at longer orbital periods. Finally, we estimate the expected number of flares for a given source for our limiting flux and provide the recipe for calculating them for the limiting :flux of future hard X-ray observatories. C1 [Romano, P. y; Vercellone, S.] INAF, Ist Astrofis Spaziale & Fis Cosm Palermo, I-90146 Palermo, Italy. [Krimm, H. A.; Barthelmy, S. D.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD USA. [Palmer, D. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Ducci, L.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Esposito, P.] INAF, Ist Astrofis Spaziale & Fis Cosm Milano, I-20133 Milan, Italy. [Evans, P. A.] Univ Leicester, Dept Phys & Astron, Xray & Observat Astron Grp, Leicester LE1 7RH, Leics, England. [Guidorzi, C.] Univ Ferrara, Dept Phys & Earth Sci, I-44122 Ferrara, Italy. [Mangano, V.; Kennea, J. A.; Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Romano, P (reprint author), INAF, Ist Astrofis Spaziale & Fis Cosm Palermo, Via U La Malfa 153, I-90146 Palermo, Italy. EM romano@ifc.inaf.it FU NASA [NAS5-00136]; NASA Swift GO [NNX09AU85G, NNX12AD32G, NNX12AE57G, NNX13AC756] FX We thank W. Baumgartner and C. Markwardt for support with the BAT survey products, and E. Bozzo and M. Capalbi, for helpful discussions. We also thank the anonymous referee for constructive comments that helped improve the paper. We acknowledge financial contribution from NASA contract NAS5-00136 at PSU. FIAK acknowledges NASA Swift GO grants NNX09AU85G, NNX12AD32G, NNX12AE57G, and NNX13AC756. This work made use of the results of the Swift/BAT hard X-ray transient monitor: http://swift.gsfc.nasa.gov/docs/swift/results/transients/. NR 140 TC 20 Z9 20 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2014 VL 562 AR A2 DI 10.1051/0004-6361/201322516 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC0CG UT WOS:000332161800082 ER PT J AU Santini, P Maiolino, R Magnelli, B Lutz, D Lamastra, A Causi, GL Eales, S Andreani, P Berta, S Buat, V Cooray, A Cresci, G Daddi, E Farrah, D Fontana, A Franceschini, A Genzel, R Granato, G Grazian, A Le Floc'h, E Magdis, G Magliocchetti, M Mannucci, F Menci, N Nordon, R Oliver, S Popesso, P Pozzi, F Riguccini, L Rodighiero, G Rosario, DJ Salvato, M Scott, D Silva, L Tacconi, L Viero, M Wang, L Wuyts, S Xu, K AF Santini, P. Maiolino, R. Magnelli, B. Lutz, D. Lamastra, A. Causi, G. Li Eales, S. Andreani, P. Berta, S. Buat, V. Cooray, A. Cresci, G. Daddi, E. Farrah, D. Fontana, A. Franceschini, A. Genzel, R. Granato, G. Grazian, A. Le Floc'h, E. Magdis, G. Magliocchetti, M. Mannucci, F. Menci, N. Nordon, R. Oliver, S. Popesso, P. Pozzi, F. Riguccini, L. Rodighiero, G. Rosario, D. J. Salvato, M. Scott, D. Silva, L. Tacconi, L. Viero, M. Wang, L. Wuyts, S. Xu, K. TI The evolution of the dust and gas content in galaxies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: evolution; galaxies: fundamental parameters; galaxies: high-redshift; galaxies: ISM; infrared: galaxies ID STAR-FORMING GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; CO-TO-H-2 CONVERSION FACTOR; MASS-METALLICITY RELATION; HIGH-REDSHIFT GALAXIES; ACTIVE GALACTIC NUCLEI; LARGE-MAGELLANIC-CLOUD; GOODS-MUSIC SAMPLE; M-ASTERISK PLANE; SIMILAR-TO 2.5 AB We use deep Herschel observations taken with both PACS and SPIRE imaging cameras to estimate the dust mass of a sample of galaxies extracted from the GOODS-S, GOODS-N and the COSMOS fields. We divide the redshift-stellar mass (M-star)-star formation rate (SFR) parameter space into small bins and investigate average properties over this grid. In the first part of the work we investigate the scaling relations between dust mass, stellar mass and SFR out to z = 2.5. No clear evolution of the dust mass with redshift is observed at a given SFR and stellar mass. We find a tight correlation between the SFR and the dust mass, which, under reasonable assumptions, is likely a consequence of the Schmidt-Kennicutt (S-K) relation. The previously observed correlation between the stellar content and the dust content flattens or sometimes disappears when considering galaxies with the same SFR. Our finding suggests that most of the correlation between dust mass and stellar mass obtained by previous studies is likely a consequence of the correlation between the dust mass and the SFR combined with the main sequence, i.e., the tight relation observed between the stellar mass and the SFR and followed by the majority of star-forming galaxies. We then investigate the gas content as inferred from dust mass measurements. We convert the dust mass into gas mass by assuming that the dust-to-gas ratio scales linearly with the gas metallicity (as supported by many observations). For normal star-forming galaxies (on the main sequence) the inferred relation between the SFR and the gas mass (integrated S-K relation) broadly agrees with the results of previous studies based on CO measurements, despite the completely different approaches. We observe that all galaxies in the sample follow, within uncertainties, the same S-K relation. However, when investigated in redshift intervals, the S-K relation shows a moderate, but significant redshift evolution. The bulk of the galaxy population at z similar to 2 converts gas into stars with an efficiency (star formation efficiency, SFE = SFR/M-gas, equal to the inverse of the depletion time) about 5 times higher than at z similar to 0. However, it is not clear what fraction of such variation of the SFE is due to an intrinsic redshift evolution and what fraction is simply a consequence of high-z galaxies having, on average, higher SFR, combined with the super-linear slope of the S-K relation (while other studies find a linear slope). We confirm that the gas fraction (f(gas) = M-gas/(M-gas + M-star)) decreases with stellar mass and increases with the SFR. We observe no evolution with redshift once M-star and SFR are fixed. We explain these trends by introducing a universal relation between gas fraction, stellar mass and SFR that does not evolve with redshift, at least out to z similar to 2.5. Galaxies move across this relation as their gas content evolves across the cosmic epochs. We use the 3D fundamental f(gas)-M-star-SFR relation, along with the evolution of the main sequence with redshift, to estimate the evolution of the gas fraction in the average population of galaxies as a function of redshift and as a function of stellar mass: we find that M-star greater than or similar to 10(11) M-circle dot galaxies show the strongest evolution at z greater than or similar to 1. 3 and a flatter trend at lower redshift, while f(gas) decreases more regularly over the entire redshift range probed in M-star less than or similar to 10(11) M-circle dot galaxies, in agreement with a downsizing scenario. C1 [Santini, P.; Lamastra, A.; Causi, G. Li; Fontana, A.; Grazian, A.; Menci, N.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Maiolino, R.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Maiolino, R.] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HE, England. [Magnelli, B.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Lutz, D.; Berta, S.; Genzel, R.; Popesso, P.; Rosario, D. J.; Salvato, M.; Tacconi, L.; Wuyts, S.] Max Planck Inst Extraterr Phys, MPE, D-85741 Garching, Germany. [Eales, S.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Andreani, P.] ESO, D-85748 Garching, Germany. [Andreani, P.; Granato, G.; Silva, L.] Osserv Astron Roma, INAF, I-34131 Trieste, Italy. [Buat, V.] Aix Marseille Univ, CNRS, LAM, F-13388 Marseille, France. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Cresci, G.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Daddi, E.; Le Floc'h, E.] Univ Paris Diderot, CEA Saclay, DSM CNRS, Lab AIM,CEA IRFU Serv Astrophys, F-91191 Gif Sur Yvette, France. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Franceschini, A.; Rodighiero, G.] Univ Padua, Dipartimento Astron, Vicolo Osservatorio, I-35122 Padua, Italy. [Magdis, G.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Magliocchetti, M.] INAF, IAPS, I-00133 Rome, Italy. [Mannucci, F.] Osservatorio Astros Arcetri, INAF, I-50125 Florence, Italy. [Nordon, R.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Oliver, S.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Popesso, P.] Excellence Cluster Universe, D-85748 Garching, Germany. [Pozzi, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Riguccini, L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Riguccini, L.] BAER Inst, Sonoma, CA USA. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Viero, M.] CALTECH, Pasadena, CA 91125 USA. [Wang, L.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Xu, K.] Caltech, IPAC, NHSC, Pasadena, CA 91125 USA. RP Santini, P (reprint author), Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, Italy. RI Daddi, Emanuele/D-1649-2012; Magdis, Georgios/C-7295-2014; OI Daddi, Emanuele/0000-0002-3331-9590; Magdis, Georgios/0000-0002-4872-2294; Li Causi, Gianluca/0000-0001-9539-2112; Scott, Douglas/0000-0002-6878-9840; Granato, Gian Luigi/0000-0002-4480-6909; Menci, Nicola/0000-0002-4096-2680; Cresci, Giovanni/0000-0002-5281-1417; Santini, Paola/0000-0002-9334-8705; fontana, adriano/0000-0003-3820-2823 FU BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain); CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA); [ASI I/005/11/0] FX P.S. thanks N. Scoville for interesting and useful discussions and A. Marconi and G. Risaliti for helping with fitting routines and statistical issues. This work was supported by grant ASI I/005/11/0. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada), NAOC (China), CEA, LAM (France), IFSI, University of Padua (Italy), IAC (Spain), Stockholm Observatory (Sweden), Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK), Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). NR 123 TC 60 Z9 60 U1 1 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2014 VL 562 AR A30 DI 10.1051/0004-6361/201322835 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC0CG UT WOS:000332161800124 ER PT J AU Tadesse, T Wiegelmann, T Gosain, S MacNeice, P Pevtsov, AA AF Tadesse, T. Wiegelmann, T. Gosain, S. MacNeice, P. Pevtsov, A. A. TI First use of synoptic vector magnetograms for global nonlinear, force-free coronal magnetic field models SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE magnetic fields; Sun: corona; Sun: photosphere ID SOLAR ACTIVE-REGION; SPHERICAL GEOMETRY; MASS EJECTIONS; FREE-ENERGY; QUIET SUN; SDO/HMI; FLARE; SOLIS; RECONSTRUCTION; EXTRAPOLATION AB Context. The magnetic field permeating the solar atmosphere is generally thought to provide the energy for much of the activity seen in the solar corona, such as flares, coronal mass ejections (CMEs), etc. To overcome the unavailability of coronal magnetic field measurements, photospheric magnetic field vector data can be used to reconstruct the coronal field. Currently, there are several modelling techniques being used to calculate three-dimensional field lines into the solar atmosphere. Aims. For the first time, synoptic maps of a photospheric-vector magnetic field synthesized from the vector spectromagnetograph (VSM) on Synoptic Optical Long-term Investigations of the Sun (SOLIS) are used to model the coronal magnetic field and estimate free magnetic energy in the global scale. The free energy (i.e., the energy in excess of the potential field energy) is one of the main indicators used in space weather forecasts to predict the eruptivity of active regions. Methods. We solve the nonlinear force-free field equations using an optimization principle in spherical geometry. The resulting three-dimensional magnetic fields are used to estimate the magnetic free energy content E-free = E-nlfff = E-pot, which is the difference of the magnetic energies between the nonpotential field and the potential field in the global solar corona. For comparison, we overlay the extrapolated magnetic field lines with the extreme ultraviolet (EUV) observations by the atmospheric imaging assembly (AIA) on board the Solar Dynamics Observatory (SDO). Results. For a single Carrington rotation 2121, we find that the global nonlinear force-free field (NLFFF) magnetic energy density is 10.3% higher than the potential one. Most of this free energy is located in active regions. C1 [Tadesse, T.; MacNeice, P.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. [Wiegelmann, T.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Gosain, S.; Pevtsov, A. A.] Natl Solar Observ, Sunspot, NM 88349 USA. RP Tadesse, T (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. EM tilaye.tadesse.asfaw@nasa.gov; wiegelmann@mps.mpg.de; sgosain@nso.edu; peter.j.macneice@nasa.gov; apevtsov@nso.edu OI Pevtsov, Alexei/0000-0003-0489-0920 FU National Science Foundation; NASA Postdoctoral Program at the Goddard Space Flight Center (GSFC); NASA; DLR-grant [50 OC 453 0501] FX The authors would like to thank the referee for his/her constructive and helpful comments. This work utilizes SOLIS data obtained by the NSO Integrated Synoptic Program (NISP), managed by the National Solar Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc. under a cooperative agreement with the National Science Foundation. This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center (GSFC), administered by Oak Ridge Associated Universities through a contract with NASA. The work of T. Wiegelmann was supported by DLR-grant 50 OC 453 0501. NR 51 TC 7 Z9 7 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2014 VL 562 AR A105 DI 10.1051/0004-6361/201322418 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC0CG UT WOS:000332161800065 ER PT J AU Liston, DB Adelstein, BD Stone, LS AF Liston, Dorion B. Adelstein, Bernard D. Stone, Leland S. TI Onset of Positional Vertigo During Exposure to Combined G Loading and Chest-to-Spine Vibration SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE BPPV; tumbling; wobblies ID BODY AB Background: Aerospace environments commonly expose pilots to vibration and sustained acceleration, alone and in combination. Case Reports: Of 16 experimental research participants, 3 reported symptoms of vertigo and signs of torsional nystagmus during or shortly following exposure to sustained chest-to-spine (+3.8 G(x)) acceleration (G loading) and chest-to-spine (0.5 g(x)) vibration in the 8-16 Hz band. Two of the participants reported intermittent vertigo for up to 2 wk, were diagnosed with benign paroxysmal positional vertigo (BPPV), and were treated successfully with the Epley Maneuver. On a follow-up survey, a third participant reported transient BPPV-like vertigo, which resolved spontaneously. The follow-up survey also prompted participants to self-report other effects following research protocol exposure to vibration and G loading, revealing details about other minor and transient, but more common, effects that resolved within 3 h. Discussion: Our studies indicated a significantly elevated incidence of BPPV following exposure to vibration plus G loading compared to vibration alone that was positively correlated with participant age. One mechanism for the rolling sensation in BPPV involves broken or dislodged otoconia floating within one of the posterior semicircular canals, making the canal gravity-sensitive. Our observations highlight a heretofore unforeseen risk of otolith damage sustained during launch, undetectable in space, potentially contributing to vertigo and perceived tumbling upon re-entry from microgravity. C1 [Liston, Dorion B.; Adelstein, Bernard D.; Stone, Leland S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Liston, Dorion B.] San Jose State Univ, San Jose, CA 95192 USA. RP Liston, DB (reprint author), NASA, Ames Res Ctr, Mail Stop 262-2, Moffett Field, CA 94035 USA. EM dorion.b.liston@nasa.gov FU NSBRI SA FX We thank Dr. Brent Beutter and Dr. Rich Williams for helpful comments on an earlier draft. We thank Dr. Ralph Pelligra for his medical insight and guidance, and input on the manuscript. This work was supported by NSBRI SA 2002. NR 17 TC 2 Z9 2 U1 1 U2 5 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 EI 1943-4448 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD FEB PY 2014 VL 85 IS 2 BP 183 EP 186 DI 10.3357/ASEM.3784.2014 PG 4 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA AD1MB UT WOS:000332997000012 PM 24597164 ER PT J AU Golding, J Steer, CD Lowery, T Hibbeln, JR AF Golding, Jean Steer, Colin D. Lowery, Tony Hibbeln, Joseph R. TI ALSPAC Mercury Study and Fish Consumers: Golding et al. Respond SO ENVIRONMENTAL HEALTH PERSPECTIVES LA English DT Letter ID UK TOTAL DIET; CONSUMPTION; EXPOSURE; COHORT C1 [Golding, Jean; Steer, Colin D.] Univ Bristol, Ctr Child & Adolescent Hlth, Bristol, Avon, England. [Lowery, Tony] NOAA, Natl Seafood Inspect Lab, Natl Marine Fisheries Serv, Pascagoula, MS USA. [Hibbeln, Joseph R.] NIAAA, NIH, US Dept HHS, Bethesda, MD USA. RP Golding, J (reprint author), Univ Bristol, Ctr Child & Adolescent Hlth, Bristol, Avon, England. EM jean.golding@bristol.ac.uk NR 7 TC 0 Z9 0 U1 2 U2 5 PU US DEPT HEALTH HUMAN SCIENCES PUBLIC HEALTH SCIENCE PI RES TRIANGLE PK PA NATL INST HEALTH, NATL INST ENVIRONMENTAL HEALTH SCIENCES, PO BOX 12233, RES TRIANGLE PK, NC 27709-2233 USA SN 0091-6765 EI 1552-9924 J9 ENVIRON HEALTH PERSP JI Environ. Health Perspect. PD FEB PY 2014 VL 122 IS 2 BP A38 EP A39 PG 2 WC Environmental Sciences; Public, Environmental & Occupational Health; Toxicology SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Toxicology GA AC6QY UT WOS:000332650500003 PM 24486699 ER PT J AU Parashar, TN Vasquez, BJ Markovskii, SA AF Parashar, Tulasi N. Vasquez, Bernard J. Markovskii, Sergei A. TI The role of electron equation of state in heating partition of protons in a collisionless plasma SO PHYSICS OF PLASMAS LA English DT Article ID SOLAR-WIND ELECTRONS; ORSZAG-TANG VORTEX; MAGNETOHYDRODYNAMIC TURBULENCE; RECONNECTION; DISSIPATION; CONDUCTION; SIMULATION; EVOLUTION AB One of the outstanding questions related to the solar wind is the heating of solar wind plasma. Addressing this question requires a self consistent treatment of the kinetic physics of a collisionless plasma. A hybrid code (with particle ions and fluid electrons) is one of the most convenient computational tools, which allows us to explore self consistent ion kinetics, while saving us computational time as compared to the full particle in cell codes. A common assumption used in hybrid codes is that of isothermal electrons. In this paper, we discuss the role that the equation of state for electrons could potentially play in determining the ion kinetics. (C) 2014 AIP Publishing LLC. C1 [Parashar, Tulasi N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Vasquez, Bernard J.; Markovskii, Sergei A.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. RP Parashar, TN (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU NASA/ORAU Postdoctoral Fellowship; NASA Solar and Heliospheric Physics SRT Grant [NNX10AC18G]; NASA Heliophysics Theory Grant [NNX11AJ37G]; NASA Guest Investigator Grant [NNX09AG28G]; NSF SHINE Grant [ATM0850705] FX T.N.P. was supported by the NASA/ORAU Postdoctoral Fellowship for this work. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. S. Markovskii and B. Vasquez were supported by the NASA Solar and Heliospheric Physics SR&T Grant No. NNX10AC18G and the NASA Heliophysics Theory Grant No. NNX11AJ37G to the University of New Hampshire. B. Vasquez was also supported by the NASA Guest Investigator Grant No. NNX09AG28G and the NSF SHINE Grant No. ATM0850705 to the University of New Hampshire. NR 34 TC 9 Z9 9 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD FEB PY 2014 VL 21 IS 2 AR 022301 DI 10.1063/1.4863422 PG 5 WC Physics, Fluids & Plasmas SC Physics GA AC2IJ UT WOS:000332323400028 ER PT J AU Acciari, VA Arlen, T Aune, T Benbow, W Bird, R Bouvier, A Bradbury, SM Buckley, JH Bugaev, V Perez, ID Carter-Lewis, DA Cesarini, A Ciupik, L Collins-Hughes, E Connolly, MP Cui, W Duke, C Dumm, J Falcone, A Federici, S Fegan, DJ Fegan, SJ Finley, JP Finnegan, G Fortson, L Gaidos, J Galante, N Gall, D Gibbs, K Gillanders, GH Griffin, S Grube, J Gyuk, G Hanna, D Horan, D Humensky, TB Kaaret, P Kertzman, M Khassen, Y Kieda, D Krawczynski, H Krennrich, F Lang, MJ McEnery, JE Madhavan, AS Moriarty, P Nelson, T de Bhroithe, AO Ong, RA Orr, M Otte, AN Perkins, JS Petry, D Pichel, A Pohl, M Quinn, J Ragan, K Reynolds, T Roache, E Rovero, A Schroedter, M Sembroski, GH Smith, A Telezhinsky, I Theiling, M Toner, J Tyler, J Varlotta, A Vivier, M Wakely, SP Ward, JE Weekes, TC Weinstein, A Welsing, R Williams, DA Wissel, S AF Acciari, V. A. Arlen, T. Aune, T. Benbow, W. Bird, R. Bouvier, A. Bradbury, S. M. Buckley, J. H. Bugaev, V. de la Calle Perez, I. Carter-Lewis, D. A. Cesarini, A. Ciupik, L. Collins-Hughes, E. Connolly, M. P. Cui, W. Duke, C. Dumm, J. Falcone, A. Federici, S. Fegan, D. J. Fegan, S. J. Finley, J. P. Finnegan, G. Fortson, L. Gaidos, J. Galante, N. Gall, D. Gibbs, K. Gillanders, G. H. Griffin, S. Grube, J. Gyuk, G. Hanna, D. Horan, D. Humensky, T. B. Kaaret, P. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Lang, M. J. McEnery, J. E. Madhavan, A. S. Moriarty, P. Nelson, T. de Bhroithe, A. O'Faolain Ong, R. A. Orr, M. Otte, A. N. Perkins, J. S. Petry, D. Pichel, A. Pohl, M. Quinn, J. Ragan, K. Reynolds, T. Roache, E. Rovero, A. Schroedter, M. Sembroski, G. H. Smith, A. Telezhinsky, I. Theiling, M. Toner, J. Tyler, J. Varlotta, A. Vivier, M. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Welsing, R. Williams, D. A. Wissel, S. TI Observation of Markarian 421 in TeV gamma rays over a 14-year time span SO ASTROPARTICLE PHYSICS LA English DT Article DE AGN; TeV gamma rays; Markarian 421 ID ACTIVE GALACTIC NUCLEI; MULTIWAVELENGTH OBSERVATIONS; CORRELATED VARIABILITY; BLAZAR MARKARIAN-421; TIMING EXPLORER; CRAB-NEBULA; ENERGY; TELESCOPE; EMISSION; FLARE AB The variability of the blazar Markarian 421 in TeV gamma rays over a 14-year time period has been explored with the Whipple 10 m telescope. It is shown that the dynamic range of its flux variations is large and similar to that in X-rays. A correlation between the X-ray and TeV energy bands is observed during some bright flares and when the complete data sets are binned on long timescales. The main database consists of 878.4 h of observation with the Whipple telescope, spread over 783 nights. The peak energy response of the telescope was 400 GeV with 20% uncertainty. This is the largest database of any TeV-emitting active galactic nucleus (AGN) and hence was used to explore the variability profile of Markarian 421. The tithe-averaged flux from Markarian 421 over this period was 0.446 +/- 0.008 Crab flux units. The flux exceeded 10 Crab flux units on three separate occasions. For the 2000-2001 season the average flux reached 1.86 Crab units, while in the 1996-1997 season the average flux was only 0.23 Crab units. (C) 2013 Elsevier B.V. All rights reserved. C1 [Acciari, V. A.; Moriarty, P.] Galway Mayo Inst Technol, Sch Sci, Galway, Ireland. [Acciari, V. A.; Benbow, W.; Galante, N.; Gibbs, K.; Roache, E.; Schroedter, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Arlen, T.; Ong, R. A.; Wissel, S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Bouvier, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Bouvier, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Bird, R.; Collins-Hughes, E.; Fegan, D. J.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Natl Univ Ireland Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Bradbury, S. M.] Univ Leeds, Dept Phys, Leeds LS2 9JT, Yorks, England. [Buckley, J. H.; Bugaev, V.; Krawczynski, H.; Ward, J. E.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [de la Calle Perez, I.] European Space Astron Ctr, Madrid 28080, Spain. [Carter-Lewis, D. A.; Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Cesarini, A.; Connolly, M. P.; Gillanders, G. H.; Lang, M. J.; Toner, J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Finley, J. P.; Gaidos, J.; Sembroski, G. H.; Theiling, M.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Dumm, J.; Fortson, L.; Nelson, T.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Federici, S.; Pohl, M.; Telezhinsky, I.; Welsing, R.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Federici, S.; Pohl, M.; Telezhinsky, I.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Fegan, S. J.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Riguet, F-91128 Palaiseau, France. [Finnegan, G.; Kieda, D.; Smith, A.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Gall, D.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Griffin, S.; Hanna, D.; Ragan, K.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Humensky, T. B.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [McEnery, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Otte, A. N.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Perkins, J. S.] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA. [Perkins, J. S.] NASA, Astroparticle Phys Lab, GSFC, Greenbelt, MD 20771 USA. [Perkins, J. S.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Petry, D.] ESO, ALMA Reg Ctr, D-85748 Garching, Germany. [Pichel, A.; Rovero, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. [Reynolds, T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Vivier, M.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Vivier, M.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. RP Weekes, TC (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. EM pat.moriarty@gmit.ie; weekes@veritas.sao.arizona.edu RI Khassen, Yerbol/I-3806-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610; Lang, Mark/0000-0003-4641-4201; Bird, Ralph/0000-0002-4596-8563 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U.K. FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748) and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instruments. NR 43 TC 11 Z9 11 U1 1 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 EI 1873-2852 J9 ASTROPART PHYS JI Astropart Phys. PD FEB PY 2014 VL 54 BP 1 EP 10 DI 10.1016/j.astropartphys.2013.10.004 PG 10 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AC3PW UT WOS:000332434700001 ER PT J AU Moon, JH Hirose, N AF Moon, Jae-Hong Hirose, Naoki TI Seasonal response of the southern East China Sea shelf water to wind-modulated throughflow in the Taiwan Strait SO PROGRESS IN OCEANOGRAPHY LA English DT Review ID KUROSHIO EAST; CONTINENTAL-SHELF; WARM CURRENT; TRANSPORT; INTRUSION; CURRENTS; SURFACE; YELLOW; MODEL AB Seasonal change of the southern East China Sea (ECS) shelf water and its relation to the throughflow in the Taiwan Strait (TS) was examined based on comparative experiments with inserting passive tracers into a regional ocean model. Through analyzing the model output results, we found that from autumn to winter strong northeasterly wind over the TS significantly weakens the outflow from the TS (i.e., flowing into the ECS) and the Kuroshio water intrudes farther shoreward across the northern shelf of Taiwan in response to the weakened outflow. On the other hand, water flowing into the shelf from the TS extends further offshore from spring to summer when the TS throughflow is enhanced by a wind change from northeasterly to southwesterly and the Kuroshio water retreats seaward off the shelf due to the offshore extension of the shelf water. It suggests that the weakening (strengthening) of the TS throughflow could allow (inhibit) shelf-ward Kuroshio water onto the northeastern shelf of Taiwan, emphasizing that the throughflow modulated by a local wind can be an important factor controlling the seasonal variation of the southern ECS shelf water. (c) 2013 Elsevier Ltd. All rights reserved. C1 [Moon, Jae-Hong; Hirose, Naoki] Kyushu Univ, Appl Mech Res Inst, Kasuga, Fukuoka 8168580, Japan. RP Moon, JH (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Jae-Hong.Moon@jpl.nasa.gov RI Kyushu, RIAM/F-4018-2015; U-ID, Kyushu/C-5291-2016; OI Hirose, Naoki/0000-0001-6234-8676 NR 32 TC 1 Z9 2 U1 0 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0079-6611 J9 PROG OCEANOGR JI Prog. Oceanogr. PD FEB PY 2014 VL 121 BP 74 EP 82 DI 10.1016/j.pocean.2013.11.009 PG 9 WC Oceanography SC Oceanography GA AC3OV UT WOS:000332432000006 ER PT J AU Pun, IF Lin, II Ko, DS AF Pun, Iam-Fei Lin, I. -I. Ko, Dong S. TI New generation of satellite-derived ocean thermal structure for the western north pacific typhoon intensity forecasting SO PROGRESS IN OCEANOGRAPHY LA English DT Review ID TROPICAL CYCLONE INTENSITY; SEA-SURFACE TEMPERATURE; RESOLUTION COUPLED MODEL; HEAT-CONTENT VARIABILITY; HURRICANE INTENSITY; SUBTROPICAL COUNTERCURRENT; NUMERICAL SIMULATIONS; ALTIMETRIC HEIGHT; STERIC HEIGHT; EDDY FIELD AB Ocean thermal structure is critical for the intensity change of tropical cyclones (TCs). It has been operationally derived from satellite altimetry for TC forecasting and research. The existing derivation is, however, based on a simple two-layer method; as a result, only two isotherms can be obtained to coarsely characterize the subsurface ocean thermal structure. Improvement on the vertical resolution to enhance ocean characterization is desirable for more accurately estimating ocean's energy supply for TC intensity change. In this study, we present a new generation of derivation to improve ocean's subsurface characterization for the Western North Pacific Ocean (WNPO) because this region has the highest TC occurrence on the Earth. In addition to the presently used two isotherms for the depths of 20 degrees C and 26 degrees C isotherms (D20 and D26), we derive continuous isotherms from D4 up to 029 (maximum 26 subsurface layers) to characterize the subsurface ocean thermal structure in detail. This is achieved through applying a large set (>38,000) of in situ Argo thermal profiles to regression development. A smaller set of in situ Argo profiles (>7000), independent of those used for regression, is utilized for validation, to assess the accuracy of the new derivation. The root-mean-square differences (RMSDs) between the derived and the in situ isotherms are found to be within 10-20 m for the upper isotherms (D20 to D29) and within similar to 40-60 m for the lower isotherms (D4 to 019). No significant biases of derived isotherms are found. In addition to increasing the vertical resolution from two layers to 26 layers, higher accuracy for the two isotherms of D20 and D26 is also achieved. For example, in the existing two-layer method, 020 in the northern WNPO is grossly overestimated with a high RMSD of similar to 80-100 m; the new method significantly reduces the RMSD to 20 m. Better subsurface characterization leads to improvement in important TC-intensity related parameters, like during-cyclone sea surface temperature (SST) cooling and airsea enthalpy flux supply. Based on a series of ocean mixed layer numerical experiments using 16 randomly-selected profiles, we find that the error in SST cooling (air-sea flux supply) can be reduced from 36% (120%) to 13% (20%). (c) 2013 Elsevier Ltd. All rights reserved. C1 [Pun, Iam-Fei; Lin, I. -I.] Natl Taiwan Univ, Dept Atmospher Sci, Taipei 106, Taiwan. [Pun, Iam-Fei] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. [Lin, I. -I.] Acad Sinica, Res Ctr Environm Changes, Taipei 115, Taiwan. [Ko, Dong S.] Naval Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS USA. RP Lin, II (reprint author), Natl Taiwan Univ, Dept Atmospher Sci, 1,Sec 4,Roosevelt Rd, Taipei 106, Taiwan. EM iilin@as.ntu.edu.tw RI Lin, I-I/J-4695-2013 OI Lin, I-I/0000-0002-8364-8106 FU NSC [102-2811-M-002095, 101-2111-M-002-002-MY2, NSC 101-2628-M-002-001-MY4]; ONR [N00014-11-1-0394]; ONR ITOP program [N00014-08WX-2-1170] FX The authors appreciate the Argo team for the in situ temperature profiles, the AVISO team for the SSHA data, the RSS team for the SST data, and the NOAA/NODC for the climatological ocean temperature data. The authors sincerely thank Dr. Jim Price of Woods Hole Oceanographic Institution (WHOI) and three anonymous reviewers for their valuable comments and suggestions. With their helps, this work is able to be accomplished. Thanks also to US Office of Naval Research (ONR) and WHOI, part of this work was done when lam-Fei Pun was working at WHOI, supported by ONR. Iam-Fei Pun is supported by Grants NSC 102-2811-M-002095 and ONR N00014-11-1-0394. I.-I. Lin is supported by Grants NSC 101-2111-M-002-002-MY2 and NSC 101-2628-M-002-001-MY4. Dong S. Ko is supported by ONR ITOP program under Contract N00014-08WX-2-1170. NR 67 TC 9 Z9 9 U1 2 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0079-6611 J9 PROG OCEANOGR JI Prog. Oceanogr. PD FEB PY 2014 VL 121 BP 109 EP 124 DI 10.1016/j.pocean.2013.10.004 PG 16 WC Oceanography SC Oceanography GA AC3OV UT WOS:000332432000010 ER PT J AU Garrett, HB Whittlesey, AC AF Garrett, Henry B. Whittlesey, Albert C. TI 2014 Spacecraft Charging Technology Conference (2014 SCTC), 23-27 June 2014 SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE spacecraft charging; space weather; spacecraft interactions AB Key Points Announcement of 13th international Spacecraft Charging Technology Conference Website for abstracts and registration is open Contact authors if there are any questions C1 [Garrett, Henry B.; Whittlesey, Albert C.] CALTECH, Jet Prop Lab, Off Safety & Mission Success, Pasadena, CA 91125 USA. RP Garrett, HB (reprint author), CALTECH, Jet Prop Lab, Off Safety & Mission Success, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM Henry.B.Garrett@jpl.nasa.gov; Albert.Whittlesey@jpl.nasa.gov NR 0 TC 0 Z9 0 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD FEB PY 2014 VL 12 IS 2 BP 111 EP 111 DI 10.1002/2014SW001037 PG 1 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AD1HU UT WOS:000332985800001 ER PT J AU Joyce, CJ Schwadron, NA Wilson, JK Spence, HE Kasper, JC Golightly, M Blake, JB Townsend, LW Case, AW Semones, E Smith, S Zeitlin, CJ AF Joyce, C. J. Schwadron, N. A. Wilson, J. K. Spence, H. E. Kasper, J. C. Golightly, M. Blake, J. B. Townsend, L. W. Case, A. W. Semones, E. Smith, S. Zeitlin, C. J. TI Radiation modeling in the Earth and Mars atmospheres using LRO/CRaTER with the EMMREM Module SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE radiation; modulation potential; galactic cosmic rays AB We expand upon the efforts of Joyce et al. (2013), who computed the modulation potential at the Moon using measurements from the Cosmic Ray Telescope for the Effects of Radiation (CRaTER) instrument on the Lunar Reconnaissance Orbiter (LRO) spacecraft along with data products from the Earth-Moon-Mars Radiation Environment Module (EMMREM). Using the computed modulation potential, we calculate galactic cosmic ray (GCR) dose and dose equivalent rates in the Earth and Mars atmospheres for various altitudes over the course of the LRO mission. While we cannot validate these predictions by directly comparable measurement, we find that our results conform to expectations and are in good agreement with the nearest available measurements and therefore may be used as reasonable estimates for use in efforts in risk assessment in the planning of future space missions as well as in the study of GCRs. PREDICCS (Predictions of radiation from REleASE, EMMREM, and Data Incorporating the CRaTER, COSTEP, and other solar energetic particles measurements) is an online system designed to provide the scientific community with a comprehensive resource on the radiation environments of the inner heliosphere. The data products shown here will be incorporated into PREDICCS in order to further this effort and daily updates will be made available on the PREDICCS website (http://prediccs.sr.unh.edu). C1 [Joyce, C. J.; Schwadron, N. A.; Wilson, J. K.; Spence, H. E.; Golightly, M.; Smith, S.] Univ New Hampshire, Ctr Space Sci, Dept Phys, Durham, NH 03824 USA. [Kasper, J. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Blake, J. B.] Aerosp Corp, Los Angeles, CA 90009 USA. [Townsend, L. W.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA. [Case, A. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Semones, E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Zeitlin, C. J.] Southwest Res Inst, Boulder, CO USA. RP Joyce, CJ (reprint author), Univ New Hampshire, Ctr Space Sci, Dept Phys, Durham, NH 03824 USA. EM cjl46@unh.edu OI Spence, Harlan/0000-0002-2526-2205 FU NASA LRO/CRaTER/PREDICCS Project [NNG11PA03C]; NSF/FESD Sun-to-Ice Project [AGS1135432]; NASA/LWS/NSF EMMREM Project [NNX11AC06G] FX Thanks to everyone on the CRaTER team for their help and guidance. This work is supported by NASA LRO/CRaTER/PREDICCS Project (contract NNG11PA03C), the NSF/FESD Sun-to-Ice Project (grant AGS1135432), and the NASA/LWS/NSF EMMREM Project (grant NNX11AC06G). NR 10 TC 3 Z9 3 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD FEB PY 2014 VL 12 IS 2 BP 112 EP 119 DI 10.1002/2013SW000997 PG 8 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AD1HU UT WOS:000332985800002 ER PT J AU Mertens, CJ Meier, MM AF Mertens, Christopher J. Meier, Matthias M. TI Reply to comment by Socol et al. on " NAIRAS aircraft radiation model development, dose climatology, and initial validation" SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Editorial Material DE cosmic radiation C1 [Mertens, Christopher J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Meier, Matthias M.] DLR German Aerosp Ctr, Inst Aerosp Med, Cologne, Germany. RP Mertens, CJ (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM christopher.j.mertens@nasa.gov OI Meier, Matthias/0000-0003-0918-6473 NR 0 TC 1 Z9 1 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD FEB PY 2014 VL 12 IS 2 BP 122 EP 122 DI 10.1002/2014SW001034 PG 1 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AD1HU UT WOS:000332985800004 ER PT J AU Kim, BR Ham, SH Kim, D Sohn, BJ AF Kim, Bo-Ra Ham, Seung-Hee Kim, Dohyeong Sohn, Byung-Ju TI Post-flight radiometric calibration of the Korean geostationary satellite COMS meteorological imager SO ASIA-PACIFIC JOURNAL OF ATMOSPHERIC SCIENCES LA English DT Article DE COMS MI; calibration status; vicarious calibration; inter-satellite calibration ID BULK SCATTERING PROPERTIES; ICE CLOUDS; PART II; MODIS; MTSAT-1R; BIAS; TARGETS; MODELS AB The first Korean geostationary satellite, the Communication, Ocean, Meteorological Satellite (COMS) carries the Meteorological Imager (MI) that measures solar radiance at 0.675 mu m and infrared (IR) brightness temperatures at four spectral bands centered at 3.8, 6.7, 10.8, and 12.0 mu m. This study reports the calibration status of the COMS MI solar and four IR channels, based mainly on a comparison with Moderate Resolution Imaging Spectroradiometer (MODIS) measurements. The results obtained from four months of COMS MI solar channel measurements demonstrate that the solar channel has a dark bias of about 9-10%. On the other hand, the four IR channels appear to be well-calibrated as evidenced by a high correlation and near-unity slope between COMS and MODIS data. Nevertheless, existing biases of tenths of a kelvin are still considered to be substantial. Overall, the interpretation of COMS-derived meteorological products should take into account some uncertainty caused by possible calibration errors. C1 [Kim, Bo-Ra; Sohn, Byung-Ju] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul 151747, South Korea. [Ham, Seung-Hee] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Kim, Dohyeong] Natl Meteorol Satellite Center, KMA, Jincheon, South Korea. RP Sohn, BJ (reprint author), Seoul Natl Univ, Sch Earth & Environm Sci, 1 Gwanak Ro, Seoul 151747, South Korea. EM sohn@snu.ac.kr FU Korea Meteorological Administration Research and Development Program [CATER 2012-2092] FX We convey our sincere thanks to two anonymous reviewers whose comments helped to improve the manuscript. This work was funded by the Korea Meteorological Administration Research and Development Program under Grant CATER 2012-2092. NR 23 TC 4 Z9 4 U1 1 U2 1 PU KOREAN METEOROLOGICAL SOC PI SEOUL PA SHINKIL-DONG 508, SIWON BLDG 704, YONGDUNGPO-GU, SEOUL, 150-050, SOUTH KOREA SN 1976-7633 EI 1976-7951 J9 ASIA-PAC J ATMOS SCI JI Asia-Pac. J. Atmos. Sci. PD FEB PY 2014 VL 50 IS 2 BP 201 EP 210 DI 10.1007/s13143-014-0008-7 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AC4JZ UT WOS:000332488500007 ER PT J AU Jones, CE Blom, RG AF Jones, Cathleen E. Blom, Ronald G. TI Bayou Corne, Louisiana, sinkhole: Precursory deformation measured by radar interferometry SO GEOLOGY LA English DT Article AB Catastrophic sinkholes are formed through the collapse of natural or human-made subterranean caverns, and are common in areas with evaporite and carbonate rock. Despite their danger, advance warning of these events is rare. We report a measurement of precursory surface deformation of as much as 260 mm, derived with interferometric synthetic aperture radar (InSAR) and evident over a month before surface collapse, at the site of the Bayou Corne, Louisiana (USA) sinkhole that formed in August 2012. Data collected by the airborne Uninhabited Aerial Vehicle SAR (UAVSAR) instrument were used for the study. Analysis of data acquired from two flight tracks with near-opposing imaging geometries reveal a deformation pattern consistent with compressive loading at the surface due to loss of support from a subterranean cavity collapse related to Texas Brine Oxy Geismar Well #3. The precursor deformation was nearly entirely horizontal, i.e., oriented along the surface, and manifested as movement of surface material toward the location where the sinkhole later formed. The sinkhole formed in the area with the largest gradient in surface strain, but did not cover the full extent of the precursory deformation detected with radar. This work suggests that InSAR data collected operationally for hazard monitoring could, in some cases, identify sinkhole development before surface collapse, and decrease subsequent danger to people and property. C1 [Jones, Cathleen E.; Blom, Ronald G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Jones, CE (reprint author), CALTECH, Jet Prop Lab, MS 300-319,4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 21 TC 7 Z9 7 U1 0 U2 17 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 EI 1943-2682 J9 GEOLOGY JI Geology PD FEB PY 2014 VL 42 IS 2 BP 111 EP 114 DI 10.1130/G34972.1 PG 4 WC Geology SC Geology GA AD4TO UT WOS:000333243700006 ER PT J AU Misra, A Meadows, V Claire, M Crisp, D AF Misra, Amit Meadows, Victoria Claire, Mark Crisp, Dave TI Using Dimers to Measure Biosignatures and Atmospheric Pressure for Terrestrial Exoplanets SO ASTROBIOLOGY LA English DT Article ID NEAR-INFRARED OBSERVATIONS; HUBBLE-SPACE-TELESCOPE; GIANT PLANET TRANSITS; EARTH-LIKE PLANETS; TRANSMISSION SPECTRUM; EXTRASOLAR PLANET; WATER-VAPOR; ABSORPTION; OXYGEN; SPECTROSCOPY AB We present a new method to probe atmospheric pressure on Earth-like planets using (O-2-O-2) dimers in the near-infrared. We also show that dimer features could be the most readily detectable biosignatures for Earth-like atmospheres and may even be detectable in transit transmission with the James Webb Space Telescope (JWST). The absorption by dimers changes more rapidly with pressure and density than that of monomers and can therefore provide additional information about atmospheric pressures. By comparing the absorption strengths of rotational and vibrational features to the absorption strengths of dimer features, we show that in some cases it may be possible to estimate the pressure at the reflecting surface of a planet. This method is demonstrated by using the O-2 A band and the 1.06 mu m dimer feature, either in transmission or reflected spectra. It works best for planets around M dwarfs with atmospheric pressures between 0.1 and 10 bar and for O-2 volume mixing ratios above 50% of Earth's present-day level. Furthermore, unlike observations of Rayleigh scattering, this method can be used at wavelengths longer than 0.6 mu m and is therefore potentially applicable, although challenging, to near-term planet characterization missions such as JWST. We also performed detectability studies for JWST transit transmission spectroscopy and found that the 1.06 and 1.27 mu m dimer features could be detectable (SNR>3) for an Earth analogue orbiting an M5V star at a distance of 5 pc. The detection of these features could provide a constraint on the atmospheric pressure of an exoplanet and serve as biosignatures for oxygenic photosynthesis. We calculated the required signal-to-noise ratios to detect and characterize O-2 monomer and dimer features in direct imaging-reflected spectra and found that signal-to-noise ratios greater than 10 at a spectral resolving power of R=100 would be required. Key Words: Remote sensing-Extrasolar terrestrial planets-Habitability-Radiative transfer-Biosignatures. Astrobiology 14, 67-86. C1 [Misra, Amit; Meadows, Victoria] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Misra, Amit; Meadows, Victoria; Claire, Mark; Crisp, Dave] NAI Virtual Planetary Lab, Seattle, WA USA. [Misra, Amit; Meadows, Victoria] Univ Washington, Astrobiol Program, Seattle, WA 98195 USA. [Claire, Mark] Univ St Andrews, Dept Earth & Environm Sci, St Andrews KY16 9AJ, Fife, Scotland. [Claire, Mark] Blue Marble Space Inst Sci, Seattle, WA USA. [Crisp, Dave] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Misra, A (reprint author), Univ Washington, Box 351580, Seattle, WA 98195 USA. EM amit0@astro.washington.edu FU National Aeronautics and Space Administration through the NASA Astrobiology Institute [NNH05ZDA001C]; ARCS; Astrobiology Program at the University of Washington under an NSF IGERT award FX This work was performed by the NASA Astrobiology Institute's Virtual Planetary Laboratory, supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement solicitation NNH05ZDA001C. This work has also been supported by a generous fellowship from the ARCS Seattle chapter and funding from the Astrobiology Program at the University of Washington under an NSF IGERT award. NR 52 TC 22 Z9 22 U1 2 U2 16 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD FEB 1 PY 2014 VL 14 IS 2 BP 67 EP 86 DI 10.1089/ast.2013.0990 PG 20 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AB0CY UT WOS:000331460600001 PM 24432758 ER PT J AU Cook, AM Mattioda, AL Ricco, AJ Quinn, RC Elsaesser, A Ehrenfreund, P Ricca, A Jones, NC Hoffmann, SV AF Cook, Amanda M. Mattioda, Andrew L. Ricco, Antonio J. Quinn, Richard C. Elsaesser, Andreas Ehrenfreund, Pascale Ricca, Alessandra Jones, Nykola C. Hoffmann, Soren V. TI The Organism/Organic Exposure to Orbital Stresses (O/OREOS) Satellite: Radiation Exposure in Low-Earth Orbit and Supporting Laboratory Studies of Iron Tetraphenylporphyrin Chloride SO ASTROBIOLOGY LA English DT Article ID SPACE ENVIRONMENT VIABILITY; CIRCULAR-DICHROISM; OPTICAL-ABSORPTION; DIATOMIC IRON; SOLID ARGON; THIN-FILMS; MISSION; COMPLEXES; SEVO; SPECTROSCOPY AB We report results from the exposure of the metalloporphyrin iron tetraphenylporphyrin chloride (FeTPPCl) to the outer space environment, measured in situ aboard the Organism/Organic Exposure to Orbital Stresses nanosatellite. FeTPPCl was exposed for a period of 17 months (3700 h of direct solar exposure), which included broad-spectrum solar radiation (similar to 122 nm to the near infrared). Motivated by the potential role of metalloporphyrins as molecular biomarkers, the exposure of thin-film samples of FeTPPCl to the space environment in low-Earth orbit was monitored in situ via ultraviolet/visible spectroscopy and reported telemetrically. The space data were complemented by laboratory exposure experiments that used a high-fidelity solar simulator covering the spectral range of the spaceflight measurements. We found that thin-film samples of FeTPPCl that were in contact with a humid headspace gas (0.8-2.3% relative humidity) were particularly susceptible to destruction upon irradiation, degrading up to 10 times faster than identical thin films in contact with dry headspace gases; this degradation may also be related to the presence of oxides of nitrogen in those cells. In the companion terrestrial experiments, simulated solar exposure of FeTPPCl films in contact with either Ar or CO2:O-2:Ar (10:0.01:1000) headspace gas resulted in growth of a band in the films' infrared spectra at 1961 cm(-1). We concluded that the most likely carriers of this band are allene (C3H4) and chloropropadiene (C3H3Cl), putative molecular fragments of the destruction of the porphyrin ring. The thin films studied in space and in solar simulator-based experiments show qualitatively similar spectral evolution as a function of contacting gaseous species but display significant differences in the time dependence of those changes. The relevance of our findings to planetary science, biomarker research, and the photostability of organic materials in astrobiologically relevant environments is discussed. Key Words: Astrobiology-Spectroscopy-Low-Earth orbit-Organic matter-UV radiation. Astrobiology 14, 87-101. C1 [Cook, Amanda M.; Mattioda, Andrew L.; Ricco, Antonio J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Quinn, Richard C.; Ricca, Alessandra] SETI Inst, Mountain View, CA USA. [Elsaesser, Andreas] Leiden Univ, Leiden, Netherlands. [Ehrenfreund, Pascale] George Washington Univ, Inst Space Policy, Washington, DC 20052 USA. [Jones, Nykola C.; Hoffmann, Soren V.] Aarhus Univ, Dept Phys & Astron, ISA, Aarhus, Denmark. RP Cook, AM (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA. EM amanda.m.cook@nasa.gov RI Elsaesser, Andreas/K-2264-2014; OI Ricco, Antonio/0000-0002-2355-4984 FU NASA; Exobiology Program [09-EXOB09-1030] FX The authors would like to thank the NASA Astrobiology Small Payloads program for support, Robert Walker for technical support, Emmett Quigley and Ryan Walker of the NASA Ames Airborne Instrument Development Lab for their work in producing the hardware necessary for the production of the sample cells and the glove box experiment. We thank Dr. El-Nahass at Ain Shams University for useful discussion regarding the nature of our porphyrin spectra. The authors also thank the NASA Astrobiology Institute, the NASA Postdoctoral Program (NPP) administered by Oak Ridge Associated Universities through a contract with NASA, and the Exobiology Program for additional support (proposal number 09-EXOB09-1030). We also thank Cindy Taylor for assistance with deposition and characterization of the thin films, and members of the NASA Ames Small Spacecraft Payloads and Technologies Team. We are also grateful for the efforts of the highly effective student-and-staff O/OREOS mission operations team at Santa Clara University. NR 31 TC 4 Z9 4 U1 0 U2 12 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD FEB 1 PY 2014 VL 14 IS 2 BP 87 EP 101 DI 10.1089/ast.2013.0998 PG 15 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AB0CY UT WOS:000331460600002 PM 24512475 ER PT J AU Heldmann, JL Schurmeier, L McKay, C Davila, A Stoker, C Marinova, M Wilhelm, MB AF Heldmann, J. L. Schurmeier, L. McKay, C. Davila, A. Stoker, C. Marinova, M. Wilhelm, M. B. TI Midlatitude Ice-Rich Ground on Mars as a Target in the Search for Evidence of Life and for in situ Resource Utilization on Human Missions SO ASTROBIOLOGY LA English DT Article ID LANDING SITE; GLOBAL DISTRIBUTION; SUBSURFACE ICE; NEAR-SURFACE; STABILITY; EXPLORATION; PERMAFROST; WATER; HYDROGEN; BEHAVIOR AB Midlatitude ground ice on Mars is of significant scientific interest for understanding the history and evolution of ice stability on Mars and is relevant for human exploration as a possible in situ resource. For both science and exploration, assessing the astrobiological potential of the ice is important in terms of (1) understanding the potential for life on Mars and (2) evaluating the presence of possible biohazards in advance of human exploration. In the present study, we review the evidence for midlatitude ground ice on Mars, discuss the possible explanations for its occurrence, and assess its potential habitability. During the course of study, we systematically analyzed remote-sensing data sets to determine whether a viable landing site exists in the northern midlatitudes to enable a robotic mission that conducts in situ characterization and searches for evidence of life in the ice. We classified each site according to (1) presence of polygons as a proxy for subsurface ice, (2) presence and abundance of rough topographic obstacles (e.g., large cracks, cliffs, uneven topography), (3) rock density, (4) presence and abundance of large boulders, and (5) presence of craters. We found that a suitable landing site exists within Amazonis Planitia near ground ice that was recently excavated by a meteorite impact. Key Words: Mars-Missions-Habitability-Landing sites-Ice. Astrobiology 14, 102-118. C1 [Heldmann, J. L.; Schurmeier, L.; McKay, C.; Davila, A.; Stoker, C.; Marinova, M.; Wilhelm, M. B.] NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94043 USA. [Schurmeier, L.] Univ Illinois, Dept Earth & Environm Sci, Chicago, IL USA. [Davila, A.] SETI Inst, Mountain View, CA USA. [Marinova, M.] Bay Area Environm Res Inst, Sonoma, CA USA. [Wilhelm, M. B.] Georgia Inst Technol, Atlanta, GA 30332 USA. RP Heldmann, JL (reprint author), NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94043 USA. EM Jennifer.Heldmann@nasa.gov RI Davila, Alfonso/A-2198-2013 OI Davila, Alfonso/0000-0002-0977-9909 NR 61 TC 3 Z9 3 U1 5 U2 20 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD FEB 1 PY 2014 VL 14 IS 2 BP 102 EP 118 DI 10.1089/ast.2013.1103 PG 17 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AB0CY UT WOS:000331460600003 PM 24506507 ER PT J AU Nuevo, M Chen, YJ Hu, WJ Qiu, JM Wu, SR Fung, HS Chu, CC Yih, TS Ip, WH Wu, CYR AF Nuevo, Michel Chen, Yu-Jung Hu, Wei-Jie Qiu, Jun-Ming Wu, Shang-Ruei Fung, Hok-Sum Chu, Ching-Chi Yih, Tai-Sone Ip, Wing-Huen Wu, C. -Y. Robert TI Irradiation of Pyrimidine in Pure H2O Ice with High-Energy Ultraviolet Photons SO ASTROBIOLOGY LA English DT Article ID POLYCYCLIC AROMATIC-HYDROCARBONS; INFRARED SPECTRAL PROPERTIES; CARBONACEOUS METEORITES; MURCHISON METEORITE; HETEROCYCLIC-COMPOUNDS; INTERSTELLAR ICE; BUTYLDIMETHYLSILYL DERIVATIVES; EXTRATERRESTRIAL NUCLEOBASES; PREBIOTIC MOLECULES; PROTON IRRADIATION AB The detection of nucleobases, the informational subunits of DNA and RNA, in several meteorites suggests that these compounds of biological interest were formed via astrophysical, abiotic processes. This hypothesis is in agreement with recent laboratory studies of irradiation of pyrimidine in H2O-rich ices with vacuum UV photons emitted by an H-2-discharge lamp in the 6.9-11.3 eV (110-180 nm) range at low temperature, shown to lead to the abiotic formation of several compounds including the nucleobases uracil, cytosine, and thymine. In this work, we irradiated H2O:pyrimidine ice mixtures under astrophysically relevant conditions (14 K, <= 10(-9) torr) with high-energy UV photons provided by a synchrotron source in three different ranges: the 0(th) order light (4.1-49.6 eV, 25-300 nm), the He i line (21.2 eV, 58.4 nm), and the He ii line (40.8 eV, 30.4 nm). The photodestruction of pyrimidine was monitored with IR spectroscopy, and the samples recovered at room temperature were analyzed with liquid and gas chromatographies. Uracil and its precursor 4(3H)-pyrimidone were found in all samples, with absolute and relative abundances varying significantly from one sample to another. These results support a scenario in which compounds of biological interest can be formed and survive in environments subjected to high-energy UV radiation fields. Key Words: Pyrimidine-Nucleobases-Interstellar ices-Cometary ices-High-energy photons-Molecular processes-Prebiotic chemistry. Astrobiology 14, 119-131. C1 [Nuevo, Michel] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Nuevo, Michel] SETI Inst, Mountain View, CA USA. [Chen, Yu-Jung; Wu, C. -Y. Robert] Univ So Calif, Ctr Space Sci, Los Angeles, CA 90089 USA. [Chen, Yu-Jung; Wu, C. -Y. Robert] Univ So Calif, Dept Phys & Astron, Los Angeles, CA USA. [Chen, Yu-Jung; Hu, Wei-Jie; Qiu, Jun-Ming; Wu, Shang-Ruei; Chu, Ching-Chi; Yih, Tai-Sone] Natl Cent Univ, Dept Phys, Jhongli, Taiwan. [Fung, Hok-Sum] Natl Synchrotron Radiat Res Ctr, Hsinchu, Taiwan. [Ip, Wing-Huen] Natl Cent Univ, Grad Inst Astron, Jhongli, Taiwan. RP Nuevo, M (reprint author), NASA, Ames Res Ctr, Div Space Sci, MS 245-6, Moffett Field, CA 94035 USA. EM michel.nuevo-1@nasa.gov FU NSC [99-2112-M-008-011-MY3, 101-2811-M-008-023]; National Synchrotron Radiation Research Center; NSF [AST-1108898] FX This work was supported by the NSC grants #99-2112-M-008-011-MY3 and #101-2811-M-008-023 (T.-S.Y.), the National Synchrotron Radiation Research Center, and the NSF Planetary Astronomy Program under grant AST-1108898 (C.-Y.R.W.). M.N. acknowledges S. A. Sandford for the use of the HPLC and GC-MS devices at the Astrophysics & Astrochemistry Laboratory of NASA Ames Research Center. The authors are grateful for the helpful reviews of two anonymous reviewers, from which this manuscript benefited significantly. NR 75 TC 4 Z9 4 U1 0 U2 12 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD FEB 1 PY 2014 VL 14 IS 2 BP 119 EP 131 DI 10.1089/ast.2013.1093 PG 13 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AB0CY UT WOS:000331460600004 PM 24512484 ER PT J AU Nunez, JI Farmer, JD Sellar, RG Swayze, GA Blaney, DL AF Nunez, Jorge I. Farmer, Jack D. Sellar, R. Glenn Swayze, Gregg A. Blaney, Diana L. TI Science Applications of a Multispectral Microscopic Imager for the Astrobiological Exploration of Mars SO ASTROBIOLOGY LA English DT Review ID RESOLUTION REFLECTANCE SPECTROSCOPY; REMOTE-SENSING IMPLICATIONS; OMEGA/MARS EXPRESS; IRON-OXIDES; SPECTRAL CHARACTERISTICS; SPECTROMETER DATA; MERIDIANI-PLANUM; MARTIAN SURFACE; MINERALS; OLIVINE AB Future astrobiological missions to Mars are likely to emphasize the use of rovers with in situ petrologic capabilities for selecting the best samples at a site for in situ analysis with onboard lab instruments or for caching for potential return to Earth. Such observations are central to an understanding of the potential for past habitable conditions at a site and for identifying samples most likely to harbor fossil biosignatures. The Multispectral Microscopic Imager (MMI) provides multispectral reflectance images of geological samples at the microscale, where each image pixel is composed of a visible/shortwave infrared spectrum ranging from 0.46 to 1.73 mu m. This spectral range enables the discrimination of a wide variety of rock-forming minerals, especially Fe-bearing phases, and the detection of hydrated minerals. The MMI advances beyond the capabilities of current microimagers on Mars by extending the spectral range into the infrared and increasing the number of spectral bands. The design employs multispectral light-emitting diodes and an uncooled indium gallium arsenide focal plane array to achieve a very low mass and high reliability. To better understand and demonstrate the capabilities of the MMI for future surface missions to Mars, we analyzed samples from Mars-relevant analog environments with the MMI. Results indicate that the MMI images faithfully resolve the fine-scale microtextural features of samples and provide important information to help constrain mineral composition. The use of spectral endmember mapping reveals the distribution of Fe-bearing minerals (including silicates and oxides) with high fidelity, along with the presence of hydrated minerals. MMI-based petrogenetic interpretations compare favorably with laboratory-based analyses, revealing the value of the MMI for future in situ rover-mediated astrobiological exploration of Mars. Key Words: Mars-Microscopic imager-Multispectral imaging-Spectroscopy-Habitability-Arm instrument. Astrobiology 14, 132-169. C1 [Nunez, Jorge I.; Farmer, Jack D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Sellar, R. Glenn; Blaney, Diana L.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Swayze, Gregg A.] US Geol Survey, Denver, CO 80225 USA. RP Nunez, JI (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM jorge.nunez@jhuapl.edu RI Nunez, Jorge/J-4027-2015 OI Nunez, Jorge/0000-0003-0930-6674 FU NASA; National Geographic Society (NGS); NASA Astrobiology Institute (NAI); American Philosophical Society (AMS) FX Development of the MMI and analysis of MMI data sets were carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology, and at Arizona State University (ASU), under contracts with the National Aeronautics and Space Administration (NASA). Laboratory analysis of test samples was carried out at ASU and the U. S. Geological Survey (USGS) in Denver, Colorado. This research was supported by grants from NASA's Moon and Mars Analog Mission Activities (MMAMA) Program (2008; 2011-2012); the NASA Mars Instrument Development Program (MIDP; 2008-2010); the NASA-JPL Director's Discretionary Fund (2007-2008); and NASA's Astrobiology Science Technology Instrumentation Development (ASTID) Program (2005-2007). Support for J.I. Nunez was provided by a doctoral fellowship from the NASA Earth and Space Science Fellowship (NESSF) program, a Young Explorers Grant from the National Geographic Society (NGS), and a Lewis and Clark Fellowship in Astrobiology from the NASA Astrobiology Institute (NAI) and the American Philosophical Society (AMS). We are grateful to Charles Sarture, Paul Gardner, and Andrew Kieta at JPL for their assistance with development of the MMI, and Vicki Mills at ASU for assistance with preparation of test samples and preliminary analysis of XRD results. We also thank Neil Pearson and an anonymous reviewer for helpful reviews and comments that improved this manuscript. NR 111 TC 1 Z9 1 U1 0 U2 17 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD FEB 1 PY 2014 VL 14 IS 2 BP 132 EP 169 DI 10.1089/ast.2013.1079 PG 38 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AB0CY UT WOS:000331460600005 PM 24552233 ER PT J AU White, LM Gibson, EK Thomas-Keprta, KL Clemett, SJ McKay, DS AF White, Lauren M. Gibson, Everett K. Thomas-Keprta, Kathie L. Clemett, Simon J. McKay, David S. TI Putative Indigenous Carbon-Bearing Alteration Features in Martian Meteorite Yamato 000593 SO ASTROBIOLOGY LA English DT Article ID AQUEOUS ALTERATION; CHASSIGNY METEORITE; CALCIUM-CARBONATE; ORGANIC-COMPOUNDS; ISOTOPIC EVIDENCE; VOLCANIC GLASS; MARS; NAKHLA; IDDINGSITE; LAFAYETTE AB We report the first observation of indigenous carbonaceous matter in the martian meteorite Yamato 000593. The carbonaceous phases are heterogeneously distributed within secondary iddingsite alteration veins and present in a range of morphologies including areas composed of carbon-rich spheroidal assemblages encased in multiple layers of iddingsite. We also observed microtubular features emanating from iddingsite veins penetrating into the host olivine comparable in shape to those interpreted to have formed by bioerosion in terrestrial basalts. Key Words: Meteorite-Yamato 000593-Mars-Carbon. Astrobiology 14, 170-181. C1 [White, Lauren M.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Gibson, Everett K.; McKay, David S.] NASA, Lyndon B Johnson Space Ctr, KR, Houston, TX 77058 USA. [Thomas-Keprta, Kathie L.; Clemett, Simon J.] Jacobs Engn, ESCG, Houston, TX USA. RP White, LM (reprint author), NASA, Jet Prop Lab, Mail Stop 321-451,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM lauren.spencer@jpl.nasa.gov NR 92 TC 5 Z9 5 U1 2 U2 12 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD FEB 1 PY 2014 VL 14 IS 2 BP 170 EP 181 DI 10.1089/ast.2011.0733 PG 12 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AB0CY UT WOS:000331460600006 PM 24552234 ER PT J AU Gruenthal, KM Witting, DA Ford, T Neuman, MJ Williams, JP Pondella, DJ Bird, A Caruso, N Hyde, JR Seeb, LW Larson, WA AF Gruenthal, K. M. Witting, D. A. Ford, T. Neuman, M. J. Williams, J. P. Pondella, D. J., II Bird, A. Caruso, N. Hyde, J. R. Seeb, L. W. Larson, W. A. TI Development and application of genomic tools to the restoration of green abalone in southern California SO CONSERVATION GENETICS LA English DT Article DE Abalone; Genomics; Population genetics; Restriction site associated DNA sequencing; Single nucleotide polymorphism; Stock enhancement ID EFFECTIVE POPULATION-SIZE; MICROSATELLITE DNA MARKERS; MULTILOCUS GENOTYPE DATA; HALIOTIS-CRACHERODII LEACH; WESTSLOPE CUTTHROAT TROUT; HATCHERY-PRODUCED ABALONE; GENETIC-STRUCTURE; NATURAL-POPULATIONS; BLACK ABALONE; STOCK ENHANCEMENT AB Due to severe declines in abundance throughout southern California, the green abalone (Haliotis fulgens Philippi 1845) became protected under a state-sponsored fishery moratorium in 1997 and was declared a NOAA NMFS Species of Concern in 2004. Recently, H. fulgens was chosen for possible stock restoration via translocation of wild adults to depleted habitat and supplementation through releasing cultured individuals. Before a management plan could be developed, however, an understanding of the species' natural population genetic structure was needed. We used a genomic technique called restriction site associated DNA sequencing (RADSeq) to address the issue. RADSeq enabled discovery of 1,209 single nucleotide polymorphisms theoretically spread genome-wide in H. fulgens. Analyses suggested the species may be panmictic throughout our sampled range, with an effective population size (N-e) of 1,100-3,600. Hence, limitations to management, such as requiring local broodstock and restricting translocation potential, might be unnecessary. Sites with larger populations may be suitable sources for restoration of depleted sites (e.g. the Palos Verdes Peninsula), although the extent of local adaptation remains unknown. Despite this potential for restoration, results gathered on a sample of cultured H. fulgens illustrated how quickly genetic diversity can be lost through captive breeding. To help mitigate a drop in Ne due to hatchery supplementation, we recommend collection and replacement of >= 100 wild abalone per generation for broodstock and close management of the proportion of cultured individuals in the wild. Successful implementation will depend on operational capacity and the resilience of the source populations to broodstock collection. C1 [Gruenthal, K. M.] Hubbs SeaWorld Res Inst, San Diego, CA 92109 USA. [Gruenthal, K. M.] NOAA, Conservat Biol Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Seattle, WA 98112 USA. [Witting, D. A.] NOAA, Restorat Ctr, Off Habitat Conservat, Natl Marine Fisheries Serv, Long Beach, CA 90802 USA. [Ford, T.] Santa Monica Bay Restorat Fdn, Los Angeles, CA 90045 USA. [Neuman, M. J.] NOAA, Protected Resources Div, Southwest Reg Off, Natl Marine Fisheries Serv, Long Beach, CA 90802 USA. [Williams, J. P.; Pondella, D. J., II] Occidental Coll, Vantuna Res Grp, Moore Lab, Los Angeles, CA 90041 USA. [Bird, A.] Orange Cty Coastkeeper, Costa Mesa, CA 92626 USA. [Caruso, N.] Get Inspired Inc, Garden Grove, CA 92845 USA. [Hyde, J. R.] NOAA, Fisheries Resources Div, Southwest Fisheries Sci Ctr, Natl Marine Fisheries Serv, La Jolla, CA 92037 USA. [Seeb, L. W.; Larson, W. A.] Univ Washington, Sch Aquat & Fisheries Sci, Seattle, WA 98105 USA. RP Gruenthal, KM (reprint author), Hubbs SeaWorld Res Inst, 2595 Ingraham St, San Diego, CA 92109 USA. EM kgruenthal@hswri.org FU U.S. Department of Commerce's National Oceanic and Atmospheric Administration (NOAA); Office of Aquaculture Research Tiger Team Internal Grant; National Science Foundation Graduate Research Fellowship Grant [DGE-0718124] FX This work was supported by the U.S. Department of Commerce's National Oceanic and Atmospheric Administration (NOAA) under a Species of Concern Internal Grant awarded to Ford et al. and an Office of Aquaculture Research Tiger Team Internal Grant awarded to Dr. Hyde. Wesley Larson was supported by a National Science Foundation Graduate Research Fellowship Grant # DGE-0718124. The views expressed herein do not necessarily reflect the views of those organizations. Tissue from wild H. fulgens was collected by the authors, as well as Brian Meux, Ray Hiemstra, and several staff. The SEA Lab sample was provided by Brent Scheiwe. Dr. Jim Seeb at the University of Washington provided guidance and laboratory space. We would like to thank Seeb Lab members Carita Pascal for lab instruction and Ryan Waples for help initiating the Stacks pipeline. We would also like to thank Drs. Fred Utter, Brent Vadopalas, and Robin Waples and two anonymous reviewers for valuable commentary on this manuscript. NR 101 TC 7 Z9 8 U1 5 U2 59 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1566-0621 EI 1572-9737 J9 CONSERV GENET JI Conserv. Genet. PD FEB PY 2014 VL 15 IS 1 BP 109 EP 121 DI 10.1007/s10592-013-0524-5 PG 13 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA AC2UR UT WOS:000332372300009 ER PT J AU Larsen, AB Wagner, JR Jain, A Vaidehi, N AF Larsen, Adrien B. Wagner, Jeffrey R. Jain, Abhinandan Vaidehi, Nagarajan TI Protein Structure Refinement of CASP Target Proteins Using GNEIMO Torsional Dynamics Method SO JOURNAL OF CHEMICAL INFORMATION AND MODELING LA English DT Article ID CONSTRAINED MOLECULAR-DYNAMICS; STRUCTURE PREDICTION; HOMOLOGY MODELS; SIMULATIONS; ROSETTA; CLASSIFICATION; CONFORMATIONS; MINIMIZATION; ACCURATE; LONG AB A longstanding challenge in using computational methods for protein structure prediction is the refinement of low-resolution structural models derived from comparative modeling methods into highly accurate atomistic models useful for detailed structural studies. Previously, we have developed and demonstrated the utility of the internal coordinate molecular dynamics (MD) technique, generalized Newton-Euler inverse mass operator (GNEIMO), for refinement of small proteins. Using GNEIMO, the high-frequency degrees of freedom are frozen and the protein is modeled as a collection of rigid clusters connected by torsional hinges. This physical model allows larger integration time steps and focuses the conformational search in the low frequency torsional degrees of freedom. Here, we have applied GNEIMO with temperature replica exchange to refine low-resolution protein models of 30 proteins taken from the continuous assessment of structure prediction (CASP) competition. We have shown that GNEIMO torsional MD method leads to refinement of up to 1.3 angstrom in the root-mean-square deviation in coordinates for 30 CASP target proteins without using any experimental data as restraints in performing the GNEIMO simulations. This is in contrast with the unconstrained all-atom Cartesian MD method performed under the same conditions, where refinement requires the use of restraints during the simulations. C1 [Larsen, Adrien B.; Wagner, Jeffrey R.; Vaidehi, Nagarajan] City Hope Natl Med Ctr, Beckman Res Inst, Div Immunol, Duarte, CA 91010 USA. [Jain, Abhinandan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Vaidehi, N (reprint author), City Hope Natl Med Ctr, Beckman Res Inst, Div Immunol, 1500 E Duarte Rd, Duarte, CA 91010 USA. EM nvaidehi@coh.org FU NIGMS [R01-GM082896]; National Aeronautics and Space Administration (NASA); California Institute of Regenerative Medicine FX Funding for this work was provided by NIGMS R01-GM082896. We thank Simbios, the NIH Center for Biomedical Computation at Stanford University, for providing us with the GB/SA solvation module. Part of the research described in this paper was performed at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). A.B.L. thanks the California Institute of Regenerative Medicine for fellowship. NR 48 TC 4 Z9 4 U1 0 U2 5 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1549-9596 EI 1549-960X J9 J CHEM INF MODEL JI J. Chem Inf. Model. PD FEB PY 2014 VL 54 IS 2 BP 508 EP 517 DI 10.1021/ci400484c PG 10 WC Chemistry, Medicinal; Chemistry, Multidisciplinary; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Pharmacology & Pharmacy; Chemistry; Computer Science GA AB7SW UT WOS:000331992000017 PM 24397429 ER PT J AU Turk, FJ Haddad, ZS You, YL AF Turk, F. Joseph Haddad, Ziad S. You, Yalei TI Principal Components of Multifrequency Microwave Land Surface Emissivities. Part I: Estimation under Clear and Precipitating Conditions SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Precipitation; Microwave observations; Principal components analysis; Soil moisture; Satellite observations; Land surface ID UNITED-STATES; SYSTEM; RAIN; FREQUENCIES; SIGNATURES; DESERTS; IMAGER; MODEL AB The upcoming Global Precipitation Measurement mission will provide considerably more overland observations over complex terrain, high-elevation river basins, and cold surfaces, necessitating an improved assessment of the microwave land surface emissivity. Current passive microwave overland rainfall algorithms developed for the Tropical Rainfall Measuring Mission (TRMM) rely upon hydrometeor scattering-induced signatures at high-frequency (85 GHz) brightness temperatures (TBs) and are empirical in nature. A multiyear global database of microwave surface emissivities encompassing a wide range of surface conditions was retrieved from Advanced Microwave Scanning Radiometer for Earth Observing System (EOS; AMSR-E) radiometric clear scenes using companion A-Train [CloudSat, Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO), and Atmospheric Infrared Sounder (AIRS)] data. To account for the correlated emissivity structure, the procedure first derives the TRMM Microwave Imager-like nine-channel emissivity principal component (PC) structure. Relations are derived to estimate the emissivity PCs directly from the instantaneous TBs, which allows subsequent TB observations to estimate the PC structure and reconstruct the emissivity vector without need for ancillary data regarding the surface or atmospheric conditions. Radiative transfer simulations matched the AMSR-E TBs within 5-7-K RMS difference in the absence of precipitation. Since the relations are derived specifically for clear-scene conditions, discriminant analysis was performed to find the PC discriminant that best separates clear and precipitation scenes. When this technique is applied independently to two years of TRMM data, the PC-based discriminant demonstrated superior relative operating characteristics relative to the established 85-GHz scattering index, most notably during cold seasons. C1 [Turk, F. Joseph; Haddad, Ziad S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [You, Yalei] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA. RP Turk, FJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 300-243, Pasadena, CA 91109 USA. EM jturk@jpl.nasa.gov RI Measurement, Global/C-4698-2015 FU NASA's Precipitation Measurement Missions (PMM); National Aeronautics and Space Administration FX We acknowledge support from NASA's Precipitation Measurement Missions (PMM) through Dr. Ramesh Kakar. TRMM data were provided through the Precipitation Processing System (PPS) at NASA Goddard Space Flight Center. CloudSat data were made available via the CloudSat Data Processing Center (DPC) at Colorado State University. NMQ data were provided courtesy of Dr. Jian Zhang of the Cooperative Institute for Mesoscale Meteorological Studies (CIMMS) at the University of Oklahoma. This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 45 TC 10 Z9 10 U1 0 U2 12 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2014 VL 15 IS 1 BP 3 EP 19 DI 10.1175/JHM-D-13-08.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AC2BI UT WOS:000332301900001 ER PT J AU You, YL Turk, FJ Haddad, ZS Li, L Liu, GS AF You, Yalei Turk, F. Joseph Haddad, Ziad S. Li, Li Liu, Guosheng TI Principal Components of Multifrequency Microwave Land Surface Emissivities. Part II: Effects of Previous-Time Precipitation SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Surface observations; Microwave observations; Satellite observations; Remote sensing ID UNITED-STATES; FREQUENCIES; RETRIEVAL; ICE AB The microwave land surface emissivity (MLSE) over the continental United States was examined during 2011 as a function of prior rainfall conditions using two independent emissivity estimation techniques, one providing instantaneous estimates based on a clear-scene emissivity principal component (PC) analysis and the other based on physical radiative transfer modeling. Results show that over grass, closed shrub, and cropland, prior rainfall can cause the horizontally polarized 10-GHz brightness temperature (TB) to drop by as much as 20 K, with a corresponding emissivity drop of approximately 0.06, whereby prior rain exhibited little influence on the emissivity over forest because of the dense vegetation. The correlation between emissivity and its leading principal components and the prior rainfall over grass, closed shrub, and cropland is -0.6, while it is only -0.1 over forested areas. Forward-simulated TB using the PC-based emissivity derived from instantaneous Tropical Rainfall Measuring Mission (TRMM) satellite overpasses agrees much better with TRMM Microwave Imager (TMI) observations relative to a climatologically based emissivity, especially after a period of heavy rain. Two potential applications of the PC-based emissivity are demonstrated. The first exploits the time history change of the MLSE to estimate the amount of prior rainfall. The second application is a method to estimate the emissivity underneath precipitating radiometric scenes by first adjusting the surface-sensitive principal components that were derived under clear-sky scenes and then by reconstructing the joint emissivity (all channels simultaneously) from the modified PC structure. The results are applicable to future overland passive microwave rainfall retrieval algorithms to simultaneously detect and estimate precipitation amounts under dynamically changing surface conditions. C1 [You, Yalei; Liu, Guosheng] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA. [Turk, F. Joseph; Haddad, Ziad S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Li, Li] Naval Res Lab, Washington, DC USA. RP You, YL (reprint author), Florida State Univ, Dept Earth Ocean & Atmospher Sci, 1017 Acad Way, Tallahassee, FL 32306 USA. EM yy08@fsu.edu RI Liu, Guosheng/D-3479-2011; Measurement, Global/C-4698-2015 OI Liu, Guosheng/0000-0001-7899-6125; FU NASA's Precipitation Measurement Missions (PMM); NASA [NNX10AG76G, NNX10AM30G]; NSF Grant [AGS1037936]; National Aeronautics and Space Administration FX We acknowledge support from NASA's Precipitation Measurement Missions (PMM) through Dr. Ramesh Kakar. Y. You and G. Liu acknowledge support from NASA Grants NNX10AG76G and NNX10AM30G and NSF Grant AGS1037936. TRMM data were provided through the Precipitation Processing System (PPS) at NASA Goddard Space Flight Center. NMQ data were provided courtesy of Dr. Jian Zhang of the Cooperative Institute for Mesoscale Meteorological Studies (CIMMS) at the University of Oklahoma. This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 30 TC 4 Z9 4 U1 0 U2 11 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2014 VL 15 IS 1 BP 20 EP 37 DI 10.1175/JHM-D-13-07.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AC2BI UT WOS:000332301900002 ER PT J AU Koster, RD Walker, GK Mahanama, SPP Reichle, RH AF Koster, Randal D. Walker, Gregory K. Mahanama, Sarith P. P. Reichle, Rolf H. TI Soil Moisture Initialization Error and Subgrid Variability of Precipitation in Seasonal Streamflow Forecasting SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Seasonal forecasting; Climate variability; Drought; Hydrology; Land surface model; Runoff ID EASTERN UNITED-STATES; PREDICTION; SYSTEM; SKILL; BASIN; SNOW AB Offline simulations over the conterminous United States (CONUS) with a land surface model are used to address two issues relevant to the forecasting of large-scale seasonal streamflow: (i) the extent to which errors in soil moisture initialization degrade streamflow forecasts, and (ii) the extent to which a realistic increase in the spatial resolution of forecasted precipitation would improve streamflow forecasts. The addition of error to a soil moisture initialization field is found to lead to a nearly proportional reduction in large-scale seasonal streamflow forecast skill. The linearity of the response allows the determination of a lower bound for the increase in streamflow forecast skill achievable through improved soil moisture estimation, for example, through the assimilation of satellite-based soil moisture measurements. An increase in the resolution of precipitation is found to have an impact on large-scale seasonal streamflow forecasts only when evaporation variance is significant relative to precipitation variance. This condition is met only in the western half of the CONUS domain. Taken together, the two studies demonstrate the utility of a continental-scale land surface-modeling system as a tool for addressing the science of hydrological prediction. C1 [Koster, Randal D.; Reichle, Rolf H.] NASA, Global Modeling & Assimilat Off, GSFC, Greenbelt, MD 20771 USA. [Walker, Gregory K.; Mahanama, Sarith P. P.] SSAI, Lanham, MD USA. RP Koster, RD (reprint author), NASA, Global Modeling & Assimilat Off, GSFC, Code 610-1, Greenbelt, MD 20771 USA. EM randal.d.koster@nasa.gov RI Reichle, Rolf/E-1419-2012; Koster, Randal/F-5881-2012 OI Koster, Randal/0000-0001-6418-6383 FU Modeling, Analysis, Predictions, and Projections Program of the NOAA/Climate Program Office; NASA Terrestrial Hydrology Program; SMAP Science Definition Team FX The authors thank Lifeng Luo and Xing Yuan for their helpful comments on the precipitation disaggregation study. Providers of basin streamflow measurements include the U.S. Army Corps of Engineers (Omaha and Tulsa offices), the Columbia River Basin Climate Change Scenarios Database, the California Data Exchange Commission, and the U.S. Bureau of Reclamation; Edwin Maurer of Santa Clara University provided additional streamflow data. This work was supported by the Modeling, Analysis, Predictions, and Projections Program of the NOAA/Climate Program Office, the NASA Terrestrial Hydrology Program, and the SMAP Science Definition Team. NR 40 TC 4 Z9 4 U1 1 U2 17 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2014 VL 15 IS 1 BP 69 EP 88 DI 10.1175/JHM-D-13-050.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AC2BI UT WOS:000332301900004 ER PT J AU Dirmeyer, PA Wei, JF Bosilovich, MG Mocko, DM AF Dirmeyer, Paul A. Wei, Jiangfeng Bosilovich, Michael G. Mocko, David M. TI Comparing Evaporative Sources of Terrestrial Precipitation and Their Extremes in MERRA Using Relative Entropy SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Moisture/moisture budget; Precipitation; Flood events; Lagrangian circulation/transport; Evaporation; Drought ID WARM-SEASON PRECIPITATION; GENERAL-CIRCULATION MODEL; ATMOSPHERIC WATER-VAPOR; MISSISSIPPI RIVER-BASIN; MOISTURE SOURCES; LAGRANGIAN ANALYSIS; LOCAL EVAPORATION; HYDROLOGIC-CYCLE; AMAZON BASIN; PART II AB A quasi-isentropic, back-trajectory scheme is applied to output from the Modern-Era Retrospective Analysis for Research and Applications (MERRA) and a land-only replay with corrected precipitation to estimate surface evaporative sources of moisture supplying precipitation over every ice-free land location for the period 1979-2005. The evaporative source patterns for any location and time period are effectively two-dimensional probability distributions. As such, the evaporative sources for extreme situations like droughts or wet intervals can be compared to the corresponding climatological distributions using the method of relative entropy. Significant differences are found to be common and widespread for droughts, but not wet periods, when monthly data are examined. At pentad temporal resolution, which is more able to isolate floods and situations of atmospheric rivers, values of relative entropy over North America are typically 50%-400% larger than at monthly time scales. Significant differences suggest that moisture transport may be a key factor in precipitation extremes. Where evaporative sources do not change significantly, it implies other local causes may underlie the extreme events. C1 [Dirmeyer, Paul A.] George Mason Univ, Dept Atmospher Ocean & Earth Sci, Fairfax, VA 22030 USA. [Dirmeyer, Paul A.] Inst Global Environm & Soc, Ctr Ocean Land Atmosphere Studies, Calverton, MD USA. [Wei, Jiangfeng] Univ Texas Austin, Jackson Sch Geosci, Austin, TX 78712 USA. [Bosilovich, Michael G.; Mocko, David M.] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD USA. [Mocko, David M.] SAIC, Greenbelt, MD USA. RP Dirmeyer, PA (reprint author), George Mason Univ, Dept Atmospher Ocean & Earth Sci, 4400 Univ Dr,Mail Stop 2B3, Fairfax, VA 22030 USA. EM dirmeyer@cola.iges.org RI Wei, Jiangfeng/C-6342-2009; Dirmeyer, Paul/B-6553-2016; Bosilovich, Michael/F-8175-2012 OI Wei, Jiangfeng/0000-0001-8981-8674; Dirmeyer, Paul/0000-0003-3158-1752; FU National Aeronautics and Space Administration [NNX09AI84G] FX This research was supported by National Aeronautics and Space Administration Grant NNX09AI84G. Much of the data used in this effort were acquired as part of the activities of NASA's Science Mission Directorate and are archived and distributed by the Goddard Earth Sciences (GES) Data and Information Services Center (DISC). NR 58 TC 11 Z9 11 U1 0 U2 18 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2014 VL 15 IS 1 BP 102 EP 116 DI 10.1175/JHM-D-13-053.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AC2BI UT WOS:000332301900006 ER PT J AU Burns, SP Molotch, NP Williams, MW Knowles, JF Seok, B Monson, RK Turnipseed, AA Blanken, PD AF Burns, Sean P. Molotch, Noah P. Williams, Mark W. Knowles, John F. Seok, Brian Monson, Russell K. Turnipseed, Andrew A. Blanken, Peter D. TI Snow Temperature Changes within a Seasonal Snowpack and Their Relationship to Turbulent Fluxes of Sensible and Latent Heat SO JOURNAL OF HYDROMETEOROLOGY LA English DT Review DE Hydrometeorology; Surface fluxes; Snow cover; Sublimation; Small scale processes; Forest canopy ID SUB-ALPINE FOREST; ECOSYSTEM CO2 EXCHANGE; HIGH-ELEVATION; COMPLEX TERRAIN; ENERGY-BALANCE; NIWOT-RIDGE; THERMAL-CONDUCTIVITY; VEGETATION CANOPIES; CONIFER FOREST; BOUNDARY-LAYER AB Snowpack temperatures from a subalpine forest below Niwot Ridge, Colorado, are examined with respect to atmospheric conditions and the 30-min above-canopy and subcanopy eddy covariance fluxes of sensible Q(h) and latent Q(e) heat. In the lower snowpack, daily snow temperature changes greater than 1 degrees C day(-1) occurred about 1-2 times in late winter and early spring, which resulted in transitions to and from an isothermal snowpack. Though air temperature was a primary control on snowpack temperature, rapid snowpack warm-up events were sometimes preceded by strong downslope winds that kept the nighttime air (and canopy) temperature above freezing, thus increasing sensible heat and longwave radiative transfer from the canopy to the snowpack. There was an indication that water vapor condensation on the snow surface intensified the snowpack warm-up. In late winter, subcanopy Q(h) was typically between -10 and 10 W m(-2) and rarely had a magnitude larger than 20 W m(-2). The direction of subcanopy Q(h) was closely related to the canopy temperature and only weakly dependent on the time of day. The daytime subcanopy Q(h) monthly frequency distribution was near normal, whereas the nighttime distribution was more peaked near zero with a large positive skewness. In contrast, above-canopy Q(h) was larger in magnitude (100-400 W m(-2)) and primarily warmed the forest-surface at night and cooled it during the day. Around midday, decoupling of subcanopy and above-canopy air led to an apparent cooling of the snow surface by sensible heat. Sources of uncertainty in the subcanopy eddy covariance flux measurements are suggested. Implications of the observed snowpack temperature changes for future climates are discussed. C1 [Burns, Sean P.; Molotch, Noah P.; Williams, Mark W.; Knowles, John F.; Blanken, Peter D.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA. [Burns, Sean P.; Turnipseed, Andrew A.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Molotch, Noah P.; Williams, Mark W.; Knowles, John F.; Seok, Brian] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. [Molotch, Noah P.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Seok, Brian] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA. [Monson, Russell K.] Univ Arizona, Sch Nat Resources & Environm, Tucson, AZ USA. RP Burns, SP (reprint author), NCAR MMM, POB 3000, Boulder, CO 80307 USA. EM sean@ucar.edu RI Burns, Sean/A-9352-2008; Seok, Brian/K-6712-2012; Knowles, John/B-1631-2013; Molotch, Noah/C-8576-2009; OI Burns, Sean/0000-0002-6258-1838; Seok, Brian/0000-0002-4513-3224; Knowles, John/0000-0002-3697-9439; BLANKEN, PETER/0000-0002-7405-2220 FU U.S. Department of Energy (DOE); National Institute for Climate Change Research (NICCR); Terrestrial Carbon Processes Program (TCP); National Science Foundation (NSF) Long-Term Research in Environmental Biology (LTREB) [0918565]; NSF [EAR 1032295, EAR 1032308]; NSF FX We gratefully acknowledge the Niwot Ridge LTER team (Jennifer Morse, Kurt Chowanski, Mark Losleben, and many others) for maintaining the LTER instruments; Jeff Beauregard for field help at the NWT site; and discussions with Dave Bowling, Don Lenschow, Ned Patton, and Jielun Sun. We also acknowledge the NRCS SNOTEL and NOAA SURFRAD networks for making their data readily available and Mage Hultstrand for providing information about the Niwot SNOTEL site. Finally, we thank three anonymous reviewers for comments that improved the manuscript. The AmeriFlux tower has been supported by two grants from the U.S. Department of Energy (DOE) [the National Institute for Climate Change Research (NICCR) and Terrestrial Carbon Processes Program (TCP)], as well as a grant from the National Science Foundation (NSF) Long-Term Research in Environmental Biology (LTREB, Grant 0918565). N.P.M. acknowledges funding from NSF EAR 1032295 and EAR 1032308. The National Center for Atmospheric Research (NCAR) is sponsored by NSF. NR 114 TC 9 Z9 9 U1 3 U2 53 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2014 VL 15 IS 1 BP 117 EP 142 DI 10.1175/JHM-D-13-026.1 PG 26 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AC2BI UT WOS:000332301900007 ER PT J AU Kumar, A Houze, RA Rasmussen, KL Peters-Lidard, C AF Kumar, Anil Houze, Robert A., Jr. Rasmussen, Kristen L. Peters-Lidard, Christa TI Simulation of a Flash Flooding Storm at the Steep Edge of the Himalayas* SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Flood events; Mesoscale systems; Monsoons; Hydrology; Orographic effects; Convection ID MESOSCALE CONVECTIVE SYSTEMS; MID-TROPOSPHERIC CYCLONES; DATA ASSIMILATION SYSTEM; PRECIPITATION RADAR; MONSOON CONVECTION; MODELING SYSTEM; SUMMER MONSOON; BIG THOMPSON; ANVIL CLOUDS; RESOLUTION AB A flash flood and landslide in the Leh region of the Indus Valley in the Indian state of Jammu and Kashmir on 5-6 August 2010 resulted in hundreds of deaths and great property damage. Observations have led to the hypothesis that the storm, which formed over the Tibetan Plateau, was steered over the steep edge of the plateau by 500-hPa winds and then energized by the ingestion of lower-level moist air, which was approaching from the Arabian Sea and Bay of Bengal and rose up the Himalayan barrier. A coupled land surface and atmospheric model simulation validates this hypothesized storm scenario, with the model storm taking the form of a traveling mesoscale squall line with a leading convective line, trailing stratiform region, and midlevel inflow jet. In this region, the development of a mesoscale storm over high terrain is highly unusual, especially one in the form of a propagating squall line system. This unusual storm occurrence and behavior could serve as a warning sign in flash flood prediction. The coupled atmosphere and land surface model showed that the excessive runoff leading to the flood and landslide were favored by the occurrence of this unusual meteorological event coinciding temporally and spatially with favorable hydrologic conditions. Additionally, the model simulations showed that previous rainstorms had moistened the soil during the entire season and especially over the few days leading up to the Leh flood, so the normally arid mountainsides were likely not able to rapidly absorb the additional rainfall of the sudden 5 August squall line. C1 [Kumar, Anil; Peters-Lidard, Christa] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. [Kumar, Anil] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Houze, Robert A., Jr.; Rasmussen, Kristen L.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. RP Kumar, A (reprint author), NASA, Hydrol Sci Branch, Goddard Space Flight Ctr, Code 617, Greenbelt, MD 20770 USA. EM anil.kumar@nasa.gov RI Rasmussen, Kristen/J-6421-2014; Peters-Lidard, Christa/E-1429-2012 OI Rasmussen, Kristen/0000-0003-1321-0974; Peters-Lidard, Christa/0000-0003-1255-2876 FU NSF Grants [ATM-0820586, AGS-1144105]; NASA Grants [NNX10AH70G, NNX11AL65H]; National Aeronautics and Space Administration grants from the NASA Modeling, Analysis and Prediction (MAP) Program FX This research was sponsored by NSF Grants ATM-0820586 and AGS-1144105 and NASA Grants NNX10AH70G and NNX11AL65H (Dr. Ramesh Kakar). This research was also supported by National Aeronautics and Space Administration grants from the NASA Modeling, Analysis and Prediction (MAP) Program (Dr. David Considine, MAP program manager). The NASA Center for Climate Simulation (NCCS) computing system provided resources for the model simulations. Thara Prabhakaran participated in an early phase of this study. Graphics art and manuscript editing were provided by Beth Tully. The authors thank Dr. Russ Schumacher and two anonymous reviewers for their comments and suggestions, which have greatly improved this manuscript. NR 49 TC 12 Z9 12 U1 0 U2 39 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2014 VL 15 IS 1 BP 212 EP 228 DI 10.1175/JHM-D-12-0155.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AC2BI UT WOS:000332301900012 ER PT J AU Hirsch, AL Kala, J Pitman, AJ Carouge, C Evans, JP Haverd, V Mocko, D AF Hirsch, Annette L. Kala, Jatin Pitman, Andy J. Carouge, Claire Evans, Jason P. Haverd, Vanessa Mocko, David TI Impact of Land Surface Initialization Approach on Subseasonal Forecast Skill: A Regional Analysis in the Southern Hemisphere SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Soil moisture; Atmosphere-land interaction; Regional models; Forecast verification/skill ID SOIL-MOISTURE; CONVECTIVE PARAMETERIZATION; RAINFALL VARIABILITY; CLIMATE; MODEL; AUSTRALIA; PERFORMANCE; EXTREMES; SYSTEM; SET AB The authors use a sophisticated coupled land-atmosphere modeling system for a Southern Hemisphere subdomain centered over southeastern Australia to evaluate differences in simulation skill from two different land surface initialization approaches. The first approach uses equilibrated land surface states obtained from offline simulations of the land surface model, and the second uses land surface states obtained from reanalyses. The authors find that land surface initialization using prior offline simulations contribute to relative gains in subseasonal forecast skill. In particular, relative gains in forecast skill for temperature of 10%-20% within the first 30 days of the forecast can be attributed to the land surface initialization method using offline states. For precipitation there is no distinct preference for the land surface initialization method, with limited gains in forecast skill irrespective of the lead time. The authors evaluated the asymmetry between maximum and minimum temperatures and found that maximum temperatures had the largest gains in relative forecast skill, exceeding 20% in some regions. These results were statistically significant at the 98% confidence level at up to 60 days into the forecast period. For minimum temperature, using reanalyses to initialize the land surface contributed to relative gains in forecast skill, reaching 40% in parts of the domain that were statistically significant at the 98% confidence level. The contrasting impact of the land surface initialization method between maximum and minimum temperature was associated with different soil moisture coupling mechanisms. Therefore, land surface initialization from prior offline simulations does improve predictability for temperature, particularly maximum temperature, but with less obvious improvements for precipitation and minimum temperature over southeastern Australia. C1 [Hirsch, Annette L.; Kala, Jatin; Pitman, Andy J.; Carouge, Claire; Evans, Jason P.] Univ New S Wales, ARC Ctr Excellence Climate Syst Sci, Sydney, NSW 2052, Australia. [Hirsch, Annette L.; Kala, Jatin; Pitman, Andy J.; Carouge, Claire; Evans, Jason P.] Univ New S Wales, Climate Change Res Ctr, Sydney, NSW 2052, Australia. [Haverd, Vanessa] CSIRO Marine & Atmospher Res, Canberra, ACT, Australia. [Mocko, David] NASA, SAIC, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Hirsch, AL (reprint author), Univ New S Wales, ARC Ctr Excellence Climate Syst Sci, Level 4 Mathews Bldg, Sydney, NSW 2052, Australia. EM a.hirsch@student.unsw.edu.au RI Pitman, Andrew/A-7353-2011; kala, Jatin/G-8408-2011; haverd, vanessa/G-8683-2011; Evans, Jason/F-3716-2011; Hirsch, Annette/B-6892-2011; OI Pitman, Andrew/0000-0003-0604-3274; kala, Jatin/0000-0001-9338-2965; Evans, Jason/0000-0003-1776-3429; Hirsch, Annette/0000-0002-5811-2465; Carouge, Claire/0000-0002-0313-8385 FU Australian Research Council Centre of Excellence for Climate System Science Grant [CE110001028]; Australian Postgraduate Award; CSIRO OCE Postgraduate Top Up Scholarship FX This study was supported by the Australian Research Council Centre of Excellence for Climate System Science Grant CE110001028. The computational modeling was supported by the NCI National Facility at the ANU, Australia. Annette Hirsch was supported by an Australian Postgraduate Award and CSIRO OCE Postgraduate Top Up Scholarship. The authors thank Mark Decker for providing the bias-corrected MERRA data, Scott Sisson for advice on evaluating the statistical significance of our results, and Randal Koster and Bart van den Hurk for clarification on the GLACE-2 methodology. The authors would also like to thank the anonymous reviewers who provided constructive comments on the manuscript. NR 48 TC 14 Z9 14 U1 0 U2 7 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2014 VL 15 IS 1 BP 300 EP 319 DI 10.1175/JHM-D-13-05.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AC2BI UT WOS:000332301900017 ER PT J AU Tapiador, FJ Haddad, ZS Turk, J AF Tapiador, Francisco J. Haddad, Ziad S. Turk, Joe TI A Probabilistic View on Raindrop Size Distribution Modeling: A Physical Interpretation of Rain Microphysics SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Drop size distribution; Radars/Radar observations; Hydrometeorology ID DISTRIBUTION PARAMETERS; RADAR; DISDROMETER; SPECTRA; ATTENUATION; ERRORS AB The raindrop size distribution (RDSD) is defined as the relative frequency of raindrops per given diameter in a volume. This paper describes a mathematically consistent modeling of the RDSD drawing on probability theory. It is shown that this approach is simpler than the use of empirical fits and that it provides a more consistent procedure to estimate the rainfall rate (R) from reflectivity (Z) measurements without resorting to statistical regressions between both parameters. If the gamma distribution form is selected, the modeling expresses the integral parameters Z and R in terms of only the total number of drops per volume (N-T), the sample mean [m = E(D)], and the sample variance [sigma(2) = E(m - D)(2)] of the drop diameters (D) or, alternatively, in terms of N-T, E(D), and E[log(D)]. Statistical analyses indicate that (N-T, m) are independent, as are (N-T, sigma(2)). The Z-R relationship that arises from this model is a linear R = T x Z expression (or Z = T-1R), with T a factor depending on m and sigma(2) only and thus independent of N-T. The Z-R so described is instantaneous, in contrast with the operational calculation of the RDSD in radar meteorology, where the Z-R arises from a regression line over a usually large number of measurements. The probabilistic approach eliminates the need of intercept parameters N-0 or , which are often used in statistical approaches but lack physical meaning. The modeling presented here preserves a well-defined and consistent set of units across all the equations, also taking into account the effects of RDSD truncation. It is also shown that the rain microphysical processes such as coalescence, breakup, or evaporation can then be easily described in terms of two parameters-the sample mean and the sample variance-and that each of those processes have a straightforward translation in changes of the instantaneous Z-R relationship. C1 [Tapiador, Francisco J.] Univ Castilla La Mancha, Fac Environm Sci & Biochem, Toledo 45071, Spain. [Haddad, Ziad S.; Turk, Joe] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Tapiador, FJ (reprint author), Univ Castilla La Mancha, Fac Environm Sci & Biochem, Avda Carlos 3 S-N, Toledo 45071, Spain. EM francisco.tapiador@uclm.es FU JCCM [PPII10-0162-5543]; MiCInn [CGL2010-20787-C02-01, CGL2010-20787-C02-02, UNCM08-1E-086]; Cenit project Prometeo (CDTI); CYTEMA FX Funding from projects PPII10-0162-5543 (JCCM), CGL2010-20787-C02-01, CGL2010-20787-C02-02 (MiCInn), Cenit project Prometeo (CDTI), CYTEMA, and UNCM08-1E-086 (MiCInn) is gratefully acknowledged. F.J.T. acknowledges Ramiro Checa and Luis Duran for double checking some early calculations and for their assistance in organizing and filtering the UCLM's RDSD database. The authors also wish to acknowledge fruitful discussions in the Drop Size Distribution Working Group (DSDWG) of the Global Precipitation Measurement (GPM) mission. NR 33 TC 4 Z9 4 U1 2 U2 9 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2014 VL 15 IS 1 BP 427 EP 443 DI 10.1175/JHM-D-13-033.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AC2BI UT WOS:000332301900024 ER PT J AU Smalley, M L'Ecuyer, T Lebsock, M Haynes, J AF Smalley, Mark L'Ecuyer, Tristan Lebsock, Matthew Haynes, John TI A Comparison of Precipitation Occurrence from the NCEP Stage IV QPE Product and the CloudSat Cloud Profiling Radar SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Remote sensing; Snowfall; Radars/Radar observations; Water budget; Rainfall; Precipitation ID CONTIGUOUS UNITED-STATES; WSR-88D; ALGORITHM; GAUGE; CALIBRATION; FORECASTS; NETWORK; SYSTEM AB Because of its extensive quality control procedures and uniform space-time grid, the NCEP Stage IV merged Weather Surveillance Radar-1988 Doppler (WSR-88D) radar and surface rain gauge dataset is often considered to be the best long-term gridded dataset of precipitation observations covering the contiguous United States. Stage IV accumulations are employed in a variety of applications, and while the WSR-88D systems are well suited for observing heavy rain events that are likely to affect flooding, limitations in surface radar and gauge measurements can result in missed precipitation, especially near topography and in the western United States. This paper compares hourly Stage IV observations of precipitation occurrence to collocated observations from the 94-GHz CloudSat Cloud Profiling Radar, which provides excellent sensitivity to light and frozen precipitation. Statistics from 4 yr of comparisons show that the CloudSat observes precipitation considerably more frequently than the Stage IV dataset, especially in northern states where frozen precipitation is prevalent in the cold season. The skill of Stage IV for precipitation detection is found to decline rapidly when the near-surface air temperature falls below 0 degrees C. As a result, agreement between Stage IV and CloudSat tends to be best in the southeast, where radar coverage is good and moderate-to-heavy liquid precipitation dominates. Stage IV and CloudSat precipitation detection characteristics are documented for each of the individual river forecast centers that contribute to the Stage IV dataset to provide guidance regarding potential sampling biases that may impact hydrologic applications. C1 [Smalley, Mark; L'Ecuyer, Tristan] Univ Wisconsin, Madison, WI 53706 USA. [Lebsock, Matthew] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Haynes, John] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA. RP Smalley, M (reprint author), Univ Wisconsin, Dept Atmospher & Ocean Sci, 1225 W Dayton St, Madison, WI 53706 USA. EM smalley2@wisc.edu RI L'Ecuyer, Tristan/E-5607-2012 OI L'Ecuyer, Tristan/0000-0002-7584-4836 FU NASA CloudSat/CALIPSO Science Team (CCST) Grant [NNX12AC51G] FX This work was supported by NASA CloudSat/CALIPSO Science Team (CCST) Grant NNX12AC51G. The authors acknowledge the efforts made at the CloudSat Data Processing Center (http://www.cloudsat.cira.colostate.edu) and the National Center for Atmospheric Research (NCAR) Earth Observing Laboratory (EOL) (http://www.emc.ncep.noaa.gov/mmb/ylin/pcpanl/stage4/) in making these data available. NR 43 TC 10 Z9 11 U1 2 U2 17 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2014 VL 15 IS 1 BP 444 EP 458 DI 10.1175/JHM-D-13-048.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AC2BI UT WOS:000332301900025 ER PT J AU Kala, J Decker, M Exbrayat, JF Pitman, AJ Carouge, C Evans, JP Abramowitz, G Mocko, D AF Kala, Jatin Decker, Mark Exbrayat, Jean-Francois Pitman, Andy J. Carouge, Claire Evans, Jason P. Abramowitz, Gab Mocko, David TI Influence of Leaf Area Index Prescriptions on Simulations of Heat, Moisture, and Carbon Fluxes SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Hydrometeorology; Surface fluxes; Carbon cycle; Fluxes ID GENERAL-CIRCULATION MODELS; INTERANNUAL VARIABILITY; CLIMATE SIMULATIONS; STOMATAL-RESISTANCE; ROUGHNESS LENGTH; BIOSPHERE MODEL; LAND; SENSITIVITY; VEGETATION; AUSTRALIA AB Leaf area index (LAI), the total one-sided surface area of leaf per ground surface area, is a key component of land surface models. The authors investigate the influence of differing, plausible LAI prescriptions on heat, moisture, and carbon fluxes simulated by the Community Atmosphere Biosphere Land Exchange version 1.4b (CABLEv1.4b) model over the Australian continent. A 15-member ensemble monthly LAI dataset is generated using the Moderate Resolution Imaging Spectroradiometer (MODIS) LAI product and gridded observations of temperature and precipitation. Offline simulations lasting 29 years (1980-2008) are carried out at 25-km resolution with the composite monthly means from the MODIS LAI product (control simulation) and compared with simulations using each of the 15-member ensemble monthly varying LAI datasets generated. The imposed changes in LAI did not strongly influence the sensible and latent fluxes, but the carbon fluxes were more strongly affected. Croplands showed the largest sensitivity in gross primary production with differences ranging from -90% to 60%. Plant function types (PFTs) with high absolute LAI and low interannual variability, such as evergreen broadleaf trees, showed the least response to the different LAI prescriptions, while those with lower absolute LAI and higher interannual variability, such as croplands, were more sensitive. The authors show that reliance on a single LAI prescription may not accurately reflect the uncertainty in the simulation of terrestrial carbon fluxes, especially for PFTs with high interannual variability. The study highlights that accurate representation of LAI in land surface models is key to the simulation of the terrestrial carbon cycle. Hence, this will become critical in quantifying the uncertainty in future changes in primary production. C1 [Kala, Jatin; Decker, Mark; Exbrayat, Jean-Francois; Pitman, Andy J.; Carouge, Claire; Evans, Jason P.; Abramowitz, Gab] Univ New S Wales, Australian Res Council, Ctr Excellence Climate Syst Sci, Sydney, NSW 2052, Australia. [Kala, Jatin; Decker, Mark; Exbrayat, Jean-Francois; Pitman, Andy J.; Carouge, Claire; Evans, Jason P.; Abramowitz, Gab] Univ New S Wales, Climate Change Res Ctr, Sydney, NSW 2052, Australia. [Mocko, David] NASA, Goddard Space Flight Ctr, SAIC, Greenbelt, MD 20771 USA. RP Kala, J (reprint author), Univ New S Wales, Australian Res Council, Ctr Excellence Climate Syst Sci, Gate 11 Bot St,Level 4,Mathews Bldg, Sydney, NSW 2052, Australia. EM j.kala@unsw.edu.au RI Exbrayat, Jean-Francois/H-5645-2012; Pitman, Andrew/A-7353-2011; kala, Jatin/G-8408-2011; Evans, Jason/F-3716-2011; OI Exbrayat, Jean-Francois/0000-0002-3671-8626; Pitman, Andrew/0000-0003-0604-3274; kala, Jatin/0000-0001-9338-2965; Evans, Jason/0000-0003-1776-3429; Decker, Mark/0000-0003-1071-611X; Carouge, Claire/0000-0002-0313-8385 FU Australian Research Council Centre of Excellence for Climate System Science [CE110001028]; NSW Environment Trust [RM08603] FX All the authors except David Mocko are supported by the Australian Research Council Centre of Excellence for Climate System Science (CE110001028). This work was also supported by the NSW Environment Trust (RM08603). We thank CSIRO and the Bureau of Meteorology through the Centre for Australian Weather and Climate Research for their support in the use of the CABLE model. We thank the National Computational Infrastructure at the Australian National University, an initiative of the Australian Government, for access to supercomputer resources. We thank the NASA GSFC LIS team for support in coupling CABLE to LIS. The MODIS-derived background soil albedo was provided by Peter R. J. North from the Department of Geography, Swansea University, Swansea, United Kingdom. The modified MODIS LAI data were provided by Hua Yuan from the Land-Atmosphere Interaction Research Group at Beijing Normal University. All of this assistance is gratefully acknowledged. NR 51 TC 7 Z9 8 U1 5 U2 37 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2014 VL 15 IS 1 BP 489 EP 503 DI 10.1175/JHM-D-13-063.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AC2BI UT WOS:000332301900028 ER PT J AU Babuscia, A Cheung, KM AF Babuscia, Alessandra Cheung, Kar-Ming TI An approach to perform expert elicitation for engineering design risk analysis: methodology and experimental results SO JOURNAL OF THE ROYAL STATISTICAL SOCIETY SERIES A-STATISTICS IN SOCIETY LA English DT Article DE Bonferroni test; Gaussianity; Linearity; Time reversibility; Trispectrum ID PROBABILITY-DISTRIBUTIONS; RECONCILIATION; ASSESSMENTS; JUDGMENT AB Expert elicitation is increasingly applied to different research areas. Multiple approaches have been implemented, but the development of methods to quantify experts' biases and calibration represents a challenge. As a result, the integration of multiple and often conflicting opinions can be demanding, owing to the complexity of properly weighting experts' contributions. We propose an approach to address this problem when probability densities for seed calibration variables are not available. The methodology generates an expert score that is employed to aggregate multiple-expert assessments. The approach has been experimentally applied to engineering design risk analysis. Results indicate that the approach improves the quality of the estimations. The weighted aggregations of experts' estimates based on the experts' scores achieve better results than the corresponding aggregations based on experts' opinions equally weighted. C1 [Babuscia, Alessandra] MIT, Cambridge, MA 02139 USA. [Cheung, Kar-Ming] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Cheung, Kar-Ming] CALTECH, Pasadena, CA 91125 USA. RP Babuscia, A (reprint author), MIT, Dept Aeronaut & Astronaut, 70 Vassar Sreet, Cambridge, MA 02139 USA. EM babuscia@mit.edu FU MIT Space System Laboratory, MIT Department of Aeronautics and Astronautics; Amelia Earhart Fellowship Program FX The research was partially carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This research was partially carried out at the Massachusetts Institute of Technology (MIT), and it was partially sponsored by the MIT Space System Laboratory, MIT Department of Aeronautics and Astronautics, and Amelia Earhart Fellowship Program. The authors thank Professor David W. Miller, Professor Moe Z. Win, Dr Alvar Saenz Otero and the MIT META Project Team (Professor John Deyst, Professor Karen Willcox, Dr Doug Allaire, Ms Chelsea He and Ms Emily Clements) for their support and suggestions. The authors also thank the Associate Editor and the referees for their comments and suggestions. NR 24 TC 4 Z9 4 U1 1 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0964-1998 EI 1467-985X J9 J R STAT SOC A STAT JI J. R. Stat. Soc. Ser. A-Stat. Soc. PD FEB PY 2014 VL 177 IS 2 BP 475 EP 497 DI 10.1111/rssa.12028 PG 23 WC Social Sciences, Mathematical Methods; Statistics & Probability SC Mathematical Methods In Social Sciences; Mathematics GA AA8WX UT WOS:000331376800008 ER PT J AU Han, JW Kim, B Li, J Meyyappan, M AF Han, Jin-Woo Kim, Beomseok Li, Jing Meyyappan, M. TI Carbon nanotube ink for writing on cellulose paper SO MATERIALS RESEARCH BULLETIN LA English DT Article DE Electronic materials; Chemical synthesis; Electron microscopy; Electrical properties ID SUBSTRATE AB A water-based conductive carbon nanotube (CNT) ink was synthesized with single-walled CNT and sodium dodecylbenezenesulfonate as surfactant. Direct writing on paper using this ink was demonstrated with off-the-shelf nib and cartridges in a fountain pen handwriting tool. It is lightweight and portable which allows writing on curved substrates. The through paper via was easily achieved by wetting method. Dual-side and multi-layer paper circuit boards were demonstrated by direct writing. The drawn pattern displays uniformity and reproducibility. The exceptional adhesion of CNT on cellulose paper shows good robustness against bending, folding, crumpling and other mechanical stress. A chemical sensor fabricated by direct writing showed good response down to 10 ppm of ammonia vapor in air. Published by Elsevier Ltd. C1 [Han, Jin-Woo; Kim, Beomseok; Li, Jing; Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Han, JW (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. EM jin-woo.han@nasa.gov NR 14 TC 11 Z9 12 U1 4 U2 43 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0025-5408 EI 1873-4227 J9 MATER RES BULL JI Mater. Res. Bull. PD FEB PY 2014 VL 50 BP 249 EP 253 DI 10.1016/j.materresbull.2013.10.048 PG 5 WC Materials Science, Multidisciplinary SC Materials Science GA AB6ST UT WOS:000331920500041 ER PT J AU Liechty, DS Lewis, MJ AF Liechty, D. S. Lewis, M. J. TI Extension of the quantum-kinetic model to lunar and Mars return physics SO PHYSICS OF FLUIDS LA English DT Article ID SIMULATION MONTE-CARLO; ELECTRON-IMPACT EXCITATION; FUTURE NASA MISSIONS; CROSS-SECTIONS; REENTRY FLOWS; RADIATION; NITROGEN; RELAXATION; COEFFICIENTS; TEMPERATURE AB The ability to compute rarefied, ionized hypersonic flows is becoming more important as missions such as Earth reentry, landing high-mass payloads on Mars, and the exploration of the outer planets and their satellites are being considered. A recently introduced molecular-level chemistry model, the quantum-kinetic, or Q-K, model that predicts reaction rates for gases in thermal equilibrium and non-equilibrium using only kinetic theory and fundamental molecular properties, is extended in the current work to include electronic energy level transitions and reactions involving charged particles. Like the Q-K procedures for neutral species chemical reactions, these new models are phenomenological procedures that aim to reproduce the reaction/transition rates but do not necessarily capture the exact physics. These engineering models are necessarily efficient due to the requirement to compute billions of simulated collisions in direct simulation Monte Carlo (DSMC) simulations. The new models are shown to generally agree within the spread of reported transition and reaction rates from the literature for near equilibrium conditions. (C) 2014 AIP Publishing LLC. C1 [Liechty, D. S.] NASA Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. [Lewis, M. J.] Univ Maryland, Dept Aerosp Engn, College Pk, MD 20742 USA. RP Liechty, DS (reprint author), NASA Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. NR 56 TC 2 Z9 2 U1 0 U2 6 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1070-6631 EI 1089-7666 J9 PHYS FLUIDS JI Phys. Fluids PD FEB PY 2014 VL 26 IS 2 AR 027106 DI 10.1063/1.4866319 PG 18 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA AC2HZ UT WOS:000332322000060 ER PT J AU Mankbadi, MR Balachandar, S AF Mankbadi, Mina R. Balachandar, S. TI Multiphase effects on spherical Rayleigh-Taylor interfacial instability SO PHYSICS OF FLUIDS LA English DT Article ID FLOWS AB A spherical shock-tube model is implemented to focus the attention on the flow instability produced by the release of the driver mixture of gas-particles into the cold driven pure gas. Four discontinuous spherical surfaces are produced which are in order from outward to inward the Primary Shock, gas Contact Interface, Particle Interface, and Secondary Shock. An appropriate methodology is developed to capture the base flows and the physics of Rayleigh-Taylor-based instabilities. The interaction forces between the two phases and the heat transfer are modeled for both the base and the perturbation flows. The parametric space is explored by varying the particle characteristics in order to reveal the mechanisms involved. The results indicate that the gas-gas contact interface remains unstable for the multiphase cases; however, the growth rate of the instability is dampened due to the inclusion of the particles. Results are compared with theoretical models to explain the mechanisms involved. (C) 2014 AIP Publishing LLC. C1 [Mankbadi, Mina R.; Balachandar, S.] Univ Florida, Dept Mech & Aerosp Engn, Gainesville, FL 32611 USA. RP Mankbadi, MR (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA. EM mina.r.mankbadi@nasa.gov FU Department of Energy's Sandia National Laboratories; AF OSR [FA9550-10-1-0309] FX This work is supported by a Fellowship from the Department of Energy's Sandia National Laboratories and AF OSR under Grant No. FA9550-10-1-0309. Special thanks to A. Brown and T. Aselage of Sandia National Labs for their guidance and advice, and to the reviewers of this paper for their valuable comments. Also, we are grateful to the reviewers of this paper for their thoroughness. NR 31 TC 3 Z9 3 U1 2 U2 12 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1070-6631 EI 1089-7666 J9 PHYS FLUIDS JI Phys. Fluids PD FEB PY 2014 VL 26 IS 2 AR 023301 DI 10.1063/1.4863447 PG 26 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA AC2HZ UT WOS:000332322000014 ER PT J AU Lazio, JW Kimball, A Barger, AJ Brandt, WN Chatterjee, S Clarke, TE Condon, JJ Dickman, RL Hunyh, MT Jarvis, MJ Juric, M Kassim, NE Myers, ST Nissanke, S Osten, R Zauderer, BA AF Lazio, Joseph W. Kimball, A. Barger, A. J. Brandt, W. N. Chatterjee, S. Clarke, T. E. Condon, J. J. Dickman, Robert L. Hunyh, M. T. Jarvis, Matt J. Juric, Mario Kassim, N. E. Myers, S. T. Nissanke, Samaya Osten, Rachel Zauderer, B. A. TI Radio Astronomy in LSST Era SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID RAY BURST AFTERGLOWS; NEUTRON-STARS; X-RAY; SUPER-NOVAE; HOST GALAXY; SKY; SAMPLE; EMISSION; CLASSIFICATION; SIMULATION C1 [Lazio, Joseph W.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Kimball, A.; Condon, J. J.; Dickman, Robert L.; Myers, S. T.] Natl Radio Astron Observ, Charlottesville, VA USA. [Kimball, A.] CSIRO Astron & Space Sci, Sydney, NSW, Australia. [Barger, A. J.] Univ Wisconsin, Madison, WI 53706 USA. [Brandt, W. N.] Penn State Univ, University Pk, PA 16802 USA. [Chatterjee, S.] Cornell Univ, Ithaca, NY 14853 USA. [Clarke, T. E.; Kassim, N. E.] Naval Res Lab, Washington, DC USA. [Hunyh, M. T.] Int Ctr Radio Astron Res, Perth, WA, Australia. [Jarvis, Matt J.] Univ Oxford, Oxford OX1 2JD, England. [Jarvis, Matt J.] Univ Western Cape, ZA-7535 Bellville, South Africa. [Nissanke, Samaya] CALTECH, Pasadena, CA 91125 USA. [Osten, Rachel] Space Telescope Sci Inst, Baltimore, MD USA. [Zauderer, B. A.] Harvard Univ, Cambridge, MA 02138 USA. RP Lazio, JW (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RI Brandt, William/N-2844-2015 OI Brandt, William/0000-0002-0167-2453 FU 6.1 Base funding FX We thank the National Radio Astronomy Observatory staff who provided logistical support for this workshop, particularly K. Ransom and C. Hunsinger. We thank K. Kellermann and L. Walkowicz for helpful discussions. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Basic research in radio astronomy at the Naval Research Laboratory is supported by 6.1 Base funding. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Manuscript (C) 2013. All rights reserved. NR 57 TC 3 Z9 3 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD FEB 1 PY 2014 VL 126 IS 936 BP 196 EP 209 DI 10.1086/675262 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB8ED UT WOS:000332022000007 ER PT J AU Van Den Hoek, J Ozdogan, M Burnicki, A Zhu, AX AF Van Den Hoek, Jamon Ozdogan, Mutlu Burnicki, Amy Zhu, A-Xing TI Evaluating forest policy implementation effectiveness with a cross-scale remote sensing analysis in a priority conservation area of Southwest China SO APPLIED GEOGRAPHY LA English DT Article DE China; Deforestation; Forest policy; Cross-scale; Spatial variability; Natural Forest Protection Program; Sloping Land Conversion Program ID NORTHWEST YUNNAN; ECOSYSTEM SERVICES; TASSELED CAP; LANDSAT DATA; COVER; DEFORESTATION; DISTURBANCE; IMPACT; CLASSIFICATION; REFORESTATION AB China's Natural Forest Protection Program (NFPP) and Sloping Land Conversion Program (SLCP), introduced in 1998 and 1999, respectively, are integral parts of the world's largest reforestation effort. Statereported forest cover data indicate effective policy implementation through net forest cover expansion but overlook the scale-dependence of and spatial variation in forest cover change patterns and also lack reliable data on small-scale and illegal logging. As a result, there is considerable uncertainty over the spatial distribution of forest cover change and ultimately the policies' effectiveness at increasing forest cover. This research uses Landsat Thematic Mapper imagery-derived multitemporal Tasseled Cap variables and a decision tree classifier to map short- and long-term forest cover change across three administrative levels in the priority conservation area of Diqing Tibetan Autonomous Prefecture in Yunnan Province. Results indicate a 73% reduction in the rate of forest cover loss and a more than doubled rate of forest cover gain from 1990-1999 to 1999-2009 across the prefecture, both of which support a positive assessment of policy implementation. However, prefectural results are countered by spatially disparate forest cover gain and loss trends at the county- and township-level in the decade following the policies' introductions. Further, more than half of Diqing's townships, mainly those in the prefecture's south where tourism has been rapidly developing, saw continued net forest cover loss attributable to small-scale timber harvesting for tourism-driven construction. This research thus exposes cross-scale spatially disparate forest cover change indicative of highly differentiated policy implementation effectiveness, and shows the pattern by which regional development has redirected, rather than reduced, forest cover loss, contrary to the goals of the NFPP and SLCP. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Van Den Hoek, Jamon; Zhu, A-Xing] Univ Wisconsin, Dept Geog, Madison, WI 53706 USA. [Ozdogan, Mutlu] Univ Wisconsin, Dept Forest & Wildlife Ecol, Madison, WI 53706 USA. [Burnicki, Amy] Univ Michigan, Sch Nat Resources & Environm, Ann Arbor, MI 48109 USA. RP Van Den Hoek, J (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Code 618-0,8800 Greenbelt Rd, Greenbelt, MD 20711 USA. EM jamon.vandenhoek@nasa.gov OI Van Den Hoek, Jamon/0000-0001-8074-0022; Ozdogan, Mutlu/0000-0002-1707-3375 NR 92 TC 5 Z9 5 U1 3 U2 39 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0143-6228 EI 1873-7730 J9 APPL GEOGR JI Appl. Geogr. PD FEB PY 2014 VL 47 BP 177 EP 189 DI 10.1016/j.apgeog.2013.12.010 PG 13 WC Geography SC Geography GA AB6RX UT WOS:000331918300016 ER PT J AU Shin, DH Mueller, D Choi, T Noh, YM Yoon, YJ Lee, KH Shin, SK Chae, N Kim, K Kim, YJ AF Shin, Dong Ho Mueller, Detlef Choi, Taejin Noh, Young Min Yoon, Young Jun Lee, Kwon H. Shin, Sung Kyun Chae, Namyi Kim, Kwanchul Kim, Young J. TI Influence of wind speed on optical properties of aerosols in the marine boundary layer measured by ship-borne DePolarization Lidar in the coastal area of Korea SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Lidar; Aerosol; Wind speed; Marine boundary layer ID SEA-SALT AEROSOL; FILM DROP PRODUCTION; VERTICAL-DISTRIBUTION; NORTH-ATLANTIC; SAHARAN DUST; BUBBLE-SIZE; SEVERE HAZE; OCEAN; EXTINCTION; PACIFIC AB Shipboard measurements of microphysical and optical properties of marine boundary-layer aerosols were performed around the Korean Peninsula from 2 to 5 December 2009. The measurements were conducted aboard the Korean icebreaking research vessel Araon during cruise tracks in the East Sea of Korea near Busan and Pohang. This paper describes the results of optical aerosol measurements acquired with a Depolarization Lidar (DPL) and an optical particle counter (OPC) and data on meteorological parameters. Backward trajectory analyses indicate that two different aerosol characteristics according to different pathways of air mass were encountered during the cruise. We find a high correlation between wind speeds across the east coast of Korea and extinction coefficient, depolarization ratio and mass concentration Correlation coefficient (R-2) are 0.57, 0.52 and 0.67, respectively. The increase of extinction coefficient, depolarization ratio and number concentration with wind speed may have been caused by the increase of sea-salt aerosol production and transport. Crown Copyright (C) 2013 Published by Elsevier Ltd. All rights reserved. C1 [Shin, Dong Ho; Noh, Young Min; Shin, Sung Kyun; Kim, Kwanchul; Kim, Young J.] Gwangju Inst Sci & Technol, Sch Environm Sci & Engn, Kwangju 500712, South Korea. [Mueller, Detlef] Univ Hertfordshire, Hatfield AL10 9AB, Herts, England. [Mueller, Detlef] NASA Langley Res Ctr, Sci Syst & Applicat Inc, Hampton, VA 23681 USA. [Choi, Taejin; Yoon, Young Jun; Chae, Namyi] Korea Polar Res Inst KOPRI, Inchon, South Korea. [Lee, Kwon H.] Kyungil Univ, Dept Geoinformat Engn, Gyongsan 712701, South Korea. [Chae, Namyi] Yonsei Univ, Seoul 120749, South Korea. RP Mueller, D (reprint author), Univ Hertfordshire, Coll Lane, Hatfield AL10 9AB, Herts, England. EM d.mueller@herts.ac.uk RI MUELLER, DETLEF/F-1010-2015; OI MUELLER, DETLEF/0000-0002-0203-7654; Kim, Kwanchul/0000-0002-7440-6703; Lee, Kwon-Ho/0000-0002-0844-5245 FU Korea Meteorological Administration Research and Development Program [CATER 2012-7080]; project titled 'Korea-Polar Ocean in Rapid Transition (KOPRI)' [PM12020]; Ministry of Oceans and Fisheries, Korea; GEMS program of the Ministry of Environment, Korea; Eco Innovation Program of KEITI [2012000160004] FX This work was funded by the Korea Meteorological Administration Research and Development Program under Grant CATER 2012-7080. This research was a part of the project titled 'Korea-Polar Ocean in Rapid Transition (KOPRI, PM12020)', funded by the Ministry of Oceans and Fisheries, Korea. This research was supported by the GEMS program of the Ministry of Environment, Korea and the Eco Innovation Program of KEITI (2012000160004). The authors gratefully acknowledge the NOAA Air Resources Laboratory (ARL) for the provision of the HYSPLIT transport and dispersion model and/or READY website (http://www.arl.noaa.gov/ready.php). NR 68 TC 4 Z9 4 U1 1 U2 19 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD FEB PY 2014 VL 83 BP 282 EP 290 DI 10.1016/j.atmosenv.2013.10.027 PG 9 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AB3DB UT WOS:000331670400032 ER PT J AU Scowen, PA Perez, MR Neff, SG Benford, DJ AF Scowen, Paul A. Perez, Mario R. Neff, Susan G. Benford, Dominic J. TI Scientific objectives for UV/visible astrophysics investigations: a summary of responsesby the community (2012) SO EXPERIMENTAL ASTRONOMY LA English DT Article DE Conference summary; Astronomical instrumentation; Galaxies; Stars; Extrasolar planets ID SPECTROGRAPH AB Following several recommendations presented by the Astrophysics Decadal Survey 2010 centered around the need to define "a future ultraviolet-optical space capability", on 2012 May 25, NASA issued a Request for Information (RFI) seeking persuasive ultraviolet (UV) and visible wavelength astrophysics science investigations. The goal was to develop a cohesive and compelling set of science objectives that motivate and support the development of the next generation of ultraviolet/visible space astrophysics missions. Responses were due on 10 August 2012 when 34 submissions were received addressing a number of potential science drivers. A UV/visible Mission RFI Workshop was held on 2012 September 20 where each of these submissions was summarized and discussed in the context of each other. We present a scientific analysis of these submissions and presentations and the pursuant measurement capability needs, which could influence ultraviolet/visible technology development plans for the rest of this decade. We also describe the process and requirements leading to the inception of this community RFI, subsequent workshop and the expected evolution of these ideas and concepts for the remainder of this decade. C1 [Scowen, Paul A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Perez, Mario R.] NASA Headquarters, Div Astrophys, Washington, DC 20546 USA. [Neff, Susan G.; Benford, Dominic J.] NASA, Goddard Space Flight Ctr, Cosm Origins Program Off, Greenbelt, MD 20771 USA. RP Scowen, PA (reprint author), Arizona State Univ, Sch Earth & Space Explorat, POB 876004, Tempe, AZ 85287 USA. EM paul.scowen@asu.edu; mario.perez@nasa.gov; susan.g.neff@nasa.gov; dominic.benford@nasa.gov RI Benford, Dominic/D-4760-2012 OI Benford, Dominic/0000-0002-9884-4206 FU Astrophysics Division at NASA Headquarters FX We thanks to all the members of the community that freely and openly participated in the different meetings, teleconferences, workshops, and to the many authors and co-authors of the RFI submissions that made possible the description and analysis presented here. In particular, we are grateful to the executive committee of the COPAG for their generous contributions in their efforts of science and technology prioritization for this theme. The Astrophysics Division at NASA Headquarters funded most of the work presented here related to the RFI, activity managed under the overall Cosmic Origins Program. NR 18 TC 0 Z9 0 U1 0 U2 5 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0922-6435 EI 1572-9508 J9 EXP ASTRON JI Exp. Astron. PD FEB PY 2014 VL 37 IS 1 BP 11 EP 35 DI 10.1007/s10686-013-9363-0 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB3QZ UT WOS:000331706600002 ER PT J AU Kollias, P Tanelli, S Battaglia, A Tatarevic, A AF Kollias, Pavlos Tanelli, Simone Battaglia, Alessandro Tatarevic, Aleksandra TI Evaluation of EarthCARE Cloud Profiling Radar Doppler Velocity Measurements in Particle Sedimentation Regimes SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article DE Satellite observations; Remote sensing; Sampling; Algorithms; Radars/Radar observations ID BOUNDARY-LAYER; SPACEBORNE; RAINFALL; MODELS; UNCERTAINTIES; REFLECTIVITY; PROPOSAL; SPECTRA; SURFACE; SCHEME AB The joint European Space Agency-Japan Aerospace Exploration Agency (ESA-JAXA) Earth Clouds, Aerosols and Radiation Explorer (EarthCARE) mission is scheduled for launch in 2016 and features the first atmospheric Cloud Profiling Radar (CPR) with Doppler capability in space. Here, the uncertainty of the CPR Doppler velocity measurements in cirrus clouds and large-scale precipitation areas is discussed. These regimes are characterized by weak vertical motion and relatively horizontally homogeneous conditions and thus represent optimum conditions for acquiring high-quality CPR Doppler measurements. A large dataset of radar reflectivity observations from ground-based radars is used to examine the homogeneity of the cloud fields at the horizontal scales of interest. In addition, a CPR instrument model that uses as input ground-based radar observations and outputs simulations of CPR Doppler measurements is described. The simulator accurately accounts for the beam geometry, nonuniform beam-filling, and signal integration effects, and it is applied to representative cases of cirrus cloud and stratiform precipitation. The simulated CPR Doppler velocities are compared against those derived from the ground-based radars. The unfolding of the CPR Doppler velocity is achieved using simple conditional rules and a smoothness requirement for the CPR Doppler measurements. The application of nonuniform beam-filling Doppler velocity bias-correction algorithms is found necessary even under these optimum conditions to reduce the CPR Doppler biases. Finally, the analysis indicates that a minimum along-track integration of 5000 m is needed to reduce the uncertainty in the CPR Doppler measurements to below 0.5 m s(-1) and thus enable the detection of the melting layer and the characterization of the rain- and ice-layer Doppler velocities. C1 [Kollias, Pavlos; Tatarevic, Aleksandra] McGill Univ, Dept Atmospher & Ocean Sci, Montreal, PQ H3A 0B9, Canada. [Tanelli, Simone] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Battaglia, Alessandro] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Battaglia, Alessandro] Univ Bonn, Inst Meteorol, Bonn, Germany. RP Kollias, P (reprint author), McGill Univ, Dept Atmospher & Ocean Sci, Room 945,Burnside Hall,805 Sherbrooke St West, Montreal, PQ H3A 0B9, Canada. EM pavlos.kollias@mcgill.ca OI Battaglia, Alessandro/0000-0001-9243-3484 FU European Space Agency under the Doppler Air Motion Estimate project; STSE program; National Aeronautics and Space Administration; NASA SALMON/USPI FX This work was supported by the European Space Agency under the Doppler Air Motion Estimate project funded by the STSE program. The contributions by Simone Tanelli were performed at the Jet Propulsion Laboratory under contract with the National Aeronautics and Space Administration. Support for the Instrument Simulator Suite for Atmospheric Remote Sensing project from the Advanced Information Systems Technology program and for the Doppler Velocity Products for the EarthCARE mission from the NASA SALMON/USPI programs are gratefully acknowledged. Dr. Battaglia acknowledges the NCEO EO Mission Support. NR 37 TC 11 Z9 11 U1 0 U2 9 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD FEB PY 2014 VL 31 IS 2 BP 366 EP 386 DI 10.1175/JTECH-D-11-00202.1 PG 21 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA AA3XX UT WOS:000331029600007 ER PT J AU Menzies, RT Spiers, GD Jacob, J AF Menzies, Robert T. Spiers, Gary D. Jacob, Joseph TI Airborne Laser Absorption Spectrometer Measurements of Atmospheric CO2 Column Mole Fractions: Source and Sink Detection and Environmental Impacts on Retrievals SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article DE Lidars/Lidar observations; Aircraft observations; Remote sensing ID SURFACE WIND-SPEED; 1.57 MU-M; DIFFERENTIAL ABSORPTION; LIDAR MEASUREMENTS; MIXING-RATIO; OPTIMIZATION; REFLECTANCE; PARAMETERS; SPECTRA; REGIONS AB This paper provides atmospheric CO2 column abundance measurement results from a summer 2011 series of flights of a 2.05-mu m laser absorption spectrometer on the NASA DC-8 research aircraft. The integrated path differential absorption (IPDA) method is used for the CO2 column mole fraction retrievals. This instrument and the data analysis methodology developed to achieve retrievals over complex terrain and variable atmospheric conditions provide insight into the capabilities of the IPDA method for both airborne measurements and future global-scale CO2 measurements from low-Earth orbit pertinent to the proposed NASA Active Sensing of CO2 Emissions over Nights, Days, and Seasons (ASCENDS) mission. Demonstrated in this paper is the capability to measure CO2 drawdown caused by crop activity during a midday flight over the U.S. upper Midwest area. In addition, an example is provided of high spatial resolution measurements of CO2 plumes from individual stack clusters of the Four Corners Power Plant in northwestern New Mexico. Complex terrain, the spectral properties of the aboveground scatterers, and potential cloud contamination are factors that complicate the column abundance retrieval. The impacts of these factors and various means of minimizing these influences in the retrievals are discussed. C1 [Menzies, Robert T.; Spiers, Gary D.; Jacob, Joseph] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Menzies, RT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM rmenzies@jpl.nasa.gov FU National Aeronautics and Space Administration FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 37 TC 8 Z9 8 U1 2 U2 19 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD FEB PY 2014 VL 31 IS 2 BP 404 EP 421 DI 10.1175/JTECH-D-13-00128.1 PG 18 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA AA3XX UT WOS:000331029600009 ER PT J AU Holstein-Rathlou, C Merrison, J Iversen, JJ Jakobsen, AB Nicolajsen, R Nornberg, P Rasmussen, K Merlone, A Lopardo, G Hudson, T Banfield, D Portyankina, G AF Holstein-Rathlou, C. Merrison, J. Iversen, J. J. Jakobsen, A. B. Nicolajsen, R. Nornberg, P. Rasmussen, K. Merlone, A. Lopardo, G. Hudson, T. Banfield, D. Portyankina, G. TI An Environmental Wind Tunnel Facility for Testing Meteorological Sensor Systems SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article DE Boundary layer; Planetary atmospheres; Atmosphere-land interaction; Atmospheric circulation; Wind; Instrumentation/sensors ID LASER ANEMOMETER; MARS; CALIBRATION; TRANSPORT AB Reliable and accurate environmental sensing is a cornerstone of modern meteorology. This paper presents a laboratory environmental simulator capable of reproducing extreme environments and performing tests and calibrations of meteorological sensor systems under controlled conditions. This facility is available to the research community as well as industry and is intended to encourage advancement in the field of sensor metrology applied to meteorology and climatology. Discussion will be made of the temperature, pressure, humidity and wind flow control, and sensing systems with reference to specific sensor test programs and future research activities. C1 [Holstein-Rathlou, C.; Merrison, J.; Iversen, J. J.; Jakobsen, A. B.; Nicolajsen, R.] Aarhus Univ, Dept Phys & Astron, Aarhus, Denmark. [Nornberg, P.; Rasmussen, K.] Aarhus Univ, Dept Geosci, Aarhus, Denmark. [Merlone, A.; Lopardo, G.] Ist Nazl Ric Metrol, Turin, Italy. [Hudson, T.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Banfield, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Portyankina, G.] Univ Bern, Inst Phys, Bern, Switzerland. RP Holstein-Rathlou, C (reprint author), Ctr Space Phys, 725 Commonwealth Ave, Boston, MA 02134 USA. EM rathlou@bu.edu RI Rasmussen, Keld/A-4079-2012; OI Rasmussen, Keld/0000-0003-1625-4163; Banfield, Don/0000-0003-2664-0164; merrison, jonathan/0000-0003-4362-6356 FU European Metrology Research Programme (EMRP); 18 European National Institutes of Metrology; EMRP within the EURAMET; European Union; ESA; Villum Foundation; Jet Propulsion Laboratory; California Institute of Technology; National Aeronautics and Space Administration FX This research was performed in connection with the European MeteoMet project, which is cofunded by the European Metrology Research Programme (EMRP) and 18 European National Institutes of Metrology. This work is being developed within the frame of the EMRP, which is jointly funded by the EMRP's participating countries within the EURAMET and the European Union. We thank ESA and the Villum Foundation for financial support to the wind tunnel facility. Part of the research was funded by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 14 TC 4 Z9 4 U1 2 U2 13 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD FEB PY 2014 VL 31 IS 2 BP 447 EP 457 DI 10.1175/JTECH-D-13-00141.1 PG 11 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA AA3XX UT WOS:000331029600012 ER PT J AU Fu, LL Ubelmann, C AF Fu, Lee-Lueng Ubelmann, Clement TI On the Transition from Profile Altimeter to Swath Altimeter for Observing Global Ocean Surface Topography SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article DE Satellite observations; Remote sensing; Radars/Radar observations; Altimetry ID RESOLUTION ALTIMETRY; SEA; CHALLENGES AB Conventional radar altimeter makes measurement of sea surface height (SSH) in one-dimensional profiles along the ground tracks of a satellite. Such profiles are combined via various mapping techniques to construct two-dimensional SSH maps, providing a valuable data record over the past two decades for studying the global ocean circulation and sea level change. However, the spatial resolution of the SSH is limited by both coarse sampling across the satellite tracks and the instrument error in the profile measurements. A new satellite mission based on radar interferometry offers the capability of making high-resolution wide-swath measurement of SSH. This mission is called Surface Water and Ocean Topography (SWOT), which will demonstrate the application of swath altimeter to both oceanography and land hydrology. This paper presents a brief introduction to the design of SWOT, its performance specification for SSH, and the anticipated spatial resolution and coverage, demonstrating the promise of SWOT for fundamental advancement in observing SSH. A main objective of the paper is to address issues in the anticipated transition of conventional profile altimetry to swath altimetry in the future-in particular, the need for consistency of the new observing system with the old for extending the existing data record into the future. A viable approach is to carry a profile altimeter in the SWOT payload to provide calibration and validation of the new measurement against the old at large scales. This is the baseline design of SWOT. The unique advantages of the approach are discussed in the context of a new standard for observing the global SSH in the future. C1 [Fu, Lee-Lueng; Ubelmann, Clement] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Fu, LL (reprint author), CALTECH, Jet Prop Lab, MS 300-329,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM llf@jpl.nasa.gov FU SWOT projects FX The research presented in the paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautic and Space Administration. We are grateful to Dr. Zhijin Li of JPL, Dr. Yi Chao of Remote Sensing Solutions, and Dr. Carrie Zhang of the Joint Institute for Regional Earth System Science and Engineering of UCLA for providing comprehensive assistance with the modeling simulation presented in Fig. 4. Support from the SWOT projects is acknowledged. NR 20 TC 22 Z9 22 U1 1 U2 16 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD FEB PY 2014 VL 31 IS 2 BP 560 EP 568 DI 10.1175/JTECH-D-13-00109.1 PG 9 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA AA3XX UT WOS:000331029600021 ER PT J AU Batra, AK Chilvery, AK Guggilla, P Aggarwal, M Currie, JR AF Batra, Ashok K. Chilvery, A. K. Guggilla, Padmaja Aggarwal, Mohan Currie, James R., Jr. TI Micro- and Nano-Structured Metal Oxides Based Chemical Sensors: An Overview SO JOURNAL OF NANOSCIENCE AND NANOTECHNOLOGY LA English DT Review DE Chemical Sensors; Nanostructured Chemical Sensors; Nanorods; Nanotubes; Nanocomposite; Binary Metal Oxide Composite; Volatile Organic Compound ID GAS-SENSING PROPERTIES; SURFACE-ACOUSTIC-WAVE; DOPED SNO2 NANOWIRES; TIN-OXIDE; ROOM-TEMPERATURE; THIN-FILMS; SEMICONDUCTING OXIDES; NANOCRYSTALLINE SNO2; ZNO; NO2 AB This article examines various kinds of chemical sensors, their mechanism of operation and the ways to improve their performance. It reports the results of exploratory investigation of binary composite polycrystalline thick-films such as SnO2-WO3, SnO2-In2O3, and SnO2-ZnO for the detection of volatile organic compound (isopropanol) are reported. It also contains an overview on the status of the new types of metal oxide based nanostructured sensors, such as nano belts, nanorods, nanotubes, nanofibers, nanocomposites, etc. C1 [Batra, Ashok K.; Chilvery, A. K.; Guggilla, Padmaja; Aggarwal, Mohan] Alabama A&M Univ, Dept Phys Chem & Math, Normal, AL 35762 USA. [Currie, James R., Jr.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35012 USA. RP Batra, AK (reprint author), Alabama A&M Univ, Dept Phys Chem & Math, POB 1268, Normal, AL 35762 USA. FU National Science Foundation [EPSCoR R-II-3 (EPS-1158862), HBCU-UP-0928904-HRD]; DHS [2010-ST-062-000034] FX The authors gratefully acknowledge support for this work through the National Science Foundation grant #EPSCoR R-II-3 (EPS-1158862), HBCU-UP-0928904-HRD grant, and DHS grant #2010-ST-062-000034. The authors extend special appreciation to Professor Emeritus R. B. Lal for his keen interest in the subject, and thanks to Mr. Garland Sharp for fabrication of the vapor test system and Ms. Sheral Roberson for graphics. NR 120 TC 14 Z9 14 U1 9 U2 172 PU AMER SCIENTIFIC PUBLISHERS PI VALENCIA PA 26650 THE OLD RD, STE 208, VALENCIA, CA 91381-0751 USA SN 1533-4880 EI 1533-4899 J9 J NANOSCI NANOTECHNO JI J. Nanosci. Nanotechnol. PD FEB PY 2014 VL 14 IS 2 BP 2065 EP 2085 DI 10.1166/jnn.2014.9266 PG 21 WC Chemistry, Multidisciplinary; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA AB2FP UT WOS:000331608900065 PM 24749474 ER PT J AU Elipot, S Frajka-Williams, E Hughes, CW Willis, JK AF Elipot, Shane Frajka-Williams, Eleanor Hughes, Chris W. Willis, Josh K. TI The Observed North Atlantic Meridional Overturning Circulation: Its Meridional Coherence and Ocean Bottom Pressure SO JOURNAL OF PHYSICAL OCEANOGRAPHY LA English DT Article ID VARIABILITY; 26-DEGREES-N; TRANSPORTS; ARRAY; MOC AB Analyses of meridional transport time series from the Rapid Climate Change-Meridional Overturning Circulation (RAPID MOC) array at 26 degrees N and from Argo float and altimetry data at 41 degrees N reveal that, at semiannual and longer time scales, the contribution from the western boundary dominates the variability of the North Atlantic meridional overturning circulation (MOC), defined as the transport in the upper 1000 m of the ocean. Because the variability of the western boundary contribution is associated with a geostrophic overturning, it is reflected in independent estimates of transports from gradient of ocean bottom pressure (OBP) relative to and below 1000 m on the continental slope of the western boundary at three nominal latitudes (26 degrees, 39 degrees, and 42.5 degrees N). Time series of western meridional transports relative to and below 1000 m derived from the OBP gradient, or equivalently derived from the transport shear profile, exhibit approximately the same phase relationship between 26 degrees and 39 degrees-42.5 degrees N as the western contribution to the geostrophic MOC time series do: the western geostrophic MOC at 41 degrees N precedes the MOC at 26 degrees N by approximately a quarter of an annual cycle, resulting in a zero correlation at this time scale. This study therefore demonstrates how OBP gradients on basin boundaries can be used to monitor the MOC and its meridional coherence. C1 [Elipot, Shane; Hughes, Chris W.] Natl Oceanog Ctr, Liverpool, Merseyside, England. [Frajka-Williams, Eleanor] Univ Southampton, Natl Oceanog Ctr, Southampton, Hants, England. [Willis, Josh K.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Elipot, S (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, 4600 Rickenbacker Causeway, Miami, FL 33149 USA. EM selipot@rsmas.miami.edu RI Frajka-Williams, Eleanor/H-2415-2011; OI Frajka-Williams, Eleanor/0000-0001-8773-7838; Hughes, Chris/0000-0002-9355-0233 FU U.K. Natural Environment Research Council of the RAPID program; U.S. National Science Foundation; U.K. Natural Environment Research Council FX This work was supported by the U.K. Natural Environment Research Council as part of the RAPID program. Part of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Thanks to Miguel angel Morales Maqueda for supervising the deployment and recovery of the data. Conversations with Ric Williams and Sofia Olhede were helpful in the development of this work. Data from the RAPID-MOCHA program are funded by the U.S. National Science Foundation and U.K. Natural Environment Research Council (and are freely available at http://www.rapid.ac.uk/rapidmoc/ and www.rsmas.miami.edu/users/mocha). NR 34 TC 10 Z9 10 U1 2 U2 16 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-3670 EI 1520-0485 J9 J PHYS OCEANOGR JI J. Phys. Oceanogr. PD FEB PY 2014 VL 44 IS 2 BP 517 EP 537 DI 10.1175/JPO-D-13-026.1 PG 21 WC Oceanography SC Oceanography GA AA3VY UT WOS:000331024500007 ER PT J AU Smith, S Watts, N Hans, D LeBlanc, A Spector, E Evans, H King, L Sibonga, J AF Smith, S. Watts, N. Hans, D. LeBlanc, A. Spector, E. Evans, H. King, L. Sibonga, J. TI TBS (TRABECULAR BONE SCORE) EXPANDS UNDERSTANDING OF SPACEFLIGHT EFFECTS ON THE LUMBAR SPINE OF LONG-DURATION ASTRONAUTS SO OSTEOPOROSIS INTERNATIONAL LA English DT Meeting Abstract CT International-Osteoporosis-Foundation (IOF) - International-Society-for-Clinical-Densitometry (ISCD) Skeletal Health Meeting CY FEB 20-22, 2014 CL Orlando, FL SP Int Osteoporosis Fdn, Int Soc Clin Densitometry C1 [Smith, S.; Spector, E.; Evans, H.; King, L.] Wyle, Bone & Mineral Lab, Houston, TX USA. [Watts, N.] Mercy Hlth, Cincinnati, OH USA. [Hans, D.] Univ Lausanne, Lausanne, Switzerland. [LeBlanc, A.] USRA, Houston, TX USA. [Evans, H.] Wyle, Houston, TX USA. [Sibonga, J.] NASA JSC, Bone & Mineral Lab, Houston, TX USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER LONDON LTD PI LONDON PA 236 GRAYS INN RD, 6TH FLOOR, LONDON WC1X 8HL, ENGLAND SN 0937-941X EI 1433-2965 J9 OSTEOPOROSIS INT JI Osteoporosis Int. PD FEB PY 2014 VL 25 SU 1 BP S53 EP S53 PG 1 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA AB3ML UT WOS:000331694800083 ER PT J AU Wang, L Eldridge, JI Guo, SM AF Wang, Li Eldridge, Jeffrey I. Guo, S. M. TI Comparison of different models for the determination of the absorption and scattering coefficients of thermal barrier coatings SO ACTA MATERIALIA LA English DT Article DE Thermal barrier coatings; Plasma spraying; Yttria-stabilized zirconia; Thermal radiation; Modeling ID TAILORED MICROSTRUCTURE; RADIATIVE PROPERTIES; MIE THEORY; EB-PVD; REFLECTANCE; ZIRCONIA; CONDUCTIVITY; TEMPERATURES; 2-FLUX; LAYERS AB The thermal radiative properties of thermal barrier coatings (TBCs) are becoming more important as the inlet temperatures of advanced gas-turbine engines are continuously being pushed higher in order to improve efficiency. To determine the absorption and scattering coefficients of TBCs, four-flux, two-flux and Kubelka-Munk models were introduced and used to characterize the thermal radiative properties of plasma-sprayed yttria-stabilized zirconia (YSZ) coatings. The results show that the absorption coefficient of YSZ is extremely low for wavelengths <6 mu m and the scattering coefficient is high and decreases with increasing wavelength. The obvious deviation of absorption and scattering coefficients obtained by the Kubelka-Munk model from those values calculated by four-flux and two-flux models indicates that surface reflection is an important parameter which cannot be neglected when characterizing the radiative property of the coating. The excellent agreement of predicted reflectance and transmittance spectra by the two-flux and four-flux models for coating thicknesses >200 mu m suggests that when the coating thickness is larger than around twice the average scattering distance, the collimated flux can be simply treated as a diffuse flux inside the coating, and thus the two-flux model can be used to determine the absorption and scattering coefficients as a simplification of the four-flux model. (C) 2013 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved. C1 [Wang, Li; Guo, S. M.] Louisiana State Univ, Dept Mech & Ind Engn, Baton Rouge, LA 70803 USA. [Eldridge, Jeffrey I.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Guo, SM (reprint author), Louisiana State Univ, Dept Mech & Ind Engn, Baton Rouge, LA 70803 USA. EM sguo2@lsu.edu FU NASA [NNX09AP72A] FX This research is sponsored by NASA under Cooperative Agreement No. NNX09AP72A. NR 37 TC 10 Z9 11 U1 2 U2 32 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-6454 EI 1873-2453 J9 ACTA MATER JI Acta Mater. PD FEB PY 2014 VL 64 BP 402 EP 410 DI 10.1016/j.actamat.2013.10.053 PG 9 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA AA3TW UT WOS:000331017800038 ER PT J AU Brenneman, LW Madejski, G Fuerst, F Matt, G Elvis, M Harrison, FA Ballantyne, DR Boggs, SE Christensen, FE Craig, WW Fabian, AC Grefenstette, BW Hailey, CJ Madsen, KK Marinucci, A Rivers, E Stern, D Walton, DJ Zhang, WW AF Brenneman, L. W. Madejski, G. Fuerst, F. Matt, G. Elvis, M. Harrison, F. A. Ballantyne, D. R. Boggs, S. E. Christensen, F. E. Craig, W. W. Fabian, A. C. Grefenstette, B. W. Hailey, C. J. Madsen, K. K. Marinucci, A. Rivers, E. Stern, D. Walton, D. J. Zhang, W. W. TI MEASURING THE CORONAL PROPERTIES OF IC 4329A WITH NuSTAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion; accretion disks; galaxies: active; galaxies: individual (IC 4329A); galaxies: nuclei galaxies: Seyfert; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; X-RAY-SPECTRA; SEYFERT-GALAXIES; COMPTONIZATION MODELS; BEPPOSAX OBSERVATIONS; IC-4329A; EMISSION; CATALOG; SUZAKU AB We present an analysis of a similar to 160 ks NuSTAR observation of the nearby bright Seyfert galaxy IC 4329A. The high-quality broadband spectrum enables us to separate the effects of distant reflection from the direct coronal continuum, and to therefore accurately measure the high-energy cutoff to be E-cut = 178(-40)(+74) keV. The coronal emission arises from accretion disk photons Compton up-scattered by a thermal plasma, with the spectral index and cutoff being due to a combination of the finite plasma temperature and optical depth. Applying standard Comptonization models, we measure both physical properties independently using the best signal to noise obtained to date in an active galactic nucleus over the 3-79 keV band. We derive kTe = 37+ 6 keV with tau = 1.25(-0.10)(+0.20) assuming a slab geometry for the plasma, and kT(e) = 33(-6)(+6) keV with tau = 3.41(-0.38)(+0.58) for a spherical geometry, with both having an equivalent goodness-of-fit. C1 [Brenneman, L. W.; Elvis, M.] Harvard Smithsonian CfA, Cambridge, MA 02138 USA. [Madejski, G.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Fuerst, F.; Harrison, F. A.; Grefenstette, B. W.; Madsen, K. K.; Rivers, E.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Matt, G.; Marinucci, A.] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 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, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Brenneman, LW (reprint author), Harvard Smithsonian CfA, 60 Garden St MS-67, Cambridge, MA 02138 USA. RI Boggs, Steven/E-4170-2015 OI Boggs, Steven/0000-0001-9567-4224 FU NASA [NNG08FD60C, NNX13AE90G]; National Aeronautics and Space Administration; Italian Space Agency [ASI/INAF 1/037/12/0-011/13] 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). L. B. gratefully acknowledges funding from NASA grant NNX13AE90G. G. M. and A. M. acknowledge financial support from the Italian Space Agency under contract ASI/INAF 1/037/12/0-011/13. NR 40 TC 17 Z9 17 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2014 VL 781 IS 2 AR 83 DI 10.1088/0004-637X/781/2/83 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5WV UT WOS:000331171200027 ER PT J AU Donato, D Cenko, SB Covino, S Troja, E Pursimo, T Cheung, CC Fox, O Kutyrev, A Campana, S Fugazza, D Landt, H Butler, NR AF Donato, D. Cenko, S. B. Covino, S. Troja, E. Pursimo, T. Cheung, C. C. Fox, O. Kutyrev, A. Campana, S. Fugazza, D. Landt, H. Butler, N. R. TI A TIDAL DISRUPTION EVENT IN A NEARBY GALAXY HOSTING AN INTERMEDIATE MASS BLACK HOLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (A1795); galaxies: general; galaxies: nuclei; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; GAMMA-RAY BURSTS; DIGITAL SKY SURVEY; SEYFERT 1 GALAXIES; X-RAY; XMM-NEWTON; STELLAR DISRUPTION; ABELL 1795; SPACE-TELESCOPE; RADIO-EMISSION AB We report the serendipitous discovery of a bright point source flare in the Abell cluster A1795 with archival EUVE and Chandra observations. Assuming the EUVE emission is associated with the Chandra source, the X-ray 0.5-7 keV flux declined by a factor of similar to 2300 over a time span of 6 yr, following a power-law decay with index similar to 2.44 +/- 0.40. The Chandra data alone vary by a factor of similar to 20. The spectrum is well fit by a blackbody with a constant temperature of kT similar to 0.09 keV (similar to 10(6) K). The flare is spatially coincident with the nuclear region of a faint, inactive galaxy with a photometric redshift consistent at the la level with the cluster (z = 0.062476). We argue that these properties are indicative of a tidal disruption of a star by a black hole (BH) with log(M-BH/M-O) similar to 5.5 +/- 0.5. If so, such a discovery indicates that tidal disruption flares may be used to probe BHs in the intermediate mass range, which are very difficult to study by other means. C1 [Donato, D.; Troja, E.] NASA, GSFC, CRESST, Greenbelt, MD 20771 USA. [Donato, D.; Troja, E.] NASA, GSFC, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. [Donato, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Cenko, S. B.; Fox, O.] NASA, GSFC, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Cenko, S. B.; Campana, S.; Fugazza, D.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Covino, S.] INAF, Osservatorio Astronom Brera, I-23807 Merate, LC, Italy. [Pursimo, T.] Nord Opt Telescope, E-38700 Santa Cruz De La Palma, Spain. [Cheung, C. C.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Kutyrev, A.] NASA, GSFC, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Landt, H.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Butler, N. R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. RP Donato, D (reprint author), NASA, GSFC, CRESST, Greenbelt, MD 20771 USA. EM davide.donato-1@nasa.gov OI Campana, Sergio/0000-0001-6278-1576; Covino, Stefano/0000-0001-9078-5507 FU NSF [AST-9987045]; NSF Telescope System Instrumentation Program (TSIP); Ohio Board of Regents; Ohio State University Office of Research; UNAM; CONACyT; NASA; H2RG; NRL by a Karles' Fellowship; NASA [DPR S-15633-Y]; European Union FX The LBT is an international collaboration among institutions in the United States, Italy, and Germany. LBT Corporation partners are The University of Arizona on behalf of the Arizona university system; Istituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany, representing the MaxPlanck Society, the Astrophysical Institute Potsdam, and Heidelberg University; The Ohio State University; and The Research Corporation, on behalf of The University of Notre Dame, University of Minnesota, and University of Virginia. This paper used data obtained with the MODS spectrographs built with funding from NSF grant AST-9987045 and the NSF Telescope System Instrumentation Program (TSIP), with additional funds from the Ohio Board of Regents and the Ohio State University Office of Research.; We thank the staff of the Observatorio Astronomico Nacional on Sierra San Pedro Martir and the RATIR instrument team (ratir.astroscu.unam.mx). RATIR observations with the Harold L. Johnson 1.5 m telescope of the Obervatorio Astronomico Nacional on Sierra San Pedro Martir are partially funded by UNAM, CONACyT and NASA, and supported by the loan of an H2RG detector by Teledyne Scientific and Imaging.; C.C.C. was supported at NRL by a Karles' Fellowship and NASA DPR S-15633-Y.; H.L. acknowledges financial support by the European Union through the COFUND scheme. NR 117 TC 19 Z9 19 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2014 VL 781 IS 2 AR 59 DI 10.1088/0004-637X/781/2/59 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5WV UT WOS:000331171200003 ER PT J AU Hirano, S Hosokawa, T Yoshida, N Umeda, H Omukai, K Chiaki, G Yorke, HW AF Hirano, Shingo Hosokawa, Takashi Yoshida, Naoki Umeda, Hideyuki Omukai, Kazuyuki Chiaki, Gen Yorke, Harold W. TI ONE HUNDRED FIRST STARS: PROTOSTELLAR EVOLUTION AND THE FINAL MASSES SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; early universe; stars: evolution; stars: formation; stars: population III; stars: pre-main sequence ID OBSERVATIONS COSMOLOGICAL INTERPRETATION; SUPERMASSIVE BLACK-HOLES; POPULATION III BINARIES; LONG-TERM EVOLUTION; LAMBDA-CDM UNIVERSE; PRIMORDIAL STAR; RADIATIVE FEEDBACK; LAYERED ACCRETION; METAL ENRICHMENT; MAGNETIC-FIELDS AB We perform a large set of radiation hydrodynamic simulations of primordial star formation in a fully cosmological context. Our statistical sample of 100 First Stars shows that the first generation of stars has a wide mass distribution M-popIII = 10 similar to 1000 M-O. We first run cosmological simulations to generate a set of primordial star-forming gas clouds. We then follow protostar formation in each gas cloud and the subsequent protostellar evolution until the gas mass accretion onto the protostar is halted by stellar radiative feedback. The accretion rates differ significantly among the primordial gas clouds that largely determine the final stellar masses. For low accretion rates, the growth of a protostar is self-regulated by radiative feedback effects, and the final mass is limited to several tens of solar masses. At high accretion rates the protostar's outer envelope continues to expand, and the effective surface temperature remains low; such protostars do not exert strong radiative feedback and can grow in excess of 100 solar masses. The obtained wide mass range suggests that the first stars play a variety of roles in the early universe, by triggering both core-collapse supernovae and pair-instability supernovae as well as by leaving stellar mass black holes. We find certain correlations between the final stellar mass and the physical properties of the star-forming cloud. These correlations can be used to estimate the mass of the first star from the properties of the parent cloud or of the host halo without following the detailed protostellar evolution. C1 [Hirano, Shingo; Umeda, Hideyuki] Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Hosokawa, Takashi] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. [Hosokawa, Takashi] Univ Tokyo, Res Ctr Early Universe, Tokyo 1130033, Japan. [Yoshida, Naoki; Chiaki, Gen] Univ Tokyo, Sch Sci, Dept Phys, Tokyo 1130033, Japan. [Yoshida, Naoki] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. [Omukai, Kazuyuki] Tohoku Univ, Astron Inst, Sendai, Miyagi 9808578, Japan. [Yorke, Harold W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hirano, S (reprint author), Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. EM hirano@astron.s.u-tokyo.ac.jp NR 86 TC 141 Z9 141 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2014 VL 781 IS 2 AR 60 DI 10.1088/0004-637X/781/2/60 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5WV UT WOS:000331171200004 ER PT J AU Jones, BM Kaiser, RI Strazzulla, G AF Jones, Brant M. Kaiser, Ralf I. Strazzulla, Giovanni TI UV-VIS, INFRARED, AND MASS SPECTROSCOPY OF ELECTRON IRRADIATED FROZEN OXYGEN AND CARBON DIOXIDE MIXTURES WITH WATER SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: laboratory: molecular; methods: laboratory: solid state; planets and satellites: physical evolution; planets and satellites: surfaces; techniques: photometric ID INTERSTELLAR ICE ANALOGS; SOLAR-SYSTEM ICES; COSMIC-RAY PARTICLES; ION IRRADIATION; HYDROGEN-PEROXIDE; GALILEAN SATELLITES; OZONE SYNTHESIS; OPTICAL-PROPERTIES; REFRACTIVE-INDEX; ABSORPTION-BAND AB Ozone has been detected on the surface of Ganymede via observation of the Hartley band through the use of ultraviolet spectroscopy and is largely agreed upon to be formed by radiolytic processing via interaction of magnetospheric energetic ions and/or electrons with oxygen-bearing ices on Ganymede's surface. Interestingly, a clearly distinct band near 300 nm within the shoulder of the UV-Vis spectrum of Ganymede was also observed, but currently lacks an acceptable physical or chemical explanation. Consequently, the primary motivation behind this work was the collection of UV-Vis absorption spectroscopy of ozone formation by energetic electron bombardment of a variety of oxygen-bearing ices (oxygen, carbon dioxide, water) relevant to this moon as well as other solar system. Ozone was indeed synthesized in pure ices of molecular oxygen, carbon dioxide and a mixture of water and oxygen, in agreement with previous studies. The Hartley band of the ozone synthesized in these ice mixtures was observed in the UV-Vis spectra and compared with the spectrum of Ganymede. In addition, a solid state ozone absorption cross section of 6.0 +/- 0.6 x 10(-1)7 cm(2) molecule(-1) was obtained from the UV-Vis spectral data. Ozone was not produced in the irradiated carbon dioxide-water mixtures; however, a spectrally "red" UV continuum is observed and appears to reproduce well what is observed in a large number of icy moons such as Europa. C1 [Jones, Brant M.; Kaiser, Ralf I.] Univ Hawaii, Dept Chem, WM Keck Res Lab Astrochem, Honolulu, HI 96822 USA. [Jones, Brant M.; Kaiser, Ralf I.] Univ Hawaii, NASA, Astrobiol Inst, Honolulu, HI 96822 USA. [Strazzulla, Giovanni] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy. RP Jones, BM (reprint author), Univ Hawaii, Dept Chem, WM Keck Res Lab Astrochem, Honolulu, HI 96822 USA. OI Strazzulla, Giovanni/0000-0003-1412-4023 FU W. M. Keck Foundation; University of Hawaii at Manoa; National Aeronautics and Space Administration through the NASA Astrobiology Institute [NNA09DA77A] FX B.M.J. and R.I.K. would like to thank the W. M. Keck Foundation and The University of Hawaii at Manoa for their generous financial support (80%). G. S. would like to acknowledge support from the National Aeronautics and Space Administration through the NASA Astrobiology Institute (20%; Cooperative Agreement No. NNA09DA77A issued through the Office of Space Science). NR 115 TC 12 Z9 12 U1 2 U2 17 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 FEB 1 PY 2014 VL 781 IS 2 AR 85 DI 10.1088/0004-637X/781/2/85 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5WV UT WOS:000331171200029 ER PT J AU Krivonos, RA Tomsick, JA Bauer, FE Baganoff, FK Barriere, NM Bodaghee, A Boggs, SE Christensen, FE Craig, WW Grefenstette, BW Hailey, CJ Harrison, FA Hong, J Madsen, KK Mori, K Nynka, M Stern, D Zhang, WW AF Krivonos, Roman A. Tomsick, John A. Bauer, Franz E. Baganoff, Frederick K. Barriere, Nicolas M. Bodaghee, Arash Boggs, Steven E. Christensen, Finn E. Craig, William W. Grefenstette, Brian W. Hailey, Charles J. Harrison, Fiona A. Hong, JaeSub Madsen, Kristin K. Mori, Kaya Nynka, Melania Stern, Daniel Zhang, William W. TI FIRST HARD X-RAY DETECTION OF THE NON-THERMAL EMISSION AROUND THE ARCHES CLUSTER: MORPHOLOGY AND SPECTRAL STUDIES WITH NuSTAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays - Galaxy; center - ISM; general - X-rays; individual (Arches cluster) ID SGR-A-ASTERISK; XMM-NEWTON OBSERVATION; GALACTIC-CENTER REGION; MOLECULAR CLOUDS; LINE EMISSION; STELLAR CLUSTERS; BRIGHTEST FLARE; MASSIVE STARS; DISCOVERY; CHANDRA AB The Arches cluster is a young, densely packed massive star cluster in our Galaxy that shows a high level of star formation activity. The nature of the extended non-thermal X-ray emission around the cluster remains unclear. The observed bright Fe Ku line emission at 6.4 keV from material that is neutral or in a low ionization state can be produced either by X-ray photoionization or by cosmic-ray particle bombardment or both. In this paper, we report on the first detection of the extended emission around the Arches cluster above 10 keV with the NuSTAR mission, and present results on its morphology and spectrum. The spatial distribution of the hard X-ray emission is found to be consistent with the broad region around the cluster where the 6.4 keV line is observed. The interpretation of the hard X-ray emission within the context of the X-ray reflection model puts a strong constraint on the luminosity of the possible illuminating hard X-ray source. The properties of the observed emission are also in broad agreement with the low-energy cosmic-ray proton excitation scenario. C1 [Krivonos, Roman A.; Tomsick, John A.; Barriere, Nicolas M.; Bodaghee, Arash; Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Bauer, Franz E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, Franz E.] Space Sci Inst, Boulder, CO 80301 USA. [Baganoff, Frederick K.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Christensen, Finn E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Grefenstette, Brian W.; Harrison, Fiona A.; Madsen, Kristin K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Hailey, Charles J.; Mori, Kaya; Nynka, Melania] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Hong, JaeSub] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Krivonos, RA (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM krivonos@ssl.berkeley.edu RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Madsen, Kristin/0000-0003-1252-4891; Krivonos, Roman/0000-0003-2737-5673 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration 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). F. E. B. acknowledges support from Basal-CATA (PFB- 06/2007) and CONICYT- Chile (FONDECYT 1101024 and Anillo ACT1101). R. K. thanks Eugene Churazov for fruitful discussions and valuable suggestions to the paper. Facility: NuSTAR NR 50 TC 10 Z9 10 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2014 VL 781 IS 2 DI 10.1088/0004-637X/781/2/107 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5WV UT WOS:000331171200051 ER PT J AU Moya, PS Navarro, R Vinas, AF Munoz, V Valdivia, JA AF Moya, P. S. Navarro, R. Vinas, A. F. Munoz, V. Valdivia, J. A. TI WEAK TURBULENCE CASCADING EFFECTS IN THE ACCELERATION AND HEATING OF IONS IN THE SOLAR WIND SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; methods: numerical; plasmas; solar wind; turbulence; waves ID CYCLOTRON INSTABILITY; CORONAL HOLES; HYBRID SIMULATIONS; MINOR IONS; VELOCITY DISTRIBUTIONS; RESONANT ACCELERATION; THERMAL ANISOTROPY; ALFVEN WAVES; FLUCTUATIONS; PROTONS AB We study the wave-particle interaction and the evolution of electromagnetic waves propagating through a solarwind- like plasma composed of cold electrons, isotropic protons, and a small portion of drifting anisotropic He+2 (T-perpendicular to alpha = 6 T-parallel to alpha) and O+6 (T-perpendicular to alpha = 11 T-parallel to O) ions as suggested in Gomberoff & Valdivia and Gomberoff et al., using two approaches. First, we use quasilinear kinetic theory to study the energy transfer between waves and particles, with the subsequent acceleration and heating of ions. Second, 1.5 D (one spatial dimension and three dimensions in velocity space) hybrid numerical simulations are performed to investigate the fully nonlinear evolution of this wave-particle interaction. Numerical results of both approaches show that the temperatures of all species evolve anisotropically, consistent with the time-dependent wave-spectrum energy. In a cascade effect, we observe the emergence of modes at frequencies higher than those initially considered, peaking at values close to the resonance frequencies of O+6 ions (omega similar to Omega(cO)) and He+2 ions (omega similar to Omega(c alpha)), being the peak due to O+6 ions about three times bigger than the peak associated with He+2 ions. Both the heating of the plasma and the energy cascade were more efficient in the nonlinear analysis than in the quasilinear one. These results suggest that this energy cascade mechanism may participate in the acceleration and heating of the solar wind plasma close to the Sun during fast streams associated with coronal holes. C1 [Moya, P. S.; Vinas, A. F.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Moya, P. S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Navarro, R.; Munoz, V.; Valdivia, J. A.] Univ Chile, Fac Ciencias, Dept Fis, Santiago 3425, Chile. RP Moya, PS (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Geospace Phys Lab, Mail Code 673, Greenbelt, MD 20771 USA. EM pablo.s.moyafuentes@nasa.gov RI Moya, Pablo/C-3163-2011; Valdivia, Juan/A-3631-2008; Navarro, Roberto/F-7045-2014; Munoz, Victor/A-2255-2008 OI Moya, Pablo/0000-0002-9161-0888; Valdivia, Juan/0000-0003-3381-9904; Navarro, Roberto/0000-0003-0782-1904; FU Comision Nacional de Ciencia y Tecnologia (CONICyT, Chile) [21100691]; FONDECyT [1080658, 1110135, 1110729, 1121144] FX We give thanks to Comision Nacional de Ciencia y Tecnologia (CONICyT, Chile) for a Becas-Chile Postdoctoral Fellowship (PSM) and Doctoral Fellowship No. 21100691 (R.N.). We also acknowledge support from FONDECyT grants Nos. 1080658, 1110135, and 1110729 (J.A.V.) and No. 1121144 (V.M.). We also thank Cedenna for support. NR 72 TC 8 Z9 8 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2014 VL 781 IS 2 AR 76 DI 10.1088/0004-637X/781/2/76 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5WV UT WOS:000331171200020 ER PT J AU Patsourakos, S Klimchuk, JA Young, PR AF Patsourakos, S. Klimchuk, J. A. Young, P. R. TI CORE AND WING DENSITIES OF ASYMMETRIC CORONAL SPECTRAL PROFILES: IMPLICATIONS FOR THE MASS SUPPLY OF THE SOLAR CORONA SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona ID ACTIVE-REGION LOOPS; ULTRAVIOLET EMISSION-LINES; EUV IMAGING SPECTROMETER; AN ATOMIC DATABASE; HINODE-EIS; SPECTROSCOPIC OBSERVATIONS; SPICULES; CHIANTI; PLASMA; CHROMOSPHERE AB Recent solar spectroscopic observations have shown that coronal spectral lines can exhibit asymmetric profiles, with enhanced emissions at their blue wings. These asymmetries correspond to rapidly upflowing plasmas at speeds exceeding 50 km s(-1). Here, we perform a study of the density of the rapidly upflowing material and compare it with that of the line core that corresponds to the bulk of the plasma. For this task, we use spectroscopic observations of several active regions taken by the Extreme Ultraviolet Imaging Spectrometer of the Hinode mission. The density sensitive ratio of the Fe xiv lines at 264.78 and 274.20 A is used to determine wing and core densities. We compute the ratio of the blue wing density to the core density and find that most values are of order unity. This is consistent with the predictions for coronal nanoflares if most of the observed coronal mass is supplied by chromospheric evaporation driven by the nanoflares. However, much larger blue wing-to-core density ratios are predicted if most of the coronal mass is supplied by heated material ejected with type II spicules. Our measurements do not rule out a spicule origin for the blue wing emission, but they argue against spicules being a primary source of the hot plasma in the corona. We note that only about 40% of the pixels where line blends could be safely ignored have blue wing asymmetries in both Fe xiv lines. Anticipated sub-arcsecond spatial resolution spectroscopic observations in future missions could shed more light on the origin of blue, red, and mixed asymmetries. C1 [Patsourakos, S.] Univ Ioannina, Dept Phys, Sect Astrogeophys, GR-45110 Ioannina, Greece. [Klimchuk, J. A.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Young, P. R.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. RP Patsourakos, S (reprint author), Univ Ioannina, Dept Phys, Sect Astrogeophys, POB 1186, GR-45110 Ioannina, Greece. EM spatsour@cc.uoi.gr; james.a.klimchuk@nasa.gov RI Klimchuk, James/D-1041-2012; OI Klimchuk, James/0000-0003-2255-0305; Young, Peter/0000-0001-9034-2925 FU FP7 Marie Curie Re-integration grant [FP7-PEOPLE-2010-RG/268288]; European Union (European Social Fund ESF); Greek national funds through the Operational Program "Education and Lifelong Learning" of the National Strategic Reference Framework (NSRF)-Thales; European Social Fund; NASA; Naval Research Laboratory FX The authors thank the referee for useful and constructive comments and suggestions that led to a significant improvement of the manuscript. S.P. acknowledges support from FP7 Marie Curie Re-integration grant FP7-PEOPLE-2010-RG/268288 and from the European Union (European Social Fund ESF) and Greek national funds through the Operational Program "Education and Lifelong Learning" of the National Strategic Reference Framework (NSRF)-Research Funding Program: Thales. Investing in knowledge society through the European Social Fund. The work of J.A.K. was supported by the NASA Supporting Research and Technology Program. The work of P.R.Y. was performed under contract with the Naval Research Laboratory and was funded by NASA. NR 56 TC 10 Z9 10 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 FEB 1 PY 2014 VL 781 IS 2 AR 58 DI 10.1088/0004-637X/781/2/58 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5WV UT WOS:000331171200002 ER PT J AU Schmieder, B Kucera, TA Knizhnik, K Luna, M Lopez-Ariste, A Toot, D AF Schmieder, B. Kucera, T. A. Knizhnik, K. Luna, M. Lopez-Ariste, A. Toot, D. TI PROPAGATING WAVES TRANSVERSE TO THE MAGNETIC FIELD IN A SOLAR PROMINENCE (vol 777, pg 108, 2013) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Schmieder, B.] Observ Paris, CNRS, LESIA, UMR 8109, F-92195 Meudon, France. [Kucera, T. A.; Knizhnik, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Knizhnik, K.] Johns Hopkins Univ, Baltimore, MD USA. [Luna, M.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Luna, M.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Lopez-Ariste, A.] CNRS UPS853, THEMIS, E-38205 Lalaguna, Spain. [Toot, D.] Alfred Univ, Alfred, NY 14802 USA. RP Schmieder, B (reprint author), Observ Paris, CNRS, LESIA, UMR 8109, F-92195 Meudon, France. NR 1 TC 0 Z9 0 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 FEB 1 PY 2014 VL 781 IS 2 AR 129 DI 10.1088/0004-637X/781/2/129 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5WV UT WOS:000331171200073 ER PT J AU Winkler, PF Williams, BJ Reynolds, SP Petre, R Long, KS Katsuda, S Hwang, U AF Winkler, P. Frank Williams, Brian J. Reynolds, Stephen P. Petre, Robert Long, Knox S. Katsuda, Satoru Hwang, Una TI A HIGH-RESOLUTION X-RAY AND OPTICAL STUDY OF SN 1006: ASYMMETRIC EXPANSION AND SMALL-SCALE STRUCTURE IN A TYPE IA SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (SN 1006); ISM: kinematics and dynamics; ISM: supernova remnants; supernovae: individual (SN 1006); X-rays: individual (SN1006); X-rays: ISM ID DELAYED-DETONATION MODELS; BALMER-DOMINATED SHOCKS; NOVA AD 1006; MAGNETIC-FIELD; PARTICLE-ACCELERATION; SYNCHROTRON EMISSION; NORTHEASTERN LIMB; SPATIAL STRUCTURE; SN-1006 REMNANT; PROPER MOTIONS AB We introduce a deep (670 ks) X-ray survey of the entire SN 1006 remnant from the Chandra X-Ray Observatory, together with a deep Ha image of SN 1006 from the 4 m Blanco telescope at CTIO. Comparison with Chandra images from 2003 gives the first measurement of the X-ray proper motions around the entire periphery, carried out over a 9 yr baseline. We find that the expansion velocity varies significantly with azimuth. The highest velocity of similar to 7400 km s(-1) (almost 2.5 times that in the northwest (NW)) is found along the southeast (SE) periphery, where both the kinematics and the spectra indicate that most of the X-ray emission stems from ejecta that have been decelerated little, if at all. Asymmetries in the distribution of ejecta are seen on a variety of spatial scales. Si-rich ejecta are especially prominent in the SE quadrant, while O and Mg are more uniformly distributed, indicating large-scale asymmetries arising from the explosion itself. Neon emission is strongest in a sharp filament just behind the primary shock along the NW rim, where the pre-shock density is highest. Here the Ne is likely interstellar, while Ne within the shell may include a contribution from ejecta. Within the interior of the projected shell we find a few isolated "bullets" of what appear to be supernova ejecta that are immediately preceded by bowshocks seen in Ha, features that we interpret as ejecta knots that have reached relatively dense regions of the surrounding interstellar medium, but that appear in the interior in projection. Recent three-dimensional hydrodynamic models for Type Ia supernovae display small-scale features that strongly resemble the ones seen in X-rays in SN 1006; an origin in the explosion itself or from subsequent hydrodynamic instabilities both remain viable options. We have expanded the search for precursor X-ray emission ahead of a synchrotron-dominated shock front, as expected from diffusive shock acceleration theory, to numerous regions along both the northeast and southwest rims of the shell. Our data require that a precursor be thinner than about 3", and fainter than about 5% of the post-shock peak. These limits suggest that the magnetic field is amplified by a factor of seven or more in a narrow precursor region, promoting diffusive particle acceleration. C1 [Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. [Williams, Brian J.; Petre, Robert; Hwang, Una] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reynolds, Stephen P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. [Long, Knox S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Katsuda, Satoru] RIKEN, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan. RP Winkler, PF (reprint author), Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. EM winkler@middlebury.edu; brian.j.williams@nasa.gov; reynolds@ncsu.edu; robert.petre-1@nasa.gov; long@stsci.edu FU National Aeronautics and Space Administration through Chandra [GO2-13066]; Chandra X-ray Observatory Center; NASA [NAS8-03060]; National Science Foundation [AST-0908566] FX We acknowledge several suggestions from the anonymous referee that have led to greater clarity in this paper. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Grant Number GO2-13066, issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. P. F. W. also acknowledges financial support from the National Science Foundation through grant AST-0908566. NR 65 TC 16 Z9 16 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 FEB 1 PY 2014 VL 781 IS 2 AR 65 DI 10.1088/0004-637X/781/2/65 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5WV UT WOS:000331171200009 ER PT J AU Wuyts, E Rigby, JR Gladders, MD Sharon, K AF Wuyts, Eva Rigby, Jane R. Gladders, Michael D. Sharon, Keren TI A MAGNIFIED VIEW OF THE KINEMATICS AND MORPHOLOGY OF RCSGA 032727-132609: ZOOMING IN ON A MERGER AT z=1.7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; galaxies: kinematics and dynamics; galaxies: structure; gravitational lensing: strong ID STAR-FORMING GALAXIES; SIMILAR-TO 2; H-II REGIONS; ULTRALUMINOUS INFRARED GALAXIES; MASS-METALLICITY RELATION; INTEGRAL FIELD SPECTROSCOPY; KILOPARSEC-SCALE CLUMPS; ADAPTIVE OPTICS SYSTEM; ULTRA DEEP FIELD; HIGH-REDSHIFT AB We present a detailed analysis of multi-wavelength Hubble Space Telescope/Wide Field Camera 3 (WFC3) imaging and Keck/OSIRIS near-infrared adaptive optics-assisted integral field spectroscopy for a highly magnified lensed galaxy at z = 1.70. This young starburst is representative of ultraviolet-selected star-forming galaxies (SFGs) at z similar to 2 and contains multiple individual star-forming regions. Due to the lensing magnification, we can resolve spatial scales down to 100 pc in the source plane of the galaxy. The velocity field shows disturbed kinematics suggestive of an ongoing interaction and there is a clear signature of a tidal tail. We constrain the age, reddening, star formation rate, and stellar mass of the star-forming clumps from spectral energy distribution ( SED) modeling of the WFC3 photometry and measure their H alpha luminosity, metallicity, and outflow properties from the OSIRIS data. With strong star-formation-driven outflows in four clumps, RCSGA0327 is the first high-redshift SFG at stellar mass <10(10) M-O with spatially resolved stellar winds. We compare the H alpha luminosities, sizes, and dispersions of the star-forming regions with other high-z clumps as well as local giant H II regions and find no evidence for increased clump star formation surface densities in interacting systems, unlike in the local universe. Spatially resolved SED modeling unveils an established stellar population at the location of the largest clump and a second mass concentration near the edge of the system that is not detected in H alpha emission. This suggests a picture of an equal-mass mixed major merger, which has not triggered a new burst of star formation or caused a tidal tail in the gas-poor component. C1 [Wuyts, Eva] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Gladders, Michael D.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Gladders, Michael D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Sharon, Keren] Univ Michigan, Dept Astron & Astrophys, Ann Arbor, MI 48109 USA. RP Wuyts, E (reprint author), Max Planck Inst Extraterr Phys, Postfach 1312,Giessenbachstr, D-85741 Garching, Germany. RI Rigby, Jane/D-4588-2012 OI Rigby, Jane/0000-0002-7627-6551 FU NASA through a grant from the Space Telescope Science Institute [12267]; NASA [NAS 5-26555]; Sigma Xi Scientific Research Society; NASA Keck PI Data Award; University of Michigan's Presidential Fellowship; W. M. Keck Foundation FX We thank our anonymous referee for a thorough reading of the paper and insightful comments. E. W. thanks John Hibbard, Tucker Jones, Rachael Livermore, Chris Mihos, Thorsten Naab, Sarah Newman, Emily Wisnioski, and Tian-Tian Yuan for sharing data and/or stimulating discussions. Support for HST program 12267 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Travel support for the Keck observations was provided by the Grants-in-Aid of Research Program of the Sigma Xi Scientific Research Society and the NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. K. S. acknowledges support from the University of Michigan's Presidential Fellowship.; Data presented in this paper were partly obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 118 TC 15 Z9 15 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 FEB 1 PY 2014 VL 781 IS 2 AR 61 DI 10.1088/0004-637X/781/2/61 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5WV UT WOS:000331171200005 ER PT J AU Jung, JH Pasolli, E Prasad, S Tilton, JC Crawford, MM AF Jung, Jinha Pasolli, Edoardo Prasad, Saurabh Tilton, James C. Crawford, Melba M. TI A Framework for Land Cover Classification Using Discrete Return LiDAR Data: Adopting Pseudo-Waveform and Hierarchical Segmentation SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE Classification; hierarchical segmentation (HSeg); light detection and ranging (LiDAR); pseudo-waveform; support vector machine (SVM) ID REMOTE-SENSING IMAGES; SPECTRAL-SPATIAL CLASSIFICATION; RESOLUTION MULTISPECTRAL DATA; BINARY PARTITION TREE; URBAN AREAS; HYPERSPECTRAL IMAGES; RAIN-FOREST; EXTRACTION; REPRESENTATION; INFORMATION AB Acquiring current, accurate land-use information is critical for monitoring and understanding the impact of anthropogenic activities on natural environments. Remote sensing technologies are of increasing importance because of their capability to acquire information for large areas in a timely manner, enabling decision makers to be more effective in complex environments. Although optical imagery has demonstrated to be successful for land cover classification, active sensors, such as light detection and ranging (LiDAR), have distinct capabilities that can be exploited to improve classification results. However, utilization of LiDAR data for land cover classification has not been fully exploited. Moreover, spatial-spectral classification has recently gained significant attention since classification accuracy can be improved by extracting additional information from the neighboring pixels. Although spatial information has been widely used for spectral data, less attention has been given to LiDAR data. In this work, a new framework for land cover classification using discrete return LiDAR data is proposed. Pseudo-waveforms are generated from the LiDAR data and processed by hierarchical segmentation. Spatial features are extracted in a region-based way using a new unsupervised strategy for multiple pruning of the segmentation hierarchy. The proposed framework is validated experimentally on a real dataset acquired in an urban area. Better classification results are exhibited by the proposed framework compared to the cases in which basic LiDAR products such as digital surface model and intensity image are used. Moreover, the proposed region-based feature extraction strategy results in improved classification accuracies in comparison with a more traditional window-based approach. C1 [Jung, Jinha; Crawford, Melba M.] Purdue Univ, Sch Civil Engn, W Lafayette, IN 47907 USA. [Pasolli, Edoardo; Tilton, James C.] NASA, Goddard Space Flight Ctr, Computat & Informat Sci & Technol Off, Greenbelt, MD 20771 USA. [Prasad, Saurabh] Univ Houston, Dept Elect & Comp Engn, Houston, TX 77004 USA. RP Jung, JH (reprint author), Purdue Univ, Sch Civil Engn, W Lafayette, IN 47907 USA. EM jinha@purdue.edu; epasolli@purdue.edu; sprasad2@uh.edu; james.c.tilton@nasa.gov; mcrawford@purdue.edu OI Pasolli, Edoardo/0000-0003-0799-3490 FU NSF FX The authors would like to thank the Hyperspectral Image Analysis group and the NSF Funded Center for Airborne Laser Mapping (NCALM) at the University of Houston for providing the datasets used in this study, and the IEEE GRSS Data Fusion Technical Committee for organizing the 2013 Data Fusion Contest. NR 48 TC 10 Z9 10 U1 2 U2 23 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD FEB PY 2014 VL 7 IS 2 BP 491 EP 502 DI 10.1109/JSTARS.2013.2292032 PG 12 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA AB0BS UT WOS:000331457400011 ER PT J AU Yeo, IY Lang, M Vermote, E AF Yeo, In-Young Lang, Megan Vermote, Eric TI Improved Understanding of Suspended Sediment Transport Process Using Multi-Temporal Landsat Data: A Case Study From the Old Woman Creek Estuary (Ohio) SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE Landsat time-series images; remote sensing; suspended sediment; turbidity; wetland ID WATER-QUALITY; CHESAPEAKE BAY; RIVER ESTUARY; IN-SITU; REFLECTANCE; ALGORITHM; QUANTIFICATION; SPECTRUM; IMAGERY; MODELS AB We used historical water quality data, continuous in situ water quality monitoring data, and multi-temporal Landsat-7 ETM+ imagery for the period of September 1999-April 2003 to study the distribution of total suspended sediments (TSS) in Old Woman Creek (OWC), a freshwater coastal wetland adjacent to Lake Erie. A multiple linear regression model was developed to describe the relationship between turbidity and atmospherically corrected reflectance from Landsat-7 ETM+ bands 2 and 4 (R-2 = 0.65). Turbidity was then converted to total suspended sediments (TSS), based on in situ historical data. Mapped spatial patterns of TSS provided useful information on key physical drivers affecting the transport process of suspended sediment. This study demonstrates the potential and limitations of using medium-spatial scale multispectral data, such as Landsat, to understand important factors that control suspended sediment transport processes within an estuary. C1 [Yeo, In-Young] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Lang, Megan] US Forest Serv, USDA, No Res Stn, Beltsville, MD 20705 USA. [Vermote, Eric] NASA, Goddard Space Flight Ctr, Terr Informat Syst Lab, Greenbelt, MD 20771 USA. RP Yeo, IY (reprint author), Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. FU NASA Land Cover Land Use Change Program [NNX12AG21G] FX This work was supported by NASA Land Cover Land Use Change Program (contract no. NNX12AG21G). NR 50 TC 3 Z9 3 U1 3 U2 25 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD FEB PY 2014 VL 7 IS 2 BP 636 EP 647 DI 10.1109/JSTARS.2013.2265191 PG 12 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA AB0BS UT WOS:000331457400022 ER PT J AU Montoya, J Rathinam, S Wood, Z AF Montoya, Justin Rathinam, Sivakumar Wood, Zachary TI Multiobjective Departure Runway Scheduling Using Dynamic Programming SO IEEE TRANSACTIONS ON INTELLIGENT TRANSPORTATION SYSTEMS LA English DT Article DE Aircraft scheduling; multiple objective dynamic programming; Pareto-optimality; runway scheduling ID PARETO-OPTIMAL SOLUTIONS; ALGORITHM; OPTIMALITY; PRINCIPLE; AIRCRAFT AB At busy airports, air traffic controllers seek to find schedules for aircraft at the runway that aim to minimize delays of the aircraft while maximizing runway throughput. In reality, finding optimal schedules by a human controller is hard to accomplish since the number of feasible schedules available for the scheduling problem is quite large. In this paper, we pose this problem as a multiobjective optimization problem, with respect to total aircraft delay and runway throughput. Using principles of multiobjective dynamic programming, we develop an algorithm to find a set of Pareto-optimal solutions that completely specify the nondominated frontier. In addition to finding these solutions, this paper provides a proof of the algorithm's correctness and gives an analysis of its performance against a baseline algorithm using the operational data for a model of the Dallas/Fort Worth International Airport. C1 [Montoya, Justin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rathinam, Sivakumar] Texas A&M Univ, Dept Mech Engn, College Stn, TX 77843 USA. [Wood, Zachary] PayPal Inc, San Jose, CA 95131 USA. RP Montoya, J (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM justin.v.montoya@nasa.gov; srathinam@gmail.com; z.wood23@gmail.com NR 57 TC 2 Z9 3 U1 1 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1524-9050 EI 1558-0016 J9 IEEE T INTELL TRANSP JI IEEE Trans. Intell. Transp. Syst. PD FEB PY 2014 VL 15 IS 1 BP 399 EP 413 DI 10.1109/TITS.2013.2283256 PG 15 WC Engineering, Civil; Engineering, Electrical & Electronic; Transportation Science & Technology SC Engineering; Transportation GA AA7QP UT WOS:000331292300036 ER PT J AU Aher, GR Pawar, GV Gupta, P Devara, PCS AF Aher, G. R. Pawar, G. V. Gupta, Pawan Devara, P. C. S. TI Effect of major dust storm on optical, physical, and radiative properties of aerosols over coastal and urban environments in Western India SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID WAVELENGTH DEPENDENCE; ANGSTROM EXPONENT; MINERAL DUST; BLACK CARBON; MODIS; ASIA; INSTRUMENT; ALGORITHM; AERONET; SYSTEM C1 [Aher, G. R.; Pawar, G. V.] Nowrosjee Wadia Coll, Dept Phys, Atmospher Phys Res Lab, Pune 411001, Maharashtra, India. [Gupta, Pawan] Univ Space Res Assoc, Greenbelt, MD USA. [Gupta, Pawan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Devara, P. C. S.] Indian Inst Trop Meteorol, Pune 411008, Maharashtra, India. RP Aher, GR (reprint author), Nowrosjee Wadia Coll, Dept Phys, Atmospher Phys Res Lab, Pune 411001, Maharashtra, India. EM aher.g.r@gmail.com FU ISRO-UoP Space Science Technology Cell, Pune University Campus FX The authors thank the Director, ISRO-UoP Space Science Technology Cell, Pune University Campus, for providing funding support for the research carried out under this project. NR 101 TC 8 Z9 9 U1 1 U2 10 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0143-1161 EI 1366-5901 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PD FEB 1 PY 2014 VL 35 IS 3 BP 871 EP 903 DI 10.1080/01431161.2013.873153 PG 33 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA AA8GJ UT WOS:000331333300005 ER PT J AU Lee, H Park, I Konishi, C Mudawar, I May, RI Juergens, JR Wagner, JD Hall, NR Nahra, HK Hasan, MM Mackey, JR AF Lee, Hyoungsoon Park, Ilchung Konishi, Christopher Mudawar, Issam May, Rochelle I. Juergens, Jeffrey R. Wagner, James D. Hall, Nancy R. Nahra, Henry K. Hasan, Mohammad M. Mackey, Jeffrey R. TI Experimental Investigation of Flow Condensation in Microgravity SO JOURNAL OF HEAT TRANSFER-TRANSACTIONS OF THE ASME LA English DT Article DE microgravity; condensation; annular flow ID HEAT-TRANSFER COEFFICIENT; FALLING LIQUID-FILMS; PARALLEL MICRO-CHANNELS; PRESSURE-DROP; MOMENTUM TRANSPORT; UNIVERSAL APPROACH; TUBE; MASS AB Future manned space missions are expected to greatly increase the space vehicle's size, weight, and heat dissipation requirements. An effective means to reducing both size and weight is to replace single-phase thermal management systems with two-phase counterparts that capitalize upon both latent and sensible heat of the coolant rather than sensible heat alone. This shift is expected to yield orders of magnitude enhancements in flow boiling and condensation heat transfer coefficients. A major challenge to this shift is a lack of reliable tools for accurate prediction of two-phase pressure drop and heat transfer coefficient in reduced gravity. Developing such tools will require a sophisticated experimental facility to enable investigators to perform both flow boiling and condensation experiments in microgravity in pursuit of reliable databases. This study will discuss the development of the Flow Boiling and Condensation Experiment (FBCE) for the International Space Station (ISS), which was initiated in 2012 in collaboration between Purdue University and NASA Glenn Research Center. This facility was recently tested in parabolic flight to acquire condensation data for FC-72 in microgravity, aided by high-speed video analysis of interfacial structure of the condensation film. The condensation is achieved by rejecting heat to a counter flow of water, and experiments were performed at different mass velocities of FC-72 and water and different FC-72 inlet qualities. It is shown that the film flow varies from smooth-laminar to wavy-laminar and ultimately turbulent with increasing FC-72 mass velocity. The heat transfer coefficient is highest near the inlet of the condensation tube, where the film is thinnest, and decreases monotonically along the tube, except for high FC-72 mass velocities, where the heat transfer coefficient is enhanced downstream. This enhancement is attributed to both turbulence and increased interfacial waviness. One-g(e) correlations are shown to predict the average condensation heat transfer coefficient with varying degrees of success, and a recent correlation is identified for its superior predictive capability, evidenced by a mean absolute error of 21.7%. C1 [Lee, Hyoungsoon; Park, Ilchung; Konishi, Christopher; Mudawar, Issam] BTPFL, W Lafayette, IN 47907 USA. [May, Rochelle I.; Juergens, Jeffrey R.; Wagner, James D.; Hall, Nancy R.; Nahra, Henry K.; Hasan, Mohammad M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Mackey, Jeffrey R.] Vantage Partners LLC, Brookpark, OH 44142 USA. RP Mudawar, I (reprint author), BTPFL, Mech Engn Bldg,585 Purdue Mall, W Lafayette, IN 47907 USA. EM mudawar@ecn.purdue.edu FU National Aeronautics and Space Administration (NASA) [NNX13AB01G] FX The authors are grateful for the support of the National Aeronautics and Space Administration (NASA) under Grant No. NNX13AB01G. The authors also thank George Saad, David F. Chao, Robert L. Butcher, Alban D. Seigneur, Bruce J. Franken-field, Paul A. Trimarchi, Richard A. Kelsch, Daniel J. Gotti, Chip Redding, and Frank L. Kmiecik of the NASA Glenn Research Center for their technical assistance. NR 36 TC 1 Z9 1 U1 6 U2 35 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 0022-1481 EI 1528-8943 J9 J HEAT TRANS-T ASME JI J. Heat Transf.-Trans. ASME PD FEB PY 2014 VL 136 IS 2 AR 021502 DI 10.1115/1.4025683 PG 11 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA AB0IH UT WOS:000331474700003 ER PT J AU Brooke, JSA Ram, RS Western, CM Li, G Schwenke, DW Bernath, PF AF Brooke, James S. A. Ram, Ram S. Western, Colin M. Li, Gang Schwenke, David W. Bernath, Peter F. TI EINSTEIN A COEFFICIENTS AND OSCILLATOR STRENGTHS FOR THE A(2)Pi-X-2 Sigma(+) (RED) AND B-2 Sigma(+)-X-2 Sigma(+) (VIOLET) SYSTEMS AND ROVIBRATIONAL TRANSITIONS IN THE X-2 Sigma(+) STATE OF CN SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE astronomical databases: miscellaneous; methods: laboratory: molecular; molecular data; opacity stars: abundances; techniques: spectroscopic ID TRANSFORM EMISSION-SPECTROSCOPY; TAIL BAND SYSTEM; CONFIGURATION-INTERACTION CALCULATIONS; DIPOLE-MOMENT FUNCTION; RADIATIVE LIFETIMES; INTERSTELLAR CN; ROTATIONAL PERTURBATIONS; PROJECTION OPERATORS; MOLECULAR-PROPERTIES; INFRARED-SPECTRUM AB Line strengths have been calculated in the form of Einstein A coefficients and f-values for a large number of bands of the A(2)Pi-X-2 Sigma(+) and B-2 Sigma(+)-X-2 Sigma(+) systems and rovibrational transitions within the X-2 Sigma(+) state of CN using Western's pgopher program. The J dependence of the transition dipole moment matrix elements (the Herman-Wallis effect) has been taken into account. Rydberg-Klein-Rees potential energy functions for the A(2)Pi, B-2 Sigma(+), and X-2 Sigma(+) states were computed using spectroscopic constants from the A(2)Pi-X-2 Sigma(+) and B-2 Sigma(+)-X-2 Sigma(+) transitions. New electronic transition dipole moment functions for these systems and a dipole moment function for the X-2 Sigma(+) state were generated from high level ab initio calculations and have been used in Le Roy's level program to produce transition dipole moment matrix elements (including their J dependence) for a large number of vibrational bands. The program pgopher was used to calculate Einstein A coefficients, and a line list was generated containing the observed and calculated wavenumbers, Einstein A coefficients and f-values for 290 bands of the A(2)Pi-X-2 Sigma(+) transition with v' = 0-22, v '' = 0-15, 250 bands of the B-2 Sigma(+)-X-2 Sigma(+) transition with v' = 0-15, v '' = 0-15 and 120 bands of the rovibrational transitions within the X-2 Sigma(+) state with v = 0-15. The Einstein A coefficients have been used to compute radiative lifetimes of several vibrational levels of the A(2)Pi and B-2 Sigma(+) states and the values compared with those available from previous experimental and theoretical studies. C1 [Brooke, James S. A.; Ram, Ram S.; Bernath, Peter F.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. [Western, Colin M.] Univ Bristol, Sch Chem, Bristol BS8 1TS, Avon, England. [Li, Gang] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schwenke, David W.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Bernath, Peter F.] Old Dominion Univ, Dept Chem & Biochem, Norfolk, VA 23529 USA. RP Brooke, JSA (reprint author), Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. EM jsabrooke@gmail.com RI Bernath, Peter/B-6567-2012; schwenke, david/I-3564-2013; Li, Gang/P-2272-2015 OI Bernath, Peter/0000-0002-1255-396X; Li, Gang/0000-0002-5605-7896 FU Leverhulme Trust of UK; NASA laboratory astrophysics program FX The research described here was supported by funding from the Leverhulme Trust of UK and the NASA laboratory astrophysics program. The spectra used in this work were recorded at the National Solar Observatory at Kitt Peak, USA. NR 90 TC 25 Z9 25 U1 3 U2 25 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD FEB PY 2014 VL 210 IS 2 AR 23 DI 10.1088/0067-0049/210/2/23 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA6WN UT WOS:000331239000009 ER PT J AU Burke, CJ Bryson, ST Mullally, F Rowe, JF Christiansen, JL Thompson, SE Coughlin, JL Haas, MR Batalha, NM Caldwell, DA Jenkins, JM Still, M Barclay, T Borucki, WJ Chaplin, WJ Ciardi, DR Clarke, BD Cochran, WD Demory, BO Esquerdo, GA Gautier, TN Gilliland, RL Girouard, FR Havel, M Henze, CE Howell, SB Huber, D Latham, DW Li, J Morehead, RC Morton, TD Pepper, J Quintana, E Ragozzine, D Seader, SE Shah, Y Shporer, A Tenenbaum, P Twicken, JD Wolfgang, A AF Burke, Christopher J. Bryson, Stephen T. Mullally, F. Rowe, Jason F. Christiansen, Jessie L. Thompson, Susan E. Coughlin, Jeffrey L. Haas, Michael R. Batalha, Natalie M. Caldwell, Douglas A. Jenkins, Jon M. Still, Martin Barclay, Thomas Borucki, William J. Chaplin, William J. Ciardi, David R. Clarke, Bruce D. Cochran, William D. Demory, Brice-Olivier Esquerdo, Gilbert A. Gautier, Thomas N., III Gilliland, Ronald L. Girouard, Forrest R. Havel, Mathieu Henze, Christopher E. Howell, Steve B. Huber, Daniel Latham, David W. Li, Jie Morehead, Robert C. Morton, Timothy D. Pepper, Joshua Quintana, Elisa Ragozzine, Darin Seader, Shawn E. Shah, Yash Shporer, Avi Tenenbaum, Peter Twicken, Joseph D. Wolfgang, Angie TI PLANETARY CANDIDATES OBSERVED BY KEPLER IV: PLANET SAMPLE FROM Q1-Q8 (22 MONTHS) SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; eclipses; planetary systems; space vehicles ID TRANSIT TIMING OBSERVATIONS; SUN-LIKE STAR; 1ST 4 MONTHS; HABITABLE ZONE; LIGHT CURVES; ECLIPSING BINARIES; ERROR-CORRECTION; FALSE POSITIVES; BLEND SCENARIOS; MULTIPLE SYSTEM AB We provide updates to the Kepler planet candidate sample based upon nearly two years of high-precision photometry (i.e., Q1-Q8). From an initial list of nearly 13,400 threshold crossing events, 480 new host stars are identified from their flux time series as consistent with hosting transiting planets. Potential transit signals are subjected to further analysis using the pixel-level data, which allows background eclipsing binaries to be identified through small image position shifts during transit. We also re-evaluate Kepler Objects of Interest (KOIs) 1-1609, which were identified early in the mission, using substantially more data to test for background false positives and to find additional multiple systems. Combining the new and previous KOI samples, we provide updated parameters for 2738 Kepler planet candidates distributed across 2017 host stars. From the combined Kepler planet candidates, 472 are new from the Q1-Q8 data examined in this study. The new Kepler planet candidates represent similar to 40% of the sample with R-P similar to 1R(circle plus) and represent similar to 40% of the low equilibrium temperature (T-eq < 300 K) sample. We review the known biases in the current sample of Kepler planet candidates relevant to evaluating planet population statistics with the current Kepler planet candidate sample. C1 [Burke, Christopher J.; Mullally, F.; Rowe, Jason F.; Thompson, Susan E.; Coughlin, Jeffrey L.; Caldwell, Douglas A.; Jenkins, Jon M.; Li, Jie; Quintana, Elisa; Seader, Shawn E.; Tenenbaum, Peter; Twicken, Joseph D.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Bryson, Stephen T.; Haas, Michael R.; Batalha, Natalie M.; Borucki, William J.; Havel, Mathieu; Henze, Christopher E.; Howell, Steve B.; Huber, Daniel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Christiansen, Jessie L.; Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Still, Martin; Barclay, Thomas] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Chaplin, William J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Chaplin, William J.] Aarhus Univ, SAC, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Clarke, Bruce D.; Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cochran, William D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Demory, Brice-Olivier] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Esquerdo, Gilbert A.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Girouard, Forrest R.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. [Morehead, Robert C.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Morton, Timothy D.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Pepper, Joshua] Lehigh Univ, Dept Phys, Bethlehem, PA 18015 USA. [Pepper, Joshua] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Ragozzine, Darin] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Shah, Yash] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Shporer, Avi] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Wolfgang, Angie] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Burke, CJ (reprint author), NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. EM christopher.j.burke@nasa.gov RI Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Ciardi, David/0000-0002-5741-3047; Demory, Brice-Olivier/0000-0002-9355-5165; Pepper, Joshua/0000-0002-3827-8417 FU NASA Postdoctoral Program at Ames Research Center FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. M.H. and D.H. are supported by an appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 70 TC 124 Z9 124 U1 2 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD FEB PY 2014 VL 210 IS 2 AR 19 DI 10.1088/0067-0049/210/2/19 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA6WN UT WOS:000331239000005 ER PT J AU Cook, AM Mattioda, AL Quinn, RC Ricco, AJ Ehrenfreund, P Bramall, NE Minelli, G Quigley, E Walker, R Walker, R AF Cook, Amanda M. Mattioda, Andrew L. Quinn, Richard C. Ricco, Antonio J. Ehrenfreund, Pascale Bramall, Nathan E. Minelli, Giovanni Quigley, Emmett Walker, Ryan Walker, Robert TI SEVO ON THE GROUND: DESIGN OF A LABORATORY SOLAR SIMULATION IN SUPPORT OF THE O/OREOS MISSION SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE astrochemistry; instrumentation: miscellaneous; Sun: UV radiation; techniques: spectroscopic ID ICE ANALOGS; EARTH-ORBIT; WATER ICE; SPACE; PHOTOLYSIS; EVOLUTION AB This technical note describes a novel solar simulation experiment designed to mimic the solar radiation experienced by the Organism/Organics Exposure to Orbital Stresses (O/OREOS) nanosatellite in low-Earth orbit. Thin films of organic compounds within hermetically sealed sample cells (identical to the films and cells of the spaceflight mission) were exposed to simulated AM0 solar radiation in the laboratory for a total of 6 months, and monitored for spectral changes at two-week intervals. The laboratory experiment accurately simulated ultraviolet and visible solar irradiance to within 2% from 200-1000 nm and the Ly alpha (121.6 nm) emission line radiation to within 8%. Design and calibration parameters for the experiment are discussed in detail for this ground-based laboratory irradiation experiment, which was built as a complement to, and as scientific validation of, the O/OREOS SEVO experiment in space. C1 [Cook, Amanda M.; Mattioda, Andrew L.; Ricco, Antonio J.; Minelli, Giovanni; Quigley, Emmett; Walker, Ryan; Walker, Robert] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. [Quinn, Richard C.] SETI Inst, Mountain View, CA 94043 USA. [Ehrenfreund, Pascale] George Washington Univ, Inst Space Policy, Washington, DC 20052 USA. [Bramall, Nathan E.] Los Gatos Res, Mountain View, CA 94041 USA. RP Cook, AM (reprint author), NASA, Ames Res Ctr, Mountain View, CA 94035 USA. EM andrew.1.mattioda@nasa.gov OI Ricco, Antonio/0000-0002-2355-4984 FU NASA [09-EXOB09-1030] FX The authors thank the NASA Astrobiology Small Payloads program for support and Greg Defouw for assisting with the initial design/engineering of the exposure cells. The authors also thank the NASA Astrobiology Institute, the NASA Postdoctoral Program administered by Oak Ridge Associated Universities through a contract with NASA, and the NASA Exobiology Program for additional support (proposal number 09-EXOB09-1030). NR 27 TC 5 Z9 5 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD FEB PY 2014 VL 210 IS 2 AR 15 DI 10.1088/0067-0049/210/2/15 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA6WN UT WOS:000331239000001 ER PT J AU Cuzzi, JN Estrada, PR Davis, SS AF Cuzzi, Jeffrey N. Estrada, Paul R. Davis, Sanford S. TI UTILITARIAN OPACITY MODEL FOR AGGREGATE PARTICLES IN PROTOPLANETARY NEBULAE AND EXOPLANET ATMOSPHERES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE opacity; planets and satellites: atmospheres; protoplanetary disks; radiative transfer ID EXTRASOLAR GIANT PLANETS; DISCRETE DIPOLE APPROXIMATION; DUST GROWTH PEBBLES; EARTH-LIKE PLANETS; ACCRETION DISKS; GRAIN-GROWTH; CIRCUMSTELLAR DISKS; OPTICAL-PROPERTIES; SIZE DISTRIBUTION; BROWN DWARFS AB As small solid grains grow into larger ones in protoplanetary nebulae, or in the cloudy atmospheres of exoplanets, they generally form porous aggregates rather than solid spheres. A number of previous studies have used highly sophisticated schemes to calculate opacity models for irregular, porous particles with sizes much smaller than a wavelength. However, mere growth itself can affect the opacity of the medium in far more significant ways than the detailed compositional and/or structural differences between grain constituents once aggregate particle sizes exceed the relevant wavelengths. This physics is not new; our goal here is to provide a model that provides physical insight and is simple to use in the increasing number of protoplanetary nebula evolution and exoplanet atmosphere models appearing in recent years, yet quantitatively captures the main radiative properties of mixtures of particles of arbitrary size, porosity, and composition. The model is a simple combination of effective medium theory with small-particle closed-form expressions, combined with suitably chosen transitions to geometric optics behavior. Calculations of wavelength-dependent emission and Rosseland mean opacity are shown and compared with Mie theory. The model's fidelity is very good in all comparisons we have made except in cases involving pure metal particles or monochromatic opacities for solid particles with sizes comparable to the wavelength. C1 [Cuzzi, Jeffrey N.; Davis, Sanford S.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Estrada, Paul R.] SETI Inst, Mountain View, CA 94043 USA. RP Cuzzi, JN (reprint author), NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. EM jeffrey.cuzzi@nasa.gov FU Origins of Solar Systems Program; LASER program; Astrobiology program FX J.N.C. benefitted greatly from many discussions of radiative transfer with Jim Pollack over the years. We thank Ted Roush for providing tabular values of the refractive indices used by Pollack et al. (1994). We thank Pat Cassen, Ke Chang, Tom Greene, Lee Hartmann, Stu Weidenschilling, and Diane Wooden for helpful conversations. We thank Kees Dullemond and Naor Movshovitz for encouragement to make this work more widely available. We thank our reviewer for helpful comments. J.N.C. and P.R.E. were supported under a grant from the Origins of Solar Systems Program. S.S.D. was partially supported by Grants from the LASER and Astrobiology programs. NR 96 TC 14 Z9 14 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD FEB PY 2014 VL 210 IS 2 AR 21 DI 10.1088/0067-0049/210/2/21 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA6WN UT WOS:000331239000007 ER PT J AU Marcy, GW Isaacson, H Howard, AW Rowe, JF Jenkins, JM Bryson, ST Latham, DW Howell, SB Gautier, TN Batalha, NM Rogers, L Ciardi, D Fischer, DA Gilliland, RL Kjeldsen, H Christensen-Dalsgaard, J Huber, D Chaplin, WJ Basu, S Buchhave, LA Quinn, SN Borucki, WJ Koch, DG Hunter, R Caldwell, DA Van Cleve, J Kolbl, R Weiss, LM Petigura, E Seager, S Morton, T Johnson, JA Ballard, S Burke, C Cochran, WD Endl, M MacQueen, P Everett, ME Lissauer, JJ Ford, EB Torres, G Fressin, F Brown, TM Steffen, JH Charbonneau, D Basri, GS Sasselov, DD Winn, J Sanchis-Ojeda, R Christiansen, J Adams, E Henze, C Dupree, A Fabrycky, DC Fortney, JJ Tarter, J Holman, MJ Tenenbaum, P Shporer, A Lucas, PW Welsh, WF Orosz, JA Bedding, TR Campante, TL Davies, GR Elsworth, Y Handberg, R Hekker, S Karoff, C Kawaler, SD Lund, MN Lundkvist, M Metcalfe, TS Miglio, A Aguirre, VS Stello, D White, TR Boss, A Devore, E Gould, A Prsa, A Agol, E Barclay, T Coughlin, J Brugamyer, E Mullally, F Quintana, EV Still, M Thompson, SE Morrison, D Twicken, JD Desert, JM Carter, J Crepp, JR Hebrard, G Santerne, A Moutou, C Sobeck, C Hudgins, D Haas, MR Robertson, P Lillo-Box, J Barrado, D AF Marcy, Geoffrey W. Isaacson, Howard Howard, Andrew W. Rowe, Jason F. Jenkins, Jon M. Bryson, Stephen T. Latham, David W. Howell, Steve B. Gautier, Thomas N., III Batalha, Natalie M. Rogers, Leslie Ciardi, David Fischer, Debra A. Gilliland, Ronald L. Kjeldsen, Hans Christensen-Dalsgaard, Jorgen Huber, Daniel Chaplin, William J. Basu, Sarbani Buchhave, Lars A. Quinn, Samuel N. Borucki, William J. Koch, David G. Hunter, Roger Caldwell, Douglas A. Van Cleve, Jeffrey Kolbl, Rea Weiss, Lauren M. Petigura, Erik Seager, Sara Morton, Timothy Johnson, John Asher Ballard, Sarah Burke, Chris Cochran, William D. Endl, Michael MacQueen, Phillip Everett, Mark E. Lissauer, Jack J. Ford, Eric B. Torres, Guillermo Fressin, Francois Brown, Timothy M. Steffen, Jason H. Charbonneau, David Basri, Gibor S. Sasselov, Dimitar D. Winn, Joshua Sanchis-Ojeda, Roberto Christiansen, Jessie Adams, Elisabeth Henze, Christopher Dupree, Andrea Fabrycky, Daniel C. Fortney, Jonathan J. Tarter, Jill Holman, Matthew J. Tenenbaum, Peter Shporer, Avi Lucas, Philip W. Welsh, William F. Orosz, Jerome A. Bedding, T. R. Campante, T. L. Davies, G. R. Elsworth, Y. Handberg, R. Hekker, S. Karoff, C. Kawaler, S. D. Lund, M. N. Lundkvist, M. Metcalfe, T. S. Miglio, A. Aguirre, V. Silva Stello, D. White, T. R. Boss, Alan Devore, Edna Gould, Alan Prsa, Andrej Agol, Eric Barclay, Thomas Coughlin, Jeff Brugamyer, Erik Mullally, Fergal Quintana, Elisa V. Still, Martin Thompson, Susan E. Morrison, David Twicken, Joseph D. Desert, Jean-Michel Carter, Josh Crepp, Justin R. Hebrard, Guillaume Santerne, Alexandre Moutou, Claire Sobeck, Charlie Hudgins, Douglas Haas, Michael R. Robertson, Paul Lillo-Box, Jorge Barrado, David TI MASSES, RADII, AND ORBITS OF SMALL KEPLER PLANETS: THE TRANSITION FROM GASEOUS TO ROCKY PLANETS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE planetary systems; planets and satellites: detection; stars: individual (Kepler-25, Kepler-37, Kepler-48, Kepler-68, Kepler-93, Kepler-94, Kepler-95, Kepler-96, Kepler-97, Kepler-98, Kepler-99, Kepler-100, Kepler-102, Kepler-103, Kepler-106, Kepler-109, Kepler-113, Kepler-131, Kepler-406, Kepler-407, Kepler-409); techniques: photometric; techniques: radial velocities ID CANDIDATE HOST STARS; EARTH-SIZED PLANET; SOLAR-TYPE STARS; IN SUPER-EARTHS; TIMING VARIATIONS; M-DWARF; VELOCITY MEASUREMENTS; SOLID EXOPLANETS; BULK COMPOSITION; FALSE POSITIVES AB We report on the masses, sizes, and orbits of the planets orbiting 22 Kepler stars. There are 49 planet candidates around these stars, including 42 detected through transits and 7 revealed by precise Doppler measurements of the host stars. Based on an analysis of the Kepler brightness measurements, along with high-resolution imaging and spectroscopy, Doppler spectroscopy, and (for 11 stars) asteroseismology, we establish low false-positive probabilities (FPPs) for all of the transiting planets (41 of 42 have an FPP under 1%), and we constrain their sizes and masses. Most of the transiting planets are smaller than three times the size of Earth. For 16 planets, the Doppler signal was securely detected, providing a direct measurement of the planet's mass. For the other 26 planets we provide either marginal mass measurements or upper limits to their masses and densities; in many cases we can rule out a rocky composition. We identify six planets with densities above 5 g cm(-3), suggesting a mostly rocky interior for them. Indeed, the only planets that are compatible with a purely rocky composition are smaller than similar to 2 R-circle plus. Larger planets evidently contain a larger fraction of low-density material (H, He, and H2O). C1 [Marcy, Geoffrey W.; Isaacson, Howard; Kolbl, Rea; Weiss, Lauren M.; Petigura, Erik; Basri, Gibor S.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Howard, Andrew W.] Univ Hawaii, Honolulu, HI 96822 USA. [Rowe, Jason F.; Bryson, Stephen T.; Howell, Steve B.; Batalha, Natalie M.; Huber, Daniel; Borucki, William J.; Koch, David G.; Hunter, Roger; Lissauer, Jack J.; Christiansen, Jessie; Henze, Christopher; Morrison, David; Sobeck, Charlie; Haas, Michael R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Jenkins, Jon M.; Caldwell, Douglas A.; Van Cleve, Jeffrey; Burke, Chris; Tarter, Jill; Tenenbaum, Peter; Devore, Edna; Mullally, Fergal; Quintana, Elisa V.; Thompson, Susan E.; Twicken, Joseph D.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Latham, David W.; Buchhave, Lars A.; Quinn, Samuel N.; Torres, Guillermo; Fressin, Francois; Charbonneau, David; Sasselov, Dimitar D.; Dupree, Andrea; Holman, Matthew J.; Desert, Jean-Michel] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rogers, Leslie; Morton, Timothy; Johnson, John Asher; Shporer, Avi] CALTECH, Pasadena, CA 91109 USA. [Ciardi, David] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Fischer, Debra A.; Basu, Sarbani] Yale Univ, New Haven, CT 06510 USA. [Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Kjeldsen, Hans; Christensen-Dalsgaard, Jorgen; Chaplin, William J.; Campante, T. L.; Davies, G. R.; Elsworth, Y.; Handberg, R.; Karoff, C.; Lund, M. N.; Lundkvist, M.; Miglio, A.; Aguirre, V. Silva] Aarhus Univ, SAC, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Christensen-Dalsgaard, Jorgen] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Chaplin, William J.; Campante, T. L.; Davies, G. R.; Elsworth, Y.; Handberg, R.; Miglio, A.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. [Seager, Sara; Winn, Joshua; Sanchis-Ojeda, Roberto; Carter, Josh] MIT, Cambridge, MA 02139 USA. [Ballard, Sarah; Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Cochran, William D.; Endl, Michael; MacQueen, Phillip; Robertson, Paul] Univ Texas Austin, Austin, TX 78712 USA. [Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Ford, Eric B.; Robertson, Paul] Penn State Univ, Ctr Exoplanets & Habitable Worlds, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Steffen, Jason H.] Northwestern Univ, Evanston, IL 60208 USA. [Adams, Elisabeth] Planetary Sci Inst, Tucson, AZ 85719 USA. [Fabrycky, Daniel C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Lucas, Philip W.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Welsh, William F.; Orosz, Jerome A.] San Diego State Univ, San Diego, CA 92182 USA. [Bedding, T. R.; Stello, D.; White, T. R.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia. [Hekker, S.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1012 WX Amsterdam, Netherlands. [Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Metcalfe, T. S.] Space Sci Inst, Boulder, CO 80301 USA. [Boss, Alan] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Gould, Alan] Lawrence Hall Sci, Berkeley, CA 94720 USA. [Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. [Barclay, Thomas; Coughlin, Jeff; Still, Martin] Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Brugamyer, Erik] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Crepp, Justin R.] Univ Notre Dame, Notre Dame, IN 46556 USA. [Hebrard, Guillaume] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR7095, F-75014 Paris, France. [Hebrard, Guillaume] Observ Haute Provence, CNRS, OAMP, F-04870 St Michel, France. [Santerne, Alexandre] Aix Marseille Univ, CNRS, LAM UMR 7326, F-13388 Marseille, France. [Santerne, Alexandre] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Moutou, Claire] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Hudgins, Douglas] NASA Headquarters, Washginton, DC USA. [Lillo-Box, Jorge; Barrado, David] CSIC, Depto Astrofis, Ctr Astrobiol, INTA, E-28691 Villanueva De La Canada, Spain. RP Marcy, GW (reprint author), Univ Calif Berkeley, Berkeley, CA 94720 USA. RI Santerne, Alexandre/M-9265-2013; Caldwell, Douglas/L-7911-2014; Howard, Andrew/D-4148-2015; Lillo-Box, Jorge/I-2841-2015; Barrado Navascues, David/C-1439-2017; OI Handberg, Rasmus/0000-0001-8725-4502; Kawaler, Steven/0000-0002-6536-6367; Fabrycky, Daniel/0000-0003-3750-0183; Buchhave, Lars A./0000-0003-1605-5666; Weiss, Lauren/0000-0002-3725-3058; Metcalfe, Travis/0000-0003-4034-0416; Ciardi, David/0000-0002-5741-3047; Karoff, Christoffer/0000-0003-2009-7965; Bedding, Tim/0000-0001-5222-4661; Basu, Sarbani/0000-0002-6163-3472; /0000-0001-6545-639X; Lund, Mikkel Norup/0000-0001-9214-5642; Lundkvist, Mia Sloth/0000-0002-8661-2571; Fischer, Debra/0000-0003-2221-0861; Santerne, Alexandre/0000-0002-3586-1316; Caldwell, Douglas/0000-0003-1963-9616; Howard, Andrew/0000-0001-8638-0320; Lillo-Box, Jorge/0000-0003-3742-1987; Barrado Navascues, David/0000-0002-5971-9242; Bedding, Timothy/0000-0001-5943-1460; Fortney, Jonathan/0000-0002-9843-4354; Davies, Guy/0000-0002-4290-7351; /0000-0002-0802-9145 FU NASA Science Mission Directorate; W. M. Keck Foundation; Danish National Research Foundation [DNRF106]; ASTERISK project (ASTERoseismic Investigations with SONG and Kepler); European Research Council [267864]; UK Science and Technology Facilities Council (STFC); NSF [AST-1105930, AST-1109928, AST-0645416]; Netherlands organisation for Scientific Research (NWO); European Research Council under the European Community's Seventh Framewrok Programme/ERC [338251]; NASA [ADAP12-0172, NNX08AR04G, NNX12AF73G, NNX09AG09A]; Kepler Participating Scientist Program (PSP) [NNX12AC76G]; European Research Council/European Community [239953]; National Aeronautics and Space Administration FX Kepler was competitively selected as the tenth NASA Discovery mission. Funding for this mission is provided by the NASA Science Mission Directorate. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Keck Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Some of the asteroseismology analysis was performed by the Stellar Astrophysics Centre which is funded by the Danish National Research Foundation (Grant DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (Grant 267864). D. H. is supported by an appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. W.J.C., Y.E., T.L.C., G.R.D, R.H and A.M. acknowledge financial support from the UK Science and Technology Facilities Council (STFC). S.B. acknowledges NSF grant AST-1105930. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement no.: DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (Grant agreement no. 267864). S H. acknowledges financial support from the Netherlands organisation for Scientific Research (NWO). The research leading to the presented results has received funding from the European Research Council under the European Community's Seventh Framewrok Programme (FP7/2007-2013)/ERC grant agreement no. 338251 (StellarAges). W.F. Welsh and J.A. Orosz acknowledge support from NASA through the Kepler Participating Scientist Program and from the NSF via grant AST-1109928. D. Fischer acknowledges support from NASA ADAP12-0172. O. R. Sanchis-Ojeda & J. N. Winn are supported by the Kepler Participating Scientist Program (PSP) through grant NNX12AC76G. E. Ford is partially supported by NASA PSP grants NNX08AR04G & NNX12AF73G. Eric Agol acknowledges NSF Career grant AST-0645416. R.L.G. has been partially supported by NASA co-operative agreement: NNX09AG09A. A. Santerne acknowledges the support by the European Research Council/European Community under the FP7 through Starting Grant agreement number 239953. The authors would like to thank the many people who gave so generously of their time to make this Mission a success. All Kepler data products are available to the public at the Mikulski Archive for Space Telescopes http://stdatu.stsci.edu/kepler and the spectra and their products are made available at the NExSci Exoplanet Archive and its CFOP Web site: http://exoplanetarchive.ipac.caltech.edu. We thank the many observers who contributed to the measurements reported here. We gratefully acknowledge the efforts and dedication of the Keck Observatory staff, especially Scott Dahm, Hien Tran, and Grant Hill for support with HIRES and Greg Wirth for support with remote observing. This work made use of the SIMBAD database (operated at CDS, Strasbourg, France) and NASA's Astrophysics Data System Bibliographic Services. 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.; Finally, the authors wish to extend special thanks to those of Hawai'ian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. Without their generous hospitality, the Keck observations presented herein would not have been possible. NR 119 TC 166 Z9 166 U1 24 U2 96 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD FEB PY 2014 VL 210 IS 2 AR 20 DI 10.1088/0067-0049/210/2/20 PG 70 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA6WN UT WOS:000331239000006 ER PT J AU Seljebotn, DS Mardal, KA Jewell, JB Eriksen, HK Bull, P AF Seljebotn, D. S. Mardal, K. -A. Jewell, J. B. Eriksen, H. K. Bull, P. TI A MULTI-LEVEL SOLVER FOR GAUSSIAN CONSTRAINED COSMIC MICROWAVE BACKGROUND REALIZATIONS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmic background radiation; methods: numerical; methods: statistical ID SPHERICAL HARMONIC TRANSFORMS; POWER SPECTRUM ESTIMATION; BAYESIAN-ANALYSIS; MAPS; ALGORITHMS AB We present a multi-level solver for drawing constrained Gaussian realizations or finding the maximum likelihood estimate of the cosmic microwave background sky, given noisy sky maps with partial sky coverage. The method converges substantially faster than existing Conjugate Gradient (CG) methods for the same problem. For instance, for the 143 GHz Planck frequency channel, only three multi-level W-cycles result in an absolute error smaller than 1 mu K in any pixel. Using 16 CPU cores, this translates to a computational expense of 6 minutes wall time per realization, plus 8 minutes wall time for a power-spectrum-dependent precomputation. Each additional W-cycle reduces the error by more than an order of magnitude, at an additional computational cost of 2 minutes. For comparison, we have never been able to achieve similar absolute convergence with conventional CG methods for this high signal-to-noise data set, even after thousands of CG iterations and employing expensive preconditioners. The solver is part of the Commander 2 code, which is available with an open source license at http://commander.bitbucket.org/. C1 [Seljebotn, D. S.; Eriksen, H. K.; Bull, P.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. [Mardal, K. -A.] Univ Oslo, Dept Informat, NO-0316 Oslo, Norway. [Mardal, K. -A.] Simula Res Lab, Ctr Biomed Comp, NO-1325 Lysaker, Norway. [Jewell, J. B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Seljebotn, DS (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, NO-0315 Oslo, Norway. EM d.s.seljebotn@astro.uio.no FU European Research Council [StG2010-257080]; Research Council of Norway through a Centre of Excellence grant FX We thank Mikolaj Szydlarski and Martin Reinecke for useful discussions. D.S.S., H.K.E., and P.B. are supported by European Research Council grant StG2010-257080. K.A.M. is supported by the Research Council of Norway through a Centre of Excellence grant to the Centre for Biomedical Computing at Simula Research Laboratory. NR 32 TC 6 Z9 6 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD FEB PY 2014 VL 210 IS 2 AR 24 DI 10.1088/0067-0049/210/2/24 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA6WN UT WOS:000331239000010 ER PT J AU Viero, MP Asboth, V Roseboom, IG Moncelsi, L Marsden, G Cooper, EM Zemcov, M Addison, G Baker, AJ Beelen, A Bock, J Bridge, C Conley, A Devlin, MJ Dore, O Farrah, D Finkelstein, S Font-Ribera, A Geach, JE Gebhardt, K Gill, A Glenn, J Hajian, A Halpern, M Jogee, S Kurczynski, P Lapi, A Negrello, M Oliver, SJ Papovich, C Quadri, R Ross, N Scott, D Schulz, B Somerville, R Spergel, DN Vieira, JD Wang, L Wechsler, R AF Viero, M. P. Asboth, V. Roseboom, I. G. Moncelsi, L. Marsden, G. Cooper, E. Mentuch Zemcov, M. Addison, G. Baker, A. J. Beelen, A. Bock, J. Bridge, C. Conley, A. Devlin, M. J. Dore, O. Farrah, D. Finkelstein, S. Font-Ribera, A. Geach, J. E. Gebhardt, K. Gill, A. Glenn, J. Hajian, A. Halpern, M. Jogee, S. Kurczynski, P. Lapi, A. Negrello, M. Oliver, S. J. Papovich, C. Quadri, R. Ross, N. Scott, D. Schulz, B. Somerville, R. Spergel, D. N. Vieira, J. D. Wang, L. Wechsler, R. TI THE HERSCHEL STRIPE 82 SURVEY (HerS): MAPS AND EARLY CATALOG SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology: observations; galaxies: evolution; infrared: galaxies; large-scale structure of universe; submillimeter: galaxies ID DIGITAL SKY SURVEY; SOUTH-POLE TELESCOPE; INFRARED BACKGROUND ANISOTROPIES; STAR-FORMING GALAXIES; DEEP FIELD-SOUTH; NUMBER COUNTS; EXTRAGALACTIC SURVEY; POWER SPECTRUM; DATA RELEASE; DARK-MATTER AB We present the first set of maps and band-merged catalog from the Herschel Stripe 82 Survey (HerS). Observations at 250, 350, and 500 mu m were taken with the Spectral and Photometric Imaging Receiver instrument aboard the Herschel Space Observatory. HerS covers 79 deg(2) along the SDSS Stripe 82 to an average depth of 13.0, 12.9, and 14.8 mJy beam(-1) (including confusion) at 250, 350, and 500 mu m, respectively. HerS was designed to measure correlations with external tracers of the dark matter density field-either point-like (i.e., galaxies selected from radio to X-ray) or extended (i.e., clusters and gravitational lensing)-in order to measure the bias and redshift distribution of intensities of infrared-emitting dusty star-forming galaxies and active galactic nuclei. By locating HerS in Stripe 82, we maximize the overlap with available and upcoming cosmological surveys. The band-merged catalog contains 3.3 x 10(4) sources detected at a significance of >= 3 sigma (including confusion noise). The maps and catalog are available at http://www.astro.caltech.edu/hers/. C1 [Viero, M. P.; Moncelsi, L.; Zemcov, M.; Bock, J.; Bridge, C.; Dore, O.; Schulz, B.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [Asboth, V.; Marsden, G.; Addison, G.; Halpern, M.; Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Roseboom, I. G.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Cooper, E. Mentuch; Finkelstein, S.; Gebhardt, K.; Jogee, S.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Zemcov, M.; Bock, J.; Dore, O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Baker, A. J.; Kurczynski, P.; Somerville, R.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Beelen, A.] Univ Paris 11, IAS, F-91405 Orsay, France. [Beelen, A.] CNRS, UMR 8617, F-91405 Orsay, France. [Conley, A.; Gill, A.; Glenn, J.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA. [Devlin, M. J.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Font-Ribera, A.] Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland. [Font-Ribera, A.; Ross, N.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Geach, J. E.] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England. [Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA UCB 389, Boulder, CO 80309 USA. [Hajian, A.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Lapi, A.] Univ Roma Tor Vergata, Dip Fis, I-00133 Rome, Italy. [Lapi, A.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Negrello, M.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Oliver, S. J.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Papovich, C.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, College Stn, TX 77843 USA. [Quadri, R.] Carnegie Observ, Pasadena, CA 91101 USA. [Schulz, B.] CALTECH, Infrared Proc & Anal Ctr, JPL, Pasadena, CA 91125 USA. [Spergel, D. N.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Wang, L.] Univ Durham, Inst Computat Cosmol, Dept Phys, Durham DH1 3LE, England. [Wechsler, R.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Wechsler, R.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. RP Viero, MP (reprint author), CALTECH, 1200 East Calif Blvd, Pasadena, CA 91125 USA. EM marco.viero@caltech.edu OI Scott, Douglas/0000-0002-6878-9840 FU CSA (Canada); NAOC (China); CEA, (France); CNES, (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA) FX The authors warmly thank Duncan Hanson, Brandon Hensley, Edward Chapin, and Lyman Page for their input and participation. We also thank the anonymous referee, whose comments have greatly improved this paper. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including: the University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, the University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, the University of Sussex (UK); and Caltech, JPL, NHSC, the University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). NR 76 TC 36 Z9 36 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD FEB PY 2014 VL 210 IS 2 AR 22 DI 10.1088/0067-0049/210/2/22 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA6WN UT WOS:000331239000008 ER PT J AU Goldberg, DL Loughner, CP Tzortziou, M Stehr, JW Pickering, KE Marufu, LT Dickerson, RR AF Goldberg, Daniel L. Loughner, Christopher P. Tzortziou, Maria Stehr, Jeffrey W. Pickering, Kenneth E. Marufu, Lackson T. Dickerson, Russell R. TI Higher surface ozone concentrations over the Chesapeake Bay than over the adjacent land: Observations and models from the DISCOVER-AQ and CBODAQ campaigns SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Ozone; Total reactive nitrogen; Chesapeake Bay; Community multiscale air quality (CMAQ) model ID EASTERN UNITED-STATES; LAKE-MICHIGAN OZONE; POLLUTANT TRANSPORT; ALKYL NITRATES; DEPOSITION; AIR; SENSITIVITY; METEOROLOGY; PRECURSORS; COMPONENTS AB Air quality models, such as the Community Multiscale Air Quality (CMAQ) model, indicate decidedly higher ozone near the surface of large interior water bodies, such as the Great Lakes and Chesapeake Bay. In order to test the validity of the model output, we performed surface measurements of ozone (O-3) and total reactive nitrogen (NO3,) on the 26-m Delaware II NOAA Small Research Vessel experimental (SRVx), deployed in the Chesapeake Bay for 10 daytime cruises in July 2011 as part of NASA's GEO-CAPE CBODAQ oceanographic field campaign in conjunction with NASA's DISCOVER-AQ air quality field campaign. During this 10-day period, the EPA O-3 regulatory standard of 75 ppbv averaged over an 8-h period was exceeded four times over water while ground stations in the area only exceeded the standard at most twice. This suggests that on days when the Baltimore/Washington region is in compliance with the EPA standard, air quality over the Chesapeake Bay might exceed the EPA standard. Ozone observations over the bay during the afternoon were consistently 10-20% higher than the closest upwind ground sites during the 10-day campaign; this pattern persisted during good and poor air quality days. A lower boundary layer, reduced cloud cover, slower dry deposition rates, and other lesser mechanisms, contribute to the local maximum of ozone over the Chesapeake Bay. Observations from this campaign were compared to a CMAQ simulation at 1.33 km resolution. The model is able to predict the regional maximum of ozone over the Chesapeake Bay accurately, but NO concentrations are significantly overestimated. Explanations for the overestimation of NO), in the model simulations are also explored. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Goldberg, Daniel L.; Stehr, Jeffrey W.; Pickering, Kenneth E.; Marufu, Lackson T.; Dickerson, Russell R.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Loughner, Christopher P.; Tzortziou, Maria] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Loughner, Christopher P.; Tzortziou, Maria; Pickering, Kenneth E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Goldberg, DL (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. EM dgoldb@atmos.umd.edu RI Pickering, Kenneth/E-6274-2012; Dickerson, Russell/F-2857-2010; OI Dickerson, Russell/0000-0003-0206-3083; Loughner, Christopher/0000-0002-3833-2014 FU NASA-Air Pollution Over the Eastern US; MDE Air Pollution in Maryland; NASA [NASA.NNX10AQ79G, NASA.NNX11APO7G] FX This research was supported by the NASA-Air Pollution Over the Eastern US: Integration of AURA/OMI NO2 and SO2, Aircraft, and Ground-Based Observations with Numerical Models grant the MDE Air Pollution in Maryland 2011 grant, and NASA grants NASA.NNX10AQ79G and NASA.NNX11APO7G. The authors would like to thank William Thorn III of NIST for his in situ calibration of the NOy analyzer, Heather Arkinson, Lacey Brent and Hao He for their help in laboratory calibrations of the analyzers, Ross Salawitch, Tim Canty and Linda Hembeck for their comments and help with model simulations, Antonio Mannino for his tireless organization of the SRVx cruises as part of NASA's GEO-CAPE CBDOAQ oceanographic field campaign, Ronald Cohen and his group at UC-Berkley for their total reactive nitrogen data on-board the P3-B, Chris Hostetler and Rich Ferrare and the HSRL/UC-12B teams for measurements and operations during DISCOVER-AQ, Amy Jo Scarino for the derived mixed layer height values from the HSRL backscatter profiles, John Barrick and Ali Aknan for their j(NO2) data aboard the P3-B aircraft, and Jim Crawford, Gao Chen and Mary Kleb for their work in organizing the DISCOVER-AQ campaign. NR 57 TC 14 Z9 14 U1 1 U2 26 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD FEB PY 2014 VL 84 BP 9 EP 19 DI 10.1016/j.atmosenv.2013.11.008 PG 11 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 302JZ UT WOS:000330602100002 ER PT J AU Khouri, MG Hornsby, WE Risum, N Velazquez, EJ Thomas, S Lane, A Scott, JM Koelwyn, GJ Herndon, JE Mackey, J Douglas, PS Jones, LW AF Khouri, Michel G. Hornsby, Whitney E. Risum, Niels Velazquez, Eric J. Thomas, Samantha Lane, Amy Scott, Jessica M. Koelwyn, Graeme J. Herndon, James E. Mackey, John R. Douglas, Pamela S. Jones, Lee W. TI Utility of 3-dimensional echocardiography, global longitudinal strain, and exercise stress echocardiography to detect cardiac dysfunction in breast cancer patients treated with doxorubicin-containing adjuvant therapy SO BREAST CANCER RESEARCH AND TREATMENT LA English DT Article DE Adjuvant therapy; Breast cancer; Cardiotoxicity; Echocardiography; Stress testing ID VENTRICULAR EJECTION FRACTION; CONGESTIVE-HEART-FAILURE; CELL LUNG-CANCER; MYOCARDIAL DYSFUNCTION; CARDIOVASCULAR-DISEASE; STANDARDS COMMITTEE; OF-ECHOCARDIOGRAPHY; EUROPEAN-SOCIETY; TASK-FORCE; FOLLOW-UP AB Conventional resting left ventricular ejection fraction (LVEF) assessments have limitations for detecting doxorubicin (DOX)-related cardiac dysfunction. Novel resting echocardiographic parameters, including 3-dimensional echocardiography (3DE) and global longitudinal strain (GLS), have potential for early identification of chemotherapy-related myocardial injury. Exercise "stress" is an established method to uncover impairments in cardiac function but has received limited attention in the adult oncology setting. We evaluated the utility of an integrated approach using 3DE, GLS, and exercise stress echocardiography for detecting subclinical cardiac dysfunction in early breast cancer patients treated with DOX-containing chemotherapy. Fifty-seven asymptomatic women with early breast cancer (mean 26 +/- A 22 months post-chemotherapy) and 20 sex-matched controls were studied. Resting left ventricular (LV) function was assessed by LVEF using 2-dimensional echocardiography (2DE) and 3DE and by GLS using 2-dimensional speckle-tracking echocardiography (2D-STE). After resting assessments, subjects completed cardiopulmonary exercise testing with stress 2DE. Resting LVEF was lower in patients than controls by 3DE (55 +/- A 4 vs. 59 +/- A 5 %; p = 0.005) but not 2DE (56 +/- A 4 vs. 58 +/- A 3 %; p = 0.169). 10 of 51 (20 %) patients had GLS greater than or equal to -17 %, which was below the calculated lower limit of normal (control mean 2SD); this patient subgroup had a mean 20 % impairment in GLS (-16.1 +/- A 0.9 vs. -20.1 +/- A 1.5 %; p < 0.001), despite similar LVEF by 2DE and 3DE compared to controls (p > 0.05). Cardiopulmonary function (VO2peak) was 20 % lower in patients than controls (p < 0.001). Exercise stress 2DE assessments of stroke volume (61 +/- A 11 vs. 69 +/- A 15 ml; p = 0.018) and cardiac index (2.3 +/- A 0.9 vs. 3.1 +/- A 0.8 l min(-1) m(-2) mean increase; p = 0.003) were lower in patients than controls. Post-exercise increase in cardiac index predicted VO2peak (r = 0.429, p = 0.001). Resting 3DE, GLS, and exercise stress 2DE detect subclinical cardiac dysfunction not apparent with resting 2DE in post-DOX breast cancer patients. C1 [Khouri, Michel G.; Hornsby, Whitney E.; Velazquez, Eric J.; Thomas, Samantha; Lane, Amy; Herndon, James E.; Douglas, Pamela S.; Jones, Lee W.] Duke Univ, Med Ctr, Duke Canc Inst, Durham, NC 27710 USA. [Risum, Niels] Rigshosp, Ctr Heart, DK-2100 Copenhagen, Denmark. [Scott, Jessica M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Koelwyn, Graeme J.] Univ British Columbia, Sch Hlth & Exercise Sci, Kelowna, BC, Canada. [Mackey, John R.] Cross Canc Inst, Edmonton, AB T6G 1Z2, Canada. RP Jones, LW (reprint author), Duke Univ, Med Ctr, Duke Canc Inst, Box 3085, Durham, NC 27710 USA. EM lee.w.jones@dm.duke.edu FU NCI NIH HHS [P30 CA014236] NR 42 TC 14 Z9 15 U1 1 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0167-6806 EI 1573-7217 J9 BREAST CANCER RES TR JI Breast Cancer Res. Treat. PD FEB PY 2014 VL 143 IS 3 BP 531 EP 539 DI 10.1007/s10549-013-2818-1 PG 9 WC Oncology SC Oncology GA AA3DS UT WOS:000330973700012 PM 24390149 ER EF