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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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 Astrophy