FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Colliander, A Mckague, D AF Colliander, Andreas Mckague, Darren TI The Microwave Radiometer Working Group SO IEEE GEOSCIENCE AND REMOTE SENSING MAGAZINE LA English DT Article C1 [Colliander, Andreas] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Mckague, Darren] Univ Michigan, Ann Arbor, MI 48109 USA. RP Colliander, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 10 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 2168-6831 J9 IEEE GEOSC REM SEN M JI IEEE Geosci. Remote Sens. Mag. PD SEP PY 2016 VL 4 IS 3 SI SI BP 69 EP 72 DI 10.1109/MGRS.2016.2588442 PG 4 WC Geochemistry & Geophysics; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Remote Sensing; Imaging Science & Photographic Technology GA EF0HY UT WOS:000390007700009 ER PT J AU Eingorn, M Kiefer, C Zhuk, A AF Eingorn, Maxim Kiefer, Claus Zhuk, Alexander TI Scalar and vector perturbations in a universe with discrete and continuous matter sources SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE cosmological perturbation theory; dark energy theory; gravity ID COSMOLOGICAL PERTURBATIONS; DARK-MATTER; NETWORKS; ENERGY AB We study a universe filled with dust-like matter in the form of discrete inhomogeneities (e.g., galaxies and their groups and clusters) and two sets of perfect fluids with linear and nonlinear equations of state, respectively. The background spacetime geometry is defined by the FLRW metric. In the weak gravitational field limit, we develop the first-order scalar and vector cosmological perturbation theory. Our approach works at all cosmological scales (i.e. sub-horizon and super-horizon ones) and incorporates linear and nonlinear effects with respect to energy density fluctuations. We demonstrate that the scalar perturbation (i.e. the gravitational potential) as well as the vector perturbation can be split into individual contributions from each matter source. Each of these contributions satisfies its own equation. The velocity-independent parts of the individual gravitational potentials are characterized by a finite time-dependent Yukawa interaction range being the same for each individual contribution. We also obtain the exact form of the gravitational potential and vector perturbation related to the discrete matter sources. The self-consistency of our approach is thoroughly checked. The derived equations can form the theoretical basis for numerical simulations for a wide class of cosmological models. C1 [Eingorn, Maxim] North Carolina Cent Univ, CREST, Fayetteville St 1801, Durham, NC 27707 USA. [Eingorn, Maxim] NASA, Res Ctr, Fayetteville St 1801, Durham, NC 27707 USA. [Eingorn, Maxim; Kiefer, Claus] Univ Cologne, Inst Theoret Phys, Zulpicher Str 77, D-50937 Cologne, Germany. [Zhuk, Alexander] Odessa Natl Univ, Astron Observ, Dvoryanskaya St 2, UA-65082 Odessa, Ukraine. RP Eingorn, M (reprint author), North Carolina Cent Univ, CREST, Fayetteville St 1801, Durham, NC 27707 USA.; Eingorn, M (reprint author), NASA, Res Ctr, Fayetteville St 1801, Durham, NC 27707 USA.; Eingorn, M (reprint author), Univ Cologne, Inst Theoret Phys, Zulpicher Str 77, D-50937 Cologne, Germany. EM maxim.eingorn@gmail.com; kiefer@thp.uni-koeln.de; ai.zhuk2@gmail.com FU Albert's Researcher Reunion Grant of the University of Cologne FX The work of M. Eingorn was partially supported by an Albert's Researcher Reunion Grant of the University of Cologne. NR 39 TC 0 Z9 0 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 SEP PY 2016 IS 9 AR 032 DI 10.1088/1475-7516/2016/09/032 PG 19 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA EE7CM UT WOS:000389772300017 ER PT J AU Eliasson, B Speirs, DC Daldorff, LKS AF Eliasson, B. Speirs, D. C. Daldorff, L. K. S. TI Electrostatic electron cyclotron instabilities near the upper hybrid layer due to electron ring distributions SO PLASMA PHYSICS AND CONTROLLED FUSION LA English DT Article DE electron cyclotron instability; electron Bernstein waves; ring distribution ID STIMULATED ELECTROMAGNETIC EMISSION; BROAD UPSHIFTED MAXIMUM; MAGNETIC-FIELD; PLASMA-WAVES; BERNSTEIN MODES; SIMULATION; SPACE; HARMONICS; RADIATION; DISCHARGE AB A theoretical study is presented of the electrostatic electron cyclotron instability involving Bernstein modes in a magnetized plasma. The presence of a tenuous thermal ring distribution in a Maxwellian plasma decreases the frequency of the upper hybrid branch of the electron Bernstein mode until it merges with the nearest lower branch with a resulting instability. The instability occurs when the upper hybrid frequency is somewhat above the third, fourth, and higher electron cyclotron harmonics, and gives rise to a narrow spectrum of waves around the electron cyclotron harmonic nearest to the upper hybrid frequency. For a tenuous cold ring distribution together with a Maxwellian distribution an instability can take place also near the second electron cyclotron harmonic. Noise-free Vlasov simulations are used to assess the theoretical linear growth-rates and frequency spectra, and to study the nonlinear evolution of the instability. The relevance of the results to laboratory and ionospheric heating experiments is discussed. C1 [Eliasson, B.; Speirs, D. C.] Univ Strathclyde, Dept Phys, SUPA, John Anderson Bldg, Glasgow G4 0NG, Lanark, Scotland. [Daldorff, L. K. S.] Catholic Univ Amer, 620 Michigan Ave NE, Washington, DC 20064 USA. [Daldorff, L. K. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Eliasson, B (reprint author), Univ Strathclyde, Dept Phys, SUPA, John Anderson Bldg, Glasgow G4 0NG, Lanark, Scotland. EM bengt.eliasson@strath.ac.uk FU Engineering and Physical Sciences Research Council (EPSRC), U.K. [EP/M009386/1] FX Discussions with Thomas Leyser at the Swedish Institute of Space Physics are gratefully acknowledged. This work was supported by the Engineering and Physical Sciences Research Council (EPSRC), U.K., Grant no. EP/M009386/1. Simulation data supporting the figures are available at http://dx.doi.org/10.15129/56448d9e-adb0-4d2b-afdb-029165a40f54. NR 50 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0741-3335 EI 1361-6587 J9 PLASMA PHYS CONTR F JI Plasma Phys. Control. Fusion PD SEP PY 2016 VL 58 IS 9 AR 095002 DI 10.1088/0741-3335/58/9/095002 PG 10 WC Physics, Fluids & Plasmas SC Physics GA EE2TI UT WOS:000389437000002 ER PT J AU Bartholomaus, TC Stearns, LA Sutherland, DA Shroyer, EL Nash, JD Walker, RT Catania, G Felikson, D Carroll, D Fried, MJ Noel, BPY Van Den Broeke, MR AF Bartholomaus, Timothy C. Stearns, Leigh A. Sutherland, David A. Shroyer, Emily L. Nash, Jonathan D. Walker, Ryan T. Catania, Ginny Felikson, Denis Carroll, Dustin Fried, Mason J. Noel, Brice P. Y. Van Den Broeke, Michiel R. TI Contrasts in the response of adjacent fjords and glaciers to ice-sheet surface melt in West Greenland SO ANNALS OF GLACIOLOGY LA English DT Article DE atmosphere/ice/ocean interactions; ice velocity; ice/ocean interactions; iceberg calving; subglacial processes ID SIGNIFICANT SUBMARINE MELT; JAKOBSHAVN ISBRAE; OUTLET GLACIERS; OCEAN WATERS; SOUTHEAST GREENLAND; TIDEWATER GLACIER; HELHEIM GLACIER; MASS-BALANCE; DYNAMICS; TERMINUS AB Neighboring tidewater glaciers often exhibit asynchronous dynamic behavior, despite relatively uniform regional atmospheric and oceanic forcings. This variability may be controlled by a combination of local factors, including glacier and fjord geometry, fjord heat content and circulation, and glacier surface melt. In order to characterize and understand contrasts in adjacent tidewater glacier and fjord dynamics, we made coincident ice-ocean-atmosphere observations at high temporal resolution (minutes to weeks) within a 10 000 km(2) area near Uummannaq, Greenland. Water column velocity, temperature and salinity measurements reveal systematic differences in neighboring fjords that imply contrasting circulation patterns. The observed ocean velocity and hydrography, combined with numerical modeling, suggest that subglacial discharge plays a major role in setting fjord conditions. In addition, satellite remote sensing of seasonal ice flow speed and terminus position reveal both speedup and slow-down in response to melt, as well as differences in calving style among the neighboring glaciers. Glacier force budgets and modeling also point toward subglacial discharge as a key factor in glacier behavior. For the studied region, individual glacier and fjord geometry modulate subglacial discharge, which leads to contrasts in both fjord and glacier dynamics. C1 [Bartholomaus, Timothy C.; Catania, Ginny; Felikson, Denis; Fried, Mason J.] Univ Texas Austin, Inst Geophys, Austin, TX 78712 USA. [Stearns, Leigh A.] Univ Kansas, Lawrence, KS 66045 USA. [Sutherland, David A.; Carroll, Dustin] Univ Oregon, Eugene, OR 97403 USA. [Shroyer, Emily L.; Nash, Jonathan D.] Oregon State Univ, Corvallis, OR 97331 USA. [Walker, Ryan T.] Univ Maryland, Greenbelt, MD USA. [Walker, Ryan T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Noel, Brice P. Y.; Van Den Broeke, Michiel R.] Univ Utrecht, Inst Marine & Atmospher Res Utrecht IMAU, Utrecht, Netherlands. RP Bartholomaus, TC (reprint author), Univ Texas Austin, Inst Geophys, Austin, TX 78712 USA. EM tbartholomaus@ig.utexas.edu RI Van den Broeke, Michiel/F-7867-2011; Catania, Ginny/B-9787-2008; OI Van den Broeke, Michiel/0000-0003-4662-7565; Bartholomaus, Timothy/0000-0002-1470-6720; Felikson, Denis/0000-0002-3785-5112 FU National Aeronautics and Space Administration [NNX12AP50G]; University of Texas Institute for Geophysics; Polar Program of the Netherlands Organization for Scientific Research (NOW/ALW) FX This work was partially supported by the National Aeronautics and Space Administration through grant NNX12AP50G. T.C.B. was supported by a postdoctoral fellowship from the University of Texas Institute for Geophysics. We acknowledge field support from CH2MHill Polar Services and the captain and crew of the R/V Sanna. We thank Ian Joughin for deriving glacier velocities from TerraSAR-X scenes within our area and the Polar Geospatial Center for providing World View imagery. B.N. and M.vdB. acknowledge support of the Polar Program of the Netherlands Organization for Scientific Research (NOW/ALW). The constructive critiques of two anonymous reviewers significantly improved the quality and clarity of this publication. NR 75 TC 1 Z9 1 U1 8 U2 8 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA EDINBURGH BLDG, SHAFTESBURY RD, CB2 8RU CAMBRIDGE, ENGLAND SN 0260-3055 EI 1727-5644 J9 ANN GLACIOL JI Ann. Glaciol. PD SEP PY 2016 VL 57 IS 73 BP 25 EP 38 DI 10.1017/aog.2016.19 PG 14 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA ED6GJ UT WOS:000388953800005 ER PT J AU Shuman, C Scambos, T Berthier, E AF Shuman, Christopher Scambos, Ted Berthier, Etienne TI Ice loss processes in the Seal Nunataks ice shelf region from satellite altimetry and imagery SO ANNALS OF GLACIOLOGY LA English DT Article DE Antarctic glaciology; ice shelves; remote sensing ID ANTARCTIC PENINSULA; MASS-BALANCE; LARSEN; SHEET; ELEVATION; GLACIERS; DISINTEGRATION; RESOLUTION; DISCHARGE; TRIBUTARY AB The Seal Nunataks ice shelf (SNIS, similar to 743 km(2) in 2013) is an unofficial name for a remnant area between the former Larsen A and Larsen B ice shelves off the northeastern Antarctic Peninsula. Analyses using Landsat 7 ETM+ and Terra ASTER images from 2001 to 13 and ICESat altimetry from 2003 to 09 show it has retreated and thinned following the Larsen A (1995) and Larsen B (2002) disintegrations. Despite some regional cooling and more fast ice since 2008, SNIS continues to lose ice along its margins and may be losing contact with some nunataks. Detailed analysis of data from four ICESat tracks indicates that ice shelf thinning rates range between 1.9 and 2.7 m a(-1), and generally increase from west to east. An ICESat repeat track crossing the adjacent Robertson Island shows a mean elevation loss of 1.8 m a(-1). Two tracks crossing the SNIS's remaining tributary, Rogosh Glacier, show sub-meter elevation losses. Comparing shelf remnant and grounded ice thinning rates implies that basal ocean melting augments SNIS thinning by similar to 1 m a(-1), a rate that is consistent with other estimates of ocean-driven shelf thinning in the region. C1 [Shuman, Christopher] NASA, Goddard Space Flight Ctr, UMBC, JCET, Greenbelt, MD USA. [Scambos, Ted] Univ Colorado Boulder, CIRES, NSIDC, Boulder, CO USA. [Berthier, Etienne] Univ Toulouse, UPS, CNRS, CNES,IRD,LEGOS, Toulouse, France. RP Shuman, C (reprint author), NASA, Goddard Space Flight Ctr, UMBC, JCET, Greenbelt, MD USA. EM Christopher.A.Shuman@nasa.gov RI Berthier, Etienne/B-8900-2009 OI Berthier, Etienne/0000-0001-5978-9155 FU NSF [NSF ANT-0732921]; NASA [NASA NNX10AR76G]; TOSCA program of the French Space Agency (CNES); ISIS program of the French Space Agency (CNES); NASA FX The authors would like to acknowledge the support of H. Pritchard for additional insights on a previously published analysis for the area (Pritchard and others, 2012). The authors would also like to thank J. Bohlander, K. Melocik, V. Suchdeo, and P. Vornberger for help with aspects of the imagery analysis. This project also benefitted from the help of M. Siegfried and L. Padman regarding the best available ocean tide model for the ICESat data. The ICESat data for this paper are available at the NASA Distributed Active Archive Center at the National Snow and Ice Data Center (GLA12 - GLAS/ICESat L2 Antarctic and Greenland Ice Sheet Altimetry Data). The Landsat data were acquired at no cost via the Earth Explorer website from the US Geological Survey's Earth Resource Observation and Science Center (EROS), home of the national archive for Landsat imagery. The ASTER data were provided at no cost through the Global Land Ice Measurements from Space (GLIMS) project. This work was supported by NSF and NASA grants to T. Scambos (NSF ANT-0732921; NASA NNX10AR76G), the TOSCA and ISIS programs of the French Space Agency (CNES) to E. Berthier, and NASA Cryospheric Sciences Program funds to C. Shuman. The final paper benefitted from the many helpful comments provided by two anonymous reviewers. NR 50 TC 0 Z9 0 U1 3 U2 3 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA EDINBURGH BLDG, SHAFTESBURY RD, CB2 8RU CAMBRIDGE, ENGLAND SN 0260-3055 EI 1727-5644 J9 ANN GLACIOL JI Ann. Glaciol. PD SEP PY 2016 VL 57 IS 73 BP 94 EP 104 DI 10.1017/aog.2016.29 PG 11 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA ED6GJ UT WOS:000388953800012 ER PT J AU Geller, MA Zhou, TH Shindell, D Ruedy, R Aleinov, I Nazarenko, L Tausnev, NL Kelley, M Sun, S Cheng, Y Field, RD Faluvegi, G AF Geller, Marvin A. Zhou, Tiehan Shindell, D. Ruedy, R. Aleinov, I. Nazarenko, L. Tausnev, N. L. Kelley, M. Sun, S. Cheng, Y. Field, R. D. Faluvegi, G. TI Modeling the QBO-Improvements resulting from higher-model vertical resolution SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS LA English DT Article DE modeling the QBO; fine vertical resolution; other model improvements ID QUASI-BIENNIAL OSCILLATION; STRATOSPHERIC WATER-VAPOR; TROPICAL TROPOPAUSE; GENERAL-CIRCULATION; ATMOSPHERE MODEL; GLOBAL CLIMATE; GRAVITY-WAVES; TRANSPORT; SIMULATION; CHEMISTRY AB Using the NASA Goddard Institute for Space Studies (GISS) climate model, it is shown that with proper choice of the gravity wave momentum flux entering the stratosphere and relatively fine vertical layering of at least 500 m in the upper troposphere-lower stratosphere (UTLS), a realistic stratospheric quasi-biennial oscillation (QBO) is modeled with the proper period, amplitude, and structure down to tropopause levels. It is furthermore shown that the specified gravity wave momentum flux controls the QBO period whereas the width of the gravity wave momentum flux phase speed spectrum controls the QBO amplitude. Fine vertical layering is required for the proper downward extension to tropopause levels as this permits wave-mean flow interactions in the UTLS region to be resolved in the model. When vertical resolution is increased from 1000 to 500 m, the modeled QBO modulation of the tropical tropopause temperatures increasingly approach that from observations, and the tape recorder of stratospheric water vapor also approaches the observed. The transport characteristics of our GISS models are assessed using age-of-air and N2O diagnostics, and it is shown that some of the deficiencies in model transport that have been noted in previous GISS models are greatly improved for all of our tested model vertical resolutions. More realistic tropical-extratropical transport isolation, commonly referred to as the tropical pipe, results from the finer vertical model layering required to generate a realistic QBO. C1 [Geller, Marvin A.] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA. [Zhou, Tiehan; Ruedy, R.; Aleinov, I.; Nazarenko, L.; Tausnev, N. L.; Kelley, M.; Cheng, Y.; Field, R. D.; Faluvegi, G.] NASA Goddard Inst Space Studies, New York, NY USA. [Zhou, Tiehan; Aleinov, I.; Nazarenko, L.; Cheng, Y.; Faluvegi, G.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Shindell, D.] Duke Univ, Nicholas Sch Environm, Earth & Ocean Sci, Durham, NC 27708 USA. [Ruedy, R.; Tausnev, N. L.; Kelley, M.] Trinnovim LLC, New York, NY USA. [Sun, S.] NOAA Earth Syst Res Lab, Boulder, CO USA. [Field, R. D.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. RP Geller, MA (reprint author), SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA. EM marvin.geller@stonybrook.edu FU NASA Modeling, Analysis and Prediction Program; NASA High-End Computing (HEC) Program through NASA Center for Climate Simulation (NCCS) at Goddard Space Flight Center FX This work was supported by the NASA Modeling, Analysis and Prediction Program and the NASA High-End Computing (HEC) Program through the NASA Center for Climate Simulation (NCCS) at Goddard Space Flight Center. Data from these runs are available from Tiehan Zhou (tz2131@columbia.edu). We thank Jae N. Lee for kindly providing the AURA MLS water vapor data. The authors acknowledge the two anonymous reviewers for their helpful comments, which led to an improved paper. NR 49 TC 0 Z9 0 U1 1 U2 1 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 SEP PY 2016 VL 8 IS 3 BP 1092 EP 1105 DI 10.1002/2016MS000699 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EC0LV UT WOS:000387793500004 PM 27917258 ER PT J AU Pithan, F Ackerman, A Angevine, WM Hartung, K Ickes, L Kelley, M Medeiros, B Sandu, I Steeneveld, GJ Sterk, HAM Svensson, G Vaillancourt, PA Zadra, A AF Pithan, Felix Ackerman, Andrew Angevine, Wayne M. Hartung, Kerstin Ickes, Luisa Kelley, Maxwell Medeiros, Brian Sandu, Irina Steeneveld, Gert-Jan Sterk, H. A. M. Svensson, Gunilla Vaillancourt, Paul A. Zadra, Ayrton TI Select strengths and biases of models in representing the Arctic winter boundary layer over sea ice: the Larcform 1 single column model intercomparison SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS LA English DT Article DE Arctic; boundary-layer; mixed-phase clouds; models; intercomparison; inversion ID LARGE-EDDY SIMULATIONS; CLIMATE MODELS; CLOUDS; PARAMETERIZATION; PRECIPITATION; INVERSIONS; RADIATION; SYSTEM; SHEBA AB Weather and climate models struggle to represent lower tropospheric temperature and moisture profiles and surface fluxes in Arctic winter, partly because they lack or misrepresent physical processes that are specific to high latitudes. Observations have revealed two preferred states of the Arctic winter boundary layer. In the cloudy state, cloud liquid water limits surface radiative cooling, and temperature inversions are weak and elevated. In the radiatively clear state, strong surface radiative cooling leads to the build-up of surface-based temperature inversions. Many large-scale models lack the cloudy state, and some substantially underestimate inversion strength in the clear state. Here, the transformation from a moist to a cold dry air mass is modeled using an idealized Lagrangian perspective. The trajectory includes both boundary layer states, and the single-column experiment is the first Lagrangian Arctic air formation experiment (Larcform 1) organized within GEWEX GASS (Global atmospheric system studies). The intercomparison reproduces the typical biases of large-scale models: some models lack the cloudy state of the boundary layer due to the representation of mixed-phase microphysics or to the interaction between micro- and macrophysics. In some models, high emissivities of ice clouds or the lack of an insulating snow layer prevent the build-up of surface-based inversions in the radiatively clear state. Models substantially disagree on the amount of cloud liquid water in the cloudy state and on turbulent heat fluxes under clear skies. Observations of air mass transformations including both boundary layer states would allow for a tighter constraint of model behavior. C1 [Pithan, Felix] Univ Reading, Dept Meteorol, Reading, Berks, England. [Ackerman, Andrew; Kelley, Maxwell] NASA Goddard Inst Space Studies, New York, NY USA. [Angevine, Wayne M.] Univ Colorado, CIRES, Boulder, CO 80309 USA. [Angevine, Wayne M.] NOAA Earth Syst Res Lab, Boulder, CO USA. [Hartung, Kerstin; Svensson, Gunilla] Stockholm Univ, Dept Meteorol, Stockholm, Sweden. [Ickes, Luisa] ETHZ, Inst Atmosphere & Climate, Zurich, Switzerland. [Medeiros, Brian] NCAR, Boulder, CO USA. [Sandu, Irina] ECMWF, Reading, Berks, England. [Steeneveld, Gert-Jan; Sterk, H. A. M.] Wageningen Univ, Meteorol & Air Qual Sect, Wageningen, Netherlands. [Vaillancourt, Paul A.; Zadra, Ayrton] Environm Canada, Rech Previs Numer Atmospher, Dorval, PQ, Canada. RP Pithan, F (reprint author), Univ Reading, Dept Meteorol, Reading, Berks, England. EM felix.pithan@awi.de RI Steeneveld, Gert-Jan/B-2816-2010; Manager, CSD Publications/B-2789-2015 OI Steeneveld, Gert-Jan/0000-0002-5922-8179; FU GASS (Global atmospheric system studies) steering group; ERC under Marie-Curie grant UACSURF [GAP-654492]; NASA MAP program; NWO [863.10.010, 829.09.005]; Regional and Global Climate Modeling Program of the U.S. Department of Energy's Office of Science [DE-FC02-97ER62402]; National Science Foundation; Swedish e-Science Research Centre SeRC FX We gratefully acknowledge support from the GASS (Global atmospheric system studies) steering group. We thank the researchers involved in the collection of SHEBA and ARM data for making their data sets available, and the modeling groups, the Program for Climate Model Diagnosis and Intercomparison and the World Climate Research Program's Working Group on Coupled Modeling for making available the CMIP5 multimodel data set. F.P. was funded by the ERC under Marie-Curie grant UACSURF (GAP-654492) for parts of this study. AA and MK were funded by the NASA MAP program. GJS acknowledges funding from NWO contract 863.10.010. M.S. acknowledges the support from NWO (The Dutch Science Foundation) with grant 829.09.005 ("Quantifying contributions of surface climate feedbacks to the Arctic amplification of greenhouse warming'' in the Sustainable Earth program). B.M. was supported by the Regional and Global Climate Modeling Program of the U.S. Department of Energy's Office of Science, Cooperative Agreement DE-FC02-97ER62402. NCAR is sponsored by the National Science Foundation. K.H. was supported by the Swedish e-Science Research Centre SeRC. Thanks to Bert Holtslag for comments on an earlier version of this manuscript, and to Thorsten Mauritsen for advice and support in the development of the case. We gratefully acknowledge the input and advice of two anonymous reviewers. Model results are available at https://doi.org/10.1594/PANGAEA.856770. NR 50 TC 1 Z9 1 U1 1 U2 1 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 SEP PY 2016 VL 8 IS 3 BP 1345 EP 1357 DI 10.1002/2016MS000630 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EC0LV UT WOS:000387793500017 ER PT J AU Hudson, J Spangelo, S Hine, A Kolosa, D Lemmer, K AF Hudson, Jennifer Spangelo, Sara Hine, Andrew Kolosa, Daniel Lemmer, Kristina TI Mission Analysis for CubeSats with Micropropulsion SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID ORBIT TRANSFERS; PROPULSION; THRUSTER AB The orbital maneuver capabilities of several CubeSat propulsion systems are analyzed using trajectory simulations. Properties of several types of developmental micropropulsion systems are reviewed, and Delta V capabilities are compared. Mission simulations are used to analyze the relationship between thrust arc length and orbit change capability in a low-thrust spiral trajectory. Constraints on power, fuel mass, and mission duration, as well as system-level constraints, are considered. Feasible CubeSat architectures and mission designs are developed for three electric propulsion systems. The most effective combinations of thruster operational modes and trajectory control strategies are discussed. C1 [Hudson, Jennifer; Hine, Andrew; Kolosa, Daniel; Lemmer, Kristina] Western Michigan Univ, Dept Mech & Aerosp Engn, 1903 West Michigan Ave,Mail Stop 5343, Kalamazoo, MI 49008 USA. [Spangelo, Sara] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Hudson, J (reprint author), Western Michigan Univ, Dept Mech & Aerosp Engn, 1903 West Michigan Ave,Mail Stop 5343, Kalamazoo, MI 49008 USA. FU NASA [NNX13AR18A] FX The authors acknowledge support from NASA cooperative agreement NNX13AR18A. NR 47 TC 0 Z9 0 U1 2 U2 2 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD SEP PY 2016 VL 53 IS 5 BP 836 EP 846 DI 10.2514/1.A33564 PG 11 WC Engineering, Aerospace SC Engineering GA ED1FY UT WOS:000388591400006 ER PT J AU Blandino, JJ Martinez-Baquero, N Demetriou, MA Gatsonis, NA Paschalidis, N AF Blandino, John J. Martinez-Baquero, Nicolas Demetriou, Michael A. Gatsonis, Nikolaos A. Paschalidis, Nicholas TI Feasibility for Orbital Life Extension of a CubeSat in the Lower Thermosphere SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT 54th AIAA Aerospace Sciences Meeting / AIAA Science and Technology Forum and Exposition CY JAN 04-08, 2016 CL San Diego, CA SP AIAA ID ATMOSPHERE; SATELLITE; THRUSTER; MISSION AB Orbital flight of CubeSats at altitudes between 150 and 250 km has the potential to enable a new class of scientific, commercial, and defense-related missions. A study is presented to demonstrate the feasibility of extending the orbital lifetime of a CubeSat in a 210 km orbit. Propulsion consists of an electrospray thruster operating at a 2 W, 0.175 mN thrust, and an specific impulse (Isp) of 500 s. The mission consists of two phases. In phase 1, the CubeSat is deployed from a 414 km orbit and uses the thruster to deorbit to the target altitude of 210 km. In phase 2, the propulsion system is used to extend the mission lifetime until propellant is fully expended. A control algorithm based on maintaining a target orbital energy is presented that uses an extended Kalman filter to generate estimates of the orbital dynamic state, which are periodically updated by Global Positioning System measurements. For phase 1, the spacecraft requires 25.21 days to descend from 414 to 210 km, corresponding to a Delta V = 96.25 m/s and a propellant consumption of 77.8 g. Phase 2 lasts 57.83 days, corresponding to a Delta V = 119.15 m/s, during which the remaining 94.2 g of propellant are consumed. C1 [Blandino, John J.; Martinez-Baquero, Nicolas; Demetriou, Michael A.; Gatsonis, Nikolaos A.] Worcester Polytech Inst, Aerosp Engn Program, 100 Inst Rd, Worcester, MA 01609 USA. [Paschalidis, Nicholas] NASA, Goddard Space Flight Ctr, Technol, Greenbelt, MD 20771 USA. RP Blandino, JJ (reprint author), Worcester Polytech Inst, Aerosp Engn Program, 100 Inst Rd, Worcester, MA 01609 USA. NR 29 TC 0 Z9 0 U1 2 U2 2 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD SEP PY 2016 VL 53 IS 5 BP 864 EP 875 DI 10.2514/1.A33462 PG 12 WC Engineering, Aerospace SC Engineering GA ED1FY UT WOS:000388591400008 ER PT J AU Shapiro, AA Borgonia, JP Chen, QN Dillon, RP McEnerney, B Polit-Casillas, R Soloway, L AF Shapiro, A. A. Borgonia, J. P. Chen, Q. N. Dillon, R. P. McEnerney, B. Polit-Casillas, R. Soloway, L. TI Additive Manufacturing for Aerospace Flight Applications SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID INCONEL 718; LASER; STEEL; DEPOSITION; CERAMICS; PARTS; MICROSTRUCTURE; OPTIMIZATION; ELECTRONICS; FABRICATION AB Additive manufacturing can provide many advantages to the future of space flight. Although it has been in use for plastic prototyping applications, it is only more recently that additive technologies have been investigated to produce metal and ceramic flight parts. This review paper presents some of the specific issues that arise for space flight applications, including materials selection, processing and postprocessing parameters, and the qualification process. With these concerns in mind, there are seven main applications in which additive manufacturing can provide a benefit. These applications include innovative design strategies that use the unique parameters of additive manufacturing, as well as some specific uses such as mass reduction or in situ production in space. C1 [Shapiro, A. A.] CALTECH, Jet Prop Lab, Space Technol Program Off, 4800 Oak Grove Dr,M-S 180-701, Pasadena, CA 91109 USA. [Borgonia, J. P.; Dillon, R. P.] CALTECH, Jet Prop Lab, Mech Syst Engn Fabricat & Test, 4800 Oak Grove Dr,M-S 170-104, Pasadena, CA 91109 USA. [Chen, Q. N.] CALTECH, Jet Prop Lab, Mech Syst Engn Fabricat & Test, 4800 Oak Grove Dr,M-S 158-103, Pasadena, CA 91109 USA. [McEnerney, B.] CALTECH, Jet Prop Lab, Mech Syst Engn Fabricat & Test, 4800 Oak Grove Dr,M-S 125-109, Pasadena, CA 91109 USA. [Polit-Casillas, R.] CALTECH, Jet Prop Lab, Mech Syst Engn Fabricat & Test, 4800 Oak Grove Dr,M-S 154-410, Pasadena, CA 91109 USA. [Soloway, L.] CALTECH, Jet Prop Lab, Engn & Sci Directorate, 4800 Oak Grove Dr,M-S 180-502, Pasadena, CA 91109 USA. RP Shapiro, AA (reprint author), CALTECH, Jet Prop Lab, Space Technol Program Off, 4800 Oak Grove Dr,M-S 180-701, Pasadena, CA 91109 USA. NR 43 TC 0 Z9 0 U1 20 U2 20 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 SEP PY 2016 VL 53 IS 5 BP 952 EP 959 DI 10.2514/1.A33544 PG 8 WC Engineering, Aerospace SC Engineering GA ED1FY UT WOS:000388591400015 ER PT J AU Jacobson, AR Holzworth, RH Pfaff, R Heelis, R AF Jacobson, Abram R. Holzworth, Robert H. Pfaff, Robert Heelis, Roderick TI Automated identification of discrete, lightning-generated, multiple-dispersed whistler waves in C/NOFS-VEFI very low frequency observations SO RADIO SCIENCE LA English DT Article ID LOW-LATITUDE IONOSPHERE; RADIATION BELT; TEMPORAL SIGNATURES; TWEEK ATMOSPHERICS; LOCATION NETWORK; PLASMASPHERE; PROPAGATION; ORIGIN; GUIDE AB Automated wave feature detection is required to efficiently analyze large archives of very low frequency broadband recordings for discrete whistler identification and feature extraction. We describe a new method to do this, even in the presence of simultaneous, multiple whistler phase dispersions. Previous techniques of whistler identification were unable to deal with simultaneous, multiple phase dispersions. We demonstrate the new method with data from the Vector Electric Field Investigation (VEFI) payload on the Communication/Navigation Outage Forecast System (C/NOFS) satellite, from the mission years 2008-2014. C1 [Jacobson, Abram R.; Holzworth, Robert H.] Univ Washington, Earth & Space Sci Dept, Seattle, WA 98195 USA. [Pfaff, Robert] NASA, Goddard Spaceflight Ctr, Greenbelt, MD USA. [Heelis, Roderick] Univ Texas Dallas, Ctr Space Sci, Richardson, TX 75083 USA. RP Jacobson, AR (reprint author), Univ Washington, Earth & Space Sci Dept, Seattle, WA 98195 USA. EM abramj@u.washington.edu FU NSF [1443011] FX This work was partially supported by NSF grant 1443011, "Wave-vector-resolved Study of Lightning Whistler Propagation and Energetics in the Low-latitude Plasmasphere." Readers wishing to examine the original data are invited to contact the corresponding author. NR 37 TC 0 Z9 0 U1 3 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 SEP PY 2016 VL 51 IS 9 BP 1547 EP 1569 DI 10.1002/2016RS005989 PG 23 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA ED6EI UT WOS:000388947900009 ER PT J AU Wilson, SA Howard, AD Moore, JM Grant, JA AF Wilson, Sharon A. Howard, Alan D. Moore, Jeffrey M. Grant, John A. TI A cold-wet middle-latitude environment on Mars during the Hesperian-Amazonian transition: Evidence from northern Arabia valleys and paleolakes SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID GALE CRATER; TERRA-CIMMERIA; SURFACE RUNOFF; ALLUVIAL FANS; EVOLUTION; ORIGIN; PRECIPITATION; NETWORKS; IMPACTS; SYSTEMS AB The growing inventory of post-Noachian fluvial valleys may represent a late, widespread episode of aqueous activity on Mars, contrary to the paradigm that fluvial activity largely ceased around the Noachian-Hesperian boundary. Fresh shallow valleys (FSVs) are widespread from similar to 30 to 45 degrees in both hemispheres with a high concentration in northern Arabia Terra. Valleys in northern Arabia Terra characteristically start abruptly on steeper slopes and terminate in topographic depressions at elevations corresponding to model-predicted lake levels. Longer valley systems flowed into and out of chains of paleolakes. Minimum discharges based on the dimensions of the incised channel assuming medium to coarse sand-size grains ranges from tens to hundreds of m(3) s(-1), respectively, consistent with formation via snowmelt from surface or sub-ice flows. Hydrologic calculations indicate the valleys likely formed in hundreds of years or less, and crater statistics constrain the timing of fluvial activity to between the Hesperian and middle Amazonian. Several craters with channels extending radially outward supports evidence for overflow of interior crater lakes possibly fed by groundwater. Most FSVs occur away from young impact craters which make an association with impact processes improbable. The widespread occurrence of FSVs along with their similar morphology and shared modest state of degradation is consistent with most forming during a global interval of favorable climate, perhaps contemporaneous with alluvial fan formation in equatorial and midlatitudes. Evidence for a snowmelt-based hydrology and considerable depths of water on the landscape in Arabia supports a cold, wet, and possibly habitable environment late in Martian history. C1 [Wilson, Sharon A.; Grant, John A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Wilson, Sharon A.; Howard, Alan D.] Univ Virginia, Dept Environm Sci, Clark Hall, Charlottesville, VA 22903 USA. [Moore, Jeffrey M.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Wilson, SA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.; Wilson, SA (reprint author), Univ Virginia, Dept Environm Sci, Clark Hall, Charlottesville, VA 22903 USA. EM wilsons@si.edu FU NASA [12-MDAP12-0033] FX Thanks to Cathy Quantin-Nataf and Nick Warner for their insightful reviews and to Caleb Fassett for his Associate Editor evaluation. This work was supported by a NASA grant 12-MDAP12-0033 from the Mars Data Analysis Program. The data used are listed in the figures, tables, supplemental material, and or repository at http://airandspace.si.edu/CEPSData. NR 82 TC 1 Z9 1 U1 4 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 SEP PY 2016 VL 121 IS 9 BP 1667 EP 1694 DI 10.1002/2016JE005052 PG 28 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EC0MO UT WOS:000387795400006 ER PT J AU Miljkovic, K Collins, GS Wieczorek, MA Johnson, BC Soderblom, JM Neumann, GA Zuber, MT AF Miljkovic, K. Collins, G. S. Wieczorek, M. A. Johnson, B. C. Soderblom, J. M. Neumann, G. A. Zuber, M. T. TI Subsurface morphology and scaling of lunar impact basins SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID INNER SOLAR-SYSTEM; POLE-AITKEN BASIN; HEAVY BOMBARDMENT; MASCON BASINS; MARE BASALTS; MOON; ORIGIN; GRAVITY; GRAIL; CRUST AB Impact bombardment during the first billion years after the formation of the Moon produced at least several tens of basins. The Gravity Recovery and Interior Laboratory (GRAIL) mission mapped the gravity field of these impact structures at significantly higher spatial resolution than previous missions, allowing for detailed subsurface and morphological analyses to be made across the entire globe. GRAIL-derived crustal thickness maps were used to define the regions of crustal thinning observed in centers of lunar impact basins, which represents a less unambiguous measure of a basin size than those based on topographic features. The formation of lunar impact basins was modeled numerically by using the iSALE-2D hydrocode, with a large range of impact and target conditions typical for the first billion years of lunar evolution. In the investigated range of impactor and target conditions, the target temperature had the dominant effect on the basin subsurface morphology. Model results were also used to update current impact scaling relationships applicable to the lunar setting (based on assumed target temperature). Our new temperature-dependent impact-scaling relationships provide estimates of impact conditions and transient crater diameters for the majority of impact basins mapped by GRAIL. As the formation of lunar impact basins is associated with the first similar to 700 Myr of the solar system evolution when the impact flux was considerably larger than the present day, our revised impact scaling relationships can aid further analyses and understanding of the extent of impact bombardment on the Moon and terrestrial planets in the early solar system. C1 [Miljkovic, K.; Johnson, B. C.; Soderblom, J. M.; Zuber, M. T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Miljkovic, K.] Curtin Univ, Dept Appl Geol, Perth, WA, Australia. [Collins, G. S.] Imperial Coll London, Dept Earth Sci & Engn, London, England. [Wieczorek, M. A.] Univ Paris Diderot, Sorbonne Paris Cite, Inst Phys Globe Paris, Paris, France. [Johnson, B. C.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA. [Neumann, G. A.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Miljkovic, K (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.; Miljkovic, K (reprint author), Curtin Univ, Dept Appl Geol, Perth, WA, Australia. EM katarina.miljkovic@curtin.edu.au RI Neumann, Gregory/I-5591-2013; OI Neumann, Gregory/0000-0003-0644-9944; Soderblom, Jason/0000-0003-3715-6407; Collins, Gareth/0000-0002-6087-6149 FU NASA; French Space Agency (CNES); STFC [ST/N000803/1] FX The GRAIL mission is supported by the Discovery Program of NASA and is performed under contract to the Massachusetts Institute of Technology and the Jet Propulsion Laboratory, California Institute of Technology. Additional support for this work was provided by the French Space Agency (CNES). We gratefully acknowledge the developers of iSALE-2D, including Kai Wunnemann, Dirk Elbeshausen, Boris Ivanov, and Jay Melosh. G.S.C. was funded by STFC grant ST/N000803/1. The data used in this study are attached as supporting information and are also available upon request from the main author (Katarina. Miljkovic@curtin.edu.au). NR 64 TC 0 Z9 0 U1 2 U2 2 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 SEP PY 2016 VL 121 IS 9 BP 1695 EP 1712 DI 10.1002/2016JE005038 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EC0MO UT WOS:000387795400007 ER PT J AU Fraeman, AA Ehlmann, BL Arvidson, RE Edwards, CS Grotzinger, JP Milliken, RE Quinn, DP Rice, MS AF Fraeman, A. A. Ehlmann, B. L. Arvidson, R. E. Edwards, C. S. Grotzinger, J. P. Milliken, R. E. Quinn, D. P. Rice, M. S. TI The stratigraphy and evolution of lower Mount Sharp from spectral, morphological, and thermophysical orbital data sets SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID THERMAL-CONDUCTIVITY MEASUREMENTS; GALE CRATER; REFLECTANCE SPECTROSCOPY; LANDING SITE; PARTICULATE MATERIALS; SEDIMENTARY-ROCKS; EARLY MARS; SULFATE; MINERALOGY; CONSTRAINTS AB We have developed a refined geologic map and stratigraphy for lower Mount Sharp using coordinated analyses of new spectral, thermophysical, and morphologic orbital data products. The Mount Sharp group consists of seven relatively planar units delineated by differences in texture, mineralogy, and thermophysical properties. These units are (1-3) three spatially adjacent units in the Murray formation which contain a variety of secondary phases and are distinguishable by thermal inertia and albedo differences, (4) a phyllosilicate-bearing unit, (5) a hematite-capped ridge unit, (6) a unit associated with material having a strongly sloped spectral signature at visible near-infrared wavelengths, and (7) a layered sulfate unit. The Siccar Point group consists of the Stimson formation and two additional units that unconformably overlie the Mount Sharp group. All Siccar Point group units are distinguished by higher thermal inertia values and record a period of substantial deposition and exhumation that followed the deposition and exhumation of the Mount Sharp group. Several spatially extensive silica deposits associated with veins and fractures show that late-stage silica enrichment within lower Mount Sharp was pervasive. At least two laterally extensive hematitic deposits are present at different stratigraphic intervals, and both are geometrically conformable with lower Mount Sharp strata. The occurrence of hematite at multiple stratigraphic horizons suggests redox interfaces were widespread in space and/or in time, and future measurements by the Mars Science Laboratory Curiosity rover will provide further insights into the depositional settings of these and other mineral phases. C1 [Fraeman, A. A.; Ehlmann, B. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Ehlmann, B. L.; Grotzinger, J. P.; Quinn, D. P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Arvidson, R. E.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Edwards, C. S.] US Geol Survey, Flagstaff, AZ 86001 USA. [Edwards, C. S.] Northern Univ Arizona, Dept Phys & Astron, Flagstaff, AZ USA. [Milliken, R. E.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA. [Rice, M. S.] Western Washington Univ, Dept Phys & Astron, Dept Geol, Bellingham, WA 98225 USA. RP Fraeman, AA (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM abigail.a.fraeman@jpl.nasa.gov FU W.M. Keck Institution for Space Studies; Caltech; National Aeronautics and Space Administration; National Aeronautics and Space Administration through the internal Research and Technology Development program; MSL Participating Scientist Program grant FX We thank two anonymous reviewers for their careful reading and insight comments that improved the quality of this manuscript. Thanks to Lulu Pan for providing helpful advice on CRISM parameter mapping techniques, Ara Oshagan for assistance in generating the HiRISE color mosaic, Dawn Sumner for nomenclature guidance, and Kathryn Stack Morgan for fruitful discussions about orbital mapping interpretations and sharing her general knowledge of the Gale Crater geologic context. A.A.F. was partially supported by a W.M. Keck Institution for Space Studies Postdoctoral Fellowship and Caltech Geological and Planetary Sciences Texaco Postdoctoral Fellowship. A portion of this research was also carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration and funded through the internal Research and Technology Development program. B.L.E. was partially supported by an MSL Participating Scientist Program grant. All raw data products supporting the conclusions of this work can be obtained from the NASA Planetary Data System (PDS). NR 66 TC 1 Z9 1 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD SEP PY 2016 VL 121 IS 9 BP 1713 EP 1736 DI 10.1002/2016JE005095 PG 24 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EC0MO UT WOS:000387795400008 PM 27867788 ER PT J AU Blewett, DT Stadermann, AC Susorney, HC Ernst, CM Xiao, ZY Chabot, NL Denevi, BW Murchie, SL McCubbin, FM Kinczyk, MJ Gillis-Davis, JJ Solomon, SC AF Blewett, David T. Stadermann, Amanda C. Susorney, Hannah C. Ernst, Carolyn M. Xiao, Zhiyong Chabot, Nancy L. Denevi, Brett W. Murchie, Scott L. McCubbin, Francis M. Kinczyk, Mallory J. Gillis-Davis, Jeffrey J. Solomon, Sean C. TI Analysis of MESSENGER high-resolution images of Mercury's hollows and implications for hollow formation SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID LOW-REFLECTANCE MATERIAL; DUAL IMAGING-SYSTEM; IMPACT CRATERS; SURFACE VOLATILES; RAY SPECTROMETER; SULFUR; CARBON; MOON; EROS; STRATIGRAPHY AB High-resolution images from MESSENGER provide morphological information on the nature and origin of Mercury's hollows, small depressions that likely formed when a volatile constituent was lost from the surface. Because graphite may be a component of the low-reflectance material that hosts hollows, we suggest that loss of carbon by ion sputtering or conversion to methane by proton irradiation could contribute to hollows formation. Measurements of widespread hollows in 565 images with pixel scales <20m indicate that the average depth of hollows is 24 +/- 16m. We propose that hollows cease to increase in depth when a volatile-depleted lag deposit becomes sufficiently thick to protect the underlying surface. The difficulty of developing a lag on steep topography may account for the common occurrence of hollows on crater central peaks and walls. Disruption of the lag, e.g., by secondary cratering, could restart growth of hollows in a location that had been dormant. Images at extremely high resolution (similar to 3 m/pixel) show that the edges of hollows are straight, as expected if the margins formed by scarp retreat. These highest-resolution images reveal no superposed impact craters, implying that hollows are very young. The width of hollows within rayed crater Balanchine suggests that the maximum time for lateral growth by 1 cm is similar to 10,000 yr. A process other than entrainment of dust by gases evolved in a steady-state sublimation-like process is likely required to explain the high-reflectance haloes that surround many hollows. C1 [Blewett, David T.; Ernst, Carolyn M.; Chabot, Nancy L.; Denevi, Brett W.; Murchie, Scott L.; Kinczyk, Mallory J.] Johns Hopkins Univ, Appl Phys Lab, Planetary Explorat Grp, Laurel, MD 20723 USA. [Stadermann, Amanda C.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Susorney, Hannah C.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Xiao, Zhiyong] China Univ Geosci, Wuhan, Peoples R China. [Xiao, Zhiyong] Univ Oslo, Ctr Earth Evolut & Dynam, Oslo, Norway. [McCubbin, Francis M.] NASA, Johnson Space Ctr, Houston, TX USA. [Gillis-Davis, Jeffrey J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DE USA. RP Blewett, DT (reprint author), Johns Hopkins Univ, Appl Phys Lab, Planetary Explorat Grp, Laurel, MD 20723 USA. EM david.blewett@jhuapl.edu RI Murchie, Scott/E-8030-2015; Denevi, Brett/I-6502-2012 OI Murchie, Scott/0000-0002-1616-8751; Denevi, Brett/0000-0001-7837-6663 FU NASA [NAS5-97271, NASW-00002]; NASA MESSENGER Participating Scientist grant [NNX08AN29G]; NASA/APL; NASA FX We appreciate discussions on the physics of dust lofting with David Jewitt (University of California, Los Angeles). Helpful reviews from Rebecca Thomas (University of Colorado), an anonymous reviewer, and Editor David Baratoux led us to make key improvements to this paper. The MESSENGER project is supported by the NASA Discovery Program under contracts NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory (APL) and NASW-00002 to the Carnegie Institution of Washington. D.T.B. is supported by NASA MESSENGER Participating Scientist grant NNX08AN29G. A.C.S. was supported by the NASA/APL internship program. F.M.M. acknowledges support from the NASA Solar System Workings Program. This work made use of the Integrated Software for Imagers and Spectrometers (ISIS), which is a product maintained by the U.S. Geological Survey Astrogeology Science Center. MESSENGER data are available through the NASA Planetary Data System. Supporting information "2016JE005070-ds01.txt" gives the file names of the 882 high-resolution images that contain hollows along with latitude, longitude, and pixel scale. Supporting information "2016JE005070-ds02.txt" contains information for the 2518 individual depth measurements: file name, pixel scale, depth, latitude, and longitude. NR 64 TC 0 Z9 0 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD SEP PY 2016 VL 121 IS 9 BP 1798 EP 1813 DI 10.1002/2016JE005070 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EC0MO UT WOS:000387795400013 ER PT J AU Trammell, HJ Li, LM Jiang, X Pan, YF Smith, MA Bering, EA Horst, SM Vasavada, AR Ingersoll, AP Janssen, MA West, RA Porco, CC Li, C Simon, AA Baines, KH AF Trammell, Harold Justin Li, Liming Jiang, Xun Pan, Yefeng Smith, Mark A. Bering, Edgar A., III Horst, Sarah M. Vasavada, Ashwin R. Ingersoll, Andrew P. Janssen, Michael A. West, Robert A. Porco, Carolyn C. Li, Cheng Simon, Amy A. Baines, Kevin H. TI Vortices in Saturn's Northern Hemisphere (2008-2015) observed by Cassini ISS SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID GROUND-BASED OBSERVATIONS; POLAR SPOT; THERMAL STRUCTURE; MOIST CONVECTION; IMAGING SCIENCE; CLOUD STRUCTURE; VOYAGER IMAGES; JUPITER; ATMOSPHERE; DYNAMICS AB We use observations from the Imaging Science Subsystem on Cassini to create maps of Saturn's Northern Hemisphere (NH) from 2008 to 2015, a time period including a seasonal transition (i.e., spring equinox in 2009) and the 2010 giant storm. The processed maps are used to investigate vortices in the NH during the period of 2008-2015. All recorded vortices have diameters (east-west) smaller than 6000km except for the largest vortex that developed from the 2010 giant storm. The largest vortex decreased its diameter from similar to 11,000 km in 2011 to similar to 5000 km in 2015, and its average diameter is similar to 6500 km during the period of 2011-2015. The largest vortex lasts at least 4 years, which is much longer than the lifetimes of most vortices (less than 1 year). The largest vortex drifts to north, which can be explained by the beta drift effect. The number of vortices displays varying behaviors in the meridional direction, in which the 2010 giant storm significantly affects the generation and development of vortices in the middle latitudes (25-45 degrees N). In the higher latitudes (45-90 degrees N), the number of vortices also displays strong temporal variations. The solar flux and the internal heat do not directly contribute to the vortex activities, leaving the temporal variations of vortices in the higher latitudes (45-90 degrees N) unexplained. C1 [Trammell, Harold Justin; Jiang, Xun] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX USA. [Li, Liming; Pan, Yefeng; Bering, Edgar A., III] Univ Houston, Dept Phys, Houston, TX 77004 USA. [Smith, Mark A.] Univ Houston, Dept Chem, Houston, TX USA. [Horst, Sarah M.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Vasavada, Ashwin R.; Janssen, Michael A.; West, Robert A.; Baines, Kevin H.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Ingersoll, Andrew P.; Li, Cheng] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Porco, Carolyn C.] Univ Wisconsin, Space Sci & Engn Ctr, Madison, WI USA. [Simon, Amy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Li, LM (reprint author), Univ Houston, Dept Phys, Houston, TX 77004 USA. EM lli7@central.uh.eduu RI Simon, Amy/C-8020-2012; Horst, Sarah/A-9906-2010 OI Simon, Amy/0000-0003-4641-6186; Horst, Sarah/0000-0003-4596-0702 FU NASA ROSES Cassini Data Analysis and Participating Scientists program; NASA ROSES Planetary Data Archiving, Restoration, and Tools program FX We gratefully acknowledge the Cassini ISS team for recording the raw data sets. We also acknowledge the support from the NASA ROSES Cassini Data Analysis and Participating Scientists program and Planetary Data Archiving, Restoration, and Tools program. Finally, we thank the two anonymous reviewers for providing their constructive suggestions to significantly improve the manuscript. We used the new Cassini data in 2015, which are not archived in the public Planetary Data System (PDS) (https://pds.nasa.gov) yet. The 2015 Cassini ISS raw data will be released by the Cassini ISS team and archived in the PDS in late 2016. We cannot archive the processed 2015 data before the release of the ISS raw data, so we plan to archive the data of the processed NH maps in the atmospheres node of PDS (http://atmos.pds.nasa.gov) in the beginning of 2017 or so. NR 48 TC 0 Z9 0 U1 5 U2 5 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 SEP PY 2016 VL 121 IS 9 BP 1814 EP 1826 DI 10.1002/2016JE005122 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EC0MO UT WOS:000387795400014 ER PT J AU Travinsky, A Vorobiev, D Ninkov, Z Raisanen, AD Pellish, J Robberto, M Heap, S AF Travinsky, Anton Vorobiev, Dmitry Ninkov, Zoran Raisanen, Alan D. Pellish, Jonny Robberto, Massimo Heap, Sara TI Effects of heavy ion radiation on digital micromirror device performance SO OPTICAL ENGINEERING LA English DT Article DE digital micromirror device; digital micromirror device; digital micromirror array; multiobject spectrometer; multiple-object spectroscopy; heavy-ion radiation ID MULTIOBJECT SPECTROGRAPH; SPECTROMETER; SPECTROSCOPY; TELESCOPE AB There is a pressing need in the astronomical community for space-suitable multiobject spectrometers (MOSs). Several digital micromirror device (DMD)-based prototype MOSs have been developed for ground-based observatories; however, their main use will come with deployment on a space-based mission. Therefore, the performance of DMDs under exoatmospheric radiation needs to be evaluated. DMDs were rewindowed with 2-mu m thick pellicle and tested under accelerated heavy-ion radiation (control electronics shielded from radiation), with a focus on the detection of single-event effects (SEEs) including latch-up events. Testing showed that while DMDs are sensitive to nondestructive ion-induced state changes, all SEEs are cleared with a soft reset (i.e., sending a pattern to the device). The DMDs did not experience single-event induced permanent damage or functional changes that required a hard reset (power cycle), even at high ion fluences. This suggests that the SSE rate burden will be manageable for a DMD-based instrument when exposed to solar particle fluxes and cosmic rays in orbit. (C) 2016 Society of Photo-Optical Instrumentation Engineers (SPIE) C1 [Travinsky, Anton; Vorobiev, Dmitry; Ninkov, Zoran] Rochester Inst Technol, Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14623 USA. [Raisanen, Alan D.] Rochester Inst Technol, Dept Mfg & Mech Engn Technol, 78 Lomb Mem Dr, Rochester, NY 14623 USA. [Pellish, Jonny; Heap, Sara] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. [Robberto, Massimo] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. RP Travinsky, A (reprint author), Rochester Inst Technol, Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14623 USA. EM at4395@g.rit.edu FU National Aeronautics and Space Administration (NASA) [NNX14AI62G S01] FX This research was supported by the National Aeronautics and Space Administration (NASA), Grant No. NNX14AI62G S01. We thank Dr. Vladimir Horvat and Bruce Hyman from Texas A&M University Cyclotron Institute for providing their prompt assistance during the testing and answering practical questions about the facility. We thank Michael Douglas and Benjamin Lee from Texas Instruments for productive discussions about DMD performance under extreme conditions. We are also thankful to Mike Buffalin and John "Sean" Greenslade from The Construct at RIT for sharing their expertise in rapid manufacturing and help in producing custom made parts for the test setup. Last but not least, we thank Emily Berkson from Rochester Institute of Technology for her help with the manuscript. NR 34 TC 0 Z9 0 U1 1 U2 1 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 0091-3286 EI 1560-2303 J9 OPT ENG JI Opt. Eng. PD SEP PY 2016 VL 55 IS 9 AR 094107 DI 10.1117/1.OE.55.9.094107 PG 8 WC Optics SC Optics GA EC6FV UT WOS:000388232800037 ER PT J AU Ahnen, ML Ansoldi, S Antonelli, LA Antoranz, P Babic, A Banerjee, B Bangale, P de Almeida, UB Barrio, JA Gonzalez, JB Bednarek, W Bernardini, E Biasuzzi, B Bilandl, A Blanch, O Bonnefoy, S Bonnoli, G Borracci, F Bretz, T Buson, S Carosi, A Chatterjee, A Clavero, R Colin, P Colombo, E Contreras, JL Cortina, J Covino, S da Vela, P Dazzi, F De Angelis, A De Lotto, B Wilhelmi, ED Di Pierro, F Dominguez, A Prester, DD Dorner, D Doro, M Einecke, S Glawion, DE Elsaesser, D Fernandez-Barra, A Fidalgo, D Fonseca, MV Font, L Frantzen, K Fruck, C Galindo, D Lopez, RJG Garczarczyk, M Terrats, DG Gaug, M Giammaria, P Godinovic, N Munoz, AG Gora, D Guberman, D Hadasch, D Hahn, A Hanabata, Y Hayashida, M Herrera, J Hose, J Hrupec, D Hughes, G Idec, W Kodani, K Konno, Y Kubo, H Kushida, J La Barbera, A Lelas, D Lindfors, E Lombardi, S Longo, F Lopez, M Lopez-Coto, R Majumdar, P Makariev, M Manganaro, M Mannheim, K Maraschi, L Marcote, B Mariotti, M Martinez, M Mazin, D Menzel, U Miranda, JM Mirzoyan, R Moralejo, A Moretti, E Nakajima, D Neustroev, V Niedzwieckil, A Rosillo, MN Nilsson, K Nishijima, K Noda, K Nogues, L Orito, R Overkemping, A Paiano, S Palacio, J Palatiello, M Paneque, D Paoletti, R Paredes, JM Paredes-Fortuny, X Pedaletti, G Perri, L Persic, M Poutanen, J Moroni, PGP Prandini, E Puljak, I Rhode, W Ribo, M Rico, J Garcia, JR Saito, T Satalecka, K Schultz, C Schweizer, T Shore, SN Sillanpaa, A Sitarek, J Snidaric, I Sobczynska, D Stamerra, A Steinbring, T Strzys, M Takalo, L Takami, H Tavecchio, F Temnikov, P Terzic, T Tescaro, D Teshima, M Thaele, J Torres, DF Toyama, T Treves, A Verguilov, V Vovk, I Ward, JE Will, M Wu, MH Zanin, R Blinov, DA Chen, WP Efimova, NV Forne, E Grishina, TS Hovatta, T Jordan, B Kimeridze, GN Kopatskaya, EN Koptelova, E Kurtanidze, OM Kurtanidze, SO Lahteenmaki, A Larionov, VM Larionova, EG Larionova, LV Ligustri, R Lin, HC McBreen, B Morozova, DA Nikolashvili, MG Raiteri, CM Ros, JA Sadun, AC Sigua, LA Tornikoski, M Troitsky, IS Villata, M AF Ahnen, M. L. Ansoldi, S. Antonelli, L. A. Antoranz, P. Babic, A. Banerjee, B. Bangale, P. de Almeida, U. Barres Barrio, J. A. Gonzalez, J. Becerra Bednarek, W. Bernardini, E. Biasuzzi, B. Bilandl, A. Blanch, O. Bonnefoy, S. Bonnoli, G. Borracci, F. Bretz, T. Buson, S. Carosi, A. Chatterjee, A. Clavero, R. Colin, P. Colombo, E. Contreras, J. L. Cortina, J. Covino, S. da Vela, P. Dazzi, F. De Angelis, A. De Lotto, B. Wilhelmi, E. de Ona Di Pierro, F. Dominguez, A. Prester, D. Dominis Dorner, D. Doro, M. Einecke, S. Glawion, D. Eisenacher Elsaesser, D. Fernandez-Barral, A. Fidalgo, D. Fonseca, M. V. Font, L. Frantzen, K. Fruck, C. Galindo, D. Lopez, R. J. Garcia Garczarczyk, M. Terrats, D. Garrido Gaug, M. Giammaria, P. Godinovic, N. Munoz, A. Gonzalez Gora, D. Guberman, D. Hadasch, D. Hahn, A. Hanabata, Y. Hayashida, M. Herrera, J. Hose, J. Hrupec, D. Hughes, G. Idec, W. Kodani, K. Konno, Y. Kubo, H. Kushida, J. La Barbera, A. Lelas, D. Lindfors, E. Lombardi, S. Longo, F. Lopez, M. Lopez-Coto, R. Majumdar, P. Makariev, M. Manganaro, M. Mannheim, K. Maraschi, L. Marcote, B. Mariotti, M. Martinez, M. Mazin, D. Menzel, U. Miranda, J. M. Mirzoyan, R. Moralejo, A. Moretti, E. Nakajima, D. Neustroev, V. Niedzwieckil, A. Rosillo, M. Nievas Nilsson, K. Nishijima, K. Noda, K. Nogues, L. Orito, R. Overkemping, A. Paiano, S. Palacio, J. Palatiello, M. Paneque, D. Paoletti, R. Paredes, J. M. Paredes-Fortuny, X. Pedaletti, G. Perri, L. Persic, M. Poutanen, J. Moroni, P. G. Prada Prandini, E. Puljak, I. Rhode, W. Ribo, M. Rico, J. Garcia, J. Rodriguez Saito, T. Satalecka, K. Schultz, C. Schweizer, T. Shore, S. N. Sillanpaa, A. Sitarek, J. Snidaric, I. Sobczynska, D. Stamerra, A. Steinbring, T. Strzys, M. Takalo, L. Takami, H. Tavecchio, F. Temnikov, P. Terzic, T. Tescaro, D. Teshima, M. Thaele, J. Torres, D. F. Toyama, T. Treves, A. Verguilov, V. Vovk, I. Ward, J. E. Will, M. Wu, M. H. Zanin, R. Blinov, D. A. Chen, W. P. Efimova, N. V. Forne, E. Grishina, T. S. Hovatta, T. Jordan, B. Kimeridze, G. N. Kopatskaya, E. N. Koptelova, E. Kurtanidze, O. M. Kurtanidze, S. O. Lahteenmaki, A. Larionov, V. M. Larionova, E. G. Larionova, L. V. Ligustri, R. Lin, H. C. McBreen, B. Morozova, D. A. Nikolashvili, M. G. Raiteri, C. M. Ros, J. A. Sadun, A. C. Sigua, L. A. Tornikoski, M. Troitsky, I. S. Villata, M. CA Magic Collaboration TI Long-term multi-wavelength variability and correlation study of Markarian 421 from 2007 to 2009 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astroparticle physics; BL Lacertae objects: individual: Markarian 421; radiation mechanisms: non-thermal ID X-RAY; MAGIC TELESCOPES; MAJOR UPGRADE; TEV PHOTONS; CRAB-NEBULA; EMISSION; BLAZAR; RADIO; VIEW; PERFORMANCE AB Aims. We study the multi-band variability and correlations of the TeV blazar Mrk 421 on year timescales, which can bring additional insight on the processes responsible for its broadband emission. Methods. We observed Mrk 421 in the very high energy (VHE) gamma-ray range with the Cherenkov telescope MAGIC-I from March 2007 to June 2009 for a total of 96 h of effective time after quality cuts. The VHE flux variability is quantified using several methods, including the Bayesian Block algorithm, which is applied to data from Cherenkov telescopes here for the first time. The 2.3 yr long MAGIC light curve is complemented with data from the Swift/BAT and RXTE/ASM satellites and the KVA, GASP-WEBT, OVRO, and Metsahovi telescopes from February 2007 to July 2009, allowing for an excellent characterisation of the multi-band variability and correlations over year timescales. Results. Mrk 421 was found in different gamma-ray emission states during the 2.3 yr long observation period: The flux above 400 GeV spans from the minimum nightly value of (1.3 +/- 0.4) x 10(-11) cm(-2) s(-1) to the maximum flux, that is about 24 times higher, at (3.1 +/- 0.1) x 10(-10) cm(-2) s(-1). Flares and different levels of variability in the gamma-ray light curve could be identified with the Bayesian Block algorithm. The same behaviour of a quiet and active emission was found in the X-ray light curves measured by Swift/BAT and the RXTE/ASM, with a direct correlation in time. The behaviour of the optical light curve of GASP-WEBT and the radio light curves by OVRO and Metsahovi are different as they show no coincident features with the higher energetic light curves and a less variable emission. Overall, the fractional variability increases with energy. The comparable variability in the X-ray and VHE bands and their direct correlation during both high-and low-activity periods spanning many months show that the electron populations radiating the X-ray and gamma-ray photons are either the same, as expected in the synchrotron-self-Compton mechanism, or at least strongly correlated, as expected in electromagnetic cascades. C1 [Ahnen, M. L.; Bilandl, A.; Hughes, G.; Prandini, E.] Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland. [Ansoldi, S.; Biasuzzi, B.; De Lotto, B.; Longo, F.; Palatiello, M.; Persic, M.; Treves, A.] Univ Udine, I-33100 Udine, Italy. [Ansoldi, S.; Biasuzzi, B.; De Lotto, B.; Longo, F.; Palatiello, M.; Persic, M.; Treves, A.] INFN Trieste, I-33100 Udine, Italy. [Antonelli, L. A.; Bonnoli, G.; Carosi, A.; Covino, S.; Di Pierro, F.; Giammaria, P.; La Barbera, A.; Lombardi, S.; Maraschi, L.; Perri, L.; Stamerra, A.; Tavecchio, F.] INAF Natl Inst Astrophys, I-00136 Rome, Italy. [Antoranz, P.; da Vela, P.; Miranda, J. M.; Paoletti, R.] Univ Siena, I-53100 Siena, Italy. [Antoranz, P.; da Vela, P.; Miranda, J. M.; Paoletti, R.] INFN Pisa, I-53100 Siena, Italy. [Babic, A.; Prester, D. Dominis; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Terzic, T.] Univ Split, Univ Rijeka, Rudjer Boskov Inst, Croatian MAGIC Consortium, Split, Croatia. [Babic, A.; Prester, D. Dominis; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Terzic, T.] Univ Zagreb, Zagreb 41000, Croatia. [Banerjee, B.; Chatterjee, A.; Majumdar, P.] Saha Inst Nucl Phys, 1-AF Bidhannagar,Sect 1, Kolkata 700064, India. [Bangale, P.; de Almeida, U. Barres; Borracci, F.; Colin, P.; Dazzi, F.; Fruck, C.; Hahn, A.; Hose, J.; Mazin, D.; Menzel, U.; Mirzoyan, R.; Moretti, E.; Noda, K.; Paneque, D.; Garcia, J. Rodriguez; Schweizer, T.; Strzys, M.; Teshima, M.; Toyama, T.; Vovk, I.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Barrio, J. A.; Bonnefoy, S.; Contreras, J. L.; Dominguez, A.; Fidalgo, D.; Fonseca, M. V.; Lopez, M.; Rosillo, M. Nievas] Univ Complutense, E-28040 Madrid, Spain. [Gonzalez, J. Becerra; Clavero, R.; Colombo, E.; Lopez, R. J. Garcia; Herrera, J.; Manganaro, M.; Will, M.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain. [Gonzalez, J. Becerra; Clavero, R.; Colombo, E.; Lopez, R. J. Garcia; Herrera, J.; Manganaro, M.; Will, M.] Univ La Laguna, Dept Astrofis, Tenerife 38206, Spain. [Bednarek, W.; Idec, W.; Niedzwieckil, A.; Sitarek, J.; Sobczynska, D.] Univ Lodz, PL-90236 Lodz, Poland. [Bernardini, E.; Garczarczyk, M.; Gora, D.; Pedaletti, G.; Satalecka, K.] Deutsch Elekt Synchrotron DESY, D-15738 Zeuthen, Germany. [Blanch, O.; Cortina, J.; Fernandez-Barral, A.; Munoz, A. Gonzalez; Guberman, D.; Lopez-Coto, R.; Martinez, M.; Moralejo, A.; Nogues, L.; Palacio, J.; Rico, J.; Ward, J. E.] Campus UAB, Barcelona Inst Sci & Technol, Inst Fis Altes Energies IFAE, Bellaterra 08193, Barcelona, Spain. [Bretz, T.; Dorner, D.; Glawion, D. Eisenacher; Mannheim, K.; Steinbring, T.] Univ Wurzburg, D-97074 Wurzburg, Germany. [Buson, S.; De Angelis, A.; Doro, M.; Mariotti, M.; Paiano, S.; Schultz, C.; Tescaro, D.] Univ Padua, I-35131 Padua, Italy. [Buson, S.; De Angelis, A.; Doro, M.; Mariotti, M.; Paiano, S.; Schultz, C.; Tescaro, D.] Ist Nazl Fis Nucl, I-35131 Padua, Italy. [Wilhelmi, E. de Ona; Wu, M. H.] CSIC IEEC, Inst Space Sci, Barcelona 08193, Spain. [Einecke, S.; Elsaesser, D.; Frantzen, K.; Overkemping, A.; Rhode, W.; Thaele, J.] Tech Univ Dortmund, D-44221 Dortmund, Germany. [Font, L.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, Dept Fis, Unitat Fis Radiat, Bellaterra 08193, Spain. [Font, L.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, CERES IEEC, Bellaterra 08193, Spain. [Galindo, D.; Marcote, B.; Paredes, J. M.; Paredes-Fortuny, X.; Ribo, M.; Zanin, R.] Univ Barcelona, ICC, IEEC UB, E-08028 Barcelona, Spain. [Hadasch, D.; Hanabata, Y.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Nakajima, D.; Nishijima, K.; Orito, R.; Saito, T.; Takami, H.] Univ Tokyo, Dept Phys, ICRR, Japanese MAGIC Consortium, Tokyo 1138654, Japan. [Hadasch, D.; Hanabata, Y.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Nakajima, D.; Nishijima, K.; Orito, R.; Saito, T.; Takami, H.] Univ Tokushima, Tokai Univ, Kyoto Univ, Hakubi Ctr,KEK, Tokushima, Japan. [Lindfors, E.; Neustroev, V.; Nilsson, K.; Poutanen, J.; Sillanpaa, A.; Takalo, L.] Univ Turku, Tuorla Observ, Finnish MAGIC Consortium, Oulu 90014, Finland. [Lindfors, E.; Neustroev, V.; Nilsson, K.; Poutanen, J.; Sillanpaa, A.; Takalo, L.] Univ Oulu, Astron Div, Oulu 90014, Finland. [Makariev, M.; Temnikov, P.; Verguilov, V.] Inst Nucl Energy Res, Sofia 1784, Bulgaria. [Moroni, P. G. Prada; Shore, S. N.] Univ Pisa, I-56126 Pisa, Italy. [Moroni, P. G. Prada; Shore, S. N.] Ist Nazl Fis Nucl, I-56126 Pisa, Italy. [Torres, D. F.] ICREA, Barcelona 08193, Spain. [Torres, D. F.] CSIC IEEC, Inst Space Sci, Barcelona 08193, Spain. [de Almeida, U. Barres] CBPF MCTI, 150 Urca, BR-22290180 Rio De Janeiro, Brazil. [Gonzalez, J. Becerra] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gonzalez, J. Becerra] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Gonzalez, J. Becerra] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Bernardini, E.] Humboldt Univ, Inst Phys Newtonstr 15, D-12489 Berlin, Germany. [Bretz, T.] Ecole Polytech Fed Lausanne, Lausanne, Switzerland. [Mazin, D.; Teshima, M.] Japanese MAGIC Consortium, Kyoto, Japan. [Nilsson, K.] Finnish Ctr Astron ESO FINCA, Turku, Finland. [Persic, M.] INAF Trieste, I-34143 Trieste, Italy. [Prandini, E.] ISDC Sci Data Ctr Astrophys, CH-1290 Geneva, Switzerland. [Blinov, D. A.; Grishina, T. S.; Kopatskaya, E. N.; Larionov, V. M.; Larionova, E. G.; Larionova, L. V.; Morozova, D. A.; Troitsky, I. S.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia. [Blinov, D. A.] Univ Crete, Iraklion, Greece. [Chen, W. P.; Koptelova, E.; Lin, H. C.] Natl Cent Univ, Grad Inst Astron, 300 Zhongda Rd, Taoyuan 32001, Taiwan. [Efimova, N. V.; Larionov, V. M.] Pulkovo Observ, St Petersburg 196140, Russia. [Forne, E.; Ros, J. A.] Agrupacio Astron Sabadell, Barcelona 08206, Spain. [Hovatta, T.; Lahteenmaki, A.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, Metsahovintie 114, Kylmala 02540, Finland. [Jordan, B.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. [Kimeridze, G. N.; Kurtanidze, O. M.; Kurtanidze, S. O.; Nikolashvili, M. G.; Sigua, L. A.] Abastumani Observ, GE-0301 Abastumani, Rep of Georgia. [Kurtanidze, O. M.] Kazan Fed Univ, Engelhardt Astron Observ, Tatarstan, Russia. [Lahteenmaki, A.] Aalto Univ, Dept Radio Sci & Engn, POB 3000, Aalto 00076, Finland. [Ligustri, R.] Circolo Astrofili Talmassons, Via Cadorna,57, I-33030 Talmassons, Italy. [McBreen, B.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Raiteri, C. M.; Villata, M.] INAF Osservatorio Astrofis Torino, I-10025 Pino Torinese, TO, Italy. [Sadun, A. C.] Univ Colorado, Dept Phys, Denver, CO 80217 USA. RP Overkemping, A (reprint author), Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain.; Overkemping, A (reprint author), Univ La Laguna, Dept Astrofis, Tenerife 38206, Spain.; Tescaro, D (reprint author), Univ Padua, I-35131 Padua, Italy.; Tescaro, D (reprint author), Ist Nazl Fis Nucl, I-35131 Padua, Italy.; Manganaro, M (reprint author), Tech Univ Dortmund, D-44221 Dortmund, Germany. EM manganaro@iac.es; ann-kristin.overkemping@tu-dortmund.de; diego.tescaro@gmail.com RI Lahteenmaki, Anne/L-5987-2013; Manganaro, Marina/B-7657-2011; Miranda, Jose Miguel/F-2913-2013; Barrio, Juan/L-3227-2014; GAug, Markus/L-2340-2014; Cortina, Juan/C-2783-2017; Morozova, Daria/H-1298-2013; Puljak, Ivica/D-8917-2017; OI Larionov, Valeri/0000-0002-4640-4356; Moretti, Elena/0000-0001-5477-9097; Poutanen, Juri/0000-0002-0983-0049; Torres, Diego F./0000-0002-1522-9065; Prandini, Elisa/0000-0003-4502-9053; Manganaro, Marina/0000-0003-1530-3031; Miranda, Jose Miguel/0000-0002-1472-9690; Barrio, Juan/0000-0002-0965-0259; GAug, Markus/0000-0001-8442-7877; Cortina, Juan/0000-0003-4576-0452; Morozova, Daria/0000-0002-9407-7804; Blinov, Dmitry/0000-0003-0611-5784; Larionova, Elena/0000-0002-2471-6500; Grishina, Tatiana/0000-0002-3953-6676 FU German BMBF; German MPG; Italian INFN; Italian INAF; Swiss National Fund SNF; ERDF under the Spanish MINECO [FPA2012-39502]; Japanese JSPS; Japanese MEXT; Centro de Excelencia Severo Ochoa of Spanish Consolider-Ingenio programme [SEV-2012-0234]; Academy of Finland [268740, 212656, 210338, 121148]; Croatian Science Foundation (HrZZ) Project [09/176]; University of Rijeka [13.12.1.3.02]; DFG [SFB823/C4, SFB876/C3]; Polish MNiSzW grant [745/N-HESS-MAGIC/2010/0]; NASA [NNX08AW31G, NNX11A043G]; NFS [AST-0808050, AST-1109911]; Russian RFBR [15-02-00949]; St. Petersburg University [6.38.335.2015]; Shota Rustaveli National Science Foundation [FR/577/6-320/13]; CPAN Spanish Consolider-Ingenio programme [CSD2007-00042]; MultiDark project of the Spanish Consolider-Ingenio programme [CSD2009-00064] FX We would like to thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2012-39502), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Centro de Excelencia Severo Ochoa SEV-2012-0234, CPAN CSD2007-00042, and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 268740 of the Academy of Finland, by the Croatian Science Foundation (HrZZ) Project 09/176 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. The public data archives of Swift/BAT and RXTE/ASM are acknowledged. We thank the OVRO telescope for making its results available for the public. The OVRO 40 m monitoring program is supported in part by NASA grants NNX08AW31G and NNX11A043G, and NFS grants AST-0808050 and AST-1109911. We also thank the KVA and Metsahovi telescopes for making their light curves available. M. Villata organized the optical-to-radio observations by GASP-WEBT as the president of the collaboration. The Metsahovi team acknowledges the support from the Academy of Finland to our observing projects (numbers 212656, 210338, 121148, and others). St. Petersburg University team acknowledges support from Russian RFBR grant 15-02-00949 and St. Petersburg University research grant 6.38.335.2015. The Abastumani Observatory team acknowledges financial support by the Shota Rustaveli National Science Foundation under contract FR/577/6-320/13. NR 52 TC 0 Z9 0 U1 5 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 SEP PY 2016 VL 593 AR A91 DI 10.1051/0004-6361/201628447 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4HU UT WOS:000385820100071 ER PT J AU Asensio-Torres, R Janson, M Hashimoto, J Thalmann, C Currie, T Buenzli, E Kudo, T Kuzuhara, M Kusakabe, N Abe, L Akiyama, E Brandner, W Brandt, TD Carson, J Egner, S Feldt, M Goto, M Grady, C Guyon, O Hayano, Y Hayashi, M Hayashi, S Henning, T Hodapp, K Ishii, M Iye, M Kandori, R Knapp, G Kwon, J Matsuo, T McElwain, M Mayama, S Miyama, S Morino, J Moro-Martin, A Nishimura, T Pyo, T Serabyn, E Suenaga, T Suto, H Suzuki, R Takahashi, Y Takami, M Takato, N Terada, H Turner, E Watanabe, M Wisniewski, J Yamada, T Takami, H Usuda, T Tamura, M AF Asensio-Torres, R. Janson, M. Hashimoto, J. Thalmann, C. Currie, T. Buenzli, E. Kudo, T. Kuzuhara, M. Kusakabe, N. Abe, L. Akiyama, E. Brandner, W. Brandt, T. D. Carson, J. Egner, S. Feldt, M. Goto, M. Grady, C. Guyon, O. Hayano, Y. Hayashi, M. Hayashi, S. Henning, T. Hodapp, K. Ishii, M. Iye, M. Kandori, R. Knapp, G. Kwon, J. Matsuo, T. McElwain, M. Mayama, S. Miyama, S. Morino, J. Moro-Martin, A. Nishimura, T. Pyo, T. Serabyn, E. Suenaga, T. Suto, H. Suzuki, R. Takahashi, Y. Takami, M. Takato, N. Terada, H. Turner, E. Watanabe, M. Wisniewski, J. Yamada, T. Takami, H. Usuda, T. Tamura, M. TI Polarimetry and flux distribution in the debris disk around HD 32297 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE protoplanetary disks; techniques: high angular resolution; stars: individual: HD 32297 ID CIRCUMSTELLAR DISK; IMAGING POLARIMETRY; PROTOPLANETARY DISK; HR 4796A; HD-32297; DISCOVERY; IMAGES; DUST; SUBTRACTION; EXOPLANETS AB We present high-contrast angular differential imaging (ADI) observations of the debris disk around HD32297 in H-band, as well as the first polarimetric images for this system in polarized differential imaging (PDI) mode with Subaru/HICIAO. In ADI, we detect the nearly edge-on disk at > 5 sigma levels from similar to 0.45 '' to similar to 1.7 '' (50-192AU) from the star and recover the spine deviation from the midplane already found in previous works. We also find for the first time imaging and surface brightness (SB) indications for the presence of a gapped structure on both sides of the disk at distances of similar to 0.75 '' (NE side) and similar to 0.65 '' (SW side). Global forward-modelling work delivers a best-fit model disk and well-fitting parameter intervals that essentially match previous results, with high-forward scattering grains and a ring located at 110AU. However, this single ring model cannot account for the gapped structure seen in our SB profiles. We create simple double ring models and achieve a satisfactory fit with two rings located at 60 and 95AU, respectively, low-forward scattering grains and very sharp inner slopes. In polarized light we retrieve the disk extending from similar to 0.25-1.6 '', although the central region is quite noisy and high S/N are only found in the range similar to 0.75-1.2 ''. The disk is polarized in the azimuthal direction, as expected, and the departure from the midplane is also clearly observed. Evidence for a gapped scenario is not found in the PDI data. We obtain a linear polarization degree of the grains that increases from similar to 10% at 0.55 '' to similar to 25% at 1.6 ''. The maximum is found at scattering angles of similar to 90 degrees, either from the main components of the disk or from dust grains blown out to larger radii. C1 [Asensio-Torres, R.; Janson, M.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden. [Hashimoto, J.; Kusakabe, N.] NINS, Astrobiol Ctr, Mitaka, Tokyo 1818588, Japan. [Thalmann, C.; Buenzli, E.] ETH, Inst Astron, Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland. [Currie, T.; Kudo, T.; Egner, S.; Guyon, O.; Hayano, Y.; Hayashi, S.; Nishimura, T.; Pyo, T.; Takato, N.] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Kuzuhara, M.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan. [Abe, L.] Univ Nice Sophia Antipolis, Lab Lagrange UMR 7293, CNRS, Observ Cote Azur, F-06108 Nice 2, France. [Akiyama, E.; Hayashi, M.; Ishii, M.; Iye, M.; Kandori, R.; Morino, J.; Suto, H.; Suzuki, R.; Takahashi, Y.; Terada, H.; Takami, H.; Usuda, T.; Tamura, M.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Brandner, W.; Carson, J.; Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Brandt, T. D.; Feldt, M.] Inst Adv Study, Dept Astrophys, Princeton, NJ 08540 USA. [Carson, J.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA. [Goto, M.] Ludwig Maximilians Univ Munchen, Univ Sternwarte Munchen, D-81679 Munich, Germany. [Grady, C.] Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Grady, C.] Eureka Sci, Oakland, CA 96002 USA. [Grady, C.] Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [Hodapp, K.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [Knapp, G.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Kwon, J.; Tamura, M.] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Matsuo, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto, Kyoto 6068502, Japan. [Mayama, S.] Grad Univ Adv Studies SOKENDAI, Ctr Promot Integrated Sci, Hayama, Kanagawa 2400193, Japan. [Miyama, S.] Hiroshima Univ, Higashihiroshima, Hiroshima 7398511, Japan. [Moro-Martin, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Moro-Martin, A.] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA. [Serabyn, E.; Turner, E.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan. [Suenaga, T.] Grad Univ Adv Studies SOKENDAI, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan. [Takami, M.] Acad Sin, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan. [Wisniewski, J.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Yamada, T.] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. RP Asensio-Torres, R (reprint author), Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden. EM ruben.torres@astro.su.se; markus.janson@astro.su.se RI MIYAMA, Shoken/A-3598-2015; OI Feldt, Markus/0000-0002-4188-5242 FU Knut and Alice Wallenberg foundation; US National Science Foundation [1009203] FX We would like to thank J.C. Augereau for providing the GraTeR code used to create our disk models. R. Asensio-Torres and M. Janson gratefully acknowledge funding from the Knut and Alice Wallenberg foundation. J. Carson acknowledges support via the US National Science Foundation under Award No. 1009203. NR 47 TC 0 Z9 0 U1 2 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2016 VL 593 AR A73 DI 10.1051/0004-6361/201628543 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4HU UT WOS:000385820100081 ER PT J AU Drouart, G Rocca-Volmerange, B De Breuck, C Fioc, M Lehnert, M Seymour, N Stern, D Vernet, J AF Drouart, G. Rocca-Volmerange, B. De Breuck, C. Fioc, M. Lehnert, M. Seymour, N. Stern, D. Vernet, J. TI Disentangling star formation and AGN activity in powerful infrared luminous radio galaxies at 1 < z < 4 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: high-redshift; galaxies: star formation; quasars: general; galaxies: starburst ID SPECTRAL ENERGY-DISTRIBUTIONS; INITIAL MASS FUNCTION; BLACK-HOLE ACCRETION; DEEP FIELD SOUTH; SIMILAR-TO 2; HIGH-REDSHIFT; GALACTIC NUCLEI; ELLIPTIC GALAXIES; STELLAR POPULATIONS; STARBURST GALAXIES AB High-redshift radio galaxies present signs of both star formation and AGN activity, making them ideal candidates to investigate the connection and coevolution of AGN and star formation in the progenitors of present-day massive galaxies. We make use of a sample of 11 powerful radio galaxies spanning 1 < z < 4 which have complete coverage of their spectral energy distribution (SED) from UV to FIR wavelengths. Using Herschel data, we disentangle the relative contribution of the AGN and star formation by combining the galaxy evolution code PEGASE.3 with an AGN torus model. We find that three components are necessary to reproduce the observed SEDs: an evolved and massive stellar component, a submm bright young starburst, and an AGN torus. We find that powerful radio galaxies form at very high-redshift, but experience episodic and important growth at 1 < z < 4 as the mass of the associated starburst varies from 5 to 50% of the total mass of the system. The properties of star formation differ from source to source, indicating no general trend of the star formation properties in the most infrared luminous high-redshift radio galaxies and no correlation with the AGN bolometric luminosity. Moreover, we find that AGN scattered light have a very limited impact on broad-band SED fitting on our sample. Finally, our analysis also suggests a wide range in origins for the observed star formation, which we partially constrain for some sources. C1 [Drouart, G.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Drouart, G.; Seymour, N.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA, Australia. [Drouart, G.; Rocca-Volmerange, B.; Fioc, M.; Lehnert, M.] Inst Astrophys Paris, 98bis Blvd Arago, F-75014 Paris, France. [De Breuck, C.; Vernet, J.] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Stern, D.] CALTECH, Jet Prop Lab, Mail Stop 169-221, Pasadena, CA 91109 USA. RP Drouart, G (reprint author), Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden.; Drouart, G (reprint author), Curtin Univ, Int Ctr Radio Astron Res, Perth, WA, Australia.; Drouart, G (reprint author), Inst Astrophys Paris, 98bis Blvd Arago, F-75014 Paris, France. EM guillaume.drouart@curtin.edu.au FU ARC; NASA; ESO scientific visitor programme FX G.D. would like to warmly thank Alessandro Romeo, Kirsten Knudsen, and Clive Tadhunter for the useful discussions that contributed to improve this paper. The authors also thank the referee for detailed suggestions and a thorough report that helped to clarify this paper. G.D. also thanks Nina Hatch for providing HST fluxes for the Spiderweb galaxy and A. Galametz for providing images for part of the sample. G.D. thanks Philip Best for providing the 3C 368 and 3C 470 data. N.S. is the recipient of an ARC Future Fellowship. The work of DS was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Based on observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA). GD acknowledges the support from the ESO scientific visitor programme. NR 161 TC 1 Z9 1 U1 2 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2016 VL 593 AR A109 DI 10.1051/0004-6361/201526880 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4HU UT WOS:000385820100015 ER PT J AU El-Marry, MR Thomas, N Gracia-Berna, A Pajola, M Lee, JC Massironi, M Davidsson, B Marchi, S Keller, HU Hviid, SF Besse, S Sierks, H Barbieri, C Lamy, PL Koschny, D Rickman, H Rodrigo, R A'Hearn, MF Auger, AT Barucci, MA Bertaux, JL Bertini, I Bodewits, D Gremonese, G Deppo, V Cecco, M Dehei, S Guttler, C Fornasier, S Fulle, M Giacomini, L Groussin, O Gutierrez, PJ Ip, WH Jorda, L Knollenberg, J Kovacs, G Kramm, JR Kuhrt, E Kuppers, M Lara, LM Lazzarin, M Moreno, JJL Marschall, R Marzari, F Naletto, G Oklay, N Pommerol, A Preusker, F Scholten, F Tubiana, C Vincent, JB AF El-Marry, M. R. Thomas, N. Gracia-Berna, A. Pajola, M. Lee, J. -C. Massironi, M. Davidsson, B. Marchi, S. Keller, H. U. Hviid, S. F. Besse, S. Sierks, H. Barbieri, C. Lamy, P. L. Koschny, D. Rickman, H. Rodrigo, R. A'Hearn, M. F. Auger, A. -T. Barucci, M. A. Bertaux, J. -L. Bertini, I. Bodewits, D. Gremonese, G. Da Deppo, V. De Cecco, M. Dehei, S. Guettler, C. Fornasier, S. Fulle, M. Giacomini, L. Groussin, O. Gutierrez, P. J. Ip, W. -H Jorda, L. Knollenberg, J. Kovacs, G. Kramm, J. -R. Kuehrt, E. Kueppers, M. Lara, L. M. Lazzarin, M. Moreno, J. J. Lopez Marschall, R. Marzari, F. Naletto, G. Oklay, N. Pommerol, A. Preusker, F. Scholten, F. Tubiana, C. Vincent, J. -B. TI Regional surface morphology of comet 67P/Churyumov-Gerasimenko from Rosetta/OSIRIS images: The southern hemisphere SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE comets: general; comets: individual: 67P/Churyumov-Gerasimenko; methods: observational ID NUCLEUS; OSIRIS; 67P AB Aims. The OSIRIS camera on board the Rosetta spacecraft has been acquiring images of the comet 67P/Churyumov-Gerasimenko (67P)'s nucleus since August 2014. Starting in May 2015, the southern hemisphere gradually became illuminated and was imaged for the first time. Here we present the regional morphology of the southern hemisphere, which serves as a companion to an earlier paper that presented the regional morphology of the northern hemisphere. Methods. We used OSIRIS images that were acquired at orbits similar to 45-125 km from the center of the comet (corresponding to spatial resolutions of similar to 0.8 to 2.3 m/pixel) coupled with the use of digital terrain models to define the different regions on the surface, and identify structural boundaries accurately. Results. Seven regions have been defined in the southern hemisphere bringing the total number of defined regions on the surface of the nucleus to 26. These classifications are mainly based on morphological and/or topographic boundaries. The southern hemisphere shows a remarkable dichotomy with its northern counterpart mainly because of the absence of wide-scale smooth terrains, dust coatings and large unambiguous depressions. As a result, the southern hemisphere closely resembles previously identified consolidated regions. An assessment of the overall morphology of comet 67P suggests that the comet's two lobes show surface heterogeneities manifested in different physical/mechanical characteristics, possibly extending to local (i.e., within a single region) scales. C1 [El-Marry, M. R.; Thomas, N.; Gracia-Berna, A.; Pommerol, A.] Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland. [Pajola, M.] Univ Padua, Ctr Ateneo Studied Attivita Spaziali Giuseppe Col, I-35131 Padua, Italy. [Lee, J. -C.] Natl Cent Univ, Dept Earth Sci, Chungli 32054, Taiwan. [Massironi, M.] Univ Padua, Dipartimento Geosci, Via G Gradenigo 6, I-35131 Padua, Italy. [Davidsson, B.] Jet Prop Lab, M S 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Marchi, S.] Southwest Res Inst, Solar Syst Explorat Res Virtual Inst, 1050 Walnut St,Suite 300, Boulder, CO 80302 USA. [Keller, H. U.] TU Braunschweig, Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany. [Hviid, S. F.; Preusker, F.; Scholten, F.] Inst Planetenforsch, Deutsch Zentrum Luft & Raumfahrt DLR, Rutherfordstr 2, D-12489 Berlin, Germany. [Besse, S.; Koschny, D.] European Space Agcy, Sci Support Off, NL-2201 Noordwijk, Netherlands. [Sierks, H.; Guettler, C.; Kovacs, G.; Kramm, J. -R.; Oklay, N.; Tubiana, C.; Vincent, J. -B.] Max Planck Inst Sonnensystemforsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany. [Barbieri, C.; Gremonese, G.; Lazzarin, M.; Marzari, F.] INAF Osservatorio Astrono, Vicolo Osservatorio 5, I-35122 Padua, Italy. [Lamy, P. L.; Auger, A. -T.] Aix Marseille Univ, CNRS, LAM, UMR 7326, 38 Rue Frederic Joliot Curie, F-13388 Marseille, France. [Rodrigo, R.] Int Space Sci Inst, Hallerstr 6, CH-3012 Bern, Switzerland. [Rickman, H.; Rodrigo, R.] CSIC INTA, Ctr Astrobiol, Madrid 28850, Spain. [Rickman, H.] Uppsala Univ, Dept Phys & Astron, Box 516, S-75120 Uppsala, Sweden. PAS Space Res Ctr, Bartycka 18A, PL-00716 Warsaw, Poland. [A'Hearn, M. F.; Bodewits, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Barucci, M. A.] Univ Paris Diderot, Univ Paris 06, CNRS, Obs Paris,LESIA, 5 Pl J Janssen, F-92195 Meudon, France. [Bertaux, J. -L.] CNRS UVSQ IPSL, LATMOS, 11 Blvd Alembert, F-78280 Guyancourt, France. [Bertini, I.] Univ Padua, Ctr Ateneo Studied Attivita Spaziali Giuseppe Col, I-35131 Padua, Italy. [Da Deppo, V.] CNR IFN UOS Padova LUXOR, Via Trasea 7, I-35131 Padua, Italy. [De Cecco, M.] Univ Trento, UNITN, Via Mesiano 77, I-38100 Trento, Italy. [Dehei, S.] Univ Padua, Dept Mech Engn, Via Venezia 1, I-35131 Padua, Italy. [Fulle, M.] INAF Osservatorio Astron, Via Tiepolo 11, I-34014 Trieste, Italy. [Gutierrez, P. J.; Lara, L. M.; Moreno, J. J. Lopez] CSIC, Inst Astrofis Andalucia, C Glorieta Astron S-N, E-18008 Granada, Spain. [Ip, W. -H] Natl Cent Univ, Grad Inst Astron, 300 Chung Da Rd, Chungli 32054, Taiwan. [Jorda, L.] Lab Astrophys Marseille, 38 Rue Frederic Joliot Curie, F-13388 Marseille 13, France. [Kueppers, M.] European Space Astron Ctr ESA, Sci Support Off, POB 78, Madrid 28691, Spain. [Naletto, G.] Univ Padua, Dept Informat Engn, Via Gradenigo 6-B, I-35131 Padua, Italy. RP El-Marry, MR (reprint author), Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland. EM mohammed.elmaarry@space.unibe.ch RI Naletto, Giampiero/S-6329-2016; Gutierrez, Pedro/K-9637-2014; OI Naletto, Giampiero/0000-0003-2007-3138; Gutierrez, Pedro/0000-0002-7332-6269; fulle, marco/0000-0001-8435-5287; Massironi, Matteo/0000-0002-7757-8818 FU Germany (DLR); France (CNES); Italy (ASI); Spain (MEC); Sweden (SNSB); ESA Technical Directorate; Rosetta mission FX OSIRIS was built by a consortium of the Max-Planck-Institut fur Sonnensystemforschung, in Gottingen, Germany, CISAS-University of Padova, Italy, the Laboratoire d'Astrophysique de Marseille, France, the Instituto de Astrofisica de Andalucia, CSIC, Granada, Spain, the Research and Scientific Support Department of the European Space Agency, Noordwijk, The Netherlands, the Instituto Nacional de Tecnica Aeroespacial, Madrid, Spain, the Universidad Politechnica de Madrid, Spain, the Department of Physics and Astronomy of Uppsala University, Sweden, and the Institut fur Datentechnik und Kommunikationsnetze der Technischen Universitat Braunschweig, Germany. The support of the national funding agencies of Germany (DLR), France (CNES), Italy (ASI), Spain (MEC), Sweden (SNSB), and the ESA Technical Directorate is gratefully acknowledged. We thank the ESA teams at ESAC, ESOC and ESTEC for their work in support of the Rosetta mission. NR 26 TC 5 Z9 5 U1 5 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 SEP PY 2016 VL 593 AR A110 DI 10.1051/0004-6361/201628634 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4HU UT WOS:000385820100095 ER PT J AU Luna, M Diaz, AJ Oliver, R Terradas, J Karpen, J AF Luna, M. Diaz, A. J. Oliver, R. Terradas, J. Karpen, J. TI The effects of magnetic-field geometry on longitudinal oscillations of solar prominences: Cross-sectional area variation for thin tubes SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: corona; Sun: filaments, prominences; Sun: oscillations; Sun: magnetic fields ID MAGNETOHYDRODYNAMIC WAVES; FILAMENT; MODEL AB Context. Solar prominences are subject to both field-aligned (longitudinal) and transverse oscillatory motions, as evidenced by an increasing number of observations. Large-amplitude longitudinal motions provide valuable information on the geometry of the filament-channel magnetic structure that supports the cool prominence plasma against gravity. Our pendulum model, in which the restoring force is the gravity projected along the dipped field lines of the magnetic structure, best explains these oscillations. However, several factors can influence the longitudinal oscillations, potentially invalidating the pendulum model. Aims. The aim of this work is to study the influence of large-scale variations in the magnetic field strength along the field lines, i.e., variations of the cross-sectional area along the flux tubes supporting prominence threads. Methods. We studied the normal modes of several flux tube configurations, using linear perturbation analysis, to assess the influence of different geometrical parameters on the oscillation properties. Results. We found that the influence of the symmetric and asymmetric expansion factors on longitudinal oscillations is small. Conclusions. We conclude that the longitudinal oscillations are not significantly influenced by variations of the cross-section of the flux tubes, validating the pendulum model in this context. C1 [Luna, M.] Inst Astrofis Canarias, Tenerife 38205, Spain. [Luna, M.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Diaz, A. J.; Oliver, R.; Terradas, J.] Univ Illes Balears, Dept Fis, Palma de Mallorca 07122, Spain. [Oliver, R.; Terradas, J.] Inst Appl Comp & Community Code IAC3, Palma de Mallorca 07122, Spain. [Karpen, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Luna, M (reprint author), Inst Astrofis Canarias, Tenerife 38205, Spain.; Luna, M (reprint author), Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. EM mluna@iac.es FU Spanish Ministry of Economy and Competitiveness [AYA2011-24808, AYA2010-18029, AYA2014-55078-P]; FP7 European Research Council [277829]; Spanish "Ministerio de Educacion y Ciencia"; MINECO; FEDER [AYA2014-54485-P]; International Space Science Institute (ISSI) [314] FX M. Luna acknowledges the support by the Spanish Ministry of Economy and Competitiveness through projects AYA2011-24808, AYA2010-18029, and AYA2014-55078-P. This work contributes to the deliverables identified in FP7 European Research Council grant agreement 277829, "Magnetic Connectivity through the Solar Partially Ionized Atmosphere" (PI: E. Khomenko). J.T. acknowledges support from the Spanish "Ministerio de Educacion y Ciencia" through a Ramon y Cajal grant and support from MINECO and FEDER funds through project AYA2014-54485-P. M.L., J.T., and J.K. acknowledge support from the International Space Science Institute (ISSI) to the Team 314 on "Large-Amplitude Oscillation in prominences" led by M. Luna. NR 18 TC 0 Z9 0 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2016 VL 593 AR A64 DI 10.1051/0004-6361/201628845 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4HU UT WOS:000385820100124 ER PT J AU Montesinos, B Eiroa, C Krivov, AV Marshall, JP Pilbratt, GL Liseau, R Mora, A Maldonado, J Wolf, S Ertel, S Bayo, A Augereau, JC Heras, AM Fridlund, M Danchi, WC Solano, E Kirchschlager, F del Burgo, C Montes, D AF Montesinos, B. Eiroa, C. Krivov, A. V. Marshall, J. P. Pilbratt, G. L. Liseau, R. Mora, A. Maldonado, J. Wolf, S. Ertel, S. Bayo, A. Augereau, J. -C. Heras, A. M. Fridlund, M. Danchi, W. C. Solano, E. Kirchschlager, F. del Burgo, C. Montes, D. TI Incidence of debris discs around FGK stars in the solar neighbourhood SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: late-type; circumstellar matter; protoplanetary disks; infrared: stars ID MAIN-SEQUENCE STARS; CA-II H; ABSOLUTE FLUX CALIBRATION; SUN-LIKE STARS; NEARBY STARS; BOLOMETRIC CORRECTIONS; PLANET-SEARCH; FIELD STARS; HOST STARS; COOL STARS AB Context. Debris discs are a consequence of the planet formation process and constitute the fingerprints of planetesimal systems. Their counterparts in the solar system are the asteroid and Edgeworth-Kuiper belts. Aims. The aim of this paper is to provide robust numbers for the incidence of debris discs around FGK stars in the solar neighbourhood. Methods. The full sample of 177 FGK stars with d <= 20 pc proposed for the DUst around NEarby Stars (DUNES) survey is presented. Herschel/PACS observations at 100 and 160 mu m were obtained, and were complemented in some cases with data at 70 mu m and at 250, 350, and 500 mu m SPIRE photometry. The 123 objects observed by the DUNES collaboration were presented in a previous paper. The remaining 54 stars, shared with the Disc Emission via a Bias-free Reconnaissance in IR and Sub-mm (DEBRIS) consortium and observed by them, and the combined full sample are studied in this paper. The incidence of debris discs per spectral type is analysed and put into context together with other parameters of the sample, like metallicity, rotation and activity, and age. Results. The subsample of 105 stars with d <= 15 pc containing 23 F, 33 G, and 49 K stars is complete for F stars, almost complete for G stars, and contains a substantial number of K stars from which we draw solid conclusions on objects of this spectral type. The incidence rates of debris discs per spectral type are 0.26(-0.14)(+0.21) (6 objects with excesses out of 23 F stars), 0.21(-0.11)(+0.17) (7 out of 33 G stars), and 0.20(-0.09)(+0.14) (10 out of 49 K stars); the fraction for all three spectral types together is 0.22(-0.07)(+0.08) (23 out of 105 stars). The uncertainties correspond to a 95% confidence level. The medians of the upper limits of L-dust/L-* for each spectral type are 7.8 x 10(-7) (F), 1.4 x 10(-6) (G), and 2.2 x 10(-6) (K); the lowest values are around 4.0 x 10(-7). The incidence of debris discs is similar for active (young) and inactive (old) stars. The fractional luminosity tends to drop with increasing age, as expected from collisional erosion of the debris belts. C1 [Montesinos, B.; Solano, E.] CSIC INTA, Ctr Astrobiol CAB, Dept Astrofis, ESAC Campus,Camino Bajo Castillo S-N, Madrid 28692, Spain. [Eiroa, C.] Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, Modulo 15,Campus Cantoblanco, E-28049 Madrid, Spain. [Montesinos, B.; Eiroa, C.] UAM, Unidad Asociada CAB, Madrid, Spain. [Krivov, A. V.] Univ Jena, Astrophys Inst & Univ, Schillergasschen 2-3, D-07745 Jena, Germany. [Marshall, J. P.] UNSW Australia, Sch Phys, Sydney, NSW 2052, Australia. [Marshall, J. P.] UNSW Australia, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia. [Pilbratt, G. L.; Heras, A. M.] European Space Res & Technol Ctr ESTEC SCIS, Sci Support Off, Directorate Sci, ESA, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. [Liseau, R.; Fridlund, M.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Mora, A.] ESA ESAC Gaia SOC, POB 78, Madrid 28691, Spain. INAF, Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy. [Wolf, S.; Kirchschlager, F.] Univ Kiel, Inst Theoret Phys & Astrophys, Leibnizstr 15, D-24118 Kiel, Germany. [Ertel, S.] Univ Arizona, Dept Astron, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. [Bayo, A.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Av Gran Bretana 1111,5030 Casilla, Valparaiso, Chile. [Bayo, A.] Univ Valparaiso, ICM Nucleus Protoplanetary Disks, Av Gran Bretana 1111, Valparaiso 2360102, Chile. [Augereau, J. -C.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. [Augereau, J. -C.] CNRS, IPAG, F-38000 Grenoble, France. [Fridlund, M.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Danchi, W. C.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys, Code 667, Greenbelt, MD 20771 USA. [Solano, E.] CSIC INTA, Ctr Astrobiol CAB, Spanish Virtual Observ, ESAC Campus,Camino Bajo Castillo S-N, Madrid 28692, Spain. [del Burgo, C.] Inst Nacl Astrofis Opt & Electr, Luis Enrique Erro 1, Puebla, Mexico. [Montes, D.] Univ Complutense Madrid, Fac Ciencias Fis, Dept Astrofis, E-28040 Madrid, Spain. RP Montesinos, B (reprint author), CSIC INTA, Ctr Astrobiol CAB, Dept Astrofis, ESAC Campus,Camino Bajo Castillo S-N, Madrid 28692, Spain.; Montesinos, B (reprint author), UAM, Unidad Asociada CAB, Madrid, Spain. EM benjamin.montesinos@cab.inta-csic.es RI Solano, Enrique/C-2895-2017; Montesinos, Benjamin/C-3493-2017; OI Montesinos, Benjamin/0000-0002-7982-2095; Montes, David/0000-0002-7779-238X FU Spanish grant [AYA2013-45347-P]; DFG [KR 2164/13-1, KR 2164/15-1, WO 857/151]; UNSW Vice-Chancellor's postdoctoral fellowship; Proyecto Fondecyt de Iniciacion [11140572]; PNP; CNES; Mexican CONACyT [CB-2012-183007]; [AYA2011-26202] FX The authors are grateful to the referee for the careful revision of the original manuscript, and for the comments and suggestions. We also thank Francisco Galindo, Mauro Lopez del Fresno, and Pablo Riviere for their valuable help. B. Montesinos and C. Eiroa are supported by Spanish grant AYA2013-45347-P; they and J.P. Marshall and J. Maldonado were supported by grant AYA2011-26202. A.V. Krivov acknowledges the DFG support under contracts KR 2164/13-1 and KR 2164/15-1. J.P. Marshall is supported by a UNSW Vice-Chancellor's postdoctoral fellowship. R. Liseau thanks the Swedish National Space Board for its continued support. A. Bayo acknowledges financial support from the Proyecto Fondecyt de Iniciacion 11140572 and scientific support from the Millenium Science Initiative, Chilean Ministry of Economy, Nucleus RC130007. J.-C. Augereau acknowledges support from PNP and CNES. F. Kirchschlager thanks the DFG for finantial support under contract WO 857/151. C. del Burgo has been supported by Mexican CONACyT research grant CB-2012-183007. NR 95 TC 0 Z9 0 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2016 VL 593 AR A51 DI 10.1051/0004-6361/201628329 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4HU UT WOS:000385820100058 ER PT J AU Muller, C Burd, PR Schulz, R Coppejans, R Falcke, H Intema, H Kadler, M Krauss, F Ojha, R AF Mueller, C. Burd, P. R. Schulz, R. Coppejans, R. Falcke, H. Intema, H. Kadler, M. Krauss, F. Ojha, R. TI The MHz-peaked radio spectrum of the unusual gamma-ray source PMNJ1603-4904 SO ASTRONOMY & ASTROPHYSICS LA English DT Letter DE galaxies: active; galaxies: jets; galaxies: individual: PMN J1603-4904 ID LARGE-AREA TELESCOPE; COMPACT STEEP-SPECTRUM; ACTIVE GALACTIC NUCLEI; FREE-FREE ABSORPTION; SOURCE CATALOG; SYMMETRIC OBJECTS; EVOLUTION; YOUNG; EMISSION; GALAXIES AB Context. The majority of bright extragalactic gamma-ray sources are blazars. Only a few radio galaxies have been detected by Fermi/LAT. Recently, the GHz-peaked spectrum source PKS 1718-649 was confirmed to be gamma-ray bright, providing further evidence for the existence of a population of gamma-ray loud, compact radio galaxies. A spectral turnover in the radio spectrum in the MHz to GHz range is a characteristic feature of these objects, which are thought to be young due to their small linear sizes. The multiwavelength properties of the gamma-ray source PMNJ1603-4904 suggest that it is a member of this source class. Aims. The known radio spectrum of PMNJ1603-4904 can be described by a power law above 1 GHz. Using observations from the Giant Metrewave Radio Telescope (GMRT) at 150, 325, and 610 MHz, we investigate the behavior of the spectrum at lower frequencies to search for a low-frequency turnover. Methods. Data from the TIFR GMRT Sky Survey (TGSS ADR) catalog and archival GMRT observations were used to construct the first MHz to GHz spectrum of PMNJ1603-4904. Results. We detect a low-frequency turnover of the spectrum and measure the peak position at about 490 MHz (rest-frame), which, using the known relation of peak frequency and linear size, translates into a maximum linear source size of similar to 1.4 kpc. Conclusions. The detection of the MHz peak indicates that PMNJ1603-4904 is part of this population of radio galaxies with turnover frequencies in the MHz to GHz regime. Therefore it can be considered the second confirmed object of this kind detected in gamma-rays. Establishing this gamma-ray source class will help to investigate the gamma-ray production sites and to test broadband emission models. C1 [Mueller, C.; Coppejans, R.; Falcke, H.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands. [Burd, P. R.; Kadler, M.] Univ Wurzburg, Inst Theoret Phys & Astrophys, Hubland, D-97074 Wurzburg, Germany. [Schulz, R.] ASTRON, Netherlands Inst Radio Astron, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. [Intema, H.] Leiden Univ, Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands. [Krauss, F.] Univ Amsterdam, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. [Krauss, F.] Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. [Ojha, R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 661, Greenbelt, MD 20771 USA. [Ojha, R.] CRESST Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Ojha, R.] Catholic Univ Amer, Washington, DC 20064 USA. RP Muller, C (reprint author), Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands. EM cmueller@astro.ru.nl NR 51 TC 0 Z9 0 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2016 VL 593 AR L19 DI 10.1051/0004-6361/201629547 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4HU UT WOS:000385820100159 ER PT J AU Werner, K Rauch, T Kruk, JW AF Werner, K. Rauch, T. Kruk, J. W. TI The far-ultraviolet spectra of two hot PG1159 stars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: abundances; stars: atmospheres; stars: evolution; stars: AGB and post-AGB; white dwarfs ID PRE-WHITE-DWARFS; TO-OXYGEN RATIO; POST-AGB STARS; PLANETARY-NEBULAE; INTERSTELLAR-MEDIUM; ATOMIC DATABASE; IRON ABUNDANCE; LINES; SPECTROSCOPY; MODEL AB PG 115(stars are hot, hydrogen-deficient (pre-) white dwarfs with atmospheres mainly composed of helium, carbon, and oxygen. The unusual surface chemistry is the result of a late helium-shell flash. Observed element abundances enable us to test stellar evolution models quantitatively with respect to their nucleosynthesis products formed near the helium-burning shell of the progenitor asymptotic giant branch stars. Because of the high effective temperatures (T-eff), abundance determinations require ultraviolet spectroscopy and non-local thermodynamic equilibrium model atmosphere analyses. Up to now, we have presented results for the prototype of this spectral class and two cooler members (T-eff in the range 85 000-140 000 K). Here we report on the results for two even hotter stars (PG 1520 + 525 and PG 1144 + 005, both with T-eff = 150 000 K) which are the only two objects in this temperature-gravity region for which useful far-ultraviolet spectra are available, and revisit the prototype star. Previous results on the abundances of some species are confirmed, while results on others (Si, P, S) are revised. In particular, a solar abundance of sulphur is measured in contrast to earlier claims of a strong S deficiency that contradicted stellar evolution models. For the first time, we assess the abundances of Na, Al, and Cl with newly constructed non-LTE model atoms. Besides the main constituents (He, C, O), we determine the abundances (or upper limits) of N, F, Ne, Na, Al, Si, P, S, Cl, Ar, and Fe. Generally, good agreement with stellar models is found. C1 [Werner, K.; Rauch, T.] Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany. [Kruk, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Werner, K (reprint author), Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany. EM werner@astro.uni-tuebingen.de FU German Aerospace Center (DLR) [50 OR 1507] FX We thank Amanda Karakas and Luke Shingles for reporting unpublished results to us. T. Rauch is supported by the German Aerospace Center (DLR) under grant 50 OR 1507. The TMAD service (http://astro-uni-tuebingen.de/similar to TMAD) used to compile atomic data for this paper was constructed as part of the activities of the German Astrophysical Virtual Observatory. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and of NASA's Astrophysics Data System Bibliographic Services. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). This work had been done using the profile fitting procedure OWENS, developed by M. Lemoine and the FUSE French Team. NR 48 TC 0 Z9 0 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2016 VL 593 AR A104 DI 10.1051/0004-6361/201628892 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4HU UT WOS:000385820100130 ER PT J AU Hopkins, FM Ehleringer, JR Bush, SE Duren, RM Miller, CE Lai, CT Hsu, YK Carranza, V Randerson, JT AF Hopkins, Francesca M. Ehleringer, James R. Bush, Susan E. Duren, Riley M. Miller, Charles E. Lai, Chun-Ta Hsu, Ying-Kuang Carranza, Valerie Randerson, James T. TI Mitigation of methane emissions in cities: How new measurements and partnerships can contribute to emissions reduction strategies SO EARTHS FUTURE LA English DT Article ID GREENHOUSE-GAS EMISSIONS; WASTE-WATER TREATMENT; MUNICIPAL SOLID-WASTE; CLIMATE-CHANGE ACTION; NATURAL-GAS; CARBON-DIOXIDE; UNITED-STATES; NITROUS-OXIDE; LOS-ANGELES; PIPELINE LEAKS AB Cities generate 70% of anthropogenic greenhouse gas emissions, a fraction that is growing with global urbanization. While cities play an important role in climate change mitigation, there has been little focus on reducing urban methane (CH4) emissions. Here, we develop a conceptual framework for CH4 mitigation in cities by describing emission processes, the role of measurements, and a need for new institutional partnerships. Urban CH4 emissions are likely to grow with expanding use of natural gas and organic waste disposal systems in growing population centers; however, we currently lack the ability to quantify this increase. We also lack systematic knowledge of the relative contribution of these distinct source sectors on emissions. We present new observations from four North American cities to demonstrate that CH4 emissions vary in magnitude and sector from city to city and hence require different mitigation strategies. Detections of fugitive emissions from these systems suggest that current mitigation approaches are absent or ineffective. These findings illustrate that tackling urban CH4 emissions will require research efforts to identify mitigation targets, develop and implement new mitigation strategies, and monitor atmospheric CH4 levels to ensure the success of mitigation efforts. This research will require a variety of techniques to achieve these objectives and should be deployed in cities globally. We suggest that metropolitan scale partnerships may effectively coordinate systematic measurements and actions focused on emission reduction goals. C1 [Hopkins, Francesca M.; Randerson, James T.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Hopkins, Francesca M.; Duren, Riley M.; Miller, Charles E.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. [Ehleringer, James R.; Bush, Susan E.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Ehleringer, James R.] Univ Utah, Global Change & Sustainabil Ctr, Salt Lake City, UT USA. [Lai, Chun-Ta] San Diego State Univ, Dept Biol, San Diego, CA 92182 USA. [Hsu, Ying-Kuang] Calif Air Resources Board, Monitoring & Lab Div, Sacramento, CA USA. [Carranza, Valerie] Univ Calif Los Angeles, Environm Sci, Los Angeles, CA USA. RP Hopkins, FM (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.; Hopkins, FM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM francesca.m.hopkins@jpl.nasa.gov FU U.S. Department of Energy Office of Science (BER) [DE-SC0005266]; NASA Postdoctoral Program fellowship; NASA FX This study was supported by U.S. Department of Energy Office of Science (BER), Grant No. DE-SC0005266. F.M.H. also acknowledges support from a NASA Postdoctoral Program fellowship. We thank Liz Wiggins, Gergana Mouteva, Massimo Lupascu, Clayton Elder, Nicky Cuozzo, Ashley Braunthal, Joshua Miu, and Simon Fahrni for collecting Fairbanks data, Joshua Rambo for collecting San Diego data, and Bill Johnson for thermal camera images. Portions of this work were performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. The data used are listed in the references, tables, figures, and supplement. Raw data are available by contacting francesca.m.hopkins@jpl.nasa.gov. NR 123 TC 0 Z9 0 U1 11 U2 11 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2328-4277 J9 EARTHS FUTURE JI Earth Future PD SEP PY 2016 VL 4 IS 9 BP 408 EP 425 DI 10.1002/2016EF000381 PG 18 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA EC0BB UT WOS:000387761400001 ER PT J AU Verma, M Fisher, JB Mallick, K Ryu, Y Kobayashi, H Guillaume, A Moore, G Ramakrishnan, L Hendrix, V Wolf, S Sikka, M Kiely, G Wohlfahrt, G Gielen, B Roupsard, O Toscano, P Arain, A Cescatti, A AF Verma, Manish Fisher, Joshua B. Mallick, Kaniska Ryu, Youngryel Kobayashi, Hideki Guillaume, Alexandre Moore, Gregory Ramakrishnan, Lavanya Hendrix, Valerie Wolf, Sebastian Sikka, Munish Kiely, Gerard Wohlfahrt, Georg Gielen, Bert Roupsard, Olivier Toscano, Piero Arain, Altaf Cescatti, Alessandro TI Global Surface Net-Radiation at 5 km from MODIS Terra SO REMOTE SENSING LA English DT Article DE surface net-radiation; MODIS; FLUXNET; SURFRAD; modeling; validation ID DOWNWELLING LONGWAVE RADIATION; CLEAR-SKY DAYS; HETEROGENEOUS LANDSCAPE; LAND; EVAPOTRANSPIRATION; VALIDATION; ATMOSPHERE; FLUX; ALGORITHMS; PRODUCT AB Reliable and fine resolution estimates of surface net-radiation are required for estimating latent and sensible heat fluxes between the land surface and the atmosphere. However, currently, fine resolution estimates of net-radiation are not available and consequently it is challenging to develop multi-year estimates of evapotranspiration at scales that can capture land surface heterogeneity and are relevant for policy and decision-making. We developed and evaluated a global net-radiation product at 5 km and 8-day resolution by combining mutually consistent atmosphere and land data from the Moderate Resolution Imaging Spectroradiometer (MODIS) on board Terra. Comparison with net-radiation measurements from 154 globally distributed sites (414 site-years) from the FLUXNET and Surface Radiation budget network (SURFRAD) showed that the net-radiation product agreed well with measurements across seasons and climate types in the extratropics (Wilmott's index ranged from 0.74 for boreal to 0.63 for Mediterranean sites). Mean absolute deviation between the MODIS and measured net-radiation ranged from 38.0 +/- 1.8 W.m(-2) in boreal to 72.0 +/- 4.1 W.m(-2) in the tropical climates. The mean bias was small and constituted only 11%, 0.7%, 8.4%, 4.2%, 13.3%, and 5.4% of the mean absolute error in daytime net-radiation in boreal, Mediterranean, temperate-continental, temperate, semi-arid, and tropical climate, respectively. To assess the accuracy of the broader spatiotemporal patterns, we upscaled error-quantified MODIS net-radiation and compared it with the net-radiation estimates from the coarse spatial (1 degrees x 1 degrees) but high temporal resolution gridded net-radiation product from the Clouds and Earth's Radiant Energy System (CERES). Our estimates agreed closely with the net-radiation estimates from the CERES. Difference between the two was less than 10 W center dot m(-2) in 94% of the total land area. MODIS net-radiation product will be a valuable resource for the science community studying turbulent fluxes and energy budget at the Earth's surface. C1 [Verma, Manish; Fisher, Joshua B.; Guillaume, Alexandre; Moore, Gregory; Sikka, Munish] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Mallick, Kaniska] LIST, Dept Environm Res & Innovat ERIN, L-4422 Belvaux, Luxembourg. [Ryu, Youngryel] Seoul Natl Univ, Dept Landscape Architecture & Rural Syst Engn, Seoul 151921, South Korea. [Kobayashi, Hideki] Japan Agcy Marine Earth Sci & Technol, Yokohama, Kanagawa 2360001, Japan. [Ramakrishnan, Lavanya; Hendrix, Valerie] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Wolf, Sebastian] Swiss Fed Inst Technol, Dept Environm Syst Sci, CH-8092 Zurich, Switzerland. [Kiely, Gerard] Univ Coll, Environm Res Inst, Civil & Environm Engn Dept, Cork T12P2FY, Ireland. [Wohlfahrt, Georg] Univ Innsbruck, Inst Ecol, Sternwartestr 15, A-6020 Innsbruck, Austria. [Gielen, Bert] Univ Antwerp, Dept Biol, Res Grp Plant & Vegetat Ecol, B-2610 Antwerp, Belgium. [Roupsard, Olivier] CIRAD, UMR Eco & Sols Ecol Fonct Biogeochim Sols & Agroe, F-34000 Montpellier, France. [Roupsard, Olivier] CATIE Trop Agr Ctr Res & Higher Educ, Turrialba 937170, Costa Rica. [Toscano, Piero] CNR, Inst Biometeorol IBIMET, Via G Caproni 8, I-50145 Florence, Italy. [Arain, Altaf] McMaster Univ, McMaster Ctr Climate Change, Sch Geog & Earth Sci, 1280 Main St West, Hamilton, ON L8S 4K1, Canada. [Cescatti, Alessandro] European Commiss, Joint Res Ctr, Directorate Sustainable Resources, I-21027 Ispra, Italy. RP Verma, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM manishve@umich.edu; Joshua.B.Fisher@jpl.nasa.gov; kaniska.mallick@gmail.com; ryuyr77@gmail.com; hkoba@jamstec.go.jp; alexandre.guillaume@jpl.nasa.gov; Gregory.J.Moore@jpl.nasa.gov; LRamakrishnan@lbl.gov; vchendrix@lbl.gov; sewolf@ethz.ch; Munish.Sikka@jpl.nasa.gov; g.kiely@ucc.ie; Georg.Wohlfahrt@uibk.ac.at; bert.gielen@uantwerpen.be; olivier.roupsard@cirad.fr; p.toscano@ibimet.cnr.it; arainm@mcmaster.ca; alessandro.cescatti@jrc.ec.europa.eu RI Wohlfahrt, Georg/D-2409-2009; Wolf, Sebastian/B-4580-2010; OI Wohlfahrt, Georg/0000-0003-3080-6702; Wolf, Sebastian/0000-0001-7717-6993; Toscano, Piero/0000-0001-9184-0707; Mallick, Kaniska/0000-0002-2735-930X; Fisher, Joshua/0000-0003-4734-9085 FU NASA Terrestrial Hydrology Program; Jet Propulsion Laboratory Strategic Research & Technology Development Climate Initiative; U.S. Department of Energy, Biological and Environmental Research, Terrestrial Carbon Program [DE-FG02-04ER63917, DE-FG02-04ER63911]; AfriFlux; AsiaFlux; CarboAfrica; CarboEuropeIP; CarboItaly; CarboMont; ChinaFlux; Fluxnet-Canada; CFCAS; NSERC; BIOCAP; Environment Canada; NRCan; GreenGrass; KoFlux; LBA; NECC; OzFlux; TCOS-Siberia; USCCC; Australian Research Council [DP0451247, DP0344744, DP0772981, DP130101566]; European Commission [300083] FX Support for this study was provided by the NASA Terrestrial Hydrology Program and Jet Propulsion Laboratory Strategic Research & Technology Development Climate Initiative. The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Copyright 2015 California Institute of Technology. Government sponsorship acknowledged. This work used net-radiation data acquired by the FLUXNET community and in particular by the following networks: AmeriFlux (U.S. Department of Energy, Biological and Environmental Research, Terrestrial Carbon Program (DE-FG02-04ER63917 and DE-FG02-04ER63911)), AfriFlux, AsiaFlux, CarboAfrica, CarboEuropeIP, CarboItaly, CarboMont, ChinaFlux, Fluxnet-Canada (supported by CFCAS, NSERC, BIOCAP, Environment Canada, and NRCan), GreenGrass, KoFlux, LBA, NECC, OzFlux, TCOS-Siberia, USCCC. The authors gratefully acknowledge the efforts of the FLUXNET community to compile and make available the La Thuile data set. Data from AU-Fog-Fogg Dam, AU-How-Howard Springs, AU-Wac-Wallaby Creek was funded by the Australian Research Council (DP0451247, DP0344744, DP0772981 and DP130101566). Support for collection and archiving was provided through the Australia Terrestrial Ecosystem Research Network (TERN) (http://www.tern.org.au). SW was supported by the European Commission with a Marie Curie International Outgoing Fellowship (grant 300083). NR 61 TC 0 Z9 0 U1 7 U2 7 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD SEP PY 2016 VL 8 IS 9 AR UNSP 739 DI 10.3390/rs8090739 PG 20 WC Remote Sensing SC Remote Sensing GA DY9XB UT WOS:000385488000049 ER PT J AU Wang, XJ Key, J Kwok, R Zhang, JL AF Wang, Xuanji Key, Jeffrey Kwok, Ron Zhang, Jinlun TI Comparison of Arctic Sea Ice Thickness from Satellites, Aircraft, and PIOMAS Data SO REMOTE SENSING LA English DT Article DE sea ice thickness; Arctic; remote sensing; satellite; ICESat; CryoSat-2; SMOS; IceBridge; PIOMAS; APP-x ID SNOW DEPTH; OPERATION ICEBRIDGE; MODEL; RETRIEVAL; FREEBOARD; ALGORITHM; CLOUD AB In this study, six Arctic sea ice thickness products are compared: the AVHRR Polar Pathfinder-extended (APP-x), ICESat, CryoSat-2, SMOS, NASA IceBridge aircraft flights, and the Pan-Arctic Ice Ocean Modeling and Assimilation System (PIOMAS). The satellite products are based on three different retrieval methods: an energy budget approach, measurements of ice freeboard, and the relationship between passive microwave brightness temperatures and thin ice thickness. Inter-comparisons are done for the periods of overlap from 2003 to 2013. Results show that ICESat sea ice is thicker than APP-x and PIOMAS overall, particularly along the north coast of Greenland and Canadian Archipelago. The relative differences of APP-x and PIOMAS with ICESat are -0.48 m and -0.31 m, respectively. APP-x underestimates thickness relative to CryoSat-2, with a mean difference of -0.19 m. The biases for APP-x, PIOMAS, and CryoSat-2 relative to IceBridge thicknesses are 0.18 m, 0.18 m, and 0.29 m. The mean difference between SMOS and CryoSat-2 for 0 similar to 1 m thick ice is 0.13 m in March and -0.24 m in October. All satellite-retrieved ice thickness products and PIOMAS overestimate the thickness of thin ice (1 m or less) compared to IceBridge for which SMOS has the smallest bias (0.26 m). The spatial correlation between the datasets indicates that APP-x and PIOMAS are the most similar, followed by APP-x and CryoSat-2. C1 [Wang, Xuanji] UW Madison, CIMSS, SSEC, Madison, WI 53706 USA. [Key, Jeffrey] NOAA NESDIS, Ctr Satellite Applicat & Res, Madison, WI 53706 USA. [Kwok, Ron] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Zhang, Jinlun] Univ Washington, Appl Phys Lab, Polar Sci Ctr, 1013 NE 40th St, Seattle, WA 98105 USA. RP Wang, XJ (reprint author), UW Madison, CIMSS, SSEC, Madison, WI 53706 USA. EM xuanjiw@ssec.wisc.edu; jeff.key@noaa.gov; ronald.kwok@jpl.nasa.gov; zhang@apl.washington.edu OI Wang, Xuanji/0000-0002-5893-758X; Key, Jeffrey/0000-0001-6109-3050 FU JPSS Program Office; GOES-R Program Office; National Science Foundation [ARC-1023371]; NASA Cryosphere Program [NNX15AG68G] FX This work was supported by the JPSS Program Office, the GOES-R Program Office, the National Science Foundation (ARC-1023371), and the NASA Cryosphere Program (NNX15AG68G). We thank the Alfred Wegener Institute/Helmholtz Centre for Polar and Marine Research and the European Space Agency for making the Cryosat-2 ice thickness product available to the scientific community, the University of Hamburg for the SMOS ice thicknesses, and the National Snow and Ice Data Center and NASA for the IceBridge data. The views, opinions, and findings contained in this report are those of the author(s) and should not be construed as an official National Oceanic and Atmospheric Administration or U.S. Government position, policy, or decision. NR 31 TC 2 Z9 2 U1 6 U2 6 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD SEP PY 2016 VL 8 IS 9 AR 713 DI 10.3390/rs8090713 PG 17 WC Remote Sensing SC Remote Sensing GA DY9XB UT WOS:000385488000023 ER PT J AU Meier, MM Matthia, D Forkert, T Wirtz, M Scheibinger, M Hubel, R Mertens, CJ AF Meier, Matthias M. Matthiae, Daniel Forkert, Tomas Wirtz, Michael Scheibinger, Markus Huebel, Robert Mertens, Christopher J. TI RaD-X: Complementary measurements of dose rates at aviation altitudes SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID GALACTIC COSMIC-RAYS; CALIBRATION; MODEL; DOSIMETERS AB The RaD-X stratospheric balloon flight organized by the National Aeronautics and Space Administration was launched from Fort Sumner on 25 September 2015 and carried several instruments to measure the radiation field in the upper atmosphere at the average vertical cutoff rigidity R-c of 4.1 GV. The German Aerospace Center (Deutsches Zentrum fur Luft-und Raumfahrt) in cooperation with Lufthansa German Airlines supported this campaign with an independent measuring flight at the altitudes of civil aviation on a round trip from Germany to Japan. The goal was to measure dose rates under similar space weather conditions over an area on the Northern Hemisphere opposite to the RaD-X flight. Dose rates were measured in the target areas, i.e., around vertical cutoff rigidity Rc of 4.1 GV, at two flight altitudes for about 1 h at each position with acceptable counting statistics. The analysis of the space weather situation during the flights shows that measuring data were acquired under stable and moderate space weather conditions with a virtually undisturbed magnetosphere. The measured rates of absorbed dose in silicon and ambient dose equivalent complement the data recorded during the balloon flight. The combined measurements provide a set of experimental data suitable for validating and improving numerical models for the calculation of radiation exposure at aviation altitudes. C1 [Meier, Matthias M.; Matthiae, Daniel; Forkert, Tomas; Wirtz, Michael] Inst Aerosp Med, German Aerosp Ctr, Cologne, Germany. [Scheibinger, Markus; Huebel, Robert] Lufthansa German Airlines, Lufthansa Basis, Frankfurt, Germany. [Mertens, Christopher J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Meier, MM (reprint author), Inst Aerosp Med, German Aerosp Ctr, Cologne, Germany. EM Matthias.Meier@dlr.de OI Matthia, Daniel/0000-0003-1507-0143 FU Lufthansa German Airlines FX We would like to especially express our gratitude to Lufthansa German Airlines for their support during the preparation and performance of the measuring flights. Furthermore, we would like to thank the Sodankyla Geophysical Observatory and the website team (http://cosmicrays.oulu.fi) for providing the Oulu neutron monitor data. The flight data are available from the German Aerospace Center upon request. NR 19 TC 3 Z9 3 U1 2 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD SEP PY 2016 VL 14 IS 9 BP 689 EP 694 DI 10.1002/2016SW001418 PG 6 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA EC0PE UT WOS:000387802300006 ER PT J AU Kannawadi, A Shapiro, CA Mandelbaum, R Hirata, CM Kruk, JW Rhodes, JD AF Kannawadi, Arun Shapiro, Charles A. Mandelbaum, Rachel Hirata, Christopher M. Kruk, Jeffrey W. Rhodes, Jason D. TI The Impact of Interpixel Capacitance in CMOS Detectors on PSF Shapes and Implications for WFIRST SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE instrumentation: detectors; instrumentation: high angular resolution ID DARK-MATTER HALOES; COSMOLOGICAL PARAMETER CONSTRAINTS; IMAGE COMBINATION; LARGE SCALES; SDSS DR7; WEAK; CFHTLENS; CONNECTION; EVOLUTION; GALAXIES AB Unlike optical CCDs, near-infrared detectors, which are based on CMOS hybrid readout technology, typically suffer from electrical crosstalk between the pixels. The interpixel capacitance (IPC) responsible for the crosstalk affects the point-spread function (PSF) of the telescope, increasing the size and modifying the shape of all objects in the images while correlating the Poisson noise. Upcoming weak lensing surveys that use these detectors, such as WFIRST, place stringent requirements on the PSF size and shape (and the level at which these are known), which in turn must be translated into requirements on IPC. To facilitate this process, we present a first study of the effect of IPC on WFIRST PSF sizes and shapes. Realistic PSFs are forward-simulated from physical principles for each WFIRST bandpass. We explore how the PSF size and shape depends on the range of IPC coupling with pixels that are connected along an edge or corner; for the expected level of IPC in WFIRST, IPC increases the PSF sizes by similar to 5%. We present a linear fitting formula that describes the uncertainty in the PSF size or shape due to uncertainty in the IPC, which could arise for example due to unknown time evolution of IPC as the detectors age or due to spatial variation of IPC across the detector. We also study of the effect of a small anisotropy in the IPC, which further modifies the PSF shapes. Our results are a first, critical step in determining the hardware and characterization requirements for the detectors used in the WFIRST survey. C1 [Kannawadi, Arun; Mandelbaum, Rachel] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Shapiro, Charles A.; Rhodes, Jason D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Hirata, Christopher M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, 191 West Woodruff Lane, Columbus, OH 43210 USA. [Kruk, Jeffrey W.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rhodes, Jason D.] CALTECH, Pasadena, CA 91125 USA. RP Kannawadi, A (reprint author), Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. EM arunkannawadi@cmu.edu RI Mandelbaum, Rachel/N-8955-2014 OI Mandelbaum, Rachel/0000-0003-2271-1527 FU WFIRST study office; US Department of Energy; Packard Foundation; Simons Foundation FX The authors thank Roger Smith, Bernard Rauscher, and Andres Plazas Malagon for many useful discussions and Mike Jarvis and Joshua Meyers for their inputs in developing the GalSim WFIRST module. We thank Edward Cheng of Conceptual Analytics for his comments in improving the manuscript and the referee, David Spergel, for correcting a few minor errors in the original version of the manuscript. This work was carried out in part at the Jet Propulsion Laboratory (JPL), a NASA center run by California Institute of Technology. The authors acknowledge funding from WFIRST study office. CMH is supported by the US Department of Energy, the Packard Foundation, and the Simons Foundation. NR 49 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD SEP PY 2016 VL 128 IS 967 AR 095001 DI 10.1088/1538-3873/128/967/095001 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EB1LK UT WOS:000387113200007 ER PT J AU Nguyen, HT Zemcov, M Battle, J Bock, JJ Hristov, V Korngut, P Meek, A AF Nguyen, Hien T. Zemcov, Michael Battle, John Bock, James J. Hristov, Viktor Korngut, Phillip Meek, Andrew TI Spatial and Temporal Stability of Airglow Measured in the Meinel Band Window at 1191.3 nm SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE atmospheric effects; site testing; techniques: imaging spectroscopy ID BACKGROUND-EXPERIMENT CIBER; SKY BRIGHTNESS; EMISSION; FLUCTUATIONS; SUPPRESSION; ATMOSPHERE; MODEL; LINES AB We report on the temporal and spatial fluctuations in the atmospheric brightness in the narrow band between Meinel emission lines at 1191.3 nm using a lambda/Delta lambda = 320 near-infrared instrument. We present the instrument design and implementation, followed by a detailed analysis of data taken over the course of a night from Table Mountain Observatory. At low airmasses, the absolute sky brightness at this wavelength is found to be 5330 +/- 30 nW m(-2) sr(-1), consistent with previous measurements of the inter-band airglow at these wavelengths. This amplitude is larger than simple models of the continuum component of the airglow emission at these wavelengths, confirming that an extra emissive or scattering component is required to explain the observations. We perform a detailed investigation of the noise properties of the data and find no evidence for a noise component associated with temporal instability in the inter-line continuum. This result demonstrates that in several hours of similar to 100 s integrations the noise performance of the instrument does not appear to significantly degrade from expectations, giving a proof of concept that near-infrared line intensity mapping may be feasible from ground-based sites. C1 [Nguyen, Hien T.; Zemcov, Michael; Bock, James J.; Korngut, Phillip] NASA, JPL, Pasadena, CA 91109 USA. [Nguyen, Hien T.; Zemcov, Michael; Battle, John; Bock, James J.; Hristov, Viktor; Korngut, Phillip; Meek, Andrew] CALTECH, Dept Phys Math & Astron, Pasadena, CA 91125 USA. RP Nguyen, HT (reprint author), NASA, JPL, Pasadena, CA 91109 USA.; Nguyen, HT (reprint author), CALTECH, Dept Phys Math & Astron, Pasadena, CA 91125 USA. EM htnguyen@jpl.nasa.gov FU JPL Research and Technology Development Fund; National Aeronautics and Space Administration; National Science Foundation FX The authors wish to thank Jaime Luna for his help designing the LAMP mechanical assembly, Heath Rhoades at JPL's Table Mountain Observatory for his assistance setting up the instrument and guidance using the 24 '' telescope, and the Gemini Observatory for making their sky model tables public. The development of LAMP was supported by the JPL Research and Technology Development Fund. This publication makes use of data products from the Two Micron All Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 26 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD SEP PY 2016 VL 128 IS 967 AR 094504 DI 10.1088/1538-3873/128/967/094504 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EB1LK UT WOS:000387113200006 ER PT J AU Stevenson, KB Lewis, NK Bean, JL Beichman, C Fraine, J Kilpatrick, BM Krick, JE Lothringer, JD Mandell, AM Valenti, JA Agol, E Angerhausen, D Barstow, JK Birkmann, SM Burrows, A Charbonneau, D Cowan, NB Crouzet, N Cubillos, PE Curry, SM Dalba, PA de Wit, J Deming, D Desert, JM Doyon, R Dragomir, D Ehrenreich, D Fortney, JJ Munoz, AG Gibson, NP Gizis, JE Greene, TP Harrington, J Heng, K Kataria, T Kempton, EMR Knutson, H Kreidberg, L Lafreniere, D Lagage, PO Line, MR Lopez-Morales, M Madhusudhan, N Morley, CV Rocchetto, M Schlawin, E Shkolnik, EL Shporer, A Sing, DK Todorov, KO Tucker, GS Wakeford, HR AF Stevenson, Kevin B. Lewis, Nikole K. Bean, Jacob L. Beichman, Charles Fraine, Jonathan Kilpatrick, Brian M. Krick, J. E. Lothringer, Joshua D. Mandell, Avi M. Valenti, Jeff A. Agol, Eric Angerhausen, Daniel Barstow, Joanna K. Birkmann, Stephan M. Burrows, Adam Charbonneau, David Cowan, Nicolas B. Crouzet, Nicolas Cubillos, Patricio E. Curry, S. M. Dalba, Paul A. de Wit, Julien Deming, Drake Desert, Jean-Michel Doyon, Rene Dragomir, Diana Ehrenreich, David Fortney, Jonathan J. Munoz, Antonio Garcia Gibson, Neale P. Gizis, John E. Greene, Thomas P. Harrington, Joseph Heng, Kevin Kataria, Tiffany Kempton, Eliza M. -R. Knutson, Heather Kreidberg, Laura Lafreniere, David Lagage, Pierre-Olivier Line, Michael R. Lopez-Morales, Mercedes Madhusudhan, Nikku Morley, Caroline V. Rocchetto, Marco Schlawin, Everett Shkolnik, Evgenya L. Shporer, Avi Sing, David K. Todorov, Kamen O. Tucker, Gregory S. Wakeford, Hannah R. TI Transiting Exoplanet Studies and Community Targets for JWST's Early Release Science Program SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE planets and satellites: atmospheres; planets and satellites: individual; telescopes ID WEBB-SPACE-TELESCOPE; FIELD CAMERA 3; HOT JUPITERS; MIDINFRARED INSTRUMENT; RESOLUTION SPECTROMETER; TRANSMISSION SPECTRUM; GIANT PLANET; KEPLER FIELD; HD 149026B; WASP-SOUTH AB The James Webb Space Telescope (JWST) will likely revolutionize transiting exoplanet atmospheric science, due to a combination of its capability for continuous, long duration observations and its larger collecting area, spectral coverage, and spectral resolution compared to existing space-based facilities. However, it is unclear precisely how well JWST will perform and which of its myriad instruments and observing modes will be best suited for transiting exoplanet studies. In this article, we describe a prefatory JWST Early Release Science (ERS) Cycle. 1 program that focuses on testing specific observing modes to quickly give the community the data and experience it needs to plan more efficient and successful transiting exoplanet characterization programs in later cycles. We propose a multi-pronged approach wherein one aspect of the program focuses on observing transits of a single target with all of the recommended observing modes to identify and understand potential systematics, compare transmission spectra at overlapping and neighboring wavelength regions, confirm throughputs, and determine overall performances. In our search for transiting exoplanets that are well suited to achieving these goals, we identify 12 objects (dubbed "community targets") that meet our defined criteria. Currently, the most favorable target is WASP-62b because of its large predicted signal size, relatively bright host star, and location in JWST's continuous viewing zone. Since most of the community targets do not have well-characterized atmospheres, we recommend initiating preparatory observing programs to determine the presence of obscuring clouds/hazes within their atmospheres. Measurable spectroscopic features are needed to establish the optimal resolution and wavelength regions for exoplanet characterization. Other initiatives from our proposed ERS program include testing the instrument brightness limits and performing phase-curve observations. The latter are a unique challenge compared to transit observations because of their significantly longer durations. Using only a single mode, we propose to observe a full-orbit phase curve of one of the previously characterized, short-orbital-period planets to evaluate the facility-level aspects of long, uninterrupted time-series observations. C1 [Stevenson, Kevin B.; Bean, Jacob L.; Dragomir, Diana; Kreidberg, Laura] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Lewis, Nikole K.; Valenti, Jeff A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Beichman, Charles] CALTECH, Jet Prop Lab, NASA Exoplanet Sci Inst, Pasadena, CA USA. [Fraine, Jonathan; Schlawin, Everett] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Kilpatrick, Brian M.; Tucker, Gregory S.] Brown Univ, Dept Phys, Providence, RI 02912 USA. [Krick, J. E.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91106 USA. [Lothringer, Joshua D.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Mandell, Avi M.] NASA Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Agol, Eric] Univ Washington, Box 351580, Seattle, WA 98195 USA. [Angerhausen, Daniel; Wakeford, Hannah R.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Barstow, Joanna K.] Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. [Birkmann, Stephan M.] European Space Agcy, Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. [Charbonneau, David; Lopez-Morales, Mercedes] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Cowan, Nicolas B.] McGill Space Inst, 3550 Rue Univ, Montreal, PQ H3A 1A1, Canada. [Crouzet, Nicolas] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON, Canada. [Cubillos, Patricio E.] Austrian Acad Sci, Space Res Inst, Schmiedlstr 6, A-8042 Graz, Austria. [Curry, S. M.] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. [Dalba, Paul A.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [de Wit, Julien] MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Desert, Jean-Michel] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Doyon, Rene; Lafreniere, David] Univ Montreal, Dept Phys, Inst Rech Exoplanetes, CP 6128,Succ Ctr Vile, Montreal, PQ H3C 3J7, Canada. [Ehrenreich, David] Observ Univ Geneve, 51 Chemin Maillettes, CH-1290 Versoix, Switzerland. [Fortney, Jonathan J.; Morley, Caroline V.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Munoz, Antonio Garcia] Tech Univ Berlin, Zentrum Astron & Astrophys, D-10623 Berlin, Germany. [Gibson, Neale P.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Gizis, John E.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Greene, Thomas P.; Line, Michael R.] NASA Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Harrington, Joseph] Univ Cent Florida, Dept Phys, Planetary Sci Grp, Orlando, FL 32816 USA. [Heng, Kevin] Univ Bern, Ctr Space & Habitabil, Sidlerstr 5, CH-3012 Bern, Switzerland. [Kataria, Tiffany; Sing, David K.] Univ Exeter, Sch Phys, Astrophys Grp, Stocker Rd, Exeter EX4 4QL, Devon, England. [Kempton, Eliza M. -R.] Grinnell Coll, Dept Phys, Noyce Sci Bldg, Grinnell, IA 50112 USA. [Knutson, Heather] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Lagage, Pierre-Olivier] Paris Saclay Univ, Irfu AIM, CEA Saclay, F-91191 Gif Sur Yvette, France. [Madhusudhan, Nikku] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Rocchetto, Marco] UCL, Dept Phys & Astron, London NW1 2PS, England. [Shkolnik, Evgenya L.] Arizona State Univ, Sch Earth & Space Explorat, 781 S Terrace Rd, Tempe, AZ 85281 USA. [Shporer, Avi] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Todorov, Kamen O.] ETH, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. RP Stevenson, KB (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM kbs@uchicago.edu RI Harrington, Joseph/E-6250-2011; OI Gibson, Neale/0000-0002-9308-2353 FU Sagan Fellowship Program - NASA FX K.B.S. recognizes support from the Sagan Fellowship Program, supported by NASA and administered by the NASA Exoplanet Science Institute (NExScI). NR 50 TC 4 Z9 4 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD SEP PY 2016 VL 128 IS 967 AR 094401 DI 10.1088/1538-3873/128/967/094401 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EB1LK UT WOS:000387113200002 ER PT J AU Brown, PJ Yang, Y Cooke, J Olaes, M Quimby, RM Baade, D Gehrels, N Hoeflich, P Maund, J Mould, J Wang, LF Wheeler, JC AF Brown, Peter J. Yang, Yi Cooke, Jeff Olaes, Melanie Quimby, Robert M. Baade, Dietrich Gehrels, Neil Hoeflich, Peter Maund, Justyn Mould, Jeremy Wang, Lifan Wheeler, J. Craig TI ASASSN-15LH: A SUPERLUMINOUS ULTRAVIOLET REBRIGHTENING OBSERVED BY SWIFT AND HUBBLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE polarization; supernovae: individual (ASASSN-15lh, SN2015L); ultraviolet: general; X-rays: general ID X-RAY OBSERVATIONS; PAIR-INSTABILITY SUPERNOVAE; MASSIVE BLACK-HOLE; CORE-COLLAPSE SUPERNOVAE; TIDAL DISRUPTION; SPACE-TELESCOPE; IIN SUPERNOVA; LUMINOUS SUPERNOVAE; LINEAR-POLARIZATION; MAGNETAR BIRTH AB We present and discuss ultraviolet and optical photometry from the Ultraviolet/Optical Telescope, X-ray limits from the X-Ray Telescope on Swift, and imaging polarimetry and ultraviolet/optical spectroscopy with the Hubble Space Telescope, all from observations of ASASSN-15lh. It has been classified as a hydrogen-poor superluminous supernova (SLSN I), making it more luminous than any other supernova observed. ASASSN-15lh is not detected in the X-rays in individual or co-added observations. From the polarimetry we determine that the explosion was only mildly asymmetric. We find the flux of ASASSN-15lh to increase strongly into the ultraviolet, with an ultraviolet luminosity 100 times greater than the hydrogen-rich, ultraviolet-bright SLSN II SN 2008es. We find that objects as bright as ASASSN-15lh are easily detectable beyond redshifts of similar to 4 with the single-visit depths planned for the Large Synoptic Survey Telescope. Deep near-infrared surveys could detect such objects past a redshift of similar to 20, enabling a probe of the earliest star formation. A late rebrightening-most prominent at shorter wavelengths -is seen about two months after the peak brightness, which is itself as bright as an SLSN. The ultraviolet spectra during the rebrightening are dominated by the continuum without the broad absorption or emission lines seen in SLSNe or tidal disruption events (TDEs) and the early optical spectra of ASASSN-15lh. Our spectra show no strong hydrogen emission, showing only Lya absorption near the redshift previously found by optical absorption lines of the presumed host. The properties of ASASSN-15lh are extreme when compared to either SLSNe or TDEs. C1 [Brown, Peter J.; Yang, Yi; Wang, Lifan] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, 4242 TAMU, College Stn, TX 77843 USA. [Cooke, Jeff; Mould, Jeremy] Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Olaes, Melanie; Quimby, Robert M.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Quimby, Robert M.] Univ Tokyo, UTIAS, Kavli IPMU WPI, Kashiwa, Chiba 2778583, Japan. [Baade, Dietrich] Southern Hemisphere ESO, European Org Astron Res, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hoeflich, Peter] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Maund, Justyn] Dept Phys & Astron, F39 Hicks Bldg,Hounsfield Rd, Sheffield S3 7RH, S Yorkshire, England. [Wheeler, J. Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Brown, PJ (reprint author), Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, 4242 TAMU, College Stn, TX 77843 USA. OI Maund, Justyn/0000-0003-0733-7215 FU NASA from Space Telescope Science Institute [NASA 5-26555, HST-GO-14450.001-A]; NASA [NAS5-26555]; STSCi by STScI [HST-AR-13276.02-A]; Swift GI program [NNX15AR41G]; NASA's Astrophysics Data Analysis Program [NNX13AF35G]; [14348]; [14450] FX We thank the HST director for approving the DDT requests. We thank Matt McMaster and Dean Hines for helping with the calibration of the ACS/WFC polarizers. This work is based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NASA 5-26555. These observations are associated with programs #14348 and #14450. Support for this work was provided by NASA through grant number HST-GO-14450.001-A from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS5-26555. J.C.W. was supported by STSCi by STScI grant HST-AR-13276.02-A. This work is supported by the Swift GI program through grant NNX15AR41G. The Swift Optical/ Ultraviolet Supernova Archive (SOUSA) is supported by NASA's Astrophysics Data Analysis Program through grant NNX13AF35G. This work made use of public data in the Swift data archive from observations requested by several others (PIs: Dong, Godoy, Holoien, Leloudas, Jonker). This research has made use of NASA's Astrophysics Data System Bibliographic Services. NR 101 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2016 VL 828 IS 1 AR 3 DI 10.3847/0004-637X/828/1/3 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA8OE UT WOS:000386894900003 ER PT J AU Cordiner, MA Boogert, ACA Charnley, SB Justtanont, K Cox, NLJ Smith, RG Tielens, AGGM Wirstrom, ES Milam, SN Keane, JV AF Cordiner, M. A. Boogert, A. C. A. Charnley, S. B. Justtanont, K. Cox, N. L. J. Smith, R. G. Tielens, A. G. G. M. Wirstrom, E. S. Milam, S. N. Keane, J. V. TI ON THE NATURE OF THE ENIGMATIC OBJECT IRAS 19312+1950: A RARE PHASE OF MASSIVE STAR FORMATION? SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: molecules; masers; stars: AGB and post-AGB; stars: formation; stars: protostars; stars: winds, outflows ID YOUNG STELLAR OBJECTS; POSTASYMPTOTIC GIANT BRANCH; WIDE-FIELD CAMERA; HI-GAL SURVEY; FORMING REGIONS; HERSCHEL OBSERVATIONS; MOLECULAR CLOUDS; MASER SURVEY; H2O MASERS; CLASS-I AB IRAS 19312+1950 is a peculiar object that has eluded firm characterization since its discovery, with combined maser properties similar to an evolved star and a young stellar object (YSO). To help determine its true nature, we obtained infrared spectra of IRAS 19312+1950 in the range 5-550 mu m using the Herschel and Spitzer space observatories. The Herschel PACS maps exhibit a compact, slightly asymmetric continuum source at 170 mu m, indicative of a large, dusty circumstellar envelope. The far-IR CO emission line spectrum reveals two gas temperature components: approximate to 0.22 Me of material at 280 +/- 18 K, and approximate to 1.6 M-circle dot of material at 157 +/- 3 K. The O I 63 mu m line is detected on-source but no significant emission from atomic ions was found. The HIFI observations display shocked, high-velocity gas with outflow speeds up to 90 km s(-1) along the line of sight. From Spitzer spectroscopy, we identify ice absorption bands due to H2O at 5.8 mu m and CO2 at 15 mu m. The spectral energy distribution is consistent with a massive, luminous (similar to 2 x 10(4) Le) central source surrounded by a dense, warm circumstellar disk and envelope of total mass similar to 500-700 Me, with large bipolar outflow cavities. The combination of distinctive far-IR spectral features suggest that IRAS 19312+1950 should be classified as an accreting, highmass YSO rather than an evolved star. In light of this reclassification, IRAS 19312+1950 becomes only the fifth high-mass protostar known to exhibit SiO maser activity, and demonstrates that 18 cm OH maser line ratios may not be reliable observational discriminators between evolved stars and YSOs. C1 [Cordiner, M. A.; Charnley, S. B.; Milam, S. N.] NASA, Astrochem Lab, Goddard Space Flight Ctr, Code 691,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. [Cordiner, M. A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Boogert, A. C. A.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, NASA, Ames Res Ctr, MS 232-11, Moffett Field, CA 94035 USA. [Justtanont, K.; Wirstrom, E. S.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden. [Cox, N. L. J.] Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D,Bus 2401, B-3001 Leuven, Belgium. [Cox, N. L. J.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse, France. [Smith, R. G.] Univ New South Wales, Australian Def Force Acad, Sch Phys Environm & Math Sci, Canberra, ACT 2600, Australia. [Tielens, A. G. G. M.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Keane, J. V.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Cordiner, MA (reprint author), NASA, Astrochem Lab, Goddard Space Flight Ctr, Code 691,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.; Cordiner, MA (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. EM martin.cordiner@nasa.gov OI Wirstrom, Eva/0000-0002-0656-876X; /0000-0003-1689-9201 FU NASA through JPL/Caltech; NASA through NASA's Origins of Solar Systems program FX Support for this work was provided by NASA through an award issued by JPL/Caltech and through NASA's Origins of Solar Systems program. We gratefully acknowledge the work of Thomas Robitaille for providing and supporting the Hyperion radiative transfer code. NR 95 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2016 VL 828 IS 1 AR 51 DI 10.3847/0004-637X/828/1/51 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA8OE UT WOS:000386894900051 ER PT J AU D'Angelo, G Bodenheimer, P AF D'Angelo, Gennaro Bodenheimer, Peter TI IN SITU AND EX SITU FORMATION MODELS OF KEPLER 11 PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planet-disk interactions; planetary systems; planets and satellites: formation; planets and satellites: individual (Kepler 11); planets and satellites: interiors; protoplanetary disks ID MEAN-MOTION RESONANCES; EQUATION-OF-STATE; X-RAY-DIFFRACTION; DISK-SATELLITE INTERACTION; ISOTHERMAL GASEOUS DISK; TERRESTRIAL MAGMA OCEAN; EARTHS CORE CONDITIONS; LOW-MASS STARS; SUPER-EARTHS; GIANT PLANETS AB We present formation simulations of the six Kepler 11 planets. Models assume either in situ or ex situ assembly, the latter with migration, and are evolved to the estimated age of the system, approximate to 8 Gyr. Models combine detailed calculations of both the gaseous envelope and the condensed core structures, including accretion of gas and solids, of the disk's viscous and thermal evolution, including photo-evaporation and disk-planet interactions, and of the planet's evaporative mass loss after disk dispersal. Planet-planet interactions are neglected. Both sets of simulations successfully reproduce measured radii, masses, and orbital distances of the planets, except for the radius of Kepler 11b, which loses its entire gaseous envelope shortly after formation. Gaseous (H+ He) envelopes account for less than or similar to 18% of the planet masses, and between approximate to 35 and approximate to 60% of the planet radii. In situ models predict a very massive inner disk, whose solid surface density (sigma(Z)) varies from over 10(4) to approximate to 10(3) g cm(-2) at stellocentric distances 0.1 less than or similar to r less than or similar to 0.5 au. Initial gas densities would be in excess of 10(5) g cm(-2) if solids formed locally. Given the high disk temperatures (greater than or similar to 1000 K), planetary interiors can only be composed of metals and highly refractory materials. Sequestration of hydrogen by the core and subsequent outgassing is required to account for the observed radius of Kepler 11b. Ex situ models predict a relatively low-mass disk, whose initial sigma(Z) varies from approximate to 10 to approximate to 5 g cm(-2) at 0.5 less than or similar to r less than or similar to 7 au and whose initial gas density ranges from approximate to 10(3) to approximate to 100 g cm(-2). All planetary interiors are expected to be rich in H2O, as core assembly mostly occurs exterior to the ice condensation front. Kepler 11b is expected to have a steam atmosphere, and H2O is likely mixed with H+He in the envelopes of the other planets. Results indicate that Kepler. 11g may not be more massive than Kepler. 11e. C1 [D'Angelo, Gennaro] NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA. [D'Angelo, Gennaro] SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA. [Bodenheimer, Peter] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. RP D'Angelo, G (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA.; D'Angelo, G (reprint author), SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA. EM gennaro.dangelo@nasa.gov; peter@ucolick.org OI D'Angelo, Gennaro/0000-0002-2064-0801; Bodenheimer, Peter/0000-0001-6093-3097 FU NASA Outer Planets Research Program [202844.02.02.01.75]; NASA Origins of Solar Systems Program [NNX14AG92G]; NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center FX We thank Uma Gorti for numerous helpful discussions and for her precious guidance during the implementation of the disk photo-evaporation module. We are grateful to an anonymous referee, whose insightful comments helped improve several parts of this paper. G.D. thanks the Los Alamos National Laboratory for its hospitality. G.D. acknowledges support from NASA Outer Planets Research Program grant 202844.02.02.01.75 and from NASA Origins of Solar Systems Program grant NNX14AG92G. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. NR 186 TC 1 Z9 1 U1 3 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2016 VL 828 IS 1 AR 33 DI 10.3847/0004-637X/828/1/33 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA8OE UT WOS:000386894900033 ER PT J AU Deller, AT Vigeland, SJ Kaplan, DL Goss, WM Brisken, WF Chatterjee, S Cordes, JM Janssen, GH Lazio, TJW Petrov, L Stappers, BW Lyne, A AF Deller, A. T. Vigeland, S. J. Kaplan, D. L. Goss, W. M. Brisken, W. F. Chatterjee, S. Cordes, J. M. Janssen, G. H. Lazio, T. J. W. Petrov, L. Stappers, B. W. Lyne, A. TI MICROARCSECOND VLBI PULSAR ASTROMETRY WITH PSR pi. I. TWO BINARY MILLISECOND PULSARS WITH WHITE DWARF COMPANIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; pulsars: individual (PSR J1022+1001, J2145-0750); stars: neutron; techniques: high angular resolution; white dwarfs ID BASE-LINE ARRAY; DATA RELEASE; SPECTROSCOPIC ANALYSIS; SOFTWARE CORRELATOR; PROPER MOTION; PARALLAXES; SKY; DISTANCE; MASS; INTERFEROMETRY AB Model-independent distance constraints to binary millisecond pulsars (MSPs) are of great value to both the timing observations of the radio pulsars and multiwavelength observations of their companion stars. Astrometry using very long baseline interferometry (VLBI) can be employed to provide these model-independent distances with very high precision via the detection of annual geometric parallax. Using the Very Long Baseline Array, we have observed two binary MSPs, PSR J1022+1001 and J2145-0750, over a two-year period and measured their distances to be 700(10)(+14) pc and 613(-14)(+16) pc respectively. We use the well-calibrated distance in conjunction with revised analysis of optical photometry to tightly constrain the nature of their massive (M similar to 0.85 M-circle dot) white dwarf companions. Finally, we show that several measurements of the parallax and proper motion of PSR J1022 + 1001 and PSR J2145-0750 obtained by pulsar timing array projects are incorrect, differing from the more precise VLBI values by up to 5 sigma. We investigate possible causes for the discrepancy, and find that imperfect modeling of the solar wind is a likely candidate for the errors in the timing model given the low ecliptic latitude of these two pulsars. C1 [Deller, A. T.; Janssen, G. H.] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. [Vigeland, S. J.; Kaplan, D. L.] Univ Wisconsin Milwaukee, POB 413, Milwaukee, WI 53201 USA. [Goss, W. M.; Brisken, W. F.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Chatterjee, S.; Cordes, J. M.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Petrov, L.] Astrogeo Ctr, Falls Church, VA 22043 USA. [Stappers, B. W.; Lyne, A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. RP Deller, AT (reprint author), Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. OI Deller, Adam/0000-0001-9434-3837 FU NWO Veni Fellowship; NANOGrav project through National Science Foundation (NSF) PIRE program [0968296]; NSF Physics Frontiers Center [1430284]; National Aeronautics and Space Administration; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science FX A.T.D. was supported by an NWO Veni Fellowship. D.L.K. an d S.J.V. receive support from the NANOGrav project through National Science Foundation (NSF) PIRE program award number 0968296 and NSF Physics Frontiers Center award number 1430284. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The authors thank David Nice and Pierre Bergeron for useful discussions. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Pulsar research at the Jodrell Bank Centre for Astrophysics and the observations using the Lovell Telescope are supported by a consolidated grant from the STFC in the UK. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. NR 55 TC 2 Z9 2 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2016 VL 828 IS 1 AR 8 DI 10.3847/0004-637X/828/1/8 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA8OE UT WOS:000386894900008 ER PT J AU Furst, F Grinberg, V Tomsick, JA Bachetti, M Boggs, SE Brightman, M Christensen, FE Craig, WW Gandhi, P Grefenstette, B Hailey, CJ Harrison, FA Madsen, KK Parker, ML Pottschmidt, K Stern, D Walton, DJ Wilms, J Zhang, WW AF Furst, F. Grinberg, V. Tomsick, J. A. Bachetti, M. Boggs, S. E. Brightman, M. Christensen, F. E. Craig, W. W. Gandhi, P. Grefenstette, B. Hailey, C. J. Harrison, F. A. Madsen, K. K. Parker, M. L. Pottschmidt, K. Stern, D. Walton, D. J. Wilms, J. Zhang, W. W. TI SPECTRO-TIMING STUDY OF GX 339-4 IN A HARD INTERMEDIATE STATE SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars: black holes; X-rays: binaries; X-rays: individual (GX 339-4) ID QUASI-PERIODIC OSCILLATIONS; X-RAY BINARIES; BLACK-HOLE CANDIDATES; ADVECTION-DOMINATED ACCRETION; RELATIVISTIC PRECESSION MODEL; LENS-THIRRING PRECESSION; NOVA XTE J1550-564; LOW/HARD STATE; CYGNUS X-1; FREQUENCY CORRELATION AB We present an analysis of Nuclear Spectroscopic Telescope Array. observations of a hard intermediate state of the transient. black hole GX 339-4 taken in 2015 January. With. the source softening significantly over the course of the 1.3 day long observation we split the data into 21 sub-sets and find that the spectrum of all of them can be well described by a power-law continuum with an additional relativistically blurred reflection component. The photon index increases from similar to 1.69 to similar to 1.77 over the course of the observation. The accretion disk is truncated at around nine gravitational radii in all spectra. We also perform timing analysis on the same 21 individual data sets, and find a strong type-C quasi-periodic oscillation (QPO), which increases. in frequency from similar to 0.68 to similar to 1.05 Hz with time. The frequency change is well correlated with the softening of the spectrum. We discuss possible scenarios for the production of the QPO and calculate predicted inner radii in the relativistic precession model as well as the global disk mode oscillations model. We find discrepancies with respect to the observed values in both models unless we allow for a black hole mass of similar to 100 M-circle dot, which is highly unlikely. We discuss possible systematic uncertainties, in particular with the measurement of the inner accretion disk radius in the relativistic reflection model. We conclude that the combination of observed QPO frequencies and inner accretion disk radii, as obtained from spectral fitting,. is difficult to reconcile with current models. C1 [Furst, F.; Brightman, M.; Grefenstette, B.; Harrison, F. A.; Madsen, K. K.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Grinberg, V.] MIT, Kavli Inst Astrophys, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Tomsick, J. A.; Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Bachetti, M.] INAF, Osservatorio Astron Cagliari, I-09047 Selargius, CA, Italy. [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Gandhi, P.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Parker, M. L.] Inst Astron, Cambridge CB3 0HA, England. [Pottschmidt, K.] UMBC, CRESST, Dept Phys, Baltimore, MD 21250 USA. [Pottschmidt, K.] UMBC, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Pottschmidt, K.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Stern, D.; Walton, D. J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & ECAP, D-96049 Bamberg, Germany. RP Furst, F (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RI Wilms, Joern/C-8116-2013 OI Wilms, Joern/0000-0003-2065-5410 FU NASA [NNG08FD60C, NAS8-03060]; National Aeronautics and Space Administration; NASA through Smithsonian Astrophysical Observatory (SAO) [SV3-73016] FX We thank the anonymous referee for the constructive and helpful comments. We thank the NuSTAR schedulers and SOC, in particular Karl Forster, for making this observation possible. We thank Javier Garcia and Thomas Dauser for helpful discussions about the reflection models. 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. Support for this work was provided by NASA through the Smithsonian Astrophysical Observatory (SAO) contract SV3-73016 to MIT for Support of the Chandra X-ray Center (CXC) and Science Instruments; CXC is operated by SAO for and on behalf of NASA under contract NAS8-03060. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has made use of a collection of ISIS functions (ISISscripts) provided by ECAP/Remeis observatory and MIT (http://www.sternwarte.uni-erlangen.de/isis/). We would like to thank John E. Davis for the slxfig module, which was used to produce all figures in this work. This research has made use of MAXI data provided by RIKEN, JAXA and the MAXI team. NR 69 TC 3 Z9 3 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2016 VL 828 IS 1 AR 34 DI 10.3847/0004-637X/828/1/34 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA8OE UT WOS:000386894900034 ER PT J AU Hamren, K Beaton, RL Guhathakurta, P Gilbert, KM Tollerud, EJ Boyer, ML Rockosi, CM Smith, GH Majewski, SR Howley, K AF Hamren, Katherine Beaton, Rachael L. Guhathakurta, Puragra Gilbert, Karoline M. Tollerud, Erik J. Boyer, Martha L. Rockosi, Constance M. Smith, Graeme H. Majewski, Steven R. Howley, Kirsten TI CARBON STARS IN THE SATELLITES AND HALO OF M31 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M31); stars: AGB and post-AGB; stars: carbon ID ASYMPTOTIC GIANT BRANCH; DIGITAL-SKY-SURVEY; LOCAL GROUP GALAXIES; DWARF SPHEROIDAL GALAXIES; SPITZER-SPACE-TELESCOPE; SURVEY STELLAR SPECTRA; LARGE-MAGELLANIC-CLOUD; AGB STARS; SPLASH SURVEY; METAL-POOR AB We spectroscopically identify a sample of carbon stars in the satellites and halo of M31 using moderate-resolution optical spectroscopy from the Spectroscopic and Photometric Landscape of Andromeda's Stellar Halo survey. We present the photometric properties of our sample of 41 stars, including their brightness with respect to the tip of the red giant branch (TRGB) and their distributions in various color-color spaces. This analysis reveals a bluer population of carbon stars fainter than the TRGB and a redder population of carbon stars brighter than the TRGB. We then apply principal component analysis to determine the sample's eigenspectra and eigencoefficients. Correlating the eigencoefficients with various observable properties reveals the spectral features that trace effective temperature and metallicity. Putting the spectroscopic and photometric information together, we find the carbon stars in the satellites and halo of M31 to be minimally impacted by dust and internal dynamics. We also find that while there is evidence to suggest that the sub-TRGB stars are extrinsic in origin, it is also possible that they are are particularly faint members of the asymptotic giant branch. C1 [Hamren, Katherine; Guhathakurta, Puragra; Rockosi, Constance M.; Smith, Graeme H.] Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA. [Beaton, Rachael L.] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA. [Gilbert, Karoline M.; Tollerud, Erik J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Gilbert, Karoline M.] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA. [Boyer, Martha L.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. [Majewski, Steven R.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Howley, Kirsten] Lawrence Livermore Natl Lab, POB 808, Livermore, CA 94551 USA. RP Hamren, K (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA. EM khamren@ucolick.org OI Guhathakurta, Puragra/0000-0001-8867-4234 FU NSF [AST-1010039, AST-1412648, AST-1413269]; NASA [HST-GO-12055]; NSF Graduate Research Fellowship; Giacconi Fellowship FX The authors would like to thank Bernhard Aringer and Leo Girardi for helpful conversations and an early look at the 2016 cool star models. We would also like to thank Marla Geha, James Bullock, and Jason Kalirai for their work on the SPLASH survey over the years. and their willingness to provide data for this paper. P.G. and K.H. acknowledge NSF grants AST-1010039 and AST-1412648 and NASA grant HST-GO-12055. R.L.B. and S.R.M. thank NSF grant AST-1413269. K. H. was supported by an NSF Graduate Research Fellowship, and E.J.T. was supported by a Giacconi Fellowship. We appreciate the very significant cultural role and reverence that the summit of Mauna Kea has always held within the indigenous Hawaiian community. We are most grateful to have had the opportunity to conduct observations from this mountain. NR 100 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2016 VL 828 IS 1 AR 15 DI 10.3847/0004-637X/828/1/15 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA8OE UT WOS:000386894900015 ER PT J AU Han, C Udalski, A Gould, A Zhu, W Street, RA Yee, JC Beichman, C Bryden, C Novati, SC Carey, S Fausnaugh, M Gaudi, BS Henderson, CB Shvartzvald, Y Wibking, B Szymanski, MK Soszynski, I Skowron, J Mroz, P Poleski, R Pietrukowicz, P Kozlowski, S Ulaczyk, K Wyrzykowski, L Pawlak, M Tsapras, Y Hundertmark, M Bachelet, E Dominik, M Bramich, DM Cassan, A Jaimes, RF Horne, K Ranc, C Schmidt, R Snodgrass, C Wambsganss, J Steele, IA Menzies, J Mao, S Bozza, V Jorgensen, UG Alsubai, KA Ciceri, S D'Ago, G Haugbolle, T Hessman, FV Hinse, TC Juncher, D Korhonen, H Mancini, L Popovas, A Rabus, M Rahvar, S Scarpetta, G Skottfelt, J Southworth, J Starkey, D Surdej, J Wertz, O Zarucki, M Pogge, RW DePpoy, DL AF Han, C. Udalski, A. Gould, A. Zhu, Wei Street, R. A. Yee, J. C. Beichman, C. Bryden, C. Novati, S. Calchi Carey, S. Fausnaugh, M. Gaudi, B. S. Henderson, Calen B. Shvartzvald, Y. Wibking, B. Szymanski, M. K. Soszynski, I. Skowron, J. Mroz, P. Poleski, R. Pietrukowicz, P. Kozlowski, S. Ulaczyk, K. Wyrzykowski, L. Pawlak, M. Tsapras, Y. Hundertmark, M. Bachelet, E. Dominik, M. Bramich, D. M. Cassan, A. Jaimes, R. Figuera Horne, K. Ranc, C. Schmidt, R. Snodgrass, C. Wambsganss, J. Steele, I. A. Menzies, J. Mao, S. Bozza, V. Jorgensen, U. G. Alsubai, K. A. Ciceri, S. D'Ago, G. Haugbolle, T. Hessman, F. V. Hinse, T. C. Juncher, D. Korhonen, H. Mancini, L. Popovas, A. Rabus, M. Rahvar, S. Scarpetta, G. Skottfelt, J. Southworth, J. Starkey, D. Surdej, J. Wertz, O. Zarucki, M. Pogge, R. W. DePpoy, D. L. CA Spitzer Microlensing Team OGLE Collaboration RoboNet Collaboration MINDSTEp Consortium Fun Collaboration TI OGLE-2015-BLG-0479LA,B: BINARY GRAVITATIONAL MICROLENS CHARACTERIZED BY SIMULTANEOUS GROUND-BASED AND SPACE-BASED OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; gravitational lensing: micro ID DIFFERENCE IMAGE-ANALYSIS; PARALLAX SATELLITE MASS; LENSING EXPERIMENT; PLANET PHOTOMETRY; GALACTIC BULGE; OGLE-III; SPITZER; EVENTS; STARS; DISTANCES AB We present a combined analysis of the observations of the gravitational microlensing event OGLE-2015-BLG-0479 taken both from the ground and by the Spitzer Space Telescope. The light curves seen from the ground and from space exhibit a time offset of similar to 13 days between the caustic spikes, indicating that the relative lens-source positions seen from the two places are displaced by parallax effects. From modeling the light curves, we measure the space-based microlens parallax. Combined with the angular Einstein radius measured by analyzing the caustic crossings, we determine the mass and distance of the lens. We find that the lens is a binary composed of two G-type stars with masses of similar to 1.0 M-circle dot and similar to 0.9 M-circle dot located at a distance. of similar to 3 kpc. In addition, we are able to constrain the complete orbital parameters of the lens thanks to the precise measurement of the microlens parallax derived from the joint analysis. In contrast to the binary event OGLE-2014-BLG-1050, which was also observed by Spitzer, we find that the interpretation of OGLE-2015-BLG-0479 does not suffer from the degeneracy between (+/-, +/-) and (+/-, -/+) solutions, confirming that the four-fold parallax degeneracy in single-lens events collapses into the two-fold degeneracy for the general case of binary-lens events. The location of the blend in the color-magnitude diagram is consistent with the lens properties, suggesting that the blend is the lens itself. The blend is bright enough for spectroscopy and thus this possibility can be checked from future follow-up observations. C1 [Han, C.] Chungbuk Natl Univ, Dept Phys, Cheongju 361763, South Korea. [Udalski, A.; Szymanski, M. K.; Soszynski, I.; Skowron, J.; Mroz, P.; Poleski, R.; Pietrukowicz, P.; Kozlowski, S.; Ulaczyk, K.; Wyrzykowski, L.; Pawlak, M.] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland. [Gould, A.; Zhu, Wei; Gaudi, B. S.; Wibking, B.] Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. [Gould, A.; Ciceri, S.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Street, R. A.] Queen Mary Univ London, Sch Phys & Astron, Mile End Rd, London E1 4NS, England. [Yee, J. C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Beichman, C.] CALTECH, NASA, Exoplanet Sci Inst, MS 100-22, Pasadena, CA 91125 USA. [Bryden, C.; Henderson, Calen B.; Shvartzvald, Y.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Novati, S. Calchi] Univ Salerno, Dipartimento Fis ER Caianiello, Via Giovanni Paolo II, I-84084 Fisciano, SA, Italy. [Novati, S. Calchi] IIASS, Via G Pellegrino 19, I-84019 Vietri Sul Mare, SA, Italy. [Carey, S.] CALTECH, Spitzer Sci Ctr, MS 220-6, Pasadena, CA 91125 USA. [Tsapras, Y.; Jaimes, R. Figuera; Schmidt, R.; Wambsganss, J.] Univ Heidelberg ZAH, Zentrum Astron, Astronom Rechen Inst, D-69120 Heidelberg, Germany. [Hundertmark, M.] Univ Copenhagen, Niels Bohr Inst, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark. [Hundertmark, M.] Univ Copenhagen, Ctr Star & Planet Format, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark. [Bachelet, E.] Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA. [Bachelet, E.; Bramich, D. M.; Alsubai, K. A.] Qatar Fdn, HBKU, QEERI, Doha, Qatar. [Dominik, M.; Jaimes, R. Figuera; Horne, K.; Starkey, D.] Univ St Andrews, Sch Phys Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Ranc, C.] UPMC Univ Paris 6, Sorbonne Univ, CNRS, Inst Astrophys Paris,UMR 7095, 98 Bis Bd Arago, F-75014 Paris, France. [Snodgrass, C.] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England. [Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool CH41 1LD, Merseyside, England. [Menzies, J.] South African Astron Observ, POB 9, ZA-7935 Observatory, South Africa. [Mao, S.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Jorgensen, U. G.; Haugbolle, T.; Juncher, D.; Korhonen, H.; Popovas, A.; Skottfelt, J.] Univ Copenhagen, Niels Bohr Inst, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. [Hessman, F. V.] Georg August Univ Gottingen, Inst Astrophys, Friedrich Hund Pl 1, D-37077 Gottingen, Germany. [Hinse, T. C.] Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Daejeon 305348, South Korea. [Korhonen, H.] Univ Turku, Finnish Ctr Astron ESO FINCA, Vaisalantie 20, FI-21500 Piikkio, Finland. [Rabus, M.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Av Vicuna Mackenna 4860, Santiago 7820436, Chile. [Rahvar, S.] Sharif Univ Technol, Dept Phys, POB 11155-9161, Tehran, Iran. [Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Surdej, J.; Wertz, O.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [DePpoy, D. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. RP Han, C (reprint author), Chungbuk Natl Univ, Dept Phys, Cheongju 361763, South Korea. RI Korhonen, Heidi/E-3065-2016; D'Ago, Giuseppe/N-8318-2016 OI Korhonen, Heidi/0000-0003-0529-1161; D'Ago, Giuseppe/0000-0001-9697-7331 FU Creative Research Initiative Program of National Research Foundation of Korea [2009-0081561]; National Science Centre, Poland [MAESTRO 2014/14/A/ST9/00121]; JPL grant [1500811]; NASA through the Sagan Fellowship Program; NASA FX Work by C. Han was supported by the Creative Research Initiative Program (2009-0081561) of National Research Foundation of Korea. The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U. The OGLE Team thanks Profs. M.. Kubiak and G.. Pietrzynski, former members of the OGLE team, for their contribution to the collection of the OGLE photometric data over the past years. Work by A.G. was supported by JPL grant 1500811. Work by J.C.Y. was performed under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. Work by C.B.H. and Y.S. was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Universities Space Research Association through a contract with NASA. The Spitzer Team thanks Christopher S. Kochanek for graciously trading us his allocated observing time on the CTIO 1.3m during the Spitzer campaign. We acknowledge the high-speed internet service (KREONET) provided by Korea Institute of Science and Technology Information (KISTI). NR 40 TC 2 Z9 2 U1 3 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2016 VL 828 IS 1 AR 53 DI 10.3847/0004-637X/828/1/53 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA8OE UT WOS:000386894900053 ER PT J AU Lieman-Sifry, J Hughes, AM Carpenter, JM Gorti, U Hales, A Flaherty, KM AF Lieman-Sifry, Jesse Hughes, A. Meredith Carpenter, John M. Gorti, Uma Hales, Antonio Flaherty, Kevin M. TI DEBRIS DISKS IN THE SCORPIUS-CENTAURUS OB ASSOCIATION RESOLVED BY ALMA SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; planets and satellites: formation; protoplanetary disks; submillimeter: planetary systems ID TERRESTRIAL PLANET FORMATION; CIRCLE-DOT STARS; ANALOG HD 107146; A-TYPE STARS; BETA-PICTORIS; DUSTY DEBRIS; MOLECULAR GAS; MILLIMETER EMISSION; CIRCUMSTELLAR DISK; SCATTERED-LIGHT AB We present a CO(2-1) and 1240 mu m continuum survey of 23 debris disks with spectral types B9-G1, observed at an angular resolution of 0.5 ''-1 '' with the Atacama Large Millimeter/Submillimeter Array (ALMA). The sample was selected for large infrared excess and age similar to 10 Myr, to characterize the prevalence of molecular gas emission in young debris disks. We identify three CO-rich debris disks, plus two additional tentative (3 sigma) CO detections. Twenty disks were detected in the continuum at the >3 sigma level. For the 12 disks in the sample that are spatially resolved by our observations, we perform an independent analysis of the interferometric continuum visibilities to constrain the basic dust disk geometry, as well as a simultaneous analysis of the visibilities and broadband spectral energy distribution to constrain the characteristic grain size and disk mass. The gas-rich debris disks exhibit preferentially larger outer radii in their dust disks, and a higher prevalence of characteristic grain sizes smaller than the blowout size. The gas-rich disks do not exhibit preferentially larger dust masses, contrary to expectations for a scenario in which a higher cometary destruction rate would be expected to result in a larger mass of both CO and dust. The three debris disks in our sample with strong CO detections are all around A stars: the conditions in disks around intermediate-mass stars appear to be the most conducive to the survival or formation of CO. C1 [Lieman-Sifry, Jesse; Hughes, A. Meredith; Flaherty, Kevin M.] Wesleyan Univ, Van Vleck Observ, Dept Astron, 96 Foss Hill Dr, Middletown, CT 06459 USA. [Carpenter, John M.] CALTECH, Dept Astron, MC 249-17, Pasadena, CA 91125 USA. [Carpenter, John M.; Hales, Antonio] Joint ALMA Observ, Atacama Large Millimeter Submillimeter Array, Alonso Cordova 3107, Santiago 7630355, Chile. [Gorti, Uma] SETI Inst, Mountain View, CA USA. [Gorti, Uma] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hales, Antonio] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. RP Lieman-Sifry, J (reprint author), Wesleyan Univ, Van Vleck Observ, Dept Astron, 96 Foss Hill Dr, Middletown, CT 06459 USA. FU NSF [AST-1412647, CNS-0619508]; NASA CT Space Grant Directed Campus Scholarship FX The authors thank Angelo Ricarte for his contributions to the code base and helpful comments, and the anonymous referee for a careful commentary that improved the paper. J.L.S. and A.M.H. gratefully acknowledge support from NSF grant AST-1412647. J.L.S. was also supported in part by a NASA CT Space Grant Directed Campus Scholarship. We acknowledge Wesleyan University for time on its high-performance computing cluster, supported by the NSF under grant number CNS-0619508. This work makes use of the following ALMA data: ADS/JAO. ALMA#2012.1.00688. S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/ NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of NASA's Astrophysics Data System Bibliographic Services, as well as Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013). NR 87 TC 2 Z9 2 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2016 VL 828 IS 1 AR 25 DI 10.3847/0004-637X/828/1/25 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA8OE UT WOS:000386894900025 ER PT J AU Lomax, JR Wisniewski, JP Grady, CA McElwain, MW Hashimoto, J Kudo, T Kusakabe, N Okamoto, YK Fukagawa, M Abe, L Brandner, W Brandt, TD Carson, JC Currie, TM Egner, S Feldt, M Goto, M Guyon, O Hayano, Y Hayashi, M Hayashi, SS Henning, T Hodapp, KW Inoue, A Ishii, M Iye, M Janson, M Kandori, R Knapp, GR Kuzuhara, M Kwon, J Matsuo, T Mayama, S Miyama, S Momose, M Morino, JI Moro-Martin, A Nishimura, T Pyo, TS Schneider, GH Serabyn, E Sitko, ML Suenaga, T Suto, H Suzuki, R Takahashi, YH Takami, M Takato, N Terada, H Thalmann, C Tomono, D Turner, EL Watanabe, M Yamada, T Takami, H Usuda, T Tamura, M AF Lomax, Jamie R. Wisniewski, John P. Grady, Carol A. McElwain, Michael W. Hashimoto, Jun Kudo, Tomoyuki Kusakabe, Nobuhiko Okamoto, Yoshiko K. Fukagawa, Misato Abe, Lyu Brandner, Wolfgang Brandt, Timothy D. Carson, Joseph C. Currie, Thayne M. Egner, Sebastian Feldt, Markus Goto, Miwa Guyon, Olivier Hayano, Yutaka Hayashi, Masahiko Hayashi, Saeko S. Henning, Thomas Hodapp, Klaus W. Inoue, Akio Ishii, Miki Iye, Masanori Janson, Markus Kandori, Ryo Knapp, Gillian R. Kuzuhara, Masayuki Kwon, Jungmi Matsuo, Taro Mayama, Satoshi Miyama, Shoken Momose, Munetake Morino, Jun-Ichi Moro-Martin, Amaya Nishimura, Tetsuo Pyo, Tae-Soo Schneider, Glenn H. Serabyn, Eugene Sitko, Michael L. Suenaga, Takuya Suto, Hiroshi Suzuki, Ryuji Takahashi, Yasuhiro H. Takami, Michihiro Takato, Naruhisa Terada, Hiroshi Thalmann, Christian Tomono, Daigo Turner, Edwin L. Watanabe, Makoto Yamada, Toru Takami, Hideki Usuda, Tomonori Tamura, Motohide TI CONSTRAINING THE MOVEMENT OF THE SPIRAL FEATURES AND THE LOCATIONS OF PLANETARY BODIES WITHIN THE AB AUR SYSTEM SO ASTROPHYSICAL JOURNAL LA English DT Article DE planet-disk interactions; planetary systems; protoplanetary disks; radiative transfer; stars: individual (AB Aur); stars: pre-main sequence ID YOUNG STELLAR OBJECTS; HERBIG AE STARS; SPECTRAL ENERGY-DISTRIBUTIONS; CIRCUMSTELLAR DUST; PROTOPLANETARY DISK; RADIATION TRANSFER; INTERSTELLAR DUST; SIZE DISTRIBUTION; HIGH-RESOLUTION; TAURUS-AURIGA AB We present a new analysis of multi-epoch, H-band, scattered light images of the AB Aur system. We use a Monte Carlo radiative transfer code to simultaneously model the system's spectral energy distribution (SED) and H-band polarized intensity (PI) imagery. We find that a disk-dominated model, as opposed to one that is envelope-dominated, can plausibly reproduce AB Aur's SED and near-IR imagery. This is consistent with previous modeling attempts presented in the literature and supports the idea that at least a subset of AB Aur's spirals originate within the disk. In light of this, we also analyzed the movement of spiral structures in multi-epoch H-band total light and PI imagery of the disk. We detect no significant rotation or change in spatial location of the spiral structures in these data, which span a 5.8-year baseline. If such structures are caused by disk-planet interactions, the lack of observed rotation constrains the location of the orbit of planetary perturbers to be >47 au. C1 [Lomax, Jamie R.; Wisniewski, John P.; Hashimoto, Jun] Univ Oklahoma, Homer L Dodge Dept Phys, Norman, OK 73071 USA. [Grady, Carol A.] Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA. [Grady, Carol A.] Eureka Sci, 2452 Delmer,Suite 100, Oakland, CA 96002 USA. [Grady, Carol A.] Goddard Ctr Astrobiol, Pasadena, CA USA. [McElwain, Michael W.] NASA, Goddard Space Flight Ctr, Code 6681, Greenbelt, MD 20771 USA. [Kudo, Tomoyuki; Currie, Thayne M.; Egner, Sebastian; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko S.; Nishimura, Tetsuo; Pyo, Tae-Soo; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daigo] Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Pl, Hilo, HI 96720 USA. [Kusakabe, Nobuhiko; Hayashi, Masahiko; Ishii, Miki; Iye, Masanori; Kandori, Ryo; Morino, Jun-Ichi; Suenaga, Takuya; Suto, Hiroshi; Suzuki, Ryuji; Takahashi, Yasuhiro H.; Takami, Hideki; Tamura, Motohide] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Okamoto, Yoshiko K.] Ibaraki Univ, Fac Sci, Inst Astrophys & Planetary Sci, 2-1-1 Bunkyo, Mito, Ibaraki 3108512, Japan. [Fukagawa, Misato] Osaka Univ, Grad Sch Sci, 1-1 Machikaneyama, Toyonaka, Osaka 5600043, Japan. [Abe, Lyu] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange UMR 7293, 28 Ave Valrose, F-06108 Nice 2, France. [Brandner, Wolfgang] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Brandt, Timothy D.; Turner, Edwin L.] Inst Adv Study, Dept Astrophys, Princeton, NJ 08540 USA. [Carson, Joseph C.] Coll Charleston, Dept Phys & Astron, 58 Coming St, Charleston, SC 29424 USA. [Goto, Miwa] Univ Munich, Univ Sternwarte Munchen, Scheinerstr 1, D-81679 Munich, Germany. [Hodapp, Klaus W.] Univ Hawaii, Inst Astron, 640 N Aohoku Pl, Hilo, HI 96720 USA. [Janson, Markus] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, SE-10691 Stockholm, Sweden. [Knapp, Gillian R.] Princeton Univ, Dept Astrophys Sci, Peyton Hall,Ivy Lane, Princeton, NJ 08544 USA. [Kuzuhara, Masayuki] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan. [Kwon, Jungmi; Usuda, Tomonori; Tamura, Motohide] Univ Tokyo, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. [Matsuo, Taro] Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan. [Mayama, Satoshi] Grad Univ Adv Studies SOKENDAI, Ctr Promot Integrated Sci, Hayama Cho, Hayama, Kanagawa 2400193, Japan. [Miyama, Shoken] Hiroshima Univ, 1-3-2 Kagamiyama, Higashihiroshima 7398511, Japan. [Momose, Munetake] Ibaraki Univ, Coll Sci, Bunkyo 2-1-1, Mito, Ibaraki 3108512, Japan. [Moro-Martin, Amaya] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Moro-Martin, Amaya] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA. [Schneider, Glenn H.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. [Serabyn, Eugene] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Sitko, Michael L.] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA. [Sitko, Michael L.] Space Sci Inst, 475 Walnut St,Suite 205, Boulder, CO 80301 USA. [Suenaga, Takuya] Grad Univ Adv Studies, Dept Astron Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Takami, Michihiro] Acad Sinica, Inst Astron & Astrophys, POB 23141, Taipei 10617, Taiwan. [Thalmann, Christian] Swiss Fed Inst Technol, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. [Watanabe, Makoto] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan. [Yamada, Toru] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. RP Lomax, JR (reprint author), Univ Oklahoma, Homer L Dodge Dept Phys, Norman, OK 73071 USA. EM Jamie.R.Lomax@ou.edu; wisniewski@ou.edu; carol.a.grady@nasa.gov RI MIYAMA, Shoken/A-3598-2015 FU NASA Origins of Solar System program [NNX13AK17G, RTOP 12-OSS12-0045, NNG13PB64P]; MEXT Japan; Mitsubishi Foundation; [NSF-AST 1009203]; [1008440]; [1009314] FX We acknowledge support from NSF-AST 1009203 (J.C.), 1008440 (C.G.), and 1009314 (E.R., J.W., J.H.) and the NASA Origins of Solar System program under NNX13AK17G (J.W.), RTOP 12-OSS12-0045 (M.M.), and NNG13PB64P (C.G.). This work is partly supported by a Grant-in-Aid for Science Research in a Priority Area from MEXT Japan and by the Mitsubishi Foundation. The authors recognize and acknowledge the significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. This work is based in part on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. We also thank Barbara Whitney for providing us with helpful feedback that improved our paper and for clarifying aspects of her HOCHUNK3D code, and Anthony Paat for helping run models. Additionally, we would like to thank the anonymous reviewer for providing comments that led to an improved paper. NR 40 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2016 VL 828 IS 1 AR 2 DI 10.3847/0004-637X/828/1/2 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA8OE UT WOS:000386894900002 ER PT J AU Nelson, EJ van Dokkum, PG Schreiber, NMF Franx, M Brammer, GB Momcheva, IG Wuyts, S Whitaker, KE Skelton, RE Fumagalli, M Hayward, CC Kriek, M Labbe, I Leja, J Rix, HW Tacconi, LJ van der Wel, A van den Bosch, FC Oesch, PA Dickey, C Lange, JU AF Nelson, Erica June van Dokkum, Pieter G. Schreiber, Natascha M. Foerster Franx, Marijn Brammer, Gabriel B. Momcheva, Ivelina G. Wuyts, Stijn Whitaker, Katherine E. Skelton, Rosalind E. Fumagalli, Mattia Hayward, Christopher C. Kriek, Mariska Labbe, Ivo Leja, Joel Rix, Hans-Walter Tacconi, Linda J. van der Wel, Arjen van den Bosch, Frank C. Oesch, Pascal A. Dickey, Claire Lange, Johannes Ulf TI WHERE STARS FORM: INSIDE-OUT GROWTH AND COHERENT STAR FORMATION FROM HST H alpha MAPS OF 3200 GALAXIES ACROSS THE MAIN SEQUENCE AT 0.7 < z < 1.5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: star formation; galaxies: structure ID SIMILAR-TO 2; HUBBLE-SPACE-TELESCOPE; SINS/ZC-SINF SURVEY; INTEGRAL FIELD SPECTROSCOPY; LYMAN BREAK GALAXIES; ULTRA-DEEP FIELD; EXTRAGALACTIC LEGACY SURVEY; COMPACT QUIESCENT GALAXIES; MASS-METALLICITY RELATION; KILOPARSEC-SCALE CLUMPS AB We present H alpha maps at 1 kpc spatial resolution for star-forming galaxies at z similar to 1, made possible by the Wide Field Camera 3 grism on Hubble Space Telescope (HST). Employing this capability over all five 3D-HST/CANDELS fields provides a sample of 3200 galaxies enabling a division into subsamples based on stellar mass and star formation rate (SFR). By creating deep stacked H alpha images, we reach surface brightness limits of 1 x 10(-18) erg s(-1) cm(-2) arc sec(-2), allowing us to map the distribution of ionized gas to similar to 10 kpc for typical L* galaxies at this epoch. We find that the spatial extent of the H alpha distribution increases with stellar mass as r(H alpha) = 1.5(M-*/10(10) M-circle dot)(0.23) kpc. The H alpha emission is more extended than the stellar continuum emission, consistent with inside-out assembly of galactic disks. This effect grows stronger with mass as r(H alpha)/r(*) = 1.1(M-*/10(10) M-circle dot)(0.054). We map the H alpha distribution as a function of SFR(IR+UV) and find evidence for "coherent star formation" across the SFR-M-* plane: above the main sequence (MS), H alpha is enhanced at all radii; below the MS, H alpha is depressed at all radii. This suggests that at all masses the physical processes driving the enhancement or suppression of star formation act throughout the disks of galaxies. At high masses (10(10.5) < M-*/M-circle dot < 10(11)), above the MS, H alpha is particularly enhanced in the center, potentially building bulges and/or supermassive black holes. Below the MS, a strong central dip in the EW(H alpha), as well as. the inferred specific SFR, appears. Importantly, though, across the entirety of the SFR-M-* plane, the absolute SFR as traced by H alpha is always centrally peaked, even in galaxies below the MS. C1 [Nelson, Erica June; van Dokkum, Pieter G.; Momcheva, Ivelina G.; Leja, Joel; van den Bosch, Frank C.; Oesch, Pascal A.; Dickey, Claire; Lange, Johannes Ulf] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Schreiber, Natascha M. Foerster; Wuyts, Stijn; Tacconi, Linda J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Franx, Marijn; Fumagalli, Mattia; Labbe, Ivo] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Brammer, Gabriel B.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Wuyts, Stijn] Univ Bath, Dept Phys, Bath BA2 7AY, Avon, England. [Whitaker, Katherine E.] Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Skelton, Rosalind E.] South African Astron Observ, POB 9, ZA-7935 Observatory, South Africa. [Hayward, Christopher C.] CALTECH, TAPIR, Pasadena, CA 91125 USA. [Hayward, Christopher C.] Harvard Smithsonian CfA, Cambridge, MA 02138 USA. [Kriek, Mariska] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Rix, Hans-Walter; van der Wel, Arjen] MPIA, Konigstuhl 17, Heidelberg, Germany. RP Nelson, EJ (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA. RI Skelton, Rosalind/S-1845-2016 OI Skelton, Rosalind/0000-0001-7393-3336 FU 3D-HST Treasury Program [GO 12177, 12328]; NASA [NAS5-26555]; National Science Foundation Graduate Research Fellowship FX We thank the referee for their thoughtful report,. which improved the paper. This work is based on observations taken by the 3D-HST Treasury Program (GO 12177 and 12328) with the NASA/ESA HST, which is operated by the Associations of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. E.J.N. gratefully acknowledges support from the National Science Foundation Graduate Research Fellowship. NR 202 TC 9 Z9 9 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2016 VL 828 IS 1 AR 27 DI 10.3847/0004-637X/828/1/27 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA8OE UT WOS:000386894900027 ER PT J AU Odegard, N Kogut, A Chuss, DT Miller, NJ AF Odegard, N. Kogut, A. Chuss, D. T. Miller, N. J. TI ASSESSMENT OF MODELS OF GALACTIC THERMAL DUST EMISSION USING COBE/FIRAS AND COBE/DIRBE OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; infrared: ISM; submillimeter: ISM ID BACKGROUND EXPERIMENT SEARCH; TEMPERATURE-DEPENDENCE; AMORPHOUS SOLIDS; COBE FIRAS; ABSORPTION-COEFFICIENT; SPECTRAL OBSERVATIONS; INFRARED-EMISSION; GAL OBSERVATIONS; COLD CLUMPS; PLANCK AB Accurate modeling of the spectrum of thermal dust emission at millimeter wavelengths is important for improving the accuracy of foreground subtraction for cosmic microwave background (CMB) measurements, for improving the accuracy with which the contributions of different foreground emission components can be determined, and for improving our understanding of dust composition and dust physics. We fit four models of dust emission to high Galactic latitude COBE/FIRAS and COBE/DIRBE observations from 3 mm to 100 mu m and compare the quality of the fits. We consider the two-level systems (TLS) model because it provides a physically motivated explanation for the observed long wavelength flattening of the dust spectrum and the anti-correlation between emissivity index and dust temperature. We consider the model of Finkbeiner et al. because it has been widely used for CMB studies, and the generalized version of this model that was recently applied to Planck data by Meisner and Finkbeiner. For comparison we have also fit a phenomenological model consisting of the sum of two graybody components. We find that the two-graybody model gives the best fit and the FDS model gives a significantly poorer fit than the other models. The Meisner and Finkbeiner model and the TLS model remain viable for use in Galactic foreground subtraction, but the FIRAS data do not have a sufficient signal-to-noise ratio to provide a strong test of the predicted spectrum at millimeter wavelengths. C1 [Odegard, N.] NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Code 665, Greenbelt, MD 20771 USA. [Kogut, A.; Miller, N. J.] NASA, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA. [Chuss, D. T.] Villanova Univ, Dept Phys, 800 E Lancaster Ave, Villanova, PA 19085 USA. [Miller, N. J.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. RP Odegard, N (reprint author), NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Code 665, Greenbelt, MD 20771 USA. EM Nils.Odegard@nasa.gov NR 47 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2016 VL 828 IS 1 AR 16 DI 10.3847/0004-637X/828/1/16 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA8OE UT WOS:000386894900016 ER PT J AU Parmentier, V Fortney, JJ Showman, AP Morley, C Marley, MS AF Parmentier, Vivien Fortney, Jonathan J. Showman, Adam P. Morley, Caroline Marley, Mark S. TI TRANSITIONS IN THE CLOUD COMPOSITION OF HOT JUPITERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: atmospheres; planets and satellites: gaseous planets; radiative transfer; scattering ID 3-DIMENSIONAL ATMOSPHERIC CIRCULATION; EXTRASOLAR GIANT PLANETS; GREY ANALYTICAL-MODEL; EXOPLANET HD 189733B; OPTICAL-PHASE CURVES; MASS DWARF STARS; BROWN DWARFS; IRRADIATED ATMOSPHERES; THERMAL STRUCTURE; TRANSMISSION SPECTRUM AB Over a large range of equilibrium temperatures, clouds shape the transmission spectrum of hot Jupiter atmospheres, yet their composition remains unknown. Recent observations show that the Kepler light. curves of some hot Jupiters are asymmetric: for the hottest planets, the light. curve peaks before secondary eclipse, whereas for planets cooler than similar to 1900 K, it peaks after secondary eclipse. We use the thermal structure from 3D global circulation models to determine the expected cloud distribution and Kepler light. curves of hot Jupiters. We demonstrate that the change from an optical light. curve dominated by thermal emission to one dominated by scattering (reflection) naturally explains the observed trend from negative to positive offset. For the cool planets the presence of an asymmetry in the Kepler light curve is a telltale sign of the cloud composition, because each cloud species can produce an offset only over a narrow range of effective temperatures. By comparing our models and the observations, we show that the cloud composition of hot Jupiters likely varies with equilibrium temperature. We suggest that a transition occurs between silicate and manganese sulfide clouds at a temperature near 1600 K, analogous to the L/T transition on brown dwarfs. The cold trapping of cloud species below the photosphere naturally produces such a transition and predicts similar transitions for other condensates, including TiO. We predict that most hot Jupiters should have cloudy nightsides, that partial cloudiness should be common at the limb, and that the dayside hot spot should often be cloud-free. C1 [Parmentier, Vivien; Fortney, Jonathan J.; Morley, Caroline] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Parmentier, Vivien; Showman, Adam P.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Parmentier, Vivien; Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Marley, Mark S.] NASA, Ames Res Ctr, MS-245-3, Moffett Field, CA 94035 USA. RP Parmentier, V (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.; Parmentier, V (reprint author), Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.; Parmentier, V (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. OI Marley, Mark/0000-0002-5251-2943 FU Sagan Postdoctoral Fellowship through NASA Exoplanet Science Institute; Origins grant [NNX12AI196] FX We thank Mike Line for reading the manuscript and providing useful comments and Kevin Stevenson for useful discussions. V. P. acknowledges support from the Sagan Postdoctoral Fellowship through the NASA Exoplanet Science Institute. A.P.S. was supported by Origins grant NNX12AI196. NR 85 TC 6 Z9 6 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2016 VL 828 IS 1 AR 22 DI 10.3847/0004-637X/828/1/22 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA8OE UT WOS:000386894900022 ER PT J AU Sadykov, VM Kosovichev, AG Sharykin, IN Zimovets, IV Dominguez, SV AF Sadykov, Viacheslav M. Kosovichev, Alexander G. Sharykin, Ivan N. Zimovets, Ivan V. Vargas Dominguez, Santiago TI RELATIONSHIP BETWEEN CHROMOSPHERIC EVAPORATION AND MAGNETIC FIELD TOPOLOGY IN AN M-CLASS SOLAR FLARE SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: chromosphere; Sun: flares; Sun: magnetic fields; Sun: UV radiation; techniques: spectroscopic ID LOOP RADIATIVE HYDRODYNAMICS; QUASI-SEPARATRIX LAYERS; REGION-IMAGING-SPECTROGRAPH; SLIP-RUNNING RECONNECTION; THICK-TARGET; RESOLUTION OBSERVATIONS; MODEL; IRIS; DYNAMICS; PLASMA AB Chromospheric evaporation is observed as Doppler blueshift during solar flares. It plays a key role in the dynamics and energetics of solar flares; however, its mechanism is still unknown. In this paper,. we present a detailed analysis of spatially resolved multi-wavelength observations of chromospheric evaporation during an M 1.0-class solar flare (SOL2014-06-12T21:12) using data from NASA's Interface Region Imaging Spectrograph and HMI/SDO (the. Helioseismic and Magnetic Imager on. board. the. Solar Dynamics Observatory), and high-resolution observations from VIS/NST (the. Visible Imaging Spectrometer at the. New Solar Telescope). The results show that the averaged over the flare region Fe XXI blueshift of the hot (10(7) K) evaporating plasma is delayed relative to the C II redshift of the relatively cold (10(4) K) chromospheric plasma by about one minute. The spatial distribution of the delays is not uniform across the region and can be as long as two minutes in several zones. Using vector magnetograms from HMI, we reconstruct the magnetic field topology and the quasi-separatrix layer, and find that the blueshift delay regions as well as the Ha flare ribbons are connected to the region of the. magnetic polarity inversion line (PIL) and an expanding flux rope via a system of low-lying loop arcades with a. height of less than or similar to 4.5 Mm. As a result, the chromospheric evaporation may be driven by the energy release in the vicinity of PIL, and has the observed properties due to a local magnetic field topology. C1 [Sadykov, Viacheslav M.; Kosovichev, Alexander G.] New Jersey Inst Technol, Dept Phys, Newark, NJ 07102 USA. [Kosovichev, Alexander G.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Kosovichev, Alexander G.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Sharykin, Ivan N.; Zimovets, Ivan V.] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia. [Vargas Dominguez, Santiago] Univ Nacl Colombia, Observ Astron, Sede Bogota, Carrera 45 26-85, Bogota, Colombia. RP Sadykov, VM (reprint author), New Jersey Inst Technol, Dept Phys, Newark, NJ 07102 USA. RI Zimovets, Ivan/E-4431-2017 OI Zimovets, Ivan/0000-0001-6995-3684 FU NJIT; US NSF [AGS-1250818]; NASA [NNX13AG14G, NNX14AB68G, NNX14AB70G, NNX11AO736]; Korea Astronomy and Space Science Institute; Seoul National University; strategic priority research program of CAS [XDB09000000]; ESA; Norwegian Space Centre; NSF [AGS-1250818]; RFBR [15-32-21078, 16-32-00462] FX The authors acknowledge the BBSO, IRIS, and SDO mission teams for their contribution and support. The BBSO operation is supported by NJIT, US NSF AGS-1250818, and NASA NNX13AG14G grants, and the NST operation is partly supported by the Korea Astronomy and Space Science Institute and Seoul National University and by the strategic priority research program of CAS with grant No. XDB09000000. IRIS is a NASA small explorer mission developed and operated by LMSAL with mission operations executed at the NASA Ames Research Center and major contributions to downlink communications funded by ESA and the Norwegian Space Centre. The authors thank NASA's SDO HMI team for the availability of the high-quality scientific data. The authors also thank the. anonymous referee for valuable comments. The work was partially supported by NASA grants NNX14AB68G, NNX14AB70G, and NNX11AO736; NSF grant AGS-1250818; RFBR grants 15-32-21078 and 16-32-00462; and an NJIT grant. NR 56 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2016 VL 828 IS 1 AR 4 DI 10.3847/0004-637X/828/1/4 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA8OE UT WOS:000386894900004 ER PT J AU Watson, DM Calvet, NP Fischer, WJ Forrest, WJ Manoj, P Megeath, ST Melnick, GJ Najita, J Neufeld, DA Sheehan, PD Stutz, AM Tobin, JJ AF Watson, Dan M. Calvet, Nuria P. Fischer, William J. Forrest, W. J. Manoj, P. Megeath, S. Thomas Melnick, Gary J. Najita, Joan Neufeld, David A. Sheehan, Patrick D. Stutz, Amelia M. Tobin, John J. TI EVOLUTION OF MASS OUTFLOW IN PROTOSTARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Herbig-Haro objects; ISM: jets and outflows; shock waves; stars: jets; stars: pre-main sequence stars: protostars ID SPITZER-SPACE-TELESCOPE; YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; T-TAURI STARS; MAGNETOCENTRIFUGALLY DRIVEN FLOWS; PROTOSTELLAR ACCRETION DISCS; FAST INTERSTELLAR SHOCKS; O I LINE; 63 MU-M; C-II AB We have surveyed 84 Class 0, Class I, and flat-spectrum protostars in mid-infrared [Si II], [Fe II], and [S I] line emission, and 11 of these in far-infrared [O I] emission. We use the results to derive their mass. outflow rates, (M) over dot(w). Thereby we observe a strong correlation of (M) over dot(w) with bolometric luminosity, and with the inferred mass accretion rates of the central objects, (M) over dot(a), which continues through the Class 0 range the trend observed in Class II young stellar objects. Along this trend from large to small mass. flow rates, the different classes of young stellar objects lie in the sequence Class 0-Class I/flat-spectrum-Class II, indicating that the trend is an evolutionary sequence in which (M) over dot(a) and (M) over dot(w) decrease together with increasing age, while maintaining rough proportionality. The survey results include two that. are key tests of magnetocentrifugal outflow-acceleration mechanisms: the distribution of the outflow/accretion branching ratio b = (M) over dot(w)/(M) over dot(a), and limits on the distribution of outflow speeds. Neither rules out any of the three leading outflow-acceleration, angular-momentum-ejection mechanisms, but they provide some evidence that disk winds and accretion-powered stellar winds (APSWs) operate in many protostars. An upper edge observed in the branching-ratio distribution is consistent with the upper bound of b = 0.6 found in models of APSWs, and a large fraction (31%) of the sample have a. branching ratio sufficiently small that only disk winds, launched on scales as large as several au, have been demonstrated to account for them. C1 [Watson, Dan M.; Forrest, W. J.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Calvet, Nuria P.] Univ Michigan, Dept Astron, 825 Dennison Bldg,500 Church St, Ann Arbor, MI 48109 USA. [Fischer, William J.; Megeath, S. Thomas] Univ Toledo, Dept Phys & Astron, 2801 W Bancroft St, Toledo, OH 43606 USA. [Fischer, William J.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. [Manoj, P.] Tata Inst Fundamental Res, Homi Bhabha Rd, Bombay 400005, Maharashtra, India. [Melnick, Gary J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Najita, Joan] Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA. [Neufeld, David A.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. [Sheehan, Patrick D.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. [Stutz, Amelia M.] Max Planck Inst Astron, Koenigstuhl 17, D-69117 Heidelberg, Germany. [Tobin, John J.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. RP Watson, DM (reprint author), Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. EM dmw@pas.rochester.edu FU NASA [NNX14AF79G] FX We are grateful to Ingrid Koch for her help with the IRS data reduction. This work was supported in part by NASA grant NNX14AF79G. NR 77 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2016 VL 828 IS 1 AR 52 DI 10.3847/0004-637X/828/1/52 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA8OE UT WOS:000386894900052 ER PT J AU Koster, RD Brocca, L Crow, WT Burgin, MS De Lannoy, GJM AF Koster, Randal D. Brocca, Luca Crow, Wade T. Burgin, Mariko S. De Lannoy, Gabrielle J. M. TI Precipitation estimation using L-band and C-band soil moisture retrievals SO WATER RESOURCES RESEARCH LA English DT Article DE precipitation; soil moisture; remote sensing ID TIME SATELLITE PRECIPITATION; DATA SETS; RAINFALL AB An established methodology for estimating precipitation amounts from satellite-based soil moisture retrievals is applied to L-band products from the Soil Moisture Active Passive (SMAP) and Soil Moisture and Ocean Salinity (SMOS) satellite missions and to a C-band product from the Advanced Scatterometer (ASCAT) mission. The precipitation estimates so obtained are evaluated against in situ (gauge-based) precipitation observations from across the globe. The precipitation estimation skill achieved using the L-band SMAP and SMOS data sets is higher than that obtained with the C-band product, as might be expected given that L-band is sensitive to a thicker layer of soil and thereby provides more information on the response of soil moisture to precipitation. The square of the correlation coefficient between the SMAP-based precipitation estimates and the observations (for aggregations to approximate to 100 km and 5 days) is on average about 0.6 in areas of high rain gauge density. Satellite missions specifically designed to monitor soil moisture thus do provide significant information on precipitation variability, information that could contribute to efforts in global precipitation estimation. C1 [Koster, Randal D.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Brocca, Luca] CNR, Res Inst Geohydrol Protect, Perugia, Italy. [Crow, Wade T.] USDA, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. [Burgin, Mariko S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [De Lannoy, Gabrielle J. M.] Katholieke Univ Leuven, Dept Earth & Environm Sci, Heverlee, Belgium. RP Koster, RD (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. EM randal.d.koster@nasa.gov RI Brocca, Luca/F-2854-2010; Koster, Randal/F-5881-2012 OI Brocca, Luca/0000-0002-9080-260X; Koster, Randal/0000-0001-6418-6383 FU NASA SMAP mission; SMAP Science Team; Italian Department of Civil Protection FX Part of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). This work (mainly carried out at the NASA Goddard Space Flight Center) was supported by the NASA SMAP mission and the SMAP Science Team. Author Brocca appreciates support from the Italian Department of Civil Protection. Qing Liu and Clara Draper assisted with the processing of the data. SMAP data are available from https://nsidc.org/data/smap, SMOS data from https://smos-ds-02.eo.esa.int/oads/access/, and ASCAT data from http://www.eumetsat.int/website/home/index.htm. Precipitation data are available from ftp://ftp.cpc.ncep.noaa.gov/precip/CPC_UNI_PRCP/GAUGE_GLB. NR 28 TC 4 Z9 4 U1 8 U2 8 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 SEP PY 2016 VL 52 IS 9 BP 7213 EP 7225 DI 10.1002/2016WR019024 PG 13 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA EA9QC UT WOS:000386977900029 ER PT J AU Wiese, DN Landerer, FW Watkins, MM AF Wiese, David N. Landerer, Felix W. Watkins, Michael M. TI Quantifying and reducing leakage errors in the JPL RL05M GRACE mascon solution SO WATER RESOURCES RESEARCH LA English DT Article DE GRACE; postprocessing; mascon; leakage errors; gain factors ID SEA-LEVEL; MASS; DECADE; OCEAN; SYSTEM AB Recent advances in processing data from the Gravity Recovery and Climate Experiment (GRACE) have led to a new generation of gravity solutions constrained within a Bayesian framework to remove correlated errors rather than relying on empirical filters. The JPL RL05M mascon solution is one such solution, solving for mass variations using spherical cap mass concentration elements (mascons), while relying on external information provided by near-global geophysical models to constrain the solution. This new gravity solution is fundamentally different than the traditional spherical harmonic gravity solution, and as such, requires different care when postprocessing. Here we discuss two classes of postprocessing considerations for the JPL RL05M GRACE mascon solution: (1) reducing leakage errors across land/ocean boundaries, and (2) scaling the solutions to account for leakage errors introduced through parameterizing the gravity solution in terms of mascons. A Coastline Resolution Improvement (CRI) filter is developed to reduce leakage errors across coastlines. Synthetic simulations reveal a reduction in leakage errors of approximate to 50%, such that residual leakage errors are approximate to 1 cm equivalent water height (EWH) averaged globally. A set of gain factors is derived to reduce leakage errors for continental hydrology applications. The combined effect of the CRI filter coupled with application of the gain factors, is shown to reduce leakage errors when determining the mass balance of large (>160,000 km(2)) hydrological basins from 11% to 30% (0.6-1.5 mm EWH) averaged globally, with local improvements up to 38%-81% (9-19 mm EWH). C1 [Wiese, David N.; Landerer, Felix W.; Watkins, Michael M.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Wiese, DN (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM david.n.wiese@jpl.nasa.gov NR 31 TC 2 Z9 2 U1 2 U2 2 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 SEP PY 2016 VL 52 IS 9 BP 7490 EP 7502 DI 10.1002/2016WR019344 PG 13 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA EA9QC UT WOS:000386977900044 ER PT J AU Molotch, NP Barnard, DM Burns, SP Painter, TH AF Molotch, Noah P. Barnard, David M. Burns, Sean P. Painter, Thomas H. TI Measuring spatiotemporal variation in snow optical grain size under a subalpine forest canopy using contact spectroscopy SO WATER RESOURCES RESEARCH LA English DT Article DE snow; forests; snow grain size; spectroscopy; snow temperature; snow-forest interactions ID INFRARED REFLECTANCE; SURFACE-AREA; WATER EQUIVALENT; NUMERICAL-MODEL; COVERED AREA; STRATIGRAPHY; ACCUMULATION; COVARIANCE; ABLATION; DENSITY AB The distribution of forest cover exerts strong controls on the spatiotemporal distribution of snow accumulation and snowmelt. The physical processes that govern these controls are poorly understood given a lack of detailed measurements of snow states. In this study, we address one of many measurement gaps by using contact spectroscopy to measure snow optical grain size at high spatial resolution in trenches dug between tree boles in a subalpine forest. Trenches were collocated with continuous measurements of snow depth and vertical profiles of snow temperature and supplemented with manual measurements of snow temperature, geometric grain size, grain type, and density from trench walls. There was a distinct difference in snow optical grain size between winter and spring periods. In winter and early spring, when facetted snow crystal types were dominant, snow optical grain size was 6% larger in canopy gaps versus under canopy positions; a difference that was smaller than the measurement uncertainty. By midspring, the magnitude of snow optical grain size differences increased dramatically and patterns of snow optical grain size became highly directional with 34% larger snow grains in areas south versus north of trees. In winter, snow temperature gradients were up to 5-15 degrees C m(-1) greater under the canopy due to shallower snow accumulation. However, in canopy gaps, snow depths were greater in fall and early winter and therefore more significant kinetic growth metamorphism occurred relative to under canopy positions, resulting in larger snow grains in canopy gaps. Our findings illustrate the novelty of our method of measuring snow optical grain size, allowing for future studies to advance the understanding of how forest and meteorological conditions interact to impact snowpack evolution. C1 [Molotch, Noah P.; Barnard, David M.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. [Molotch, Noah P.; Burns, Sean P.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA. [Molotch, Noah P.; Painter, Thomas H.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Burns, Sean P.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. RP Molotch, NP (reprint author), Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.; Molotch, NP (reprint author), Univ Colorado, Dept Geog, Boulder, CO 80309 USA.; Molotch, NP (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM noah.molotch@colorado.edu RI Molotch, Noah/C-8576-2009; Painter, Thomas/B-7806-2016 FU U.S. National Aeronautics and Space Administration [NNXIIAK35A]; U.S. National Science Foundation (NSF) [EAR 1141764]; U.S. Department of Agriculture [2012-67003-19802]; NSF Niwot Ridge Long Term Ecological Research program; Department of Energy Ameriflux program FX This work was supported by the U.S. National Aeronautics and Space Administration under grant NNXIIAK35A, by the U.S. National Science Foundation (NSF) under grant EAR 1141764, and by the U.S. Department of Agriculture under grant 2012-67003-19802. Additional support was provided by the NSF Niwot Ridge Long Term Ecological Research program and by the Department of Energy Ameriflux program. Part of this work was conducted at the Jet Propulsion Laboratory, California Institute of Technology under contract from NASA. Snow grain size data sets can be downloaded from ftp://snowserver.colorado.edu/pub/NWT_snow_grain_size_trenches2006/grain -Size.zip. All meteorological data can be obtained from http://fluxnet.ornl.gov/site/997. NR 40 TC 0 Z9 0 U1 1 U2 1 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 SEP PY 2016 VL 52 IS 9 BP 7513 EP 7522 DI 10.1002/2016WR018954 PG 10 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA EA9QC UT WOS:000386977900046 PM 27917006 ER PT J AU Jung-Kubiak, C Reck, TJ Siles, JV Lin, R Lee, C Gill, J Cooper, K Mehdi, I Chattopadhyay, G AF Jung-Kubiak, Cecile Reck, Theodore J. Siles, Jose V. Lin, Robert Lee, Choonsup Gill, John Cooper, Ken Mehdi, Imran Chattopadhyay, Goutam TI A Multistep DRIE Process for Complex Terahertz Waveguide Components SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Article DE Deep reactive-ion etching (DRIE); orthomode transducer (OMT); silicon dioxide (SiO2); silicon micromachining; submillimeter waves; terahertz (THz) ID SATELLITE; GHZ AB Asilicon deep reactive-ion etching (DRIE) process has been developed, using multiple SiO2 masks to enable multidepth waveguide features with +/- 2% tolerance. The unique capability of this process is demonstrated by designing, fabricating, and testing an orthomode transducer working in the 500-600 GHz frequency range. Straight waveguide measurements are also performed to characterize the losses associated with the multistep DRIE process, giving results slightly better than expected for metal-machined waveguides. This process enables the integration of multiple terahertz waveguide components such as mixers, multipliers, quadrature hybrids, and polarization twists onto a single silicon package. C1 [Jung-Kubiak, Cecile; Reck, Theodore J.; Siles, Jose V.; Lin, Robert; Lee, Choonsup; Gill, John; Cooper, Ken; Mehdi, Imran; Chattopadhyay, Goutam] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA. RP Jung-Kubiak, C (reprint author), CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA. EM Cecile.D.Jung@jpl.nasa.gov; theodore.reck@jpl.nasa.gov; Jose.V.Siles@jpl.nasa.gov; Robert.H.Lin@jpl.nasa.gov; Choonsup.Lee@jpl.nasa.gov; John.J.Gill@jpl.nasa.gov; Ken.B.Cooper@jpl.nasa.gov; imran.mehdi@jpl.nasa.gov; goutam.chattopadhyay@jpl.nasa.gov FU National Aeronautical and Space Administration FX This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology supported under a contract with the National Aeronautical and Space Administration. NR 19 TC 1 Z9 1 U1 3 U2 3 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 SEP PY 2016 VL 6 IS 5 BP 690 EP 695 DI 10.1109/TTHZ.2016.2593793 PG 6 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA DZ7QF UT WOS:000386060200007 ER PT J AU Shah, U Decrossas, E Jung-Kubiak, C Reck, T Chattopadhyay, G Mehdi, I Oberhammer, J AF Shah, Umer Decrossas, Emmanuel Jung-Kubiak, Cecile Reck, Theodore Chattopadhyay, Goutam Mehdi, Imran Oberhammer, Joachim TI Submillimeter-Wave 3.3-bit RF MEMS Phase Shifter Integrated in Micromachined Waveguide SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Article DE Micromachined waveguide; phase shifter; radio-frequency (RF) microelectromechanical system (MEMS); rectangular waveguide; submillimeter-wave; terahertz (THz) ID E-PLANE; BAND; TECHNOLOGY; COMPONENTS; FILTERS AB This paper presents a submillimeter-wave 500-550-GHz MEMS-reconfigurable phase shifter, which is based on loading a micromachined rectangular waveguide with 9 E-plane stubs. The phase shifter uses MEMS-reconfigurable surfaces to individually block/unblock the E-plane stubs from the micromachined waveguide. Each MEMS-reconfigurable surface is designed so that in the nonblocking state, it allows the electromagnetic wave to pass freely through it into the stub, while in the blocking state, it serves as the roof of the main waveguide and blocks the wave propagation into the stub. The phase-shifter design comprises three micromachined chips that are mounted in the H-plane cuts of the rectangular waveguide. Experimental results of the first device prototypes show that the microelectromechanical system (MEMS)- reconfigurable phase shifter has a linear phase shift of 20 degrees in ten discrete steps (3.3 bits). The measured insertion loss is better than 3 dB, of which only 0.5-1.5 dB is attributed to the MEMS surfaces and switched stubs, and the measured return loss is better than 15 dB in the design frequency band of 500-550 GHz. It is also shown that the major part of the insertion loss is attributed to misalignment and assembly uncertainties of the micromachined chips and the waveguide flanges, shown by simulations and reproducibility measurements. The MEMS-reconfigurable phase shifter is also operated in an analog tuning mode for high phase resolution. Furthermore, a detailed study has been carried out identifying the reason for the discrepancy between the simulated (90 degrees) and the measured (20 degrees) phase shift. Comb-drive actuators with spring constant variations between 2.13 and 8.71 N/m are used in the phase shifter design. An actuation voltage of 21.94 V with a reproducibility better than sigma = 0.0503 V is measured for the actuator design with a spring constant of 2.13 N/m. Reliability measurement on this actuator was performed in an uncontrolled laboratory environment and showed no deterioration in the functioning of the actuator observed over one hundred million cycles. C1 [Shah, Umer; Oberhammer, Joachim] KTH Royal Inst Technol, Sch Elect Engn, Micro & Nanosyst, SE-10044 Stockholm, Sweden. [Decrossas, Emmanuel; Jung-Kubiak, Cecile; Reck, Theodore; Chattopadhyay, Goutam; Mehdi, Imran] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Shah, U (reprint author), KTH Royal Inst Technol, Sch Elect Engn, Micro & Nanosyst, SE-10044 Stockholm, Sweden. EM umers@kth.se; Emmanuel.Decrossas@jpl.nasa.gov; Cecile.D.Jung@jpl.nasa.gov; theodore.reck@jpl.nasa.gov; goutam.chattopadhyay@jpl.nasa.gov; imran.mehdi@jpl.nasa.gov; joachim.oberhammer@ee.kth.se OI Oberhammer, Joachim/0000-0003-3339-9137 FU European Research Council Consolidator Grant [616846]; Swedish Foundation for Strategic Research Synergy Grant Electronics [SE13-007]; Nils and Hans Backmark scholarship FX The contribution by KTH to this work was supported under the European Research Council Consolidator Grant 616846, under the Swedish Foundation for Strategic Research Synergy Grant Electronics SE13-007, and under a Nils and Hans Backmark scholarship. NR 19 TC 0 Z9 0 U1 7 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 SEP PY 2016 VL 6 IS 5 BP 706 EP 715 DI 10.1109/TTHZ.2016.2584924 PG 10 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA DZ7QF UT WOS:000386060200009 ER PT J AU Kempes, CP Wang, L Amend, JP Doyle, J Hoehler, T AF Kempes, Christopher P. Wang, Lawrence Amend, Jan P. Doyle, John Hoehler, Tori TI Evolutionary tradeoffs in cellular composition across diverse bacteria SO ISME JOURNAL LA English DT Article ID ESCHERICHIA-COLI; AEROBACTER-AEROGENES; UNIFYING THEORY; SIZE CONTROL; GROWTH; PROTEIN; CELLS; RATES; RNA; EUKARYOTES AB One of the most important classic and contemporary interests in biology is the connection between cellular composition and physiological function. Decades of research have allowed us to understand the detailed relationship between various cellular components and processes for individual species, and have uncovered common functionality across diverse species. However, there still remains the need for frameworks that can mechanistically predict the tradeoffs between cellular functions and elucidate and interpret average trends across species. Here we provide a comprehensive analysis of how cellular composition changes across the diversity of bacteria as connected with physiological function and metabolism, spanning five orders of magnitude in body size. We present an analysis of the trends with cell volume that covers shifts in genomic, protein, cellular envelope, RNA and ribosomal content. We show that trends in protein content are more complex than a simple proportionality with the overall genome size, and that the number of ribosomes is simply explained by cross-species shifts in biosynthesis requirements. Furthermore, we show that the largest and smallest bacteria are limited by physical space requirements. At the lower end of size, cell volume is dominated by DNA and protein content-the requirement for which predicts a lower limit on cell size that is in good agreement with the smallest observed bacteria. At the upper end of bacterial size, we have identified a point at which the number of ribosomes required for biosynthesis exceeds available cell volume. Between these limits we are able to discuss systematic and dramatic shifts in cellular composition. Much of our analysis is connected with the basic energetics of cells where we show that the scaling of metabolic rate is surprisingly superlinear with all cellular components. C1 [Kempes, Christopher P.] Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA. [Kempes, Christopher P.; Wang, Lawrence; Doyle, John] CALTECH, Control & Dynam Syst, Pasadena, CA 91125 USA. [Kempes, Christopher P.; Hoehler, Tori] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Amend, Jan P.] Univ Southern Calif, Dept Earth Sci, Los Angeles, CA USA. [Amend, Jan P.] Univ Southern Calif, Dept Biol Sci, Los Angeles, CA USA. RP Kempes, CP (reprint author), Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA. EM ckempes@gmail.com FU 'Life Underground' NASA Astrobiology Institute [NNA13AA92A]; Gordon and Betty Moore Foundation FX CPK acknowledges the support of the 'Life Underground' NASA Astrobiology Institute (NNA13AA92A) and the Gordon and Betty Moore Foundation. NR 41 TC 4 Z9 4 U1 13 U2 13 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1751-7362 EI 1751-7370 J9 ISME J JI ISME J. PD SEP PY 2016 VL 10 IS 9 BP 2145 EP 2157 DI 10.1038/ismej.2016.21 PG 13 WC Ecology; Microbiology SC Environmental Sciences & Ecology; Microbiology GA EA5MK UT WOS:000386664600007 PM 27046336 ER PT J AU Saghaian, SM Karaca, HE Tobe, H Pons, J Santamarta, R Chumlyakov, YI Noebe, RD AF Saghaian, S. M. Karaca, H. E. Tobe, H. Pons, J. Santamarta, R. Chumlyakov, Y. I. Noebe, R. D. TI Effects of Ni content on the shape memory properties and microstructure of Ni-rich NiTi-20Hf alloys SO SMART MATERIALS AND STRUCTURES LA English DT Article DE Ni-rich NiTiHf; high temperature shape memory alloys; martensite morphology; high strength ID NITIHFPD SINGLE-CRYSTALS; MARTENSITIC-TRANSFORMATION; COMPRESSIVE RESPONSE; BEHAVIOR; PHASE; TEMPERATURES; STRENGTH AB Shape memory properties and microstructure of four Ni-rich NiTiHf alloys (Ni50.3Ti29.7Hf20, Ni50.7Ti29.3Hf20, Ni51.2Ti28.8Hf20, and Ni52Ti28Hf20 (at.%)) were systematically characterized in the furnace cooled condition. H-phase precipitates were formed during furnace cooling in compositions with greater than 50.3Ni and the driving force for nucleation increased with Ni content. Alloy strength increased while recoverable strain decreased with increasing Ni content due to changes in precipitate characteristics. When the precipitates were small (similar to 5-15 nm), they were readily absorbed by martensite plates, which resulted in maximum recoverable strain of 2% in Ni50.7Ti29.3Hf20. With increasing Ni content, the size (>100 nm) and volume fraction of precipitates increased and the growth of martensite plates was constrained between the precipitates when the Ni concentration was greater than 50.7 at.%. Near perfect dimensional stability with negligible irrecoverable strain was observed at stress levels as high as 2 GPa in the Ni52Ti28Hf20 alloy, though the recoverable strain was rather small. In general, strong local stress fields were created at precipitate/matrix interphases, which lead to high stored elastic energy during the martensitic transformation. C1 [Saghaian, S. M.; Karaca, H. E.; Tobe, H.] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA. [Pons, J.; Santamarta, R.] Univ Illes Balears, Dept Fis, E-07122 Palma De Mallorca, Spain. [Chumlyakov, Y. I.] Tomsk State Univ, Siberian Phys Tech Inst, Tomsk 634050, Russia. [Noebe, R. D.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH USA. RP Karaca, HE (reprint author), Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA. EM karacahaluk@uky.edu RI Chumlyakov, Yuriy/R-6496-2016 FU NASA Transformative Aeronautics Concepts Program (TACP), Transformational Tools and Technologies Project; NASA EPSCOR program [NNX11AQ31A]; RFBR [10-03-0154-a]; RSF program [14-29-00012]; Spanish MINECO [MAT2011-28217-C02-01]; MECOMP-DGICT [MAT2014-56116-C4-1-R]; FEDER FX This work was supported in part by the NASA Transformative Aeronautics Concepts Program (TACP), Transformational Tools and Technologies Project and the NASA EPSCOR program under grant No: NNX11AQ31A and RFBR project with grant No: 10-03-0154-a and RSF program under grant No: 14-29-00012. J Pons and R Santamarta also acknowledge the financial support from the Spanish MINECO (ref. MAT2011-28217-C02-01), MECOMP-DGICT (ref. MAT2014-56116-C4-1-R) and FEDER. NR 42 TC 0 Z9 0 U1 12 U2 12 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 SEP PY 2016 VL 25 IS 9 AR 095029 DI 10.1088/0964-1726/25/9/095029 PG 11 WC Instruments & Instrumentation; Materials Science, Multidisciplinary SC Instruments & Instrumentation; Materials Science GA DZ6UJ UT WOS:000385997500029 ER PT J AU Meskhidze, N Johnson, MS Hurley, D Dawson, K AF Meskhidze, Nicholas Johnson, Matthew S. Hurley, David Dawson, Kyle TI Influence of measurement uncertainties on fractional solubility of iron in mineral aerosols over the oceans SO AEOLIAN RESEARCH LA English DT Article DE Soluble iron; Mineral dust; Measurement techniques; 3-D chemical transport model ID DRY DEPOSITION; SIZE DISTRIBUTION; SAHARAN DUST; DISSOLUTION; MODEL; DISTRIBUTIONS; TRANSPORT; PACIFIC; CYCLE; FE AB The atmospheric supply of mineral dust iron (Fe) plays a crucial role in the Earth's biogeochemical cycle and is of specific importance as a micronutrient in the marine environment. Observations show several orders of magnitude variability in the fractional solubility of Fe in mineral dust aerosols, making it hard to assess the role of mineral dust in the global ocean biogeochemical Fe cycle. In this study we compare the operational solubility of mineral dust aerosol Fe associated with the flow-through leaching protocol to the results of the global 3-D chemical transport model GEOS-Chem. According to the protocol, aerosol Fe is defined as soluble by first deionized water leaching of mineral dust through a 0.45 mu m pore size membrane followed by acidification and storage of the leachate over a long period of time prior to analysis. To estimate the uncertainty in soluble Fe results introduced by the flow-through leaching protocol, we prescribe an average 50% (range of 30-70%) fractional solubility to sub-0.45 mu m sized mineral dust particles that may inadvertently pass the filter and end up in the acidified (at pH similar to 1.7) leachate for a couple of month period. In the model, the fractional solubility of Fe is either explicitly calculated using a complex mineral aerosol Fe dissolution equations; or prescribed to be 1% and 4% often used by global ocean biogeochemical Fe cycle models to reproduce the broad characteristics of the presently observed ocean dissolved iron distribution. Calculations show that the fractional solubility of Fe derived through the flow-through leaching is higher compared to the model results. The largest differences (similar to 40%) are predicted to occur farther away from the dust source regions, over the areas where sub-0.45 mu m sized mineral dust particles contribute a larger fraction of the total mineral dust mass. This study suggests that different methods used in soluble Fe measurements and inconsistences in the operational definition of filterable Fe in marine environment and soluble Fe in atmospheric aerosols are likely to contribute to the wide range of fractional solubility of aerosol Fe reported in the literature. (C) 2016 Elsevier B.V. All rights reserved. C1 [Meskhidze, Nicholas; Hurley, David; Dawson, Kyle] North Carolina State Univ, Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA. [Johnson, Matthew S.] NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA. RP Meskhidze, N (reprint author), North Carolina State Univ, Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA. EM nmeskhidze@ncsu.edu RI Chem, GEOS/C-5595-2014; OI Dawson, Kyle/0000-0003-3175-0456 FU NCSU Faculty Research & Professional Development Fund; Office of Undergraduate Research at North Carolina State University; NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at NASA Ames Research Center FX This research was supported by NCSU Faculty Research & Professional Development Fund and the grant from the Office of Undergraduate Research at North Carolina State University. The authors would like to thank Daniel Jacob and the Harvard University Atmospheric Chemistry Modeling Group for providing the base GEOS-Chem model used during our research. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at NASA Ames Research Center. We also thank Dr. Akinori Ito from the Japan Agency for Marine-Earth Science and Technology (JAMSTEC) for providing the dust-Fe dissolution code used in Ito and Xu (2014). NR 79 TC 1 Z9 1 U1 6 U2 6 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1875-9637 EI 2212-1684 J9 AEOLIAN RES JI Aeolian Res. PD SEP PY 2016 VL 22 BP 85 EP 92 DI 10.1016/j.aeolia.2016.07.002 PG 8 WC Geography, Physical SC Physical Geography GA DZ1NP UT WOS:000385605400008 ER PT J AU Nicolas, MJ Sullivan, RW Richards, WL AF Nicolas, Matthew J. Sullivan, Rani W. Richards, W. Lance TI Large Scale Applications Using FBG Sensors: Determination of In-Flight Loads and Shape of a Composite Aircraft Wing SO AEROSPACE LA English DT Article DE fiber Bragg grating; FBG; carbon composite wing; optical fiber strain measurement; flight loads; wing deflection; wing shape; structural health monitoring ID FIBER-OPTIC SENSORS; BRAGG GRATING SENSORS; STRAIN AB Technological advances have enabled the development of a number of optical fiber sensing methods over the last few years. The most prevalent optical technique involves the use of fiber Bragg grating (FBG) sensors. These small, lightweight sensors have many attributes that enable their use for a number of measurement applications. Although much literature is available regarding the use of FBGs for laboratory level testing, few publications in the public domain exist of their use at the operational level. Therefore, this paper gives an overview of the implementation of FBG sensors for large scale structures and applications. For demonstration, a case study is presented in which FBGs were used to determine the deflected wing shape and the out-of-plane loads of a 5.5-m carbon-composite wing of an ultralight aerial vehicle. The in-plane strains from the 780 FBG sensors were used to obtain the out-of-plane loads as well as the wing shape at various load levels. The calculated out-of-plane displacements and loads were within 4.2% of the measured data. This study demonstrates a practical method in which direct measurements are used to obtain critical parameters from the high distribution of FBG sensors. This procedure can be used to obtain information for structural health monitoring applications to quantify healthy vs. unhealthy structures. C1 [Nicolas, Matthew J.] PACCAR Engine Co, Dept Mfg Engn, Columbus, MS 39701 USA. [Sullivan, Rani W.] Mississippi State Univ, Dept Aerosp Engn, Mississippi State, MS 39762 USA. [Richards, W. Lance] NASA Langley Res Ctr, NASA Engn & Safety Ctr, Hampton, VA 23681 USA. RP Sullivan, RW (reprint author), Mississippi State Univ, Dept Aerosp Engn, Mississippi State, MS 39762 USA. EM matthewnicolas52@gmail.com; sullivan@ae.msstate.edu; lance.richards-1@nasa.gov OI Nicolas, Matthew/0000-0001-9807-5817 FU NASA Armstrong Flight Research Center [AERO532 11020161]; Raspet Flight Research Laboratory; NASA/Mississippi Space Grant Consortium [12040456 12070825] FX The support provided for this study by the NASA Armstrong Flight Research Center (Award No. AERO532 11020161), Raspet Flight Research Laboratory, and the NASA/Mississippi Space Grant Consortium (Award No. 12040456 12070825) is gratefully acknowledged. NR 38 TC 0 Z9 0 U1 5 U2 5 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 2226-4310 J9 AEROSPACE JI Aerospace PD SEP PY 2016 VL 3 IS 3 AR 18 DI 10.3390/aerospace3030018 PG 15 WC Engineering, Aerospace SC Engineering GA DZ0LQ UT WOS:000385531300001 ER PT J AU Sree, D Stephens, DB AF Sree, Dave Stephens, David B. TI Improved Separation of Tone and Broadband Noise Components from Open Rotor Acoustic Data SO AEROSPACE LA English DT Article DE acoustic; broadband; open rotor; phase-shift; segment-pair; separation; spectrum; spike; tone AB The term open rotor refers to unducted counter-rotating dual rotors or propellers used for propulsion. The noise generated by an open rotor is very complicated and requires special techniques for its analysis. The determination of its tone and broadband components is vital for properly assessing the noise control parameters and also for validating open rotor noise prediction codes. The data analysis technique developed by Sree for processing raw acoustic data of open rotors has been modified to yield much better results of tone and broadband separation particularly for the case when the two rotor speeds are approximately the same. The modified algorithm is found to eliminate most or all of the spikes previously observed in the broadband spectra computed from the original algorithm. A full description of the modified algorithm and examples of improved results from its application are presented in this paper. C1 [Sree, Dave] Tuskegee Univ, Dept Mech Engn, Tuskegee, AL 36088 USA. [Stephens, David B.] NASA, Acoust Branch, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Sree, D (reprint author), Tuskegee Univ, Dept Mech Engn, Tuskegee, AL 36088 USA. EM dave.sree@gmail.com; david.stephens@nasa.gov FU NASA Environmentally Responsible Aviation project; GE Aviation, Evendale, OH, USA; NASA Advanced Air Transportation Technology project FX Sincere thanks and appreciation are expressed to Acoustics Branch at NASA GRC for providing the non-proprietary open rotor acoustic data used in this work, in particular to Daniel L. Sutliff regarding the mini-open rotor data. The open rotor wind tunnel test campaign was funded by the NASA Environmentally Responsible Aviation project, in collaboration with GE Aviation, Evendale, OH, USA. The NASA Advanced Air Transportation Technology project funded David B. Stephens during the preparation of this report. NR 14 TC 0 Z9 0 U1 0 U2 0 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 2226-4310 J9 AEROSPACE JI Aerospace PD SEP PY 2016 VL 3 IS 3 AR 29 DI 10.3390/aerospace3030029 PG 15 WC Engineering, Aerospace SC Engineering GA DZ0LQ UT WOS:000385531300012 ER PT J AU Righter, K Sutton, SR Danielson, L Pando, K Newville, M AF Righter, Kevin Sutton, Steve R. Danielson, Lisa Pando, Kellye Newville, Matt TI Redox variations in the inner solar system with new constraints from vanadium XANES in spinels SO AMERICAN MINERALOGIST LA English DT Review DE Oxygen fugacity; meteorites; solar nebula; spinel; chromite; vanadium; Invited Centennial article ID INTERPLANETARY DUST PARTICLES; COMET 81P/WILD 2; OXYGEN FUGACITY; OXIDATION-STATE; CARBONACEOUS CHONDRITES; ENSTATITE CHONDRITES; MARTIAN BASALTS; ELECTROCHEMICAL MEASUREMENTS; THERMODYNAMIC CONSTRAINTS; LAYERED INTRUSION AB Many igneous rocks contain mineral assemblages that are not appropriate for application of common mineral equilibria or oxybarometers to estimate oxygen fugacity. Spinel-structured oxides, common minerals in 1916 z A 2016 many igneous rocks, typically contain sufficient V for XANES measurements, allowing use of the correlation between oxygen fugacity and V K pre-edge peak intensity. Here we report V pre-edge peak intensities for a wide range of spinels from source rocks ranging from terrestrial basalt to achondrites to oxidized chondrites. The XANES measurements are used to calculate oxygen fugacity from experimentally produced spinels of known f(o2). We obtain values, in order of increasing f(o2), from IW-3 for lodranites and acapulcoites, to diogenites, brachinites (near IW), ALH 84001, terrestrial basalt, hornblende-bearing R chondrite LAP 04840 (IW+1.6), and finally ranging up to IW+3.1 for CK chondrites (where the Delta IW notation = logf(o2), of a sample relative to the logf(o2), of the IW buffer at specific 7). To place the significance of these new measurements into context we then review the range of oxygen fugacities recorded in major achondrite groups, chondritic and primitive materials, and planetary materials. This range extends from IW-8 to IW+2. Several chondrite groups associated with aqueous alteration exhibit values that are slightly higher than this range, suggesting that water and oxidation may be linked. The range in planetary materials is even wider than that defined by meteorite groups. Earth and Mars exhibit values higher than IW+2, due to a critical role played by pressure. Pressure allows dissolution of volatiles into magmas, which can later cause oxidation or reduction during fractionation, cooling, and degassing. Fluid mobility, either in the sub-arc mantle and crust, or in regions of metasomatism, can generate values >IW+2, again suggesting an important link between water and oxidation. At the very least, Earth exhibits a higher range of oxidation than other planets and astromaterials due to the presence of an O-rich atmosphere, liquid water, and hydrated interior. New analytical techniques and sample suites will revolutionize our understanding of oxygen fugacity variation in the inner solar system, and the origin of our solar system in general. C1 [Righter, Kevin] NASA, JSC, NASA Pkwy, Houston, TX 77058 USA. [Sutton, Steve R.; Newville, Matt] Univ Chicago, GSECARS, 9700 South Cass Ave,Bldg 434A, Argonne, IL 60439 USA. [Danielson, Lisa; Pando, Kellye] Jacobs Engn, ESCG, Houston, TX 77058 USA. RP Righter, K (reprint author), NASA, JSC, NASA Pkwy, Houston, TX 77058 USA. EM kevin.righter-1@nasa.gov FU RTOP from the NASA Cosmochemistry/Emerging Worlds programs; National Science Foundation, Earth Sciences [EAR-1128799]; Department of Energy-GeoSciences [DE-FG02-94ER14466]; DOE Office of Science [DE-AC02-06CH11357] FX This work was supported by an RTOP from the NASA Cosmochemistry/Emerging Worlds programs. Portions of this work were performed at GeoSoilEnviroCARS (Sector 13), Advanced Photon Source (APS), Argonne National Laboratory. GeoSoilEnviroCARS is supported by the National Science Foundation, Earth Sciences (EAR-1128799) and Department of Energy-GeoSciences (DE-FG02-94ER14466). This research used resources of the Advanced Photon Source, a U.S. Department of Energy (DOE) Office of Science User Facility operated for the DOE Office of Science by Argonne National Laboratory under Contract No. DE-AC02-06CH11357. All meteorite samples were provided by the Meteorite Working Group except for the acapulcoites/lodranites (J. Herrin), GRA 06128 (A. Treiman), and ALH 84001 (M. Righter). The manuscript benefitted from the careful reviews and constructive comments of P. Burger, S. Paque, and AE S. Simon. We thank K. Putirka for the invitation to contribute a paper in celebration of the American Mineralogist centennial, and K.R. acknowledges the enormous and continuing influence the Mineralogical Society of America has had on his science and understanding of the natural world. NR 140 TC 1 Z9 1 U1 8 U2 8 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD SEP-OCT PY 2016 VL 101 IS 9-10 BP 1928 EP 1942 DI 10.2138/am-2016-5638 PG 15 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA DZ1NM UT WOS:000385605100003 ER PT J AU Lee, S Shen, ZZ Xu, HF AF Lee, Seungyeol Shen, Zhizhang Xu, Huifang TI Study on nanophase iron oxyhydroxides in freshwater ferromanganese nodules from Green Bay, Lake Michigan, with implications for the adsorption of As and heavy metals SO AMERICAN MINERALOGIST LA English DT Article DE XRD; HRTEM; Z-contrast imaging; ab initio; two-line ferrihydrite; proto-goethite; nanophase goethite; feroxyhyte; ferromanganese nodule; arsenic ID AB-INITIO; POWDER DIFFRACTION; STRUCTURAL MODEL; AKDALAITE MODEL; FERRIHYDRITE; SPECIATION; SEDIMENTS; MANGANESE; FEOOH; MN AB Nanophase Fe-oxyhydroxides in freshwater ferromanganese nodules (FFN) from Green Bay, Lake Michigan, and adsorbed arsenate have been investigated by X-ray powder diffraction (XRD), high-resolution transmission electron microscopy (HRTEM), Z-contrast imaging, and ab initio calculations using the density functional theory (DFT). The samples from northern Green Bay can be divided into two types: Fe-Mn nodules and Fe-rich nodules. The manganese-bearing phases are todorokite, birnessite, and buserite. The iron-bearing phases are feroxyhyte, nanophase goethite, two-line ferrihydrite, and nanophase FeOOH with guyanaite structure. Z-contrast images of the Fe-oxyhydroxides show ordered FeOOH nano-domains with guyanaite structure intergrown with nanophase goethite. The FeOOH nanophase is a precursor to the goethite. Henceforth, we will refer to it as "proto-goethite." DFT calculations indicate that goethite is more stable than proto-goethite. Our results suggest that ordering between Fe and vacancies in octahedral sites result in the transformation from feroxyhyte to goethite through a proto-goethite intermediate phase. Combining Z-contrast images and TEM-EDS reveals that arsenate (AsO43-) tetrahedra are preferentially adsorbed on the proto-goethite (001) surface via tridentate adsorption. Our study directly shows the atomic positions of Fe-oxyhydroxides with associated trace elements. The methods can be applied for identifying structures of nano-phases and adsorbed trace elements and heavy metals. C1 [Lee, Seungyeol; Shen, Zhizhang; Xu, Huifang] Univ Wisconsin, NASA, Astrobiol Inst, Dept Geosci, Madison, WI 53706 USA. RP Xu, HF (reprint author), Univ Wisconsin, NASA, Astrobiol Inst, Dept Geosci, Madison, WI 53706 USA. EM hfxu@geology.wisc.edu FU NASA Astrobiology Institute [N07-5489] FX The authors acknowledge the financial support from NASA Astrobiology Institute (N07-5489). The authors thank Carl Bowser for providing the samples and their locations, Hiromi Konishi for assistance in acquiring Z-contrast images, Izabela Szlufarska for allowing us to access computing facility, Gabor J. Kemeny of Middleton Spectral Vision and Michael Beauchaine of Bruker AXS for XRF mapping. The authors also thank Philip E. Brown, John W. Valley, Clark M. Johnson, Eric E. Roden, and Franklin Hobbs for their helpful suggestions. NR 53 TC 1 Z9 1 U1 8 U2 8 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD SEP-OCT PY 2016 VL 101 IS 9-10 BP 1986 EP 1995 DI 10.2138/am-2016-5729 PG 10 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA DZ1NM UT WOS:000385605100007 ER PT J AU Chan, QHS Zolensky, ME Martinez, JE Tsuchiyama, A Miyake, A AF Chan, Queenie H. S. Zolensky, Michael E. Martinez, James E. Tsuchiyama, Akira Miyake, Akira TI Magnetite plaquettes are naturally asymmetric materials in meteorites SO AMERICAN MINERALOGIST LA English DT Article DE Magnetite; plaquettes; carbonaceous chondrites; symmetry-breaking; scanning electron microscopy; SEM; electron backscatter diffraction; EBSD; synchrotron X-ray computed microtomography; SXRCT; aqueous alteration; crystal structure ID EXTRATERRESTRIAL AMINO-ACIDS; CARBONACEOUS CHONDRITE; TAGISH LAKE; ADSORPTION; HOMOCHIRALITY; MINERALOGY; EVOLUTION; CRYSTALS; PARTICLES; CHEMISTRY AB Life on Earth shows preference toward the set of organics with particular spatial configurations. Enantiomeric excesses have been observed for a-methyl amino acids in meteorites, which suggests that chiral asymmetry might have an abiotic origin. A possible abiotic mechanism that could produce chiral asymmetry in meteoritic amino acids is their formation under the influence of asymmetric catalysts, as mineral crystallization can produce spatially asymmetric structures. Although magnetite plaquettes have been proposed to be a possible candidate for an asymmetric catalyst, based on the suggestion that they have a spiral structure, a comprehensive description of their morphology and interpretation of the mechanism associated with symmetry-breaking in biomolecules remain elusive. Here we report observations of magnetite plaquettes in carbonaceous chondrites (CC) that were made with scanning electron microscopy and synchrotron X-ray computed microtomography (SXRCT). We obtained the crystal orientation of the plaquettes using electron backscatter diffraction (EBSD) analysis. SXRCT permits visualization of the internal features of the plaquettes. It provides an unambiguous conclusion that the plaquettes are devoid of a spiral feature and, rather that they are stacks of individual magnetite disks that do not join to form a continuous spiral. Despite the lack of spiral features, our EBSD data show significant changes in crystal orientation between adjacent magnetite disks. The magnetite disks are displaced in a consistent relative direction that lead to an overall crystallographic rotational mechanism. This work offers an explicit understanding of the structures of magnetite plaquettes in CC, which provides a fundamental basis for future interpretation of the proposed symmetry-breaking mechanism. C1 [Chan, Queenie H. S.; Zolensky, Michael E.] NASA, ARES, Johnson Space Ctr, Houston, TX 77058 USA. [Martinez, James E.] Jacobs Engn, Houston, TX 77058 USA. [Tsuchiyama, Akira; Miyake, Akira] Kyoto Univ, Grad Sch Sci, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan. RP Chan, QHS (reprint author), NASA, ARES, Johnson Space Ctr, Houston, TX 77058 USA. EM hschan@nasa.gov FU NASA Cosmochemistry Program; NASA Postdoctoral Program at the Johnson Space Center; Japan Ministry of Education, Culture, Sports, Science and Technology [15H05695] FX We acknowledge CAPTEM for loan of the Bench Crater sample, which is an Apollo lunar sample. We thank Field Museum for Orgueil, Murchison, Mighei, Renazzo, National Museum of Natural History for the Alais meteorite sample, and American Museum of Natural History for the Ivuna sample. This study was supported by the NASA Cosmochemistry Program (M.E.Z. is the PI). Q.H.S.C. acknowledges support from the NASA Postdoctoral Program at the Johnson Space Center, administered by the Universities Space Research Association. A.T. was supported by a Grant-in-aid of the Japan Ministry of Education, Culture, Sports, Science and Technology (15H05695). We thank Tomoki Nakamura, John Bradley, and Rhian Jones for careful reviews of the manuscript, and Sandra Pizzarello, Jose Aponte, and Aaron Burton for the helpful comments and insightful discussions. The microtomography experiment was made by the project at SPring-8 (proposal no. 2015A1413) with help of Kentaro Uesugi and Tsukasa Nakano. NR 58 TC 0 Z9 0 U1 4 U2 4 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD SEP-OCT PY 2016 VL 101 IS 9-10 BP 2041 EP 2050 DI 10.2138/am-2016-5604 PG 10 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA DZ1NM UT WOS:000385605100012 ER PT J AU Gullikson, AL Hagerty, JJ Reid, MR Rapp, JF Draper, DS AF Gullikson, Amber L. Hagerty, Justin J. Reid, Mary R. Rapp, Jennifer F. Draper, David S. TI Silicic lunar volcanism: Testing the crustal melting model SO AMERICAN MINERALOGIST LA English DT Article DE Moon; silicic volcanism; crustal melting; partial melting experiments; silicate liquid immiscibility ID LIQUID IMMISCIBILITY; QUARTZ MONZODIORITE; MAIRAN DOMES; MOON; GRANITE; PETROLOGY; GEOCHEMISTRY; GRUITHUISEN; CHEMISTRY; ROCKS AB Lunar silicic rocks were first identified by granitic fragments found in samples brought to Earth by the Apollo missions, followed by the discovery of silicic domes on the lunar surface through remote sensing. Although these silicic lithologies are thought to make up a small portion of the lunar crust, their presence indicates that lunar crustal evolution is more complex than originally thought. Models currently used to describe the formation of silicic lithologies on the Moon include in situ differentiation of a magma, magma differentiation with silicate liquid immiscibility, and partial melting of the crust. This study focuses on testing a crustal melting model through partial melting experiments on compositions representing lithologies spatially associated with the silicic domes. The experiments were guided by the results of modeling melting temperatures and residual melt compositions of possible protoliths for lunar silicic rocks using the thermodynamic modeling software, rhyolite-MELTS. Rhyolite-MELTS simulations predict liquidus temperatures of 950-1040 degrees C for lunar granites under anhydrous conditions, which guided the temperature range for the experiments. Monzogabbro, alkali gabbronorite, and KREEP basalt were identified as potential protoliths due to their ages, locations on the Moon (i.e., located near observed silicic domes), chemically evolved compositions, and the results from rhyolite-MELTS modeling. Partial melting experiments, using mixtures of reagent grade oxide powders representing bulk rock compositions of these rock types, were carried out at atmospheric pressure over the temperature range of 900-1100 degrees C. Because all lunar granite samples and remotely sensed domes have an elevated abundance of Th, some of the mixtures were doped with Th to observe its partitioning behavior. Run products show that at temperatures of 1050 and 1100 degrees C, melts of the three protoliths are not silicic in nature (i.e., they have <63 wt% SiO2). By 1000 degrees C, melts of both monzogabbro and alkali gabbronorite approach the composition of granite, but are also characterized by immiscible Si-rich and Fe-rich liquids. Furthermore, Th strongly partitions into the Fe-rich, and not the Si-rich glass in all experimental runs. Our work provides important constraints on the mechanism of silicic melt formation on the Moon. The observed high-Th content of lunar granite is difficult to explain by silicate liquid immiscibility, because through this process, Th is not fractionated into the Si-rich phase. Results of our experiments and modeling suggests that silicic lunar rocks could be produced from monzogabbro and alkali gabbronorite protoliths by partial melting at T < 1000 degrees C. Additionally, we speculate that at higher pressures (P >= 0.005 GPa), the observed immiscibility in the partial melting experiments would be suppressed. C1 [Gullikson, Amber L.; Reid, Mary R.] Northern Univ Arizona, Flagstaff, AZ 86011 USA. [Hagerty, Justin J.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Rapp, Jennifer F.] NASA, Johnson Space Ctr, Jacobs, Mail Code JE20, Houston, TX 77058 USA. [Draper, David S.] NASA, Astromat Res Off, ARES Directorate, Johnson Space Ctr, Houston, TX USA. RP Gullikson, AL (reprint author), Northern Univ Arizona, Flagstaff, AZ 86011 USA. EM agullikson@usgs.gov FU Geological Society of America; Sigma Xi; NAU Support for Graduate Students program; Tom and Rose Bedwell Earth Physics Scholarship FX We thank Brad Jolliff and Malcolm Rutherford for their insightful comments, which greatly improved this paper. Funding for this work was provided by the Geological Society of America research grant, Sigma Xi Grants-in-Aid Research, the NAU Support for Graduate Students program, and the Tom and Rose Bedwell Earth Physics Scholarship. NR 68 TC 0 Z9 0 U1 6 U2 6 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD SEP-OCT PY 2016 VL 101 IS 9-10 BP 2312 EP 2321 DI 10.2138/am-2016-5619 PG 10 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA DZ1NM UT WOS:000385605100034 ER PT J AU Singer, LP Chen, HY Holz, DE Farr, WM Price, LR Raymond, V Cenko, SB Gehrels, N Cannizzo, J Kasliwal, MM Nissanke, S Coughlin, M Farr, B Urban, AL Vitale, S Veitch, J Graff, P Berry, CPL Mohapatra, S Mandel, I AF Singer, Leo P. Chen, Hsin-Yu Holz, Daniel E. Farr, Will M. Price, Larry R. Raymond, Vivien Cenko, S. Bradley Gehrels, Neil Cannizzo, John Kasliwal, Mansi M. Nissanke, Samaya Coughlin, Michael Farr, Ben Urban, Alex L. Vitale, Salvatore Veitch, John Graff, Philip Berry, Christopher P. L. Mohapatra, Satya Mandel, Ilya TI SUPPLEMENT: "GOING THE DISTANCE: MAPPING HOST GALAXIES OF LIGO AND VIRGO SOURCES IN THREE DIMENSIONS USING LOCAL COSMOGRAPHY AND TARGETED FOLLOW-UP" (2016, ApJL, 829, L15) SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; galaxies: distances and redshifts; gravitational waves; surveys AB This is a supplement to the Letter of Singer et al., in which we demonstrated a rapid algorithm for obtaining joint 3D estimates of sky location and luminosity distance from observations of binary neutron star mergers with Advanced LIGO and Virgo. We argued that combining the reconstructed volumes with positions and redshifts of possible host galaxies can provide large-aperture but small field of view instruments with a manageable list of targets to search for optical or infrared emission. In this Supplement, we document the new HEALPix-based file format for 3D localizations of gravitational-wave transients. We include Python sample code to show the reader how to perform simple manipulations of the 3D sky maps and extract ranked lists of likely host galaxies. Finally, we include mathematical details of the rapid volume reconstruction algorithm. C1 [Singer, Leo P.; Cenko, S. Bradley; Gehrels, Neil; Cannizzo, John] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Mail Code 661, Greenbelt, MD 20771 USA. [Chen, Hsin-Yu; Holz, Daniel E.; Farr, Ben] Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA. [Chen, Hsin-Yu; Holz, Daniel E.; Farr, Ben] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Farr, Will M.; Veitch, John; Berry, Christopher P. L.; Mandel, Ilya] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Price, Larry R.; Raymond, Vivien] CALTECH, LIGO Lab, Pasadena, CA 91125 USA. [Raymond, Vivien] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Potsdam, Germany. [Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Kasliwal, Mansi M.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Nissanke, Samaya] Radboud Univ Nijmegen, Inst Math Astrophys & Particle Phys, Heyendaalseweg 135, NL-6525 AJ Nijmegen, Netherlands. [Coughlin, Michael] Harvard Univ, Dept Phys & Astron, Cambridge, MA 02138 USA. [Urban, Alex L.] Univ Wisconsin, Leonard E Parker Ctr Gravitat Cosmol & Astrophys, Milwaukee, WI 53201 USA. [Vitale, Salvatore; Mohapatra, Satya] MIT, LIGO Lab, 185 Albany St, Cambridge, MA 02139 USA. [Graff, Philip] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. RP Singer, LP (reprint author), NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Mail Code 661, Greenbelt, MD 20771 USA. OI Singer, Leo/0000-0001-9898-5597; Chen, Hsin-Yu/0000-0001-5403-3762 FU NSF [1066293] FX We thank the Aspen Center for Physics and NSF grant #1066293 for hospitality during the conception, writing, and editing of this paper. We thank P. Shawhan and F. Tombesi for detailed feedback on the manuscript. The online data release is available at https://dcc.ligo.org/P1500071/public/html. This is LIGO document P1500071-v7. NR 16 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2016 VL 226 IS 1 AR 10 DI 10.3847/0067-0049/226/1/10 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY8SH UT WOS:000385400500001 ER PT J AU Jensen, MP Petersen, WA Bansemer, A Bharadwaj, N Carey, LD Cecil, DJ Collis, SM Del Genio, AD Dolan, B Gerlach, J Giangrande, SE Heymsfield, A Heymsfield, G Kollias, P Lang, TJ Nesbitt, SW Neumann, A Poellot, M Rutledge, SA Schwaller, M Tokay, A Williams, CR Wolff, DB Xie, S Zipser, EJ AF Jensen, M. P. Petersen, W. A. Bansemer, A. Bharadwaj, N. Carey, L. D. Cecil, D. J. Collis, S. M. Del Genio, A. D. Dolan, B. Gerlach, J. Giangrande, S. E. Heymsfield, A. Heymsfield, G. Kollias, P. Lang, T. J. Nesbitt, S. W. Neumann, A. Poellot, M. Rutledge, S. A. Schwaller, M. Tokay, A. Williams, C. R. Wolff, D. B. Xie, S. Zipser, E. J. TI THE MIDLATITUDE CONTINENTAL CONVECTIVE CLOUDS EXPERIMENT (MC3E) SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID RADIATION MEASUREMENT PROGRAM; ATMOSPHERIC RADIATION; POLARIMETRIC RADAR; WIND PROFILERS; PRECIPITATION; RADIOMETER; RESOLUTION; MESOSCALE; SYSTEMS; GHZ AB The Midlatitude Continental Convective Clouds Experiment (MC3E), a field program jointly led by the U.S. Department of Energy's Atmospheric Radiation Measurement (ARM) Program and the National Aeronautics and Space Administration's (NASA) Global Precipitation Measurement (GPM) mission, was conducted in south-central Oklahoma during April-May 2011. MC3E science objectives were motivated by the need to improve our understanding of midlatitude continental convective cloud system life cycles, microphysics, and GPM precipitation retrieval algorithms. To achieve these objectives, a multi scale surface- and aircraft-based in situ and remote sensing observing strategy was employed. A variety of cloud and precipitation events were sampled during MC3E, of which results from three deep convective events are highlighted. Vertical structure, air motions, precipitation drop size distributions, and ice properties were retrieved from multiwavelength radar, profiler, and aircraft observations for a mesoscale convective system (MCS) on 11 May. Aircraft observations for another MCS observed on 20 May were used to test agreement between observed radar reflectivities and those calculated with forward-modeled reflectivity and microwave brightness temperatures using in situ particle size distributions and ice water content. Multiplatform observations of a supercell that occurred on 23 May allowed for an integrated analysis of kinematic and microphysical interactions. A core updraft of 25 m supported growth of hail and large raindrops. Data collected during the MC3E campaign are being used in a number of current and ongoing research projects and are available through the ARM and NASA data archives. C1 [Jensen, M. P.; Giangrande, S. E.] Brookhaven Natl Lab, POB 5000,MS 490D, Upton, NY 11973 USA. [Petersen, W. A.; Gerlach, J.; Heymsfield, G.; Schwaller, M.; Tokay, A.; Wolff, D. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Petersen, W. A.; Gerlach, J.; Wolff, D. B.] NASA, Wallops Flight Facil, Wallops Isl, VA USA. [Bansemer, A.; Heymsfield, A.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. [Bharadwaj, N.] Pacific Northwest Natl Lab, Richland, WA USA. [Carey, L. D.] Univ Alabama, Huntsville, AL 35899 USA. [Cecil, D. J.; Lang, T. J.] NASA, Marshall Space Flight Ctr, Huntsville, AL USA. [Collis, S. M.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA. [Del Genio, A. D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Dolan, B.; Rutledge, S. A.] Colorado State Univ, Ft Collins, CO 80523 USA. [Kollias, P.] McGill Univ, Montreal, PQ, Canada. [Nesbitt, S. W.] Univ Illinois, Urbana, IL USA. [Neumann, A.; Poellot, M.] Univ North Dakota, Grand Forks, ND USA. [Tokay, A.] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. [Williams, C. R.] Univ Colorado, Boulder, CO 80309 USA. [Xie, S.] Lawrence Livermore Natl Lab, Livermore, CA USA. [Zipser, E. J.] Univ Utah, Salt Lake City, UT USA. RP Jensen, MP (reprint author), Brookhaven Natl Lab, POB 5000,MS 490D, Upton, NY 11973 USA. EM mjensen@bnl.gov RI Xie, Shaocheng/D-2207-2013 OI Xie, Shaocheng/0000-0001-8931-5145 FU U.S. Department of Energy's ARM Program; NASA's Global Precipitation Measurement mission's Ground Validation Program; NASA [NNX10AN38G, NNX10AH67G, NNX14AH06G]; U.S. Department of Energy, Office of Science, Office of Biological and Environmental Research (BER), as part of the Atmospheric System Research (ASR) program; U.S. Department of Energy, Office of Science, Office of Biological and Environmental Research (BER), as part of the ARM program; DOE [DE-SC0007016]; U.S. Department of Energy [DE-AC02-98CH10886] FX The MC3E field campaign was jointly funded by the U.S. Department of Energy's ARM Program and NASA's Global Precipitation Measurement mission's Ground Validation Program. We acknowledge the important contributions of the ARM SGP site operations staff members for their contributions to the siting, deployment, and maintenance of NASA MC3E and SGP ARM Climate Facility instrumentation. We also acknowledge the UND Citation flight and support crews for their excellent conduct of airborne microphysical sampling, and Offutt AFB and Ponca City Regional Airport for their hosting and field support of the NASA ER-2 and UND Citation, respectively. Operations of the UND Citation aircraft were funded under NASA Grant NNX10AN38G. MJ and SG were funded by the U.S. Department of Energy, Office of Science, Office of Biological and Environmental Research (BER), as part of the Atmospheric System Research (ASR) and ARM programs. AH and AB were funded by NASA Grant NNX10AH67G. SR and BD were funded by DOE Grant DE-SC0007016 and NASA Grant NNX14AH06G. This paper has been coauthored by employees of Brookhaven Science Associates, LLC, under Contract DE-AC02-98CH10886 with the U.S. Department of Energy. NR 56 TC 10 Z9 10 U1 6 U2 6 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD SEP PY 2016 VL 97 IS 9 BP 1667 EP + DI 10.1175/BAMS-D-14-00228.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DZ5PG UT WOS:000385913400016 ER PT J AU Wood, R Jensen, MP Wang, J Bretherton, CS Burrows, SM Del Genio, AD Fridlind, AM Ghan, SJ Ghate, VP Kollias, P Krueger, SK McGraw, RL Miller, MA Painemal, D Russell, LM Yuter, SE Zuidema, P AF Wood, Robert Jensen, Michael P. Wang, Jian Bretherton, Christopher S. Burrows, Susannah M. Del Genio, Anthony D. Fridlind, Ann M. Ghan, Steven J. Ghate, Virendra P. Kollias, Pavlos Krueger, Steven K. McGraw, Robert L. Miller, Mark A. Painemal, David Russell, Lynn M. Yuter, Sandra E. Zuidema, Paquita TI PLANNING THE NEXT DECADE OF COORDINATED RESEARCH TO BETTER UNDERSTAND AND SIMULATE MARINE LOW CLOUDS SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Editorial Material ID STRATOCUMULUS C1 [Wood, Robert; Bretherton, Christopher S.] Univ Washington, Seattle, WA 98195 USA. [Jensen, Michael P.; Wang, Jian; McGraw, Robert L.] Brookhaven Natl Lab, Upton, NY 11973 USA. [Burrows, Susannah M.; Ghan, Steven J.] Pacific Northwest Natl Lab, Richland, WA USA. [Del Genio, Anthony D.; Fridlind, Ann M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Ghate, Virendra P.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA. [Kollias, Pavlos] SUNY Stony Brook, Stony Brook, NY 11794 USA. [Krueger, Steven K.] Univ Utah, Salt Lake City, UT USA. [Miller, Mark A.] Rutgers State Univ, New Brunswick, NJ USA. [Painemal, David] NASA, Langley Res Ctr, Sci Syst & Applicat Inc, Hampton, VA 23665 USA. [Russell, Lynn M.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Yuter, Sandra E.] North Carolina State Univ, Raleigh, NC USA. [Zuidema, Paquita] Univ Miami, Miami, FL USA. RP Wood, R (reprint author), Univ Washington, Dept Atmospher Sci, Box 351640, Seattle, WA 98195 USA. EM robwood2@uw.edu RI Ghan, Steven/H-4301-2011; Zuidema, Paquita/C-9659-2013; Wang, Jian/G-9344-2011; Burrows, Susannah/A-7429-2011; Wood, Robert/A-2989-2008 OI Ghan, Steven/0000-0001-8355-8699; Zuidema, Paquita/0000-0003-4719-372X; Burrows, Susannah/0000-0002-0745-7252; Wood, Robert/0000-0002-1401-3828 NR 12 TC 0 Z9 0 U1 5 U2 5 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD SEP PY 2016 VL 97 IS 9 BP 1699 EP 1702 DI 10.1175/BAMS-D-16-0160.1 PG 4 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DZ5PG UT WOS:000385913400018 ER PT J AU Ichoku, C Ellison, LT Willmot, KE Matsui, T Dezfuli, AK Gatebe, CK Wang, J Wilcox, EM Lee, J Adegoke, J Okonkwo, C Bolten, J Policelli, FS Habib, S AF Ichoku, Charles Ellison, Luke T. Willmot, K. Elena Matsui, Toshihisa Dezfuli, Amin K. Gatebe, Charles K. Wang, Jun Wilcox, Eric M. Lee, Jejung Adegoke, Jimmy Okonkwo, Churchill Bolten, John Policelli, Frederick S. Habib, Shahid TI Biomass burning, land-cover change, and the hydrological cycle in Northern sub-Saharan Africa SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE sub-Saharan Africa; biomass burning; water cycle; land cover change; precipitation; fire ID WESTERN EQUATORIAL AFRICA; FIRE DETECTION; CLIMATE-CHANGE; RAINFALL VARIABILITY; TROPICAL OCEANS; SAHEL RAINFALL; SOIL-MOISTURE; LAKE CHAD; PART I; SURFACE AB The Northern Sub-Saharan African (NSSA) region, which accounts for 20%-25% of the global carbon emissions from biomass burning, also suffers from frequent drought episodes and other disruptions to the hydrological cycle whose adverse societal impacts have been widely reported during the last several decades. This paper presents a conceptual framework of the NSSA regional climate system components that may be linked to biomass burning, as well as detailed analyses of a variety of satellite data for 2001-2014 in conjunction with relevant model-assimilated variables. Satellite fire detections in NSSA show that the vast majority (>75%) occurs in the savanna and woody savanna land-cover types. Starting in the 2006-2007 burning season through the end of the analyzed data in 2014, peak burning activity showed a net decrease of 2-7%/yr in different parts of NSSA, especially in the savanna regions. However, fire distribution shows appreciable coincidence with land-cover change. Although there is variable mutual exchange of different land cover types, during 2003-2013, cropland increased at an estimated rate of 0.28%/yr of the total NSSA land area, with most of it (0.18%/yr) coming from savanna. During the last decade, conversion to croplands increased in some areas classified as forests and wetlands, posing a threat to these vital and vulnerable ecosystems. Seasonal peak burning is anti-correlated with annual water-cycle indicators such as precipitation, soil moisture, vegetation greenness, and evapotranspiration, except in humid West Africa (5 degrees-10 degrees latitude), where this anti-correlation occurs exclusively in the dry season and burning virtually stops when monthly mean precipitation reaches 4 mm d(-1). These results provide observational evidence of changes in land-cover and hydrological variables that are consistent with feedbacks from biomass burning in NSSA, and encourage more synergistic modeling and observational studies that can elaborate this feedback mechanism. C1 [Ichoku, Charles; Ellison, Luke T.; Matsui, Toshihisa; Dezfuli, Amin K.; Gatebe, Charles K.; Bolten, John; Policelli, Frederick S.; Habib, Shahid] NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA. [Ellison, Luke T.] Sci Syst & Applicat Inc, Lanham, MD USA. [Willmot, K. Elena] Vanderbilt Univ, Nashville, TN 37235 USA. [Matsui, Toshihisa] Univ Maryland, ESSIC, College Pk, MD 20742 USA. [Dezfuli, Amin K.; Gatebe, Charles K.] USRA, Columbia, MD USA. [Wang, Jun] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE USA. [Wang, Jun] Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA 52242 USA. [Wang, Jun] Univ Iowa, Dept Chem & Biochem Engn, Iowa City, IA 52242 USA. [Wilcox, Eric M.] Desert Res Inst, Reno, NV USA. [Lee, Jejung; Adegoke, Jimmy] Univ Missouri, Kansas City, MO 64110 USA. [Okonkwo, Churchill] Howard Univ, Beltsville Ctr Climate Syst Observat, Washington, DC 20059 USA. RP Ichoku, C (reprint author), NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA. EM Charles.Ichoku@nasa.gov RI Wang, Jun/A-2977-2008 OI Wang, Jun/0000-0002-7334-0490 FU NASA under its Research Opportunities in Space and Earth Sciences (ROSES) through the Radiation Sciences Program; NASA under its Interdisciplinary Studies (IDS) Program through the Radiation Sciences Program FX This research was fully funded by NASA under its Research Opportunities in Space and Earth Sciences (ROSES)-2009 and 2013 Interdisciplinary Studies (IDS) Program (Dr Jack Kaye, Earth Science Research Director) through the Radiation Sciences Program managed by Dr Hal Maring. We also appreciate the efforts of providers of the large diversity of data products used for this study from various satellite sensors and global models. NR 72 TC 1 Z9 1 U1 15 U2 15 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 SEP PY 2016 VL 11 IS 9 AR 095005 DI 10.1088/1748-9326/11/9/095005 PG 13 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA DY8PW UT WOS:000385393300001 ER PT J AU Marchand, P Carr, JA Dell'Angelo, J Fader, M Gephart, JA Kummu, M Magliocca, NR Porkka, M Puma, MJ Ratajczak, Z Rulli, MC Seekell, DA Suweis, S Tavoni, A D'Odorico, P AF Marchand, Philippe Carr, Joel A. Dell'Angelo, Jampel Fader, Marianela Gephart, Jessica A. Kummu, Matti Magliocca, Nicholas R. Porkka, Miina Puma, Michael J. Ratajczak, Zak Rulli, Maria Cristina Seekell, David A. Suweis, Samir Tavoni, Alessandro D'Odorico, Paolo TI Reserves and trade jointly determine exposure to food supply shocks SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Letter DE food systems; resilience; food crises ID LAND-USE; INTERNATIONAL-TRADE; AGRICULTURAL TRADE; GLOBALIZATION; DISPLACEMENT; SECURITY; NATIONS; WATER AB While a growing proportion of global food consumption is obtained through international trade, there is an ongoing debate on whether this increased reliance on trade benefits or hinders food security, and specifically, the ability of global food systems to absorb shocks due to local or regional losses of production. This paper introduces a model that simulates the short-term response to a food supply shock originating in a single country, which is partly absorbed through decreases in domestic reserves and consumption, and partly transmitted through the adjustment of trade flows. By applying the model to publicly-available data for the cereals commodity group over a 17 year period, we find that differential outcomes of supply shocks simulated through this time period are driven not only by the intensification of trade, but as importantly by changes in the distribution of reserves. Our analysis also identifies countries where trade dependency may accentuate the risk of food shortages from foreign production shocks; such risk could be reduced by increasing domestic reserves or importing food from a diversity of suppliers that possess their own reserves. This simulation-based model provides a framework to study the short-term, nonlinear and out-of-equilibrium response of trade networks to supply shocks, and could be applied to specific scenarios of environmental or economic perturbations. C1 [Marchand, Philippe; Dell'Angelo, Jampel; Magliocca, Nicholas R.; D'Odorico, Paolo] Natl Socioenvironm Synth Ctr SESYNC, Annapolis, MD 21401 USA. [Carr, Joel A.; Gephart, Jessica A.; Ratajczak, Zak; D'Odorico, Paolo] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. [Fader, Marianela] German Fed Inst Hydrol, Int Ctr Water Resources & Global Change UNESCO, POB 200253, D-56002 Koblenz, Germany. [Kummu, Matti; Porkka, Miina] Aalto Univ, WDRG, FI-00076 Aalto, Finland. [Puma, Michael J.] Columbia Univ, Ctr Climate Syst Res, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Rulli, Maria Cristina] Politecn Milan, Dept Hydraul Roadways Environm & Surveying Engn, I-20133 Milan, Italy. [Seekell, David A.] Umea Univ, Dept Ecol & Environm Sci, SE-90187 Ume, Sweden. [Suweis, Samir] Univ Padua, Dept Phys & Astron, I-35131 Padua, Italy. [Tavoni, Alessandro] London Sch Econ, Grantham Res Inst Climate Change & Environm, London WC2A 2AE, England. RP Marchand, P (reprint author), Natl Socioenvironm Synth Ctr SESYNC, Annapolis, MD 21401 USA. NR 44 TC 0 Z9 0 U1 3 U2 3 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 SEP PY 2016 VL 11 IS 9 AR 095009 DI 10.1088/1748-9326/11/9/095009 PG 11 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA DZ2XT UT WOS:000385707100001 ER PT J AU Marchand, P Carr, JA Dell'Angelo, J Fader, M Gephart, JA Kummu, M Magliocca, NR Porkka, M Puma, MJ Ratajczak, Z Rulli, MC Seekell, DA Suweis, S Tavoni, A D'Odorico, P AF Marchand, Philippe Carr, Joel A. Dell'Angelo, Jampel Fader, Marianela Gephart, Jessica A. Kummu, Matti Magliocca, Nicholas R. Porkka, Miina Puma, Michael J. Ratajczak, Zak Rulli, Maria Cristina Seekell, David A. Suweis, Samir Tavoni, Alessandro D'Odorico, Paolo TI Reserves and trade jointly determine exposure to food supply shocks SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE food systems; resilience; food crises ID LAND-USE; INTERNATIONAL-TRADE; AGRICULTURAL TRADE; GLOBALIZATION; DISPLACEMENT; SECURITY; NATIONS; WATER AB While a growing proportion of global food consumption is obtained through international trade, there is an ongoing debate on whether this increased reliance on trade benefits or hinders food security, and specifically, the ability of global food systems to absorb shocks due to local or regional losses of production. This paper introduces a model that simulates the short-term response to a food supply shock originating in a single country, which is partly absorbed through decreases in domestic reserves and consumption, and partly transmitted through the adjustment of trade flows. By applying the model to publicly-available data for the cereals commodity group over a 17 year period, we find that differential outcomes of supply shocks simulated through this time period are driven not only by the intensification of trade, but as importantly by changes in the distribution of reserves. Our analysis also identifies countries where trade dependency may accentuate the risk of food shortages from foreign production shocks; such risk could be reduced by increasing domestic reserves or importing food from a diversity of suppliers that possess their own reserves. This simulation-based model provides a framework to study the short-term, nonlinear and out-of-equilibrium response of trade networks to supply shocks, and could be applied to specific scenarios of environmental or economic perturbations. C1 [Marchand, Philippe; Dell'Angelo, Jampel; Magliocca, Nicholas R.; D'Odorico, Paolo] Natl Socioenvironm Synth Ctr SESYNC, Annapolis, MD 21401 USA. [Carr, Joel A.; Gephart, Jessica A.; Ratajczak, Zak; D'Odorico, Paolo] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. [Fader, Marianela] German Fed Inst Hydrol, Int Ctr Water Resources & Global Change UNESCO, POB 200253, D-56002 Koblenz, Germany. [Kummu, Matti; Porkka, Miina] Aalto Univ, WDRG, FI-00076 Aalto, Finland. [Puma, Michael J.] Columbia Univ, Ctr Climate Syst Res, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Rulli, Maria Cristina] Politecn Milan, Dept Hydraul Roadways Environm & Surveying Engn, I-20133 Milan, Italy. [Seekell, David A.] Umea Univ, Dept Ecol & Environm Sci, SE-90187 Umea, Sweden. [Suweis, Samir] Univ Padua, Dept Phys & Astron, I-35131 Padua, Italy. [Tavoni, Alessandro] London Sch Econ, Grantham Res Inst Climate Change & Environm, London WC2A 2AE, England. RP Marchand, P (reprint author), Natl Socioenvironm Synth Ctr SESYNC, Annapolis, MD 21401 USA. RI Kummu, Matti/C-4797-2011 OI Kummu, Matti/0000-0001-5096-0163 FU National Socio-Environmental Synthesis Center (SESYNC) under National Science Foundation (NSF) [DBI-1052875]; Academy of Finland SRC project Winland; Academy of Finland project SCART; Columbia University Center for Climate and Life; Interdisciplinary Global Change Research under NASA [NNX08AJ75A]; Carl Trygger Foundation for Scientific Research; NSF [DBI-1402033]; Centre for Climate Change Economics and Policy - ESRC; Grantham Foundation for the Protection of the Environment FX We thank Roberto Patricio Korzeniewicz and Christina Prell for their participation in early discussions on this project. This work was supported by the National Socio-Environmental Synthesis Center (SESYNC) under funding received from the National Science Foundation (NSF) grant DBI-1052875. M Kummu received support from Academy of Finland SRC project Winland and Academy of Finland project SCART. M J Puma is supported by a fellowship from the Columbia University Center for Climate and Life and the Interdisciplinary Global Change Research under NASA cooperative agreement NNX08AJ75A. D A Seekell was supported by the Carl Trygger Foundation for Scientific Research. Z Ratajczak received support from NSF grant DBI-1402033. A Tavoni is supported by the Centre for Climate Change Economics and Policy, funded by the ESRC, and the Grantham Foundation for the Protection of the Environment. NR 44 TC 0 Z9 0 U1 4 U2 4 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 SEP PY 2016 VL 11 IS 9 AR 095009 DI 10.1088/1748-9326/11/9/095009 PG 11 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA DY8PW UT WOS:000385393300005 ER PT J AU Sedano, F Silva, JA Machoco, R Meque, CH Sitoe, A Ribeiro, N Anderson, K Ombe, ZA Baule, SH Tucker, CJ AF Sedano, F. Silva, J. A. Machoco, R. Meque, C. H. Sitoe, A. Ribeiro, N. Anderson, K. Ombe, Z. A. Baule, S. H. Tucker, C. J. TI The impact of charcoal production on forest degradation: a case study in Tete, Mozambique SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE forest degradation; charcoal; carbon emissions; remote sensing; very high-resolution; Africa ID DEVELOPING-COUNTRIES; DEVELOPING-WORLD; DEFORESTATION; IMAGERY; POLICY; LIVELIHOODS; EMISSIONS; AFRICA; MAPS AB Charcoal production for urban energy consumption is a main driver of forest degradation in sub Saharan Africa. Urban growth projections for the continent suggest that the relevance of this process will increase in the coming decades. Forest degradation associated to charcoal production is difficult to monitor and commonly overlooked and underrepresented in forest cover change and carbon emission estimates. We use a multitemporal dataset of very high-resolution remote sensing images to map kiln locations in a representative study area of tropical woodlands in central Mozambique. The resulting maps provided a characterization of the spatial extent and temporal dynamics of charcoal production. Using an indirect approach we combine kiln maps and field information on charcoal making to describe the magnitude and intensity of forest degradation linked to charcoal production, including aboveground biomass and carbon emissions. Our findings reveal that forest degradation associated to charcoal production in the study area is largely independent from deforestation driven by agricultural expansion and that its impact on forest cover change is in the same order of magnitude as deforestation. Our work illustrates the feasibility of using estimates of urban charcoal consumption to establish a link between urban energy demands and forest degradation. This kind of approach has potential to reduce uncertainties in forest cover change and carbon emission assessments in sub-Saharan Africa. C1 [Sedano, F.; Silva, J. A.; Anderson, K.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Machoco, R.; Sitoe, A.; Ribeiro, N.] UEM, Fac Agron & Forest Engn, Dept Forest Engn, Maputo, Mozambique. [Meque, C. H.] Mozambican Minist Sci & Technol, Zambezia, Mozambique. [Ombe, Z. A.] Univ Pedagog, Fac Earth Sci & Environm, Maputo, Mozambique. [Baule, S. H.] Univ Pedagog, Dept Language Commun & Arts, Beira, Mozambique. [Tucker, C. J.] NASA, Goddard Space Flight Ctr, Washington, DC 20546 USA. RP Sedano, F (reprint author), Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. EM fsedano@umd.edu FU National Science Foundation-Dynamics of Coupled Natural and Human Systems program [1413999] FX This research is part of the 'CNH-Ex: Investigating the Dynamic Intersections Among Economic Development, Urbanization, and Forest Degradation' project, funded under the National Science Foundation-Dynamics of Coupled Natural and Human Systems program (Award number 1413999). The authors express their gratitude to students and representatives of the Universidade Eduardo Mondlane, Universidade Pegagogica-Tete branch and the personnel of the provincial Forest Services of Tete whose contribution and support made possible field data collection. NR 39 TC 0 Z9 0 U1 10 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-9326 J9 ENVIRON RES LETT JI Environ. Res. Lett. PD SEP PY 2016 VL 11 IS 9 AR 094020 DI 10.1088/1748-9326/11/9/094020 PG 12 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA DY8PU UT WOS:000385393100008 ER PT J AU Rani, B Krichbaum, T Hodgson, JA Koyama, S Zensus, AJ Fuhramnn, L Marscher, A Jorstad, S AF Rani, Bindu Krichbaum, Thomas Hodgson, Jeff A. Koyama, Shoko Zensus, Anton J. Fuhramnn, Lars Marscher, Alan Jorstad, Svetlana TI Exploring the Magnetic Field Configuration in BL Lac Using GMVA SO GALAXIES LA English DT Article DE active galaxies; BL Lacertae object: BL Lac; jets; GMVA; high-resolution VLBI; magnetic field; polarization ID JET AB The high radio frequency polarization imaging of non-thermal emission from active galactic nuclei (AGN) is a direct way to probe the magnetic field strength and structure in the immediate vicinity of supermassive black holes (SMBHs) and is crucial in testing the jet-launching scenario. To explore the the magnetic field configuration at the base of jets in blazars, we took advantage of the full polarization capabilities of the Global Millimeter VLBI Array (GMVA). With an angular resolution of similar to 50 micro-arcseconds (m as) at 86 GHz, one could resolve scales up to similar to 450 gravitational radii (for a 10(9) solar mass black hole at a redshift of 0.1). We present here the preliminary results of our study on the blazar BL Lac. Our results suggest that on sub-mas scales the core and the central jet of BL Lac are significantly polarized with two distinct regions of polarized intensity. We also noted a great morphological similarity between the 7 mm/3 mm VLBI images at very similar angular resolution. C1 [Rani, Bindu] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rani, Bindu; Krichbaum, Thomas; Koyama, Shoko; Zensus, Anton J.; Fuhramnn, Lars] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Hodgson, Jeff A.] Korea Astron & Space Inst, 776 Daedeokdae Ro, Daejeon 34055, South Korea. [Marscher, Alan; Jorstad, Svetlana] Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA. RP Rani, B (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Rani, B (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM bindu.rani@nasa.gov; tkrichbaum@mpifr-bonn.mpg.de; jhodgo@gmail.com; skoyama@mpifr-bonn.mpg.de; azensus@mpifr-bonn.mpg.de; fuhrmann.lars@googlemail.com; marscher@bu.edu; jorstad@bu.edu OI Jorstad, Svetlana/0000-0001-6158-1708 NR 18 TC 0 Z9 0 U1 0 U2 0 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 2075-4434 J9 GALAXIES JI Galaxies PD SEP PY 2016 VL 4 IS 3 AR 32 DI 10.3390/galaxies4030032 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY9UM UT WOS:000385480600024 ER PT J AU Wilder, FD Ergun, RE Schwartz, SJ Newman, DL Eriksson, S Stawarz, JE Goldman, MV Goodrich, KA Gershman, DJ Malaspina, DM Holmes, JC Sturner, AP Burch, JL Torbert, RB Lindqvist, PA Marklund, GT Khotyaintsev, Y Strangeway, RJ Russell, CT Pollock, CJ Giles, BL Dorrelli, JC Avanov, LA Patterson, WR Plaschke, F Magnes, W AF Wilder, F. D. Ergun, R. E. Schwartz, S. J. Newman, D. L. Eriksson, S. Stawarz, J. E. Goldman, M. V. Goodrich, K. A. Gershman, D. J. Malaspina, D. M. Holmes, J. C. Sturner, A. P. Burch, J. L. Torbert, R. B. Lindqvist, P. -A. Marklund, G. T. Khotyaintsev, Y. Strangeway, R. J. Russell, C. T. Pollock, C. J. Giles, B. L. Dorrelli, J. C. Avanov, L. A. Patterson, W. R. Plaschke, F. Magnes, W. TI Observations of large-amplitude, parallel, electrostatic waves associated with the Kelvin-Helmholtz instability by the magnetospheric multiscale mission SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Kelvin-Helmholtz; electrostatic waves; boundary layer; turbulence ID LATITUDE BOUNDARY-LAYER; MAGNETIC RECONNECTION; PLASMA TRANSPORT AB On 8 September 2015, the four Magnetospheric Multiscale spacecraft encountered a Kelvin-Helmholtz unstable magnetopause near the dusk flank. The spacecraft observed periodic compressed current sheets, between which the plasma was turbulent. We present observations of large-amplitude (up to 100mV/m) oscillations in the electric field. Because these oscillations are purely parallel to the background magnetic field, electrostatic, and below the ion plasma frequency, they are likely to be ion acoustic-like waves. These waves are observed in a turbulent plasma where multiple particle populations are intermittently mixed, including cold electrons with energies less than 10eV. Stability analysis suggests a cold electron component is necessary for wave growth. C1 [Wilder, F. D.; Ergun, R. E.; Schwartz, S. J.; Eriksson, S.; Stawarz, J. E.; Goodrich, K. A.; Malaspina, D. M.; Holmes, J. C.; Sturner, A. P.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA. [Ergun, R. E.; Stawarz, J. E.; Goodrich, K. A.; Holmes, J. C.; Sturner, A. P.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Schwartz, S. J.] Imperial Coll London, Dept Phys, London, England. [Newman, D. L.; Goldman, M. V.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Gershman, D. J.; Pollock, C. J.; Giles, B. L.; Dorrelli, J. C.; Avanov, L. A.; Patterson, W. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Burch, J. L.] Southwest Res Inst, San Antonio, TX USA. [Torbert, R. B.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Lindqvist, P. -A.; Marklund, G. T.] Royal Inst Technol, Stockholm, Sweden. [Khotyaintsev, Y.] Swedish Inst Space Phys, Uppsala, Sweden. [Strangeway, R. J.; Russell, C. T.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. [Plaschke, F.; Magnes, W.] Austrian Acad Sci, Space Res Inst, Graz, Austria. RP Wilder, FD (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA. EM frederick.wilder@lasp.colorado.edu RI Stawarz, Julia/L-7387-2016; NASA MMS, Science Team/J-5393-2013; OI Stawarz, Julia/0000-0002-5702-5802; NASA MMS, Science Team/0000-0002-9504-5214; Eriksson, Stefan/0000-0002-5619-1577 FU NASA MMS project; Leverhulme Trust FX This work was funded by the NASA MMS project. S.J.S. thanks the Leverhulme Trust for the award of a research fellowship. We thank the MMS search coil magnetometer team for providing burst data and comments on our analyses. Level 2 spacecraft data are available via the MMS Science Data Center (https://lasp.colorado.edu/mms/sdc/public/). NR 22 TC 0 Z9 0 U1 1 U2 1 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 SEP PY 2016 VL 43 IS 17 BP 8859 EP 8866 DI 10.1002/2016GL070404 PG 8 WC Geosciences, Multidisciplinary SC Geology GA DY8CX UT WOS:000385357200005 ER PT J AU Xu, SS Mitchell, D Liemohn, M Dong, CF Bougher, S Fillingim, M Lillis, R McFadden, J Mazelle, C Connerney, J Jakosky, B AF Xu, Shaosui Mitchell, David Liemohn, Michael Dong, Chuanfei Bougher, Stephen Fillingim, Matthew Lillis, Robert McFadden, James Mazelle, Christian Connerney, Jack Jakosky, Bruce TI Deep nightside photoelectron observations by MAVEN SWEA: Implications for Martian northern hemispheric magnetic topology and nightside ionosphere source SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Mars; photoelectrons; nightside ionosphere; magnetic topology; weak crustal fields; MAVEN ID SOLAR-WIND INTERACTION; ELECTRON REFLECTOMETRY; MARS; FIELD; ATMOSPHERE; MODEL; INSTRUMENT; MISSION; FLUXES; ATOMS AB The Mars Atmosphere and Volatile EvolutioN (MAVEN) mission samples the Mars ionosphere down to altitudes of approximate to 150km over a wide range of local times and solar zenith angles. On 5 January 2015 (Orbit 520) when the spacecraft was in darkness at high northern latitudes (solar zenith angle, SZA>120 degrees; latitude>60 degrees), the Solar Wind Electron Analyzer (SWEA) instrument observed photoelectrons at altitudes below 200km. Such observations imply the presence of closed crustal magnetic field loops that cross the terminator and extend thousands of kilometers to the deep nightside. This occurs over the weak northern crustal magnetic source regions, where the magnetic field has been thought to be dominated by draped interplanetary magnetic fields (IMF). Such a day-night magnetic connectivity also provides a source of plasma and energy to the deep nightside. Simulations with the SuperThermal Electron Transport (STET) model show that photoelectron fluxes measured by SWEA precipitating onto the nightside atmosphere provide a source of ionization that can account for the O(2)(+)density measured by the Suprathermal and Thermal Ion Composition (STATIC) instrument below 200km. This finding indicates another channel for Martian energy redistribution to the deep nightside and consequently localized ionosphere patches and potentially aurora. C1 [Xu, Shaosui; Mitchell, David; Fillingim, Matthew; Lillis, Robert; McFadden, James] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Xu, Shaosui; Liemohn, Michael; Dong, Chuanfei; Bougher, Stephen] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA. [Dong, Chuanfei] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Dong, Chuanfei] Princeton Univ, Princeton Plasma Phys Lab, POB 451, Princeton, NJ 08543 USA. [Mazelle, Christian] CNRS, IRAP, Toulouse, France. [Mazelle, Christian] Univ Toulouse 3, Toulouse, France. [Connerney, Jack] GSFC, Greenbelt, MD USA. [Jakosky, Bruce] Univ Colorado, LASP, Boulder, CO 80309 USA. RP Xu, SS (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.; Xu, SS (reprint author), Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA. EM shaosui.xu@ssl.berkeley.edu RI Dong, Chuanfei/E-6485-2010; OI Dong, Chuanfei/0000-0002-8990-094X; Xu, Shaosui/0000-0002-5121-600X; connerney, jack/0000-0001-7478-6462 FU NASA; NSF [NNX13AG26G, AST-0908311]; NASA Mars Scout Program; Rackham graduate school of University of Michigan; NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program FX The authors would like to thank NASA and NSF for their support of this project under grants NNX13AG26G and AST-0908311. This work was also supported by the NASA Mars Scout Program. The authors thank the Rackham graduate school of University of Michigan for the research grant that supports S. Xu's visit at SSL, University of California, Berkeley, which makes this study possible. C.F. Dong is supported by the NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program, administered by the University Corporation for Atmospheric Research. The MAVEN data used in this study are available through Planetary Data System. The BATS-R-US code is publicly available from http://csem.engin.umich.edu/tools/swmf. For distribution of the model results used in this study, please contact C. Dong (dcfy@pppl.gov). NR 53 TC 1 Z9 1 U1 8 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP PY 2016 VL 43 IS 17 BP 8876 EP 8884 DI 10.1002/2016GL070527 PG 9 WC Geosciences, Multidisciplinary SC Geology GA DY8CX UT WOS:000385357200007 ER PT J AU Edwards, CS Piqueux, S AF Edwards, Christopher S. Piqueux, Sylvain TI The water content of recurring slope lineae on Mars SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Mars; recurring slope lineae; water budget; THEMIS; thermophysics ID THERMAL-CONDUCTIVITY MEASUREMENTS; EMISSION SPECTROMETER; PARTICULATE MATERIALS; REFLECTANCE; STABILITY; SURFACE; THEMIS; ICE AB Observations of recurring slope lineae (RSL) from the High-Resolution Imaging Science Experiment have been interpreted as present-day, seasonally variable liquid water flows; however, orbital spectroscopy has not confirmed the presence of liquid H2O, only hydrated salts. Thermal Emission Imaging System (THEMIS) temperature data and a numerical heat transfer model definitively constrain the amount of water associated with RSL. Surface temperature differences between RSL-bearing and dry RSL-free terrains are consistent with no water associated with RSL and, based on measurement uncertainties, limit the water content of RSL to at most 0.5-3wt %. In addition, distinct high thermal inertia regolith signatures expected with crust-forming evaporitic salt deposits from cyclical briny water flows are not observed, indicating low water salinity (if any) and/or low enough volumes to prevent their formation. Alternatively, observed salts may be preexisting in soils at low abundances (i.e., near or below detection limits) and largely immobile. These RSL-rich surfaces experience similar to 100K diurnal temperature oscillations, possible freeze/thaw cycles and/or complete evaporation on time scales that challenge their habitability potential. The unique surface temperature measurements provided by THEMIS are consistent with a dry RSL hypothesis or at least significantly limit the water content of Martian RSL. C1 [Edwards, Christopher S.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Edwards, Christopher S.] Northern Univ Arizona, Dept Phys & Astron, Flagstaff, AZ 86011 USA. [Piqueux, Sylvain] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Edwards, CS (reprint author), US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.; Edwards, CS (reprint author), Northern Univ Arizona, Dept Phys & Astron, Flagstaff, AZ 86011 USA. EM Christopher.Edwards@nau.edu FU National Aeronautics and Space Administration FX The authors thank the 2001 Mars Odyssey THEMIS team, who aided in the collection of needed seasonal data. We thank Joshua Bandfield, Shane Byrne, and two anonymous reviewers that greatly improved the manuscript. All THEMIS, CTX, and HiRISE data presented in this work are available on the Planetary Data System (http://pds-geosciences.wustl.edu), data processing software was completed using davinci (http://davinci.asu.edu) and the Integrated Software for Imaging Spectrometers (http://isis.astrogeology.usgs.gov), and modeling was conducted using the KRC thermal model (http://krc.mars.asu.edu). Work at the Jet Propulsion Laboratory, California Institute of Technology was performed under a contract with the National Aeronautics and Space Administration. NR 59 TC 2 Z9 2 U1 4 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP PY 2016 VL 43 IS 17 BP 8912 EP 8919 DI 10.1002/2016GL070179 PG 8 WC Geosciences, Multidisciplinary SC Geology GA DY8CX UT WOS:000385357200011 ER PT J AU Coats, S Mankin, JS AF Coats, Sloan Mankin, Justin S. TI The challenge of accurately quantifying future megadrought risk in the American Southwest SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE hydroclimate; drought; North America; climate; megadrought; projections ID LAST MILLENNIUM; NORTH-AMERICA; DROUGHT; RECONSTRUCTIONS; VARIABILITY; FREQUENCY; EVENTS; WATER AB American Southwest (ASW) megadroughts represent decadal-scale periods of dry conditions the near-term risks of which arise from natural low-frequency hydroclimate variability and anthropogenic forcing. A large single-climate-model ensemble indicates that anthropogenic forcing increases near-term ASW megadrought risk by a factor of 100; however, accurate risk assessment remains a challenge. At the global-scale we find that anthropogenic forcing may alter the variability driving megadroughts over 55% of land areas, undermining accurate assessments of their risk. For the remaining areas, current ensembles are too small to characterize megadroughts' driving variability. For example, constraining uncertainty in near-term ASW megadrought risk to 5 percentage points with high confidence requires 287 simulations. Such ensemble sizes are beyond current computational and storage resources, and these limitations suggest that constraining errors in near-term megadrought risk projections with high confidenceeven in places where underlying variability is stationaryis not currently possible. C1 [Coats, Sloan] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Mankin, Justin S.] Columbia Univ, Ocean & Climate Phys, Lamont Doherty Earth Observ, Palisades, NY USA. [Mankin, Justin S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Coats, S (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. EM sloan.coats@colorado.edu FU Center for International Security and Cooperation at Stanford University; Earth Institute Fellowship at Columbia University; Cooperative Institute for Research in Environmental Sciences at the University of Colorado, Boulder FX The authors would like to thank the National Center for Atmospheric Research's CESM1 (CAM5) Large Ensemble Community Project (LENS) and supercomputing resources provided by Stanford Center for Computational Earth and Environmental Science in the School of Earth, Energy, and Environmental Sciences at Stanford University. The model output employed from the LENS can be accessed at https://www2.cesm.ucar.edu/models/experiments/LENS. Our work was supported by the Center for International Security and Cooperation at Stanford University and the Earth Institute Fellowship at Columbia University to J.S.M. and the Cooperative Institute for Research in Environmental Sciences at the University of Colorado, Boulder, and Kristopher B. Karnauskas to S.C. LDEO publication 8051. NR 31 TC 0 Z9 0 U1 5 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP PY 2016 VL 43 IS 17 BP 9225 EP 9233 DI 10.1002/2016GL070445 PG 9 WC Geosciences, Multidisciplinary SC Geology GA DY8CX UT WOS:000385357200049 ER PT J AU Tong, D Pan, L Chen, WW Lamsal, L Lee, P Tang, YH Kim, H Kondragunta, S Stajner, I AF Tong, Daniel Pan, Li Chen, Weiwei Lamsal, Lok Lee, Pius Tang, Youhua Kim, Hyuncheol Kondragunta, Shobha Stajner, Ivanka TI Impact of the 2008 Global Recession on air quality over the United States: Implications for surface ozone levels from changes in NOx emissions SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE ozone; recession; NO2; air quality ID NITROGEN-OXIDES; NORTH-AMERICA; SATELLITE; POLLUTION; MODEL; CAPABILITY; SYSTEM; TRENDS; CITIES; SPACE AB Satellite and ground observations detected large variability in nitrogen oxides (NOx) during the 2008 economic recession, but the impact of the recession on air quality has not been quantified. This study combines observed NOx trends and a regional chemical transport model to quantify the impact of the recession on surface ozone (O-3) levels over the continental United States. The impact is quantified by simulating O-3 concentrations under two emission scenarios: business-as-usual (BAU) and recession. In the BAU case, the emission projection from the Cross-State Air Pollution Rule is used to estimate the would-be NOx emission level in 2011. In the recession case, the actual NO2 trends observed from Air Quality System ground monitors and the Ozone Monitoring Instrument on the Aura satellite are used to obtain realistic changes in NOx emissions. The model prediction with the recession effect agrees better with ground O-3 observations over time and space than the prediction with the BAU emission. The results show that the recession caused a 1-2ppbv decrease in surface O-3 concentration over the eastern United States, a slight increase (0.5-1ppbv) over the Rocky Mountain region, and mixed changes in the Pacific West. The gain in air quality benefits during the recession, however, could be quickly offset by the much slower emission reduction rate during the post-recession period. C1 [Tong, Daniel] Univ Maryland, Cooperat Inst Climate & Satellites, College Pk, MD 20742 USA. [Tong, Daniel; Pan, Li; Tang, Youhua; Kim, Hyuncheol] George Mason Univ, Ctr Spatial Informat Sci & Syst, Fairfax, VA 22030 USA. [Tong, Daniel; Pan, Li; Chen, Weiwei; Lee, Pius; Tang, Youhua; Kim, Hyuncheol] NOAA, Air Resources Lab, College Pk, MD 20740 USA. [Lamsal, Lok] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Lamsal, Lok] Univ Space Res Assoc, Greenbelt, MD USA. [Kondragunta, Shobha] NOAA, Satellite & Informat Serv, Ctr Satellite Res & Applicat, College Pk, MD USA. [Stajner, Ivanka] NOAA, Natl Weather Serv, Off Sci & Technol Integrat, Silver Spring, MD 20910 USA. RP Tong, D (reprint author), Univ Maryland, Cooperat Inst Climate & Satellites, College Pk, MD 20742 USA.; Tong, D (reprint author), George Mason Univ, Ctr Spatial Informat Sci & Syst, Fairfax, VA 22030 USA.; Tong, D (reprint author), NOAA, Air Resources Lab, College Pk, MD 20740 USA. EM daniel.tong@noaa.gov RI Kondragunta, Shobha/F-5601-2010; Tong, Daniel/A-8255-2008; Kim, Hyun/G-1315-2012 OI Kondragunta, Shobha/0000-0001-8593-8046; Tong, Daniel/0000-0002-4255-4568; Kim, Hyun/0000-0003-3968-6145 FU NOAA's US Weather Research Program (USWRP); Joint Polar Satellite System (JPSS) Proving Ground and Risk Reduction Programs FX This work has been financially supported by grants from the NOAA's US Weather Research Program (USWRP) and Joint Polar Satellite System (JPSS) Proving Ground and Risk Reduction Programs. Modeling system development was supported by the NOAA's National Air Quality Forecast Capability program. The authors are grateful to Nina Randazzo for data analysis and two anonymous reviewers for their constructive comments. The scientific results and conclusions, as well as any views or opinions expressed herein, are those of the authors and do not necessarily reflect the view of NOAA or the Department of Commerce. NR 34 TC 0 Z9 0 U1 6 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP PY 2016 VL 43 IS 17 BP 9280 EP 9288 DI 10.1002/2016GL069885 PG 9 WC Geosciences, Multidisciplinary SC Geology GA DY8CX UT WOS:000385357200055 ER PT J AU Schobesberger, S Lopez-Hilfiker, FD Taipale, D Millet, DB D'Ambro, EL Rantala, P Mammarella, I Zhou, PT Wolfe, GM Lee, BH Boy, M Thornton, JA AF Schobesberger, Siegfried Lopez-Hilfiker, Felipe D. Taipale, Ditte Millet, Dylan B. D'Ambro, Emma L. Rantala, Pekka Mammarella, Ivan Zhou, Putian Wolfe, Glenn M. Lee, Ben H. Boy, Michael Thornton, Joel A. TI High upward fluxes of formic acid from a boreal forest canopy SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE formic acid; eddy covariance fluxes; chemical ionization mass spectrometry; boreal forest; biogenic emissions ID ORGANIC-COMPOUND EMISSIONS; GASEOUS DRY DEPOSITION; ACETIC-ACIDS; SCOTS PINE; MASS-SPECTROMETER; EDDY COVARIANCE; PEROXY NITRATES; SULFURIC-ACID; NEW-MODEL; GAS AB Eddy covariance fluxes of formic acid, HCOOH, were measured over a boreal forest canopy in spring/summer 2014. The HCOOH fluxes were bidirectional but mostly upward during daytime, in contrast to studies elsewhere that reported mostly downward fluxes. Downward flux episodes were explained well by modeled dry deposition rates. The sum of net observed flux and modeled dry deposition yields an upward gross flux of HCOOH, which could not be quantitatively explained by literature estimates of direct vegetative/soil emissions nor by efficient chemical production from other volatile organic compounds, suggesting missing or greatly underestimated HCOOH sources in the boreal ecosystem. We implemented a vegetative HCOOH source into the GEOS-Chem chemical transport model to match our derived gross flux and evaluated the updated model against airborne and spaceborne observations. Model biases in the boundary layer were substantially reduced based on this revised treatment, but biases in the free troposphere remain unexplained. C1 [Schobesberger, Siegfried; Lopez-Hilfiker, Felipe D.; Lee, Ben H.; Thornton, Joel A.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Schobesberger, Siegfried; Rantala, Pekka; Mammarella, Ivan; Zhou, Putian; Boy, Michael] Univ Helsinki, Dept Phys, Helsinki, Finland. [Taipale, Ditte] Estonian Univ Life Sci, Dept Plant Physiol, Tartu, Estonia. [Taipale, Ditte] Univ Helsinki, Dept Forest Sci, Helsinki, Finland. [Millet, Dylan B.] Univ Minnesota, Dept Soil Water & Climate, Minneapolis, MN USA. [D'Ambro, Emma L.] Univ Washington, Dept Chem, Seattle, WA 98195 USA. [Wolfe, Glenn M.] NASA, Atmospher Chem & Dynam Lab, Goddard Space Flight Ctr, Greenbelt, MD USA. [Wolfe, Glenn M.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. RP Schobesberger, S (reprint author), Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.; Schobesberger, S (reprint author), Univ Helsinki, Dept Phys, Helsinki, Finland. EM sschobes@uw.edu RI Millet, Dylan/G-5832-2012; Chem, GEOS/C-5595-2014; Thornton, Joel/C-1142-2009; Wolfe, Glenn/D-5289-2011; OI Thornton, Joel/0000-0002-5098-4867; Taipale, Ditte/0000-0002-2023-2461; Boy, Michael/0000-0002-8107-4524; Mammarella, Ivan/0000-0002-8516-3356; Zhou, Putian/0000-0003-0803-7337 FU U.S. Department of Energy [DE-SC0006867]; European Commission (OXFLUX) [701958]; European Regional Development Fund (Centre of Excellence EcolChange); NSF CAREER [1148951]; Minnesota Supercomputing Institute FX We thank T. Vesala, P. Kolari, P. Keronen, E. Siivola, M. Kajos, and A. Manninen at U. Helsinki for helpful discussions and model and measurement data related to SMEAR II. We also thank J. de Gouw (NOAA ESRL), and the SENEX and TES science teams for providing observations, and P. Punttila (Ymparisto) and D.M. Sorger (NC State) for entomological insights. The University of Washington participated in the BAECC campaign with funds from the U.S. Department of Energy (DE-SC0006867). S. Schobesberger acknowledges support from the European Commission (OXFLUX, project 701958), D. Taipale from the European Regional Development Fund (Centre of Excellence EcolChange), and D. B. M. from NSF CAREER (1148951) and the Minnesota Supercomputing Institute. We thank K. Cady-Pereira (AER), M. Shephard (Environment Canada), and M. Luo (JPL) for developing TES HCOOH measurements, publicly available at http://tes.jpl.nasa.gov/data/. GEOS-Chem model code is available at www.geos-chem.org. SOSAA model output, the high-frequency HCOOH mixing ratio measurements by CIMS, and anemometer wind measurements are available at http://hdl.handle.net/1773/36867. NR 68 TC 0 Z9 0 U1 11 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 SEP PY 2016 VL 43 IS 17 BP 9342 EP 9351 DI 10.1002/2016GL069599 PG 10 WC Geosciences, Multidisciplinary SC Geology GA DY8CX UT WOS:000385357200062 ER PT J AU Zhou, DK Liu, X Larar, AM Tian, JL Smith, WL Kizer, SH Wu, W Liu, QH Goldberg, MD AF Zhou, Daniel K. Liu, Xu Larar, Allen M. Tian, Jialin Smith, William L. Kizer, Susan H. Wu, Wan Liu, Quanhua Goldberg, Mitch D. TI First Suomi NPP Cal/Val Campaign: Intercomparison of Satellite and Aircraft Sounding Retrievals SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE Atmospheric measurements; geophysical inverse problems; infrared measurements; remote sensing ID VALIDATION; EAQUATE; CLOUD AB Satellite ultraspectral infrared sensors provide key data records essential for weather forecasting and climate change science. The Suomi National Polar-orbiting Partnership (NPP) satellite environmental data records (EDRs) are retrieved from calibrated ultraspectral radiance or sensor data records (SDRs). Understanding the accuracy of retrieved EDRs is critical. The first Suomi NPP Calibration/Validation Campaign was conducted during May 2013. The NASA high-altitude ER-2 aircraft carrying ultraspectral interferometer sounders such as the National Airborne Sounder Testbed-Interferometer (NAST-I) flew under the Suomi NPP satellite that carries the cross-track infrared sounder (CrIS) and the advanced technology microwave sounder (ATMS). Here, we intercompare the EDRs produced with different retrieval algorithms from SDRs measured from satellite and aircraft. The available dropsonde and radiosonde measurements together with the European Centre for Medium-Range Weather Forecasts (ECMWF) analysis are used to assess the results of this experiment. This study indicates that the CrIS/ATMS retrieval accuracy meets the Suomi NPP EDR requirement, except in the planetary boundary layer (PBL) where we have less confidence in meeting the requirement due to retrieval null-space error. C1 [Zhou, Daniel K.; Liu, Xu; Larar, Allen M.; Tian, Jialin] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Smith, William L.; Kizer, Susan H.; Wu, Wan] Sci Syst & Applicat Inc, Hampton, VA 23681 USA. [Liu, Quanhua; Goldberg, Mitch D.] NOAA, NESDIS, College Pk, MD 20740 USA. RP Zhou, DK (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM daniel.k.zhou@nasa.gov FU NASA Headquarters; NASA Langley Research Center; NOAA NESDIS/JPSS Program Office; NAST-I program FX The authors greatly appreciate the contributions of NASA's Langley Research Center and the U.K. Met Office. The authors would like to thank NASA ER-2 aircraft pilots and crewmembers based at NASA's Armstrong Flight Research Center for their dedication. The NAST-I program is supported by NASA Headquarters, NASA Langley Research Center, and NOAA NESDIS/JPSS Program Office. The authors would also like to thank Dr. A. Gambacorta of NOAA NESDIS for useful discussion; and Dr. J. Kaye of NASA's Science Mission Directorate for his continued, enabling support of the NAST-I program. NR 21 TC 1 Z9 1 U1 2 U2 2 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 SEP PY 2016 VL 9 IS 9 BP 4037 EP 4046 DI 10.1109/JSTARS.2016.2516765 PG 10 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA DY6NW UT WOS:000385245000005 ER PT J AU Selvakumaran, R Veenadhari, B Akiyama, S Pandya, M Gopalswamy, N Yashiro, S Kumar, S Makela, P Xie, H AF Selvakumaran, R. Veenadhari, B. Akiyama, S. Pandya, Megha Gopalswamy, N. Yashiro, S. Kumar, Sandeep Maekelae, P. Xie, H. TI On the reduced geoeffectiveness of solar cycle 24: A moderate storm perspective SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE moderate storms; solar source identification; reduced geoeffectiveness ID CORONAL MASS EJECTIONS; INTENSE GEOMAGNETIC STORMS; DST LESS-THAN-OR-EQUAL-TO-50 NT; MAGNETIC STORMS; RING CURRENT; INTERPLANETARY ORIGIN; INTERACTION REGIONS; SPACE WEATHER; TAIL CURRENT; MAIN PHASE AB The moderate and intense geomagnetic storms are identified for the first 77months of solar cycles 23 and 24. The solar sources responsible for the moderate geomagnetic storms are indentified during the same epoch for both the cycles. Solar cycle 24 has shown nearly 80% reduction in the occurrence of intense storms whereas it is only 40% in case of moderate storms when compared to previous cycle. The solar and interplanetary characteristics of the moderate storms driven by coronal mass ejection (CME) are compared for solar cycles 23 and 24 in order to see reduction in geoeffectiveness has anything to do with the occurrence of moderate storm. Though there is reduction in the occurrence of moderate storms, the Dst distribution does not show much difference. Similarly, the solar source parameters like CME speed, mass, and width did not show any significant variation in the average values as well as the distribution. The correlation between VBz and Dst is determined, and it is found to be moderate with value of 0.68 for cycle 23 and 0.61 for cycle 24. The magnetospheric energy flux parameter epsilon (epsilon) is estimated during the main phase of all moderate storms during solar cycles 23 and 24. The energy transfer decreased in solar cycle 24 when compared to cycle 23. These results are significantly different when all geomagnetic storms are taken into consideration for both the solar cycles. C1 [Selvakumaran, R.; Veenadhari, B.; Pandya, Megha; Kumar, Sandeep] Indian Inst Geomagnetism, New Panvel, India. [Akiyama, S.; Gopalswamy, N.; Yashiro, S.; Maekelae, P.; Xie, H.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD USA. [Akiyama, S.; Yashiro, S.; Maekelae, P.; Xie, H.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Selvakumaran, R (reprint author), Indian Inst Geomagnetism, New Panvel, India. EM selva2986@gmail.com FU NASA's LWS TRT program FX R. Selvakumaran benefited from the SCOSTEP Visiting Scholar Program, under which he visited NASA Goddard Space Flight Center, where this research was performed. Authors from Indian Institute of Geomagnetism (IIG) are grateful to Director, IIG, for support and encouragement to carry out the work. We thank the ACE, Wind, and OMNIWeb teams for providing the solar wind data. We acknowledge the use of solar imagery from SDO, SOHO, and STEREO missions. This work greatly benefited from the open data policy of NASA. The work of N.G., S.A., S.Y., P.M., and H.X. was supported by NASA's LWS TR&T program. NR 76 TC 0 Z9 0 U1 3 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 SEP PY 2016 VL 121 IS 9 BP 8188 EP 8202 DI 10.1002/2016JA022885 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4QM UT WOS:000385844000003 ER PT J AU Neugebauer, M Reisenfeld, D Richardson, IG AF Neugebauer, Marcia Reisenfeld, Daniel Richardson, Ian G. TI Comparison of algorithms for determination of solar wind regimes SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE solar wind ID CORONAL MASS EJECTIONS; COROTATING INTERACTION REGIONS; STREAM INTERFACES; QUASI-STATIONARY; EARTH; SPACECRAFT; MISSION; CLOUDS; MATTER AB This study compares the designation of different solar wind flow regimes (transient, coronal hole, and streamer belt) according to two algorithms derived from observations by the Solar Wind Ion Composition Spectrometer, the Solar Wind Electron Proton Alpha Monitor, and the Magnetometer on the ACE spacecraft, with a similar regime determination performed on board the Genesis spacecraft. The comparison is made for the interval from late 2001 to early 2004 when Genesis was collecting solar wind ions for return to Earth. The agreement between hourly regime assignments from any pair of algorithms was less than two thirds, while the simultaneous agreement between all three algorithms was only 49%. When the results of the algorithms were compared to a catalog of interplanetary coronal mass ejection events, it was found that almost all the events in the catalog were confirmed by the spacecraft algorithms. On the other hand, many short transient events, lasting 1 to 13h, that were unanimously selected as transient like by the algorithms, were not included in the catalog. C1 [Neugebauer, Marcia] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Reisenfeld, Daniel] Univ Montana, Dept Phys & Astron, Missoula, MT 59812 USA. [Richardson, Ian G.] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Richardson, Ian G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Richardson, Ian G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Neugebauer, M (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. EM mneugeb@lpl.arizona.edu FU ACE mission; NSF; NASA Laboratory Analysis of Returned Samples (LARS) program [NNX15AG19G] FX The Genesis, SWICS, SWEPAM, and MAG parameters are all available at http://cdaweb.gsfc.nasa.gov and other sites listed in the text. The times of Genesis collector (regime) changes are available in the supporting information of the paper by Reisenfeld et al. [2013]. I.G.R. acknowledges support from the ACE mission. The Thule neutron monitor of the Bartol Research Institute is supported by NSF. D.B.R. acknowledges support from the NASA Laboratory Analysis of Returned Samples (LARS) program, grant NNX15AG19G. NR 35 TC 0 Z9 0 U1 0 U2 0 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 SEP PY 2016 VL 121 IS 9 BP 8215 EP 8227 DI 10.1002/2016JA023142 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4QM UT WOS:000385844000005 ER PT J AU Chamberlin, PC Gong, Q AF Chamberlin, Phillip C. Gong, Qian TI An integral field spectrograph utilizing mirrorlet arrays SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Heliophysics; instrumentation; EUV; solar; photons; solar eruptive events ID IMAGING SPECTROMETER; SOLAR; REGION; 3D AB An integral field spectrograph (IFS) has been developed that utilizes a new and novel optical design to observe two spatial dimensions simultaneously with one spectral dimension. This design employs an optical 2-D array of reflecting and focusing mirrorlets. This mirrorlet array is placed at the imaging plane of the front-end telescope to generate a 2-D array of tiny spots replacing what would be the slit in a traditional slit spectrometer design. After the mirrorlet in the optical path, a grating on a concave mirror surface will image the spot array and provide high-resolution spectrum for each spatial element at the same time; therefore, the IFS simultaneously obtains the 3-D data cube of two spatial and one spectral dimensions. The new mirrorlet technology is currently in-house and undergoing laboratory testing at NASA Goddard Space Flight Center. Section 1 describes traditional classes of instruments that are used in Heliophysics missions and a quick introduction to the new IFS design. Section 2 discusses the details of the most generic mirrorlet IFS, while section 3 presents test results of a lab-based instrument. An example application to a Heliophysics mission to study solar eruptive events in extreme ultraviolet wavelengths is presented in section 4 that has high spatial resolution (0.5arcsecpixels) in the two spatial dimensions and high spectral resolution (66m angstrom) across a 15 angstrom spectral window. Section 4 also concludes with some other optical variations that could be employed on the more basic IFS for further capabilities of this type of instrument. C1 [Chamberlin, Phillip C.] NASA, Goddard Space Flight Ctr, Heliophys Div, Solar Phys Lab, Greenbelt, MD 20771 USA. [Gong, Qian] NASA, Goddard Space Flight Ctr, Instrument Syst & Technol Div, Greenbelt, MD USA. RP Chamberlin, PC (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Div, Solar Phys Lab, Greenbelt, MD 20771 USA. EM Phillip.C.Chamberlin@NASA.gov RI Chamberlin, Phillip/C-9531-2012 OI Chamberlin, Phillip/0000-0003-4372-7405 FU NASA Goddard Space Flight Center's Internal Research and Development (IRAD) program FX This work was support under NASA Goddard Space Flight Center's Internal Research and Development (IRAD) program. The authors would like to thank RPC Photonics for producing the mirrorlet array. No data were used in producing this manuscript. NR 25 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD SEP PY 2016 VL 121 IS 9 BP 8250 EP 8259 DI 10.1002/2016JA022487 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4QM UT WOS:000385844000008 ER PT J AU Poh, G Slavin, JA Jia, XZ DiBraccio, GA Raines, JM Imber, SM Gershman, DJ Sun, WJ Anderson, BJ Korth, H Zurbuchen, TH McNutt, RL Solomon, SC AF Poh, Gangkai Slavin, James A. Jia, Xianzhe DiBraccio, Gina A. Raines, Jim M. Imber, Suzanne M. Gershman, Daniel J. Sun, Wei-Jie Anderson, Brian J. Korth, Haje Zurbuchen, Thomas H. McNutt, Ralph L., Jr. Solomon, Sean C. TI MESSENGER observations of cusp plasma filaments at Mercury SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE cusp filaments; Mercury; reconnection ID FLUX-TRANSFER EVENTS; MAGNETIC-FIELD; SOLAR-WIND; MAGNETOPAUSE RECONNECTION; DAYSIDE MAGNETOPAUSE; MAGNETOSPHERE; INSTRUMENT; MODEL; HOLES; SHEAR AB The MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft while in orbit about Mercury observed highly localized, similar to 3-s-long reductions in the dayside magnetospheric magnetic field, with amplitudes up to 90% of the ambient intensity. These magnetic field depressions are termed cusp filaments because they were observed from just poleward of the magnetospheric cusp to midlatitudes, i.e., similar to 55 degrees to 85 degrees N. We analyzed 345 high- and low-altitude cusp filaments identified from MESSENGER magnetic field data to determine their physical properties. Minimum variance analysis indicates that most filaments resemble cylindrical flux tubes within which the magnetic field intensity decreases toward its central axis. If the filaments move over the spacecraft at an estimated magnetospheric convection speed of similar to 35km/s, then they have a typical diameter of similar to 105km or similar to 7gyroradii for 1keVH(+) ions in a 300nT magnetic field. During these events, MESSENGER's Fast Imaging Plasma Spectrometer observed H+ ions with magnetosheath-like energies. MESSENGER observations during the spacecraft's final low-altitude campaign revealed that these cusp filaments likely extend down to Mercury's surface. We calculated an occurrence-rate-normalized integrated particle precipitation rate onto the surface from all filaments of (2.700.09)x10(25)s(-1). This precipitation rate is comparable to published estimates of the total precipitation rate in the larger-scale cusp. Overall, the MESSENGER observations analyzed here suggest that cusp filaments are the magnetospheric extensions of the flux transfer events that form at the magnetopause as a result of localized magnetic reconnection. C1 [Poh, Gangkai; Slavin, James A.; Jia, Xianzhe; Raines, Jim M.; Imber, Suzanne M.; Gershman, Daniel J.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [DiBraccio, Gina A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD USA. [Imber, Suzanne M.] Univ Leicester, Dept Phys & Astron, Leicester, Leics, England. [Gershman, Daniel J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Sun, Wei-Jie] Peking Univ, Sch Earth & Space Sci, Beijing, Peoples R China. [Anderson, Brian J.; Korth, Haje; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA. RP Poh, G (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. EM gangkai@umich.edu RI Jia, Xianzhe/C-5171-2012; Slavin, James/H-3170-2012 OI Jia, Xianzhe/0000-0002-8685-1484; Slavin, James/0000-0002-9206-724X FU NASA [NASW-00002, NAS5-97271, NNX15K88G, NNX15AL01G]; Living With a Star Program [NNX16AJ67G]; Solar System Workings Program [NNX15AH28G] FX Conversations with J. C. Kasper on the identification method used here are appreciated. We also thank two anonymous reviewers for constructive comments on an earlier draft. The MESSENGER project is supported by the NASA Discovery Program under contracts NASW-00002 to the Carnegie Institution of Washington and NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory. All data analyzed in this paper are archived with the NASA Planetary Data System. Further support was provided by NASA Discovery Data Analysis Program grants NNX15K88G and NNX15AL01G, Living With a Star Program grant NNX16AJ67G, and Solar System Workings Program grant NNX15AH28G to the University of Michigan. NR 58 TC 0 Z9 0 U1 2 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD SEP PY 2016 VL 121 IS 9 BP 8260 EP 8285 DI 10.1002/2016JA022552 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4QM UT WOS:000385844000009 ER PT J AU Fennell, JF Blake, JB Claudepierre, S Mazur, J Kanekal, S O'Brien, P Baker, D Crain, W Mabry, D Clemmons, J AF Fennell, J. F. Blake, J. B. Claudepierre, S. Mazur, J. Kanekal, S. O'Brien, P. Baker, D. Crain, W. Mabry, D. Clemmons, J. TI Current energetic particle sensors SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE energetic particles; sensors ID ALLEN PROBES OBSERVATIONS; RELATIVISTIC ELECTRONS; IMPENETRABLE BARRIER; MAGNETOSONIC WAVES; RADIATION BELTS; STORM; PRECIPITATION; ACCELERATION; PLASMASPHERE; ZONE AB Several energetic particle sensors designed to make measurements in the current decade are described and their technology and capabilities discussed and demonstrated. Most of these instruments are already on orbit or approaching launch. These include the Magnetic Electron Ion Spectrometers (MagEIS) and the Relativistic Electron Proton Telescope (REPT) that are flying on the Van Allen Probes, the Fly's Eye Electron Proton Spectrometers (FEEPS) flying on the Magnetospheric Multiscale (MMS) mission, and Dosimeters flying on the AC6 Cubesat mission. We focus mostly on the electron measurement capability of these sensors while providing summary comments of their ion measurement capabilities if they have any. C1 [Fennell, J. F.; Blake, J. B.; Claudepierre, S.; Mazur, J.; O'Brien, P.; Crain, W.; Mabry, D.; Clemmons, J.] Aerosp Corp, El Segundo, CA 90245 USA. [Kanekal, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Baker, D.] Univ Colorado, LASP, Boulder, CO 80309 USA. RP Fennell, JF (reprint author), Aerosp Corp, El Segundo, CA 90245 USA. EM joseph.fennell@aero.org OI Claudepierre, Seth/0000-0001-5513-5947; Clemmons, James/0000-0002-5298-5222 FU Van Allen Probes ECT - JHU/APL [967399]; Southwest Research Institute [792084N/E99017JD]; JHU/APL under NASA's prime [967399, NAS5-01072]; Research Opportunities in Space and Earth Science (ROSES) [NNH12ZDA001N-GEO]; US Air Force SMC/AD (Space and Missile Systems Center Advanced Systems and Development Directorate) FX The development of the MagEIS and FEEPS sensors and the analysis of their data were supported in part by Van Allen Probes ECT funding provided by JHU/APL contract 967399 and by Southwest Research Institute contract 792084N/E99017JD, respectively. The REPT sensor development at LASP, University of Colorado, was supported by JHU/APL contract 967399 under NASA's prime contract NAS5-01072. CeREs is funded under the NNH12ZDA001N-GEO for Research Opportunities in Space and Earth Science-2012 (ROSES-2012). The AC6 bus was developed under the Aerospace Corporation Multi-Program Acquisition Capability Enhancement Program, and the AC6 dosimeter payload was funded by US Air Force SMC/AD (Space and Missile Systems Center Advanced Systems and Development Directorate). The Van Allen Probes ECT data are available at http://www.rbsp-ect.lanl.gov/science/DataDirectories.php or from the authors. The MMS/FEEPS data are available at https://lasp.colorado.edu/mms/sdc/about/browse-wrapper/ or from the authors. NR 45 TC 0 Z9 0 U1 0 U2 0 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 SEP PY 2016 VL 121 IS 9 BP 8840 EP 8858 DI 10.1002/2016JA022588 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4QM UT WOS:000385844000044 ER PT J AU Peterson, WK Thiemann, EMB Eparvier, FG Andersson, L Fowler, CM Larson, D Mitchell, D Mazelle, C Fontenla, J Evans, JS Xu, SS Liemohn, M Bougher, S Sakai, S Cravens, TE Elrod, MK Benna, M Mahaffy, P Jakosky, B AF Peterson, W. K. Thiemann, E. M. B. Eparvier, Francis G. Andersson, Laila Fowler, C. M. Larson, Davin Mitchell, Dave Mazelle, Christian Fontenla, Juan Evans, J. Scott Xu, Shaosui Liemohn, Mike Bougher, Stephen Sakai, Shotaro Cravens, T. E. Elrod, M. K. Benna, M. Mahaffy, P. Jakosky, Bruce TI Photoelectrons and solar ionizing radiation at Mars: Predictions versus MAVEN observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE photoelectron; observation; model; Mars; thermosphere ID ELECTRON; IRRADIANCE; MODEL; CODE; EUV AB Understanding the evolution of the Martian atmosphere requires knowledge of processes transforming solar irradiance into thermal energy well enough to model them accurately. Here we compare Martian photoelectron energy spectra measured at periapsis by Mars Atmosphere and Volatile Evolution MissioN (MAVEN) with calculations made using three photoelectron production codes and three solar irradiance models as well as modeled and measured CO2 densities. We restricted our comparisons to regions where the contribution from solar wind electrons and ions were negligible. The two intervals examined on 19 October 2014 have different observed incident solar irradiance spectra. In spite of the differences in photoionization cross sections and irradiance spectra used, we find the agreement between models to be within the combined uncertainties associated with the observations from the MAVEN neutral density, electron flux, and solar irradiance instruments. C1 [Peterson, W. K.; Thiemann, E. M. B.; Eparvier, Francis G.; Andersson, Laila; Fowler, C. M.; Jakosky, Bruce] Univ Colorado, LASP, Boulder, CO 80309 USA. [Larson, Davin; Mitchell, Dave; Xu, Shaosui] Univ Calif Berkeley, SSL, Berkeley, CA 94720 USA. [Mazelle, Christian] Univ Toulouse, IRAP, UPS OMP, Toulouse, France. [Mazelle, Christian] CNRS, IRAP, Toulouse, France. [Fontenla, Juan] Northwest Res Associates, Boulder, CO USA. [Evans, J. Scott] Computat Phys Inc, Springfield, VA USA. [Xu, Shaosui; Liemohn, Mike; Bougher, Stephen] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA. [Sakai, Shotaro; Cravens, T. E.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Elrod, M. K.; Benna, M.; Mahaffy, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Elrod, M. K.] Univ Maryland, CRESST, College Pk, MD 20742 USA. RP Peterson, WK (reprint author), Univ Colorado, LASP, Boulder, CO 80309 USA. EM bill.peterson@lasp.colorado.edu RI Peterson, WK/A-8706-2009; OI Peterson, WK/0000-0002-1513-6096; EPARVIER, FRANCIS/0000-0001-7143-2730; Sakai, Shotaro/0000-0001-9135-2076 FU CNES; NASA's Planetary Science Division FX We thank the MAVEN team for providing spacecraft instruments capable of returning the exceptionally good data used in this report. Input values used for the models are available on request from the lead author. Work related to observations with the SWEA instrument was partially supported by CNES. This research was supported by NASA's Planetary Science Division. NR 30 TC 1 Z9 1 U1 4 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 SEP PY 2016 VL 121 IS 9 BP 8859 EP 8870 DI 10.1002/2016JA022677 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4QM UT WOS:000385844000045 ER PT J AU Verkhoglyadova, OP Tsurutani, BT Mannucci, AJ Mlynczak, MG Hunt, LA Paxton, LJ Komjathy, A AF Verkhoglyadova, O. P. Tsurutani, B. T. Mannucci, A. J. Mlynczak, M. G. Hunt, L. A. Paxton, L. J. Komjathy, A. TI Solar wind driving of ionosphere-thermosphere responses in three storms near St. Patrick's Day in 2012, 2013, and 2015 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE ionosphere; thermosphere; coupling; solar wind; ICME; geomagnetic storm ID ULTRAVIOLET IMAGER GUVI; GEOMAGNETIC STORMS; MAGNETIC STORMS; MASS EJECTIONS; LOW-LATITUDE; CAWSES II; SUBSTORMS; SHOCKS; ELECTRODYNAMICS; PROMINENCE AB We identify interplanetary plasma regions associated with three intense interplanetary coronal mass ejections (ICMEs)-driven geomagnetic storm intervals which occurred around the same time of the year: day of year 74-79 (March) of 2012, 2013, and 2015. We show that differences in solar wind drivers lead to different dynamical ionosphere-thermosphere (IT) responses and to different preconditioning of the IT system. We introduce a new hourly based global metric for average low-latitude and northern middle-latitude vertical total electron content responses in the morning, afternoon, and evening local time ranges, derived from measurements from globally distributed Global Navigation Satellite System ground stations. Our novel technique of estimating nitric oxide (NO) cooling radiation in 11 degrees latitudinal zones is based on Thermosphere-Ionosphere-Mesosphere Energetics and Dynamics (TIMED)/Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) measurements. The thermospheric cooling throughout the storm phases is studied with this high latitudinal resolution for the first time. Additionally, TIMED/Global Ultraviolet Imager (GUVI) observations of the dynamical response of the thermospheric composition (O/N-2 ratio) are utilized to study negative ionospheric storm effects. Based on these data sets, we describe and quantify distinct IT responses to driving by ICME sheaths, magnetic clouds, coronal loop remnants, plasma discontinuities, and high-speed streams following ICMEs. Our analysis of coupling functions indicates strong connection between coupling with the solar wind and IT system response in ICME-type storms and also some differences. Knowledge of interplanetary features is crucial for understanding IT storm dynamics. C1 [Verkhoglyadova, O. P.; Tsurutani, B. T.; Mannucci, A. J.; Komjathy, A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Mlynczak, M. G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Hunt, L. A.] Sci Syst & Applicat Inc, Hampton, VA USA. [Paxton, L. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Verkhoglyadova, OP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Olga.Verkhoglyadova@jpl.nasa.gov RI Paxton, Larry/D-1934-2015; OI Paxton, Larry/0000-0002-2597-347X; Hunt, Linda/0000-0002-5330-541X FU NASA TIMED project office FX Portions of this work were done at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. M. Mlynczak and L. Paxton would like to acknowledge support from the NASA TIMED project office. O. Verkhoglyadova would like to thank M. Butala (now at University of Illinois at Urbana-Champaign) for help with TEC data processing and E. Astafyeva for stimulating discussions. SABER data are available at http://saber.gats-inc.com/. GUVI data are available at http://timedguvi.jhuapl.edu. Solar wind parameters and activity indices are taken from the OMNI database (http://omniweb.gsfc.nasa.gov/form/omni_min.html). We acknowledge IGS data service, Geoscience Australia (ftp://ftp.ga.gov.au/geodesy-outgoing/gnss/pub/maps/argn_map.pdf) and the Geospatial Information Authority of Japan for providing GEONET data (http://www.gsi.go.jp/ENGLISH/page_e30233.html). ACE magnetometer data were provided by the ACE Science Center through http://www.srl.caltech.edu/ACE/ASC/level2/index.html. NR 75 TC 1 Z9 1 U1 3 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 SEP PY 2016 VL 121 IS 9 BP 8900 EP 8923 DI 10.1002/2016JA022883 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4QM UT WOS:000385844000048 ER PT J AU Zhou, YL Luhr, H Xiong, C Pfaff, RF AF Zhou, Yun-Liang Luehr, Hermann Xiong, Chao Pfaff, Robert F. TI Ionospheric storm effects and equatorial plasma irregularities during the 17-18 March 2015 event SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE ionospheric storms; equatorial plasma irregularities; prompt penetration electric field; disturbance dynamo electric field ID PATRICKS DAY STORM; GEOMAGNETIC STORMS; ELECTRIC-FIELDS; F-REGION; THERMOSPHERIC DYNAMICS; TOPSIDE IONOSPHERE; CHAMP OBSERVATIONS; BUBBLE OCCURRENCE; MAGNETIC STORM; LOW LATITUDES AB The intense magnetic storm on 17-18 March 2015 caused large disturbances of the ionosphere. Based on the plasma density (Ni) observations performed by the Swarm fleet of satellites, the Gravity Recovery and Climate Experiment mission, and the Communications/Navigation Outage Forecasting System satellite, we characterize the storm-related perturbations at low latitudes. All these satellites sampled the ionosphere in morning and evening time sectors where large modifications occurred. Modifications of plasma density are closely related to changes of the solar wind merging electric field (E-m). We consider two mechanisms, prompt penetration electric field (PPEF) and disturbance dynamo electric field (DDEF), as the main cause for the Ni redistribution, but effects of meridional wind are also taken into account. At the start of the storm main phase, the PPEF is enhancing plasma density on the dayside and reducing it on the nightside. Later, DDEF takes over and causes the opposite reaction. Unexpectedly, there appears during the recovery phase a strong density enhancement in the morning/prenoon sector and a severe Ni reduction in the afternoon/evening sector, and we suggest a combined effect of vertical plasma drift, and meridional wind is responsible for these ionospheric storm effects. Different from earlier studies about this storm, we also investigate the influence of storm dynamics on the initiation of equatorial plasma irregularities (EPIs). Shortly after the start of the storm main phase, EPIs appear in the postsunset sector. As a response to a short-lived decline of E-m, EPI activity appears in the early morning sector. Following the second start of the main phase, EPIs are generated for a few hours in the late evening sector. However, for the rest of the storm main phase, no more EPIs are initiated for more than 12h. Only after the onset of recovery phase does EPI activity start again in the postmidnight sector, lasting more than 7h. This comprehensive view of ionospheric storm effects and plasma irregularities adds to our understanding of conditions that lead to ionospheric instabilities. C1 [Zhou, Yun-Liang] Wuhan Univ, Sch Elect Informat, Dept Space Phys, Wuhan, Peoples R China. [Zhou, Yun-Liang; Luehr, Hermann; Xiong, Chao] GFZ German Res Ctr Geosci, Potsdam, Germany. [Pfaff, Robert F.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD USA. RP Luhr, H (reprint author), GFZ German Res Ctr Geosci, Potsdam, Germany. EM hluehr@gfz-potsdam.de RI Barbosa, Flavio/G-3630-2013 FU Space Agency of the German Aerospace Center (DLR) through funds of the Federal Ministry of Economics and Technology; National Nature Science Foundation of China [41274194, 41431073]; China Scholarship Council [201506275011] FX The European Space Agency (ESA) is acknowledged for providing the Swarm data. The electron density is obtained from http://earth.esa.int/swarm. The GRACE mission is sponsored by the Space Agency of the German Aerospace Center (DLR) through funds of the Federal Ministry of Economics and Technology. The GRACE data are available at the Information System and Data Center (ISDC) of GFZ German Research Centre for Geosciences. Data set names are as follows: GA-OG-1B-NAVSOL, GB-OG-1B-NAVSOL, and GX-OG-1B-KBRDAT. The solar wind and interplanetary magnetic field data are derived from NASA's ACE mission, and they can be found at http://www.srl.caltech.edu/ACE/ASC/level2/. The SYMH data are provided by the World Data Center for Geomagnetism, Kyoto, and downloaded from http://wdc.kugi.kyoto-u.ac.jp/aeasy/index.html. The global ionospheric maps (GIM) are available from ftp://cddis.gsfc.nasa.gov/gps/products/ionex/. The work of YunLiang Zhou is supported by the National Nature Science Foundation of China (41274194 and 41431073) and China Scholarship Council (201506275011). NR 58 TC 1 Z9 1 U1 6 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 SEP PY 2016 VL 121 IS 9 BP 9146 EP 9163 DI 10.1002/2016JA023122 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4QM UT WOS:000385844000065 ER PT J AU Qiu, JX Crow, WT Nearing, GS AF Qiu, Jianxiu Crow, Wade T. Nearing, Grey S. TI The Impact of Vertical Measurement Depth on the Information Content of Soil Moisture for Latent Heat Flux Estimation SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID NEAR-SURFACE; ERS SCATTEROMETER; ASSIMILATION; VALIDATION; VEGETATION; PRODUCTS; QUALITY AB This study aims to identify the impact of vertical support on the information content of soil moisture (SM) for latent heat flux estimation. This objective is achieved via calculation of the mutual information (MI) content between multiple soil moisture variables (with different vertical supports) and current/future evaporative fraction (EF) using ground-based soil moisture and latent/sensible heat flux observations acquired from the AmeriFlux network within the contiguous United States. Through the intercomparison of MI results from different SM-EF pairs, the general value (for latent heat flux estimation) of superficial soil moisture observations theta(S), vertically integrated soil moisture observations theta(V), and vertically extrapolated soil moisture time series [soil wetness index (SWI) from a simple low-pass transformation of theta(S)] are examined. Results suggest that, contrary to expectations, 2-day averages of theta(S) and theta(V) have comparable mutual information with regards to EF. That is, there is no clear evidence that the information content for flux estimation is enhanced via deepening the vertical support of superficial soil moisture observations. In addition, the utility of SWI in monitoring and forecasting EF is partially dependent on the adopted parameterization of time-scale parameter T in the exponential filter. Similar results are obtained when analyses are conducted at the monthly time scale, only with larger error bars. The contrast between the results of this paper and past work focusing on utilizing soil moisture to predict vegetation condition demonstrates that the particular application should be considered when characterizing the information content of soil moisture time series measurements. C1 [Qiu, Jianxiu] Sun Yat Sen Univ, Sch Geog & Planning, Guangdong Prov Key Lab Urbanizat & Geosimulat, 135 Xingang Xi Rd, Guangzhou 510275, Guangdong, Peoples R China. [Crow, Wade T.] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD USA. [Nearing, Grey S.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD USA. RP Qiu, JX (reprint author), Sun Yat Sen Univ, Sch Geog & Planning, Guangdong Prov Key Lab Urbanizat & Geosimulat, 135 Xingang Xi Rd, Guangzhou 510275, Guangdong, Peoples R China. EM qiujianxiu@mail.sysu.edu.cn FU National Natural Science Foundation of China [41501450]; Natural Science Foundation of Guangdong Province, China [2016A030310154]; Fundamental Research Funds for the Central Universities [16lgpy06] FX This work was supported by National Natural Science Foundation of China (Grant 41501450), Natural Science Foundation of Guangdong Province, China (Grant 2016A030310154), and the Fundamental Research Funds for the Central Universities (16lgpy06). We thank the anonymous reviewers for their helpful comments. NR 31 TC 1 Z9 1 U1 3 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD SEP PY 2016 VL 17 IS 9 BP 2419 EP 2430 DI 10.1175/JHM-D-16-0044.1 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DY8YZ UT WOS:000385419800005 ER PT J AU Tan, J Petersen, WA Tokay, A AF Tan, Jackson Petersen, Walter A. Tokay, Ali TI A Novel Approach to Identify Sources of Errors in IMERG for GPM Ground Validation SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID MULTISATELLITE PRECIPITATION ANALYSIS; UNCERTAINTY QUANTIFICATION; PASSIVE MICROWAVE; UNITED-STATES; ANALYSIS TMPA; DAY-1 IMERG; REAL-TIME; PRODUCTS; RESOLUTION; RAINFALL AB The comparison of satellite and high-quality, ground-based estimates of precipitation is an important means to assess the confidence in satellite-based algorithms and to provide a benchmark for their continued development and future improvement. To these ends, it is beneficial to identify sources of estimation uncertainty, thereby facilitating a precise understanding of the origins of the problem. This is especially true for new datasets such as the Integrated Multisatellite Retrievals for GPM(IMERG) product, which provides global precipitation gridded at a high resolution using measurements from different sources and techniques. Here, IMERG is evaluated against a dense network of gauges in the mid-Atlantic region of the United States. A novel approach is presented, leveraging ancillary variables in IMERG to attribute the errors to the individual instruments or techniques within the algorithm. As a whole, IMERG exhibits some misses and false alarms for rain detection, while its rain-rate estimates tend to overestimate drizzle and underestimate heavy rain with considerable random error. Tracing the errors to their sources, the most reliable IMERG estimates come from passive microwave satellites, which in turn exhibit a hierarchy of performance. The morphing technique has comparable proficiency with the less skillful satellites, but infrared estimations perform poorly. The approach here demonstrated that, underlying the overall reasonable performance of IMERG, different sources have different reliability, thus enabling both IMERG users and developers to better recognize the uncertainty in the estimate. Future validation efforts are urged to adopt such a categorization to bridge between gridded rainfall and instantaneous satellite estimates. C1 [Tan, Jackson] Univ Space Res Assoc, Greenbelt, MD USA. [Tan, Jackson; Tokay, Ali] NASA, Goddard Space Flight Ctr, Code 613,Bldg 33,Room C327,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. [Petersen, Walter A.] NASA, Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL USA. [Tokay, Ali] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. RP Tan, J (reprint author), NASA, Goddard Space Flight Ctr, Code 613,Bldg 33,Room C327,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM jackson.tan@nasa.gov RI Measurement, Global/C-4698-2015; OI Tan, Jackson/0000-0001-7085-3074 FU GPM Mission; PMM Science Team FX We thank George Huffman and David Bolvin for informative discussions on IMERG and Yudong Tian for instructive consultation on the multiplicative error model. The gauge data are maintained by the NASA Wallops GPM GV Team, and we acknowledge David Wolff for his assistance with the data. The MRMS data were processed for the GPM GV Program by Pierre-Emmanuel Kirstetter, and we appreciate the further assistance provided by Jianxin Wang. We also thank two anonymous reviewers for their comments and suggestions. J.T. is supported by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Universities Space Research Association through a contract with NASA. W.A.P. and A.T. acknowledge support from the GPM Mission (Project Scientist, Gail S. Jackson, and GV Systems Manager, Mathew Schwaller) and also PMM Science Team funding provided by Dr. Ramesh Kakar. The IMERG data were provided by the NASA Goddard Space Flight Center's PMM and PPS teams, which develop and compute the IMERG as a contribution to GPM, and archived at the NASA GES DISC. All codes used in this analysis are freely available at https://github.com/JacksonTanBS/2016_Tan-et-al._JHM. NR 52 TC 1 Z9 1 U1 10 U2 10 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD SEP PY 2016 VL 17 IS 9 BP 2477 EP 2491 DI 10.1175/JHM-D-16-0079.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DY8YZ UT WOS:000385419800008 ER PT J AU Righter, K Cosca, MA Morgan, LE AF Righter, K. Cosca, M. A. Morgan, L. E. TI Preservation of ancient impact ages on the R chondrite parent body: Ar-40/Ar-39 age of hornblende-bearing R chondrite LAP 04840 SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID INNER SOLAR-SYSTEM; RUMURUTI CHONDRITE; EXPOSURE AGES; HISTORY; MINERALOGY; METEORITE; AMPHIBOLE; SHOCK; ABUNDANCES; CHRONOLOGY AB The hornblende- and biotite-bearing R chondrite LAP 04840 is a rare kind of meteorite possibly containing outer solar system water stored during metamorphism or postshock annealing deep within an asteroid. Because little is known regarding its age and origin, we determined Ar-40/Ar-39 ages on hornblende-rich separates of the meteorite, and obtained plateau ages of 4340(+/- 40) to 4380(+/- 30) Ma. These well-defined plateau ages, coupled with evidence for postshock annealing, indicate this meteorite records an ancient shock event and subsequent annealing. The age of 4340-4380Ma (or 4.34-4.38Ga) for this and other previously dated R chondrites is much older than most impact events recorded by ordinary chondrites and points to an ancient event or events that predated the late heavy bombardment that is recorded in so many meteorites and lunar samples. C1 [Righter, K.] NASA, Johnson Space Ctr, Mailcode XI2,2101 NASA Pkwy, Houston, TX 77058 USA. [Cosca, M. A.; Morgan, L. E.] US Geol Survey, Denver Fed Ctr, MS 963, Denver, CO 80225 USA. RP Righter, K (reprint author), NASA, Johnson Space Ctr, Mailcode XI2,2101 NASA Pkwy, Houston, TX 77058 USA. EM kevin.righter-1@nasa.gov FU RTOP from NASA Cosmochemistry program; NSF; NASA FX Funding for this study was provided by an RTOP to KR from the NASA Cosmochemistry program. U.S. Antarctic meteorite samples are recovered by the Antarctic Search for Meteorites (ANSMET) program which has been funded by NSF and NASA, and characterized and curated by the Department of Mineral Sciences of the Smithsonian Institution and Astromaterials Curation Office at NASA Johnson Space Center. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the U.S. government. Reviews by J. Park, M. McCanta, and comments of AE Yamaguchi helped to improve presentation of our results. NR 47 TC 0 Z9 0 U1 2 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2016 VL 51 IS 9 BP 1678 EP 1684 DI 10.1111/maps.12692 PG 7 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DW4QX UT WOS:000383629200008 ER PT J AU Pugh, TAM Muller, C Elliott, J Deryng, D Folberth, C Olin, S Schmid, E Arneth, A AF Pugh, T. A. M. Mueller, C. Elliott, J. Deryng, D. Folberth, C. Olin, S. Schmid, E. Arneth, A. TI Climate analogues suggest limited potential for intensification of production on current croplands under climate change SO NATURE COMMUNICATIONS LA English DT Article ID RISING CO2 CONCENTRATIONS; CROP YIELD; IMPACTS; FOOD; AGRICULTURE; MANAGEMENT; MODEL AB Climate change could pose a major challenge to efforts towards strongly increase food production over the coming decades. However, model simulations of future climate-impacts on crop yields differ substantially in the magnitude and even direction of the projected change. Combining observations of current maximum-attainable yield with climate analogues, we provide a complementary method of assessing the effect of climate change on crop yields. Strong reductions in attainable yields of major cereal crops are found across a large fraction of current cropland by 2050. These areas are vulnerable to climate change and have greatly reduced opportunity for agricultural intensification. However, the total land area, including regions not currently used for crops, climatically suitable for high attainable yields of maize, wheat and rice is similar by 2050 to the present-day. Large shifts in land-use patterns and crop choice will likely be necessary to sustain production growth rates and keep pace with demand. C1 [Pugh, T. A. M.; Arneth, A.] Karlsruhe Inst Technol, Inst Meteorol & Climate Res Atmospher Environm Re, Kreuzeckbahnstr 19, D-82467 Garmisch Partenkirchen, Germany. [Pugh, T. A. M.] Univ Birmingham, Sch Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England. [Pugh, T. A. M.] Univ Birmingham, Birmingham Inst Forest Res, Birmingham B15 2TT, W Midlands, England. [Mueller, C.] Potsdam Inst Climate Impact Res, POB 60 12 03, D-14412 Potsdam, Germany. [Elliott, J.; Deryng, D.] Univ Chicago, Chicago, IL 60637 USA. [Elliott, J.; Deryng, D.] Argonne Natl Lab, Computat Inst, Chicago, IL 60637 USA. [Deryng, D.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. [Deryng, D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Folberth, C.] Int Inst Appl Syst Anal, Ecosyst Serv & Management Program, A-2361 Laxenburg, Austria. [Folberth, C.] Univ Munich, Dept Geog, D-80333 Munich, Germany. [Olin, S.] Lund Univ, Dept Phys Geog & Ecosyst Sci, Solvegatan 12, S-22362 Lund, Sweden. [Schmid, E.] Univ Nat Resources & Life Sci, Dept Econ & Social Sci, Feistmantelstr 4, A-1180 Vienna, Austria. RP Pugh, TAM (reprint author), Karlsruhe Inst Technol, Inst Meteorol & Climate Res Atmospher Environm Re, Kreuzeckbahnstr 19, D-82467 Garmisch Partenkirchen, Germany. EM t.a.m.pugh@bham.ac.uk RI Deryng, Delphine/F-7417-2010; Pugh, Thomas/A-3790-2010; OI Deryng, Delphine/0000-0001-6214-7241; Pugh, Thomas/0000-0002-6242-7371; Schmid, Erwin/0000-0003-4783-9666; Muller, Christoph/0000-0002-9491-3550 FU European Commission [603542 (LUC4C)]; German Federal Ministry of Education and Research (BMBF), through the Helmholtz Association; MACMIT project - BMBF [01LN1317A]; Research Fellowship of Ludwig Maximilian University Munich; Global Gridded Crop Model Intercomparison project (GGCMI) of the Agricultural Model Intercomparison and Improvement Project (AgMIP) FX T.A.M.P. and A.A. were funded by the European Commission's 7th Framework Programme, under Grant Agreement number 603542 (LUC4C). This work was supported, in part, by the German Federal Ministry of Education and Research (BMBF), through the Helmholtz Association and its research program ATMO. C.M. acknowledges financial support from the MACMIT project (01LN1317A) funded through the BMBF. C.F. was supported by a Research Fellowship of Ludwig Maximilian University Munich. We acknowledge the World Climate Research Programme's Working Group on Coupled Modelling, which is responsible for CMIP, and we thank the climate modelling groups for producing and making available their model output. The Global Gridded Crop Model Intercomparison project (GGCMI) of the Agricultural Model Intercomparison and Improvement Project (AgMIP) is thanked for funding travel to workshops where the ideas in this manuscript were developed. This is paper number 17 of the Birmingham Institute of Forest Research. NR 34 TC 0 Z9 0 U1 9 U2 9 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 SEP PY 2016 VL 7 AR 12608 DI 10.1038/ncomms12608 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DY7BH UT WOS:000385283700001 PM 27646707 ER PT J AU Wang, ZC Monteiro, CD Jagodnik, KM Fernandez, NF Gundersen, GW Rouillard, AD Jenkins, SL Feldmann, AS Hu, KS McDermott, MG Duan, QN Clark, NR Jones, MR Kou, Y Goff, T Woodland, H Amaral, FMR Szeto, GL Fuchs, O Rose, SMSF Sharma, S Schwartz, U Bausela, XB Szymkiewicz, M Maroulis, V Salykin, A Barra, CM Kruth, CD Bongio, NJ Mathur, V Todoric, RD Rubin, UE Malatras, A Fulp, CT Galindo, JA Motiejunaite, R Juschke, C Dishuck, PC Lahl, K Jafari, M Aibar, S Zaravinos, A Steenhuizen, LH Allison, LR Gamallo, P Segura, FD Devlin, TD Perez-Garcia, V Ma'ayan, A AF Wang, Zichen Monteiro, Caroline D. Jagodnik, Kathleen M. Fernandez, Nicolas F. Gundersen, Gregory W. Rouillard, Andrew D. Jenkins, Sherry L. Feldmann, Axel S. Hu, Kevin S. McDermott, Michael G. Duan, Qiaonan Clark, Neil R. Jones, Matthew R. Kou, Yan Goff, Troy Woodland, Holly Amaral, Fabio M. R. Szeto, Gregory L. Fuchs, Oliver Rose, Sophia M. Schussler-Fiorenza Sharma, Shvetank Schwartz, Uwe Bengoetxea Bausela, Xabier Szymkiewicz, Maciej Maroulis, Vasileios Salykin, Anton Barra, Carolina M. Kruth, Candice D. Bongio, Nicholas J. Mathur, Vaibhav Todoric, Radmila D. Rubin, Udi E. Malatras, Apostolos Fulp, Carl T. Galindo, John A. Motiejunaite, Ruta Jueschke, Christoph Dishuck, Philip C. Lahl, Katharina Jafari, Mohieddin Aibar, Sara Zaravinos, Apostolos Steenhuizen, Linda H. Allison, Lindsey R. Gamallo, Pablo de Andres Segura, Fernando Devlin, Tyler Dae Perez-Garcia, Vicente Ma'ayan, Avi TI Extraction and analysis of signatures from the Gene Expression Omnibus by the crowd SO NATURE COMMUNICATIONS LA English DT Article ID FACIOSCAPULOHUMERAL MUSCULAR-DYSTROPHY; ENDOMETRIAL CANCER-RISK; ESTROGEN-RECEPTOR; HEPATOCELLULAR-CARCINOMA; DIFFERENTIAL EXPRESSION; DATABASE; DISEASE; DISCOVERY; INSULIN; GROWTH AB Gene expression data are accumulating exponentially in public repositories. Reanalysis and integration of themed collections from these studies may provide new insights, but requires further human curation. Here we report a crowdsourcing project to annotate and reanalyse a large number of gene expression profiles from Gene Expression Omnibus (GEO). Through a massive open online course on Coursera, over 70 participants from over 25 countries identify and annotate 2,460 single-gene perturbation signatures, 839 disease versus normal signatures, and 906 drug perturbation signatures. All these signatures are unique and are manually validated for quality. Global analysis of these signatures confirms known associations and identifies novel associations between genes, diseases and drugs. The manually curated signatures are used as a training set to develop classifiers for extracting similar signatures from the entire GEO repository. We develop a web portal to serve these signatures for query, download and visualization. C1 [Wang, Zichen; Monteiro, Caroline D.; Jagodnik, Kathleen M.; Fernandez, Nicolas F.; Gundersen, Gregory W.; Rouillard, Andrew D.; Jenkins, Sherry L.; Feldmann, Axel S.; Hu, Kevin S.; McDermott, Michael G.; Duan, Qiaonan; Clark, Neil R.; Jones, Matthew R.; Kou, Yan; Goff, Troy; Ma'ayan, Avi] Icahn Sch Med Mt Sinai, Dept Pharmacol Sci, LINCS Data Coordinat & Integrat Ctr BD2K, Illuminating Druggable Genome Knowledge Managemen, One Gustave L Levy Pl Box 1215, New York, NY 10029 USA. [Jagodnik, Kathleen M.] NASA, Fluid Phys & Transport Processes Branch, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. [Jagodnik, Kathleen M.] Baylor Coll Med, Ctr Space Med, 1 Baylor Plaza, Houston, TX 77030 USA. [Woodland, Holly] Daylesford, Weybridge KT13 0RZ, Surrey, England. [Amaral, Fabio M. R.] Univ Nottingham, Sch Biosci, Sutton Bonington Campus, Loughborough LE12 5RD, Leics, England. [Szeto, Gregory L.] MIT, Dept Biol Engn, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Szeto, Gregory L.] MIT, David H Koch Inst Integrat Canc Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Szeto, Gregory L.] MIT, Dept Mat Sci & Engn, Cambridge, MA 02139 USA. [Szeto, Gregory L.] MIT, Ragon Inst MGH, 400 Technol Sq, Cambridge, MA 02139 USA. [Szeto, Gregory L.] Harvard, 400 Technol Sq, Cambridge, MA 02139 USA. [Fuchs, Oliver] Univ Munich, German Ctr Lung Res DZL, Dr von Hauner Univ Childrens Hosp, Paediat Allergol & Pulmonol, Lindwurmstr 4, D-80337 Munich, Germany. [Rose, Sophia M. Schussler-Fiorenza] Veteran Affairs Palo Alto Hlth Care Syst, Spinal Cord Injury Serv, Palo Alto, CA 94304 USA. [Rose, Sophia M. Schussler-Fiorenza] Stanford Sch Med, Dept Neurosurg, Stanford, CA 94304 USA. [Sharma, Shvetank] Inst Liver & Biliary Sci, Dept Res, D1 Vasant Kunj, New Delhi 110070, India. [Schwartz, Uwe] Univ Regensburg, Dept Biochem 3, Univ Str 31, D-93053 Regensburg, Germany. [Bengoetxea Bausela, Xabier] Univ Navarra, Dept Pharmacol & Toxicol, Irunlarrea 1, E-31008 Pamplona, Spain. [Szymkiewicz, Maciej] Polish Acad Sci, Warsaw Sch Informat Technol Auspices, 6 Newelska St, PL-01447 Warsaw, Poland. [Maroulis, Vasileios] Plomariou 1 St, Athens 15126, Greece. [Salykin, Anton] Masaryk Univ, Fac Med, Dept Biol, Brno 62500, Czech Republic. [Barra, Carolina M.] Hosp del Mar, IMIM, PRBB Barcelona, Dr Aiguader 88, Barcelona 08003, Spain. [Kruth, Candice D.] 85 Hailey Ln,Apt C-11, Strasburg, VA 22657 USA. [Bongio, Nicholas J.] Shenandoah Univ, Dept Biol, 1460 Univ Dr Winchester, Winchester, VA 22601 USA. [Mathur, Vaibhav] IBM India Pvt Ltd, Bengaluru 560045, India. [Todoric, Radmila D.] Dr Aleksandra Sijacica 20, Backa Topola 24300, Serbia. [Rubin, Udi E.] Columbia Univ, Dept Biol Sci, 600 Fairchild Ctr,Mail Code 2402, New York, NY 10032 USA. [Malatras, Apostolos] Univ Paris 04, Univ Paris 06, INSERM UMRS975, Ctr Res Myol,CNRS FRE3617, 47 Blvd Hop, F-75013 Paris, France. [Fulp, Carl T.] 13-1,Higashi 4 Chome Shibuya Ku, Tokyo 1500011, Japan. [Galindo, John A.] Univ Nacl Colombia, Dept Biol, Cr 30 45-08, Bogota, Colombia. [Galindo, John A.] Univ Nacl Colombia, Inst Genet, Cr 30 45-08, Bogota, Colombia. [Motiejunaite, Ruta] Brigham & Womens Hosp, Ctr Interdisciplinary Cardiovasc Sci, 3 Blackfan Circle, Boston, MA 02115 USA. [Jueschke, Christoph] Carl von Ossietzky Univ Oldenburg, Fac Med & Hlth Sci, Dept Human Genet, Ammerlander Heerstr 114-118, D-26129 Oldenburg, Germany. [Dishuck, Philip C.] 2312 40th ST NW 2, Washington, DC 20007 USA. [Lahl, Katharina] Tech Univ Denmark, Natl Vet Inst, Bulowsvej 27 Bldg 2-3, DK-1870 Frederiksberg, Denmark. [Jafari, Mohieddin] Pasteur Inst Iran, Biotechnol Res Ctr, Prot Chem & Prote Unit, 358,12th Farwardin Ave,Jomhhoori St, Tehran 13164, Iran. [Jafari, Mohieddin] Inst Res Fundamental Sci, Sch Biol Sci, Niavaran Sq,POB, Tehran 193955746, Iran. [Aibar, Sara] Univ Salamanca, Madrid 37008, Spain. [Zaravinos, Apostolos] Karolinska Inst, Dept Lab Med, Div Clin Immunol, Alfred Nobels Alle 8,Level 7, SE-14186 Stockholm, Sweden. [Zaravinos, Apostolos] European Univ Cyprus, Sch Sci, Dept Life Sci, 6 Diogenes Str Engomi,POB 22006, CY-1516 Nicosia, Cyprus. [Steenhuizen, Linda H.] Anna Blamansingel 216, NL-102 SW Amsterdam, Netherlands. [Allison, Lindsey R.] 7300 Brompton 6024, Houston, TX 77025 USA. [Gamallo, Pablo] Aligustre 30 1-C, Madrid 28039, Spain. [de Andres Segura, Fernando] Extremadura Univ Hosp, Clin Res Ctr, CICAB, Elvas Av,S-N 06006, Badajoz 06006, Spain. [Devlin, Tyler Dae] 69 Brown St,Box 8278, Providence, RI 02912 USA. [Perez-Garcia, Vicente] CSIC, Ctr Nacl Biotecnol, Dept Immunol & Oncol, C-Darwin 3, E-28049 Madrid, Spain. RP Ma'ayan, A (reprint author), Icahn Sch Med Mt Sinai, Dept Pharmacol Sci, LINCS Data Coordinat & Integrat Ctr BD2K, Illuminating Druggable Genome Knowledge Managemen, One Gustave L Levy Pl Box 1215, New York, NY 10029 USA. EM avi.maayan@mssm.edu OI Wang, Zichen/0000-0002-1415-1286; Szymkiewicz, Maciej/0000-0003-1469-9396; Schussler-Fiorenza Rose, Sophia Miryam/0000-0002-6311-6671; De Andres, Fernando/0000-0003-1076-0743 FU NIH [R01GM098316, U54HL127624, U54CA189201] FX This work is supported by NIH grants: R01GM098316, U54HL127624 and U54CA189201 to A.M. NR 78 TC 1 Z9 1 U1 5 U2 5 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 SEP PY 2016 VL 7 AR 12846 DI 10.1038/ncomms12846 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DY8FA UT WOS:000385363000014 PM 27667448 ER PT J AU Kassemi, M Thompson, D AF Kassemi, Mohammad Thompson, David TI Prediction of renal crystalline size distributions in space using a PBE analytic model. 1. Effect of microgravity-induced biochemical alterations SO AMERICAN JOURNAL OF PHYSIOLOGY-RENAL PHYSIOLOGY LA English DT Article DE nephrolithiasis; gravity; weightlessness; crystal nucleation; crystal growth; agglomeration ID URINARY STONE FORMATION; CALCIUM-OXALATE; RISK-FACTORS; GROWTH; DISEASE; AGGLOMERATION; INHIBITION; ASTRONAUTS; KINETICS; KIDNEY AB An analytical Population Balance Equation model is developed and used to assess the risk of critical renal stone formation for astronauts during future space missions. The model uses the renal biochemical profile of the subject as input and predicts the steady-state size distribution of the nucleating, growing, and agglomerating calcium oxalate crystals during their transit through the kidney. The model is verified through comparison with published results of several crystallization experiments. Numerical results indicate that the model is successful in clearly distinguishing between 1-G normal and 1-G recurrent stone-former subjects based solely on their published 24-h urine biochemical profiles. Numerical case studies further show that the predicted renal calculi size distribution for a microgravity astronaut is closer to that of a recurrent stone former on Earth rather than to a normal subject in 1 G. This interestingly implies that the increase in renal stone risk level in microgravity is relatively more significant for a normal person than a stone former. However, numerical predictions still underscore that the stone-former subject carries by far the highest absolute risk of critical stone formation during space travel. C1 [Kassemi, Mohammad; Thompson, David] NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, 21000 Brookpark Rd,MS 110-3, Cleveland, OH 44135 USA. RP Kassemi, M (reprint author), NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, 21000 Brookpark Rd,MS 110-3, Cleveland, OH 44135 USA. EM Mohammad.Kassemi@nasa.gov FU Exploration Medical Capabilities Element of NASA's Human Research FX We gratefully acknowledge funding support from the Exploration Medical Capabilities Element of NASA's Human Research. NR 41 TC 0 Z9 0 U1 2 U2 2 PU AMER PHYSIOLOGICAL SOC PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA SN 1931-857X EI 1522-1466 J9 AM J PHYSIOL-RENAL JI Am. J. Physiol.-Renal Physiol. PD SEP 1 PY 2016 VL 311 IS 3 BP F520 EP F530 DI 10.1152/ajprenal.00401.2015 PG 11 WC Physiology; Urology & Nephrology SC Physiology; Urology & Nephrology GA DY3FZ UT WOS:000384977500004 PM 27279490 ER PT J AU Kassemi, M Thompson, D AF Kassemi, Mohammad Thompson, David TI Prediction of renal crystalline size distributions in space using a PBE analytic model. 2. Effect of dietary countermeasures SO AMERICAN JOURNAL OF PHYSIOLOGY-RENAL PHYSIOLOGY LA English DT Article DE nephrolithiasis; gravity; weightlessness; crystal nucleation; crystal growth; agglomeration; inhibition; dietary countermeasures ID OXALATE MONOHYDRATE CRYSTALLIZATION; POTASSIUM-MAGNESIUM CITRATE; CALCIUM-OXALATE; STONE FORMATION; DIHYDRATE CRYSTALLIZATION; BED REST; INHIBITION; GROWTH; URINE; FLIGHT AB An analytic Population Balance Equation model is used to assess the efficacy of citrate, pyrophosphate, and augmented fluid intake as dietary countermeasures aimed at reducing the risk of renal stone formation for astronauts. The model uses the measured biochemical profile of the astronauts as input and predicts the steady-state size distribution of the nucleating, growing, and agglomerating renal calculi subject to biochemical changes brought about by administration of these dietary countermeasures. Numerical predictions indicate that an increase in citrate levels beyond its average normal ground-based urinary values is beneficial but only to a limited extent. Unfortunately, results also indicate that any decline in the citrate levels during space travel below its normal urinary values on Earth can easily move the astronaut into the stone-forming risk category. Pyrophosphate is found to be an effective inhibitor since numerical predictions indicate that even at quite small urinary concentrations, it has the potential of shifting the maximum crystal aggregate size to a much smaller and plausibly safer range. Finally, our numerical results predict a decline in urinary volume below 1.5 liters/day can act as a dangerous promoter of renal stone development in microgravity while urinary volume levels of 2.5-3 liters/day can serve as effective space countermeasures. C1 [Kassemi, Mohammad; Thompson, David] NASA, Natl Ctr Space Explorat Res, Glenn Res Ctr, 21000 Brookpk Rd,MS 110-3, Cleveland, OH 44135 USA. RP Kassemi, M (reprint author), NASA, Natl Ctr Space Explorat Res, Glenn Res Ctr, 21000 Brookpk Rd,MS 110-3, Cleveland, OH 44135 USA. EM Mohammad.Kassemi@nasa.gov FU Exploration Medical Capabilities Element of NASA's Human Research Project FX We gratefully acknowledge funding support from the Exploration Medical Capabilities Element of NASA's Human Research Project. NR 44 TC 0 Z9 0 U1 3 U2 3 PU AMER PHYSIOLOGICAL SOC PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA SN 1931-857X EI 1522-1466 J9 AM J PHYSIOL-RENAL JI Am. J. Physiol.-Renal Physiol. PD SEP 1 PY 2016 VL 311 IS 3 BP F531 EP F538 DI 10.1152/ajprenal.00402.2015 PG 8 WC Physiology; Urology & Nephrology SC Physiology; Urology & Nephrology GA DY3FZ UT WOS:000384977500005 PM 27279491 ER PT J AU Mukai, K Luna, GJM Cusumano, G Segreto, A Munari, U Sokoloski, JL Lucy, AB Nelson, T Nunez, NE AF Mukai, K. Luna, G. J. M. Cusumano, G. Segreto, A. Munari, U. Sokoloski, J. L. Lucy, A. B. Nelson, T. Nunez, N. E. TI SU Lyncis, a hard X-ray bright M giant: clues point to a large hidden population of symbiotic stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: symbiotic; stars: individual: SU Lyn; X-rays: binaries ID SWIFT-BAT; T CRB; HIPPARCOS; EVOLUTION; OUTBURST; CATALOG; BINARY; NOVAE AB Symbiotic star surveys have traditionally relied almost exclusively on low resolution optical spectroscopy. However, we can obtain a more reliable estimate of their total Galactic population by using all available signatures of the symbiotic phenomenon. Here we report the discovery of a hard X-ray source, 4PBC J0642.9+5528, in the Swift hard X-ray all-sky survey, and identify it with a poorly studied red giant, SU Lyn, using pointed Swift observations and ground-based optical spectroscopy. The X-ray spectrum, the optical to UV spectrum, and the rapid UV variability of SU Lyn are all consistent with our interpretation that it is a symbiotic star containing an accreting white dwarf. The symbiotic nature of SU Lyn went unnoticed until now, because it does not exhibit emission lines strong enough to be obvious in low resolution spectra. We argue that symbiotic stars without shell-burning have weak emission lines, and that the current lists of symbiotic stars are biased in favour of shell-burning systems. We conclude that the true population of symbiotic stars has been underestimated, potentially by a large factor. C1 [Mukai, K.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Mukai, K.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Mukai, K.] Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA. [Luna, G. J. M.] UBA, CONICET, IAFE, Ave Inte Guiraldes 2620,C1428ZAA, Buenos Aires, DF, Argentina. [Cusumano, G.; Segreto, A.] INAF Ist Astrofis Spaziale & Fis Cosm, Via U La Malfa 153, I-90146 Palermo, Italy. [Munari, U.] INAF Astron Observ Padova, I-36012 Asiago, VI, Italy. [Sokoloski, J. L.; Lucy, A. B.] Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA. [Nelson, T.] Univ Pittsburgh, Dept Phys & Astron, 3941 OHara St, Pittsburgh, PA 15260 USA. [Nunez, N. E.] UNSJ, ICATE, CONICET, Ave Espana S E-1512,J5402 DSP, San Juan, Argentina. RP Mukai, K (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.; Mukai, K (reprint author), NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.; Mukai, K (reprint author), Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA. EM Koji.Mukai@nasa.gov FU NASA ADAP grant [NNX15AF19G]; [ANPCYT-PICT 0478/14] FX We thank Neil Gehrels, the PI of the Swift mission, for a generous allocation of TOO time. GJML and NEN are members of the 'Carrera del Investigador Cientifico (CIC)' of CONICET and acknowledge support from Argentina under grant ANPCYT-PICT 0478/14. JLS and ABL acknowledge support from NASA ADAP grant NNX15AF19G. JLS thanks Scott Kenyon for conversations (a decade ago) about shell burning and selection bias. NR 30 TC 1 Z9 1 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 1 PY 2016 VL 461 IS 1 BP L1 EP L5 DI 10.1093/mnrasl/slw087 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DV9OE UT WOS:000383269900001 ER PT J AU Fierce, L Bond, TC Bauer, SE Mena, F Riemer, N AF Fierce, Laura Bond, Tami C. Bauer, Susanne E. Mena, Francisco Riemer, Nicole TI Black carbon absorption at the global scale is affected by particle-scale diversity in composition SO NATURE COMMUNICATIONS LA English DT Article ID MIXING STATE; SIZE DISTRIBUTIONS; OPTICAL-PROPERTIES; LIGHT-ABSORPTION; BROWN CARBON; AEROSOL; SOOT; MODEL; CLIMATE; AMPLIFICATION AB Atmospheric black carbon (BC) exerts a strong, but uncertain, warming effect on the climate. BC that is coated with non-absorbing material absorbs more strongly than the same amount of BC in an uncoated particle, but the magnitude of this absorption enhancement (E-abs) is not well constrained. Modelling studies and laboratory measurements have found stronger absorption enhancement than has been observed in the atmosphere. Here, using a particle-resolved aerosol model to simulate diverse BC populations, we show that absorption is overestimated by as much as a factor of two if diversity is neglected and population-averaged composition is assumed across all BC-containing particles. If, instead, composition diversity is resolved, we find E-abs=1-1.5 at low relative humidity, consistent with ambient observations. This study offers not only an explanation for the discrepancy between modelled and observed absorption enhancement, but also demonstrates how particle-scale simulations can be used to develop relationships for global-scale models. C1 [Fierce, Laura] Brookhaven Natl Lab, Dept Environm & Climate Sci, Upton, NY 11973 USA. [Fierce, Laura] Univ Corp Atmospheric Res, Visiting Scientists Program, Boulder, CO 80307 USA. [Bond, Tami C.; Mena, Francisco] Univ Illinois, Dept Civil & Environm Engn, Urbana, IL 61801 USA. [Bauer, Susanne E.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Bauer, Susanne E.] Columbia Univ, Earth Inst, New York, NY 10025 USA. [Riemer, Nicole] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA. RP Fierce, L (reprint author), Brookhaven Natl Lab, Dept Environm & Climate Sci, Upton, NY 11973 USA.; Fierce, L (reprint author), Univ Corp Atmospheric Res, Visiting Scientists Program, Boulder, CO 80307 USA. EM lfierce@bnl.gov FU US Environmental Protection Agency [R83504201]; NASA [NNX09AK66G]; Department of Energy [DE-FG02-08ER64533]; Fulbright-Chile CONICYT fellowship; NOAA Climate & Global Change Postdoctoral Fellowship through the University Corporation for Atmospheric Research Visiting Scientists Program FX This work was supported by the US Environmental Protection Agency (R83504201) and by NASA (NNX09AK66G). F. Mena was funded by the Department of Energy under DE-FG02-08ER64533 and by a Fulbright-Chile CONICYT fellowship. L. Fierce is funded by a NOAA Climate & Global Change Postdoctoral Fellowship through the University Corporation for Atmospheric Research Visiting Scientists Program. NR 49 TC 3 Z9 3 U1 28 U2 29 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 SEP PY 2016 VL 7 AR 12361 DI 10.1038/ncomms12361 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DY3CG UT WOS:000384967800001 PM 27580627 ER PT J AU Thiery, W Davin, EL Seneviratne, SI Bedka, K Lhermitte, S van Lipzig, NPM AF Thiery, Wim Davin, Edouard L. Seneviratne, Sonia I. Bedka, Kristopher Lhermitte, Stef van Lipzig, Nicole P. M. TI Hazardous thunderstorm intensification over Lake Victoria SO NATURE COMMUNICATIONS LA English DT Article ID REGIONAL CLIMATE MODEL; AFRICAN GREAT-LAKES; EAST-AFRICA; PRECIPITATION EXTREMES; RESOLUTION MODEL; TEMPERATURE; IMPACT; BASIN; PARAMETERIZATION; SIMULATIONS AB Weather extremes have harmful impacts on communities around Lake Victoria, where thousands of fishermen die every year because of intense night-time thunderstorms. Yet how these thunderstorms will evolve in a future warmer climate is still unknown. Here we show that Lake Victoria is projected to be a hotspot of future extreme precipitation intensification by using new satellite-based observations, a high-resolution climate projection for the African Great Lakes and coarser-scale ensemble projections. Land precipitation on the previous day exerts a control on night-time occurrence of extremes on the lake by enhancing atmospheric convergence (74%) and moisture availability (26%). The future increase in extremes over Lake Victoria is about twice as large relative to surrounding land under a high-emission scenario, as only over-lake moisture advection is high enough to sustain Clausius-Clapeyron scaling. Our results highlight a major hazard associated with climate change over East Africa and underline the need for high-resolution projections to assess local climate change. C1 [Thiery, Wim; Lhermitte, Stef; van Lipzig, Nicole P. M.] Katholieke Univ Leuven, Dept Earth & Environm Sci, Celestijnenlaan 200E, B-3001 Leuven, Belgium. [Thiery, Wim; Davin, Edouard L.; Seneviratne, Sonia I.] ETH, Inst Atmospher & Climate Sci, Univ Str 16, CH-8092 Zurich, Switzerland. [Bedka, Kristopher] NASA, Langley Res Ctr, Sci Directorate, 21 Langley Blvd, Hampton, VA 23681 USA. [Lhermitte, Stef] Delft Univ Technol, Dept Geosci & Remote Sensing, Stevinweg 1, NL-2600 GA Delft, Netherlands. RP Thiery, W (reprint author), Katholieke Univ Leuven, Dept Earth & Environm Sci, Celestijnenlaan 200E, B-3001 Leuven, Belgium.; Thiery, W (reprint author), ETH, Inst Atmospher & Climate Sci, Univ Str 16, CH-8092 Zurich, Switzerland. EM wim.thiery@env.ethz.ch RI Davin, Edouard/L-7033-2016 OI Davin, Edouard/0000-0003-3322-9330 FU Research Foundation Flanders (FWO); ETH Zurich [Fel-45 15-1]; FWO; Belgian Science Policy Office (BELSPO) [CD/AR/02A]; Hercules Foundation; Flemish Government-department EWI FX We acknowledge the CLM community (http://www.clm-community.eu) for developing COSMO-CLM2 and making the model code available, and Hans-Jurgen Panitz for providing the lateral boundary conditions. In addition, we are grateful to the World Climate Research Programme (WRCP) for initiating and coordinating the CORDEX-Africa initiative, to the modelling centres for making their downscaling results publicly available through ESGF, to ECMWF for providing access to ERA-Interim, and to NASA and JAXA for developing the TRMM-3B42 data set. We particularly thank Fabien Chatterjee, Matthias Demuzere, David Docquier, Niels Souverijns and Kristof Van Tricht for their useful suggestions. W.T. was supported by a PhD fellowship from the Research Foundation Flanders (FWO) and an ETH Zurich postdoctoral fellowship (Fel-45 15-1). S.L. was supported by an FWO postdoctoral fellowship. The Belgian Science Policy Office (BELSPO) is acknowledged for the support through the research project EAGLES (CD/AR/02A). Computational resources and services used for the COSMO-CLM2 simulation were provided by the VSC (Flemish Supercomputer Center), funded by the Hercules Foundation and the Flemish Government-department EWI. NR 52 TC 4 Z9 4 U1 8 U2 8 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD SEP PY 2016 VL 7 AR 12786 DI 10.1038/ncomms12786 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DY6RU UT WOS:000385256500016 PM 27658848 ER PT J AU Donnelly, M AF Donnelly, Michael TI You can't sit in an office and issue edicts via email. You need to go where the work is being performed SO AEROSPACE AMERICA LA English DT Editorial Material C1 [Donnelly, Michael] NASA, OSIRIS REx, Washington, DC 20546 USA. RP Donnelly, M (reprint author), NASA, OSIRIS REx, Washington, DC 20546 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0740-722X J9 AEROSPACE AM JI Aerosp. Am. PD SEP PY 2016 VL 54 IS 8 BP 64 EP 64 PG 1 WC Engineering, Aerospace SC Engineering GA DX9TN UT WOS:000384738200015 ER PT J AU Han, JW Wong, HY Moon, DI Braga, N Meyyappan, M AF Han, Jin-Woo Wong, Hiu Yung Moon, Dong-Il Braga, Nelson Meyyappan, M. TI Stringer Gate FinFET on Bulk Substrate SO IEEE TRANSACTIONS ON ELECTRON DEVICES LA English DT Article DE FinFET; low standby power; steep retrograde well; stringer gate; sub-fin leakage ID SUBTHRESHOLD LOGIC; DEVICE DESIGN; SOI MOSFETS; OPTIMIZATION; TRANSISTORS; OPERATION; MOBILITY AB A gate stringer normally considered parasitic is used as a subthreshold leakage suppressor in a bulk FinFET. The gate stringer remaining along the source/drain extension suppresses the formation of a sub-fin leakage path and improves the subthreshold slope. The stringer gate structure is implemented by simple process modification in the gate etch step while the other process steps are unchanged. The fabricated stringer gate FinFET shows 35% reduction in the OFF-state leakage current compared with a conventional FinFET without a retrograde well process at the expense of only 5% increase in parasitic capacitance. The power-delay product enhancement at reduced drive voltage characteristics exhibits that the stringer gate FinFET can be an attractive candidate for low standby power and subthreshold logic applications. C1 [Han, Jin-Woo; Moon, Dong-Il; Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Wong, Hiu Yung; Braga, Nelson] Synopsys Inc, Mountain View, CA 94043 USA. RP Han, JW (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM jin-woo.han@nasa.gov; hywong@synopsys.com; dong-il.moon@nasa.gov; nelson.braga@synopsys.com; m.meyyappan@nasa.gov NR 27 TC 0 Z9 0 U1 3 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9383 EI 1557-9646 J9 IEEE T ELECTRON DEV JI IEEE Trans. Electron Devices PD SEP PY 2016 VL 63 IS 9 BP 3432 EP 3438 DI 10.1109/TED.2016.2586607 PG 7 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA DX7NK UT WOS:000384574400009 ER PT J AU Singh, D Swain, DL Mankin, JS Horton, DE Thomas, LN Rajaratnam, B Diffenbaugh, NS AF Singh, Deepti Swain, Daniel L. Mankin, Justin S. Horton, Daniel E. Thomas, Leif N. Rajaratnam, Bala Diffenbaugh, Noah S. TI Recent amplification of the North American winter temperature dipole SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE climate change detection; climate change impacts; extreme event attribution; atmospheric dynamics ID ARCTIC SEA-ICE; ATMOSPHERIC CIRCULATION; INTERNAL VARIABILITY; CALIFORNIA DROUGHT; CLIMATE; TRENDS; SNOW; PATTERNS; EXTREMES; WEATHER AB During the winters of 2013-2014 and 2014-2015, anomalously warm temperatures in western North America and anomalously cool temperatures in eastern North America resulted in substantial human and environmental impacts. Motivated by the impacts of these concurrent temperature extremes and the intrinsic atmospheric linkage between weather conditions in the western and eastern United States, we investigate the occurrence of concurrent warm-West/cool-East surface temperature anomalies, which we call the North American winter temperature dipole. We find that, historically, warm-West/cool-East dipole conditions have been associated with anomalous mid-tropospheric ridging over western North America and downstream troughing over eastern North America. We also find that the occurrence and severity of warm-West/cool-East events have increased significantly between 1980 and 2015, driven largely by an increase in the frequency with which high-amplitude ridge-trough wave patterns result in simultaneous severe temperature conditions in both the West and East. Using a large single-model ensemble of climate simulations, we show that the observed positive trend in the warm-West/cool-East events is attributable to historical anthropogenic emissions including greenhouse gases, but that the co-occurrence of extreme western warmth and eastern cold will likely decrease in the future as winter temperatures warm dramatically across the continent, thereby reducing the occurrence of severely cold conditions in the East. Although our analysis is focused on one particular region, our analysis framework is generally transferable to the physical conditions shaping different types of extreme events around the globe. C1 [Singh, Deepti; Swain, Daniel L.; Horton, Daniel E.; Thomas, Leif N.; Rajaratnam, Bala; Diffenbaugh, Noah S.] Stanford Univ, Dept Earth Syst Sci, Stanford, CA 94305 USA. [Singh, Deepti; Mankin, Justin S.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Mankin, Justin S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Horton, Daniel E.] Northwestern Univ, Dept Earth & Planetary Sci, Evanston, IL USA. [Horton, Daniel E.; Diffenbaugh, Noah S.] Stanford Univ, Woods Inst Environm, Stanford, CA 94305 USA. [Rajaratnam, Bala] Stanford Univ, Dept Stat, Stanford, CA 94305 USA. RP Singh, D (reprint author), Stanford Univ, Dept Earth Syst Sci, Stanford, CA 94305 USA.; Singh, D (reprint author), Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. EM dsingh@ldeo.columbia.edu OI Swain, Daniel/0000-0003-4276-3092 FU Lamont Doherty Postdoctoral Fellowship; Switzer Foundation; ARCS Foundation; Earth Institute Postdoctoral Fellowship; US National Science Foundation [DMS-CMG 1025465, AGS-1003823, DMS-1106642, DMS-CAREER-1352656]; U.S. Air Force Office of Scientific Research [FA9550-13-1-0043]; NSF AGS CAREER [0955283]; DOE Integrated Assessment Research Program [DE-SC005171] FX We thank the National Oceanic and Atmospheric Administration's NCDC for access to historical temperature and geopotential height data sets, PRISM Climate Group and University of Idaho for access to historical temperature data sets, and NCAR for access to the CESM LENS simulations. We also thank Nathaniel Johnson for providing us the Self-Organizing Maps algorithm. Our work is supported by the Lamont Doherty Postdoctoral Fellowship to D.S.; graduate fellowships from the Switzer Foundation and the ARCS Foundation to D.L.S.; Earth Institute Postdoctoral Fellowship to J.S.M.; US National Science Foundation grants DMS-CMG 1025465, AGS-1003823, DMS-1106642, and DMS-CAREER-1352656; and U.S. Air Force Office of Scientific Research grant award FA9550-13-1-0043 to B.R.; and NSF AGS CAREER grant 0955283 and DOE Integrated Assessment Research Program grant DE-SC005171 to N.S.D. Gridded 2 m temperatures, geopotential heights, meridional winds, and omega from the NCEP R1 and 2 m temperatures from the NCEP North American Regional Reanalysis (NARR) are available at the NOAA ESRL website (http://www.esrl.noaa.gov/psd/data/gridded/). Gridded temperatures from PRISM Climate Group and University of Idaho Metdata data sets are available at their respective websites (http://www.prism.oregonstate.edu/ and http://metdata.northwestknowledge.net/). All analysis scripts used in this study can be obtained by contacting Deepti Singh (dsingh@ldeo.columbia.edu). NR 56 TC 3 Z9 3 U1 10 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP PY 2016 VL 121 IS 17 BP 9911 EP 9928 DI 10.1002/2016JD025116 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DY0YV UT WOS:000384823000024 PM 27840780 ER PT J AU Payne, RC Britt, AV Chen, H Kasting, JF Catling, DC AF Payne, Rebecca C. Britt, Amber V. Chen, Howard Kasting, James F. Catling, David C. TI The response of Phanerozoic surface temperature to variations in atmospheric oxygen concentration SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE atmospheric O-2 levels; surface temperature; Phanerozoic climate; Cenomanian climate ID MODEL; EVOLUTION; RECORD; EARTH; TIME; O-2; CO2 AB Recently, Poulsen et al. (2015) suggested that O-2 has played a major role in climate forcing during the Phanerozoic. Specifically, they argued that decreased O-2 levels during the Cenomanian stage of the middle Cretaceous (94-100Ma) could help explain the extremely warm climate during that time. The postulated warming mechanism involves decreased Rayleigh scattering by a thinner atmosphere, which reduces the planetary albedo and allows greater surface warming. This warming effect is then amplified by cloud feedbacks within their 3-D climate model. This increase in shortwave surface forcing, in their calculations, exceeds any decrease in the greenhouse effect caused by decreased O-2. Here we use a 1-D radiative-convective climate model (with no cloud feedback) to check their results. We also include a self-consistent calculation of the change in atmospheric ozone and its effect on climate. Our results are opposite to those of Poulsen et al.: we find that the climate warms by 1.4K at 35% O-2 concentrations as a result of increased pressure broadening of CO2 and H2O absorption lines and cools by 0.8K at 10% O-2 as a result of decreased pressure broadening. The surface temperature changes are only about 1K either way, though, for reasonable variations in Phanerozoic O-2 concentrations (10%-35% by volume). Hence, it seems unlikely that changes in atmospheric O-2 account for the warm climate of the Cenomanian. Other factors, such as a higher-than-expected sensitivity of climate to increased CO2 concentrations, may be required to obtain agreement with the paleoclimate data. C1 [Payne, Rebecca C.; Britt, Amber V.; Kasting, James F.] Penn State Univ, Dept Geosci, State Coll, PA 16801 USA. [Chen, Howard] Northwestern Univ, Dept Earth & Planetary Sci, Evanston, IL USA. [Kasting, James F.] Penn State Astrobiol Res Ctr, University Pk, PA USA. [Kasting, James F.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Kasting, James F.; Catling, David C.] NASA, Astrobiol Inst, Virtual Planetary Lab, Seattle, WA USA. [Catling, David C.] Univ Washington, Dept Earth & Space Sci, Seattle, WA USA. RP Payne, RC (reprint author), Penn State Univ, Dept Geosci, State Coll, PA 16801 USA. EM rvp5143@psu.edu FU Undergraduate Research Opportunities Program (UROP) at Boston University; NASA's Exobiology and Astrobiology programs FX We are grateful to Jing-Jun Liu for his help with the photochemical analysis. H. C. thanks the Undergraduate Research Opportunities Program (UROP) at Boston University for primarily funding the research while in residence at Penn State University in State College in the summer of 2015. J.F.K. acknowledge financial support from NASA's Exobiology and Astrobiology programs. Data can be obtained from R.C. Payne (rvp5143@psu.edu). NR 18 TC 0 Z9 0 U1 5 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 SEP PY 2016 VL 121 IS 17 BP 10089 EP 10096 DI 10.1002/2016JD025459 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DY0YV UT WOS:000384823000022 ER PT J AU Dong, XQ Xi, BK Qiu, SY Minnis, P Sun-Mack, S Rose, F AF Dong, Xiquan Xi, Baike Qiu, Shaoyue Minnis, Patrick Sun-Mack, Sunny Rose, Fred TI A radiation closure study of Arctic stratus cloud microphysical properties using the collocated satellite-surface data and Fu-Liou radiative transfer model SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Arctic stratus cloud properties; radiation closure study; surface remote sensing; satellite remote sensing ID ANGULAR-DISTRIBUTION MODELS; GROUND-BASED MEASUREMENTS; ENERGY SYSTEM INSTRUMENT; STRATIFORM CLOUDS; FLUX CALCULATION; TERRA SATELLITE; PART I; CERES; BUDGET; RADAR AB Retrievals of cloud microphysical properties based on passive satellite imagery are especially difficult over snow-covered surfaces because of the bright and cold surface. To help quantify their uncertainties, single-layered overcast liquid-phase Arctic stratus cloud microphysical properties retrieved by using the Clouds and the Earth's Radiant Energy System Edition 2 and Edition 4 (CERES Ed2 and Ed4) algorithms are compared with ground-based retrievals at the Atmospheric Radiation Measurement North Slope of Alaska (ARM NSA) site at Barrow, AK, during the period from March 2000 to December 2006. A total of 206 and 140 snow-free cases (R(sfc)0.3), and 108 and 106 snow cases (R-sfc>0.3), respectively, were selected from Terra and Aqua satellite passes over the ARM NSA site. The CERES Ed4 and Ed2 optical depth () and liquid water path (LWP) retrievals from both Terra and Aqua are almost identical and have excellent agreement with ARM retrievals under snow-free and snow conditions. In order to reach a radiation closure study for both the surface and top of atmosphere (TOA) radiation budgets, the ARM precision spectral pyranometer-measured surface albedos were adjusted (63.6% and 80% of the ARM surface albedos for snow-free and snow cases, respectively) to account for the water and land components of the domain of 30kmx30km. Most of the radiative transfer model calculated SWsfc and SWTOA fluxes by using ARM and CERES cloud retrievals and the domain mean albedos as input agree with the ARM and CERES flux observations within 10Wm(-2) for both snow-free and snow conditions. Sensitivity studies show that the ARM LWP and r(e) retrievals are less dependent on solar zenith angle (SZA), but all retrieved optical depths increase with SZA. C1 [Dong, Xiquan; Xi, Baike; Qiu, Shaoyue] Univ North Dakota, Dept Atmospher Sci, Grand Forks, ND 58202 USA. [Minnis, Patrick] NASA Langley Res Ctr, Hampton, VA USA. [Sun-Mack, Sunny; Rose, Fred] SSAI Inc, Hampton, VA USA. RP Dong, XQ (reprint author), Univ North Dakota, Dept Atmospher Sci, Grand Forks, ND 58202 USA. EM dong@aero.und.edu FU U.S. Department of Energy (DOE) Office of Energy Research, Office of Health and Environmental Research, Environmental Sciences Division; NASA CERES project at the University of North Dakota [NNX14AP84G]; DOE ARM Program at NASA Langley [DE-SC0013896] FX The ground-based measurements were obtained from the Atmospheric Radiation Measurement (ARM) Program sponsored by the U.S. Department of Energy (DOE) Office of Energy Research, Office of Health and Environmental Research, Environmental Sciences Division. The data can be downloaded from http://www.archive.arm.gov/. The satellite data were obtained from the NASA CERES cloud working group at NASA Langley Research Center. Special thanks to Seiji Kato for the useful discussion about NASA Langley Modified Fu-Liou radiative transfer model. This research was supported by the NASA CERES project under grant NNX14AP84G at the University of North Dakota and by the DOE ARM Program under contract DE-SC0013896 at NASA Langley. Dates and times corresponding to the sample numbers used in several figures are available from the lead author on request (dong@aero.und.edu). NR 46 TC 1 Z9 1 U1 6 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP PY 2016 VL 121 IS 17 BP 10175 EP 10198 DI 10.1002/2016JD025255 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DY0YV UT WOS:000384823000018 ER PT J AU Saide, PE Thompson, G Eidhammer, T da Silva, AM Pierce, RB Carmichael, GR AF Saide, Pablo E. Thompson, Gregory Eidhammer, Trude da Silva, Arlindo M. Pierce, R. Bradley Carmichael, Gregory R. TI Assessment of biomass burning smoke influence on environmental conditions for multiyear tornado outbreaks by combining aerosol-aware microphysics and fire emission constraints SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE biomass burning; severe weather; tornadoes; fires; aerosol-cloud-radiation interactions; WRF ID MARINE STRATOCUMULUS; SPATIAL-DISTRIBUTION; WEATHER FORECASTS; OPTICAL DEPTH; WRF-CHEM; MODEL; IMPACTS; CLIMATE; PARAMETERIZATION; ASSIMILATION AB We use the Weather Research and Forecasting (WRF) system to study the impacts of biomass burning smoke from Central America on several tornado outbreaks occurring in the U.S. during spring. The model is configured with an aerosol-aware microphysics parameterization capable of resolving aerosol-cloud-radiation interactions in a cost-efficient way for numerical weather prediction (NWP) applications. Primary aerosol emissions are included, and smoke emissions are constrained using an inverse modeling technique and satellite-based aerosol optical depth observations. Simulations turning on and off fire emissions reveal smoke presence in all tornado outbreaks being studied and show an increase in aerosol number concentrations due to smoke. However, the likelihood of occurrence and intensification of tornadoes is higher due to smoke only in cases where cloud droplet number concentration in low-level clouds increases considerably in a way that modifies the environmental conditions where the tornadoes are formed (shallower cloud bases and higher low-level wind shear). Smoke absorption and vertical extent also play a role, with smoke absorption at cloud-level tending to burn-off clouds and smoke absorption above clouds resulting in an increased capping inversion. Comparing these and WRF-Chem simulations configured with a more complex representation of aerosol size and composition and different optical properties, microphysics, and activation schemes, we find similarities in terms of the simulated aerosol optical depths and aerosol impacts on near-storm environments. This provides reliability on the aerosol-aware microphysics scheme as a less computationally expensive alternative to WRF-Chem for its use in applications such as NWP and cloud-resolving simulations. C1 [Saide, Pablo E.] Natl Ctr Atmospher Res, Adv Study Program, POB 3000, Boulder, CO 80307 USA. [Saide, Pablo E.] Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA. [Thompson, Gregory; Eidhammer, Trude] Natl Ctr Atmospher Res, Res Applicat Lab, POB 3000, Boulder, CO 80307 USA. [da Silva, Arlindo M.] NASA, Goddard Space Flight Ctr, Global Modeling & Data Assimilat Off, Greenbelt, MD USA. [Pierce, R. Bradley] NOAA, Satellite & Informat Serv NESDIS, Ctr Satellite Applicat & Res STAR, Madison, WI USA. [Carmichael, Gregory R.] Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA USA. RP Saide, PE (reprint author), Natl Ctr Atmospher Res, Adv Study Program, POB 3000, Boulder, CO 80307 USA.; Saide, PE (reprint author), Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA. EM saide@ucar.edu RI Pierce, Robert Bradley/F-5609-2010 OI Pierce, Robert Bradley/0000-0002-2767-1643 FU National Science Foundation FX The National Center for Atmospheric Research is supported by the National Science Foundation. Contact P.E. Saide (saide@ucar.edu) for data and code requests. This work was carried out with the aid of NASA grant NNXAF95G. A.M. da Silva is funded by NASA's Modeling and Application Program. We acknowledge use of MOZART-4 global model output available at http://www.acom.ucar.edu/wrf-chem/mozart.shtml. CALIPSO data were obtained from the NASA Langley Research Center Atmospheric Science Data Center (https://earthdata.nasa.gov/). The views, opinions, and findings contained in this report are those of the author(s) and should not be construed as an official National Oceanic and Atmospheric Administration or U.S. Government position, policy, or decision. NR 60 TC 0 Z9 0 U1 15 U2 15 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 SEP PY 2016 VL 121 IS 17 BP 10294 EP 10311 DI 10.1002/2016JD025056 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DY0YV UT WOS:000384823000014 ER PT J AU Sullivan, JT Mcgee, TJ Langford, AO Alvarez, RJ Senff, CJ Reddy, PJ Thompson, AM Twigg, LW Sumnicht, GK Lee, P Weinheimer, A Knote, C Long, RW Hoff, RM AF Sullivan, John T. McGee, Thomas J. Langford, Andrew O. Alvarez, Raul J., II Senff, Christoph J. Reddy, Patrick J. Thompson, Anne M. Twigg, Laurence W. Sumnicht, Grant K. Lee, Pius Weinheimer, Andrew Knote, Christoph Long, Russell W. Hoff, Raymond M. TI Quantifying the contribution of thermally driven recirculation to a high-ozone event along the Colorado Front Range using lidar SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE ozone; air quality; remote sensing; lidar; air quality modeling; TOLNet ID REGIONAL-SCALE FLOWS; MOUNTAINOUS TERRAIN; BOUNDARY-LAYER AB A high-ozone (O-3) pollution episode was observed on 22 July 2014 during the concurrent Deriving Information on Surface Conditions from Column and Vertically Resolved Observations Relevant to Air Quality (DISCOVER-AQ) and Front Range Air Pollution and Photochemistry Experiment (FRAPPE) campaigns in northern Colorado. Surface O-3 monitors at three regulatory sites exceeded the Environmental Protection Agency (EPA) 2008 National Ambient Air Quality Standard (NAAQS) daily maximum 8h average (MDA8) of 75ppbv. To further characterize the polluted air mass and assess transport throughout the event, measurements are presented from O-3 and wind profilers, O-3-sondes, aircraft, and surface-monitoring sites. Observations indicate that thermally driven upslope flow was established throughout the Colorado Front Range during the pollution episode. As the thermally driven flow persisted throughout the day, O-3 concentrations increased and affected high-elevation Rocky Mountain sites. These observations, coupled with modeling analyses, demonstrate a westerly return flow of polluted air aloft, indicating that the mountain-plains solenoid circulation was established and impacted surface conditions within the Front Range. C1 [Sullivan, John T.; McGee, Thomas J.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA. [Langford, Andrew O.; Alvarez, Raul J., II; Senff, Christoph J.] NOAA, Earth Syst Res Lab, Boulder, CO USA. [Senff, Christoph J.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Reddy, Patrick J.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. [Thompson, Anne M.] NASA, Goddard Space Flight Ctr, Earth Sci Div, Greenbelt, MD USA. [Twigg, Laurence W.; Sumnicht, Grant K.] Sci Syst & Applicat Inc, Lanham, MD USA. [Lee, Pius] NOAA, Ctr Weather & Climate Predict, Air Resources Lab, College Pk, MD USA. [Weinheimer, Andrew] Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA. [Knote, Christoph] Univ Munich, Meteorol Inst, Munich, Germany. [Long, Russell W.] US EPA, Off Res & Dev, Res Triangle Pk, NC 27711 USA. [Hoff, Raymond M.] Joint Ctr Earth Syst Technol, Baltimore, MD USA. [Hoff, Raymond M.] Univ Maryland, Dept Atmospher Phys, Baltimore, MD 21201 USA. RP Sullivan, JT (reprint author), NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA. EM john.t.sullivan@nasa.gov RI Langford, Andrew/D-2323-2009; Thompson, Anne /C-3649-2014; Manager, CSD Publications/B-2789-2015 OI Langford, Andrew/0000-0002-2932-7061; Thompson, Anne /0000-0002-7829-0920; FU UMBC/JCET [374, 8306]; Maryland Department of the Environment (MDE) [U00P4400079]; NOAA-CREST CCNY Foundation [49173B-02]; NASA/USRA Postdoctoral Program at the Goddard Space Flight Center; NASA DISCOVER-AQ [NNX10AR39G]; Pennsylvania State University; NASA Tropospheric Chemistry Program; Tropospheric Ozone Lidar Network (TOLNet) FX Unless otherwise noted, all data used in this study can be found in the DISCOVER-AQ data archive (http://www-air.larc.nasa.gov/missions/discover-aq/), the FRAPPE data archive (http://catalog.eol.ucar.edu/frappe), or the TOLNet data archive (http://www-air.larc.nasa.gov/missions/TOLNet/). This work was supported by UMBC/JCET (task 374, project 8306), the Maryland Department of the Environment (MDE, contract U00P4400079), and NOAA-CREST CCNY Foundation (subcontract 49173B-02). This research was supported by an appointment to the NASA/USRA Postdoctoral Program at the Goddard Space Flight Center. The Platteville Nittany Atmospheric Trailer and Integrated Validation Experiment (NATIVE) operations were sponsored by NASA DISCOVER-AQ grant NNX10AR39G and the Pennsylvania State University. The authors gratefully acknowledge support provided by the NASA Tropospheric Chemistry Program and the Tropospheric Ozone Lidar Network (TOLNet). Thanks to the helpfulness and expertise of Ryan Stauffer, Hannah Halliday, and Nikolai Balashov, who worked with the NATIVE trailer at Platteville. Thanks to Debra Wicks Kollonige for providing her insight and recommendations on this work. Thanks to Kenneth Pickering, Yonhua Tang, Li Pan, and Barry Baker for their expertise in evaluating and managing the CMAQ model output. Thanks to Timothy Coleman (NOAA ESRL PSD) for providing the Greeley wind profiles. Thanks to the NOAA Physical Science Division for their continued efforts in managing the instrumentation and site coordination necessary for this work from the 300 m BAO Tower. Finally, thanks to the CDPHE for the continued efforts to obtain observations at the many remote and urban sites throughout the region used in this work. The views, opinions, and findings contained in this report are those of the author(s) and should not be construed as an official National Oceanic and Atmospheric Administration or U.S. Government position, policy, or decision. NR 34 TC 0 Z9 0 U1 8 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 SEP PY 2016 VL 121 IS 17 BP 10377 EP 10390 DI 10.1002/2016JD025229 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DY0YV UT WOS:000384823000008 ER PT J AU Bokhorst, S Pedersen, SH Brucker, L Anisimov, O Bjerke, JW Brown, RD Ehrich, D Essery, RLH Heilig, A Ingvander, S Johansson, C Johansson, M Jonsdottir, IS Inga, N Luojus, K Macelloni, G Mariash, H McLennan, D Rosqvist, GN Sato, A Savela, H Schneebeli, M Sokolov, A Sokratov, SA Terzago, S Vikhamar-Schuler, D Williamson, S Qiu, YB Callaghan, TV AF Bokhorst, Stef Pedersen, Stine Hojlund Brucker, Ludovic Anisimov, Oleg Bjerke, Jarle W. Brown, Ross D. Ehrich, Dorothee Essery, Richard L. H. Heilig, Achim Ingvander, Susanne Johansson, Cecilia Johansson, Margareta Jonsdottir, Ingibjorg Svala Inga, Niila Luojus, Kari Macelloni, Giovanni Mariash, Heather McLennan, Donald Rosqvist, Gunhild Ninis Sato, Atsushi Savela, Hannele Schneebeli, Martin Sokolov, Aleksandr Sokratov, Sergey A. Terzago, Silvia Vikhamar-Schuler, Dagrun Williamson, Scott Qiu, Yubao Callaghan, Terry V. TI Changing Arctic snow cover: A review of recent developments and assessment of future needs for observations, modelling, and impacts SO AMBIO LA English DT Review DE Climate change; Ecosystem services; Human health; Societal costs; Indigenous; Snow ID WINTER WARMING EVENTS; MICROWAVE BRIGHTNESS TEMPERATURE; LIGHT-ABSORBING PARTICLES; GROUND-PENETRATING RADAR; LIQUID WATER-CONTENT; SEA-ICE; SURFACE-AREA; ALBEDO FEEDBACK; CLIMATE MODELS; INFRARED REFLECTANCE AB Snow is a critically important and rapidly changing feature of the Arctic. However, snow-cover and snowpack conditions change through time pose challenges for measuring and prediction of snow. Plausible scenarios of how Arctic snow cover will respond to changing Arctic climate are important for impact assessments and adaptation strategies. Although much progress has been made in understanding and predicting snow-cover changes and their multiple consequences, many uncertainties remain. In this paper, we review advances in snow monitoring and modelling, and the impact of snow changes on ecosystems and society in Arctic regions. Interdisciplinary activities are required to resolve the current limitations on measuring and modelling snow characteristics through the cold season and at different spatial scales to assure human well-being, economic stability, and improve the ability to predict manage and adapt to natural hazards in the Arctic region. C1 [Bokhorst, Stef; Bjerke, Jarle W.] Norwegian Inst Nat Res NINA, FRAM High North Res Ctr Climate & Environm, POB 6606, N-9296 Tromso, Norway. [Bokhorst, Stef] Vrije Univ Amsterdam, Dept Ecol Sci, De Boelelaan 1085, NL-1081 HV Amsterdam, Netherlands. [Pedersen, Stine Hojlund] Aarhus Univ, Dept Biosci, Arctic Res Ctr, Frederiksborgvej 399, DK-4000 Roskilde, Denmark. [Brucker, Ludovic] NASA, GSFC, Cryospher Sci Lab, Code 615, Greenbelt, MD 20771 USA. [Brucker, Ludovic] Univ Space Res Assoc, Goddard Earth Sci Technol & Res Studies & Invest, Columbia, MD 21044 USA. [Anisimov, Oleg] State Hydrol Inst Roshydromet, 23 Second Line VO, St Petersburg 199053, Russia. [Anisimov, Oleg] North East Fed Univ, Int Ctr Sci & Educ Best, Yakutsk, Russia. [Brown, Ross D.] Environm Canada Ouranos, Div Climate Res, 550 Sherbrooke St West,19th Floor, Montreal, PQ H3A 1B9, Canada. [Ehrich, Dorothee] Univ Tromso, Dept Arctic & Marine Biol, N-9037 Tromso, Norway. [Essery, Richard L. H.] Univ Edinburgh, Sch GeoSci, Edinburgh, Midlothian, Scotland. [Heilig, Achim] Heidelberg Univ, Inst Environm Phys, Neuenheimer Feld 229, D-69120 Heidelberg, Germany. [Ingvander, Susanne; Rosqvist, Gunhild Ninis] Stockholm Univ, Dept Phys Geog, S-10691 Stockholm, Sweden. [Johansson, Cecilia] Uppsala Univ, Dept Earth Sci, Villavagen 16, S-75236 Uppsala, Sweden. [Johansson, Margareta; Callaghan, Terry V.] Lund Univ, Dept Phys Geog & Ecosyst Sci, Solvegatan 12, S-22362 Lund, Sweden. [Johansson, Margareta] Royal Swedish Acad Sci, POB 50005, S-10405 Stockholm, Sweden. [Jonsdottir, Ingibjorg Svala] Univ Ctr Svalbard, POB 156, N-9171 Longyearbyen, Norway. [Jonsdottir, Ingibjorg Svala] Univ Iceland, Fac Life & Environm Sci, Sturlugata 7, IS-101 Reykjavik, Iceland. [Inga, Niila] Leavas Sami Commun, Box 53, S-98121 Kiruna, Sweden. [Luojus, Kari] Finnish Meteorol Inst, Arctic Res, POB 503, Helsinki 00101, Finland. [Macelloni, Giovanni] CNR, IFAC CNR, Inst Appl Phys Nello Carrara, Via Madonna del Piano 10, I-50019 Sesto Fiorentino, FI, Italy. [Mariash, Heather] Environm Canada, Natl Wildlife Res Ctr, 1125 Colonel By Dr, Ottawa, ON K1A 0H3, Canada. [McLennan, Donald] CHARS, 360 Albert St,Suite 1710, Ottawa, ON K1R 7X7, Canada. [Rosqvist, Gunhild Ninis] Univ Bergen, Dept Earth Sci, N-5020 Bergen, Norway. [Sato, Atsushi] Natl Res Inst Earth Sci & Disaster Prevent, Snow & Ice Res Ctr, 187-16 Suyoshi, Nagaoka, Niigata 9400821, Japan. [Savela, Hannele] Univ Oulu, Thule Insitute, POB 7300, Oulu 90014, Finland. [Schneebeli, Martin] WSL Inst Snow & Avalanche Res SLF, Fluelastr 11, CH-7260 Davos, Switzerland. [Sokolov, Aleksandr] Russian Acad Sci, Arctic Res Stn, Inst Plant & Anim Ecol, Ural Branch, Labytnangi 629400, Russia. [Sokolov, Aleksandr] State Org Yamal Nenets Autonomous Dist, Sci Ctr Arctic Studies, Salekhard, Russia. [Sokratov, Sergey A.] Moscow MV Lomonosov State Univ, Arctic Environm Lab, Fac Geog, Leninskie Gory 1, Moscow 119991, Russia. [Terzago, Silvia] Natl Res Council ISAC CNR, Inst Atmospher Sci & Climate, Corso Fiume 4, I-10133 Turin, Italy. [Vikhamar-Schuler, Dagrun] Norwegian Meteorol Inst, Div Model & Climate Anal, R&D Dept, Postboks 43, N-0313 Oslo, Norway. [Williamson, Scott] Univ Alberta, Dept Biol Sci, CW 405,Biol Sci Bldg, Edmonton, AB T6G 2E9, Canada. [Qiu, Yubao] Chinese Acad Sci, Inst Remote Sensing & Digital Earth, Beijing 100094, Peoples R China. [Qiu, Yubao] Cold Reg Initiat, Grp Earth Observat, Geneva, Switzerland. [Callaghan, Terry V.] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England. [Callaghan, Terry V.] Natl Res Tomsk Stated Univ, 36 Lenin Ave, Tomsk 634050, Russia. RP Bokhorst, S (reprint author), Norwegian Inst Nat Res NINA, FRAM High North Res Ctr Climate & Environm, POB 6606, N-9296 Tromso, Norway. EM stefbokhorst@hotmail.com; shp@bios.au.dk; ludovic.brucker@nasa.gov; oleg@oa7661.spb.edu; jarle.werner.bjerke@nina.no; ross.brown@ec.gc.ca; dorothee.ehrich@uit.no; richard.essery@ed.ac.uk; achim.heilig@wsl.ch; susanne.ingvander@natgeo.su.se; cecilia.johansson@met.uu.se; margareta.johansson@nateko.lu.se; isj@hi.is; niila@laevas.se; kari.luojus@fmi.fi; g.macelloni@ifac.cnr.it; heather.mariash@gmail.com; donald.mclennan@polar.gc.ca; gunhild.rosqvist@natgeo.su.se; asato@bosai.go.jp; hannele.savela@oulu.fi; martin.schneebeli@wsl.ch; sokhol@yandex.ru; sokratov@geol.msu.ru; s.terzago@isac.cnr.it; dagrun@met.no; snw@ualberta.ca; terry_callaghan@btinternet.com RI Sokratov, Sergey/A-6602-2011; Ehrich, Dorothee/F-6492-2015; Schneebeli, Martin/B-1063-2008; Brucker, Ludovic/A-8029-2010; Callaghan, Terens/N-7640-2014; OI Sokratov, Sergey/0000-0001-9265-2935; Ehrich, Dorothee/0000-0002-3028-9488; Schneebeli, Martin/0000-0003-2872-4409; Brucker, Ludovic/0000-0001-7102-8084; Essery, Richard/0000-0003-1756-9095; Bjerke, Jarle/0000-0003-2721-1492 FU IASC ICARP III Activity grant FX The writing of this paper was initiated by an IASC ICARP III Activity grant to TVC enabling a workshop hosted by the European Environment Agency. The authors acknowledge funding from their respective national and international funding bodies, which has enabled the contribution of all authors to this work. NR 167 TC 5 Z9 5 U1 37 U2 37 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0044-7447 EI 1654-7209 J9 AMBIO JI Ambio PD SEP PY 2016 VL 45 IS 5 BP 516 EP 537 DI 10.1007/s13280-016-0770-0 PG 22 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA DT6GD UT WOS:000381580800002 PM 26984258 ER PT J AU McIntire, J Moyer, D Brown, SW Lykke, KR Waluschka, E Oudrari, H Xiong, XX AF McIntire, Jeff Moyer, David Brown, Steven W. Lykke, Keith R. Waluschka, Eugene Oudrari, Hassan Xiong, Xiaoxiong TI Monochromatic measurements of the JPSS-1 VIIRS polarization sensitivity SO APPLIED OPTICS LA English DT Article ID PERFORMANCE; CALIBRATION; SATELLITE; MODIS AB Polarization sensitivity is a critical property that must be characterized for spaceborne remote sensing instruments designed to measure reflected solar radiation. Broadband testing of the first Joint Polar-orbiting Satellite System (JPSS-1) Visible Infrared Imaging Radiometer Suite (VIIRS) showed unexpectedly large polarization sensitivities for the bluest bands on VIIRS (centered between 400 and 600 nm). Subsequent ray trace modeling indicated that large diattenuation on the edges of the bandpass for these spectral bands was the driver behind these large sensitivities. Additional testing using the National Institute of Standards and Technology's Traveling Spectral Irradiance and Radiance Responsivity Calibrations Using Uniform Sources was added to the test program to verify and enhance the model. The testing was limited in scope to two spectral bands at two scan angles; nonetheless, this additional testing provided valuable insight into the polarization sensitivity. Analysis has shown that the derived diattenuation agreed with the broadband measurements to within an absolute difference of about 0.4% and that the ray trace model reproduced the general features of the measured data. Additionally, by deriving the spectral responsivity, the linear diattenuation is shown to be explicitly dependent on the changes in bandwidth with polarization state. (C) 2016 Optical Society of America C1 [McIntire, Jeff; Oudrari, Hassan] Sci Syst Applicat Int, Lanham, MD 20706 USA. [Moyer, David] Aerosp Corp, El Segundo, CA 90245 USA. [Brown, Steven W.; Lykke, Keith R.] NIST, Gaithersburg, MD 20899 USA. [Waluschka, Eugene; Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP McIntire, J (reprint author), Sci Syst Applicat Int, Lanham, MD 20706 USA. EM jeffrey.mcintire@ssaihq.com NR 16 TC 0 Z9 0 U1 5 U2 5 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 SEP PY 2016 VL 55 IS 27 BP 7444 EP 7454 DI 10.1364/AO.55.007444 PG 11 WC Optics SC Optics GA DW9QO UT WOS:000383996900001 PM 27661568 ER PT J AU Sun, JQ Xiong, XX Waluschka, E Wang, MH AF Sun, Junqiang Xiong, Xiaoxiong Waluschka, Eugene Wang, Menghua TI Suomi National Polar-Orbiting Partnership Visible Infrared Imaging Radiometer Suite polarization sensitivity analysis SO APPLIED OPTICS LA English DT Article ID REFLECTIVE SOLAR BANDS; CALIBRATION; SPECTRORADIOMETER; PERFORMANCE; DIFFUSER AB The Visible Infrared Imaging Radiometer Suite (VIIRS) is one of five instruments onboard the Suomi National Polar-Orbiting Partnership (SNPP) satellite that launched from Vandenberg Air Force Base, California, on October 28, 2011. It is a whiskbroom radiometer that provides +/- 56.28 degrees scans of the Earth view. It has 22 bands, among which 14 are reflective solar bands (RSBs). The RSBs cover a wavelength range from 410 to 2250 nm. The RSBs of a remote sensor are usually sensitive to the polarization of incident light. For VIIRS, it is specified that the polarization factor should be smaller than 3% for 410 and 862 nm bands and 2.5% for other RSBs for the scan angle within +/- 45 degrees. Several polarization sensitivity tests were performed prelaunch for SNPP VIIRS. The first few tests either had large uncertainty or were less reliable, while the last one was believed to provide the more accurate information about the polarization property of the instrument. In this paper, the measured data in the last polarization sensitivity test are analyzed, and the polarization factors and phase angles are derived from the measurements for all the RSBs. The derived polarization factors and phase angles are band, detector, and scan angle dependent. For near-infrared bands, they also depend on the half-angle mirror side. Nevertheless, the derived polarization factors are all within the specification, although the strong detector dependence of the polarization parameters was not expected. Compared to the Moderate Resolution Imaging Spectroradiometer on both Aqua and Terra satellites, the polarization effect on VIIRS RSB is much smaller. (C) 2016 Optical Society of America C1 [Sun, Junqiang; Wang, Menghua] NOAA, Natl Environm Satellite Data & Informat Serv, Ctr Satellite Applicat & Res, E RA3,5830 Univ Res Ct, College Pk, MD 20740 USA. [Sun, Junqiang] Global Sci & Technol, 7855 Walker Dr,Suite 200, Greenbelt, MD 20770 USA. [Xiong, Xiaoxiong; Waluschka, Eugene] NASA, Sci & Explorat Directorate, GSFC, Greenbelt, MD 20771 USA. RP Sun, JQ (reprint author), NOAA, Natl Environm Satellite Data & Informat Serv, Ctr Satellite Applicat & Res, E RA3,5830 Univ Res Ct, College Pk, MD 20740 USA.; Sun, JQ (reprint author), Global Sci & Technol, 7855 Walker Dr,Suite 200, Greenbelt, MD 20770 USA. EM junqiang.sun@noaa.gov RI Wang, Menghua/F-5631-2010 OI Wang, Menghua/0000-0001-7019-3125 FU National Oceanic and Atmospheric Administration (NOAA) National Aeronautics and Space Administration (NASA) Joint Polar Satellite System FX National Oceanic and Atmospheric Administration (NOAA) National Aeronautics and Space Administration (NASA) Joint Polar Satellite System. NR 31 TC 0 Z9 0 U1 5 U2 5 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 SEP PY 2016 VL 55 IS 27 BP 7645 EP 7658 DI 10.1364/AO.55.007645 PG 14 WC Optics SC Optics GA DW9QO UT WOS:000383996900027 PM 27661594 ER PT J AU Guerrero, G Smolarkiewicz, PK Dal Pino, EMD Kosovichev, AG Mansour, NN AF Guerrero, G. Smolarkiewicz, P. K. de Gouveia Dal Pino, E. M. Kosovichev, A. G. Mansour, N. N. TI UNDERSTANDING SOLAR TORSIONAL OSCILLATIONS FROM GLOBAL DYNAMO MODELS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: interior; Sun: magnetic fields; Sun: rotation ID CONVECTION-ZONE; MERIDIONAL FLOW; CYCLE VARIATION; ROTATION; INTERIOR; SURFACE; SUN AB The phenomenon of solar "torsional oscillations" (TO) represents migratory zonal flows associated with the solar cycle. These flows are observed on the solar surface and, according to helioseismology, extend through the convection zone. We study the origin of the TO using results from a global MHD simulation of the solar interior that reproduces several of the observed characteristics of the mean-flows and magnetic fields. Our results indicate that the magnetic tension (MT) in the tachocline region is a key factor for the periodic changes in the angular momentum transport that causes the TO. The torque induced by the MT at the base of the convection zone is positive at the poles and negative at the equator. A rising MT torque at higher latitudes causes the poles to speed up, whereas a declining negative MT torque at the lower latitudes causes the equator to slow-down. These changes in the zonal flows propagate through the convection zone up to the surface. Additionally, our results suggest that it is the magnetic field at the tachocline that modulates the amplitude of the surface meridional flow rather than the opposite as assumed by flux-transport dynamo models of the solar cycle. C1 [Guerrero, G.] Univ Fed Minas Gerais, Dept Phys, Av Antonio Carlos 6627, BR-31270901 Belo Horizonte, MG, Brazil. [Smolarkiewicz, P. K.] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England. [de Gouveia Dal Pino, E. M.] Univ Sao Paulo, Dept Astron, IAG USP, Rua Matao 1226, BR-05508090 Sao Paulo, SP, Brazil. [Kosovichev, A. G.] New Jersey Inst Technol, Newark, NJ 07103 USA. [Mansour, N. N.] NASA, Ames Res Ctr, Mountain View, CA 94040 USA. RP Guerrero, G (reprint author), Univ Fed Minas Gerais, Dept Phys, Av Antonio Carlos 6627, BR-31270901 Belo Horizonte, MG, Brazil. EM guerrero@fisica.ufmg.br; smolar@ecmwf.int; dalpino@astro.iag.usp.br; alexander.g.kosovichev@njit.edu; Nagi.N.Mansour@nasa.gov FU FAPEMIG [APQ-01168/14]; FAPESP [2013/10559-5, 2009/54006-4]; CNPq [306598/2009-4]; NASA [NNX09AJ85g, NNX14AB70G]; European Research Council under the European Union's Seventh Framework Programme (FP7/ERC) [320375] FX We thank the anonymous referee for insightful comments that helped to improve the paper. This work was partly funded by FAPEMIG grant APQ-01168/14 (GG), FAPESP grant 2013/10559-5 (EMGDP), CNPq grant 306598/2009-4 (EMGDP), and NASA grants NNX09AJ85g and NNX14AB70G. P.K.S. is supported by funding received from the European Research Council under the European Union's Seventh Framework Programme (FP7/2012/ERC grant agreement no. 320375). The simulations were performed in the NASA cluster Pleiades and the computing facilities of the Laboratory of Astroinformatics (IAG/USP, NAT/Unicsul) supported by a FAPESP (grant 2009/54006-4). NR 25 TC 0 Z9 0 U1 4 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 1 PY 2016 VL 828 IS 1 AR L3 DI 10.3847/2041-8205/828/1/L3 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW9MZ UT WOS:000383985500003 ER PT J AU Sterling, AC Moore, RL AF Sterling, Alphonse C. Moore, Ronald L. TI A MICROFILAMENT-ERUPTION MECHANISM FOR SOLAR SPICULES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: chromosphere; Sun: filaments, prominences; Sun: flares; Sun: magnetic fields; Supporting material: animations ID X-RAY JETS; POLAR CORONAL HOLES; ACTIVE-REGION; II SPICULES; TELESCOPE; EVOLUTION; HINODE; PARAMETERS; RESOLUTION; NETWORK AB Recent investigations indicate that solar coronal jets result from eruptions of small-scale chromospheric filaments, called minifilaments; that is, the jets are produced by scaled-down versions of typical-sized filament eruptions. We consider whether solar spicules might in turn be scaled-down versions of coronal jets, being driven by eruptions of microfilaments. Assuming a microfilament' s size is about a spicule' s width (similar to 300 km), the estimated occurrence number plotted against the estimated size of erupting filaments, minifilaments, and microfilaments approximately follows a power-law distribution (based on counts of coronal mass ejections, coronal jets, and spicules), suggesting that many or most spicules could result from microfilament eruptions. Observed spicule-base Ca II brightenings plausibly result from such microfilament eruptions. By analogy with coronal jets, microfilament eruptions might produce spicules with many of their observed characteristics, including smooth rise profiles, twisting motions, and EUV counterparts. The postulated microfilament eruptions are presumably eruptions of twisted-core micro-magnetic bipoles that are similar to 1 ''.0 wide. These explosive bipoles might be built and destabilized by merging and cancelation of approximately a few to 100 G magnetic-flux elements of size less than or similar to 0 ''.5-1 ''.0. If, however, spicules are relatively more numerous than indicated by our extrapolated distribution, then only a fraction of spicules might result from this proposed mechanism. C1 [Sterling, Alphonse C.; Moore, Ronald L.] Marshall Space Flight Ctr, Heliophys & Planetary Sci Off, ZP13, Huntsville, AL 35812 USA. [Moore, Ronald L.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. RP Sterling, AC (reprint author), Marshall Space Flight Ctr, Heliophys & Planetary Sci Off, ZP13, Huntsville, AL 35812 USA. EM alphonse.sterling@nasa.gov; ron.moore@nasa.gov FU Heliophysics Division of NASA's Science Mission Directorate through the Heliophysics Guest Investigator (HGI) Program; Hinode Project FX The authors thank two referees for useful comments and interesting discussions. This work was supported by funding from the Heliophysics Division of NASA's Science Mission Directorate through the Heliophysics Guest Investigator (HGI) Program, and the Hinode Project. We thank T. Tarbell for assistance with SOT images. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners, and operated by these agencies in co-operation with ESA and NSC (Norway). Figure 1 and Figures 3(g)-(i) and animations, adapted by permission from Macmillan Publishers Ltd: Nature, Sterling et al. (2015), copyright 2015. NR 37 TC 0 Z9 0 U1 2 U2 2 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 SEP 1 PY 2016 VL 828 IS 1 AR L9 DI 10.3847/2041-8205/828/1/L9 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW9MZ UT WOS:000383985500009 ER PT J AU Wernet, MP AF Wernet, Mark P. TI Application of Tomo-PIV in a large-scale supersonic jet flow facility SO EXPERIMENTS IN FLUIDS LA English DT Article ID PARTICLE IMAGE VELOCIMETRY AB Particle imaging velocimetry (PIV) has been used extensively at NASA GRC over the last 15 years to build a benchmark data set of hot and cold jet flow measurements in an effort to understand acoustic noise sources in high-speed jets. Identifying the noise sources in highspeed jets is critical for ultimately modifying the nozzle hardware design/operation and therefore reducing the jet noise. Tomographic PIV (Tomo-PIV) is an innovative approach for acquiring and extracting velocity information across extended volumes of a flow field, enabling the computation of additional fluid mechanical properties not typically available using traditional PIV techniques. The objective of this work was to develop and implement the Tomo-PIV measurement capability and apply it in a large-scale outdoor test facility, where seeding multiple flow streams and operating in the presence of daylight presents formidable challenges. The newly developed Tomo-PIV measurement capability was applied in both a subsonic M 0.9 flow and an under-expanded M 1.4 heated jet flow field. Measurements were also obtained using traditional two-component (2C) PIV and stereo PIV in the M 0.9 flow field for comparison and validation of the Tomo-PIV results. In the case of the M 1.4 flow, only the 2C PIV was applied to allow a comparison with the Tomo-PIV measurement. The Tomo-PIV fields-of-view covered 180 x 180 x 10 mm, and the reconstruction domains were 3500 x 3500 x 200 voxels. These Tomo-PIV measurements yielded all three components of vorticity across entire planes for the first time in heated supersonic jet flows and provided the first full 3D reconstruction of the Mach disk and oblique shock intersections inside of the barrel shocks. Measuring all three components of vorticity across multiple planes in the flow, potentially reduces the number of measurement configurations (streamwise and cross-stream PIV) required to fully characterize the mixing-enhanced nozzle flows routinely studied in aeroacoustics research. C1 [Wernet, Mark P.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Wernet, MP (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM mark.p.wernet@nasa.gov FU NASA's Fundamental Aeronautics' Transformational Tools and Technologies Program FX The author would like to thank NASA's Fundamental Aeronautics' Transformational Tools and Technologies Program for their support of this effort. The author also thanks Dr. Randy Locke, Dr. Adam Wroblewski and Garrett Clayo for their efforts in the setting up and implementation of the 2C PIV, SPIV and Tomo-PIV systems. The author thanks Dr. James Bridges for helpful discussions and for the use of the SHJAR facility. Lastly, the author thanks the staff at the AAPL for their dedication and support in making these tests possible. NR 33 TC 0 Z9 0 U1 5 U2 5 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0723-4864 EI 1432-1114 J9 EXP FLUIDS JI Exp. Fluids PD SEP PY 2016 VL 57 IS 9 AR 144 DI 10.1007/s00348-016-2228-3 PG 24 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA DX2QM UT WOS:000384215700007 ER PT J AU Tang, A Kim, Y Xu, Y Chang, MCF AF Tang, Adrian Kim, Yanghyo Xu, Yinuo Chang, Mau-Chung Frank TI A 5.8 GHz 54 Mb/s Backscatter Modulator for WLAN With Symbol Pre-Distortion and Transmit Pulse Shaping SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS LA English DT Article DE CMOS backscatter link; pre-distortion; pulse shaping; reflector link AB This letter discusses the implementation of microwave backscatter links in CMOS technology which are similar to existing systems at mid-UHF for RFID, but intended for use at the 5.8 GHz ISM band for supporting future low-power WLAN applications. In order for backscatter links to operate in highly channelized environments we introduce a pulse-shaping technique to reduce out-of-band emissions as well as a symbol pre-distortion technique to improve the constellation spacing. Both techniques are introduced into a 65 nm prototype backscatter modulator chip and are shown to operate with QPSK modulation at 54 Mb/s (typical of WLAN standards). The backscatter modulator chip was shown to consume 1.61 mW of power. C1 [Tang, Adrian; Kim, Yanghyo; Xu, Yinuo; Chang, Mau-Chung Frank] Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90025 USA. [Tang, Adrian] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Tang, A (reprint author), Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90025 USA. EM atang@seas.ucla.edu; yanghyokim@ucla.edu; yinuo@ucla.edu; mfchang@ee.ucla.edu NR 4 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 1531-1309 EI 1558-1764 J9 IEEE MICROW WIREL CO JI IEEE Microw. Wirel. Compon. Lett. PD SEP PY 2016 VL 26 IS 9 BP 729 EP 731 DI 10.1109/LMWC.2016.2597173 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA DX0PV UT WOS:000384067100029 ER PT J AU Lall, P Mirza, KM Harsha, M Goebel, K AF Lall, Pradeep Mirza, Kazi Mahmud Harsha, Mahendra Goebel, Kai TI Microstructural Indicators for Assessment of Effect of Prolonged and Intermittent Storage on Reliability of Lead-free Electronics SO IEEE TRANSACTIONS ON DEVICE AND MATERIALS RELIABILITY LA English DT Article DE Materials reliability; integrated circuit reliability; soldering; integrated circuit interconnections ID BOUNDARY-SCAN; TESTABILITY; DESIGN; BIST; BIT AB Electronic systems may be subjected to prolonged and intermittent periods of storage prior to deployment or usage. Prior studies have shown that the lead-free solder interconnects show measurable degradation in the mechanical properties even after the brief exposures to high temperature. In this paper, a method has been developed for determining the equivalent storage time to produce identical damage at a different temperature. Electronics subjected to accelerated tests often have a well-defined thermal profile for a specified period of time. Quantification of the thermal profile in field-deployed electronics may be often difficult because of the variance in the environment conditions and usage profile. There is a need for tools and techniques to quantify the damage in deployed systems in the absence of macroindicators of damage without the knowledge of prior stress history. The approach for mapping damage in the lead-free second-level interconnects between different thermal conditions is new. High-reliability applications, such as avionics and missile systems, may be often exposed to long periods of storage prior to deployment. The effect of storage at different temperature conditions can be mapped using the presented approach. A framework has been developed to investigate the system state and estimate the remaining useful life of the solder ball subjected to a variety of isothermal aging conditions, including 60 degrees C, 75 degrees C, and 125 degrees C for periods of time between 1 and 4 weeks. Data on damage precursors, including the rate of change in the normalized phase growth and the normalized IMC thickness, has been collected and analyzed to derive physics-based damage mapping relationships for aging. Mathematical relationships have been derived for the damage mapping to various thermal storage environments to facilitate determining an appropriate time-temperature combination to reach a particular level of damage state. Activation energy for the leading indicators of failure is also computed. Specific damage proxies examined include the phase-growth indicator and the intermetallic thickness. The viability of the approach has been demonstrated for the lead-free test assemblies subjected to multiple thermal aging at 60 degrees C, 75 degrees C, and 125 degrees C. Damage mapping relationships are derived from the data based on the two separate leading indicators. C1 [Lall, Pradeep; Mirza, Kazi Mahmud; Harsha, Mahendra] Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA. [Harsha, Mahendra] Skyworks Solut Inc, Woburn, MA 01801 USA. [Goebel, Kai] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. RP Lall, P (reprint author), Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA. EM lall@auburn.edu; kmm0039@tigermail.auburn.edu; mahendra.harsha@skyworksinc.com; kai.f.goebel@nasa.gov OI Lall, Pradeep/0000-0002-4074-937X NR 27 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 1530-4388 EI 1558-2574 J9 IEEE T DEVICE MAT RE JI IEEE Trans. Device Mater. Reliab. PD SEP PY 2016 VL 16 IS 3 BP 304 EP 317 DI 10.1109/TDMR.2016.2597740 PG 14 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA DX0QP UT WOS:000384069500005 ER PT J AU Thipphavong, DP AF Thipphavong, David P. TI Top-of-Climb Matching Method for Reducing Aircraft Trajectory Prediction Errors SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA Guidance, Navigation, and Control (GNC) Conference / AIAA Infotech at Aerospace Conference CY AUG 19-22, 2013 CL Boston, MA SP AIAA AB The inaccuracies of the aircraft performance models used by trajectory predictors with regard to takeoff weight, thrust, climb profile, and other parameters result in altitude errors during the climb phase that often exceed the vertical separation standard of 1000 ft. This study investigates the potential reduction in altitude trajectory prediction errors that could be achieved for climbing flights if just one additional parameter is made available: top-of-climb time. The top-of-climb matching method developed and evaluated in this paper is straightforward: A set of candidate trajectory predictions is generated using different aircraft weight parameters, and the one that most closely matches top of climb in terms of time is selected. This algorithm was tested using more than 1000 climbing flights in Fort Worth Center. Compared with the baseline trajectory predictions of a real-time research prototype (Center/Terminal Radar Approach Control Automation System), the top-of-climb matching method reduced the altitude root mean square error for a 5min prediction time by 38%. It also decreased the percentage of flights with absolute altitude error greater than the vertical separation standard of 1000ft for the same look-ahead time from 55 to 30%. C1 [Thipphavong, David P.] NASA, Ames Res Ctr, Flight Trajectory Dynam & Controls Branch, Mail Stop 210-10, Moffett Field, CA 94035 USA. [Thipphavong, David P.] AIAA, Reston, VA 20191 USA. RP Thipphavong, DP (reprint author), NASA, Ames Res Ctr, Flight Trajectory Dynam & Controls Branch, Mail Stop 210-10, Moffett Field, CA 94035 USA.; Thipphavong, DP (reprint author), AIAA, Reston, VA 20191 USA. NR 10 TC 0 Z9 0 U1 1 U2 1 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD SEP-OCT PY 2016 VL 53 IS 5 BP 1211 EP 1223 DI 10.2514/1.C032966 PG 13 WC Engineering, Aerospace SC Engineering GA DX3TS UT WOS:000384297800003 ER PT J AU Brandon, JM Morelli, EA AF Brandon, Jay M. Morelli, Eugene A. TI Real-Time Onboard Global Nonlinear Aerodynamic Modeling from Flight Data SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA Atmospheric Flight Mechanics Conference CY JUN 16-20, 2014 CL Atlanta, GA SP AIAA ID IDENTIFICATION AB Flight test and modeling techniques were developed to accurately identify global nonlinear aerodynamic models onboard an aircraft. The techniques were developed and demonstrated during piloted flight testing of an Aermacchi MB-326M Impala jet aircraft. Advanced piloting techniques and nonlinear modeling techniques based on fuzzy logic and multivariate orthogonal function methods were implemented with efficient onboard calculations and flight operations to achieve real-time maneuver monitoring, near-real-time global nonlinear aerodynamic modeling, and prediction validation testing in flight. Results demonstrated that global nonlinear aerodynamic models for a large portion of the flight envelope were identified rapidly and accurately using piloted flight test maneuvers during a single flight, with the final identified and validated models available before the aircraft landed. C1 [Brandon, Jay M.] NASA, Langley Res Ctr, Flight Dynam Branch, Mail Stop 308, Hampton, VA 23681 USA. [Morelli, Eugene A.] NASA, Langley Res Ctr, Dynam Syst & Control Branch, Mail Stop 308, Hampton, VA 23681 USA. [Brandon, Jay M.; Morelli, Eugene A.] AIAA, Reston, VA 20191 USA. RP Brandon, JM (reprint author), NASA, Langley Res Ctr, Flight Dynam Branch, Mail Stop 308, Hampton, VA 23681 USA.; Brandon, JM (reprint author), AIAA, Reston, VA 20191 USA. NR 15 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD SEP-OCT PY 2016 VL 53 IS 5 BP 1261 EP 1297 DI 10.2514/1.C033133 PG 37 WC Engineering, Aerospace SC Engineering GA DX3TS UT WOS:000384297800007 ER PT J AU Su, WH Swei, SSM Zhu, GMG AF Su, Weihua Swei, Sean Shan-Min Zhu, Guoming G. TI Optimum Wing Shape of Highly Flexible Morphing Aircraft for Improved Flight Performance SO JOURNAL OF AIRCRAFT LA English DT Article ID NONLINEAR AEROELASTICITY; DESIGN OPTIMIZATION; BODY AIRCRAFT; DYNAMICS; AIRFOIL AB In this paper, optimum wing bending and torsion deformations are explored for a mission adaptive, highly flexible morphing aircraft. The complete highly flexible aircraft is modeled using a strain-based geometrically nonlinear beam formulation, coupled with unsteady aerodynamics and six-degree-of-freedom rigid-body motions. Since there are no conventional discrete control surfaces for trimming the flexible aircraft, the design space for searching the optimum wing geometries is enlarged. To achieve high-performance flight, the wing geometry is best tailored according to the specific flight mission needs. In this study, the steady level flight and the coordinated turn flight are considered, and the optimum wing deformations with the minimum drag at these flight conditions are searched by using a modal-based optimization procedure, subject to the trim and other constraints. The numerical study verifies the feasibility of the modal-based optimization approach, and it shows the resulting optimum wing configuration and its sensitivity under different flight profiles. C1 [Su, Weihua] Univ Alabama, Dept Aerosp Engn & Mech, Tuscaloosa, AL 35487 USA. [Swei, Sean Shan-Min] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA. [Zhu, Guoming G.] Michigan State Univ, Dept Mech Engn, E Lansing, MI 48824 USA. [Su, Weihua; Swei, Sean Shan-Min] AIAA, Reston, VA 20191 USA. RP Su, WH (reprint author), Univ Alabama, Dept Aerosp Engn & Mech, Tuscaloosa, AL 35487 USA.; Su, WH (reprint author), AIAA, Reston, VA 20191 USA. EM suw@eng.ua.edu; sean.s.swei@nasa.gov; zhug@egr.msu.edu RI Su, Weihua/F-1561-2011 OI Su, Weihua/0000-0002-4458-0524 FU NASA Ames Research Center's Summer Faculty Fellowship; NASA Aeronautics Research Mission Directorate's Team Seedling Fund; Convergent Aeronautics Solutions project FX The first author acknowledges sponsorship from the NASA Ames Research Center's Summer Faculty Fellowship. The work was partially supported by the NASA Aeronautics Research Mission Directorate's Team Seedling Fund and the Convergent Aeronautics Solutions project. NR 29 TC 0 Z9 0 U1 11 U2 11 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 SEP-OCT PY 2016 VL 53 IS 5 BP 1305 EP 1316 DI 10.2514/1.C033490 PG 12 WC Engineering, Aerospace SC Engineering GA DX3TS UT WOS:000384297800009 ER PT J AU Perry, B AF Perry, Boyd, III TI Results of National Advisory Committee for Aeronautics Report Number 496: Revisited SO JOURNAL OF AIRCRAFT LA English DT Article C1 [Perry, Boyd, III] NASA Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA. RP Perry, B (reprint author), NASA Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD SEP-OCT PY 2016 VL 53 IS 5 BP 1561 EP + DI 10.2514/1.C033663 PG 4 WC Engineering, Aerospace SC Engineering GA DX3TS UT WOS:000384297800030 ER PT J AU Liao, L Meneghini, R Tokay, A Bliven, LF AF Liao, Liang Meneghini, Robert Tokay, Ali Bliven, Larry F. TI Retrieval of Snow Properties for Ku- and Ka-Band Dual-Frequency Radar SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID SINGLE-SCATTERING PROPERTIES; ICE PARTICLES; FALL SPEED; SIZE; HYDROMETEORS; PARAMETERS; APPROXIMATION; DISDROMETER; CRYSTALS; DATABASE AB The focus of this study is on the estimation of snow microphysical properties and the associated bulk parameters such as snow water content and water equivalent snowfall rate for Ku- and Ka-band dual-frequency radar. This is done by exploring a suitable scattering model and the proper particle size distribution (PSD) assumption that accurately represent, in the electromagnetic domain, the micro-/macrophysical properties of snow. The scattering databases computed from simulated aggregates for small-to-moderate particle sizes are combined with a simple scattering model for large particle sizes to characterize snow-scattering properties over the full range of particle sizes. With use of the single-scattering results, the snow retrieval lookup tables can be formed in a way that directly links the Ku- and Ka-band radar reflectivities to snow water content and equivalent snowfall rate without use of the derived PSD parameters. A sensitivity study of the retrieval results to the PSD and scattering models is performed to better understand the dual-wavelength retrieval uncertainties. To aid in the development of the Ku- and Ka-band dual-wavelength radar technique and to further evaluate its performance, self-consistency tests are conducted using measurements of the snow PSD and fall velocity acquired from the Snow Video Imager/Particle Image Probe (SVI/PIP) during the winter of 2014 at the NASA Wallops Flight Facility site in Wallops Island, Virginia. C1 [Liao, Liang] Morgan State Univ, Goddard Earth Sci Technol & Res Program, Baltimore, MD 21239 USA. [Meneghini, Robert] NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA. [Tokay, Ali] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. [Tokay, Ali] Joint Ctr Earth Syst Technol, Baltimore, MD USA. [Bliven, Larry F.] NASA, Wallops Flight Facil, Wallops Isl, VA USA. RP Liao, L (reprint author), NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA. EM liang.liao-1@nasa.gov FU Dr. R. Kakar of NASA Headquarters under NASA's Precipitation Measurement Mission (PMM) [NNH12ZDA001N-PMM] FX This work is supported by Dr. R. Kakar of NASA Headquarters under NASA's Precipitation Measurement Mission (PMM; Grant NNH12ZDA001N-PMM). The authors also thank Mr. Jorel Torres of the South Dakota School of Mines and Technology for providing and processing SVI/PIP data, and Dr. Kwo-Sen Kuo of the University of Maryland for providing the scattering database. NR 40 TC 0 Z9 0 U1 3 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD SEP PY 2016 VL 55 IS 9 BP 1845 EP 1858 DI 10.1175/JAMC-D-15-0355.1 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DX1QM UT WOS:000384142100001 ER PT J AU Bedka, KM Khlopenkov, K AF Bedka, Kristopher M. Khlopenkov, Konstantin TI A Probabilistic Multispectral Pattern Recognition Method for Detection of Overshooting Cloud Tops Using Passive Satellite Imager Observations SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID PROFILING RADAR OBSERVATIONS; STRATOSPHERIC WATER-VAPOR; GOES-R; PRECIPITATION SYSTEMS; GLOBAL DISTRIBUTION; SEVERE WEATHER; CLIMATE-CHANGE; CONVECTION AB Deep convective updrafts often penetrate through the surrounding cirrus anvil and into the lower stratosphere. Cross-tropopause transport of ice, water vapor, and chemicals occurs within these "overshooting tops'' (OTs) along with a variety of hazardous weather conditions. OTs are readily apparent in satellite imagery, and, given the importance of OTs for weather and climate, a number of automated satellite-based detection methods have been developed. Some of these methods have proven to be relatively reliable, and their products are used in diverse Earth science applications. Nevertheless, analysis of these methods and feedback from product users indicate that use of fixed infrared temperature-based detection criteria often induces biases that can limit their utility for weather and climate analysis. This paper describes a new multispectral OT detection approach that improves upon those previously developed by minimizing use of fixed criteria and incorporating pattern recognition analyses to arrive at an OT probability product. The product is developed and validated using OT and non-OT anvil regions identified by a human within MODIS imagery. The product offered high skill for discriminating between OTs and anvils and matched 69% of human OT identifications for a particular probability threshold with a false-detection rate of 18%, outperforming previously existing methods. The false-detection rate drops to 1% when OT-induced texture detected within visible imagery is used to constrain the IR-based OT probability product. The OT probability product is also shown to improve severe-storm detection over the United States by 20% relative to the best existing method. C1 [Bedka, Kristopher M.] NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. [Khlopenkov, Konstantin] Sci Syst & Applicat Inc, Hampton, VA USA. RP Bedka, KM (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. EM kristopher.m.bedka@nasa.gov FU GOES-R Risk Reduction Research (R3) program FX This research has been supported by the GOES-R Risk Reduction Research (R3) program. In particular, we thank Dr. Steven Goodman, senior (chief) scientist, GOES-R System Program, for his guidance and support throughout this effort. We thank Patrick Minnis and Christopher Velden for their advice and collaboration throughout the algorithm-development process. We thank Cameron Homeyer for providing the WSR-88D data shown in this paper. We also thank Jake Smith for manually identifying OT locations in GOES-14 satellite imagery. NR 41 TC 0 Z9 0 U1 2 U2 2 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD SEP PY 2016 VL 55 IS 9 BP 1983 EP 2005 DI 10.1175/JAMC-D-15-0249.1 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DX1QM UT WOS:000384142100008 ER PT J AU Magi, BI Winesett, T Cecil, DJ AF Magi, Brian I. Winesett, Thomas Cecil, Daniel. J. TI Estimating Lightning from Microwave Remote Sensing Data SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID CLIMATE DATA RECORD; UNITED-STATES; SSM/I SENSORS; PART I; CLOUD; THUNDERSTORMS; RATES; EARTH; FIRE; IMAGER/SOUNDER AB This study evaluates a method for estimating the cloud-to-ground (CG) lightning flash rate from microwave remote sensing data. Defense Meteorological Satellite Program satellites have been in operation since 1987 and include global-viewing microwave sensors that capture thunderstorms as brightness temperature depressions. The National Lightning Detection Network (NLDN) has monitored CG lightning in the United States since 1997. This study investigates the relationship between CG lightning and microwave brightness temperature fields for the contiguous United States from April to September for the years 2005-12. The findings suggest that an exponential function, empirically fit to the NLDN and SSM/I data, provides lightning count measurements that agree to within 60%-70% with NLDN lightning, but with substantial misses and false alarms in the predictions. The discrepancies seem to be attributable to regional differences in thunderstorm characteristics that require a detailed study at smaller spatial scales to truly resolve, but snow at higher elevations also produces some anomalous microwave temperature depressions similar to those of thunderstorms. The results for the contiguous United States in this study are a step toward potentially using SSM/I data to estimate CG lightning around the world, although the sensitivity of the results to regional differences related to meteorological regimes would need further study. C1 [Magi, Brian I.; Winesett, Thomas] Univ North Carolina Charlotte, Dept Geog & Earth Sci, 9201 Univ City Blvd, Charlotte, NC 28223 USA. [Cecil, Daniel. J.] NASA Marshall Space Flight Ctr, Huntsville, AL USA. RP Magi, BI (reprint author), Univ North Carolina Charlotte, Dept Geog & Earth Sci, 9201 Univ City Blvd, Charlotte, NC 28223 USA. EM brian.magi@uncc.edu OI Magi, Brian/0000-0001-8131-0083 FU North Carolina Space Grant Consortium's New Investigator Program; UNC Charlotte faculty research grant; Lightning Imaging Sensor (LIS) team via the NASA Tropical Rainfall Measuring Mission FX The authors thank the staff at the Precipitation Research Group at Colorado State University for maintaining and managing the SSM/I data distribution. BIM and TW were partially supported by the North Carolina Space Grant Consortium's New Investigator Program. BIM was also partially supported by a UNC Charlotte faculty research grant. DJC was supported through the Lightning Imaging Sensor (LIS) team via the NASA Tropical Rainfall Measuring Mission. NR 46 TC 0 Z9 0 U1 4 U2 4 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD SEP PY 2016 VL 55 IS 9 BP 2021 EP 2036 DI 10.1175/JAMC-D-15-0306.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DX1QM UT WOS:000384142100010 ER PT J AU Huang, XL Chen, XH Zhou, DK Liu, X AF Huang, Xianglei Chen, Xiuhong Zhou, Daniel K. Liu, Xu TI An Observationally Based Global Band-by-Band Surface Emissivity Dataset for Climate and Weather Simulations SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID SEA-SURFACE; ALGORITHM; DATABASE; WINDOW; MODEL; SNOW; ICE AB While current atmospheric general circulation models (GCMs) still treat the surface as a blackbody in their longwave radiation scheme, recent studies suggest the need for taking realistic surface spectral emissivity into account. There have been few measurements available for the surface emissivity in the far IR (<650 cm(-1)). Based on first-principle calculation, the authors compute the spectral emissivity over the entire longwave spectrum for a variety of surface types. MODIS-retrieved mid-IR surface emissivity at 0.05 degrees x 0.05 degrees spatial resolution is then regressed against the calculated spectral emissivity to determine the surface type for each grid. The derived spectral emissivity data are then spatially averaged onto 0.5 degrees x 0.5 degrees grids and spectrally integrated onto the bandwidths used by the RRTMG_LW-a longwave radiation scheme widely used in current climate and numerical weather models. The band-by-band surface emissivity dataset is then compared with retrieved surface spectral emissivities from Infrared Atmospheric Sounding Interferometer (IASI) measurements. The comparison shows favorable agreement between two datasets in all the bands covered by the IASI measurements. The authors further use the dataset in conjunction with ERA-Interim to evaluate its impact on the top-of-atmosphere radiation budget. Depending on the blackbody surface assumptions used in the original calculation, the globally averaged difference caused by the inclusion of realistic surface emissivity ranges from -1.2 to -1.5 W m(-2) for clear-sky OLR and from -0.67 to -0.94 W m(-2) for all-sky OLR. Moreover, the difference is not spatially uniform and has a distinct spatial pattern. C1 [Huang, Xianglei; Chen, Xiuhong] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA. [Zhou, Daniel K.; Liu, Xu] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Huang, XL (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, 2455 Hayward St, Ann Arbor, MI 48109 USA. EM xianglei@umich.edu FU DOE Office of Biological and Environmental Research [DE-SC0012969]; NASA [NNX15AC25G] FX We wish to thank three anonymous reviewers for their thorough and thoughtful comments, which improved the clarity of the presentation. The ECMWF-Interim data were obtained from http://apps.ecmwf.int/datasets/. The MODIS retrievals of surface emissivity were from ftp://ftp.ssec.wisc.edu/pub/g_emis/. This research is supported by DOE Office of Biological and Environmental Research under Grant DE-SC0012969 and by NASA under Grant NNX15AC25G awarded to the University of Michigan. NR 36 TC 0 Z9 0 U1 1 U2 1 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 SEP PY 2016 VL 73 IS 9 BP 3541 EP 3555 DI 10.1175/JAS-D-15-0355.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DW8RP UT WOS:000383923500011 ER PT J AU Guimond, SR Heymsfield, GM Reasor, PD Didlake, AC AF Guimond, Stephen R. Heymsfield, Gerald M. Reasor, Paul D. Didlake, Anthony C., Jr. TI The Rapid Intensification of Hurricane Karl (2010): New Remote Sensing Observations of Convective Bursts from the Global Hawk Platform SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID TROPICAL CYCLONE INTENSIFICATION; HIGH-RESOLUTION SIMULATION; INNER-CORE; PART I; 3-DIMENSIONAL PERTURBATIONS; DOPPLER RADAR; BONNIE 1998; EVOLUTION; EYEWALL; EYE AB The evolution of rapidly intensifying Hurricane Karl (2010) is examined from a suite of remote sensing observations during the NASA Genesis and Rapid Intensification Processes (GRIP) field experiment. The novelties of this study are in the analysis of data from the airborne Doppler radar High-Altitude Imaging Wind and Rain Airborne Profiler (HI WRAP) and the new Global Hawk airborne platform that allows long endurance sampling of hurricanes. Supporting data from the High-Altitude Monolithic Microwave Integrated Circuit (MMIC) Sounding Radiometer (HAMSR) microwave sounder coincident with HIWRAP and coordinated flights with the NOAA WP-3D aircraft help to provide a comprehensive understanding of the storm. The focus of the analysis is on documenting and understanding the structure, evolution, and role of small-scale deep convective forcing in the storm intensification process. Deep convective bursts are sporadically initiated in the downshear quadrants of the storm and rotate into the upshear quadrants for a period of similar to 12 h during the rapid intensification. The aircraft data analysis indicates that the bursts are being formed and maintained through a combination of two main processes: 1) convergence generated from counterrotating mesovortex circulations and the larger vortex-scale flow and 2) the turbulent (scales of similar to 25 km) transport of anomalously warm, buoyant air from the eye to the eyewall at low levels. The turbulent mixing across the eyewall interface and forced convective descent adjacent to the bursts assists in carving out the eye of Karl, which leads to an asymmetric enhancement of the warm core. The mesovortices play a key role in the evolution of the features described above. The Global Hawk aircraft allowed an examination of the vortex response and axisymmetrization period in addition to the burst pulsing phase. A pronounced axisymmetric development of the vortex is observed following the pulsing phase that includes a sloped eyewall structure and formation of a clear, wide eye. C1 [Guimond, Stephen R.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Guimond, Stephen R.; Heymsfield, Gerald M.; Didlake, Anthony C., Jr.] NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA. [Reasor, Paul D.] NOAA, Atlantic Oceanog & Meteorol Lab, Hurricane Res Div, Miami, FL 33149 USA. [Didlake, Anthony C., Jr.] Oak Ridge Associated Univ, Oak Ridge, TN USA. RP Guimond, SR (reprint author), NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA. EM stephen.guimond@nasa.gov RI Reasor, Paul/B-2932-2014 OI Reasor, Paul/0000-0001-6407-017X FU Heymsfield's NASA GRIP through NASA; Heymsfield's NASA HS3 through NASA; NOAA; NASA; Institute of Geophysics and Planetary Physics (IGPP) at Los Alamos National Laboratory FX We thank Dr. Lihua Li, Matt McLinden, Martin Perrine, and Jaime Cervantes for their engineering efforts on HIWRAP during GRIP. We also thank the JPL HAMSR team for providing level 1B data used in this study, which was obtained from NASA Global Hydrology Resource Center in Huntsville, Alabama. Discussions with Dr. Scott Braun were useful and helped to clarify the presentation of the data. Dr. Lin Tian helped with early HIWRAP data processing. Author Guimond and coauthors Heymsfield and Didlake were funded under Heymsfield's NASA GRIP and HS3 funding, through NASA headquarters Program Manager Dr. Ramesh Kakar. Coauthor Reasor was funded through NOAA base funds. The NASA weather program under Dr. Ramesh Kakar supported GRIP. The first author was also partially supported by the Institute of Geophysics and Planetary Physics (IGPP) at Los Alamos National Laboratory. The first author thanks Robert Kilgore for his work on the conceptual diagram. Finally, we thank Rob Rogers and two anonymous reviewers for their very helpful comments. NR 47 TC 1 Z9 1 U1 5 U2 5 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 SEP PY 2016 VL 73 IS 9 BP 3617 EP 3639 DI 10.1175/JAS-D-16-0026.1 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DW8RP UT WOS:000383923500016 ER PT J AU Lin, Y Wang, Y Pan, BW Hu, JX Liu, YG Zhang, RY AF Lin, Yun Wang, Yuan Pan, Bowen Hu, Jiaxi Liu, Yangang Zhang, Renyi TI Distinct Impacts of Aerosols on an Evolving Continental Cloud Complex during the RACORO Field Campaign SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID DEEP CONVECTIVE CLOUDS; FINE PARTICULATE MATTER; LONG-TERM IMPACTS; ANTHROPOGENIC AEROSOLS; SHALLOW CUMULUS; MICROPHYSICS PARAMETERIZATION; STRATOCUMULUS CLOUDS; ABSORBING AEROSOLS; RESOLVING MODEL; CLIMATE MODELS AB A continental cloud complex, consisting of shallow cumuli, a deep convective cloud (DCC), and stratus, is simulated by a cloud-resolving Weather Research and Forecasting Model to investigate the aerosol micro physical effect (AME) and aerosol radiative effect (ARE) on the various cloud regimes and their transitions during the Department of Energy Routine Atmospheric Radiation Measurement Aerial Facility Clouds with Low Optical Water Depths Optical Radiative Observations (RACORO) campaign. Under an elevated aerosol loading with AME only, a reduced cloudiness for the shallow cumuli and stratus resulted from more droplet evaporation competing with suppressed precipitation, but an enhanced cloudiness for the DCC is attributed to more condensation. With the inclusion of ARE, the shallow cumuli are suppressed owing to the thermodynamic effects of light-absorbing aerosols. The responses of DCC and stratus to aerosols are monotonic with AME only but nonmonotonic with both AME and ARE. The DCC is invigorated because of favorable convection and moisture conditions at night induced by daytime ARE, via the so-called aerosol-enhanced conditional instability mechanism. The results reveal that the overall aerosol effects on the cloud complex are distinct from the individual cloud types, highlighting that the aerosol cloud interactions for diverse cloud regimes and their transitions need to be evaluated to assess the regional and global climatic impacts. C1 [Lin, Yun; Pan, Bowen; Hu, Jiaxi; Zhang, Renyi] Texas A&M Univ, College Stn, TX USA. [Wang, Yuan] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Liu, Yangang] Brookhaven Natl Lab, Upton, NY 11973 USA. RP Zhang, RY (reprint author), Texas A&M Univ, Dept Atmospher Sci, Oceanog & Meteorol Bldg,Room 1108,MS 3150, College Stn, TX 77843 USA. EM renyi-zhang@tamu.edu OI Lin, Yun/0000-0001-8222-0346 FU DOE's Earth System Modeling (ESM) Program via the FASTER project [DOE-DE-AC02-98CH10886]; NASA [ROSES14-ACMAP, 105357-281945.02.31.03.24] FX This research is supported by DOE's Earth System Modeling (ESM) Program via the FASTER project (www.bnl.gov/faster), under Grant DOE-DE-AC02-98CH10886. The RACORO field campaign was supported by DOE's ARM program. We are grateful for discussions on RACORO with Dr. Andrew Vogelmann at BNL and on aerosol microphysics effects on various clouds with Dr. Jonathan H. Jiang at JPL. The data from the RACORO field campaign, utilized only for education and research, are open to public after registration and application. Supercomputing computational facilities were provided by the Texas A&M University. Yuan Wang's contribution to this work was sponsored by NASA ROSES14-ACMAP and was carried at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA (Grant 105357-281945.02.31.03.24). NR 93 TC 0 Z9 0 U1 9 U2 9 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 SEP PY 2016 VL 73 IS 9 BP 3681 EP 3700 DI 10.1175/JAS-D-15-0361.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DW8RP UT WOS:000383923500019 ER PT J AU Holt, LA Alexander, MJ Coy, L Molod, A Putman, W Pawson, S AF Holt, Laura A. Alexander, M. Joan Coy, Lawrence Molod, Andrea Putman, William Pawson, Steven TI Tropical Waves and the Quasi-Biennial Oscillation in a 7-km Global Climate Simulation SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID GENERAL-CIRCULATION MODEL; COUPLED EQUATORIAL WAVES; QBO-LIKE OSCILLATION; GRAVITY-WAVES; CONVECTION; TEMPERATURE; PARAMETERIZATION; STRATOSPHERE; IMPROVEMENTS; VARIABILITY AB This study investigates tropical waves and their role in driving a quasi-biennial oscillation (QBO)-like signal in stratospheric winds in a global 7-km-horizontal-resolution atmospheric general circulation model. The Nature Run (NR) is a 2-yr global mesoscale simulation of the Goddard Earth Observing System Model, version 5 (GEOS-5). In the tropics, there is evidence that the NR supports a broad range of convectively generated waves. The NR precipitation spectrum resembles the observed spectrum in many aspects, including the preference for westward-propagating waves. However, even with very high horizontal resolution and a healthy population of resolved waves, the zonal force provided by the resolved waves is still too low in the QBO region and parameterized gravity wave drag is the main driver of the NR-QBO-like oscillation (NR-QBO). The authors suggest that causes include coarse vertical resolution and excessive dissipation. Nevertheless, the very-high-resolution NR provides an opportunity to analyze the resolved wave forcing of the NR-QBO. In agreement with previous studies, large-scale Kelvin and small-scale waves contribute to the NR-QBO driving in eastward shear zones and small-scale waves dominate the NR-QBO driving in westward shear zones. Waves with zonal wavelength < 1000 km account for up to half of the small-scale (<3300 km) resolved wave forcing in eastward shear zones and up to 70% of the small-scale resolved wave forcing in westward shear zones of the NR-QBO. C1 [Holt, Laura A.; Alexander, M. Joan] NorthWest Res Associates, 3380 Mitchell Lane, Boulder, CO 80301 USA. [Coy, Lawrence; Putman, William; Pawson, Steven] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD USA. [Coy, Lawrence] Sci Syst & Applicat Inc, Lanham, MD USA. [Molod, Andrea] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. RP Holt, LA (reprint author), NorthWest Res Associates, 3380 Mitchell Lane, Boulder, CO 80301 USA. EM laura@nwra.com FU NASA Global Modeling and Assimilation Office [NNX14O76G]; NASA's Modeling, Analysis and Prediction (MAP) program FX We thank Dr. Ji-Eun Kim for providing the TRMM spectrum for Fig. 2, and we thank three anonymous reviewers for their thoughtful and helpful suggestions. This work is funded by the NASA Global Modeling and Assimilation Office, Grant NNX14O76G. This work was also supported by NASA's Modeling, Analysis and Prediction (MAP) program. NR 51 TC 2 Z9 2 U1 5 U2 5 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 SEP PY 2016 VL 73 IS 9 BP 3771 EP 3783 DI 10.1175/JAS-D-15-0350.1 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DW8RP UT WOS:000383923500024 ER PT J AU Thurman, D Poinsatte, P Ameri, A Culley, D Raghu, S Shyam, V AF Thurman, Douglas Poinsatte, Philip Ameri, Ali Culley, Dennis Raghu, Surya Shyam, Vikram TI Investigation of Spiral and Sweeping Holes SO JOURNAL OF TURBOMACHINERY-TRANSACTIONS OF THE ASME LA English DT Article AB Surface infrared thermography, hotwire anemometry, and thermocouple surveys were performed on two new film cooling hole geometries: spiral/rifled holes and fluidic sweeping holes. The spiral holes attempt to induce large-scale vorticity to the film cooling jet as it exits the hole to prevent the formation of the kidney-shaped vortices commonly associated with film cooling jets. The fluidic sweeping hole uses a passive in-hole geometry to induce jet sweeping at frequencies that scale with blowing ratios. The spiral hole performance is compared to that of round holes with and without compound angles. The fluidic hole is of the diffusion class of holes and is therefore compared to a 777 hole and square holes. A patent-pending spiral hole design showed the highest potential of the nondiffusion-type hole configurations. Velocity contours and flow temperature were acquired at discreet cross sections of the downstream flow field. The passive fluidic sweeping hole shows the most uniform cooling distribution but suffers from low span-averaged effectiveness levels due to enhanced mixing. The data were taken at a Reynolds number of 11,000 based on hole diameter and freestream velocity. Infrared thermography was taken for blowing ratios of 1.0, 1.5, 2.0, and 2.5 at a density ratio of 1.05. The flow inside the fluidic sweeping hole was studied using 3D unsteady Reynolds-average Navier-Stokes (RANS). C1 [Thurman, Douglas] US Army Res Lab, Cleveland, OH 44135 USA. [Poinsatte, Philip; Culley, Dennis; Shyam, Vikram] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. [Ameri, Ali] Ohio State Univ, Dept Mech & Aerosp Engn, Columbus, OH 43210 USA. [Raghu, Surya] Adv Fluid LLC, Columbia, MD 21045 USA. RP Thurman, D (reprint author), US Army Res Lab, Cleveland, OH 44135 USA. EM drthurman@nasa.gov; poinsatte@nasa.gov; ali.a.ameri@nasa.gov; dennis.e.culley@nasa.gov; sraghu@advancedfluidics.com; vikram.shyam-1@nasa.gov FU NASA's Fundamental Aeronautics Program's Fixed Wing Project; NASA's Center Innovation Fund FX This work was funded by NASA's Fundamental Aeronautics Program's Fixed Wing Project and NASA's Center Innovation Fund. The authors would also like to thank Dr. Mark Wernet and Dr. Adam Wroblewski for the particle image velocimetry results. NR 15 TC 0 Z9 0 U1 0 U2 0 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 0889-504X EI 1528-8900 J9 J TURBOMACH JI J. Turbomach.-Trans. ASME PD SEP PY 2016 VL 139 IS 9 AR 091007 DI 10.1115/1.4032839 PG 11 WC Engineering, Mechanical SC Engineering GA DX3BE UT WOS:000384246800007 ER PT J AU Abarca, SF Montgomery, MT Braun, SA Dunion, J AF Abarca, Sergio F. Montgomery, Michael T. Braun, Scott A. Dunion, Jason TI On the Secondary Eyewall Formation of Hurricane Edouard (2014) SO MONTHLY WEATHER REVIEW LA English DT Article ID TROPICAL CYCLONES; RITA 2005; REPLACEMENT; INTENSITY; EVOLUTION; DYNAMICS; VORTEX; CORE; CYCLE; FIELD AB A first observationally based estimation of departures from gradient wind balance during secondary eyewall formation is presented. The study is based on the Atlantic Hurricane Edouard (2014). This storm was observed during the National Aeronautics and Space Administration's (NASA) Hurricane and Severe Storm Sentinel (HS3) experiment, a field campaign conducted in collaboration with the National Oceanic and Atmospheric Administration (NOAA). A total of 135 dropsondes are analyzed in two separate time periods: one named the secondary eyewall formation period and the other one referred to as the decaying double eyewalled storm period. During the secondary eyewall formation period, a time when the storm was observed to have only one eyewall, the diagnosed agradient force has a secondary maximum that coincides with the radial location of the secondary eyewall observed in the second period of study. The maximum spinup tendency of the radial influx of absolute vertical vorticity is within the boundary layer in the region of the eyewall of the storm and the spinup tendency structure elongates radially outward into the secondary region of supergradient wind, where the secondary wind maximum is observed in the second period of study. An analysis of the boundary layer averaged vertical structure of equivalent potential temperature reveals a conditionally unstable environment in the secondary eyewall formation region. These findings support the hypothesis that deep convective activity in this region contributed to spinup of the boundary layer tangential winds and the formation of a secondary eyewall that is observed during the decaying double eyewalled storm period. C1 [Abarca, Sergio F.] Natl Ocean & Atmospher Adm, IM Syst Grp, Natl Ctr Environm Protect, Natl Weather Serv, College Pk, MD USA. [Montgomery, Michael T.] Naval Postgrad Sch, Monterey, CA USA. [Braun, Scott A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Dunion, Jason] Univ Miami, Cooperat Inst Marine & Atmospher Studies, Miami, FL USA. [Dunion, Jason] NOAA, Atlantic Oceanog & Meteorol Lab, Hurricane Res Div, Miami, FL 33149 USA. RP Abarca, SF (reprint author), NOAA, IM Syst Grp, NWS, NCEP, 5830 Univ Res Court, College Pk, MD 20740 USA. EM sergio.abarca@noaa.gov RI Dunion, Jason/B-1352-2014 OI Dunion, Jason/0000-0001-7489-0569 FU National Research Council (NRC) through Research Associateship Program; Naval Postgraduate School (NPS) in Monterey, California; NSF [AGS-1313948]; NOAA HFIP Grant [N0017315WR00048]; NASA HS3 Grant [NNG11PK021]; U.S. Naval Postgraduate School FX The first author gratefully acknowledges the support from the National Research Council (NRC) through its Research Associateship Program; the host institution, the Naval Postgraduate School (NPS) in Monterey, California; and Scott Braun for the funding that made it possible for him to participate in the H53 deployment during the 2014 hurricane season. MTM acknowledges the support of NSF Grant AGS-1313948, NOAA HFIP Grant N0017315WR00048, NASA HS3 Grant NNG11PK021, and the U.S. Naval Postgraduate School. NR 37 TC 0 Z9 0 U1 2 U2 2 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 EI 1520-0493 J9 MON WEATHER REV JI Mon. Weather Rev. PD SEP PY 2016 VL 144 IS 9 BP 3321 EP 3331 DI 10.1175/MWR-D-15-0421.1 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DW8RN UT WOS:000383923300014 ER PT J AU Lee, JH Biging, GS Fisher, JB AF Lee, Jun-Hak Biging, Gregory S. Fisher, Joshua B. TI An Individual Tree-Based Automated Registration of Aerial Images to Lidar Data in a Forested Area SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING LA English DT Article ID MULTISPECTRAL DATA FUSION; AIRBORNE LASER SCANNER; CROWN DETECTION; LAND-COVER; DELINEATION; HEIGHT; CLASSIFICATION; RECONSTRUCTION; SEGMENTATION; MOSAICKING AB In this paper, we demonstrate an approach to align aerial images to airborne lidar data by using common object features (tree tops) from both data sets under the condition that conventional correlation-based approaches are challenging due to the fact that the spatial pattern of pixel gray-scale values in aerial images hardly exist in lidar data. We extracted tree tops by using an image processing technique called extended-maxima transformation from both aerial images and lidar data. Our approach was tested at the Angelo Coast Range Reserve on the South Fork Eel River forests in Mendocino County, California. Although the aerial images were acquired simultaneously with the lidar data, the images had only approximate exposure point locations and average flight elevation information, which mimicked the condition of limited information availability about the aerial images. Our results showed that this approach enabled us to align aerial images to airborne lidar data at the single-tree level with reasonable accuracy. With a local transformation model (piecewise linear model), the RMSE and the median absolute deviation (MAD) of the registration were 9.2 pixels (2.3 meters) and 6.8 pixels (1.41 meters), respectively. We expect our approach to be applicable to fine scale change detection for forest ecosystems and may serve to extract detailed forest biophysical parameters. C1 [Lee, Jun-Hak] Univ Oregon, Dept Landscape Architecture, Eugene, OR 97403 USA. [Biging, Gregory S.] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lee, JH (reprint author), Univ Oregon, Dept Landscape Architecture, Eugene, OR 97403 USA. EM junhaklee@uoregon.edu FU W.S. Rosecrans Fellowship, Environmental Science, Policy, and Management, University of California, Berkeley; National Aeronautics and Space Administration FX We gratefully acknowledge the use of lidar data sets supplied by Dr. William E. Dietrich and the National Center of Airborne Laser Mapping (NCALM). The first author was partially funded by the W.S. Rosecrans Fellowship, Environmental Science, Policy, and Management, University of California, Berkeley. Dr. Joshua B. Fisher contributed to this paper through work by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 60 TC 0 Z9 0 U1 12 U2 12 PU AMER SOC PHOTOGRAMMETRY PI BETHESDA PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA SN 0099-1112 EI 2374-8079 J9 PHOTOGRAMM ENG REM S JI Photogramm. Eng. Remote Sens. PD SEP PY 2016 VL 82 IS 9 BP 699 EP 710 DI 10.14358/PERS.82.9.699 PG 12 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA DX0NR UT WOS:000384060300007 ER PT J AU Mendez-Villanueva, A Suarez-Arrones, L Rodas, G Fernandez-Gonzalo, R Tesch, P Linnehan, R Kreider, R Di Salvo, V AF Mendez-Villanueva, Alberto Suarez-Arrones, Luis Rodas, Gil Fernandez-Gonzalo, Rodrigo Tesch, Per Linnehan, Richard Kreider, Richard Di Salvo, Valter TI MRI-Based Regional Muscle Use during Hamstring Strengthening Exercises in Elite Soccer Players SO PLOS ONE LA English DT Article ID MEDICAL-RESEARCH PROGRAM; PROFESSIONAL FOOTBALL; ECCENTRIC OVERLOAD; NONUNIFORM CHANGES; INJURIES; PREVENTION; MECHANICS; STRAINS; SCIENCE; RETURN AB The present study examined site-specific hamstring muscles use with functional magnetic resonance imaging (MRI) in elite soccer players during strength training. Thirty-six players were randomized into four groups, each performing either Nordic hamstring, flywheel legcurl, Russian belt or the hip-extension conic-pulley exercise. The transverse relaxation time (T-2) shift from pre-to post-MRI were calculated for the biceps femoris long (BFI) and short (BFs) heads, semitendinosus (ST) and semimembranosus (SM) muscles at proximal, middle and distal areas of the muscle length. T-2 values increased substantially after flywheel leg-curl in all regions of the BFI (from 9 +/- 8 to 16 +/- 8%), BFs (41 +/- 6-71 +/- 11%), and ST (60 +/- 1-69 +/- 7%). Nordic hamstring induced a substantial T2 increase in all regions of the BFs (13 +/- 8-16 +/- 5%) and ST (15 +/- 7-17 +/- 5%). T-2 values after the Russian belt deadlift substantially increased in all regions of the BFI (6 +/- 4-7 +/- 5%), ST (8 +/- 3-11 +/- 2%), SM (6 +/- 4-10 +/- 4%), and proximal and distal regions of BFs (6 +/- 6-8 +/- 5%). T-2 values substantially increased after hip-extension conic-pulley only in proximal and middle regions of BFI (11 +/- 5-7 +/- 5%) and ST (7 +/- 3-12 +/- 4%). The relevance of such MRI-based inter-and intra-muscle use in designing more effective resistance training for improving hamstring function and preventing hamstring injuries in elite soccer players should be explored with more mechanistic studies. C1 [Mendez-Villanueva, Alberto; Suarez-Arrones, Luis; Di Salvo, Valter] ASPIRE Acad, Football Performance & Sci Dept, Doha, Qatar. [Suarez-Arrones, Luis] Pablo de Olavide Univ, Sports Dept, Seville, Spain. [Rodas, Gil] Futbol Club Barcelona, Dept Med, Barcelona, Spain. [Fernandez-Gonzalo, Rodrigo; Tesch, Per] Karolinska Inst, Dept Physiol & Pharmacol, Stockholm, Sweden. [Linnehan, Richard] Johnson Space Ctr, Natl Aeronaut & Space Adm, Houston, TX USA. [Kreider, Richard] Texas A&M Univ, Dept Hlth & Kinesiol, College Stn, TX USA. [Di Salvo, Valter] Univ Rome Foro Italico, Dept Movement Human & Hlth Sci, Rome, Italy. RP Mendez-Villanueva, A (reprint author), ASPIRE Acad, Football Performance & Sci Dept, Doha, Qatar. EM jose.villanueva@aspire.qa FU NPRP grant from the Qatar National Research Fund [NPRP 6-1526-3-363] FX This study was made possible by NPRP grant #NPRP 6-1526-3-363 from the Qatar National Research Fund (a member of Qatar Foundation). The funder provided support in the form of salaries for authors LSA, RFG and PT, but did not have any additional role in the study design, data collection and analysis, decision to publish, or preparation of the manuscript. The specific roles of these authors are articulated in the 'author contributions' section. NR 31 TC 0 Z9 0 U1 14 U2 14 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD SEP 1 PY 2016 VL 11 IS 9 AR e0161356 DI 10.1371/journal.pone.0161356 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DV3WN UT WOS:000382855600024 PM 27583444 ER PT J AU Ayers, A Miller, K Park, J Schwartz, L Antcliff, R AF Ayers, Alan Miller, Kimberly Park, Jongwon Schwartz, Lawrence Antcliff, Rich TI The Hollywood Model Leveraging the Capabilities of Freelance Talent to Advance Innovation and Reduce Risk SO RESEARCH-TECHNOLOGY MANAGEMENT LA English DT Article DE Hollywood model; Talent management; Futures; IRI2038; IRI Research ID ERA AB In 2013, the Industrial Research Institute (IRI) commissioned the IRI2038 foresight project to research how developments in technology, business processes, regulation and other spheres will impact the art and science of research and technology management over the next 25 years. That study defined three scenarios likely to shape the innovation process in coming years. One of those scenarios was the Hollywood model, in which scientists, engineers, and innovators no longer work for a single firm but rather contract out their services to individual projects and then move on to other projects and companies. Over the course of six months, an IRI Research working group conducted four workshops with R&D leaders at IRI member companies to explore how talent management would be affected in this scenario. The workshops identified challenges and opportunities associated with the Hollywood model as a paradigm for industrial R&D, focused around eight critical aspects of current talent management practice. Although the Hollywood model faces significant infrastructure and legal impediments today, its employment of external R&D workers with diverse experiences and perspectives is likely to create a greater opportunity for significant innovation. C1 [Ayers, Alan] UConn, Storrs, CT 06269 USA. [Ayers, Alan] IDCC, Doha, Qatar. [Ayers, Alan] Research on Res Comm, Arlington, VA 22203 USA. [Ayers, Alan] ROR Grp Rad Innovat & Levels Innovat, Arlington, TX USA. [Miller, Kimberly] Sutton House Consulting LLC, Florence, OR USA. [Miller, Kimberly] Cargills Global R&D Team, Minneapolis, MN USA. [Miller, Kimberly] Univ St Thomas, Org Dev, St Paul, MN USA. [Park, Jongwon] Korea Innovat Ctr, Washington, DC USA. [Park, Jongwon] Arizona State Univ, Consortium Sci Policy & Outcomes, Tempe, AZ 85287 USA. [Schwartz, Lawrence] IP Business Tech Solut, Menlo Pk, CA USA. [Antcliff, Rich] NASA, Langley Res Ctr, Off Strateg Anal Commun & Business Dev, Hampton, VA 23665 USA. RP Ayers, A (reprint author), UConn, Storrs, CT 06269 USA.; Ayers, A (reprint author), IDCC, Doha, Qatar.; Ayers, A (reprint author), Research on Res Comm, Arlington, VA 22203 USA.; Ayers, A (reprint author), ROR Grp Rad Innovat & Levels Innovat, Arlington, TX USA. EM adayers@buildinnovation.com; kim@suttonhouseconsulting.com; jpglobalconsultingllc@gmail.com; larryschwartz333@aol.com; Richard.R.Antcliff@nasa.gov NR 18 TC 0 Z9 0 U1 15 U2 15 PU INDUSTRIAL RESEARCH INST, INC PI ARLINGTON PA 2300 CLARENDON BLVD, STE 400, ARLINGTON, VA 22201 USA SN 0895-6308 EI 1930-0166 J9 RES TECHNOL MANAGE JI Res.-Technol. Manage. PD SEP-OCT PY 2016 VL 59 IS 5 BP 27 EP 37 DI 10.1080/08956308.2016.1208041 PG 11 WC Business; Engineering, Industrial; Management SC Business & Economics; Engineering GA DX6ZQ UT WOS:000384535600009 ER PT J AU Haarig, M Engelmann, R Ansmann, A Veselovskii, I Whiteman, DN Althausen, D AF Haarig, Moritz Engelmann, Ronny Ansmann, Albert Veselovskii, Igor Whiteman, David N. Althausen, Dietrich TI 1064 nm rotational Raman lidar for particle extinction and lidar-ratio profiling: cirrus case study SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID SPECTRAL-RESOLUTION LIDAR; ELASTIC-BACKSCATTER LIDAR; INDIAN AEROSOL PLUME; MULTIWAVELENGTH LIDAR; SAHARAN DUST; WATER-VAPOR; PHYSICAL-PROPERTIES; 6-WAVELENGTH LIDAR; OPTICAL-PROPERTIES; RETRIEVAL AB For the first time, vertical profiles of the 1064 nm particle extinction coefficient obtained from Raman lidar observations at 1058 nm (nitrogen and oxygen rotational Raman backscatter) are presented. We applied the new technique in the framework of test measurements and performed several cirrus observations of particle backscatter and extinction coefficients, and corresponding extinction-to-backscatter ratios at the wavelengths of 355, 532, and 1064 nm. The cirrus backscatter coefficients were found to be equal for all three wavelengths keeping the retrieval uncertainties in mind. The multiple-scattering-corrected cirrus extinction coefficients at 355 nm were on average about 20-30% lower than the ones for 532 and 1064 nm. The cirrus-mean extinction-to-backscatter ratio (lidar ratio) was 31 +/- 5 sr (355 nm), 36 +/- 5 sr (532 nm), and 38 +/- 5 sr (1064 nm) in this single study. We further discussed the requirements needed to obtain aerosol extinction profiles in the lower troposphere at 1064 nm with good accuracy (20% relative uncertainty) and appropriate temporal and vertical resolution. C1 [Haarig, Moritz; Engelmann, Ronny; Ansmann, Albert; Althausen, Dietrich] Leibniz Inst Tropospher Res, Leipzig, Germany. [Veselovskii, Igor] Phys Instrumentat Ctr, Moscow, Russia. [Whiteman, David N.] NASA, GSFC, Greenbelt, MD USA. RP Haarig, M (reprint author), Leibniz Inst Tropospher Res, Leipzig, Germany. EM haarig@tropos.de FU Russian Science Foundation [16-17-10241] FX We thank Johannes Buhl for providing Doppler lidar observations of vertical velocity and estimated ice crystal sizes. Modeling of the rotational Raman filter parameters was supported by the Russian Science Foundation (project no. 16-17-10241). NR 63 TC 0 Z9 0 U1 2 U2 2 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 EI 1867-8548 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PD SEP 1 PY 2016 VL 9 IS 9 BP 4269 EP 4278 DI 10.5194/amt-9-4269-2016 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DW8FZ UT WOS:000383891500002 ER PT J AU Diskin, B Thomas, JL Rumsey, CL Schwoppe, A AF Diskin, Boris Thomas, James L. Rumsey, Christopher L. Schwoeppe, Axel TI Grid-Convergence of Reynolds-Averaged Navier-Stokes Solutions for Benchmark Flows in Two Dimensions SO AIAA JOURNAL LA English DT Article ID TURBULENCE MODEL; EULER EQUATIONS AB A detailed grid-convergence study has been conducted to establish reference solutions corresponding to the one-equation linear eddy-viscosity Spalart-Allmaras turbulence model for two-dimensional turbulent flows around the NACA0012 airfoil and a flat plate. The study involved the three widely used codes CFL3D (NASA), FUN3D (NASA), and TAU (DLR, The German Aerospace Center), as well as families of uniformly refined structured grids that differed in the grid density patterns. Solutions computed by different codes on different grid families appeared to converge to the same continuous limit but exhibited strikingly different convergence characteristics. The grid resolution in the vicinity of geometric singularities, such as a sharp trailing edge, was found to be the major factor affecting accuracy and convergence of discrete solutions; the effects of this local grid resolution were more prominent than differences in discretization schemes and/or grid elements. The results reported for these relatively simple turbulent flows demonstrated that CFL3D, FUN3D, and TAU solutions were very similar on the finest grids used in the study, but even those grids were not sufficient to conclusively establish an asymptotic convergence order. C1 [Diskin, Boris] Natl Inst Aerosp, MAE Dept, Hampton, VA 23666 USA. [Thomas, James L.; Rumsey, Christopher L.] NASA Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA. [Schwoeppe, Axel] German Aerosp Ctr, DLR, Inst Aerodynam & Flow Technol, D-38108 Braunschweig, Germany. [Diskin, Boris] Univ Virginia, Charlottesville, VA 22904 USA. RP Diskin, B (reprint author), Natl Inst Aerosp, MAE Dept, Hampton, VA 23666 USA. FU NASA [NNL09AA00A] FX The first author acknowledges support from NASA Cooperative Agreement NNL09AA00A. NR 38 TC 0 Z9 0 U1 3 U2 3 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD SEP PY 2016 VL 54 IS 9 BP 2563 EP 2588 DI 10.2514/1.J054555 PG 26 WC Engineering, Aerospace SC Engineering GA DV8GN UT WOS:000383175600002 ER PT J AU Pandya, MJ Diskin, B Thomas, JL Frink, NT AF Pandya, Mohagna J. Diskin, Boris Thomas, James L. Frink, Neal T. TI Improved Convergence and Robustness of USM3D Solutions on Mixed-Element Grids SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT 53rd AIAA Aerospace Sciences Meeting / AIAA Atmospheric Flight Mechanics Conference / 17th AIAA Non-Deterministic Approaches Conference / AIAA Science and Technology Forum and Exposition (SciTech) / AIAA Infotech at Aerospace Conference CY JAN 05-09, 2015 CL Kissimmee, FL SP AIAA ID EULER EQUATIONS; GENERATION; ALGORITHM; DYNAMICS; TETRUSS; FLOWS; CODES AB Several improvements to the mixed-element USM3D discretization and defect-correction schemes have been made. A new methodology for nonlinear iterations, called the Hierarchical Adaptive Nonlinear Iteration Method, has been developed and implemented. The Hierarchical Adaptive Nonlinear Iteration Method provides two additional hierarchies around a simple and approximate preconditioner of USM3D. The hierarchies are a matrix-free linear solver for the exact linearization of Reynolds-averaged Navier-Stokes equations and a nonlinear control of the solution update. Two variants of the Hierarchical Adaptive Nonlinear Iteration Method are assessed on four benchmark cases, namely, a zero-pressure-gradient flat plate, a bump-in-channel configuration, the NACA 0012 airfoil, and a NASA Common Research Model configuration. The new methodology provides a convergence acceleration factor of 1.4 to 13 over the preconditioner-alone method representing the baseline solver technology. C1 [Pandya, Mohagna J.] NASA Langley Res Ctr, Configurat Aerodynam Branch, Mail Stop 499, Hampton, VA 23681 USA. [Diskin, Boris] Natl Inst Aerosp, Hampton, VA 23666 USA. [Thomas, James L.; Frink, Neal T.] NASA Langley Res Ctr, Computat Aerosci Branch, Mail Stop 499, Hampton, VA 23681 USA. [Diskin, Boris] Univ Virginia, MAE Dept, Charlottesville, VA USA. RP Pandya, MJ (reprint author), NASA Langley Res Ctr, Configurat Aerodynam Branch, Mail Stop 499, Hampton, VA 23681 USA. NR 47 TC 0 Z9 0 U1 3 U2 3 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD SEP PY 2016 VL 54 IS 9 BP 2589 EP 2610 DI 10.2514/1.J054545 PG 22 WC Engineering, Aerospace SC Engineering GA DV8GN UT WOS:000383175600003 ER PT J AU Ceze, MA Fidkowski, KJ AF Ceze, Marco A. Fidkowski, Krzysztof J. TI High-Order Output-Based Adaptive Simulations of Turbulent Flow in Two Dimensions SO AIAA JOURNAL LA English DT Article ID NAVIER-STOKES EQUATIONS; DISCONTINUOUS GALERKIN DISCRETIZATIONS; MESH ADAPTATION; FLUID-DYNAMICS; PREDICTION AB Output-based high-order adaptive results are presented for several benchmark two-dimensional turbulent-flow simulations. The discretization is a high-order discontinuous Galerkin finite element method, and the equations solved are compressible Navier-Stokes, Reynolds-averaged with a modified version of the Spalart-Allmaras one-equation model. Mesh refinement requirements are studied through automated output-based adaptation in which a discrete adjoint solution associated with an output (e.g., the drag coefficient) weights a fine-space residual and automatically selects the elements that need more resolution. The roles of high-order and mesh anisotropy are also investigated. Finally, differences are investigated between two mesh refinement strategies: hanging-node refinement of structured meshes versus metric-based remeshing of unstructured triangles. C1 [Ceze, Marco A.] NASA Ames Res Ctr, Moffett Field, CA USA. [Fidkowski, Krzysztof J.] Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA. [Ceze, Marco A.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. RP Ceze, MA (reprint author), NASA Ames Res Ctr, Moffett Field, CA USA.; Ceze, MA (reprint author), Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. EM marco.a.ceze@nasa.gov FU U.S. Air Force Office of Scientific Research [FA9550-11-1-0081] FX The authors acknowledge support from the U.S. Air Force Office of Scientific Research under grant FA9550-11-1-0081. NR 23 TC 0 Z9 0 U1 1 U2 1 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD SEP PY 2016 VL 54 IS 9 BP 2611 EP 2625 DI 10.2514/1.J054517 PG 15 WC Engineering, Aerospace SC Engineering GA DV8GN UT WOS:000383175600004 ER PT J AU Eisfeld, B Rumsey, C Togiti, V AF Eisfeld, Bernhard Rumsey, Chris Togiti, Vamshi TI Verification and Validation of a Second-Moment Closure Model (vol 54, pg 1524, 2016) SO AIAA JOURNAL LA English DT Correction C1 [Eisfeld, Bernhard; Togiti, Vamshi] DLR Inst Aerodynam & Flow Technol, D-38108 Braunschweig, Germany. [Rumsey, Chris] NASA Langley Res Ctr, MS 128, Hampton, VA USA. RP Eisfeld, B (reprint author), DLR Inst Aerodynam & Flow Technol, D-38108 Braunschweig, Germany. NR 1 TC 0 Z9 0 U1 2 U2 2 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD SEP PY 2016 VL 54 IS 9 BP 2925 EP 2925 DI 10.2514/1.J055336 PG 1 WC Engineering, Aerospace SC Engineering GA DV8GN UT WOS:000383175600030 ER PT J AU Young, KE Evans, CA Hodges, KV Bleacher, JE Graff, TG AF Young, Kelsey E. Evans, Cynthia A. Hodges, Kip V. Bleacher, Jacob E. Graff, Trevor G. TI A review of the handheld X-ray fluorescence spectrometer as a tool for field geologic investigations on Earth and in planetary surface exploration SO APPLIED GEOCHEMISTRY LA English DT Review DE Handheld X-ray fluorescence spectrometer (hXRF); In situ geochemistry; Planetary field geology; In situ field geologic instrument; Field portable technology; Field spectroscopy ID PORTABLE XRF; ROCKS; SAMPLES; DETECTOR; MARS; SOIL AB X-ray fluorescence (XRF) spectroscopy is a well-established and commonly used technique in obtaining diagnostic compositional data on geological samples. Recently, developments in X-ray tube and detector technologies have resulted in miniaturized, field-portable instruments that enable new applications both in and out of standard laboratory settings. These applications, however, have not been extensively applied to geologic field campaigns. This study investigates the feasibility of using developing handheld XRF (hXRF) technology to enhance terrestrial field geology, with potential applications in planetary surface exploration missions. We demonstrate that the hXRF is quite stable, providing reliable and accurate data continuously over a several year period. Additionally, sample preparation is proved to have a marked effect on the strategy for collecting and assimilating hXRF data. While the hXRF is capable of obtaining data that are comparable to laboratory XRF analysis for several geologically-important elements (such as Si, Ca, Ti, and K), the instrument is unable to detect other elements (such as Mg and Na) reliably. While this limits the use of the hXRF, especially when compared to laboratory XRF techniques, the hXRF is still capable of providing the field user with significantly improved contextual awareness of a field site, and more work is needed to fully evaluate the potential of this instrument in more complex geologic environments. (C) 2016 The Authors. Published by Elsevier Ltd. This is an open access article under the CC BY-NC-ND license. C1 [Young, Kelsey E.; Hodges, Kip V.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Evans, Cynthia A.; Graff, Trevor G.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Bleacher, Jacob E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Graff, Trevor G.] Jacobs Engn Grp Inc, Houston, TX 77058 USA. [Young, Kelsey E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Young, Kelsey E.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. RP Young, KE (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.; Young, KE (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.; Young, KE (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. EM Kelsey.E.Young@nasa.gov RI Bleacher, Jacob/D-1051-2012 OI Bleacher, Jacob/0000-0002-8499-4828 FU GSRP (Graduate Student Researcher's Program) [NNX10AK72H] FX The authors would like to thank Dr. Chris Condit for his thoughtful review. The majority of this work was completed under the GSRP (Graduate Student Researcher's Program) Grant Number NNX10AK72H as well as under the RIS4E SSERVI team (Remote, In Situ and Synchrotron Studies for Science and Exploration Solar System Exploration Research Virtual Institute), led by Dr. Timothy Glotch at Stony Brook University. The authors of this paper would also like to acknowledge Dr. Richard Morris. Without his permission for access to the sample standards, this work would not have been possible. In addition, we thank Dr. Stanley Mertzman for his thoughtful discussions about calibrating against laboratory data. We would also like to thank Dr. Carlton Allen and Andrea Mosie for their assistance in both obtaining access to and working with the lunar samples at NASA Johnson Space Center. Finally, we thank Cameron Mercer for his figure organization insights. This is SSERVI publication number SSERVI-2016-061. NR 45 TC 1 Z9 1 U1 21 U2 21 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0883-2927 J9 APPL GEOCHEM JI Appl. Geochem. PD SEP PY 2016 VL 72 BP 77 EP 87 DI 10.1016/j.apgeochem.2016.07.003 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DW3DI UT WOS:000383521900008 ER PT J AU Chirayath, V Earle, SA AF Chirayath, Ved Earle, Sylvia A. TI Drones that see through waves - preliminary results from airborne fluid lensing for centimetre-scale aquatic conservation SO AQUATIC CONSERVATION-MARINE AND FRESHWATER ECOSYSTEMS LA English DT Article; Proceedings Paper CT 6th IUCN World Parks Congress CY NOV, 2014 CL Sydney, AUSTRALIA SP IUCN DE fluid lensing; airborne remote sensing; coastal bathymetry; coral reef; stromatolite; American Samoa; Shark Bay AB 1. The use of fluid lensing technology on unmanned aerial vehicles (UAVs, or drones) is presented as a novel means for 3D imaging of aquatic ecosystems from above the water's surface at the centimetre scale. Preliminary results are presented from airborne fluid lensing campaigns conducted over the coral reefs of Ofu Island, American Samoa (2013) and the stromatolite reefs of Shark Bay, Western Australia (2014), covering a combined area of 15 km(2). These reef ecosystems were revealed with centimetre-scale 2D resolution, and an accompanying 3D bathymetry model was derived using fluid lensing, Structure from Motion and UAV position data. Data products were validated from in situ survey methods including underwater calibration targets, depth measurements and millimetre-scale high-dynamic-range gigapixel photogrammetry. 2. Fluid lensing is an experimental technology that uses water-transmitting wavelengths to passively image underwater objects at high-resolution by exploiting time-varying optical lensing events caused by surface waves. Fluid lensing data are captured from low-altitude, cost-effective electric UAVs to achieve multispectral imagery and bathymetry models at the centimetre scale over regional areas. As a passive system, fluid lensing is presently limited by signal-to-noise ratio and water column inherent optical properties to similar to 10 m depth over visible wavelengths in clear waters. 3. The datasets derived from fluid lensing present the first centimetre-scale images of a reef acquired from above the ocean surface, without wave distortion. The 3D multispectral data distinguish coral, fish and invertebrates in American Samoa, and reveal previously undocumented, morphologically distinct, stromatolite structures in Shark Bay. These findings suggest fluid lensing and multirotor electric drones represent a promising advance in the remote sensing of aquatic environments at the centimetre scale, or 'reef scale' relevant to the conservation of reef ecosystems. Pending further development and validation of fluid lensing methods, these technologies present a solution for large-scale 3D surveys of shallow aquatic habitats with centimetre-scale spatial resolution and hourly temporal sampling. Copyright (C) 2016 John Wiley & Sons, Ltd. C1 [Chirayath, Ved] NASA, Ames Res Ctr, Lab Adv Sensing, Div Earth Sci, Moffett Field, CA 94035 USA. RP Chirayath, V (reprint author), NASA, Ames Res Ctr, Mailstop 232-22, Moffett Field, CA 94305 USA. EM ved.chirayath@nasa.gov NR 15 TC 1 Z9 1 U1 17 U2 17 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1052-7613 EI 1099-0755 J9 AQUAT CONSERV JI Aquat. Conserv.-Mar. Freshw. Ecosyst. PD SEP PY 2016 VL 26 SU 2 BP 237 EP 250 DI 10.1002/aqc.2654 PG 14 WC Environmental Sciences; Marine & Freshwater Biology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA DW5FL UT WOS:000383668500017 ER PT J AU McCaig, HC Stockton, A Crilly, C Chung, S Kanik, I Lin, Y Zhong, F AF McCaig, Heather C. Stockton, Amanda Crilly, Candice Chung, Shirley Kanik, Isik Lin, Ying Zhong, Fang TI Supercritical Carbon Dioxide Extraction of Coronene in the Presence of Perchlorate for In Situ Chemical Analysis of Martian Regolith SO ASTROBIOLOGY LA English DT Article DE Biomarkers; Carbon dioxide; In situ measurement; Mars; Search for Mars' organics ID POLYCYCLIC AROMATIC-HYDROCARBONS; MASS-SPECTROMETRY; ORGANIC-MATTER; SUBCRITICAL WATER; METEORITE ALH84001; FLUID EXTRACTION; GALE CRATER; MARS; MOLECULES; ORIGIN AB The analysis of the organic compounds present in the martian regolith is essential for understanding the history and habitability of Mars, as well as studying the signs of possible extant or extinct life. To date, pyrolysis, the only technique that has been used to extract organic compounds from the martian regolith, has not enabled the detection of unaltered native martian organics. The elevated temperatures required for pyrolysis extraction can cause native martian organics to react with perchlorate salts in the regolith and possibly result in the chlorohydrocarbons that have been detected by in situ instruments. Supercritical carbon dioxide (SCCO2) extraction is an alternative to pyrolysis that may be capable of delivering unaltered native organic species to an in situ detector. In this study, we report the SCCO2 extraction of unaltered coronene, a representative polycyclic aromatic hydrocarbon (PAH), from martian regolith simulants, in the presence of 3 parts per thousand (ppth) sodium perchlorate. PAHs are a class of nonpolar molecules of astrobiological interest and are delivered to the martian surface by meteoritic infall. We also determined that the extraction efficiency of coronene was unaffected by the presence of perchlorate on the regolith simulant, and that no sodium perchlorate was extracted by SCCO2. This indicates that SCCO2 extraction can provide de-salted samples that could be directly delivered to a variety of in situ detectors. SCCO2 was also used to extract trace native fluorescent organic compounds from the martian regolith simulant JSC Mars-1, providing further evidence that SCCO2 extraction may provide an alternative to pyrolysis to enable the delivery of unaltered native organic compounds to an in situ detector on a future Mars rover. C1 [McCaig, Heather C.; Crilly, Candice; Chung, Shirley; Kanik, Isik; Lin, Ying; Zhong, Fang] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Stockton, Amanda] Georgia Inst Technol, Atlanta, GA 30332 USA. [Crilly, Candice] Occidental Coll, Los Angeles, CA 90041 USA. RP Zhong, F (reprint author), CALTECH, Jet Prop Lab, M-S 70-24,4800 Oak Grove Dr, Pasadena, CA 91109 USA.; Lin, Y (reprint author), CALTECH, Jet Prop Lab, M-S 321-550,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ying.lin@jpl.nasa.gov; fang.zhong@jpl.nasa.gov FU National Aeronautics and Space Administration (NASA); NASA Astrobiology Science and Technology Instrument Development program FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA) and was supported by the NASA Astrobiology Science and Technology Instrument Development program. The JPL author's copyright for this paper is held by the California Institute of Technology. Government sponsorship is acknowledged. NR 48 TC 0 Z9 0 U1 11 U2 11 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 SEP PY 2016 VL 16 IS 9 BP 703 EP 714 DI 10.1089/ast.2015.1443 PG 12 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA DW9IK UT WOS:000383971100004 PM 27623199 ER PT J AU Misra, AK Acosta-Maeda, TE Sharma, SK Mckay, CP Gasda, PJ Taylor, GJ Lucey, PG Flynn, L Abedin, MN Clegg, SM Wiens, R AF Misra, Anupam K. Acosta-Maeda, Tayro E. Sharma, Shiv K. Mckay, Christopher P. Gasda, Patrick J. Taylor, G. Jeffrey Lucey, Paul G. Flynn, Luke Abedin, M. Nurul Clegg, Samuel M. Wiens, Roger TI "Standoff Biofinder" for Fast, Noncontact, Nondestructive, Large-Area Detection of Biological Materials for Planetary Exploration SO ASTROBIOLOGY LA English DT Article DE Standoff Biofinder; Luminescence; Time-resolved fluorescence; Biofluorescence; Planetary exploration; Planetary protection; Noncontact nondestructive biodetection ID LASER-INDUCED FLUORESCENCE; TIME-RESOLVED FLUORESCENCE; CHEMCAM INSTRUMENT SUITE; REMOTE RAMAN; ULTRAVIOLET FLUORESCENCE; SPECTROSCOPIC DETECTION; ROOM-TEMPERATURE; NUCLEIC-ACIDS; STEADY-STATE; EXCITATION AB We developed a prototype instrument called the Standoff Biofinder, which can quickly locate biological material in a 500 cm(2) area from a 2 m standoff distance with a detection time of 0.1 s. All biogenic materials give strong fluorescence signals when excited with UV and visible lasers. In addition, the luminescence decay time of biogenic compounds is much shorter (<100 ns) than the micro-to millisecond decay time of transition metal ions and rare-earth ions in minerals and rocks. The Standoff Biofinder takes advantage of the short lifetime of biofluorescent materials to obtain real-time fluorescence images that show the locations of biological materials among luminescent minerals in a geological context. The Standoff Biofinder instrument will be useful for locating biological material during future NASA rover, lander, and crewed missions. Additionally, the instrument can be used for nondestructive detection of biological materials in unique samples, such as those obtained by sample return missions from the outer planets and asteroids. The Standoff Biofinder also has the capacity to detect microbes and bacteria on space instruments for planetary protection purposes. C1 [Misra, Anupam K.; Acosta-Maeda, Tayro E.; Sharma, Shiv K.; Taylor, G. Jeffrey; Lucey, Paul G.; Flynn, Luke] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Mckay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gasda, Patrick J.; Clegg, Samuel M.; Wiens, Roger] Los Alamos Natl Lab, Los Alamos, NM USA. [Abedin, M. Nurul] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Misra, AK (reprint author), Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Sch Ocean & Earth Sci & Technol, 1680 East West Rd,POST 602, Honolulu, HI 96822 USA. EM anupam@hawaii.edu OI Gasda, Patrick/0000-0003-0895-1153; Clegg, Sam/0000-0002-0338-0948 FU NASA EPSCoR grant [NNX13AM98A] FX This work has been supported by NASA EPSCoR grant NNX13AM98A. The authors would like to thank Nancy Hulbirt and May Izumi for their valuable help with figures and editing. Authors would like to thank the reviewers for their valuable time in providing critical review and constructive comments, which greatly helped improve the manuscript. NR 83 TC 0 Z9 0 U1 6 U2 6 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 SEP PY 2016 VL 16 IS 9 BP 715 EP 729 DI 10.1089/ast.2015.1400 PG 15 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA DW9IK UT WOS:000383971100005 PM 27623200 ER PT J AU Bannister, MT Kavelaars, JJ Petit, JM Gladman, BJ Gwyn, SDJ Chen, YT Volk, K Alexandersen, M Benecchi, SD Delsanti, A Fraser, WC Granvik, M Grundy, WM Guilbert-Lepoutre, A Hestroffer, D Ip, WH Jakubik, M Jones, RL Kaib, N Kavelaars, CF Lacerda, P Lawler, S Lehner, MJ Lin, HW Lister, T Lykawka, PS Monty, S Marsset, M Murray-Clay, R Noll, KS Parker, A Pike, RE Rousselot, P Rusk, D Schwamb, ME Shankman, C Sicardy, B Vernazza, P Wang, SY AF Bannister, Michele T. Kavelaars, J. J. Petit, Jean-Marc Gladman, Brett J. Gwyn, Stephen D. J. Chen, Ying-Tung Volk, Kathryn Alexandersen, Mike Benecchi, Susan D. Delsanti, Audrey Fraser, Wesley C. Granvik, Mikael Grundy, Will M. Guilbert-Lepoutre, Aurelie Hestroffer, Daniel Ip, Wing-Huen Jakubik, Marian Jones, R. Lynne Kaib, Nathan Kavelaars, Catherine F. Lacerda, Pedro Lawler, Samantha Lehner, Matthew J. Lin, Hsing Wen Lister, Tim Lykawka, Patryk Sofia Monty, Stephanie Marsset, Michael Murray-Clay, Ruth Noll, Keith S. Parker, Alex Pike, Rosemary E. Rousselot, Philippe Rusk, David Schwamb, Megan E. Shankman, Cory Sicardy, Bruno Vernazza, Pierre Wang, Shiang-Yu TI THE OUTER SOLAR SYSTEM ORIGINS SURVEY. I. DESIGN AND FIRST-QUARTER DISCOVERIES SO ASTRONOMICAL JOURNAL LA English DT Article DE Kuiper Belt: general; surveys ID KUIPER-BELT OBJECTS; ABSOLUTE MAGNITUDE DISTRIBUTION; TRANS-NEPTUNIAN POPULATIONS; SIZE DISTRIBUTION; DATA RELEASE; DYNAMICAL CLASSIFICATION; ORBITAL STRUCTURE; SCATTERED DISK; PLANE; SEARCH AB We report the discovery, tracking, and detection circumstances for 85 trans-Neptunian objects (TNOs) from the first 42 deg(2) of the Outer Solar System Origins Survey. This ongoing r-band solar system survey uses the 0.9 deg(2) field of view MegaPrime camera on the 3.6m Canada-France-Hawaii Telescope. Our orbital elements for these TNOs are precise to a fractional semimajor axis uncertainty <0.1%. We achieve this precision in just two oppositions, as compared to the normal three to five oppositions, via a dense observing cadence and innovative astrometric technique. These discoveries are free of ephemeris bias, a first for large trans-Neptunian surveys. We also provide the necessary information to enable models of TNO orbital distributions to be tested against our TNO sample. We confirm the existence of a cold "kernel" of objects within the main cold classical Kuiper Belt and infer the existence of an extension of the "stirred" cold classical Kuiper Belt to at least several au beyond the 2:1 mean motion resonance with Neptune. We find that the population model of Petit et al. remains a plausible representation of the Kuiper Belt. The full survey, to be completed in 2017, will provide an exquisitely characterized sample of important resonant TNO populations, ideal for testing models of giant planet migration during the early history of the solar system. C1 [Bannister, Michele T.; Kavelaars, J. J.; Kavelaars, Catherine F.; Monty, Stephanie; Pike, Rosemary E.; Rusk, David; Shankman, Cory] Univ Victoria, Dept Phys & Astron, Elliott Bldg,3800 Finnerty Rd, Victoria, BC V8P 5C2, Canada. [Bannister, Michele T.; Kavelaars, J. J.; Gwyn, Stephen D. J.; Lawler, Samantha] Natl Res Council Canada, NRC Herzberg Astron & Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada. [Petit, Jean-Marc; Rousselot, Philippe] Univ Bourgogne Franche Comte, CNRS, Inst UTINAM UMR6213, OSU Theta, F-25000 Besancon, France. [Gladman, Brett J.; Alexandersen, Mike] Univ British Columbia, Dept Phys & Astron, Vancouver, BC, Canada. [Chen, Ying-Tung; Alexandersen, Mike; Lehner, Matthew J.; Schwamb, Megan E.; Wang, Shiang-Yu] Acad Sinica, Inst Astron & Astrophys, 1 Roosevelt Rd,Sec 4, Taipei 10617, Taiwan. [Chen, Ying-Tung; Alexandersen, Mike; Lehner, Matthew J.; Schwamb, Megan E.; Wang, Shiang-Yu] Natl Taiwan Univ, AS NTU11F, 1 Roosevelt Rd,Sec 4, Taipei 10617, Taiwan. [Volk, Kathryn] Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, 1629 Univ Blvd, Tucson, AZ 85721 USA. [Benecchi, Susan D.] Planetary Sci Inst, 1700 East Ft Lowell,Suite 106, Tucson, AZ 85719 USA. [Delsanti, Audrey] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Fraser, Wesley C.; Lacerda, Pedro] Queens Univ Belfast, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Granvik, Mikael] Univ Helsinki, Dept Phys, POB 64, FI-00014 Helsinki, Finland. [Granvik, Mikael] Finnish Geospatial Res Inst, POB 15, FI-02430 Masala, Finland. [Grundy, Will M.] Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA. [Hestroffer, Daniel] Univ Lille 1, Univ Paris 06, CNRS, IMCCE,Observ Paris,PSL Res Univ, F-75014 Paris, France. [Ip, Wing-Huen; Lin, Hsing Wen] Natl Cent Univ, Inst Astron, Taoyuan, Taiwan. [Ip, Wing-Huen] Macau Univ Sci & Technol, Space Sci Inst, Macau, Peoples R China. [Jakubik, Marian] Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960, Slovakia. [Jones, R. Lynne] Univ Washington, Washington, DC USA. [Kaib, Nathan] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Lehner, Matthew J.] Univ Penn, Dept Phys & Astron, 209 S 33rd St, Philadelphia, PA 19104 USA. Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Lehner, Matthew J.; Lister, Tim] Las Cumbres Observ Global Telescope Network Inc, 6740 Cortona Dr Suite 102, Goleta, CA 93117 USA. [Lykawka, Patryk Sofia] Kinki Univ, Sch Interdisciplinary Social & Human Sci, Astron Grp, Higashiosaka, Osaka 577, Japan. [Marsset, Michael] ESO, Alonso de Cordova 3107,1900 Casilla Vitacura, Santiago, Chile. [Murray-Clay, Ruth] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Noll, Keith S.] NASA, Goddard Space Flight Ctr, Code 693, Greenbelt, MD 20771 USA. [Parker, Alex] Southwest Res Inst, Boulder, CO USA. [Sicardy, Bruno] Univ Paris 06, Univ Paris Diderot, CNRS UMR 8109, LESIA,Observ Paris, 5 Pl Jules Janssen, F-92195 Meudon, France. RP Bannister, MT (reprint author), Univ Victoria, Dept Phys & Astron, Elliott Bldg,3800 Finnerty Rd, Victoria, BC V8P 5C2, Canada. EM micheleb@uvic.ca OI Volk, Kathryn/0000-0001-8736-236X; Bannister, Michele/0000-0003-3257-4490; Sofia Lykawka, Patryk/0000-0003-0926-2448 FU National Research Council of Canada; National Science and Engineering Research Council of Canada; Academia Sinica Postdoctoral Fellowship FX This research was supported by funding from the National Research Council of Canada and the National Science and Engineering Research Council of Canada. This project could not have been a success without the dedicated staff of the Canada France Hawaii telescope. The authors recognize and acknowledge the sacred nature of Maunakea, and appreciate the opportunity to observe from the mountain. This research has made use of NASA's Astrophysics Data System, GNU parallel (Tange 2011), and many Python packages, particularly astropy (The Astropy Collaboration et al. 2013), matplotlib (Hunter 2007) and SciPy (Jones et al. 2001); we thank their contributors for their open-source efforts. MES is supported in part by an Academia Sinica Postdoctoral Fellowship. Based on observations obtained with MegaPrime/MegaCam, a joint project of the Canada France Hawaii Telescope (CFHT) and CEA/DAPNIA, at CFHT which is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l'universe of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data produced and hosted at the Canadian Astronomy Data Centre. NR 70 TC 6 Z9 6 U1 2 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 SEP PY 2016 VL 152 IS 3 AR 70 DI 10.3847/0004-6256/152/3/70 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW7AV UT WOS:000383804300018 ER PT J AU McCandliss, SR Feldman, PD Weaver, H Fleming, B Redwine, K Li, MJ Kutyrev, A Moseley, SH AF McCandliss, Stephan R. Feldman, Paul D. Weaver, Harold Fleming, Brian Redwine, Keith Li, Mary J. Kutyrev, Alexander Moseley, S. Harvey TI FAR-ULTRAVIOLET OBSERVATIONS OF COMET C/2012 S1 (ISON) FROM FORTIS SO ASTRONOMICAL JOURNAL LA English DT Article DE general; comets: individual (C/2012 S1 (ISON), C/2001 Q4 (NEAT), C/2004 Q2 (MACHHOLZ)); molecular processes; Oort Cloud ID SPECTROSCOPY; EVOLUTION; HYDROGEN AB We have used the unique far-UV imaging capability offered by a sounding-rocket-borne instrument to acquire observations of C/2012 S1 (ISON) when its angular separation with respect to the Sun was 26.degrees 3 on 2013 November 20.49. At the time of observation, the comet's heliocentric distance and velocity relative to the Sun were r(h) = 0.43 au and (r) over dot(h) = -62.7 km s(-1). Images dominated by C I lambda 1657 and H I lambda 1216 were acquired over a 10(6) x 10(6) km(2) region. The water production rate implied by the Ly alpha observations is constrained to be Q(H2O)approximate to 8 x 10(29) s(-1) while the neutral carbon production rate was Q(C) approximate to 4 x 10(28) s(-1). The radial profile of C I was consistent with it being a dissociation product of a parent molecule with a lifetime tau similar to 5 x 10(4) s, favoring a parent other than CO. We constrain the Q(CO) production rate to 5(-7.5)(+1.5) x 10(28) s(-1) with 1 sigma errors derived from photon statistics. The upper limit on the Q(CO)/Q(H2O) is less than or similar to 6%. C1 [McCandliss, Stephan R.; Feldman, Paul D.; Redwine, Keith] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Weaver, Harold] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Fleming, Brian] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Li, Mary J.; Kutyrev, Alexander; Moseley, S. Harvey] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP McCandliss, SR (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. EM stephan@pha.jhu.edu OI Feldman, Paul/0000-0002-9318-259X FU Johns Hopkins University through NASA [NNX11AG54G, NNX14A178G] FX The authors would like to acknowledge the sacrifices made by the personnel associated with the NASA Sounding Rocket Program Office, their Contractors, the Navy Launcher Team, and the Army Range Control at White Sands Missile Range, all of whom showed exemplary dedication in carrying out this time critical mission. We would also like to acknowledge the innumerable, essential, and critical contributions of our JHU project engineer, Russell Pelton, in providing support to this mission. Funding for this work was provided to the Johns Hopkins University through NASA sounding rocket grants No. NNX11AG54G and NNX14A178G. NR 28 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD SEP PY 2016 VL 152 IS 3 AR 65 DI 10.3847/0004-6256/152/3/65 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW7AV UT WOS:000383804300013 ER PT J AU Nugent, CR Mainzer, A Bauer, J Cutri, RM Kramer, EA Grav, T Masiero, J Sonnett, S Wright, EL AF Nugent, C. R. Mainzer, A. Bauer, J. Cutri, R. M. Kramer, E. A. Grav, T. Masiero, J. Sonnett, S. Wright, E. L. TI NEOWISE REACTIVATION MISSION YEAR TWO: ASTEROID DIAMETERS AND ALBEDOS SO ASTRONOMICAL JOURNAL LA English DT Article DE minor planets, asteroids: general; surveys ID MAIN-BELT ASTEROIDS; NEAR-EARTH OBJECTS; THERMAL-MODEL CALIBRATION; INFRARED-SURVEY-EXPLORER; WISE/NEOWISE OBSERVATIONS; ABSOLUTE MAGNITUDES; POPULATION; PERFORMANCE; FAMILIES; IDENTIFICATION AB The Near-Earth Object Wide-Field Infrared Survey Explorer (NEOWISE) mission continues to detect, track, and characterize minor planets. We present diameters and albedos calculated from observations taken during the second year since the spacecraft was reactivated in late 2013. These include 207 near-Earth asteroids (NEAs) and 8885 other asteroids. Of the NEAs, 84% NEAs did not have previously measured diameters and albedos by the NEOWISE mission. Comparison of sizes and albedos calculated from NEOWISE measurements with those measured by occultations, spacecraft, and radar-derived shapes shows accuracy consistent with previous NEOWISE publications. Diameters and albedos fall within +/-similar to 20% and +/-similar to 40%, 1-sigma, respectively, of those measured by these alternate techniques. NEOWISE continues to preferentially discover near-Earth objects which are large (>100 m), and have low albedos. C1 [Nugent, C. R.; Cutri, R. M.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Mainzer, A.; Bauer, J.; Kramer, E. A.; Masiero, J.; Sonnett, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Grav, T.] Planetary Sci Inst, Tucson, AZ USA. [Wright, E. L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. RP Nugent, CR (reprint author), CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. EM cnugent@ipac.caltech.edu OI Cutri, Roc/0000-0002-0077-2305 FU NASA; Planetary Science Division of NASA; JPL Office of the CIO; U.S. Department of Energy; U.S. National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; Collaborating Institutions in the Dark Energy Survey; Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) [GS-2015A-LP-3, GS-2015B-LP-3] FX This publication makes use of data products from the Wide field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and JPL/California Institute of Technology, funded by NASA. This publication also makes use of data products from NEOWISE, which is a project of the JPL/California Institute of Technology, funded by the Planetary Science Division of NASA. The JPL High Performance Computing Facility used for our simulations is supported by the JPL Office of the CIO.; This project used data obtained with the Dark Energy Camera (DECam), which was constructed by the Dark Energy Survey (DES) collaboration. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d' Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, the Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University.; This publication makes use of observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina), and Ministerio da Ciencia, Tecnologia e Inovacao (Brazil). Observing Program IDs: GS-2015A-LP-3, GS-2015B-LP-3. NR 55 TC 2 Z9 2 U1 6 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD SEP PY 2016 VL 152 IS 3 AR 63 DI 10.3847/0004-6256/152/3/63 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW7AV UT WOS:000383804300011 ER PT J AU Schneider, G Grady, CA Stark, CC Gaspar, A Carson, J Debes, JH Henning, T Hines, DC Jang-Condell, H Kuchner, MJ Perrin, M Rodigas, TJ Tamura, M Wisniewski, JP AF Schneider, Glenn Grady, Carol A. Stark, Christopher C. Gaspar, Andras Carson, Joseph Debes, John H. Henning, Thomas Hines, Dean C. Jang-Condell, Hannah Kuchner, Marc J. Perrin, Marshall Rodigas, Timothy J. Tamura, Motohide Wisniewski, John P. TI DEEP HST/STIS VISIBLE-LIGHT IMAGING OF DEBRIS SYSTEMS AROUND SOLAR ANALOG HOSTS SO ASTRONOMICAL JOURNAL LA English DT Article DE methods: observational; planet-disk interactions; stars: individual (HD 207129, HD 202628, HD 202917); stars: solar-type ID MAIN-SEQUENCE STARS; INTERSTELLAR-MEDIUM; HD 207129; SPACE-TELESCOPE; MOVING GROUP; DISK; PLANETS; RING; DUST; AGE AB We present new Hubble Space Telescope observations of three a priori known starlight-scattering circumstellar debris systems (CDSs) viewed at intermediate inclinations around nearby close-solar analog stars: HD 207129, HD 202628, and HD 202917. Each of these CDSs possesses ring-like components that are more massive analogs of our solar system's Edgeworth-Kuiper Belt. These systems were chosen for follow-up observations to provide imaging with higher fidelity and better sensitivity for the sparse sample of solar-analog CDSs that range over two decades in systemic ages, with HD 202628 and HD 207129 (both similar to 2.3 Gyr) currently the oldest CDSs imaged in visible or near-IR light. These deep (10-14 ks) observations, made with six-roll point-spread-function template visible-light coronagraphy. using the Space Telescope Imaging Spectrograph, were designed to better reveal their angularly large debris rings of diffuse/low surface brightness, and for all targets probe their exo-ring environments for starlight-scattering materials that present observational challenges for current ground-based facilities and instruments. Contemporaneously also observing with a narrower occulter position, these observations additionally probe the CDS endo-ring environments that are seen to be relatively devoid of scatterers. We discuss the morphological, geometrical, and photometric properties of these CDSs also in the context of other CDSs hosted by FGK stars that we have previously imaged as a homogeneously observed ensemble. From this combined sample we report a general decay in quiescent-disk F-disk/F-star optical brightness similar to t(-0.8), similar to what is seen at thermal IR wavelengths, and CDSs with a significant diversity in scattering phase asymmetries, and spatial distributions of their starlight-scattering grains. C1 [Schneider, Glenn; Gaspar, Andras] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. [Schneider, Glenn; Gaspar, Andras] Univ Arizona, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 USA. [Grady, Carol A.] Eureka Sci, 2452 Delmer,Suite 100, Oakland, CA 96002 USA. [Stark, Christopher C.; Kuchner, Marc J.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA. [Carson, Joseph] Coll Charleston, Dept Phys & Astron, 66 George St, Charleston, SC 29424 USA. [Debes, John H.; Hines, Dean C.; Perrin, Marshall] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Henning, Thomas] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Jang-Condell, Hannah] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Rodigas, Timothy J.] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Branch Rd NW, Washington, DC 20015 USA. [Tamura, Motohide] Univ Tokyo, Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Wisniewski, John P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, 440 West Brooks St, Norman, OK 73019 USA. RP Schneider, G (reprint author), Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.; Schneider, G (reprint author), Univ Arizona, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 USA. EM gschneider@as.arizona.edu OI Gaspar, Andras/0000-0001-8612-3236 FU Association of Universities for Research in Astronomy, Inc., under NASA [NAS 5-26555]; NASA through STScI [13786]; South Carolina Space Grant Consortium; [12228] FX Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programs #13786 and 12228. Support for program #13786 was provided by NASA through a grant from STScI. J. Carson acknowledges support from the South Carolina Space Grant Consortium. NR 42 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD SEP PY 2016 VL 152 IS 3 AR 64 DI 10.3847/0004-6256/152/3/64 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW7AV UT WOS:000383804300012 ER PT J AU Hinkel, NR Young, PA Pagano, MD Desch, SJ Anbar, AD Adibekyan, V Blanco-Cuaresma, S Carlberg, JK Mena, ED Liu, F Nordlander, T Sousa, SG Korn, A Gruyters, P Heiter, U Jofre, P Santos, NC Soubiran, C AF Hinkel, Natalie R. Young, Patrick A. Pagano, Michael D. Desch, Steven J. Anbar, Ariel D. Adibekyan, Vardan Blanco-Cuaresma, Sergi Carlberg, Joleen K. Mena, Elisa Delgado Liu, Fan Nordlander, Thomas Sousa, Sergio G. Korn, Andreas Gruyters, Pieter Heiter, Ulrike Jofre, Paula Santos, Nuno C. Soubiran, Caroline TI A COMPARISON OF STELLAR ELEMENTAL ABUNDANCE TECHNIQUES AND MEASUREMENTS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE stars: abundances; stars: individual (HD 361, HD 10700, HD 121504, HD 202206); techniques: spectroscopic ID METAL-POOR STARS; PLANET-HOST STARS; GENEVA-COPENHAGEN SURVEY; GALACTIC CHEMICAL EVOLUTION; NEUTRAL HYDROGEN COLLISIONS; I OSCILLATOR-STRENGTHS; SOLAR-TYPE STARS; WAY THICK DISK; DWARF STARS; OXYGEN ABUNDANCES AB Stellar elemental abundances are important for understanding the fundamental properties of a star or stellar group, such as age and evolutionary history, as well as the composition of an orbiting planet. However, as abundance measurement techniques have progressed, there has been little standardization between individual methods and their comparisons. As a result, different stellar abundance procedures determine measurements that vary beyond the quoted error for the same elements within the same stars. The purpose of this paper is to better understand the systematic variations between methods and offer recommendations for producing more accurate results in the future. We invited a number of participants from around the world (Australia, Portugal, Sweden, Switzerland, and the United States) to calculate 10 element abundances (C, O, Na, Mg, Al, Si, Fe, Ni, Ba, and Eu) using the same stellar spectra for four stars (HD 361, HD 10700, HD 121504, and HD 202206). Each group produced measurements for each star using (1) their own autonomous techniques, (2) standardized stellar parameters, (3) a standardized line list, and (4) both standardized parameters and a line list. We present the resulting stellar parameters, absolute abundances, and a metric of data similarity that quantifies the homogeneity of the data. We conclude that standardization of some kind, particularly stellar parameters, improves the consistency between methods. However, because results did not converge as more free parameters were standardized, it is clear there are inherent issues within the techniques that need to be reconciled. Therefore, we encourage more conversation and transparency within the community such that stellar abundance determinations can be reproducible as well as accurate and precise. C1 [Hinkel, Natalie R.; Young, Patrick A.; Pagano, Michael D.; Desch, Steven J.; Anbar, Ariel D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Adibekyan, Vardan; Mena, Elisa Delgado; Sousa, Sergio G.; Santos, Nuno C.] Univ Porto, Inst Astrofis & Ciencias Espaco, CAUP, Rua Estrelas, P-4150762 Oporto, Portugal. [Blanco-Cuaresma, Sergi] Univ Geneva, Observ Geneve, CH-1290 Versoix, Switzerland. [Carlberg, Joleen K.] NASA, Goddard Space Flight Ctr, Code 667, Greenbelt, MD 20771 USA. [Carlberg, Joleen K.] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. [Liu, Fan] Australian Natl Univ, Res Sch Astron & Astrophys, Cotter Rd, Weston, ACT 2611, Australia. [Nordlander, Thomas; Korn, Andreas; Gruyters, Pieter; Heiter, Ulrike] Uppsala Univ, Dept Phys & Astron, Box 516, S-75120 Uppsala, Sweden. [Gruyters, Pieter] Lund Observ, Dept Astron & Theoret Phys, Box 43, S-22100 Lund, Sweden. [Jofre, Paula] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Santos, Nuno C.] Univ Porto, Fac Ciencias, Dept Fis & Astron, Rua Campo Alegre, P-4169007 Oporto, Portugal. [Soubiran, Caroline] Univ Bordeaux, CNRS, LAB, UMR 5804, F-33270 Floirac, France. RP Hinkel, NR (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. EM natalie.hinkel@gmail.com FU NASA's Science Mission Directorate; Fundacao para a Ciencia e Tecnologia (FCT, Portugal) [SFRH/BPD/76606/2011, SFRH/BPD/70574/2010]; Swedish National Space Board (SNSB); FCT [IF/00169/2012, IF/00028/2014, PTDC/FIS-AST/7073/2014 (POCI-01-0145-FEDER-007672), PTDC/FIS-AST/1526/2014]; POPH/FSE (EC) by FEDER funding through the program "Programa Operacional de Factores de Competitividade" FX The authors would like to thank Paul Butler for providing the original stellar spectra in addition to Eric Mamajek for his help determining accurate stellar types for our sample. They would also like to thank the anonymous referee for support and guidance, which has greatly improved the manuscript. NRH would like to thank CHW3. The ASU team (NRH, PAY, MDP, SJD, and ADA) acknowledge that the results reported herein benefited from collaborations and/or information exchange within NASA's Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA's Science Mission Directorate. EDM and VA acknowledge the support from the Fundacao para a Ciencia e Tecnologia (FCT, Portugal) in the form of the grants SFRH/BPD/76606/2011 and SFRH/BPD/70574/2010, respectively. JKC acknowledges partial support from an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Universities Space Research Association through a contract with NASA. TN, AK, and UH acknowledge support by the Swedish National Space Board (SNSB). NCS and SGS acknowledge the support from FCT through Investigador FCT contracts of reference IF/00169/2012 and IF/00028/2014, respectively, and POPH/FSE (EC) by FEDER funding through the program "Programa Operacional de Factores de Competitividade." The Porto group also acknowledges the support from FCT in the form of grant reference PTDC/FIS-AST/7073/2014 (POCI-01-0145-FEDER-007672) and project PTDC/FIS-AST/1526/2014. This research has made use of the SIMBAD database and VizieR catalog access tools operated at CDS, Strasbourg, France, as well as the Exoplanet Orbit Database at exoplanets.org. NR 179 TC 1 Z9 1 U1 3 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2016 VL 226 IS 1 AR 4 DI 10.3847/0067-0049/226/1/4 PG 66 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW9XF UT WOS:000384015400004 ER PT J AU Paganini, L Mumma, MJ AF Paganini, L. Mumma, M. J. TI A SOLAR-PUMPED FLUORESCENCE MODEL FOR LINE-BY-LINE EMISSION INTENSITIES IN THE B-X, A-X, AND X-X BAND SYSTEMS OF (CN)-C-12-N-14 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE astronomical databases: miscellaneous; comets: general; molecular data; molecular processes; comets: individual; C/2014 Q2 (Lovejoy); techniques: spectroscopic ID OH PROMPT EMISSION; CHEMICAL-COMPOSITION; VIOLET SYSTEMS; COMETS; CN; SPECTRUM; CYANOGEN; WATER; EXCITATION; MOLECULES AB We present a new quantitative model for detailed solar-pumped fluorescent emission of the main isotopologue of CN. The derived fluorescence efficiencies permit estimation and interpretation of ro-vibrational infrared line intensities of CN in exospheres exposed to solar (or stellar) radiation. Our g-factors are applicable to astronomical observations of CN extending from infrared to optical wavelengths, and we compare them with previous calculations in the literature. The new model enables extraction of rotational temperature, column abundance, and production rate from astronomical observations of CN in the inner coma of comets. Our model accounts for excitation and de-excitation of rotational levels in the ground vibrational state by collisions, solar excitation to the A(2)Pi(i) and B-2 Sigma(+) electronically excited states followed by cascade to ro-vibrational levels of X-2 Sigma(+), and direct solar infrared pumping of ro-vibrational levels in the X-2 Sigma(+) state. The model uses advanced solar spectra acquired at high spectral resolution at the relevant infrared and optical wavelengths and considers the heliocentric radial velocity of the comet (the Swings effect) when assessing the exciting solar flux for a given transition. We present model predictions for the variation of fluorescence rates with rotational temperature and heliocentric radial velocity. Furthermore, we test our fluorescence model by comparing predicted and measured line-by-line intensities for X-2 Sigma(+) (1-0) in comet C/2014 Q2 (Lovejoy), thereby identifying multiple emission lines observed at IR wavelengths. C1 [Paganini, L.; Mumma, M. J.] NASA, Goddard Ctr Astrobiol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Paganini, L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Paganini, L (reprint author), NASA, Goddard Ctr Astrobiol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Paganini, L (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. FU NASA's Planetary Astronomy Program; Keck PI Data Award FX The authors would like to thank David Schleicher and James S. A. Brooke for interesting insights about this work. We also acknowledge support by NASA's Planetary Astronomy Program (L.P., M.J.M.) and Keck PI Data Award (L.P.), administered by the NASA Exoplanet Science Institute. Data were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. NR 61 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2016 VL 226 IS 1 AR 3 DI 10.3847/0067-0049/226/1/3 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW9XF UT WOS:000384015400003 ER PT J AU Haarig, M Engelmann, R Ansmann, A Veselovskii, I Whiteman, DN Althausen, D AF Haarig, Moritz Engelmann, Ronny Ansmann, Albert Veselovskii, Igor Whiteman, David N. Althausen, Dietrich TI 1064 nm rotational Raman lidar for particle extinction and lidar-ratio profiling: cirrus case study SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID SPECTRAL-RESOLUTION LIDAR; ELASTIC-BACKSCATTER LIDAR; INDIAN AEROSOL PLUME; MULTIWAVELENGTH LIDAR; WATER-VAPOR; SAHARAN DUST; PHYSICAL-PROPERTIES; 6-WAVELENGTH LIDAR; OPTICAL-PROPERTIES; RETRIEVAL AB For the first time, vertical profiles of the 1064 nm particle extinction coefficient obtained from Raman lidar observations at 1058 nm (nitrogen and oxygen rotational Raman backscatter) are presented. We applied the new technique in the framework of test measurements and performed several cirrus observations of particle backscatter and extinction coefficients, and corresponding extinctiont-o-backscatter ratios at the wavelengths of 355, 532, and 1064 nm. The cirrus backscatter coefficients were found to be equal for all three wavelengths keeping the retrieval uncertainties in mind. The multiple-scattering-corrected cirrus extinction coefficients at 355 nm were on average about 20-30% lower than the ones for 532 and 1064 nm. The cirrus-mean extinction-to-backscatter ratio (lidar ratio) was 31 +/- 5 sr (355 nm), 36 +/- 5 sr (532 nm), and 38 +/- 5 sr (1064 nm) in this single study. We further discussed the requirements needed to obtain aerosol extinction profiles in the lower troposphere at 1064 nm with good accuracy (20% relative uncertainty) and appropriate temporal and vertical resolution. C1 [Haarig, Moritz; Engelmann, Ronny; Ansmann, Albert; Althausen, Dietrich] Leibniz Inst Tropospher Res, Leipzig, Germany. [Veselovskii, Igor] Phys Instrumentat Ctr, Moscow, Russia. [Whiteman, David N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Haarig, M (reprint author), Leibniz Inst Tropospher Res, Leipzig, Germany. EM haarig@tropos.de FU Russian Science Foundation [16-17-10241] FX We thank Johannes Buhl for providing Doppler lidar observations of vertical velocity and estimated ice crystal sizes. Modeling of the rotational Raman filter parameters was supported by the Russian Science Foundation (project no. 16-17-10241). NR 63 TC 0 Z9 0 U1 2 U2 2 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 EI 1867-8548 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PD SEP 1 PY 2016 VL 9 IS 9 BP 4269 EP 4278 DI 10.5194/amt-9-4269-2016 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DW8LC UT WOS:000383906300001 ER PT J AU Colman, DR Feyhl-Buska, J Fecteau, KM Xu, HF Shock, EL Boyd, ES AF Colman, Daniel R. Feyhl-Buska, Jayme Fecteau, Kristopher M. Xu, Huifang Shock, Everett L. Boyd, Eric S. TI Ecological differentiation in planktonic and sediment-associated chemotrophic microbial populations in Yellowstone hot springs SO FEMS MICROBIOLOGY ECOLOGY LA English DT Article DE Yellowstone hot springs; chemotroph; thermophiles; archaea; Aquificales; ecological differentiation ID STREAMER BIOFILM COMMUNITIES; NATIONAL-PARK; GEOTHERMAL SPRINGS; RIBOSOMAL-RNA; SP-NOV; HIGH-TEMPERATURE; GLOBAL PATTERNS; GEN. NOV.; DIVERSITY; SULFUR AB Chemosynthetic sediment and planktonic community composition and sizes, aqueous geochemistry and sediment mineralogy were determined in 15 non-photosynthetic hot springs in Yellowstone National Park (YNP). These data were used to evaluate the hypothesis that differences in the availability of dissolved or mineral substrates in the bulk fluids or sediments within springs coincides with ecologically differentiated microbial communities and their populations. Planktonic and sediment-associated communities exhibited differing ecological characteristics including community sizes, evenness and richness. pH and temperature influenced microbial community composition among springs, but within-spring partitioning of taxa into sediment or planktonic communities was widespread, statistically supported (P < 0.05) and could be best explained by the inferred metabolic strategies of the partitioned taxa. Microaerophilic genera of the Aquificales predominated in many of the planktonic communities. In contrast, taxa capable of mineral-based metabolism such as S-o oxidation/reduction or Fe-oxide reduction predominated in sediment communities. These results indicate that ecological differentiation within thermal spring habitats is common across a range of spring geochemistry and is influenced by the availability of dissolved nutrients and minerals that can be used in metabolism.The presence of minerals, such as elemental sulfur, that can support microbial metabolism promotes the ecological differentiation of sediment- and planktonic-associated microbial populations within Yellowstone National Park hot springs.The presence of minerals, such as elemental sulfur, that can support microbial metabolism promotes the ecological differentiation of sediment- and planktonic-associated microbial populations within Yellowstone National Park hot springs. C1 [Colman, Daniel R.; Feyhl-Buska, Jayme; Boyd, Eric S.] Montana State Univ, Dept Microbiol & Immunol, POB 173520, Bozeman, MI 59717 USA. [Fecteau, Kristopher M.; Shock, Everett L.] Arizona State Univ, Dept Chem & Biochem, Tempe, AZ 85287 USA. [Xu, Huifang] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Xu, Huifang; Shock, Everett L.; Boyd, Eric S.] NASA, Astrobiol Inst, Mountain View, CA 94035 USA. [Shock, Everett L.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. RP Boyd, ES (reprint author), Montana State Univ, Dept Microbiol & Immunol, POB 173520, Bozeman, MI 59717 USA. EM eboyd@montana.edu FU National Aeronautics and Space Administration (NASA) Exobiology and Evolutionary Biology [NNX13AI11G]; [EAR- 1529963]; [NNA15BB02A]; [NNA13AA94A] FX This work was supported by a National Aeronautics and Space Administration (NASA) Exobiology and Evolutionary Biology [grant number NNX13AI11G] grant to ESB and a National Science Foundation grant [grant number EAR- 1529963] to ELS. The NASA Astrobiology Institute is supported by grant numbers NNA15BB02A (to ELS and ESB) and NNA13AA94A (to HX and ESB). NR 72 TC 1 Z9 1 U1 8 U2 8 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0168-6496 EI 1574-6941 J9 FEMS MICROBIOL ECOL JI FEMS Microbiol. Ecol. PD SEP PY 2016 VL 92 IS 9 AR fiw137 DI 10.1093/femsec/fiw137 PG 13 WC Microbiology SC Microbiology GA DW8IL UT WOS:000383898400011 ER PT J AU van Vliet, MTH van Beek, LPH Eisner, S Florke, M Wada, Y Bierkens, MFP AF van Vliet, M. T. H. van Beek, L. P. H. Eisner, S. Floerke, M. Wada, Y. Bierkens, M. F. P. TI Multi-model assessment of global hydropower and cooling water discharge potential under climate change SO GLOBAL ENVIRONMENTAL CHANGE-HUMAN AND POLICY DIMENSIONS LA English DT Article DE Water resources; Water temperature; Hydropower; Cooling water; Climate change; Global hydrological models ID PACIFIC-NORTHWEST; POWER-GENERATION; CHANGE IMPACTS; MODEL; ELECTRICITY; VALIDATION; TEMPERATURE; RESOURCES; HYDROLOGY; SCALE AB Worldwide, 98% of total electricity is currently produced by thermoelectric power and hydropower. Climate change is expected to directly impact electricity supply, in terms of both water availability for hydropower generation and cooling water usage for thermoelectric power. Improved understanding of how climate change may impact the availability and temperature of water resources is therefore of major importance. Here we use a multi-model ensemble to show the potential impacts of climate change on global hydropower and cooling water discharge potential. For the first time, combined projections of streamflow and water temperature were produced with three global hydrological models (GHMs) to account for uncertainties in the structure and parametrization of these GHMs in both water availability and water temperature. The GHMs were forced with bias-corrected output of five general circulation models (GCMs) for both the lowest and highest representative concentration pathways (RCP2.6 and RCP8.5). The ensemble projections of streamflow and water temperature were then used to quantify impacts on gross hydropower potential and cooling water discharge capacity of rivers worldwide. We show that global gross hydropower potential is expected to increase between +2.4% (GCM-GHM ensemble mean for RCP 2.6) and +6.3% (RCP 8.5) for the 2080s compared to 1971-2000. The strongest increases in hydropower potential are expected for Central Africa, India, central Asia and the northern high-latitudes, with 18-33% of the world population living in these areas by the 2080s. Global mean cooling water discharge capacity is projected to decrease by 4.5-15% (2080s). The largest reductions are found for the United States, Europe, eastern Asia, and southern parts of South America, Africa and Australia, where strong water temperature increases are projected combined with reductions in mean annual streamflow. These regions are expected to affect 11-14% (for RCP2.6 and the shared socioeconomic pathway (SSP)1, SSP2, SSP4) and 41-51% (RCP8.5-SSP3, SSP5) of the world population by the 2080s. (C) 2016 Elsevier Ltd. All rights reserved. C1 [van Vliet, M. T. H.] Wageningen Univ, Water Syst & Global Change Grp, POB 47, NL-6700 AA Wageningen, Netherlands. [van Vliet, M. T. H.; Wada, Y.] Int Inst Appl Syst Anal IIASA, Schlosspl 1, A-2361 Laxenburg, Austria. [van Beek, L. P. H.; Wada, Y.; Bierkens, M. F. P.] Univ Utrecht, Dept Phys Geog, POB 80115, NL-3508 TC Utrecht, Netherlands. [Eisner, S.; Floerke, M.] Univ Kassel, Ctr Environm Syst Res, Wilhelmshoher Allee 47, D-34109 Kassel, Germany. [Wada, Y.] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. [Wada, Y.] Columbia Univ, Ctr Climate Syst Res, 2880 Broadway, New York, NY 10025 USA. [Bierkens, M. F. P.] Deltares, Soil & Groundwater Syst Unit, POB 80015, NL-3508 TA Utrecht, Netherlands. RP van Vliet, MTH (reprint author), Wageningen Univ, Water Syst & Global Change Grp, POB 47, NL-6700 AA Wageningen, Netherlands. EM michelle.vanvliet@wur.nl RI van Beek, Rens/B-4904-2014 OI van Beek, Rens/0000-0002-4758-108X FU Niels Stensen Fellowship; Veni-grant of NWO Earth and Life Sciences (ALW) [863.14.008] FX The Inter-Sectoral Impact Model Intercomparison Project (ISIMIP) is kindly acknowledged for providing the bias-corrected general circulation model output and gridded population projections for this study. Dr. Michelle van Vliet was supported by a contribution from the Niels Stensen Fellowship and a Veni-grant (project 863.14.008) of NWO Earth and Life Sciences (ALW). NR 58 TC 1 Z9 1 U1 8 U2 8 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0959-3780 EI 1872-9495 J9 GLOBAL ENVIRON CHANG JI Glob. Environ. Change-Human Policy Dimens. PD SEP PY 2016 VL 40 BP 156 EP 170 DI 10.1016/j.gloenvcha.2016.07.007 PG 15 WC Environmental Sciences; Environmental Studies; Geography SC Environmental Sciences & Ecology; Geography GA DV9YD UT WOS:000383297200014 ER PT J AU Holzmann, GJ AF Holzmann, Gerard J. TI Brace Yourself SO IEEE SOFTWARE LA English DT Editorial Material C1 [Holzmann, Gerard J.] Jet Prop Lab, Pasadena, CA 91125 USA. RP Holzmann, GJ (reprint author), Jet Prop Lab, Pasadena, CA 91125 USA. EM gholzmann@acm.org NR 4 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 0740-7459 EI 1937-4194 J9 IEEE SOFTWARE JI IEEE Softw. PD SEP-OCT PY 2016 VL 33 IS 5 BP 34 EP 37 PG 4 WC Computer Science, Software Engineering SC Computer Science GA DV7DI UT WOS:000383095900008 ER PT J AU Zhu, YY Antao, DS Chu, KH Chen, SY Hendricks, TJ Zhang, TJ Wang, EN AF Zhu, Yangying Antao, Dion S. Chu, Kuang-Han Chen, Siyu Hendricks, Terry J. Zhang, Tiejun Wang, Evelyn N. TI Surface Structure Enhanced Microchannel Flow Boiling SO JOURNAL OF HEAT TRANSFER-TRANSACTIONS OF THE ASME LA English DT Article DE microchannel flow boiling; surface microstructures; flow instabilities; critical heat flux ID CRITICAL HEAT-FLUX; PRESSURE-DROP; PIN FIN; MICROPILLAR ARRAYS; LIQUID; PREDICTION; CHANNELS; REGIME; SINK AB We investigated the role of surface microstructures in two-phase microchannels on suppressing flow instabilities and enhancing heat transfer. We designed and fabricated microchannels with well-defined silicon micropillar arrays on the bottom heated microchannel wall to promote capillary flow for thin film evaporation while facilitating nucleation only from the sidewalls. Our experimental results show significantly reduced temperature and pressure drop fluctuation especially at high heat fluxes. A critical heat flux (CHF) of 969 W/cm(2) was achieved with a structured surface, a 57% enhancement compared to a smooth surface. We explain the experimental trends for the CHF enhancement with a liquid wicking model. The results suggest that capillary flow can be maximized to enhance heat transfer via optimizing the microstructure geometry for the development of high performance two-phase microchannel heat sinks. C1 [Zhu, Yangying; Antao, Dion S.; Chu, Kuang-Han; Chen, Siyu; Wang, Evelyn N.] MIT, Dept Mech Engn, Cambridge, MA 02139 USA. [Hendricks, Terry J.] CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Zhang, Tiejun] Masdar Inst Sci & Technol, Dept Mech & Mat Engn, Bldg 1A,POB 54224, Abu Dhabi, U Arab Emirates. RP Wang, EN (reprint author), MIT, Dept Mech Engn, Cambridge, MA 02139 USA. EM yyzhu@mit.edu; dantao@mit.edu; flyjohn@gmail.com; chensiyu@mit.edu; terry.j.hendricks@jpl.nasa.gov; tjzhang@masdar.ac.ae; enwang@mit.edu FU Office of Naval Research (ONR) [N00014-15-1-2483]; Masdar Institute of Science and Technology (Masdar Institute), Abu Dhabi, UAE [02/MI/MI/CP/11/07633/GEN/G/00]; Massachusetts Institute of Technology (MIT), Cambridge, MA [02/MI/MI/CP/11/07633/GEN/G/00]; Battelle Memorial Institute; Air Force Office of Scientific Research (AFOSR); Singapore-MIT Alliance for Research and Technology (SMART) FX This work was partially funded by the Office of Naval Research (ONR) with Dr. Mark Spector as program manager (N00014-15-1-2483), the Cooperative Agreement between the Masdar Institute of Science and Technology (Masdar Institute), Abu Dhabi, UAE and the Massachusetts Institute of Technology (MIT), Cambridge, MA,-Reference 02/MI/MI/CP/11/07633/GEN/G/00, the Battelle Memorial Institute, the Air Force Office of Scientific Research (AFOSR) and the Singapore-MIT Alliance for Research and Technology (SMART). The research was technically supported and encouraged by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The authors would also like to acknowledge the MIT Microsystems Technology Lab for fabrication staff support, help, and use of equipment. NR 49 TC 3 Z9 3 U1 16 U2 16 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 0022-1481 EI 1528-8943 J9 J HEAT TRANS-T ASME JI J. Heat Transf.-Trans. ASME PD SEP PY 2016 VL 138 IS 9 AR 091501 DI 10.1115/1.4033497 PG 13 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA DW6TS UT WOS:000383784700014 ER PT J AU Otto, SE Trefny, CJ Slater, JW AF Otto, Samuel E. Trefny, Charles J. Slater, John W. TI Inward-Turning Streamline-Traced Inlet Design Method Low-Boom Low-Drag Applications SO JOURNAL OF PROPULSION AND POWER LA English DT Article; Proceedings Paper CT AIAA Propulsion and Energy Forum CY JUL 27-29, 2015 CL Orlando, FL SP AIAA ID BUSEMANN-INLET; SPEEDS AB A new design method for inward-turning streamline-traced inlets is presented. Resulting designs are intended for low-supersonic low-drag low-boom applications such as that required for NASA's proposed low-boom flight demonstration aircraft. A critical feature of these designs is the internal cowl lip angle that allows for little or no flow turning on the outer nacelle. Present methods using conical-flow Busemann parent flowfields have simply truncated, or otherwise modified, the stream-traced contours to include this internal cowl angle. Such modifications disrupt the parent flowfield, reducing inlet performance and flow uniformity. The method presented herein merges a conical flowfield that includes a leading shock with a truncated Busemann flowfield in a manner that minimizes unwanted interactions. A leading internal cowl angle is now inherent in the parent flowfield, and inlet contours traced from this flowfield retain its high performance and good flow uniformity. Computational fluid dynamics analysis of a candidate inlet design is presented that verifies the design technique, and it reveals a starting issue with the basic geometry. A minor modification to the cowl lip region is shown to eliminate this phenomenon, thereby allowing starting and smooth transition to subcritical operation as backpressure is increased. An inlet critical-point total pressure recovery of 96% is achieved based on computational fluid dynamics results for a Mach 1.7 freestream design. Correction for boundary-layer displacement thickness and sizing for a given engine airflow requirement are also discussed. C1 [Otto, Samuel E.] Purdue Univ, Inlets & Nozzles Branch, W Lafayette, IN 47906 USA. [Trefny, Charles J.; Slater, John W.] NASA, John H Glenn Res Ctr, Inlets & Nozzles Branch, 21000 Brookpark Rd Mail Stop 5-11, Cleveland, OH 44135 USA. RP Otto, SE (reprint author), Purdue Univ, Inlets & Nozzles Branch, W Lafayette, IN 47906 USA. NR 12 TC 0 Z9 0 U1 4 U2 4 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 SEP PY 2016 VL 32 IS 5 BP 1178 EP 1189 DI 10.2514/1.B36028 PG 12 WC Engineering, Aerospace SC Engineering GA DW2MH UT WOS:000383476000015 ER PT J AU Pokhrel, R Gutermuth, R Ali, B Megeath, T Pipher, J Myers, P Fischer, WJ Henning, T Wolk, SJ Allen, L Tobin, JJ AF Pokhrel, R. Gutermuth, R. Ali, B. Megeath, T. Pipher, J. Myers, P. Fischer, W. J. Henning, T. Wolk, S. J. Allen, L. Tobin, J. J. TI A Herschel-SPIRE survey of the Mon R2 giant molecular cloud: analysis of the gas column density probability density function SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM: clouds; ISM: individual objects: Mon R2; ISM: structure ID YOUNG STELLAR CLUSTERS; GOULD BELT SURVEY; STAR-FORMATION; MONOCEROS R2; INTERSTELLAR CLOUDS; REFLECTION NEBULAE; DUST TEMPERATURE; TURBULENCE; ORION; RESOLUTION AB We present a far-IR survey of the entire Mon R2 giant molecular cloud (GMC) with Herschel-Spectral and Photometric Imaging REceiver cross-calibrated with Planck-High Frequency Instrument data. We fit the spectral energy distributions of each pixel with a greybody function and an optimal beta value of 1.8. We find that mid-range column densities obtained from far-IR dust emission and near-IR extinction are consistent. For the entire GMC, we find that the column density histogram, or column density probability distribution function (N-PDF), is lognormal below similar to 10(21) cm(-2). Above this value, the distribution takes a power law form with an index of -2.15. We analyse the gas geometry, N-PDF shape, and young stellar object (YSO) content of a selection of subregions in the cloud. We find no regions with pure lognormal N-PDFs. The regions with a combination of lognormal and one power-law N-PDF have a YSO cluster and a corresponding centrally concentrated gas clump. The regions with a combination of lognormal and two power-law N-PDF have significant numbers of typically younger YSOs but no prominent YSO cluster. These regions are composed of an aggregate of closely spaced gas filaments with no concentrated dense gas clump. We find that for our fixed scale regions, the YSO count roughly correlates with the N-PDF power-law index. The correlation appears steeper for single power-law regions relative to two power-law regions with a high column density cut-off, as a greater dense gas mass fraction is achieved in the former. A stronger correlation is found between embedded YSO count and the dense gas mass among our regions. C1 [Pokhrel, R.; Gutermuth, R.] Univ Massachusetts, Amherst, MA 01003 USA. [Ali, B.] Space Sci Inst, Boulder, CO 80301 USA. [Megeath, T.] Univ Toledo, 2801 W Bancroft St, Toledo, OH 43606 USA. [Pipher, J.] Univ Rochester, 601 Elmwood Ave, Rochester, NY 14627 USA. [Myers, P.; Wolk, S. J.] Harvard Univ, CFA, Cambridge, MA 02138 USA. [Fischer, W. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Henning, T.] MPIA Heidelberg, Konigstuhl 17, D-69117 Heidelberg, Germany. [Allen, L.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Tobin, J. J.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. RP Gutermuth, R (reprint author), Univ Massachusetts, Amherst, MA 01003 USA. EM rgutermu@astro.umass.edu FU NASA through JPL/Caltech [1489384]; NASA [NAS8-03060]; CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); NASA (USA); BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); CICT/MCT (Spain) FX This work is based on observations made with Herschel, a European Space Agency cornerstone mission with science instruments provided by European-led Principal Investigator consortia and with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech (contract number 1489384). SJW was supported by NASA contract NAS8-03060. We are thankful to Stella Offner, Mark Heyer, Grant Wilson and Ronald Snell from the University of Massachusetts (UMASS), Amherst for helpful conversations, suggestions, and feedback. We also thank Amy Stutz of the Max-Planck Institute for Astronomy, Germany for important suggestions on the paper. We also thank Bernhard Schulz and David Shupe from NASA Herschel Science Center for helping us with data reduction. We are grateful to Manikarajamuthaly Sri Saravana for helping us with technical aspects. Finally, we would like to thank the anonymous referee for valuable comments and suggestions. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada); NAOC (China); CEA, LAM(France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK); Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI (Italy), and CICT/MCT (Spain). NR 60 TC 0 Z9 0 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 SEP 1 PY 2016 VL 461 IS 1 BP 22 EP 35 DI 10.1093/mnras/stw1303 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DV9PE UT WOS:000383272500003 ER PT J AU Archambault, S Archer, A Barnacka, A Behera, B Beilicke, M Benbow, W Berger, K Bird, R Bottcher, M Buckley, JH Bugaev, V Cardenzana, JV Cerruti, M Chen, X Christiansen, JL Ciupik, L Collins-Hughes, E Connolly, MP Cui, W Dickinson, HJ Dumm, J Eisch, JD Errando, M Falcone, A Federici, S Feng, Q Finley, JP Fleischhack, H Fortson, L Furniss, A Gillanders, GH Godambe, S Griffin, S Griffiths, ST Grube, J Gyuk, G Hakansson, N Hanna, D Holder, J Hughes, G Johnson, CA Kaaret, P Kar, P Kertzman, M Khassen, Y Kieda, D Krawczynski, H Kumar, S Lang, MJ Madhavan, AS Maier, G McArthur, S McCann, A Meagher, K Millis, J Moriarty, P Nelson, T Nieto, D de Bhroithe, AO Ong, RA Otte, AN Park, N Perkins, JS Pohl, M Popkow, A Prokoph, H Pueschel, E Quinn, J Ragan, K Rajotte, J Reyes, LC Reynolds, PT Richards, GT Roache, E Sembroski, GH Shahinyan, K Smith, AW Staszak, D Sweeney, K Telezhinsky, I Tucci, JV Tyler, J Varlotta, A Vassiliev, VV Wakely, SP Welsing, R Wilhelm, A Williams, DA Zitzer, B AF Archambault, S. Archer, A. Barnacka, A. Behera, B. Beilicke, M. Benbow, W. Berger, K. Bird, R. Bottcher, M. Buckley, J. H. Bugaev, V. Cardenzana, J. V. Cerruti, M. Chen, X. Christiansen, J. L. Ciupik, L. Collins-Hughes, E. Connolly, M. P. Cui, W. Dickinson, H. J. Dumm, J. Eisch, J. D. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fleischhack, H. Fortson, L. Furniss, A. Gillanders, G. H. Godambe, S. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Hakansson, N. Hanna, D. Holder, J. Hughes, G. Johnson, C. A. Kaaret, P. Kar, P. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Kumar, S. Lang, M. J. Madhavan, A. S. Maier, G. McArthur, S. McCann, A. Meagher, K. Millis, J. Moriarty, P. Nelson, T. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Park, N. Perkins, J. S. Pohl, M. Popkow, A. Prokoph, H. Pueschel, E. Quinn, J. Ragan, K. Rajotte, J. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Sembroski, G. H. Shahinyan, K. Smith, A. W. Staszak, D. Sweeney, K. Telezhinsky, I. Tucci, J. V. Tyler, J. Varlotta, A. Vassiliev, V. V. Wakely, S. P. Welsing, R. Wilhelm, A. Williams, D. A. Zitzer, B. TI Discovery of very high energy gamma rays from 1ES 1440+122 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE BL Lacertae objects: general; gamma-rays: general ID BL-LACERTAE OBJECTS; LARGE-AREA TELESCOPE; EXTRAGALACTIC BACKGROUND LIGHT; INTERGALACTIC MAGNETIC-FIELD; ACTIVE GALACTIC NUCLEI; EINSTEIN SLEW SURVEY; TEV BLAZARS; MULTIWAVELENGTH OBSERVATIONS; BRIGHT BLAZARS; SOURCE CATALOG AB The BL Lacertae object 1ES 1440+ 122 was observed in the energy range from 85 GeV to 30 TeV by the VERITAS array of imaging atmospheric Cherenkov telescopes. The observations, taken between 2008 May and 2010 June and totalling 53 h, resulted in the discovery of gamma-ray emission from the blazar, which has a redshift z = 0.163. 1ES 1440+ 122 is detected at a statistical significance of 5.5 standard deviations above the background with an integral flux of (2.8 +/- 0.7(stat) +/- 0.8sys) x 10(-12) cm(-2) s(-1) (1.2 per cent of the Crab Nebula's flux) above 200 GeV. The measured spectrum is described well by a power law from 0.2 to 1.3 TeV with a photon index of 3.1 +/- 0.4(stat) +/- 0.2(sys). Quasi-simultaneous multiwavelength data from the Fermi Large Area Telescope (0.3-300 GeV) and the Swift X-ray Telescope (0.2-10 keV) are additionally used to model the properties of the emission region. A synchrotron self-Compton model produces a good representation of the multiwavelength data. Adding an external-Compton or a hadronic component also adequately describes the data. C1 [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Rajotte, J.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Archer, A.; Beilicke, M.; Buckley, J. H.; Bugaev, V.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Barnacka, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Behera, B.; Chen, X.; Federici, S.; Fleischhack, H.; Hughes, G.; Maier, G.; de Bhroithe, A. O'Faolain; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Welsing, R.; Wilhelm, A.] DESY, Platanenallee 6, D-15738 Zeuthen, Germany. [Benbow, W.; Cerruti, M.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Bartol Res Inst, Newark, DE 19716 USA. [Bird, R.; Collins-Hughes, E.; Khassen, Y.; Pueschel, E.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Bottcher, M.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa. [Cardenzana, J. V.; Dickinson, H. J.; Eisch, J. D.; Madhavan, A. S.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Chen, X.; Federici, S.; Hakansson, N.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Golm, Germany. [Christiansen, J. L.; Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [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.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Univ Rd, Galway, Ireland. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Tucci, J. V.; Varlotta, A.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA. [Dumm, J.; Fortson, L.; Nelson, T.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Errando, M.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Godambe, S.] Bhabha Atom Res Ctr, Astrophys Sci Div, Bombay 400085, Maharashtra, India. [Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Van Allen Hall, Iowa City, IA 52242 USA. [Kar, P.; Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [McArthur, S.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, 5640 S Ellis Ave, Chicago, IL 60637 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, 837 State St NW, Atlanta, GA 30332 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, 837 State St NW, Atlanta, GA 30332 USA. [Millis, J.] Anderson Univ, Dept Phys, 1100 East 5th St, Anderson, IN 46012 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Dublin Rd, Dublin, Ireland. [Nieto, D.] Columbia Univ, Dept Phys, 538 W 120th St, New York, NY 10027 USA. [Ong, R. A.; Popkow, A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Sci, Cork, Ireland. [Sweeney, K.] Ohio Univ, Dept Phys & Astron, Clippinger Res Lab 251B, Athens, OH 45701 USA. [Zitzer, B.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA. RP Dumm, J (reprint author), Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. EM dumm@physics.umn.edu FU US Department of Energy Office of Science; US National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the UK; South African Department of Science and Technology through the National Research Foundation under NRF SARChI Chair [64789] FX This research is supported by grants from the US Department of Energy Office of Science, the US National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748), and by STFC in the UK. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. M. Bottcher acknowledges support by the South African Department of Science and Technology through the National Research Foundation under NRF SARChI Chair grant no. 64789. The VERITAS Collaboration is grateful to Trevor Weekes for his seminal contributions and leadership in the field of VHE gamma-ray astrophysics, which made this study possible. NR 59 TC 1 Z9 1 U1 5 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 1 PY 2016 VL 461 IS 1 BP 202 EP 208 DI 10.1093/mnras/stw1319 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DV9PE UT WOS:000383272500017 ER PT J AU Sifon, C Battaglia, N Hasselfield, M Menanteau, F Barrientos, LF Bond, JR Crichton, D Devlin, MJ Dunner, R Hilton, M Hincks, AD Hlozek, R Huffenberger, KM Hughes, JP Infante, L Kosowsky, A Marsden, D Marriage, TA Moodley, K Niemack, MD Page, LA Spergel, DN Staggs, ST Trac, H Wollack, EJ AF Sifon, Cristobal Battaglia, Nick Hasselfield, Matthew Menanteau, Felipe Felipe Barrientos, L. Bond, J. Richard Crichton, Devin Devlin, Mark J. Dunner, Rolando Hilton, Matt Hincks, Adam D. Hlozek, Renee Huffenberger, Kevin M. Hughes, John P. Infante, Leopoldo Kosowsky, Arthur Marsden, Danica Marriage, Tobias A. Moodley, Kavilan Niemack, Michael D. Page, Lyman A. Spergel, David N. Staggs, Suzanne T. Hy Trac Wollack, Edward J. TI The Atacama Cosmology Telescope: dynamical masses for 44 SZ-selected galaxy clusters over 755 square degrees SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: general; Galaxies: distances and redshifts; cosmology: observations; large-scale structure of Universe ID DIGITAL SKY SURVEY; SOUTH-POLE TELESCOPE; WEAK-LENSING MASSES; ZELDOVICH-SELECTED CLUSTERS; ACT-CL J0102-4915; X-RAY-PROPERTIES; SUNYAEV-ZELDOVICH; SCALING RELATIONS; VELOCITY DISPERSIONS; RICH CLUSTERS AB We present galaxy velocity dispersions and dynamical mass estimates for 44 galaxy clusters selected via the Sunyaev-Zel'dovich (SZ) effect by the Atacama Cosmology Telescope. Dynamical masses for 18 clusters are reported here for the first time. Using N-body simulations, we model the different observing strategies used to measure the velocity dispersions and account for systematic effects resulting from these strategies. We find that the galaxy velocity distributions may be treated as isotropic, and that an aperture correction of up to 7 per cent in the velocity dispersion is required if the spectroscopic galaxy sample is sufficiently concentrated towards the cluster centre. Accounting for the radial profile of the velocity dispersion in simulations enables consistent dynamical mass estimates regardless of the observing strategy. Cluster masses M200 are in the range (1-15) x 10(14)M(circle dot). Comparing with masses estimated from the SZ distortion assuming a gas pressure profile derived from X-ray observations gives a mean SZ-to-dynamical mass ratio of 1.10 +/- 0.13, but there is an additional 0.14 systematic uncertainty due to the unknown velocity bias; the statistical uncertainty is dominated by the scatter in the mass-velocity dispersion scaling relation. This ratio is consistent with previous determinations at these mass scales. C1 [Sifon, Cristobal; Hughes, John P.] Gemini South Observ, Hilo, HI 96720 USA. [Sifon, Cristobal] Leiden Univ, Leiden Observ, POB 513, NL-2300 RA Leiden, Netherlands. [Battaglia, Nick; Hasselfield, Matthew; Hlozek, Renee; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. [Hasselfield, Matthew] Penn State Univ, Dept Astron & Astrophys, Davey Lab, 525 Davey Lab, University Pk, PA 16802 USA. [Menanteau, Felipe] Univ Illinois, Natl Ctr Supercomp Applicat, 1205 W Clark St, Urbana, IL 61801 USA. [Menanteau, Felipe] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Felipe Barrientos, L.; Dunner, Rolando; Infante, Leopoldo] Pontificia Univ Catolica, Fac Fis, Inst Astrofis, Casilla 306, Santiago 22, Chile. [Bond, J. Richard] Canadian Inst Theoret Astrophys, 60 St George, Toronto, ON M5S 3H8, Canada. [Crichton, Devin; Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. [Devlin, Mark J.; Marsden, Danica] Univ Penn, Dept Phys & Astron, 209 South 33rd St, Philadelphia, PA 19104 USA. [Hilton, Matt; Moodley, Kavilan] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Hincks, Adam D.] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada. [Hincks, Adam D.] Pontificia Univ Gregoriana, Piazza Pilotta 4, I-00187 Rome, Italy. [Huffenberger, Kevin M.] Florida State Univ, Dept Phys, POB 3064350, Tallahassee, FL 32306 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA. [Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Page, Lyman A.; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Jadwin Hall, Princeton, NJ 08544 USA. [Hy Trac] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sifon, C (reprint author), Gemini South Observ, Hilo, HI 96720 USA.; Sifon, C (reprint author), Leiden Univ, Leiden Observ, POB 513, NL-2300 RA Leiden, Netherlands. EM sifon@strw.leidenuniv.nl RI Wollack, Edward/D-4467-2012; Trac, Hy/N-8838-2014; OI Wollack, Edward/0000-0002-7567-4451; Trac, Hy/0000-0001-6778-3861; Huffenberger, Kevin/0000-0001-7109-0099; Menanteau, Felipe/0000-0002-1372-2534; Sifon, Cristobal/0000-0002-8149-1352 FU European Research Council under FP7 grant [279396]; FONDECYT [1120676]; NSF [1312380]; US National Science Foundation [AST-0408698, AST-0965625, PHY-0855887, PHY-1214379]; Princeton University; University of Pennsylvania; Canada Foundation for Innovation (CFI) award; Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT); CFI under the auspices of Compute Canada; Government of Ontario; Ontario Research Fund - Research Excellence; University of Toronto; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science; Spanish MultiDark Consolider Project [CSD2009-00064] FX CS acknowledges support from the European Research Council under FP7 grant number 279396 awarded to H. Hoekstra. NB and RH acknowledge support from the iii Fellowship. LFB's research is supported by FONDECYT under project 1120676. AK acknowledges support from NSF grant 1312380. This work was supported by the US National Science Foundation through awards AST-0408698 and AST-0965625 for the ACT project, as well as awards PHY-0855887 and PHY-1214379. Funding was also provided by Princeton University, the University of Pennsylvania, and a Canada Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque Astronomico Atacama in northern Chile under the auspices of the Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT). Computations were performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by the CFI under the auspices of Compute Canada, the Government of Ontario, the Ontario Research Fund - Research Excellence; and the University of Toronto. 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 web site is http://www.sdss9.org/. The MultiDark Database used in this paper and the web application providing online access to it were constructed as part of the activities of the German Astrophysical Virtual Observatory as result of a collaboration between the Leibniz-Institute for Astrophysics Potsdam (AIP) and the Spanish MultiDark Consolider Project CSD2009-00064. The Bolshoi and MultiDark simulations were run on the NASA's Pleiades supercomputer at the NASA Ames Research Center. The MDPL and the BigMD simulation suite have been performed in the Supermuc supercomputer at LRZ using time granted by PRACE. NR 141 TC 4 Z9 4 U1 2 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 SEP 1 PY 2016 VL 461 IS 1 BP 248 EP 270 DI 10.1093/mnras/stw1284 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DV9PE UT WOS:000383272500022 ER PT J AU Clavel, M Tomsick, JA Bodaghee, A Chiu, JL Fornasini, FM Hong, J Krivonos, R Ponti, G Rahoui, F Stern, D AF Clavel, M. Tomsick, J. A. Bodaghee, A. Chiu, J. -L. Fornasini, F. M. Hong, J. Krivonos, R. Ponti, G. Rahoui, F. Stern, D. TI IGR J18293-1213 is an eclipsing cataclysmic variable SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: eclipsing; stars: individual: IGR J18293-1213-white dwarfs; X-rays: stars ID X-RAY BINARIES; INTERMEDIATE POLARS; MILKY-WAY; EMISSION; MISSION; REFLECTION; TELESCOPE; EVOLUTION; STARS; SKY AB Studying the population of faint hard X-ray sources along the plane of the Galaxy is challenging because of high extinction and crowding, which make the identification of individual sources more difficult. IGR J18293-1213 is part of the population of persistent sources which have been discovered by the INTEGRAL satellite. We report on NuSTAR and Swift/XRT observations of this source, performed on 2015 September 11. We detected three eclipsing intervals in the NuSTAR light curve, allowing us to constrain the duration of these eclipses, Delta t = 30.8(-0.0)(+6.3) min, and the orbital period of the system, T = 6.92 +/- 0.01 h. Even though we only report an upper limit on the amplitude of a putative spin modulation, the orbital period and the hard thermal bremsstrahlung spectrum of IGR J18293-1213 provide strong evidence that this source is a magnetic cataclysmic variable. Our NuSTAR and Swift/XRT joint spectral analysis places strong constraints on the white dwarf mass M-wd = 0.78(-0.09)(+0.10) M-circle dot. Assuming that the mass to radius ratio of the companion star M star /R star = 1 (solar units) and using T, Delta t, and M-wd, we derived the mass of the companion star M-star = 0.82 +/- 0.01 M-circle dot, the orbital separation of the binary system a = 2.14 +/- 0.04 R-circle dot, and its orbital inclination compared to the line of sight i = (72 degrees.2(-0.0)(+2.4)) +/- 1 degrees.0. C1 [Clavel, M.; Tomsick, J. A.; Chiu, J. -L.; Fornasini, F. M.] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. [Bodaghee, A.] Georgia Coll, 231 W Hancock St, Milledgeville, GA 31061 USA. [Fornasini, F. M.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Hong, J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Krivonos, R.] Russian Acad Sci, Space Res Inst, Profsoyuznaya 84-32, Moscow 117997, Russia. [Ponti, G.] Max Planck Inst Extraterr Phys, Gissenbachstr, D-85748 Garching, Germany. [Rahoui, F.] European Southern Observ, Karl Schwarzchild Str 2, D-85748 Garching, Germany. [Rahoui, F.] Harvard Univ, Dept Astron, 60 Garden St, Cambridge, MA 02138 USA. [Stern, D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Clavel, M (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. EM maica.clavel@ssl.berkeley.edu OI Clavel, Maica/0000-0003-0724-2742 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; Russian Science Foundation [14-22-00271]; Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur Luftund Raumfahrt (BMWI/DLR) [FKZ 50 OR 1408] 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). RK acknowledges support from Russian Science Foundation (grant 14-22-00271). GP acknowledges the Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur Luftund Raumfahrt (BMWI/DLR, FKZ 50 OR 1408). NR 34 TC 0 Z9 0 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 SEP 1 PY 2016 VL 461 IS 1 BP 304 EP 311 DI 10.1093/mnras/stw1330 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DV9PE UT WOS:000383272500026 ER PT J AU Joachimi, K Gatuzz, E Garcia, JA Kallman, TR AF Joachimi, Katerine Gatuzz, Efrain Garcia, Javier A. Kallman, Timothy R. TI On the detectability of CO molecules in the interstellar medium via X-ray spectroscopy SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: spectroscopic; ISM: molecules; ISM: structure; X-rays: ISM ID K-SHELL PHOTOABSORPTION; MILKY-WAY; ABSORPTION MODEL; XMM-NEWTON; OXYGEN; BINARIES; CLOUDS; NEON; EDGE; PHOTOIONIZATION AB We present a study of the detectability of CO molecules in the Galactic interstellar medium using high-resolution X-ray spectra obtained with the XMM-Newton Reflection Grating Spectrometer. We analysed 10 bright low mass X-ray binaries (LMXBs) to study the CO contribution in their line of sights. A total of 25 observations were fitted with the ISMabs X-ray absorption model which includes photoabsorption cross-sections for OI, OII, OIII and CO. We performed a Monte Carlo (MC) simulation analysis of the goodness of fit in order to estimate the significance of the CO detection. We determine that the statistical analysis prevents a significant detection of CO molecular X-ray absorption features, except for the lines of sight towards XTE J1718-330 and 4U 1636-53. In the case of XTE J1817-330, this is the first report of the presence of CO along its line of sight. Our results reinforce the conclusion that molecules have a minor contribution to the absorption features in the O K-edge spectral region. We estimate a CO column density lower limit to perform a significant detection with XMM-Newton of N(CO) > 6 x 10(16) cm(-2) for typical exposure times. C1 [Joachimi, Katerine; Gatuzz, Efrain] Cent Univ Venezuela, Fac Ciencias, Escuela Fis, POB 20632, Caracas 1020A, Venezuela. [Gatuzz, Efrain] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Garcia, Javier A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Kallman, Timothy R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gatuzz, E (reprint author), Cent Univ Venezuela, Fac Ciencias, Escuela Fis, POB 20632, Caracas 1020A, Venezuela.; Gatuzz, E (reprint author), Max Planck Inst Astrophys, D-85741 Garching, Germany. EM efraingatuzz@gmail.com; jajgarcia@gmail.com NR 33 TC 0 Z9 0 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 SEP 1 PY 2016 VL 461 IS 1 BP 352 EP 357 DI 10.1093/mnras/stw1371 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DV9PE UT WOS:000383272500030 ER PT J AU Davies, LJM Driver, SP Robotham, ASG Grootes, MW Popescu, CC Tuffs, RJ Hopkins, A Alpaslan, M Andrews, SK Bland-Hawthorn, J Bremer, MN Brough, S Brown, MJI Cluver, ME Croom, S da Cunha, E Dunne, L Lara-Lopez, MA Liske, J Loveday, J Moffett, AJ Owers, M Phillipps, S Sansom, AE Taylor, EN Michalowski, MJ Ibar, E Smith, M Bourne, N AF Davies, L. J. M. Driver, S. P. Robotham, A. S. G. Grootes, M. W. Popescu, C. C. Tuffs, R. J. Hopkins, A. Alpaslan, M. Andrews, S. K. Bland-Hawthorn, J. Bremer, M. N. Brough, S. Brown, M. J. I. Cluver, M. E. Croom, S. da Cunha, E. Dunne, L. Lara-Lopez, M. A. Liske, J. Loveday, J. Moffett, A. J. Owers, M. Phillipps, S. Sansom, A. E. Taylor, E. N. Michalowski, M. J. Ibar, E. Smith, M. Bourne, N. TI GAMA/H-ATLAS: a meta-analysis of SFR indicators - comprehensive measures of the SFR-M* relation and cosmic star formation history at z < 0.4 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: star formation ID MASS ASSEMBLY GAMA; DIGITAL SKY SURVEY; SPECTRAL ENERGY-DISTRIBUTION; HIGH-REDSHIFT GALAXIES; DEEP FIELD SOUTH; FORMING GALAXIES; SPIRAL GALAXIES; STELLAR MASS; MAIN-SEQUENCE; FORMATION RATES AB We present a meta-analysis of star formation rate (SFR) indicators in the Galaxy And Mass Assembly (GAMA) survey, producing 12 different SFR metrics and determining the SFRM* relation for each. We compare and contrast published methods to extract the SFR from each indicator, using a well-defined local sample of morphologically selected spiral galaxies, which excludes sources which potentially have large recent changes to their SFR. The different methods are found to yield SFR-M* relations with inconsistent slopes and normalizations, suggesting differences between calibration methods. The recovered SFR-M* relations also have a large range in scatter which, as SFRs of the targets may be considered constant over the different time-scales, suggests differences in the accuracy by which methods correct for attenuation in individual targets. We then recalibrate all SFR indicators to provide new, robust and consistent luminosity-to-SFR calibrations, finding that the most consistent slopes and normalizations of the SFR-M* relations are obtained when recalibrated using the radiation transfer method of Popescu et al. These new calibrations can be used to directly compare SFRs across different observations, epochs and galaxy populations. We then apply our calibrations to the GAMA II equatorial data set and explore the evolution of star formation in the local Universe. We determine the evolution of the normalization to the SFR-M* relation from 0 < z < 0.35 - finding consistent trends with previous estimates at 0.3 < z < 1.2. We then provide the definitive z < 0.35 cosmic star formation history, SFR-M* relation and its evolution over the last 3 billion years. C1 [Davies, L. J. M.; Driver, S. P.; Robotham, A. S. G.; Andrews, S. K.; Moffett, A. J.] Univ Western Australia, ICRAR, 35 Stirling Highway, Crawley, WA 6009, Australia. [Driver, S. P.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Grootes, M. W.] ESA ESTEC SCI S, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. [Popescu, C. C.; Sansom, A. E.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Popescu, C. C.] Romanian Acad, Astron Inst, Str Cutitul Argint 5, Bucharest 040557, Romania. [Tuffs, R. J.] Max Planck Inst Kernphys, Saupfercheckweg 1, D-69117 Heidelberg, Germany. [Hopkins, A.; Brough, S.; Owers, M.] Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia. [Alpaslan, M.] NASA, Ames Res Ctr, N232, Mountain View, CA 94034 USA. [Bland-Hawthorn, J.; Croom, S.] Univ Sydney, Sch Phys A28, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Bremer, M. N.; Phillipps, S.] Univ Bristol, Sch Phys, Astrophys Grp, Tyndall Ave, Bristol BS8 1TL, Avon, England. [Brown, M. J. I.] Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia. [Cluver, M. E.] Univ Western Cape, Dept Phys & Astron, Robert Sobukwe Rd, ZA-7535 Bellville, South Africa. [da Cunha, E.; Taylor, E. N.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, POB 218, Hawthorn, Vic 3122, Australia. [Dunne, L.; Michalowski, M. J.; Bourne, N.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Dunne, L.; Smith, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Lara-Lopez, M. A.] Univ Nacl Autonoma Mexico, Inst Astron, AP 70-264, Mexico City 04510, DF, Mexico. [Liske, J.] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. [Loveday, J.] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Owers, M.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia. [Ibar, E.] Univ Valparaiso, Inst Fis & Astron, Avda Gran Bretana 1111, Valparaiso, Chile. RP Davies, LJM (reprint author), Univ Western Australia, ICRAR, 35 Stirling Highway, Crawley, WA 6009, Australia. EM luke.j.davies@uwa.edu.au RI Brown, Michael/B-1181-2015; OI Brown, Michael/0000-0002-1207-9137; Alpaslan, Mehmet/0000-0003-0321-1033 FU STFC (UK); ARC (Australia); AAO; UNAM through the PAPIIT project [IA101315]; European Research Council Advanced Investigator grant Cosmic Dust FX GAMA is a joint European-Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalogue is based on data taken from the Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programmes including GALEX MIS, VST KiDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT and ASKAP providing UV-to-radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO and the participating institutions. The GAMA website is http://www.gama-survey.org/.; MALL acknowledges support from UNAM through the PAPIIT project IA101315. LD acknowledges support from European Research Council Advanced Investigator grant Cosmic Dust. NR 118 TC 5 Z9 5 U1 2 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 SEP 1 PY 2016 VL 461 IS 1 BP 458 EP 485 DI 10.1093/mnras/stw1342 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DV9PE UT WOS:000383272500037 ER PT J AU Pieres, A Santiago, B Balbinot, E Luque, E Queiroz, A da Costa, LN Maia, MAG Drlica-Wagner, A Roodman, A Abbott, TMC Allam, S Benoit-Levy, A Bertin, E Brooks, D Buckley-Geer, E Burke, DL Rosell, AC Kind, MC Carretero, J Cunha, CE Desai, S Diehl, HT Eifler, TF Finley, DA Flaugher, B Fosalba, P Frieman, J Gerdes, DW Gruen, D Gruendl, RA Gutierrez, G Honscheid, K James, DJ Kuehn, K Kuropatkin, N Lahav, O Li, TS Marshall, L Martini, P Miller, CJ Miquel, R Nichol, RC Nord, B Ogando, R Plazas, AA Romer, AK Sanchez, E Scarpine, V Schubnell, M Sevilla-Noarbe, I Smith, RC Soares-Santos, M Sobreira, F Suchyta, E Swanson, MEC Tarle, G Thaler, J Thomas, D Tucker, DL Walker, AR AF Pieres, A. Santiago, B. Balbinot, E. Luque, E. Queiroz, A. da Costa, L. N. Maia, M. A. G. Drlica-Wagner, A. Roodman, A. Abbott, T. M. C. Allam, S. Benoit-Levy, A. Bertin, E. Brooks, D. Buckley-Geer, E. Burke, D. L. Rosell, A. Carnero Kind, M. Carrasco Carretero, J. Cunha, C. E. Desai, S. Diehl, H. T. Eifler, T. F. Finley, D. A. Flaugher, B. Fosalba, P. Frieman, J. Gerdes, D. W. Gruen, D. Gruendl, R. A. Gutierrez, G. Honscheid, K. James, D. J. Kuehn, K. Kuropatkin, N. Lahav, O. Li, T. S. Marshall, L. Martini, P. Miller, C. J. Miquel, R. Nichol, R. C. Nord, B. Ogando, R. Plazas, A. A. Romer, A. K. Sanchez, E. Scarpine, V. Schubnell, M. Sevilla-Noarbe, I. Smith, R. C. Soares-Santos, M. Sobreira, F. Suchyta, E. Swanson, M. E. C. Tarle, G. Thaler, J. Thomas, D. Tucker, D. L. Walker, A. R. TI Physical properties of star clusters in the outer LMC as observed by the DES SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: statistical; Magellanic Cloud; galaxies: star clusters: general ID LARGE-MAGELLANIC-CLOUD; COLOR-MAGNITUDE DIAGRAMS; CHEMICAL ENRICHMENT HISTORY; SIMPLE STELLAR POPULATIONS; STRUCTURAL PARAMETERS; METALLICITY RELATION; PHOTOMETRIC SYSTEMS; SOURCE EXTRACTION; AGE DISTRIBUTION; RED CLUMP AB The Large Magellanic Cloud (LMC) harbours a rich and diverse system of star clusters, whose ages, chemical abundances and positions provide information about the LMC history of star formation. We use Science Verification imaging data from the Dark Energy Survey (DES) to increase the census of known star clusters in the outer LMC and to derive physical parameters for a large sample of such objects using a spatially and photometrically homogeneous data set. Our sample contains 255 visually identified cluster candidates, of which 109 were not listed in any previous catalogue. We quantify the crowding effect for the stellar sample produced by the DES Data Management pipeline and conclude that the stellar completeness is < 10 per cent inside typical LMC cluster cores. We therefore reanalysed the DES co-add images around each candidate cluster and remeasured positions and magnitudes for their stars. We also implement a maximum-likelihood method to fit individual density profiles and colour-magnitude diagrams. For 117 (from a total of 255) of the cluster candidates (28 uncatalogued clusters), we obtain reliable ages, metallicities, distance moduli and structural parameters, confirming their nature as physical systems. The distribution of cluster metallicities shows a radial dependence, with no clusters more metal rich than [Fe/H] similar or equal to -0.7 beyond 8 kpc from the LMC centre. The age distribution has two peaks at similar or equal to 1.2 and similar or equal to 2.7 Gyr. C1 [Pieres, A.; Santiago, B.; Luque, E.; Queiroz, A.] Univ Fed Rio Grande do Sul, Inst Fis, Caixa Postal 15051, BR-91501970 Porto Alegre, RS, Brazil. [Pieres, A.; Santiago, B.; Luque, E.; Queiroz, A.; da Costa, L. N.; Maia, M. A. G.; Rosell, A. Carnero; Ogando, R.; Sobreira, F.] Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Balbinot, E.] Univ Surrey, Dept Phys, Guildford GU2 7XH, Surrey, England. [da Costa, L. N.; Maia, M. A. G.; Rosell, A. Carnero; Ogando, R.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Drlica-Wagner, A.; Allam, S.; Buckley-Geer, E.; Diehl, H. T.; Finley, D. A.; Flaugher, B.; Frieman, J.; Gutierrez, G.; Kuropatkin, N.; Nord, B.; Scarpine, V.; Soares-Santos, M.; Tucker, D. L.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. [Roodman, A.; Burke, D. L.; Cunha, C. E.; Frieman, J.; Gruen, D.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA. [Roodman, A.; Burke, D. L.; Gruen, D.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Abbott, T. M. C.; James, D. J.; Smith, R. C.; Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile. [Benoit-Levy, A.; Bertin, E.] CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Benoit-Levy, A.; Brooks, D.; Lahav, O.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Benoit-Levy, A.; Bertin, E.] Univ Paris 06, Sorbonne Univ, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Kind, M. Carrasco; Gruendl, R. A.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Kind, M. Carrasco; Gruendl, R. A.; Swanson, M. E. C.] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA. [Carretero, J.; Fosalba, P.] IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans,S-N, E-08193 Barcelona, Spain. [Carretero, J.; Miquel, R.] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Barcelona, Spain. [Desai, S.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Desai, S.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Eifler, T. F.; Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Gerdes, D. W.; Miller, C. J.; Schubnell, M.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Honscheid, K.; Martini, P.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Honscheid, K.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Li, T. S.; Marshall, L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Li, T. S.; Marshall, L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Martini, P.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. [Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Nichol, R. C.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England. [Sanchez, E.; Sevilla-Noarbe, I.] Ctr Invest Energet Medioambientales & Tecnol CIEM, Madrid, Spain. [Sobreira, F.] Univ Estadual Paulista, ICTP South Amer Inst Fundamental Res, Inst Fis Teor, Sao Paulo, Brazil. [Suchyta, E.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Thaler, J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. RP Pieres, A (reprint author), Univ Fed Rio Grande do Sul, Inst Fis, Caixa Postal 15051, BR-91501970 Porto Alegre, RS, Brazil.; Pieres, A (reprint author), Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. EM adriano.pieres@ufrgs.br; basilio.santiago@ufrgs.br; e.balbinot@surrey.ac.uk RI Ogando, Ricardo/A-1747-2010; OI Ogando, Ricardo/0000-0003-2120-1154; Sobreira, Flavia/0000-0002-7822-0658 FU Brazilian Institution CNPq; European Research Council [ERC-StG-335936]; US Department of Energy; US National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; Collaborating Institutions in the Dark Energy Survey; National Science Foundation [AST-1138766]; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; European Research Council under the European Union [240672, 291329, 306478] FX AdP acknowledges financial support from the Brazilian Institution CNPq. EdB acknowledges financial support from the European Research Council (ERC-StG-335936, CLUSTERS).; Funding for the DES Projects has been provided by the US Department of Energy, the US National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey.; The DES data management system is supported by the National Science Foundation under Grant Number AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986 and Centro de Excelencia Severo Ochoa SEV-2012-0234. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013) including ERC grant agreements 240672, 291329 and 306478. NR 67 TC 2 Z9 2 U1 5 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 1 PY 2016 VL 461 IS 1 BP 519 EP 541 DI 10.1093/mnras/stw1260 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DV9PE UT WOS:000383272500041 ER PT J AU LeGrande, AN Tsigaridis, K Bauer, SE AF LeGrande, Allegra N. Tsigaridis, Kostas Bauer, Susanne E. TI Role of atmospheric chemistry in the climate impacts of stratospheric volcanic injections SO NATURE GEOSCIENCE LA English DT Article ID WATER-VAPOR; NORTHERN MIDLATITUDES; ERUPTIONS; OZONE; PINATUBO; WINTER; RECONSTRUCTIONS; SPECTROMETER; SENSITIVITY; AEROSOLS AB The climate impact of a volcanic eruption is known to be dependent on the size, location and timing of the eruption. However, the chemistry and composition of the volcanic plume also control its impact on climate. It is not just sulfur dioxide gas, but also the coincident emissions of water, halogens and ash that influence the radiative and climate forcing of an eruption. Improvements in the capability of models to capture aerosol microphysics, and the inclusion of chemistry and aerosol microphysics modules in Earth system models, allow us to evaluate the interaction of composition and chemistry within volcanic plumes in a new way. These modelling efforts also illustrate the role of water vapour in controlling the chemical evolution - and hence climate impacts - of the plume. A growing realization of the importance of the chemical composition of volcanic plumes is leading to a more sophisticated and realistic representation of volcanic forcing in climate simulations, which in turn aids in reconciling simulations and proxy reconstructions of the climate impacts of past volcanic eruptions. More sophisticated simulations are expected to help, eventually, with predictions of the impact on the Earth system of any future large volcanic eruptions. C1 [LeGrande, Allegra N.; Tsigaridis, Kostas; Bauer, Susanne E.] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. [Tsigaridis, Kostas; Bauer, Susanne E.] Columbia Univ, Ctr Climate Syst Res, 2880 Broadway, New York, NY USA. RP LeGrande, AN (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM allegra.n.legrande@nasa.gov; kostas.tsigaridis@columbia.edu FU NASA High-End Computing (HEC) Program through the NASA Center for Climate Simulation (NCCS) at Goddard Space Flight Center FX We thank NASA GISS for institutional support. We also thank the NASA MAP programme for continued support. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Center for Climate Simulation (NCCS) at Goddard Space Flight Center. NR 50 TC 3 Z9 3 U1 14 U2 14 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 SEP PY 2016 VL 9 IS 9 BP 652 EP 655 DI 10.1038/NGEO2771 PG 4 WC Geosciences, Multidisciplinary SC Geology GA DV9TA UT WOS:000383283700006 ER PT J AU Wooden, DH Cook, AM Colaprete, A Glenar, DA Stubbs, TJ Shirley, M AF Wooden, D. H. Cook, A. M. Colaprete, A. Glenar, D. A. Stubbs, T. J. Shirley, M. TI Evidence for a dynamic nanodust cloud enveloping the Moon SO NATURE GEOSCIENCE LA English DT Article ID GENERATED DUST CLOUDS; HYPERVELOCITY IMPACTS; PLANETARY SATELLITES; COMET P/HALLEY; SURFACES; SPACE; FE AB The exospheres that surround airless bodies such as the Moon are tenuous, atmosphere-like layers whose constituent particles rarely collide with one another. Some particles contained within such exospheres are the product of direct interactions between airless bodies and the space environment, and offer insights into space weathering processes. NASA's Lunar Atmosphere and Dust Environment Explorer (LADEE) mission studied the Moon's exospheric constituents in situ and detected a permanent dust exosphere(1) of particles with radii as small as 300 nm. Here we present evidence from LADEE spectral data for an additional fluctuating nanodust exosphere at the Moon containing a population of particles sufficiently dense to be detectable via scattered sunlight. We compare two anti-Sun spectral observations: one near the peak of the Quadrantid meteoroid stream, the other during a period of comparatively weak stream activity. The former shows a negative spectral slope consistent with backscattering of sunlight by nanodust grains with radii less than 20 to 30 nm; the latter has a flatter spectral slope. We hypothesize that a spatially and temporally variable nanodust exosphere may exist at the Moon, and that it is modulated by changes in meteoroid impact rates, such as during encounters with meteoroid streams. The findings suggest that similar nanodust exospheres-and the particle ejection and transport processes that form them-may occur at other airless bodies. C1 [Wooden, D. H.; Cook, A. M.; Colaprete, A.; Shirley, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Cook, A. M.] Millenium Engn & Integrat Co, 350 North Akron Rd Bldg 19,Suite 2080, Moffett Field, CA 94035 USA. [Glenar, D. A.] Univ Maryland Baltimore Cty, 1000 Hilltop Circle, Baltimore, MD 21250 USA. [Stubbs, T. J.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. RP Wooden, DH (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM diane.wooden@nasa.gov RI Stubbs, Timothy/I-5139-2013 OI Stubbs, Timothy/0000-0002-5524-645X FU NASA Lunar Quest Program; LADEE Guest Observer Program; NASA's Science Mission Directorate FX LADEE UVS was supported through the NASA Lunar Quest Program. The authors also acknowledge financial support from the LADEE Guest Observer Program and NASA's Science Mission Directorate. NR 29 TC 0 Z9 0 U1 5 U2 5 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 SEP PY 2016 VL 9 IS 9 BP 665 EP + DI 10.1038/NGEO2779 PG 7 WC Geosciences, Multidisciplinary SC Geology GA DV9TA UT WOS:000383283700008 ER PT J AU Dhakal, B Nicholson, DE Saleeb, AF Padula, SA Vaidyanathan, R AF Dhakal, B. Nicholson, D. E. Saleeb, A. F. Padula, S. A., II Vaidyanathan, R. TI Three-dimensional deformation response of a NiTi shape memory helical-coil actuator during thermomechanical cycling: experimentally validated numerical model SO SMART MATERIALS AND STRUCTURES LA English DT Article DE experimental validation; NiTi; multi-axial; shape memory alloy; thermal cycling; helical-coil actuators; springs ID PERFORMANCE-CHARACTERISTICS; CONSTITUTIVE MODEL; ALLOYS; TRANSFORMATION; EVOLUTION; PHASE AB Shape memory alloy (SMA) actuators often operate under a complex state of stress for an extended number of thermomechanical cycles in many aerospace and engineering applications. Hence, it becomes important to account for multi-axial stress states and deformation characteristics (which evolve with thermomechanical cycling) when calibrating any SMA model for implementation in large-scale simulation of actuators. To this end, the present work is focused on the experimental validation of an SMA model calibrated for the transient and cyclic evolutionary behavior of shape memory Ni49.9Ti50.1, for the actuation of axially loaded helical-coil springs. The approach requires both experimental and computational aspects to appropriately assess the thermomechanical response of these multi-dimensional structures. As such, an instrumented and controlled experimental setup was assembled to obtain temperature, torque, degree of twist and extension, while controlling end constraints during heating and cooling of an SMA spring under a constant externally applied axial load. The computational component assesses the capabilities of a general, multi-axial, SMA material-modeling framework, calibrated for Ni49.9Ti50.1 with regard to its usefulness in the simulation of SMA helical-coil spring actuators. Axial extension, being the primary response, was examined on an axially-loaded spring with multiple active coils. Two different conditions of end boundary constraint were investigated in both the numerical simulations as well as the validation experiments: Case (1) where the loading end is restrained against twist (and the resulting torque measured as the secondary response) and Case (2) where the loading end is free to twist (and the degree of twist measured as the secondary response). The present study focuses on the transient and evolutionary response associated with the initial isothermal loading and the subsequent thermal cycles under applied constant axial load. The experimental results for the helical-coil actuator under two different boundary conditions are found to be within error to their counterparts in the numerical simulations. The numerical simulation and the experimental validation demonstrate similar transient and evolutionary behavior in the deformation response under the complex, inhomogeneous, multi-axial stress-state and large deformations of the helical-coil actuator. This response, although substantially different in magnitude, exhibited similar evolutionary characteristics to the simple, uniaxial, homogeneous, stress-state of the isobaric tensile tests results used for the model calibration. There was no significant difference in the axial displacement (primary response) magnitudes observed between Cases (1) and (2) for the number of cycles investigated here. The simulated secondary responses of the two cases evolved in a similar manner when compared to the experimental validation of the respective cases. C1 [Dhakal, B.; Saleeb, A. F.] Univ Akron, Dept Civil Engn, 302 Buchtel Common, Akron, OH 44325 USA. [Nicholson, D. E.; Vaidyanathan, R.] Univ Cent Florida, Dept Mat Sci & Engn, Dept Mech & Aerosp Engn, 4000 Cent Florida Blvd, Orlando, FL 32816 USA. [Padula, S. A., II] NASA, Glenn Res Ctr, 21000 Brookpark Rd, Cleveland, OH 44135 USA. RP Dhakal, B (reprint author), Univ Akron, Dept Civil Engn, 302 Buchtel Common, Akron, OH 44325 USA. EM bd27@zips.uakron.edu FU Fundamental Aeronautics Program, Fixed-Wing [NNH10ZEA001N-SFW1, NNX11AI57A]; University of Central Florida FX This work was supported by the Fundamental Aeronautics Program, Fixed-Wing, Project No. NNH10ZEA001N-SFW1, Grant No: NNX11AI57A to the University of Akron with the University of Central Florida as Sub Contractor. The authors would like to acknowledge Dr S M Arnold for his technical guidance and programmatic support during the different phases of the project. The authors thank Dr O Benafan for helpful technical discussions regarding the experiments. NR 39 TC 0 Z9 0 U1 7 U2 7 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 SEP PY 2016 VL 25 IS 9 AR 095056 DI 10.1088/0964-1726/25/9/095056 PG 16 WC Instruments & Instrumentation; Materials Science, Multidisciplinary SC Instruments & Instrumentation; Materials Science GA DW9SF UT WOS:000384002200008 ER PT J AU Narapusetty, B Murtugudde, R Wang, H Kumar, A AF Narapusetty, Balachandrudu Murtugudde, Raghu Wang, Hui Kumar, Arun TI Ocean-atmosphere processes driving Indian summer monsoon biases in CFSv2 hindcasts SO CLIMATE DYNAMICS LA English DT Article DE CFSv2 forecast biases; Indian summer monsoon rainfall; Dry-land biases ID WESTERN ARABIAN SEA; INTRASEASONAL OSCILLATIONS; RAINFALL VARIABILITY; GLOBAL PRECIPITATION; ASIAN MONSOON; PREDICTION; CLIMATE; MODEL; DYNAMICS AB This paper analyzes the role of the Indian Ocean (IO) and the atmosphere biases in generating and sustaining large-scale precipitation biases over Central India (CI) during the Indian summer monsoon (ISM) in the climate forecast system version 2 (CFSv2) hindcasts that are produced by initializing the system each month from January 1982 to March 2011. The CFSv2 hindcasts are characterized by a systematic dry monsoon bias over CI that deteriorate with forecast lead-times and coexist with a wet bias in the tropical IO suggesting a large-scale interplay between coupled ocean-atmosphere and land biases. The biases evolving from spring-initialized forecasts are analyzed in detail to understand the evolution of summer biases. The northward migration of the Inter Tropical Convergence Zone (ITCZ) that typically crosses the equator in the IO sector during April in nature is delayed in the hindcasts when the forecast system is initialized in early spring. Our analyses show that the delay in the ITCZ coexists with wind and SST biases and the associated processes project onto the seasonal evolution of the coupled ocean-atmosphere features. This delay in conjunction with the SST and the wind biases during late spring and early summer contributes to excessive precipitation over the ocean and leading to a deficit in rainfall over CI throughout the summer. Attribution of bias to a specific component in a coupled forecast system is particularly challenging as seemingly independent biases from one component affect the other components or are affected by their feedbacks. In the spring-initialized forecasts, the buildup of deeper thermocline in association with warmer SSTs due to the enhanced Ekman pumping in the southwest IO inhibits the otherwise typical northward propagation of ITCZ in the month of April. Beyond this deficiency in the forecasts, two key ocean-atmosphere coupled mechanisms are identified; one in the Arabian Sea, where a positive windstress curl bias in conjunction with warmer SSTs lead to a weakening of Findlater jet and the other in the east equatorial IO where a remote forcing by the predominantly westerly bias in the western-central equatorial IO in the summer strengthen the seasonal downwelling Kelvin wave that in turn deepens the thermocline in the eastern IO. The equatorial Kelvin wave continues as a coastal Kelvin wave and disperses as Rossby waves off Sumatra and induces positive SST and precipitation biases in the eastern and southern Bay of Bengal. This study shows that the biases that first appear in winds lead to a cascade of coupled processes that exacerbate the subsequent biases by modulating the evolution of seasonal processes such as the annual Kelvin and Rossby waves and the cross-equatorial vertically integrated moisture transport. While this analysis does not offer any particular insights into improving the ISM forecasts, it is a foundational first step towards this goal. C1 [Narapusetty, Balachandrudu; Murtugudde, Raghu] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Narapusetty, Balachandrudu] NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wang, Hui] INNOVIM, College Pk, MD USA. [Wang, Hui] NOAA, NCEP, Climate Predict Ctr, College Pk, MD USA. [Kumar, Arun] NOAA, NWS, NCEP, Climate Predict Ctr, College Pk, MD USA. RP Narapusetty, B (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.; Narapusetty, B (reprint author), NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM bnarapus@umd.edu FU Earth System Science Organization, Ministry of Earth Sciences, Government of India [MM/SERP/Univ_Maryland_USA/2013/INT-16/002] FX The authors gratefully acknowledge the financial support given by the Earth System Science Organization, Ministry of Earth Sciences, Government of India (MM/SERP/Univ_Maryland_USA/2013/INT-16/002) to conduct this research under Monsoon Mission. The authors also acknowledge Dr. Krishnan, Dr. Rajeevan, Dr. Shukla, and Dr. Kinter for helpful comments and discussions. NR 48 TC 0 Z9 0 U1 3 U2 3 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 EI 1432-0894 J9 CLIM DYNAM JI Clim. Dyn. PD SEP PY 2016 VL 47 IS 5-6 BP 1417 EP 1433 DI 10.1007/s00382-015-2910-9 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DU3LK UT WOS:000382112000005 ER PT J AU Stanfield, RE Jiang, JH Dong, XQ Xi, BK Su, H Donner, L Rotstayn, L Wu, TW Cole, J Shindo, E AF Stanfield, Ryan E. Jiang, Jonathan H. Dong, Xiquan Xi, Baike Su, Hui Donner, Leo Rotstayn, Leon Wu, Tongwen Cole, Jason Shindo, Eiki TI A quantitative assessment of precipitation associated with the ITCZ in the CMIP5 GCM simulations SO CLIMATE DYNAMICS LA English DT Article DE GCM; Global climate models; GCM precipitation; Model precipitation; AMIP; CMIP; CMIP5; Climate change; ITCZ; GCM bias ID GENERAL-CIRCULATION MODEL; PACIFIC COLD-TONGUE; LARGE-SCALE MODELS; INCLUDING MASS FLUXES; GLOBAL CLIMATE MODEL; EARTH SYSTEM MODEL; NASA GISS CMIP5; PART I; CUMULUS CONVECTION; RAINFALL PRODUCTS AB According to the Intergovernmental Panel on Climate Change 5th Assessment Report, the broad-scale features of precipitation as simulated by Phase 5 of the Coupled Model Intercomparison Project (CMIP5) are in modest agreement with observations, however, large systematic errors are found in the Tropics. In this study, a new algorithm has been developed to define the North Pacific Intertropical Convergence Zone (ITCZ) through several metrics, including: the centerline position of the ITCZ, the width of the ITCZ, and the magnitude of precipitation along the defined ITCZ. These metrics provide a quantitative analysis of precipitation associated with the ITCZ over the equatorial northern Pacific. Results from 29 CMIP5 Atmospheric Model Intercomparison Project (AMIP) Global Circulation Model (GCM) runs are compared with Global Precipitation Climatology Project (GPCP) and Tropical Rainfall Measuring Mission (TRMM) observations. Similarities and differences between the GCM simulations and observations are analyzed with the intent of quantifying magnitude-, location-, and width-based biases within the GCMs. Comparisons show that most of the GCMs tend to simulate a stronger, wider ITCZ shifted slightly northward compared to the ITCZ in GPCP and TRMM observations. Comparisons of CMIP and AMIP simulated precipitation using like-models were found to be nearly equally distributed, with roughly half of GCMs showing an increase (decrease) in precipitation when coupled (decoupled) from their respective ocean model. Further study is warranted to understand these differences. C1 [Stanfield, Ryan E.; Dong, Xiquan; Xi, Baike] Univ North Dakota, Dept Atmospher Sci, 4149 Univ Ave Stop 9006, Grand Forks, ND 58202 USA. [Jiang, Jonathan H.; Su, Hui] Jet Prop Lab, Pasadena, CA USA. [Donner, Leo] Geophys Fluid Dynam Lab, Princeton, NJ USA. [Rotstayn, Leon] CSIRO, Clayton, Vic, Australia. [Wu, Tongwen] China Meteorol Adm, Beijing Climate Ctr, Beijing, Peoples R China. [Cole, Jason] Environm Canada, Canadian Ctr Climate Modeling & Anal, Toronto, ON, Canada. [Shindo, Eiki] Japan Meteorol Agcy, Meteorol Res Inst, Tsukuba, Ibaraki, Japan. RP Dong, XQ (reprint author), Univ North Dakota, Dept Atmospher Sci, 4149 Univ Ave Stop 9006, Grand Forks, ND 58202 USA. EM dong@aero.und.edu FU Jet Propulsion Laboratory (JPL), California Institute of Technology under NASA; NASA CERES [NNX14AP84G]; EPSCoR projects; NASA [ROSES12-MAP, ROSE13-NDOA] FX We would like to acknowledge the contributions made by Trond Iversen, for providing information and references on the NorESM model, and the contributions made by Cyril Morcrette, for his comments and suggestions related to HadGEM2-A model. The authors acknowledge the support by the Jet Propulsion Laboratory (JPL), California Institute of Technology under contract with NASA. The researchers at University of North Dakota were supported by NASA CERES (NNX14AP84G) and EPSCoR projects, and the researchers at JPL were supported by NASA ROSES12-MAP and ROSE13-NDOA projects. Data were obtained from the CMIP5 ESGF PCMDI database at http://pcmdi9.llnl.gov/esgf-web-fe/. GPCP and TRMM data are also provided by the Obs4MIPS program and are available as well from the ESGF PCMDI database at http://pcmdi9.llnl.gov/esgf-web-fe/. The GPCP SG combined precipitation data were developed and computed at the NASA/Goddard Space Flight Center's Mesoscale Atmospheric Processes Laboratory - Atmospheres as a contribution to the GEWEX Global Precipitation Climatology Project. NR 64 TC 0 Z9 0 U1 7 U2 7 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 EI 1432-0894 J9 CLIM DYNAM JI Clim. Dyn. PD SEP PY 2016 VL 47 IS 5-6 BP 1863 EP 1880 DI 10.1007/s00382-015-2937-y PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DU3LK UT WOS:000382112000031 ER PT J AU Abdi, AM Vrieling, A Yengoh, GT Anyamba, A Seaquist, JW Ummenhofer, CC Ardo, J AF Abdi, A. M. Vrieling, A. Yengoh, G. T. Anyamba, A. Seaquist, J. W. Ummenhofer, C. C. Ardo, J. TI The El Nio - La Nia cycle and recent trends in supply and demand of net primary productivity in African drylands SO CLIMATIC CHANGE LA English DT Article DE Sub-Saharan Africa; Drylands; El Nino-southern oscillation; Net primary productivity; Climate variability ID FOOD INSECURITY; CLIMATE; ECOSYSTEMS; PATTERNS; RAINFALL; ETHIOPIA; CHARCOAL; ENSO AB Inter-annual climatic variability over a large portion of sub-Saharan Africa is under the influence of the El Nio-Southern Oscillation (ENSO). Extreme variability in climate is a threat to rural livelihoods in sub-Saharan Africa, yet the role of ENSO in the balance between supply and demand of net primary productivity (NPP) over this region is unclear. Here, we analyze the impact of ENSO on this balance in a spatially explicit framework using gridded population data from the WorldPop project, satellite-derived data on NPP supply, and statistical data from the United Nations. Our analyses demonstrate that between 2000 and 2013 fluctuations in the supply of NPP associated with moderate ENSO events average +/- 2.8 g C m(-2) yr.(-1) across sub-Saharan drylands. The greatest sensitivity is in arid Southern Africa where a + 1 A degrees C change in the Nio-3.4 sea surface temperature index is associated with a mean change in NPP supply of -6.6 g C m(-2) yr.(-1). Concurrently, the population-driven trend in NPP demand averages 3.5 g C m(-2) yr.(-1) over the entire region with densely populated urban areas exhibiting the highest mean demand for NPP. Our findings highlight the importance of accounting for the role ENSO plays in modulating the balance between supply and demand of NPP in sub-Saharan drylands. An important implication of these findings is that increase in NPP demand for socio-economic metabolism must be taken into account within the context of climate-modulated supply. C1 [Abdi, A. M.; Seaquist, J. W.; Ardo, J.] Lund Univ, Dept Phys Geog & Ecosyst Sci, Solvegatan 12, S-22362 Lund, Sweden. [Vrieling, A.] Univ Twente, Fac Geoinformat Sci & Earth Observat, POB 217, NL-7500 AE Enschede, Netherlands. [Yengoh, G. T.] Lund Univ, Ctr Sustainabil Studies, S-22362 Lund, Sweden. [Anyamba, A.] Natl Aeronaut & Space Adm, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD USA. [Ummenhofer, C. C.] Woods Hole Oceanog Inst, Dept Phys Oceanog, Woods Hole, MA 02543 USA. RP Abdi, AM (reprint author), Lund Univ, Dept Phys Geog & Ecosyst Sci, Solvegatan 12, S-22362 Lund, Sweden. EM hakim.abdi@gmail.com RI Vrieling, Anton/B-2639-2012; OI Vrieling, Anton/0000-0002-7979-1540; Abdi, PhD, Abdulhakim/0000-0001-6486-8747 FU Swedish National Space Board [100/11]; Royal Physiographic Society in Lund; Lund University Center for Studies of Carbon Cycle and Climate Interactions (LUCCI); NSF [OCE-1203892] FX We thank Dan Metcalfe, Lina Eklund, A.J. (Han) Dolman, and Katharina Waha for their insight and comments during early stages of the manuscript. We also thank the programming assistance provided by the volunteers at the Stack Overflow and Cross Validated online communities. Funding for this project was provided by the Swedish National Space Board (contract no. 100/11 to J.A.). A.M.A. received support from the Royal Physiographic Society in Lund and the Lund University Center for Studies of Carbon Cycle and Climate Interactions (LUCCI). C.C.U. was supported by NSF grant OCE-1203892. NR 49 TC 0 Z9 0 U1 14 U2 14 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0165-0009 EI 1573-1480 J9 CLIMATIC CHANGE JI Clim. Change PD SEP PY 2016 VL 138 IS 1-2 BP 111 EP 125 DI 10.1007/s10584-016-1730-1 PG 15 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA DU3UT UT WOS:000382138400009 ER PT J AU Morgan, D Subramanian, GP Chung, SJ Hadaegh, FY AF Morgan, Daniel Subramanian, Giri P. Chung, Soon-Jo Hadaegh, Fred Y. TI Swarm assignment and trajectory optimization using variable-swarm, distributed auction assignment and sequential convex programming SO INTERNATIONAL JOURNAL OF ROBOTICS RESEARCH LA English DT Article ID FORMATION FLYING GUIDANCE; MODEL-PREDICTIVE CONTROL; SATELLITE CLUSTERS; MULTIPLE ROBOTS; SPACECRAFT; ALGORITHM; STRATEGIES; OPTIMALITY; NETWORKS AB This paper presents a distributed, guidance and control algorithm for reconfiguring swarms composed of hundreds to thousands of agents with limited communication and computation capabilities. This algorithm solves both the optimal assignment and collision-free trajectory generation for robotic swarms, in an integrated manner, when given the desired shape of the swarm ( without pre-assigned terminal positions). The optimal assignment problem is solved using a distributed auction assignment that can vary the number of target positions in the assignment, and the collision-free trajectories are generated using sequential convex programming. Finally, model predictive control is used to solve the assignment and trajectory generation in real time using a receding horizon. The model predictive control formulation uses current state measurements to resolve for the optimal assignment and trajectory. The implementation of the distributed auction algorithm and sequential convex programming using model predictive control produces the swarm assignment and trajectory optimization ( SATO) algorithm that transfers a swarm of robots or vehicles to a desired shape in a distributed fashion. Once the desired shape is uploaded to the swarm, the algorithm determines where each robot goes and how it should get there in a fuel-efficient, collision-free manner. Results of flight experiments using multiple quadcopters show the effectiveness of the proposed SATO algorithm. C1 [Morgan, Daniel; Subramanian, Giri P.; Chung, Soon-Jo] Univ Illinois, Urbana, IL USA. [Hadaegh, Fred Y.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Chung, SJ (reprint author), Univ Illinois, Dept Aerosp Engn, Urbana, IL 61801 USA.; Chung, SJ (reprint author), Univ Illinois, Coordinated Sci Lab, Urbana, IL 61801 USA. EM sjchung@illinois.edu FU National Aeronautics and Space Administration; NASA Office of the Chief Technologist Space Technology Research Fellowship; Air Force Office of Scientific Research (AFOSR) [FA95501210193] FX This research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. (C)2016 California Institute of Technology. This work was supported by a NASA Office of the Chief Technologist Space Technology Research Fellowship and an Air Force Office of Scientific Research (AFOSR grant number FA95501210193). Government sponsorship acknowledged. NR 43 TC 1 Z9 1 U1 7 U2 7 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0278-3649 EI 1741-3176 J9 INT J ROBOT RES JI Int. J. Robot. Res. PD SEP PY 2016 VL 35 IS 10 BP 1261 EP 1285 DI 10.1177/0278364916632065 PG 25 WC Robotics SC Robotics GA DV5PY UT WOS:000382981300006 ER PT J AU Schonberg, WP Hull, SM AF Schonberg, William P. Hull, Scott M. TI Current Design Criteria for MMOD Impact of Metallic Pressurized Tanks SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article ID HYPERVELOCITY IMPACT; VESSELS AB Most spacecraft have at least one pressurized vessel on board. For robotic spacecraft, it is usually a liquid propellant tank or battery. For human spacecraft, there are also pressurized living quarters and life-support systems. One of the design considerations of such spacecraft is the possible damage that might occur in the event of an on-orbit impact by a micrometeoroid or orbital debris (MMOD) particle. While considerable energy and effort has been expended in the study of the response of nonpressurized spacecraft components to these kinds of impacts, relatively few studies have been conducted on the pressurized elements of such spacecraft. In addition, the design criteria currently used by the National Aeronautics and Space Administration (NASA) for pressurized tanks operating in the MMOD environment have not been tested or scrutinized since they were first proposed nearly 45 years ago. This paper reviews current NASA design criteria for pressurized vessels and offers suggestions for next steps in their further development. (C) 2016 American Society of Civil Engineers. C1 [Schonberg, William P.] Missouri Univ Sci & Technol, Dept Civil Architectural & Environm Engn, 1401 N Pine St, Rolla, MO 65409 USA. [Hull, Scott M.] NASA, Goddard Space Flight Ctr, Mission Engn & Syst Anal Div, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. RP Schonberg, WP (reprint author), Missouri Univ Sci & Technol, Dept Civil Architectural & Environm Engn, 1401 N Pine St, Rolla, MO 65409 USA. EM wschon@mst.edu FU NASA/Jet Propulsion Laboratory; NASA/Engineering Safety Center FX The authors wish to extend their gratitude to the NASA/Jet Propulsion Laboratory and the NASA/Engineering Safety Center for providing the support that made this study possible. NR 24 TC 0 Z9 0 U1 1 U2 1 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0893-1321 EI 1943-5525 J9 J AEROSPACE ENG JI J. Aerosp. Eng. PD SEP PY 2016 VL 29 IS 5 DI 10.1061/(ASCE)AS.1943-5525.0000635 PG 4 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA DV7VJ UT WOS:000383145800024 ER PT J AU Salinas, A Altecor, A Lizcano, M Lozano, K AF Salinas, A. Altecor, A. Lizcano, M. Lozano, K. TI Production of beta-Silicon Carbide Nanofibers using the Forcespinning (R) Method SO JOURNAL OF CERAMIC SCIENCE AND TECHNOLOGY LA English DT Article DE Silicon carbide; high-temperature materials; ceramic nanofibers; Forcespinning (R) ID FIBERS; NANOWIRES AB Silicon carbide (SiC) nanofibers were produced on a large scale using the Forcespinning (R) method. Non-oxide ceramics such as SiC are known for their low density, oxidation resistance, thermal stability, and wear resistance. The nanofibers were prepared using a solution-based method with polystyrene and polycarbomethylsilane as the precursor materials. Fiber spinning was performed under different parameters to obtain high yield, fiber homogeneity, and small diameters. The fibers were spun under a controlled nitrogen environment to prevent fiber oxidation. The resultant nonwoven nanofiber mats were then subjected to different heat treatments to evaluate the effect of these on the crystalline structure. Characterization was conducted using scanning electron microscopy, x-ray diffraction, and thermogravimetric analysis. The results show high yield, semi-continuous bead-free nanofibers with diameters ranging from 280 nm to 2 micron depending on the selected processing parameters. The sintered precursors show formation of SiC nanofibers with a beta phase crystalline structure and oxygen content below 15 %. C1 [Salinas, A.; Altecor, A.; Lozano, K.] Univ Texas Pan Amer, Dept Mech Engn, Edinburg, TX 78539 USA. [Lizcano, M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Salinas, A (reprint author), Univ Texas Pan Amer, Dept Mech Engn, Edinburg, TX 78539 USA. EM asalinasz73@broncs.utpa.edu FU National Science Foundation under DMR grant [1523577] FX The authors gratefully acknowledge financial support received from the National Science Foundation under DMR grant No. 1523577 (PREM- UTRGV-UMN Partnership for Fostering Innovation by Bridging Excellence in Research and Student Success). We are also grateful to the Biology Department at the University of Texas Rio Grande Valley for allowing use of the EDS instrument. NR 26 TC 0 Z9 0 U1 5 U2 5 PU GOLLER VERLAG GMBH PI BADEN BADEN PA ASCHMATTSTRASSE 8, D-76532 BADEN BADEN, GERMANY SN 2190-9385 J9 J CERAM SCI TECHNOL JI J. Ceram. Sci. Technol. PD SEP PY 2016 VL 7 IS 3 BP 229 EP 234 DI 10.4416/JCST2016-00026 PG 6 WC Materials Science, Ceramics SC Materials Science GA DW0FO UT WOS:000383316500002 ER PT J AU Li, T Calvo, N Yue, J Russell, JM Smith, AK Mlynczak, MG Chandran, A Dou, XK Liu, AZ AF Li, Tao Calvo, Natalia Yue, Jia Russell, James M., III Smith, Anne K. Mlynczak, Martin G. Chandran, Amal Dou, Xiankang Liu, Alan Z. TI Southern Hemisphere Summer Mesopause Responses to El Nino-Southern Oscillation SO JOURNAL OF CLIMATE LA English DT Article ID STRATOSPHERE; ATMOSPHERE; MIDDLE; MODEL; TEMPERATURES; CIRCULATION; ENSO AB In the Southern Hemisphere (SH) polar region, satellite observations reveal a significant upper-mesosphere cooling and a lower-thermosphere warming during warm ENSO events in December. An opposite pattern is observed in the tropical mesopause region. The observed upper-mesosphere cooling agrees with a climate model simulation. Analysis of the simulation suggests that enhanced planetary wave (PW) dissipation in the Northern Hemisphere (NH) high-latitude stratosphere during El Nino strengthens the Brewer-Dobson circulation and cools the equatorial stratosphere. This increases the magnitude of the SH stratosphere meridional temperature gradient and thus causes the anomalous stratospheric easterly zonal wind and early breakdown of the SH stratospheric polar vortex. The resulting perturbation to gravity wave (GW) filtering causes anomalous SH mesospheric eastward GW forcing and polar upwelling and cooling. In addition, constructive inference of ENSO and quasi-biennial oscillation (QBO) could lead to stronger stratospheric easterly zonal wind anomalies at the SH high latitudes in November and December and early breakdown of the SH stratospheric polar vortex during warm ENSO events in the easterly QBO phase (defined by the equatorial zonal wind at similar to 25 hPa). This would in turn cause much more SH mesospheric eastward GW forcing and much colder polar temperatures, and hence it would induce an early onset time of SH summer polar mesospheric clouds (PMCs). The opposite mechanism occurs during cold ENSO events in the westerly QBO phase. This implies that ENSO together with QBO could significantly modulate the breakdown time of SH stratospheric polar vortex and the onset time of SH PMC. C1 [Li, Tao; Dou, Xiankang] Univ Sci & Technol China, Sch Earth & Space Sci, CAS Key Lab Geospace Environm, Hefei 230026, Anhui, Peoples R China. [Li, Tao; Dou, Xiankang] Univ Sci & Technol China, Sch Earth & Space Sci, Mengcheng Natl Geophys Observ, Hefei 230026, Anhui, Peoples R China. [Calvo, Natalia] Univ Complutense Madrid, Dept Fis Tierra 2, Madrid, Spain. [Yue, Jia; Russell, James M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. [Smith, Anne K.] Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA. [Mlynczak, Martin G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Chandran, Amal] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Liu, Alan Z.] Embry Riddle Aeronaut Univ, Dept Phys Sci, Daytona Beach, FL 32114 USA. RP Li, T (reprint author), Univ Sci & Technol China, Sch Earth & Space Sci, 96 Jinzhai Rd, Hefei 230026, Anhui, Peoples R China. EM litao@ustc.edu.cn RI Dou, xiankang/M-9106-2013; Yue, Jia/D-8177-2011; Li, Tao/J-8950-2014 OI Li, Tao/0000-0002-5100-4429 FU National Natural Science Foundation of China [41225017, 41421063]; National Basic Research Program of China [2012CB825605]; NSF [AGS-1115249, AGS-1110199]; Spanish Ministry of Economy and Competitiveness through the PALEOSTRAT project [CGL2015-69699-R]; European Project under program [603557-STRATOCLIM, FP7-ENV.2013.6.1-2]; NASA AIM satellite mission; NASA TIMED satellite mission; NASA SABER Grant [NNX15AD22G]; NASA TIMED satellite project; National Science Foundation [AGS-1115249, AGS-1110199] FX TL would like to thank Han-Li Liu and Chengyun Yang for helpful discussion. TL and XD are supported by the National Natural Science Foundation of China Grants 41225017 and 41421063 and the National Basic Research Program of China Grant 2012CB825605. TL's visit to ERAU is partially supported by the NSF Grants AGS-1115249 and AGS-1110199. NC acknowledges partial support from the Spanish Ministry of Economy and Competitiveness through the PALEOSTRAT project (Paleomodelization desde una perspective estratoferica; Ref. CGL2015-69699-R) and the European Project 603557-STRATOCLIM under program FP7-ENV.2013.6.1-2. JY is supported by the NASA AIM and TIMED satellite missions. JMR is supported under NASA SABER Grant NNX15AD22G. MGM is supported by the NASA TIMED satellite project. AZL is supported by National Science Foundation Grants AGS-1115249 and AGS-1110199. The WACCM 3.5 results were obtained from the Atmospheric Chemistry Division at the National Center for Atmospheric Research. The radiosonde dataset is downloaded from http://www.geo.fu-berlin.de/en/met/ag/strat/produkte/qbo/index.html. We want to thank Bodil Karlsson and two other anonymous reviewers for their constructive comments on this paper. NR 28 TC 1 Z9 1 U1 5 U2 5 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD SEP 1 PY 2016 VL 29 IS 17 BP 6319 EP 6328 DI 10.1175/JCLI-D-15-0816.1 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DV3DO UT WOS:000382801400016 ER PT J AU Russell, RP Lantukh, D Broschart, SB AF Russell, Ryan P. Lantukh, Demyan Broschart, Stephen B. TI Heliotropic Orbits with Zonal Gravity and Shadow Perturbations: Application at Bennu SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID SOLAR-RADIATION PRESSURE; ASTEROID 101955 BENNU; PLANETARY OBLATENESS; EVEN HARMONICS; DUST DYNAMICS; SATELLITE; DENSITY; MOTION AB Heliotropic orbits provide long-lifetime low-altitude orbits in the presence of large J2 and solar radiation pressure perturbations. Formal inclusion of high-degree zonal gravity harmonics and simple shadowing provides a more realistic model to initiate the search for heliotropic orbits at irregular primitive bodies like Bennu, which is the target of the OSIRIS-Rex mission. The constrained, doubly averaged potential and the Lagrange planetary equations yield a single equation to enforce the heliotropic constraint. The equation is solved for inclinations across a range of semimajor axes and eccentricities, providing a surface of potential solutions. The fast process allows for MonteCarlo simulations to assess the likelihood of a heliotropic orbit existing in the presence of parameter uncertainty. The existence of heliotropic orbits is shown to be reasonably robust to uncertainty in the solar radiation pressure acceleration and reference gravity parameters for Bennu. C1 [Russell, Ryan P.; Lantukh, Demyan] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA. [Broschart, Stephen B.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Russell, RP (reprint author), Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA. EM ryan.russell@utexas.edu; demyan@utexas.edu; Stephen.B.Broschart@jpl.nasa.gov FU NASA Office of the Chief Technologist via a NASA Space Technology Research Fellowship [NNX12AI77H]; W. M. Keck Foundation; NASA FX This work was supported in part by the NASA Office of the Chief Technologist via a NASA Space Technology Research Fellowship grant (NNX12AI77H). In particular, the authors thank Claudia Meyer for continued interest and support of the project. The authors also thank the W. M. Keck Foundation for supporting, in part, the presented work through the W. M. Keck Foundation Endowed Graduate Fellowship in Engineering. Part of the work described here was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 22 TC 0 Z9 0 U1 2 U2 2 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 SEP PY 2016 VL 39 IS 9 BP 1925 EP 1933 DI 10.2514/1.G001279 PG 9 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA DV9LH UT WOS:000383261500001 ER PT J AU Swei, SSM Fusco, JC Nakamura, RH AF Swei, Sean S. M. Fusco, Jesse C. Nakamura, Robert H. TI Design of Sun-Safe Controllers for Lunar Atmosphere and Dust Environment Explorer SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article AB This paper presents the development of sun-safe controllers, which are designed to keep the spacecraft power positive and thermally balanced in the event an anomaly is detected. Employed by NASA's Lunar Atmosphere and Dust Environment Explorer, the controllers use the measured sun vector and the spacecraft body rates for feedback control. To improve the accuracy of sun vector estimation, the least-square minimization approach is applied to process the sensor data. A rotation with respect to the sun vector, which is proven to be effective in mitigating the momentum buildup due to the lunar gravity gradient, hence significantly extending the sun-safe duration, is commanded. To validate the controllers, the Lunar Atmosphere and Dust Environment Explorer spacecraft model engaging the sun-safe mode is first simulated and then compared with the actual Lunar Atmosphere and Dust Environment Explorer orbital flight data. The results demonstrate the applicability of the proposed sun-safe controllers. C1 [Swei, Sean S. M.] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA. [Fusco, Jesse C.; Nakamura, Robert H.] NASA, Ames Res Ctr, Engn Syst Div, Moffett Field, CA 94035 USA. RP Swei, SSM (reprint author), NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA. NR 9 TC 1 Z9 1 U1 0 U2 0 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD SEP PY 2016 VL 39 IS 9 BP 2022 EP 2033 DI 10.2514/1.G000270 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA DV9LH UT WOS:000383261500008 ER PT J AU Sung, K Yu, SS Pearson, J Pirali, O Tchana, FK Manceron, L AF Sung, Keeyoon Yu, Shanshan Pearson, John Pirali, Olivier Tchana, Fridolin Kwabia Manceron, Laurent TI Far-infrared (NH3)-N-14 line positions and intensities measured with a FT-IR and AILES beamline, Synchrotron SOLEIL SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE Ammonia spectroscopy; Ammonia line intensity; NH3 far-infrared transitions; Inversion-rotation; FT-IR measurements; AILES beamline ID SELF-BROADENING COEFFICIENTS; LASER STARK SPECTROSCOPY; MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; ENERGY-LEVELS; NH3; AMMONIA; BANDS; MICROWAVE; STATE AB Extensive measurements of line positions and intensities are reported for the inversion-rotation and rovibrational transitions of (NH3)-N-14 in the 50-660 cm(-1) region. This study analyzes high-resolution (0.00167 cm(-1), unapodized) Fourier-transform spectra of high purity (99.5%) normal ammonia sample obtained using the AILES beamline of Synchrotron SOLEIL. The experimental conditions are designed to study transitions with intensities weaker than 1 x 10(-22) cm(-1)/(molecule cm(-2)) at room temperature. Line positions and intensities of more than 2830 transitions of (NH3)-N-14 are measured and compiled after proper quality control; the features from minor isotopologues ((NH3)-N-15 and NH2D) and H2O are identified and excluded. Based on the predictions of recent work from the empirical Hamiltonian modeling, systematic quantum assignments are made for 2047 transitions from eight bands including four inversion rotation (gs, v(2), 2v(2), and v(4)) and four ro-vibrational bands (v(2)-gs, 2v(2)-v(2), v(4)-v(2), and 2v(2)-v(4)), as well as covering their Delta K = 3 forbidden transitions. The measured line positions for the assigned transitions are in an excellent agreement (typically better than 0.001 cm(-1)) with the predictions in a wide range of J and K for all the eight bands. The comparison with the HITRAN 2012 database is also satisfactory, although systematic offsets are seen for transitions with high J and K and those from weak bands. Also we note that out of the eight bands, the 2v(2)-v(4) has not been listed in the HITRAN 2012 database. Differences of 20% are seen between our measured and calculated intensities depending on the bands. For line positions, greater differences are found for some NH3 bands in HITRAN 2012 than recent predictions. Measurements of the individual line positions and intensities are presented for the eight bands, and the final spectroscopic line positions and intensities are compiled as an electronic supplement. (C) 2016 Elsevier Inc. All rights reserved. C1 [Sung, Keeyoon; Yu, Shanshan; Pearson, John] CALTECH, Jet Prop Lab, M-S 200-105,4800 Oak Grove Dr, Pasadena, CA 91125 USA. [Pirali, Olivier; Manceron, Laurent] LOrme Merisiers St Aubin, Synchrotron SOLEIL, AILES Beamline, F-91192 Gif Sur Yvette, France. [Pirali, Olivier] Univ Paris Saclay, Univ Paris 11, CNRS, ISMO, F-91405 Orsay, France. [Tchana, Fridolin Kwabia] UPEC, CNRS, UMR 7583, LISA, 61 Ave Gen Gaulle, F-94010 Creteil, France. [Tchana, Fridolin Kwabia] UPD, 61 Ave Gen Gaulle, F-94010 Creteil, France. [Manceron, Laurent] Univ Paris 06, CNRS, UMR 8233, MONARIS, Paris, France. RP Sung, K (reprint author), CALTECH, Jet Prop Lab, M-S 200-105,4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM ksung@jpl.nasa.gov RI Yu, Shanshan/D-8733-2016; Sung, Keeyoon/I-6533-2015 FU Synchrotron SOLEIL [2013080]; Astrophysics Research and Analysis (APRA) Program under the National Aeronautics and Space Administration; SOLEIL; LISA FX K. Sung and S. Yu are grateful to Linda R. Brown for useful discussion on the NH3 spectroscopy and designing the experimental study. The JPL authors also acknowledge the Synchrotron SOLEIL for granting us with the AILES beamline time (project #2013080). Research described in this work was performed at Jet Propulsion Laboratory, California Institute of Technology, and was supported by the Astrophysics Research and Analysis (APRA) Program under the National Aeronautics and Space Administration. F.K.T. and L.M. acknowledge SOLEIL and LISA support. NR 64 TC 0 Z9 0 U1 4 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 EI 1096-083X J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD SEP PY 2016 VL 327 SI SI BP 1 EP 20 DI 10.1016/j.jms.2016.06.011 PG 20 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA DV8WY UT WOS:000383218600001 ER PT J AU Orphal, J Staehelin, J Tamminen, J Braathen, G De Backer, MR Bais, A Balis, D Barbe, A Bhartia, PK Birk, M Burkholder, JB Chance, K von Clarmann, T Cox, A Degenstein, D Evans, R Flaud, JM Flittner, D Godin-Beekmann, S Gorshelev, V Gratien, A Hare, E Janssen, C Kyrola, E McElroy, T McPeters, R Pastel, M Petersen, M Petropavlovskikh, I Picquet-Varrault, B Pitts, M Labow, G Rotger-Languereau, M Leblanc, T Lerot, C Liu, X Moussay, P Redondas, A Van Roozendael, M Sander, SP Schneider, M Serdyuchenko, A Veefkind, P Viallon, J Viatte, C Wagner, G Weber, M Wielgosz, RI Zehner, C AF Orphal, Johannes Staehelin, Johannes Tamminen, Johanna Braathen, Geir De Backer, Marie -Renee Bais, Alkiviadis Balis, Dimitris Barbe, Alain Bhartia, Pawan K. Birk, Manfred Burkholder, James B. Chance, Kelly von Clarmann, Thomas Cox, Anthony Degenstein, Doug Evans, Robert Flaud, Jean-Marie Flittner, David Godin-Beekmann, Sophie Gorshelev, Viktor Gratien, Aline Hare, Edward Janssen, Christof Kyrola, Erkki McElroy, Thomas McPeters, Richard Pastel, Maud Petersen, Michael Petropavlovskikh, Irina Picquet-Varrault, Benedicte Pitts, Michael Labow, Gordon Rotger-Languereau, Maud Leblanc, Thierry Lerot, Christophe Liu, Xiong Moussay, Philippe Redondas, Alberto Van Roozendael, Michel Sander, Stanley P. Schneider, Matthias Serdyuchenko, Anna Veefkind, Pepijn Viallon, Joele Viatte, Camille Wagner, Georg Weber, Mark Wielgosz, Robert I. Zehner, Claus TI Absorption cross-sections of ozone in the ultraviolet and visible spectral regions: Status report 2015 SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE Ozone; Absorption; Cross sections; Atmosphere; Remote sensing; Reference data ID 10 MU-M; TEMPERATURE-DEPENDENCE; PROFILE RETRIEVALS; MONITORING INSTRUMENT; UV SPECTROSCOPY; TOTAL COLUMN; STRAY LIGHT; NM REGION; BREWER; O-3 AB The activity "Absorption Cross-Sections of Ozone" (ACSO) started in 2008 as a joint initiative of the International Ozone Commission (IO3C), the World Meteorological Organization (WMO) and the IGACO ("Integrated Global Atmospheric Chemistry Observations") O-3/UV subgroup to study, evaluate, and recommend the most suitable ozone absorption cross-section laboratory data to be used in atmospheric ozone measurements. The evaluation was basically restricted to ozone absorption cross-sections in the UV range with particular focus on the Huggins band. Up until now, the data of Bass and Paur published in 1985 (BP, 1985) are still officially recommended for such measurements. During the last decade it became obvious that BP (1985) cross-section data have deficits for use in advanced space-borne ozone measurements. At the same time, it was recognized that the origin of systematic differences in ground-based measurements of ozone required further investigation, in particular whether the BP (1985) cross-section data might contribute to these differences. In ACSO, different sets of laboratory ozone absorption cross-section data (including their dependence on temperature) of the group of Reims (France) (Brion et al., 1993, 1998, 1992, 1995, abbreviated as BDM, 1995) and those of Serdyuchenko et al. (2014), and Gorshelev et al. (2014), (abbreviated as SER, 2014) were examined for use in atmospheric ozone measurements in the Huggins band. In conclusion, ACSO recommends: The spectroscopic data of BP (1985) should no longer be used for retrieval of atmospheric ozone measurements For retrieval of ground-based instruments of total ozone and ozone profile measurements by the Umkehr method performed by Brewer and Dobson instruments data of SER (2014) are recommended to be used. When SER (2014) is used, the difference between total ozone measurements of Brewer and Dobson instruments are very small and the difference between Dobson measurements at AD and CD wavelength pairs are diminished. For ground-based Light Detection and Ranging (LIDAR) measurements the use of BDM (1995) or SER (2014) is recommended. For satellite retrieval the presently widely used data of BDM (1995) should be used because SER (2014) seems less suitable for retrievals that use wavelengths close to 300 nm due to a deficiency in the signal-to-noise ratio in the SER (2014) dataset. The work of ACSO also showed: The need to continue laboratory cross-section measurements of ozone of highest quality. The importance of careful characterization of the uncertainties of the laboratory measurements. The need to extend the scope of such studies to other wavelength ranges (particularly to cover not only the Huggins band but also the comparison with the mid-infrared region). The need for regular cooperation of experts in spectral laboratory measurements and specialists in atmospheric (ozone) measurements. (C) 2016 Elsevier Inc. All rights reserved. C1 [Orphal, Johannes; von Clarmann, Thomas; Schneider, Matthias] KIT, Inst Meteorol & Climate Res IMK, Karlsruhe, Germany. [Staehelin, Johannes] Swiss Fed Inst Technol, Zurich, Switzerland. [Tamminen, Johanna; Kyrola, Erkki] FMI, Helsinki, Finland. [Braathen, Geir] WMO, Geneva, Switzerland. [De Backer, Marie -Renee; Barbe, Alain; Rotger-Languereau, Maud] CNRS, GSMA, Reims, France. [De Backer, Marie -Renee; Barbe, Alain] Univ Reims, Reims, France. [Bais, Alkiviadis; Balis, Dimitris] Aristotele Univ Thessaloniki, Thessaloniki, Greece. [Bhartia, Pawan K.; McPeters, Richard; Labow, Gordon] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Birk, Manfred; Wagner, Georg] German Aerosp Ctr DLR, Oberpfaffenhofen, Germany. [Evans, Robert; Petropavlovskikh, Irina] Univ Colorado, CIRES, Boulder, CO 80309 USA. [Chance, Kelly; Liu, Xiong] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Cox, Anthony] Univ Cambridge, Cambridge, England. [Degenstein, Doug] Univ Saskatchewan, Saskatoon, SK, Canada. [Flaud, Jean-Marie; Gratien, Aline; Picquet-Varrault, Benedicte] CNRS, LISA, Creteil, France. [Flaud, Jean-Marie; Gratien, Aline; Picquet-Varrault, Benedicte] Univ Paris Est, Creteil, France. [Flittner, David; Pitts, Michael] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Godin-Beekmann, Sophie; Pastel, Maud] CNRS, LATMOS, Paris, France. [Godin-Beekmann, Sophie; Pastel, Maud] UVSQ, Paris, France. [Gorshelev, Viktor; Serdyuchenko, Anna; Weber, Mark] Univ Bremen, Bremen, Germany. [Hare, Edward] Environm Canada, Toronto, ON, Canada. [Janssen, Christof] Univ Paris 06, Sorbonne Univ, LERMA, IPSL, Paris, France. [Janssen, Christof] PSL Res Univ, Observ Paris, Paris, France. [Janssen, Christof] CNRS, Paris, France. [McElroy, Thomas] Univ Toronto, Toronto, ON, Canada. [Petersen, Michael; Moussay, Philippe; Viallon, Joele; Wielgosz, Robert I.] BIPM, Sevres, France. [Leblanc, Thierry; Sander, Stanley P.] NASA, JPL, Pasadena, CA USA. [Lerot, Christophe; Van Roozendael, Michel] Belgian Inst Space Aeron BIRA IASB, Brussels, Belgium. [Redondas, Alberto] State Meteorol Agcy AEMET, Izana, Spain. [Veefkind, Pepijn] KNMI, De Bilt, Netherlands. [Viatte, Camille] CALTECH, Pasadena, CA 91125 USA. [Zehner, Claus] ESA, ESRIN, Frascati, Italy. [Burkholder, James B.] NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO USA. [Petropavlovskikh, Irina] NOAA, Global Monitoring Div, Boulder, CO USA. [Petersen, Michael] Univ Neuchatel, CH-2000 Neuchatel, Switzerland. RP Orphal, J (reprint author), KIT, Inst Meteorol & Climate Res IMK, Karlsruhe, Germany. EM orphal@kit.edu RI Schneider, Matthias/B-1441-2013; Liu, Xiong/P-7186-2014; Bais, Alkiviadis/D-2230-2009; Tamminen, Johanna/D-7959-2014; Manager, CSD Publications/B-2789-2015; OI Liu, Xiong/0000-0003-2939-574X; Bais, Alkiviadis/0000-0003-3899-2001; Tamminen, Johanna/0000-0003-3095-0069; Kyrola, Erkki/0000-0001-9197-9549 FU EU FP7 programme [284421]; NASA [NNX09AJ24G] FX The work of Maud Pastel was performed in the frame of the NORS project (Demonstration Network Of ground-based Remote Sensing Observations in support of the Copernicus Atmospheric Service), funded by the EU FP7 programme under grant agreement no 284421. The work of Irina Petropavlovskikh was supported by NASA Grant No. NNX09AJ24G (Enhancement of ozone products from established Brewer ground-based networks for validation of satellite-derived stratospheric ozone change). Johanna Tamminen would like to thank the Finnish Academy INQUIRE project. NR 76 TC 4 Z9 4 U1 12 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 SEP PY 2016 VL 327 SI SI BP 105 EP 121 DI 10.1016/j.jms.2016.07.007 PG 17 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA DV8WY UT WOS:000383218600006 ER PT J AU Dreessen, J Sullivan, J Delgado, R AF Dreessen, Joel Sullivan, John Delgado, Ruben TI Observations and impacts of transported Canadian wildfire smoke on ozone and aerosol air quality in the Maryland region on June 9-12, 2015 SO JOURNAL OF THE AIR & WASTE MANAGEMENT ASSOCIATION LA English DT Article; Proceedings Paper CT 7th International Workshop on Air Quality Forecasting Research (IWAQFR) CY SEP 01-03, 2015 CL College Park, MD ID VOLATILE ORGANIC-COMPOUNDS; SOUTHERN CALIFORNIA WILDFIRES; FOREST-FIRE EMISSIONS; UNITED-STATES; PARTICULATE MATTER; NITROGEN-OXIDES; CLIMATE-CHANGE; URBAN AREA; BOREAL; POLLUTION AB Canadian wildfire smoke impacted air quality across the northern Mid-Atlantic (MA) of the United States during June 9-12, 2015. A multiday exceedance of the new 2015 70-ppb National Ambient Air Quality Standard (NAAQS) for ozone (O-3) followed, resulting in Maryland being incompliant with the Environmental Protection Agency's (EPA) revised 2015 O-3 NAAQS. Surface in situ, balloon-borne, and remote sensing observations monitored the impact of the wildfire smoke at Maryland air quality monitoring sites. At peak smoke concentrations in Maryland, wildfire-attributable volatile organic compounds (VOCs) more than doubled, while non-NOx oxides of nitrogen (NOz) tripled, suggesting long range transport of NOx within the smoke plume. Peak daily average PM2.5 was 32.5 mu g m(-3) with large fractions coming from black carbon (BC) and organic carbon (OC), with a synonymous increase in carbon monoxide (CO) concentrations. Measurements indicate that smoke tracers at the surface were spatially and temporally correlated with maximum 8-hr O-3 concentrations in the MA, all which peaked on June 11. Despite initial smoke arrival late on June 9, 2015, O-3 production was inhibited due to ultraviolet (UV) light attenuation, lower temperatures, and nonoptimal surface layer composition. Comparison of Community Multiscale Air Quality (CMAQ) model surface O-3 forecasts to observations suggests 14 ppb additional O-3 due to smoke influences in northern Maryland. Despite polluted conditions, observations of a nocturnal low-level jet (NLLJ) and Chesapeake Bay Breeze (BB) were associated with decreases in O-3 in this case. While infrequent in the MA, wildfire smoke may be an increasing fractional contribution to high-O-3 days, particularly in light of increased wildfire frequency in a changing climate, lower regional emissions, and tighter air quality standards.Implications: The presented event demonstrates how a single wildfire event associated with an ozone exceedance of the NAAQS can prevent the Baltimore region from complying with lower ozone standards. This relatively new problem in Maryland is due to regional reductions in NOx emissions that led to record low numbers of ozone NAAQS violations in the last 3 years. This case demonstrates the need for adequate means to quantify and justify ozone impacts from wildfires, which can only be done through the use of observationally based models. The data presented may also improve future air quality forecast models. C1 [Dreessen, Joel] Maryland Dept Environm, Air Monitoring Program, 1800 Washington Blvd, Baltimore, MD 21230 USA. [Sullivan, John] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD USA. [Delgado, Ruben] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. RP Dreessen, J (reprint author), Maryland Dept Environm, Air Monitoring Program, 1800 Washington Blvd, Baltimore, MD 21230 USA. EM joel.dreessen@maryland.gov NR 64 TC 1 Z9 1 U1 19 U2 19 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 1096-2247 EI 2162-2906 J9 J AIR WASTE MANAGE JI J. Air Waste Manage. Assoc. PD SEP PY 2016 VL 66 IS 9 SI SI BP 842 EP 862 DI 10.1080/10962247.2016.1161674 PG 21 WC Engineering, Environmental; Environmental Sciences; Meteorology & Atmospheric Sciences SC Engineering; Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA DV5IE UT WOS:000382959700003 PM 26963934 ER PT J AU Albers, M Zhu, S Ayangeakaa, AD Janssens, RVF Gellanki, J Ragnarsson, I Alcorta, M Baugher, T Bertone, PF Carpenter, MP Chiara, CJ Chowdhury, P David, HM Deacon, AN DiGiovine, B Gade, A Hoffman, CR Kondev, FG Lauritsen, T Lister, CJ McCutchan, EA Nair, C Rogers, AM Seweryniak, D AF Albers, M. Zhu, S. Ayangeakaa, A. D. Janssens, R. V. F. Gellanki, J. Ragnarsson, I. Alcorta, M. Baugher, T. Bertone, P. F. Carpenter, M. P. Chiara, C. J. Chowdhury, P. David, H. M. Deacon, A. N. DiGiovine, B. Gade, A. Hoffman, C. R. Kondev, F. G. Lauritsen, T. Lister, C. J. McCutchan, E. A. Nair, C. Rogers, A. M. Seweryniak, D. TI Single-particle and collective excitations in Ni-62 SO PHYSICAL REVIEW C LA English DT Article ID ROTATIONAL BANDS; TERMINATION; ISOTOPES; NUCLEUS; DECAY AB Background: Level sequences of rotational character have been observed in several nuclei in the A = 60 mass region. The importance of the deformation-driving pi f(7/2) and nu g(9/2) orbitals on the onset of nuclear deformation is stressed. Purpose: A measurement was performed in order to identify collective rotational structures in the relatively neutron-rich Ni-62 isotope. Method: The Mg-26(Ca-48,2 alpha 4n gamma)Ni-62 complex reaction at beam energies between 275 and 320 MeV was utilized. Reaction products were identified in mass (A) and charge (Z) with the fragment mass analyzer (FMA) and gamma rays were detected with the Gammasphere array. Results: Two collective bands, built upon states of single-particle character, were identified and sizable deformation was assigned to both sequences based on the measured transitional quadrupole moments, herewith quantifying the deformation at high spin. Conclusions: Based on cranked Nilsson-Strutinsky calculations and comparisons with deformed bands in the A = 60 mass region, the two rotational bands are understood as being associated with configurations involving multiple f(7/2) protons and g(9/2) neutrons, driving the nucleus to sizable prolate deformation. C1 [Albers, M.; Zhu, S.; Ayangeakaa, A. D.; Janssens, R. V. F.; Alcorta, M.; Bertone, P. F.; Carpenter, M. P.; Chiara, C. J.; David, H. M.; DiGiovine, B.; Hoffman, C. R.; Lauritsen, T.; Lister, C. J.; McCutchan, E. A.; Nair, C.; Rogers, A. M.; Seweryniak, D.] Argonne Natl Lab, Div Phys, Argonne, IL 60439 USA. [Gellanki, J.] Univ Groningen, KVI CART, NL-9747 AA Groningen, Netherlands. [Ragnarsson, I.] Lund Univ, LTH, Div Math Phys, S-22100 Lund, Sweden. [Baugher, T.; Gade, A.] Michigan State Univ, Natl Superconducting Cyclotron Lab, E Lansing, MI 48824 USA. [Baugher, T.; Gade, A.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Chiara, C. J.] Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA. [Chowdhury, P.; Lister, C. J.; Rogers, A. M.] Univ Massachusetts Lowell, Dept Phys, Lowell, MA 01854 USA. [Deacon, A. N.] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Kondev, F. G.] Argonne Natl Lab, Nucl Engn Div, 9700 S Cass Ave, Argonne, IL 60439 USA. [Alcorta, M.] TRIUMF, 4004 Wesbrook Mall, Vancouver, BC V6T 2A3, Canada. [Bertone, P. F.] Marshall Space Flight Ctr, Bldg 4600 Rideout Rd, Huntsville, AL 35812 USA. [Chiara, C. J.] US Army Res Lab, Adelphi, MD 20783 USA. [David, H. M.] GSI Helmholtzzentrum Schwerionenforsch GmbH, D-64291 Darmstadt, Germany. [McCutchan, E. A.] Brookhaven Natl Lab, Natl Nucl Data Ctr, Upton, NY 11973 USA. RP Albers, M (reprint author), Argonne Natl Lab, Div Phys, Argonne, IL 60439 USA. RI Gade, Alexandra/A-6850-2008 OI Gade, Alexandra/0000-0001-8825-0976 FU US Department of Energy, Office of Science, Office of Nuclear Physics [DE-AC02-06CH11357, DE-FG02-94ER40834, DE-FG02-94ER40848, DE-FG02-08ER41556]; National Science Foundation [PHY-1102511]; Swedish Research Council; United Kingdom Science and Technology Facilities Council (STFC) FX The authors thank J. P. Greene (ANL) for target preparation and the ATLAS operations staff for the efficient running of the accelerator during the experiment. This work was supported in part by the US Department of Energy, Office of Science, Office of Nuclear Physics, under Contract No. DE-AC02-06CH11357 and Grant Nos. DE-FG02-94ER40834, DE-FG02-94ER40848, and DE-FG02-08ER41556, by the National Science Foundation under Contract No. PHY-1102511, by the Swedish Research Council, and by the United Kingdom Science and Technology Facilities Council (STFC). This research used resources of ANL's ATLAS facility, which is a DOE Office of Science User Facility. NR 53 TC 0 Z9 0 U1 2 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9985 EI 2469-9993 J9 PHYS REV C JI Phys. Rev. C PD SEP 1 PY 2016 VL 94 IS 3 AR 034301 DI 10.1103/PhysRevC.94.034301 PG 10 WC Physics, Nuclear SC Physics GA DV6KZ UT WOS:000383045700001 ER PT J AU Sherwood, B AF Sherwood, Brent TI Strategic map for exploring the ocean-world Enceladus SO ACTA ASTRONAUTICA LA English DT Article ID PLUME; FUTURE; LIFE AB Among the many "ocean worlds" of our solar system, Enceladus appears unique in its combination of astrobiologically relevant and exploration-worthy attributes: extensive liquid-water ocean with active hydrothermal activity, containing salts and organics expressed predictably into space. The Enceladus south polar plume allows direct access to telltale molecules, ions, isotopes, and potential cytofragments in space. Plume mass spectroscopy and sample return, in situ investigation of surface fallback deposits, direct vent exploration, and eventually oceanographic exploration can all be envisioned. However, building consensus to fund such ambitious exploration hinges on acquiring key new data. A roadmap is essential. It could start with cost-capped onramps such as flythrough analysis of the plume, following up on Cassini measurements with modern instruments; and sample return of plume material for analysis on Earth. A methodical mission sequence in which each step depends on emergent results from prior missions would push in situ oceanographic exploration into the second half of this century. Even for this scenario, prioritization by the next planetary Decadal Survey would be pivotal. (C) 2016 IAA Published by Elsevier Ltd. All rights reserved. C1 [Sherwood, Brent] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. RP Sherwood, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM brent.sherwood@jpl.nasa.gov FU NASA FX The author is grateful to several colleagues who shared insights that were key to formulating the strategic analysis presented here: Linda Spilker, Christophe Sotin, Jonathan Lunine, Kevin Hand, Hunter Waite, Hajime Yano, Peter Tsou, and Carolyn Porco. NR 21 TC 1 Z9 1 U1 9 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD SEP-OCT PY 2016 VL 126 SI SI BP 52 EP 58 DI 10.1016/j.actaastro.2016.04.013 PG 7 WC Engineering, Aerospace SC Engineering GA DU7RL UT WOS:000382412200008 ER PT J AU Nag, S Gatebe, CK Miller, DW de Weck, OL AF Nag, Sreeja Gatebe, Charles K. Miller, David W. de Weck, Olivier L. TI Effect of satellite formations and imaging modes on global albedo estimation SO ACTA ASTRONAUTICA LA English DT Article DE Small satellite; Formation flight; Cubesat; BRDF; Multi-angular; Remote sensing; Constellation ID AIRBORNE SPECTRAL MEASUREMENTS; MISSION; SURFACE; SPACE; CONSTELLATION; ATMOSPHERE; OCEAN AB We confirm the applicability of using small satellite formation flight for multi-angular earth observation to retrieve global, narrow band, narrow field-of-view albedo. The value of formation flight is assessed using a coupled systems engineering and science evaluation model, driven by Model Based Systems Engineering and Observing System Simulation Experiments. Albedo errors are calculated against bi-directional reflectance data obtained from NASA airborne campaigns made by the Cloud Absorption Radiometer for the seven major surface types, binned using MODIS' land cover map water, forest, cropland, grassland, snow, desert and cities. A full tradespace of architectures with three to eight satellites, maintainable orbits and imaging modes (collective payload pointing strategies) are assessed. For an arbitrary 4-sat formation, changing the reference, nadir-pointing satellite dynamically reduces the average albedo error to 0.003, from 0.006 found in the static reference case. Tracking pre-selected waypoints with all the satellites reduces the average error further to 0.001, allows better polar imaging and continued operations even with a broken formation. An albedo error of 0.001 translates to 136 W/m(2) or 0.4% in Earth's outgoing radiation error. Estimation errors are found to be independent of the satellites' altitude and inclination, if the nadir-looking is changed dynamically. The formation satellites are restricted to differ in only right ascension of planes and mean anomalies within slotted bounds. Three satellites in some specific formations show average albedo errors of less than 2% with respect to airborne, ground data and seven satellites in any slotted formation outperform the monolithic error of 3.6%. In fact, the maximum possible albedo error, purely based on angular sampling, of 12% for monoliths is outperformed by a five-satellite formation in any slotted arrangement and an eight satellite formation can bring that error down four fold to 3%. More than 70% ground spot overlap between the satellites is possible with 0.5 of pointing accuracy, 2 Km of GPS accuracy and commands uplinked once a day. The formations can be maintained at less than 1 m/s of monthly Delta V per satellite. (C) 2016 IAA. Published by Elsevier Ltd. All rights reserved. C1 [Nag, Sreeja] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nag, Sreeja] Bay Area Environm Res Inst, Petaluma, CA USA. [Gatebe, Charles K.] Univ Space Res Org, NASA, Goddard Space Flight Ctr, Columbia, MD USA. [Miller, David W.] MIT, NASA Headquarters, Cambridge, MA 02139 USA. [de Weck, Olivier L.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA. RP Nag, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Nag, S (reprint author), Bay Area Environm Res Inst, Petaluma, CA USA. EM sreejanag@alum.mit.edu; Charles.K.Gatebe@nasa.gov; millerd@mit.edu; deweck@mit.edu FU Schlumberger Faculty for the Future Fellowship (FFTF); NASA Earth and Space Science Fellowship (NESSF) FX The authors acknowledge the following people, without whose help this paper in its present quality would not have been possible: Rajesh Poudyal (GSFC) for extracting and post processing the BRDF data for the CAR instrument, Warren Wiscombe (GSFC) for his contribution and consistent drive toward Leonardo-BRDF which first proposed the concept of formation flight for BRDF, Jacqueline LeMoigne (GSFC), Ralph Kahn (GSFC), Kerri Cahoy (MIT), Daniel Selva (Cornell), Alexei Lyapustin (GSFC) for their invaluable ideas toward making this study better and three anonymous reviewers for their comments to improve its readability. The primary author was funded by the Schlumberger Faculty for the Future Fellowship (FFTF) and the NASA Earth and Space Science Fellowship (NESSF). NR 59 TC 1 Z9 1 U1 8 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD SEP-OCT PY 2016 VL 126 SI SI BP 77 EP 97 DI 10.1016/j.actaastro.2016.04.004 PG 21 WC Engineering, Aerospace SC Engineering GA DU7RL UT WOS:000382412200011 ER PT J AU Yang, FY Nelson, B Aziz, J Carlino, R Perez, AD Faber, N Foster, C Frost, C Henze, C Karacalioglu, AG Levit, C Marshall, W Mason, J O'Toole, C Swenson, J Worden, SP Stupl, J AF Yang, Fan Yang Nelson, Bron Aziz, Jonathan Carlino, Roberto Perez, Andres Dono Faber, Nicolas Foster, Cyrus Frost, Chad Henze, Chris Karacalioglu, Arif Goktug Levit, Creon Marshall, William Mason, James O'Toole, Conor Swenson, Jason Worden, Simon P. Stupl, Jan TI LightForce photon-pressure collision avoidance: Efficiency analysis in the current debris environment and long-term simulation perspective SO ACTA ASTRONAUTICA LA English DT Article ID MODEL; NASA AB This work provides an efficiency analysis of the LightForce space debris collision avoidance scheme in the current debris environment and describes a simulation approach to assess its impact on the long-term evolution of the space debris environment LightForce aims to provide just-in-time collision avoidance by utilizing photon pressure from ground-based industrial lasers. These ground stations impart minimal accelerations to increase the miss distance for a predicted conjunction between two objects. In the first part of this paper we will present research that investigates the short-term effect of a few systems consisting of 20 kW class lasers directed by 1.5 m diameter telescopes using adaptive optics. The results found such a network of ground stations to mitigate more than 85 percent of conjunctions and could lower the expected number of collisions in Low Earth Orbit (LEO) by an order of magnitude. While these are impressive numbers that indicate LightForce's utility in the short-term, the remaining 15 % of possible collisions contain (among others) conjunctions between two massive objects that would add large amount of debris if they collide. Still, conjunctions between massive objects and smaller objects can be mitigated. Hence, we choose to expand the capabilities of the simulation software to investigate the overall effect of a network of LightForce stations on the long-term debris evolution. In the second part of this paper, we will present the planned simulation approach for that effort. For the efficiency analysis of collision avoidance in the current debris environment, we utilize a simulation approach that uses the entire Two Line Element (TLE) catalog in LEO for a given day as initial input These objects are propagated for one year and an all-on-all conjunction analysis is performed. For conjunctions that fall below a range threshold, we calculate the probability of collision and record those values. To assess efficiency, we compare a baseline (without collision avoidance) conjunction analysis with an analysis where LightForce is active. Using that approach, we take into account that collision avoidance maneuvers could have effects on third objects. Performing all-on-all conjunction analyses for extended period of time requires significant computer resources; hence we implemented this simulation utilizing a highly parallel approach on the NASA Pleiades supercomputer. (C) 2016 Published by Elsevier Ltd. on behalf of IAA. C1 [Yang, Fan Yang; Perez, Andres Dono] NASA, Ames Res Ctr, MEI, Washington, DC USA. [Nelson, Bron] NASA, Ames Res Ctr, Comp Sci Corp, Washington, DC USA. [Aziz, Jonathan] Univ Colorado, Boulder, CO 80309 USA. [Carlino, Roberto] NASA, Ames Res Ctr, STC, Washington, DC USA. [Faber, Nicolas; Stupl, Jan] NASA, Ames Res Ctr, SGT, Washington, DC 20546 USA. [Foster, Cyrus; Levit, Creon; Marshall, William; Mason, James] Planet Labs, San Francisco, CA USA. [Frost, Chad; Henze, Chris] NASA, Ames Res Ctr, Washington, DC USA. [O'Toole, Conor] Univ Coll Dublin, NASA, Ames Res Ctr, Dublin, Ireland. [Swenson, Jason] NASA, Ames Res Ctr, LMCO Space OPNS, Washington, DC USA. [Worden, Simon P.] Breakthrough Prize Fdn, Stanford, CA USA. RP Stupl, J (reprint author), NASA, Ames Res Ctr, SGT, Washington, DC 20546 USA. EM jan.stupl@nasa.gov FU center management at NASA Ames Research Center FX We would like to thank our colleagues and the center management at NASA Ames Research Center for continuing support. We also would like to thank the NAIF SPICE team at JPL, especially Nat Bachman for providing a long term version of their Earth orientation file. Special thanks go to Wang Ting (Princeton) for sharing his area-to-mass ratio database and for providing insight in a past implementation of the EVOLVE breakup model. For useful discussions we would like to thank Gene Stansbery, Paula Krisko, Carsten Wiedemann, Jonas Radtke and Holger Krag. We thank Andrew Shacker for providing useful input for future versions of the software. We thank Jonas Jonsson for useful discussions and his help editing this paper. NR 32 TC 0 Z9 0 U1 2 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD SEP-OCT PY 2016 VL 126 SI SI BP 411 EP 423 DI 10.1016/j.actaastro.2016.04.032 PG 13 WC Engineering, Aerospace SC Engineering GA DU7RL UT WOS:000382412200042 ER PT J AU Guzzetti, D Bosanac, N Haapala, A Howell, KC Folta, DC AF Guzzetti, Davide Bosanac, Natasha Haapala, Amanda Howell, Kathleen C. Folta, David C. TI Rapid trajectory design in the Earth Moon ephemeris system via an interactive catalog of periodic and quasi-periodic orbits SO ACTA ASTRONAUTICA LA English DT Article; Proceedings Paper CT IAF 66th International Astronautical Congress (IAC) CY OCT, 2015 CL Jerusalem, ISRAEL SP IAF DE Multi-body systems; Three-body problem; Libration points; Quasi-periodic solutions; Periodic solutions ID LIBRATION POINTS AB Upcoming missions and prospective design concepts in the Earth-Moon system extensively leverage multi-body dynamics that may facilitate access to strategic locations or reduce propellant usage. To incorporate these dynamical structures into the mission design process, Purdue University and the NASA Goddard Flight Space Center have initiated the construction of a trajectory design framework to rapidly access and compare solutions from the circular restricted three-body problem. This framework, based upon a 'dynamic' catalog of periodic and quasi-periodic orbits within the Earth-Moon system, can guide an end-to-end trajectory design in an ephemeris model. In particular, the inclusion of quasi-periodic orbits further expands the design space, potentially enabling the detection of additional orbit options. To demonstrate the concept of a 'dynamic' catalog, a prototype graphical interface is developed. Strategies to characterize and represent periodic and quasi-periodic information for interactive trajectory comparison and selection are discussed. Two sample applications for formation flying near the Earth-Moon 1,2 point and lunar space infrastructures are explored to demonstrate the efficacy of a 'dynamic' catalog for rapid trajectory design and validity in higher-fidelity models. (C) 2016 IAA. Published by Elsevier Ltd. All rights reserved. C1 [Guzzetti, Davide; Bosanac, Natasha; Haapala, Amanda; Howell, Kathleen C.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA. [Folta, David C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Haapala, Amanda] Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. RP Guzzetti, D (reprint author), Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA. EM dguzzett@purdue.edu; nbosanac@purdue.edu; amanda.haapala@jhuapl.edu; howell@purdue.edu; david.c.folta@nasa.gov NR 31 TC 0 Z9 0 U1 2 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD SEP-OCT PY 2016 VL 126 SI SI BP 439 EP 455 DI 10.1016/j.actaastro.2016.06.029 PG 17 WC Engineering, Aerospace SC Engineering GA DU7RL UT WOS:000382412200044 ER PT J AU Rai, A Robinson, JA Tate-Brown, J Buckley, N Zell, M Tasaki, K Karabadzhak, G Sorokin, IV Pignataro, S AF Rai, Amelia Robinson, Julie A. Tate-Brown, Judy Buckley, Nicole Zell, Martin Tasaki, Kazuyuki Karabadzhak, Georgy Sorokin, Igor V. Pignataro, Salvatore TI Expanded benefits for humanity from the International Space Station SO ACTA ASTRONAUTICA LA English DT Article ID MICROGRAVITY; EXPERIENCE; RESOLUTION AB In 2012, the International Space Station (ISS) (Fig. 1) partnership published the updated International Space Station Benefits for Humanity [1], a compilation of stories about the many benefits being realized in the areas of human health, Earth observations and disaster response, and global education. This compilation has recently been revised to include updated statistics on the impacts of the benefits, and new benefits that have developed since the first publication. Two new sections have also been added to the book, economic development of space and innovative technology. This paper will summarize the updates on behalf of the ISS Program Science Forum, made up of senior science representatives across the international partnership. The new section on "Economic Development of Space" highlights case studies from public-private partnerships that are leading to a new economy in low earth orbit (LEO). Businesses provide both transportation to the ISS as well as some research facilities and services. These relationships promote a paradigm shift of government-funded, contractor-provided goods and services to commercially-provided goods purchased by government agencies. Other examples include commercial firms spending research and development dollars to conduct investigations on ISS and commercial service providers selling services directly to ISS users. This section provides examples of ISS as a test bed for new business relationships, and illustrates successful partnerships. The second new section, "Innovative Technology," merges technology demonstration and physical science findings that promise to return Earth benefits through continued research. Robotic refueling concepts for life extensions of costly satellites in geo-synchronous orbit have applications to robotics in industry on Earth. Flame behavior experiments reveal insight into how fuel burns in microgravity leading to the possibility of improving engine efficiency on Earth. Nanostructures and smart fluids are examples of materials improvements that are being developed using data from ISS. The publication also expands the benefits of research results in human health, environmental change and disaster response and in education activities developed to capture student imaginations in support of science, technology, engineering and mathematics, or STEM, education internationally. Applications to human health of the knowledge gained on ISS continue to grow and improve healthcare technologies and our understanding of human physiology. Distinct benefits return to Earth from the only orbiting multi-disciplinary laboratory of its kind. The ISS is a stepping stone for future space exploration by providing findings that develop LEO and improve life on our planet. (C) 2016 Published by Elsevier Ltd. on behalf of IAA. C1 [Rai, Amelia; Robinson, Julie A.] NASA, Johnson Space Ctr, Washington, DC 20546 USA. [Tate-Brown, Judy] Barrios Technol, Houston, TX 77058 USA. [Buckley, Nicole] Canadian Space Agcy, Longueuil, PQ, Canada. [Zell, Martin] European Space Agcy, Noordwijk, Netherlands. [Tasaki, Kazuyuki] Japan Aerosp Explorat Agcy JAXA, Chofu, Tokyo, Japan. [Karabadzhak, Georgy] TSNIIMASH, Kaliningrad, Russia. [Sorokin, Igor V.] SP Korolev Rocket & Space Corp Energia, Korolev, Russia. [Pignataro, Salvatore] Italian Space Agcy ASI, Rome, Italy. RP Rai, A (reprint author), NASA, Johnson Space Ctr, Washington, DC 20546 USA. EM amelia.e.rai@nasa.gov; julie.a.robinson@nasa.gov; judy.tate-brown-1@nasa.gov; nicole.buckley@asc-csa.gc.ca; martin.zell@esa.int; tasaki.kazuyuki@jaxa.jp; gfk@tsniimash.ru; igor.v.sorokin@rsce.ru; salvatore.pignataro@asi.it OI Robinson, Julie/0000-0002-6832-6459 NR 43 TC 0 Z9 0 U1 12 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD SEP-OCT PY 2016 VL 126 SI SI BP 463 EP 474 DI 10.1016/j.actaastro.2016.06.030 PG 12 WC Engineering, Aerospace SC Engineering GA DU7RL UT WOS:000382412200046 ER PT J AU Arvani, B Pierce, RB Lyapustin, AI Wang, YJ Ghermandi, G Teggi, S AF Arvani, Barbara Pierce, R. Bradley Lyapustin, Alexei I. Wang, Yujie Ghermandi, Grazia Teggi, Sergio TI Seasonal monitoring and estimation of regional aerosol distribution over Po valley, northern Italy, using a high-resolution MAIAC product SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Aerosol optical depth (AOD); High resolution aerosol retrieval; Seasonality AOD-PM10 correlation; MAIAC; MODIS; PM10; Planetary boundary layer (PBL) ID AIR-QUALITY ASSESSMENT; MODIS 3 KM; PARTICULATE MATTER PREDICTIONS; SOUTHEASTERN UNITED-STATES; OPTICAL DEPTH RETRIEVALS; PM2.5 CONCENTRATIONS; EPIDEMIOLOGIC EVIDENCE; AOD RETRIEVALS; BOUNDARY-LAYER; SATELLITE DATA AB In this work, the new 1 km-resolved Multi-Angle Implementation of Atmospheric Correction (MAIAC) algorithm is employed to characterize seasonal PM10 - AOD correlations over northern Italy. The accuracy of the new dataset is assessed compared to the widely used Moderate Resolution Imaging Spectroradiometer (MODIS) Collection 5.1 Aerosol Optical Depth (AOD) data, retrieved at 0.55 gm with spatial resolution of 10 km (MYD04_12). We focused on evaluating the ability of these two products to characterize both temporal and spatial distributions of aerosols within urban and suburban areas. Ground PM10 measurements were obtained from 73 of the Italian Regional Agency for Environmental Protection (ARPA) monitoring stations, spread across northern Italy, during a three-year period from 2010 to 2012. The Po Valley area (northern Italy) was chosen as the study domain because of its severe urban. air pollution, resulting from it having the highest population and industrial manufacturing density in the country, being located in a valley where two surrounding mountain chains favor the stagnation of pollutants. We found that the global correlations between the bin-averaged PM-to and AOD are R-2 = 0.83 and R-2 = 0.44 for MYD04_L2 and for MAIAC, respectively, suggesting a greater sensitivity of the high resolution product to small-scale deviations. However, the introduction of Relative Humidity (RH) and Planetary Boundary Layer (PBL) depth corrections allowed for a significant improvement to the bin averaged PM AOD correlation, which led to a similar performance: R-2 = 0.96 for MODIS and R-2 = 0.95 for MAIAC. Furthermore, the introduction of the PBL information in the corrected AOD values was found to be crucial in order to capture the clear seasonal cycle shown by measured PM10 values. The study allowed us to define four seasonal linear correlations that estimate PM10 concentrations satisfactorily from the remotely sensed MAIAC AOD retrieval. Overall, the results show that the high resolution provided by MAIAC retrieval data is much more relevant than the 10 km MODIS data to characterize PM10 in this region of Italy which has a pretty limited geographical domain but a broad variety of land usages and consequent particulate concentrations. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Arvani, Barbara; Ghermandi, Grazia; Teggi, Sergio] Univ Modena & Reggio Emilia, Dipartimento Ingn Enzo Ferrari, Via P Vivarelli 10, I-41125 Modena, Italy. [Pierce, R. Bradley] NOAA NESDIS Adv Satellite Prod Branch, 1225 W Dayton St, Madison, WI 53706 USA. [Lyapustin, Alexei I.] NASA, Goddard Space Flight Ctr, Code 613, Greenbelt, MD 20771 USA. [Wang, Yujie] Univ Maryland Baltimore Cty, 1000 Hilltop Circle, Baltimore, MD 21228 USA. RP Arvani, B (reprint author), Univ Modena & Reggio Emilia, Dipartimento Ingn Enzo Ferrari, Via P Vivarelli 10, I-41125 Modena, Italy. EM barbara.arvani@unimore.it RI Pierce, Robert Bradley/F-5609-2010; OI Pierce, Robert Bradley/0000-0002-2767-1643; Teggi, Sergio/0000-0001-7375-0599 FU Italian Ministero dell'Istruzione, dell' Universita e della Ricerca (Project PRIN) [2010WLNFY2] FX This research has been funded by the Italian Ministero dell'Istruzione, dell' Universita e della Ricerca (Project PRIN2010-11, 2010WLNFY2). The authors are thankful for Italian agencies ARPA Emilia-Romagna, ARPA Lombardia, ARPA Piemonte, and ARPA Veneto for providing ground PM10 data. The views, opinions, and findings contained in this report are those of the author(s) and should not be construed as an official National Oceanic and Atmospheric Administration or U.S. Government position, policy, or decision. NR 61 TC 1 Z9 1 U1 10 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD SEP PY 2016 VL 141 BP 106 EP 121 DI 10.1016/j.atmosenv.2016.06.037 PG 16 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA DU1EL UT WOS:000381950900010 ER PT J AU Dolan, W Payne, VH Kualwik, SS Bowman, KW AF Dolan, Wayana Payne, Vivienne H. Kualwik, Susan S. Bowman, Kevin W. TI Satellite observations of ethylene (C2H4) from the Aura Tropospheric Emission Spectrometer: A scoping study SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Ethylene; Tropospheric Emission Spectrometer; Satellite remote sensing ID ARCTAS; OZONE; AIRCRAFT; ISOPRENE; ATLANTIC; MISSION; IMPACT; FIRES; TES; PAN AB We present a study focusing on detection and initial quantitative estimates of ethylene (C2H4) in observations from the Tropospheric Emission Spectrometer (TES), a Fourier transform spectrometer aboard the Aura satellite that measures thermal infrared radiances with high spectral resolution (0.1 cm(-1)). We analyze observations taken in support of the 2008 Arctic Research of the Composition of the Troposphere from Aircraft and Satellites (ARCTAS) mission and demonstrate the feasibility of future development of C2H4 into a TES standard product. In the Northern Hemisphere, C2H4 is commonly associated with boreal fire plumes, motor vehicle exhaust and petrochemical emissions. It has a short lifetime (similar to 14-32 h) in the troposphere due to its reaction with OH and O-3. Chemical destruction of C2H4 in the atmosphere leads to the production of ozone and other species such as carbon monoxide (CO) and formaldehyde. Results indicate a correlation between C2H4 and CO in boreal fire plumes. Quantitative C2H4 estimates are sensitive to assumptions about the plume height and width. We find that C2H4 greater than 2-3 ppbv can be detected in a single TES observation (for a fire plume at 3 km altitude and 1.5 km width). Spatial averaging will be needed for surface-peaking profiles where TES sensitivity is lower. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Dolan, Wayana; Payne, Vivienne H.; Bowman, Kevin W.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Dolan, Wayana] Occidental Coll, Eagle Rock, CA USA. [Kualwik, Susan S.] Bay Area Environm Res Inst Moffett Field, Moffett Field, CA USA. RP Payne, VH (reprint author), Jet Prop Lab, M-S 233-200,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM vivienne.h.payne@jpl.nasa.gov NR 31 TC 0 Z9 0 U1 3 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD SEP PY 2016 VL 141 BP 388 EP 393 DI 10.1016/j.atmosenv.2016.07.009 PG 6 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA DU1EL UT WOS:000381950900035 ER PT J AU Titos, G Cazorla, A Zieger, P Andrews, E Lyamani, H Granados-Munoz, MJ Olmo, FJ Alados-Arboledas, L AF Titos, G. Cazorla, A. Zieger, P. Andrews, E. Lyamani, H. Granados-Munoz, M. J. Olmo, F. J. Alados-Arboledas, L. TI Effect of hygroscopic growth on the aerosol light-scattering coefficient: A review of measurements, techniques and error sources SO ATMOSPHERIC ENVIRONMENT LA English DT Review DE Scattering enhancement; Water uptake; Hygroscopicity; Aerosol light scattering ID ALPINE SITE JUNGFRAUJOCH; OPTICAL-PROPERTIES; RELATIVE-HUMIDITY; RADIATIVE PROPERTIES; IN-SITU; HUMIDIFICATION FACTORS; AMMONIUM-SULFATE; WATER-UPTAKE; ACE-ASIA; ATMOSPHERIC AEROSOLS AB Knowledge of the scattering enhancement factor,.f(RH), is important for an accurate description of direct aerosol radiative forcing. This factor is defined as the ratio between the scattering coefficient at enhanced relative humidity, RH, to a reference (dry) scattering coefficient. Here, we review the different experimental designs used to measure the scattering coefficient at dry and humidified conditions as well as the procedures followed to analyze the measurements. Several empirical parameterizations for the relationship between f(RH) and RH have been proposed in the literature. These parameterizations have been reviewed and tested using experimental data representative of different hygroscopic growth behavior and a new parameterization is presented. The potential sources of error in f(RH) are discussed. A Monte Carlo method is used to investigate the overall measurement uncertainty, which is found to be around 20-40% for moderately hygroscopic aerosols. The main factors contributing to this uncertainty are the uncertainty in RH measurement, the dry reference state and the nephelometer uncertainty. A literature survey of nephelometry-based f(RH) measurements is presented as a function of aerosol type. In general, the highest f(RH) values were measured in clean marine environments, with pollution having a major influence on f(RH). Dust aerosol tended to have the lowest reported hygroscopicity of any of the aerosol types studied. Major open questions and suggestions for future research priorities are outlined. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Titos, G.; Cazorla, A.; Lyamani, H.; Granados-Munoz, M. J.; Olmo, F. J.; Alados-Arboledas, L.] Univ Granada, Andalusian Inst Earth Syst Res, Granada 18006, Spain. [Titos, G.; Cazorla, A.; Lyamani, H.; Granados-Munoz, M. J.; Olmo, F. J.; Alados-Arboledas, L.] Univ Granada, Dept Appl Phys, Granada 18071, Spain. [Zieger, P.] Stockholm Univ, Bolin Ctr Climate Res, Dept Environm Sci & Analyt Chem, S-11418 Stockholm, Sweden. [Andrews, E.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80305 USA. [Titos, G.] IDAEA CSIC, Inst Environm Assessment & Water Res, Barcelona, Spain. [Granados-Munoz, M. J.] CALTECH, NASA, Jet Prop Lab, Table Mt Facil, Wrightwood, CA USA. RP Titos, G (reprint author), Univ Granada, Andalusian Inst Earth Syst Res, Granada 18006, Spain. EM gtitos@ugr.es RI Granados-Munoz, Maria Jose/G-9308-2014; OI Granados-Munoz, Maria Jose/0000-0001-8718-5914; Titos Vela, Gloria/0000-0003-3630-5079 FU Andalusia Regional Government [P10-RNM-6299, P12-RNM-2409]; FEDER [CGL2013_45410-R]; Spanish Ministry of Economy and Competitiveness; European Union [654109, ACTRIS-2]; Programa del Plan Propio de Investigacion "Contrato Puente" of the University of Granada FX This work was supported by the Andalusia Regional Government through projects P10-RNM-6299 and P12-RNM-2409; by the Spanish Ministry of Economy and Competitiveness and FEDER through project CGL2013_45410-R; and by European Union's Horizon 2020 research and innovation programme under grant agreement No 654109, ACTRIS-2. G. Titos was partially funded by Programa del Plan Propio de Investigacion "Contrato Puente" of the University of Granada. We thank the Stockholm International Meteorological Institute (IMI) for travel support of G. Titos. NR 90 TC 1 Z9 1 U1 20 U2 23 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD SEP PY 2016 VL 141 BP 494 EP 507 DI 10.1016/j.atmosenv.2016.07.021 PG 14 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA DU1EL UT WOS:000381950900046 ER PT J AU Duval, S Santini, JM Lemaire, D Chaspoul, F Russell, MJ Grimaldi, S Nitschke, W Schoepp-Cothenet, B AF Duval, Simon Santini, Joanne M. Lemaire, David Chaspoul, Florence Russell, Michael J. Grimaldi, Stephane Nitschke, Wolfgang Schoepp-Cothenet, Barbara TI The H-bond network surrounding the pyranopterins modulates redox cooperativity in the molybdenum-bisPGD cofactor in arsenite oxidase SO BIOCHIMICA ET BIOPHYSICA ACTA-BIOENERGETICS LA English DT Article DE Arsenite oxidase; Molybdenum enzyme; Optical spectroscopy; EPR spectroscopy; Redox titrations ID COLI NITRATE REDUCTASE; IRON-SULFUR CENTERS; PARAMAGNETIC-RESONANCE SPECTROSCOPY; ESCHERICHIA-COLI; DIMETHYLSULFOXIDE REDUCTASE; ALCALIGENES-FAECALIS; BINDING-SITE; SEMIQUINONE; OXIDATION; SUBUNIT AB While the molybdenum cofactor in the majority of bisPGD enzymes goes through two consecutive 1-electron redox transitions, previous protein-film voltammetric results indicated the possibility of cooperative (n = 2) redox behavior in the bioenergetic enzyme arsenite oxidase (Aio). Combining equilibrium redox titrations, optical and EPR spectroscopies on concentrated samples obtained via heterologous expression, we unambiguously confirm this claim and quantify Aio's redox cooperativity. The stability constant, K-s of the Mo-v semi-reduced intermediate is found to be lower than 10(-3). Site-directed mutagenesis of residues in the vicinity of the Mo-cofactor demonstrates that the degree of redox cooperativity is sensitive to H-bonding interactions between the pyranopterin moieties and amino acid residues. Remarkably, in particular replacing the Gln-726 residue by Gly results in stabilization of (low-temperature) EPR-observable Mo-v with K-s = 4. As evidenced by comparison of room temperature optical and low temperature EPR titrations, the degree of stabilization is temperature dependent. This highlights the importance of room-temperature redox characterizations for correctly interpreting catalytic properties in this group of enzymes. Geochemical and phylogenetic data strongly indicate that molybdenum played an essential biocatalytic roles in early life. Molybdenum's redox versatility and in particular the ability to show cooperative (n = 2) redox behavior provide a rationale for its paramount catalytic importance throughout the evolutionary history of life. Implications of the H-bonding network modulating Molybdenum's redox properties on details of a putative inorganic metabolism at life's origin are discussed. (C) 2016 Published by Elsevier B.V. C1 [Duval, Simon; Grimaldi, Stephane; Nitschke, Wolfgang; Schoepp-Cothenet, Barbara] Aix Marseille Univ, CNRS, BIP UMR 7281, IMM FR 3479, 31 Chemin J Aiguier, F-13402 Marseille 20, France. [Santini, Joanne M.] UCL, Inst Struct & Mol Biol, London WC1E 6BT, England. [Lemaire, David] CEA Cadarache, Inst Biol Environm & Biotechnol, F-13108 St Paul Les Durance, France. [Chaspoul, Florence] Aix Marseille Univ, IMBE, IRD CNRS UAPV, Fac Pharm, F-13005 Marseille, France. [Russell, Michael J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Schoepp-Cothenet, B (reprint author), Aix Marseille Univ, CNRS, BIP UMR 7281, IMM FR 3479, 31 Chemin J Aiguier, F-13402 Marseille 20, France. EM schoepp@imm.cnrs.fr OI Grimaldi, Stephane/0000-0002-9559-6112 FU CNRS; CEA; Aix-Marseille University; ANR [11-BSV5-005-01]; NASA Astrobiology Institute (Icy Worlds); French EPR network (RENARD) [IR3443] FX We thank Axel Magalon and Frederic Biaso for helpful discussions and Pierre Ceccaldi for Nar preparation. Our work is funded by the CNRS, CEA, Aix-Marseille University, ANR (Project MC2, 11-BSV5-005-01). MJR's research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration and with support by the NASA Astrobiology Institute (Icy Worlds). The authors are grateful to the EPR facilities available at the Aix-Marseille University EPR center, and to financial support from the French EPR network (RENARD, IR3443). NR 54 TC 0 Z9 0 U1 10 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0005-2728 EI 0006-3002 J9 BBA-BIOENERGETICS JI Biochim. Biophys. Acta-Bioenerg. PD SEP PY 2016 VL 1857 IS 9 BP 1353 EP 1362 DI 10.1016/j.bbabio.2016.05.003 PG 10 WC Biochemistry & Molecular Biology; Biophysics SC Biochemistry & Molecular Biology; Biophysics GA DV0EI UT WOS:000382590400001 PM 27207587 ER PT J AU Gilman, E Chaloupka, M Swimmer, Y Piovano, S AF Gilman, Eric Chaloupka, Milani Swimmer, Yonat Piovano, Susanna TI A cross-taxa assessment of pelagic longline by-catch mitigation measures: conflicts and mutual benefits to elasmobranchs SO FISH AND FISHERIES LA English DT Article DE At-vessel mortality; by-catch; circle hook; ray; shark; wire leader ID SHARK ALOPIAS-SUPERCILIOSUS; EASTERN PACIFIC-OCEAN; TUNA THUNNUS-OBESUS; SEA-TURTLE BYCATCH; CIRCLE HOOKS; POSTRELEASE SURVIVAL; RELATIVE ABUNDANCE; DISCARD MORTALITY; ATLANTIC-OCEAN; NORTH-ATLANTIC AB Elasmobranch mortality in pelagic longline fisheries poses a risk to some populations, alters the distribution of abundance between sympatric competitors, changing ecosystem structure, processes and stability. Individual and synergistic effects on elasmobranch catch and survival from pelagic longline gear factors, including methods prescribed to mitigate bycatch of other vulnerable taxa, were determined. Overall relative risk of higher circle vs. J-shaped hook shark catch rates conditioned on potentially informative moderators, from 30 studies, was estimated using an inverse-precision weighted mixed-effects meta-regression modelling approach. Sharks had a 1.20 times (95% CI: 1.03-1.39) significantly higher pooled relative risk of capture on circle hooks, with two significant moderators. The pooled relative risk estimate of ray circle hook catch from 15 studies was not significant (RR=1.22, 95% CI: 0.89-1.66) with no significant moderators. From a literature review, wire leaders had higher shark catch and haulback mortality than monofilament. Interacting effects of hook, bait and leader affect shark catch rates: hook shape and width and bait type determine hooking position and ability to sever monofilament leaders. Circle hooks increased elasmobranch catch, but reduced haulback mortality and deep hooking relative to J-shaped hooks of the same or narrower width. Using fish vs. squid for bait increased shark catch and deep hooking. Pelagic stingray (Pteroplatytrygon violacea) catch and mortality were lower on wider hooks. Using circle instead of J-shaped hooks and fish instead of squid for bait, while benefitting sea turtles, odontocetes and possibly seabirds, exacerbates elasmobranch catch and injury, therefore warranting fishery-specific assessments to determine relative risks. C1 [Gilman, Eric] Nature Conservancy, Honolulu, HI USA. [Gilman, Eric] Pelag Fisheries Res Serv, Honolulu, HI USA. [Chaloupka, Milani] Univ Queensland, Ecol Modeling Serv, St Lucia, Qld 4067, Australia. [Chaloupka, Milani] Univ Queensland, POB 6150, St Lucia, Qld 4067, Australia. [Swimmer, Yonat] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, 501 W Ocean Blvd, Long Beach, CA 90802 USA. [Piovano, Susanna] Univ South Pacific, Laucala Campus,Private Mail Bag, Suva, Fiji. RP Gilman, E (reprint author), 3661 Loulu St, Honolulu, HI 96822 USA. EM EGilman@FisheriesResearchGroup.org FU Sustainable Fisheries Fund Program of the Resources Legacy Fund; Nature Conservancy FX We are grateful for assistance provided by Victoria Jeffers, University of Exeter, with compiling literature. We acknowledge the assistance provided by Andre Afonso to correct copyediting errors in a table in Afonso et al. (2012). We are grateful for clarifications provided by John Watson and Daniel Foster on leader materials used in an experiment from which findings were published in Watson et al. (2005), Epperly et al. (2012), and Foster et al. (2012). Peer reviewer and journal editor comments greatly improved the manuscript. The Sustainable Fisheries Fund Program of the Resources Legacy Fund and The Nature Conservancy contributed financial support for this study. NR 160 TC 4 Z9 4 U1 16 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1467-2960 EI 1467-2979 J9 FISH FISH JI Fish. Fish. PD SEP PY 2016 VL 17 IS 3 BP 748 EP 784 DI 10.1111/faf.12143 PG 37 WC Fisheries SC Fisheries GA DU8VW UT WOS:000382494600012 ER PT J AU Cavosie, AJ Timms, NE Erickson, TM Hagerty, JJ Horz, F AF Cavosie, Aaron J. Timms, Nicholas E. Erickson, Timmons M. Hagerty, Justin J. Horz, Friedrich TI Transformations to granular zircon revealed: Twinning, reidite, and ZrO2 in shocked zircon from Meteor Crater (Arizona, USA) SO GEOLOGY LA English DT Article ID U-PB; VREDEFORT IMPACT; SOUTH-AFRICA; METAMORPHISM; MICROSTRUCTURES; DECOMPOSITION; DEFORMATION; BADDELEYITE; MINERALS; EVENTS AB Granular zircon in impact environments has long been recognized but remains poorly understood due to lack of experimental data to identify mechanisms involved in its genesis. Meteor Crater in Arizona (USA) contains abundant evidence of shock metamorphism, including shocked quartz, the high-pressure polymorphs coesite and stishovite, diaplectic SiO2 glass, and lechatelierite (fused SiO2). Here we report the presence of granular zircon, a new shocked-mineral discovery at Meteor Crater, that preserve critical orientation evidence of specific transformations that occurred during formation at extreme impact conditions. The zircon grains occur as aggregates of sub-micrometer neoblasts in highly shocked Coconino Sandstone (CS) comprised of lechatelierite. Electron backscatter diffraction shows that each grain consists of multiple domains, some with boundaries disoriented by 65 degrees around < 110 >, a known {112} shock-twin orientation. Other domains have {001} in alignment with {110} of neighboring domains, consistent with the former presence of the high-pressure ZrSiO4 polymorph reidite. Additionally, nearly all zircon preserve ZrO2 + SiO2, providing evidence of partial dissociation. The genesis of CS granular zircon started with detrital zircon that experienced shock twinning and reidite formation at pressures from 20 to 30 GPa, ultimately yielding a phase that retained crystallographic memory; this phase subsequently recrystallized to systematically oriented zircon neoblasts, and in some areas partially dissociated to ZrO2. The lechatelierite matrix, experimentally constrained to form at >2000 degrees C, provided the ultrahigh-temperature environment for zircon dissociation (similar to 1670 degrees C) and neoblast formation. The capacity of granular zircon to preserve a cumulative pressure-temperature record has not been recognized previously, and provides a new method for investigating histories of impact-related mineral transformations in the crust at conditions far beyond those at which most rocks melt. C1 [Cavosie, Aaron J.; Timms, Nicholas E.; Erickson, Timmons M.] Curtin Univ, Dept Appl Geol, TIGeR Inst Geosci Res, Perth, WA 6102, Australia. [Cavosie, Aaron J.] Univ Wisconsin, Dept Geosci, Astrobiol Inst, NASA, Madison, WI 53706 USA. [Cavosie, Aaron J.] Univ Puerto Rico, Dept Geol, Mayaguez, PR 00681 USA. [Hagerty, Justin J.] USGS, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Horz, Friedrich] NASA, Johnson Space Ctr, Dept Sci, Jets,HX5,ARES, Houston, TX 77058 USA. RP Cavosie, AJ (reprint author), Curtin Univ, Dept Appl Geol, TIGeR Inst Geosci Res, Perth, WA 6102, Australia.; Cavosie, AJ (reprint author), Univ Wisconsin, Dept Geosci, Astrobiol Inst, NASA, Madison, WI 53706 USA.; Cavosie, AJ (reprint author), Univ Puerto Rico, Dept Geol, Mayaguez, PR 00681 USA. OI Erickson, Timmons/0000-0003-4520-7294 FU National Science Foundation [EAR-1145118]; USGS Meteor Crater Sample Collection; NASA Astrobiology program; Curtin Research Fellowship; Microscopy and Microanalysis Facility at Curtin University FX B. Hess prepared the sample. Editor J.B. Murphy, S. Kamo, W. Cordua, and an anonymous reviewer provided helpful comments. Support was provided by the National Science Foundation (grant EAR-1145118), the USGS Meteor Crater Sample Collection, the NASA Astrobiology program, a Curtin Research Fellowship, and the Microscopy and Microanalysis Facility at Curtin University. NR 32 TC 3 Z9 3 U1 5 U2 5 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 SEP PY 2016 VL 44 IS 9 BP 703 EP 706 DI 10.1130/G38043.1 PG 4 WC Geology SC Geology GA DU9FV UT WOS:000382522700004 ER PT J AU Wang, YS Hyyppa, J Liang, XL Kaartinen, H Yu, XW Lindberg, E Holmgren, J Qin, YC Mallet, C Ferraz, A Torabzadeh, H Morsdorf, F Zhu, LL Liu, JB Alho, P AF Wang, Yunsheng Hyyppa, Juha Liang, Xinlian Kaartinen, Harri Yu, Xiaowei Lindberg, Eva Holmgren, Johan Qin, Yuchu Mallet, Clement Ferraz, Antonio Torabzadeh, Hossein Morsdorf, Felix Zhu, Lingli Liu, Jingbin Alho, Petteri TI International Benchmarking of the Individual Tree Detection Methods for Modeling 3-D Canopy Structure for Silviculture and Forest Ecology Using Airborne Laser Scanning SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Airborne laser scanning (ALS); benchmark; canopy structure; crown class; individual tree detection (ITD); LiDAR; point cloud; subordinate tree ID LIDAR POINT CLOUD; SEGMENTATION; CROWNS; STANDS AB Canopy structure plays an essential role in biophysical activities in forest environments. However, quantitative descriptions of a 3-D canopy structure are extremely difficult because of the complexity and heterogeneity of forest systems. Airborne laser scanning (ALS) provides an opportunity to automatically measure a 3-D canopy structure in large areas. Compared with other point cloud technologies such as the image-based Structure from Motion, the power of ALS lies in its ability to penetrate canopies and depict subordinate trees. However, such capabilities have been poorly explored so far. In this paper, the potential of ALS-based approaches in depicting a 3-D canopy structure is explored in detail through an international benchmarking of five recently developed ALS-based individual tree detection (ITD) methods. For the first time, the results of the ITD methods are evaluated for each of four crown classes, i.e., dominant, codominant, intermediate, and suppressed trees, which provides insight toward understanding the current status of depicting a 3-D canopy structure using ITD methods, particularly with respect to their performances, potential, and challenges. This benchmarking study revealed that the canopy structure plays a considerable role in the detection accuracy of ITD methods, and its influence is even greater than that of the tree species as well as the species composition in a stand. The study also reveals the importance of utilizing the point cloud data for the detection of intermediate and suppressed trees. Different from what has been reported in previous studies, point density was found to be a highly influential factor in the performance of the methods that use point cloud data. Greater efforts should be invested in the point-based or hybrid ITD approaches to model the 3-D canopy structure and to further explore the potential of high-density and multiwavelengths ALS data. C1 [Wang, Yunsheng; Hyyppa, Juha; Liang, Xinlian; Kaartinen, Harri; Yu, Xiaowei; Zhu, Lingli; Liu, Jingbin; Alho, Petteri] FGI, Finnish Geospatial Res Inst, Dept Remote Sensing & Photogrammetry, Masala 02431, Finland. [Wang, Yunsheng; Alho, Petteri] Univ Turku, Geog Sect, Dept Geog & Geol, Turku 20014, Finland. [Hyyppa, Juha; Liang, Xinlian; Kaartinen, Harri; Yu, Xiaowei; Zhu, Lingli; Liu, Jingbin] Acad Finland, Ctr Excellence Laser Scanning Res, Helsinki 00531, Finland. [Lindberg, Eva; Holmgren, Johan] Swedish Univ Agr Sci, Dept Forest Resource Management, S-90183 Umea, Sweden. [Qin, Yuchu; Mallet, Clement; Ferraz, Antonio] Univ Paris Est, IGN, MATIS, F-94160 Paris, France. [Ferraz, Antonio] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Torabzadeh, Hossein; Morsdorf, Felix] Univ Zurich, Remote Sensing Labs, CH-8057 Zurich, Switzerland. [Torabzadeh, Hossein] Bu Ali Sina Univ, Dept Civil Engn, Hamadan 651784161, Iran. RP Liang, XL (reprint author), FGI, Finnish Geospatial Res Inst, Dept Remote Sensing & Photogrammetry, Masala 02431, Finland. EM xinlian.liang@fgi.fi RI Alho, Petteri/B-7989-2013; Ferraz, Antonio/D-9662-2017; OI Alho, Petteri/0000-0001-5252-9609; Ferraz, Antonio/0000-0002-5328-5471; Mallet, Clement/0000-0002-2675-165X FU Finnish Academy through project "Centre of Excellence in Laser Scanning Research (CoE-LaSR)" [272195]; Finnish Academy through project "Interaction of Lidar/Radar Beams with Forests Using Mini-UAV and Mobile Forest Tomography" [259348]; Finnish Academy through project "Competence Based Growth Through Integrated Disruptive Technologies of 3-D Digitalization, Robotics, Geospatial Information and Image Processing/Computing Point Cloud Ecosystem" [293389]; European Community [606971]; French National Research Agency through the FORESEE Project [ANR-2010-BIOE-008]; Jet Propulsion Laboratory through the NASA Postdoctoral Program; Oak Ridge Associated Universities through a contract with NASA FX This work was supported in part by the Finnish Academy through projects "Centre of Excellence in Laser Scanning Research (CoE-LaSR)" under Grant 272195, "Interaction of Lidar/Radar Beams with Forests Using Mini-UAV and Mobile Forest Tomography" under Grant 259348, and "Competence Based Growth Through Integrated Disruptive Technologies of 3-D Digitalization, Robotics, Geospatial Information and Image Processing/Computing Point Cloud Ecosystem" under Grant 293389 and in part by the European Community's Seventh Framework Program (FP7/2007-2013) under Grant Agreement 606971. The work of Y. Qin, C. Mallet, and A. Ferraz was supported by the French National Research Agency through the FORESEE Project under Grant ANR-2010-BIOE-008. The work of A. Ferraz was supported by the Jet Propulsion Laboratory through the NASA Postdoctoral Program, which was administrated by the Oak Ridge Associated Universities through a contract with NASA. Y. Wang, J. Hyyppa, and X. Liang contributed equally to this work. NR 24 TC 1 Z9 1 U1 22 U2 22 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 SEP PY 2016 VL 54 IS 9 BP 5011 EP 5027 DI 10.1109/TGRS.2016.2543225 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 DV1NZ UT WOS:000382689300001 ER PT J AU Smith, GL Thomas, S Priestley, KJ Walikainen, D AF Smith, G. Louis Thomas, Susan Priestley, Kory J. Walikainen, Dale TI Tropical Mean Fluxes: A Tool for Calibration and Validation of CERES Radiometers SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Clouds and the earth's radiant energy system (CERES); in-flight calibration; radiation budget; radiometry; remote sensing; validation ID RADIANT ENERGY SYSTEM; DATA RECORD VALIDATION; ABOARD EOS TERRA; FLIGHT MODEL 5; INSTRUMENTS ABOARD; OCEAN MEASUREMENTS; CLOUDS; PERFORMANCE; SENSORS AB The Clouds and the Earth's Radiant Energy System (CERES) instrument requires in-flight calibration and validation to maintain its accuracy during orbit operations over an extended period. An internal calibration system provides calibration for the three channels; however, there is no device for calibration of the shortwave response of the total channel. A three-channel comparison technique has been developed to calibrate the shortwave response of the total channel using the tropical oceans as a vicarious calibration target. The difference between day and night outgoing longwave radiances (OLR) averaged over the tropical oceans is used to validate the day OLR. This paper evaluates the efficacy of the technique. A relation is computed at night between the window channel radiance and the OLR retrieved from the total channel for each month for each instrument. The relation has a standard deviation of 0.28 W.m(-2).sr(-1). Given 120 months of data, the precision of the curved line faired through these data is better than 0.05 W.m(-2).sr(-1). A bias is found between FM-1 and FM-3 of 0.3 W.m(-2).sr(-1), which is taken to be the accuracy with which the total channels can be calibrated with the internal blackbodies. This result includes the differences of longwave spectral responses of the instruments. The tropical mean OLR is between 87.4 and 90.2 W.m(-2).sr(-1) at night, with a standard deviation of 0.44 for FM-1 and 0.47 W.m(-2).sr(-1) for FM-3. The average difference between day and night tropical mean from the four instruments is 0.6 +/- 0.09 W.m(-2).sr(-1) over their data periods. C1 [Smith, G. Louis; Thomas, Susan; Walikainen, Dale] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Priestley, Kory J.] Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. RP Smith, GL (reprint author), Sci Syst & Applicat Inc, Hampton, VA 23666 USA. EM g.l.smith@nasa.gov FU Earth Science Directorate of the National Aeronautics and Space Administration through the Science Directorate of the Langley Research Center (LaRC); LaRC through Space Sciences Applications, Inc FX This work was supported by the Earth Science Directorate of the National Aeronautics and Space Administration through the Science Directorate of the Langley Research Center (LaRC). The work of G. L. Smith, S. Thomas and D. Walikainen was supported by LaRC through a contract with Space Sciences Applications, Inc. NR 25 TC 0 Z9 0 U1 4 U2 4 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 SEP PY 2016 VL 54 IS 9 BP 5135 EP 5142 DI 10.1109/TGRS.2016.2556581 PG 8 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA DV1NZ UT WOS:000382689300010 ER PT J AU Polivka, TN Wang, J Ellison, LT Hyer, EJ Ichoku, CM AF Polivka, Thomas N. Wang, Jun Ellison, Luke T. Hyer, Edward J. Ichoku, Charles M. TI Improving Nocturnal Fire Detection With the VIIRS Day-Night Band SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Day-night band (DNB); fire detection; fires; gas flares; Visible Infrared Imaging Radiometer Suite (VIIRS); visible light at night; wildfires ID PIXEL-BASED CALCULATION; RADIATIVE POWER; SENSITIVITY-ANALYSIS; SATELLITE DETECTION; INITIAL ASSESSMENT; SOUTH-AMERICA; INFRARED DATA; GAS FLARES; SCAR-B; MODIS AB Building on existing techniques for satellite remote sensing of fires, this paper takes advantage of the day-night band (DNB) aboard the Visible Infrared Imaging Radiometer Suite (VIIRS) to develop the Firelight Detection Algorithm (FILDA), which characterizes fire pixels based on both visible-light and infrared (IR) signatures at night. By adjusting fire pixel selection criteria to include visible-light signatures, FILDA allows for significantly improved detection of pixels with smaller and/or cooler subpixel hotspots than the operational Interface Data Processing System (IDPS) algorithm. VIIRS scenes with near-coincident Advanced Spaceborne Thermal Emission and Reflection (ASTER) overpasses are examined after applying the operational VIIRS fire product algorithm and including a modified "candidate fire pixel selection" approach from FILDA that lowers the 4-mu m brightness temperature (BT) threshold but includes a minimum DNB radiance. FILDA is shown to be effective in detecting gas flares and characterizing fire lines during large forest fires (such as the Rim Fire in California and High Park fire in Colorado). Compared with the operational VIIRS fire algorithm for the study period, FILDA shows a large increase (up to 90%) in the number of detected fire pixels that can be verified with the finer resolution ASTER data (90 m). Part (30%) of this increase is likely due to a combined use of DNB and lower 4-mu m BT thresholds for fire detection in FILDA. Although further studies are needed, quantitative use of the DNB to improve fire detection could lead to reduced response times to wildfires and better estimate of fire characteristics (smoldering and flaming) at night. C1 [Polivka, Thomas N.; Wang, Jun] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE 68588 USA. [Ellison, Luke T.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Ellison, Luke T.; Ichoku, Charles M.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hyer, Edward J.] Naval Res Lab, Marine Meteorol Div, Monterey, CA 93943 USA. RP Polivka, TN (reprint author), Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE 68588 USA. EM thomas.polivka@huskers.unl.edu; jwangjun@gmail.com; luke.ellison@nasa.gov; edward.hyer@nrlmry.navy.mil; charles.ichoku@nasa.gov RI Hyer, Edward/E-7734-2011; Wang, Jun/A-2977-2008 OI Hyer, Edward/0000-0001-8636-2026; Wang, Jun/0000-0002-7334-0490 FU NASA FX This work was supported in part by the NASA Suomi NPP Program and Applied Science Program managed by John A. Haynes and Lawrence A. Friedl and in part by the Interdisciplinary Studies (IDS) Program directed by J. Kaye and administered through the Radiation Sciences Program managed by Hal B. Maring. The work of T. Polivka was also supported by the NASA Nebraska Space Grant. NR 75 TC 0 Z9 0 U1 10 U2 10 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 SEP PY 2016 VL 54 IS 9 BP 5503 EP 5519 DI 10.1109/TGRS.2016.2566665 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 DV1NZ UT WOS:000382689300038 ER PT J AU Khan, A van Driel, M Bose, M Giardini, D Ceylan, S Yan, J Clinton, J Euchner, F Lognonne, P Murdoch, N Mimoun, D Panning, M Knapmeyer, M Banerdt, WB AF Khan, A. van Driel, M. Bose, M. Giardini, D. Ceylan, S. Yan, J. Clinton, J. Euchner, F. Lognonne, P. Murdoch, N. Mimoun, D. Panning, M. Knapmeyer, M. Banerdt, W. B. TI Single-station and single-event marsquake location and inversion for structure using synthetic Martian waveforms SO PHYSICS OF THE EARTH AND PLANETARY INTERIORS LA English DT Article DE Mars; Waveforms; Marsquakes; Interior structure; Surface waves; Body-waves; Travel times; Surface-wave overtones; Inversion ID LUNAR MANTLE; GEOPHYSICAL CONSTRAINTS; INTERIOR STRUCTURE; TIDAL DISSIPATION; SEISMIC DETECTION; MARS; MODEL; EARTH; CORE; MOON AB In anticipation of the upcoming InSight mission, which is expected to deploy a single seismic station on the Martian surface in November 2018, we describe a methodology that enables locating marsquakes and obtaining information on the interior structure of Mars. The method works sequentially and is illustrated using single representative 3 -component seismograms from two separate events: a relatively large teleseismic event (Mw5.1) and a small-to-moderate-sized regional event (M(w)3.8). Location and origin time of the event is determined probabilistically from observations of Rayleigh waves and body-wave arrivals. From the recording of surface waves, averaged fundamental-mode group velocity dispersion data can be extracted and, in combination with body-wave arrival picks, inverted for crust and mantle structure. In the absence of Martian seismic data, we performed full waveform computations using a spectral element method (AxiSEM) to compute seismograms down to a period of 1 s. The model (radial profiles of density, P- and S-wave-speed, and attenuation) used for this purpose is constructed on the basis of an average Martian mantle composition and model areotherm using thermodynamic principles, mineral physics data, and viscoelastic modeling. Noise was added to the synthetic seismic data using an up-todate noise model that considers a whole series of possible noise sources generated in instrument and Iander, including wind-, thermal-, and pressure-induced effects and electromagnetic noise. The examples studied here, which are based on the assumption of spherical symmetry, show that we are able to determine epicentral distance and origin time to accuracies of similar to 0.5-1 degrees and +/- 3-6 s, respectively. For the events and the particular noise level chosen, information on Rayleigh-wave group velocity dispersion in the period range similar to 14-48 s (M(w)5.1) and similar to 14-34 s (M(w)3.8) could be determined. Stochastic inversion of dispersion data in combination with body-wave travel time information for interior structure, allows us to constrain mantle velocity structure to an uncertainty of 5%. Employing the travel times obtained with the initially inverted models, we are able to locate additional body-wave arrivals including depth phases, surface and Moho (multiple) reflections that may otherwise elude visual identification. This expanded data set is reinverted to refine interior structure models and source parameters (epicentral distance and origin time). (C) 2016 Elsevier B.V. All rights reserved. C1 [Khan, A.; van Driel, M.; Bose, M.; Giardini, D.; Ceylan, S.; Yan, J.; Euchner, F.] Swiss Fed Inst Technol, Inst Geophys, Zurich, Switzerland. [Bose, M.; Clinton, J.] Swiss Fed Inst Technol, Swiss Seismol Serv, Zurich, Switzerland. [Lognonne, P.] Inst Phys Globe Paris, Paris, France. [Murdoch, N.; Mimoun, D.] Univ Toulouse, ISAE SUPAERO, DEOS Syst Spatiaux, Toulouse, France. [Panning, M.] Univ Florida, Dept Geol Sci, Gainesville, FL USA. [Knapmeyer, M.] DLR, Inst Planetary Res, Berlin, Germany. [Banerdt, W. B.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Khan, A (reprint author), Swiss Fed Inst Technol, Inst Geophys, Zurich, Switzerland. EM amir.khan@erdw.ethz.ch RI Lognonne, Philippe/F-8846-2010; Panning, Mark/B-3805-2011 OI Panning, Mark/0000-0002-2041-3190 FU Swiss National Science Foundation (SNF-ANR project) [157133]; Swiss National Supercomputing Centre (CSCS) [s528] FX We would like to thank Lapo Boschi and an anonymous reviewer for comments on the manuscript. We would also like to acknowledge Francis Nimmo for sharing his visco-elastic attenuation code. This work was supported by grants from the Swiss National Science Foundation (SNF-ANR project 157133 "Seismology on Mars") and from the Swiss National Supercomputing Centre (CSCS) under project ID s528. Numerical computations have also been performed on the ETH cluster Brutus. NR 89 TC 1 Z9 1 U1 9 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-9201 EI 1872-7395 J9 PHYS EARTH PLANET IN JI Phys. Earth Planet. Inter. PD SEP PY 2016 VL 258 BP 28 EP 42 DI 10.1016/j.pepi.2016.05.017 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DU7SK UT WOS:000382414700003 ER PT J AU McClelland, M Campbell, M Estlin, T AF McClelland, Mark Campbell, Mark Estlin, Tara TI Qualitative relational mapping and navigation for planetary rovers SO ROBOTICS AND AUTONOMOUS SYSTEMS LA English DT Article DE Navigation; Qualitative spatial reasoning; Qualitative methods; Mapping; Landmark navigation ID MOBILE ROBOTS; MAP; CONSISTENCY; INFORMATION; SPACE; SLAM AB This paper presents a novel method for qualitative mapping of large scale spaces which decouples the mapping problem from that of position estimation. The proposed framework makes use of a graphical representation of the world in order to build a map consisting of qualitative constraints on the geometric relationships between landmark triplets. This process allows a mobile robot to extract information about landmark positions using a set of minimal sensors in the absence of GPS. A novel measurement method based on camera imagery is presented which extends previous work from the field of Qualitative Spatial Reasoning. A Branch-and-Bound approach is taken to solve a set of non-convex feasibility problems required for generating off-line operator lookup tables and on-line measurements, which are fused into the map using an iterative graph update. A navigation approach for travel between distant landmarks is developed, using estimates of the Relative Neighborhood Graph extracted from the qualitative map in order to generate a sequence of landmark objectives based on proximity. Average and asymptotic performance of the mapping algorithm is evaluated using Monte Carlo tests on randomly generated maps, and a data-driven simulation is presented for a robot traversing the Jet Propulsion Laboratory Mars Yard while building a relational map. These results demonstrate that the system can be effectively used to build a map sufficiently complete and accurate for long-distance navigation as well as other applications. (C) 2016 Elsevier B.V. All rights reserved. C1 [McClelland, Mark; Campbell, Mark] Cornell Univ, Dept Mech & Aerosp Engn, Ithaca, NY 14853 USA. [Estlin, Tara] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [McClelland, Mark] Cornell Univ, Mech Engn, Ithaca, NY 14853 USA. [Campbell, Mark] Cornell Univ, Sibley Sch Mech & Aerosp Engn, Ithaca, NY 14853 USA. [Estlin, Tara] Mission Syst & Operat Div, Pasadena, CA USA. RP McClelland, M (reprint author), Cornell Univ, Dept Mech & Aerosp Engn, Ithaca, NY 14853 USA.; McClelland, M (reprint author), Cornell Univ, Mech Engn, Ithaca, NY 14853 USA. EM mjm496@cornell.edu; mc288@cornell.edu; Tara.Estlin@jpl.nasa.gov RI Campbell, Mark/F-8312-2013 OI Campbell, Mark/0000-0003-0775-4297 FU National Science Foundation [IIS-1320490]; NASA Graduate Student Research Program FX The research presented in this paper has been supported by National Science Foundation grant IIS-1320490 and a fellowship from the NASA Graduate Student Research Program. This work was performed by Cornell University and by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 31 TC 0 Z9 0 U1 7 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0921-8890 EI 1872-793X J9 ROBOT AUTON SYST JI Robot. Auton. Syst. PD SEP PY 2016 VL 83 BP 73 EP 86 DI 10.1016/j.robot.2016.05.017 PG 14 WC Automation & Control Systems; Computer Science, Artificial Intelligence; Robotics SC Automation & Control Systems; Computer Science; Robotics GA DU6SB UT WOS:000382343800006 ER PT J AU Patarasuk, R Gurney, KR O'Keeffe, D Song, Y Huang, JH Rao, P Buchert, M Lin, JC Mendoza, D Ehleringer, JR AF Patarasuk, Risa Gurney, Kevin Robert O'Keeffe, Darragh Song, Yang Huang, Jianhua Rao, Preeti Buchert, Martin Lin, John C. Mendoza, Daniel Ehleringer, James R. TI Urban high-resolution fossil fuel CO2 emissions quantification and exploration of emission drivers for potential policy applications SO URBAN ECOSYSTEMS LA English DT Article DE Residential; Onroad; STIRPAT; Urban carbon; Hestia; Bottom-up approach ID HOUSEHOLD ENERGY-CONSUMPTION; GREENHOUSE-GAS EMISSIONS; CARBON-DIOXIDE SOURCES; SEA-LEVEL RISE; CLIMATE-CHANGE; INTEGRATED APPROACH; IMPACT; SECTOR; MODEL; LIFE AB Fossil fuel carbon dioxide (FFCO2) emissions are the largest driver of anthropogenic climate change. Approximately three-quarters of the world's fossil fuels carbon dioxide emissions are generated in urban areas. We used the Hestia high resolution approach to quantify FFCO2 for Salt Lake County, Utah, USA and demonstrate the importance of high resolution quantification to urban emissions mitigation policymaking. We focus on the residential and onroad sectors across both urbanized and urbanizing parts of the valley. Stochastic Impact by Regression on Population, Affluence, and Technology (STIRPAT) regression models using sociodemographic data at the census block group level shows that population, per capita income, and building age exhibit positive relationships while household size shows a negative relationship with FFCO2 emissions. Compact development shows little effect on FFCO2 emissions in this domain. FFCO2 emissions in high income block groups is twice as sensitive to income than low income block groups. Emissions are four times as sensitive to household size in low-income versus high-income block groups. These results suggest that policy options targeting personal responsibility or knowledge feedback loops may be the most effective strategies. Examples include utility bill performance comparison or publicly available energy maps identifying high-emitting areas. Within the onroad sector, high emissions density (FFCO2/km) is associated with primary roads, while high emissions intensity (FFCO2/VMT) is associated with secondary roads. Opportunities exist for alignment of public transportation extension with remaining high emission road segments, offering a prioritization of new onroad transportation policy in Salt Lake County. C1 [Patarasuk, Risa; Gurney, Kevin Robert; O'Keeffe, Darragh; Song, Yang; Huang, Jianhua] Arizona State Univ, Sch Life Sci, POB 874501, Tempe, AZ 85287 USA. [Gurney, Kevin Robert; O'Keeffe, Darragh] Arizona State Univ, Global Inst Sustainabil, POB 875502, Tempe, AZ 85287 USA. [Rao, Preeti] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Buchert, Martin] Univ Utah, Global Change & Sustainabil Ctr, 155 South 1452 East, Salt Lake City, UT USA. [Lin, John C.; Mendoza, Daniel] Univ Utah, Dept Atmospher Sci, 135 South 1460 East, Salt Lake City, UT 84112 USA. [Ehleringer, James R.] Univ Utah, Dept Biol, 257 South 1400 East, Salt Lake City, UT 84112 USA. RP Patarasuk, R (reprint author), Arizona State Univ, Sch Life Sci, POB 874501, Tempe, AZ 85287 USA. EM risa.patarasuk@asu.edu OI Buchert, Martin/0000-0001-5974-001X; Rao, Preeti/0000-0002-5549-0583 FU Department of Energy [DE-SC-001-0624]; National Science Foundation [EF-01241286]; National Institute of Standards and Technology [70NANB14H321]; National Oceanic and Atmospheric Administration Climate Program Office's Atmospheric Chemistry, Carbon Cycle, and Climate Program [NA14OAR4310178] FX This research was supported by grants from the Department of Energy DE-SC-001-0624, the National Science Foundation grant EF-01241286, National Institute of Standards and Technology grant 70NANB14H321, and National Oceanic and Atmospheric Administration Climate Program Office's Atmospheric Chemistry, Carbon Cycle, and Climate Program grant NA14OAR4310178. We also would like to thank Jerome Zenger, Kevin Bell, and Semih Yildiz for assisting with the data collection and inquiry. NR 109 TC 1 Z9 1 U1 19 U2 19 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1083-8155 EI 1573-1642 J9 URBAN ECOSYST JI Urban Ecosyst. PD SEP PY 2016 VL 19 IS 3 BP 1013 EP 1039 DI 10.1007/s11252-016-0553-1 PG 27 WC Biodiversity Conservation; Ecology; Environmental Sciences; Urban Studies SC Biodiversity & Conservation; Environmental Sciences & Ecology; Urban Studies GA DV1HB UT WOS:000382670600001 ER PT J AU Liu, YC Xu, YH Hicks, MC Avedisian, CT AF Liu, Yu Cheng Xu, Yuhao Hicks, Michael C. Avedisian, C. Thomas TI Comprehensive study of initial diameter effects and other observations on convection-free droplet combustion in the standard atmosphere for n-heptane, n-octane, and n-decane SO COMBUSTION AND FLAME LA English DT Article DE Droplet combustion; Microgravity; Extinction; Radiation; Low temperature combustion; Soot formation ID MICROGRAVITY CONDITIONS; SOOT FORMATION; FUEL DROPLETS; BURNING RATE; COOL-FLAMES; LOW-GRAVITY; EXTINCTION; MIXTURES; VAPORIZATION; RADIATION AB This paper reports the results of a comprehensive experimental study on the effect of initial droplet diameter (Do) over a very wide range (0.5 mm < D-0 < 5 mm) on the spherically symmetric droplet burning characteristics in the standard atmosphere of three alkanes - n-heptane, n-octane and n-decane - that are representative of components found in petroleum-based transportation fuels and their surrogates. Spherical symmetry in the burning process was promoted by carrying out the experiments in a reduced convection (stagnant ambience) and buoyancy (low gravity) environment using the facilities of a ground based drop tower for D-0 < 0.8 mm and a spaced-based platform (the International Space Station) for D-0 > 1.0 mm. The results show that for Do greater than about 2 mm, K decreases with increasing Do in an early period of burning and with the data being correlated in the form K similar to D-0(-n) based on a scale analysis of an energy balance on the flame. For Do larger than approximately 2 mm the droplet flames often disappeared indicating an extinction mechanism that was speculated to be due to radiative losses from the flame. Concurrently, measurements of wideband radiation dropped significantly and the burning rate gradually approached pure evaporation. In some instances for n-heptane and n-octane radiative extinction was accompanied by droplet evaporation rates that were significantly higher than evaporation in a hot ambience which persisted for a significant fraction of the burning history before decreasing to evaporation in a cold ambience. An energy balance on the drop related the flame temperature to droplet diameter from which it was predicted that flame temperatures after ignition were greater than 1200 K before dropping to under approximately 800 K and remaining constant thereafter until eventually reaching near ambient conditions. This intermediate regime of burning was conjectured to be associated with a low temperature combustion process. The transition to this intermediate regime upon radiative extinction was occasionally accompanied by flame oscillations, the origin of which was uncertain but could have been initiated by motion of the droplet owing to the deployment process. (C) 2016 The Combustion Institute. Published by Elsevier Inc. All rights reserved. C1 [Liu, Yu Cheng] Univ Michigan Flint, Dept Comp Sci Engn & Phys, Flint, MI 48502 USA. [Xu, Yuhao; Avedisian, C. Thomas] Cornell Univ, Sibley Sch Mech & Aerosp Engn, Ithaca, NY 14853 USA. [Hicks, Michael C.] NASA, Glenn Res Ctr, Combust & Reacting Syst Branch, Cleveland, OH 44135 USA. [Liu, Yu Cheng] Tsinghua Univ, Ctr Combust Energy, Beijing 100084, Peoples R China. RP Avedisian, CT (reprint author), Cornell Univ, Sibley Sch Mech & Aerosp Engn, Ithaca, NY 14853 USA. EM cta2@cornell.edu OI Liu, Yu Cheng/0000-0001-7954-717X FU National Administration of Space and Aeronautics (NASA) [NNX08AI51G] FX This work was supported by the National Administration of Space and Aeronautics (NASA) under Grants NNX08AI51G to Cornell University (where the ground-based experiments were carried out). The authors are pleased to acknowledge Drs. Vedha Nayagam and Daniel Dietrich of NASA-Glenn who offered insights regarding data analysis and combustion physics of some of the observed trends and assistance with some of the reported experiments. Messrs Jeff Rah, Koffi Trenou, Wei-Chih Kuo and Anthony Savas of Cornell provided assistance with the experiments reported here and analyses of the data. The interest of F.A. Williams (UC-San Diego), F.L. Dryer (Princeton), T. Farouk (U. South Carolina), and B.D. Shaw (UC-Davis)) is also greatly appreciated. NR 60 TC 4 Z9 4 U1 10 U2 12 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0010-2180 EI 1556-2921 J9 COMBUST FLAME JI Combust. Flame PD SEP PY 2016 VL 171 BP 27 EP 41 DI 10.1016/j.combustfiame.2016.05.013 PG 15 WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary; Engineering, Chemical; Engineering, Mechanical SC Thermodynamics; Energy & Fuels; Engineering GA DU9CE UT WOS:000382513000003 ER PT J AU de Wit, J Wakeford, HR Gillon, M Lewis, NK Valenti, JA Demory, BO Burgasser, AJ Burdanov, A Delrez, L Jehin, E Lederer, SM Queloz, D Triaud, AHMJ Van Grootel, V AF de Wit, Julien Wakeford, Hannah R. Gillon, Michael Lewis, Nikole K. Valenti, Jeff A. Demory, Brice-Olivier Burgasser, Adam J. Burdanov, Artem Delrez, Laetitia Jehin, Emmanuel Lederer, Susan M. Queloz, Didier Triaud, Amaury H. M. J. Van Grootel, Valerie TI A combined transmission spectrum of the Earth-sized exoplanets TRAPPIST-1 b and c SO NATURE LA English DT Article ID HUBBLE-SPACE-TELESCOPE; HABITABLE-ZONE; LIGHT CURVES; SUPER-EARTHS; GJ 1214B; SPECTROSCOPY; ATMOSPHERES; PLANETS; KEPLER; EVAPORATION AB Three Earth-sized exoplanets were recently discovered close to the habitable zone(1,2) of the nearby ultracool dwarf star TRAPPIST-1 (ref. 3). The nature of these planets has yet to be determined, as their masses remain unmeasured and no observational constraint is available for the planetary population surrounding ultracool dwarfs, of which the TRAPPIST-1 planets are the first transiting example. Theoretical predictions span the entire atmospheric range, from depleted to extended hydrogen-dominated atmospheres(4-8). Here we report observations of the combined transmission spectrum of the two inner planets during their simultaneous transits on 4 May 2016. The lack of features in the combined spectrum rules out doud-free hydrogen-dominated atmospheres for each planet at >= 10 sigma levels; TRAPPIST-1 b and c are therefore unlikely to have an extended gas envelope as they occupy a region of parameter space in which high-altitude cloud/haze formation is not expected to be significant for hydrogen-dominated atmospheres(9). Many denser atmospheres remain consistent with the featureless transmission spectrum from a cloud-free water-vapour atmosphere to a Venus-like one. C1 [de Wit, Julien] MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Wakeford, Hannah R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gillon, Michael; Burdanov, Artem; Delrez, Laetitia; Jehin, Emmanuel; Van Grootel, Valerie] Univ Liege, Inst Astrophys & Geophys, Allee 6 Aout 19C, B-4000 Liege, Belgium. [Lewis, Nikole K.; Valenti, Jeff A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Demory, Brice-Olivier; Queloz, Didier] Cavendish Lab, Astrophys Grp, 19 JJ Thomson Ave, Cambridge CB3 0HE, England. [Burgasser, Adam J.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Lederer, Susan M.] NASA, Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. [Triaud, Amaury H. M. J.] Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. RP de Wit, J (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM jdewit@mit.edu OI Wakeford, Hannah/0000-0003-4328-3867 FU NASA through Space Telescope Science Institute [HST-GO-14500]; European Research Council (ERC) [336480]; Action de Recherche Concertee (ARC) by Wallonia-Brussels Federation; NASA; Fund for Research Training in Industry and Agriculture of the FRS-FNRS FX This work is based on observations made with the NASA/ESA Hubble Space Telescope that were obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. These observations are associated with program HST-GO-14500 (principal investigator J.d.W.), support for which was provided by NASA through a grant from the Space Telescope Science Institute. The research leading to our results was funded in part by the European Research Council (ERC) under the FP/2007-2013 ERC grant 336480, and through an Action de Recherche Concertee (ARC) grant financed by the Wallonia-Brussels Federation. H.R.W. acknowledges support through an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by the Universities Space Research Association through a contract with NASA. M.G. is Research Associate at the Belgian Fonds (National) de la Recherche Scientifique (FRS-FNRS). L.D. acknowledges support of the Fund for Research Training in Industry and Agriculture of the FRS-FNRS. We thank D. Taylor, S. Deustua, P. McCullough, and N. Reid for their assistance in planning and executing our observations. We are also grateful for discussions with Z. Berta-Thompson and Pierre Magain about this study and manuscript. We thank the ATLAS and PHOENIX teams for providing stellar models. NR 26 TC 6 Z9 6 U1 12 U2 15 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 SEP 1 PY 2016 VL 537 IS 7618 BP 69 EP 72 DI 10.1038/nature18641 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DU7XC UT WOS:000382426900039 PM 27437572 ER PT J AU Sears, DWG AF Sears, Derek W. G. TI The CO chondrites: Major recent Antarctic finds, their thermal and radiation history, and describing the metamorphic history of members of the class SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article DE CO chondrites; Metamorphism; Thermoluminescence; Antarctic meteorites ID UNEQUILIBRATED ORDINARY CHONDRITES; NATURAL THERMOLUMINESCENCE; CARBONACEOUS CHONDRITES; TERRESTRIAL AGES; TYPE-3 CHONDRITES; OXYGEN-ISOTOPE; PARENT-BODY; METEORITES; LUMINESCENCE; ORBITS AB Thermoluminescence (TL) properties of 29 CO chondrites from the Miller Range (MIL) and five chondrites from the Dominion Range (DOM) have been measured. MIL has a relatively strong natural TL signal (19.6 +/- 14.7 krad), while some of the DOM samples have a very weak natural TL signal (<1 krad) whereas others resemble the MIL meteorites. I argue that MIL and some of the DOM samples had a normal perihelion (similar to 1.0 AU) and terrestrial age of similar to 450-700 ka, while some of the DOM samples have a terrestrial age of similar to 100 ka but a perihelion of similar to 0.8 AU. The DOM meteorites also show considerable heterogeneity in their induced TL properties, also suggesting that the DOM fragments represent more than one fall. The induced TL data for the MIL samples studied here are consistent with them all being from a single fragmented meteorite. Small (50 mg) chips have TL properties similar to 500 mg chips, so that the smaller chips are representative, although samples taken from original masses less than similar to 2 g have low natural TL suggesting that they were heated during atmospheric fall. The properties of CO chondrites are reviewed in terms of their petrologic types. Correlations between TL sensitivity, the most quantitative technique for evaluating metamorphic alteration in CO chondrites, and data for olivine composition and heterogeneity, matrix composition, inert gas content, metal composition (Ni, Co, and Cr in the kamacite), bulk carbon, C and O isotopes, graphite ordering, spectral reflectance at 0.8 mu m, and textural characteristics of the ameboid olivine and Ca-rich inclusions are examined. The petrographic types appear to be largely metamorphic in origin with perhaps a minor role for metasomatism. Contrary to recent proposals it is here argued that petrologic type definitions should (1) be specific enough to be meaningful, but broad enough to be simple in application and robust to new developments, (2) be descriptive and not interpretative, (3) should not oversimplify and obscure important class-to-class differences, and (4) take account of all the available information, while avoiding reliance on any one technique or single observation whose application is based on interpretation. With these considerations in mind the petrographic type definitions for CO chondrites are restated and the petrologic type of 3.2 assigned to both the MIL and DOM CO chondrites. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Sears, Derek W. G.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Space Sci & Astrobiol Div MS 245 3, Mountain View, CA 94035 USA. RP Sears, DWG (reprint author), NASA, Ames Res Ctr, Bay Area Environm Res Inst, Space Sci & Astrobiol Div MS 245 3, Mountain View, CA 94035 USA. FU NASA's Solar System Exploration and Research Virtual Institute FX I am grateful to Tim Lee and Chris McKay for providing facilities and an exciting research environment at NASA Ames Research Center and I am grateful to Mark Sittloh and his colleagues at the Bay Area Environmental Research Institute for management support. I am also grateful to the Antarctic Meteorite Working Group for providing the samples and the Meteorite Processing Laboratory at Johnson Space Center for so capably handling the sampling. I am also grateful to Hazel Sears for reviewing and proofing this paper, David Sears for help with the statistical analysis, four anonymous journal reviewers who provided much appreciated reviews (which included the suggestion to include Fig. 7), and Chris Herd for organizing these reviews. Finally, I am pleased to acknowledge the Field Investigations to Enable Solar System Science and Exploration team of NASA's Solar System Exploration and Research Virtual Institute (PI: Jennifer Heldmann) for financial support. NR 54 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD SEP 1 PY 2016 VL 188 BP 106 EP 124 DI 10.1016/j.gca.2016.05.033 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DS4LN UT WOS:000380752700007 ER PT J AU Robinson, KL Barnes, JJ Nagashima, K Thomen, A Franchi, IA Huss, GR Anand, M Taylor, GJ AF Robinson, Katharine L. Barnes, Jessica J. Nagashima, Kazuhide Thomen, Aurelien Franchi, Ian A. Huss, Gary R. Anand, Mahesh Taylor, G. Jeffrey TI Water in evolved lunar rocks: Evidence for multiple reservoirs SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article DE Moon; Lunar volatiles; Apatite; Water; H isotopes ID SILICATE-LIQUID-IMMISCIBILITY; HOSTED MELT INCLUSIONS; TERRESTRIAL PLANETS; VOLCANIC GLASSES; MG-SUITE; VOLATILE ABUNDANCES; QUARTZ MONZODIORITE; CRYSTAL-CHEMISTRY; COOLING HISTORY; OXYGEN FUGACITY AB We have measured the abundance and isotopic composition of water in apatites from several lunar rocks representing Potassium (K), Rare Earth Elements (REE), and Phosphorus (P) - KREEP - rich lithologies, including felsites, quartz monzodiorites (QMDs), a troctolite, and an alkali anorthosite. The H-isotope data from apatite provide evidence for multiple reservoirs in the lunar interior. Apatite measurements from some KREEP-rich intrusive rocks display moderately elevated delta D signatures, while other samples show delta D signatures similar to the range known for the terrestrial upper mantle. Apatite grains in Apollo 15 quartz monzodiorites have the lowest delta D values measured from the Moon so far (as low as -749 parts per thousand), and could potentially represent a D-depleted reservoir in the lunar interior that had not been identified until now. Apatite in all of these intrusive rocks contains <267 ppm H2O, which is relatively low compared to apatites from the majority of studied mare basalts (200 to >6500 ppm H2O). Complexities in partitioning of volatiles into apatite make this comparison uncertain, but measurements of residual glass in KREEP basalt fragments in breccia 15358 independently show that the KREEP basaltic magmas were low in water. The source of 15358 contained similar to 10 ppm H2O, about an order of magnitude lower than the source of the Apollo 17 pyroclastic glass beads, suggesting potential variations in the distribution of water in the lunar interior. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Robinson, Katharine L.; Nagashima, Kazuhide; Thomen, Aurelien; Huss, Gary R.; Taylor, G. Jeffrey] Hawaii Inst Geophys & Planetol, 1680 East West Rd,POST 602, Honolulu, HI 96822 USA. [Robinson, Katharine L.; Huss, Gary R.; Taylor, G. Jeffrey] Univ Hawaii, NASA Astrobiol Inst, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. [Robinson, Katharine L.; Huss, Gary R.; Taylor, G. Jeffrey] Univ Hawaii Manoa, Geol & Geophys, 1680 East West Rd,POST 602, Honolulu, HI 96822 USA. [Barnes, Jessica J.; Franchi, Ian A.; Anand, Mahesh] Open Univ, Planetary & Space Sci, Walton Hall, Milton Keynes MK7 6AA, Bucks, England. [Anand, Mahesh] Nat Hist Museum, Dept Earth Sci, Cromwell Rd, London SW7 5BD, England. RP Robinson, KL (reprint author), Open Univ, Planetary & Space Sci, Walton Hall, Milton Keynes MK7 6AA, Bucks, England. EM katie.robinson@open.ac.uk FU National Aeronautics and Space Administration through the NASA Astrobiology Institute through the Office of Space Science [NNA09DA77A]; NASA Lunar Advanced Science and Exploration Research [NNX11AE85G]; Solar System Exploration Research Virtual Institute (through the Center for Lunar Science and Exploration) [NNA14AB07A]; Bullard Foundation; STFC [ST/I001298/1, ST/L000776/1] FX The authors thank Romain Tartese for his assistance in collecting data and for highly useful discussions. This research was supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement No. NNA09DA77A issued through the Office of Space Science, by NASA Lunar Advanced Science and Exploration Research Grant NNX11AE85G, the Solar System Exploration Research Virtual Institute (through the Center for Lunar Science and Exploration cooperative agreement NNA14AB07A, David Kring, PI), and by The Bullard Foundation. STFC are also thanked for a PhD studentship to JJB and research grants to MA (Grant no. ST/I001298/1 and ST/L000776/1). We thank three anonymous reviewers and associate editor Alexander Nemchin for insightful and critical comments that helped improve the quality of the manuscript. NR 115 TC 2 Z9 2 U1 12 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD SEP 1 PY 2016 VL 188 BP 244 EP 260 DI 10.1016/j.gca.2016.05.030 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DS4LN UT WOS:000380752700014 ER PT J AU Peretyazhko, TS Fox, A Sutter, B Niles, PB Adams, M Morris, RV Ming, DW AF Peretyazhko, T. S. Fox, A. Sutter, B. Niles, P. B. Adams, M. Morris, R. V. Ming, D. W. TI Synthesis of akaganeite in the presence of sulfate: Implications for akaganeite formation in Yellowknife Bay, Gale Crater, Mars SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article DE Mars; Gale crater; Yellowknife Bay; Fe oxides; Akaganeite ID ACID-MINE DRAINAGE; BETA-FEOOH; AQUEOUS-SOLUTIONS; REFLECTANCE SPECTROSCOPY; SPECTRAL PROPERTIES; FORCED HYDROLYSIS; MERIDIANI-PLANUM; X-RAY; IRON; JAROSITE AB Akaganeite, a Cl-bearing Fe(III) (hydr)oxide, has been recently discovered in Yellowknife Bay in Gale crater on Mars by the Mars Science Laboratory (MSL) Curiosity Rover. Akaganeite was associated with sulfate and sulfide minerals at Yellowknife Bay indicating that sulfate ions could be present in solution during akaganeite formation. The mechanism and conditions of akaganeite formation in the Yellowknife Bay mudstone are unknown. We investigated formation of akaganeite through hydrolysis of ferric chloride solution in the presence of 0, 0.01, 0.05, 0.1 and 0.2 M sulfate and at initial pH of 1.5, 2 and 4 at 90 degrees C. Mineralogy of the precipitated Fe(III) phases was characterized by X-ray diffraction and infrared spectroscopy. The precipitates were also acid digested to determine total sulfate and chloride contents. Akaganeite and natrojarosite formed at initial solution pH of 1.5; akaganeite, goethite and natrojarosite precipitated in initial pH 2 solutions and goethite, hematite and 2-line ferrihydrite precipitated at initial solution pH of 4. Sulfate addition did not inhibit akaganeite formation. Increasing initial solution sulfate concentrations resulted in increasing sulfate to chloride ratio in the precipitated akaganeite. Infrared spectroscopy revealed akaganeite bands at similar to 2 mu m (H2O combination band) and at similar to 2.46 mu m (OH combination band). The H2O combination band position linearly correlated with total chloride content in akaganeite. Overall, laboratory studies demonstrated formation of akaganeite at initial sulfate concentration <= 0.2 M (sulfate to chloride molar ratio <= 0.3) and pH <= 2, implying that those conditions might prevail (perhaps as micro-environments) during akaganeite formation in Yellowknife Bay mudstone. The occurrence of Fe(II) sulfides (pyrite and pyrrhotite) in Yellowknife Bay mudstone is a potential acidity source. Dissolution of sulfide minerals might occur under localized oxidizing waterlimiting Cl-rich conditions creating favorable environments for akaganeite formation. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Peretyazhko, T. S.; Sutter, B.] NASA, Jacobs, Johnson Space Ctr, Houston, TX 77058 USA. [Fox, A.] Indiana Univ, Bloomington, IN 47406 USA. [Niles, P. B.; Morris, R. V.; Ming, D. W.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Adams, M.] Univ Hawaii, Hilo, HI 96720 USA. RP Peretyazhko, TS (reprint author), NASA, Jacobs, Johnson Space Ctr, Houston, TX 77058 USA. EM tanya.peretyazhko@nasa.gov FU Summer Intern Scholarship of Lunar and Planetary Institute; NASA Mars Science Laboratory Mission grants; NASA Solar System Workings grant [15-SSW15_2-0074] FX We are grateful to Z. Peng for performing ICP-MS analysis and K. Pando and D. Locke for help with ion chromatography. We thank Dr. Bishop and two anonymous reviewers for valuable suggestions and comments that help to improve the quality of the manuscript. We thank the Associate Editor Dr. Catalano for handling the manuscript. A. Fox acknowledges a Summer Intern Scholarship of Lunar and Planetary Institute. This work was supported by NASA Mars Science Laboratory Mission grants and by NASA Solar System Workings grant #15-SSW15_2-0074. The data presented in figures could be provided upon request. NR 76 TC 0 Z9 0 U1 18 U2 25 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD SEP 1 PY 2016 VL 188 BP 284 EP 296 DI 10.1016/j.gca.2016.06.002 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DS4LN UT WOS:000380752700016 ER PT J AU Ting, DZ Soibel, A Hoglund, L Hill, CJ Keo, SA Fisher, A Gunapala, SD AF Ting, David Z. Soibel, Alexander Hoeglund, Linda Hill, Cory J. Keo, Sam A. Fisher, Anita Gunapala, Sarath D. TI High-Temperature Characteristics of an InAsSb/AlAsSb n(+)Bn Detector SO JOURNAL OF ELECTRONIC MATERIALS LA English DT Article DE Infrared detector; unipolar barrier; nBn; mid-wavelength infrared AB The high-temperature characteristics of a mid-wavelength infrared (MWIR) detector based on the Maimon-Wicks InAsSb/AlAsSb nBn architecture was analyzed. The dark current characteristics are examined in reference to recent minority carrier lifetime results. The difference between the responsivity and absorption quantum efficiency (QE) at shorter wavelengths is clarified in terms of preferential absorption of higher-energy photons in the top contact layer, which cannot provide reverse-bias photo-response due to the AlAsSb electron blocking layer and strong recombination. Although the QE does not degrade when the operating temperature increases to 325 K, the turn-on bias becomes larger at higher temperatures. This behavior was originally attributed to the change in the valence band alignment between the absorber and top contact layers caused by the shift in Fermi level with temperature. In this work, we demonstrated the inadequacy of the original description, and offer a more likely explanation based on temperature-dependent band-bending effects. C1 [Ting, David Z.; Soibel, Alexander; Hoeglund, Linda; Hill, Cory J.; Keo, Sam A.; Fisher, Anita; Gunapala, Sarath D.] NASA, Jet Prop Lab, Ctr Infrared Photodetectors, M-S302-231,4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Soibel, Alexander; Hoeglund, Linda; Hill, Cory J.; Keo, Sam A.; Fisher, Anita; Gunapala, Sarath D.] CALTECH, Pasadena, CA 91109 USA. RP Ting, DZ (reprint author), NASA, Jet Prop Lab, Ctr Infrared Photodetectors, M-S302-231,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM David.Z.Ting@jpl.nasa.gov NR 8 TC 2 Z9 2 U1 11 U2 11 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0361-5235 EI 1543-186X J9 J ELECTRON MATER JI J. Electron. Mater. PD SEP PY 2016 VL 45 IS 9 BP 4680 EP 4685 DI 10.1007/s11664-016-4633-z PG 6 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA DS9CM UT WOS:000381080000027 ER PT J AU Suhir, E Ghaffarian, R AF Suhir, E. Ghaffarian, R. TI Board level drop test: exact solution to the problem of the nonlinear dynamic response of a PCB to the drop impact SO JOURNAL OF MATERIALS SCIENCE-MATERIALS IN ELECTRONICS LA English DT Article AB An analytical predictive model has been developed for the evaluation of the nonlinear dynamic response of a printed-circuit-board (PCB) to the drop impact during board-level testing. The hypothesis of "heavy-and-flexible" PCB is used in the analysis: the surface-mounted-devices (SMDs) are assumed to be small enough not to affect the PCB's flexural rigidity, but their masses have been considered and accounted for by "spreading out" the SMD total mass over the PCB surface. The analysis is restricted to the fundamental mode of vibrations, and the method of principal coordinates is used to evaluate the response. The exact solution to the nonlinear differential equation for the principal coordinate has been obtained. Another important finding is that the nonlinear amplitudes were determined even without solving the nonlinear differential equation of motion. The main objective of the analysis is to provide design guidelines for constructing a feasible experimental setup. A simply supported board is suggested as the most appropriate structure for an adequate test vehicle: the experimental data for such a board, as far as the behavior of the solder material in the second level of interconnections is concerned, can be easily and reliably interpreted and extrapolated for the practical use. The developed model enables one to predict the induced bending moments and the in-plane (membrane) forces that could be applied in the subsequent analyses to the PCB areas in the proximity of the package and its solder joint interconnections. C1 [Suhir, E.] Portland State Univ, Portland, OR 97207 USA. [Suhir, E.] ERS Co, 727 Alvina Ct, Los Altos, CA 94024 USA. [Ghaffarian, R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Suhir, E (reprint author), Portland State Univ, Portland, OR 97207 USA.; Suhir, E (reprint author), ERS Co, 727 Alvina Ct, Los Altos, CA 94024 USA. EM suhire@aol.com NR 21 TC 1 Z9 1 U1 10 U2 10 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0957-4522 EI 1573-482X J9 J MATER SCI-MATER EL JI J. Mater. Sci.-Mater. Electron. PD SEP PY 2016 VL 27 IS 9 BP 9423 EP 9430 DI 10.1007/s10854-016-4988-1 PG 8 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Engineering; Materials Science; Physics GA DT0FY UT WOS:000381159800074 ER PT J AU Xie, YS Fan, X Chen, YP Wilson, JD Simons, RN Xiao, JQ AF Xie, Yunsong Fan, Xin Chen, Yunpeng Wilson, Jeffrey D. Simons, Rainee N. Xiao, John Q. TI THE IN-PHASE REFLECTION BANDWIDTH THEORETICAL LIMIT OF ARTIFICIAL MAGNETIC CONDUCTORS BASED ON TRANSMISSION LINE MODEL SO MICROWAVE AND OPTICAL TECHNOLOGY LETTERS LA English DT Article DE artificial magnetic conductors (AMCs); transmission line model; bandwidth limitation ID HIGH-IMPEDANCE SURFACES; FREQUENCY; ANTENNAS; ABSORBERS; DESIGN AB Based on the transmission line model, the in-phase reflection (IPR) bandwidth theoretical limit using a function of permeability (l) and thickness (h) of the substrate as well as center frequency of IPR (f) was expressed. An experimental design strategy was further derived from this function for creating novel artificial magnetic conductors (AMCs). To date, they have successfully designed, simulated, and experimentally verified this proposed strategy with various AMCs, where the bandwidth ratio to the theoretical limit can be achieved by as high as 98.5%. This newly proposed theoretical limit function was further evaluated in two-ways, (1) our theoretical limit was compared with previously reported literature values, and (2) literature values were recalculated using our function. Herein, it was concluded that their IPR bandwidth theoretical limit function provided most restrictive and accurate value, and their AMC design strategy has showed evident advantages over literature. (C) 2016 Wiley Periodicals, Inc. C1 [Xie, Yunsong; Chen, Yunpeng] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Fan, Xin] Univ Denver, Dept Phys & Astron, Newark, DE 19716 USA. [Wilson, Jeffrey D.; Simons, Rainee N.; Xiao, John Q.] Glenn Res Ctr, Natl Aeronaut & Space Adm, Cleveland, OH USA. RP Xiao, JQ (reprint author), Glenn Res Ctr, Natl Aeronaut & Space Adm, Cleveland, OH USA. EM jqx@udel.edu FU National Aeronautics and Space Administration (NASA) [NNX11AQ29A] FX This work was supported by the National Aeronautics and Space Administration (NASA) under Grant No. NNX11AQ29A. NR 22 TC 0 Z9 0 U1 6 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0895-2477 EI 1098-2760 J9 MICROW OPT TECHN LET JI Microw. Opt. Technol. Lett. PD SEP PY 2016 VL 58 IS 9 BP 2257 EP 2261 DI 10.1002/mop.30024 PG 6 WC Engineering, Electrical & Electronic; Optics SC Engineering; Optics GA DS7DW UT WOS:000380944000052 ER PT J AU Bianco, WT Landis, R AF Bianco, William T. Landis, Robert TI Engineering cooperation: How Americans and Russians manage joint operation of the International Space Station SO INTERNATIONAL AREA STUDIES REVIEW LA English DT Article DE Cooperation; prisoners' dilemma; new economics of organization; International Space Station; NASA AB The 1990s agreements that created the International Space Station (ISS) described the effort as a partnership of equals, a joint venture between organizations that remained independent in terms of many procedures, norms, goals, and the assumptions underlying these factors. As a result, successful joint ISS operations required the participants, most notably the American and Russian space programs, to reconcile different procedures, norms, and training regimes, as well as the beliefs that underlie these practices. Drawing on a combination of operational experience, first-hand observation, and interviews, this paper focuses on how the two programs reduced conflict and engendered cooperation. It also uses the ISS experience to consider how future joint efforts can be designed to minimize conflict between international partners. C1 [Bianco, William T.] Indiana Univ, Woodburn Hall 210, Bloomington, IN 47401 USA. [Landis, Robert] NASA Headquarters, Washington, DC USA. RP Bianco, WT (reprint author), Indiana Univ, Woodburn Hall 210, Bloomington, IN 47401 USA. EM wbianco@indiana.edu NR 12 TC 0 Z9 0 U1 4 U2 4 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 2233-8659 EI 2049-1123 J9 INT AREA STUD REV JI Int. Area Stud. Rev. PD SEP PY 2016 VL 19 IS 3 BP 197 EP 209 DI 10.1177/2233865916636834 PG 13 WC International Relations SC International Relations GA DT6WT UT WOS:000381626100001 ER PT J AU Ghods, M Johnson, L Lauer, M Grugel, RN Tewari, SN Poirier, DR AF Ghods, M. Johnson, L. Lauer, M. Grugel, R. N. Tewari, S. N. Poirier, D. R. TI Macrosegregation in Al-7Si alloy caused by abrupt cross-section change during directional solidification SO JOURNAL OF CRYSTAL GROWTH LA English DT Article DE Directional solidification; Cross-section change; Computer simulation; Fluid flows; Segregation; Aluminum alloys ID PB-SN ALLOYS; DENDRITIC SOLIDIFICATION; NATURAL-CONVECTION; METALLIC ALLOYS; SUPERALLOY CASTINGS; GRAIN STRUCTURES; RAYLEIGH NUMBER; CRYSTAL-GROWTH; TURBINE-BLADES; BINARY-ALLOYS AB Hypoeutectic Al-7 wt.% Si alloys were directionally solidified vertically downward in cylindrical molds that incorporated an abrupt cross-section decrease (9.5 mm to 3.2 mm diameter) which, after 5 cm, reverted back to 9.5 mm diameter in a Bridgman furnace; two constant growth speeds and thermal gradients were investigated. Thermosolutal convection and cross-section-change-induced shrinkage flow effects on macrosegregation were investigated. Dendrite clustering and extensive radial macro segregation was seen, particularly in the larger cross-sections, before contraction and after expansion, this more evident at the lower growth speed. This alloy shows positive longitudinal macrosegregation near cross-section decrease followed by negative macrosegregation right after it; the extent of macro segregation, however, decreases with increasing growth speed. Primary dendrite steepling intensified as solidification proceeded into the narrower section and negative longitudinal macrosegregation was seen on the re-entrant shelves at expansion. A two-dimensional model accounting for both shrinkage and thermo-solutal convection was used to simulate solidification and the resulting mushy-zone steepling and macrosegregation. The experimentally observed longitudinal and radial macrosegregation associated with the cross-section changes during directional solidification of an Al-75i alloy is well captured by the numerical simulations. (C) 2016 Elsevier B.V. All rights reserved. C1 [Ghods, M.; Johnson, L.; Tewari, S. N.] Cleveland State Univ, Chem & Biomed Engn Dept, Cleveland, OH 44114 USA. [Lauer, M.; Poirier, D. R.] Univ Arizona, Dept Mat Sci & Engn, Tucson, AZ 85721 USA. [Grugel, R. N.] NASA, Marshall Space Flight Space Ctr, Huntsville, AL 35811 USA. [Johnson, L.] Avery Dennison Corp, Painesville, OH 44077 USA. [Lauer, M.] ME Elecmetal Inc, Duluth, MN 55808 USA. RP Ghods, M (reprint author), Cleveland State Univ, Chem & Biomed Engn Dept, Cleveland, OH 44114 USA. EM ghods.masoud@gmail.com FU NASA [NX10AV40G, NNX14AM18G]; Sandia National Laboratories Campus Executive Fellowship program FX This work was supported by NASA Grant NX10AV40G and NNX14AM18G. The Al-7% Si alloys for our current research were kindly provided by Dr. Men G. Chu at ALCOA Technical Center. M. Lauer would like to acknowledge support from the Sandia National Laboratories Campus Executive Fellowship program. NR 54 TC 1 Z9 1 U1 6 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0248 EI 1873-5002 J9 J CRYST GROWTH JI J. Cryst. Growth PD SEP 1 PY 2016 VL 449 BP 134 EP 147 DI 10.1016/j.jcrysgro.2016.06.010 PG 14 WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied SC Crystallography; Materials Science; Physics GA DS5RT UT WOS:000380840700022 ER PT J AU Ryoo, MS Matthies, L AF Ryoo, M. S. Matthies, Larry TI First-Person Activity Recognition: Feature, Temporal Structure, and Prediction SO INTERNATIONAL JOURNAL OF COMPUTER VISION LA English DT Article ID CLASSIFICATION AB This paper discusses the problem of recognizing interaction-level human activities from a first-person viewpoint. The goal is to enable an observer (e.g., a robot or a wearable camera) to understand 'what activity others are performing to it' from continuous video inputs. These include friendly interactions such as 'a person hugging the observer' as well as hostile interactions like 'punching the observer' or 'throwing objects at the observer', whose videos involve a large amount of camera ego-motion caused by physical interactions. The paper investigates multi-channel kernels to integrate global and local motion information, and presents a new activity learning/recognition methodology that explicitly considers temporal structures displayed in first-person activity videos. Furthermore, we present a novel algorithm for early recognition (i.e., prediction) of activities from first-person videos, which allows us to infer ongoing activities at their early stage. In our experiments, we not only show classification results with segmented videos, but also confirm that our new approach is able to detect activities from continuous videos and perform early recognition reliably. C1 [Ryoo, M. S.; Matthies, Larry] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. RP Ryoo, MS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM mryoo@jpl.nasa.gov FU National Aeronautics and Space Administration; Army Research Laboratory FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This research was sponsored by the Army Research Laboratory and was accomplished under Cooperative Agreement Number W911NF-10-2-0016. NR 33 TC 0 Z9 0 U1 7 U2 10 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0920-5691 EI 1573-1405 J9 INT J COMPUT VISION JI Int. J. Comput. Vis. PD SEP PY 2016 VL 119 IS 3 SI SI BP 307 EP 328 DI 10.1007/s11263-015-0847-4 PG 22 WC Computer Science, Artificial Intelligence SC Computer Science GA DS0FE UT WOS:000380270000007 ER PT J AU Barre, J Edwards, D Worden, H Arellano, A Gaubert, B Da Silva, A Lahoz, W Anderson, J AF Barre, Jerome Edwards, David Worden, Helen Arellano, Avelino Gaubert, Benjamin Da Silva, Arlindo Lahoz, William Anderson, Jeffrey TI On the feasibility of monitoring carbon monoxide in the lower troposphere from a constellation of northern hemisphere geostationary satellites: Global scale assimilation experiments (Part II) SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Atmospheric composition; Global scale; Geostationary constellation; Remote sensing; OSSE; Carbon monoxide; CO lifetime; Long-range transport of pollution; Data assimilation ID EARTH SYSTEM MODEL; CHEMISTRY; OZONE; AEROSOLS; CO; EMISSIONS; GASES; BIAS AB This paper describes the second phase of an Observing System Simulation Experiment (OSSE) that utilizes the synthetic measurements from a constellation of satellites measuring atmospheric composition from geostationary (GEO) Earth orbit presented in part I of the study. Our OSSE is focused on carbon monoxide observations over North America, East Asia and Europe where most of the anthropogenic sources are located. Here we assess the impact of a potential GEO constellation on constraining northern hemisphere (NH) carbon monoxide (CO) using data assimilation. We show how cloud cover affects the GEO constellation data density with the largest cloud cover (i.e., lowest data density) occurring during Asian summer. We compare the modeled state of the atmosphere (Control Run), before CO data assimilation, with the known "true" state of the atmosphere (Nature Run) and show that our setup provides realistic atmospheric CO fields and emission budgets. Overall, the Control Run underestimates CO concentrations in the northern hemisphere, especially in areas close to CO sources. Assimilation experiments show that constraining CO close to the main anthropogenic sources significantly reduces errors in NH CO compared to the Control Run. We assess the changes in error reduction when only single satellite instruments are available as compared to the full constellation. We find large differences in how measurements for each continental scale observation system affect the hemispherical improvement in long-range transport patterns, especially due to seasonal cloud cover. A GEO constellation will provide the most efficient constraint on NH CO during winter when CO lifetime is longer and increments from data assimilation associated with source regions are advected further around the globe. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Barre, Jerome; Edwards, David; Worden, Helen; Gaubert, Benjamin; Anderson, Jeffrey] NCAR, Boulder, CO USA. [Arellano, Avelino] Univ Arizona, Tucson, AZ USA. [Da Silva, Arlindo] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Lahoz, William] NILU, Kjeller, Norway. RP Barre, J (reprint author), NCAR, Boulder, CO USA. EM barre@ucar.edu OI Arellano, Avelino/0000-0002-2615-5831 FU NASA [NNX09AH03G S02, NNX11AI10G, NNX11AG63G]; National Science Foundation FX This work was partly supported by NASA grants NNX09AH03G S02, NNX11AI10G and NNX11AG63G. The National Center for Atmospheric Research is sponsored by the National Science Foundation. The Climate Simulation Laboratory at NCAR's Computational and Information Systems Laboratory (CISL) provided computing resources. We would like to acknowledge high-performance computing support from Yellowstone (ark:/85065/d7wd3xhc) provided by NCAR's CISL. We also thank the reviewers for their constructive comments. NR 29 TC 0 Z9 0 U1 6 U2 16 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD SEP PY 2016 VL 140 BP 188 EP 201 DI 10.1016/j.atmosenv.2016.06.001 PG 14 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA DR7MG UT WOS:000380083200018 ER PT J AU Hamill, P Giordano, M Ward, C Giles, D Holben, B AF Hamill, Patrick Giordano, Marco Ward, Carolyne Giles, David Holben, Brent TI An AERONET-based aerosol classification using the Mahalanobis distance SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Atmospheric aerosols; Aerosol typing; AERONET; Mahalanobis distance; Seasonal aerosol variation; High AOD events ID OPTICAL-PROPERTIES; ABSORPTION; MODELS; TRANSPORT; POLLUTION; MIXTURES; NETWORK; CHINA; DUST; SIZE AB We present an aerosol classification based on AERONET aerosol data from 1993 to 2012. We used the AERONET Level 2.0 almucantar aerosol retrieval products to define several reference aerosol clusters which are characteristic of the following general aerosol types: Urban-Industrial, Biomass Burning, Mixed Aerosol, Dust, and Maritime. The classification of a particular aerosol observation as one of these aerosol types is determined by its five-dimensional Mahalanobis distance to each reference cluster. We have calculated the fractional aerosol type distribution at 190 AERONET sites, as well as the monthly variation in aerosol type at those locations. The results are presented on a global map and individually in the supplementary material. Our aerosol typing is based on recognizing that different geographic regions exhibit characteristic aerosol types. To generate reference clusters we only keep data points that lie within a Mahalanobis distance of 2 from the centroid. Our aerosol characterization is based on the AERONET retrieved quantities, therefore it does not include low optical depth values. The analysis is based on "point sources" (the AERONET sites) rather than globally distributed values. The classifications obtained will be useful in interpreting aerosol retrievals from satellite borne instruments. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Hamill, Patrick] San Jose State Univ, San Jose, CA 95192 USA. [Hamill, Patrick] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Giordano, Marco] Univ Nevada, Reno, NV 89557 USA. [Giordano, Marco] Desert Res Inst, Reno, NV USA. [Ward, Carolyne] Calif State Univ Long Beach, Long Beach, CA 90840 USA. [Giles, David; Holben, Brent] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Hamill, P (reprint author), San Jose State Univ, San Jose, CA 95192 USA.; Hamill, P (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM patrick.hamill@sjsu.edu NR 60 TC 0 Z9 0 U1 8 U2 14 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD SEP PY 2016 VL 140 BP 213 EP 233 DI 10.1016/j.atmosenv.2016.06.002 PG 21 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA DR7MG UT WOS:000380083200020 ER PT J AU Creamean, JM White, AB Minnis, P Palikonda, R Spangenberg, DA Prather, KA AF Creamean, Jessie M. White, Allen B. Minnis, Patrick Palikonda, Rabindra Spangenberg, Douglas A. Prather, Kimberly A. TI The relationships between insoluble precipitation residues, clouds, and precipitation over California's southern Sierra Nevada during winter storms SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Aerosol-cloud-precipitation interactions; Ice nucleation; Cloud glaciation; Sierra nevada ID SEEDER-FEEDER MECHANISM; MINERAL DUST PARTICLES; MIXED-PHASE CLOUDS; ICE-NUCLEATION; NORTHERN CALIFORNIA; ATMOSPHERIC RIVERS; OROGRAPHIC PRECIPITATION; AQUEOUS SAMPLES; ASIAN AEROSOLS; BARRIER JETS AB Ice formation in orographic mixed -phase clouds can enhance precipitation and depends on the type of aerosols that serve as ice nucleating particles (INPs). The resulting precipitation from these clouds is a viable source of water, especially for regions such as the California Sierra Nevada. Thus, a better understanding of the sources of INPs that impact orographic clouds is important for assessing water availability in California. This study presents a multi -site, multi -year analysis of single -particle insoluble residues in precipitation samples that likely influenced cloud ice and precipitation formation above Yosemite National Park. Dust and biological particles represented the dominant fraction of the residues (64% on average). Cloud glaciation, determined using satellite observations, not only depended on high cloud tops (>5.9 km) and low temperatures (<-23 degrees C), but also on the presence of what were likely dust and biological INPs. The greatest prevalence of ice -phase clouds occurred in conjunction with biologically -rich residues and mineral dust rich in calcium, followed by iron and aluminosilicates. Dust and biological particles are known to be efficient INPs, thus these residues likely influenced ice formation in clouds above the sites and subsequent precipitation quantities reaching the surface during events with similar meteorology. The goal of this study is to use precipitation chemistry information to gain a better understanding of the potential sources of INPs in the south-central Sierra Nevada, where cloud -aerosol precipitation interactions are poorly understood and where mixed -phase orographic clouds represent a key element in the generation of precipitation and thus the water supply in California. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Creamean, Jessie M.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Creamean, Jessie M.; White, Allen B.] NOAA, Earth Syst Res Lab, Div Phys Sci, Boulder, CO USA. [Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Palikonda, Rabindra; Spangenberg, Douglas A.] Sci Syst & Applicat Inc, Hampton, VA USA. [Prather, Kimberly A.] Univ Calif San Diego, Dept Chem & Biochem, La Jolla, CA 92093 USA. [Prather, Kimberly A.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. RP Creamean, JM (reprint author), NOAA, Earth Syst Res Lab, 325 Broadway,R-PSD2, Boulder, CO 80305 USA. EM jessie.creamean@noaa.gov RI Prather, Kimberly/A-3892-2008; OI Prather, Kimberly/0000-0003-3048-9890; Creamean, Jessie/0000-0003-3819-5600 FU National Research Council Research Associate Program [EA133F-10-CN-0187]; NASA Modeling, Analysis, and Prediction Program; DOE ARM Program FX The authors would like to acknowledge the staff at the National Park Service at Yosemite National Park for sample collection, including Katy Warner, who organized the collection protocols, Rebecca Rising, and Rob and Laura Pilewski. Ryan Spackman (NOAH/Science and Technology Corporation) and Daniel Murphy (NOAH) provided insightful feedback. We would also like to acknowledge the California Nevada River Forecast Center (CNRFC) and DWR for providing the HADS data and CASTNET for providing the meteorological measurements at YOS. The GPS WCR site data was courtesy of the Plate Boundary Observatory (PBO) network operated by UNAVCO. Thanks to Chris Yost for providing the satellite validation results. Jessie Creamean was partially supported by the National Research Council Research Associate Program (contract number EA133F-10-CN-0187). Patrick Minnis, Rabindra Palikonda, and Doug Spangenberg were supported by the NASA Modeling, Analysis, and Prediction Program and DOE ARM Program. Data presented in the manuscript tables and figures are available by email request to the corresponding author. NR 91 TC 1 Z9 1 U1 14 U2 25 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD SEP PY 2016 VL 140 BP 298 EP 310 DI 10.1016/j.atmosenv.2016.06.016 PG 13 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA DR7MG UT WOS:000380083200026 ER PT J AU Nyhan, M Sobolevsky, S Kang, CG Robinson, P Corti, A Szell, M Streets, D Lu, ZF Britter, R Barrett, SRH Ratti, C AF Nyhan, Marguerite Sobolevsky, Stanislav Kang, Chaogui Robinson, Prudence Corti, Andrea Szell, Michael Streets, David Lu, Zifeng Britter, Rex Barrett, Steven R. H. Ratti, Carlo TI Predicting vehicular emissions in high spatial resolution using pervasively measured transportation data and microscopic emission's model SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Air quality; Transportation; Emissions; Microscopic emissions model; Microscopic vehicle movement ID AIR-POLLUTION; LOS-ANGELES; VEHICLE; MORTALITY; CITIES; VARIABILITY; REDUCTION; EVOLUTION; NETWORKS; QUALITY AB Air pollution related to traffic emissions pose an especially significant problem in cities; this is due to its adverse impact on human health and well-being. Previous studies which have aimed to quantify emissions from the transportation sector have been limited by either simulated or coarsely resolved traffic volume data. Emissions inventories form the basis of urban pollution models, therefore in this study, Global Positioning System (GPS) trajectory data from a taxi fleet of over 15,000 vehicles were analyzed with the aim of predicting air pollution emissions for Singapore. This novel approach enabled the quantification of instantaneous drive cycle parameters in high spatio-temporal resolution, which provided the basis for a microscopic emissions model. Carbon dioxide (CO2), nitrogen oxides (NOx), volatile organic compounds (VOCs) and particulate matter (PM) emissions were thus estimated. Highly localized areas of elevated emissions levels were identified, with a spatio-temporal precision not possible with previously used methods for estimating emissions. Relatively higher emissions areas were mainly concentrated in a few districts that were the Singapore Downtown Core area, to the north of the central urban region and to the east of it. Daily emissions quantified for the total motor vehicle population of Singapore were found to be comparable to another emissions dataset Results demonstrated that high resolution spatio-temporal vehicle traces detected using GPS in large taxi fleets could be used to infer highly localized areas of elevated acceleration and air pollution emissions in cities, and may become a complement to traditional emission estimates, especially in emerging cities and countries where reliable fine-grained urban air quality data is not easily available. This is the first study of its kind to investigate measured microscopic vehicle movement in tandem with microscopic emissions modeling for a substantial study domain. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Nyhan, Marguerite; Robinson, Prudence; Britter, Rex; Ratti, Carlo] MIT, SENSEable City Lab, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Sobolevsky, Stanislav] NYU, Ctr Urban Sci & Progress, New York, NY USA. [Kang, Chaogui] Wuhan Univ, Wuhan, Hubei, Peoples R China. [Corti, Andrea] Politecn Milan, 32 Piazza Leonardo da Vinci, Milan, Italy. [Szell, Michael] Northeastern Univ, Dept Phys, Ctr Complex Network Res, Boston, MA 02115 USA. [Streets, David; Lu, Zifeng] NASA, Argonne Natl Lab, Lemont, IL USA. [Barrett, Steven R. H.] MIT, Dept Aeronaut & Astronaut, Cambridge, MA 02139 USA. RP Nyhan, M (reprint author), MIT, SENSEable City Lab, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM mnyhan@mit.edu OI Kang, Chaogui/0000-0002-0122-9419 FU MIT SENSEable City Lab Consortium; Singapore-MIT Alliance for Research & Technology program FX All the authors wish to thank the MIT SENSEable City Lab Consortium and the Singapore-MIT Alliance for Research & Technology program for supporting the research. M. Nyhan would like to thank Fulbright and the Irish Environmental Protection Agency. The authors would also like to acknowledge Dr. Luc Int. Panis for providing advice on some modeling aspects of the study. NR 68 TC 1 Z9 1 U1 30 U2 43 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD SEP PY 2016 VL 140 BP 352 EP 363 DI 10.1016/j.atmosenv.2016.06.018 PG 12 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA DR7MG UT WOS:000380083200031 ER PT J AU Villac, BF Anderson, RL Pini, AJ AF Villac, Benjamin F. Anderson, Rodney L. Pini, Alex J. TI Computer Aided Ballistic Orbit Classification Around Small Bodies SO JOURNAL OF THE ASTRONAUTICAL SCIENCES LA English DT Article DE Trajectory design; Periodic orbits; Clustering; Data mining; Asteroid missions ID INVARIANT-MANIFOLDS; TRAJECTORY DESIGN; RESONANCE; TRANSFERS; VESTA AB Orbital dynamics around small bodies are as varied as the shapes and dynamical states of these bodies. While various classes of orbits have been analyzed in detail, the global overview of relevant ballistic orbits at particular bodies is not easily computed or organized. Yet, correctly categorizing these orbits will ease their future use in the overall trajectory design process. This paper overviews methods that have been used to organize orbits, focusing on periodic orbits in particular, and introduces new methods based on clustering approaches. C1 [Villac, Benjamin F.] Ai Solut Inc, 4500 Forbes Blvd,Suite 300, Lanham, MD 20706 USA. [Anderson, Rodney L.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-121, Pasadena, CA 91109 USA. [Pini, Alex J.] NASA, GSFC, Ai Solut Inc, B28 N278, Greenbelt, MD 20771 USA. RP Villac, BF (reprint author), Ai Solut Inc, 4500 Forbes Blvd,Suite 300, Lanham, MD 20706 USA. EM benjamin.villac@ai-solutions.com FU AMMOS technology development task FX This research has been sponsored by the AMMOS technology development task. A portion of the research presented in this paper has been carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 60 TC 0 Z9 0 U1 23 U2 23 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0021-9142 EI 2195-0571 J9 J ASTRONAUT SCI JI J. Astronaut. Sci. PD SEP PY 2016 VL 63 IS 3 BP 175 EP 205 DI 10.1007/s40295-016-0089-x PG 31 WC Engineering, Aerospace SC Engineering GA DR7SW UT WOS:000380101000001 ER PT J AU Stickle, WB Lindeberg, M Rice, SD Munley, K Reed, V AF Stickle, William B. Lindeberg, Mandy Rice, Stanley D. Munley, Kathleen Reed, Victoria TI Seasonal changes in the thermal regime and gastropod tolerance to temperature and desiccation stress in the rocky intertidal zone in Southeast Alaska SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE Thermal regime; Temperature probes; Vertical gastropod zonation; Desiccation tolerance; Temperature tolerance ID HEAT-SHOCK RESPONSE; CLIMATE-CHANGE; PHYSIOLOGICAL ECOLOGY; GENUS PETROLISTHES; VERTICAL ZONATION; PORCELAIN CRABS; LIMITS; ACCLIMATION; PATTERNS; TEGULA AB Low tide emersion of intertidal fauna in the inside passage from Puget Sound, WA to Skagway, AK produces more extreme emersion temperatures than on the outer continental coastline because the timing of low tides increases the potential for summer high temperatures and winter low temperatures. This study documents seasonal changes in water/aerial temperatures at different tidal heights in 2007-2008 and the summer of 2015 and reports the high emersion temperature (5 h) and desiccation tolerance of three species of rocky shore gastropods. Vertical transects of probes were deployed at Bridget Cove at +5.0 m (above the tidal range), +3.5, +2.5 m, +1.5 m and 0 m. Two additional probes were partially buried at +1.5 m; burial ameliorated freezing temperatures. Duration of emersion increased with intertidal height and was of longer duration at +3.5 m during Neap tides and at +1.5 and 0 m during Spring tides. Monthly measures of temperature were: average temperature, monthly maximum, average daily monthly maximum, average daily monthly minimum, and monthly minimum. Monthly maximum air temperature increased with tidal height. Winter average daily monthly minimum fell below 0 degrees C at the +3.5, +2.5, and +1.5 m tidal heights for the aerially exposed probes. The number of days when emersion temperature fell below 0 degrees C increased with intertidal height as did the number of hours per day. High temperature emersion tolerance of Nucella lamellosa, Nucella lima and Littorina sitkana varied directly with their intertidal range but their desiccation tolerance did not suggesting that desiccation is not an abiotic stressor in this temperate rain forest intertidal zone. The LT50 temperature (5 h) was considerably above recorded monthly maximum temperatures in the vertical range of N. lamellosa and L. sitkana but the LT50 of N. lima was very near the maximum monthly temperature at +2.5 m. (C) 2016 Elsevier B.V. All rights reserved. C1 [Stickle, William B.; Munley, Kathleen] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Lindeberg, Mandy; Rice, Stanley D.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Lab, Juneau, AK 99801 USA. [Reed, Victoria] Louisiana State Univ, Div Comp Sci & Engn, Baton Rouge, LA 70803 USA. RP Stickle, WB (reprint author), Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. EM zostic@lsu.edu NR 39 TC 1 Z9 1 U1 30 U2 58 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 EI 1879-1697 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD SEP PY 2016 VL 482 BP 56 EP 63 DI 10.1016/j.jembe.2016.04.011 PG 8 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA DQ7EW UT WOS:000379370700006 ER PT J AU Babcock, C Finley, AO Cook, BD Weiskittel, A Woodall, CW AF Babcock, Chad Finley, Andrew O. Cook, Bruce D. Weiskittel, Aaron Woodall, Christopher W. TI Modeling forest biomass and growth: Coupling long-term inventory and LiDAR data SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE LiDAR; Forest biomass; Biomass growth; Temporal misalignment; Long-term forest inventory; Bayesian hierarchical models; Markov Chain Monte Carlo; Gaussian process; Geospatial ID ABOVEGROUND BIOMASS; CANOPY HEIGHT; CARBON; AIRBORNE; REGRESSION; VARIABLES; COMPLEX; MISSION; PLOTS AB Combining spatially-explicit long-term forest inventory and remotely sensed information from Light Detection and Ranging (LiDAR) datasets through statistical models can be a powerful tool for predicting and mapping above-ground biomass (AGB) at a range of geographic scales. We present and examine a novel modeling approach to improve prediction of AGB and estimate AGB growth using LiDAR data. The proposed model accommodates temporal misalignment between field measurements and remotely sensed data a problem pervasive in such settings by including multiple time-indexed measurements at plot locations to estimate AGB growth. We pursue a Bayesian modeling framework that allows for appropriately complex parameter associations and uncertainty propagation through to prediction. Specifically, we identify a space-varying coefficients model to predict and map AGB and its associated growth simultaneously. The proposed model is assessed using LiDAR data acquired from NASA Goddard's LiDAR, Hyper-spectral & Thermal imager and field inventory data from the Penobscot Experimental Forest in Bradley, Maine. The proposed model outperformed the time-invariant counterpart models in predictive performance as indicated by a substantial reduction in root mean squared error. The proposed model adequately accounts for temporal misalignment through the estimation of forest AGB growth and accommodates residual spatial dependence. Results from this analysis suggest that future AGB models informed using remotely sensed data, such as LiDAR, may be improved by adapting traditional modeling frameworks to account for temporal misalignment and spatial dependence using random effects. (C) 2016 Elsevier Inc. All rights reserved. C1 [Babcock, Chad] Univ Washington, Sch Environm & Forest Sci, Seattle, WA 98195 USA. [Finley, Andrew O.] Michigan State Univ, Dept Forestry, E Lansing, MI 48824 USA. [Cook, Bruce D.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Code 618, Greenbelt, MD 20742 USA. [Weiskittel, Aaron] Univ Maine, Sch Forest Resources, Orono, ME 04469 USA. [Woodall, Christopher W.] US Forest Serv, USDA, No Res Stn, Forest Inventory & Anal Program, 1992 Folwell Ave, St Paul, MN 55114 USA. RP Babcock, C (reprint author), Univ Washington, Sch Environm & Forest Sci, Seattle, WA 98195 USA. OI Babcock, Chad/0000-0001-9597-4462 FU U.S. Forest Service [USFS 15-JV-11242307-116]; National Science Foundation (NSF) [DMS-1513481, EF-1137309, EF-1241874, EF-1253225]; NASA Carbon Monitoring System grants FX Data for this study were provided by a unit of the Northern Research Station, U.S. Forest Service, located at the Penobscot Experimental Forest in Maine. Significant funding for collection of these data was provided by the U.S. Forest Service (USFS 15-JV-11242307-116). Andrew Finley was supported by National Science Foundation (NSF) DMS-1513481, EF-1137309, EF-1241874, and EF-1253225, as well as NASA Carbon Monitoring System grants. NR 52 TC 0 Z9 0 U1 29 U2 84 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 SEP 1 PY 2016 VL 182 BP 1 EP 12 DI 10.1016/j.rse.2016.04.014 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA DQ3HP UT WOS:000379093700001 ER PT J AU Huesca, M Garcia, M Roth, KL Casas, A Ustin, SL AF Huesca, Margarita Garcia, Mariano Roth, Keely L. Casas, Angeles Ustin, Susan L. TI Canopy structural attributes derived from AVIRIS imaging spectroscopy data in a mixed broadleaf/conifer forest SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Canopy structure; AVIRIS; LiDAR; Random forest; Structural types ID SPECTRAL MIXTURE ANALYSIS; REMOTE-SENSING DATA; VEGETATION INDEXES; HYPERSPECTRAL DATA; AIRBORNE LIDAR; WATER-CONTENT; NITROGEN-CONTENT; ABOVEGROUND BIOMASS; SPATIAL-PATTERNS; LANDSAT IMAGERY AB There is a well-established need within the remote sensing community for improved estimation and understanding of canopy structure and its influence on the retrieval of leaf biochemical properties. The main goal of this research was to assess the potential of optical spectral information from NASA's Airborne Visible/Infrared Imaging Spectrometer (AVIRIS) to discriminate different canopy structural types. In the first phase, we assessed the relationships between optical metrics and canopy structural parameters obtained from LiDAR in terms of different canopy structural attributes (biomass (i.e., area under Vegetation Vertical Profile, VVPint), canopy height and vegetation complexity). Secondly, we identified and classified different "canopy structural types" by integrating several structural traits using Random Forests (RF). The study area is a heterogeneous forest in Sierra National Forest in California (USA). AVIRIS optical properties were analyzed by means of several sets of variables, including single narrow band reflectance and 1st derivative, sub-pixel cover fractions, narrow-band indices, spectral absorption features, optimized normalized difference indices and Principal Component Analysis (PCA) components. Our results demonstrate that optical data contain structural information that can be retrieved. The first principal component, used as a proxy for albedo, was the most strongly correlated optical metric with vegetation complexity, and it also correlated well with biomass (VVPint) and height. In conifer forests, the shade fraction was especially correlated to vegetation complexity, while water-sensitive optical metrics had high correlations with biomass (VVPint). Single spectral band analysis results showed that correlations differ in magnitude and in direction, across the spectrum and by vegetation type and structural variable. This research illustrates the potential of AVIRIS to analyze canopy structure and to distinguish several structural types in a heterogeneous forest. Furthermore, RF using optical metrics derived from AVIRIS proved to be a powerful technique to generate maps of structural attributes. The results emphasize the importance of using the whole optical spectrum, since all spectral regions contributed to canopy structure assessment (C) 2016 Elsevier Inc. All rights reserved. C1 [Huesca, Margarita; Roth, Keely L.; Casas, Angeles; Ustin, Susan L.] Univ Calif Davis, CSTARS, Land Air & Water Resources Dept, Davis, CA 95616 USA. [Garcia, Mariano] Univ Leicester, Ctr Landscape & Climate Res, Leicester LE1 7RH, Leics, England. [Garcia, Mariano] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Huesca, M (reprint author), Univ Calif Davis, CSTARS, Davis, CA 95616 USA. EM mhuescamartinez@ucdavis.edu FU HyspIRI Planning Mission (NASA Grant) [NNX12AP87G]; Marie Curie IOF (ForeStMap - 3D Forest Structure Monitoring and Mapping) [629376] FX This research was conducted within the framework of the HyspIRI Planning Mission (NASA Grant # NNX12AP87G). Mariano Garcia is supported by the Marie Curie IOF (ForeStMap - 3D Forest Structure Monitoring and Mapping, Project Reference: 629376). The contents on this paper reflect only the authors' views and not the views of the European Commission. I would like to thank NEON for providing the LiDAR data and the NASA JPL AVIRIS team for collecting and preprocessing the hyperspectral data. I would also thank the anonymous reviewers for their help in improving the manuscript. NR 129 TC 3 Z9 3 U1 21 U2 40 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 SEP 1 PY 2016 VL 182 BP 208 EP 226 DI 10.1016/j.rse.2016.04.020 PG 19 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA DQ3HP UT WOS:000379093700016 ER PT J AU Malakar, NK Hulley, GC AF Malakar, Nabin K. Hulley, Glynn C. TI A water vapor scaling model for improved land surface temperature and emissivity separation of MODIS thermal infrared data SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE MODIS; Land surface temperature; Atmospheric correction; Thermal infrared; Emissivity; Validation; Infrared image sensors; Remote sensing ID ATMOSPHERIC CORRECTION; SOIL RESPIRATION; ENERGY-BALANCE; AVHRR DATA; ASTER; ALGORITHM; PRODUCTS; VALIDATION; RADIOMETER; SATELLITE AB We present an improved water vapor scaling (WVS) model for atmospherically correcting MODIS thermal infrared (TIR) bands in the temperature emissivity separation (TES) algorithm. TES is used to retrieve the land surface temperature and emissivity (LST&E) from MODIS TIR bands 29, 31, and 32. The WVS model improves the accuracy of the atmospheric correction parameters in TES on a band-by-band and pixel-by-pixel basis. We used global atmospheric radiosondes profiles to generate view angle and day-night-dependent WVS coefficients that are valid for all MODIS scan angles up to 65. We demonstrate the effects of applying the improved WVS model on the retrieval accuracy of MODIS-TES (MODTES) LST&E using a case study for a granule over the southwest USA during very warm and moist monsoonal atmospheric conditions. Furthermore, a comprehensive validation of the MODTES LST&E retrieval was performed over two sites at the quartz-rich Algodones Dunes in California and a grassland site in Texas, USA using three full years of MODIS Aqua data. Results from the case study showed that absolute errors in the emissivity retrieval for the three MODIS TIR bands were reduced on average from 1.4% to 0.4% when applying the WVS method. A Radiance-based method was used to validate the MODTES LST retrievals for and the results showed that application of the WVS method with the MODTES algorithm led to significant reduction in both bias and root mean square error (RMSE) of the LST retrievals at both sites. When the WVS model was applied, LST RMSE's were reduced on average from 1.3 K to 1.0 K at the Algodones Dunes site, and from 1.2 K to 0.7 K at the Texas Grassland site. This study demonstrated that the WVS atmospheric correction model is critical for retrieving MODTES LST with <1 K accuracy and emissivity with <1% consistently for a wide range of challenging atmospheric conditions and land surface types. (C) 2016 Elsevier Inc. All rights reserved. C1 [Malakar, Nabin K.; Hulley, Glynn C.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Malakar, NK (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Nabin.K.Malakar@jpl.nasa.gov OI Malakar, Nabin/0000-0002-4816-6304 FU NASA ROSES grant [NRA NNH13ZDA001N] FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This study is supported by the NASA ROSES 2013 grant (NRA NNH13ZDA001N). NR 53 TC 1 Z9 1 U1 16 U2 29 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD SEP 1 PY 2016 VL 182 BP 252 EP 264 DI 10.1016/j.rse.2016.04.023 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA DQ3HP UT WOS:000379093700018 ER PT J AU Cho, Y Sugita, S Miura, YN Okazaki, R Iwata, N Morota, T Kameda, S AF Cho, Yuichiro Sugita, Seiji Miura, Yayoi N. Okazaki, Ryuji Iwata, Naoyoshi Morota, Tomokatsu Kameda, Shingo TI An in-situ K-Ar isochron dating method for planetary landers using a spot-by-spot laser-ablation technique SO PLANETARY AND SPACE SCIENCE LA English DT Article DE In-situ geochronology; K-Ar dating; Planetary missions; Laser-induced breakdown spectroscopy; Noble gas mass spectrometry ID INNER SOLAR-SYSTEM; LUNAR CATACLYSM; GALE CRATER; MARS; CHRONOLOGY; ORIGIN; AGES; MASS; GEOCHRONOLOGY; STRATIGRAPHY AB Age is essential information for interpreting the geologic record on planetary surfaces. Although crater counting has been widely used to estimate the planetary surface ages, crater chronology in the inner solar system is largely built on radiometric age data from limited sites on the Moon. This has resulted in major uncertainty in planetary chronology. Because opportunities for sample-return missions are limited, in-situ geochronology measurements from one-way lander/rover missions are extremely valuable. Here we developed an in-situ isochron-based dating method using the K-Ar system, with K and Ar in a single rock sample extracted locally by laser ablation and measured using laser-induced breakdown spectroscopy (LIBS) and a quadrupole mass spectrometer (QMS), respectively. We built an experimental system combining flight equivalent instruments and measured K-Ar ages for mineral samples with known ages (similar to 1.8 Ga) and K contents (1-8 wt%); we achieved precision of 20% except for a mineral with low mechanical strength. Furthermore, validation measurements with two natural rocks (gneiss slabs) obtained K-Ar isochron ages and initial Ar-40 consistent with known values for both cases. This result supports that our LIBS-MS approach can derive both isochron ages and contributions of non-in situ radiogenic Ar-40 from natural rocks. Error assessments suggest that the absolute ages of key geologic events including the Noachian/Hesperian- and the Hesperian/Amazonian-transition can be dated with 10-20% errors for a rock containing similar to 1 wt% K2O, greatly reducing the uncertainty of current crater chronology models on Mars. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Cho, Yuichiro; Sugita, Seiji] Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. [Cho, Yuichiro; Kameda, Shingo] Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan. [Miura, Yayoi N.] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, 1-1-1 Yayoi, Tokyo 1130032, Japan. [Okazaki, Ryuji] Kyushu Univ, Dept Earth & Planetary Sci, Nishi Ku, 744 Motooka, Fukuoka 8190395, Japan. [Iwata, Naoyoshi] Yamagata Univ, Dept Earth & Environm Sci, 1-4-12 Kojirakawa, Yamagata 9908560, Japan. [Morota, Tomokatsu] Nagoya Univ, Dept Earth & Planetary Sci, Chikusa Ku, Nagoya, Aichi 4648601, Japan. [Cho, Yuichiro] NASA, Marshall Space Flight Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA. RP Cho, Y (reprint author), Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan. EM cho@rikkyo.ac.jp RI Iwata, Naoyoshi/B-7554-2008 OI Iwata, Naoyoshi/0000-0002-0017-9130 FU Institute of Space and Aeronautical Science (ISAS)/Japan Aerospace Exploration Agency (JAXA); Japan Society for the Promotion of Science (JSPS) [26247092]; JSPS [15K17796] FX The authors are grateful to two anonymous reviewers whose careful reading of this paper led to a number of significant improvements. This study was supported by funds from the Institute of Space and Aeronautical Science (ISAS)/Japan Aerospace Exploration Agency (JAXA) and by Japan Society for the Promotion of Science (JSPS) Grant-in-Aid in Scientific Research Grant Number 26247092. Y. Cho was supported by JSPS Grant-in-Aid for Young Scientists (B.) Grant Number 15K17796. The authors thank Keisuke Nagao of the University of Tokyo for providing the mineral samples. We would like to thank Takahiko Yagi, Ehime University, and Hirotada Goto, the University of Tokyo for assistance in making the pellet samples with a cubic press at the Institute of Solid State Physics, the University of Tokyo. The authors thank Naoto Ishikawa of Kyoto University and the 41st and 42nd Japanese Antarctic Research Expedition Program for acquiring the gneiss samples. Asako Takamasa in Japan Agency for Marine-Earth Science and Technology (JAMSTEC) is acknowledged for separating biotites from the gneiss rocks. We are thankful to Kenji Mibe at Earthquake Research Institute, the University of Tokyo, for preparing a basaltic glass sample used for Ar measurements. All data and programs used for producing the results in this paper are available from the lead author on request (cho@rikkyo.ac.jp). NR 59 TC 1 Z9 1 U1 10 U2 21 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD SEP 1 PY 2016 VL 128 BP 14 EP 29 DI 10.1016/j.pss.2016.05.004 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DQ1LA UT WOS:000378961300002 ER PT J AU Guo, JP Liu, H Wang, F Huang, JF Xia, F Lou, MY Wu, YR Jiang, JH Xie, T Zhaxi, YZ Yung, YL AF Guo, Jianping Liu, Huan Wang, Fu Huang, Jingfeng Xia, Feng Lou, Mengyun Wu, Yerong Jiang, Jonathan H. Xie, Tao Zhaxi, Yangzong Yung, Yuk L. TI Three-dimensional structure of aerosol in China: A perspective from multi-satellite observations SO ATMOSPHERIC RESEARCH LA English DT Article DE CALIOP; Dust; Smoke; Frequency of occurrence; China ID AIR-POLLUTION; INDUCED VARIABILITY; EASTERN CHINA; NORTH-AMERICA; WARM CLOUDS; TRANSPORT; PRECIPITATION; DUST; ATMOSPHERE; ATLANTIC AB Using eight years (2006-2014) of passive (MODIS/Aqua and OMI/Aura) and active (CALIOP/CALIPSO) satellite measurements of aerosols, we yield a three-dimensional (3D) distribution of the frequency of occurrence (FoO) of aerosols over China. As an indicator of the vertical heterogeneity of aerosol layers detected by CALIOP, two types of Most Probable Height (MPH), including MPH_FoO and MPH_AOD, are deduced. The FoO of "Total Aerosol" reveals significant geographical dependence. Eastern China showed much stronger aerosol FoD than northwestern China. The FoO vertical structures of aerosol layer are strongly dependent on altitudes. Among the eight typical ROls analyzed, aerosol layers over the Gobi Desert have the largest occurrence probability located at an altitude as high as 2.83 km, as compared to 126 km over Beijing-Tianjin-Hebei. The diurnal variation (nighttime-daytime) in MPH_AOD varies from an altitude as low as 0.07 km over the Sichuan basin to 0.27 km over the Gobi Desert, whereas the magnitude of the diurnal variation in terms of MPH_AOD is six times as large as the MPH_FoO, mostly attributable to the day/night lidar SNR difference. Also, the 3D distribution of dust and smoke aerosols was presented. The multi-sensor synergized 3D observations of dust aerosols, frequently observed in the zonal belt of 38 degrees N-45 degrees N, is markedly different from that of smoke aerosols that are predominantly located in the eastern and southern parts. The 3D FoO distribution of dust indicates a west-to-east passageway of dust originating from the westernmost Taklimakan Desert all the way to North China Plain (NCP). The findings from the multi-sensor synergetic observations greatly improved our understanding on the long-range aerosol dispersion, transport and passageway over China. (C) 2016 Elsevier B.V. All rights reserved. C1 [Guo, Jianping; Liu, Huan; Xia, Feng; Lou, Mengyun] Chinese Acad Meteorol Sci, State Key Lab Severe Weather, Beijing 100081, Peoples R China. [Wang, Fu] China Meteorol Adm, Natl Satellite Meteorol Ctr, Beijing 100081, Peoples R China. [Huang, Jingfeng] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. [Wu, Yerong] Delft Univ Technol, Geosci & Remote Sensing Fac Civil Engn & Geosci, NL-2628 CN Delft, Netherlands. [Jiang, Jonathan H.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Xie, Tao] Guangzhou MapUniverse Technol Co Ltd, Guangzhou 510070, Guangdong, Peoples R China. [Guo, Jianping; Zhaxi, Yangzong] Tibetan Inst Atmospher Environm & Sci, Lhasa 850000, Peoples R China. [Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Guo, JP (reprint author), Chinese Acad Meteorol Sci, 46 Zhong Guan Cun South Ave, Beijing 100081, Peoples R China. EM jpguo@camscma.cn RI Huang, Jingfeng/D-7336-2012 OI Huang, Jingfeng/0000-0002-8779-2922 FU Ministry of Science and Technology of the People's Republic of China [2014BAC16B01]; Natural Science Foundation of China [91544217, 41471301, 41171294]; Chinese Academy of Meteorological Sciences [2014R18]; Guangdong Provincial Science and Technology Plan Projects [2014A010101151]; NASA; California Institute of Technology FX This work was carried out under the auspices of the Ministry of Science and Technology of the People's Republic of China (Grant no. 2014BAC16B01), the Natural Science Foundation of China (Grant nos. 91544217, 41471301 and 41171294), the Chinese Academy of Meteorological Sciences (Grant no. 2014R18), and Guangdong Provincial Science and Technology Plan Projects (Grant no. 2014A010101151). The MODIS AOD data used in this study were also, acquired as part of the NASA's Earth-Sun System Division and archived and distributed by the Goddard Earth Sciences (GES) Data and Information Services Center (DISC) Distributed Active Archive Center (DAAC). Authors JHJ and YY thank the support by the NASA sponsored Jet Propulsion Laboratory and by the California Institute of Technology. NR 52 TC 3 Z9 3 U1 13 U2 26 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 SEP 1 PY 2016 VL 178 BP 580 EP 589 DI 10.1016/j.atmosres.2016.05.010 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DP2YY UT WOS:000378360700049 ER PT J AU Langseth, BJ Schueller, AM Shertzer, KW Craig, JK Smith, JW AF Langseth, Brian J. Schueller, Amy M. Shertzer, Kyle W. Craig, J. Kevin Smith, Joseph W. TI Management implications of temporally and spatially varying catchability for the Gulf of Mexico menhaden fishery SO FISHERIES RESEARCH LA English DT Article DE Catchability; Hypoxia; Spatio-temporal variation; Stock assessment; Gulf menhaden ID STOCK ASSESSMENT MODELS; BROWN SHRIMP; HYPOXIA; PERFORMANCE; ABUNDANCE; YIELD; AREA AB Catchability relates fishing effort to fishing mortality, and is an important component in fishery stock assessment models. Mis-specifying catchability can lead to inaccurate estimation of model parameters and bias in the determination of stock status. The Gulf of Mexico has one of the largest seasonal occurrences of hypoxia in the world and it overlaps in time and space with the Gulf menhaden Brevoortia patronus fishery, potentially leading to temporal and spatial patterns in stock distribution and thus catchability. These patterns are not currently modeled in the Gulf menhaden stock assessment. To better understand the implications of spatial and temporal patterns in catchability due to hypoxia, we constructed an operating model of Gulf menhaden fishery dynamics under various assumptions of spatial coverages and temporal patterns, and used the output from the operating model as input into estimation models with alternative approaches on modeling catchability. Under the most extreme assumptions about the spatial coverage and magnitude of variation in catchability, median absolute error in estimates of fishing mortality and spawning stock reference points (F-30% and S-30%) was 73% and 29%, respectively, and median absolute error in estimates of fishing mortality and spawning stock based stock status was 23% and 79%, supporting the notion that errors in catchability are important. Under more reasonable assumptions, median absolute error declined to 20% and 2.9% for F-30% and S-30%, respectively, and to 3.8% and 2.4% for fishing mortality and spawning stock-based stock status, respectively. Modeling catchability as a random walk further reduced median absolute error to 5.0% for F-30% and 1.4% for S-30%, but slightly increased median absolute error for stock status indicators to 4.0% and 3.3%. Our results show generally that the spatial coverage, temporal pattern, and estimation approach of catchability affects the influence of mis-specifying catchability; and show specifically that the Gulf menhaden stock assessment is robust to the effects of hypoxia on catchability if assuming random-walk catchability. Published by Elsevier B.V. C1 [Langseth, Brian J.; Schueller, Amy M.; Shertzer, Kyle W.; Craig, J. Kevin; Smith, Joseph W.] NOAA, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, 101 Pivers Isl Rd, Beaufort, NC 28516 USA. [Langseth, Brian J.] NOAA, Natl Marine Fisheries Serv, Pacific Islands Fisheries Sci Ctr, 1845 Wasp Blvd,Bldg 176, Honolulu, HI 96818 USA. RP Langseth, BJ (reprint author), NOAA, Natl Marine Fisheries Serv, Pacific Islands Fisheries Sci Ctr, 1845 Wasp Blvd,Bldg 176, Honolulu, HI 96818 USA. EM brian.langseth@noaa.gov FU Fisheries and the Environment (FATE) Program of the National Oceanic and Atmospheric Administration (NOAA) FX We thank A. Yau and K. Siegfried, J. Thorson, and an anonymous reviewer for contributions to previous drafts of the manuscript. This research was supported by a grant from the Fisheries and the Environment (FATE) Program of the National Oceanic and Atmospheric Administration (NOAA). The views expressed herein are those of the authors and do not necessarily reflect the view of NOAA or any of its subagencies. NR 42 TC 0 Z9 0 U1 21 U2 25 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-7836 EI 1872-6763 J9 FISH RES JI Fish Res. PD SEP PY 2016 VL 181 BP 186 EP 197 DI 10.1016/j.fishres.2016.04.013 PG 12 WC Fisheries SC Fisheries GA DP0LS UT WOS:000378181900019 ER PT J AU Pajola, M Rossato, S Carter, J Baratti, E Pozzobon, R Erculiani, MS Coradini, M McBride, K AF Pajola, Maurizio Rossato, Sandro Carter, John Baratti, Emanuele Pozzobon, Riccardo Erculiani, Marco Sergio Coradini, Marcello McBride, Karen TI Eridania Basin: An ancient paleolake floor as the next landing site for the Mars 2020 rover SO ICARUS LA English DT Article DE Mars, surface; Geological processes; Spectroscopy; Image processing; Exobiology ID ORBITER LASER ALTIMETER; EMISSION SPECTROMETER EXPERIMENT; LACUSTRINE ENVIRONMENTS; PHYSICAL-PROPERTIES; THERMAL INERTIA; MARTIAN SURFACE; GLOBAL SURVEYOR; MAADIM-VALLIS; CRATER LAKES; ORIGIN AB The search for traces of past Martian life is directly connected to ancient paleolakes, where ponding water or low-energy water fluxes were present for long time intervals. The Eridania paleolakes system, located along the 180 meridian, is one of the largest lacustrine environments that were once present on Mars. Morphological features suggest that it was constituted by connected depressions filled by water to maximum depths of similar to 2400 m and a volume of at least 562,000 km(3). We focused our attention on the northern side of the Eridania Basin, where high-albedo, uneven patches of material characterized by the absence of dust are present. Based on OMEGA and CRISM orbital imaging spectroscopy data, a large clay-bearing unit has been identified there. In particular, a set of aqueous minerals in present in the stratigraphy, being visible through erosional windows in the first several tens of meters of the sedimentary sequence. Below this capping unit, a thin Al-rich clay stratum attributable to Al-smectite and/or kaolins is present. This overlies a Fe-rich clay stratum, attributable to the nontronite smectite. At the base of the mineralogic sequence a stratum that could be either a zeolite or more likely a hydrated sulfate is present. In addition, small deposits of alunite (a rare phase on Mars), and jarosite are here found at several locations. Such stratigraphy is interpreted as originating from a surface weathering process similar to terrestrial abiotic pedogenesis; nonetheless, possible exobiologic processes can be also invoked to explain it. NASA's Spirit rover landed on Gusev crater in 2004, near the mouth of the Ma'adim Vallis, which connects this crater with the considered paleolakes system. The Eridania site provides the unique opportunity to complete the measurements obtained in Gusev crater, while investigating the exposed mineralogical sequence in its depositionary setting. In addition, the extremely favorable landing parameters, such as elevation, slope, roughness, rock distribution, thermal inertia and dust coverage, support this location as a possible landing site for the NASA Mars 2020 rover. (C) 2016 Elsevier Inc. All rights reserved. C1 [Pajola, Maurizio] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Pajola, Maurizio; Erculiani, Marco Sergio] Univ Padua, Ctr Studies & Act Space G Colombo, Via Venezia 15, I-35131 Padua, Italy. [Rossato, Sandro; Pozzobon, Riccardo] Univ Padua, Geosci Dept, I-3513 Padua, Italy. [Carter, John] Univ Paris 11, IAS, F-91405 Orsay, France. [Baratti, Emanuele] Univ Bologna, Dept DICAM, Sch Civil Engn, I-40136 Bologna, Italy. [Coradini, Marcello] European Space Agcy, F-75015 Paris, France. [Coradini, Marcello] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [McBride, Karen] Univ Calif Los Angeles, Los Angeles, CA 90024 USA. RP Pajola, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM maurizio.pajola@nasa.gov OI Pajola, Maurizio/0000-0002-3144-1277; Coradini, Marcello/0000-0002-1711-3197 NR 142 TC 0 Z9 0 U1 13 U2 24 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 SEP 1 PY 2016 VL 275 BP 163 EP 182 DI 10.1016/j.icarus.2016.03.029 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO8FB UT WOS:000378016900012 ER PT J AU Meriggiola, R Iess, L Stiles, BW Lunine, JI Mitri, G AF Meriggiola, Rachele Iess, Luciano Stiles, Bryan. W. Lunine, Jonathan. I. Mitri, Giuseppe TI The rotational dynamics of Titan from Cassini RADAR images SO ICARUS LA English DT Article DE Titan, interior; Satellites, dynamics; Geophysics ID INTERNAL STRUCTURE; GRAVITY-FIELD; OCEAN; TOPOGRAPHY; OBLIQUITY; STATE; SHAPE; ICE AB Between 2004 and 2009 the RADAR instrument of the Cassini mission provided 31 SAR images of Titan. We tracked the position of 160 surface landmarks as a function of time in order to monitor the rotational dynamics of Titan. We generated and processed RADAR observables using a least squares fit to determine the updated values of the rotational parameters. We provide a new rotational model of Titan, which includes updated values for spin pole location, spin rate, precession and nutation terms. The estimated pole location is compatible with the occupancy of a Cassini state 1. We found a synchronous value of the spin rate (22.57693 deg/day), compatible at a 3-sigma level with IAU predictions. The estimated obliquity is equal to 0.31, incompatible with the assumption of a rigid body with fully-damped pole and a moment of inertia factor of 0.34, as determined by gravity measurements. (C) 2016 Elsevier Inc. All rights reserved. C1 [Meriggiola, Rachele; Iess, Luciano] Univ Roma La Sapienza, Dipartimento Ingn Meccan & Aerospaziale, Via Eudossiana 18, I-00184 Rome, Italy. [Stiles, Bryan. W.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Lunine, Jonathan. I.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Mitri, Giuseppe] Univ Nantes, Lab Planetol & Geodynam Nantes, Nantes, France. RP Meriggiola, R (reprint author), Univ Roma La Sapienza, Dipartimento Ingn Meccan & Aerospaziale, Via Eudossiana 18, I-00184 Rome, Italy. EM rachele.meriggiola@uniromal.it RI IESS, Luciano/F-4902-2011 OI IESS, Luciano/0000-0002-6230-5825 FU Cassini Project FX We thank W. Jacobson and the Cassini Navigation Team (JPL) for the provided support on the error source analysis. Support by the Cassini Project is gratefully acknowledged. JIL is grateful for support from the Cassini Project. A portion of the work described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 33 TC 3 Z9 3 U1 2 U2 2 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD SEP 1 PY 2016 VL 275 BP 183 EP 192 DI 10.1016/j.icarus.2016.01.019 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO8FB UT WOS:000378016900013 ER PT J AU Gautier, T Schmitz-Afonso, I Touboul, D Szopa, C Buch, A Carrasco, N AF Gautier, Thomas Schmitz-Afonso, Isabelle Touboul, David Szopa, Cyril Buch, Arnaud Carrasco, Nathalie TI Development of HPLC-Orbitrap method for identification of N-bearing molecules in complex organic material relevant to planetary environments SO ICARUS LA English DT Article DE Titan, atmosphere; Atmospheres, chemistry; Organic chemistry; Prebiotic chemistry ID TITANS THOLINS PRODUCTION; COMETARY ICE ANALOGS; MASS-SPECTROMETRY; HEXAMETHYLENETETRAMINE HMT; PREBIOTIC CHEMISTRY; INTERSTELLAR ICE; SOLID-STATE; PRODUCTS; MELAMINE; SPECTROSCOPY AB Although the cassini Spacecraft and the Huygens Lander provided vast information about Titan atmospheric chemistry and the formation of its aerosols, the exact composition of these aerosols still remains unknown. A fruitful proxy to investigate these aerosols is the use of laboratory experiments that allow producing and studying analogs of Titan aerosol, the so-called tholins. Even when produced in the laboratory, unveiling the exact composition of the aerosol remains problematic due to the high complexity of the material. Numerous advances have been recently made using high-resolution mass spectrometry (HRMS) (Pernot et al. [2010] Anal. Chem. 82, 1371; Somogyi et al. [2012] Int. J. Mass Spectrom. 316-318, 157-163; Gautier et al. [2014] Earth Planet. Sci. Lett. 404, 33-42) that allowed the separation of isobaric compounds and a robust identification of chemical species composing tholins regarding their molecular formulae. Nevertheless isomeric species cannot be resolved by a simple mass measurement. We propose here an analysis of tholins by high performance liquid chromatography (HPLC) coupled to HRMS to unveil this isomeric ambiguity for some of the major tholins compounds. By comparing chromatograms obtained when analyzing tholins and chemical standards, we strictly identified seven molecules in our tholins samples: melamine, cyanoguanidine, 6-methyl-1,3,5-triazine-2,4-diamine, 2,4,6-triaminopyrimidine, 3-amino-1,2,4-triazole, 3,5-Dimethyl-1,2,4-triazole and 2,4-diamino-1,3,5-triazine. Several molecules, including hexamethylenetriamine (HMT) were not present at detectable levels in our sample. The use for the first time of a coupled HPLC-HRMS technique applied to tholins study demonstrated the interest of such a technique compared to single high-resolution mass spectrometry for the study of tholins composition. (C) 2016 Elsevier Inc. All rights reserved. C1 [Gautier, Thomas] NASA, Goddard Space Flight Ctr, Code 699,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. [Gautier, Thomas; Szopa, Cyril; Carrasco, Nathalie] Univ Paris 06, UVSQ Univ Paris Saclay, LATMOS IPSL, F-78280 Guyancourt, France. [Schmitz-Afonso, Isabelle; Touboul, David] Univ Paris 11, ICSN, CNRS UPR 2301, 1 Ave Terrasse, F-91198 Gif Sur Yvette, France. [Schmitz-Afonso, Isabelle] Normandie Univ, COBRA, UMR 6014, 1 Rue Tesniere, F-76821 Mont St Aignan, France. [Schmitz-Afonso, Isabelle] Univ Rouen, INSA Rouen, CNRS, FR3038,IRCOF, 1 Rue Tesniere, F-76821 Mont St Aignan, France. [Szopa, Cyril; Carrasco, Nathalie] Inst Univ France, 103 Bvd St Michel, F-75005 Paris, France. [Buch, Arnaud] Ecole Cent Paris, LGPM, F-92295 Chatenay Malabry, France. RP Gautier, T (reprint author), NASA, Goddard Space Flight Ctr, Code 699,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM thomas.j.gautier@nasa.gov RI Carrasco, Nathalie/D-2365-2012; szopa, cyril/C-6865-2015 OI Carrasco, Nathalie/0000-0002-0596-6336; szopa, cyril/0000-0002-0090-4056 FU French Program National de Planetologie (PNP); European Research Council (ERC Starting Grant PRIMCHEM) [636829] FX The research presented in this paper was partially funded through the French Program National de Planetologie (PNP). NC acknowledges the European Research Council for their financial support (ERC Starting Grant PRIMCHEM, Grant agreement no. 636829). TG acknowledges the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities. NR 33 TC 0 Z9 0 U1 12 U2 25 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 SEP 1 PY 2016 VL 275 BP 259 EP 266 DI 10.1016/j.icarus.2016.03.007 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO8FB UT WOS:000378016900021 ER PT J AU Leon, JJD Fryauf, DM Cormia, RD Zhang, MXM Samuels, K Williams, RS Kobayashi, NP AF Leon, Juan J. Diaz Fryauf, David M. Cormia, Robert D. Zhang, Min-Xian Max Samuels, Kathryn Williams, R. Stanley Kobayashi, Nobuhiko P. TI Reflectometry-Ellipsometry Reveals Thickness, Growth Rate, and Phase Composition in Oxidation of Copper SO ACS APPLIED MATERIALS & INTERFACES LA English DT Article DE copper oxide; reflectometry; ellipsometry; memristor; volatile conductive bridge ID THIN-FILMS; NATIVE OXIDATION; SINGLE-CRYSTAL; OXIDE; SURFACES; KINETICS; BULK; XPS AB The oxidation of copper is a complicated process. Copper oxide develops two stable phases at room temperature and standard pressure (RTSP): cuprous oxide (Cu2O) and cupric oxide (CuO). Both phases:have different optical and electrical characteristics that make them interesting for applications such as solar cells or resistive switching devices. For a given application, it is necessary to selectively control oxide thickness and cupric/cuprous oxide phase volume fraction. The thickness and composition of a copper oxide film growing on the surface of copper widely depend on the characteristics of as-deposited copper. In this Research Article, two samples, copper films prepared by two different deposition techniques, electron-beam evaporation and, sputtering, were studied. As the core part of the study, the formation of the oxidized copper was analyzed routinely over a period of 253 days using spectroscopic polarized reflectometry-spectroscopic ellipsometry (RE). An effective medium approximation (EMA) model was used to fit the RE data. The RE measurements were complemented and validated by using X-ray photoelectron spectroscopy (XPS), atomic force microscopy (AFM) and X-ray diffraction (XRD). Our results show that the two samples oxidized under identical laboratory ambient conditions (RTSP, 87% average relative humidity) developed unique oxide films following an inverse-logarithmic growth rate with thickness and composition different from each other over time. Discussion is focused on the ability of RE to simultaneously extract thickness (i.e., growth rate) and composition of copper oxide films and on plausible physical mechanisms responsible for unique oxidation habits observed in the two copper samples. It appears that extended surface characteristics (i.e., surface roughness and grain boundaries) and preferential crystalline orientation of as deposited polycrystalline copper films control the growth kinetics of the copper oxide film. Analysis based on a noncontact and nondestructive measurement, such as RE, to extract key material parameters is beneficial for conveniently understanding the oxidation process that would ultimately enable copper oxide-based devices at manufacturing scales. C1 [Leon, Juan J. Diaz; Fryauf, David M.; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. [Leon, Juan J. Diaz; Fryauf, David M.; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Nanostruct Energy Convers Technol & Res NECTAR, Adv Studies Labs, NASA Ames Res Ctr, Moffett Field, CA 94035 USA. [Cormia, Robert D.] Foothill Coll, Los Altos, CA 94022 USA. [Zhang, Min-Xian Max; Samuels, Kathryn; Williams, R. Stanley] Hewlett Packard Labs, Palo Alto, CA 94304 USA. RP Leon, JJD (reprint author), Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA.; Leon, JJD (reprint author), Univ Calif Santa Cruz, Nanostruct Energy Convers Technol & Res NECTAR, Adv Studies Labs, NASA Ames Res Ctr, Moffett Field, CA 94035 USA. EM jdiazleo@ucsc.edu RI Williams, R. Stanley/A-8281-2009 OI Williams, R. Stanley/0000-0003-0213-4259 FU NSF [DMR-1126845] FX We would like to acknowledge the Scott Oliver lab at the University of California Santa Cruz for the work of Jesse Hauser in X-ray diffractometry using a Rigaku SmartLab X-ray diffractometer, funded by the NSF Major Research Instrument (MRI) Program under Grant DMR-1126845. We would also like to thank Vince Crist (XPS international) for helpful assistance in interpreting the XPS data. NR 36 TC 0 Z9 0 U1 30 U2 30 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1944-8244 J9 ACS APPL MATER INTER JI ACS Appl. Mater. Interfaces PD AUG 31 PY 2016 VL 8 IS 34 BP 22337 EP 22344 DI 10.1021/acsami.6b06626 PG 8 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Science & Technology - Other Topics; Materials Science GA DU9CP UT WOS:000382514100060 ER PT J AU Nedoluha, GE Connor, BJ Mooney, T Barrett, JW Parrish, A Gomez, RM Boyd, I Allen, DR Kotkamp, M Kremser, S Deshler, T Newman, P Santee, ML AF Nedoluha, Gerald E. Connor, Brian J. Mooney, Thomas Barrett, James W. Parrish, Alan Gomez, R. Michael Boyd, Ian Allen, Douglas R. Kotkamp, Michael Kremser, Stefanie Deshler, Terry Newman, Paul Santee, Michelle L. TI 20 years of ClO measurements in the Antarctic lower stratosphere SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID CHLORINE MONOXIDE; SPRING STRATOSPHERE; LOW ALTITUDES; OZONE; REANALYSIS; SATELLITE; CHEMISTRY; CIO AB We present 20 years (1996-2015) of austral springtime measurements of chlorine monoxide (ClO) over Antarctica from the Chlorine Oxide Experiment (ChlOE1) ground-based millimeter wave spectrometer at Scott Base, Antarctica, as well 12 years (2004-2015) of ClO measurements from the Aura Microwave Limb Sounder (MLS). From August onwards we observe a strong increase in lower stratospheric ClO, with a peak column amount usually occurring in early September. From mid-September onwards we observe a strong decrease in ClO. In order to study interannual differences, we focus on a 3-week period from 28 August to 17 September for each year and compare the average column ClO anomalies. These column ClO anomalies are shown to be highly correlated with the average ozone mass deficit for September and October of each year. We also show that anomalies in column ClO are strongly anti-correlated with 30 hPa temperature anomalies, both on a daily and an interannual timescale. Making use of this anti-correlation we calculate the linear dependence of the interannual variations in column ClO on interannual variations in temperature. By making use of this relationship, we can better estimate the underlying trend in the total chlorine (Cl-y = HCl + ClONO2 + HOCl + 2 x Cl-2 + 2 x Cl2O2 + ClO + Cl). The resultant trends in Cl-y, which determine the long-term trend in ClO, are estimated to be -0.5 +/- 0.2, -1.4 +/- 0.9, and -0.6 +/- 0.4% year(-1), for zonal MLS, Scott Base MLS (both 2004-2015), and ChlOE (1996-2015) respectively. These trends are within 1 sigma of trends in stratospheric Cl-y previously found at other latitudes. The decrease in ClO is consistent with the trend expected from regulations enacted under the Montreal Protocol. C1 [Nedoluha, Gerald E.; Gomez, R. Michael; Allen, Douglas R.] Naval Res Lab, Washington, DC 20375 USA. [Connor, Brian J.; Mooney, Thomas; Boyd, Ian] BC Sci Consulting LLC, Stony Brook, NY USA. [Barrett, James W.] SUNY Stony Brook, Stony Brook, NY 11794 USA. [Parrish, Alan] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Kotkamp, Michael] Natl Inst Water & Atmospher Res, Lauder, New Zealand. [Kremser, Stefanie] Bodeker Sci, Alexandra, New Zealand. [Deshler, Terry] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA. [Newman, Paul] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Santee, Michelle L.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Nedoluha, GE (reprint author), Naval Res Lab, Washington, DC 20375 USA. EM nedoluha@nrl.navy.mil OI /0000-0002-3573-7083 FU NASA under the Upper Atmosphere Research Program; Naval Research Laboratory; Office of Naval Research; National Aeronautics and Space Administration FX This project was funded by NASA under the Upper Atmosphere Research Program, by the Naval Research Laboratory, and by the Office of Naval Research. We would like to acknowledge the many Antarctica New Zealand technicians who have supported the daily operation of ChlOE over two decades of measurements. We also acknowledge the logistical support that Antarctica New Zealand has supplied over this period. Work at the Jet Propulsion Laboratory, California Institute of Technology, was carried out under a contract with the National Aeronautics and Space Administration. Sonde temperature data were collected under support from the National Science Foundation. NR 30 TC 1 Z9 1 U1 5 U2 5 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD AUG 30 PY 2016 VL 16 IS 16 BP 10725 EP 10734 DI 10.5194/acp-16-10725-2016 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DW6EZ UT WOS:000383743600002 ER PT J AU Dolant, C Langlois, A Montpetit, B Brucker, L Roy, A Royer, A AF Dolant, Caroline Langlois, Alexandre Montpetit, Benoit Brucker, Ludovic Roy, Alexandre Royer, Alain TI Development of a rain-on-snow detection algorithm using passive microwave radiometry SO HYDROLOGICAL PROCESSES LA English DT Article DE snow; passive microwave; rain-on-snow; extreme winter events ID THERMAL-CONDUCTIVITY; ACTIVE LAYER; IMPACTS; TEMPERATURE; SVALBARD; CLIMATE; EVENTS; MODEL; ICE AB Currently observed climate warming in the Arctic has numerous consequences. Of particular relevance, the precipitation regime is modified where mixed and liquid precipitation can occur during the winter season leading to rain-on-snow (ROS) events. This phenomenon is responsible for ice crust formation, which has a significant impact on ecosystems (such as biological, hydrological, ecological and physical processes). The spatially and temporally sporadic nature of ROS events makes the phenomenon difficult to monitor using meteorological observations. This paper focuses on the detection of ROS events using passive microwave (PMW) data from a modified brightness temperature (T-B) gradient approach at 19 and 37GHz. The approach presented here was developed empirically for observed ROS events with coincident ground-based PMW measurements in Sherbrooke, Quebec, Canada. It was then tested in Nunavik, Quebec, with the Advanced Microwave Scanning Radiometer for the Earth Observing System (AMSR-E). We obtained a detection accuracy of 57, 71 and 89% for ROS detection for three AMSR-E grid cells with a maximum error of 7% when considering all omissions and commissions with regard to the total number of AMSR-E passes throughout the winter period. Copyright (c) 2016 John Wiley & Sons, Ltd. C1 [Dolant, Caroline; Langlois, Alexandre; Montpetit, Benoit; Roy, Alexandre; Royer, Alain] Univ Sherbrooke, Ctr Applicat & Rech Teledetect CARTEL, Sherbrooke, PQ J1K 2R1, Canada. [Dolant, Caroline; Langlois, Alexandre; Montpetit, Benoit; Royer, Alain] Ctr Etud Nord, Kuujjuarapik, PQ, Canada. [Montpetit, Benoit] Environm Canada, Canadian Ice Serv, Ottawa, ON, Canada. [Brucker, Ludovic] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Code 615, Greenbelt, MD 20771 USA. [Brucker, Ludovic] Univ Space Res Assoc, Goddard Earth Sci Technol & Res Studies & Invest, Columbia, MD 21044 USA. RP Dolant, C (reprint author), Univ Sherbrooke, Ctr Applicat & Rech Teledetect CARTEL, Sherbrooke, PQ J1K 2R1, Canada. EM caroline.dolant@USherbrooke.ca RI Brucker, Ludovic/A-8029-2010 OI Brucker, Ludovic/0000-0001-7102-8084 FU Natural Sciences and Engineering Research Council of Canada (NSERC); Centre for Northern Studies; EnviroNorth; Canadian Foundation for Innovation (CFI) FX Funding for this research was provided by the Natural Sciences and Engineering Research Council of Canada (NSERC), the Centre for Northern Studies, EnviroNorth and the Canadian Foundation for Innovation (CFI). Thanks to the National Snow and Ice Data Center (NSIDC) for satellite data access. The authors would also like to thank the Universite de Sherbrooke and the Centre d'Applications et de Recherches en TELedetection (CARTEL) for logistical and administrative support. NR 46 TC 3 Z9 3 U1 10 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0885-6087 EI 1099-1085 J9 HYDROL PROCESS JI Hydrol. Process. PD AUG 30 PY 2016 VL 30 IS 18 BP 3184 EP 3196 DI 10.1002/hyp.10828 PG 13 WC Water Resources SC Water Resources GA DW2IU UT WOS:000383466900006 ER PT J AU Bonnett, C Troxel, MA Hartley, W Amara, A Leistedt, B Becker, MR Bernstein, GM Bridle, SL Bruderer, C Busha, MT Kind, MC Childress, MJ Castander, FJ Chang, C Crocce, M Davis, TM Eifler, TF Frieman, J Gangkofner, C Gaztanaga, E Glazebrook, K Gruen, D Kacprzak, T King, A Kwan, J Lahav, O Lewis, G Lidman, C Lin, H MacCrann, N Miquel, R O'Neill, CR Palmese, A Peiris, HV Refregier, A Rozo, E Rykoff, ES Sadeh, I Sanchez, C Sheldon, E Uddin, S Wechsler, RH Zuntz, J Abbott, T Abdalla, FB Allam, S Armstrong, R Banerji, M Bauer, AH Benoit-Levy, A Bertin, E Brooks, D Buckley-Geer, E Burke, DL Capozzi, D Rosell, AC Carretero, J Cunha, CE D'Andrea, CB da Costa, LN DePoy, DL Desai, S Diehl, HT Dietrich, JP Doel, P Neto, AF Fernandez, E Flaugher, B Fosalba, P Gerdes, DW Gruendl, RA Honscheid, K Jain, B James, DJ Jarvis, M Kim, AG Kuehn, K Kuropatkin, N Li, TS Lima, M Maia, MAG March, M Marshall, JL Martini, P Melchior, P Miller, CJ Neilsen, E Nichol, RC Nord, B Ogando, R Plazas, AA Reil, K Romer, AK Roodman, A Sako, M Sanchez, E Santiago, B Smith, RC Soares-Santos, M Sobreira, F Suchyta, E Swanson, MEC Tarle, G Thaler, J Thomas, D Vikram, V Walker, AR AF Bonnett, C. Troxel, M. A. Hartley, W. Amara, A. Leistedt, B. Becker, M. R. Bernstein, G. M. Bridle, S. L. Bruderer, C. Busha, M. T. Kind, M. Carrasco Childress, M. J. Castander, F. J. Chang, C. Crocce, M. Davis, T. M. Eifler, T. F. Frieman, J. Gangkofner, C. Gaztanaga, E. Glazebrook, K. Gruen, D. Kacprzak, T. King, A. Kwan, J. Lahav, O. Lewis, G. Lidman, C. Lin, H. MacCrann, N. Miquel, R. O'Neill, C. R. Palmese, A. Peiris, H. V. Refregier, A. Rozo, E. Rykoff, E. S. Sadeh, I. Sanchez, C. Sheldon, E. Uddin, S. Wechsler, R. H. Zuntz, J. Abbott, T. Abdalla, F. B. Allam, S. Armstrong, R. Banerji, M. Bauer, A. H. Benoit-Levy, A. Bertin, E. Brooks, D. Buckley-Geer, E. Burke, D. L. Capozzi, D. Carnero Rosell, A. Carretero, J. Cunha, C. E. D'Andrea, C. B. da Costa, L. N. DePoy, D. L. Desai, S. Diehl, H. T. Dietrich, J. P. Doel, P. Fausti Neto, A. Fernandez, E. Flaugher, B. Fosalba, P. Gerdes, D. W. Gruendl, R. A. Honscheid, K. Jain, B. James, D. J. Jarvis, M. Kim, A. G. Kuehn, K. Kuropatkin, N. Li, T. S. Lima, M. Maia, M. A. G. March, M. Marshall, J. L. Martini, P. Melchior, P. Miller, C. J. Neilsen, E. Nichol, R. C. Nord, B. Ogando, R. Plazas, A. A. Reil, K. Romer, A. K. Roodman, A. Sako, M. Sanchez, E. Santiago, B. Smith, R. C. Soares-Santos, M. Sobreira, F. Suchyta, E. Swanson, M. E. C. Tarle, G. Thaler, J. Thomas, D. Vikram, V. Walker, A. R. CA Dark Energy Survey Collaboration TI Redshift distributions of galaxies in the Dark Energy Survey Science Verification shear catalogue and implications for weak lensing SO PHYSICAL REVIEW D LA English DT Article ID STAR-FORMING GALAXIES; LARGE-SCALE STRUCTURE; PHOTO-Z PERFORMANCE; VLT DEEP SURVEY; PHOTOMETRIC REDSHIFTS; DATA RELEASE; PRECISION COSMOLOGY; SURVEY REQUIREMENTS; SHAPE MEASUREMENT; NEURAL-NETWORKS AB We present photometric redshift estimates for galaxies used in the weak lensing analysis of the Dark Energy Survey Science Verification (DES SV) data. Four model-or machine learning-based photometric redshift methods-ANNZ2, BPZ calibrated against BCC-Ufig simulations, SKYNET, and TPZ-are analyzed. For training, calibration, and testing of these methods, we construct a catalogue of spectroscopically confirmed galaxies matched against DES SV data. The performance of the methods is evaluated against the matched spectroscopic catalogue, focusing on metrics relevant for weak lensing analyses, with additional validation against COSMOS photo-z's. From the galaxies in the DES SV shear catalogue, which have mean redshift 0.72 +/- 0.01 over the range 0.3 < z < 1.3, we construct three tomographic bins with means of z = {0.45; 0.67; 1.00}. These bins each have systematic uncertainties delta z <= 0.05 in the mean of the fiducial SKYNET photo-z (dz). We propagate the errors in the redshift distributions through to their impact on cosmological parameters estimated with cosmic shear, and find that they cause shifts in the value of sigma(8) of approximately 3%. This shift is within the one sigma statistical errors on sigma(8) for the DES SV shear catalogue. We further study the potential impact of systematic differences on the critical surface density, Sigma(crit), finding levels of bias safely less than the statistical power of DES SV data. We recommend a final Gaussian prior for the photo-z bias in the mean of n(z) of width 0.05 for each of the three tomographic bins, and show that this is a sufficient bias model for the corresponding cosmology analysis. C1 [Bonnett, C.; Miquel, R.; Sanchez, C.; Carretero, J.; Fernandez, E.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain. [Troxel, M. A.; Bridle, S. L.; MacCrann, N.; Zuntz, J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England. [Hartley, W.; Amara, A.; Bruderer, C.; Chang, C.; Kacprzak, T.; Refregier, A.] ETH, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland. [Leistedt, B.; Lahav, O.; Palmese, A.; Peiris, H. V.; Sadeh, I.; Abdalla, F. B.; Benoit-Levy, A.; Brooks, D.; Doel, P.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Becker, M. R.; Busha, M. T.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. [Becker, M. R.; Rykoff, E. S.; Wechsler, R. H.; Burke, D. L.; Cunha, C. E.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA. [Bernstein, G. M.; Eifler, T. F.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [King, A.] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia. [Kind, M. Carrasco; Gruendl, R. A.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Kind, M. Carrasco; Gruendl, R. A.; Swanson, M. E. C.] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA. [Castander, F. J.; Crocce, M.; Gaztanaga, E.; Bauer, A. H.; Carretero, J.; Fosalba, P.] IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, Barcelona 08193, Spain. [Eifler, T. F.; Abdalla, F. B.; Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Frieman, J.; Lin, H.; Allam, S.; Buckley-Geer, E.; Diehl, H. T.; Flaugher, B.; Kuropatkin, N.; Neilsen, E.; Nord, B.; Soares-Santos, M.; Sobreira, F.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. [Frieman, J.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Kwan, J.; Vikram, V.] Argonne Natl Lab, 9700 South Cass Ave, Lemont, IL 60439 USA. [Lidman, C.; Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Rozo, E.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. [Rykoff, E. S.; Wechsler, R. H.; Burke, D. L.; Reil, K.; Roodman, A.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Glazebrook, K.; Uddin, S.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Abbott, T.; James, D. J.; Smith, R. C.; Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile. [Armstrong, R.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. [Banerji, M.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Banerji, M.] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England. [Bertin, E.] Inst Astrophys, CNRS, UMR 7095, F-75014 Paris, France. [Bertin, E.] Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Capozzi, D.; D'Andrea, C. B.; Nichol, R. C.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Carnero Rosell, A.; da Costa, L. N.; Fausti Neto, A.; Lima, M.; Maia, M. A. G.; Ogando, R.; Santiago, B.; Sobreira, F.] Lab Interinst Eastron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carnero Rosell, A.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [DePoy, D. L.; Li, T. S.; Marshall, J. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [DePoy, D. L.; Li, T. S.; Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Desai, S.] Univ Munich, Dept Phys, Scheinerstr 1, D-81679 Munich, Germany. [Gangkofner, C.; Sheldon, E.; Desai, S.; Dietrich, J. P.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Gruen, D.; Dietrich, J. P.] Univ Munich, Univ Sternwarte, Fak Phys, Scheinerstr 1, D-81679 Munich, Germany. [Gerdes, D. W.; Miller, C. J.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Gruen, D.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. [Honscheid, K.; Martini, P.; Melchior, P.; Suchyta, E.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Honscheid, K.; Melchior, P.; Suchyta, E.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA. [Kim, A. G.] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Martini, P.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. [Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England. [Sanchez, E.] CIEMAT, Madrid, Spain. [Santiago, B.] Univ Fed Rio Grande do Sul, Inst Fis, Caixa Postal 15051, BR-91501970 Porto Alegre, RS, Brazil. [Thaler, J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. [Lima, M.] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil. [Lewis, G.] South East Phys Network, SEPnet, Southampton, Hants, England. [Davis, T. M.; O'Neill, C. R.] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia. [Childress, M. J.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Sheldon, E.] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA. [Gangkofner, C.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. RP Bonnett, C (reprint author), Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain. RI Lima, Marcos/E-8378-2010; Ogando, Ricardo/A-1747-2010; Davis, Tamara/A-4280-2008; Gaztanaga, Enrique/L-4894-2014; OI Ogando, Ricardo/0000-0003-2120-1154; Davis, Tamara/0000-0002-4213-8783; Gaztanaga, Enrique/0000-0001-9632-0815; Abdalla, Filipe/0000-0003-2063-4345; Sobreira, Flavia/0000-0002-7822-0658 FU European Research Council [240672]; DFG Cluster of Excellence Origin and Structure of the Universe; U.S. Department of Energy; U.S. National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia e Tecnologia; Deutsche Forschungsgemeinschaft; National Science Foundation [AST-1138766]; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; ERDF funds from the European Union; Argonne National Laboratory; University of California at Santa Cruz; University of Cambridge; Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid; University of Chicago; University College London; DES-Brazil Consortium; Eidgenossische Technische Hochschule (ETH) Zurich; Fermi National Accelerator Laboratory; University of Edinburgh; University of Illinois at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory; Ludwig-Maximilians Universitat and the associated Excellence Cluster Universe; University of Michigan; National Optical Astronomy Observatory; University of Nottingham; Ohio State University; University of Pennsylvania; University of Portsmouth; SLAC National Accelerator Laboratory, Stanford University; University of Sussex; Texas AM University; Australian Astronomical Observatory [A/2013B/012]; Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; Swiss National Science Foundation [200021_14944, 200021_143906]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Pennsylvania State University; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University; ESO Telescopes at the La Silla Paranal Observatory [179.A-2004, 177.A-3016] FX We are grateful for the extraordinary contributions of our CTIO colleagues and the DECam Construction, Commissioning and Science Verification teams in achieving the excellent instrument and telescope conditions that have made this work possible. The success of this project also relies critically on the expertise and dedication of the DES Data Management group. M. T., S. B., N. M., and J. Z. acknowledge support from the European Research Council in the form of a Starting Grant with number 240672. D. G. acknowledges the support by the DFG Cluster of Excellence Origin and Structure of the Universe. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia e Tecnologia, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. C. G. acknowledges the support by the DFG Cluster of Excellence Origin and Structure of the Universe. The DES data management system is supported by the National Science Foundation under Grant Number AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234, some of which include ERDF funds from the European Union. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Edinburgh, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University. Based in part on observations taken at the Australian Astronomical Observatory under program A/2013B/012. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. This work was supported in part by grants 200021_14944 and 200021_143906 from the Swiss National Science Foundation. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science.; r The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 179.A-2004. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 177.A-3016. This paper is Fermilab publication FERMILAB-PUB-15-306 and DES publication DES2015-0060. This paper has gone through internal review by the DES Collaboration. NR 95 TC 10 Z9 10 U1 5 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD AUG 30 PY 2016 VL 94 IS 4 AR 042005 DI 10.1103/PhysRevD.94.042005 PG 26 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA DU4IW UT WOS:000382177300001 ER PT J AU Frankenberg, C Thorpe, AK Thompson, DR Hulley, G Kort, EA Vance, N Borchardt, J Krings, T Gerilowski, K Sweeney, C Conley, S Bue, BD Aubrey, AD Hook, S Green, RO AF Frankenberg, Christian Thorpe, Andrew K. Thompson, David R. Hulley, Glynn Kort, Eric Adam Vance, Nick Borchardt, Jakob Krings, Thomas Gerilowski, Konstantin Sweeney, Colm Conley, Stephen Bue, Brian D. Aubrey, Andrew D. Hook, Simon Green, Robert O. TI Airborne methane remote measurements reveal heavy-tail flux distribution in Four Corners region SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE methane; Four Corners; remote sensing; heavy-tail ID IMAGING SPECTROMETER AVIRIS; MATCHED-FILTER DETECTION; GAS PRODUCTION SITES; EMISSION RATES; UNITED-STATES; TRACE GASES; RETRIEVAL; QUANTIFICATION; SPECTROSCOPY; CO2 AB Methane (CH4) impacts climate as the second strongest anthropogenic greenhouse gas and air quality by influencing tropospheric ozone levels. Space-based observations have identified the Four Corners region in the Southwest United States as an area of large CH4 enhancements. We conducted an airborne campaign in Four Corners during April 2015 with the next-generation Airborne Visible/Infrared Imaging Spectrometer (near-infrared) and Hyperspectral Thermal Emission Spectrometer (thermal infrared) imaging spectrometers to better understand the source of methane by measuring methane plumes at 1-to 3-m spatial resolution. Our analysis detected more than 250 individual methane plumes from fossil fuel harvesting, processing, and distributing infrastructures, spanning an emission range from the detection limit similar to 2 kg/h to 5 kg/h through similar to 5,000 kg/h. Observed sources include gas processing facilities, storage tanks, pipeline leaks, and well pads, as well as a coal mine venting shaft. Overall, plume enhancements and inferred fluxes follow a lognormal distribution, with the top 10% emitters contributing 49 to 66% to the inferred total point source flux of 0.23 Tg/y to 0.39 Tg/y. With the observed confirmation of a lognormal emission distribution, this airborne observing strategy and its ability to locate previously unknown point sources in real time provides an efficient and effective method to identify and mitigate major emissions contributors over a wide geographic area. With improved instrumentation, this capability scales to spaceborne applications [Thompson DR, et al. (2016) Geophys Res Lett 43(12): 6571-6578]. Further illustration of this potential is demonstrated with two detected, confirmed, and repaired pipeline leaks during the campaign. C1 [Frankenberg, Christian] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Frankenberg, Christian; Thorpe, Andrew K.; Thompson, David R.; Hulley, Glynn; Vance, Nick; Bue, Brian D.; Aubrey, Andrew D.; Hook, Simon; Green, Robert O.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Kort, Eric Adam] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA. [Borchardt, Jakob; Krings, Thomas; Gerilowski, Konstantin] Univ Bremen, Inst Environm Phys, D-28334 Bremen, Germany. [Sweeney, Colm] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Sweeney, Colm] NOAA, Global Monitoring Div, Earth Syst Res Lab, Boulder, CO 80305 USA. [Conley, Stephen] Sci Aviat, Boulder, CO 80301 USA. [Conley, Stephen] Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA. RP Frankenberg, C (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.; Frankenberg, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM cfranken@caltech.edu RI Kort, Eric/F-9942-2012; Frankenberg, Christian/A-2944-2013 OI Kort, Eric/0000-0003-4940-7541; Frankenberg, Christian/0000-0002-0546-5857 FU NASA Headquarters; state of Bremen; University of Bremen; National Oceanic and Atmospheric Administration AC4 program [NA14OAR0110139] FX We thank the AVIRIS-NG flight and instrument teams, including Michael Eastwood, Sarah Lundeen, Scott Nolte, Mark Helmlinger, and Betina Pavri. Didier Keymeulen and Joseph Boardman assisted with the real-time system. We also thank the HyTES flight and instrument teams, including Bjorn Eng, Jonathan Mihaly, Seth Chazanoff, and Bill Johnson. We thank the organizers and all the participants in the TOPDOWN campaign for the fruitful collaboration. We thank NASA Headquarters, in particular Jack Kaye, for funding this flight campaign, which augmented the overall Twin Otter Projects Defining Oil/Gas Well Emissions (TOPDOWN) campaign. J.B., T.K., and K.G. were funded by the state of Bremen and University of Bremen. E.A.K. and C.S. were supported, in part, by the National Oceanic and Atmospheric Administration AC4 program under Grant NA14OAR0110139. NR 23 TC 3 Z9 3 U1 9 U2 9 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD AUG 30 PY 2016 VL 113 IS 35 BP 9734 EP 9739 DI 10.1073/pnas.1605617113 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DV7BL UT WOS:000383090700039 PM 27528660 ER PT J AU Zhang, RY Peng, JF Wang, Y Hu, M AF Zhang, Renyi Peng, Jianfei Wang, Yuan Hu, Min TI Rate and timescale of black carbon aging regulate direct radiative forcing SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter ID AEROSOLS; IMPACTS; CHINA C1 [Zhang, Renyi; Peng, Jianfei] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. [Zhang, Renyi; Peng, Jianfei] Texas A&M Univ, Dept Chem, College Stn, TX 77843 USA. [Zhang, Renyi; Peng, Jianfei; Hu, Min] Peking Univ, Coll Environm Sci & Engn, State Key Joint Lab Environm Simulat & Pollut Con, Beijing 100871, Peoples R China. [Wang, Yuan] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. RP Zhang, RY (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.; Zhang, RY (reprint author), Texas A&M Univ, Dept Chem, College Stn, TX 77843 USA.; Zhang, RY; Hu, M (reprint author), Peking Univ, Coll Environm Sci & Engn, State Key Joint Lab Environm Simulat & Pollut Con, Beijing 100871, Peoples R China. EM renyi-zhang@tamu.edu; minhu@pku.edu.cn RI Peng, Jianfei/F-1438-2015 NR 10 TC 0 Z9 0 U1 32 U2 32 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 AUG 30 PY 2016 VL 113 IS 35 BP E5094 EP E5095 DI 10.1073/pnas.1610241113 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DV7BL UT WOS:000383090700002 PM 27555593 ER PT J AU Feyhl-Buska, J Chen, YF Jia, CL Wang, JX Zhang, CLL Boyd, ES AF Feyhl-Buska, Jayme Chen, Yufei Jia, Chengling Wang, Jin-Xiang Zhang, Chuanlun L. Boyd, Eric S. TI Influence of Growth Phase, pH, and Temperature on the Abundance and Composition of Tetraether Lipids in the Thermoacidophile Picrophilus torridus SO FRONTIERS IN MICROBIOLOGY LA English DT Article DE tetraether; GDGT; GTGT; growth phase; temperature; pH; thermoacidophile; stress ID FATTY-ACID-COMPOSITION; TERRESTRIAL HOT-SPRINGS; LOWER PEARL RIVER; SOUTH CHINA SEA; MEMBRANE-LIPIDS; POLAR LIPIDS; NITROSOPUMILUS-MARITIMUS; ARCHAEBACTERIAL LIPIDS; THERMOPHILIC ARCHAEA; MASS-SPECTROMETRY AB The abundance and composition of glycerol dibiphytanyl glycerol tetraether (GDGT) and glycerol tribiphytanyl glycerol tetraether (GTGT) lipids were determined as a function of growth phase as a proxy for nutrient availability, the pH of growth medium, and incubation temperature in cultures of the thermoacidophile Picrophilus torridus. Regardless of the cultivation condition, the abundance of GDGTs and GTGTs was greater in the polar than core fraction, with a marked decrease in core GDGTs in cultures harvested during log phase growth. These data are consistent with previous suggestions indicating that core GDGTs are re-functionalized during polar lipid synthesis. Under all conditions examined, polar lipids were enriched in a GDGT with 2 cyclopentyl rings (GDGT-2), indicating GDGT-2 is the preferred lipid in this taxon. However, lag or stationary phase grown cells or cells subjected to pH or thermal stress were enriched in GDGTs with 4, 5, or 6 rings and depleted in GDGTs with 1, 2, 3, rings relative to log phase cells grown under optimal conditions. Variation in the composition of polar GDGT lipids in cells harvested during various growth phases tended to be greater than in cells cultivated over a pH range of 0.31.1 and a temperature range of 5363 degrees C. These results suggest that the growth phase, the pH of growth medium, and incubation temperature are all important factors that shape the composition of tetraether lipids in Picrophilus. The similarity in enrichment of GDGTs with more rings in cultures undergoing nutrient, pH, and thermal stress points to GDGT cyclization as a generalized physiological response to stress in this taxon. C1 [Feyhl-Buska, Jayme; Boyd, Eric S.] Montana State Univ, Dept Microbiol & Immunol, Bozeman, MT 59717 USA. [Chen, Yufei; Jia, Chengling; Wang, Jin-Xiang; Zhang, Chuanlun L.] Tongji Univ, State Key Lab Marine Geol, Shanghai, Peoples R China. [Boyd, Eric S.] NASA, Astrobiol Inst, Mountain View, CA 94043 USA. [Feyhl-Buska, Jayme] Univ Southern Calif, Dept Earth Sci, Los Angeles, CA USA. [Wang, Jin-Xiang] Univ Bremen, MARUM Ctr Marine Environm Sci, Bremen, Germany. RP Boyd, ES (reprint author), Montana State Univ, Dept Microbiol & Immunol, Bozeman, MT 59717 USA.; Boyd, ES (reprint author), NASA, Astrobiol Inst, Mountain View, CA 94043 USA. EM eboyd@montana.edu FU National Science Foundation [PIRE-0968421]; National Natural Science Foundation of China [40972211, 41373072]; National Science Foundation Research Experience for Undergraduates grant [DBI REU 1005223]; NASA Astrobiology Institute [NNA15BB02A]; NASA Exobiology and Evolutionary Biology Program [NNX13AI11G] FX This work was supported by grants from the National Science Foundation (PIRE-0968421) to CZ and EB and from the National Natural Science Foundation of China (40972211 and 41373072) to CZ. A National Science Foundation Research Experience for Undergraduates grant (DBI REU 1005223) supported JF during the completion of this work. EB acknowledges support from the NASA Astrobiology Institute (NNA15BB02A) and the NASA Exobiology and Evolutionary Biology Program (NNX13AI11G). Two reviewers are acknowledged for comments which significantly improved this manuscript. NR 60 TC 0 Z9 0 U1 8 U2 8 PU FRONTIERS MEDIA SA PI LAUSANNE PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015, SWITZERLAND SN 1664-302X J9 FRONT MICROBIOL JI Front. Microbiol. PD AUG 30 PY 2016 VL 7 AR 1323 DI 10.3389/fmicb.2016.01323 PG 12 WC Microbiology SC Microbiology GA DU3KC UT WOS:000382108200001 PM 27625636 ER PT J AU Mandra, S Zhu, Z Wang, WL Perdomo-Ortiz, A Katzgraber, HG AF Mandra, Salvatore Zhu, Zheng Wang, Wenlong Perdomo-Ortiz, Alejandro Katzgraber, Helmut G. TI Strengths and weaknesses of weak-strong cluster problems: A detailed overview of state-of-the-art classical heuristics versus quantum approaches SO PHYSICAL REVIEW A LA English DT Article ID MONTE-CARLO; SPIN-GLASS; OPTIMIZATION; COMPUTATION; ANNEALERS; QUBITS AB To date, a conclusive detection of quantum speedup remains elusive. Recently, a team by Google Inc. [V. S. Denchev et al., Phys. Rev. X 6, 031015 (2016)] proposed a weak-strong cluster model tailored to have tall and narrow energy barriers separating local minima, with the aim to highlight the value of finite-range tunneling. More precisely, results from quantum Monte Carlo simulations as well as the D-Wave 2X quantum annealer scale considerably better than state-of-the-art simulated annealing simulations. Moreover, the D-Wave 2X quantum annealer is similar to 10(8) times faster than simulated annealing on conventional computer hardware for problems with approximately 10(3) variables. Here, an overview of different sequential, nontailored, as well as specialized tailored algorithms on the Google instances is given. We show that the quantum speedup is limited to sequential approaches and study the typical complexity of the benchmark problems using insights from the study of spin glasses. C1 [Mandra, Salvatore] Harvard Univ, Dept Chem & Chem Biol, 12 Oxford St, Cambridge, MA 02138 USA. [Zhu, Zheng; Wang, Wenlong; Katzgraber, Helmut G.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Perdomo-Ortiz, Alejandro] NASA, Ames Res Ctr, Quantum Artificial Intelligence Lab, Moffett Field, CA 94035 USA. [Perdomo-Ortiz, Alejandro] Univ Calif Santa Cruz, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Katzgraber, Helmut G.] Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA. [Katzgraber, Helmut G.] Coventry Univ, Appl Math Res Ctr, Coventry CV1 5FB, W Midlands, England. RP Mandra, S (reprint author), Harvard Univ, Dept Chem & Chem Biol, 12 Oxford St, Cambridge, MA 02138 USA. EM smandra@fas.harvard.edu; zzwtgts@tamu.edu; wenlong@physics.umass.edu; alejandro.perdomoortiz@nasa.gov; hgk@tamu.edu FU NSF [DMR-1151387]; NASA [NNX14AF62G]; Office of the Director of National Intelligence (ODNI), Intelligence Advanced Research Projects Activity (IARPA), via MIT Lincoln Laboratory Air Force [FA8721-05-C-0002] FX We thank the Google Quantum A. I. Lab members for sharing their QMC and SA data, multiple discussions, as well as making the weak-strong cluster instances available to us. We also thank A. Aspuru-Guzik, F. Hamze, A.J. Ochoa, and Eleanor G. Rieffel for many fruitful discussions, as well as H. Munoz-Bauza for help with the graphics. H.G.K. and W.W. acknowledge support from the NSF (Grant No. DMR-1151387). H.G.K. thanks D. Humm, M.P. White, T. Keller, H. Blumenthal, and P. Bocuse for inspiration during the initial stages of the manuscript. S.M. was supported by NASA (Sponsor Award No. NNX14AF62G). We thank the Texas Advanced Computing Center (TACC) at The University of Texas at Austin for providing HPC resources (Stampede Cluster) and Texas A&M University for access to their Ada and Lonestar clusters. This research is based upon work supported in part by the Office of the Director of National Intelligence (ODNI), Intelligence Advanced Research Projects Activity (IARPA), via MIT Lincoln Laboratory Air Force Contract No. FA8721-05-C-0002. NR 80 TC 2 Z9 2 U1 1 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD AUG 29 PY 2016 VL 94 IS 2 AR 022337 DI 10.1103/PhysRevA.94.022337 PG 13 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA DU2BR UT WOS:000382016400003 ER PT J AU Matsuyama, I Nimmo, F Keane, JT Chan, NH Taylor, GJ Wieczorek, MA Kiefer, WS Williams, JG AF Matsuyama, Isamu Nimmo, Francis Keane, James T. Chan, Ngai H. Taylor, G. Jeffrey Wieczorek, Mark A. Kiefer, Walter S. Williams, James G. TI GRAIL, LLR, and LOLA constraints on the interior structure of the Moon SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE lunar interior ID DEEP LUNAR INTERIOR; SEISMIC DATA; POLYCRYSTALLINE OLIVINE; FREQUENCY-DEPENDENCE; CHANDLER-WOBBLE; TIDAL RESPONSE; GRAVITY-FIELD; GIANT IMPACT; MARE BASALTS; MODEL AB The interior structure of the Moon is constrained by its mass, moment of inertia, and k(2) and h(2) tidal Love numbers. We infer the likely radius, density, and (elastic limit) rigidity of all interior layers by solving the inverse problem using these observational constraints assuming spherical symmetry. Our results do not favor the presence of a low rigidity transition layer between a liquid outer core and mantle. If a transition layer exists, its rigidity is constrained to 43-9+26GPa, with a preference for the high rigidity values. Therefore, if a transition layer exists, it is more likely to have a rigidity similar to that of the mantle (approximate to 70GPa). The total (solid and liquid) core mass fraction relative to the lunar mass is constrained to 0.0098-0.0094+0.0066 and 0.0198-0.0049+0.0026 for interior structures with and without a transition layer, respectively, narrowing the range of possible giant impact formation scenarios. C1 [Matsuyama, Isamu; Keane, James T.; Chan, Ngai H.] Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Nimmo, Francis] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Taylor, G. Jeffrey] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Wieczorek, Mark A.] Inst Phys Globe Paris, Paris, France. [Kiefer, Walter S.] Lunar & Planetary Inst, 3303 NASA Rd 1, Houston, TX 77058 USA. [Williams, James G.] Inst Technol, Jet Prop Lab, Pasadena, CA USA. RP Matsuyama, I (reprint author), Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA. EM isa@lpl.arizona.edu RI Wieczorek, Mark/G-6427-2010; OI Wieczorek, Mark/0000-0001-7007-4222; Matsuyama, Isamu/0000-0002-2917-8633; Kiefer, Walter/0000-0001-6741-5460 FU NASA's Discovery Program FX The GRAIL mission is supported by NASA's Discovery Program and is performed under contract to the Massachusetts Institute of Technology and the Jet Propulsion Laboratory, California Institute of Technology. A portion of the research described in this paper was carried out at the Jet Propulsion Laboratory of the California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Government sponsorship is acknowledged. The data used are listed in the references and tables. NR 51 TC 0 Z9 0 U1 4 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 28 PY 2016 VL 43 IS 16 BP 8365 EP 8375 DI 10.1002/2016GL069952 PG 11 WC Geosciences, Multidisciplinary SC Geology GA DX5TC UT WOS:000384443800005 ER PT J AU Way, MJ Del Genio, AD Kiang, NY Sohl, LE Grinspoon, DH Aleinov, I Kelley, M Clune, T AF Way, M. J. Del Genio, Anthony D. Kiang, Nancy Y. Sohl, Linda E. Grinspoon, David H. Aleinov, Igor Kelley, Maxwell Clune, Thomas TI Was Venus the first habitable world of our solar system? SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE ancient Venus; habitability ID EARTH; ATMOSPHERE; WATER; PLANETS; EVOLUTION; HYDROGEN; OCEAN; DEUTERIUM; ROTATION; HISTORY AB Present-day Venus is an inhospitable place with surface temperatures approaching 750K and an atmosphere 90 times as thick as Earth's. Billions of years ago the picture may have been very different. We have created a suite of 3-D climate simulations using topographic data from the Magellan mission, solar spectral irradiance estimates for 2.9 and 0.715 Gya, present-day Venus orbital parameters, an ocean volume consistent with current theory, and an atmospheric composition estimated for early Venus. Using these parameters we find that such a world could have had moderate temperatures if Venus had a prograde rotation period slower than similar to 16 Earth days, despite an incident solar flux 46-70% higher than Earth receives. At its current rotation period, Venus's climate could have remained habitable until at least 0.715 Gya. These results demonstrate the role rotation and topography play in understanding the climatic history of Venus-like exoplanets discovered in the present epoch. C1 [Way, M. J.; Del Genio, Anthony D.; Kiang, Nancy Y.; Sohl, Linda E.; Aleinov, Igor; Kelley, Maxwell] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Way, M. J.] Uppsala Univ, Dept Astron & Space Phys, Uppsala, Sweden. [Sohl, Linda E.; Aleinov, Igor] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Grinspoon, David H.] Planetary Sci Inst, Tucson, AZ USA. [Clune, Thomas] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Way, MJ (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.; Way, MJ (reprint author), Uppsala Univ, Dept Astron & Space Phys, Uppsala, Sweden. EM michael.j.way@nasa.gov OI Way, Michael/0000-0003-3728-0475 FU NASA Astrobiology Program through the Nexus for Exoplanet System Science (NExSS) research coordination network - NASA's Science Mission Directorate; NASA Goddard Space Flight Center ROCKE-3D Science Task Group funding FX This research was supported by the NASA Astrobiology Program through the Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA's Science Mission Directorate. This work was also supported by NASA Goddard Space Flight Center ROCKE-3D Science Task Group funding. 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. This research has made use of NASA's Astrophysics Data System Bibliographic Services. Thanks to Jeffrey A. Jonas, Kostas Tsigaridis, and David S. Amundsen for their assistance in this work and thanks to June Wang at Washington University in St. Louis for help with the Magellan PDS data. We also thank referee Norman Sleep for his constructive comments. The data products associated with this paper can be obtained by contacting the first author Michael J. Way. NR 53 TC 2 Z9 2 U1 14 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 28 PY 2016 VL 43 IS 16 BP 8376 EP 8383 DI 10.1002/2016GL069790 PG 8 WC Geosciences, Multidisciplinary SC Geology GA DX5TC UT WOS:000384443800006 ER PT J AU Scheuchl, B Mouginot, J Rignot, E Morlighem, M Khazendar, A AF Scheuchl, B. Mouginot, J. Rignot, E. Morlighem, M. Khazendar, A. TI Grounding line retreat of Pope, Smith, and Kohler Glaciers, West Antarctica, measured with Sentinel-1a radar interferometry data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Grounding Line; Synthetic Aperture Radar; Sentinel-1 ID AMUNDSEN SEA EMBAYMENT; ICE-SHEET; PINE ISLAND; SHELF; WIDESPREAD; STABILITY; GREENLAND; CRYOSAT-2; THWAITES; SURFACE AB We employ Sentinel-1a C band satellite radar interferometry data in Terrain Observation with Progressive Scans mode to map the grounding line and ice velocity of Pope, Smith, and Kohler glaciers, in West Antarctica, for the years 2014-2016 and compare the results with those obtained using Earth Remote Sensing Satellites (ERS-1/2) in 1992, 1996, and 2011. We observe an ongoing, rapid grounding line retreat of Smith at 2km/yr (40km since 1996), an 11km retreat of Pope (0.5km/yr), and a 2km readvance of Kohler since 2011. The variability in glacier retreat is consistent with the distribution of basal slopes, i.e., fast along retrograde beds and slow along prograde beds. We find that several pinning points holding Dotson and Crosson ice shelves disappeared since 1996 due to ice shelf thinning, which signal the ongoing weakening of these ice shelves. Overall, the results indicate that ice shelf and glacier retreat in this sector remain unabated. C1 [Scheuchl, B.; Mouginot, J.; Rignot, E.; Morlighem, M.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Rignot, E.; Khazendar, A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Scheuchl, B (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. EM bscheuch@uci.edu 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 and the USGS for providing the data. SAR data acquisition was coordinated by the Polar Space Task Group. The 2014 grounding line is available at NSIDC as part of the updated MEaSUREs InSAR based grounding line product. NR 39 TC 1 Z9 1 U1 12 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 AUG 28 PY 2016 VL 43 IS 16 BP 8572 EP 8579 DI 10.1002/2016GL069287 PG 8 WC Geosciences, Multidisciplinary SC Geology GA DX5TC UT WOS:000384443800029 ER PT J AU Peyser, CE Yin, JJ Landerer, FW Cole, JE AF Peyser, Cheryl E. Yin, Jianjun Landerer, Felix W. Cole, Julia E. TI Pacific sea level rise patterns and global surface temperature variability SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE sea level rise; Pacific; warming hiatus; global temperature ID WESTERN TROPICAL PACIFIC; OCEAN HEAT UPTAKE; WARMING HIATUS; INTENSIFICATION; CIRCULATION; ATLANTIC; TRENDS AB During 1998-2012, climate change and sea level rise (SLR) exhibit two notable features: a slowdown of global surface warming (hiatus) and a rapid SLR in the tropical western Pacific. To quantify their relationship, we analyze the long-term control simulations of 38 climate models. We find a significant and robust correlation between the east-west contrast of dynamic sea level (DSL) in the Pacific and global mean surface temperature (GST) variability on both interannual and decadal time scales. Based on linear regression of the multimodel ensemble mean, the anomalously fast SLR in the western tropical Pacific observed during 1998-2012 indicates suppression of a potential global surface warming of 0.16 degrees 0.06 degrees C. In contrast, the Pacific contributed 0.29 degrees 0.10 degrees C to the significant interannual GST increase in 1997/1998. The Pacific DSL anomalies observed in 2015 suggest that the strong El Nino in 2015/2016 could lead to a 0.21 degrees 0.07 degrees C GST jump. C1 [Peyser, Cheryl E.; Yin, Jianjun; Cole, Julia E.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. [Landerer, Felix W.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA USA. RP Yin, JJ (reprint author), Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. EM yin@email.arizona.edu FU Strategic University Research Partnership Program of the NASA Jet Propulsion Laboratory [1492484/NNN12AA01C] FX We thank many observation and modeling centers for making their data available. We thank the anonymous reviewers for detailed reviews and P. Goddard, S. Griffies, S. Malyshev, J. Pelletier, J. Russell, and R. Stouffer for discussion. The work was supported by the Strategic University Research Partnership Program of the NASA Jet Propulsion Laboratory (grant # 1492484/NNN12AA01C). The work of F.W.L. was performed at the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. The observational, reanalysis, and model data used in this study can be accessed from the URLs found in the section 2. For all other data inquiries, please contact Cheryl Peyser (peyser@email.arizona.edu). NR 31 TC 2 Z9 2 U1 8 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 28 PY 2016 VL 43 IS 16 BP 8662 EP 8669 DI 10.1002/2016GL069401 PG 8 WC Geosciences, Multidisciplinary SC Geology GA DX5TC UT WOS:000384443800039 ER PT J AU Lyu, F Cummer, SA Briggs, M Marisaldi, M Blakeslee, RJ Bruning, E Wilson, JG Rison, W Krehbiel, P Lu, GP Cramer, E Fitzpatrick, G Mailyan, B McBreen, S Roberts, OJ Stanbro, M AF Lyu, Fanchao Cummer, Steven A. Briggs, Michael Marisaldi, Martino Blakeslee, Richard J. Bruning, Eric Wilson, Jennifer G. Rison, William Krehbiel, Paul Lu, Gaopeng Cramer, Eric Fitzpatrick, Gerard Mailyan, Bagrat McBreen, Sheila Roberts, Oliver J. Stanbro, Matthew TI Ground detection of terrestrial gamma ray flashes from distant radio signals SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE terrestrial gamma ray flashes; energetic in-cloud pulses; lightning; ground detection ID ALTITUDE AB Terrestrial gamma ray flashes (TGFs) are brief bursts of energetic gammy-ray photons generated during thunderstorms, which have been detected almost exclusively by satellite-based instruments. Here we present three lines of evidence which includes the three out of three simultaneously observed pairs, the same occurrence contexts, and the consistent estimated occurrence rate, which indicate a direct relationship between a subset of TGFs and a class of energetic radio signal easily detectable by ground-based sensors. This connection indicates that these gamma ray and radio emissions are two views of the same phenomenon and further enable detection of these TGFs from ground distant radio signals alone. Besides dramatically increasing the detection rate of TGFs, this ground detection approach can identify TGFs in continental and coastal areas that are at latitudes too high for present TGF-detecting satellites and will provide more insights into the mechanism of TGF production. C1 [Lyu, Fanchao; Cummer, Steven A.] Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA. [Briggs, Michael; Cramer, Eric; Fitzpatrick, Gerard; Mailyan, Bagrat] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. [Briggs, Michael; Stanbro, Matthew] Univ Alabama, Dept Space Sci, Huntsville, AL 35899 USA. [Marisaldi, Martino] INAF IASF Bologna, Bologna, Italy. [Marisaldi, Martino] Univ Bergen, Dept Phys & Technol, Birkeland Ctr Space Sci, Bergen, Norway. [Blakeslee, Richard J.] NASA, Marshall Space Flight Ctr, Huntsville, AL USA. [Bruning, Eric] Texas Tech Univ, Dept Geosci, Atmospher Sci Grp, Lubbock, TX 79409 USA. [Wilson, Jennifer G.] NASA, Kennedy Space Ctr, Kennedy Space Ctr, FL USA. [Rison, William; Krehbiel, Paul] New Mexico Inst Min & Technol, Langmuir Lab Atmospher Res, Geophys Res Ctr, Socorro, NM 87801 USA. [Lu, Gaopeng] Chinese Acad Sci, Inst Atmospher Phys, Key Lab Middle Atmosphere & Global Environm Obser, Beijing, Peoples R China. [Lu, Gaopeng] Nanjing Univ Informat Sci & Technol, Collaborat Innovat Ctr Forecast & Evaluat Meteoro, Nanjing, Jiangsu, Peoples R China. [Cramer, Eric] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Fitzpatrick, Gerard; McBreen, Sheila; Roberts, Oliver J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. RP Cummer, SA (reprint author), Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA. EM cummer@ee.duke.edu RI Roberts, Oliver/N-6284-2016 OI Roberts, Oliver/0000-0002-7150-9061 FU National Science Foundation Dynamic and Physical Meteorology program [ATM-1047588]; DARPA Nimbus program [HR0011-10-10059]; Science Foundation Ireland [12/IP/1288] FX The authors would like to acknowledge the support from the National Science Foundation Dynamic and Physical Meteorology program through grant ATM-1047588 and the DARPA Nimbus program through grant HR0011-10-10059. The authors would like to thank those colleges at Florida Institute of Technology, University of Oklahoma, University of Mississippi, and Kansas State University which assist us with the operation of LF networks. We thank Vaisala Inc. for providing the real-time lightning data which enabled us to start the investigation. O.J.R. and S.M.B. acknowledge support from Science Foundation Ireland under grant 12/IP/1288. We thank the Fermi team for providing the Fermi-GBM gamma ray data (http://fermi.gsfc.nasa.gov/ssc/data/access/gbm/). The recent TGF catalog can be accessed on the website (http://fermi.gsfc.nasa.gov/ssc/data/access/gbm/tgf/). All data are available by request (cummer@ee.duke.edu). The authors would like to thank two anonymous reviewers for their comments to improve the paper. NR 31 TC 1 Z9 1 U1 1 U2 1 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 AUG 28 PY 2016 VL 43 IS 16 BP 8728 EP 8734 DI 10.1002/2016GL070154 PG 7 WC Geosciences, Multidisciplinary SC Geology GA DX5TC UT WOS:000384443800047 ER PT J AU Kahn, BH Huang, XL Stephens, GL Collins, WD Feldman, DR Su, H Wong, S Yue, Q AF Kahn, Brian H. Huang, Xianglei Stephens, Graeme L. Collins, William D. Feldman, Daniel R. Su, Hui Wong, Sun Yue, Qing TI ENSO regulation of far- and mid-infrared contributions to clear-sky OLR SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE far infrared; clear sky; tropics; ENSO; upper troposphere; water vapor ID SEA-SURFACE TEMPERATURE; TROPICAL DEEP CONVECTION; WATER-VAPOR; EL-NINO; CHANGING CLIMATE; CLOUDS; TROPOSPHERE; DEPENDENCE; SIGNATURE; RADIATION AB NASA Aqua-derived thermodynamic profiles, calculated spectral clear-sky outgoing longwave radiation (OLR), and vertical velocity fields from meteorological reanalyses are combined to determine the relative proportion of the far-infrared (FIR) and mid-infrared (MIR) spectral contributions to the total clear-sky OLR during different phases of El Nino-Southern Oscillation (ENSO). In the ascending branch of the tropical circulation, the spatial variance of upper tropospheric water vapor is shown to be larger during La Nina than El Nino and is consistent with zonal symmetry changes in the tropical waveguide and associated tropical-extratropical mixing. In the descending branch, upper tropospheric water vapor shows weaker coupling to lower layers that is evidenced by changes in the ratio of FIR to MIR in the clear-sky OLR. Diagnostics from the Geophysical Fluid Dynamics Laboratory AM3 model simulation are generally similar to satellite data, but the ratio of FIR to MIR is 5-10% larger with respect to dynamic regime. C1 [Kahn, Brian H.; Stephens, Graeme L.; Su, Hui; Wong, Sun; Yue, Qing] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Huang, Xianglei] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA. [Collins, William D.; Feldman, Daniel R.] Lawrence Berkeley Natl Lab, Climate & Ecosyst Div, Berkeley, CA USA. [Collins, William D.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. RP Kahn, BH (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM brian.h.kahn@jpl.nasa.gov RI Collins, William/J-3147-2014; Yue, Qing/F-4619-2017 OI Collins, William/0000-0002-4463-9848; Yue, Qing/0000-0002-3559-6508 FU JPL; University of Michigan; NASA [NNX14AJ50G]; U.S. Department of Energy, Office of Science, Office of Biological and Environmental Research, Terrestrial Ecosystem Science and Atmospheric System Research programs [DE-ACO2-05CH11231] FX A portion of this research was carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We thank two anonymous reviewers for very constructive feedback and insights that led to an improved manuscript. B. Kahn was supported by Strategic University Research Partnership (SURP) proposal between JPL and the University of Michigan. X. Huang was supported by NASA under grant NNX14AJ50G awarded to the University of Michigan. D. Feldman and W. Collins acknowledge support by the U.S. Department of Energy, Office of Science, Office of Biological and Environmental Research, Terrestrial Ecosystem Science and Atmospheric System Research programs, under award DE-ACO2-05CH11231. The AIRS version 6 data sets were processed by and obtained from the Goddard Earth Services Data and Information Services Center (http://daac.gsfc.nasa.gov/). The MERRA data sets were processed by and obtained from the NASA Goddard's Global Modeling and Assimilation Office (GMAO). Copyright 2016. All rights reserved. Government sponsorship acknowledged. NR 43 TC 0 Z9 0 U1 6 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 28 PY 2016 VL 43 IS 16 BP 8751 EP 8759 DI 10.1002/2016GL070263 PG 9 WC Geosciences, Multidisciplinary SC Geology GA DX5TC UT WOS:000384443800050 ER PT J AU Wu, LH Hasekamp, O van Diedenhoven, B Cairns, B Yorks, JE Chowdhary, J AF Wu, Lianghai Hasekamp, Otto van Diedenhoven, Bastiaan Cairns, Brian Yorks, John E. Chowdhary, Jacek TI Passive remote sensing of aerosol layer height using near-UV multiangle polarization measurements SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE aerosol layer height ID RESEARCH SCANNING POLARIMETER; RADIATIVE-TRANSFER MODEL; PHOTOPOLARIMETRIC MEASUREMENTS; SPECTRAL-RESOLUTION; OPTICAL-PROPERTIES; RETRIEVAL; OCEAN; SENSITIVITY; LIDAR; BAND AB We demonstrate that multiangle polarization measurements in the near-UV and blue part of the spectrum are very well suited for passive remote sensing of aerosol layer height. For this purpose we use simulated measurements with different setups (different wavelength ranges, with and without polarization, different polarimetric accuracies) as well as airborne measurements from the Research Scanning Polarimeter (RSP) obtained over the continental USA. We find good agreement of the retrieved aerosol layer height from RSP with measurements from the Cloud Physics Lidar showing a mean absolute difference of less than 1km. Furthermore, we found that the information on aerosol layer height is provided for large part by the multiangle polarization measurements with high accuracy rather than the multiangle intensity measurements. The information on aerosol layer height is significantly decreased when the shortest RSP wavelength (410nm) is excluded from the retrieval and is virtually absent when 550nm is used as shortest wavelength. C1 [Wu, Lianghai; Hasekamp, Otto] SRON Netherlands Inst Space Res, Utrecht, Netherlands. [van Diedenhoven, Bastiaan] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [van Diedenhoven, Bastiaan; Cairns, Brian; Chowdhary, Jacek] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Yorks, John E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Chowdhary, Jacek] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. RP Wu, LH (reprint author), SRON Netherlands Inst Space Res, Utrecht, Netherlands. EM l.wu@sron.nl FU NASA Radiation Sciences Program FX The RSP data are available from NASA Goddard Institute for Space Studies (http://data.giss.nasa.gov/pub/rsp/). The RSP data from the SEAC4RS and PODEX field experiments that are used in this study were funded by the NASA Radiation Sciences Program managed by Hal Maring and by the NASA Earth Science Division as part of the preformulation study for the Aerosol Cloud and ocean Ecosystem (ACE) mission. The CPL data are provided by NASA Goddard Space Flight Center from the Web site at http://cpl.gsfc.nasa.gov/. NR 42 TC 0 Z9 0 U1 2 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 28 PY 2016 VL 43 IS 16 BP 8783 EP 8790 DI 10.1002/2016GL069848 PG 8 WC Geosciences, Multidisciplinary SC Geology GA DX5TC UT WOS:000384443800054 ER PT J AU Newman, PA Coy, L Pawson, S Lait, LR AF Newman, P. A. Coy, L. Pawson, S. Lait, L. R. TI The anomalous change in the QBO in 2015-2016 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE QBO ID QUASI-BIENNIAL OSCILLATION; EQUATORIAL STRATOSPHERE; GENERAL-CIRCULATION; WIND; MODEL AB The quasi-biennial oscillation (QBO) is a tropical lower stratospheric, downward propagating zonal wind variation, with an average period of similar to 8months. The QBO has been constantly documented since 1953. Here we describe the evolution of the QBO during the Northern Hemisphere winter of 2015-2016 using radiosonde observations and meteorological reanalyses. Normally, the QBO would show a steady downward propagation of the westerly phase. In 2015-2016, there was an anomalous upward displacement of this westerly phase from similar to 30hPa to 15hPa. These westerlies impinge on or cutoff the normal downward propagation of the easterly phase. In addition, easterly winds develop at 40hPa. Comparisons to tropical wind statistics for the 1953 to present record demonstrate that this 2015-2016 QBO disruption is unprecedented. C1 [Newman, P. A.; Coy, L.; Pawson, S.; Lait, L. R.] NASA, GSFC, Greenbelt, MD 20771 USA. [Coy, L.] SSAI, Lanham, MD USA. [Lait, L. R.] Morgan State Univ, Baltimore, MD 21239 USA. RP Newman, PA (reprint author), NASA, GSFC, Greenbelt, MD 20771 USA. EM paul.a.newman@nasa.gov FU NASA Modeling, Analysis, and Prediction program; NASA Atmospheric Composition Modeling and Analysis Program FX The help of Eric R. Nash and Gerald Ziemke is greatly appreciated. This research was performed with funding from the NASA Modeling, Analysis, and Prediction program and the NASA Atmospheric Composition Modeling and Analysis Program. The MERRA-2 reanalysis fields were obtained from the NASA Earth Observing System Data and Information System (https://earthdata.nasa.gov). The monthly mean QBO data for the 1953-1978 period were obtained from the Freie Universitat Berlin (http://www.geo.fu-berlin.de/en/met/ag/strat/produkte/qbo/). Daily global radiosondes have been collected at NASA/GSFC and are provided from the Global Telecommunications System (available via the NOAA/NCEP web site: ftp://ftp.cpc.ncep.noaa.gov/wd53rl/rsonde/). NR 16 TC 3 Z9 3 U1 6 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 28 PY 2016 VL 43 IS 16 BP 8791 EP 8797 DI 10.1002/2016GL070373 PG 7 WC Geosciences, Multidisciplinary SC Geology GA DX5TC UT WOS:000384443800055 ER PT J AU Mackie, CJ Candian, A Huang, XC Maltseva, E Petrignani, A Oomens, J Mattioda, AL Buma, WJ Lee, TJ Tielens, AGGM AF Mackie, Cameron J. Candian, Alessandra Huang, Xinchuan Maltseva, Elena Petrignani, Annemieke Oomens, Jos Mattioda, Andrew L. Buma, Wybren Jan Lee, Timothy J. Tielens, Alexander G. G. M. TI The anharmonic quartic force field infrared spectra of five non-linear polycyclic aromatic hydrocarbons: Benz[a]anthracene, chrysene, phenanthrene, pyrene, and triphenylene SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID EMISSION FEATURES; SPECTROSCOPY; PAHS; MOLECULES; GRAPHENE; DATABASE; RINGS; IONS AB The study of interstellar polycyclic aromatic hydrocarbons (PAHs) relies heavily on theoretically predicted infrared spectra. Most earlier studies use scaled harmonic frequencies for band positions and the double harmonic approximation for intensities. However, recent high-resolution gas-phase experimental spectroscopic studies have shown that the harmonic approximation is not sufficient to reproduce experimental results. In our previous work, we presented the anharmonic theoretical spectra of three linear PAHs, showing the importance of including anharmonicities into the theoretical calculations. In this paper, we continue this work by extending the study to include five non-linear PAHs (benz[a]anthracene, chrysene, phenanthrene, pyrene, and triphenylene), thereby allowing us to make a full assessment of how edge structure, symmetry, and size influence the effects of anharmonicities. The theoretical anharmonic spectra are compared to spectra obtained under matrix isolation low-temperature conditions, low-resolution, high-temperature gas-phase conditions, and high-resolution, low-temperature gas-phase conditions. Overall, excellent agreement is observed between the theoretical and experimental spectra although the experimental spectra show subtle but significant differences. Published by AIP Publishing. C1 [Mackie, Cameron J.; Candian, Alessandra; Petrignani, Annemieke; Tielens, Alexander G. G. M.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Huang, Xinchuan] SETI Inst, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA. [Maltseva, Elena; Petrignani, Annemieke; Buma, Wybren Jan] Univ Amsterdam, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. [Petrignani, Annemieke; Oomens, Jos] Radboud Univ Nijmegen, Toernooiveld 7, NL-6525 ED Nijmegen, Netherlands. [Mattioda, Andrew L.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Mackie, CJ (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM mackie@strw.leidenuniv.nl RI Buma, Wybren Jan/F-6691-2011; Lee, Timothy/K-2838-2012; HUANG, XINCHUAN/A-3266-2013; OI Buma, Wybren Jan/0000-0002-1265-8016; Petrignani, Annemieke/0000-0002-6116-5867; Candian, Alessandra/0000-0002-5431-4449 FU Advanced European Research Council [246976]; Spinoza award; Dutch Astrochemistry Network - Netherlands Organization for Scientific Research, NWO; NWO Exacte Wetenschappen [MP-270-13, MP-264]; NWO [639.041.543, 723.014.007]; NASA [12-APRA12-0107]; NASA/SETI [NNX15AF45A]; National Aeronautics and Space Administration through the NASA Astrobiology Institute through the Science Mission Directorate [NNH13ZDA017C] FX The authors would like to thank the two anonymous reviewers for their helpful comments that improved the clarity of the manuscript. The spectroscopic study of interstellar PAHs at Leiden Observatory has been supported through the Advanced European Research Council Grant No. 246976, a Spinoza award, and through the Dutch Astrochemistry Network funded by the Netherlands Organization for Scientific Research, NWO. Computing time has been made available by NWO Exacte Wetenschappen (Project Nos. MP-270-13 and MP-264) and calculations were performed at the LISA Linux cluster of the SurfSARA supercomputer center in Almere, The Netherlands. A.C. acknowledges NWO for a VENI grant (639.041.543). A.P. acknowledges NWO for a VIDI grant (723.014.007). X.H. and T.J.L. gratefully acknowledge support from the NASA 12-APRA12-0107 grant. X.H. acknowledges the support from NASA/SETI Co-op Agreement NNX15AF45A. This material is based upon work supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement Notice NNH13ZDA017C issued through the Science Mission Directorate. NR 44 TC 3 Z9 3 U1 17 U2 17 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 AUG 28 PY 2016 VL 145 IS 8 AR 084313 DI 10.1063/1.4961438 PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA DW8AL UT WOS:000383875500034 PM 27586928 ER PT J AU Battaglia, A Mroz, K Lang, T Tridon, F Tanelli, S Tian, L Heymsfield, GM AF Battaglia, A. Mroz, K. Lang, Tim Tridon, F. Tanelli, S. Tian, Lin Heymsfield, Gerald M. TI Using a multiwavelength suite of microwave instruments to investigate the microphysical structure of deep convective cores SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID DUAL-WAVELENGTH RADAR; HYDROMETEOR IDENTIFICATION ALGORITHM; RAIN-PROFILING ALGORITHM; MULTIPLE-SCATTERING; PART II; PRECIPITATION RETRIEVAL; LIQUID WATER; CLOUD; ATTENUATION; RADIOMETER AB Due to the large natural variability of its microphysical properties, the characterization of solid precipitation is a longstanding problem. Since in situ observations are unavailable in severe convective systems, innovative remote sensing retrievals are needed to extend our understanding of such systems. This study presents a novel technique able to retrieve the density, mass, and effective diameter of graupel and hail in severe convection through the combination of airborne microwave remote sensing instruments. The retrieval is applied to measure solid precipitation properties within two convective cells observed on 23-24 May 2014 over North Carolina during the IPHEx campaign by the NASA ER-2 instrument suite. Between 30 and 40 degrees of freedom of signal are associated with the measurements, which is insufficient to provide full microphysics profiling. The measurements have the largest impact on the retrieval of ice particle sizes, followed by ice water contents. Ice densities are mainly driven by a priori assumptions, though low relative errors in ice densities suggest that in extensive regions of the convective system, only particles with densities larger than 0.4 g/cm(3) are compatible with the observations. This is in agreement with reports of large hail on the ground and with hydrometeor classification derived from ground-based polarimetric radars observations. This work confirms that multiple scattering generated by large ice hydrometeors in deep convection is relevant for airborne radar systems already at Ku band. A fortiori, multiple scattering will play a pivotal role in such conditions also for Ku band spaceborne radars (e.g., the GPM Dual Precipitation Radar). C1 [Battaglia, A.; Mroz, K.] Univ Leicester, Natl Ctr Earth Observat, Leicester, Leics, England. [Battaglia, A.; Tridon, F.] Univ Leicester, Dept Phys & Astron, Earth Observat Sci, Leicester, Leics, England. [Lang, Tim] NASA Marshall Space Flight Ctr, Huntsville, AL USA. [Tanelli, S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Tian, Lin; Heymsfield, Gerald M.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Tian, Lin] Morgan State Univ, Goddard Earth Sci Technol & Res Program, Baltimore, MD 21239 USA. RP Battaglia, A (reprint author), Univ Leicester, Natl Ctr Earth Observat, Leicester, Leics, England.; Battaglia, A (reprint author), Univ Leicester, Dept Phys & Astron, Earth Observat Sci, Leicester, Leics, England. EM a.battaglia@leicester.ac.uk RI Tridon, Frederic/M-4127-2013; OI Tridon, Frederic/0000-0002-0436-283X; Battaglia, Alessandro/0000-0001-9243-3484 FU project "Calibration and validation studies over the North Atlantic and UK for the Global Precipitation Mission" - UK NERC [NE/L007169/1]; NASA ACE Mission formulation; GPM Ground Validation; NASA Airborne Instrument Technology Transition (AITT); ACE; GPM GV; NASA FX The work done by A. Battaglia and F. Tridon was funded by the project "Calibration and validation studies over the North Atlantic and UK for the Global Precipitation Mission" funded by the UK NERC (NE/L007169/1). The forward radar model code was courteously provided by R. Hogan (http://www.met.rdg.ac.uk/clouds/multiscatter/). This research used the ALICE High Performance Computing Facility at the University of Leicester. CRS was supported by the NASA ACE Mission formulation. HIWRAP was supported by GPM Ground Validation. EXRAD was supported by the NASA Airborne Instrument Technology Transition (AITT). ER-2 flights were jointly sponsored by GPM ground validation and the ACE Decadal Mission study. AMPRs participation was supported by GPM GV. Timothy Lang was supported by GPM GV. The work performed by Simone Tanelli was carried out at the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA in support to the preformulation phase studies for the ACE mission concept and to the GPM Science Team. NEXRAD data were obtained from NOAA via the online data set hosted by Amazon Web Services. NEXRAD processing code is available from https://github.com/ARM-DOE/pyart, https://github.com/CSU-Radarmet/CSU_RadarTools, and https://github.com/nasa/DualPol. AMPR processing code is available from https://github.com/nasa/PyAMPR. NR 62 TC 0 Z9 0 U1 7 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 AUG 27 PY 2016 VL 121 IS 16 BP 9356 EP 9381 DI 10.1002/2016JD025269 PG 26 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DZ9OQ UT WOS:000386207200006 PM 27708991 ER PT J AU Li, JLF Wang, YH Lee, T Waliser, D Lee, WL Yu, JY Chen, YC Fetzer, E Hasson, A AF Li, J. -L. F. Wang, Yi-Hui Lee, Tong Waliser, Duane Lee, Wei-Liang Yu, Jia-Yuh Chen, Yi-Chun Fetzer, Eric Hasson, Audrey TI The impacts of precipitating cloud radiative effects on ocean surface evaporation, precipitation, and ocean salinity in coupled GCM simulations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GLOBAL WATER CYCLE; GENERAL-CIRCULATION MODEL; ABRUPT CLIMATE-CHANGE; THERMOHALINE CIRCULATION; FLUX CORRECTION; PART I; CMIP3; VARIABILITY; ARGO; INTENSIFICATION AB The coupled global climate model (GCM) fidelity in representing upper ocean salinity including near sea surface bulk salinity (SSS) is evaluated in this study, with a focus on the Pacific Ocean. The systematic biases in ocean surface evaporation (E) minus precipitation (P) and SSS are found to be fairly similar in the twentieth century simulations of the Coupled Model Intercomparison Phase 3 (CMIP3) and Phase 5 (CMIP5) relative to the observations. One of the potential causes of the CMIP model biases is the missing representation of the radiative effects of precipitating hydrometeors (i.e., snow) in most CMIP models. To examine the radiative effect of cloud snow on SSS, sensitivity experiments with and without such effect are conducted by the National Center for Atmospheric Research-coupled Community Earth System Model (CESM). This study investigates the difference in SSS between sensitivity experiments and its relationship with atmospheric circulation, E - P and air-sea heat fluxes. It is found that the exclusion of the cloud snow radiative effect in CESM produces weaker Pacific trade winds, resulting in enhanced precipitation, reduced evaporation, and a reduction of the upper ocean salinity in the tropical and subtropical Pacific. The latter results in an improved comparison with climatological upper ocean bulk salinity. The introduction of cloud snow also altered the budget terms that maintain the time-mean salinity in the mixed layer. C1 [Li, J. -L. F.; Wang, Yi-Hui; Lee, Tong; Waliser, Duane; Fetzer, Eric; Hasson, Audrey] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Li, J. -L. F.; Lee, Tong; Waliser, Duane; Fetzer, Eric] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. [Lee, Wei-Liang; Chen, Yi-Chun] Acad Sinica, Res Ctr Environm Change, Taipei, Taiwan. [Yu, Jia-Yuh] Natl Cent Univ, Dept Atmospher Sci, Taoyuan, Taiwan. RP Li, JLF (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.; Li, JLF (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. EM Juilin.F.Li@jpl.nasa.gov FU Earth Science Program, the Modeling, Analysis, and Prediction (MAP) [NNH12ZDA001N ROSES 2012]; ATMOS COMP [NNH12ZDA001N-CCST]; NDOA; National Aeronautics and Space Administration (NASA); NASA Physical Oceanography Program; NASA; Ministry of Science and Technology of Taiwan [NSC100-2119-M-001-029-MY5, NSC102-2111-M-001-009] FX We acknowledge PCMDI/DOE and the WCRP's WGCM for their roles in making CMIP3/CMIP5 available. We thank Qing Yue and Graeme Stephens for their useful comments. The contribution by J.L.L. and D.E.W. to this study were carried out on behalf of the Jet Propulsion Laboratory, California Institute of Technology, under contracts of NNH12ZDA001N ROSES 2012, Earth Science Program, the Modeling, Analysis, and Prediction (MAP), and ATMOS COMP 2013 (NNH12ZDA001N-CCST) and J.J.L. under NDOA with the National Aeronautics and Space Administration (NASA) as well as T.L. from NASA Physical Oceanography Program. This work has been supported in part by the NASA Making Earth System Data Records for Use in Research Environments (MEaSUREs) programs. W.L.L. was supported by Ministry of Science and Technology of Taiwan under contracts NSC100-2119-M-001-029-MY5 and NSC102-2111-M-001-009. The subsurface ocean salinity data from the World Ocean Atlas 2009 (WOA09) is used in this study and can be found in http://www.nodc.noaa.gov/OC5/WOA09/pr_woa09.html. The long-term mean evaporation is based on the Objectively Analyzed air-sea Fluxes (OAFlux) product [Yu and Weller,]. The OAFlux project began in 1958, and its utilization of satellite-based, high-resolution ocean surface vector winds since July 1987 weights the long-term mean in favor of the late twentieth century and can be found at http://oaflux.whoi.edu/. The long-term mean precipitation is obtained from the Global Precipitation Climatology Project (GPCP) (http://www.esrl.noaa.gov/psd/data/gridded/data.gpcp.html). NR 72 TC 0 Z9 0 U1 2 U2 2 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 AUG 27 PY 2016 VL 121 IS 16 BP 9474 EP 9491 DI 10.1002/2016JD024911 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DZ9OQ UT WOS:000386207200012 ER PT J AU Wen, GY Marshak, A Varnai, T Levy, R AF Wen, Guoyong Marshak, Alexander Varnai, Tamas Levy, Robert TI Testing the two-layer model for correcting near-cloud reflectance enhancement using LES/SHDOM-simulated radiances SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID RADIATIVE-TRANSFER; CALIPSO OBSERVATIONS; AEROSOL PROPERTIES; BROKEN CLOUDS; MODIS; PRODUCTS; VALIDATION; SCATTERING; SATELLITE; SURFACE AB A transition zone exists between cloudy skies and clear sky; such that, clouds scatter solar radiation into clear-sky regions. From a satellite perspective, it appears that clouds enhance the radiation nearby. We seek a simple method to estimate this enhancement, since it is so computationally expensive to account for all three-dimensional (3-D) scattering processes. In previous studies, we developed a simple two-layer model (2LM) that estimated the radiation scattered via cloud-molecular interactions. Here we have developed a new model to account for cloud-surface interaction (CSI). We test the models by comparing to calculations provided by full 3-D radiative transfer simulations of realistic cloud scenes. For these scenes, the Moderate Resolution Imaging Spectroradiometer (MODIS)-like radiance fields were computed from the Spherical Harmonic Discrete Ordinate Method (SHDOM), based on a large number of cumulus fields simulated by the University of California, Los Angeles (UCLA) large eddy simulation (LES) model. We find that the original 2LM model that estimates cloud-air molecule interactions accounts for 64% of the total reflectance enhancement and the new model (2LM + CSI) that also includes cloud-surface interactions accounts for nearly 80%. We discuss the possibility of accounting for cloud-aerosol radiative interactions in 3-D cloud-induced reflectance enhancement, which may explain the remaining 20% of enhancements. Because these are simple models, these corrections can be applied to global satellite observations (e.g., MODIS) and help to reduce biases in aerosol and other clear-sky retrievals. C1 [Wen, Guoyong; Marshak, Alexander; Varnai, Tamas; Levy, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wen, Guoyong] Morgan State Univ, GESTAR, Baltimore, MD 21239 USA. [Varnai, Tamas] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. RP Wen, GY (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Wen, GY (reprint author), Morgan State Univ, GESTAR, Baltimore, MD 21239 USA. EM Guoyong.Wen-1@nasa.gov RI Marshak, Alexander/D-5671-2012; Levy, Robert/M-7764-2013 OI Levy, Robert/0000-0002-8933-5303 FU NASA Radiation Program; NASA CALIPSO project; NASA Terra/Aqua projects FX We gratefully acknowledge support for this research by the NASA Radiation Program managed by Hal Maring, the NASA CALIPSO project supervised by David Considine, and the NASA Terra/Aqua projects managed by Paula Bontempi. We also thank Frank Evans for providing the results of radiative transfer calculations for cumulus fields from Large-Eddy Simulations. NR 45 TC 0 Z9 0 U1 1 U2 1 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 AUG 27 PY 2016 VL 121 IS 16 BP 9661 EP 9674 DI 10.1002/2016JD025021 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DZ9OQ UT WOS:000386207200023 ER PT J AU Lang, TJ Lyons, WA Cummer, SA Fuchs, BR Dolan, B Rutledge, SA Krehbiel, P Rison, W Stanley, M Ashcraft, T AF Lang, Timothy J. Lyons, Walter A. Cummer, Steven A. Fuchs, Brody R. Dolan, Brenda Rutledge, Steven A. Krehbiel, Paul Rison, William Stanley, Mark Ashcraft, Thomas TI Observations of two sprite-producing storms in Colorado SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID CHARGE MOMENT CHANGES; SEVERE THUNDERSTORM ELECTRIFICATION; MESOSCALE CONVECTIVE SYSTEMS; CONTINENTAL UNITED-STATES; LIGHTNING FLASH RATE; PART II; PRECIPITATION; RADAR; STEPS; ELVES AB Two sprite-producing thunderstorms were observed on 8 and 25 June 2012 in northeastern Colorado by a combination of low-light cameras, a lightning mapping array, polarimetric and Doppler radars, the National Lightning Detection Network, and charge moment change measurements. The 8 June event evolved from a tornadic hailstorm to a larger multicellular system that produced 21 observed positive sprites in 2 h. The majority of sprites occurred during a lull in convective strength, as measured by total flash rate, flash energy, and radar echo volume. Mean flash area spiked multiple times during this period; however, total flash rates still exceeded 60 min(-1), and portions of the storm featured a complex anomalous charge structure, with midlevel positive charge near -20 degrees C. The storm produced predominantly positive cloud-to-ground lightning. All sprite-parent flashes occurred on the northeastern flank of the storm, where strong westerly upper level flow was consistent with advection of charged precipitation away from convection, providing a pathway for stratiform lightning. The 25 June event was another multicellular hailstorm with an anomalous charge structure that produced 26 positive sprites in less than 1 h. The sprites again occurred during a convective lull, with relatively weaker reflectivity and lower total flash rate but relatively larger mean flash area. However, all sprite parents occurred in or near convection and tapped charge layers in adjacent anvil cloud. The results demonstrate the sprite production by convective ground strokes in anomalously charged storms and also indicate that sprite production and convective vigor are inversely related in mature storms. C1 [Lang, Timothy J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Lyons, Walter A.] FMA Res Inc, Ft Collins, CO USA. [Cummer, Steven A.] Duke Univ, Durham, NC USA. [Fuchs, Brody R.; Dolan, Brenda; Rutledge, Steven A.] Colorado State Univ, Ft Collins, CO 80523 USA. [Krehbiel, Paul; Rison, William; Stanley, Mark] New Mexico Inst Min & Technol, Socorro, NM 87801 USA. [Ashcraft, Thomas] Heliotown Observ, Lamy, NM USA. RP Lang, TJ (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM timothy.j.lang@nasa.gov OI Fuchs, Brody/0000-0002-7629-0687 FU NASA; Defense Advanced Research Project Agency (DARPA); National Science Foundation (NSF); NSF; National Oceanic and Atmospheric Administration (NOAA) FX Pat Kennedy, Dave Brunkow, Jim George, and Bob Bowie all contributed to the CSU-CHILL and CSU-Pawnee radar scanning on the storm days analyzed in this study, and thus, important data sets would not have been available without their help. CSU radar data and COLMA data from DC3 are available from the National Center for Atmospheric Research (NCAR; http://data.eol.ucar.edu/master_list/?project=DC3). NEXRAD volumetric radar data are available from Amazon Web Services (https://aws.amazon.com/noaa-big-data/nexrad/), while MRMS data are available from the National Severe Storms Laboratory (http://www.nssl.noaa.gov/projects/mrms/). NLDN data are available from the NASA Global Hydrology Resource Center (https://ghrc.nsstc.nasa.gov/home/). Sounding data were obtained from the University of Wyoming (http://weather.uwyo.edu/upperair/sounding.html). Key open source software packages used in this study include Py-ART (http://arm-doe.github.io/pyart/), ARTview (https://github.com/nguy/artview), lmatools (https://github.com/deeplycloudy/lmatools), CSU_RadarTools (https://github.com/CSU-Radarmet/CSU_RadarTools), DualPol (https://github.com/nasa/DualPol), MMM-Py (https://github.com/nasa/MMM-Py), SkewT (https://pypi.python.org/pypi/SkewT), and SHARPpy (http://sharppy.github.io/SHARPpy/). CEDRIC and SPRINT can be obtained from NCAR (https://wiki.ucar.edu/display/raygridding/Home) along with other useful radar software, such as Radx (https://www.ral.ucar.edu/projects/titan/docs/radial_formats/radx.html). Contact the first author (timothy.j.lang@nasa.gov) for access to other data sets, such as sprite imagery and CMCN measurements. Lang also can provide access to customized analysis software, such as CLEAR and XLMA. Funding for this work was provided by the NASA Lightning Imaging Sensor (LIS) project, the Defense Advanced Research Project Agency (DARPA) Nimbus program, and the National Science Foundation (NSF) Physical Meteorology and Lower Atmosphere Observing Facilities programs. DC3 was made possible by the financial and logistical support of NSF, NASA, and the National Oceanic and Atmospheric Administration (NOAA). The views, opinions, and findings in this report are those of the authors and should not be construed as an official NASA or U.S. Government position, policy, or decision. NR 85 TC 0 Z9 0 U1 7 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 AUG 27 PY 2016 VL 121 IS 16 BP 9675 EP 9695 DI 10.1002/2016JD025299 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DZ9OQ UT WOS:000386207200024 ER PT J AU Fast, JD Berg, LK Zhang, K Easter, RC Ferrare, RA Hair, JW Hostetler, CA Liu, Y Ortega, I Sedlacek, A Shilling, JE Shrivastava, M Springston, SR Tomlinson, JM Volkamer, R Wilson, J Zaveri, RA Zelenyuk, A AF Fast, Jerome D. Berg, Larry K. Zhang, Kai Easter, Richard C. Ferrare, Richard A. Hair, Johnathan W. Hostetler, Chris A. Liu, Ying Ortega, Ivan Sedlacek, Arthur, III Shilling, John E. Shrivastava, Manish Springston, Stephen R. Tomlinson, Jason M. Volkamer, Rainer Wilson, Jacqueline Zaveri, Rahul A. Zelenyuk, Alla TI Model representations of aerosol layers transported from North America over the Atlantic Ocean during the Two-Column Aerosol Project SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID COMMUNITY ATMOSPHERE MODEL; PHASE FRAGMENTATION REACTIONS; CLOUD MICROPHYSICS SCHEME; SPECTRAL-RESOLUTION LIDAR; CARBON VERTICAL PROFILES; GLOBAL CLIMATE MODEL; LONG-RANGE TRANSPORT; LOW-VOLATILITY SOA; BASIS-SET APPROACH; ORGANIC AEROSOL AB The ability of the Weather Research and Forecasting model with chemistry (WRF-Chem) version 3.7 and the Community Atmosphere Model version 5.3 (CAM5) in simulating profiles of aerosol properties is quantified using extensive in situ and remote sensing measurements from the Two-Column Aerosol Project (TCAP) conducted during July of 2012. TCAP was supported by the U.S. Department of Energy's Atmospheric Radiation Measurement program and was designed to obtain observations within two atmospheric columns; one fixed over Cape Cod, Massachusetts, and the other several hundred kilometers over the ocean. The performance is quantified using most of the available aircraft and surface measurements during July, and 2 days are examined in more detail to identify the processes responsible for the observed aerosol layers. The higher-resolution WRF-Chem model produced more aerosol mass in the free troposphere than the coarser-resolution CAM5 model so that the fraction of aerosol optical thicknessabove the residual layer from WRF-Chem was more consistent with lidar measurements. We found that the free troposphere layers are likely due to mean vertical motions associated with synoptic-scale convergence that lifts aerosols from the boundary layer. The vertical displacement and the time period associated with upward transport in the troposphere depend on the strength of the synoptic system and whether relatively high boundary layer aerosol concentrations are present where convergence occurs. While a parameterization of subgrid scale convective clouds applied in WRF-Chem modulated the concentrations of aerosols aloft, it did not significantly change the overall altitude and depth of the layers. C1 [Fast, Jerome D.; Berg, Larry K.; Zhang, Kai; Easter, Richard C.; Liu, Ying; Shilling, John E.; Shrivastava, Manish; Tomlinson, Jason M.; Wilson, Jacqueline; Zaveri, Rahul A.; Zelenyuk, Alla] Pacific Northwest Natl Lab, Richland, WA 99352 USA. [Ferrare, Richard A.; Hair, Johnathan W.; Hostetler, Chris A.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Ortega, Ivan; Volkamer, Rainer] Univ Colorado, Dept Chem, Boulder, CO 80309 USA. [Sedlacek, Arthur, III; Springston, Stephen R.] Brookhaven Natl Lab, Upton, NY 11973 USA. RP Fast, JD (reprint author), Pacific Northwest Natl Lab, Richland, WA 99352 USA. EM jerome.fast@pnl.gov RI Zhang, Kai/F-8415-2010; Volkamer, Rainer/B-8925-2016 OI Zhang, Kai/0000-0003-0457-6368; Volkamer, Rainer/0000-0002-0899-1369 FU Office of Science of the U.S. Department of Energy; DOE ARM [DE-SC0006730]; National Science Foundation; [DE-A06-76RLO976 1830] FX This research was supported by the Office of Science of the U.S. Department of Energy as part of the Atmospheric Radiation Measurement (ARM) and Atmospheric System Research (ASR) programs. The Pacific Northwest National Laboratory (PNNL) is operated by DOE by the Battelle Memorial Institute under contract DE-A06-76RLO976 1830. We thank the contributions of numerous individuals, including the G-1 flight crew (M. Hubbell, W. Svancara, J. Hone, and E. Dukes), King Air flight crew (R. Yasky, L. Kagey, M. Wusk, D. Bowser, S. Sims, D. Riddick, and G. Slover), staff from the Cape Cod National Seashore (Superintendent G. Price, L. McKean, C. Skowron, and B. Dougan), Cape Cod National Seashore Atlantic Research and Learning Center, and the radiosonde launch team from the Provincetown Center for Coastal Studies (M. Dunn, S. Greene, C. Hudak, L. Ludwig, J. Melander, D. Minsky, K. Shorr, S. Sollog, D. Towler, E. Larson, D. Dionne, C. Skowron). Support for the HSRL-2 flight operations during TCAP was provided by the DOE ARM program, Interagency Agreement DE-SC0006730, while support for the development of HSRL-2 was provided by the NASA Science Mission Directorate, ESTO, AITT, and Radiation Science Programs. The NOAA-MFRSR measurements were supported by NOAA GOES-R Cal/Val Activities within NOAA's National Environmental Satellite, Data, and Information Service. We thank Joseph Michalsky (NOAA) for providing the AOD measurements from the MFRSR instrument, Louisa Emmons (NCAR) for providing the MOZART global chemistry model output, Christine Wiedinmyer (NCAR) for providing the fire emissions inventory, Stuart McKeen (NOAA) for processing the 2011 NEI, Michael Sprenger and Heini Wernli (ETH) for providing the Lagrangian Analysis Tool LAGRANTO for the CAM5 back trajectory calculations, and Po-Lun Ma (PNNL) for assisting with the set up of CAM5. The Environmental Molecular Science Laboratory (EMSL), a DOE Office of Science User Facility located at PNNL, provided computational resources for the WRF-Chem simulations. For the CAM5 simulations, we would like to acknowledge the computing support from Yellowstone (ark:/85065/d7wd3xhc) provided by NCAR's Computational and Information Systems Laboratory (sponsored by the National Science Foundation) and from the PNNL Institutional Computing (PIC). Data used in this manuscript are available from the ARM data archive (www.archive.arm.gov) or from the corresponding author (jerome.fast@pnnl.gov). NR 108 TC 1 Z9 1 U1 8 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 AUG 27 PY 2016 VL 121 IS 16 BP 9814 EP 9848 DI 10.1002/2016JD025248 PG 35 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DZ9OQ UT WOS:000386207200031 ER PT J AU Li, JY Mao, JQ Min, KE Washenfelder, RA Brown, SS Kaiser, J Keutsch, FN Volkamer, R Wolfe, GM Hanisco, TF Pollack, IB Ryerson, TB Graus, M Gilman, JB Lerner, BM Warneke, C de Gouw, JA Middlebrook, AM Liao, J Welti, A Henderson, BH McNeill, VF Hall, SR Ullmann, K Donner, LJ Paulot, F Horowitz, LW AF Li, Jingyi Mao, Jingqiu Min, Kyung-Eun Washenfelder, Rebecca A. Brown, Steven S. Kaiser, Jennifer Keutsch, Frank N. Volkamer, Rainer Wolfe, Glenn M. Hanisco, Thomas F. Pollack, Ilana B. Ryerson, Thomas B. Graus, Martin Gilman, Jessica B. Lerner, Brian M. Warneke, Carsten de Gouw, Joost A. Middlebrook, Ann M. Liao, Jin Welti, Andre Henderson, Barron H. McNeill, V. Faye Hall, Samuel R. Ullmann, Kirk Donner, Leo J. Paulot, Fabien Horowitz, Larry W. TI Observational constraints on glyoxal production from isoprene oxidation and its contribution to organic aerosol over the Southeast United States SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID RADICAL-INITIATED OXIDATION; MASTER CHEMICAL MECHANISM; METHYL VINYL KETONE; GAS-PHASE; ATMOSPHERIC CHEMISTRY; TROPOSPHERIC DEGRADATION; HETEROGENEOUS CHEMISTRY; AIRCRAFT MEASUREMENTS; PARTICULATE MATTER; PEROXY-RADICALS AB We use a 0-D photochemical box model and a 3-D global chemistry-climate model, combined with observations from the NOAA Southeast Nexus (SENEX) aircraft campaign, to understand the sources and sinks of glyoxal over the Southeast United States. Box model simulations suggest a large difference in glyoxal production among three isoprene oxidation mechanisms (AM3ST, AM3B, and Master Chemical Mechanism (MCM) v3.3.1). These mechanisms are then implemented into a 3-D global chemistry-climate model. Comparison with field observations shows that the average vertical profile of glyoxal is best reproduced by AM3ST with an effective reactive uptake coefficient.glyx of 2 x 10(-3) and AM3B without heterogeneous loss of glyoxal. The two mechanisms lead to 0-0.8 mu gm(-3) secondary organic aerosol (SOA) from glyoxal in the boundary layer of the Southeast U.S. in summer. We consider this to be the lower limit for the contribution of glyoxal to SOA, as other sources of glyoxal other than isoprene are not included in our model. In addition, we find that AM3B shows better agreement on both formaldehyde and the correlation between glyoxal and formaldehyde (RGF = [GLYX]/[HCHO]), resulting from the suppression of d-isoprene peroxy radicals. We also find that MCM v3.3.1 may underestimate glyoxal production from isoprene oxidation, in part due to an underestimated yield from the reaction of isoprene epoxydiol (IEPOX) peroxy radicals with HO2. Our work highlights that the gas-phase production of glyoxal represents a large uncertainty in quantifying its contribution to SOA. C1 [Li, Jingyi; Mao, Jingqiu; Paulot, Fabien] Princeton Univ, Program Atmospher & Ocean Sci, Princeton, NJ 08544 USA. [Mao, Jingqiu; Donner, Leo J.; Paulot, Fabien; Horowitz, Larry W.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08540 USA. [Min, Kyung-Eun; Washenfelder, Rebecca A.; Brown, Steven S.; Pollack, Ilana B.; Ryerson, Thomas B.; Graus, Martin; Gilman, Jessica B.; Lerner, Brian M.; Warneke, Carsten; de Gouw, Joost A.; Middlebrook, Ann M.; Liao, Jin; Welti, Andre] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO USA. [Min, Kyung-Eun; Washenfelder, Rebecca A.; Volkamer, Rainer; Pollack, Ilana B.; Graus, Martin; Gilman, Jessica B.; Lerner, Brian M.; Warneke, Carsten; de Gouw, Joost A.; Liao, Jin; Welti, Andre] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Min, Kyung-Eun] Gwangju Inst Sci & Technol, Sch Environm Sci & Engn, Gwangju, South Korea. [Brown, Steven S.; Volkamer, Rainer] Univ Colorado, Dept Chem & Biochem, Campus Box 215, Boulder, CO 80309 USA. [Kaiser, Jennifer; Keutsch, Frank N.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Keutsch, Frank N.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. [Wolfe, Glenn M.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. [Wolfe, Glenn M.; Hanisco, Thomas F.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD USA. [Pollack, Ilana B.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Graus, Martin] Univ Innsbruck, Inst Atmospher & Cryospher Sci, Innsbruck, Austria. [Welti, Andre] Leibniz Inst Tropospher Res, Leipzig, Germany. [Henderson, Barron H.] Univ Florida, Dept Environm Engn Sci, Engn Sch Sustainable Infrastruct & Environm, Gainesville, FL 32611 USA. [McNeill, V. Faye] Columbia Univ, Dept Chem Engn, New York, NY USA. [Hall, Samuel R.; Ullmann, Kirk] Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA. RP Mao, JQ (reprint author), Princeton Univ, Program Atmospher & Ocean Sci, Princeton, NJ 08544 USA.; Mao, JQ (reprint author), NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08540 USA. EM Jingqiu.Mao@noaa.gov RI Volkamer, Rainer/B-8925-2016; Graus, Martin/E-7546-2010; Mao, Jingqiu/F-2511-2010; de Gouw, Joost/A-9675-2008; Gilman, Jessica/E-7751-2010; Pollack, Ilana/F-9875-2012; Washenfelder, Rebecca/E-7169-2010; Middlebrook, Ann/E-4831-2011; Wolfe, Glenn/D-5289-2011; Brown, Steven/I-1762-2013; Manager, CSD Publications/B-2789-2015 OI Volkamer, Rainer/0000-0002-0899-1369; Graus, Martin/0000-0002-2025-9242; Mao, Jingqiu/0000-0002-4774-9751; de Gouw, Joost/0000-0002-0385-1826; Gilman, Jessica/0000-0002-7899-9948; Washenfelder, Rebecca/0000-0002-8106-3702; Middlebrook, Ann/0000-0002-2984-6304; FU NOAA Climate Program Office [NA13OAR4310071, NA14OAR4320106]; NOAA Atmospheric Chemistry, Climate, and Carbon Cycle (AC4) program; EPA [83540601]; NASA [NNH10ZDA001N-SEAC4RS]; NASA Headquarters under the NASA Earth and Space Science Fellowship Program [NNX14AK97H]; NSF EAGER [AGS-1452317]; NSF [AGS-1546136] FX The authors thank Charles A. Brock (NOAA) for providing the aerosol size data, Vaishali Naik (UCAR/NOAA) for providing the emission inventories from the SENEX campaign, and William Cooke for the help with convection scheme of the AM3 model. J.L., J.M., and L.W.H. acknowledge supports by the NOAA Climate Program Office grant NA13OAR4310071 and NA14OAR4320106. K.E.M., R.A.W., and S.S.B. acknowledge the support from the NOAA Atmospheric Chemistry, Climate, and Carbon Cycle (AC4) program. J.K., F.N.K., G.M.W., and T.F.H. are grateful for the support from EPA Science to Achieve Results program grant 83540601 and NASA grant NNH10ZDA001N-SEAC4RS. J. Kaiser acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program grant NNX14AK97H. R.V. is grateful for the support from NSF EAGER award AGS-1452317. V.F.M. acknowledges support from NSF (AGS-1546136). We thank the staff at the NOAA Aircraft Operations Center and the WP-3D flight crew for their help in instrumenting the aircraft and for conducting the flights. Special thanks go to Songmiao Fan (NOAA) for the helpful discussions. This research has not been subjected to any EPA review and therefore does not necessarily reflect the views of the agency, and no official endorsement should be inferred. Observational data sets and modeling results are available upon request to the corresponding author (Jingqiu.Mao@noaa.gov). NR 92 TC 0 Z9 0 U1 19 U2 19 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 AUG 27 PY 2016 VL 121 IS 16 BP 9849 EP 9861 DI 10.1002/2016JD025331 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DZ9OQ UT WOS:000386207200032 ER PT J AU Ware, J Kort, EA DeCola, P Duren, R AF Ware, John Kort, Eric A. DeCola, Phil Duren, Riley TI Aerosol lidar observations of atmospheric mixing in Los Angeles: Climatology and implications for greenhouse gas observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID BOUNDARY-LAYER HEIGHT; AIR-POLLUTANT TRANSPORT; FIELD-OF-VIEW; CO2 EMISSIONS; COASTAL ENVIRONMENT; SIMULATIONS; BACKSCATTER; DEPENDENCE; SYSTEM; DEPTH AB Atmospheric observations of greenhouse gases provide essential information on sources and sinks of these key atmospheric constituents. To quantify fluxes from atmospheric observations, representation of transport-especially vertical mixing-is a necessity and often a source of error. We report on remotely sensed profiles of vertical aerosol distribution taken over a 2 year period in Pasadena, California. Using an automated analysis system, we estimate daytime mixing layer depth, achieving high confidence in the afternoon maximum on 51% of days with profiles from a Sigma Space Mini Micropulse LiDAR (MiniMPL) and on 36% of days with a Vaisala CL51 ceilometer. We note that considering ceilometer data on a logarithmic scale, a standard method, introduces, an offset in mixing height retrievals. The mean afternoon maximum mixing height is 770 m Above Ground Level in summer and 670 m in winter, with significant day-to-day variance (within season sigma = 220 m approximate to 30%). Taking advantage of the MiniMPL's portability, we demonstrate the feasibility of measuring the detailed horizontal structure of the mixing layer by automobile. We compare our observations to planetary boundary layer (PBL) heights from sonde launches, North American regional reanalysis (NARR), and a custom Weather Research and Forecasting (WRF) model developed for greenhouse gas (GHG) monitoring in Los Angeles. NARR and WRF PBL heights at Pasadena are both systematically higher than measured, NARR by 2.5 times; these biases will cause proportional errors in GHG flux estimates using modeled transport. We discuss how sustained lidar observations can be used to reduce flux inversion error by selecting suitable analysis periods, calibrating models, or characterizing bias for correction in post processing. C1 [Ware, John] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Ware, John; Kort, Eric A.] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA. [DeCola, Phil] Sigma Space Corp, Lanham, MD USA. [Duren, Riley] NASA, Jet Prop Lab, Pasadena, CA USA. RP Ware, J (reprint author), Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.; Ware, J (reprint author), Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA. EM johnware@umich.edu RI Kort, Eric/F-9942-2012 OI Kort, Eric/0000-0003-4940-7541 FU NASA [NNN12AA01C]; NASA FX This work was supported by NASA under grant NNN12AA01C. Portions of this work were performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. We thank Taylor Jones for assistance in setting up and operating the MiniMPL instrument and Athena Sparks for help with data preprocessing. We thank Vineet Yadav for generating and providing WRF model output. NARR data provided by the NOAA/OAR/ESRL PSD, Boulder, Colorado, USA, from their Web site at http://www.esrl.noaa.gov/psd/. The authors would also like to thank the Megacities Carbon Project team for useful discussion and feedback. Mixing depth data will be available through the Megacities Carbon Project portal at https://megacities.jpl.nasa.gov. To obtain a copy of the analysis system used to generate the estimates, please contact the authors at johnware@umich.edu. NR 50 TC 0 Z9 0 U1 6 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 27 PY 2016 VL 121 IS 16 BP 9862 EP 9878 DI 10.1002/2016JD024953 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DZ9OQ UT WOS:000386207200033 PM 27867786 ER PT J AU Mezuman, K Bauer, SE Tsigaridis, K AF Mezuman, Keren Bauer, Susanne E. Tsigaridis, Kostas TI Evaluating secondary inorganic aerosols in three dimensions SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID GENERAL-CIRCULATION MODEL; AQUEOUS-PHASE-TRANSITIONS; TROPOSPHERIC OZONE; GODDARD-INSTITUTE; ATMOSPHERIC AEROSOLS; AMMONIUM-NITRATE; UNITED-STATES; GLOBAL-MODEL; MINERAL DUST; EMISSIONS AB The spatial distribution of aerosols and their chemical composition dictates whether aerosols have a cooling or a warming effect on the climate system. Hence, properly modeling the three-dimensional distribution of aerosols is a crucial step for coherent climate simulations. Since surface measurement networks only give 2-D data, and most satellites supply integrated column information, it is thus important to integrate aircraft measurements in climate model evaluations. In this study, the vertical distribution of secondary inorganic aerosol (i.e., sulfate, ammonium, and nitrate) is evaluated against a collection of 14 AMS flight campaigns and surface measurements from 2000 to 2010 in the USA and Europe. GISS ModelE2 is used with multiple aerosol microphysics (MATRIX, OMA) and thermodynamic (ISOR-ROPIA II, EQSAM) configurations. Our results show that the MATRIX microphysical scheme improves the model performance for sulfate, but that there is a systematic underestimation of ammonium and nitrate over the USA and Europe in all model configurations. In terms of gaseous precursors, nitric acid concentrations are largely underestimated at the surface while overestimated in the higher levels of the model. Heterogeneous reactions on dust surfaces are an important sink for nitric acid, even high in the troposphere. At high altitudes, nitrate formation is calculated to be ammonia limited. The underestimation of ammonium and nitrate in polluted regions is most likely caused by a too simplified treatment of the NH3 / NH4+ partitioning which affects the HNO3 / NO3- partitioning. C1 [Mezuman, Keren] Columbia Univ, Earth & Environm Sci, New York, NY USA. [Mezuman, Keren; Bauer, Susanne E.; Tsigaridis, Kostas] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Bauer, Susanne E.; Tsigaridis, Kostas] Columbia Univ, Ctr Climate Syst Res, New York, NY 10027 USA. RP Bauer, SE (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.; Bauer, SE (reprint author), Columbia Univ, Ctr Climate Syst Res, New York, NY 10027 USA. EM susanne.bauer@columbia.edu FU NASA; NASA High-End Computing (HEC) Program through NASA Center for Climate Simulation (NCCS) at Goddard Space Flight Center; NASA's Atmospheric Composition Modeling and Analysis Program (ACMAP) [NNX15AE36G] FX Climate modeling at GISS is supported by the NASA Modeling, Analysis, and Prediction program. 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. SEB and KT acknowledge funding from NASA's Atmospheric Composition Modeling and Analysis Program (ACMAP), contract number NNX15AE36G. We acknowledge the IMPROVE monitoring program for providing data. EMEP measurement data were extracted from the EBAS database, which is maintained and further developed by the Norwegian Institute for Air Research (NILU). We acknowledge the Toolsets for Airborne Data (TAD) website:https://tad.larc.nasa.gov, as well as the site https://sites.google.com/site/amsglobaldatabase/ maintained by the Zhang and Jimenez groups. NR 70 TC 1 Z9 1 U1 15 U2 15 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD AUG 26 PY 2016 VL 16 IS 16 BP 10651 EP 10669 DI 10.5194/acp-16-10651-2016 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DW6EW UT WOS:000383743200002 ER PT J AU Adams, C Normand, EN McLinden, CA Bourassa, AE Lloyd, ND Degenstein, DA Krotkov, NA Rivas, MB Boersma, KF Eskes, H AF Adams, Cristen Normand, Elise N. McLinden, Chris A. Bourassa, Adam E. Lloyd, Nicholas D. Degenstein, Douglas A. Krotkov, Nickolay A. Rivas, Maria Belmonte Boersma, K. Folkert Eskes, Henk TI Limb-nadir matching using non-coincident NO2 observations: proof of concept and the OMI-minus-OSIRIS prototype product SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID OZONE MONITORING INSTRUMENT; TROPOSPHERIC NO2; NITROGEN-DIOXIDE; STRATOSPHERIC OZONE; RETRIEVAL ALGORITHM; MIDDLE ATMOSPHERE; COLUMN RETRIEVAL; SCIAMACHY; SATELLITE; MISSION AB A variant of the limb-nadir matching technique for deriving tropospheric NO2 columns is presented in which the stratospheric component of the NO2 slant column density (SCD) measured by the Ozone Monitoring Instrument (OMI) is removed using non-coincident profiles from the Optical Spectrograph and InfraRed Imaging System (OSIRIS). In order to correct their mismatch in local time and the diurnal variation of stratospheric NO2 OSIRIS profiles, which were measured just after sunrise, were mapped to the local time of OMI observations using a photochemical box model. Following the profile time adjustment, OSIRIS NO2 stratospheric vertical column densities (VCDs) were calculated. For profiles that did not reach down to the tropopause, VCDs were adjusted using the photochemical model. Using air mass factors from the OMI Standard Product (SP), a new tropospheric NO2 VCD product -referred to as OMI-minus-OSIRIS (OmO) - was generated through limb-nadir matching. To accomplish this, the OMI total SCDs were scaled using correction factors derived from the next-generation SCDs that improve upon the spectral fitting used for the current operational products. One year, 2008, of OmO was generated for 60 degrees S to 60 degrees N and a cursory evaluation was performed. The OmO product was found to capture the main features of tropospheric NO2, including a background value of about 0.3 x 10(15) molecules cm(-2) over the tropical Pacific and values comparable to the OMI operational products over anthropogenic source areas. While additional study is required, these results suggest that a limb-nadir matching approach is feasible for the removal of stratospheric NO2 measured by a polar orbiter from a nadir-viewing instrument in a geostationary orbit such as Tropospheric Emissions: Monitoring of Pollution (TEMPO) or Sentinel-4. C1 [Adams, Cristen; Normand, Elise N.; Bourassa, Adam E.; Lloyd, Nicholas D.; Degenstein, Douglas A.] Univ Saskatchewan, Inst Space & Atmospher Studies, Saskatoon, SK, Canada. [Adams, Cristen] Alberta Environm & Pk, Alberta Environm Monitoring & Sci Div, Edmonton, AB, Canada. [McLinden, Chris A.] Environm Canada, Air Qual Res Div, Toronto, ON, Canada. [Krotkov, Nickolay A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Rivas, Maria Belmonte; Boersma, K. Folkert; Eskes, Henk] Royal Netherlands Meteorol Inst KNMI, De Bilt, Netherlands. [Boersma, K. Folkert] Wageningen Univ, Meteorol & Air Qual Grp, Wageningen, Netherlands. RP Adams, C (reprint author), Univ Saskatchewan, Inst Space & Atmospher Studies, Saskatoon, SK, Canada.; Adams, C (reprint author), Alberta Environm & Pk, Alberta Environm Monitoring & Sci Div, Edmonton, AB, Canada. EM cristenlfadams@gmail.com RI Boersma, Klaas/H-4559-2012 OI Boersma, Klaas/0000-0002-4591-7635 FU Natural Sciences and Engineering Research Council (Canada); Canadian Space Agency; Sweden (SNSB); Canada (CSA); France (CNES); Finland (Tekes) FX This work was supported by the Natural Sciences and Engineering Research Council (Canada) and the Canadian Space Agency. Odin is a Swedish-led satellite project funded jointly by Sweden (SNSB), Canada (CSA), France (CNES), and Finland (Tekes). The authors thank David Plummer for the provision of climatological fields from the Canadian Middle Atmosphere Model. Thanks to Sergey Marchenko for providing the OMI SCD bias correction factors. Thank you also to Chris Roth for help with the OSIRIS database. NR 56 TC 1 Z9 1 U1 3 U2 3 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 EI 1867-8548 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PD AUG 26 PY 2016 VL 9 IS 8 BP 4103 EP 4122 DI 10.5194/amt-9-4103-2016 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DW7PH UT WOS:000383842900001 ER PT J AU Aguilar, M Alpat, B Alpat, B Ambrosi, G Arruda, L Attig, N Aupetit, S Azzarello, P Bachlechner, A Barao, F Barrau, A Barrin, L Bartoloni, A Basara, L Basegmez-du Pree, S Battarbee, M Battiston, R Bazo, J Becker, U Behlmann, M Beischer, B Berdugo, J Bertucci, B Bindi, V Boella, G de Boer, W Bollweg, K Bonnivard, V Borgia, B Boschini, MJ Bourquin, M Bueno, EF Burger, J Cadoux, F Cai, XD Capell, M Caroff, S Casaus, J Castellini, G Cernuda, I Cervelli, F Chae, MJ Chang, YH Chen, AI Chen, GM Chen, HS Cheng, L Chou, HY Choumilov, E Choutko, V Chung, CH Clark, C Clavero, R Coignet, G Consolandi, C Contin, A Corti, C Coste, B Creus, W Crispoltoni, M Cui, Z Dai, YM Delgado, C Della Torre, S Demirkoz, MB Derome, L Di Falco, S Dimiccoli, F Diaz, C von Doetinchem, P Dong, F Donnini, F Duranti, M D'Urso, D Egorov, A Eline, A Eronen, T Feng, J Fiandrini, E Finch, E Fisher, P Formato, V Galaktionov, Y Gallucci, G Garcia, B Garcia-Lopez, RJ Gargiulo, C Gast, H Gebauer, I Gervasi, M Ghelfi, A Giovacchini, F Goglov, P Gomez-Coral, DM Gong, J Goy, C Grabski, V Grandi, D Graziani, M Guerri, I Guo, KH Habiby, M Haino, S Han, KC He, ZH Heil, M Hoffman, J Hsieh, TH Huang, H Huang, ZC Huh, C Incagli, M Ionica, M Jang, WY Jinchi, H Kang, SC Kanishev, K Kim, GN Kim, KS Kirn, T Konak, C Kounina, O Kounine, A Koutsenko, V Krafczyk, MS La Vacca, G Laudi, E Laurenti, G Lazzizzera, I Lebedev, A Lee, HT Lee, SC Leluc, C Li, HS Li, JQ Li, JQ Li, Q Li, TX Li, W Li, ZH Li, ZY Lim, S Lin, CH Lipari, P Lippert, T Liu, D Liu, H Lu, SQ Lu, YS Luebelsmeyer, K Luo, F Luo, JZ Lv, SS Majka, R Mana, C Marin, J Martin, T Martinez, G Masi, N Maurin, D Menchaca-Rocha, A Meng, Q Mo, DC Morescalchi, L Mott, P Nelson, T Ni, JQ Nikonov, N Nozzoli, F Nunes, P Oliva, A Orcinha, M Palmonari, F Palomares, C Paniccia, M Pauluzzi, M Pensotti, S Pereira, R Picot-Clemente, N Pilo, F Pizzolotto, C Plyaskin, V Pohl, M Poireau, V Putze, A Quadrani, L Qi, XM Qin, X Qu, ZY Raiha, T Rancoita, PG Rapin, D Ricol, JS Rodriguez, I Rosier-Lees, S Rozhkov, A Rozza, D Sagdeev, R Sandweiss, J Saouter, P Schael, S Schmidt, SM von Dratzig, AS Schwering, G Seo, ES Shan, BS Shi, JY Siedenburg, T Son, D Song, JW Sun, WH Tacconi, M Tang, XW Tang, ZC Tao, L Tescaro, D Ting, SCC Ting, SM Tomassetti, N Torsti, J Turkoglu, C Urban, T Vagelli, V Valente, E Vannini, C Valtonen, E Acosta, MV Vecchi, M Velasco, M Vialle, JP Vitale, V Vitillo, S Wang, LQ Wang, NH Wang, QL Wang, X Wang, XQ Wang, ZX Wei, CC Weng, ZL Whitman, K Wienkenhover, J Willenbrock, M Wu, H Wu, X Xia, X Xiong, RQ Xu, W Yan, Q Yang, J Yang, M Yang, Y Yi, H Yu, YJ Yu, ZQ Zeissler, S Zhang, C Zhang, J Zhang, JH Zhang, SD Zhang, SW Zhang, Z Zheng, ZM Zhu, ZQ Zhuang, HL Zhukov, V Zichichi, A Zimmermann, N Zuccon, P AF Aguilar, M. Alpat, B. Alpat, B. Ambrosi, G. Arruda, L. Attig, N. Aupetit, S. Azzarello, P. Bachlechner, A. Barao, F. Barrau, A. Barrin, L. Bartoloni, A. Basara, L. Basegmez-du Pree, S. Battarbee, M. Battiston, R. Bazo, J. Becker, U. Behlmann, M. Beischer, B. Berdugo, J. Bertucci, B. Bindi, V. Boella, G. de Boer, W. Bollweg, K. Bonnivard, V. Borgia, B. Boschini, M. J. Bourquin, M. Bueno, E. F. Burger, J. Cadoux, F. Cai, X. D. Capell, M. Caroff, S. Casaus, J. Castellini, G. Cernuda, I. Cervelli, F. Chae, M. J. Chang, Y. H. Chen, A. I. Chen, G. M. Chen, H. S. Cheng, L. Chou, H. Y. Choumilov, E. Choutko, V. Chung, C. H. Clark, C. Clavero, R. Coignet, G. Consolandi, C. Contin, A. Corti, C. Coste, B. Creus, W. Crispoltoni, M. Cui, Z. Dai, Y. M. Delgado, C. Della Torre, S. Demirkoz, M. B. Derome, L. Di Falco, S. Dimiccoli, F. Diaz, C. von Doetinchem, P. Dong, F. Donnini, F. Duranti, M. D'Urso, D. Egorov, A. Eline, A. Eronen, T. Feng, J. Fiandrini, E. Finch, E. Fisher, P. Formato, V. Galaktionov, Y. Gallucci, G. Garcia, B. Garcia-Lopez, R. J. Gargiulo, C. Gast, H. Gebauer, I. Gervasi, M. Ghelfi, A. Giovacchini, F. Goglov, P. Gomez-Coral, D. M. Gong, J. Goy, C. Grabski, V. Grandi, D. Graziani, M. Guerri, I. Guo, K. H. Habiby, M. Haino, S. Han, K. C. He, Z. H. Heil, M. Hoffman, J. Hsieh, T. H. Huang, H. Huang, Z. C. Huh, C. Incagli, M. Ionica, M. Jang, W. Y. Jinchi, H. Kang, S. C. Kanishev, K. Kim, G. N. Kim, K. S. Kirn, Th. Konak, C. Kounina, O. Kounine, A. Koutsenko, V. Krafczyk, M. S. La Vacca, G. Laudi, E. Laurenti, G. Lazzizzera, I. Lebedev, A. Lee, H. T. Lee, S. C. Leluc, C. Li, H. S. Li, J. Q. Li, J. Q. Li, Q. Li, T. X. Li, W. Li, Z. H. Li, Z. Y. Lim, S. Lin, C. H. Lipari, P. Lippert, T. Liu, D. Liu, Hu Lu, S. Q. Lu, Y. S. Luebelsmeyer, K. Luo, F. Luo, J. Z. Lv, S. S. Majka, R. Mana, C. Marin, J. Martin, T. Martinez, G. Masi, N. Maurin, D. Menchaca-Rocha, A. Meng, Q. Mo, D. C. Morescalchi, L. Mott, P. Nelson, T. Ni, J. Q. Nikonov, N. Nozzoli, F. Nunes, P. Oliva, A. Orcinha, M. Palmonari, F. Palomares, C. Paniccia, M. Pauluzzi, M. Pensotti, S. Pereira, R. Picot-Clemente, N. Pilo, F. Pizzolotto, C. Plyaskin, V. Pohl, M. Poireau, V. Putze, A. Quadrani, L. Qi, X. M. Qin, X. Qu, Z. Y. Raiha, T. Rancoita, P. G. Rapin, D. Ricol, J. S. Rodriguez, I. Rosier-Lees, S. Rozhkov, A. Rozza, D. Sagdeev, R. Sandweiss, J. Saouter, P. Schael, S. Schmidt, S. M. von Dratzig, A. Schulz Schwering, G. Seo, E. S. Shan, B. S. Shi, J. Y. Siedenburg, T. Son, D. Song, J. W. Sun, W. H. Tacconi, M. Tang, X. W. Tang, Z. C. Tao, L. Tescaro, D. Ting, Samuel C. C. Ting, S. M. Tomassetti, N. Torsti, J. Turkoglu, C. Urban, T. Vagelli, V. Valente, E. Vannini, C. Valtonen, E. Acosta, M. Vazquez Vecchi, M. Velasco, M. Vialle, J. P. Vitale, V. Vitillo, S. Wang, L. Q. Wang, N. H. Wang, Q. L. Wang, X. Wang, X. Q. Wang, Z. X. Wei, C. C. Weng, Z. L. Whitman, K. Wienkenhover, J. Willenbrock, M. Wu, H. Wu, X. Xia, X. Xiong, R. Q. Xu, W. Yan, Q. Yang, J. Yang, M. Yang, Y. Yi, H. Yu, Y. J. Yu, Z. Q. Zeissler, S. Zhang, C. Zhang, J. Zhang, J. H. Zhang, S. D. Zhang, S. W. Zhang, Z. Zheng, Z. M. Zhu, Z. Q. Zhuang, H. L. Zhukov, V. Zichichi, A. Zimmermann, N. Zuccon, P. CA AMS Collaboration TI Antiproton Flux, Antiproton-to-Proton Flux Ratio, and Properties of Elementary Particle Fluxes in Primary Cosmic Rays Measured with the Alpha Magnetic Spectrometer on the International Space Station SO PHYSICAL REVIEW LETTERS LA English DT Article ID ABSORPTION CROSS-SECTIONS; GEOMAGNETIC REFERENCE FIELD; DARK-MATTER; RICH DETECTOR; ANTI-PROTONS; AMS-02 TRD; GEV-C; POSITRONS; NUCLEI; CARBON AB A precision measurement by AMS of the antiproton flux and the antiproton-to-proton flux ratio in primary cosmic rays in the absolute rigidity range from 1 to 450 GV is presented based on 3.49 x 10(5) antiproton events and 2.42 x 10(9) proton events. The fluxes and flux ratios of charged elementary particles in cosmic rays are also presented. In the absolute rigidity range similar to 60 to similar to 500 GV, the antiproton (p) over bar, proton p, and positron e(+) fluxes are found to have nearly identical rigidity dependence and the electron e(-) flux exhibits a different rigidity dependence. Below 60 GV, the ((p) over bar /p), ((p) over bar /e(+)), and (p/e(+)) flux ratios each reaches a maximum. From similar to 60 to similar to 500 GV, the ((p) over bar /p), ((p) over bar /e(+)), and (p/e(+)) flux ratios show no rigidity dependence. These are new observations of the properties of elementary particles in the cosmos. C1 [Bachlechner, A.; Beischer, B.; Chung, C. H.; Gast, H.; Kirn, Th.; Luebelsmeyer, K.; Nikonov, N.; Raiha, T.; Schael, S.; von Dratzig, A. Schulz; Schwering, G.; Siedenburg, T.; Wienkenhover, J.; Zhukov, V.; Zimmermann, N.] Rhein Westfal TH Aachen, Inst Phys 1, D-52056 Aachen, Germany. [Bachlechner, A.; Beischer, B.; Chung, C. H.; Gast, H.; Kirn, Th.; Luebelsmeyer, K.; Nikonov, N.; Raiha, T.; Schael, S.; von Dratzig, A. Schulz; Schwering, G.; Siedenburg, T.; Wienkenhover, J.; Zhukov, V.; Zimmermann, N.] Rhein Westfal TH Aachen, JARA FAME, D-52056 Aachen, Germany. [Demirkoz, M. B.; Konak, C.; Turkoglu, C.] Middle E Tech Univ, Dept Phys, TR-06800 Ankara, Turkey. [Caroff, S.; Coignet, G.; Goy, C.; Poireau, V.; Putze, A.; Rosier-Lees, S.; Tao, L.; Vialle, J. P.] CNRS IN2P3, Lab Annecy Le Vieux Phys Particules LAPP, F-74941 Annecy Le Vieux, France. [Li, W.; Shan, B. S.; Zheng, Z. M.] Beihang Univ BUAA, Beijing 100191, Peoples R China. [Dai, Y. M.; Wang, Q. L.; Yu, Y. J.] Chinese Acad Sci, Inst Elect Engn IEE, Beijing 100190, Peoples R China. [Bachlechner, A.; Basegmez-du Pree, S.; Chen, G. M.; Chen, H. S.; Li, Z. H.; Lu, Y. S.; Tang, X. W.; Tang, Z. C.; Wang, X. Q.; Yang, M.; Yu, Z. Q.; Zhang, C.; Zhang, S. W.; Zhuang, H. L.] Chinese Acad Sci, Inst High Energy Phys IHEP, Beijing 100049, Peoples R China. 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[Bindi, V.; Consolandi, C.; Corti, C.; von Doetinchem, P.; Hoffman, J.; Nelson, T.; Pereira, R.; Whitman, K.] Univ Hawaii, Dept Phys & Astron, Honolulu, HI 96822 USA. [Bollweg, K.; Clark, C.; Martin, T.; Mott, P.; Urban, T.] NASA, Johnson Space Ctr JSC, Jacobs Engn & Business Integra, Houston, TX 77058 USA. [Attig, N.; Lippert, T.; Schmidt, S. M.] Julich Supercomp Ctr, D-52425 Julich, Germany. [Attig, N.; Lippert, T.; Schmidt, S. M.] Res Ctr Julich, JARA FAME, D-52425 Julich, Germany. [de Boer, W.; Gebauer, I.; Zeissler, S.] KIT, Inst Expt Kernphys, D-76128 Karlsruhe, Germany. [Clavero, R.; Garcia-Lopez, R. J.; Tescaro, D.; Acosta, M. Vazquez] IAC, E-38205 San Cristobal la Laguna, Spain. [Clavero, R.; Garcia-Lopez, R. J.; Tescaro, D.; Acosta, M. Vazquez] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Arruda, L.; Barao, F.; Nunes, P.; Orcinha, M.] Lab Instrumentacao & Fis Expt Particulas LIP, P-1000 Lisbon, Portugal. [Han, K. 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[Alpat, B.; Ambrosi, G.; Bazo, J.; Bertucci, B.; Crispoltoni, M.; Donnini, F.; Duranti, M.; D'Urso, D.; Fiandrini, E.; Formato, V.; Graziani, M.; Ionica, M.; Nozzoli, F.; Pauluzzi, M.; Pizzolotto, C.; Qin, X.; Vagelli, V.; Vitale, V.] Ist Nazl Fis Nucl, Sez Perugia, I-06100 Perugia, Italy. [Bertucci, B.; Crispoltoni, M.; Donnini, F.; Duranti, M.; Fiandrini, E.; Graziani, M.; Pauluzzi, M.] Univ Perugia, I-06100 Perugia, Italy. [Cervelli, F.; Di Falco, S.; Gallucci, G.; Guerri, I.; Incagli, M.; Morescalchi, L.; Pilo, F.; Vannini, C.] Ist Nazl Fis Nucl, Sez Pisa, I-56100 Pisa, Italy. [Guerri, I.] Univ Pisa, I-56100 Pisa, Italy. [Basara, L.; Battiston, R.; Coste, B.; Dimiccoli, F.; Kanishev, K.; Lazzizzera, I.] Ist Nazl Fis Nucl, TIFPA, I-38123 Povo, Trento, Italy. [Battiston, R.; Dimiccoli, F.; Kanishev, K.; Lazzizzera, I.] Univ Trento, I-38123 Povo, Trento, Italy. [Bartoloni, A.; Borgia, B.; Lipari, P.; Valente, E.] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy. [Borgia, B.; Valente, E.] Univ Roma La Sapienza, I-00185 Rome, Italy. [Bueno, E. F.; Vecchi, M.] Univ Sao Paulo, Inst Fis Sao Carlos, CP 369, BR-13560970 Sao Carlos, SP, Brazil. [Chae, M. J.; Yang, J.] Ewha Womans Univ, Dept Phys, Seoul 120750, South Korea. [Cheng, L.; Cui, Z.; Luo, F.; Song, J. W.; Wang, L. Q.; Wang, N. H.] Shandong Univ SDU, Jinan 250100, Shandong, Peoples R China. [Li, H. S.; Yang, Y.] Natl Cheng Kung Univ, Tainan 70101, Taiwan. [Lee, H. T.] Acad Sinica Grid Ctr ASGC, Taipei 11529, Taiwan. [Feng, J.; Haino, S.; Huang, H.; Lee, S. C.; Li, Z. Y.; Lin, C. H.; Liu, D.; Lu, S. Q.; Qu, Z. Y.; Wei, C. C.] Acad Sinica, Inst Phys, Taipei 11529, Taiwan. [Battarbee, M.; Eronen, T.; Torsti, J.; Valtonen, E.] Univ Turku, Dept Phys & Astron, Space Res Lab, FI-20014 Turku, Finland. ASI, I-00133 Rome, Italy. [Bazo, J.] PUCP, Dept Ciencias, Lima 32, Peru. [Bachlechner, A.; D'Urso, D.; Nozzoli, F.; Pizzolotto, C.; Vitale, V.] ASDC, I-00133 Rome, Italy. [Feng, J.; Li, Z. Y.; Lu, S. Q.] Sun Yat Sen Univ, Guangzhou 510275, Guangdong, Peoples R China. [Huang, H.; Zhang, J.] Wuhan Univ, Wuhan 430072, Peoples R China. [Li, J. Q.; Zhang, S. D.] Harbin Inst Technol HIT, Harbin 150001, Peoples R China. [Liu, Hu] Huazhong Univ Sci & Technol HUST, Wuhan 430074, Peoples R China. [Morescalchi, L.] Univ Siena, I-53100 Siena, Italy. [Putze, A.] CNRS, Lab Annecy le Vieux Phys Theor LAPTh, F-74941 Annecy Le Vieux, France. [Putze, A.] Univ Savoie Mt Blanc, F-74941 Annecy Le Vieux, France. [Qin, X.; Xia, X.] Shandong Univ SDU, Jinan 250100, Shandong, Peoples R China. [Qu, Z. Y.] Nankai Univ, Tianjin 300071, Peoples R China. [Sun, W. H.] Southeast Univ SEU, Nanjing 210096, Jiangsu, Peoples R China. [Wei, C. C.] Chinese Acad Sci, Inst Theoretial Phys, Beijing 100190, Peoples R China. [Zhu, Z. Q.] Jilin Univ, Jilin 130012, Peoples R China. RI Vecchi, Manuela/J-9180-2014; Sao Carlos Institute of Physics, IFSC/USP/M-2664-2016; Paniccia, Mercedes/A-4519-2017; Delgado, Carlos/K-7587-2014; OI Paniccia, Mercedes/0000-0001-8482-2703; Delgado, Carlos/0000-0002-7014-4101; Corti, Claudio/0000-0001-9127-7133; Morescalchi, Luca/0000-0002-7819-8139; Bertucci, Bruna/0000-0001-7584-293X; La Vacca, Giuseppe/0000-0002-2168-9447; Della Torre, Stefano/0000-0002-7669-0859 FU Sao Paulo Research Foundation (FAPESP), Brazil [2014/19149-7, 2014/50747-8, 2015-50378-5]; CAS, China; NSFC, China; MOST, China; NLAA, China; provincial government of Shandong, China; provincial government of Jiangsu, China; provincial government of Guangdong, China; China Scholarship Council, China; Finnish Funding Agency for Innovation (Tekes), Finland [40361/01, 40518/03]; Academy of Finland, Finland [258963]; CNRS, France; IN2P3, France; CNES, France; Enigmass, France; ANR, France; Pascale Ehrenfreund, Germany; DLR, Germany; JARA-HPC, Germany [JARA0052]; INFN, Italy [2013-002-R.0, 2014-037-R.0]; ASI, Italy [2013-002-R.0, 2014-037-R.0]; CHEP Grants at Kyungpook National University, Korea [NRF-2009-0080142, NRF-2012-010226]; CHEP Grants at Ewha Womans University, Korea [NRF-2013-004883]; Consejo Nacional de Ciencia y Tecnologia, Mexico; UNAM, Mexico; FCT, Portugal [PTDC/FIS/122567/2010]; CIEMAT, Spain; IAC, Spain; CDTI, Spain; SEIDI-MINECO, Spain [AYA2012-39526-C02-(01/02), ESP2015-71662-C2-(1-P/2-P), SEV-2011-0187, SEV-2015-0548, MDM-2015-0509]; Swiss National Science Foundation (SNSF), federal and cantonal authorities, Switzerland; Academia Sinica, Taiwan; Ministry of Science and Technology (MOST), Taiwan [103-2112-M-006-018-MY3, 104-2112-M-001-027, CDA-105-M06]; Turkish Atomic Energy Authority at METU, Turkey; NSF Grant, USA [1455202]; Wyle Laboratories Grant, USA [2014/T72497]; NASA NESSF Grant, USA [HELIO15F-0005] FX We thank former NASA Administrator Daniel S. Goldin for his dedication to the legacy of the ISS as a scientific laboratory and his decision for NASA to fly AMS as a DOE payload. We also acknowledge the continuous support of the NASA leadership including Charles Bolden and William H. Gerstenmaier and of the JSC and MSFC flight control teams which has allowed AMS to operate optimally on the ISS for five years. We are grateful for the support of Jim Siegrist and his staff of the DOE. We also acknowledge the continuous support from MIT and its School of Science, Michael Sipser, Marc Kastner, Ernest Moniz, Richard Milner, and Boleslaw Wyslouch. Research supported by Sao Paulo Research Foundation (FAPESP) Grants No. 2014/19149-7, No. 2014/50747-8, and No. 2015-50378-5, Brazil; CAS, NSFC, MOST, NLAA, the provincial governments of Shandong, Jiangsu, Guangdong, and the China Scholarship Council, China; the Finnish Funding Agency for Innovation (Tekes) Grants No. 40361/01 and No. 40518/03 and the Academy of Finland Grant No. 258963, Finland; CNRS, IN2P3, CNES, Enigmass, and the ANR, France; Pascale Ehrenfreund, DLR, and JARA-HPC under Project No. JARA0052, Germany; INFN and ASI under ASI-INFN Agreements No. 2013-002-R.0 and No. 2014-037-R.0, Italy; CHEP Grants No. NRF-2009-0080142 and No. NRF-2012-010226 at Kyungpook National University and No. NRF-2013-004883 at Ewha Womans University, Korea; the Consejo Nacional de Ciencia y Tecnologia and UNAM, Mexico; FCT under Grant No. PTDC/FIS/122567/2010, Portugal; CIEMAT, IAC, CDTI, and SEIDI-MINECO under Grants No. AYA2012-39526-C02-(01/02), No. ESP2015-71662-C2-(1-P/2-P), No. SEV-2011-0187, No. SEV-2015-0548, and No. MDM-2015-0509, Spain; the Swiss National Science Foundation (SNSF), federal and cantonal authorities, Switzerland; Academia Sinica and the Ministry of Science and Technology (MOST) under Grants No. 103-2112-M-006-018-MY3, No. 104-2112-M-001-027, and No. CDA-105-M06, former President of Academia Sinica Yuan-Tseh Lee, and former Ministers of MOST Maw-Kuen Wu and Luo-Chuan Lee, Taiwan; the Turkish Atomic Energy Authority at METU, Turkey; and NSF Grant No. 1455202, Wyle Laboratories Grant No. 2014/T72497, and NASA NESSF Grant No. HELIO15F-0005, USA. We gratefully acknowledge the strong support from CERN including Rolf-Dieter Heuer and Fabiola Gianotti, from the CERN IT department and Bernd Panzer-Steindel, and from the European Space Agency including Johann-Dietrich Worner and Simonetta Di Pippo. We are grateful for important discussions with Fiorenza Donato, Jonathan Ellis, Jonathan Feng, Igor Moskalenko, Michael Salamon, Subir Sarkar, Joachim Trumper, Michael S. Turner, Steven Weinberg, and Arnold Wolfendale. NR 85 TC 8 Z9 8 U1 27 U2 27 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD AUG 26 PY 2016 VL 117 IS 9 AR 091103 DI 10.1103/PhysRevLett.117.091103 PG 10 WC Physics, Multidisciplinary SC Physics GA DU1ZE UT WOS:000382008900001 PM 27610839 ER PT J AU Leblanc, T Sica, RJ van Gijsel, JAE Godin-Beekmann, S Haefele, A Trickl, T Payen, G Gabarrot, F AF Leblanc, Thierry Sica, Robert J. van Gijsel, Joanna A. E. Godin-Beekmann, Sophie Haefele, Alexander Trickl, Thomas Payen, Guillaume Gabarrot, Frank TI Proposed standardized definitions for vertical resolution and uncertainty in the NDACC lidar ozone and temperature algorithms - Part 1: Vertical resolution SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID RAMAN LIDAR; STRATOSPHERIC OZONE; RAYLEIGH; DIFFERENTIATION; RETRIEVAL; PROFILES; DENSITY AB A standardized approach for the definition and reporting of vertical resolution of the ozone and temperature lidar profiles contributing to the Network for the Detection for Atmospheric Composition Change (NDACC) database is proposed. Two standardized definitions homogeneously and unequivocally describing the impact of vertical filtering are recommended. The first proposed definition is based on the width of the response to a finite-impulse-type perturbation. The response is computed by convolving the filter coefficients with an impulse function, namely, a Kronecker delta function for smoothing filters, and a Heaviside step function for derivative filters. Once the response has been computed, the proposed standardized definition of vertical resolution is given by Delta z = delta z x H-FWHM, where delta z is the lidar's sampling resolution and H-FWHM is the full width at half maximum (FWHM) of the response, measured in sampling intervals. The second proposed definition relates to digital filtering theory. After applying a Laplace transform to a set of filter coefficients, the filter's gain characterizing the effect of the filter on the signal in the frequency domain is computed, from which the cut-off frequency f(C), defined as the frequency at which the gain equals 0.5, is computed. Vertical resolution is then defined by Delta z = delta z/(2f(C)). Unlike common practice in the field of spectral analysis, a factor 2 f(C) instead of f(C) is used here to yield vertical resolution values nearly equal to the values obtained with the impulse response definition using the same filter coefficients. When using either of the proposed definitions, unsmoothed signals yield the best possible vertical resolution Delta z = delta z (one sampling bin). Numerical tools were developed to support the implementation of these definitions across all NDACC lidar groups. The tools consist of ready-to-use "plug-in" routines written in several programming languages that can be inserted into any lidar data processing software and called each time a filtering operation occurs in the data processing chain. When data processing implies multiple smoothing operations, the filtering information is analytically propagated through the multiple calls to the routines in order for the standardized values of vertical resolution to remain theoretically and numerically exact at the very end of data processing. C1 [Leblanc, Thierry] CALTECH, Jet Prop Lab, Wrightwood, CA 92397 USA. [Sica, Robert J.] Univ Western Ontario, Dept Phys & Astron, London, ON, Canada. [van Gijsel, Joanna A. E.] Royal Netherlands Meteorol Inst KNMI, Bilthoven, Netherlands. [Godin-Beekmann, Sophie] CNRS INSU, LATMOS IPSL, Paris, France. [Haefele, Alexander] Meteoswiss, Payerne, Switzerland. [Trickl, Thomas] IMK IFU, Karlsruhe Inst Technol, Garmisch Partenkirchen, Germany. [Payen, Guillaume; Gabarrot, Frank] Univ Le Reunion, Observ Sci, CNRS, St Denis De La Reunion, Reunion. [Payen, Guillaume; Gabarrot, Frank] Univ Reunion, UMS3365, St Denis De La Reunion, Reunion. RP Leblanc, T (reprint author), CALTECH, Jet Prop Lab, Wrightwood, CA 92397 USA. EM thierry.leblanc@jpl.nasa.gov RI Trickl, Thomas/F-7331-2010 FU VALID project; Canadian National Sciences and Engineering Research Council FX This work was initiated in response to the 2010 call for international teams of experts in earth and space science by the International Space Science Institute (ISSI) in Bern, Switzerland. It could not have been performed without the travel and logistical support of ISSI. Part of the work described in this report was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under agreements with the National Aeronautics and Space Administration. Part of this work was carried out in support of the VALID project. Robert J. Sica would like to acknowledge the support of the Canadian National Sciences and Engineering Research Council for support of the University of Western Ontario lidar work. The team would also like to acknowledge J. Bandoro for his help in the design of the MATLAB filtering tools. NR 29 TC 3 Z9 3 U1 0 U2 0 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 EI 1867-8548 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PD AUG 25 PY 2016 VL 9 IS 8 BP 4029 EP 4049 DI 10.5194/amt-9-4029-2016 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DW6YY UT WOS:000383798500001 ER PT J AU Leblanc, T Sica, RJ van Gijsel, JAE Godin-Beekmann, S Haefele, A Trickl, T Payen, G Liberti, G AF Leblanc, Thierry Sica, Robert J. van Gijsel, Joanna A. E. Godin-Beekmann, Sophie Haefele, Alexander Trickl, Thomas Payen, Guillaume Liberti, Gianluigi TI Proposed standardized definitions for vertical resolution and uncertainty in the NDACC lidar ozone and temperature algorithms - Part 2: Ozone DIAL uncertainty budget SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID ABSORPTION CROSS-SECTIONS; FOURIER-TRANSFORM SPECTROSCOPY; O-2 HERZBERG BANDS; STRATOSPHERIC OZONE; RAYLEIGH-SCATTERING; UV SPECTROSCOPY; NM REGION; NO2; TROPOSPHERE; SPECTRA AB A standardized approach for the definition, propagation, and reporting of uncertainty in the ozone differential absorption lidar data products contributing to the Network for the Detection for Atmospheric Composition Change (NDACC) database is proposed. One essential aspect of the proposed approach is the propagation in parallel of all independent uncertainty components through the data processing chain before they are combined together to form the ozone combined standard uncertainty. The independent uncertainty components contributing to the overall budget include random noise associated with signal detection, uncertainty due to saturation correction, background noise extraction, the absorption cross sections of O-3, NO2, SO2, and O-2, the molecular extinction cross sections, and the number densities of the air, NO2, and SO2. The expression of the individual uncertainty components and their step-by-step propagation through the ozone differential absorption lidar (DIAL) processing chain are thoroughly estimated. All sources of uncertainty except detection noise imply correlated terms in the vertical dimension, which requires knowledge of the covariance matrix when the lidar signal is vertically filtered. In addition, the covariance terms must be taken into account if the same detection hardware is shared by the lidar receiver channels at the absorbed and non-absorbed wavelengths. The ozone uncertainty budget is presented as much as possible in a generic form (i.e., as a function of instrument performance and wavelength) so that all NDACC ozone DIAL investigators across the network can estimate, for their own instrument and in a straightforward manner, the expected impact of each reviewed uncertainty component. In addition, two actual examples of full uncertainty budget are provided, using nighttime measurements from the tropospheric ozone DIAL located at the Jet Propulsion Laboratory (JPL) Table Mountain Facility, California, and nighttime measurements from the JPL stratospheric ozone DIAL located at Mauna Loa Observatory, Hawai'i. C1 [Leblanc, Thierry] CALTECH, Jet Prop Lab, Wrightwood, CA 92397 USA. [Sica, Robert J.] Univ Western Ontario, Dept Phys & Astron, London, ON, Canada. [van Gijsel, Joanna A. E.] Royal Netherlands Meteorol Inst KNMI, Bilthoven, Netherlands. [Godin-Beekmann, Sophie] CNRS INSU, LATMOS IPSL, Paris, France. [Haefele, Alexander] Meteoswiss, Payerne, Switzerland. [Trickl, Thomas] IMK IFU, Karlsruhe Inst Technol, Garmisch Partenkirchen, Germany. [Payen, Guillaume] Univ La Reunion, Observ Sci, CNRS, St Denis De La Reunion, France. [Payen, Guillaume] Univ Reunion, UMS3365, St Denis De La Reunion, France. [Liberti, Gianluigi] ISAC CNR, Via Fosso Cavaliere 100, I-00133 Rome, Italy. RP Leblanc, T (reprint author), CALTECH, Jet Prop Lab, Wrightwood, CA 92397 USA. EM thierry.leblanc@jpl.nasa.gov RI Trickl, Thomas/F-7331-2010 FU European Space Agency VALID project; Canadian National Sciences and Engineering Research Council FX This work was initiated in response to the 2010 call for international teams of experts in Earth and Space Science by the International Space Science Institute (ISSI) in Bern, Switzerland. It could not have been performed without the travel and logistical support of ISSI. Part of the work described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under agreements with the National Aeronautics and Space Administration. Part of this work was carried out in support of the European Space Agency VALID project. Robert J. Sica would like to acknowledge the support of the Canadian National Sciences and Engineering Research Council for support of the University of Western Ontario lidar work. NR 58 TC 2 Z9 2 U1 2 U2 2 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 EI 1867-8548 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PD AUG 25 PY 2016 VL 9 IS 8 BP 4051 EP 4078 DI 10.5194/amt-9-4051-2016 PG 28 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DW6YY UT WOS:000383798500002 ER PT J AU Leblanc, T Sica, RJ van Gijsel, JAE Haefele, A Payen, G Liberti, G AF Leblanc, Thierry Sica, Robert J. van Gijsel, Joanna A. E. Haefele, Alexander Payen, Guillaume Liberti, Gianluigi TI Proposed standardized definitions for vertical resolution and uncertainty in the NDACC lidar ozone and temperature algorithms - Part 3: Temperature uncertainty budget SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID ABSORPTION CROSS-SECTIONS; RAYLEIGH-SCATTER; RAMAN LIDAR; MIDDLE ATMOSPHERE; NO2 ABSORPTION; NM REGION; SPECTRA; MODEL; VALIDATION; RANGE AB A standardized approach for the definition, propagation, and reporting of uncertainty in the temperature lidar data products contributing to the Network for the Detection for Atmospheric Composition Change (NDACC) database is proposed. One important aspect of the proposed approach is the ability to propagate all independent uncertainty components in parallel through the data processing chain. The individual uncertainty components are then combined together at the very last stage of processing to form the temperature combined standard uncertainty. The identified uncertainty sources comprise major components such as signal detection, saturation correction, background noise extraction, temperature tie-on at the top of the profile, and absorption by ozone if working in the visible spectrum, as well as other components such as molecular extinction, the acceleration of gravity, and the molecular mass of air, whose magnitudes depend on the instrument, data processing algorithm, and altitude range of interest. The expression of the individual uncertainty components and their step-by-step propagation through the temperature data processing chain are thoroughly estimated, taking into account the effect of vertical filtering and the merging of multiple channels. All sources of uncertainty except detection noise imply correlated terms in the vertical dimension, which means that covariance terms must be taken into account when vertical filtering is applied and when temperature is integrated from the top of the profile. Quantitatively, the uncertainty budget is presented in a generic form (i.e., as a function of instrument performance and wavelength), so that any NDACC temperature lidar investigator can easily estimate the expected impact of individual uncertainty components in the case of their own instrument. Using this standardized approach, an example of uncertainty budget is provided for the