FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Canavan, ER Stevenson, TR Nagler, PC Mok, M AF Canavan, Edgar R. Stevenson, Thomas R. Nagler, Peter C. Mok, Mason TI Demonstration of a Pixel-Scale Superconducting Heat Switch for an Ideal Integrating Bolometer SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Heat switch; superconducting devices; superconducting films ID THERMAL-CONDUCTIVITY; FILMS; TEMPERATURES AB The sensitivity of a bolometer is in principle limited by the phonon noise, which is a function of the conductance between its absorber and the thermal sink. However, practical issues limit the degree to which conductance can be minimized. For example, in a high-radiation environment, extremely low conductance, or, equivalently, long thermal recovery time, can lead to high data loss. To circumvent such limitations, we are developing a technique of modulating the conductance through the use of pixel-scale superconducting heat switches. We have fabricated bolometer-like test devices consisting of isolated regions connected to a thermal ground plane through narrow aluminum strips. Niobium coils are patterned around the aluminum strips. Flowing current through a coil allows the aluminum to be driven into the normal or high thermal conductance state. We have measured the conductance of these devices as a function of temperature and drive coil current. C1 [Canavan, Edgar R.; Stevenson, Thomas R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nagler, Peter C.] Brown Univ, Providence, RI 02912 USA. [Mok, Mason] Univ Wisconsin, Madison, WI 53706 USA. RP Canavan, ER (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Edgar.R.Canavan@nasa.gov; Thomas.R.Stevenson@nasa.gov; peter.c.nagler@nasa.gov; mmok@wisc.edu FU NASA under the Center Innovation Fund FX This work was supported by NASA under the Center Innovation Fund. NR 19 TC 0 Z9 0 U1 1 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 EI 1558-2515 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2017 VL 27 IS 4 AR 2500705 DI 10.1109/TASC.2017.2664830 PG 5 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA EN6HO UT WOS:000396105300001 ER PT J AU Chiao, MP Smith, SJ Kilbourne, CA Adams, JS Bandler, SR Betancourt-Martinez, GL Chervenak, JA Datesman, AM Eckart, ME Ewin, AJ Finkbeiner, FM Figueroa-Feliciano, E Kelley, RL Lee, SJ Leutenegger, M Porter, FS Sadleir, JE Wassell, EJ Yoon, W AF Chiao, Meng P. Smith, Stephen James Kilbourne, Caroline A. Adams, Joseph S. Bandler, Simon R. Betancourt-Martinez, Gabriele L. Chervenak, James A. Datesman, Aaron M. Eckart, Megan E. Ewin, Audrey J. Finkbeiner, Fred Michael Figueroa-Feliciano, Enectali Kelley, Richard L. Lee, Sang Jun Leutenegger, Maurice Porter, Frederick Scott Sadleir, John E. Wassell, Edward J. Yoon, Wonsik TI Parametric Characterization of TES Detectors Under DC Bias SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Model checking; parametric study; transition-edge sensors; x-ray microcalorimeter AB The X-ray integrated field unit (X-IFU) in European Space Agency's (ESA's) Athena mission will be the first high-resolution X-ray spectrometer in space using a large-format transition-edge sensor microcalorimeter array. Motivated by optimization of detector performance for X-IFU, we have conducted an extensive campaign of parametric characterization on transition-edge sensor (TES) detectors with nominal geometries and physical properties in order to establish sensitivity trends relative to magnetic field, dc bias on detectors, operating temperature, and to improve our understanding of detector behavior relative to its fundamental properties such as thermal conductivity, heat capacity, and transition temperature. These results were used for validation of a simple linear detector model in which a small perturbation can be introduced to one or multiple parameters to estimate the error budget for X-IFU. We will show here results of our parametric characterization of TES detectors and briefly discuss the comparison with the TES model. C1 [Chiao, Meng P.; Smith, Stephen James; Kilbourne, Caroline A.; Adams, Joseph S.; Bandler, Simon R.; Betancourt-Martinez, Gabriele L.; Chervenak, James A.; Datesman, Aaron M.; Eckart, Megan E.; Ewin, Audrey J.; Finkbeiner, Fred Michael; Kelley, Richard L.; Leutenegger, Maurice; Porter, Frederick Scott; Sadleir, John E.; Wassell, Edward J.; Yoon, Wonsik] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Chiao, Meng P.; Smith, Stephen James; Adams, Joseph S.; Leutenegger, Maurice] Univ Maryland, Baltimore, MD 21250 USA. [Betancourt-Martinez, Gabriele L.] Univ Maryland, College Pk, MD 20742 USA. [Datesman, Aaron M.; Wassell, Edward J.] Stinger Ghaffarian Technol Inc, Lanham, MD 20706 USA. [Finkbeiner, Fred Michael] Wyle Informat Syst, Mclean, VA 22102 USA. [Figueroa-Feliciano, Enectali] Northwest Univ, Evanston, IL 60206 USA. [Lee, Sang Jun] Stanford Univ, Stanford, CA 94305 USA. [Yoon, Wonsik] Univ Space Res Assoc, Washington, DC 20024 USA. RP Chiao, MP (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM meng.p.chiao@nasa.gov; stephen.j.smith@nasa.gov; Caroline.A.Kilbourne@nasa.gov; Joseph.S.Adams@nasa.gov; Simon.R.Bandler@nasa.gov; Gabriele.L.Betancourt-Martinez@nasa.gov; James.A.Chervenak@nasa.gov; aaron.m.datesman@nasa.gov; Megan.E.Eckart@nasa.gov; Audrey.J.Ewin@nasa.gov; Fred.M.Finkbeiner@nasa.gov; enectali@northwestern.edu; Richard.L.Kelley@nasa.gov; sangjun2@stanford.edu; maurice.a.leutenegger@nasa.gov; Frederick.S.Porter@nasa.gov; john.e.sadleir@nasa.gov; edward.wassell@nasa.gov; wonsik.yoon@nasa.gov NR 5 TC 0 Z9 0 U1 1 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 EI 1558-2515 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2017 VL 27 IS 4 AR 2100305 DI 10.1109/TASC.2016.2645164 PG 5 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA EM6WC UT WOS:000395452200001 ER PT J AU Cunnane, D Kawamura, JH Wolak, MA Acharya, N Xi, XX Karasik, BS AF Cunnane, Daniel Kawamura, Jonathan H. Wolak, Matthaus A. Acharya, Narendra Xi, Xiao Xing Karasik, Boris S. TI Optimization of Parameters of MgB2 Hot-Electron Bolometers SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Hot electron bolometers; MgB2; superconducting devices; terahertz mixers ID MIXER AB Hot-electron bolometers (HEBs) made with MgB2 have proven to have a large intermediate frequency and have shown potential for a low noise into the terahertz range. Although practical results from these mixers have been achieved fairly quickly, effort is still needed to realize an MgB2 HEB with improved sensitivity to compete with state-of-the-art mixers. Here, we present the results of our mixer work to achieve MgB2 HEBs based on hybrid physical chemical vapor deposition grown films, with improved sensitivity and higher temperature operation. A new fabrication process is developed which utilizes even thinner films (< 10 nm) allowing for the improvement of the impedance match of the mixer device with the Au spiral antenna. Integrated superconducting contacts prevent deterioration of the sensitivity due to the electron diffusion. The mixer noise temperature is 2000 and 3600 K at 600 and 1.9 THz, respectively, with minimal dependence on the bath temperature until over 20 K. The noise bandwidth of the mixer is 6.5 GHz at 4.2 K and is expected to be larger at higher operating temperature. C1 [Cunnane, Daniel; Kawamura, Jonathan H.; Karasik, Boris S.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Wolak, Matthaus A.; Acharya, Narendra; Xi, Xiao Xing] Temple Univ, Dept Phys, Philadelphia, PA 19122 USA. RP Cunnane, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM daniel.p.cunnane@jpl.nasa.gov; jonathan.h.kawamura@jpl.nasa.gov; tue99694@temple.edu; tud53450@temple.edu; xiaoxing@temple.edu; boris.s.karasik@jpl.nasa.gov FU NASA Astrophysics Research and Analysis Program through JPL FX The work at the Jet Propulsion Laboratory, California Institute of Technology, was carried out under a contract with the National Aeronautics and Space Administration. The work at Temple University was supported by the NASA Astrophysics Research and Analysis Program through a contract from JPL. NR 23 TC 0 Z9 0 U1 6 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 EI 1558-2515 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2017 VL 27 IS 4 AR 2300405 DI 10.1109/TASC.2017.2655502 PG 5 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA EM9QM UT WOS:000395646200001 ER PT J AU Datesman, AM Adams, JS Bandler, SR Betancourt-Martinez, GL Chang, MP Chervenak, JA Eckart, ME Ewin, AE Finkbeiner, FM Ha, JY Kelley, RL Kilbourne, CA Miniussi, AR Porter, FS Sadleir, JE Sakai, K Smith, SJ Wakeham, NA Williams, EH Wassell, EJ Yoon, W AF Datesman, Aaron M. Adams, Joseph S. Bandler, Simon R. Betancourt-Martinez, Gabriele L. Chang, Meng-Ping Chervenak, James A. Eckart, Megan E. Ewin, Audrey E. Finkbeiner, Fred M. Ha, Jong Yoon Kelley, Richard L. Kilbourne, Caroline A. Miniussi, Antoine R. Porter, Frederick S. Sadleir, John E. Sakai, Kazuhiro Smith, Stephen J. Wakeham, Nicholas A. Williams, Elissa H. Wassell, Edward J. Yoon, Wonsik TI Reduced-Scale Transition-Edge Sensor Detectors for Solar and X-Ray Astrophysics SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Arrays; low temperature detectors; microcalorimeters; transition-edge sensors (TES); X-ray spectroscopy AB We have developed large-format, close-packed X-ray microcalorimeter arrays fabricated on solid substrates, designed to achieve high energy resolution with count rates up to a few hundred counts per second per pixel for X-ray photon energies up to 8 keV. Our most recent arrays feature 31-micron absorbers on a 35-micron pitch, reducing the size of pixels by about a factor of two. This change will enable an instrument with significantly higher angular resolution. In order to wire out large format arrays with an increased density of smaller pixels, we have reduced the lateral size of both the microstrip wiring and the Mo/Au transition-edge sensors (TES). We report on the key physical properties of these small TESs and the fine Nb leads attached, including the critical currents and weak-link properties associated with the longitudinal proximity effect. C1 [Datesman, Aaron M.; Adams, Joseph S.; Bandler, Simon R.; Betancourt-Martinez, Gabriele L.; Chang, Meng-Ping; Chervenak, James A.; Eckart, Megan E.; Ewin, Audrey E.; Finkbeiner, Fred M.; Ha, Jong Yoon; Kelley, Richard L.; Kilbourne, Caroline A.; Miniussi, Antoine R.; Porter, Frederick S.; Sadleir, John E.; Sakai, Kazuhiro; Smith, Stephen J.; Wakeham, Nicholas A.; Williams, Elissa H.; Wassell, Edward J.; Yoon, Wonsik] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Datesman, Aaron M.; Chang, Meng-Ping; Wassell, Edward J.] Stinger Ghaffarian Technol Inc, Greenbelt, MD 20771 USA. [Adams, Joseph S.; Smith, Stephen J.] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Betancourt-Martinez, Gabriele L.] Univ Maryland, College Pk, MD 20742 USA. [Finkbeiner, Fred M.] Wyle Informat Syst, Mclean, VA 22102 USA. [Ha, Jong Yoon; Williams, Elissa H.] SB Microsyst Inc, Glen Burnie, MD 20161 USA. [Miniussi, Antoine R.; Sakai, Kazuhiro; Wakeham, Nicholas A.; Yoon, Wonsik] Univ Space Res Assoc, Columbia, MD 21046 USA. RP Datesman, AM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Datesman, AM (reprint author), Stinger Ghaffarian Technol Inc, Greenbelt, MD 20771 USA. EM aaron.m.datesman@nasa.gov; Joseph.S.Adams@nasa.gov; Simon.R.Bandler@nasa.gov; Gabriele.L.Betancourt-Martinez@nasa.gov; meng-ping.chang@nasa.gov; James.A.Chervenak@nasa.gov; Megan.E.Eckart@nasa.gov; Audrey.E.Ewin@nasa.gov; Fred.M.Finkbeiner@nasa.gov; jongyoon.ha@sbmicrosystems.us; Richard.L.Kelley@nasa.gov; Caroline.A.Kilbourne@nasa.gov; antoine.r.miniussi@nasa.gov; Frederick.S.Porter@nasa.gov; john.e.sadleir@nasa.gov; kazuhiro.sakai@nasa.gov; stephen.j.smith@nasa.gov; Nicholas.a.wakeham@nasa.gov; elissa@sbmicrosystems.us; edward.j.wassell@nasa.gov; wonsik.yoon@nasa.gov FU NASA, Office of Space Science, from ROSES; Heliophysics Technology and Instrument Development for Science [NNH13ZDA001N-HTIDS] FX This work was supported in part by NASA, Office of Space Science, from ROSES 2013 and in part by Heliophysics Technology and Instrument Development for Science under Grant NNH13ZDA001N-HTIDS. NR 13 TC 0 Z9 0 U1 5 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 EI 1558-2515 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2017 VL 27 IS 4 AR 2100505 DI 10.1109/TASC.2017.2649839 PG 5 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA EM9QI UT WOS:000395645800001 ER PT J AU Denis, KL Brown, AD Chang, MP Hu, R Rostem, K U-Yen, K Wollack, EJ AF Denis, Kevin L. Brown, Ari David Chang, Meng-Ping Hu, Ron Rostem, Karwan U-Yen, Kongpop Wollack, Edward J. TI Fabrication of Superconducting Vacuum-Gap Crossovers for High Performance Microwave Applications SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Crossover; air-bridge; microstrip and co-planar waveguide transmission lines; MEMS; superconducting circuit design and fabrication ID TRANSITIONS AB The fabrication of low-loss wide-bandwidth superconducting vacuum-gap crossovers for high performance millimeter wave applications is described. In order to reduce ohmic and parasitic losses atmillimeter wavelengths a vacuum gap is preferred relative to dielectric spacer. Here, vacuum-gap crossovers were realized by using a sacrificial polymer layer followed by niobium sputter deposition optimized for coating coverage over an underlying niobium signal layer. Both coplanar waveguide and microstrip crossover topologies have been explored in detail. The resulting fabrication process is compatible with a bulk micromachining process for realizing waveguide coupled detectors, which includes sacrificial wax bonding, and wafer backside deep reactive ion etching for creation of leg isolated silicon membrane structures. Release of the vacuum-gap structures along with the wax bonded wafer after deep reactive ion etching is implemented in the same process step used to complete the detector fabrication. C1 [Denis, Kevin L.; Brown, Ari David; U-Yen, Kongpop; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Chang, Meng-Ping; Hu, Ron] Stinger Ghaffarian Technol Inc, Greenbelt, MD 20771 USA. [Rostem, Karwan] Johns Hopkins Univ, Baltimore, MD 21218 USA. RP Denis, KL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM kevin.l.denis@nasa.gov; ari.d.brown@nasa.gov; meng-ping.chang@nasa.gov; Gang.hu-1@nasa.gov; karwan.rostem@nasa.gov; kongpop.u-yen-1@nasa.gov; edward.j.wollack@nasa.gov RI Wollack, Edward/D-4467-2012; OI Wollack, Edward/0000-0002-7567-4451; Denis, Kevin/0000-0002-3592-5703 FU NASA Astrophysics Research and Analysis; Goddard Space Flight Center Internal Research and Development Programs FX This work was supported in part by the NASA Astrophysics Research and Analysis and in part by the Goddard Space Flight Center Internal Research and Development Programs. NR 15 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 1051-8223 EI 1558-2515 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2017 VL 27 IS 4 AR 1100404 DI 10.1109/TASC.2016.2646917 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA EM6XS UT WOS:000395456500001 ER PT J AU U-yen, K Brown, AD Moseley, SH Noroozian, O Wollack, EJ AF U-yen, Kongpop Brown, Ari D. Moseley, Samuel H. Noroozian, Omid Wollack, Edward J. TI A Cryogenic Waveguide Mount for Microstrip Circuit and Material Characterization SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Material testing; millimeter wave devices; millimeter wave propagation; superconducting microwave devices ID SUPERCONDUCTING MICROSTRIP; FREQUENCIES; TRANSITION AB A waveguide split-block fixture used in the characterization of thin-film superconducting planar circuitry at millimeter wavelengths is described in detail. The test fixture is realized from a pair of mode converters, which transition from rectangular-waveguide to on-chip microstrip-line signal propagation via a stepped ridge-guide impedance transformer. The observed performance of the W-band package at 4.2 K has a maximum in-band transmission ripple of 2 dB between 1.53 and 1.89 times the waveguide cutoff frequency. This metrology approach enables the characterization of superconducting microstrip test structures as a function of temperature and frequency. The limitations of the method are discussed and representative data for superconducting Nb and NbTiN thin-film microstrip resonators on single-crystal Si dielectric substrates are presented. C1 [U-yen, Kongpop; Brown, Ari D.; Moseley, Samuel H.; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Noroozian, Omid] Univ Maryland, College Pk, MD 20742 USA. RP U-yen, K (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM kongpop.u-yen-1@nasa.gov; ari.d.brown@nasa.gov; samuel.h.moseley@nasa.gov; omid.noroozian@nasa.gov; edward.j.wollack@nasa.gov RI Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 FU National Aeronautics and Space Administration [NNH12ZDA001N-APRA]; Goddard Space Flight Center Internal Research and Development grants FX This work was supported in part by the National Aeronautics and Space Administration under Grant NNH12ZDA001N-APRA and in part by the Goddard Space Flight Center Internal Research and Development grants. NR 23 TC 0 Z9 0 U1 2 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 EI 1558-2515 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2017 VL 27 IS 4 AR 1200304 DI 10.1109/TASC.2016.2645740 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA EM9PX UT WOS:000395644700001 ER PT J AU Yoon, W Adams, JS Bandler, SR Betancourt-Martinez, GL Chiao, MP Chang, MP Chervenak, JA Datesman, A Eckart, ME Ewin, AJ Finkbeiner, FM Ha, JY Kelley, R Kilbourne, CA Miniussi, AR Porter, FS Sadleir, JE Sakai, K Smith, SJ Wakeham, NA Wassell, E AF Yoon, Wonsik Adams, Joseph S. Bandler, Simon R. Betancourt-Martinez, Gabriele L. Chiao, Meng P. Chang, Meng-Ping Chervenak, James A. Datesman, Aaron Eckart, Megan E. Ewin, Audrey J. Finkbeiner, Fred Michael Ha, Jong Yoon Kelley, Richard Kilbourne, Caroline A. Miniussi, Antoine R. Porter, Frederick Scott Sadleir, John E. Sakai, Kazuhiro Smith, Stephen James Wakeham, Nicholas A. Wassell, Edward TI Design and Performance of Hybrid Arrays of Mo/Au Bilayer Transition-Edge Sensors SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Transition-edge sensors; hybrid array; transition temperature AB For future X-ray astrophysics missions, X-ray microcalorimeters can be optimized with different properties in different regions of the focal plane. This approach has the potential to improve microcalorimeter instrument capabilities with efficient use of instrument resources. For example a point-source array optimized for high angular resolution, high count-rate observations could be accompanied by a main array to expand the field of view for diffuse observations. In this approach, it is desirable to be able to simultaneously optimize different transition-edge sensor (TES) geometries on a single wafer design. The key properties of TESs such as transition temperature and shape are a strong function of size and geometry due to the complex interplay between the proximity effect from the superconducting bias electrodes and the normal metal features used for noise suppression and absorber contact. As a result, devices fabricated with the same deposited layer but with different sizes will have different transition temperatures and different response to X-ray events. In this paper, we present measurements of the transition temperature and properties of devices with different sizes and normal metal features, and discuss how by tuning the geometry we can achieve the desired pixel parameters for a given application. We also describe measurements of transition properties from large-format hybrid arrays containing three different pixel types. C1 [Yoon, Wonsik; Adams, Joseph S.; Bandler, Simon R.; Betancourt-Martinez, Gabriele L.; Chiao, Meng P.; Chang, Meng-Ping; Chervenak, James A.; Datesman, Aaron; Eckart, Megan E.; Ewin, Audrey J.; Finkbeiner, Fred Michael; Ha, Jong Yoon; Kelley, Richard; Kilbourne, Caroline A.; Miniussi, Antoine R.; Porter, Frederick Scott; Sadleir, John E.; Sakai, Kazuhiro; Smith, Stephen James; Wakeham, Nicholas A.; Wassell, Edward] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Yoon, Wonsik; Wakeham, Nicholas A.] Univ Space Res Assoc, NASA, Postdoctoral Program, Columbia, MD 21046 USA. [Adams, Joseph S.; Chiao, Meng P.; Smith, Stephen James] Univ Maryland, Baltimore, MD 21250 USA. [Betancourt-Martinez, Gabriele L.] Univ Maryland, College Pk, MD 20742 USA. [Chang, Meng-Ping; Datesman, Aaron; Wassell, Edward] SGT Inc, Greenbelt, MD 20706 USA. [Ha, Jong Yoon] SB Microsyst Inc, Glen Burnie, MD 21061 USA. [Finkbeiner, Fred Michael] Wyle Informat Syst, Mclean, VA 22102 USA. [Miniussi, Antoine R.; Sakai, Kazuhiro] Univ Space Res Assoc, Columbia, MD 21046 USA. RP Yoon, W (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Yoon, W (reprint author), Univ Space Res Assoc, NASA, Postdoctoral Program, Columbia, MD 21046 USA. EM wonsik.yoon@nasa.gov; Joseph.S.Adams@nasa.gov; Simon.R.Bandler@nasa.gov; Gabriele.L.Betancourt-Martinez@nasa.gov; meng.p.chiao@nasa.gov; meng-ping.chang@nasa.gov; James.A.Chervenak@nasa.gov; aaron.m.datesman@nasa.gov; Megan.E.Eckart@nasa.gov; Audrey.J.Ewin@nasa.gov; Fred.M.Finkbeiner@nasa.gov; jongyoon.ha@sbmicrosystems.us; Richard.L.Kelley@nasa.gov; Caroline.A.Kilbourne@nasa.gov; antoine.r.miniussi@nasa.gov; Frederick.S.Porter@nasa.gov; john.e.sadleir@nasa.gov; kazuhiro.sakai@nasa.gov; stephen.j.smith@nasa.gov; Nicholas.a.wakeham@nasa.gov; edward.wassell@nasa.gov NR 17 TC 0 Z9 0 U1 5 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 EI 1558-2515 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2017 VL 27 IS 4 AR 2100705 DI 10.1109/TASC.2017.2655718 PG 5 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA EN1VX UT WOS:000395799500001 ER PT J AU Finkbeiner, FM Adams, JS Bandler, SR Betancourt-Martinez, GL Brown, AD Chang, MP Chervenak, JA Chiao, MP Datesman, AM Eckart, ME Kelley, RL Kilbourne, CA Miniussi, AR Moseley, SJ Porter, FS Sadleir, JE Sakai, K Smith, SJ Wakeham, NA Wassell, EJ Yoon, W AF Finkbeiner, Fred Michael Adams, Joseph S. Bandler, Simon R. Betancourt-Martinez, Gabriele L. Brown, Ari David Chang, Meng-Ping Chervenak, James A. Chiao, Meng P. Datesman, Aaron M. Eckart, Megan E. Kelley, Richard L. Kilbourne, Caroline A. Miniussi, Antoine R. Moseley, Samuel J. Porter, Frederick Scott Sadleir, John E. Sakai, Kazuhiro Smith, Stephen James Wakeham, Nicholas A. Wassell, Edward J. Yoon, Wonisk TI Electron-Beam Deposition of Superconducting Molybdenum Thin Films for the Development of Mo/Au TES X-ray Microcalorimeter SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Molybdenum; superconducting; transition temperature; thin film; X-ray microcalorimeter AB We are exploring the properties of electron-beam evaporated molybdenum thin films on silicon nitride coated silicon wafers at substrate temperatures between room temperature and 650 degrees C. The temperature dependence of film stress, transition temperature, and electrical properties are presented. X-ray diffraction measurements are performed to gain information on molybdenum crystallite size and growth. Results show the dominant influence of the crystallite size on the intrinsic properties of our films. Wafer-scale uniformity, wafer yield, and optimal thermal bias regime for TES fabrication are discussed. C1 [Finkbeiner, Fred Michael; Adams, Joseph S.; Bandler, Simon R.; Betancourt-Martinez, Gabriele L.; Brown, Ari David; Chang, Meng-Ping; Chervenak, James A.; Chiao, Meng P.; Datesman, Aaron M.; Eckart, Megan E.; Kelley, Richard L.; Kilbourne, Caroline A.; Porter, Frederick Scott; Sadleir, John E.; Sakai, Kazuhiro; Smith, Stephen James; Wakeham, Nicholas A.; Wassell, Edward J.; Yoon, Wonisk] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Adams, Joseph S.; Miniussi, Antoine R.; Sakai, Kazuhiro; Smith, Stephen James] CRESST, Baltimore, MD 21250 USA. [Adams, Joseph S.; Miniussi, Antoine R.; Sakai, Kazuhiro; Smith, Stephen James] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Betancourt-Martinez, Gabriele L.; Moseley, Samuel J.] Univ Maryland, College Pk, MD 20742 USA. [Chang, Meng-Ping; Datesman, Aaron M.; Wassell, Edward J.] SGT Inc, Greenbelt, MD 20770 USA. [Moseley, Samuel J.] ADNET Syst Inc, Bethesda, MD 20817 USA. RP Finkbeiner, FM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Fred.M.Finkbeiner@nasa.gov; Joseph.S.Adams@nasa.gov; Simon.R.Bandler@nasa.gov; Gabriele.L.Betancourt-Martinez@nasa.gov; ari.d.brown@nasa.gov; meng-ping.chang@nasa.gov; James.A.Chervenak@nasa.gov; meng.p.chia-o@nasa.gov; aaron.m.datesman@nasa.gov; Megan.E.Eckart@nasa.gov; Richard.L.Kelley@nasa.gov; Caroli-ne.A.Kilbourne@nasa.gov; antoine.r.miniussi@nasa.gov; samuel.j.moseley@nasa.gov; Frederick.S.Porter@nasa.gov; john.e.sadleir@nasa.gov; kazuhiro.sakai@nasa.gov; stephen.j.smith@nasa.gov; Nicholas.a.wakeham@nasa.gov; edward.wassell@nasa.gov; wonsik.yoon@nasa.gov RI Porter, Frederick/D-3501-2012 OI Porter, Frederick/0000-0002-6374-1119 NR 8 TC 1 Z9 1 U1 28 U2 28 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 EI 1558-2515 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2017 VL 27 IS 4 AR 2100104 DI 10.1109/TASC.2016.2633785 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA EH4IT UT WOS:000391735600001 ER PT J AU Wassell, EJ Adams, JS Bandler, SR Betancourt-Martinez, GL Chiao, MP Chang, MP Chervenak, JA Datesman, AM Eckart, ME Ewin, AJ Finkbeiner, FM Ha, JY Kelley, R Kilbourne, CA Miniussi, AR Sakai, K Porter, FS Sadleir, JE Smith, SJ Wakeham, NA Yoon, W AF Wassell, Edward J. Adams, Joseph S. Bandler, Simon R. Betancourt-Martinez, Gabriele L. Chiao, Meng P. Chang, Meng Ping Chervenak, James A. Datesman, Aaron M. Eckart, Megan E. Ewin, Audrey J. Finkbeiner, Fred Michael Ha, Jong Yoon Kelley, Richard Kilbourne, Caroline A. Miniussi, Antoine R. Sakai, Kazuhiro Porter, Frederick Scott Sadleir, John E. Smith, Stephen James Wakeham, Nicholas A. Yoon, Wonisk TI Fabrication of X-Ray Microcalorimeter Focal Planes Composed of Two Distinct Pixel Types SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Arrays; low temperature detectors; microcalorimeters; transition-edge sensors (TES); X-ray spectroscopy AB We develop superconducting transition-edge sensor (TES) microcalorimeter focal planes for versatility in meeting the specifications of X-ray imaging spectrometers, including high count rate, high energy resolution, and large field of view. In particular, a focal plane composed of two subarrays: one of fine pitch, high count-rate devices and the other of slower, larger pixels with similar energy resolution, offers promise for the next generation of astrophysics instruments, such as the X-ray Integral Field Unit Instrument on the European Space Agency's ATHENA mission. We have based the subarrays of our current design on successful pixel designs that have been demonstrated separately. Pixels with an all-gold X-ray absorber on 50 and 75 mu m pitch, where the Mo/Au TES sits atop a thick metal heatsinking layer, have shown high resolution and can accommodate high count rates. The demonstrated larger pixels use a silicon nitride membrane for thermal isolation, thinner Au, and an added bismuth layer in a 250-mu m(2) absorber. To tune the parameters of each subarray requires merging the fabrication processes of the two detector types. We present the fabrication process for dual production of different X-ray absorbers on the same substrate, thick Au on the small pixels and thinner Au with a Bi capping layer on the larger pixels to tune their heat capacities. The process requires multiple electroplating and etching steps, but the absorbers are defined in a single-ion milling step. We demonstrate methods for integrating the heatsinking of the two types of pixel into the same focal plane consistent with the requirements for each subarray, including the limiting of thermal crosstalk. We also discuss fabrication process modifications for tuning the intrinsic transition temperature (T-c) of the bilayers for the different device types through variation of the bilayer thicknesses. The latest results on these "hybrid" arrays will be presented. C1 [Wassell, Edward J.; Adams, Joseph S.; Bandler, Simon R.; Betancourt-Martinez, Gabriele L.; Chiao, Meng P.; Chang, Meng Ping; Chervenak, James A.; Datesman, Aaron M.; Eckart, Megan E.; Ewin, Audrey J.; Finkbeiner, Fred Michael; Ha, Jong Yoon; Kelley, Richard; Kilbourne, Caroline A.; Miniussi, Antoine R.; Sakai, Kazuhiro; Porter, Frederick Scott; Sadleir, John E.; Smith, Stephen James; Wakeham, Nicholas A.; Yoon, Wonisk] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wassell, Edward J.; Datesman, Aaron M.] Stinger Ghaffarian Technol Inc, Greenbelt, MD 20771 USA. [Adams, Joseph S.; Smith, Stephen James] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Betancourt-Martinez, Gabriele L.] Univ Maryland, College Pk, MD 20742 USA. [Finkbeiner, Fred Michael] Wyle Informat Syst, Mclean, VA 22102 USA. [Ha, Jong Yoon] SB Microsyst Inc, Glen Burnie, MD 20161 USA. [Sakai, Kazuhiro; Wakeham, Nicholas A.; Yoon, Wonisk] Univ Space Res Assoc, Columbia, MD 21046 USA. RP Wassell, EJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM edward.wassell@nasa.gov; Joseph.S.Adams@nasa.gov; Simon.R.Bandler@nasa.gov; Gabriele.L.Betancourt-Martinez@nasa.gov; meng.p.chiao@nasa.gov; meng-ping.chang@nasa.gov; James.A.Chervenak@nasa.gov; aaron.m.datesman@nasa.gov; Megan.E.Eckart@nasa.gov; Audrey.J.Ewin@nasa.gov; Fred.M.Finkbeiner@nasa.gov; jongyoon.ha@sbmicrosystems.us; Richard.L.Kelley@nasa.gov; Caroline.A.Kilbourne@nasa.gov; antoine.r.miniussi@nasa.gov; kazuhiro.sakai@nasa.gov; Frederick.S.Porter@nasa.gov; john.e.sadleir@nasa.gov; stephen.j.smith@nasa.gov; Nicholas.a.wakeham@nasa.gov; wonsik.yoon@nasa.gov RI Porter, Frederick/D-3501-2012 OI Porter, Frederick/0000-0002-6374-1119 FU NASA (Office of Space Science from ROSES) [NNX11AB47G] FX This work was supported by NASA (Office of Space Science, Contract NNX11AB47G from ROSES 2009). NR 12 TC 1 Z9 1 U1 27 U2 27 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 EI 1558-2515 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2017 VL 27 IS 4 AR 2300205 DI 10.1109/TASC.2016.2633783 PG 5 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA EG9KR UT WOS:000391378100001 ER PT J AU Arcones, A Bardayan, DW Beers, TC Bernstein, LA Blackmon, JC Messer, B Brown, BA Brown, EF Brune, CR Champagne, AE Chieffi, A Couture, AJ Danielewicz, P Diehl, R El-Eid, M Escher, JE Fields, BD Frohlich, C Herwig, F Hix, WR Iliadis, C Lynch, WG McLaughlin, GC Meyer, BS Mezzacappa, A Nunes, F O'Shea, BW Prakash, M Pritychenko, B Reddy, S Rehm, E Rogachev, G Rutledge, RE Schatz, H Smith, MS Stairs, IH Steiner, AW Strohmayer, TE Timmes, FX Townsley, DM Wiescher, M Zegers, RGT Zingale, M AF Arcones, Almudena Bardayan, Dan W. Beers, Timothy C. Bernstein, Lee A. Blackmon, Jeffrey C. Messer, Bronson Brown, B. Alex Brown, Edward F. Brune, Carl R. Champagne, Art E. Chieffi, Alessandro Couture, Aaron J. Danielewicz, Pawel Diehl, Roland El-Eid, Mounib Escher, Jutta E. Fields, Brian D. Frohlich, Carla Herwig, Falk Hix, William Raphael Iliadis, Christian Lynch, William G. McLaughlin, Gail C. Meyer, Bradley S. Mezzacappa, Anthony Nunes, Filomena O'Shea, Brian W. Prakash, Madappa Pritychenko, Boris Reddy, Sanjay Rehm, Ernst Rogachev, Grigory Rutledge, Robert E. Schatz, Hendrik Smith, Michael S. Stairs, Ingrid H. Steiner, Andrew W. Strohmayer, Tod E. Timmes, F. X. Townsley, Dean M. Wiescher, Michael Zegers, Remco G. T. Zingale, Michael TI White paper on nuclear astrophysics and low energy nuclear physics Part 1: Nuclear astrophysics SO PROGRESS IN PARTICLE AND NUCLEAR PHYSICS LA English DT Article DE Nuclear astrophysics; White paper; Nucleosynthesis AB This white paper informs the nuclear astrophysics community and funding agencies about the scientific directions and priorities of the field and provides input from this community for the 2015 Nuclear Science Long Range Plan. It summarizes the outcome of the nuclear astrophysics town meeting that was held on August 21-23, 2014 in College Station at the campus of Texas A&M University in preparation of the NSAC Nuclear Science Long Range Plan. It also reflects the outcome of an earlier town meeting of the nuclear astrophysics community organized by the Joint Institute for Nuclear Astrophysics (JINA) on October 9-10, 2012 Detroit, Michigan, with the purpose of developing a vision for nuclear astrophysics in light of the recent NRC decadal surveys in nuclear physics (NP2010) and astronomy (ASTRO2010). The white paper is furthermore informed by the town meeting of the Association of Research at University Nuclear Accelerators (ARUNA) that took place at the University of Notre Dame on June 12-13, 2014. In summary we find that nuclear astrophysics is a modern and vibrant field addressing fundamental science questions at the intersection of nuclear physics and astrophysics. These questions relate to the origin of the elements, the nuclear engines that drive life and death of stars, and the properties of dense matter. A broad range of nuclear accelerator facilities, astronomical observatories, theory efforts, and computational capabilities are needed. With the developments outlined in this white paper, answers to long standing key questions are well within reach in the coming decade. (C) 2016 Published by Elsevier B.V. C1 [Arcones, Almudena] Tech Univ Darmstadt, Inst Kernphys, Theory Ctr, Schlossgartenstr 2, D-64289 Darmstadt, Germany. [Arcones, Almudena] GSI Helmholtzzentrum Schwerionenforsch GmbH, Planckstr 1, D-64291 Darmstadt, Germany. [Bardayan, Dan W.; Beers, Timothy C.; Wiescher, Michael] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Bardayan, Dan W.; Beers, Timothy C.; Wiescher, Michael] Univ Notre Dame, JINA Ctr Evolut Elements, Notre Dame, IN 46556 USA. [Bernstein, Lee A.; Escher, Jutta E.] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. [Blackmon, Jeffrey C.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Messer, Bronson] Oak Ridge Natl Lab, Natl Ctr Computat Sci, Oak Ridge, TN 37831 USA. [Messer, Bronson; Hix, William Raphael; Smith, Michael S.; Steiner, Andrew W.] Oak Ridge Natl Lab, Div Phys, Oak Ridge, TN 37831 USA. [Brown, B. Alex; Brown, Edward F.; Danielewicz, Pawel; Lynch, William G.; Nunes, Filomena; Schatz, Hendrik; Zegers, Remco G. T.] Michigan State Univ, Natl Superconducting Cyclotron Lab, E Lansing, MI 48824 USA. [Brown, B. Alex; Brown, Edward F.; Danielewicz, Pawel; Lynch, William G.; Nunes, Filomena; O'Shea, Brian W.; Schatz, Hendrik; Zegers, Remco G. T.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Brune, Carl R.; Prakash, Madappa] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. [Champagne, Art E.; Iliadis, Christian] Univ North Carolina Chapel Hill, Chapel Hill, NC 27599 USA. [Champagne, Art E.; Iliadis, Christian] Triangle Univ, Nucl Lab, Durham, NC 27708 USA. [Chieffi, Alessandro] INAF IAPS, Via Fosso Cavaliere, I-00133 Rome, Italy. [Couture, Aaron J.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Diehl, Roland] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Diehl, Roland] Excellence Cluster Universe, D-85748 Garching, Germany. [El-Eid, Mounib] Amer Univ Beirut, Dept Phys, Bliss St 11-0236, Beirut 11072020, Lebanon. [Fields, Brian D.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Frohlich, Carla; McLaughlin, Gail C.] North Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. [Herwig, Falk] Univ Victoria, Dept Phys & Astron, Victoria, BC, Canada. [Meyer, Bradley S.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Hix, William Raphael; Mezzacappa, Anthony] Univ Tennessee, Dept Phys & Astron, Knoxville, TN 37996 USA. [Mezzacappa, Anthony] Oak Ridge Natl Lab, Joint Inst Computat Sci, Oak Ridge, TN 37831 USA. [O'Shea, Brian W.] Michigan State Univ, Dept Computat Math Sci & Engn, E Lansing, MI 48824 USA. [Pritychenko, Boris] Brookhaven Natl Lab, Natl Nucl Data Ctr, Upton, NY 11973 USA. [Reddy, Sanjay] Univ Washington, Inst Nucl Theory, Seattle, WA 98195 USA. [Rehm, Ernst] Argonne Natl Lab, Div Phys, Argonne, IL 60439 USA. [Rogachev, Grigory] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Rogachev, Grigory] Texas A&M Univ, Inst Cyclotron, College Stn, TX 77843 USA. [Rutledge, Robert E.] McGill Univ, Dept Phys, 3600 Rue Univ, Montreal, PQ H3A 2T8, Canada. [Stairs, Ingrid H.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Strohmayer, Tod E.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Timmes, F. X.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Townsley, Dean M.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Zingale, Michael] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Arcones, Almudena; Bardayan, Dan W.; Beers, Timothy C.; Blackmon, Jeffrey C.; Brown, B. Alex; Brown, Edward F.; Brune, Carl R.; Couture, Aaron J.; Diehl, Roland; Fields, Brian D.; Frohlich, Carla; Herwig, Falk; Lynch, William G.; McLaughlin, Gail C.; Nunes, Filomena; O'Shea, Brian W.; Prakash, Madappa; Reddy, Sanjay; Rehm, Ernst; Rutledge, Robert E.; Schatz, Hendrik; Steiner, Andrew W.; Timmes, F. X.; Wiescher, Michael; Zegers, Remco G. T.; Zingale, Michael] Joint Inst Nucl Astrophys, Ctr Evolut Elements, Multiinst, Notre Dame, MI 46556 USA. RP Schatz, H (reprint author), Michigan State Univ, Natl Superconducting Cyclotron Lab, E Lansing, MI 48824 USA.; Schatz, H (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.; Schatz, H (reprint author), Joint Inst Nucl Astrophys, Ctr Evolut Elements, Multiinst, Notre Dame, MI 46556 USA. EM schatz@nscl.msu.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0146-6410 EI 1873-2224 J9 PROG PART NUCL PHYS JI Prog. Part. Nucl. Phys. PD MAY PY 2017 VL 94 BP 1 EP 67 DI 10.1016/j.ppnp.2016.12.003 PG 67 WC Physics, Nuclear; Physics, Particles & Fields SC Physics GA EP9LA UT WOS:000397693900001 ER PT J AU Mandija, F Sicard, M Comeron, A Alados-Arboledas, L Guerrero-Rascado, JL Barragan, R Bravo-Aranda, JA Granados-Munoz, MJ Lyamani, H Porcar, CM Rocadenbosch, F Rodriguez, A Valenzuela, A Vizcaino, DG AF Mandija, Florian Sicard, Michael Comeron, Adolfo Alados-Arboledas, Lucas Luis Guerrero-Rascado, Juan Barragan, Ruben Antonio Bravo-Aranda, Juan Jose Granados-Munoz, Maria Lyamani, Hassan Munoz Porcar, Constantino Rocadenbosch, Francisco Rodriguez, Alejandro Valenzuela, Antonio Garcia Vizcaino, David TI Origin and pathways of the mineral dust transport to two Spanish EARLINET sites: Effect on the observed columnar and range-resolved dust optical properties SO ATMOSPHERIC RESEARCH LA English DT Article DE Saharan dust events; Barcelona and Granada EARLINET sites; Aerosol optical properties; Dust plume geometrical structure; Backwatd trajectories ID ANGSTROM TURBIDITY PARAMETERS; 2003 HEAT-WAVE; SAHARAN DUST; SOUTHEASTERN SPAIN; SIZE DISTRIBUTION; DESERT DUST; AEROSOL CHARACTERIZATION; ATMOSPHERIC AEROSOLS; MEDITERRANEAN REGION; IBERIAN PENINSULA AB In this paper, is presented a method for estimation of the effect of the transport process to aerosol optical properties. Aerosol optical data retrieved by lidars and sun-photometer measurements, are applied to Saharan dust events observed simultaneously at the two EARLINET/AERONET sites of Barcelona and Granada during the periods ofJune-September of 2012 and 2013. For this purpose, elastic lidar profiles and sun-photometer columnar retrievals are analyzed together with satellite observations and dust forecast models. Granada presents more than twice Saharan dust outbreaks compared to Barcelona. The scenarios favoring the Saharan dust outbreaks are identified in both places. The mineral dust originating in the Sahara region and arriving at both stations is usually transport wither over the Atlas Mountains or through an Atlantic pathway. Analyses of dust events affecting both stations reveal how differences in the transport process lead to differences in the aerosol optical properties measured at each station. Mean dust related Angstrom exponent is 1.8 times higher in Barcelona than in Granada. This difference is a result of the additional contribution of anthropogenic aerosol, mainly in the aerosol fine mode, during the transport of the mineral dust plume over the Iberian Peninsula. (C) 2016 Elsevier B.V. All rights reserved. C1 [Mandija, Florian] Univ Shkodra, Fac Nat Sci, Dept Phys, Shkoder, Albania. [Mandija, Florian; Sicard, Michael; Comeron, Adolfo; Barragan, Ruben; Munoz Porcar, Constantino; Rocadenbosch, Francisco; Rodriguez, Alejandro; Garcia Vizcaino, David] Univ Politecn Cataluna, Dept Signal Theory & Commun, Remote Sensing Lab RSLab, Barcelona, Spain. [Sicard, Michael; Barragan, Ruben; Rocadenbosch, Francisco] Univ Politecn Cataluna, CTE CRAE, IEEC, Barcelona, Spain. [Alados-Arboledas, Lucas; Luis Guerrero-Rascado, Juan; Antonio Bravo-Aranda, Juan; Jose Granados-Munoz, Maria; Lyamani, Hassan; Valenzuela, Antonio] Univ Granada, Fac Sci, Dpt Appl Phys, Fuentenueva S-N, Granada 18071, Spain. [Mandija, Florian; Alados-Arboledas, Lucas; Luis Guerrero-Rascado, Juan; Antonio Bravo-Aranda, Juan; Jose Granados-Munoz, Maria; Lyamani, Hassan; Valenzuela, Antonio] Andalusian Inst Earth Syst Res IISTA CEAMA, Avda Mediterraneo S-N, Granada 18006, Spain. [Antonio Bravo-Aranda, Juan] CNRS, Ecole Polytech, Inst Pierre Simon Laplace, Paris, France. [Valenzuela, Antonio] Univ Evora, Inst Ciencias Terra, Inst Invest Formacao Avancada, Dept Fis, Evora, Portugal. [Jose Granados-Munoz, Maria] CALTECH, NASA Jet Prop Lab, Table Mt Facil, Wrightwood, CA USA. RP Mandija, F (reprint author), L Vojo Kushi Rr Clirimi 53, Shkoder, Albania. EM fmandija@unishk.edu.al OI Mandija, Florian/0000-0002-9324-9440 FU European Union [654169, 262254]; Andalusia Regional Government [P12-RNM-2409]; Spanish Ministry of Economy and Competitiveness [CGL2013-45410-R, TEC2012-34575, TEC2015-63832-P]; EFRD (European Fund for Regional Development) [FEDER REFS UNGR08-1E-023 y UNGR13-1E-1525]; Ministry of Science and Innovation [UNPC10-4E-442]; Department of Economy and Knowledge of the Catalan autonomous government [2014 SGR 583]; JoinEU-SEE Erasmus Mundus Partnerships Action 2 FX Lidar measurements in Granada and Barcelona were supported by the ACTRIS (Aerosols, Clouds, and Trace Gases Research Infrastructure Network) Research Infrastructure Project funded by the European Union's Horizon 2020 research and innovation program under grant agreement no. 654169 and previously under grant agreement no. 262254 in the European Union Seventh Framework Programme (FP7/2007-2013). Measurements in Granada were also supported by the Andalusia Regional Government through the project P12-RNM-2409 and by the Spanish Ministry of Economy and Competitiveness through the project CGL2013-45410-R. The authors thankfully acknowledge the EFRD (European Fund for Regional Development (FEDER REFS UNGR08-1E-023 y UNGR13-1E-1525)) program for the instrumentation used in this work. Measurements in Barcelona were also supported by the Spanish Ministry of Economy and Competitiveness (projects TEC2012-34575 and TEC2015-63832-P) and Ministry of Science and Innovation (project UNPC10-4E-442) and EFRD, and by the Department of Economy and Knowledge of the Catalan autonomous government (grant 2014 SGR 583). This work was supported also by the JoinEU-SEE Erasmus Mundus Partnerships Action 2, which enabled the coordination between the authors of the these research institutions. NR 63 TC 0 Z9 0 U1 3 U2 3 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0169-8095 EI 1873-2895 J9 ATMOS RES JI Atmos. Res. PD MAY 1 PY 2017 VL 187 BP 69 EP 83 DI 10.1016/j.atmosres.2016.12.002 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EK0RR UT WOS:000393635300006 ER PT J AU Clarke, JDA Willson, D Smith, H Hobbs, SW Jones, E AF Clarke, J. D. A. Willson, D. Smith, H. Hobbs, S. W. Jones, E. TI Southern Meridiani Planum - A candidate landing site for the first crewed mission to Mars SO ACTA ASTRONAUTICA LA English DT Article DE Mars; Meridiani planum; Exploration; Crewed missions; Landing site selection; ISRU ID OPPORTUNITY ROVER; IMPACT CRATERS; LIFE; MINERALOGY; CHEMISTRY; SELECTION; SOILS; ROCKS; ICE AB Astronauts working on the surface of Mars have the capability to explore efficiently, rapidly, and flexibly, allowing them to perform a wide range of field investigations. NASA has begun an open international process to identify and evaluate candidate locations where crews could land, live and work on the martian surface, beginning with the First Landing Site/Exploration Zone Workshop for Human Missions to the Surface of Mars in October 2015. Forty seven sites were proposed, including several at or near the Meridiani area, the subject of this paper. We consider the Meridiani area an excellent candidate for the first missions to Mars. It is accessible, safe, contains potential water resources in the form of poly-hydrated magnesium sulphates, has diverse science features with high likelihood of meeting all science goals, has other potential resources and potential for further longer-ranged exploration. The presence of hardware from previous missions will be of benefit to studies of materials to martian conditions, assessing the effectiveness of historic planetary protection strategies, and engaging public interest. Lastly, parts of the Meridiani region have been well studied from the surface by the Opportunity mission, providing ground truth for orbital data. As one of the best documented regions of Mars this will allow a "Go where you know" approach for the first crewed missions, especially with regard to safety, trafficability, and water resource potential. C1 [Clarke, J. D. A.; Willson, D.; Hobbs, S. W.; Jones, E.] Mars Soc Australia, POB 327, Clifton Hills, Vic 3068, Australia. [Clarke, J. D. A.] UNSW, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia. [Willson, D.; Smith, H.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hobbs, S. W.] UNSW Canberra, Australian Def Force Acad, Sch Phys Environm & Math Sci, Northcott Dr, Canberra, ACT 2600, Australia. [Jones, E.] Univ South Australia, Div IT Engn & Environm, Bonython Jubilee Bldg,GPO Box 2471, Adelaide, SA 5001, Australia. RP Clarke, JDA (reprint author), Mars Soc Australia, POB 327, Clifton Hills, Vic 3068, Australia. EM jon.clarke@bigpond.com; david.willson@nasa.gov; heather.d.smith@nasa.gov; swhobbs2000@hotmail.com; eriita.jones@unisa.edu.au NR 114 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD APR PY 2017 VL 133 BP 195 EP 220 DI 10.1016/j.actaastro.2016.12.039 PG 26 WC Engineering, Aerospace SC Engineering GA EO8NS UT WOS:000396946700021 ER PT J AU Vallat, C Altobelli, N Geiger, B Grieger, B Kueppers, M Crego, CM Moissl, R Taylor, MGGT Alexander, C Buratti, B Choukroun, M AF Vallat, Claire Altobelli, Nicolas Geiger, Bernhard Grieger, Bjoern Kueppers, Michael Munoz Crego, Claudio Moissl, Richard Taylor, Matthew G. G. T. Alexander, Claudia Buratti, Bonnie Choukroun, Mathieu CA RSGS Liaison Sci Grp TI The science planning process on the Rosetta mission SO ACTA ASTRONAUTICA LA English DT Article DE Rosetta; Comet; Science Planning; Operations ID COMET 67P/CHURYUMOV-GERASIMENKO AB The Rosetta mission arrived at comet 67 P/Churyumov-Gerasimenko in Summer 2014, after more than 10 years in space. All previous mission encounters with a comet have provided a snapshot of the cometary activity at a given heliocentric distance. In contrast, Rosetta has escorted the comet nucleus for an extended period (> 2 years) at a large range of cometo-centric and heliocentric distances, which has provided exceptional and unprecedented observing conditions to study, analyse and monitor 67 P during its passage to, through and away from perihelion. One of the biggest challenges of this mission is the development of an observation plan that adequately addresses the mission's science objectives while coping with a largely unknown and continuously evolving environment that constantly modifies the planning constraints. The Rosetta Science Ground Segment (RSGS), in support of the Project Scientist and the Science Working Team, is in charge of translating the high level mission science objectives into a low level pointing and operations plan. We present here the high-level science planning process adopted during the comet escort phase. We describe the main science objectives addressed along the mission lifetime, the different groups involved in the science planning, and the approach followed to translate those requirements into a viable and scientifically valid operations plan. Finally, we describe how the science planning scheme has evolved since arrival at the comet to react to the unexpected environment, largely reducing the planning lead times. C1 [Vallat, Claire] European Space Astron Ctr ESA, Telespazio VEGA PLC, Camino Bajo del Castillo S-N, Madrid 28691, Spain. [Altobelli, Nicolas; Kueppers, Michael; Moissl, Richard] European Space Astron Ctr ESA, Madrid, Spain. [Geiger, Bernhard; Grieger, Bjoern] European Space Astron Ctr ESA, Aurora Technol BV, Madrid, Spain. [Munoz Crego, Claudio] European Space Astron Ctr ESA, GMV, Madrid, Spain. [Taylor, Matthew G. G. T.] European Space Res & Technol Ctr ESA, Noordwijk, Netherlands. [Alexander, Claudia; Buratti, Bonnie; Choukroun, Mathieu] Jet Prop Lab, Pasadena, CA USA. RP Vallat, C (reprint author), European Space Astron Ctr ESA, Telespazio VEGA PLC, Camino Bajo del Castillo S-N, Madrid 28691, Spain. EM cvallat@sciops.esa.int NR 22 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD APR PY 2017 VL 133 BP 244 EP 257 DI 10.1016/j.actaastro.2017.01.018 PG 14 WC Engineering, Aerospace SC Engineering GA EO8NS UT WOS:000396946700024 ER PT J AU Burton, R Rock, S Springmann, J Cutler, J AF Burton, R. Rock, S. Springmann, J. Cutler, J. TI Online attitude determination of a passively magnetically stabilized spacecraft SO ACTA ASTRONAUTICA LA English DT Article DE Attitude determination; Nano satellites; Passive magnetic stabilization; Kalman Filter; MEKF; Online estimation AB An online attitude determination filter is developed for a nano satellite that has no onboard attitude sensors or gyros. Specifically, the attitude of NASA Ames Research Center's O/OREOS, a passively magnetically stabilized 3U CubeSat, is determined using only an estimate of the solar vector obtained from solar panel currents. The filter is based upon the existing multiplicative extended Kalman filter (MEKF) but instead of relying on gyros to drive the motion model, the filter instead incorporates a model of the spacecraft's attitude dynamics in the motion model. An attitude determination accuracy of five degrees is demonstrated, a performance verified using flight data from the University of Michigan's RAX-1. Although the filter was designed for the specific problem of a satellite without gyros or attitude determination it could also be used to provide smoothing of noisy gyro signals or to provide a backup in the event of gyro failures. C1 [Burton, R.; Rock, S.] Stanford Univ, 496 Lomita Mall, Stanford, CA 94305 USA. [Burton, R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Burton, R.] Millennium Engn & Integrat Serv, 2231 Crystal Dr, Arlington, VA 22202 USA. [Springmann, J.; Cutler, J.] Univ Michigan, 1320 Beal Ave, Ann Arbor, MI 48109 USA. RP Burton, R (reprint author), Stanford Univ, 496 Lomita Mall, Stanford, CA 94305 USA. FU National Aeronautics and Space Administration [NNX09AD83G]; U.S. National Science Foundation [AGS 08-38054, AGS 08-28046] FX The research described in this paper was funded by a grant from the National Aeronautics and Space Administration (Grant no. NNX09AD83G). Orbital data for the O/OREOS spacecraft was provided by Santa Clara University. Orbital data for the RAX-1 spacecraft was provided by the University of Michigan. RAX-1 was funded by the U.S. National Science Foundation (Grant nos. AGS 08-38054 and AGS 08-28046). NR 15 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD APR PY 2017 VL 133 BP 269 EP 281 DI 10.1016/j.actaastro.2017.01.024 PG 13 WC Engineering, Aerospace SC Engineering GA EO8NS UT WOS:000396946700026 ER PT J AU Payler, SJ Biddle, JF Coates, AJ Cousins, CR Cross, RE Cullen, DC Downs, MT Direito, SOL Edwards, T Gray, AL Genis, J Gunn, M Hansford, GM Harkness, P Holt, J Josset, JL Li, X Lees, DS Lim, DSS Mchugh, M Mcluckie, D Meehan, E Paling, SM Souchon, A Yeoman, L Cockell, CS AF Payler, Samuel J. Biddle, Jennifer F. Coates, Andrew J. Cousins, Claire R. Cross, Rachel E. Cullen, David C. Downs, Michael T. Direito, Susana O. L. Edwards, Thomas Gray, Amber L. Genis, Jac Gunn, Matthew Hansford, Graeme M. Harkness, Patrick Holt, John Josset, Jean-Luc Li, Xuan Lees, David S. Lim, Darlene S. S. Mchugh, Melissa Mcluckie, David Meehan, Emma Paling, Sean M. Souchon, Audrey Yeoman, Louise Cockell, Charles S. TI Planetary science and exploration in the deep subsurface: results from the MINAR Program, Boulby Mine, UK SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY LA English DT Article DE Analog research; deep subsurface; habitability; instrument testing; spin-off ID X-RAY-DIFFRACTION; MARS; ANALOG; INSTRUMENT; ENVIRONMENT; PANCAM; WATER; EARTH; ROCK AB The subsurface exploration of other planetary bodies can be used to unravel their geological history and assess their habitability. On Mars in particular, present-day habitable conditions may be restricted to the subsurface. Using a deep subsurface mine, we carried out a program of extraterrestrial analog research - MINe Analog Research (MINAR). MINAR aims to carry out the scientific study of the deep subsurface and test instrumentation designed for planetary surface exploration by investigating deep subsurface geology, whilst establishing the potential this technology has to be transferred into the mining industry. An integrated multi-instrument suite was used to investigate samples of representative evaporite minerals from a subsurface Permian evaporite sequence, in particular to assess mineral and elemental variations which provide small-scale regions of enhanced habitability. The instruments used were the Panoramic Camera emulator, Close-Up Imager, Raman spectrometer, Small Planetary Linear Impulse Tool, Ultrasonic drill and handheld X-ray diffraction (XRD). We present science results from the analog research and show that these instruments can be used to investigate in situ the geological context and mineralogical variations of a deep subsurface environment, and thus habitability, from millimetre to metre scales. We also show that these instruments are complementary. For example, the identification of primary evaporite minerals such as NaCl and KCl, which are difficult to detect by portable Raman spectrometers, can be accomplished with XRD. By contrast, Raman is highly effective at locating and detecting mineral inclusions in primary evaporite minerals. MINAR demonstrates the effective use of a deep subsurface environment for planetary instrument development, understanding the habitability of extreme deep subsurface environments on Earth and other planetary bodies, and advancing the use of space technology in economic mining. C1 [Payler, Samuel J.; Direito, Susana O. L.; Cockell, Charles S.] Univ Edinburgh, UK Ctr Astrobiol, Sch Phys & Astron, Kings Bldgs, Edinburgh EH9 3JZ, Midlothian, Scotland. [Biddle, Jennifer F.] Univ Delaware, Coll Earth Ocean & Environm, Delaware, DC USA. [Coates, Andrew J.] UCL, Mullard Space Sci Lab, London, England. [Cross, Rachel E.] Univ St Andrews, Dept Earth & Environm Sci, Irvine Bldg, St Andrews KY16 9AL, Fife, Scotland. [Cross, Rachel E.] Aberystwyth Univ, Inst Math Phys & Comp Sci IMPaCS, Aberystwyth, Dyfed, Wales. [Cullen, David C.] Cranfield Univ, Sch Aerosp Transport & Mfg, Space Grp, Cranfield, Beds, England. [Downs, Michael T.; Gray, Amber L.] Kennedy Space Ctr, Kennedy Space Ctr, FL USA. [Edwards, Thomas; Genis, Jac; Mcluckie, David] Cleveland Potash Ltd, Cleveland, England. [Gray, Amber L.] Blekinge Inst Technol, Karlskrona, Sweden. [Hansford, Graeme M.; Holt, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England. [Harkness, Patrick; Li, Xuan] Univ Glasgow, Sch Engn, Glasgow, Lanark, Scotland. [Josset, Jean-Luc; Souchon, Audrey] Space Explorat Inst, Neuchatel, Switzerland. [Lees, David S.; Lim, Darlene S. S.] Bay Area Environm Res Inst BAERI, 625 2nd St Ste 209, Petaluma, CA 94952 USA. [Lim, Darlene S. S.] NASA, Ames Res Ctr, Mail Stop 245-3, Moffett Field, CA 94035 USA. [Meehan, Emma; Paling, Sean M.; Yeoman, Louise] STFC Boulby Underground Sci Facil, Cleveland, England. RP Payler, SJ (reprint author), Univ Edinburgh, UK Ctr Astrobiol, Sch Phys & Astron, Kings Bldgs, Edinburgh EH9 3JZ, Midlothian, Scotland. EM S.J.Payler@ed.ac.uk FU MINAR program; STFC Impact Acceleration Fund; Royal Society of Edinburgh Research Fellowship; UK Space Agency; European Community's Seventh Framework Program FX We thank The Crown Estate, as mineral owner for the part of the mine beneath the seabed, for generous support of the MINAR program. Equally, we thank ICL for extensive logistical support at Boulby. We would also like to acknowledge the funding provided by the STFC Impact Acceleration Fund. Claire R. Cousins is supported by a Royal Society of Edinburgh Research Fellowship. The development of the ExoMars PanCam, the AUPE2 system and the PanCam data processing pipeline has been supported by funding from the UK Space Agency (lead funding agency) and the European Community's Seventh Framework Program. NR 41 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1473-5504 EI 1475-3006 J9 INT J ASTROBIOL JI Int. J. Astrobiol. PD APR PY 2017 VL 16 IS 2 BP 114 EP 129 DI 10.1017/S1473550416000045 PG 16 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA EM7KG UT WOS:000395489300002 ER PT J AU Fredsgaard, C Moore, DB Al Soudi, AF Crisler, JD Chen, F Clark, BC Schneegurt, MA AF Fredsgaard, Casper Moore, Donald B. Al Soudi, Amer F. Crisler, James D. Chen, Fei Clark, Benton C. Schneegurt, Mark A. TI Relationships between sucretolerance and salinotolerance in bacteria from hypersaline environments and their implications for the exploration of Mars and the icy worlds SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY LA English DT Article DE extreme environments; salinity tolerance; sucrose; sugar tolerance ID GREAT SALT PLAINS; WATER ACTIVITY; MICROBIAL STABILITY; MAGNESIUM-SULFATE; GROWTH; SURFACE; LIFE; MINERALS; DYNAMICS; OKLAHOMA AB The most extremely osmotolerant microbial isolates are fungi from high-sugar environments that tolerate the lowest water activity (0.61) for growth yet reported. Studies of osmotolerant bacteria have focused on halotolerance rather than sucretolerance (ability to grow in high sugar concentrations). A collection of salinotolerant (>= 10% NaCl or >= 50% MgSO4) bacterial isolates from the Great Salt Plains of Oklahoma and Hot Lake in Washington were screened for sucretolerance in medium supplemented with >= 50% fructose, glucose or sucrose. Tolerances significantly differed between solutes, even though water activities for saline media (0.92 and 0.85 for 10 and 20% NaCl Salt Plains media, respectively) were comparable or lower than water activities for high-sugar media (0.93 and 0.90 for 50 and 70% sucrose artificial nectar media, respectively). These specific solute effects were differentially expressed among individual isolates. Extrapolating the results of earlier food science studies with yeasts at high sugar concentrations to bacteria in salty environments with low water activity should be done with caution. Furthermore, the discussion of habitable Special Regions on Mars and the icy worlds should reflect an understanding of specific solute effects. C1 [Fredsgaard, Casper; Moore, Donald B.; Al Soudi, Amer F.; Crisler, James D.; Schneegurt, Mark A.] Wichita State Univ, Dept Biol Sci, Wichita, KS 67208 USA. [Chen, Fei] NASA, Jet Prop Lab, Planetary Protect Grp, Pasadena, CA USA. [Clark, Benton C.] Space Sci Inst, Boulder, CO USA. RP Schneegurt, MA (reprint author), Wichita State Univ, Dept Biol Sci, Wichita, KS 67208 USA. EM mark.schneegurt@wichita.edu FU NASA ROSES Planetary Protection Research [09-PPR09-0004, 14-PPR14-2-0002]; INBRE NIH NIGMS IDeA [P20 GM103418]; Flossie E. West Memorial Trust Foundation FX The authors are grateful for the contributions of Todd Caton, Timothy Eberl, Brian Kilmer, Tammy Kurz, Hieu Nguyen, Christopher Rogers, and Noah Schneegurt. We thank Fadi Aramouni for performing water activity measurements. Preliminary accounts of thiswork have been presented previously and abstracted ( Fredsgaard et al. 2013, 2014). This work was supported by awards from NASA ROSES Planetary Protection Research (09-PPR09-0004 and 14-PPR14-2-0002), Kansas INBRE NIH NIGMS IDeA (P20 GM103418) and The Flossie E. West Memorial Trust Foundation. NR 41 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1473-5504 EI 1475-3006 J9 INT J ASTROBIOL JI Int. J. Astrobiol. PD APR PY 2017 VL 16 IS 2 BP 156 EP 162 DI 10.1017/S1473550416000240 PG 7 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA EM7KG UT WOS:000395489300006 ER PT J AU Corbetta, M Saxena, A Giglio, M Goebel, K AF Corbetta, Matteo Saxena, Abhinav Giglio, Marco Goebel, Kai TI An investigation of strain energy release rate models for real-time prognosis of fiber-reinforced laminates SO COMPOSITE STRUCTURES LA English DT Article DE CFRP; Fatigue; Damage estimation; Energy release rate; Structural health monitoring; Damage prognosis ID HOLE COMPOSITE SPECIMENS; DAMAGE DEVELOPMENT; FATIGUE DAMAGE; MATRIX CRACKING; DELAMINATION; IDENTIFICATION; STRESSES; GROWTH; WAVES; LIFE AB Technological advancements in real-time distributed sensing and processing for structural health monitoring systems have enabled exploration of the next frontier in structural health monitoring for in situ condition-based prediction of remaining life of damaged or aging structures. In that context, model based prognostics methods have shown considerable promising results. These methods require that suitable damage progression models are available or be developed. Recent works have shown that energy release rate models work effectively for predicting material stiffness degradation based on matrix cracking. However, since delamination and matrix-cracking damage modes are known to co-exist and fuel each other's progression, it is desirable to investigate extension of these models for multiple damage modes. To that end, this paper analyzes several multiple damage-mode models from composite modeling literature and assesses them against experimental data from run-to-failure aging experiments. These models aim to estimate and correlate strain energy release rate and the residual stiffness as a function of the damage extent. Model review in this work reports modeling behavior and mathematical complexity along with strengths and limitations of these models. This is expected to guide selection of suitable model for a more robust prognostic solution generalized for more realistic degradation scenarios. (C) 2017 Elsevier Ltd. All rights reserved. C1 [Corbetta, Matteo; Giglio, Marco] Politecn Milan, Dipartimento Meccan, Via La Masa 1, I-20156 Milan, Italy. [Saxena, Abhinav] Gen Elect Global Res, San Ramon, CA 94583 USA. [Goebel, Kai] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Corbetta, M (reprint author), Politecn Milan, Dipartimento Meccan, Via La Masa 1, I-20156 Milan, Italy. EM matteo.corbetta@polimi.it FU NASA [NNX12-AK33A] FX The material is based upon work supported by NASA under award No: NNX12-AK33A. The authors would like to thank Prof. Fu-Kuo Chang, Dr. Cecilia Larrosa, and the Structures and Composites Laboratory at Stanford University for performing the fatigue tests of the dataset used in this article. The first author would like to thank the Prognostics Center of Excellence at NASA Ames Research Center, which kindly hosted him during the course of this work, and the University Space Research Association (USRA). NR 45 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0263-8223 EI 1879-1085 J9 COMPOS STRUCT JI Compos. Struct. PD APR 1 PY 2017 VL 165 BP 99 EP 114 DI 10.1016/j.compstruct.2017.01.002 PG 16 WC Materials Science, Composites SC Materials Science GA EL2UD UT WOS:000394474800010 ER PT J AU Nordheim, TA Hand, KP Paranicas, C Howett, CJA Hendrix, AR Jones, GH Coates, AJ AF Nordheim, T. A. Hand, K. P. Paranicas, C. Howett, C. J. A. Hendrix, A. R. Jones, G. H. Coates, A. J. TI The near-surface electron radiation environment of Saturn's moon Mimas SO ICARUS LA English DT Article ID E-RING PARTICLES; ICY SATELLITES; INNER MAGNETOSPHERE; INTERPLANETARY DUST; ENCELADUS; PLASMA; BOMBARDMENT; TEMPERATURE; DYNAMICS; VICINITY AB Saturn's inner mid-size moons are exposed to a number of external weathering processes, including charged particle bombardment and UV photolysis, as well as deposition of E-ring grains and interplanetary dust. While optical remote sensing observations by several instruments onboard the Cassini spacecraft have revealed a number of weathering patterns across the surfaces of these moons, it is not entirely clear which external process is responsible for which observed weathering pattern. Here we focus on Saturn's moon Mimas and model the effect of energetic electron bombardment across its surface. By using a combination of a guiding center, bounce-averaged charged particle tracing approach and a particle physics code, we investigate how the radiation dose due to energetic electrons is deposited with depth at different locations. We predict a lens-shaped electron energy deposition pattern that extends down to cm depths at low latitudes centered around the apex of the leading hemisphere (90 degrees W). These results are consistent with previous remote sensing observations of a lens-shaped color anomaly observed by the Imaging Science Subsystem (ISS) instrument as well as a thermal inertia anomaly observed by the Visual and Infrared Mapping Spectrometer (VIMS) and the Composite Infrared Spectrometer (CIRS). Our results confirm that these features are produced by MeV electrons that have a penetration depth into the surface comparable to the effective sampling depths of these instruments. On the trailing hemisphere we predict a similar lens-shaped electron energy deposition pattern, whose effects have to date not been observed by the Cassini remote sensing instruments. We suggest that no corresponding lens-shaped weathering pattern has been observed on the trailing hemisphere because of the comparatively short range of lower energy (<1 MeV) electrons into surface ice, as well as competing effects from cold plasma, neutral, and dust bombardment. (C) 2017 Elsevier Inc. All rights reserved. C1 [Nordheim, T. A.; Hand, K. P.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Paranicas, C.] Johns Hopkins Univ, Appl Phys Lab, 11100 John Hopkins Rd, Laurel, MD 20723 USA. [Howett, C. J. A.] Southwest Res Inst, 1050 Walnut St,Suite 300, Boulder, CO 80304 USA. [Hendrix, A. R.] Planetary Sci Inst, 1700 East Ft Lowell,Suite 106, Tucson, AZ 85719 USA. [Jones, G. H.; Coates, A. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Jones, G. H.; Coates, A. J.] UCL, Ctr Planetary Sci UCL Birkbeck, London WC1E 6BT, England. RP Nordheim, TA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM tom.nordheim@jpl.nasa.gov OI Coates, Andrew/0000-0002-6185-3125; Jones, Geraint/0000-0002-5859-1136 FU Jet Propulsion Laboratory, California Institute of Technology under NASA; NASA Cassini Data Analysis program [NNX12AC23G]; UK Science and Technology Facilities Council FX This research was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory administered by Oak Ridge Associated Universities and Universities Space Research Association through a contract with the National Aeronautics and Space Administration (NASA). K. P. Hand acknowledges support from the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the NASA. C. Howett would like to thank the NASA Cassini Data Analysis program, which partly funded this work (NNX12AC23G). AJC and GHJ acknowledge support by the UK Science and Technology Facilities Council. NR 54 TC 0 Z9 0 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD APR PY 2017 VL 286 BP 56 EP 68 DI 10.1016/j.icarus.2017.01.002 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EL1VI UT WOS:000394409100005 ER PT J AU Buhler, PB Ingersoll, AP Ehlmann, BL Fassett, CI Head, JW AF Buhler, Peter B. Ingersoll, Andrew P. Ehlmann, Bethany L. Fassett, Caleb I. Head, James W. TI How the martian residual south polar cap develops quasi-circular and heart-shaped pits, troughs, and moats SO ICARUS LA English DT Article ID SUBLIMATION-DRIVEN ACTIVITY; CO2 ICE; HIRISE OBSERVATIONS; CARBON-DIOXIDE; MARS; EVOLUTION; SURFACE; STRATIGRAPHY; CONSTRAINTS; DEPOSITION AB The martian Residual South Polar Cap (RSPC) is a 1-10 m thick deposit of permanent CO2 ice perched on the much larger H2O ice cap. The CO2 ice is dissected into mesas by erosional landforms that can be broadly classified as (i) quasi-circular pits, (ii) heart-shaped pits, (iii) linear troughs, and (iv) moats. We use HiRISE (25-50 cm/px) images taken at a cadence of days to months to track meter-scale changes in the RSPC in order to investigate the mechanisms that lead to the development of these four distinct morphologies. For the first time, we report the development of dark fans on the sides of the CO2 mesas and the fracturing and deterioration of the initially smooth upper surface of CO2 mesas. We interpret these features as indicating the sublimation and subsequent escape of CO2 from the interiors of mesas, which undermines structural support of mesa tops, causing them to collapse. The collapse of mesa tops, along with uneven deposition of CO2 ice, creates steep scarps that erode during the summer due to preferential sunlight absorption. During the winter, CO2 deposition acts to smooth topography, creating gently sloping ramps. We propose that the interplay between the steep scarps and gentle slopes leads to either quasi-circular pits, heart-shaped pits, linear troughs, or moats, depending on local conditions. (C) 2017 The Authors. Published by Elsevier Inc. C1 [Buhler, Peter B.; Ingersoll, Andrew P.; Ehlmann, Bethany L.] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. [Ehlmann, Bethany L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Fassett, Caleb I.] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. [Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. RP Buhler, PB (reprint author), CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. EM bpeter@caltech.edu FU NESSF grant [16-PLANET16F-0071]; MFRP grant [NNX14AG54G] FX We gratefully acknowledge funding from NESSF grant #16-PLANET16F-0071 and MFRP grant #NNX14AG54G. We also thank Timothy Titus and an anonymous reviewer for their feedback, which helped to improve this work. NR 49 TC 0 Z9 0 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD APR PY 2017 VL 286 BP 69 EP 93 DI 10.1016/j.icarus.2017.01.012 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EL1VI UT WOS:000394409100006 ER PT J AU Fletcher, LN Orton, GS Rogers, JH Giles, RS Payne, AV Irwin, PGJ Vedovato, M AF Fletcher, Leigh N. Orton, G. S. Rogers, J. H. Giles, R. S. Payne, A. V. Irwin, P. G. J. Vedovato, M. TI Moist convection and the 2010-2011 revival of Jupiter's South Equatorial Belt SO ICARUS LA English DT Article DE Jupiter; Atmospheres composition; Atmospheres dynamics ID INFRARED TELESCOPE FACILITY; SATURNS THERMAL EMISSION; GALILEO PROBE DATA; GREAT WHITE SPOT; DYNAMICAL IMPLICATIONS; SPATIAL-DISTRIBUTION; CLOUD VARIABILITY; 2.2-CM WAVELENGTH; UPPER TROPOSPHERE; 2009-2010 FADE AB The transformation of Jupiter's South Equatorial Belt (SEB) from its faded, whitened state in 2009-2010 (Fletcher et al., 2011b) to its normal brown appearance is documented via comparisons of thermal infrared (5-20 mu m) and visible-light imaging between November 2010 and November 2011. The SEB revival consisted of convective eruptions triggered over similar to 100 days, potentially powered by the latent heat released by the condensation of water. The plumes rise from the water cloud base and ultimately diverge and cool in the stably-stratified upper troposphere. Thermal-IR images from the Very Large Telescope (VLT) were acquired 2 days after the SEB disturbance was first detected as a small white spot by amateur observers on November 9th 2010. Subsequent images over several months revealed the cold, putatively anticyclonic and cloudy plume tops (area 2.5 x 10(6) km(2)) surrounded by warm, cloud-free conditions at their peripheries due to subsidence. The latent heating was not directly detectable in the 5-20 mu m range. The majority of the plumes erupted from a single source near 140 - 160 degrees W, coincident with the remnant cyclonic circulation of a brown barge that had formed during the fade. The warm remnant of the cyclone could still be observed in IRTF imaging 5 days before the November 9th eruption. Additional plumes erupted from the leading edge of the central disturbance immediately east of the source, which propagated slowly eastwards to encounter the Great Red Spot. The tropospheric plumes were sufficiently vigorous to excite stratospheric thermal waves over the SEB with a 20 - 30 degrees longitudinal wavelength and 5-6 K temperature contrasts at 5 mbar, showing a direct connection between moist convection and stratospheric wave activity. The subsidence and compressional heating of dry, unsaturated air warmed the troposphere (particularly to the northwest of the central branch of the revival) and removed the aerosols that had been responsible for the fade. Dark, cloud-free lanes west of the plumes were the first to show the colour change, and elongated due to the zonal windshear to form the characteristic 'S-shape' of the revival complex. The aerosol-free air was redistributed and mixed throughout the SEB by the zonal flow, following a westward-moving southern branch and an eastward-moving northern branch that revived the brown colouration over-200 days. The transition from the cool conditions of the SEBZ during the fade to the revived SEB caused a 2-4 K rise in 500-mbar temperatures (leaving a particularly warm southern SEB) and a reduction of aerosol opacity by factors of 2-3. Newly-cleared gaps in the upper tropospheric aerosol layer appeared different in filters sensing the similar to 700-mbar cloud deck and the 2-3 bar cloud deck, suggesting complex vertical structure in the downdrafts. The last stage of the revival was the re-establishment of normal convective activity northwest of the GRS in September 2011, similar to 840 days after the last occurrence in June 2009. Moist convection may therefore play an important role in controlling the timescale and atmospheric variability during the SEB life cycle. (C) 2017 The Authors. Published by Elsevier Inc. C1 [Fletcher, Leigh N.] Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. [Orton, G. S.; Payne, A. V.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Rogers, J. H.] British Astron Assoc, Burlington House, London W1J 0DU, England. [Giles, R. S.; Irwin, P. G. J.] Univ Oxford, Dept Phys, Clarendon Lab, Atmospher Ocean & Planetary Phys, Parks Rd, Oxford OX1 3PU, England. [Vedovato, M.] Unione Astrofili Italiani, JUPOS Team, Rome, Italy. RP Fletcher, LN (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. EM leigh.fletcher@leicester.ac.uk FU Royal Society Research Fellowship at the University of Leicester; Royal Society research grant at the University of Oxford; Science and Technology Facilities Council (STFC); ESO Very Large Telescope Paranal UT3/Melipal Observatory using Directors Discretionary Time [286.C-5009, 087.C-0024]; National Astronomical Observatory of Japan [011154]; University of Hawaii [NNH14CK55B]; National Aeronautics and Space Administration [2010B010, 2011A010, 2011B027]; Association of Universities for Research in Astronomy, Inc. [GN-2010B-DD-3, GS-2010B-Q-8, GS-2011A-Q-11]; National Science Foundation (United States); National Research Council (Canada); CONICYT (Chile); Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina); Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) FX Fletcher was supported by a Royal Society Research Fellowship at the University of Leicester, Giles was supported by a Royal Society research grant at the University of Oxford. The UK authors acknowledge the support of the Science and Technology Facilities Council (STFC). A portion of this work was performed by Orton and Payne at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This research used the ALICE High Performance Computing Facility at the University of Leicester. We are extremely grateful for the combined efforts of the numerous amateur observers (including those listed in the figure captions) for sharing their data, and for the JUPOS software developed by Grischa Hahn and Hans-Jorg Mettig to reproject the visible-light data.; This investigation was partially based on thermal-infrared observations acquired at (i) the ESO Very Large Telescope Paranal UT3/Melipal Observatory using Directors Discretionary Time (program ID 286.C-5009) and regular service time (program ID 087.C-0024); (ii) the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan (program ID 011154); (iii) NASA's Infrared Telescope Facility, which is operated by the University of Hawaii under contract NNH14CK55B with the National Aeronautics and Space Administration (program IDs 2010B010, 2011A010, 2011B027); and (iv) observations obtained at the Gemini Observatory (program IDs GN-2010B-DD-3, GS-2010B-Q-8 and GS-2011A-Q-11), 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). We wish to recognise and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 80 TC 0 Z9 0 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD APR PY 2017 VL 286 BP 94 EP 117 DI 10.1016/j.icarus.2017.01.001 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EL1VI UT WOS:000394409100007 ER PT J AU Nayak, M Hemingway, D Garrick-Bethell, I AF Nayak, Michael Hemingway, Doug Garrick-Bethell, Ian TI Magnetization in the South Pole-Aitken basin: Implications for the lunar dynamo and true polar wander SO ICARUS LA English DT Article DE Moon; Magnetic fields; Impact processes ID SOLAR-WIND; SEAMOUNT MAGNETISM; MOON; ANOMALIES; PROSPECTOR; SURFACE; FIELDS; CRATERS; DRIVEN; MODEL AB A number of magnetic anomalies are present along the northern edge of the lunar South Pole-Aitken (SPA) basin. A variety of hypotheses for their formation have been proposed, but an in-depth study of their properties has not been performed. Here we use two different methods to invert for their source body characteristics: one that completely searches a small parameter space of less than ten uniform strength dipoles per anomaly, and another that uses grids of hundreds of dipoles with variable magnetization strengths. Both methods assume uniform magnetization directions at each anomaly and with one exception, produce nearly the same results. We introduce new Monte Carlo methods to quantify errors in our inversions arising from Gaussian time-dependent changes in the external field and the uncertain geometry of the source bodies. We find the errors from uncertainty in source body geometry are almost always higher. We also find a diverse set of magnetization directions around SPA, which we combine with other physical arguments to conclude that the source bodies were likely magnetized in a dynamo field. Igneous intrusions are a reasonable explanation (Purucker et al., 2012) for the directional variability, since they could be intruded over different magnetic epochs. However, the directional variability also implies either surprisingly large amounts of true polar wander or a dynamo not aligned with the lunar spin axis. We also explore the possibility that true polar wander caused by the SPA impact could allow iron-rich SPA ejecta to record a diverse set of magnetic field directions. Some of this material may have also become "sesquinary" ejecta and re-impacted across the Moon on 10(4)-10(6) year timescales to capture such changes. No completely satisfactory answer emerges, except that the dipole-axis of the lunar dynamo may have been variable in direction. Published by Elsevier Inc. C1 [Nayak, Michael; Hemingway, Doug; Garrick-Bethell, Ian] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, 1156 High St, Santa Cruz, CA 95064 USA. [Nayak, Michael] Red Sky Res LLC, 67 Northland Meadows Dr, Edgewood, NM 87105 USA. [Garrick-Bethell, Ian] Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi Do, South Korea. [Nayak, Michael] NASA Ames Res Ctr, Planetary Syst Branch SST, Moffett Field, CA 94035 USA. [Nayak, Michael] AFRL, Maui High Performance Comp Ctr, Wright Patterson AFB, OH USA. [Hemingway, Doug] Univ Calif Berkeley, Dept Earth & Planetary Sci, Miller Inst Basic Res Sci, Berkeley, CA 94720 USA. RP Nayak, M (reprint author), Univ Calif Santa Cruz, Dept Earth & Planetary Sci, 1156 High St, Santa Cruz, CA 95064 USA. EM mnayak@ucsc.edu FU NASA Discovery [NNX16AJO7G]; BK21 plus program through the National Research Foundation (NRF) - Ministry of Education of Korea; National Defense Science and Engineering Graduate (NDSEG) Fellowship - Air Force Office of Scientific Research, Department of Defense [32 CFR 168a]; Alfred P. Sloan Foundation; UC Santa Cruz / NASA Ames University Affiliated Research Center, Aligned Research Program; Red Sky Research, LLC FX This research was supported by the NASA Discovery Data Analysis Program (grant NNX16AJO7G), and the BK21 plus program through the National Research Foundation (NRF), funded by the Ministry of Education of Korea. MN acknowledges support from the National Defense Science and Engineering Graduate (NDSEG) Fellowship, 32 CFR 168a, funded by the Air Force Office of Scientific Research, Department of Defense. Partial support was also provided by (1) The Alfred P. Sloan Foundation, (2) The UC Santa Cruz / NASA Ames University Affiliated Research Center, Aligned Research Program and (3) Red Sky Research, LLC. Thanks to Rob Coe and Gary Glatzmaier for helpful comments. Opinions, interpretations and recommendations expressed are those of the authors and are not necessarily endorsed by the US Air Force or the Department of Defense. NR 50 TC 0 Z9 0 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD APR PY 2017 VL 286 BP 153 EP 192 DI 10.1016/j.icarus.2016.09.038 PG 40 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EL1VI UT WOS:000394409100011 ER PT J AU Fletcher, LN de Pater, I Reach, WT Wong, M Orton, GS Irwin, PGJ Gehrz, RD AF Fletcher, Leigh N. de Pater, I. Reach, W. T. Wong, M. Orton, G. S. Irwin, P. G. J. Gehrz, R. D. TI Jupiter's para-H-2 distribution from SOFIA/FORCAST and Voyager/IRIS 17-37 mu m spectroscopy SO ICARUS LA English DT Article DE Jupiter; Atmospheres; Composition; Atmospheres; Dynamics ID GREAT-RED-SPOT; COLLISION-INDUCED ABSORPTION; PARA-HYDROGEN FRACTION; THERMAL STRUCTURE; JOVIAN ATMOSPHERE; TROPOSPHERIC TEMPERATURES; INFRARED OBSERVATIONS; OUTER PLANETS; CASSINI-CIRS; SPATIAL-ORGANIZATION AB Spatially resolved maps of Jupiter's far-infrared 17-37 pm hydrogen-helium collision-induced spectrum were acquired by the FORCAST instrument on the Stratospheric Observatory for Infrared Astronomy (SOFIA) in May 2014. Spectral scans in two grisms covered the broad S(0) and S(1) absorption lines, in addition to contextual imaging in eight broad-band filters (5-37 mu m) with spatial resolutions of 2-4". The spectra were inverted to map the zonal-mean temperature and para-H-2 distribution (f(p), the fraction of the para spin isomer with respect to the ortho spin isomer) in Jupiter's upper troposphere (the 100700 mbar range). We compared these to a reanalysis of Voyager-1 and -2 IRIS spectra covering the same spectral range. Tropospheric temperature contrasts match those identified by Voyager in 1979, within the limits of temporal variability consistent with previous investigations. Para-H-2 increases from equator to pole, with low fp air at the equator representing sub-equilibrium conditions (i.e., less para-H-2 than expected from thermal equilibration), and high fp air and possible super-equilibrium at higher latitudes. In particular, we confirm the continued presence of a region of high f(p) air at high northern latitudes discovered by Voyager/IRIS, and an asymmetry with generally higher f(p) in the north than in the south. Far-IR aerosol opacity is not required to fit the data, but cannot be completely ruled out. We note that existing collision-induced absorption databases lack opacity from (H-2)(2) dimers, leading to under-prediction of the absorption near the S(0) and S(1) peaks. There appears to be no spatial correlation between para-H-2 and tropospheric ammonia, phosphine and cloud opacity derived from Voyager/IRIS at mid-infrared wavelengths (7-15 mu m). We note, however, that para-H-2 tracks the similar latitudinal distribution of aerosols within Jupiter's upper tropospheric and stratospheric hazes observed in reflected sunlight, suggesting that catalysis of hydrogen equilibration within the hazes (and not the main clouds) may govern the equator to-pole gradient, with conditions closer to equilibrium at higher latitudes. This gradient is superimposed onto smaller-scale variations associated with regional advection of para-H-2 at the equator and poles. (C) 2016 The Authors. Published by Elsevier Inc. C1 [Fletcher, Leigh N.] Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. [de Pater, I.; Wong, M.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, NASA Ames Res Ctr, Mail Stop 232-11, Moffett Field, CA 94035 USA. [Orton, G. S.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Irwin, P. G. J.] Univ Oxford, Clarendon Lab, Dept Phys, Atmospher Ocean & Planetary Phys, Parks Rd, Oxford OX1 3PU, England. [Gehrz, R. D.] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, 116 Church St,SE, Minneapolis, MN 55455 USA. RP Fletcher, LN (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. EM leigh.fletcher@leicester.ac.uk FU NASA [NAS297001]; Deutsches SOFIA Institut (DSI) under DLR [50 OK 0901]; Royal Society Research Fellowship at the University of Leicester; Science and Technology Facilities Council (STFC); United States Air Force; [SOF0012] FX This work was based on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA), and was financially supported through SOF0012 to the University of California, Berkeley. SOFIA is jointly operated by the Universities Space Research Association, Inc. (USRA), under NASA contract NAS297001, and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901 to the University of Stuttgart. We are grateful for all those involved in the telescope engineering, operations support and the flight crews. We thank Luke Keller, Matthew Bellardini and Joseph Quinn (Ithaca College) and Joseph Adams for their assistance with the initial planning and calibration of the SOFIA data. Fletcher was supported by a Royal Society Research Fellowship at the University of Leicester. The UK authors acknowledge the support of the Science and Technology Facilities Council (STFC). A portion of this work was performed by Orton at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Gehrz received partial support from the United States Air Force. This research used the ALICE High Performance Computing Facility at the University of Leicester. NR 71 TC 0 Z9 0 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD APR PY 2017 VL 286 BP 223 EP 240 DI 10.1016/j.icarus.2016.10.002 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EL1VI UT WOS:000394409100015 ER PT J AU Brozovic, M Benner, LAM Magri, C Scheeres, DJ Busch, MW Giorgini, JD Nolan, MC Jao, JS Lee, CG Snedeker, LG Silva, MA Lawrence, KJ Slade, MA Hicks, MD Howell, ES Taylor, PA Sanchez, JA Reddy, V Dykhuis, M Le Corre, L AF Brozovic, Marina Benner, Lance A. M. Magri, Christopher Scheeres, Daniel J. Busch, Michael W. Giorgini, Jon D. Nolan, Michael C. Jao, Joseph S. Lee, Clement G. Snedeker, Lawrence G. Silva, Marc A. Lawrence, Kenneth J. Slade, Martin A. Hicks, Michael D. Howell, Ellen S. Taylor, Patrick A. Sanchez, Juan A. Reddy, Vishnu Dykhuis, Melissa Le Corre, Lucille TI Goldstone radar evidence for short-axis mode non-principal-axis rotation of near-Earth asteroid (214869) 2007 PA8 SO ICARUS LA English DT Article DE Asteroids; Rotation; Radar observations ID SPIN-STATE; PHYSICAL MODEL; 4179 TOUTATIS; SHAPE MODEL; CONSTRAINTS; LIGHTCURVES; POPULATION; SURFACE; PHOTOMETRY; EVOLUTION AB We report radar and optical photometric observations of near-Earth asteroid (214869) 2007 PA8 obtained during October 2-November 13, 2012. We observed 2007 PA8 on sixteen days with Goldstone (8560 MHz, 3.5 cm) and on five days with the 0.6 m telescope at Table Mountain Observatory. Closest approach was on November 5 at a distance of 0.043 au. Images obtained with Goldstone's new chirp system achieved range resolutions as fine as 3.75 m, placing thousands of pixels on the asteroid's surface, and revealing that 2007 PA8 is an elongated, asymmetric object. Surface features include angularities, facets, and a concavity approximately 400 m in diameter. We used the Shape software to estimate the asteroid's 3D shape and spin state. 2007 PA8 has a broad, rounded end and a tapered, angular end with sharp-crested ridges. The asteroid's effective diameter is 1.35 +/- 0.07 km, which in combination with the absolute magnitude of 16.30 +/- 0.52 gives an optical albedo of pv = 0.29 +/- 0.14. The shape modeling of the radar data revealed that 2007 PA8 is a non-principal axis (NPA) rotator in the short-axis mode with an average period of precession by the long axis around the angular momentum vector of 4.26 +/- 0.02 days and an oscillatory period around the long axis of 20.55 +/- 3.75 days. The amplitude of rolling around the long axis is 42 +/- 7 degrees. The angular momentum vector points toward ecliptic longitude and latitude of 273.6 +/- 10 degrees, +16.9 +/- 5 degrees. 2007 PA8 is only the second confirmed short-axis mode NPA rotator known in the near-Earth asteroid population after (99942) Apophis (Pravec et al., 2014). 2007 PA8 has a geopotential high at the equator, where the equator is defined as the plane that contains the long and intermediate axis. This geopotential extreme could be interpreted as a large, hidden surface depression, or as evidence that 2007 PA8 is a multi-component body. (C) 2016 Elsevier Inc. All rights reserved. C1 [Brozovic, Marina; Benner, Lance A. M.; Giorgini, Jon D.; Jao, Joseph S.; Lee, Clement G.; Lawrence, Kenneth J.; Slade, Martin A.; Hicks, Michael D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Magri, Christopher] Univ Maine Farmington, Preble Hall, Farmington, ME 04938 USA. [Scheeres, Daniel J.] Univ Colorado, Aerosp Engn Sci, Boulder, CO 80309 USA. [Busch, Michael W.] SETI Inst, Mountain View, CA 94043 USA. [Nolan, Michael C.; Howell, Ellen S.] Univ Arizona, Tucson, AZ 85721 USA. [Snedeker, Lawrence G.; Silva, Marc A.] SAITECH, Goldstone Deep Space Commun Complex, Ft Irwin, CA 92310 USA. [Taylor, Patrick A.] Univ Space Res Assoc, Arecibo Observ, Arecibo, PR 00612 USA. [Sanchez, Juan A.; Reddy, Vishnu; Dykhuis, Melissa] Univ Arizona, Lunary & Planetary Lab, Tucson, AZ USA. [Le Corre, Lucille] Planetary Sci Inst, Tucson, AZ 85719 USA. RP Brozovic, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM marina.brozovic@jpl.nasa.gov FU NASA under the Science Mission Directorate Research and Analysis Programs; Human Exploration and Operations Mission Directorate Advanced Exploration Systems Program; National Radio Astronomy Observatory FX We thank the Goldstone technical and support staffs for help with the radar observations. This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). This material is based in part upon work supported by NASA under the Science Mission Directorate Research and Analysis Programs and the Human Exploration and Operations Mission Directorate Advanced Exploration Systems Program. Co-author M. W. Busch was partially supported by the National Radio Astronomy Observatory's Jansky Fellowship program. We thank two anonymous reviewers for suggestions that improved this manuscript. NR 65 TC 0 Z9 0 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD APR PY 2017 VL 286 BP 314 EP 329 DI 10.1016/j.icarus.2016.10.016 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EL1VI UT WOS:000394409100022 ER PT J AU Righter, K Go, BM Pando, KA Danielson, L Ross, DK Rahman, Z Keller, LP AF Righter, K. Go, B. M. Pando, K. A. Danielson, L. Ross, D. K. Rahman, Z. Keller, L. P. TI Phase equilibria of a low S and C lunar core: Implications for an early lunar dynamo and physical state of the current core SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE core dynamo; lunar paleomagnetism; Apollo seismic data; lunar laser ranging; lunar thermal history; core crystallization ID HIGH-PRESSURE IMPLICATIONS; IRON-SULFUR COMPOUND; SIDEROPHILE ELEMENTS; GIANT IMPACT; CONVECTION MODELS; MANTLE CONVECTION; MELTING RELATIONS; VOLCANIC GLASSES; SOUND-VELOCITY; SILICATE MELT AB Multiple lines of geochemical and geophysical evidence suggest the Moon has a small metallic core, yet the composition of the core is poorly constrained. The physical state of the core(now or in the past) depends on detailed knowledge of its composition, and unfortunately, there is little available data on relevant multicomponent systems (i. e., Fe-Ni-S-C) at lunar interior conditions. In particular, there is a dearth of phase equilibrium data to elucidate whether a specific core composition could help to explain an early lunar geodynamo and magnetic field intensities, or current solid inner core/liquid outer core states. We utilize geochemical information to estimate the Ni, S and C contents of the lunar core, and then carry out phase equilibria experiments on several possible core compositions at the pressure and temperature conditions relevant to the lunar interior. The first composition is 0.5 wt% S and 0.375 wt% C, based on S and C contents of Apollo glasses. A second composition contains 1 wt% each of S and C, and assumes that the lunar mantle experienced degassing of up to 50% of its S and C. Finally a third composition contains C as the dominant light element. Phase equilibrium experiments were completed at 1, 3 and 5 GPa, using piston cylinder and multi-anvil techniques. The first composition has a liquidus near 1550 degrees C and solidus near 1250 degrees C. The second composition has a narrower liquidus and solidus temperatures of 1400 and 1270 degrees C, respectively, while the third composition is molten down to 1150 degrees C. As the composition crystallizes, the residual liquid becomes enriched in S and C, but S enrichment is greater due to the incorporation of C (but not S) into solid metallic FeNi. Comparison of these results to thermal models for the Moon allow an evaluation of which composition is consistent with the geophysical data of an early dynamo and a currently solid inner and liquid outer core. Composition 1 has a high enough liquidus to start crystallizing early in lunar history (4.3 Ga), consistent with the possible core dynamo initiated by crystallization of a solid inner core. Composition 1 also stays partially molten throughout lunar history, and could easily explain the seismic data. Composition 2, on the other hand, can satisfy one or the other set of geophysical data, but not both and thus seems like a poor candidate for a lunar core composition. Composition 3 remains molten to temperatures that are lower than current estimates for the lunar core, thus ruling out the possibility of a C-rich (and S-poor) lunar core. The Sand C-poor core composition studied here (composition 1) is consistent with all available geochemical and geophysical data and provides a simple heat source and mechanism for a lunar core dynamo (core crystallization) that would obviate the need for other primary mechanisms such as impacts, core-mantle coupling, or unusual thermal histories. (C) 2017 Published by Elsevier B. V. C1 [Righter, K.] NASA, Johnson Space Ctr, Mailcode XI2,2101 NASA Pkwy, Houston, TX 77058 USA. [Go, B. M.] Univ Chicago, Dept Geophys Sci, 5801 S Ellis Ave, Chicago, IL 60637 USA. [Pando, K. A.; Danielson, L.; Ross, D. K.] NASA, Jacobs JETS, Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. [Rahman, Z.] NASA, Johnson Space Ctr, Jacobs, Houston, TX 77058 USA. [Keller, L. P.] NASA, Johnson Space Ctr, Mailcode XI3,2101 NASA Pkwy, Houston, TX 77058 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 the NASA LASER program; LPI Summer Internship FX This work was supported by an RTOP from the NASA LASER program to KR. Support for BMG was provided by an LPI Summer Internship. We thank M. Habermann and J. Rapp for support in the high pressure lab. Finally, we thank two anonymous reviewers for sensible advice which improved the clarity of this work. NR 76 TC 0 Z9 0 U1 2 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD APR 1 PY 2017 VL 463 BP 323 EP 332 DI 10.1016/j.epsl.2017.02.003 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EN3PA UT WOS:000395919200030 ER PT J AU Pulver, JR AF Pulver, J. R. TI Sink or swim? Factors affecting immediate discard mortality for the gulf of Mexico commercial reef fish fishery SO FISHERIES RESEARCH LA English DT Article DE Discard mortality; Reef fish; Grouper; Snapper; Barotrauma; Logistic regression ID RELEASE MORTALITY; RED SNAPPER; SURVIVAL; BAROTRAUMA; RECAPTURE; CAUGHT; COAST AB Fishery observer data collected from June 2006 through December 2015 in the Gulf of Mexico commercial reef fish fishery were examined to determine if any covariates available affected immediate discard mortality for six species: red grouper Epinephelus morio, red snapper Lutjanus campechanus, vermilion snapper Rhomboplites aurorubens, gag grouper Mycteroperca microlepis, scamp grouper Mycteroperca phenax, and speckled hind Epinephelus drummondhayi. Using logistic regression models, this study predicted immediate discard mortality was positively correlated with increased depths, seasons associated with warmer water temperatures, and external evidence of barotrauma. Additionally, bottom longline gear increased the predicted probability of immediate mortality compared to vertical line gear for all species except vermilion snapper. Air bladder venting significantly decreased the predicted probability of immediate mortality for all species except speckled hind. Future research incorporating tag-recapture data into the current observer program for the commercial reef fish fishery is vital to assess if condition assessment at release can be relied on as an accurate proxy for long-term survival. This research provides information that managers could potentially use to make more informed decisions when implementing measures such as changes to existing size limits, venting requirements, and seasonal, area, or gear restrictions intended to reduce unwanted discard mortality. Published by Elsevier B.V. C1 [Pulver, J. R.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Galveston Lab, 4700 Ave U, Galveston, TX 77551 USA. RP Pulver, JR (reprint author), Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Galveston Lab, 4700 Ave U, Galveston, TX 77551 USA. EM jeff.pulver@noaa.gov NR 22 TC 0 Z9 0 U1 0 U2 0 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 APR PY 2017 VL 188 BP 166 EP 172 DI 10.1016/j.fishres.2016.12.018 PG 7 WC Fisheries SC Fisheries GA EK7AG UT WOS:000394077100017 ER PT J AU Herzfeld, UC Trantow, TM Harding, D Dabney, PW AF Herzfeld, Ute C. Trantow, Thomas M. Harding, David Dabney, Philip W. TI Surface-Height Determination of Crevassed Glaciers-Mathematical Principles of an Autoadaptive Density-Dimension Algorithm and Validation Using ICESat-2 Simulator (SIMPL) Data SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Algorithms; altimetry; ice ID LASER ALTIMETER MEASUREMENTS; PHOTON-COUNTING LIDAR; SEA-LEVEL RISE; BERING GLACIER; JAKOBSHAVN ISBRAE; ELEVATION CHANGES; SATELLITE RADAR; ICE SHEETS; GREENLAND; MISSION AB Glacial acceleration is a main source of uncertainty in sea-level-change assessment. Measurement of ice-surface heights with a spatial and temporal resolution that not only allows elevation-change calculation, but also captures ice-surface morphology and its changes is required to aid in investigations of the geophysical processes associated with glacial acceleration. The Advanced Topographic Laser Altimeter System aboard NASA's future ICESat-2 Mission (launch 2017) will implement multibeam micropulse photon-counting lidar altimetry aimed at measuring ice-surface heights at 0.7-m along-track spacing. The instrument is designed to resolve spatial and temporal variability of rapidly changing glaciers and ice sheets and the Arctic sea ice. The new technology requires the development of a new mathematical algorithm for the retrieval of height information. We introduce the density-dimension algorithm (DDA) that utilizes the radial basis function to calculate a weighted density as a form of data aggregation in the photon cloud and considers density an additional dimension as an aid in autoadaptive threshold determination. The autoadaptive capability of the algorithm is necessary to separate returns from noise and signal photons under changing environmental conditions. The algorithm is evaluated using data collected with an ICESat-2 simulator instrument, the Slope Imaging Multi-polarization Photon-counting Lidar, over the heavily crevassed Giesecke Braer in Northwestern Greenland in summer 2015. Results demonstrate that ICESat-2 may be expected to provide ice-surface height measurements over crevassed glaciers and other complex ice surfaces. The DDA is generally applicable for the analysis of airborne and spaceborne micropulse photon-counting| lidar data over complex and simple surfaces. C1 [Herzfeld, Ute C.; Trantow, Thomas M.] Univ Colorado, Dept Elect Comp & Energy Engn, Geomath & Remote Sensing, Boulder, CO 80309 USA. [Herzfeld, Ute C.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Harding, David] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Dabney, Philip W.] NASA, Goddard Space Flight Ctr, Laser Remote Sensing Lab, Greenbelt, MD 20771 USA. RP Herzfeld, UC (reprint author), Univ Colorado, Dept Elect Comp & Energy Engn, Geomath & Remote Sensing, Boulder, CO 80309 USA.; Herzfeld, UC (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. EM ute.herzfeld@colorado.edu FU NASA Cryospheric Sciences FX The authors would like to thank B. McDonald and B. Wallin, former student members of our geomathematics group (ECEE and CIRES, University of Coloroado Boulder), for early contributions to algorithm development for the analysis of ICESat-2-type micropulse photon-counting lidar altimeter data over various surfaces. They would like to thank D. Hancock, K. Brunt, and K. Barbieri, all NASA Goddard Space Flight Center, for making SIMPL data available quickly and efficiently. They would also like to thank G. Medley, Geomathematics, CU Boulder, for assistance with data processing, and also A. Anker Bjork, University of Copenhagen, for help with identification of the names of the Giesecke Braer. SIMPL data can be downloaded from the ICESat-2 Web site under http://icesat.gsfc.nasa.gov/icesat2/data.php. SIMPL was developed by D. Harding, P. Dabney, and collaborators at the Solar System Exploration Division, NASA Goddard Space Flight Center, under the Instrument Incubator Program of the NASA Earth Science Technology Office. The DDA was developed by Ute Herzfeld and students at the Geomathematics and Remote Sensing Group, University of Colorado Boulder, under a grant from NASA Cryospheric Sciences. NR 52 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 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD APR PY 2017 VL 55 IS 4 BP 1874 EP 1896 DI 10.1109/TGRS.2016.2617323 PG 23 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA EO0NN UT WOS:000396394900002 ER PT J AU Kim, SB van Zyl, JJ Johnson, JT Moghaddam, M Tsang, L Colliander, A Dunbar, RS Jackson, TJ Jaruwatanadilok, S West, R Berg, A Caldwell, T Cosh, MH Goodrich, DC Livingston, S Lopez-Baeza, E Rowlandson, T Thibeault, M Walker, JP Entekhabi, D Njoku, EG O'Neill, PE Yueh, SH AF Kim, Seung-Bum van Zyl, Jakob J. Johnson, Joel T. Moghaddam, Matha Tsang, Leung Colliander, Andreas Dunbar, Roy Scott Jackson, Thomas J. Jaruwatanadilok, Sermsak West, Richard Berg, Aaron Caldwell, Todd Cosh, Michael H. Goodrich, David C. Livingston, Stanley Lopez-Baeza, Ernesto Rowlandson, Tracy Thibeault, Marc Walker, Jeffrey P. Entekhabi, Dara Njoku, Eni G. O'Neill, Peggy E. Yueh, Simon H. TI Surface Soil Moisture Retrieval Using the L-Band Synthetic Aperture Radar Onboard the Soil Moisture Active-Passive Satellite and Evaluation at Core Validation Sites SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Soil moisture; synthetic aperture radar (SAR); vegetation ID BACKSCATTERING COEFFICIENTS; SMAP MISSION; SAR DATA; MODEL; ALGORITHMS; VEGETATION; SCATTERING; ROUGHNESS; AIRBORNE; SERIES AB This paper evaluates the retrieval of soil moisture in the top 5-cm layer at 3-km spatial resolution using L-band dual-copolarized Soil Moisture Active-Passive (SMAP) synthetic aperture radar (SAR) data that mapped the globe every three days from mid-April to early July, 2015. Surface soil moisture retrievals using radar observations have been challenging in the past due to complicating factors of surface roughness and vegetation scattering. Here, physically based forward models of radar scattering for individual vegetation types are inverted using a time-series approach to retrieve soil moisture while correcting for the effects of static roughness and dynamic vegetation. Compared with the past studies in homogeneous field scales, this paper performs a stringent test with the satellite data in the presence of terrain slope, subpixel heterogeneity, and vegetation growth. The retrieval process also addresses any deficiencies in the forward model by removing any time-averaged bias between model and observations and by adjusting the strength of vegetation contributions. The retrievals are assessed at 14 core validation sites representing a wide range of global soil and vegetation conditions over grass, pasture, shrub, woody savanna, corn, wheat, and soybean fields. The predictions of the forward models used agree with SMAP measurements to within 0.5 dB unbiased-root-mean-square error (ubRMSE) and -0.05 dB (bias) for both copolarizations. Soil moisture retrievals have an accuracy of 0.052 m(3)/m(3) ubRMSE, -0.015 m(3)/m(3) bias, and a correlation of 0.50, compared to in situ measurements, thus meeting the accuracy target of 0.06 m(3)/m(3) ubRMSE. The successful retrieval demonstrates the feasibility of a physically based time series retrieval with L-band SAR data for characterizing soil moisture over diverse conditions of soil moisture, surface roughness, and vegetation. C1 [Kim, Seung-Bum; van Zyl, Jakob J.; Colliander, Andreas; Dunbar, Roy Scott; Jaruwatanadilok, Sermsak; West, Richard; Njoku, Eni G.; Yueh, Simon H.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Johnson, Joel T.] Ohio State Univ, Dept Elect & Comp Engn, Columbus, OH 43212 USA. [Johnson, Joel T.] Ohio State Univ, Electrosci Lab, Columbus, OH 43212 USA. [Moghaddam, Matha] Univ Southern Calif, Elect Engn, Los Angeles, CA 90089 USA. [Tsang, Leung] Univ Michigan, Ann Arbor, MI 48109 USA. [Jackson, Thomas J.; Cosh, Michael H.] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. [Berg, Aaron] Univ Guelph, Dept Geog, Hydrol & Remote Sensing, Guelph, ON N1G 2W1, Canada. [Rowlandson, Tracy] Univ Guelph, Dept Geog, Guelph, ON N1G 2W1, Canada. [Caldwell, Todd] Univ Texas Austin, Bur Econ Geol, Jackson Sch Geosci, Austin, TX 78713 USA. [Goodrich, David C.] USDA ARS, Southwest Watershed Res Ctr, Washington, DC 20250 USA. [Livingston, Stanley] USDA ARS, Natl Soil Eros Res Lab, W Lafayette, IN 47907 USA. [Lopez-Baeza, Ernesto] Univ Valencia, Appl Phys, E-46100 Valencia, Spain. [Thibeault, Marc] Comis Nacl Act Espaciales, Buenos Aires, DF, Argentina. [Walker, Jeffrey P.] Monash Univ, Dept Civil Engn, Melbourne, Vic 3800, Australia. [Entekhabi, Dara] MIT, Dept Civil & Environm Engn, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Entekhabi, Dara] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [O'Neill, Peggy E.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. RP Kim, SB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM seungbum.kim@jpl.nasa.gov FU Canadian Space Agency; Environment Canada FX Discussions with Drs. Rajat Bindlish, Mariko Burgin, Steven Chan, and Narendra Das were very helpful. Suggestions by the anonymous reviewers greatly improved the quality of the manuscript. They would also like to thank the following, for provision of the sets of ancillary data: MODIS-IGBP landcover, Cropland Data Layer, European ECOCLIMAP, Canadian AAFC Crop Inventory, Global Crop Map (Monfreda), MOD44W water classification, Shuttle Radar Topography Mission topography, Harmonized World Soil Database soil texture, Goddard Modeling and Assimilation Office surface temperature, Global Rural-Urban Mapping Project urban map, ECMWF total precipitation forecasts, and NOAA Snow and Ice Mapping System snow cover. The author would like to thank E. Tetlock acknowledged for the work with the Kenaston network data; the network is supported from the Canadian Space Agency and Environment Canada. NR 49 TC 0 Z9 0 U1 2 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD APR PY 2017 VL 55 IS 4 BP 1897 EP 1914 DI 10.1109/TGRS.2016.2631126 PG 18 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA EO0NN UT WOS:000396394900003 ER PT J AU Carter, LM Campbell, BA Neish, CD Nolan, MC Patterson, GW Jensen, JR Bussey, DBJ AF Carter, Lynn M. Campbell, Bruce A. Neish, Catherine D. Nolan, Michael C. Patterson, G. Wesley Jensen, J. Robert Bussey, D. B. J. TI A Comparison of Radar Polarimetry Data of the Moon From the LRO Mini-RF Instrument and Earth-Based Systems SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Moon; radar imaging; radar polarimetry; remote sensing; spaceborne radar ID COHERENT BACKSCATTER; VENUS; MAGELLAN; ARECIBO; SATELLITES; DEPOSITS AB The Mini-RF radar, launched on the Lunar Reconnaissance Orbiter, imaged the lunar surface using hybrid-polarimetric, transmitting one circular polarization and receiving linear H and V polarizations. Earth-based radar operating at the same frequency has acquired data of the same terrains using circular-polarized transmit waves and sampling circular polarizations. For lunar targets where the viewing geometry is nearly the same, the polarimetry derived from Mini-RF and the earth-based data should be very similar. However, we have discovered that there is a considerable difference in circular polarization ratio (CPR) values between the two data sets. We investigate possible causes for this discrepancy, including cross-talk between channels, sampling, and the ellipticity of the Mini-RF transmit wave. We find that none of these can reproduce the observed CPR differences, though a nonlinear block adaptive quantization function used to compress the data will significantly distort some other polarimetry products. A comparison between earth-based data sets acquired using two different sampling modes (sampling received linear polarizations and sampling circular polarizations) suggests that the CPR differences may be partially due to sampling the data in a different receive polarimetry bases. C1 [Carter, Lynn M.; Nolan, Michael C.] Univ Arizona, Tucson, AZ 85721 USA. [Campbell, Bruce A.] Smithsonian Inst, Washington, DC 20013 USA. [Neish, Catherine D.] Univ Western Ontario, London, ON N6A 3K7, Canada. [Patterson, G. Wesley; Jensen, J. Robert] Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. [Bussey, D. B. J.] NASA Headquarters, Washington, DC 20546 USA. RP Carter, LM (reprint author), Univ Arizona, Tucson, AZ 85721 USA. EM lmcarter@lpl.arizona.edu; campbellb@si.edu; cneish@uwo.ca; nolan@lpl.arizona.edu; wes.patterson@jhuapl.edu; bob.jensen@jhuapl.edu; david.b.bussey@nasa.gov RI Carter, Lynn/D-2937-2012 FU National Aeronautics and Space Administration [NNX12AF24G] FX The authors would like to thank B. L. Tise of Sandia National Laboratories for supplying the BAQ analysis and comments on the manuscript. They would like to thank three anonymous reviewers and R. F. Rincon of the NASA Goddard Space Flight Center who provided helpful comments and suggestions that improved this paper. They would also like to thank the staff members of Arecibo Observatory and the GBT for the observing help. We appreciate observing help from the staffs of Arecibo Observatory and the Green Bank Telescope. The Arecibo Observatory is operated by SRI International under a cooperative agreement with the National Science Foundation (AST-1100968), and in alliance with Ana G. Mendez-Universidad Metropolitana, and the Universities Space Research Association. The Arecibo Planetary Radar Program is supported by the National Aeronautics and Space Administration under Grant No. NNX12AF24G issued through the Near Earth Object Observations program. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 34 TC 0 Z9 0 U1 2 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD APR PY 2017 VL 55 IS 4 BP 1915 EP 1927 DI 10.1109/TGRS.2016.2631144 PG 13 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA EO0NN UT WOS:000396394900004 ER PT J AU Piepmeier, JR Focardi, P Horgan, KA Knuble, J Ehsan, N Lucey, J Brambora, C Brown, PR Hoffman, PJ French, RT Mikhaylov, RL Kwack, EY Slimko, EM Dawson, DE Hudson, D Peng, JZ Mohammed, PN De Amici, G Freedman, AP Medeiros, J Sacks, F Estep, R Spencer, MW Chen, CW Wheeler, KB Edelstein, WN O'Neill, PE Njoku, EG AF Piepmeier, Jeffrey R. Focardi, Paolo Horgan, Kevin A. Knuble, Joseph Ehsan, Negar Lucey, Jared Brambora, Clifford Brown, Paula R. Hoffman, Pamela J. French, Richard T. Mikhaylov, Rebecca L. Kwack, Eug-Yun Slimko, Eric M. Dawson, Douglas E. Hudson, Derek Peng, Jinzheng Mohammed, Priscilla N. De Amici, Giovanni Freedman, Adam P. Medeiros, James Sacks, Fred Estep, Robert Spencer, Michael W. Chen, Curtis W. Wheeler, Kevin B. Edelstein, Wendy N. O'Neill, Peggy E. Njoku, Eni G. TI SMAP L-Band Microwave Radiometer: Instrument Design and First Year on Orbit SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Calibration; microwave radiometry; polarimetry ID SOIL-MOISTURE; RADIOFREQUENCY INTERFERENCE; CALIBRATION; MISSION; POLARIMETRY; MITIGATION AB The Soil Moisture Active-Passive (SMAP) L-band microwave radiometer is a conical scanning instrument designed to measure soil moisture with 4% volumetric accuracy at 40-km spatial resolution. SMAP is NASA's first Earth Systematic Mission developed in response to its first Earth science decadal survey. Here, the design is reviewed and the results of its first year on orbit are presented. Unique features of the radiometer include a large 6-m rotating reflector, fully polarimetric radiometer receiver with internal calibration, and radio-frequency interference detection and filtering hardware. The radiometer electronics are thermally controlled to achieve good radiometric stability. Analyses of on-orbit results indicate that the electrical and thermal characteristics of the electronics and internal calibration sources are very stable and promote excellent gain stability. Radiometer NEDT < 1 K for 17-ms samples. The gain spectrum exhibits low noise at frequencies >1 MHz and 1/f noise rising at longer time scales fully captured by the internal calibration scheme. Results from sky observations and global swath imagery of all four Stokes antenna temperatures indicate that the instrument is operating as expected. C1 [Piepmeier, Jeffrey R.; Horgan, Kevin A.; Knuble, Joseph; Ehsan, Negar; Lucey, Jared; Brambora, Clifford; Hudson, Derek; Peng, Jinzheng; Mohammed, Priscilla N.; De Amici, Giovanni; Medeiros, James; Sacks, Fred; Estep, Robert; O'Neill, Peggy E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Focardi, Paolo; Brown, Paula R.; Hoffman, Pamela J.; French, Richard T.; Mikhaylov, Rebecca L.; Kwack, Eug-Yun; Slimko, Eric M.; Dawson, Douglas E.; Freedman, Adam P.; Spencer, Michael W.; Chen, Curtis W.; Wheeler, Kevin B.; Edelstein, Wendy N.; Njoku, Eni G.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Piepmeier, JR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM jeff.piepmeier@nasa.gov; paolo.focardi@jpl.nasa.gov NR 30 TC 0 Z9 0 U1 2 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD APR PY 2017 VL 55 IS 4 BP 1954 EP 1966 DI 10.1109/TGRS.2016.2631978 PG 13 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA EO0NN UT WOS:000396394900008 ER PT J AU Lei, N Xiong, XX AF Lei, Ning Xiong, Xiaoxiong TI Products of the SNPP VIIRS SD Screen Transmittance and the SD BRDFs From Both Yaw Maneuver and Regular On-Orbit Data SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Bidirectional reflectance distribution function (BRDF) degradation; radiometric calibration; reflective solar band (RSB); solar diffuser (SD); solar diffuser screen transmittance; Visible Infrared Imaging Radiometer Suite (VIIRS); yaw maneuver ID REFLECTIVE SOLAR BANDS; CALIBRATION; PERFORMANCE AB To ensure data quality, the Earth-observing Visible Infrared Imaging Radiometer Suite (VIIRS) on the Suomi National Polar-orbiting Partnership satellite regularly performs on-orbit radiometric calibration of its 22 spectral bands. The primary radiance source for the calibration of the VIIRS reflective solar bands (RSBs) is a sunlit onboard solar diffuser (SD). During the calibration process, sunlight goes through a perforated plate (the SD screen) and then strikes the SD. The sunlight, scattered off the SD of near-Lambertian property, is used for the calibration. Consequently, the spectral radiance of the scattered sunlight is proportional to the product of the SD screen transmittance and the SD bidirectional reflectance distribution function (BRDF) value at the observation direction. The BRDF value is decomposed to the product of its initial value at launch and a numerical degradation factor that quantifies the decrease from the initial value. The degradation factor is determined by an onboard SD stability monitor (SDSM). During the BRDF degradation factor determination process, the SDSM receives the SD scattered sunlight and the sunlight that goes through another perforated plate at almost the same time. The ratio of the signal strengths from the two observations is used to determine the BRDF degradation factor. Consequently, the RSB radiometric calibration requires the accurate knowledge of the product of the SD screen transmittance and the initial BRDF value as sensed by the RSB and the SDSM detectors. We use both yaw maneuver and a small portion of regular on-orbit data to determine the products. C1 [Lei, Ning] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. RP Lei, N (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA. EM ning.lei@ssaihq.com; xiaoxiong.xiong-1@nasa.gov NR 21 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 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD APR PY 2017 VL 55 IS 4 BP 1975 EP 1987 DI 10.1109/TGRS.2016.2633967 PG 13 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA EO0NN UT WOS:000396394900010 ER PT J AU Rosenberg, R Maxwell, S Johnson, BC Chapsky, L Lee, RAM Pollock, R AF Rosenberg, Robert Maxwell, Stephen Johnson, B. Carol Chapsky, Lars Lee, Richard A. M. Pollock, Randy TI Preflight Radiometric Calibration of Orbiting Carbon Observatory 2 SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Integrating sphere; Orbiting Carbon Observatory (OCO-2); radiometry; remote sensing AB The imaging spectrometers of the second orbiting carbon observatory were radiometrically calibrated before launch during instrumentlevel ground testing. The gain and dark responses were characterized for each focal plane array detector element. An integrating sphere source with an integrated monitoring spectroradiometer illuminated the OCO-2 spectrometers at many light levels. Instrument output was compared with the calibrated output of the source to derive gain coefficients. This source was calibrated in situ with respect to the National Institute of Standards and Technology reference standards, and the instrument met its absolute performance requirement of 5%. Matching fields of view for the internal monitor detectors and the external instrument under test was found to be particularly important, as observed in the results and supported by modeling. Temperature-dependent dark offsets were corrected in a separate process. Solar spectra with varying neutral density filters were used to validate the linearity of the spectrometers. C1 [Rosenberg, Robert; Chapsky, Lars; Lee, Richard A. M.; Pollock, Randy] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Maxwell, Stephen; Johnson, B. Carol] NIST, Gaithersburg, MD 20899 USA. RP Rosenberg, R (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM Rob.Rosenberg@jpl.nasa.gov FU NIST Greenhouse Gas and Climate Science Measurements program FX A portion of the research described in this paper was carried out at JPL, California Institute of Technology, under a contract with NASA. Support was also provided by the NIST Greenhouse Gas and Climate Science Measurements program. NR 14 TC 2 Z9 2 U1 0 U2 0 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD APR PY 2017 VL 55 IS 4 BP 1994 EP 2006 DI 10.1109/TGRS.2016.2634023 PG 13 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA EO0NN UT WOS:000396394900012 ER PT J AU Wang, ZP Xiong, XX AF Wang, Zhipeng Xiong, Xiaoxiong TI Band-to-Band Misregistration of the Images of MODIS Onboard Calibrators and Its Impact on Calibration SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Calibration; image registration; moderate resolution imaging spectroradiometer (MODIS); optical design ID TERRA MODIS; PERFORMANCE AB The Moderate Resolution Imaging Spectroradiometer (MODIS) instruments aboard Terra and Aqua satellites are radiometrically calibrated on-orbit with a set of onboard calibrators (OBCs), including a solar diffuser, a blackbody, and a space view port through which the detectors can view the dark space. As a whisk-broom scanning spectroradiometer, 36 MODIS spectral bands are assembled in the along-scan direction on four focal plane assemblies (FPAs). These bands capture images of the same target sequentially with the motion of a scan mirror. Then the images are coregistered onboard by delaying the appropriate band-dependent amount of time, depending on the band locations on the FPA. While this coregistration mechanism is functioning well for the "far-field" remote targets such as earth view scenes or the moon, noticeable band-to-band misregistration in the along-scan direction has been observed for "near field" targets, particularly in OBCs. In this paper, the misregistration phenomenon is presented and analyzed. It is concluded that the root cause of the misregistration is that the rotating element of the instrument, the scan mirror, is displaced from the focus of the telescope primary mirror. The amount of the misregistration is proportional to the band location on the FPA and is inversely proportional to the distance between the target and the scan mirror. The impact of this misregistration on the calibration of MODIS bands is discussed. In particular, the calculation of the detector gain coefficient m(1) of bands 8-16 (412-870 nm) is improved by up to 1.5% for Aqua MODIS. C1 [Wang, Zhipeng] Sci Syst & Applicat Inc, Greenbelt, MD 20706 USA. [Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wang, ZP (reprint author), Sci Syst & Applicat Inc, Greenbelt, MD 20706 USA. EM zhipeng.wang@ssaihq.com; Xiaoxiong.Xiong-1@nasa.gov OI Wang, Zhipeng/0000-0002-9108-9009 NR 13 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 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD APR PY 2017 VL 55 IS 4 BP 2136 EP 2143 DI 10.1109/TGRS.2016.2637167 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 EO0NN UT WOS:000396394900023 ER PT J AU Lim, YX Burgin, MS van Zyl, JJ AF Lim, Yu Xian Burgin, Mariko S. van Zyl, Jakob J. TI An Optimal Nonnegative Eigenvalue Decomposition for the Freeman and Durden Three-Component Scattering Model SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Model-based decomposition; optimal nonnegative eigenvalue decomposition (NNED); radar polarimetry ID SAR IMAGE DECOMPOSITION; COHERENCY MATRIX; RADAR POLARIMETRY AB Model-based decomposition allows the physical interpretation of polarimetric radar scattering in terms of various scattering mechanisms. A three-component decomposition proposed by Freeman and Durden has been popular, though significant shortcomings have been identified. In particular, it can result in negative eigenvalues for the component terms and the remainder matrix, hence violating fundamental requirements for physically meaningful decompositions. In addition, since the algorithm solves for the canopy term first, the contribution of the canopy is often over-estimated. In this paper, we show how to determine the parameters for the Freeman-Durden model in a way that minimizes the total power in the remainder matrix without favoring any individual component in the model, while simultaneously satisfying the constraints of non-negative eigenvalues. We illustrate our analytical solution by comparison with the Freeman-Durden algorithm, as well as the nonnegative eigenvalue decomposition (NNED) proposed by van Zyl et al. The results show that this optimum algorithm generally assigns less power to the volume scattering than either the original Freeman-Durden or the NNED algorithms. C1 [Lim, Yu Xian] CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA. [Burgin, Mariko S.; van Zyl, Jakob J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Lim, YX (reprint author), CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA. EM ylim@caltech.edu FU Jet Propulsion Laboratory, California Institute of Technology under National Aeronautics and Space Administration FX This work was supported in part by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 22 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 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD APR PY 2017 VL 55 IS 4 BP 2167 EP 2176 DI 10.1109/TGRS.2016.2637882 PG 10 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA EO0NN UT WOS:000396394900025 ER PT J AU Nandan, V Geldsetzer, T Yackel, JJ Islam, T Gill, JPS Mahmud, M AF Nandan, Vishnu Geldsetzer, Torsten Yackel, John J. Islam, Tanvir Gill, Jagvijay P. S. Mahmud, Mallik TI Multifrequency Microwave Backscatter From a Highly Saline Snow Cover on Smooth First-Year Sea Ice: First-Order Theoretical Modeling SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Active microwaves; backscatter; multifrequency; sea ice; snow ID APERTURE RADAR DATA; ELECTROMAGNETIC PROPERTIES; POLARIMETRIC SIGNATURES; DIELECTRIC-PROPERTIES; SCATTERING; BAND; FREQUENCIES; EMISSION; BRINE; MELT AB A theoretical understanding of a multifrequency microwave approach to understand complex microwave interactions from a highly saline snow cover on a relatively smooth first-year sea ice is presented. We examine the sensitivity of Ku-, X-, and C-band sigma(0)(VV) and sigma(0)(HH) to variability in snow geophysical properties such as salinity, density, temperature, and snow grain radius, sampled from a highly saline snow cover on first-year sea ice. A first-order multilayer snow and ice backscatter model is used to calculate sigma(0)(VV) and sigma(0)(HH) by taking into account the surface and volume scattering contributions within each snow layer of the snow pack. Penetration depth models are used to calculate the potential penetration of all three frequencies, at initial and perturbed snow property conditions. Sensitivity analyses suggest that variability in salinity and snow grain radius have the greatest effect, followed by density and temperature. This phenomenon is observed for all three frequencies, influencing microwave penetration and backscatter. Dielectric loss associated with highly saline snow covers and substantial changes in scattering contributions from snow grain radius perturbations were found to be the dominant factors affecting microwave penetration and backscatter. Results from this paper demonstrate the potential of using a multifrequency theoretical approach to correlate with active microwave observations to determine the geophysical and electrical state of snow/sea ice system. The paper also represents an evolution in a theoretical understanding on how an active microwave approach using multiple frequencies can be further utilized toward the development of snow thickness and/or snow water equivalent algorithm on smooth FYI. C1 [Nandan, Vishnu; Geldsetzer, Torsten; Yackel, John J.; Gill, Jagvijay P. S.; Mahmud, Mallik] Univ Calgary, Dept Geog, Calgary, AB T2L 1N4, Canada. [Islam, Tanvir] Jet Prop Lab, Pasadena, CA 91109 USA. RP Nandan, V (reprint author), Univ Calgary, Dept Geog, Calgary, AB T2L 1N4, Canada. EM vishnunandan.nandaku@ucalgary.ca; geldsetz@ucalgary.ca; yackel@ucalgary.ca; tanvir.islam@jpl.nasa.gov; jpsgill@ucalgary.ca; msmahmud@ucalgary.ca FU Natural Science and Engineering Research Council Discovery Grant FX This work was supported by the Natural Science and Engineering Research Council Discovery Grant. NR 53 TC 0 Z9 0 U1 1 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD APR PY 2017 VL 55 IS 4 BP 2177 EP 2190 DI 10.1109/TGRS.2016.2638323 PG 14 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA EO0NN UT WOS:000396394900026 ER PT J AU Chang, TJ Xiong, XX Angal, A Wu, AS Geng, X AF Chang, Tiejun Xiong, Xiaoxiong Angal, Amit Wu, Aisheng Geng, Xu TI Aqua and Terra MODIS RSB Calibration Comparison Using BRDF Modeled Reflectance SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Atmospheric correction; bidirectional reflectance distribution function (BRDF); intercomparison; Moderate Resolution Imaging Spectroradiometer (MODIS); Radiometric calibration ID RESOLUTION IMAGING SPECTRORADIOMETER; RADIATIVE-TRANSFER CODE; SOLAR BANDS; CROSS-CALIBRATION; ATMOSPHERIC CORRECTION; VECTOR VERSION; SATELLITE DATA; PERFORMANCE; RETRIEVAL; SENSORS AB The intercomparison of Moderate Resolution Imaging Spectroradiometer (MODIS) reflective solar bands onboard Aqua and Terra is very important for the assessment of each instrument's calibration. One of the limitations is the lack of simultaneous nadir overpasses. Their measurements over a selected Earth view target have significant differences in solar and view angles, which magnify the effects of atmospheric scattering and bidirectional reflectance distribution function (BRDF). In this paper, an intercomparison technique is formulated after correction for site's BRDF and atmospheric effects. The reflectance measurements over Libya desert sites 1, 2, and 4 from both the Aqua and Terra MODIS are regressed to a BRDF model with an adjustable coefficient accounting for calibration difference. The ratio between Aqua and Terra reflectance measurements is derived for bands 1-9 and the results from different sites show good agreement. For year 2003, the ratios are in the range of 0.985-1.010 for bands 1-9. Band 3 shows the lowest ratio 0.985 and band 1 shows the highest ratio 1.010. For the year 2014, the ratio ranges from approximately 0.983 for bands 2 and 1.012 for band 8. The BRDF corrected reflectance for the two instruments is also derived for every year from 2003 to 2014 for stability assessment. Bands 1 and 2 show greater than 1% differences between the two instruments. Aqua bands 1 and 2 show downward trends while Terra bands 1 and 2 show upward trends. Bands 8 and 9 of both Aqua and Terra show large variations of reflectance measurement over time. C1 [Chang, Tiejun; Angal, Amit; Wu, Aisheng; Geng, Xu] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. RP Chang, TJ (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA. NR 37 TC 0 Z9 0 U1 1 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD APR PY 2017 VL 55 IS 4 BP 2288 EP 2298 DI 10.1109/TGRS.2016.2641258 PG 11 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA EO0NN UT WOS:000396394900035 ER PT J AU Bomarito, GF Hochhalter, JD Ruggles, TJ Cannon, AH AF Bomarito, G. F. Hochhalter, J. D. Ruggles, T. J. Cannon, A. H. TI Increasing accuracy and precision of digital image correlation through pattern optimization SO OPTICS AND LASERS IN ENGINEERING LA English DT Article DE Image correlation; Pattern optimization; Pattern quality metrics; 2D full-field measurements ID SPECKLE PATTERNS; QUALITY ASSESSMENT; SYSTEMATIC-ERRORS; INTERPOLATION; GRADIENT; MOTION; NOISE AB The accuracy and precision of digital image correlation (DIC) is based on three primary components: image acquisition, image analysis, and the subject of the image. Focus on the third component, the image subject, has been relatively limited and primarily concerned with comparing pseudo-random surface patterns. In the current work, a strategy is proposed for the creation of optimal DIC patterns. In this strategy, a pattern quality metric is developed as a combination of quality metrics from the literature rather than optimization based on any single one of them. In this way, optimization produces a pattern which balances the benefits of multiple quality metrics. Specifically, sum of square of subset intensity gradients (SSSIG) was found to be the metric most strongly correlated to DIC accuracy and thus is the main component of the newly proposed pattern quality metric. A term related to the secondary auto-correlation peak height is also part of the proposed quality metric which effectively acts as a constraint upon SSSIG ensuring that a regular (e.g., checkerboard-type) pattern is not achieved. The combined pattern quality metric is used to generate a pattern that was on average 11.6% more accurate than a randomly generated pattern in a suite of numerical experiments. Furthermore, physical experiments were performed which confirm that there is indeed improvement of a similar magnitude in DIC measurements for the optimized pattern compared to a random pattern. C1 [Bomarito, G. F.; Hochhalter, J. D.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Ruggles, T. J.] NIA, Hampton, VA USA. [Cannon, A. H.] 1900 Engn LLC, Clemson, SC USA. [Cannon, A. H.] Clemson Univ, Dept Chem & Biomol Engn, Clemson, SC USA. RP Bomarito, GF (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM geoffrey.f.bomarito@nasa.gov FU National Aeronautics and Space Administration's Aeronautics Research Mission Directorate through the Digital Twin effort within the Convergent Aeronautics Solutions project FX This work was supported by the National Aeronautics and Space Administration's Aeronautics Research Mission Directorate through the Digital Twin effort within the Convergent Aeronautics Solutions project. NR 34 TC 0 Z9 0 U1 4 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0143-8166 EI 1873-0302 J9 OPT LASER ENG JI Opt. Lasers Eng. PD APR PY 2017 VL 91 BP 73 EP 85 DI 10.1016/j.optlaseng.2016.11.005 PG 13 WC Optics SC Optics GA EJ5NF UT WOS:000393264300008 ER PT J AU Hong, N Park, C Kim, D Jeong, KS Yoon, JS Jin, B Meyyappan, M Lee, JS AF Hong, Nanki Park, ChanOh Kim, Donghoon Jeong, Ki-Soo Yoon, Jun-Sik Jin, Bo Meyyappan, M. Lee, Jeong-Soo TI Buffer effects of two functional groups against pH variation at aminosilanized Electrolyte-Oxide-Semiconductor (EOS) capacitor SO SENSORS AND ACTUATORS B-CHEMICAL LA English DT Article DE pH sensitivity; Silanization; Electrolyte-Oxide-Semiconductor capacitor; Buffer effect ID SURFACE MODIFICATION; SILICON SURFACES; OPTIMIZATION; SENSITIVITY; APTES; 3-AMINOPROPYLTRIETHOXYSILANE; IMMOBILIZATION; SILANIZATION; NANOSENSORS; EXPLOSIVES AB The pH sensitivity variations of Electrolyte-Oxide-Semiconductor (EOS) capacitor with both silanol and amine groups are analyzed in terms of their functional group ratio theoretically and experimentally. The phenomena causing the pH sensitivity variations are explained by the buffer effect of each functional group by using Henderson-Hasselbalch equation to compare the state ratio of the acid and the conjugate base of silanol and amine groups. When p is defined as the amine group fraction among the total functional groups, the theoretical pH sensitivity is relatively high around p = 0.3 or 0.7, but low at p = 0, 0.5 or 1. In addition, EOS capacitors with four types of surface treatments for various p are fabricated and characterized by C-V measurements. The pH sensitivity values of the fabricated EOS capacitors corresponding to all p values fit well with the theoretical results. This work allows to explain the reactions on the surface membrane and the characteristics of the pH sensitivity depending on the functional group ratio. (C) 2016 Elsevier B.V. All rights reserved. C1 [Hong, Nanki; Kim, Donghoon; Jeong, Ki-Soo; Jin, Bo; Lee, Jeong-Soo] Pohang Univ Sci & Technol, Dept Elect Engn, Pohang 37673, South Korea. [Park, ChanOh; Lee, Jeong-Soo] Pohang Univ Sci & Technol, Div IT Convergence Engn, Pohang 37673, South Korea. [Yoon, Jun-Sik] Pohang Univ Sci & Technol, Creat IT Engn & Future IT Innovat Lab, Pohang 37673, South Korea. [Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Lee, JS (reprint author), Pohang Univ Sci & Technol, Dept Elect Engn, Pohang 37673, South Korea. EM ljs6951@postech.ac.kr FU Agency for Defense Development [ADD-14-02-06-20]; National Research Foundation of Korea (NRF) grant - Korean government (MSIP) [2015R1A2A2A09001553]; POSTECH; Samsung Display Co. Ltd. FX This work was supported by the Agency for Defense Development(ADD-14-02-06-20); the National Research Foundation of Korea (NRF) grant funded by the Korean government (MSIP) (No. 2015R1A2A2A09001553); and Semiconductor Industry Collaborative project between POSTECH and Samsung Display Co. Ltd. NR 34 TC 0 Z9 0 U1 3 U2 3 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0925-4005 J9 SENSOR ACTUAT B-CHEM JI Sens. Actuator B-Chem. PD APR PY 2017 VL 242 BP 324 EP 331 DI 10.1016/j.snb.2016.10.146 PG 8 WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation SC Chemistry; Electrochemistry; Instruments & Instrumentation GA EJ5ON UT WOS:000393267700040 ER PT J AU Sanson, F Villedieu, N Panerai, F Chazot, O Congedo, PM Magin, TE AF Sanson, Francois Villedieu, Nadege Panerai, Francesco Chazot, Olivier Congedo, Pietro M. Magin, Thierry E. TI Quantification of uncertainty on the catalytic property of reusable thermal protection materials from high enthalpy experiments SO EXPERIMENTAL THERMAL AND FLUID SCIENCE LA English DT Article DE Uncertainty quantification; Catalysis; Thermal protection systems ID PLASMA WIND-TUNNEL; DISSOCIATED AIR; HEAT TRANSFER; RECOMBINATION; OXYGEN; COMPOSITES; ATOMS; OXIDE; FLOW AB An accurate determination of the catalytic property of thermal protection materials is crucial to design reusable atmospheric entry vehicles. This property is determined by combining experimental measurements and simulations of the reactive boundary layer near the material surface. The inductively-driven Plasmatron facility at the von Karman Institute for Fluid Dynamics provides a test environment to analyze gas-surface interactions under effective hypersonic conditions. In this study, we develop an uncertainty quantification methodology to rebuild values of the gas enthalpy and material catalytic property from Plasmatron experiments. A non-intrusive spectral projection method is coupled with an in-house boundary-layer solver, to propagate uncertainties and provide error bars on the rebuilt gas enthalpy and material catalytic property, as well as to determine which uncertainties have the largest contribution to the outputs of the experiments. We show that the uncertainties computed with the methodology developed are significantly reduced compared to those determined using a more conservative engineering approach adopted in the analysis of previous experimental campaigns. (C) 2016 Elsevier Inc. All rights reserved. C1 [Sanson, Francois; Congedo, Pietro M.] INRIA Bordeaux Sud Ouest, 200 Rue Vieille Tour, F-33405 Talence, France. [Villedieu, Nadege; Panerai, Francesco; Chazot, Olivier; Magin, Thierry E.] von Karman Inst Fluid Dynam, Chaussee Waterloo 72, B-1640 Rhode St Genese, Belgium. RP Panerai, F (reprint author), NASA Ames Res Ctr, AMA Inc, Mail Stop 234-1, Moffett Field, CA 94035 USA. EM panerai@vki.ac.be FU European Research Council [259354]; European Space Agency (ESA) General Support Technology Programme (GSTP) "Plasmatron+" [4000105388/12/NL/ SFe] FX Research of T.E.M. was sponsored by the European Research Council Starting Grant #259354. The work was partly supported by the European Space Agency (ESA) General Support Technology Programme (GSTP) "Plasmatron+" (contract #4000105388/12/NL/ SFe). NR 37 TC 0 Z9 0 U1 6 U2 6 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0894-1777 EI 1879-2286 J9 EXP THERM FLUID SCI JI Exp. Therm. Fluid Sci. PD APR PY 2017 VL 82 BP 414 EP 423 DI 10.1016/j.expthermflusci.2016.11.013 PG 10 WC Thermodynamics; Engineering, Mechanical; Physics, Fluids & Plasmas SC Thermodynamics; Engineering; Physics GA EI8PI UT WOS:000392769400042 ER PT J AU Li, W Yan, L Karnati, S Liou, F Newkirk, J Taminger, KMB Seufzer, WJ AF Li, Wei Yan, Lei Karnati, Sreekar Liou, Frank Newkirk, Joseph Taminger, Karen M. Brown Seufzer, William J. TI Ti-Fe intermetallics analysis and control in joining titanium alloy and stainless steel by Laser Metal Deposition SO JOURNAL OF MATERIALS PROCESSING TECHNOLOGY LA English DT Article DE Ti-Fe intermetallic; Laser metal deposition; Ti6Al4V; SS316 ID COPPER INTERLAYER SHEET; PHASE PRECIPITATION; SIGMA-PHASE; 304-STAINLESS-STEEL; CORROSION; JOINTS AB There are urgent needs to join titanium alloy and stainless steel so that their outstanding mechanical properties can be utilized integratedly in the aeronautics and astronautics industries. However, direct fusion joining two alloys can cause brittle Ti-Fe intermetallics which compromise the mechanical properties of diffusion bonds between titanium alloys and stainless steel. Therefore, filler metals are required as transition layers. In this research, stainless steel metallic powder was directly deposited on the titanium alloy substrate by laser beam, the Ti-Fe intermetallic phases formed in this process were investigated through analyzing fracture morphology, phase identification, and Vickers Hardness Number (VHN). After that, Laser Metal Deposition (LMD) was applied to explore a new fabricating process to join Ti6Al4V and SS316. A transition composition route was introduced (Ti6A14 -> V -> Cr -> Fe -> SS316) to avoid the intermetallic phase between Ti6Al4V and SS316. A thin wall sample was fabricated via LMD following the transition composition route. X-ray Diffraction (XRD) tests were conducted. The results demonstrate that the generation of intermetallic phases is effectively avoided following the composition route. Microstructure characterization and composition distribution analysis were performed via Scanning Electron Microscope (SEM) and Energy Dispersive Spectrometry (EDS). The SEM results indicated that rapid solidification results in the elongated Microstructure. The EDS result can reflect the transition composition route design. Besides, the diffusions of metals are detected in the EDS results. Vickers hardness test was executed to observe the VHN distribution from Ti6Al4V to SS316. Vickers hardness result showed that there was no significant formation of intermetallic phases. Comparing with directly depositing SS316 on Ti6Al4V, the usage of the new transition route can eliminate the Ti-Fe intermetallics effectively. (C) 2016 Elsevier B.V. All rights reserved. C1 [Li, Wei; Yan, Lei; Karnati, Sreekar; Liou, Frank] Missouri Univ Sci & Technol, Dept Mech & Aerosp Engn, Rolla, MO 65409 USA. [Newkirk, Joseph] Missouri Univ Sci & Technol, Dept Met Engn, Rolla, MO 65409 USA. [Taminger, Karen M. Brown; Seufzer, William J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM wldp5@mst.edu FU NASA EPSCoR Grant [NNX13AM99A] FX The authors gratefully acknowledge the financial support provided for this study by the NASA EPSCoR Grant number NNX13AM99A. NR 16 TC 0 Z9 0 U1 24 U2 24 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0924-0136 J9 J MATER PROCESS TECH JI J. Mater. Process. Technol. PD APR PY 2017 VL 242 BP 39 EP 48 DI 10.1016/j.jmatprotec.2016.11.010 PG 10 WC Engineering, Industrial; Engineering, Manufacturing; Materials Science, Multidisciplinary SC Engineering; Materials Science GA EI5XB UT WOS:000392568500004 ER PT J AU El-Maarry, MR Groussin, O Thomas, N Pajola, M Auger, AT Davidsson, B Hu, X Hviid, SF Knollenberg, J Guttler, C Tubiana, C Fornasier, S Feller, C Hasselmann, P Vincent, JB Sierks, H Barbieri, C Lamy, P Rodrigo, R Koschny, D Keller, HU Rickman, H A'Hearn, MF Barucci, MA Bertaux, JL Bertini, I Besse, S Bodewits, D Cremonese, G Da Deppo, V Debei, S De Cecco, M Deller, J Deshapriya, JDP Fulle, M Gutierrez, PJ Hofmann, M Ip, WH Jorda, L Kovacs, G Kramm, JR Kuhrt, E Kuppers, M Lara, LM Lazzarin, M Lin, ZY Moreno, JJL Marchi, S Marzari, F Mottola, S Naletto, G Oklay, N Pommerol, A Preusker, F Scholten, F Shi, X AF El-Maarry, M. Ramy Groussin, O. Thomas, N. Pajola, M. Auger, A. -T. Davidsson, B. Hu, X. Hviid, S. F. Knollenberg, J. Guettler, C. Tubiana, C. Fornasier, S. Feller, C. Hasselmann, P. Vincent, J. -B. Sierks, H. Barbieri, C. Lamy, P. Rodrigo, R. Koschny, D. Keller, H. U. Rickman, H. A'Hearn, M. F. Barucci, M. A. Bertaux, J. -L. Bertini, I. Besse, S. Bodewits, D. Cremonese, G. Da Deppo, V. Debei, S. De Cecco, M. Deller, J. Deshapriya, J. D. P. Fulle, M. Gutierrez, P. J. Hofmann, M. Ip, W. -H. Jorda, L. Kovacs, G. Kramm, J. -R. Kuehrt, E. Kueppers, M. Lara, L. M. Lazzarin, M. Lin, Z. -Yi Moreno, J. J. Lopez Marchi, S. Marzari, F. Mottola, S. Naletto, G. Oklay, N. Pommerol, A. Preusker, F. Scholten, F. Shi, X. TI Surface changes on comet 67P/Churyumov-Gerasimenko suggest a more active past SO SCIENCE LA English DT Article ID IMHOTEP REGION; NUCLEUS; ROSETTA/OSIRIS; ROTATION; OSIRIS; SHAPE AB The Rosetta spacecraft spent similar to 2 years orbiting comet 67P/Churyumov-Gerasimenko, most of it at distances that allowed surface characterization and monitoring at submeter scales. From December 2014 to June 2016, numerous localized changes were observed, which we attribute to cometary-specific weathering, erosion, and transient events driven by exposure to sunlight and other processes. While the localized changes suggest compositional or physical heterogeneity, their scale has not resulted in substantial alterations to the comet's landscape. This suggests that most of the major landforms were created early in the comet's current orbital configuration. They may even date from earlier if the comet had a larger volatile inventory, particularly of CO or CO2 ices, or contained amorphous ice, which could have triggered activity at greater distances from the Sun. C1 [El-Maarry, M. Ramy; Thomas, N.; Pommerol, A.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [El-Maarry, M. Ramy] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80301 USA. [Groussin, O.; Auger, A. -T.; Jorda, L.] Aix Marseille Univ, CNRS, UMR 7326, Lab Astrophys Marseille, F-13388 Marseille, France. [Pajola, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Davidsson, B.] Jet Prop Lab, Pasadena, CA 91109 USA. [Hu, X.; Guettler, C.; Tubiana, C.; Sierks, H.; Deller, J.; Hofmann, M.; Kovacs, G.; Kramm, J. -R.; Shi, X.] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany. [Hviid, S. F.; Knollenberg, J.; Vincent, J. -B.; Keller, H. U.; Kuehrt, E.; Mottola, S.; Oklay, N.; Preusker, F.; Scholten, F.] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Planetenforsch, D-12489 Berlin, Germany. [Fornasier, S.; Feller, C.; Hasselmann, P.; Barucci, M. A.; Deshapriya, J. D. P.] Sorbonne Univ, Univ Paris Diderot, PSL Res Univ,CNRS,LESIA, UPMC Univ Paris 06,Observ Paris,Sorbonne Paris Ci, F-92195 Meudon, France. [Barbieri, C.; Bertini, I.; Lazzarin, M.; Marzari, F.] Univ Padua, Dept Phys & Astron, I-35122 Padua, Italy. [Lamy, P.] CNRS, Lab Astrophys Marseille, UMR 7326, F-13388 Marseille 13, France. [Lamy, P.] Univ Aix Marseille, F-13388 Marseille 13, France. [Rodrigo, R.] Inst Nacl Tecn Aeroespacial, Ctr Astrobiol, Madrid 28850, Spain. [Rodrigo, R.] Int Space Sci Inst, CH-3012 Bern, Switzerland. [Koschny, D.; Besse, S.; Kueppers, M.] European Space Astron Ctr ESA, Operat Dept, POB 78, Madrid 28691, Spain. [Keller, H. U.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany. [Rickman, H.] Uppsala Univ, Dept Phys & Astron, Box 516, S-75120 Uppsala, Sweden. [Rickman, H.] Polish Acad Sci, Space Res Ctr, PL-00716 Warsaw, Poland. [A'Hearn, M. F.; Bodewits, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Bertaux, J. -L.] Univ Versailles St Quentin En Yvelines, Lab Atmospheres Milieux Observat Spatiales LATMOS, Inst Pierre Simon Laplace, CNRS, F-78280 Guyancourt, France. [Cremonese, G.] Osserv Astron Padova, Ist Nazl Astrofis, I-35122 Padua, Italy. [Da Deppo, V.; Naletto, G.] CNR, Ist Foton & Nanotecnol, Unita Org Supporto, Padova Luxor, I-35131 Padua, Italy. [Debei, S.] Univ Padua, Dept Ind Engn, I-35131 Padua, Italy. [De Cecco, M.] Univ Trento, I-38123 Trento, Italy. [Fulle, M.] Osserv Astron Trieste, INAF, I-34014 Trieste, Italy. [Gutierrez, P. J.; Lara, L. M.; Moreno, J. J. Lopez] Inst Astrofis Andalucia CSIC, C Glorieta Astron S-N, Granada 18008, Spain. [Ip, W. -H.; Lin, Z. -Yi] Natl Cent Univ, Grad Inst Astron, Chungli 32054, Taiwan. [Marchi, S.] Southwest Res Inst, Virtual Inst, Solar Syst Explorat Res, Boulder, CO 80302 USA. [Naletto, G.] Univ Padua, Dept Informat Engn, I-35131 Padua, Italy. [Naletto, G.] Univ Padua, Ctr Ateneo Studi & Attivita Spaziali Giuseppe Col, I-35131 Padua, Italy. RP El-Maarry, MR (reprint author), Univ Bern, Inst Phys, CH-3012 Bern, Switzerland.; El-Maarry, MR (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80301 USA. EM mohamed.el-maarry@lasp.colorado.edu FU Germany (Deutschen Zentrums Luft- und Raumfahrt); France (Centre National d'Etudee Spatiales); Italy (Ageripia Spzicle Italiana); Spain (Ministerio de Education, Cultura y Denote); Sweden (Swedish National Space Board) [74/10:2]; ESA Technical Directorate; Polish National Science Center [2011/01/B/ST9/05442]; Ministry of Science and Technology, Taiwan [NSC 101-2111-M-008-016]; NASA through Jet Propulsion Laboratory [1267923]; Swiss National Science Foundation [200020_165684]; NCCR PlanetS FX We thank three anonymous reviewers for thee constructive suggestions that have improved this work. OSIRIS was built by a consortium of the Max-Planck-Institut fur Sonnensysternforschung (MPS), Gottingen, Germany; Centro Interdipartimentale Studi e Attivita Spaziali-University of Padova, Italy; the Laboratoire d'Astrophysique de Marseille, France; the Instituto de Astrotisica de Adalucia, Consejo Superior de Investigaciones Cientificas, Granada, Spain; the Research and Scientific Support Department of the European Space Agency (ESA), Noordwijk, Netherlands: the Institute Nacional de Tecnica Aeroespacial, Madrid Spain; the Universidad Politecnica de Madrid, Spain; the Department of Physics and Astronomy of Uppsala University, Sweden; and the Institit fur Datentechnik und Kommunikatiorisnetpe der Technischen Universitat Braunschweig, Germany. The support of the national funding agencies of Germany (Deutschen Zentrums Luft- und Raumfahrt), France (Centre National d'Etudee Spatiales), Italy (Ageripia Spzicle Italiana), Spain (Ministerio de Education, Cultura y Denote), Sweden (Swedish National Space Board; grant 74/10:2), and the ESA Technical Directorate is gratefully acknowledged. Also supported by Polish National Science Center grant 2011/01/B/ST9/05442 (H.R.); Ministry of Science and Technology, Taiwan, grant NSC 101-2111-M-008-016 W.-H.I.); NASA through Jet Propulsion Laboratory contract 1267923 (M.F.A); and Swiss National Science Foundation grant 200020_165684 and NCCR PlanetS (M.R.E., N.T., and A.P.). We thank the ESA teams at European Space Astronomy Centre, European Space Operations Centre, and European Space Research and Technology Centre for their work in support of the Rosetta mission. Rosetta/OSIRIS data are available through ESA's Planetary Science Archive (PSA), www.cosrnos.esaint/web/psa/rosetta. Images used in this study that are not yet available at PSA can be downloaded from the MPS OSIRIS wesite https://planetgate.mps.mpg.de/WebFileShare/Released_Images/El-Maarry+Sci ence/. NR 24 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD MAR 31 PY 2017 VL 355 IS 6332 BP 1392 EP + DI 10.1126/science.aak9384 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EQ1DL UT WOS:000397809500035 PM 28325842 ER PT J AU Jakosky, BM Slipski, M Benna, M Mahaffy, P Elrod, M Yelle, R Stone, S Alsaeed, N AF Jakosky, B. M. Slipski, M. Benna, M. Mahaffy, P. Elrod, M. Yelle, R. Stone, S. Alsaeed, N. TI Mars' atmospheric history derived from upper-atmosphere measurements of Ar-38/Ar-36 SO SCIENCE LA English DT Article ID MARTIAN ATMOSPHERE; VOLATILE EVOLUTION; SOLAR-WIND; ISOTOPES; FRACTIONATION; IONOSPHERE; CURIOSITY; ESCAPE; CARBON AB The history of Mars' atmosphere is important for understanding the geological evolution and potential habitability of the planet. We determine the amount of gas lost to space through time using measurements of the upper-atmospheric structure made by the Mars Atmosphere and Volatile Evolution (MAVEN) spacecraft. We derive the structure of Ar-38/Ar-36 between the homopause and exobase altitudes. Fractionation of argon occurs as a result of loss of gas to space by pickup-ion sputtering, which preferentially removes the lighter atom. The measurements require that 66% of the atmospheric argon has been lost to space. Thus, a large fraction of Mars' atmospheric gas has been lost to space, contributing to the transition in climate from an early, warm, wet environment to today's cold, dry atmosphere. C1 [Jakosky, B. M.; Slipski, M.; Alsaeed, N.] Univ Colorado, Boulder, CO 80309 USA. [Benna, M.; Mahaffy, P.; Elrod, M.] NASA, Goddard Spaceflight Ctr, Greenbelt, MD USA. [Yelle, R.; Stone, S.] Univ Arizona, Tucson, AZ USA. [Alsaeed, N.] Amer Univ Sharjah, Sharjah, U Arab Emirates. RP Jakosky, BM (reprint author), Univ Colorado, Boulder, CO 80309 USA. EM bruce.jakosky@lasp.colorado.edu FU NASA; Mohammed Bin Rashid Space Center in the United Arab Emirates FX The MAVEN mission is supported by NASA. We are grateful for support from all components of the project, including the spacecraft, operations, instrument, science, and project teams. N.A. was supported by the Mohammed Bin Rashid Space Center in the United Arab Emirates. Data from the MAVEN mission have been made available via the Planetary Data System and are accessible at http://atmos.nmsu.edu/data_and_services/atmospheres_data/MAVEN/maven_mai n.html. NR 31 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD MAR 31 PY 2017 VL 355 IS 6332 BP 1408 EP + DI 10.1126/science.aai7721 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EQ1DL UT WOS:000397809500039 PM 28360326 ER PT J AU Schipani, F Miller, DR Ponce, MA Aldao, CM Akbar, SA Morris, PA Xu, JC AF Schipani, F. Miller, D. R. Ponce, M. A. Aldao, C. M. Akbar, S. A. Morris, P. A. Xu, J. C. TI Conduction mechanisms in SnO2 single-nanowire gas sensors: An impedance spectroscopy study SO SENSORS AND ACTUATORS B-CHEMICAL LA English DT Article DE Impedance spectroscopy; SnO2; Single nanowire; Multiple nanowire; Equivalent circuit ID THERMIONIC-FIELD EMISSION; SCHOTTKY-BARRIER; METAL-OXIDES; THICK-FILMS; DIFFUSION; OXYGEN; MODEL; NANOELECTRONICS; SEMICONDUCTORS; NANOCONTACT AB Results of studies on single and multiple SnO2 nanowire gas sensors with impedance spectroscopy are reported. Equivalent circuit modeling is used to draw fundamental conclusions about the dominant conduction mechanism in single-nanowire sensors, where the diameter of the nanowire is found to play a key role. This is then extended to multiple-nanowire sensors. For single-nanowire sensors, I-V measurements are also used to demonstrate that the contribution from the electrode-nanowire contact to the overall resistance changes with atmosphere and temperature. We find that for the randomly-orientated multiple-nanowire sensors, the main contribution to the resistance comes from the nanowire-nanowire junction. (C) 2016 Elsevier B.V. All rights reserved. C1 [Schipani, F.; Miller, D. R.; Akbar, S. A.; Morris, P. A.] Ohio State Univ, Dept Mat Sci & Engn, Columbus, OH 43212 USA. [Schipani, F.; Ponce, M. A.; Aldao, C. M.] Univ Mar del Plata, Inst Mat Sci & Technol INTEMA, B7608FDQ, Mar Del Plata, Buenos Aires, Argentina. [Schipani, F.; Ponce, M. A.; Aldao, C. M.] Natl Res Council CONICET, B7608FDQ, Mar Del Plata, Buenos Aires, Argentina. [Miller, D. R.; Xu, J. C.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Akbar, SA (reprint author), 2041 N Coll Rd, Columbus, OH 43210 USA. EM akbar.1@osu.edu FU Fulbright/BEC.AR Fellowship; NASA Space Technology Research Fellowship FX The current work was partially supported by a Fulbright/BEC.AR Fellowship and by a NASA Space Technology Research Fellowship. NR 41 TC 1 Z9 1 U1 36 U2 36 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0925-4005 J9 SENSOR ACTUAT B-CHEM JI Sens. Actuator B-Chem. PD MAR 31 PY 2017 VL 241 BP 99 EP 108 DI 10.1016/j.snb.2016.10.061 PG 10 WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation SC Chemistry; Electrochemistry; Instruments & Instrumentation GA EJ5JH UT WOS:000393253700013 ER PT J AU Moreno, A Olsen, CS AF Moreno, Adam Olsen, Christine S. TI Take rural road trips to promote science SO NATURE LA English DT Letter C1 [Moreno, Adam] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Olsen, Christine S.] Oregon State Univ, Corvallis, OR 97331 USA. RP Moreno, A (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM adam.l.moreno@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD MAR 30 PY 2017 VL 543 IS 7647 BP 623 EP 623 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EP8IS UT WOS:000397619700028 PM 28358059 ER PT J AU Dalin, C Wada, Y Kastner, T Puma, MJ AF Dalin, Carole Wada, Yoshihide Kastner, Thomas Puma, Michael J. TI Groundwater depletion embedded in international food trade SO NATURE LA English DT Article ID WATER-STRESS; RESOURCES; TRANSFERS; AQUIFERS AB Recent hydrological modelling(1) and Earth observations(2,3) have located and quantified alarming rates of groundwater depletion worldwide. This depletion is primarily due to water withdrawals for irrigation(1,2,4), but its connection with the main driver of irrigation, global food consumption, has not yet been explored. Here we show that approximately eleven per cent of non-renewable groundwater use for irrigation is embedded in international food trade, of which two-thirds are exported by Pakistan, the USA and India alone. Our quantification of groundwater depletion embedded in the world's food trade is based on a combination of global, crop-specific estimates of non-renewable groundwater abstraction and international food trade data. A vast majority of the world's population lives in countries sourcing nearly all their staple crop imports from partners who deplete groundwater to produce these crops, highlighting risks for global food and water security. Some countries, such as the USA, Mexico, Iran and China, are particularly exposed to these risks because they both produce and import food irrigated from rapidly depleting aquifers. Our results could help to improve the sustainability of global food production and groundwater resource management by identifying priority regions and agricultural products at risk as well as the end consumers of these products. C1 [Dalin, Carole] UCL, Inst Sustainable Resources, 14 Upper Woburn Pl, London WC1H 0NN, England. [Wada, Yoshihide] Int Inst Appl Syst Anal, Schlosspl 1, A-2361 Laxenburg, Austria. [Wada, Yoshihide; Puma, Michael J.] Columbia Univ, Ctr Climate Syst Res, 2880 Broadway, New York, NY 10025 USA. [Wada, Yoshihide; Puma, Michael J.] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. [Wada, Yoshihide] Univ Utrecht, Dept Phys Geog, Heidelberglaan 2, NL-3584 CS Utrecht, Netherlands. [Kastner, Thomas] Alpen Adria Univ Klagenfurt, Inst Social Ecol, Schottenfeldgasse 29, A-1070 Vienna, Austria. [Kastner, Thomas] Senckenberg Biodivers & Climate Res Ctr BiK F, Senckenberganlage 25, D-60325 Frankfurt, Germany. [Puma, Michael J.] Columbia Univ, Ctr Climate & Life, 61 Route 9W, Palisades, NY 10964 USA. RP Dalin, C (reprint author), UCL, Inst Sustainable Resources, 14 Upper Woburn Pl, London WC1H 0NN, England. EM c.dalin@ucl.ac.uk FU Belmont Forum (SAHEWS project) [NERC NE/L008785/1]; Economic and Social Research Council through the Centre for Climate Change Economics and Policy; Natural Environment Research Council Fellowship [NERC NE/N01524X/1]; European Research Council Starting Grant LUISE [263522]; Swedish Research Council Formas [231-2014-1181]; Columbia University Center for Climate and Life; Japan Society for the Promotion of Science (JSPS) [JSPS-2014-878]; OECD FX C.D. acknowledges the funding support of the Belmont Forum (SAHEWS project, NERC NE/L008785/1), the Economic and Social Research Council through the Centre for Climate Change Economics and Policy, and the Natural Environment Research Council Fellowship (NERC NE/N01524X/1). T.K. was supported by the European Research Council Starting Grant LUISE (263522) and the Swedish Research Council Formas (grant number 231-2014-1181). M.J.P. acknowledges fellowship support from the Columbia University Center for Climate and Life. Y.W. is supported by a Japan Society for the Promotion of Science (JSPS) Oversea Research Fellowship (JSPS-2014-878). This paper was presented at the conference Virtual Water in Agricultural Products: Quantification, Limitations and Trade Policy (Lincoln, Nebraska, USA, 14-16 September 2016), sponsored by the OECD Co-operative Research Programme: Biological Resource Management for Sustainable Agricultural Systems (CRP). The CRP financially supported C.D. to participate in the conference. The opinions expressed and arguments employed in this paper are the sole responsibility of the authors and do not necessarily reflect those of the OECD or of the governments of its Member countries. NR 30 TC 1 Z9 1 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD MAR 30 PY 2017 VL 543 IS 7647 BP 700 EP + DI 10.1038/nature21403 PG 17 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EP8IS UT WOS:000397619700052 PM 28358074 ER PT J AU Smith, R Li, JM Muller, A Salama, F AF Smith, Randall Li, Jia-Ming Mueller, Alfred Salama, Farid TI Special issue on atomic and molecular data for astrophysics SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Editorial Material C1 [Smith, Randall] Harvard Smithsonian Ctr Astrophys, High Energy Astrophys Dept, Cambridge, MA USA. [Li, Jia-Ming] Shanghai Jiao Tong Univ, Dept Phys, Shanghai 200030, Peoples R China. [Mueller, Alfred] Justus Liebig Univ Giessen, Inst Atom & Molphys, Giessen, Germany. [Salama, Farid] NASA, Ames Res Ctr, Space Sci Astrophys Branch, Mountain View, CA USA. RP Smith, R (reprint author), Harvard Smithsonian Ctr Astrophys, High Energy Astrophys Dept, Cambridge, MA USA. RI Muller, Alfred/A-3548-2009 OI Muller, Alfred/0000-0002-0030-6929 NR 0 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD MAR 28 PY 2017 VL 50 IS 6 AR 060201 DI 10.1088/1361-6455/aa5b22 PG 1 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA EN1KJ UT WOS:000395768600001 ER PT J AU Zevin, M Coughlin, S Bahaadini, S Besler, E Rohani, N Allen, S Cabero, M Crowston, K Katsaggelos, AK Larson, SL Lee, TK Lintott, C Littenberg, TB Lundgren, A Osterlund, C Smith, JR Trouille, L Kalogera, V AF Zevin, M. Coughlin, S. Bahaadini, S. Besler, E. Rohani, N. Allen, S. Cabero, M. Crowston, K. Katsaggelos, A. K. Larson, S. L. Lee, T. K. Lintott, C. Littenberg, T. B. Lundgren, A. Osterlund, C. Smith, J. R. Trouille, L. Kalogera, V. TI Gravity Spy: integrating advanced LIGO detector characterization, machine learning, and citizen science SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article DE gravitational waves; LIGO; detector characterization; citizen science; machine learning ID GALAXY ZOO; PROJECT AB With the first direct detection of gravitational waves, the advanced laser interferometer gravitational-wave observatory (LIGO) has initiated a new field of astronomy by providing an alternative means of sensing the universe. The extreme sensitivity required to make such detections is achieved through exquisite isolation of all sensitive components of LIGO from non-gravitational-wave disturbances. Nonetheless, LIGO is still susceptible to a variety of instrumental and environmental sources of noise that contaminate the data. Of particular concern are noise features known as glitches, which are transient and non-Gaussian in their nature, and occur at a high enough rate so that accidental coincidence between the two LIGO detectors is non-negligible. Glitches come in a wide range of time-frequency-amplitude morphologies, with new morphologies appearing as the detector evolves. Since they can obscure or mimic true gravitational-wave signals, a robust characterization of glitches is paramount in the effort to achieve the gravitational-wave detection rates that are predicted by the design sensitivity of LIGO. This proves a daunting task for members of the LIGO Scientific Collaboration alone due to the sheer amount of data. In this paper we describe an innovative project that combines crowdsourcing with machine learning to aid in the challenging task of categorizing all of the glitches recorded by the LIGO detectors. Through the Zooniverse platform, we engage and recruit volunteers from the public to categorize images of time-frequency representations of glitches into preidentified morphological classes and to discover new classes that appear as the detectors evolve. In addition, machine learning algorithms are used to categorize images after being trained on human-classified examples of the morphological classes. Leveraging the strengths of both classification methods, we create a combined method with the aim of improving the efficiency and accuracy of each individual classifier. The resulting classification and characterization should help LIGO scientists to identify causes of glitches and subsequently eliminate them from the data or the detector entirely, thereby improving the rate and accuracy of gravitational-wave observations. We demonstrate these methods using a small subset of data from LIGO's first observing run. C1 [Zevin, M.; Coughlin, S.; Larson, S. L.; Trouille, L.; Kalogera, V.] Northwestern Univ, CIERA, 2145 Sheridan Rd, Evanston, IL 60208 USA. [Zevin, M.; Coughlin, S.; Larson, S. L.; Trouille, L.; Kalogera, V.] Northwestern Univ, Deptartment Phys & Astron, 2145 Sheridan Rd, Evanston, IL 60208 USA. [Bahaadini, S.; Besler, E.; Rohani, N.; Katsaggelos, A. K.] Northwestern Univ, Elect Engn & Comp Sci, Evanston, IL 60201 USA. [Allen, S.; Larson, S. L.; Trouille, L.] Adler Planetarium, Chicago, IL 60605 USA. [Cabero, M.; Lundgren, A.] Max Planck Inst Gravitat Phys, Callinstr 38, D-30167 Hannover, Germany. [Crowston, K.; Osterlund, C.] Syracuse Univ, Sch Informat Studies, Syracuse, NY 13210 USA. [Lee, T. K.] Univ Utah, Dept Commun, Salt Lake City, UT 84112 USA. [Lintott, C.] Univ Oxford, Dept Phys, Oxford, England. [Littenberg, T. B.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Smith, J. R.] Calif State Univ Fullerton, Dept Phys, Fullerton, CA 92831 USA. RP Zevin, M (reprint author), Northwestern Univ, CIERA, 2145 Sheridan Rd, Evanston, IL 60208 USA.; Zevin, M (reprint author), Northwestern Univ, Deptartment Phys & Astron, 2145 Sheridan Rd, Evanston, IL 60208 USA. EM zevin@u.northwestern.edu; scottcoughlin2014@u.northwestern.edu FU National Science Foundation [INSPIRE 15-47880] FX The Gravity Spy team would like to acknowledge and thank the many Zooniverse volunteers who provided invaluable feedback during Gravity Spy beta tests, and delivered initial glitch classifications for which to test the methods presented in this paper. In addition, the team would like to thank the detector characterization working group of the LSC for useful comments and suggestions, in particular Jess McIver for input during the planning phases, Chris Pankow for useful discussions, and Duncan Macleod for technical support and thorough comments on this manuscript. We would like to thank our undergraduate research team: Luke Calian, Jessie Duncan, Ethan Marx, Isa Patane, Leah Perri, and Ben Sandeen, for contributing to multiple components of the project, including the building and curation of the initial training set of glitches. Lastly, we would like to thank the anonymous referees for useful comments on this manuscript. Gravity Spy is partly supported by the National Science Foundation, award INSPIRE 15-47880. This paper has been assigned LIGO document number ligo-P1600303. 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 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD MAR 23 PY 2017 VL 34 IS 6 AR 064003 DI 10.1088/1361-6382/aa5cea PG 22 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA EN3RF UT WOS:000395924900002 ER PT J AU Strohmayer, TE AF Strohmayer, T. E. TI X-Ray Spectro-polarimetry with Photoelectric Polarimeters SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation: polarimeters; methods: data analysis; polarization; techniques: polarimetric; X-rays: general ID POLARIZATION MEASUREMENTS AB We derive a generalization of forward fitting for X-ray spectroscopy to include linear polarization of X-ray sources, appropriate for the anticipated next generation of space-based photoelectric polarimeters. We show that the inclusion of polarization sensitivity requires joint fitting to three observed spectra, one for each of the Stokes parameters, I(E), U(E), and Q(E). The equations for Stokes' I(E) (the total intensity spectrum) are identical to the familiar case with no polarization sensitivity, and for which the model-predicted spectrum is obtained by a convolution of the source spectrum, F(E'), with the familiar energy response function, epsilon(E') R(E', E), where epsilon(E') and R(E', E) are the effective area and energy redistribution matrix, respectively. In addition to the energy spectrum, the two new relations for U(E) and Q(E) include the source polarization fraction and position angle versus energy, a(E'), and psi(')(0)(E'), respectively, and the model-predicted spectra for these relations are obtained by a convolution with the "modulated" energy response function, mu(E') is an element of(E')R(E, E'), where mu(E') is the energy-dependent modulation fraction that quantifies a polarimeter's angular response to 100% polarized radiation. We present results of simulations with response parameters appropriate for the proposed PRAXyS Small Explorer observatory to illustrate the procedures and methods, and we discuss some aspects of photoelectric polarimeters with relevance to understanding their calibration and operation. C1 [Strohmayer, T. E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, X Ray Astrophys Lab, Greenbelt, MD 20771 USA. RP Strohmayer, TE (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, X Ray Astrophys Lab, Greenbelt, MD 20771 USA. NR 29 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 MAR 20 PY 2017 VL 838 IS 1 AR 72 DI 10.3847/1538-4357/aa643d PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EQ2KA UT WOS:000397896600005 ER PT J AU Moore, RH Thornhill, KL Weinzierl, B Sauer, D D'Ascoli, E Kim, J Lichtenstern, M Scheibe, M Beaton, B Beyersdorf, AJ Barrick, J Bulzan, D Corr, CA Crosbie, E Jurkat, T Martin, R Riddick, D Shook, M Slover, G Voigt, C White, R Winstead, E Yasky, R Ziemba, LD Brown, A Schlager, H Anderson, BE AF Moore, Richard H. Thornhill, Kenneth L. Weinzierl, Bernadett Sauer, Daniel D'Ascoli, Eugenio Kim, Jin Lichtenstern, Michael Scheibe, Monika Beaton, Brian Beyersdorf, Andreas J. Barrick, John Bulzan, Dan Corr, Chelsea A. Crosbie, Ewan Jurkat, Tina Martin, Robert Riddick, Dean Shook, Michael Slover, Gregory Voigt, Christiane White, Robert Winstead, Edward Yasky, Richard Ziemba, Luke D. Brown, Anthony Schlager, Hans Anderson, Bruce E. TI Biofuel blending reduces particle emissions from aircraft engines at cruise conditions SO NATURE LA English DT Article ID IN-SITU OBSERVATIONS; BLACK CARBON EMISSIONS; FISCHER-TROPSCH FUELS; YOUNG CONTRAILS; CLIMATE IMPACT; JET ENGINE; AVIATION; ABSORPTION; INDEXES; PLUMES AB Aviation-related aerosol emissions contribute to the formation of contrail cirrus clouds that can alter upper tropospheric radiation and water budgets, and therefore climate(1). The magnitude of air-traffic-related aerosol-cloud interactions and the ways in which these interactions might change in the future remain uncertain(1). Modelling studies of the present and future effects of aviation on climate require detailed information about the number of aerosol particles emitted per kilogram of fuel burned and the microphysical properties of those aerosols that are relevant for cloud formation(2). However, previous observational data at cruise altitudes are sparse for engines burning conventional fuels2,3, and no data have previously been reported for biofuel use in-flight. Here we report observations from research aircraft that sampled the exhaust of engines onboard a NASA DC-8 aircraft as they burned conventional Jet A fuel and a 50: 50 (by volume) blend of Jet A fuel and a biofuel derived from Camelina oil. We show that, compared to using conventional fuels, biofuel blending reduces particle number and mass emissions immediately behind the aircraft by 50 to 70 per cent. Our observations quantify the impact of biofuel blending on aerosol emissions at cruise conditions and provide key microphysical parameters, which will be useful to assess the potential of biofuel use in aviation as a viable strategy to mitigate climate change. C1 [Moore, Richard H.; Thornhill, Kenneth L.; Beaton, Brian; Beyersdorf, Andreas J.; Barrick, John; Corr, Chelsea A.; Crosbie, Ewan; Martin, Robert; Riddick, Dean; Shook, Michael; Slover, Gregory; White, Robert; Winstead, Edward; Yasky, Richard; Ziemba, Luke D.; Anderson, Bruce E.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Thornhill, Kenneth L.; Barrick, John; Shook, Michael; Winstead, Edward] SSAI, Hampton, VA USA. [Weinzierl, Bernadett; Sauer, Daniel; D'Ascoli, Eugenio; Kim, Jin; Lichtenstern, Michael; Scheibe, Monika; Jurkat, Tina; Voigt, Christiane; Schlager, Hans] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Atmospher Phys, Oberpfaffenhofen, Germany. [Weinzierl, Bernadett] Univ Vienna, Vienna, Austria. [Sauer, Daniel; D'Ascoli, Eugenio] Ludwig Maximillians Univ, Munich, Germany. [Beyersdorf, Andreas J.] Calif State Univ San Bernardino, San Bernardino, CA 92407 USA. [Bulzan, Dan] NASA, Glenn Res Ctr, Cleveland, OH USA. [Corr, Chelsea A.] Bennington Coll, Bennington, VT USA. [Crosbie, Ewan] NASA, Postdoctoral Program, Columbia, MD USA. [Voigt, Christiane] Johannes Gutenberg Univ Mainz, Mainz, Germany. [Brown, Anthony] Natl Res Council Canada, Ottawa, ON, Canada. RP Moore, RH (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM richard.h.moore@nasa.gov OI Sauer, Daniel/0000-0002-0317-5063 FU NASA Advanced Air Vehicles Program, Advanced Air Transport Technology Project; DLR Aeronautics Research Programme; Transport Canada Clean Transportation Initiative; National Research Council Canada CAAFER Project [46FA-JA12]; NASA Postdoctoral Program fellowship; Helmholtz Association [VH-NG-606, W2/W3-060]; European Research Council [640458]; German Science Foundation (DFG) [JU3059/1-1] FX We thank the flight crew of the NASA DC-8 and DLR Falcon, W. Ringelberg, D. Fedors, T. Asher, M. Berry, B. Elit, T. Sandon, P. Weber, R. Welser, S. Kaufmann, T. Klausner, A. Reiter, A. Roiger, R. Schlage and U. Schumann for providing meteorological forecasts, and B. Karcher and P. Le Clercq for discussions. This work was supported by the NASA Advanced Air Vehicles Program, Advanced Air Transport Technology Project, the DLR Aeronautics Research Programme, the Transport Canada Clean Transportation Initiative, and the National Research Council Canada CAAFER Project (46FA-JA12). R.H.M. was supported, in part, by a NASA Postdoctoral Program fellowship. B. W. was supported by the Helmholtz Association (grant number VH-NG-606) and by the European Research Council grant agreement number 640458. C.V. and T.J. were supported by the Helmholtz Association (grant number W2/W3-060) and the German Science Foundation (DFG grant number JU3059/1-1). NR 47 TC 0 Z9 0 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD MAR 16 PY 2017 VL 543 IS 7645 BP 411 EP + DI 10.1038/nature21420 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EN9RN UT WOS:000396337400048 PM 28300096 ER PT J AU Soares, DD Lee, H Loikith, PC Barkhordarian, A Mechoso, CR AF Soares, Daniel de Barros Lee, Huikyo Loikith, Paul C. Barkhordarian, Armineh Mechoso, Carlos R. TI Can significant trends be detected in surface air temperature and precipitation over South America in recent decades? SO INTERNATIONAL JOURNAL OF CLIMATOLOGY LA English DT Article DE temperature trends; precipitation trends; South America; CMIP5 models ID EARTH SYSTEM MODEL; CLIMATE-CHANGE DETECTION; REGIONAL-SCALE; COUPLED MODEL; BASIC EVALUATION; OSCILLATION; CMIP5; SIMULATIONS; VARIABILITY; STREAMFLOW AB Trends in near-surface air temperature and precipitation over South America are examined for the periods 1975-2004 and 1955-2004, respectively, using multiple observational and climate model data sets. The results for observed near-surface air temperature show an overall warming trend over much of the continent, with the largest magnitudes over central Brazil. These observed trends are found to be statistically significant using pre-industrial control simulations from the fifth phase of the Coupled Model Intercomparison Project (CMIP5) as the baseline to estimate natural climate variability. The observed trends are compared with those obtained in natural-only CMIP5 simulations, in which only natural forcings (i.e. volcanoes and solar variability) are included, and in historical CMIP5 simulations, in which anthropogenic forcings (i.e. changes in the atmospheric composition) are further incorporated. The historical CMIP5 simulations are more successful in capturing the observed temperature trends than the simulations with natural forcings only. It is suggested that anthropogenic warming is already evident over much of South America. Unlike the warming trends, observed precipitation trends over South America are less spatially coherent with both negative and positive values across the continent. Significant positive trends are found over South America in only one of the data sets used, and over a region that roughly encompasses the southern part of La Plata Basin (southern Brazil, Uruguay, and northeastern Argentina) in all data sets used. The historical CMIP5 simulations do not capture this feature. No firm conclusions are reached, therefore, for anthropogenic influences on precipitation changes in the period selected for study. C1 [Soares, Daniel de Barros; Barkhordarian, Armineh; Mechoso, Carlos R.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90024 USA. [Soares, Daniel de Barros] Ecole Polytech, Palaiseau, France. [Lee, Huikyo] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Loikith, Paul C.] Portland State Univ, Dept Geog, POB 751 GEOG, Portland, OR 97207 USA. RP Loikith, PC (reprint author), Portland State Univ, Dept Geog, POB 751 GEOG, Portland, OR 97207 USA. EM ploikith@pdx.edu FU US Department of Energy under the GoAmazon programme; US National Science Foundation [AGS-1547899]; National Aeronautics and Space Administration FX Partial support at University of California Los Angeles was provided by the US Department of Energy under the GoAmazon2014/5 programme. Support was provided by the US National Science Foundation AGS-1547899. The contribution by H.L. to this study was carried out on behalf of the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 48 TC 0 Z9 0 U1 0 U2 0 PU WILEY PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0899-8418 EI 1097-0088 J9 INT J CLIMATOL JI Int. J. Climatol. PD MAR 15 PY 2017 VL 37 IS 3 BP 1483 EP 1493 DI 10.1002/joc.4792 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EM5KD UT WOS:000395349500026 ER PT J AU Choi, YS Gim, HJ Ho, CH Jeong, SJ Park, SK Hayes, MJ AF Choi, Yong-Sang Gim, Hyeon-Ju Ho, Chang-Hoi Jeong, Su-Jong Park, Seon Ki Hayes, Michael J. TI Climatic influence on corn sowing date in the Midwestern United States SO INTERNATIONAL JOURNAL OF CLIMATOLOGY LA English DT Article DE corn (maize); sowing date; climatic influence; the Midwestern United Sates ID RAIN-FED CONDITIONS; PLANTING DATE; POTENTIAL IMPACT; NORTH-AMERICA; BURKINA-FASO; MAIZE YIELDS; CROP MODEL; PHENOLOGY; AGRICULTURE; BALANCE AB This study investigated the climatic influence on the corn sowing date in the Midwestern United States by comparing the survey data of corn cultivation with meteorological records in nine states for the last 36years (1979-2014). The results show that the year-to-year changes in the sowing date were significantly affected by springtime air temperature and precipitation in the nine states, although large state-to-state differences were found in the degree of sowing date-meteorology relationship. We determined that the 36-year climatological warm period (CWP) with daily mean temperatures 10 degrees C plays an important role in the state-to-state differences. For the states with longer CWPs, the influence of air temperature (precipitation) was generally weaker (stronger). This observed counteractive relationship should be considered for crop modelling for more effective assessment of the impact of climate change on agriculture. C1 [Choi, Yong-Sang; Park, Seon Ki] Ewha Womans Univ, Dept Environm Sci & Engn, Seoul, South Korea. [Gim, Hyeon-Ju; Ho, Chang-Hoi] Seoul Natl Univ, Sch Earth & Environm Sci, 1 Gwanak Ro, Seoul 151747, South Korea. [Choi, Yong-Sang; Gim, Hyeon-Ju; Ho, Chang-Hoi; Park, Seon Ki] Ewha Womans Univ, Ctr Climate Environm Change Predict Res, Seoul, South Korea. [Jeong, Su-Jong] South Univ Sci & Technol China, Sch Environm Sci & Engn, Shenzhen, Peoples R China. [Hayes, Michael J.] Univ Nebraska Lincoln, Natl Drought Mitigat Ctr, Lincoln, NE USA. [Choi, Yong-Sang] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Ho, CH (reprint author), Seoul Natl Univ, Sch Earth & Environm Sci, 1 Gwanak Ro, Seoul 151747, South Korea. EM hoch@cpl.snu.ac.kr FU Korea Meteorological Administration Research and Development Program [KMIPA2015-6110]; Jet Propulsion Laboratory, California Institute of Technology; South University of Science and Technology of China FX This study was funded by the Korea Meteorological Administration Research and Development Program (KMIPA2015-6110). Y.-S. Choi is supported by Jet Propulsion Laboratory, California Institute of Technology. S.-J. Jeong is supported by the internal research fund of the South University of Science and Technology of China. NR 44 TC 0 Z9 0 U1 0 U2 0 PU WILEY PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0899-8418 EI 1097-0088 J9 INT J CLIMATOL JI Int. J. Climatol. PD MAR 15 PY 2017 VL 37 IS 3 BP 1595 EP 1602 DI 10.1002/joc.4799 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EM5KD UT WOS:000395349500033 ER PT J AU Sangha, S Peltzer, G Zhang, AL Meng, LS Liang, CR Lundgren, P Fielding, E AF Sangha, Simran Peltzer, Gilles Zhang, Ailin Meng, Lingsen Liang, Cunren Lundgren, Paul Fielding, Eric TI Fault geometry of 2015, Mw7.2 Murghab, Tajikistan earthquake controls rupture propagation: Insights from InSAR and seismological data SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE earthquake; Tajikistan; InSAR; geodesy; seismology; back-projection ID NORTHERN KARAKORAM FAULT; SHAN EXTENSIONAL SYSTEM; SAREZ-PAMIR EARTHQUAKE; STRIKE-SLIP MOTION; CENTRAL-ASIA; SATELLITE RADAR; SOUTHERN TIBET; SEISMIC DATA; TIEN-SHAN; DEFORMATION AB Combining space-based geodetic and array seismology observations can provide detailed information about earthquake ruptures in remote regions. Here we use Landsat-8 imagery and ALOS-2 and Sentinel-1 radar interferometry data combined with data from the European seismology network to describe the source of the December 7, 2015, Mw7.2 Murghab (Tajikistan) earthquake. The earthquake reactivated a similar to 79 km-long section of the Sarez-Karakul Fault, a NE oriented sinistral, trans-tensional fault in northern Pamir. Pixel offset data delineate the geometry of the surface break and line of sight ground shifts from two descending and three ascending interferograms constrain the fault dip and slip solution. Two right stepping, NE-striking segments connected by a more easterly oriented segment, sub-vertical or steeply dipping to the west were involved. The solution shows two main patches of slip with up to 3.5 m of left lateral slip on the southern and central fault segments. The northern segment has a left-lateral and normal oblique slip of up to a meter. Back-projection of high-frequency seismic waves recorded by the European network, processed using the Multitaper-MUSIC approach, focuses sharply along the surface break. The time progression of the high-frequency radiators shows that, after a 10 second initiation phase at slow speed, the rupture progresses in 2 phases at super-shear velocity (similar to 4.3-5 km/s) separated by a 3 second interval of slower propagation corresponding to the passage through the restraining bend. The intensity of the high-frequency radiation reaches maxima during the initial and middle phases of slow propagation and is reduced by 50% during the super-shear phases of the propagation. These findings are consistent with studies of other strike-slip earthquakes in continental domain, showing the importance of fault geometric complexities in controlling the speed of fault propagation and related spatiotemporal pattern of the high-frequency radiation. (C) 2017 Elsevier B.V. All rights reserved. C1 [Sangha, Simran; Peltzer, Gilles; Zhang, Ailin; Meng, Lingsen] Univ Calif Los Angeles, Earth Planetary & Space Sci Dept, Los Angeles, CA 90024 USA. [Peltzer, Gilles; Liang, Cunren; Lundgren, Paul; Fielding, Eric] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Sangha, S; Peltzer, G (reprint author), Univ Calif Los Angeles, Earth Planetary & Space Sci Dept, Los Angeles, CA 90024 USA.; Peltzer, G (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM sssangha@ucla.edu; peltzer@ucla.edu FU Japan Aerospace Exploration Agency (JAXA) under PI Project [P1372]; NSF EarthScope [EAR-1614609] FX We thank M.-H. Huang and C. Yin for discussions on inversion approaches. Two anonymous reviewers gave detailed and constructive comments that improved the original manuscript. European Space Agency, Copernicus Sentinel data 2015, retrieved from ASF DAAC 7 January 2016. ALOS-2 data were provided by the Japan Aerospace Exploration Agency (JAXA) under PI Project P1372. Panchromatic Remote-sensing instrument for Stereo Mapping (PRISM) data was obtained from JAXA (http://www.eorc.jaxa.jp/ALOS/en/aw3d30/). The Incorporated Research Institutions for Seismology (IRIS) (www.iris.edu) and the European ORFEUS (www.orfeus-eu.org) data centers provided access to broadband seismograms. The earthquake catalogs were obtained from the International Seismological Center (ISC) bulletin (http://www.isc.ac.uk/), National Earthquake Information Center (NEIC) (http:// earthquake.usgs.gov/), and IRIS (http://ds.iris.edu/). A. Zhang was supported by NSF EarthScope proposal EAR-1614609. Some figures were prepared using the Generic Mapping Tools (GMT; Wessel and Smith, 1998). The work was done in part at the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. NR 50 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD MAR 15 PY 2017 VL 462 BP 132 EP 141 DI 10.1016/j.epsl.2017.01.018 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EM8ZP UT WOS:000395600900013 ER PT J AU Anderson, RL Easton, RW Lo, MW AF Anderson, Rodney L. Easton, Robert W. Lo, Martin W. TI Isolating blocks as computational tools in the circular restricted three-body problem SO PHYSICA D-NONLINEAR PHENOMENA LA English DT Article DE Circular restricted three-body problem; Isolating blocks; Invariant manifolds; Invariant 3-sphere ID INVARIANT-MANIFOLDS; PERIODIC-ORBITS AB Isolating blocks may be used as computational tools to search for the invariant manifolds of orbits and hyperbolic invariant sets associated with libration points while also giving additional insight into the dynamics of the flow in these regions. We use isolating blocks to investigate the dynamics of objects entering the Earth-Moon system in the circular restricted three-body problem with energies close to the energy of the L-2 libration point. Specifically, the stable and unstable manifolds of Lyapunov orbits and the hyperbolic invariant set around the libration points are obtained by numerically computing the way orbits exit from an isolating block in combination with a bisection method. Invariant spheres of solutions in the spatial problem may then be located using the resulting manifolds. (C) 2016 Elsevier B.V. All rights reserved. C1 [Anderson, Rodney L.; Lo, Martin W.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-121, Pasadena, CA 91109 USA. [Easton, Robert W.] Univ Colorado, Appl Math, Boulder, CO 80309 USA. RP Anderson, RL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-121, Pasadena, CA 91109 USA. EM rodney.l.anderson@jpl.nasa.gov FU AMMOS/MGSS program FX The research presented here has been carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This research was funded under the AMMOS/MGSS program. The authors would like to thank Jim Meiss and Holger Dullin for their helpful discussions.(c)2016 California Institute of Technology. Government sponsorship acknowledged. Earlier version presented as a conference paper at the AAS/AIAA Astro. Spec. Conf., MS 15-615, Vail, CO, Aug. 9-13,2015. NR 19 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0167-2789 EI 1872-8022 J9 PHYSICA D JI Physica D PD MAR 15 PY 2017 VL 343 BP 38 EP 50 DI 10.1016/j.physd.2016.10.004 PG 13 WC Mathematics, Applied; Physics, Multidisciplinary; Physics, Mathematical SC Mathematics; Physics GA EL4ZL UT WOS:000394631000004 ER PT J AU Wiesner, VL Vempati, UK Bansal, NP AF Wiesner, Valerie L. Vempati, Udaya K. Bansal, Narottam P. TI High temperature viscosity of calcium-magnesium-aluminosilicate glass from synthetic sand (vol 124, pg 189, 2016) SO SCRIPTA MATERIALIA LA English DT Correction C1 [Wiesner, Valerie L.; Bansal, Narottam P.] NASA, Mat & Struct Div, Glenn Res Ctr, Cleveland, OH 44135 USA. [Vempati, Udaya K.] Owens Brockway Glass Container Inc, Perrysburg, OH 43551 USA. RP Wiesner, VL (reprint author), NASA, Mat & Struct Div, Glenn Res Ctr, Cleveland, OH 44135 USA. EM valerie.l.wiesner@nasa.gov NR 1 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 1359-6462 J9 SCRIPTA MATER JI Scr. Mater. PD MAR 15 PY 2017 VL 130 BP 298 EP 298 DI 10.1016/j.scriptamat.2016.12.007 PG 1 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA EK8SI UT WOS:000394194200065 ER PT J AU Steeves, J Pellegrino, S AF Steeves, John Pellegrino, Sergio TI Post-cure shape errors of ultra-thin symmetric CFRP laminates: Effect of ply-level imperfections SO COMPOSITE STRUCTURES LA English DT Article DE Thin-ply composites; CFRP; Cross-ply; Imperfections; Shape errors ID TOOL-PART INTERACTION; FIBER COMPOSITES; MISALIGNMENT; DEFORMATION AB This paper discusses the effect of misalignments in ply orientation, uniform variations in ply thickness, and through-thickness thermal gradients on the post-cure shape errors for symmetric cross-ply laminates constructed from ultra-thin composite materials. Photogrammetry-based surface measurements are performed for laminates cured at elevated temperatures. Significant out-of-plane shape errors are observed, with amplitudes 75 times the laminate thickness. The magnitude of each imperfection is also characterized experimentally on coupon-level samples. A non-linear finite element model is developed and demonstrates that these imperfections result in cylindrical and twisting modes of deformation. Results are compared to Classical Lamination Theory predictions which are shown to be inadequate in predicting shape errors that require changes in Gaussian curvature. Through these studies, it is determined that thickness variations between the top and bottom plies have the most pronounced effect on shape errors. (C) 2017 Elsevier Ltd. All rights reserved. C1 [Steeves, John] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Pellegrino, Sergio] CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA. RP Steeves, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM john.b.steeves@jp1.nasa.gov FU Natural Sciences and Engineering Research Council (NSERC) of Canada FX Financial support from the Natural Sciences and Engineering Research Council (NSERC) of Canada is gratefully acknowledged. A 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 (NASA). NR 30 TC 0 Z9 0 U1 3 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0263-8223 EI 1879-1085 J9 COMPOS STRUCT JI Compos. Struct. PD MAR 15 PY 2017 VL 164 BP 237 EP 247 DI 10.1016/j.compstruct.2016.12.075 PG 11 WC Materials Science, Composites SC Materials Science GA EK0PE UT WOS:000393628100023 ER PT J AU Prockter, LM Shirley, JH Dalton, JB Kamp, L AF Prockter, Louise M. Shirley, James H. Dalton, James B., III Kamp, L. TI Surface composition of pull-apart bands in Argadnel Regio, Europa: Evidence of localized cryovolcanic resurfacing during basin formation SO ICARUS LA English DT Article DE Europa; Galileo; NIMS; SSI; Bands ID SULFURIC-ACID HYDRATE; GALILEAN SATELLITES; ICE SHELL; WATER ICE; CHAOS TERRAIN; GRAIN-SIZE; RADIOLYSIS; ORIGIN; SEPARATION; EVOLUTION AB We combine Galileo Solid State Imager (SSI) and Near-Infrared Mapping Spectrometer (NIMS) data to investigate the composition of pull-apart bands in Europa's Argadnel Regio. Using spectral linear mixture modeling employing cryogenic laboratory reference spectra, we find that bands of intermediate age ("grey" bands) are compositionally distinct from bands that are stratigraphically younger ("dark" bands). The grey bands have higher abundances of larger ice grains and lower abundances of hydrated salts than the dark bands; both of these tendencies are statistically significant at the 1% level. The grey and dark bands have similar abundances of hexahydrite, a material which is relatively stable under irradiation; however, the derived abundances of frozen magnesium sulfate brine and of mirabilite, which are more susceptible to fragmentation by radiation, are significantly higher in the dark bands than in the grey bands. These results are consistent with a physical model in which the differences in composition and in ice grain sizes are linked to space weathering and radiolytic processing levels; the grey bands have presumably undergone higher levels of processing, due to being exposed on Europa's surface for a longer period of time. One prominent wedge-shaped band exhibits an anomalous albedo variation across its northern portion, appearing dark in its top third, and grey in its southernmost two-thirds. We find that the dark part of the band has a modeled composition that is in-family with other dark bands, while the grey portion has a modeled composition that is indistinguishable from other grey bands in the study area. Because these variations cannot easily be attributed to the band's formation mechanism (bands open sequentially along a central axis), we surmise that the northern part has been resurfaced, probably in response to the formation of a large topographic basin that cuts through the band. Faulting accompanying basin formation may provide conduits allowing transport to the surface of materials from Europa's interior. We hypothesize that the formation of the basin resulted in fresh cryovolcanic material being deposited across the northern portion of the band, effectively "resetting" its surface age. If, as has been suggested, the giant arcuate basins resulted from an episode of true polar wander, our study may help to more tightly constrain the age of that event within Europa's geologic column. (C) 2016 Elsevier Inc. All rights reserved. C1 [Prockter, Louise M.] Johns Hopkins Univ, Appl Phys Lab, 11101 Johns Hopkins Rd, Laurel, MD 20723 USA. [Prockter, Louise M.] Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA. [Shirley, James H.; Dalton, James B., III; Kamp, L.] Jet Prop Lab, Mail Stop 183-601,4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Prockter, LM (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11101 Johns Hopkins Rd, Laurel, MD 20723 USA.; Prockter, LM (reprint author), Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA. EM prockter@lpi.usra.edu FU NASA ROSES Outer Planets Research [NRANNH09ZDA001N] FX The authors would like to thank Tim Cassidy for reviewing an earlier draft of the manuscript. Comments and questions from two anonymous referees materially improved this paper. Funding for this project was gratefully received from NASA ROSES Outer Planets Research grant NRANNH09ZDA001N to JBD and through a subcontract to LP at JHU/APL. LPI Contribution No. 1992. NR 62 TC 0 Z9 0 U1 1 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR 15 PY 2017 VL 285 BP 27 EP 42 DI 10.1016/j.icarus.2016.11.024 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EJ5KP UT WOS:000393257200003 ER PT J AU Vander Kaaden, KE McCubbin, FM Nittler, LR Peplowski, PN Weider, SZ Frank, EA McCoy, TJ AF Vander Kaaden, Kathleen E. McCubbin, Francis M. Nittler, Larry R. Peplowski, Patrick N. Weider, Shoshana Z. Frank, Elizabeth A. McCoy, Timothy J. TI Geochemistry, mineralogy, and petrology of boninitic and komatiitic rocks on the mercurian surface: Insights into the mercurian mantle SO ICARUS LA English DT Article DE Mercury; Petrologic classification; IUGS; Boninites; Komatiites ID X-RAY SPECTROMETER; EXPLOSIVE VOLCANISM; PLANETS FORMATION; MAGNETIC-FIELD; SMOOTH PLAINS; LUNAR CRUST; MESSENGER; MARINER-10; REFLECTANCE; CONSTRAINTS AB Orbital data from the MESSENGER mission to Mercury have facilitated a new view of the planet's structure, chemical makeup, and diverse surface, and have confirmed Mercury's status as a geochemical end member among the terrestrial planets. In this work, the most recent results from MESSENGER's X-Ray Spectrometer, Gamma-Ray Spectrometer, and Neutron Spectrometer have been used to identify nine distinct geochemical regions on Mercury. Using a variation on the classical CIPW normative mineralogy calculation, elemental composition data is used to constrain the potential mineralogy of Mercury's surface; the calculated silicate mineralogy is dominated by plagioclase, pyroxene (both orthopyroxene and clinopyroxene), and olivine, with lesser amounts of quartz. The range in surface compositions indicate that the rocks on the surface of Mercury are diverse and vary from komatiitic to boninitic. The high abundance of alkalis on Mercury's surface results in several of the nine regions being classified as alkali rich komatiites and/or boninites. In addition, Mercury's surface terranes span a wide range of SiO2 values that encompass crustal compositions that are more silica-rich than geochemical terranes on the Moon, Mars, and Vesta, but the range is similar to that of Earth. Although the composition of Mercury's surface appears to be chemically evolved, the high SiO2 content is a primitive feature and a direct result of the planet's low oxygen fugacity. (C) 2016 Elsevier Inc. All rights reserved. C1 [Vander Kaaden, Kathleen E.; McCubbin, Francis M.] Univ New Mexico, Dept Earth & Planetary Sci, Inst Meteorit, Albuquerque, NM 87131 USA. [Vander Kaaden, Kathleen E.] Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA. [Vander Kaaden, Kathleen E.; McCubbin, Francis M.] NASA, Johnson Space Ctr, Mailcode XI2,2101 NASA Pkwy, Houston, TX 77058 USA. [Nittler, Larry R.; Weider, Shoshana Z.; Frank, Elizabeth A.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Peplowski, Patrick N.] Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. [McCoy, Timothy J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, 10th & Constitut Aves NW, Washington, DC 20560 USA. RP Vander Kaaden, KE (reprint author), Univ New Mexico, Dept Earth & Planetary Sci, Inst Meteorit, Albuquerque, NM 87131 USA. EM kvander@unm.edu FU NASA Solar System Workings Grant [NNX16AK39G]; NASA Headquarters under the NASA Earth and Space Science Fellowship [NNX15AQ8OH] FX We thank the MESSENGER Science Team, with special thanks to the MESSENGER Geochemistry Discipline Group, for fruitful discussions regarding the interpretation of MESSENGER data and preparation of this manuscript. We also thank Ryan Zeigler, Randy Korotev, Alison Santos, and Dave Mittlefehldt for helpful discussions regarding lunar, martian, and vestan chemical compositions. This manuscript benefitted from thoughtful reviews by Justin Filiberto and Rachel Klima as well as editorial handling by Oded Aharonson. This work was funded by a NASA Solar System Workings Grant NNX16AK39G to FMM. This work was also supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program-Grant NNX15AQ8OH awarded to KEVK. NR 100 TC 0 Z9 0 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 MAR 15 PY 2017 VL 285 BP 155 EP 168 DI 10.1016/j.icarus.2016.11.041 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EJ5KP UT WOS:000393257200013 ER PT J AU Levy, JS Goudge, TA Head, JW Fassett, CI AF Levy, Joseph S. Goudge, Timothy A. Head, James W. Fassett, Caleb I. TI Candidate volcanic and impact-induced ice depressions on Mars SO ICARUS LA English DT Article DE Mars; Mars surface; Impact processes; Volcanism ID MOUNTAIN GLACIER DEPOSITS; CONCENTRIC CRATER FILL; LOBATE DEBRIS APRONS; ARSIA MONS; HEAT-TRANSFER; NORTH-SEA; LANDFORMS; ERUPTION; FLOW; ACCUMULATION AB We present an analysis of two concentrically-fractured depressions on Mars, one in northern Hellas and the second in Galaxias Fossae. Volumetric measurements indicate that similar to 2.4 km(3) and similar to 0.2 km(3) of material was removed in order to form the North Hellas and Galaxias depressions. The removed material is inferred to be predominantly water ice. Calorimetric estimates suggest that up to similar to 10(3)-10(5) m(3) of magma would have been required to melt/sublimate such a volume of ice under an ice/magma interaction scenario. This process would lead to subsidence and cracking of the surface, which could produce the observed concentric fracture (crevasse-like) morphology. While the Galaxias Fossae landform morphology is consistent with an impact origin, the large volume of removed material in North Hellas is less consistent with an impact origin and is interpreted to have resulted from volcanic melting of ice. The possibility of liquid water formation during or subsequent to volcanism or an impact could generate locally-enhanced habitable conditions, making these features tantalizing geological and astrobiological exploration targets. (C) 2016 Elsevier Inc. All rights reserved. C1 [Levy, Joseph S.] Univ Texas Austin, Inst Geophys, Austin, TX 78758 USA. [Goudge, Timothy A.] Univ Texas Austin, Jackson Sch Geosci, Austin, TX 78712 USA. [Head, James W.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA. [Fassett, Caleb I.] Mt Holyoke Coll, S Hadley, MA 01075 USA. [Fassett, Caleb I.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Levy, JS (reprint author), Univ Texas Austin, Inst Geophys, Austin, TX 78758 USA. EM joe.levy@utexas.edu FU NASA Mars Data Analysis Program award [NNX13AN5OG]; CIF FX Special thanks to the HiRISE and CTX teams for access to the high-quality image datasets used in this analysis. Thanks to Sam Peel and Cassie Stuurman for helpful discussion and to Dr. John Smellie and Dr. David Shean for their constructive reviews. This work was supported in part by NASA Mars Data Analysis Program award NNX13AN5OG to JSL and CIF. NR 62 TC 0 Z9 0 U1 6 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR 15 PY 2017 VL 285 BP 185 EP 194 DI 10.1016/j.icarus.2016.10.021 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EJ5KP UT WOS:000393257200015 ER PT J AU Schaible, MJ Johnson, RE Zhigilei, LV Piqueux, S AF Schaible, M. J. Johnson, R. E. Zhigilei, L. V. Piqueux, S. TI High energy electron sintering of icy regoliths: Formation of the PacMan thermal anomalies on the icy Saturnian moons SO ICARUS LA English DT Article ID E-RING; DUST MEASUREMENTS; SOLAR-SYSTEM; ENCELADUS; SURFACE; INTERSTELLAR; ORIGIN; ION; CONDUCTIVITY; CONDUCTANCE AB The so-called 'PacMan' features on the leading hemispheres of the icy Saturnian moons of Mimas, Tethys and Dione were initially identified as anomalous optical discolorations and subsequently shown to have greater thermal inertia than the surrounding regions. The shape of these regions matches calculated deposition contours of high energy plasma electrons moving opposite to the moon's orbital direction, thus suggesting that electron interactions with the grains produce the observed anomalies. Here, descriptions of radiation-induced diffusion processes are given, and various sintering models are considered to calculate the rate of increase in the contact volume between grains in an icy regolith. Estimates of the characteristic sintering timescale, i.e. the time necessary for the thermal inertia to increase from that measured outside the anomalous regions to that within, are given for each of the moons. Since interplanetary dust particle (IDP) impact gardening and E-ring grain infall would be expected to mix the regolith and obscure the effects of high energy electrons, sintering rates are compared to rough estimates of the impact-induced resurfacing rates. Estimates of the sintering timescale determined by extrapolating laboratory measurements are below similar to 0.03 Myr, while the regolith renewal timescales are larger than similar to 0.1 Myr, thus indicating that irradiation by the high energy electrons should be sufficient to form stable thermal anomalies. More detailed models developed for sintering of spherical grains are able to account for the radiation-induced anomalies on Mimas and Tethys only if the regoliths on those bodies are relatively compact and composed of small (less than or similar to 5 mu m) grains or grain aggregates, and/or the grains are highly non-spherical with surface defect densities in the inter-grain contact regions that are much higher than expected for crystalline water ice grains at thermal equilibrium. These results are consistent with regolith thermal conductivity models which can only be reconciled with spacecraft observations if the contacts between grains are assumed to have much lower thermal conductance than predicted for idealized grains. The strength of the anomalies on Tethys and Dione appear to be limited by E-ring grain infall, while on Mimas IDP gardening limits the strength of the anomaly. The smaller flux of more deeply penetrating high energy (>1 MeV) electrons on Dione can account for the small thermal inertia differences measured there. Determining regolith sintering rates and the corresponding effect on thermal conductivity can, in principle, provide an independent constraint on the regolith grain geometries and exposure timescales for icy bodies. (C) 2016 Elsevier Inc. All rights reserved. C1 [Schaible, M. J.; Johnson, R. E.; Zhigilei, L. V.] Univ Virginia, Dept Mat Sci & Engn, Charlottesville, VA 22903 USA. [Piqueux, S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Schaible, MJ (reprint author), Univ Virginia, Dept Mat Sci & Engn, Charlottesville, VA 22903 USA. EM ms5vf@virginia.edu NR 70 TC 1 Z9 1 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 MAR 15 PY 2017 VL 285 BP 211 EP 223 DI 10.1016/j.icarus.2016.08.033 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EJ5KP UT WOS:000393257200017 ER PT J AU Heggy, E Scabbia, G Bruzzone, L Pappalardo, RT AF Heggy, Essam Scabbia, Giovanni Bruzzone, Lorenzo Pappalardo, Robert T. TI Radar probing of Jovian icy moons: Understanding subsurface water and structure detectability in the JUICE and Europa missions SO ICARUS LA English DT Article DE Radar; Dielectric; Ganymede; Europa; Callisto; JUICE ID GALILEAN SATELLITES; CRATERING RATES; GROOVED TERRAIN; GANYMEDE; SURFACE; CALLISTO; OCEANS; CONSTRAINTS; TOPOGRAPHY; DEPOSITS AB Radar probing of Jovian icy satellites is fundamental for understanding the moons' origin and their thermal evolution as potential habitable environments in our Solar System. Using the current state of knowledge of the geological and geophysical properties of Ganymede, Europa and Callisto, we perform a comprehensive radar detectability study to quantify the exploration depth and the lower limit for subsurface identification of water and key tectonic structural elements. To achieve these objectives, we establish parametric dielectric models that reflect different hypotheses on the formation and thermal evolution of each moon. The models are then used for FDTD radar propagation simulations at the 9-MHz sounding frequency proposed for both ESA JUICE and NASA Europa missions. We investigate the detectability above the galactic noise level of four predominant subsurface features: brittle-ductile interfaces, shallow faults, brine aquifers, and the hypothesized global oceans. For Ganymede, our results suggest that the brittle-ductile interface could be within radar detectability range in the bright terrains, but is more challenging for the dark terrains. Moreover, understanding the slope variation of the brittle-ductile interface is possible after clutter reduction and focusing. For Europa, the detection of shallow subsurface structural elements few kilometers deep (such as fractures, faults and brine lenses) is achievable and not compromised by surface clutter. The objective of detecting the potential deep global ocean on Europa is also doable under both the convective and conductive hypotheses. Finally, for Callisto, radar waves can achieve an average penetration depth of 15 km, although the current understanding of Callisto's subsurface dielectric properties does not suggest sufficiently strong contrasts to produce unambiguous radar returns. (C) 2016 Elsevier Inc. All rights reserved. C1 [Heggy, Essam; Scabbia, Giovanni] Univ Southern Calif, Ming Hsieh Dept Elect Engn, 1042 Downey Way, Los Angeles, CA 90089 USA. [Heggy, Essam; Scabbia, Giovanni; Pappalardo, Robert T.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Bruzzone, Lorenzo] Univ Trento, Dept Informat Engn & Comp Sci, Remote Sensing Lab, Via Sommar 14, I-38123 Trento, Italy. RP Heggy, E (reprint author), Univ Southern Calif, Ming Hsieh Dept Elect Engn, 1042 Downey Way, Los Angeles, CA 90089 USA.; Heggy, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM heggy@usc.edu OI Heggy, Essam/0000-0001-7476-2735; Bruzzone, Lorenzo/0000-0002-6036-459X; Pappalardo, Robert/0000-0003-2571-4627 FU NASA Planetary Geology and Geophysics program [NNXZO8AKA2G, NNGO5GL11G] FX This work was supported in part by NASA Planetary Geology and Geophysics program under grants NNXZO8AKA2G and NNGO5GL11G. The authors would like to acknowledge the Italian Space Agency ASI for its support to the part of this study performed in the University of Trento. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 79 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 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR 15 PY 2017 VL 285 BP 237 EP 251 DI 10.1016/j.icarus.2016.11.039 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EJ5KP UT WOS:000393257200019 ER PT J AU Choblet, G Tobie, G Sotin, C Kalousova, K Grasset, O AF Choblet, G. Tobie, G. Sotin, C. Kalousova, K. Grasset, O. TI Heat transport in the high-pressure ice mantle of large icy moons SO ICARUS LA English DT Article DE Ganymede; Titan; Callisto; Ices; Interiors ID INTERNAL STRUCTURE; THERMAL EVOLUTION; OCEAN PLANETS; DYNAMICS; GANYMEDE; CONVECTION; CALLISTO; PHASE; TITAN; SHELL AB While the existence of a buried ocean sandwiched between surface ice and high-pressure (HP) poly morphs of ice emerges as the most plausible structure for the hundreds-of-kilometers thick hydrospheres within large icy moons of the Solar System (Ganymede, Callisto, Titan), little is known about the thermal structure of the deep HP ice mantle and its dynamics, possibly involving melt production and extraction. This has major implications for the thermal history of these objects as well as on the habitability of their ocean as the HP ice mantle is presumed to limit chemical transport from the rock component to the ocean. Here, we describe 3D spherical simulations of subsolidus thermal convection tailored to the specific structure of the HP ice mantle of large icy moons. Melt production is monitored and melt transport is simplified by assuming instantaneous extraction to the ocean above. The two controlling parameters for these models are the rheology of ice VI and the heat flux from the rock core. Reasonable end-members are considered for both parameters as disagreement remains on the former (especially the pressure effect on viscosity) and as the latter is expected to vary significantly during the moon's history. We show that the heat power produced by radioactive decay within the rock core is mainly transported through the HP ice mantle by melt extraction to the ocean, with most of the melt produced directly above the rock/water interface. While the average temperature in the bulk of the HP ice mantle is always relatively cool when compared to the value at the interface with the rock core (similar to 5 K above the value at the surface of the HP ice mantle), maximum temperatures at all depths are close to the melting point, often leading to the interconnection of a melt path via hot convective plume conduits throughout the HP ice mantle. Overall, we predict long periods of time during these moons' history where water generated in contact with the rock core is transported to the above ocean. (C) 2016 Elsevier Inc. All rights reserved. C1 [Choblet, G.; Tobie, G.; Grasset, O.] Univ Nantes, CNRS, UMR 6112, Lab Planetol & Geodynam, 2 Rue Houssiniere, F-44322 Nantes, France. [Sotin, C.; Kalousova, K.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Kalousova, K.] Charles Univ Prague, Fac Math & Phys, Dept Geophys, V Holesovickach 2, CR-18000 Prague 8, Czech Republic. RP Choblet, G (reprint author), Univ Nantes, CNRS, UMR 6112, Lab Planetol & Geodynam, 2 Rue Houssiniere, F-44322 Nantes, France. EM gael.choblet@univ-nantes.fr OI Kalousova, Klara/0000-0002-1602-8142 FU European Research Council under the European Community's Seventh Framework Programme FP7 [259285]; CNES FX We thank Hauke Hussmann and an anonymous reviewer for helpful reviews. The research leading to these results has received financial support from the European Research Council under the European Community's Seventh Framework Programme FP7/2007-2013, Grant Agreement no. 259285 (GC, GT,OG). GC, GT and OG also benefited from CNES funding to prepare the JUICE mission. This work was partly performed at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under contract to NASA. CS acknowledges support by the NAI Icy worlds. KK acknowledges support by the office of the JPL Chief Scientist. Numerical simulations were performed on CCIPL facilities in Nantes (France). NR 60 TC 0 Z9 0 U1 1 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR 15 PY 2017 VL 285 BP 252 EP 262 DI 10.1016/j.icarus.2016.12.002 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EJ5KP UT WOS:000393257200020 ER PT J AU Kraft-Bermuth, S Andrianov, V Bleile, A Echler, A Egelhof, P Grabitz, P Ilieva, S Kiselev, O Kilbourne, C McCammon, D Meier, JP Scholz, P AF Kraft-Bermuth, S. Andrianov, V. Bleile, A. Echler, A. Egelhof, P. Grabitz, P. Ilieva, S. Kiselev, O. Kilbourne, C. McCammon, D. Meier, J. P. Scholz, P. TI Precise determination of the 1s Lamb shift in hydrogen-like lead and gold using microcalorimeters SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article DE high-precision x-ray spectroscopy; precision test of QED; microcalorimeters for x-rays ID HIGHLY-CHARGED IONS; X-RAY SPECTROSCOPY; LOW-TEMPERATURE CALORIMETERS; NUCLEAR-DATA SHEETS; BARE URANIUM IONS; HEAVY-IONS; STORAGE-RING; DETECTORS; PHYSICS; ENERGY AB Quantum electrodynamics in very strong Coulomb fields is one scope which has not yet been tested experimentally with sufficient accuracy to really determine whether the perturbative approach is valid. One sensitive test is the determination of the 1s Lamb shift in highly-charged very heavy ions. The 1s Lamb shift of hydrogen-like lead (Pb81+) and gold (Au78+) has been determined using the novel detector concept of silicon microcalorimeters for the detection of hard x-rays. The results of (260 +/- 53) eV for lead and (211 +/- 42) eV for gold are within the error bars in good agreement with theoretical predictions. To our knowledge, for hydrogen-like lead, this represents the most accurate determination of the 1s Lamb shift. C1 [Kraft-Bermuth, S.; Echler, A.; Scholz, P.] Justus Liebig Univ, Inst Atom & Mol Phys, Giessen, Germany. [Andrianov, V.; Bleile, A.; Echler, A.; Egelhof, P.; Grabitz, P.; Ilieva, S.; Kiselev, O.; Meier, J. P.] GSI Helmholtz Ctr Heavy Ion Res, Darmstadt, Germany. [Echler, A.; Egelhof, P.; Grabitz, P.] Johannes Gutenberg Univ Mainz, Inst Phys, Mainz, Germany. [Kilbourne, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [McCammon, D.] Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA. [Andrianov, V.] Lomonosov Moscow State Univ, Inst Nucl Phys, Moscow, Russia. RP Kraft-Bermuth, S (reprint author), Justus Liebig Univ, Inst Atom & Mol Phys, Giessen, Germany. EM saskia.kraft-bermuth@iamp.physik.uni-giessen.de FU Emmy Noether Young Researchers Program of the Deutsche Forschungsgemeinschaft (DFG) [KR3721/1-1] FX We thank K Eberhard and J Runke from the Institute of Nuclear Chemistry of the Johannes Gutenberg Universitat Mainz for producing the Dy-159 source. We also thank our co-experimentators from the FOCAL collaboration for good cooperation during the measurements. The helpful discussions during data analysis with T Stohlker, H Beyer and T Gassner are gratefully acknowledged. The accelerator group of GSI, in particular the ESR operators, provided us with excellent, stable experimental conditions. This work was supported by the Emmy Noether Young Researchers Program of the Deutsche Forschungsgemeinschaft (DFG) under grant KR3721/1-1. NR 52 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD MAR 14 PY 2017 VL 50 IS 5 AR 055603 DI 10.1088/1361-6455/50/5/055603 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA EN2XV UT WOS:000395874500001 ER PT J AU Ruf, A Kanawati, B Hertkorn, N Yin, QZ Moritz, F Harir, M Lucio, M Michalke, B Wimpenny, J Shilobreeva, S Bronsky, B Saraykin, V Gabelica, Z Gougeon, RD Quirico, E Ralew, S Jakubowski, T Haack, H Gonsior, M Jenniskens, P Hinman, NW Schmitt-Kopplin, P AF Ruf, Alexander Kanawati, Basem Hertkorn, Norbert Yin, Qing-Zhu Moritz, Franco Harir, Mourad Lucio, Marianna Michalke, Bernhard Wimpenny, Joshua Shilobreeva, Svetlana Bronsky, Basil Saraykin, Vladimir Gabelica, Zelimir Gougeon, Regis D. Quirico, Eric Ralew, Stefan Jakubowski, Tomasz Haack, Henning Gonsior, Michael Jenniskens, Peter Hinman, Nancy W. Schmitt-Kopplin, Philippe TI Previously unknown class of metalorganic compounds revealed in meteorites SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE metalorganic chemistry; meteorites; astrochemistry; Fourier transform ion cyclotron resonance mass spectrometry; organic evolution ID EXTRATERRESTRIAL AMINO-ACIDS; ORGANIC-MATTER; MURCHISON METEORITE; CARBONACEOUS METEORITES; MASS-SPECTROMETRY; PARENT BODY; MAGNESIUM; CHEMISTRY; CHONDRITE; FALL AB The rich diversity and complexity of organic matter found in meteorites is rapidly expanding our knowledge and understanding of extreme environments from which the early solar system emerged and evolved. Here, we report the discovery of a hitherto unknown chemical class, dihydroxymagnesium carboxylates [(OH)(2)MgO2CR](-), in meteoritic soluble organic matter. High collision energies, which are required for fragmentation, suggest substantial thermal stability of these Mg-metalorganics (CHOMg compounds). This was corroborated by their higher abundance in thermally processed meteorites. CHOMg compounds were found to be present in a set of 61 meteorites of diverse petrological classes. The appearance of this CHOMg chemical class extends the previously investigated, diverse set of CHNOS molecules. A connection between the evolution of organic compounds and minerals is made, as Mg released from minerals gets trapped into organic compounds. These CHOMg metalorganic compounds and their relation to thermal processing in meteorites might shed new light on our understanding of carbon speciation at a molecular level in meteorite parent bodies. C1 [Ruf, Alexander; Kanawati, Basem; Hertkorn, Norbert; Moritz, Franco; Harir, Mourad; Lucio, Marianna; Michalke, Bernhard; Schmitt-Kopplin, Philippe] Helmholtz Zentrum Munchen, Res Unit Analyt BioGeoChem, D-85764 Neuherberg, Germany. [Ruf, Alexander; Harir, Mourad; Schmitt-Kopplin, Philippe] Tech Univ Munich, Analyt Food Chem, D-85354 Freising Weihenstephan, Germany. [Yin, Qing-Zhu; Wimpenny, Joshua] Univ Calif, Dept Earth & Planetary Sci, Davis, CA 95616 USA. [Shilobreeva, Svetlana; Bronsky, Basil; Saraykin, Vladimir] Russian Acad Sci, Vernadsky Inst Geochemistry & Analyt Chem, Moscow 119991, Russia. [Saraykin, Vladimir] Res Inst Phys, Moscow 124460, Russia. [Gabelica, Zelimir] Univ Haute Alsace, Ecole Natl Super Chim Mulhouse, F-68094 Mulhouse, France. [Gougeon, Regis D.] Univ Bourgogne AgroSupDijon, Inst Univ Vigne & Vin Jules Guyot, UMR Procedes Alimentaires & Microbiol, F-21000 Dijon, France. [Quirico, Eric] Univ Grenoble Alpes, CNRS Inst Natl Sci Univers, Inst Planetol Grenoble, UMR 5274, F-38041 Grenoble, France. [Ralew, Stefan] SR Meteorites, D-12681 Berlin, Germany. [Jakubowski, Tomasz] Drohobycka 32-6, PL-54620 Wroclaw, Poland. [Haack, Henning] Univ Copenhagen, Nat Hist Museum Denmark, Sect Geobiol & Minerals, DK-1350 Copenhagen, Denmark. [Haack, Henning] Maine Mineral & Gem Museum, Bethel, ME 04217 USA. [Gonsior, Michael] Univ Maryland, Ctr Environm Sci, Chesapeake Biol Lab, Solomons, MD 20688 USA. [Jenniskens, Peter] SETI Inst, Mountain View, CA 94043 USA. [Jenniskens, Peter] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hinman, Nancy W.] Univ Montana, Missoula, MT 59812 USA. RP Schmitt-Kopplin, P (reprint author), Helmholtz Zentrum Munchen, Res Unit Analyt BioGeoChem, D-85764 Neuherberg, Germany.; Schmitt-Kopplin, P (reprint author), Tech Univ Munich, Analyt Food Chem, D-85354 Freising Weihenstephan, Germany. EM schmitt-kopplin@helmholtz-muenchen.de RI quirico, eric/K-9650-2013; Gonsior, Michael/D-3964-2012 OI quirico, eric/0000-0003-2768-0694; Gonsior, Michael/0000-0003-0542-4614 FU NASA Cosmochemistry Grant [NNX14AM62G]; Emerging Worlds Grant [NNX16AD34D] FX We thank Rainer Bartoschewitz, Maria Elizabeth Zucolotto, Ansgar Greshake, Herbert Raab, Michael Farmer, Greg Hupe, Andre Moutinho, Sonny Clary, Fabien Kuntz, Valery Bogdanovsky, Aid Mohamed, Ismailly Sidi Mohamed, Abdel Fattah Gharrad, and the National Institute of Polar Research for providing meteorite samples. We also thank the reviewers for their open-mindedness regarding our concept and their constructive comments, which substantially improved the quality of the manuscript, and Matthew Sanborn for proofreading the manuscript. This work was supported by NASA Cosmochemistry Grant NNX14AM62G and Emerging Worlds Grant NNX16AD34D (to Q.-Z. Y.). NR 62 TC 0 Z9 0 U1 0 U2 0 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 14 PY 2017 VL 114 IS 11 BP 2819 EP 2824 DI 10.1073/pnas.1616019114 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EN6DH UT WOS:000396094200031 PM 28242686 ER PT J AU Hartmann, A Gleeson, T Wada, Y Wagener, T AF Hartmann, Andreas Gleeson, Tom Wada, Yoshihide Wagener, Thorsten TI Enhanced groundwater recharge rates and altered recharge sensitivity to climate variability through subsurface heterogeneity SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE groundwater recharge; subsurface heterogeneity; water resources; climate variability; climate change ID SOUTHERN SPAIN; KARST AQUIFERS; ISI-MIP; WATER; MODEL; RESOURCES; RUNOFF; EUROPE; PROJECTIONS; STRATEGIES AB Our environment is heterogeneous. In hydrological sciences, the heterogeneity of subsurface properties, such as hydraulic conductivities or porosities, exerts an important control on water balance. This notably includes groundwater recharge, which is an important variable for efficient and sustainable groundwater resources management. Current large-scale hydrological models do not adequately consider this subsurface heterogeneity. Here we show that regions with strong subsurface heterogeneity have enhanced present and future recharge rates due to a different sensitivity of recharge to climate variability compared with regions with homogeneous subsurface properties. Our study domain comprises the carbonate rock regions of Europe, Northern Africa, and the Middle East, which cover similar to 25% of the total land area. We compare the simulations of two large-scale hydrological models, one of them accounting for subsurface heterogeneity. Carbonate rock regions strongly exhibit "karstification," which is known to produce particularly strong subsurface heterogeneity. Aquifers from these regions contribute up to half of the drinking water supply for some European countries. Our results suggest that water management for these regions cannot rely on most of the presently available projections of groundwater recharge because spatially variable storages and spatial concentration of recharge result in actual recharge rates that are up to four times larger for present conditions and changes up to five times larger for potential future conditions than previously estimated. These differences in recharge rates for strongly heterogeneous regions suggest a need for groundwater management strategies that are adapted to the fast transit of water from the surface to the aquifers. C1 [Hartmann, Andreas] Univ Freiburg, Inst Earth & Environm Sci, D-79098 Freiburg, Germany. [Hartmann, Andreas; Wagener, Thorsten] Univ Bristol, Dept Civil Engn, Bristol BS8 1TR, Avon, England. [Gleeson, Tom] Univ Victoria, Dept Civil Engn, Victoria, BC V8W 2Y2, Canada. [Gleeson, Tom] Univ Victoria, Sch Earth & Ocean Sci, Victoria, BC V8W 2Y2, Canada. [Wada, Yoshihide] Int Inst Appl Syst Anal, A-2361 Laxenburg, Austria. [Wada, Yoshihide] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Wada, Yoshihide] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. [Wada, Yoshihide] Univ Utrecht, Dept Phys Geog, NL-3584 CS Utrecht, Netherlands. [Wagener, Thorsten] Univ Bristol, Cabot Inst, Bristol BS8 1TR, Avon, England. RP Hartmann, A (reprint author), Univ Freiburg, Inst Earth & Environm Sci, D-79098 Freiburg, Germany.; Hartmann, A (reprint author), Univ Bristol, Dept Civil Engn, Bristol BS8 1TR, Avon, England. EM andreas.hartmann@hydrology.uni-freiburg.de RI Wagener, Thorsten/C-2062-2008 OI Wagener, Thorsten/0000-0003-3881-5849 FU A.H. within the Postdoc Programme of the German Academic Exchange Service; Natural Environment Research Council [Consortium on Risk in the Environment: Diagnostics, Integration, Benchmarking, Learning, and Elicitation (CREDIBLE) Grant [NE/J017450/1] FX This work was supported by a fellowship to A.H. within the Postdoc Programme of the German Academic Exchange Service. This work was partially supported by the Natural Environment Research Council [Consortium on Risk in the Environment: Diagnostics, Integration, Benchmarking, Learning, and Elicitation (CREDIBLE) Grant NE/J017450/1]. NR 50 TC 0 Z9 0 U1 4 U2 4 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 14 PY 2017 VL 114 IS 11 BP 2842 EP 2847 DI 10.1073/pnas.1614941114 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EN6DH UT WOS:000396094200035 PM 28242703 ER PT J AU Berger, T Burmeister, S Matthiae, D Przybyla, B Reitz, G Bilski, P Hajek, M Sihver, L Szabo, J Ambrozova, I Vanhavere, F Gaza, R Semones, E Yukihara, EG Benton, ER Uchihori, Y Kodaira, S Kitamura, H Boehme, M AF Berger, Thomas Burmeister, Soenke Matthiae, Daniel Przybyla, Bartos Reitz, Guenther Bilski, Pawel Hajek, Michael Sihver, Lembit Szabo, Julianna Ambrozova, Iva Vanhavere, Filip Gaza, Ramona Semones, Edward Yukihara, Eduardo G. Benton, Eric R. Uchihori, Yukio Kodaira, Satoshi Kitamura, Hisashi Boehme, Matthias TI DOSIS & DOSIS 3D: radiation measurements with the DOSTEL instruments onboard the Columbus Laboratory of the ISS in the years 2009-2016 SO JOURNAL OF SPACE WEATHER AND SPACE CLIMATE LA English DT Article DE International Space Station; Columbus; Space radiation; DOSTEL; DOSIS 3D ID INTERNATIONAL-SPACE-STATION; CIVIL AIRCRAFT; DOSIMETRY; EXPOSURE; ENVIRONMENT AB The natural radiation environment in Low Earth Orbit (LEO) differs significantly in composition and energy from that found on Earth. The space radiation field consists of high energetic protons and heavier ions from Galactic Cosmic Radiation (GCR), as well as of protons and electrons trapped in the Earth's radiation belts (Van Allen belts). Protons and some heavier particles ejected in occasional Solar Particle Events (SPEs) might in addition contribute to the radiation exposure in LEO. All sources of radiation are modulated by the solar cycle. During solar maximum conditions SPEs occur more frequently with higher particle intensities. Since the radiation exposure in LEO exceeds exposure limits for radiation workers on Earth, the radiation exposure in space has been recognized as a main health concern for humans in space missions from the beginning of the space age on. Monitoring of the radiation environment is therefore an inevitable task in human spaceflight. Since mission profiles are always different and each spacecraft provides different shielding distributions, modifying the radiation environment measurements needs to be done for each mission. The experiments "Dose Distribution within the ISS (DOSIS)'' (2009-2011) and "Dose Distribution within the ISS 3D (DOSIS 3D)'' (2012-onwards) onboard the Columbus Laboratory of the International Space Station (ISS) use a detector suite consisting of two silicon detector telescopes (DOSimetry TELescope = DOSTEL) and passive radiation detector packages (PDP) and are designed for the determination of the temporal and spatial variation of the radiation environment. With the DOSTEL instruments' changes of the radiation composition and the related exposure levels in dependence of the solar cycle, the altitude of the ISS and the influence of attitude changes of the ISS during Space Shuttle dockings inside the Columbus Laboratory have been monitored. The absorbed doses measured at the end of May 2016 reached up to 286 mu Gy/day with dose equivalent values of 647 mu Sv/day. C1 [Berger, Thomas; Matthiae, Daniel; Przybyla, Bartos; Reitz, Guenther] German Aerosp Ctr DLR, Inst Aerosp Med, D-51147 Cologne, Germany. [Burmeister, Soenke] Christian Albrechts Univ Kiel CAU, Christian Albrechts Pl, D-24118 Kiel, Germany. [Bilski, Pawel] Polish Acad Sci IFJ, Inst Nucl Phys, PL-31342 Krakow, Poland. [Hajek, Michael] IAEA, Div Radiat, Transport & Waste Safety, A-1400 Vienna, Austria. [Hajek, Michael; Sihver, Lembit] Tech Univ Wien, Atominst ATI, Stadionallee 2, A-1020 Vienna, Austria. [Sihver, Lembit] EGB MedAustron, Marie Curie Strasse 5, A-2700 Wiener, Austria. [Szabo, Julianna] MTA EK, Energy Res Ctr, Konkoly Thege Ut 29-33, H-1121 Budapest, Hungary. [Ambrozova, Iva] Nucl Phys Inst CAS NPI, Dept Radiat Dosimetry, Truhlarce 39-64, Prague 18000, Czech Republic. [Vanhavere, Filip] Belgian Nucl Res Ctr SCK CEN, Boeretang 200, B-2400 Mol, Belgium. [Gaza, Ramona; Semones, Edward] NASA, SRAG, Houston, TX 77058 USA. [Gaza, Ramona] Leidos, Explorat Miss Support, 2400 NASA Pkwy, Houston, TX 77058 USA. [Yukihara, Eduardo G.; Benton, Eric R.] Oklahoma State Univ, Dept Phys, Stillwater, OK 74078 USA. [Uchihori, Yukio; Kodaira, Satoshi; Kitamura, Hisashi] Natl Inst Quantum & Radiol Sci & Technol QST, NIRS, 4-9-1 Anagawa, Inage, Chiba 2638555, Japan. [Boehme, Matthias] OHB Syst AG, Univ St-29, D-28359 Bremen, Germany. RP Berger, T (reprint author), German Aerosp Ctr DLR, Inst Aerosp Med, D-51147 Cologne, Germany. EM thomas.berger@dlr.de FU DLR [50WB0826, 50WB1026, 50WB1232, 50WB1533]; Austrian Space Applications Programme (ASAP) [819643]; National Science Center [DEC-2012/06/M/ST9/00423]; ESA PECS [PECS4000108464]; grant of Czech Science Foundation (GACR) [15-16622Y]; European Space Agency (ESA) FX The CAU, University of Kiel was supported by DLR under Grants 50WB0826, 50WB1026, 50WB1232 and 50WB1533. The participation of the Technische Universitat Wien, Atominstitut (ATI), Vienna, Austria in the DOSIS experiments was supported by the Austrian Space Applications Programme (ASAP) under Contract No. 819643. The Polish contribution for the Institute of Nuclear Physics (IFJ), Krakow, Poland was supported by the National Science Center (Project No. DEC-2012/06/M/ST9/00423). MTA EK greatly acknowledges ESA PECS for the Financial Grant No. PECS4000108464. The participation of the Nuclear Physics Institute of the Czech Academy of Sciences has been supported by the grant of Czech Science Foundation (GACR) No. 15-16622Y.; The authors gratefully acknowledge the support of the European Space Agency (ESA) especially Jason Hatton, Rene Demets, Chiara Lombardi and Liesbeth De Smet as well as colleagues from CADMOS (Lourdes Oro Marot, Cecile Thevenot) Toulouse, France, DLR-MUSC (Pascaline Kerbeci), Cologne, Germany and ESA-EAC, Cologne, Germany. NR 36 TC 0 Z9 0 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 2115-7251 J9 J SPACE WEATHER SPAC JI J. Space Weather Space Clim. PD MAR 13 PY 2017 VL 7 AR A8 DI 10.1051/swsc/2017005 PG 19 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA EN3FG UT WOS:000395893800001 ER PT J AU Litvak, ML Sanin, AB Golovin, DV Jun, I Mitrofanov, IG Shvetsov, VN Timoshenko, GN Vostrukhin, AA AF Litvak, M. L. Sanin, A. B. Golovin, D. V. Jun, I. Mitrofanov, I. G. Shvetsov, V. N. Timoshenko, G. N. Vostrukhin, A. A. TI Ground tests with prototype of CeBr3 active gamma ray spectrometer proposed for future venus surface missions SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article DE Active gamma spectrometer; Pulsed neutron generator; Elemental abundances; Surface measurements ID NEUTRONS DAN EXPERIMENT; DYNAMIC ALBEDO; MARS; INSTRUMENTATION; SPECTROSCOPY AB The results of a series of ground tests with a prototype of an active gamma-ray spectrometer based on a new generation of scintillation crystal (CeBr3) are presented together with a consideration to its applicability to future Venus landing missions. We evaluated the instrument's capability to distinguish the subsurface elemental composition of primary rock forming elements such as 0, Na, Mg, Al, Si, K and Fe. Our study uses heritage from previous ground and field tests and applies to the analysis of gamma lines from activation reaction products generated by a pulsed neutron generator. We have estimated that the expected accuracies achieved in this approach could be as high as 1-10% for the particular chemical element being studied. C1 [Litvak, M. L.; Sanin, A. B.; Golovin, D. V.; Mitrofanov, I. G.; Vostrukhin, A. A.] RAS, Space Res Inst, Moscow 117997, Russia. [Jun, I.] Jet Prop Lab, Pasadena, CA USA. [Shvetsov, V. N.; Timoshenko, G. N.] Joint Inst Nucl Res, Dubna, Russia. RP Litvak, ML (reprint author), RAS, Space Res Inst, Moscow 117997, Russia. EM litvak@mx.iki.rssi.ru FU Russian Science Foundation [14-22-00249] FX This work is supported by the Grant # 14-22-00249 from Russian Science Foundation NR 28 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 EI 1872-9576 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD MAR 11 PY 2017 VL 848 BP 9 EP 18 DI 10.1016/j.nima.2016.12.047 PG 10 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA EL4YJ UT WOS:000394627600002 ER PT J AU Sudek, LA Wanger, G Templeton, AS Staudigel, H Tebo, BM AF Sudek, Lisa A. Wanger, Greg Templeton, Alexis S. Staudigel, Hubert Tebo, Bradley M. TI Submarine Basaltic Glass Colonization by the Heterotrophic Fe(II)-Oxidizing and Siderophore-Producing Deep-Sea Bacterium Pseudomonas stutzeri VS-10: The Potential Role of Basalt in Enhancing Growth SO FRONTIERS IN MICROBIOLOGY LA English DT Article DE biofilm; basalt; Fe(II) oxidation; microbial fuel cell; siderophores; diffusion chamber ID SHEWANELLA-ONEIDENSIS MR-1; MICROBIAL FUEL-CELLS; EXTRACELLULAR ELECTRON-TRANSFER; IRON-OXIDIZING BACTERIA; HYDROTHERMAL PLUMES; BIOMASS PRODUCTION; MARINE BASALTS; LOIHI SEAMOUNT; FLOOR BASALT; OCEAN AB Phylogenetically and metabolically diverse bacterial communities have been found in association with submarine basaltic glass surfaces. The driving forces behind basalt colonization are for the most part unknown. It remains ambiguous if basalt provides ecological advantages beyond representing a substrate for surface colonization, such as supplying nutrients and/or energy. Pseudomonas stutzeri VS-10, a metabolically versatile bacterium isolated from Vailulu'u Seamount, was used as a model organism to investigate the physiological responses observed when biofilms are established on basaltic glasses. In Fe-limited heterotrophic media, P. stutzeri VS-10 exhibited elevated growth in the presence of basaltic glass. Diffusion chamber experiments demonstrated that physical attachment or contact of soluble metabolites such as siderophores with the basaltic glass plays a pivotal role in this process. Electrochemical data indicated that P. stutzeri VS-10 is able to use solid substrates (electrodes) as terminal electron donors and acceptors. Siderophore production and heterotrophic Fe(II) oxidation are discussed as potential mechanisms enhancing growth of P. stutzeri VS-10 on glass surfaces. In correlation with that we discuss the possibility that metabolic versatility could represent a common and beneficial physiological trait in marine microbial communities being subject to oligotrophic and rapidly changing deep-sea conditions. C1 [Sudek, Lisa A.; Tebo, Bradley M.] Univ Calif San Diego, Scripps Inst Oceanog, Div Marine Biol Res, La Jolla, CA 92103 USA. [Wanger, Greg] Univ Southern Calif, Calif Inst Technol, Jet Prop Lab, Pasadena, CA USA. [Templeton, Alexis S.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. [Staudigel, Hubert] Univ Calif San Diego, Scripps Inst Oceanog, Inst Geophys & Planetary Phys, La Jolla, CA 92093 USA. [Tebo, Bradley M.] Oregon Hlth & Sci Univ, Inst Environm Hlth, Portland, OR 97201 USA. RP Sudek, LA (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Div Marine Biol Res, La Jolla, CA 92103 USA. EM lisasudek@gmail.com FU National Science Foundation Microbial Observatories [MCB-0348668/0742010]; Biogeosciences [OCE-0433692]; Ocean Sciences [OCE-0526285]; Agouron Institute FX Funding sources include the National Science Foundation Microbial Observatories (MCB-0348668/0742010), Biogeosciences (OCE-0433692), and the Ocean Sciences (OCE-0526285) programs and the Agouron Institute. NR 67 TC 0 Z9 0 U1 0 U2 0 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 MAR 10 PY 2017 VL 8 AR 363 DI 10.3389/fmicb.2017.00363 PG 12 WC Microbiology SC Microbiology GA EN2WD UT WOS:000395870100001 PM 28344573 ER PT J AU Noohi, F Kinnaird, C DeDios, Y Kofman, IS Wood, S Bloomberg, J Mulavara, A Seidler, R AF Noohi, Fatemeh Kinnaird, Catherine DeDios, Yin Kofman, Igor S. Wood, Scott Bloomberg, Jacob Mulavara, Ajitkumar Seidler, Rachael TI Functional Brain Activation in Response to a Clinical Vestibular Test Correlates with Balance SO FRONTIERS IN SYSTEMS NEUROSCIENCE LA English DT Article DE VEMP; fMRI; skull tap; auditory tone burst; balance ID EVOKED MYOGENIC POTENTIALS; NEAR-INFRARED SPECTROSCOPY; BONE-CONDUCTED VIBRATION; CALORIC STIMULATION; SKULL TAPS; CORTICAL PROJECTION; UTRICULAR FUNCTION; MIDLINE FOREHEAD; HEALTHY-SUBJECTS; SPATIAL MEMORY AB The current study characterizes brain fMRI activation in response to two modes of vestibular stimulation: Skull tap and auditory tone burst. The auditory tone burst has been used in previous studies to elicit either a vestibulo-spinal reflex [saccular-mediated colic Vestibular Evoked Myogenic Potentials (cVEMP)], or an ocular muscle response [utricle-mediated ocular VEMP (oVEMP)]. Research suggests that the skull tap elicits both saccular and utricle-mediated VEMPs, while being faster and less irritating for subjects than the high decibel tones required to elicit VEMPs. However, it is not clear whether the skull tap and auditory tone burst elicit the same pattern of brain activity. Previous imaging studies have documented activity in the anterior and posterior insula, superior temporal gyrus, inferior parietal lobule, inferior frontal gyrus, and the anterior cingulate cortex in response to different modes of vestibular stimulation. Here we hypothesized that pneumatically powered skull taps would elicit a similar pattern of brain activity as shown in previous studies. Our results provide the first evidence of using pneumatically powered skull taps to elicit vestibular activity inside the MRI scanner. A conjunction analysis revealed that skull taps elicit overlapping activation with auditory tone bursts in the canonical vestibular cortical regions. Further, our postural control assessments revealed that greater amplitude of brain activation in response to vestibular stimulation was associated with better balance control for both techniques. Additionally, we found that skull taps elicit more robust vestibular activity compared to auditory tone bursts, with less reported aversive effects, highlighting the utility of this approach for future clinical and basic science research. C1 [Noohi, Fatemeh; Seidler, Rachael] Univ Michigan, Sch Kinesiol, Ann Arbor, MI 48109 USA. [Noohi, Fatemeh; Seidler, Rachael] Univ Michigan, Dept Psychol, Ann Arbor, MI 48109 USA. [Kinnaird, Catherine] Univ Michigan, Dept Mech Engn, Ann Arbor, MI 48109 USA. [DeDios, Yin; Kofman, Igor S.; Mulavara, Ajitkumar] KBRwyle, Houston, TX USA. [Wood, Scott; Bloomberg, Jacob] NASA Johnson Space Ctr, Houston, TX USA. RP Noohi, F (reprint author), Univ Michigan, Sch Kinesiol, Ann Arbor, MI 48109 USA.; Noohi, F (reprint author), Univ Michigan, Dept Psychol, Ann Arbor, MI 48109 USA. EM fnoohi@umich.edu FU National Space Biomedical Research Institute [NASA NCC 9-58]; NASA [NNX11AR02G] FX We thank Tina Wu for her assistance with data collection. This work was supported by grants from the National Space Biomedical Research Institute (NASA NCC 9-58) and NASA (NNX11AR02G). NR 75 TC 0 Z9 0 U1 0 U2 0 PU FRONTIERS MEDIA SA PI LAUSANNE PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015, SWITZERLAND SN 1662-5137 J9 FRONT SYST NEUROSCI JI Front. Syst. Neurosci. PD MAR 10 PY 2017 VL 11 AR 11 DI 10.3389/fnsys.2017.00011 PG 18 WC Neurosciences SC Neurosciences & Neurology GA EN2WP UT WOS:000395871300001 PM 28344549 ER PT J AU Carn, SA Fioletov, VE McLinden, CA Li, C Krotkov, NA AF Carn, S. A. Fioletov, V. E. McLinden, C. A. Li, C. Krotkov, N. A. TI A decade of global volcanic SO2 emissions measured from space SO SCIENTIFIC REPORTS LA English DT Article ID OZONE MONITORING INSTRUMENT; SULFUR-DIOXIDE EMISSIONS; GAS EMISSIONS; ERUPTION; INDONESIA; FLUXES; PLUME; PETROLOGY; IMPACTS; HAWAII AB The global flux of sulfur dioxide (SO2) emitted by passive volcanic degassing is a key parameter that constrains the fluxes of other volcanic gases (including carbon dioxide, CO2) and toxic trace metals (e.g., mercury). It is also a required input for atmospheric chemistry and climate models, since it impacts the tropospheric burden of sulfate aerosol, a major climate-forcing species. Despite its significance, an inventory of passive volcanic degassing is very difficult to produce, due largely to the patchy spatial and temporal coverage of ground-based SO2 measurements. We report here the first volcanic SO2 emissions inventory derived from global, coincident satellite measurements, made by the Ozone Monitoring Instrument (OMI) on NASA's Aura satellite in 2005-2015. The OMI measurements permit estimation of SO2 emissions from over 90 volcanoes, including new constraints on fluxes from Indonesia, Papua New Guinea, the Aleutian Islands, the Kuril Islands and Kamchatka. On average over the past decade, the volcanic SO2 sources consistently detected from space have discharged a total of similar to 63 kt/day SO2 during passive degassing, or -23 +/- 2 Tg/yr. We find that -30% of the sources show significant decadal trends in SO2 emissions, with positive trends observed at multiple volcanoes in some regions including Vanuatu, southern Japan, Peru and Chile. C1 [Carn, S. A.] Michigan Technol Univ, Dept Geol & Min Engn & Sci, Houghton, MI 49931 USA. [Fioletov, V. E.; McLinden, C. A.] Environm & Climate Change Canada, Air Qual Res Div, Toronto, ON, Canada. [Li, C.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD USA. [Li, C.; Krotkov, N. A.] NASA Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA. RP Carn, SA (reprint author), Michigan Technol Univ, Dept Geol & Min Engn & Sci, Houghton, MI 49931 USA. EM scarn@mtu.edu FU NASA [NNX13AF50G] FX We acknowledge NASA support for development of the OMI SO2 products and volcanic SO2 emissions inventories through grant NNX13AF50G (Multi-Decadal Sulfur Dioxide Climatology from Satellite Instruments; PI: N.A. Krotkov). The volcanic SO2 emissions database described in this paper will be made publicly available from the NASA Goddard Earth Sciences (GES) Data and Information Services Center ( DISC) as a level 4 MEaSUREs ( Making Earth System Data Records for Use in Research Environments) data product (MSDEGSO2L4). NR 61 TC 0 Z9 0 U1 1 U2 1 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2045-2322 J9 SCI REP-UK JI Sci Rep PD MAR 9 PY 2017 VL 7 AR 44095 DI 10.1038/srep44095 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EN6UE UT WOS:000396138100001 PM 28275238 ER PT J AU Espinosa, WR Remer, LA Dubovik, O Ziemba, L Beyersdorf, A Orozco, D Schuster, G Lapyonok, T Fuertes, D Martins, JV AF Espinosa, W. Reed Remer, Lorraine A. Dubovik, Oleg Ziemba, Luke Beyersdorf, Andreas Orozco, Daniel Schuster, Gregory Lapyonok, Tatyana Fuertes, David Martins, J. Vanderlei TI Retrievals of aerosol optical and microphysical properties from Imaging Polar Nephelometer scattering measurements SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID SKY RADIANCE MEASUREMENTS; REFRACTIVE-INDEX; LIGHT-SCATTERING; PERFORMANCE-CHARACTERISTICS; INVERSION ALGORITHM; HYGROSCOPIC GROWTH; SIZE DISTRIBUTION; AMMONIUM-SULFATE; HIGH-SENSITIVITY; PARTICLES AB A method for the retrieval of aerosol optical and microphysical properties from in situ light-scattering measurements is presented and the results are compared with existing measurement techniques. The Generalized Retrieval of Aerosol and Surface Properties (GRASP) is applied to airborne and laboratory measurements made by a novel polar nephelometer. This instrument, the Polarized Imaging Nephelometer (PI-Neph), is capable of making high-accuracy field measurements of phase function and degree of linear polarization, at three visible wavelengths, over a wide angular range of 3 to 177 degrees. The resulting retrieval produces particle size distributions (PSDs) that agree, within experimental error, with measurements made by commercial optical particle counters (OPCs). Additionally, the retrieved real part of the refractive index is generally found to be within the predicted error of 0.02 from the expected values for three species of humidified salt particles, with a refractive index that is well established. The airborne measurements used in this work were made aboard the NASA DC-8 aircraft during the Studies of Emissions and Atmospheric Composition, Clouds and Climate Coupling by Regional Surveys (SEAC(4)RS) field campaign, and the inversion of this data represents the first aerosol retrievals of airborne polar nephelometer data. The results provide confidence in the real refractive index product, as well as in the retrieval's ability to accurately deter-mine PSD, without assumptions about refractive index that are required by the majority of OPCs. C1 [Espinosa, W. Reed; Remer, Lorraine A.; Orozco, Daniel; Martins, J. Vanderlei] Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA. [Espinosa, W. Reed; Remer, Lorraine A.; Orozco, Daniel; Martins, J. Vanderlei] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, 5523 Res Pk DR, Baltimore, MD 21228 USA. [Dubovik, Oleg; Lapyonok, Tatyana] Univ Lille, CNRS, Lab Opt Atmospher, F-59655 Villeneuve Dascq, France. [Ziemba, Luke; Beyersdorf, Andreas; Schuster, Gregory] Natl Aeronaut & Space Adm, Langley Res Ctr Sci Directorate, Hampton, VA USA. [Beyersdorf, Andreas] Calif State Univ San Bernardino, Dept Chem & Biochem, 5500 Univ Pkwy, San Bernardino, CA 92407 USA. [Fuertes, David] Univ Lille 1, GRASP SAS, Bat P5, F-59655 Villeneuve Dascq, France. RP Espinosa, WR (reprint author), Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA.; Espinosa, WR (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, 5523 Res Pk DR, Baltimore, MD 21228 USA. EM reedespinosa@umbc.edu FU NASA Earth Science Enterprise for the SEAC4RS campaign [NNX12AC37G]; Atmospheric Composition Campaign Data Analysis and Modeling Program (ACCDAM) [NNX14AP73G] FX We acknowledge funding support from the NASA Earth Science Enterprise for the SEAC4RS campaign under Grant NNX12AC37G, and under the Atmospheric Composition Campaign Data Analysis and Modeling Program (ACCDAM) grant NNX14AP73G, both managed by Hal Maring. The authors would also like to thank the members of the LARGE group, particularly Bruce Anderson, Edward Winstead and Lee Thornhill for their support incorporating the PI-Neph into the LARGE instrument package. We are also grateful for the scientific and technical support of the LACO team at UMBC, especially Dominik Cieslak and Frank Harris. Additionally, we would like to thank the entire SEAC4RS science team for providing supporting data and relevant discussion. NR 48 TC 0 Z9 0 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 MAR 8 PY 2017 VL 10 IS 3 BP 811 EP 824 DI 10.5194/amt-10-811-2017 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EN7SX UT WOS:000396203600002 ER PT J AU Brunt, KM Hawley, RL Lutz, ER Studinger, M Sonntag, JG Hofton, MA Andrews, LC Neumann, TA AF Brunt, Kelly M. Hawley, Robert L. Lutz, Eric R. Studinger, Michael Sonntag, John G. Hofton, Michelle A. Andrews, Lauren C. Neumann, Thomas A. TI Assessment of NASA airborne laser altimetry data using ground-based GPS data near Summit Station, Greenland SO CRYOSPHERE LA English DT Article ID SHEET MASS-BALANCE; ICE-SHEET; ICESAT-2 MISSION; ANTARCTICA; LIDAR; MABEL AB A series of NASA airborne lidars have been used in support of satellite laser altimetry missions. These airborne laser altimeters have been deployed for satellite instrument development, for spaceborne data validation, and to bridge the data gap between satellite missions. We used data from ground-based Global Positioning System (GPS) surveys of an 11 km long track near Summit Station, Greenland, to assess the surface-elevation bias and measurement precision of three airborne laser altimeters including the Airborne Topographic Mapper (ATM), the Land, Vegetation, and Ice Sensor (LVIS), and the Multiple Altimeter Beam Experimental Lidar (MABEL). Ground-based GPS data from the monthly ground-based traverses, which commenced in 2006, allowed for the assessment of nine airborne lidar surveys associated with ATM and LVIS between 2007 and 2016. Surface-elevation biases for these altimeters - over the flat, ice-sheet interior - are less than 0.12 m, while assessments of measurement precision are 0.09m or better. Ground-based GPS positions determined both with and without differential post-processing techniques provided internally consistent solutions. Results from the analyses of ground-based and airborne data provide validation strategy guidance for the Ice, Cloud, and land Elevation Satellite 2 (ICESat-2) elevation and elevation-change data products. C1 [Brunt, Kelly M.] Univ Maryland, ESSIC, College Pk, MD 20742 USA. [Brunt, Kelly M.; Studinger, Michael; Andrews, Lauren C.; Neumann, Thomas A.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Hawley, Robert L.; Lutz, Eric R.] Dartmouth Coll, Dept Earth Sci, Hanover, NH USA. [Sonntag, John G.] AECOM Corp, Wallops Isl, VA USA. [Sonntag, John G.] NASA Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA USA. [Hofton, Michelle A.] Univ Maryland, Dept Geog Sci, College Pk, MD USA. [Andrews, Lauren C.] USRA, Columbia, MD USA. RP Brunt, KM (reprint author), Univ Maryland, ESSIC, College Pk, MD 20742 USA. EM kelly.m.brunt@nasa.gov FU NASA; National Science Foundation [PLR 1042358]; Summit Station Science Coordination Office (SCO) FX We thank the NASA ICESat-2 Project Science Office for funding this data analysis and for MABEL data collection, processing, and distribution. Further, we thank the NASA Armstrong Air Operations Facility for MABEL data collection (specifically pilots T. Williams and D. S. Broce). We thank Operation IceBridge for the data collection and processing associated with the ATM and LVIS airborne components of this project. We thank the National Science Foundation and the Summit Station Science Coordination Office (SCO) (NSF PLR 1042358) for support for the ground-based field component of this project. Further, this project would not have been possible without the work of many Summit Station Science Technicians who collected the in-situ GPS data. We thank K. Krabill (NASA GSFC WFF), C. Brooks, and D. Rabine (NASA GSFC) for GPS support. We thank the National Snow and Ice Data Center (NSIDC) for IceBridge data distribution. Finally, we thank our editor (Etienne Berthier) and two anonymous reviewers for insightful and constructive comments to earlier drafts of this manuscript. NR 34 TC 0 Z9 0 U1 0 U2 0 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1994-0416 EI 1994-0424 J9 CRYOSPHERE JI Cryosphere PD MAR 8 PY 2017 VL 11 IS 2 BP 681 EP 692 DI 10.5194/tc-11-681-2017 PG 12 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA EN7VF UT WOS:000396209600001 ER PT J AU Viggiano, RP Williams, JC Schiraldi, DA Meador, MAB AF Viggiano, Rocco P. Williams, Jarrod C. Schiraldi, David A. Meador, Mary Ann B. TI Effect of Bulky Substituents in the Polymer Backbone on the Properties of Polyimide Aerogels SO ACS APPLIED MATERIALS & INTERFACES LA English DT Article DE aerogels; polyimides; porous polymers; thermal shrinkage; mesoporous ID AROMATIC TETRACARBOXYLIC DIANHYDRIDES; SYNDIOTACTIC POLYSTYRENE AEROGELS; MODIFIED SILICA AEROGELS; MECHANICALLY STRONG; TEMPERATURE POLYMERS; SOLUBLE POLYIMIDES; ORGANIC AEROGELS; CARBON AEROGELS; FORMALDEHYDE; PERFORMANCE AB With unique advantages over inorganic aerogels including higher strengths and compressive moduli, greater toughness, and the ability to be fabricated as a flexible thin film, polymer aerogels have the potential to supplant inorganic aerogels in numerous applications. Among polymer aerogels, polyimide aerogels possess a high degree of high thermal stability as well as outstanding mechanical properties. However, while the onset of thermal decomposition for these materials is typically very high (greater than 500 degrees C), the polyimide aerogels undergo dramatic thermally induced shrinkage at temperatures well below their glass transition (T-g) or decomposition temperature, which limits their use. In this study, we show that shrinkage is reduced when a bulky moiety is incorporated in the polymer backbone. Twenty different formulations of polyimide aerogels were synthesized from 3,3,'4,4'-biphenyltetracarboxylic dianhydride (BPDA) and 4,4'-oxidianiline (ODA) or a combination of ODA and 9,9'-bis(4-aminophenyl)fluorene (BAPF) and cross-linked with 1,3,5-benzenetricarbonyl trichloride (BTC) in a statistically designed study. The polymer concentration, n-value, and molar concentration of ODA and BAPF were varied to demonstrate the effect of these variables on certain properties. Samples containing BAPF showed a reduction in shrinkage by as much as 50% after aging at elevated temperatures for 500 h compared to those made with ODA alone. C1 [Viggiano, Rocco P.; Williams, Jarrod C.; Meador, Mary Ann B.] NASA Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. [Schiraldi, David A.] Case Western Reserve Univ, 2100 Adelbert Rd, Cleveland, OH 44106 USA. RP Viggiano, RP; Meador, MAB (reprint author), NASA Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM rocco.p.viggiano@nasa.gov; maryann.meador@nasa.gov FU National Aeronautics and Space Administration's Space Technology Mission Directorate Game Changing Development Program FX We gratefully acknowledge support from the National Aeronautics and Space Administration's Space Technology Mission Directorate Game Changing Development Program. We would also like to thank Daniel Scheiman (Ohio Aerospace Institute) for carrying out porosimetry measurements, FT-IR, and thermal analysis; Linda McCorkle (Ohio Aerospace Institute) for SEM imaging; Baochau Nguyen (Ohio Aerospace Institute) for NMR spectra; and Haiquan Guo (Ohio Aerospace Institute) for nitrogen sorption experiments. NR 54 TC 0 Z9 0 U1 4 U2 4 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 MAR 8 PY 2017 VL 9 IS 9 BP 8287 EP 8296 DI 10.1021/acsami.6b15440 PG 10 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Science & Technology - Other Topics; Materials Science GA EN7MD UT WOS:000396186000048 PM 28186399 ER PT J AU Lorente, A Boersma, KF Yu, H Dorner, S Hilboll, A Richter, A Liu, MY Lamsal, LN Barkley, M De Smedt, I Van Roozendael, M Wang, Y Wagner, T Beirle, S Lin, JT Krotkov, N Stammes, P Wang, P Eskes, HJ Krol, M AF Lorente, Alba Boersma, K. Folkert Yu, Huan Doerner, Steffen Hilboll, Andreas Richter, Andreas Liu, Mengyao Lamsal, Lok N. Barkley, Michael De Smedt, Isabelle Van Roozendael, Michel Wang, Yang Wagner, Thomas Beirle, Steffen Lin, Jin-Tai Krotkov, Nickolay Stammes, Piet Wang, Ping Eskes, Henk J. Krol, Maarten TI Structural uncertainty in air mass factor calculation for NO2 and HCHO satellite retrievals SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID TROPOSPHERIC NITROGEN-DIOXIDE; CHEMISTRY TRANSPORT; MULTIMODEL ENSEMBLE; COLUMN RETRIEVALS; OMI; ALGORITHM; EMISSIONS; AEROSOLS; SPACE; MODEL AB Air mass factor (AMF) calculation is the largest source of uncertainty in NO2 and HCHO satellite retrievals in situations with enhanced trace gas concentrations in the lower troposphere. Structural uncertainty arises when different retrieval methodologies are applied within the scientific community to the same satellite observations. Here, we address the issue of AMF structural uncertainty via a detailed comparison of AMF calculation methods that are structurally different between seven retrieval groups for measurements from the Ozone Monitoring Instrument (OMI). We estimate the escalation of structural uncertainty in every sub-step of the AMF calculation process. This goes beyond the algorithm uncertainty estimates provided in state-of-the-art retrievals, which address the theoretical propagation of uncertainties for one particular retrieval algorithm only. We find that top-of-atmosphere reflectances simulated by four radiative transfer models (RTMs) (DAK, McArtim, SCIATRAN and VLIDORT) agree within 1.5 %. We find that different retrieval groups agree well in the calculations of altitude re-solved AMFs from different RTMs (to within 3%), and in the tropospheric AMFs (to within 6%) as long as identical ancillary data (surface albedo, terrain height, cloud parameters and trace gas profile) and cloud and aerosol correction procedures are being used. Structural uncertainty increases sharply when retrieval groups use their preference for ancillary data, cloud and aerosol correction. On average, we estimate the AMF structural uncertainty to be 42% over polluted regions and 31% over unpolluted regions, mostly driven by substantial differences in the a priori trace gas profiles, surface albedo and cloud parameters. Sensitivity studies for one particular algorithm indicate that different cloud correction approaches result in substantial AMF differences in polluted conditions (5 to 40% depending on cloud fraction and cloud pressure, and 11% on average) even for low cloud fractions (< 0.2) and the choice of aerosol correction introduces an average uncertainty of 50% for situations with high pollution and high aerosol loading. Our work shows that structural uncertainty in AMF calculations is significant and that it is mainly caused by the assumptions and choices made to represent the state of the atmosphere. In order to decide which approach and which ancillary data are best for AMF calculations, we call for well-designed validation exercises focusing on polluted conditions in which AMF structural uncertainty has the highest impact on NO2 and HCHO retrievals. C1 [Lorente, Alba; Boersma, K. Folkert; Krol, Maarten] Wageningen Univ, Meteorol & Air Qual Grp, Wageningen, Netherlands. [Boersma, K. Folkert; Stammes, Piet; Wang, Ping; Eskes, Henk J.] Royal Netherlands Meteorol Inst, De Bilt, Netherlands. [Yu, Huan; De Smedt, Isabelle; Van Roozendael, Michel] Belgian Inst Space Aeron BIRA IASB, Brussels, Belgium. [Doerner, Steffen; Wang, Yang; Wagner, Thomas; Beirle, Steffen] MPI C, Mainz, Germany. [Hilboll, Andreas; Richter, Andreas] Univ Bremen, Inst Environm Phys IUP UB, Bremen, Germany. [Hilboll, Andreas] Univ Bremen, MARUM Ctr Marine Environm Sci, Bremen, Germany. [Liu, Mengyao; Lin, Jin-Tai] Peking Univ, Sch Phys, Dept Atmospher & Ocean Sci, Lab Climate & Ocean Atmosphere Studies, Beijing 100871, Peoples R China. [Lamsal, Lok N.; Krotkov, Nickolay] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD USA. [Barkley, Michael] Univ Leicester, Dept Phys & Astron, EOS Grp, Leicester, Leics, England. [Krol, Maarten] Netherlands Inst Space Res SRON, Utrecht, Netherlands. [Krol, Maarten] Univ Utrecht, Inst Marine & Atmospher Res Utrecht, Utrecht, Netherlands. RP Lorente, A (reprint author), Wageningen Univ, Meteorol & Air Qual Grp, Wageningen, Netherlands. EM alba.lorentedelgado@wur.nl FU Quality Assurance for Essential Climate Variables (QA4ECV) [607405]; DLR [50EE1247] FX This research has been supported by the FP7 Project Quality Assurance for Essential Climate Variables (QA4ECV), grant No. 607405. Andreas Hilboll and Andreas Richter acknowledge funding by DLR in the scope of the Sentinel- 5 Precursor verification project (grant 50EE1247). UoL acknowledges the use of the ALICE and SPECTRE High Performance Computing Facility at the University of Leicester. We would like to thank the two anonymous referees for the useful interactive discussion in the review process. NR 66 TC 0 Z9 0 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 MAR 7 PY 2017 VL 10 IS 3 BP 759 EP 782 DI 10.5194/amt-10-759-2017 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EN6QO UT WOS:000396128700003 ER PT J AU Liu, JH Rodriguez, JM Steenrod, SD Douglass, AR Logan, JA Olsen, MA Wargan, K Ziemke, JR AF Liu, Junhua Rodriguez, Jose M. Steenrod, Stephen D. Douglass, Anne R. Logan, Jennifer A. Olsen, Mark A. Wargan, Krzysztof Ziemke, Jerald R. TI Causes of interannual variability over the southern hemispheric tropospheric ozone maximum SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID TROPICAL UPPER TROPOSPHERE; BIOMASS BURNING EMISSIONS; 1997-1998 EL-NINO; SATELLITE MEASUREMENTS; COLUMN OZONE; ATMOSPHERIC CHEMISTRY; DEEP CONVECTION; TRANSPORT MODEL; FIRE EMISSIONS; ATLANTIC AB We examine the relative contribution of processes controlling the interannual variability (IAV) of tropospheric ozone over four sub-regions of the southern hemispheric tropospheric ozone maximum (SHTOM) over a 20-year period. Our study is based on hindcast simulations from the National Aeronautics and Space Administration Global Modeling Initiative chemistry transport model (NASA GMI-CTM) of tropospheric and stratospheric chemistry, driven by assimilated Modern Era Retrospective Analysis for Research and Applications (MERRA) meteorological fields. Our analysis shows that over SHTOM region, the IAV of the stratospheric contribution is the most important factor driving the IAV of upper tropospheric ozone (270 hPa), where ozone has a strong radiative effect. Over the South Atlantic region, the contribution from surface emissions to the IAV of ozone exceeds that from stratospheric input at and below 430 hPa. Over the South Indian Ocean, the IAV of stratospheric ozone makes the largest contribution to the IAV of ozone with little or no influence from surface emissions at 270 and 430 hPa in austral winter. Over the tropical South Atlantic region, the contribution from IAV of stratospheric input dominates in austral winter at 270 hPa and drops to less than half but is still significant at 430 hPa. Emission contributions are not significant at these two levels. The IAV of lightning over this region also contributes to the IAV of ozone in September and December. Over the tropical southeastern Pacific, the contribution of the IAV of stratospheric input is significant at 270 and 430 hPa in austral winter, and emissions have little influence. C1 [Liu, Junhua; Steenrod, Stephen D.] Univ Space Res Assoc, GESTAR, Columbia, MD 21044 USA. [Liu, Junhua; Rodriguez, Jose M.; Steenrod, Stephen D.; Douglass, Anne R.; Olsen, Mark A.; Wargan, Krzysztof; Ziemke, Jerald R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Logan, Jennifer A.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Olsen, Mark A.; Ziemke, Jerald R.] Morgan State Univ, Baltimore, MD 21239 USA. [Wargan, Krzysztof] Sci Syst & Applicat Inc, Lanham, MD USA. RP Liu, JH (reprint author), Univ Space Res Assoc, GESTAR, Columbia, MD 21044 USA.; Liu, JH (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM junhua.liu@nasa.gov FU NASA's Atmospheric Chemistry Modeling and Analysis Program (ACMAP) [NNH12ZDA001N] FX I gratefully acknowledge the financial support from NASA's Atmospheric Chemistry Modeling and Analysis Program (ACMAP) (grant NNH12ZDA001N). Work was performed under contract with NASA at the Goddard Space Flight Center. I would like to thank K. Pickering, L. Oman, A. Thompson, and H. Liu for their helpful discussion. NR 77 TC 0 Z9 0 U1 0 U2 0 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 MAR 7 PY 2017 VL 17 IS 5 BP 3279 EP 3299 DI 10.5194/acp-17-3279-2017 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EN6QN UT WOS:000396128600002 ER PT J AU Nicholls, SD Decker, SG Tao, WK Lang, SE Shi, JJ Mohr, KI AF Nicholls, Stephen D. Decker, Steven G. Tao, Wei-Kuo Lang, Stephen E. Shi, Jainn J. Mohr, Karen I. TI Influence of bulk microphysics schemes upon Weather Research and Forecasting (WRF) version 3.6.1 nor'easter simulations SO GEOSCIENTIFIC MODEL DEVELOPMENT LA English DT Article ID CONVECTIVE SYSTEMS; RADAR REFLECTIVITIES; CLOUD MICROPHYSICS; MESOSCALE MODEL; WINTER STORMS; IN-SITU; PARAMETERIZATION; IMPACT; PRECIPITATION; SENSITIVITY AB This study evaluated the impact of five single- or double-moment bulk microphysics schemes (BMPSs) on Weather Research and Forecasting model (WRF) simulations of seven intense wintertime cyclones impacting the mid-Atlantic United States; 5-day long WRF simulations were initialized roughly 24 h prior to the onset of coastal cyclogenesis off the North Carolina coastline. In all, 35 model simulations (five BMPSs and seven cases) were run and their associated microphysics-related storm properties (hydrometer mixing ratios, precipitation, and radar reflectivity) were evaluated against model analysis and available gridded radar and ground-based precipitation products. Inter-BMPS comparisons of column-integrated mixing ratios and mixing ratio profiles reveal little variability in non-frozen hydrometeor species due to their shared programming heritage, yet their assumptions concerning snow and graupel intercepts, ice supersaturation, snow and graupel density maps, and terminal velocities led to considerable variability in both simulated frozen hydrometeor species and radar reflectivity. WRF-simulated precipitation fields exhibit minor spatiotemporal variability amongst BMPSs, yet their spatial extent is largely conserved. Compared to ground-based precipitation data, WRF simulations demonstrate low-to-moderate (0.217-0.414) threat scores and a rainfall distribution shifted toward higher values. Finally, an analysis of WRF and gridded radar reflectivity data via contoured frequency with altitude diagrams (CFADs) reveals notable variability amongst BMPSs, where better performing schemes favored lower graupel mixing ratios and better underlying aggregation assumptions. C1 [Nicholls, Stephen D.; Tao, Wei-Kuo; Lang, Stephen E.; Shi, Jainn J.; Mohr, Karen I.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20716 USA. [Nicholls, Stephen D.] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. [Decker, Steven G.] Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08850 USA. [Lang, Stephen E.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Shi, Jainn J.] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21251 USA. RP Nicholls, SD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20716 USA.; Nicholls, SD (reprint author), Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. EM stephen.d.nicholls@nasa.gov FU Joint Center for Earth Systems Technology (JCET); University of Maryland Baltimore County (UMBC); New Jersey Agricultural Experiment Station FX This research was supported by the Joint Center for Earth Systems Technology (JCET), the University of Maryland Baltimore County (UMBC), and in part by the New Jersey Agricultural Experiment Station. 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 66 TC 0 Z9 0 U1 1 U2 1 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1991-959X EI 1991-9603 J9 GEOSCI MODEL DEV JI Geosci. Model Dev. PD MAR 3 PY 2017 VL 10 IS 2 BP 1033 EP 1049 DI 10.5194/gmd-10-1033-2017 PG 17 WC Geosciences, Multidisciplinary SC Geology GA EM5ZD UT WOS:000395391700002 ER PT J AU de Putter, R Dore, O Green, D Meyers, J AF de Putter, Roland Dore, Olivier Green, Daniel Meyers, Joel TI Single-field inflation and the local ansatz: Distinguishability and consistency SO PHYSICAL REVIEW D LA English DT Article ID PRIMORDIAL NON-GAUSSIANITY; MODEL AB The single-field consistency conditions and the local ansatz have played separate but important roles in characterizing the non-Gaussian signatures of single-and multifield inflation respectively. We explore the precise relationship between these two approaches and their predictions. We demonstrate that the predictions of the single-field consistency conditions can never be satisfied by a general local ansatz with deviations necessarily arising at order (n(s) - 1)(2). This implies that there is, in principle, a minimum difference between single-and (fully local) multifield inflation in observables sensitive to the squeezed limit such as scale-dependent halo bias. We also explore some potential observational implications of the consistency conditions and its relationship to the local ansatz. In particular, we propose a new scheme to test the consistency relations. In analogy with delensing of the cosmic microwave background, one can deproject the coupling of the long wavelength modes with the short wavelength modes and test for residual anomalous coupling. C1 [de Putter, Roland; Dore, Olivier] CALTECH, Pasadena, CA 91125 USA. [Dore, Olivier] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Green, Daniel] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Green, Daniel; Meyers, Joel] Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. RP de Putter, R (reprint author), CALTECH, Pasadena, CA 91125 USA. FU NSERC; Canadian Institute for Advanced Research; Heising-Simons foundation; Vincent and Beatrice Tremaine Fellowship FX We thank Daniel Baumann, Rafael Porto, and Alex van Engelen for helpful discussions. D. G. was supported by an NSERC Discovery Grant and the Canadian Institute for Advanced Research. R. d. P. and O. D. acknowledge support by the Heising-Simons foundation. J. M. was supported by the Vincent and Beatrice Tremaine Fellowship. Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 55 TC 0 Z9 0 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD MAR 3 PY 2017 VL 95 IS 6 AR 063501 DI 10.1103/PhysRevD.95.063501 PG 11 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA EN5FP UT WOS:000396031300005 ER PT J AU Kundan, A Nguyen, TTT Plawsky, JL Wayner, PC Chao, DF Sicker, RJ AF Kundan, Akshay Nguyen, Thao T. T. Plawsky, Joel L. Wayner, Peter C., Jr. Chao, David F. Sicker, Ronald J. TI Condensation on Highly Superheated Surfaces: Unstable Thin Films in a Wickless Heat Pipe SO PHYSICAL REVIEW LETTERS LA English DT Article ID DROPWISE CONDENSATION; CONSTANT-AREA; ADIABATIC TIP; MICROGRAVITY; EVAPORATION; MODEL; CAPILLARY; TRANSPORT; STANDARD; GROOVES AB A wickless heat pipe was operated on the International Space Station to provide a better understanding of how the microgravity environment might alter the physical and interfacial forces driving evaporation and condensation. Traditional heat pipes are divided into three zones: evaporation at the heated end, condensation at the cooled end, and intermediate or adiabatic in between. The microgravity experiments reported herein show that the situation may be dramatically more complicated. Beyond a threshold heat input, there was a transition from evaporation at the heated end to large-scale condensation, even as surface temperatures exceeded the boiling point by 160 Kappa. The hotter the surface, the more vapor was condensed onto it. The condensation process at the heated end is initiated by thickness and temperature disturbances in the thin liquid film that wet the solid surface. Those disturbances effectively leave the vapor "superheated" in that region. Condensation is amplified and sustained by the high Marangoni stresses that exist near the heater and that drive liquid to cooler regions of the device. C1 [Kundan, Akshay; Nguyen, Thao T. T.; Plawsky, Joel L.; Wayner, Peter C., Jr.] Rensselaer Polytech Inst, Howard P Isermann Dept Chem & Biol Engn, Troy, NY 12180 USA. [Chao, David F.; Sicker, Ronald J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Plawsky, JL (reprint author), Rensselaer Polytech Inst, Howard P Isermann Dept Chem & Biol Engn, Troy, NY 12180 USA. EM akshaykundan@gmail.com; nguyen.thaoche@gmail.com; plawsky@rpi.edu; wayner@rpi.edu; David.F.Chao@nasa.gov; Ronald.J.Sicker@nasa.gov FU National Aeronautics and Space Administration (NASA) [NNX13AQ78G]; National Science Foundation [CBET-1603318] FX This material is based on the work supported by the National Aeronautics and Space Administration (NASA) under Grant No. NNX13AQ78G and the National Science Foundation under Grant No. CBET-1603318. The raw data and full-resolution composite images are available from NASA's Physical Sciences Informatics System. NR 41 TC 0 Z9 0 U1 1 U2 1 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 MAR 3 PY 2017 VL 118 IS 9 AR 094501 DI 10.1103/PhysRevLett.118.094501 PG 6 WC Physics, Multidisciplinary SC Physics GA EN5LC UT WOS:000396045900010 PM 28306276 ER PT J AU Gao, Y Casalena, L Bowers, ML Noebe, RD Mills, MJ Wang, Y AF Gao, Y. Casalena, L. Bowers, M. L. Noebe, R. D. Mills, M. J. Wang, Y. TI An origin of functional fatigue of shape memory alloys SO ACTA MATERIALIA LA English DT Article DE Shape memory alloys; Martensitic phase transformations; Crystal symmetry; Alloy design; Defects ID MARTENSITIC TRANSFORMATIONS; PHASE-TRANSFORMATIONS; NITI; DEFORMATION; MICROSTRUCTURE; REVERSIBILITY; BEHAVIOR; SUPERELASTICITY; PRECIPITATION; MICROCRYSTALS AB Functional fatigue (FF) during thermal and mechanical cycling, which leads to the generation of macroscopic irrecoverable strain and the loss of dimensional stability, is a critical issue that limits the service life of shape memory alloys (SMAs). Although it has been demonstrated experimentally that such a phenomenon is related to microstructural changes, a fundamental understanding of the physical origin of FF is still lacking, especially from a crystallographic point of view. In this study, we show that in addition to the normal martensitic phase transformation pathway (PTP), there is a symmetry-dictated non-phase-transformation pathway (SDNPTP) during phase transformation cycling, whose activation could play a key role in leading to FR By investigating crystal symmetry changes along both the PTPs and SDNPTPs, the characteristic types of defects (e.g., dislocations and grain boundaries) generated during transformation cycling can be predicted systematically, and agree well with those observed experimentally in NiTi. By analyzing key materials parameters that could suppress the SDNPTP5, strategies to develop high performance SMAs with much improved FF resistance through crystallographic design and transformation pathway engineering are suggested. (C) 2017 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved. C1 [Gao, Y.; Casalena, L.; Bowers, M. L.; Mills, M. J.; Wang, Y.] Ohio State Univ, Dept Mat Sci & Engn, Columbus, OH 43210 USA. [Noebe, R. D.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA. RP Wang, Y (reprint author), Ohio State Univ, Dept Mat Sci & Engn, Columbus, OH 43210 USA. EM wang.363@osu.edu FU Department of Energy [DE-SC0001258]; Natural Science Foundation [DMR-141032]; NASA Transformative Aeronautics Concepts Program (TACP), Transformational Tools & Technologies Project FX The work was supported by the Department of Energy Grant No. DE-SC0001258 and Natural Science Foundation Grant No. DMR-141032. RDN gratefully acknowledges support from the NASA Transformative Aeronautics Concepts Program (TACP), Transformational Tools & Technologies Project. NR 57 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 1359-6454 EI 1873-2453 J9 ACTA MATER JI Acta Mater. PD MAR PY 2017 VL 126 BP 389 EP 400 DI 10.1016/j.actamat.2017.01.001 PG 12 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA EL9DB UT WOS:000394918500037 ER PT J AU Gao, P Marley, MS Zahnle, K Robinson, TD Lewis, NK AF Gao, Peter Marley, Mark S. Zahnle, Kevin Robinson, Tyler D. Lewis, Nikole K. TI Sulfur Hazes in Giant Exoplanet Atmospheres: Impacts on Reflected Light Spectra SO ASTRONOMICAL JOURNAL LA English DT Article DE planets and satellites; atmospheres ID HUBBLE-SPACE-TELESCOPE; HR 8799 PLANETS; TRANSMISSION SPECTRUM; BROWN DWARFS; ULTRAVIOLET ABSORBER; THERMAL STRUCTURE; ELEMENTAL SULFUR; CLOUD PROPERTIES; HEATING RATES; GAMMA-CEPHEI AB Recent work has shown that sulfur hazes may arise in the atmospheres of some giant exoplanets, due to the photolysis of H2S. We investigate the impact such a haze would have on an exoplanet's geometric albedo spectrum and how it may affect the direct imaging results of the Wide Field Infrared Survey Telescope ( WFIRST), a planned NASA space telescope. For temperate ( 250 K= 0.5. A wide ring favors a rim that, on the star-facing side, looks more like a knife edge than a doughnut. The data are also compatible with the combination of a narrow ring and an inner disk of unspecified nature inside the dust sublimation radius. The disk inner part has a thickness z/r approximate to 0.2, flaring to z/r approximate to 0.5 in the outer part. We confirm the known luminosity- radius relation; a simple physical model is consistent with both the mean luminosity- radius relation and the ring relative width; however, a significant spread around the mean relation is present. In some of the objects we find a halo component, fully resolved at the shortest interferometer spacing, that is related to the HAeBe class. C1 [Lazare, B.; Berger, J. -P.; Le Bouquin, J. -B.; Benisty, M.; Malbet, F.; Delboulbe, A.; Duvert, G.; Jocou, L.; Menard, F.; Moulin, T.; Perraut, K.; Rochat, S.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. [Lazare, B.; Berger, J. -P.; Le Bouquin, J. -B.; Benisty, M.; Malbet, F.; Delboulbe, A.; Duvert, G.; Jocou, L.; Menard, F.; Moulin, T.; Perraut, K.; Rochat, S.] CNRS, IPAG, F-38000 Grenoble, France. [Berger, J. -P.] ESO, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Kluska, J.; Kraus, S.] Univ Exeter, Dept Phys & Astron, Stocker Rd, Exeter EX4 4QL, Devon, England. [Koen, C.] Univ Western Cape, Dept Stat, Private Bag X17, ZA-7535 Bellville, South Africa. [Absil, O.] Univ Liege, STAR, 19c Allee Six Aout, B-4000 Liege, Belgium. [Pinte, C.] CNRS INSU, UMI FCA, Paris, France. [Thi, W. -F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Baron, F.] Georgia State Univ, Ctr High Angular Resolut Astron, POB 3969, Atlanta, GA 30302 USA. [Juhasz, A.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Isella, A.] Rice Univ, Dept Phys & Astron, 6100 Main St, Houston, TX 77005 USA. [Lachaume, R.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Ctr Astroingn, Casilla 306, Santiago 22, Chile. [Lachaume, R.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Monnier, J. D.] Univ Michigan, Dept Astron, 1085 S Univ Ave,311 West Hall, Ann Arbor, MI 48109 USA. [Millan-Gabet, R.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Millan-Gabet, R.] CALTECH, NASA, Exoplanet Sci Inst, 770 S Wilson Ave, Pasadena, CA 91125 USA. [Soulez, F.; Tallon, M.; Thiebaut, E.] Univ Lyon 1, CNRS, Ecole Normale Super Lyon, CRAL,Observ Lyon, F-69364 Lyon, France. [Soulez, F.] Ecole Polytech Fed Lausanne, Biomed Imaging Grp, CH-1015 Lausanne, Switzerland. [Traub, W.] Jet Prop Lab, M-S 321-100,4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Zins, G.] ESO Vitacura, Alonso de Cordova 3107,Casilla 19001, Santiago, Chile. [Pinte, C.] Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile. RP Lazare, B (reprint author), Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.; Lazare, B (reprint author), CNRS, IPAG, F-38000 Grenoble, France. EM Bernard.Lazareff@univ-grenoble-alpes.fr FU ESO Telescopes at the La Silla Paranal Observatory [190.C-0963]; Marie Sklodowska-Curie CIG grant [618910]; NSF-AST [1210972] FX Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 190.C-0963. Generous time allocations by SAAO are gratefully acknowledged. We are grateful to Francois Van Wyk for diligently carrying out the infrared part of the photometry at Sutherland. J.K. acknowledges support from a Marie Sklodowska-Curie CIG grant (Ref. 618910, PI: Stefan Kraus). J.D.M. and F.B. acknowledge support from NSF-AST 1210972. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This research has made use of: the Jean-Marie Mariotti Center Aspro2 and SearchCal services6; the SIM-BAD database, operated at CDS, Strasbourg, France; and data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology. This work has made use of data from the European Space Agency (ESA) mission Gaia (http://www.cosmos.esa.int/gaia). NR 102 TC 1 Z9 1 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2017 VL 599 AR A85 DI 10.1051/0004-6361/201629305 PG 41 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN2EH UT WOS:000395821900048 ER PT J AU Milli, J Vigan, A Mouillet, D Lagrange, AM Augereau, JC Pinte, C Mawet, D Schmid, HM Boccaletti, A Matra, L Kral, Q Ertel, S Chauvin, G Bazzon, A Menard, F Beuzit, JL Thalmann, C Dominik, C Feldt, M Henning, T Min, M Girard, JH Galicher, R Bonnefoy, M Fusco, T de Boer, J Janson, M Maire, AL Mesa, D Schlieder, JE AF Milli, J. Vigan, A. Mouillet, D. Lagrange, A. -M. Augereau, J. -C. Pinte, C. Mawet, D. Schmid, H. M. Boccaletti, A. Matra, L. Kral, Q. Ertel, S. Chauvin, G. Bazzon, A. Menard, F. Beuzit, J. -L. Thalmann, C. Dominik, C. Feldt, M. Henning, T. Min, M. Girard, J. H. Galicher, R. Bonnefoy, M. Fusco, T. de Boer, J. Janson, M. Maire, A. -L. Mesa, D. Schlieder, J. E. CA SPHERE Consortium TI Near-infrared scattered light properties of the HR4796A dust ring A measured scattering phase function from 13.6 degrees to 166.6 degrees SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE instrumentation: high angular resolution; planet-disk interactions; planets and satellites: detection; scattering; planetary systems ID STAR HR 4796A; CIRCUMSTELLAR DISK; DEBRIS DISKS; BETA-PICTORIS; GAS CONTENT; OPTICAL-PROPERTIES; MASSIVE COLLISION; PLANET FORMATION; SELF-CONSISTENT; GIANT PLANETS AB Context. HR4796A is surrounded by a debris disc, observed in scattered light as an inclined ring with a high surface brightness. Past observations have raised several questions. First, a strong brightness asymmetry detected in polarised reflected light has recently challenged our understanding of scattering by the dust particles in this system. Secondly, the morphology of the ring strongly suggests the presence of planets, although no planets have been detected to date. Aims. We aim here at measuring with high accuracy the morphology and photometry of the ring in scattered light, in order to derive the phase function of the dust and constrain its near-infrared spectral properties. We also want to constrain the presence of planets and set improved constraints on the origin of the observed ring morphology. Methods. We obtained high-angular resolution coronagraphic images of the circumstellar environment around HR4796A with VLT/SPHERE during the commissioning of the instrument in May 2014 and during guaranteed-time observations in February 2015. The observations reveal for the first time the entire ring of dust, including the semi-minor axis that was previously hidden either behind the coronagraphic spot or in the speckle noise. Results. We determine empirically the scattering phase function of the dust in the H band from 13.6 degrees to 166.6 degrees. It shows a prominent peak of forward scattering, never detected before, for scattering angles below 30 degrees. We analyse the reflectance spectra of the disc from the 0.95 mu m to 1.6 mu m, confirming the red colour of the dust, and derive detection limits on the presence of planetary mass objects. Conclusions. We confirm which side of the disc is inclined towards the Earth. The analysis of the phase function, especially below 45 degrees, suggests that the dust population is dominated by particles much larger than the observation wavelength, of about 20 mu m. Compact Mie grains of this size are incompatible with the spectral energy distribution of the disc, however the observed rise in scattering efficiency beyond 50 degrees points towards aggregates which could reconcile both observables. We do not detect companions orbiting the star, but our high-contrast observations provide the most stringent constraints yet on the presence of planets responsible for the morphology of the dust. C1 [Milli, J.; Girard, J. H.] ESO, Alonso Cordova 3107, Santiago 19001, Chile. [Milli, J.; Mouillet, D.; Lagrange, A. -M.; Augereau, J. -C.; Pinte, C.; Chauvin, G.; Menard, F.; Beuzit, J. -L.; Bonnefoy, M.] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France. [Vigan, A.] Aix Marseille Univ, CNRS, LAM, Marseille, France. [Pinte, C.] Univ Chile, UMI FCA, CNRS, INSU France UMI 3386, Santiago, Chile. [Menard, F.] Univ Chile, UMI FCA, Santiago, Chile. [Mawet, D.] CALTECH, Dept Astron, 1200 E Calif Blvd,MC 249-17, Pasadena, CA 91125 USA. [Mawet, D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Schmid, H. M.; Bazzon, A.; Thalmann, C.] Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland. [Bazzon, A.; Galicher, R.] Univ Paris 06, Univ Paris Diderot, UPMC,LESIA, Sorbonne Univ,PSL Res Univ,CNRS,Observ Paris, Sorbonne Paris Cite 5 Pl Jules Janssen, F-92190 Meudon, France. [Matra, L.; Kral, Q.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Ertel, S.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85719 USA. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, POB 94249, NL-1090 GE Amsterdam, Netherlands. [Feldt, M.; Henning, T.; Maire, A. -L.; Schlieder, J. E.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Min, M.] SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. [Fusco, T.] Off Natl Etud & Rech Aerosp, French Aerosp Lab, BP 72,29 Ave Div Leclerc, F-92322 Chatillon, France. [de Boer, J.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Janson, M.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden. [Mesa, D.] Osserv Astron Padova, INAF, Vicolo Osservatorio 5, I-35122 Padua, Italy. [Schlieder, J. E.] NASA Exoplanet Sci Inst, Pasadena, CA USA. RP Milli, J (reprint author), ESO, Alonso Cordova 3107, Santiago 19001, Chile.; Milli, J (reprint author), Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France. EM jmilli@eso.org FU ESO; ANR blanche GIPSE [ANR-14-CE33-0018]; Labex OSUG; STFC; European Union through ERC [279973]; CNRS (France); MPIA (Germany); INAF (Italy); FINES (Switzerland); NOVA (Netherlands); European Commission Sixth and Seventh Framework Programmes as part of the Optical Infrared Coordination Network [RII3-Ct2004-001566]; [226604]; [312430] FX J.M. acknowledges financial support from the ESO fellowship programme. A.M.L. acknowledges the support from the ANR blanche GIPSE (ANR-14-CE33-0018) and the Labex OSUG. L.M. acknowledges support by STFC and ESO through graduate studentships and by the European Union through ERC grant number 279973. We would like to thank ESO staff and technical operators at the Paranal Observatory. We thank M. Meyer and D. Rouan for their valueable suggestions and comments during the review by the Center) for their work during the data reduction process. We thank V. Faramaz for the discussion on the eccentricity of the disc. SPHERE is an instrument designed and built by a consortium consisting of IPAG (Grenoble, France), MPIA (Heidelberg, Germany), LAM (Marseille, France), LESIA (Paris, France), Laboratoire Lagrange (Nice, France), INAF - Osservatorio di Padova (Italy), Observatoire de Geneve (Switzerland), ETH Zurich (Switzerland), NOVA (Netherlands), ONERA (France) and ASTRON (Netherlands) in collaboration with ESO. SPHERE was funded by ESO, with additional contributions from CNRS (France), MPIA (Germany), INAF (Italy), FINES (Switzerland) and NOVA (Netherlands). SPHERE also received funding from the European Commission Sixth and Seventh Framework Programmes as part of the Optical Infrared Coordination Network for Astronomy (OPTICON) under grant number RII3-Ct2004-001566 for FP6 (2004-2008), grant number 226604 for FP7 (2009-2012) and grant number 312430 for FP7 (2013-2016). NR 77 TC 0 Z9 0 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2017 VL 599 AR A108 DI 10.1051/0004-6361/201527838 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN2EH UT WOS:000395821900007 ER PT J AU Venuti, L Bouvier, J Cody, AM Stauffer, JR Micela, G Rebull, LM Alencar, SHP Sousa, AP Hillenbrand, LA Flaccomio, E AF Venuti, L. Bouvier, J. Cody, A. M. Stauffer, J. R. Micela, G. Rebull, L. M. Alencar, S. H. P. Sousa, A. P. Hillenbrand, L. A. Flaccomio, E. TI CSI 2264: Investigating rotation and its connection with disk accretion in the young open cluster NGC 2264 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; stars: low-mass; stars: pre-main sequence; stars: rotation stars: variables: T Tauri, Herbig Ae/Be; open clusters and associations: individual: NGC 2264 ID PRE-MAIN-SEQUENCE; T-TAURI STARS; ORION NEBULA CLUSTER; LOW-MASS STARS; ANGULAR-MOMENTUM EVOLUTION; MAGNETOCENTRIFUGALLY DRIVEN FLOWS; TERM PHOTOMETRIC VARIABILITY; BROWN DWARF CANDIDATES; POWERED STELLAR WINDS; SOLAR-LIKE STARS AB Context. The low spin rates measured for solar-type stars at an age of a few Myr (similar to 10% of the break-up velocity) indicate that some mechanism of angular momentum regulation must be at play in the early pre-main sequence. This may be associated with magnetospheric accretion and star-disk interaction, as suggested by observations that disk-bearing objects (CTTS) are slower rotators than diskless sources (WTTS) in young star clusters. Aims. We characterize the rotation properties for members of the star-forming region NGC 2264 (similar to 3 Myr) as a function of mass, and investigate the accretion-rotation connection at an age where about 50% of the stars have already lost their disks. Methods. We examined a sample of 500 cluster members (40% with disks, 60% without disks), distributed in mass between similar to 0.15 and 2 M-circle dot, whose photometric variations were monitored in the optical for 38 consecutive days with the CoRoT space observatory. Light curves were analyzed for periodicity using three different techniques: the Lomb-Scargle periodogram, the autocorrelation function and the string-length method. Periods were searched in the range between 0.17 days (i.e., 4 h, twice the data sampling adopted) and 19 days (half the total time span). Period detections were confirmed using a variety of statistical tools (false alarm probability, Q-statistics), as well as visual inspection of the direct and phase-folded light curves. Results. About 62% of sources in our sample were found to be periodic; the period detection rate is 70% among WTTS and 58% among CTTS. The vast majority of periodic sources exhibit rotational periods shorter than 13 d. The period distribution obtained for the cluster consists of a smooth distribution centered around P = 5 : 2 d with two peaks, located respectively at P = 1-2 d and at P = 3-4 d. A separate analysis of the rotation properties for CTTS and WTTS indicates that the P = 1-2 d peak is associated with the latter, while both groups contribute to the P = 3-4 d peak. The comparison between CTTS and WTTS supports the idea of a rotation-accretion connection: their respective rotational properties are statistically different, and CTTS rotate on average more slowly than WTTS. We also observe that CTTS with the strongest signatures of accretion (largest UV flux excesses) tend to exhibit slow rotation rates; a clear dearth of fast rotators with strong accretion signatures emerges from our sample. This connection between rotation properties and accretion traced via UV excess measurements is consistent with earlier findings, revealed by IR excess measurements, that fast rotators in young star clusters are typically devoid of dusty disks. On the other hand, WTTS span the whole range of rotation periods detected across the cluster. We also investigated whether the rotation properties we measure for NGC 2264 members show any dependence on stellar mass or on stellar inner structure (radiative core mass to total mass ratio). No statistically significant correlation emerged from our analysis regarding the second issue; however, we did infer some evidence of a period-mass trend, lower-mass stars spinning on average faster than higher-mass stars, although our data did not allow us to assess the statistical significance of such a trend beyond the 10% level. Conclusions. This study confirms that disks impact the rotational properties of young stars and influence their rotational evolution. The idea of disk-locking, recently tested in numerical models of the rotational evolution of young stars between 1 and 12 Myr, may be consistent with the pictures of rotation and rotation-accretion connection that we observe for the NGC 2264 cluster. However, the origin of the several substructures that we observe in the period distribution, notably the multiple peaks, deserves further investigation. C1 [Venuti, L.; Micela, G.; Flaccomio, E.] Osserv Astron Palermo, Inst Nazionale Astrofis, Piazza Parlamento 1, I-90134 Palermo, Italy. [Venuti, L.; Bouvier, J.] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France. [Cody, A. M.] NASA, Ames Res Ctr, Kepler Sci Office, Moffett Field, CA 94035 USA. RP Venuti, L (reprint author), Osserv Astron Palermo, Inst Nazionale Astrofis, Piazza Parlamento 1, I-90134 Palermo, Italy. EM lvenuti@astropa.unipa.it FU National Institute for Astrophysics (INAF) of the Italian Ministry of Education, University and Research ("The GAIA-ESO Survey"); CNPq; CAPES; [ANR 2011 Blanc SIMI5-6 020 01] FX We thank the referee for a prompt and constructive report. This work is based on data from the CoRoT space mission, which has been developed and operated by CNES, with the contribution of Austria, Belgium, Brazil, ESA (RSSD and Science Programme), Germany, and Spain. This publication also makes use of data from MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. We thank Suzanne Aigrain for detrending the CoRoT light curves used in this work. L.V. acknowledges useful discussions on histogram statistics with Dipan Sengupta. The authors acknowledge support through the PRIN INAF 2014 funding scheme of the National Institute for Astrophysics (INAF) of the Italian Ministry of Education, University and Research ("The GAIA-ESO Survey", P.I.: S. Randich). This study was also supported by the grant ANR 2011 Blanc SIMI5-6 020 01 "Toupies: Towards understanding the spin evolution of stars". S.H.P.A. acknowledges financial support from CNPq, CAPES and Fapemig. NR 122 TC 0 Z9 0 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2017 VL 599 AR A23 DI 10.1051/0004-6361/201629537 PG 44 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN2EH UT WOS:000395821900068 ER PT J AU Aharonian, FA Akamatsu, H Akimoto, F Allen, SW Angelini, L Arnaud, KA Audard, M Awaki, H Axelsson, M Bamba, A Bautz, MW Blandford, RD Bulbul, E Brenneman, LW Brown, GV Cackett, EM Chernyakova, M Chiao, MP Coppi, P Costantini, E de Plaa, J den Herder, JW Done, C Dotani, T Ebisawa, K Eckart, ME Enoto, T Ezoe, Y Fabian, AC Ferrigno, C Foster, AR Fujimoto, R Fukazawa, Y Furuzawa, A Galeazzi, M Gallo, LC Gandhi, P Giustini, M Goldwurm, A Gu, L Guainazzi, M Haba, Y Hagino, K Hamaguchi, K Harrus, I Hatsukade, I Hayashi, K Hayashi, T Hayashida, K Hiraga, J Hornschemeier, AE Hoshino, A Hughes, JP Ichinohe, Y Iizuka, R Inoue, H Inoue, S Inoue, Y Ishibashi, K Ishida, M Ishikawa, K Ishisaki, Y Itoh, M Iwai, M Iyomoto, N Kaastra, JS Kallman, T Kamae, T Kara, E Kataoka, J Katsuda, S Katsuta, J Kawaharada, M Kawai, N Kelley, RL Khangulyan, D Kilbourne, CA King, AL Kitaguchi, T Kitamoto, S Kitayama, T Kohmura, T Kokubun, M Koyama, S Koyama, K Kretschmar, P Krimm, HA Kubota, A Kunieda, H Laurent, P Lebrun, F Lee, SH Leutenegger, MA Limousin, O Loewenstein, M Long, KS Lumb, DH Madejski, GM Maeda, Y Maier, D Makishima, K Markevitch, M Matsumoto, H Matsushita, K McCammon, D McNamara, BR Mehdipour, M Miller, ED Miller, JM Mineshige, S Mitsuda, K Mitsuishi, I Miyazawa, T Mizuno, T Mori, H Mori, K Moseley, H Mukai, K Murakami, H Murakami, T Mushotzky, RF Nakagawa, T Nakajima, H Nakamori, T Nakano, T Nakashima, S Nakazawa, K Nobukawa, K Nobukawa, M Noda, H Nomachi, M O'Dell, SL Odaka, H Ohashi, T Ohno, M Okajima, T Ota, N Ozaki, M Paerels, F Paltani, S Parmar, A Petre, R Pinto, C Pohl, M Porter, FS Pottschmidt, K Ramsey, BD Reynolds, CS Russell, HR Safi-Harb, S Saito, S Sakai, K Sameshima, H Sasaki, T Sato, G Sato, K Sato, R Sawada, M Schartel, N Serlemitsos, PJ Seta, H Shidatsu, M Simionescu, A Smith, RK Soong, Y Stawarz, L Sugawara, Y Sugita, S Szymkowiak, AE Tajima, H Takahashi, H Takahashi, T Takeda, S Takei, Y Tamagawa, T Tamura, K Tamura, T Tanaka, T Tanaka, Y Tanaka, Y Tashiro, M Tawara, Y Terada, Y Terashima, Y Tombesi, F Tomida, H Tsuboi, Y Tsujimoto, M Tsunemi, H Tsuru, T Uchida, H Uchiyama, H Uchiyama, Y Ueda, S Ueda, Y Ueno, S Uno, S Urry, CM Ursino, E de Vries, CP Watanabe, S Werner, N Wik, DR Wilkins, DR Williams, BJ Yamada, S Yamaguchi, H Yamaoka, K Yamasaki, NY Yamauchi, M Yamauchi, S Yaqoob, T Yatsu, Y Yonetoku, D Yoshida, A Zhuravleva, I Zoghbi, A AF Aharonian, F. A. Akamatsu, H. Akimoto, F. Allen, S. W. Angelini, L. Arnaud, K. A. Audard, M. Awaki, H. Axelsson, M. Bamba, A. Bautz, M. W. Blandford, R. D. Bulbul, E. Brenneman, L. W. Brown, G. V. Cackett, E. M. Chernyakova, M. Chiao, M. P. Coppi, P. Costantini, E. de Plaa, J. den Herder, J. -W. Done, C. Dotani, T. Ebisawa, K. Eckart, M. E. Enoto, T. Ezoe, Y. Fabian, A. C. Ferrigno, C. Foster, A. R. Fujimoto, R. Fukazawa, Y. Furuzawa, A. Galeazzi, M. Gallo, L. C. Gandhi, P. Giustini, M. Goldwurm, A. Gu, L. Guainazzi, M. Haba, Y. Hagino, K. Hamaguchi, K. Harrus, I. Hatsukade, I. Hayashi, K. Hayashi, T. Hayashida, K. Hiraga, J. Hornschemeier, A. E. Hoshino, A. Hughes, J. P. Ichinohe, Y. Iizuka, R. Inoue, H. Inoue, S. Inoue, Y. Ishibashi, K. Ishida, M. Ishikawa, K. Ishisaki, Y. Itoh, M. Iwai, M. Iyomoto, N. Kaastra, J. S. Kallman, T. Kamae, T. Kara, E. Kataoka, J. Katsuda, S. Katsuta, J. Kawaharada, M. Kawai, N. Kelley, R. L. Khangulyan, D. Kilbourne, C. A. King, A. L. Kitaguchi, T. Kitamoto, S. Kitayama, T. Kohmura, T. Kokubun, M. Koyama, S. Koyama, K. Kretschmar, P. Krimm, H. A. Kubota, A. Kunieda, H. Laurent, P. Lebrun, F. Lee, S. -H. Leutenegger, M. A. Limousin, O. Loewenstein, M. Long, K. S. Lumb, D. H. Madejski, G. M. Maeda, Y. Maier, D. Makishima, K. Markevitch, M. Matsumoto, H. Matsushita, K. McCammon, D. McNamara, B. R. Mehdipour, M. Miller, E. D. Miller, J. M. Mineshige, S. Mitsuda, K. Mitsuishi, I. Miyazawa, T. Mizuno, T. Mori, H. Mori, K. Moseley, H. Mukai, K. Murakami, H. Murakami, T. Mushotzky, R. F. Nakagawa, T. Nakajima, H. Nakamori, T. Nakano, T. Nakashima, S. Nakazawa, K. Nobukawa, K. Nobukawa, M. Noda, H. Nomachi, M. O'Dell, S. L. Odaka, H. Ohashi, T. Ohno, M. Okajima, T. Ota, N. Ozaki, M. Paerels, F. Paltani, S. Parmar, A. Petre, R. Pinto, C. Pohl, M. Porter, F. S. Pottschmidt, K. Ramsey, B. D. Reynolds, C. S. Russell, H. R. Safi-Harb, S. Saito, S. Sakai, K. Sameshima, H. Sasaki, T. Sato, G. Sato, K. Sato, R. Sawada, M. Schartel, N. Serlemitsos, P. J. Seta, H. Shidatsu, M. Simionescu, A. Smith, R. K. Soong, Y. Stawarz, L. Sugawara, Y. Sugita, S. Szymkowiak, A. E. Tajima, H. Takahashi, H. Takahashi, T. Takeda, S. Takei, Y. Tamagawa, T. Tamura, K. Tamura, T. Tanaka, T. Tanaka, Yasuo Tanaka, Yasuyuki Tashiro, M. Tawara, Y. Terada, Y. Terashima, Y. Tombesi, F. Tomida, H. Tsuboi, Y. Tsujimoto, M. Tsunemi, H. Tsuru, T. Uchida, H. Uchiyama, H. Uchiyama, Y. Ueda, S. Ueda, Y. Ueno, S. Uno, S. Urry, C. M. Ursino, E. de Vries, C. P. Watanabe, S. Werner, N. Wik, D. R. Wilkins, D. R. Williams, B. J. Yamada, S. Yamaguchi, H. Yamaoka, K. Yamasaki, N. Y. Yamauchi, M. Yamauchi, S. Yaqoob, T. Yatsu, Y. Yonetoku, D. Yoshida, A. Zhuravleva, I. Zoghbi, A. CA Hitomi Collaboration TI Hitomi Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE dark matter; galaxies: clusters: individual (A426); galaxies: clusters: intracluster medium; X-rays: galaxies: clusters ID DECAYING DARK-MATTER; X-RAY; SUZAKU; TEMPERATURE; SEARCH AB X-ray spectroscopy with Hitomi was expected to resolve the origin of the faint unidentified E approximate to 3.5 keV emission line reported in several low-resolution studies of various massive systems, such as galaxies and clusters, including the Perseus cluster. We have analyzed the Hitomi first-light observation of the Perseus cluster. The emission line expected for Perseus based on the XMM-Newton signal from the large cluster sample under the dark matter decay scenario is too faint to be detectable in the Hitomi data. However, the previously reported 3.5 keV flux from Perseus was anomalously high compared to the sample-based prediction. We find no unidentified line at the reported high flux level. Taking into account the XMM measurement uncertainties for this region, the inconsistency with Hitomi is at a 99% significance for a broad dark matter line and at 99.7% for a narrow line from the gas. We do not find anomalously high fluxes of the nearby faint K line or the Ar satellite line that were proposed as explanations for the earlier 3.5 keV detections. We do find a hint of a broad excess near the energies of high-n transitions of S XVI (E similar or equal to 3.44 keV rest-frame)-a possible signature of charge exchange in the molecular nebula and another proposed explanation for the unidentified line. While its energy is consistent with XMM pn detections, it is unlikely to explain the MOS signal. A confirmation of this interesting feature has to wait for a more sensitive observation with a future calorimeter experiment. C1 [Aharonian, F. A.; Chernyakova, M.] Dublin Inst Adv Studies, Astron & Astrophys Sect, Dublin 2, Ireland. [Aharonian, F. A.] Natl Res Nucl Univ MEPHI, Moscow 115409, Russia. [Akamatsu, H.; Costantini, E.; de Plaa, J.; den Herder, J. -W.; Giustini, M.; Gu, L.; Kaastra, J. S.; Mehdipour, M.; de Vries, C. P.] SRON Netherlands Inst Space Res, Utrecht, Netherlands. [Akimoto, F.; Hayashi, T.; Ishibashi, K.; Kunieda, H.; Mitsuishi, I.; Tamura, K.; Tawara, Y.; Yamaoka, K.] Nagoya Univ, Dept Phys, Nagoya, Aichi 4648602, Japan. [Allen, S. W.; Blandford, R. D.; Kamae, T.; King, A. L.; Madejski, G. M.; Zhuravleva, I.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Allen, S. W.; Blandford, R. D.; King, A. L.; Zhuravleva, I.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Allen, S. W.; Blandford, R. D.; Madejski, G. M.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Angelini, L.; Arnaud, K. A.; Chiao, M. P.; Eckart, M. E.; Hamaguchi, K.; Harrus, I.; Hornschemeier, A. E.; Kallman, T.; Kelley, R. L.; Kilbourne, C. A.; Krimm, H. A.; Leutenegger, M. A.; Loewenstein, M.; Markevitch, M.; Mori, H.; Moseley, H.; Mukai, K.; Okajima, T.; Petre, R.; Porter, F. S.; Pottschmidt, K.; Sakai, K.; Serlemitsos, P. J.; Soong, Y.; Tombesi, F.; Wik, D. R.; Williams, B. J.; Yamaguchi, H.; Yaqoob, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Arnaud, K. A.; Kara, E.; Loewenstein, M.; Mushotzky, R. F.; Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Audard, M.; Ferrigno, C.; Paltani, S.; Pohl, M.] Univ Geneva, CH-1211 Geneva 4, Switzerland. [Awaki, H.; Terashima, Y.] Ehime Univ, Dept Phys, Matsuyama, Ehime 7908577, Japan. [Axelsson, M.; Ezoe, Y.; Ichinohe, Y.; Ishisaki, Y.; Ohashi, T.; Seta, H.; Yamada, S.] Tokyo Metropolitan Univ, Dept Phys, Tokyo 1920397, Japan. [Bamba, A.; Nakazawa, K.] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. [Bautz, M. W.; Bulbul, E.; Miller, E. D.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Brenneman, L. W.; Foster, A. R.; Smith, R. K.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Brown, G. V.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Cackett, E. M.; Fabian, A. C.; Pinto, C.; Russell, H. R.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Coppi, P.; Szymkowiak, A. E.; Urry, C. M.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Done, C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Dotani, T.; Ebisawa, K.; Guainazzi, M.; Hagino, K.; Hayashi, K.; Iizuka, R.; Inoue, H.; Inoue, Y.; Ishida, M.; Ishikawa, K.; Iwai, M.; Kokubun, M.; Koyama, S.; Lee, S. -H.; Maeda, Y.; Mitsuda, K.; Nakagawa, T.; Nakashima, S.; Odaka, H.; Ozaki, M.; Sameshima, H.; Sato, G.; Sato, R.; Simionescu, A.; Sugawara, Y.; Takahashi, T.; Takei, Y.; Tamura, T.; Tanaka, Yasuo; Tomida, H.; Tsujimoto, M.; Ueda, S.; Ueno, S.; Watanabe, S.; Yamasaki, N. Y.] Japan Aerosp Explorat Agcy JAXA, ISAS, Sagamihara, Kanagawa 2525210, Japan. [Enoto, T.; Mineshige, S.; Ueda, Y.] Kyoto Univ, Dept Astron, Kyoto 6068502, Japan. [Enoto, T.] Kyoto Univ, Hakubi Ctr Adv Res, Kyoto 6068302, Japan. [Fujimoto, R.; Murakami, T.; Yonetoku, D.] Kanazawa Univ, Fac Math & Phys, Kanazawa, Ishikawa 9201192, Japan. [Fukazawa, Y.; Katsuta, J.; Kitaguchi, T.; Mizuno, T.; Ohno, M.; Takahashi, H.; Tanaka, Yasuyuki] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Furuzawa, A.] Fujita Hlth Univ, Toyoake, Aichi 4701192, Japan. [Galeazzi, M.; Ursino, E.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA. [Gallo, L. C.; Wilkins, D. R.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Gandhi, P.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. [Goldwurm, A.; Laurent, P.; Lebrun, F.; Limousin, O.; Maier, D.] CEA Saclay, Serv Astrophys, IRFU, F-91191 Gif Sur Yvette, France. [Guainazzi, M.; Kretschmar, P.; Schartel, N.] European Space Agcy, ESAC, Madrid, Spain. [Haba, Y.] Aichi Univ Educ, Dept Phys & Astron, Kariya, Aichi 4488543, Japan. [Hamaguchi, K.; Harrus, I.; Mukai, K.; Pottschmidt, K.; Yaqoob, T.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Hatsukade, I.; Mori, K.; Yamauchi, M.] Miyazaki Univ, Dept Appl Phys & Elect Engn, Miyazaki 8892192, Japan. [Hayashida, K.; Inoue, S.; Nakajima, H.; Tsunemi, H.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. [Hiraga, J.] Kwansei Gakuin Univ, Dept Phys, Sch Sci & Technol, Sanda, Hyogo 6691337, Japan. [Hoshino, A.; Khangulyan, D.; Kitamoto, S.; Saito, S.; Uchiyama, Y.] Rikkyo Univ, Dept Phys, Tokyo 1718501, Japan. [Hughes, J. P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Itoh, M.] Kobe Univ, Fac Human Dev, Kobe, Hyogo 6578501, Japan. [Iyomoto, N.] Kyushu Univ, Fukuoka 8190395, Japan. [Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Tokyo 1698555, Japan. [Katsuda, S.; Tsuboi, Y.] Chuo Univ, Dept Phys, Tokyo 1128551, Japan. [Kawaharada, M.] Japan Aerosp Explorat Agcy JAXA, Tsukuba Space Ctr TKSC, Tsukuba, Ibaraki 3058505, Japan. [Kawai, N.; Sugita, S.; Yatsu, Y.] Tokyo Inst Technol, Dept Phys, Tokyo 1528551, Japan. [Kitayama, T.] Toho Univ, Dept Phys, Chiba 2748510, Japan. [Kohmura, T.] Tokyo Univ Sci, Dept Phys, Chiba 2788510, Japan. [Koyama, K.; Tanaka, T.; Tsuru, T.; Uchida, H.] Kyoto Univ, Dept Phys, Kyoto 6068502, Japan. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21046 USA. [Kubota, A.] Shibaura Inst Technol, Dept Elect Informat Syst, Saitama 3378570, Japan. [Long, K. S.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Lumb, D. H.; Parmar, A.] European Space Agcy, European Space Res & Technol Ctr ESTEC, NL-2200 AG Noordwijk, Netherlands. [Makishima, K.; Shidatsu, M.] RIKEN, Wako, Saitama 3510198, Japan. [Matsumoto, H.] Nagoya Univ, Kobayashi Maskawa Inst, Nagoya, Aichi 4648602, Japan. [Matsushita, K.; Sasaki, T.; Sato, K.] Tokyo Univ Sci, Dept Phys, Tokyo 1628601, Japan. [McCammon, D.] Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA. [McNamara, B. R.] Univ Waterloo, Waterloo, ON N2L 3G1, Canada. [Miller, J. M.; Zoghbi, A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Miyazawa, T.] Okinawa Inst Sci & Technol Grad Univ OIST, Onna, Okinawa 9040495, Japan. [Murakami, H.] Tohoku Gakuin Univ, Fac Liberal Arts, Dept Informat Sci, Sendai, Miyagi 9813193, Japan. [Nakamori, T.] Yamagata Univ, Dept Phys, Fac Sci, Yamagata 9908560, Japan. [Nakano, T.; Tamagawa, T.] RIKEN Nishina Ctr, Wako, Saitama 3510198, Japan. [Nobukawa, K.; Ota, N.; Yamauchi, S.] Nara Womens Univ, Dept Phys, Fac Sci, Nara 6308506, Japan. [Nobukawa, M.] Nara Univ Educ, Dept Teacher Training, Takabatake, Nara 6308528, Japan. [Nobukawa, M.] Nara Univ Educ, Sch Educ, Takabatake, Nara 6308528, Japan. [Noda, H.] Tohoku Univ, Frontier Res Inst Interdisciplinary Sci, Sendai, Miyagi 9808578, Japan. [Nomachi, M.] Osaka Univ, Res Ctr Nucl Phys Toyonaka, 1-1 Machikaneyama Machi, Toyonaka, Osaka 5600043, Japan. [O'Dell, S. L.; Ramsey, B. D.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Paerels, F.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Safi-Harb, S.; Yoshida, A.] Univ Manitoba, Dept Math & Astron, Winnipeg, MB R3T 2N2, Canada. [Sawada, M.] Aoyama Gakuin Univ, Dept Math & Phys, Sagamihara, Kanagawa 2525258, Japan. [Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Tajima, H.] Nagoya Univ, Inst Space Earth Environm Res, Nagoya, Aichi 4648601, Japan. [Takeda, S.] Okinawa Inst Sci & Technol Grad Univ OIST, Adv Med Instrumentat Unit, Onna, Okinawa 9040495, Japan. [Tashiro, M.; Terada, Y.] Saitama Univ, Dept Phys, Saitama 3388570, Japan. [Uchiyama, H.] Shizuoka Univ, Sci Educ, Fac Educ, Shizuoka 4228529, Japan. [Uno, S.] Nihon Fukushi Univ, Fac Hlth Sci, Mihama, Aichi 4750012, Japan. [Werner, N.] MTA Eotvos Univ Lendulet Hot Universe Res Grp, H-1117 Budapest, Hungary. [Werner, N.] Masaryk Univ, Fac Sci, Dept Theoret Phys & Astrophys, CS-61137 Brno, Czech Republic. [Wik, D. R.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Tamura, K (reprint author), Nagoya Univ, Dept Phys, Nagoya, Aichi 4648602, Japan.; Kilbourne, CA; Markevitch, M (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM caroline.a.kilbourne@nasa.gov; maxim.markevitch@nasa.gov; tamura.takayuki@jaxa.jp FU NASA Science Mission Directorate; DoE; NASA [NNX15AM19G]; LLNL [DE-AC5207NA27344]; NASA grants; European Space Agency; CNES; Centre National d'Etudes Spatiales; NWO; Netherlands Organization for Scientific Research; Swiss Secretariat for Education, Research and Innovation SERI; ESA's PRODEX programme; Canadian Space Agency; JSPS/MEXT KAKENHI [15H02070, 15K05107, 23340071, 26109506, 24103002, 25400236, 25800119, 25400237, 25287042, 24540229, 25105516, 23540280, 25400235, 25247028, 26800095, 25400231, 26220703, 24105007, 23340055, 15H00773, 23000004, 15H02090, 15K17610, 15H05438, 15H00785, 24540232]; JSPS International Research Fellowship; STFC [ST/L00075X/1]; JAXA International Top Young Fellowship; UK Science and Technology Funding Council (STFC) grant [ST/J003697/2]; ERC Advanced Grant [340442]; Hungarian Academy of Sciences [LP2016-11]; [DEAC376SF00515] FX We are grateful to the referee for insightful comments that improved the paper. We thank the JSPS Core-to-Core Program for support. We acknowledge all the JAXA members who have contributed to the Astro-H (Hitomi) project. All U.S. members gratefully acknowledge support through the NASA Science Mission Directorate. Stanford and SLAC members acknowledge support via DoE contract to SLAC National Accelerator Laboratory DEAC376SF00515 and NASA grant NNX15AM19G. Part of this work was performed under the auspices of the U.S. DoE by LLNL under Contract DE-AC5207NA27344 and also supported by NASA grants to LLNL.Support from the European Space Agency is gratefully acknowledged. French members acknowledge support from CNES, the Centre National d'Etudes Spatiales. SRON is supported by NWO, the Netherlands Organization for Scientific Research. Swiss team acknowledges support of the Swiss Secretariat for Education, Research and Innovation SERI and ESA's PRODEX programme. The Canadian Space Agency is acknowledged for the support of Canadian members. We acknowledge support from JSPS/MEXT KAKENHI grant numbers 15H02070, 15K05107, 23340071, 26109506, 24103002, 25400236, 25800119, 25400237, 25287042, 24540229, 25105516, 23540280, 25400235, 25247028, 26800095, 25400231, 25247028, 26220703, 24105007, 23340055, 15H00773, 23000004 15H02090, 15K17610, 15H05438, 15H00785, and 24540232. H. Akamatsu acknowledges support of NWO via Veni grant. M. Axelsson acknowledges JSPS International Research Fellowship. C.D. acknowledges STFC funding under grant ST/L00075X/1.P.G. acknowledges JAXA International Top Young Fellowship and UK Science and Technology Funding Council (STFC) grant ST/J003697/2. A.C.F., C.P., and H.R. acknowledge support from ERC Advanced Grant Feedback 340442. N.W. has been supported by the Lendulet LP2016-11 grant from the Hungarian Academy of Sciences. We thank contributions by many companies, including, in particular, NEC, Mitsubishi Heavy Industries, Sumitomo Heavy Industries, and Japan Aviation Electronics Industry. NR 31 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 1 PY 2017 VL 837 IS 1 AR L15 DI 10.3847/2041-8213/aa61fa PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN6OF UT WOS:000396122600001 ER PT J AU Rampino, MR AF Rampino, Michael R. TI Are Some Tillites Impact-Related Debris-Flow Deposits? SO JOURNAL OF GEOLOGY LA English DT Article ID PORT ASKAIG FORMATION; NON-GLACIAL ORIGIN; NORTHERN NORWAY; GLACIOMARINE SEDIMENTATION; BIGGANJARGGA TILLITE; GOWGANDA FORMATION; ALBION ISLAND; NW SCOTLAND; STAC FADA; EJECTA AB A number of ancient glacial deposits, or tillites, are currently interpreted as originating by subaqueous debris-flow processes at glacial termini. Problems in identifying the glacial origin of such deposits can arise because some criteria commonly used for establishing glaciation, especially outsize clasts interpreted as dropstones from icebergs, can apparently be produced by nonglacial debris flows and debris falls. Could some of these debris-flow diamictite deposits be related to large-body impacts, especially those that occurred at times other than established glacial periods? Debris-flow ejecta of known impacts seem to be marked by mildly shocked clasts showing evidence of plastic behavior with brittle failure, commonly resulting in multiple, partially displaced fractures, grading into crushed and brecciated clasts. These deformation features entail brief periods of high confining pressures, in accord with a hypervelocity-impact origin. I report here several debris-flow diamictites, currently interpreted as tillites, that exhibit these characteristic deformed stones. C1 [Rampino, Michael R.] NYU, Dept Biol, New York, NY 10003 USA. [Rampino, Michael R.] NYU, Dept Environm Studies, 550 1St Ave, New York, NY 10003 USA. [Rampino, Michael R.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Rampino, MR (reprint author), NYU, Dept Biol, New York, NY 10003 USA.; Rampino, MR (reprint author), NYU, Dept Environm Studies, 550 1St Ave, New York, NY 10003 USA.; Rampino, MR (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM mrr1@nyu.edu NR 81 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0022-1376 EI 1537-5269 J9 J GEOL JI J. Geol. PD MAR PY 2017 VL 125 IS 2 BP 155 EP 164 DI 10.1086/690212 PG 10 WC Geology SC Geology GA EM6YO UT WOS:000395458800004 ER PT J AU Bult, P AF Bult, Peter TI The Stochastic X-Ray Variability of the Accreting Millisecond Pulsar MAXI J0911-655 SO ASTROPHYSICAL JOURNAL LA English DT Article DE X-rays; individual (MAXI J0911-655) - stars; neutron - X-rays; binaries ID QUASI-PERIODIC OSCILLATIONS; ATOLL SOURCE STATES; SAX J1808.4-3658; HETE J1900.1-2455; TIMING FEATURES; NEUTRON-STARS; TERZAN 5; BINARIES; DISK; MASS AB In this work, I report on the stochastic X-ray variability of the 340 Hz accreting millisecond pulsar MAXI J0911-655. Analyzing pointed observations of the XMM-Newton and NuSTAR observatories, I find that the source shows broad band-limited stochastic variability in the 0.01-10 Hz range with a total fractional variability of similar to 24% rms in the 0.4-3 keV energy band that increases to similar to 40% rms in the 3-10 keV band. Additionally, a pair of harmonically related quasi-periodic oscillations (QPOs) are discovered. The fundamental frequency of this harmonic pair is observed between frequencies of 62 and 146 mHz. Like the band-limited noise, the amplitudes of the QPOs show a steep increase as a function of energy; this suggests that they share a similar origin, likely the inner accretion flow. Based on their energy dependence and frequency relation with respect to the noise terms, the QPOs are identified as low-frequency oscillations and discussed in terms of the Lense-Thirring precession model. C1 [Bult, Peter] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Bult, P (reprint author), NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 53 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 MAR 1 PY 2017 VL 837 IS 1 AR 61 DI 10.3847/1538-4357/aa607f PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN6AU UT WOS:000396087700002 ER PT J AU Chen, CTJ Brandt, WN Reines, AE Lansbury, G Stern, D Alexander, DM Bauer, F Del Moro, A Gandhi, P Harrison, FA Hickox, RC Koss, MJ Lanz, L Luo, B Mullaney, JR Ricci, C Trump, JR AF Chen, C. -T. J. Brandt, W. N. Reines, A. E. Lansbury, G. Stern, D. Alexander, D. M. Bauer, F. Del Moro, A. Gandhi, P. Harrison, F. A. Hickox, R. C. Koss, M. J. Lanz, L. Luo, B. Mullaney, J. R. Ricci, C. Trump, J. R. TI Hard X-Ray-selected AGNs in Low-mass Galaxies from the NuSTAR Serendipitous Survey SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: dwarf; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; SUPERMASSIVE BLACK-HOLES; RESOLUTION SPECTRAL TEMPLATES; SPITZER-SPACE-TELESCOPE; NEARBY DWARF GALAXIES; H-ALPHA EMISSION; MIDINFRARED SELECTION; HIGH-LUMINOSITY; STAR-FORMATION AB We present a sample of 10 low-mass active galactic nuclei (AGNs) selected from the 40-month Nuclear Spectroscopic Telescope Array (NuSTAR) serendipitous survey. The sample is selected to have robust NuSTAR detections at 3-24 keV, to be at z < 0.3, and to have optical r-band magnitudes at least 0.5. mag fainter than an L-* galaxy at its redshift. The median values of absolute magnitude, stellar mass, and 2-10 X-ray luminosity of our sample are < Mr > = -20.03, < M-*> = 4.6 x 10(9) M-circle dot, and < L2- 10keV > = 3.1 x 10(42) erg s (1), respectively. Five objects have detectable broad Ha emission in their optical spectra, indicating black hole masses of (1.1-10.4) x 10(6) M-circle dot. We find that 30(-10)(+17)% of the galaxies in our sample do not show AGN-like optical narrow emission lines, and one of the 10 galaxies in our sample, J115851 + 4243.2, shows evidence for heavy X-ray absorption. This result implies that a non-negligible fraction of low-mass galaxies might harbor accreting massive black holes that are missed by optical spectroscopic surveys and < 10 keV X-ray surveys. The mid-IR colors of our sample also indicate that these optically normal low-mass AGNs cannot be efficiently identified with typical AGN selection criteria based on Wide Field Infrared Survey Explorer colors. While the hard (> 10 keV) X-ray-selected low-mass AGN sample size is still limited, our results show that sensitive NuSTAR observations are capable of probing faint hard X-ray emission originating from the nuclei of low-mass galaxies out to moderate redshift ( z < 0.3), thus providing a critical step in understanding AGN demographics in low-mass galaxies. C1 [Chen, C. -T. J.; Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Chen, C. -T. J.; Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Reines, A. E.] Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA. [Lansbury, G.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Stern, D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Alexander, D. M.] Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England. [Bauer, F.; Ricci, C.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Casilla 306, Santiago 22, Chile. [Bauer, F.; Ricci, C.] Pontificia Univ Catolica Chile, Fac Fis, Ctr Astroingn, Casilla 306, Santiago 22, Chile. [Bauer, F.; Ricci, C.] Millennium Inst Astrophys, Santiago, Chile. [Bauer, F.] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA. [Del Moro, A.] Max Planck Inst Extraterr Phys MPE, Postfach 1312, D-85741 Garching, Germany. [Gandhi, P.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. [Harrison, F. A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Hickox, R. C.; Lanz, L.] Dartmouth Coll, Dept Phys & Astron, 6127 Wilder Lab, Hanover, NH 03755 USA. [Koss, M. J.] ETH, Dept Phys, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. [Luo, B.] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. [Mullaney, J. R.] Univ Sheffield, Dept Phys & Astron, Hounsfield Rd, Sheffield S3 7RH, S Yorkshire, England. [Ricci, C.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Trump, J. R.] Univ Connecticut, Dept Phys, 2152 Hillside Rd, Storrs, CT 06269 USA. RP Chen, CTJ (reprint author), Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.; Chen, CTJ (reprint author), Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. EM ctchen@psu.edu FU NASA [NNG08FD60C, NAS 5-26555]; National Aeronautics and Space Administration; Caltech NuSTAR subcontract [44A-1092750]; NASA through Hubble Fellowship grant - Space Telescope Science Institute [HST-HF2-51347.001-A]; Science and Technology Facilities Council [ST/L00075X/1]; NASA NuSTAR A01 Award [NNX15AV27G]; CONICYT-Chile [Basal-CATA PFB-06/2007]; FONDECYT Regular [1141218, 1151408]; China-CONICYT Fellowship; Ministry of Economy, Development, and Tourisms Millennium Science Initiative [IC120009]; National Science Foundation; Alfred P. Sloan Foundation; U.S. Department of Energy Office of Science FX We thank the referee for carefully reading the manuscript and providing helpful comments. This work was supported under NASA contract no. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by 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). C.-T.J.C. and W.N.B. acknowledge support from Caltech NuSTAR subcontract 44A-1092750. Support for A.E.R. was provided by NASA through Hubble Fellowship grant HST-HF2-51347.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. D.M.A. gratefully acknowledges support from Science and Technology Facilities Council (ST/L00075X/1). F.E.B. and C.R. acknowledge support from NASA NuSTAR A01 Award NNX15AV27G, CONICYT-Chile grants Basal-CATA PFB-06/2007, FONDECYT Regular 1141218 and 1151408, China-CONICYT Fellowship, and the Ministry of Economy, Development, and Tourisms Millennium Science Initiative through grant IC120009, awarded to the Millennium Institute of Astrophysics, MAS. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. 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/. This research has made use of the "Aladin sky atlas" developed at CDS, Strasbourg Observatory, France (Bonnarel et al. 2000). This work has also made use of observations made with the Spitzer Space Telescope, obtained from the NASA/IPAC Infrared Science Archive, both of which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 132 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 MAR 1 PY 2017 VL 837 IS 1 AR 48 DI 10.3847/1538-4357/aa5d5b PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN3OU UT WOS:000395918600013 ER PT J AU Luger, R Lustig-Yaeger, J Fleming, DP Tilley, MA Agol, E Meadows, VS Deitrick, R Barnes, R AF Luger, Rodrigo Lustig-Yaeger, Jacob Fleming, David P. Tilley, Matt A. Agol, Eric Meadows, Victoria S. Deitrick, Russell Barnes, Rory TI The Pale Green Dot: A Method to Characterize Proxima Centauri b Using Exo-Aurorae SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites; atmospheres - planets and satellites; aurorae - planets and satellites; detection - planets and satellites; terrestrial planets ID PLANETARY MAGNETIC-FIELDS; EARTH-LIKE EXOPLANETS; THERMAL PHASE CURVES; LOW-MASS STAR; SOLAR-WIND; EXTRASOLAR PLANETS; HD 209458B; TERRESTRIAL EXOPLANETS; GEOMAGNETIC STORMS; HABITABLE ZONES AB We examine the feasibility of detecting auroral emission from the potentially habitable exoplanet Proxima Centauri b. Detection of aurorae would yield an independent confirmation of the planet's existence, constrain the presence and composition of its atmosphere, and determine the planet's eccentricity and inclination, thereby breaking the mass-inclination degeneracy. If Proxima Centauri b is a terrestrial world with an Earth-like atmosphere and magnetic field, we estimate that the power at the 5577 angstrom O I auroral line is on the order of 0.1. TW under steady-state stellar wind, or similar to 100x. stronger than that on Earth. This corresponds to a planet-star contrast ratio of 10(-6)-10(-7) in a narrow band about the 5577 angstrom line, though higher contrast (10(-4)-10(-5)) may be possible during periods of strong magnetospheric disturbance (auroral power 1-10 TW). We searched the Proxima Centauri b HARPS data for the 5577 angstrom line and for other prominent oxygen and nitrogen lines, but find no signal, indicating that the O I auroral line contrast must be lower than 2 x 10(-2) (with power less than or similar to 3000 TW), consistent with our predictions. We find that observations of 0.1. TW auroral emission lines are likely infeasible with current and planned telescopes. However, future observations with a space-based coronagraphic telescope or a ground-based extremely large telescope (ELT) with a coronagraph could push sensitivity down to terawatt oxygen aurorae (contrast 7 x 10(-6)) with exposure times of similar to 1 day. If a coronagraph design contrast of 10(-7) can be achieved with negligible instrumental noise, a future concept ELT could observe steady-state auroral emission in a few nights. C1 [Luger, Rodrigo; Lustig-Yaeger, Jacob; Fleming, David P.; Agol, Eric; Meadows, Victoria S.; Deitrick, Russell; Barnes, Rory] Univ Washington, Dept Astron, Box 951580, Seattle, WA 98195 USA. [Luger, Rodrigo; Lustig-Yaeger, Jacob; Fleming, David P.; Tilley, Matt A.; Agol, Eric; Meadows, Victoria S.; Deitrick, Russell; Barnes, Rory] NASA, Astrobiol Inst, Virtual Planetary Lab Lead Team, Washington, DC 20546 USA. [Luger, Rodrigo; Lustig-Yaeger, Jacob; Tilley, Matt A.; Agol, Eric; Meadows, Victoria S.; Deitrick, Russell; Barnes, Rory] Univ Washington, Astrobiol Program, 3910 15th Ave NE,Box 351580, Seattle, WA 98195 USA. [Tilley, Matt A.] Univ Washington, Dept Earth & Space Sci, Box 351310, Seattle, WA 98195 USA. RP Luger, R (reprint author), Univ Washington, Dept Astron, Box 951580, Seattle, WA 98195 USA.; Luger, R (reprint author), NASA, Astrobiol Inst, Virtual Planetary Lab Lead Team, Washington, DC 20546 USA.; Luger, R (reprint author), Univ Washington, Astrobiol Program, 3910 15th Ave NE,Box 351580, Seattle, WA 98195 USA. EM rodluger@uw.edu FU NSF IGERT [DGE-1258485]; NASA [NNA13AA93A] FX We thank G. Anglada-Escude and the Pale Red Dot team for making their data publicly available, Giada Arney for useful discussions, R. W. Service for poetic inspiration, and the anonymous referee for their excellent comments and suggestions. D.P.F. is supported by an NSF IGERT DGE-1258485 fellowship. This work was supported by the NASA Astrobiology Institute's Virtual Planetary Laboratory under Cooperative Agreement number NNA13AA93A and was based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 072.C-0488(E), 082.C-0718(B), 096.C-0082(A), 096.C-0082(B), 096.C-0082 (C), 096.C-0082(D), 096.C-0082(E), 096.C-0082(F), 183.C-0437(A), and 191.C-0505(A). This work made use of the advanced computational, storage, and networking infrastructure provided by the Hyak supercomputer system at the University of Washington. Finally, this work also made use of the Python coronagraph noise model, developed by J. Lustig-Yaeger and available at https://github.com/jlustigy/coronagraph/. NR 110 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 MAR 1 PY 2017 VL 837 IS 1 AR 63 DI 10.3847/1538-4357/aa6040 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN6AU UT WOS:000396087700004 ER PT J AU Martinez, AO Crossfield, IJM Schlieder, JE Dressing, CD Obermeier, C Livingston, J Ciceri, S Peacock, S Beichman, CA Lepine, S Aller, KM Chance, QA Petigura, EA Howard, AW Werner, MW AF Martinez, Arturo O. Crossfield, Ian J. M. Schlieder, Joshua E. Dressing, Courtney D. Obermeier, Christian Livingston, John Ciceri, Simona Peacock, Sarah Beichman, Charles A. Lepine, Sebastien Aller, Kimberly M. Chance, Quadry A. Petigura, Erik A. Howard, Andrew W. Werner, Michael W. TI Stellar and Planetary Parameters for K2's Late-type Dwarf Systems from C1 to C5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; planetary systems; stars: fundamental parameters; stars: late-type; techniques: spectroscopic ID NEARBY M DWARFS; INFRARED TELESCOPE FACILITY; MAIN-SEQUENCE STARS; LOW-MASS STARS; ASTROPHYSICAL PARAMETERS; SPECTROSCOPIC SURVEY; SOLAR NEIGHBORHOOD; SPECTRAL TYPES; SIZED PLANETS; BAND SPECTRA AB The NASA K2 mission uses photometry to find planets transiting stars of various types. M dwarfs are of high interest since they host more short-period planets than any other type of main-sequence star and transiting planets around M dwarfs have deeper transits compared to other main-sequence stars. In this paper, we present stellar parameters from K and M dwarfs hosting transiting planet candidates discovered by our team. Using the SOFI spectrograph on the European Southern Observatory's New Technology Telescope, we obtained R approximate to 1000 J-, H-, and K-band (0.95-2.52 mu m) spectra of 34 late-type K2 planet and candidate planet host systems and 12 bright K4-M5 dwarfs with interferometrically measured radii and effective temperatures. Out of our 34 late-type K2 targets, we identify 27 of these stars as M dwarfs. We measure equivalent widths of spectral features, derive calibration relations using stars with interferometric measurements, and estimate stellar radii, effective temperatures, masses, and luminosities for the K2 planet hosts. Our calibrations provide radii and temperatures with median uncertainties of 0.059 R-circle dot (16.09%) and 160 K (4.33%), respectively. We then reassess the radii and equilibrium temperatures of known and candidate planets based on our spectroscopically derived stellar parameters. Since a planet's radius and equilibrium temperature depend on the parameters of its host star, our study provides more precise planetary parameters for planets and candidates orbiting late-type stars observed with K2. We find a median planet radius and an equilibrium temperature of approximately 3 R-circle plus and 500 K, respectively, with several systems (K2-18b and K2-72e) receiving near-Earth-like levels of incident irradiation. C1 [Martinez, Arturo O.] San Diego State Univ, Dept Astron, 5500 Campanile Dr, San Diego, CA 92182 USA. [Martinez, Arturo O.; Lepine, Sebastien] Georgia State Univ, Dept Phys & Astron, 25 Pk Pl NE 605, Atlanta, GA 30303 USA. [Martinez, Arturo O.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85719 USA. [Crossfield, Ian J. M.] Univ Arizona, Lunar & Planetary Lab, 1629 E Univ Blvd, Tucson, AZ 85721 USA. [Crossfield, Ian J. M.] UC Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA. [Schlieder, Joshua E.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. [Schlieder, Joshua E.; Beichman, Charles A.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Dressing, Courtney D.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Obermeier, Christian] Max Planck Inst Astron, Heidelberg, Germany. [Obermeier, Christian] Max Planck Inst Extraterr Phys, Garching, Germany. [Livingston, John; Petigura, Erik A.] Univ Tokyo, Grad Sch Sci, Dept Astron, 7-3-1 Bunkyo Ku, Tokyo 1130033, Japan. [Ciceri, Simona] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Aller, Kimberly M.] Univ Hawaii Manoa, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. [Chance, Quadry A.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85719 USA. [Howard, Andrew W.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Werner, Michael W.] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Martinez, AO (reprint author), San Diego State Univ, Dept Astron, 5500 Campanile Dr, San Diego, CA 92182 USA.; Martinez, AO (reprint author), Georgia State Univ, Dept Phys & Astron, 25 Pk Pl NE 605, Atlanta, GA 30303 USA.; Martinez, AO (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85719 USA. FU National Science Foundation [AST-1322432]; PAARE Grant for the California-Arizona Minority Partnership for Astronomy Research and Education (CAMPARE) [DUE-1356133]; Cal-Bridge CSU-UC PhD Bridge Program; Spitzer [GO 11026]; California Institute of Technology/Jet Propulsion Laboratory - NASA through the Sagan Fellowship Program; National Geographic Society FX This material is based on work supported by the National Science Foundation under Award nos. AST-1322432, a PAARE Grant for the California-Arizona Minority Partnership for Astronomy Research and Education (CAMPARE), and DUE-1356133, an S-STEM Grant for the Cal-Bridge CSU-UC PhD Bridge Program. This work was funded in part by Spitzer GO 11026 (PI Werner), managed by JPL/Caltech under a contract with NASA and locally by the University of Arizona. This work was performed in part under contract with the California Institute of Technology/Jet Propulsion Laboratory funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. Travel costs were partially supported by the National Geographic Society. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation. NR 80 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 MAR 1 PY 2017 VL 837 IS 1 AR 72 DI 10.3847/1538-4357/aa56c7 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN6AV UT WOS:000396087800004 ER PT J AU Prochazka, O Milligan, RO Allred, JC Kowalski, AF Kotrc, P Mathioudakis, M AF Prochazka, Ondrej Milligan, Ryan O. Allred, Joel C. Kowalski, Adam F. Kotrc, Pavel Mathioudakis, Mihalis TI Suppression of Hydrogen Emission in an X-class White-light Solar Flare SO ASTROPHYSICAL JOURNAL LA English DT Article DE line: formation; Sun: atmosphere; Sun: flares; techniques: spectroscopic ID DYNAMICS-OBSERVATORY SDO; 2014 MARCH 29; H-ALPHA; CONTINUUM; CHROMOSPHERE; SPECTRUM; SIMULATIONS; ULTRAVIOLET; IONIZATION; ATMOSPHERE AB We present unique NUV observations of a well-observed X-class flare from NOAA 12087 obtained at the Ondrejov Observatory. The flare shows a strong white-light continuum but no detectable emission in the higher Balmer and Lyman lines. Reuven Ramaty High-Energy Solar Spectroscopic Imager and Fermi observations indicate an extremely hard X-ray spectrum and gamma-ray emission. We use the RADYN radiative hydrodynamic code to perform two types of simulations: one where an energy of 3 x 10(11) erg cm(-2) s(-1) is deposited by an electron beam with a spectral index of approximate to 3, and a second where the same energy is applied directly to the photosphere. The combination of observations and simulations allows us to conclude that the white-light emission and the suppression or complete lack of hydrogen emission lines is best explained by a model where the dominant energy deposition layer is located in the lower layers of the solar atmosphere, rather than the chromosphere. C1 [Prochazka, Ondrej; Milligan, Ryan O.; Mathioudakis, Mihalis] Queens Univ Belfast, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Milligan, Ryan O.; Allred, Joel C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Milligan, Ryan O.] Catholic Univ Amer, Dept Phys, 620 Michigan Ave Northeast, Washington, DC 20064 USA. [Kowalski, Adam F.] Univ Colorado, Dept Astrophys & Planetary Sci, 2000 Colorado Ave, Boulder, CO 80305 USA. [Kowalski, Adam F.] Univ Colorado, Natl Solar Observ, 3665 Discovery Dr, Boulder, CO 80303 USA. [Kotrc, Pavel] Acad Sci Czech Republic, Astron Inst, Ondrejov 25165, Czech Republic. RP Prochazka, O (reprint author), Queens Univ Belfast, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. EM oprochazka01@qub.ac.uk FU European Community's Seventh Framework Programme (FP7) [606862]; NASA LWS/SDO Data Analysis grant [NNX14AE07G]; GA CR grant [16-18495S] FX The research leading to these results has received funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 606862 (F-CHROMA). Ryan O. Milligan acknowledges support from NASA LWS/SDO Data Analysis grant NNX14AE07G. Pavel Kotrc acknowledges support from GA CR grant 16-18495S. NR 52 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 MAR 1 PY 2017 VL 837 IS 1 AR 46 DI 10.3847/1538-4357/aa5da8 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN3OU UT WOS:000395918600011 ER PT J AU Provencal, S Buchard, V da Silva, AM Leduc, R Barrette, N AF Provencal, Simon Buchard, Virginie da Silva, Arlindo M. Leduc, Richard Barrette, Nathalie TI Evaluation of PM surface concentrations simulated by Version 1 of NASA's MERRA Aerosol Reanalysis over Europe SO ATMOSPHERIC POLLUTION RESEARCH LA English DT Article DE MERRAero; Evaluation; Particulate matter (PM); Air quality; Europe ID RESIDENTIAL WOOD COMBUSTION; PARTICULATE MATTER; AIR-QUALITY; MODEL PERFORMANCE; SAHARAN DUST; TRANSPORT; CITIES; URBAN AB This article evaluates the concentrations of particulate matter (PM) and some of its chemical speciation such as sulfate, organic carbon, black carbon and sea salt particles simulated at the surface by Version 1 of the Aerosol Reanalysis of NASA's Modern-Era Retrospective Analysis for Research and Application (MERRAero) over Europe. Measurement data from the European Monitoring and Evaluation Programme database were used. The concentrations of coarse PM (PM10), fine PM (PM2.5), sulfate and black carbon particles are overall well simulated, despite a slight and consistent overestimation of PM10 concentration, and a slight and consistent underestimation of PM2.5 and sulfate concentrations throughout most of the year. The concentration of organic carbon was largely underestimated, especially in winter, caused by two specific monitoring stations in Italy, resulting in an overall poor performance for this particular species. After removing these two stations from the sample, the evaluation of OC substantially improved but an underestimation in winter remained. Carbon emissions originating from anthropogenic sources, such as residential wood burning in winter, unresolved by MERRAero provide a plausible explanation for this discrepancy. The evaluation of PM2.5, sulfate and organic carbon concentrations improved during the summer. The concentration of fine sea salt particles was consistently and largely overestimated, but contributes relatively little to total PM2.5 concentration. Copyright (C) 2016 Turkish National Committee for Air Pollution Research and Control. Production and hosting by Elsevier B.V. All rights reserved. C1 [Provencal, Simon; Leduc, Richard; Barrette, Nathalie] Univ Laval, Dept Geog, Quebec City, PQ, Canada. [Buchard, Virginie; da Silva, Arlindo M.] NOAA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Buchard, Virginie] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA. RP Provencal, S (reprint author), Univ Laval, Dept Geog, Quebec City, PQ, Canada. EM simon.provencal.1@ulaval.ca NR 25 TC 0 Z9 0 U1 0 U2 0 PU TURKISH NATL COMMITTEE AIR POLLUTION RES & CONTROL-TUNCAP PI BUCA PA DOKUZ EYLUL UNIV, DEPT ENVIRONMENTAL ENGINEERING, TINAZTEPE CAMPUS, BUCA, IZMIR 35160, TURKEY SN 1309-1042 J9 ATMOS POLLUT RES JI Atmos. Pollut. Res. PD MAR PY 2017 VL 8 IS 2 BP 374 EP 382 DI 10.1016/j.apr.2016.10.009 PG 9 WC Environmental Sciences SC Environmental Sciences & Ecology GA EP5RF UT WOS:000397435600018 ER PT J AU Bufanda, E Hollowood, D Jeltema, TE Rykoff, ES Rozo, E Martini, P Abbott, TMC Abdalla, FB Allam, S Banerji, M Benoit-Levy, A Bertin, E Brooks, D Rosell, AC Kind, MC Carretero, J Cunha, CE da Costa, LN Desai, S Diehl, HT Dietrich, JP Evrard, AE Neto, AF Flaugher, B Frieman, J Gerdes, DW Goldstein, DA Gruen, D Gruendl, RA Gutierrez, G Honscheid, K James, DJ Kuehn, K Kuropatkin, N Lima, M Maia, MAG Marshall, JL Melchior, P Miquel, R Mohr, JJ Ogando, R Plazas, AA Romer, AK Rooney, P Sanchez, E Santiago, B Scarpine, V Sevilla-Noarbe, I Smith, RC Soares-Santos, M Sobreira, F Suchyta, E Tarle, G Thomas, D Tucker, DL Walker, AR AF Bufanda, E. Hollowood, D. Jeltema, T. E. Rykoff, E. S. Rozo, E. Martini, P. Abbott, T. M. C. Abdalla, F. B. Allam, S. Banerji, M. Benoit-Levy, A. Bertin, E. Brooks, D. Carnero Rosell, A. Kind, M. Carrasco Carretero, J. Cunha, C. E. da Costa, L. N. Desai, S. Diehl, H. T. Dietrich, J. P. Evrard, A. E. Fausti Neto, A. Flaugher, B. Frieman, J. Gerdes, D. W. Goldstein, D. A. Gruen, D. Gruendl, R. A. Gutierrez, G. Honscheid, K. James, D. J. Kuehn, K. Kuropatkin, N. Lima, M. Maia, M. A. G. Marshall, J. L. Melchior, P. Miquel, R. Mohr, J. J. Ogando, R. Plazas, A. A. Romer, A. K. Rooney, P. Sanchez, E. Santiago, B. Scarpine, V. Sevilla-Noarbe, I. Smith, R. C. Soares-Santos, M. Sobreira, F. Suchyta, E. Tarle, G. Thomas, D. Tucker, D. L. Walker, A. R. CA DES Collaboration TI The evolution of active galactic nuclei in clusters of galaxies from the Dark Energy Survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; X-rays: galaxies; X-rays: galaxies: clusters. ID SUPERMASSIVE BLACK-HOLES; STAR-FORMATION ACTIVITY; AGN HOST GALAXIES; SIMILAR-TO 2; X-RAY; VELOCITY DISPERSION; MULTIWAVELENGTH SURVEY; REDSHIFT CLUSTERS; FUNDAMENTAL PLANE; INACTIVE GALAXIES AB The correlation between active galactic nuclei (AGNs) and environment provides important clues to AGN fuelling and the relationship of black hole growth to galaxy evolution. In this paper, we analyse the fraction of galaxies in clusters hosting AGN as a function of redshift and cluster richness for X-ray-detected AGN associated with clusters of galaxies in Dark Energy Survey (DES) Science Verification data. The present sample includes 33 AGNs with LX > 1043 erg s(-1) in non-central, host galaxies with luminosity greater than 0.5L(*) from a total sample of 432 clusters in the redshift range of 0.1< z <0.95. Analysis of the present sample reveals that the AGN fraction in red-sequence cluster members has a strong positive correlation with redshift such that the AGN fraction increases by a factor of similar to 8 from low to high redshift, and the fraction of cluster galaxies hosting AGN at high redshifts is greater than the low-redshift fraction at 3.6 sigma. In particular, the AGN fraction increases steeply at the highest redshifts in our sample at z > 0.7. This result is in good agreement with previous work and parallels the increase in star formation in cluster galaxies over the same redshift range. However, the AGN fraction in clusters is observed to have no significant correlation with cluster mass. Future analyses with DES Year 1 through Year 3 data will be able to clarify whether AGN activity is correlated to cluster mass and will tightly constrain the relationship between cluster AGN populations and redshift. C1 [Bufanda, E.; Hollowood, D.; Jeltema, T. E.] Univ Calif Santa Cruz, Dept Phys & Santa Cruz, Inst Particle Phys, Santa Cruz, CA 95064 USA. [Rykoff, E. S.; Cunha, C. E.; Gruen, D.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA. [Rykoff, E. S.; Gruen, D.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Rozo, E.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. [Martini, P.; Honscheid, K.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Martini, P.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Abbott, T. M. C.; James, D. J.; Smith, R. C.; Walker, A. R.] Natl Optic Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile. [Abdalla, F. B.; Brooks, D.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Abdalla, F. B.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa. [Allam, S.; Diehl, H. T.; Flaugher, B.; Frieman, J.; Gutierrez, G.; Kuropatkin, N.; Scarpine, V.; Soares-Santos, M.; Tucker, D. L.] Fermilab Natl Accelerator Lab, PO 500, Batavia, IL 60510 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. [Benoit-Levy, A.; Bertin, E.] Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France. [Benoit-Levy, A.; Bertin, E.] UPMC Univ Paris 06, Sorbonne Univ, UMR 7095, Inst Astrophys Paris, F-75014 F- Paris, France. [Carnero Rosell, A.; da Costa, L. N.; Fausti Neto, A.; Lima, M.; Maia, M. A. G.; Ogando, R.; Santiago, B.; Sobreira, F.] Lab Interinst E Astron LlneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carnero Rosell, A.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Kind, M. Carrasco; Gruendl, R. A.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Kind, M. Carrasco; Gruendl, R. A.] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA. [Carretero, J.] IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans,S-N, E-08193 Barcelona, Spain. [Carretero, J.] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Barcelona, Spain. [Desai, S.; Dietrich, J. P.; Mohr, J. J.] Ludwig Maximilians Univ Munchen, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Desai, S.; Dietrich, J. P.; Mohr, J. J.] Excellence Cluster Univ, Boltzmannstr 2, D-85748 Garching, Germany. [Evrard, A. E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Evrard, A. E.; Gerdes, D. W.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Frieman, J.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Goldstein, D. A.] Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA. [Goldstein, D. A.] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Honscheid, K.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Lima, M.] Univ Sao Paulo, Dept Fis Matemat, Inst Fis, CP 66318, BR-05314970 Sao Paulo, SP, Brazil. [Marshall, J. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Melchior, P.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. [Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Mohr, J. J.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. [Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Romer, A. K.; Rooney, P.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England. [Sanchez, E.; Sevilla-Noarbe, I.] Ctr Invest Energet Medioambientales & Tecnol CIEM, E-28040 Madrid, Spain. [Santiago, B.] Univ Fed Rio Grande do Sul, Inst Fis, Caixa Postal 15051, BR-91501970 Porto Alegre, RS, Brazil. [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. [Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. RP Jeltema, TE (reprint author), Univ Calif Santa Cruz, Dept Phys & Santa Cruz, Inst Particle Phys, Santa Cruz, CA 95064 USA. EM tesla@ucsc.edu FU National Science Foundation [AST- 1138766]; MINECO [AYA2012- 39559, ESP201348274, FPA2013- 47986]; Centro de Excelencia Severo Ochoa [SEV- 2012- 0234]; European Research Council under the European Unions Seventh Framework Programme; ERC [240672, 291329, 306478] FX 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, ESP201348274, 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 Unions Seventh Framework Programme (FP7/ 2007- 2013) including ERC grant agreements 240672, 291329, and 306478. 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. NR 91 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 MAR PY 2017 VL 465 IS 3 BP 2531 EP 2539 DI 10.1093/mnras/stw2824 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EM2SM UT WOS:000395165900002 ER PT J AU MacCrann, N Aleksic, J Amara, A Bridle, SL Bruderer, C Chang, C Dodelson, S Eifler, TF Huff, EM Huterer, D Kacprzak, T Refregier, A Suchyta, E Wechsler, RH Zuntz, J Abbott, TMC Allam, S Annis, J Armstrong, R Benoit-Levy, A Brooks, D Burke, DL Rosell, AC Kind, MC Carretero, J Castander, FJ Crocce, M Cunha, CE da Costa, LN Desai, S Diehl, HT Dietrich, JP Doel, P Evrard, AE Flaugher, B Fosalba, P Gerdes, DW Goldstein, DA Gruen, D Gruendl, RA Gutierrez, G Honscheid, K James, DJ Jarvis, M Krause, E Kuehn, K Kuropatkin, N Lima, M Marshall, JL Melchior, P Menanteau, F Miquel, R Plazas, AA Romer, AK Rykoff, ES Sanchez, E Scarpine, V Sevilla-Noarbe, I Sheldon, E Soares-Santos, M Swanson, MEC Tarle, G Thomas, D Vikram, V AF MacCrann, N. Aleksic, J. Amara, A. Bridle, S. L. Bruderer, C. Chang, C. Dodelson, S. Eifler, T. F. Huff, E. M. Huterer, D. Kacprzak, T. Refregier, A. Suchyta, E. Wechsler, R. H. Zuntz, J. Abbott, T. M. C. Allam, S. Annis, J. Armstrong, R. Benoit-Levy, A. Brooks, D. Burke, D. L. Carnero Rosell, A. Kind, M. Carrasco Carretero, J. Castander, F. J. Crocce, M. Cunha, C. E. da Costa, L. N. Desai, S. Diehl, H. T. Dietrich, J. P. Doel, P. Evrard, A. E. Flaugher, B. Fosalba, P. Gerdes, D. W. Goldstein, D. A. Gruen, D. Gruendl, R. A. Gutierrez, G. Honscheid, K. James, D. J. Jarvis, M. Krause, E. Kuehn, K. Kuropatkin, N. Lima, M. Marshall, J. L. Melchior, P. Menanteau, F. Miquel, R. Plazas, A. A. Romer, A. K. Rykoff, E. S. Sanchez, E. Scarpine, V. Sevilla-Noarbe, I. Sheldon, E. Soares-Santos, M. Swanson, M. E. C. Tarle, G. Thomas, D. Vikram, V. CA DES Collaboration TI Inference from the small scales of cosmic shear with current and future Dark Energy Survey data SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: weak; large-scale structure of Universe. ID MATTER POWER SPECTRUM; WEAK-LENSING SURVEYS; INTRINSIC ALIGNMENTS; GALAXY FORMATION; HALO MODEL; PRECISION COSMOLOGY; BARYONS; SIMULATIONS; PHYSICS; CFHTLENS AB Cosmic shear is sensitive to fluctuations in the cosmological matter density field, including on small physical scales, where matter clustering is affected by baryonic physics in galaxies and galaxy clusters, such as star formation, supernovae feedback, and active galactic nuclei feedback. While muddying any cosmological information that is contained in small-scale cosmic shear measurements, this does mean that cosmic shear has the potential to constrain baryonic physics and galaxy formation. We perform an analysis of the Dark Energy Survey (DES) Science Verification (SV) cosmic shear measurements, now extended to smaller scales, and using the Mead et al. (2015) halo model to account for baryonic feedback. While the SV data has limited statistical power, we demonstrate using a simulated likelihood analysis that the final DES data will have the statistical power to differentiate among baryonic feedback scenarios. We also explore some of the difficulties in interpreting the small scales in cosmic shear measurements, presenting estimates of the size of several other systematic effects that make inference from small scales difficult, including uncertainty in the modelling of intrinsic alignment on non-linear scales, ' lensing bias ', and shape measurement selection effects. For the latter two, we make use of novel image simulations. While future cosmic shear data sets have the statistical power to constrain baryonic feedback scenarios, there are several systematic effects that require improved treatments, in order to make robust conclusions about baryonic feedback. C1 [MacCrann, N.; Bridle, S. L.; Zuntz, J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England. [Aleksic, J.] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain. [Amara, A.; Bruderer, C.; Chang, C.; Kacprzak, T.; Refregier, A.] Swiss Fed Inst Technol, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland. [Dodelson, S.; Gutierrez, G.; Kuropatkin, N.; Scarpine, V.; Soares-Santos, M.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. [Dodelson, S.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Eifler, T. F.; Huff, E. M.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Huterer, D.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Suchyta, E.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Wechsler, R. H.] StanfordUniversity, Dept Phys, 382 Via PuebloMall, Stanford, CA 94305 USA. [Wechsler, R. H.; Cunha, C. E.; Gruen, D.; Krause, E.; Rykoff, E. S.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Box 2450, Stanford, CA 94305 USA. [Wechsler, R. H.; Burke, D. L.; Rykoff, E. S.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Abbott, T. M. C.] 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. [Benoit-Levy, A.] Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France. [Benoit-Levy, A.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Benoit-Levy, A.] UPMC, Sorbonne Univ, Univ Paris 06, UMR Inst Astrophys Paris 7095, F-75014 Paris, France. [Carnero Rosell, A.; da Costa, L. N.; Lima, M.] Lab Interinstituc & Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carnero Rosell, A.; da Costa, L. N.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, Brazil. [Kind, M. Carrasco; Gruendl, R. A.; Menanteau, F.; Swanson, M. E. C.] Univ Illinois, Dept Astron, 1002 Green St, Urbana, IL 61801 USA. [Kind, M. Carrasco; Gruendl, R. A.; Menanteau, F.; Swanson, M. E. C.] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA. [Carretero, J.; Castander, F. J.; Crocce, M.] IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans,S-N, E-08193 Barcelona, Spain. [Desai, S.; Dietrich, J. P.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Desai, S.; Dietrich, J. P.] Ludwig Maximilians Univ Munchen, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Evrard, A. E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Goldstein, D. A.] Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA. [Goldstein, D. A.] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Honscheid, K.] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA. [Honscheid, K.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Lima, M.] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil. [Marshall, J. L.] Texas A& M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, College Stn, TX 77843 USA. [Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England. [Sanchez, E.; Sevilla-Noarbe, I.] CIEMAT, Avda Complutense,40, Madrid 28040, Spain. [Sheldon, E.] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA. [Thomas, D.] Univ Portsmouth, Inst Cosmol Gravitat, Portsmouth PO1 3FX, Hants, England. [Vikram, V.] Argonne Natl Lab, 9700 South Cass Ave, Lemont, IL 60439 USA. RP MacCrann, N (reprint author), Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England. EM maccrann.2@osu.edu FU MINECO [AYA2012- 39559, ESP201348274, FPA2013- 47986]; Centro de Excelencia Severo Ochoa [SEV- 2012-0234, SEV- 2012-0249]; European Research Council under the European Union Seventh [240672, 291329, 306478] FX supported by MINECO under grants AYA2012- 39559, ESP201348274, FPA2013- 47986, and Centro de Excelencia Severo Ochoa SEV- 2012-0234 and SEV- 2012-0249. Research leading to these results has received funding from the European Research Council under the European Union Seventh Framework Programme ( FP7/ 2007- 2013) includingERCgrant agreements 240672, 291329, and 306478. NR 88 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 MAR PY 2017 VL 465 IS 3 BP 2567 EP 2583 DI 10.1093/mnras/stw2849 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EM2SM UT WOS:000395165900005 ER PT J AU Gordon, YA Owers, MS Pimbblet, KA Croom, SM Alpaslan, M Baldry, IK Brough, S Brown, MJI Cluver, ME Conselice, CJ Davies, LJM Holwerda, BW Hopkins, AM Gunawardhana, MLP Loveday, J Taylor, EN Wang, LY AF Gordon, Yjan A. Owers, Matt S. Pimbblet, Kevin A. Croom, Scott M. Alpaslan, Mehmet Baldry, Ivan K. Brough, Sarah Brown, Michael J. I. Cluver, Michelle E. Conselice, Christopher J. Davies, Luke J. M. Holwerda, Benne W. Hopkins, Andrew M. Gunawardhana, Madusha L. P. Loveday, Jonathan Taylor, Edward N. Wang, Lingyu TI Galaxy and Mass Assembly (GAMA): active galactic nuclei in pairs of galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: observational; galaxies: active; galaxies: evolution; galaxies: interactions. ID DIGITAL SKY SURVEY; 1ST DATA RELEASE; STAR-FORMATION; STARBURST GALAXIES; SEYFERT-GALAXIES; REDSHIFT SURVEY; MULTIOBJECT SPECTROGRAPH; METALLICITY RELATION; LUMINOSITY FUNCTION; 2DF-SDSS LRG AB There exist conflicting observations on whether or not the environment of broad-and narrowline active galatic nuclei (AGN) differ and this consequently questions the validity of the AGN unification model. The high spectroscopic completeness of the Galaxy and Mass Assembly (GAMA) survey makes it ideal for a comprehensive analysis of the close environment of galaxies. To exploit this, and conduct a comparative analysis of the environment of broad-and narrow-line AGN within GAMA, we use a double-Gaussian emission line fitting method to model the more complex line profiles associated with broad-line AGN. We select 209 type 1 (i.e. unobscured), 464 type 1.5-1.9 (partially obscured), and 281 type 2 (obscured) AGN within the GAMA II data base. Comparing the fractions of these with neighbouring galaxies out to a pair separation of 350 kpc h(-1) and triangle z < 0.012 shows no difference between AGN of different type, except at separations less than 20 kpc h(-1) where our observations suggest an excess of type 2 AGN in close pairs. We analyse the properties of the galaxies neighbouring our AGN and find no significant differences in colour or the star formation activity of these galaxies. Further to this, we find that Sigma(5) is also consistent between broad-and narrow-line AGN. We conclude that the observations presented here are consistent with AGN unification. C1 [Gordon, Yjan A.; Pimbblet, Kevin A.] Univ Hull, EA Milne Ctr Astrophys, Cottingham Rd, Kingston Upon Hull HU6 7RX, N Humberside, England. [Gordon, Yjan A.; Pimbblet, Kevin A.] Univ Hull, Sch Math & Phys Sci, Cottingham Rd, Kingston Upon Hull HU6 7RX, N Humberside, England. [Owers, Matt S.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia. [Owers, Matt S.; Brough, Sarah; Hopkins, Andrew M.] AAO, POB 915, N Ryde, NSW 1670, Australia. [Pimbblet, Kevin A.; Brown, Michael J. I.] Monash Univ, Monash Ctr Astrophys MoCA, Clayton, Vic 3800, Australia. [Pimbblet, Kevin A.; Brown, Michael J. I.] Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia. [Croom, Scott M.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Alpaslan, Mehmet] NASA, Ames Res Ctr, Moffett Field, N232, Mountain View, CA 94035 USA. [Baldry, Ivan K.] Liverpool John Moores Univ, Astrophys Res Inst, IC2,Liverpool Sci Pk,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England. [Cluver, Michelle E.] Univ Western Cape, Dept Phys & Astron, Robert Sobukwe Rd, ZA-7535 Bellville, South Africa. [Conselice, Christopher J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Davies, Luke J. M.] Univ Western Australia, ICRAR, 35 Stirling Highway, Crawley, WA 6009, Australia. [Holwerda, Benne W.] Leiden Univ, Sterrenwacht Leiden, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands. [Gunawardhana, Madusha L. P.] Pontificia Univ Catolica Chile, Inst Astrofis, Vicuna Mackenna 4860, Santiago 7820436, Chile. [Gunawardhana, Madusha L. P.] Pontificia Univ Catolica Chile, Fac Fis, Ctr Astroingn, Vicuna Mackenna 4860, Santiago 7820436, Chile. [Loveday, Jonathan] Univ Sussex, Astron Ctr, Brighton BN1 9QH, E Sussex, England. [Taylor, Edward N.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Wang, Lingyu] SRON, Netherlands Inst Space Res, Landleven 12, NL-9747 AD Groningen, Netherlands. [Wang, Lingyu] Univ Groningen, Kapteyn Astron Inst, Postbus 800, NL-9700 AV Groningen, Netherlands. RP Gordon, YA (reprint author), Univ Hull, EA Milne Ctr Astrophys, Cottingham Rd, Kingston Upon Hull HU6 7RX, N Humberside, England.; Gordon, YA (reprint author), Univ Hull, Sch Math & Phys Sci, Cottingham Rd, Kingston Upon Hull HU6 7RX, N Humberside, England. EM y.gordon@2014.hull.ac.uk FU University of Hull through an internally funded PhDstudentship; Australian Research Council [FT140100255]; SDSS-III; [FONDECYT 3160492] FX The authors wish to thank the anonymous referee for their constructive comments. YAG acknowledges the financial support of the University of Hull through an internally funded PhDstudentship that has enabled this research to be undertaken, as well as discussions with Jacob Crossett and Dane Kleiner. MSO acknowledges the funding support from the Australian Research Council through a Future Fellowship (FT140100255). MLPG acknowledges CONICYT-Chile grant FONDECYT 3160492. 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, 1 www.taipan-survey.org 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. 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 website 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. This research made use of Astropy, a community- developed core PYTHON package for Astronomy (Astropy Collaboration 2013). NR 75 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2017 VL 465 IS 3 BP 2671 EP 2686 DI 10.1093/mnras/stw2925 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EM2SM UT WOS:000395165900013 ER PT J AU Hudson, TB Hou, TH Grimsley, BW Yuan, FG AF Hudson, Tyler B. Hou, Tan-Hung Grimsley, Brian W. Yuan, Fuh-Gwo TI Imaging of local porosity/voids using a fully non-contact air-coupled transducer and laser Doppler vibrometer system SO STRUCTURAL HEALTH MONITORING-AN INTERNATIONAL JOURNAL LA English DT Article DE Non-contact inspection; air-coupled transducer; laser Doppler vibrometer; frequency-wavenumber filtering; porosity; voids; structural health monitoring; non-destructive evaluation ID ULTRASONIC WAVE; GUIDED-WAVES; COMPOSITES; CURE AB This study exploits the feasibility of imaging zones of local porosity/voids simulated by introducing microspheres during layup of a unidirectional carbon fiber-reinforced polymer composite panel. A fully non-contact hybrid system primarily composed of an air-coupled transducer and a laser Doppler vibrometer was used for imaging the local porosity/void zones from the guided wave response. To improve image resolution, several preprocessing techniques are performed. The wavefield reconstructed from the laser Doppler vibrometer measurements was first denoised using a one-dimensional wavelet transform in the time domain followed by a two-dimensional wavelet transform in the spatial domain. From the total wavefield, the much weaker backscattered waves were separated from the stronger incident wave by frequency-wavenumber domain filtering. In order to further enhance the signal-to-noise ratio and sharpen the image, the attenuation of incident wave propagation to the damage site was compensated through two proposed weight functions. Finally, a zero-lag cross-correlation was performed for imaging the zone where the compensated incident and backscattered waves were in phase. This improved imaging condition, the denoised weighted zero-lag cross-correlation, was proposed and tested for defect imaging in the composite panel with eight intentionally introduced zones of high porosity/voids of varying diameters (1.59-6.35mm) and depths (0.36-1.08mm). As expected, the sensitivity of the non-contact air-coupled transducer/laser Doppler vibrometer hybrid system was limited by the wavelength of the excitation signal. The system incorporated with the denoised weighted zero-lag cross-correlation imaging condition for guided wave interrogation gave similar image quality in comparison with that by the immersion C-scan. C1 [Hudson, Tyler B.; Yuan, Fuh-Gwo] North Carolina State Univ, Dept Mech & Aerosp Engn, Raleigh, NC USA. [Hudson, Tyler B.; Yuan, Fuh-Gwo] Natl Inst Aerosp, Hampton, VA USA. [Hou, Tan-Hung; Grimsley, Brian W.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23665 USA. RP Hudson, TB (reprint author), 100 Explorat Way, Hampton, VA 23666 USA. EM tyler.b.hudson@nasa.gov FU Graduate Research Assistantship at National Institute of Aerospace through the Advanced Composites Project (ACP) at NASA Langley Research Center FX The author(s) disclosed receipt of the following financial support for the research, authorship, and/or publication of this article: The authors would like to acknowledge the financial support from a Graduate Research Assistantship at National Institute of Aerospace through the Advanced Composites Project (ACP) at NASA Langley Research Center. NR 30 TC 0 Z9 0 U1 0 U2 0 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1475-9217 EI 1741-3168 J9 STRUCT HEALTH MONIT JI Struct. Health Monit. PD MAR PY 2017 VL 16 IS 2 BP 164 EP 173 DI 10.1177/1475921716668843 PG 10 WC Engineering, Multidisciplinary; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA EM6BL UT WOS:000395397700004 ER PT J AU Godin-Beekmann, S Petropavloskikh, I Reis, S Newman, P Steinbrecht, W Rex, M Santee, ML Eckman, RS Zheng, XD Tully, MB Stevenson, DS Young, P Pyle, J Weber, M Tamminen, J Mills, G Bais, AF Heaviside, C Zerefos, C AF Godin-Beekmann, Sophie Petropavloskikh, Irina Reis, Stefan Newman, Paul Steinbrecht, Wolfgang Rex, Markus Santee, Michelle L. Eckman, Richard S. Zheng, Xiandong Tully, Matthew B. Stevenson, David S. Young, Paul Pyle, John Weber, Mark Tamminen, Johanna Mills, Gina Bais, Alkis F. Heaviside, Clare Zerefos, Christos TI The Quadrennial Ozone Symposium 2016 SO ADVANCES IN ATMOSPHERIC SCIENCES LA English DT Editorial Material C1 [Godin-Beekmann, Sophie] Univ Versailles St Quentin En Yvelines, CNRS, Observ Versailles St Quentin En Yvelines, F-78280 Guyancourt, France. [Petropavloskikh, Irina] Univ Colorado, CIRES, Boulder, CO 80309 USA. [Reis, Stefan] NERC Ctr Ecol & Hydrol, Edinburgh EH26 0QB, Midlothian, Scotland. [Newman, Paul] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Steinbrecht, Wolfgang] Deutsch Wetterdienst, Hohenpeissenberg Meteorol Observ, D-82383 Hohenpeissenberg, Germany. [Rex, Markus] Alfred Wegener Inst, D-14401 Potsdam, Germany. [Santee, Michelle L.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Eckman, Richard S.] NASA Headquarters, Div Earth Sci, Washington, DC USA. [Zheng, Xiandong] Chinese Acad Meteorol Sci, Beijing 100081, Peoples R China. [Tully, Matthew B.] Bur Meteorol, Melbourne, Vic 3001, Australia. [Stevenson, David S.] Univ Edinburgh, Sch GeoSci, Edinburgh EH9 3FE, Midlothian, Scotland. [Young, Paul] Univ Lancaster, Lancaster Environm Ctr, Lancaster LA1 4YQ, England. [Pyle, John] Univ Cambridge, Dept Chem, Cambridge CB2 1EW, England. [Weber, Mark] Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany. [Tamminen, Johanna] Finnish Meteorol Inst, Earth Observat, FI-00101 Helsinki, Finland. [Mills, Gina] NERC Ctr Ecol & Hydrol, Bangor LL57 2UW, Gwynedd, Wales. [Bais, Alkis F.] Aristotle Univ Thessaloniki, ELKE AUTH, Thessaloniki, Greece. [Heaviside, Clare] Publ Hlth England, Ctr Radiat Chem & Environm Hazards, London, England. [Zerefos, Christos] Acad Athens, Res Ctr Atmospher Phys & Climatol, Athens 10680, Greece. [Reis, Stefan] Univ Exeter, Sch Med, Truro TR1 3HD, England. RP Godin-Beekmann, S (reprint author), Univ Versailles St Quentin En Yvelines, CNRS, Observ Versailles St Quentin En Yvelines, F-78280 Guyancourt, France. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SCIENCE PRESS PI BEIJING PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA SN 0256-1530 EI 1861-9533 J9 ADV ATMOS SCI JI Adv. Atmos. Sci. PD MAR PY 2017 VL 34 IS 3 BP 283 EP 288 DI 10.1007/s00376-016-6309-2 PG 6 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EM1WZ UT WOS:000395109200001 ER PT J AU Hirsch, LA Ciardi, DR Howard, AW Everett, ME Furlan, E Saylors, M Horch, EP Howell, SB Teske, J Marcy, GW AF Hirsch, Lea A. Ciardi, David R. Howard, Andrew W. Everett, Mark E. Furlan, Elise Saylors, Mindy Horch, Elliott P. Howell, Steve B. Teske, Johanna Marcy, Geoffrey W. TI Assessing the Effect of Stellar Companions from High-resolution Imaging of Kepler Objects of Interest SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: visual; planets and satellites: detection; planets and satellites: fundamental parameters; techniques: high angular resolution; techniques: photometric ID CANDIDATE HOST STARS; TRANSIT TIMING VARIATION; MULTIPLE-PLANET SYSTEMS; SOLAR-TYPE STARS; VALIDATION; RADII; AU; I.; METALLICITIES; CONFIRMATION AB We report on 176 close (< 2") stellar companions detected with high-resolution imaging near 170 hosts of Kepler Objects of Interest (KOIs). These Kepler targets were prioritized for imaging follow-up based on the presence of small planets, so most of the KOIs in these systems (176 out of 204) have nominal radii < 6 R-circle plus. Each KOI in our sample was observed in at least two filters with adaptive optics, speckle imaging, lucky imaging, or the Hubble Space Telescope. Multi-filter photometry provides color information on the companions, allowing us to constrain their stellar properties and assess the probability that the companions are physically bound. We find that 60%-80% of companions within 1" are bound, and the bound fraction is >90% for companions within 0" 5; the bound fraction decreases with increasing angular separation. This picture is consistent with simulations of the binary and background stellar populations in the Kepler field. We also reassess the planet radii in these systems, converting the observed differential magnitudes to a contamination in the Kepler bandpass and calculating the planet radius correction factor, X-R = R-p(true)/R-p(single). Under the assumption that planets in bound binaries are equally likely to orbit the primary or secondary, we find a mean radius correction factor for planets in stellar multiples of X-R = 1.65. If stellar multiplicity in the Kepler field is similar to the solar neighborhood, then nearly half of all Kepler planets may have radii underestimated by an average of 65%, unless vetted using high-resolution imaging or spectroscopy. C1 [Hirsch, Lea A.; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, 510 Campbell Hall, Berkeley, CA 94720 USA. [Ciardi, David R.; Saylors, Mindy] CALTECH, IPAC, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Howard, Andrew W.] CALTECH, Dept Astron, MC 249-17, Pasadena, CA 91125 USA. [Everett, Mark E.] Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA. [Furlan, Elise] CALTECH, IPAC, Mail Code 100-22,1200 E Calif Blvd, Pasadena, CA 91125 USA. [Teske, Johanna] Carnegie DTM, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. [Horch, Elliott P.] Southern Connecticut State Univ, Dept Phys, 501 Crescent St, New Haven, CT 06515 USA. [Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Saylors, Mindy] Coll Canyons, 26455 Rockwell Canyon Rd, Santa Clarita, CA 91355 USA. RP Hirsch, LA (reprint author), Univ Calif Berkeley, Dept Astron, 510 Campbell Hall, Berkeley, CA 94720 USA. EM lhirsch@berkeley.edu OI Furlan, Elise/0000-0001-9800-6248 FU Infrared Processing and Analysis Center's Visiting Graduate Student Fellowship at the California Institute of Technology FX We thank the anonymous referee for a thorough and detailed report and many helpful suggestions and comments. This project was begun during and partially funded by the Infrared Processing and Analysis Center's Visiting Graduate Student Fellowship at the California Institute of Technology. The authors would like to thank James Graham for useful discussions while working on this project. This research has made use of the NASA Exoplanet Archive and ExoFOP, which are operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. NR 40 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAR PY 2017 VL 153 IS 3 AR 117 DI 10.3847/1538-3881/153/3/117 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN2SX UT WOS:000395861500002 ER PT J AU Park, RS Folkner, WM Konopliv, AS Williams, JG Smith, DE Zuber, MT AF Park, Ryan S. Folkner, William M. Konopliv, Alexander S. Williams, James G. Smith, David E. Zuber, Maria T. TI Precession of Mercury's Perihelion from Ranging to the MESSENGER Spacecraft SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; celestial mechanics; ephemerides; planets and satellites: individual (Mercury); relativistic processes; Sun: interior ID GENERAL-RELATIVITY; GRAVITY-FIELD; TRACKING DATA; MISSION; MOTION; SYSTEM; ORBIT AB The perihelion of Mercury's orbit precesses due to perturbations from other solar system bodies, solar quadrupole moment (J(2)), and relativistic gravitational effects that are proportional to linear combinations of the parametrized post-Newtonian parameters beta and gamma. The orbits and masses of the solar system bodies are quite well known, and thus the uncertainty in recovering the precession rate of Mercury's perihelion is dominated by the uncertainties in the parameters J(2), beta, and gamma. Separating the effects due to these parameters is challenging since the secular precession rate has a linear dependence on each parameter. Here we use an analysis of radiometric range measurements to the MESSENGER (MErcury Surface, Space ENvironment, GEochemistry, and Ranging) spacecraft in orbit about Mercury to estimate the precession of Mercury's perihelion. We show that the MESSENGER ranging data allow us to measure not only the secular precession rate of Mercury's perihelion with substantially improved accuracy, but also the periodic perturbation in the argument of perihelion sensitive to beta and gamma. When combined with the gamma estimate from a Shapiro delay experiment from the Cassini mission, we can decouple the effects due to beta and J(2) and estimate both parameters, yielding (beta - 1)=(-2.7 +/- 3.9) x 10(-5) and J(2) =. (2.25 +/- 0.09) x 10(-7). We also estimate the total precession rate of Mercury's perihelion as 575.3100 +/- 0.0015 ''/century and provide estimated contributions and uncertainties due to various perturbing effects. C1 [Park, Ryan S.; Folkner, William M.; Konopliv, Alexander S.; Williams, James G.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. RP Park, RS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Ryan.S.Park@jpl.nasa.gov FU NASA/MESSENGER mission FX We thank the MESSENGER project for providing information regarding spacecraft activities. This research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. J.G.W. discussed secular and periodic relativistic terms for Mercury with J. Bootello. M.T.Z. and D.E.S. were supported by the NASA/MESSENGER mission, performed under contract from NASA to the Carnegie Institution of Washington and Columbia University. NR 44 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 MAR PY 2017 VL 153 IS 3 AR 121 DI 10.3847/1538-3881/aa5be2 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN3GF UT WOS:000395896300001 ER PT J AU Mylapilli, H Jain, A AF Mylapilli, Harshavardhan Jain, Abhinandan TI Complementarity Techniques for Minimal Coordinate Contact Dynamics SO JOURNAL OF COMPUTATIONAL AND NONLINEAR DYNAMICS LA English DT Article ID FRICTION AB In this paper, nonsmooth contact dynamics of articulated rigid multibody systems is formulated as a complementarity problem. Minimal coordinate (MC) formulation is used to derive the dynamic equations of motion as it provides significant computational cost benefits and leads to a smaller-sized complementarity problem when compared with the frequently used redundant coordinate (RC) formulation. Additionally, an operational space (OS) formulation is employed to take advantage of the low-order structure-based recursive algorithms that do not require mass matrix inversion, leading to a further reduction in these computational costs. Based on the accuracy with which Coulomb's friction cone is modeled, the complementarity problem can be posed either as a linear complementarity problem (LCP), where the friction cone is approximated using a polygon, or as a nonlinear complementarity problem (NCP), where the friction cone is modeled exactly. Both formulations are studied in this paper. These complementarity problems are further recast as nonsmooth unconstrained optimization problems, which are solved by employing a class of Levenberg-Marquardt (LM) algorithms. The necessary theory detailing these techniques is discussed and five solvers are implemented to solve contact dynamics problems. A simple test case of a sphere moving on a plane surface is used to validate these solvers for a single contact, whereas a 12-link complex pendulum example is chosen to compare the accuracy of the solvers for the case of multiple simultaneous contacts. The simulation results validate the MC-based NCP formulations developed in this paper. Moreover, we observe that the LCP solvers deliver accuracy comparable to that of the NCP solvers when the friction cone direction vectors in the contact tangent plane are aligned with the sliding contact velocity at each time step. The theory and simulation results show that the NCP approach can be seamlessly recast into an MC OS formulation, thus allowing for accurate modeling of frictional contacts, while at the same time reducing overall computational costs associated with contact and collision dynamics problems in articulated rigid body systems. C1 [Mylapilli, Harshavardhan] Univ Southern Calif, Dept Aerosp & Mech Engn, Los Angeles, CA 90089 USA. [Jain, Abhinandan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mylapilli, H (reprint author), Univ Southern Calif, Dept Aerosp & Mech Engn, Los Angeles, CA 90089 USA. EM mylapill@usc.edu; Abhinandan.Jain@jpl.nasa.gov NR 35 TC 0 Z9 0 U1 0 U2 0 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 1555-1423 EI 1555-1415 J9 J COMPUT NONLIN DYN JI J. Comput. Nonlinear Dyn. PD MAR PY 2017 VL 12 IS 2 SI SI AR 021004 DI 10.1115/1.4033520 PG 18 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA EM2XI UT WOS:000395178700005 ER PT J AU Guruswamy, GP AF Guruswamy, Guru P. TI Modeling of Oscillating Control Surfaces Using Overset-GridBased Navier-Stokes Equations Solver SO JOURNAL OF DYNAMIC SYSTEMS MEASUREMENT AND CONTROL-TRANSACTIONS OF THE ASME LA English DT Article ID COMPUTATIONS AB A modular procedure is presented to simulate moving control surfaces within an overset grid environment using the Navier-Stokes equations. Gaps are modeled by locally shearing the wing grids instead of using separate grids to model gaps. Grid movements for control surfaces are defined through a separate module, which is driven by an external grid generation tool. Results are demonstrated for a wing with a part-span control surface. Grids for the test case are determined from detailed grid sensitivity studies based on both nonoscillating and oscillating cases. Steady and, for the first time, unsteady pressures from overset grid computations are validated with wind tunnel data. This paper addresses the current needs of high-fidelity flow modeling to design advanced active-controls. C1 [Guruswamy, Guru P.] NASA Adv Supercomp Div, Computat Phys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Guruswamy, GP (reprint author), NASA Adv Supercomp Div, Computat Phys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. EM guru.p.guruswamy@nasa.gov FU NAS FX The author thanks Shishir Pandya, William Chan, and Henry Lee of NASA Ames Research Center (ARC) for providing help in using CGT grid tool. Consultations by Dennis Jespersen of NASA Advanced Super Computing Division (NAS) on parallel computing aspects of OVERFLOW were helpful. Terry Holst, CFD lead of Rotary wing (RW) project made valuable suggestions on grid refinement studies. This work was supported by RW and IRAD projects of NAS. NR 28 TC 0 Z9 0 U1 0 U2 0 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 0022-0434 EI 1528-9028 J9 J DYN SYST-T ASME JI J. Dyn. Syst. Meas. Control-Trans. ASME PD MAR PY 2017 VL 139 IS 3 AR 031005 DI 10.1115/1.4034945 PG 8 WC Automation & Control Systems; Instruments & Instrumentation SC Automation & Control Systems; Instruments & Instrumentation GA EM2BB UT WOS:000395120300005 ER PT J AU Schatzman, DM Thomas, FO AF Schatzman, D. M. Thomas, F. O. TI An experimental investigation of an unsteady adverse pressure gradient turbulent boundary layer: embedded shear layer scaling SO JOURNAL OF FLUID MECHANICS LA English DT Article DE turbulent boundary layers; turbulent flows ID DISCHARGE PLASMA ACTUATORS; FLOW-CONTROL; REYNOLDS STRESS; CONVEX SURFACE; SEPARATION; WALL; DELAY AB An experimental investigation of an unsteady adverse pressure gradient turbulent boundary layer is described. It is demonstrated that the local flow physics is largely dominated by an inflectional instability which gives rise to an embedded shear layer contained within the boundary layer. Experimental measurements are presented which are fully consistent with the presence of clockwise spanwise-oriented coherent vorticity within the embedded shear layer. Using embedded shear layer scaling parameters in the form of the shear layer vorticity thickness and the velocity defect at the upper inflection point, both the mean and the phase-averaged boundary layer velocity profiles exhibit similarity in both space and time over a large wall-normal extent. In a similar manner, the profiles of the streamwise-component turbulence intensity and Reynolds stress also exhibit similarity when scaled with the embedded shear layer parameters. The embedded shear layer scaling of previously published adverse pressure gradient turbulent boundary layer measurements confirms its generic applicability in a wide range of flow-field geometries and extending to high Reynolds numbers. C1 [Schatzman, D. M.] US Army Aero Flight Dynam Directorate, Ames Res Ctr, Moffett Field, CA 94035 USA. [Thomas, F. O.] Univ Notre Dame, Insti Flow Phys & Control, Notre Dame, IN 46556 USA. RP Thomas, FO (reprint author), Univ Notre Dame, Insti Flow Phys & Control, Notre Dame, IN 46556 USA. EM fthomas@nd.edu FU US Army Research Office [W911NF-07-1-0122] FX The authors would like to recognize the support of the US Army Research Office under grant W911NF-07-1-0122 monitored by T. Doligalski. NR 54 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-1120 EI 1469-7645 J9 J FLUID MECH JI J. Fluid Mech. PD MAR PY 2017 VL 815 BP 592 EP 642 DI 10.1017/jfm.2017.65 PG 51 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA EM6MJ UT WOS:000395426400023 ER PT J AU Scott, CJ Ozimek, MT Haapala, AF Siddique, FE Buffington, BB AF Scott, Christopher J. Ozimek, Martin T. Haapala, Amanda F. Siddique, Fazle E. Buffington, Brent B. TI Dual Satellite-Aided Planetary Capture with Interplanetary Trajectory Constraints SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID BROAD-SEARCH ALGORITHMS; TRIPLE FLYBY SEQUENCES; LAPLACE RESONANCE; GANYMEDE; DESIGN; JUPITER AB The system entry problem entails the capture of a spacecraft about a planet by way of propulsive maneuver(s) or flyby(s) of a planetary satellite(s), or both. In the case of the Jovian system, a balance is sought between the interplanetary time-of-flight, orbit insertion maneuver magnitude, mass delivered to the system, capture orbit period, radiation dose, and mission complexity. Based on a nominal asymptote, this paper introduces the analytical equations necessary to solve the phase-free, singly aided and doubly aided capture problems, with a focus on the doubly aided capture problem in the Jovian system. An analytical approximation for the required phasing is derived and the implications of the Laplace resonance are discussed. Analytical approximations are used to seamlessly seed a multiple-shooting algorithm in order to arrive at the converged high-fidelity solution space for the Europa Mission. C1 [Scott, Christopher J.; Ozimek, Martin T.; Haapala, Amanda F.; Siddique, Fazle E.] Johns Hopkins Univ, Appl Phys Lab, Space Explorat Sector, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. [Buffington, Brent B.] CALTECH, Jet Prop Lab, Outer Planet Miss Anal Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Scott, CJ (reprint author), Johns Hopkins Univ, Appl Phys Lab, Space Explorat Sector, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. NR 19 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 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD MAR PY 2017 VL 40 IS 3 BP 548 EP 562 DI 10.2514/1.G002102 PG 15 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA EN1GA UT WOS:000395757300005 ER PT J AU Sanmartin, JR Charro, M Garrett, HB Sanchez-Arriaga, G Sanchez-Torres, A AF Sanmartin, Juan R. Charro, Mario Garrett, Henry B. Sanchez-Arriaga, Gonzalo Sanchez-Torres, Antonio TI Analysis of Tether-Mission Concept for Multiple Flybys of Moon Europa SO JOURNAL OF PROPULSION AND POWER LA English DT Article ID JUPITER AB All four giant planets, far from the Earth and sun and having deep gravitational wells, present propulsion and power mission issues, but they also have an ambient plasma and magnetic field that allows for a common mission concept. Electrodynamic tethers can provide propellantless drag for planetary capture and operation down the gravitational well, and they can generate power to use along with or be stored for inverting tether current. The design for an alternative to NASA's proposed Europa mission is presented here. The operation requires the spacecraft to pass repeatedly near Jupiter, for greater plasma density and magnetic field, raising a radiation-dose issue that past analyses did take into account; tape tethers tens of kilometers long and tens of micrometers thick, for greater operation efficiency, are considered. This might result, however, in attracted electrons reaching the tape with a penetration range that exceeds tape thickness, thereby escaping collection. The mission design requires keeping the range below thickness throughout, resulting in an orbit perijove only hundreds of kilometers above Jupiter and tapes a few kilometers long. A somewhat similar mission design might apply to other giant outer planets. C1 [Sanmartin, Juan R.; Charro, Mario] Univ Politecn Madrid, Sch Aerosp Engn, Dept Appl Phys, Plaza Cardenal Cisneros 3, Madrid 28040, Spain. [Garrett, Henry B.] CALTECH, Jet Prop Lab, Reliabil Engn & Mission Environm Assurance Off, 4800 Oak Grove Drive, Pasadena, CA 91109 USA. [Sanchez-Arriaga, Gonzalo; Sanchez-Torres, Antonio] Univ Carlos III Madrid, Dept Bioengn & Aerosp Engn, Ave Univ 30, Leganes 28911, Spain. RP Sanmartin, JR (reprint author), Univ Politecn Madrid, Sch Aerosp Engn, Dept Appl Phys, Plaza Cardenal Cisneros 3, Madrid 28040, Spain. RI SANCHEZ-ARRIAGA, GONZALO/L-4227-2014 OI SANCHEZ-ARRIAGA, GONZALO/0000-0002-8122-4051 FU Ministerio de Economia y Competitividad of Spain [RYC-2014-15357, FJCI-2014-20291] FX Work by G. Sanchez-Arriaga was supported by the Ministerio de Economia y Competitividad of Spain (grant no. RYC-2014-15357). Work by A. Sanchez-Torres was partially supported by the Ministerio de Economia y Competitividad of Spain (grant no. FJCI-2014-20291). The authors acknowledge helpful comments and criticism by the Reviewers and the Associate Editor. The research described in this paper by H. Garrett was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. The authors acknowledge helpful comments and criticism by the Reviewers and the Associate Editor. NR 16 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 0748-4658 EI 1533-3876 J9 J PROPUL POWER JI J. Propul. Power PD MAR PY 2017 VL 33 IS 2 BP 338 EP 342 DI 10.2514/1.B36205 PG 5 WC Engineering, Aerospace SC Engineering GA EN1AE UT WOS:000395741800006 ER PT J AU Thompson, MS Zega, TJ Howe, JY AF Thompson, Michelle S. Zega, Thomas J. Howe, Jane Y. TI In situ experimental formation and growth of Fe nanoparticles and vesicles in lunar soil SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID IRON OXIDATION-STATES; LASER IRRADIATION; SPACE; MINERALS; REGOLITH; SURFACE; PARTICLES; RIMS AB We report the results of the first dynamic, in situ heating of lunar soils to simulate micrometeorite impacts on the lunar surface. We performed slow-and rapid-heating experiments inside the transmission electron microscope to understand the chemical and microstructural changes in surface soils resulting from space-weathering processes. Our slow-heating experiments show that the formation of Fe nanoparticles begins at similar to 575 degrees C. These nanoparticles also form as a result of rapid-heating experiments, and electron energyloss spectroscopy measurements indicate the Fe nanoparticles are composed entirely of Fe-0, suggesting this simulation accurately mimics micrometeorite space-weathering processes occurring on airless body surfaces. In addition to Fe nanoparticles, rapid-heating experiments also formed vesiculated textures in the samples. Several grains were subjected to repeated thermal shocks, and the measured size distribution and number of Fe nanoparticles evolved with each subsequent heating event. These results provide insight into the formation and growth mechanisms for Fe nanoparticles in space-weathered soils and could provide a new methodology for relative age dating of individual soil grains from within a sample population. C1 [Thompson, Michelle S.; Zega, Thomas J.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Thompson, Michelle S.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Howe, Jane Y.] Hitachi High Technol Canada Inc, Rexdale, ON M9W 6A4, Canada. [Howe, Jane Y.] Univ Toronto, Dept Mat Sci & Engn, Toronto, ON M5S 1A1, Canada. RP Thompson, MS (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.; Thompson, MS (reprint author), NASA, Johnson Space Ctr, Houston, TX 77058 USA. EM mst@lpl.arizona.edu FU NASA Earth and Space Science Fellowship (NESSF); NASA FX We thank CAPTEM for allocation of lunar samples for this study. We gratefully acknowledge the use of facilities within the LeRoy Eyring Center for Solid State Science at Arizona State University, with assistance from Dr. Zhaofeng Gan. We gratefully acknowledge the use of facilities in the Ontario Centre for the Characterization of Advanced Materials and Dr. Doug Perovic at the University of Toronto for making this project possible. The authors thank reviewers H. Ishii and J. Cahill, and AE C. Pieters for constructive reviews which improved the manuscript. Funding for M.S. Thompson is provided by the NASA Earth and Space Science Fellowship (NESSF). Research supported, in part, by NASA. NR 37 TC 0 Z9 0 U1 0 U2 0 PU WILEY 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 MAR PY 2017 VL 52 IS 3 BP 413 EP 427 DI 10.1111/maps.12798 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EO6SZ UT WOS:000396824100001 ER PT J AU Hartmann, WK Daubar, IJ AF Hartmann, W. K. Daubar, I. J. TI Martian cratering 11. Utilizing decameter scale crater populations to study Martian history SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID SATURATION EQUILIBRIUM; IMPACT CRATERS; HIGH OBLIQUITY; MARS; LUNAR; SURFACE; CHRONOLOGY; MORPHOLOGY; VOLCANISM; METEORITE AB New information has been obtained in recent years regarding formation rates and the production size-frequency distribution (PSFD) of decameter-scale primary Martian craters formed during recent orbiter missions. Here we compare the PSFD of the currently forming small primaries (P) with new data on the PSFD of the total small crater population that includes primaries and field secondaries (P + fS), which represents an average over longer time periods. The two data sets, if used in a combined manner, have extraordinary potential for clarifying not only the evolutionary history and resurfacing episodes of small Martian geological formations (as small as one or few km 2) but also possible episodes of recent climatic change. In response to recent discussions of statistical methodologies, we point out that crater counts do not produce idealized statistics, and that inherent uncertainties limit improvements that can be made by more sophisticated statistical analyses. We propose three mutually supportive procedures for interpreting crater counts of small craters in this context. Applications of these procedures support suggestions that topographic features in upper meters of mid-latitude ice-rich areas date only from the last few periods of extreme Martian obliquity, and associated predicted climate excursions. C1 [Hartmann, W. K.] Planetary Sci Inst, 1700 E Ft Lowell Rd,Suite 106, Tucson, AZ 85719 USA. [Daubar, I. J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Hartmann, WK (reprint author), Planetary Sci Inst, 1700 E Ft Lowell Rd,Suite 106, Tucson, AZ 85719 USA. EM hartmann@psi.edu FU International Space Science Institute (ISSI) in Bern, Switzerland; Mars Data Analysis Program (MDAP) grant from NASA [NNX10AO24G] FX WKH thanks the International Space Science Institute (ISSI) in Bern, Switzerland, for supporting various stages of this work. WKH's initial measurements of the primary production SFD were supported by a Mars Data Analysis Program (MDAP) grant (NNX10AO24G) from NASA, and done in collaboration with Stephanie Werner, Cathy Quantin, and Olga Popova as part of a larger ISSI project on small Martian craters (Werner et al. 2015). A portion of IJD's research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We thank Elaine Owens and Emily Joseph at the Planetary Science Institute for invaluable help with editing, software issues, and submission of our paper. NR 60 TC 0 Z9 0 U1 0 U2 0 PU WILEY 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 MAR PY 2017 VL 52 IS 3 BP 493 EP 510 DI 10.1111/maps.12807 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EO6SZ UT WOS:000396824100007 ER PT J AU Cuzzi, JN Olson, DM AF Cuzzi, Jeffrey N. Olson, Daniel M. TI Recovering 3D particle size distributions from 2D sections SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID GENERAL SPHEROID PROBLEM; FREQUENCY-DISTRIBUTIONS; SHAPE DISTRIBUTIONS; ORDINARY CHONDRITES; MASS-DISTRIBUTION; CHONDRULES; MODEL AB We discuss different ways to convert observed, apparent particle size distributions from 2D sections (thin sections, SEM maps on planar surfaces, etc.) into true 3D particle size distributions. We give a simple, flexible, and practical method to do this; show which of these techniques gives the most faithful conversions; and provide (online) short computer codes to calculate both 2D-3D recoveries and simulations of 2D observations by random sectioning. The most important systematic bias of 2D sectioning, from the standpoint of most chondrite studies, is an overestimate of the abundance of the larger particles. We show that fairly good recoveries can be achieved from observed size distributions containing 100300 individual measurements of apparent particle diameter. C1 [Cuzzi, Jeffrey N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Olson, Daniel M.] BAERI Inc, Petaluma, CA 94952 USA. RP Cuzzi, JN (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM jeffrey.cuzzi@nasa.gov FU NASA's Origins of Solar Systems Program FX We are grateful to Quentin Williams for pointing out the work of Cruz-Orive; to Don Eisenhour, Michael Enfield and Wuwei Liang for helpful conversations; and to Seth Teitler for pointing out a notational error which rippled through the paper. Jon Friedrich and Derek Sears provided internal reviews that improved the paper; Justin Simon and Denton Ebel also provided useful feedback. We also thank Jon Friedrich for his very thorough journal review that included actually smoke-testing the fortran codes, as well as Michael Cato at JSC, who retested them based on newly written documentation and added useful comments to the documentation. We acknowledge the invaluable support of the Ames Research Center Research Library staff, in particular Dan Pappas and Kathy Ponce, for helping us locate and acquire diverse reference materials. This kind of expert information access and retrieval is essential to a person working out of their narrow discipline, even in an age when supposedly "everything is online." This work was supported by NASA's Origins of Solar Systems Program. NR 25 TC 0 Z9 0 U1 0 U2 0 PU WILEY 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 MAR PY 2017 VL 52 IS 3 BP 532 EP 545 DI 10.1111/maps.12812-2531 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EO6SZ UT WOS:000396824100010 ER PT J AU Waszczak, A Prince, TA Laher, R Masci, F Bue, B Rebbapragada, U Barlow, T Surace, J Helou, G Kulkarni, S AF Waszczak, Adam Prince, Thomas A. Laher, Russ Masci, Frank Bue, Brian Rebbapragada, Umaa Barlow, Tom Surace, Jason Helou, George Kulkarni, Shrinivas TI Small Near-Earth Asteroids in the Palomar Transient Factory Survey: a Real-Time Streak-detection System SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE minor planets; asteroids: general ID PERIODIC VARIABLE-STARS; PAN-STARRS; AUTOMATED CLASSIFICATION; ROTATION PERIODS; LIGHT CURVES; POPULATION; DISCOVERY; TELESCOPE; REDSHIFT; CALIBRATION AB Near-Earth asteroids (NEAs) in the 1-100 meter size range are estimated to be similar to 1,000 times more numerous than the similar to 15,000 currently cataloged NEAs, most of which are in the 0.5-10 kilometer size range. Impacts from 10-100 meter size NEAs are not statistically life-threatening, but may cause significant regional damage, while 1-10 meter size NEAs with low velocities relative to Earth are compelling targets for space missions. We describe the implementation and initial results of a real-time NEA-discovery system specialized for the detection of small, high angular rate (visually streaked) NEAs in Palomar Transient Factory (PTF) images. PTF is a 1.2-m aperture, 7.3 deg(2) field of view (FOV) optical survey designed primarily for the discovery of extragalactic transients (e.g., supernovae) in 60-second exposures reaching similar to 20.5 visual magnitude. Our real-time NEA discovery pipeline uses a machine-learned classifier to filter a large number of false-positive streak detections, permitting a human scanner to efficiently and remotely identify real asteroid streaks during the night. Upon recognition of a streaked NEA detection (typically within an hour of the discovery exposure), the scanner triggers follow-up with the same telescope and posts the observations to the Minor Planet Center for worldwide confirmation. We describe our 11 initial confirmed discoveries, all small NEAs that passed 0.3-15 lunar distances from Earth. Lastly, we derive useful scaling laws for comparing streaked-NEA-detection capabilities of different surveys as a function of their hardware and survey-pattern characteristics. This work most directly informs estimates of the streak-detection capabilities of the Zwicky Transient Facility (ZTF, planned to succeed PTF in 2017), which will apply PTF's current resolution and sensitivity over a 47-deg(2) FOV. C1 [Waszczak, Adam] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Prince, Thomas A.; Barlow, Tom; Kulkarni, Shrinivas] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Laher, Russ; Surace, Jason] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Masci, Frank; Helou, George] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Bue, Brian; Rebbapragada, Umaa] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Prince, TA (reprint author), CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. EM prince@caltech.edu NR 81 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD MAR 1 PY 2017 VL 129 IS 973 BP 1 EP 25 AR 034402 DI 10.1088/1538-3873/129/973/034402 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN0NX UT WOS:000395707800001 ER PT J AU Kharuk, VI Im, ST Petrov, IA Dvinskaya, ML Fedotova, EV Ranson, KJ AF Kharuk, Viacheslav I. Im, Sergei T. Petrov, Ilya A. Dvinskaya, Mariya L. Fedotova, Elena V. Ranson, Kenneth J. TI Fir decline and mortality in the southern Siberian Mountains SO REGIONAL ENVIRONMENTAL CHANGE LA English DT Article DE Abies sibirica; Climate-induced tree mortality; Conifer mortality; Water stress; Climate change; Drought; Forest die-off; Tree pathogens ID NATIONAL-PARK; DROUGHT; FORESTS; ADAPTATION AB Increased dieback and mortality of ``dark needle conifer'' (DNC) stands (composed of fir (Abies sibirica), Siberian pine (Pinus sibirica) and spruce (Picea obovata)) were documented in Russia during recent decades. Here we analyzed spatial and temporal patterns of fir decline and mortality in the southern Siberian Mountains based on satellite, in situ and dendrochronological data. The studied stands are located within the boundary between DNC taiga to the north and forest-steppe to the south. Fir decline and mortality were observed to originate where topographic features contributed to maximal water-stress risk, i.e., steep (18 degrees - 25 degrees), convex, south-facing slopes with a shallow well-drained root zone. Fir regeneration survived droughts and increased stem radial growth, while upper canopy trees died. Tree ring width (TRW) growth negatively correlated with vapor pressure deficit (VPD), drought index and occurrence of late frosts, and positively with soil water content. Previous year growth conditions (i.e., drought index, VPD, soil water anomalies) have a high impact on current TRW (r = 0.60-0.74). Fir mortality was induced by increased water stress and severe droughts (as a primary factor) in synergy with bark-beetles and fungi attacks (as secondary factors). Dendrochronology data indicated that fir mortality is a periodic process. In a future climate with increased aridity and drought frequency, fir (and Siberian pine) may disappear from portions of its current range (primarily within the boundary with the foreststeppe) and is likely to be replaced by drought-tolerant species such as Pinus sylvestris and Larix sibirica. C1 [Kharuk, Viacheslav I.; Im, Sergei T.; Petrov, Ilya A.; Dvinskaya, Mariya L.; Fedotova, Elena V.] Sukachev Inst Forest, Krasnoyarsk, Russia. [Kharuk, Viacheslav I.; Im, Sergei T.; Fedotova, Elena V.] Siberian Fed Univ, Krasnoyarsk, Russia. [Im, Sergei T.] Siberian State Aerosp Univ, Krasnoyarsk, Russia. [Ranson, Kenneth J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kharuk, VI (reprint author), Sukachev Inst Forest, Krasnoyarsk, Russia.; Kharuk, VI (reprint author), Siberian Fed Univ, Krasnoyarsk, Russia. EM kharuk@ksc.krasn.ru; stim@ksc.krasn.ru; mizrail0412@mail.ru; mary_dvi@ksc.krasn.ru; elfed@ksc.krasn.ru; kenneth.j.ranson@nasa.gov FU Russian Science Fund (RNF) [14-24-00112]; NASA's Terrestrial Ecology Program FX This study was supported by Russian Science Fund (RNF) (Grant No. 14-24-00112). K. J. Ranson's contribution was supported in part by the NASA's Terrestrial Ecology Program. NR 44 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1436-3798 EI 1436-378X J9 REG ENVIRON CHANGE JI Reg. Envir. Chang. PD MAR PY 2017 VL 17 IS 3 BP 803 EP 812 DI 10.1007/s10113-016-1073-5 PG 10 WC Environmental Sciences; Environmental Studies SC Environmental Sciences & Ecology GA EM0EG UT WOS:000394991000015 ER PT J AU Scheidler, JJ Asnani, VM AF Scheidler, Justin J. Asnani, Vivake M. TI Validated linear dynamic model of electrically-shunted magnetostrictive transducers with application to structural vibration control SO SMART MATERIALS AND STRUCTURES LA English DT Article DE magnetostrictive materials; vibration control; shunt damping; stiffness tuning; piezoelectric materials ID TERFENOL-D; ALLOYS; ABSORBER; CIRCUITS AB This paper presents a linear model of the fully-coupled electromechanical behavior of a generally-shunted magnetostrictive transducer. The impedance and admittance representations of the model are reported. The model is used to derive the effect of the shunt's electrical impedance on the storage modulus and loss factor of the transducer without neglecting the inherent resistance of the transducer's coil. The expressions are normalized and then shown to also represent generally-shunted piezoelectric materials that have a finite leakage resistance. The generalized expressions are simplified for three shunts: resistive, series resistive-capacitive, and inductive, which are considered for shunt damping, resonant shunt damping, and stiffness tuning, respectively. For each shunt, the storage modulus and loss factor are plotted for a wide range of the normalized parameters. Then, important trends and their impact on different applications are discussed. An experimental validation of the transducer model is presented for the case of resistive and resonant shunts. The model closely predicts the measured response for a variety of operating conditions. This paper also introduces a model for the dynamic compliance of a vibrating structure that is coupled to a magnetostrictive transducer for shunt damping and resonant shunt damping applications. This compliance is normalized and then shown to be analogous to that of a structure that is coupled to a piezoelectric material. The derived analogies allow for the observations and equations in the existing literature on structural vibration control using shunted piezoelectric materials C1 [Scheidler, Justin J.; Asnani, Vivake M.] NASA, Rotating & Drive Syst Branch, Mat & Struct Div, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Scheidler, JJ (reprint author), NASA, Rotating & Drive Syst Branch, Mat & Struct Div, Glenn Res Ctr, Cleveland, OH 44135 USA. EM justin.j.scheidler@nasa.gov; vivake.m.asnani@nasa.gov FU NASA's Revolutionary Vertical Lift Technology (RVLT) Project [NNC13BA10B] FX This work was supported by NASA's Revolutionary Vertical Lift Technology (RVLT) Project (contract # NNC13BA10B). NR 38 TC 0 Z9 0 U1 0 U2 0 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 MAR PY 2017 VL 26 IS 3 AR 035057 DI 10.1088/1361-665X/aa5c48 PG 17 WC Instruments & Instrumentation; Materials Science, Multidisciplinary SC Instruments & Instrumentation; Materials Science GA EN3XR UT WOS:000395941700003 ER PT J AU Jenett, B Calisch, S Cellucci, D Cramer, N Gershenfeld, N Swei, S Cheung, KC AF Jenett, Benjamin Calisch, Sam Cellucci, Daniel Cramer, Nick Gershenfeld, Neil Swei, Sean Cheung, Kenneth C. TI Digital Morphing Wing: Active Wing Shaping Concept Using Composite Lattice-Based Cellular Structures SO SOFT ROBOTICS LA English DT Article DE discrete reconfigurable lattice assembly; morphing aerostructure; ultralight elastomeric cellular solid ID SOFT; ROBOTS AB We describe an approach for the discrete and reversible assembly of tunable and actively deformable structures using modular building block parts for robotic applications. The primary technical challenge addressed by this work is the use of this method to design and fabricate low density, highly compliant robotic structures with spatially tuned stiffness. This approach offers a number of potential advantages over more conventional methods for constructing compliant robots. The discrete assembly reduces manufacturing complexity, as relatively simple parts can be batch-produced and joined to make complex structures. Global mechanical properties can be tuned based on sub-part ordering and geometry, because local stiffness and density can be independently set to a wide range of values and varied spatially. The structure's intrinsic modularity can significantly simplify analysis and simulation. Simple analytical models for the behavior of each building block type can be calibrated with empirical testing and synthesized into a highly accurate and computationally efficient model of the full compliant system. As a case study, we describe a modular and reversibly assembled wing that performs continuous span-wise twist deformation. It exhibits high performance aerodynamic characteristics, is lightweight and simple to fabricate and repair. The wing is constructed from discrete lattice elements, wherein the geometric and mechanical attributes of the building blocks determine the global mechanical properties of the wing. We describe the mechanical design and structural performance of the digital morphing wing, including their relationship to wind tunnel tests that suggest the ability to increase roll efficiency compared to a conventional rigid aileron system. We focus here on describing the approach to design, modeling, and construction as a generalizable approach for robotics that require very lightweight, tunable, and actively deformable structures. C1 [Jenett, Benjamin; Calisch, Sam; Gershenfeld, Neil] MIT, Ctr Bits & Atoms, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Cellucci, Daniel] Cornell Univ, Dept Mech Engn, Ithaca, NY USA. [Cramer, Nick] Univ Calif Santa Cruz, Dept Comp Engn, Santa Cruz, CA 95064 USA. [Swei, Sean; Cheung, Kenneth C.] NASA, Ames Res Ctr, MS 202-3, Moffett Field, CA 94035 USA. RP Cheung, KC (reprint author), NASA, Ames Res Ctr, MS 202-3, Moffett Field, CA 94035 USA. EM kenny@nasa.gov FU NASA Aeronautics Research Institute Team Seedling Program (Active Wing Shaping Control Concept Using Composite Lattice-based Cellular Materials); NASA ARMD Convergent Aeronautics Solutions Program (Mission Adaptive Digital Composite Aero-structures Technologies); NASA Space Technology Research Fellowship (NSTRF) Program; NASA grant [NNX14AG47A] FX The authors would like to acknowledge the efforts of the Langley Research Center Flight Dynamics Branch and the 12-Foot Wind Tunnel test team: Mike Fremeaux, Mark Croom, Mia Siochi, Wes Oneal, Clinton Duncan, Lee Pollard, Earl Harris, Sue Grafton, and Gary Wainwright, as well as the MIT AeroAstro Department, including Dick Perdichizzi with the MIT Wright Brothers Wind Tunnel. Funding for this work was provided by the NASA Aeronautics Research Institute Team Seedling Program (Active Wing Shaping Control Concept Using Composite Lattice-based Cellular Materials), including NASA grant NNX14AG47A, as well as the NASA ARMD Convergent Aeronautics Solutions Program (Mission Adaptive Digital Composite Aero-structures Technologies), and the NASA Space Technology Research Fellowship (NSTRF) Program. NR 42 TC 0 Z9 0 U1 1 U2 1 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 2169-5172 EI 2169-5180 J9 SOFT ROBOT JI Soft Robot. PD MAR PY 2017 VL 4 IS 1 BP 33 EP 48 DI 10.1089/soro.2016.0032 PG 16 WC Robotics SC Robotics GA EN1KI UT WOS:000395768500005 PM 28289574 ER PT J AU Yingst, RA Berger, J Cohen, BA Hynek, B Schmidt, ME AF Yingst, R. A. Berger, J. Cohen, B. A. Hynek, B. Schmidt, M. E. TI Determining best practices in reconnoitering sites for habitability potential on Mars using a semi-autonomous rover: A GeoHeuristic Operational Strategies Test SO ACTA ASTRONAUTICA LA English DT Article DE MER; Science operations; Rover; Analog field test ID MERIDIANI-PLANUM; BURNS FORMATION; MOON; EXPLORATION; SYSTEM AB We tested science operations strategies developed for use in remote mobile spacecraft missions, to determine whether reconnoitering a site of potential habitability prior to in-depth study (a walkabout-first strategy) can be a more efficient use of time and resources than the linear approach commonly used by planetary rover missions. Two field teams studied a sedimentary sequence in Utah to assess habitability potential. At each site one team commanded a human "rover" to execute observations and conducted data analysis and made follow-on decisions based solely on those observations. Another team followed the same traverse using traditional terrestrial field methods, and the results of the two teams were compared. Test results indicate that for a mission with goals similar to our field case, the walkabout-first strategy may save time and other mission resources, while improving science return. The approach enabled more informed choices and higher team confidence in choosing where to spend time and other consumable resources. The walkabout strategy may prove most efficient when many close sites must be triaged to a smaller subset for detailed study or sampling. This situation would arise when mission goals include finding, identifying, characterizing or sampling a specific material, feature or type of environment within a certain area. C1 [Yingst, R. A.] Planetary Sci Inst, 1700 E Ft Lowell,Suite 106, Tucson, AZ 85719 USA. [Berger, J.] Univ Western Ontario, Dept Earth Sci, London, ON N6A 5B7, Canada. [Cohen, B. A.] NASA, Marshall Space Flight Ctr, VP62,320 Sparkman Dr, Huntsville, AL 35805 USA. [Hynek, B.] Univ Colorado, Lab Atmospher & Space Phys & Geol Sci, 392 UCB, Boulder, CO 80309 USA. [Schmidt, M. E.] Brock Univ, Dept Earth Sci, St Catharines, ON L2S 3A1, Canada. RP Yingst, RA (reprint author), Planetary Sci Inst, 1700 E Ft Lowell,Suite 106, Tucson, AZ 85719 USA. EM yingst@psi.edu; jeffberger@cpsx.uwo.ca; barbara.a.cohen@nasa.gov; hynek@lasp.colorado.edu; mschmidt2@brocku.ca FU Moon and Mars Analog Mission Activities Program [NNG05GL66G] FX We gratefully acknowledge the efforts of field assistant Ross Nova, our "rover" for the field test. This research was supported through Moon and Mars Analog Mission Activities Program grant NNG05GL66G to RAY. NR 44 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD MAR PY 2017 VL 132 BP 268 EP 281 DI 10.1016/j.actaastro.2016.12.018 PG 14 WC Engineering, Aerospace SC Engineering GA EL5BH UT WOS:000394636100029 ER PT J AU Bray, C Cuisset, A Hindle, F Bocquet, R Mouret, G Drouin, BJ AF Bray, Cedric Cuisset, Arnaud Hindle, Francis Bocquet, Robin Mouret, Gael Drouin, Brian J. TI CH3D photomixing spectroscopy up to 2.5 THz: New set of rotational and dipole parameters, first THz self-broadening measurements SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE THz photomixing; Frequency-comb; Deuterated methane; Line positions; Dipole moment; Self-broadening coefficients ID HIGH-RESOLUTION SPECTROSCOPY; MULTISPECTRUM ANALYSIS; FITTING TECHNIQUE; ROOM-TEMPERATURE; COEFFICIENTS; SPECTRA; MOMENT; BAND; (CH3D)-C-12; STATE AB Several previously unmeasured transitions of (CH3D)-C-12 have been recorded by a terahertz photomixing continuous-wave spectrometer up to R-Q(10) branch at 2.5 THz. An improved set of rotational constants has been obtained utilizing a THz frequency metrology based on a frequency comb that achieved an averaged frequency position better than 150 kHz on more than fifty ground-state transitions. A detailed analysis of the measured line intensities was undertaken using the multispectrum fitting program and has resulted in a determination of new dipole moment parameters. Measurements at different pressures of the R-Q(7) transitions provide the first determination of self-broadening coefficients from pure rotational CH3D lines. The THz rotational measurements are consistent with IR rovibrational data but no significant vibrational dependence of self-broadening coefficient may be observed by comparison. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Bray, Cedric; Cuisset, Arnaud; Hindle, Francis; Bocquet, Robin; Mouret, Gael] Univ Littoral Cote dOpale, Lab Physicochim Atmosphere, EA 4493, F-59140 Dunkerque, France. [Drouin, Brian J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Bray, C (reprint author), Univ Littoral Cote dOpale, Lab Physicochim Atmosphere, EA 4493, F-59140 Dunkerque, France. EM cedric.bray@univ-littoral.fr FU Institut de Recherche en Environnement Industriel (IRENI); European Commission via the Interreg IVA-2seas (Clean tech Project); Region ''Hauts de France''; Ministere de l'Enseignement Superieur et de la Recherche (CPER Climibio); European Fund for Regional Economic Development; National Aeronautics and Space Administration FX The photomixing CW-THz spectrometer has been funded both by the Institut de Recherche en Environnement Industriel (IRENI) and the European Commission via the Interreg IVA-2seas (Clean tech Project). C.B. acknowledges the Region ''Hauts de France'' and the Ministere de l'Enseignement Superieur et de la Recherche (CPER Climibio), and the European Fund for Regional Economic Development, for their financial support. Portions of the research described in this paper were performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration, government sponsorship acknowledged. NR 42 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 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD MAR PY 2017 VL 189 BP 198 EP 205 DI 10.1016/j.jqsrt.2016.11.011 PG 8 WC Optics; Spectroscopy SC Optics; Spectroscopy GA EK6UJ UT WOS:000394060900020 ER PT J AU Anjomani, Z Hanu, AR Prestwich, WV Byun, SH AF Anjomani, Z. Hanu, A. R. Prestwich, W. V. Byun, S. H. TI Development of a multi-element microdosimetric detector based on a thick gas electron multiplier SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article DE Tissue equivalent proportional counter; Thick gas electron multiplier; Microdosimetry; Multi-element detector ID EQUIVALENT PROPORTIONAL-COUNTERS; RADIATION PROTECTION DOSIMETRY; GEM; OPERATION; TEPC; IONIZATION; DESIGN AB A prototype multi-element gaseous microdosimetric detector was developed using the Thick Gas Electron Multiplier (THGEM) technique. The detector aims at measuring neutron and gamma-ray dose rates for weak neutron-gamma radiation fields. The multi element design was employed to increase the neutron detection efficiency. The prototype THGEM multi element detector consists of three layers of tissue equivalent plastic hexagons and each layer houses a hexagonal array of seven cylindrical gas cavity elements with equal heights and diameters of 17 mm. The final detector structure incorporates 21 gaseous volumes. Owing to the absence of wire electrodes, the THGEM multi element detector offers flexible and convenient fabrication. The detector responses to neutron and gamma ray were investigated using the McMaster Tandetron Li-7(p,n) neutron source. The dosimetric performance of the detector is presented in contrast to the response of a commercial tissue equivalent proportional counter. Compared to the standard TEPC response, the detector gave a consistent microdosimetric response with an average discrepancy of 8 % in measured neutron absorbed dose. An improvement of a factor of 3.0 in neutron detection efficiency has been accomplished with only a small degradation in energy resolution. However, its low energy cut off is about 6 keV/mu m, which is not sufficient to measure the gamma ray dose. This problem will be addressed by increasing the electron multiplication gain using double THGEM layers. C1 [Anjomani, Z.; Prestwich, W. V.; Byun, S. H.] McMaster Univ, Dept Med Phys & Appl Radiat Sci, Hamilton, ON L8S 4K1, Canada. [Hanu, A. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Anjomani, Z (reprint author), McMaster Univ, Dept Med Phys & Appl Radiat Sci, Hamilton, ON L8S 4K1, Canada. EM anjomaz@mcmaster.ca FU Natural Sciences and Engineering Research Council of Canada [CRDPJ 484381-15] FX This work has received support from the Natural Sciences and Engineering Research Council of Canada (Grant no. CRDPJ 484381-15) through research grants to S.H.B. NR 35 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 EI 1872-9576 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD MAR 1 PY 2017 VL 847 BP 117 EP 124 DI 10.1016/j.nima.2016.11.051 PG 8 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA EL1QT UT WOS:000394396800017 ER PT J AU Ryan Bellmore, J Duda, JJ Craig, LS Greene, SL Torgersen, CE Collins, MJ Vittum, K AF Ryan Bellmore, J. Duda, Jeffrey J. Craig, Laura S. Greene, Samantha L. Torgersen, Christian E. Collins, Mathias J. Vittum, Katherine TI Status and trends of dam removal research in the United States SO WILEY INTERDISCIPLINARY REVIEWS-WATER LA English DT Review ID ELWHA RIVER; DECISION-MAKING; BASE-LINE; RESTORATION; WISCONSIN; SCIENCE; CHANNEL; WASHINGTON; RESPONSES; IMPACTS AB Aging infrastructure coupled with growing interest in river restoration has driven a dramatic increase in the practice of dam removal. With this increase, there has been a proliferation of studies that assess the physical and ecological responses of rivers to these removals. As more dams are considered for removal, scientific information from these dam-removal studies will increasingly be called upon to inform decisions about whether, and how best, to bring down dams. This raises a critical question: what is the current state of dam-removal science in the United States? To explore the status, trends, and characteristics of dam-removal research in the U.S., we searched the scientific literature and extracted basic information from studies on dam removal. Our literature review illustrates that although over 1200 dams have been removed in the U.S., fewer than 10% have been scientifically evaluated, and most of these studies were short in duration (<4 years) and had limited ( 1-2 years) or no pre-removal monitoring. The majority of studies focused on hydrologic and geomorphic responses to removal rather than biological and water-quality responses, and few studies were published on linkages between physical and ecological components. Our review illustrates the need for long-term, multidisciplinary case studies, with robust study designs, in order to anticipate the effects of dam removal and inform future decision making. Published 2016. This article is a U.S. Government work and is in the public domain in the USA. C1 [Ryan Bellmore, J.] USDA, Forest Serv, Pacific Northwest Res Stn, Juneau, AK 70124 USA. [Duda, Jeffrey J.; Vittum, Katherine] Western Fisheries Res Ctr, USGS, Seattle, WA USA. [Craig, Laura S.] Amer Rivers, Philadelphia, PA USA. [Greene, Samantha L.; Torgersen, Christian E.] Forest & Rangeland Ecosyst Sci Ctr, USGS, Seattle, WA USA. [Collins, Mathias J.] NOAA, Natl Marine Fisheries Serv, Gloucester, MA USA. RP Ryan Bellmore, J (reprint author), USDA, Forest Serv, Pacific Northwest Res Stn, Juneau, AK 70124 USA. EM jbellmore@fs.fed.us OI Collins, Mathias/0000-0003-4238-2038 FU U.S. Geological Survey's John Wesley Powell Center for Analysis and Synthesis FX This article was produced with support from the U.S. Geological Survey's John Wesley Powell Center for Analysis and Synthesis. We thank Amy East, Chris Magirl, Jim Evans, Kathryn Ronnenberg, Stuart Lane and two anonymous reviewers for their feedback on this manuscript, as well as our fellow Powell Center working group participants for their insights about dam removal and the many discussions that sustained this project. We also thank Jill Baron and Leah Colasuonno for logistical support at the Powell Center. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the U.S. Government, the authors, or their affiliations. NR 66 TC 0 Z9 0 U1 0 U2 0 PU WILEY PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2049-1948 J9 WIRES-WATER JI Wiley Interdiscip. Rev.-Water PD MAR-APR PY 2017 VL 4 IS 2 AR UNSP e1164 DI 10.1002/wat2.1164 PG 13 WC Water Resources SC Water Resources GA EL8XT UT WOS:000394904400001 ER PT J AU Fleisher, DH Condori, B Quiroz, R Alva, A Asseng, S Barreda, C Bindi, M Boote, KJ Ferrise, R Franke, AC Govindakrishnan, PM Harahagazwe, D Hoogenboom, G Kumar, SN Merante, P Nendel, C Olesen, JE Parker, PS Raes, D Raymundo, R Ruane, AC Stockle, C Supit, I Vanuytrecht, E Wolf, J Woli, P AF Fleisher, David H. Condori, Bruno Quiroz, Roberto Alva, Ashok Asseng, Senthold Barreda, Carolina Bindi, Marco Boote, Kenneth J. Ferrise, Roberto Franke, Angelinus C. Govindakrishnan, Panamanna M. Harahagazwe, Dieudonne Hoogenboom, Gerrit Kumar, Soora Naresh Merante, Paolo Nendel, Claas Olesen, Jorgen E. Parker, Phillip S. Raes, Dirk Raymundo, Rubi Ruane, Alex C. Stockle, Claudio Supit, Iwan Vanuytrecht, Eline Wolf, Joost Woli, Prem TI A potato model intercomparison across varying climates and productivity levels SO GLOBAL CHANGE BIOLOGY LA English DT Article DE climate change; crop modeling; model improvement; solanum tuberosum; uncertainty analysis; yield sensitivity ID SOLANUM-TUBEROSUM L.; ELEVATED CARBON-DIOXIDE; WATER-USE EFFICIENCY; GAS-EXCHANGE; SIMULATING IMPACTS; ATMOSPHERIC CO2; YIELD RESPONSE; CROP MODELS; GROWTH; TEMPERATURE AB A potato crop multimodel assessment was conducted to quantify variation among models and evaluate responses to climate change. Nine modeling groups simulated agronomic and climatic responses at low-input (Chinoli, Bolivia and Gisozi, Burundi)-and high-input (Jyndevad, Denmark and Washington, United States) management sites. Two calibration stages were explored, partial (P1), where experimental dry matter data were not provided, and full (P2). The median model ensemble response outperformed any single model in terms of replicating observed yield across all locations. Uncertainty in simulated yield decreased from 38% to 20% between P1 and P2. Model uncertainty increased with interannual variability, and predictions for all agronomic variables were significantly different from one model to another (P < 0.001). Uncertainty averaged 15% higher for low-vs. high-input sites, with larger differences observed for evapotranspiration (ET), nitrogen uptake, and water use efficiency as compared to dry matter. A minimum of five partial, or three full, calibrated models was required for an ensemble approach to keep variability below that of common field variation. Model variation was not influenced by change in carbon dioxide (C), but increased as much as 41% and 23% for yield and ET, respectively, as temperature (T) or rainfall (W) moved away from historical levels. Increases in T accounted for the highest amount of uncertainty, suggesting that methods and parameters for T sensitivity represent a considerable unknown among models. Using median model ensemble values, yield increased on average 6% per 100-ppm C, declined 4.6% per degrees C, and declined 2% for every 10% decrease in rainfall (for nonirrigated sites). Differences in predictions due to model representation of light utilization were significant (P < 0.01). These are the first reported results quantifying uncertainty for tuber/root crops and suggest modeling assessments of climate change impact on potato may be improved using an ensemble approach. C1 [Fleisher, David H.; Condori, Bruno] ARS, Crop Syst & Global Change Lab, USDA, Beltsville, MD 20705 USA. [Quiroz, Roberto; Barreda, Carolina] Int Potato Ctr, Prod Syst & Environm, Lima, Peru. [Alva, Ashok] Kuwait Inst Sci Res, Desert Agr & Ecosyst Program, Safat, Kuwait. [Asseng, Senthold; Boote, Kenneth J.; Hoogenboom, Gerrit; Raymundo, Rubi] Univ Florida, Agr & Biol Engn Dept, Gainesville, FL USA. [Bindi, Marco; Ferrise, Roberto; Merante, Paolo] Univ Florence, Dept Agrifood Prod & Environm Sci, Florence, Italy. [Franke, Angelinus C.] Univ Free State, Soil Crop & Climate Sci, Bloemfontein, South Africa. [Govindakrishnan, Panamanna M.] Cent Potato Res Inst, Shimla, India. [Harahagazwe, Dieudonne] Int Potato Ctr SSA, Prod Syst & Environm, Nairobi, Kenya. [Kumar, Soora Naresh] Indian Agr Res Inst, Ctr Environm Sci & Climate Resilient Agr, New Delhi, India. [Nendel, Claas; Parker, Phillip S.] Inst Landscape Syst Anal, Leibniz Ctr Agr Landscape Res, Muncheberg, Germany. [Olesen, Jorgen E.] Aarhus Univ, Dept Agroecol, Tjele, Denmark. [Raes, Dirk; Vanuytrecht, Eline] KU Leuven Univ, Dept Earth & Environm Sci, Leuven, Belgium. [Ruane, Alex C.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Stockle, Claudio] Washington State Univ, Biol Syst Engn, Pullman, WA 99164 USA. [Supit, Iwan] Wageningen Univ & Res Ctr, Earth Syst Sci & Climate Adapt Land Management, Wageningen, Netherlands. [Wolf, Joost] Wageningen Univ & Res Ctr, Plant Prod Syst, Wageningen, Netherlands. [Woli, Prem] Washington State Univ, AgWeatherNet Program, Pullman, WA 99164 USA. RP Fleisher, DH (reprint author), ARS, Crop Syst & Global Change Lab, USDA, Beltsville, MD 20705 USA. EM David.fleisher@ars.usda.gov NR 85 TC 0 Z9 0 U1 1 U2 1 PU WILEY PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1354-1013 EI 1365-2486 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD MAR PY 2017 VL 23 IS 3 BP 1258 EP 1281 DI 10.1111/gcb.13411 PG 24 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA EO6UZ UT WOS:000396829300024 PM 27387228 ER PT J AU Finley, AO Banerjee, S Zhou, YZ Cook, BD Babcock, C AF Finley, Andrew O. Banerjee, Sudipto Zhou, Yuzhen Cook, Bruce D. Babcock, Chad TI Joint hierarchical models for sparsely sampled high-dimensional LiDAR and forest variables SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Forest biomass; Uncertainty quantification; Functional analysis; Dimension reduction; Predictive process; Hierarchical models; Markov chain Monte Carlo ID SPATIAL REGRESSION-MODELS; COVARIANCE FUNCTIONS; INVENTORY; COMPLEX; MISSION; BIOMASS; GROWTH AB Recent advancements in remote sensing technology, specifically Light Detection and Ranging (LiDAR) sensors, provide the data needed to quantify forest characteristics at a fine spatial resolution over large geographic domains. From an inferential standpoint, there is interest in prediction and interpolation of the often sparsely sampled and spatially misaligned LiDAR signals and forest variables. We propose a fully process-based Bayesian hierarchical model for above ground biomass (AGB) and LiDAR signals. The process based framework offers richness in inferential capabilities, e.g., inference on the entire underlying processes instead of estimates only at pre-specified points. Key challenges we obviate include misalignment between the AGB observations and LiDAR signals and the high-dimensionality in the model emerging from LiDAR signals in conjunction with the large number of spatial locations. We offer simulation experiments to evaluate our proposed models and also apply them to a challenging dataset comprising LiDAR and spatially coinciding forest inventory variables collected on the Penobscot Experimental Forest (PEF), Maine. Our key substantive contributions include AGB data products with associated measures of uncertainty for the PEF and, more broadly, a methodology that should find use in a variety of current and upcoming forest variable mapping efforts using sparsely sampled remotely sensed high-dimensional data. (C) 2016 Elsevier Inc. All rights reserved. C1 [Finley, Andrew O.] Michigan State Univ, Dept Forestry, E Lansing, MI 48824 USA. [Banerjee, Sudipto] Univ Calif Los Angeles, Dept Biostat, Los Angeles, CA 90095 USA. [Zhou, Yuzhen] Univ Nebraska Lincoln, Dept Stat, Lincoln, NE 68583 USA. [Cook, Bruce D.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20742 USA. [Babcock, Chad] Univ Washington, Sch Environm & Forest Sci, Seattle, WA 98195 USA. RP Finley, AO (reprint author), Michigan State Univ, Dept Forestry, E Lansing, MI 48824 USA. FU National Science Foundation (NSF) [DMS-1513481, EF-1137309, EF-1241874, EF-1253225]; NASACarbon Monitoring System grants; NSF [DMS-1513654, IIS-1562303] FX Andrew Finley was supported by the National Science Foundation (NSF) DMS-1513481, EF-1137309, EF-1241874, and EF-1253225, as well as NASACarbon Monitoring System grants. Sudipto Banerjee was supported by NSF DMS-1513654 and IIS-1562303. NR 45 TC 0 Z9 0 U1 1 U2 1 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD MAR 1 PY 2017 VL 190 BP 149 EP 161 DI 10.1016/j.rse.2016.12.004 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA EL1RS UT WOS:000394399300012 ER PT J AU Jeong, SJ Schimel, D Frankenberg, C Drewry, DT Fisher, JB Verma, M Berry, JA Lee, JE Joiner, J AF Jeong, Su-Jong Schimel, David Frankenberg, Christian Drewry, Darren T. Fisher, Joshua B. Verma, Manish Berry, Joseph A. Lee, Jung-Eun Joiner, Joanna TI Application of satellite solar-induced chlorophyll fluorescence to understanding large-scale variations in vegetation phenology and function over northern high latitude forests SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Solar-induced chlorophyll fluorescence; SIF; NDVI; GPP; Phenology; Large-scale ID TEMPERATE DECIDUOUS FOREST; ATMOSPHERIC CO2; GROWING-SEASON; CLIMATE-CHANGE; PHOTOSYNTHETIC CAPACITY; TERRESTRIAL BIOSPHERE; SPRING PHENOLOGY; LEAF PHENOLOGY; CARBON FLUXES; EXCHANGE AB This study evaluates the large-scale seasonal phenology and physiology of vegetation over northern high latitude forests (40 degrees-55 degrees N) during spring and fall by using remote sensing of solar-induced chlorophyll fluorescence (SIF), normalized difference vegetation index (NDVI) and observation-based estimate of gross primary productivity (GPP) from 2009 to 2011. Based on GPP phenology estimation in GPP, the growing season determined by SIF time-series is shorter in length than the growing season length determined solely using NDVI. This is mainly due to the extended period of high NDVI values, as compared to SIF, by about 46 days (+/- 11 days), indicating a large-scale seasonal decoupling of physiological activity and changes in greenness in the fall. In addition to phenological timing, mean seasonal NDVI and SIF have different responses to temperature changes throughout the growing season. We observed that both NDVI and SIF linearly increased with temperature increases throughout the spring. However, in the fall, although NDVI linearly responded to temperature increases, SIF and GPP did not linearly increase with temperature increases, implying a seasonal hysteresis of SIF and GPP in response to temperature changes across boreal ecosystems throughout their growing season. Seasonal hysteresis of vegetation at large-scales is consistent with the known phenomena that light limits boreal forest ecosystem productivity in the fall. Our results suggest that continuing measurements from satellite remote sensing of both SIF and NDVI can help to understand the differences between, and information carried by, seasonal variations vegetation structure and greenness and physiology at large-scales across the critical boreal regions. (C) 2016 Elsevier Inc. All rights reserved. C1 [Jeong, Su-Jong; Schimel, David; Frankenberg, Christian; Drewry, Darren T.; Fisher, Joshua B.; Verma, Manish] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Berry, Joseph A.] Carnegie Inst Sci, Dept Global Ecol, 260 Panama St, Stanford, CA 94305 USA. [Lee, Jung-Eun] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Joiner, Joanna] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Drewry, Darren T.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90024 USA. [Jeong, Su-Jong] South Univ Sci & Technol, Sch Environm Sci & Engn, Shenzhen, Peoples R China. [Verma, Manish] Univ Michigan, Stat Comp & Analyt Res, Ann Arbor, MI 48109 USA. RP Jeong, SJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM waterbell77@gmail.com NR 71 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD MAR 1 PY 2017 VL 190 BP 178 EP 187 DI 10.1016/j.rse.2016.11.021 PG 10 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA EL1RS UT WOS:000394399300014 ER PT J AU Royer, A Roy, A Montpetit, B Saint-Jean-Rondeau, O Picard, G Brucker, L Langlois, A AF Royer, Alain Roy, Alexandre Montpetit, Benoit Saint-Jean-Rondeau, Olivier Picard, Ghislain Brucker, Ludovic Langlois, Alexandre TI Comparison of commonly-used microwave radiative transfer models for snow remote sensing SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Snow microwave-emission model; Snow microstructure; Radiative transfer model; Canada; Ground-based measurements; Brightness temperature ID WATER EQUIVALENT RETRIEVAL; EMISSION MODEL; DENSE MEDIA; BRIGHTNESS TEMPERATURE; GRAIN-SIZE; DOME C; LAYERED SNOWPACKS; SCATTERING; SURFACE; ANTARCTICA AB This paper reviews four commonly-used microwave radiative transfer models that take different electromagnetic approaches to simulate snow brightness temperature (T-B): the Dense Media Radiative Transfer - Multi-Layer model (DMRT-ML), the Dense Media Radiative Transfer - Quasi-Crystalline Approximation Mie scattering of Sticky spheres (DMRT-QMS), the Helsinki University of Technology n-Layers model (HUT-nlayers) and the Microwave Emission Model of Layered Snowpacks (MEMLS). Using the same extensively measured physical snow pack properties, we compared the simulated T-B at 11, 19 and 37 GHz from these four models. The analysis focuses on the impact of using different types of measured snow microstructure metrics in the simulations. In addition to density, snow microstructure is defined for each snow layer by grain optical diameter (Do) and stickiness for DMRT-ML and DMRT-QMS, mean grain geometrical maximum extent (Dmax) for HUT n-layers and the exponential correlation length for MEMLS. These metrics were derived from either in-situ measurements of snow specific surface area (SSA) or macrophotos of grain sizes (D-max), assuming non-sticky spheres for the DMRT models. Simulated T-B sensitivity analysis using the same inputs shows relatively consistent T-B behavior as a function of Do and density variations for the vertical polarization (maximum deviation of 18 K and 27 K, respectively), while some divergences appear in simulated variations for the polarization ratio (PR). Comparisons with ground based radiometric measurements show that the simulations based on snow SSA measurements have to be scaled with a model-specific factor of Do in order to minimize the root mean square error (RMSE) between measured and simulated T-B. Results using in-situ grain size measurements (SSA or D-max, depending on the model) give a mean T-B RMSE (19 and 37 GHz) of the order of 16-26 K, which is similar for all models when the snow microstructure metrics are scaled. However, the MEMLS model converges to better results when driven by the correlation length estimated from in-situ SSA measurements rather than D-max measurements. On a practical level, this paper shows that the SSA parameter, a snow property that is easy to retrieve in-situ, appears to be the most relevant parameter for characterizing snow microstructure, despite the need for a scaling factor. (C) 2017 Elsevier Inc. All rights reserved. C1 [Royer, Alain; Roy, Alexandre; Montpetit, Benoit; Saint-Jean-Rondeau, Olivier; Langlois, Alexandre] Univ Sherbrooke, Ctr Applicat & Rech Teledetect CARTEL, 2500 Boul Univ, Sherbrooke, PQ J1K 2R1, Canada. [Royer, Alain; Roy, Alexandre; Saint-Jean-Rondeau, Olivier; Langlois, Alexandre] Ctr & Etud Nord, Quebec City, PQ, Canada. [Picard, Ghislain] Univ Grenoble Alpes, CNRS, LGGE UMR5183, F-38041 Grenoble, France. [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, Columbia, MD 21046 USA. [Montpetit, Benoit] Environm & Climate Change Canada, Canadian Ice Serv, Ottawa, ON, Canada. RP Royer, A (reprint author), Univ Sherbrooke, Ctr Applicat & Rech Teledetect CARTEL, 2500 Boul Univ, Sherbrooke, PQ J1K 2R1, Canada. EM Alain.royer@usherbrooke.ca RI Brucker, Ludovic/A-8029-2010 OI Brucker, Ludovic/0000-0001-7102-8084 FU National Sciences and Engineering Research Council of Canada (NSERC); Canadian Foundation for Innovation; Programme de developpement de partenariats strategiques en matiere d'enseignement et de recherche of the Conseil franco-quebecois de la cooperation universitaire, a France-Quebec research collaboration; Environment Canada; NASA-Goddard FX This study was supported by the National Sciences and Engineering Research Council of Canada (NSERC), the Canadian Foundation for Innovation, Environment Canada, NASA-Goddard (L.B.) and by the Programme de developpement de partenariats strategiques en matiere d'enseignement et de recherche of the Conseil franco-quebecois de la cooperation universitaire, a France-Quebec research collaboration. The authors would like to thank Patrick Cliche and Miroslav Chum for creating the Shadow-box, all participants to the field works for their contributions to obtain the ground-based measurements, and Peter Toose and Chris Derksen (Environment Canada) for providing part of the Churchill data. NR 67 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD MAR 1 PY 2017 VL 190 BP 247 EP 259 DI 10.1016/j.rse.2016.12.020 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA EL1RS UT WOS:000394399300020 ER PT J AU Markus, T Neumann, T Martino, A Abdalati, W Brunt, K Csatho, B Farrell, S Fricker, H Gardner, A Harding, D Jasinski, M Kwok, R Magruder, L Lubin, D Luthcke, S Morison, J Nelson, R Neuenschwander, A Palm, S Popescu, S Shum, CK Schutz, BE Smith, B Yang, YK Zwally, J AF Markus, Thorsten Neumann, Tom Martino, Anthony Abdalati, Waleed Brunt, Kelly Csatho, Beata Farrell, Sinead Fricker, Helen Gardner, Alex Harding, David Jasinski, Michael Kwok, Ron Magruder, Lori Lubin, Dan Luthcke, Scott Morison, James Nelson, Ross Neuenschwander, Amy Palm, Stephen Popescu, Sorin Shum, C. K. Schutz, Bob E. Smith, Benjamin Yang, Yuekui Zwally, Jay TI The Ice, Cloud, and land Elevation Satellite-2 (ICESat-2): Science requirements, concept, and implementation SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE ICESat-2; Land ice; Sea ice; Vegetation; Climate change; Satellite mission ID SEA-LEVEL RISE; PHOTON-COUNTING LIDAR; INCREASED MASS-LOSS; LASER ALTIMETRY; RECONCILED ESTIMATE; WEST ANTARCTICA; GROUNDING ZONE; SHEET DYNAMICS; FOREST BIOMASS; CARBON BALANCE AB The Ice, Cloud, and land Elevation Satellite (ICESat) mission used laser altimetry measurements to determine changes in elevations of glaciers and ice sheets, as well as sea ice thickness distribution. These measurements have provided important information on the response of the cryopshere (Earth's frozen surfaces) to changes in atmosphere and ocean condition. ICESat operated from 2003 to 2009 and provided repeat altimetry measurements not only to the cryosphere scientific community but also to the ocean, terrestrial and atmospheric scientific communities. The conclusive assessment of significant ongoing rapid changes in the Earth's ice cover, in part supported by ICESat observations, has strengthened the need for sustained, high accuracy, repeat observations similar to what was provided by the ICESat mission. Following recommendations from the National Research Council for an ICESat follow-on mission, the ICESat-2 mission is now under development for planned launch in 2018. The primary scientific aims of the ICESat-2 mission are to continue measurements of sea ice freeboard and ice sheet elevation to determine their changes at scales from outlet glaciers to the entire ice sheet, and from 105 of meters to the entire polar oceans for sea ice freeboard. ICESat carried a single beam profiling laser altimeter that produced similar to 70 m diameter footprints on the surface of the Earth at similar to 150 m along-track intervals. In contrast, ICESat-2 will operate with three pairs of beams, each pair separated by about 3 km cross-track with a pair spacing of 90 m. Each of the beams will have a nominal 17 m diameter footprint with an along -track sampling interval of 0.7 m. The differences in the ICESat-2 measurement concept are a result of overcoming some limitations associated with the approach used in the ICESat mission. The beam pair configuration of ICESat-2 allows for the determination of local cross -track slope, a significant factor in measuring elevation change for the outlet glaciers surrounding the Greenland and Antarctica coasts. The multiple beam pairs also provide improved spatial coverage. The dense spatial sampling eliminates along -track measurement gaps, and the small footprint diameter is especially useful for sea surface height measurements in the often narrow leads needed for sea ice freeboard and ice thickness retrievals. The ICESat-2 instrumentation concept uses a low energy 532 nm (green) laser in conjunction with single-photon sensitive detectors to measure range. Combining ICESat-2 data with altimetry data collected since the start of the ICESat mission in 2003, such as Operation IceBridge and ESA's CryoSat-2, will yield a 15+ year record of changes in ice sheet elevation and sea ice thickness. ICESat-2 will also provide information of mountain glacier and ice cap elevations changes, land and vegetation heights, inland water elevations, sea surface heights, and cloud layering and optical thickness. Published by Elsevier Inc. This is an open access article under the CC BY license C1 [Markus, Thorsten; Neumann, Tom; Martino, Anthony; Brunt, Kelly; Harding, David; Jasinski, Michael; Luthcke, Scott; Nelson, Ross; Palm, Stephen; Yang, Yuekui; Zwally, Jay] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Abdalati, Waleed] Univ Colorado, Boulder, CO 80309 USA. [Brunt, Kelly; Farrell, Sinead; Zwally, Jay] Univ Maryland, College Pk, MD 20742 USA. [Csatho, Beata] SUNY Buffalo, Buffalo, NY USA. [Fricker, Helen; Lubin, Dan] Scripps Inst Oceanog, La Jolla, CA USA. [Gardner, Alex; Kwok, Ron] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Magruder, Lori; Neuenschwander, Amy; Schutz, Bob E.] Univ Texas Austin, Austin, TX 78712 USA. [Morison, James; Smith, Benjamin] Univ Washington, Seattle, WA 98195 USA. [Popescu, Sorin] Texas A&M Univ, College Stn, TX USA. [Shum, C. K.] Ohio State Univ, Columbus, OH 43210 USA. [Yang, Yuekui] Univ Space Res Assoc, Columbia, MD USA. RP Markus, T (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Thorsten.Markus@nasa.gov FU NASA HQ [ICESat-23] FX We would like to thank Tom Wagner and Richard Slonaker, Program Scientist and Program Executive for ICESat-23 at NASA HQ for their support. We also would like to thank all the members of the project science office for their help. Finally, we would like to thank the reviewers for their thorough reading of the manuscript and constructive comments. NR 72 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD MAR 1 PY 2017 VL 190 BP 260 EP 273 DI 10.1016/j.rse.2016.12.029 PG 14 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA EL1RS UT WOS:000394399300021 ER PT J AU Pahlevan, N Schott, JR Franz, BA Zibordi, G Markham, B Bailey, S Schaaf, CB Ondrusek, M Greb, S Strait, CM AF Pahlevan, Nima Schott, John R. Franz, Bryan A. Zibordi, Giuseppe Markham, Brian Bailey, Sean Schaaf, Crystal B. Ondrusek, Michael Greb, Steven Strait, Christopher M. TI Landsat 8 remote sensing reflectance (R-rs) products: Evaluations, intercomparisons, and enhancements SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Landsat 8; Aquatic science; Ocean color; Atmospheric correction; Calibration Coastal/inland ID AEROSOL OPTICAL-THICKNESS; WATER-LEAVING RADIANCE; OCEAN COLOR SENSORS; ATMOSPHERIC CORRECTION; MODIS DATA; CALIBRATION; RETRIEVAL; ALGORITHM; SEAWIFS AB The Operational Land Imager (OLI) onboard Landsat-8 is generating high-quality aquatic science products, the most critical of which is the remote sensing reflectance (R-rs), defined as the ratio of water-leaving radiance to the total downwelling irradiance just above water. The quality of the R-rs products has not, however, been extensively assessed. This manuscript provides a comprehensive evaluation of Level-1B, i.e., top of atmosphere reflectance, and R-rs products available from OLI imagery under near-ideal atmospheric conditions in moderately turbid waters. The procedure includes a) evaluations of the R-rs products at sites included in the Ocean Color component of the Aerosol Robotic Network (AERONET-OC), b) intercomparisons and cross-calibrations against other ocean color products, and c) optimizations of vicarious calibration gains across the entire OLI observing swath. Results indicate that the near-infrared and shortwave infrared (NIR-SWIR) band combinations yield the most robust and stable R-rs retrievals in moderately turbid waters. Intercomparisons against products derived from the Visible Infrared Imaging Radiometer Suite (VIIRS) and the Moderate Resolution Imaging Spectroradiometer onboard the Aqua platform (MODISA) indicate slight across-track non-uniformities (<1%) associated with OLI scenes in the blue bands. In both product domains (TOA and R-rs), on average, the OLI products were found larger in radiometric responses in the blue channels. Following the implementation of updated vicarious calibration gains and accounting for across-track non-uniformities, matchup analyses using independent in-situ validation data confirmed improvements in R-rs products. These findings further support high-fidelity OLI-derived aquatic science products in terms of both demonstrating a robust atmospheric correction method and providing consistent products across OLI's imaging swath. (C) 2017 The Authors. Published by Elsevier Inc. This is an open access article under the CC BY license C1 [Pahlevan, Nima; Franz, Bryan A.; Markham, Brian; Bailey, Sean] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. [Pahlevan, Nima] Sci Syst & Applicat Inc, 10210 Greenbelt Rd, Lanham, MD 20706 USA. [Schott, John R.] Rochester Inst Technol, 54 Lomb Mem Dr, Rochester, NY 14623 USA. [Zibordi, Giuseppe] European Commiss, Joint Res Ctr, I-21027 Ispra, Italy. [Schaaf, Crystal B.] Univ Massachusetts, 100 Morrissey Blvd, Boston, MA 02125 USA. [Ondrusek, Michael] NOAA, NESDIS, STAR, SOCD, College Pk, MD 20740 USA. [Greb, Steven] Wisconsin Dept Nat Resources, 2801 Progress Rd, Madison, WI 53716 USA. [Strait, Christopher M.] Upstate Freshwater Inst, 224 Midler Pk Dr, Syracuse, NY 13206 USA. RP Pahlevan, N (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM nima.pahlevan@nasa.gov OI Bailey, Sean/0000-0001-8339-9763; Pahlevan, Nima/0000-0002-5454-5212 FU NASA [NNX16AI16G, NNX14AI73G, NNX14AQ18A]; USGS [G14AC00372, G11PS00422]; MIT SeaGrant [2015-R/RC-140] FX The authors would like to extend their gratitude to the Landsat Cal/Val team led by the USGS/NASA consortium. In particular, we thank James Storey (NASA GSFC) for providing the most up-to-date code to compute accurate OLI geometry files. Pahlevan is funded by the NASA grant # NNX16AI16G and the USGS grant # G14AC00372. Partial funding support was also provided by the MIT SeaGrant award #2015-R/RC-140. Schaaf is funded by NASA NNX14AI73G, NNX14AQ18A and the USGS grant # G11PS00422. We would like to also thank Eugene Fosnight with the USGS for the development of Landsat-8 matchup identification tool. We acknowledge the AERONET-OC data that was used in this study. This includes Hui Feng, Heidi M. Sosik, Alex Gilerson, Samir Ahmed, Alan Wideman, Burton Jones, Curtiss Davis, Alan Weidemann, Bill Gibson, Robert Arnone, Dimitry Van der Zande, and Susanne Kratzer. We also appreciate efforts made by Qingsong Song (for the n-SNO matchup search analysis) and Obaidul Haque (for implementation of the gains). NR 34 TC 0 Z9 0 U1 3 U2 3 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD MAR 1 PY 2017 VL 190 BP 289 EP 301 DI 10.1016/j.rse.2016.12.030 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA EL1RS UT WOS:000394399300023 ER PT J AU Twing, KI Brazelton, WJ Kubo, MDY Hyer, AJ Cardace, D Hoehler, TM McCollom, TM Schrenk, MO AF Twing, Katrina I. Brazelton, William J. Kubo, Michael D. Y. Hyer, Alex J. Cardace, Dawn Hoehler, Tori M. McCollom, Tom M. Schrenk, Matthew O. TI Serpentinization-Influenced Groundwater Harbors Extremely Low Diversity Microbial Communities Adapted to High pH SO FRONTIERS IN MICROBIOLOGY LA English DT Article DE serpentinization; alkaliphile; extremophile; groundwater; borehole ID CITY HYDROTHERMAL FIELD; SP NOV.; GEOCHEMICAL PROCESSES; DEEP; ECOSYSTEM; METHANE; CLASSIFICATION; HYDROGENASES; METAGENOMES; PHILIPPINES AB Serpentinization is a widespread geochemical process associated with aqueous alteration of ultramafic rocks that produces abundant reductants (H-2 and CH4) for life to exploit, but also potentially challenging conditions, including high pH, limited availability of terminal electron acceptors, and low concentrations of inorganic carbon. As a consequence, past studies of serpentinites have reported low cellular abundances and limited microbial diversity. Establishment of the Coast Range Ophiolite Microbial Observatory (California, U.S.A.) allowed a comparison of microbial communities and physicochemical parameters directly within serpentinization-influenced subsurface aquifers. Samples collected from seven wells were subjected to a range of analyses, including solute and gas chemistry, microbial diversity by 16S rRNA gene sequencing, and metabolic potential by shotgun metagenomics, in an attempt to elucidate what factors drive microbial activities in serpentinite habitats. This study describes the first comprehensive interdisciplinary analysis of microbial communities in hyperalkaline groundwater directly accessed by boreholes into serpentinite rocks. Several environmental factors, including pH, methane, and carbon monoxide, were strongly associated with the predominant subsurface microbial communities. A single operational taxonomic unit (OTU) of Betaproteobacteria and a few OTUs of Clostridia were the almost exclusive inhabitants of fluids exhibiting the most serpentinized character. Metagenomes from these extreme samples contained abundant sequences encoding proteins associated with hydrogen metabolism, carbon monoxide oxidation, carbon fixation, and acetogenesis. Metabolic pathways encoded by Clostridia and Betaproteobacteria, in particular, are likely to play important roles in the ecosystems of serpentinizing groundwater. These data provide a basis for further biogeochemical studies of key processes in serpentinite subsurface environments. C1 [Twing, Katrina I.; Schrenk, Matthew O.] Michigan State Univ, Dept Microbiol & Mol Genet, E Lansing, MI 48824 USA. [Twing, Katrina I.; Brazelton, William J.; Hyer, Alex J.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Kubo, Michael D. Y.] SETI Inst, Mountain View, CA USA. [Cardace, Dawn] Univ Rhode Isl, Dept Geosci, Kingston, RI 02881 USA. [Hoehler, Tori M.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. [McCollom, Tom M.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. RP Twing, KI (reprint author), Michigan State Univ, Dept Microbiol & Mol Genet, E Lansing, MI 48824 USA.; Twing, KI (reprint author), Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. EM katrinatwing@gmail.com FU NASA Astrobiology Institute; Alfred P. Sloan Foundation's Deep Carbon Observatory [2011-12-01]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231] FX The establishment of CROMO was funded by the NASA Astrobiology Institute and the research conducted was funded by the Alfred P. Sloan Foundation's Deep Carbon Observatory (2011-12-01). All of the sequencing was performed by the DOE Joint Genome Institute (supported by the Office of Science of the U.S. Department of Energy under the contract DE-AC02-05CH11231). NR 66 TC 0 Z9 0 U1 0 U2 0 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 MAR 1 PY 2017 VL 8 AR 308 DI 10.3389/fmicb.2017.00308 PG 16 WC Microbiology SC Microbiology GA EL9YY UT WOS:000394977200001 PM 28298908 ER PT J AU Shah, R Xu, XL Yueh, S Chae, CS Elder, K Starr, B Kim, YJ AF Shah, Rashmi Xu, Xiaolan Yueh, Simon Chae, Chun Sik Elder, Kelly Starr, Banning Kim, Yunjin TI Remote Sensing of Snow Water Equivalent Using P-Band Coherent Reflection SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Bistatic radar; P-band; signals of opportunity (SoOp); snow remote sensing; snow water equivalent (SWE) ID DRY-SNOW AB A proof-of-concept experiment was carried out to demonstrate the feasibility of retrieving snow water equivalent (SWE) using P-band signals of opportunity. The fundamental observation is the change in the phase of the reflected waveforms as related to the change in SWE. Through theoretical modeling it was found that the change in SWE was approximately linearly dependent on the change in phase. This was verified by retrieving SWE data collected and processed from a tower-based experiment at Fraser, CO, USA. A linear regression was performed on measured phase and in situ SWE. The correlation was found to be 0.94 and root mean square deviation was found to be 7.5 mm. C1 [Shah, Rashmi; Xu, Xiaolan; Yueh, Simon; Chae, Chun Sik; Kim, Yunjin] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Elder, Kelly; Starr, Banning] US Forest Serv, Ft Collins, CO 80526 USA. RP Shah, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM rashmi.shah@jpl.nasa.gov; xiaolan.xu@jpl.nasa.gov; simon.h.yueh@jpl.nasa.gov; chun.sik.chae@jpl.nasa.gov; kelder@fs.fed.us; bjstarr@fs.fed.us; yunjin.kim@jpl.nasa.gov FU Jet Propulsion Laboratory, California Institute of Technology under National Aeronautics and Space Administration FX This work was supported by the Jet Propulsion Laboratory, California Institute of Technology under a Contract with the National Aeronautics and Space Administration. NR 16 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 1545-598X EI 1558-0571 J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD MAR PY 2017 VL 14 IS 3 BP 309 EP 313 DI 10.1109/LGRS.2016.2636664 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA EN3KY UT WOS:000395908600007 ER PT J AU Cooper, KB Durden, SL Cochrane, CJ Monje, RR Dengler, RJ Baldi, C AF Cooper, Ken B. Durden, Stephen L. Cochrane, Corey J. Monje, Raquel Rodriguez Dengler, Robert J. Baldi, Chad TI Using FMCW Doppler Radar to Detect Targets up to the Maximum Unambiguous Range SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Millimeter wave radar; radar theory AB Most applications of frequency-modulated continuous-wave radar described in the literature involve targets that are in relatively close proximity to the radar. In these cases, the round-trip travel time of the target's radar signature is small relative to the transmit chirp duration, simplifying the processing required for range and velocity extraction. This is not the case for more distant targets, where much of the radar signature is received after the start of the subsequent transmit waveform. In this letter, we examine various signal-processing options for coping with this long-range condition. We analytically demonstrate how to retain both range and Doppler shift information for an arbitrary number of targets spaced anywhere from very near the target up to the radar's unambiguous range. The motivation for this work is to develop a 95-GHz Doppler radar for measuring ice and dust particle dynamics in cometary jets. Simulations and experimental results are provided to validate our methods. C1 [Cooper, Ken B.; Durden, Stephen L.; Cochrane, Corey J.; Monje, Raquel Rodriguez; Dengler, Robert J.; Baldi, Chad] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Cooper, KB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ken.b.cooper@jpl.nasa.gov FU Jet Propulsion Laboratory; California Institute of Technology; National Aeronautics and Space Administration FX This work was supported in part by the Jet Propulsion Laboratory, California Institute of Technology and in part by the National Aeronautics and Space Administration. NR 13 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 1545-598X EI 1558-0571 J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD MAR PY 2017 VL 14 IS 3 BP 339 EP 343 DI 10.1109/LGRS.2016.2640954 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA EN3KY UT WOS:000395908600013 ER PT J AU Montes, C Jacob, F AF Montes, Carlo Jacob, Frederic TI Comparing Landsat-7 ETM+ and ASTER Imageries to Estimate Daily Evapotranspiration Within a Mediterranean Vineyard Watershed SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER); daily evapotranspiration (ET); Landsat-7 Enhanced Thematic Mapper Plus (ETM plus ); simplified surface energy balance index (S-SEBI); solar and thermal infrared remote sensing; vineyard landscape ID SURFACE-ENERGY BALANCE; SPACEBORNE THERMAL EMISSION; REFLECTION RADIOMETER ASTER; HEAT-FLUX ESTIMATION; S-SEBI; MODEL; PRODUCT; ALBEDO; BAND; AREA AB We compared the capabilities of Landsat-7 Enhanced Thematic Mapper Plus (ETM+) and Advanced Space-borne Thermal Emission and Reflection Radiometer (ASTER) imageries for mapping daily evapotranspiration (ET) within a Mediterranean vineyard watershed. We used Landsat and ASTER data simultaneously collected on four dates in 2007 and 2008, along with the simplified surface energy balance index (S-SEBI) model. We used previously ground-validated good quality ASTER estimates as reference, and we analyzed the differences with Landsat retrievals in light of the instrumental factors and methodology. Although Landsat and ASTER retrievals of S-SEBI inputs were different, estimates of daily ET from the two imageries were similar. This is ascribed to the S-SEBI spatial differencing in temperature, and opens the path for using historical Landsat time series over vineyards. C1 [Montes, Carlo; Jacob, Frederic] Inst Rech Dev, UMR Lab Etud Interact Entre Sol Agrosyst Hydrosys, F-34060 Montpellier, France. [Montes, Carlo] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Montes, C (reprint author), Inst Rech Dev, UMR Lab Etud Interact Entre Sol Agrosyst Hydrosys, F-34060 Montpellier, France. EM ccmontesv@gmail.com; frederic.jacob@ird.fr RI Jacob, Frederic/A-5946-2011 OI Jacob, Frederic/0000-0002-2491-3096 FU Centre National d'Etudes Spatiales [127186]; Agence Nationale de la Recherche [ANR-12-TMED-0003-01]; CONICYT-Chile; National Aeronautics and Space Administration Postdoctoral Program; Universities Space Research Association; FP7 [262060] FX This work was supported in part by the Centre National d'Etudes Spatiales under Contract 127186, in part by FP7 under Contract 262060, and in part by the Agence Nationale de la Recherche under Contract ANR-12-TMED-0003-01. The work of C. Montes was supported in part by CONICYT-Chile in part by the National Aeronautics and Space Administration Postdoctoral Program, and in part by the Universities Space Research Association. NR 41 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 1545-598X EI 1558-0571 J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD MAR PY 2017 VL 14 IS 3 BP 459 EP 463 DI 10.1109/LGRS.2017.2650143 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA EN3KY UT WOS:000395908600037 ER PT J AU Repko, TW Nix, AC Uysal, C Heidmann, JD AF Repko, Timothy W. Nix, Andrew C. Uysal, Can Heidmann, James D. TI Numerical Study on the Effects of Freestream Turbulence on Antivortex Film Cooling Design at High Blowing Ratio SO JOURNAL OF THERMAL SCIENCE AND ENGINEERING APPLICATIONS LA English DT Article DE gas turbines; film cooling; freestream turbulence; high blowing ratio; heat transfer; multihole AB An advanced, high-effectiveness film cooling design, the antivortex hole (AVH) has been investigated by several research groups and shown to mitigate or counter the vorticity generated by conventional holes and increase film effectiveness at high blowing ratios and low freestream turbulence levels. The effects of increased turbulence on an AVH geometry were previously investigated in a preliminary steady computational fluid dynamics (CFD) study by Hunley et al. on the film effectiveness and net heat flux reduction (NHFR) at high blowing ratio. The current paper presents the results of an extended numerical parametric study, which attempts to separate the effects of turbulence intensity and length scale on film cooling performance of the AVH concept at high blowing ratio (2.0) and density ratio (2.0). In this extended study, steady Reynolds-averaged Navier-Stokes (RANS) analysis was performed with turbulence intensities of 5, 10, and 20% and length scales based on cooling hole diameter of K-x/d(m) = 1, 3, and 6. Increasing turbulence intensity was shown to increase the centerline, span-averaged, and area-averaged adiabatic film cooling effectiveness and NHFR. Larger turbulent length scales in the steady RANS analysis were shown to have little to no effect on the centerline, span-averaged, and area-averaged adiabatic film cooling effectiveness and NHFR at lower turbulence levels, but moderate effect at the highest turbulence levels investigated. Heat transfer results were in good agreement with the findings from adiabatic cases from previous work. Unsteady RANS results also provided supplementary flow visualization for the AVH film cooling flow under varying turbulence levels. C1 [Repko, Timothy W.; Nix, Andrew C.; Uysal, Can] West Virginia Univ, Dept Mech & Aerosp Engn, Morgantown, WV 26505 USA. [Heidmann, James D.] NASA, Turbomachinery & Heat Transfer Branch, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Nix, AC (reprint author), West Virginia Univ, Dept Mech & Aerosp Engn, Morgantown, WV 26505 USA. EM andrew.nix@mail.wvu.edu; heidmann@nasa.gov FU Department of Energy, Office of Science, Experimental Program to Stimulate Competitive Research (EPSCoR) [DE-FG02-09ER46615] FX The authors would like to acknowledge the support of the Department of Energy, Office of Science, Experimental Program to Stimulate Competitive Research (EPSCoR) under Grant/Contract No. DE-FG02-09ER46615, monitored by Dr. Tim Fitz-simmons of the DOE Office of Science/EPSCoR. The authors would also like to thank CD-ADAPCO for their software training and support throughout this analysis. NR 28 TC 0 Z9 0 U1 0 U2 0 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 1948-5085 EI 1948-5093 J9 J THERM SCI ENG APPL JI J. Therm. Sci. Eng. Appl. PD MAR PY 2017 VL 9 IS 1 AR 011013 DI 10.1115/1.4034851 PG 12 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA EL2EX UT WOS:000394434000013 ER PT J AU Abdollahi, S Ackermann, M Ajello, M Albert, A Atwood, WB Baldini, L Barbiellini, G Bellazzini, R Bissaldi, E Bloom, ED Bonino, R Bottacini, E Brandt, TJ Bruel, P Buson, S Caragiulo, M Cavazzuti, E Chekhtman, A Ciprini, S Costanza, F Cuoco, A Cutini, S D'Ammando, F de Palma, F Desiante, R Digel, SW Di Lalla, N Di Mauro, M Di Venere, L Donaggio, B Drell, PS Favuzzi, C Focke, WB Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Giglietto, N Giordano, F Giroletti, M Green, D Guiriec, S Harding, AK Jogler, T Johannesson, G Kamae, T Kuss, M Larsson, S Latronico, L Li, J Longo, F Loparco, F Lubrano, P Magill, JD Malyshev, D Manfreda, A Mazziotta, MN Meehan, M Michelson, PF Mitthumsiri, W Mizuno, T Moiseev, AA Monzani, ME Morselli, A Negro, M Nuss, E Ohsugi, T Omodei, N Paneque, D Perkins, JS Pesce-Rollins, M Piron, F Pivato, G Principe, G Raino, S Rando, R Razzano, M Reimer, A Reimer, O Sgro, C Simone, D Siskind, EJ Spada, F Spandre, G Spinelli, P Strong, AW Tajima, H Thayer, JB Torres, DF Troja, E Vandenbroucke, J Zaharijas, G Zimmer, S AF Abdollahi, S. Ackermann, M. Ajello, M. Albert, A. Atwood, W. B. Baldini, L. Barbiellini, G. Bellazzini, R. Bissaldi, E. Bloom, E. D. Bonino, R. Bottacini, E. Brandt, T. J. Bruel, P. Buson, S. Caragiulo, M. Cavazzuti, E. Chekhtman, A. Ciprini, S. Costanza, F. Cuoco, A. Cutini, S. D'Ammando, F. de Palma, F. Desiante, R. Digel, S. W. Di Lalla, N. Di Mauro, M. Di Venere, L. Donaggio, B. Drell, P. S. Favuzzi, C. Focke, W. B. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Giglietto, N. Giordano, F. Giroletti, M. Green, D. Guiriec, S. Harding, A. K. Jogler, T. Johannesson, G. Kamae, T. Kuss, M. Larsson, S. Latronico, L. Li, J. Longo, F. Loparco, F. Lubrano, P. Magill, J. D. Malyshev, D. Manfreda, A. Mazziotta, M. N. Meehan, M. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monzani, M. E. Morselli, A. Negro, M. Nuss, E. Ohsugi, T. Omodei, N. Paneque, D. Perkins, J. S. Pesce-Rollins, M. Piron, F. Pivato, G. Principe, G. Raino, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Sgro, C. Simone, D. Siskind, E. J. Spada, F. Spandre, G. Spinelli, P. Strong, A. W. Tajima, H. Thayer, J. B. Torres, D. F. Troja, E. Vandenbroucke, J. Zaharijas, G. Zimmer, S. CA Fermi-LAT Collaboration TI Search for Cosmic-Ray Electron and Positron Anisotropies with Seven Years of Fermi Large Area Telescope Data SO PHYSICAL REVIEW LETTERS LA English DT Article AB The Large Area Telescope on board the Fermi Gamma-ray Space Telescope has collected the largest ever sample of high-energy cosmic-ray electron and positron events since the beginning of its operation. Potential anisotropies in the arrival directions of cosmic-ray electrons or positrons could be a signature of the presence of nearby sources. We use almost seven years of data with energies above 42 GeV processed with the Pass 8 reconstruction. The present data sample can probe dipole anisotropies down to a level of 10(-3). We take into account systematic effects that could mimic true anisotropies at this level. We present a detailed study of the event selection optimization of the cosmic-ray electrons and positrons to be used for anisotropy searches. Since no significant anisotropies have been detected on any angular scale, we present upper limits on the dipole anisotropy. The present constraints are among the strongest to date probing the presence of nearby young and middle-aged sources. C1 [Abdollahi, S.; Fukazawa, Y.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Ackermann, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA. [Albert, A.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Atwood, W. B.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Atwood, W. B.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Baldini, L.; Di Lalla, N.; Manfreda, A.] Univ Pisa, Dipartimento Fis Enrico Fermi, I-56126 Pisa, Italy. [Baldini, L.; Bellazzini, R.; Di Lalla, N.; Kuss, M.; Manfreda, A.; Pesce-Rollins, M.; Pivato, G.; Razzano, M.; Sgro, C.; Spada, F.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Barbiellini, G.; Longo, F.; Zaharijas, G.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bissaldi, E.; Caragiulo, M.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Bissaldi, E.; Caragiulo, M.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Bissaldi, E.; Caragiulo, M.; Costanza, F.; de Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Simone, D.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bloom, E. D.; Bottacini, E.; Digel, S. W.; Di Mauro, M.; Drell, P. S.; Focke, W. B.; Michelson, P. F.; Monzani, M. E.; Omodei, N.; Reimer, A.; Reimer, O.; Tajima, H.; Thayer, J. B.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Bloom, E. D.; Bottacini, E.; Digel, S. W.; Di Mauro, M.; Drell, P. S.; Focke, W. B.; Michelson, P. F.; Monzani, M. E.; Omodei, N.; Reimer, A.; Reimer, O.; Tajima, H.; Thayer, J. B.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Bonino, R.; Cuoco, A.; Desiante, R.; Latronico, L.; Negro, M.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Bonino, R.; Negro, M.] Univ Turin, Dipartimento Fis, I-10125 Turin, Italy. [Brandt, T. J.; Buson, S.; Green, D.; Guiriec, S.; Harding, A. K.; Moiseev, A. A.; Perkins, J. S.; Troja, E.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bruel, P.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.] ASI, Sci Data Ctr, I-00133 Rome, Italy. [Chekhtman, A.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Chekhtman, A.] Naval Res Lab, Washington, DC 20375 USA. [Ciprini, S.; Cutini, S.; Gasparrini, D.; Lubrano, P.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Cuoco, A.] Rhein Westfal TH Aachen, Inst Theoret Particle Phys & Cosmol, TTK, D-52056 Aachen, Germany. [D'Ammando, F.; Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [de Palma, F.] Univ Telemat Pegaso, Piazza Trieste & Trento 48, I-80132 Naples, Italy. [Desiante, R.] Univ Udine, I-33100 Udine, Italy. [Donaggio, B.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Funk, S.; Malyshev, D.; Principe, G.] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany. [Green, D.; Magill, J. D.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Green, D.; Magill, J. D.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Jogler, T.] Friedrich Alexander Univ, Schlosspl 4, D-91054 Erlangen, Germany. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Kamae, T.] Univ Tokyo, Grad Sch Sci, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. [Larsson, S.] KTH Royal Inst Technol, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden. [Larsson, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Li, J.; Torres, D. F.] CSIC, Inst Space Sci IEEC, Campus UAB, E-08193 Barcelona, Spain. [Meehan, M.; Vandenbroucke, J.] Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA. [Mitthumsiri, W.] Mahidol Univ, Dept Phys, Fac Sci, Bangkok 10400, Thailand. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Moiseev, A. A.] CRESST, Greenbelt, MD 20771 USA. [Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Nuss, E.; Piron, F.] Univ Montpellier, IN2P3, CNRS, Lab Univers & Particules Montpellier, F-34095 Montpellier, France. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Torres, D. F.] ICREA, E-08010 Barcelona, Spain. [Zaharijas, G.] Univ Trieste, I-34127 Trieste, Italy. [Zaharijas, G.] Univ Nova Gorica, Lab Astroparticle Phys, Vipavska 13, SI-5000 Nova Gorica, Slovenia. [Zimmer, S.] Univ Geneva, DPNC, CH-1211 Geneva 4, Switzerland. RP Costanza, F (reprint author), Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. EM francesco.costanza@cern.ch; mazziotta@ba.infn.it FU National Aeronautics and Space Administration in the United States; Department of Energy in the United States; Commissariat a l'Energie Atomique in France; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana in Italy; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT) in Japan; High Energy Accelerator Research Organization (KEK) in Japan; Japan Aerospace Exploration Agency (JAXA) in Japan; K. A. Wallenberg Foundation in Sweden; Swedish Research Council in Sweden; Swedish National Space Board in Sweden; Italian Ministry of Education, University and Research (MIUR) [FIRB-2012-RBFR12PM1F] FX The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. The authors acknowledge the use of HEALPix [35] described in [7]. S. B. and S. G. acknowledge support as a NASA Postdoctoral Program Fellow of USA. M. R. acknowledges funded by contract FIRB-2012-RBFR12PM1F from the Italian Ministry of Education, University and Research (MIUR). NR 28 TC 0 Z9 0 U1 1 U2 1 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 MAR 1 PY 2017 VL 118 IS 9 AR 091103 DI 10.1103/PhysRevLett.118.091103 PG 7 WC Physics, Multidisciplinary SC Physics GA EN5KJ UT WOS:000396043900001 PM 28306280 ER PT J AU Reischke, R Kiessling, A Schafer, BM AF Reischke, Robert Kiessling, Alina Schafer, Bjorn Malte TI Variations of cosmic large-scale structure covariance matrices across parameter space SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: weak; dark energy; large-scale structure of Universe ID LENSING POWER SPECTRUM; GRAVITATIONAL-INSTABILITY; COSMOLOGICAL PARAMETERS; PERTURBATION-THEORY; DARK ENERGY; WEAK; SHEAR; SIMULATIONS; BISPECTRUM; FIELDS AB The likelihood function for cosmological parameters, given by e.g. weak lensing shear measurements, depends on contributions to the covariance induced by the non-linear evolution of the cosmic web. As highly non-linear clustering to date has only been described by numerical N-body simulations in a reliable and sufficiently precise way, the necessary computational costs for estimating those covariances at different points in parameter space are tremendous. In this work, we describe the change of the matter covariance and the weak lensing covariance matrix as a function of cosmological parameters by constructing a suitable basis, where we model the contribution to the covariance from non-linear structure formation using Eulerian perturbation theory at third order. We show that our formalism is capable of dealing with large matrices and reproduces expected degeneracies and scaling with cosmological parameters in a reliable way. Comparing our analytical results to numerical simulations, we find that the method describes the variation of the covariance matrix found in the SUNGLASS weak lensing simulation pipeline within the errors at one-loop and tree-level for the spectrum and the trispectrum, respectively, for multipoles up to l <= 1300. We show that it is possible to optimize the sampling of parameter space where numerical simulations should be carried out by minimizing interpolation errors and propose a corresponding method to distribute points in parameter space in an economical way. C1 [Reischke, Robert; Schafer, Bjorn Malte] Heidelberg Univ, Astron Recheninst, Zentrum Astron, Philosophenweg 12, D-69120 Heidelberg, Germany. [Kiessling, Alina] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA. RP Reischke, R (reprint author), Heidelberg Univ, Astron Recheninst, Zentrum Astron, Philosophenweg 12, D-69120 Heidelberg, Germany. EM reischke@stud.uni-heidelberg.de FU Jet Propulsion Laboratory by the California Institute of Technology; NASA ROSES [13-ATP13-0019]; graduate college Astrophysics of cosmological probes of gravity by Landesgraduiertenakademie Baden-Wurttemberg FX RR acknowledges funding by the graduate college Astrophysics of cosmological probes of gravity by Landesgraduiertenakademie Baden-Wurttemberg. AK was supported in part by the Jet Propulsion Laboratory, run under contract by the California Institute of Technology for the National Aeronautics and Space Administration. AK was also supported in part by NASA ROSES 13-ATP13-0019. NR 48 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 MAR PY 2017 VL 465 IS 4 BP 4016 EP 4025 DI 10.1093/mnras/stw2976 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EM2UC UT WOS:000395170200019 ER PT J AU Kovacs, A Sanchez, C Garcia-Bellido, J Nadathur, S Crittenden, R Gruen, D Huterer, D Bacon, D Clampitt, J DeRose, J Dodelson, S Gaztanaga, E Jain, B Kirk, D Lahav, O Miquel, R Naidoo, K Peacock, JA Soergel, B Whiteway, L Abdalla, FB Allam, S Annis, J Benoit-Levy, A Bertin, E Brooks, D Buckley-Geer, E Rosell, AC Kind, MC Carretero, J Cunha, CE D'Andrea, CB da Costa, LN DePoy, DL Desai, S Eifler, TF Finley, DA Flaugher, B Fosalba, P Frieman, J Giannantonio, T Goldstein, DA Gruendl, RA Gutierrez, G James, DJ Kuehn, K Kuropatkin, N Marshall, JL Melchior, P Menanteau, F Nord, B Ogando, R Plazas, AA Romer, AK Sanchez, E Scarpine, V Sevilla-Noarbe, I Sobreira, F Suchyta, E Swanson, M Tarle, G Thomas, D Walker, AR AF Kovacs, A. Sanchez, C. Garcia-Bellido, J. Nadathur, S. Crittenden, R. Gruen, D. Huterer, D. Bacon, D. Clampitt, J. DeRose, J. Dodelson, S. Gaztanaga, E. Jain, B. Kirk, D. Lahav, O. Miquel, R. Naidoo, K. Peacock, J. A. Soergel, B. Whiteway, L. Abdalla, F. B. Allam, S. Annis, J. Benoit-Levy, A. Bertin, E. Brooks, D. Buckley-Geer, E. Rosell, A. Carnero Kind, M. Carrasco Carretero, J. Cunha, C. E. D'Andrea, C. B. da Costa, L. N. DePoy, D. L. Desai, S. Eifler, T. F. Finley, D. A. Flaugher, B. Fosalba, P. Frieman, J. Giannantonio, T. Goldstein, D. A. Gruendl, R. A. Gutierrez, G. James, D. J. Kuehn, K. Kuropatkin, N. Marshall, J. L. Melchior, P. Menanteau, F. Nord, B. Ogando, R. Plazas, A. A. Romer, A. K. Sanchez, E. Scarpine, V. Sevilla-Noarbe, I. Sobreira, F. Suchyta, E. Swanson, M. Tarle, G. Thomas, D. Walker, A. R. CA DES Collaboration TI Imprint of DES superstructures on the cosmic microwave background SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; cosmic background radiation; large-scale structure of Universe ID INTEGRATED SACHS-WOLFE; SCIENCE VERIFICATION DATA; LUMINOUS RED GALAXIES; COLD SPOT; DARK ENERGY; CROSS-CORRELATION; VOIDS; CATALOG; PLANCK; WMAP AB Small temperature anisotropies in the cosmic microwave background (CMB) can be sourced by density perturbations via the late-time integrated Sachs-Wolfe (ISW) effect. Large voids and superclusters are excellent environments to make a localized measurement of this tiny imprint. In some cases excess signals have been reported. We probed these claims with an independent data set, using the first year data of the Dark Energy Survey (DES) in a different footprint, and using a different superstructure finding strategy. We identified 52 large voids and 102 superclusters at redshifts 0.2 < z < 0.65. We used the Jubilee simulation to a priori evaluate the optimal ISW measurement configuration for our compensated top-hat filtering technique, and then performed a stacking measurement of the CMB temperature field based on the DES data. For optimal configurations, we detected a cumulative cold imprint of voids with Delta T-f approximate to -5.0 +/- 3.7 mu K and a hot imprint of superclusters Delta T-f approximate to 5.1 +/- 3.2 mu K; this is similar to 1.2 sigma higher than the expected vertical bar Delta T-f vertical bar approximate to 0.6 mu K imprint of such superstructures in Lambda cold dark matter (Lambda CDM). If we instead use an a posteriori selected filter size (R/R-v = 0.6), we can find a temperature decrement as large as Delta T-f approximate to -9.8 +/- 4.7 mu K for voids, which is similar to 2 sigma above Lambda CDM expectations and is comparable to previous measurements made using Sloan Digital Sky Survey superstructure data. C1 [Kovacs, A.; Sanchez, C.; Miquel, R.; Carretero, J.] Barcelona Inst Sci & Technol, Inst Fisica Altes Energies IFAE, Campus UAB, E-08193 Barcelona, Spain. [Garcia-Bellido, J.] Univ Autonoma Madrid, Inst Fisica Teorica IFT UAM, CSIC, E-28049 Madrid, Spain. [Nadathur, S.; Crittenden, R.; Bacon, D.; D'Andrea, C. B.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Gruen, D.; DeRose, J.; Cunha, C. E.] Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA. [Gruen, D.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Huterer, D.; Brooks, D.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Clampitt, J.; Jain, B.; Suchyta, E.] Univ Pennsylvania, Dept Phys & Astron, Philadelphia, PA 19104 USA. [DeRose, J.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. [Dodelson, S.; Allam, S.; Annis, J.; Buckley-Geer, E.; Finley, D. A.; Flaugher, B.; Frieman, J.; Gutierrez, G.; Kuropatkin, N.; Nord, B.; Scarpine, V.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. [Dodelson, S.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Gaztanaga, E.; Carretero, J.] Inst Ciencies Espai, IEEC CSIC, Campus UAB,Carrer Can Magrans,S-N, E-08193 Barcelona, Spain. [Kirk, D.; Lahav, O.; Naidoo, K.; Whiteway, L.; Abdalla, F. B.; Benoit-Levy, A.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Miquel, R.] Inst Catalana Recerca Estudis Avanc, E-08010 Barcelona, Spain. [Peacock, J. A.] Univ Edinburgh, Inst Astron, Royal Observ, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. [Soergel, B.; Giannantonio, T.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Soergel, B.; Giannantonio, T.] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England. [Abdalla, F. B.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa. [Benoit-Levy, A.; Bertin, E.] Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France. [Benoit-Levy, A.; Bertin, E.] Sorbonne Univ, UPMC Univ Paris 06, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Rosell, A. Carnero; da Costa, L. N.; Ogando, R.; Sobreira, F.] Laboratorio Interinstituc Astron LIneA, Rua Gal Jos Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Rosell, A. Carnero; da Costa, L. N.; Ogando, R.] Observatorio Nacl, Rua Gal Jos Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Kind, M. Carrasco; Gruendl, R. A.] Univ Illinois, Dept Astron, 1002 Green St, Urbana, IL 61801 USA. [Kind, M. Carrasco; Gruendl, R. A.] Natl Ctr Supercomp Applicat, 1205 W Clark St, Urbana, IL 61801 USA. [D'Andrea, C. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [DePoy, D. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, College Stn, TX 77843 USA. [Desai, S.] Excellence Cluster Univ, Boltzmannstr 2, D-85748 Garching, Germany. [Desai, S.] Ludwig Maximilians Univ Munchen, 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. [Goldstein, D. A.] Univ Calif, Dept Astron, 501 Camp bell Hall 3411, Berkeley, CA 94720 USA. [Goldstein, D. A.] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [James, D. J.; DES Collaboration] Cerro Tololo Interamer Observ, Natl Optic Astron Observ, Casilla 603, La Serena, Chile. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Marshall, J. L.] Carnegie Observatories, 813 Santa Barbara St, Pasadena, CA 91101 USA. [Melchior, P.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England. [Sanchez, E.; Sevilla-Noarbe, I.] Centro Investigac Energeticas Medioambient Tecnol, E-28040 Madrid, Spain. [Sobreira, F.] Univ Estadual Paulista, ICTP S Amer Inst Fundamental Res Inst Fisica Teor, Sao Paulo, Brazil. RP Kovacs, A (reprint author), Barcelona Inst Sci & Technol, Inst Fisica Altes Energies IFAE, Campus UAB, E-08193 Barcelona, Spain. EM akovacs@ifae.es RI Ogando, Ricardo/A-1747-2010 OI Ogando, Ricardo/0000-0003-2120-1154 FU Spanish Ministerio de Economia y Competitividad (MINECO) [FPA2012-39684]; Centro de Excelencia Severo Ochoa [SEV-2012-0234, SEV-2012-0249]; 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; Fundayao Carlos Chagas Filho de Amparo aPesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; Argonne National Laboratory; University of California at Santa Cruz; University of Cambridge; Centro de Investigaciones Energeticas [SEV-2012-0234, SEV-2012-0249]; Medioambientales y Tecnologicas-Madrid; University of Chicago; University College London; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) Zurich; Fermi National Accelerator Laboratory; University of Illinois at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory; Ludwig-Maximilians Universitar Munchen; 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; OzDES Membership Consortium; National Science Foundation [AST-1138766]; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; European Research Council under the European Union [240672, 291329, 306478]; NASA [PF5-160138] FX Funding for this project was partially provided by the Spanish Ministerio de Economia y Competitividad (MINECO) under projects FPA2012-39684 and Centro de Excelencia Severo Ochoa SEV-2012-0234 and SEV-2012-0249.; 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, Fundayao Carlos Chagas Filho de Amparo aPesquisa 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 Universitar 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, Texas A&M University, and the OzDES Membership Consortium.; 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 and SEV-2012-0249. 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. Support for DG was provided by NASA through the Einstein Fellowship Program, grant PF5-160138.; 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 and SEV-2012-0249. 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. Support for DG was provided by NASA through the Einstein Fellowship Program, grant PF5-160138. NR 66 TC 0 Z9 0 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 MAR PY 2017 VL 465 IS 4 BP 4166 EP 4179 DI 10.1093/mnras/stw2968 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EM2UC UT WOS:000395170200032 ER PT J AU Clampitt, J Sanchez, C Kwan, J Krause, E MacCrann, N Park, Y Troxel, MA Jain, B Rozo, E Rykoff, ES Wechsler, RH Blazek, J Bonnett, C Crocce, M Fang, Y Gaztanaga, E Gruen, D Jarvis, M Miquel, R Prat, J Ross, AJ Sheldon, E Zuntz, J Abbott, TMC Abdalla, FB Armstrong, R Becker, MR Benoit-Levy, A Bernstein, GM Bertin, E Brooks, D Burke, DL Rosell, AC Kind, MC Cunha, CE D'Andrea, CB da Costa, LN Desai, S Diehl, HT Dietrich, JP Doel, P Estrada, J Evrard, AE Neto, AF Flaugher, B Fosalba, P Frieman, J Gruendl, RA Honscheid, K James, DJ Kuehn, K Kuropatkin, N Lahav, O Lima, M March, M Marshall, JL Martini, P Melchior, P Mohr, JJ Nichol, RC Nord, B 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 Thomas, D Vikram, V Walker, AR AF Clampitt, J. Sanchez, C. Kwan, J. Krause, E. MacCrann, N. Park, Y. Troxel, M. A. Jain, B. Rozo, E. Rykoff, E. S. Wechsler, R. H. Blazek, J. Bonnett, C. Crocce, M. Fang, Y. Gaztanaga, E. Gruen, D. Jarvis, M. Miquel, R. Prat, J. Ross, A. J. Sheldon, E. Zuntz, J. Abbott, T. M. C. Abdalla, F. B. Armstrong, R. Becker, M. R. Benoit-Levy, A. Bernstein, G. M. Bertin, E. Brooks, D. Burke, D. L. Carnero Rosell, A. Kind, M. Carrasco Cunha, C. E. D'Andrea, C. B. da Costa, L. N. Desai, S. Diehl, H. T. Dietrich, J. P. Doel, P. Estrada, J. Evrard, A. E. Fausti Neto, A. Flaugher, B. Fosalba, P. Frieman, J. Gruendl, R. A. Honscheid, K. James, D. J. Kuehn, K. Kuropatkin, N. Lahav, O. Lima, M. March, M. Marshall, J. L. Martini, P. Melchior, P. Mohr, J. J. Nichol, R. C. Nord, B. 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. Thomas, D. Vikram, V. Walker, A. R. TI Galaxy-galaxy lensing in the Dark Energy Survey Science Verification data SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: weak; galaxies: haloes ID HALO OCCUPATION DISTRIBUTION; SHEAR POWER SPECTRA; DIGITAL SKY SURVEY; 100 SQUARE DEGREES; SDSS-III; COSMOLOGICAL CONSTRAINTS; INTRINSIC ALIGNMENTS; MAXIMUM-LIKELIHOOD; MATTER HALOES; DATA RELEASE AB We present galaxy-galaxy lensing results from 139 deg(2) of Dark Energy Survey (DES) Science Verification (SV) data. Our lens sample consists of red galaxies, known as redMaGiC, which are specifically selected to have a low photometric redshift error and outlier rate. The lensing measurement has a total signal-to-noise ratio of 29 over scales 0.09 < R < 15 Mpc h(-1), including all lenses over a wide redshift range 0.2 < z < 0.8. Dividing the lenses into three redshift bins for this constant moving number density sample, we find no evidence for evolution in the halo mass with redshift. We obtain consistent results for the lensing measurement with two independent shear pipelines, NGMIX and IM3SHAPE. We perform a number of null tests on the shear and photometric redshift catalogues and quantify resulting systematic uncertainties. Covariances from jackknife subsamples of the data are validated with a suite of 50 mock surveys. The result and systematic checks in this work provide a critical input for future cosmological and galaxy evolution studies with the DES data and redMaGiC galaxy samples. We fit a halo occupation distribution (HOD) model, and demonstrate that our data constrain the mean halo mass of the lens galaxies, despite strong degeneracies between individual HOD parameters. C1 [Clampitt, J.; Kwan, J.; Jain, B.; Fang, Y.; Jarvis, M.; Bernstein, G. M.; March, M.] Univ Pennsylvania, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Sanchez, C.; Bonnett, C.; Miquel, R.; Prat, J.] Barcelona Inst Sci ence & Technol, Inst Fisica Altes Energies IFAE, Campus UAB, E-08193 Barcelona, Spain. [Krause, E.; Rykoff, E. S.; Wechsler, R. H.; Gruen, D.; Becker, M. R.; Burke, D. L.] Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA. [MacCrann, N.; Troxel, M. A.; Zuntz, J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England. [Park, Y.; Rozo, E.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. [Park, Y.; Frieman, J.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Rykoff, E. S.; Wechsler, R. H.; Gruen, D.; Burke, D. L.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Wechsler, R. H.; Becker, M. R.] StanfordUniversity, Dept Phys, 382 Via PuebloMall, Stanford, CA 94305 USA. [Blazek, J.; Ross, A. J.; Honscheid, K.; Martini, P.] Ohio State Univ sity, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA. [Crocce, M.; Gaztanaga, E.; Fosalba, P.] CSIC, IEEC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans,S-N, E-08193 Barcelona, Spain. Institucio Catalana Recerca Estudis Avancats, E-08010 Barcelona, Spain. [Sheldon, E.] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA. [Abbott, T. M. C.; James, D. J.; Smith, R. C.; Walker, A. R.] Cerro Tololo Interamer Observ, Natl Optic Astron Observ, Casilla 603, La Serena, Chile. [Abdalla, F. B.; Benoit-Levy, A.; Brooks, D.; Doel, P.; Lahav, O.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Abdalla, F. B.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa. [Armstrong, R.; Melchior, P.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. [Benoit-Levy, A.; Bertin, E.] Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France. [Benoit-Levy, A.; Bertin, E.] Sorbonne Univ, UPMC Univ Paris 06, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Carnero Rosell, A.; da Costa, L. N.; Fausti Neto, A.; Sobreira, F.] Laboratorio Interinstituc Astron LIneA, Rua Gal Jos Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carnero Rosell, A.; da Costa, L. N.] Observatorio Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Kind, M. Carrasco; Gruendl, R. A.] Univ Illinois, Dept Astron, 1002 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. [D'Andrea, C. B.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [D'Andrea, C. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Desai, S.; Dietrich, J. P.; Mohr, J. J.] Ludwig Maximilians Univ Munchen, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Desai, S.; Dietrich, J. P.; Mohr, J. J.] Excellence Cluster Univ, Boltzmannstr 2, D-85748 Garching, Germany. [Diehl, H. T.; Estrada, J.; Flaugher, B.; Frieman, J.; Kuropatkin, N.; Scarpine, V.; Soares-Santos, M.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. [Evrard, A. E.; Sanchez, E.; Sevilla-Noarbe, I.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Evrard, A. E.; Schubnell, M.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Honscheid, K.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Kuehn, K.; Lima, M.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Kuehn, K.; Lima, M.] Univ Sao Paulo, Inst Fis, Departamento Fis Matemat, CP 66318, BR-05314970 Sao Paulo, Brazil. [Marshall, J. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamen, College Stn, TX 77843 USA. [Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Martini, P.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Mohr, J. J.] Max Planck Inst Extraterrestrial Phys, Giessenbachstrasse, D-85748 Garching, Germany. [Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England. [Sevilla-Noarbe, I.] Centro Investigac Energeticas Medioambient Tecnol, Madrid, Spain. [Suchyta, E.] Oak Ridge Natl Lab, Comp Sci & Math Div, Oak Ridge, TN 37831 USA. [Vikram, V.] Argonne Natl Lab, 9700 South Cass Ave, Lemont, IL 60439 USA. RP Clampitt, J (reprint author), Univ Pennsylvania, Dept Phys & Astron, Philadelphia, PA 19104 USA. EM clampitt@sas.upenn.edu FU US Department of Energy; US National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Center for Particle Cosmology; Warren Center at the University of Pennsylvania; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundayao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia e Tecnologia; Deutsche Forschungsgemeinschaft; Collaborating Institutions in the Dark Energy Survey; 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; 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; OzDES Membership Consortium FX Funding for the DES Projects has been provided by the US Department of Energy, the US National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Center for Particle Cosmology and the Warren Center at the University of Pennsylvania, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundayao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia e Tecnologia, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey.; The 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, Texas A&M University, and the OzDES Membership Consortium. NR 90 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 MAR PY 2017 VL 465 IS 4 BP 4204 EP 4218 DI 10.1093/mnras/stw2988 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EM2UC UT WOS:000395170200034 ER PT J AU Ostrovski, F McMahon, RG Connolly, AJ Lemon, CA Auger, MW Banerji, M Hung, JM Koposov, SE Lidman, CE Reed, SL Allam, S Benoit-Levy, A Bertin, E Brooks, D Buckley-Geer, E Rosell, AC Kind, MC Carretero, J Cunha, CE da Costa, LN Desai, S Diehl, HT Dietrich, JP Evrard, AE Finley, DA Flaugher, B Fosalba, P Frieman, J Gerdes, DW Goldstein, DA Gruen, D Gruendl, RA Gutierrez, G Honscheid, K James, DJ Kuehn, K Kuropatkin, N Lima, M Lin, H Maia, MAG Marshall, JL Martini, P Melchior, P Miquel, R Ogando, R Malagon, AP Reil, K Romer, K Sanchez, E Santiago, B Scarpine, V Sevilla-Noarbe, I Soares-Santos, M Sobreira, F Suchyta, E Tarle, G Thomas, D Tucker, DL Walker, AR AF Ostrovski, Fernanda McMahon, Richard G. Connolly, Andrew J. Lemon, Cameron A. Auger, Matthew W. Banerji, Manda Hung, Johnathan M. Koposov, Sergey E. Lidman, Christopher E. Reed, Sophie L. Allam, Sahar Benoit-Levy, Aurelien Bertin, Emmanuel Brooks, David Buckley-Geer, Elizabeth Rosell, Aurelio Carnero Kind, Matias Carrasco Carretero, Jorge Cunha, Carlos E. da Costa, Luiz N. Desai, Shantanu Diehl, H. Thomas Dietrich, Jorg P. Evrard, August E. Finley, David A. Flaugher, Brenna Fosalba, Pablo Frieman, Josh Gerdes, David W. Goldstein, Daniel A. Gruen, Daniel Gruendl, Robert A. Gutierrez, Gaston Honscheid, Klaus James, David J. Kuehn, Kyler Kuropatkin, Nikolay Lima, Marcos Lin, Huan Maia, Marcio A. G. Marshall, Jennifer L. Martini, Paul Melchior, Peter Miquel, Ramon Ogando, Ricardo Malagon, Andres Plazas Reil, Kevin Romer, Kathy Sanchez, Eusebio Santiago, Basilio Scarpine, Vic Sevilla-Noarbe, Ignacio Soares-Santos, Marcelle Sobreira, Flavia Suchyta, Eric Tarle, Gregory Thomas, Daniel Tucker, Douglas L. Walker, Alistair R. TI VDES J2325-5229 a z=2.7 gravitationally lensed quasar discovered using morphology-independent supervised machine learning SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: strong; methods: observational; methods: statistical; quasars: general ID DIGITAL SKY SURVEY; DARK ENERGY SURVEY; ACTIVE GALACTIC NUCLEI; 7TH DATA RELEASE; 3RD DATA RELEASE; MIDINFRARED SELECTION; CANDIDATE SELECTION; SDSS J1029+2623; ACCRETION DISK; FOLLOW-UP AB We present the discovery and preliminary characterization of a gravitationally lensed quasar with a source redshift z(s) = 2.74 and image separation of 2.9 arcsec lensed by a foreground z(l) = 0.40 elliptical galaxy. Since optical observations of gravitationally lensed quasars showthe lens system as a superposition of multiple point sources and a foreground lensing galaxy, we have developed a morphology-independent multi-wavelength approach to the photometric selection of lensed quasar candidates based on Gaussian Mixture Models (GMM) supervised machine learning. Using this technique and gi multicolour photometric observations from the Dark Energy Survey (DES), near-IR JK photometry from the VISTA Hemisphere Survey (VHS) and WISE mid-IR photometry, we have identified a candidate system with two catalogue components with i(AB) = 18.61 and i(AB) = 20.44 comprising an elliptical galaxy and two blue point sources. Spectroscopic follow-up with NTT and the use of an archival AAT spectrum show that the point sources can be identified as a lensed quasar with an emission line redshift of z = 2.739 +/- 0.003 and a foreground early-type galaxy with z = 0.400 +/- 0.002. We model the system as a single isothermal ellipsoid and find the Einstein radius theta(E) similar to 1.47 arcsec, enclosed mass M-enc similar to 4 x 10(11) M-circle dot and a time delay of similar to 52 d. The relatively wide separation, month scale time delay duration and high redshift make this an ideal system for constraining the expansion rate beyond a redshift of 1. C1 [Ostrovski, Fernanda; McMahon, Richard G.; Connolly, Andrew J.; Lemon, Cameron A.; Auger, Matthew W.; Banerji, Manda; Hung, Johnathan M.; Koposov, Sergey E.; Reed, Sophie L.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Ostrovski, Fernanda; McMahon, Richard G.; Lemon, Cameron A.; Banerji, Manda; Reed, Sophie L.] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England. [Ostrovski, Fernanda] Minist Educ Brazil, CAPES Fdn, BR-70040200 Brasilia, DF, Brazil. [Connolly, Andrew J.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Hung, Johnathan M.] Ctr Math Sci, DAMTP, Cambridge CB3 0WA, England. [Lidman, Christopher E.] Univ Wollongong, Sch Phys, Wollongong, NSW 2522, Australia. [Lidman, Christopher E.] Australian Astron Observ, N Ryde, NSW, Australia. [Buckley-Geer, Elizabeth; Diehl, H. Thomas; Finley, David A.; Flaugher, Brenna; Frieman, Josh; Gutierrez, Gaston; Kuropatkin, Nikolay; Lin, Huan; Soares-Santos, Marcelle; Tucker, Douglas L.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. [Benoit-Levy, Aurelien; Bertin, Emmanuel] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Benoit-Levy, Aurelien; Brooks, David] Univ London Univ Coll, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Benoit-Levy, Aurelien; Bertin, Emmanuel] UPMC Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Rosell, Aurelio Carnero; da Costa, Luiz N.; Maia, Marcio A. G.; Ogando, Ricardo; Santiago, Basilio; Sobreira, Flavia] Lab Interinst Astron LIneA, Rua Gal Jos Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Rosell, Aurelio Carnero; da Costa, Luiz N.; Maia, Marcio A. G.; Ogando, Ricardo; Santiago, Basilio; Sobreira, Flavia] Observ Nacl, Rua Gal Jos Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Kind, Matias Carrasco; Gruendl, Robert A.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Kind, Matias Carrasco; Gruendl, Robert A.] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA. [Carretero, Jorge; Fosalba, Pablo] Inst Ciencies Espai, IEEC CSIC, Campus UAB,Carrer Can Magrans S N, E-08193 Barcelona, Spain. [Carretero, Jorge; Miquel, Ramon] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain. [Cunha, Carlos E.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA. [Desai, Shantanu; Dietrich, Jorg P.] Excellence Cluster Univ, Boltzmannstr 2, D-85748 Garching, Germany. [Desai, Shantanu; Dietrich, Jorg P.] Ludwig Maximilians Univ Munchen, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Evrard, August E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Evrard, August E.; Gerdes, David W.; Tarle, Gregory] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Frieman, Josh] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Goldstein, Daniel A.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Goldstein, Daniel A.] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Gruen, Daniel; Reil, Kevin] SLAC Natl Accelerator Lab, Menlo Pk, Menlo Pk, CA 94025 USA. [Honscheid, Klaus] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA. [James, David J.; Walker, Alistair R.] Natl Optic Astron Observ, Cerro Tololo Inter Amer Observ, Casilla 603, La Serena, Chile. [Kuehn, Kyler] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Lima, Marcos] Univ Sao Paulo, Inst Fis, Dept Fis Mat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil. [Marshall, Jennifer L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Martini, Paul] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. [Melchior, Peter] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Miquel, Ramon] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Malagon, Andres Plazas] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Romer, Kathy] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England. [Sanchez, Eusebio; Sevilla-Noarbe, Ignacio] Ctr Invest Energet Medioambientales & Technol CIE, Madrid, Spain. [Santiago, Basilio] Univ Fed Rio Grande do Sul, Inst Fis, Caixa Postal 15051, BR-91501970 Porto Alegre, RS, Brazil. [Sobreira, Flavia] Univ Estadual Paulista, ICTP Souh Amer Inst Fundamental Res, Inst Fis Teor, Sao Paulo, Brazil. [Suchyta, Eric] Oak Ridge Natl Lab, Comp Sci & Math Div, Oak Ridge, TN 37831 USA. [Thomas, Daniel] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. RP Ostrovski, F (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.; Ostrovski, F (reprint author), Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England.; Ostrovski, F (reprint author), Minist Educ Brazil, CAPES Fdn, BR-70040200 Brasilia, DF, Brazil. EM fostrovski@ast.cam.ac.uk RI Ogando, Ricardo/A-1747-2010 OI Ogando, Ricardo/0000-0003-2120-1154 FU CAPES (the Science without Borders programme); Cambridge Commonwealth Trust; UK Science and Technology Research Council (STFC); Raymond and Beverly Sackler visiting fellowship at the Institute of Astronomy; 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; Fundayao Carlos Chagas Filho de Amparo Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; University of California at Santa Cruz; University of Cambridge; Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid; University of Chicago; University College London; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) Zurich; Fermi National Accelerator Laboratory; University of Illinois at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory; Ludwig-Maximilians Universitar Munchen; 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; OzDES Membership Consortium; National Science Foundation [AST-1138766]; MINECO [AYA2012-39559, ESP-201348274, FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; European Research Council under the European Union [240672, 291329, 306478]; ESO [179.A-2010, 096.A-0411]; Australian Astronomical Observatory [A/2013A/018, A/2013B/001] FX FO is supported jointly by CAPES (the Science without Borders programme) and the Cambridge Commonwealth Trust.; RGM, CAL, MWA, MB, SLR acknowledge the support of UK Science and Technology Research Council (STFC).; AJC acknowledges the support of a Raymond and Beverly Sackler visiting fellowship at the Institute of Astronomy.; 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, Fundayao Carlos Chagas Filho de Amparo 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 DES.; 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 Universitar 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, Texas A&M University, and the OzDES Membership Consortium.; 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, ESP-201348274, 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.; The analysis presented here is based on observations obtained as part of the VISTA Hemisphere Survey, ESO Programme, 179.A-2010 (PI: McMahon) and ESO Programme 096.A-0411.; This work was based in part on data acquired through the Australian Astronomical Observatory, under programmes A/2013A/018 and A/2013B/001. NR 76 TC 0 Z9 0 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 MAR PY 2017 VL 465 IS 4 BP 4325 EP 4334 DI 10.1093/mnras/stw2958 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EM2UC UT WOS:000395170200041 ER PT J AU McLaughlin, BM Bizau, JM Cubaynes, D Guilbaud, S Douix, S Al Shorman, MM El Ghazaly, MOA Sakho, I Gharaibeh, MF AF McLaughlin, B. M. Bizau, J. -M. Cubaynes, D. Guilbaud, S. Douix, S. Al Shorman, M. M. El Ghazaly, M. O. A. Sakho, I. Gharaibeh, M. F. TI K-shell photoionizationof O-4 (+) and O-5 (+) ions: experiment and theory SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE atomic data; atomic processes ID X-RAY SPECTROSCOPY; DIELECTRONIC SATELLITE SPECTRA; LI-LIKE IONS; BE-LIKE OXYGEN; INTERSTELLAR-MEDIUM; EXCITED-STATES; XMM-NEWTON; CONFIGURATION-INTERACTION; ISOELECTRONIC SEQUENCE; CROSS-SECTIONS AB Absolute cross-sections for the K-shell photoionization of Be-like (O-4 (+)) and Li-like (O-5 (+)) atomic oxygen ions were measured for the first time (in their respective K-shell regions) by employing the ion-photon merged-beam technique at the SOLEIL synchrotron-radiation facility in Saint-Aubin, France. High-resolution spectroscopy with E/Delta E approximate to 3200 (approximate to 170 meV, full width at half-maximum) was achieved with photon energy from 550 to 670 eV. Rich resonance structure observed in the experimental spectra is analysed using the R-matrix with pseudo-states (RMPS) method. Results are also compared with the screening constant by unit nuclear charge (SCUNC) calculations. We characterize and identify the strong 1s -> 2p resonances for both ions and the weaker 1s -> np resonances (n >= 3) observed in the K-shell spectra of O4 +. C1 [McLaughlin, B. M.] Queens Univ Belfast, Sch Math & Phys, Ctr Theoret Atom & Mol Phys CTAMOP, Belfast BT7 1NN, Antrim, North Ireland. [McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, ITAMP, MS-14, Cambridge, MA 02138 USA. [Bizau, J. -M.; Cubaynes, D.; Guilbaud, S.] Univ Paris Saclay, Univ Paris Sud, CNRS UMR 8214, ISMO, F-91405 Orsay, France. [Bizau, J. -M.; Cubaynes, D.; Douix, S.] Synchrotron SOLEIL, St Aubin BP 48, F-91192 Gif Sur Yvette, France. [Al Shorman, M. M.] Tafila Tech Univ, Dept Appl Phys, Fac Sci, Tafila 66110, Jordan. [El Ghazaly, M. O. A.] CALTECH, Jet Prop Lab, Astrophys & Space Sci Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Sakho, I.] Univ Assane Seck Ziguinchor, Dept Phys, UFR Sci & Technol, Ziguinchor, Senegal. [Gharaibeh, M. F.] Qatar Univ, Dept Math Stat & Phys, POB 2713, Doha, Qatar. [Gharaibeh, M. F.] Jordan Univ Sci, Dept Phys, Technol, Irbid 22110, Jordan. RP McLaughlin, BM (reprint author), Queens Univ Belfast, Sch Math & Phys, Ctr Theoret Atom & Mol Phys CTAMOP, Belfast BT7 1NN, Antrim, North Ireland.; McLaughlin, BM (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, MS-14, Cambridge, MA 02138 USA.; Bizau, JM (reprint author), Univ Paris Saclay, Univ Paris Sud, CNRS UMR 8214, ISMO, F-91405 Orsay, France.; Bizau, JM (reprint author), Synchrotron SOLEIL, St Aubin BP 48, F-91192 Gif Sur Yvette, France.; Gharaibeh, MF (reprint author), Qatar Univ, Dept Math Stat & Phys, POB 2713, Doha, Qatar. EM bmclaughlin899@btinternet.com; jean-marc.bizau@u-psud.fr; mgharaibeh@qu.edu.qa FU U.S. National Science Foundation through ITAMP at the Harvard-Smithsonian Center for Astrophysics; Queen's University Belfast for the award of a Visiting Research Fellowship (VRF); Qatar University [QUSG-CAS-DMSP-14/15-4]; RTRA network Triangle de la Physique FX The authors would like to thank the SOLEIL staff, in particular, J. Bozek and S. Nandi, for their helpful assistance during the measurements. We thank F. Nicastro for the provision of the Chandra spectra for the blazar Mrk 421 and illuminating discussions on the differences with the Chandra observations. T. R. Kallman, at Nasa Goddard, J. C. Raymond and R. K. Smith at the HarvardSmithsonian Center for Astrophysics are also thanked for discussions on the astrophysical applications. BMMcL acknowledges support from the U.S. National Science Foundation through a grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics, the RTRA network Triangle de la Physique and Queen's University Belfast for the award of a Visiting Research Fellowship (VRF). MFG acknowledges Qatar University for funding support through the startup grant No.QUSG-CAS-DMSP-14/15-4. The R-matrix computational work was performed at the National EnergyResearch Scientific Computing Center (NERSC), Berkeley, CA, USA, and at the High Performance Computing Center Stuttgart (HLRS) of the University of Stuttgart, Stuttgart, Germany. Grants of computational time at the NERSC and at the HLRS are gratefully acknowledged. NR 93 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 MAR PY 2017 VL 465 IS 4 BP 4690 EP 4702 DI 10.1093/mnras/stw2998 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EM2UC UT WOS:000395170200067 ER PT J AU Alam, S Miyatake, H More, S Ho, S Mandelbaum, R AF Alam, Shadab Miyatake, Hironao More, Surhud Ho, Shirley Mandelbaum, Rachel TI Testing gravity on large scales by combining weak lensing with galaxy clustering using CFHTLenS and BOSS CMASS SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitation; galaxies: statistics; cosmological parameters; large-scale structure of Universe ID DIGITAL SKY SURVEY; OSCILLATION SPECTROSCOPIC SURVEY; BARYON ACOUSTIC-OSCILLATIONS; DARK-MATTER HALOES; COSMOLOGICAL PARAMETER CONSTRAINTS; REDSHIFT-SPACE DISTORTIONS; POWER-SPECTRUM ANALYSIS; SDSS-III; DATA RELEASE; GROWTH-RATE AB We measure a combination of gravitational lensing, galaxy clustering and redshift-space distortions (RSDs) called E-G. The quantity EG probes both parts of metric potential and is insensitive to galaxy bias and sigma(8). These properties make it an attractive statistic to test lambda cold dark matter, general relativity and its alternate theories. We have combined CMASS Data Release 11 with CFHTLenS and recent measurements of beta from RSD analysis, and find E-G(z = 0.57) = 0.42 +/- 0.056, a 13 per cent measurement in agreement with the prediction of general relativity EG(z = 0.57) = 0.396 +/- 0.011 using the Planck 2015 cosmological parameters. We have corrected our measurement for various observational and theoretical systematics. Our measurement is consistent with the first measurement of EG using cosmic microwave background lensing in place of galaxy lensing at small scales, but shows 2.8 sigma tension when compared with their final results including large scales. This analysis with future surveys will provide improved statistical error and better control over systematics to test general relativity and its alternate theories. C1 [Alam, Shadab; Ho, Shirley; Mandelbaum, Rachel] Carnegie Mellon Univ, Dept Phys, 5000 Forbes Ave, Pittsburgh, PA 15213 USA. [Alam, Shadab; Ho, Shirley; Mandelbaum, Rachel] Carnegie Mellon Univ, McWilliams Ctr Cosmol, 5000 Forbes Ave, Pittsburgh, PA 15213 USA. [Alam, Shadab] Univ Edinburgh, Royal Observ, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. [Miyatake, Hironao] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Miyatake, Hironao; More, Surhud] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Chiba 2778583, Japan. [Miyatake, Hironao] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. RP Alam, S (reprint author), Carnegie Mellon Univ, Dept Phys, 5000 Forbes Ave, Pittsburgh, PA 15213 USA.; Alam, S (reprint author), Carnegie Mellon Univ, McWilliams Ctr Cosmol, 5000 Forbes Ave, Pittsburgh, PA 15213 USA.; Alam, S (reprint author), Univ Edinburgh, Royal Observ, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. EM salam@roe.ac.uk FU NASA [12-EUCLID11-0004]; NSF [AST1412966, AST1517593]; DOE; Japan Society for the Promotion of Science (JSPS) Research Fellowships for Young Scientists; Jet Propulsion Laboratory, California Institute of Technology; National Aeronautics and Space Administration; Department of Energy Early Career Award programme; Canadian Space Agency FX We would like to thank Sukhdeep Singh for many insightful discussions during the course of this project. We would also like to thank the anonymous referee for useful comments. SA and SH are supported by NASA grants 12-EUCLID11-0004 and NSF AST1412966 for this work. SH is also supported by DOE and NSF AST1517593. HM acknowledges the support of Japan Society for the Promotion of Science (JSPS) Research Fellowships for Young Scientists and the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. RM acknowledges the support of the Department of Energy Early Career Award programme.; This work is based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, at the Canada-France-Hawaii Telescope (CFHT) that is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France and the University of Hawaii. This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. The CFHTLenS data processing was made possible thanks to significant computing support from the NSERC Research Tools and Instruments grant programme. NR 116 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 MAR PY 2017 VL 465 IS 4 BP 4853 EP 4865 DI 10.1093/mnras/stw3056 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EM2UC UT WOS:000395170200078 ER PT J AU Dell'Elce, L Baresi, N Naidu, SP Benner, LAM Scheeres, DJ AF Dell'Elce, L. Baresi, N. Naidu, S. P. Benner, L. A. M. Scheeres, D. J. TI Numerical investigation of the dynamical environment of 65803 Didymos SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Didymos; AIDA mission; Restricted three-body problem ID BINARY ASTEROIDS; RADAR; SPACECRAFT; ORBITS AB The Asteroid Impact & Deflection Assessment (AIDA) mission is planning to visit the Didymos binary system in 2022 in order to perform the first demonstration ever of the kinetic impact technique. Binary asteroids are an ideal target for this since the deflection of the secondary body can be accurately measured by a satellite orbiting in the system. However, these binaries offer an extremely rich dynamical environment whose accurate investigation through analytical approaches is challenging at best and requires a significant number of restrictive assumptions. For this reason, a numerical investigation of the dynamical environment in the vicinity of the Didymos system is offered in this paper. After computing various families of periodic orbits, their robustness is assessed in a high-fidelity environment consisting of the perturbed restricted full three-body problem. The results of this study suggest that several nominally stable trajectories, including the triangular libration points, should not be considered as safe as a state vector perturbation may cause the spacecraft to drift from the nominal orbit and possibly impact one of the primary bodies within a few days. Nonetheless, there exist two safe solutions, namely terminator and interior retrograde orbits. The first one is adequate for observation purposes of the entire system and for communications. The second one is more suitable to perform close investigations of the primary body. (C) 2016 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Dell'Elce, L.] Univ Liege, B-4000 Liege, Belgium. [Baresi, N.; Scheeres, D. J.] Univ Colorado, Boulder, CO 80309 USA. [Naidu, S. P.; Benner, L. A. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Dell'Elce, L (reprint author), Univ Liege, B-4000 Liege, Belgium. EM lamberto.dellelce@ulg.ac.be FU Belgian National Fund for Scientific Research (FNRS); John Hopkins University Applied Physics Laboratory FX This work was partially supported by the Belgian National Fund for Scientific Research (FNRS) and by the John Hopkins University Applied Physics Laboratory. NR 25 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD MAR 1 PY 2017 VL 59 IS 5 BP 1304 EP 1320 DI 10.1016/j.asr.2016.12.018 PG 17 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA EK6WF UT WOS:000394066000010 ER PT J AU Clebone, A Burian, BK Watkins, SC Galvez, JA Lockman, JL Heitmiller, ES AF Clebone, Anna Burian, Barbara K. Watkins, Scott C. Galvez, Jorge A. Lockman, Justin L. Heitmiller, Eugenie S. CA Soc Pediat Anesthesia Quality Safe TI The Development and Implementation of Cognitive Aids for Critical Events in Pediatric Anesthesia: The Society for Pediatric Anesthesia Critical Events Checklists SO ANESTHESIA AND ANALGESIA LA English DT Article ID RANDOMIZED CONTROLLED-TRIAL; CARDIOPULMONARY-RESUSCITATION; NEONATAL RESUSCITATION; CRISIS CHECKLISTS; CARDIAC-ARREST; SIMULATION; GUIDELINES; EMERGENCIES; CARE; RETENTION AB Cognitive aids such as checklists are commonly used in modern operating rooms for routine processes, and the use of such aids may be even more important during critical events. The Quality and Safety Committee of the Society for Pediatric Anesthesia (SPA) has developed a set of critical-event checklists and cognitive aids designed for 3 purposes: (1) as a repository of the latest evidence-based and expert opinion-based information to guide response and management of critical events, (2) as a source of just-in-time information during critical events, and (3) as a method to facilitate a shared understanding of required actions among team members during a critical event. Committee members, who represented children's hospitals from across the nation, used the recent literature and established guidelines (where available) and incorporated the expertise of colleagues at their institutions to develop these checklists, which included relevant factors to consider and steps to take in response to critical events. Human factors principles were incorporated to enhance checklist usability, facilitate error-free accomplishment, and ensure a common approach to checklist layout, formatting, structure, and design. The checklists were made available in multiple formats: a PDF version for easy printing, a mobile application, and at some institutions, a Web-based application using the anesthesia information management system. After the checklists were created, training commenced, and plans for validation were begun. User training is essential for successful implementation and should ideally include explanation of the organization of the checklists; familiarization of users with the layout, structure, and formatting of the checklists; coaching in how to use the checklists in a team environment; reviewing of the items; and simulation of checklist use. Because of the rare and unpredictable nature of critical events, clinical trials that use crisis checklists are difficult to conduct; however, recent and future simulation studies with adult checklists provide a promising avenue for future validation of the SPA checklists. This article will review the developmental steps in producing the SPA crisis checklists, including creation of content, incorporation of human factors elements, and validation in simulation. Critical-events checklists have the potential to improve patient care during emergency events, and it is hoped that incorporating the elements presented in this article will aid in successful implementation of these essential cognitive aids. C1 [Clebone, Anna] Univ Chicago, Dept Anesthesia & Crit Care, 5841 S Maryland Ave, Chicago, IL 60637 USA. [Burian, Barbara K.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Watkins, Scott C.] Vanderbilt Univ, Med Ctr, Dept Anesthesiol, Nashville, TN USA. [Galvez, Jorge A.; Lockman, Justin L.] Univ Penn, Childrens Hosp Philadelphia, Perelman Sch Med, Dept Anesthesiol & Crit Care Med, Philadelphia, PA 19104 USA. [Heitmiller, Eugenie S.] Childrens Natl Hlth Syst, Div Anesthesiol Pain & Perioperat Med, Washington, DC USA. RP Clebone, A (reprint author), Univ Chicago, Dept Anesthesia & Crit Care, 5841 S Maryland Ave, Chicago, IL 60637 USA. EM aclebone@dacc.uchicago.edu NR 35 TC 0 Z9 0 U1 1 U2 1 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA TWO COMMERCE SQ, 2001 MARKET ST, PHILADELPHIA, PA 19103 USA SN 0003-2999 J9 ANESTH ANALG JI Anesth. Analg. PD MAR PY 2017 VL 124 IS 3 BP 900 EP 907 DI 10.1213/ANE.0000000000001746 PG 8 WC Anesthesiology SC Anesthesiology GA EK9QX UT WOS:000394260100031 PM 28079584 ER PT J AU Roa, J Pelaez, J AF Roa, Javier Pelaez, Jesus TI The theory of asynchronous relative motion I: time transformations and nonlinear corrections SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY LA English DT Article DE Relative motion; Nonlinear effects; Time transformations; Regularization; Stability; Clohessy-Wiltshire solution ID ELLIPTIC RENDEZVOUS PROBLEM; STATE TRANSITION MATRIX; REFERENCE ORBIT; KEPLER MOTION; BODY PROBLEM; PERTURBATIONS; EQUATIONS; ELEMENTS; REGULARIZATION AB Using alternative independent variables in lieu of time has important advantages when propagating the partial derivatives of the trajectory. This paper focuses on spacecraft relative motion, but the concepts presented here can be extended to any problem involving the variational equations of orbital motion. A usual approach for modeling the relative dynamics is to evaluate how the reference orbit changes when modifying the initial conditions slightly. But when the time is a mere dependent variable, changes in the initial conditions will result in changes in time as well: a time delay between the reference and the neighbor solution will appear. The theory of asynchronous relative motion shows how the time delay can be corrected to recover the physical sense of the solution and, more importantly, how this correction can be used to improve significantly the accuracy of the linear solutions to relative motion found in the literature. As an example, an improved version of the Clohessy-Wiltshire (CW) solution is presented explicitly. The correcting terms are extremely compact, and the solution proves more accurate than the second and even third order CW equations for long propagations. The application to the elliptic case is also discussed. The theory is not restricted to Keplerian orbits, as it holds under any perturbation. To prove this statement, two examples of realistic trajectories are presented: a pair of spacecraft orbiting the Earth and perturbed by a realistic force model; and two probes describing a quasi-periodic orbit in the Jupiter-Europa system subject to third-body perturbations. The numerical examples show that the new theory yields reductions in the propagation error of several orders of magnitude, both in position and velocity, when compared to the linear approach. C1 [Roa, Javier; Pelaez, Jesus] Tech Univ Madrid UPM, Space Dynam Grp, Pza Cardenal Cisneros 3, Madrid 28040, Spain. [Roa, Javier] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Roa, J (reprint author), Tech Univ Madrid UPM, Space Dynam Grp, Pza Cardenal Cisneros 3, Madrid 28040, Spain.; Roa, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM javier.roa@upm.es FU Spanish Ministry of Economy and Competitiveness [ESP2013-41634-P]; Spanish Government; "La Caixa" FX This work was carried out within the framework of the research project entitled "Dynamical Analysis, Advanced Orbital Propagation, and Simulation of Complex Space Systems" (ESP2013-41634-P) supported by the Spanish Ministry of Economy and Competitiveness. Authors thank the Spanish Government for its support and H. Urrutxua for reading the manuscript carefully and making valuable suggestions. J. Roa especially thanks "La Caixa" for his doctoral fellowship. The comments from an anonymous reviewer greatly improved the quality of the paper. NR 52 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0923-2958 EI 1572-9478 J9 CELEST MECH DYN ASTR JI Celest. Mech. Dyn. Astron. PD MAR PY 2017 VL 127 IS 3 BP 301 EP 330 DI 10.1007/s10569-016-9728-6 PG 30 WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications SC Astronomy & Astrophysics; Mathematics GA EL0CI UT WOS:000394290000003 ER PT J AU Roa, J Pelaez, J AF Roa, Javier Pelaez, Jesus TI The theory of asynchronous relative motion II: universal and regular solutions SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY LA English DT Article DE Relative motion; Elliptic rendezvous; Hyperbolic rendezvous; Kustaanheimo-Stiefel transformation; Sperling-Burdet regularization; Sundman transformation; Stumpff functions ID 2-BODY PROBLEM; RENDEZVOUS PROBLEM; ORBITAL DYNAMICS; KEPLER EQUATION; BODY PROBLEM; TRANSFORMATION; VARIABLES; FORM; ELEMENTS AB Two fully regular and universal solutions to the problem of spacecraft relative motion are derived from the Sperling-Burdet (SB) and the Kustaanheimo-Stiefel (KS) regularizations. There are no singularities in the resulting solutions, and their form is not affected by the type of reference orbit (circular, elliptic, parabolic, or hyperbolic). In addition, the solutions to the problem are given in compact tensorial expressions and directly referred to the initial state vector of the leader spacecraft. The SB and KS formulations introduce a fictitious time by means of the Sundman transformation. Because of using an alternative independent variable, the solutions are built based on the theory of asynchronous relative motion. This technique simplifies the required derivations. Closed-form expressions of the partial derivatives of orbital motion with respect to the initial state are provided explicitly. Numerical experiments show that the performance of a given representation of the dynamics depends strongly on the time transformation, whereas it is virtually independent from the choice of variables to parameterize orbital motion. In the circular and elliptic cases, the linear solutions coincide exactly with the results obtained with the Clohessy-Wiltshire and Yamanaka-Ankersen state-transition matrices. Examples of relative orbits about parabolic and hyperbolic reference orbits are also presented. Finally, the theory of asynchronous relative motion provides a simple mechanism to introduce nonlinearities in the solution, improving its accuracy. C1 [Roa, Javier; Pelaez, Jesus] Tech Univ Madrid UPM, Space Dynam Grp, Pza Cardenal Cisneros 3, Madrid 28040, Spain. [Roa, Javier] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Roa, J (reprint author), Tech Univ Madrid UPM, Space Dynam Grp, Pza Cardenal Cisneros 3, Madrid 28040, Spain.; Roa, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM javier.roa@upm.es FU Spanish Ministry of Economy and Competitiveness [ESP2013-41634-P]; Spanish Government; "La Caixa" FX This work was carried out within the framework of the research project entitled "Dynamical Analysis, Advanced Orbital Propagation, and Simulation of Complex Space Systems" (ESP2013-41634-P) supported by the Spanish Ministry of Economy and Competitiveness. Authors thank Spanish Government for its support. J. Roa especially thanks "La Caixa" for his doctoral fellowship, and J. L. Gonzalo and H. Urrutxua for stimulating discussions about the Stumpff functions. The comments and suggestions from two anonymous reviewers are acknowledged. NR 44 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0923-2958 EI 1572-9478 J9 CELEST MECH DYN ASTR JI Celest. Mech. Dyn. Astron. PD MAR PY 2017 VL 127 IS 3 BP 343 EP 368 DI 10.1007/s10569-016-9730-z PG 26 WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications SC Astronomy & Astrophysics; Mathematics GA EL0CI UT WOS:000394290000005 ER PT J AU Arkoosh, MR Van Gaest, AL Strickland, SA Hutchinson, GP Krupkin, AB Dietrich, JP AF Arkoosh, Mary R. Van Gaest, Ahna L. Strickland, Stacy A. Hutchinson, Greg P. Krupkin, Alex B. Dietrich, Joseph P. TI Alteration of thyroid hormone concentrations in juvenile Chinook salmon (Oncorhynchus tshawytscha) exposed to polybrominated diphenyl ethers, BDE-47 and BDE-99 SO CHEMOSPHERE LA English DT Article DE PBDE; Chinook salmon; Thyroid hormones; T3, T4; Endocrine disruption ID BROMINATED FLAME RETARDANTS; ENDOCRINE DISRUPTION; ORGANIC POLLUTANTS; DIETARY EXPOSURE; FATHEAD MINNOWS; COLUMBIA RIVER; PBDES; FISH; TRANSTHYRETIN; ZEBRAFISH AB Polybrominated diphenyl ethers (PBDEs) have been used as flame-retardants in consumer products and are currently detected in salmon globally. The two most predominant PBDE congeners found in salmon are BDE-47 (2,2',4,4'-tetrabromodiphenyl ether) and BDE-99 (2,2',4,4',5-pentabromodiphenyl ether). In the present study, groups of juvenile Pacific Chinook salmon were fed five environmentally relevant concentrations of either BDE-47 (0.3-552 ng total PBDEs/g food), BDE-99 (0.3-580 ng total PBDEs/g food), or nearly equal mixtures of both congeners (0.7-690 ng total PBDEs/g food) for 39-40 days. The concentrations of circulating total thyroid hormones, thyroxine (T-4) and 3,5,3'-triiodothyronine (T-3), were measured using a hormone-specific time-resolved fluoroimmunoassay to determine if PBDE exposure disrupts the hypothalamic-pituitary-thyroid endocrine axis. The concentrations of both circulating T-4 and T-3 were altered in juvenile salmon by dietary uptake of BDE-99. Exposure to BDE-47 did not alter either T-3 or T-4 circulating hormone concentrations. However, exposure to a mixture of BDE-47 and BDE-99 reduced T-3 in fish with lower concentrations of total whole body PBDEs than with either congener alone at equivalent PBDE whole body concentrations. Accordingly, the disruption of PBDEs on circulating thyroid hormone concentrations has the potential to impact a number of critical functions in juvenile salmon including growth, parr-smolt transformation, and immunological processes. Published by Elsevier Ltd. C1 [Arkoosh, Mary R.; Dietrich, Joseph P.] NOAA, Environm & Fisheries Sci Div, Northwest Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2032 South East OSU Dr, Newport, OR 97365 USA. [Van Gaest, Ahna L.; Strickland, Stacy A.; Hutchinson, Greg P.; Krupkin, Alex B.] NOAA, Frank Orth & Associates, Northwest Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2032 South East OSU Dr, Newport, OR 97365 USA. RP Arkoosh, MR (reprint author), NOAA, Environm & Fisheries Sci Div, Northwest Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2032 South East OSU Dr, Newport, OR 97365 USA. EM mary.arkoosh@noaa.gov FU NOAA; US EPA, Region 10, Puget Sound Science and Technical Studies Assistance Program [EPA-R10-PS-1004, 13-923270-01] FX Funds for this work were provided by NOAA and US EPA, Region 10, Puget Sound Science and Technical Studies Assistance Program; EPA-R10-PS-1004, Federal Grant No. 13-923270-01. We thank Dr. Andrew Dittman from NOAA's Northwest Fisheries Science Center for determining the concentrations of total T3 and T4 in the plasma samples. NR 55 TC 0 Z9 0 U1 7 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0045-6535 EI 1879-1298 J9 CHEMOSPHERE JI Chemosphere PD MAR PY 2017 VL 171 BP 1 EP 8 DI 10.1016/j.chemosphere.2016.12.035 PG 8 WC Environmental Sciences SC Environmental Sciences & Ecology GA EK4XL UT WOS:000393931100001 PM 28006665 ER PT J AU Drusch, M Moreno, J Del Bello, U Franco, R Goulas, Y Huth, A Kraft, S Middleton, EM Miglietta, F Mohammed, G Nedbal, L Rascher, U Schttemeyer, D Verhoef, W AF Drusch, Matthias Moreno, Jose Del Bello, Umberto Franco, Raffaella Goulas, Yves Huth, Andreas Kraft, Stefan Middleton, Elizabeth M. Miglietta, Franco Mohammed, Gina Nedbal, Ladislav Rascher, Uwe Schttemeyer, Dirk Verhoef, Wout TI The FLuorescence EXplorer Mission Concept-ESA's Earth Explorer 8 SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Fluorescence; remote sensing; spectrometry ID INDUCED CHLOROPHYLL FLUORESCENCE; PHOTOSYNTHESIS AB In November 2015, the FLuorescence EXplorer (FLEX) was selected as the eighth Earth Explorer mission of the European Space Agency. The tandem mission concept will provide measurements at a spectral and spatial resolution enabling the retrieval and interpretation of the full chlorophyll fluorescence spectrum emitted by the terrestrial vegetation. This paper provides a mission concept overview of the scientific goals, the key objectives related to fluorescence, and the requirements guaranteeing the fitness for purpose of the resulting scientific data set. We present the mission design at the time of selection, i.e., at the end of project phase Phase A/B1, as developed by two independent industrial consortia. The mission concepts both rely on a single payload Fluorescence Imaging Spectrometer, covering the spectral range from 500 to 780 nm. In the oxygen absorption bands, its spectral resolution will be 0.3 nm with a spectral sampling interval of 0.1 nm. The swath width of the spectrometer is 150 km and the spatial resolution will be 300 x 300 m(2). The satellite will fly in tandem with Sentinel-3 providing different and complementary measurements with a temporal collocation of 6 to 15 s. The FLEX launch is scheduled for 2022. C1 [Drusch, Matthias; Del Bello, Umberto; Franco, Raffaella; Kraft, Stefan; Schttemeyer, Dirk] European Space Agcy, Miss Sci Div, NL-2200 AG Noordwijk, Netherlands. [Moreno, Jose] Univ Valencia, Valencia 46100, Spain. [Goulas, Yves] Ecole Polytech, Lab Meteorol Dynam, F-91128 Palaiseau, France. [Huth, Andreas] UFZ Leipzig Halle GmbH, D-04318 Leipzig, Germany. [Middleton, Elizabeth M.] Natl Aeronaut & Space Adm, Greenbelt, MD 21077 USA. [Miglietta, Franco] CNR, I-40129 Bologna, Italy. [Mohammed, Gina] P&M Technol, Sault Ste, Marie, ON P6A 6S7, Canada. [Nedbal, Ladislav; Rascher, Uwe] Forschungszentrum Julich, D-52428 Julich, Germany. [Verhoef, Wout] Univ Twente, NL-7500 AE Enschede, Netherlands. RP Drusch, M; Del Bello, U; Franco, R; Kraft, S; Schttemeyer, D (reprint author), European Space Agcy, Miss Sci Div, NL-2200 AG Noordwijk, Netherlands.; Moreno, J (reprint author), Univ Valencia, Valencia 46100, Spain.; Goulas, Y (reprint author), Ecole Polytech, Lab Meteorol Dynam, F-91128 Palaiseau, France.; Huth, A (reprint author), UFZ Leipzig Halle GmbH, D-04318 Leipzig, Germany.; Middleton, EM (reprint author), Natl Aeronaut & Space Adm, Greenbelt, MD 21077 USA.; Miglietta, F (reprint author), CNR, I-40129 Bologna, Italy.; Mohammed, G (reprint author), P&M Technol, Sault Ste, Marie, ON P6A 6S7, Canada.; Mohammed, G; Nedbal, L; Rascher, U (reprint author), Forschungszentrum Julich, D-52428 Julich, Germany.; Verhoef, W (reprint author), Univ Twente, NL-7500 AE Enschede, Netherlands. EM matthias.drusch@esa.int; jose.moreno@uv.es; umbertodelbello@esa.int; raffaella.franco@esa.int; yves.goulas@lmd.polytechnique.fr; andreas.huth@ufz.de; stefan.kraft@esa.int; elizabeth.m.middleton@nasa.gov; f.miglietta@ibimet.cnr.it; gina.mohammed@pmtech.ca; l.nedbal@fz-juelich.de; u.rascher@fz-juelich.de; dirk.schuettemeyer@esa.int; w.verhoef@utwente.nl NR 25 TC 0 Z9 0 U1 2 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD MAR PY 2017 VL 55 IS 3 BP 1273 EP 1284 DI 10.1109/TGRS.2016.2621820 PG 12 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA EN6IC UT WOS:000396106700005 ER PT J AU Dinnat, EP Brucker, L AF Dinnat, Emmanuel P. Brucker, Ludovic TI Improved Sea Ice Fraction Characterization for L-Band Observations by the Aquarius Radiometers SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Aquarius; L-band; microwave radiometry; ocean; sea ice; Soil Moisture Active Passive (SMAP) ID RADIOMETER/SCATTEROMETER OBSERVATIONS; SALINITY RETRIEVALS; POLAR-REGIONS; MISSION; IMPACT AB Radiometers operating at L-band (1.4 GHz) are used to retrieve sea surface salinity over ice-free oceans and have been used recently to study the cryosphere. One hindrance of their use in the high latitudes is the preponderance of mixed scenes, where seawater and sea ice are both present in the sensor's field of view (FOV). Accurately characterizing the scene is crucial for oceanographic and cryospheric applications. To that end, a sea ice fraction model, composed of passive microwave sea ice concentration retrievals and an instrument simulator that integrates radiative power coming from all around the antenna, is used. We investigate the model currently used operationally to derive the ice fraction affecting the Aquarius observations and show that it can be significantly improved. On the one hand, the current model tends to overestimate sea ice fraction in the marginal ice zone where observations are used for salinity retrievals. On the other hand, the current model underestimates ice fraction within the ice pack where observations are used to derive sea ice properties. For the northern hemisphere, we also find evidence of the sea ice type impact on L-band radiometric observations. We present a model to derive sea ice fractions that are in better agreement with Aquarius radiometric observations using the Advanced Microwave Scanning Radiometer 2 Bootstrap algorithm for sea ice concentration and using high-resolution integration over the sensor's FOV. C1 [Dinnat, Emmanuel P.] Chapman Univ, Ctr Excellence Earth Syst Modeling & Observat, Orange, CA 92866 USA. [Dinnat, Emmanuel P.; Brucker, Ludovic] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Brucker, Ludovic] Universities Space Res Assoc, Goddard Earth Sci Technol & Res Studies & Investi, Columbia, MD 21044 USA. RP Dinnat, EP (reprint author), Chapman Univ, Ctr Excellence Earth Syst Modeling & Observat, Orange, CA 92866 USA.; Dinnat, EP (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. EM emmanuel.dinnat@nasa.gov RI Brucker, Ludovic/A-8029-2010 OI Brucker, Ludovic/0000-0001-7102-8084 FU National Aeronautics and Space Administration [NNX14AR31G, NNX14AN46G] FX This work was supported by the National Aeronautics and Space Administration under Grants NNX14AR31G (E.D.) and NNX14AN46G (L.B.). NR 32 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 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD MAR PY 2017 VL 55 IS 3 BP 1285 EP 1304 DI 10.1109/TGRS.2016.2622011 PG 20 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA EN6IC UT WOS:000396106700006 ER PT J AU Lei, N Xiong, XX AF Lei, Ning Xiong, Xiaoxiong TI Impacts of the Angular Dependence of the Solar Diffuser BRDF Degradation Factor on the SNPP VIIRS Reflective Solar Band On-Orbit Radiometric Calibration SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Angular dependence; bidirectional reflectance distribution function (BRDF) degradation; radiometric calibration; reflective solar bands (RSBs); solar diffuser (SD); Suomi National Polar-orbiting Partnership (SNPP) Visible Infrared Imaging Radiometer Suite (VIIRS) ID STABILITY MONITOR; PERFORMANCE; SUITE AB Using an onboard sunlit solar diffuser (SD) as the primary radiance source, the visible infrared imaging radiometer suite (VIIRS) on the Suomi National Polar-orbiting Partnership satellite regularly performs radiometric calibration of its reflective solar bands (RSBs). The SD bidirectional reflectance distribution function (BRDF) value decreases over time. A numerical degradation factor is used to quantify the degradation and is determined by an onboard SD stability monitor (SDSM), which observes the sun and the sunlit SD at almost the same time. We had shown previously that the BRDF degradation factor was angle-dependent. Consequently, due to that the SDSM and the RSB view the SD at very different angles relative to both the solar and the SD surface normal vectors, directly applying the BRDF degradation factor determined by the SDSM to the VIIRS RSB calibration can result in large systematic errors. We develop a phenomenological model to calculate the BRDF degradation factor for the RSB SD view from the degradation factor for the SDSM SD view. Using the yearly undulations observed in the VIIRS detector gains for the M1-M4 bands calculated with the SD BRDF degradation factor for the SDSM SD view and the difference between the VIIRS detector gains calculated from the SD and the lunar observations, we obtain the model parameter values and thus establish the relation between the BRDF degradation factors for the RSB and the SDSM SD view directions. C1 [Lei, Ning] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Xiong, Xiaoxiong] NASA, Sci & Explorat Directorate, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lei, N (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA. NR 30 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 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD MAR PY 2017 VL 55 IS 3 BP 1537 EP 1543 DI 10.1109/TGRS.2016.2626963 PG 7 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA EN6IC UT WOS:000396106700026 ER PT J AU Angal, A Xiong, XX Wu, AS AF Angal, Amit Xiong, Xiaoxiong Wu, Aisheng TI Monitoring the On-Orbit Calibration of Terra MODIS Reflective Solar Bands Using Simultaneous Terra MISR Observations SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Calibration; moderate resolution imaging spectroradiometer (MODIS); multiangle imaging spectroradiometer (MISR); response versus scan angle (RVS) ID RADIOMETRIC CALIBRATION AB On December 18, 2015, the Terra spacecraft completed 16 years of successful operation in space. Terra has five instruments designed to facilitate scientific measurements of the earth's land, ocean, and atmosphere. The Moderate Resolution Imaging Spectroradiometer (MODIS) and the Multiangle Imaging Spectroradiometer (MISR) instruments provide information for the temporal studies of the globe. After providing over 16 years of complementary measurements, a synergistic use of the measurements obtained from these sensors is beneficial for various science products. The 20 reflective solar bands (RSBs) of MODIS are calibrated using a combination of solar diffuser and lunar measurements, supplemented by measurements from pseudoinvariant desert sites. MODIS views the on-board calibrators and the earth via a two-sided scan mirror at three spatial resolutions: 250 m using 40 detectors in bands 1 and 2, 500 m using 20 detectors in bands 3 and 4, and 1000 m using 10 detectors in bands 8-19 and 26. Simultaneous measurements of the earth's surface are acquired in a push-broom fashion by MISR at nine view angles spreading out in the forward and backward directions along the flight path. While the swath width for MISR acquisitions is 360 km, MODIS scans a wider swath of 2330 km via its two-sided scan mirror. The reflectance of the MODIS scan mirror has an angle dependence characterized by the response versus scan angle (RVS). Its on-orbit change is derived using the gain from a combination of on-board and earth-view measurements. The on-orbit RVS for MODIS has experienced a significant change, especially for the short-wavelength bands. The on-orbit RVS change for the short-wavelength bands (bands 3, 8, and 9) at nadir is observed to be greater than 10% over the mission lifetime. Due to absence of a scanning mechanism, MISR can serve as an effective tool to evaluate and monitor the on-orbit performance of the MODIS RVS. Furthermore, it can also monitor the detector and scan-mirror differences for the MODIS bands using simultaneous measurements from earth-scene targets, e.g., North Atlantic Ocean and North African desert. Simultaneous measurements provide the benefit of minimizing the impact of earth-scene features while comparing the radiometric performance using vicarious techniques. Long-term observations of both instruments using select ground targets also provide an evaluation of the long-term calibration stability. The goal of this paper is to demonstrate the use of MISR to monitor and enhance the on-orbit calibration of the MODIS RSB. The radiometric calibration requirements for the MODIS RSB are +/- 2% in reflectance and +/- 5% in radiance at typical radiance levels within +/- 45 degrees of nadir. The results show that the long-term changes in the MODIS reflectance at nadir frames are generally within 1%. The MODIS level 1B calibrated products, generated after correcting for the on-orbit changes in the gain and RVS, do not have any correction for changes in the instrument's polarization sensitivity. The mirror-side-dependent polarization sensitivity exhibits an on-orbit change, primarily in the blue bands, that manifests in noticeable mirror side differences in the MODIS calibrated products. The mirror side differences for other RSB are observed to be less than 1%, therefore demonstrating an excellent on-orbit performance. The detector differences in the blue bands of MODIS exhibit divergence in recent years beyond 1%, and a calibration algorithm improvement has been identified to mitigate this effect. Short-term variations in the recent year caused by the forward updates were identified in bands 1 and 2 and are planned to be corrected in the next reprocess. C1 [Angal, Amit; Wu, Aisheng] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Xiong, Xiaoxiong] NASA Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. RP Angal, A (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA. EM amit.angal@ssaihq.com; xiaoxiong.xiong-1@nasa.gov; aisheng.wu@ssaihq.com NR 20 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 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD MAR PY 2017 VL 55 IS 3 BP 1648 EP 1659 DI 10.1109/TGRS.2016.2628704 PG 12 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA EN6IC UT WOS:000396106700034 ER PT J AU Meneghini, R Kim, H AF Meneghini, Robert Kim, Hyokyung TI Minimizing the Standard Deviation of Spatially Averaged Surface Cross-Sectional Data From the Dual-Frequency Precipitation Radar SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Normalized radar cross section; rain attenuation; spaceborne meteorological radar ID RAIN-RATE; ATTENUATION AB For an airborne or spaceborne radar, the precipitation-induced path attenuation can be estimated from the measurements of the normalized surface cross section, sigma(0), in the presence and absence of precipitation. In one implementation, the mean rain-free estimate and its variability are found from a lookup table (LUT) derived from previously measured data. For the dual-frequency precipitation radar aboard the global precipitation measurement satellite, the nominal table consists of the statistics of the rain-free sigma(0) over a 0.5 degrees x 0.5 degrees latitude-longitude grid using a three-month set of input data. However, a problem with the LUT is an insufficient number of samples in many cells. An alternative table is constructed by a stepwise procedure that begins with the statistics over a 0.25 degrees x 0.25 degrees grid. If the number of samples at a cell is too few, the area is expanded, cell by cell, choosing at each step that cell that minimizes the variance of the data. The question arises, however, as to whether the selected region corresponds to the smallest variance. To address this question, a second type of variable-averaging grid is constructed using all possible spatial configurations and computing the variance of the data within each region. Comparisons of the standard deviations for the fixed and variable-averaged grids are given as a function of incidence angle and surface type using a three-month set of data. The advantage of variable spatial averaging is that the average standard deviation can be reduced relative to the fixed grid while satisfying the minimum sample requirement. C1 [Meneghini, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kim, Hyokyung] Morgan State Univ, Goddard Earth Sci & Technol Ctr, Greenbelt, MD 20771 USA. RP Meneghini, R (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM robert.meneghini-1@nasa.gov FU NASA [NNH12ZDA001N-PMM] FX This work is supported by NASA under Grant NNH12ZDA001N-PMM by Dr. R. Kakar of NASA Headquarters. NR 13 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 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD MAR PY 2017 VL 55 IS 3 BP 1709 EP 1716 DI 10.1109/TGRS.2016.2630669 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 EN6IC UT WOS:000396106700039 ER PT J AU Patel, A Paden, J Leuschen, C Kwok, R Gomez-Garcia, D Panzer, B Davidson, MWJ Gogineni, S AF Patel, Aqsa Paden, John Leuschen, Carl Kwok, Ron Gomez-Garcia, Daniel Panzer, Ben Davidson, Malcolm W. J. Gogineni, Sivaprasad TI Fine-Resolution Radar Altimeter Measurements on Land and Sea Ice (vol 53, pg 2547, 2015) SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Correction C1 [Patel, Aqsa; Paden, John; Leuschen, Carl; Gomez-Garcia, Daniel; Panzer, Ben; Gogineni, Sivaprasad] Univ Kansas, Dept Elect Engn & Comp Sci, Lawrence, KS 66044 USA. [Kwok, Ron] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Davidson, Malcolm W. J.] European Space Agcy, EOP SMS, NL-2201 AZ Noordwijk, Netherlands. RP Patel, A (reprint author), Univ Kansas, Dept Elect Engn & Comp Sci, Lawrence, KS 66044 USA. EM aqsa.patel@gmail.com FU U.S. National Science Foundation [ANT-0424589]; U.S. National Aeronautics and Space Administration [NNX09AR77G, NNG10HP19C, NNX10AT68G, NNX13AD53A] FX This work was supported in part by the U.S. National Science Foundation under Grant ANT-0424589 and in part by the U.S. National Aeronautics and Space Administration under Grant NNX09AR77G, Grant NNG10HP19C, Grant NNX10AT68G, and Grant NNX13AD53A. NR 1 TC 0 Z9 0 U1 1 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD MAR PY 2017 VL 55 IS 3 BP 1853 EP 1853 DI 10.1109/TGRS.2017.2653558 PG 1 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA EN6IC UT WOS:000396106700052 ER PT J AU Hur, J Moon, DI Han, JW Kim, GH Jeon, CH Choi, YK AF Hur, Jae Moon, Dong-Il Han, Jin-Woo Kim, Gun-Hee Jeon, Chang-Hoon Choi, Yang-Kyu TI Tunneling Effects in a Charge-Plasma Dopingless Transistor SO IEEE TRANSACTIONS ON NANOTECHNOLOGY LA English DT Article DE Band-to-band tunneling (BBT); charge-plasma (C-P); dopingless transistor (DLT); fermi level pinning (FLP); gate-induced drain leakage (GIDL); junctionless transistor (JLT); metal-induced gap states (MIGS); universal schottky tunneling (UST) ID JUNCTIONLESS TRANSISTOR; SCHOTTKY; SOURCE/DRAIN; PERFORMANCE; MOSFETS; CHANNEL AB The recently proposed device concept, the so-called charge-plasma (C-P) dopingless transistor (DLT), is revisited. The novel device, which utilizes the workfunction difference between the source/drain (S/D) metal and the substrate enclosing the S/D junction, does not demand external S/D chemical doping via ion implant. It shows excellent immunity against short-channel effects due to an extremely thin junction depth arisen from internal S/D electrical doping, which is the counter-part of the aforementioned chemical doping. For a deeper understanding of C-P devices, the tunneling effects must be considered because of the unavoidable presence of a Schottky barrier at the S/D contact interface. These tunneling effects were found to have a huge impact on current under an ON-and OFF-state. And they strongly depend on the spacer and contact length of the device. The device performance and the feasibility of the C-P DLT are also discussed, specifically, in terms of the Fermi level pinning. C1 [Hur, Jae; Kim, Gun-Hee; Jeon, Chang-Hoon; Choi, Yang-Kyu] Korea Adv Inst Sci & Technol, Sch Elect Engn, Daejeon 34141, South Korea. [Moon, Dong-Il; Han, Jin-Woo] NASA, Ames Res Ctr, Sunnyvale, CA 94035 USA. RP Hur, J (reprint author), Korea Adv Inst Sci & Technol, Sch Elect Engn, Daejeon 34141, South Korea. EM ykchoi@ee.kaist.ac.kr; dong-il.moon@nasa.gov; jin-woo.han@nasa.gov; ghkim@nobelab.kaist.ac.kr; chjeon@nobelab.kaist.ac.kr; ykchoi@ee.kaist.ac.kr FU Pioneer Research Center Program through National Research Foundation of Korea within Ministry of Science, ICT & Future Planning [2012-0009600]; Center for Integrated Smart Sensors within MSIP through the Global Frontier Project [CISS-2011-0031848]; IDEC (EDA Tool, MPW) FX This work was supported in part by the Pioneer Research Center Program through the National Research Foundation of Korea within the Ministry of Science, ICT & Future Planning under Grant 2012-0009600, in part by the Center for Integrated Smart Sensors within the MSIP through the Global Frontier Project under Grant CISS-2011-0031848, and in part by the IDEC (EDA Tool, MPW). The review of this paper was arranged by Associate Editor Ant Ural. NR 24 TC 0 Z9 0 U1 2 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1536-125X EI 1941-0085 J9 IEEE T NANOTECHNOL JI IEEE Trans. Nanotechnol. PD MAR PY 2017 VL 16 IS 2 BP 315 EP 320 DI 10.1109/TNANO.2017.2663659 PG 6 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Science & Technology - Other Topics; Materials Science; Physics GA EO0OA UT WOS:000396396300021 ER PT J AU Alonso-DelPino, M Reck, T Jung-Kubiak, C Lee, C Chattopadhyay, G AF Alonso-DelPino, Maria Reck, Theodore Jung-Kubiak, Cecile Lee, Choonsup Chattopadhyay, Goutam TI Development of Silicon Micromachined Microlens Antennas at 1.9 THz SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Article DE Antenna; leaky-wave terahertz (THz); lens; microlens; shallow lens; submillimeter wave ID WAVE-GUIDE; TERAHERTZ AB The development at 1.9 THz of a microlens antenna consisting of a leaky-wave waveguide feeding and a silicon microlens is presented in this paper. The antenna has excellent performances compared to horn antennas and can be fabricated entirely using silicon micromachining. Two antenna prototypes were developed: one with a 2.6-mm-diameter microlens and a directivity of 33.2 dB and the other with a 6.35-mm-diameter microlens and a directivity of 41.2 dB. Both prototypes were fabricated and measured, obtaining good agreements with simulations. The fabrication, assembly, and measurement process are explained and detailed in this paper. C1 [Alonso-DelPino, Maria; Reck, Theodore; Jung-Kubiak, Cecile; Lee, Choonsup; Chattopadhyay, Goutam] Jet Prop Lab, Submillimeter Wave Adv Technol Grp, Pasadena, CA 91109 USA. RP Alonso-DelPino, M (reprint author), Jet Prop Lab, Submillimeter Wave Adv Technol Grp, Pasadena, CA 91109 USA. EM maria.alonso@jpl.nasa.com; theodore.reck@jpl.nasa.gov; Cecile.D.Jung@jpl.nasa.gov; Choonsup.Lee@jpl.nasa.gov; goutam.chattopadhyay@jpl.nasa.gov FU National Aeronautics and Space Administration; Submillimeter-Wave Advanced Technology Group of the JPL FX This work was carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This work was supported by the Submillimeter-Wave Advanced Technology Group of the JPL. NR 18 TC 0 Z9 0 U1 1 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD MAR PY 2017 VL 7 IS 2 BP 191 EP 198 DI 10.1109/TTHZ.2017.2655340 PG 8 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA EO0LI UT WOS:000396388900010 ER PT J AU Enzer, DG Diener, WA Murphy, DW Rao, SR Tjoelker, RL AF Enzer, Daphna G. Diener, William A. Murphy, David W. Rao, Shanti R. Tjoelker, Robert L. TI Drifts and Environmental Disturbances in Atomic Clock Subsystems: Quantifying Local Oscillator, Control Loop, and Ion Resonance Interactions SO IEEE TRANSACTIONS ON ULTRASONICS FERROELECTRICS AND FREQUENCY CONTROL LA English DT Article DE Atomic clocks; atomic frequency standards; local oscillators (LOs) AB Linear ion trap frequency standards are among the most stable continuously operating frequency references and clocks. Depending on the application, they have been operated with a variety of local oscillators (LOs), including quartz ultrastable oscillators, hydrogen-masers, and cryogenic sapphire oscillators. The short-, intermediate-, and long-term stability of the frequency output is a complicated function of the fundamental performances, the time dependence of environmental disturbances, the atomic interrogation algorithm, the implemented control loop, and the environmental sensitivity of the LO and the atomic system components. For applications that require moving these references out of controlled lab spaces and into less stable environments, such as fieldwork or spaceflight, a deeper understanding is needed of how disturbances at different timescales impact the various subsystems of the clock and ultimately the output stability. In this paper, we analyze which perturbations have an impact and to what degree. We also report on a computational model of a control loop, which keeps the microwave source locked to the ion resonance. This model is shown to agree with laboratory measurements of how well the feedback removes various disturbances and also with a useful analytic approach we developed for predicting these impacts. C1 [Enzer, Daphna G.; Diener, William A.; Murphy, David W.; Rao, Shanti R.; Tjoelker, Robert L.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Enzer, DG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM daphna.g.enzer@jpl.nasa.gov FU Jet Propulsion Laboratory, California Institute of Technology; National Aeronautics and Space Administration FX This work was supported in part by the Jet Propulsion Laboratory, California Institute of Technology, and in part by the National Aeronautics and Space Administration. NR 15 TC 0 Z9 0 U1 1 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0885-3010 EI 1525-8955 J9 IEEE T ULTRASON FERR JI IEEE Trans. Ultrason. Ferroelectr. Freq. Control PD MAR PY 2017 VL 64 IS 3 BP 623 EP 633 DI 10.1109/TUFFC.2016.2636088 PG 11 WC Acoustics; Engineering, Electrical & Electronic SC Acoustics; Engineering GA EO0PD UT WOS:000396399400013 PM 28029621 ER PT J AU Suhir, E Yi, S Ghaffarian, R AF Suhir, E. Yi, S. Ghaffarian, R. TI How Many Peripheral Solder Joints in a Surface Mounted Design Experience Inelastic Strains? SO JOURNAL OF ELECTRONIC MATERIALS LA English DT Article DE solder material; yield strain; low-cycle fatigue; stress analysis ID CERAMIC CHIP CARRIERS; BIMETAL THERMOSTATS; STRESSES; BOARDS AB It has been established that it is the peripheral solder joints that are the most vulnerable in the ball-grid-array (BGA) and column-grid-array (CGA) designs and most often fail. As far as the long-term reliability of a soldered microelectronics assembly as a whole is concerned, it makes a difference, if just one or more peripheral joints experience inelastic strains. It is clear that the low cycle fatigue lifetime of the solder system is inversely proportional to the number of joints that simultaneously experience inelastic strains. A simple and physically meaningful analytical expression (formula) is obtained for the prediction, at the design stage, of the number of such joints, if any, for the given effective thermal expansion (contraction) mismatch of the package and PCB; materials and geometrical characteristics of the package/PCB assembly; package size; and, of course, the level of the yield stress in the solder material. The suggested formula can be used to determine if the inelastic strains in the solder material could be avoided by the proper selection of the above characteristics and, if not, how many peripheral joints are expected to simultaneously experience inelastic strains. The general concept is illustrated by a numerical example carried out for a typical BGA package. The suggested analytical model (formula) is applicable to any soldered microelectronics assembly. The roles of other important factors, such as, e.g., solder material anisotropy, grain size, and their random orientation within a joint, are viewed in this analysis as less important factors than the level of the interfacial stress. The roles of these factors will be accounted for in future work and considered, in addition to the location of the joint, in a more complicated, more sophisticated, and more comprehensive reliability/fatigue model. C1 [Suhir, E.; Yi, S.] 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 31 TC 0 Z9 0 U1 0 U2 0 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 MAR PY 2017 VL 46 IS 3 BP 1747 EP 1753 DI 10.1007/s11664-016-5224-8 PG 7 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA EK8ZF UT WOS:000394212600038 ER PT J AU Wilson, EL DiGregorio, AJ Riot, VJ Ammons, MS Bruner, WW Carter, D Mao, JP Ramanathan, A Strahan, SE Oman, LD Hoffman, C Garner, RM AF Wilson, Emily L. DiGregorio, A. J. Riot, Vincent J. Ammons, Mark S. Bruner, William W. Carter, Darrell Mao, Jianping Ramanathan, Anand Strahan, Susan E. Oman, Luke D. Hoffman, Christine Garner, Richard M. TI A 4 U laser heterodyne radiometer for methane (CH4) and carbon dioxide (CO2) measurements from an occultation-viewing CubeSat SO MEASUREMENT SCIENCE AND TECHNOLOGY LA English DT Article DE laser heterodyne radiometer; CubeSat; carbon dioxide; methane; water vapor; occultation; greenhouse gases ID ATMOSPHERIC COLUMN; MISSION; SATELLITE; SPACE; SENSITIVITY AB We present a design for a 4 U (20 cm x 20 cm x 10 cm) occultation-viewing laser heterodyne radiometer (LHR) that measures methane (CH4), carbon dioxide (CO2) and water vapor (H2O) in the limb that is designed for deployment on a 6 U CubeSat. The LHR design collects sunlight that has undergone absorption by the trace gas and mixes it with a distributive feedback (DFB) laser centered at 1640 nm that scans across CO2, CH4, and H2O absorption features. Upper troposphere/lower stratosphere measurements of these gases provide key inputs to stratospheric circulation models: measuring stratospheric circulation and its variability is essential for projecting how climate change will affect stratospheric ozone. C1 [Wilson, Emily L.; Oman, Luke D.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. [DiGregorio, A. J.; Garner, Richard M.] Sci Syst & Applicat Inc, 10210 Greenbelt Rd 20, Lanham, MD 20706 USA. [Riot, Vincent J.; Ammons, Mark S.; Bruner, William W.; Carter, Darrell] Lawrence Livermore Natl Lab, 7000 East Ave, Livermore, CA 94550 USA. [Mao, Jianping; Ramanathan, Anand] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. [Strahan, Susan E.] Univ Space Res Assoc, 7178 Columbia Gateway Dr, Columbia, MD 21046 USA. [Hoffman, Christine] Univ Calif Merced, 5200 Lake Rd, Merced, CA 95343 USA. RP Wilson, EL (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM Emily.L.Wilson@nasa.gov FU NASA God-dard Space Flight Center Internal Research and Development program; US Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; NASA Science Innovation fund FX Mini-LHR development was supported by the NASA God-dard Space Flight Center Internal Research and Development program and Science Innovation fund. This work was performed in part under the auspices of the US Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. NR 28 TC 0 Z9 0 U1 5 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0957-0233 EI 1361-6501 J9 MEAS SCI TECHNOL JI Meas. Sci. Technol. PD MAR PY 2017 VL 28 IS 3 AR 035902 DI 10.1088/1361-6501/aa5440 PG 8 WC Engineering, Multidisciplinary; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA EK4OT UT WOS:000393907200002 ER PT J AU Didlake, AC Heymsfield, GM Reasor, PD Guimond, SR AF Didlake, Anthony C., Jr. Heymsfield, Gerald M. Reasor, Paul D. Guimond, Stephen R. TI Concentric Eyewall Asymmetries in Hurricane Gonzalo (2014) Observed by Airborne Radar SO MONTHLY WEATHER REVIEW LA English DT Article ID VERTICAL WIND SHEAR; BOUNDARY-LAYER STRUCTURE; AXISYMMETRICAL BALANCE DYNAMICS; TRMM PRECIPITATION RADAR; TROPICAL CYCLONE; PART I; RAPID INTENSIFICATION; KINEMATIC STRUCTURE; BONNIE 1998; REPLACEMENT CYCLES AB Two eyewall replacement cycles were observed in Hurricane Gonzalo by the NOAA P3 Tail (TA) radar and the recently developed NASA High-Altitude Imaging Wind and Rain Airborne Profiler (HIWRAP) radar. These observations captured detailed precipitation and kinematic features of Gonzalo's concentric eyewalls both before and after the outer eyewall's winds became the vortex maximum winds. The data were analyzed relative to the deep-layer environmental wind shear vector. During the beginning eyewall replacement cycle stages, the inner and outer eyewalls exhibited different asymmetries. The inner eyewall asymmetry exhibited significant low-level inflow, updrafts, and positive tangential acceleration in the downshear quadrants, consistent with observational and theoretical studies. The outer eyewall asymmetry exhibited these features in the left-of-shear quadrants, further downwind from those of the inner eyewall. It is suggested that the low-level inflow occurring at the outer but not at the inner eyewall in the downwind regions signals a barrier effect that contributes to the eventual decay of the inner eyewall. Toward the later eyewall replacement stages, the outer eyewall asymmetry shifts upwind, becoming more aligned with the asymmetry of the earlier inner eyewall. This upwind shift is consistent with the structural evolution of eyewall replacement as the outer eyewall transitions into the primary eyewall of the storm. C1 [Didlake, Anthony C., Jr.] Penn State Univ, Dept Meteorol & Atmospher Sci, University Pk, PA 16802 USA. [Heymsfield, Gerald M.; Guimond, Stephen R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reasor, Paul D.] NOAA, Hurricane Res Div, Atlantic Oceanog & Meteorol Lab, Miami, FL USA. [Guimond, Stephen R.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD USA. RP Didlake, AC (reprint author), Penn State Univ, Dept Meteorol & Atmospher Sci, University Pk, PA 16802 USA. EM didlake@psu.edu FU NASA's Earth Venture Program; Office of Naval Research; NASA Postdoctoral Program; NASA New Investigator Program (NIP) [NNX16AI21G] FX We thank John Gamache for his tremendous efforts in developing and maintaining the Doppler Tail radar analysis dataset at HRD. We also thank Lihua Li and Matthew McLinden for their engineering support and data processing for the HIWRAP radar. We thank Beth Tully for her work on the summarizing conceptual model. Last, we thank the three anonymous reviewers whose comments led to significant improvements in the manuscript. The HS3 project was funded under NASA's Earth Venture Program. The TCI project was funded by the Office of Naval Research. This research was supported by the NASA Postdoctoral Program and the NASA New Investigator Program (NIP) under Grant NNX16AI21G. NR 82 TC 0 Z9 0 U1 0 U2 0 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 MAR PY 2017 VL 145 IS 3 BP 730 EP 750 DI 10.1175/MWR-D-16-0175.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EL0XV UT WOS:000394346000001 ER PT J AU Waliser, D Guan, B AF Waliser, Duane Guan, Bin TI Extreme winds and precipitation during landfall of atmospheric rivers SO NATURE GEOSCIENCE LA English DT Article ID US WEST-COAST; HYDROMETEOROLOGICAL CHARACTERISTICS; INLAND PENETRATION; FUTURE CHANGES; CLIMATE-CHANGE; EUROPE; CALIFORNIA; FREQUENCY; IMPACTS; EVENTS AB Atmospheric rivers-long, narrow filaments of large integrated water vapour transport-are associated with weather and water extremes, such as precipitation extremes and flooding in western North America and northern Europe. Here we apply a global detection algorithm for atmospheric rivers to reanalysis data during 1997-2014 to investigate the impact of atmospheric rivers on wind extremes as well as precipitation extremes. We find that atmospheric rivers are associated with up to half of the extreme events in the top 2% of the precipitation and wind distribution, across most mid-latitude regions globally. Landfalling atmospheric rivers are associated with about 40-75% of extreme wind and precipitation events over 40% of the world's coastlines. Atmospheric rivers are associated with a doubling or more of the typical wind speed compared to all storm conditions, and a 50-100% increase in the wind and precipitation values for extreme events. We also find that the majority of extreme wind events catalogued between 1997 and 2013 over Europe with billion US dollar losses were associated with atmospheric rivers. We conclude that landfalling atmospheric rivers can represent a significant hazard around the globe, because of their association with not only extreme precipitation, but also extreme winds. C1 [Waliser, Duane] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Guan, Bin] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. RP Waliser, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM duane.waliser@jpl.nasa.gov RI Guan, Bin/F-6735-2010 FU National Aeronautics and Space Administration; NASA FX This work was supported by the National Aeronautics and Space Administration. The contribution of D.W. was carried out on behalf of the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 38 TC 0 Z9 0 U1 4 U2 4 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD MAR PY 2017 VL 10 IS 3 BP 179 EP U183 DI 10.1038/NGEO2894 PG 6 WC Geosciences, Multidisciplinary SC Geology GA EN1SX UT WOS:000395791400008 ER PT J AU Garatti, ACO Stecklum, B Lopez, RG Eisloffel, J Ray, TP Sanna, A Cesaroni, R Walmsley, CM Oudmaijer, RD de Wit, WJ Moscadelli, L Greiner, J Krabbe, A Fischer, C Klein, R Ibanez, JM AF Garatti, A. Caratti O. Stecklum, B. Lopez, R. Garcia Eisloeffel, J. Ray, T. P. Sanna, A. Cesaroni, R. Walmsley, C. M. Oudmaijer, R. D. de Wit, W. J. Moscadelli, L. Greiner, J. Krabbe, A. Fischer, C. Klein, R. Ibanez, J. M. TI Disk-mediated accretion burst in a high-mass young stellar object SO NATURE PHYSICS LA English DT Article ID EVOLUTION; FRAGMENTATION; PROTOSTARS; RATES; STARS; CORES AB Solar-mass stars form via disk-mediated accretion. Recent findings indicate that this process is probably episodic in the form of accretion bursts(1), possibly caused by disk fragmentation(2-4). Although it cannot be ruled out that high-mass young stellar objects arise from the coalescence of their low-mass brethren(5), the latest results suggest that they more likely form via disks(6-9). It follows that disk-mediated accretion bursts should occur(10,11). Here we report on the discovery of the first disk-mediated accretion burst from a roughly twenty-solar-mass high-mass young stellar object(12). Our near-infrared images show the brightening of the central source and its outflow cavities. Near-infrared spectroscopy reveals emission lines typical for accretion bursts in low-mass protostars, but orders of magnitude more luminous. Moreover, the released energy and the inferred mass-accretion rate are also orders of magnitude larger. Our results identify disk-accretion as the common mechanism of star formation across the entire stellar mass spectrum. C1 [Garatti, A. Caratti O.; Lopez, R. Garcia; Ray, T. P.; Walmsley, C. M.] Dublin Inst Adv Studies, Astron & Astrophys Sect, 31 Fitzwilliam Pl, Dublin 2, Ireland. [Stecklum, B.; Eisloeffel, J.] Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany. [Sanna, A.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Cesaroni, R.; Walmsley, C. M.; Moscadelli, L.] Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy. [Oudmaijer, R. D.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [de Wit, W. J.] ESO European Org Astron Res Southern Hemisphere, Alonso de Cordova 3107, Santiago, Chile. [Greiner, J.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Krabbe, A.; Fischer, C.] Deutsch SOFIA Inst, Pfaffenwaldring 29, D-70569 Stuttgart, Germany. [Klein, R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ibanez, J. M.] CSIC, Inst Astrofis Andalucia, Glorieta Astron 3, E-18008 Granada, Spain. RP Garatti, ACO (reprint author), Dublin Inst Adv Studies, Astron & Astrophys Sect, 31 Fitzwilliam Pl, Dublin 2, Ireland. EM alessio@cp.dias.ie OI Caratti o Garatti, Alessio/0000-0001-8876-6614 FU Science Foundation Ireland [13/ERC/I2907]; Deutsche Forschungsgemeinschaft (DFG) Priority Program 1573; Gemini Observatory [GN-2016A-DD-5]; [296.C-5037(A)] FX A.C.o.G., R.G.L. and T.P.R. were supported by Science Foundation Ireland, grant 13/ERC/I2907. A.S. was supported by the Deutsche Forschungsgemeinschaft (DFG) Priority Program 1573. We thank the ESO Paranal and Gemini Observatory staff for their support. B.S. thanks Sylvio Klose for helpful discussions concerning the light echo. This research is partly based on observations collected at the VLT (ESO Paranal, Chile) with programme 296.C-5037(A) and at the Gemini Observatory (Program ID GN-2016A-DD-5). Gemini Observatory is operated by the Association of Universities for Research in Astronomy, 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). NR 47 TC 0 Z9 0 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1745-2473 EI 1745-2481 J9 NAT PHYS JI Nat. Phys. PD MAR PY 2017 VL 13 IS 3 BP 276 EP + DI 10.1038/NPHYS3942 PG 6 WC Physics, Multidisciplinary SC Physics GA EN2BI UT WOS:000395814000020 ER PT J AU Smith, KE House, CH Dworkin, JP Callahan, MP AF Smith, Karen E. House, Christopher H. Dworkin, Jason P. Callahan, Michael P. TI Spontaneous Oligomerization of Nucleotide Alternatives in Aqueous Solutions SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES LA English DT Article DE Liquid chromatography; Mass spectrometry; Oligomerization; Prebiotic chemistry; Pyrimidines ID RNA WORLD; CHEMISTRY; EVOLUTION; ADENINE; ANALOGS AB On early Earth, a primitive polymer that could spontaneously form from likely available precursors may have preceded both RNA and DNA as the first genetic material. Here, we report that heated aqueous solutions containing 5-hydroxymethyluracil (HMU) result in oligomers of uracil, heated solutions containing 5-hydroxymethylcytosine (HMC) result in oligomers of cytosine, and heated solutions containing both HMU and HMC result in mixed oligomers of uracil and cytosine. Oligomerization of hydroxymethylated pyrimidines, which may have been abundant on the primitive Earth, might have been important in the development of simple informational polymers. C1 [Smith, Karen E.; House, Christopher H.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Smith, Karen E.; House, Christopher H.] Penn State Univ, Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA. [Dworkin, Jason P.; Callahan, Michael P.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dworkin, Jason P.; Callahan, Michael P.] NASA, Goddard Ctr Astrobiol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Callahan, Michael P.] Boise State Univ, Dept Chem & Biochem, Boise, ID 83725 USA. RP Callahan, MP (reprint author), NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Callahan, MP (reprint author), NASA, Goddard Ctr Astrobiol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Callahan, MP (reprint author), Boise State Univ, Dept Chem & Biochem, Boise, ID 83725 USA. EM michaelcallahan914@boisestate.edu FU NASA Pennsylvania Space Grant Consortium; NASA Astrobiology Institute via the Penn State Astrobiology Research Center [NNA09DA76A]; NASA Astrobiology Institute via the Goddard Center for Astrobiology FX This research was supported by the NASA Pennsylvania Space Grant Consortium, NASA Astrobiology Institute via the Penn State Astrobiology Research Center (cooperative agreement #NNA09DA76A), and the NASA Astrobiology Institute via the Goddard Center for Astrobiology. We thank Prof. Jim Kubicki (Penn State) for assistance with DFT calculations. We also thank Dr. Henderson (Jim) Cleaves (Institute for Advanced Study/Tokyo Institute of Technology) for helpful discussions. NR 19 TC 0 Z9 0 U1 1 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-6149 EI 1573-0875 J9 ORIGINS LIFE EVOL B JI Orig. Life Evol. Biosph. PD MAR PY 2017 VL 47 IS 1 BP 3 EP 11 DI 10.1007/s11084-016-9484-3 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA EL0UM UT WOS:000394337300002 PM 27029792 ER PT J AU Barge, LM Branscomb, E Brucato, JR Cardoso, SSS Cartwright, JHE Danielache, SO Galante, D Kee, TP Miguel, Y Mojzsis, S Robinson, KJ Russell, MJ Simoncini, E Sobron, P AF Barge, L. M. Branscomb, E. Brucato, J. R. Cardoso, S. S. S. Cartwright, J. H. E. Danielache, S. O. Galante, D. Kee, T. P. Miguel, Y. Mojzsis, S. Robinson, K. J. Russell, M. J. Simoncini, E. Sobron, P. TI Thermodynamics, Disequilibrium, Evolution: Far-From-Equilibrium Geological and Chemical Considerations for Origin-Of-Life Research SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES LA English DT Article DE Far-from-equilibrium thermodynamics; Life origins; Geochemical disequilibrium; Hydrothermal vents; Early earth; Habitability; Chemiosmosis; Self-organization; Laboratory simulation ID ISUA SUPRACRUSTAL BELT; LIGAND-ACCELERATED CATALYSIS; ALKALINE HYDROTHERMAL VENTS; EARTHS EARLY ATMOSPHERE; ION MICROPROBE ANALYSIS; LOW-MASS STAR; OXIDATION-STATE; WEST GREENLAND; SEDIMENTARY-ROCKS; HABITABLE ZONE C1 [Barge, L. M.; Russell, M. J.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. [Barge, L. M.; Russell, M. J.] NASA, Icy Worlds Team, Astrobiol Inst, Mountain View, CA 94043 USA. [Branscomb, E.] Univ Illinois, Carl R Woese Inst Genom Biol, Champaign, IL 61820 USA. [Brucato, J. R.; Simoncini, E.] Astrophys Observ Arcetri, Florence, Italy. [Cardoso, S. S. S.] Univ Cambridge, Dept Chem Engn & Biotechnol, Cambridge CB2 3RA, England. [Cartwright, J. H. E.] Univ Granada, CSIC, Inst Andaluz Ciencias Tierra, E-18100 Granada, Spain. [Cartwright, J. H. E.] Univ Granada, Inst Carlos I Fis Teor & Computac, E-18071 Granada, Spain. [Danielache, S. O.] Sophia Univ, Tokyo, Japan. [Danielache, S. O.] Tokyo Tech Univ, Earth & Life Sci Inst, Tokyo, Japan. [Galante, D.] LNLS CNPEM, Brazilian Synchrotron Light Lab, Campinas, SP, Brazil. [Kee, T. P.] Univ Leeds, Sch Chem, Woodhouse Lane, Leeds LS2 9JT, W Yorkshire, England. [Miguel, Y.] Observ Cote Azur, Nice, France. [Mojzsis, S.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. [Robinson, K. J.] Arizona State Univ, Sch Mol Sci, Tempe, AZ 85287 USA. [Robinson, K. J.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Sobron, P.] SETI Inst, Carl Sagan Ctr, Mountain View, CA USA. [Sobron, P.] Impossible Sensing, St Louis, MO USA. RP Barge, LM (reprint author), CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA.; Barge, LM (reprint author), NASA, Icy Worlds Team, Astrobiol Inst, Mountain View, CA 94043 USA. EM Laura.M.Barge@jpl.nasa.gov FU NASA Astrobiology Institute (NAI); NAI (Icy Worlds); ORIGINS COST Action [TD1308]; ASI/INAF [2015 - 002]; Spanish MINCINN [FIS2013-48444-C2-2-P] FX The authors wish to thank the Earth-Life Science Institute of the Tokyo Institute of Technology for supporting and hosting the TDE Focus Group meeting on which this publication is based. The Thermodynamics, Disequilibrium, Evolution (TDE) Focus Group is supported by the NASA Astrobiology Institute (NAI). Parts of this work were carried out at the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration; LMB and MJR are supported by NAI (Icy Worlds). ES thanks the ORIGINS COST Action (TD1308) for the STSM Reference Number: COST-STSM-TD1308-26973. ES is supported by Agreement ASI/INAF 2015 - 002 - R.O. JHEC acknowledges the financial support of the Spanish MINCINN project FIS2013-48444-C2-2-P. (C) 2016, all rights reserved. NR 164 TC 1 Z9 1 U1 5 U2 5 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-6149 EI 1573-0875 J9 ORIGINS LIFE EVOL B JI Orig. Life Evol. Biosph. PD MAR PY 2017 VL 47 IS 1 BP 39 EP 56 DI 10.1007/s11084-016-9508-z PG 18 WC Biology SC Life Sciences & Biomedicine - Other Topics GA EL0UM UT WOS:000394337300004 PM 27271006 ER PT J AU Lu, T Zhang, Y Kidane, Y Feiveson, A Stodieck, L Karouia, F Ramesh, G Rohde, L Wu, HL AF Lu, Tao Zhang, Ye Kidane, Yared Feiveson, Alan Stodieck, Louis Karouia, Fathi Ramesh, Govindarajan Rohde, Larry Wu, Honglu TI Cellular responses and gene expression profile changes due to bleomycin-induced DNA damage in human fibroblasts in space SO PLOS ONE LA English DT Article ID RADIATION INTERACTION EXPERIMENT; DOUBLE-STRAND BREAKS; HUMAN-LYMPHOCYTES; MODELED MICROGRAVITY; SIMULATED MICROGRAVITY; IONIZING-RADIATION; HUMAN-CELLS; LYMPHOBLASTOID-CELLS; GAMMA-RAYS; IN-VITRO AB Living organisms in space are constantly exposed to radiation, toxic chemicals or reactive oxygen species generated due to increased levels of environmental and psychological stresses. Understanding the impact of spaceflight factors, microgravity in particular, on cellular responses to DNA damage is essential for assessing the radiation risk for astronauts and the mutation rate in microorganisms. In a study conducted on the International Space Station, confluent human fibroblasts in culture were treated with bleomycin for three hours in the true microgravity environment. The degree of DNA damage was quantified by immunofluorescence staining for gamma-H2AX, which is manifested in three types of staining patterns. Although similar percentages of these types of patterns were found between flight and ground cells, there was a slight shift in the distribution of foci counts in the flown cells with countable numbers of gamma-H2AX foci. Comparison of the cells in confluent and in exponential growth conditions indicated that the proliferation rate between flight and the ground may be responsible for such a shift. We also performed a microarray analysis of gene expressions in response to bleomycin treatment. A qualitative comparison of the responsive pathways between the flown and ground cells showed similar responses with the p53 network being the top upstream regulator. The microarray data was confirmed with a PCR array analysis containing a set of genes involved in DNA damage signaling; with BBC3, CDKN1A, PCNA and PPM1D being significantly upregulated in both flight and ground cells after bleomycin treatment. Our results suggest that whether microgravity affects DNA damage response in space can be dependent on the cell type and cell growth condition. C1 [Lu, Tao; Kidane, Yared; Feiveson, Alan; Wu, Honglu] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Lu, Tao; Rohde, Larry] Univ Houston Clear Lake, Houston, TX USA. [Zhang, Ye] NASA, Kennedy Space Ctr, Houston, TX USA. [Kidane, Yared] Wyle Labs, Houston, TX USA. [Stodieck, Louis] BioServe Space Technol, Boulder, CO USA. [Karouia, Fathi] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ramesh, Govindarajan] Norfolk State Univ, Norfolk, VA USA. RP Wu, HL (reprint author), NASA, Johnson Space Ctr, Houston, TX 77058 USA. EM honglu.wu-1@nasa.gov FU NASA Fundamental Space Biology Program; BioServe Space Technologies; NASA FX This work was supported by the NASA Fundamental Space Biology Program. The project was supported by BioServe Space Technologies. We thank Ashleigh Ruggles and Satyanand Narayan of NASA Kennedy Space Center, and Kevin Sato of NASA Ames Research Center for the support during various phases of the project. This study involved participation of personnel from two commercial companies, Wyle Laboratories and BioServe. Wyle Laboratories is a NASA contractor and employs one of the coauthors (YZ). YZ performed the gene expression data analysis for the study. BioServe (LS) was the implementation partner for this spaceflight study and received funds from NASA to support the project. LS was responsible for the hardware development, and contributed to the study design. NASA was the funding agency of the study. The funder provided support in the form of salaries for TL, YZ, YK, AF, LS, FK, and HW, 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. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 52 TC 0 Z9 0 U1 1 U2 1 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAR 1 PY 2017 VL 12 IS 3 AR e0170358 DI 10.1371/journal.pone.0170358 PG 19 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EN4NF UT WOS:000395983500003 PM 28248986 ER PT J AU Borden, M Lewis, D Ochoa, H Jones-Wilson, L Susca, S Porter, M Massey, R Clark, P Netterfield, B AF Borden, Michael Lewis, Derek Ochoa, Hared Jones-Wilson, Laura Susca, Sara Porter, Michael Massey, Richard Clark, Paul Netterfield, Barth TI Thermal, Structural, and Optical Analysis of a Balloon-Based Imaging System SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE balloons; telescopes; methods: analytical ID TELESCOPE AB The Subarcsecond Telescope And BaLloon Experiment, STABLE, is the fine stage of a guidance system for a high-altitude ballooning platform designed to demonstrate subarcsecond pointing stability over one minute using relatively dim guide stars in the visible spectrum. The STABLE system uses an attitude rate sensor and the motion of the guide star on a detector to control a Fast Steering Mirror to stabilize the image. The characteristics of the thermal-optical-mechanical elements in the system directly affect the quality of the point-spread function of the guide star on the detector, so a series of thermal, structural, and optical models were built to simulate system performance and ultimately inform the final pointing stability predictions. This paper describes the modeling techniques employed in each of these subsystems. The results from those models are discussed in detail, highlighting the development of the worst-case cold and hot cases, the optical metrics generated from the finite element model, and the expected STABLE residual wavefront error and decenter. Finally, the paper concludes with the predicted sensitivities in the STABLE system, which show that thermal deadbanding, structural pre-loading, and self-deflection under different loading conditions, and the speed of individual optical elements were particularly important to the resulting STABLE optical performance. C1 [Borden, Michael; Lewis, Derek; Ochoa, Hared; Jones-Wilson, Laura; Susca, Sara] CALTECH, NASA, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Borden, Michael] Gen Atom ASI, 16868 Via Campo Court, San Diego, CA 92127 USA. [Porter, Michael] CALTECH, Opt Observ, 1200 E Calif Blvd, Pasadena, CA 91101 USA. [Massey, Richard; Clark, Paul] Univ Durham, Ctr Adv Instrumentat, South Rd, Durham DH1 3LE, England. [Netterfield, Barth] Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada. RP Borden, M (reprint author), CALTECH, NASA, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.; Borden, M (reprint author), Gen Atom ASI, 16868 Via Campo Court, San Diego, CA 92127 USA. EM mike.b.borden@gmail.com FU NASA JPL Astronomy Directorate; National Aeronautics and Space Administration; JPL; Royal Society; University of Durham FX The work described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, and was sponsored by the NASA JPL Astronomy Directorate through an agreement with the National Aeronautics and Space Administration. The authors would like to thank Jeff Booth at JPL for his continued support for the STABLE project and providing the funding for the write up of this work. The authors would also like to thank John Peacock for his help securing funding for work done at the University of Durham. RJM is supported by the Royal Society. NR 16 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD MAR 1 PY 2017 VL 129 IS 973 BP 1 EP 31 DI 10.1088/1538-3873/129/973/035001 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EM6HT UT WOS:000395414200001 ER PT J AU Nayak, M Lupu, R Marley, MS Fortney, JJ Robinson, T Lewis, N AF Nayak, Michael Lupu, Roxana Marley, Mark S. Fortney, Jonathan J. Robinson, Tyler Lewis, Nikole TI Atmospheric Retrieval for Direct Imaging Spectroscopy of Gas Giants In Reflected Light. II. Orbital Phase and Planetary Radius SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE radiative transfer; scattering; methods: statistical; techniques: imaging spectroscopy; techniques: spectroscopic; planets and satellites: atmospheres; planets and satellites: composition; planets and satellites: gaseous planets ID SUPER-EARTHS; EXOPLANET ATMOSPHERES; EXTRASOLAR PLANETS; THERMAL STRUCTURE; GJ 1214B; SPECTRA; SEPARATION; CLOUDS; I.; HD189733B AB Future space-based telescopes, such as the Wide-Field Infrared Survey Telescope (WFIRST), will observe the reflected light spectra of directly imaged extrasolar planets. Interpretation of such data presents a number of novel challenges, including accounting for unknown planet radius and uncertain stellar illumination phase angle. Here, we report on our continued development of Markov Chain Monte Carlo retrieval methods for addressing these issues in the interpretation of such data. Specifically, we explore how the unknown planet radius and potentially poorly known observer-planet-star phase angle impacts retrievals of parameters of interest such as atmospheric methane abundance, cloud properties, and surface gravity. As expected, the uncertainty in retrieved values is a strong function of the signal-to-noise ratio (S/N) of the observed spectra, particularly for low metallicity atmospheres, which lack deep absorption signatures. Meaningful results may only be possible above certain S/N thresholds; for cases across a metallicity range of 1-50 times solar, we find that only an S/N of 20 systematically reproduces a value close to the correct methane abundance at all phase angles. However, even in cases where the phase angle is poorly known we find that the planet radius can be constrained to within a factor of two. We find that uncertainty in planet radius decreases at phase angles past quadrature, as the highly forward-scattering nature of the atmosphere at these geometries limits the possible volume of phase space that relevant parameters can occupy. Finally, we present an estimation of possible improvement that can result from combining retrievals against observations at multiple phase angles. C1 [Nayak, Michael; Lupu, Roxana; Marley, Mark S.; Robinson, Tyler] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Nayak, Michael; Lupu, Roxana; Marley, Mark S.; Robinson, Tyler] Maui High Performance Comp Ctr, Kihei, HI 96753 USA. [Nayak, Michael] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Nayak, Michael] Red Sky Res LLC, Edgewood, NM 87015 USA. [Fortney, Jonathan J.; Robinson, Tyler] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Lupu, Roxana] Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Lewis, Nikole] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. RP Nayak, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.; Nayak, M (reprint author), Maui High Performance Comp Ctr, Kihei, HI 96753 USA.; Nayak, M (reprint author), Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.; Nayak, M (reprint author), Red Sky Res LLC, Edgewood, NM 87015 USA. EM nayak@redskyresearch.org FU NASA High-End Computing (HEC) Program, through the NASA Advanced Supercomputing (NAS) division at the Ames Research Center; NASA Science Mission Directorate; National Defense Science and Engineering Graduate Fellowship (NDSEG) [32 CFR 168a]; Red Sky Research, LLC; WFIRST Preparatory Science Program; NASA through the Sagan Fellowship FX The NASA High-End Computing (HEC) Program, through the NASA Advanced Supercomputing (NAS) division at the Ames Research Center, provided resources supporting this work. Results reported herein benefited from collaborations and/or information exchange within NASA's Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by the NASA Science Mission Directorate. M.N. is supported by the National Defense Science and Engineering Graduate Fellowship (NDSEG, 32 CFR 168a) and Red Sky Research, LLC. M.S.M. acknowledges the support of the WFIRST Preparatory Science Program. T.R. gratefully acknowledges support from NASA through the Sagan Fellowship executed by the NASA Exoplanet Science Institute. The opinions, interpretations, and recommendations expressed here are those of the authors and are not necessarily endorsed by the US Air Force or the Department of Defense. NR 41 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD MAR 1 PY 2017 VL 129 IS 973 BP 1 EP 21 DI 10.1088/1538-3873/129/973/034401 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EM6OJ UT WOS:000395431700001 ER PT J AU Lopez-Pacheco, CP Nieto-Camacho, A Zarate-Reyes, L Garcia-Romero, E Suarez, M Kaufhold, S Zepeda, EG Cervini-Silva, J AF Paola Lopez-Pacheco, Cynthia Nieto-Camacho, Antonio Zarate-Reyes, Luis Garcia-Romero, Emilia Suarez, Mercedes Kaufhold, Stephan Garcia Zepeda, Eduardo Cervini-Silva, Javiera TI Sepiolite and palygorskite-underpinned regulation of mRNA expression of pro-inflammatory cytokines as determined by a murine inflammation model SO APPLIED CLAY SCIENCE LA English DT Article DE Therapeutic; Regulation; Cytokines; Expression of IL-1 and TNF-alpha ID SKIN INFLAMMATION; MOUSE EAR; GENE-EXPRESSION; EDEMA; MICE; INVOLVEMENT; INHIBITION; HISTAMINE; MIGRATION; ZEOLITES AB This paper shows that clay minerals, sepiolite and palygorskite collected from Torrejon El Rubio and Vallecas, Spain, respectively, altered the expression of four, namely, pro-inflammatory cytokines: interleukins IL-1 and IL-6, tumor necrosis factor (TNF-alpha), and interferon gamma (IFN-gamma) as determined using a 12-0tetradecanoylphorbol-13-acetate model for inflammation. Quantitative RT-PCR analyses after 4 and 24 h inflammatory stimuli showed that sepiolite or palygorskite brought about a reduction in mRNA expression. Sepiolite provoked, the highest mRNA expression inhibition for all cytokines, except for TNF-alpha, and primarily after 4 h. Conversely, the anti-inflammatory effect for cytoldne TNF-alpha was found to be true in the presence of palygorskite. Most notably, the significant reduction in mRNA expression of IL-1 registered just shortly.after exposure pointed to that the anti-inflammatory effect may be important for modulation of the late inflammatory response. These clay minerals caused modifications in the mRNA expression of IL-1 and its receptor in endothelial cells and downstreaming inflammatory cascades resulting in the recruitment of neutrophils. In addition, polymorphonuclear peroxidase activity was severely reduced just after short exposure to either sepiolite or palygorskite. Evidence provided herein agree well with the idea that these clay minerals impaired neutrophils infiltration to inflamed skin, notwithstanding ear edema and deficient cell localization to skin coupled with such impairment may affect the later stages of inflammation. (C) 2016 Elsevier B.V. All rights reserved. C1 [Paola Lopez-Pacheco, Cynthia; Zarate-Reyes, Luis; Garcia Zepeda, Eduardo] Univ Nacl Autonoma Mexico, Fac Quim, Posgrad Bioquim, Mexico City 04510, DF, Mexico. [Paola Lopez-Pacheco, Cynthia; Garcia Zepeda, Eduardo] Univ Nacl Autonoma Mexico, Inst Invest Biomed, Dept Inmunol, Chemokine Biol Res Lab, Sede Circuito Escolar Edificio A,Lab 019, Mexico City 04510, DF, Mexico. [Nieto-Camacho, Antonio] Univ Nacl Autonoma Mexico, Inst Quim, Lab Pruebas Biol, Mexico City 04510, DF, Mexico. [Garcia-Romero, Emilia] Univ Complutense Madrid, Dept Cristalog & Mineral, E-28040 Madrid, Spain. [Garcia-Romero, Emilia] Univ Complutense Madrid, CSIC, Inst Geociencias, E-28040 Madrid, Spain. [Suarez, Mercedes] Univ Salamanca, Dept Geol, E-37008 Salamanca, Spain. [Kaufhold, Stephan] Bundesanstalt Geowissensch & Rohstoffe, Stilleweg 2, D-30655 Hannover, Germany. [Cervini-Silva, Javiera] Univ Autonoma Metropolitana, Unidad Cuajimalpa, Dept Proc & Tecnol, Mexico City, DF, Mexico. [Cervini-Silva, Javiera] Lawrence Berkeley Natl Lab, Div Earth Sci, Berkeley, CA USA. [Cervini-Silva, Javiera] NASA, Astrobiol Inst, Washington, DC 20546 USA. RP Zepeda, EG (reprint author), Univ Nacl Autonoma Mexico, Inst Invest Biomed, Dept Inmunol, Chemokine Biol Res Lab, Sede Circuito Escolar Edificio A,Lab 019, Mexico City 04510, DF, Mexico.; Cervini-Silva, J (reprint author), Univ Autonoma Metropolitana, Div Ciencias Nat & Ingn, Dept Proc & Tecnol, Unidad Cuajimalpa, Prol Vasco de Quiroga 4871, Mexico City 05348, DF, Mexico. EM garciaze@unam.mx; jcervini@correo.cua.uam.mx NR 40 TC 0 Z9 0 U1 4 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-1317 EI 1872-9053 J9 APPL CLAY SCI JI Appl. Clay Sci. PD MAR 1 PY 2017 VL 137 BP 43 EP 49 DI 10.1016/j.clay.2016.12.006 PG 7 WC Chemistry, Physical; Materials Science, Multidisciplinary; Mineralogy SC Chemistry; Materials Science; Mineralogy GA EJ1WX UT WOS:000393002300007 ER PT J AU Cervini-Silva, J Ramirez-Apan, MT Kaufhold, S Palacios, E Gomez-Vidales, V Ufer, K del Angel, P Montoya, A AF Cervini-Silva, Javiera Teresa Ramirez-Apan, Maria Kaufhold, Stephan Palacios, Eduardo Gomez-Vidales, Virginia Ufer, Kristian del Angel, Paz Montoya, Ascencion TI Cell growth underpinned by sepiolite SO APPLIED CLAY SCIENCE LA English DT Article DE Human cancer; Surface charge; Porosity ID IN-VITRO BIOCOMPATIBILITY; EGF RECEPTOR; CHEMOSENSITIVITY; ANTIBACTERIAL; BENTONITE AB This paper reports the role of clay minerals, sepiolites, on the proliferation behaviour of human cancer cells. It reports as well on the proliferation of U251 (central nervous system, glioblastoma) and SKLU-1 (lung adenocarcinoma) cells by sepiolite bearing different extent of isomorphic substitution (IS), either because of the inclusion of Al3+, Fe3+2+, or Ti4+ in Si structural sites (IS at the tetrahedral sheet, T) or that of Ni2+ in Mg structural sites (IS at the octahedral sheet, O). Studied sepiolites were originally from Ampandrandara, Madagascar; Cerro del Almodovar, Spain; Deiva Forest, Italy; Eskidir, Turkey; Peguera, Falcondo Plant, Dominican Republic; Sepetcikoyii, Turkey; Shimien, China; and Vallecas, Spain. Furthermore, obtained results for sepiolites were compared against those for clays (bentonites). Diffractograms showed characteristic patterns for sepiolite, with no evidence of significant accumulation of secondary phases. XRF data confirmed the incorporation of Al, Fe and, Ti; and Ni, consistent with IS at T and O. The effect of sepiolite on cellular proliferation was determined using the SRB protocol. All sepiolites induced inhibition or increment on the proliferation response of U251 or SKLU cells, depending on the sepiolite; however no correlation between proliferation against composition or microporosity properties became evident. Most notably, sepiolite from Sepetcikoyu, Turkey, owning the highest microporosity (evidenced by surface area as) of the sepiolite series, 343 m(2) g(-1) exerted the highest proliferation response for U251 and SKLU-1 cells, namely, 100% inhibition and 22.8 +/- 12.1% increase, respectively. Sepiolites from Ampandrandara, Sepetcikoyu, and Deiva Forest, owing very low contents of Al (Al2O3 <= 0.2%) and variable sigma(s) yielded the highest inhibition in U251 cells proliferation, best accounted for by growth was limited by specific-adsorption mechanisms in which structural changes associated to Al-for-Si IS at T favoured the adsorption of metabolic growth components [epidermal growth factor receptor (EGFR)], thereby inhibiting the development of primary glioblastomas. On the other hand, increments (%) in SKLU-1 cells proliferation did not correlate with microporosity (measured as values), yet two data clusters were identified, higher and lower data values, i.e., 22.8 <= % increment <= 39% (sigma(s) = 83, 220, or 343 m(2) g(-1)) and 6.9 <= % increment <= 14.2% (96 <= sigma(s) <= 266). The second group was composed by Ampandrandara, Sepetcikoyu, and Deiva Forest, generating surface sites that catalyze the over expression of activin A. So, the growth behaviour for both U251 and SKLU-1 cells was affected by Al at T via Al-for-Si IS if proceeded to a small degree. In all, however, the overall chemical composition lacked to serve as predictor for growth. Structural considerations supported the idea that controlled cell growth by sepiolite was not limited by the retention of small solutes at inner surfaces. Finally, whether variations in microporosity exerted changes in the cell proliferation behaviour was strongly dependent if the phyllosilicate was a clay mineral (sepiolite) or a clay (bentonite). (C) 2016 Elsevier B.V. All rights reserved. C1 [Cervini-Silva, Javiera] Univ Autonoma Metropolitana, Unidad Cuajimalpa, Dept Proc & Tecnol, Col Santa Fe Cuajimalpa, Cdmx, Mexico. [Cervini-Silva, Javiera] Lawrence Berkeley Natl Lab, Div Earth Sci, Berkeley, CA USA. [Cervini-Silva, Javiera] NASA, Astrobiol Inst, Washington, DC 20546 USA. [Teresa Ramirez-Apan, Maria] Univ Nacl Autonoma Mexico, Inst Quim, Lab Pruebas Biol, Ciudad Univ, Mexico City, DF, Mexico. [Kaufhold, Stephan; Ufer, Kristian] BGR, Stilleweg 2, D-30655 Hannover, Germany. [Palacios, Eduardo; del Angel, Paz; Montoya, Ascencion] Inst Mexicano Petr, Direcc Invest & Posgrad, Mexico City, DF, Mexico. [Gomez-Vidales, Virginia] Univ Nacl Autonoma Mexico, Inst Quim, Lab Resonancia Paramagnet Elect, Ciudad Univ, Mexico City, DF, Mexico. RP Cervini-Silva, J (reprint author), Univ Automoma Metropolitana, Dept Proc & Tecnol, Av Vasco de Quiroga 4871, Col Santa Fe Cuajimalpa 05348, Cdmx, Mexico. EM jcervini@correo.cua.uam.mx FU Universidad Autonoma Metropolitana Unidad Cuajimalpa [33678] FX The authors thank Natascha Schleuning (Bundesansalt fur Geowissenschaften and Rohstoffe, BGR) for technical assistance. This project was supported in part by the Universidad Autonoma Metropolitana Unidad Cuajimalpa (Grant No. 33678). NR 27 TC 0 Z9 0 U1 5 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-1317 EI 1872-9053 J9 APPL CLAY SCI JI Appl. Clay Sci. PD MAR 1 PY 2017 VL 137 BP 77 EP 82 DI 10.1016/j.clay.2016.11.032 PG 6 WC Chemistry, Physical; Materials Science, Multidisciplinary; Mineralogy SC Chemistry; Materials Science; Mineralogy GA EJ1WX UT WOS:000393002300011 ER PT J AU Borner, A Panerai, F Mansour, NN AF Borner, Arnaud Panerai, Francesco Mansour, Nagi N. TI High temperature permeability of fibrous materials using direct simulation Monte Carlo SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER LA English DT Article DE DSMC; Carbon fiber; Permeability; Porosity ID POROUS-MEDIA; GAS-FLOW; CARBON; DENSITY; OXIDATION AB Porous carbon fiber materials are used as effective insulators in many applications where high temperatures are involved. In particular, they are used as the substrate of ablative thermal protection materials for atmospheric entry systems. In this application and in many other industrial uses, quantifying the permeability of porous materials is needed to compute the flow rate of gases through them, under certain environmental conditions. In this work, direct simulation Monte Carlo (DSMC) simulations are used to compute permeability of several fibrous substrates to high temperature gases. The actual porous geometry of the materials is digitized using X-ray microtomography. Numerical results at various pressures and Knudsen numbers are compared with experimental data published in the literature. The method confirms that the pressure dependence of effective gas permeability is well represented by the Klinkenberg formulation. The method is validated by showing close agreement between measurements of permeability from simulations and experimental investigations. Four carbon fiber materials with different microstructures are investigated. We show that the permeability strongly depends on the pore size distribution, as well as on the porosity of the material. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Borner, Arnaud] Univ Illinois, Dept Mech Sci & Engn, 4417 Mech Engn Lab MC-144,1206 West Green St, Urbana, IL 61801 USA. [Borner, Arnaud; Mansour, Nagi N.] NASA, Computat Phys Branch, Ames Res Ctr, Mail Stop 258-5, Moffett Field, CA 94035 USA. [Panerai, Francesco] Univ Kentucky, Dept Mech Engn, 151 Ralph G Anderson Bldg, Lexington, KY 40506 USA. RP Borner, A (reprint author), NASA, Ames Res Ctr, Mail Stop 258-6, Moffett Field, CA 94035 USA. EM arnaud.p.borner@nasa.gov FU NASA EAP Program; Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy [DE-AC02-05CH11231] FX The authors are indebted to Drs. M. Gallis and S. Plimpton (Sandia National Laboratories) for their assistance with SPARTA, and J. Ferguson (University of Kentucky) for fruitful discussions. Drs. A. A. McDowell and D.Y. Parkinson are gratefully acknowledged for their help in the LBNL/NASA Ames collaboration on micro-CT measurements. This work was performed under the Entry System Modeling Project (M J. Wright project manager) of the NASA Game Changing Development (GCD) Program. This work was partially supported by NASA EAP Program administered by USRA. The Advanced Light Source is supported by the Director, Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. NR 33 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 0017-9310 EI 1879-2189 J9 INT J HEAT MASS TRAN JI Int. J. Heat Mass Transf. PD MAR PY 2017 VL 106 BP 1318 EP 1326 DI 10.1016/j.ijheatmasstransfer.2016.10.113 PG 9 WC Thermodynamics; Engineering, Mechanical; Mechanics SC Thermodynamics; Engineering; Mechanics GA EJ2BN UT WOS:000393015000116 ER PT J AU Bukowsky, CR Grandidier, J Fountaine, KT Callahan, DM Stanbery, BJ Atwater, HA AF Bukowsky, Colton R. Grandidier, Jonathan Fountaine, Katherine T. Callahan, Dennis M. Stanbery, Billy J. Atwater, Harry A. TI Photon and carrier management design for nonplanar thin-film copper indium gallium selenide photovoltaics SO SOLAR ENERGY MATERIALS AND SOLAR CELLS LA English DT Article DE Solar cells; Thin film; Light trapping; CIGS; Nanotextured ID NANOSTRUCTURED SOLAR-CELLS; EFFICIENCY; OPTIMIZATION; ABSORPTION; DEVICES; ARRAYS AB Nonplanar structured photovoltaic absorber design has potential to achieve high solar cell efficiency with significantly reduced material use. We report optoelectronic simulations that highlight photon and generated carrier management opportunities for improvement of thin film Cu(InxGa1-x)Se-2 (CIGS) device performance. Structures realized via either self-assembly or patterning via nanoimprint lithography, and also a combination of both are predicted to exhibit significant increases in short circuit current density and open circuit voltage simultaneously. The structures investigated include: 1) self-assembled nonplanar structures that strongly scatter incident light and enhance carrier generation near regions of high electric potential, 2) lithographically patterned embedded periodic dielectric structures, 3) planar dielectric layers that separate the CIGS absorber from the molybdenum back-contact via reduced-area contacts that minimize optical and electronic losses, 4) a combination of these for combined effects. We find that the self-assembled nonplanar CIGS cells with 700 nm planar equivalent Thickness, combined with dielectric separation layers yield increases in short circuit current density and open circuit voltage up to 3.4 mA cm(-2) and 29 mV, respectively. The absolute efficiency increases from 15.4% to 18.1%, compared to the predicted efficiency for planar CIGS thin film cells of equivalent thickness. The addition of a single layer MgF2 anti-reflection coating brings the maximum predicted efficiency up to 19.7% for randomly textured devices. C1 [Bukowsky, Colton R.; Grandidier, Jonathan; Fountaine, Katherine T.; Callahan, Dennis M.; Atwater, Harry A.] CALTECH, 1200 E Calif Dr, Pasadena, CA 91125 USA. [Grandidier, Jonathan] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Fountaine, Katherine T.] Northrup Grumman Aerosp Syst, NG Next, One Space Pk Dr, Redondo Beach, CA 90278 USA. [Callahan, Dennis M.] Charles Stark Draper Lab Inc, 555 Technology Sq, Cambridge, MA 02139 USA. [Stanbery, Billy J.] HelioVolt Corp, 6301 E Stassney Ln, Austin, TX 78744 USA. [Stanbery, Billy J.] Siva Power, 5102 Calle Sol, Santa Clara, CA 95054 USA. RP Bukowsky, CR; Atwater, HA (reprint author), CALTECH, 1200 E Calif Dr, Pasadena, CA 91125 USA. EM cb@caltech.edu; haa@caltech.edu OI Fountaine, Katherine/0000-0002-0414-8227 FU U.S. Department of Energy [DE-EE0004946]; Bay Area Photovoltaic Consortium [DE-EE0004946]; Joint Center for Artificial Photosynthesis; DOE Energy Innovation Hub, through the Office of Science of the U.S. Department of Energy [DE-SC0004993]; National Science Foundation [DGE-1144469] FX The authors thank Hal Emmer, Chris T. Chen, Yulia Tolstova, and Stefan Olmelcheko for helpful discussions. Dr. Stanbery acknowledges the HelioVolt team of co-inventors that developed the processing technology to create these nanotextured absorbers [10]. This work was supported by the U.S. Department of Energy and the Bay Area Photovoltaic Consortium under award number DE-EE0004946 (C.R.B. and D.M.C.) and the Joint Center for Artificial Photosynthesis (KT.F. and H.A.A.), a DOE Energy Innovation Hub, supported through the Office of Science of the U.S. Department of Energy under Award No. DE-SC0004993. K.T. Fountaine was supported by the National Science Foundation Graduate Research Fellowship under Grant No DGE-1144469. NR 39 TC 0 Z9 0 U1 11 U2 11 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-0248 EI 1879-3398 J9 SOL ENERG MAT SOL C JI Sol. Energy Mater. Sol. Cells PD MAR PY 2017 VL 161 BP 149 EP 156 DI 10.1016/j.solmat.2016.11.008 PG 8 WC Energy & Fuels; Materials Science, Multidisciplinary; Physics, Applied SC Energy & Fuels; Materials Science; Physics GA EJ6RR UT WOS:000393347000014 ER PT J AU Ito, T Wang, O AF Ito, Takamitsu Wang, Ou TI Transit Time Distribution based on the ECCO-JPL Ocean Data Assimilation SO JOURNAL OF MARINE SYSTEMS LA English DT Article DE Transit Time Distribution; Ocean Data Assimilation; CFC-11 ID OXYGEN UTILIZATION RATES; GLOBAL GENERAL-CIRCULATION; ANTHROPOGENIC CO2; PACIFIC-OCEAN; SULFUR-HEXAFLUORIDE; NORTH-ATLANTIC; WEDDELL SEA; WATER; CARBON; CHLOROFLUOROCARBONS AB Oceanic water mass is a mixture of waters with varying ages, and the Transit Time Distribution (TTD) measures its age spectrum. We construct a model-based TTD using the data-constrained circulation fields from the ECCO-JPL Ocean Data Assimilation, and test it against the observed and directly simulated distribution of pCFC-11 from the Pacific and Atlantic basins. The ECCO-JPL circulation provides overall reliable estimates of the upper ocean ventilation rates suitable for biogeochemical studies. Observed distributions of pCFC-11 in the upper ocean thermocline are well reproduced by the convolution integral of the model-based TTD (mean bias <6%, spatial correlation > 0.87) but there are significant regional biases in particular near the base of the thermocline and in the deep water formation regions. The model underestimates the deep pCFC-11 (>2000 m) in the North Atlantic and in the Southern Ocean. The ratio between the mean and the spread of the age spectrum (Gamma/Delta) is close to unity (mean = 1.04, median = 0.99) in the ventilated thermodine of the Pacific basin but there are significant regional variations of the ratio. (C) 2016 Published by Elsevier B.V. C1 [Ito, Takamitsu] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Wang, Ou] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Ito, T (reprint author), Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. EM taka.ito@eas.gatech.edu FU U.S. National Science Foundation [OCE-1357373, PLR-1142009]; National Aeronautics and Space Administration (NASA) FX TI is supported by the U.S. National Science Foundation Grant Numbers OCE-1357373 and PLR-1142009. 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). NR 48 TC 0 Z9 0 U1 3 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0924-7963 EI 1879-1573 J9 J MARINE SYST JI J. Mar. Syst. PD MAR PY 2017 VL 167 BP 1 EP 10 DI 10.1016/j.jmarsys.2016.10.015 PG 10 WC Geosciences, Multidisciplinary; Marine & Freshwater Biology; Oceanography SC Geology; Marine & Freshwater Biology; Oceanography GA EJ0LE UT WOS:000392899300001 ER PT J AU Mangold, N Schmidt, ME Fisk, MR Forni, O McLennan, SM Ming, DW Sautter, V Sumner, D Williams, AJ Clegg, SM Cousin, A Gasnault, O Gellert, R Grotzinger, JP Wiens, RC AF Mangold, N. Schmidt, M. E. Fisk, M. R. Forni, O. McLennan, S. M. Ming, D. W. Sautter, V. Sumner, D. Williams, A. J. Clegg, S. M. Cousin, A. Gasnault, O. Gellert, R. Grotzinger, J. P. Wiens, R. C. TI Classification scheme for sedimentary and igneous rocks in Gale crater, Mars SO ICARUS LA English DT Article ID SCIENCE LABORATORY MISSION; CHEMCAM INSTRUMENT SUITE; X-RAY SPECTROMETER; CHEMICAL CLASSIFICATION; CLASTIC SEDIMENTS; CURIOSITY ROVER; VOLCANIC-ROCKS; CRUST; CONSTRAINTS; CALIBRATION AB Rocks analyzed by the Curiosity rover in Gale crater include a variety of clastic sedimentary rocks and igneous float rocks transported by fluvial and impact processes. To facilitate the discussion of the range of lithologies, we present in this article a petrological classification framework adapting terrestrial classification schemes to Mars compositions (such as Fe abundances typically higher than for comparable lithologies on Earth), to specific Curiosity observations (such as common alkali-rich rocks), and to the capabilities of the rover instruments. Mineralogy was acquired only locally for a few drilled rocks, and so it does not suffice as a systematic classification tool, in contrast to classical terrestrial rock classification. The core of this classification involves (1) the characterization of rock texture as sedimentary, igneous or undefined according to grain/crystal sizes and shapes using imaging from the ChemCam Remote Micro Imager (RMI), Mars Hand Lens Imager (MAHLI) and Mastcam instruments, and (2) the assignment of geochemical modifiers based on the abundances of Fe, Si, alkali, and S determined by the Alpha Particle X-ray Spectrometer (APXS) and ChemCam instruments. The aims are to help understand Gale crater geology by highlighting the various categories of rocks analyzed by the rover. Several implications are proposed from the cross-comparisons of rocks of various texture and composition, for instance between in place outcrops and float rocks. All outcrops analyzed by the rover are sedimentary; no igneous outcrops have been observed. However, some igneous rocks are clasts in conglomerates, suggesting that part of them are derived from the crater rim. The compositions of in-place sedimentary rocks contrast significantly with the compositions of igneous float rocks. While some of the differences between sedimentary rocks and igneous floats may be related to physical sorting and diagenesis of the sediments, some of the sedimentary rocks (e.g., potassic rocks) cannot be paired with any igneous rocks analyzed so far. In contrast, many float rocks, which cannot be classified from their poorly defined texture, plot on chemistry diagrams close to float rocks defined as igneous from their textures, potentially constraining their nature. (C) 2016 Elsevier Inc. All rights reserved. C1 [Mangold, N.] Univ Nantes, CNRS, LPG Nantes, F-44322 Nantes, France. [Schmidt, M. E.] Brock Univ, Dept Earth Sci, St Catharines, ON, Canada. [Fisk, M. R.] Oregon State Univ, Corvallis, OR 97331 USA. [Forni, O.; Cousin, A.; Gasnault, O.] Univ Toulouse, UPS OMP, CNRS, Inst Rech Astrophys & Planetol, Toulouse, France. [McLennan, S. M.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. [Ming, D. W.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Sautter, V.] Museum Natl Hist Nat, IMPMC, Paris, France. [Sumner, D.] Univ Calif Davis, Davis, CA 95616 USA. [Williams, A. J.] Towson Univ, Towson, MD USA. [Clegg, S. M.; Wiens, R. C.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Gellert, R.] Univ Guelph, Guelph, ON N1G 2W1, Canada. [Grotzinger, J. P.] CALTECH, Pasadena, CA 91125 USA. EM nicolas.mangold@univ-nantes.fr OI Williams, Amy/0000-0001-6299-0845 FU Canadian Space Agency (CSA); French space agency; Centre National d'Etudes Spatiales (CNES); NASA FX Imaging and chemical data presented here are available in the NASA Planetary Data System (PDS) http://pds-geosciences.wustl.edu/missions/msl. We are grateful to the MSL engineering and management teams (and especially the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA) for making the mission and this scientific investigation possible and to science team members who contributed to mission operations. The APXS instrument is managed and financed by the Canadian Space Agency (CSA). Development and operation of the ChemCam instrument was supported in France by funds from the French space agency, Centre National d'Etudes Spatiales (CNES) and in the US by NASA funding to the Mars Exploration Program. NR 72 TC 0 Z9 0 U1 22 U2 22 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR 1 PY 2017 VL 284 BP 1 EP 17 DI 10.1016/j.icarus.2016.11.005 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EI5XM UT WOS:000392569600001 ER PT J AU Bills, BG Scott, BR AF Bills, Bruce G. Scott, Bryan R. TI Secular obliquity variations of Ceres and Pallas SO ICARUS LA English DT Article DE Ceres; Pallas; Asteroid; Rotation ID ASTEROIDS; PRECESSION; EVOLUTION; NUTATION; MOTION; VESTA; MODEL; POLE AB We examine variations in the orientations of the orbit poles and spin poles of Ceres and Pallas, on time scales of a few million years. We consider these two bodies together because they have similar orbits, but very different present states of knowledge concerning internal mass distribution and spin pole orientation. For Ceres, the Dawn mission has recently provided accurate estimates of the current spin pole orientation, and the degree 2 spherical harmonics of the gravitational potential. The polar moment of inertia is not as well constrained, but plausible bounds are known. For Pallas, we have estimates of the shape of the body, and spin pole orientation and angular rate, all derived from optical light curves. Using those input parameters, and the readily computed secular variations in the orbit pole, we can compute long term variations in the spin pole orientation. This provides information concerning long term variations in insolation, which controls stability of surface volatiles. (C) 2016 Published by Elsevier Inc. C1 [Bills, Bruce G.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Scott, Bryan R.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. EM bruce.bills@jpl.nasa.gov FU Dawn mission FX Part of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Support was provided to BGB by the Dawn mission. We appreciate conversations with Ryan Park and Francis Nimmo, and constructive suggestions from two anonymous reviewers. NR 33 TC 1 Z9 1 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 MAR 1 PY 2017 VL 284 BP 59 EP 69 DI 10.1016/j.icarus.2016.10.024 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EI5XM UT WOS:000392569600005 ER PT J AU Alvarellos, JL Dobrovolskis, AR Zahnle, KJ Hamill, P Dones, L Robbins, S AF Alvarellos, Jose Luis Dobrovolskis, Anthony R. Zahnle, Kevin J. Hamill, Patrick Dones, Luke Robbins, Stuart TI Fates of satellite ejecta in the Saturn system, II SO ICARUS LA English DT Article DE Saturn; Satellites; Cratering; Impact processes; Satellites; Dynamics ID CRATERING RATES; ENCELADUS; SECONDARY; EUROPA; FRAGMENTS; BEHAVIOR; GANYMEDE; IMPACTS; SURFACE; ORBITS AB We assess the fates of ejecta from the large craters Aeneas on Dione and Ali Baba on Enceladus (161 and 39 km in diameter, respectively), as well as that from Herschel (130 km in diameter) on Mimas. The ejecta are treated either as 'spalls' launched from hard surfaces, or as 'rubble' launched from a weak rubble pile regolith. Once in orbit we consider the ejecta as massless test particles subject to the gravity of Saturn and its classical satellites. The great majority of escaped ejecta get swept up by the source moons. The best fit to the ejecta population decay is a stretched exponential with exponent near 1/2 (Dobrovolskis et al., Icarus 188, 481-505, 2007). We bracket the characteristic ejecta sizes corresponding to Grady-Kipp fragments and spalls. Based on this and computed impact velocities and incidence angles, the resulting sesquinary craters, if they exist, should have diameters on the order of a few meters to a few km. The observed longitude distribution of small craters on Mimas along with the findings of Bierhaus et al. that small moons should not have a secondary crater population (Icarus 218, 602-621, 2012) suggest that the most likely place to find sesquinary craters in the Saturn system is the antapex of Mimas. (C) 2016 Elsevier Inc. All rights reserved. C1 [Alvarellos, Jose Luis] SSL, 3825 Fabian Way,MS G-76, Palo Alto, CA 94303 USA. [Dobrovolskis, Anthony R.] SETI Inst, MS 245-3, Moffett Field, CA 94035 USA. [Zahnle, Kevin J.] NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA. [Hamill, Patrick] San Jose State Univ, Dept Phys, San Jose, CA 95192 USA. [Dones, Luke; Robbins, Stuart] Southwest Res Inst, 1050 Walnut St,Suite 300, Boulder, CO 80302 USA. EM jl_alvarellos@yahoo.com FU Cassini Data Analysis Program; National Aeronautics and Space Administration FX J.L.A. would like to acknowledge K. Singer for useful discussions. Thanks to R. Jacobson for providing initial conditions. JLA thanks the patience of my "pichus": Alejandra, Jose Jr., Isabella and Danito. This work has made use of NASA's Astrophysics Data System (ADS located at http://adswww.harvard.edu) and was written using TeXMaker ver. 3.5.2. We thank the Cassini Data Analysis Program as well as the National Aeronautics and Space Administration for support. This paper greatly benefited from the reviews of S. Charnoz and an anonymous referee, both of whom are duly acknowledged. This paper is dedicated to the memory of Victor Ramon Alvarellos (1941-2016). NR 47 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 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR 1 PY 2017 VL 284 BP 70 EP 89 DI 10.1016/j.icarus.2016.10.028 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EI5XM UT WOS:000392569600006 ER PT J AU Gacesa, M Lewkow, N Kharchenko, V AF Gacesa, M. Lewkow, N. Kharchenko, V. TI Non-thermal production and escape of OH from the upper atmosphere of Mars SO ICARUS LA English DT Article ID HOT OXYGEN CORONA; MARTIAN ATMOSPHERE; SOLAR-WIND; PHOTOCHEMICAL ESCAPE; CROSS-SECTIONS; MAVEN; VARIABILITY; SCATTERING; MOLECULES; EMISSION AB We present a theoretical analysis of formation and kinetics of hot OH molecules in the upper atmosphere of Mars produced in reactions of thermal molecular hydrogen and energetic oxygen atoms. Two major sources of energetic O considered are the photochemical production, via dissociative recombination of O-2(+) ions, and energizing collisions with fast atoms produced by the precipitating Solar Wind (SW) ions, mostly H+ and He2+, and energetic neutral atoms (ENAs) originating in the charge-exchange collisions between the SW ions and atmospheric gases. Energizing collisions of 0 with atmospheric secondary hot atoms, induced by precipitating SW ions and ENAs, are also included in our consideration. The non-thermal reaction O + H-2(v, j) -> H + OH(v', j') is described using recent quantum mechanical state-to-state cross sections, which allow us to predict non-equilibrium distributions of excited rotational and vibrational states (v', j') of OH and expected emission spectra. A fraction of produced translationally hot OH is sufficiently energetic to overcome Mars' gravitational potential and escape into space, contributing to the hot corona. We estimate its total escape flux from the dayside of Mars for low solar activity conditions at about 1.1 x 10(23) s(-1), or about 0.1% of the total escape rate of atomic O and H. The described non-thermal OH production mechanism is general and expected to contribute to the evolution of atmospheres of the planets, satellites, and exoplanets with similar atmospheric compositions. (C) 2016 Elsevier Inc. All rights reserved. C1 [Gacesa, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Lewkow, N.; Kharchenko, V.] Univ Connecticut, Dept Phys, Storrs, CT 06268 USA. [Kharchenko, V.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. EM marko.gacesa@nasa.gov; nlewkow@gmail.com; kharchenko@cfa.harvard.edu OI Gacesa, Marko/0000-0001-5145-051X NR 47 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 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR 1 PY 2017 VL 284 BP 90 EP 96 DI 10.1016/j.icarus.2016.10.030 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EI5XM UT WOS:000392569600007 ER PT J AU Farnham, TL Kelley, MSP A'Hearn, MF Feaga, LM Bodewits, D Sunshine, JM Wellnitz, DD Wissler, S AF Farnham, T. L. Kelley, M. S. P. A'Hearn, M. F. Feaga, L. M. Bodewits, D. Sunshine, J. M. Wellnitz, D. D. Wissler, S. TI Comet C/2012 S1 (ISON): Final observations from the Deep Impact spacecraft SO ICARUS LA English DT Article DE Comets, coma; Comets, dynamics; Comets, dust ID HELIOCENTRIC DISTANCE; 67P/CHURYUMOV-GERASIMENKO; MORPHOLOGY; OUTBURSTS; NUCLEUS AB The Deep Impact spacecraft observed comet C/2012 S1 (ISON) between 17 January and 10 March 2013 when the comet was similar to 5 AU from the Sun. Continuous, high-cadence, images spanning as much as 6 days at a time, and high-cadence IR spectral scans spanning 2 days, represent the most intensive set of observations available from the early part of ISON's apparition. These observations were used to investigate the comet's detailed behavior, including variability in the lightcurve and changes in the coma morphology. ISON experienced a gradual brightening throughout this time period, with A(0)f rho increasing from 1150 cm in January to 1430 cm in March. Although no periodic variability was detected to a level <3%, DI did record several events showing the comet spontaneously brightening by 10-15% for several hours, indicating that the comet was experiencing spontaneous bursts of enhanced activity. These small outbursts may be the result of residual pockets of the volatiles that drove the rapid brightening seen between 8 and 5 AU. No changes were detected in the coma morphology over the course of the observations, and no gas emission was detected in either the narrowband comet gas filters or the IR spectra. (C) 2016 Elsevier Inc. All rights reserved. C1 [Farnham, T. L.; Kelley, M. S. P.; A'Hearn, M. F.; Feaga, L. M.; Bodewits, D.; Sunshine, J. M.; Wellnitz, D. D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Wissler, S.] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM farnham@astro.umd.edu OI Bodewits, Dennis/0000-0002-2668-7248; Kelley, Michael/0000-0002-6702-7676; A'Hearn, Michael/0000-0002-9362-1193 FU NASA [NNM07AA99C] FX This work was funded by NASA, through the Discovery Program, via contract NNM07AA99C to the University of Maryland. We would also like to thank Rich Rieber, Amy Walsh and Kyle Bygott for diagnosing the problem that led to the spacecraft demise, and Tim Larson and all the personnel at the Jet Propulsion Laboratory and Ball Aerospace who worked to make Deep Impact's eight year mission such a success. Thanks to Jian-Yang Li and an anonymous reviewer for their comments. NR 38 TC 0 Z9 0 U1 1 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR 1 PY 2017 VL 284 BP 106 EP 113 DI 10.1016/j.icarus.2016.11.015 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EI5XM UT WOS:000392569600009 ER PT J AU Schunova-Lilly, E Jedicke, R Veres, P Denneau, L Wainscoat, RJ AF Schunova-Lilly, Eva Jedicke, Robert Veres, Peter Denneau, Larry Wainscoat, Richard J. TI The size-frequency distribution of H > 13 NEOs and ARM target candidates detected by Pan-STARRS1 SO ICARUS LA English DT Article DE Near-Earth objects; Asteroids; Asteroids; Dynamics ID NEAR-EARTH OBJECTS; SURVEY TELESCOPE ARRAY; PAN-STARRS; DYNAMICAL EVOLUTION; PHYSICAL-PROPERTIES; MAIN-BELT; ASTEROIDS; CHELYABINSK; IMPACTORS; AIRBURST AB We determine the absolute magnitude (H) distribution (or size-frequency distribution, SFD; N(H)alpha 10(alpha H) where a is the slope of the distribution) for near-Earth objects (NEO) with 13 < H < 30 and Asteroid Retrieval Mission (ARM) targets with 27 < H < 31 that were detected by the 1st telescope of the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS1; e.g. Kaiser et al., 2002; Kaiser, 2004; Hodapp et al., 2004). The NEO and ARM target detection efficiencies were calculated using the Greenstreet et al. (2012) NEO orbit distribution. The debiased Pan-STARRS1 NEO absolute magnitude distribution is more complex than a single slope power law - it shows two transitions - at H similar to 16 from steep to shallow slope, and in the 21 < H < 23 interval from a shallow to steep slope, which is consistent with other recent works (e.g. Mainzer et al., 2011c; Brown et al., 2013; Harris and D'Abramo, 2015). We fit alpha = 0.48 +/- 0.02 for NEOs with 13 < H < 16, alpha = 0.33 +/- 0.01 for NEOs with 16 < H < 22, and alpha = 0.62 +/- 0.03 for the smaller objects with H > 22. There is also another change in slope from steep to shallow around H = 27. The three ARM target candidates detected by Pan-STARRS1 in one year of surveying have a corrected SFD with slope alpha = 0.40(-0.45)(+0.33). We also show that the window for follow up observations of small (H greater than or similar to 22) NEOs with the NASA IRTF telescope and Arecibo and Goldstone radars are extremely short-on order of days, and procedures for fast response must be implemented in order to measure physical characteristics of small Earth approaching objects. CFHT's MegaCam and Pan-STARRSI have longer observing windows and are capable of following-up more NEOs due to their deeper limiting magnitudes and wider fields of view. (C) 2016 Elsevier Inc. All rights reserved. C1 [Schunova-Lilly, Eva; Jedicke, Robert; Denneau, Larry; Wainscoat, Richard J.] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. [Veres, Peter] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM eva.schunova@gmail.com OI Jedicke, Robert/0000-0001-7830-028X FU National Aeronautics and Space Administration [NNX08AR22G, NNX12AR65G, NNX14AM74G]; National Science Foundation [AST-1238877] FX The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant Nos. NNX08AR22G, NNX12AR65G, and NNX14AM74G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE) and the Los Alamos National Laboratory. NR 47 TC 0 Z9 0 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 MAR 1 PY 2017 VL 284 BP 114 EP 125 DI 10.1016/j.icarus.2016.11.010 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EI5XM UT WOS:000392569600010 ER PT J AU Tsapin, A Jones, S Petkov, M Borchardt, D Anderson, M AF Tsapin, A. Jones, S. Petkov, M. Borchardt, D. Anderson, M. TI Aerogel volatiles concentrator and analyzer (AVCA) - Collection and concentration of trace volatile organics in aerogel for spectroscopic detection SO ICARUS LA English DT Article DE Aerogel; Spectroscopic analysis; Volatile detection ID POLYCYCLIC AROMATIC-HYDROCARBONS; SOL-GEL PROCESS; CHEMISTRY; METEORITES; COMETARY; DUST AB A study was conducted to determine the efficacy of using silica aerogel to collect and concentrate ambient trace organics for spectroscopic analysis. Silica aerogel was exposed to atmospheres containing trace amounts of polycyclic aromatic and aliphatic hydrocarbons. The organics present were concentrated in the aerogels by factors varying from 10 to more than 1000 over the levels found in the atmospheres, depending on the specific organic present. Since silica aerogel is transparent over a wide range of optical and near infrared wavelengths, UV-induced fluorescence, Raman and infrared spectroscopies were used to detect and identify the organics collected by the aerogel. Measurements were conducted to determine the sensitivity of these spectroscopic methods for determining organics concentrated by aerogels and the effectiveness of this method for identifying systems containing multiple organic species. Polycyclic aromatic hydrocarbons (PAHs) were added to simulated Mars regolith and then vaporized by modest heating in the presence of aerogel. The aerogels adsorbed and concentrated the PAHs, which were detected by induced fluorescence and Raman and FTIR spectroscopies. (C) 2016 Elsevier Inc. All rights reserved. C1 [Tsapin, A.; Borchardt, D.] Univ Calif Riverside, 900 Univ Ave, Riverside, CA 92521 USA. [Jones, S.; Petkov, M.; Anderson, M.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 125-109, Pasadena, CA 91109 USA. EM steven.m.jones@jpl.nasa.gov NR 22 TC 0 Z9 0 U1 5 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR 1 PY 2017 VL 284 BP 150 EP 156 DI 10.1016/j.icarus.2016.11.001 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EI5XM UT WOS:000392569600012 ER PT J AU Register, PJ Mathias, DL Wheeler, LF AF Register, Paul J. Mathias, Donovan L. Wheeler, Lorien F. TI Asteroid fragmentation approaches for modeling atmospheric energy deposition SO ICARUS LA English DT Article DE Meteors; Asteroids; Near-earth objects; Asteroid dynamics; Fragmentation ID IMPACTS AB During asteroid entry, energy is deposited in the atmosphere through thermal ablation and momentum loss due to aerodynamic drag. Analytic models of asteroid entry and breakup physics are used to compute the energy deposition, which can then be compared against measured light curves and used to estimate ground damage due to airburst events. This work assesses and compares energy deposition results from four existing approaches to asteroid breakup modeling, and presents a new model that combines key elements of those approaches. The existing approaches considered include a liquid drop or "pancake" model where the object is treated as a single deforming body, and a set of discrete fragment models where the object breaks progressively into individual fragments. The new model incorporates both independent fragments and aggregate debris clouds to represent a broader range of fragmentation behaviors and reproduce more detailed light curve features. All five models are used to estimate the energy deposition rate versus altitude for the Chelyabinsk meteor impact, and results are compared with an observationally derived energy deposition curve. Comparisons show that four of the five approaches are able to match the overall observed energy deposition profile, but the features of the combined model are needed to better replicate both the primary and secondary peaks of the Chelyabinsk curve. (C) 2016 The Authors. Published by Elsevier Inc. C1 [Register, Paul J.] Vanderbilt Univ, PMB 401807,2301 Vanderbilt Pl, Nashville, TN 37235 USA. [Mathias, Donovan L.] NASA, Ames Res Ctr, MS 258-5, Moffett Field, CA 94035 USA. [Wheeler, Lorien F.] NASA, Ames Res Ctr, CSRA, MS 258-6, Moffett Field, CA 94035 USA. EM paul.j.register@vanderbilt.edu; donovan.mathias@nasa.gov; lorien.wheeler@nasa.gov FU NASA's Planetary Defense Coordination Office (PDCO); San Jose State University Foundation FX This work was funded by NASA's Planetary Defense Coordination Office (PDCO), and was partially performed under a grant supported by the San Jose State University Foundation. The authors would also like to thank Jessie Dotson, Michael Aftosmis, and David Morrison of NASA Ames for their reviews and support in preparing this manuscript. NR 20 TC 0 Z9 0 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 MAR 1 PY 2017 VL 284 BP 157 EP 166 DI 10.1016/j.icarus.2016.11.020 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EI5XM UT WOS:000392569600013 ER PT J AU Kelley, MSP Woodward, CE Gehrz, RD Reach, WT Harker, DE AF Kelley, Michael S. P. Woodward, Charles E. Gehrz, Robert D. Reach, William T. Harker, David E. TI Mid-infrared spectra of comet nuclei SO ICARUS LA English DT Article DE Comets; Comets nucleus; Comets composition; Infrared observations; Spectroscopy; Asteroid surfaces ID SPITZER-SPACE-TELESCOPE; NEAR-EARTH ASTEROIDS; MULTIBAND IMAGING PHOTOMETER; DEEP-IMPACT; TROJAN ASTEROIDS; INFRARED-SPECTROSCOPY; P/AREND-RIGAUX; 9P/TEMPEL 1; HALE-BOPP; WATER-ICE AB Comet nuclei and D-type asteroids have several similarities at optical and near-IR wavelengths, including near-featureless red reflectance spectra, and low albedos. Mineral identifications based on these characteristics are fraught with degeneracies, although some general trends can be identified. In contrast, spectral emissivity features in the mid-infrared provide important compositional information that might not otherwise be achievable. Jovian Trojan D-type asteroids have emissivity features strikingly similar to comet comae, suggesting that they have the same compositions and that the surfaces of the Trojans are highly porous. However, a direct comparison between a comet and asteroid surface has not been possible due to the paucity of spectra of comet nuclei at mid-infrared wavelengths. We present 5-35 mu m thermal emission spectra of comets 10P/Tempel 2, and 49P/Arend-Rigaux observed with the Infrared Spectrograph on the Spitzer Space Telescope. Our analysis reveals no evidence for a coma or tail at the time of observation, suggesting the spectra are dominated by the comet nucleus. We fit each spectrum with the near-Earth asteroid thermal model (NEATM) and find sizes in agreement with previous values. However, the NEATM beaming parameters of the nuclei, 0.74-0.83, are systematically lower than the Jupiter-family comet population mean of 1.03 +/- 0.11, derived from 16- and 22-mu m photometry. We suggest this may be either an artifact of the spectral reduction, or the consequence of an emissivity low near 16 gm. When the spectra are normalized by the NEATM model, a weak 10-mu m silicate plateau is evident, with a shape similar to those seen in mid-infrared spectra of D-type asteroids. A silicate plateau is also evident in previously published Spitzer spectra of the nucleus of comet 9P/Tempel 1. We compare, in detail, these comet nucleus emission features to those seen in spectra of the Jovian Trojan D-types (624) Hektor, (911) Agamemnon, and (1172) Aneas, as well as those seen in the spectra of seven comet comae. The comet comae present silicate features with two distinct shapes, either trapezoidal, or more rounded, the latter apparently due to enhanced emission near 8 to 8.5 mu m. The surfaces of Tempel 2, Arend-Rigaux, and Hektor best agree with the comae that present trapezoidal features, furthering the hypothesis that the surfaces of these targets must have high porosities in order to exhibit a spectrum similar to a comet coma. An emissivity minimum at 15 mu m, present in the spectra of Tempel 2, Arend-Rigaux, Hektor, and Agamemnon, is also described, the origin of which remains unidentified. The compositional similarity between D-type asteroids and comets is discussed, and our data supports the hypothesis that they have similar origins in the early Solar System. (C) 2016 Elsevier Inc. All rights reserved. C1 [Kelley, Michael S. P.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Woodward, Charles E.; Gehrz, Robert D.] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, 116 Church St S E, Minneapolis, MN 55455 USA. [Reach, William T.] Univ Space Res Corp, Stratospher Observ Infrared Astron, NASA, Ames Res Ctr, MS 232-11, Moffett Field, CA 94035 USA. [Harker, David E.] Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM mslc@astro.umd.edu OI Kelley, Michael/0000-0002-6702-7676 FU NASA (USA) Planetary Astronomy Program award [NNX13AH67G]; Emerging Worlds Program award [NNX16ADD33G]; NASA (USA) [1256406, 1215746] FX The authors thank the three referees for comments that improved this paper, J. P. Emery for sharing the Jovian Trojan spectra from Emery et al. (2006), and C. M. Lisse for sharing the spectra of comet Tempel 1 from Lisse et al. (2005). M.S.P.K. and D.E.H. were supported for this work by the NASA (USA) Planetary Astronomy Program award NNX13AH67G. C.E.W. was supported by Emerging Worlds Program award NNX16ADD33G. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA (USA). R.D.G., C.E.W., and M.S.P.K. were supported for these observations by NASA (USA) through Contract Nos. 1256406 and 1215746 issued by JPL/Caltech to the University of Minnesota. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration, 2013). This research also made use of Tiny Tim/Spitzer (STinyTim), developed by John Krist for the Spitzer Science Center. The Center is managed by the California Institute of Technology under a contract with NASA (USA). NR 106 TC 0 Z9 0 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 MAR 1 PY 2017 VL 284 BP 344 EP 358 DI 10.1016/j.icarus.2016.11.029 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EI5XM UT WOS:000392569600025 ER PT J AU Vasavada, AR Piqueux, S Lewis, KW Lemmon, MT Smith, MD AF Vasavada, Ashwin R. Piqueux, Sylvain Lewis, Kevin W. Lemmon, Mark T. Smith, Michael D. TI Thermophysical properties along Curiosity's traverse in Gale crater, Mars, derived from the REMS ground temperature sensor SO ICARUS LA English DT Article DE Mars; Surface geological processes; Infrared observations; Mars; Atmosphere ID SCIENCE LABORATORY MISSION; REMOTE-SENSING DATA; WATER ICE CLOUDS; THERMAL INERTIA; OPTICAL DEPTH; SURFACE-PROPERTIES; ATMOSPHERIC DUST; GUSEV CRATER; ROVER; AEROSOL AB The REMS instrument onboard the Mars Science Laboratory rover, Curiosity, has measured ground temperature nearly continuously at hourly intervals for two Mars years. Coverage of the entire diurnal cycle at 1 Hz is available every few martian days. We compare these measurements with predictions of surface atmosphere thermal models to derive the apparent thermal inertia and thermally derived albedo along the rover's traverse after accounting for the radiative effects of atmospheric water ice during fall and winter, as is necessary to match the measured seasonal trend. The REMS measurements can distinguish between active sand, other loose materials, mudstone, and sandstone based on their thermophysical properties. However, the apparent thermal inertias of bedrock-dominated surfaces (similar to 350-550 J m(-2) K-1 s-(1/2)) are lower than expected. We use rover imagery and the detailed shape of the diurnal ground temperature curve to explore whether lateral or vertical heterogeneity in the surface materials within the sensor footprint might explain the low inertias. We find that the bedrock component of the surface can have a thermal inertia as high as 650-1700 J m(-2) K-1 s(-1/2) for mudstone sites and 700 J m(-2) K-1 s(-1/2) for sandstone sites in models runs that include lateral and vertical mixing. Although the results of our forward modeling approach may be non-unique, they demonstrate the potential to extract information about lateral and vertical variations in thermophysical properties from temporally resolved measurements of ground temperature. (C) 2016 Elsevier Inc. All rights reserved. C1 [Vasavada, Ashwin R.; Piqueux, Sylvain] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Lewis, Kevin W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Lemmon, Mark T.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. [Smith, Michael D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM ashwin@jpl.nasa.gov NR 65 TC 0 Z9 0 U1 10 U2 10 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR 1 PY 2017 VL 284 BP 372 EP 386 DI 10.1016/j.icarus.2016.11.035 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EI5XM UT WOS:000392569600027 ER PT J AU Eke, VR Lawrence, DJ Teodoro, LFA AF Eke, Vincent R. Lawrence, David J. Teodoro, Luis F. A. TI How thick are Mercury's polar water ice deposits? SO ICARUS LA English DT Article DE Mercury; surface; Radar observations; Ices ID LASER ALTIMETER; IMPACT CRATERS; NORTH-POLE; COHERENT BACKSCATTER; MESSENGER SPACECRAFT; TERRESTRIAL PLANETS; THERMAL-STABILITY; SURFACE VOLATILES; GROUND ICE; MOON AB An estimate is made of the thickness of the radar-bright deposits in craters near to Mercury's north pole. To construct an objective set of craters for this measurement, an automated crater finding algorithm is developed and applied to a digital elevation model based on data from the Mercury Laser Altimeter onboard the MESSENGER spacecraft. This produces a catalogue of 663 craters with diameters exceeding 4 km, northwards of latitude +55 degrees. A subset of 12 larger, well-sampled and fresh polar craters are selected to search for correlations between topography and radar same-sense backscatter cross-section. It is found that the typical excess height associated with the radar-bright regions within these fresh polar craters is (50 +/- 35) m. This puts an approximate upper limit on the total polar water ice deposits on Mercury of similar to 3 x 10(15) kg. (C) 2016 Elsevier Inc. All rights reserved. C1 [Eke, Vincent R.] Univ Durham, Inst Computat Cosmol, Dept Phys, Sci Labs, South Rd, Durham DH1 3LE, England. [Lawrence, David J.] Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. [Teodoro, Luis F. A.] NASA, Ames Res Ctr, BAER, Planetary Syst Branch,Space Sci & Astrobiol Div, MS 245-3, Moffett Field, CA 94035 USA. RP Eke, VR (reprint author), Univ Durham, Inst Computat Cosmol, Dept Phys, Sci Labs, South Rd, Durham DH1 3LE, England. EM v.r.eke@durham.ac.uk FU STFC [ST/L00075X/1, ST/H008519/1, ST/K00087X/1, ST/K003267/1]; BIS National E-infrastructure capital grant [ST/K00042X/1]; Durham University FX VRE acknowledges helpful discussions with Adrian Jenkins and Wenzhe Fa. VRE was supported by the STFC rolling grant ST/L00075X/1. This work used the DiRAC Data Centric system at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (http://www.dirac.ac.uk). This equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grants ST/H008519/1 and ST/K00087X/1, STFC DiRAC Operations grant ST/K003267/1 and Durham University. DiRAC is part of the National E-Infrastructure. NR 59 TC 0 Z9 0 U1 8 U2 8 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR 1 PY 2017 VL 284 BP 407 EP 415 DI 10.1016/j.icarus.2016.12.001 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EI5XM UT WOS:000392569600030 ER PT J AU Quick, LC Glaze, LS Baloga, SM AF Quick, Lynnae C. Glaze, Lori S. Baloga, Stephen M. TI Cryovolcanic emplacement of domes on Europa SO ICARUS LA English DT Article DE Europa; Volcanism; Geological processes; Satellites; Surfaces ID VENUSIAN PANCAKE DOMES; STEEP-SIDED DOMES; ICE SHELL; GEOLOGICAL EVIDENCE; GRAVITY CURRENTS; WATER VOLCANISM; RHYOLITE LAVAS; SEA-FLOOR; SATELLITES; ENCELADUS AB Here we explore the hypothesis that certain domes on Europa may have been produced by the extrusion of viscous cryolavas. A new mathematical method for the emplacement and relaxation of viscous lava domes is presented and applied to putative cryovolcanic domes on Europa. A similarity solution approach is applied to the governing equation for fluid flow in a cylindrical geometry, and dome relaxation is explored assuming a volume of cryolava has been rapidly emplaced onto the surface. Nonphysical singularities inherent in previous models for dome relaxation have been eliminated, and cryolava cooling is represented by a time-variable viscosity. We find that at the onset of relaxation, bulk kinematic viscosities may lie in the range between 10(3) and 10(6) m(2)/s, while the actual fluid lava viscosity may be much lower. Plausible relaxation times to form the domes, which are linked to bulk cryolava rheology, are found to range from 3.6 days to 7.5 years. We find that cooling of the cryolava, while dominated by conduction through an icy skin, should not prevent fluids from advancing and relaxing to form domes within the timescales considered. Determining the range of emplacement conditions for putative cryolava domes will shed light on Europa's resurfacing history. In addition, the rheologies and compositions of erupted cryolavas have implications for subsurface cryomagma ascent and local surface stress conditions on Europa. (C) 2016 Elsevier Inc. All rights reserved. C1 [Quick, Lynnae C.; Glaze, Lori S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Baloga, Stephen M.] Proxemy Res, 20528 Farcroft Lane, Gaithersburg, MD 20882 USA. [Quick, Lynnae C.] Planetary Sci Inst, 1700 East Ft Lowell Rd,Suite 106, Tucson, AZ 85719 USA. EM lquick@psi.edu RI Glaze, Lori/D-1314-2012 FU NASA Postdoctoral Program; NASA's Solar System Workings Program [WBS 811073.02.35.01.07] FX We wish to thank Dr. Catherine Neish and Dr. Ralph Lorenz for thoughtful reviews that improved the manuscript. We also thank Sarah Fagents, Louise Prockter and Simon Kattenhorn for useful discussions. The authors acknowledge support from the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities, and funding from NASA's Solar System Workings Program [WBS 811073.02.35.01.07]. NR 86 TC 1 Z9 1 U1 8 U2 8 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR 1 PY 2017 VL 284 BP 477 EP 488 DI 10.1016/j.icarus.2016.06.029 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EI5XM UT WOS:000392569600035 ER PT J AU Carvalho, D Rocha, A Gomez-Gesteira, M Santos, CS AF Carvalho, D. Rocha, A. Gomez-Gesteira, M. Silva Santos, C. TI Offshore winds and wind energy production estimates derived from ASCAT, OSCAT, numerical weather prediction models and buoys - A comparative study for the Iberian Peninsula Atlantic coast SO RENEWABLE ENERGY LA English DT Article DE Offshore wind energy; Ocean wind; Scatterometers; Iberian peninsula; Reanalyses; WRF ID WAVE ENERGY; SIMULATION; RESOURCE; WRF; FORECASTS; AREAS AB Different offshore wind datasets were compared with buoys measurements in the Iberian Peninsula Atlantic coast, aiming to assess the best alternatives to ocean surface measured winds for offshore wind energy assessment and other applications. Results: show that although ASCAT (Advanced SCATterometer) high-resolution product showed the lowest wind speed temporal variability and wind power flux estimations errors, a WRF (Weather Research and Forecast) model high-resolution simulation can be considered as the best alternative for offshore wind energy applications. WRF's simulation showed wind power flux estimations errors very similar to ASCAT, the best representation of the wind speed mean state and Weibull probability density functions, and provide offshore wind data at typical turbines hub heights. CCMP (Cross-Calibrated Multi Platform Ocean Surface Wind Vectors) can also be seen as a valid and readily available alternative of offshore wind data. The findings presented here can be of great value for offshore wind energy applications that focus on ocean areas where measured wind data are not available, or are insufficient for the desired purposes. An informed choice of the most accurate offshore wind databases will provide more realistic wind energy production estimates that will positively impact the preliminary planning stages of offshore wind energy exploration projects. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Carvalho, D.; Rocha, A.] Univ Aveiro, CESAM Dept Phys, Campus Univ Santiago, P-3810193 Aveiro, Portugal. [Gomez-Gesteira, M.] Univ Vigo, Fac Ciencias, EPHYSIAB Environm Phys Lab, Orense 32004, Spain. [Silva Santos, C.] MEGAJOULE Inovacao Lda, TECMAIA, Rua Engn Frederico Ulrich 2650, Moreira Da Maia, Portugal. [Carvalho, D.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res GESTAR, Columbia, MD 21046 USA. [Carvalho, D.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off GMAO, Greenbelt, MD 20771 USA. RP Carvalho, D (reprint author), Univ Aveiro, CESAM Dept Phys, Campus Univ Santiago, P-3810193 Aveiro, Portugal.; Carvalho, D (reprint author), Univ Space Res Assoc, Goddard Earth Sci Technol & Res GESTAR, Columbia, MD 21046 USA.; Carvalho, D (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off GMAO, Greenbelt, MD 20771 USA. EM david.carvalho@ua.pt; alfredo.rocha@ua.pt; mggesteira@uvigo.es; carlos.santos@megajoule.pt FU Xunta de Galicia under the project "Programa de Consolidacion e Estructuracion de Unidades de Investigacion Competitivas: Grupos de Referencia Competitiva" - European Regional Development Fund (FEDER) [GRC2013-001]; FEDER funds through the "Programa Operacional Factores de Competitividade - COMPETE"; FCT - Fundacao para a Ciencia e a Tecnologia, within the framework of Project "Urban Atmospheric Quality, Climate Change and Resilience" [EXCL/AAG-MAA/0383/2012] FX This work was partially supported by Xunta de Galicia under the project "Programa de Consolidacion e Estructuracion de Unidades de Investigacion Competitivas: Grupos de Referencia Competitiva" (GRC2013-001) co-funded by the European Regional Development Fund (FEDER) The authors would like to express their gratitude to all climate, meteorological and oceanographic institutions referred in the text, for providing the data used in this work. This study was supported by FEDER funds through the "Programa Operacional Factores de Competitividade - COMPETE" and by Portuguese national funds through FCT - Fundacao para a Ciencia e a Tecnologia, within the framework of Project "Urban Atmospheric Quality, Climate Change and Resilience." EXCL/AAG-MAA/0383/2012. NR 34 TC 0 Z9 0 U1 17 U2 17 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0960-1481 J9 RENEW ENERG JI Renew. Energy PD MAR PY 2017 VL 102 BP 433 EP 444 DI 10.1016/j.renene.2016.10.063 PN B PG 12 WC GREEN & SUSTAINABLE SCIENCE & TECHNOLOGY; Energy & Fuels SC Science & Technology - Other Topics; Energy & Fuels GA EF9CM UT WOS:000390628300015 ER PT J AU Parrens, M Wigneron, JP Richaume, P Al Bitar, A Mialon, A Fernandez-Moran, R Al-Yaari, A O'Neill, P Kerr, Y AF Parrens, Marie Wigneron, Jean-Pierre Richaume, Philippe Al Bitar, Ahmad Mialon, Arnaud Fernandez-Moran, Roberto Al-Yaari, Amen O'Neill, Peggy Kerr, Yann TI Considering combined or separated roughness and vegetation effects in soil moisture retrievals SO International Journal of Applied Earth Observation and Geoinformation LA English DT Article DE Soil moisture; Soil roughness; SMOS; L-band; Retrievals; Optical vegetation depth ID BAND MICROWAVE EMISSION; IN-SITU OBSERVATIONS; L-MEB MODEL; AMSR-E; SURFACE-ROUGHNESS; REFLECTIVITY MODEL; LAND SURFACES; NEAR-SURFACE; SMAP MISSION; SMOS MISSION AB For more than six years, the Soil Moisture and Ocean Salinity (SMOS) mission has provided multi angular and full-polarization brightness temperature (TB) measurements at L-band. Geophysical products such as soil moisture (SM) and vegetation optical depth at nadir (tau(nad)) are retrieved by an operational algorithm using TB observations at different angles of incidence and polarizations. However, the quality of the retrievals depends on several surface effects, such as vegetation, soil roughness and texture, etc. In the microwave forward emission model used in the retrievals (L-band Microwave Emission Model, L-MEB), soil roughness is modelled with a semi-empirical equation using four main parameters (Q(r), H-r, N-rp, with p=H or V polarizations). At present, these parameters are calibrated with data provided by airborne studies and in situ measurements made at a local scale that is not necessarily representative of the large SMOS footprints (43 km on average) at global scale. In this study, we evaluate the impact of the calibrated values of N-rp and H-r on the SM and tau(nad) retrievals based on SMOS TB measurements (SMOS Level 3 product) over the Soil Climate Analysis Network (SCAN) network located in North America over five years (2011-2015). In this study, Q(r) was set equal to zero and we assumed that N-rH = N-rV. The retrievals were performed by varying N-rp from-1 to 2 by steps of 1 and H-r from 0 to 0.6 by steps of 0.1. At satellite scale, the results show that combining vegetation and roughness effects in a single parameter provides the best results in terms of soil moisture retrievals, as evaluated against the in situ SM data. Even though our retrieval approach was very simplified, as we did not account for pixel heterogeneity, the accuracy we obtained in the SM retrievals was almost systematically better than those of the Level 3 product. Improved results were also obtained in terms of optical depth retrievals. These new results may have key consequences in terms of calibration of roughness effects within the algorithms of the SMOS (ESA) and the SMAP (NASA) space missions. (C) 2016 Elsevier B.V. All rights reserved. C1 [Parrens, Marie; Richaume, Philippe; Al Bitar, Ahmad; Mialon, Arnaud; Kerr, Yann] Univ Fed Toulouse, Ctr Etud Spatiales BIOsphere CESBIO, UMR5126, CNES,CNRS,IRD, BPI 2801, F-31401 Toulouse 9, France. [Wigneron, Jean-Pierre; Fernandez-Moran, Roberto; Al-Yaari, Amen] Ctr INRA Bordeaux, Aquitaine, ISPA UR1263, F-33140 Villenave Dornon, France. [Wigneron, Jean-Pierre; Fernandez-Moran, Roberto; Al-Yaari, Amen] Ctr INRA Bordeaux, Aquitaine, France. [O'Neill, Peggy] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Parrens, M (reprint author), Univ Fed Toulouse, Ctr Etud Spatiales BIOsphere CESBIO, UMR5126, CNES,CNRS,IRD, BPI 2801, F-31401 Toulouse 9, France. EM matie.parrens@cesbio.cnes.fr RI Al-Yaari, Amen/B-1444-2016; OI Al-Yaari, Amen/0000-0001-7530-6088; Parrens, Marie/0000-0001-7643-2211 FU European Space Agency (ESA); program Terre Ocean Surfaces Continentales et Atmosphere (TOSCA, France) FX This work was funded by the European Space Agency (ESA) in the framework of the Expert Support Laboratories and by the program Terre Ocean Surfaces Continentales et Atmosphere (TOSCA, France). The authors acknowledge the CATDS for the SMOS L3 dataset and the NRCS for making available the SCAN data. NR 78 TC 0 Z9 0 U1 42 U2 42 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0303-2434 J9 INT J APPL EARTH OBS JI Int. J. Appl. Earth Obs. Geoinf. PD MAR PY 2017 VL 55 BP 73 EP 86 DI 10.1016/j.jag.2016.11.001 PG 14 WC Remote Sensing SC Remote Sensing GA ED9BT UT WOS:000389165800008 ER PT J AU Barrila, J Yang, JS Crabbe, A Sarker, SF Liu, YL Ott, CM Nelman-Gonzalez, MA Clemett, SJ Nydam, SD Forsyth, RJ Davis, RR Crucian, BE Quiriarte, H Roland, KL Brenneman, K Sams, C Loscher, C Nickerson, CA AF Barrila, Jennifer Yang, Jiseon Crabbe, Aurelie Sarker, Shameema F. Liu, Yulong Ott, C. Mark Nelman-Gonzalez, Mayra A. Clemett, Simon J. Nydam, Seth D. Forsyth, Rebecca J. Davis, Richard R. Crucian, Brian E. Quiriarte, Heather Roland, Kenneth L. Brenneman, Karen Sams, Clarence Loscher, Christine Nickerson, Cheryl A. TI Three-dimensional organotypic co-culture model of intestinal epithelial cells and macrophages to study Salmonella enterica colonization patterns SO NPJ MICROGRAVITY LA English DT Article ID TRANSMEMBRANE CONDUCTANCE REGULATOR; SEROVAR GALLINARUM REQUIRES; COMPLETE GENOME SEQUENCE; STG FIMBRIAL OPERON; IN-VITRO; TYPHIMURIUM INVASION; BACTERIAL SURVIVAL; HOST-CELLS; IVB PILI; TYPHI AB Three-dimensional models of human intestinal epithelium mimic the differentiated form and function of parental tissues often not exhibited by two-dimensional monolayers and respond to Salmonella in key ways that reflect in vivo infections. To further enhance the physiological relevance of three-dimensional models to more closely approximate in vivo intestinal microenvironments encountered by Salmonella, we developed and validated a novel three-dimensional co-culture infection model of colonic epithelial cells and macrophages using the NASA Rotating Wall Vessel bioreactor. First, U937 cells were activated upon collagen-coated scaffolds. HT-29 epithelial cells were then added and the three-dimensional model was cultured in the bioreactor until optimal differentiation was reached, as assessed by immunohistochemical profiling and bead uptake assays. The new co-culture model exhibited in vivo-like structural and phenotypic characteristics, including three-dimensional architecture, apical-basolateral polarity, well-formed tight/adherens junctions, mucin, multiple epithelial cell types, and functional macrophages. Phagocytic activity of macrophages was confirmed by uptake of inert, bacteria-sized beads. Contribution of macrophages to infection was assessed by colonization studies of Salmonella pathovars with different host adaptations and disease phenotypes (Typhimurium ST19 strain SL1344 and ST313 strain D23580; Typhi Ty2). In addition, Salmonella were cultured aerobically or microaerobically, recapitulating environments encountered prior to and during intestinal infection, respectively. All Salmonella strains exhibited decreased colonization in co-culture (HT-29-U937) relative to epithelial (HT-29) models, indicating antimicrobial function of macrophages. Interestingly, D23580 exhibited enhanced replication/survival in both models following invasion. Pathovar-specific differences in colonization and intracellular co-localization patterns were observed. These findings emphasize the power of incorporating a series of related three-dimensional models within a study to identify microenvironmental factors important for regulating infection. C1 [Barrila, Jennifer; Yang, Jiseon; Crabbe, Aurelie; Sarker, Shameema F.; Liu, Yulong; Nydam, Seth D.; Forsyth, Rebecca J.; Davis, Richard R.; Roland, Kenneth L.; Brenneman, Karen; Nickerson, Cheryl A.] Arizona State Univ, Biodesign Inst, Ctr Infect Dis & Vaccinol, Tempe, AZ 85287 USA. [Crabbe, Aurelie] Univ Ghent, Lab Pharmaceut Microbiol, Ghent, Belgium. [Ott, C. Mark; Crucian, Brian E.; Sams, Clarence] NASA, Johnson Space Ctr, Biomed Res & Environm Sci Div, Houston, TX USA. [Nelman-Gonzalez, Mayra A.] Wyle Sci, Technol & Engn Grp, Houston, TX USA. [Clemett, Simon J.] ERC Inc, Jacobs JETS, Houston, TX USA. [Quiriarte, Heather] JES Tech, Houston, TX USA. [Loscher, Christine] Dublin City Univ, Sch Biotechnol, Immunomodulat Res Grp, Glasnevin, Ireland. [Nickerson, Cheryl A.] Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. RP Nickerson, CA (reprint author), Arizona State Univ, Biodesign Inst, Ctr Infect Dis & Vaccinol, Tempe, AZ 85287 USA.; Nickerson, CA (reprint author), Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. EM Cheryl.Nickerson@asu.edu FU NASA [NNX13AM01G]; NIH [R01-AI081759] FX We thank Carolyn Coyne for helpful discussions and Debra Baluch for her kind imaging help. Funded by NASA grant NNX13AM01G (C.A.N., J.B., and C.M.O.), and NIH R01-AI081759 (C.A.N.). The funders had no role in study design, data collection and interpretation, or the decision to submit the work for publication. NR 84 TC 0 Z9 0 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 2373-8065 J9 NPJ MICROGRAVITY JI NPJ Microgravity PD FEB 28 PY 2017 VL 3 AR 10 DI 10.1038/s41526-017-0011-2 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EN5QH UT WOS:000396060100001 ER PT J AU Bristow, TF Haberle, RM Blake, DF Des Marais, DJ Eigenbrode, JL Fairen, AG Grotzinger, JP Stack, KM Mischna, MA Rampe, EB Siebach, KL Sutter, B Vaniman, DT Vasavada, AR AF Bristow, Thomas F. Haberle, Robert M. Blake, David F. Des Marais, David J. Eigenbrode, Jennifer L. Fairen, Alberto G. Grotzinger, John P. Stack, Kathryn M. Mischna, Michael A. Rampe, Elizabeth B. Siebach, Kirsten L. Sutter, Brad Vaniman, David T. Vasavada, Ashwin R. TI Low Hesperian P-CO2 constrained from in situ mineralogical analysis at Gale Crater, Mars SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Hesperian Mars; martian atmosphere; Mars Science Laboratory; Gale Crater; carbon dioxide ID PRECIPITATION KINETICS; YELLOWKNIFE BAY; REDOX CHEMISTRY; CLAY-MINERALS; CARBON; EVOLUTION; SIDERITE; DIAGENESIS; HISTORY; ORIGIN AB Carbon dioxide is an essential atmospheric component in martian climate models that attempt to reconcile a faint young sun with planetwide evidence of liquid water in the Noachian and Early Hesperian. In this study, we use mineral and contextual sedimentary environmental data measured by the Mars Science Laboratory (MSL) Rover Curiosity to estimate the atmospheric partial pressure of CO2 (PCO2) coinciding with a long-lived lake system in Gale Crater at similar to 3.5 Ga. A reaction-transport model that simulates mineralogy observed within the Sheepbed member at Yellowknife Bay (YKB), by coupling mineral equilibria with carbonate precipitation kinetics and rates of sedimentation, indicates atmospheric PCO2 levels in the 10s mbar range. At such low PCO2 levels, existing climate models are unable to warm Hesperian Mars anywhere near the freezing point of water, and other gases are required to raise atmospheric pressure to prevent lake waters from being lost to the atmosphere. Thus, either lacustrine features of Gale formed in a cold environment by a mechanism yet to be determined, or the climatemodels still lack an essential component that would serve to elevate surface temperatures, at least locally, on Hesperian Mars. Our results also impose restrictions on the potential role of atmospheric CO2 in inferred warmer conditions and valley network formation of the late Noachian. C1 [Bristow, Thomas F.; Blake, David F.; Des Marais, David J.] NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. [Haberle, Robert M.] NASA, Planetary Syst Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. [Eigenbrode, Jennifer L.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fairen, Alberto G.] Ctr Astrobiol, Dept Planetol & Habitabil, Madrid 28850, Spain. [Grotzinger, John P.; Siebach, Kirsten L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Stack, Kathryn M.; Mischna, Michael A.; Vasavada, Ashwin R.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Rampe, Elizabeth B.] NASA, Astromat Res & Explorat Sci Div, Johnson Space Ctr, Houston, TX 77058 USA. [Sutter, Brad] Jacobs Technol Inc, NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Vaniman, David T.] Planetary Sci Inst, Tucson, AZ 85719 USA. RP Bristow, TF (reprint author), NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. EM thomas.f.bristow@nasa.gov FU Project "icyMARS" European Research Council Starting Grant [307496]; NASA Mars Exploration Program; National Aeronautics and Space Administration FX We acknowledge the support of the Jet Propulsion Lab engineering and MSL operations staff. Thanks to K. Zahnle, E. Kite, and M. Daswani for discussions, and constructive reviews from I. Halevy, J. Kasting, P. Niles, and two anonymous reviewers on this and a previous version of the manuscript. We thank P. Sadler for advice and access to sedimentation rate data. Modeling efforts were supported by a NASA Habitable Worlds grant (T.F.B.). This work was supported by the Project "icyMARS" European Research Council Starting Grant 307496 (to A.G.F.). This research was supported by the NASA Mars Exploration Program. Some of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 53 TC 0 Z9 0 U1 0 U2 0 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 FEB 28 PY 2017 VL 114 IS 9 BP 2166 EP 2170 DI 10.1073/pnas.1616649114 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EM1TZ UT WOS:000395101200039 PM 28167765 ER PT J AU Shuster, JR Argall, MR Torbert, RB Chen, LJ Farrugia, CJ Alm, L Wang, S Daughton, W Gershman, DJ Giles, BL Russell, CT Burch, JL Pollock, CJ AF Shuster, J. R. Argall, M. R. Torbert, R. B. Chen, L. -J. Farrugia, C. J. Alm, L. Wang, S. Daughton, W. Gershman, D. J. Giles, B. L. Russell, C. T. Burch, J. L. Pollock, C. J. TI Hodographic approach for determining spacecraft trajectories throughmagnetic reconnection diffusion regions SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MAGNETIC RECONNECTION; ANISOTROPY AB We develop an algorithm that finds a trajectory through simulations of magnetic reconnection along which input Magnetospheric Multiscale (MMS) spacecraft observations are matched. Using two-dimensional particle-in-cell simulations of asymmetric reconnection, the method is applied to a magnetopause electron diffusion region (EDR) encountered by the MMS spacecraft to facilitate interpretation of the event based on fully kinetic models. The recently discovered crescent-shaped electron velocity distributions measured by MMS in the EDR are consistent with simulation distributions at the corresponding time along the computed trajectory. C1 [Shuster, J. R.; Chen, L. -J.; Wang, S.; Gershman, D. J.; Giles, B. L.; Pollock, C. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Shuster, J. R.; Wang, S.; Gershman, D. J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Shuster, J. R.; Argall, M. R.; Torbert, R. B.; Farrugia, C. J.; Alm, L.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Daughton, W.] Los Alamos Natl Lab, Los Alamos, NM 87544 USA. [Russell, C. T.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90024 USA. [Burch, J. L.] Southwest Res Inst, San Antonio, TX 78238 USA. RP Shuster, JR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM jason.r.shuster@nasa.gov FU NSF [AGS-1543598, AGS-1202537, AGS-1552142]; NASA Earth and Space Science Fellowship (NESSF); NASA FX This research was supported in part by NSF grants AGS-1543598, AGS-1202537, AGS-1552142; NASA Earth and Space Science Fellowship (NESSF); NASA grants to the Theory and Modeling Program, FIELDS team; and the Fast Plasma Investigation of the MMS mission. The simulation data are available upon request from the authors. We especially thank the MMS instrument teams for their outstanding engineering and determination, which has culminated in the delivery of such exceptional data, available to the public via https://lasp.colorado.edu/mms/sdc/public/. NR 28 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 FEB 28 PY 2017 VL 44 IS 4 BP 1625 EP 1633 DI 10.1002/2017GL072570 PG 9 WC Geosciences, Multidisciplinary SC Geology GA EO0TO UT WOS:000396411100002 ER PT J AU Stephan, K Jaumann, R Krohn, K Schmedemann, N Zambon, F Tosi, F Carrozzo, FG McFadden, LA Otto, K De Sanctis, MC Ammannito, E Matz, KD Roatsch, T Preusker, F Raymond, CA Russell, CT AF Stephan, K. Jaumann, R. Krohn, K. Schmedemann, N. Zambon, F. Tosi, F. Carrozzo, F. G. McFadden, L. A. Otto, K. De Sanctis, M. C. Ammannito, E. Matz, K. -D. Roatsch, T. Preusker, F. Raymond, C. A. Russell, C. T. TI An investigation of the bluish material on Ceres SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CASSINI-VIMS; CARBONACEOUS CHONDRITES; REFLECTANCE SPECTRA; WATER ICE; SURFACE; SPECTROSCOPY; PARTICLES; SYSTEM; DARK AB The dwarf planet Ceres shows spatially well-defined regions, which exhibit a negative (blue) spectral slope between 0.5 and 2.5 mu m. Comparisons with planetary bodies known to exhibit a blue slope and spectral properties of materials identified on Ceres's surface based on infrared wavelength signatures indicate that the spectral changes could be related to physical properties of the surface material rather than variations in its composition. The close association of bluish surface regions to fresh impact craters implies a possible relationship to an impact-triggered alteration and/or space weathering processes. The bluish regions could be linked with blankets of ultrafine grains and partly amorphous phyllosilicates, which form larger agglomerates due to the sticky behavior of impact-induced phyllosilicate dust and/or the amorphization of the ejecta material during the impact process. Space weathering processes (micrometeoritic impacts, temperature changes) cause a reversal of the agglutination process and a recrystallization of the surface material with time resulting in a reddening of the spectral slope. C1 [Stephan, K.; Jaumann, R.; Krohn, K.; Otto, K.; Matz, K. -D.; Roatsch, T.; Preusker, F.] Inst Planetary Res, DLR, Berlin, Germany. [Jaumann, R.; Schmedemann, N.] Free Univ Berlin, Inst Geosci, Dept Earth Sci, Berlin, Germany. [Tosi, F.; Carrozzo, F. G.; De Sanctis, M. C.] Natl Inst Astrophys, INAF IAPS, Rome, Italy. [McFadden, L. A.] Goddard Space Flight Ctr, Greenbelt, MD USA. [Ammannito, E.; Russell, C. T.] UCLA, Inst Geophys & Planetary Phys, Los Angeles, CA USA. [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Stephan, K (reprint author), Inst Planetary Res, DLR, Berlin, Germany. EM Katrin.Stephan@dlr.de OI Krohn, Katrin/0000-0001-8518-4985; Tosi, Federico/0000-0003-4002-2434; Zambon, Francesca/0000-0002-4190-6592 FU NASA FX We thank the Dawn team for the development, cruise, orbital insertion, and operations of the Dawn spacecraft at Ceres. Portions of this work were performed at the DLR Institute of Planetary Research, at the Jet Propulsion Laboratory (JPL) under contract with NASA, as well as at the National Institute for Astrophysics (Rome, Italy). Dawn data are archived with the NASA Planetary Data System (http://sbn.pds.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 FEB 28 PY 2017 VL 44 IS 4 BP 1660 EP 1668 DI 10.1002/2016GL071652 PG 9 WC Geosciences, Multidisciplinary SC Geology GA EO0TO UT WOS:000396411100006 ER PT J AU He, XG Wada, Y Wanders, N Sheffield, J AF He, Xiaogang Wada, Yoshihide Wanders, Niko Sheffield, Justin TI Intensification of hydrological drought in California by human water management SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CLIMATE-CHANGE; SOUTHERN-OSCILLATION; UNITED-STATES; PRECIPITATION; VARIABILITY; IMPACTS; 21ST-CENTURY; SNOWPACK; CONTEXT; EVENTS AB We analyze the contribution of human water management to the intensification or mitigation of hydrological drought over California using the PCR-GLOBWB hydrological model at 0.5 degrees resolution for the period 1979-2014. We demonstrate that including water management in the modeling framework results in more accurate discharge representation. During the severe 2014 drought, water management alleviated the drought deficit by similar to 50% in Southern California through reservoir operation during low-flow periods. However, human water consumption (mostly irrigation) in the Central Valley increased drought duration and deficit by 50% and 50-100%, respectively. Return level analysis indicates that there is more than 50% chance that the probability of occurrence of an extreme 2014 magnitude drought event was at least doubled under the influence of human activities compared to natural variability. This impact is most significant over the San Joaquin Drainage basin with a 50% and 75% likelihood that the return period is more than 3.5 and 1.5 times larger, respectively, because of human activities. C1 [He, Xiaogang; Wanders, Niko; Sheffield, Justin] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. [Wada, Yoshihide] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Wada, Yoshihide] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Wada, Yoshihide] Univ Utrecht, Dept Phys Geog, Utrecht, Netherlands. [Wada, Yoshihide] Int Inst Appl Syst Anal, Laxenburg, Austria. [Sheffield, Justin] Univ Southampton, Geog & Environm, Southampton, Hants, England. RP He, XG (reprint author), Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. EM hexg@princeton.edu OI He, Xiaogang/0000-0001-7428-0269 FU NOAA [NA14OAR4310218]; Peter B. Lewis Fund for Student Innovation in Energy; Environment. N. Wanders; NWO Rubicon Fellowship [825.15.003]; Japan Society for the Promotion of Science (JSPS) Oversea Research Fellowship [JSPS-2014-878] FX This study is supported by NOAA grant NA14OAR4310218. X. He would like to acknowledge the partial support from Peter B. Lewis Fund for Student Innovation in Energy and the Environment. N. Wanders is supported by a NWO Rubicon Fellowship 825.15.003 (Forecasting to Reduce Socio-Economic Effects of Droughts). Y. Wada is supported by Japan Society for the Promotion of Science (JSPS) Oversea Research Fellowship (grant JSPS-2014-878). Model simulation is available upon request to Y. Wada (Y.Wada@uu.nl). Climate divisions used in this study are provided by NOAA National Centers for Environmental Information at http://www.ncdc.noaa.gov/ monitoring-references/maps/us-climate-divisions.php. NR 52 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 FEB 28 PY 2017 VL 44 IS 4 BP 1777 EP 1785 DI 10.1002/2016GL071665 PG 9 WC Geosciences, Multidisciplinary SC Geology GA EO0TO UT WOS:000396411100019 ER PT J AU Karcher, B Jensen, EJ AF Kaercher, B. Jensen, E. J. TI Microscale characteristics of homogeneous freezing events in cirrus clouds SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID TROPICAL TROPOPAUSE LAYER; ICE NUCLEATION; VERTICAL VELOCITY; GRAVITY-WAVES; TEMPERATURE; WATER; FLUCTUATIONS; ATMOSPHERE; MODEL AB We investigate homogeneous freezing of aqueous aerosol particles, a fundamental ice formation process in cirrus clouds. We estimate freezing time scales and vertical extensions of freezing layers, demonstrating that such freezing events are highly transient and localized. While time scales decrease with increasing vertical velocity driving ice nucleation, layer depths are weak functions of the vertical velocity. Our results are used to discuss possible effects of turbulent diffusion and entrainment-mixing on homogeneous freezing in cirrus. Large turbulent diffusivity acts to broaden water vapor-depleted freezing layers and facilitate sedimentation of freshly nucleated ice crystals out of them into ice-supersaturated air. Homogeneous freezing events could be affected by microscale turbulence in episodes of intense turbulence dissipation rates, although such episodes are rare. We conjecture that freezing layers are broader in the case of heterogeneous ice nucleation and effects of sedimentation on nucleation increase in importance. Our findings point to the difficulty of inferring nucleated cirrus ice crystal numbers from measurements and place tight constraints on cirrus models with regard to spatial and temporal resolution. C1 [Kaercher, B.] Inst Atmospher Phys, Deutsch Zentrum Luft & Raumfahrt, Wessling, Germany. [Jensen, E. J.] NASA, Ames Res Ctr, Moffett Field, CA USA. RP Karcher, B (reprint author), Inst Atmospher Phys, Deutsch Zentrum Luft & Raumfahrt, Wessling, Germany. EM bernd.kaercher@dlr.de RI Karcher, Bernd/D-5325-2014 OI Karcher, Bernd/0000-0003-0278-4980 NR 25 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 FEB 28 PY 2017 VL 44 IS 4 BP 2027 EP 2034 DI 10.1002/2016GL072486 PG 8 WC Geosciences, Multidisciplinary SC Geology GA EO0TO UT WOS:000396411100049 ER PT J AU Zhang, ZB Dong, XQ Xi, BK Song, H Ma, PL Ghan, SJ Platnick, S Minnis, P AF Zhang, Zhibo Dong, Xiquan Xi, Baike Song, Hua Ma, Po-Lun Ghan, Steven J. Platnick, Steven Minnis, Patrick TI Intercomparisons of marine boundary layer cloud properties from the ARM CAP-MBL campaign and two MODIS cloud products SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID LIQUID WATER PATH; PART I; INSTRUMENT SIMULATORS; STRATIFORM CLOUDS; MOBILE FACILITY; AZORES; RETRIEVALS; SATELLITE; FRACTION; IMPACT AB From April 2009 to December 2010, the Department of Energy Atmospheric Radiation Measurement (ARM) program carried out an observational field campaign on Graciosa Island, targeting the marine boundary layer (MBL) clouds over the Azores region. In this paper, we present an intercomparison of the MBL cloud properties, namely, cloud liquid water path (LWP), cloud optical thickness (COT), and cloud-droplet effective radius (CER), among retrievals from the ARM mobile facility and two Moderate Resolution Imaging Spectroradiometer (MODIS) cloud products (Goddard Space Flight Center (GSFC)-MODIS and Clouds and Earth's Radiant Energy System-MODIS). A total of 63 daytime single-layer MBL cloud cases are selected for intercomparison. Comparison of collocated retrievals indicates that the two MODIS cloud products agree well on both COT and CER retrievals, with the correlation coefficient R>0.95, despite their significant difference in spatial sampling. In both MODIS products, the CER retrievals based on the 2.1 mu m band (CER2.1) are significantly larger than those based on the 3.7 mu m band (CER3.7). The GSFC-MODIS cloud product is collocated and compared with ground-based ARM observations at several temporal-spatial scales. In general, the correlation increases with more precise collocation. For the 63 selected MBL cloud cases, the GSFC-MODIS LWP and COT retrievals agree reasonably well with the ground-based observations with no apparent bias and correlation coefficient R around 0.85 and 0.70, respectively. However, GSFC-MODIS CER3.7 and CER2.1 retrievals have a lower correlation (R similar to 0.5) with the ground-based retrievals. For the 63 selected cases, they are on average larger than ground observations by about 1.5 mu m and 3.0 mu m, respectively. Taking into account that the MODIS CER retrievals are only sensitive to cloud top reduces the bias only by 0.5 mu m. C1 [Zhang, Zhibo] UMBC, Dept Phys, Baltimore, MD 21250 USA. [Zhang, Zhibo; Song, Hua] UMBC, Joint Ctr Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. [Dong, Xiquan] Univ Arizona, Dept Hydrol & Atmospher Sci, Tucson, AZ USA. [Xi, Baike] Univ North Dakota, Dept Atmospher Sci, Grand Forks, ND USA. [Ma, Po-Lun; Ghan, Steven J.] Pacific Northwest Natl Lab, Richland, WA USA. [Platnick, Steven] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Zhang, ZB (reprint author), UMBC, Dept Phys, Baltimore, MD 21250 USA.; Zhang, ZB (reprint author), UMBC, Joint Ctr Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. EM zzbatmos@umbc.edu RI Ghan, Steven/H-4301-2011; OI Ghan, Steven/0000-0001-8355-8699; Ma, Po-Lun/0000-0003-3109-5316 FU Department of Energy (DOE) Regional & Global Climate Modeling Program [DE-SC0014641]; U.S. National Science Foundation through the MRI program [CNS-0821258, CNS-1228778]; U.S. National Science Foundation through the SCREMS program [DMS-0821311] FX This research is supported by Department of Energy (DOE) Regional & Global Climate Modeling Program (grant DE-SC0014641) managed by Renu Joseph. The computations in this study were performed at the UMBC High Performance Computing Facility (HPCF). The facility is supported by the U.S. National Science Foundation through the MRI program (grants CNS-0821258 and CNS-1228778) and the SCREMS program (grant DMS-0821311), with additional substantial support from UMBC. The ground-based retrievals and measurements from the DOE CAP-MBL campaign are available from DOE ARM data server http://www.archive.arm.gov/armlogin/login.jsp. The MODISdata are obtained from NASA's Level 1 and Atmosphere Archive and Distribution System (LAADS http://ladsweb.nascom.nasa.gov/). NR 36 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 27 PY 2017 VL 122 IS 4 BP 2351 EP 2365 DI 10.1002/2016JD025763 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EN6NR UT WOS:000396121200019 ER PT J AU Lacagnina, C Hasekamp, OP Torres, O AF Lacagnina, Carlo Hasekamp, Otto P. Torres, Omar TI Direct radiative effect of aerosols based on PARASOL and OMI satellite observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OPTICAL-PROPERTIES; A-TRAIN; ANTHROPOGENIC AEROSOLS; GLOBAL OCEANS; EC-EARTH; CLOUDS; MODEL; AERONET; AEROCOM; RETRIEVALS AB Accurate portrayal of the aerosol characteristics is crucial to determine aerosol contribution to the Earth's radiation budget. We employ novel satellite retrievals to make a new measurement-based estimate of the shortwave direct radiative effect of aerosols (DREA), both over land and ocean. Global satellite measurements of aerosol optical depth, single-scattering albedo (SSA), and phase function from PARASOL (Polarization and Anisotropy of Reflectances for Atmospheric Sciences coupled with Observations from a Lidar) are used in synergy with OMI (Ozone Monitoring Instrument) SSA. Aerosol information is combined with land-surface bidirectional reflectance distribution function and cloud characteristics from MODIS (Moderate Resolution Imaging Spectroradiometer) satellite products. Eventual gaps in observations are filled with the state-of-the-art global aerosol model ECHAM5-HAM2. It is found that our estimate of DREA is largely insensitive to model choice. Radiative transfer calculations show that DREA at top-of-atmosphere is -4.6 +/- 1.5 W/m(2) for cloud-free and -2.1 +/- 0.7 W/m(2) for all-sky conditions, during year 2006. These fluxes are consistent with, albeit generally less negative over ocean than, former assessments. Unlike previous studies, our estimate is constrained by retrievals of global coverage SSA, which may justify different DREA values. Remarkable consistency is found in comparison with DREA based on CERES (Clouds and the Earth's Radiant Energy System) and MODIS observations. C1 [Lacagnina, Carlo; Hasekamp, Otto P.] SRON Netherlands Inst Space Res, Utrecht, Netherlands. [Torres, Omar] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD USA. RP Lacagnina, C (reprint author), SRON Netherlands Inst Space Res, Utrecht, Netherlands. EM C.Lacagnina@sron.nl FU User Support Space Research program of the Netherlands Organization for Scientific Research (NWO) [ALW-GO/13-38] FX This work has been supported by the User Support Space Research program of the Netherlands Organization for Scientific Research (NWO) through project ALW-GO/13-38. The authors are grateful to the anonymous reviewers for their constructive comments that have helped for the improvement of this paper. We thank the AERONET principal investigators and their staff for establishing and maintaining the sites used in this study. The AERONET data set can be obtained from http://aeronet.gsfc.nasa.gov/. We thank NASA for the online availability of the OMI (http://disc.sci.gsfc.nasa.gov/Aura/data-holdings/OMI/omaeruv_v003) and MODIS products (https://ladsweb.nascom.nasa.gov/data/search.html and https://lpdaac.usgs.gov/dataset_discovery/modis/modis_products_table/mcd 43b3). The authors are grateful to Kai Zhang for providing ECHAM5-HAM2 model's data and to Twan van Noije for making available TM5 model's data. These modeling data can be accessed following the instructions at the AeroCom portal http://aerocom.met.no/data.html. The PARASOL data set, the results, and the code used in this study are available at ftp://ftp.sron.nl/open-access-data/carlol/doi-jgr-2016. NR 85 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 27 PY 2017 VL 122 IS 4 BP 2366 EP 2388 DI 10.1002/2016JD025706 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EN6NR UT WOS:000396121200020 ER PT J AU Painemal, D Chiu, JYC Minnis, P Yost, C Zhou, XL Cadeddu, M Eloranta, E Lewis, ER Ferrare, R Kollias, P AF Painemal, David Chiu, J. -Y. Christine Minnis, Patrick Yost, Christopher Zhou, Xiaoli Cadeddu, Maria Eloranta, Edwin Lewis, Ernie R. Ferrare, Richard Kollias, Pavlos TI Aerosol and cloud microphysics covariability in the northeast Pacific boundary layer estimated with ship-based and satellite remote sensing observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID LIQUID WATER PATH; VOCALS-REX; PERFORMANCE-CHARACTERISTICS; STRATOCUMULUS CLOUDS; MARINE STRATOCUMULUS; NUMBER CONCENTRATION; HIGH-SENSITIVITY; LEAST-SQUARES; VARIABILITY; RETRIEVALS AB Ship measurements collected over the northeast Pacific along transects between the port of Los Angeles (33.7 degrees N, 118.2 degrees W) and Honolulu (21.3 degrees N, 157.8 degrees W) during May to August 2013 were utilized to investigate the covariability between marine low cloud microphysical and aerosol properties. Ship-based retrievals of cloud optical depth (tau) from a Sun photometer and liquid water path (LWP) from a microwave radiometer were combined to derive cloud droplet number concentration N-d and compute a cloud-aerosol interaction (ACI) metric defined as ACI(CCN) = partial derivative ln(N-d)/partial derivative ln(CCN), with CCN denoting the cloud condensation nuclei concentration measured at 0.4% (CCN0.4) and 0.3% (CCN0.3) supersaturation. Analysis of CCN0.4, accumulation mode aerosol concentration (N-a), and extinction coefficient (sigma(ext)) indicates that N-a and sigma(ext) can be used as CCN0.4 proxies for estimating ACI. ACI(CCN) derived from 10 min averaged N-d and CCN0.4 and CCN0.3, and CCN0.4 regressions using N-a and sigma(ext), produce high ACI(CCN): near 1.0, that is, a fractional change in aerosols is associated with an equivalent fractional change in N-d. ACI(CCN) computed in deep boundary layers was small (ACI(CCN) = 0.60), indicating that surface aerosol measurements inadequately represent the aerosol variability below clouds. Satellite cloud retrievals from MODerate-resolution Imaging Spectroradiometer and GOES-15 data were compared against ship-based retrievals and further analyzed to compute a satellite-based ACI(CCN). Satellite data correlated well with their ship-based counterparts with linear correlation coefficients equal to or greater than 0.78. Combined satellite N-d and ship-based CCN0.4 and N-a yielded a maximum ACI(CCN) = 0.88-0.92, a value slightly less than the ship-based ACI(CCN), but still consistent with aircraft-based studies in the eastern Pacific. C1 [Painemal, David; Yost, Christopher] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Painemal, David; Minnis, Patrick; Ferrare, Richard] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Chiu, J. -Y. Christine] Univ Reading, Dept Meteorol, Reading, Berks, England. [Zhou, Xiaoli] McGill Univ, Dept Atmospher & Ocean Sci, Montreal, PQ, Canada. [Cadeddu, Maria] Argonne Natl Lab, Div Environm Sci, Lemont, IL USA. [Eloranta, Edwin] Univ Wisconsin Madison, Space Sci & Engn Ctr, Madison, WI USA. [Lewis, Ernie R.] Brookhaven Natl Lab, Upton, NY 11973 USA. [Kollias, Pavlos] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA. RP Painemal, D (reprint author), Sci Syst & Applicat Inc, Hampton, VA 23666 USA.; Painemal, D (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM david.painemal@nasa.gov FU U.S. Department of Energy (DOE), Office of Science, Office of Biological and Environmental Research (OBER): DOE-BER Atmospheric Science Research Program (ASR) [DE-FOA-0000885, DE-SC0011666, DE-AC02-06CH11357, DE-SC00112704]; NASA CERES program FX This work was supported by the U.S. Department of Energy (DOE), Office of Science, Office of Biological and Environmental Research (OBER): DOE-BER Atmospheric Science Research Program (ASR) grants DE-FOA-0000885 (D. Painemal, P. Minnis, and C. Yost) and DE-SC0011666 (J.C. Chiu), Atmospheric Radiation Measurement Infrastructure Basic Energy Sciences, under contract DE-AC02-06CH11357 (M. Cadeddu), and DOE-BER under contract DE-SC00112704 (E.R. Lewis). C. Yost was also supported by the NASA CERES program. The MAGIC data set was downloaded from the ARM archive available at http://www.archive.arm.gov/. MODIS and GOES-15 retrievals are available at http://www-pm.larc.nasa.gov or upon request. We thank Horizon Lines and the Captain and crew of the Horizon Spirit for their support and hospitality during MAGIC. The constructive comments and suggestions provided by three anonymous reviewers are greatly appreciated. NR 52 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 27 PY 2017 VL 122 IS 4 BP 2403 EP 2418 DI 10.1002/2016JD025771 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EN6NR UT WOS:000396121200022 ER PT J AU Hartmann, JM Boulet, C Toon, GC AF Hartmann, J. -M. Boulet, C. Toon, G. C. TI Collision-induced absorption by N-2 near 2.16 mu m: Calculations, model, and consequences for atmospheric remote sensing SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID N2-N2 PAIRS; SPECTRA; TEMPERATURES; MOLECULES; O-2; DEPENDENCE; MISSION; BANDS; CO2; N2 AB Classical molecular dynamics simulations (CMDS) are used for calculations of the collision-induced absorption (CIA) by pure N-2 in the (2.1-2.2 mu m) region of the first overtone band. They lead to reasonable (+/- 15%) agreement with the only two laboratory measurements available, at 97 K and room temperature. Based on these experiment/theory comparisons, empirical corrections are made to the CMDS-calculated CIA of pure N-2 in the 200-300 K temperature range. In addition, the contribution of N-2-O-2 collisions is, in the absence of any laboratory measurement, calculated and a simple semiempirical model (the first of its kind) is built in order to predict the CIA of N-2 under Earth atmosphere conditions. This is successfully validated by comparisons with ground-based atmospheric transmission spectra in the 2.1-2.2 mu m region. C1 [Hartmann, J. -M.] Univ Paris Saclay, Ecole Polytech, CNRS IPSL, Lab Meteorol Dynam, Palaiseau, France. [Boulet, C.] Univ Paris Saclay, Univ Paris Sud, CNRS, ISMO, Orsay, France. [Toon, G. C.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Hartmann, JM (reprint author), Univ Paris Saclay, Ecole Polytech, CNRS IPSL, Lab Meteorol Dynam, Palaiseau, France. EM jean-michel.hartmann@lmd.polytechni-que.fr NR 37 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 27 PY 2017 VL 122 IS 4 BP 2419 EP 2428 DI 10.1002/2016JD025677 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EN6NR UT WOS:000396121200023 ER PT J AU Daly, EA Brodeur, RD Auth, TD AF Daly, Elizabeth A. Brodeur, Richard D. Auth, Toby D. TI Anomalous ocean conditions in 2015: impacts on spring Chinook salmon and their prey field SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Warm anomaly; Ichthyoplankton; Salmon feeding; Salmon condition; Ocean survival ID COLUMBIA RIVER PLUME; NORTHERN CALIFORNIA CURRENT; ICHTHYOPLANKTON COMMUNITY; ONCORHYNCHUS-TSHAWYTSCHA; OCEANOGRAPHIC CONDITIONS; JUVENILE SALMONIDS; PACIFIC SALMON; SURVIVAL RATES; UPWELLING ZONE; COHO SALMON AB In the northern California Current, Columbia River Chinook salmon Oncorhynchus tshawytscha that return as adults in spring are primarily hatchery-produced, though they include natural-origin fish listed under the US Endangered Species Act. Anomalously warm ocean conditions persisted in the California Current during 2015 (> 2.5 degrees C above normal) through the winter period when fish prey resources of juvenile salmon develop and during spring as salmon enter the ocean. The biomass of ichthyoplankton in winter 2015 was the 4th highest of our 18 yr time-series (1998-2015), predicting good food conditions for salmon and high adult salmon returns several years later. The larval composition of 2015 ichthyoplankton included abnormally large amounts of the warm-water taxa northern anchovy Engraulis mordax and rockfish Sebastes spp. When the composition of ichthyoplankton is dominated by warm-water taxa in winter, we would predict poor returns of salmon. May diets of juvenile Chinook salmon collected in coastal waters reflected high proportions of juvenile rockfish, no evidence of northern anchovy, and most closely resembled those of other warm years. June diets also reflected a warm prey community being consumed, predicting poor returns of salmon. Chinook salmon had high percentages of empty stomachs and were small and thin in 2015, with fish weighing 17.6% less than the same-length fish in a cold year (2008). Lower condition of juvenile Chinook salmon related to decreased returns of adult salmon. Overall, all but one biological predictor (biomass of prey) suggests that the prospects for the 2015 ocean-entry smolts were not favorable for survival. C1 [Daly, Elizabeth A.] Oregon State Univ, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA. [Brodeur, Richard D.] NOAA, Fish Ecol Div, Northwest Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. [Auth, Toby D.] Pacific States Marine Fisheries Commiss, Newport, OR 97365 USA. RP Daly, EA (reprint author), Oregon State Univ, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA. EM elizabeth.daly@oregonstate.edu FU Bonneville Power Administration [1998-014-00]; NOAA through the Cooperative Research Program FX We thank the many scientists who assisted in collecting and processing the stomach samples over the years and Jennifer Fisher from Oregon State University and others from the NOAA zooplankton laboratory in Newport, OR for assistance in collecting samples along the NH line. We thank 3 anonymous journal reviewers for helpful comments on the manuscript. This work was funded by the Bonneville Power Administration (project #1998-014-00) and NOAA through the Cooperative Research Program. NR 61 TC 0 Z9 0 U1 0 U2 0 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 EI 1616-1599 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PD FEB 27 PY 2017 VL 566 BP 169 EP 182 DI 10.3354/meps12021 PG 14 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA EN5NB UT WOS:000396051300013 ER PT J AU Copeman, LA Laurel, BJ Spencer, M Sremba, A AF Copeman, Louise A. Laurel, Benjamin J. Spencer, Mara Sremba, Angie TI Temperature impacts on lipid allocation among juvenile gadid species at the Pacific Arctic-Boreal interface: an experimental laboratory approach SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Temperature; Climate change; Arctic-Boreal; Cod; Lipid storage; Condition index ID POLLOCK THERAGRA-CHALCOGRAMMA; COD GADUS-MORHUA; SOUTHEASTERN BERING-SEA; AGE-0 WALLEYE POLLOCK; CLIMATE-CHANGE; BOREOGADUS-SAIDA; ATLANTIC COD; ENERGY ALLOCATION; FISH COMMUNITIES; CHUKCHI SEAS AB Climate change impacts on Arctic fish communities will largely be determined by temperature-dependent vital metabolic rates of resident and invading species. In this study, we experimentally measured total lipids and lipid class storage in the liver and muscle of 2 juvenile Arctic gadids (Arctic cod Boreogadus saida and saffron cod Eleginus gracilis) and 2 juvenile boreal gadids (walleye pollock Gadus chalcogrammus and Pacific cod Gadus macrocephalus). Experiments were conducted over a 4 wk period across 5 temperatures (0, 5, 9, 16 and 20 degrees C) at the Hatfield Marine Science Center in Newport, OR, USA. Results indicated clear species-specific non-linear effects of temperature on lipid accumulation. Arctic cod demonstrated a cold-water, stenothermic response with relatively high lipid storage (28 mg lipid g(-1) WWT) and growth at 0 degrees C. In contrast, saffron cod demonstrated a warmer-water, eurythermic response with elevated growth at temperatures beyond 16 degrees C but comparatively low lipid storage across all thermal habitats (10 to 17 mg lipid g(-1) WWT). Lipid storage and growth in the boreal species was dome-shaped and notably higher at intermediate temperatures (maximum lipid values of 44 mg lipid g(-1) WWT for walleye pollock, 28 mg lipid g(-1) WWT for Pacific cod). Further, the combined effects of temperature on both growth and lipid storage led to elevated lipid accumulation rate (LAR) indices in boreal species (4 to 11) compared to Arctic species (< 3) at temperatures above 4 degrees C. These results suggest that warming in the Arctic will lead to decreased condition in the resident mid-trophic fish assemblage in the absence of replacement by more boreal-type species shifting poleward. C1 [Copeman, Louise A.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, 2030 SE Marine Sci Dr, Newport, OR 97365 USA. [Copeman, Louise A.; Sremba, Angie] Oregon State Univ, Cooperat Inst Marine Resources Studies, 2030 SE Marine Sci Dr, Newport, OR 97365 USA. [Laurel, Benjamin J.; Spencer, Mara] NOAA, Fisheries Behav Ecol Program, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2030 SE Marine Sci Dr, Newport, OR 97365 USA. RP Copeman, LA (reprint author), Oregon State Univ, Coll Earth Ocean & Atmospher Sci, 2030 SE Marine Sci Dr, Newport, OR 97365 USA.; Copeman, LA (reprint author), Oregon State Univ, Cooperat Inst Marine Resources Studies, 2030 SE Marine Sci Dr, Newport, OR 97365 USA. EM lcopeman@coas.oregonstate.edu FU North Pacific Research Board (NPRB) [1228]; NOAA-AFSC FX We thank Karolin Klinck for assistance with tissue extractions, fish dissections and general management of the Marine Lipids Laboratory during the time of this experiment. We thank C. Ryer for reviewing earlier drafts of this manuscript. Thanks also to Bill Kopplin, Robert Fechhelm, Kyle McCain, Bill Streever and the LGL field crew for their assistance in the collection of Arctic and saffron cod in Prudhoe Bay as well as to Scott Haines, Paul Iseri and Michele Ottmar for their assistance with the fish transport and animal husbandry. This project was supported with funding from the North Pacific Research Board (NPRB) Grant #1228 and 2014 Essential Fish Habitat funding from NOAA-AFSC. This study is NPRB contribution no. 614. The findings and conclusions in the paper are those of the authors and do not necessarily represent the views of the National Marine Fisheries Service. NR 85 TC 0 Z9 0 U1 0 U2 0 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 EI 1616-1599 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PD FEB 27 PY 2017 VL 566 BP 183 EP 198 DI 10.3354/meps12040 PG 16 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA EN5NB UT WOS:000396051300014 ER PT J AU Chiow, SW Williams, J Yu, N Muller, H AF Chiow, Sheng-wey Williams, Jason Yu, Nan Mueller, Holger TI Gravity-gradient suppression in spaceborne atomic tests of the equivalence principle SO PHYSICAL REVIEW A LA English DT Article AB The gravity gradient is one of the most serious systematic effects in atomic tests of the equivalence principle (EP). While differential acceleration measurements performed with different atomic species under free fall test the validity of the EP, minute displacements between the test masses in a gravity gradient produce a false EP-violating signal that limits the precision of the test. We show that gravity inversion and modulation using a gimbal mount can suppress the systematics due to gravity gradients caused by both moving and stationary parts of the instrument as well as the environment, strongly reducing the need to overlap two species. C1 [Chiow, Sheng-wey; Williams, Jason; Yu, Nan] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Mueller, Holger] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. RP Yu, N (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM nan.yu@jpl.nasa.gov; hm@berkeley.edu NR 16 TC 0 Z9 0 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD FEB 27 PY 2017 VL 95 IS 2 AR 021603 DI 10.1103/PhysRevA.95.021603 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA EN4LR UT WOS:000395979500001 ER PT J AU Remy, S Veira, A Paugam, R Sofiev, M Kaiser, JW Marenco, F Burton, SP Benedetti, A Engelen, RJ Ferrare, R Hair, JW AF Remy, Samuel Veira, Andreas Paugam, Ronan Sofiev, Mikhail Kaiser, Johannes W. Marenco, Franco Burton, Sharon P. Benedetti, Angela Engelen, Richard J. Ferrare, Richard Hair, Jonathan W. TI Two global data sets of daily fire emission injection heights since 2003 SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID WILD-LAND FIRES; SMOKE PLUME-RISE; RADIATIVE POWER; FORECASTING SYSTEM; TRANSPORT MODELS; CLIMATE SYSTEM; BURNED AREA; RESOLUTION; MODIS; AIRBORNE AB The Global Fire Assimilation System (GFAS) assimilates fire radiative power (FRP) observations from satellite-based sensors to produce daily estimates of biomass burning emissions. It has been extended to include information about injection heights derived from fire observations and meteorological information from the operational weather forecasts of ECMWF. Injection heights are provided by two distinct methods: the Integrated Monitoring and Modelling System for wildland fires (IS4FIRES) parameterisation and the one-dimensional plume rise model (PRM). A global database of daily biomass burning emissions and injection heights at 0.1 degrees resolution has been produced for 2003-2015 and is continuously extended in near-real time with the operational GFAS service of the Copernicus Atmospheric Monitoring Service (CAMS). In this study, the two injection height data sets were compared with the new MPHP2 (MISR Plume Height Project 2) satellite-based plume height retrievals. The IS4FIRES parameterisation showed a better overall agreement than the observations, while the PRM was better at capturing the variability of injection heights. The performance of both parameterisations is also dependent on the type of vegetation. Furthermore, the use of biomass burning emission heights from GFAS in atmospheric composition forecasts was assessed in two case studies: the South AMerican Biomass Burning Analysis (SAMBBA) campaign which took place in September 2012 in Brazil, and a series of large fire events in the western USA in August 2013. For these case studies, forecasts of biomass burning aerosol species by the Composition Integrated Forecasting System (C-IFS) of CAMS were found to better reproduce the observed vertical distribution when using PRM injection heights from GFAS compared to aerosols emissions being prescribed at the surface. The globally available GFAS injection heights introduced and evaluated in this study provide a comprehensive data set for future fire and atmospheric composition modelling studies. C1 [Remy, Samuel] UPMC CNRS, Lab Meteorol Dynam, Paris, France. [Veira, Andreas] Max Planck Inst Meteorol, Hamburg, Germany. [Paugam, Ronan] Kings Coll London, London, England. [Sofiev, Mikhail] Finnish Meteorol Inst, Helsinki, Finland. [Kaiser, Johannes W.] Max Planck Inst Chem, Mainz, Germany. [Marenco, Franco] Met Off, Satellite Applicat, Exeter, Devon, England. [Burton, Sharon P.; Ferrare, Richard; Hair, Jonathan W.] NASA, Langley Res Ctr, Hampton, CA USA. [Benedetti, Angela; Engelen, Richard J.] European Ctr Medium Range Weather Forecasts, Reading, Berks, England. RP Remy, S (reprint author), UPMC CNRS, Lab Meteorol Dynam, Paris, France. EM samuel.remy@ecmwf.int FU EU Seventh Research Framework Programme (MACC-III project) [283576] FX This research was supported by the EU Seventh Research Framework Programme (MACC-III project, contract number 283576). NR 72 TC 0 Z9 0 U1 1 U2 1 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 FEB 27 PY 2017 VL 17 IS 4 BP 2921 EP 2942 DI 10.5194/acp-17-2921-2017 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EM1ZZ UT WOS:000395117400001 ER PT J AU Boyda, E Basu, S Ganguly, S Michaelis, A Mukhopadhyay, S Nemani, RR AF Boyda, Edward Basu, Saikat Ganguly, Sangram Michaelis, Andrew Mukhopadhyay, Supratik Nemani, Ramakrishna R. TI Deploying a quantum annealing processor to detect tree cover in aerial imagery of California SO PLOS ONE LA English DT Article AB Quantum annealing is an experimental and potentially breakthrough computational technology for handling hard optimization problems, including problems of computer vision. We present a case study in training a production-scale classifier of tree cover in remote sensing imagery, using early-generation quantum annealing hardware built by D-wave Systems, Inc. Beginning within a known boosting framework, we train decision stumps on texture features and vegetation indices extracted from four-band, one-meter-resolution aerial imagery from the state of California. We then impose a regulated quadratic training objective to select an optimal voting subset from among these stumps. The votes of the subset define the classifier. For optimization, the logical variables in the objective function map to quantum bits in the hardware device, while quadratic couplings encode as the strength of physical interactions between the quantum bits. Hardware design limits the number of couplings between these basic physical entities to five or six. To account for this limitation in mapping large problems to the hardware architecture, we propose a truncation and rescaling of the training objective through a trainable metaparameter. The boosting process on our basic 108- and 508-variable problems, thus constituted, returns classifiers that incorporate a diverse range of color-and texture-based metrics and discriminate tree cover with accuracies as high as 92% in validation and 90% on a test scene encompassing the open space preserves and dense suburban build of Mill Valley, CA. C1 [Boyda, Edward] St Marys Coll Calif, Dept Phys & Astron, Moraga, CA 94556 USA. [Boyda, Edward; Ganguly, Sangram] Bay Area Environm Res Inst, Moffett Field, CA 94952 USA. [Basu, Saikat; Mukhopadhyay, Supratik] Louisiana State Univ, Dept Comp Sci, Baton Rouge, LA 70803 USA. [Ganguly, Sangram; Michaelis, Andrew] NASA Ames Res Ctr, Div Earth Sci, Moffett Field, CA USA. [Michaelis, Andrew] CSU Monterey Bay, Univ Corp, Seaside, CA USA. [Nemani, Ramakrishna R.] NASA Ames Res Ctr, NASA Adv Supercomp Div, Moffett Field, CA USA. RP Boyda, E (reprint author), St Marys Coll Calif, Dept Phys & Astron, Moraga, CA 94556 USA.; Boyda, E (reprint author), Bay Area Environm Res Inst, Moffett Field, CA 94952 USA. EM ekb2@stmarys-ca.edu FU NASA Earth Science Division FX This work was supported by the NASA Earth Science Division and performed using the computing facilities of the NASA Advanced Supercomputing (NAS) division and NASA Earth Exchange (NEX). Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect that of NASA or the United States Government. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 42 TC 0 Z9 0 U1 1 U2 1 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD FEB 27 PY 2017 VL 12 IS 2 AR e0172505 DI 10.1371/journal.pone.0172505 PG 22 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EN3UW UT WOS:000395934400024 PM 28241028 ER PT J AU Klimas, AJ Uritsky, VM AF Klimas, Alexander J. Uritsky, Vadim M. TI Criticality and turbulence in a resistive magnetohydrodynamic current sheet SO PHYSICAL REVIEW E LA English DT Review ID SELF-ORGANIZED CRITICALITY; DRIVEN DISSIPATIVE SYSTEMS; DYNAMICS; EARTHQUAKES; SIMILARITY; DISRUPTION; AVALANCHE; EXPONENTS; EVOLUTION; MODELS AB Scaling properties of a two-dimensional (2d) plasma physical current-sheet simulation model involving a full set of magnetohydrodynamic (MHD) equations with current-dependent resistivity are investigated. The current sheet supports a spatial magnetic field reversal that is forced through loading of magnetic flux containing plasma at boundaries of the simulation domain. A balance is reached between loading and annihilation of the magnetic flux through reconnection at the current sheet; the transport of magnetic flux from boundaries to current sheet is realized in the form of spatiotemporal avalanches exhibiting power-law statistics of lifetimes and sizes. We identify this dynamics as self-organized criticality (SOC) by verifying an extended set of scaling laws related to both global and local properties of the current sheet (critical susceptibility, finite-size scaling of probability distributions, geometric exponents). The critical exponents obtained from this analysis suggest that the model operates in a slowly driven SOC state similar to the mean-field state of the directed stochastic sandpile model. We also investigate multiscale correlations in the velocity field and find them numerically indistinguishable from certain intermittent turbulence (IT) theories. The results provide clues on physical conditions for SOC behavior in a broad class of plasma systems with propagating instabilities, and suggest that SOC and IT may coexist in driven current sheets which occur ubiquitously in astrophysical and space plasmas. C1 [Klimas, Alexander J.] Univ Maryland Baltimore Cty, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Uritsky, Vadim M.] Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Klimas, AJ (reprint author), Univ Maryland Baltimore Cty, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. FU NASA Geospace Sciences program; NASA through the CUA's Institute for Astrophysics and Computational Sciences [NNG11PL10A 670.014] FX The work of A.J.K. was supported by the NASA Geospace Sciences program. V.U. was supported by the NASA Grant No. NNG11PL10A 670.014 through the CUA's Institute for Astrophysics and Computational Sciences. The authors thank M. Paczuski for useful discussions and remarks on the manuscript. NR 51 TC 0 Z9 0 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0045 EI 2470-0053 J9 PHYS REV E JI Phys. Rev. E PD FEB 24 PY 2017 VL 95 IS 2 DI 10.1103/PhysRevE.95.023209 PG 6 WC Physics, Fluids & Plasmas; Physics, Mathematical SC Physics GA EL5MT UT WOS:000394665900012 PM 28297949 ER PT J AU Shelestov, A Lavreniuk, M Kussul, N Novikov, A Skakun, S AF Shelestov, Andrii Lavreniuk, Mykola Kussul, Nataliia Novikov, Alexei Skakun, Sergii TI Exploring Google Earth Engine Platform for Big Data Processing: Classification of Multi-Temporal Satellite Imagery for Crop Mapping SO FRONTIERS IN EARTH SCIENCE LA English DT Article DE Google Earth Engine; big data; classification; optical satellite imagery; land cover; land use; image processing ID LANDSAT DATA; EFFICIENCY ASSESSMENT; BIOPHYSICAL MODELS; UKRAINE; REFLECTANCE; FUSION AB Many applied problems arising in agricultural monitoring and food security require reliable crop maps at national or global scale. Large scale crop mapping requires processing andmanagement of large amount of heterogeneous satellite imagery acquired by various sensors that consequently leads to a "Big Data" problem. The main objective of this study is to explore efficiency of using the Google Earth Engine (GEE) platform when classifying multi-temporal satellite imagery with potential to apply the platform for a larger scale (e.g., country level) and multiple sensors (e.g., Landsat-8 and Sentinel-2). In particular, multiple state-of-the-art classifiers available in the GEE platformare compared to produce a high resolution (30 m) crop classification map for a large territory (similar to 28,100 km(2) and 1.0 M ha of cropland). Though this study does not involve large volumes of data, it does address efficiency of the GEE platform to effectively execute complex workflows of satellite data processing required with large scale applications such as crop mapping. The study discusses strengths and weaknesses of classifiers, assesses accuracies that can be achieved with different classifiers for the Ukrainian landscape, and compares them to the benchmark classifier using a neural network approach that was developed in our previous studies. The study is carried out for the Joint Experiment of Crop Assessment and Monitoring (JECAM) test site in Ukraine covering the Kyiv region (North of Ukraine) in 2013. We found that GEE provides very good performance in terms of enabling access to the remote sensing products through the cloud platform and providing pre-processing; however, in terms of classification accuracy, the neural network based approach outperformed support vector machine (SVM), decision tree and random forest classifiers available in GEE. C1 [Shelestov, Andrii; Lavreniuk, Mykola; Kussul, Nataliia] Space Res Inst NASU SSAU, Dept Space Informat Technol & Syst, Kiev, Ukraine. [Shelestov, Andrii; Lavreniuk, Mykola; Kussul, Nataliia; Novikov, Alexei] Natl Tech Univ Ukraine, Igor Sikorsky Kyiv Polytech Inst, Dept Informat Secur, Kiev, Ukraine. [Skakun, Sergii] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Skakun, Sergii] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Lavreniuk, M (reprint author), Space Res Inst NASU SSAU, Dept Space Informat Technol & Syst, Kiev, Ukraine.; Lavreniuk, M (reprint author), Natl Tech Univ Ukraine, Igor Sikorsky Kyiv Polytech Inst, Dept Informat Secur, Kiev, Ukraine. EM nick_93@ukr.net FU Google Inc FX This research was conducted in the framework of the "Large scale crop mapping in Ukraine using SAR and optical data fusion" Google Earth Engine Research Award funded by the Google Inc. NR 36 TC 0 Z9 0 U1 4 U2 4 PU FRONTIERS MEDIA SA PI LAUSANNE PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015, SWITZERLAND SN 2296-6463 J9 FRONT EARTH SCI JI Front. Earth Sci. PD FEB 24 PY 2017 VL 5 BP 1 EP 10 AR UNSP 17 DI 10.3389/feart.2017.00017 PG 10 WC Geosciences, Multidisciplinary SC Geology GA EL6BA UT WOS:000394704200001 ER PT J AU Susko, D Karunatillake, S Kodikara, G Skok, JR Wray, J Heldmann, J Cousin, A Judice, T AF Susko, David Karunatillake, Suniti Kodikara, Gayantha Skok, J. R. Wray, James Heldmann, Jennifer Cousin, Agnes Judice, Taylor TI A record of igneous evolution in Elysium, a major martian volcanic province SO SCIENTIFIC REPORTS LA English DT Article ID THERMAL INERTIA; MARS; GEOCHEMISTRY; PLANITIA; HISTORY; WATER; LAVA AB A major knowledge gap exists on how eruptive compositions of a single martian volcanic province change over time. Here we seek to fill that gap by assessing the compositional evolution of Elysium, a major martian volcanic province. A unique geochemical signature overlaps with the southeastern flows of this volcano, which provides the context for this study of variability of martian magmatism. The southeastern lava fields of Elysium Planitia show distinct chemistry in the shallow subsurface (down to several decimeters) relative to the rest of the martian mid-to-low latitudes (average crust) and flows in northwest Elysium. By impact crater counting chronology we estimated the age of the southeastern province to be 0.85 +/- 0.08 Ga younger than the northwestern fields. This study of the geochemical and temporal differences between the NW and SE Elysium lava fields is the first to demonstrate compositional variation within a single volcanic province on Mars. We interpret the geochemical and temporal differences between the SE and NW lava fields to be consistent with primary magmatic processes, such as mantle heterogeneity or change in depth of melt formation within the martian mantle due to crustal loading. C1 [Susko, David; Karunatillake, Suniti; Judice, Taylor] Louisiana State Univ, Dept Geol & Geophys, Baton Rouge, LA 70803 USA. [Kodikara, Gayantha] Univ Rahuna, Fac Fisheries & Marine Sci Technol, Dept Oceanog & Marine Geol, Matara, Sri Lanka. [Skok, J. R.] SETI Inst, Mountain View, CA 94043 USA. [Wray, James] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Heldmann, Jennifer] NASA Ames, Moffett Field, CA USA. [Cousin, Agnes] Inst Rech Astrophys & Planetol, Toulouse, France. RP Susko, D (reprint author), Louisiana State Univ, Dept Geol & Geophys, Baton Rouge, LA 70803 USA. EM Davidsusko@gmail.com RI Wray, James/B-8457-2008 OI Wray, James/0000-0001-5559-2179 FU NASA Mars Data Analysis Program (MDAP) [NNX13A198G]; LA Space Grant Consortium REA [115-40-4139]; Graduate Student Research Award (GSRA) [NNX15AH82H]; LSU Chancellor's Aide student Scholarship FX We acknowledge NASA Mars Data Analysis Program (MDAP) grant NNX13A198G, the LA Space Grant Consortium REA grant 115-40-4139 and Graduate Student Research Award (GSRA) NNX15AH82H, and the LSU Chancellor's Aide student Scholarship without which none of this research would have been possible. We acknowledge Charles Everhardt and Rory Bentley for their hard work with crater counting and image analysis. Thank you to Lorrie Carnes and Don Hood for providing editorial revisions. Also, thank you to the reviewers of this manuscript James Dohm and a second reviewer who wished to remain anonymous. Their comments and revisions forced this work to mature to be the most scientifically robust that it could be. NR 55 TC 0 Z9 0 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2045-2322 J9 SCI REP-UK JI Sci Rep PD FEB 24 PY 2017 VL 7 AR 43177 DI 10.1038/srep43177 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EM2UY UT WOS:000395172500001 PM 28233797 ER PT J AU Gong, J Wu, DL AF Gong, Jie Wu, Dong L. TI Microphysical properties of frozen particles inferred from Global Precipitation Measurement (GPM) Microwave Imager (GMI) polarimetric measurements SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID RADIATIVE-TRANSFER SIMULATIONS; ICE PARTICLES; CLOUD SYSTEMS; POLARIZATION; CRYSTALS; GHZ; ORIENTATION; RETRIEVALS; EXTINCTION; INSTRUMENT AB Scattering differences induced by frozen particle microphysical properties are investigated, using the vertically (V) and horizontally (H) polarized radiances from the Global Precipitation Measurement (GPM) Microwave Imager (GMI) 89 and 166 GHz channels. It is the first study on frozen particle microphysical properties on a global scale that uses the dual-frequency microwave polarimetric signals. From the ice cloud scenes identified by the 183.3 +/- 3 GHz channel brightness temperature (T-b), we find that the scattering by frozen particles is highly polarized, with V-H polarimetric differences (PDs) being positive throughout the tropics and the winter hemisphere mid-latitude jet regions, including PDs from the GMI 89 and 166 GHz TBs, as well as the PD at 640 GHz from the ER-2 Compact Scanning Submillimeter-wave Imaging Radiometer (CoSSIR) during the TC4 campaign. Large polarization dominantly occurs mostly near convective outflow regions (i.e., anvils or stratiform precipitation), while the polarization signal is small inside deep convective cores as well as at the remote cirrus region. Neglecting the polarimetric signal would easily result in as large as 30% error in ice water path retrievals. There is a universal "bell curve" in the PD-TBV relationship, where the PD amplitude peaks at similar to 10K for all three channels in the tropics and increases slightly with latitude (2-4 K). Moreover, the 166 GHz PD tends to increase in the case where a melting layer is beneath the frozen particles aloft in the atmosphere, while 89 GHz PD is less sensitive than 166 GHz to the melting layer. This property creates a unique PD feature for the identification of the melting layer and stratiform rain with passive sensors. Horizontally oriented non-spherical frozen particles are thought to produce the observed PD because of different ice scattering properties in the V and H polarizations. On the other hand, turbulent mixing within deep convective cores inevitably promotes the random orientation of these particles, a mechanism that works effectively in reducing the PD. The current GMI polarimetric measurements themselves cannot fully disentangle the possible mechanisms. C1 [Gong, Jie] Univ Space Res Assoc, Columbia, MD 21046 USA. [Gong, Jie; Wu, Dong L.] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD USA. RP Gong, J (reprint author), Univ Space Res Assoc, Columbia, MD 21046 USA. EM jie.gong@nasa.gov FU NASA [NNH12ZDA001N-INVEST] FX We thank Frank Evans for providing the RT4 code with GMI configuration, and help on interpreting the CoSSIR data. We are also grateful to Ben Johnson, Stephen Munchak and Paul Racette for helpful discussions. Jeffrey Piepmeier and Rachael Kroodsma are acknowledged for assisting in the interpretation of the GMI's channel noises. Two anonymous reviewers' and Yana Mentrok's insightful comments and suggestions are highly appreciated. This work is supported by the NASA NNH12ZDA001N-INVEST fund. NR 48 TC 0 Z9 0 U1 1 U2 1 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 FEB 23 PY 2017 VL 17 IS 4 BP 2741 EP 2757 DI 10.5194/acp-17-2741-2017 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EM1XA UT WOS:000395109300001 ER PT J AU Abbott, BP Abbott, R Abbott, TD Abernathy, MR Ackley, K Adams, C Addesso, P Adhikari, RX Adya, VB Affeldt, C Aggarwal, N Aguiar, OD Ain, A Ajith, P Allen, B Altin, PA Anderson, SB Anderson, WG Arai, K Araya, MC Arceneaux, CC Areeda, JS Arun, KG Ashton, G Ast, M Aston, SM Aufmuth, P Aulbert, C Babak, S Baker, PT Ballmer, SW Barayoga, JC Barclay, SE Barish, BC Barker, D Barr, B Barsotti, L Bartlett, J Bartos, I Bassiri, R Batch, JC Baune, C Bell, AS Berger, BK Bergmann, G Berry, CPL Betzwieser, J Bhagwat, S Bhandare, R Bilenko, IA Billingsley, G Birch, J Birney, R Biscans, S Bisht, A Biwer, C Blackburn, JK Blair, CD Blair, DG Blair, RM Bock, O Bogan, C Bohe, A Bond, C Bork, R Bose, S Brady, PR Braginsky, VB Brau, JE Brinkmann, M Brockill, P Broida, JE Brooks, AF Brown, DA Brown, DD Brown, NM Brunett, S Buchanan, CC Buikema, A Buonanno, A Byer, RL Cabero, M Cadonati, L Cahillane, C Bustillo, JC Callister, T Camp, JB Cannon, KC Cao, J Capano, CD Caride, S Caudill, S Cavaglia, M Cepeda, CB Chamberlin, SJ Chan, M Chao, S Charlton, P Cheeseboro, BD Chen, HY Chen, Y Cheng, C Cho, HS Cho, M Chow, JH Christensen, N Chu, Q Chung, S Ciani, G Clara, F Clark, JA Collette, CG Cominsky, L Constancio, M Cook, D Corbitt, TR Cornish, N Corsi, A Costa, CA Coughlin, MW Coughlin, SB Countryman, ST Couvares, P Cowan, EE Coward, DM Cowart, MJ Coyne, DC Coyne, R Craig, K Creighton, JDE Cripe, J Crowder, SG Cumming, A Cunningham, L Dal Canton, T Danilishin, SL Danzmann, K Darman, NS Dasgupta, A Costa, CFD Dave, I Davies, GS Daw, EJ De, S Debra, D Del Pozzo, W Denker, T Dent, T Dergachev, V DeRosa, RT DeSalvo, R Devine, RC Dhurandhar, S Diaz, MC Di Palma, I Donovan, F Dooley, KL Doravari, S Douglas, R Downes, TP Drago, M Drever, RWP Driggers, JC Dwyer, SE Edo, TB Edwards, MC Effler, A Eggenstein, HB Ehrens, P Eichholz, J Eikenberry, SS Engels, W Essick, RC Etzel, T Evans, M Evans, TM Everett, R Factourovich, M Fair, H Fairhurst, S Fan, X Fang, Q Farr, B Farr, WM Favata, M Fays, M Fehrmann, H Fejer, MM Fenyvesi, E Ferreira, EC Fisher, RP Fletcher, M Frei, Z Freise, A Frey, R Fritschel, P Frolov, VV Fulda, P Fyffe, M Gabbard, HAG Gair, JR Gaonkar, SG Gaur, G Gehrels, N Geng, P George, J Gergely, L Ghosh, A Ghosh, A Giaime, JA Giardina, KD Gill, K Glaefke, A Goetz, E Goetz, R Gondan, L Gonzalez, G Gopakumar, A Gordon, NA Gorodetsky, ML Gossan, SE Graef, C Graff, PB Grant, A Gras, S Gray, C Green, AC Grote, H Grunewald, S Guo, X Gupta, A Gupta, MK Gushwa, KE Gustafson, EK Gustafson, R Hacker, JJ Hall, BR Hall, ED Hammond, G Haney, M Hanke, MM Hanks, J Hanna, C Hannam, MD Hanson, J Hardwick, T Harry, GM Harry, IW Hart, MJ Hartman, MT Haster, CJ Haughian, K Heintze, MC Hendry, M Heng, IS Hennig, J Henry, J Heptonstall, AW Heurs, M Hild, S Hoak, D Holt, K Holz, DE Hopkins, P Hough, J Houston, EA Howell, EJ Hu, YM Huang, S Huerta, EA Hughey, B Husa, S Huttner, SH Huynh-Dinh, T Indik, N Ingram, DR Inta, R Isa, HN Isi, M Isogai, T Iyer, BR Izumi, K Jang, H Jani, K Jawahar, S Jian, L Jimenez-Forteza, F Johnson, WW Jones, DI Jones, R Ju, L Haris, K Kalaghatgi, CV Kalogera, V Kandhasamy, S Kang, G Kanner, JB Kapadia, SJ Karki, S Karvinen, KS Kasprzack, M Katsavounidis, E Katzman, W Kaufer, S Kaur, T Kawabe, K Kehl, MS Keitel, D Kelley, DB Kells, W Kennedy, R Key, JS Khalili, FY Khan, S Khan, Z Khazanov, EA Kijbunchoo, N Kim, CW Kim, C Kim, J Kim, K Kim, N Kim, W Kim, YM Kimbrell, SJ King, EJ King, PJ Kissel, JS Klein, B Kleybolte, L Klimenko, S Koehlenbeck, SM Kondrashov, V Kontos, A Korobko, M Korth, WZ Kozak, DB Kringel, V Krueger, C Kuehn, G Kumar, P Kumar, R Kuo, L Lackey, BD Landry, M Lange, J Lantz, B Lasky, PD Laxen, M Lazzarini, A Leavey, S Lebigot, EO Lee, CH Lee, HK Lee, HM Lee, K Lenon, A Leong, JR Levin, Y Lewis, JB Li, TGF Libson, A Littenberg, TB Lockerbie, NA Lombardi, AL London, LT Lord, JE Lormand, M Lough, JD Luck, H Lundgren, AP Lynch, R Ma, Y Machenschalk, B MacInnis, M Macleod, DM Magana-Sandoval, F Zertuche, LM Magee, RM Mandic, V Mangano, V Mansell, GL Manske, M Marka, S Marka, Z Markosyan, AS Maros, E Martin, IW Martynov, DV Mason, K Massinger, TJ Masso-Reid, M Matichard, F Matone, L Mavalvala, N Mazumder, N McCarthy, R McClelland, DE McCormick, S McGuire, SC McIntyre, G McIver, J McManus, DJ McRae, T McWilliams, ST Meacher, D Meadors, GD Melatos, A Mendell, G Mercer, RA Merilh, EL Meshkov, S Messenger, C Messick, C Meyers, PM Miao, H Middleton, H Mikhailov, EE Miller, AL Miller, A Miller, BB Miller, J Millhouse, M Ming, J Mirshekari, S Mishra, C Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Mohapatra, SRP Moore, BC Moore, CJ Moraru, D Moreno, G Morriss, SR Mossavi, K Mow-Lowry, CM Mueller, G Muir, AW Mukherjee, A Mukherjee, D Mukherjee, S Mukund, N Mullavey, A Munch, J Murphy, DJ Murray, PG Mytidis, A Nayak, RK Nedkova, K Nelson, TJN Neunzert, A Newton, G Nguyen, TT Nielsen, AB Nitz, A Nolting, D Normandin, MEN Nuttall, LK Oberling, J Ochsner, E O'Dell, J Oelker, E Ogin, GH Oh, JJ Oh, SH Ohme, F Oliver, M Oppermann, P Oram, RJ O'Reilly, B O'Shaughnessy, R Ottaway, DJ Overmier, H Owen, BJ Pai, A Pai, SA Palamos, JR Palashov, O Pal-Singh, A Pan, H Pankow, C Pannarale, F Pant, BC Papa, MA Paris, HR Parker, W Pascucci, D Patrick, Z Pearlstone, BL Pedraza, M Pekowsky, L Pele, A Penn, S Perreca, A Perri, LM Phelps, M Pierro, V Pinto, IM Pitkin, M Poe, M Post, A Powell, J Prasad, J Predoi, V Prestegard, T Price, LR Prijatelj, M Principe, M Privitera, S Prokhorov, L Puncken, O Purrer, M Qi, H Qin, J Qiu, S Quetschke, V Quintero, EA Quitzow-James, R Raab, FJ Rabeling, DS Radkins, H Raffai, P Raja, S Rajan, C Rakhmanov, M Raymond, V Read, J Reed, CM Reid, S Reitze, DH Rew, H Reyes, SD Riles, K Rizzo, M Robertson, NA Robie, R Rollins, JG Roma, VJ Romanov, G Romie, JH Rowan, S Rudiger, A Ryan, K Sachdev, S Sadecki, T Sadeghian, L Sakellariadou, M Saleem, M Salemi, F Samajdar, A Sammut, L Sanchez, EJ Sandberg, V Sandeen, B Sanders, JR Sathyaprakash, BS Saulson, PR Sauter, OES Savage, RL Sawadsky, A Schale, P Schilling, R Schmidt, J Schmidt, P Schnabel, R Schofield, RMS Schonbeck, A Schreiber, E Schuette, D Schutz, BF Scott, J Scott, SM Sellers, D Sengupta, AS Sergeev, A Shaddock, DA Shaffer, T Shahriar, MS Shaltev, M Shapiro, B Shawhan, P Sheperd, A Shoemaker, DH Shoemaker, DM Siellez, K Siemens, X Sigg, D Silva, AD Singer, A Singer, LP Singh, A Singh, R Sintes, AM Slagmolen, BJJ Smith, JR Smith, ND Smith, RJE Son, EJ Sorazu, B Souradeep, T Srivastava, AK Staley, A Steinke, M Steinlechner, J Steinlechner, S Steinmeyer, D Stephens, BC Stone, R Strain, KA Strauss, NA Strigin, S Sturani, R Stuver, AL Summerscales, TZ Sun, L Sunil, S Sutton, PJ Szczepanczyk, MJ Talukder, D Tanner, DB Tapai, M Tarabrin, SP Taracchini, A Taylor, R Theeg, T Thirugnanasambandam, MP Thomas, EG Thomas, M Thomas, P Thorne, KA Thrane, E Tiwari, V Tokmakov, KV Toland, K Tomlinson, C Tornasi, Z Torres, CV Torrie, CI Toyra, D Traylor, G Trifiro, D Tse, M Tuyenbayev, D Ugolini, D Unnikrishnan, CS Urban, AL Usman, SA Vahlbruch, H Vajente, G Valdes, G Vander-Hyde, DC van Veggel, AA Vass, S Vaulin, R Vecchio, A Veitch, J Veitch, PJ Venkateswara, K Vinciguerra, S Vine, DJ Vitale, S Vo, T Vorvick, C Voss, DV Vousden, WD Vyatchanin, SP Wade, AR Wade, LE Wade, M Walker, M Wallace, L Walsh, S Wang, H Wang, M Wang, X Wang, Y Ward, RL Warner, J Weaver, B Weinert, M Weinstein, AJ Weiss, R Wen, L Wessels, P Westphal, T Wette, K Whelan, JT Whiting, BF Williams, RD Williamson, AR Willis, JL Willke, B Wimmer, MH Winkler, W Wipf, CC Wittel, H Woan, G Woehler, J Worden, J Wright, JL Wu, DS Wu, G Yablon, J Yam, W Yamamoto, H Yancey, CC Yu, H Zanolin, M Zevin, M Zhang, L Zhang, M Zhang, Y Zhao, C Zhou, M Zhou, Z Zhu, XJ Zucker, ME Zuraw, SE Zweizig, J Harms, J AF Abbott, B. P. Abbott, R. Abbott, T. D. Abernathy, M. R. Ackley, K. Adams, C. Addesso, P. Adhikari, R. X. Adya, V. B. Affeldt, C. Aggarwal, N. Aguiar, O. D. Ain, A. Ajith, P. Allen, B. Altin, P. A. Anderson, S. B. Anderson, W. G. Arai, K. Araya, M. C. Arceneaux, C. C. Areeda, J. S. Arun, K. G. Ashton, G. Ast, M. Aston, S. M. Aufmuth, P. Aulbert, C. Babak, S. Baker, P. T. Ballmer, S. W. Barayoga, J. C. Barclay, S. E. Barish, B. C. Barker, D. Barr, B. Barsotti, L. Bartlett, J. Bartos, I. Bassiri, R. Batch, J. C. Baune, C. Bell, A. S. Berger, B. K. Bergmann, G. Berry, C. P. L. Betzwieser, J. Bhagwat, S. Bhandare, R. Bilenko, I. A. Billingsley, G. Birch, J. Birney, R. Biscans, S. Bisht, A. Biwer, C. Blackburn, J. K. Blair, C. D. Blair, D. G. Blair, R. M. Bock, O. Bogan, C. Bohe, A. Bond, C. Bork, R. Bose, S. Brady, P. R. Braginsky, V. B. Brau, J. E. Brinkmann, M. Brockill, P. Broida, J. E. Brooks, A. F. Brown, D. A. Brown, D. D. Brown, N. M. Brunett, S. Buchanan, C. C. Buikema, A. Buonanno, A. Byer, R. L. Cabero, M. Cadonati, L. Cahillane, C. Bustillo, J. Calderon Callister, T. Camp, J. B. Cannon, K. C. Cao, J. Capano, C. D. Caride, S. Caudill, S. Cavaglia, M. Cepeda, C. B. Chamberlin, S. J. Chan, M. Chao, S. Charlton, P. Cheeseboro, B. D. Chen, H. Y. Chen, Y. Cheng, C. Cho, H. S. Cho, M. Chow, J. H. Christensen, N. Chu, Q. Chung, S. Ciani, G. Clara, F. Clark, J. A. Collette, C. G. Cominsky, L. Constancio, M., Jr. Cook, D. Corbitt, T. R. Cornish, N. Corsi, A. Costa, C. A. Coughlin, M. W. Coughlin, S. B. Countryman, S. T. Couvares, P. Cowan, E. E. Coward, D. M. Cowart, M. J. Coyne, D. C. Coyne, R. Craig, K. Creighton, J. D. E. Cripe, J. Crowder, S. G. Cumming, A. Cunningham, L. Dal Canton, T. Danilishin, S. L. Danzmann, K. Darman, N. S. Dasgupta, A. Costa, C. F. Da Silva Dave, I. Davies, G. S. Daw, E. J. De, S. Debra, D. Del Pozzo, W. Denker, T. Dent, T. Dergachev, V. DeRosa, R. T. DeSalvo, R. Devine, R. C. Dhurandhar, S. Diaz, M. C. Di Palma, I. Donovan, F. Dooley, K. L. Doravari, S. Douglas, R. Downes, T. P. Drago, M. Drever, R. W. P. Driggers, J. C. Dwyer, S. E. Edo, T. B. Edwards, M. C. Effler, A. Eggenstein, H-B Ehrens, P. Eichholz, J. Eikenberry, S. S. Engels, W. Essick, R. C. Etzel, T. Evans, M. Evans, T. M. Everett, R. Factourovich, M. Fair, H. Fairhurst, S. Fan, X. Fang, Q. Farr, B. Farr, W. M. Favata, M. Fays, M. Fehrmann, H. Fejer, M. M. Fenyvesi, E. Ferreira, E. C. Fisher, R. P. Fletcher, M. Frei, Z. Freise, A. Frey, R. Fritschel, P. Frolov, V. V. Fulda, P. Fyffe, M. Gabbard, H. A. G. Gair, J. R. Gaonkar, S. G. Gaur, G. Gehrels, N. Geng, P. George, J. Gergely, L. Ghosh, Abhirup Ghosh, Archisman Giaime, J. A. Giardina, K. D. Gill, K. Glaefke, A. Goetz, E. Goetz, R. Gondan, L. Gonzalez, G. Gopakumar, A. Gordon, N. A. Gorodetsky, M. L. Gossan, S. E. Graef, C. Graff, P. B. Grant, A. Gras, S. Gray, C. Green, A. C. Grote, H. Grunewald, S. Guo, X. Gupta, A. Gupta, M. K. Gushwa, K. E. Gustafson, E. K. Gustafson, R. Hacker, J. J. Hall, B. R. Hall, E. D. Hammond, G. Haney, M. Hanke, M. M. Hanks, J. Hanna, C. Hannam, M. D. Hanson, J. Hardwick, T. Harry, G. M. Harry, I. W. Hart, M. J. Hartman, M. T. Haster, C-J Haughian, K. Heintze, M. C. Hendry, M. Heng, I. S. Hennig, J. Henry, J. Heptonstall, A. W. Heurs, M. Hild, S. Hoak, D. Holt, K. Holz, D. E. Hopkins, P. Hough, J. Houston, E. A. Howell, E. J. Hu, Y. M. Huang, S. Huerta, E. A. Hughey, B. Husa, S. Huttner, S. H. Huynh-Dinh, T. Indik, N. Ingram, D. R. Inta, R. Isa, H. N. Isi, M. Isogai, T. Iyer, B. R. Izumi, K. Jang, H. Jani, K. Jawahar, S. Jian, L. Jimenez-Forteza, F. Johnson, W. W. Jones, D. I. Jones, R. Ju, L. Haris, K. Kalaghatgi, C. V. Kalogera, V. Kandhasamy, S. Kang, G. Kanner, J. B. Kapadia, S. J. Karki, S. Karvinen, K. S. Kasprzack, M. Katsavounidis, E. Katzman, W. Kaufer, S. Kaur, T. Kawabe, K. Kehl, M. S. Keitel, D. Kelley, D. B. Kells, W. Kennedy, R. Key, J. S. Khalili, F. Y. Khan, S. Khan, Z. Khazanov, E. A. Kijbunchoo, N. Kim, Chi-Woong Kim, Chunglee Kim, J. 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Thomas, M. Thomas, P. Thorne, K. A. Thrane, E. Tiwari, V. Tokmakov, K. V. Toland, K. Tomlinson, C. Tornasi, Z. Torres, C. V. Torrie, C. I. Toyra, D. Traylor, G. Trifiro, D. Tse, M. Tuyenbayev, D. Ugolini, D. Unnikrishnan, C. S. Urban, A. L. Usman, S. A. Vahlbruch, H. Vajente, G. Valdes, G. Vander-Hyde, D. C. van Veggel, A. A. Vass, S. Vaulin, R. Vecchio, A. Veitch, J. Veitch, P. J. Venkateswara, K. Vinciguerra, S. Vine, D. J. Vitale, S. Vo, T. Vorvick, C. Voss, D. V. Vousden, W. D. Vyatchanin, S. P. Wade, A. R. Wade, L. E. Wade, M. Walker, M. Wallace, L. Walsh, S. Wang, H. Wang, M. Wang, X. Wang, Y. Ward, R. L. Warner, J. Weaver, B. Weinert, M. Weinstein, A. J. Weiss, R. Wen, L. Wessels, P. Westphal, T. Wette, K. Whelan, J. T. Whiting, B. F. Williams, R. D. Williamson, A. R. Willis, J. L. Willke, B. Wimmer, M. H. Winkler, W. Wipf, C. C. Wittel, H. Woan, G. Woehler, J. Worden, J. Wright, J. L. Wu, D. S. Wu, G. Yablon, J. Yam, W. Yamamoto, H. Yancey, C. C. Yu, H. Zanolin, M. Zevin, M. Zhang, L. Zhang, M. Zhang, Y. Zhao, C. Zhou, M. Zhou, Z. Zhu, X. J. Zucker, M. E. Zuraw, S. E. Zweizig, J. Harms, J. CA LIGO Sci Collaboration TI Exploring the sensitivity of next generation gravitational wave detectors SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article DE gravitational waves; cosmic explorer; LIGO ID SQUEEZED VACUUM STATES; NEUTRON-STAR MASSES; QUANTUM OPTICS; BLACK-HOLES; LIGHT; INTERFEROMETRY; COLLAPSE; NOISE AB The second-generation of gravitational-wave detectors are just starting operation, and have already yielding their first detections. Research is now concentrated on how to maximize the scientific potential of gravitational-wave astronomy. To support this effort, we present here design targets for a new generation of detectors, which will be capable of observing compact binary sources with high signal-to-noise ratio throughout the Universe. C1 [Abbott, B. P.; Abbott, R.; Adhikari, R. X.; Anderson, S. B.; Arai, K.; Araya, M. C.; Barayoga, J. C.; Barish, B. C.; Berger, B. K.; Billingsley, G.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Brunett, S.; Cahillane, C.; Callister, T.; Cepeda, C. B.; Couvares, P.; Coyne, D. C.; Dergachev, V.; Drever, R. W. P.; Ehrens, P.; Eichholz, J.; Etzel, T.; Gossan, S. E.; Gushwa, K. E.; Gustafson, E. K.; Hall, E. D.; Heptonstall, A. W.; Isi, M.; Kanner, J. B.; Kells, W.; Kondrashov, V.; Korth, W. Z.; Kozak, D. B.; Lazzarini, A.; Lewis, J. B.; Maros, E.; McIntyre, G.; McIver, J.; Meshkov, S.; Pedraza, M.; Perreca, A.; Price, L. R.; Quintero, E. A.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Sachdev, S.; Sanchez, E. J.; Schmidt, P.; Singer, A.; Smith, N. D.; Smith, R. J. E.; Taylor, R.; Thirugnanasambandam, M. P.; Torrie, C. I.; Vajente, G.; Vass, S.; Wallace, L.; Weinstein, A. J.; Williams, R. D.; Wipf, C. C.; Yamamoto, H.; Zhang, L.; Zucker, M. E.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Abbott, T. D.; Buchanan, C. C.; Corbitt, T. R.; Cripe, J.; Giaime, J. A.; Gonzalez, G.; Hardwick, T.; Johnson, W. W.; Kasprzack, M.; Macleod, D. M.; Singh, R.; Walker, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA. [Abernathy, M. R.; Harry, G. M.] Amer Univ, Washington, DC 20016 USA. [Ackley, K.; Ciani, G.; Costa, C. F. Da Silva; Eichholz, J.; Eikenberry, S. S.; Fulda, P.; Goetz, R.; Hartman, M. T.; Klimenko, S.; Miller, A. L.; Mitselmakher, G.; Mueller, G.; Mytidis, A.; Reitze, D. H.; Tanner, D. B.; Voss, D. V.; Whiting, B. F.] Univ Florida, Gainesville, FL 32611 USA. [Adams, C.; Aston, S. M.; Betzwieser, J.; Birch, J.; Cowart, M. J.; DeRosa, R. T.; Effler, A.; Evans, T. M.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Hanson, J.; Heintze, M. C.; Holt, K.; Huynh-Dinh, T.; Katzman, W.; Laxen, M.; Lormand, M.; McCormick, S.; Mullavey, A.; Nelson, T. J. N.; Nolting, D.; Oram, Richard J.; O'Reilly, B.; Overmier, H.; Parker, W.; Pele, A.; Romie, J. H.; Sellers, D.; Stuver, A. L.; Thomas, M.; Thorne, K. 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[Harms, J.] Univ Urbino Carlo Bo, I-61029 Urbino, Italy. INFN, Sez Firenze, I-50019 Sesto Fiorentino, Italy. RP Abbott, BP (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA. EM lsc-spokesperson@ligo.org RI Strigin, Sergey/I-8337-2012; Danilishin, Stefan/K-7262-2012; Sergeev, Alexander/F-3027-2017; Harms, Jan/J-4359-2012; OI Danilishin, Stefan/0000-0001-7758-7493; Nitz, Alexander/0000-0002-1850-4587; Davies, Gareth/0000-0002-4289-3439; Principe, Maria/0000-0002-6327-0628 FU National Science Foundation [PHY-0757058]; [PHY-0823459] FX LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation, and operates under cooperative agreement PHY-0757058. Advanced LIGO was built under award PHY-0823459. This paper carries LIGO Document Number LIGO-P1600143. NR 92 TC 1 Z9 1 U1 6 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD FEB 23 PY 2017 VL 34 IS 4 AR 044001 DI 10.1088/1361-6382/aa51f4 PG 18 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA EM6BN UT WOS:000395397900001 ER PT J AU Lunt, DJ Huber, M Anagnostou, E Baatsen, MLJ Caballero, R DeConto, R Dijkstra, HA Donnadieu, Y Evans, D Feng, R Foster, GL Gasson, E von der Heydt, AS Hollis, CJ Inglis, GN Jones, SM Kiehl, J Turner, SK Korty, RL Kozdon, R Krishnan, S Ladant, JB Langebroek, P Lear, CH LeGrande, AN Littler, K Markwick, P Otto-Bliesner, B Pearson, P Poulsen, CJ Salzmann, U Shields, C Snell, K Starz, M Super, J Tabor, C Tierney, JE Tourte, GJL Tripati, A Upchurch, GR Wade, BS Wing, SL Winguth, AME Wright, NM Zachos, JC Zeebe, RE AF Lunt, Daniel J. Huber, Matthew Anagnostou, Eleni Baatsen, Michiel L. J. Caballero, Rodrigo DeConto, Rob Dijkstra, Henk A. Donnadieu, Yannick Evans, David Feng, Ran Foster, Gavin L. Gasson, Ed von der Heydt, Anna S. Hollis, Chris J. Inglis, Gordon N. Jones, Stephen M. Kiehl, Jeff Turner, Sandy Kirtland Korty, Robert L. Kozdon, Reinhardt Krishnan, Srinath Ladant, Jean-Baptiste Langebroek, Petra Lear, Caroline H. LeGrande, Allegra N. Littler, Kate Markwick, Paul Otto-Bliesner, Bette Pearson, Paul Poulsen, Christopher J. Salzmann, Ulrich Shields, Christine Snell, Kathryn Staerz, Michael Super, James Tabor, Clay Tierney, Jessica E. Tourte, Gregory J. L. Tripati, Aradhna Upchurch, Garland R. Wade, Bridget S. Wing, Scott L. Winguth, Arne M. E. Wright, Nicky M. Zachos, James C. Zeebe, Richard E. TI The DeepMIP contribution to PMIP4: experimental design for model simulations of the EECO, PETM, and pre-PETM (version 1.0) SO GEOSCIENTIFIC MODEL DEVELOPMENT LA English DT Article ID EARLY EOCENE; INTERCOMPARISON PROJECT; BOUNDARY-CONDITIONS; CLIMATE FEEDBACKS; REGIONAL UPLIFT; OCEAN; PROXY; PALEOCENE; PALEOGENE AB Past warm periods provide an opportunity to evaluate climate models under extreme forcing scenarios, in particular high (>800 ppmv) atmospheric CO2 concentrations. Although a post hoc intercomparison of Eocene (similar to 50 Ma) climate model simulations and geological data has been carried out previously, models of past high-CO2 periods have never been evaluated in a consistent framework. Here, we present an experimental design for climate model simulations of three warm periods within the early Eocene and the latest Paleocene (the EECO, PETM, and pre-PETM). Together with the CMIP6 pre-industrial control and abrupt 4 x CO2 simulations, and additional sensitivity studies, these form the first phase of DeepMIP - the Deep-time Model Intercomparison Project, itself a group within the wider Paleo-climate Modelling Intercomparison Project (PMIP). The experimental design specifies and provides guidance on boundary conditions associated with palaeogeography, greenhouse gases, astronomical configuration, solar constant, land surface processes, and aerosols. Initial conditions, simulation length, and output variables are also specified. Finally, we explain how the geological data sets, which will be used to evaluate the simulations, will be developed. C1 [Lunt, Daniel J.; Tourte, Gregory J. L.] Univ Bristol, Sch Geog Sci, Bristol, Avon, England. [Huber, Matthew] Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA. [Baatsen, Michiel L. J.; Dijkstra, Henk A.; von der Heydt, Anna S.] Univ Utrecht, Inst Marine & Atmospher Res Utrecht IMAU, Utrecht, Netherlands. [Caballero, Rodrigo] Stockholm Univ, Dept Meteorol, Stockholm, Sweden. [DeConto, Rob; Gasson, Ed] Univ Massachusetts, Dept Geosci, Amherst, MA USA. [Donnadieu, Yannick; Ladant, Jean-Baptiste] CNRS, CEA, Lab Sci Climat & Environm, Gif Sur Yvette, France. [Krishnan, Srinath; Super, James] Yale Univ, Dept Geol & Geophys, New Haven, CT 06520 USA. [Feng, Ran; Otto-Bliesner, Bette; Shields, Christine; Tabor, Clay] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. [Anagnostou, Eleni; Foster, Gavin L.] Univ Southampton, Natl Oceanog Ctr Southampton, Ocean & Earth Sci, Southampton, Hants, England. [Hollis, Chris J.] GNS Sci, Wellington, New Zealand. [Turner, Sandy Kirtland] Univ Calif Riverside, Dept Earth Sci, Riverside, CA 92521 USA. [Korty, Robert L.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. [Kozdon, Reinhardt] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Langebroek, Petra] Bjerknes Ctr Climate Res, Uni Res Climate, Bergen, Norway. [Lear, Caroline H.] Cardiff Univ, Sch Earth & Ocean Sci, Cardiff, S Glam, Wales. [LeGrande, Allegra N.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Littler, Kate] Univ Exeter, Camborne Sch Mines, Exeter, Devon, England. [Markwick, Paul] Getech Grp Plc, Leeds, W Yorkshire, England. [Poulsen, Christopher J.] Univ Michigan, Dept Earth & Environm Sci, Ann Arbor, MI 48109 USA. [Salzmann, Ulrich] Northumbria Univ, Dept Geog, Newcastle Upon Tyne, Tyne & Wear, England. [Snell, Kathryn] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. [Staerz, Michael] Alfred Wegener Inst, Bremerhaven, Germany. [Tierney, Jessica E.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. [Upchurch, Garland R.] Texas State Univ, Dept Biol, San Marcos, TX 78666 USA. [Wade, Bridget S.] UCL, Dept Earth Sci, London, England. [Wing, Scott L.] Smithsonian Inst, Dept Paleobiol, Washington, DC USA. [Winguth, Arne M. E.] Univ Texas Arlington, Earth & Environm Sci, Arlington, TX 76019 USA. [Wright, Nicky M.] Univ Sydney, Sch Geosci, Sydney, NSW, Australia. [Zachos, James C.] Univ Calif Santa Cruz, Inst Marine Sci, PBSci Earth & Planetary Sci Dept, Santa Cruz, CA 95064 USA. [Zeebe, Richard E.] Univ Hawaii Manoa, Dept Oceanog, Honolulu, HI 96822 USA. [Evans, David] Univ St Andrews, Dept Earth Sci, St Andrews, Fife, Scotland. [Inglis, Gordon N.] Univ Bristol, Sch Chem, Bristol, Avon, England. [Tripati, Aradhna] Univ Calif Los Angeles, Inst Environm & Sustainabil, Atmospher & Ocean Sci, Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. [Jones, Stephen M.] Univ Birmingham, Sch Geog Earth & Environm Sci, Birmingham, W Midlands, England. RP Lunt, DJ (reprint author), Univ Bristol, Sch Geog Sci, Bristol, Avon, England. EM d.j.lunt@bristol.ac.uk RI Korty, Robert/E-2534-2012; Huber, Matthew/A-7677-2008; Caballero, Rodrigo/E-4637-2010 OI Korty, Robert/0000-0002-8743-5044; Huber, Matthew/0000-0002-2771-9977; Caballero, Rodrigo/0000-0002-5507-9209 FU NERC [NE/N006828/1, NE/K014757/1]; ERC [340923]; NSF [OCE-0902882]; Netherlands Earth System Science Centre (NESSC); Ministry of Education, Culture and Science (OCW) [024.002.001] FX We thank NERC grant NE/N006828/1 for providing funds for the first DeepMIP meeting in Boulder, Colorado, USA, in January 2016. Daniel J. Lunt acknowledges the NERC grant "Cretaceous-Paleocene-Eocene: Exploring Climate and Climate Sensitivity" (NE/K014757/1), and advanced ERC grant "The Greenhouse Earth System" (T-GRES, project reference 340923), awarded to Rich Pancost. Matthew Huber acknowledges funding from NSF OCE-0902882. Michiel L. J. Baatsen, Henk A. Dijkstra, and Anna S. von der Heydt acknowledge support by the Netherlands Earth System Science Centre (NESSC), financially supported by the Ministry of Education, Culture and Science (OCW), 024.002.001. We thank two anonymous reviewers whose comments were very useful in improving and clarifying the experimental design. NR 46 TC 0 Z9 0 U1 4 U2 4 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1991-959X EI 1991-9603 J9 GEOSCI MODEL DEV JI Geosci. Model Dev. PD FEB 23 PY 2017 VL 10 IS 2 BP 889 EP 901 DI 10.5194/gmd-10-889-2017 PG 13 WC Geosciences, Multidisciplinary SC Geology GA EM1XW UT WOS:000395111600001 ER PT J AU Gillon, M Triaud, AHMJ Demory, BO Jehin, E Agol, E Deck, KM Lederer, SM de Wit, J Burdanov, A Ingalls, JG Bolmont, E Leconte, J Raymond, SN Selsis, F Turbet, M Barkaoui, K Burgasser, A Burleigh, MR Carey, SJ Chaushev, A Copperwheat, CM Delrez, L Fernandes, CS Holdsworth, DL Kotze, EJ Van Grootel, V Almleaky, Y Benkhaldoun, Z Magain, P Queloz, D AF Gillon, Michael Triaud, Amaury H. M. J. Demory, Brice-Olivier Jehin, Emmanuel Agol, Eric Deck, Katherine M. Lederer, Susan M. de Wit, Julien Burdanov, Artem Ingalls, James G. Bolmont, Emeline Leconte, Jeremy Raymond, Sean N. Selsis, Franck Turbet, Martin Barkaoui, Khalid Burgasser, Adam Burleigh, Matthew R. Carey, Sean J. Chaushev, Aleksander Copperwheat, Chris M. Delrez, Laetitia Fernandes, Catarina S. Holdsworth, Daniel L. Kotze, Enrico J. Van Grootel, Valerie Almleaky, Yaseen Benkhaldoun, Zouhair Magain, Pierre Queloz, Didier TI Seven temperate terrestrial planets around the nearby ultracool dwarf star TRAPPIST-1 SO NATURE LA English DT Article ID MAIN-SEQUENCE STARS; TRANSITING PLANETS; HABITABLE ZONES; SUPER-EARTHS; SYSTEMS; STELLAR; MODELS; ECCENTRICITY; RESONANCES; INVERSION AB One aim of modern astronomy is to detect temperate, Earth-like exoplanets that are well suited for atmospheric characterization. Recently, three Earth-sized planets were detected that transit (that is, pass in front of) a star with a mass just eight per cent that of the Sun, located 12 parsecs away(1). The transiting configuration of these planets, combined with the Jupiter-like size of their host star-named TRAPPIST-1-makes possible in-depth studies of their atmospheric properties with present-day and future astronomical facilities(1-3). Here we report the results of a photometric monitoring campaign of that star from the ground and space. Our observations reveal that at least seven planets with sizes and masses similar to those of Earth revolve around TRAPPIST-1. The six inner planets form a near-resonant chain, such that their orbital periods (1.51, 2.42, 4.04, 6.06, 9.1 and 12.35 days) are near-ratios of small integers. This architecture suggests that the planets formed farther from the star and migrated inwards(4,5). Moreover, the seven planets have equilibrium temperatures low enough to make possible the presence of liquid water on their surfaces(6-8). C1 [Gillon, Michael; Jehin, Emmanuel; Burdanov, Artem; Magain, Pierre] Univ Liege, Space Sci Technol & Astrophys Res STAR Inst, Allee 6 Auot 19C,Bat B5C, B-4000 Liege, Belgium. [Triaud, Amaury H. M. J.] Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Demory, Brice-Olivier] Univ Bern, Ctr Space & Habitabil, Sidlerstr 5, CH-3012 Bern, Switzerland. [Demory, Brice-Olivier] Cavendish Lab, JJ Thomson Ave, Cambridge CB3 0HE, England. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Agol, Eric] NASA, Astrobiol Inst, Virtual Planetary Lab, Seattle, WA 98195 USA. [Deck, Katherine M.] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. [Lederer, Susan M.] NASA, Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. [de Wit, Julien] MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Ingalls, James G.; Carey, Sean J.] CALTECH, Spitzer Sci Ctr, 1200 E Calif Blvd,Mail Code 314-6, Pasadena, CA 91125 USA. [Bolmont, Emeline] Univ Namur, Dept Math, NaXys, 8 Rempart La Vierge, B-5000 Namur, Belgium. [Bolmont, Emeline] Univ Paris Diderot, CNRS, Ctr Saclay, IRFU,SAp,DRF,CEA,Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. [Leconte, Jeremy; Raymond, Sean N.; Selsis, Franck] Univ Bordeaux, CNRS, Lab Astrophys Bordeaux, B18N Allee Geoffroy St Hilaire, F-33615 Pessac, France. [Turbet, Martin; Delrez, Laetitia] Univ Paris 06, Sorbonne Univ, CNRS, Lab Meteorol Dynam, 4 Pl Jussieu, F-75005 Paris, France. [Barkaoui, Khalid; Benkhaldoun, Zouhair] Cadi Ayyad Univ, FSSM, Lab LPHEA, Oukaimeden Observ, BP 2390, Marrakech, Morocco. [Burgasser, Adam] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Burleigh, Matthew R.; Chaushev, Aleksander] Univ Leicester, Dept Phys & Astron, Leicester Inst Space & Earth Observ, Leicester LE1 7RH, Leics, England. [Copperwheat, Chris M.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Holdsworth, Daniel L.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Kotze, Enrico J.] South African Astron Observ, Observ, POB 9, ZA-7935 Cape Town, South Africa. [Almleaky, Yaseen] King Abdulaziz Univ, Fac Sci, Space & Astron Dept, Jeddah 21589, Saudi Arabia. [Almleaky, Yaseen] King Abdullah Ctr Crescent Observat & Astron, Makkah Clock, Mecca 24231, Saudi Arabia. [Queloz, Didier] Univ Geneva, Observ Geneva, 51 Chemin Maillettes, CH-1290 Sauverny, Switzerland. RP Gillon, M (reprint author), Univ Liege, Space Sci Technol & Astrophys Res STAR Inst, Allee 6 Auot 19C,Bat B5C, B-4000 Liege, Belgium. EM michael.gillon@ulg.ac.be RI Faculty of, Sciences, KAU/E-7305-2017 FU NASA; NASA [NNX15AI75G, NNX13AF62G, NNH05ZDA001C]; Belgian Fonds (National) de la Recherche Scientifique (F.R.S.-FNRS) [FRFC 2.5.594.09.F]; University of Liege; European Research Council (ERC) [336480, 679030]; Actions de Recherche Concertee (ARC) grant - Wallonia-Brussels Federation; UK Science and Technology Facilities Council; Swiss National Science Foundation [PP00P2_163967]; National Science Foundation (NSF) [AST-1615315]; European Research Council through ERC [SPIRE 647383]; Agence Nationale pour la Recherche (ANR) [ANR-13-BS05-0003-002]; [296.C-5010(A)] FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. The material presented here is based on work supported in part by NASA under contract no. NNX15AI75G. TRAPPIST-South is a project funded by the Belgian Fonds (National) de la Recherche Scientifique (F.R.S.-FNRS) under grant FRFC 2.5.594.09.F, with the participation of the Swiss National Science Foundation (FNS/SNSF). TRAPPIST-North is a project funded by the University of Liege, and performed in collaboration with Cadi Ayyad University of Marrakesh. The research leading to these results has received funding from the European Research Council (ERC) under the FP/2007-2013 ERC grant agreement no. 336480, and under the H2020 ERC grant agreement no. 679030; and from an Actions de Recherche Concertee (ARC) grant, financed by the Wallonia-Brussels Federation. The VLT data used in this work were taken under program 296.C-5010(A). UKIRT is supported by NASA and operated under an agreement among the University of Hawaii, the University of Arizona, and Lockheed Martin Advanced Technology Center; operations are enabled through the cooperation of the East Asian Observatory. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University (JMU) in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, with financial support from the UK Science and Technology Facilities Council. This paper uses observations made at the South African Astronomical Observatory (SAAO). M.G., E.J. and V.V.G. are F.R.S.-FNRS research associates. B.-O.D. acknowledges support from the Swiss National Science Foundation in the form of a SNSF Professorship (PP00P2_163967). E.A. acknowledges support from National Science Foundation (NSF) grant AST-1615315, and NASA grants NNX13AF62G and NNH05ZDA001C. E.B. acknowledges that this work is part of the F.R.S.-FNRS ExtraOrDynHa research project and acknowledges funding by the European Research Council through ERC grant SPIRE 647383. S.N.R. thanks the Agence Nationale pour la Recherche (ANR) for support via grant ANR-13-BS05-0003-002 (project MOJO). D.L.H. acknowledges financial support from the UK Science and Technology Facilities Council. The authors thank C. Owen, C. Wolf and the rest of the SkyMapper team for their attempts to monitor the star from Australia; from UKIRT, the director R. Green and the staff scientists W. Varricatt and T. Kerr; the ESO staff at Paranal for their support with the HAWK-I observations; JMU and their flexibility as regards the Liverpool Telescope schedule, which allowed us to search actively for the planets, and to extend our time allocation in the face of amazing results; for the William Herschel Telescope, C. Farina, F. Riddick, F. Jimenez and O. Vaduvescu for their help and kindness during observations; and for SAAO, the telescopes operations manager R. Sefako for his support. NR 58 TC 3 Z9 3 U1 3 U2 3 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD FEB 23 PY 2017 VL 542 IS 7642 BP 456 EP + DI 10.1038/nature21360 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EM1RG UT WOS:000395094100031 PM 28230125 ER PT J AU Myhre, G Aas, W Cherian, R Collins, W Faluvegi, G Flanner, M Forster, P Hodnebrog, O Klimont, Z Lund, MT Mulmenstadt, J Myhre, CL Olivie, D Prather, M Quaas, J Samset, BH Schnell, JL Schulz, M Shindell, D Skeie, RB Takemura, T Tsyro, S AF Myhre, Gunnar Aas, Wenche Cherian, Ribu Collins, William Faluvegi, Greg Flanner, Mark Forster, Piers Hodnebrog, Oivind Klimont, Zbigniew Lund, Marianne T. Muelmenstaedt, Johannes Myhre, Cathrine Lund Olivie, Dirk Prather, Michael Quaas, Johannes Samset, Bjorn H. Schnell, Jordan L. Schulz, Michael Shindell, Drew Skeie, Ragnhild B. Takemura, Toshihiko Tsyro, Svetlana TI Multi-model simulations of aerosol and ozone radiative forcing due to anthropogenic emission changes during the period 1990-2015 SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID FUTURE CLIMATE SIMULATIONS; EARTH SYSTEM MODEL; BLACK CARBON; ATMOSPHERIC CHEMISTRY; TEMPERATURE TRENDS; SURFACE OZONE; SENSITIVITY; IMPACTS; REPRESENTATION; IMPROVEMENTS AB Over the past few decades, the geographical distribution of emissions of substances that alter the atmospheric energy balance has changed due to economic growth and air pollution regulations. Here, we show the resulting changes to aerosol and ozone abundances and their radiative forcing using recently updated emission data for the period 1990-2015, as simulated by seven global atmospheric composition models. The models broadly reproduce large-scale changes in surface aerosol and ozone based on observations (e.g. -1 to -3% yr(-1) in aerosols over the USA and Europe). The global mean radiative forcing due to ozone and aerosol changes over the 1990-2015 period increased by +0.17 +/- 0.08 W m(-2), with approximately one-third due to ozone. This increase is more strongly positive than that reported in IPCC AR5. The main reasons for the increased positive radiative forcing of aerosols over this period are the substantial reduction of global mean SO2 emissions, which is stronger in the new emission inventory compared to that used in the IPCC analysis, and higher black carbon emissions. C1 [Myhre, Gunnar; Hodnebrog, Oivind; Lund, Marianne T.; Samset, Bjorn H.; Skeie, Ragnhild B.] CICERO, Oslo, Norway. [Aas, Wenche; Myhre, Cathrine Lund] NILU Norwegian Inst Air Res, Kjeller, Norway. [Cherian, Ribu; Muelmenstaedt, Johannes; Quaas, Johannes] Univ Leipzig, Inst Meteorol, Leipzig, Germany. [Collins, William] Univ Reading, Dept Meteorol, Reading, Berks, England. [Faluvegi, Greg] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Faluvegi, Greg] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Flanner, Mark] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA. [Forster, Piers] Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England. [Klimont, Zbigniew] IIASA, Laxenburg, Austria. [Olivie, Dirk; Schulz, Michael; Tsyro, Svetlana] Norwegian Meteorol Inst, Oslo, Norway. [Prather, Michael; Schnell, Jordan L.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Shindell, Drew] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. [Takemura, Toshihiko] Kyushu Univ, Res Inst Appl Mech, Fukuoka, Japan. RP Myhre, G (reprint author), CICERO, Oslo, Norway. EM gunnar.myhre@cicero.oslo.no FU Norwegian research council [229796]; European Union [282688]; National Science Foundation [DGE-1321846]; US Environmental Protection Agency; National Park Service FX This study benefitted from the Norwegian research council projects #229796 (AeroCom-P3) and the European Union Seventh Framework Programme (FP7/2007-2013) project # 282688. Jordan L. Schnell was supported by the National Science Foundation's Graduate Research Fellowship Program (DGE-1321846). We would like to express our thanks those who are involved in the EMEP and IMPROVE monitoring efforts and have contributed through operating sites, performing chemical analysis and by submissions of data. EMEP are funded through national contributions. US Environmental Protection Agency is the primary funding source of IMPROVE, with contracting and research support from the National Park Service. The Air Quality Group at the University of California, Davis is the central analytical laboratory. NR 61 TC 0 Z9 0 U1 1 U2 1 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 FEB 22 PY 2017 VL 17 IS 4 BP 2709 EP 2720 DI 10.5194/acp-17-2709-2017 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EM1RP UT WOS:000395095000002 ER PT J AU Williamson, HR Sehanobish, E Shiller, AM Sanchez-Amat, A Davidson, VL AF Williamson, Heather R. Sehanobish, Esha Shiller, Alan M. Sanchez-Amat, Antonio Davidson, Victor L. TI Roles of Copper and a Conserved Aspartic Acid in the Autocatalytic Hydroxylation of a Specific Tryptophan Residue during Cysteine Tryptophylquinone Biogenesis SO BIOCHEMISTRY LA English DT Article ID LYSINE-EPSILON-OXIDASE; CONTAINING AMINE OXIDASE; METHYLAMINE DEHYDROGENASE; MARINOMONAS-MEDITERRANEA; ACTIVE-SITE; COFACTOR BIOGENESIS; QUINONE COFACTOR; GLYCINE OXIDASE; REDOX COFACTOR; LYSYL OXIDASE AB The first posttranslational modification step in the biosynthesis of the tryptophan-derived quinone cofactors is the autocatalytic hydroxylation of a specific Trp residue at position C-7 on the indole side chain. Subsequent modifications are catalyzed by modifying enzymes, but the mechanism by which this first step occurs is unknown. LodA possesses a cysteine tryptophylquinone (CTQ) cofactor. Metal analysis as well as spectroscopic and kinetic studies of the mature and precursor forms of a D512A LodA variant provides evidence that copper is required for the initial hydroxylation of the precursor protein and that if alternative metals are bound, the modification does not occur and the precursor is unstable. It is shown that the mature native LodA also contains loosely bound copper, which affects the visible absorbance spectrum and quenches the fluorescence spectrum that is attributed to the mature CTQ cofactor. When copper is removed, the fluorescence appears, and when it is added back to the protein, the fluorescence is quenched, indicating that copper reversibly binds in the proximity of CTQ, Removal of copper does not diminish the enzymatic activity of LodA. This distinguishes LodA from enzymes with protein-derived tyrosylquinone cofactors in which copper is present near the cofactor and is absolutely required for activity. Mechanisms are proposed for the role of copper in the hydroxylation of the unactivated Trp side chain. These results demonstrate that the reason that the highly conserved Asp512 is critical for LodA, and possibly all tryptophylquinone enzymes, is not because it is required for catalysis but because it is necessary for CTQ biosynthesis, more specifically to facilitate the initial copper-dependent hydroxylation of a specific Trp residue. C1 [Williamson, Heather R.; Sehanobish, Esha; Davidson, Victor L.] Univ Cent Florida, Coll Med, Burnett Sch Biomed Sci, 6900 Lake Nona Blvd, Orlando, FL 32827 USA. [Shiller, Alan M.] Univ Southern Mississippi, Stennis Space Ctr, Div Marine Sci, Hattiesburg, MS 39529 USA. [Sanchez-Amat, Antonio] Univ Murcia, Dept Genet & Microbiol, E-30100 Murcia, Spain. [Williamson, Heather R.] Xavier Univ Louisiana, Dept Chem, 1 Drexel Dr, New Orleans, LA 70125 USA. RP Davidson, VL (reprint author), Univ Cent Florida, Coll Med, Burnett Sch Biomed Sci, 6900 Lake Nona Blvd, Orlando, FL 32827 USA. EM victor.davidson@ucf.du FU National Institute of General Medical Sciences of the National Institutes of Health [R37GM41574] FX This research was supported by the National Institute of General Medical Sciences of the National Institutes of Health via Grant R37GM41574 (V.L.D.). NR 44 TC 0 Z9 0 U1 1 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0006-2960 J9 BIOCHEMISTRY-US JI Biochemistry PD FEB 21 PY 2017 VL 56 IS 7 BP 997 EP 1004 DI 10.1021/acs.biochem.6b01137 PG 8 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA EL6IL UT WOS:000394725300010 PM 28140566 ER PT J AU Zhang, S Eckart, ME Jaeckel, FT Kripps, KL McCammon, D Morgan, KM Zhou, Y AF Zhang, Shuo Eckart, Megan E. Jaeckel, Felix T. Kripps, Kari L. McCammon, Dan Morgan, Kelsey M. Zhou, Yu TI Mapping of the resistance of a superconducting transition edge sensor as a function of temperature, current, and applied magnetic field SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID IMPEDANCE MEASUREMENTS AB We have measured the resistance R(T, I, B-ext) of a superconducting transition edge sensor over the entire transition region on a fine scale, producing a four-dimensional map of the resistance surface. The dimensionless temperature and current sensitivities (alpha partial derivative log R/partial derivative log T|(I) and beta partial derivative log R/partial derivative log I|(T)) of the TES resistance have been determined at each point. alpha and beta are closely related to the sensor performance, but show a great deal of complex, large amplitude fine structure over large portions of the surface that is sensitive to the applied magnetic field. We discuss the relation of this structure to the presence of Josephson "weak link" fringes. Published by AIP Publishing. C1 [Zhang, Shuo; Jaeckel, Felix T.; Kripps, Kari L.; McCammon, Dan; Morgan, Kelsey M.; Zhou, Yu] Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA. [Eckart, Megan E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Morgan, Kelsey M.] Natl Inst Stand & Technol, Boulder, CO 80305 USA. RP Zhang, S (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA. OI Morgan, Kelsey/0000-0002-6597-1030; McCammon, Dan/0000-0001-5170-4567 FU NASA [NNX13AH21G] FX James Chervenak, Edward Wassell, Jennette Mateo, and Caroline Kilbourne were instrumental in the design and construction of the devices tested here. We thank two anonymous referees for their careful reading and many suggestions that have greatly improved the paper. We acknowledge the support of NASA Grant No. NNX13AH21G. NR 20 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-8979 EI 1089-7550 J9 J APPL PHYS JI J. Appl. Phys. PD FEB 21 PY 2017 VL 121 IS 7 AR 074503 DI 10.1063/1.4976562 PG 6 WC Physics, Applied SC Physics GA EM4LE UT WOS:000395283700015 ER PT J AU Rovituso, M Schuy, C Weber, U Brons, S Cortes-Giraldo, MA La Tessa, C Piasetzky, E Izraeli, D Schardt, D Toppi, M Scifoni, E Kramer, M Durante, M AF Rovituso, M. Schuy, C. Weber, U. Brons, S. Cortes-Giraldo, M. A. La Tessa, C. Piasetzky, E. Izraeli, D. Schardt, D. Toppi, M. Scifoni, E. Kraemer, M. Durante, M. TI Fragmentation of 120 and 200 MeV u(-1) He-4 ions in water and PMMA targets SO PHYSICS IN MEDICINE AND BIOLOGY LA English DT Article DE particle therapy; helium ions; nuclear fragmentation ID REACTION CROSS-SECTIONS; PARTICLE THERAPY; ALPHA-PARTICLES; BEAM THERAPY; HELIUM-IONS; HIGH-ENERGY; C-12; CHARGE; OPTIMIZATION; RADIOTHERAPY AB Recently, the use of He-4 particles in cancer radiotherapy has been reconsidered as they potentially represent a good compromise between protons and C-12 ions. The first step to achieve this goal is the development of a dedicated treatment planning system, for which basic physics information such as the characterization of the beam lateral scattering and fragmentation cross sections are required. In the present work, the attenuation of 4He primary particles and the build-up of secondary charged fragments at various depths in water and polymethyl methacrylate were investigated experimentally for 120 and 200 MeV u(-1) beams delivered by the synchrotron at the Heidelberg Ion-Beam Therapy Center, Heidelberg. Species and isotope identification was accomplished combining energy loss and time-of-flight measurements. Differential yields and energy spectra of all fragments types were recorded between 0 degrees and 20 degrees with respect to the primary beam direction. C1 [Rovituso, M.; Schuy, C.; Weber, U.; Schardt, D.; Scifoni, E.; Kraemer, M.; Durante, M.] GSI Helmholtzzentrum Schwerionenforsch, Darmstadt, Germany. [Brons, S.] Heidelberger Ionenstrahl Therapiezentrum, Heidelberg, Germany. [Cortes-Giraldo, M. A.] Univ Seville, Seville, Spain. [La Tessa, C.] NASA, Space Radiat Lab, Brookhaven Natl Lab, Upton, NY USA. [Piasetzky, E.; Izraeli, D.] Tel Aviv Univ, IL-69978 Tel Aviv, Israel. [Toppi, M.] Ist Nazl Fis Nucl, Lab Nazl Frascati, Frascati, Italy. [Scifoni, E.; Durante, M.] INFN Trento, TIFPA, Povo, TN, Italy. RP Durante, M (reprint author), GSI Helmholtzzentrum Schwerionenforsch, Darmstadt, Germany.; Durante, M (reprint author), INFN Trento, TIFPA, Povo, TN, Italy. EM marco.durante@tifpa.infn.it NR 38 TC 0 Z9 0 U1 4 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0031-9155 EI 1361-6560 J9 PHYS MED BIOL JI Phys. Med. Biol. PD FEB 21 PY 2017 VL 62 IS 4 BP 1310 EP 1326 DI 10.1088/1361-6560/aa5302 PG 17 WC Engineering, Biomedical; Radiology, Nuclear Medicine & Medical Imaging SC Engineering; Radiology, Nuclear Medicine & Medical Imaging GA EL4KM UT WOS:000394590100006 PM 28114125 ER PT J AU Sun, K Tao, L Miller, DJ Pan, D Golston, LM Zondlo, MA Griffin, RJ Wallace, HW Leong, YJ Yang, MM Zhang, Y Mauzerall, DL Zhu, T AF Sun, Kang Tao, Lei Miller, David J. Pan, Da Golston, Levi M. Zondlo, Mark A. Griffin, Robert J. Wallace, H. W. Leong, Yu Jun Yang, M. Melissa Zhang, Yan Mauzerall, Denise L. Zhu, Tong TI Vehicle Emissions as an Important Urban Ammonia Source in the United States and China SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID ON-ROAD MEASUREMENTS; HIGH-RESOLUTION; ATMOSPHERIC AMMONIA; PARTICULATE MATTER; CATALYTIC-REDUCTION; EXHAUST EMISSIONS; DIURNAL-VARIATION; DUTY VEHICLES; DIODE-LASER; NH3 AB Ammoniated aerosols are important for urban air quality, but emissions of the key precursor NH3 are not well quantified. Mobile laboratory observations are used to characterize fleet-integrated NH3 emissions in six cities in the U.S. and China. Vehicle NH3:CO2 emission ratios in the U.S. are similar between cities (0.33-0.40 ppbv/ppmv, 15% uncertainty) despite differences in fleet composition, climate, and fuel composition. While Beijing, China has a comparable emission ratio (0.36 ppbv/ppmv) to the U.S. cities, less developed Chinese cities show higher emission ratios (0.44 and 0.55 ppbv/ppmv). If the vehicle CO, inventories are accurate, NH3 emissions from U.S. vehicles (0.26 +/- 0.07 Tg/yr) are more than twice those of the National Emission Inventory (0.12 Tg/yr), while Chinese NH3 vehicle emissions (0.09 +/- 0.02 Tg/yr) are similar to a bottom-up inventory. Vehicle NH3 emissions are greater than agricultural emissions in counties containing near half of the U.S. population and require reconsideration in urban air quality models due to their colocation with other aerosol precursors and the uncertainties regarding NH3 losses from upwind agricultural sources. Ammonia emissions in developing cities are especially important because of their high emission ratios and rapid motorizations. C1 [Sun, Kang; Tao, Lei; Miller, David J.; Pan, Da; Golston, Levi M.; Zondlo, Mark A.; Mauzerall, Denise L.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. [Sun, Kang; Tao, Lei; Miller, David J.; Pan, Da; Golston, Levi M.; Zondlo, Mark A.] NSF ERC, Ctr Midinfrared Technol Hlth & Environm, Princeton, NJ 08544 USA. [Griffin, Robert J.; Wallace, H. W.; Leong, Yu Jun] Rice Univ, Dept Civil & Environm Engn, Houston, TX 77005 USA. [Yang, M. Melissa] NASA, Langley Res Ctr, Chem & Dynam Branch, Hampton, VA 23681 USA. [Zhang, Yan] Nanjing P&Y Environm Technol Co Ltd, Nanjing 210014, Jiangsu, Peoples R China. [Mauzerall, Denise L.] Princeton Univ, Woodrow Wilson Sch Publ & Int Affairs, Princeton, NJ 08544 USA. [Zhu, Tong] Peking Univ, Coll Environm Sci & Engn, State Key Lab Environm Simulat & Pollut Control, Beijing 100871, Peoples R China. [Sun, Kang] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tao, Lei] NEC Labs Amer, Princeton, NJ 08540 USA. [Miller, David J.] Brown Univ, Inst Brown Environm & Soc, Providence, RI 02912 USA. RP Zondlo, MA (reprint author), Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.; Zondlo, MA (reprint author), NSF ERC, Ctr Midinfrared Technol Hlth & Environm, Princeton, NJ 08544 USA. EM mzondlo@princeton.edu RI ZHU, TONG/H-6501-2011 FU National Natural Science Foundation Committee of China [21190051, 41121004, 41421064]; Council for International Teaching and Research at Princeton University; Fung Global Forum; National Geographic Air and Water Conservation Fund [GEFC16-13]; NSF-ERC MIRTHE [EEC-0540832]; NASA [NNX14AT36G, NNX14AT32G]; NASA Earth and Space Science Fellowship [NN12AN64H]; TCEQ Air Quality Research Program; Houston Endowment FX We acknowledge the DISCOVER-AQ science team and CAREBeijing/NCP science team (funded by the National Natural Science Foundation Committee of China, 21190051, 41121004, 41421064). The field work was supported by the Council for International Teaching and Research at Princeton University with funds from the Fung Global Forum, the National Geographic Air and Water Conservation Fund (GEFC16-13), NSF-ERC MIRTHE (EEC-0540832), NASA grants NNX14AT36G and NNX14AT32G. K.S. acknowledges NASA Earth and Space Science Fellowship (NN12AN64H). Special thanks to the support and helpful discussions with LICOR Environmental division and for providing a set of LICOR sensors. The Rice university authors acknowledge support of the TCEQ Air Quality Research Program and the Houston Endowment. NR 68 TC 0 Z9 0 U1 9 U2 9 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X EI 1520-5851 J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD FEB 21 PY 2017 VL 51 IS 4 BP 2472 EP 2481 DI 10.1021/acs.est.6b02805 PG 10 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA EL6ID UT WOS:000394724300065 PM 28140570 ER PT J AU Liu, YH Hesse, M Guo, F Daughton, W Li, H Cassak, PA Shay, MA AF Liu, Yi-Hsin Hesse, M. Guo, F. Daughton, W. Li, H. Cassak, P. A. Shay, M. A. TI Why does Steady-State Magnetic Reconnection have a Maximum Local Rate of Order 0.1? SO PHYSICAL REVIEW LETTERS LA English DT Article ID CURRENT SHEETS; SOLAR-FLARE; COLLISIONLESS; PLASMA; FIELDS AB Simulations suggest collisionless steady-state magnetic reconnection of Harris-type current sheets proceeds with a rate of order 0.1, independent of dissipation mechanism. We argue this long-standing puzzle is a result of constraints at the magnetohydrodynamic (MHD) scale. We predict the reconnection rate as a function of the opening angle made by the upstream magnetic fields, finding a maximum reconnection rate close to 0.2. The predictions compare favorably to particle-in-cell simulations of relativistic electron-positron and nonrelativistic electron-proton reconnection. The fact that simulated reconnection rates are close to the predicted maximum suggests reconnection proceeds near the most efficient state allowed at the MHD scale. The rate near the maximum is relatively insensitive to the opening angle, potentially explaining why reconnection has a similar fast rate in differing models. C1 [Liu, Yi-Hsin; Hesse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Guo, F.; Daughton, W.; Li, H.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Cassak, P. A.] West Virginia Univ, Morgantown, WV 26506 USA. [Shay, M. A.] Univ Delaware, Newark, DE 19716 USA. RP Liu, YH (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. FU NASA's MMS mission; NASA [NNH16AC601, NNX16AG75G, NNX16AG76G]; DOE through the LDRD program at LANL; DOE/OFES; CMSO; NSF [AGS-0953463, AGS-1460037, AGS-1219382] FX Y.-H. L. thanks M. Swisdak and J. C. Dorelli for helpful discussions, and P. Wu and I. Honkonen for sharing their simulation data. Y.-H. L. is supported by NASA Grant No. NNX16AG75G. M. H. acknowledges support by NASA's MMS mission. F. G. is supported by NASA Grant No. NNH16AC601. H. L. is supported by the DOE through the LDRD program at LANL and DOE/OFES support to LANL in collaboration with CMSO. P. A. C. acknowledges support from NSF Grants No. AGS-0953463 and No. AGS-1460037 and NASA Grants No. NNX16AF75G and No. NNX16AG76G. M. S. is supported by NSF Grant No. AGS-1219382. Simulations were performed with LANL institutional computing, NASA Advanced Supercomputing and NERSC Advanced Supercomputing. NR 63 TC 0 Z9 0 U1 1 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD FEB 21 PY 2017 VL 118 IS 8 AR 085101 DI 10.1103/PhysRevLett.118.085101 PG 6 WC Physics, Multidisciplinary SC Physics GA EL5NH UT WOS:000394667300012 ER PT J AU Ackermann, M Ajello, M Albert, A Baldini, L Ballet, J Barbiellini, G Bastieri, D Bellazzini, R Bissaldi, E Bloom, ED Bonino, R Bottacini, E Brandt, TJ Bregeon, J Bruel, P Buehler, R Cameron, RA Caputo, R Caragiulo, M Caraveo, PA Cavazzuti, E Cecchi, C Charles, E Chekhtman, A Chiaro, G Ciprini, S Costanza, F Cutini, S D'Ammando, F de Palma, F Desiante, R Digel, SW Di Lalla, N Di Mauro, M Di Venere, L Favuzzi, C Funk, S Fusco, P Gargano, F Giglietto, N Giordano, F Giroletti, M Glanzman, T Green, D Grenier, IA Guillemot, L Guiriec, S Hayashi, K Hou, X Johannesson, G Kamae, T Knodlseder, J Kong, AKH Kuss, M La Mura, G Larsson, S Latronico, L Li, J Longo, F Loparco, F Lubrano, P Maldera, S Malyshev, D Manfreda, A Martin, P Mazziotta, MN Michelson, PF Mirabal, N Mitthumsiri, W Mizuno, T Monzani, ME Morselli, A Moskalenko, IV Negro, M Nuss, E Ohsugi, T Omodei, N Orlando, E Ormes, JF Paneque, D Persic, M Pesce-Rollins, M Piron, F Porter, TA Principe, G Raino, S Rando, R Razzano, M Reimer, O Sanchez-Conde, M Sgro, C Simone, D Siskind, EJ Spada, F Spandre, G Spinelli, P Tanaka, K Tibaldo, L Torres, DF Troja, E Uchiyama, Y Wang, JC Wood, KS Wood, M Zaharijas, G Zhou, M AF Ackermann, M. Ajello, M. Albert, A. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bellazzini, R. Bissaldi, E. Bloom, E. D. Bonino, R. Bottacini, E. Brandt, T. J. Bregeon, J. Bruel, P. Buehler, R. Cameron, R. A. Caputo, R. Caragiulo, M. Caraveo, P. A. Cavazzuti, E. Cecchi, C. Charles, E. Chekhtman, A. Chiaro, G. Ciprini, S. Costanza, F. Cutini, S. D'Ammando, F. de Palma, F. Desiante, R. Digel, S. W. Di Lalla, N. Di Mauro, M. Di Venere, L. Favuzzi, C. Funk, S. Fusco, P. Gargano, F. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Green, D. Grenier, I. A. Guillemot, L. Guiriec, S. Hayashi, K. Hou, X. Johannesson, G. Kamae, T. Knodlseder, J. Kong, A. K. H. Kuss, M. La Mura, G. Larsson, S. Latronico, L. Li, J. Longo, F. Loparco, F. Lubrano, P. Maldera, S. Malyshev, D. Manfreda, A. Martin, P. Mazziotta, M. N. Michelson, P. F. Mirabal, N. Mitthumsiri, W. Mizuno, T. Monzani, M. E. Morselli, A. Moskalenko, I. V. Negro, M. Nuss, E. Ohsugi, T. Omodei, N. Orlando, E. Ormes, J. F. Paneque, D. Persic, M. Pesce-Rollins, M. Piron, F. Porter, T. A. Principe, G. Raino, S. Rando, R. Razzano, M. Reimer, O. Sanchez-Conde, M. Sgro, C. Simone, D. Siskind, E. J. Spada, F. Spandre, G. Spinelli, P. Tanaka, K. Tibaldo, L. Torres, D. F. Troja, E. Uchiyama, Y. Wang, J. C. Wood, K. S. Wood, M. Zaharijas, G. Zhou, M. TI Observations of M31 and M33 with the Fermi Large Area Telescope: A Galactic Center Excess in Andromeda? SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; gamma rays: galaxies; Local Group ID LARGE-MAGELLANIC-CLOUD; STAR-FORMING GALAXIES; GAMMA-RAY EMISSION; LOCAL GROUP GALAXIES; HERSCHEL EXPLOITATION; GLOBULAR-CLUSTERS; STELLAR MASS; DARK-MATTER; COSMIC-RAYS; ATOMIC GAS AB The Fermi Large Area Telescope (LAT) has opened the way for comparative studies of cosmic rays (CRs) and high-energy objects in the Milky Way (MW) and in other, external, star-forming galaxies. Using 2 yr of observations with the Fermi LAT, Local Group galaxy M31 was detected as a marginally extended gamma-ray source, while only an upper limit has been derived for the other nearby galaxy M33. We revisited the gamma-ray emission in the direction of M31 and M33 using more than 7 yr of LAT Pass 8 data in the energy range 0.1-100 GeV, presenting detailed morphological and spectral analyses. M33 remains undetected, and we computed an upper limit of 2.0 x 10(-12) erg cm(-2) s(-1) on the 0.1-100 GeV energy flux (95% confidence level). This revised upper limit remains consistent with the observed correlation between gamma-ray luminosity and star formation rate tracers and implies an average CR density in M33 that is at most half of that of the MW. M31 is detected with a significance of nearly 10 sigma. Its spectrum is consistent with a power law with photon index Gamma = 2.4 +/- 0.1(stat) (vertical bar) (syst) and a 0.1-100 GeV energy flux of (5.6 +/- 0.6(stat vertical bar syst)) x 10(-12) erg cm(-1) s(-1). M31 is detected to be extended with a 4 sigma significance. The spatial distribution of the emission is consistent with a uniform-brightness disk with a radius of 0 degrees.4 and no offset from the center of the galaxy, but nonuniform intensity distributions cannot be excluded. The flux from M31 appears confined to the inner regions of the galaxy and does not fill the disk of the galaxy or extend far from it. The gamma-ray signal is not correlated with regions rich in gas or star formation activity, which suggests that the emission is not interstellar in origin, unless the energetic particles radiating in gamma rays do not originate in recent star formation. Alternative and nonexclusive interpretations are that the emission results from a population of millisecond pulsars dispersed in the bulge and disk of M31 by disrupted globular clusters or from the decay or annihilation of dark matter particles, similar to what has been proposed to account for the so-called Galactic center excess found in Fermi-LAT observations of the MW. C1 [Ackermann, M.; Buehler, R.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA. [Albert, A.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Baldini, L.; Di Lalla, N.; Manfreda, A.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.; Di Lalla, N.; Manfreda, A.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Grenier, I. A.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.; Persic, M.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Chiaro, G.; La Mura, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bellazzini, R.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spada, F.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Bissaldi, E.; Caragiulo, M.; Costanza, F.; de Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Simone, D.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bloom, E. D.; Bottacini, E.; Cameron, R. A.; Charles, E.; Digel, S. W.; Di Mauro, M.; Glanzman, T.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Porter, T. A.; Reimer, O.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Bloom, E. D.; Bottacini, E.; Cameron, R. A.; Charles, E.; Digel, S. W.; Di Mauro, M.; Glanzman, T.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Porter, T. A.; Reimer, O.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Bonino, R.; Desiante, R.; Latronico, L.; Maldera, S.; Negro, M.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Bonino, R.; Negro, M.] Univ Turin, Dipartimento Fis, I-10125 Turin, Italy. [Brandt, T. J.; Green, D.; Guiriec, S.; Mirabal, N.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bregeon, J.; Nuss, E.; Piron, F.] Univ Montpellier, CNRS, IN2P3, Lab Univers & Particules Montpellier, F-34095 Montpellier, France. [Bruel, P.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Caputo, R.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Caputo, R.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Caragiulo, M.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Caragiulo, M.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm Milano, Via E Bassini 15, I-20133 Milan, Italy. [Cavazzuti, E.; Ciprini, S.; Cutini, S.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00133 Rome, Italy. [Cecchi, C.; Ciprini, S.; Cutini, S.; Lubrano, P.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Cecchi, C.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Chekhtman, A.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [D'Ammando, F.; Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [de Palma, F.] Univ Telemat Pegaso, Piazza Trieste & Trento 48, I-80132 Naples, Italy. [Desiante, R.] Univ Udine, I-33100 Udine, Italy. [Funk, S.; Malyshev, D.; Principe, G.] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany. [Green, D.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Green, D.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Guillemot, L.] Univ Orleans, Lab Phys & Chim Environm & Espace, CNRS, F-45071 Orleans 02, France. [Guillemot, L.] CNRS, INSU, Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France. [Hayashi, K.] Nagoya Univ, Dept Phys & Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Hou, X.; Wang, J. C.; Zhou, M.] Chinese Acad Sci, Yunnan Observ, 396 Yangfangwang, Kunming 650216, Peoples R China. [Hou, X.; Kong, A. K. H.] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. [Hou, X.; Kong, A. K. H.] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. [Hou, X.; Wang, J. C.; Zhou, M.] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, 396 Yangfangwang, Kunming 650216, Peoples R China. [Hou, X.; Wang, J. C.; Zhou, M.] Chinese Acad Sci, Ctr Astron Mega Sci, 20A Datun Rd, Beijing 100012, Peoples R China. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Kamae, T.] Univ Tokyo, Grad Sch Sci, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. [Knodlseder, J.; Martin, P.] CNRS, IRAP, F-31028 Toulouse 4, France. [Knodlseder, J.; Martin, P.] Univ Toulouse, UPS OMP, IRAP, F-31400 Toulouse, France. [Larsson, S.] KTH Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Larsson, S.; Sanchez-Conde, M.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Li, J.; Torres, D. F.] Inst Space Sci IEEC CSIC, Campus UAB,Carrer Magrans S-N, E-08193 Barcelona, Spain. [Mitthumsiri, W.] Mahidol Univ, Dept Phys, Fac Sci, Bangkok 10400, Thailand. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Persic, M.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Sanchez-Conde, M.] Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Tanaka, K.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Tibaldo, L.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Torres, D. F.] ICREA, E-08010 Barcelona, Spain. [Uchiyama, Y.] Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan. [Wood, K. S.] Praxis Inc, Alexandria, VA 22303 USA. [Zaharijas, G.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Zaharijas, G.] Univ Trieste, I-34127 Trieste, Italy. [Zaharijas, G.] Univ Nova Gorica, Lab Astroparticle Phys, Vipavska 13, SI-5000 Nova Gorica, Slovenia. [Chekhtman, A.; Wood, K. S.] Naval Res Lab, Washington, DC 20375 USA. RP Hou, X (reprint author), Chinese Acad Sci, Yunnan Observ, 396 Yangfangwang, Kunming 650216, Peoples R China.; Hou, X (reprint author), Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan.; Hou, X (reprint author), Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan.; Hou, X (reprint author), Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, 396 Yangfangwang, Kunming 650216, Peoples R China.; Hou, X (reprint author), Chinese Acad Sci, Ctr Astron Mega Sci, 20A Datun Rd, Beijing 100012, Peoples R China. EM xianhou.astro@gmail.com; pierrick.martin@irap.omp.eu OI Ajello, Marco/0000-0002-6584-1703 FU National Aeronautics and Space Administration; Department of Energy in the United States; Commissariat a l'Energie Atomique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan; K. A. Wallenberg Foundation; Swedish Research Council; Swedish National Space Board in Sweden; National Natural Science Foundation of China [11503078, 11573060]; Ministry of Science and Technology of the Republic of China (Taiwan) [104-2811-M-007-059, 103-2628-M-007-003-MY3] FX The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT, as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States; the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy; the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK), and Japan Aerospace Exploration Agency (JAXA) in Japan; and the K. A. Wallenberg Foundation, the Swedish Research Council, and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France.; X.H. is supported by the National Natural Science Foundation of China through grant 11503078 and by the Ministry of Science and Technology of the Republic of China (Taiwan) through grant 104-2811-M-007-059. A.K. H.K. is supported by the Ministry of Science and Technology of the Republic of China (Taiwan) through grant 103-2628-M-007-003-MY3. J.C.W. and M.Z. are supported by the National Natural Science Foundation of China through grant 11573060. NR 51 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 FEB 20 PY 2017 VL 836 IS 2 AR 208 DI 10.3847/1538-4357/aa5c3d PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN2WL UT WOS:000395870900001 ER PT J AU Annuar, A Alexander, DM Gandhi, P Lansbury, GB Asmus, D Ballantyne, DR Bauer, FE Boggs, SE Boorman, PG Brandt, WN Brightman, M Christensen, FE Craig, WW Farrah, D Goulding, AD Hailey, CJ Harrison, FA Koss, MJ LaMassa, SM Murray, SS Ricci, C Rosario, DJ Stanley, F Stern, D Zhang, W AF Annuar, A. Alexander, D. M. Gandhi, P. Lansbury, G. B. Asmus, D. Ballantyne, D. R. Bauer, F. E. Boggs, S. E. Boorman, P. G. Brandt, W. N. Brightman, M. Christensen, F. E. Craig, W. W. Farrah, D. Goulding, A. D. Hailey, C. J. Harrison, F. A. Koss, M. J. LaMassa, S. M. Murray, S. S. Ricci, C. Rosario, D. J. Stanley, F. Stern, D. Zhang, W. TI A New Compton-thick AGN in Our Cosmic Backyard: Unveiling the Buried Nucleus in NGC 1448 with NuSTAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: nuclei; techniques: spectroscopic; X-rays: galaxies; X-rays: individual (NGC 1448) ID ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; X-RAY-EMISSION; SUBARCSECOND MIDINFRARED VIEW; SUPERMASSIVE BLACK-HOLES; SWIFT-BAT SURVEY; POPULATION SYNTHESIS; NEARBY GALAXIES; COMPLETE CENSUS; HOST GALAXIES AB NGC 1448 is one of the nearest luminous galaxies (L-8-1000(mu m) > 10(9) L-circle dot) to ours (z = 0.00390), and yet the active galactic nucleus (AGN) it hosts was only recently discovered, in 2009. In this paper, we present an analysis of the nuclear source across three wavebands: mid-infrared (MIR) continuum, optical, and X-rays. We observed the source with the Nuclear Spectroscopic Telescope Array (N(u)STAR), and combined these data with archival Chandra data to perform broadband X-ray spectral fitting (approximate to 0.5-40 keV) of the AGN for the first time. Our X-ray spectral analysis reveals that the AGN is buried under a Compton-thick (CT) column of obscuring gas along our line of sight, with a column density of N-H(los)greater than or similar to 2.5 x 10(24) cm(-2). The best-fitting torus models measured an intrinsic 2-10 keV luminosity of L-2-10, int = (3.5-7.6). x. 10(40)erg s(-1), making NGC 1448 one of the lowest luminosity CTAGNs known. In addition to the NuSTAR observation, we also performed optical spectroscopy for the nucleus in this edge-on galaxy using the European Southern Observatory New Technology Telescope. We reclassify the optical nuclear spectrum as a Seyfert on the basis of the Baldwin-Philips-Terlevich diagnostic diagrams, thus identifying the AGN at optical wavelengths for the first time. We also present high spatial resolution MIR observations of NGC 1448 with Gemini/T-ReCS, in which a compact nucleus is clearly detected. The absorption-corrected 2-10 keV luminosity measured from our X-ray spectral analysis agrees with that predicted from the optical [O III]lambda 5007 angstrom emission line and the MIR 12 mu m. continuum, further supporting the CT nature of the AGN. C1 [Annuar, A.; Alexander, D. M.; Lansbury, G. B.; Rosario, D. J.; Stanley, F.] Univ Durham, Ctr Extragalact Astron, Dept Phys, South Rd, Durham DH1 3LE, England. [Gandhi, P.; Boorman, P. G.] Univ Southampton, Dept Phys & Astron, Fac Phys Sci & Engn, Southampton SO17 1BJ, Hants, England. [Asmus, D.] European Southern Observ, Casilla 19001, Santiago, Chile. [Ballantyne, D. R.] Georgia Inst Technol, Ctr Relativist Astrophys, Sch Phys, Atlanta, GA 30332 USA. [Bauer, F. E.; Ricci, C.] Pontificia Univ Catolica Chile, Inst Astrofis, Casilla 306, Santiago 22, Chile. [Bauer, F. E.; Ricci, C.] Pontificia Univ Catolica Chile, Centro Astroingn, Fac Fis, Casilla 306, Santiago 22, Chile. [Bauer, F. E.] Millennium Inst Astrophys MAS, Nuncio Monsenor Sotero Sanz 100, Santiago, Chile. [Bauer, F. E.] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA. [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Dept Phys, 525 Davey Lab, University Pk, PA 16802 USA. [Brightman, M.; Harrison, F. A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Christensen, F. E.] Tech Univ Denmark, DTU Space, Natl Space Inst3, Elektrovej 327, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Goulding, A. D.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Koss, M. J.] Swiss Fed Inst Technol, Inst Astron, Dept Phys, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. [LaMassa, S. M.; Stern, D.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Murray, S. S.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Murray, S. S.] Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA. [Ricci, C.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Stanley, F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Annuar, A (reprint author), Univ Durham, Ctr Extragalact Astron, Dept Phys, South Rd, Durham DH1 3LE, England. OI Ballantyne, David/0000-0001-8128-6976; Lansbury, George/0000-0002-5328-9827 FU Majlis Amanah Rakyat (MARA) Malaysia; Science and Technology Facilities Council (STFC) [ST/L00075X/1, ST/J003697/1, ST/K501979/1]; CONICYT-Chile [Basal-CATA PFB-06/2007]; Ministry of Economy, Development, and Tourism's Millennium Science [IC120009]; Millennium Institute of Astrophysics, MAS; STFC; NASA Postdoctoral Program at the NASA Goddard Space Flight Center; Swiss National Science Foundation; Ambizione fellowship [PZ00P2_154799/1]; National Aeronautics and Space Administration (NASA); FONDECYT [1141218]; China-CONICYT FX We thank the anonymous referee for useful comments which have helped to improve the paper. We acknowledge financial support from Majlis Amanah Rakyat (MARA) Malaysia (A.A.), the Science and Technology Facilities Council (STFC) grant ST/L00075X/1 (D.M.A.), ST/J003697/1 (P.G.), and ST/K501979/1 (G.B.L.). F.E.B. acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT Regular 1141218, "EMBIGGEN" Anillo ACT1101), and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. P.B. would like to thank the STFC for funding. S.M.L. 's research was supported by an appointment to the NASA Postdoctoral Program at the NASA Goddard Space Flight Center, administered by the Universities Space Research Association under contract with NASA. M.K. acknowledges support from the Swiss National Science Foundation and Ambizione fellowship grant PZ00P2_154799/1. We acknowledge financial support from the CONICYT-Chile grants "EMBIGGEN" Anillo ACT1101 (C.R.), FONDECYT 1141218 (C.R.), BasalCATA PFB-06/2007 (C.R.) and from the China-CONICYT fund (C.R.). NuSTAR is a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL), and funded by the National Aeronautics and Space Administration (NASA). We thank the NuSTAR Operations, Software and Calibrations teams for support with 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 also made use of the data obtained through the High Energy Astrophysics Science Archive Research Center (HEASARC) Online Service, provided by the NASA/Goddard Space Flight Center, and the NASA/IPAC extragalactic Database (NED) operated by JPL, Caltech under contract with NASA. Facilities: Chandra, Gemini: South, NTT, NuSTAR. NR 75 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 FEB 20 PY 2017 VL 836 IS 2 AR 165 DI 10.3847/1538-4357/836/2/165 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN3OI UT WOS:000395917400006 ER PT J AU Dressing, CD Newton, ER Schlieder, JE Charbonneau, D Knutson, HA Vanderburg, A Sinukoff, E AF Dressing, Courtney D. Newton, Elisabeth R. Schlieder, Joshua E. Charbonneau, David Knutson, Heather A. Vanderburg, Andrew Sinukoff, Evan TI Characterizing K2 Candidate Planetary Systems Orbiting Low-mass Stars. I. Classifying Low-mass Host Stars Observed during Campaigns 1-7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: fundamental parameters; stars: fundamental parameters; stars: late-type; stars: low-mass; techniques: spectroscopic ID INFRARED TELESCOPE FACILITY; GIANT BRANCH STARS; TP-AGB MODELS; M DWARFS; SOLAR NEIGHBORHOOD; BAND SPECTRA; LIGHT CURVES; DATA RELEASE; COOL STARS; MILKY-WAY AB We present near-infrared spectra for 144 candidate planetary systems identified during Campaigns 1-7 of the NASA K2 Mission. The goal of the survey was to characterize planets orbiting low-mass stars, but our IRTF/SpeX and Palomar/TripleSpec spectroscopic observations revealed that 49% of our targets were actually giant stars or hotter dwarfs reddened by interstellar extinction. For the 72 stars with spectra consistent with classification as cool dwarfs (spectral types K3 - M4), we refined their stellar properties by applying empirical relations based on stars with interferometric radius measurements. Although our revised temperatures are generally consistent with those reported in the Ecliptic Plane Input Catalog (EPIC), our revised stellar radii are typically 0.13 R circle dot(39%) larger than the EPIC values, which were based on model isochrones that have been shown to underestimate the radii of cool dwarfs. Our improved stellar characterizations will enable more efficient prioritization of K2 targets for follow-up studies. C1 [Dressing, Courtney D.; Knutson, Heather A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Newton, Elisabeth R.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Schlieder, Joshua E.] CALTECH, IPAC NExScI, Pasadena, CA 91125 USA. [Charbonneau, David; Vanderburg, Andrew] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Schlieder, Joshua E.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sinukoff, Evan] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Sinukoff, Evan] CALTECH, Cahill Ctr Astrophys, 1216 East Calif Blvd, Pasadena, CA 91125 USA. RP Dressing, CD (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM dressing@caltech.edu OI Vanderburg, Andrew/0000-0001-7246-5438; Newton, Elisabeth/0000-0003-4150-841X FU NASA through the Sagan Fellowship; John Templeton Foundation; NASA Science Mission directorate; University of Hawaii [NNH14CK55B] FX This work was performed under contract with the Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed here are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. This paper includes data collected by the K2 mission, which is funded by the NASA Science Mission directorate. Our follow-up observations were obtained at the IRTF, which is operated by the University of Hawaii under contract NNH14CK55B with the National Aeronautics and Space Administration and at Palomar Observatory. We thank the staff at both observatories and the Caltech Remote Observing Facilities staff for supporting us during our many observing runs. We are grateful to the IRTF and Caltech TACs for awarding us telescope time. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. NR 65 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 FEB 20 PY 2017 VL 836 IS 2 AR 167 DI 10.3847/1538-4357/836/2/167 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN1HM UT WOS:000395761100001 ER PT J AU Fox, OD Van Dyk, SD Dwek, E Smith, N Filippenko, AV Andrews, J Arendt, RG Foley, RJ Kelly, PL Miller, AA Shivvers, I AF Fox, Ori D. Van Dyk, Schuyler D. Dwek, Eli Smith, Nathan Filippenko, Alexei V. Andrews, Jennifer Arendt, Richard G. Foley, Ryan J. Kelly, Patrick L. Miller, Adam A. Shivvers, Isaac TI The Candidate Progenitor of the Type IIn SN 2010jl Is Not an Optically Luminous Star SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; dust, extinction; infrared: stars; supernovae: general; supernovae: individual (SN 2010jl) ID MASSIVE STAR; ETA-CARINAE; SUPERNOVA; SPITZER; DUST; TRANSIENTS; 1961V; PHOTOMETRY; DIVERSITY; EVOLUTION AB A blue source in pre-explosion Hubble Space Telescope (HST)/Wide-Field Planetary Camera 2 (WFPC2) images falls within the 5 sigma. astrometric error circle (similar to 0.'' 24) derived from post-explosion ground-based imaging of SN 2010jl. At the time the ground-based astrometry was published, however, the SN had not faded sufficiently for post-explosion HST follow-up observations to determine a more precise astrometric solution and/or confirm if the pre-explosion source had disappeared, both of which are necessary to ultimately disentangle the possible progenitor scenarios. Here we present HST/WFC3 imaging of the SN 2010jl field obtained in 2014, 2015, and 2016 when the SN had faded sufficiently to allow for new constraints on the progenitor. The SN, which is still detected in the new images, is offset by 0.'' 061 +/- 0.'' 008 (15 +/- 2 pc) from the underlying and extended source of emission that contributes at least partially, if not entirely, to the blue source previously suggested as the candidate progenitor in the WFPC2 data. This point alone rules out the possibility that the blue source in the pre-explosion images is the exploding star, but may instead suggest an association with a young (< 5-6 Myr) cluster and still argues for a massive (> 30M(circle dot)) progenitor. We obtain new upper limits on the flux from a single star at the SN position in the pre-explosion WFPC2 and Spitzer/IRAC images that may ultimately be used to constrain the progenitor properties. C1 [Fox, Ori D.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Van Dyk, Schuyler D.] CALTECH, IPAC, Mailcode 100-22, Pasadena, CA 91125 USA. [Dwek, Eli] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Mail Code 665, Greenbelt, MD 20771 USA. [Smith, Nathan; Andrews, Jennifer] Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. [Filippenko, Alexei V.; Kelly, Patrick L.; Shivvers, Isaac] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Arendt, Richard G.] NASA, GSFC, CRESST, UMBC, GSFC Code 665, Greenbelt, MD 20771 USA. [Foley, Ryan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Foley, Ryan J.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Foley, Ryan J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. [Miller, Adam A.] Jet Prop Lab, 4800 Oak Grove Dr,MS 169-506, Pasadena, CA 91109 USA. [Miller, Adam A.] CALTECH, Pasadena, CA 91125 USA. RP Fox, OD (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM ofox@stsci.edu OI Van Dyk, Schuyler/0000-0001-9038-9950 FU NASA [NAS 5-26555, ADP13-0094]; NASA from STScI [GO-13341, GO-14149, GO-14668]; Christopher R. Redlich Fund; TABASGO Foundation; NSF [AST-1211916, AST-1518052]; Alfred P. Sloan Foundation FX This work is 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. It is also based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with NASA. Support was provided by NASA through grants GO-13341, GO-14149, and GO-14668 from STScI. A.V.F.'s group is also grateful for generous financial assistance from the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. Part of the research was carried out at JPL. E.D. acknowledges NASA's ADP13-0094 grant for support on this project. R.J.F. gratefully acknowledges support from NSF grant AST-1518052 and the Alfred P. Sloan Foundation. The authors would like to thank Christa Gall, Rubab Khan, Jon Mauerhan, and Arka Sarangi for their helpful discussions. We would especially like to thank the Spitzer Help Desk at IPAC for their useful support with the MOPEX tool. 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 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2017 VL 836 IS 2 AR 222 DI 10.3847/1538-4357/836/2/222 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN2WL UT WOS:000395870900015 ER PT J AU Hensley, BS Draine, BT AF Hensley, Brandon S. Draine, B. T. TI Modeling the Anomalous Microwave Emission with Spinning Nanoparticles: No PAHs Required SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; radiation mechanisms: general; radio continuum: ISM ID POLYCYCLIC AROMATIC-HYDROCARBONS; DIFFUSE INTERSTELLAR-MEDIUM; GRAIN-SIZE DISTRIBUTIONS; DUST EMISSION; INFRARED-EMISSION; TRANSLUCENT CLOUDS; GALACTIC EMISSION; MILKY-WAY; PLANCK; POLARIZATION AB In light of recent observational results indicating an apparent lack of correlation between the anomalous microwave emission (AME) and mid-infrared emission from polycyclic aromatic hydrocarbons, we assess whether rotational emission from spinning silicate and/or iron nanoparticles could account for the observed AME without violating observational constraints on interstellar abundances, ultraviolet extinction, and infrared emission. By modifying the SpDust code to compute the rotational emission from these grains, we find that nanosilicate grains could account for the entirety of the observed AME, whereas iron grains could be responsible for only a fraction, even for extreme assumptions on the amount of interstellar iron concentrated in ultrasmall iron nanoparticles. Given the added complexity of contributions from multiple grain populations to the total spinning dust emission, as well as existing uncertainties due to the poorly constrained grain size, charge, and dipole moment distributions, we discuss generic, carrier-independent predictions of spinning dust theory and observational tests that could help identify the AME carrier(s). C1 [Hensley, Brandon S.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Draine, B. T.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Hensley, BS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM brandon.s.hensley@jpl.nasa.gov FU NSF [AST-1408723]; National Aeronautics and Space Administration FX We thank the organizers and participants of the 2016 AME Workshop at ESTEC for many stimulating conversations that informed this work and the anonymous referee for helpful comments. B.T.D. acknowledges support from NSF grant AST-1408723. The 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. NR 69 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 FEB 20 PY 2017 VL 836 IS 2 AR 179 DI 10.3847/1538-4357/aa5c37 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN3PX UT WOS:000395921500005 ER PT J AU Hosseinzadeh, G Arcavi, I Valenti, S McCully, C Howell, DA Johansson, J Sollerman, J Pastorello, A Benetti, S Cao, Y Cenko, SB Clubb, KI Corsi, A Duggan, G Elias-Rosa, N Filippenko, AV Fox, OD Fremling, C Horesh, A Karamehmetoglu, E Kasliwal, M Marion, GH Ofek, E Sand, D Taddia, F Zheng, WK Fraser, M Gal-Yam, A Inserra, C Laher, R Masci, F Rebbapragada, U Smartt, S Smith, KW Sullivan, M Surace, J Wozniak, P AF Hosseinzadeh, Griffin Arcavi, Iair Valenti, Stefano McCully, Curtis Howell, D. Andrew Johansson, Joel Sollerman, Jesper Pastorello, Andrea Benetti, Stefano Cao, Yi Cenko, S. Bradley Clubb, Kelsey I. Corsi, Alessandra Duggan, Gina Elias-Rosa, Nancy Filippenko, Alexei V. Fox, Ori D. Fremling, Christoffer Horesh, Assaf Karamehmetoglu, Emir Kasliwal, Mansi Marion, G. H. Ofek, Eran Sand, David Taddia, Francesco Zheng, WeiKang Fraser, Morgan Gal-Yam, Avishay Inserra, Cosimo Laher, Russ Masci, Frank Rebbapragada, Umaa Smartt, Stephen Smith, Ken W. Sullivan, Mark Surace, Jason Wozniak, Przemek TI Type Ibn Supernovae Show Photometric Homogeneity and Spectral Diversity at Maximum Light SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general; supernovae: individual (PTF11rfh, PTF12ldy, iPTF14aki, SN 2015U, iPTF15ul, SN 2015G, iPTF15akq) ID RICH CIRCUMSTELLAR MEDIUM; WOLF-RAYET STAR; SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; CORE-COLLAPSE SUPERNOVAE; MASSIVE STAR; OPTICAL-SPECTRA; LOW-RESOLUTION; IA SUPERNOVAE; II SUPERNOVAE; DATA RELEASE AB Type Ibn supernovae (SNe) are a small yet intriguing class of explosions whose spectra are characterized by low-velocity helium emission lines with little to no evidence for hydrogen. The prevailing theory has been that these are the core-collapse explosions of very massive stars embedded in helium-rich circumstellar material (CSM). We report optical observations of six new SNe Ibn: PTF11rfh, PTF12ldy, iPTF14aki, iPTF15ul, SN 2015G, and iPTF15akq. This brings the sample size of such objects in the literature to 22. We also report new data, including a near-infrared spectrum, on the Type Ibn SN 2015U. In order to characterize the class as a whole, we analyze the photometric and spectroscopic properties of the full Type Ibn sample. We find that, despite the expectation that CSM interaction would generate a heterogeneous set of light curves, as seen in SNe IIn, most Type Ibn light curves are quite similar in shape, declining at rates around 0.1 mag day(-1) during the first month after maximum light, with a few significant exceptions. Early spectra of SNe Ibn come in at least two varieties, one that shows narrow P Cygni lines and another dominated by broader emission lines, both around maximum light, which may be an indication of differences in the state of the progenitor system at the time of explosion. Alternatively, the spectral diversity could arise from viewing-angle effects or merely from a lack of early spectroscopic coverage. Together, the relative light curve homogeneity and narrow spectral features suggest that the CSM consists of a spatially confined shell of helium surrounded by a less dense extended wind. C1 [Hosseinzadeh, Griffin; Arcavi, Iair; McCully, Curtis; Howell, D. Andrew] Las Cumbres Observ, 6740 Cortona Dr Ste 102, Goleta, CA 93117 USA. [Hosseinzadeh, Griffin; McCully, Curtis; Howell, D. Andrew] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Arcavi, Iair] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Valenti, Stefano] Univ Calif Davis, Dept Phys, 1 Shields Ave, Davis, CA 95616 USA. [Johansson, Joel; Ofek, Eran; Gal-Yam, Avishay] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Sollerman, Jesper; Fremling, Christoffer; Karamehmetoglu, Emir; Taddia, Francesco] Stockholm Univ, Dept Astron, Oskar Klein Ctr, Albanova Univ Ctr, SE-10691 Stockholm, Sweden. [Pastorello, Andrea; Benetti, Stefano; Elias-Rosa, Nancy] Osserv Astron Padova, INAF, Vicolo Osservatorio 5, I-35122 Padua, Italy. [Cao, Yi; Duggan, Gina; Horesh, Assaf; Kasliwal, Mansi] CALTECH, Cahill Ctr Astron & Astrophys, Mail Code 249-17, Pasadena, CA 91125 USA. [Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Mail Code 661, Greenbelt, MD 20771 USA. [Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Clubb, Kelsey I.; Filippenko, Alexei V.; Zheng, WeiKang] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Corsi, Alessandra; Sand, David] Texas Tech Univ, Dept Phys, Box 41051, Lubbock, TX 79409 USA. [Fox, Ori D.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Marion, G. H.] Univ Texas Austin, 1 Univ Stn C1400, Austin, TX 78712 USA. [Fraser, Morgan] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Inserra, Cosimo; Smartt, Stephen; Smith, Ken W.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Laher, Russ; Masci, Frank; Surace, Jason] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Rebbapragada, Umaa] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Sullivan, Mark] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. [Wozniak, Przemek] Los Alamos Natl Lab, Space & Remote Sensing, MS B244, Los Alamos, NM 87545 USA. RP Hosseinzadeh, G (reprint author), Las Cumbres Observ, 6740 Cortona Dr Ste 102, Goleta, CA 93117 USA.; Hosseinzadeh, G (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. EM griffin@lco.global OI McCully, Curtis/0000-0001-5807-7893; Arcavi, Iair/0000-0001-7090-4898 FU US Department of Energy, Laboratory Directed Research and Development program; National Science Foundation (NSF) [1313484]; PRIN-INAF; Knut and Alice Wallenberg Foundation; Swedish Research Council; European Union FP7 programme through ERC [320360, 307260, 615929]; Quantum universe I-Core program, Israeli Committee for Planning and Budgeting; Minerva grant; Weizmann-UK "making connections" program; Kimmel award; NSF CAREER [1455090]; NSF PIRE program [1545949]; Christopher R. Redlich Fund; TABASGO Foundation; NSF [AST-1211916]; ESO program [191.D-0935(C)]; W. M. Keck Foundation; California Institute of Technology; University of California; National Aeronautics and Space Administration (NASA); ISF; ISF grant; YeS award FX This work is based on observations obtained with the 48 inch Samuel Oschin Telescope and the 60 inch telescope at the Palomar Observatory as part of the intermediate Palomar Transient Factory (iPTF) project, a scientific collaboration among the California Institute of Technology, Los Alamos National Laboratory, the University of Wisconsin-Milwaukee, the Oskar Klein Center, the Weizmann Institute of Science, the TANGO Program of the University System of Taiwan, and the Kavli Institute for the Physics and Mathematics of the universe; the New Technology Telescope, operated by the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, as part of PESSTO, ESO program 191.D-0935(C); the Las Cumbres Observatory Global Telescope Network; both the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association, and the Telescopio Nazionale Galileo, operated by the Fundacion Galileo Galilei of the Italian Istituto Nazionale di Astrofisica, at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias; the Lick Observatory owned and operated by the University of California; and the W. M. Keck Observatory, which was made possible by the generous financial support of the W. M. Keck Foundation and is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration (NASA). We thank the staffs at all of these observatories for their assistance with the observations.; We thank Lars Bildsten and Matteo Cantiello for useful discussions, and all those whose observations and data reduction contributed to this work. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. The authors made extensive use of the Astropy package Astropy Collaboration et al. (2013) for data analysis. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. LANL participation in iPTF was funded by the US Department of Energy as part of the Laboratory Directed Research and Development program.; G.H., D.A.H., and C.M. are supported by the National Science Foundation (NSF) under Grant No. 1313484.; A.P., S.B., and N.E.R. are partially supported by PRIN-INAF 2014 with the project "Transient universe: unveiling new types of stellar explosions with PESSTO."; J.S., C.F., E.K., and F.T. gratefully acknowledge support from the Knut and Alice Wallenberg Foundation. The Oskar Klein Centre is funded by the Swedish Research Council.; M.F., A.G.-Y.,and M.S. acknowledge support from the European Union FP7 programme through ERC grant numbers 320360, 307260, and 615929, respectively. A.G.-Y. is also supported by the Quantum universe I-Core program by the Israeli Committee for Planning and Budgeting and the ISF; by Minerva and ISF grants; by the Weizmann-UK "making connections" program; and by Kimmel and YeS awards.; A.C. acknowledges support from NSF CAREER award #1455090.; M.M.K. acknowledges support from NSF PIRE program grant 1545949.; The supernova research of A.V.F.'s group at UC Berkeley is supported by the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. Research at Lick Observatory is partially supported by a generous gift from Google. NR 123 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 FEB 20 PY 2017 VL 836 IS 2 AR 158 DI 10.3847/1538-4357/836/2/158 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN1HK UT WOS:000395760900001 ER PT J AU Jarrett, TH Cluver, ME Magoulas, C Bilicki, M Alpaslan, M Bland-Hawthorn, J Brough, S Brown, MJI Croom, S Driver, S Holwerda, BW Hopkins, AM Loveday, J Norberg, P Peacock, JA Popescu, CC Sadler, EM Taylor, EN Tuffs, RJ Wang, L AF Jarrett, T. H. Cluver, M. E. Magoulas, C. Bilicki, M. Alpaslan, M. Bland-Hawthorn, J. Brough, S. Brown, M. J. I. Croom, S. Driver, S. Holwerda, B. W. Hopkins, A. M. Loveday, J. Norberg, P. Peacock, J. A. Popescu, C. C. Sadler, E. M. Taylor, E. N. Tuffs, R. J. Wang, L. TI Galaxy and Mass Assembly (GAMA): Exploring the WISE Web in G12 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: statistics; infrared: galaxies; large-scale structure of universe ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; PHOTOMETRIC REDSHIFT CATALOG; 2-POINT CORRELATION-FUNCTION; ANGULAR-CORRELATION FUNCTION; LARGE-SCALE STRUCTURE; STAR-FORMATION; STELLAR MASS; SKY SURVEY; DATA RELEASE AB We present an analysis of the mid-infrared Wide-field Infrared Survey Explorer (WISE) sources seen within the equatorial GAMA G12 field, located in the North Galactic Cap. Our motivation is to study and characterize the behavior of WISE source populations in anticipation of the deep multiwavelength surveys that will define the next decade, with the principal science goal of mapping the 3D large-scale structures and determining the global physical attributes of the host galaxies. In combination with cosmological redshifts, we identify galaxies from their WISE W1 (3.4 mu m) resolved emission, and we also perform a star-galaxy separation using apparent magnitude, colors, and statistical modeling of star counts. The resulting galaxy catalog has; 590,000 sources in 60 deg(2), reaching a W1 5 sigma depth of 31 mu Jy. At the faint end, where redshifts are not available, we employ a luminosity function analysis to show that approximately 27% of all WISE extragalactic sources to a limit of 17.5 mag (31 mu Jy) are at high redshift, z > 1. The spatial distribution is investigated using two-point correlation functions and a 3D source density characterization at 5 Mpc and 20 Mpc scales. For angular distributions, we find that brighter and more massive sources are strongly clustered relative to fainter sources with lower mass; likewise, based on WISE colors, spheroidal galaxies have the strongest clustering, while late-type disk galaxies have the lowest clustering amplitudes. In three dimensions, we find a number of distinct groupings, often bridged by filaments and superstructures. Using special visualization tools, we map these structures, exploring how clustering may play a role with stellar mass and galaxy type. C1 [Jarrett, T. H.; Magoulas, C.; Bilicki, M.] Univ Cape Town, Dept Astron, Private Bag X3, ZA-7701 Rondebosch, South Africa. [Cluver, M. E.] Univ Western Cape, Dept Phys & Astron, Robert Sobukwe Rd, ZA-7535 Bellville, South Africa. [Bilicki, M.; Holwerda, B. W.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Bilicki, M.] Univ Zielona Gora, Janusz Gil Inst Astron, Ul Szafrana 2, PL-65516 Zielona Gora, Poland. [Alpaslan, M.] NASA Ames Res Ctr, N232, Mountain View, CA 94035 USA. [Bland-Hawthorn, J.; Croom, S.; Sadler, E. M.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Brough, S.; Hopkins, A. M.] Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia. [Brown, M. J. I.] Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia. [Driver, S.] Univ Western Australia, ICRAR, 35 Stirling Highway, Crawley, WA 6009, Australia. [Driver, S.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Loveday, J.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Norberg, P.] Univ Durham, Dept Phys, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England. [Peacock, J. A.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Popescu, C. C.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Popescu, C. C.] Romanian Acad, Astron Inst, Str Cutitul de Argint 5, Bucharest, Romania. [Taylor, E. N.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Tuffs, R. J.] Max Planck Inst Kernphys, Saupfercheckweg 1, D-69117 Heidelberg, Germany. [Wang, L.] SRON Netherlands Inst Space Res Landleven, Landleven 12, NL-9747 AD Groningen, Netherlands. RP Jarrett, TH (reprint author), Univ Cape Town, Dept Astron, Private Bag X3, ZA-7701 Rondebosch, South Africa. EM jarrett@ast.uct.ac.za OI Brown, Michael/0000-0002-1207-9137; Cluver, Michelle/0000-0002-9871-6490 FU STFC (UK); ARC (Australia); AAO FX GAMA is a joint European-Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalog 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 programs 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/. NR 106 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 FEB 20 PY 2017 VL 836 IS 2 AR 182 DI 10.3847/1538-4357/836/2/182 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN3PX UT WOS:000395921500008 ER PT J AU Huang, SY Sahraoui, F Yuan, ZG He, JS Zhao, JS Le Contel, O Deng, XH Zhou, M Fu, HS Shi, QQ Lavraud, B Pang, Y Yang, J Wang, DD Li, HM Yu, XD Pollock, CJ Giles, BL Torbert, RB Russell, CT Goodrich, KA Gershman, DJ Moore, TE Ergun, RE Khotyaintsev, YV Lindqvist, PA Strangeway, RJ Magnes, W Bromund, K Leinweber, H Plaschke, F Anderson, BJ Burch, JL AF Huang, S. Y. Sahraoui, F. Yuan, Z. G. He, J. S. Zhao, J. S. Le Contel, O. Deng, X. H. Zhou, M. Fu, H. S. Shi, Q. Q. Lavraud, B. Pang, Y. Yang, J. Wang, D. D. Li, H. M. Yu, X. D. Pollock, C. J. Giles, B. L. Torbert, R. B. Russell, C. T. Goodrich, K. A. Gershman, D. J. Moore, T. E. Ergun, R. E. Khotyaintsev, Y. V. Lindqvist, P. -A. Strangeway, R. J. Magnes, W. Bromund, K. Leinweber, H. Plaschke, F. Anderson, B. J. Burch, J. L. TI Magnetospheric Multiscale Observations of Electron Vortex Magnetic Hole in the Turbulent Magnetosheath Plasma SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Earth; planets and satellites: magnetic fields; planets and satellites: terrestrial planets; plasmas; turbulence ID SOLAR-WIND; ROTATIONAL DISCONTINUITIES; EARTHS MAGNETOSHEATH; CLUSTER OBSERVATIONS; KINETIC SIMULATIONS; DISSIPATION RANGE; RECONNECTION; FIELD; DYNAMICS; SPECTRA AB We report on the observations of an electron vortex magnetic hole corresponding to a new type of coherent structure in the turbulent magnetosheath plasma using the Magnetospheric Multiscale mission data. The magnetic hole is characterized by a magnetic depression, a density peak, a total electron temperature increase (with a parallel temperature decrease but a perpendicular temperature increase), and strong currents carried by the electrons. The current has a dip in the core region and a peak in the outer region of the magnetic hole. The estimated size of the magnetic hole is about 0.23 rho(i) (similar to 30 rho(e)) in the quasi-circular cross-section perpendicular to its axis, where rho(i) and rho(e) are respectively the proton and electron gyroradius. There are no clear enhancements seen in high-energy electron fluxes. However, there is an enhancement in the perpendicular electron fluxes at 90 degrees pitch angle inside the magnetic hole, implying that the electrons are trapped within it. The variations of the electron velocity components V-em and V-en suggest that an electron vortex is formed by trapping electrons inside the magnetic hole in the cross-section in the M-N plane. These observations demonstrate the existence of a new type of coherent structures behaving as an electron vortex magnetic hole in turbulent space plasmas as predicted by recent kinetic simulations. C1 [Huang, S. Y.; Yuan, Z. G.; Yu, X. D.] Wuhan Univ, Sch Elect Informat, Wuhan, Peoples R China. [Huang, S. Y.; Sahraoui, F.; Le Contel, O.] UPMC, CNRS, Ecole Polytech, Lab Phys Plasmas, Palaiseau, France. [He, J. S.] Peking Univ, Sch Earth & Space Sci, Beijing, Peoples R China. [Zhao, J. S.] Chinese Acad Sci, Key Lab Planetary Sci, Purple Mt Observ, Nanjing, Peoples R China. [Deng, X. H.; Pang, Y.; Li, H. M.] Nanchang Univ, Inst Space Sci & Technol, Nanchang, Jiangxi, Peoples R China. [Zhou, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA. [Fu, H. S.; Yang, J.] Beihang Univ, Sch Space & Environm, Beijing, Peoples R China. [Shi, Q. Q.] Shandong Univ, Inst Space Sci, Shandong Prov Key Lab Opt Astron & Solar Terr Env, Weihai, Peoples R China. [Lavraud, B.] Univ Toulouse UPS, Inst Rech & Astrophys & Planetol, Toulouse, France. [Lavraud, B.] CNRS, UMR 5277, Toulouse, France. [Pollock, C. J.; Giles, B. L.; Gershman, D. J.; Moore, T. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Torbert, R. B.] Univ New Hampshire, Durham, NH 03824 USA. [Russell, C. T.; Strangeway, R. J.; Leinweber, H.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA. [Goodrich, K. A.; Ergun, R. E.] Univ Colorado, Boulder, CO 80309 USA. [Khotyaintsev, Y. V.] Swedish Inst Space Phys, Uppsala, Sweden. [Lindqvist, P. -A.] Royal Inst Technol, Stockholm, Sweden. [Magnes, W.; Plaschke, F.] Austrian Acad Sci, Space Res Inst, Graz, Austria. [Bromund, K.; Anderson, B. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Burch, J. L.] Southwest Res Inst, San Antonio, TX USA. RP Huang, SY (reprint author), Wuhan Univ, Sch Elect Informat, Wuhan, Peoples R China.; Huang, SY (reprint author), UPMC, CNRS, Ecole Polytech, Lab Phys Plasmas, Palaiseau, France. EM shiyonghuang@whu.edu.cn OI He, Jiansen/0000-0001-8179-417X FU National Natural Science Foundation of China [41374168, 41404132, 41574168, 41674161]; Program for New Century Excellent Talents in University [NCET-13-0446]; China Postdoctoral Science Foundation Funded Project [2015T80830]; project THESOW [ANR-11-JS56-0008]; LABEX Plas@Par, program "Investissementsd'Avenir" [ANR-11-IDEX-0004-02]; CNES; CNRS FX We thank the entire MMS team and instrument leads for data access and support. This work was supported by the National Natural Science Foundation of China (41374168, 41404132, 41574168, 41674161), Program for New Century Excellent Talents in University (NCET-13-0446), and China Postdoctoral Science Foundation Funded Project (2015T80830). S.Y.H. and F.S. acknowledge financial support from the project THESOW, grant ANR-11-JS56-0008, and from LABEX Plas@Par through a grant managed by the AgenceNationale de la Recherche (ANR), as part of the program "Investissementsd'Avenir" under the reference ANR-11-IDEX-0004-02. Data are publicly available from the MMS Science Data Center at http://lasp.colorado.edu/mms/sdc/. Work at IRAP was supported by CNES and CNRS. NR 48 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2017 VL 836 IS 2 AR L27 DI 10.3847/2041-8213/aa5f50 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN4WN UT WOS:000396007700001 ER PT J AU Paganini, L Mumma, MJ Gibb, EL Villanueva, GL AF Paganini, L. Mumma, M. J. Gibb, E. L. Villanueva, G. L. TI Ground-based Detection of Deuterated Water in Comet C/2014 Q2 (Lovejoy) at IR Wavelengths SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrobiology; comets: individual (C/2014 Q2 (Lovejoy)); methods: observational; planets and satellites: formation; techniques: spectroscopic ID SOLAR-SYSTEM; CHEMICAL-COMPOSITION; GIANT PLANETS; ORIGIN; INSTABILITY; ASTEROIDS; HDO/H2O; HISTORY; II. AB We conducted a deep search for deuterated water (HDO) in the Oort Cloud comet C/2014 Q2 (Lovejoy), through infrared (IR) spectroscopy with NIRSPEC at the Keck Observatory. In this Letter, we present our detections of HDO and water (H2O) in comet Lovejoy on 2015 February 4 (post-perihelion) after 1 hr integration on source. The IR observations allowed simultaneous detection of H2O and HDO, yielding production rates of 5.9 +/- 0.13 x 10(29) and 3.6 +/- 1.0 x 10(26) molecules s(-1), respectively. The simultaneous detection permitted accurate determination of the isotopic ratio (D/H) in water of 3.02 +/- 0.87 x 10(-4), i.e., larger than the value for water in terrestrial oceans (or Vienna Standard Mean Ocean Water, VSMOW) by a factor of 1.94 +/- 0.56. This D/H ratio in water exceeds the value obtained independently at millimeter wavelengths (0.89 +/- 0.25 VSMOW; pre-perihelion). We discuss these parameters in the context of origins and emphasize the need for contemporaneous measurements of HDO and H2O. C1 [Paganini, L.; Mumma, M. J.; Villanueva, G. L.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [Paganini, L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Gibb, E. L.] Univ Missouri, Dept Phys & Astron, St Louis, MO 63121 USA. RP Paganini, L (reprint author), NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.; Paganini, L (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. OI Mumma, Michael/0000-0003-4627-750X FU Keck PI Data Award; NSF Planetary Astronomy [AST-1211362, AST-1615441]; ISSI-Bern FX The authors would like to thank the anonymous referee and N. Biver and D. Bockelee-Morvan for interesting insights about this work. We also acknowledge support by the Keck PI Data Award (L.P.), administered by the NASA Exoplanet Science Institute. E.L.G. acknowledges support from NSF Planetary Astronomy Grants AST-1211362 and AST-1615441 and ISSI-Bern. 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. NR 32 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2017 VL 836 IS 2 AR L25 DI 10.3847/2041-8213/aa5cb3 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN3JD UT WOS:000395903900003 ER PT J AU Strohmayer, T Keek, L AF Strohmayer, Tod Keek, Laurens TI IGR J17062-6143 Is an Accreting Millisecond X-Ray Pulsar SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars: neutron; stars: oscillations; stars: rotation; X-rays: binaries; X-rays: individual (IGR J17062-6143) AB We present the discovery of 163.65 Hz X-ray pulsations from IGR J17062-6143 in the only observation obtained from the source with the Rossi X-ray Timing Explorer. This detection makes IGR J17062-6143 the lowest-frequency accreting millisecond X-ray pulsar presently known. The pulsations are detected in the 2-12 keV band with an overall significance of 4.3 sigma and an observed pulsed amplitude of 5.54% +/- 0.67% (in this band). Both dynamic power spectral and coherent phase timing analysis indicate that the pulsation frequency is decreasing during the approximate to 1.2 ks observation in a manner consistent with orbital motion of the neutron star. Because the observation interval is short, we cannot precisely measure the orbital period; however, periods shorter than 17 minutes are excluded at 90% confidence. For the range of acceptable circular orbits the inferred binary mass function substantially overlaps the observed range for the AMXP population as a whole. C1 [Strohmayer, Tod] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Strohmayer, Tod] NASA, Goddard Space Flight Ctr, Joint Space Sci Inst, Greenbelt, MD 20771 USA. [Keek, Laurens] Univ Maryland, NASA, GSFC, Xray Astrophys Lab, College Pk, MD 20742 USA. [Keek, Laurens] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Keek, Laurens] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Strohmayer, T (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.; Strohmayer, T (reprint author), NASA, Goddard Space Flight Ctr, Joint Space Sci Inst, Greenbelt, MD 20771 USA. FU NASA [NNG06EO90A]; International Space Science Institute in Bern, Switzerland; National Science Foundation [PHY-1430152] FX L.K. and T.S. acknowledge support by NASA under award number NNG06EO90A. L.K. thanks the International Space Science Institute in Bern, Switzerland and the National Science Foundation under grant No. PHY-1430152 (JINA Center for the Evolution of the Elements) for supporting events that benefited this work. We thank the anonymous referee for a helpful review. NR 18 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2017 VL 836 IS 2 AR L23 DI 10.3847/2041-8213/aa5e51 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN3JD UT WOS:000395903900001 ER PT J AU Peeters, E Bauschlicher, CW Allamandola, LJ Tielens, AGGM Ricca, A Wolfire, MG AF Peeters, Els Bauschlicher, Charles W., Jr. Allamandola, Louis J. Tielens, Alexander G. G. M. Ricca, Alessandra Wolfire, Mark G. TI The PAH Emission Characteristics of the Reflection Nebula NGC 2023 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; infrared: ISM; ISM: lines and bands; ISM: molecules; line: identification; molecular data ID POLYCYCLIC AROMATIC-HYDROCARBONS; MU-M EMISSION; MATRIX-ISOLATED NAPHTHALENE; BLIND SIGNAL SEPARATION; SPITZER-SPACE-TELESCOPE; PHOTON-DOMINATED REGION; PHOTODISSOCIATION REGIONS; INFRARED-EMISSION; SPECTROSCOPIC DATABASE; SPECTRAL VARIATIONS AB We present 5-20 mu m spectral maps of the reflection nebula NGC. 2023 obtained with the Infrared Spectrograph SL and SH modes on board the Spitzer Space Telescope, which reveal emission from polycyclic aromatic hydrocarbons (PAHs), C-60, and H-2 superposed on a dust continuum. We show that several PAH emission bands correlate with each other and exhibit distinct spatial distributions. that. reveal. a spatial sequence with distance from the illuminating star. We explore the distinct morphology of the 6.2, 7.7, and 8.6 mu m PAH bands and find that at least two spatially distinct components contribute to the 7-9 mu m PAH emission in NGC. 2023. We report that the PAH features behave independently of the underlying plateaus. We present spectra of compact, oval PAHs ranging in size from C-66 to C-210, determined computationally using density functional theory, and we. investigate trends in the band positions and relative intensities as a function of PAH size, charge, and geometry. Based on the NASA Ames PAH database, we discuss the 7-9 mu m components in terms of band assignments and relative intensities. We assign the plateau emission to very small grains with possible contributions from PAH clusters and identify components in the 7-9 mu m emission that likely originate. in these structures. Based on the assignments and the observed spatial sequence, we discuss the photochemical evolution of the interstellar PAH family as the PAHs. are more and more exposed to the radiation field of the central star in the evaporative flows associated with the Photo-Dissociation Regions in NGC. 2023. C1 [Peeters, Els] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Peeters, Els; Ricca, Alessandra] SETI Inst, Carl Sagan Ctr, 189 N Bernardo Ave,Suite 100, Mountain View, CA 94043 USA. [Bauschlicher, Charles W., Jr.] NASA, Ames Res Ctr, Entry Syst & Technol Div, Mail Stop 230-3, Moffett Field, CA 94035 USA. [Allamandola, Louis J.] NASA, Ames Res Ctr, Div Space Sci, Mail Stop 245-6, Moffett Field, CA 94035 USA. [Tielens, Alexander G. G. M.] Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Wolfire, Mark G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Peeters, E (reprint author), Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.; Peeters, E (reprint author), SETI Inst, Carl Sagan Ctr, 189 N Bernardo Ave,Suite 100, Mountain View, CA 94043 USA. EM epeeters@uwo.ca FU NASA Spitzer Space Telescope General Observer Program; Natural Sciences and Engineering Research Council of Canada (NSERC); NASA's Astrobiology Program and Laboratory Astrophysics Carbon in the Galaxy consortium; NASA's Laboratory Astrophysics program [NNX11AK09A]; European Research Council [246976]; Dutch Science Agency, NWO, as part of the Dutch Astrochemistry Network; Dutch Science Agency, NWO FX The authors thank the referee Kris Sellgren for the careful reading of the manuscript and very useful feedback. The authors are extremely grateful to Henry Leparskas for creating Figure 21. E.P. thanks Dr. D. Stock for fruitful discussions and feedback on the manuscript. We gratefully acknowledge support from the NASA Spitzer Space Telescope General Observer Program. E.P. gratefully acknowledges sustained support from the Natural Sciences and Engineering Research Council of Canada (NSERC: Discovery grant and Accelerator grant). L.J.A. gratefully acknowledges support from NASA's Astrobiology Program and Laboratory Astrophysics Carbon in the Galaxy consortium. A.R. thanks NASA's Laboratory Astrophysics program grant NNX11AK09A for its generous support of this work. Studies of interstellar chemistry at Leiden Observatory are supported through advanced-ERC grant 246976 from the European Research Council, through a grant by the Dutch Science Agency, NWO, as part of the Dutch Astrochemistry Network and through the Spinoza premie from the Dutch Science Agency, NWO. NR 84 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 FEB 20 PY 2017 VL 836 IS 2 AR 198 DI 10.3847/1538-4357/836/2/198 PG 40 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN1VI UT WOS:000395797900014 ER PT J AU Bohe, A Shao, LJ Taracchini, A Buonanno, A Babak, S Harry, IW Hinder, I Ossokine, S Purrer, M Raymond, V Chu, T Fong, H Kumar, P Pfeiffer, HP Boyle, M Hemberger, DA Kidder, LE Lovelace, G Scheel, MA Szilagyi, B AF Bohe, Alejandro Shao, Lijing Taracchini, Andrea Buonanno, Alessandra Babak, Stanislav Harry, Ian W. Hinder, Ian Ossokine, Serguei Puerrer, Michael Raymond, Vivien Chu, Tony Fong, Heather Kumar, Prayush Pfeiffer, Harald P. Boyle, Michael Hemberger, Daniel A. Kidder, Lawrence E. Lovelace, Geoffrey Scheel, Mark A. Szilagyi, Bela TI Improved effective-one-body model of spinning, nonprecessing binary black holes for the era of gravitational-wave astrophysics with advanced detectors SO PHYSICAL REVIEW D LA English DT Article ID NUMERICAL RELATIVITY; INITIAL DATA; RADIATION; EQUATIONS; EVOLUTION AB We improve the accuracy of the effective-one-body (EOB) waveforms that were employed during the first observing run of Advanced LIGO for binaries of spinning, nonprecessing black holes by calibrating them to a set of 141 numerical-relativity (NR) waveforms. The NR simulations expand the domain of calibration toward larger mass ratios and spins, as compared to the previous EOBNR model. Merger-ringdown waveforms computed in black-hole perturbation theory for Kerr spins close to extremal provide additional inputs to the calibration. For the inspiral-plunge phase, we use a Markov-chain Monte Carlo algorithm to efficiently explore the calibration space. For the merger-ringdown phase, we fit the NR signals with phenomenological formulae. After extrapolation of the calibrated model to arbitrary mass ratios and spins, the (dominant-mode) EOBNR waveforms have faithfulness-at design Advanced-LIGO sensitivity-above 99% against all the NR waveforms, including 16 additional waveforms used for validation, when maximizing only on initial phase and time. This implies a negligible loss in event rate due to modeling for these binary configurations. We find that future NR simulations at mass ratios greater than or similar to 4 and double spin greater than or similar to 0.8 will be crucial to resolving discrepancies between different ways of extrapolating waveform models. We also find that some of the NR simulations that already exist in such region of parameter space are too short to constrain the low-frequency portion of the models. Finally, we build a reduced-order version of the EOBNR model to speed up waveform generation by orders of magnitude, thus enabling intensive data-analysis applications during the upcoming observation runs of Advanced LIGO. C1 [Bohe, Alejandro; Shao, Lijing; Taracchini, Andrea; Buonanno, Alessandra; Babak, Stanislav; Harry, Ian W.; Hinder, Ian; Ossokine, Serguei; Puerrer, Michael; Raymond, Vivien; Pfeiffer, Harald P.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, Muhlenberg 1, D-14476 Potsdam, Germany. [Buonanno, Alessandra] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Chu, Tony] Princeton Univ, Dept Phys, Jadwin Hall, Princeton, NJ 08544 USA. [Chu, Tony; Fong, Heather; Kumar, Prayush; Pfeiffer, Harald P.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Fong, Heather] Univ Toronto, Dept Phys, Toronto, ON M5S 3H8, Canada. [Pfeiffer, Harald P.] Canadian Inst Adv Res, Toronto, ON M5G 1Z8, Canada. [Boyle, Michael; Kidder, Lawrence E.] Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA. [Hemberger, Daniel A.; Scheel, Mark A.; Szilagyi, Bela] CALTECH, Theoret Astrophys 350 17, Pasadena, CA 91125 USA. [Szilagyi, Bela] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Lovelace, Geoffrey] Calif State Univ Fullerton, Gravitat Wave Phys & Astron Ctr, Fullerton, CA 92834 USA. RP Bohe, A; Shao, LJ; Taracchini, A (reprint author), Max Planck Inst Gravitat Phys, Albert Einstein Inst, Muhlenberg 1, D-14476 Potsdam, Germany. EM alejandro.bohe@aei.mpg.de; lijing.shao@aei.mpg.de; andrea.taracchini@aei.mpg.de FU Sherman Fairchild Foundation; NSF [PHY-1404569, PHY-1606654, AST-1333129, PHY-1307489, PHY-1606522]; NSERC of Canada; Ontario Early Researcher Awards Program; Canada Research Chairs Program; Canadian Institute for Advanced Research; Canada Foundation for Innovation (CFI) under Compute Canada; Government of Ontario; Ontario Research Fund (ORF)-Research Excellence; University of Toronto; Canada Foundation for Innovation (CFI); Ministere de l'Economie, de l'Innovation et des Exportations du Quebec (MEIE); RMGA; Fonds de recherche du Quebec-Nature et Technologies (FRQ-NT); Research Corporation for Science Advancement [PHY-1429873]; Cal State Fullerton FX We would like to thank Mark Hannam and Sascha Husa for kindly providing us with the nonpublic BAM (q, chi1, chi2) = (8, 0.85, 0.85) waveform, which was used in Sec. IV to calibrate the EOB model. This work was supported in part at Caltech by the Sherman Fairchild Foundation and NSF Grants No. PHY-1404569, at Cornell by NSF Grants No. PHY-1606654 and No. AST-1333129 and the Sherman Fairchild Foundation and at Cal State Fullerton by NSF grants PHY-1307489 and PHY-1606522. We gratefully acknowledge support for this research at CITA from NSERC of Canada, the Ontario Early Researcher Awards Program, the Canada Research Chairs Program, and the Canadian Institute for Advanced Research. Calculations were performed at the GPC supercomputer at the SciNet HPC Consortium; SciNet is funded by: the Canada Foundation for Innovation (CFI) under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund (ORF)-Research Excellence; and the University of Toronto. Further calculations were performed on the Briaree cluster at Sherbrooke University, managed by Calcul Quebec and Compute Canada and with operation funded by the Canada Foundation for Innovation (CFI), Ministere de l'Economie, de l'Innovation et des Exportations du Quebec (MEIE), RMGA and the Fonds de recherche du Quebec-Nature et Technologies (FRQ-NT). Some of the calculations were performed on the ORCA cluster at Cal State Fullerton, which is supported by the Research Corporation for Science Advancement, PHY-1429873, and Cal State Fullerton. New NR simulations were performed on the AEI Datura and Minerva clusters. The Markov-chain Monte Carlo runs were performed on the AEI Vulcan cluster. NR 125 TC 0 Z9 0 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD FEB 17 PY 2017 VL 95 IS 4 AR 044028 DI 10.1103/PhysRevD.95.044028 PG 29 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA EL1HG UT WOS:000394370500010 ER PT J AU Zeng, ZC Zhang, Q Natraj, V Margolis, JS Shia, RL Newman, S Fu, DJ Pongetti, TJ Wong, KW Sander, SP Wennberg, PO Yung, YL AF Zeng, Zhao-Cheng Zhang, Qiong Natraj, Vijay Margolis, Jack S. Shia, Run-Lie Newman, Sally Fu, Dejian Pongetti, Thomas J. Wong, Kam W. Sander, Stanley P. Wennberg, Paul O. Yung, Yuk L. TI Aerosol scattering effects on water vapor retrievals over the Los Angeles Basin SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID SIMULATED RETRIEVALS; OPTICAL DEPTH; CO2 EMISSIONS; CLARS-FTS; ALGORITHM; CH4; UNCERTAINTIES; REANALYSIS; CALIFORNIA; SATELLITE AB In this study, we propose a novel approach to describe the scattering effects of atmospheric aerosols in a complex urban environment using water vapor (H2O) slant column measurements in the near infrared. This approach is demonstrated using measurements from the California Laboratory for Atmospheric Remote Sensing Fourier Transform Spectrometer on the top of Mt. Wilson, California, and a two-stream-exact single scattering (2S-ESS) radiative transfer (RT) model. From the spectral measurements, we retrieve H2O slant column density (SCD) using 15 different absorption bands between 4000 and 8000 cm(-1). Due to the wavelength dependence of aerosol scattering, large variations in H2O SCD retrievals are observed as a function of wavelength. Moreover, the variations are found to be correlated with aerosol optical depths (AODs) measured at the AERONET-Caltech station. Simulation results from the RT model reproduce this correlation and show that the aerosol scattering effect is the primary contributor to the variations in the wavelength dependence of the H2O SCD retrievals. A significant linear correlation is also found between variations in H2O SCD retrievals from different bands and corresponding AOD data; this correlation is associated with the asymmetry parameter, which is a first-order measure of the aerosol scattering phase function. The evidence from both measurements and simulations suggests that wavelength-dependent aerosol scattering effects can be derived using H2O retrievals from multiple bands. This understanding of aerosol scattering effects on H2O retrievals suggests a promising way to quantify the effect of aerosol scattering on greenhouse gas retrievals and could potentially contribute towards reducing biases in greenhouse gas retrievals from space. C1 [Zeng, Zhao-Cheng; Zhang, Qiong; Shia, Run-Lie; Newman, Sally; Wong, Kam W.; Wennberg, Paul O.; Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Zeng, Zhao-Cheng] Chinese Univ Hong Kong, Inst Space & Earth Informat Sci, Hong Kong, Hong Kong, Peoples R China. [Natraj, Vijay; Fu, Dejian; Pongetti, Thomas J.; Wong, Kam W.; Sander, Stanley P.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Margolis, Jack S.] 1842 Rose Villa St, Pasadena, CA 91107 USA. RP Zeng, ZC (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.; Zeng, ZC (reprint author), Chinese Univ Hong Kong, Inst Space & Earth Informat Sci, Hong Kong, Hong Kong, Peoples R China. EM zzhaoch@gmail.com FU National Aeronautics and Space Administration (NASA); Caltech KISS Megacity project; NIST GHG and Climate Science Program; NASA's Carbon Cycle Science Program through the JPL; Chinese University of Hong Kong FX We thank M. Gunson and A. Eldering for stimulating discussions and support, and M. Gerstell for proofreading the manuscript. Part of the research in this study was performed at the Jet Propulsion Laboratory (JPL), California Institute of Technology (Caltech), under a contract with the National Aeronautics and Space Administration (NASA). Support from the Caltech KISS Megacity project, the NIST GHG and Climate Science Program and NASA's Carbon Cycle Science Program through the JPL is gratefully acknowledged. Zhao-Cheng Zeng was supported by a postgraduate studentship for overseas academic exchange from the Chinese University of Hong Kong. We thank Jochen Stutz and his staff for their effort in establishing and maintaining the AERONET Caltech site. We also thank the anonymous reviewers whose comments helped improve the paper significantly. NR 36 TC 0 Z9 0 U1 1 U2 1 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 FEB 17 PY 2017 VL 17 IS 4 BP 2495 EP 2508 DI 10.5194/acp-17-2495-2017 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EM2GQ UT WOS:000395134800001 ER PT J AU De Sanctis, MC Ammannito, E McSween, HY Raponi, A Marchi, S Capaccioni, F Capria, MT Carrozzo, FG Ciarniello, M Fonte, S Formisano, M Frigeri, A Giardino, M Longobardo, A Magni, G McFadden, LA Palomba, E Pieters, CM Tosi, F Zambon, F Raymond, CA Russell, CT AF De Sanctis, M. C. Ammannito, E. McSween, H. Y. Raponi, A. Marchi, S. Capaccioni, F. Capria, M. T. Carrozzo, F. G. Ciarniello, M. Fonte, S. Formisano, M. Frigeri, A. Giardino, M. Longobardo, A. Magni, G. McFadden, L. A. Palomba, E. Pieters, C. M. Tosi, F. Zambon, F. Raymond, C. A. Russell, C. T. TI Localized aliphatic organic material on the surface of Ceres SO SCIENCE LA English DT Article ID SOLAR-SYSTEM; WATER-ICE; MATTER; SPECTROSCOPY; EVOLUTION; ORIGIN; CHONDRITES; METEORITE; PHOEBE AB Organic compounds occur in some chondritic meteorites, and their signatures on solar system bodies have been sought for decades. Spectral signatures of organics have not been unambiguously identified on the surfaces of asteroids, whereas they have been detected on cometary nuclei. Data returned by the Visible and InfraRed Mapping Spectrometer on board the Dawn spacecraft show a clear detection of an organic absorption feature at 3.4 micrometers on dwarf planet Ceres. This signature is characteristic of aliphatic organic matter and is mainly localized on a broad region of similar to 1000 square kilometers close to the similar to 50-kilometer Ernutet crater. The combined presence on Ceres of ammonia-bearing hydrated minerals, water ice, carbonates, salts, and organic material indicates a very complex chemical environment, suggesting favorable environments to prebiotic chemistry. C1 [De Sanctis, M. C.; Ammannito, E.; Raponi, A.; Marchi, S.; Capaccioni, F.; Capria, M. T.; Carrozzo, F. G.; Ciarniello, M.; Fonte, S.; Formisano, M.; Frigeri, A.; Giardino, M.; Longobardo, A.; Magni, G.; Palomba, E.; Tosi, F.; Zambon, F.] Ist Nazl Astrofis, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy. [Ammannito, E.; Russell, C. T.] Univ Calif Los Angeles, Earth Planetary & Space Sci, 603 Charles Young Dr, Los Angeles, CA 90095 USA. [McSween, H. Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Marchi, S.] Southwest Res Inst, Boulder, CO 80302 USA. [McFadden, L. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pieters, C. M.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA. [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP De Sanctis, MC (reprint author), Ist Nazl Astrofis, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy. EM mariacristina.desanctis@iaps.inafit OI Marchi, Simone/0000-0003-2548-3291; Palomba, Ernesto/0000-0002-9101-6774; Tosi, Federico/0000-0003-4002-2434; Zambon, Francesca/0000-0002-4190-6592 FU Italian Space Agency (ASI); NASA; VIR instrument FX We thank the Italian Space Agency (ASI) and NASA for supporting this work. The VIR instrument was funded and coordinated by the ASI and built by Selex ES, with the scientific leadership of the Institute for Space Astrophysics and Planetology, Italian National Institute for Astrophysics, Italy. The VIR is operated byte Institute for Space Astrophysics and Planetology, Rome, Italy. A portion of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA. Dawn data are archived in NASA's Planetary Data System; VIR spectral data may be obtained at http://sbn.psi.edu/pds/resource/dwncvir.html. We thank E. Quirico for providing the IOM data. NR 32 TC 1 Z9 1 U1 3 U2 3 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD FEB 17 PY 2017 VL 355 IS 6326 BP 719 EP + DI 10.1126/science.aaj2305 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EM2AC UT WOS:000395117700035 PM 28209893 ER PT J AU Yang, Y Anderson, MC Gao, F Hain, CR Semmens, KA Kustas, WP Noormets, A Wynne, RH Thomas, VA Sun, G AF Yang, Yun Anderson, Martha C. Gao, Feng Hain, Christopher R. Semmens, Kathryn A. Kustas, William P. Noormets, Asko Wynne, Randolph H. Thomas, Valerie A. Sun, Ge TI Daily Landsat-scale evapotranspiration estimation over a forested landscape in North Carolina, USA, using multi-satellite data fusion SO HYDROLOGY AND EARTH SYSTEM SCIENCES LA English DT Article ID MAPPING DAILY EVAPOTRANSPIRATION; CONTINENTAL SCALES; SURFACE-TEMPERATURE; SATELLITE IMAGERY; LEAF-AREA; WATER-USE; MODIS; MODEL; SENSITIVITY; DROUGHT AB As a primary flux in the global water cycle, evapotranspiration (ET) connects hydrologic and biological processes and is directly affected by water and land management, land use change and climate variability. Satellite remote sensing provides an effective means for diagnosing ET patterns over heterogeneous landscapes; however, limitations on the spatial and temporal resolution of satellite data, combined with the effects of cloud contamination, constrain the amount of detail that a single satellite can provide. In this study, we describe an application of a multi-sensor ET data fusion system over a mixed forested/agricultural landscape in North Carolina, USA, during the growing season of 2013. The fusion system ingests ET estimates from the Two-Source Energy Balance Model (TSEB) applied to thermal infrared remote sensing retrievals of land surface temperature from multiple satellite platforms: hourly geostationary satellite data at 4 km resolution, daily 1 km imagery from the Moderate Resolution Imaging Spectroradiometer (MODIS) and biweekly Landsat thermal data sharpened to 30 m. These multiple ET data streams are combined using the Spatial and Temporal Adaptive Reflectance Fusion Model (STARFM) to estimate daily ET at 30m resolution to investigate seasonal water use behavior at the level of individual forest stands and land cover patches. A new method, also exploiting the STARFM algorithm, is used to fill gaps in the Land-sat ET retrievals due to cloud cover and/or the scan-line corrector (SLC) failure on Landsat 7. The retrieved daily ET time series agree well with observations at two AmeriFlux eddy covariance flux tower sites in a managed pine plantation within the modeling domain: US-NC2 located in a mid-rotation (20-year-old) loblolly pine stand and US-NC3 located in a recently clear-cut and replanted field site. Root mean square errors (RMSEs) for NC2 and NC3 were 0.99 and 1.02 mm day(-1), respectively, with mean absolute errors of approximately 29% at the daily time step, 12% at the monthly time step and 0.7% over the full study period at the two flux tower sites. Analyses of water use patterns over the plantation indicate increasing seasonal ET with stand age for young to mid-rotation stands up to 20 years, but little dependence on age for older stands. An accounting of consumptive water use by major land cover classes representative of the modeling domain is presented, as well as relative partitioning of ET between evaporation (E) and transpiration (T) components obtained with the TSEB. The study provides new insights about the effects of management and land use change on water yield over forested landscapes. C1 [Yang, Yun; Anderson, Martha C.; Gao, Feng; Kustas, William P.] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. [Hain, Christopher R.] Marshall Space Flight Ctr, Earth Sci Branch, Huntsville, AL USA. [Semmens, Kathryn A.] Nurture Nat Ctr, Easton, PA USA. [Noormets, Asko] North Carolina State Univ, Dept Forestry & Environm Resources, Raleigh, NC USA. [Wynne, Randolph H.; Thomas, Valerie A.] Virginia Polytech Inst & State Univ, Dept Forest Resources & Environm Conservat, Blacksburg, VA 24061 USA. [Sun, Ge] USDA ARS, Eastern Forest Environm Threat Assessment Ctr, Southern Res Stn, Raleigh, NC 27695 USA. RP Yang, Y (reprint author), USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. EM yun.yang@ars.usda.gov FU NASA [NNH14AX36I] FX This work was funded in part by a grant from NASA (NNH14AX36I). We thank the Weyerhaeuser Company for providing stand age data. The US Department of Agriculture (USDA) prohibits discrimination in all its programs and activities on the basis of race, color, national origin, age, disability, and where applicable, sex, marital status, familial status, parental status, religion, sexual orientation, genetic information, political beliefs, reprisal or because all or part of an individual's income is derived from any public assistance program. (Not all prohibited bases apply to all programs.) Persons with disabilities who require alternative means for communication of program information (Braille, large print, audiotape, etc.) should contact USDA's TARGET Center at (202) 720-2600 (voice and TDD). To file a complaint of discrimination, write to USDA, Director, Office of Civil Rights, 1400 Independence Avenue, S.W., Washington, D.C. 20250-9410, or call (800) 795-3272 (voice) or (202) 7206382 (TDD). USDA is an equal opportunity provider and employer. NR 81 TC 0 Z9 0 U1 6 U2 6 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1027-5606 EI 1607-7938 J9 HYDROL EARTH SYST SC JI Hydrol. Earth Syst. Sci. PD FEB 17 PY 2017 VL 21 IS 2 BP 1017 EP 1037 DI 10.5194/hess-21-1017-2017 PG 21 WC Geosciences, Multidisciplinary; Water Resources SC Geology; Water Resources GA EM2YB UT WOS:000395180600001 ER PT J AU Mandra, S Zhu, Z Katzgraber, HG AF Mandra, Salvatore Zhu, Zheng Katzgraber, Helmut G. TI Exponentially Biased Ground-State Sampling of Quantum Annealing Machines with Transverse-Field Driving Hamiltonians SO PHYSICAL REVIEW LETTERS LA English DT Article ID ADIABATIC EVOLUTION; SPIN-GLASSES; MONTE-CARLO; OPTIMIZATION; ALGORITHM AB We study the performance of the D-Wave 2Xquantum annealing machine on systems with well-controlled ground-state degeneracy. While obtaining the ground state of a spin-glass benchmark instance represents a difficult task, the gold standard for any optimization algorithm or machine is to sample all solutions that minimize the Hamiltonian with more or less equal probability. Our results show that while naive transverse-field quantum annealing on the D-Wave 2X device can find the ground-state energy of the problems, it is not well suited in identifying all degenerate ground-state configurations associated with a particular instance. Even worse, some states are exponentially suppressed, in agreement with previous studies on toy model problems [New J. Phys. 11, 073021 (2009)]. These results suggest that more complex driving Hamiltonians are needed in future quantum annealing machines to ensure a fair sampling of the ground-state manifold. C1 [Mandra, Salvatore] Harvard Univ, Dept Chem & Chem Biol, 12 Oxford St, Cambridge, MA 02138 USA. [Mandra, Salvatore] NASA, Ames Res Ctr, Quantum Artificial Intelligence Lab QuAIL, Mail Stop 269-1, Moffett Field, CA 94035 USA. [Mandra, Salvatore] Stinger Ghaffarian Technol Inc, 7701 Greenbelt Rd,Suite 400, Greenbelt, MD 20770 USA. [Zhu, Zheng; Katzgraber, Helmut G.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Katzgraber, Helmut G.] Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA. RP Mandra, S (reprint author), Harvard Univ, Dept Chem & Chem Biol, 12 Oxford St, Cambridge, MA 02138 USA.; Mandra, S (reprint author), NASA, Ames Res Ctr, Quantum Artificial Intelligence Lab QuAIL, Mail Stop 269-1, Moffett Field, CA 94035 USA.; Mandra, S (reprint author), Stinger Ghaffarian Technol Inc, 7701 Greenbelt Rd,Suite 400, Greenbelt, MD 20770 USA. EM smandra@fas.harvard.edu; zzwtgts@tamu.edu; 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 would like to thank A. Aspuru-Guzik, F. Hamze, A. King, A. J. Ochoa and A. Perdomo-Ortiz for fruitful discussions. We also thank E. G. Rieffel and D. Venturelli for carefully reading the manuscript. H. G. K. acknowledges support from the NSF (Grant No. DMR-1151387) and would like to thank Zaya for inspiration to initiate this project. S. M. was supported by NASA (Sponsor Grant 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. The research of H. G. K. and Z. Z. 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. The views and conclusions contained herein are those of the authors and should not be interpreted as necessarily representing the official policies or endorsements, either expressed or implied, of ODNI, IARPA, or the U.S. Government. NR 40 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 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD FEB 17 PY 2017 VL 118 IS 7 AR 070502 DI 10.1103/PhysRevLett.118.070502 PG 6 WC Physics, Multidisciplinary SC Physics GA EL1IV UT WOS:000394374800002 PM 28256849 ER PT J AU Haddad, ZS Sawaya, RC Kacimi, S Sy, OO Turk, FJ Steward, J AF Haddad, Z. S. Sawaya, R. C. Kacimi, S. Sy, O. O. Turk, F. J. Steward, J. TI Interpreting millimeter-wave radiances over tropical convective clouds SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MICROWAVE RADIATIVE PROPERTIES; SCATTERING PROPERTIES; 183 GHZ; PART I; PRECIPITATION; PARAMETERIZATION; ALGORITHMS; PARTICLES; DATABASE; MODEL AB Attempts to interpret the measurements of millimeter-wave radiometers over tropical storms must overcome the difficulty of modeling the scattering signatures of hydrometeors at these frequencies. Most approaches to date try to retrieve surface precipitation, to which the observations are not directly sensitive. In fact, millimeter wavelengths are most sensitive to the scattering from solid hydrometeors within the upper levels of the cloud. Millimeter-wavelength radiometers have a definite advantage over the lower frequency radiometers in that they have finer spatial resolution to resolve deep convection. Preliminary analyses summarized here indicate that the measurements are indeed sensitive to the depth and intensity of convection. The challenge is to derive a robust approach to make quantitative estimates of the characteristics of the convection directly from the observations, and conversely to derive a robust forward representation of the dependence of the radiances on the underlying moisture fields, to enable effective data assimilation. This is accomplished using a two-step semiempirical approach: first, nearly simultaneous coincident observations by millimeter-wave radiometers and orbiting atmospheric profiling radars are used to enforce unbiased consistency between modeled brightness temperatures and radar and radiometer observations; second, the departure from the first-step mean empirical relations are explained in terms of the moisture variables, using cloud-resolving simulations with different microphysical schemes, including an original microphysical representation that proves to be more consistent with remote sensing observations than existing schemes. The results are a retrieval approach and a forward representation that are unbiased by construction, with uncertainties quantified by the corresponding conditional variances. C1 [Haddad, Z. S.; Sy, O. O.; Turk, F. J.; Steward, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Haddad, Z. S.; Kacimi, S.; Steward, J.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. [Sawaya, R. C.] Univ Calif Irvine, Dept Phys, Irvine, CA 92717 USA. RP Haddad, ZS (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.; Haddad, ZS (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. EM zsh@jpl.nasa.gov FU National Oceanic and Atmospheric Administration's Hurricane Forecasting Improvement Project; National Aeronautics and Space Administration FX This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The work was partially supported by the National Oceanic and Atmospheric Administration's Hurricane Forecasting Improvement Project. The remote sensing data and our forward simulations can be found at https://trmm.jpl.nasa.gov/2016jgrdata/. NR 23 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 16 PY 2017 VL 122 IS 3 BP 1650 EP 1664 DI 10.1002/2016JD025923 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EN6MX UT WOS:000396119200015 ER PT J AU Feng, L Hu, CM Barnes, BB Mannino, A Heidinger, AK Strabala, K Iraci, LT AF Feng, Lian Hu, Chuanmin Barnes, Brian B. Mannino, Antonio Heidinger, Andrew K. Strabala, Kathleen Iraci, Laura T. TI Cloud and Sun-glint statistics derived from GOES and MODIS observations over the Intra-Americas Sea for GEO-CAPE mission planning SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OCEAN COLOR DATA; PRODUCTS; COASTAL; WATERS; GOCI AB Knowledge of cloud cover, frequency, and duration is not only important to study cloud dynamics, but also critical in determiningwhenand where to take ocean measurements from geostationary orbits such as the Geostationary Coastal and Air Pollution Events (GEO-CAPE) mission due to the challenges in achieving complete hemispheric coverage of coastal oceans, estuaries, and inland waters at hourly frequency. Using GOES hourly measurements at 4 km nadir resolution between 2006 and 2011, the number of cloud-free hourly observations per day (N-cf) for solar zenith angle theta(o) < 80 degrees was estimated for each 0.1 degrees location of the Intra-Americas Sea. The number of Sun-glint-affected hourly observations per day (N-sg) was also calculated based on the planned GEO-CAPE observation geometry and realistic wind speed. High-latitude and equatorial oceans showed the lowest N-cf (< 2.4) in all climatological months, and highest N-cf was observed in the Gulf of Mexico (GoM) and Caribbean (> 4.5). Different regions showed differences in seasonality of cloud-free conditions and also showed differences in the hour of a day at which the satellite observations would have the maximal cloud-free and glint-free probability (T-max). Cloud cover from Moderate Resolution Imaging Spectroradiometer (MODIS) 1 km measurements are > 10% higher than those from the MODIS 250m measurements, supporting ocean color missions at subkilometer resolutions to enhance both spatial coverage and temporal frequency. These findings provide valuable information for GEO-CAPE mission planning to maximize its science value through minimizing the impacts of clouds and Sun glint. C1 [Feng, Lian; Hu, Chuanmin; Barnes, Brian B.] Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA. [Mannino, Antonio] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Heidinger, Andrew K.; Strabala, Kathleen] Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI USA. [Iraci, Laura T.] NASA, Ames Res Ctr, Atmospher Sci Branch, Moffett Field, CA 94035 USA. RP Hu, CM (reprint author), Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA. EM huc@usf.edu FU NASA Ocean Biology and Biogeochemistry program FX This work was supported by the NASA Ocean Biology and Biogeochemistry program and particularly through a grant to support NASA's GEO-CAPE mission design. 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. The manuscript received extensive comments and suggestions from four reviewers, whose effort to help improve the manuscript is greatly appreciated. The GOES cloud mask data were provided by the NOAA, from their website at http://www.ospo.noaa.gov/Products/atmosphere/clavr/index.html. MODIS cloud fraction data were obtained from the NASA's Giovanni website at http://giovanni.gsfc.nasa.gov/giovanni/. MODIS level 1A data were obtained from the NASA's OceanColor Web at http://oceancolor.gsfc.nasa.gov/cms/. NR 40 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 16 PY 2017 VL 122 IS 3 BP 1725 EP 1745 DI 10.1002/2016JD025372 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EN6MX UT WOS:000396119200020 ER PT J AU Khan, AL Dierssen, H Schwarz, JP Schmitt, C Chlus, A Hermanson, M Painter, TH McKnight, DM AF Khan, Alia L. Dierssen, Heidi Schwarz, Joshua P. Schmitt, Carl Chlus, Adam Hermanson, Mark Painter, Thomas H. McKnight, Diane M. TI Impacts of coal dust from an active mine on the spectral reflectance of Arctic surface snow in Svalbard, Norway SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID LIGHT-ABSORBING IMPURITIES; INDUSTRIAL BLACK CARBON; IMAGING SPECTROSCOPY; GRAIN-SIZE; SOOT; ALBEDO; ANTARCTICA; DEPOSITION; PARTICLES AB Light-absorbing particles (LAPs) in snow such as dust and black carbon influence the radiative forcing at the Earth's surface, which has major implications for global climate models. LAPs also significantly influence the melting of glaciers, sea ice, and seasonal snow. Here we present an in situ study of surface snow near an active coal mine in the Norwegian Arctic. We couple measurements of spectral hemispherical directional reflectance factor (HDRF) with measurements of LAPs characterized in two ways, as refractory black carbon using a Single Particle Soot Photometer and the total light absorption of LAPs measured with the Light Absorption Heating Method. The Snow Ice and Aerosol Radiation model was constrained by LAP measurements. Results were compared to observed spectral albedo measurements. Modeled and observed albedos were similar at the cleaner and more remote sites. However, the modeled spectral albedos do not fully account for the low spectral albedo measured next to the mine. LAP measurements also showed a large variation in particle sizes (tenths to tens of microns) related to transport distance of the particles from the mine. Here we find that LAPs from coal dust reduce the spectral HDRF by up to 84% next to the mine and 55% 0.5 km downwind of the mine. The coupling of extreme LAP observations (1 ng g(-1) to 4863 ng g(-1)) with HDRF measurements from 350 to 2500nm has facilitated the development of spectral band pairs, which could be used in the future to remotely assess LAPs in Arctic snow. C1 [Khan, Alia L.; McKnight, Diane M.] Univ Colorado, Dept Civil & Environm Engn, Boulder, CO 80309 USA. [Khan, Alia L.; McKnight, Diane M.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. [Khan, Alia L.] Univ Colorado, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA. [Dierssen, Heidi; Chlus, Adam] Univ Connecticut, Dept Marine Sci, Storrs, CT USA. [Schwarz, Joshua P.] NOAA, Earth Syst Res Lab, Boulder, CO USA. [Schmitt, Carl] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. [Hermanson, Mark] Univ Ctr Svalbard, Dept Arctic Technol, Longyearbyen, Svalbard. [Painter, Thomas H.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Khan, AL (reprint author), Univ Colorado, Dept Civil & Environm Engn, Boulder, CO 80309 USA.; Khan, AL (reprint author), Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.; Khan, AL (reprint author), Univ Colorado, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA. EM alia.khan@colorado.edu FU National Science Foundation-Graduate Research Fellowship Program [DGE 1144083]; Consortium of Universities for the Advancement of Hydrologic Sciences (CUAHSI); U.S. NASA Ocean Biology and Biogeochemistry [NNX15AC32G, NNX13AH88G]; NASA FX The funding for Khan came from the National Science Foundation-Graduate Research Fellowship Program, AWARD DGE 1144083 and a Pathfinder Travel Fellowship from the Consortium of Universities for the Advancement of Hydrologic Sciences (CUAHSI). The field sampling was supported in conjunction with course AT-331 at the University Center in Svalbard (UNIS) in the Arctic Technology Department on Arctic Pollution. Funding for Dierssen and Chlus was provided by the U.S. NASA Ocean Biology and Biogeochemistry (NNX15AC32G and NNX13AH88G). Part of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. We thank McKenzie Skiles and three anonymous reviewers for helpful comments on earlier drafts of the paper. Supporting data are included as four tables in the supporting information file; any additional data may be obtained from A.L.K. (email: alia.khan@colorado.edu). McKnight acknowledges support for independent research while being a program officer at the National Science Foundation. NR 49 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 16 PY 2017 VL 122 IS 3 BP 1767 EP 1778 DI 10.1002/2016JD025757 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EN6MX UT WOS:000396119200022 ER PT J AU Zhang, L Henze, DK Grell, GA Torres, O Jethva, H Lamsal, LN AF Zhang, Li Henze, Daven K. Grell, Georg A. Torres, Omar Jethva, Hiren Lamsal, Lok N. TI What factors control the trend of increasing AAOD over the United States in the last decade? SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OZONE MONITORING INSTRUMENT; SIZE DISTRIBUTION; MINERAL DUST; GOCART MODEL; AEROSOL EMISSIONS; OPTICAL DEPTH; BLACK CARBON; EAST-ASIA; GEOS-CHEM; DEEP-SEA AB We examine the spatial and temporal trends of absorbing aerosol optical depth (AAOD) in the last decade over the United States (U. S.) observed by the Ozone Monitoring Instrument (OMI). Monthly average OMI AAOD has increased over broad areas of the central U. S. from 2005 to 2015, by up to a factor of 4 in some grid cells (similar to 60 km resolution). The AAOD increases in all seasons, although the percentage increases are larger in summer (June-July-August) than in winter (December-January-February) by a factor of 3. Despite enhancements in AAOD, OMI AOD exhibits insignificant trend over most of the U. S. except parts of the central and western U. S., the latter which may partly be due to decreases in precipitation. Trends in AAOD contrast with declining trends in surface concentrations of black carbon (BC) aerosol. Interannual variability of local biomass burning emissions of BC may contribute to the positive trend in AAOD over the western U. S. Changes in both dust aerosol measured at the surface (in terms of concentration and size) and dust AAOD indicate distinct enhancements, especially over the central U. S. by 50-100%, which appears to be one of the major factors that impacts positive trends in AAOD. C1 [Zhang, Li] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Zhang, Li; Henze, Daven K.] Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA. [Zhang, Li; Grell, Georg A.] NOAA, Global Syst Div, Earth Syst Res Lab, Boulder, CO 80305 USA. [Torres, Omar; Lamsal, Lok N.] NOAA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Jethva, Hiren; Lamsal, Lok N.] NASA, Goddard Space Flight Ctr, GESTAR Univ Space Res Assoc, Greenbelt, MD USA. RP Zhang, L (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.; Zhang, L (reprint author), Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA.; Zhang, L (reprint author), NOAA, Global Syst Div, Earth Syst Res Lab, Boulder, CO 80305 USA. EM li.zhang@colorado.edu FU NASA [NNX15AC30G]; Environmental Protection Agency (EPA)-STAR grant [RD-83503701-0]; U.S. EPA's STAR program [RD-83503701-0] FX This work was supported from NASA grant NNX15AC30G and the Environmental Protection Agency (EPA)-STAR grant RD-83503701-0. Although the research described in the article has been funded wholly or in part by the U.S. EPA's STAR program through grant (RD-83503701-0), it 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. The OMI data for this paper are freely available from https://earthdata.nasa.gov/ and properly cited and referred to in the reference list. The Interagency Monitoring of Protected Visual Environment (IMPROVE) data are freely available at http://vista.cira.colostate.edu/improve/. The source code for the GEOS-Chem model used in this study is freely available at http://acmg.seas.harvard.edu/geos/. The authors would like to thank the anonymous reviewers for their insightful comments and suggestions that have contributed to improve this paper. NR 73 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 16 PY 2017 VL 122 IS 3 BP 1797 EP 1810 DI 10.1002/2016JD025472 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EN6MX UT WOS:000396119200024 ER PT J AU Lamsal, LN Janz, SJ Krotkov, NA Pickering, KE Spurr, RJD Kowalewski, MG Loughner, CP Crawford, JH Swartz, WH Herman, JR AF Lamsal, L. N. Janz, S. J. Krotkov, N. A. Pickering, K. E. Spurr, R. J. D. Kowalewski, M. G. Loughner, C. P. Crawford, J. H. Swartz, W. H. Herman, J. R. TI High-resolution NO2 observations from the Airborne Compact Atmospheric Mapper: Retrieval and validation SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OZONE MONITORING INSTRUMENT; ABSORPTION CROSS-SECTION; SURFACE REFLECTANCE ANISOTROPY; TROPOSPHERIC NITROGEN-DIOXIDE; MAX-DOAS MEASUREMENTS; IN-SITU; SATELLITE RETRIEVALS; BOUNDARY-LAYER; DISCOVER-AQ; AIR-QUALITY AB Nitrogen dioxide (NO2) is a short-lived atmospheric pollutant that serves as an air quality indicator and is itself a health concern. The Airborne Compact Atmospheric Mapper (ACAM) was flown on board the NASA UC-12 aircraft during the Deriving Information on Surface Conditions from Column and Vertically Resolved Observations Relevant to Air Quality Maryland field campaign in July 2011. The instrument collected hyperspectral remote sensing measurements in the 304-910nm range, allowing daytime observations of several tropospheric pollutants, including nitrogen dioxide (NO2), at an unprecedented spatial resolution of 1.5 x 1.1 km(2). Retrievals of slant column abundance are based on the differential optical absorption spectroscopy method. For the air mass factor computations needed to convert these retrievals to vertical column abundance, we include high-resolution information for the surface reflectivity by using bidirectional reflectance distribution function data from the Moderate Resolution Imaging Spectroradiometer. We use high-resolution simulated vertical distributions of NO2 from the Community Multiscale Air Quality and Global Modeling Initiative models to account for the temporal variation in atmospheric NO2 to retrieve middle and lower tropospheric NO2 columns (NO2 below the aircraft). We compare NO2 derived from ACAM measurements with in situ observations from NASA's P-3B research aircraft, total column observations from the ground-based Pandora spectrometers, and tropospheric column observations from the space-based Ozone Monitoring Instrument. The high-resolution ACAM measurements not only give new insights into our understanding of atmospheric composition and chemistry through observation of subsampling variability in typical satellite and model resolutions, but they also provide opportunities for testing algorithm improvements for forthcoming geostationary air quality missions. C1 [Lamsal, L. N.; Kowalewski, M. G.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21046 USA. [Lamsal, L. N.; Janz, S. J.; Krotkov, N. A.; Pickering, K. E.; Kowalewski, M. G.; Loughner, C. P.; Herman, J. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Spurr, R. J. D.] RT Solut, Cambridge, MA USA. [Loughner, C. P.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Loughner, C. P.] NOAA, Air Resources Lab, College Pk, MD USA. [Crawford, J. H.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Swartz, W. H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Herman, J. R.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. RP Lamsal, LN (reprint author), Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21046 USA.; Lamsal, LN (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM lok.lamsal@nasa.gov OI Krotkov, Nickolay/0000-0001-6170-6750 FU NASA's Earth Venture DISCOVER-AQ project FX We thank two anonymous reviewers for helpful comments that improved the manuscript. We would like to thank Andrew J. Weinheimer from the National Center for Atmospheric Research for making the P-3B data available. The data generated from this study will be made available from NASA's DISCOVER-AQ archive (http://www-air.larc.nasa.gov/missions/discover-aq/dataaccess.htm). The model data and routines used to make figures will be made available from the authors upon request. The work was supported by NASA's Earth Venture DISCOVER-AQ project. NR 81 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 16 PY 2017 VL 122 IS 3 BP 1953 EP 1970 DI 10.1002/2016JD025483 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EN6MX UT WOS:000396119200034 ER PT J AU Nicely, JM Salawitch, RJ Canty, T Anderson, DC Arnold, SR Chipperfield, MP Emmons, LK Flemming, J Huijnen, V Kinnison, DE Lamarque, JF Mao, JQ Monks, SA Steenrod, SD Tilmes, S Turquety, S AF Nicely, Julie M. Salawitch, Ross J. Canty, Timothy Anderson, Daniel C. Arnold, Steve R. Chipperfield, Martyn P. Emmons, Louisa K. Flemming, Johannes Huijnen, Vincent Kinnison, Douglas E. Lamarque, Jean-Francois Mao, Jingqiu Monks, Sarah A. Steenrod, Stephen D. Tilmes, Simone Turquety, Solene TI Quantifying the causes of differences in tropospheric OH within global models SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID VOLATILE ORGANIC-COMPOUNDS; CHEMISTRY TRANSPORT MODEL; BIOMASS BURNING POLLUTION; EARTH SYSTEM MODEL; ATMOSPHERIC CHEMISTRY; OXIDATIVE CAPACITY; METHANE LIFETIME; NEURAL-NETWORKS; OZONE; DEGRADATION AB The hydroxyl radical (OH) is the primary daytime oxidant in the troposphere and provides the main loss mechanism for many pollutants and greenhouse gases, including methane (CH4). Global mean tropospheric OH differs by as much as 80% among various global models, for reasons that are not well understood. We use neural networks (NNs), trained using archived output from eight chemical transport models (CTMs) that participated in the Polar Study using Aircraft, Remote Sensing, Surface Measurements and Models, of Climate, Chemistry, Aerosols and Transport Model Intercomparison Project (POLMIP), to quantify the factors responsible for differences in tropospheric OH and resulting CH4 lifetime (tau(CH4)) between these models. Annual average tau(CH4), for loss by OH only, ranges from 8.0 to 11.6 years for the eight POLMIP CTMs. The factors driving these differences were quantified by inputting 3-D chemical fields from one CTM into the trained NN of another CTM. Across all CTMs, the largest mean differences in tCH4 (Delta tau(CH4)) result from variations in chemical mechanisms (Delta tau(CH4) = 0.46 years), the photolysis frequency (J) of O-3 -> O(D-1) (0.31 years), local O-3 (0.30 years), and CO (0.23 years). The Delta tau(CH4) due to CTM differences in NOx (NO + NO2) is relatively low (0.17 years), although large regional variation in OH between the CTMs is attributed to NOx. Differences in isoprene and J(NO2) have negligible overall effect on globally averaged tropospheric OH, although the extent of OH variations due to each factor depends on the model being examined. This study demonstrates that NNs can serve as a useful tool for quantifying why tropospheric OH varies between global models, provided that essential chemical fields are archived. C1 [Nicely, Julie M.; Salawitch, Ross J.] Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA. [Nicely, Julie M.; Steenrod, Stephen D.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA. [Nicely, Julie M.; Steenrod, Stephen D.] Univ Space Res Assoc, Columbia, MD 21046 USA. [Salawitch, Ross J.; Canty, Timothy; Anderson, Daniel C.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Salawitch, Ross J.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Arnold, Steve R.; Chipperfield, Martyn P.] Univ Leeds, Inst Climate & Atmospher Sci, Sch Earth & Environm, Leeds, W Yorkshire, England. [Chipperfield, Martyn P.] Univ Leeds, Natl Ctr Earth Observat, Leeds, W Yorkshire, England. [Emmons, Louisa K.; Kinnison, Douglas E.; Lamarque, Jean-Francois; Tilmes, Simone] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. [Flemming, Johannes] European Ctr Medium Range Weather Forecasts, Reading, Berks, England. [Huijnen, Vincent] Royal Netherlands Meteorol Inst, De Bilt, Netherlands. [Mao, Jingqiu] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. [Mao, Jingqiu] Univ Alaska Fairbanks, Dept Chem, Fairbanks, AK USA. [Monks, Sarah A.] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO USA. [Monks, Sarah A.] Univ Colorado Boulder, Cooperat Inst Res Environm Sci, Boulder, CO USA. [Turquety, Solene] UPMC Univ Paris 6, Sorbonne Univ, IPSL, Lab Meteorol Dynam, Paris, France. RP Nicely, JM (reprint author), Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA.; Nicely, JM (reprint author), NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA.; Nicely, JM (reprint author), Univ Space Res Assoc, Columbia, MD 21046 USA. EM julie.m.nicely@nasa.gov RI Mao, Jingqiu/F-2511-2010; OI Mao, Jingqiu/0000-0002-4774-9751; Kinnison, Douglas/0000-0002-3418-0834 FU NASA Modeling and Analysis Program; NASA; National Science Foundation; European Union [283576] FX We thank the three anonymous reviewers for providing constructive feedback that led to improvement of this manuscript. We also thank Bryan Duncan for helpful discussions concerning the development of this method. The POLMIP model simulations are available upon request to the authors (julie.m.nicely@nasa.gov). Work conducted at the University of Maryland was supported, in part, by the NASA Modeling and Analysis Program. J.M.N. was also supported by an appointment to the NASA Postdoctoral Program at the NASA Goddard Space Flight Center, administered by Universities Space Research Association under contract with NASA. The National Center for Atmospheric Research is funded by the National Science Foundation. V.H. acknowledges funding by the European Union's Seventh Framework Programme (FP7) for MACC III under grant agreement 283576. NR 72 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 16 PY 2017 VL 122 IS 3 BP 1983 EP 2007 DI 10.1002/2016JD026239 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EN6MX UT WOS:000396119200036 ER PT J AU Abbott, BP Abbott, R Abbott, TD Abernathy, MR Acernese, F Ackley, K Adams, C Adams, T Addesso, P Adhikari, RX Adya, VB Affeldt, C Agathos, M Agatsuma, K Aggarwal, N Aguiar, OD Aiello, L Ain, A Allen, B Allocca, A Altin, PA Ananyeva, A Anderson, SB Anderson, WG Appert, S Arai, K Araya, MC Areeda, JS Arnaud, N Arun, KG Ascenzi, S Ashton, G Ast, M Aston, SM Astone, P Aufmuth, P Aulbert, C Avila-Alvarez, A Babak, S Bacon, P Bader, MKM Baker, PT Baldaccini, F Ballardin, G Ballmer, SW Barayoga, JC Barclay, SE Barish, BC Barker, D Barone, F Barr, B Barsotti, L Barsuglia, M Barta, D Bartlett, J Bartos, I Bassiri, R Basti, A Batch, JC Baune, C Bavigadda, V Bazzan, M Beer, C Bejger, M Belahcene, I Belgin, M Bell, AS Berger, BK Bergmann, G Berry, CPL Bersanetti, D Bertolini, A Betzwieser, J Bhagwat, S Bhandare, R Bilenko, IA Billingsley, G Billman, CR Birch, J Birney, R Birnholtz, O Biscans, S Bisht, A Bitossi, M Biwer, C Bizouard, MA Blackburn, JK Blackman, J Blair, CD Blair, DG Blair, RM Bloemen, S Bock, O Boer, M Bogaert, G Bohe, A Bondu, F Bonnand, R Boom, BA Bork, R Boschi, V Bose, S Bouffanais, Y Bozzi, A Bradaschia, C Brady, PR Braginsky, VB Branchesi, M Brau, JE Briant, T Brillet, A Brinkmann, M Brisson, V Brockill, P Broida, JE Brooks, AF Brown, DA Brown, DD Brown, NM Brunett, S Buchanan, CC Buikema, A Bulik, T Bulten, HJ Buonanno, A Buskulic, D Buy, C Byer, RL Cabero, M Cadonati, L Cagnoli, G Cahillane, C Bustillo, JC Callister, TA Calloni, E Camp, JB Canepa, M Cannon, KC Cao, H Cao, J Capano, CD Capocasa, E Carbognani, F Caride, S Diaz, JC Casentini, C Caudill, S Cavaglia, M Cavalier, F Cavalieri, R Cella, G Cepeda, CB Baiardi, LC Cerretani, G Cesarini, E Chamberlin, SJ Chan, M Chao, S Charlton, P Chassande-Mottin, E Cheeseboro, BD Chen, HY Chen, Y Cheng, HP Chincarini, A Chiummo, A Chmiel, T Cho, HS Cho, M Chow, JH Christensen, N Chu, Q Chua, AJK Chua, S Chung, S Ciani, G Clara, F Clark, JA Cleva, F Cocchieri, C Coccia, E Cohadon, PF Colla, A Collette, CG Cominsky, L Constancio, M Conti, L Cooper, SJ Corbitt, TR Cornish, N Corsi, A Cortese, S Costa, CA Coughlin, MW Coughlin, SB Coulon, JP Countryman, ST Couvares, P Covas, PB Cowan, EE Coward, DM Cowart, MJ Coyne, DC Coyne, R Creighton, JDE Creighton, TD Cripe, J Crowder, SG Cullen, TJ Cumming, A Cunningham, L Cuoco, E Dal Canton, T Danilishin, SL D'Antonio, S Danzmann, K Dasgupta, A Costa, CFD Dattilo, V Dave, I Davier, M Davies, GS Davis, D Daw, EJ Day, B Day, R De, S Debra, D Debreczeni, G Degallaix, J De Laurentis, M Deleglise, S Del Pozzo, W Denker, T Dent, T Dergachev, V De Rosa, R DeRosa, RT DeSalvo, R Devenson, J Devine, RC Dhurandhar, S Diaz, MC Di Fiore, L Di Giovanni, M Di Girolamo, T Di Lieto, A Di Pace, S Di Palma, I Di Virgilio, A Doctor, Z Dolique, V Donovan, F Dooley, KL Doravari, S 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Schofield, R. M. S. Schoenbeck, A. Schreiber, E. Schuette, D. Schutz, B. F. Schwalbe, S. G. Scott, J. Scott, S. M. Sellers, D. Sengupta, A. S. Sentenac, D. Sequino, V. Sergeev, A. Setyawati, Y. Shaddock, D. A. Shaffer, T. J. Shahriar, M. S. Shapiro, B. Shawhan, P. Sheperd, A. Shoemaker, D. H. Shoemaker, D. M. Siellez, K. Siemens, X. Sieniawska, M. Sigg, D. Silva, A. D. Singer, A. Singer, L. P. Singh, A. Singh, R. Singhal, A. Sintes, A. M. Slagmolen, B. J. J. Smith, B. Smith, J. R. Smith, R. J. E. Son, E. J. Sorazu, B. Sorrentino, F. Souradeep, T. Spencer, A. P. Srivastava, A. K. Staley, A. Steinke, M. Steinlechner, J. Steinlechner, S. Steinmeyer, D. Stephens, B. C. Stevenson, S. P. Stone, R. Strain, K. A. Straniero, N. Stratta, G. Strigin, S. E. Sturani, R. Stuver, A. L. Summerscales, T. Z. Sun, L. Sunil, S. Sutton, P. J. Swinkels, B. L. Szczepanczyk, M. J. Tacca, M. Talukder, D. Tanner, D. B. Tapai, M. Taracchini, A. Taylor, R. Theeg, T. Thomas, E. G. Thomas, M. Thomas, P. Thorne, K. A. Thrane, E. Tippens, T. Tiwari, S. Tiwari, V. Tokmakov, K. V. Toland, K. Tomlinson, C. Tonelli, M. Tornasi, Z. Torrie, C. I. Torya, D. Travasso, F. Traylor, G. Trifiro, D. Trinastic, J. Tringali, M. C. Trozzo, L. Tse, M. Tso, R. Turconi, M. Tuyenbayev, D. Ugolini, D. Unnikrishnan, C. S. Urban, A. L. Usman, S. A. Vahlbruch, H. Vajente, G. Valdes, G. van Bakel, N. van Beuzekom, M. van den Brand, J. F. J. Van Den Broeck, C. Vander-Hyde, D. C. van der Schaaf, L. van Heijningen, J. V. van Veggel, A. A. Vardaro, M. Varma, V. Vass, S. Vasuth, M. Vecchio, A. Vedovato, G. Veitch, J. Veitch, P. J. Venkateswara, K. Venugopalan, G. Verkindt, D. Vetrano, F. Vicere, A. Viets, A. D. Vinciguerra, S. Vine, D. J. Vinet, J. -Y. Vitale, S. Vo, T. Vocca, H. Vorvick, C. Voss, D. V. Vousden, W. D. Vyatchanin, S. P. Wade, A. R. Wade, L. E. Wade, M. Walker, M. Wallace, L. Walsh, S. Wang, G. Wang, H. Wang, M. Wang, Y. Ward, R. L. Warner, J. Was, M. Watchi, J. Weaver, B. Wei, L. -W. Weinert, M. Weinstein, A. J. Weiss, R. Wen, L. Wessels, P. Westphal, T. Wette, K. Whelan, J. T. Whiting, B. F. Whittle, C. Williams, D. Williams, R. D. Williamson, A. R. Willis, J. L. Willke, B. Wimmer, M. H. Winkler, W. Wipf, C. C. Wittel, H. Woan, G. Woehler, J. Worden, J. Wright, J. L. Wu, D. S. Wu, G. Yam, W. Yamamoto, H. Yancey, C. C. Yap, M. J. Yu, Hang Yu, Haocun Yvert, M. Zadrozny, A. Zangrando, L. Zanolin, M. Zendri, J. -P. Zevin, M. Zhang, L. Zhang, M. Zhang, T. Zhang, Y. Zhao, C. Zhou, M. Zhou, Z. Zhu, S. J. Zhu, X. J. Zucker, M. E. Zweizig, J. CA LIGO Sci Collaboration VIRGO Collaboration TI All-sky search for short gravitational-wave bursts in the first Advanced LIGO run SO PHYSICAL REVIEW D LA English DT Article AB We present the results from an all-sky search for short-duration gravitational waves in the data of the first run of the Advanced LIGO detectors between September 2015 and January 2016. The search algorithms use minimal assumptions on the signal morphology, so they are sensitive to a wide range of sources emitting gravitational waves. The analyses target transient signals with duration ranging from milliseconds to seconds over the frequency band of 32 to 4096 Hz. The first observed gravitational-wave event, GW150914, has been detected with high confidence in this search; the other known gravitational-wave event, GW151226, falls below the search's sensitivity. Besides GW150914, all of the search results are consistent with the expected rate of accidental noise coincidences. Finally, we estimate rate-density limits for a broad range of non-binary-black-hole transient gravitational-wave sources as a function of their gravitational radiation emission energy and their characteristic frequency. These rate-density upper limits are stricter than those previously published by an order of magnitude. C1 [Abbott, B. P.; Abbott, R.; Abbott, T. D.; Adhikari, R. 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[Melatos, A.] Univ Melbourne, Parkville, Vic 3010, Australia. [Mikhailov, E. E.; Rew, H.; Zhang, M.] Coll William & Mary, Williamsburg, VA 23187 USA. [Mirshekari, S.; Sturani, R.] Univ Estadual Paulista, Inst Fis Teor, ICTP, South Amer Inst Fundamental Res, BR-01140070 Sao Paulo, SP, Brazil. [Ogin, G. H.] Whitman Coll, 345 Boyer Ave, Walla Walla, WA 99362 USA. [Pedurand, R.] Univ Lyon, F-69361 Lyon, France. [Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA. [Rosinska, D.] Univ Zielona Gora, Janusz Gil Inst Astron, PL-65265 Zielona Gora, Poland. [Sakellariadou, M.] Univ London, Kings Coll London, London WC2R 2LS, England. [Samajdar, A.] IISER Kolkata, Mohanpur 741252, W Bengal, India. [Sengupta, A. S.] Indian Inst Technol, Ahmadabad 382424, Gujarat, India. [Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA. [Trozzo, L.] Univ Siena, I-53100 Siena, Italy. [Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA. [Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA. [Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA. RP Abbott, BP (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA. RI Gemme, Gianluca/C-7233-2008; Sergeev, Alexander/F-3027-2017; Harms, Jan/J-4359-2012; Leonardi, Matteo/G-9694-2015; Rocchi, Alessio/O-9499-2015; OI Gemme, Gianluca/0000-0002-1127-7406; Rocchi, Alessio/0000-0002-1382-9016; Davies, Gareth/0000-0002-4289-3439 FU Australian Research Council; European Gravitational Observatory (EGO) consortium; Council of Scientific and Industrial Research of India; Department of Science and Technology, India; Science & Engineering Research Board, India; Ministry of Human Resource Development, India; Spanish Ministerio de Economia y Competitividad of the Govern de les Illes Balears; Conselleria d'Economia i Competitivitat of the Govern de les Illes Balears; Conselleria d'Educacio, Cultura i Universitats of the Govern de les Illes Balears; National Science Centre of Poland; European Commission; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; Hungarian Scientific Research Fund; Lyon Institute of Origins; National Research Foundation of Korea; Industry Canada; Province of Ontario through the Ministry of Economic Development and Innovation; Natural Science and Engineering Research Council Canada; Canadian Institute for Advanced Research; Brazilian Ministry of Science, Technology, and Innovation; Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP); Russian Foundation for Basic Research; Leverhulme Trust; Research Corporation; Ministry of Science and Technology, Taiwan; Kavli Foundation FX The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS), and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the European Gravitational Observatory (EGO) consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, Department of Science and Technology, India, Science & Engineering Research Board, India; Ministry of Human Resource Development, India; the Spanish Ministerio de Economia y Competitividad, the Conselleria d'Economia i Competitivitat and Conselleria d'Educacio, Cultura i Universitats of the Govern de les Illes Balears; the National Science Centre of Poland; the European Commission; the Royal Society; the Scottish Funding Council; the Scottish Universities Physics Alliance; the Hungarian Scientific Research Fund; the Lyon Institute of Origins; the National Research Foundation of Korea; Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation; the Natural Science and Engineering Research Council Canada; Canadian Institute for Advanced Research; the Brazilian Ministry of Science, Technology, and Innovation, Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP); Russian Foundation for Basic Research; the Leverhulme Trust; the Research Corporation; Ministry of Science and Technology, Taiwan; and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS, and the State of Niedersachsen/Germany for the provision of computational resources. NR 36 TC 0 Z9 0 U1 3 U2 3 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 FEB 16 PY 2017 VL 95 IS 4 AR 042003 DI 10.1103/PhysRevD.95.042003 PG 14 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA EK7FS UT WOS:000394092200001 ER PT J AU Blum, LW Bonnell, JW Agapitov, O Paulson, K Kletzing, C AF Blum, L. W. Bonnell, J. W. Agapitov, O. Paulson, K. Kletzing, C. TI EMIC wave scale size in the inner magnetosphere: Observations from the dual Van Allen Probes SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID RELATIVISTIC ELECTRON-PRECIPITATION; MAGNETIC LOCAL TIME; RADIATION BELTS; JANUARY 2013; PULSATIONS; DISTRIBUTIONS; PROTONS; EVENT AB Estimating the spatial scales of electromagnetic ion cyclotron (EMIC) waves is critical for quantifying their overall scattering efficiency and effects on thermal plasma, ring current, and radiation belt particles. Using measurements from the dual Van Allen Probes in 2013-2014, we characterize the spatial and temporal extents of regions of EMIC wave activity and how these depend on local time and radial distance within the inner magnetosphere. Observations are categorized into three types-waves observed by only one spacecraft, waves measured by both spacecraft simultaneously, and waves observed by both spacecraft with some time lag. Analysis reveals that dayside (and H+ band) EMIC waves more frequently span larger spatial areas, while nightside (and He+ band) waves are more often localized but can persist many hours. These investigations give insight into the nature of EMIC wave generation and support more accurate quantification of their effects on the ring current and outer radiation belt. C1 [Blum, L. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bonnell, J. W.; Agapitov, O.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Paulson, K.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Kletzing, C.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. RP Blum, LW (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM lauren.w.blum@nasa.gov OI AGAPITOV, OLEKSIY/0000-0001-6427-1596; Paulson, Kristoff/0000-0002-5699-090X FU NSF Atmospheric and Geospace Sciences (AGS) Postdoctoral Research Fellowship; NASA [NNX16AF85G]; JHU/APL [922613]; Van Allen Probes EMFISIS team FX This work was supported by the NSF Atmospheric and Geospace Sciences (AGS) Postdoctoral Research Fellowship, NASA grant NNX16AF85G, JHU/APL contract 922613 (RBSP-EFW), and the Van Allen Probes EMFISIS team. Van Allen Probes EMFISIS data can be found at http://emfisis.physics.uiowa.edu/data/index. NR 40 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD FEB 16 PY 2017 VL 44 IS 3 BP 1227 EP 1233 DI 10.1002/2016GL072316 PG 7 WC Geosciences, Multidisciplinary SC Geology GA EN6LH UT WOS:000396115000005 ER PT J AU Sori, MM Byrne, S Bland, MT Bramson, AM Ermakov, AI Hamilton, CW Otto, KA Ruesch, O Russell, CT AF Sori, Michael M. Byrne, Shane Bland, Michael T. Bramson, Ali M. Ermakov, Anton I. Hamilton, Christopher W. Otto, Katharina A. Ruesch, Ottaviano Russell, Christopher T. TI The vanishing cryovolcanoes of Ceres SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID WATER ICE; DIFFERENTIATION; SATELLITES; TOPOGRAPHY; EVOLUTION; RATES AB Ahuna Mons is a 4 km tall mountain on Ceres interpreted as a geologically young cryovolcanic dome. Other possible cryovolcanic features are more ambiguous, implying that cryovolcanism is only a recent phenomenon or that other cryovolcanic structures have been modified beyond easy identification. We test the hypothesis that Cerean cryovolcanic domes viscously relax, precluding ancient domes from recognition. We use numerical models to predict flow velocities of Ahuna Mons to be 10-500 m/Myr, depending upon assumptions about ice content, rheology, grain size, and thermal parameters. Slower flow rates in this range are sufficiently fast to induce extensive relaxation of cryovolcanic structures over 10(8)-10(9) years, but gradual enough for Ahuna Mons to remain identifiable today. Positive topographic features, including a tholus underlying Ahuna Mons, may represent relaxed cryovolcanic structures. A composition for Ahuna Mons of >40% ice explains the observed distribution of cryovolcanic structures because viscous relaxation renders old cryovolcanoes unrecognizable. C1 [Sori, Michael M.; Byrne, Shane; Bramson, Ali M.; Hamilton, Christopher W.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Bland, Michael T.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Ermakov, Anton I.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Otto, Katharina A.] German Aerosp Ctr DLR, Berlin, Germany. [Ruesch, Ottaviano] NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD USA. [Russell, Christopher T.] Univ Calif Los Angeles, Earth Planetary & Space Sci, Los Angeles, CA USA. RP Sori, MM (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. EM michael.sori@gmail.com OI Russell, Christopher/0000-0003-1639-8298 NR 42 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD FEB 16 PY 2017 VL 44 IS 3 BP 1243 EP 1250 DI 10.1002/2016GL072319 PG 8 WC Geosciences, Multidisciplinary SC Geology GA EN6LH UT WOS:000396115000007 ER PT J AU Koike, M Sugiura, N Takahata, N Ishida, A Sano, Y AF Koike, M. Sugiura, N. Takahata, N. Ishida, A. Sano, Y. TI U-Pb and Hf-W dating of young zircon in mesosiderite Asuka 882023 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID EARLY CORE FORMATION; SOLAR-SYSTEM; EUCRITE ZIRCON; PARENT BODY; ESTHERVILLE MESOSIDERITE; ISOTOPE SYSTEMATICS; OXYGEN-ISOTOPE; TRACE-ELEMENT; TH-PB; HISTORY AB Mesosiderites are unique stony-iron meteorites, composed of eucrite-like silicates and Fe-Ni metals. Their formation, including silicate-metal mixing and metamorphisms, provides important insights into early planetary processes in the inner solar system. This report describes the first in situ U-Pb and Hf-W dating of zircon in a mesosiderite Asuka 882023. The U-Pb (4502 +/- 75 Ma) and Hf-W (4532.8 + 5.7/-10.5 Ma) ages may represent timing of the zircon formation, which is considerably younger than crustal differentiation of the parent body. This evidence, combined with earlier studies of chronology, implies that mesosiderites were reheated at 4530-4520 Ma, clearly after the silicate-metal mixing. C1 [Koike, M.; Takahata, N.; Ishida, A.; Sano, Y.] Univ Tokyo, Atmosphere & Ocean Res Inst, Tokyo, Japan. [Sugiura, N.] Univ Tokyo, Dept Earth & Planetary Sci, Tokyo, Japan. [Ishida, A.] Univ Wisconsin, NASA Astrobiol Inst, Dept Geosci, Madison, WI USA. RP Koike, M (reprint author), Univ Tokyo, Atmosphere & Ocean Res Inst, Tokyo, Japan. EM mizuho_k@aori.u-tokyo.ac.jp FU JSPS KAKENHI [16J07403, 26106005] FX The thin section of Asuka 882023 analyzed for this study was provided from National Institute of Polar Research, Tokyo, Japan. This work was partly supported by JSPS KAKENHI grants 16J07403 to M.K. and 26106005 to N.T. Constructive and important reviews by A. Rubin and an anonymous reviewer and the editorial efforts by J. Ritsema helped to improve the manuscript. They are gratefully acknowledged. Supporting data are included as two tables in the supporting information (Tables S1 and S2). NR 52 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 FEB 16 PY 2017 VL 44 IS 3 BP 1251 EP 1259 DI 10.1002/2016GL071609 PG 9 WC Geosciences, Multidisciplinary SC Geology GA EN6LH UT WOS:000396115000008 ER PT J AU Huang, MH Fielding, EJ Liang, CR Milillo, P Bekaert, D Dreger, D Salzer, J AF Huang, Mong-Han Fielding, Eric J. Liang, Cunren Milillo, Pietro Bekaert, David Dreger, Douglas Salzer, Jacqueline TI Coseismic deformation and triggered landslides of the 2016 M-w 6.2 Amatrice earthquake in Italy SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CENTRAL APENNINES; SURFACE DISPLACEMENT; GEODETIC DATA; HECTOR MINE; CALIFORNIA; INVERSION; AREA; GPS AB The Central Apennines in Italy have had multiple moderate-size but damaging shallow earthquakes. In this study, we optimize the fault geometry and invert for fault slip based on coseismic GPS and interferometric synthetic aperture radar (InSAR) for the 2016 M-w 6.2 Amatrice earthquake in Italy. Our results show that nearly all the fault slip occurred between 3 and 6 km depth but extends 20 km along strike. There was less than 4 cm static surface displacement at the town Amatrice where the most devastating damage occurred. Landslides triggered by earthquake ground shaking are not uncommon, but triggered landslides with submeter movement are challenging to be observed in the field. We find evidence of coseismically triggered deep-seated landslides northwest and northeast of the epicenter where coseismic peak ground acceleration was estimated >0.5 g. By combining ascending and descending InSAR data, we are able to estimate the landslide thickness as at least 100 and 80 m near Monte Vettore and west of Castelluccio, respectively. The landslide near Monte Vettore terminates on the preexisting fault Monte Vettore Fault (MVEF) scarp. Our results imply that the long-term fault slip rate of MVEF estimated based on paleoseismic studies could potentially have errors due to triggered landslides from nearby earthquake events. C1 [Huang, Mong-Han; Fielding, Eric J.; Liang, Cunren; Milillo, Pietro; Bekaert, David] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Dreger, Douglas] Univ Calif Berkeley, Berkeley Seismol Lab, Berkeley, CA 94720 USA. [Salzer, Jacqueline] GFZ German Res Ctr Geosci, Phys Earthquakes & Volcanoes, Potsdam, Germany. RP Huang, MH (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Mong-Han.Huang@jpl.nasa.gov OI Huang, Mong-Han/0000-0003-2331-3766; Bekaert, David/0000-0002-0408-0488; Milillo, Pietro/0000-0002-1171-3976 FU NASA Earth Surface and Interior focus area; NASA Postdoctoral Program at the Jet Propulsion Laboratory FX We thank an anonymous reviewer for giving insightful comments that improved the original manuscript. The Sentinel-1 images contain modified Copernicus data. Original ALOS-2 data are copyright by Japan Aerospace Exploration Agency (JAXA) and were provided under JAXA ALOS RA-4 projects (S.H. Yun) and P1372 (E. Fielding). COSMO-SkyMed products were processed by JPL under license from ASI; Original COSMO-SkyMed Productsc ASI-Agenzia Spaziale Italiana-(2016). TanDEM-X IDEM data were provided by Deutsches Zentrum fur Luft- und Raumfahrt (DLR) under proposal IDEM_CALVAL0052. The geologic map of Lazio Region is from www.dati.lazio.it (last data accessed 7 September 2016), and the geologic map of Marche region is from www.ambiente.marche.it (last data accessed 7 September 2016). Aftershocks relocation data are from the ISIDE INGV database. The Sentinel ascending interferogram was processed by the JPL Advanced Rapid Imaging and Analysis (ARIA) Center. We thank INGV for making the GPS measurements publicly available. The interferograms and the fault model are available upon request to the corresponding author. Part of this research was supported by the NASA Earth Surface and Interior focus area and performed at the Jet Propulsion Laboratory, California Institute of Technology. M.-H. Huang, C. Liang, and P. Milillo are supported by appointments to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by the Universities Space and Research Association through a contract with NASA. NR 38 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD FEB 16 PY 2017 VL 44 IS 3 BP 1266 EP 1274 DI 10.1002/2016GL071687 PG 9 WC Geosciences, Multidisciplinary SC Geology GA EN6LH UT WOS:000396115000010 ER PT J AU Marshall, ST Funning, GJ Krueger, HE Owen, SE Loveless, JP AF Marshall, Scott T. Funning, Gareth J. Krueger, Hannah E. Owen, Susan E. Loveless, John P. TI Mechanical models favor a ramp geometry for the Ventura-pitas point fault, Californiae SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID LOS-ANGELES BASIN; SAN-ANDREAS FAULT; TECTONIC BOUNDARY-CONDITIONS; WESTERN TRANSVERSE RANGES; SOUTHERN-CALIFORNIA; SEISMIC HAZARD; SLIP RATES; WENCHUAN EARTHQUAKE; STRAIN ACCUMULATION; 1994 NORTHRIDGE AB Recent investigations have provided new and significantly revised constraints on the subsurface structure of the Ventura-Pitas Point fault system in southern California; however, few data directly constrain fault surfaces below similar to 6 km depth. Here, we use geometrically complex three-dimensional mechanical models driven by current geodetic strain rates to test two proposed subsurface models of the fault system. We find that the model that incorporates a ramp geometry for the Ventura-Pitas Point fault better reproduces both the regional long term geologic slip rate data and interseismic GPS observations of uplift in the Santa Ynez Mountains. The model-calculated average reverse slip rate for the Ventura-Pitas Point fault is 3.5 +/- 0.3 mm/yr, although slip rates are spatially variable on the fault surface with > 8 mm/yr predicted on portions of the lower ramp section at depth. C1 [Marshall, Scott T.; Krueger, Hannah E.] Appalachian State Univ, Dept Geol, Boone, NC 28608 USA. [Funning, Gareth J.] Univ Calif Riverside, Dept Earth Sci, Riverside, CA 92521 USA. [Owen, Susan E.] Jet Prop Lab, Pasadena, CA USA. [Loveless, John P.] Smith Coll, Dept Geosci, Northampton, MA 01063 USA. RP Marshall, ST (reprint author), Appalachian State Univ, Dept Geol, Boone, NC 28608 USA. EM marshallst@appstate.edu OI Marshall, Scott/0000-0001-8879-6514 FU Southern California Earthquake Center; NSF [EAR-1033462]; USGS [G12AC20038] FX This work benefitted from constructive reviews by W. Ashley Griffith and an anonymous reviewer. The authors would like to thank Judith Hubbard, John Shaw, and Andreas Plesch for sharing their three-dimensional model of the Ventura-Pitas Point fault system, creating an early version of the no ramp model geometry, and sharing these models the via the web. We thank Craig Nicholson for guidance in creating the final no ramp model geometry. Zhen Liu and Angelyn Moore provided help with GPS time series data issues, Christian Walls assisted in identifying GPS sites that are recording non-tectonic motions, and Hugh Harper assisted with fault meshing. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This work was supported by the Southern California Earthquake Center. SCEC is funded by NSF Cooperative Agreement EAR-1033462 & USGS Cooperative Agreement G12AC20038. This is SCEC contribution #7073. All figures were produced with Generic Mapping Tools [Wessel et al., 2013]. NR 49 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD FEB 16 PY 2017 VL 44 IS 3 BP 1311 EP 1319 DI 10.1002/2016GL072289 PG 9 WC Geosciences, Multidisciplinary SC Geology GA EN6LH UT WOS:000396115000015 ER PT J AU Millan, R Rignot, E Bernier, V Morlighem, M Dutrieux, P AF Millan, Romain Rignot, Eric Bernier, Vincent Morlighem, Mathieu Dutrieux, Pierre TI Bathymetry of the Amundsen Sea Embayment sector of West Antarctica from Operation IceBridge gravity and other data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID PINE ISLAND GLACIER; ICE-SHEET; THWAITES GLACIER; BENEATH; SHELF; RETREAT AB We employ airborne gravity data from NASA's Operation IceBridge collected in 2009-2014 to infer the bathymetry of sub-ice shelf cavities in front of Pine Island, Thwaites, Smith, and Kohler glaciers, West Antarctica. We use a three-dimensional inversion constrained by multibeam echo sounding data offshore and bed topography from a mass conservation reconstruction on land. The seamless bed elevation data refine details of the Pine Island sub-ice shelf cavity, a slightly thinner cavity beneath Thwaites, and previously unknown deep (> 1200 m) channels beneath the Crosson and Dotson ice shelves that shallow (500 m and 750 m, respectively) near the ice shelf fronts. These sub-ice shelf channels define the natural pathways for warm, circumpolar deep water to reach the glacier grounding lines, melt the ice shelves from below, and constrain the pattern of past and future glacial retreat. C1 [Millan, Romain; Rignot, Eric; Bernier, Vincent; Morlighem, Mathieu] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Rignot, Eric] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Dutrieux, Pierre] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. RP Millan, R (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. EM millanr1@uci.edu OI Rignot, Eric/0000-0002-3366-0481; Dutrieux, Pierre/0000-0002-8066-934X FU National Aeronautics and Space Administration's Cryosphere Science Program; Operation IceBridge Mission; Interdisciplinary Science program at the University of California Irvine and at Caltech's Jet Propulsion Laboratory; NASA FX This work was funded by grants from the National Aeronautics and Space Administration's Cryosphere Science Program, Operation IceBridge Mission, and Interdisciplinary Science program at the University of California Irvine and at Caltech's Jet Propulsion Laboratory. We thank the NASA-funded OIB instrument team for their achievements in collecting OIB data pole-to-pole since 2009 and making this kind of study possible. We also thank A. Muto and K. Tinto for useful discussions at the project inception and P. Dutrieux, L. Peters, A. Muto, and S. Anandakrishnan for sharing the AUV and seismic data. The bed topography described herein is available from the authors and will be posted at NSIDC. NR 29 TC 0 Z9 0 U1 3 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD FEB 16 PY 2017 VL 44 IS 3 BP 1360 EP 1368 DI 10.1002/2016GL072071 PG 9 WC Geosciences, Multidisciplinary SC Geology GA EN6LH UT WOS:000396115000021 ER PT J AU Heymann, J Reuter, M Buchwitz, M Schneising, O Bovensmann, H Burrows, JP Massart, S Kaiser, JW Crisp, D AF Heymann, J. Reuter, M. Buchwitz, M. Schneising, O. Bovensmann, H. Burrows, J. P. Massart, S. Kaiser, J. W. Crisp, D. TI CO2 emission of Indonesian fires in 2015 estimated from satellite-derived atmospheric CO2 concentrations SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID RETRIEVAL ALGORITHM; XCO2 RETRIEVALS; SOUTHEAST-ASIA AB Indonesia experienced an exceptional number of fires in 2015 as a result of droughts related to the recent El Nio event and human activities. These fires released large amounts of carbon dioxide (CO2) into the atmosphere. Emission databases such as the Global Fire Assimilation System version 1.2 and the Global Fire Emission Database version 4s estimated the CO2 emission to be approximately 1100 MtCO(2) in the time period from July to November 2015. This emission was indirectly estimated by using parameters like burned area, fire radiative power, and emission factors. In the study presented in this paper, we estimate the Indonesian fire CO2 emission by using the column-averaged dry air mole fraction of CO2, XCO2, derived from measurements of the Orbiting Carbon Observatory-2 satellite mission. The estimated CO2 emission is 748 +/- 209 MtCO(2), which is about 30% lower than provided by the emission databases. C1 [Heymann, J.; Reuter, M.; Buchwitz, M.; Schneising, O.; Bovensmann, H.; Burrows, J. P.] Univ Bremen, Inst Environm Phys, Bremen, Germany. [Massart, S.] European Ctr Medium Range Weather Forecasts, Reading, Berks, England. [Kaiser, J. W.] Max Planck Inst Chem, Mainz, Germany. [Crisp, D.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Heymann, J (reprint author), Univ Bremen, Inst Environm Phys, Bremen, Germany. EM heymann@iup.physik.uni-bremen.de OI Burrows, John Philip/0000-0002-6821-5580; Bovensmann, Heinrich/0000-0001-8882-4108; Buchwitz, Michael/0000-0001-7616-1837 FU ESA (Living Planet Fellowship project CARBOFIRES); ESA (GHG-CCI project); EU Copernicus (Copernicus Atmosphere Monitoring Service); State and the University of Bremen FX We thank NASA for making available the OCO-2 L2 data product. We are also grateful to ECMWF for the meteorological, GFAS, and CO2 model data. The CarbonTracker CT-NRT results have been obtained from NOAA ESRL, Boulder, CO, USA, from the website at http://carbontracker.noaa.gov. This work is funded in part by ESA (Living Planet Fellowship project CARBOFIRES and GHG-CCI project), EU Copernicus (Copernicus Atmosphere Monitoring Service), and the State and the University of Bremen. NR 21 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD FEB 16 PY 2017 VL 44 IS 3 BP 1537 EP 1544 DI 10.1002/2016GL072042 PG 8 WC Geosciences, Multidisciplinary SC Geology GA EN6LH UT WOS:000396115000041 ER PT J AU Luus, KA Commane, R Parazoo, NC Benmergui, J Euskirchen, ES Frankenberg, C Joiner, J Lindaas, J Miller, CE Oechel, WC Zona, D Wofsy, S Lin, JC AF Luus, K. A. Commane, R. Parazoo, N. C. Benmergui, J. Euskirchen, E. S. Frankenberg, C. Joiner, J. Lindaas, J. Miller, C. E. Oechel, W. C. Zona, D. Wofsy, S. Lin, J. C. TI Tundra photosynthesis captured by satellite-observed solar-induced chlorophyll fluorescence SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID PERMAFROST CARBON; COVER PRODUCTS; GROWING-SEASON; CLIMATE-CHANGE; VEGETATION; ECOSYSTEM; CYCLE; SNOW; SIMULATIONS; PHENOLOGY AB Accurately quantifying the timing and magnitude of respiration and photosynthesis by high-latitude ecosystems is important for understanding how a warming climate influences global carbon cycling. Data-driven estimates of photosynthesis across Arctic regions often rely on satellite-derived enhanced vegetation index (EVI); we find that satellite observations of solar-induced chlorophyll fluorescence (SIF) provide a more direct proxy for photosynthesis. We model Alaskan tundra CO2 cycling (2012-2014) according to temperature and shortwave radiation and alternately input EVI or SIF to prescribe the annual seasonal cycle of photosynthesis. We find that EVI-based seasonality indicates spring "green-up" to occur 9 days prior to SIF-based estimates, and that SIF-based estimates agree with aircraft and tower measurements of CO2. Adopting SIF, instead of EVI, for modeling the seasonal cycle of tundra photosynthesis can result in more accurate estimates of growing season duration and net carbon uptake by arctic vegetation. C1 [Luus, K. A.] Ctr Appl Data Analyt Res, Dublin, Ireland. [Commane, R.; Benmergui, J.; Lindaas, J.; Wofsy, S.] Harvard Univ, John A Paulson Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Parazoo, N. C.; Miller, C. E.] Jet Prop Lab, Pasadena, CA USA. [Euskirchen, E. S.] Univ Alaska Fairbanks, Inst Arctic Biol, Fairbanks, AK USA. [Frankenberg, C.] CALTECH, Environm Sci & Engn, Pasadena, CA 91125 USA. [Joiner, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Lindaas, J.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Oechel, W. C.; Zona, D.] San Diego State Univ, Dept Biol, San Diego, CA 92182 USA. [Oechel, W. C.] Univ Exeter, Coll Life & Environm Sci, Exeter, Devon, England. [Zona, D.] Univ Sheffield, Dept Anim & Plant Sci, Sheffield, S Yorkshire, England. [Lin, J. C.] Univ Utah, Dept Atmospher Sci, Salt Lake City, UT USA. RP Luus, KA (reprint author), Ctr Appl Data Analyt Res, Dublin, Ireland. EM kristina.luus@gmail.com OI Lindaas, Jakob/0000-0003-1872-3162; Commane, Roisin/0000-0003-1373-1550 FU NSERC; NASA [NNX16AF94A]; National Aeronautics and Space Administration; National Science Foundation Collaborative Research on Carbon, Water, and Energy Balance of the Arctic Landscape at Flagship Observatories in Alaska and Siberia; CARVE subcontract [1443296]; Division of Polar Programs of the National Science Foundation (NSF) [1204263] FX The authors wish to acknowledge contributions from the OCO-2 and GOME-2 teams. Funding from NSERC through a Postdoctoral Fellowship (KAL) is gratefully acknowledged. Some of the research described in this paper was performed for the Carbon in Arctic Reservoirs Vulnerability Experiment (CARVE), an Earth Ventures (EV-1) investigation, under contract with NASA. A portion of the research described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Data from Imnavait, Alaska, were provided by E. Euskirchen, C. Edgar, and M.S. Bret-Harte and collected through a grant from the National Science Foundation Collaborative Research on Carbon, Water, and Energy Balance of the Arctic Landscape at Flagship Observatories in Alaska and Siberia. Eddy covariance and meteorological observations from Barrow and Atqasuk were provided by W. Oechel, D. Zona, and the Global Change Research Group. Funding and support were provided by CARVE subcontract 1443296, under contract with NASA, and by the NASA grant, award NNX16AF94A, Arctic-Boreal Vulnerability Experiment (ABoVE) to W. Oechel and by Division of Polar Programs of the National Science Foundation (NSF) (award 1204263) to D. Zona. NCEP Reanalysis data were provided by the NOAA/OAR/ESRL PSD, Boulder, Colorado, USA, from their Web site at http://www.esrl.noaa.gov/psd/. The MODIS MOD13A1, MOD10A2, and MOD09A1 data products were retrieved from the online Data Pool, courtesy of the NASA Land Processes Distributed Active Archive Center (LP DAAC), USGS/Earth Resources Observation and Science (EROS) Center, Sioux Falls, South Dakota, https://lpdaac.usgs.gov/data_access/data_pool. MOD17A2 GPP was provided by the Numerical Terradynamic Simulation Group (NTSG) at the University of Montana. We wish to thank the Oak Ridge National Lab for hosting open access to all Alaskan PolarVPRM outputs presented here, which can be downloaded from Luus and Lin [2016]. NR 58 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 FEB 16 PY 2017 VL 44 IS 3 BP 1564 EP 1573 DI 10.1002/2016GL070842 PG 10 WC Geosciences, Multidisciplinary SC Geology GA EN6LH UT WOS:000396115000044 ER PT J AU Ladino, LA Korolev, A Heckman, I Wolde, M Fridlind, AM Ackerman, AS AF Ladino, Luis A. Korolev, Alexei Heckman, Ivan Wolde, Mengistu Fridlind, Ann M. Ackerman, Andrew S. TI On the role of ice-nucleating aerosol in the formation of ice particles in tropical mesoscale convective systems SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MIXED-PHASE CLOUDS; LOW RADAR REFLECTIVITY; GLOBAL CLIMATE MODEL; OPTICAL ARRAY PROBES; IN-SITU; ATMOSPHERIC AEROSOLS; BIOLOGICAL PARTICLES; DEEP CONVECTION; CIRRUS CLOUDS; WATER-CONTENT AB Over the decades, the cloud physics community has debated the nature and role of aerosol particles in ice initiation. The present study shows that the measured concentration of ice crystals in tropical mesoscale convective systems exceeds the concentration of ice nucleating particles (INPs) by several orders of magnitude. The concentration of INPs was assessed from the measured aerosol particle concentration in the size range of 0.5 to 1 mu m. The observations from this study suggest that primary ice crystals formed on INPs make only a minor contribution to the total concentration of ice crystals in tropical mesoscale convective systems. This is found by comparing the predicted INP number concentrations with in situ ice particle number concentrations. The obtained measurements suggest that ice multiplication is the likely explanation for the observed high concentrations of ice crystals in this type of convective system. C1 [Ladino, Luis A.; Korolev, Alexei; Heckman, Ivan] Environm & Climate Change Canada, Cloud Phys & Severe Weather Res Sect, Toronto, ON, Canada. [Ladino, Luis A.] Univ Nacl Autonoma Mexico, Ctr Ciencias Atmosfera, Mexico City, DF, Mexico. [Wolde, Mengistu] Natl Res Council Canada, Flight Res Lab, Ottawa, ON, Canada. [Fridlind, Ann M.; Ackerman, Andrew S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Korolev, A (reprint author), Environm & Climate Change Canada, Cloud Phys & Severe Weather Res Sect, Toronto, ON, Canada. EM alexei.korolev@canada.ca OI Korolev, Alexei/0000-0003-3877-8419 FU Transport Canada; Federal Aviation Administration; NRC RAIR program; Natural Sciences and Engineering Research Council of Canada (NSERC); NASA Modeling and Analysis Program FX ECCC participation in the HIWC program was supported by Transport Canada and the Federal Aviation Administration. The NRC RAIR program has generously provided partial funding for this project. The authors are grateful for the technical support provided during the data collection period and would like to thank Mohammed Wasey, Michel Harwood, Jason Iwachow (ECCC); Anne Marie McDonald (ECCC) for sharing the UHSAS; Gary Giles, Eric Roux, and Mathew Bastian (NRC); and the NRC Convair 580 Aircraft Maintenance Engineers. Special thanks to the NRC FRL pilots Paul Kissman, Anthony Brown, and Rob Erdos for their outstanding cooperation and aircraft navigation through convective cloud regions during the data collection. Authors appreciate Walter Strapp (MetAnalyics Inc.), Tom Ratvasky, and Kurt Blankenship (NASA GRC) for the ground support of the Convair 580 flight operations. L.A. Ladino thanks the Natural Sciences and Engineering Research Council of Canada (NSERC) for his fellowship. A.M. Fridlind and A.S. Ackerman thank the NASA Modeling and Analysis Program for funding their contribution to this study. The data used in this study are available at Environment and Climate Change Canada upon request from Alexei Korolev (alexei.korolev@canada.ca). NR 90 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 FEB 16 PY 2017 VL 44 IS 3 BP 1574 EP 1582 DI 10.1002/2016GL072455 PG 9 WC Geosciences, Multidisciplinary SC Geology GA EN6LH UT WOS:000396115000045 ER PT J AU Ryu, YH Hodzic, A Descombes, G Hall, S Minnis, P Spangenberg, D Ullmann, K Madronich, S AF Ryu, Young-Hee Hodzic, Alma Descombes, Gael Hall, Samuel Minnis, Patrick Spangenberg, Douglas Ullmann, Kirk Madronich, Sasha TI Improved modeling of cloudy-sky actinic flux using satellite cloud retrievals SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID PHOTOLYSIS FREQUENCY; LOWER TROPOSPHERE; SURFACE; OZONE; NO2; FIELD; PHOTODISSOCIATION; INSTRUMENTATION; ATMOSPHERE; ALGORITHM AB Clouds play a critical role in modulating tropospheric radiation and thus photochemistry. We develop a methodology for calculating the vertical distribution of tropospheric ultraviolet (300-420 nm) actinic fluxes using satellite cloud retrievals and a radiative transfer model. We demonstrate that our approach can accurately reproduce airborne-measured actinic fluxes from the 2013 Studies of Emissions and Atmospheric Composition, Clouds and Climate Coupling by Regional Surveys (SEAC4RS) campaign as a case study. The results show that the actinic flux is reduced below moderately thick clouds with increasing cloud optical depth and can be enhanced by a factor of 2 above clouds. Inside clouds, the actinic flux can be enhanced by up to 2.4 times in the upper part of clouds or reduced up to 10 times in the lower parts of clouds. Our study suggests that the use of satellite-derived actinic fluxes as input to chemistry-transport models can improve the accuracy of photochemistry calculations. C1 [Ryu, Young-Hee; Hodzic, Alma; Descombes, Gael; Hall, Samuel; Ullmann, Kirk; Madronich, Sasha] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. [Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Spangenberg, Douglas] Sci Syst & Applicat Inc, Hampton, VA USA. RP Hodzic, A (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. EM alma@ucar.edu OI Madronich, Sasha/0000-0003-0983-1313; Hall, Samuel/0000-0002-2060-7112; Ullmann, Kirk/0000-0002-4724-9634 FU NASA-ROSES grant [NNX15AE38G]; National Science Foundation; SEAC4RS Project; NASA Modeling, Analysis, and Prediction (MAP) Program FX We acknowledge Fred Rose for providing single scattering albedo and asymmetry factor data for the satellite products. Y.-H. Ryu and G. Descombes acknowledge support from NASA-ROSES grant NNX15AE38G. The National Center for Atmospheric Research is sponsored by the National Science Foundation. P. Minnis and D. Spangenberg are supported by the SEAC4RS Project led by Hal Maring and by the NASA Modeling, Analysis, and Prediction (MAP) Program led by David Considine. The TUV model can be downloaded at https://www2.acom.ucar.edu/modeling/tuv-download. The satellite cloud data used in this study are available at http://www-air.larc.nasa.gov/cgi-bin/ArcView/seac4rs?SATELLITE=1. The in situ airborne data of actinic flux can be requested from Samuel Hall. NR 43 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 FEB 16 PY 2017 VL 44 IS 3 BP 1592 EP 1600 DI 10.1002/2016GL071892 PG 9 WC Geosciences, Multidisciplinary SC Geology GA EN6LH UT WOS:000396115000047 ER PT J AU Gao, CY Tsigaridis, K Bauer, SE AF Gao, Chloe Y. Tsigaridis, Kostas Bauer, Susanne E. TI MATRIX-VBS (v1.0): implementing an evolving organic aerosol volatility in an aerosol microphysics model SO GEOSCIENTIFIC MODEL DEVELOPMENT LA English DT Article ID CHEMICAL-TRANSPORT MODEL; BASIS-SET APPROACH; MIXING STATE; SEMIVOLATILE; EMISSIONS; CONDENSATION; NUCLEATION; ATMOSPHERE; PARTICLES; CAMPAIGN AB The gas-particle partitioning and chemical aging of semi-volatile organic aerosol are presented in a newly developed box model scheme, where its effect on the growth, composition, and mixing state of particles is examined. The volatility-basis set (VBS) framework is implemented into the aerosol microphysical scheme MATRIX (Multiconfiguration Aerosol TRacker of mIXing state), which resolves mass and number aerosol concentrations and in multiple mixing-state classes. The new scheme, MATRIX-VBS, has the potential to significantly advance the representation of organic aerosols in Earth system models by improving upon the conventional representation as non-volatile particulate organic matter, often also with an assumed fixed size distribution. We present results from idealized cases representing Beijing, Mexico City, a Finnish forest, and a southeastern US forest, and investigate the evolution of mass concentrations and volatility distributions for organic species across the gas and particle phases, as well as assessing their mixing state among aerosol populations. Emitted semi-volatile primary organic aerosols evaporate almost completely in the intermediate-volatility range, while they remain in the particle phase in the low-volatility range. Their volatility distribution at any point in time depends on the applied emission factors, oxidation by OH radicals, and temperature. We also compare against parallel simulations with the original scheme, which represented only the particulate and non-volatile component of the organic aerosol, examining how differently the condensed-phase organic matter is distributed across the mixing states in the model. The results demonstrate the importance of representing organic aerosol as a semi-volatile aerosol, and explic-itly calculating the partitioning of organic species between the gas and particulate phases. C1 [Gao, Chloe Y.] Columbia Univ, Dept Earth & Environm Sci, New York, NY 10027 USA. [Gao, Chloe Y.; Tsigaridis, Kostas; Bauer, Susanne E.] NASA, Goddard Inst Space Studies, New York, NY USA. [Tsigaridis, Kostas; Bauer, Susanne E.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. RP Tsigaridis, K (reprint author), NASA, Goddard Inst Space Studies, New York, NY USA.; Tsigaridis, K (reprint author), Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. EM kostas.tsigaridis@columbia.edu FU NASA Modeling, Analysis, and Prediction program FX We thank the NASA Modeling, Analysis, and Prediction program, which supports the GISS ModelE development. NR 51 TC 0 Z9 0 U1 3 U2 3 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1991-959X EI 1991-9603 J9 GEOSCI MODEL DEV JI Geosci. Model Dev. PD FEB 16 PY 2017 VL 10 IS 2 BP 751 EP 764 DI 10.5194/gmd-10-751-2017 PG 14 WC Geosciences, Multidisciplinary SC Geology GA EM2XK UT WOS:000395178900001 ER PT J AU Gacita, MS Longo, KM Freire, JLM Freitas, SR Martin, ST AF Gacita, Madeleine Sanchez Longo, Karla M. Freire, Julliana L. M. Freitas, Saulo R. Martin, Scot T. TI Impact of mixing state and hygroscopicity on CCN activity of biomass burning aerosol in Amazonia SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID CLOUD CONDENSATION NUCLEI; SIZE-RESOLVED MEASUREMENTS; DROPLET GROWTH-KINETICS; CHEMICAL-COMPOSITION; ATMOSPHERIC AEROSOL; ORGANIC AEROSOL; ACTIVATION KINETICS; SURFACE-TENSION; FIRE EMISSIONS; WATER-UPTAKE AB Smoke aerosols prevail throughout Amazonia because of widespread biomass burning during the dry season, and external mixing, low variability in the particle size distribution and low particle hygroscopicity are typical. There can be profound effects on cloud properties. This study uses an adiabatic cloud model to simulate the activation of smoke particles as cloud condensation nuclei (CCN) for three hypothetical case studies, chosen as to resemble biomass burning aerosol observations in Amazonia. The relative importance of variability in hygroscopicity, mixing state, and activation kinetics for the activated fraction and maximum supersaturation is assessed. For a population with kappa(p) = 0.04 an overestimation of the cloud droplet number concentration N d for the three selected case studies between 22.4 +/- 1.4 and 54.3 +/- 3.7% was obtained when assuming a hygroscopicity parameter kappa(p) = 0.20. Assuming internal mixing of the aerosol population led to overestimations of up to 20% of N d when a group of particles with medium hygroscopicity was present in the externally mixed population cases. However, the overestimations were below 10% for external mixtures between very low and low-hygroscopicity particles, as seems to be the case for Amazon smoke particles. Kinetic limitations were significant for medium-and high-hygroscopicity particles, and much lower for very low and low-hygroscopicity particles. When particles were assumed to be at equilibrium and to respond instantly to changes in the air parcel supersaturation, the overestimation of the droplet concentration was up to similar to 100% in internally mixed populations, and up to similar to 250% in externally mixed ones, being larger for the higher values of hygroscopicity. In addition, a perceptible delay between the times when maximum supersaturation and maximum aerosol activated fraction are reached was noticed and, for aerosol populations with effective hygroscopicity kappa(Peff) higher than a certain threshold value, the delay in particle activation was such that no particles were activated at the time of maximum supersaturation. Considering internally mixed populations, for an updraft velocity W = 0.5 m s(-1) this threshold of no activation varied between kappa(Peff) = 0.35 and kappa(Peff) = 0.5 for the different case studies. However, for low hygroscopicity, kinetic limitations played a weaker role for CCN activation of particles, even when taking into account the large aerosol mass and number concentrations. For the very low range of hygroscopicities, the overestimation of the droplet concentration due to the equilibrium assumption was lowest and the delay between the times when maximum supersaturation and maximum activated fraction were reached was greatly reduced or no longer observed (depending on the case study). These findings on uncertainties and sensitivities provide guidance on appropriate simplifications that can be used for modeling of smoke aerosols within general circulation models. The use of medium values of hygroscopicity representative of smoke aerosols for other biomass burning regions on Earth can lead to significant errors compared to the use of low hygroscopicity for Amazonia (between 0.05 and 0.13, according to available observations). Also in this region, consideration of the biomass burning population as internally mixed will lead to small errors in the droplet concentration, while significantly increasing the computational burden. Regardless of the large smoke aerosol loads in the region during the dry season, kinetic limitations are expected to be low. C1 [Gacita, Madeleine Sanchez; Longo, Karla M.; Freire, Julliana L. M.; Freitas, Saulo R.] INPE, Ctr Weather Forecasting & Climate Res, Cachoeira Paulista, SP, Brazil. [Martin, Scot T.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Longo, Karla M.; Freitas, Saulo R.] NASA Goddard Space Flight Ctr, Univ Space Res Associat, Goddard Earth Sci Technol & Res USRA GESTAR, Global Modeling & Assimilat Off, Greenbelt, MD USA. RP Gacita, MS (reprint author), INPE, Ctr Weather Forecasting & Climate Res, Cachoeira Paulista, SP, Brazil. EM madeleine.sanchez@cptec.inpe.br FU Sao Paulo Research Foundation (FAPESP) [2012/13575-9, DR 2012/09934-3, BEPE 2013/02101-9, BPE 2014/01564-8] FX The authors thank three anonymous referees for their valuable suggestions and comments that contributed significantly to the improvement of the present paper. This work was supported by the Sao Paulo Research Foundation (FAPESP), through the projects 2012/13575-9, DR 2012/09934-3, BEPE 2013/02101-9 and BPE 2014/01564-8. NR 77 TC 1 Z9 1 U1 0 U2 0 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 FEB 15 PY 2017 VL 17 IS 3 BP 2373 EP 2392 DI 10.5194/acp-17-2373-2017 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EM2FA UT WOS:000395130600002 ER PT J AU Eldering, A O'Dell, CW Wennberg, PO Crisp, D Gunson, MR Viatte, C Avis, C Braverman, A Castano, R Chang, A Chapsky, L Cheng, C Connor, B Dang, L Doran, G Fisher, B Frankenberg, C Fu, DJ Granat, R Hobbs, J Lee, RAM Mandrake, L McDuffie, J Miller, CE Myers, V Natraj, V O'Brien, D Osterman, GB Oyafuso, F Payne, VH Pollock, HR Polonsky, I Roehl, CM Rosenberg, R Schwandner, F Smyth, M Tang, VV Taylor, TE To, C Wunch, D Yoshimizu, J AF Eldering, Annmarie O'Dell, Chris W. Wennberg, Paul O. Crisp, David Gunson, Michael R. Viatte, Camille Avis, Charles Braverman, Amy Castano, Rebecca Chang, Albert Chapsky, Lars Cheng, Cecilia Connor, Brian Dang, Lan Doran, Gary Fisher, Brendan Frankenberg, Christian Fu, Dejian Granat, Robert Hobbs, Jonathan Lee, Richard A. M. Mandrake, Lukas McDuffie, James Miller, Charles E. Myers, Vicky Natraj, Vijay O'Brien, Denis Osterman, Gregory B. Oyafuso, Fabiano Payne, Vivienne H. Pollock, Harold R. Polonsky, Igor Roehl, Coleen M. Rosenberg, Robert Schwandner, Florian Smyth, Mike Tang, Vivian Taylor, Thomas E. To, Cathy Wunch, Debra Yoshimizu, Jan TI The Orbiting Carbon Observatory-2: first 18 months of science data products SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID CO2 RETRIEVAL ALGORITHM; CHLOROPHYLL FLUORESCENCE; ATMOSPHERIC CO2; SPACE; OCO-2; GOSAT; SCIAMACHY; CYCLE; CALIBRATION; VALIDATION AB The Orbiting Carbon Observatory-2 (OCO-2) is the first National Aeronautics and Space Administration (NASA) satellite designed to measure atmospheric carbon dioxide (CO2/with the accuracy, resolution, and coverage needed to quantify CO2 fluxes (sources and sinks) on regional scales. OCO-2 was successfully launched on 2 July 2014 and has gathered more than 2 years of observations. The v7/v7r operational data products from September 2014 to January 2016 are discussed here. On monthly timescales, 7 to 12% of these measurements are sufficiently cloud and aerosol free to yield estimates of the column-averaged atmospheric CO2 dry air mole fraction, XCO2, that pass all quality tests. During the first year of operations, the observing strategy, instrument calibration, and retrieval algorithm were optimized to improve both the data yield and the accuracy of the products. With these changes, global maps of XCO2 derived from the OCO-2 data are revealing some of the most robust features of the atmospheric carbon cycle. This includes XCO2 enhancements co-located with intense fossil fuel emissions in eastern US and eastern China, which are most obvious between October and December, when the north-south XCO2 gradient is small. Enhanced XCO2 coin-cident with biomass burning in the Amazon, central Africa, and Indonesia is also evident in this season. In May and June, when the north- south XCO2 gradient is largest, these sources are less apparent in global maps. During this part of the year, OCO- 2 maps show a more than 10 ppm reduction in XCO2 across the Northern Hemisphere, as photosynthesis by the land biosphere rapidly absorbs CO2. As the carbon cycle science community continues to analyze these OCO-2 data, information on regional-scale sources 9emitters) and sinks 9absorbers) which impart XCO2 changes on the order of 1 ppm, as well as far more subtle features, will emerge from this high-resolution global dataset. C1 [Eldering, Annmarie; Crisp, David; Gunson, Michael R.; Avis, Charles; Braverman, Amy; Castano, Rebecca; Chang, Albert; Chapsky, Lars; Cheng, Cecilia; Dang, Lan; Doran, Gary; Fisher, Brendan; Frankenberg, Christian; Fu, Dejian; Granat, Robert; Hobbs, Jonathan; Lee, Richard A. M.; McDuffie, James; Miller, Charles E.; Myers, Vicky; Natraj, Vijay; Osterman, Gregory B.; Oyafuso, Fabiano; Payne, Vivienne H.; Pollock, Harold R.; Rosenberg, Robert; Schwandner, Florian; Smyth, Mike; Tang, Vivian; To, Cathy; Yoshimizu, Jan] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [O'Dell, Chris W.; O'Brien, Denis; Polonsky, Igor; Taylor, Thomas E.] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA. [Wennberg, Paul O.; Viatte, Camille; Frankenberg, Christian; Roehl, Coleen M.; Wunch, Debra] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. [Connor, Brian] BC Sci Consulting, Stony Brook, NY USA. [Polonsky, Igor] Atmospheric & Environm Res Inc, Lexington, MA USA. [Wunch, Debra] Univ Toronto, Dept Phys, Toronto, ON, Canada. RP Eldering, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM annmarie.eldering@jpl.nasa.gov FU OCO-2 Project FX Part of this work was conducted at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA) for the Orbiting Carbon Observatory-2 Project. Work at Colorado State University and the Geology and Planetary Sciences Department at the California Institute of Technology was supported by subcontracts from the OCO-2 Project. NR 56 TC 0 Z9 0 U1 1 U2 1 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 FEB 15 PY 2017 VL 10 IS 2 BP 549 EP 563 DI 10.5194/amt-10-549-2017 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EM2PF UT WOS:000395157400001 ER PT J AU Maiorano, A Martre, P Asseng, S Ewert, F Muller, C Rotter, RP Ruane, AC Semenov, MA Wallach, D Wang, EL Alderman, PD Kassie, BT Biernath, C Basso, B Cammaran, D Challinor, AJ Doltra, J Dumont, B Rezaei, EE Gayler, S Kersebaum, KC Kimball, BA Koehler, AK Liu, B O'Leary, GJ Olesen, JE Ottman, MJ Priesack, E Reynolds, M Stratonovitch, P Streck, T Thorburn, PJ Waha, K Wall, GW White, JW Zhao, ZG Zhu, Y AF Maiorano, Andrea Martre, Pierre Asseng, Senthold Ewert, Frank Mueller, Christoph Rotter, Reimund P. Ruane, Alex C. Semenov, Mikhail A. Wallach, Daniel Wang, Enli Alderman, Phillip D. Kassie, Belay T. Biernath, Christian Basso, Bruno Cammarano, Davide Challinor, Andrew J. Doltra, Jordi Dumont, Benjamin Rezaei, Ehsan Eyshi Gayler, Sebastian Kersebaum, Kurt Christian Kimball, Bruce A. Koehler, Ann-Kristin Liu, Bing O'Leary, Garry J. Olesen, Jorgen E. Ottman, Michael J. Priesack, Eckart Reynolds, Matthew Stratonovitch, Pierre Streck, Thilo Thorburn, Peter J. Waha, Katharina Wall, Gerard W. White, Jeffrey W. Zhao, Zhigan Zhu, Yan TI Crop model improvement reduces the uncertainty of the response to temperature of multi-model ensembles SO FIELD CROPS RESEARCH LA English DT Article DE Impact uncertainty; High temperature; Model improvement; Multi-model ensemble; Wheat crop model ID TRITICUM-AESTIVUM-L; CLIMATE-CHANGE; SIMULATION-MODEL; SPRING WHEAT; NITROGEN UPTAKE; WINTER-WHEAT; YIELD; GROWTH; WATER; IMPACTS AB To improve climate change impact estimates and to quantify their uncertainty, multi-model ensembles (MMES) have been suggested. Model improvements can improve the accuracy of simulations and reduce the uncertainty of climate change impact assessments. Furthermore, they can reduce the number of models needed in a MME. Herein, 15 wheat growth models of a larger MME were improved through re-parameterization and/or incorporating or modifying heat stress effects on phenology, leaf growth and senescence, biomass growth, and grain number and size using detailed field experimental data from the USDA Hot Serial Cereal experiment (calibration data set). Simulation results from before and after model improvement were then evaluated with independent field experiments from a CIMMYT worldwide field trial network (evaluation data set). Model improvements decreased the variation (10th to 90th model ensemble percentile range) of grain yields simulated by the MME on average by 39% in the calibration data set and by 26% in the independent evaluation data set for crops grown in mean seasonal temperatures >24 degrees C. MME mean squared error in simulating grain yield decreased by 37%. A reduction in MME uncertainty range by 27% increased MME prediction skills by 47%. Results suggest that the mean level of variation observed in field experiments and used as a benchmark can be reached with half the number of models in the MME. Improving crop models is therefore important to increase the certainty of model-based impact assessments and allow more practical, i.e. smaller MMES to be used effectively. (C)2016 Elsevier B.V. All rights reserved. C1 [Maiorano, Andrea; Martre, Pierre] Montpellier SupAgro, INRA, UMR LEPSE, 2 Pl Viala, F-34060 Montpellier, France. [Asseng, Senthold; Kassie, Belay T.; Cammarano, Davide] Univ Florida, Agr & Biol Engn Dept, Gainesville, FL 32611 USA. [Ewert, Frank; Rezaei, Ehsan Eyshi] Univ Bonn, Inst Crop Sci & Resource Conservat, D-53115 Bonn, Germany. [Mueller, Christoph; Waha, Katharina] Potsdam Inst Climate Impact Res, D-14473 Potsdam, Germany. [Rotter, Reimund P.] Nat Resources Inst Finland Luke, FI-01301 Vantaa, Finland. [Ruane, Alex C.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Semenov, Mikhail A.; Stratonovitch, Pierre] Rothamsted Res, Computat & Syst Biol Dept, Harpenden AL5 2JQ, Herts, England. [Wallach, Daniel] INRA, Agrosyst & Dev Terr, UMR 1248, F-31326 Castanet Tolosan, France. [Wang, Enli; Zhao, Zhigan] CSIRO Agr, Black Mountain, ACT 2601, Australia. [Alderman, Phillip D.; Reynolds, Matthew] CIMMYT, Int AP 6-641, Mexico City 06600, DF, Mexico. [Biernath, Christian; Priesack, Eckart] Helmholtz Zentrum Munchen, German Res Ctr Environm Hlth, Inst Biochem Plant Pathol, D-85764 Neuherberg, Germany. [Basso, Bruno; Dumont, Benjamin] Michigan State Univ, Dept Geol Sci, E Lansing, MI 48823 USA. [Basso, Bruno; Dumont, Benjamin] Michigan State Univ, WK Kellogg Biol Stn, E Lansing, MI 48823 USA. [Challinor, Andrew J.; Koehler, Ann-Kristin] Univ Leeds, Sch Earth & Environm, Inst Climate & Atmospher Sci, Leeds LS2 9JT, W Yorkshire, England. [Challinor, Andrew J.] Ctr Int Agr Trop, CGIAR ESSP Program Climate Change Agr & Food Secu, Cali 6713, Colombia. [Doltra, Jordi] Cantabrian Agr Res & Training Ctr, Muriedas 39600, Spain. [Gayler, Sebastian] Univ Hohenheim, Inst Soil Sci & Land Evaluat, D-70599 Stuttgart, Germany. [Kersebaum, Kurt Christian] Leibniz Ctr Agr Landscape Res, Inst Landscape Syst Anal, D-15374 Muncheberg, Germany. [Kimball, Bruce A.; Wall, Gerard W.; White, Jeffrey W.] ARS, USDA, US Arid Land Agr Res Ctr, Maricopa, AZ 85138 USA. [Liu, Bing] Nanjing Agr Univ, Coll Agr, Nanjing 210095, Jiangsu, Peoples R China. [O'Leary, Garry J.] Grains Innovat Pk, Dept Econ Dev Jobs Transport & Resources, Horsham, Vic 3400, Australia. [Olesen, Jorgen E.] Aarhus Univ, Dept Agroecol, DK-8830 Tjele, Denmark. [Ottman, Michael J.] Univ Arizona, Sch Plant Sci, Tucson, AZ 85721 USA. [Streck, Thilo] Univ Hohenheim, Inst Soil Sci & Land Evaluat, D-70599 Stuttgart, Germany. [Thorburn, Peter J.] CSIRO Agr, 306 Carmody Rd, St Lucia, Qld 4067, Australia. [Rezaei, Ehsan Eyshi] Ctr Dev Res ZEF, Walter Flex Str 3, D-53133 Bonn, Germany. [Zhao, Zhigan] China Agr Univ, Beijing 100193, Peoples R China. [Ewert, Frank] Leibniz Ctr Agr, 36 Landscape Res, D-15374 Muncheberg, Germany. [Rotter, Reimund P.] Univ Gottingen, Dept Crop Sci, Div Crop Prod Syst Trop, D-37077 Gottingen, Germany. [Cammarano, Davide] James Hutton Inst, Dundee DD2 5DA, Scotland. [Waha, Katharina] CSIRO Agr, 306 Carmody Rd, St Lucia, Qld 4067, Australia. [Alderman, Phillip D.] Oklahoma State Univ, Dept Plant & Soil Sci, Stillwater, OK 74078 USA. RP Maiorano, A; Martre, P (reprint author), Montpellier SupAgro, INRA, UMR LEPSE, 2 Pl Viala, Montpellier 34060, France. EM maiorano.andrea@gmail.com; pierre.martre@supagro.inra.fr RI Thorburn, Peter/A-6884-2011; Doltra, Jordi/C-2106-2015; OI Maiorano, Andrea/0000-0002-0497-9303; Muller, Christoph/0000-0002-9491-3550; Cammarano, Davide/0000-0003-0918-550X; Eyshi Rezaei, Ehsan/0000-0003-2603-8034; Wallach, Daniel/0000-0003-3500-8179 FU EU [PCOFUND-GA-2010-267196]; FACCE JPI MACSUR project through the metaprogram Adaptation of Agriculture and Forests to Climate Change (AAFCC) of the French National Institute for Agricultural Research (INRA) [031A103B]; International Food Policy Research Institute (IFPRI); International Maize and Wheat Improvement Center (CIMMYT); FACCE MACSUR project through the German Federal Ministry of Education and Research [031A103B, 2812ERA115]; EER through the German Federal Ministry of Economic Cooperation and Development (Project: PARI); CSIRO; Chinese Academy of Sciences through the project 'Advancing crop yield while reducing the use of water and nitrogen'; KULUNDA project [01LL0905L]; MACMIT project [01LN1317A]; German Federal Ministry of Education and Research (BMBF); FACCE MACSUR project; Finnish Ministry of Agriculture and Forestry; CGIAR Research Program on Climate Change, Agriculture, and Food Security (CCAFS); Helmholtz project 'REKLIM-Regional Climate Change: Causes and Effects' Topic 9: 'Climate Change and Air Quality'; FACCE MACSUR project through the German Federal Office for Agriculture and Food (BLE); Australian Grains Research and Development Corporation; Department of Environment and Primary Industries Victoria, Australia; FACCE MACSUR project by the Danish Strategic Research Innovation Foundation; China Scholarship Council through the CSIRO; Chinese Ministry of Education PhD Research Program; UK Biotechnology and Biological Sciences Research Council FX AM has received the support of the EU in the framework of the Marie-Curie FP7COFUND People Programme, through the award of an AgreenSkills fellowship under grant agreement no. PCOFUND-GA-2010-267196. PM and DW acknowledge support from the FACCE JPI MACSUR project (031A103B) through the metaprogram Adaptation of Agriculture and Forests to Climate Change (AAFCC) of the French National Institute for Agricultural Research (INRA). SA and DC received financial support from the International Food Policy Research Institute (IFPRI) and the International Maize and Wheat Improvement Center (CIMMYT). FE received support from the FACCE MACSUR project (031A103B) funded through the German Federal Ministry of Education and Research (2812ERA115) and EER was funded through the German Federal Ministry of Economic Cooperation and Development (Project: PARI). EW was funded by the by CSIRO and the Chinese Academy of Sciences through the project 'Advancing crop yield while reducing the use of water and nitrogen'. CM received financial support from the KULUNDA project (01LL0905L) and the MACMIT project (01LN1317A) funded through the German Federal Ministry of Education and Research (BMBF). RPR received financial support from FACCE MACSUR project funded through the Finnish Ministry of Agriculture and Forestry. MPR and PDA received funding from the CGIAR Research Program on Climate Change, Agriculture, and Food Security (CCAFS). CB was funded through the Helmholtz project 'REKLIM-Regional Climate Change: Causes and Effects' Topic 9: 'Climate Change and Air Quality'. KCK and CN were funded by the FACCE MACSUR project through the German Federal Office for Agriculture and Food (BLE). GO'L was funded through the Australian Grains Research and Development Corporation and the Department of Environment and Primary Industries Victoria, Australia. JEO were funded through the FACCE MACSUR project by the Danish Strategic Research Innovation Foundation. ZZ received scholarship from the China Scholarship Council through the CSIRO and Chinese Ministry of Education PhD Research Program. Rothamsted Research is supported via the 20:20 Wheat Programme by the UK Biotechnology and Biological Sciences Research Council. NR 103 TC 1 Z9 1 U1 9 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-4290 EI 1872-6852 J9 FIELD CROP RES JI Field Crop. Res. PD FEB 15 PY 2017 VL 202 SI SI BP 5 EP 20 DI 10.1016/j.fcr.2016.05.001 PG 16 WC Agronomy SC Agriculture GA EK4XQ UT WOS:000393931600002 ER PT J AU Satkoski, AM Beukes, NJ Li, WQ Beard, BL Johnson, CM AF Satkoski, Aaron M. Beukes, Nicolas J. Li, Weiqiang Beard, Brian L. Johnson, Clark M. TI A redox-stratified ocean 3.2 billion years ago (vol 430, pg 43, 2015) SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Correction C1 [Satkoski, Aaron M.; Beard, Brian L.; Johnson, Clark M.] Univ Wisconsin Madison, Dept Geosci, 1215 West Dayton St, Madison, WI 53706 USA. [Satkoski, Aaron M.; Beard, Brian L.; Johnson, Clark M.] NASA, Astrobiol Inst, Mountain View, CA USA. [Beukes, Nicolas J.] Univ Johannesburg, CIMERA, Dept Geol, POB 524, ZA-2006 Johannesburg, South Africa. [Li, Weiqiang] Sch Earth Sci & Engn, State Key Lab Mineral Deposits Res, Nanjing 210093, Jiangsu, Peoples R China. RP Satkoski, AM (reprint author), Univ Wisconsin Madison, Dept Geosci, 1215 West Dayton St, Madison, WI 53706 USA. EM satkoski@wisc.edu NR 2 TC 0 Z9 0 U1 1 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD FEB 15 PY 2017 VL 460 BP 317 EP 319 DI 10.1016/j.epsl.2016.12.013 PG 3 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EJ1ZF UT WOS:000393008500033 ER PT J AU Yamaleev, NK Carpenter, MH AF Yamaleev, Nail K. Carpenter, Mark H. TI A family of fourth-order entropy stable nonoscillatory spectral collocation schemes for the 1-D Navier-Stokes equations SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE Summation-by-parts (SBP) operators; Entropy stability; Spectral collocation methods; Weighted essentially nonoscillatory (WENO) schemes; The Navier-Stokes equations ID DISCONTINUOUS GALERKIN METHOD; COMPUTATIONAL FLUID-DYNAMICS; NONLINEAR CONSERVATION-LAWS; UNSTRUCTURED MESHES; NUMERICAL-METHODS; WENO LIMITERS; SYSTEMS; CONVERGENCE; FORM AB High-order numerical methods that satisfy a discrete analog of the entropy inequality are uncommon. Indeed, no proofs of nonlinear entropy stability currently exist for high-order weighted essentially nonoscillatory (WENO) finite volume or weak-form finite element methods. Herein, a new family of fourth-order WENO spectral collocation schemes is developed, that are nonlinearly entropy stable for the one-dimensional compressible Navier Stokes equations. Individual spectral elements are coupled using penalty type interface conditions. The resulting entropy stable WENO spectral collocation scheme achieves design order accuracy, maintains the WENO stencil biasing properties across element interfaces, and satisfies the summation-by-parts (SBP) operator convention, thereby ensuring nonlinear entropy stability in a diagonal norm. Numerical results demonstrating accuracy and nonoscillatory properties of the new scheme are presented for the one-dimensional Euler and Navier Stokes equations for both continuous and discontinuous compressible flows. (C) 2016 Elsevier Inc. All rights reserved. C1 [Yamaleev, Nail K.] Old Dominion Univ, Dept Math & Stat, Norfolk, VA 23529 USA. [Carpenter, Mark H.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Yamaleev, NK (reprint author), Old Dominion Univ, Dept Math & Stat, Norfolk, VA 23529 USA. EM nyamalee@odu.edu NR 38 TC 0 Z9 0 U1 1 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9991 EI 1090-2716 J9 J COMPUT PHYS JI J. Comput. Phys. PD FEB 15 PY 2017 VL 331 BP 90 EP 107 DI 10.1016/j.jcp.2016.11.039 PG 18 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA EJ5IJ UT WOS:000393250700006 ER PT J AU Chidester, BA Rahman, Z Righter, K Campbell, AJ AF Chidester, Bethany A. Rahman, Zia Righter, Kevin Campbell, Andrew J. TI Metal-silicate partitioning of U: Implications for the heat budget of the core and evidence for reduced U in the mantle SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article DE Uranium; Radiogenic heat; Core energy budget; Magma ocean ID DEEP MAGMA-OCEAN; SI-C SYSTEM; EARTHS CORE; HIGH-PRESSURE; OXYGEN FUGACITY; ELECTRICAL-CONDUCTIVITY; THERMAL-CONDUCTIVITY; OXIDATION-STATE; TRACE-ELEMENTS; SOLID IRON AB Earth's core might require an internal heat source, such as radioactive decay, to explain the presence of the magnetic field through geologic time. To investigate whether U would be an important heat source in the core, we performed metal-silicate partitioning experiments of U at P-T (up to 67 GPa and 5400 K) conditions more relevant to a magma ocean scenario than has previously been reported. This study finds the partitioning of U to be strongly dependent on fO(2), temperature, the S content of the metal and the SiO2 content of the silicate during core-mantle differentiation. Differentiation at mean conditions of 42-58 GPa and 3900-4200 K would put 1.4-3.5 ppb U (2-8 wt% S) in the core, amounting to a maximum of 1.4 (+1/-0.7) TW of heat 4.5 billion years ago. This is likely not enough heat to mitigate early widespread mantle melting. It was also found that U likely exists in the 2+ oxidation state in silicate melts in the deep Earth, a state which has not been previously observed in nature. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Chidester, Bethany A.; Campbell, Andrew J.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Rahman, Zia; Righter, Kevin] NASA Johnson Space Ctr, Houston, TX 77058 USA. RP Chidester, BA (reprint author), Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. EM chidesterba@uchicago.edu OI RAHMAN, ZIA/0000-0002-4923-767X FU NSF [DGE-1144082, EAR-1427123]; RTOP through the NASA Cosmochemistry Program FX This work was funded by a NSF Graduate Research Fellowship Grant #DGE-1144082, NSF Grant #EAR-1427123, and an RTOP through the NASA Cosmochemistry Program. The FIB and TEM work were completed in the Electron Beam Analysis Labs within the Astromaterials Research and Exploration Science office at Johnson Space Center. The authors thank four anonymous reviewers and the associate editor, Munir Humayun, for helpful comments. B.A.C. thanks R. Fischer, N. Dauphas and D. Heinz for helpful discussions. NR 46 TC 0 Z9 0 U1 5 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD FEB 15 PY 2017 VL 199 BP 1 EP 12 DI 10.1016/j.gca.2016.11.035 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EJ3QA UT WOS:000393125500001 ER PT J AU Jogo, K Nakamura, T Ito, M Wakita, S Zolotov, MY Messenger, SR AF Jogo, Kaori Nakamura, Tomoki Ito, Motoo Wakita, Shigeru Zolotov, Mikhail Yu. Messenger, Scott R. TI Mn-Cr ages and formation conditions of fayalite in CV3 carbonaceous chondrites: Constraints on the accretion ages of chondritic asteroids SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article DE Aqueous alteration; Fayalite; CV3 carbonaceous chondrites; Mn-Cr method; Age determination; Equilibrium thermodynamics; Thermal modeling ID PARENT-BODY PROCESSES; EARLY SOLAR-SYSTEM; ALLENDE METEORITE; AQUEOUS ALTERATION; PROTOPLANETARY DISK; ORGANIC-MATTER; OLIVINE; MG; BODIES; NEBULA AB Chondritic planetesimals are among the first planetary bodies that accreted inside and outside water snow line in the protoplanetary disk. CV3 carbonaceous chondrite parent body accreted relatively small amount of water ice, probably near the snow line, and experienced water-assisted metasomatic alteration that resulted in formation of diverse secondary minerals, including fayalite (Fa(80-100)). Chemical compositions of the CV3 fayalite and its Mn-Cr isotope systematics indicate that it formed at different temperature (10-300 degrees C) and fluid pressure (3-300 bars) but within a relatively short period of time. Thermal modeling of the CV3 parent body suggests that it accreted similar to 3.2-3.3 Ma after CV3 CAIs formation and had a radius of >110-150 km. The inferred formation age of the CV3 parent body is similar to that of the CM2 chondrite parent body that probably accreted beyond the snow line, but appears to have postdated accretion of the CO and ordinary chondrite parent bodies that most likely formed inside the snow line. The inferred differences in the accretion ages of chondrite parent bodies that formed inside and outside snow line are consistent with planetesimal formation by gravitational/streaming instability. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Jogo, Kaori] Korea Polar Res Inst, Div Earth Syst Sci, 26 Songdomirae Ro, Incheon 406840, South Korea. [Nakamura, Tomoki] Tohoku Univ, Dept Earth & Planetary Mat Sci, Fac Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Ito, Motoo] Kochi Inst Core Sample Res, JAMSTEC B200 Monobe, Nankoku, Kochi 7838502, Japan. [Wakita, Shigeru] Natl Astron Observ Japan, Ctr Computat Astrophys, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Zolotov, Mikhail Yu.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Messenger, Scott R.] NASA Johnson Space Ctr, Robert M Walker Lab Space Sci, ARES, 2101 NASA Pkwy, Houston, TX 77058 USA. RP Jogo, K (reprint author), Korea Polar Res Inst, Div Earth Syst Sci, 26 Songdomirae Ro, Incheon 406840, South Korea. EM kaorijogo@kopri.re.kr OI Wakita, Shigeru/0000-0002-3161-3454 FU Korea Polar Research Institute [PM16030]; JSPS [22224010]; NASA Cosmochemistry grant [NNX14AG19G] FX The meteoritic samples of Y86009, A881317, MET01074 and MET00430 were provided by National Institute of Polar Research, Japan and NASA Johnson Space center. The manuscript was improved by constructive comments from Dr. Nagahara and review by Dr. A. N. Krot. Thermal modelling was carried out on the PC cluster at the Center for Computational Astrophysics, National Astronomical Observatory of Japan. We thank Dr. Ikeda for the support to use JEOL-5800LV SEM and Mr. Shimada for technical assistant in the use of JEM-733 EPMA at Kyushu University. We also thank Dr. Nagahara for the support and Mr. Yoshida for their technical assistance in the use of JSM-7000F FE-SEM at the University of Tokyo. We also thank Dr. K. R. Ludwig for providing the Isoplot/Ex program for Mn-Cr age calibration. This work was supported by Korea Polar Research Institute project PM16030 and JSPS Grant-in-Aid for Scientific Research(S) Grant Number 22224010. M. Zolotov was supported by NASA Cosmochemistry grant NNX14AG19G. S. Messenger was supported by a NASA Cosmochemistry grant. NR 88 TC 0 Z9 0 U1 1 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD FEB 15 PY 2017 VL 199 BP 58 EP 74 DI 10.1016/j.gca.2016.11.027 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EJ3QA UT WOS:000393125500005 ER PT J AU Nguyen, TTT Kundan, A Wayner, PC Plawsky, JL Chao, DF Sicker, RJ AF Nguyen, Thao T. T. Kundan, Akshay Wayner, Peter C., Jr. Plawsky, Joel L. Chao, David F. Sicker, Ronald J. TI Experimental study of the heated contact line region for a pure fluid and binary fluid mixture in microgravity SO JOURNAL OF COLLOID AND INTERFACE SCIENCE LA English DT Article DE Contact line region; Ideal liquid mixture; Concentration; Heat pipe ID EVAPORATING WETTING FILM; THIN-FILM; DISJOINING PRESSURE; INTERFACIAL PROFILE; EXTENDED MENISCUS; MODEL; BUBBLE; DYNAMICS; SURFACE; PIPE AB Understanding the dynamics of phase change heat and mass transfer in the three-phase contact line region is a critical step toward improving the efficiency of phase change processes. Phase change becomes especially complicated when a fluid mixture is used. In this paper, a wickless heat pipe was operated on the International Space Station (ISS) to study the contact line dynamics of a pentane/isohexane mixture. Different interfacial regions were identified, compared, and studied. Using high resolution (50x), interference images, we calculated the curvature gradient of the liquid-vapor interface at the contact line region along the edges of the heat pipe. We found that the curvature gradient in the evaporation region increases with increasing heat flux magnitude and decreasing pentane concentration. The curvature gradient for the mixture case is larger than for the pure pentane case. The difference between the two cases increases as pentane concentration decreases. Our data showed that the curvature gradient profile within the evaporation section is separated into two regions with the boundary between the two corresponding to the location of a thick, liquid, "central drop" region at the point of maximum internal local heat flux. We found that the curvature gradients at the central drop and on the flat surfaces where condensation begins are one order of magnitude smaller than the gradients in the corner meniscus indicating the driving forces for fluid flow are much larger in the corners. (C) 2016 Elsevier Inc. All rights reserved. C1 [Nguyen, Thao T. T.; Kundan, Akshay; Wayner, Peter C., Jr.; Plawsky, Joel L.] Rensselaer Polytech Inst, Howard P Isermann Dept Chem & Biol Engn, Troy, NY 12180 USA. [Chao, David F.; Sicker, Ronald J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Plawsky, JL (reprint author), Rensselaer Polytech Inst, Howard P Isermann Dept Chem & Biol Engn, Troy, NY 12180 USA. EM nguyen.thaoche@gmail.com; akshaykundan@gmail.com; wayner@rpi.edu; plawsky@rpi.edu; david.f.chao@nasa.gov; ronald.j.sicker@nasa.gov FU National Aeronautics and Space Administration [NNX13AQ78G] FX This material is based on the work supported by the National Aeronautics and Space Administration under Grant number NNX13AQ78G. Any opinions, findings, and conclusions or recommendations expressed in this publication are those of the authors and do not necessarily reflect the view of NASA. NR 54 TC 0 Z9 0 U1 9 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9797 EI 1095-7103 J9 J COLLOID INTERF SCI JI J. Colloid Interface Sci. PD FEB 15 PY 2017 VL 488 BP 48 EP 60 DI 10.1016/j.jcis.2016.10.082 PG 13 WC Chemistry, Physical SC Chemistry GA EE7HC UT WOS:000389785500007 PM 27821339 ER PT J AU Che, H Goldstein, ML Diamond, PH Sagdeev, RZ AF Che, Haihong Goldstein, Melvyn L. Diamond, Patrick H. Sagdeev, Roald Z. TI How electron two-stream instability drives cyclic Langmuir collapse and continuous coherent emission SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE electron beams; nonlinear wave interaction; Langmuir collapse; coherent emission; plasma turbulence ID III RADIO-BURSTS; NONLINEAR STABILITY; WAVE COLLAPSE; SOLAR; PLASMA; RADIATION AB Continuous plasma coherent emission is maintained by repetitive Langmuir collapse driven by the nonlinear evolution of a strong electron two-stream instability. The Langmuir waves are modulated by solitary waves in the linear stage and electrostatic whistler waves in the nonlinear stage. Modulational instability leads to Langmuir collapse and electron heating that fills in cavitons. The high pressure is released via excitation of a short-wavelength ion acoustic mode that is damped by electrons and reexcites small-scale Langmuir waves; this process closes a feedback loop that maintains the continuous coherent emission. C1 [Che, Haihong] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Che, Haihong; Goldstein, Melvyn L.] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA. [Diamond, Patrick H.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Sagdeev, Roald Z.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. RP Che, H (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.; Che, H (reprint author), NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA. EM chehh06@gmail.com OI Che, Haihong/0000-0002-2240-6728 FU NASA Magneto-spheric Multiscale Mission; Department of Energy [DE-FG02-04ER54738]; NASA High-End Computing Program Awards [SMD-14-4848, SMD-15-5715]; NASA [NNG04EB99C] FX H.C. and P.H.D. thank participants for discussions in the "8th Festival de Theorie," Aix-en-Provence, France, 2015. P.H.D. thanks M. Malkov for discussions. This work was supported by the NASA Magneto-spheric Multiscale Mission in association with NASA Contract NNG04EB99C (to H.C.) and Department of Energy Grant DE-FG02-04ER54738 (to P.H.D.). The simulations and analysis were carried out at the NASA Advanced Supercomputing facility at Ames Research Center under NASA High-End Computing Program Awards SMD-14-4848 and SMD-15-5715. NR 35 TC 0 Z9 0 U1 0 U2 0 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 FEB 14 PY 2017 VL 114 IS 7 BP 1502 EP 1507 DI 10.1073/pnas.1614055114 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EK5TR UT WOS:000393989300047 PM 28137887 ER PT J AU Smith, MD Oglend, A Kirkpatrick, AJ Asche, F Bennear, LS Craig, JK Nance, JM AF Smith, Martin D. Oglend, Atle Kirkpatrick, A. Justin Asche, Frank Bennear, Lori S. Craig, J. Kevin Nance, James M. TI Seafood prices reveal impacts of a major ecological disturbance SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE hypoxia; fisheries; coupled human-natural systems; bioeconomics; spatial dynamics ID GULF-OF-MEXICO; SHRIMP FARFANTEPENAEUS-AZTECUS; BROWN SHRIMP; MARINE RESERVES; FISHERIES MANAGEMENT; SPATIAL-DISTRIBUTION; HYPOXIC ZONE; TIME-SERIES; DEAD ZONES; UNIT-ROOT AB Coastal hypoxia (dissolved oxygen <= 2 mg/L) is a growing problem worldwide that threatens marine ecosystem services, but little is known about economic effects on fisheries. Here, we provide evidence that hypoxia causes economic impacts on a major fishery. Ecological studies of hypoxia and marine fauna suggest multiple mechanisms through which hypoxia can skew a population's size distribution toward smaller individuals. These mechanisms produce sharp predictions about changes in seafood markets. Hypoxia is hypothesized to decrease the quantity of large shrimp relative to small shrimp and increase the price of large shrimp relative to small shrimp. We test these hypotheses using time series of size-based prices. Naive quantity-based models using treatment/control comparisons in hypoxic and nonhypoxic areas produce null results, but we find strong evidence of the hypothesized effects in the relative prices: Hypoxia increases the relative price of large shrimp compared with small shrimp. The effects of fuel prices provide supporting evidence. Empirical models of fishing effort and bioeconomic simulations explain why quantifying effects of hypoxia on fisheries using quantity data has been inconclusive. Specifically, spatial-dynamic feedbacks across the natural system (the fish stock) and human system (the mobile fishing fleet) confound "treated" and "control" areas. Consequently, analyses of price data, which rely on a market counterfactual, are able to reveal effects of the ecological disturbance that are obscured in quantity data. Our results are an important step toward quantifying the economic value of reduced upstream nutrient loading in the Mississippi Basin and are broadly applicable to other coupled human-natural systems. C1 [Smith, Martin D.; Kirkpatrick, A. Justin; Bennear, Lori S.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. [Smith, Martin D.; Bennear, Lori S.] Duke Univ, Dept Econ, Durham, NC 27708 USA. [Oglend, Atle; Asche, Frank] Univ Stavanger, Dept Ind Econ, N-4036 Stavanger, Norway. [Asche, Frank] Univ Florida, Sch Forest Resources & Conservat, Inst Sustainable Food Syst, Gainesville, FL 32611 USA. [Bennear, Lori S.] Duke Univ, Sanford Sch Publ Policy, Durham, NC 27708 USA. [Craig, J. Kevin] NOAA, Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Beaufort Lab, Beaufort, NC 28516 USA. [Nance, James M.] NOAA, Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Galveston Lab, Galveston, TX 77551 USA. RP Smith, MD (reprint author), Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA.; Smith, MD (reprint author), Duke Univ, Dept Econ, Durham, NC 27708 USA. EM marsmith@duke.edu FU National Oceanic and Atmospheric Administration [NA09NOS4780235, NA09NOS4780186]; Fulbright Scholar Program; Research Council of Norway FX We thank Dan Obenour for providing annual estimates of the areal extent of hypoxia with alternative DO cutoffs (1.5 mg/L and 2.5 mg/L). Financial support for this research was provided by National Oceanic and Atmospheric Administration Grants NA09NOS4780235 and NA09NOS4780186, the Fulbright Scholar Program, and the Research Council of Norway. NR 46 TC 0 Z9 0 U1 4 U2 4 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 FEB 14 PY 2017 VL 114 IS 7 BP 1512 EP 1517 DI 10.1073/pnas.1617948114 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EK5TR UT WOS:000393989300049 PM 28137850 ER PT J AU McNally, A Arsenault, K Kumar, S Shukla, S Peterson, P Wang, SG Funk, C Peters-Lidard, CD Verdin, JP AF McNally, Amy Arsenault, Kristi Kumar, Sujay Shukla, Shraddhanand Peterson, Pete Wang, Shugong Funk, Chris Peters-Lidard, Christa D. Verdin, James P. TI Data Descriptor: A land data assimilation system for sub-Saharan Africa food and water security applications SO SCIENTIFIC DATA LA English DT Article; Data Paper ID SATELLITE RAINFALL PRODUCTS; SOIL-MOISTURE; WEST-AFRICA; EAST-AFRICA; SURFACE MODEL; PRECIPITATION CLIMATOLOGY; DROUGHT; FRAMEWORK; RETRIEVALS; VALIDATION AB Seasonal agricultural drought monitoring systems, which rely on satellite remote sensing and land surface models (LSMs), are important for disaster risk reduction and famine early warning. These systems require the best available weather inputs, as well as a long-term historical record to contextualize current observations. This article introduces the Famine Early Warning Systems Network (FEWS NET) Land Data Assimilation System (FLDAS), a custom instance of the NASA Land Information System (LIS) framework. The FLDAS is routinely used to produce multi-model and multi-forcing estimates of hydro-climate states and fluxes over semi-arid, food insecure regions of Africa. These modeled data and derived products, like soil moisture percentiles and water availability, were designed and are currently used to complement FEWS NET's operational remotely sensed rainfall, evapotranspiration, and vegetation observations. The 30+ years of monthly outputs from the FLDAS simulations are publicly available from the NASA Goddard Earth Science Data and Information Services Center (GES DISC) and recommended for use in hydroclimate studies, early warning applications, and by agro-meteorological scientists in Eastern, Southern, and Western Africa. C1 [McNally, Amy] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. [McNally, Amy; Arsenault, Kristi; Kumar, Sujay; Wang, Shugong; Peters-Lidard, Christa D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Arsenault, Kristi; Wang, Shugong] SAIC Inc, Mclean, VA 22102 USA. [Shukla, Shraddhanand; Peterson, Pete; Funk, Chris] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA. [Shukla, Shraddhanand; Peterson, Pete; Funk, Chris] Univ Calif Santa Barbara, Climate Hazards Grp, Santa Barbara, CA 93106 USA. [Funk, Chris; Verdin, James P.] US Geol Survey, Earth Resources Observat & Sci EROS Ctr, Sioux Falls, SD 57105 USA. RP McNally, A (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.; McNally, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM amy.l.mcnally@nasa.gov RI Kumar, Sujay/B-8142-2015; Peters-Lidard, Christa/E-1429-2012 OI Peters-Lidard, Christa/0000-0003-1255-2876 FU NASA Earth Science Applications: Water Resources program [13-WATER13-0010]; NASA ROSES [08-0070]; NASA's Science Mission Directorate (SMD) FX We gratefully acknowledge the financial support from the NASA Earth Science Applications: Water Resources program award 13-WATER13-0010. Computing was supported by the resources at the NASA Center for Climate Simulation (NCCS).; Initial support was provided by NASA ROSES Decisions-08-0070 'A Land Data Assimilation System for Famine Early Warning', continued support provided by FEWS NET's Participating Agency Program Agreement Water Availability Monitoring Activity. Some analyses and visualizations used in this paper were produced with the Giovanni online data system, developed and maintained by the NASA GES DISC. Distribution of data from the Goddard Earth Sciences Data and Information Services Center (GES DISC) is funded by NASA's Science Mission Directorate (SMD). We would also like to thank Diego Pedreros for WRSI estimates, Shahriar Pervez for feedback on remotely sensed and FLDAS soil moisture comparisons, and Greg Husak for feedback on earlier versions of the figures and analysis. NR 72 TC 0 Z9 0 U1 2 U2 2 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2052-4463 J9 SCI DATA JI Sci. Data PD FEB 14 PY 2017 VL 4 AR UNSP 170012 DI 10.1038/sdata.2017.12 PG 19 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EK3VF UT WOS:000393855800002 ER PT J AU Liu, XM Shemansky, DE Yoshii, J Liu, MJ Johnson, PV Malone, CP AF Liu, Xianming Shemansky, Donald E. Yoshii, Jean Liu, Melinda J. Johnson, Paul V. Malone, Charles P. TI Energies, transition probabilities, predissociation rates, and lifetimes of the H-2, HD, and D-2 c (3)Pi(-)(u) state SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article DE predissociation rates; transition probabilities; energies; lifetimes; metastable molecular hydrogen ID ELECTRON-IMPACT EXCITATION; QUANTUM-DEFECT THEORY; INFRARED-LASER SPECTROSCOPY; ANGULAR-MOMENTUM STATES; METASTABLE HYDROGEN MOLECULES; DIFFERENTIAL CROSS-SECTIONS; MINIMUM 1-SIGMA-G+ STATES; TRIPLET GERADE COMPLEX; AB-INITIO CALCULATION; D2 RYDBERG STATES AB Transition probabilities of H-2, HD, and D-2 c (3)Pi(-)(u) -a (3)Sigma(+)(g) electric dipole, c (3)Pi(-)(u) -b (3)Sigma(+)(u) discrete-continuum magnetic dipole, and electric quadrupole transitions have been calculated using accurate energies and ro-vibrational wave functions obtained from precise ab initio potential energy curves. The predissociation rates of the c (3)Pi(-)(u) (v, N) levels by direct and indirect spin-spin and spin-orbit coupling between c (3)Pi(u) -b (3)Sigma(+)(u) fine structure levels, have been also determined. The present investigation achieved good agreement with measured lifetimes of the c (3)Pi(-)(u) fine structure levels without adjustment. A comparison of the calculated and observed lifetimes of metastable H-2, HD, and D-2 suggests that the c (3)Pi(-)(u) -b (3)Sigma(+)(u) magnetic dipole and electric quadrupole transition moments underestimate the spontaneous emission rate of the metastable levels by similar to 370 s(-1). The measured and calculated lifetimes of H-2, HD, and D-2 fine structure levels are in very good agreement after the adjustment of 370 s(-1) to the spontaneous decay rate of the c (3)Pi(-)(u) -b (3)Sigma(+)(u) transition. The calculated energies, transition probabilities, and predissociation rates obtained in the present work, along with the c (3)Pi(u) state excitation function, are sufficient to determine the c (3)Pi(u) state emission cross section, the kinetic energy distribution of H(1s) atoms, and the energy deposition rate of the (1)Sigma(+)(g) -c (3)Pi(u) excitation. In a previous investigation by Berg and Ottinger (1994 J. Chem. Phys. 100 8746), the authors were forced to insert a large scale factor into the predissociation rate in order to reconcile with measured lifetimes. Errors introduced in the approximations made in the previous investigations are discussed in the text. The H-2 c (3)Pi(u) state has the second largest triplet state excitation cross section. Predissociation and spontaneous emission of the c (3)Pi(u) state plays an important role in the energy deposition of H-2-dominated atmospheres. C1 [Liu, Xianming; Shemansky, Donald E.; Yoshii, Jean; Liu, Melinda J.] Space Environm Technol, Planetary & Space Sci Div, 1676 Palisades Dr, Pacific Palisades, CA 90272 USA. [Johnson, Paul V.; Malone, Charles P.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Liu, XM (reprint author), Space Environm Technol, Planetary & Space Sci Div, 1676 Palisades Dr, Pacific Palisades, CA 90272 USA. EM xliu@spacewx.com FU National Aeronautics and Space Administration (NASA); NASA's Planetary Atmospheres (PATM) program; NASA's Astrophysics Research and Analysis (APRA) program; National Science Foundation's AST program [1518304]; Cassini UVIS; University of Colorado FX The analysis described in this paper was carried out at Space Environment Technologies. A portion of the work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). We gratefully acknowledge financial support through NASA's Planetary Atmospheres (PATM) and Astrophysics Research and Analysis (APRA) programs, through the National Science Foundation's AST program (#1518304), and through a Cassini UVIS contract with the University of Colorado. NR 143 TC 0 Z9 0 U1 4 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD FEB 14 PY 2017 VL 50 IS 3 AR 035101 DI 10.1088/1361-6455/50/3/035101 PG 21 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA EK6SM UT WOS:000394054400001 ER PT J AU Peelukhana, SV Banerjee, R van de Hoef, TP Kolli, K Effat, M Helmy, T Leesar, M Kerr, H Piek, JJ Succop, P Back, L Arif, I AF Peelukhana, Srikara Viswanath Banerjee, Rupak van de Hoef, Tim P. Kolli, Kranthi Effat, Mohamed Helmy, Tarek Leesar, Massoud Kerr, Hanan Piek, Jan J. Succop, Paul Back, Lloyd Arif, Imran TI Evaluation Of Lesion Flow Coefficient For The Detection Of Coronary Artery Disease In Patient Groups From Two Academic Medical Centers SO JACC-CARDIOVASCULAR INTERVENTIONS LA English DT Meeting Abstract C1 [Peelukhana, Srikara Viswanath; Banerjee, Rupak; Kolli, Kranthi; Succop, Paul] Univ Cincinnati, Cincinnati, OH USA. [van de Hoef, Tim P.; Piek, Jan J.] Acad Med Ctr, Amsterdam, Netherlands. [Effat, Mohamed; Helmy, Tarek; Kerr, Hanan; Arif, Imran] Univ Cincinnati, Med Ctr, Cincinnati, OH 45267 USA. [Leesar, Massoud] Univ Alabama Birmingham, Birmingham, AL USA. [Back, Lloyd] Jet Prop Lab, Pasadena, CA USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 1936-8798 EI 1876-7605 J9 JACC-CARDIOVASC INTE JI JACC-Cardiovasc. Interv. PD FEB 13 PY 2017 VL 10 IS 3 SU S MA CRT-200.29 BP S38 EP S38 PG 1 WC Cardiac & Cardiovascular Systems SC Cardiovascular System & Cardiology GA EP2MJ UT WOS:000397217000109 ER PT J AU Morgenstern, O Hegglin, MI Rozanov, E O'Connor, FM Abraham, NL Akiyoshi, H Archibald, AT Bekki, S Butchart, N Chipperfield, MP Deushi, M Dhomse, SS Garcia, RR Hardiman, SC Horowitz, LW Jockel, P Josse, B Kinnison, D Lin, MY Mancini, E Manyin, ME Marchand, M Marecal, V Michou, M Oman, LD Pitari, G Plummer, DA Revell, LE Saint-Martin, D Schofield, R Stenke, A Stone, K Sudo, K Tanaka, TY Tilmes, S Yamashita, Y Yoshida, K Zeng, G AF Morgenstern, Olaf Hegglin, Michaela I. Rozanov, Eugene O'Connor, Fiona M. Abraham, N. Luke Akiyoshi, Hideharu Archibald, Alexander T. Bekki, Slimane Butchart, Neal Chipperfield, Martyn P. Deushi, Makoto Dhomse, Sandip S. Garcia, Rolando R. Hardiman, Steven C. Horowitz, Larry W. Joeckel, Patrick Josse, Beatrice Kinnison, Douglas Lin, Meiyun Mancini, Eva Manyin, Michael E. Marchand, Marion Marecal, Virginie Michou, Martine Oman, Luke D. Pitari, Giovanni Plummer, David A. Revell, Laura E. Saint-Martin, David Schofield, Robyn Stenke, Andrea Stone, Kane Sudo, Kengo Tanaka, Taichu Y. Tilmes, Simone Yamashita, Yousuke Yoshida, Kohei Zeng, Guang TI Review of the global models used within phase 1 of the Chemistry-Climate Model Initiative (CCMI) SO GEOSCIENTIFIC MODEL DEVELOPMENT LA English DT Review ID GENERAL-CIRCULATION MODEL; CHEMICAL-TRANSPORT MODEL; SUBMODEL SYSTEM MESSY; GASEOUS DRY DEPOSITION; OFFICE UNIFIED MODEL; DOPPLER-SPREAD PARAMETERIZATION; POLAR STRATOSPHERIC CLOUDS; SEMI-LAGRANGIAN ADVECTION; LAND-SURFACE PROCESSES; GRAVITY-WAVE DRAG AB We present an overview of state-of-the-art chemistry-climate and chemistry transport models that are used within phase 1 of the Chemistry-Climate Model Initiative (CCMI-1). The CCMI aims to conduct a detailed evaluation of participating models using process-oriented diagnostics derived from observations in order to gain confidence in the models' projections of the stratospheric ozone layer, tropospheric composition, air quality, where applicable global climate change, and the interactions between them. Interpretation of these diagnostics requires detailed knowledge of the radiative, chemical, dynamical, and physical processes incorporated in the models. Also an understanding of the degree to which CCMI-1 recommendations for simulations have been followed is necessary to understand model responses to anthropogenic and natural forcing and also to explain intermodel differences. This becomes even more important given the ongoing development and the ever-growing complexity of these models. This paper also provides an overview of the available CCMI-1 simulations with the aim of informing CCMI data users. C1 [Morgenstern, Olaf; Zeng, Guang] Natl Inst Water & Atmospher Res NIWA, Wellington, New Zealand. [Hegglin, Michaela I.] Univ Reading, Dept Meteorol, Reading, Berks, England. [Mancini, Eva; Pitari, Giovanni] Univ Aquila, Dept Phys & Chem Sci, Laquila, Italy. [Plummer, David A.] Environm & Climate Change Canada, Montreal, PQ, Canada. [Rozanov, Eugene; Revell, Laura E.; Stenke, Andrea] ETHZ, Inst Atmospher & Climate Sci, Zurich, Switzerland. [Revell, Laura E.] Bodeker Sci, Christchurch, New Zealand. [Garcia, Rolando R.; Kinnison, Douglas; Tilmes, Simone] NCAR, Boulder, CO USA. [Akiyoshi, Hideharu; Yamashita, Yousuke] NIES, Tsukuba, Ibaraki, Japan. [Josse, Beatrice; Marecal, Virginie; Michou, Martine; Saint-Martin, David; Sudo, Kengo] Meteo France CNRS, CNRM, UMR 3589, Toulouse, France. [Joeckel, Patrick] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Phys Atmosphare, Oberpfaffenhofen, Germany. [Schofield, Robyn; Stone, Kane] Univ Melbourne, Sch Earth Sci, Melbourne, Vic, Australia. [Manyin, Michael E.; Oman, Luke D.] NASA, GSFC, Greenbelt, MD USA. [Horowitz, Larry W.; Lin, Meiyun] NOAA, GFDL, Princeton, NJ USA. [O'Connor, Fiona M.; Butchart, Neal; Hardiman, Steven C.] MOHC, Exeter, Devon, England. [Deushi, Makoto; Tanaka, Taichu Y.; Yoshida, Kohei] Mission Res Inc, Tsukuba, Ibaraki, Japan. [Chipperfield, Martyn P.; Dhomse, Sandip S.] Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England. [Abraham, N. Luke; Archibald, Alexander T.] Univ Cambridge, Dept Chem, Cambridge, England. [Rozanov, Eugene] WRC, PMOD, Davos, Switzerland. [Sudo, Kengo] Nagoya Univ, Grad Sch Environm Studies, Nagoya, Aichi, Japan. [Abraham, N. Luke; Archibald, Alexander T.] NCAS, Oxford, England. [Bekki, Slimane; Marchand, Marion] IPSL, LATMOS, Paris, France. [Manyin, Michael E.] Sci Syst & Applicat Inc, Lanham, MD USA. [Lin, Meiyun] Princeton Univ, Program Atmospher & Ocean Sci, Princeton, NJ 08544 USA. [Stone, Kane] MIT, Boston, MA USA. [Yamashita, Yousuke] Japan Agcy Marine Earth Sci & Technol JAMSTEC, Yokohama, Kanagawa, Japan. RP Morgenstern, O (reprint author), Natl Inst Water & Atmospher Res NIWA, Wellington, New Zealand. EM olaf.morgenstern@niwa.co.nz RI Jockel, Patrick/C-3687-2009; Dhomse, Sandip/C-8198-2011 OI Jockel, Patrick/0000-0002-8964-1394; Dhomse, Sandip/0000-0003-3854-5383 FU NIWA; Royal Society Marsden Fund [12-NIW-006]; Deep South National Science Challenge; NeSI; Ministry of Business, Innovation & Employment's Research Infrastructure programme; Swiss National Science Foundation [CRSII2_147659 (FUPSOL II)]; Environment Research and Technology Development Fund of the Ministry of the Environment, Japan [2-1303]; UK DECC/Defra Met Office Hadley Centre Climate Programme [GA01101]; European Project [603557-STRATOCLIM, FP7-ENV.2013.6.1-2]; Horizon European Union's Framework Programme for Research and Innovation CRESCENDO project [641816]; Centre National d'Etudes Spatiales (CNES, France) within the SOLSPEC project; Australian Government's Australian Antarctic science grant program [FoRCES 4012]; Australian Research Council's Centre of Excellence for Climate System Science [CE110001028]; Commonwealth Department of the Environment [2011/16853]; National computational infrastructure INCMAS project [q90]; Meteo-France; CNRS; CERFACS FX We thank the Centre for Environmental Data Analysis (CEDA) for hosting the CCMI data archive. This work has been supported by NIWA as part of its government-funded, core research. Olaf Morgenstern acknowledges support from the Royal Society Marsden Fund, grant 12-NIW-006, and under the Deep South National Science Challenge.. The authors wish to acknowledge the contribution of NeSI high-performance computing facilities to the results of this research. New Zealand's national facilities are provided by the New Zealand eScience Infrastructure (NeSI) and funded jointly by NeSI's collaborator institutions and through the Ministry of Business, Innovation & Employment's Research Infrastructure programme (https://www.nesi.org.nz). The SOCOL team acknowledges support from the Swiss National Science Foundation under grant agreement CRSII2_147659 (FUPSOL II). CCSRNIES's research was supported by the Environment Research and Technology Development Fund (2-1303) of the Ministry of the Environment, Japan, and computations were performed on NEC-SX9/A(ECO) computers at the CGER, NIES. Wuhu Feng (NCAS) provided support for the TOMCAT simulations. Neal Butchart, Steven C. Hardiman, and Fiona M. O'Connor and the development of HadGEM3-ES were supported by the Joint UK DECC/Defra Met Office Hadley Centre Climate Programme (GA01101). Neal Butchart and Steven C. Hardiman also acknowledge additional support from the European Project 603557-STRATOCLIM under the FP7-ENV.2013.6.1-2 programme. Fiona M. O'Connor acknowledges additional support from the Horizon 2020 European Union's Framework Programme for Research and Innovation CRESCENDO project under grant agreement no. 641816. Slimane Bekki acknowledges support from the European Project 603557-STRATOCLIM under the FP7-ENV. 2013.6.1-2 programme and from the Centre National d'Etudes Spatiales (CNES, France) within the SOLSPEC project. Kane Stone and Robyn Schofield acknowledge funding from the Australian Government's Australian Antarctic science grant program (FoRCES 4012), the Australian Research Council's Centre of Excellence for Climate System Science (CE110001028), the Commonwealth Department of the Environment (grant 2011/16853), and computational support from National computational infrastructure INCMAS project q90. The CNRM-CM chemistry-climate people acknowledge the support from Meteo-France, CNRS, and CERFACS, and in particular the work of the entire team in charge of the CNRM/CERFACS climate model. NR 262 TC 2 Z9 2 U1 0 U2 0 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1991-959X EI 1991-9603 J9 GEOSCI MODEL DEV JI Geosci. Model Dev. PD FEB 13 PY 2017 VL 10 IS 2 BP 639 EP 671 DI 10.5194/gmd-10-639-2017 PG 33 WC Geosciences, Multidisciplinary SC Geology GA EM1YN UT WOS:000395113300001 ER PT J AU Ryan, NJ Palm, M Raffalski, U Larsson, R Manney, G Millan, L Notholt, J AF Ryan, Niall J. Palm, Mathias Raffalski, Uwe Larsson, Richard Manney, Gloria Millan, Luis Notholt, Justus TI Strato-mesospheric carbon monoxide profiles above Kiruna, Sweden (67.8 degrees N, 20.4 degrees E), since 2008 SO EARTH SYSTEM SCIENCE DATA LA English DT Article ID MICROWAVE RADIOMETER; MIDDLE ATMOSPHERE; WATER-VAPOR; CO; SATELLITE; RETRIEVAL; TRANSPORT; WINTER AB This paper presents the retrieval and validation of a self-consistent time series of carbon monoxide (CO) above Kiruna using measurements from the Kiruna Microwave Radiometer (KIMRA). The data set currently spans the years 2008-2015, and measurements are ongoing at Kiruna. The spectra are inverted using an optimal estimation method to retrieve altitude profiles of CO concentrations in the atmosphere within an average altitude range of 48-84 km. Atmospheric temperature data from the Special Sensor Microwave Imager/Sounder aboard the US Air Force meteorological satellite DMSP-F18, are used in the inversion of KIMRA spectra between January 2011 and May 2014. This KIMRA CO data set is compared with CO data from the Microwave Limb Sounder aboard the Aura satellite: there is a maximum bias for KIMRA of similar to 0.65 ppmv at 68 km (corresponding to 14.7% of the mean CO value at 68 km) and a maximum relative bias of 22% (0.44 ppmv) at 60 km. Standard deviations of the differences between profiles are similar in magnitude to the estimated uncertainties in the profiles. Correlations between the instruments are within 0.87 and 0.94. These numbers indicate agreement between the instruments. To expand the CO data set outside of the lifetime of DMSP-F18, another inversion setup was used that incorporates modelled temperatures from the European Centre for Medium-Range Weather Forecasts. The effect on the retrieved CO profiles when using a different temperature data set in the inversion was assessed. A comparison of the two overlapping KIMRA CO data sets shows a positive bias of < 5% in the extended data set and a correlation > 0.98 between the lower retrievable altitude limit and 82.5 km. The extended data set shows a larger range (<= 6 %) of CO concentrations that is not explained by random error estimates. Measurements are continuing and the extended KIMRA CO time series currently spans 2008-2015, with gaps corresponding to non-operation and summer periods when CO concentrations below similar to 90 km drop to very low values. C1 [Ryan, Niall J.; Palm, Mathias; Notholt, Justus] Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany. [Raffalski, Uwe] Swedish Inst Space Phys, Box 812, S-98128 Kiruna, Sweden. [Larsson, Richard] Natl Inst Informat & Commun Technol, Tokyo, Japan. [Manney, Gloria] NorthWest Res Associates, Socorro, NM USA. [Manney, Gloria] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA. [Millan, Luis] Jet Prop Lab, M-S 183-701,4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Ryan, NJ (reprint author), Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany. EM n_ryan@iup.physik.uni-bremen.de RI Millan, Luis/J-2759-2015 FU German Federal Ministry of Education and Research (BMBF) [01LG1214A] FX This work has been funded by the German Federal Ministry of Education and Research (BMBF) through the research project: Role Of the Middle atmosphere in Climate (ROMIC), sub-project ROMICCO, project number 01LG1214A. We would like to express our gratitude to the MLS teams for making their CO and sPV products available. We would also like to thank the ECMWF and NCEP teams for making their products available, as well as the Qpack and ARTS communities for making their software available. Work at the Jet Propulsion Laboratory, California Institute of Technology, was done under contract with the National Aeronautics and Space Administration. We thank the editor and three anonymous referees for their valuable input to the paper. Thank you to Dagmar Eikenroth, Gerrit Armbrecht, and Helen Imhoff for making the published version of the paper look nice. NR 48 TC 0 Z9 0 U1 1 U2 1 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1866-3508 EI 1866-3516 J9 EARTH SYST SCI DATA JI Earth Syst. Sci. Data PD FEB 13 PY 2017 VL 9 IS 1 BP 77 EP 89 DI 10.5194/essd-9-77-2017 PG 13 WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Geology; Meteorology & Atmospheric Sciences GA EM1XL UT WOS:000395110500001 ER PT J AU Karim, MT Mamajek, EE AF Karim, M. T. Mamajek, Eric E. TI Revised geometric estimates of the North Galactic Pole and the Sun's height above the Galactic mid-plane SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE Galaxy: centre; Galaxy: disc; Galaxy: fundamental parameters; Galaxy: general; Galaxy: kinematics and dynamics; Galaxy: structure ID WOLF-RAYET STARS; OPEN CLUSTERS; MILKY-WAY; COORDINATE SYSTEM; SOLAR NEIGHBORHOOD; INTERSTELLAR EXTINCTION; SPATIAL-DISTRIBUTION; STELLAR POPULATION; INNER GALAXY; CATALOG AB Astronomers are entering an era of mu as-level astrometry utilizing the 5-decade-old IAU Galactic coordinate system which was only originally defined to similar to 0 degrees.1 accuracy, and where the dynamical centre of the Galaxy (Sgr A*) is located similar to 0 degrees.07 from the origin. We calculate new independent estimates of the North Galactic Pole (NGP) using recent catalogues of Galactic disc tracer objects such as embedded and open clusters, infrared bubbles, dark clouds and young massive stars. Using these catalogues, we provide two new estimates of the NGP. Solution 1 is an 'unconstrained' NGP determined by the Galactic tracer sources, which does not take into account the location of Sgr A*, and which lies 90.degrees 120 +/- 0 degrees.029 from Sgr A*, and Solution 2 is a 'constrained' NGP which lies exactly 90 degrees from Sgr A*. The 'unconstrained' NGP has International Celestial Reference System (ICRS) position: alpha(NGP) = 192 degrees.729 +/- 0 degrees.035, delta(NGP) = 27 degrees.084 +/- 0 degrees.023 and theta= 122 degrees.928 +/- 0 degrees.016. The 'constrained' NGP which lies exactly 90 theta away from Sgr A* has ICRS position: alpha(NGP) = 192 degrees.728 +/- 0 degrees.010, delta(NGP) = 26 degrees.863 +/- 0 degrees.019 and theta = 122 degrees.928 +/- 0 degrees.016. The difference between the solutions is likely due to the Sun lying above the Galactic mid-plane. Considering the angular separation between Sgr A* and our unconstrained NGP, and if one adopts the recent estimate of the Galactocentric distance for the Sun of R-0 = 8.2 +/- 0.1 kpc, then we estimate that the Sun lies z(circle dot) similar or equal to 17 +/- 5 pc above the Galactic mid-plane. Our value of z(circle dot) is consistent with the true median of 55 previous estimates published over the past century of the Sun's height above the Galactic mid-plane (z(circle dot) similar or equal to 17 +/- 2 pc). C1 [Karim, M. T.; Mamajek, Eric E.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Mamajek, Eric E.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Karim, MT (reprint author), Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. EM mkarim2@u.rochester.edu FU University of Rochester Research Experience for Undergraduates (REU) programme [PHY-1156339]; National Science Foundation (NSF) [AST-1313029]; NASA Nexus for Exoplanet System Science (NExSS) programme FX MTK participated in the summer 2014 University of Rochester Research Experience for Undergraduates (REU) programme supported by PHY-1156339. MTK and EEM acknowledge support from the National Science Foundation (NSF) awards AST-1313029. EEM acknowledges support from the NASA Nexus for Exoplanet System Science (NExSS) programme. We thank Eric Feigelson, Segev Ben-Zvi, Sanha Cheong and Alec Kirkley for discussions on statistics, and Matthias Steinmetz for discussions at the 2015 IAU meeting on the Milky Way. NR 97 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 FEB 11 PY 2017 VL 465 IS 1 BP 472 EP 481 DI 10.1093/mnras/stw2772 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EK2UK UT WOS:000393782000034 ER PT J AU Soam, A Maheswar, G Lee, CW Neha, S Andersson, BG AF Soam, A. Maheswar, G. Lee, Chang Won Neha, S. Andersson, B. -G. TI Magnetic field structure of IC 63 and IC 59 associated with HII region Sh 185 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE polarization; ISM: general; ISM: magnetic fields ID BRIGHT-RIMMED CLOUDS; RADIATION-DRIVEN IMPLOSION; TRIGGERED STAR-FORMATION; NEAR-INFRARED POLARIMETRY; H-II REGIONS; PROLATE MOLECULAR CLOUDS; DUST GRAIN ALIGNMENT; IRAS POINT SOURCES; B-TYPE STARS; 350 MU-M AB Bright-rimmed clouds (BRCs) are formed at the periphery of HII regions as the radiation from the central star interacts with dense gas. The ionization and resulting compression of the clouds may lead to cloud disruption causing secondary star formation depending on the stellar and gas parameters. Here we use R-band polarimetry to probe the plane-of-the sky magnetic field for two nearby BRCs, IC 59 and IC 63. Both nebulae are illuminated by gamma Cas with the direction of the ionizing radiation being orientated parallel or perpendicular to the local magnetic field, allowing us to probe the importance of magnetic field pressure in the evolution of BRCs. Because of the proximity of the system (similar to 200 pc), we have acquired a substantial sample of over 500 polarization measurements for stars that form the background to the nebulae. On large scales, the magnetic field geometries of both clouds are anchored to the ambient magnetic field. For IC 63, the magnetic field is aligned parallel to the head-tail morphology of the main condensation, with a convex morphology relative to the direction of the ionizing radiation. We estimate the plane-of-the-sky magnetic field strength in IC 63 to be similar to 90 mu G. In IC 59, the projected magnetic field follows the M-shape morphology of the cloud. Here, field lines present a concave shape with respect to the direction of the ionizing radiation from gamma Cas. Comparing our observations to published theoretical models, we find good general agreement, supporting the importance of magnetic fields in BRC evolution. C1 [Soam, A.; Lee, Chang Won] Korea Astron & Space Sci Inst KASI, 776 Daedeokdae Ro, Daejeon 305348, South Korea. [Soam, A.; Maheswar, G.; Neha, S.] Aryabhatta Res Inst Observ Sci ARIES, Naini Tal 263002, Uttarakhand, India. [Lee, Chang Won] Univ Sci & Technol, 176 Gajeong Dong, Daejeon, South Korea. [Neha, S.] Pt Ravishankar Shukla Univ, Amanaka GE Rd, Raipur 492010, Chhatisgarh, India. [Andersson, B. -G.] NASA, SOFIA Sci Ctr, USRA, Ames Res Ctr, MS N211-3, Moffett Field, CA 94035 USA. RP Soam, A (reprint author), Korea Astron & Space Sci Inst KASI, 776 Daedeokdae Ro, Daejeon 305348, South Korea.; Soam, A (reprint author), Aryabhatta Res Inst Observ Sci ARIES, Naini Tal 263002, Uttarakhand, India. EM archanasoam.bhu@gmail.com FU Basic Science Research Program though the National Research Foundation of Korea (NRF) - Ministry of Education, Science, and Technology [NRF-2016R1A2B4012593] FX The authors thanks the referee for an encouraging report resulting in significant improvement to the paper. We acknowledge the use of SIMBAD and NASA's SkyView facility (http://skyview.gsfc.nasa.gov) located at NASA Goddard Space Flight Center. CWL was supported by the Basic Science Research Program though the National Research Foundation of Korea (NRF) funded by the Ministry of Education, Science, and Technology (NRF-2016R1A2B4012593). AS thanks Piyush Bhardwaj for help during the observations. NR 106 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 FEB 11 PY 2017 VL 465 IS 1 BP 559 EP 568 DI 10.1093/mnras/stw2649 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EK2UK UT WOS:000393782000040 ER PT J AU Sanchez, C Clampitt, J Kovacs, A Jain, B Garcia-Bellido, J Nadathur, S Gruen, D Hamaus, N Huterer, D Vielzeuf, P Amara, A Bonnett, C DeRose, J Hartley, WG Jarvis, M Lahav, O Miquel, R Rozo, E Rykoff, ES Sheldon, E Wechsler, RH Zuntz, J Abbott, TMC Abdalla, FB Annis, J Benoit-Levy, A Bernstein, GM Bernstein, RA Bertin, E Brooks, D Buckley-Geer, E Rosell, AC Kind, MC Carretero, J Crocce, M Cunha, CE D'Andrea, CB da Costa, LN Desai, S Diehl, HT Dietrich, JP Doel, P Evrard, AE Neto, AF Flaugher, B Fosalba, P Frieman, J Gaztanaga, E Gruendl, RA Gutierrez, G Honscheid, K James, DJ Krause, E Kuehn, K Lima, M Maia, MAG Marshall, JL Melchior, P Plazas, AA Reil, K Romer, AK Sanchez, E Schubnell, M Sevilla-Noarbe, I Smith, RC Soares-Santos, M Sobreira, F Suchyta, E Tarle, G Thomas, D Walker, AR Weller, J AF Sanchez, C. Clampitt, J. Kovacs, A. Jain, B. Garcia-Bellido, J. Nadathur, S. Gruen, D. Hamaus, N. Huterer, D. Vielzeuf, P. Amara, A. Bonnett, C. DeRose, J. Hartley, W. G. Jarvis, M. Lahav, O. Miquel, R. Rozo, E. Rykoff, E. S. Sheldon, E. Wechsler, R. H. Zuntz, J. Abbott, T. M. C. Abdalla, F. B. Annis, J. Benoit-Levy, A. Bernstein, G. M. Bernstein, R. A. Bertin, E. Brooks, D. Buckley-Geer, E. Carnero Rosell, A. Kind, M. Carrasco Carretero, J. Crocce, M. Cunha, C. E. D'Andrea, C. B. da Costa, L. N. Desai, S. Diehl, H. T. Dietrich, J. P. Doel, P. Evrard, A. E. Fausti Neto, A. Flaugher, B. Fosalba, P. Frieman, J. Gaztanaga, E. Gruendl, R. A. Gutierrez, G. Honscheid, K. James, D. J. Krause, E. Kuehn, K. Lima, M. Maia, M. A. G. Marshall, J. L. Melchior, P. Plazas, A. A. Reil, K. Romer, A. K. Sanchez, E. Schubnell, M. Sevilla-Noarbe, I. Smith, R. C. Soares-Santos, M. Sobreira, F. Suchyta, E. Tarle, G. Thomas, D. Walker, A. R. Weller, J. CA DES Collaboration TI Cosmic voids and void lensing in the Dark Energy Survey Science Verification data SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: weak; cosmology: observations; large-scale structure of Universe ID DIGITAL SKY SURVEY; COSMOLOGICAL PARAMETERS; DYNAMICAL PROPERTIES; GALAXY SURVEYS; DATA RELEASE; SDSS VOIDS; 1ST DATA; GRAVITY; SIMULATIONS; RESOLUTION AB Cosmic voids are usually identified in spectroscopic galaxy surveys, where 3D information about the large-scale structure of the Universe is available. Although an increasing amount of photometric data is being produced, its potential for void studies is limited since photometric redshifts induce line-of-sight position errors of >= 50 Mpc h(-1)which can render many voids undetectable. We present a new void finder designed for photometric surveys, validate it using simulations, and apply it to the high-quality photo-z redMaGiC galaxy sample of the DES Science Verification data. The algorithm works by projecting galaxies into 2D slices and finding voids in the smoothed 2D galaxy density field of the slice. Fixing the line-of-sight size of the slices to be at least twice the photo-z scatter, the number of voids found in simulated spectroscopic and photometric galaxy catalogues is within 20 per cent for all transverse void sizes, and indistinguishable for the largest voids (R-v >= 70 Mpc h(-1)). The positions, radii, and projected galaxy profiles of photometric voids also accurately match the spectroscopic void sample. Applying the algorithm to the DES-SV data in the redshift range 0.2 < z < 0.8, we identify 87 voids with comoving radii spanning the range 18-120 Mpc h(-1), and carry out a stacked weak lensing measurement. With a significance of 4.4 sigma, the lensing measurement confirms that the voids are truly underdense in the matter field and hence not a product of Poisson noise, tracer density effects or systematics in the data. It also demonstrates, for the first time in real data, the viability of void lensing studies in photometric surveys. C1 [Sanchez, C.; Kovacs, A.; Vielzeuf, P.; Bonnett, C.; Miquel, R.] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain. [Clampitt, J.; Jain, B.; Jarvis, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Garcia-Bellido, J.; Sanchez, E.] Ctr Invest Energet Medioambientales & Tecnol CIEM, E-28040 Madrid, Spain. [Nadathur, S.; D'Andrea, C. B.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Gruen, D.; DeRose, J.; Rykoff, E. S.; Wechsler, R. H.; Cunha, C. E.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA. [Gruen, D.; Rykoff, E. S.; Wechsler, R. H.; Reil, K.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Hamaus, N.; Weller, J.] Univ Munich, Fak Phys, Univ Sternwarte, Scheinerstr 1, D-81679 Munich, Germany. [Huterer, D.; Schubnell, M.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Amara, A.; Hartley, W. G.; Evrard, A. E.] ETH, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland. [DeRose, J.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. [Hartley, W. G.; Abdalla, F. B.; Benoit-Levy, A.; Brooks, D.; Doel, P.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Miquel, R.] Inst Catalana Rec & Estudis Avancats, E-08010 Barcelona, Spain. [Rozo, E.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. [Sheldon, E.] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA. [Zuntz, J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Abbott, T. M. C.; Smith, R. C.; Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, Casilla 603, La Serena, Chile. [Abdalla, F. B.] Rhodes Univ, Dept Phys & Elect, POB 94, Grahamstown 6140, South Africa. [Annis, J.; Buckley-Geer, E.; Flaugher, B.; Frieman, J.; Gutierrez, G.; Soares-Santos, M.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. [Benoit-Levy, A.; Bertin, E.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Benoit-Levy, A.; Bertin, E.] UPMC Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Bernstein, R. A.] Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA. [Carnero Rosell, A.; da Costa, L. N.; Fausti Neto, A.; Sobreira, F.] Lab Interinst Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carnero Rosell, A.; da Costa, L. N.; Maia, M. A. G.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Kind, M. Carrasco; Gruendl, R. A.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Kind, M. Carrasco; Gruendl, R. A.] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA. [Carretero, J.; Crocce, M.; Gaztanaga, E.] CSIC, IEEC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S N, E-08193 Barcelona, Spain. [D'Andrea, C. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Desai, S.; Dietrich, J. P.; Weller, J.] Excellence Cluster Univ, Boltzmannstr 2, D-85748 Garching, Germany. [Desai, S.; Dietrich, J. P.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Evrard, A. E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Frieman, J.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Honscheid, K.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Honscheid, K.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Lima, M.] Univ Sao Paulo, Inst Fis, Dept Fis Mat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil. [Marshall, J. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Melchior, P.] Princeton Univ, Dept Biol, Peyton Hall, Princeton, NJ 08544 USA. [Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England. [Sobreira, F.] Univ Estadual Paulista, Fundamental Res Inst Fis Teor, ICTP South Amer Inst, BR-01140070 Sao Paulo, Brazil. [Suchyta, E.] Oak Ridge Natl Lab, Comp Sci & Math Div, Oak Ridge, TN 37831 USA. [Weller, J.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. RP Sanchez, C (reprint author), Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain. EM csanchez@ifae.es OI Garcia-Bellido, Juan/0000-0002-9370-8360; Sobreira, Flavia/0000-0002-7822-0658 FU 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 andAstro-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's Seventh Framework Programme (FP7)/including ERC grant [240672, 291329, 306478]; NASA through the Einstein Fellowship Program [PF5-160138] FX 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 andAstro-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. Support for DG was provided by NASA through the Einstein Fellowship Program, grant PF5-160138. NR 94 TC 2 Z9 2 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 FEB 11 PY 2017 VL 465 IS 1 BP 746 EP 759 DI 10.1093/mnras/stw2745 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EK2UK UT WOS:000393782000052 ER PT J AU Mancini, L Southworth, J Raia, G Tregloan-Reed, J Molliere, P Bozza, V Bretton, M Bruni, I Ciceri, S D'Ago, G Dominik, M Hinse, TC Hundertmark, M Jorgensen, UG Korhonen, H Rabus, M Rahvar, S Starkey, D Novati, SC Jaimes, RF Henning, T Juncher, D Haugbolle, T Kains, N Popovas, A Schmidt, RW Skottfelt, J Snodgrass, C Surdej, J Wertz, O AF Mancini, L. Southworth, J. Raia, G. Tregloan-Reed, J. Molliere, P. Bozza, V. Bretton, M. Bruni, I. Ciceri, S. D'Ago, G. Dominik, M. Hinse, T. C. Hundertmark, M. Jorgensen, U. G. Korhonen, H. Rabus, M. Rahvar, S. Starkey, D. Novati, S. Calchi Jaimes, R. Figuera Henning, Th. Juncher, D. Haugbolle, T. Kains, N. Popovas, A. Schmidt, R. W. Skottfelt, J. Snodgrass, C. Surdej, J. Wertz, O. TI Orbital alignment and star-spot properties in the WASP-52 planetary system SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; stars: fundamental parameters; stars: individual: WASP-52; planetary systems ID OPTICAL-TRANSMISSION SPECTRUM; STELLAR EVOLUTION DATABASE; HIGH-PRECISION PHOTOMETRY; EXOPLANET HOST STARS; TRANSIT LIGHT-CURVE; MULTICOLOR PHOTOMETRY; PHYSICAL-PROPERTIES; HOT-JUPITER; MODEL ATMOSPHERES; TIDAL-EVOLUTION AB We report 13 high-precision light curves of eight transits of the exoplanet WASP-52 b, obtained by using four medium-class telescopes, through different filters, and adopting the defocussing technique. One transit was recorded simultaneously from two different observatories and another one from the same site but with two different instruments, including a multiband camera. Anomalies were clearly detected in five light curves and modelled as star-spots occulted by the planet during the transit events. We fitted the clean light curves with the JKTEBOP code, and those with the anomalies with the PRISM + GEMC codes in order to simultaneously model the photometric parameters of the transits and the position, size and contrast of each star-spot. We used these new light curves and some from the literature to revise the physical properties of the WASP-52 system. Star-spots with similar characteristics were detected in four transits over a period of 43 d. In the hypothesis that we are dealing with the same star-spot, periodically occulted by the transiting planet, we estimated the projected orbital obliquity of WASP-52 b to be. = 3 degrees.8 +/- 8 degrees.4. We also determined the true orbital obliquity, psi = 20 degrees +/- 50 degrees, which is, although very uncertain, the first measurement of. purely from star-spot crossings. We finally assembled an optical transmission spectrum of the planet and searched for variations of its radius as a function of wavelength. Our analysis suggests a flat transmission spectrum within the experimental uncertainties. C1 [Mancini, L.; Molliere, P.; Ciceri, S.; Rabus, M.; Henning, Th.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Mancini, L.] Osserv Astron Torino, INAF, Via Osservatorio 20, I-10025 Pino Torinese, Italy. [Mancini, L.] Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, I-00133 Rome, Italy. [Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Raia, G.] Osserv Astron Capodimonte, INAF, Via Moiariello 16, I-80131 Naples, Italy. [Tregloan-Reed, J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [D'Ago, G.; Novati, S. Calchi] Univ Salerno, Dipartimenti Fis E R Caianiello, Via Giovanni Paolo II 132, I-84084 Fisciano, SA, Italy. [Bozza, V.; D'Ago, G.] Ist Nazl Fis Nucl, Sez Napoli, Via Cintia, I-80126 Naples, Italy. [Bretton, M.] Observ Baronnies Provencales, Route Nyons, F-05150 Moydans, France. [Bruni, I.] Osservatorio Astron Bologna, INAF, Via Ranzani 1, I-40127 Bologna, Italy. [D'Ago, G.; Novati, S. Calchi] Int Inst Adv Sci Studies, Via G Pellegrino 19, I-84019 Vietri Sul Mare, SA, Italy. [Dominik, M.; Jaimes, R. Figuera] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Hinse, T. C.] Korea Astron & Space Sci Inst, 776 Daedukdae Ro, Daejeon 305348, South Korea. [Hundertmark, M.; Jorgensen, U. G.; Korhonen, H.; Juncher, D.; Haugbolle, T.; Popovas, A.; Skottfelt, J.] Univ Copenhagen, Niels Bohr Inst, Oster Voldgade 5, DK-1350 Copenhagen, Denmark. [Hundertmark, M.; Jorgensen, U. G.; Korhonen, H.; Juncher, D.; Haugbolle, T.; Popovas, A.; Skottfelt, J.] Univ Copenhagen, Ctr Star & Planet Format, Oster Voldgade 5, DK-1350 Copenhagen, Denmark. [Korhonen, H.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark. [Korhonen, H.] Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland. [Rabus, M.] Pontificia Univ Catolica Chile, Inst Astrofis, Av Vicuna Mackenna 4860, Santiago 7820436, Chile. [Rahvar, S.] Sharif Univ Technol, Dept Phys, POB 111559161, Tehran, Iran. [Novati, S. Calchi] CALTECH, NASA, Exoplanet Sci Inst, MS 100-22, Pasadena, CA 91125 USA. [Jaimes, R. Figuera] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Kains, N.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Schmidt, R. W.] Heidelberg Univ, Zentrum Astron, Astron Rech Inst, Monchhofstr 12-14, D-69120 Heidelberg, Germany. [Skottfelt, J.] Open Univ, Ctr Elect Imaging, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Snodgrass, C.] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England. [Surdej, J.] Inst Astrophys & Geophys, Allee 6 Aout 19c, B-4000 Liege, Belgium. RP Mancini, L (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.; Mancini, L (reprint author), Osserv Astron Torino, INAF, Via Osservatorio 20, I-10025 Pino Torinese, Italy.; Mancini, L (reprint author), Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, I-00133 Rome, Italy. EM mancini@mpia-hd.mpg.de FU UGJ from the Danish Natural Science Research Council (FNU); Communaute francaise de Belgique - Actions de recherche concertees - Academie Wallonie-Europe; Korea Research Council for Fundamental Science and Technology (KRCF) through the Young Research Scientist Fellowship Programme; KASI research grant [2014-1-400-06, 2016-1-832-01] FX This paper is based on observations collected with (i) the Zeiss 1.23 m telescope at the Centro Astronomico Hispano Aleman (CAHA) at Calar Alto, Spain; (ii) the Danish 1.54 m telescope at the ESO Observatory in La Silla, Chile; (iii) the Cassini 1.52 m telescope at the Astronomical Observatory of Bologna in Loiano, Italy; (iv) the MPG 2.2 m telescope located at the ESO Observatory in La Silla, Chile. Operations at the Calar Alto telescopes are jointly performed by the Max Planck Institute for Astronomy (MPIA) and the Instituto de Astrofisica de Andaluica (CSIC). Operation of the Danish 1.54 m telescope is financed by a grant to UGJ from the Danish Natural Science Research Council (FNU). Operation of the MPG 2.2 m telescope is jointly performed by the Max Planck Gesellschaft and the European Southern Observatory. GROND was built by the high-energy group of MPE in collaboration with the LSW Tautenburg and ESO, and is operated as a PI-instrument at the MPG 2.2 m telescope. OW and J. Surdej acknowledge support from the Communaute francaise de Belgique - Actions de recherche concertees - Academie Wallonie-Europe. TCH acknowledges financial support from the Korea Research Council for Fundamental Science and Technology (KRCF) through the Young Research Scientist Fellowship Programme and is supported by the KASI research grant 2014-1-400-06 and 2016-1-832-01. The reduced light curves presented in this work will be made available at the CDS (http://cdsweb.u-strasbg.fr/). We thank the anonymous referee for their useful criticisms and suggestions that helped us to improve the quality of this paper. The following internet-based resources were used in research for this paper: the ESO Digitized Sky Survey; the NASA Astrophysics Data System; the SIMBAD data base operated at CDS, Strasbourg, France; the arXiv scientific paper preprint service operated by the Cornell University. NR 56 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 FEB 11 PY 2017 VL 465 IS 1 BP 843 EP 857 DI 10.1093/mnras/stw1987 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EK2UK UT WOS:000393782000059 ER PT J AU Giles, PA Maughan, BJ Dahle, H Bonamente, M Landry, D Jones, C Joy, M Murray, SS van der Pyl, N AF Giles, P. A. Maughan, B. J. Dahle, H. Bonamente, M. Landry, D. Jones, C. Joy, M. Murray, S. S. van der Pyl, N. TI Chandra measurements of a complete sample of X-ray luminous galaxy clusters: the luminosity-mass relation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: general; X-rays: galaxies: clusters ID SCALING RELATIONS; INTRACLUSTER MEDIUM; NONTHERMAL PRESSURE; OBSERVED GROWTH; RICH CLUSTERS; HALO MASS; COSMOLOGICAL CONSTRAINTS; TEMPERATURE RELATION; ANALYTICAL-MODEL; DATA RELEASE AB We present the results of work involving a statistically complete sample of 34 galaxy clusters, in the redshift range 0.15 <= z <= 0.3 observed with Chandra. We investigate the luminositymass (LM) relation for the cluster sample, with the masses obtained via a full hydrostatic mass analysis. We utilize a method to fully account for selection biases when modelling the LM relation, and find that the LM relation is significantly different from the relationmodelled when not account for selection effects. We find that the luminosity of our clusters is 2.2 +/- 0.4 times higher (when accounting for selection effects) than the average for a given mass and its mass is 30 per cent lower than the population average for a given luminosity. Equivalently, using the LM relation measured from this sample without correcting for selection biases would lead to the underestimation by 40 per cent of the average mass of a cluster with a given luminosity. Comparing the hydrostatic masses to mass estimates determined from the YX parameter, we find that they are entirely consistent, irrespective of the dynamical state of the cluster. C1 [Giles, P. A.; Maughan, B. J.; van der Pyl, N.] HH Wills Phys Lab, Tyndall Ave, Bristol BS8 1TL, Avon, England. [Maughan, B. J.] Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0315 Oslo, Norway. [Bonamente, M.; Landry, D.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Bonamente, M.; Joy, M.] NASA, Natl Space Sci & Technol Ctr, Huntsville, AL 35812 USA. [Jones, C.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Giles, PA (reprint author), HH Wills Phys Lab, Tyndall Ave, Bristol BS8 1TL, Avon, England. EM P.Giles@bristol.ac.uk FU UK Science and Technology Facilities Council FX PG acknowledges support from the UK Science and Technology Facilities Council. We thank A. Mantz for useful discussions and for providing additional fits used in the comparison to his work. NR 89 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 FEB 11 PY 2017 VL 465 IS 1 BP 858 EP 884 DI 10.1093/mnras/stw2621 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EK2UK UT WOS:000393782000060 ER PT J AU Arney, GN Meadows, VS Domagal-Goldman, SD Deming, D Robinson, TD Tovar, G Wolf, ET Schwieterman, E AF Arney, Giada N. Meadows, Victoria S. Domagal-Goldman, Shawn D. Deming, Drake Robinson, Tyler D. Tovar, Guadalupe Wolf, Eric T. Schwieterman, Edward TI Pale Orange Dots: The Impact of Organic Haze on the Habitability and Detectability of Earthlike Exoplanets SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; Earth; planets and satellites: atmospheres ID MASS-INDEPENDENT FRACTIONATION; TITANS UPPER-ATMOSPHERE; WEBB-SPACE-TELESCOPE; ARCHEAN EARTH; TRANSMISSION SPECTROSCOPY; EPSILON-ERIDANI; PREBIOTIC EARTH; SUPER EARTHS; COOL STARS; GJ 1214B AB Hazes are common in known planetary atmospheres, and geochemical evidence suggests that early Earth occasionally supported an organic haze with significant environmental and spectral consequences. The UV spectrum of the parent star drives organic haze formation through methane photochemistry. We use a 1D photochemical-climate model to examine production of fractal organic haze on Archean Earth-analogs in the habitable zones of several stellar types: the modern and early Sun, AD Leo (M3.5V), GJ 876 (M4V), epsilon Eridani (K2V), and sigma Botis (F2V). For Archean-like atmospheres, planets orbiting stars with the highest UV fluxes do not form haze because of the formation of photochemical oxygen radicals that destroy haze precursors. Organic hazes impact planetary habitability via UV shielding and surface cooling, but this cooling is minimized around M dwarfs, whose energy is emitted at wavelengths where organic hazes are relatively transparent. We generate spectra to test the detectability of haze. For 10 transits of a planet orbiting GJ 876 observed by the James Webb Space Telescope, haze makes gaseous absorption features at wavelengths < 2.5 mu m 2-10 sigma shallower than a haze-free planet, and methane and carbon dioxide are detectable at >5s. A haze absorption feature can be detected at 5 sigma near 6.3 mu m, but a higher signal-to-noise ratio is needed to distinguish haze from adjacent absorbers. For direct imaging of a planet at 10 pc using a coronagraphic 10 m class ultraviolet-visible-near-infrared telescope, a UV-blue haze absorption feature would be strongly detectable at >12 sigma in 200 hr. C1 [Arney, Giada N.; Meadows, Victoria S.; Tovar, Guadalupe; Schwieterman, Edward] Univ Washington, Dept Astron, Box 351580, U.W. Seattle, Seattle, WA 98195 USA. [Arney, Giada N.; Meadows, Victoria S.; Domagal-Goldman, Shawn D.; Deming, Drake; Robinson, Tyler D.; Schwieterman, Edward] NASA Astrobiol Inst, Virtual Planet Lab, Box 351580, U.W. Seattle, Seattle, WA 98195 USA. [Arney, Giada N.; Meadows, Victoria S.; Schwieterman, Edward] Univ Washington, Astron Program, Box 351580, U.W. Seattle, Seattle, WA 98195 USA. [Arney, Giada N.; Domagal-Goldman, Shawn D.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Road, Greenbelt, MD 20771 USA. [Arney, Giada N.; Schwieterman, Edward] Univ Space Res Assoc, NASA, Postdoctoral Program, Greenbelt, MD 20771 USA. [Deming, Drake] Univ Maryland Baltimore Cty, Dept Astron, Baltimore, MD 20742 USA. [Robinson, Tyler D.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Wolf, Eric T.] Univ Colorado, Boulder Lab Astrophys & Space Phys, Boulder, CO 80303 USA. [Schwieterman, Edward] Univ Calif Riverside, Riverside, CA 92521 USA. [Schwieterman, Edward] Blue Marble Space Inst Sci, 1200 Westlake Ave, N Suite 1006, Seattle, WA 98109 USA. RP Arney, GN (reprint author), Univ Washington, Dept Astron, Box 351580, U.W. Seattle, Seattle, WA 98195 USA. EM giada.n.arney@nasa.gov OI Schwieterman, Edward/0000-0002-2949-2163; Robinson, Tyler/0000-0002-3196-414X; WOLF, ERIC/0000-0002-7188-1648; Domagal-Goldman, Shawn/0000-0003-0354-9325 FU National Aeronautics and Space Administration through the NASA Astrobiology Institute [NNH12ZDA002C, NNA13AA93A]; NASA Planetary Atmospheres Program [NNH13ZDA001N-PATM]; NASA Exobiology Program [NNX10AR17G] FX We are grateful to our anonymous reviewer for their thorough and extremely useful comments that improved our manuscript. This work was performed as part of the NASA Astrobiology Institute's Virtual Planetary Laboratory, supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under solicitation NNH12ZDA002C and Cooperative Agreement Number NNA13AA93A. E.T.W. acknowledges NASA Planetary Atmospheres Program award NNH13ZDA001N-PATM and NASA Exobiology Program award NNX10AR17G for financial support. G.N.A. and E.W.S. acknowledge support from appointments to the NASA Postdoctoral Program, administered by Universities Space Research Association. Simulations were facilitated through the use of the Hyak supercomputer system at the University of Washington eScience Institute. We thank Dave Crisp, Thomas Gautier, Sonny Harman, Jacob Lustig-Yaeger, Aki Roberge, and the whole VPL team for useful conversations and advice on this project. Spectra shown in this work will be archived at the Virtual Planetary Laboratory online spectral database. NR 104 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 FEB 10 PY 2017 VL 836 IS 1 AR 49 DI 10.3847/1538-4357/836/1/49 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EP3TL UT WOS:000397304500001 ER PT J AU Dennis, BR Tolbert, AK Inglis, A Ireland, J Wang, TJ Holman, GD Hayes, LA Gallagher, PT AF Dennis, Brian R. Tolbert, Anne K. Inglis, Andrew Ireland, Jack Wang, Tongjiang Holman, Gordon D. Hayes, Laura A. Gallagher, Peter T. TI Detection and Interpretation of Long-lived X-Ray Quasi-periodic Pulsations in the X-class Solar Flare on 2013 May 14 SO ASTROPHYSICAL JOURNAL LA English DT Article DE 2Sun: corona; Sun: flares; Sun: X-rays, gamma rays ID CORONAL MAGNETIC-FIELD; REGION-IMAGING-SPECTROGRAPH; STANDING SAUSAGE MODES; LOOP OSCILLATIONS; BURST MONITOR; RHESSI; RECONNECTION; MICROWAVE; EMISSION; INTENSITY AB Quasi-periodic pulsations (QPP) seen in the time derivative of the GOES soft X-ray light curves are analyzed for the X3.2 event on 2013 May 14. The pulsations are apparent for a total of at least two hours from the impulsive phase to well into the decay phase, with a total of 163 distinct pulses evident to the naked eye. A wavelet analysis shows that the characteristic timescale of these pulsations increases systematically from similar to 25 s at 01:10 UT, the time of the GOES peak, to similar to 100 s at 02:00 UT. A second "ridge" in the wavelet power spectrum, most likely associated with flaring emission from a different active region, shows an increase from similar to 40 s at 01:40 UT to similar to 100 s at 03:10 UT. We assume that the QPP that produced the first ridge result from vertical kink-mode oscillations of the newly formed loops following magnetic reconnection in the coronal current sheet. This allows us to estimate the magnetic field strength as a function of altitude given the density, loop length, and QPP timescale as functions of time determined from the GOES light curves and RamatyHigh Energy Solar Spectroscopic Imager (RHESSI) images. The calculated magnetic field strength of the newly formed loops ranges from similar to 500 G at an altitude of 24Mm to a low value of similar to 10 G at 60 Mm, in general agreement with the expected values at these altitudes. Fast sausage-mode oscillations are also discussed and cannot be ruled out as an alternate mechanism for producing the QPP. C1 [Dennis, Brian R.; Tolbert, Anne K.; Inglis, Andrew; Ireland, Jack; Wang, Tongjiang; Holman, Gordon D.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Heliophys Sci Div, Code 671, Greenbelt, MD 20771 USA. [Tolbert, Anne K.; Inglis, Andrew; Wang, Tongjiang] Catholic Univ Amer, 620 Michigan Ave NE, Washington, DC 20064 USA. [Ireland, Jack; Hayes, Laura A.] NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Greenbelt, MD 20771 USA. [Hayes, Laura A.; Gallagher, Peter T.] Trinity Coll Dublin, Sch Phys, Dublin 2, Ireland. RP Dennis, BR (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Heliophys Sci Div, Code 671, Greenbelt, MD 20771 USA. EM brian.r.dennis@nasa.gov OI Gallagher, Peter/0000-0001-9745-0400 FU NASA [NNG11PL10A] FX The work of TW was supported by the NASA Cooperative Agreement NNG11PL10A to the Catholic University of America. NR 54 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 FEB 10 PY 2017 VL 836 IS 1 AR 84 DI 10.3847/1538-4357/836/1/84 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EP3TL UT WOS:000397304500036 ER PT J AU Ezer, C Bulbul, E Ercan, EN Smith, RK Bautz, MW Loewenstein, M McDonald, M Miller, ED AF Ezer, Cemile Bulbul, Esra Ercan, E. Nihal Smith, Randall K. Bautz, Mark W. Loewenstein, Mike McDonald, Mike Miller, Eric D. TI Uniform Contribution of Supernova Explosions to the Chemical Enrichment of Abell 3112 out to R-200 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (A3112); galaxies: clusters: intracluster medium; nuclear reactions, nucleosynthesis abundances ID RAY EXCESS EMISSION; GALAXY CLUSTERS; XMM-NEWTON; METAL ABUNDANCE; STAR-FORMATION; IA SUPERNOVAE; CHANDRA OBSERVATIONS; INTRACLUSTER MEDIUM; SUZAKU OBSERVATIONS; CORE-COLLAPSE AB The spatial distribution of the metals residing in the intra-cluster medium (ICM) of galaxy clusters records all the information on a cluster's nucleosynthesis and chemical enrichment history. We present measurements from a total of 1.2. Ms Suzaku XIS and 72. ks Chandra observations of the cool-core galaxy cluster Abell 3112 out to its virial radius (similar to 1470 kpc). We find that the ratio of the observed supernova type Ia explosions to the total supernova explosions has a uniform distribution at a level of 12%-16% out to the cluster's virial radius. The observed fraction of type Ia supernova explosions is in agreement with the corresponding fraction found in our Galaxy and the chemical enrichment of our Galaxy. The non-varying supernova enrichment suggests that the ICM in cluster outskirts was enriched by metals at an early stage before the cluster itself was formed during a period of intense star formation activity. Additionally, we find that the 2D delayed detonation model CDDT produce significantly worse fits to the X-ray spectra compared to simple 1D W7 models. This is due to the relative overestimate of Si, and the underestimate of Mg in these models with respect to the measured abundances. C1 [Ezer, Cemile; Ercan, E. Nihal] Bogazici Univ, Dept Phys, Istanbul, Turkey. [Ezer, Cemile; Smith, Randall K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Bulbul, Esra; Bautz, Mark W.; McDonald, Mike; Miller, Eric D.] MIT, Kavli Inst Astrophys Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Loewenstein, Mike] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Loewenstein, Mike] NASA, Goddard Space Flight Ctr, CRESST, X ray Astrophys Lab, Code 661, Greenbelt, MD 20771 USA. RP Ezer, C (reprint author), Bogazici Univ, Dept Phys, Istanbul, Turkey. EM cemile.ezer@boun.edu.tr OI Ercan, E.Nihal/0000-0003-0639-7048; Smith, Randall/0000-0003-4284-4167 FU NASA [NNX14AF78G, NNX123AE77G, NNX09AV65G, NNX10AV02G]; Bogazici University BAP [5052, Tubitak-113F117] FX We are grateful to the referee for the insight and detailed comments that helped improve the manuscript. The authors thank Francois Mernier and Tulun Ergin for their valuable comments and suggestions. E.B. acknowledges support by NASA through contracts NNX14AF78G and NNX123AE77G. E. N. E. would like to thank both Bogazici University BAP under code 5052 and Tubitak-113F117 for financial support. E. D. M. acknowledges support from NASA grants NNX09AV65G and NNX10AV02G. NR 54 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2017 VL 836 IS 1 AR 110 DI 10.3847/1538-4357/836/1/110 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EP3TL UT WOS:000397304500062 ER PT J AU Keek, L Iwakiri, W Serino, M Ballantyne, DR in't Zand, JJM Strohmayer, TE AF Keek, L. Iwakiri, W. Serino, M. Ballantyne, D. R. in't Zand, J. J. M. Strohmayer, T. E. TI X-Ray Reflection and an Exceptionally Long Thermonuclear Helium Burst from IGR J17062-6143 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion; accretion disks; stars: individual (IGR J17062-6143); stars: neutron; X-rays: binaries; X-rays: bursts ID ACCRETING NEUTRON-STARS; SLIT CAMERA GSC; ANGULAR-DISTRIBUTION; SHELL FLASHES; BLACK-HOLE; MULTIWAVELENGTH OBSERVATIONS; INTERSTELLAR-MEDIUM; IONIZED REFLECTION; AQL X-1; RADIATION AB Thermonuclear X-ray bursts from accreting neutron stars power brief but strong irradiation of their surroundings, providing a unique way to study accretion physics. We analyze MAXI/Gas Slit Camera and Swift/XRT spectra of a day-long flash observed from IGR J17062-6143 in 2015. It is a rare case of recurring bursts at a low accretion luminosity of 0.15% Eddington. Spectra from MAXI, Chandra, and NuSTAR observations taken between the 2015 burst and the previous one in 2012 are used to determine the accretion column. We find it to be consistent with the burst ignition column of 5. x. 1010 g cm-2, which indicates that it is likely powered by burning in a deep helium layer. The burst flux is observed for over a day, and decays as a straight power law: F alpha t(-1.15) . The burst and persistent spectra are well described by thermal emission from the neutron star, Comptonization of this emission in a hot optically thin medium surrounding the star, and reflection off the photoionized accretion disk. At the burst peak, the Comptonized component disappears, when the burst may dissipate the Comptonizing gas, and it returns in the burst tail. The reflection signal suggests that the inner disk is truncated at similar to 10(2) gravitational radii before the burst, but may move closer to the star during the burst. At the end of the burst, the flux drops below the burst cooling trend for 2 days, before returning to the pre-burst level. C1 [Keek, L.; Strohmayer, T. E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, X ray Astrophys Lab, Greenbelt, MD 20771 USA. [Keek, L.] Univ Maryland, CRESST, Dept Astron, College Pk, MD 20742 USA. [Iwakiri, W.; Serino, M.] RIKEN, MAXI Team, 2-1 Hirosawa, Wako, Saitama 3510198, Japan. [Ballantyne, D. R.] Georgia Inst Technol, Ctr Relativist Astrophys, Sch Phys, 837 State St, Atlanta, GA 30332 USA. [in't Zand, J. J. M.] SRON Netherlands, Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. RP Keek, L (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, X ray Astrophys Lab, Greenbelt, MD 20771 USA. EM laurens.keek@nasa.gov OI Ballantyne, David/0000-0001-8128-6976 FU NASA [NNG06EO90A]; National Science Foundation [PHY1430152] FX L. K. is supported by NASA under award number NNG06EO90A. L. K. thanks the International Space Science Institute in Bern, Switzerland for hosting an International Team on X- ray bursts. This work benefited from events supported by the National Science Foundation under Grant No. PHY1430152 (JINA Center for the Evolution of the Elements). This research has made use of MAXI data provided by RIKEN, JAXA, and the MAXI team. We thank the Swift observatory for performing the observations described in this paper. NR 98 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 FEB 10 PY 2017 VL 836 IS 1 AR 111 DI 10.3847/1538-4357/836/1/111 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EP3TL UT WOS:000397304500063 ER PT J AU Kumar, P Nakariakov, VM Cho, KS AF Kumar, Pankaj Nakariakov, Valery M. Cho, Kyung-Suk TI Observation of a Short Period Quasi-periodic Pulsation in Solar X-Ray, Microwave, and EUV Emissions SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: flares; Sun: oscillations; Supporting material: animations ID CURRENT LOOP COALESCENCE; CORONAL LOOPS; MAGNETIC RECONNECTION; MAGNETOHYDRODYNAMIC OSCILLATIONS; SAUSAGE OSCILLATIONS; RADIO PULSATIONS; STELLAR FLARES; CURRENT SHEET; MODE; ACCELERATION AB This paper presents the multiwavelength analysis of a 13 s quasi-periodic pulsation (QPP) observed in hard X-ray (12-300 keV) and microwave (4.9-34 GHz) emissions during a C-class flare that occurred on 2015 September 21. Atmospheric Image Assembly (AIA) 304 and 171 similar to. images show an emerging loop/ flux tube (L1) moving radially outward, which interacts with the preexisting structures within the active region (AR). The QPP was observed during the expansion of and rising motion of L1. The Nobeyama Radioheliograph microwave images in 17/ 34 GHz channels reveal a single radio source that was co-spatial with a neighboring loop (L2). In addition, using AIA 304 similar to. images, we detected intensity oscillations in the legs of L2 with a period of about 26. s. A similar oscillation period was observed in the GOES soft X-ray flux derivative. This oscillation period seems to increase with time. We suggest that the observed QPP is most likely generated by the interaction between L2 and L3 observed in the AIA hot channels (131 and 94 similar to). The merging speed of loops L2 and L3 was similar to 35 km. s-1.. L1 was destroyed possibly by its interaction with preexisting structures in the AR, and produced a cool jet with the speed of similar to 106-118 km. s(-1) associated with a narrow CME (similar to 770 km. s(-1)). Another mechanism of the QPP in terms of a sausage oscillation of the loop (L2) is also possible. C1 [Kumar, Pankaj; Cho, Kyung-Suk] Korea Astron & Space Sci Inst KASI, Daejeon 305348, South Korea. [Kumar, Pankaj] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Nakariakov, Valery M.] Univ Warwick, Ctr Fus Space & Astrophys, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Nakariakov, Valery M.] Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi, South Korea. [Nakariakov, Valery M.] Russian Acad Sci, Special Astrophys Observ, St Petersburg Branch, St Petersburg 196140, Russia. [Cho, Kyung-Suk] Univ Sci & Technol, Daejeon 305348, South Korea. RP Kumar, P (reprint author), Korea Astron & Space Sci Inst KASI, Daejeon 305348, South Korea. EM pankaj@kasi.re.kr OI Kumar, Dr. Pankaj/0000-0001-6289-7341 FU "Development of the Korea Space Weather Center" of KASI; KASI basic research funds; U.S. Air Force Research Laboratory [FA 2386-14-1-4078]; "Planetary System Research for Space Exploration" from KASI; European Research Council under the SeismoSun Research Project [321141]; BK21 plus program through the National Research Foundation - Ministry of Education of Korea FX SDO is a mission for the NASA Living With a Star (LWS) program. This work was supported by the "Development of the Korea Space Weather Center" of KASI and the KASI basic research funds. The SDO data were (partly) provided by the Korean Data Center (KDC) for SDO in cooperation with NASA and the SDO/HMI team. The Nobeyama RadioHeliograph and Polarimeters are operated by the International Consortium for the Continued Operation of Nobeyama. K. S. C. acknowledges the support by a grant from the U.S. Air Force Research Laboratory, under agreement number FA 2386-14-1-4078 and by the "Planetary System Research for Space Exploration" from KASI. V. M. N. acknowledges the support from the European Research Council under the SeismoSun Research Project No. 321141, and the BK21 plus program through the National Research Foundation funded by the Ministry of Education of Korea. Wavelet software was provided by C. Torrence and G. Compo, and is available at http://paos.colorado.edu/research/wavelets/. This work was (partly) carried out on the Solar Data Analysis System operated by the Astronomy Data Center in cooperation with the Solar Observatory of the National Astronomical Observatory of Japan. NR 51 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 FEB 10 PY 2017 VL 836 IS 1 AR 121 DI 10.3847/1538-4357/836/1/121 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EP3TL UT WOS:000397304500073 ER PT J AU Lansbury, GB Stern, D Aird, J Alexander, DM Fuentes, C Harrison, FA Treister, E Bauer, FE Tomsick, JA Balokovic, M Del Moro, A Gandhi, P Ajello, M Annuar, A Ballantyne, DR Boggs, SE Brandt, WN Brightman, M Chen, CTJ Christensen, FE Civano, F Comastri, A Craig, WW Forster, K Grefenstette, BW Hailey, CJ Hickox, RC Jiang, B Jun, HD Koss, M Marchesi, S Melo, AD Mullaney, JR Noirot, G Schulze, S Walton, DJ Zappacosta, L Zhang, WW AF Lansbury, G. B. Stern, D. Aird, J. Alexander, D. M. Fuentes, C. Harrison, F. A. Treister, E. Bauer, F. E. Tomsick, J. A. Balokovic, M. Del Moro, A. Gandhi, P. Ajello, M. Annuar, A. Ballantyne, D. R. Boggs, S. E. Brandt, W. N. Brightman, M. Chen, C. -T. J. Christensen, F. E. Civano, F. Comastri, A. Craig, W. W. Forster, K. Grefenstette, B. W. Hailey, C. J. Hickox, R. C. Jiang, B. Jun, H. D. Koss, M. Marchesi, S. Melo, A. D. Mullaney, J. R. Noirot, G. Schulze, S. Walton, D. J. Zappacosta, L. Zhang, W. W. TI The NuSTAR Serendipitous Survey: The 40-month Catalog and the Properties of the Distant High-energy X-Ray Source Population SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; galaxies: active; galaxies: nuclei; quasars: general; surveys; Xrays: general Supporting material: figure sets; machine-readable tables ID ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; MEDIUM-SENSITIVITY SURVEY; SEYFERT 1 GALAXIES; POINT-SOURCE CATALOGS; DIGITAL SKY SURVEY; AREA SURVEY HELLAS; SWIFT-BAT SURVEY; SPECTRAL PROPERTIES; OPTICAL-IDENTIFICATION AB We present the first full catalog and science results for the Nuclear Spectroscopic Telescope Array (NuSTAR) serendipitous survey. The catalog incorporates data taken during the first 40 months of NuSTAR operation, which provide approximate to 20 Ms of effective exposure time over 331 fields, with an areal coverage of 13 deg2, and 497 sources detected in total over the 324 keV energy range. There are 276 sources with spectroscopic redshifts and classifications, largely resulting from our extensive campaign of ground-based spectroscopic follow-up. We characterize the overall sample in terms of the X-ray, optical, and infrared source properties. The sample is primarily composed of active galactic nuclei (AGNs), detected over a large range in redshift from z = 0.002 to 3.4 (median of < Z > = 0.56), but also includes 16 spectroscopically confirmed Galactic sources. There is a large range in X-ray flux, from log(L10-40 (keV)/erg s(-1) cm(-2)) approximate to-14 to -11, and in rest-frame 1040 keV luminosity, from log(L10-40 (keV)/erg s(-1)) approximate to 39 to 46, with a median of 44.1. Approximately 79% of the NuSTAR sources have lower-energy (<10 keV) X-ray counterparts from XMM-Newton, Chandra, and Swift XRT. The mid-infrared (MIR) analysis, using WISE all-sky survey data, shows that MIR AGN color selections miss a large fraction of the NuSTAR-selected AGN population, from (similar to)15% at the highest luminosities (L-X >10(44) erg s(-1)) to approximate to 80% at the lowest luminosities (L-X <10(43) erg s(-1)). Our optical spectroscopic analysis finds that the observed fraction of optically obscured AGNs (i.e., the type 2 fraction) is F-TYPE (2) =53(-15)(+14)% , for a well-defined subset of the 824 keV selected sample. This is higher, albeit at a low significance level, than the type 2 fraction measured for redshift- and luminosity-matched AGNs selected by <10 keV X-ray missions. C1 [Lansbury, G. B.; Aird, J.; Alexander, D. M.; Del Moro, A.; Gandhi, P.; Annuar, A.] Univ Durham, Ctr Extragalact Astron, Dept Phys, South Rd, Durham DH1 3LE, England. [Lansbury, G. B.; Aird, J.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Stern, D.; Jun, H. D.; Noirot, G.; Walton, D. J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 169-221, Pasadena, CA 91109 USA. [Fuentes, C.; Treister, E.; Melo, A. D.] Univ Concepcion, Dept Astronom, Casilla 160-C, Concepcion, Chile. [Harrison, F. A.; Balokovic, M.; Brightman, M.; Forster, K.; Grefenstette, B. W.; Jiang, B.; Walton, D. J.] CALTECH, Cahill Ctr Astrophys, 1216 East Calif Blvd, Pasadena, CA 91125 USA. [Treister, E.; Bauer, F. E.; Schulze, S.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, 306, Santiago 22, Chile. [Bauer, F. E.; Schulze, S.] Millennium Inst Astrophys, Vicu Mackenna 4860, Santiago 7820436, Chile. [Bauer, F. E.] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA. [Tomsick, J. A.; Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. [Del Moro, A.] Max Planck Inst Extraterr Phys MPE, Postfach 1312, D-85741 Garching, Germany. [Gandhi, P.] Univ Southampton, Sch Phys & Astron, Highfield, Southampton SO17 1BJ, Hants, England. [Ajello, M.; Marchesi, S.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Brandt, W. N.; Chen, C. -T. J.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, Elektrovej 327, DK-2800 Lyngby, Denmark. [Civano, F.] Yale Univ, Yale Ctr Astron & Astrophys, Dept Phys, New Haven, CT 06520 USA. [Civano, F.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Comastri, A.] INAF Osservatorio Astronomico Bologna, Via Ranzani 1, I-40127 Bologna, Italy. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, 550 W 120th St, Columbia, NY 10027 USA. [Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, 6127 Wilder Lab, Hanover, NH 03755 USA. [Koss, M.] Swiss Fed Inst Technol, Inst Astron, Dept Phys, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. [Mullaney, J. R.] Univ Sheffield, Dept Phys & Astron, Hounsfield Rd, Sheffield S3 7RH, S Yorkshire, England. [Noirot, G.] Univ Paris Diderot Paris VII, Univ Paris Sorbonne Cite PSC, F-75205 Paris 13, France. [Zappacosta, L.] INAF Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy. [Zhang, W. W.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lansbury, GB (reprint author), Univ Durham, Ctr Extragalact Astron, Dept Phys, South Rd, Durham DH1 3LE, England. EM gbl23@ast.cam.ac.uk FU Science and Technology Facilities Council (STFC) [ST/K501979/1, ST/I001573/1, ST/J003697/2]; Herchel Smith Postdoctoral Fellowship of the University of Cambridge; ERC Advanced Grant FEEDBACK at the University of Cambridge [340442]; Institute of Advanced Study, Durham University; Leverhulme Trust; CONICYT-Chile [1120061, 1160999, 3140534]; Anillo [ACT1101]; Center of Excellence in Astrophysics and Associated Technologies [PFB 06]; NASA Earth and Space Science Fellowship Program [NNX14AQ07H]; NASA [NNG08FD60C]; National Aeronautics and Space Administration FX The authors first thank the anonymous referee for the constructive comments. We acknowledge financial support from the Science and Technology Facilities Council (STFC) grants ST/K501979/1 (G.B.L.), ST/I001573/1 (D.M.A.), and ST/J003697/2 (P.G.); a Herchel Smith Postdoctoral Fellowship of the University of Cambridge (G.B.L.); the ERC Advanced Grant FEEDBACK 340442 at the University of Cambridge (J.A.); a COFUND Junior Research Fellowship from the Institute of Advanced Study, Durham University (J.A.); the Leverhulme Trust (D.M.A.); CONICYT-Chile grants FONDECYT 1120061 and 1160999 (E.T.), 3140534 (S.S.), and Anillo ACT1101 (E.T. and F.E.B.); the Center of Excellence in Astrophysics and Associated Technologies (PFB 06; E.T. and F. E.B.); and the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H (M.B.). We extend gratitude to Felipe Ardila, Roberto Assef, Eduardo Banados, Stanislav George Djorgovski, Andrew Drake, Jack Gabel, Audrey Galametz, Daniel Gawerc, David Girou, Marianne Heida, Nikita Kamraj, Peter Kosec, Thomas Kruhler, Ashish Mahabal, Alessandro Rettura, and Aaron Stemo for their support during the ground-based follow-up observations. We thank John Lucey for unearthing the J1410 spectrum, and Sophie Reed, David Rosario, Mara Salvato, and Martin Ward for the informative discussions. Additional thanks to Eden Stern for lending a hand during the 2015 August Keck run. 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). NR 135 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 FEB 10 PY 2017 VL 836 IS 1 AR 99 DI 10.3847/1538-4357/836/1/99 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EP3TL UT WOS:000397304500051 ER PT J AU Reeves, KK Freed, MS McKenzie, DE Savage, SL AF Reeves, Katharine K. Freed, Michael S. McKenzie, David E. Savage, Sabrina L. TI An Exploration of Heating Mechanisms in a Supra-arcade Plasma Sheet Formed after a Coronal Mass Ejection SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: coronal mass ejections (CMEs); Sun: flares ID LOCAL CORRELATION TRACKING; X-RAY TELESCOPE; SOLAR-FLARE; MAGNETIC RECONNECTION; ACTIVE REGIONS; FLUX ROPE; EMISSION; DOWNFLOWS; DYNAMICS; HINODE AB We perform a detailed analysis of the thermal structure of the region above the post-eruption arcade for a flare that occurred on 2011 October 22. During this event, a sheet of hot plasma is visible above the flare loops in the 131 angstrom bandpass of the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory. Supra-arcade downflows (SADs) are observed traveling sunward through the post-eruption plasma sheet. We calculate differential emission measures using the AIA data and derive an emission measure weighted average temperature in the supra-arcade region. In areas where many SADs occur, the temperature of the supra-arcade plasma tends to increase, while in areas where no SADs are observed, the temperature tends to decrease. We calculate the plane-ofsky velocities in the supra-arcade plasma and use them to determine the potential heating due to adiabatic compression and viscous heating. Of the 13 SADs studied, 10 have noticeable signatures in both the adiabatic and the viscous terms. The adiabatic heating due to compression of plasma in front of the SADs is on the order of 0.1-0.2MK/ s, which is similar in magnitude to the estimated conductive cooling rate. This result supports the notion that SADs contribute locally to the heating of plasma in the supra-arcade region. We also find that in the region without SADs, the plasma cools at a rate that is slower than the estimated conductive cooling, indicating that. additional heating mechanisms may act globally to keep the plasma temperature high. C1 [Reeves, Katharine K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Freed, Michael S.; McKenzie, David E.] Montana State Univ, Bozeman, MT 59717 USA. [Freed, Michael S.] Radford Univ, Radford, VA 24142 USA. [McKenzie, David E.; Savage, Sabrina L.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Reeves, KK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kreevs@cfa.harvard.edu OI Freed, Michael/0000-0003-3816-031X; Reeves, Katharine/0000-0002-6903-6832 FU NASA [NNX13AG54G, NNX14AD43G, NNX15AJ93G]; Hinode Project Office at Marshall Space Flight Center FX The authors thank the anonymous referee for comments that improved the paper. This work is supported by NASA grants NNX13AG54G, NNX14AD43G, and NNX15AJ93G. S.L.S. is supported by the Hinode Project Office at Marshall Space Flight Center. This work has benefited from the use of NASA's Astrophysics Data System. NR 45 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 FEB 10 PY 2017 VL 836 IS 1 AR 55 DI 10.3847/1538-4357/836/1/55 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EP3TL UT WOS:000397304500007 ER PT J AU Roediger, JC Ferrarese, L Cote, P MacArthur, LA Sanchez-Janssen, R Blakeslee, JP Peng, EW Liu, C Munoz, R Cuillandre, JC Gwyn, S Mei, S Boissier, S Boselli, A Cantiello, M Courteau, S Duc, PA Lancon, A Mihos, JC Puzia, TH Taylor, JE Durrell, PR Toloba, E Guhathakurta, P Zhang, HX AF Roediger, Joel C. Ferrarese, Laura Cote, Patrick MacArthur, Lauren A. Sanchez-Janssen, Ruben Blakeslee, John P. Peng, Eric W. Liu, Chengze Munoz, Roberto Cuillandre, Jean-Charles Gwyn, Stephen Mei, Simona Boissier, Samuel Boselli, Alessandro Cantiello, Michele Courteau, Phane Duc, Pierre-Alain Lancon, Ariane Mihos, J. Christopher Puzia, Thomas H. Taylor, James E. Durrell, Patrick R. Toloba, Elisa Guhathakurta, Puragra Zhang, Hongxin TI The Next Generation Virgo Cluster Survey (NGVS). XXIV. The Red Sequence to similar to 10(6)L(circle dot) and Comparisons with Galaxy Formation Models SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (Virgo); galaxies: dwarf; galaxies: elliptical and lenticular; cD galaxies: evolution; galaxies: stellar content ID COLOR-MAGNITUDE RELATION; STELLAR POPULATION SYNTHESIS; DIGITAL SKY SURVEY; SUPERMASSIVE BLACK-HOLES; STAR-FORMATION HISTORIES; BOUND-CONSTRAINED OPTIMIZATION; COMPACT DWARF GALAXIES; HIGH-REDSHIFT CLUSTERS; DARK-MATTER COSMOLOGY; LOW-MASS GALAXIES AB We use deep optical photometry from the Next Generation Virgo Cluster Survey (NGVS) to investigate the colormagnitude diagram for the galaxies inhabiting the core of this cluster. The sensitivity of the NGVS imaging allows us to continuously probe galaxy colors over a factor of similar to 2 x 105 in luminosity, from brightest cluster galaxies to scales overlapping classical satellites of the Milky Way (M-g' similar to -9; M-*. similar to 10(6)M(circle dot)), within a single environment. Remarkably, we find the first evidence that the red sequence (RS) flattens in all colors at the faint-magnitude end (starting between -14 <= M-g' <= -13, around M-* similar to 4 x 10(7)M(circle dot)), with the slope decreasing to similar to 60% or less of its value at brighter magnitudes. This could indicate that the stellar populations of faint dwarfs in Virgo's core share similar characteristics (e.g., constant mean age) over similar to 3 mag in luminosity, suggesting that these galaxies were quenched coevally, likely via pre-processing in smaller hosts. We also compare our results to galaxy formation models, finding that the RS in model clusters have slopes at intermediate magnitudes that are too shallow, and in the case of semianalytic models, do not reproduce the flattening seen at both extremes (bright/faint) of the Virgo RS. Deficiencies in the chemical evolution of model galaxies likely contribute to the model-data discrepancies at all masses, while overly efficient quenching may also be a factor at dwarf scales. Deep UV and near-IR photometry are required to unambiguously diagnose the cause of the faint-end flattening. C1 [Roediger, Joel C.; Ferrarese, Laura; Cote, Patrick; MacArthur, Lauren A.; Sanchez-Janssen, Ruben; Blakeslee, John P.; Gwyn, Stephen] Natl Res Council Canada, Herzberg Astron & Astrophys Program, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada. [MacArthur, Lauren A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Peng, Eric W.] Peking Univ, Dept Astron, Beijing 100871, Peoples R China. [Peng, Eric W.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Liu, Chengze] Shanghai Jiao Tong Univ, Ctr Astron & Astrophys, Dept Phys & Astron, Shanghai 200240, Peoples R China. [Munoz, Roberto; Puzia, Thomas H.; Zhang, Hongxin] Pontificia Univ Catolica Chile, Inst Astrofis, Av Vicuna Mackenna 4860, Santiago 7820436, Chile. [Cuillandre, Jean-Charles; Duc, Pierre-Alain] Univ Paris Diderot, CNRS INSU, CEA Irfu, AIM Paris Saclay, Orme Merisiers, F-91191 Gif Sur Yvette, France. [Mei, Simona] UPMC Univ Paris 06, Sorbonne Univ, CNRS, LERMA,Observ Paris,PSL Res Univ, F-F75014 Paris, France. [Mei, Simona] Univ Paris Denis Diderot, Univ Paris Sorbonne Cite, F-75205 Paris 13, France. [Mei, Simona] CALTECH, Cahill Ctr Astron & Astrophys Calif, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Boissier, Samuel; Boselli, Alessandro] Aix Marseille Univ, CNRS, Lab Astrophys Marseille UMR 7326, F-13388 Marseille, France. [Cantiello, Michele] INAF Osservatorio Astr Teramo, Via Maggini, I-64100 Teramo, Italy. [Cantiello, Michele] INAF Osservatorio Astr Capodimonte, Salita Moiariello, I-80131 I- Napoli, Italy. [Courteau, Phane] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON, Canada. [Lancon, Ariane] Univ Strasbourg & CNRS UMR 7550, Observ Astronom, 11 rue IUniversity, F-67000 Strasbourg, France. [Mihos, J. Christopher] Case Western Reserve Univ, Dept Astron, Cleveland, OH 41106 USA. [Taylor, James E.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Durrell, Patrick R.] Youngstown State Univ, Dept Phys & Astron, Youngstown, OH 44555 USA. [Toloba, Elisa; Guhathakurta, Puragra] Univ Calif, UCO Lick Observ, 1156 High St, Santa Cruz, CA 95064 USA. [Toloba, Elisa] Texas Tech Univ, Dept Phys, Box 41051, Lubbock, TX 79409 USA. [Zhang, Hongxin] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. RP Roediger, JC (reprint author), Natl Res Council Canada, Herzberg Astron & Astrophys Program, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada. EM Joel.Roediger@nrc-cnrc.gc.ca FU National Natural Science Foundation of China [11173003]; National Key Basic Research Program of China [2015CB857002]; NSFC [11673017, 11203017, 11433002]; CORFO project [15COTE-46317]; French Agence Nationale de la Recherche (ANR) [ANR10-BLANC-0506-01]; Institut Universitaire de France (IUF); PRIN INAF "EXCALIBURS: EXtragalactic distance scale CALIBration Using first-Rank Standard candles"; Natural Science and Engineering Research Council of Canada; FONDECYT [1161817]; BASAL Center for Astrophysics and Associated Technologies [PFB-06]; NSF [AST-1010039, AST-1412504]; Canadian Advanced Network for Astronomical Research (CANFAR); CANARIE under the Network-Enabled Platforms program FX E.W.P. acknowledges support from the National Natural Science Foundation of China, grant 11173003. C.L. acknowledges the National Key Basic Research Program of China (2015CB857002) and the NSFC grants 11673017, 11203017, and 11433002. R.M. acknowledges support from CORFO project No. 15COTE-46317. S.M. acknowledges the support of the French Agence Nationale de la Recherche (ANR), under the reference ANR10-BLANC-0506-01-Projet VIRAGE (PI: S. Mei), and financial support from the Institut Universitaire de France (IUF), of which she is a senior member. M.C. acknowledges partial support from PRIN INAF-2014 "EXCALIBURS: EXtragalactic distance scale CALIBration Using first-Rank Standard candles" (P.I.: G. Clementini). S.C. acknowledges support from the Natural Science and Engineering Research Council of Canada through a generous Research Discovery Grant. T.H.P. acknowledges support through the FONDECYT Regular Project Grant (No. 1161817) and the BASAL Center for Astrophysics and Associated Technologies (PFB-06). E.T. acknowledges the NSF grants AST-1010039 and AST-1412504.; This work was supported in part by the Canadian Advanced Network for Astronomical Research (CANFAR) which has been made possible by funding from CANARIE under the Network-Enabled Platforms program. This research also used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. NR 157 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 FEB 10 PY 2017 VL 836 IS 1 AR 120 DI 10.3847/1538-4357/836/1/120 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EP3TL UT WOS:000397304500072 ER PT J AU Scoville, N Murchikova, L Walter, F Vlahakis, C Koda, J Bout, PV Barnes, J Hernquist, L Sheth, K Yun, M Sanders, D Armus, L Cox, P Thompson, T Robertson, B Zschaechner, L Tacconi, L Torrey, P Hayward, CC Genzel, R Hopkins, P Werf, PD Decarli, R AF Scoville, Nick Murchikova, Lena Walter, Fabian Vlahakis, Catherine Koda, Jin Bout, Paul Vanden Barnes, Joshua Hernquist, Lars Sheth, Kartik Yun, Min Sanders, David Armus, Lee Cox, Pierre Thompson, Todd Robertson, Brant Zschaechner, Laura Tacconi, Linda Torrey, Paul Hayward, Christopher C. Genzel, Reinhard Hopkins, Phil van der Werf, Paul Decarli, Roberto TI ALMA Resolves the Nuclear Disks of Arp 220 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (Arp 220); galaxies: starburst; Galaxy: evolution; ISM: clouds; ISM: molecules ID ULTRALUMINOUS INFRARED GALAXIES; MOLECULAR GAS; NGC 6240; ARP-220; LUMINOSITY; CLOUDS; REGION; HCN; SUPERNOVAE; CONTINUUM AB We present 90 mas (37 pc) resolution ALMA imaging of Arp 220 in the CO (1-0) line and continuum at gimel = 2.6 mm. The internal gas distribution and kinematics of both galactic nuclei are well. resolved for the first time. In the west nucleus, the major gas and dust emission extends out to 0 2 radius (74 pc); the central resolution element shows a strong peak in the dust emission but a factor of. 3 dip in the CO line emission. In this nucleus, the dust is apparently optically thick (tau(2.6) mm similar to 1) at lambda = 2.6 mm with a dust brightness temperature of similar to 147 K. The column of interstellar matter. at this nucleus is NH2. 2 x 10(26) cm(-2), corresponding to similar to 900 gr cm(-2). The east nucleus is more elongated with radial extent 0 3 or similar to 111 pc. The derived kinematics of the nuclear disks provide a good fit to the line profiles, yielding the emissivity distributions, the rotation curves, and velocity dispersions. In the west nucleus, there is evidence of a central Keplerian component requiring a central mass of 8 x 10(8) M-circle dot. The intrinsic widths of the emission lines are Delta v(FWHM)= 250 (west) and 120 (east) km s(-1). Given the very short dissipation timescales for turbulence (less than or similar to 10(5) years), we suggest that the line widths may be due to semicoherent motions within the nuclear disks. The symmetry of the nuclear disk structures is impressive,. implying the merger timescale is significantly longer than the rotation period of the disks. C1 [Scoville, Nick; Murchikova, Lena; Hopkins, Phil] CALTECH, MC 249-17,1200 East Calif Blvd, Pasadena, CA 91125 USA. [Walter, Fabian; Zschaechner, Laura; Decarli, Roberto] Max Planck Inst Astronomie, Konigstuhl 17, D-69117 Heidelberg, Germany. [Vlahakis, Catherine; Bout, Paul Vanden] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22901 USA. [Koda, Jin] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Barnes, Joshua; Yun, Min] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan. [Barnes, Joshua; Sanders, David] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. [Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Sheth, Kartik] NASA Headquarters, 300 St SW, Washington, DC 20546 USA. [Armus, Lee] CALTECH, Infrared Proc & Anal Ctr, 1200 E Calif Blvd, Pasadena, CA 91125 USA. [Cox, Pierre] Joint ALMA Observ, Alonso Cordova 3107, Santiago, Chile. [Cox, Pierre] European Southern Observ, Alonso Cordova 3107, Santiago, Chile. [Thompson, Todd] Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA. [Thompson, Todd] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, 191 West Woodruff Ave, Columbus, OH 43210 USA. [Robertson, Brant] Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA. [Tacconi, Linda] Max Planck Inst extraterrestr Physik MPE, Giessenbachstr, D-85748 Garching, Germany. [Torrey, Paul] CALTECH, TAPIR 35017, 1200 E Calif Blvd, Pasadena, CA 91125 USA. [Torrey, Paul] MIT, Kavli Inst Astrophys & Space Res, Dept Phys, Cambridge, MA 02139 USA. [van der Werf, Paul] Leiden Univ, Leiden Observ, PO Box 9513, NL-2300 RA Leiden, Netherlands. RP Scoville, N (reprint author), CALTECH, MC 249-17,1200 East Calif Blvd, Pasadena, CA 91125 USA. OI Yun, Min/0000-0001-7095-7543; Koda, Jin/0000-0002-8762-7863; Vlahakis, Catherine/0000-0003-3745-4228 FU National Science Foundation [PHY-1066293]; NSF [1516967]; Simons Foundation FX This paper makes use of the following ALMA data: https://almascience:nrao:edu/aq/?project code = 2015:1:00113: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. This work was done in part at the Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1066293. T.A.T. is supported by NSF Grant #1516967. T.A.T. thanks the Simons Foundation and organizers Juna Kollmeier and Andrew Benson for support for the Galactic Winds: Beyond Phenomenology symposium series. NR 44 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 FEB 10 PY 2017 VL 836 IS 1 AR 66 DI 10.3847/1538-4357/836/1/66 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EP3TL UT WOS:000397304500018 ER PT J AU Temim, T Dwek, E Arendt, RG Borkowski, KJ Reynolds, SP Slane, P Gelfand, JD Raymond, JC AF Temim, Tea Dwek, Eli Arendt, Richard G. Borkowski, Kazimierz J. Reynolds, Stephen P. Slane, Patrick Gelfand, Joseph D. Raymond, John C. TI A Massive Shell of Supernova-formed Dust in SNR G54.1+0.3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: general; ISM: individual objects (SNR G54.1+0.3); ISM: supernova remnants; pulsars: individual (PSR J1930+1852) ID PULSAR-WIND NEBULA; II-P SUPERNOVAE; REMNANT G54.1+0.3; CRAB-NEBULA; EARLY UNIVERSE; STAR-FORMATION; HERSCHEL; 1987A; CASSIOPEIA; EVOLUTION AB While theoretical models of dust condensation predict that most refractory elements produced in core-collapse supernovae (SNe) efficiently condense into dust, a large quantity of dust has so far only been observed in SN 1987A. We present an analysis of observations from the Spitzer Space Telescope, Herschel Space Observatory, Stratospheric Observatory for Infrared Astronomy, and AKARI of the infrared shell surrounding the pulsar wind nebula in the supernova remnant G54.1+0.3. We attribute a distinctive spectral feature at 21 mu m to a magnesium silicate grain species that has been invoked in modeling the ejecta-condensed dust in Cas A, which exhibits the same spectral signature. If this species is responsible for producing the observed spectral feature and accounts for a significant fraction of the observed infrared continuum, we find that it would be the dominant constituent of the dust in G54.1+0.3, with possible secondary contributions from other compositions, such as carbon, silicate, or alumina grains. The total mass of SN-formed dust required by this model is at least 0.3M(circle dot). We discuss how these results may be affected by varying dust grain properties and self-consistent grain heating models. The spatial distribution of the dust mass and temperature in G54.1+0.3 confirms the scenario in which the SN-formed dust has not yet been processed by the SN reverse shock and is being heated by stars belonging to a cluster in which the SN progenitor exploded. The dust mass and composition suggest a progenitor mass of 16-27M(circle dot) and imply a high dust condensation efficiency, similar to that found for Cas A and SN. 1987A. The study provides another example of significant dust formation in a Type IIP SN explosion and sheds light on the properties of pristine SN-condensed dust. C1 [Temim, Tea] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Dwek, Eli; Arendt, Richard G.] NASA Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. [Arendt, Richard G.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Borkowski, Kazimierz J.; Reynolds, Stephen P.] North Carolina State Univ, Raleigh, NC 27695 USA. [Slane, Patrick; Raymond, John C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Gelfand, Joseph D.] New York Univ, Abu Dhabi, U Arab Emirates. RP Temim, T (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. OI Gelfand, Joseph/0000-0003-4679-1058; Arendt, Richard/0000-0001-8403-8548; Temim, Tea/0000-0001-7380-3144 FU NASA [12-ADAP12-0145]; NASA through award SOF [04-0167] FX This work is based in part on observations made with Herschel. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This research includes observations with AKARI, a JAXA project with the participation of ESA. Based (in part) on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). SOFIA is jointly operated by the Universities Space Research Association, Inc. (USRA), under NASA contract NAS297001, and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901 to the University of Stuttgart. E.D. acknowledges the support of NASA 12-ADAP12-0145 for this project. We acknowledge financial support for this work that was provided by NASA through award SOF # 04-0167 issued by USRA. We would also like to thank the anonymous referee for providing useful feedback on the manuscript. NR 54 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2017 VL 836 IS 1 AR 129 DI 10.3847/1538-4357/836/1/129 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EP3TL UT WOS:000397304500081 ER PT J AU Wakita, S Nozawa, T Hasegawa, Y AF Wakita, Shigeru Nozawa, Takaya Hasegawa, Yasuhiro TI Diffusion of Oxygen Isotopes in Thermally Evolving Planetesimals and Size Ranges of Presolar Silicate Grains SO ASTROPHYSICAL JOURNAL LA English DT Article DE meteorites; meteors; meteoroids; planets and satellites: formation ID EXTINCTION CURVES; DUST GRAINS; CARBONACEOUS CHONDRITES; PRIMITIVE CHONDRITES; METAMORPHIC HISTORY; INTERPLANETARY DUST; INTERSTELLAR-MEDIUM; PETROLOGIC TYPE; ABUNDANCES; EVOLUTION AB Presolar grains are small particles found in meteorites through their isotopic compositions, which are considerably different from those of materials in the solar system. If some isotopes in presolar grains diffused out beyond their grain sizes when they were embedded in parent bodies of meteorites, their isotopic compositions could be washed out, and hence the grains could no longer be identified as presolar grains. We explore this possibility for the first time by self-consistently simulating the thermal evolution of planetesimals and the diffusion length of O-18 in presolar silicate grains. Our results show that presolar silicate grains smaller than similar to 0.03 mu m cannot keep their original isotopic compositions even if the host planetesimals experienced a maximum temperature as low as 600 degrees C. Since this temperature corresponds to that experienced by petrologic type 3 chondrites, isotopic diffusion can constrain the size of presolar silicate grains discovered in such chondrites to be larger than similar to 0.03 mu m. We also find that the diffusion length of 18O reaches similar to 0.3- 2 mu m in planetesimals that were heated up to 700- 800 degrees C. This indicates that, if the original size of presolar grains spans a range from similar to 0.001 mu m to similar to 0.3 mu m like that in the interstellar medium, then the isotopic records of the presolar grains may be almost completely lost in such highly thermalized parent bodies. We propose that isotopic diffusion could be a key process to control the size distribution and abundance of presolar grains in some types of chondrites. C1 [Wakita, Shigeru] Natl Astron Observ Japan, Ctr Computat Astrophys, Tokyo 1818588, Japan. [Nozawa, Takaya] Natl Astron Observ Japan, Div Theoret Astron, Mitaka, Tokyo 1818588, Japan. [Hasegawa, Yasuhiro] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wakita, S (reprint author), Natl Astron Observ Japan, Ctr Computat Astrophys, Tokyo 1818588, Japan. EM shigeru@cfca.jp FU JSPS [26400223]; JPL/Caltech FX We thank an anonymous referee for helpful comments and suggestions. Numerical computations were carried out on the PC cluster at Center for Computational Astrophysics, National Astronomical Observatory of Japan.S.W. thanks Hiroyuki R. Takahashi for discussions about numerical simulations. T. N. has been supported in part by a JSPS Grant-in-Aid for Scientific Research (26400223). Part of this research was carried out at JPL/ Caltech under a contract with NASA. Y. H. is supported by JPL/Caltech. NR 44 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 FEB 10 PY 2017 VL 836 IS 1 AR 106 DI 10.3847/1538-4357/aa5b8c PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EP3TL UT WOS:000397304500058 ER PT J AU Aschwanden, MJ Caspi, A Cohen, CMS Holman, G Jing, J Kretzschmar, M Kontar, EP McTiernan, JM Mewaldt, RA O'Flannagain, A Richardson, IG Ryan, D Warren, HP Xu, Y AF Aschwanden, Markus J. Caspi, Amir Cohen, Christina M. S. Holman, Gordon Jing, Ju Kretzschmar, Matthieu Kontar, Eduard P. McTiernan, James M. Mewaldt, Richard A. O'Flannagain, Aidan Richardson, Ian G. Ryan, Daniel Warren, Harry P. Xu, Yan TI Global Energetics of Solar Flares. V. Energy Closure in Flares and Coronal Mass Ejections SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: particle emission; Sun: UV radiation; Sun: X-rays; gamma rays ID X-RAY OBSERVATIONS; WHITE-LIGHT FLARES; PARTICLE-ACCELERATION; EMISSION MEASURES; NONTHERMAL ENERGIES; MAGNETIC ENERGIES; PEAK INTENSITIES; THERMAL ENERGIES; ATOMIC DATABASE; ACTIVE REGIONS AB In this study we synthesize the results of four previous studies on the global energetics of solar flares and associated coronal mass ejections (CMEs), which include magnetic, thermal, nonthermal, and CME energies in 399 solar M-and X-class flare events observed during the first 3.5 yr of the Solar Dynamics Observatory (SDO) mission. Our findings are as follows. (1) The sum of the mean nonthermal energy of flare-accelerated particles (E-nt), the energy of direct heating (E-dir), and the energy in CMEs (E-CME), which are the primary energy dissipation processes in a flare, is found to have a ratio of (E-nt + E-dir + ECME)/E-mag = 0.87 +/- 0.18, compared with the dissipated magnetic free energy E-mag, which confirms energy closure within the measurement uncertainties and corroborates the magnetic origin of flares and CMEs. (2) The energy partition of the dissipated magnetic free energy is: 0.51 +/- 0.17 in nonthermal energy of >= 6 keV electrons, 0.17 +/- 0.17 in nonthermal >= 1 MeV ions, 0.07 +/- 0.14 in CMEs, and 0.07 +/- 0.17 in direct heating. (3) The thermal energy is almost always less than the nonthermal energy, which is consistent with the thick-target model. (4) The bolometric luminosity in white-light flares is comparable to the thermal energy in soft X-rays (SXR). (5) Solar energetic particle events carry a fraction approximate to 0.03 of the CME energy, which is consistent with CME-driven shock acceleration. (6) The warm-target model predicts a lower limit of the low-energy cutoff at e(c) approximate to 6 keV, based on the mean peak temperature of the differential emission measure of T-e = 8.6MK during flares. This work represents the first statistical study that establishes energy closure in solar flare/CME events. C1 [Aschwanden, Markus J.] Lockheed Martin, Solar & Astrophys Lab, Org A021S,Bldg 252,3251 Hanover St, Palo Alto, CA 94304 USA. [Caspi, Amir] Southwest Res Inst, Planetary Sci Directorate, Boulder, CO 80302 USA. [Cohen, Christina M. S.; Mewaldt, Richard A.] CALTECH, Mail Code 290-17, Pasadena, CA 91125 USA. [Holman, Gordon] NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA. [Jing, Ju; Xu, Yan] Ctr Solar Terr Res, New Jersey Inst Technol, Space Weather Res Lab, 323 Martin Luther King Blvd, Newark, NJ 07102 USA. [Kretzschmar, Matthieu] CNRS, UMR 6115, LPC2E, 3a Ave Rech Sci, F-45071 Orleans, France. [Kretzschmar, Matthieu] Univ Orleans, 3a Ave Rech Sci, F-45071 Orleans, France. [Kontar, Eduard P.] Univ Glasgow, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. [McTiernan, James M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [O'Flannagain, Aidan] Sch Phys, Trinity Coll Dublin, Astrophys Res Grp, Dublin 2, Ireland. [Richardson, Ian G.] NASA, Goddard Space Flight Ctr, GPHI, Code 672, Greenbelt, MD 20770 USA. [Richardson, Ian G.] Univ Maryland, NASA, Goddard Space Flight Ctr, Dept Astron, Code 672, Greenbelt, MD 20770 USA. [Ryan, Daniel] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20770 USA. [Warren, Harry P.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. RP Aschwanden, MJ (reprint author), Lockheed Martin, Solar & Astrophys Lab, Org A021S,Bldg 252,3251 Hanover St, Palo Alto, CA 94304 USA. EM aschwanden@lmsal.com; amir.caspi@swri.org; gordon.d.holman@nasa.gov; ju.jing@njit.edu; matthieu.kretzschmar@cnrs-orleans.fr; eduard.kontar@astro.gla.ac.uk; jimm@ssl.berkeley.edu; rmewaldt@srl.caltech.edu; aidanoflann@gmail.com; ian.g.richardson@nasa.gov; ryand5@tcd.ie; harry.warren@nrl.navy.mil; yan.xu@njit.edu OI Kontar, Eduard/0000-0002-8078-0902; Aschwanden, markus/0000-0003-0260-2673; Caspi, Amir/0000-0001-8702-8273 FU NASA of the project Global Energetics of Solar Flares and CMEs [NNX16AF92G]; NASA of the SDO/AIA instrument [NNG04EA00C]; NASA [NNX15AK26G, NNX14AH54G, NAS5-90833, NNX13A66G, 00008864NNX15AG09G, NNX15AG09G]; NASA PostDoc program through the Universities Space Research Association (USRA); Royal Observatory of Belgium (ROB) FX We acknowledge useful comments from an anonymous referee and discussions with Gordon Emslie, Nat Gopalswamy, Ryan Milligan, Nariaki Nitta, Albert Shih, Manuela Temmer, Barbara Thompson, Astrid Veronig, Angelos Vourlidas, Alexander Warmuth, and Jie Zhang. Contributors to the analysis of SEP events are Richard Mewaldt, Christina Cohen, David Lario, Glenn Mason, Ian Richardson, and Mihir Desai. This work was partially supported by NASA contract NNX16AF92G of the project Global Energetics of Solar Flares and CMEs, and by NASA contract NNG04EA00C of the SDO/AIA instrument. Amir Caspi and Jim McTiernan were supported by NASA Grants NNX15AK26G and NNX14AH54G, and by NASA Contract NAS5-90833. Christina Cohen and Richard Mewaldt were supported by NASA under grants NNX13A66G and subcontract 00008864NNX15AG09G of grant NNX15AG09G. Daniel Ryan was supported by the NASA PostDoc program through the Universities Space Research Association (USRA) and the Royal Observatory of Belgium (ROB). NR 70 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 FEB 10 PY 2017 VL 836 IS 1 AR 17 DI 10.3847/1538-4357/836/1/17 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN7BL UT WOS:000396157000001 ER PT J AU Cody, AM Hillenbrand, LA David, TJ Carpenter, JM Everett, ME Howell, SB AF Cody, Ann Marie Hillenbrand, Lynne A. David, Trevor J. Carpenter, John M. Everett, Mark E. Howell, Steve B. TI A Continuum of Accretion Burst Behavior in Young Stars Observed by K2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion; accretion disks; protoplanetary disks; stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be; techniques: photometric ID T-TAURI STARS; SCORPIUS OB ASSOCIATION; MAIN-SEQUENCE STARS; LOW-MASS STARS; X-RAY SOURCES; RHO-OPHIUCHI CLOUD; H-ALPHA-EMISSION; ANGULAR RESOLUTION MEASUREMENTS; MIDINFRARED MOLECULAR-EMISSION; MULTIPLE PROTOSTELLAR SYSTEMS AB We present 29 likely members of the young rho Oph or Upper Sco regions of recent star formation that exhibit "accretion burst" type light curves in K2 time series photometry. The bursters were identified by visual examination of their similar to 80-daylight curves, though all satisfy the M < -0.25 flux asymmetry criterion for burst behavior defined by Cody et al. The burst sources represent approximate to 9% of cluster members with strong infrared excess indicative of circumstellar material. Higher amplitude burster behavior is correlated with larger inner disk infrared excesses, as inferred from WISE W1 - W2 color. The burst sources are also outliers in their large Ha emission equivalent widths. No distinction between bursters and non-bursters is seen in stellar properties such as multiplicity or spectral type. The frequency of bursters is similar between the younger, more compact. Oph region, and the older, more dispersed Upper Sco region. The bursts exhibit a range of shapes, amplitudes (similar to 10%-700%), durations (similar to 1-10 days), repeat timescales (similar to 3-80 days), and duty cycles (similar to 10%-100%). Our results provide important input to models of magnetospheric accretion, in particular, by elucidating the properties of accretion-related variability in the low state between major longer duration events such as EX Lup and FU Ori type accretion outbursts. We demonstrate the broad continuum of accretion burst behavior in young stars-extending the phenomenon to lower amplitudes and shorter timescales than traditionally considered in the theory of pre-main sequence accretion history. C1 [Cody, Ann Marie; Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hillenbrand, Lynne A.; David, Trevor J.; Carpenter, John M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Everett, Mark E.] Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA. [Carpenter, John M.] Joint ALMA Observ, Av Alonso de Cordova 3107, Santiago, Chile. RP Cody, AM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. OI David, Trevor/0000-0001-6534-6246 FU NASA/NPP fellowship; W.M. Keck Foundation; Gemini Observatory [GS-2016A-Q64] FX The work of AMC was supported by a NASA/NPP fellowship. We thank the referee for useful feedback that improved this paper. We acknowledge Luisa Rebull for calling our attention to one of the burst type objects that we had overlooked in our initial examination. Thanks also to Nic Scott for assistance with DSSI observations on the Gemini South telescope.; This paper includes data collected by the K2 mission. Funding for the K2 mission is provided by the NASA Science Mission directorate. The spectroscopic data were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. These results are also based on observations obtained as part of the program GS-2016A-Q64 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). NR 167 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 FEB 10 PY 2017 VL 836 IS 1 AR 41 DI 10.3847/1538-4357/836/1/41 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN0ZT UT WOS:000395740700014 ER PT J AU Gonzalez-Alfonso, E Fischer, J Spoon, HWW Stewart, KP Ashby, MLN Veilleux, S Smith, HA Sturm, E Farrah, D Falstad, N Melendez, M Gracia-Carpio, J Janssen, AW Lebouteiller, V AF Gonzalez-Alfonso, E. Fischer, J. Spoon, H. W. W. Stewart, K. P. Ashby, M. L. N. Veilleux, S. Smith, H. A. Sturm, E. Farrah, D. Falstad, N. Melendez, M. Gracia-Carpio, J. Janssen, A. W. Lebouteiller, V. TI Molecular Outflows in Local ULIRGs: Energetics from Multitransition OH Analysis SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies; ISM-infrared; glaxies-ISM; jets and outflows-ine; formation-ine; profiles-radiative transfer ID ULTRALUMINOUS INFRARED GALAXIES; BLACK-HOLE MASS; ACTIVE GALACTIC NUCLEI; M-BH-SIGMA; EXTREME L-FIR/M-H2 RATIOS; COMPACT OBSCURED NUCLEUS; STAR-FORMATION; MRK 231; HERSCHEL-PACS; AGN FEEDBACK AB We report on the energetics of molecular outflows in 14 local ultraluminous infrared galaxies (ULIRGs) that show unambiguous outflow signatures (P Cygni profiles or high-velocity absorption wings) in the far-infrared lines of OH measured with the Herschel/PACS spectrometer. All sample galaxies are gas-rich mergers at various stages of the merging process. Detection of both ground-state (at 119 and 79 mu m) and one or more radiatively excited (at 65 and 84 mu m) lines allows us to model the nuclear gas (. 300 pc) and the more extended components using spherically symmetric radiative transfer models. Reliable models and the corresponding energetics are found in 12 of the 14 sources. The highest molecular outflow velocities are found in buried sources, in which slower but massive expansion of the nuclear gas is also observed. With the exception of a few outliers, the outflows have momentum fluxes of (2-5) x L-IR/c and mechanical luminosities of (0.1-0.3)% of L-IR. The moderate momentum boosts in these sources (. 3) suggest that the outflows are mostly momentum driven by the combined effects of active galactic nuclei (AGNs) and nuclear starbursts, as a result of radiation pressure, winds, and supernova remnants. In some sources ( similar to 20%), however, powerful (10(10.5- 11) L circle dot) AGN feedback and (partially) energy-conserving phases are required, with momentum boosts in the range of 3-20. These outflows appear to be stochastic, strong AGN feedback events that occur throughout the merging process. In a few sources, the outflow activity in the innermost regions has subsided in the past similar to 1 Myr. While OH traces the molecular outflows at subkiloparsec scales, comparison of the masses traced by OH with those previously inferred from tracers of more extended outflowing gas suggests that most mass is loaded (with loading factors of M/SFR = 1-10) from the central galactic cores (a few. x. 100 pc), qualitatively consistent with an ongoing inside-out quenching of star formation. Outflow depletion timescales are <10(8) yr, shorter than the gas consumption timescales by factors of 1.1-15, and are anticorrelated with the AGN luminosity. C1 [Gonzalez-Alfonso, E.] Univ Alcala De Henares, Dept Fis & Matemat, Campus Univ, E-28871 Madrid, Spain. [Gonzalez-Alfonso, E.; Ashby, M. L. N.; Smith, H. A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Fischer, J.; Stewart, K. P.] Remote Sensing Div, Naval Res Lab, 4555 Overlook Ave SW, Washington, DC 20375 USA. [Spoon, H. W. W.] Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA. [Veilleux, S.; Melendez, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Veilleux, S.; Melendez, M.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Sturm, E.; Gracia-Carpio, J.; Janssen, A. W.] Max Planck Inst Extraterr Phys MPE, Giessenbachstr 1, D-85748 Garching, Germany. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Falstad, N.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, Onsala, Sweden. [Melendez, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Melendez, M.] KBRwyle Sci Technol & Engn Grp, 1290 Hercules Ave, Houston, TX 77058 USA. [Lebouteiller, V.] CEA Saclay, Lab AIM, F-91191 Gif Sur Yvette, France. RP Gonzalez-Alfonso, E (reprint author), Univ Alcala De Henares, Dept Fis & Matemat, Campus Univ, E-28871 Madrid, Spain.; Gonzalez-Alfonso, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Gonzalez-Alfonso, Eduardo/0000-0001-5285-8517; Veilleux, Sylvain/0000-0002-3158-6820 NR 156 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 FEB 10 PY 2017 VL 836 IS 1 AR 11 DI 10.3847/1538-4357/836/1/11 PG 41 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EP3RF UT WOS:000397298700010 ER PT J AU Harper, GM DeWitt, C Richter, MJ Greathouse, TK Ryde, N Guinan, EF O'Gorman, E Vacca, WD AF Harper, G. M. DeWitt, C. Richter, M. J. Greathouse, T. K. Ryde, N. Guinan, E. F. O'Gorman, E. Vacca, W. D. TI SOFIA-EXES Mid-IR Observations of [Fe II] Emission from the Extended Atmosphere of Betelgeuse SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; line: formation; stars: individual ( alpha Ori alpha Sco); stars: late; type-stars: mass loss ID LATE-TYPE STARS; SPACE-TELESCOPE SPECTRA; WATER-VAPOR ABSORPTION; ALPHA-ORIONIS; CIRCUMSTELLAR ENVELOPE; EVOLVED STARS; RADIAL-VELOCITY; ALFVEN WAVES; TRANSITION-PROBABILITIES; MODEL ATMOSPHERES AB We present a NASA-DLR SOFIA-Echelon Cross Echelle Spectrograph ( EXES) and NASA Infrared Telescope Facility-Texas Echelon Cross Echelle Spectrograph ( TEXES) mid-IR R 50,000 spectral study of forbidden Fe II transitions in the early-type M supergiants, Betelgeuse (alpha Ori: M2 Iab) and Antares (alpha Sco: M1 Iab vertical bar B3 V). With EXES, we spectrally resolve the ground term [ Fe II] 25.99 mu m (a D-6(J)= 7/2-9/2: E-up = 540 K) emission from Betelgeuse. We find a small centroid blueshift of 1.9 (+)-0.4 km s-1 that is a significant fraction (20%) of the current epoch wind speed, with a FWHM of 14.3 (+)-0.1 km s(-1). The TEXES observations of [ Fe II] 17.94 mu m. (a F-4(J)-7/2-9/2: E-up = 3400 K) show a broader FWHM of 19.1 (+)-0.2 km s(-1), consistent with previous observations, and a small redshift of 1.6 (+)-0.6 km s(-1) with respect to the adopted stellar center-ofmass velocity of V-CoM= 20.9 (+)-0.3 km s(-1). To produce [ Fe II] 25.99 mu m. blueshifts of 20% wind speed requires that the emission arises closer to the star than existing thermal models for alpha Ori's circumstellar envelope predict. This implies a more rapid wind cooling to below 500 K within 10R(*) (theta(*) = 44 mas, dist = 200 pc) of the star, where the wind has also reached a significant fraction of the maximum wind speed. The line width is consistent with the turbulence in the outflow being close to the hydrogen sound speed. EXES observations of [ Fe II] 22.90 mu m. (a (4)DJ-5/2-7/2: E-up = 11,700 K) reveal no emission from either star. These findings confirm the dominance of cool plasma in the mixed region where hot chromospheric plasma emits copiously in the UV, and they also constrain the wind heating produced by the poorly understood mechanisms that drive stellar outflows from these low variability and weak-dust signature stars. C1 [Harper, G. M.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [DeWitt, C.; Richter, M. J.] Univ Calif Davis, Davis, CA 95616 USA. [Greathouse, T. K.] Southwest Res Inst, San Antonio, TX 78238 USA. [Ryde, N.] Lund Univ, Lund, Sweden. [Guinan, E. F.] Villanova Univ, Villanova, PA 19085 USA. [O'Gorman, E.] Dublin Inst Adv Studies, Dublin 2, Ireland. [Vacca, W. D.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. RP Harper, GM (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. EM graham.harper@colorado.edu OI Harper, Graham/0000-0002-7042-4541 FU Universities Space Research Association, Inc. (USRA), under NASA [NAS2-97001]; Deutsches SOFIA Institut (DSI) under DLR [50 OK 0901]; NASA [0415.12.0827B]; NADA ADP [NNG04GD33G] FX This work was based on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). SOFIA is jointly operated by the Universities Space Research Association, Inc. (USRA), under NASA contract NAS2-97001, and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901 to the University of Stuttgart. Financial support for this work was provided by NASA through award no. 0415.12.0827B, issued by USRA. We thank the referee for suggestions that have improved the value and clarity of this work. This research would not have been possible without NADA ADP grant NNG04GD33G (GMH). This research has made use of NASA's Astrophysics Data System Bibliographic Services. NR 82 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 FEB 10 PY 2017 VL 836 IS 1 AR 22 DI 10.3847/1538-4357/836/1/22 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EP3RI UT WOS:000397299000005 ER PT J AU Kowalski, AF Allred, JC Daw, A Cauzzi, G Carlsson, M AF Kowalski, Adam F. Allred, Joel C. Daw, Adrian Cauzzi, Gianna Carlsson, Mats TI The Atmospheric Response to High Nonthermal Electron Beam Fluxes in Solar Flares. I. Modeling the Brightest NUV Footpoints in the X1 Solar Flare of 2014 March 29 SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: atmosphere; Sun: flares; radiation: dynamics; radiative transfer ID WHITE-LIGHT FLARES; REGION-IMAGING-SPECTROGRAPH; MG II H; RADIATIVE HYDRODYNAMIC MODELS; THICK-TARGET; MULTIWAVELENGTH OBSERVATIONS; OPTICAL-SPECTRA; K LINES; CHROMOSPHERIC CONDENSATIONS; TRANSITION-PROBABILITIES AB The 2014 March 29 X1 solar flare (SOL20140329T17:48) produced bright continuum emission in the far-and near-ultraviolet (NUV) and highly asymmetric chromospheric emission lines, providing long- sought constraints on the heating mechanisms of the lower atmosphere in solar flares. We analyze the continuum and emission line data from the Interface Region Imaging Spectrograph (IRIS) of the brightest flaring magnetic footpoints in this flare. We compare the NUV spectra of the brightest pixels to new radiative- hydrodynamic predictions calculated with the RADYN code using constraints on a nonthermal electron beam inferred from the collisional thick-target modeling of hard X-ray data from Reuven Ramaty High Energy Solar Spectroscopic Imager. We show that the atmospheric response to a high beam flux density satisfactorily achieves the observed continuum brightness in the NUV. The NUV continuum emission in this flare is consistent with hydrogen (Balmer) recombination radiation that originates from low optical depth in a dense chromospheric condensation and from the stationary beam-heated layers just below the condensation. A model producing two flaring regions (a condensation and stationary layers) in the lower atmosphere is also consistent with the asymmetric Fe II chromospheric emission line profiles observed in the impulsive phase. C1 [Kowalski, Adam F.] Univ Colorado Boulder, Dept Astrophys & Planetary Sci, 2000 Colorado Ave, Boulder, CO 80305 USA. [Kowalski, Adam F.] Univ Colorado Boulder, Natl Solar Observ, 3665 Discovery Dr, Boulder, CO 80303 USA. [Kowalski, Adam F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Kowalski, Adam F.; Allred, Joel C.; Daw, Adrian] NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA. [Cauzzi, Gianna] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Carlsson, Mats] Univ Oslo, Inst Theoret Astrophys, POB 1029, NO-0315 Oslo, Norway. RP Kowalski, AF (reprint author), Univ Colorado Boulder, Dept Astrophys & Planetary Sci, 2000 Colorado Ave, Boulder, CO 80305 USA. EM Adam.Kowalski@lasp.colorado.edu OI Carlsson, Mats/0000-0001-9218-3139 NR 134 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 FEB 10 PY 2017 VL 836 IS 1 DI 10.3847/1538-4357/836/1/12 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EP3RF UT WOS:000397298700011 ER PT J AU Sutton, AD Swartz, DA Roberts, TP Middleton, MJ Soria, R Done, C AF Sutton, Andrew D. Swartz, Douglas A. Roberts, Timothy P. Middleton, Matthew J. Soria, Roberto Done, Chris TI Crossing the Eddington Limit: Examining Disk Spectra at High Accretion Rates SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; X-rays binaries ID X-RAY SOURCE; BLACK-HOLE SPIN; XMM-NEWTON OBSERVATIONS; LARGE-MAGELLANIC-CLOUD; HOLMBERG-IX X-1; GX 339-4; LMC X-3; ULTRALUMINOUS STATE; ANGULAR-MOMENTUM; LOW/HARD STATE AB The faintest ultraluminous X-ray sources (ULXs), those with 0.3-10 keV luminosities 1 < L-x/10(39) < 3 erg s(-1), tend to have X-ray spectra that are disk-like but broader than expected for thin accretion disks. These "broadened disk ( BD)" spectra are thought to indicate near- or mildly super-Eddington accretion onto stellar remnant black holes. Here we report that a sample of bright thermal-dominant black hole binaries, which have Eddington ratios constrained to moderate values, also show BD spectra in the 0.3-10 keV band at an order of magnitude lower luminosities. This broadening would be missed in studies that only look above similar to 2 keV. While this may suggest that BD ULXs could be powered by accretion onto massive stellar remnant black holes with close to maximal spin, we argue in favor of a scenario where they are at close to the Eddington luminosity, such that radiation pressure would be expected to result in geometrically slim, advective accretion disks. However, this implies that an additional physical mechanism is required to produce the observed broad spectra at low Eddington ratios. C1 [Sutton, Andrew D.; Swartz, Douglas A.] NASA, Astrophys Off, Marshall Space Flight Ctr, ZP12, Huntsville, AL 35812 USA. [Roberts, Timothy P.; Done, Chris] Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England. [Middleton, Matthew J.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Soria, Roberto] Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia. [Soria, Roberto] Univ Sydney, Sydney Inst Astron, Sch Phys A28, Sydney, NSW 2006, Australia. RP Sutton, AD (reprint author), NASA, Astrophys Off, Marshall Space Flight Ctr, ZP12, Huntsville, AL 35812 USA. EM andrew.d.sutton@nasa.gov OI Roberts, Timothy/0000-0001-8252-6337 FU NASA Postdoctoral Program appointment at Marshall Space Flight Center; STFC [ST/L00075X/1]; ESA; NASA FX The authors thank the anonymous referee for useful comments. A. D. S. acknowledges funding through a NASA Postdoctoral Program appointment at Marshall Space Flight Center, administered by Universities Space Research Association on behalf of NASA. T. P. R. acknowledges funding from STFC as part of the consolidated grant ST/L00075X/1.; All data used in this paper are publicly available in NASA's High Energy Astrophysics Archive Research Center (HEASARC) archive, which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. This paper is mainly based on observations obtained with Swift and XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. It also makes use of RXTE ASM light curves, provided by the ASM/RXTE teams at MIT and at the RXTE SOF and GOF at NASA's GSFC. NR 98 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 FEB 10 PY 2017 VL 836 IS 1 AR 48 DI 10.3847/1538-4357/836/1/48 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN0ZT UT WOS:000395740700021 ER PT J AU Zoghbi, A Matt, G Miller, JM Lohfink, AM Walton, DJ Ballantyne, DR Garcia, JA Stern, D Koss, MJ Farrah, D Harrison, FA Boggs, SE Christensen, FE Craig, W Hailey, CJ Zhang, WW AF Zoghbi, Abderahmen Matt, G. Miller, J. M. Lohfink, A. M. Walton, D. J. Ballantyne, D. R. Garcia, J. A. Stern, D. Koss, M. J. Farrah, D. Harrison, F. A. Boggs, S. E. Christensen, F. E. Craig, W. Hailey, C. J. Zhang, W. W. TI A Long Look at MCG-5-23-16 with NuSTAR. I. Relativistic Reflection and Coronal Properties SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: active; galaxies: individual (MCG-5-23-16); galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; X-RAY-SPECTRUM; HIGH-ENERGY CUTOFF; XMM-NEWTON; GAMMA-RAY; SEYFERT-GALAXIES; BLACK-HOLE; THERMAL PLASMAS; NGC 4151; MRK 335 AB MCG-5-23-16 was targeted in early 2015 with a half mega-second. observing campaign using NuSTAR. Here we present the spectral analysis of these data sets along with an earlier observation and study the relativistic reflection and the primary coronal source. The data show strong reflection features in the form of both narrow and broad iron lines plus a Compton reflection hump. A cutoff energy is significantly detected in all exposures. The shape of the reflection spectrum does not change in the two years spanned by the observations, suggesting a stable geometry. A strong positive correlation is found between the cutoff energy and both the hard X-ray flux and spectral index. The measurements imply that the coronal plasma is not at the runaway electron-positron pair limit, and instead contains mostly electrons. The observed variability in the coronal properties is driven by a variable optical depth. A constant heating-to-cooling ratio is measured, implying that there is a feedback mechanism in which a significant fraction of the photons cooling the corona are due to reprocessed hard X-rays. C1 [Zoghbi, Abderahmen; Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Matt, G.] Univ Roma Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy. [Lohfink, A. M.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 OHA, England. [Walton, D. J.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Garcia, J. A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Garcia, J. A.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Koss, M. J.] ETH, Dept Phys, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Boggs, S. E.; Craig, W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. RP Zoghbi, A (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. EM abzoghbi@umich.edu OI Koss, Michael/0000-0002-7998-9581; Garcia, Javier/0000-0003-3828-2448; Ballantyne, David/0000-0001-8128-6976 FU NASA [NNX14AF89G]; National Aeronautics and Space Administration FX We thank the referee, A. Zdziarski, for the useful comments and suggestions that helped with the interpretation of the data. This work has been partly supported by NASA grant NNX14AF89G. This work 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). NR 76 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 FEB 10 PY 2017 VL 836 IS 1 AR 2 DI 10.3847/1538-4357/aa582c PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EP3RF UT WOS:000397298700001 ER PT J AU Airapetian, VS Glocer, A Khazanov, GV Loyd, ROP France, K Sojka, J Danchi, WC Liemohn, MW AF Airapetian, Vladimir S. Glocer, Alex Khazanov, George V. Loyd, R. O. P. France, Kevin Sojka, Jan Danchi, William C. Liemohn, Michael W. TI How Hospitable Are Space Weather Affected Habitable Zones? The Role of Ion Escape SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE hydrodynamics; planets and satellites: atmospheres; planets and satellites: magnetic fields; radiation mechanisms: general; stars: activity; stars: late-type ID POLAR WIND; X-RAY; EVOLUTION; PLANETS; STARS; THERMOSPHERE; IONOSPHERE; EXOPLANETS; ROTATION; OUTFLOW AB Atmospheres of exoplanets in the habitable zones around active young G-K-M stars are subject to extreme X- ray and EUV (XUV) fluxes from their host stars that can initiate atmospheric erosion. Atmospheric loss affects exoplanetary habitability in terms of surface water inventory, atmospheric pressure, the efficiency of greenhouse warming, and the dosage of the UV surface irradiation. Thermal escape models suggest that exoplanetary atmospheres around active K-M stars should undergo massive hydrogen escape, while heavier species including oxygen will accumulate forming an oxidizing atmosphere. Here, we show that non-thermal oxygen ion escape could be as important as thermal, hydrodynamic H escape in removing the constituents of water from exoplanetary atmospheres under supersolar XUV irradiation. Our models suggest that the atmospheres of a significant fraction of Earth-like exoplanets around M dwarfs and active K stars exposed to high XUV fluxes will incur a significant atmospheric loss rate of oxygen and nitrogen, which will make them uninhabitable within a few tens to hundreds of Myr, given a low replenishment rate from volcanism or cometary bombardment. Our non-thermal escape models have important implications for the habitability of the Proxima Centauri's terrestrial planet. C1 [Airapetian, Vladimir S.; Glocer, Alex; Khazanov, George V.; Danchi, William C.] NASA, GSFC, Greenbelt, MD 20771 USA. [Loyd, R. O. P.; France, Kevin] Univ Colorado, LASP, Boulder, CO 80309 USA. [Sojka, Jan] Utah State Univ, Logan, UT 84322 USA. [Liemohn, Michael W.] Univ Michigan, Ann Arbor, MI 48109 USA. RP Airapetian, VS (reprint author), NASA, GSFC, Greenbelt, MD 20771 USA. OI Loyd, Robert/0000-0001-5646-6668; Airapetian, Vladimir/0000-0003-4452-0588; FRANCE, KEVIN/0000-0002-1002-3674 FU internal Science Task Group funds FX This paper is dedicated to the memory of Dr. Piers Sellers, who served as a great inspiration for our ongoing interdisciplinary team project "Mission to Young Earth 2.0". This study was supported by the internal Science Task Group funds administered by NASA Goddard Space Flight Center's Sciences and Exploration Directorate. The authors also wish to thank the anonymous referee for the constructive comments and suggestions. 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 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 10 PY 2017 VL 836 IS 1 AR L3 DI 10.3847/2041-8213/836/1/L3 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN0ZM UT WOS:000395740000001 ER PT J AU Badia, A Jorba, O Voulgarakis, A Dabdub, D Garcia-Pando, CP Hilboll, A Goncalves, M Janjic, Z AF Badia, Alba Jorba, Oriol Voulgarakis, Apostolos Dabdub, Donald Perez Garcia-Pando, Carlos Hilboll, Andreas Goncalves, Maria Janjic, Zavisa TI Description and evaluation of the Multiscale Online Nonhydrostatic AtmospheRe CHemistry model (NMMB-MONARCH) version 1.0: gas-phase chemistry at global scale SO GEOSCIENTIFIC MODEL DEVELOPMENT LA English DT Article ID INTERCOMPARISON PROJECT ACCMIP; TROPOSPHERIC NITROGEN-DIOXIDE; CONVECTIVE ADJUSTMENT SCHEME; GENERAL-CIRCULATION MODEL; CHEMICAL-TRANSPORT MODEL; PEROXYACETYL NITRATE PAN; ISOPRENE EMISSIONS; COASTAL/OROGRAPHIC SITES; RADIATIVE-TRANSFER; DRY DEPOSITION AB This paper presents a comprehensive description and benchmark evaluation of the tropospheric gas-phase chemistry component of the Multiscale Online Nonhydrostatic AtmospheRe CHemistry model (NMMB-MONARCH), formerly known as NMMB/BSC-CTM, that can be run on both regional and global domains. Here, we provide an extensive evaluation of a global annual cycle simulation using a variety of background surface stations (EMEP, WDCGG and CASTNET), ozonesondes (WOUDC, CMD and SHADOZ), aircraft data (MOZAIC and several campaigns), and satellite observations (SCIAMACHY and MOPITT). We also include an extensive discussion of our results in comparison to other state-of-the-art models. We note that in this study, we omitted aerosol processes and some natural emissions (lightning and volcano emissions). The model shows a realistic oxidative capacity across the globe. The seasonal cycle for CO is fairly well represented at different locations (correlations around 0.3-0.7 in surface concentrations), although concentrations are underestimated in spring and winter in the Northern Hemisphere, and are overestimated throughout the year at 800 and 500 hPa in the Southern Hemisphere. Nitrogen species are well represented in almost all locations, particularly NO2 in Europe (root mean square error - RMSE - below 5 ppb). The modeled vertical distributions of NOx and HNO3 are in excellent agreement with the observed values and the spatial and seasonal trends of tropospheric NO2 columns correspond well to observations from SCIAMACHY, capturing the highly polluted areas and the biomass burning cycle throughout the year. Over Asia, the model underestimates NOx from March to August, probably due to an underestimation of NOx emissions in the region. Overall, the comparison of the modeled CO and NO2 with MOPITT and SCIAMACHY observations emphasizes the need for more accurate emission rates from anthropogenic and biomass burning sources (i.e., specification of temporal variability). The resulting ozone (O-3) burden (348 Tg) lies within the range of other state-of-the-art global atmospheric chemistry models. The model generally captures the spatial and seasonal trends of background surface O-3 and its vertical distribution. However, the model tends to overestimate O-3 throughout the troposphere in several stations. This may be attributed to an overestimation of CO concentration over the Southern Hemisphere leading to an excessive production of O-3 or to the lack of specific chemistry (e.g., halogen chemistry, aerosol chemistry). Overall, O-3 correlations range between 0.6 and 0.8 for daily mean values. The overall performance of the NMMB-MONARCH is comparable to that of other state-of-the-art global chemistry models. C1 [Badia, Alba; Jorba, Oriol; Perez Garcia-Pando, Carlos; Goncalves, Maria] Barcelona Supercomput Ctr, Dept Earth Sci, Barcelona, Spain. [Voulgarakis, Apostolos] Imperial Coll, Dept Phys, London, England. [Voulgarakis, Apostolos] Univ Calif Irvine, Mech & Aerosp Engn, Irvine, CA USA. [Perez Garcia-Pando, Carlos] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Perez Garcia-Pando, Carlos] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. [Hilboll, Andreas] Univ Bremen, Inst Environm Phys, Bremen, Germany. [Hilboll, Andreas] Univ Bremen, MARUM Ctr Marine Environm Sci, Bremen, Germany. [Goncalves, Maria] Univ Politecn Cataluna, Project & Construct Engn Dept, Barcelona, Spain. [Janjic, Zavisa] Natl Ctr Environm Predict, College Pk, MD USA. [Badia, Alba] Univ East Anglia, Ctr Ocean & Atmospher Sci, Sch Environm Sci, Norwich, Norfolk, England. RP Jorba, O (reprint author), Barcelona Supercomput Ctr, Dept Earth Sci, Barcelona, Spain. EM oriol.jorba@bsc.es OI Badia, Alba/0000-0003-0906-8258; Jorba, Oriol/0000-0001-5872-0244 FU INSU-CNRS (France); Meteo-France; Forschungszentrum (FZJ, Julich, Germany); ETHER (CNES); ETHER (INSU-CNRS); Spanish Ministry of Economy and Competitiveness [CGL2013-46736-R, CSD2007-0050]; Severo Ochoa Program - Spanish Government [SEV-2011-00067]; Earth System Science Research School (ESSReS), an initiative of the Helmholtz Association of German research centres (HGF) at the Alfred Wegener Institute for Polar and Marine Research; AXA Research Fund FX The authors wish to thank WOUDC, GAW, EMEP, WDCGG, CASTNET-EPA, NADP and EANET for the provision of measurement stations. The authors acknowledge for the strong support of the European Commission, Airbus, and the Airlines (Lufthansa, Austrian, Air France) who carry free of charge the MOZAIC equipment and perform the maintenance since 1994. MOZAIC is presently funded by INSU-CNRS (France), Meteo-France, and Forschungszentrum (FZJ, Julich, Germany). The MOZAIC database is supported by ETHER (CNES and INSU-CNRS). Also, thanks go to the free use of the MOPITT CO data obtained from the NASA Langley Research Center Atmospheric Science Data Center. SCIAMACHY radiances have been provided by ESA. We also thank Beatriz Monge-Sanz for providing the COPCAT coefficients. This work is funded by grants CGL2013-46736-R, Supercomputacion and e-ciencia Project (CSD2007-0050) from the Consolider-Ingenio 2010 program of the Spanish Ministry of Economy and Competitiveness. Further support was provided by the SEV-2011-00067 grant of the Severo Ochoa Program, awarded by the Spanish Government. Andreas Hilboll received funding from the Earth System Science Research School (ESSReS), an initiative of the Helmholtz Association of German research centres (HGF) at the Alfred Wegener Institute for Polar and Marine Research. Carlos Perez Garcia-Pando acknowledges long-term support from the AXA Research Fund. The authors thankfully acknowledge the computer resources at MareNostrum and the technical support provided by Barcelona Supercomputing Center (RES-AECT-2015-1-0007). Comments from two anonymous reviewers are gratefully acknowledge. NR 118 TC 2 Z9 2 U1 1 U2 1 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1991-959X EI 1991-9603 J9 GEOSCI MODEL DEV JI Geosci. Model Dev. PD FEB 10 PY 2017 VL 10 IS 2 BP 609 EP 638 DI 10.5194/gmd-10-609-2017 PG 30 WC Geosciences, Multidisciplinary SC Geology GA EM1SI UT WOS:000395096900001 ER PT J AU Smelyanskiy, VN Venturelli, D Perdomo-Ortiz, A Knysh, S Dykman, MI AF Smelyanskiy, Vadim N. Venturelli, Davide Perdomo-Ortiz, Alejandro Knysh, Sergey Dykman, Mark I. TI Quantum Annealing via Environment-Mediated Quantum Diffusion SO PHYSICAL REVIEW LETTERS LA English DT Article ID ISING-MODEL; ALGORITHM; KINETICS AB We show that quantum diffusion near a quantum critical point can provide an efficient mechanism of quantum annealing. It is based on the diffusion-mediated recombination of excitations in open systems far from thermal equilibrium. We find that, for an Ising spin chain coupled to a bosonic bath and driven by a monotonically decreasing transverse field, excitation diffusion sharply slows down below the quantum critical region. This leads to spatial correlations and effective freezing of the excitation density. Still, obtaining an approximate solution of an optimization problem via the diffusion-mediated quantum annealing can be faster than via closed-system quantum annealing or Glauber dynamics. C1 [Smelyanskiy, Vadim N.] Google, Venice, CA 90291 USA. [Venturelli, Davide; Perdomo-Ortiz, Alejandro] USRA, RIACS, Mountain View, CA 94043 USA. [Venturelli, Davide; Perdomo-Ortiz, Alejandro; Knysh, Sergey] NASA, Ames Res Ctr, Mail Stop 269-1, Moffett Field, CA 94035 USA. [Knysh, Sergey] Stinger Ghaffarian Technol Inc, 7701 Greenbelt Rd,Suite 400, Greenbelt, MD 20770 USA. [Dykman, Mark I.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP Smelyanskiy, VN (reprint author), Google, Venice, CA 90291 USA. EM smelyan@google.com; dykman@pa.msu.edu FU Office of the Director of National Intelligence (ODNI), Intelligence Advanced Research Projects Activity (IARPA) [IAA 145483]; AFRL Information Directorate [F4HBKC4162G001]; NASA [NNX12AK33A]; Sandia National Laboratory AQUARIUS project FX This work was supported in part by the Office of the Director of National Intelligence (ODNI), Intelligence Advanced Research Projects Activity (IARPA), via IAA 145483, by the AFRL Information Directorate under Grant No. F4HBKC4162G001, and by NASA (Sponsor Award No. NNX12AK33A). D. V. and A. P.-O. were also supported in part by the Sandia National Laboratory AQUARIUS project. M. I. D. is grateful to the NASA Ames Research Center for the warm hospitality and partial support during his sabbatical. NR 40 TC 0 Z9 0 U1 4 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD FEB 10 PY 2017 VL 118 IS 6 AR 066802 DI 10.1103/PhysRevLett.118.066802 PG 5 WC Physics, Multidisciplinary SC Physics GA EK2HB UT WOS:000393747300011 PM 28234537 ER PT J AU Schulze, BC Wallace, HW Flynn, JH Lefer, BL Erickson, MH Jobson, BT Dusanter, S Griffith, SM Hansen, RF Stevens, PS VanReken, T Griffin, RJ AF Schulze, Benjamin C. Wallace, Henry W. Flynn, James H. Lefer, Barry L. Erickson, Matt H. Jobson, B. Tom Dusanter, Sebastien Griffith, Stephen M. Hansen, Robert F. Stevens, Philip S. VanReken, Timothy Griffin, Robert J. TI Differences in BVOC oxidation and SOA formation above and below the forest canopy SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID SECONDARY ORGANIC AEROSOL; SOUTHEASTERN UNITED-STATES; MASTER CHEMICAL MECHANISM; HO2 RADICAL CHEMISTRY; TORCH 2003 CAMPAIGN; GAS-PHASE; ALPHA-PINENE; TROPOSPHERIC DEGRADATION; BIOGENIC HYDROCARBONS; ABSORPTION-MODEL AB Gas-phase biogenic volatile organic compounds (BVOCs) are oxidized in the troposphere to produce secondary pollutants such as ozone (O-3), organic nitrates (RONO2), and secondary organic aerosol (SOA). Two coupled zero-dimensional models have been used to investigate differences in oxidation and SOA production from isoprene and alpha-pinene, especially with respect to the nitrate radical (NO3), above and below a forest canopy in rural Michigan. In both modeled environments (above and below the canopy), NO3 mixing ratios are relatively small (<0.5 pptv); however, daytime (08:00-20:00 LT) mixing ratios below the canopy are 2 to 3 times larger than those above. As a result of this difference, NO3 contributes 12% of total daytime alpha-pinene oxidation below the canopy while only contributing 4% above. Increasing background pollutant levels to simulate a more polluted suburban or peri-urban forest environment increases the average contribution of NO3 to daytime below-canopy alpha-pinene oxidation to 32 %. Gas-phase RONO2 produced through NO3 oxidation undergoes net transport upward from the below-canopy environment during the day, and this transport contributes up to 30% of total NO3-derived RONO2 production above the canopy in the morning (similar to 07:00). Modeled SOA mass loadings above and below the canopy ultimately differ by less than 0.5 mu g m(-3), and extremely low-volatility organic compounds dominate SOA composition. Lower temperatures below the canopy cause increased partitioning of semi-volatile gas-phase products to the particle phase and up to 35% larger SOA mass loadings of these products relative to above the canopy in the model. Including transport between above-and below-canopy environments increases above-canopy NO3-derived alpha-pinene RONO2 SOA mass by as much as 45 %, suggesting that below-canopy chemical processes substantially influence above-canopy SOA mass loadings, especially with regard to monoterpene-derived RONO2. C1 [Schulze, Benjamin C.; Wallace, Henry W.; Griffin, Robert J.] Rice Univ, Dept Civil & Environm Engn, Houston, TX 77005 USA. [Flynn, James H.; Erickson, Matt H.] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA. [Lefer, Barry L.] NASA, Airborne Sci Program, Washington, DC 20546 USA. [Jobson, B. Tom; VanReken, Timothy] Washington State Univ, Lab Atmospher Res, Dept Civil & Environm Engn, Pullman, WA 99164 USA. [Dusanter, Sebastien] SAGE, Mines Douai, F-59508 Douai, France. [Dusanter, Sebastien] Univ Lille, F-59655 Villeneuve Dascq, France. [Dusanter, Sebastien; Griffith, Stephen M.] Indiana Univ, Sch Publ & Environm Affairs, Bloomington, IN 47405 USA. [Hansen, Robert F.; Stevens, Philip S.] Indiana Univ, Dept Chem, Bloomington, IN 47405 USA. [Griffith, Stephen M.] Hong Kong Univ Sci & Technol, Dept Chem, Kowloon, Hong Kong, Peoples R China. [Hansen, Robert F.] Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England. [VanReken, Timothy] Natl Sci Fdn, Washington, DC 20230 USA. RP Griffin, RJ (reprint author), Rice Univ, Dept Civil & Environm Engn, Houston, TX 77005 USA. EM rob.griffin@rice.edu FU National Science Foundation [AGS-0904214, AGS-0904167] FX We would like to acknowledge the National Science Foundation for funding this work with grant numbers AGS-0904214 and AGS-0904167. NR 117 TC 0 Z9 0 U1 0 U2 0 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 FEB 7 PY 2017 VL 17 IS 3 BP 1805 EP 1828 DI 10.5194/acp-17-1805-2017 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EM2DN UT WOS:000395126700002 ER PT J AU Khaykin, SM Godin-Beekmann, S Keckhut, P Hauchecorne, A Jumelet, J Vernier, JP Bourassa, A Degenstein, DA Rieger, LA Bingen, C Vanhellemont, F Robert, C DeLand, M Bhartia, PK AF Khaykin, Sergey M. Godin-Beekmann, Sophie Keckhut, Philippe Hauchecorne, Alain Jumelet, Julien Vernier, Jean-Paul Bourassa, Adam Degenstein, Doug A. Rieger, Landon A. Bingen, Christine Vanhellemont, Filip Robert, Charles DeLand, Matthew Bhartia, Pawan K. TI Variability and evolution of the midlatitude stratospheric aerosol budget from 22 years of ground-based lidar and satellite observations SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID ASIAN MONSOON ANTICYCLONE; GLOBAL CLIMATE-CHANGE; VOLCANIC AEROSOL; GARMISCH-PARTENKIRCHEN; GOMOS OBSERVATIONS; CIRRUS CLOUDS; LAYER; TRANSPORT; EXTINCTION; EMISSIONS AB The article presents new high-quality continuous stratospheric aerosol observations spanning 1994-2015 at the French Observatoire de Haute-Provence (OHP, 44 degrees N, 6 degrees E) obtained by two independent, regularly maintained lidar systems operating within the Network for Detection of Atmospheric Composition Change (NDACC). Lidar series are compared with global-coverage observations by Stratospheric Aerosol and Gas Experiment (SAGE II), Global Ozone Monitoring by Occultation of Stars (GOMOS), Optical Spectrograph and InfraRed Imaging System (OSIRIS), Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP), and Ozone Mapping Profiling Suite (OMPS) satellite instruments, altogether covering the time span of OHP lidar measurements. Local OHP and zonal-mean satellite series of stratospheric aerosol optical depth are in excellent agreement, allowing for accurate characterization of stratospheric aerosol evolution and variability at northern midlatitudes during the last 2 decades. The combination of local and global observations is used for a careful separation between volcanically perturbed and quiescent periods. While the volcanic signatures dominate the stratospheric aerosol record, the background aerosol abundance is found to be modulated remotely by the poleward transport of convectively cleansed air from the deep tropics and aerosol-laden air from the Asian monsoon region. The annual cycle of background aerosol at midlatitudes, featuring a minimum during late spring and a maximum during late summer, correlates with that of water vapor from the Aura Microwave Limb Sounder (MLS). Observations covering two volcanically quiescent periods over the last 2 decades provide an indication of a growth in the nonvolcanic component of stratospheric aerosol. A statistically significant factor of 2 increase in nonvolcanic aerosol since 1998, seasonally restricted to late summer and fall, is associated with the influence of the Asian monsoon and growing pollution therein. C1 [Khaykin, Sergey M.; Godin-Beekmann, Sophie; Keckhut, Philippe; Hauchecorne, Alain; Jumelet, Julien] UPMC Univ Paris 06, CNRS, UVSQ Univ Paris Saclay, LATMOS IPSL, Guyancourt, France. [Vernier, Jean-Paul] Sci Syst & Applicat Inc, Hampton, VA USA. [Vernier, Jean-Paul] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Bourassa, Adam; Degenstein, Doug A.; Rieger, Landon A.] Univ Saskatchewan, Inst Space & Atmospher Studies, Saskatoon, SK, Canada. [Bingen, Christine; Vanhellemont, Filip; Robert, Charles] Royal Belgian Inst Space Aeron, Brussels, Belgium. [DeLand, Matthew] Sci Syst & Applicat Inc, Lanham, MD USA. [Bhartia, Pawan K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Khaykin, SM (reprint author), UPMC Univ Paris 06, CNRS, UVSQ Univ Paris Saclay, LATMOS IPSL, Guyancourt, France. EM sergey.khaykin@latmos.ipsl.fr FU French Institut National des Sciences de l'Univers (INSU) of the Centre National de la Recherche Scientifique (CNRS); Centre National d'Etudes Spatiales (CNES); European Space Agency [22022/OP/I-OL]; Marie Curie Career Integration Grant within the 7th European Community Framework Programme [293560]; European Space Agency within the Aerosol_CCI project of the Climate Change Initiative; Belgian Space Science Office (BELSPO) through the Chercheur Supplementaire programme FX We thank the personnel of OHP for conducting lidar measurements. The work was done with the support of the French Institut National des Sciences de l'Univers (INSU) of the Centre National de la Recherche Scientifique (CNRS) and of the Centre National d'Etudes Spatiales (CNES). We thank Laurent Blanot (Acri ST) and Nickolay Kadygrov (IPSL) for their help with satellite data handling. OMPS LP Version 0.5 aerosol extinction coefficient data are produced by the LP processing team (https://ozoneaq.gsfc.nasa.gov/data/omps/). The AerGom project was financed by the European Space Agency (contract number 22022/OP/I-OL). Charles Robert's research was supported by a Marie Curie Career Integration Grant within the 7th European Community Framework Programme under grant agreement no. 293560, the European Space Agency within the Aerosol_CCI project of the Climate Change Initiative and the Belgian Space Science Office (BELSPO) through the Chercheur Supplementaire programme. We also thank three anonymous reviewers for useful remarks that helped to improve the article. NR 70 TC 0 Z9 0 U1 2 U2 2 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 FEB 7 PY 2017 VL 17 IS 3 BP 1829 EP 1845 DI 10.5194/acp-17-1829-2017 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EM2DN UT WOS:000395126700003 ER PT J AU Messick, C Blackburn, K Brady, P Brockill, P Cannon, K Cariou, R Caudill, S Chamberlin, SJ Creighton, JDE Everett, R Hanna, C Keppel, D Lang, RN Li, TGF Meacher, D Nielsen, A Pankow, C Privitera, S Qi, H Sachdev, S Sadeghian, L Singer, L Thomas, EG Wade, L Wade, M Weinstein, A Wiesner, K AF Messick, Cody Blackburn, Kent Brady, Patrick Brockill, Patrick Cannon, Kipp Cariou, Romain Caudill, Sarah Chamberlin, Sydney J. Creighton, Jolien D. E. Everett, Ryan Hanna, Chad Keppel, Drew Lang, Ryan N. Li, Tjonnie G. F. Meacher, Duncan Nielsen, Alex Pankow, Chris Privitera, Stephen Qi, Hong Sachdev, Surabhi Sadeghian, Laleh Singer, Leo Thomas, E. Gareth Wade, Leslie Wade, Madeline Weinstein, Alan Wiesner, Karsten TI Analysis framework for the prompt discovery of compact binary mergers in gravitational-wave data SO PHYSICAL REVIEW D LA English DT Article ID INSPIRALING BINARIES; SEARCH TEMPLATES; ADVANCED LIGO; FOLLOW-UP; VIRGO AB We describe a stream-based analysis pipeline to detect gravitational waves from the merger of binary neutron stars, binary black holes, and neutron-star-black-hole binaries within similar to 1 min of the arrival of the merger signal at Earth. Such low-latency detection is crucial for the prompt response by electromagnetic facilities in order to observe any fading electromagnetic counterparts that might be produced by mergers involving at least one neutron star. Even for systems expected not to produce counterparts, low-latency analysis of the data is useful for deciding when not to point telescopes, and as feedback to observatory operations. Analysts using this pipeline were the first to identify GW151226, the second gravitational-wave event ever detected. The pipeline also operates in an offline mode, in which it incorporates more refined information about data quality and employs acausal methods that are inapplicable to the online mode. The pipeline's offline mode was used in the detection of the first two gravitational-wave events, GW150914 and GW151226, as well as the identification of a third candidate, LVT151012. C1 [Messick, Cody; Chamberlin, Sydney J.; Everett, Ryan; Hanna, Chad; Meacher, Duncan] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Messick, Cody; Chamberlin, Sydney J.; Everett, Ryan; Hanna, Chad; Meacher, Duncan] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Blackburn, Kent; Sachdev, Surabhi; Weinstein, Alan] CALTECH, LIGO Lab, MS 100-36, Pasadena, CA 91125 USA. [Brady, Patrick; Brockill, Patrick; Caudill, Sarah; Creighton, Jolien D. E.; Lang, Ryan N.; Qi, Hong; Sadeghian, Laleh] Univ Wisconsin, Leonard E Parker Ctr Gravitat Cosmol & Astrophys, Milwaukee, WI 53201 USA. [Cannon, Kipp] Univ Toronto, Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 3H8, Canada. [Cannon, Kipp] Univ Tokyo, RESCEU, Tokyo 1130033, Japan. [Cariou, Romain] Ecole Normale Super, Dept Phys, F-94230 Cachan, France. [Hanna, Chad] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Keppel, Drew; Nielsen, Alex; Wiesner, Karsten] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. [Li, Tjonnie G. F.] Chinese Univ Hong Kong, Dept Phys, Shatin, Hong Kong, Peoples R China. [Pankow, Chris] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Pankow, Chris] Northwestern Univ, Dept Phys & Astron, 2145 Sheridan Rd, Evanston, IL 60208 USA. [Privitera, Stephen] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. [Singer, Leo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Thomas, E. Gareth] Univ Birmingham, Birmingham B15 2TT, W Midlands, England. [Wade, Leslie; Wade, Madeline] Kenyon Coll, Dept Phys, Hayes Hall, Gambier, OH 43022 USA. RP Messick, C (reprint author), Penn State Univ, Dept Phys, University Pk, PA 16802 USA.; Messick, C (reprint author), Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. EM Cody.Messick@ligo.org FU Eberly Research Funds of Penn State; National Science Foundation [PHY-0757058, PHY-0923409, PHY-1104371, PHY-1454389, PHY-1607585, PHY-1307429]; JSPS KAKENHI Grant [16H06714] FX The authors wish to thank B. Sathyaprakash, the LIGO Scientific Collaboration, and the Compact Binary Coalescence working group for many useful discussions. We gratefully acknowledge the support of the Eberly Research Funds of Penn State and the National Science Foundation through Grants No. PHY-0757058, No. PHY-0923409, No. PHY-1104371, No. PHY-1454389, No. PHY-1607585, and No. PHY-1307429. K. C. was supported in part by JSPS KAKENHI Grant No. 16H06714. This document has LIGO Document No. P1600009. NR 53 TC 0 Z9 0 U1 1 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD FEB 7 PY 2017 VL 95 IS 4 AR 042001 DI 10.1103/PhysRevD.95.042001 PG 15 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA EJ8XR UT WOS:000393511100001 ER PT J AU Taylor, SR Lentati, L Babak, S Brem, P Gair, JR Sesana, A Vecchio, A AF Taylor, S. R. Lentati, L. Babak, S. Brem, P. Gair, J. R. Sesana, A. Vecchio, A. TI All correlations must die: Assessing the significance of a stochastic gravitational-wave background in pulsar timing arrays SO PHYSICAL REVIEW D LA English DT Article ID MILLISECOND PULSARS; PRECISION; LIMITS; EFFICIENT; PACKAGE; MERGERS; TEMPO2; SIGNAL; NOISE; MODEL AB We present two methods for determining the significance of a stochastic gravitational-wave (GW) background affecting a pulsar-timing array, where detection is based on evidence for quadrupolar spatial correlations between pulsars. Rather than constructing noise simulations, we eliminate the GWB spatial correlations in the true data sets to assess detection significance with all real data features intact. In our first method, we perform random phase shifts in the signal-model basis functions. This phase shifting eliminates signal phase coherence between pulsars, while keeping the statistical properties of the pulsar timing residuals intact. We then explore a method to null correlations between pulsars by using a "scrambled" overlap-reduction function in the signal model for the array. This scrambled function is orthogonal to what we expect of a real GW background signal. We demonstrate the efficacy of these methods using Bayesian model selection on a set of simulated data sets that contain a stochastic GW signal, timing noise, undiagnosed glitches, and uncertainties in the Solar system ephemeris. Finally, we introduce an overarching formalism under which these two techniques are naturally linked. These methods are immediately applicable to all current pulsar-timing array data sets, and should become standard tools for future analyses. C1 [Taylor, S. R.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91106 USA. [Lentati, L.] Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England. [Babak, S.; Brem, P.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. [Gair, J. R.] Univ Edinburgh, Sch Math, Kings Bldg, Edinburgh EH9 3JZ, Midlothian, Scotland. [Sesana, A.; Vecchio, A.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. RP Taylor, SR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91106 USA. EM Stephen.R.Taylor@jpl.nasa.gov FU University Research Fellowship of the Royal Society; National Science Foundation [PHYS-1066293]; NSF [0923409] FX We thank the anonymous referee for many useful suggestions that improved the quality of this paper. We also thank Justin Ellis, Michele Vallisneri, Rutger van Haasteren, Joseph Lazio, Neil Cornish, Laura Sampson, Paul Demorest, G. J. Babu, as well as the entire NANOGrav and EPTA detection working groups for many useful suggestions and fruitful discussions. S. R. T. was supported by appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities and the Universities Space Research Association through a contract with NASA. A. S. is supported by a University Research Fellowship of the Royal Society. The authors acknowledge the support of colleagues in the EPTA. This work was supported in part by National Science Foundation Grant No. PHYS-1066293 and by the hospitality of the Aspen Center for Physics. A majority of the computational work was performed on the Nemo cluster at UWM supported by NSF Grant No. 0923409. The research was partially carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 49 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 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD FEB 7 PY 2017 VL 95 IS 4 AR 042002 DI 10.1103/PhysRevD.95.042002 PG 13 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA EJ8XR UT WOS:000393511100002 ER PT J AU Poinar, K Joughin, I Lilien, D Brucker, L Kehrl, L Nowicki, S AF Poinar, Kristin Joughin, Ian Lilien, David Brucker, Ludovic Kehrl, Laura Nowicki, Sophie TI Drainage of Southeast Greenland Firn Aquifer Water through Crevasses to the Bed SO FRONTIERS IN EARTH SCIENCE LA English DT Article DE firn aquifer; crevasse; englacial hydrology; meltwater runoff; meltwater retention ID SUPRAGLACIAL LAKE DRAINAGE; ICE-SHEET; SOUTHWEST GREENLAND; MELTWATER STORAGE; GLACIER; ACCELERATION; VARIABILITY; VELOCITY; BENEATH; EXTENT AB A firn aquifer in the Helheim Glacier catchment of Southeast Greenland lies directly upstream of a crevasse field. Previous measurements show that a 3.5-km long segment of the aquifer lost a large volume of water (26,000-65,000 m(2) in cross section) between spring 2012 and spring 2013, compared to annual meltwater accumulation of 6000-15,000 m(2). The water is thought to have entered the crevasses, but whether the water reached the bed or refroze within the ice sheet is unknown. We used a thermo-visco-elastic model for crevasse propagation to calculate the depths and volumes of these water-filled crevasses. We compared our model output to data from the Airborne Topographic Mapper (ATM), which reveals the near-surface geometry of specific crevasses, and WorldView images, which capture the surface expressions of crevasses across our 1.5-km study area. We found a best fit with a shear modulus between 0.2 and 1.5 GPa within our study area. We show that surface meltwater can drive crevasses to the top surface of the firn aquifer (similar to 20m depth), whereupon it receives water at rates corresponding to the water flux through the aquifer. Our model shows that crevasses receiving firn-aquifer water hydrofracture through to the bed, similar to 1000m below, in 10-40 days. Englacial refreezing of firn-aquifer water raises the average local ice temperature by similar to 4 degrees C over a ten-year period, which enhances deformational ice motion by similar to 50m year(-1), compared to the observed surface velocity of similar to 200m year(-1). The effect of the basal water on the sliding velocity remains unknown. Were the firn aquifer not present to concentrate surface meltwater into crevasses, we find that no surface melt would reach the bed; instead, it would refreeze annually in crevasses at depths < 500 m. The crevasse field downstream of the firn aquifer likely allows a large fraction of the aquifer water in our study area to reach the bed. Thus, future studies should consider the aquifer and crevasses as part of a common system. This system may uniquely affect ice-sheet dynamics by routing a large volume of water to the bed outside of the typical runoff period. C1 [Poinar, Kristin; Brucker, Ludovic; Nowicki, Sophie] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Joughin, Ian; Lilien, David; Kehrl, Laura] Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA. [Lilien, David; Kehrl, Laura] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. [Brucker, Ludovic] Univ Space Res Assoc, Goddard Earth Sci Technol & Res Studies & Invest, Columbia, MD USA. RP Poinar, K (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. EM kristin.poinar@nasa.gov NR 60 TC 0 Z9 0 U1 3 U2 3 PU FRONTIERS MEDIA SA PI LAUSANNE PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015, SWITZERLAND SN 2296-6463 J9 FRONT EARTH SCI JI Front. Earth Sci. PD FEB 7 PY 2017 VL 5 AR UNSP 5 DI 10.3389/feart.2017.00005 PG 15 WC Geosciences, Multidisciplinary SC Geology GA EK0JJ UT WOS:000393612400001 ER PT J AU Handsteiner, J Friedman, AS Rauch, D Gallicchio, J Liu, B Hosp, H Kofler, J Bricher, D Fink, M Leung, C Mark, A Nguyen, HT Sanders, I Steinlechner, F Ursin, R Wengerowsky, S Guth, AH Kaiser, DI Scheidl, T Zeilinger, A AF Handsteiner, Johannes Friedman, Andrew S. Rauch, Dominik Gallicchio, Jason Liu, Bo Hosp, Hannes Kofler, Johannes Bricher, David Fink, Matthias Leung, Calvin Mark, Anthony Nguyen, Hien T. Sanders, Isabella Steinlechner, Fabian Ursin, Rupert Wengerowsky, Soeren Guth, Alan H. Kaiser, David I. Scheidl, Thomas Zeilinger, Anton TI Cosmic Bell Test: Measurement Settings from Milky Way Stars SO PHYSICAL REVIEW LETTERS LA English DT Article ID HIDDEN-VARIABLE THEORIES; INFLATIONARY UNIVERSE; ENTANGLED PHOTONS; ELECTRON SPINS; VIOLATION; INEQUALITIES; THEOREM; NONLOCALITY; EXTINCTION; RANDOMNESS AB Bell's theorem states that some predictions of quantum mechanics cannot be reproduced by a local-realist theory. That conflict is expressed by Bell's inequality, which is usually derived under the assumption that there are no statistical correlations between the choices of measurement settings and anything else that can causally affect the measurement outcomes. In previous experiments, this "freedom of choice" was addressed by ensuring that selection of measurement settings via conventional "quantum random number generators" was spacelike separated from the entangled particle creation. This, however, left open the possibility that an unknown cause affected both the setting choices and measurement outcomes as recently as mere microseconds before each experimental trial. Here we report on a new experimental test of Bell's inequality that, for the first time, uses distant astronomical sources as "cosmic setting generators." In our tests with polarization-entangled photons, measurement settings were chosen using real-time observations of Milky Way stars while simultaneously ensuring locality. Assuming fair sampling for all detected photons, and that each stellar photon's color was set at emission, we observe statistically significant. greater than or similar to 7.31s and. greater than or similar to 11.93 sigma violations of Bell's inequality with estimated p values of. less than or similar to 1.8 x 10(-13) and. less than or similar to 4.0 x 10(-33), respectively, thereby pushing back by similar to 600 years the most recent time by which any local-realist influences could have engineered the observed Bell violation. C1 [Handsteiner, Johannes; Rauch, Dominik; Liu, Bo; Hosp, Hannes; Bricher, David; Fink, Matthias; Steinlechner, Fabian; Ursin, Rupert; Wengerowsky, Soeren; Scheidl, Thomas; Zeilinger, Anton] Austrian Acad Sci, IQOQI, Boltzmanngasse 3, A-1090 Vienna, Austria. [Friedman, Andrew S.; Mark, Anthony; Sanders, Isabella; Guth, Alan H.; Kaiser, David I.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Gallicchio, Jason; Leung, Calvin] Harvey Mudd Coll, Dept Phys, Claremont, CA 91711 USA. [Liu, Bo] NUDT, Sch Comp, Changsha 410073, Hunan, Peoples R China. [Kofler, Johannes] Max Planck Inst Quantum Opt, Hans Kopfermann Str 1, D-85748 Garching, Germany. [Nguyen, Hien T.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Ursin, Rupert; Zeilinger, Anton] Univ Vienna, Fac Phys, Vienna Ctr Quantum Sci & Technol VCQ, Boltzmanngasse 5, A-1090 Vienna, Austria. RP Handsteiner, J; Zeilinger, A (reprint author), Austrian Acad Sci, IQOQI, Boltzmanngasse 3, A-1090 Vienna, Austria.; Friedman, AS (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA.; Zeilinger, A (reprint author), Univ Vienna, Fac Phys, Vienna Ctr Quantum Sci & Technol VCQ, Boltzmanngasse 5, A-1090 Vienna, Austria. EM johannes.handsteiner@univie.ac.at; asf@mit.edu; anton.zeilinger@univie.ac.at OI Friedman, Andrew/0000-0003-1334-039X; Steinlechner, Fabian/0000-0003-0122-1182 FU Austrian Academy of Sciences (OEAW); Austrian Science Fund (FWF) [SFB F40]; FWF project CoQuS [W1210-N16]; Austrian Federal Ministry of Science, Research and Economy (BMWFW); NSF INSPIRE Grant [PHY-1541160]; NSF Grant [SES-1056580, PLR-1248097]; MIT's Undergraduate Research Opportunities Program (UROP); U.S. Department of Energy [DE-SC0012567]; Harvey Mudd College FX The authors would like to thank Brian Keating, Michael J. W. Hall, Jan-Ake Larsson, Marissa Giustina, Ned Hall, Craig Callender, Jacob Barandes, David Kagan, and Larry Guth for useful discussions. Thanks to the Austrian National Bank (OENB) and the Bundesimmobiliengesellschaft (BIG) for providing the rooms for our receiving stations. This work was supported by the Austrian Academy of Sciences (OEAW), by the Austrian Science Fund (FWF) with SFB F40 (FOQUS) and FWF project CoQuS No. W1210-N16 and the Austrian Federal Ministry of Science, Research and Economy (BMWFW). A.S.F., D.I.K., A.H.G., and J.G. acknowledge support for this project from NSF INSPIRE Grant no. PHY-1541160. A.S.F. acknowledges support from NSF Grant No. SES-1056580. A. M. and I. S. acknowledge support from MIT's Undergraduate Research Opportunities Program (UROP). Portions of this work were conducted in MIT's Center for Theoretical Physics and supported in part by the U.S. Department of Energy under Contract No. DE-SC0012567. J. G. acknowledges support from NSF Grant No. PLR-1248097 and Harvey Mudd College. NR 74 TC 0 Z9 0 U1 10 U2 10 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD FEB 7 PY 2017 VL 118 IS 6 AR 060401 DI 10.1103/PhysRevLett.118.060401 PG 8 WC Physics, Multidisciplinary SC Physics GA EJ8ZQ UT WOS:000393516400001 PM 28234500 ER PT J AU Li, C Krotkov, NA Carn, S Zhang, Y Spurr, RJD Joiner, J AF Li, Can Krotkov, Nickolay A. Carn, Simon Zhang, Yan Spurr, Robert J. D. Joiner, Joanna TI New-generation NASA Aura Ozone Monitoring Instrument (OMI) volcanic SO2 dataset: algorithm description, initial results, and continuation with the Suomi-NPP Ozone Mapping and Profiler Suite (OMPS) SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID GLOBAL CLIMATE-CHANGE; PINATUBO ERUPTION; AIR-POLLUTION; RETRIEVAL; AEROSOL; SPECTROMETER; TEMPERATURE; EMISSIONS; SENSORS; SPACE AB Since the fall of 2004, the Ozone Monitoring Instrument (OMI) has been providing global monitoring of volcanic SO2 emissions, helping to understand their climate impacts and to mitigate aviation hazards. Here we introduce a new-generation OMI volcanic SO2 dataset based on a principal component analysis (PCA) retrieval technique. To reduce retrieval noise and artifacts as seen in the current operational linear fit (LF) algorithm, the new algorithm, OMSO2VOLCANO, uses characteristic features extracted directly from OMI radiances in the spectral fitting, thereby helping to minimize interferences from various geophysical processes (e.g., O-3 absorption) and measurement details (e.g., wavelength shift). To solve the problem of low bias for large SO2 total columns in the LF product, the OMSO2VOLCANO algorithm employs a table lookup approach to estimate SO2 Jacobians (i.e., the instrument sensitivity to a perturbation in the SO2 column amount) and iteratively adjusts the spectral fitting window to exclude shorter wavelengths where the SO2 absorption signals are saturated. To first order, the effects of clouds and aerosols are accounted for using a simple Lambertian equivalent reflectivity approach. As with the LF algorithm, OMSO2VOLCANO provides total column retrievals based on a set of predefined SO2 profiles from the lower troposphere to the lower stratosphere, including a new profile peaked at 13 km for plumes in the upper troposphere. Examples given in this study in-dicate that the new dataset shows significant improvement over the LF product, with at least 50% reduction in retrieval noise over the remote Pacific. For large eruptions such as Kasatochi in 2008 (similar to 1700 kt total SO2) and Sierra Negra in 2005 (>1100DU maximum SO2), OMSO2VOLCANO generally agrees well with other algorithms that also utilize the full spectral content of satellite measurements, while the LF algorithm tends to underestimate SO2. We also demonstrate that, despite the coarser spatial and spectral resolution of the Suomi National Polar-orbiting Partnership (Suomi-NPP) Ozone Mapping and Profiler Suite (OMPS) instrument, application of the new PCA algorithm to OMPS data produces highly consistent retrievals between OMI and OMPS. The new PCA algorithm is therefore capable of continuing the volcanic SO2 data record well into the future using current and future hyperspectral UV satellite instruments. C1 [Li, Can; Zhang, Yan] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Li, Can; Krotkov, Nickolay A.; Zhang, Yan; Joiner, Joanna] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Carn, Simon] Michigan Technol Univ, Dept Geol & Min Engn & Sci, Houghton, MI 49931 USA. [Spurr, Robert J. D.] RT Solut Inc, Cambridge, MA 02138 USA. RP Li, C (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.; Li, C (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM can.li@nasa.gov FU NASA Earth Science Division (ESD) Aura Science Team program; NASA's Earth Science New Investigator Program [NNX14AI02G] FX The authors acknowledge the NASA Earth Science Division (ESD) Aura Science Team program (managed by Ken Jucks) for funding of OMI SO2 product development and analysis. The Dutch-and Finnish-built OMI instrument is part of the NASA's Earth Observing System (EOS) Aura satellite payload. The OMI project is managed by the Royal Meteorological Institute of the Netherlands (KNMI) and the Netherlands Space Agency (NSO). Can Li acknowledges partial support from NASA's Earth Science New Investigator Program in developing the OMPS SO2 algorithm (grant no. NNX14AI02G). NR 59 TC 0 Z9 0 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 FEB 6 PY 2017 VL 10 IS 2 BP 445 EP 458 DI 10.5194/amt-10-445-2017 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EM1UO UT WOS:000395102800002 ER PT J AU Cui, H Kaufman, AJ Xiao, SH Zhou, CM Liu, XM AF Cui, Huan Kaufman, Alan J. Xiao, Shuhai Zhou, Chuanming Liu, Xiao-Ming TI Was the Ediacaran Shuram Excursion a globally synchronized early diagenetic event? Insights from methane-derived authigenic carbonates in the uppermost Doushantuo Formation, South China SO CHEMICAL GEOLOGY LA English DT Article DE Shuram Excursion; Authigenic carbonate; Early diagenesis; Ediacaran Period; Sulfate-Methane Transition Zone (SMTZ); Anaerobic Oxidation of Methane (AOM); Neoproterozoic Oxygenation Event (NOE); delta C-13 and delta O-18 co-variation ID OXYGEN-ISOTOPE COMPOSITION; CONTINENTAL-MARGIN SEDIMENTS; POSTGLACIAL CAP CARBONATES; MARINE SULFATE RESERVOIR; FORMATION NAFUN GROUP; SULTANATE-OF-OMAN; YANGTZE PLATFORM; SEA-FLOOR; DEATH-VALLEY; PORE-WATER AB The Ediacaran Period is characterized by the most profound negative carbon isotope (delta C-13) excursion in Earth history, the Shuram Excursion. Various hypotheses - including the massive oxidation of dissolved organic carbon (DOC) in the oceans, the weathering of terrestrial organic carbon, or the release and oxidation of methane hydrates and/or expelled petroleum from the subsurface - have been proposed as sources of the C-13-depleted carbon. More recently, it has been suggested that global-scale precipitation of early authigenic carbonates, driven by anaerobic microbial metabolism in unconsolidated sediments, may have caused the Shuram Excursion, but empirical evidence is lacking. Here we present a comprehensive analysis of a Shuram-associated interval from the uppermost Doushantuo Formation in South China. Our study reveals petrographic evidence of methane-derived authigenic calcite (formed as early diagenetic cements and nodules) that are remarkably depleted in C-13- suggesting a buildup of alkalinity in pore fluids through the anaerobic oxidation of methane (AOM) - and systematically depleted in O-18 relative to co-occurring dolomite. Early authigenesis of these minerals is likely to be driven by increased microbial sulfate reduction, triggered by enhanced continental weathering in the context of a marked rise in atmospheric oxygen levels. In light of the finding of methane-derived authigenic carbonates at Zhongling, and based on our basin-scale stratigraphic correlation, we hypothesize that the marked C-13 and O-18 depletion (including their co-variation noted worldwide) in the Shuram Excursion may reflect an episode of authigenesis occurring within a sulfate-methane transition zone (SMTZ). If true, the Shuram Excursion was then a global biogeochemical response to enhanced seawater sulfate concentration in the Ediacaran ocean driven by the Neoproterozoic oxidation of surface environments. This paleo-oceanographic transition may have therefore paved the way for subsequent evolution and diversification of animals. Our study highlights the significance of an integrated approach that combines petrography, mineralogy, and texture-specific micro-drilling geochemistry in chemostratigraphic studies. (C) 2016 Elsevier B.V. All rights reserved. C1 [Cui, Huan] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Cui, Huan] Univ Wisconsin, NASA Astrobiol Inst, Madison, WI 53706 USA. [Cui, Huan; Kaufman, Alan J.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Cui, Huan; Kaufman, Alan J.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Xiao, Shuhai] Virginia Polytech Inst & State Univ, Dept Geosci, Blacksburg, VA 24061 USA. [Zhou, Chuanming] Chinese Acad Sci, Nanjing Inst Geol & Palaeontol, Key Lab Econ Stratig & Palaeogeog, Nanjing 210008, Jiangsu, Peoples R China. [Liu, Xiao-Ming] Univ N Carolina, Dept Geol Sci, Chapel Hill, NC 27599 USA. RP Cui, H (reprint author), Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.; Cui, H (reprint author), Univ Wisconsin, NASA Astrobiol Inst, Madison, WI 53706 USA. EM Huan.Cui@wisc.edu FU NASA [NNX12AR91G, NNX15AL27G]; NSF [EAR0844270, EAR1528553]; Chinese Academy of Sciences [KZZD-EW-02]; Mineralogical Society of America (MSA) Grant for Student Research in Mineralogy and Petrology; Society of Economic Geologists (SEG) Student Research Grant; Explorers Club Exploration Fund Grant; International Association of Sedimentologists (IAS) Graduate Student Research Grant FX This research is funded by NASA Exobiology (NNX12AR91G to AJK and NNX15AL27G to SX), NSF Sedimentary Geology and Paleontology (EAR0844270 to AJK; EAR1528553 to SX), Chinese Academy of Sciences (KZZD-EW-02 to CZ), and multiple graduate student research grants to HC, including the Mineralogical Society of America (MSA) Grant for Student Research in Mineralogy and Petrology, the Society of Economic Geologists (SEG) Student Research Grant, the Explorers Club Exploration Fund Grant, and the International Association of Sedimentologists (IAS) Graduate Student Research Grant. HC also wants to thank the NASA Astrobiology Institute in UW-Madison for support. NR 219 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2541 EI 1878-5999 J9 CHEM GEOL JI Chem. Geol. PD FEB 5 PY 2017 VL 450 BP 59 EP 80 DI 10.1016/j.chemgeo.2016.12.010 PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EL2TR UT WOS:000394473600005 ER PT J AU Fatoyinbo, L AF Fatoyinbo, Lola TI ECOLOGY Vast peatlands found in the Congo Basin SO NATURE LA English DT Editorial Material C1 [Fatoyinbo, Lola] NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Fatoyinbo, L (reprint author), NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM lola.fatoyinbo@nasa.gov NR 10 TC 0 Z9 0 U1 2 U2 2 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD FEB 2 PY 2017 VL 542 IS 7639 BP 38 EP 39 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EN6MY UT WOS:000396119300025 PM 28150755 ER PT J AU Dhillon, SS Vitiello, MS Linfield, EH Davies, AG Hoffmann, MC Booske, J Paoloni, C Gensch, M Weightman, P Williams, GP Castro-Camus, E Cumming, DRS Simoens, F Escorcia-Carranza, I Grant, J Lucyszyn, S Kuwata-Gonokami, M Konishi, K Koch, M Schmuttenmaer, CA Cocker, TL Huber, R Markelz, AG Taylor, ZD Wallace, VP Zeitler, JA Sibik, J Korter, TM Ellison, B Rea, S Goldsmith, P Cooper, KB Appleby, R Pardo, D Huggard, PG Krozer, V Shams, H Fice, M Renaud, C Seeds, A Stohr, A Naftaly, M Ridler, N Clarke, R Cunningham, JE Johnston, MB AF Dhillon, S. S. Vitiello, M. S. Linfield, E. H. Davies, A. G. Hoffmann, Matthias C. Booske, John Paoloni, Claudio Gensch, M. Weightman, P. Williams, G. P. Castro-Camus, E. Cumming, D. R. S. Simoens, F. Escorcia-Carranza, I. Grant, J. Lucyszyn, Stepan Kuwata-Gonokami, Makoto Konishi, Kuniaki Koch, Martin Schmuttenmaer, Charles A. Cocker, Tyler L. Huber, Rupert Markelz, A. G. Taylor, Z. D. Wallace, Vincent P. Zeitler, J. Axel Sibik, Juraj Korter, Timothy M. Ellison, B. Rea, S. Goldsmith, P. Cooper, Ken B. Appleby, Roger Pardo, D. Huggard, P. G. Krozer, V. Shams, Haymen Fice, Martyn Renaud, Cyril Seeds, Alwyn Stoehr, Andreas Naftaly, Mira Ridler, Nick Clarke, Roland Cunningham, John E. Johnston, Michael B. TI The 2017 terahertz science and technology roadmap SO JOURNAL OF PHYSICS D-APPLIED PHYSICS LA English DT Review DE terahertz; time-domain spectroscopy; semiconductors ID QUANTUM-CASCADE LASERS; TIME-DOMAIN SPECTROSCOPY; PLASMONIC CONTACT ELECTRODES; BASAL-CELL CARCINOMA; METAL WAVE-GUIDES; NEAR-FIELD; PHOTOCONDUCTIVE EMITTERS; BIOLOGICAL-SYSTEMS; COHERENT-DETECTION; GRAPHENE PLASMONS AB Science and technologies based on terahertz frequency electromagnetic radiation (100 GHz-30 THz) have developed rapidly over the last 30 years. For most of the 20th Century, terahertz radiation, then referred to as sub-millimeter wave or far-infrared radiation, was mainly utilized by astronomers and some spectroscopists. Following the development of laser based terahertz time-domain spectroscopy in the 1980s and 1990s the field of THz science and technology expanded rapidly, to the extent that it now touches many areas from fundamental science to 'real world' applications. For example THz radiation is being used to optimize materials for new solar cells, and may also be a key technology for the next generation of airport security scanners. While the field was emerging it was possible to keep track of all new developments, however now the field has grown so much that it is increasingly difficult to follow the diverse range of new discoveries and applications that are appearing. At this point in time, when the field of THz science and technology is moving from an emerging to a more established and interdisciplinary field, it is apt to present a roadmap to help identify the breadth and future directions of the field. The aim of this roadmap is to present a snapshot of the present state of THz science and technology in 2017, and provide an opinion on the challenges and opportunities that the future holds. To be able to achieve this aim, we have invited a group of international experts to write 18 sections that cover most of the key areas of THz science and technology. We hope that The 2017 Roadmap on THz science and technology will prove to be a useful resource by providing a wide ranging introduction to the capabilities of THz radiation for those outside or just entering the field as well as providing perspective and breadth for those who are well established. We also feel that this review should serve as a useful guide for government and funding agencies. C1 [Dhillon, S. S.] Univ Paris 06, Univ Paris Diderot, Sorbonne Univ,CNRS,Lab Pierre Aigrain, Sorbonne Paris Cite,Ecole Normale Super,PSL Res U, F-75231 Paris, France. [Vitiello, M. S.] CNR, Ist Nanosci, NEST, Piazza San Silvestro 12, I-56127 Pisa, Italy. [Vitiello, M. S.] Scuola Normale Super Pisa, Piazza San Silvestro 12, I-56127 Pisa, Italy. [Linfield, E. H.; Davies, A. G.; Cunningham, John E.] Univ Leeds, Sch Elect & Elect Engn, Leeds LS2 9JT, W Yorkshire, England. [Hoffmann, Matthias C.] SLAC Natl Accelerator Lab, Linac Coherent Light Source, Menlo Pk, CA 94025 USA. [Booske, John] Univ Wisconsin Madison, Dept Elect & Comp Engn, Madison, WI USA. [Paoloni, Claudio] Univ Lancaster, Dept Engn, Lancaster, England. [Gensch, M.] Helmholtz Zentrum Dresden Rossendorf, Inst Radiat Phys, Bautzner Landstr 400, D-01328 Dresden, Germany. [Weightman, P.] Univ Liverpool, Dept Phys, Liverpool L69 7ZE, Merseyside, England. [Williams, G. P.] Jefferson Lab, 12000 Jefferson Ave Suite 21, Newport News, VA 23606 USA. [Castro-Camus, E.] Ctr Invest Opt AC, Loma Bosque 115, Guanajuato 37150, Mexico. [Cumming, D. R. S.; Escorcia-Carranza, I.; Grant, J.] Glasgow, Sch Engn, Microsyst Technol Grp, Glasgow G12 8LT, Lanark, Scotland. [Simoens, F.] CEA Leti MINATEC, 17 Rue Martyrs, F-38054 Grenoble 9, France. [Lucyszyn, Stepan] Imperial Coll London, Dept EEE, Ctr Terahertz Sci & Engn, London, England. [Kuwata-Gonokami, Makoto; Konishi, Kuniaki] Univ Tokyo, Dept Phys, Tokyo, Japan. [Koch, Martin] Philipps Univ Marburg, Fac Phys, D-35032 Marburg, Germany. [Koch, Martin] Philipps Univ Marburg, Ctr Mat Sci, D-35032 Marburg, Germany. [Schmuttenmaer, Charles A.] Yale Univ, Dept Chem, 225 Prospect St,POB 208107, New Haven, CT 06520 USA. [Schmuttenmaer, Charles A.] Yale Univ, Energy Sci Inst, 225 Prospect St,POB 208107, New Haven, CT 06520 USA. [Cocker, Tyler L.; Huber, Rupert] Univ Regensburg, Inst Expt & Angew Phys, Univ Str 31, D-93053 Regensburg, Germany. [Markelz, A. G.] Univ Buffalo State Univ New York, Dept Phys, Buffalo, NY 14620 USA. [Taylor, Z. D.] Univ Calif Los Angeles, Dept Bioengn, Los Angeles, CA 90095 USA. [Wallace, Vincent P.] Univ Western Australia M013, 35 Stirling Highway, Crawley, WA 6009, Australia. [Zeitler, J. Axel; Sibik, Juraj] Magnet Resonance Res Ctr, Dept Chem Engn, JJ Thompson Ave, Cambridge CB3 0HE, England. [Korter, Timothy M.] Syracuse Univ, Dept Chem, 1-014 CST,111 Coll Pl, Syracuse, NY 13244 USA. [Ellison, B.; Rea, S.; Pardo, D.; Huggard, P. G.] RAL Space, STFC, Millimetre Wave Technol Grp, Didcot OX11 0QX, Oxon, England. [Goldsmith, P.] Jet Prop Lab, M-S 180-703,4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Cooper, Ken B.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Appleby, Roger] Innovasec Ltd, 212b West Malvern Rd, Malvern WR14 4BA, Worcs, England. [Krozer, V.] Goethe Univ Frankfurt Main, Goethe Leibniz Terahertz Ctr, D-60323 Frankfurt, Germany. [Shams, Haymen; Fice, Martyn; Renaud, Cyril; Seeds, Alwyn] UCL, Dept Elect & Elect Engn, Torrington Pl, London WC1E 7JE, England. [Stoehr, Andreas] Univ Duisburg Essen, Fac Engn, Dept Optoelect, Lotharstr 55, D-47057 Duisburg, Germany. [Naftaly, Mira; Ridler, Nick] Natl Phys Lab, Div Time Quantum & Electromagnet, Teddington TW11 0LW, Middx, England. [Clarke, Roland] Univ Leeds, Sch Elect & Elect Engn, Leeds LS2 9JT, W Yorkshire, England. [Johnston, Michael B.] Univ Oxford, Dept Phys, Clarendon Lab, Parks Rd, Oxford OX1 3PU, England. RP Cunningham, JE (reprint author), Univ Leeds, Sch Elect & Elect Engn, Leeds LS2 9JT, W Yorkshire, England.; Johnston, MB (reprint author), Univ Oxford, Dept Phys, Clarendon Lab, Parks Rd, Oxford OX1 3PU, England. EM enrique@cio.mx; david.cumming.2@glasgow.ac.uk; J.E.Cunningham@leeds.ac.uk; michael.johnston@physics.ox.ac.uk RI Hoffmann, Matthias/B-3893-2009; Johnston, Michael/B-9813-2008 OI Hoffmann, Matthias/0000-0002-3596-9853; Johnston, Michael/0000-0002-0301-8033 NR 209 TC 0 Z9 0 U1 76 U2 76 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0022-3727 EI 1361-6463 J9 J PHYS D APPL PHYS JI J. Phys. D-Appl. Phys. PD FEB 2 PY 2017 VL 50 IS 4 AR 043001 DI 10.1088/1361-6463/50/4/043001 PG 49 WC Physics, Applied SC Physics GA EI0HL UT WOS:000392153700001 ER PT J AU McGregor, S Sen Gupta, A Dommenget, D Lee, T McPhaden, MJ Kessler, WS AF McGregor, Shayne Sen Gupta, Alex Dommenget, Dietmar Lee, Tong McPhaden, Michael J. Kessler, William S. TI Factors influencing the skill of synthesized satellite wind products in the tropical Pacific SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID GLOBAL-WARMING HIATUS; OCEANIC ROSSBY WAVES; SEA-LEVEL TRENDS; SURFACE; REANALYSIS; CURRENTS; ENSO; CIRCULATION; PREDICTION; DYNAMICS AB Given the importance of tropical Pacific winds to global climate, it is interesting to examine differences in the mean and trend among various wind products, and their implications for ocean circulation. Past analysis has revealed that despite the assimilation of observational data, there remain large differences among reanalysis products. Thus, here we examine if satellite-based synthesis products may provide more consistent estimate than reanalysis. Reanalysis product winds are, however, typically used as a background constraint in constructing the synthesis products to fill spatiotemporal gaps and to deal with satellite wind direction ambiguity. Our study identified two important factors that influence both the mean and trends from synthesized wind products. First, the choice of background wind product in synthesized satellite wind products affects the mean and long-term trends, which has implications for simulations of ocean circulation, sea level, and presumably SST. Second, we identify a clear need for developing a better understanding of, and correcting differences between in situ observations of absolute winds with the satellite-derived relative winds prior to synthesizing. This correction requires careful analysis of satellite surface winds with existing colocated in situ measurements of surface winds and currents, and will benefit from near-surface current observations of the proposed Tropical Pacific Observing System. These results also illustrate the difficulty in independently evaluating the synthesis wind products because the in situ data have been utilized at numerous steps during their development. Addressing these identified issues effectively, will require enhanced collaborations among the wind observation (both satellite and in situ), reanalysis, and synthesis communities. C1 [McGregor, Shayne; Dommenget, Dietmar] Monash Univ, Sch Earth Atmosphere & Environm, Clayton, Vic, Australia. [McGregor, Shayne; Sen Gupta, Alex; Dommenget, Dietmar] ARC Ctr Excellence Climate Syst Sci, Sydney, NSW, Australia. [Sen Gupta, Alex] Univ New South Wales, Climate Change Res Ctr, Sydney, NSW, Australia. [Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA USA. [McPhaden, Michael J.; Kessler, William S.] NOAA, Pacific Marine Environm Lab, 7600 Sand Point Way Ne, Seattle, WA 98115 USA. RP McGregor, S (reprint author), Monash Univ, Sch Earth Atmosphere & Environm, Clayton, Vic, Australia.; McGregor, S (reprint author), ARC Ctr Excellence Climate Syst Sci, Sydney, NSW, Australia. EM shayne.mcgregor@monash.edu NR 39 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD FEB PY 2017 VL 122 IS 2 BP 1072 EP 1089 DI 10.1002/2016JC012340 PG 18 WC Oceanography SC Oceanography GA EQ4QN UT WOS:000398063100018 ER PT J AU Adam, R Bartalucci, I Pratt, GW Ade, P Andre, P Arnaud, M Beelen, A Benoit, A Bideaud, A Billot, N Bourdin, H Bourrion, O Calvo, M Catalano, A Coiffard, G Comis, B D'Addabbo, A De Petris, M Democles, J Desert, FX Doyle, S Egami, E Ferrari, C Goupy, J Kramer, C Lagache, G Leclercq, S Macias-Perez, JF Maurogordato, S Mauskopf, P Mayet, F Monfardini, A Mroczkowski, T Pajot, F Pascale, E Perotto, L Pisano, G Pointecouteau, E Ponthieu, N Reveret, V Ritacco, A Rodriguez, L Romero, C Ruppin, F Schuster, K Sievers, A Triqueneaux, S Tucker, C Zemcov, M Zylka, R AF Adam, R. Bartalucci, I. Pratt, G. W. Ade, P. Andre, P. Arnaud, M. Beelen, A. Benoit, A. Bideaud, A. Billot, N. Bourdin, H. Bourrion, O. Calvo, M. Catalano, A. Coiffard, G. Comis, B. D'Addabbo, A. De Petris, M. Democles, J. Desert, F. -X. Doyle, S. Egami, E. Ferrari, C. Goupy, J. Kramer, C. Lagache, G. Leclercq, S. Macias-Perez, J. -F. Maurogordato, S. Mauskopf, P. Mayet, F. Monfardini, A. Mroczkowski, T. Pajot, F. Pascale, E. Perotto, L. Pisano, G. Pointecouteau, E. Ponthieu, N. Reveret, V. Ritacco, A. Rodriguez, L. Romero, C. Ruppin, F. Schuster, K. Sievers, A. Triqueneaux, S. Tucker, C. Zemcov, M. Zylka, R. TI Mapping the kinetic Sunyaev-Zel'dovich effect toward MACS J0717.5+3745 with NIKA SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques: high angular resolution; galaxies: clusters: individual: MACS J0717.5+3745; galaxies: clusters: intracluster medium ID HIGH ANGULAR RESOLUTION; STRONG-LENSING ANALYSIS; PHOTON IMAGING CAMERA; 30 M TELESCOPE; GALAXY CLUSTERS; XMM-NEWTON; INDUCTANCE DETECTORS; PECULIAR VELOCITIES; CROSS-CALIBRATION; COMPLETE SAMPLE AB Measurement of the gas velocity distribution in galaxy clusters provides insight into the physics of mergers, through which large scale structures form in the Universe. Velocity estimates within the intracluster medium (ICM) can be obtained via the Sunyaev-Zel'dovich (SZ) effect, but its observation is challenging both in term of sensitivity requirement and control of systematic effects, including the removal of contaminants. In this paper we report resolved observations, at 150 and 260 GHz, of the SZ effect toward the triple merger MACS J0717.5 + 3745 (z = 0.55), using data obtained with the NIKA camera at the IRAM 30 m telescope. Assuming that the SZ signal is the sum of a thermal (tSZ) and a kinetic (kSZ) component and by combining the two NIKA bands, we extract for the first time a resolved map of the kSZ signal in a cluster. The kSZ signal is dominated by a dipolar structure that peaks at -5.1 and + 3.4 sigma, corresponding to two subclusters moving respectively away and toward us and coincident with the cold dense X-ray core and a hot region undergoing a major merging event. We model the gas electron density and line-of-sight velocity of MACS J0717.5 + 3745 as four subclusters. Combining NIKA data with X-ray observations from XMM-Newton and Chandra, we fit this model to constrain the gas line-of-sight velocity of each component, and we also derive, for the first time, a velocity map from kSZ data (i. e. that is model-dependent). Our results are consistent with previous constraints on the merger velocities, and thanks to the high angular resolution of our data, we are able to resolve the structure of the gas velocity. Finally, we investigate possible contamination and systematic effects with a special care given to radio and submillimeter galaxies. Among the sources that we detect with NIKA, we find one which is likely to be a high redshift lensed submillimeter galaxy. C1 [Adam, R.; Ferrari, C.; Maurogordato, S.] Univ Cote Azur, Lab Lagrange, Observ Cote Azur, CNRS, Blvd Observ,CS 34229, F-06304 Nice 4, France. [Adam, R.; Bourrion, O.; Catalano, A.; Comis, B.; Macias-Perez, J. -F.; Mayet, F.; Perotto, L.; Ritacco, A.; Ruppin, F.] Univ Grenoble Alpes, Lab Phys Subatom & Cosmol, CNRS, IN2P3, 53 Ave Martyrs, F-38026 Grenoble, France. [Bartalucci, I.; Pratt, G. W.; Andre, P.; Arnaud, M.; Democles, J.; Reveret, V.; Rodriguez, L.] Univ Paris Diderot, CEA Saclay, CNRS INSU, Lab AIM,CEA IRFU, F-91191 Gif Sur Yvette, France. [Ade, P.; Bideaud, A.; Doyle, S.; Mauskopf, P.; Pascale, E.; Pisano, G.; Tucker, C.] Cardiff Univ, Astron Instrumentat Grp, Cardiff CF10 3AT, S Glam, Wales. [Beelen, A.; Pajot, F.] CNRS, IAS, F-91405 Orsay, France. [Beelen, A.; Pajot, F.] Univ Paris 11, F-91405 Orsay, France. [Benoit, A.; Calvo, M.; D'Addabbo, A.; Goupy, J.; Monfardini, A.; Triqueneaux, S.] CNRS, Inst Neel, 25 Rue Martyrs,BP 166, F-38000 Grenoble, France. [Benoit, A.; Calvo, M.; D'Addabbo, A.; Goupy, J.; Monfardini, A.; Triqueneaux, S.] Univ Grenoble Alpes, 25 Rue Martyrs,BP 166, F-38000 Grenoble, France. [Billot, N.; Kramer, C.; Sievers, A.] IRAM, E-18012 Granada, Spain. [Bourdin, H.] Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, I-00133 Rome, Italy. [Coiffard, G.; Leclercq, S.; Romero, C.; Schuster, K.; Zylka, R.] IRAM, F-38406 Grenoble, France. [D'Addabbo, A.; De Petris, M.] Sapienza Univ Roma, Dipartimento Fis, Piazzale Aldo Moro 5, I-00185 Rome, Italy. [Desert, F. -X.; Ponthieu, N.] CNRS, IPAG, F-38058 Grenoble 9, France. [Desert, F. -X.; Ponthieu, N.] Univ Grenoble Alpes, F-38058 Grenoble 9, France. [Egami, E.] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. [Lagache, G.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Mauskopf, P.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Mauskopf, P.] Arizona State Univ, Dept Phys, Tempe, AZ 85287 USA. [Mroczkowski, T.] European Org Astron Res Southern Hemisphere, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Pointecouteau, E.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Pointecouteau, E.] CNRS, IRAP, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France. [Zemcov, M.] Rochester Inst Technol, Ctr Detectors, Sch Phys & Astron, Rochester, NY 14623 USA. [Zemcov, M.] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Adam, R (reprint author), Univ Cote Azur, Lab Lagrange, Observ Cote Azur, CNRS, Blvd Observ,CS 34229, F-06304 Nice 4, France.; Adam, R (reprint author), Univ Grenoble Alpes, Lab Phys Subatom & Cosmol, CNRS, IN2P3, 53 Ave Martyrs, F-38026 Grenoble, France. EM remi.adam@oca.eu FU Foundation Nanoscience Grenoble; LabEx FOCUS [ANR-11-LABX-0013]; ANR [ANR-15-CE31-0017]; European Research Council Advanced Grant ORISTARS under the European Union's Seventh Framework Programme [291294]; ENIGMASS French LabEx; CNES post-doctoral fellowship program; CNES doctoral fellowship program; FOCUS French LabEx doctoral fellowship program; French Agence Nationale de la Recherche [ANR-11-BS56-015]; European Research Council under the European Unions Seventh Framework Programme (FP7)/ERC grant [340519] FX We are thankful to the anonymous referee for useful comments that helped improve the quality of the paper. We are grateful to Jack Sayers for helping us obtain the Herschel SPIRE catalog we use in this paper. We would like to thank the IRAM staff for their support during the campaigns. The NIKA dilution cryostat has been designed and built at the Institut Neel. In particular, we acknowledge the crucial contribution of the Cryogenics Group, and in particular Gregory Garde, Henri Rodenas, Jean Paul Leggeri, Philippe Camus. This work has been partially funded by the Foundation Nanoscience Grenoble, the LabEx FOCUS ANR-11-LABX-0013 and the ANR under the contracts "MKIDS", "NIKA" and ANR-15-CE31-0017. This work has benefited from the support of the European Research Council Advanced Grant ORISTARS under the European Union's Seventh Framework Programme (Grant Agreement No. 291294). We acknowledge fundings from the ENIGMASS French LabEx (B.C. and F.R.), the CNES post-doctoral fellowship program (R.A.), the CNES doctoral fellowship program (A.R.) and the FOCUS French LabEx doctoral fellowship program (A.R.). E.P. acknowledges the support of the French Agence Nationale de la Recherche under grant ANR-11-BS56-015. This research has received funding from the European Research Council under the European Unions Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 340519. NR 94 TC 1 Z9 1 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2017 VL 598 AR A115 DI 10.1051/0004-6361/201629182 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EL2QR UT WOS:000394465000114 ER PT J AU Amundsen, DS Tremblin, P Manners, J Baraffe, I Mayne, NJ AF Amundsen, David S. Tremblin, Pascal Manners, James Baraffe, Isabelle Mayne, Nathan J. TI Treatment of overlapping gaseous absorption with the correlated-k method in hot Jupiter and brown dwarf atmosphere models SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE opacity; radiative transfer; methods: numerical; planets and satellites: atmospheres; brown dwarfs; planets and satellites: gaseous planets ID GLOBAL CIRCULATION MODEL; HD 209458B; RADIATIVE-TRANSFER; GIANT PLANETS; LINE LIST; NONHOMOGENEOUS ATMOSPHERES; SCHEME; EXOPLANETS; RETRIEVAL; EMISSION AB The correlated-k method is frequently used to speed up radiation calculations in both one-dimensional and three-dimensional atmosphere models. An inherent difficulty with this method is how to treat overlapping absorption, i.e. absorption by more than one gas in a given spectral region. We have evaluated the applicability of three different methods in hot Jupiter and brown dwarf atmosphere models, all of which have been previously applied within models in the literature: (i) random overlap, both with and without resorting and rebinning, (ii) equivalent extinction and (iii) pre-mixing of opacities, where (i) and (ii) combine k-coefficients for different gases to obtain k-coefficients for a mixture of gases, while (iii) calculates k-coefficients for a given mixture from the corresponding mixed line-by-line opacities. We find that the random overlap method is the most accurate and flexible of these treatments, and is fast enough to be used in one-dimensional models with resorting and rebinning. In three-dimensional models such as global circulation models (GCMs) it is too slow, however, and equivalent extinction can provide a speed-up of at least a factor of three with only a minor loss of accuracy while at the same time retaining the flexibility gained by combining k-coefficients computed for each gas individually. Pre-mixed opacities are significantly less flexible, and we also find that particular care must be taken when using this method in order to to adequately resolve steep variations in composition at important chemical equilibrium boundaries. We use the random overlap method with resorting and rebinning in our one-dimensional atmosphere model and equivalent extinction in our GCM, which allows us to e.g. consistently treat the feedback of non-equilibrium chemistry on the total opacity and therefore the calculated P-T profiles in our models. C1 [Amundsen, David S.; Tremblin, Pascal; Manners, James; Baraffe, Isabelle; Mayne, Nathan J.] Univ Exeter, Astrophys Grp, Exeter EX4 4QL, Devon, England. [Amundsen, David S.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA. [Amundsen, David S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Tremblin, Pascal] Ctr Etud Saclay, CEA CNRS INRIA UPS UVSQ, Maison Simulat, USR 3441, F-91191 Gif Sur Yvette, France. [Manners, James] Met Off, Exeter EX1 3PB, Devon, England. [Baraffe, Isabelle] Univ Lyon 1, CNRS, ENS Lyon, CRAL,UMR 5574, F-69007 Lyon, France. RP Amundsen, DS (reprint author), Univ Exeter, Astrophys Grp, Exeter EX4 4QL, Devon, England. EM d.s.amundsen@columbia.edu FU European Research Council under the European Community's Seventh Framework Programme (FP7) [247060-PEPS, 320478-TOFU]; NASA Astrobiology Program through the Nexus for Exoplanet System Science; Met Office Academic Partnership secondment; STFC; Large Facilities Capital Fund of BIS; University of Exeter Super-computer; University of Exeter FX We thank the referee, Mark Marley, for comments that significantly improved the paper. This work is partly supported by the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013 Grant Agreement No. 247060-PEPS and grant No. 320478-TOFU). D.S.A. acknowledges support from the NASA Astrobiology Program through the Nexus for Exoplanet System Science. J.M. acknowledges the support of a Met Office Academic Partnership secondment. The calculations for this paper were performed on the DiRAC Complexity machine, jointly funded by STFC and the Large Facilities Capital Fund of BIS, and the University of Exeter Super-computer, a DiRAC Facility jointly funded by STFC, the Large Facilities Capital Fund of BIS and the University of Exeter. NR 41 TC 1 Z9 1 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2017 VL 598 AR A97 DI 10.1051/0004-6361/201629322 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EL2QR UT WOS:000394465000096 ER PT J AU Ciarniello, M De Sanctis, MC Ammannito, E Raponi, A Longobardo, A Palomba, E Carrozzo, FG Tosi, F Li, JY Schroder, SE Zambon, F Frigeri, A Fonte, S Giardino, M Pieters, CM Raymond, CA Russell, CT AF Ciarniello, M. De Sanctis, M. C. Ammannito, E. Raponi, A. Longobardo, A. Palomba, E. Carrozzo, F. G. Tosi, F. Li, J. -Y. Schroeder, S. E. Zambon, F. Frigeri, A. Fonte, S. Giardino, M. Pieters, C. M. Raymond, C. A. Russell, C. T. TI Spectrophotometric properties of dwarf planet Ceres from the VIR spectrometer on board the Dawn mission SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE minor planets, asteroids: individual: Ceres; techniques: photometric; techniques: spectroscopic; techniques: imaging spectroscopy; planets and satellites: surfaces; methods: data analysis ID ASTEROID 21 LUTETIA; BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; DISK-RESOLVED PHOTOMETRY; SATURNS MAIN RINGS; ROSETTA FLY-BY; GALILEO PHOTOMETRY; RADIAL PROFILES; FRAMING CAMERA; PHASE CURVES; LIGHT-CURVE AB Aims. We present a study of the spectrophotometric properties of dwarf planet Ceres in the visual-to-infrared (VIS-IR) spectral range by means of hyper-spectral images acquired by the VIR imaging spectrometer on board the NASA Dawn mission. Methods. Disk-resolved observations with a phase angle within the 7 degrees < alpha < 132 degrees interval were used to characterize Ceres' phase curve in the 0.465-4.05 mu m spectral range. Hapke's model was applied to perform the photometric correction of the dataset to standard observation geometry at VIS-IR wavelength, allowing us to produce albedo and color maps of the surface. The V-band magnitude phase function of Ceres has been computed from disk-resolved images and fitted with both the classical linear model and H-G formalism. Results. The single-scattering albedo and the asymmetry parameter at 0.55 mu m are w = 0.14 +/- 0.02 and xi = 0.11 +/- 0.08, respectively (two-lobe Henyey-Greenstein phase function); at the same wavelength, Ceres' geometric albedo as derived from our modeling is 0.094 +/- 0.007; the roughness parameter is (theta) over bar = 29 degrees +/- 6 degrees. Albedo maps indicate small variability on a global scale with an average reflectance at standard geometry of 0.034 +/- 0.003. Nonetheless, isolated areas such as the Occator bright spots, Haulani, and Oxo show an albedo much higher than average. We measure a significant spectral phase reddening, and the average spectral slope of Ceres' surface after photometric correction is 1.1% k angstrom(-1) and 0.85% k angstrom(-1) at VIS and IR wavelengths, respectively. Broadband color indices are V-R = 0.38 +/- 0.01 and R I = 0.33 +/- 0.02. Color maps show that the brightest features typically exhibit smaller slopes. The H-G modeling of the V-band magnitude phase curve for alpha < 30 degrees gives H = 3.14 +/- 0.04 and G = 0.10 +/- 0.04, while the classical linear model provides V(1; 1; 0 degrees) = 3.48 +/- 0.03 and beta = 0.036 +/- 0.002. The comparison of our results with spectrophotometric properties of other minor bodies indicates that Ceres has a less back-scattering phase function and a slightly higher albedo than comets and C-type objects. However, the latter represents the closest match in the usual asteroid taxonomy. C1 [Ciarniello, M.; De Sanctis, M. C.; Raponi, A.; Longobardo, A.; Palomba, E.; Carrozzo, F. G.; Tosi, F.; Zambon, F.; Frigeri, A.; Fonte, S.; Giardino, M.] IAPS INAF, Via Fosso del Cavaliere 100, I-00133 Rome, Italy. [Ammannito, E.; Russell, C. T.] Univ Calif Los Angeles, Earth Planetary & Space Sci, Los Angeles, CA USA. [Li, J. -Y.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Schroeder, S. E.] German Aerosp Ctr DLR, Inst Planetary Res, D-12489 Berlin, Germany. [Pieters, C. M.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA. [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Ciarniello, M (reprint author), IAPS INAF, Via Fosso del Cavaliere 100, I-00133 Rome, Italy. FU Italian Space Agency; National Aeronautics and Space Administration (NASA, USA); Deutsches Zentrum fur Luft- und Raum-fahrt (DLR, Germany); SELEX ES; Institute for Space Astrophysics and Planetology; Italian National Institute for Astrophysics FX We thank the following institutions and agencies that supported this work: the Italian Space Agency, the National Aeronautics and Space Administration (NASA, USA) and the Deutsches Zentrum fur Luft- und Raum-fahrt (DLR, Germany). The VIR was funded and coordinated by the Italian Space Agency and built by SELEX ES, with the scientific leadership of the Institute for Space Astrophysics and Planetology and the Italian National Institute for Astrophysics, and is operated by the Institute for Space Astrophysics and Planetology, Italy. A portion of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, USA, under contract to NASA. We also thank the Dawn Mission Operations team and the Framing Camera team. NR 81 TC 1 Z9 1 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2017 VL 598 AR A130 DI 10.1051/0004-6361/201629490 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EL2QR UT WOS:000394465000129 ER PT J AU El-Maarry, 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 Cremonese, G Da Deppo, V De Cecco, M Debei, 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-Maarry, 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. Cremonese, G. Da Deppo, V. De Cecco, M. Debei, 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. Kuppers, 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 hemispher (vol 593, A110, 2016) SO ASTRONOMY & ASTROPHYSICS LA English DT Correction DE comets:general; comets:individual: 67P/Churyumov-Gerasimenko; methods:observational; errata, addenda C1 [El-Maarry, M. R.; Thomas, N.; Gracia-Berna, A.; Marschall, R.; Pommerol, A.] Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland. [Bertini, I.; Naletto, G.] Univ Padua, Ctr Ateneo Studi & Attivita Spaziali, Giuseppe Colombo CISAS, I-35131 Padua, Italy. [Lee, J. -C.] Natl Cent Univ, Dept Earth Sci, Chungli 32054, Taiwan. [Massironi, M.; Giacomini, L.] Univ Padua, Dept Geosci, Via G Gradenigo 6, I-35131 Padua, Italy. [Davidsson, B.] Jet Prop Lab, 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.; Knollenberg, J.; Kuehrt, E.; Oklay, N.; Preusker, F.; Scholten, F.; Vincent, J. -B.] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Planetenforsch, 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.; Tubiana, C.] Max Planck Inst Sonnensyst Forsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany. [Barbieri, C.; Cremonese, G.; Lazzarin, M.; Marzari, F.] Osserv Astron Padova, INAF, Vicolo Osservatorio 5, I-35122 Padua, Italy. [Lamy, P. L.; Auger, A. -T.; Groussin, O.] 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. [Rodrigo, R.] CSIC, INTA, Ctr Astrobiol, Madrid 28850, Spain. [Rickman, H.] Uppsala Univ, Dept Phys & Astron, POB 516, S-75120 Uppsala, Sweden. [Rickman, H.] 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 06, Univ Paris Diderot, CNRS, LESIA,Obs Paris, 5 Pl J Janssen, F-92195 Meudon, France. [Bertaux, J. -L.; Fornasier, S.] CNRS, UVSQ, IPSL, LATMOS, 11 Blvd dAlembert, F-78280 Guyancourt, France. [Da Deppo, V.; Naletto, G.] IFN UOS Padova LUXOR, CNR, Via Trasea 7, I-35131 Padua, Italy. [De Cecco, M.] Univ Trento, UNITN, Via Mesiano 77, I-38100 Trento, Italy. [Debei, S.] Univ Padua, Dept Mech Engn, Via Venezia 1, I-35131 Padua, Italy. [Fulle, M.] Osserv Astron Trieste, INAF, 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. [Kuppers, M.] ESA, European Space Astron Ctr, Sci Support Off, POB 78, Madrid 28691, Spain. [Naletto, G.] Univ Padua, Dept Informat Engn, Via Gradenigo 6-B, I-35131 Padua, Italy. [Pajola, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP El-Maarry, MR (reprint author), Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland. EM mohammed.elmaarry@space.unibe.ch NR 1 TC 0 Z9 0 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2017 VL 598 AR C2 DI 10.1051/0004-6361/201628634e PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EL2QR UT WOS:000394465000137 ER PT J AU Hoyer, D Rauch, T Werner, K Kruk, JW Quinet, P AF Hoyer, D. Rauch, T. Werner, K. Kruk, J. W. Quinet, P. TI Complete spectral energy distribution of the hot, helium-rich white dwarf RX J0503.9-2854 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE atomic data; line:identification; stars:abundances; stars:individual:RX J0503.9-2854; virtual observatory tools ID VII OSCILLATOR-STRENGTHS; CONSISTENT DIFFUSION-MODELS; LOCAL INTERSTELLAR-MEDIUM; DATA RELEASE 10; STELLAR LABORATORIES; RE 0503-289; SKY-SURVEY; ULTRAVIOLET SPECTROSCOPY; HIGH-RESOLUTION; CENTRAL STARS AB Context. In the line-of-sight toward the DO-type white dwarf RX J0503.9-2854, the density of the interstellar medium (ISM) is very low, and thus the contamination of the stellar spectrum almost negligible. This allows us to identify many metal lines in a wide wavelength range from the extreme ultraviolet to the near infrared. Aims. In previous spectral analyses, many metal lines in the ultraviolet spectrum of RX J0503.9-2854 have been identified. A complete line list of observed and identified lines is presented here. Methods. We compared synthetic spectra that had been calculated from model atmospheres in non-local thermodynamical equilibrium, with observations. Results. In total, we identified 1272 lines (279 of them were newly assigned) in the wavelength range from the extreme ultraviolet to the near infrared. 287 lines remain unidentified. A close inspection of the EUV shows that still no good fit to the observed shape of the stellar continuum flux can be achieved although He, C, N, O, Al, Si, P, S, Ca, Sc, Ti, V, Cr, Mn, Fe, Cr, Ni Zn, Ga, Ge, As, Kr, Zr, Mo, Sn, Xe, and Ba are included in the stellar atmosphere models. Conclusions. There are two possible reasons for the deviation between observed and synthetic flux in the EUV. Opacities from hitherto unconsidered elements in the model-atmosphere calculation may be missing, and/or the effective temperature is slightly lower than previously determined. C1 [Hoyer, D.; Rauch, T.; Werner, K.] Eberhard Karls 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. [Quinet, P.] Univ Mons UMONS, Phys Atom & Astrophys, B-7000 Mons, Belgium. [Quinet, P.] Univ Liege, IPNAS, B-4000 Liege, Belgium. RP Rauch, T (reprint author), Eberhard Karls Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany. EM rauch@astro.uni-tuebingen.de FU German Aerospace Center (DLR) [50OR1501, 05OR1507]; Federal Ministry of Education and Research (BMBF) [05AC6 VTB, 05AC 11 VTB]; Belgian FRS-FNRS; NASA [NAS526555]; NASA Office of Space Science via grant [NNX09AF08G] FX D.H. and T.R. are supported by the German Aerospace Center (DLR, grants 50OR1501 and 05OR1507, respectively). The German Astrophysical Virtual Observatory (GAVO) project at Tubingen had been supported by the Federal Ministry of Education and Research (BMBF, 05AC6 VTB, 05AC 11 VTB). Financial support from the Belgian FRS-FNRS is also acknowledged. P.Q. is research director of this organization. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS526555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. We thank Ralf Napiwotzki for putting the reduced ESO/VLT spectra at our disposal. NR 56 TC 0 Z9 0 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2017 VL 598 AR A135 DI 10.1051/0004-6361/201629869 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EL2QR UT WOS:000394465000134 ER PT J AU Wertz, O Absil, O Gonzalez, CAG Milli, J Girard, JH Mawet, D Pueyo, L AF Wertz, O. Absil, O. Gonzalez, C. A. Gomez Milli, J. Girard, J. H. Mawet, D. Pueyo, L. TI VLT/SPHERE robust astrometry of the HR8799 planets at milliarcsecond-level accuracy Orbital architecture analysis with PyAstrOFit SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary systems; stars: individual: HR8799; methods: data analysis ID CHAIN MONTE-CARLO; HR 8799 PLANETS; EXTRASOLAR PLANETS; GIANT PLANET; BETA-PICTORIS; DEBRIS DISK; FOMALHAUT B; 1ST LIGHT; MU-M; SYSTEM AB Context. HR8799 is orbited by at least four giant planets, making it a prime target for the recently commissioned Spectro-Polarimetric High-contrast Exoplanet REsearch (VLT/SPHERE). As such, it was observed on five consecutive nights during the SPHERE science verification in December 2014. Aims. We aim to take full advantage of the SPHERE capabilities to derive accurate astrometric measurements based on H-band images acquired with the Infra-Red Dual-band Imaging and Spectroscopy (IRDIS) subsystem, and to explore the ultimate astrometric performance of SPHERE in this observing mode. We also aim to present a detailed analysis of the orbital parameters for the four planets. Methods. We performed thorough post-processing of the IRDIS images with the Vortex Imaging Processing (VIP) package to derive a robust astrometric measurement for the four planets. This includes the identification and careful evaluation of the different contributions to the error budget, including systematic errors. Combining our astrometric measurements with the ones previously published in the literature, we constrain the orbital parameters of the four planets using PyAstrOFit, our new open-source python package dedicated to orbital fitting using Bayesian inference with Monte-Carlo Markov Chain sampling. Results. We report the astrometric positions for epoch 2014.93 with an accuracy down to 2.0 mas, mainly limited by the astrometric calibration of IRDIS. For each planet, we derive the posterior probability density functions for the six Keplerian elements and identify sets of highly probable orbits. For planet d, there is clear evidence for nonzero eccentricity (e similar to 0.35), without completely excluding solutions with smaller eccentricities. The three other planets are consistent with circular orbits, although their probability distributions spread beyond e = 0.2, and show a peak at e similar or equal to 0.1 for planet e. The four planets have consistent inclinations of approximately 30 degrees with respect to the sky plane, but the confidence intervals for the longitude of the ascending node are disjointed for planets b and c, and we find tentative evidence for non-coplanarity between planets b and c at the 2 sigma level. C1 [Wertz, O.; Absil, O.; Gonzalez, C. A. Gomez] Univ Liege, Space Sci Technol & Astrophys Res STAR Inst, 19c Allee Six Aout, B-4000 Liege, Belgium. [Milli, J.; Girard, J. H.] European Southern Observ, Alonso Cordova 3107, Casilla 19001, Santiago De Chi, Chile. [Mawet, D.] CALTECH, Dept Astron, 1200 E Calif Blvd,MC 249-17, Pasadena, CA 91125 USA. [Mawet, D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Pueyo, L.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Wertz, O.] Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany. RP Wertz, O (reprint author), Univ Liege, Space Sci Technol & Astrophys Res STAR Inst, 19c Allee Six Aout, B-4000 Liege, Belgium.; Wertz, O (reprint author), Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany. EM owertz@astro.uni-bonn.de FU e European Research Council under the European Union's Seventh Framework Programme (ERC) [337569]; French Community of Belgium through an ARC grant FX The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (ERC Grant Agreement No. 337569), and from the French Community of Belgium through an ARC grant for Concerted Research Action. NR 78 TC 1 Z9 1 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2017 VL 598 AR A83 DI 10.1051/0004-6361/201628730 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EL2QR UT WOS:000394465000082 ER PT J AU Matthews, JC Bacak, A Khan, MAH Wright, MD Priestley, M Martin, D Percival, CJ Shallcross, DE AF Matthews, James C. Bacak, Asan Khan, M. Anwar H. Wright, Matthew D. Priestley, Michael Martin, Damien Percival, Carl J. Shallcross, Dudley E. TI Urban Pollutant Transport and Infiltration into Buildings Using Perfluorocarbon Tracers SO INTERNATIONAL JOURNAL OF ENVIRONMENTAL RESEARCH AND PUBLIC HEALTH LA English DT Article DE indoor air quality (IAQ); air pollution; dispersion experiments; dynamics of indoor air contaminants; human exposure; indoor; outdoor ratio; perfluorocarbons; tracer; infiltration ID IONIZATION MASS-SPECTROMETRY; INDOOR AIR-POLLUTION; DISPERSION EXPERIMENTS; DEVELOPING-COUNTRIES; EXPOSURE; VARIABILITY; ATMOSPHERE; PRODUCTS; IMPACTS; SCHOOLS AB People spend the majority of their time indoors and therefore the quality of indoor air is worthy of investigation; indoor air quality is affected by indoor sources of pollutants and from pollutants entering buildings from outdoors. In this study, unique perfluorocarbon tracers were released in five experiments at a 100 m and similar to 2 km distance from a large university building in Manchester, UK and tracer was also released inside the building to measure the amount of outdoor material penetrating into buildings and the flow of material within the building itself. Air samples of the tracer were taken in several rooms within the building, and a CO2 tracer was used within the building to estimate air-exchange rates. Air-exchange rates were found to vary between 0.57 and 10.90 per hour. Indoor perfluorocarbon tracer concentrations were paired to outdoor tracer concentrations, and in-out ratios were found to vary between 0.01 and 3.6. The largest room with the lowest air-exchange rate exhibited elevated tracer concentrations for over 60 min after the release had finished, but generally had the lowest concentrations, the room with the highest ventilation rates had the highest concentration over 30 min, but the peak decayed more rapidly. Tracer concentrations indoors compared to outdoors imply that pollutants remain within buildings after they have cleared outside, which must be considered when evaluating human exposure to outdoor pollutants. C1 [Khan, M. Anwar H.; Martin, Damien; Shallcross, Dudley E.] Univ Bristol, Sch Chem, Atmospher Chem Res Grp, Cantocks Close, Bristol BS8 1TS, Avon, England. [Bacak, Asan; Priestley, Michael] Univ Manchester, Ctr Atmospher Sci, Sch Earth Atmospher & Environm Sci, Simon Bldg,Brunswick St, Manchester M13 9PL, Lancs, England. [Percival, Carl J.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA. RP Shallcross, DE (reprint author), Univ Bristol, Sch Chem, Atmospher Chem Res Grp, Cantocks Close, Bristol BS8 1TS, Avon, England. EM j.c.matthews@bristol.ac.uk; asan.bacak@manchester.ac.uk; anwar.khan@bristol.ac.uk; matthew.wright@bristol.ac.uk; michael.priestley@manchester.ac.uk; d.martin@bristol.ac.uk; carl.j.percival@jpl.nasa.gov; d.e.shallcross@bris.ac.uk FU NERC [NE/K01501X/1] FX This work was funded by NERC Grant NE/K01501X/1 (Bristol) and NERC Grant NE/KO14811/1 (Manchester). NR 33 TC 0 Z9 0 U1 0 U2 0 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 1660-4601 J9 INT J ENV RES PUB HE JI Int. J. Environ. Res. Public Health PD FEB PY 2017 VL 14 IS 2 AR 214 DI 10.3390/ijerph14020214 PG 17 WC Environmental Sciences; Public, Environmental & Occupational Health SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health GA EM7CA UT WOS:000395467900106 ER PT J AU Giachero, A Alpert, BK Becker, DT Bennett, DA Biasotti, M Brofferio, C Ceriale, V Ceruti, G Corsini, D Day, PK De Gerone, M Dressler, R Faverzani, M Ferri, E Fowler, JW Fumagalli, E Gallucci, G Gard, JD Gatti, F Hays-Wehle, JP Heinitz, S Hilton, GC Koster, U Lusignoli, M Mates, JAB Nisi, S Nucciotti, A Orlando, A Parodi, L Pessina, G Pizzigoni, G Puiu, A Ragazzi, S Reintsema, CD Gomes, MR Schmidt, DR Schumann, D Siccardi, F Sisti, M Swetz, DS Terranova, F Ullom, JN Vale, LR AF Giachero, A. Alpert, B. K. Becker, D. T. Bennett, D. A. Biasotti, M. Brofferio, C. Ceriale, V. Ceruti, G. Corsini, D. Day, P. K. De Gerone, M. Dressler, R. Faverzani, M. Ferri, E. Fowler, J. W. Fumagalli, E. Gallucci, G. Gard, J. D. Gatti, F. Hays-Wehle, J. P. Heinitz, S. Hilton, G. C. Koster, U. Lusignoli, M. Mates, J. A. B. Nisi, S. Nucciotti, A. Orlando, A. Parodi, L. Pessina, G. Pizzigoni, G. Puiu, A. Ragazzi, S. Reintsema, C. D. Ribeiro Gomes, M. Schmidt, D. R. Schumann, D. Siccardi, F. Sisti, M. Swetz, D. S. Terranova, F. Ullom, J. N. Vale, L. R. TI Measuring the electron neutrino mass with improved sensitivity: the HOLMES experiment SO JOURNAL OF INSTRUMENTATION LA English DT Article DE Cryogenic detectors; Neutrino detectors; Superconductive detectors (bolometers tunnel junctions etc); X-ray detectors ID TRANSITION-EDGE SENSORS; HO-163; DECAY AB HOLMES is a new experiment aiming at directly measuring the neutrino mass with a sensitivity below 2 eV. HOLMES will perform a calorimetric measurement of the energy released in the decay of Ho-163. The calorimetric measurement eliminates systematic uncertainties arising from the use of external beta sources, as in experiments with spectrometers. This measurement was proposed in 1982 by A. De Rujula and M. Lusignoli, but only recently the detector technological progress has allowed to design a sensitive experiment. HOLMES will deploy a 1000 pixels array of low temperature microcalorimeters with implanted 163Ho nuclei. HOLMES, besides being an important step forward in the direct neutrino mass measurement with a calorimetric approach, will also establish the potential of this approach to extend the sensitivity down to 0.1 eV and lower. The detectors used for the HOLMES experiment will be Mo/Cu bilayers TESs (Transition Edge Sensors) on SiNx membrane with gold absorbers. Microwave multiplexed rf-SQUIDs are the best available technique to read out large array of such detectors. An extensive R&D activity is in progress in order to maximize the multiplexing factor while preserving the performances of the individual detectors. To embed the 163Ho into the gold absorbers a custom mass separator ion implanter is being developed. The current activities are focused on the the single detector performances optimization and on the 163Ho isotope production and embedding. A preliminary measurement of a sub-array of 4 x 16 detectors is planned late in 2017. In this contribution we present the HOLMES project with its technical challenges, its status and perspectives. C1 [Giachero, A.; Brofferio, C.; Ceruti, G.; Faverzani, M.; Ferri, E.; Hays-Wehle, J. P.; Nucciotti, A.; Pessina, G.; Puiu, A.; Ragazzi, S.; Sisti, M.; Terranova, F.] Ist Nazl Fis Nucl, Sez Milano Bicocca, I-20126 Milan, Italy. [Alpert, B. K.; Becker, D. T.; Bennett, D. A.; Fowler, J. W.; Gard, J. D.; Hays-Wehle, J. P.; Hilton, G. C.; Mates, J. A. B.; Reintsema, C. D.; Schmidt, D. R.; Swetz, D. S.; Ullom, J. N.; Vale, L. R.] NIST, Boulder, CO 80305 USA. [Nisi, S.; Ragazzi, S.] Ist Nazl Fis Nucl, Lab Nazl Gran Sasso LNGS, I-67010 Laquila, Italy. [Biasotti, M.; Ceriale, V.; Corsini, D.; De Gerone, M.; Fumagalli, E.; Gallucci, G.; Gatti, F.; Orlando, A.; Parodi, L.; Pizzigoni, G.; Siccardi, F.] Ist Nazl Fis Nucl, Sez Genova, I-16146 Genoa, Italy. [Biasotti, M.; Corsini, D.; De Gerone, M.; Gatti, F.; Pizzigoni, G.] Univ Genoa, Dipartimento Fis, I-16146 Genoa, Italy. [Brofferio, C.; Faverzani, M.; Nucciotti, A.; Puiu, A.; Ragazzi, S.; Sisti, M.; Terranova, F.] Univ Milano Bicocca, Dipartimento Fis, I-20126 Milan, Italy. [Day, P. K.] Jet Prop Lab, Pasadena, CA 91107 USA. [Dressler, R.; Heinitz, S.; Schumann, D.] Paul Scherrer Inst, CH-5232 Villigen, Switzerland. [Koster, U.] Inst Laue Langevin ILL, F-38000 Grenoble, France. [Lusignoli, M.] Sapienza Univ Roma, Dipartimento Fis, I-00185 Rome, Italy. [Lusignoli, M.] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy. [Ribeiro Gomes, M.] Univ Lisbon, Multidisciplinary Ctr Astrophys, CENTRA, P-1049001 Lisbon, Portugal. RP Giachero, A (reprint author), Ist Nazl Fis Nucl, Sez Milano Bicocca, I-20126 Milan, Italy. EM Andrea.Giachero@.mib.infn.it FU European Research Council [340321]; INFN through the MARE project; NIST Innovations in Measurement Science program for the TES detector development FX This work was supported by the European Research Council (FP7/2007- 2013) under Grant Agreement HOLMES no. 340321. We also acknowledge the support from INFN through the MARE project and from the NIST Innovations in Measurement Science program for the TES detector development. NR 18 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-0221 J9 J INSTRUM JI J. Instrum. PD FEB PY 2017 VL 12 AR C02046 DI 10.1088/1748-0221/12/02/C02046 PG 12 WC Instruments & Instrumentation SC Instruments & Instrumentation GA EQ1JK UT WOS:000397825800046 ER PT J AU Nguyen, H Cressie, N Braverman, A AF Hai Nguyen Cressie, Noel Braverman, Amy TI Multivariate Spatial Data Fusion for Very Large Remote Sensing Datasets SO REMOTE SENSING LA English DT Article DE EM algorithm; Fixed Rank Kriging; multivariate geostatistics; Spatial Random; Effects model ID COLUMN OBSERVING NETWORK; CO2 RETRIEVAL ALGORITHM; SPATIOTEMPORAL DATA; DATA SETS; CALIBRATION; VALIDATION AB Global maps of total-column carbon dioxide (CO2) mole fraction (in units of parts per million) are important tools for climate research since they provide insights into the spatial distribution of carbon intake and emissions as well as their seasonal and annual evolutions. Currently, two main remote sensing instruments for total-column CO2 are the Orbiting Carbon Observatory-2 (OCO-2) and the Greenhouse gases Observing SATellite (GOSAT), both of which produce estimates of CO2 concentration, called profiles, at 20 different pressure levels. Operationally, each profile estimate is then convolved into a single estimate of column-averaged CO2 using a linear pressure weighting function. This total-column CO2 is then used for subsequent analyses such as Level 3 map generation and colocation for validation. In principle, total-column CO2 in these applications may be more efficiently estimated by making optimal estimates of the vector-valued CO2 profiles and applying the pressure weighting function afterwards. These estimates will be more efficient if there is multivariate dependence between CO2 values in the profile. In this article, we describe a methodology that uses a modified Spatial Random Effects model to account for the multivariate nature of the data fusion of OCO-2 and GOSAT. We show that multivariate fusion of the profiles has improved mean squared error relative to scalar fusion of the column-averaged CO2 values from OCO-2 and GOSAT. The computations scale linearly with the number of data points, making it suitable for the typically massive remote sensing datasets. Furthermore, the methodology properly accounts for differences in instrument footprint, measurement-error characteristics, and data coverages. C1 [Hai Nguyen; Cressie, Noel] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. [Cressie, Noel; Braverman, Amy] Univ Wollongong, Natl Inst Appl Stat Res Australia, Wollongong, NSW 2500, Australia. RP Nguyen, H (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM hai.nguyen@jpl.nasa.gov; ncressie@uow.edu.au; hai.nguyen@jpl.nasa.gov FU NASA's Earth Science Technology Office through its Advanced Information Systems Technology program; Discovery Grant, from the Australian Research Council [DP150104576]; NASA [NNHII-ZDA001N-OCO2] FX We would like to thank the reviewers and the editor of Remote Sensing for their insightful comments. The research described in this paper was carried out in part by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. It is supported by NASA's Earth Science Technology Office through its Advanced Information Systems Technology program. Noel Cressie's research was also partially supported by a 2015-2017 Discovery Grant, DP150104576, from the Australian Research Council, and by NASA grant NNHII-ZDA001N-OCO2. ACOS and OCO-2 data were obtained from Goddard Earth Sciences Data and Information Services Center, operated by NASA, from the website http://daac.gsfc.nasa.gov/.TCCON data were obtained from the TCCON Data Archive, hosted by the Carbon Dioxide Information Analysis Center, from the website http://tccon.ornl.gov/. NR 37 TC 0 Z9 0 U1 0 U2 0 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 FEB PY 2017 VL 9 IS 2 AR 142 DI 10.3390/rs9020142 PG 19 WC Remote Sensing SC Remote Sensing GA EO9MV UT WOS:000397013700044 ER PT J AU Wang, Y Cordes, JM Jenet, FA Chatterjee, S Demorest, PB Dolch, T Ellis, JA Lam, MT Madison, DR McLaughlin, MA Perrodin, D Rankin, J Siemens, X Vallisneri, M AF Wang, Yan Cordes, James M. Jenet, Fredrick A. Chatterjee, Shami Demorest, Paul B. Dolch, Timothy Ellis, Justin A. Lam, Michael T. Madison, Dustin R. McLaughlin, Maura A. Perrodin, Delphine Rankin, Joanna Siemens, Xavier Vallisneri, Michele TI Statistical analyses for NANOGrav 5-year timing residuals SO RESEARCH IN ASTRONOMY AND ASTROPHYSICS LA English DT Article DE pulsar timing array; general-statistical tests ID BLACK-HOLE BINARIES; GRAVITATIONAL-WAVE SIGNALS; RELATIVISTIC GRAVITY; GENERAL-RELATIVITY; SPACED DATA; ARRAY DATA; PULSAR; LIMITS; TESTS; RADIATION AB In pulsar timing, timing residuals are the differences between the observed times of arrival and predictions from the timing model. A comprehensive timing model will produce featureless residuals, which are presumably composed of dominating noise and weak physical effects excluded from the timing model (e. g. gravitational waves). In order to apply optimal statistical methods for detecting weak gravitational wave signals, we need to know the statistical properties of noise components in the residuals. In this paper we utilize a variety of non-parametric statistical tests to analyze the whiteness and Gaussianity of the NorthAmerican Nanohertz Observatory for GravitationalWaves (NANOGrav) 5year timing data, which are obtained from Arecibo Observatory and Green Bank Telescope from 2005 to 2010. We find that most of the data are consistent with white noise; many data deviate from Gaussianity at different levels, nevertheless, removing outliers in some pulsars will mitigate the deviations. C1 [Wang, Yan] Huazhong Univ Sci & Technol, Sch Phys, MOE Key Lab Fundamental Phys Quant Measurements, Wuhan 430074, Peoples R China. [Wang, Yan; Jenet, Fredrick A.] Univ Texas Brownsville, Ctr Adv Radio Astron, 1 West Univ Blvd, Brownsville, TX 78520 USA. [Wang, Yan; Jenet, Fredrick A.] Univ Texas Brownsville, Dept Phys & Astron, 1 West Univ Blvd, Brownsville, TX 78520 USA. [Cordes, James M.; Chatterjee, Shami; Lam, Michael T.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Demorest, Paul B.; Madison, Dustin R.] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. [Dolch, Timothy] Hillsdale Coll, Dept Phys, 33 E Coll St, Hillsdale, MI 49242 USA. [Ellis, Justin A.; Vallisneri, Michele] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91106 USA. [McLaughlin, Maura A.] West Virginia Univ, Dept Phys, POB 6315, Morgantown, WV 26505 USA. [Perrodin, Delphine] INAF Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, CA, Italy. [Rankin, Joanna] Univ Vermont, Dept Phys, Burlington, VT 05405 USA. [Siemens, Xavier] Univ Wisconsin, Dept Phys, Ctr Gravitat Cosmol & Astrophys, POB 413, Milwaukee, WI 53201 USA. RP Wang, Y (reprint author), Huazhong Univ Sci & Technol, Sch Phys, MOE Key Lab Fundamental Phys Quant Measurements, Wuhan 430074, Peoples R China.; Wang, Y (reprint author), Univ Texas Brownsville, Ctr Adv Radio Astron, 1 West Univ Blvd, Brownsville, TX 78520 USA.; Wang, Y (reprint author), Univ Texas Brownsville, Dept Phys & Astron, 1 West Univ Blvd, Brownsville, TX 78520 USA. EM ywang12@hust.edu.cn FU National Science Foundation (NSF) under PIRE [0968296]; National Natural Science Foundation of China [11503007, 91636111, 11690021]; New York Space Grant Consortium; NASA through the Einstein Fellowship [PF4-150120]; JPL RTD program; SRI International under NSF [AST-1100968] FX This work was supported by the National Science Foundation (NSF) under PIRE grant 0968296. We are grateful to the NANOGrav members for helpful comments and discussions. Y. W. acknowledges support by the National Natural Science Foundation of China (Grant Nos.11503007, 91636111 and 11690021). D. R. M. acknowledges partial support through the New York Space Grant Consortium. J.A.E.acknowledges support by NASA through the Einstein Fellowship grant PF4-150120. M. V. acknowledges support from the JPL RTD program. Data for this project were collected using the facilities of the National Radio Astronomy Observatory and the Arecibo Observatory. The National Radio Astronomy Observatory is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. The Arecibo Observatory is operated by SRI International under a cooperative agreement with the NSF (AST-1100968),and in alliance with Ana G. M 'endez-UniversidadMetropolitana and the Universities Space Research Association. NR 59 TC 0 Z9 0 U1 0 U2 0 PU NATL ASTRONOMICAL OBSERVATORIES, CHIN ACAD SCIENCES PI BEIJING PA 20A DATUN RD, CHAOYANG, BEIJING, 100012, PEOPLES R CHINA SN 1674-4527 J9 RES ASTRON ASTROPHYS JI Res. Astron. Astrophys. PD FEB PY 2017 VL 17 IS 2 AR 19 DI 10.1088/1674-4527/17/2/19 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EP2JK UT WOS:000397209100009 ER PT J AU Gobeyn, S Van Wesemael, A Neal, J Lievens, H Van Eerdenbrugh, K De Vleeschouwer, N Vernieuwe, H Schumann, GJP Di Baldassarre, G De Baets, B Bates, PD Verhoest, NEC AF Gobeyn, Sacha Van Wesemael, Alexandra Neal, Jeffrey Lievens, Hans Van Eerdenbrugh, Katrien De Vleeschouwer, Niels Vernieuwe, Hilde Schumann, Guy J. -P. Di Baldassarre, Giuliano De Baets, Bernard Bates, Paul D. Verhoest, Niko E. C. TI Impact of the timing of a SAR image acquisition on the calibration of a flood inundation model SO ADVANCES IN WATER RESOURCES LA English DT Article DE Flood inundation; Hydraulic modelling; Remote sensing; Calibration ID RASTER-BASED MODEL; SEQUENTIAL ASSIMILATION; DISTRIBUTED MODELS; LEVEL OBSERVATIONS; FINITE-ELEMENT; WATER STAGES; UNCERTAINTY; EXTENT; PREDICTIONS; SIMULATION AB Synthetic Aperture Radar (SAR) data have proven to be a very useful source of information for the calibration of flood inundation models. Previous studies have focused on assigning uncertainties to SAR images in order to improve flood forecast systems (e.g. Giustarini et al. (2015) and Stephens et al. (2012)). This paper investigates whether the timing of a SAR acquisition of a flood has an important impact on the calibration of a flood inundation model. As no suitable time series of SAR data exists, we generate a sequence of consistent SAR images through the use of a synthetic framework. This framework uses two available ERS-2 SAR images of the study area, one taken during the flood event of interest, the second taken during a dry reference period. The obtained synthetic observations at different points in time during the flood event are used to calibrate the flood inundation model. The results of this study indicate that the uncertainty of the roughness parameters is lower when the model is calibrated with an image taken before rather than during or after the flood peak. The results also show that the error on the modelled extent is much lower when the model is calibrated with a pre-flood peak image than when calibrated with a near-flood peak or a post-flood peak image. It is concluded that the timing of the SAR image acquisition of the flood has a clear impact on the model calibration and consequently on the precision of the predicted flood extent. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Gobeyn, Sacha; Van Wesemael, Alexandra; Lievens, Hans; Van Eerdenbrugh, Katrien; De Vleeschouwer, Niels; Verhoest, Niko E. C.] Univ Ghent, Lab Hydrol & Water Management, Coupure Links 653, B-9000 Ghent, Belgium. [Neal, Jeffrey; Schumann, Guy J. -P.; Bates, Paul D.] Univ Bristol, Sch Geog Sci, Univ Rd, Bristol BS8 1SS, Avon, England. [Lievens, Hans] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Vernieuwe, Hilde; De Baets, Bernard] Univ Ghent, Dept Math Modelling Stat & Bioinformat, KERMIT, Coupure Links 653, B-9000 Ghent, Belgium. [Schumann, Guy J. -P.] Remote Sensing Solut Inc, 248 E Foothill Blvd,Suite 200, Monrovia, CA 91016 USA. [Di Baldassarre, Giuliano] Uppsala Univ, Dept Earth Sci, Villav 16, S-75236 Uppsala, Sweden. RP Van Wesemael, A (reprint author), Univ Ghent, Lab Hydrol & Water Management, Coupure Links 653, B-9000 Ghent, Belgium. EM Alexandra.VanWesemael@UGent.be FU Belgian Science Policy; Research Foundation Flanders (FWO) [G.0179.16N]; "Bijzonder Onderzoeksfonds" of Ghent University [01J04015]; Ghent University; Hercules Foundation; Flemish Government department EWI FX The work in this paper has been funded by the Belgian Science Policy for the FLOODMOIST project in the framework of the STEREO II programme and through project G.0179.16N of the Research Foundation Flanders (FWO) and project 01J04015 of the "Bijzonder Onderzoeksfonds" of Ghent University. Hans Lievens is a postdoctoral research fellow of the FWO. Part of Guy Schumann's time on this manuscript was spent at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The computational resources (Stevin Supercomputer Infrastructure) and services used in this work were provided by the VSC (Flemish Supercomputer Center), funded by Ghent University, the Hercules Foundation and the Flemish Government department EWI. NR 48 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0309-1708 EI 1872-9657 J9 ADV WATER RESOUR JI Adv. Water Resour. PD FEB PY 2017 VL 100 BP 126 EP 138 DI 10.1016/j.advwatres.2016.12.005 PG 13 WC Water Resources SC Water Resources GA EL4ZM UT WOS:000394631100010 ER PT J AU Baurle, RA AF Baurle, R. A. TI Hybrid Reynolds-Averaged/Large-Eddy Simulation of a Cavity Flameholder: Modeling Sensitivities SO AIAA JOURNAL LA English DT Article ID NAVIER-STOKES; FLOWS; TURBULENCE; SCHEME AB Steady-state and scale-resolving simulations have been performed for flow in and around a model scramjet combustor flameholder. The cases simulated corresponded to those used to examine this flowfield experimentally using particle image velocimetry. A variety of turbulence models were used for the steady-state Reynolds-averaged simulations, which included both linear and nonlinear eddy viscosity models. The scale-resolving simulations used a hybrid Reynolds-averaged/large-eddy simulation strategy that is designed to be a large-eddy simulation everywhere except in the inner portion (log layer and below) of the boundary layer. Hence, this formulation can be regarded as a wall-modeled large-eddy simulation. This effort was undertaken to formally assess the performance of the hybrid Reynolds-averaged/large-eddy simulation modeling approach in a flowfield of interest to the scramjet research community. The numerical errors were quantified for both the steady-state and scale-resolving simulations before making any claims of predictive accuracy relative to the measurements. The hybrid Reynolds-averaged/large-eddy simulation results were also carefully scrutinized to ensure that even the coarsest grid had an acceptable level of resolution to meet accepted guidelines for large-eddy simulation and that the time-averaged statistics were acceptably accurate. The autocorrelation and its Fourier transform were the primary tools used for this assessment. Both simulation strategies accurately predicted the mean streamwise velocity distribution within the cavity, although the Reynolds-averaged simulations that used a linear eddy viscosity model tended to overpredict the strength of the primary cavity recirculation zone. Second-order moments of the velocity field were found to be highly sensitive to the turbulence model chosen for the Reynolds-averaged simulations, with all models overpredicting the intensity of the velocity fluctuations within the cavity flameholder. The hybrid Reynolds-averaged/large-eddy simulation results also overpredicted the velocity variances and covariances, unless a filtering operation was applied using a filter size that matched the control volume used to process the particle image velocimetry measurements. This observation suggests that a significant fraction of the turbulence energy was not resolved by the measurements. Taking this uncertainty into account, the second-order statistics extracted from the hybrid simulation strategy could not be shown to be any more accurate than the "best" Reynolds-averaged result. C1 [Baurle, R. A.] NASA, Langley Res Ctr, Hyperson Airbreathing Prop Branch, Hampton, VA 23681 USA. RP Baurle, RA (reprint author), NASA, Langley Res Ctr, Hyperson Airbreathing Prop Branch, Hampton, VA 23681 USA. FU High-Speed Project of the Fundamental Aeronautics Program FX This effort was funded through the High-Speed Project of the Fundamental Aeronautics Program and carried out at the Hypersonic Airbreathing Propulsion Branch at NASA Langley Research Center. Computational resources for this work were provided by the NASA Langley Research Center and the NASA Advanced Supercomputing Division. The author would like to thank Tomasz Drozda for many helpful discussions pertaining to this research effort. The author would also like to acknowledge the efforts of Steven Tuttle from the Naval Research Laboratory for graciously providing the experimental data for this study and David Peterson from the U.S. Air Force Research Laboratory for providing the geometry and other information based on his simulations of this flowpath. NR 39 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 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD FEB PY 2017 VL 55 IS 2 BP 524 EP 543 DI 10.2514/1.J055257 PG 20 WC Engineering, Aerospace SC Engineering GA EM8IR UT WOS:000395555300016 ER PT J AU Baurle, RA AF Baurle, R. A. TI Hybrid Reynolds-Averaged/Large-Eddy Simulation of a Scramjet Cavity Flameholder SO AIAA JOURNAL LA English DT Article ID NAVIER-STOKES; SCHEME; FLOWS; MODEL AB Steady-state and scale-resolving simulations have been performed for flow in and around a model scramjet combustor flameholder. Experimental data available for this configuration include velocity statistics obtained from particle image velocimetry as well as a limited number of scalar measurements using laser-induced breakdown spectroscopy. Several turbulence models were used for the steady-state Reynolds-averaged simulations, which included both linear and nonlinear eddy viscosity models. The scale-resolving simulations used a hybrid Reynolds-averaged/large-eddy simulation strategy that is designed to be a large-eddy simulation everywhere except in the inner portion (log layer and below) of the boundary layer. Hence, this formulation can be regarded as a wall-modeled large-eddy simulation. This effort was undertaken to not only assess the performance of the hybrid Reynolds-averaged/large-eddy simulation modeling approach in a flowfield of interest to the scramjet research community but also to begin to understand how this capability can best be used to augment standard Reynolds-averaged simulations. The numerical errors were quantified for the steady-state simulations and at least qualitatively assessed for the scale-resolving simulations before making any claims of predictive accuracy relative to the measurements. The steady-state Reynolds-averaged results displayed a high degree of variability when comparing the flameholder fuel distributions obtained from each turbulence model. This prompted the consideration of applying the higher-fidelity scale-resolving simulations as a surrogate truth model to calibrate the Reynolds-averaged closures in a nonreacting setting before their use for the combusting simulations. In general, the Reynolds-averaged velocity profile predictions at the lowest fueling level matched the particle imaging measurements almost as well as was observed for the nonreacting condition. However, the velocity field predictions proved to be more sensitive to the flameholder fueling rate than was indicated in the measurements. C1 [Baurle, R. A.] NASA, Langley Res Ctr, Hyperson Airbreathing Prop Branch, Hampton, VA 23681 USA. RP Baurle, RA (reprint author), NASA, Langley Res Ctr, Hyperson Airbreathing Prop Branch, Hampton, VA 23681 USA. FU Aeronautics Evaluation and Test Capabilities Project of the Advanced Air Vehicles Program FX This effort was funded through the Aeronautics Evaluation and Test Capabilities Project of the Advanced Air Vehicles Program and carried out at the Hypersonic Airbreathing Propulsion Branch at the NASA Langley Research Center. Computational resources for this work were provided by the NASA Langley Research Center and the NASA Advanced Supercomputing Division. The author would also like to acknowledge the efforts of Steven Tuttle from the Naval Research Laboratory for graciously providing the measured velocity data for this study and David Peterson from Innovative Scientific Solutions, Inc., for providing the geometry and the laser-induced breakdown spectroscopy data. NR 35 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 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD FEB PY 2017 VL 55 IS 2 BP 544 EP 560 DI 10.2514/1.J055339 PG 17 WC Engineering, Aerospace SC Engineering GA EM8IR UT WOS:000395555300017 ER PT J AU Burns, RA Danehy, PM Halls, BR Jiang, NB AF Burns, Ross A. Danehy, Paul M. Halls, Benjamin R. Jiang, Naibo TI Femtosecond Laser Electronic Excitation Tagging Velocimetry in a Transonic, Cryogenic Wind Tunnel SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT 31st AIAA Aerodynamic Measurement Technology and Ground Testing Conference CY JUN 22-26, 2015 CL Dallas, TX SP AIAA C1 [Burns, Ross A.] NASA, Langley Res Ctr, NIA, Hampton, VA 23681 USA. [Danehy, Paul M.] NASA, Langley Res Ctr, Adv Measurements & Data Syst Branch, Hampton, VA 23681 USA. [Halls, Benjamin R.; Jiang, Naibo] Spectral Energies LLC, Dayton, OH 45431 USA. [Halls, Benjamin R.] US Air Force, Res Lab, Aerosp Syst Directorate, Wright Patterson AFB, OH 45433 USA. RP Burns, RA (reprint author), NASA, Langley Res Ctr, NIA, Hampton, VA 23681 USA. FU NASA Internal Research and Development Program; NASA Small Business Innovation Research Program [NNX14CL74P] FX This work was funded by the NASA Internal Research and Development Program, with Marty Waszak as Program Manager; and the NASA Small Business Innovation Research Program (contract number NNX14CL74P). The authors would like to thank the facility operations team at the 0.3 m transonic cryogenic tunnel facility, including Wes Goodman, Mike Chambers, Karl Maddox, and Cliff Obara, among others. Their contributions allowed these experiments to be conducted efficiently, and they were a pleasure to work alongside for the duration of these tests. Additionally, Stephen Jones was an invaluable part of the team in the construction and implementation of the testing apparatus. Finally, the contributions and moral support of Michael Button from the George Washington University, Brett Bathel and Jennifer Inman from NASA Langley Research Center, and Sukesh Roy from Spectral Energies, LLC were greatly appreciated. NR 14 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 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD FEB PY 2017 VL 55 IS 2 BP 680 EP 685 DI 10.2514/1.J055325 PG 6 WC Engineering, Aerospace SC Engineering GA EM8IR UT WOS:000395555300029 ER PT J AU Ashley, T Simpson, CE Elmegreen, BG Johnson, M Pokhrel, NR AF Ashley, Trisha Simpson, Caroline E. Elmegreen, Bruce G. Johnson, Megan Pokhrel, Nau Raj TI The HI Chronicles of LITTLE THINGS BCDs. III. Gas Clouds in and around Mrk 178, VII Zw 403, and NGC 3738 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : dwarf; galaxies : individual ( Mrk 178VII Zw 403NGC 3738); galaxies : star formation ID COMPACT DWARF GALAXIES; LOW-MASS GALAXIES; STAR-FORMATION THRESHOLDS; INFRARED STELLAR CENSUS; CAMPANAS IMAGING ATLAS; WOLF-RAYET GALAXIES; IRREGULAR GALAXIES; NEUTRAL HYDROGEN; LARGE-SAMPLE; INTERSTELLAR-MEDIUM AB In most blue compact dwarf (BCD) galaxies, it remains unclear what triggers their bursts of star formation. We study the H I of three relatively isolated BCDs, Mrk 178, VII Zw 403, and NGC 3738, in detail to look for signatures of star formation triggers, such as gas cloud consumption, dwarf-dwarf mergers, and interactions with companions. High angular and velocity resolution atomic hydrogen (H I) data from the Very Large Array (VLA) dwarf galaxy H I survey, Local Irregulars That Trace Luminosity Extremes, The H I Nearby Galaxy Survey (LITTLE THINGS), allow us to study the detailed kinematics and morphologies of the BCDs in H I. We also present high-sensitivity H I maps from the NRAO Green Bank Telescope (GBT) of each BCD to search their surrounding regions for extended tenuous emission or companions. The GBT data do not show any distinct galaxies obviously interacting with the BCDs. The VLA data indicate several possible star formation triggers in these BCDs. Mrk 178 likely has a gas cloud impacting the southeast end of its disk or it is experiencing ram pressure stripping. VII Zw 403 has a large gas cloud in its foreground or background that shows evidence of accreting onto the disk. NGC 3738 has several possible explanations for its stellar morphology and H I morphology and kinematics: an advanced merger, strong stellar feedback, or ram pressure stripping. Although apparently isolated, the H I data of all three BCDs indicate that they may be interacting with their environments, which could be triggering their bursts of star formation. C1 [Ashley, Trisha; Simpson, Caroline E.; Pokhrel, Nau Raj] Florida Int Univ, Dept Phys, 11200 SW 8th St,CP 204, Miami, FL 33199 USA. [Elmegreen, Bruce G.] IBM TJ Watson Res Ctr, 1101 Kitchawan Rd, Yorktown Hts, NY 10598 USA. [Johnson, Megan] CSIRO Astron & Space Sci, POB 76, Epping, NSW 1710, Australia. [Ashley, Trisha] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. RP Ashley, T (reprint author), Florida Int Univ, Dept Phys, 11200 SW 8th St,CP 204, Miami, FL 33199 USA.; Ashley, T (reprint author), NASA Ames Res Ctr, Moffett Field, CA 94035 USA. EM trisha.l.ashley@nasa.gov; simpsonc@fiu.edu; bge@us.ibm.com; megan.johnson@csiro.au; npokh001@fiu.edu NR 91 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 FEB PY 2017 VL 153 IS 3 DI 10.3847/1538-3881/aa5ca7 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN3ZZ UT WOS:000395948000004 ER PT J AU Engelhardt, T Jedicke, R Veres, P Fitzsimmons, A Denneau, L Beshore, E Meinke, B AF Engelhardt, Toni Jedicke, Robert Veres, Peter Fitzsimmons, Alan Denneau, Larry Beshore, Ed Meinke, Bonnie TI An Observational Upper Limit on the Interstellar Number Density of Asteroids and Comets SO ASTRONOMICAL JOURNAL LA English DT Article DE comets; general - minor planets; asteroids; general - planetary systems; protoplanetary disks ID OBJECT PROCESSING SYSTEM; PAN-STARRS; SOLAR-SYSTEM; SIZE DISTRIBUTION; ORBITAL EVOLUTION; 96P/MACHHOLZ 1; PERIOD COMETS; TELESCOPE; NUCLEI; BELT AB We derived 90% confidence limits (CLs) on the interstellar number density (rho(CL)(IS)) of interstellar objects (ISOs; comets and asteroids) as a function of the slope of their size-frequency distribution (SFD) and limiting absolute magnitude. To account for gravitational focusing, we first generated a quasi-realistic ISO population to similar to 750 au from the Sun and propagated it forward in time to generate a steady state population of ISOs with heliocentric distance <50 au. We then simulated the detection of the synthetic ISOs using pointing data for each image and average detection efficiencies for each of three contemporary solar system surveys-Pan-STARRS1, the Mt. Lemmon Survey, and the Catalina Sky Survey. These simulations allowed us to determine the surveys' combined ISO detection efficiency under several different but realistic modes of identifying ISOs in the survey data. Some of the synthetic detected ISOs had eccentricities as small as 1.01, which is in the range of the largest eccentricities of several known comets. Our best CL of rho(CL)(SI) = 1.4 x 10(-4) au(-3) implies that the expectation that extra-solar systems form like our solar system, eject planetesimals in the same way, and then distribute them throughout the Galaxy, is too simplistic, or that the SFD or behavior of ISOs as they pass through our solar system is far from expectation. C1 [Engelhardt, Toni; Jedicke, Robert; Veres, Peter; Denneau, Larry; Meinke, Bonnie] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. [Engelhardt, Toni] Tech Univ Munich, Munich, Germany. [Veres, Peter] Comenius Univ, Bratislava, Slovakia. [Veres, Peter] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Fitzsimmons, Alan] Queens Univ, Belfast, Antrim, North Ireland. [Beshore, Ed] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Meinke, Bonnie] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. RP Engelhardt, T (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.; Engelhardt, T (reprint author), Tech Univ Munich, Munich, Germany. NR 57 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 FEB PY 2017 VL 153 IS 3 DI 10.3847/1538-3881/aa5c8a PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN3ZZ UT WOS:000395948000005 ER PT J AU Jung, YK Udalski, A Yee, JC Sumi, T Gould, A Han, C Albrow, MD Lee, CU Kim, SL Chung, SJ Hwang, KH Ryu, YH Shin, IG Zhu, W Cha, SM Kim, DJ Lee, Y Park, BG Pogge, RW Pietrukowicz, P Kozlowski, S Poleski, R Skowron, J Mroz, P Szymanski, MK Soszynski, I Pawlak, M Ulaczyk, K Abe, F Bennett, DP Barry, R Bond, IA Asakura, Y Bhattacharya, A Donachie, M Freeman, M Fukui, A Hirao, Y Itow, Y Koshimoto, N Li, MCA Ling, CH Masuda, K Matsubara, Y Muraki, Y Nagakane, M Oyokawa, H Rattenbury, NJ Sharan, A Sullivan, DJ Suzuki, D Tristram, PJ Yamada, T Yamada, T Yonehara, A AF Jung, Y. K. Udalski, A. Yee, J. C. Sumi, T. Gould, A. Han, C. Albrow, M. D. Lee, C. -U. Kim, S. -L. Chung, S. -J. Hwang, K. -H. Ryu, Y. -H. Shin, I. -G. Zhu, W. Cha, S. -M. Kim, D. -J. Lee, Y. Park, B. -G. Pogge, R. W. Pietrukowicz, P. Kozlowski, S. Poleski, R. Skowron, J. Mroz, P. Szymanski, M. K. Soszynski, I. Pawlak, M. Ulaczyk, K. Abe, F. Bennett, D. P. Barry, R. Bond, I. A. Asakura, Y. Bhattacharya, A. Donachie, M. Freeman, M. Fukui, A. Hirao, Y. Itow, Y. Koshimoto, N. Li, M. C. A. Ling, C. H. Masuda, K. Matsubara, Y. Muraki, Y. Nagakane, M. Oyokawa, H. Rattenbury, N. J. Sharan, A. Sullivan, D. J. Suzuki, D. Tristram, P. J. Yamada, T. Yamada, T. Yonehara, A. CA KMTNet Collaboration OGLE Collaboration MOA Collaboration TI Binary Source Microlensing Event OGLE-2016-BLG-0733: Interpretation of a Long-term Asymmetric Perturbation SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries; general - gravitational lensing; micro ID GRAVITATIONAL LENSING EXPERIMENT; GALACTIC BULGE; OGLE-III; PLANET; DEGENERACY; BREAKING; NETWORK; SYSTEMS; SEARCH; MODELS AB In the process of analyzing an observed light curve, one often confronts various scenarios that can mimic the planetary signals causing difficulties in the accurate interpretation of the lens system. In this paper, we present the analysis of the microlensing event OGLE-2016-BLG-0733. The light curve of the event shows a long-term asymmetric perturbation that would appear to be due to a planet. From the detailed modeling of the lensing light curve, however, we find that the perturbation originates from the binarity of the source rather than the lens. This result demonstrates that binary sources with roughly equal-luminosity components can mimic long-term perturbations induced by planets with projected separations near the Einstein ring. The result also represents the importance of the consideration of various interpretations in planet-like perturbations and of high-cadence observations for ensuring the unambiguous detection of the planet. C1 [Jung, Y. K.; Yee, J. C.; Shin, I. -G.] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. [Udalski, A.; Pietrukowicz, P.; Kozlowski, S.; Poleski, R.; Skowron, J.; Mroz, P.; Szymanski, M. K.; Soszynski, I.; Pawlak, M.; Ulaczyk, K.] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland. [Sumi, T.; Hirao, Y.; Koshimoto, N.; Nagakane, M.; Yamada, T.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. [Gould, A.; Lee, C. -U.; Kim, S. -L.; Chung, S. -J.; Hwang, K. -H.; Ryu, Y. -H.; Cha, S. -M.; Kim, D. -J.; Lee, Y.; Park, B. -G.] Korea Astron & Space Sci Inst, Daejon 305348, South Korea. [Gould, A.; Zhu, W.; Pogge, R. W.; Poleski, R.] Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. [Gould, A.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Han, C.] Chungbuk Natl Univ, Dept Phys, Cheongju 371763, South Korea. [Albrow, M. D.] Univ Canterbury, Dept Phys & Astron, Private Bag 4800, Christchurch 8020, New Zealand. [Lee, C. -U.; Kim, S. -L.; Chung, S. -J.; Park, B. -G.] Korea Univ Sci & Technol, 217 Gajeong Ro, Daejeon 34113, South Korea. [Cha, S. -M.; Lee, Y.] Kyung Hee Univ, Sch Space Res, Yongin 446701, South Korea. [Abe, F.; Asakura, Y.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Oyokawa, H.] Nagoya Univ, Inst Space Earth Environm Res, Nagoya, Aichi 4648601, Japan. [Bennett, D. P.; Bhattacharya, A.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Bennett, D. P.; Suzuki, D.] NASA Goddard Space Flight Ctr, Lab Exoplanets & Stellar Astrophys, Greenbelt, MD 20771 USA. [Barry, R.] NASA Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Bond, I. A.] Massey Univ, Inst Nat & Math Sci, Auckland 0745, New Zealand. [Donachie, M.; Freeman, M.; Li, M. C. A.; Rattenbury, N. J.; Sharan, A.] Univ Auckland, Dept Phys, Private Bag 92019, Auckland, New Zealand. [Fukui, A.] Natl Astron Observ Japan, Okayama Astrophys Observ, 3037-5 Honjo, Okayama 7190232, Japan. [Ling, C. H.] Massey Univ, Inst Informat & Math Sci, Private Bag 102-904,North Shore Mail Ctr, Auckland, New Zealand. [Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand. [Tristram, P. J.] Mt John Univ Observ, POB 56, Lake Tekapo 8770, New Zealand. [Yamada, T.; Yonehara, A.] Kyoto Sangyo Univ, Fac Sci, Dept Phys, Kyoto 6038555, Japan. RP Jung, YK (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. FU National Science Centre, Poland [MAESTRO 2014/14/A/ST9/00121]; JSPS KAKENHI [JSPS24253004, JSPS26247023, JSPS23340064, JSPS15H00781]; Creative Research Initiative Program [20090081561]; National Research Foundation of Korea; NSF [AST-1516842]; Korea Astronomy and Space Science Institute (KASI) [2016-1-832-01] FX The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U. The MOA project is supported by JSPS KAKENHI Grant Numbers JSPS24253004, JSPS26247023, JSPS23340064, and JSPS15H00781. C. H.. acknowledges support from Creative Research Initiative Program (20090081561) of National Research Foundation of Korea. A. G.. is supported from NSF grant AST-1516842 and Korea Astronomy and Space Science Institute (KASI) grant 2016-1-832-01. The KMTNet telescopes are operated by the Korea Astronomy and Space Science Institute (KASI). 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 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD FEB PY 2017 VL 153 IS 3 DI 10.3847/1538-3881/aa5d07 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EN3ZZ UT WOS:000395948000001 ER PT J AU Miller, AA Kulkarni, MK Cao, Y Laher, RR Masci, FJ Surace, JA AF Miller, A. A. Kulkarni, M. K. Cao, Y. Laher, R. R. Masci, F. J. Surace, J. A. TI PREPARING FOR ADVANCED LIGO: A STAR-GALAXY SEPARATION CATALOG FOR THE PALOMAR TRANSIENT FACTORY SO ASTRONOMICAL JOURNAL LA English DT Article DE catalogs; galaxies: statistics; methods: data analysis; methods: statistical; stars: statistics; surveys ID DIGITAL SKY SURVEY; OSCILLATION SPECTROSCOPIC SURVEY; SDSS-III; VARIABLE-STARS; DATA RELEASES; CLASSIFICATION; DISCOVERY; COUNTERPART; PHOTOMETRY; MERGERS AB The search for fast optical transients, such as the expected electromagnetic counterparts to binary neutron star mergers, is riddled with false positives (FPs) ranging from asteroids to stellar flares. While moving objects are readily rejected via image pairs separated by similar to 1 hr, stellar flares represent a challenging foreground, significantly outnumbering rapidly evolving explosions. Identifying stellar sources close to and fainter than the transient detection limit can eliminate these FPs. Here, we present a method to reliably identify stars in deep co-adds of Palomar Transient Factory (PTF) imaging. Our machine-learning methodology utilizes the random forest (RF) algorithm, which is trained using > 3 x 10(6) sources with Sloan Digital Sky Survey (SDSS) spectra. When evaluated on an independent test set, the PTF RF model outperforms the SExtractor star classifier by similar to 4%. For faint sources (r' >= 21 mag), which dominate the field population, the PTF RF model produces a similar to 19% improvement over SExtractor. To avoid false negatives in the PTF transient-candidate stream, we adopt a conservative stellar classification threshold, corresponding to a galaxy misclassification rate of 0.005. Ultimately, similar to 1.70 x 10(8) objects are included in our PTF point-source catalog, of which only similar to 10(6) are expected to be galaxies. We demonstrate that the PTF RF catalog reveals transients that otherwise would have been missed. To leverage its superior image quality, we additionally create an SDSS point-source catalog, which is also tuned to have a galaxy misclassification rate of 0.005. These catalogs have been incorporated into the PTF real-time pipelines to automatically reject stellar sources as non-extragalactic transients. C1 [Miller, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 169-506, Pasadena, CA 91109 USA. [Miller, A. A.; Kulkarni, M. K.; Cao, Y.] CALTECH, Pasadena, CA 91125 USA. [Kulkarni, M. K.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Laher, R. R.; Surace, J. A.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Masci, F. J.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. RP Miller, AA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 169-506, Pasadena, CA 91109 USA.; Miller, AA (reprint author), CALTECH, Pasadena, CA 91125 USA. EM amiller@astro.caltech.edu FU Alfred P. Sloan Foundation; NASA from Hubble Fellowship [HST-HF-51325.01]; NASA [5-26555] FX A.A.M. acknowledges support for this work by NASA from Hubble Fellowship grant HST-HF-51325.01, awarded by STScI, operated by AURA, Inc., for NASA, under contract NAS 5-26555. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA.; 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 51 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 FEB PY 2017 VL 153 IS 2 AR 73 DI 10.3847/1538-3881/153/2/73 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EM6JT UT WOS:000395419400002 ER PT J AU Nugent, CR Mainzer, A Masiero, J Wright, EL Bauer, J Grav, T Kramer, E Sonnett, S AF Nugent, C. R. Mainzer, A. Masiero, J. Wright, E. L. Bauer, J. Grav, T. Kramer, E. Sonnett, S. TI OBSERVED ASTEROID SURFACE AREA IN THE THERMAL INFRARED SO ASTRONOMICAL JOURNAL LA English DT Article DE minor planets, asteroids: general; radiation mechanisms: thermal ID NEOWISE REACTIVATION MISSION; MAIN BELT ASTEROIDS; NEAR-EARTH ASTEROIDS; ASTRONOMICAL-SATELLITE; THERMOPHYSICAL MODEL; PHYSICAL-PROPERTIES; DIAMETERS; ALBEDOS; PERFORMANCE; CALIBRATION AB The rapid accumulation of thermal infrared observations and shape models of asteroids has led to increased interest in thermophysical modeling. Most of these infrared observations are unresolved. We consider what fraction of an asteroid's surface area contributes the bulk of the emitted thermal flux for two model asteroids of different shapes over a range of thermal parameters. The resulting observed surface in the infrared is generally more fragmented than the area observed in visible wavelengths, indicating high sensitivity to shape. For objects with low values of the thermal parameter, small fractions of the surface contribute the majority of thermally emitted flux. Calculating observed areas could enable the production of spatially resolved thermal inertia maps from non-resolved observations of asteroids. C1 [Nugent, C. R.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Mainzer, A.; Masiero, J.; Bauer, J.; Kramer, E.; Sonnett, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wright, E. L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Grav, T.] Planetary Sci Inst, Tucson, AZ USA. RP Nugent, CR (reprint author), CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. OI Kramer, Emily/0000-0003-0457-2519 NR 41 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 FEB PY 2017 VL 153 IS 2 AR 90 DI 10.3847/1538-3881/153/2/90 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EM7KN UT WOS:000395490000003 ER PT J AU Vernazza, P Castillo-Rogez, J Beck, P Emery, J Brunetto, R Delbo, M Marsset, M Marchis, F Groussin, O Zanda, B Lamy, P Jorda, L Mousis, O Delsanti, A Djouadi, Z Dionnet, Z Borondics, F Carry, B AF Vernazza, P. Castillo-Rogez, J. Beck, P. Emery, J. Brunetto, R. Delbo, M. Marsset, M. Marchis, F. Groussin, O. Zanda, B. Lamy, P. Jorda, L. Mousis, O. Delsanti, A. Djouadi, Z. Dionnet, Z. Borondics, F. Carry, B. TI DIFFERENT ORIGINS OR DIFFERENT EVOLUTIONS? DECODING THE SPECTRAL DIVERSITY AMONG C-TYPE ASTEROIDS SO ASTRONOMICAL JOURNAL LA English DT Article DE meteorites, meteors, meteoroids; methods: data analysis; methods: laboratory:solid state; methods: observational; minor planets, asteroids: general; techniques: spectroscopic ID INTERPLANETARY DUST PARTICLES; SPITZER-SPACE-TELESCOPE; MAIN BELT ASTEROIDS; OUTER SOLAR-SYSTEM; 3 MU-M; CARBONACEOUS CHONDRITES; AQUEOUS ALTERATION; JUPITER TROJANS; DARK MATERIAL; THERMAL METAMORPHISM AB Anhydrous pyroxene-rich interplanetary dust particles (IDPs) have been proposed as surface analogs for about two-thirds of all C-complex asteroids. However, this suggestion appears to be. inconsistent with the presence of hydrated silicates on the surfaces of some of these asteroids, including Ceres. Here, we report the presence of enstatite (pyroxene) on the surface of two C-type asteroids (Ceres and Eugenia) based on their spectral properties in the mid-infrared range. The presence of this component is particularly unexpected in the case of Ceres, because. most thermal evolution models predict a surface consisting of hydrated compounds only. The most plausible scenario is that Ceres' surface has been partially contaminated by exogenous enstatite-rich material, possibly coming from the Beagle asteroid family. This scenario questions a similar origin for Ceres and the remaining C-types, and it possibly supports recent results obtained by the Dawn mission (NASA) that Ceres may have formed in the very outer solar system. Concerning the smaller D similar to 200 km C-types such as Eugenia, both their derived surface composition (enstatite and amorphous silicates) and low density (< 1.5 g cm (3)) suggest that these bodies accreted from the same building blocks, namely chondritic porous, pyroxene-rich IDPs and volatiles (mostly water ice), and that a significant volume fraction of these bodies has remained unaffected by hydrothermal activity likely implying a late accretion. In addition, their current heliocentric distance may best explain the presence or absence of water ice at their surfaces. Finally, we raise the possibility that CI chondrites, Tagish-Lake-like material, or hydrated IDPs may be representative samples of the cores of these bodies. C1 [Vernazza, P.; Marsset, M.; Groussin, O.; Lamy, P.; Jorda, L.; Mousis, O.; Delsanti, A.] Aix Marseille Univ, CNRS, LAM, Marseille, France. [Castillo-Rogez, J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Beck, P.] UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France. [Emery, J.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Emery, J.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA. [Brunetto, R.; Djouadi, Z.; Dionnet, Z.] Univ Paris 11, CNRS, UMR 8617, Inst Astrophys Spatiale, Batiment 121, F-91405 Orsay, France. [Delbo, M.; Carry, B.] Observ Cote Azur, CNRS, UNS, Lab Lagrange, Blvd Observ,CS 34229, F-06304 Nice 4, France. [Marchis, F.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Zanda, B.] Observ Paris, IMCCE, 77 Ave Denfert Rochereau, F-75014 Paris, France. [Zanda, B.] UPMC Univ Paris 06, IMPMC, Sorbonne Univ, Museum Natl Hist Nat,UMR 7590,CNRS,IRD,UMR 206, 61 Rue Buffon, F-75005 Paris, France. [Borondics, F.] Soleil Synchrotron, SMIS Beamline, BP48, F-91192 Gif Sur Yvette, France. RP Vernazza, P (reprint author), Aix Marseille Univ, CNRS, LAM, Marseille, France. EM pierre.vernazza@lam.fr OI Borondics, Ferenc/0000-0001-9975-4301 FU Universities Space Research Association, Inc. (USRA), under NASA [NAS2-97001]; Deutsches SOFIA Institut (DSI) under DLR [50 OK 0901] FX We thank the referee for pertinent and constructive remarks. This work is based on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). SOFIA is jointly operated by the Universities Space Research Association, Inc. (USRA), under NASA contract NAS2-97001, and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901 to the University of Stuttgart. We warmly thank Melody Didier for producing Figure 5's artwork. NR 86 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 FEB PY 2017 VL 153 IS 2 AR 72 DI 10.3847/1538-3881/153/2/72 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EM6JT UT WOS:000395419400001 ER PT J AU Cruikshank, DP AF Cruikshank, Dale P. TI Ewen Adair Whitaker 1922-2016 SO ASTRONOMY & GEOPHYSICS LA English DT Biographical-Item C1 [Cruikshank, Dale P.] NASA, Ames Res Ctr, Washington, DC 20546 USA. RP Cruikshank, DP (reprint author), NASA, Ames Res Ctr, Washington, DC 20546 USA. EM dale.p.cruikshank@nasa.gov NR 1 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1366-8781 EI 1468-4004 J9 ASTRON GEOPHYS JI Astron. Geophys. PD FEB 1 PY 2017 VL 58 IS 1 PG 1 WC Astronomy & Astrophysics; Geochemistry & Geophysics SC Astronomy & Astrophysics; Geochemistry & Geophysics GA EP3IO UT WOS:000397276200019 ER PT J AU David, TJ Petigura, EA Hillenbrand, LA Cody, AM Cameron, AC Stauffer, JR Fulton, BJ Isaacson, HT Howard, AW Howell, SB Everett, ME Wang, J Benneke, B Hellier, C West, RG Pollacco, D Anderson, DR AF David, Trevor J. Petigura, Erik A. Hillenbrand, Lynne A. Cody, Ann Marie Cameron, Andrew Collier Stauffer, John R. Fulton, B. J. Isaacson, Howard T. Howard, Andrew W. Howell, Steve B. Everett, Mark E. Wang, Ji Benneke, Bjorn Hellier, Coel West, Richard G. Pollacco, Don Anderson, David R. TI A Transient Transit Signature Associated with the Young Star RIK-210 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planet-star interactions; stars: magnetic field; stars: pre-main sequence; stars: rotation; starspots ID T-TAURI STAR; PRE-MAIN-SEQUENCE; LOW-MASS STARS; RADIAL-VELOCITY VARIABILITY; SCORPIUS OB ASSOCIATION; BETA-PICTORIS SYSTEM; EXTRA-SOLAR COMETS; SIGMA-ORI-E; EVOLUTIONARY MODELS; PLANET CANDIDATE AB We find transient. transit-like dimming events within the K2 time series photometry of the young star RIK-210 in the Upper Scorpius OB association. These dimming events are variable in depth, duration, and morphology. High spatial resolution imaging revealed that. the star is single. and radial velocity monitoring indicated that the dimming events cannot be due to an eclipsing stellar or brown dwarf companion. Archival and follow-up photometry suggest the dimming events are transient in nature. The variable morphology of the dimming events suggests they are not due to a single. spherical body. The ingress of each dimming event is always shallower than egress, as one would expect for an orbiting body with a leading tail. The dimming events are periodic and synchronous with the stellar rotation. However, we argue it is unlikely the dimming events could be attributed to anything on the stellar surface based on the observed depths and durations. Variable obscuration by a protoplanetary disk is unlikely on the basis that the star is not actively accreting and lacks the infrared excess associated with an inner disk. Rather, we explore the possibilities that the dimming events are due to magnetospheric clouds, a transiting protoplanet surrounded by circumplanetary dust and debris, eccentric orbiting bodies undergoing periodic tidal disruption, or an extended field of dust or debris near the corotation radius. C1 [David, Trevor J.; Hillenbrand, Lynne A.; Howard, Andrew W.; Wang, Ji] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Petigura, Erik A.; Benneke, Bjorn] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Cody, Ann Marie; Howell, Steve B.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. [Cameron, Andrew Collier] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Stauffer, John R.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Fulton, B. J.; Howard, Andrew W.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Isaacson, Howard T.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Everett, Mark E.] Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA. [Hellier, Coel; Anderson, David R.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [West, Richard G.; Pollacco, Don] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. RP David, TJ (reprint author), CALTECH, Dept Astron, Pasadena, CA 91125 USA. EM tjd@astro.caltech.edu OI Isaacson, Howard/0000-0002-0531-1073; David, Trevor/0000-0001-6534-6246; Fulton, Benjamin/0000-0003-3504-5316 FU NSF [DGE1144469]; Hubble Fellowship; National Science Foundation [2014184874]; NASA Office of Space Science [NNX09AF08G]; W.M. Keck Foundation FX The authors thank Todd Boroson for allocation of LCOGT director's discretionary time and Nikolaus Volgenau for assistance scheduling observations. We thank the anonymous referee for a thorough review, Saul Rappaport for helpful comments on an early draft and for providing the Fisher matrix analysis of the RVs, Jim Fuller for bringing sigma Ori E to our attention, Eugene Chiang, Konstantin Batygin, Kat Deck, Brad Hansen, and Lee Hartmann for helpful discussions, as well as Norio Narita and John Livingston for attempting follow-up observations. T.J.D. is supported by an NSF Graduate Research Fellowship under Grant DGE1144469. E. A. P. is supported through a Hubble Fellowship. A. M. C.'s research was supported by an appointment to the NASA Postdoctoral Program at the NASA Ames Research Center, administered by Universities Space Research Association under contract with NASA. B.J.F. was supported by the National Science Foundation Graduate Research Fellowship under grant No. 2014184874. Any opinion, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. This paper includes data collected by the Kepler/K2 mission, funded by the NASA Science Mission directorate and obtained from the Mikulski Archive for Space Telescopes (MAST), supported by the NASA Office of Space Science via grant NNX09AF08G. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 108 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 FEB 1 PY 2017 VL 835 IS 2 AR 168 DI 10.3847/1538-4357/835/2/168 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EM1NT UT WOS:000395085000007 ER PT J AU Karna, N Zhang, J Pesnell, WD AF Karna, N. Zhang, J. Pesnell, W. D. TI The Formation and Maintenance of the Dominant Southern Polar Crown Cavity of Cycle 24 SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: filaments, prominences; Sun: magnetic fields ID MAGNETIC-FIELD; SOLAR-CYCLE; DIFFERENTIAL ROTATION; PROMINENCES; FILAMENTS; MODELS; DYNAMO AB In this article, we report a study of the longest- lived polar crown cavity of Solar Cycle 24, using an. observation from 2013, and propose a physical mechanism to explain its sustained existence. We used high temporal and spatial resolution observations from the Atmospheric Imaging Assembly (AIA) and the Helioseismic Magnetic Imager (HMI) instruments on board the Solar Dynamics Observatory (SDO) to explore the structure and evolution of the cavity. Although it existed for more than a year, we examined the circumpolar cavity in great detail from 2013 March 21 to. 2013 October 31. Our study reinforces the existing theory of formation of polar crown filaments that involves two basic processes to form any polar crown cavity as well as the long- lived cavity that we studied here. First, the underlying polarity inversion line (PIL) of the circumpolar cavity is formed between (1) the trailing part of dozens of decayed active regions distributed in different longitudes and (2) the unipolar magnetic field in the polar coronal hole. Second, the long life of the cavity is sustained by the continuing flux cancellation along the PIL. The flux is persistently transported toward the polar region through surface meridional flow and diffusion. The continuing flux cancellation leads to the shrinking of the polar coronal hole.In this article, we report a study of the longest- lived polar crown cavity of Solar Cycle 24, using an. observation from 2013, and propose a physical mechanism to explain its sustained existence. We used high temporal and spatial resolution observations from the Atmospheric Imaging Assembly (AIA) and the Helioseismic Magnetic Imager (HMI) instruments on board the Solar Dynamics Observatory (SDO) to explore the structure and evolution of the cavity. Although it existed for more than a year, we examined the circumpolar cavity in great detail from 2013 March 21 to. 2013 October 31. Our study reinforces the existing theory of formation of polar crown filaments that involves two basic processes to form any polar crown cavity as well as the long- lived cavity that we studied here. First, the underlying polarity inversion line (PIL) of the circumpolar cavity is formed between (1) the trailing part of dozens of decayed active regions distributed in different longitudes and (2) the unipolar magnetic field in the polar coronal hole. Second, the long life of the cavity is sustained by the continuing flux cancellation along the PIL. The flux is persistently transported toward the polar region through surface meridional flow and diffusion. The continuing flux cancellation leads to the shrinking of the polar coronal hole. C1 [Karna, N.; Pesnell, W. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Karna, N.; Zhang, J.] George Mason Univ, Fairfax, VA 22030 USA. RP Karna, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Karna, N (reprint author), George Mason Univ, Fairfax, VA 22030 USA. OI Pesnell, Dean/0000-0002-8306-2500; Zhang, Jie/0000-0003-0951-2486 FU NSF [AGS-1249270, AGS-1460188]; Schlumberger Foundation Faculty for the Future; NASA's Solar Dynamics Observatory FX N. K. thanks the Schlumberger Foundation Faculty for the Future and NASA's Solar Dynamics Observatory for supporting this research. W. D. P. was supported by NASA's Solar Dynamics Observatory. J. Z. is supported by NSF AGS-1249270 and AGS-1460188. The AIA and HMI data are courtesy of NASA/SDO and the AIA and HMI Science Investigation Teams. The GMU AIA and HMI Synoptic Maps Data set can be accessed at http://spaceweather. gmu. edu/projects/synop. The HMI vector synoptic maps were obtained from http://jsoc.stanford. edu/data/hmi/synoptic/. NR 23 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 FEB 1 PY 2017 VL 835 IS 2 AR 135 DI 10.3847/1538-4357/835/2/135 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EL4IV UT WOS:000394585800023 ER PT J AU Kay, C Gopalswamy, N Reinard, A Opher, M AF Kay, C. Gopalswamy, N. Reinard, A. Opher, M. TI Predicting the Magnetic Field of Earth-impacting CMEs SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: coronal mass ejections (CMEs) ID CORONAL MASS EJECTIONS; SOLAR-WIND; INTERPLANETARY SPACE; ARRIVAL TIMES; FLUX ROPES; CYCLE 24; 1 AU; EVOLUTION; PROPAGATION; CLOUDS AB Predicting the impact of coronal mass ejections (CMEs) and the southward component of their magnetic field is one of the key goals of space weather forecasting. We present a new model, the ForeCAT In situ Data Observer (FIDO), for predicting the in situ magnetic field of CMEs. We first simulate a CME using ForeCAT, a model for CME deflection and rotation resulting from the background solar magnetic forces. Using the CME position and orientation from ForeCAT, we then determine the passage of the CME over a simulated spacecraft. We model the CME's magnetic field using a force-free flux rope and we determine the in situ magnetic profile at the synthetic spacecraft. We show that FIDO can reproduce the general behavior of four observed CMEs. FIDO results are very sensitive to the CME's position and orientation, and we show that the uncertainty in a CME's position and orientation from coronagraph images corresponds to a wide range of in situ magnitudes and even polarities. This small range of positions and orientations also includes CMEs that entirely miss the satellite. We show that two derived parameters (the normalized angular distance between the CME nose and satellite position and the angular difference between the CME tilt and the position angle of the satellite with respect to the CME nose) can be used to reliably determine whether an impact or miss occurs. We find that the same criteria separate the impacts and misses for cases representing all four observed CMEs. C1 [Kay, C.; Gopalswamy, N.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Reinard, A.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80505 USA. [Reinard, A.] NOAA, Space Weather Predict Ctr, Boulder, CO 80505 USA. [Opher, M.] Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. RP Kay, C (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. EM christina.d.kay@nasa.gov FU NASA [NNH14ZDA001N-LWS]; NASA Heliophysics Guest Investigator program FX C.K.'s research was supported by an appointment to the NASA Postdoctoral Program at NASA GSFC, administered by the Universities Space Research Association under contract with NASA. The work of N.G. was supported by NASA Heliophysics Guest Investigator program. A.R. was supported by NASA grant NNH14ZDA001N-LWS. NR 71 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 FEB 1 PY 2017 VL 835 IS 2 AR 117 DI 10.3847/1538-4357/835/2/117 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EL4IV UT WOS:000394585800005 ER PT J AU Woods, TN Caspi, A Chamberlin, PC Jones, A Kohnert, R Mason, JP Moore, CS Palo, S Rouleau, C Solomon, SC Machol, J Viereck, R AF Woods, Thomas N. Caspi, Amir Chamberlin, Phillip C. Jones, Andrew Kohnert, Richard Mason, James Paul Moore, Christopher S. Palo, Scott Rouleau, Colden Solomon, Stanley C. Machol, Janet Viereck, Rodney TI New Solar Irradiance Measurements from the Miniature X-Ray Solar Spectrometer Cubesat SO ASTROPHYSICAL JOURNAL LA English DT Article DE space vehicles: instruments; Sun: abundances; Sun: corona; Sun: flares; Sun: X-rays, gamma rays ID PHOTOMETER SYSTEM XPS; ATOMIC DATABASE; EMISSION MEASURES; FLARES; ABUNDANCES; CHIANTI; RHESSI; CALIBRATIONS; TEMPERATURE; SPACECRAFT AB The goal of the Miniature X-ray Solar Spectrometer (MinXSS) CubeSat is to explore the energy distribution of soft X-ray (SXR) emissions from the quiescent Sun, active regions, and during solar flares. and to model the impact on Earth's ionosphere and thermosphere. The energy emitted in the SXR range (0.1-10 keV) can vary by more than a factor of 100, yet we have limited spectral measurements in the SXRs to accurately quantify the spectral dependence of this variability. The MinXSS primary science instrument is an Amptek, Inc. X123 X-ray spectrometer that has an energy range of 0.5-30 keV with a nominal 0.15 keV energy resolution. Two flight models have been built. The first, MinXSS-1, has been making science observations since 2016 June 9. and has observed numerous flares, including more than 40 C-class and 7 M-class flares. These SXR spectral measurements have advantages over broadband SXR observations, such as providing the capability to derive multiple-temperature components and elemental abundances of coronal plasma, improved irradiance accuracy, and higher resolution spectral irradiance as input to planetary ionosphere simulations. MinXSS spectra obtained during the M5.0 flare on 2016 July 23 highlight these advantages. and indicate how the elemental abundance appears to change from primarily coronal to more photospheric during the flare. MinXSS-1 observations are compared to the Geostationary Operational Environmental Satellite (GOES) X-ray Sensor (XRS) measurements of SXR irradiance and estimated corona temperature. Additionally, a suggested improvement to the calibration of the GOES XRS data is presented. C1 [Woods, Thomas N.; Jones, Andrew; Kohnert, Richard; Mason, James Paul; Moore, Christopher S.; Palo, Scott; Rouleau, Colden] Univ Colorado, Boulder, CO 80309 USA. [Caspi, Amir] Southwest Res Inst, Boulder, CO USA. [Chamberlin, Phillip C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Solomon, Stanley C.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. [Machol, Janet; Viereck, Rodney] NOAA, Space Weather Predict Ctr, Boulder, CO USA. RP Woods, TN (reprint author), Univ Colorado, Boulder, CO 80309 USA. OI WOODS, THOMAS/0000-0002-2308-6797; Caspi, Amir/0000-0001-8702-8273 FU NSF; NASA [NNX14AN84G] FX We thank the many students and staff at the University of Colorado for the development, testing, and operations of the MinXSS CubeSat. The early student project design classes were supported by NSF. NASA grant NNX14AN84G has supported the flight build, testing, and operations for the MinXSS mission. 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 FEB 1 PY 2017 VL 835 IS 2 AR 122 DI 10.3847/1538-4357/835/2/122 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EL4IV UT WOS:000394585800010 ER PT J AU Lau, RM Hankins, MJ Schodel, R Sanchez-Bermudez, J Moffat, AFJ Ressler, ME AF Lau, R. M. Hankins, M. J. Schoedel, R. Sanchez-Bermudez, J. Moffat, A. F. J. Ressler, M. E. TI Stagnant Shells in the Vicinity of the Dusty Wolf-Rayet-OB Binary WR 112 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE infrared: stars; stars: individual (WR 112); stars: winds; outflows; stars: Wolf-Rayet ID MASSIVE STARS; QUINTUPLET CLUSTER; INTERSTELLAR DUST; EMISSION; EVOLUTION; YELLOW; SPECTROMETER; SPECTROSCOPY; SUPERGIANTS; CONSISTENT AB We present high spatial resolution mid-infrared images of the nebula around the late-type carbon-rich Wolf-Rayet (WC)-OB binary system WR. 112 taken by the recently upgraded VLT spectrometer and imager for the mid-infrared (VISIR) with the PAH1, Ne II_2, and Q3 filters. The observations reveal a morphology resembling a series of arc-like filaments and broken shells. Dust temperatures and masses are derived for each of the identified filamentary structures, which exhibit temperatures ranging from 179(-6)(+8) K at the exterior W2 filament to 355(-25)(+37) K in the central 3.. The total dust mass summed over the features is 2.6 +/- 0.4 x 10(-5)M(circle dot). A multi-epoch analysis of mid-IR photometry of WR. 112 over the past similar to 20 years reveals no significant variability in the observed dust temperature and mass. The morphology of the mid-IR dust emission from WR. 112 also exhibits no significant expansion from imaging data taken in 2001, 2007, and 2016, which disputes the current interpretation of the nebula as a high expansion velocity (similar to 1200 km s(-1)) "pinwheel"-shaped outflow driven by the central WC-OB collidingwind binary. An upper limit of less than or similar to 120 km s(-1) is derived for the expansion velocity assuming a distance of 4.15. kpc. The upper limit on the average total mass-loss rate from the central 3 '' of WR. 112 is estimated to be less than or similar to 8 x 10(-6)M(circle dot)year(-1). We leave its true nature as an open question, but propose that the WR. 112 nebula may have formed in the outflow during a previous red or yellow supergiant phase of the central Wolf-Rayet star. C1 [Lau, R. M.; Ressler, M. E.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Lau, R. M.] CALTECH, Pasadena, CA 91125 USA. [Hankins, M. J.] Cornell Univ, Dept Astron, Space Sci Bldg, Ithaca, NY 14853 USA. [Schoedel, R.] CSIC, Inst Astrofis Andalucia, Glorieta Astron S-N, E-18008 Granada, Spain. [Sanchez-Bermudez, J.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Moffat, A. F. J.] Univ Montreal, Dept Phys, CP 6128,Succ CV, Montreal, PQ H3C 3J7, Canada. [Moffat, A. F. J.] Ctr Rech Astrophys Quebec, Montreal, PQ, Canada. RP Lau, RM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.; Lau, RM (reprint author), CALTECH, Pasadena, CA 91125 USA. FU National Aeronautics and Space Administration; National Science Foundation Graduate Research Fellowship [DGE-1144153]; OPTICON; European Commission's FP7 Capacities programme [312430]; NSERC (Canada); FQRNT (Quebec); European Research Council under the European Union's Seventh Framework Programme [614922] FX This work is based on observations made with the VISIR instrument on the ESO VLT telescope (program ID. 097.D-0707A) and observations obtained at the Gemini Observatory (P.ID: GS-2007A-Q-38), 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), Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina), and Ministerio da Ciencia, Tecnologia e Inovacao (Brazil). This work was partially carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. M.J.H. acknowledges support from the National Science Foundation Graduate Research Fellowship under grant No. DGE-1144153. J.S.B. acknowledges that this work was partly supported by OPTICON, which is sponsored by the European Commission's FP7 Capacities programme (grant No. 312430). A.F.J.M. is grateful for financial aid to NSERC (Canada) and FQRNT (Quebec). R.S. acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013) / ERC grant agreement No. [614922]. NR 48 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 1 PY 2017 VL 835 IS 2 AR L31 DI 10.3847/2041-8213/835/2/L31 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EM7QF UT WOS:000395506600010 ER PT J AU Carbon, DF Henze, C Nelson, BC AF Carbon, Duane F. Henze, Christopher Nelson, Bron C. TI Exploring the SDSS Data Set with Linked Scatter Plots. I. EMP, CEMP, and CV Stars SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE methods data analysis; stars: abundances; stars: carbon; stars: emission line, Be; stars: Population II - surveys ID METAL-POOR STARS; DIGITAL SKY SURVEY; OLD STELLAR POPULATIONS; DATA RELEASE; MILKY-WAY; CHEMICAL ABUNDANCES; WHITE-DWARF; ATMOSPHERIC PARAMETERS; CATACLYSMIC VARIABLES; SPECTROSCOPIC SURVEY AB We present the results of a search for extremely metal-poor (EMP), carbon-enhanced metal-poor (CEMP), and cataclysmic variable (CV) stars using a new exploration tool based on linked scatter plots (LSPs). Our approach is especially designed to work with very large spectrum data sets such as the SDSS, LAMOST, RAVE, and Gaia data sets, and it can be applied to stellar, galaxy, and quasar spectra. As a demonstration, we conduct our search using the SDSS DR10 data set. We first created a 3326-dimensional phase space containing nearly 2 billion measures of the strengths of over 1600 spectral features in 569,738 SDSS stars. These measures capture essentially all the stellar atomic and molecular species visible at the resolution of SDSS spectra. We show how LSPs can be used to quickly isolate and examine interesting portions of this phase space. To illustrate, we use LSPs coupled with cuts in selected portions of phase space to extract EMP stars, CEMP stars, and CV stars. We present identifications for 59 previously unrecognized candidate EMP stars and 11 previously unrecognized candidate CEMP stars. We also call attention to 2 candidate He II emission CV stars found by the LSP approach that have not yet been discussed in the literature. C1 [Carbon, Duane F.; Henze, Christopher; Nelson, Bron C.] NASA, Ames Res Ctr, Adv Supercomp Facil, Moffett Field, CA 94035 USA. RP Carbon, DF (reprint author), NASA, Ames Res Ctr, Adv Supercomp Facil, Moffett Field, CA 94035 USA. EM Duane.F.Carbon@nasa.gov FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science FX The authors wish to sincerely thank Karen Huyser, Ruth Peterson, and David Schwenke for their insightful comments on the draft of this paper. D.F.C. is indebted to Richard O. Gray for his help in interpreting the WD/dMe spectra encountered in the search for CV stars. We also wish to thank the anonymous referee for pointing out sections of the paper needing additional clarification. 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/. 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. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. MATLAB c. 2015 The MathWorks, Inc. MATLAB and Simulink are registered trademarks of The MathWorks, Inc. See www.mathworks.com/trademarks for a list of additional trademarks. Other product or brand names may be trademarks or registered trademarks of their respective holders. NR 77 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD FEB PY 2017 VL 228 IS 2 AR 19 DI 10.3847/1538-4365/228/2/19 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EP3WJ UT WOS:000397312100009 ER PT J AU Gagne, J Faherty, JK Mamajek, EE Malo, L Doyon, R Filippazzo, JC Weinberger, AJ Donaldson, JK Lepine, S Lafreniere, D Artigau, E Burgasser, AJ Looper, D Boucher, A Beletsky, Y Camnasio, S Brunette, C Arboit, G AF Gagne, Jonathan Faherty, Jacqueline K. Mamajek, Eric E. Malo, Lison Doyon, Rene Filippazzo, Joseph C. Weinberger, Alycia J. Donaldson, Jessica K. Lepine, Sebastien Lafreniere, David Artigau, Etienne Burgasser, Adam J. Looper, Dagny Boucher, Anne Beletsky, Yuri Camnasio, Sara Brunette, Charles Arboit, Genevieve TI BANYAN. IX. The Initial Mass Function and Planetary-mass Object Space Density of the TW HYA Association SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE brown dwarfs; methods: data analysis; open clusters and associations: individual (TW Hya); stars: kinematics and dynamics; stars: low mass; stars: luminosity function, mass function ID PRE-MAIN-SEQUENCE; PICTORIS MOVING GROUP; ALL-SKY SURVEY; VERY-LOW-MASS; SUBSTELLAR CANDIDATE MEMBERS; GENEVA-COPENHAGEN SURVEY; BROWN DWARF CANDIDATE; CENTAURUS OB ASSOCIATION; YOUNG KINEMATIC GROUPS; STAR-FORMATION HISTORY AB A determination of the initial mass function (IMF) of the current, incomplete census of the 10 Myr-old TW. Hya association (TWA) is presented. This census is built from a literature compilation supplemented with new spectra and 17 new radial velocities from ongoing membership surveys, as well as a reanalysis of Hipparcos data that confirmed HR. 4334 (A2 Vn) as a member. Although the dominant uncertainty in the IMF remains census incompleteness, a detailed statistical treatment is carried out to make the IMF determination independent of binning while accounting for small number statistics. The currently known high-likelihood members are fitted by a log-normal distribution with a central mass of 0.21(-0.06) M-+0.11(circle dot) Me and a characteristic width of 0.8(-0.1)(+0.2) dex in the 12M(Jup)-2M(circle dot) range, whereas a Salpeter power law with alpha= 2.2(-0.5)(+1.1) best describes the IMF slope in the 0.1-2M(circle dot) range. This characteristic width is higher than other young associations, which may be due to incompleteness in the current census of low-mass TWA stars. A tentative overpopulation of isolated planetary-mass members similar to 2MASS. J11472421-2040204 and 2MASS. J11193254-1137466 is identified: this indicates that there might be as many as 10(-5)(+13) similar members of TWA with hot-start model-dependent masses estimated at similar to 5-7M(Jup), most of which would be too faint to be detected in 2MASS. Our new radial velocity measurements corroborate the membership of 2MASS. J11472421-2040204, and secure TWA. 28 (M8.5 gamma), TWA. 29 (M9.5 gamma), and TWA. 33 (M4.5 e) as members. The discovery of 2MASS. J09553336-0208403, a young L7-type interloper unrelated to TWA, is also presented. C1 [Gagne, Jonathan; Faherty, Jacqueline K.; Weinberger, Alycia J.; Donaldson, Jessica K.] Carnegie Inst Sci, DTM, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. [Mamajek, Eric E.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Mamajek, Eric E.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Malo, Lison] Canada France Hawaii Telescope, 65-1238 Mamalahoa Highway, Kamuela, HI 96743 USA. [Malo, Lison; Doyon, Rene; Lafreniere, David; Artigau, Etienne; Boucher, Anne; Brunette, Charles; Arboit, Genevieve] Univ Montreal, Inst Res Exoplanets, Dept Phys, CP 6128 Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada. [Filippazzo, Joseph C.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Lepine, Sebastien] Georgia State Univ, Dept Phys & Astron, 25 Pk Pl, Atlanta, GA 30302 USA. [Burgasser, Adam J.] Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr,Mail Code 0424, La Jolla, CA 92182 USA. [Looper, Dagny] New York Univ, Tisch Sch Arts, 721 Broadway 10th Floor, New York, NY 10003 USA. [Beletsky, Yuri] Carnegie Inst Sci, La Campanas Observ, Colina El Pino, La Serena 601, Chile. [Camnasio, Sara] CUNY, Hunter Coll, Dept Phys & Astron, New York, NY 10065 USA. RP Gagne, J (reprint author), Carnegie Inst Sci, DTM, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. EM jgagne@carnegiescience.edu OI Mamajek, Eric/0000-0003-2008-1488; Weinberger, Alycia/0000-0001-6654-7859; Filippazzo, Joseph/0000-0002-0201-8306 FU Natural Science and Engineering Research Council of Canada; National Science Foundation (NSF) [AST-1313029]; NASA NExSS program; NSF [AST09-08419]; CNTAC program [CN2013A-135]; ESO Progam [179.A-2010]; Gemini Observatory [GN-2013A-Q-106, GN2014A-Q-94, GS-2012B-Q-70, GS-2013A-Q-66, GS-2014A-Q55, GS-2015A-Q-85, GS-2015A-Q-60]; IRTF [2015B091]; AURA [AST 0132798] FX This work was supported in part through grants from the Natural Science and Engineering Research Council of Canada. E.E.M. acknowledges support from National Science Foundation (NSF) award AST-1313029 and the NASA NExSS program, and S.L. acknowledges support from NSF grant AST09-08419. This research has benefited from the SpeX Prism Spectral Libraries, maintained by Adam Burgasser at http://ono.ucsd.edu/similar to adam/browndwarfs/spexprism. This document has benefited from technical report SRON/EPS/TN/09-002 prepared by Paul Tol on color blind-friendly color schemes. This research made use of the SIMBAD database and VizieR catalog access tool, operated at the Centre de Donnees astronomiques de Strasbourg, France (Ochsenbein et al. 2000); data products from the Two Micron All Sky Survey (2MASS; Kirkpatrick et al. 2003; Skrutskie et al. 2006), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center (IPAC)/California Institute of Technology (Caltech), funded by the National Aeronautics and Space Administration (NASA) and the National Science Foundation (Skrutskie et al. 2006); data products from the Wide-field Infrared Survey Explorer (WISE; Wright et al. 2010), which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory (JPL)/Caltech, funded by NASA; the VISTA Hemisphere Survey, ESO Progam, 179. A-2010 (PI: McMahon); the NASA/IPAC Infrared Science Archive (IRSA), which is operated by JPL, Caltech, under contract with NASA; and the Infrared Telescope Facility (IRTF), which is operated by the University of Hawaii under Cooperative Agreement NNX-08AE38A with NASA, Science Mission Directorate, Planetary Astronomy Program. This work has made use of data from the European Space Agency (ESA) mission Gaia (http://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, http://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Part of this research was carried out at the JPL, Caltech, under a contract with NASA.; This paper includes data gathered with the 6.5m Magellan Telescopes located at Las Campanas Observatory, Chile (CNTAC program CN2013A-135). Based on observations obtained as part of the VISTA Hemisphere Survey, ESO Progam, 179.A-2010 (PI: McMahon). Based on observations obtained at the Gemini Observatory through programs number GN-2013A-Q-106, GN2014A-Q-94, GS-2012B-Q-70, GS-2013A-Q-66, GS-2014A-Q55, GS-2015A-Q-85, and GS-2015A-Q-60. The Gemini Observatory is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the National Science Foundation (NSF) on behalf of the Gemini partnership: the NSF (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). All data were acquired through the Canadian Astronomy Data Center. This material is based upon work supported by AURA through the National Science Foundation under AURA Cooperative Agreement AST 0132798 as amended. This publication uses observations obtained at IRTF through program number 2015B091. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 232 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD FEB PY 2017 VL 228 IS 2 AR 18 DI 10.3847/1538-4365/228/2/18 PG 51 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EP3WJ UT WOS:000397312100008 ER PT J AU Carman, JC Eleuterio, DP Gallaudet, TC Geernaert, GL Harr, PA Kaye, JA McCarren, DH McLean, CN Sandgathe, SA Toepfer, F Uccellini, LW AF Carman, Jessie C. Eleuterio, Daniel P. Gallaudet, Timothy C. Geernaert, Gerald L. Harr, Patrick A. Kaye, Jack A. McCarren, David H. McLean, Craig N. Sandgathe, Scott A. Toepfer, Frederick Uccellini, Louis W. TI THE NATIONAL EARTH SYSTEM PREDICTION CAPABILITY Coordinating the Giant SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID WEATHER C1 [Carman, Jessie C.] NOAA, Off Weather & Air Qual, Silver Spring, MD USA. [Eleuterio, Daniel P.] Off Naval Res, Arlington, VA 22217 USA. [Gallaudet, Timothy C.] US Navy, Washington, DC USA. [Gallaudet, Timothy C.] Naval Meteorol & Oceanog Command, Stennis Space Ctr, MS USA. [Geernaert, Gerald L.] US DOE, Climate & Environm Sci Div, Germantown, MD USA. [Harr, Patrick A.] Natl Sci Fdn, Div Atmospher & Geospace Sci, 4201 Wilson Blvd, Arlington, VA 22230 USA. [Kaye, Jack A.] NASA, Div Earth Sci, Washington, DC 20546 USA. [McCarren, David H.] Naval Meteorol & Oceanog Command, Silver Spring, MD USA. [McLean, Craig N.] NOAA, Off Ocean & Atmospher Res, Silver Spring, MD USA. [Sandgathe, Scott A.] Univ Washington, Appl Phys Lab, Seattle, WA 98105 USA. [Toepfer, Frederick] NOAA, Natl Weather Serv, Off Sci Technol Integrat, Silver Spring, MD 20910 USA. [Uccellini, Louis W.] NOAA, Natl Weather Serv, Silver Spring, MD 20910 USA. RP Sandgathe, SA (reprint author), Univ Washington, Appl Phys Lab, Seattle, WA 98105 USA. EM sandgathe@apl.washington.edu NR 27 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD FEB PY 2017 VL 98 IS 2 BP 239 EP 252 DI 10.1175/BAMS-D-16-0002.1 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EN2GA UT WOS:000395826700007 ER PT J AU Wu, DL Baum, BA Choi, YS Foster, MJ Karlsslsslsson, KG Heidinger, A Poulslsen, C Pavolonis, M Riedi, J Roebeling, R Sherwood, S Thossss, A Watts, P AF Wu, Dong L. Baum, Bryan A. Choi, Yong-Sang Foster, Michael J. Karlsslsslsson, Karl-Goran Heidinger, Andrew Poulslsen, Caroline Pavolonis, Michael Riedi, Jerome Roebeling, Robert Sherwood, Steven Thossss, Anke Watts, Philip TI TOWARD GLOBAL HARMONIZATION OF DERIVED CLOUD PRODUCTS SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Editorial Material C1 [Wu, Dong L.] NASA, Goddard Space Flight Ctr, CRL, Greenbelt, MD 20771 USA. [Baum, Bryan A.; Foster, Michael J.] Univ Wisconsin, SSEC, Madison, WI USA. [Choi, Yong-Sang] Ewha Womans Univ, DESE, Seoul, South Korea. [Karlsslsslsson, Karl-Goran; Thossss, Anke] Swedish Meteorol & Hydrol Inst, Norrkoping, Sweden. [Heidinger, Andrew; Pavolonis, Michael] NOAA, Ctr Satellite Applicat & Res, NESDIS, Madison, WI USA. [Poulslsen, Caroline] Rutherford Appleton Lab, STFC, Harwell, Berks, England. [Riedi, Jerome] Univ Lille, LOA, Villeneuve Dascq, France. [Roebeling, Robert; Watts, Philip] EUMETSAT, Darmstadt, Germany. [Sherwood, Steven] Univ New South Wales, CCRC, Sydney, NSW, Australia. RP Wu, DL (reprint author), NASA, Goddard Space Flight Ctr, CRL, Greenbelt, MD 20771 USA. EM dong.l.wu@nasa.gov RI Baum, Bryan/B-7670-2011 OI Baum, Bryan/0000-0002-7193-2767 FU KMA; EUMETSAT; University of Lille FX The comparison and evaluation of cloud retrievals, done as preparatory work to this workshop, was performed by the Center for Satellite Applications and Research, NOAA/NESDIS, and by Ewha Womans University, Seoul, South Korea, under the Cloud Algorithm Development project funded by KMA. Financial and organizational contributions for this workshop were made by EUMETSAT and the University of Lille NR 3 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD FEB PY 2017 VL 98 IS 2 BP ES49 EP ES52 DI 10.1175/BAMS-D-16-0234.1 PG 4 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EN2GA UT WOS:000395826700001 ER PT J AU Marchione, D Izquierdo, MA Bistoni, G Havenith, RWA Macchioni, A Zuccaccia, D Tarantelli, F Belpassi, L AF Marchione, Demian Izquierdo, Maria A. Bistoni, Giovanni Havenith, Remco W. A. Macchioni, Alceo Zuccaccia, Daniele Tarantelli, Francesco Belpassi, Leonardo TI C-13 NMR Spectroscopy of N-Heterocyclic Carbenes Can Selectively Probe sigma Donation in Gold(I) Complexes SO CHEMISTRY-A EUROPEAN JOURNAL LA English DT Article DE bond theory; gold; N-heterocyclic carbenes; NMR spectroscopy ID TRANSITION-METAL-COMPLEXES; DENSITY-FUNCTIONAL THEORY; ELECTROCHEMICAL PARAMETRIZATION; CHEMICAL-SHIFTS; BACK-DONATION; LIGAND; BOND; CATALYSIS; APPROXIMATION; CHARACTER AB The Dewar-Chatt-Duncanson (DCD) model provides a successful theoretical framework to describe the nature of the chemical bond in transition-metal compounds and is especially useful in structural chemistry and catalysis. However, how to actually measure its constituents (substrate- to-metal donation and metal-to-substrate back-donation) is yet uncertain. Recently, we demonstrated that the DCD components can be neatly disentangled and the pi back-donation component put in strict correlation with some experimental observables. In the present work we make a further crucial step forward, showing that, in a large set of charged and neutral N-heterocyclic carbene complexes of gold(I), a specific component of the NMR chemical shift tensor of the carbenic carbon provides a selective measure of the sigma donation. This work opens the possibility of 1) to characterize unambiguously the electronic structure of a metal fragment (LAu(In+/0 in this case) by actually measuring its sigma-withdrawing ability, 2) to quickly establish a comparative trend for the ligand trans effect, and 3) to achieve a more rigorous control of the ligand electronic effect, which is a key aspect for the design of new catalysts and metal complexes. C1 [Marchione, Demian] CALTECH, Jet Prop Lab, Div Sci, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Izquierdo, Maria A.; Havenith, Remco W. A.] Univ Groningen, Theoret Chem, Zernike Inst Adv Mat, Groningen, Netherlands. [Izquierdo, Maria A.] Vrije Univ, Software Chem & Mat, Theoret Chem, De Boelelaan 1083, NL-1081 HV Amsterdam, Netherlands. [Bistoni, Giovanni] Max Planck Inst Chem Energy Convers, Stiftstr 34-36, D-45470 Mulheim, Germany. [Havenith, Remco W. A.] Univ Groningen, Stratingh Inst Chem, Nijenborgh 4, NL-9747 AG Groningen, Netherlands. [Havenith, Remco W. A.] Univ Ghent, Dept Inorgan & Phys Chem, Krijgslaan 281 S3, B-9000 Ghent, Belgium. [Macchioni, Alceo; Tarantelli, Francesco] Univ Perugia, Dipartimento Chim Biol & Biotecnol, Perugia, Italy. [Zuccaccia, Daniele] Univ Udine, Sez Chim, Dipartimento Sci Agroalimentari Ambientali & Anim, Udine, Italy. [Tarantelli, Francesco; Belpassi, Leonardo] CNR, ISTM, Via Elce di Sotto 8, I-06123 Perugia, Italy. RP Tarantelli, F (reprint author), Univ Perugia, Dipartimento Chim Biol & Biotecnol, Perugia, Italy.; Tarantelli, F; Belpassi, L (reprint author), CNR, ISTM, Via Elce di Sotto 8, I-06123 Perugia, Italy. EM francesco.tarantelli@unipg.it; leonardo.belpassi@cnr.it FU MIUR (Rome, Italy); "FIRB-Futuro in ricerca" [RBFR1022UQ] FX We gratefully acknowledge financial support from the MIUR (Rome, Italy), "FIRB-Futuro in ricerca" (RBFR1022UQ). D.M. clarifies that his contribution to this work has been done as a private venture and not in the author's capacity as an affiliate of the Jet Propulsion Laboratory, California Institute of Technology. NR 61 TC 0 Z9 0 U1 0 U2 0 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0947-6539 EI 1521-3765 J9 CHEM-EUR J JI Chem.-Eur. J. PD FEB PY 2017 VL 23 IS 11 BP 2722 EP 2728 DI 10.1002/chem.201605502 PG 7 WC Chemistry, Multidisciplinary SC Chemistry GA EN1MF UT WOS:000395773600030 PM 27943454 ER PT J AU Bellan, J AF Bellan, Josette TI Direct numerical simulation of a high-pressure turbulent reacting temporal mixing layer SO COMBUSTION AND FLAME LA English DT Article DE High-pressure combustion; Uphill diffusion during high-pressure combustion; Flame index at high pressure; Direct numerical simulation ID MASS DIFFUSION-COEFFICIENTS; SPINODAL DECOMPOSITION; SUPERCRITICAL FLUIDS; HEAT-TRANSFER; A-PRIORI; AUTOIGNITION; FLAMES; FLOWS; COMBUSTION; IGNITION AB Direct Numerical Simulation realizations were created of a temporal mixing layer in which combustion occurs under high-pressure (high-p) turbulent conditions. The model combines the formulation of Masi, et al. (2013) for describing multi-species mixing under high-p conditions and a single-step chemical reaction of rate consistent with ignition prediction (Borghesi, and Bellan, 2015). In each simulation the computations are pursued past a time at which a maximum average-volumetric p is attained; most analysis is performed at this time, t(pp)(*). The ensemble of realizations explores the effect of the initial Reynolds number, Re-0, of the initial pressure, p(0), and of the initial composition of the two mixing-layer streams. The results show that the thermodynamic energy added by the reaction at the small scales is partially dissipated and partially backscattered. The formation of turbulent small scales is initiated by the morphological changes in the flow through stretching and twisting rather than vice versa. The reaction establishes primarily in the oxidizer stream and is preponderantly of diffusion type. Overwhelmingly, the higher reaction rates occur in the diffusion flame, particularly in regions of high density-gradient magnitude. At higher po the reaction rate reaches higher values and occurs in regions of higher density gradients. The range of reaction rates is independent of the Re-0 value but the magnitude of the density gradients increases with Re-0. When H2O and CO2 are initially present, uphill diffusion dominates over regular diffusion and occurs in regions of smaller density-gradient magnitude whereas regular diffusion occurs in regions of larger density-gradient magnitude where the reaction is more vigorous. H2O is more prone than CO2 to regular diffusion in the larger density-gradient magnitude regions. When H2O and CO2 only form in the flame, both H2O and CO2 are subject to regular diffusion over the entire range of density-gradient values. The dissipation probability density function is a log normal distribution at large dissipation values. (C) 2016 The Combustion Institute. Published by Elsevier Inc. All rights reserved. C1 [Bellan, Josette] CALTECH, Pasadena, CA 91125 USA. [Bellan, Josette] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Bellan, J (reprint author), CALTECH, Pasadena, CA 91125 USA. EM Josette.Bellan@jpl.nasa.gov FU Department of Energy (DOE), Basic Energy Sciences (BES) [02-GR-ER16107-14-00] FX This work was conducted at the Jet Propulsion Laboratory (JPL) of the California Institute of Technology (Caltech) and sponsored by the Department of Energy (DOE) 02-GR-ER16107-14-00, Basic Energy Sciences (BES) under the direction of Drs. Wade Sisk and Mark Pendersen. The contributions of Dr. Giulio Borghesi and Dr. Kenneth G. Harstad are acknowledged. The computational resources were provided by the NASA Advanced Supercomputing at Ames Research Center under the Aeronautics Research Mission Directorate program (Drs. Jeff Moder and Michael Rogers) and by National Energy Research Supercomputing Center of the Department of Energy. NR 50 TC 0 Z9 0 U1 0 U2 0 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 FEB PY 2017 VL 176 BP 245 EP 262 DI 10.1016/j.combustflame.2016.09.026 PG 18 WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary; Engineering, Chemical; Engineering, Mechanical SC Thermodynamics; Energy & Fuels; Engineering GA EM7ND UT WOS:000395497700023 ER PT J AU Breininger, DR Breininger, RD Hall, CR AF Breininger, David R. Breininger, Robert D. Hall, Carlton R. TI Effects of surrounding land use and water depth on seagrass dynamics relative to a catastrophic algal bloom SO CONSERVATION BIOLOGY LA English DT Article DE habitat dynamics; Indian River Lagoon; mapping; multistate models; transition probabilities; tropical storms ID INDIAN-RIVER-LAGOON; TRANSITION-PROBABILITIES; HALODULE-WRIGHTII; LIGHT ATTENUATION; COASTAL LAGOONS; LAGUNA MADRE; FLORIDA; QUALITY; MODELS; RESTORATION AB Seagrasses are the foundation of many coastal ecosystems and are in global decline because of anthropogenic impacts. For the Indian River Lagoon (Florida, U.S.A.), we developed competing multistate statistical models to quantify how environmental factors (surrounding land use, water depth, and time [year]) influenced the variability of seagrass state dynamics from 2003 to 2014 while accounting for time-specific detection probabilities that quantified our ability to determine seagrass state at particular locations and times. We classified seagrass states (presence or absence) at 764 points with geographic information system maps for years when seagrass maps were available and with aerial photographs when seagrass maps were not available. We used 4 categories (all conservation, mostly conservation, mostly urban, urban) to describe surrounding land use within sections of lagoonal waters, usually demarcated by land features that constricted these waters. The best models predicted that surrounding land use, depth, and year would affect transition and detection probabilities. Sections of the lagoon bordered by urban areas had the least stable seagrass beds and lowest detection probabilities, especially after a catastrophic seagrass die-off linked to an algal bloom. Sections of the lagoon bordered by conservation lands had the most stable seagrass beds, which supports watershed conservation efforts. Our results show that a multistate approach can empirically estimate state-transition probabilities as functions of environmental factors while accounting for state-dependent differences in seagrass detection probabilities as part of the overall statistical inference procedure. C1 [Breininger, David R.; Hall, Carlton R.] NASA, Ecol Program, IMSS 300, Kennedy Space Ctr, FL 32899 USA. [Breininger, Robert D.] Florida Inst Technol, Biol Sci, 150 W Univ Blvd, Melbourne, FL 32901 USA. RP Breininger, DR (reprint author), NASA, Ecol Program, IMSS 300, Kennedy Space Ctr, FL 32899 USA. EM david.r.breininger@nasa.gov NR 64 TC 0 Z9 0 U1 0 U2 0 PU WILEY PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 EI 1523-1739 J9 CONSERV BIOL JI Conserv. Biol. PD FEB PY 2017 VL 31 IS 1 BP 67 EP 75 DI 10.1111/cobi.12791 PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA EL2CQ UT WOS:000394428100008 PM 27346673 ER PT J AU Nowicki, SF Evans, LG Starr, RD Schweitzer, JS Karunatillake, S McClanahan, TP Moersch, JE Parsons, AM Tate, CG AF Nowicki, Suzanne F. Evans, Larry G. Starr, Richard D. Schweitzer, Jeffrey S. Karunatillake, Suniti McClanahan, Timothy P. Moersch, Jeffrey E. Parsons, Ann M. Tate, Christopher G. TI Modeled Martian subsurface elemental composition measurements with the Probing In situ with Neutron and Gamma ray instrument SO EARTH AND SPACE SCIENCE LA English DT Article ID DYNAMIC ALBEDO; MARS; CHEMISTRY AB The Probing In situ with Neutron and Gamma ray (PING) instrument is an innovative application of active neutron-induced gamma ray technology. The objective of PING is to measure the elemental composition of the Martian regolith. This manuscript presents PING's sensitivities as a function of the Martian regolith depth and PING's uncertainties in the measurements as a function of observation time in passive and active mode. The modeled sensitivities show that in PING's active mode, where both a pulsed neutron generator (PNG) and a gamma ray spectrometer (GRS) are used, PING can interrogate the material below the rover to about 20cm due to the penetrating nature of the high-energy neutrons and the resulting secondary gamma rays observed with the GRS. PING is capable of identifying most major and minor rock-forming elements, including H, O, Na, Mn, Mg, Al, Si, P, S, Cl, Cr, K, Ca, Ti, Fe, and Th. The modeled uncertainties show that PING's use of a PNG reduces the required observation times by an order of magnitude over a passive operating mode where the PNG is turned off. While the active mode allows for more complete elemental inventories with higher sensitivity, the gamma ray signatures of some elements are strong enough to detect in passive mode. We show that PING can detect changes in key marker elements and make thermal neutron measurements in about 1min that are sensitive to H and Cl. C1 [Nowicki, Suzanne F.] Los Alamos Natl Lab, Los Alamos, NM 87544 USA. [Evans, Larry G.] Comp Sci Corp, Lanham, MD USA. [Starr, Richard D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Schweitzer, Jeffrey S.] Univ Connecticut, Dept Phys, Storrs, CT USA. [Karunatillake, Suniti] Louisiana State Univ, Dept Geol & Geophys, Baton Rouge, LA 70803 USA. [Karunatillake, Suniti] A&MC, Baton Rouge, LA USA. [McClanahan, Timothy P.; Parsons, Ann M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Moersch, Jeffrey E.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN USA. [Tate, Christopher G.] Univ Tennessee, Dept Phys & Astron, Knoxville, TN 37996 USA. RP Nowicki, SF (reprint author), Los Alamos Natl Lab, Los Alamos, NM 87544 USA. EM snowicki@lanl.gov FU NASA/GSFC; NASA/JPL FX Funding for this work was provided by NASA/GSFC and NASA/JPL. NR 29 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2333-5084 J9 EARTH SPACE SCI JI Earth Space Sci. PD FEB PY 2017 VL 4 IS 2 BP 76 EP 90 DI 10.1002/2016EA000162 PG 15 WC Geosciences, Multidisciplinary SC Geology GA EN5CD UT WOS:000396022300002 ER PT J AU Timms, NE Erickson, TM Pearce, MA Cavosie, AJ Schmieder, M Tohver, E Reddy, SM Zanetti, MR Nemchin, AA Wittmann, A AF Timms, Nicholas E. Erickson, Timmons M. Pearce, Mark A. Cavosie, Aaron J. Schmieder, Martin Tohver, Eric Reddy, Steven M. Zanetti, Michael R. Nemchin, Alexander A. Wittmann, Axel TI A pressure-temperature phase diagram for zircon at extreme conditions SO EARTH-SCIENCE REVIEWS LA English DT Review DE Zircon; Reidite; Dissociation; EBSD; Granular texture; Shock; Impact; Zirconia; Phase heritage ID ELECTRON BACKSCATTER DIFFRACTION; SHOCK-METAMORPHOSED ZIRCONS; CRYSTAL-PLASTIC DEFORMATION; VREDEFORT IMPACT STRUCTURE; ATOM-PROBE TOMOGRAPHY; U-PB DATA; SOUTH-AFRICA; ISOTOPE SYSTEMATICS; RAMAN-SPECTROSCOPY; LUNAR ZIRCON AB Hypervelocity impact processes are uniquely capable of generating shock metamorphism, which causes mineralogical transformations and deformation that register pressure (P) and temperature (T) conditions far beyond even the most extreme conditions created by terrestrial tectonics. The mineral zircon (ZrSiO4) responds to shock deformation in various ways, including crystal-plasticity, twinning, polymorphism (e.g., transformation to the isochemical mineral reidite), formation of granular texture, and dissociation to ZrO2 + SiO2, which provide robust thermobarometers that record different extreme conditions. The importance of understanding these material processes is two-fold. First, these processes can mobilize and redistribute trace elements, and thus be accompanied by variable degrees of resetting of the U-Pb system, which is significant for the use of zircon as a geochronometer. Second, some features described herein form exclusively during shock events and are diagnostic criteria that can be used to confirm the hypervelocity origin of suspected impact structures. We present new P-T diagrams showing the phase relations of ZrSiO4 polymorphs and associated dissociation products under extreme conditions using available empirical and theoretical constraints. We present case studies to illustrate zircon microstructures formed in extreme environments, and present electron backscatter diffraction data for grains from three impact structures (Mistastin Lake of Canada, Ries of Germany, and Acraman of Australia) that preserve different minerals and microstructures associated with different shock conditions. For each locality, we demonstrate how systematic crystallographic orientation relationships within and between minerals can be used in conjunction with the new phase diagrams to constrain the P-T history. We outline a conceptual framework for a zircon-based approach to 'extreme thermobarometry' that incorporates both direct observation of high-P and high-T phases, as well as inferences for the former existence of phases from orientation relationships in recrystallised products, a concept we refer to here as 'phase heritage'. This new approach can be used to unravel the pressure-temperature history of zircon-bearing samples that have experienced extreme conditions, such as rocks that originated in the Earth's mantle, and those shocked during impact events on Earth and other planetary bodies. (C) 2016 Elsevier B.V. All rights reserved. C1 [Timms, Nicholas E.; Erickson, Timmons M.; Cavosie, Aaron J.; Reddy, Steven M.; Nemchin, Alexander A.] Curtin Univ, Inst Geosci Res TIGeR, Dept Appl Geol, GPO Box U1987, Perth, WA 6845, Australia. [Timms, Nicholas E.; Erickson, Timmons M.; Cavosie, Aaron J.; Schmieder, Martin; Reddy, Steven M.; Nemchin, Alexander A.] NASA, Solar Syst Explorat Res Virtual Inst SSERVI, Canberra, ACT, Australia. [Pearce, Mark A.] CSIRO Mineral Resources, Australian Resources Res Ctr, 26 Dick Perry Ave, Kensington, WA 6151, Australia. [Cavosie, Aaron J.] Univ Wisconsin Madison, NASA, Astrobiol Inst, Dept Geosci, Madison, WI 53706 USA. [Schmieder, Martin] Lunar & Planetary Inst, 3303 NASA Rd 1, Houston, TX 77058 USA. [Schmieder, Martin; Tohver, Eric] Univ Western Australia, Sch Earth & Environm, 35 Stirling Highway, Crawley, WA 6009, Australia. [Zanetti, Michael R.] Univ Western Ontario, 1151 Richmond St, London, ON N6A 5B7, Canada. [Wittmann, Axel] Arizona State Univ, Tempe, AZ 85287 USA. RP Timms, NE (reprint author), Curtin Univ, Inst Geosci Res TIGeR, Dept Appl Geol, GPO Box U1987, Perth, WA 6845, Australia.; Timms, NE (reprint author), NASA, Solar Syst Explorat Res Virtual Inst SSERVI, Canberra, ACT, Australia. EM n.timms@curtin.edu.au FU Barringer Family Award for Impact Cratering Research; Mineralogical Society of America Grant for Student Research in Mineralogy and Petrology; Eugene M. Shoemaker Award for Impact Crater Research; Meteoritical Society Travel Grant (NASA Cosmochemistry Program); National Science Foundation [EAR-1145118]; NASA Astrobiology Program; Curtin Research Fellowship; Curtin International Postgraduate Scholarship; Australian Research Council [DP0988190] FX M. Zanetti acknowledges support from a Barringer Family Award for Impact Cratering Research, the Mineralogical Society of America Grant for Student Research in Mineralogy and Petrology, and the Eugene M. Shoemaker Award for Impact Crater Research, and a Meteoritical Society Travel Grant (NASA Cosmochemistry Program). A. Cavosie acknowledges support from the National Science Foundation (EAR-1145118), the NASA Astrobiology Program, and a Curtin Research Fellowship. T. Erickson acknowledges a Curtin International Postgraduate Scholarship. E. Tohver acknowledges support from the Australian Research Council (DP0988190). Thorsten Geisler and ZERIN (Centre for Ries Crater and Impact Research in Nordlingen) are thanked for the acquisition of the sample from the Ries crater. We thank Sandy Morris, Yardea Station, for his kind support and granting E. Tohver and M. Schmieder access to the Acraman impact structure on his private land. We acknowledge technical support from the Microscopy and Microanalysis Facility at Curtin. Two anonymous reviewers are acknowledged for their constructive reviews of the manuscript, and A. Gomez-Tuena is thanked for editorial handling. This is LPI Contribution no. 1994. NR 186 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-8252 EI 1872-6828 J9 EARTH-SCI REV JI Earth-Sci. Rev. PD FEB PY 2017 VL 165 BP 185 EP 202 DI 10.1016/j.earscirev.2016.12.008 PG 18 WC Geosciences, Multidisciplinary SC Geology GA EL1QJ UT WOS:000394395800007 ER PT J AU Goordial, J Davila, A Greer, CW Cannam, R DiRuggiero, J Mckay, CP Whyte, LG AF Goordial, Jacqueline Davila, Alfonso Greer, Charles W. Cannam, Rebecca DiRuggiero, Jocelyne McKay, Christopher P. Whyte, Lyle G. TI Comparative activity and functional ecology of permafrost soils and lithic niches in a hyper-arid polar desert SO ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID MCMURDO DRY VALLEYS; ANTARCTIC COLD DESERT; MICROBIAL DIVERSITY; ENDOLITHIC MICROORGANISMS; SUBZERO TEMPERATURES; MINERAL SOILS; COMMUNITIES; GENOME; BACTERIA; MARS AB Permafrost in the high elevation McMurdo Dry Valleys of Antarctica ranks among the driest and coldest on Earth. Permafrost soils appear to be largely inhospitable to active microbial life, but sandstone lithic microhabitats contain a trophically simple but functional cryptoendolithic community. We used metagenomic sequencing and activity assays to examine the functional capacity of permafrost soils and cryptoendolithic communities in University Valley, one of the most extreme regions in the Dry Valleys. We found metagenomic evidence that cryptoendolithic microorganisms are adapted to the harsh environment and capable of metabolic activity at in situ temperatures, possessing a suite of stress response and nutrient cycling genes to fix carbon under the fluctuating conditions that the sandstone rock would experience during the summer months. We additionally identified genes involved in microbial competition and cooperation within the cryptoendolithic habitat. In contrast, permafrost soils have a lower richness of stress response genes, and instead the metagenome is enriched in genes involved with dormancy and sporulation. The permafrost soils also have a large presence of phage genes and genes involved in the recycling of cellular material. Our results underlie two different habitability conditions under extreme cold and dryness: the permafrost soil which is enriched in traits which emphasize survival and dormancy, rather than growth and activity; and the cryptoendolithic environment that selects for organisms capable of growth under extremely oligotrophic, arid and cold conditions. This study represents the first metagenomic interrogation of Antarctic permafrost and polar cryptoendolithic microbial communities. C1 [Goordial, Jacqueline; Cannam, Rebecca; Whyte, Lyle G.] McGill Univ, Macdonald Campus, Bellevue, WA USA. [Davila, Alfonso; McKay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA USA. [Greer, Charles W.] Natl Res Council Canada, Montreal, PQ, Canada. [DiRuggiero, Jocelyne] Johns Hopkins Univ, Baltimore, MD USA. RP Goordial, J (reprint author), McGill Univ, Macdonald Campus, Bellevue, WA USA. EM Jacqueline.goordial@mail.mcgill.ca FU NASA's ASTEP program; Natural Sciences and Engineering Research Council (NSERC) Discovery Grant Program; NSERC Northern Supplements Program; NSERC CREATE Canadian Astrobiology Training Program (CATP); NASA [NNX15AP18G]; National Science foundation [NSF-1556574]; NCBI Sequence Read Archive (SRA) [PRJNA290089] FX This work was supported by NASA's ASTEP program and with field support via NSF/OPP (project B-302-M). Support was provided by the Natural Sciences and Engineering Research Council (NSERC) Discovery Grant Program, NSERC Northern Supplements Program, and NSERC CREATE Canadian Astrobiology Training Program (CATP). Additionally, this work was supported by grant NNX15AP18G from NASA and grant NSF-1556574 from the National Science foundation to JDR. Metagenomic datasets are publically available at MG-RAST (4594281.3, 4594282). Pyrosequencing data has been deposited in the NCBI Sequence Read Archive (SRA) under project PRJNA290089. NR 63 TC 0 Z9 0 U1 1 U2 1 PU WILEY PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1462-2912 EI 1462-2920 J9 ENVIRON MICROBIOL JI Environ. Microbiol. PD FEB PY 2017 VL 19 IS 2 BP 443 EP 458 DI 10.1111/1462-2920.13353 PG 16 WC Microbiology SC Microbiology GA EL9XI UT WOS:000394973000009 PM 27129741 ER PT J AU Stevenson, A Hamill, PG O'Kane, CJ Kminek, G Rummel, JD Voytek, MA Dijksterhuis, J Hallsworth, JE AF Stevenson, Andrew Hamill, Philip G. O'Kane, Callum J. Kminek, Gerhard Rummel, John D. Voytek, Mary A. Dijksterhuis, Jan Hallsworth, John E. TI Aspergillus penicillioides differentiation and cell division at 0.585 water activity SO ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID TREHALOSE-BASED OLIGOSACCHARIDES; ENVIRONMENTAL-CONDITIONS; CONIDIAL GERMINATION; COMPATIBLE SOLUTES; DORMANT CONIDIA; GLYCEROL UPTAKE; FUNGI; STRESS; CHAOTROPICITY; GROWTH AB Water availability acts as the most stringent constraint for life on Earth. Thus, understanding the water relations of microbial extremophiles is imperative to our ability to increase agricultural productivity (e.g., by enhancing the processing and turnover of dead organic matter in soils of arid regions), reduce human exposure to mycotoxins in buildings and our food-supply chain, prevent the spoilage of foods/animal feeds, books, museum specimens and artworks and better control microbiology of industrial fermentations. Only a small number of microbial systems can retain activity at <0.710 water activity (ISME J 2015 9: 1333-1351). It has long-been considered that the most resilient of these is Xeromyces bisporus, which inhabits sugar-rich substrates (Appl Environ Microbiol 1968 16: 1853-1858). The current study focused on germination of Aspergillus penicillioides, a xerophile which is also able to grow under low humidity and saline conditions. Investigations of germination differed from those reported earlier: firstly, aerially borne conidia were harvested, and then used for inoculations, in their dry condition; secondly, cultures were incubated at 24 degrees C, i.e. below optimum germination temperature, to minimize the possibility of water loss from the substrate; thirdly, cultures remained sealed throughout the 73-day study period (microscopic examination was carried out directly 48 through the Petri plate lid); fourthly, the germination parameters determined were: rates and extent of conidial swelling, production of differentiated germination-structures and septate germlings, and subsequent development of mycelium and/or sporulation; fifthly, assessments were carried out over a range of water-activity values and time points to obtain a complete profile of the germination process. Conidia swelled, formed differentiated germination-structures and then produced septate germlings at a water-activity of just 0.585 (58.5% relative humidity), outside the currently understood thermodynamic window for life. Furthermore, analyses of these data suggest a theoretical water-activity minimum of 0.565 for germination of A. penicilliodes. In relation to astrobiology, these findings have an application in understanding the limits to life in extraterrestrial environments. In light of current plans for exploration missions to Mars and other places, and the need to safeguard martian scientific sites and potential resources (including water) for future human habitation, a knowledge-based and effective policy for planetary protection is essential. As it is, Mars-bound spacecraft may frequently be contaminated with aspergilli (including A. penicillioides) and other organisms which, when transported to other planetary bodies, pose a contamination risk. In crafting countermeasures to offset this, it is important to know as precisely as possible the capabilities of these potential interplanetary visitors. C1 [Stevenson, Andrew; Hamill, Philip G.; O'Kane, Callum J.; Hallsworth, John E.] Queens Univ Belfast, MBC, Sch Biol Sci, Institute Global Food Secur, Belfast BT9 7BL, Antrim, North Ireland. [Kminek, Gerhard] European Space Agcy, Independent Safety Off, NL-2200 AG Noordwijk, Netherlands. [Rummel, John D.] SETI Inst, Mountain View, CA 94043 USA. [Voytek, Mary A.] NASA Headquarters, Washington, DC 20546 USA. [Dijksterhuis, Jan] CBS, KNAW Fungal Biodivers Ctr, Uppsalalaan 8, NL-3584 CT Utrecht, CT, Netherlands. RP Hallsworth, JE (reprint author), Queens Univ Belfast, MBC, Sch Biol Sci, Institute Global Food Secur, Belfast BT9 7BL, Antrim, North Ireland. EM j.hallsworth@qub.ac.uk RI Hallsworth, John/K-7876-2013 FU Department of Agriculture, Environment and Rural Affairs (DAERA, Northern Ireland); Biotechnology and Biological Sciences Research Council (BBSRC, United Kingdom) [BBF003471] FX This article is based on work funded by the Department of Agriculture, Environment and Rural Affairs (DAERA, Northern Ireland) who supported A. Stevenson and P.G. Hamill and Biotechnology and Biological Sciences Research Council (BBSRC, United Kingdom) project BBF003471. We would like to thank D. Blain (Queen's University Belfast) for the technical assistance provided. NR 69 TC 1 Z9 1 U1 0 U2 0 PU WILEY PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1462-2912 EI 1462-2920 J9 ENVIRON MICROBIOL JI Environ. Microbiol. PD FEB PY 2017 VL 19 IS 2 BP 687 EP 697 DI 10.1111/1462-2920.13597 PG 11 WC Microbiology SC Microbiology GA EL9XI UT WOS:000394973000026 PM 27871132 ER PT J AU Seekell, D Carr, J Dell'Angelo, J D'Odorico, P Fader, M Gephart, J Kummu, M Magliocca, N Porkka, M Puma, M Ratajczak, Z Rulli, MC Suweis, S Tavoni, A AF Seekell, David Carr, Joel Dell'Angelo, Jampel D'Odorico, Paolo Fader, Marianela Gephart, Jessica Kummu, Matti Magliocca, Nicholas Porkka, Miina Puma, Michael Ratajczak, Zak Rulli, Maria Cristina Suweis, Samir Tavoni, Alessandro TI Resilience in the global food system SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Letter DE food security; resilience; food systems; food production; sustainability ID SOCIAL-ECOLOGICAL SYSTEMS; EARLY-WARNING SIGNALS; CLIMATE-CHANGE; SECURITY; VULNERABILITY; INSECURITY; TRADE; TRANSFORMABILITY; ADAPTABILITY; BIODIVERSITY AB Ensuring food security requires food production and distribution systems function throughout disruptions. Understanding the factors that contribute to the global food system's ability to respond and adapt to such disruptions (i.e. resilience) is critical for understanding the long-term sustainability of human populations. Variable impacts of production shocks on food supply between countries indicate a need for national-scale resilience indicators that can provide global comparisons. However, methods for tracking changes in resilience have had limited application to food systems. We developed an indicator-based analysis of food systems resilience for the years 1992-2011. Our approach is based on three dimensions of resilience: socio-economic access to food in terms of income of the poorest quintile relative to food prices, biophysical capacity to intensify or extensify food production, and the magnitude and diversity of current domestic food production. The socio-economic indicator has a large variability, but with low values concentrated in Africa and Asia. The biophysical capacity indicator is highest in Africa and Eastern Europe, in part because of a high potential for extensification of cropland and for yield gap closure in cultivated areas. However, the biophysical capacity indicator has declined globally in recent years. The production diversity indicator has increased slightly, with a relatively even geographic distribution. Few countries had exclusively high or low values for all indicators. Collectively, these results are the basis for global comparisons of resilience between countries, and provide necessary context for developing generalizations about resilience in the global food system. C1 [Seekell, David] Umea Univ, Dept Ecol & Environm Sci, Umea, Sweden. [Carr, Joel; D'Odorico, Paolo; Gephart, Jessica; Ratajczak, Zak] Univ Virginia, Dept Environm Sci, Clark Hall, Charlottesville, VA 22903 USA. [Dell'Angelo, Jampel; Magliocca, Nicholas] Vrije Univ Amsterdam, Inst Environm Studies IVM, Amsterdam, Netherlands. [Dell'Angelo, Jampel] Univ Maryland, Natl Ctr Socioenvironm Synth, Annapolis, MD USA. [Fader, Marianela] Fed Inst Hydrol, Int Ctr Water Resources & Global Change, UNESCO, Koblenz, Germany. [Kummu, Matti; Porkka, Miina] Aalto Univ, Water & Dev Res Grp, Aalto, Finland. [Puma, Michael] Columbia Univ, NASA, Goddard Inst Space Studies, Ctr Climate Syst Res, New York, NY USA. [Puma, Michael] Columbia Univ, NASA, Ctr Climate & Life, Goddard Inst Space Studies, New York, NY USA. [Rulli, Maria Cristina] Politecn Milan, Dipartimento Ingn Civile & Ambientale, Milan, Italy. [Suweis, Samir] Univ Padua, Dept Phys & Astron, Padua, Italy. [Tavoni, Alessandro] London Sch Econ, Grantham Inst Climate Change & Environm, London, England. RP Seekell, D (reprint author), Umea Univ, Dept Ecol & Environm Sci, Umea, Sweden. EM david.seekell@emg.umu.se OI Kummu, Matti/0000-0001-5096-0163 FU National Socio-Environmental Synthesis Center (SESYNC); National Science Foundation [DBI-1052875, DBI 1402033]; LabexOT-Med [ANR-11-LABX-0061]; French Government <> program of the French National Research Agency (ANR) through the A*MIDEX project [ANR-11IDEX-0001-02]; European Union's Seventh Framework Programme for research, technological development and demonstration under the project LUC4C [603542]; Academy of Finland SRC project Winland; Academy of Finland project SCART; Columbia University Center for Climate and Life; Interdisciplinary Global Change Research under NASA cooperative [NNX14AB99A]; NASA Climate and Earth Observing Program; Centre for Climate Change Economics and Policy-ESRC; Grantham Foundation for the Protection of the Environment FX This paper is based on research supported by the National Socio-Environmental Synthesis Center (SESYNC) with funding received from the National Science Foundation DBI-1052875. M Fader received additional support from the LabexOT-Med (no ANR-11-LABX-0061) funded by the French Government << Investissements d'Avenir >> program of the French National Research Agency (ANR) through the A*MIDEX project (no ANR-11IDEX-0001-02), and the European Union's Seventh Framework Programme for research, technological development and demonstration under the project LUC4C (grant agreement number 603542). M Kummu received support from the Academy of Finland SRC project Winland and Academy of Finland project SCART. Z Ratajczak received additional support from the National Science Foundation (DBI 1402033). M J Puma gratefully acknowledges support from the Columbia University Center for Climate and Life, where he is a Climate and Life Fellow, and from the Interdisciplinary Global Change Research under NASA cooperative agreement NNX14AB99A supported by the NASA Climate and Earth Observing Program. 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. We thank Christina Prell and Roberto Patricio Korzeniewicz for helpful conversations. NR 57 TC 0 Z9 0 U1 0 U2 0 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 FEB PY 2017 VL 12 IS 2 AR 025010 DI 10.1088/1748-9326/aa5730 PG 10 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA EM9LN UT WOS:000395633200001 ER PT J AU Jickells, TD Buitenhuis, E Altieri, K Baker, AR Capone, D Duce, RA Dentener, F Fennel, K Kanakidou, M LaRoche, J Lee, K Liss, P Middelburg, JJ Moore, JK Okin, G Oschlies, A Sarin, M Seitzinger, S Sharples, J Singh, A Suntharalingam, P Uematsu, M Zamora, LM AF Jickells, T. D. Buitenhuis, E. Altieri, K. Baker, A. R. Capone, D. Duce, R. A. Dentener, F. Fennel, K. Kanakidou, M. LaRoche, J. Lee, K. Liss, P. Middelburg, J. J. Moore, J. K. Okin, G. Oschlies, A. Sarin, M. Seitzinger, S. Sharples, J. Singh, A. Suntharalingam, P. Uematsu, M. Zamora, L. M. TI A reevaluation of the magnitude and impacts of anthropogenic atmospheric nitrogen inputs on the ocean SO GLOBAL BIOGEOCHEMICAL CYCLES LA English DT Article ID AMMONIA-OXIDIZING ARCHAEA; NORTH-ATLANTIC OCEAN; N P STOICHIOMETRY; N-2 FIXATION; DINITROGEN-FIXATION; DUST DEPOSITION; ORGANIC-MATTER; CARBON BUDGET; MINERAL DUST; ARABIAN SEA AB We report a new synthesis of best estimates of the inputs of fixed nitrogen to the world ocean via atmospheric deposition and compare this to fluvial inputs and dinitrogen fixation. We evaluate the scale of human perturbation of these fluxes. Fluvial inputs dominate inputs to the continental shelf, and we estimate that about 75% of this fluvial nitrogen escapes from the shelf to the open ocean. Biological dinitrogen fixation is the main external source of nitrogen to the open ocean, i.e., beyond the continental shelf. Atmospheric deposition is the primary mechanism by which land-based nitrogen inputs, and hence human perturbations of the nitrogen cycle, reach the open ocean. We estimate that anthropogenic inputs are currently leading to an increase in overall ocean carbon sequestration of similar to 0.4% (equivalent to an uptake of 0.15 Pg Cyr(-1) and less than the Duce et al. (2008) estimate). The resulting reduction in climate change forcing from this ocean CO2 uptake is offset to a small extent by an increase in ocean N2O emissions. We identify four important feedbacks in the ocean atmosphere nitrogen system that need to be better quantified to improve our understanding of the perturbation of ocean biogeochemistry by atmospheric nitrogen inputs. These feedbacks are recycling of (1) ammonia and (2) organic nitrogen from the ocean to the atmosphere and back, (3) the suppression of nitrogen fixation by increased nitrogen concentrations in surface waters from atmospheric deposition, and (4) increased loss of nitrogen from the ocean by denitrification due to increased productivity stimulated by atmospheric inputs. C1 [Jickells, T. D.; Buitenhuis, E.; Baker, A. R.; Liss, P.; Suntharalingam, P.] Univ East Anglia, Sch Environm Sci, Norwich, Norfolk, England. [Altieri, K.] Univ Cape Town, Energy Res Ctr, Cape Town, South Africa. [Capone, D.] Univ Southern Calif, Dept Biol Sci, Los Angeles, CA USA. [Duce, R. A.] Texas A&M Univ, Dept Oceanog & Atmospher Sci, College Stn, TX USA. [Dentener, F.] DG Joint Res Ctr, European Commiss, Ispra, Italy. [Fennel, K.] Dalhousie Univ, Dept Oceanog, Halifax, NS, Canada. [Kanakidou, M.] Univ Crete, Dept Chem, Iraklion, Greece. [LaRoche, J.] Dalhousie Univ, Dept Biol, Halifax, NS, Canada. [Lee, K.] Pohang Univ Sci & Technol, Sch Environm Sci & Engn, Pohang, South Korea. [Middelburg, J. J.] Univ Utrecht, Fac Geosci, Utrecht, Netherlands. [Moore, J. K.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. [Okin, G.] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA USA. [Oschlies, A.] GEOMAR, Kiel, Germany. [Sarin, M.; Singh, A.] Phys Res Lab, Geosci Div, Ahmadabad, Gujarat, India. [Seitzinger, S.] Univ Victoria, Dept Environm Studies, Victoria, BC, Canada. [Sharples, J.] Univ Liverpool, Sch Environm Sci, Liverpool, Merseyside, England. [Uematsu, M.] Univ Tokyo, Ctr Int Collaborat, Atmosphere & Ocean Res Inst, Tokyo, Japan. [Zamora, L. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Zamora, L. M.] Univ Space Res Assoc, Greenbelt, MD USA. RP Jickells, TD (reprint author), Univ East Anglia, Sch Environm Sci, Norwich, Norfolk, England. EM T.Jickells@uea.ac.uk RI Baker, Alex/D-1233-2011; OI Baker, Alex/0000-0002-8365-8953; fennel, katja/0000-0003-3170-2331 NR 108 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0886-6236 EI 1944-9224 J9 GLOBAL BIOGEOCHEM CY JI Glob. Biogeochem. Cycle PD FEB PY 2017 VL 31 IS 2 BP 289 EP 305 DI 10.1002/2016GB005586 PG 17 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA EN8GI UT WOS:000396238500006 ER PT J AU Stager, JC Cumming, BF Laird, KR Garrigan-Piela, A Pederson, N Wiltse, B Lane, CS Nester, J Ruzmaikin, A AF Stager, Jay Curt Cumming, Brian F. Laird, Kathleen R. Garrigan-Piela, Alex Pederson, Neil Wiltse, Brendan Lane, Chad S. Nester, Jessica Ruzmaikin, Alexander TI A 1600-year diatom record of hydroclimate variability from Wolf Lake, New York SO HOLOCENE LA English DT Article DE Adirondacks; diatoms; drought; hydroclimate; "Little Ice Age'; Medieval Climate Anomaly; paleolimnology ID EASTERN NORTH-AMERICA; LAST MILLENNIUM; CLIMATE-CHANGE; BOREAL LAKES; NEW-ENGLAND; ENVIRONMENTAL-CHANGE; SEDIMENT RECORDS; ADIRONDACK LAKE; ORGANIC-MATTER; DEPTH MODELS AB A high-resolution diatom record from Wolf Lake, a minimally disturbed heritage' lake, provides insights into the hydroclimatic history of the Adirondack Mountains of northern New York during the last c. 1600years. Three pronounced dry periods occurred during c. AD 490-610, 780-870, and 1010-1080, and low precipitation generally prevailed during the warm Medieval Climate Anomaly (c. AD 950-1350), a finding that fills an important gap in knowledge of the spatial extent of droughts across North America during that period. During the cooler Little Ice Age' interval (c. AD 1350-1800), inferred water balance was generally more positive. Seven peaks in charcoal abundance represent fire events during both wet and dry periods. Unusually high charcoal and inorganic sediment deposition c. AD 1700 could reflect human activity in the watershed, as might an abrupt rise in the relative abundances of planktonic and tychoplanktonic diatoms in Wolf Lake during the AD 1860s. The diatom record displays periodicities of c. 256 and 512years in addition to high-frequency fluctuations, suggesting that significant precipitation variability is likely to continue to disrupt climatic trends in this region. C1 [Stager, Jay Curt; Garrigan-Piela, Alex; Wiltse, Brendan] Paul Smiths Coll, Div Nat Sci, Paul Smiths, NY 12970 USA. [Cumming, Brian F.; Laird, Kathleen R.] Queens Univ, Dept Biol, Kingston, ON, Canada. [Pederson, Neil] Harvard Univ, Harvard Forest, Cambridge, MA 02138 USA. [Lane, Chad S.; Nester, Jessica] Univ N Carolina, Dept Geog & Geol, Wilmington, NC USA. [Ruzmaikin, Alexander] Jet Prop Lab, La Canada Flintridge, CA USA. RP Stager, JC (reprint author), Paul Smiths Coll, Div Nat Sci, Paul Smiths, NY 12970 USA. EM cstager@paulsmiths.edu FU National Science Foundation (P2C2) [1358362]; Paul Smith's College FX This project was supported by the National Science Foundation (P2C2, grant #1358362) and by Paul Smith's College. NR 78 TC 0 Z9 0 U1 0 U2 0 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0959-6836 EI 1477-0911 J9 HOLOCENE JI Holocene PD FEB PY 2017 VL 27 IS 2 BP 246 EP 257 DI 10.1177/0959683616658527 PG 12 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA EL9QO UT WOS:000394955300004 ER PT J AU Chen, F Crow, WT Colliander, A Cosh, MH Jackson, TJ Bindlish, R Reichle, RH Chan, SK Bosch, DD Starks, PJ Goodrich, DC Seyfried, MS AF Chen, Fan Crow, Wade T. Colliander, Andreas Cosh, Michael H. Jackson, Thomas J. Bindlish, Rajat Reichle, Rolf H. Chan, Steven K. Bosch, David D. Starks, Patrick J. Goodrich, David C. Seyfried, Mark S. TI Application of Triple Collocation in Ground-Based Validation of Soil Moisture Active/Passive (SMAP) Level 2 Data Products SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE Remote sensing; soil moisture; Soil Moisture Active/Passive (SMAP); triple collocation (TC) ID ERROR CHARACTERIZATION; RETRIEVAL; SCATTEROMETER; STABILITY; MISSION; ASCAT AB The validation of the soil moisture retrievals from the recently launched National Aeronautics and Space Administration (NASA) Soil Moisture Active/Passive (SMAP) satellite is important prior to their full public release. Uncertainty in attempts to characterize footprint-scale surface-layer soil moisture using point-scale ground observations has generally limited past validation of remotely sensed soil moisture products to densely instrumented sites covering an area approximating the satellite ground footprint. However, by leveraging independent soil moisture information obtained from land surface modeling and/or alternative remote sensing products, triple collocation (TC) techniques offer a strategy for characterizing upscaling errors in sparser ground measurements and removing the impact of such error on the evaluation of remotely sensed soil moisture products. Here, we propose and validate a TC-based strategy designed to utilize existing sparse soil moisture networks (typically with a single sampling point per satellite footprint) to obtain an unbiased correlation validation metric for satellite surface soil moisture retrieval products. Application of this TC strategy at five SMAP core validation sites suggests that unbiased estimates of correlation between the satellite product and the true footprint average can be obtained-even in cases where ground observations provide only one single reference point within the footprint. An example of preliminary validation results from the application of this TC strategy to the SMAP Level 2 Soil Moisture Passive (beta release version) product is presented. C1 [Chen, Fan; Bindlish, Rajat] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Crow, Wade T.; Cosh, Michael H.; Jackson, Thomas J.] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA. [Colliander, Andreas; Cosh, Michael H.] NASA, Jet Prop Lab, CALTECH, Pasadena, CA 91109 USA. [Reichle, Rolf H.] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bosch, David D.; Goodrich, David C.] ARS, Southeast Watershed Res Lab, USDA, Tifton, GA 31793 USA. [Starks, Patrick J.] ARS, Grazinglands Res Lab, USDA, El Reno, OK 73036 USA. [Seyfried, Mark S.] ARS, Northwest Watershed Res Ctr, USDA, Boise, ID 83712 USA. RP Chen, F (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA. EM fan.chen@ars.usda.gov; wade.crow@ars.usda.gov; andreas.colliander@jpl.nasa.gov; Michael.Cosh@ars.usda.gov; tom.jackson@ars.usda.gov; rajat.bindlish@ars.usda.gov; Rolf.Reichle@nasa.gov; steven.k.chan@jpl.nasa.gov; david.bosch@ars.usda.gov; patrick.starks@ars.usda.gov; dave.goodrich@ars.usda.gov; mark.seyfried@ars.usda.gov FU National Aeronautics and Space Administration, Soil Moisture Active/Passive mission FX This work was supported by the National Aeronautics and Space Administration, Soil Moisture Active/Passive mission via Wade Crow's membership on the SMAP Science Team NR 38 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 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD FEB PY 2017 VL 10 IS 2 BP 489 EP 502 DI 10.1109/JSTARS.2016.2569998 PG 14 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA EM7BO UT WOS:000395466700010 ER PT J AU Nag, S Gatebe, CK Hilker, T AF Nag, Sreeja Gatebe, Charles K. Hilker, Thomas TI Simulation of Multiangular Remote Sensing Products Using Small Satellite Formations SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE BRDF; constellations; CubeSat; multi-view measurements; NDVI ID LIGHT-USE EFFICIENCY; SPECTRAL MEASUREMENTS; SURFACE; AIRBORNE; MISSION; BRDF; MODEL; ATMOSPHERE; VEGETATION; RADIOMETER AB To completely capture the multiangular reflectance of an opaque surface, one must estimate the bidirectional reflectance distribution function (BRDF), which seeks to represent variations in surface reflectance as a function of measurement and illumination angles at any time instant. The gap in angular sampling abilities of existing single satellites in Earth observation missions can be complemented by small satellites in formation flight. The formation would have intercalibrated spectrometer payloads making reflectance measurements, at many zenith and azimuthal angles simultaneously. We use a systems engineering tool coupled with a science evaluation tool to demonstrate the performance impact and mission feasibility. Formation designs are generated and compared to each other and multisensor single spacecraft, in terms of estimation error of BRDF and its dependent products such as albedo, light use efficiency (LUE), and normalized difference vegetation index (NDVI). Performance is benchmarked with respect to data from previous airborne campaigns (NASA's Cloud Absorption Radiometer), and tower measurements (AMSPEC II), and assuming known BRDF models. Simulations show that a formation of six small satellites produces lesser average error (21.82%) than larger single spacecraft (23.2%), purely in terms of angular sampling benefits. The average monolithic albedo error of 3.6% is outperformed by a formation of three satellites (1.86%), when arranged optimally and by a formation of seven to eight satellites when arranged in any way. An eight-satellite formation reduces albedo errors to 0.67% and LUE errors from 89.77% (monolithic) to 78.69%. The average NDVI for an eight satellite, nominally maintained formation is better than the monolithic 0.038. C1 [Nag, Sreeja] NASA, Goddard Space Flight Ctr, Petaluma, CA 94952 USA. [Nag, Sreeja] Bay Area Environm Res Ctr, Petaluma, CA 94952 USA. [Gatebe, Charles K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gatebe, Charles K.] Univ Space Res Assoc, Greenbelt, MD 20771 USA. [Hilker, Thomas] Univ Southampton, Highfield Rd, Southampton SO17 1BJ, Hants, England. RP Nag, S (reprint author), NASA, Goddard Space Flight Ctr, Petaluma, CA 94952 USA.; Nag, S (reprint author), Bay Area Environm Res Ctr, Petaluma, CA 94952 USA. EM sree-janag@alum.mit.edu; charles.k.gatebe@nasa.gov; T.Hilker@soton.ac.uk FU Schlumberger Foundation's Faculty for the Future Fellowship; NASA Earth and Space Science Fellowship FX The work of S. Nag was supported by the Schlumberger Foundation's Faculty for the Future Fellowship and the NASA Earth and Space Science Fellowship. (Corresponding author: Sreeja Nag.) NR 58 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 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD FEB PY 2017 VL 10 IS 2 BP 638 EP 653 DI 10.1109/JSTARS.2016.2570683 PG 16 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA EM7BO UT WOS:000395466700023 ER PT J AU Gehrels, N Cannizzo, JK AF Gehrels, Neil Cannizzo, John K. TI Explosions throughout the universe SO INTERNATIONAL JOURNAL OF MODERN PHYSICS D LA English DT Article DE Black hole physics; radiation mechanisms; nonthermal; stars; activity; gamma-ray burst; general; stars; neutron; novae; galaxies; star formation ID GAMMA-RAY BURSTS; SAGITTARIUS-A-ASTERISK; ADVECTION-DOMINATED ACCRETION; NEUTRON-STAR MERGERS; MASSIVE BLACK-HOLE; TIDAL DISRUPTION EVENTS; X-RAY; V404 CYGNI; R-PROCESS; FORMATION HISTORY AB High energy transients make up a diverse and exotic class of objects, from terrestrial lightning gamma-ray bursts at cosmological distances. In this review, we provide a detailed look at some of the more exciting transients observed over the last few years by Swift and other high energy missions. C1 [Gehrels, Neil] NASA Goddard Space Flight Ctr, Astroparticle Phys Div, Greenbelt, MD 20771 USA. [Cannizzo, John K.] Univ Maryland Baltimore Cty, CRESST Joint Ctr Astrophys, Baltimore, MD 21250 USA. RP Gehrels, N (reprint author), NASA Goddard Space Flight Ctr, Astroparticle Phys Div, Greenbelt, MD 20771 USA. EM neil.gehrels@nasa.gov; john.k.cannizzo@nasa.gov NR 87 TC 0 Z9 0 U1 0 U2 0 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0218-2718 EI 1793-6594 J9 INT J MOD PHYS D JI Int. J. Mod. Phys. D PD FEB PY 2017 VL 26 IS 2 AR 1730003 DI 10.1142/S0218271817300038 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EM5SF UT WOS:000395372200003 ER PT J AU Swei, SSM Nguyen, NT AF Swei, Sean Shan-Min Nguyen, Nhan T. TI Adaptive Disturbance Torque Estimation for Orbiting Spacecraft Using Recursive Least-Squares Methods SO JOURNAL OF AEROSPACE INFORMATION SYSTEMS LA English DT Article ID UNKNOWN INPUTS; LINEAR-SYSTEMS; UNCERTAIN SYSTEMS; OBSERVER DESIGN; STATE AB This paper develops a novel disturbance torque estimator for an orbiting spacecraft by using the adaptive least-squares parameter estimation technique. The disturbance estimation is first formulated as an adaptive least-squares minimization problem using a set of polynomial functions and then integrated with the feedback momentum estimator. The covariance update law with a variable forgetting factor is used, and it is shown that the convergent rate for estimation errors can be made at the same level as the forgetting factor. The proposed approach is particularly suited for orbiting small or microsatellite applications, where the momentum management capacity is often limited. The onboard estimated disturbance torque input can then be used as a part of control resource for spacecraft momentum management. The simulation results demonstrate the efficacy of the proposed concept. C1 [Swei, Sean Shan-Min; Nguyen, Nhan T.] NASA, Ames Res Ctr, Intelligent 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 23 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 1940-3151 EI 2327-3097 J9 J AEROSP INFORM SYST JI J. Aerosp. Inf. Syst. PD FEB PY 2017 VL 14 IS 2 BP 92 EP 102 DI 10.2514/1.I010480 PG 11 WC Engineering, Aerospace SC Engineering GA EP3JB UT WOS:000397277500002 ER PT J AU Balashov, NV Thompson, AM Young, GS AF Balashov, Nikolay V. Thompson, Anne M. Young, George S. TI Probabilistic Forecasting of Surface Ozone with a Novel Statistical Approach SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID SELF-ORGANIZING MAPS; ARTIFICIAL NEURAL-NETWORKS; AIR-QUALITY; TEMPORAL VARIATIONS; ENSEMBLE FORECASTS; TROPOSPHERIC OZONE; SYSTEM; MODEL; PREDICTION; CLIMATOLOGY AB The recent change in the Environmental Protection Agency's surface ozone regulation, lowering the surface ozone daily maximum 8-h average (MDA8) exceedance threshold from 75 to 70 ppbv, poses significant challenges to U.S. air quality (AQ) forecasters responsible for ozone MDA8 forecasts. The forecasters, supplied by only a few AQ model products, end up relying heavily on self-developed tools. To help U.S. AQ forecasters, this study explores a surface ozone MDA8 forecasting tool that is based solely on statistical methods and standard meteorological variables from the numerical weather prediction (NWP) models. The model combines the self-organizing map (SOM), which is a clustering technique, with a stepwise weighted quadratic regression using meteorological variables as predictors for ozone MDA8. The SOM method identifies different weather regimes, to distinguish between various modes of ozone variability, and groups them according to similarity. In this way, when a regression is developed for a specific regime, data from the other regimes are also used, with weights that are based on their similarity to this specific regime. This approach, regression in SOM (REGiS), yields a distinct model for each regime taking into account both the training cases for that regime and other similar training cases. To produce probabilistic MDA8 ozone forecasts, REGiS weighs and combines all of the developed regression models on the basis of the weather patterns predicted by an NWP model. REGiS is evaluated over the San Joaquin Valley in California and the northeastern plains of Colorado. The results suggest that the model performs best when trained and adjusted separately for an individual AQ station and its corresponding meteorological site. C1 [Balashov, Nikolay V.; Thompson, Anne M.; Young, George S.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Thompson, Anne M.] NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD USA. RP Balashov, NV (reprint author), Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. EM nvb5011@psu.edu FU NASA [NNX10AR39G, NNX11AQ44G] FX The authors thank three reviewers for their numerous valuable comments that helped considerably to improve this article. The authors acknowledge the Seventh International Workshop on Air Quality Forecasting Research (IWAQFR), held in College Park, Maryland, in 2015, for important input regarding the state of international AQ forecasting in 2015. Special thanks are given to AQ operational forecasters William Ryan, Amy Huff, and Joel Dreessen for their feedback regarding the AQ forecasting work flow. Thanks are also given to NASA for their enlightening DISCOVER-AQ campaign experience. We give many thanks to Ryan Stauffer, Hannah Haliday, Greg Garner, and the rest of the Gator research group for their continuing help and support. This research was supported by NASA through grants to The Pennsylvania State University, DISCOVER-AQ (NNX10AR39G), and Applied Sciences Air Quality (NNX11AQ44G). NR 62 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD FEB PY 2017 VL 56 IS 2 BP 297 EP 316 DI 10.1175/JAMC-D-16-0110.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EL3DT UT WOS:000394500500004 ER PT J AU Larson, KM Ray, RD Williams, SDP AF Larson, Kristine M. Ray, Richard D. Williams, Simon D. P. TI A 10-Year Comparison of Water Levels Measured with a Geodetic GPS Receiver versus a Conventional Tide Gauge SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID TIME-SERIES AB A standard geodetic GPS receiver and a conventional Aquatrak tide gauge, collocated at Friday Harbor, Washington, are used to assess the quality of 10 years of water levels estimated from GPS sea surface reflections. The GPS results are improved by accounting for ( tidal) motion of the reflecting sea surface and for signal propagation delay by the troposphere. The RMS error of individual GPS water level estimates is about 12 cm. Lower water levels are measured slightly more accurately than higher water levels. Forming daily mean sea levels reduces the RMS difference with the tide gauge data to approximately 2 cm. For monthly means, the RMS difference is 1.3 cm. The GPS elevations, of course, can be automatically placed into a well-defined terrestrial reference frame. Ocean tide coefficients, determined from both the GPS and tide gauge data, are in good agreement, with absolute differences below 1 cm for all constituents save K-1 and S-1. The latter constituent is especially anomalous, probably owing to daily temperature-induced errors in the Aquatrak tide gauge. C1 [Larson, Kristine M.] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA. [Ray, Richard D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Williams, Simon D. P.] Natl Oceanog Ctr, Liverpool, Merseyside, England. RP Larson, KM (reprint author), Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA. EM kristinem.larson@gmail.com FU National Science Foundation [AGS 1449554]; Sea Level Change program of the National Aeronautics and Space Administration; NERC FX The tide gauge data at Friday Harbor were obtained from NOAA/National Ocean Service (http://tidesandcurrents.noaa.gov/waterlevels.html?id=9449880). Monthly tide gauge data, used for further comparisons, were obtained from the Permanent Service for Mean Sea Level. GPS data from SC02 were provided by the Earth-Scope Plate Boundary Observatory via UNAVCO (http://pbo.unavco.org). We thank the UNAVCO staff for maintaining SC02. KL's work on reflections has been supported by the National Science Foundation (AGS 1449554). RR's work is supported by the Sea Level Change program of the National Aeronautics and Space Administration. SW's work is supported by NERC national capability funding to the NOC Marine Physics and Ocean climate directorate. Permanent Service for Mean Sea Level data were retrieved from online (http://www.psmsl.org/data/obtaining). NR 36 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD FEB PY 2017 VL 34 IS 2 BP 295 EP 307 DI 10.1175/JTECH-D-16-0101.1 PG 13 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA EL3GM UT WOS:000394507600004 ER PT J AU Zhang, SX Pu, ZX Posselt, DJ Atlas, R AF Zhang, Shixuan Pu, Zhaoxia Posselt, Derek J. Atlas, Robert TI Impact of CYGNSS Ocean Surface Wind Speeds on Numerical Simulations of a Hurricane in Observing System Simulation Experiments SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID SCATTEROMETER; SSM/I AB The NASA Cyclone Global Navigation Satellite System (CYGNSS) was launched in late 2016. It will make available frequent ocean surface wind speed observations throughout the life cycle of tropical storms and hurricanes. In this study, the impact of CYGNSS ocean surface winds on numerical simulations of a hurricane case is assessed with a research version of the Hurricane Weather Research and Forecasting Model and a Gridpoint Statistical Interpolation analysis system in a regional observing system simulation experiment framework. Two different methods for reducing the CYGNSS data volume were tested: one in which the winds were thinned and one in which the winds were superobbed. The results suggest that assimilation of the CYGNSS winds has great potential to improve hurricane track and intensity simulations through improved representations of the surface wind fields, hurricane inner-core structures, and surface fluxes. The assimilation of the superobbed CYGNSS data seems to be more effective in improving hurricane track forecasts than thinning the data. C1 [Zhang, Shixuan; Pu, Zhaoxia] Univ Utah, Dept Atmospher Sci, Salt Lake City, UT USA. [Posselt, Derek J.] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA. [Atlas, Robert] NOAA, Atlantic Oceanog & Meteorol Lab, Miami, FL 33149 USA. [Posselt, Derek J.] NASA, Jet Prop Lab, Pasadena, CA USA. RP Pu, ZX (reprint author), Univ Utah, Dept Atmospher Sci, Salt Lake City, UT USA. EM zhaoxia.pu@utah.edu FU NASA Weather Program [NNX13AQ38G] FX We appreciate the useful communication with the CYGNSS science team. This study was supported by the NASA Weather Program (Award NNX13AQ38G), managed by Dr. Remesh Kakar. Computer resources from the University of Utah's Center for High Performance Computing and NASA's High-End Computing Program are greatly appreciated. The comments from two anonymous reviewers were very helpful and improved an earlier version of the manuscript. NR 33 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD FEB PY 2017 VL 34 IS 2 BP 375 EP 383 DI 10.1175/JTECH-D-16-0144.1 PG 9 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA EL3GM UT WOS:000394507600009 ER PT J AU Yu, JR Petros, M Singh, UN Refaat, TF Reithmaier, K Remus, RG Johnson, W AF Yu, Jirong Petros, Mulugeta Singh, Upendra N. Refaat, Tamer F. Reithmaier, Karl Remus, Ruben G. Johnson, William TI An Airborne 2-mu m Double-Pulsed Direct-Detection Lidar Instrument for Atmospheric CO2 Column Measurements SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID DIFFERENTIAL ABSORPTION LIDAR; LINE PARAMETERS; SENSITIVITY-ANALYSIS; COHERENT-DETECTION; MU-M; LASER; SPECTROMETER; OPTIMIZATION; CM(-1); WIND AB This study reports airborne measurements of atmospheric CO2 column density using a 2-mu m double-pulsed integrated path differential absorption (IPDA) lidar. This new 2-mu m IPDA lidar offers an alternative approach to measure CO2 column density with unique features. The online frequencies of this lidar can be tuned to 1-6 GHz from the CO2 R30 absorption line peak. It provides high measurement sensitivity to the lower-tropospheric CO2 near the ground surface. This instrument was flown in the spring of 2014 in a NASA B200 aircraft. The results of these test flights clearly demonstrate the measurement capabilities of this lidar instrument. The CO2 column dry mixing ratio is compared to an in situ CO2 measurement by a collocated NOAA flight. The IPDA lidar measurement is determined to be in good agreement with a 0.36% difference, which corresponds to 1.48 ppm. It is the average difference between the IPDA lidar measurements and the NOAA air samples in the flight altitudes from 3 to 6.1 km. C1 [Yu, Jirong; Petros, Mulugeta; Singh, Upendra N.; Refaat, Tamer F.; Remus, Ruben G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Reithmaier, Karl] Sci Syst & Applicat Inc, Hampton, VA USA. [Johnson, William] Michigan Aerosp Corp, Ann Arbor, MI USA. RP Yu, JR (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM j.yu@nasa.gov FU NASA Earth Science Technology Office (ESTO) [ATI-QRS-12-0002]; Engineering and Research Services Directorates at NASA Langley Research Center FX We thank the NASA Earth Science Technology Office (ESTO) for funding this project (ATI-QRS-12-0002). The authors acknowledge Charlie M. Boyer, James Fay, Susan G. Johnston, and Luke S. Murchison for their excellent engineering contributions to building this instrument. The authors are particularly indebted to Dr. Robert Menzies at JPL for his invaluable input on the design of the instrument and for his help in data retrieval. We also thank the Engineering and Research Services Directorates at NASA Langley Research Center for their support. Thanks are also due to the dedicated efforts of the Research Systems Integration Branch, which made airborne flight testing possible. Acknowledgements are also due to the LaRC CAPABLE team and NOAA for providing public information that is significant for the science validation process. The authors also would like to thank Dr. Michael J. Kavaya, Dr. Syed Ismail, Dr. Yingxin Bai, and Tony Notari at LaRC for the very useful discussions, advice, and assistance. NR 39 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD FEB PY 2017 VL 34 IS 2 BP 385 EP 400 DI 10.1175/JTECH-D-16-0112.1 PG 16 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA EL3GM UT WOS:000394507600010 ER PT J AU Ray, RD AF Ray, R. D. TI On Tidal Inference in the Diurnal Band SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID FREE WOBBLE-RESONANCE; RADIO INTERFEROMETRY; FORCED NUTATIONS; TIDES; EARTH; ALTIMETRY; GEODESY; MODELS AB Standard methods of tidal inference should be revised to account for a known resonance that occurs mostly within the K-1 tidal group in the diurnal band. The resonance arises from a free rotational mode of Earth caused by the fluid core. In a set of 110 bottom-pressure tide stations, the amplitude of the P-1 tidal constituent is shown to be suppressed relative to K-1, which is in good agreement with the resonance theory. Standard formulas for the K-1 nodal modulation remain essentially unaffected. Two examples are given of applications of the refined inference methodology: one with monthly tide gauge data and one with satellite altimetry. For some altimeter-constrained tide models, an inferred P-1 constituent is found to be more accurate than a directly determined one. C1 [Ray, R. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ray, RD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM richard.ray@nasa.gov FU Ocean Surface Topography program of the National Aeronautics and Space Administration FX I thank Duncan Agnew for his review and subsequent correspondence, Ben Chao and Shailen Desai for the useful discussions, and two anonymous reviewers for their comments. This work was supported by the Ocean Surface Topography program of the National Aeronautics and Space Administration. NR 36 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD FEB PY 2017 VL 34 IS 2 BP 437 EP 446 DI 10.1175/JTECH-D-16-0142.1 PG 10 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA EL3GM UT WOS:000394507600014 ER PT J AU McCormack, J Hoppel, K Kuhi, D de Wit, R Stober, G Espy, P Baker, N Brown, P Fritts, D Jacobi, C Janches, D Mitchell, N Ruston, B Swadley, S Viner, K Whitcomb, T Hibbins, R AF McCormack, J. Hoppel, K. Kuhi, D. de Wit, R. Stober, G. Espy, P. Baker, N. Brown, P. Fritts, D. Jacobi, C. Janches, D. Mitchell, N. Ruston, B. Swadley, S. Viner, K. Whitcomb, T. Hibbins, R. TI Comparison of mesospheric winds from a high-altitude meteorological analysis system and meteor radar observations during the boreal winters of 2009-2010 and 2012-2013 SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE MLT Winds; Tides; Radar observations ID STRATOSPHERIC WARMING EVENTS; LOWER THERMOSPHERE; PLANETARY-WAVES; S-TRANSFORM; MEAN WINDS; WACCM-X; VARIABILITY; NORTHERN; PARAMETERIZATION; ATMOSPHERE AB We present a study of horizontal winds in the mesosphere and lower thermosphere (MLT) during the boreal winters of 2009-2010 and 2012-2013 produced with a new high-altitude numerical weather prediction (NWP) system. This system is based on a modified version of the Navy Global Environmental Model (NAVGEM) with an extended vertical domain up to 116 km altitude coupled with a hybrid four-dimensional variational (4DVAR) data assimilation system that assimilates both standard operational meteorological observations in the troposphere and satellite-based observations of temperature, ozone and water vapor in the stratosphere and mesosphere. NAVGEM-based MLT analyzed winds are validated using independent meteor radar wind observations from nine different sites ranging from 69 degrees N-67 degrees S latitude. Time-averaged NAVGEM zonal and meridional wind profiles between 75 and 95 km altitude show good qualitative and quantitative agreement with corresponding meteor radar wind profiles. Wavelet analysis finds that the 3-hourly NAVGEM and 1-hourly radar winds both exhibit semi-diurnal, diurnal, and quasi-diurnal variations whose vertical profiles of amplitude and phase are also in good agreement. Wavelet analysis also reveals common time-frequency behavior in both NAVGEM and radar winds throughout the Northern extratropics around the times of major stratospheric sudden warmings (SSWs) in January 2010 and January 2013, with a reduction in semi-diurnal amplitudes beginning around the time of a mesospheric wind reversal at 60 degrees N that precedes the SSW, followed by an amplification of semi-diurnal amplitudes that peaks 10-14 days following the onset of the mesospheric wind reversal. The initial results presented in this study demonstrate that the wind analyses produced by the high altitude NAVGEM system accurately capture key features in the observed MLT winds during these two boreal winter periods. C1 [McCormack, J.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Hoppel, K.; Kuhi, D.] Naval Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [de Wit, R.; Janches, D.] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD USA. [Stober, G.] Univ Rostock, Leibniz Inst Atmospher Phys, Kuhlungsborn, Germany. [Espy, P.; Hibbins, R.] Norwegian Univ Sci & Technol NTNU, Trondheim, Norway. [Baker, N.; Ruston, B.; Swadley, S.; Viner, K.; Whitcomb, T.] Naval Res Lab, Marine Meteorol Div, Monterey, CA USA. [Brown, P.] Univ Western Ontario, Dept Phys & Astron, London, ON, Canada. [Fritts, D.] GATS Inc, Boulder, CO USA. [Jacobi, C.] Univ Leipzig, Leipzig, Germany. [Mitchell, N.] Univ Bath, Ctr Space Atmospher & Ocean Sci, Bath, Avon, England. RP McCormack, J (reprint author), Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. FU Chief of Naval Research; Department of Defense High Performance Computing Modernization Program; NASA Heliophysics Division Living with a Star Program [NNH13AV95I]; NASA Postdoctoral Program; National Science Foundation [AGS-1112830]; ARISE2 project; European Community's Horizon 2020 programme [653980] FX The authors thank two anonymous reviewers for their constructive comments. NAVGEM development was supported by the Chief of Naval Research. All NAVGEM experiments were performed under a grant of computer time from the Department of Defense High Performance Computing Modernization Program. Additional support for J. McCormack was provided by the NASA Heliophysics Division Living with a Star Program award NNH13AV95I. Support for R. de Wit was provided by the NASA Postdoctoral Program, administered by the Universities Space Research Association. Support for D. Fritts was provided the National Science Foundation grant AGS-1112830. Support for P. Espy and R. Hibbins was provided by the ARISE2 project, funded by the European Community's Horizon 2020 programme under grant agreement number 653980. NR 44 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 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD FEB PY 2017 VL 154 BP 132 EP 166 DI 10.1016/j.jastp.2016.12.007 PG 35 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA EN4BH UT WOS:000395952000015 ER PT J AU Bosilovich, MG Robertson, FR Takacs, L Molod, A Mocko, D AF Bosilovich, Michael G. Robertson, Franklin R. Takacs, Lawrence Molod, Andrea Mocko, David TI Atmospheric Water Balance and Variability in the MERRA-2 Reanalysis SO JOURNAL OF CLIMATE LA English DT Article ID GLOBAL PRECIPITATION; ENERGY; IRRADIANCE; EVOLUTION; RAINFALL; PROJECT; BUDGETS; SYSTEM; IMPACT; FLOWS AB Closing and balancing Earth's global water cycle remains a challenge for the climate community. Observations are limited in duration, global coverage, and frequency, and not all water cycle terms are adequately observed. Reanalyses aim to fill the gaps through the assimilation of as many atmospheric water vapor observations as possible. Former generations of reanalyses have demonstrated a number of systematic problems that have limited their use in climate studies, especially regarding low-frequency trends. This study characterizes the NASA Modern-Era Retrospective Analysis for Research and Applications version 2 (MERRA-2) water cycle relative to contemporary reanalyses and observations. MERRA-2 includes measures intended to minimize the spurious global variations related to inhomogeneity in the observational record. The global balance and cycling of water from ocean to land is presented, with special attention given to the water vapor analysis increment and the effects of the changing observing system. While some systematic regional biases can be identified, MERRA-2 produces temporally consistent time series of total column water and transport of water from ocean to land. However, the interannual variability of ocean evaporation is affected by the changing surface-wind-observing system, and precipitation variability is closely related to the evaporation. The surface energy budget is also strongly influenced by the interannual variability of the ocean evaporation. Furthermore, evaluating the relationship of temperature and water vapor indicates that the variations of water vapor with temperature are weaker in satellite data reanalyses, not just MERRA-2, than determined by observations, atmospheric models, or reanalyses without water vapor assimilation. C1 [Bosilovich, Michael G.; Takacs, Lawrence; Molod, Andrea; Mocko, David] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD USA. [Robertson, Franklin R.] NASA, Marshall Space Flight Ctr, Huntsville, AL USA. [Takacs, Lawrence] SSAI, Lanham, MD USA. [Molod, Andrea] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Mocko, David] SAIC, Greenbelt, MD USA. RP Bosilovich, MG (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD USA. EM michael.bosilovich@nasa.gov FU NASA energy and water cycle studies program [NNH13ZDA001N-NEWS]; NASA Modeling, Analysis and Prediction program FX This paper was sponsored in large part by the NASA energy and water cycle studies program (NNH13ZDA001N-NEWS). MERRA-2 data are developed by theGMAO with support from the NASA Modeling, Analysis and Prediction program. (Information on and availability of the reanalyses' data used here can be found online reanalysis. org. Similarly, information on the observation data can be found at climatedataguide. ucar. edu.) Three anonymous reviewers provided valuable input that greatly helped the final version of the manuscript. Discussions with Max Suarez streamlined the presentation of the influence of the contributions to the evaporation variability. NR 47 TC 0 Z9 0 U1 0 U2 0 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 FEB PY 2017 VL 30 IS 4 BP 1177 EP 1196 DI 10.1175/JCLI-D-16-0338.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EM7WG UT WOS:000395522400001 ER PT J AU Cox, GK Brill, RW Bonaro, KA Farrell, AP AF Cox, Georgina K. Brill, Richard W. Bonaro, Kaitlin A. Farrell, Anthony P. TI Determinants of coronary blood flow in sandbar sharks, Carcharhinus plumbeus SO JOURNAL OF COMPARATIVE PHYSIOLOGY B-BIOCHEMICAL SYSTEMIC AND ENVIRONMENTAL PHYSIOLOGY LA English DT Article DE Cardiac power output; Heart rate; Coronary blood flow; Coronary resistance; Sharks ID MYOCARDIAL OXYGEN-CONSUMPTION; DOGFISH SCYLIORHINUS-CANICULA; TROUT ONCORHYNCHUS-MYKISS; RAINBOW-TROUT; CARDIAC-PERFORMANCE; HEART-RATE; HEMITRIPTERUS-AMERICANUS; VENTRICULAR MYOCARDIUM; TRIAKIS-SEMIFASCIATA; PROGRESSIVE HYPOXIA AB The coronary circulation first appeared in the chordate lineage in cartilaginous fishes where, as in birds and mammals but unlike most teleost fishes, it supplies arterial blood to the entire myocardium. Despite the pivotal position of elasmobranch fishes in the evolution of the coronary circulation, the determinants of coronary blood flow have never been investigated in this group. Elasmobranch fishes are of special interest because of the morphological arrangement of their cardiomyocytes. Unlike teleosts, the majority of the ventricular myocardium in elasmobranch fishes is distant to the venous blood returning to the heart (i.e., the luminal blood). Also, the majority of the myocardium is in close association with the coronary circulation. To determine the relative contribution of the coronary and luminal blood supplies to cardiovascular function in sandbar sharks, Carcharhinus plumbeus, we measured coronary blood flow while manipulating cardiovascular status using acetylcholine and adrenaline. By exploring inter-and intra-individual variation in cardiovascular variables, we show that coronary blood flow is directly related to heart rate (R-2 = 0.6; P < 0.001), as it is in mammalian hearts. Since coronary blood flow is inversely related to coronary resistance both in vivo and in vitro, we suggest that in elasmobranch fishes, changes in heart rate mediate changes in coronary vascular resistance, which adjust coronary blood flow appropriately. C1 [Cox, Georgina K.; Farrell, Anthony P.] Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. [Brill, Richard W.] Natl Marine Fisheries Serv, Northeast Fisheries Sci Ctr, James J Howard Marine Sci Lab, Highlands, NJ USA. [Bonaro, Kaitlin A.] Washington & Lee Univ, Lexington, VA 24450 USA. [Farrell, Anthony P.] Univ British Columbia, Fac Land & Food Syst, Vancouver, BC, Canada. RP Cox, GK (reprint author), Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. EM cox@zoology.ubc.ca FU Natural Sciences and Engineering Research Council of Canada [RGPIN 2015 05059] FX This study was supported by a Natural Sciences and Engineering Research Council of Canada Discovery Grant (RGPIN 2015 05059) to APF. APF holds a Canada Research Chair. NR 55 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0174-1578 EI 1432-136X J9 J COMP PHYSIOL B JI J. Comp. Physiol. B-Biochem. Syst. Environ. Physiol. PD FEB PY 2017 VL 187 IS 2 BP 315 EP 327 DI 10.1007/s00360-016-1033-x PG 13 WC Physiology; Zoology SC Physiology; Zoology GA EO1CV UT WOS:000396436100004 PM 27678513 ER PT J AU Poinar, K Joughin, I Lenaerts, JTM van den Broeke, MR AF Poinar, Kristin Joughin, Ian Lenaerts, Jan T. M. van den Broeke, Michiel R. TI Englacial latent-heat transfer has limited influence on seaward ice flux in western Greenland SO JOURNAL OF GLACIOLOGY LA English DT Article DE cryo-hydrologic warming; Greenland ice sheet; ice dynamics; ice-sheet modelling; polar firn ID JAKOBSHAVN ISBRAE; FAST-FLOW; SHEET; TEMPERATURE; BOREHOLES; MOTION; FIRN; DEFORMATION; VARIABILITY; MECHANISMS AB Surface meltwater can refreeze within firn layers and crevasses to warm ice through laten-theat transfer on decadal to millennial timescales. Earlier work posited that the consequent softening of the ice might accelerate ice flow, potentially increasing ice-sheet mass loss. Here, we calculate the effect of meltwater refreezing on ice temperature and softness in the P (a) over cap ktsoq (near Swiss Camp) and Jakobshavn Isbr ae regions of western Greenland using a numeric model and existing borehole measurements. We show that in the Jakobshavn catchment, meltwater percolation within the firn warms the ice at depth by 3-5 degrees C. By contrast, meltwater refreezing in crevasses (cryo-hydrologic warming) at depths of similar to 300 m warms the ice in P (a) over cap kitsoq by up to 10 degrees C, but this causes minimal increase in ice motion (< 10 ma(-1)). P<(a)over cap>kitsoq is representative of western Greenland's land-terminating ice, where the slow movement of ice through a wide ablation zone provides ideal conditions for cryo-hydrologic warming to occur. We find that only similar to 37% of the western Greenland ice flux, however, travels through such areas. Overall, our findings suggest that cryo-hydrologic warming will likely have only a limited effect on the dynamic evolution of the Greenland ice sheet. C1 [Poinar, Kristin; Joughin, Ian] Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA. [Poinar, Kristin] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Lenaerts, Jan T. M.; van den Broeke, Michiel R.] Univ Utrecht, Inst Marine & Atmospher Res, Utrecht, Netherlands. RP Poinar, K (reprint author), Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA.; Poinar, K (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. EM kristin.poinar@nasa.gov FU National Science Foundation Graduate Research Fellowship [DGE-0718124]; CReSIS [NSF ANT-0424589]; Polar Program of the Netherlands Organisation for Scientific Research; Netherlands Earth System Science Center (NESSC) FX This material is based upon work supported by the National Science Foundation Graduate Research Fellowship Program under Grant No. DGE-0718124 (K.P.) and through CReSIS (NSF ANT-0424589, I.J. and K.P.). The Polar Program of the Netherlands Organisation for Scientific Research and the Netherlands Earth System Science Center (NESSC) supported J.T.M.L. and M.R.v.d.B. We are grateful to Michelle Koutnik, Ben Smith and Ed Waddington for helpful comments on drafts of this manuscript and to Martin Luthi and two anonymous reviewers for their insightful and constructive criticism of this work. NR 55 TC 1 Z9 1 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA EDINBURGH BLDG, SHAFTESBURY RD, CB2 8RU CAMBRIDGE, ENGLAND SN 0022-1430 EI 1727-5652 J9 J GLACIOL JI J. Glaciol. PD FEB PY 2017 VL 63 IS 237 BP 1 EP 16 DI 10.1017/jog.2016.103 PG 16 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA EL2FK UT WOS:000394435300001 ER PT J AU Skiles, SM Painter, T AF Skiles, S. McKenzie Painter, Thomas TI Daily evolution in dust and black carbon content, snow grain size, and snow albedo during snowmelt, Rocky Mountains, Colorado SO JOURNAL OF GLACIOLOGY LA English DT Article DE energy balance; melt surface; snow; snow/ice surface processes ID PARTICLE SOOT PHOTOMETER; ICE AB Light absorbing impurities (LAI) initiate powerful snow albedo feedbacks, yet due to a scarcity of observations and measurements, LAI radiative forcing is often neglected or poorly constrained in climate and hydrological models. To support physically-based modeling of LAI processes, daily measurements of dust and black carbon (BC) stratigraphy, optical grain size, snow density and spectral albedo were collected over the 2013 ablation season in the Rocky Mountains, CO. Surface impurity concentrations exhibited a wide range of values (0.02- 6.0 mg g(-1) pptw) with 98% of mass being deposited by three episodic dust events in April. Even minor dust loading initiated albedo decline, and the negative relationship between dust concentrations and albedo was log-linear. As melt progressed, individual dust layers coalesced and emerged at the snow surface, with minimal mass loss to meltwater scavenging. The observations show that the convergence of dust layers at the surface reduced albedo to 0.3 and snow depth declined similar to 50% faster than other years with similar depth but less dust. The rapid melt led to an unexpected reduction in both grain size and density in uppermost surface layers. BC concentrations covaried with dust concentrations but were several orders of magnitude lower (< 1- 20 ppb). C1 [Skiles, S. McKenzie] Utah Valley Univ, Dept Earth Sci, Orem, UT 84058 USA. [Skiles, S. McKenzie; Painter, Thomas] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Skiles, S. McKenzie; Painter, Thomas] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. RP Skiles, SM (reprint author), Utah Valley Univ, Dept Earth Sci, Orem, UT 84058 USA.; Skiles, SM (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.; Skiles, SM (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. EM mckenzie.skiles@uvu.edu FU NASA [NNX10AO97G] FX We acknowledge Chris Landry/The Center for Snow and Avalanche Studies for maintenance of Swamp Angel Study Plot and data availability from the energy balance tower. We thank Ian Delaney and Jeffrey Deems for their assistance with snow observations. We thank Shuka Schwarz and another anonymous reviewer for their comments and suggestions, which improved the paper. This work was funded by the NASA project NNX10AO97G. Part of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology under a contract from NASA. NR 30 TC 1 Z9 1 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA EDINBURGH BLDG, SHAFTESBURY RD, CB2 8RU CAMBRIDGE, ENGLAND SN 0022-1430 EI 1727-5652 J9 J GLACIOL JI J. Glaciol. PD FEB PY 2017 VL 63 IS 237 BP 118 EP 132 DI 10.1017/jog.2016.125 PG 15 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA EL2FK UT WOS:000394435300010 ER PT J AU Skiles, SM Painter, T Okin, GS AF Skiles, S. McKenzie Painter, Thomas Okin, Gregory S. TI A method to retrieve the spectral complex refractive index and single scattering optical properties of dust deposited in mountain snow SO JOURNAL OF GLACIOLOGY LA English DT Article DE energy balance; ice/atmosphere interactions; snow/ice surface processes; snow ID SAHARAN-MINERAL-DUST; RADIATIVE-TRANSFER; SIZE DISTRIBUTION; SEA-ICE; AEROSOLS; ALBEDO; SWITZERLAND; WAVELENGTHS; ATMOSPHERE; PARTICLES AB Dust deposition to snow can have regionally important climatic and hydrologic impacts resulting from direct reduction of surface albedo and indirectly from the initiation of snow albedo feedbacks. Modeling the radiative impacts of dust deposited in snow requires knowledge of the optical properties of both components. Here we present an inversion technique to retrieve the effective optical properties of dust deposited in mountain snow cover from measurements of hemispherical dust reflectance and particle size distributions using radiative transfer modeling. First, modeled reflectance is produced from single scattering properties modeled with Mie theory for a specified grain size distribution over a range of values for the imaginary part of the complex refractive index (k = 0.00001-0.1). Then, a multi-step look-up table process is employed to retrieve k(lambda) and single scattering optical properties by matching measured to modeled reflectance across the shortwave and near infrared. The real part of the complex refractive index, n, for dust aerosols ranges between 1.5 and 1.6 and a sensitivity analysis shows the method is relatively insensitive to the choice of n within this range, 1.525 was used here. Using the values retrieved by this method to update dust optical properties in a snow + aerosol radiative transfer model reduces errors in springtime albedo modeling by 50-70%. C1 [Skiles, S. McKenzie] Utah Valley Univ, Dept Earth Sci, Orem, UT 84058 USA. [Skiles, S. McKenzie; Painter, Thomas] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Skiles, S. McKenzie; Painter, Thomas] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. [Okin, Gregory S.] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90024 USA. RP Skiles, SM (reprint author), Utah Valley Univ, Dept Earth Sci, Orem, UT 84058 USA.; Skiles, SM (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.; Skiles, SM (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. EM mckenzie.skiles@uvu.edu FU NASA project [NNX10AO97G]; NASA FX We acknowledge Chris Landry/The Center for Snow and Avalanche Studies for maintenance of Swamp Angel Study Plot and data availability from the energy balance tower. We would like to thank Ian Delaney and Jeffrey Deems for their assistance with snow sample collection and observations, and Victoria Patterson for assistance in sample analysis. We would also like to thank Anne Nolin and another anonymous reviewer for their helpful comments, which improved the paper. This work was funded by the NASA project NNX10AO97G. Part of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology under a contract from NASA. NR 70 TC 1 Z9 1 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA EDINBURGH BLDG, SHAFTESBURY RD, CB2 8RU CAMBRIDGE, ENGLAND SN 0022-1430 EI 1727-5652 J9 J GLACIOL JI J. Glaciol. PD FEB PY 2017 VL 63 IS 237 BP 133 EP 147 DI 10.1017/jog.2016.126 PG 15 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA EL2FK UT WOS:000394435300011 ER PT J AU Dueri, D Acikmese, B Scharf, DP Harris, MW AF Dueri, Daniel Acikmese, Behcet Scharf, Daniel P. Harris, Matthew W. TI Customized Real-Time Interior-Point Methods for Onboard Powered-Descent Guidance SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID CONVEX-OPTIMIZATION; LOSSLESS CONVEXIFICATION; ALGORITHM; PROGRAMS; SYSTEMS AB This paper presents a new onboard-implementable, real-time convex optimization-based powered-descent guidance algorithm for planetary pinpoint landing. Earlier work provided the theoretical basis of convexification, the equivalent representation of the fuel-optimal pinpoint landing trajectory optimization problem with nonconvex control constraints as a convex optimization problem. Once the trajectory optimization problem is convexified, interior-point method algorithms can be used to solve the problem to global optimality. Though having this guarantee of convergence motivated earlier convexification results, there were no real-time interior point method algorithms available for the computation of optimal trajectories on flight computers. This paper presents the first such algorithm developed for onboard use and flight-tested on a terrestrial rocket with the NASA Jet Propulsion Laboratory and the NASA Flight Opportunities Program in 2013. First, earlier convexification results are summarized and the resulting second-order cone-programming problem for fuel-optimal trajectory optimization is presented. Then, the proposed, fairly generic, second-order cone-programming interior point method algorithm is presented in detail with an overview of the customization process for real-time computations. Customization exploits a specific problem structure to increase the computational speed, which is shown to decrease run times by two to three orders of magnitude in many applications. A new convexification result for maximal-divert trajectories with active velocity constraints is also presented herein. C1 [Dueri, Daniel; Acikmese, Behcet] Univ Washington, Seattle, WA 98195 USA. [Scharf, Daniel P.] CALTECH, Jet Prop Lab, Guidance & Control Anal Grp, 4800 Oak Grover Dr,M-S 198-326, Pasadena, CA 91109 USA. [Harris, Matthew W.] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, 1 Univ Stn,C0600, Austin, TX 78712 USA. RP Dueri, D (reprint author), Univ Washington, Seattle, WA 98195 USA. EM daniel.dueri@utexas.edu; behcet@austin.utexas.edu; Daniel.P.Scharf@jpl.nasa.gov; m_harris@utexas.edu FU Jet Propulsion Laboratory (JPL), California Institute of Technology [1492781]; Office of Naval Research [N00014-14-1-0314]; National Science Foundation [CNS-1619729] FX This research was supported in part by Jet Propulsion Laboratory (JPL), California Institute of Technology, Contract No. 1492781. Part of this research was performed at JPL, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Parts of this research are funded by Office of Naval Research Grant No. N00014-14-1-0314 and National Science Foundation Grant No. CNS-1619729. The authors thank Tim Canham of JPL, who supported the runtime characterization on a flight processor. We are grateful for our collaborators Lars Blackmore of SpaceX; John M. Carson, David S. Bayard, and Jordi Casoliva of JPL; Stephen Boyd of Stanford University; Jacob Mattingley of Metamarkets; and Ping Lu of IowaState for their valuable comments and insights. Wewould also like to thank the anonymous reviewers, whose comments were very useful in improving the quality of the paper. NR 51 TC 2 Z9 2 U1 0 U2 0 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD FEB PY 2017 VL 40 IS 2 BP 197 EP 212 DI 10.2514/1.G001480 PG 16 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA EM7TG UT WOS:000395514600003 ER PT J AU Scharf, DP Acikmese, B Dueri, D Benito, J Casoliva, J AF Scharf, Daniel P. Acikmese, Behcet Dueri, Daniel Benito, Joel Casoliva, Jordi TI Implementation and Experimental Demonstration of Onboard Powered-Descent Guidance SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID LOSSLESS CONVEXIFICATION; CONSTRAINTS AB Onboard, fuel-optimal, constrained powered-descent guidance based on the theory of lossless convexification has been implemented as the Guidance for Fuel-Optimal Large Diverts (G-FOLD) algorithm. Here, guidance means generating feedforward reference trajectories for control systems. This paper presents terrestrial flight-test demonstrations of large diverts planned by G-FOLD onboard a vertical-takeoff/vertical-landing rocket. The G-FOLD parser, which transforms the guidance problem into a second-order cone program and so encodes the divert constraints, is described at an engineering level, including new and modified constraints incorporated for these flight tests. Several practical issues, such as discretization effects, are addressed, and the flight-test architecture is presented. A total of eight flight tests were performed. In the first three, the rocket executed diverts of increasing size preplanned by G-FOLD on the ground. Then G-FOLD was demonstrated running onboard five times. Three qualitatively different types of diverts were performed, demonstrating G-FOLD over a nontrivial area of the phase space of divert boundary conditions. With one exception not involving G-FOLD, the rocket then followed diverts planned onboard to meter-level precision, consistent with preflight performance predictions. These flight tests are believed to be the first demonstrations of large diverts with constrained, onboard powered-descent guidance, readying the way for adoption of G-FOLD by future missions. C1 [Scharf, Daniel P.; Casoliva, Jordi] CALTECH, Jet Prop Lab, Guidance & Control Anal Grp, 4800 Oak Grover Dr,M-S 198-326, Pasadena, CA 91109 USA. [Acikmese, Behcet; Dueri, Daniel] Univ Washington, Dept Aeronaut & Astronaut, Seattle, WA 98195 USA. [Benito, Joel] CALTECH, Jet Prop Lab, EDL Guidance & Control Syst Grp, 4800 Oak Grover Dr,M-S 198-326, Pasadena, CA 91109 USA. RP Scharf, DP (reprint author), CALTECH, Jet Prop Lab, Guidance & Control Anal Grp, 4800 Oak Grover Dr,M-S 198-326, Pasadena, CA 91109 USA. EM Daniel.P.Scharf@jpl.nasa.gov; behcet@uw.edu; dandueri@uw.edu; Joel.Benito.Manrique@jpl.nasa.gov; Jordi.Casoliva@jpl.nasa.gov FU NASA's Flight Opportunities Program FX This research was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Funding was provided by NASA's Flight Opportunities Program. A much larger team contributed to the overall demonstrations, including Geoffery M. Vaughan, Homayoon Ansari, Nikolas Trawny, Garen Khanoyan, Swati Mohan, MiMi Aung, Martin W. Regehr, Aron Wolf, Andrew Johnson, and the TRN team of JPL; and Dave Masten, Scott Nietfeld, Travis O'Neal, Joel Scotkin, and the Operations Team of Masten Space Systems, Inc. NR 33 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 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD FEB PY 2017 VL 40 IS 2 BP 213 EP 229 DI 10.2514/1.G000399 PG 17 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA EM7TG UT WOS:000395514600004 ER PT J AU Lu, P Brunner, CW Stachowiak, SJ Mendeck, GF Tigges, MA Cerimele, CJ AF Lu, Ping Brunner, Christopher W. Stachowiak, Susan J. Mendeck, Gavin F. Tigges, Michael A. Cerimele, Christopher J. TI Verification of a Fully Numerical Entry Guidance Algorithm SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID PREDICTOR-CORRECTOR; TRAJECTORIES; CONSTRAINTS; VEHICLES; REENTRY AB The process, methodology, and results of a two year effort are presented in this paper on verification of an advanced entry guidance algorithm, called Fully Numerical Predictor-corrector Entry Guidance (FNPEG). FNPEG is a model-based numerical guidance algorithm capable of performing both direct (orbital or suborbital) entry and skip entry missions. Few vehicle-dependent adjustments are necessary, and no reference trajectory or mission-dependent planning is required. The algorithm is applicable to a wide range of vehicles with different lift-to-drag ratios and includes state-of-the-art capability to effectively control g load and damp out phugoid oscillations, without adversely affecting the guidance precision. FNPEG has undergone extensive testing and evaluation in the high-fidelity simulation environment for the Orion spacecraft at NASA Johnson Space Center. In this paper, the verification methodology and process are described. The metrics for verification are defined. Extensive testing and simulation results on FNPEG and the comparison with the primary entry guidance algorithm for Orion, PredGuid, are provided. The outcome of this effort has clearly demonstrated the capability, strong robustness, and excellent performance of FNPEG, even in the presence of dispersions and uncertainties significantly higher than the design level. C1 [Lu, Ping] San Diego State Univ, Dept Aerosp Engn, San Diego, CA 92182 USA. [Brunner, Christopher W.] Odyssey Space Res, Orbital ATK, Houston, TX 77058 USA. [Stachowiak, Susan J.; Mendeck, Gavin F.; Tigges, Michael A.] NASA Johnson Space Ctr, EG5-111, Houston, TX 77058 USA. [Cerimele, Christopher J.] NASA Johnson Space Ctr, Flight Mech & Trajectory Design Branch, EG5-111, Houston, TX 77058 USA. RP Lu, P (reprint author), San Diego State Univ, Dept Aerosp Engn, San Diego, CA 92182 USA. EM plu@mail.sdsu.edu; christopher.brunner@orbitalatk.com FU NASA Cooperative Agreement [NNX13AL88A] FX This research was supported in part by NASA Cooperative Agreement NNX13AL88A. The authors thank Kelly Smith, Ronald Sostaric, and Jeremy Rea for the valuable technical exchanges with them throughout the course of this effort. NR 39 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 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD FEB PY 2017 VL 40 IS 2 BP 230 EP 247 DI 10.2514/1.G000327 PG 18 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA EM7TG UT WOS:000395514600005 ER PT J AU Starek, JA Schmerling, E Maher, GD Barbee, BW Pavone, M AF Starek, Joseph A. Schmerling, Edward Maher, Gabriel D. Barbee, Brent W. Pavone, Marco TI Fast, Safe, Propellant-Efficient Spacecraft Motion Planning Under Clohessy-Wiltshire-Hill Dynamics SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID PROXIMITY OPERATIONS; GUIDANCE; OPTIMIZATION; NAVIGATION; ORBIT AB This paper presents a sampling-based motion planning algorithm for real-time and propellant-optimized autonomous spacecraft trajectory generation in near-circular orbits. Specifically, this paper leverages recent algorithmic advances in the field of robot motion planning to the problem of impulsively actuated, propellant-optimized rendezvous and proximity operations under the Clohessy-Wiltshire-Hill dynamics model. The approach calls upon a modified version of the FMT* algorithm to grow a set of feasible trajectories over a deterministic, low-dispersion set of sample points covering the free state space. To enforce safety, the tree is only grown over the subset of actively safe samples, from which there exists a feasible one-burn collision-avoidance maneuver that can safely circularize the spacecraft orbit along its coasting arc under a given set of potential thruster failures. Key features of the proposed algorithm include 1)theoretical guarantees in terms of trajectory safety and performance, 2)amenability to real-time implementation, and 3)generality, in the sense that a large class of constraints can be handled directly. As a result, the proposed algorithm offers the potential for widespread application, ranging from on-orbit satellite servicing to orbital debris removal and autonomous inspection missions. C1 [Starek, Joseph A.] Stanford Univ, Aeronaut & Astronaut, 496 Lomita Mall,Room 009, Stanford, CA 94305 USA. [Schmerling, Edward; Maher, Gabriel D.] Stanford Univ, Inst Computat & Math Engn, 475 Via Ortega, Stanford, CA 94305 USA. [Barbee, Brent W.] NASA, Goddard Space Flight Ctr, Nav & Miss Design Branch, Mail Code 595,8800 Greenbelt Road, Greenbelt, MD 20771 USA. [Pavone, Marco] Stanford Univ, Aeronaut & Astronaut, 496 Lomita Mall,Room 261, Stanford, CA 94305 USA. RP Starek, JA (reprint author), Stanford Univ, Aeronaut & Astronaut, 496 Lomita Mall,Room 009, Stanford, CA 94305 USA. FU Early Career Faculty grant from NASA's Space Technology Research Grants Program [NNX12AQ43G] FX This work was supported by an Early Career Faculty grant from NASA's Space Technology Research Grants Program (grant number NNX12AQ43G). NR 46 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 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD FEB PY 2017 VL 40 IS 2 BP 418 EP 438 DI 10.2514/1.G001913 PG 21 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA EM7TG UT WOS:000395514600018 ER PT J AU Niraula, R Meixner, T Ajami, H Rodell, M Gochis, D Castro, CL AF Niraula, Rewati Meixner, Thomas Ajami, Hoori Rodell, Matthew Gochis, David Castro, Christopher L. TI Comparing potential recharge estimates from three Land Surface Models across the western US SO JOURNAL OF HYDROLOGY LA English DT Article DE Recharge; Western US; Land Surface Models; VIC; Noah; Mosaic ID CLIMATE-CHANGE IMPACTS; GROUNDWATER RECHARGE; WATER-BALANCE; UNITED-STATES; RIVER-BASIN; EVAPOTRANSPIRATION; SYSTEM; RESOLUTION; PARAMETERIZATION; FOOTPRINT AB Groundwater is a major source of water in the western US. However, there are limited recharge estimates in this region due to the complexity of recharge processes and the challenge of direct observations. Land surface Models (LSMs) could be a valuable tool for estimating current recharge and projecting changes due to future climate change. In this study, simulations of three LSMs (Noah, Mosaic and VIC) obtained from the North American Land Data Assimilation System (NLDAS-2) are used to estimate potential recharge in the western US. Modeled recharge was compared with published recharge estimates for several aquifers in the region. Annual recharge to precipitation ratios across the study basins varied from 0.01% to 15% for Mosaic, 3.2% to 42% for Noah, and 6.7% to 31.8% for VIC simulations. Mosaic consistently underestimates recharge across all basins. Noah captures recharge reasonably well in wetter basins, but overestimates it in drier basins. VIC slightly overestimates recharge in drier basins and slightly underestimates it for wetter basins. While the average annual recharge values vary among the models, the models were consistent in identifying high and low recharge areas in the region. Models agree in seasonality of recharge occurring dominantly during the spring across the region. Overall, our results highlight that LSMs have the potential to capture the spatial and temporal patterns as well as seasonality of recharge at large scales. Therefore, LSMs (specifically VIC and Noah) can be used as a tool for estimating future recharge in data limited regions. (C) 2016 Elsevier B.V. All rights reserved. C1 [Niraula, Rewati; Meixner, Thomas; Castro, Christopher L.] Univ Arizona, Dept Hydrol & Atmospher Sci, Tucson, AZ USA. [Ajami, Hoori] Univ Calif Riverside, Environm Sci, Riverside, CA 92521 USA. [Rodell, Matthew] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD USA. [Gochis, David] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. RP Niraula, R (reprint author), Tarleton State Univ, TIAER, 201 St Felix St, Stephenville, TX 76401 USA. EM rewatin@email.arizona.edu FU USGS John Wesley Powell Center FX We would like to acknowledge USGS John Wesley Powell Center for funding this research. We also express our sincere gratitude to all the members of Powell Center working group (Andrew H. Manning, David A. Stonestrom, Diana M. Allen, Kyle W. Blasch, Andrea E. Brookfield, Jordan F. Clark, Alan L. Flint, Kirstin L. Neff, Bridget R. Scanlon, Kamini Singha, and Michelle A. Walvoord) for their valuable suggestions/research directions. NR 85 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-1694 EI 1879-2707 J9 J HYDROL JI J. Hydrol. PD FEB PY 2017 VL 545 BP 410 EP 423 DI 10.1016/j.jhydrol.2016.12.028 PG 14 WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA EL1RQ UT WOS:000394399100032 ER PT J AU Gebregiorgis, AS Kirstetter, PE Hong, YE Carr, NJ Gourley, JJ Petersen, W Zheng, YY AF Gebregiorgis, Abebe Sine Kirstetter, Pierre-Emmanuel Hong, Yang E. Carr, Nicholas J. Gourley, Jonathan J. Petersen, Walt Zheng, Yaoyao TI Understanding Overland Multisensor Satellite Precipitation Error in TMPA-RT Products SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID MICROWAVE SOUNDING UNIT; PASSIVE MICROWAVE; NEXT-GENERATION; RAINFALL; RADAR; RETRIEVALS; VALIDATION; ALGORITHMS; STATES; LAND AB The Tropical Rainfall Measuring Mission (TRMM) Multisatellite Precipitation Analysis (TMPA) has provided the global community a widely used multisatellite (and multisensor type) estimate of quasi-global precipitation. One of the TMPA level-3 products, 3B42RT/TMPA-RT (where RT indicates real time), is a merged product of microwave (MW) and infrared (IR) precipitation estimates, which attempts to exploit the most desirable aspects of both types of sensors, namely, quality rainfall estimation and spatiotemporal resolution. This study extensively and systematically evaluates multisatellite precipitation errors by tracking the sensor-specific error sources and quantifying the biases originating from multiple sensors. High-resolution, ground-based radar precipitation estimates from the Multi-Radar Multi-Sensor (MRMS) system, developed by the National Severe Storms Laboratory (NSSL), are utilized as reference data. The analysis procedure involves segregating the grid precipitation estimate as a function of sensor source, decomposing the bias, and then quantifying the error contribution per grid. The results of this study reveal that while all three aspects of detection (i.e., hit, missed-rain, and false-rain biases) contribute to the total bias associated with IR precipitation estimates, overestimation bias (positive hit bias) and missed precipitation are the dominant error sources for MW precipitation estimates. Considering only MW sensors, the TRMM Microwave Imager (TMI) shows the largest missed-rain and overestimation biases (nearly double that of the other MW estimates) per grid box during the summer and winter seasons. The Special Sensor Microwave Imagers/Sounders (SSMIS on board F17 and F16) also show major error during winter and spring, respectively. C1 [Gebregiorgis, Abebe Sine; Kirstetter, Pierre-Emmanuel; Hong, Yang E.] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA. [Gebregiorgis, Abebe Sine; Kirstetter, Pierre-Emmanuel; Hong, Yang E.; Carr, Nicholas J.; Zheng, Yaoyao] Univ Oklahoma, Adv Radar Res Ctr, Norman, OK 73019 USA. [Kirstetter, Pierre-Emmanuel; Hong, Yang E.; Gourley, Jonathan J.] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA. [Carr, Nicholas J.; Zheng, Yaoyao] Univ Oklahoma, Sch Meteorol, Norman, OK 73019 USA. [Petersen, Walt] NASA, Marshall Space Flight Ctr, Huntsville, AL USA. RP Gebregiorgis, AS (reprint author), Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA.; Gebregiorgis, AS (reprint author), Univ Oklahoma, Adv Radar Res Ctr, Norman, OK 73019 USA. EM abesine@ou.edu RI Kirstetter, Pierre/E-2305-2013 OI Kirstetter, Pierre/0000-0002-7381-0229 FU NASA project [NNX15AL36G, NNX13AF84G] FX This work was supported by NASA project Grants NNX15AL36G and NNX13AF84G. The authors also acknowledge the two anonymous reviewers and the editor for their comprehensive, insightful, and constructive comments during the review process of this manuscript. NR 52 TC 1 Z9 1 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2017 VL 18 IS 2 BP 285 EP 306 DI 10.1175/JHM-D-15-0207.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EO9JZ UT WOS:000397006300001 ER PT J AU Tan, J Petersen, WA Kirstetter, PE Tian, YD AF Tan, Jackson Petersen, Walter A. Kirstetter, Pierre-Emmanuel Tian, Yudong TI Performance of IMERG as a Function of Spatiotemporal Scale SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID SATELLITE PRECIPITATION PRODUCTS; INTEGRATED MULTISATELLITE RETRIEVALS; UNCERTAINTY QUANTIFICATION; ANALYSIS TMPA; DAY-1 IMERG; TRMM; RESOLUTION; SYSTEM; RADAR; MODEL AB The Integrated Multisatellite Retrievals for GPM (IMERG), a global high-resolution gridded precipitation dataset, will enable a wide range of applications, ranging from studies on precipitation characteristics to applications in hydrology to evaluation of weather and climate models. These applications focus on different spatial and temporal scales and thus average the precipitation estimates to coarser resolutions. Such amodification of scale will impact the reliability of IMERG. In this study, the performance of the Final Run of IMERG is evaluated against ground-based measurements as a function of increasing spatial resolution (from 0.1 degrees to 2.5 degrees) and accumulation periods (from 0.5 to 24 h) over a region in the southeastern United States. For ground reference, a product derived from the Multi-Radar/Multi-Sensor suite, a radar- and gauge-based operational precipitation dataset, is used. The TRMM Multisatellite Precipitation Analysis (TMPA) is also included as a benchmark. In general, both IMERG and TMPA improve when scaled up to larger areas and longer time periods, with better identification of rain occurrences and consistent improvements in systematic and random errors of rain rates. Between the two satellite estimates, IMERG is slightly better than TMPA most of the time. These results will inform users on the reliability of IMERG over the scales relevant to their studies. C1 [Tan, Jackson] Univ Space Res Assoc, Greenbelt, MD 20771 USA. [Tan, Jackson; Tian, Yudong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Petersen, Walter A.] NASA, Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL USA. [Kirstetter, Pierre-Emmanuel] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA. [Kirstetter, Pierre-Emmanuel] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA. [Tian, Yudong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. RP Tan, J (reprint author), Univ Space Res Assoc, Greenbelt, MD 20771 USA.; Tan, J (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM jackson.tan@nasa.gov RI Kirstetter, Pierre/E-2305-2013; OI Kirstetter, Pierre/0000-0002-7381-0229; Tan, Jackson/0000-0001-7085-3074 FU NASA [NNH15CO48B]; GPMMission; NASA from the GPM mission Ground Validation program [NNX16AL23G]; National Aeronautics and Space Administration Precipitation Science Program [NNH09ZDA001N] FX We are grateful to George Huffman, David Bolvin, and Ali Tokay for discussions on the direction of this study, as well as three anonymous reviewers for their detailed suggestions on improving the manuscript. 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 (Agreement Number NNH15CO48B). W. A. P. acknowledges support from the GPMMission (Project Scientist, Gail S.-Jackson, and GV Systems Manager, Mathew Schwaller) and also Precipitation Measurement Mission (PMM) Science Team funding provided by Dr. Ramesh Kakar. P. E. K. acknowledges support from NASA Grant NNX16AL23G from the GPM mission Ground Validation program. Y. T. is supported by the National Aeronautics and Space Administration Precipitation Science Program under solicitation NNH09ZDA001N. The IMERG and TMPA data were provided by the NASA/Goddard Space Flight Center's PMM and Precipitation Processing System (PPS) teams, which develop and compute IMERG and TMPA as a contribution to GPM and TRMM, respectively, and are archived at the NASA GES DISC. All codes used in this analysis are freely available at https://github.com/JacksonTanBS/2017_JHM_ScaleGV. NR 40 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2017 VL 18 IS 2 BP 307 EP 319 DI 10.1175/JHM-D-16-0174.1 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EO9JZ UT WOS:000397006300002 ER PT J AU Dai, Q Bray, M Zhuo, L Islam, T Han, DW AF Dai, Qiang Bray, Michaela Zhuo, Lu Islam, Tanvir Han, Dawei TI A Scheme for Rain Gauge Network Design Based on Remotely Sensed Rainfall Measurements SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID RADAR PRECIPITATION ESTIMATION; PRINCIPAL COMPONENTS; VARIABLE SELECTION; BIAS ADJUSTMENT; AREAL RAINFALL; WEATHER RADAR; UNCERTAINTY; GEOSTATISTICS; SATELLITE; HYDROLOGY AB A remarkable decline in the number of rain gauges is being faced in many areas of the world, as a compromise to the expensive cost of operating and maintaining rain gauges. The question of how to effectively deploy new or remove current rain gauges in order to create optimal rainfall information is becoming more and more important. On the other hand, larger-scaled, remotely sensed rainfall measurements, although poorer quality compared with traditional rain gauge rainfall measurements, provide an insight into the local storm characteristics, which are sought by traditional methods for designing a rain gauge network. Based on these facts, this study proposes a new methodology for rain gauge network design using remotely sensed rainfall datasets that aims to explore how many gauges are essential and where they should be placed. Principal component analysis (PCA) is used to analyze the redundancy of the radar grid network and to determine the number of rain gauges while the potential locations are determined by cluster analysis (CA) selection. The proposed methodology has been performed on 373 different storm events measured by a weather radar grid network and compared against an existing dense rain gauge network in southwestern England. Because of the simple structure, the proposed scheme could be easily implemented in other study areas. This study provides a new insight into rain gauge network design that is also a preliminary attempt to use remotely sensed data to solve the traditional rain gauge problems. C1 [Dai, Qiang] Nanjing Normal Univ, Key Lab Virtual Geog Environm, Minist Educ, Nanjing, Jiangsu, Peoples R China. [Dai, Qiang; Zhuo, Lu; Han, Dawei] Univ Bristol, Dept Civil Engn, Water & Environm Management Res Ctr, Bristol, Avon, England. [Dai, Qiang] Jiangsu Ctr Collaborat Innovat Geog Informat Reso, Nanjing, Jiangsu, Peoples R China. [Bray, Michaela] Cardiff Univ, Hydroenvironm Res Ctr, Cardiff, S Glam, Wales. [Islam, Tanvir] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Dai, Q (reprint author), Nanjing Normal Univ, Key Lab Virtual Geog Environm, Minist Educ, Nanjing, Jiangsu, Peoples R China.; Dai, Q (reprint author), Univ Bristol, Dept Civil Engn, Water & Environm Management Res Ctr, Bristol, Avon, England.; Dai, Q (reprint author), Jiangsu Ctr Collaborat Innovat Geog Informat Reso, Nanjing, Jiangsu, Peoples R China. EM q.dai@njnu.edu.cn FU National Natural Science Foundation of China [41501429]; Priority Academic Program Development of Jiangsu Higher Education Institutions program [164320H116]; University Natural Science Project of Jiangsu Province [16KJA170001] FX This work was supported by the National Natural Science Foundation of China (Grant 41501429), the Priority Academic Program Development of Jiangsu Higher Education Institutions program (Grant 164320H116), and the University Natural Science Project of Jiangsu Province (Grant 16KJA170001). The authors acknowledge the British Atmospheric Data Centre for providing the data. This work was done as a private venture and not in the author's (TI) capacity as an employee of the Jet Propulsion Laboratory, California Institute of Technology. NR 54 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2017 VL 18 IS 2 BP 363 EP 379 DI 10.1175/JHM-D-16-0136.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EO9JZ UT WOS:000397006300006 ER PT J AU Sinha, D Syed, TH Famiglietti, JS Reager, JT Thomas, RC AF Sinha, Debanjan Syed, Tajdarul H. Famiglietti, James S. Reager, John T. Thomas, Reis C. TI Characterizing Drought in India Using GRACE Observations of Terrestrial Water Storage Deficit SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID GROUNDWATER DEPLETION; SEVERITY INDEX; RIVER-BASIN; METEOROLOGICAL SUBDIVISIONS; CANADIAN PRAIRIE; SUMMER MONSOON; UNITED-STATES; VARIABILITY; FREQUENCY; FRAMEWORK AB Frequent recurrences of drought in India have had major societal, economical, and environmental impacts. While region-specific assessments are abundant, exhaustive appraisal over large spatial scales has been insubstantial. Here a new drought index called Water Storage Deficit Index (WSDI) is devised and analyzed for holistic representation of drought. The crux of the method is the employment of terrestrial water storage (TWS) variations from Gravity Recovery and Climate Experiment (GRACE) for quantification of drought intensity and severity. Drought events in recent times are well identified and quantified using the approach over four homogenous rainfall regions of India over the period from April 2002 to April 2015. Among the four regions, the highest peak deficit of -158.00 mm is observed in January 2015 over central India. While the drought of 2002-04 is prominent in peninsular and west-central India, the drought of 2009-10 and 2012-13 is conspicuous in almost all four regions of India. The longest deficit period of 23 months (from February 2009 to December 2010) and the highest severity value of -26.31 are observed in central and northwestern India, respectively. WSDI values show an increasing trend in west-central India (0.07 yr(-1)), indicating recovery from previously existing drought conditions. On the contrary, a decreasing trend in WSDI is observed in north-western (-0.07 yr(-1)) and central (-0.18 yr(-1)) India. Results demonstrate considerable confidence in the potential of WSDI for robust characterization of drought over large spatial scales. C1 [Sinha, Debanjan; Syed, Tajdarul H.] Indian Inst Technol ISM, Dept Appl Geol, Dhanbad, Bihar, India. [Famiglietti, James S.; Reager, John T.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA USA. [Famiglietti, James S.; Thomas, Reis C.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. [Famiglietti, James S.] Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA USA. RP Syed, TH (reprint author), Indian Inst Technol ISM, Dept Appl Geol, Dhanbad, Bihar, India. EM tsyed.ismu@gmail.com RI Syed, Tajdarul/G-6731-2014 FU Department of Science and Technology, Ministry of Science and Technology, Government of India [SR/FTP/ES-176/2010(G)]; NASA GRACE Science Team; University of California Office of the President, Multicampus Research Programs and Initiatives (JSF); Jet Propulsion Laboratory Research and Technology Development program; NASA by the California Institute of Technology FX We thank the Department of Science and Technology, Ministry of Science and Technology, Government of India for providing the funding for this research under the Fast Track Programme [Project SR/FTP/ES-176/2010(G)]. The support of the NASA GRACE Science Team is gratefully acknowledged. This work was partially funded by grants from the University of California Office of the President, Multicampus Research Programs and Initiatives (JSF), by the NASA GRACE Science Team (JSF and JTR), and by the Jet Propulsion Laboratory Research and Technology Development program (JSF). A portion of this work was conducted at the Jet Propulsion Laboratory, operated under contract with NASA by the California Institute of Technology. NR 101 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2017 VL 18 IS 2 BP 381 EP 396 DI 10.1175/JHM-D-16-0047.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EO9JZ UT WOS:000397006300007 ER PT J AU Wu, H Adler, RF Tian, YD Gu, GJ Huffman, GJ AF Wu, Huan Adler, Robert F. Tian, Yudong Gu, Guojun Huffman, George J. TI Evaluation of Quantitative Precipitation Estimations through Hydrological Modeling in IFloodS River Basins SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID SATELLITE RAINFALL PRODUCTS; STREAMFLOW SIMULATION; CLIMATE-CHANGE; LAND-SURFACE; FLOOD; UNCERTAINTY; RESOLUTION; PREDICTION; EVAPOTRANSPIRATION; RETRIEVALS AB A multiple-product-driven hydrologic modeling framework (MMF) is utilized for evaluation of quantitative precipitation estimation (QPE) products, motivated by improving the utility of satellite QPE in global flood modeling. This work addresses the challenge of objectively determining the relative value of various QPEs at river basin/subbasin scales. A reference precipitation dataset is created using a long-term water-balance approach with independent data sources. The intercomparison of nine QPEs and corresponding hydrologic simulations indicates that all products with long-term (2002-13) records have similar merits as over the short-term (April-June 2013) Iowa Flood Studies period. The model performance in calculated streamflow varies approximately linearly with precipitation bias, demonstrating that the model successfully translated the level of precipitation quality to streamflow quality with better streamflow simulations from QPEs with less bias. Phase 2 of the North American Land Data Assimilation System (NLDAS-2) has the best streamflow results for the Iowa-Cedar River basin, with daily and monthly Nash-Sutcliffe coefficients and mean annual bias of 0.81, 0.88, and -2.1%, respectively, for the long-term period. The evaluation also indicates that a further adjustment of NLDAS-2 to form the best precipitation estimation should consider spatial-temporal distribution of bias. The satellite-only products have lower performance (peak and timing) than other products, while simple bias adjustment can intermediately improve the quality of simulated streamflow. The TMPA research product (TMPA-RP; research-quality data) can generate results approaching those of the ground-based products with only monthly gauge-based adjustment to the TMPA real-time product (TMPA-RT; near-real-time data). It is further noted that the streamflow bias is strongly correlated to precipitation bias at various time scales, though other factors may play a role as well, especially on the daily time scale. C1 [Wu, Huan] Sun Yat Sen Univ, Sch Atmospher Sci, Guangzhou, Guangdong, Peoples R China. [Wu, Huan; Adler, Robert F.; Tian, Yudong; Gu, Guojun] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Huffman, George J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Wu, H (reprint author), Sun Yat Sen Univ, Sch Atmospher Sci, Guangzhou, Guangdong, Peoples R China.; Wu, H (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. EM huanwu@umd.edu FU NASA's Precipitation Measurement Mission (PMM) program [NNX16AF19G] FX This research is partially supported by NASA's Precipitation Measurement Mission (PMM) program (Award NNX16AF19G). We thank Drs. Pingping Xie (NOAA/NCEP/CPC), Felipe Quintero Duque (University of Iowa), and Dr. Jun Dong (University of Maryland) for assisting in accessing and processing of CPC-U gridded gauge data, IFC, and Q2 radar data, respectively. NR 71 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2017 VL 18 IS 2 BP 529 EP 553 DI 10.1175/JHM-D-15-0149.1 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EO9JZ UT WOS:000397006300015 ER PT J AU Hung, CC Hurst, J Santiago, D Lizcano, M Kelly, M AF Hung, Ching-cheh Hurst, Janet Santiago, Diana Lizcano, Maricela Kelly, Marisabel TI Highly thermally conductive hexagonal boron nitride/alumina composite made from commercial hexagonal boron nitride SO JOURNAL OF THE AMERICAN CERAMIC SOCIETY LA English DT Article DE alumina; boron nitride; composites; thermal conductivity AB Hexagonal BN is an unusual material in that it is both highly thermally conductive as well as an electrical insulator. Additionally, hBN is also thermally stable in air. This unusual combination of properties makes hBN of significant interest for thermal management. Unfortunately, hBN is not easily consolidated into substrates without the addition of second phases which generally result in poorer thermal performance. This research investigates the potential to utilize this material to dissipate heat from high-voltage, high-power electrical devices. Specifically, a process to coat individual platelets of commercial hexagonal BN powder with a layer of amorphous aluminum oxide was developed. The coated hexagonal BN was then hot-pressed to form a highly thermally conductive substrate. The process to coat hexagonal BN platelets with aluminum oxide was accomplished by mixing hexagonal BN with AlCl3 containing some water, then evaporation of excess AlCl3 to form a Al, Cl, and O layer on hexagonal BN. This product was then heated in air to convert the surface layer into aluminum oxide. Following hot pressing to 1950 degrees C and 10ksi, the consolidated composite has through-plane and in-plane thermal conductivity of 14 and 157W(m>K)(-1), respectively, at room temperature. C1 [Hung, Ching-cheh; Hurst, Janet; Santiago, Diana; Lizcano, Maricela; Kelly, Marisabel] NASA, Mat Chem & Phys Branch, Mat & Struct Div, Res & Engn Directorate,Glenn Res Ctr, Cleveland, OH 44135 USA. RP Hung, CC (reprint author), NASA, Mat Chem & Phys Branch, Mat & Struct Div, Res & Engn Directorate,Glenn Res Ctr, Cleveland, OH 44135 USA. EM Ching-cheh.Hung-1@nasa.gov FU NASA Advanced Air Transportation Technology Project (AATT) FX The authors thank NASA Advanced Air Transportation Technology Project (AATT) for supporting this research and NETZSCH Instruments North America, LLC, for thermal conductivity measurement. Journal reviewer's inputs are valuable and are appreciated. NR 5 TC 1 Z9 1 U1 2 U2 2 PU WILEY PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-7820 EI 1551-2916 J9 J AM CERAM SOC JI J. Am. Ceram. Soc. PD FEB PY 2017 VL 100 IS 2 BP 515 EP 519 DI 10.1111/jace.14638 PG 5 WC Materials Science, Ceramics SC Materials Science GA EL3UX UT WOS:000394545900008 ER PT J AU Loehle, S Jenniskens, P Bohrk, H Bauer, T Elsasser, H Sears, DW Zolensky, ME Shaddad, MH AF Loehle, Stefan Jenniskens, Peter Boehrk, Hannah Bauer, Thomas Elsaesser, Henning Sears, Derek W. Zolensky, Michael E. Shaddad, Muawia H. TI Thermophysical properties of Almahata Sitta meteorites (asteroid 2008 TC3) for high-fidelity entry modeling SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID HEAT-CAPACITY; THERMAL-DIFFUSIVITY; FLASH METHOD; RECOVERY AB Asteroid 2008 TC3 was characterized in a unique manner prior to impacting Earth's atmosphere, making its October 7, 2008, impact a suitable field test for or validating the application of high-fidelity re-entry modeling to asteroid entry. The accurate modeling of the behavior of 2008 TC3 during its entry in Earth's atmosphere requires detailed information about the thermophysical properties of the asteroid's meteoritic materials at temperatures ranging from room temperature up to the point of ablation (T similar to 1400 K). Here, we present measurements of the thermophysical properties up to these temperatures (in a 1 atm. pressure of argon) for two samples of the Almahata Sitta meteorites from asteroid 2008 TC3: a thick flat-faced ureilite suitably shaped for emissivity measurements and a thin flat-faced EL6 enstatite chondrite suitable for diffusivity measurements. Heat capacity was determined from the elemental composition and density from a 3-D laser scan of the sample. We find that the thermal conductivity of the enstatite chondrite material decreases more gradually as a function of temperature than expected, while the emissivity of the ureilitic material decreases at a rate of 9.5 x 10(10) 5 K-1 above 770 K. The entry scenario is the result of the actual flight path being the boundary to the load the meteorite will be affected with when entering. An accurate heat load prediction depends on the thermophysical properties. Finally, based on these data, the breakup can be calculated accurately leading to a risk assessment for ground damage. C1 [Loehle, Stefan] Inst Space Syst, High Enthalpy Flow Diagnost Grp, D-70569 Stuttgart, Germany. [Jenniskens, Peter] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Jenniskens, Peter; Sears, Derek W.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. [Boehrk, Hannah; Elsaesser, Henning] DLR, Inst Struct & Design, D-70569 Stuttgart, Germany. [Bauer, Thomas] DLR, Inst Tech Thermodynam, D-51147 Cologne, Germany. [Zolensky, Michael E.] NASA, Johnson Space Ctr, ARES, Houston, TX 77058 USA. [Shaddad, Muawia H.] Univ Khartoum, Dept Phys, Khartoum, Sudan. RP Loehle, S (reprint author), Inst Space Syst, High Enthalpy Flow Diagnost Grp, D-70569 Stuttgart, Germany. EM loehle@irs.uni-stuttgart.de FU NASA Ames Research Center's Asteroid Threat Assessment Project; NASA's Near Earth Object Observation program FX P. J. and D. S. acknowledge support from the NASA Ames Research Center's Asteroid Threat Assessment Project and the NASA's Near Earth Object Observation program. NR 28 TC 0 Z9 0 U1 0 U2 0 PU WILEY 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 FEB PY 2017 VL 52 IS 2 BP 197 EP 205 DI 10.1111/maps.12788 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EO6SO UT WOS:000396823000001 ER PT J AU Kwan, J Sanchez, C Clampitt, J Blazek, J Crocce, M Jain, B Zuntz, J Amara, A Becker, MR Bernstein, GM Bonnett, C DeRose, J Dodelson, S Eifler, TF Gaztanaga, E Giannantonio, T Gruen, D Hartley, WG Kacprzak, T Kirk, D Krause, E MacCrann, N Miquel, R Park, Y Ross, AJ Rozo, E Rykoff, ES Sheldon, E Troxel, MA Wechsler, RH Abbott, TMC Abdalla, FB Allam, S Benoit-Levy, A Brooks, D Burke, DL Rosell, AC Kind, MC Cunha, CE D'Andrea, CB da Costa, LN Desai, S Diehl, HT Dietrich, JP Doel, P Evrard, AE Fernandez, E Finley, DA Flaugher, B Fosalba, P Frieman, J Gerdes, DW Gruendl, RA Gutierrez, G Honscheid, K James, DJ Jarvis, M Kuehn, K Lahav, O Lima, M Maia, MAG Marshall, JL Martini, P Melchior, P Mohr, JJ Nichol, RC Nord, B Plazas, AA Reil, K Romer, AK Roodman, A Sanchez, E Scarpine, V Sevilla-Noarbe, I Smith, RC Soares-Santos, M Sobreira, F Suchyta, E Swanson, MEC Tarle, G Thomas, D Vikram, V Walker, AR AF Kwan, J. Sanchez, C. Clampitt, J. Blazek, J. Crocce, M. Jain, B. Zuntz, J. Amara, A. Becker, M. R. Bernstein, G. M. Bonnett, C. DeRose, J. Dodelson, S. Eifler, T. F. Gaztanaga, E. Giannantonio, T. Gruen, D. Hartley, W. G. Kacprzak, T. Kirk, D. Krause, E. MacCrann, N. Miquel, R. Park, Y. Ross, A. J. Rozo, E. Rykoff, E. S. Sheldon, E. Troxel, M. A. Wechsler, R. H. Abbott, T. M. C. Abdalla, F. B. Allam, S. Benoit-Levy, A. Brooks, D. Burke, D. L. Rosell, A. Carnero Kind, M. Carrasco Cunha, C. E. D'Andrea, C. B. da Costa, L. N. Desai, S. Diehl, H. T. Dietrich, J. P. Doel, P. Evrard, A. E. Fernandez, E. Finley, D. A. Flaugher, B. Fosalba, P. Frieman, J. Gerdes, D. W. Gruendl, R. A. Gutierrez, G. Honscheid, K. James, D. J. Jarvis, M. Kuehn, K. Lahav, O. Lima, M. Maia, M. A. G. Marshall, J. L. Martini, P. Melchior, P. Mohr, J. J. Nichol, R. C. Nord, B. Plazas, A. A. Reil, K. Romer, A. K. Roodman, A. Sanchez, E. Scarpine, V. Sevilla-Noarbe, I. Smith, R. C. Soares-Santos, M. Sobreira, F. Suchyta, E. Swanson, M. E. C. Tarle, G. Thomas, D. Vikram, V. Walker, A. R. CA DES Collaboration TI Cosmology from large-scale galaxy clustering and galaxy-galaxy lensing with Dark Energy Survey Science Verification data SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: weak; cosmological parameters; large-scale structure of Universe ID MATTER POWER SPECTRUM; BARYON ACOUSTIC-OSCILLATIONS; 100 SQUARE DEGREES; SDSS-III; PARAMETER CONSTRAINTS; PRECISION COSMOLOGY; SHEAR MEASUREMENT; WEAK; CFHTLENS; MODEL AB We present cosmological constraints from the Dark Energy Survey (DES) using a combined analysis of angular clustering of red galaxies and their cross-correlation with weak gravitational lensing of background galaxies. We use a 139 deg(2) contiguous patch of DES data from the Science Verification (SV) period of observations. Using large-scale measurements, we constrain the matter density of the Universe as Omega(m) = 0.31 +/- 0.09 and the clustering amplitude of the matter power spectrum as sigma(8) = 0.74 +/- 0.13 after marginalizing over seven nuisance parameters and three additional cosmological parameters. This translates into S-8 = sigma(8)(Omega(m)/0.3)(0.16) = 0.74 +/- 0.12 for our fiducial lens redshift bin at 0.35 < z < 0.5, while S-8 = 0.78 +/- 0.09 using two bins over the range 0.2 < z < 0.5. We study the robustness of the results under changes in the data vectors, modelling and systematics treatment, including photometric redshift and shear calibration uncertainties, and find consistency in the derived cosmological parameters. We show that our results are consistent with previous cosmological analyses from DES and other data sets and conclude with a joint analysis of DES angular clustering and galaxy-galaxy lensing with Planck Cosmic Microwave Background data, baryon accoustic oscillations and Supernova Type Ia measurements. C1 [Kwan, J.; Clampitt, J.; Jain, B.; Bernstein, G. M.; Jarvis, M.; Suchyta, E.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Sanchez, C.; Miquel, R.; Fernandez, E.; Fosalba, P.] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Barcelona, Spain. [Blazek, J.; Ross, A. J.; Honscheid, K.; Martini, P.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Crocce, M.; Gaztanaga, E.] IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain. [Zuntz, J.; MacCrann, N.; Troxel, M. A.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England. [Amara, A.; Hartley, W. G.; Kacprzak, T.] ETH, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland. [Becker, M. R.; DeRose, J.; Wechsler, R. H.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. [Becker, M. R.; DeRose, J.; Gruen, D.; Krause, E.; Rykoff, E. S.; Wechsler, R. H.; Cunha, C. E.; Roodman, A.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA. [Dodelson, S.; Allam, S.; Diehl, H. T.; Finley, D. A.; Flaugher, B.; Frieman, J.; Gutierrez, G.; Nord, B.; Scarpine, V.; Soares-Santos, M.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. [Dodelson, S.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Dodelson, S.] Univ Chicago, Dept Phys, 5640 South Ellis Ave, Chicago, IL 60637 USA. [Eifler, T. F.; Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Giannantonio, T.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Giannantonio, T.] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England. [Gruen, D.; Rykoff, E. S.; Wechsler, R. H.; Burke, D. L.; Reil, K.; Roodman, A.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Kirk, D.; Abdalla, F. B.; Benoit-Levy, A.; Brooks, D.; Doel, P.; Lahav, O.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Park, Y.; Rozo, E.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. [Sheldon, E.] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA. [Abbott, T. M. C.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile. [Abdalla, F. B.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa. [Benoit-Levy, A.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Benoit-Levy, A.] UPMC Univ Paris 06, Sorbonne Univ, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Rosell, A. Carnero; da Costa, L. N.; Maia, M. A. G.; Sobreira, F.] Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Rosell, A. Carnero; da Costa, L. N.; Maia, M. A. G.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [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. [D'Andrea, C. B.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [D'Andrea, C. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Desai, S.; Dietrich, J. P.; Mohr, J. J.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Desai, S.; Dietrich, J. P.; Mohr, J. J.] Ludwig Maximilians Univ Munchen, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Evrard, A. E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Evrard, A. E.; Gerdes, D. W.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Honscheid, K.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Lima, M.] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil. [Marshall, J. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Martini, P.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Melchior, P.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. [Mohr, J. J.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England. [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, BR-01140070 Sao Paulo, Brazil. [Suchyta, E.] Oak Ridge Natl Lab, Comp Sci & Math Div, Oak Ridge, TN 37831 USA. [Vikram, V.] Argonne Natl Lab, 9700 South Cass Ave, Lemont, IL 60439 USA. RP Kwan, J (reprint author), Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. EM kjuliana@physics.upenn.edu FU US Department of Energy; US National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Center for Particle Cosmology at the University of Pennsylvania; Warren Center at the University of Pennsylvania; 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]; European Union; Argonne National Laboratory; University of California at Santa Cruz; University of Cambridge; 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; associated Excellence Cluster Universe; University of Michigan; National Optical Astronomy Observatory; University of Nottingham; Ohio State University; University of Pennsylvania; University of Portsmouth; University of Sussex; Texas AM University; SLAC National Accelerator Laboratory; Stanford University; Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid FX Funding for the DES Projects has been provided by the US Department of Energy, the US National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Center for Particle Cosmology and the Warren Center at the University of Pennsylvania, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia e Tecnologia, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the DES.; The DES data management system is supported by the National Science Foundation under Grant no. 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. NR 100 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2017 VL 464 IS 4 BP 4045 EP 4062 DI 10.1093/mnras/stw2464 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EK2TV UT WOS:000393780500021 ER PT J AU Wakeford, HR Visscher, C Lewis, NK Kataria, T Marley, MS Fortney, JJ Mandell, AM AF Wakeford, H. R. Visscher, C. Lewis, N. K. Kataria, T. Marley, M. S. Fortney, J. J. Mandell, A. M. TI High-temperature condensate clouds in super-hot Jupiter atmospheres SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE planets and satellites: atmospheres; planets and satellites: individual: WASP; 12b ID MASS DWARF STARS; GIANT PLANETS; BROWN DWARF; MODEL ATMOSPHERES; SUBSTELLAR ATMOSPHERES; T-DWARF; CHEMISTRY; CIRCULATION; WASP-12B; DUST AB Deciphering the role of clouds is central to our understanding of exoplanet atmospheres, as they have a direct impact on the temperature and pressure structure, and observational properties of the planet. Super-hot Jupiters occupy a temperature regime similar to low-mass M-dwarfs, where minimal cloud condensation is expected. However, observations of exoplanets such as WASP-12b (T-eq similar to 2500 K) result in a transmission spectrum indicative of a cloudy atmosphere. We re-examine the temperature and pressure space occupied by these super-hot Jupiter atmospheres, to explore the role of the initial Al-and Ti-bearing condensates as the main source of cloud material. Due to the high temperatures, a majority of the more common refractory material is not depleted into deeper layers and would remain in the vapour phase. The lack of depletion into deeper layers means that these materials with relatively low cloud masses can become significant absorbers in the upper atmosphere. We provide condensation curves for the initial Al-and Ti-bearing condensates which may be used to provide quantitative estimates of the effect of metallicity on cloud masses, as planets with metal-rich hosts potentially form more opaque clouds because more mass is available for condensation. Increased metallicity also pushes the point of condensation to hotter, deeper layers in the planetary atmosphere further increasing the density of the cloud. We suggest that planets around metal-rich hosts are more likely to have thick refractory clouds, and discuss the implication on the observed spectra of WASP-12b. C1 [Wakeford, H. R.; Mandell, A. M.] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. [Visscher, C.] Dordt Coll, Dept Chem, Sioux Ctr, IA 51250 USA. [Lewis, N. K.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Kataria, T.] NASA, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Marley, M. S.] NASA, Ames Res Ctr, MS 245-5, Moffett Field, CA 94035 USA. [Fortney, J. J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Wakeford, HR (reprint author), NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA.; Visscher, C (reprint author), Dordt Coll, Dept Chem, Sioux Ctr, IA 51250 USA.; Lewis, NK (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM hannah.wakeford@nasa.gov; channon.visscher@dordt.edu; lewis@stsci.edu FU National Science Foundation (NSF) [AST-1312305] FX HRW acknowledges support by an appointment to the National Aeronautics and Space Administration (NASA) Postdoctoral Program at Goddard Space Flight Center, administered by ORAU and Universities Space Research Association (USRA) through a contract with NASA. CV acknowledges support by National Science Foundation (NSF) grant AST-1312305. The authors would also like to thank the anonymous referee for their comments and suggestions. NR 60 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2017 VL 464 IS 4 BP 4247 EP 4254 DI 10.1093/mnras/stw2639 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EK2TV UT WOS:000393780500033 ER PT J AU Baring, MG Bottcher, M Summerlin, EJ AF Baring, Matthew G. Bottcher, Markus Summerlin, Errol J. TI Probing acceleration and turbulence at relativistic shocks in blazar jets SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE acceleration of particles; plasmas; shock waves; turbulence; galaxies: active; galaxies: jets ID GAMMA-RAY EMISSION; ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTION; MAGNETIC-FIELD GENERATION; BL LACERTAE OBJECTS; NONLINEAR PARTICLE-ACCELERATION; EXTRAGALACTIC BACKGROUND LIGHT; ELECTRON-POSITRON PLASMAS; MONTE-CARLO SIMULATIONS; LARGE-AREA TELESCOPE AB Diffusive shock acceleration (DSA) at relativistic shocks is widely thought to be an important acceleration mechanism in various astrophysical jet sources, including radio-loud active galactic nuclei such as blazars. Such acceleration can produce the non-thermal particles that emit the broad-band continuum radiation that is detected from extragalactic jets. An important recent development for blazar science is the ability of Fermi-Large Area Telescope spectroscopy to pin down the shape of the distribution of the underlying non-thermal particle population. This paper highlights how multiwavelength spectra spanning optical to X-ray to gamma-ray bands can be used to probe diffusive acceleration in relativistic, oblique, magnetohydrodynamic (MHD) shocks in blazar jets. Diagnostics on the MHD turbulence near such shocks are obtained using thermal and non-thermal particle distributions resulting from detailed Monte Carlo simulations of DSA. These probes are afforded by the characteristic property that the synchrotron nu F-nu peak energy does not appear in the gamma-ray band above 100 MeV. We investigate self-consistently the radiative synchrotron and inverse Compton signatures of the simulated particle distributions. Important constraints on the diffusive mean free paths of electrons, and the level of electromagnetic field turbulence are identified for three different case study blazars, Mrk 501, BL Lacertae and AO 0235+ 164. The X-ray excess of AO 0235+ 164 in a flare state can be modelled as the signature of bulk Compton scattering of external radiation fields, thereby tightly constraining the energy-dependence of the diffusion coefficient for electrons. The concomitant interpretations that turbulence levels decline with remoteness from jet shocks, and the probable significant role for non-gyroresonant diffusion, are posited. C1 [Baring, Matthew G.] Rice Univ, Dept Phys & Astron MS 108, 6100 Main St, Houston, TX 77251 USA. [Bottcher, Markus] North West Univ, Ctr Space Res, Potchefstroom Campus, ZA-2520 Potchefstroom, South Africa. [Summerlin, Errol J.] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Code 672, Greenbelt, MD 20770 USA. RP Baring, MG (reprint author), Rice Univ, Dept Phys & Astron MS 108, 6100 Main St, Houston, TX 77251 USA.; Bottcher, M (reprint author), North West Univ, Ctr Space Res, Potchefstroom Campus, ZA-2520 Potchefstroom, South Africa.; Summerlin, EJ (reprint author), NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Code 672, Greenbelt, MD 20770 USA. EM baring@rice.edu; Markus.Bottcher@nwu.ac.za; errol.summerlin@nasa.gov FU NASA [NNX10AC79G]; Department of Energy [DE-SC0001481]; South African Research Chairs Initiative of the Department of Science and Technology [64789]; National Research Foundation2 of South Africa FX The authors thank Ana Pichel for providing a pre-publication release of VERITAS spectral data for the 2009 May flare episode of Mrk 501 that served as a guide for our MW studies. We thank Alan Marscher and Greg Madejski for a number of helpful comments and careful reading of the manuscript, and the anonymous referee for constructive suggestions that polished the presentation. MGB and MB are grateful to NASA for partial support for this research through the Astrophysics Theory Program, grant NNX10AC79G. MGB also acknowledges support from the Department of Energy under grant DE-SC0001481 during the early stages of this programme. This work is based on research supported by the South African Research Chairs Initiative (grant no. 64789) of the Department of Science and Technology and the National Research Foundation2 of South Africa. NR 118 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 FEB PY 2017 VL 464 IS 4 BP 4875 EP 4894 DI 10.1093/mnras/stw2344 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EK2TV UT WOS:000393780500080 ER PT J AU Granot, J Gill, R Younes, G Gelfand, J Harding, A Kouveliotou, C Baring, MG AF Granot, Jonathan Gill, Ramandeep Younes, George Gelfand, Josef Harding, Alice Kouveliotou, Chryssa Baring, Matthew G. TI Learning about the magnetar Swift J1834.9-0846 from its wind nebula SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE diffusion; hydrodynamics; magnetic fields; stars: magnetars; stars: winds, outflows; ISM: supernova remnants ID X-RAY PULSAR; LARGE-AREA TELESCOPE; XMM-NEWTON OBSERVATIONS; LARGE TORQUE VARIATIONS; SOFT GAMMA-REPEATERS; SUPERNOVA-REMNANTS; NEUTRON-STARS; CRAB-NEBULA; SGR 1806-20; MOLECULAR CLOUDS AB The first wind nebula around a magnetar was recently discovered in X-rays around Swift J1834.9-0846. We study this magnetar's global energetics and the properties of its particle wind or outflows. At a distance of similar to 4 kpc, Swift J1834.9-0846 is located at the centre of the supernova remnant (SNR) W41 whose radius is similar to 19 pc, an order of magnitude larger than that of the X-ray nebula (similar to 2 pc). The association with SNR W41 suggests a common age of similar to 5-100 kyr, while its spin-down age is 4.9 kyr. A small natal kick velocity may partly explain why a wind nebula was detected around this magnetar but not around other magnetars, most of which appear to have larger kick velocities and may have exited their birth SNR. We find that the GeV and TeV source detected by Fermi/Large Area Telescope (LAT) and High Energy Spectroscopic System (H.E.S.S.), respectively, of radius similar to 11 pc is most likely of hadronic origin. The dynamics and internal structure of the nebula are examined analytically to explain the nebula's current properties. Its size may naturally correspond to the diffusion-dominated cooling length of the X-ray emitting e(+)e(-) pairs. This may also account for the spectral softening of the X-ray emission from the nebula's inner to outer parts. The analysis of the X-ray synchrotron nebula implies that (i) the nebular magnetic field is greater than or similar to 11 mu G (and likely less than or similar to 30 mu G), and (ii) the nebula is not powered predominantly by the magnetar's quiescent spin-down-powered MHD wind, but by other outflows that contribute most of its energy. The latter are most likely associated with the magnetar's bursting activity, and possibly dominated by outflows associated with its past giant flares. The energy source for the required outflows cannot be the decay of the magnetar's dipole field alone, and is most likely the decay of its much stronger internal magnetic field. C1 [Granot, Jonathan; Gill, Ramandeep] Open Univ Israel, Dept Nat Sci, 1 Univ Rd,POB 808, IL-4353701 Raanana, Israel. [Younes, George; Kouveliotou, Chryssa] George Washington Univ, Dept Phys, Washington, DC 20052 USA. [Gelfand, Josef] NYU Abu Dhabi, POB 903, New York, NY 10276 USA. [Harding, Alice] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Baring, Matthew G.] Rice Univ, Dept Phys & Astron, MS-108,POB 1892, Houston, TX 77251 USA. RP Granot, J; Gill, R (reprint author), Open Univ Israel, Dept Nat Sci, 1 Univ Rd,POB 808, IL-4353701 Raanana, Israel. EM granot@openu.ac.il; rsgill.rg@gmail.com FU Israeli Science Foundation [719/14]; Open University of Israel FX We would like to thank Yuri Lyubarsky, Dale Frail, Lara Nava for very useful discussions that helped to improve the quality of this work, and George Pavlov for useful comments on the manuscript. We are very grateful to Oleg Kargaltsev for a thorough review of the article and insightful discussions on PWNe. JG and RG acknowledge support from the Israeli Science Foundation under Grant No. 719/14. RG is supported by an Outstanding Postdoctoral Researcher Fellowship at the Open University of Israel. NR 119 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2017 VL 464 IS 4 BP 4895 EP 4926 DI 10.1093/mnras/stw2554 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EK2TV UT WOS:000393780500081 ER PT J AU Wolz, L Blake, C Abdalla, FB Anderson, CJ Chang, TC Li, YC Masui, KW Switzer, E Pen, UL Voytek, TC Yadav, J AF Wolz, L. Blake, C. Abdalla, F. B. Anderson, C. J. Chang, T. -C. Li, Y. -C. Masui, K. W. Switzer, E. Pen, U. -L. Voytek, T. C. Yadav, J. TI Erasing the Milky Way: new cleaning technique applied to GBT intensity mapping data SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; methods: statistical; cosmology: observations; large-scale structure of Universe; radio lines: galaxies ID DIGITAL SKY SURVEY; INDEPENDENT COMPONENT ANALYSIS; DARK ENERGY SURVEY; ACOUSTIC-OSCILLATIONS; POWER SPECTRUM; 21-CM EMISSION; DATA RELEASE; TO 0.8; GALAXY; MAPS AB We present the first application of a new foreground removal pipeline to the current leading HI intensity mapping data set, obtained by the Green Bank Telescope (GBT). We study the 15- and 1-h-field data of the GBT observations previously presented in Mausui et al. and Switzer et al., covering about 41 deg(2) at 0.6 < z < 1.0, for which cross-correlations may be measured with the galaxy distribution of the WiggleZ Dark Energy Survey. In the presented pipeline, we subtract the Galactic foreground continuum and the point-source contamination using an independent component analysis technique (FASTICA), and develop a Fourier-based optimal estimator to compute the temperature power spectrum of the intensity maps and cross-correlation with the galaxy survey data. We show that FASTICA is a reliable tool to subtract diffuse and point-source emission through the non-Gaussian nature of their probability distributions. The temperature power spectra of the intensity maps are dominated by instrumental noise on small scales which FASTICA, as a conservative subtraction technique of non-Gaussian signals, cannot mitigate. However, we determine similar GBT-WiggleZ cross-correlation measurements to those obtained by the singular value decomposition (SVD) method, and confirm that foreground subtraction with FASTICA is robust against 21 cm signal loss, as seen by the converged amplitude of these cross-correlation measurements. We conclude that SVD and FASTICA are complementary methods to investigate the foregrounds and noise systematics present in intensity mapping data sets. C1 [Wolz, L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Wolz, L.] Univ Sydney, Sch Phys, ARC Ctr Excellence All Sky Astrophys CAASTRO, Bldg A28, Sydney, NSW 2006, Australia. [Blake, C.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, POB 218, Hawthorn, Vic 3122, Australia. [Abdalla, F. B.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Anderson, C. J.] Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA. [Chang, T. -C.] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. [Li, Y. -C.] Chinese Acad Sci, Natl Astron Observ, 20A Datun Rd, Beijing 100012, Peoples R China. [Masui, K. W.] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada. [Masui, K. W.] Canadian Inst Adv Res, CIFAR Program Cosmol & Grav, Toronto, ON M5G 1Z8, Canada. [Switzer, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pen, U. -L.] Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 3H8, Canada. [Voytek, T. C.] Univ KwaZulu Natal, Sch Chem & Phys, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Yadav, J.] Univ Delhi, Sri Aurobindo Coll, New Delhi 110017, India. RP Wolz, L (reprint author), Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia.; Wolz, L (reprint author), Univ Sydney, Sch Phys, ARC Ctr Excellence All Sky Astrophys CAASTRO, Bldg A28, Sydney, NSW 2006, Australia. EM laura.wolz@unimelb.edu.au FU Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; Australian Research Council FX We thank the anonymous referee for their useful comments and suggestions. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. CB acknowledges the support of the Australian Research Council through the award of a Future Fellowship. NR 38 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 FEB PY 2017 VL 464 IS 4 BP 4938 EP 4949 DI 10.1093/mnras/stw2556 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EK2TV UT WOS:000393780500083 ER PT J AU Russell, CMP Wang, QD Cuadra, J AF Russell, Christopher M. P. Wang, Q. Daniel Cuadra, Jorge TI Modelling the thermal X-ray emission around the Galactic Centre from colliding Wolf-Rayet winds SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE Galaxy: centre; stars: Wolf-Rayet; stars: winds; outflows; hydrodynamics; radiative transfer; X-rays: stars ID STELLAR WINDS; BLACK-HOLE; CENTRAL PARSEC; STARS; ACCRETION; SGR; GALAXY; ABSORPTION; SYSTEMS; ORBITS AB The Galactic Centre is a hotbed of astrophysical activity, with the injection of wind material from similar to 30 massive Wolf-Rayet (WR) stars orbiting within 12 arcsec of the supermassive black hole (SMBH) playing an important role. Hydrodynamic simulations of such colliding and accreting winds produce a complex density and temperature structure of cold wind material shocking with the ambient medium, creating a large reservoir of hot, X-ray-emitting gas. This work aims to confront the 3 Ms of Chandra X-ray Visionary Program observations of this diffuse emission by computing the X-ray emission from these hydrodynamic simulations of the colliding WR winds, amid exploring a variety of SMBH feedback mechanisms. The major success of the model is that it reproduces the spectral shape from the 2-5 arcsec ring around the SMBH, where most of the stellar wind material that is ultimately captured by Sgr A* is shock-heated and thermalized. This naturally explains that the hot gas comes from colliding WR winds, and that the wind speeds of these stars are, in general, well constrained. The flux level of these spectra, as well as 12 x 12-arcsec(2) images of 4-9 keV, shows that the X-ray flux is tied to the SMBH feedback strength; stronger feedback clears out more hot gas, thereby decreasing the thermal X-ray emission. The model in which Sgr A* produced an intermediate-strength outflow during the last few centuries best matches the observations to within about 10 per cent, showing that SMBH feedback is required to interpret the X-ray emission in this region. C1 [Russell, Christopher M. P.] NASA, Xray Astrophys Lab, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. [Wang, Q. Daniel] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Cuadra, Jorge] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 7820436, Chile. RP Russell, CMP (reprint author), NASA, Xray Astrophys Lab, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. EM crussell@udel.edu FU NASA via the SAO/CXC grant [TM3-14006X]; CONICYT-Chile through FONDECYT grant [1141175]; CONICYT-Chile through Basal grant [PFB0609]; CONICYT-Chile through Anillo grant [ACT1101] FX We thank the anonymous referee for helpful comments that significantly improved this paper. We acknowledge M. A. Leutenegger for providing his code to tabulate X-ray opacities for given abundances and ionization states. CMPR is supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered formerly by the Oak Ridge Associated Universities, and currently by the Universities Space Research Association, through a contract with NASA. QDW acknowledges support by NASA via the SAO/CXC grant TM3-14006X. JC acknowledges support from CONICYT-Chile through FONDECYT (1141175), Basal (PFB0609), and Anillo (ACT1101) grants. NR 36 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 FEB PY 2017 VL 464 IS 4 BP 4958 EP 4965 DI 10.1093/mnras/stw2584 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EK2TV UT WOS:000393780500085 ER PT J AU Strutner, SM Garcia, A Ula, S Adamo, C Richards, WL Wang, K Schlom, DG Carman, GP AF Strutner, Scott M. Garcia, Adam Ula, Sabina Adamo, Carolina Richards, W. Lance Wang, Kang Schlom, Darrell G. Carman, Greg P. TI Index of refraction changes under magnetic field observed in La0.66Sr0.33MnO3 correlated to the magnetorefractive effect SO OPTICAL MATERIALS EXPRESS LA English DT Article ID THIN-FILMS AB The magnetorefractive effect is a change in a sample's reflectivity with applied magentic field. This is caused by the material's index of refraction's sensitivity to magnetic fields. However, measurements of the index of refraction as a function of applied magnetic field have not been previously published. This experimental study measures both the magnetorefractive effect and the index of refraction as a function of applied magnetic field and temperature in a 70 nm thick film of lanthanum strontium manganite La0.66Sr0.33MnO3. Index of refraction characterizations were performed with 633 nm light in magnetic fields ranging from -3 kOe to 3 kOe and near the Curie point, at temperatures from 278 K to 308 K. (C) 2017 Optical Society of America C1 [Strutner, Scott M.; Garcia, Adam; Ula, Sabina; Carman, Greg P.] Univ Calif Los Angeles, Dept Mech & Aerosp Engn, Los Angeles, CA 90095 USA. [Adamo, Carolina; Schlom, Darrell G.] Cornell Univ, Dept Mat Sci & Engn, Ithaca, NY 14853 USA. [Richards, W. Lance] NASA, Armstrong Flight Res Ctr, Edwards AFB, CA 93523 USA. [Wang, Kang] Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA. [Schlom, Darrell G.] Cornell Univ, Kavli Inst Cornell Nanoscale Sci, Ithaca, NY 14853 USA. RP Strutner, SM (reprint author), Univ Calif Los Angeles, Dept Mech & Aerosp Engn, Los Angeles, CA 90095 USA. EM sstrutner@gmail.com FU National Aeronautics and Space Administration (NASA); Aero Institute [PO AERO 661]; Translational Applications of Nanoscale Multiferroic Systems (TANMS) Engineering Research Center (ERC) - National Science Foundation (NSF) [EEC 1160504] FX The authors thank the National Aeronautics and Space Administration (NASA) and the Aero Institute for funding this work through PO AERO 661. The authors thank the Translational Applications of Nanoscale Multiferroic Systems (TANMS) Engineering Research Center (ERC) funded by the National Science Foundation (NSF) through Cooperative Agreement Award EEC 1160504 for funding the interns who worked on this project. NR 18 TC 0 Z9 0 U1 0 U2 0 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 2159-3930 J9 OPT MATER EXPRESS JI Opt. Mater. Express PD FEB 1 PY 2017 VL 7 IS 2 BP 468 EP 476 DI 10.1364/OME.7.000468 PG 9 WC Materials Science, Multidisciplinary; Optics SC Materials Science; Optics GA EK8KS UT WOS:000394173200019 ER PT J AU Lepping, RP Berdichevsky, DB Wu, CC AF Lepping, R. P. Berdichevsky, D. B. Wu, C. -C. TI Average Magnetic Field Magnitude Profiles of Wind Magnetic Clouds as a Function of Closest Approach to the Clouds' Axes and Comparison to Model SO SOLAR PHYSICS LA English DT Article ID VOYAGER 2 OBSERVATIONS; SOLAR-WIND; 1 AU; FLUX ROPES; PARAMETERS; EXPANSION; SHOCK AB We examine the average magnetic field magnitude (|B| = B) within magnetic clouds (MCs) observed by the Wind spacecraft from 1995 to July 2015 to understand the difference between this B and the ideal B-profiles expected from using the static, constant-a, force-free, cylindrically symmetric model for MCs of Lepping, Jones, and Burlaga (J. Geophys. Res. 95, 11957, 1990, denoted here as the LJB model). We classify all MCs according to an assigned quality, Q(0) (= 1, 2, 3, for excellent, good, and poor). There are a total of 209 MCs and 124 when only Q0 = 1, 2 cases are considered. The average normalized field with respect to the closest approach (CA) is stressed, where we separate cases into four CA sets centered at 12.5 %, 37.5 %, 62.5 %, and 87.5 % of the average radius; the averaging is done on a percentage-duration basis to treat all cases the same. Normalized B means that before averaging, the B for each MC at each point is divided by the LJB model-estimated B for the MC axis, B-0. The actual averages for the 209 and 124 MC sets are compared to the LJB model, after an adjustment for MC expansion (e. g. Lepping et al. in Ann. Geophys. 26, 1919, 2008). This provides four separate difference-relationships, each fitted with a quadratic (Quad) curve of very small sigma. Interpreting these Quad formulae should provide a comprehensive view of the variation in normalized B throughout the average MC, where we expect external front and rear compression to be part of its explanation. These formulae are also being considered for modifying the LJB model. This modification will be used in a scheme for forecasting the timing and magnitude of magnetic storms caused by MCs. Extensive testing of the Quad formulae shows that the formulae are quite useful in correcting individual MC B-profiles, especially for the first approximate to 1/3 of these MCs. However, the use of this type of B correction constitutes a (slight) violation of the force-free assumption used in the original LJB MC model. C1 [Lepping, R. P.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Berdichevsky, D. B.] Univ Dist Columbia, Dept Elect & Comp Engn, Washington, DC 20008 USA. [Wu, C. -C.] Naval Res Lab, Washington, DC 20735 USA. RP Wu, CC (reprint author), Naval Res Lab, Washington, DC 20735 USA. EM Ronald.P.Lepping@gmail.com; Chin-Chun.Wu@nrl.navy.mil NR 29 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD FEB PY 2017 VL 292 IS 2 AR 27 DI 10.1007/s11207-016-1040-9 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EM6BV UT WOS:000395398700002 ER PT J AU Schultz, CJ Carey, LD Schultz, EV Blakeslee, RJ AF Schultz, Christopher J. Carey, Lawrence D. Schultz, Elise V. Blakeslee, Richard J. TI Kinematic and Microphysical Significance of Lightning Jumps versus Nonjump Increases in Total Flash Rate SO WEATHER AND FORECASTING LA English DT Article ID DOPPLER RADAR OBSERVATIONS; SUPERCELL STORM; PRECIPITATION DEVELOPMENT; MULTIPARAMETER RADAR; SEVERE THUNDERSTORMS; CONVECTIVE STORM; SEVERE WEATHER; MAPPING ARRAY; ELECTRIFICATION; EVOLUTION AB Thirty-nine thunderstorms are examined using multiple-Doppler, polarimetric, and total lightning observations to understand the role ofmixed-phase kinematics and microphysics in the development of lightning jumps. This sample size is larger than those of previous studies on this topic. The principal result of this study is that lightning jumps are a result of mixed-phase updraft intensification. Larger increases in intense updraft volume (>= 10ms(-1)) and larger changes in peak updraft speed are observed prior to lightning jump occurrence when compared to other nonjump increases in total flash rate. Wilcoxon-Mann-Whitney rank sum testing yields p values <= 0.05, indicating statistical independence between lightning jump and nonjump distributions for these two parameters. Similar changes inmixed-phase graupel mass magnitude are observed prior to lightning jumps and nonjump increases in total flash rate. The p value for the graupel mass change is p =0.096, so jump and nonjump distributions for the graupel mass change are not found to be statistically independent using the p = 0.05 significance level. The timing of updraft volume, speed, and graupel mass increases is found to be 4-13min in advance of lightning jump occurrence. Also, severe storms without lightning jumps lack robust mixed-phase updrafts, demonstrating that mixed-phase updrafts are not always a requirement for severe weather occurrence. Therefore, the results of this study show that lightning jump occurrences are coincident with larger increases in intense mixed-phase updraft volume and peak updraft speed than smaller nonjump increases in total flash rate. C1 [Schultz, Christopher J.; Carey, Lawrence D.] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35899 USA. [Schultz, Christopher J.; Blakeslee, Richard J.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35811 USA. [Schultz, Elise V.] Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35899 USA. RP Schultz, CJ (reprint author), Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35899 USA.; Schultz, CJ (reprint author), NASA, Marshall Space Flight Ctr, Huntsville, AL 35811 USA. EM christopher.j.schultz@nasa.gov FU Dr. Steven J. Goodman and GOES-R Risk Reduction Research; NASA Pathways Intern Program at Marshall Space Flight Center FX The authors would like to acknowledge Dr. Steven J. Goodman and GOES-R Risk Reduction Research funding for support of this research. CJS would like to acknowledge support from the NASA Pathways Intern Program at Marshall Space Flight Center, namely Julie Clift and Christopher Randall. The authors are thankful for technical support with radar data processing from Lamont Bain, Retha Mecikalski, and Danielle Kozlowski for parts during the 11 June and 10 April events. Furthermore, productive conversations with Drs. Themis Chronis, Phil Bitzer, Hugh Christian, Walt Petersen, Kristin Calhoun, and Eric Bruning benefited the outcomes of this research. We also gratefully acknowledge the technical support for maintenance of the operational instrumentation, namely Dustin Phillips, Patrick Gatlin, and Chris Phillips for the maintenance of the ARMOR radar. The authors would also like to recognize Jeff Bailey and Blair Breitreiter for the continued maintenance of the North Alabama Lightning Mapping Array. Finally, the authors thank Editor Dr. Paul Markowski and two anonymous reviewers for their helpful comments, which improved the content and technical writing of this manuscript. NR 68 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0882-8156 EI 1520-0434 J9 WEATHER FORECAST JI Weather Forecast. PD FEB PY 2017 VL 32 IS 1 BP 275 EP 288 DI 10.1175/WAF-D-15-0175.1 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EM8JN UT WOS:000395557500018 ER PT J AU Laurila, T Sainio, S Jiang, H Isoaho, N Koehne, JE Etula, J Koskinen, J Meyyappan, M AF Laurila, Tomi Sainio, Sami Jiang, Hua Isoaho, Noora Koehne, Jessica E. Etula, Jarkko Koskinen, Jari Meyyappan, M. TI Application-Specific Catalyst Layers: Pt-Containing Carbon Nanofibers for Hydrogen Peroxide Detection SO ACS OMEGA LA English DT Article ID OXYGEN REDUCTION REACTION; ELECTROCHEMICAL DETECTION; PLATINUM NANOPARTICLES; TA-C; NANOTUBES; GRAPHENE; ELECTRODE; SENSOR; IMMOBILIZATION; BIOSENSORS AB Complete removal of metal catalyst particles from carbon nanofibers (CNFs) and other carbon nanostructures is extremely difficult, and the envisioned applications may be compromised by the left-over impurities. To circumvent these problems, one should use, wherever possible, such catalyst materials that are meant to remain in the structure and have some application-specific role, making any removal steps unnecessary. Thus, as a proof-of-concept, we present here a nanocarbon-based material platform for electrochemical hydrogen peroxide measurement utilizing a Pt catalyst layer to grow CNFs with intact Pt particles at the tips of the CNFs. Backed by careful scanning transmission electron microscopy analysis, we show that this material can be readily realized with the Pt catalyst layer thickness impacting the resulting structure and also present a growth model to explain the evolution of the different types of structures. In addition, we show by electrochemical analysis that the material exhibits characteristic features of Pt in cyclic voltammetry and it can detect very small amounts of hydrogen peroxide with very fast response times. Thus, the present sensor platform provides an interesting electrode material with potential for biomolecule detection and in fuel cells and batteries. In the wider range, we propose a new approach where the selection of catalytic particles used for carbon nanostructure growth is made so that (i) they do not need to be removed and (ii) they will have essential role in the final application. C1 [Laurila, Tomi; Sainio, Sami; Isoaho, Noora] Aalto Univ, Sch Elect Engn, Dept Elect Engn & Automat, Tietotie 3, Espoo 02150, Finland. [Jiang, Hua] Aalto Univ, Sch Sci, Dept Appl Phys, Puumiehenkuja 2, Espoo 02150, Finland. [Koehne, Jessica E.; Meyyappan, M.] NASA Ames Res Ctr, Ctr Nanotechnol, Mountain View, CA 94035 USA. [Etula, Jarkko; Koskinen, Jari] Aalto Univ, Sch Chem Technol, Dept Chem & Mat Sci, Kemistintie 1, Espoo 02150, Finland. RP Laurila, T (reprint author), Aalto Univ, Sch Elect Engn, Dept Elect Engn & Automat, Tietotie 3, Espoo 02150, Finland. EM tomi.laurila@aalto.fi FU Academy of Finland [285015, 285526] FX The authors T.L. and S.S. acknowledge funding from Academy of Finland (grant numbers 285015 and 285526). Professor Krisztian Kordas and Olli Pitkanen from University of Oulu are acknowledged for Raman analyses. We acknowledge the provision of facilities and technical support by Aalto University at OtaNano - Nanomicroscopy Center (Aalto-NMC). NR 56 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 2470-1343 J9 ACS OMEGA JI ACS Omega PD FEB PY 2017 VL 2 IS 2 BP 496 EP 507 DI 10.1021/acsomega.6b00441 PG 12 WC Chemistry, Multidisciplinary SC Chemistry GA EN2TO UT WOS:000395863300015 ER PT J AU Flexas, MM Arias, MR Ojeda, MA AF Flexas, Mar M. Arias, Mariano R. Ojeda, Miguel A. TI Hydrography and dynamics of Port Foster, Deception Island, Antarctica SO ANTARCTIC SCIENCE LA English DT Article DE coastal-trapped waves; currents; tides ID COASTAL-TRAPPED WAVES; SOUTH SHETLAND ISLANDS; CURRENTS; ECOSYSTEM AB The circulation and water masses of Port Foster, Deception Island, were studied using conductivity-temperature-depth stations inside and outside the semi-enclosed bay and an array of bottom temperature sensors moored around the perimeter of the bay over two weeks in the summer of 2012. Inside Port Foster, the water column is divided into two layers separated by a temperature-forced, seasonal pycnocline at similar to 40-60m. The circulation of the upper layer is in an anticlockwise direction, with mean geostrophic currents of similar to 0.04-0.10ms(-1). The lower layer, from similar to 60 m to the seabed, shows coastal-trapped waves travelling in a clockwise direction, possibly triggered by local wind gusts. Local sea ice melt in areas surrounding the underwater hot springs of Pendulum Cove appears as a fresh, warm anomaly down to 30m. C1 [Flexas, Mar M.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Arias, Mariano R.] Univ Extremadura, Fac Ciencias, Ave Elvas S-N, Badajoz 06006, Spain. [Ojeda, Miguel A.] CMIMA CSIC, Unidad Tecnol Marina, Passeig Maritim Barceloneta 37-39, Barcelona 08003, Spain. [Flexas, Mar M.] CALTECH, 1200 East Calif Blvd, Pasadena, CA 91125 USA. RP Flexas, MM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.; Flexas, MM (reprint author), CALTECH, 1200 East Calif Blvd, Pasadena, CA 91125 USA. EM marf@caltech.edu FU Spanish Research and Innovation (I+D+i) Program [CTM2009-08287-E/ANT, CTM2010-09635-E, CTM2011-14056-E]; NASA FX We thank Manuel Berrocoso and the Laboratory of Astronomy, Geodesy and Cartography of the University of Cadiz (LAGC, Spain), in particular Amos de Gil and Luis Miguel Peci, for their help in building the temperature moorings and for providing the highresolution elevation chart of Deception Island. We wish to thank CO Jaime Cervera, officers and crew on board RV Hesperides and CO Enrique Valdes, officers and crew on board RV Las Palmas for their help in making the oceanographic cruises successful. We are grateful to the military personnel at the Gabriel de Castilla Spanish Base for their support in the deployment and recovery of the bottom temperature sensors; the Spanish Marine Hydrographic Institute (IHM), and especially Captain Daniel Gonzalez-Aller and his crew, for providing the high-resolution bathymetry of Port Foster; the Spanish Meteorological Agency (AEMET) for providing the meteorological data from station WMO-89070; and Rafael Benitez for his help with Fig. 1. This work was supported by the Spanish Research and Innovation (I+D+i) Program, through grant numbers CTM2009-08287-E/ANT, CTM2010-09635-E and CTM2011- 14056-E, and by the NASA Postdoctoral Program administered by Oak Ridge Associated Universities. This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This is a contribution to the ECCOIcES project funded by the NASA Modeling, Analysis, and Prediction (MAP) programme. We are grateful to two anonymous reviewers and to the editor for their detailed comments that greatly improved the original manuscript. This work is dedicated to Dr Pablo Sangra Inciarte, outstanding scientist and inspiring teacher. NR 27 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0954-1020 EI 1365-2079 J9 ANTARCT SCI JI Antarct. Sci. PD FEB PY 2017 VL 29 IS 1 BP 83 EP 93 DI 10.1017/S0954102016000444 PG 11 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA EN9VA UT WOS:000396346500009 ER PT J AU Kim, HS Choi, YS Kim, JH Kim, W AF Kim, Hye-Sil Choi, Yong-Sang Kim, Joo-Hong Kim, WonMoo TI Multiple Aspects of Northern Hemispheric Wintertime Cold Extremes as Revealed by Markov Chain Analysis SO ASIA-PACIFIC JOURNAL OF ATMOSPHERIC SCIENCES LA English DT Article DE Cold extremes; Markov chain analysis; multiple descriptors for extremes; decadal variations of cold extremes ID MIDLATITUDE WEATHER; TEMPERATURE; ENTROPY; VARIABILITY; OUTBREAKS; EVOLUTION; IMPACTS; EVENTS; EUROPE; RISK AB High-impact cold extremes have continued to bring devastating socioeconomic losses in recent years. In order to explain the exposure to cold extremes more comprehensively, this study investigates multiple aspects of boreal winter cold extremes, i.e., frequency, persistence, and entropy (Markovian descriptors). Cold extremes are defined by the bottom 10th percentile of daily minimum temperatures during 1950-2014 over the northern hemisphere. The spatial and temporal distributions of Markovian descriptors during 65 years are examined. Climatological mean fields show the spatial coincidence of higher frequency, shorter persistence, and higher entropy of cold extremes, and vice versa. In regard to the temporal variations over six representative regions of North America, Europe, and Asia, all regions share a decreasing tendency of frequency with the increases in regional winter mean temperature. By contrast, persistence and entropy show their intrinsic decadal variability depending on regions irrespective of the regional temperature variability, which give different information from frequency. Therefore, the exposure to cold extremes would not simply decrease with regional warming. Rather these results indicate that the descriptors with multiple aspects of the extremes would be needed to embrace the topical features as well as the holistic nature of cold extremes. C1 [Kim, Hye-Sil; Choi, Yong-Sang; Kim, WonMoo] Ewha Womans Univ, Seoul, South Korea. [Choi, Yong-Sang] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Kim, Joo-Hong] Korea Polar Res Inst, Incheon, South Korea. [Kim, WonMoo] APEC Climate Ctr, Busan, South Korea. RP Choi, YS (reprint author), Ewha Womans Univ, Dept Atmospher Sci & Engn, 52,Ewhayeodaegil,Seodaemungu, Seoul 03760, South Korea. EM ysc@ewha.ac.kr FU Korea Meteorological Administration Research and Development Program [KMIPA2015-6110]; Ewha Womans University, Korea; Korea Polar Research Institute [PE16100]; Jet Propulsion Laboratory; California Institute of Technology; National Aeronautics and Space Administration (NASA); APEC Climate Center FX This study was supported by the Korea Meteorological Administration Research and Development Program (KMIPA2015-6110),RP-Grand 2015 of Ewha Womans University, Korea, and the research project (PE16100) of the Korea Polar Research Institute. Y.-S. Choi acknowledges the support by the Jet Propulsion Laboratory, California Institute of Technology, sponsored by the National Aeronautics and Space Administration (NASA). W. Kim is currently supported by APEC Climate Center. We appreciate UK Met Office for providing the daily minimum surface temperatures used in this paper at their data server (http://www.metoffice.gov.uk/hadobs/ hadghcnd/download.html). We also thank Ms. Soo Jin Shin for her initial work. NR 39 TC 0 Z9 0 U1 0 U2 0 PU KOREAN METEOROLOGICAL SOC PI SEOUL PA SHINKIL-DONG 508, SIWON BLDG 704, YONGDUNGPO-GU, SEOUL, 150-050, SOUTH KOREA SN 1976-7633 EI 1976-7951 J9 ASIA-PAC J ATMOS SCI JI Asia-Pac. J. Atmos. Sci. PD FEB PY 2017 VL 53 IS 1 BP 51 EP 61 DI 10.1007/s13143-017-0004-9 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EP1GS UT WOS:000397134000006 ER PT J AU Petty, AA Schroder, D Stroeve, JC Markus, T Miller, J Kurtz, NT Feltham, DL Flocco, D AF Petty, A. A. Schroder, D. Stroeve, J. C. Markus, T. Miller, J. Kurtz, N. T. Feltham, D. L. Flocco, D. TI Skillful spring forecasts of September Arctic sea ice extent using passive microwave sea ice observations SO EARTHS FUTURE LA English DT Article ID MINIMUM EXTENT AB In this study, we demonstrate skillful spring forecasts of detrended September Arctic sea ice extent using passive microwave observations of sea ice concentration (SIC) and melt onset (MO). We compare these to forecasts produced using data from a sophisticated melt pond model, and find similar to higher skill values, where the forecast skill is calculated relative to linear trend persistence. The MO forecasts shows the highest skill in March-May, while the SIC forecasts produce the highest skill in June-August, especially when the forecasts are evaluated over recent years (since 2008). The high MO forecast skill in early spring appears to be driven primarily by the presence and timing of open water anomalies, while the high SIC forecast skill appears to be driven by both open water and surface melt processes. Spatial maps of detrended anomalies highlight the drivers of the different forecasts, and enable us to understand regions of predictive importance. Correctly capturing sea ice state anomalies, along with changes in open water coverage appear to be key processes in skillfully forecasting summer Arctic sea ice. C1 [Petty, A. A.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Petty, A. A.; Markus, T.; Miller, J.; Kurtz, N. T.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Schroder, D.; Feltham, D. L.; Flocco, D.] Univ Reading, Dept Meteorol, Ctr Polar Observat & Modelling, Reading, Berks, England. [Stroeve, J. C.] Univ Colorado, Natl Snow & Ice Data Ctr, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Stroeve, J. C.] UCL, Ctr Polar Observat & Modelling, London, England. RP Petty, AA (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.; Petty, AA (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. EM alek.a.petty@nasa.gov OI Petty, Alek/0000-0003-0307-3216 NR 29 TC 0 Z9 0 U1 0 U2 0 PU WILEY PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2328-4277 J9 EARTHS FUTURE JI Earth Future PD FEB PY 2017 VL 5 IS 2 BP 254 EP 263 DI 10.1002/2016EF000495 PG 10 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA EO8II UT WOS:000396932200010 ER PT J AU Nikkhoo, M Walter, TR Lundgren, PR Prats-Iraola, P AF Nikkhoo, Mehdi Walter, Thomas R. Lundgren, Paul R. Prats-Iraola, Pau TI Compound dislocation models (CDMs) for volcano deformation analyses SO GEOPHYSICAL JOURNAL INTERNATIONAL LA English DT Article DE Geomechanics; Kinematics of crustal and mantle deformation ID ELASTIC HALF-SPACE; SURFACE DEFORMATION; TENSILE FAULTS; INFLATION; SHEAR AB Volcanic crises are often preceded and accompanied by volcano deformation caused by magmatic and hydrothermal processes. Fast and efficient model identification and parameter estimation techniques for various sources of deformation are crucial for process understanding, volcano hazard assessment and early warning purposes. As a simple model that can be a basis for rapid inversion techniques, we present a compound dislocation model (CDM) that is composed of three mutually orthogonal rectangular dislocations (RDs). We present new RD solutions, which are free of artefact singularities and that also possess full rotational degrees of freedom. The CDM can represent both planar intrusions in the near field and volumetric sources of inflation and deflation in the far field. Therefore, this source model can be applied to shallow dikes and sills, as well as to deep planar and equidimensional sources of any geometry, including oblate, prolate and other triaxial ellipsoidal shapes. In either case the sources may possess any arbitrary orientation in space. After systematically evaluating the CDM, we apply it to the co-eruptive displacements of the 2015 Calbuco eruption observed by the Sentinel-1A satellite in both ascending and descending orbits. The results show that the deformation source is a deflating vertical lens-shaped source at an approximate depth of 8 km centred beneath Calbuco volcano. The parameters of the optimal source model clearly show that it is significantly different from an isotropic point source or a single dislocation model. The Calbuco example reflects the convenience of using the CDM for a rapid interpretation of deformation data. C1 [Nikkhoo, Mehdi; Walter, Thomas R.] GFZ German Res Ctr Geosci, Potsdam, Germany. [Lundgren, Paul R.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Prats-Iraola, Pau] DLR German Aerosp Ctr, Microwaves & Radar Inst, Wessling, Germany. RP Nikkhoo, M (reprint author), GFZ German Res Ctr Geosci, Potsdam, Germany. EM mehdi.nikkhoo@gfz-potsdam.de OI Prats-Iraola, Pau/0000-0002-7583-2309 FU European Research Council under the European Union/ERC [ERC-CoG 646858]; ERC project 'TOPOMOD' [264517]; InSARAP project (ESA) [4000110587/14/I-BG] FX We appreciate constructive reviews and comments from Sylvain Barbot, an anonymous reviewer and the editor. This is a contribution to VOLCAPSE, a research project funded by the European Research Council under the European Union's H2020 Programme/ERC consolidator grant No. [ERC-CoG 646858]. We acknowledge the financial support from ERC project 'TOPOMOD' (contract No. 264517), as well as from the InSARAP project (ESA Contract 4000110587/14/I-BG). The subsampled InSAR data and the MATLAB functions associated with the RD and CDM calculations in this paper are available upon request from the corresponding author and can also be downloaded under the following link: www.volcanodeformation.com. NR 29 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0956-540X EI 1365-246X J9 GEOPHYS J INT JI Geophys. J. Int. PD FEB PY 2017 VL 208 IS 2 BP 877 EP 894 DI 10.1093/gji/ggw427 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EO6QM UT WOS:000396817600017 ER PT J AU Doubre, E Deprez, A Masson, F Socquet, A Lewi, E Grandin, R Nercessian, A Ulrich, P De Chabalier, JB Saad, I Abayazid, A Peltzer, G Delorme, A Calais, E Wright, T AF Doubre, Ecile Deprez, Aline Masson, Frederic Socquet, Anne Lewi, Elias Grandin, Raphael Nercessian, Alexandre Ulrich, Patrice De Chabalier, Jean-Bernard Saad, Ibrahim Abayazid, Ahmadine Peltzer, Gilles Delorme, Arthur Calais, Eric Wright, Tim TI Current deformation in Central Afar and triple junction kinematics deduced from GPS and InSAR measurements SO GEOPHYSICAL JOURNAL INTERNATIONAL LA English DT Article DE Transient deformation; Mid-ocean ridge processes; Continental tectonics: extensional; Kinematics of crustal and mantle deformation; Africa ID EAST-AFRICAN RIFT; SOMALIA PLATE BOUNDARY; ASAL-GHOUBBET RIFT; MANDA-INAKIR RIFT; EARTHQUAKE SEQUENCE; BLOCK ROTATIONS; VELOCITY-FIELD; CONTINENTAL RUPTURE; DANAKIL MICROPLATE; PROPAGATING RIFTS AB Kinematics of divergent boundaries and Rift-Rift-Rift junctions are classically studied using long-term geodetic observations. Since significant magma-related displacements are expected, short-term deformation provides important constraints on the crustal mechanisms involved both in active rifting and in transfer of extensional deformation between spreading axes. Using InSAR and GPS data, we analyse the surface deformation in the whole Central Afar region in detail, focusing on both the extensional deformation across the Quaternary magmato-tectonic rift segments, and on the zones of deformation transfer between active segments and spreading axes. The largest deformation occurs across the two recently activated Asal-Ghoubbet (AG) and Manda Hararo-Dabbahu (MH-D) magmato-tectonic segments with very high strain rates, whereas the other Quaternary active segments do not concentrate any large strain, suggesting that these rifts are either sealed during interdyking periods or not mature enough to remain a plate boundary. Outside of these segments, the GPS horizontal velocity field shows a regular gradient following a clockwise rotation of the displacements from the Southeast to the East of Afar, with respect to Nubia. Very few shallow creeping structures can be identified as well in the InSAR data. However, using these data together with the strain rate tensor and the rotations rates deduced from GPS baselines, the present-day strain field over Central Afar is consistent with the main tectonic structures, and therefore with the long-term deformation. We investigate the current kinematics of the triple junction included in our GPS data set by building simple block models. The deformation in Central Afar can be described by adding a central microblock evolving separately from the three surrounding plates. In this model, the northern block boundary corresponds to a deep EW-trending trans-tensional dislocation, locked from the surface to 10-13 km and joining at depth the active spreading axes of the Red Sea and the Aden Ridge, from AG to MH-D rift segments. Over the long-term, this plate configuration could explain the presence of the en-echelon magmatic basins and subrifts. However, the transient behaviour of the spreading axes implies that the deformation in Central Afar evolves depending on the availability of magma supply within the well-established segments. C1 [Doubre, Ecile; Deprez, Aline; Masson, Frederic; Ulrich, Patrice] Univ Strasbourg, CNRS, IPGS, UMR 7516, F-67000 Strasbourg, France. [Socquet, Anne] Univ Grenoble Alpes, CNRS, ISTerre, Grenoble, France. [Lewi, Elias] Univ Addis Ababa, Inst Geophys Space Sci & Astron, Arat Kilo Campus, Addis Ababa, Ethiopia. [Grandin, Raphael; Nercessian, Alexandre; De Chabalier, Jean-Bernard; Delorme, Arthur] Inst Phys Globe Paris, UMR 7154, Paris, France. [Saad, Ibrahim; Abayazid, Ahmadine] Observ Geophys Arta, Ctr Etud & Rech Djibouti, Arta, Djibouti. [Peltzer, Gilles] Univ Calif Los Angeles, Earth & Space Sci Dept, Los Angeles, CA 90024 USA. [Peltzer, Gilles] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Calais, Eric] Ecole Normale Super, Dpt Geosci, CNRS, UMR 8538, Paris, France. [Wright, Tim] Univ Leeds, Sch Earth & Environm, COMET, Leeds, W Yorkshire, England. RP Doubre, E (reprint author), Univ Strasbourg, CNRS, IPGS, UMR 7516, F-67000 Strasbourg, France. EM cdoubre@unistra.fr OI Grandin, Raphael/0000-0002-1837-011X FU Agence Nationale pour la Recherche [ANR-09-JCJC-0051-01]; CNES-TOSCA; Ministry of Research and Higher Education and through the 'Investissements d'avenir' [ANR-11-EQPX-0040] FX This work was supported by the Agence Nationale pour la Recherche, in the framework of the project DoRA ANR-09-JCJC-0051-01, and partly by CNES-TOSCA. We thank all the participants of the measurement campaigns, and teams involved to make the data available. The data were acquired using the instruments belonging to the French National Research Infrastructure RESIF (http://www.resif.fr), supported by the Ministry of Research and Higher Education and through the 'Investissements d'avenir' (ANR-11-EQPX-0040). We are grateful to our colleagues from the Institute of Geophysics, Space Sciences and Astronomy from Addis Ababa University, and from the Centre d'Etudes et de Recherches Djiboutiennes (Dir. Mohamed Jalludin), and the Observatoire Geophysique d'Arta (www.oga.dj). Support from the authorities of the Afar regional government in Semera has been crucial and they are warmly thanked, as well as the policemen who accompanied us in the field. The fieldwork has been made possible with the logistic support of the Centre Francais d'Etudes Ethiopiennes in Addis-Ababa, and from Eloi Ficquet and David Ambrosetti in particular. Special thanks are addressed to the Ethiopian and Djiboutian drivers (Semeneh Bacha, Amare Setotaw, Temechache Yirfu, Wegen Amerga and Mohamed Amadou), and to Yves Bertrand and Bernard Luck for their precious help in the field. NR 104 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0956-540X EI 1365-246X J9 GEOPHYS J INT JI Geophys. J. Int. PD FEB PY 2017 VL 208 IS 2 BP 936 EP 953 DI 10.1093/gji/ggw434 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EO6QM UT WOS:000396817600020 ER PT J AU Garcia, M Saatchi, S Casas, A Koltunov, A Ustin, S Ramirez, C Garcia-Gutierrez, J Balzter, H AF Garcia, Mariano Saatchi, Sassan Casas, Angeles Koltunov, Alexander Ustin, Susan Ramirez, Carlos Garcia-Gutierrez, Jorge Balzter, Heiko TI Quantifying biomass consumption and carbon release from the California Rim fire by integrating airborne LiDAR and Landsat OLI data SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID ABOVEGROUND BIOMASS; CANOPY STRUCTURE; BRAZILIAN AMAZON; WILDLIFE HABITAT; FOREST STRUCTURE; CLIMATE-CHANGE; PINE FORESTS; TM DATA; VEGETATION; METRICS AB Quantifying biomass consumption and carbon release is critical to understanding the role of fires in the carbon cycle and air quality. We present a methodology to estimate the biomass consumed and the carbon released by the California Rim fire by integrating postfire airborne LiDAR and multitemporal Landsat Operational Land Imager (OLI) imagery. First, a support vector regression (SVR) model was trained to estimate the aboveground biomass (AGB) from LiDAR-derived metrics over the unburned area. The selected model estimated AGB with an R-2 of 0.82 and RMSE of 59.98 Mg/ha. Second, LiDAR-based biomass estimates were extrapolated to the entire area before and after the fire, using Landsat OLI reflectance bands, Normalized Difference Infrared Index, and the elevation derived from LiDAR data. The extrapolation was performed using SVR models that resulted in R-2 of 0.73 and 0.79 and RMSE of 87.18 (Mg/ha) and 75.43 (Mg/ha) for the postfire and prefire images, respectively. After removing bias from the AGB extrapolations using a linear relationship between estimated and observed values, we estimated the biomass consumption from postfire LiDAR and prefire Landsat maps to be 6.58 +/- 0.03 Tg (10(12) g), which translate into 12.06 +/- 0.06 Tg CO2(e) released to the atmosphere, equivalent to the annual emissions of 2.57 million cars. C1 [Garcia, Mariano; Saatchi, Sassan] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. [Garcia, Mariano; Balzter, Heiko] Univ Leicester, Ctr Landscape & Climate Res, Leicester, Leics, England. [Casas, Angeles; Koltunov, Alexander; Ustin, Susan] Univ Calif Davis, Ctr Spatial Technol & Remote Sensing, Davis, CA 95616 USA. [Ramirez, Carlos] USDA Forest Serv, Reg Remote Sensing Lab 5, Vallejo, CA USA. [Garcia-Gutierrez, Jorge] Univ Seville, Dept Comp Sci, Seville, Spain. [Balzter, Heiko] Univ Leicester, Natl Ctr Earth Observat, Leicester, Leics, England. RP Garcia, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM mariano.gar.alo@gmail.com FU U.S. Department of Agriculture Forest Service; University of California Davis under Cost Share [10-IA-11130400009]; Marie Curie International Outgoing Fellowship within the seventh European Community Framework Programme (ForeStMap-3-D Forest Structure Monitoring and Mapping) [629376]; Royal Society Wolfson Research Merit Award [2011/R3]; NERC National Centre for Earth Observation FX This research was carried out within the ambit of the project "Multisensor remote sensing study of California's Rim Fire to inform postfire ecosystem restoration and effective prevention of future catastrophic wildfires" funded by the U.S. Department of Agriculture Forest Service, as the main sponsor, and the University of California Davis under Cost Share Agreement 10-IA-11130400009. Mariano Garcia is supported by a Marie Curie International Outgoing Fellowship within the seventh European Community Framework Programme (ForeStMap-3-D Forest Structure Monitoring and Mapping, Project Reference: 629376). The content of this paper reflects solely the authors' views and not the views of the European Commission. Heiko Balzter was supported by the Royal Society Wolfson Research Merit Award, 2011/R3, and the NERC National Centre for Earth Observation. The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We express our gratitude to Zhao, Salas, and Bahamondez for the comments on the manuscript. We thank the help of Mitzi Thornley and the Science Division Yosemite National Park for the permission to conduct research in Yosemite National Park (YOSE-00653/YOSE-2014-SCI-0124). We greatly appreciate the constructive comments by the two anonymous reviewers, who greatly helped improve the manuscript. Data are available from the authors upon request. c 2015 California Institute of Technology. NR 77 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-8953 EI 2169-8961 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD FEB PY 2017 VL 122 IS 2 BP 340 EP 353 DI 10.1002/2015JG003315 PG 14 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA EN6RF UT WOS:000396130400005 ER PT J AU Spann, J Moore, T AF Spann, James Moore, Thomas TI Introduction: Photons and ground-based SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article AB A Conference on Measurement Techniques for Solar and Space Physics was held on 20-24 April 2015 in Boulder, Colorado, at the National Center for Atmospheric Research Center Green Campus. The present volume collects together the conference papers for photons and ground-based categories. C1 [Spann, James] NASA MSFC, Huntsville, AL 35811 USA. [Moore, Thomas] NASA GSFC, Greenbelt, MD USA. RP Spann, J (reprint author), NASA MSFC, Huntsville, AL 35811 USA. EM jim.spann@nasa.gov NR 3 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 FEB PY 2017 VL 122 IS 2 BP 1437 EP 1438 AR JA023888 DI 10.1002/2017JA023888 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EO9QJ UT WOS:000397022900001 ER PT J AU Vasquez, BJ Farrugia, CJ Simunac, KDC Galvin, AB Berdichevsky, DB AF Vasquez, Bernard J. Farrugia, C. J. Simunac, K. D. C. Galvin, A. B. Berdichevsky, D. B. TI Concerning the helium-to-hydrogen number density ratio in very slow ejecta and winds near solar minimum SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CORONAL MASS EJECTIONS; LARGE-SCALE STRUCTURE; CYCLE 23/24 MINIMUM; 1 AU; MAGNETIC CLOUDS; INTERPLANETARY MEDIUM; NUMERICAL-SIMULATION; STATISTICAL-ANALYSIS; ABUNDANCE; TRANSIENTS AB Near the solar minimum the average value of the helium-to-proton number density ratio is a strong function of speed. The average ratios for both solar ejecta and ambient winds obey approximately the same relation with speed. At the lowest speeds, the ratio takes on small values near and below 0.01. Here winds and ejecta with very slow speeds (less than or similar to 310 km/s) are examined. STEREO and Wind spacecraft data are employed that were obtained from 2007 to 2010. This was during the prolonged solar activity minimum between cycles 23 and 24. Case event and statistical studies are made with 12 very slow ejecta. The helium-to-proton ratio in very slow ejecta relative to the ratio for very slow winds of comparable speed averaged in an inclusive 1 year period is 1.06. The ejecta and ambient slow winds have, then, nearly the same concentrations on average. The values did not approach 0 with decreasing speed and are shown to deviate from a predicted form. A survey of potential solar sources of very slow ejecta and other inferences based on interplanetary data found a strong correspondence with active regions and a dependence of the properties of very slow ejecta with the solar cycle. C1 [Vasquez, Bernard J.; Farrugia, C. J.; Simunac, K. D. C.; Galvin, A. B.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Vasquez, Bernard J.; Farrugia, C. J.; Simunac, K. D. C.; Galvin, A. B.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Simunac, K. D. C.] St Petersburg Coll, Dept Nat Sci, St Petersburg, FL USA. [Berdichevsky, D. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Vasquez, BJ (reprint author), Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.; Vasquez, BJ (reprint author), Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. EM bernie.vasquez@unh.edu FU NASA STEREO/PLASTIC [NNX13AP52G, NNX15AU01G]; University of New Hampshire (UNH); NASA [NNX16A084G]; NSF [AGS1239699] FX We thank L. Ellis for aid in plotting electron pitch angle distributions. The work was supported by NASA STEREO/PLASTIC grants NNX13AP52G and NNX15AU01G to the University of New Hampshire (UNH). C. Farrugia was also supported by NASA Wind grant NNX16A084G to UNH and NSF grant AGS1239699 to UNH. Publicly available data have been used, and sources of these data are described in detail in section 2. We thank K. Ogilvie for Wind plasma data, R. Lepping for Wind magnetic data, J. Luhmann for STEREO IMPACT data, and R. Howard for STEREO SECCHI data. NR 95 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 FEB PY 2017 VL 122 IS 2 BP 1487 EP 1512 AR JA023636 DI 10.1002/2016JA023636 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EO9QJ UT WOS:000397022900006 ER PT J AU Hill, ME Mitchell, DG Andrews, GB Cooper, SA Gurnee, RS Hayes, JR Layman, RS McNutt, RL Nelson, KS Parker, CW Schlemm, CE Stokes, MR Begley, SM Boyle, MP Burgum, JM Do, DH Dupont, AR Gold, RE Haggerty, DK Hoffer, EM Hutcheson, JC Jaskulek, SE Krimigis, SM Liang, SX London, SM Noble, MW Roelof, EC Seifert, H Strohbehn, K Vandegriff, JD Westlake, JH AF Hill, M. E. Mitchell, D. G. Andrews, G. B. Cooper, S. A. Gurnee, R. S. Hayes, J. R. Layman, R. S. McNutt, R. L., Jr. Nelson, K. S. Parker, C. W. Schlemm, C. E., II Stokes, M. R. Begley, S. M. Boyle, M. P. Burgum, J. M. Do, D. H. Dupont, A. R. Gold, R. E. Haggerty, D. K. Hoffer, E. M. Hutcheson, J. C. Jaskulek, S. E. Krimigis, S. M. Liang, S. X. London, S. M. Noble, M. W. Roelof, E. C. Seifert, H. Strohbehn, K. Vandegriff, J. D. Westlake, J. H. TI The Mushroom: A half-sky energetic ion and electron detector SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID PARTICLE; SPECTROMETER; INSTRUMENT; MISSION; SPACECRAFT AB We present a time-of-flight mass spectrometer design for the measurement of ions in the similar to 30keV to 10 MeV range for protons (up to similar to 40 MeV and similar to 150 MeV for He and heavy ions, respectively) and similar to 30 keV to 1 MeV range for electrons, covering half of the sky with 80 apertures. The instrument, known as the "Mushroom," owing to its shape, solves the field of view problem for magnetospheric and heliospheric missions that employ three-axis stabilized spacecraft, yet still require extended angular coverage; the Mushroom is also compatible with a spinning spacecraft. The most important new feature of the Mushroom is the method through which uncomplicated electrostatic optics and clean position sensing combine to permit many apertures to fit into a compact, low-mass sensor head (or wedge), several of which (ideally eight) compose a full instrument. Most of the sensor head's volume is an empty, equipotential region, resulting in the modest 250 g mass of each 10-aperture wedge. The Mushroom is capable of separating ion species across most of its energy range and angular field of view. For example, separation of the neighboring He-3 and He-4 isotopes is excellent; the full width at half maximum mass resolution has been measured to be 0.24 amu to 0.32 amu, respectively. Converting this to a Gaussian width sigma(m) in mass m, this represents a sigma(m)/m mass resolution better than 0.04. This separation is highly desirable for the flight program for which the first Mushroom was built, the Solar Probe Plus mission. More generally, we estimate the mass resolution to be sigma(m)/m approximate to 0.1, but this is energy, mass, and angularly dependent. We also discuss the solid-state detector stack capability, which extends the energy range of protons and helium, with composition, to similar to 100 MeV. C1 [Hill, M. E.; Mitchell, D. G.; Andrews, G. B.; Cooper, S. A.; Hayes, J. R.; Layman, R. S.; McNutt, R. L., Jr.; Nelson, K. S.; Parker, C. W.; Schlemm, C. E., II; Begley, S. M.; Boyle, M. P.; Burgum, J. M.; Do, D. H.; Dupont, A. R.; Gold, R. E.; Haggerty, D. K.; Hoffer, E. M.; Hutcheson, J. C.; Jaskulek, S. E.; Krimigis, S. M.; Liang, S. X.; London, S. M.; Noble, M. W.; Roelof, E. C.; Seifert, H.; Strohbehn, K.; Vandegriff, J. D.; Westlake, J. H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Gurnee, R. S.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA. [Stokes, M. R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Krimigis, S. M.] Acad Athens, Off Space Res & Technol, Athens, Greece. [Noble, M. W.] Harris Corp, Ft Wayne, IN USA. RP Hill, ME (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. EM matthew.hill@jhuapl.edu FU NASA Planetary Division's Planetary Instrument Definition and Development Program [NNX07AP26G]; NASA [NNN06AA01C, NNN10AA08] FX We gratefully acknowledge support for the early development of the Mushroom instrument under a grant from the NASA Planetary Division's Planetary Instrument Definition and Development Program, grant NNX07AP26G to the Johns Hopkins University, carried out at the Applied Physics Laboratory (D. G. Mitchell, Principle Investigator). We also appreciate the useful consultations regarding the EPI-Lo/Mushroom instrument with members of the Solar Probe Plus Integrated Science Investigation of the Sun (IS.IS) team (D.J. McComas, Princeton University, Principle Investigator) and thankfully acknowledge the associated support under NASA contract NNN06AA01C, Task Order NNN10AA08, to JHU/APL and the collaboration with Southwest Research Institute thereunder. Nearly all of the instrument testing was conducted at JHU/APL, with the notable exceptions of measurements made at the Goddard Spaceflight Center's 2 MeV Van der Graff accelerator for 3 weeks in March 2015 and a continuous 36 h beam run at the Lawrence Berkeley National Laboratory's 88-inch cyclotron in May 2015; we appreciate the efforts of the personnel at these facilities. The data are available from the first author, who can be reached at matt. hill@ jhuapl. edu. NR 20 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 FEB PY 2017 VL 122 IS 2 BP 1513 EP 1530 AR JA022614 DI 10.1002/2016JA022614 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EO9QJ UT WOS:000397022900007 ER PT J AU Meziane, K Mazelle, CX Romanelli, N Mitchell, DL Espley, JR Connerney, JEP Hamza, AM Halekas, J McFadden, JP Jakosky, BM AF Meziane, K. Mazelle, C. X. Romanelli, N. Mitchell, D. L. Espley, J. R. Connerney, J. E. P. Hamza, A. M. Halekas, J. McFadden, J. P. Jakosky, B. M. TI Martian electron foreshock from MAVEN observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID EARTHS BOW SHOCK; SOLAR-WIND INTERACTION; MARS GLOBAL SURVEYOR; UPSTREAM; PHOBOS-2; FREQUENCY; LOCATIONS; WAVES AB Flux enhancements of energetic electrons are always observed when the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft is magnetically connected to the shock. The observations indicate that the foreshock electrons consist of two populations. The most energetic (E >= 237 eV) originate from a narrow region at the nearly perpendicular shock. They always appear as spikes, and their flux level reaches a maximum when the angle theta(Bn) approaches 90 degrees. The other population emanates from the entire Martian bow shock surface, and the flux level decreases slightly from the quasi-parallel to quasi-perpendicular regions. A detailed examination of the pitch angle distribution shows that the enhanced fluxes are associated with electrons moving sunward. Annulus centered along the interplanetary magnetic field direction is the most stringent feature of the 3-D angular distribution. The gyrotropic character is observed over the whole range of shock geometry. Although such signatures in the electron pitch angle distribution function strongly suggest that the reflection off the shock of a fraction of the solar wind electrons is the main mechanism for the production of Martian foreshock electrons, the decay of the flux of the second population on the other hand has yet to be understood. C1 [Meziane, K.; Hamza, A. M.] Univ New Brunswick, Dept Phys, Fredericton, NB, Canada. [Mazelle, C. X.; Romanelli, N.] Univ Paul Sabatier, CNRS, IRAP, Toulouse, France. [Mitchell, D. L.; McFadden, J. P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Espley, J. R.; Connerney, J. E. P.] NASA, Goddard Space Ctr, Greenbelt, MD USA. [Halekas, J.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Jakosky, B. M.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA. RP Meziane, K (reprint author), Univ New Brunswick, Dept Phys, Fredericton, NB, Canada. EM karim@unb.ca OI Halekas, Jasper/0000-0001-5258-6128 FU MAVEN; Canadian Natural Science and Engineering Council FX MAVEN data are publicly available through the Planetary Data System. K.M. thanks Emmanual Penou for his devotion in providing his valuable help in CL software development tool. K.M. wishes to express his thanks to the IRAP in Toulouse for the support in the collaboration work on MAVEN. C.M. and K.M. thank CNES for its support for the part of this work based on the observations with the SWEA instrument on board MAVEN. Work at UNB is supported by the Canadian Natural Science and Engineering Council. K.M. thanks both referees for their valuable comments. NR 31 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD FEB PY 2017 VL 122 IS 2 BP 1531 EP 1541 AR JA023282 DI 10.1002/2016JA023282 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EO9QJ UT WOS:000397022900008 ER PT J AU Shim, JS Jee, G Scherliess, L AF Shim, Ja Soon Jee, Geonhwa Scherliess, Ludger TI Climatology of plasmaspheric total electron content obtained from Jason 1 satellite SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID TOPEX/POSEIDON MEASUREMENTS; GPS TEC; IONOSPHERE; DENSITY; MODEL; MISSION; HEIGHT AB We used more than 40 million total electron content (TEC) measurements obtained from the GPS TurboRogue Space Receiver receiver on board the Jason 1 satellite in order to investigate the global morphology of the plasmaspheric TEC (pTEC) including the variations with local time, latitude, longitude, season, solar cycle, and geomagnetic activity. The pTEC corresponds to the total electron content between Jason 1 (1336 km) and GPS (20,200 km) satellite altitudes. The pTEC data were collected during the 7 year period from January 2002 to December 2008. It was found that pTEC increases by about 10-30% from low to high solar flux conditions with the largest variations occurring at low latitudes for equinox. During low solar flux condition, pTEC is largely independent of geomagnetic activity. However, it slightly decreases with increasing geomagnetic activity at low latitudes during high solar flux. The seasonal variations such as the annual and semiannual anomalies in the ionosphere also exist in the low-latitude plasmasphere. In particular, the American sector (around 300 degrees E) shows strong annual asymmetry in the plasmaspheric density, being larger in December than in June solstice. C1 [Shim, Ja Soon] NASA, CUA, GSFC, Greenbelt, MD USA. [Jee, Geonhwa] Korea Polar Res Inst, Incheon, South Korea. [Scherliess, Ludger] Utah State Univ, Ctr Atmospher & Space Sci, Logan, UT USA. RP Jee, G (reprint author), Korea Polar Res Inst, Incheon, South Korea. EM ghjee@kopri.re.kr FU Korea Polar Research Institute [PE17020] FX This study was supported by the grant PE17020 from Korea Polar Research Institute. The Jason 1 TEC data are obtained from the Physical Oceanography Distributed Active Archive Center at the NASA Jet Propulsion Laboratory (http://podaac.jpl.nasa.gov). NR 39 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 FEB PY 2017 VL 122 IS 2 BP 1611 EP 1623 DI 10.1002/2016JA023444 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EO9QJ UT WOS:000397022900014 ER PT J AU Zhao, H Baker, DN Jaynes, AN Li, X Elkington, SR Kanekal, SG Spence, HE Boyd, AJ Huang, CL Forsyth, C AF Zhao, H. Baker, D. N. Jaynes, A. N. Li, X. Elkington, S. R. Kanekal, S. G. Spence, H. E. Boyd, A. J. Huang, C. -L. Forsyth, C. TI On the relation between radiation belt electrons and solar wind parameters/ geomagnetic indices: Dependence on the first adiabatic invariant and L SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ALLEN PROBES MEASUREMENTS; ULF WAVE POWER; RELATIVISTIC ELECTRONS; GEOSYNCHRONOUS ORBIT; MAGNETIC STORMS; ENERGETIC ELECTRONS; PREDICTION; FLUX; MAGNETOSPHERE; MODEL AB The relation between radiation belt electrons and solar wind/magnetospheric processes is of particular interest due to both scientific and practical needs. Though many studies have focused on this topic, electron data from Van Allen Probes with wide L shell coverage and fine energy resolution, for the first time, enabled this statistical study on the relation between radiation belt electrons and solar wind parameters/geomagnetic indices as a function of first adiabatic invariant mu and L-*. Good correlations between electron phase space density (PSD) and solar wind speed, southward IMF B-z, SYM-H, and AL indices are found over wide mu and L-* ranges, with higher correlation coefficients and shorter time lags for low-mu electrons than high-mu electrons; the anticorrelation between electron PSD and solar wind proton density is limited to high-mu electrons at high L-*. The solar wind dynamic pressure has dominantly positive correlation with low-mu electrons and negative correlation with high-mu electrons at different L-*. In addition, electron PSD enhancements also correlate well with various solar wind/geomagnetic parameters, and for most parameters this correlation is even better than that of electron PSD while the time lag is also much shorter. Among all parameters investigated, AL index is shown to correlate the best with electron PSD enhancements, with correlation coefficients up to similar to 0.8 for low-mu electrons (time lag similar to 0 day) and similar to 0.7 for high-mu electrons (time lag similar to 1-2 days), suggesting the importance of seed and source populations provided by substorms in radiation belt electron PSD enhancements. C1 [Zhao, H.; Baker, D. N.; Jaynes, A. N.; Li, X.; Elkington, S. R.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Kanekal, S. G.] Goddard Space Flight Ctr, NASA, Greenbelt, MD USA. [Spence, H. E.; Huang, C. -L.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH USA. [Boyd, A. J.] New Mexico Consortium, Los Alamos, NM USA. [Forsyth, C.] UCL, Dept Space & Climate Phys, Mullard Space Sci Lab, London, England. RP Zhao, H (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. EM hong.zhao@lasp.colorado.edu OI Spence, Harlan/0000-0002-2526-2205; LI, XINLIN/0000-0002-1683-3192 NR 56 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 FEB PY 2017 VL 122 IS 2 BP 1624 EP 1642 DI 10.1002/2016JA023658 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EO9QJ UT WOS:000397022900015 ER PT J AU Falkowski, BJ Tsurutani, BT Lakhina, GS Pickett, JS AF Falkowski, Barbara J. Tsurutani, Bruce T. Lakhina, Gurbax S. Pickett, Jolene S. TI Two sources of dayside intense, quasi-coherent plasmaspheric hiss: A new mechanism for the slot region? SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID WAVE-PARTICLE INTERACTIONS; DISCRETE CHORUS EMISSIONS; RADIATION BELT ELECTRONS; PITCH-ANGLE DIFFUSION; SUDDEN COMMENCEMENTS; ELF HISS; ORIGIN; SUBSTORM; MAGNETOSPHERE; POLAR AB A study of dayside plasmaspheric hiss at frequencies from similar to 22 Hz to similar to 1.0 kHz was carried out by using 1 year of Polar data. It is shown that intense, dayside plasmaspheric hiss is correlated with solar wind pressure with P > 2.5 nPa. The dayside effect is most prominent in the similar to 300 to similar to 650 Hz range. Intense dayside waves are also present during SYM-H< similar to 5 nT. The latter is centered at local noon, with the greatest intensities in the L = 2 to 3 region. Assuming drift of similar to 25 keV electrons from midnight to the wave magnetic local time, plasmaspheric hiss is shown to be highly correlated with precursor AE* and SYM-H* indices, indicating that the hiss is associated with substorms and small injection events. Our hypothesis is that both sets of waves originate as outer zone (L = 6 to 10) chorus and then propagate into the plasmasphere. Fourteen high-intensity dayside plasmaspheric hiss events were analyzed to identify the wave k, polarization, and the degree of coherency. The waves are found to be obliquely propagating, elliptically polarized and quasi- coherent (similar to 0.5 to 0.8 correlation coefficient). It is hypothesized that the dayside plasmaspheric hiss is quasi- coherent because the chorus has been recently generated in the outer magnetosphere and have propagated directly into the plasmasphere. It is possible that the quasi- coherency of the dayside hiss at L = 2 to 3 may be an alternate explanation for the generation of the energetic particle slot region. C1 [Falkowski, Barbara J.; Tsurutani, Bruce T.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Falkowski, Barbara J.] Glendale Community Coll, Dept Phys, Glendale, CA USA. [Lakhina, Gurbax S.] Indian Inst Geomagnetism, Navi Mumbai, India. [Pickett, Jolene S.] Univ Iowa, Phys & Astron, Iowa City, IA USA. RP Tsurutani, BT (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA. EM bruce.tsurutani@jpl.nasa.gov FU National Academy of Sciences, India FX Portions of this research were performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. The Polar plasma wave data can be accessed at http:// cdaweb.gsfc.nasa.gov. The solar wind data were obtained from the OMNI website at http://omniweb. gsfc. nasa. gov/. The AE and SYM-H data used in this study were obtained from the WDC for Geomagnetism at Kyoto University (http://wdc. kugi. kyoto-u.ac.jp/wdc/ Sec3.html). G. S. L. thanks the National Academy of Sciences, India, for support under the NASI-Senior Scientist Platinum Jubilee Fellowship Scheme. NR 83 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 FEB PY 2017 VL 122 IS 2 BP 1643 EP 1657 DI 10.1002/2016JA023289 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EO9QJ UT WOS:000397022900016 ER PT J AU Ma, YJ Russell, CT Fang, X Dong, CF Nagy, AF Toth, G Halekas, JS Connerney, JEP Espley, JR Mahaffy, PR Benna, M McFadden, J Mitchell, DL Andersson, L Jakosky, BM AF Ma, Y. J. Russell, C. T. Fang, X. Dong, C. F. Nagy, A. F. Toth, G. Halekas, J. S. Connerney, J. E. P. Espley, J. R. Mahaffy, P. R. Benna, M. McFadden, J. Mitchell, D. L. Andersson, L. Jakosky, B. M. TI Variations of the Martian plasma environment during the ICME passage on 8 March 2015: A time-dependent MHD study SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CORONAL MASS EJECTIONS; SOLAR-WIND INTERACTION; GEOMAGNETIC STORMS; UPPER-ATMOSPHERE; MULTIFLUID MHD; IONOSPHERE; EXPRESS; MODEL AB The Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft observed astrong interplanetary coronal mass ejection (ICME) impacting Mars on 8 March 2015. We use a time-dependent global MHD model to investigate the response of the Martian ionosphere and induced magnetosphere to the large solar wind disturbance associated with the ICME. Taking observed upstream solar wind conditions from MAVEN as inputs to the MHD model, the variations of the Martian plasma environments are simulated realistically in a time period from 2.5 h prior to the arrival of the ICME shock to about 12 h after the impact. Detailed comparisons between the model results and the relevant MAVEN plasma measurements are presented, which clearly show that the time-dependent multispecies single-fluid MHD model is able to reproduce the main features observed by the spacecraft during the ICME passage. Model results suggest that the induced magnetosphere responds to solar wind variation on a very short time scale (approximately minutes). The variations of the plasma boundaries' distances from the planet along the subsolar line are examined in detail, which show a clear anticorrelation with the magnetosonic Mach number. Plasma properties in the ionosphere (especially the induced magnetic field) varied rapidly with solar wind changes. Model results also show that ion escape rates could be enhanced by an order of magnitude in response to the high solar wind dynamic pressure during the ICME event. C1 [Ma, Y. J.; Russell, C. T.] UCLA, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. [Fang, X.; Andersson, L.] Univ Colorado Boulder, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Dong, C. F.; Jakosky, B. M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. Princeton Univ, Princeton Plasma Phys Lab, POB 451, Princeton, NJ 08543 USA. [Nagy, A. F.; Toth, G.] Univ Michigan, Climate & Space Sci & Engn Dept, Ann Arbor, MI 48109 USA. [Halekas, J. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA USA. [Connerney, J. E. P.; Espley, J. R.; Mahaffy, P. R.; Benna, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [McFadden, J.; Mitchell, D. L.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Ma, YJ (reprint author), UCLA, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. EM yingjuan@igpp.ucla.edu OI FANG, XIAOHUA/0000-0002-6584-2837; Russell, Christopher/0000-0003-1639-8298; Dong, Chuanfei/0000-0002-8990-094X; Halekas, Jasper/0000-0001-5258-6128 FU NASA [NNX13AO31G]; NASA; Star Jack Eddy Postdoctoral Fellowship Program; NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center FX The work presented here was supported by NASA grant NNX13AO31G. 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. 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. The MAVEN observational data used in the study were obtained from the NASA Planetary Data System (PDS). The Space Weather Modeling Framework that contains the BATS-R-US code used in this study is publicly available from http://csem.engin.umich.edu/tools/swmf. For the distribution of the model results used in this study, please contact the corresponding author. NR 44 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 FEB PY 2017 VL 122 IS 2 BP 1714 EP 1730 DI 10.1002/2016JA023402 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EO9QJ UT WOS:000397022900021 ER PT J AU Xu, S Mitchell, D Liemohn, M Fang, X Ma, Y Luhmann, J Brain, D Steckiewicz, M Mazelle, C Connerney, J Jakosky, B AF Xu, Shaosui Mitchell, David Liemohn, Michael Fang, Xiaohua Ma, Yingjuan Luhmann, Janet Brain, David Steckiewicz, Morgane Mazelle, Christian Connerney, Jack Jakosky, Bruce TI Martian low-altitude magnetic topology deduced from MAVEN/SWEA observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SOLAR-WIND; POLAR WIND; MAGNETOMETER/ELECTRON REFLECTOMETER; ELECTRON REFLECTOMETRY; CRUSTAL FIELDS; MARS; IONOSPHERE; NIGHTSIDE; TRANSPORT; FLUXES AB The Mars Atmosphere and Volatile Evolution mission has obtained comprehensive particle and magnetic field measurements. The Solar Wind Electron Analyzer provides electron energy-pitch angle distributions along the spacecraft trajectory that can be used to infer magnetic topology. This study presents pitch angle-resolved electron energy shape parameters that can distinguish photoelectrons from solar wind electrons, which we use to deduce the Martian magnetic topology and connectivity to the dayside ionosphere. Magnetic topology in the Mars environment is mapped in three dimensions for the first time. At low altitudes (< 400 km) in sunlight, the northern hemisphere is found to be dominated by closed field lines (both ends intersecting the collisional atmosphere), with more day-night connections through cross-terminator closed field lines than in the south. Although draped field lines with similar to 100 km amplitude vertical fluctuations that intersect the electron exobase (similar to 160-220 km) in two locations could appear to be closed at the spacecraft, a more likely explanation is provided by crustal magnetic fields, which naturally have the required geometry. Around 30% of the time, we observe open field lines from 200 to 400 km, which implies three distinct topological layers over the northern hemisphere: closed field lines below 200 km, open field lines with foot points at lower latitudes that pass over the northern hemisphere from 200 to 400 km, and draped interplanetary magnetic field above 400 km. This study also identifies open field lines with one end attached to the dayside ionosphere and the other end connected with the solar wind, providing a path for ion outflow. C1 [Xu, Shaosui; Mitchell, David; Luhmann, Janet] Univ California, Space Sci Lab, Berkeley, CA USA. [Fang, Xiaohua; Jakosky, Bruce] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI USA. [Ma, Yingjuan] Univ California, Dept Earth Planetary & Space Sci, Los Angeles, CA USA. [Steckiewicz, Morgane; Mazelle, Christian] Univ Paul Sabatier, CNRS, IRAP, Toulouse, France. [Connerney, Jack] Goddard Space Flight Ctr, Greenbelt, MD USA. RP Xu, S (reprint author), Univ California, Space Sci Lab, Berkeley, CA USA. EM shaosui.xu@ssl.berkeley.edu OI FANG, XIAOHUA/0000-0002-6584-2837 FU NASA Mars Scout Program; NASA RA grants FX This work was supported by the NASA Mars Scout Program. Work at Michigan was supported by NASA R&A grants. 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 MHD magnetic field line tracing results used in this study, contact X. Fang (Xiaohua.Fang@lasp.colorado.edu). NR 60 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 FEB PY 2017 VL 122 IS 2 BP 1831 EP 1852 DI 10.1002/2016JA023467 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EO9QJ UT WOS:000397022900029 ER PT J AU Yao, ST Wang, XG Shi, QQ Pitkanen, T Hamrin, M Yao, ZH Li, ZY Ji, XF De Spiegeleer, A Xiao, YC Tian, AM Pu, ZY Zong, QG Xiao, CJ Fu, SY Zhang, H Russell, CT Giles, BL Guo, RL Sun, WJ Li, WY Zhou, XZ Huang, SY Vaverka, J Nowada, M Bai, SC Wang, MM Liu, J AF Yao, S. T. Wang, X. G. Shi, Q. Q. Pitkanen, T. Hamrin, M. Yao, Z. H. Li, Z. Y. Ji, X. F. De Spiegeleer, A. Xiao, Y. C. Tian, A. M. Pu, Z. Y. Zong, Q. G. Xiao, C. J. Fu, S. Y. Zhang, H. Russell, C. T. Giles, B. L. Guo, R. L. Sun, W. J. Li, W. Y. Zhou, X. Z. Huang, S. Y. Vaverka, J. Nowada, M. Bai, S. C. Wang, M. M. Liu, J. TI Observations of kinetic-size magnetic holes in the magnetosheath SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID TRAVELING CONVECTION VORTICES; DRIFT MIRROR INSTABILITY; FINITE ELECTRON-TEMPERATURE; SOLAR-WIND; PLASMA SHEET; MAGNETOSPHERIC MULTISCALE; CLUSTER-C1 OBSERVATIONS; LINEAR INSTABILITY; FIELD OBSERVATIONS; MODE STRUCTURES AB Magnetic holes (MHs), with a scale much greater than pi ( proton gyroradius), have been widely reported in various regions of space plasmas. On the other hand, kinetic-size magnetic holes (KSMHs), previously called small-size magnetic holes, with a scale of the order of magnitude of or less than.i have only been reported in the Earth's magnetospheric plasma sheet. In this study, we report such KSMHs in the magnetosheath whereby we use measurements from the Magnetospheric Multiscale mission, which provides three-dimensional (3-D) particle distribution measurements with a resolution much higher than previous missions. The MHs have been observed in a scale of 10-20 pe ( electron gyroradii) and lasted 0.1-0.3 s. Distinctive electron dynamics features are observed, while no substantial deviations in ion data are seen. It is found that at the 90 degrees pitch angle, the flux of electrons with energy 34-66 eV decreased, while for electrons of energy 109-1024 eV increased inside the MHs. We also find the electron flow vortex perpendicular to the magnetic field, a feature self-consistent with the magnetic depression. Moreover, the calculated current density is mainly contributed by the electron diamagnetic drift, and the electron vortex flow is the diamagnetic drift flow. The electron magnetohydrodynamics soliton is considered as a possible generation mechanism for the KSMHs with the scale size of 10-20 rho(e). C1 [Yao, S. T.; Shi, Q. Q.; Xiao, Y. C.; Tian, A. M.; Nowada, M.; Bai, S. C.; Wang, M. M.] Shandong Univ, Inst Space Sci, Shandong Prov Key Lab Opt Astron & Solar Terr Env, Weihai, Peoples R China. [Yao, S. T.; Pitkanen, T.; Hamrin, M.; De Spiegeleer, A.; Vaverka, J.] Umea Univ, Dept Phys, Umea, Sweden. [Wang, X. G.] Harbin Inst Technol, Dept Phys, Harbin, Peoples R China. [Yao, Z. H.] Univ Coll London, Mullard Space Sci Lab, Dorking, Surrey, England. [Yao, Z. H.] Univ Liege, STAR Inst, Lab Phys Atmospher & Planetaire, Liege, Belgium. [Li, Z. Y.; Ji, X. F.; Xiao, C. J.] Peking Univ, Sch Phys, State Key Lab Nucl Phys & Technol, Beijing, Peoples R China. [Pu, Z. Y.; Zong, Q. G.; Fu, S. Y.; Zhou, X. Z.] Peking Univ, Sch Earth & Space Sci, Beijing, Peoples R China. [Zhang, H.] Univ Alaska Fairbanks, Dept Phys, Fairbanks, AK USA. [Zhang, H.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. [Russell, C. T.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA. [Giles, B. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Guo, R. L.; Sun, W. J.] Chinese Acad Sci, Inst Geol & Geophys, Key Lab Earth & Planetary Phys, Beijing, Peoples R China. [Sun, W. J.] Swedish Inst Space Phys, Uppsala, Sweden. [Sun, W. J.; Liu, J.] Chinese Acad Sci, Natl Space Sci Ctr, State Key Lab Space Weather, Beijing, Peoples R China. [Huang, S. Y.] Wuhan Univ, Sch Elect Informat, Wuhan, Peoples R China. RP Shi, QQ (reprint author), Shandong Univ, Inst Space Sci, Shandong Prov Key Lab Opt Astron & Solar Terr Env, Weihai, Peoples R China. EM sqq@pku.edu.cn OI Yao, Zhonghua/0000-0001-6826-2486 FU National Natural Science Foundation of China [41574157, 41322031, 41628402]; European Union FX We are very grateful to the instrumental teams of MMS for providing magnetic field and plasma data. All MMS data can be obtained from the MMS Science Data Center (https://lasp.colorado.edu/mms/sdc/public/). This work was supported by the National Natural Science Foundation of China (grants 41574157, 41322031, and 41628402). Z. H. Yao is a Marie-Curie COFUND postdoctoral fellow at the University of Liege. Cofunded by the European Union. NR 86 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 FEB PY 2017 VL 122 IS 2 BP 1990 EP 2000 DI 10.1002/2016JA023858 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EO9QJ UT WOS:000397022900038 ER PT J AU Lapenta, G Berchem, J Zhou, M Walker, RJ El-Alaoui, M Goldstein, ML Paterson, WR Giles, BL Pollock, CJ Russell, CT Strangeway, RJ Ergun, RE Khotyaintsev, YV Torbert, RB Burch, JL AF Lapenta, G. Berchem, J. Zhou, M. Walker, R. J. El-Alaoui, M. Goldstein, M. L. Paterson, W. R. Giles, B. L. Pollock, C. J. Russell, C. T. Strangeway, R. J. Ergun, R. E. Khotyaintsev, Y. V. Torbert, R. B. Burch, J. L. TI On the origin of the crescent-shaped distributions observed by MMS at the magnetopause SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MAGNETIC RECONNECTION; EARTHS MAGNETOTAIL; DIFFUSION REGION; PLASMA; MULTISCALE; SYSTEMS; SHEET; LAYER AB MMS observations recently confirmed that crescent-shaped electron velocity distributions in the plane perpendicular to the magnetic field occur in the electron diffusion region near reconnection sites at Earth's magnetopause. In this paper, we reexamine the origin of the crescent-shaped distributions in the light of our new finding that ions and electrons are drifting in opposite directions when displayed in magnetopause boundary-normal coordinates. Therefore, E x B drifts cannot cause the crescent shapes. We performed a high-resolution multiscale simulation capturing subelectron skin-depth scales. The results suggest that the crescent-shaped distributions are caused by meandering orbits without necessarily requiring any additional processes found at the magnetopause such as the highly asymmetric magnetopause ambipolar electric field. We use an adiabatic Hamiltonian model of particle motion to confirm that conservation of canonical momentum in the presence of magnetic field gradients causes the formation of crescent shapes without invoking asymmetries or the presence of an E x B drift. An important consequence of this finding is that we expect crescent-shaped distributions also to be observed in the magnetotail, a prediction that MMS will soon be able to test. C1 [Lapenta, G.] Univ Leuven, Dept Wiskunde, Leuven, Belgium. [Berchem, J.; Zhou, M.; El-Alaoui, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA. [Walker, R. J.; Russell, C. T.; Strangeway, R. J.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA. [Goldstein, M. L.] Space Sci Inst, Boulder, CO USA. [Paterson, W. R.; Giles, B. L.; Pollock, C. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Ergun, R. E.] Univ Colorado, LASP, Boulder, CO 80309 USA. [Khotyaintsev, Y. V.] Swedish Inst Space Phys, Uppsala, Sweden. [Torbert, R. B.] Univ New Hampshire, Space Phys & Astron, Durham, NH 03824 USA. [Burch, J. L.] Southwest Res Inst, San Antonio, TX USA. RP Lapenta, G (reprint author), Univ Leuven, Dept Wiskunde, Leuven, Belgium. EM giovanni.lapenta@wis.kuleuven.be OI Russell, Christopher/0000-0003-1639-8298 FU Magnetospheric Multiscale Mission Interdisciplinary Scientist at UCLA [NNX08AO48G]; NASA Geospace [NNX12AD13G]; NASA Heliospheric Grand Challenges [NNX14AI16G]; Belgian Space Policy IUAP; KULeuven BOF; GOA; EC project DEEP-ER FX This work was supported by a Magnetospheric Multiscale Mission Interdisciplinary Scientist grant (NASA grant NNX08AO48G) at UCLA, a NASA Geospace grant (NNX12AD13G), and a NASA Heliospheric Grand Challenges grant (NNX14AI16G). One of the authors (G.L.) acknowledges partial support from the Belgian Space Policy IUAP grant CHARM, from KULeuven BOF and GOA grants, and from the EC project DEEP-ER. The computations were carried out at the NASA Advanced Supercomputing Facilities (Pleiades at NAS and Discover at NCCS). The data produced by the simulation are stored in HDF5 format on the NASA-NAS data server Lou. NR 39 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 FEB PY 2017 VL 122 IS 2 BP 2024 EP 2039 DI 10.1002/2016JA023290 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EO9QJ UT WOS:000397022900041 ER PT J AU Teh, WL Nakamura, TKM Nakamura, R Baumjohann, W Russell, CT Pollock, C Lindqvist, PA Ergun, RE Burch, JL Torbert, RB Giles, BL AF Teh, W. -L. Nakamura, T. K. M. Nakamura, R. Baumjohann, W. Russell, C. T. Pollock, C. Lindqvist, P. -A. Ergun, R. E. Burch, J. L. Torbert, R. B. Giles, B. L. TI Evolution of a typical ion-scale magnetic flux rope caused by thermal pressure enhancement SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MAGNETOSPHERIC MULTISCALE; INSTRUMENT; PLASMA; MMS AB With high time-resolution field and plasma measurements by the Magnetospheric Multiscale spacecraft, interior fine structures of two ion-scale magnetic flux ropes (similar to 5 and similar to 11 ion inertial length radius) separated by similar to 14 s are resolved. These two ion-scale flux ropes (FR1 and FR2) show non-frozen-in ion behavior and consist of a strong axial magnetic field at the reversal of the negative-then-positive bipolar field component. The negative bipolar field component of the FR2 is found to be depressed, where magnetic pressure and total pressure decrease, but ion and electron thermal pressures increase, a feature akin to a crater-like flux rope. The pressure enhancement is due to the magnetosheath plasma feeding into the flux rope along the field lines. Magnetic field draping and energetic electrons are also observed in the trailing part of the FR2. The ratio of perpendicular and parallel currents indicates that the FR1 appears force-free but the FR2 seems not. Moreover, the FR2 is time-dependent as a result of a low correlation coefficient (CC = 0.75) for the derivation of the deHoffmann-Teller frame using the direct measured electric fields, while the FR1 is in quasi-steady conditions (CC = 0.94). It is concluded that the crater formation within the FR2 can be interpreted by the analytical flux rope simulation as the evolution of typical flux rope to crater-like one due to the thermal pressure enhancement, which could be induced by the depression of transverse magnetic fields of the flux rope. C1 [Teh, W. -L.] Univ Kebangsaan Malaysia, Space Sci Ctr, Inst Climate Change, Bangi, Malaysia. [Nakamura, T. K. M.; Nakamura, R.; Baumjohann, W.] Austrian Acad Sci, Space Res Inst, Graz, Austria. [Russell, C. T.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA. [Russell, C. T.] Denali Sci, Healy, AK USA. [Lindqvist, P. -A.] Royal Inst Technol, Sch Elect Engn, Stockholm, Sweden. [Ergun, R. E.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Burch, J. L.; Torbert, R. B.] Southwest Res Inst, San Antonio, TX USA. [Torbert, R. B.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Giles, B. L.] NASA, Goddard Space Flight Ctr, Green Belt, MD USA. RP Teh, WL (reprint author), Univ Kebangsaan Malaysia, Space Sci Ctr, Inst Climate Change, Bangi, Malaysia. EM waileong.teh@gmail.com OI Baumjohann, Wolfgang/0000-0001-6271-0110; Russell, Christopher/0000-0003-1639-8298 FU Fundamental Research Grant Scheme (FRGS) from the Ministry Education of Malaysia [FRGS/1/2016/STG02/UKM/03/1]; Austrian Science Fund [I2016-N20] FX This work was supported by the Fundamental Research Grant Scheme (FRGS) from the Ministry Education of Malaysia (FRGS/1/2016/STG02/UKM/03/1) and the Austrian Science Fund (FWF: I2016-N20). We are grateful for the dedicated efforts of the entire MMS mission team, including development, science operations, and the Science Data Center at the University of Colorado. The simulations were performed with resources at the Space Research Institute of Austrian Academy of Sciences. MMS data can be downloaded at https:// lasp. colorado. edu/ mms/sdc/public/. W.L.T. and T.K.M.N. will provide the simulation data used to generate the figures in the paper if requested. NR 16 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 FEB PY 2017 VL 122 IS 2 BP 2040 EP 2050 DI 10.1002/2016JA023777 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EO9QJ UT WOS:000397022900042 ER PT J AU Collinson, G Mitchell, D Xu, SS Glocer, A Grebowsky, J Hara, T Lillis, R Espley, J Mazelle, C Sauvaud, JA Fedorov, A Liemohn, M Andersson, L Jakosky, B AF Collinson, Glyn Mitchell, David Xu, Shaosui Glocer, Alex Grebowsky, Joseph Hara, Takuya Lillis, Robert Espley, Jared Mazelle, Christian Sauvaud, Jean-Andre Fedorov, Andrey Liemohn, Mike Andersson, Laila Jakosky, Bruce TI Electric Mars: A large trans-terminator electric potential drop on closed magnetic field lines above Utopia Planitia SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID POLAR WIND; PLASMA ACCELERATION; GLOBAL SURVEYOR; VENUS; IONOSPHERE; ESCAPE; ANOMALIES; BOUNDARY; FLUXES; MODEL AB Parallel electric fields and their associated electric potential structures play a crucial role in ionospheric-magnetospheric interactions at any planet. Although there is abundant evidence that parallel electric fields play key roles in Martian ionospheric outflow and auroral electron acceleration, the fields themselves are challenging to directly measure due to their relatively weak nature. Using measurements by the Solar Wind Electron Analyzer instrument aboard the NASA Mars Atmosphere and Volatile EvolutioN (MAVEN) Mars Scout, we present the discovery and measurement of a substantial (Phi(Mars) = 7.7 +/- 0.6 V) parallel electric potential drop on closed magnetic field lines spanning the terminator from day to night above the great impact basin of Utopia Planitia, a region largely free of crustal magnetic fields. A survey of the previous 26 orbits passing over a range of longitudes revealed similar signatures on seven orbits, with a mean potential drop (Phi(Mars)) of 10.9 +/- 0.8 V, suggestive that although trans-terminator electric fields of comparable strength are not ubiquitous, they may be common, at least at these northerly latitudes. C1 [Collinson, Glyn; Glocer, Alex; Grebowsky, Joseph; Espley, Jared] NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. [Collinson, Glyn] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Mitchell, David; Xu, Shaosui; Hara, Takuya; Lillis, Robert] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Mazelle, Christian; Sauvaud, Jean-Andre; Fedorov, Andrey] CNRS, Inst Rech Astrophys & Planetol, Toulouse, France. [Mazelle, Christian; Sauvaud, Jean-Andre; Fedorov, Andrey] Univ Paul Sabatier, Toulouse, France. [Liemohn, Mike] Univ Michigan, Space Phys Res Lab, Ann Arbor, MI 48109 USA. [Andersson, Laila; Jakosky, Bruce] Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA. RP Collinson, G (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA.; Collinson, G (reprint author), Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. EM glyn.collinson@gmail.com FU CNES FX MAVEN data are available from the NASA Planetary Data System. This work was partially supported by the CNES for the part based on observations with the SWEA instrument embarked on MAVEN. NR 38 TC 1 Z9 1 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 FEB PY 2017 VL 122 IS 2 BP 2260 EP 2271 DI 10.1002/2016JA023589 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EO9QJ UT WOS:000397022900058 ER PT J AU Zettergren, MD Snively, JB Komjathy, A Verkhoglyadova, OP AF Zettergren, M. D. Snively, J. B. Komjathy, A. Verkhoglyadova, O. P. TI Nonlinear ionospheric responses to large-amplitude infrasonic-acoustic waves generated by undersea earthquakes SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID TOHOKU-OKI EARTHQUAKE; ELECTRON-CONTENT OBSERVATION; PACIFIC COAST; GRAVITY-WAVES; TSUNAMI; FIELD; DISTURBANCES; PROPAGATION; SIMULATION AB Numerical models of ionospheric coupling with the neutral atmosphere are used to investigate perturbations of plasma density, vertically integrated total electron content (TEC), neutral velocity, and neutral temperature associated with large-amplitude acoustic waves generated by the initial ocean surface displacements from strong undersea earthquakes. A simplified source model for the 2011 Tohoku earthquake is constructed from estimates of initial ocean surface responses to approximate the vertical motions over realistic spatial and temporal scales. Resulting TEC perturbations from modeling case studies appear consistent with observational data, reproducing pronounced TEC depletions which are shown to be a consequence of the impacts of nonlinear, dissipating acoustic waves. Thermospheric acoustic compressional velocities are similar to +/- 250-300 m/s, superposed with downward flows of similar amplitudes, and temperature perturbations are similar to 300 K, while the dominant wave periodicity in the thermosphere is similar to 3-4 min. Results capture acoustic wave processes including reflection, onset of resonance, and nonlinear steepening and dissipation-ultimately leading to the formation of ionospheric TEC depletions "holes"-that are consistent with reported observations. Three additional simulations illustrate the dependence of atmospheric acoustic wave and subsequent ionospheric responses on the surface displacement amplitude, which is varied from the Tohoku case study by factors of 1/100, 1/10, and 2. Collectively, results suggest that TEC depletions may only accompany very-large amplitude thermospheric acoustic waves necessary to induce a nonlinear response, here with saturated compressional velocities similar to 200-250 m/s generated by sea surface displacements exceeding similar to 1 m occurring over a 3 min time period. C1 [Zettergren, M. D.; Snively, J. B.] Embry Riddle Aeronaut Univ, Dept Phys Sci, Daytona Beach, FL USA. [Zettergren, M. D.; Snively, J. B.] Embry Riddle Aeronaut Univ, Ctr Space & Atmospher Res, Daytona Beach, FL USA. [Zettergren, M. D.] Boston Univ, Ctr Space Phys, Boston, MA USA. [Komjathy, A.; Verkhoglyadova, O. P.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Zettergren, MD (reprint author), Embry Riddle Aeronaut Univ, Dept Phys Sci, Daytona Beach, FL USA.; Zettergren, MD (reprint author), Embry Riddle Aeronaut Univ, Ctr Space & Atmospher Res, Daytona Beach, FL USA.; Zettergren, MD (reprint author), Boston Univ, Ctr Space Phys, Boston, MA USA. EM zettergm@erau.edu FU NASA [NNX14AQ39G]; NSF CAREER [AGS-1255181, AGS-1151746] FX Research was supported by NASA grant NNX14AQ39G to Embry-Riddle Aeronautical University. Models used in this study were developed under support from NSF CAREER grants AGS-1255181 and AGS-1151746. Portions of this work were done at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Data used to generate plots are available upon request to 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 FEB PY 2017 VL 122 IS 2 BP 2272 EP 2291 DI 10.1002/2016JA023159 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EO9QJ UT WOS:000397022900059 ER PT J AU England, SL Liu, G Yigit, E Mahaffy, PR Elrod, M Benna, M Nakagawa, H Terada, N Jakosky, B AF England, S. L. Liu, G. Yigit, E. Mahaffy, P. R. Elrod, M. Benna, M. Nakagawa, H. Terada, N. Jakosky, B. TI MAVEN NGIMS observations of atmospheric gravity waves in the Martian thermosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID TITANS UPPER-ATMOSPHERE; MARS GLOBAL SURVEYOR; THERMAL STRUCTURE; IN-SITU; ACCELEROMETER; TIDES; TEMPERATURE; AEROBRAKING; DENSITY; VENUS AB Gravity waves have a significant impact on both the dynamics and energy budget of the Martian thermosphere. Strong density variations of spatial scales indicative of gravity waves have previously been identified in this region by using in situ observations. Here we use observations from the Neutral Gas and Ion Mass Spectrometer (NGIMS) mass spectrometer on Mars Atmosphere and Volatile EvolutioN Mission to identify such waves in the observations of different atmospheric species. The wave signatures seen in CO2 and Ar are almost identical, whereas the wave signature seen in N-2, which is lighter and has a larger scale height, is generally smaller in amplitude and slightly out of phase with those seen in CO2 and Ar. Examination of the observed wave properties in these three species suggests that relatively long vertical wavelength atmospheric gravity waves are the likely source of the waves seen by NGIMS in the upper thermosphere. A two-fluid linear model of the wave perturbations in CO2 and N-2 has been used to find the best fit intrinsic wave parameters that match the observed features in these two species. We report the first observationally based estimate of the heating and cooling rates of the Martian thermosphere created by the waves observed in this region. The observed wave density amplitudes are anticorrelated with the background atmospheric temperature. The estimated heating rates show a weak positive correlation with the wave amplitude, whereas the cooling rates show a clearer negative correlation with the wave amplitude. Our estimates support previous model-based findings that atmospheric gravity waves are a significant source of both heating and cooling. C1 [England, S. L.; Liu, G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Yigit, E.] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA. [Mahaffy, P. R.; Elrod, M.; Benna, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nakagawa, H.; Terada, N.] Tohoku Univ, Dept Geophys, Sendai, Miyagi, Japan. [Jakosky, B.] Univ Colorado, Lab Atmosphere & Space Phys, Boulder, CO 80309 USA. RP England, SL (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM england@ssl.berkeley.edu OI Yigit, Erdal/0000-0002-2819-2521 FU NASA [NNX13AO36G]; NASA through the Mars Exploration Program FX All data used in the study are archived in the Planetary Atmospheres Node of the Planetary Data System (http://pds.nasa.gov). S.L.E., G.L., and E.Y. were supported by NASA through grant NNX13AO36G. The MAVEN mission has been funded by NASA through the Mars Exploration Program. NR 54 TC 1 Z9 1 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 FEB PY 2017 VL 122 IS 2 BP 2310 EP 2335 DI 10.1002/2016JA023475 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EO9QJ UT WOS:000397022900062 ER PT J AU Terada, N Leblanc, F Nakagawa, H Medvedev, AS Yigit, E Kuroda, T Hara, T England, SL Fujiwara, H Terada, K Seki, K Mahaffy, PR Elrod, M Benna, M Grebowsky, J Jakosky, BM AF Terada, Naoki Leblanc, Francois Nakagawa, Hiromu Medvedev, Alexander S. Yigit, Erdal Kuroda, Takeshi Hara, Takuya England, Scott L. Fujiwara, Hitoshi Terada, Kaori Seki, Kanako Mahaffy, Paul R. Elrod, Meredith Benna, Mehdi Grebowsky, Joseph Jakosky, Bruce M. TI Global distribution and parameter dependences of gravity wave activity in the Martian upper thermosphere derived from MAVEN/NGIMS observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID GENERAL-CIRCULATION MODEL; OXYGEN-ION PRECIPITATION; UPPER-ATMOSPHERE; MIDDLE ATMOSPHERE; MARS; VENUS; PROPAGATION; IONOSPHERE; EQUINOX; EARTH AB Wavelike perturbations in the Martian upper thermosphere observed by the Neutral Gas Ion Mass Spectrometer (NGIMS) onboard the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft have been analyzed. The amplitudes of small-scale perturbations with apparent wavelengths between similar to 100 and similar to 500 km in the Ar density around the exobase show a clear dependence on temperature (T-0) of the upper thermosphere. The average amplitude of the perturbations is similar to 10% on the dayside and similar to 20% on the nightside, which is about 2 and 10 times larger than those observed in the Venusian upper thermosphere and in the low-latitude region of Earth's upper thermosphere, respectively. The amplitudes are inversely proportional to T-0, suggesting saturation due to convective instability in the Martian upper thermosphere. After removing the dependence on T-0, dependences of the average amplitude on the geographic latitude and longitude and solar wind parameters are found to be not larger than a few percent. These results suggest that the amplitudes of small-scale perturbations are mainly determined by convective breaking/saturation in the upper thermosphere on Mars, unlike those on Venus and Earth. C1 [Terada, Naoki; Nakagawa, Hiromu; Kuroda, Takeshi; Terada, Kaori] Tohoku Univ, Grad Sch Sci, Sendai, Miyagi, Japan. [Leblanc, Francois] UPMC Univ Paris 06, LATMOS IPSL, Sorbonne Univ, UVSQ,CNRS, Paris, France. [Medvedev, Alexander S.] Max Planck Inst Solar Syst Res, Gottingen, Germany. [Medvedev, Alexander S.] Georg August Univ, Inst Astrophys, Gottingen, Germany. [Yigit, Erdal] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA. [Kuroda, Takeshi] Natl Inst Informat & Commun Technol, Big Data Integrat Res Ctr, Big Data Analyt Lab, Tokyo, Japan. [Hara, Takuya; England, Scott L.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Fujiwara, Hitoshi] Seikei Univ, Fac Sci & Technol, Tokyo, Japan. [Seki, Kanako] Univ Tokyo, Grad Sch Sci, Tokyo, Japan. [Mahaffy, Paul R.; Elrod, Meredith; Benna, Mehdi; Grebowsky, Joseph] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Elrod, Meredith] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Benna, Mehdi] Univ Maryland Baltimore Cty, CRESST, Catonsville, MD USA. [Jakosky, Bruce M.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. RP Terada, N (reprint author), Tohoku Univ, Grad Sch Sci, Sendai, Miyagi, Japan. EM teradan@pat.gp.tohoku.ac.jp OI Yigit, Erdal/0000-0002-2819-2521 FU Japan Society for the Promotion of Science (JSPS) [15H03731, 16H02229]; program "Systeme Solaire" of CNES; French space administration; NASA [NNX13AO36G]; NASA through the Mars Exploration Program; NASA's MAVEN Participating Scientist Program [12-MAVENPS12-0017] FX This work was supported by Grant-in-Aid for Scientific Research (B) 15H03731 and for Scientific Research (A) 16H02229 from the Japan Society for the Promotion of Science (JSPS). F.L. is indebted to the program "Systeme Solaire" of CNES, the French space administration, for its financial support on MAVEN. S.L.E. and E.Y. were supported by NASA through grant NNX13AO36G. The MAVEN project is supported by NASA through the Mars Exploration Program. This work was conducted under NASA's MAVEN Participating Scientist Program (proposal 12-MAVENPS12-0017, PI: K. Seki). The NGIMS, SWIA, MAG, and EUV data are available in the Planetary Data System Archive (http://atmos.nmsu.edu/data_and_services/atmospheres_data/MAVEN/maven_ma in.html). NR 78 TC 1 Z9 1 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 FEB PY 2017 VL 122 IS 2 BP 2374 EP 2397 DI 10.1002/2016JA023476 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EO9QJ UT WOS:000397022900066 ER PT J AU Emmert, JT Mannucci, AJ McDonald, SE Vergados, P AF Emmert, J. T. Mannucci, A. J. McDonald, S. E. Vergados, P. TI Attribution of interminimum changes in global and hemispheric total electron content SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SOLAR MINIMUM; GPS DATA; IONOSPHERE AB We use a new data product of electron column density (total electron content, or TEC) maps to estimate and attribute the interminimum changes (the differences between annual averages centered on the 2008 and 1996 solar minima) in TEC global and hemispheric averages (dividing the globe in three different ways). We attribute the observed changes to corresponding changes in solar and geomagnetic activity. The new TEC map product was constructed with temporally consistent processing, and it resolves some of the apparent inconsistencies of earlier studies. The estimated global average TEC interminimum change is -19.3% +/- 1.0% (2 sigma uncertainty), of which -9.1% is attributable to the interminimum change in solar extreme ultraviolet (EUV) irradiance (as represented by the F-10.7 index), -2.2% is attributable to the change in geomagnetic activity (Kp index), and -9.3% remains unattributed. The hemispheric results are very similar to the global results, but the values tend to be slightly larger in the Southern Hemisphere, at low latitudes, and at night, compared to the opposing respective hemispheres. The interminimum changes and temporal variations of thermospheric mass density anomalies (i.e., the difference between the data and the empirical model) are very similar to those of the global and hemispheric TEC residuals, suggesting that they are driven by a common, globally distributed mechanism. Thermospheric composition changes and additional (unobserved) decreases in solar EUV irradiance are possible mechanisms behind the TEC and mass density unattributed changes; we estimate a plausible range of -6% to -13% for the solar EUV irradiance interminimum change. C1 [Emmert, J. T.; McDonald, S. E.] US Naval Res Lab, Space Sci Div, Washington, DC 20375 USA. [Mannucci, A. J.; Vergados, P.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Emmert, JT (reprint author), US Naval Res Lab, Space Sci Div, Washington, DC 20375 USA. EM john.emmert@nrl.navy.mil FU NASA's Heliophysics Supporting Research Program [NNH14AX49I]; National Aeronautics and Space Administration FX This study was supported by NASA's Heliophysics Supporting Research Program (grant NNH14AX49I). The JPL35, JPL50, and JPL100 TEC map products are available upon request from the authors; global and hemispheric averages are provided in the supporting information. The IGS, CODE, JPL, ESA, and UPC TEC map products were obtained from ftp://cddis.gsfc.nasa.gov/gps/products/ionex/. F10.7 and Kp indices were obtained from ftp://ftp.ngdc.noaa.gov/STP/GEOMAGNETIC_DATA/INDICES/KP_AP/. The orbit-derived density data used in this study are contained in the supporting information of Emmert [2015a]. Portions of this research were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. J.T.E. thanks J.M. Picone for helpful discussions. NR 33 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 FEB PY 2017 VL 122 IS 2 BP 2424 EP 2439 DI 10.1002/2016JA023680 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EO9QJ UT WOS:000397022900068 ER PT J AU Humberset, BK Gjerloev, JW Samara, M Michell, RG AF Humberset, B. K. Gjerloev, J. W. Samara, M. Michell, R. G. TI Scale size-dependent characteristics of the nightside aurora SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID PARTICLE OBSERVATIONS; IMAGE-FUV AB We have determined the spatiotemporal characteristics of the magnetosphere-ionosphere (M-I) coupling using auroral imaging. Observations at fixed positions for an extended period of time are provided by a ground-based all-sky imager measuring the 557.7 nm auroral emissions. We report on a single event of nightside aurora (similar to 22 magnetic local time) preceding a substorm onset. To determine the spatiotemporal characteristics, we perform an innovative analysis of an all-sky imager movie (19 min duration, images at 3.31 Hz) that combines a two-dimensional spatial fast Fourier transform with a temporal correlation. We find a scale size-dependent variability where the largest scale sizes are stable on timescales of minutes while the small scale sizes are more variable. When comparing two smaller time intervals of different types of auroral displays, we find a variation in their characteristics. The characteristics averaged over the event are in remarkable agreement with the spatiotemporal characteristics of the nightside field-aligned currents during moderately disturbed times. Thus, two different electrodynamical parameters of the M-I coupling show similar behavior. This gives independent support to the claim of a system behavior that uses repeatable solutions to transfer energy and momentum from the magnetosphere to the ionosphere. C1 [Humberset, B. K.; Gjerloev, J. W.] Univ Bergen, Dept Phys & Technol, Birkeland Ctr Space Sci, Bergen, Norway. [Gjerloev, J. W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Samara, M.; Michell, R. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Michell, R. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Humberset, BK (reprint author), Univ Bergen, Dept Phys & Technol, Birkeland Ctr Space Sci, Bergen, Norway. EM beate.humberset@uib.no FU Research Council of Norway [223252] FX This study was supported by the Research Council of Norway under contract 223252. The authors acknowledge the use of SuperMAG indices and all-sky imager data from the Multi-spectral Observatory of Sensitive EMCCDs (MOOSE). The SuperMAG indices were obtained freely from supermag.uib.no. We greatly acknowledge James Weygand for the ACE solar wind data. MOOSE all-sky imager data were obtained from R.G. Michell and M. Samara. The data analyzed in this study are available upon request from the authors. NR 22 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 FEB PY 2017 VL 122 IS 2 BP 2455 EP 2466 DI 10.1002/2016JA023695 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EO9QJ UT WOS:000397022900070 ER PT J AU Elrod, MK Bougher, S Bell, J Mahaffy, PR Benna, M Stone, S Yelle, R Jakosky, B AF Elrod, M. K. Bougher, S. Bell, J. Mahaffy, P. R. Benna, M. Stone, S. Yelle, R. Jakosky, B. TI He bulge revealed: He and CO2 diurnal and seasonal variations in the upper atmosphere of Mars as detected by MAVEN NGIMS SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MARTIAN ATMOSPHERE; HELIUM; THERMOSPHERE; VENUS; IONOSPHERE; MODEL; CIRCULATION; EVOLUTION; EUVE AB Analysis of the Neutral Gas and Ion Mass Spectrometer (NGIMS) on the Mars Atmosphere Volatiles and EvolutioN (MAVEN) spacecraft closed source data from all orbits with good pointing revealed an enhanced Helium [He] density on the nightside orbits and a depressed He density on the dayside by about a factor of 10-20. He was also found to be larger in the polar regions than in the equatorial regions. The northern polar winter nightside He bulge was approximately twice that of the northern polar summer nightside bulge. The first 6 weeks of the MAVEN prime mission had periapsis at high latitudes on the nightside during northern winter, followed by the midlatitudes on the dayside moving to low latitudes on the nightside returning to the high latitudes during northern summer. In this study we examined the NGIMS data not only in the different latitudes but sorted by solar longitude (Ls) in order to separate the diurnal or local solar time (LST) effects from the seasonal effects. The Mars Global Ionosphere-Thermosphere Model (M-GITM) has predicted the formation of a He bulge in the upper atmosphere of Mars on the nightside early morning hours (Ls =2-5h) with more He collecting around the poles. Taking a slice at constant altitude across all orbits indicates corresponding variations in He and CO2 with respect to LST and Ls and a diurnal and seasonal dependence. C1 [Elrod, M. K.; Mahaffy, P. R.; Benna, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Elrod, M. K.] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Bougher, S.] Univ Michigan, Climate & Space Sci & Engn Dept, Ann Arbor, MI 48109 USA. [Bell, J.] Natl Inst Aerosp, Hampton, VA USA. [Benna, M.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21228 USA. [Stone, S.; Yelle, R.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ USA. [Stone, S.; Yelle, R.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Jakosky, B.] Univ Colorado Boulder, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. RP Elrod, MK (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Elrod, MK (reprint author), Univ Maryland, CRESST, College Pk, MD 20742 USA. EM meredith.k.elrod@nasa.gov OI Bougher, Stephen/0000-0002-4178-2729 FU NASA through the Mars Exploration Program FX Special acknowledgments to the MAVEN NGIMS team at NASA Goddard SFC, and the MAVEN operations team at LASP and Lockheed Martin in Colorado. All data are archived in the Planetary Atmospheres Node of the Planetary Data System (http://pds.nasa.gov). Data through 15 August 2016 are available on the Planetary Data System (PDS4) (e.g., mvn_ngi_l2_csn-abund-14015_20141018T100458_v06_r02.csvmvn_ngi_l2_cso-abu nd-20708_20160804T173834_v06_r02.csv). These data are available upon request. The MAVEN mission has been funded by NASA through the Mars Exploration Program. NR 31 TC 1 Z9 1 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 FEB PY 2017 VL 122 IS 2 BP 2564 EP 2573 DI 10.1002/2016JA023482 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EO9QJ UT WOS:000397022900077 ER PT J AU Slaba, TC Bahadori, AA Reddell, BD Singleterry, RC Clowdsley, MS Blattnig, SR AF Slaba, Tony C. Bahadori, Amir A. Reddell, Brandon D. Singleterry, Robert C. Clowdsley, Martha S. Blattnig, Steve R. TI Optimal shielding thickness for galactic cosmic ray environments SO LIFE SCIENCES IN SPACE RESEARCH LA English DT Article DE Space radiation; Radiation shielding; Radiation transport; HZETRN; Geant4; FLUKA; PHITS; MCNP6 ID INTRANUCLEAR-CASCADE CALCULATION; ACCURATE UNIVERSAL PARAMETERIZATION; ABSORPTION CROSS-SECTIONS; SPACE RADIATION; HIGH-ENERGY; CANCER-RISKS; MODELS; PARTICLE; HZETRN; SIMULATION AB Models have been extensively used in the past to evaluate and develop material optimization and shield design strategies for astronauts exposed to galactic cosmic rays (GCR) on long duration missions. A persistent conclusion from many of these studies was that passive shielding strategies are inefficient at reducing astronaut exposure levels and the mass required to significantly reduce the exposure is infeasible, given launch and associated cost constraints. An important assumption of this paradigm is that adding shielding mass does not substantially increase astronaut exposure levels. Recent studies with HZETRN have suggested, however, that dose equivalent values actually increase beyond similar to 20 g/cm(2) of aluminum shielding, primarily as a result of neutron build-up in the shielding geometry. In this work, various Monte Carlo (MC) codes and 3DHZETRN are evaluated in slab geometry to verify the existence of a local minimum in the dose equivalent versus aluminum thickness curve near 20 g/cm(2). The same codes are also evaluated in polyethylene shielding, where no local minimum is observed, to provide a comparison between the two materials. Results are presented so that the physical interactions driving build-up in dose equivalent values can be easily observed and explained. Variation of transport model results for light ions (Z = 2) and neutron-inducedtargetfragments, whichcontributesignificantlytodose equivalentforthick shielding, is also highlighted and indicates that significant uncertainties are still present in the models for some particles. The 3DHZETRN code is then further evaluated over a range of related slab geometries to draw closer connection to more realistic scenarios. Future work will examine these related geometries in more detail. Published by Elsevier Ltd on behalf of The Committee on Space Research (COSPAR). C1 [Slaba, Tony C.; Singleterry, Robert C.; Clowdsley, Martha S.; Blattnig, Steve R.] NASA Langley Res Ctr, Hampton, VA 23681 USA. [Bahadori, Amir A.] Kansas State Univ, Manhattan, KS 66506 USA. [Reddell, Brandon D.] NASA Johnson Space Ctr, Houston, TX 77004 USA. RP Slaba, TC (reprint author), 2 West Reid St,Mail Stop 188E, Hampton, VA 23681 USA. EM tony.c.slaba@nasa.gov FU Advanced Radiation Protection Project under the Game Changing Division of the Space Technology Mission Directorate of NASA FX This work was supported by the Advanced Radiation Protection Project under the Game Changing Division of the Space Technology Mission Directorate of NASA. NR 67 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 2214-5524 EI 2214-5532 J9 LIFE SCI SPACE RES JI Life Sci. Space Res. PD FEB PY 2017 VL 12 BP 1 EP 15 DI 10.1016/j.lssr.2016.12.003 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EO9ZH UT WOS:000397046100001 PM 28212703 ER PT J AU Lu, T Zhang, Y Wong, M Feiveson, A Gaza, R Stoffle, N Wang, HC Wilson, B Rohde, L Stodieck, L Karouia, F Wu, HL AF Lu, Tao Zhang, Ye Wong, Michael Feiveson, Alan Gaza, Ramona Stoffle, Nicholas Wang, Huichen Wilson, Bobby Rohde, Larry Stodieck, Louis Karouia, Fathi Wu, Honglu TI Detection of DNA damage by space radiation in human fibroblasts flown on the International Space Station SO LIFE SCIENCES IN SPACE RESEARCH LA English DT Article DE Space radiation; gamma-H2AX; Particle track ID ENERGETIC HEAVY-IONS; LOW-EARTH-ORBIT; DOSE-RATE; H2AX PHOSPHORYLATION; HUMAN-CELLS; GAMMA-IRRADIATION; CHROMOSOME-ABERRATIONS; PARTICLE RADIATION; LIGHT-FLASHES; BRAGG CURVE AB Although charged particles in space have been detected with radiation detectors on board spacecraft since the discovery of the Van Allen Belts, reports on the effects of direct exposure to space radiation in biological systems have been limited. Measurement of biological effects of space radiation is challenging due to the low dose and low dose rate nature of the radiation environment, and due to the difficulty in distinguishing the radiation effects from microgravity and other space environmental factors. In astronauts, only a few changes, such as increased chromosome aberrations in their lymphocytes and early onset of cataracts, are attributed primarily to their exposure to space radiation. In this study, cultured human fibroblasts were flown on the International Space Station (ISS). Cells were kept at 37 degrees C in space for 14 days before being fixed for analysis of DNA damage with the gamma-H2AX assay. The 3-dimensional.-H2AX foci were captured with a laser confocal microscope. Quantitative analysis revealed several foci that were larger and displayed a track pattern only in the Day 14 flight samples. To confirm that the foci data from the flight study was actually induced from space radiation exposure, cultured human fibroblasts were exposed to low dose rate.rays at 37 degrees C. Cells exposed to chronic.rays showed similar foci size distribution in comparison to the non-exposed controls. The cells were also exposed to low-and high-LET protons, and high-LET Fe ions on the ground. Our results suggest that in G1 human fibroblasts under the normal culture condition, only a small fraction of large size foci can be attributed to high-LET radiation in space. Published by Elsevier Ltd on behalf of The Committee on Space Research (COSPAR). C1 [Lu, Tao; Wong, Michael; Feiveson, Alan; Gaza, Ramona; Stoffle, Nicholas; Wu, Honglu] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Lu, Tao; Rohde, Larry] Univ Houston Clear Lake, Houston, TX USA. [Zhang, Ye] NASA, Kennedy Space Ctr, Cape Canaveral, FL USA. [Gaza, Ramona; Stoffle, Nicholas] Leidos Explorat & Mission Support, Houston, TX USA. [Wang, Huichen] Prairie View A&M Univ, Prairie View, TX USA. [Wilson, Bobby] Texas Southern Univ, Houston, TX USA. [Stodieck, Louis] BioServe Space Technol, Boulder Creek, CA USA. [Karouia, Fathi] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Karouia, Fathi] Univ Calif San Francisco, San Francisco, CA 94143 USA. RP Wu, HL (reprint author), NASA, Johnson Space Ctr, Houston, TX 77058 USA. EM honglu.wu-1@nasa.gov FU NASA Fundamental Space Biology Program; NASA Human Research Program FX This work was supported by the NASA Fundamental Space Biology Program and the NASA Human Research Program. The flight project was in collaboration with BioServe Space Technologies, and we thank Stefanie Countryman, Jon Beno, Mark Rupert and Shankini Doraisingam for working diligently on the project. We thank Ashleigh Ruggles and Satyanand Narayan of NASA Kennedy Space Center, and Kevin Sato of NASA Ames Research Center for the support during various phases of the project. We also thank Astronaut Thomas Mashburn for performing the experiment on the ISS. NR 46 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 2214-5524 EI 2214-5532 J9 LIFE SCI SPACE RES JI Life Sci. Space Res. PD FEB PY 2017 VL 12 BP 24 EP 31 DI 10.1016/j.lssr.2016.12.004 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EO9ZH UT WOS:000397046100003 PM 28212705 ER PT J AU Fei, L Ikebukuro, K Katsuta, T Kaneko, T Ueno, I Pettit, DR AF Fei, Linhao Ikebukuro, Koichi Katsuta, Takeshi Kaneko, Toshihiro Ueno, Ichiro Pettit, Donald R. TI Effect of Static Deformation on Basic Flow Patterns in Thermocapillary-Driven Free Liquid Film SO MICROGRAVITY SCIENCE AND TECHNOLOGY LA English DT Article DE Thermocapillary-driven flow; Free liquid film; Flow patterns; Surface deformation AB A series of terrestrial, parabolic-flight and onorbit experiments on thermocapillary-driven flows in free liquid films are carried out. We focus on the basic flow patterns induced in the film formed in a rectangular hole by varying the film volume in order to make a comparison with the results of the fluid physics experiments under microgravity conditions conducted by one of the authors, Pettit, on the International Space Station. The free liquid film is formed in a rectangular hole of O(0.1 mm) in thickness under a designated temperature difference between the end walls. The temperature dependence of the surface tension results in a non-uniform surface tension distribution over the free surfaces. A liquid generally has a negative temperature coefficient of surface tension; i.e., the fluid over a free surface is driven from a higher-temperature region to a lower-temperature region. In the case of a thin free liquid film with two free surfaces, however, an unusual flow pattern is realized. That is, the fluid seems to be driven toward the heated region from a colder region. In order to understand the physical mechanism of this behavior in the free liquid film, a series of on-orbit and ground experiments were conducted. We indicate several flow patterns in the film and corresponding film profiles as well as the surface temperature distribution. We also try to illustrate the cross-sectional flow structures in the thin free liquid film with two free surfaces. C1 [Fei, Linhao; Ikebukuro, Koichi; Katsuta, Takeshi; Kaneko, Toshihiro; Ueno, Ichiro] Tokyo Univ Sci, Fac Sci, Dept Mech Engn, Technol, 2641 Yamazaki, Noda, Chiba 2788510, Japan. [Pettit, Donald R.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. RP Ueno, I (reprint author), Tokyo Univ Sci, Fac Sci, Dept Mech Engn, Technol, 2641 Yamazaki, Noda, Chiba 2788510, Japan. EM ich@rs.tus.ac.jp FU Space Utilization Research Committee at Japan Aerospace Exploration Agency (JAXA); Diamond Air Survice, Inc. FX A part of this work is supported by Space Utilization Research Committee at Japan Aerospace Exploration Agency (JAXA). Prof. Katsuo Tsukamoto at Tohoku University, Japan, Ms. Natsuki Ishikawa and Mr. Hiroki Sugioka, former students at Tokyo University of Science, are gratefully acknowledged for their generous and invaluable supports for the parabolic flight experiments. The parabolic flight campaign was awarded by the Diamond Air Survice, Inc. after the 'International Mohri Poster Session' organized by Dr. Mamoru Mohri, a JAXA astronaut, at the 8th Japan-China-Korea Workshop on Microgravity Sciences (Sept. 2010, Miyagi, Japan). The authors DRP and IU acknowledge Dr. Satoshi Matsumoto, JAXA, for giving an invaluable opportunity to realize this collaborative work. NR 10 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0938-0108 EI 1875-0494 J9 MICROGRAVITY SCI TEC JI Microgravity Sci. Technol. PD FEB PY 2017 VL 29 IS 1-2 BP 29 EP 36 DI 10.1007/s12217-016-9523-8 PG 8 WC Engineering, Aerospace; Thermodynamics; Mechanics SC Engineering; Thermodynamics; Mechanics GA EO9SO UT WOS:000397028600004 ER PT J AU Sundaresan, A Mehta, SK Schlegel, TT Russomano, T Pierson, DL Mann, V Mansoor, E Olamigoke, L Okoro, E AF Sundaresan, Alamelu Mehta, Satish K. Schlegel, Todd. T. Russomano, Thais Pierson, Duane L. Mann, Vivek Mansoor, Elvedina Olamigoke, Loretta Okoro, Elvis TI Placental Growth Factor Levels in Populations with High Versus Low Risk for Cardiovascular Disease and Stressful Physiological Environments such as Microgravity: A Pilot Study SO MICROGRAVITY SCIENCE AND TECHNOLOGY LA English DT Article DE PIGF; Catheterization; Coronary artery; disease (CAD); Acute coronary syndrome ACS); Cardiovascular disease AB This pilot study compared placental growth factor (PIGF) levels in populations with high versus low risk for cardiovascular disease. Previous experiments from our laboratory (Sundaresan et al. 2005, 2009) revealed that the angiogenic factor PIGF was up regulated in modeled microgravity conditions in human lymphocytes leading to possible atherogenesis and pathogenesis in microgravity. Since the findings came from microgravity analog experiments, there is a strong link to its usefulness in the microgravity field as a biomarker. It is important to understand, that these findings came from both studies on expression levels of this cardiovascular marker in human lymphocytes in microgravity (in vitro microgravity analog), and a follow up gene expression study in hind limb suspended mice (in vivo microgravity analog). The relevance is enhanced because in life on earth, PIGF is an inflammatory biomarker for cardiovascular disease. Studies on the levels of PIGF would help to reduce the risk and prevention of heart failures in astronauts. If we can use this marker to predict and reduce the risk of cardiac events in astronauts and pilots, it would significantly help aerospace medicine operations. The investigations here confirmed that in a cardiovascular stressed population such as coronary artery disease (CAD) and acute coronary syndrome (ACS) patients, PIGF could be overexpressed. We desired to re-evaluate this marker in patients with cardiovascular disease in our own study. PIGF is a marker of inflammation and a predictor of short-term and long-term adverse outcome in ACS. In addition, elevated PIGF levels may be associated with increased risk for CAD. PIGF levels were determined in thirty-one patients undergoing cardiovascular catheterization for reasons other than ACS and in thirty-three low-risk asymptomatic subjects. Additional data on traditional cardiovascular risk factors for both populations were also compiled and compared. We found that PIGF levels were significantly higher in the high-risk population as compared to low-risk population. Also we were able to ascertain that PIGF levels were inversely correlated with HDL-cholesterol but directly correlated with the triglyceride levels. With further validation, PIGF may prove a useful addition to the armamentarium of noninvasive biomarkers for cardiovascular disease including a new area of stressful physiological conditions such as microgravity. C1 [Sundaresan, Alamelu; Mann, Vivek; Mansoor, Elvedina; Olamigoke, Loretta; Okoro, Elvis] Texas Southern Univ, Dept Biol, 3100 Cleburne St, Houston, TX 77004 USA. [Schlegel, Todd. T.; Pierson, Duane L.] NASA, Human Hlth Performance Div, Johnson Space Ctr, 2101 E NASA Pkwy, Houston, TX 77058 USA. [Mehta, Satish K.] Wyle Labs, Houston, TX USA. [Russomano, Thais] Pontificia Univ Catolica Rio Grande do Sul, Micrograv Ctr, Porto Alegre, Brazil. RP Sundaresan, A (reprint author), Texas Southern Univ, Dept Biol, 3100 Cleburne St, Houston, TX 77004 USA. EM sundaresana@tsu.edu NR 7 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0938-0108 EI 1875-0494 J9 MICROGRAVITY SCI TEC JI Microgravity Sci. Technol. PD FEB PY 2017 VL 29 IS 1-2 BP 145 EP 149 DI 10.1007/s12217-016-9534-5 PG 5 WC Engineering, Aerospace; Thermodynamics; Mechanics SC Engineering; Thermodynamics; Mechanics GA EO9SO UT WOS:000397028600015 ER PT J AU Seol, ML Han, JW Moon, DI Meyyappan, M AF Seol, Myeong-Lok Han, Jin-Woo Moon, Dong-Il Meyyappan, M. TI Hysteretic behavior of contact force response in triboelectric nanogenerator SO NANO ENERGY LA English DT Article DE Triboelectric nanogenerator; Contact electrification; Triboelectric charging; Hysteresis; Contact pressure; Memory ID ENERGY HARVESTER; ELECTRIFICATION; PERFORMANCE; MODE; TRANSPARENT; GENERATOR; PRESSURE; PACKAGE AB The hysteretic behavior of contact force response in a triboelectric nanogenerator is analyzed as the output performance in response to the applied contact force is found to be dependent on previous contact force history. The counterclockwise hysteresis curve of the contact force versus output power originates from the asymmetric time constant between triboelectric charging and natural discharging, because the charges due to contact electrification do not immediately disappear but gradually decay over a period of hours. Therefore, a low contact force followed immediately after a high contact force results in enhanced output performance but not the reverse order. However, if the intermission time becomes too long, the benefit due to charge balance gets degraded. The experimental results on sweep range and discharging time dependencies agree well with theoretical expectations. C1 [Seol, Myeong-Lok; Han, Jin-Woo; Moon, Dong-Il; Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Seol, ML (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. EM myeonglok.seol@nasa.gov NR 42 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 2211-2855 EI 2211-3282 J9 NANO ENERGY JI Nano Energy PD FEB PY 2017 VL 32 BP 408 EP 413 DI 10.1016/j.nanoen.2016.12.055 PG 6 WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA EO9IZ UT WOS:000397003700050 ER PT J AU Artemyev, AV Mourenas, D Agapitov, OV Blum, L AF Artemyev, A. V. Mourenas, D. Agapitov, O. V. Blum, L. TI Transverse eV ion heating by random electric field fluctuations in the plasmasphere SO PHYSICS OF PLASMAS LA English DT Article ID MAGNETOSONIC WAVES; CYCLOTRON INSTABILITY; EQUATORIAL NOISE; VELOCITY SPACE; EMIC WAVES; DISTRIBUTIONS; ANISOTROPY; HISS; MAGNETOSPHERE; ENERGIZATION AB Charged particle acceleration in the Earth inner magnetosphere is believed to be mainly due to the local resonant wave-particle interaction or particle transport processes. However, the Van Allen Probes have recently provided interesting evidence of a relatively slow transverse heating of eV ions at distances about 2-3 Earth radii during quiet times. Waves that are able to resonantly interact with such very cold ions are generally rare in this region of space, called the plasmasphere. Thus, non-resonant wave-particle interactions are expected to play an important role in the observed ion heating. We demonstrate that stochastic heating by random transverse electric field fluctuations of whistler (and possibly electromagnetic ion cyclotron) waves could explain this weak and slow transverse heating of H-1 and O-1 ions in the inner magnetosphere. The essential element of the proposed model of ion heating is the presence of trains of random whistler (hiss) wave packets, with significant amplitude modulations produced by strong wave damping, rapid wave growth, or a superposition of wave packets of different frequencies, phases, and amplitudes. Such characteristics correspond to measured characteristics of hiss waves in this region. Using test particle simulations with typical wave and plasma parameters, we demonstrate that the corresponding stochastic transverse ion heating reaches 0.07-0.2 eV/h for protons and 0.007-0.015 eV/h for O-1 ions. This global temperature increase of the Maxwellian ion population from an initial T-i similar to 0: 3 eV could potentially explain the observations. Published by AIP Publishing. C1 [Artemyev, A. V.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Mourenas, D.] Univ Orleans, CNRS, LPC2E, Orleans, France. [Agapitov, O. V.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Blum, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Agapitov, O. V.] Natl Taras Shevchenko Univ Kiev, Dept Phys & Astron, Kiev, Ukraine. RP Artemyev, AV (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. EM aartemyev@igpp.ucla.edu OI AGAPITOV, OLEKSIY/0000-0001-6427-1596 FU JHU/APL [922613]; NASA [16-HGI16_2-0118] FX This work was supported by the JHU/APL Contract No. 922613 (RBSP-EFW), NASA Grant No. 16-HGI16_2-0118. NR 47 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD FEB PY 2017 VL 24 IS 2 AR 022903 DI 10.1063/1.4976713 PG 9 WC Physics, Fluids & Plasmas SC Physics GA EN4YN UT WOS:000396012900063 ER PT J AU Beadles, R Wang, X Horanyi, M AF Beadles, R. Wang, X. Horanyi, M. TI Floating potential measurements in plasmas: From dust to spacecraft SO PHYSICS OF PLASMAS LA English DT Article ID COAGULATION; SURFACES AB We present measurements of the floating potential of spherical probes, used as a model of a dust particle or a spacecraft, immersed in plasmas with a wide range of Debye lengths. Our experimental results verified the theoretical prediction that the probe floating potential is a function of the Debye length. It is shown that, in an argon plasma with the ion to electron temperature ratio similar to 0.01, the magnitude of the floating potential is approximately doubled when the Debye length is changed from larger to smaller than the radius of the probe. Published by AIP Publishing. C1 [Beadles, R.; Wang, X.; Horanyi, M.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA. [Beadles, R.; Wang, X.; Horanyi, M.] NASA, SSERVIs Inst Modeling Plasma Atmospheres & Cosm D, Boulder, CO 80303 USA. RP Beadles, R (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.; Beadles, R (reprint author), NASA, SSERVIs Inst Modeling Plasma Atmospheres & Cosm D, Boulder, CO 80303 USA. OI WANG, XU/0000-0001-8472-7079 FU NASA/SSERVI's Institute for Modeling Plasma, Atmospheres and Cosmic Dust (IMPACT) FX This work was supported by the NASA/SSERVI's Institute for Modeling Plasma, Atmospheres and Cosmic Dust (IMPACT). Part of this work was inspired by discussions within International Team 336: "Plasma Surface Interactions with Airless Bodies in Space and Laboratory" at the International Space Science Institute,Bern,Switzerland. NR 12 TC 0 Z9 0 U1 2 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD FEB PY 2017 VL 24 IS 2 AR 023701 DI 10.1063/1.4975610 PG 3 WC Physics, Fluids & Plasmas SC Physics GA EN4YN UT WOS:000396012900096 ER PT J AU Mori, H Maeda, Y Ueda, Y Nakazawa, K Tawara, Y AF Mori, Hideyuki Maeda, Yoshitomo Ueda, Yoshihiro Nakazawa, Kazuhiro Tawara, Yuzuru TI Suzaku and Chandra observations of CIZA J1700.8-3144, a cluster of galaxies in the Zone of Avoidance SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE X-rays; galaxies; clusters-X-rays; individual (1RXS J170047.8-314442, CIZA J1700.8-3144) ID RAY-IMAGING SPECTROMETER; BOARD SUZAKU; GALACTIC BULGE; SKY SURVEY; ABUNDANCES; EMISSION; DETECTOR AB We present the Chandra and Suzaku observations of 1RXS J170047.8-314442, located towards the Galactic bulge, to reveal a wide-band (0.3-10 keV) X-ray morphology and spectrum of this source. With the Chandra observation, no point source was found at the position of 1RXSJ170047.8-314442. Instead, we revealed the presence of diffuse X-ray emission, via the wide-band X-ray image obtained from the Suzaku XIS. Although the X-ray emission had a nearly circular shape with a spatial extent of similar to 3'.5, the surface brightness profile was not axisymmetric; a bright spot-like emission was found at similar to 1' away in the northwestern direction from the center. The radial profile of the surface brightness, except for this spot-like emission, was reproduced with a single beta-model; beta and the core radius were found to be 1.02 and 1'.51, respectively. The X-ray spectrum of the diffuse emission showed an emission line at similar to 6 keV, indicating an origin of a thermal plasma. The spectrum was well explained with an absorbed, optically-thin thermal plasma model with a temperature of 6.2 keV and a redshift parameter of z = 0.1 +/- 0.01. Hence, the X-ray emission was considered to arise from the hot gas associated with a cluster of galaxies. Our spectroscopic result confirmed the optical identification of 1RXSJ170047.8-314442 by Kocevski et al. (2007, ApJ, 662, 224): CIZA J1700.8-3144, a member of the cluster catalogue in the Zone of Avoidance. The estimated bolometric X-ray luminosity of 5.9 x 10(44) erg s(-1) was among the lowest with this temperature, suggesting that this cluster is far from relaxed. C1 [Mori, Hideyuki] NASA, CRESST, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mori, Hideyuki] NASA, Xray Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mori, Hideyuki] Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA. [Maeda, Yoshitomo] Japan Aerosp Explorat Agcy JAXA, ISAS, Dept Space Astron & Astrophys, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan. [Ueda, Yoshihiro] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto, Kyoto 6068502, Japan. [Nakazawa, Kazuhiro] Univ Tokyo, Sch Sci, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. [Tawara, Yuzuru] Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648602, Japan. RP Mori, H (reprint author), NASA, CRESST, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Mori, H (reprint author), NASA, Xray Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Mori, H (reprint author), Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA. EM hideyuki.mori@nasa.gov FU Japan Society for the Promotion of Science [26220703] FX First of all, we are deeply grateful to Dr. Harald Ebeling for careful and fruitful comments to improve our manuscript. We would like to thank all the Suzaku team members for their support of the observation and useful information on the XIS and HXD analyses. The scientific results reported in this paper are also based on the observation made by the Chandra X-ray Observatory. This work was supported by Grant-in-Aid for Scientific Research (S) from the Japan Society for the Promotion of Science (Grant Number 26220703). NR 26 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD FEB PY 2017 VL 69 IS 1 AR 3 DI 10.1093/pasj/psw106 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EP0CD UT WOS:000397053500004 ER PT J AU Wada, Q Tsujimoto, M Ebisawa, K Hayashi, T AF Wada, Qazuya Tsujimoto, Masahiro Ebisawa, Ken Hayashi, Takayuki TI A systematic X-ray study of the dwarf novae observed with Suzaku SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE binaries: close; novae, cataclysmic variables; stars: dwarf novae; X-rays: stars ID NONMAGNETIC CATACLYSMIC VARIABLES; URSAE MAJORIS STARS; SS-CYGNI; U-GEMINORUM; ACCRETION DISKS; BOARD SUZAKU; WALRAVEN PHOTOMETRY; EUVE OBSERVATIONS; Z-CAMELOPARDALIS; V893 SCORPII AB X-ray behavior of the dwarf novae (DNe) outside the quiescent state has not been fully understood. We thus assembled 21 data sets of the 15 DNe observed by the Suzaku satellite by the end of 2013, which include spectra taken during not only the quiescence, but also the transitional, outburst, and super-outburst states. Starting with the traditional cooling flow model to explain the X-ray emission from the boundary layer, we made several modifications to account for the observed spectra. As a result, we found that the best-fitting spectral model depends strongly on the state of the DNe with only a few exceptions. Spectra in the quiescent state are explained by the cooling flow model plus a Fe fluorescent line emission attenuated by an interstellar extinction. Spectra in the transitional state require an additional partial covering extinction. Spectra in the outburst and super-outburst state require additional low-temperature thin-thermal plasma component(s). Spectra in the super-outburst state further require a high value of minimum temperature for the boundary layer. We present an interpretation on the required modifications to the cooling flow model for each state. C1 [Wada, Qazuya; Tsujimoto, Masahiro; Ebisawa, Ken] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshino, Sagamihara, Kanagawa 2525210, Japan. [Wada, Qazuya; Ebisawa, Ken] Univ Tokyo, Grad Sch Sci, Dept Astron, 7-3-1 Hongo, Tokyo 1130033, Japan. [Hayashi, Takayuki] Natl Aeronaut & Space Adm, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hayashi, Takayuki] Nagoya Univ, Fac Sci, Dept Phys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. RP Wada, Q (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshino, Sagamihara, Kanagawa 2525210, Japan.; Wada, Q (reprint author), Univ Tokyo, Grad Sch Sci, Dept Astron, 7-3-1 Hongo, Tokyo 1130033, Japan. EM wada@astro.isas.jaxa.jp FU MEXT/JSPS KAKENHI [JP14J11810, JP24105007, JP15H03642, JP16K05309, JP15J10520, JP26800113] FX We appreciate the critique by the anonymous referee for improving the manuscript. The authors are financially supported by the MEXT/JSPS KAKENHI Grant Numbers JP14J11810 (Q. W.), JP24105007, JP15H03642, and JP16K05309 (M. T.), JP16K05309 (K. E.), and JP15J10520 and JP26800113 (T. H.). We acknowledge the variable star observations from the AAVSO International Database contributed by observers worldwide. This research made use of data obtained from Data ARchives and Transmission System (DARTS), provided by the Center for Science-satellite Operation and Data Archives (C- SODA) at ISAS/JAXA, and the software tools provided by HEASARC at NASA/GSFC. NR 68 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD FEB PY 2017 VL 69 IS 1 AR 10 DI 10.1093/pasj/psw114 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EP0CD UT WOS:000397053500011 ER PT J AU McDonald, MS Gallimore, AD Goebel, DM AF McDonald, M. S. Gallimore, A. D. Goebel, D. M. TI Note: Improved heater design for high-temperature hollow cathodes SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article AB We present an improved heater design for thermionic cathodes using a rhenium filament encased in a boron nitride ceramic sleeve. This heater is relatively simple to fabricate, yet has been successfully used to reliably and repeatably light a lanthanum hexaboride (LaB6) hollow cathode based on a previously published design without noticeable filament degradation over hundreds of hours of operation. The high decomposition temperature of boron nitride (2800 C for inert environments) and melting point for rhenium (3180 C) make this heater especially attractive for use with LaB6, which may require operating temperatures upwards of 1700 C. While boron nitride decomposes in air above 1000 C, the heater was used only at vacuum with an inert gas discharge, and no degradation was observed. Limitations of current state of the art cathode heaters are also discussed and compared with the rhenium-boron nitride combination. C1 [McDonald, M. S.] Naval Res Lab, Spacecraft Engn Dept, Washington, DC 20375 USA. [Gallimore, A. D.] Univ Michigan, Ann Arbor, MI 48109 USA. [Goebel, D. M.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP McDonald, MS (reprint author), Naval Res Lab, Spacecraft Engn Dept, Washington, DC 20375 USA. EM michael.mcdonald@nrl.navy.mil NR 4 TC 0 Z9 0 U1 2 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0034-6748 EI 1089-7623 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD FEB PY 2017 VL 88 IS 2 AR 026104 DI 10.1063/1.4976728 PG 3 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA EN3IR UT WOS:000395902700072 PM 28249464 ER PT J AU Day, JMD Moynier, F Meshik, AP Pradivtseva, OV Petit, DR AF Day, James M. D. Moynier, Frederic Meshik, Alex P. Pradivtseva, Olga V. Petit, Donald R. TI Evaporative fractionation of zinc during the first nuclear detonation SO SCIENCE ADVANCES LA English DT Article ID ISOTOPIC EVIDENCE; WATER; MOON; ORIGIN; MANTLE; EARTH; DIFFERENTIATION; ABUNDANCES; RESERVOIRS; POTASSIUM AB Volatile element and compound abundances vary widely in planets and were set during the earliest stages of solar system evolution. Experiments or natural analogs approximating these early conditions are limited. Using silicate glass formed from arkosic sands during the first nuclear detonation at the Trinity test site, New Mexico, we show that the isotopes of zinc were fractionated during evaporation. The green silicate glasses, termed "trinitite," show + 0.5 +/- 0.1 parts per thousand/atomic mass unit isotopic fractionation from similar to 200 m to within 10 m of ground zero of the detonation, corresponding to an a fractionation factor between 0.999 and 0.9995. These results confirm that Zn isotopic fractionation occurs through evaporation processes at high temperatures. Evidence for similar fractionations in lunar samples consequently implies a volatile-depleted bulk Moon, with evaporation occurring during a giant impact or in a magma ocean. C1 [Day, James M. D.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Day, James M. D.; Moynier, Frederic] Univ Paris Diderot, Inst Phys Globe Paris, Sorbonne Paris Cite, 1 Rue Jussieu, F-75005 Paris, France. [Meshik, Alex P.; Pradivtseva, Olga V.] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. [Petit, Donald R.] Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Day, JMD (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.; Day, JMD (reprint author), Univ Paris Diderot, Inst Phys Globe Paris, Sorbonne Paris Cite, 1 Rue Jussieu, F-75005 Paris, France. EM jmdday@ucsd.edu FU NASA Emerging Worlds program [NNX15AL74G] FX This work was supported by the NASA Emerging Worlds program (NNX15AL74G) and a visiting professor position in the Institut de Physique du Globe de Paris to J.M.D.D. NR 39 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 2375-2548 J9 SCI ADV JI Sci. Adv. PD FEB PY 2017 VL 3 IS 2 AR e1602668 DI 10.1126/sciadv.1602668 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EO9WT UT WOS:000397039500013 PM 28246647 ER PT J AU Lapen, TJ Righter, M Andreasen, R Irving, AJ Satkoski, AM Beard, BL Nishiizumi, K Jull, AJT Caffee, MW AF Lapen, Thomas J. Righter, Minako Andreasen, Rasmus Irving, Anthony J. Satkoski, Aaron M. Beard, Brian L. Nishiizumi, Kunihiko Jull, A. J. Timothy Caffee, Marc W. TI Two billion years of magmatism recorded from a single Mars meteorite ejection site SO SCIENCE ADVANCES LA English DT Article ID ND ISOTOPIC SYSTEMATICS; MARTIAN METEORITES; RB-SR; SM-ND; DIFFERENTIATION HISTORY; LU-HF; BULK COMPOSITION; SNC METEORITES; AGE; SHERGOTTITES AB The timing and nature of igneous activity recorded at a single Mars ejection site can be determined from the isotope analyses of Martian meteorites. Northwest Africa (NWA) 7635 has an Sm-Nd crystallization age of 2.403 +/- 0.140 billion years, and isotope data indicate that it is derived from an incompatible trace element-depleted mantle source similar to that which produced a geochemically distinct group of 327-to 574-million-year-old "depleted" shergottites. Cosmogenic nuclide data demonstrate that NWA 7635 was ejected from Mars 1.1 million years ago (Ma), as were at least 10 other depleted shergottites. The shared ejection age is consistent with a common ejection site for these meteorites. The spatial association of 327-to 2403-Ma depleted shergottites indicates >2 billion years of magmatism from a long-lived and geochemically distinct volcanic center near the ejection site. C1 [Lapen, Thomas J.; Righter, Minako; Andreasen, Rasmus] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA. [Andreasen, Rasmus] Aarhus Univ, Dept Geosci, Aarhus, Denmark. [Irving, Anthony J.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. [Satkoski, Aaron M.; Beard, Brian L.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Satkoski, Aaron M.; Beard, Brian L.] Univ Wisconsin, NASA Astrobiol Inst, Madison, WI 53706 USA. [Nishiizumi, Kunihiko] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Jull, A. J. Timothy] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. [Caffee, Marc W.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Caffee, Marc W.] Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA. RP Lapen, TJ (reprint author), Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA. EM tjlapen@uh.edu OI Jull, A J Timothy/0000-0002-4079-4947 FU NASA Mars Fundamental Research [NNX11AF52G]; NASA Cosmochemistry [NNX12AX96G, NNX09AC06G, NNX14AK62G]; NASA Astrobiology [NNA13AA94A] FX This work was supported by NASA Mars Fundamental Research (NNX11AF52G to T.J.L.), NASA Cosmochemistry (NNX12AX96G and NNX09AC06G to T.J.L. and NNX14AK62G to K.N.), and NASA Astrobiology (NNA13AA94A to B.L.B.). NR 77 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 2375-2548 J9 SCI ADV JI Sci. Adv. PD FEB PY 2017 VL 3 IS 2 AR e1600922 DI 10.1126/sciadv.1600922 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EO9WT UT WOS:000397039500003 ER PT J AU Knipp, DJ Pette, DV Kilcommons, LM Isaacs, TL Cruz, AA Mlynczak, MG Hunt, LA Lin, CY AF Knipp, D. J. Pette, D. V. Kilcommons, L. M. Isaacs, T. L. Cruz, A. A. Mlynczak, M. G. Hunt, L. A. Lin, C. Y. TI Thermospheric nitric oxide response to shock-led storms SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID CORONAL MASS EJECTIONS; PLANAR MAGNETIC-STRUCTURES; SOLAR-WIND; TERRESTRIAL THERMOSPHERE; MAGNETOSPHERIC STORMS; SABER EXPERIMENT; LOW-LATITUDE; DENSITY; GEOEFFECTIVENESS; PERTURBATIONS AB We present a multiyear superposed epoch study of the Sounding of the Atmosphere using Broadband Emission Radiometry nitric oxide (NO) emission data. NO is a trace constituent in the thermosphere that acts as cooling agent via infrared (IR) emissions. The NO cooling competes with storm time thermospheric heating, resulting in a thermostat effect. Our study of nearly 200 events reveals that shock-led interplanetary coronal mass ejections (ICMEs) are prone to early and excessive thermospheric NO production and IR emissions. Excess NO emissions can arrest thermospheric expansion by cooling the thermosphere during intense storms. The strongest events curtail the interval of neutral density increase and produce a phenomenon known as thermospheric "overcooling." We use Defense Meteorological Satellite Program particle precipitation data to show that interplanetary shocks and their ICME drivers can more than double the fluxes of precipitating particles that are known to trigger the production of thermospheric NO. Coincident increases in Joule heating likely amplify the effect. In turn, NO emissions are more than double. We discuss the roles and features of shock/sheath structures that allow the thermosphere to temper the effects of extreme storm time energy input and explore the implication these structures may have on mesospheric NO. Shock-driven thermospheric NO IR cooling likely plays an important role in satellite drag forecasting challenges during extreme events. C1 [Knipp, D. J.; Pette, D. V.; Kilcommons, L. M.; Isaacs, T. L.; Cruz, A. A.] Univ Colorado Boulder, Aerospace Engn Sci, Boulder, CO 80309 USA. [Knipp, D. J.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Mlynczak, M. G.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23665 USA. [Hunt, L. A.] Sci Syst & Applicat Inc, Hampton, VA USA. [Lin, C. Y.] Univ Texas Arlington, Dept Phys, POB 19059, Arlington, TX 76019 USA. RP Knipp, DJ (reprint author), Univ Colorado Boulder, Aerospace Engn Sci, Boulder, CO 80309 USA.; Knipp, DJ (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. EM dknipp@agu.org OI Hunt, Linda/0000-0002-5330-541X FU NASA [NNX16AH94G, NNX13AG07G]; AFOSR award [FA9550-16-1-0364]; NSF [DES-1446704]; Queensborough Community College of New York; University of Colorado Engineering Excellence Fund for Summer Program for Undergraduate Research; NASA Heliophysics Guest Investigator Open Data Development Element project; NASA Science Innovation Fund project FX D.J.K. was partially supported by NASA grant NNX16AH94G and AFOSR award FA9550-16-1-0364. L.M.K. was supported by NASA grant NNX13AG07G. A. C. was partially supported by NSF grant DES-1446704 via a contract with Queensborough Community College of New York. T.I. was supported by the University of Colorado Engineering Excellence Fund for Summer Program for Undergraduate Research. M.M. and L.H. were supported by NASA Heliophysics Guest Investigator Open Data Development Element project. M. G.M. also acknowledges support from a NASA Science Innovation Fund project. D.J.K. was provided travel support by the NASA Living with a Star Satellite Drag Institute. We thank Alan Burns for the enlightening discussions. DMSP data are available from http://cdaweb.sci.gsfc.nasa.gov/index.html/, then selecting DMSP. The DREAMS Wind ICME list (http://space.ustc.edu.cn/dreams/wind_icmes/) is generated and maintained by the Solar and TErrestrial Physics group of the University of Science and Technology of China. The GRACE density measurements are available online at http://sisko.colorado.edu/sutton/data.html. The SABER measurements can be obtained from author M. G. M. (e-mail: m.g.mlynczak@nasa.gov). Those interested in the storm lists for the various figures can contact D. J. K. (delores.knipp@colorado.edu). NR 92 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD FEB PY 2017 VL 15 IS 2 BP 325 EP 342 DI 10.1002/2016SW001567 PG 18 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA EO9GN UT WOS:000396997300007 ER PT J AU Anderson, BJ Korth, H Welling, DT Merkin, VG Wiltberger, MJ Raeder, J Barnes, RJ Waters, CL Pulkkinen, AA Rastaetter, L AF Anderson, Brian J. Korth, Haje Welling, Daniel T. Merkin, Viacheslav G. Wiltberger, Michael J. Raeder, Joachim Barnes, Robin J. Waters, Colin L. Pulkkinen, Antti A. Rastaetter, Lutz TI Comparison of predictive estimates of high-latitude electrodynamics with observations of global-scale Birkeland currents SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID IONOSPHERE-THERMOSPHERE MODEL; FIELD-ALIGNED CURRENTS; PARTICLE ENERGY FLUX; MAGNETOMETER DATA; MHD SIMULATIONS; MAGNETIC-FIELD; MAGNETOSPHERE; OUTFLOW; CONDUCTANCE; EVENT AB Two of the geomagnetic storms for the Space Weather Prediction Center Geospace Environment Modeling challenge occurred after data were first acquired by the Active Magnetosphere and Planetary Electrodynamics Response Experiment (AMPERE). We compare Birkeland currents from AMPERE with predictions from four models for the 4-5 April 2010 and 5-6 August 2011 storms. The four models are the Weimer (2005b) field-aligned current statistical model, the Lyon-Fedder-Mobarry magnetohydrodynamic (MHD) simulation, the Open Global Geospace Circulation Model MHD simulation, and the Space Weather Modeling Framework MHD simulation. The MHD simulations were run as described in Pulkkinen et al. (2013) and the results obtained from the Community Coordinated Modeling Center. The total radial Birkeland current, J(Total), and the distribution of radial current density, J(r), for all models are compared with AMPERE results. While the total currents are well correlated, the quantitative agreement varies considerably. The J(r) distributions reveal discrepancies between the models and observations related to the latitude distribution, morphologies, and lack of nightside current systems in the models. The results motivate enhancing the simulations first by increasing the simulation resolution and then by examining the relative merits of implementing more sophisticated ionospheric conductance models, including ionospheric outflows or other omitted physical processes. Some aspects of the system, including substorm timing and location, may remain challenging to simulate, implying a continuing need for real-time specification. C1 [Anderson, Brian J.; Korth, Haje; Merkin, Viacheslav G.; Barnes, Robin J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 21218 USA. [Welling, Daniel T.] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA. [Wiltberger, Michael J.] Univ Colorado, Univ Ctr Atmospher Res, Boulder, CO 80309 USA. [Raeder, Joachim] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Raeder, Joachim] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Waters, Colin L.] Univ Newcastle, Dept Math & Phys Sci, Newcastle, NSW, Australia. [Pulkkinen, Antti A.; Rastaetter, Lutz] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Anderson, BJ (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 21218 USA. EM brian.anderson@jhuapl.edu OI Welling, Daniel/0000-0002-0590-1022 FU NSF [ATM-0739864, AGS-1420184] FX Support for AMPERE has been provided under NSF sponsorship under grants ATM-0739864 and AGS-1420184. B.J.A. thanks Daniel R. Weimer for helpful discussions guiding the use, evaluation, and comparison of the W05 results with AMPERE products. B.J.A. also thanks A. Pulkkinen for effective leadership of the LWS-GIC Institute efforts. All AMPERE data are available via http://ampere.jhuapl.edu. Simulation output in digital form are available via http://ccmc.gsfc.nasa.gov/challenges/dBdt/. The W05 code is available from Daniel J. Weimer (dweimer@vt.edu). Provisional auroral current data are available from the World Data Center for Geomagnetism at Kyoto University (http://wdc.kugi.kyotou.ac.jp/aedir/index.html). NR 83 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD FEB PY 2017 VL 15 IS 2 BP 352 EP 373 DI 10.1002/2016SW001529 PG 22 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA EO9GN UT WOS:000396997300009 ER PT J AU Kim, MHY Blattnig, SR Clowdsley, MC Norman, RB AF Kim, Myung-Hee Y. Blattnig, Steve R. Clowdsley, Martha C. Norman, Ryan B. TI Using spectral shape and predictor fluence to evaluate temporal dependence of exposures from solar particle events SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID GALACTIC COSMIC-RAYS; EXPLORATION MISSIONS; SPACE EXPLORATION; DEEP SPACE; RADIATION; MODEL; RISK; UNCERTAINTIES; ASTRONAUTS; FREQUENCY AB Real-time estimation of exposure levels has been considered in NASA's operational strategies and structural capability for the protection of astronauts from exposure to large solar particle events (SPEs). The temporal profile of organ dose rates is also important for the analysis of dose-rate-dependent biological responses and the optimization of radiation shielding and future mission planning. A realistic temporal estimation of exposure profiles relies on (1) the complete energy spectrum of SPE that defines the boundary condition for radiation transport simulation, (2) the radiation transport simulation with detailed shielding and body geometry models that determines particle transmission at each critical body organ, and (3) the assessment of organ dosimetric quantities and biological risks by applying the corresponding response models. This paper introduces a process of rapidly estimating temporal exposures to SPEs by implementing the distributions of the organ doses and the spectral-shape characterization of the major SPEs. Simultaneously, the unconditional probability exceeding the NASA 30 day limit of a blood-forming organ dose is estimated by taking into account the variability of detailed spectra of SPEs for a given predictor fluence. These temporal evaluations of SPEs can be applied to the development of real-time guidance and protection system on improving mitigation of adverse effects during space missions. C1 [Kim, Myung-Hee Y.] KBRwyle, Houston, TX 77058 USA. [Blattnig, Steve R.; Clowdsley, Martha C.; Norman, Ryan B.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Kim, MHY (reprint author), KBRwyle, Houston, TX 77058 USA. EM myung-hee.y.kim@nasa.gov FU NASA [NNJ15HK11B] FX The authors acknowledge the support from the NASA risk assessment project NNJ15HK11B under the Human Research Program. The authors wish to thank Michael A. Xapsos at NASA Goddard Space Flight Center for the IMP 8 GME data. All data products are possible through the IMP 8 GME home page http://spdf.sci.gsfc.nasa.gov/pub/data/imp/imp8/documents/archived_websi te/gme/GME_home.html. NR 73 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD FEB PY 2017 VL 15 IS 2 BP 374 EP 391 DI 10.1002/2016SW001552 PG 18 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA EO9GN UT WOS:000396997300010 ER PT J AU Bilitza, D Altadill, D Truhlik, V Shubin, V Galkin, I Reinisch, B Huang, X AF Bilitza, D. Altadill, D. Truhlik, V. Shubin, V. Galkin, I. Reinisch, B. Huang, X. TI International Reference Ionosphere 2016: From ionospheric climate to real-time weather predictions SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID F2 PEAK HEIGHT; GLOBAL-MODEL; MERIDIONAL WINDS; IRI MODEL; VALUES; MAXIMUM; HMF2; FOF2; TEC AB The paper presents the latest version of the International Reference Ionosphere model (IRI-2016) describing the most important changes and improvements that were included with this version and discussing their impact on the IRI predictions of ionospheric parameters. IRI-2016 includes two new model options for the F-2 peak height h(m)F(2) and a better representation of topside ion densities at very low and high solar activities. In addition, a number of smaller changes were made concerning the use of solar indices and the speedup of the computer program. We also review the latest developments toward a Real-Time IRI. The goal is to progress from predicting climatology to describing the real-time weather conditions in the ionosphere. C1 [Bilitza, D.] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA. [Bilitza, D.] NASA, Heliospher Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Altadill, D.] Univ Ramon Llull, CSIC, OE, Roquetes, Spain. [Truhlik, V.] CAS, Dept Upper Atmosphere, Inst Atmospher Phys, Prague, Czech Republic. [Shubin, V.] Russian Acad Sci, Pushkov Inst Terr Magnetism Ionosphere & Radiowav, Moscow, Russia. [Galkin, I.; Reinisch, B.] Univ Massachusetts, Space Sci Lab, Lowell, MA USA. [Reinisch, B.; Huang, X.] Lowell Digisonde Int LLC, Lowell, MA USA. RP Bilitza, D (reprint author), George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA.; Bilitza, D (reprint author), NASA, Heliospher Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM dbilitza@gmu.edu FU USAF [FA9453-14-C-0305, FA865016C9104]; Universitat Ramon Llull project - "Obra Social la Caixa" [2016-URL-Trac-001]; Spanish Ministry MINECO through project [CTM2014-52182-C3-1-P]; Grant Agency of the Czech Republic [15-07281J]; Russian Foundation for Basic Research through project [17-05-00427] FX We like to acknowledge the IRI Working Group with all its members for their support of the IRI activities. We like to dedicate this paper to our coauthor Xueqin Huang who passed away on 15 October 2016. Xueqin was a member of the IRI Working Group and contributed key IRI improvements. We thank NASA's Space Physics Data Facility (SPDF) and Community Coordinated Modeling Center (CCMC) for the IRIweb online computation service. B.R., X.H., I.G., and D.B. were in part supported by USAF contracts FA9453-14-C-0305 and FA865016C9104. D.A. is in part supported by Universitat Ramon Llull project 2016-URL-Trac-001 funded by "Obra Social la Caixa" and by Spanish Ministry MINECO through project CTM2014-52182-C3-1-P. V.T. was supported, in part, by grant 15-07281J of the Grant Agency of the Czech Republic. V.S. was supported by the Russian Foundation for Basic Research through project 17-05-00427. The IRI model code in Fortran is available from the IRI homepage at irimodel.org NR 54 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD FEB PY 2017 VL 15 IS 2 BP 418 EP 429 DI 10.1002/2016SW001593 PG 12 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA EO9GN UT WOS:000396997300013 ER PT J AU Savani, NP Vourlidas, A Richardson, IG Szabo, A Thompson, BJ Pulkkinen, A Mays, ML Nieves-Chinchilla, T Bothmer, V AF Savani, N. P. Vourlidas, A. Richardson, I. G. Szabo, A. Thompson, B. J. Pulkkinen, A. Mays, M. L. Nieves-Chinchilla, T. Bothmer, V. TI Predicting the magnetic vectors within coronal mass ejections arriving at Earth: 2. Geomagnetic response SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID SOLAR-WIND; FLUX ROPE; 1 AU; COMPLEX EJECTA; WSA-ENLIL; CLOUDS; FIELD; CME; EVOLUTION; MODEL AB This is a companion to Savani et al. (2015) that discussed how a first-order prediction of the internal magnetic field of a coronal mass ejection (CME) may be made from observations of its initial state at the Sun for space weather forecasting purposes (Bothmer-Schwenn scheme (BSS) model). For eight CME events, we investigate how uncertainties in their predicted magnetic structure influence predictions of the geomagnetic activity. We use an empirical relationship between the solar wind plasma drivers and Kp index together with the inferred magnetic vectors, to make a prediction of the time variation of Kp (Kp((BSS))). We find a 2 sigma uncertainty range on the magnetic field magnitude (|B|) provides a practical and convenient solution for predicting the uncertainty in geomagnetic storm strength. We also find the estimated CME velocity is a major source of error in the predicted maximum Kp. The time variation of Kp(BSS) is important for predicting periods of enhanced and maximum geomagnetic activity, driven by southerly directed magnetic fields, and periods of lower activity driven by northerly directed magnetic field. We compare the skill score of our model to a number of other forecasting models, including the NOAA/Space Weather Prediction Center (SWPC) and Community Coordinated Modeling Center (CCMC)/SWRC estimates. The BSS model was the most unbiased prediction model, while the other models predominately tended to significantly overforecast. The True skill score of the BSS prediction model (TSS = 0.43 +/- 0.06) exceeds the results of two baseline models and the NOAA/SWPC forecast. The BSS model prediction performed equally with CCMC/SWRC predictions while demonstrating a lower uncertainty. C1 [Savani, N. P.] Univ Maryland, Goddard Planetary Heliophys Inst, Baltimore, MD 21201 USA. [Savani, N. P.; Richardson, I. G.; Szabo, A.; Thompson, B. J.; Pulkkinen, A.; Mays, M. L.; Nieves-Chinchilla, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Vourlidas, A.] Johns Hopkins Univ, Appl Phys Lab, Solar Sect, Laurel, MD USA. [Richardson, I. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mays, M. L.; Nieves-Chinchilla, T.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DE USA. [Bothmer, V.] Georg August Univ Gottingen, Inst Astrophys, Gottingen, Germany. RP Savani, NP (reprint author), Univ Maryland, Goddard Planetary Heliophys Inst, Baltimore, MD 21201 USA.; Savani, NP (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM neel.savani@umbc.edu RI Vourlidas, Angelos/C-8231-2009 OI Vourlidas, Angelos/0000-0002-8164-5948 FU NASA/LWS; Predictive Sciences Inc (San Diego, CA); University of Alcala (Alcala de Henares, Spain); Ministerio de Ciencia e Innovacin Spain [AYA2010-12439-E]; NASA SECCHI; NSF SHINE award [1433202, 1433086]; NASA grant [NNH14AX40I]; NASA LWS Institute FX This work benefited from the NASA/LWS Coordinated Data Analysis Workshops on CME flux ropes in 2011. We acknowledge the workshop support provided by NASA/LWS, Predictive Sciences Inc. (San Diego, CA), University of Alcala (Alcala de Henares, Spain), and Ministerio de Ciencia e Innovacin (Reference AYA2010-12439-E), Spain. N.P.S. and A.V. were supported by NASA SECCHI Contract to NRL. N.P.S and T.N.C. were supported by NSF SHINE award 1433202 and 1433086, respectively. The authors wish to acknowledge Lutz Rastaetter and the rest of the CCMC staff for their generous support throughout the work discussed in the paper. This work was supported by NASA grant NNH14AX40I. N.P.S. was also supported by NASA LWS Institute 2015 for geomagnetically induced currents and the SCOSTEP Varsiti program. We thank S. Patsourakos (University of Ioannina) for constructive comments about active region helicity. We thank C. Balch (NOAA/SWPC) for providing historical NOAA forecast alerts. K.D. Leka (NorthWest Research Associates) for her advise and expertise with Skill score metrics. And, last but not the least, W. Thompson (Adnet Systems Inc.) for assistance with SECCHI products within SolarSoft. We thank the Space Physics Data Facility of NASA's Goddard Space Flight Center for use of OMNIWeb service and OMNI data NR 79 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD FEB PY 2017 VL 15 IS 2 BP 441 EP 461 DI 10.1002/2016SW001458 PG 21 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA EO9GN UT WOS:000396997300015 ER PT J AU Williams, CN Cornford, SL Jordan, TM Dowdeswell, JA Siegert, MJ Clark, CD Swift, DA Sole, A Fenty, I Bamber, JL AF Williams, Christopher N. Cornford, Stephen L. Jordan, Thomas M. Dowdeswell, Julian A. Siegert, Martin J. Clark, Christopher D. Swift, Darrel A. Sole, Andrew Fenty, Ian Bamber, Jonathan L. TI Generating synthetic fjord bathymetry for coastal Greenland SO CRYOSPHERE LA English DT Article ID ICE-SHEET MODEL; OVERDEEPENINGS BENEATH; WEST GREENLAND; DATA SET; GLACIER; TOPOGRAPHY; SHELF; MORPHOLOGY; THICKNESS; INTERPOLATION AB Bed topography is a critical boundary for the numerical modelling of ice sheets and ice-ocean interactions. A persistent issue with existing topography products for the bed of the Greenland Ice Sheet and surrounding sea floor is the poor representation of coastal bathymetry, especially in regions of floating ice and near the grounding line. Sparse data coverage, and the resultant coarse resolution at the ice-ocean boundary, poses issues in our ability to model ice flow advance and retreat from the present position. In addition, as fjord bathymetry is known to exert strong control on ocean circulation and ice-ocean forcing, the lack of bed data leads to an inability to model these processes adequately. Since the release of the last complete Greenland bed topography-bathymetry product, new observational bathymetry data have become available. These data can be used to constrain bathymetry, but many fjords remain completely unsampled and therefore poorly resolved. Here, as part of the development of the next generation of Greenland bed topography products, we present a new method for constraining the bathymetry of fjord systems in regions where data coverage is sparse. For these cases, we generate synthetic fjord geometries using a method conditioned by surveys of terrestrial glacial valleys as well as existing sinuous feature interpolation schemes. Our approach enables the capture of the general bathymetry profile of a fjord in north-west Greenland close to Cape York, when compared to observational data. We validate our synthetic approach by demonstrating reduced overestimation of depths compared to past attempts to constrain fjord bathymetry. We also present an analysis of the spectral characteristics of fjord centrelines using recently acquired bathymetric observations, demonstrating how a stochastic model of fjord bathymetry could be parameterised and used to create different realisations. C1 [Williams, Christopher N.; Cornford, Stephen L.; Jordan, Thomas M.; Bamber, Jonathan L.] Univ Bristol, Sch Geog Sci, Bristol Glaciol Ctr, Bristol, Avon, England. [Dowdeswell, Julian A.] Univ Cambridge, Scott Polar Res Inst, Cambridge, England. [Siegert, Martin J.] Imperial Coll London, Grantham Inst, London, England. [Siegert, Martin J.] Imperial Coll London, Dept Earth Sci & Engn, London, England. [Clark, Christopher D.; Swift, Darrel A.; Sole, Andrew] Univ Sheffield, Dept Geog, Sheffield, S Yorkshire, England. [Fenty, Ian] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Williams, CN (reprint author), Univ Bristol, Sch Geog Sci, Bristol Glaciol Ctr, Bristol, Avon, England. EM chris.neil.wills@gmail.com RI Siegert, Martin/A-3826-2008; OI Siegert, Martin/0000-0002-0090-4806; clark, chris/0000-0002-1021-6679; Cornford, Stephen/0000-0003-1844-274X FU UK NERC [NE/M000869/1] FX This study was supported by UK NERC grant NE/M000869/1. NR 53 TC 0 Z9 0 U1 0 U2 0 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1994-0416 EI 1994-0424 J9 CRYOSPHERE JI Cryosphere PD FEB 1 PY 2017 VL 11 IS 1 BP 363 EP 380 DI 10.5194/tc-11-363-2017 PG 18 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA EM1OO UT WOS:000395087100003 ER PT J AU Rim, T Kim, K Cho, H Jeong, W Yoon, JS Kim, Y Meyyappan, M Baek, CK AF Rim, Taiuk Kim, Kihyun Cho, Hyeonsu Jeong, Wooju Yoon, Jun-Sik Kim, Yumi Meyyappan, M. Baek, Chang-Ki TI Electrical Characteristics of Doped Silicon Nanowire Channel Field-Effect Transistor Biosensors SO IEEE SENSORS JOURNAL LA English DT Article DE Biosensors; dopamine; field-effect transistor sensors; low-frequency noise; nanowires; resolution; silicon ID DOPAMINE; ELECTRODE; SENSORS; CELLS AB Optimization of operation conditions for biosensing is investigated for the doped silicon nanowire channel transistor sensors. Sensors with phosphorus doped honeycomb nanowire channel are fabricated on 8-in wafer using the conventional CMOS technology. From the low frequency noise characteristics, the noise equivalent gate voltage fluctuation is obtained to evaluate the sensor resolution and optimize the operation condition. The sensor exhibits maximum resolution at the flat band voltage condition. Detection of a neurotransmitter, dopamine, is demonstrated using the fabricated devices, showing a detection limit of 1 fM and a sensitivity of 2.3 mV/log[dopamine] with a resolution of similar to 60 levels/log[dopamine]. C1 [Rim, Taiuk; Kim, Kihyun; Cho, Hyeonsu; Yoon, Jun-Sik; Kim, Yumi] Pohang Univ Sci & Technol, Dept Creat IT Engn, Future IT Innovat Lab, Pohang 37673, South Korea. [Jeong, Wooju] Pohang Univ Sci & Technol, Dept Elect Engn, Pohang 37673, South Korea. [Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Baek, Chang-Ki] Pohang Univ Sci & Technol, Dept Creat IT Engn, Dept Elect Engn, Pohang 37673, South Korea. RP Cho, H (reprint author), Pohang Univ Sci & Technol, Dept Creat IT Engn, Future IT Innovat Lab, Pohang 37673, South Korea. EM hacle@postech.ac.kr; m.meyyappan@nasa.gov; baekck@postech.ac.kr FU Ministry of Science, ICT, and Future Planning, Korea, through the ICT Consilience Creative Program [IITP-R0346-16-1007]; Regional Software Convergence Products Commercialization Project [S0417-16-1004] FX This work was supported in part by the supervised by the Institute for Information and communications Technology Promotion under Grant IITP-R0346-16-1007 and in part by the Regional Software Convergence Products Commercialization Project, supervised by the National IT Industry Promotion Agency under Grant S0417-16-1004. NR 30 TC 0 Z9 0 U1 1 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1530-437X EI 1558-1748 J9 IEEE SENS J JI IEEE Sens. J. PD FEB 1 PY 2017 VL 17 IS 3 BP 667 EP 673 DI 10.1109/JSEN.2016.2625420 PG 7 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Physics, Applied SC Engineering; Instruments & Instrumentation; Physics GA EK5XE UT WOS:000393998700016 ER PT J AU Suhir, E Ghaffarian, R Yi, S AF Suhir, E. Ghaffarian, R. Yi, S. TI Solder material experiencing low temperature inelastic stress and random vibration loading: predicted remaining useful lifetime SO JOURNAL OF MATERIALS SCIENCE-MATERIALS IN ELECTRONICS LA English DT Article ID JOINTS; RELIABILITY; FATIGUE AB Although there exist promising ways to avoid inelastic strains in solder joints of the second level interconnections in IC package designs, it still appears more typical than not that the peripheral joints of a package/PCB assembly experience inelastic strains. This takes place at low temperature conditions, when the deviation from the high fabrication temperature is the largest and the induced thermal stresses are the highest. On the other hand, it is well known that it is the combination of low temperatures and repetitive dynamic loading that accelerate dramatically the propagation of fatigue cracks, whether elastic or inelastic. Accordingly, a modification of the recently suggested Boltzmann-Arrhenius-Zhurkov model is developed for the evaluation of the remaining useful lifetime of the second level solder joint interconnection whose peripheral joints experience inelastic strains. The experimental basis of the approach is the highly focused and highly cost-effective failure-oriented-accelerated-testing (FOAT). The FOAT specimens are subjected in our methodology to the combined action of low temperatures (not to elevated temperatures, as in the classical Arrhenius model) and random vibrations with the given input energy spectrum. The suggested methodology is viewed as a possible, effective and attractive alternative to temperature cycling. As long as inelastic deformations take place, it is assumed that it is these deformations that determine the fatigue lifetime of the solder material, and the state of stress in the elastic mid-portion of the assembly does not have to be accounted for. The roles of the size and stiffness of this mid-portion have to be considered, however, when determining the very existence and establishing the size of the inelastic zones at the peripheral portions of the designs. The general concept is illustrated by a numerical example. Although this example is carried out for a ball-grid-array design, it is applicable to highly popular column-grid-array (CGA) and quad-flat-no-lead (QFN) designs as well. It is noteworthy that it is much easier to avoid inelastic strains in CGA and QFN structures than in the addressed BGA design. The random vibrations are considered in the developed methodology as a white noise of the given (m/s(2))(2)/Hz-the ratio of the acceleration amplitudes squared to the vibration frequency. C1 [Suhir, E.; Yi, S.] 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 55 TC 0 Z9 0 U1 0 U2 0 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 FEB PY 2017 VL 28 IS 4 BP 3585 EP 3597 DI 10.1007/s10854-016-5960-9 PG 13 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Engineering; Materials Science; Physics GA EL1AJ UT WOS:000394352600058 ER PT J AU Munsell, EB Zhang, FQ Sippel, JA Braun, SA Weng, YH AF Munsell, Erin B. Zhang, Fuqing Sippel, Jason A. Braun, Scott A. Weng, Yonghui TI Dynamics and Predictability of the Intensification of Hurricane Edouard (2014) SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID VERTICAL WIND SHEAR; DOPPLER RADAR OBSERVATIONS; INITIAL CONDITION SENSITIVITY; PERMITTING ENSEMBLE ANALYSIS; TROPICAL CYCLONE INTENSITY; RAPID INTENSIFICATION; STORM MOTION; BONNIE 1998; PART II; CONVECTION AB The dynamics and predictability of the intensification of Hurricane Edouard (2014) are explored through a 60-member convection-permitting ensemble initialized with an ensemble Kalman filter that assimilates dropsondes collected during NASA's Hurricane and Severe Storm Sentinel (HS3) investigation. The 126-h forecasts are initialized when Edouard was designated as a tropical depression and include Edouard's near-rapid intensification (RI) from a tropical storm to a strong category-2 hurricane. Although the deterministic forecast was very successful and many members correctly forecasted Edouard's intensification, there was significant spread in the timing of intensification among the members of the ensemble. Utilizing composite groups created according to the near-RI-onset times of the members, it is shown that, for increasing magnitudes of deep-layer shear, RI onset is increasingly delayed; intensification will not occur once a critical shear threshold is exceeded. Although the timing of intensification varies by as much as 48 h, a decrease in shear is observed across the intensifying composite groups similar to 6-12 h prior to RI. This decrease in shear is accompanied by a reduction in vortex tilt, as the precession and subsequent alignment process begins similar to 24-48 h prior to RI. Sensitivity experiments reveal that some of the variation in RI timing can be attributed to differences in initial intensity, as the earliest-developing members have the strongest initial vortices regardless of their environment. Significant sensitivity and limited predictability exists for members with weaker initial vortices and/or that are embedded in less conducive environments, under which the randomness of moist convective processes and minute initial differences distant from the surface center can produce divergent forecasts. C1 [Munsell, Erin B.; Zhang, Fuqing; Weng, Yonghui] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Munsell, Erin B.; Zhang, Fuqing; Weng, Yonghui] Penn State Univ, Ctr Adv Data Assimilat & Predictabil Tech, University Pk, PA 16802 USA. [Sippel, Jason A.] IM Syst Grp, Rockville, MD USA. [Sippel, Jason A.] NOAA, Environm Modeling Ctr, College Pk, MD USA. [Braun, Scott A.] NASA, Lab Mesoscale Atmospher Proc, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Zhang, FQ (reprint author), Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.; Zhang, FQ (reprint author), Penn State Univ, Ctr Adv Data Assimilat & Predictabil Tech, University Pk, PA 16802 USA. EM fzhang@psu.edu FU NASA New Investigator Program [NNX12AJ79G]; Office of Naval Research [N000140910526]; National Science Foundation [AGS-1305798]; NASA's Hurricane Science Research Program (HSRP); Hurricane and Severe Storm Sentinel (HS3) investigation under NASA's Earth Venture Program FX This work is supported by the NASA New Investigator Program (Grant NNX12AJ79G), the Office of Naval Research (Grant N000140910526), the National Science Foundation (Grant AGS-1305798), and NASA's Hurricane Science Research Program (HSRP) and the Hurricane and Severe Storm Sentinel (HS3) investigation under NASA's Earth Venture Program. Computing was performed at the Texas Advanced Computing Center (TACC). NR 47 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 EI 1520-0469 J9 J ATMOS SCI JI J. Atmos. Sci. PD FEB PY 2017 VL 74 IS 2 BP 573 EP 595 DI 10.1175/JAS-D-16-0018.1 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EL0VY UT WOS:000394341100015 ER PT J AU Keprate, A Ratnayake, RMC Sankararaman, S AF Keprate, Arvind Ratnayake, R. M. Chandima Sankararaman, Shankar TI Minimizing hydrocarbon release from offshore piping by performing probabilistic fatigue life assessment SO PROCESS SAFETY AND ENVIRONMENTAL PROTECTION LA English DT Article DE HCR; RFL; VIF; Uncertainty handling; Probabilistic Crack Growth; Offshore piping ID REMAINING USEFUL LIFE; DAMAGE TOLERANCE CONCEPT; WELDED-JOINTS; PREDICTION; HEALTH; UNCERTAINTY; SAFETY; LEVEL AB Topside piping is the major source of hydrocarbon release (HCR) on offshore oil and gas (00G) platforms in the North Sea region. Since 21% of piping failures are caused by vibration induced fatigue (VIF), an accurate remnant fatigue life (RFL) assessment has the potential to minimize the chances of HCR from an operating piping system. BS-7910 gives two possible approaches for performing a RFL assessment: the S-N curve approach and the fracture mechanics (FM) approach. Since there are large number of uncertainties (such as uncertainty due to the crack growth model, future loading, material and geometric properties, etc.) involved in the RFL calculation process, therefore it is vital to consider the aforementioned sources of uncertainty in order to arrive at an accurate RFL estimate. Nevertheless, BS-7910 provides limited guidance on how to handle uncertainty in RFL assessment. The most common way of dealing with the aforementioned uncertainty is to evaluate RFL probabilistically. This manuscript thus explains the procedure of the probabilistic RFL assessment of offshore topside piping, with an emphasis on uncertainty quantification, propagation and management. Uncertainty quantification handles the identification and characterization of the different sources of uncertainty that may influence the future behavior of the piping component and, in turn, the RFL estimate. Thereafter, uncertainty propagation employs the formerly quantified uncertainties and utilizes the aforementioned information to estimate the RFL. Finally, uncertainty management deals with performing sensitivity analysis to find the individual contributors to uncertainty in the estimated RFL. A numerical case study illustrating the deterministic and probabilistic RFL assessment of topside piping is presented. Afterwards, probabilistically predicted RFL is used to demonstrate the calculation of an inspection interval. Finally, the implications of probabilistically estimated RFL on HCR from process piping is discussed. (C) 2016 Institution of Chemical Engineers. Published by Elsevier B.V. All rights reserved. C1 [Keprate, Arvind; Ratnayake, R. M. Chandima] Univ Stavanger, Dept Mech & Struct Engn & Mat Sci, N-4036 Stavanger, Norway. [Sankararaman, Shankar] NASA, Ames Res Ctr, SGT Inc, Moffett Field, CA 94035 USA. RP Keprate, A (reprint author), Univ Stavanger, Dept Mech & Struct Engn & Mat Sci, N-4036 Stavanger, Norway. EM arvind.keprate@uis.no FU Norwegian Ministry of Education FX The authors convey their sincere thanks to the inspection engineers in Aker Solutions MMO, Norway, for the extended support to complete the current study. This work has been carried out as part of a PhD research project, performed at the University of Stavanger. The research is funded by the Norwegian Ministry of Education. NR 59 TC 0 Z9 0 U1 0 U2 0 PU INST CHEMICAL ENGINEERS PI RUGBY PA 165-189 RAILWAY TERRACE, DAVIS BLDG, RUGBY CV21 3HQ, ENGLAND SN 0957-5820 EI 1744-3598 J9 PROCESS SAF ENVIRON JI Process Saf. Environ. Protect. PD FEB PY 2017 VL 106 BP 34 EP 51 DI 10.1016/j.psep.2016.11.019 PG 18 WC Engineering, Environmental; Engineering, Chemical SC Engineering GA EN4HO UT WOS:000395968800004 ER PT J AU Norsk, P AF Norsk, P. TI Spaceflight and the cardiovascular system: surprises, paradoxes and implications for future deep space missions SO ACTA PHYSIOLOGICA LA English DT Meeting Abstract C1 [Norsk, P.] Univ Space Res Assoc, Washington, DC USA. [Norsk, P.] NASA, Washington, DC 20546 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1748-1708 EI 1748-1716 J9 ACTA PHYSIOL JI Acta Physiol. PD FEB PY 2017 VL 219 SU S710 MA K-01 BP 3 EP 3 PG 1 WC Physiology SC Physiology GA EK4SH UT WOS:000393916600002 ER PT J AU Furlan, E Ciardi, DR Everett, ME Saylors, M Teske, JK Horch, EP Howell, SB van Belle, GT Hirsch, LA Gautier, TN Adams, ER Barrado, D Cartier, KMS Dressing, CD Dupree, AK Gilliland, RL Lillo-Box, J Lucas, PW Wang, J AF Furlan, E. Ciardi, D. R. Everett, M. E. Saylors, M. Teske, J. K. Horch, E. P. Howell, S. B. van Belle, G. T. Hirsch, L. A. Gautier, T. N., III Adams, E. R. Barrado, D. Cartier, K. M. S. Dressing, C. D. Dupree, A. K. Gilliland, R. L. Lillo-Box, J. Lucas, P. W. Wang, J. TI THE KEPLER FOLLOW-UP OBSERVATION PROGRAM. I. A CATALOG OF COMPANIONS TO KEPLER STARS FROM HIGH-RESOLUTION IMAGING SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: general; catalogs; planets and satellites: detection; surveys; techniques: high angular resolution; techniques: photometric ID CANDIDATE HOST STARS; LASER ADAPTIVE OPTICS; FALSE-POSITIVE RATE; CIRCLE-PLUS PLANET; SOLAR-TYPE STARS; SUN-LIKE STAR; BINARY STARS; STELLAR MULTIPLICITY; HABITABLE ZONE; TRANSIT CANDIDATES AB We present results from high-resolution, optical to near-IR imaging of host stars of Kepler Objects of Interest (KOIs), identified in the original Kepler field. Part of the data were obtained under the Kepler imaging follow-up observation program over six years (2009-2015). Almost 90% of stars that are hosts to planet candidates or confirmed planets were observed. We combine measurements of companions to KOI host stars from different bands to create a comprehensive catalog of projected separations, position angles, and magnitude differences for all detected companion stars (some of which may not be bound). Our compilation includes 2297 companions around 1903 primary stars. From high-resolution imaging, we find that similar to 10% (similar to 30%) of the observed stars have at least one companion detected within 1 ''(4 ''). The true fraction of systems with close (less than or similar to 4 '') companions is larger than the observed one due to the limited sensitivities of the imaging data. We derive correction factors for planet radii caused by the dilution of the transit depth: assuming that planets orbit the primary stars or the brightest companion stars, the average correction factors are 1.06 and 3.09, respectively. The true effect of transit dilution lies in between these two cases and varies with each system. Applying these factors to planet radii decreases the number of KOI planets with radii smaller than 2 R-circle plus by similar to 2%-23% and thus affects planet occurrence rates. This effect will also be important for the yield of small planets from future transit missions such as TESS. C1 [Furlan, E.; Ciardi, D. R.; Saylors, M.] CALTECH, IPAC, Mail Code 314-6,1200 E Calif Blvd, Pasadena, CA 91125 USA. [Everett, M. E.] Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA. [Saylors, M.] Coll Canyons, 26455 Rockwell Canyon Rd, Santa Clarita, CA 91355 USA. [Teske, J. K.] Carnegie DTM, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. [Horch, E. P.] Southern Connecticut State Univ, Dept Phys, 501 Crescent St, New Haven, CT 06515 USA. [Horch, E. P.; van Belle, G. T.] Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA. [Howell, S. B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hirsch, L. A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Gautier, T. N., III] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Adams, E. R.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Barrado, D.] ESAC, Ctr Astrobiol CSIC INTA, Dept Astrofis, Villanueva De La Canada, Madrid, Spain. [Cartier, K. M. S.; Gilliland, R. L.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Cartier, K. M. S.; Gilliland, R. L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Dressing, C. D.; Wang, J.] CALTECH, Pasadena, CA 91125 USA. [Dupree, A. K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Lillo-Box, J.] ESO, Santiago, Chile. [Lucas, P. W.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. RP Furlan, E (reprint author), CALTECH, IPAC, Mail Code 314-6,1200 E Calif Blvd, Pasadena, CA 91125 USA. EM furlan@ipac.caltech.edu OI Ciardi, David/0000-0002-5741-3047; Furlan, Elise/0000-0001-9800-6248; Barrado, David/0000-0002-5971-9242 FU NASA [NAS 5-26555]; NSF; W.M. Keck Foundation FX We thank the Robo-AO team, in particular, its leaders Christoph Baranec, Nicholas Law, Reed Riddle, and Carl Ziegler for sharing their results on robotic laser adaptive optics imaging of KOI host stars in their publications and on CFOP. We also thank Adam Kraus and his team for sharing their results on the multiplicity of KOI host stars obtained with adaptive optics imaging and non-redundant aperture-mask interferometry in their recent publication. The results from these publications provided substantial input for this work. Support for this work was provided by NASA through awards issued by JPL/Caltech. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with NASA under the Exoplanet Exploration Program. It has also made use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/Caltech, funded by NASA and the NSF. NASA's Astrophysics Data System Bibliographic Services were also used. Some of the data presented in this work were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This work is also based in part on observations at Kitt Peak National Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The WIYN Observatory is a joint facility of the University of Wisconsin-Madison, Indiana University, the National Optical Astronomy Observatory, and the University of Missouri. Part of the observations were also obtained at the Gemini Observatory, which is operated by AURA under a cooperative agreement with the NSF on behalf of the Gemini partnership. Some of the results in this work are based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, operated by AURA, Inc., under NASA contract NAS 5-26555. NR 69 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD FEB PY 2017 VL 153 IS 2 AR 71 DI 10.3847/1538-3881/153/2/71 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EK5LM UT WOS:000393967900006 ER PT J AU Sinukoff, E Howard, AW Petigura, EA Fulton, BJ Isaacson, H Weiss, LM Brewer, JM Hansen, BMS Hirsch, L Christiansen, JL Crepp, JR Crossfield, IJM Schlieder, JE Ciardi, DR Beichman, CA Knutson, HA Benneke, B Dressing, CD Livingston, JH Deck, KM Lepine, S Rogers, LA AF Sinukoff, Evan Howard, Andrew W. Petigura, Erik A. Fulton, Benjamin J. Isaacson, Howard Weiss, Lauren M. Brewer, John M. Hansen, Brad M. S. Hirsch, Lea Christiansen, Jessie L. Crepp, Justin R. Crossfield, Ian J. M. Schlieder, Joshua E. Ciardi, David R. Beichman, Charles A. Knutson, Heather A. Benneke, Bjoern Dressing, Courtney D. Livingston, John H. Deck, Katherine M. Lepine, Sebastien Rogers, Leslie A. TI MASS CONSTRAINTS OF THE WASP-47 PLANETARY SYSTEM FROM RADIAL VELOCITIES SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: detection; planets and satellites: dynamical evolution and stability; planets and satellites: formation; techniques: radial velocities; techniques: spectroscopic ID HOT JUPITERS; GIANT PLANETS; KEPLER; EARTH; STARS; EXOPLANETS; MIGRATION; SEARCH; ORBITS; K2 AB We report precise radial velocity (RV) measurements of WASP-47, a G star that hosts three transiting planets in close proximity (a hot Jupiter, a super-Earth, and a Neptune-sized planet) and a non-transiting planet at 1.4 au. Through a joint analysis of previously published RVs and our own Keck-HIRES RVs, we significantly improve the planet mass and bulk density measurements. For the super-Earth WASP-47e (P = 0.79 days), we measure a mass of 9.11 +/- 1.17 M-circle plus, and a bulk density of 7.63 +/- 1.90 g cm(-3), consistent with a rocky composition. For the hot Jupiter WASP-47b (P = 4.2 days), we measure a mass of 356 +/- 12 M-circle plus (1.12 +/- 0.04 M-Jup) and constrain its eccentricity to < 0.021 at 3 sigma confidence. For the Neptune-size planet WASP-47d (P = 9.0 days), we measure a mass of 12.75 +/- 2.70 M circle plus and a bulk density of 1.36 +/- 0.42 g cm(-3), suggesting that it has a thick H/He envelope. For the outer non-transiting planet, we measure a minimum mass of 411 +/- 18M(circle plus) (1.29 +/- 0.06 M-Jup), an orbital period of 595.7 +/- 5.0. days, and an orbital eccentricity of 0.27 +/- 0.04. Our new measurements are consistent with but two to four times more precise than previous mass measurements. C1 [Sinukoff, Evan; Fulton, Benjamin J.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Howard, Andrew W.] CALTECH, Cahill Ctr Astrophys, 1216 East Calif Blvd, Pasadena, CA 91125 USA. [Petigura, Erik A.; Knutson, Heather A.; Benneke, Bjoern; Dressing, Courtney D.; Deck, Katherine M.] CALTECH, Div Geol & Planetary Sci, 1255 East Calif Blvd, Pasadena, CA 91125 USA. [Isaacson, Howard; Hirsch, Lea] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Weiss, Lauren M.] Univ Montreal, Dept Phys, Inst Rech Exoplanetes, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada. [Brewer, John M.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Brewer, John M.] 260 Whitney Ave, New Haven, CT 06511 USA. [Hansen, Brad M. S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Hansen, Brad M. S.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Christiansen, Jessie L.; Schlieder, Joshua E.; Ciardi, David R.; Beichman, Charles A.] CALTECH, NASA, Exoplanet Sci Inst, 770 S Wilson Ave, Pasadena, CA 91125 USA. [Crepp, Justin R.] Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA. [Crossfield, Ian J. M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA. [Livingston, John H.] Univ Tokyo, Dept Astron, 7-3-1 Bunkyo Ku, Tokyo 1130033, Japan. [Lepine, Sebastien] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Rogers, Leslie A.] Univ Chicago, Dept Astron & Astrophys, 5640 South Ellis Ave, Chicago, IL 60637 USA. RP Sinukoff, E (reprint author), Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. OI Weiss, Lauren/0000-0002-3725-3058; Brewer, John/0000-0002-9873-1471; Ciardi, David/0000-0002-5741-3047; Isaacson, Howard/0000-0002-0531-1073; Fulton, Benjamin/0000-0003-3504-5316 FU NASA Science Mission directorate; Natural Sciences and Engineering Research Council of Canada; NASA through a Hubble Fellowship grant - Space Telescope Science Institute; NASA [NAS 5-26555]; National Science Foundation [2014184874]; K2 team through a NASA Astrophysics Data Analysis Program grant; K2 Guest Observer Program; Trottier Family Foundation; NASA through the Sagan Fellowship Program FX We thank the many observers who contributed to the measurements reported here. We thank Geoff Marcy and Trevor David for helpful discussions. We thank Tom Greene, Michael Werner, Michael Endl, and William Cochrane for participation in our NASA Key Project. We gratefully acknowledge the efforts and dedication of the Keck Observatory staff. This paper includes data collected by the K2 mission. Funding for the K2 mission is provided by the NASA Science Mission directorate. E.S. is supported by a postgraduate scholarship from the Natural Sciences and Engineering Research Council of Canada. E.A.P. acknowledges support by NASA through a Hubble Fellowship grant awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. B.J.F. was supported by the National Science Foundation Graduate Research Fellowship under grant No. 2014184874. A.W.H. acknowledges support for our K2 team through a NASA Astrophysics Data Analysis Program grant. A.W.H. and I.J.M.C. acknowledge support from the K2 Guest Observer Program. L.M.W. acknowledges the Trottier Family Foundation for their generous support. This work was performed [in part] under contract with the Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Finally, the authors extend special thanks to those of Hawai' ian ancestry on whose sacred mountain of Maunakea we are privileged to be guests. Without their generous hospitality, the Keck observations presented herein would not have been possible. NR 61 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 FEB PY 2017 VL 153 IS 2 AR 70 DI 10.3847/1538-3881/153/2/70 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EK5LM UT WOS:000393967900005 ER PT J AU Stevenson, KB Line, MR Bean, JL Desert, JM Fortney, JJ Showman, AP Kataria, T Kreidberg, L Feng, YK AF Stevenson, Kevin B. Line, Michael R. Bean, Jacob L. Desert, Jean-Michel Fortney, Jonathan J. Showman, Adam P. Kataria, Tiffany Kreidberg, Laura Feng, Y. Katherina TI SPITZER PHASE CURVE CONSTRAINTS FOR WASP-43b AT 3.6 AND 4.5 mu m SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (WASP-43); techniques: photometric ID HOT JUPITER WASP-43B; SYSTEMATIC RETRIEVAL ANALYSIS; NO THERMAL INVERSION; EXOPLANET GJ 436B; HD 209458B; ATMOSPHERIC CIRCULATION; LIGHT CURVES; TRANSMISSION SPECTRUM; HEAT REDISTRIBUTION; EXTRASOLAR PLANET AB Previous measurements of heat redistribution efficiency (the ability to transport energy from a planet's highly irradiated dayside to its eternally dark nightside) show considerable variation between exoplanets. Theoretical models predict a positive correlation between heat redistribution efficiency and temperature for tidally locked planets; however, recent Hubble Space Telescope (HST) WASP-43b spectroscopic phase curve results are inconsistent with current predictions. Using the Spitzer Space Telescope, we obtained a total of three phase curve observations of WASP-43b (P = 0.813 days) at 3.6 and 4.5. mu m. The first 3.6. mu m visit exhibits spurious nightside emission that requires invoking unphysical conditions in our cloud-free atmospheric retrievals. The two other visits exhibit strong day-night contrasts that are consistent with the HST data. To reconcile the departure from theoretical predictions, WASP-43b would need to have a high-altitude, nightside cloud/haze layer blocking its thermal emission. Clouds/hazes could be produced within the planet's cool, nearly retrograde mid-latitude flows before dispersing across its nightside at high altitudes. Since mid-latitude flows only materialize in fast-rotating (less than or similar to 1 day) planets, this may explain an observed trend connecting measured day-night contrast with planet rotation rate that matches all current Spitzer phase curve results. Combining independent planetary emission measurements from multiple phases, we obtain a precise dayside hemisphere H2O abundance (2.5 x 10(-5)-1.1 x 10(-4) at 1 sigma confidence) and, assuming chemical equilibrium and a scaled solar abundance pattern, we derive a corresponding metallicity estimate that is consistent with being solar (0.4-1.7). Using the retrieved global CO+CO2 abundance under the same assumptions, we estimate a comparable metallicity of 0.3-1.7x solar. This is the first time that precise abundance and metallicity constraints have been determined from multiple molecular tracers for a transiting exoplanet. C1 [Stevenson, Kevin B.; Bean, Jacob L.; Kreidberg, Laura] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Stevenson, Kevin B.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Line, Michael R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Line, Michael R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Desert, Jean-Michel] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1012 WX Amsterdam, Netherlands. [Fortney, Jonathan J.; Feng, Y. Katherina] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Showman, Adam P.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Kataria, Tiffany] Univ Exeter, Sch Phys, Astrophys Grp, Stocker Rd, Exeter EX4 4QL, Devon, England. [Kataria, Tiffany] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Kreidberg, Laura] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Kreidberg, Laura] Harvard Univ, Harvard Soc Fellows, Cambridge, MA 02138 USA. RP Stevenson, KB (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.; Stevenson, KB (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM kbs@stsci.edu FU Sagan Fellowship Program; NASA; David and Lucile Packard Foundation FX We appreciate the thoughtful suggestions from the anonymous referee. We thank contributors to SciPy, Matplotlib, and the Python Programming Language, the free and open-source community, the NASA Astrophysics Data System, and the JPL Solar System Dynamics group for software and services. K.B.S. recognizes support from the Sagan Fellowship Program, supported by NASA and administered by the NASA Exoplanet Science Institute (NExScI). J.L.B. acknowledges support from the David and Lucile Packard Foundation. NR 75 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 FEB PY 2017 VL 153 IS 2 AR 68 DI 10.3847/1538-3881/153/2/68 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EK5LM UT WOS:000393967900003 ER PT J AU Ziegler, C Law, NM Morton, T Baranec, C Riddle, R Atkinson, D Baker, A Roberts, S Ciardi, DR AF Ziegler, Carl Law, Nicholas M. Morton, Tim Baranec, Christoph Riddle, Reed Atkinson, Dani Baker, Anna Roberts, Sarah Ciardi, David R. TI ROBO-AO KEPLER PLANETARY CANDIDATE SURVEY. III. ADAPTIVE OPTICS IMAGING OF 1629 KEPLER EXOPLANET CANDIDATE HOST STARS SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: close; instrumentation: adaptive optics; methods: data analysis; methods: observational; planets and satellites: detection; techniques: high angular resolution ID FALSE-POSITIVE PROBABILITIES; SOLAR-TYPE STARS; STELLAR MULTIPLICITY; TRANSITING PLANETS; HABITABLE PLANETS; COMPANIONS; TELESCOPE; SYSTEMS; OBJECTS; BINARY AB The Robo-AO Kepler Planetary Candidate Survey is observing every Kepler planet candidate host star with laser adaptive optics imaging to search for blended nearby stars, which may be physically associated companions and/ or responsible for transit false positives. In this paper, we present the results of our search for stars nearby 1629 Kepler planet candidate hosts. With survey sensitivity to objects as close as similar to 0 ''.15, and magnitude differences Delta m <= 6, we find 223 stars in the vicinity of 206 target KOIs; 209 of these nearby stars have not been previously imaged in high resolution. We measure an overall nearby-star probability for Kepler planet candidates of 12.6% +/- 0.9% at separations between 0 ''.15 and 4 ''.0. Particularly interesting KOI systems are discussed, including 26 stars with detected companions that host rocky, habitable zone candidates and five new candidate planet-hosting quadruple star systems. We explore the broad correlations between planetary systems and stellar binarity, using the combined data set of Baranec et al. and this paper. Our previous 2 sigma result of a low detected nearby star fraction of KOIs hosting close-in giant planets is less apparent in this larger data set. We also find a significant correlation between detected nearby star fraction and KOI number, suggesting possible variation between early and late Kepler data releases. C1 [Ziegler, Carl; Law, Nicholas M.] Univ North Carolina Chapel Hill, Dept Phys & Astron, Chapel Hill, NC 27599 USA. [Morton, Tim] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Baranec, Christoph; Atkinson, Dani] Univ Hawaii Manoa, Inst Astron, Hilo, HI 96720 USA. [Riddle, Reed] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Baker, Anna] Durham Acad Upper Sch, 3601 Ridge Rd, Durham, NC 27705 USA. [Roberts, Sarah] Juniata Coll, 1700 Moore St, Huntingdon, PA 16652 USA. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. RP Ziegler, C (reprint author), Univ North Carolina Chapel Hill, Dept Phys & Astron, Chapel Hill, NC 27599 USA. EM carlziegler@unc.edu OI Ciardi, David/0000-0002-5741-3047 FU NASA Exoplanets Research Program [NNX 15AC91G]; Alfred P. Sloan Foundation; NASA under the Kepler Participating Scientist Program [NNX 14AE11G]; NASA Space Technology Research Fellowship [NNX 13AL75H]; California Institute of Technology; Inter-University Centre for Astronomy and Astrophysics; National Science Foundation [AST-0906060, AST-0960343, AST-1207891]; Mount Cuba Astronomical Foundation; W.M. Keck Foundation FX This research is supported by the NASA Exoplanets Research Program, grant # NNX 15AC91G. C.B. acknowledges support from the Alfred P. Sloan Foundation. T.M. is supported by NASA grant # NNX 14AE11G under the Kepler Participating Scientist Program. D.A. is supported by a NASA Space Technology Research Fellowship, grant # NNX 13AL75H.; The Robo-AO system is supported by collaborating partner institutions, the California Institute of Technology, the Inter-University Centre for Astronomy and Astrophysics, the National Science Foundation under Grant Nos. AST-0906060, AST-0960343, and AST-1207891, the Mount Cuba Astronomical Foundation, and by a gift from Samuel Oschin. We are grateful to the Palomar Observatory staff for their ongoing support of Robo-AO on the 1.5 m telescope, particularly S. Kunsman, M. Doyle, J. Henning, R. Walters, G. Van Idsinga, B. Baker, K. Dunscombe, and D. Roderick.; Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. Some of the data presented herein is based on observations obtained at the Gemini Observatory, operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership. We recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 96 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD FEB PY 2017 VL 153 IS 2 AR 66 DI 10.3847/1538-3881/153/2/66 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EK5LM UT WOS:000393967900001 ER PT J AU Stafoggia, M Schwartz, J Badaloni, C Bellander, T Alessandrini, E Cattani, G de' Donato, F Gaeta, A Leone, G Lyapustin, A Sorek-Hamer, M de Hoogh, K Di, Q Forastiere, F Kloog, I AF Stafoggia, Massimo Schwartz, Joel Badaloni, Chiara Bellander, Tom Alessandrini, Ester Cattani, Giorgio de' Donato, Francesca Gaeta, Alessandra Leone, Gianluca Lyapustin, Alexei Sorek-Hamer, Meytar de Hoogh, Kees Di, Qian Forastiere, Francesco Kloog, Itai TI Estimation of daily PM10 concentrations in Italy (2006-2012) using finely resolved satellite data, land use variables and meteorology SO ENVIRONMENT INTERNATIONAL LA English DT Article DE Aerosol Optical Depth; Air pollution; Epidemiology; Exposure assessment; Particulate matter; Satellite ID AEROSOL OPTICAL DEPTH; LONG-TERM EXPOSURE; AMBIENT AIR-POLLUTION; MED-PARTICLES PROJECT; 11 EUROPEAN COHORTS; ESCAPE PROJECT; PM2.5 CONCENTRATIONS; USE REGRESSION; PARTICULATE MATTER; MEASUREMENT ERROR AB Health effects of air pollution, especially particulate matter (PM), have been widely investigated. However, most of the studies rely on few monitors located in urban areas for short-term assessments, or land use/dispersion modelling for long-term evaluations, again mostly in cities. Recently, the availability of finely resolved satellite data provides an opportunity to estimate daily concentrations of air pollutants over wide spatio-temporal domains. Italy lacks a robust and validated high resolution spatio-temporally resolved model of particulate matter. The complex topography and the air mixture from both natural and anthropogenic sources are great challenges difficult to be addressed. We combined finely resolved data on Aerosol Optical Depth (ACID) from the Multi Angle Implementation of Atmospheric Correction (MAIAC) algorithm, ground-level PM10 measurements, land use variables and meteorological parameters into a four-stage mixed model framework to derive estimates of daily PM10 concentrations at 1-km2 grid over Italy, for the years 2006-2012. We checked performance of our models by applying 10-fold cross-validation (CV) for each year. Our models displayed good fitting, with mean CV-R2 = 0.65 and little bias (average slope of predicted VS observed PM10 = 0.99). Out-of-sample predictions were more accurate in Northern Italy (Po valley) and large conurbations (e.g. Rome), for background monitoring stations, and in the winter season. Resulting concentration maps showed highest average PIVim levels in specific areas (Po river valley, main industrial and metropolitan areas) with decreasing trends over time. Our daily predictions of PM10 concentrations across the whole Italy will allow, for the first time, estimation of long-term and short-term effects of air pollution nationwide, even in areas lacking monitoring data. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Stafoggia, Massimo; Badaloni, Chiara; Alessandrini, Ester; de' Donato, Francesca; Forastiere, Francesco] Lazio Reg Hlth Serv ASL Roma 1, Dept Epidemiol, Via C Colombo 112, I-00147 Rome, Italy. [Stafoggia, Massimo; Bellander, Tom] Karolinska Inst, Inst Environm Med, Stockholm, Sweden. [Schwartz, Joel; Di, Qian] Harvard TH Chan Sch Publ Hlth, Dept Environm Hlth, Cambridge, MA USA. [Bellander, Tom] Stockholm Cty Council, Ctr Occupat & Environm Med, Stockholm, Sweden. [Cattani, Giorgio; Gaeta, Alessandra; Leone, Gianluca] Italian Natl Inst Environm Protect & Res, Rome, Italy. [Lyapustin, Alexei] NASA, GSFC, Greenbelt, MD USA. [Sorek-Hamer, Meytar] Technion, Civil & Environm Engn, Haifa, Israel. [Sorek-Hamer, Meytar; Kloog, Itai] Ben Gurion Univ Negev, Dept Geog & Environm Dev, Beer Sheva, Israel. [de Hoogh, Kees] Swiss Trop & Publ Hlth Inst, Basel, Switzerland. [de Hoogh, Kees] Univ Basel, Basel, Switzerland. RP Stafoggia, M (reprint author), Lazio Reg Hlth Serv ASL Roma 1, Dept Epidemiol, Via C Colombo 112, I-00147 Rome, Italy. EM m.stafoggia@deplazio.it NR 53 TC 1 Z9 1 U1 5 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0160-4120 EI 1873-6750 J9 ENVIRON INT JI Environ. Int. PD FEB PY 2017 VL 99 BP 234 EP 244 DI 10.1016/j.envint.2016.11.024 PG 11 WC Environmental Sciences SC Environmental Sciences & Ecology GA EK6UZ UT WOS:000394062700023 PM 28017360 ER PT J AU Dimech, JL Stern, T Lamb, S AF Dimech, Jesse-Lee Stern, Tim Lamb, Simon TI Mantle earthquakes, crustal structure, and gravitational instability beneath western North Island, New Zealand SO GEOLOGY LA English DT Article ID CONTINENTAL LITHOSPHERE; RECEIVER FUNCTIONS; SIERRA-NEVADA; DEFORMATION; ARC; DELAMINATION; EVOLUTION; VOLCANISM; TARANAKI; REMOVAL AB A cluster of 30-52-km-deep earthquakes, and a 7-10 km step in the Moho beneath western North Island, New Zealand, are both interpreted as manifestations of active delamination of the continental lower crust and mantle lithosphere. These phenomena occur in the back-arc region beneath the east-west-oriented Taranaki-Ruapehu (TR) line, which strikes at a high angle to the present-day plate boundary through New Zealand. Across the line, there is an abrupt change in crustal and mantle lid thickness, and in upper-mantle seismic attenuation (Q(p)(-1)), showing that the mantle lithosphere has been highly thinned on the north side. We show from a receiver function profile that nearly all of the deep earthquakes reside in the uppermost mantle on the northern side of the TR line. A sum of earthquake moment tensors suggests strike-slip motion either parallel, or orthogonal, to the TR line, resulting in northwestsoutheast-oriented horizontal extension. Active normal faults, oriented northwest-southeast and north-south, are seen at the surface on each side of the TR line, but the surface is uplifting here at similar to 0.4 mm/yr. This requires the mantle lithosphere to be thinning at a higher rate than the overlying crust, consistent with a delamination process. C1 [Dimech, Jesse-Lee] Victoria Univ Wellington, Sch Geog Environm & Earth Sci, Wellington 6140, New Zealand. Victoria Univ Wellington, Inst Geophys, Wellington 6140, New Zealand. [Dimech, Jesse-Lee] NASA, Marshall Space Flight Ctr USRA, Huntsville, AL 35805 USA. RP Dimech, JL (reprint author), Victoria Univ Wellington, Sch Geog Environm & Earth Sci, Wellington 6140, New Zealand.; Dimech, JL (reprint author), NASA, Marshall Space Flight Ctr USRA, Huntsville, AL 35805 USA. FU Royal Society of New Zealand Marsden funding FX Support for this research was provided by Royal Society of New Zealand Marsden funding. We thank the ANSIR partnership for the use of 10 broadband portable seismographs in this study, and G. Houseman and W. Stratford for comments on earlier versions of this paper. E. Smith is acknowledged for assistance in estimating uncertainty ellipses for the moment tensor sums. Michelle Salmon and Oliver Boyd are thanked for their assistance in creating the observed and synthetic receiver function stacks, respectively. NR 41 TC 0 Z9 0 U1 1 U2 1 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 EI 1943-2682 J9 GEOLOGY JI Geology PD FEB PY 2017 VL 45 IS 2 BP 155 EP 158 DI 10.1130/G38476.1 PG 4 WC Geology SC Geology GA EN6OZ UT WOS:000396124600019 ER PT J AU Loomis, BD Luthcke, SB AF Loomis, B. D. Luthcke, S. B. TI Mass evolution of Mediterranean, Black, Red, and Caspian Seas from GRACE and altimetry: accuracy assessment and solution calibration SO JOURNAL OF GEODESY LA English DT Article DE GRACE; Sea surface altimetry; Steric sea level; Inter-satellite range-acceleration; EEMD ID NONSTATIONARY TIME-SERIES; SATELLITE GRAVITY; VARIABLE GRAVITY; VARIABILITY; GREENLAND; SEAWATER; SYSTEM; SPACE; FIELD; GULF AB We present new measurements of mass evolution for the Mediterranean, Black, Red, and Caspian Seas as determined by the NASA Goddard Space Flight Center (GSFC) GRACE time-variable global gravity mascon solutions. These new solutions are compared to sea surface altimetry measurements of sea level anomalies with steric corrections applied. To assess their accuracy, the GRACE- and altimetry-derived solutions are applied to the set of forward models used by GSFC for processing the GRACE Level-1B datasets, with the resulting inter-satellite range-acceleration residuals providing a useful metric for analyzing solution quality. We also present a differential correction strategy to calibrate the time series of mass change for each of the seas by establishing the strong linear relationship between differences in the forward modeled mass and the corresponding range-acceleration residuals between the two solutions. These calibrated time series of mass change are directly determined from the range-acceleration residuals, effectively providing regionally-tuned GRACE solutions without the need to form and invert normal equations. Finally, the calibrated GRACE time series are discussed and combined with the steric-corrected sea level anomalies to provide new measurements of the unmodeled steric variability for each of the seas over the span of the GRACE observation record. We apply ensemble empirical mode decomposition (EEMD) to adaptively sort the mass and steric components of sea level anomalies into seasonal, non-seasonal, and long-term temporal scales. C1 [Loomis, B. D.] SGT Inc, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. [Luthcke, S. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Loomis, BD (reprint author), SGT Inc, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. EM bryant.d.loomis@nasa.gov FU NASA [NNH10ZDA0-01N, NNH15ZDA001N] FX Support for this work was provided by the NASA GRACE and GRACE Follow-On Science Team Grants NNH10ZDA0-01N and NNH15ZDA001N. We gratefully acknowledge the quality of the GRACE Level-1B products produced by our colleagues at the Jet Propulsion Laboratory, California Institute of Technology, Pasadena. We thank J.P. Boy and R.D. Ray for contributions to the forward models applied in our GRACE data reduction and analysis. We especially acknowledge the numerous contributions of D.D. Rowlands and T.J. Sabaka in developing the foundation of algorithms and software necessary to carry out this research. We also thank the reviewers who provided valuable feedback towards improving this manuscript. The GRACE Level-1B products are available at the Physical Oceanography Distributed Active Archive Center (PO. DAAC)at https://podaac.jpl.nasa.gov/. The sea level anomaly grids are produced by the Sea Level Thematic Assembly Centre (SL-TAC) and hosted by Copernicus Marine Environment Monitoring Service at http://marine.copernicus.eu/. The Gibbs Seawater Oceanographic Toolbox for implementing TEOS-10 is available at http://www.teos-10.org/. MERRA-2 data is available at http://disc.sci.gsfc.nasa.gov/mdisc/. NR 38 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0949-7714 EI 1432-1394 J9 J GEODESY JI J. Geodesy PD FEB PY 2017 VL 91 IS 2 BP 195 EP 206 DI 10.1007/s00190-016-0952-3 PG 12 WC Geochemistry & Geophysics; Remote Sensing SC Geochemistry & Geophysics; Remote Sensing GA EK9SO UT WOS:000394264400005 ER PT J AU Guo, JN Slaba, TC Zeitlin, C Wimmer-Schweingruber, RF Badavi, FF Bohm, E Bottcher, S Brinza, DE Ehresmann, B Hassler, DM Matthia, D Rafkin, S AF Guo, Jingnan Slaba, Tony C. Zeitlin, Cary Wimmer-Schweingruber, Robert F. Badavi, Francis F. Boehm, Eckart Boettcher, Stephan Brinza, David E. Ehresmann, Bent Hassler, Donald M. Matthiae, Daniel Rafkin, Scot TI Dependence of the Martian radiation environment on atmospheric depth: Modeling and measurement SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ENERGETIC PARTICLE RADIATION; SOLAR PROTON EXPOSURE; ASSESSMENT DETECTOR; ICRU SPHERE; MARS; SURFACE; VISUALIZATION; GEOMETRY; RAD AB The energetic particle environment on the Martian surface is influenced by solar and heliospheric modulation and changes in the local atmospheric pressure (or column depth). The Radiation Assessment Detector (RAD) on board the Mars Science Laboratory rover Curiosity on the surface of Mars has been measuring this effect for over four Earth years (about two Martian years). The anticorrelation between the recorded surface Galactic Cosmic Ray-induced dose rates and pressure changes has been investigated by Rafkin et al. (2014) and the long-term solar modulation has also been empirically analyzed and modeled by Guo et al. (2015). This paper employs the newly updated HZETRN2015 code to model the Martian atmospheric shielding effect on the accumulated dose rates and the change of this effect under different solar modulation and atmospheric conditions. The modeled results are compared with the most up-to-date (from 14 August 2012 to 29 June 2016) observations of the RAD instrument on the surface of Mars. Both model and measurements agree reasonably well and show the atmospheric shielding effect under weak solar modulation conditions and the decline of this effect as solar modulation becomes stronger. This result is important for better risk estimations of future human explorations to Mars under different heliospheric and Martian atmospheric conditions. C1 [Guo, Jingnan; Wimmer-Schweingruber, Robert F.; Boehm, Eckart; Boettcher, Stephan] Christian Albrechts Univ Kiel, Inst Expt & Appl Phys, Kiel, Germany. [Slaba, Tony C.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Zeitlin, Cary] Lockheed Martin IS & GS, Oakland, CA USA. [Badavi, Francis F.] Old Dominion Univ, Res Fdn, Norfolk, VA USA. [Brinza, David E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Ehresmann, Bent; Hassler, Donald M.; Rafkin, Scot] Southwest Res Inst, Space Sci & Engn Div, Boulder, CO USA. [Hassler, Donald M.] Inst Astrophys Spatiale, Orsay, France. [Matthiae, Daniel] Deutsch Zentrum Luft & Raumfahrt, Inst Aerosp Med, Cologne, Germany. RP Guo, JN (reprint author), Christian Albrechts Univ Kiel, Inst Expt & Appl Phys, Kiel, Germany. EM guo@physik.uni-kiel.de OI Matthia, Daniel/0000-0003-1507-0143 FU National Aeronautics and Space Administration (NASA, HEOMD) under Jet Propulsion Laboratory (JPL) [1273039]; DLR's Space Administration [50QM0501, 50QM1201]; DLR FX RAD is supported by the National Aeronautics and Space Administration (NASA, HEOMD) under Jet Propulsion Laboratory (JPL) subcontract 1273039 to Southwest Research Institute and in Germany by DLR and DLR's Space Administration grants 50QM0501 and 50QM1201 to the Christian Albrechts University, Kiel. Part of this research was carried out at JPL, California Institute of Technology, under a contract with NASA. We are grateful to the Cosmic Ray Station of the University of Oulu and Sodankyla Geophysical Observatory for sharing their Neutron Monitor count rate data. The data used in this paper are archived in the NASA Planetary Data System's Planetary Plasma Interactions Node at the University of California, Los Angeles. The archival volume includes the full binary raw data files, detailed descriptions of the structures therein, and higher- level data products in human readable form. The PPI node is hosted at http://ppi.pds.nasa.gov/. NR 31 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD FEB PY 2017 VL 122 IS 2 BP 329 EP 341 DI 10.1002/2016JE005206 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EN5CQ UT WOS:000396023600002 ER PT J AU Rhoden, AR Henning, W Hurford, TA Patthoff, DA Tajeddine, R AF Rhoden, Alyssa Rose Henning, Wade Hurford, Terry A. Patthoff, D. Alex Tajeddine, Radwan TI The implications of tides on the Mimas ocean hypothesis SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID NONSYNCHRONOUS ROTATION; SOUTH-POLE; WATER ICE; ENCELADUS; STRESSES; INTERIOR; EUROPA; CONSTRAINTS; SATELLITES; ERUPTIONS AB We investigate whether a present-day global ocean within Mimas is compatible with the lack of tectonic activity on its surface by computing tidal stresses for ocean-bearing interior structure models derived from observed librations. We find that, for the suite of compatible rheological models, peak surface tidal stresses caused by Mimas' high eccentricity would range from a factor of 2 smaller to an order of magnitude larger than those on tidally active Europa. Thermal stresses from a freezing ocean, or a past higher eccentricity, would enhance present-day tidal stresses, exceeding the magnitudes associated with Europa's ubiquitous tidally driven fractures and, in some cases, the failure strength of ice in laboratory studies. Therefore, in order for Mimas to have an ocean, its ice shell cannot fail at the stress values implied for Europa. Furthermore, if Mimas' ocean is freezing out, the ice shell must also be able to withstand thermal stresses that could be an order of magnitude higher than the failure strength of laboratory ice samples. In light of these challenges, we consider an ocean-free Mimas to be the most straightforward model, best supported by our tidal stress analysis. C1 [Rhoden, Alyssa Rose] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Henning, Wade] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Hurford, Terry A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Patthoff, D. Alex] Planetary Sci Inst, Tucson, AZ USA. [Tajeddine, Radwan] Cornell Univ, Ctr Astrophys & Planetary Sci, Ithaca, NY USA. RP Rhoden, AR (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. EM Alyssa.Rhoden@asu.edu FU NASA Outer Planet Research Program [NNH13ZDA001N]; Cassini mission FX This work was supported by NASA Outer Planet Research Program grant NNH13ZDA001N and the Cassini mission. The results in this paper can be reproduced using the equations reported herein and in the cited references, using the parameters values given in the tables and references. Model output is included in the supporting information. NR 31 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD FEB PY 2017 VL 122 IS 2 BP 400 EP 410 DI 10.1002/2016JE005097 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EN5CQ UT WOS:000396023600006 ER PT J AU Sears, DWG Sears, H Sehlke, A Hughes, SS AF Sears, Derek W. G. Sears, Hazel Sehlke, Alexander Hughes, Scott S. TI Induced thermoluminescence as a method for dating recent volcanism: Eastern Snake River Plain, Idaho, USA SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID THERMO-LUMINESCENCE; ORDINARY CHONDRITES; REHEATING HISTORY; METEORITES; SHOCK; TRANSITION; BASALTS; SAMPLES; TL AB The induced thermoluminescence properties of 24 samples of basalts from volcanoes in the eastern Snake River Plain, Idaho, were measured as part of an investigation into the possibility of using this technique for dating purposes. The volcanic flows sampled ranged in age from 2200 years to similar to 400,000 years. The thermoluminescence (TL) sensitivity values obtained, i.e., maximum induced TL normalized to that of the Dhajala meteorite (where Dhajala = 1000), ranged from 1.6 +/- 0.3 to 226 +/- 15 and showed a correlation between log TL and age with an r(2) value of 0.47. Thus, TL sensitivity values correlate with age in the manner expected, although there is a high level of scatter. We discuss various mechanisms for the correlation and scatter, particularly (1) the role of primary (igneous processes) and secondary (solid state processes), (2) composition of the plagioclase feldspar, and (3) weathering. The induced TL signal from feldspars, the mineral responsible for the TL, is strongly dependent on their composition, and correcting for this improved the correlation (r(2) = 0.7). Variations in primary feldspar are affecting the data, but we find no evidence that weathering of the samples is important. Further work is required to explore the remaining causes for the scatter and the TL-age trend. However, it is clear from the present study that induced TL has the potential for dating volcanism on the 2200 to 400,000 year time frame. This dating method, if successful, would be well-suited to spacecraft use since it requires low mass and low power instruments with a low data demand. C1 [Sears, Derek W. G.; Sears, Hazel] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Mountain View, CA 94035 USA. [Sehlke, Alexander] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. [Hughes, Scott S.] Idaho State Univ, Geosci Dept, Pocatello, ID 83209 USA. RP Sears, DWG (reprint author), NASA, Ames Res Ctr, Bay Area Environm Res Inst, Mountain View, CA 94035 USA. EM derek.sears@nasa.gov FU NASA's Solar System Exploration Research Virtual Institute FX All data gathered in the execution of this work are included in this article. We appreciate funding by NASA's Solar System Exploration Research Virtual Institute via the FINESSE team, Jennifer Heldmann PI, and we appreciate the help of the FINESSE team members in collecting the samples. NR 50 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD FEB PY 2017 VL 122 IS 2 BP 906 EP 922 DI 10.1002/2016JB013596 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EN6RX UT WOS:000396132200009 ER PT J AU Suhir, E Ghaffarian, R Yi, S AF Suhir, E. Ghaffarian, R. Yi, S. TI Probabilistic Palmgren-Miner rule, with application to solder materials experiencing elastic deformations SO JOURNAL OF MATERIALS SCIENCE-MATERIALS IN ELECTRONICS LA English DT Article ID THERMAL-STRESSES; BIMETAL THERMOSTATS; PREDICTED STRESSES; ENDS AB It has been recently shown that there are effective ways not only to reduce the interfacial stresses in electronic packaging assemblies with solder joint arrays as the second level of interconnections, but to do that to an extent that inelastic strains in the peripheral joints, where the induced thermal stresses and strains are the highest, are avoided. While various and numerous modifications of the empirical Coffin-Manson relationship are used to predict the fatigue life of solder materials experiencing inelastic strains and operated in low cycle fatigue conditions, the Palmgren-Miner rule of the linear accumulation of fatigue damages, although suggested many decades ago, is still viewed by many material scientists and reliability physicists as a suitable model that enables one to quantify the cumulative fatigue damage in metals experiencing elastic strains. In this analysis the Palmgren-Miner rule is extended for the case of random loading, and a simple formalism is suggested for the evaluation of the remaining useful lifetime for a solder material subjected to random loading and experiencing elastic thermally induced shearing deformations. Special highly focused and highly cost effective accelerated tests have to be conducted, of course, to establish the S-N curve for the given solder material. In the future work we intend to extend the suggested methodology to take into account various aspects of the physics-of-failure: the role of the growth kinetics of intermetallic compound layers; the random number, size and orientation of grains in the joints; position of the joint with respect to the mid-cross-section of the assembly (peripheral joints are more prone to elevated interfacial stresses); assembly size, etc. All this effort, important as it is, is, however, beyond the scope of this analysis, which is aimed at the extension of the classical Palmgren-Miner rule for the case of random loading. C1 [Suhir, E.; Yi, S.] 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 38 TC 0 Z9 0 U1 0 U2 0 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 FEB PY 2017 VL 28 IS 3 BP 2680 EP 2685 DI 10.1007/s10854-016-5845-y PG 6 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Engineering; Materials Science; Physics GA EK9DQ UT WOS:000394224600047 ER PT J AU Sarkar, S Singh, RP AF Sarkar, Sudipta Singh, Ramesh P. TI June 19 2015 Rainfall Event Over Mumbai: Some Observational Analysis SO JOURNAL OF THE INDIAN SOCIETY OF REMOTE SENSING LA English DT Article DE India; Rainfall; Mumbai; Local-disturbance; Sea-surface temperature; Geopotential height; Wind shear ID 26 JULY 2005; MONSOON; INDIA AB Some of the major metropolitan centers in the world are highly susceptible to flash floods and major disruptions, owing to sudden and excessive rainfall events. The city of Mumbai, India's financial capital, suffered one such event on 19 June, 2015. This was a second event of such nature, following the landmark event of 26 July, 2005. Such extreme rainfall events are often brought about by certain rapidly developing, local disturbances, which if actively monitored, may be provide important information that can be of great use for early warning to civic authorities and emergency planners. In this paper, we have analyzed a number of different meteorological and remotely sensed parameters, a few days before the actual event, to track the development and eventual culmination of a "perfect storm" that affected Mumbai and left the city tattered. We show how regional upper layer disturbance patterns are developed, induced by warming of sea-surface temperature (SST) and sustained by instability in the atmospheric boundary layers to quickly develop into massive cyclonic storms. C1 [Sarkar, Sudipta] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. [Sarkar, Sudipta] Sci Syst & Applicat Inc, 10210 Greenbelt Rd,Suite 600, Lanham, MD 20706 USA. [Singh, Ramesh P.] Chapman Univ, Schmid Coll Sci & Technol, Sch Life & Environm Sci, One Univ Dr, Orange, CA 92866 USA. RP Sarkar, S (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.; Sarkar, S (reprint author), Sci Syst & Applicat Inc, 10210 Greenbelt Rd,Suite 600, Lanham, MD 20706 USA. EM sdptsarkar2@gmail.com NR 17 TC 0 Z9 0 U1 1 U2 1 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0255-660X EI 0974-3006 J9 J INDIAN SOC REMOTE JI J. Indian Soc. Remote Sens. PD FEB PY 2017 VL 45 IS 1 BP 185 EP 192 DI 10.1007/s12524-016-0572-7 PG 8 WC Environmental Sciences; Remote Sensing SC Environmental Sciences & Ecology; Remote Sensing GA EK9KL UT WOS:000394243200020 ER PT J AU Kammoun, ES Risaliti, G Stern, D Jun, HD Graham, M Celotti, A Behar, E Elvis, M Harrison, FA Matt, G Walton, DJ AF Kammoun, E. S. Risaliti, G. Stern, D. Jun, H. D. Graham, M. Celotti, A. Behar, E. Elvis, M. Harrison, F. A. Matt, G. Walton, D. J. TI Coronal properties of the luminous radio-quiet quasar QSO B2202-209 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: nuclei; quasars: individual; QSO B2202-209; X-rays: galaxies ID X-RAY REFLECTION; ACTIVE GALACTIC NUCLEI; PHOTON IMAGING CAMERA; BLACK-HOLE; SEYFERT-GALAXIES; XMM-NEWTON; ACCRETION DISKS; COMPTONIZATION MODELS; SWIFT J2127.4+5654; DATA RELEASE AB We present an analysis of the joint XMM-Newton and NuSTAR observations of the radio-quiet quasar QSO B2202-209. Using an optical observation from the Hale Telescope at the Palomar Observatory, we revise the redshift of the source from the previously reported z = 1.77 to z = 0.532, and we estimate the mass of the central black hole, log (MBH/M-circle dot) = 9.08 +/- 0.18. The X-ray spectrum of this source can be well described by a power law of photon index Gamma = 1.82 +/- 0.05 with E-cut = 152(-54)(+103) keV, in the rest frame of the source. Assuming a Comptonization model, we estimate the coronal temperature to be kT(e) = 42 +/- 3 keV and kTe = 56 +/- 3 keVfor a spherical and a slab geometry, respectively. The coronal properties are comparable to the ones derived for local active galactic nuclei, despite a difference of around one order of magnitude in black hole mass and X-ray luminosity ( L-2 (-) (10) = 1.93 x 10(45) erg s(-1)). The quasar is X-ray loud, with an unusually flat observed optical-to-X-ray spectral slope alpha(OX) = 1.00 +/- 0.02, and has an exceptionally strong optical [O-III] line. Assuming that both the X-ray emission and the [O-III] line are isotropic, these two extreme properties can be explained by a nearly edge-on disc, leading to a reduction in the observed ultraviolet continuum light. C1 [Kammoun, E. S.; Celotti, A.] SISSA, Via Bonomea 265, I-34135 Trieste, Italy. [Risaliti, G.] Univ Florence, Dipartimento Fis & Astron, Via G Sansone 1, I-50019 Florence, Italy. [Risaliti, G.] Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy. [Stern, D.; Jun, H. D.; Walton, D. J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Graham, M.; Harrison, F. A.] CALTECH, 1200 East Calif Blvd, Pasadena, CA 91125 USA. [Celotti, A.] INAF Osservatorio Astron Brera, Via Bianchi 46, I-23807 Merate, Italy. [Celotti, A.] Ist Nazl Fis Nucl, Sez Trieste, Via Valerio 2, I-34127 Trieste, Italy. [Behar, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Elvis, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Matt, G.] Univ Roma Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy. RP Kammoun, ES (reprint author), SISSA, Via Bonomea 265, I-34135 Trieste, Italy. EM ekammoun@sissa.it FU NASA; ESA Member States; Hale Telescope at Palomar Observatory; European Union [655324] FX This research made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA, XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA, and the Hale Telescope at Palomar Observatory. 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). We like to acknowledge S.G. Djorgovski for providing the Palomar observations. We thank the anonymous referee for comments and suggestions, which significantly contributed to improving the quality of the manuscript. EB received funding from the European Union Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement no. 655324. 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 FEB PY 2017 VL 465 IS 2 BP 1665 EP 1671 DI 10.1093/mnras/stw2897 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EK2VT UT WOS:000393785500029 ER PT J AU Geach, JE Dunlop, JS Halpern, M Smail, I van der Werf, P Alexander, DM Almaini, O Aretxaga, I Arumugam, V Asboth, V Banerji, M Beanlands, J Best, PN Blain, AW Birkinshaw, M Chapin, EL Chapman, SC Chen, CC Chrysostomou, A Clarke, C Clements, DL Conselice, C Coppin, KEK Cowley, WI Danielson, ALR Eales, S Edge, AC Farrah, D Gibb, A Harrison, CM Hine, NK Hughes, D Ivison, RJ Jarvis, M Jenness, T Jones, SF Karim, A Koprowski, M Knudsen, KK Lacey, CG Mackenzie, T Marsden, G McAlpine, K McMahon, R Meijerink, R Michalowski, MJ Oliver, SJ Page, MJ Peacock, JA Rigopoulou, D Robson, EI Roseboom, I Rotermund, K Scott, D Serjeant, S Simpson, C Simpson, JM Smith, DJB Spaans, M Stanley, F Stevens, JA Swinbank, AM Targett, T Thomson, AP Valiante, E Wake, DA Webb, TMA Willott, C Zavala, JA Zemcov, M AF Geach, J. E. Dunlop, J. S. Halpern, M. Smail, Ian van der Werf, P. Alexander, D. M. Almaini, O. Aretxaga, I. Arumugam, V. Asboth, V. Banerji, M. Beanlands, J. Best, P. N. Blain, A. W. Birkinshaw, M. Chapin, E. L. Chapman, S. C. Chen, C-C. Chrysostomou, A. Clarke, C. Clements, D. L. Conselice, C. Coppin, K. E. K. Cowley, W. I. Danielson, A. L. R. Eales, S. Edge, A. C. Farrah, D. Gibb, A. Harrison, C. M. Hine, N. K. Hughes, D. Ivison, R. J. Jarvis, M. Jenness, T. Jones, S. F. Karim, A. Koprowski, M. Knudsen, K. K. Lacey, C. G. Mackenzie, T. Marsden, G. McAlpine, K. McMahon, R. Meijerink, R. Michalowski, M. J. Oliver, S. J. Page, M. J. Peacock, J. A. Rigopoulou, D. Robson, E. I. Roseboom, I. Rotermund, K. Scott, Douglas Serjeant, S. Simpson, C. Simpson, J. M. Smith, D. J. B. Spaans, M. Stanley, F. Stevens, J. A. Swinbank, A. M. Targett, T. Thomson, A. P. Valiante, E. Wake, D. A. Webb, T. M. A. Willott, C. Zavala, J. A. Zemcov, M. TI The SCUBA-2 Cosmology Legacy Survey: 850 mu m maps, catalogues and number counts SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE catalogues; surveys; galaxies: evolution; galaxies: high-redshift; cosmology: observations ID DEEP FIELD-SOUTH; SUBMILLIMETER GALAXY POPULATION; DEGREE EXTRAGALACTIC SURVEY; CLERK MAXWELL TELESCOPE; STAR-FORMING GALAXIES; SURVEY ALMA RESOLVES; 14 HOUR FIELD; MOLECULAR GAS; BOLOMETER CAMERA; HIGH-REDSHIFT AB We present a catalogue of similar to 3000 submillimetre sources detected (>= 3.5 sigma) at 850 mu m over similar to 5 deg(2) surveyed as part of the James Clerk Maxwell Telescope (JCMT) SCUBA-2 Cosmology Legacy Survey (S2CLS). This is the largest survey of its kind at 850 mu m, increasing the sample size of 850 mu m selected submillimetre galaxies by an order of magnitude. The wide 850 mu m survey component of S2CLS covers the extragalactic fields: UKIDSS-UDS, COSMOS, Akari-NEP, Extended Groth Strip, Lockman Hole North, SSA22 and GOODS-North. The average 1s depth of S2CLS is 1.2 mJy beam(-1), approaching the SCUBA-2 850 mu m confusion limit, which we determine to be sigma(c) approximate to 0.8 mJy beam(-1). We measure the 850 mu m number counts, reducing the Poisson errors on the differential counts to approximately 4 per cent at S-850 approximate to 3 mJy. With several independent fields, we investigate field-to-field variance, finding that the number counts on 0.5 degrees-1 degrees scales are generally within 50 per cent of the S2CLS mean for S-850 > 3 mJy, with scatter consistent with the Poisson and estimated cosmic variance uncertainties, although there is a marginal (2 sigma) density enhancement in GOODS-North. The observed counts are in reasonable agreement with recent phenomenological and semi-analytic models, although determining the shape of the faint-end slope (S-850 < 3 mJy) remains a key test. The large solid angle of S2CLS allows us to measure the bright-end counts: at S-850 > 10 mJy there are approximately 10 sources per square degree, and we detect the distinctive up-turn in the number counts indicative of the detection of local sources of 850 mu m emission, C1 [Geach, J. E.; Coppin, K. E. K.; Hine, N. K.; Koprowski, M.; Smith, D. J. B.; Stevens, J. A.] Univ Hertfordshire, Ctr Astrophys Res, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Dunlop, J. S.; Arumugam, V.; Best, P. N.; Ivison, R. J.; Peacock, J. A.; Robson, E. I.; Roseboom, I.; Simpson, J. M.] Univ Edinburgh, Royal Observ, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. [Halpern, M.; Asboth, V.; Gibb, A.; Jenness, T.; Mackenzie, T.; Marsden, G.; Michalowski, M. J.; Scott, Douglas] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada. [Smail, Ian; Alexander, D. M.; Chen, C-C.; Danielson, A. L. R.; Edge, A. C.; Harrison, C. M.; Stanley, F.; Swinbank, A. M.; Thomson, A. P.] Univ Durham, Dept Phys, Ctr Extragalact Astron, S Rd, Durham DH1 3LE, England. [van der Werf, P.; Meijerink, R.] Leiden Observ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Almaini, O.; Conselice, C.] Univ Nottingham, Sch Phys & Astron, Univ Pk, Nottingham NG9 2RD, England. [Aretxaga, I.; Hughes, D.; Zavala, J. A.] Inst Nacl Astrofis Opt & Electr, Calle Luis Enrique Erro 1, Puebla, Mexico. [Arumugam, V.; Ivison, R. J.; McMahon, R.] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Banerji, M.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 OHA, England. [Beanlands, J.] St Marys Univ, Dept Phys & Astron, 923 Robie St, Halifax, NS B3H 3C3, Canada. [Blain, A. W.] Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. [Birkinshaw, M.] Univ Bristol, HH Wills Phys Lab, Tyndall Ave, Bristol BS8 1TL, Avon, England. [Chapin, E. L.] Natl Res Council Canada, Herzberg Astron & Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada. [Chapman, S. C.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. [Chrysostomou, A.] Univ Manchester, SKA Headquarters, Manchester M13 9PL, Lancs, England. [Clarke, C.; Oliver, S. J.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, Prince Consort Rd, London SW7 2AZ, England. [Cowley, W. I.; Lacey, C. G.] Univ Durham, Dept Phys, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England. [Eales, S.; Valiante, E.] Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, Wales. [Farrah, D.] Virginia Polytech Inst & State Univ, Dept Phys, MC 0435,910 Drillfield Dr, Blacksburg, VA 24061 USA. [Jarvis, M.] Univ Oxford, Dept Phys, Keble Rd, Oxford OX1 3RH, England. [Jarvis, M.; McAlpine, K.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. [Jones, S. F.; Knudsen, K. K.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden. [Karim, A.] Univ Bonn, Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany. [Meijerink, R.; Spaans, M.] Univ Groningen, Kapteyn Inst, POB 800, NL-9700 AV Groningen, Netherlands. [Page, M. J.] Univ Coll London, Mullard Space Sci Lab, Surrey RH5 6NT, England. [Rigopoulou, D.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. [Robson, E. I.] Royal Observ, UK Astron Technol Ctr, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. [Serjeant, S.; Wake, D. A.] Open Univ, Dept Phys Sci, Robert Hooke Bldg, Milton Keynes MK7 6AA, Bucks, England. [Simpson, C.] Gemini Observ, Northern Operat Ctr, 760 N A'ohoku Pl, Hilo, HI 96720 USA. [Targett, T.] Sonoma State Univ, Dept Phys & Astron, 1801 East Cotati Ave, Rohnert Pk, CA 94928 USA. [Wake, D. A.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Webb, T. M. A.] McGill Univ, Dept Phys, 3600 Rue Univ, Montreal, PQ H3A 2T8, Canada. [Willott, C.] Natl Res Council Canada, Canadian Astron Data Ctr, 5071 West Saanich Rd, Victoria V9E 2E7, BC, Canada. [Zemcov, M.] Rochester Inst Technol, Sch Phys & Astron, Ctr Detectors, Rochester, NY 14623 USA. [Zemcov, M.] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Geach, JE (reprint author), Univ Hertfordshire, Ctr Astrophys Res, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. EM j.geach@herts.ac.uk FU Chinese Academy of Sciences [XDB09000000]; Science and Technology Facilities Council of the United Kingdom; Canadian Space Agency; BIS National E-infrastructure capital grant [ST/K00042X/1]; STFC capital grant [ST/H008519/1]; STFC DiRAC Operations grant [ST/K003267/1]; Durham University; Royal Society University Research Fellowship; ERC [321334, 321302]; Royal Society Wolfson Merit Award; European Research Council; Swedish Research Council; Collaborative Research Council 956 - Deutsche Forschungsgemeinschaft (DFG); [ST/L00075X/1] FX The authors thank M. Bethermin for supplying the SCUBA-2 850 mu m number count predictions. The James Clerk Maxwell Telescope is now operated by the East Asian Observatory on behalf of The National Astronomical Observatory of Japan, Academia Sinica Institute of Astronomy and Astrophysics, the Korea Astronomy and Space Science Institute, the National Astronomical Observatories of China and the Chinese Academy of Sciences (grant no. XDB09000000), with additional funding support from the Science and Technology Facilities Council of the United Kingdom and participating universities in the United Kingdom and Canada. The data presented in this paper were taken as part of Program ID MJLSC02. It is a pleasure to thank the entire staff of the JCMT for their superb support throughout the S2CLS campaign. Special thanks is due to Iain Coulson, Jessica Dempsey, Jim Hoge, Harriet Parsons, Callie Matulonis, William Montgomerie and Holly Thomas. This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency.; This work used the DiRAC Data Centric system at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk). This equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1, and STFC DiRAC Operations grant ST/K003267/1 and Durham University. DiRAC is part of the National E-Infrastructure.; JEG is supported by a Royal Society University Research Fellowship. IRS, AMS, JMS, ALRD, DMA, ACE and CGL acknowledge support from ST/L00075X/1. IRS also acknowledges support from the ERC Advanced Grant DUSTYGAL (321334) and a Royal Society Wolfson Merit Award. JSD acknowledges the support of the European Research Council through the award of an Advanced Grant. RJI acknowledges support from ERC in the form of the Advanced Investigator Programme COSMICISM (321302). AK acknowledges support by the Collaborative Research Council 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG). KK acknowledges supports from the Swedish Research Council. NR 121 TC 2 Z9 2 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 FEB PY 2017 VL 465 IS 2 BP 1789 EP 1806 DI 10.1093/mnras/stw2721 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EK2VT UT WOS:000393785500037 ER PT J AU Mohr-Smith, M Drew, JE Napiwotzki, R Simon-Diaz, S Wright, NJ Barentsen, G Eisloffel, J Farnhill, HJ Greimel, R Monguio, M Kalari, V Parker, QA Vink, JS AF Mohr-Smith, M. Drew, J. E. Napiwotzki, R. Simon-Diaz, S. Wright, N. J. Barentsen, G. Eisloeffel, J. Farnhill, H. J. Greimel, R. Monguio, M. Kalari, V. Parker, Q. A. Vink, J. S. TI The deep OB star population in Carina from the VST Photometric H alpha Survey (VPHAS plus ) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; stars: early-type; dust, extinction; Galaxy: disc; open clusters and associations: general ID INITIAL MASS FUNCTION; BLANKETED MODEL ATMOSPHERES; NORTHERN GALACTIC PLANE; SOUTHERN MILKY-WAY; WOLF-RAYET STARS; B-TYPE STARS; STELLAR PARAMETERS; SPACE DISTRIBUTION; FORMING COMPLEXES; MOLECULAR CLOUDS AB Massive OB stars are critical to the ecology of galaxies and yet our knowledge of OB stars in the Milky Way, fainter than V similar to 12, remains patchy. Data from the VST Photometric Ha Survey (VPHAS+) permit the construction of the first deep catalogues of blue excess-selected OB stars, without neglecting the stellar field. A total of 14 900 candidates with 2MASS cross-matches are blue-selected from a 42 deg(2) region in the Galactic plane, capturing the Carina Arm over the Galactic longitude range 282 degrees less than or similar to l less than or similar to 293 degrees. Spectral energy distribution fitting is performed on these candidates' combined VPHAS+ u, g, r, i and 2MASS J, H, K magnitudes. This delivers effective temperature constraints, statistically separating O from early-B stars and high-quality extinction parameters, A(0) and RV (random errors typically similar to 0.1). The high-confidence O-B2 candidates number 5915 and a further 5170 fit to later B spectral type. Spectroscopy of 276 of the former confirms 97 per cent of them. The fraction of emission-line stars among all candidate B stars is 7-8 per cent. Greyer (R-V > 3.5) extinction laws are ubiquitous in the region, over the distance range 2.5-3 to similar to 10 kpc. Near prominent massive clusters, RV tends to rise, with particularly large and chaotic excursions to R-V similar to 5 seen in the Carina Nebula. The data reveal a hitherto unnoticed association of 108 O-B2 stars around the O5If+ star LSS 2063 (l = 289.degrees 77, b = -1.degrees 22). Treating the OB star scaleheight as a constant within the thin disc, we find an orderly mean relation between extinction (A0) and distance in the Galactic longitude range, 287.degrees 6 < l < 293.degrees 5, and infer the subtle onset of thin-disc warping. A halo around NGC 3603, roughly a degree in diameter, of similar to 500 O-B2 stars with 4 < A(0)(mag) < 7 is noted. C1 [Mohr-Smith, M.; Drew, J. E.; Napiwotzki, R.; Wright, N. J.; Barentsen, G.; Farnhill, H. J.; Monguio, M.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Simon-Diaz, S.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Simon-Diaz, S.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain. [Wright, N. J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Barentsen, G.] NASA, Ames Res Ctr, Moffatt Field, Mountain View, CA 94043 USA. [Eisloeffel, J.] Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany. [Greimel, R.] NAWI Graz, Inst Phys Astrophys & Meteorol, Dept Geophys, Univ Pl 5, A-8010 Graz, Austria. [Kalari, V.] Univ Chile, Dept Astron, Camino El Observ 1515,Casilla 36-D, Santiago, Chile. [Parker, Q. A.] Univ Hong Kong, Dept Phys, Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China. [Vink, J. S.] Armagh Observ, Coll Hill, Armagh BT61 9DG, North Ireland. RP Drew, JE (reprint author), Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. EM j.drew@herts.ac.uk FU ESO Telescopes at the La Silla Paranal Observatory [177.D-3023]; National Aeronautics and Space Administration; National Science Foundation; NASA; Science and Technology Facilities Council (STFC) of the United Kingdom [ST/K502029/1]; STFC [ST/J001333/1, ST/M001008/1]; Spanish Ministry of Economy and Competitiveness (MINECO) [AYA2010-21697-C05-04, AYA2012-39364-C02-01, Severo Ochoa SEV-2011-0187]; Royal Astronomical Society; STFC Ernest Rutherford Fellowship [ST/M005569/1] FX This paper is based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 177.D-3023, as part of the VPHAS+ (http://www.vphas.eu). All VPHAS+ data are processed by the CASU at the Institute of Astronomy in Cambridge: we would particularly like to thank Eduardo Gonzalez-Solares and Mike Irwin for their efforts over the years. We also used data products from 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. We have also used data products from the wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by NASA. The AAT Service Observing Programme run by the Australian Astronomical Observatory is thanked for obtaining the Spectroscopy presented here. We thank the anonymous referee of this paper for their supportive remarks.; MM-S acknowledges a studentship funded by the Science and Technology Facilities Council (STFC) of the United Kingdom (ref. ST/K502029/1). JED, MM and GB acknowledge the support of research grants funded by the STFC (ref. ST/J001333/1 and ST/M001008/1). SS-D acknowledges funding by the Spanish Ministry of Economy and Competitiveness (MINECO) under the grants AYA2010-21697-C05-04, AYA2012-39364-C02-01 and Severo Ochoa SEV-2011-0187. NJW acknowledges the support of a Research Fellowship awarded by the Royal Astronomical Society (to 2015 September) and an STFC Ernest Rutherford Fellowship (from 2016 October, ref ST/M005569/1). NR 86 TC 0 Z9 0 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 FEB PY 2017 VL 465 IS 2 BP 1807 EP 1830 DI 10.1093/mnras/stw2751 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EK2VT UT WOS:000393785500038 ER PT J AU Marotzke, J Jakob, C Bony, S Dirmeyer, PA O'Gorman, PA Hawkins, E Perkins-Kirkpatrick, S Le Quere, C Nowicki, S Paulavets, K Seneviratne, SI Stevens, B Tuma, M AF Marotzke, Jochem Jakob, Christian Bony, Sandrine Dirmeyer, Paul A. O'Gorman, Paul A. Hawkins, Ed Perkins-Kirkpatrick, Sarah Le Quere, Corinne Nowicki, Sophie Paulavets, Katsia Seneviratne, Sonia I. Stevens, Bjorn Tuma, Matthias TI Climate research must sharpen its view SO NATURE CLIMATE CHANGE LA English DT Editorial Material ID CIRCULATION C1 [Marotzke, Jochem] Max Planck Inst Meteorol, Bundesstr 53, D-20146 Hamburg, Germany. [Jakob, Christian] Monash Univ, ARC Ctr Excellence Climate Syst Sci, Level 2,9 Rainforest Walk,Clayton Campus, Clayton, Vic 3800, Australia. [Bony, Sandrine] Sorbonne Univ, Lab Meteorol Dynam LMD IPSL, CNRS UPMC, Tour 45-55,3Eme Etage 4 Pl Jussieu,Boite 99, F-75252 Paris 05, France. [Dirmeyer, Paul A.] George Mason Univ, Dept Atmospher Ocean & Earth Sci, 4400 Univ Dr,Mail Stop 6C5, Fairfax, VA 22030 USA. [Dirmeyer, Paul A.] George Mason Univ, Ctr Ocean Land Atmosphere Studies, 4400 Univ Dr,Mail Stop 6C5, Fairfax, VA 22030 USA. [O'Gorman, Paul A.] MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave,Room 54-1712, Cambridge, MA 02139 USA. [Hawkins, Ed] Univ Reading, Dept Meteorol, Reading RG6 6BB, Berks, England. [Perkins-Kirkpatrick, Sarah] UNSW Australia, Climate Change Res Ctr, Sydney, NSW 2052, Australia. [Le Quere, Corinne] Univ East Anglia, Tyndall Ctr Climate Change Res, Norwich Res Pk, Norwich NR4 7TJ, Norfolk, England. [Nowicki, Sophie] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Mail Code 615, Greenbelt, MD 20771 USA. [Paulavets, Katsia] Int Council Sci ICSU, 5 Rue Auguste Vacquerie, F-75116 Paris, France. [Seneviratne, Sonia I.] ETH, Inst Atmospher & Climate Sci, CHN N11,Univ Str 16, CH-8092 Zurich, Switzerland. [Stevens, Bjorn] Max Planck Inst Meteorol, Bundesstr 53, D-20146 Hamburg, Germany. [Tuma, Matthias] WMO, 7Bis,Ave Paix,Case Postale 2300, CH-1211 Geneva 2, Switzerland. RP Marotzke, J (reprint author), Max Planck Inst Meteorol, Bundesstr 53, D-20146 Hamburg, Germany. EM jochem.marotzke@mpimet.mpg.de RI Jakob, Christian/A-1082-2010; OI Jakob, Christian/0000-0002-5012-3207; Perkins-Kirkpatrick, Sarah/0000-0001-9443-4915 NR 14 TC 0 Z9 0 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1758-678X EI 1758-6798 J9 NAT CLIM CHANGE JI Nat. Clim. Chang. PD FEB PY 2017 VL 7 IS 2 BP 89 EP 91 PG 3 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA EN9VU UT WOS:000396348500002 ER PT J AU Ballantyne, A Smith, W Anderegg, W Kauppi, P Sarmiento, J Tans, P Shevliakova, E Pan, YD Poulter, B Anav, A Friedlingstein, P Houghton, R Running, S AF Ballantyne, Ashley Smith, William Anderegg, William Kauppi, Pekka Sarmiento, Jorge Tans, Pieter Shevliakova, Elena Pan, Yude Poulter, Benjamin Anav, Alessandro Friedlingstein, Pierre Houghton, Richard Running, Steven TI Accelerating net terrestrial carbon uptake during the warming hiatus due to reduced respiration SO NATURE CLIMATE CHANGE LA English DT Article ID CLIMATE-CHANGE; SOIL RESPIRATION; TEMPERATURE SENSITIVITY; VEGETATION DYNAMICS; DIOXIDE UPTAKE; LAND; FOREST; MODEL; CO2; VARIABILITY AB The recent ` warming hiatus' presents an excellent opportunity to investigate climate sensitivity of carbon cycle processes. Here we combine satellite and atmospheric observations to show that the rate of net biome productivity (NBP) has significantly accelerated from 0.007 +/- 0.065 PgC yr(-2) over thewarming period (1982 to 1998) to 0.119 +/- 0.071 PgC yr(-2) over thewarming hiatus (1998-2012). This acceleration in NBP is not due to increased primary productivity, but rather reduced respiration that is correlated (r = 0.58; P = 0.0007) and sensitive (gamma = 4.05 to 9.40 PgC yr(-1) per degrees C) to land temperatures. Global land models do not fully capture this apparent reduced respiration over the warming hiatus; however, an empirical model including soil temperature and moisture observations better captures the reduced respiration. C1 [Ballantyne, Ashley; Running, Steven] Univ Montana, Dept Ecosyst & Conservat Sci, 32 Campus Dr, Missoula, MT 59801 USA. [Smith, William] Univ Arizona, Sch Nat Resources & Environm, 1064 East Lowell St, Tucson, AZ 85721 USA. [Anderegg, William] Univ Utah, Dept Biol, 257 South 1400 East,Room 201, Salt Lake City, UT 84112 USA. [Kauppi, Pekka] Univ Helsinki, Dept Environm Sci, POB 65 Viikinkaari 1, FIN-00014 Helsinki, Finland. [Sarmiento, Jorge] Princeton Univ, Dept Atmospher & Ocean Sci, 300 Forrestal Rd,Sayre Hall, Princeton, NJ 08544 USA. [Tans, Pieter] NOAA, ESRL, Global Monitoring Div, 325 Broadway R GMD, Boulder, CO 80305 USA. [Shevliakova, Elena] Geophys Fluids Dynam Lab, 201 Forrestal Rd, Princeton, NJ 08540 USA. [Pan, Yude] US Forest Serv, USDA, Newtown Sq, PA 19073 USA. [Poulter, Benjamin] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Anav, Alessandro; Friedlingstein, Pierre] Univ Exeter, Coll Engn Math & Phys Sci, North Pk Rd, Exeter EX4 4QF, Devon, England. [Houghton, Richard] Woods Hole Res Ctr, 149 Woods Hole Rd, Falmouth, MA 02540 USA. RP Ballantyne, A (reprint author), Univ Montana, Dept Ecosyst & Conservat Sci, 32 Campus Dr, Missoula, MT 59801 USA. EM ashley.ballantyne@umontana.edu FU Princeton University; Finnish Society of Sciences and Letters; NSF-DEB [1550932]; USDA [MONZ-1302]; NOAA global change fellowship; Luc Hoffman Fellowship; NASA [NNX08AG87A] FX This work was stimulated by a workshop on abrupt changes in the global carbon cycle sponsored by Princeton University and the The Finnish Society of Sciences and Letters. Further support for this research was provided by NSF-DEB no. 1550932 and USDA no. MONZ-1302. W.R.L.A. was supported by a NOAA global change fellowship and W.K.S. was supported by a Luc Hoffman Fellowship. Satellite observations and MOD-17 algorithm development were supported by NASA grant NNX08AG87A to S.W.R. We are also grateful to the global citizens and NOAA scientists who have helped maintain the global atmospheric CO2 observation network. This work was greatly improved through input from colleagues D. Lombardozzi and B. Sullivan. NR 80 TC 0 Z9 0 U1 4 U2 4 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1758-678X EI 1758-6798 J9 NAT CLIM CHANGE JI Nat. Clim. Chang. PD FEB PY 2017 VL 7 IS 2 BP 148 EP + DI 10.1038/NCLIMATE3204 PG 8 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA EN9VU UT WOS:000396348500019 ER PT J AU Arneth, A Sitch, S Pongratz, J Stocker, BD Ciais, P Poulter, B Bayer, AD Bondeau, A Calle, L Chini, LP Gasser, T Fader, M Friedlingstein, P Kato, E Li, W Lindeskog, M Nabel, JEMS Pugh, TAM Robertson, E Viovy, N Yue, C Zaehle, S AF Arneth, A. Sitch, S. Pongratz, J. Stocker, B. D. Ciais, P. Poulter, B. Bayer, A. D. Bondeau, A. Calle, L. Chini, L. P. Gasser, T. Fader, M. Friedlingstein, P. Kato, E. Li, W. Lindeskog, M. Nabel, J. E. M. S. Pugh, T. A. M. Robertson, E. Viovy, N. Yue, C. Zaehle, S. TI Historical carbon dioxide emissions caused by land-use changes are possibly larger than assumed SO NATURE GEOSCIENCE LA English DT Article ID CLIMATE-CHANGE; WOOD-HARVEST; FOREST MANAGEMENT; SECONDARY LANDS; ATMOSPHERIC CO2; USE TRANSITIONS; FUTURE CLIMATE; COVER CHANGE; FLUXES; AGRICULTURE AB The terrestrial biosphere absorbs about 20% of fossil-fuel CO2 emissions. The overall magnitude of this sink is constrained by the difference between emissions, the rate of increase in atmospheric CO2 concentrations, and the ocean sink. However, the land sink is actually composed of two largely counteracting fluxes that are poorly quantified: fluxes from land-use change and CO2 uptake by terrestrial ecosystems. Dynamic global vegetation model simulations suggest that CO2 emissions from land-use change have been substantially underestimated because processes such as tree harvesting and land clearing from shifting cultivation have not been considered. As the overall terrestrial sink is constrained, a larger net flux as a result of land-use change implies that terrestrial uptake of CO2 is also larger, and that terrestrial ecosystems might have greater potential to sequester carbon in the future. Consequently, reforestation projects and efforts to avoid further deforestation could represent important mitigation pathways, with co-benefits for biodiversity. It is unclear whether a larger land carbon sink can be reconciled with our current understanding of terrestrial carbon cycling. Our possible underestimation of the historical residual terrestrial carbon sink adds further uncertainty to our capacity to predict the future of terrestrial carbon uptake and losses. C1 [Arneth, A.; Bayer, A. D.; Pugh, T. A. M.] Karlsruhe Inst Technol, Deptartment Atmospher Environm Res, Kreuzeckbahnstr 19, D-82467 Garmisch Partenkirchen, Germany. [Sitch, S.] Univ Exeter, Coll Life & Environm Sci, Exeter EX4 4RJ, Devon, England. [Pongratz, J.; Nabel, J. E. M. S.] Max Planck Inst Meteorol, Bundesstr 53, D-20146 Hamburg, Germany. [Stocker, B. D.] Imperial Coll London, Dept Life Sci, Silwood Pk, Ascot SL5 7PY, Berks, England. [Stocker, B. D.] Imperial Coll London, Grantham Inst Climate Change, Silwood Pk, Ascot SL5 7PY, Berks, England. [Stocker, B. D.] Swiss Fed Inst Technol, Inst Atmospher & Climate Sci, Univ Str 16, CH-8092 Zurich, Switzerland. [Ciais, P.; Gasser, T.; Viovy, N.; Yue, C.] CEA CNRS UVSQ, Ctr Etud Orme Merisiers, IPSL LSCE, F-91191 Gif Sur Yvette, France. [Poulter, B.; Calle, L.] NASA Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Bondeau, A.] Avignon Univ, Inst Mediterraneen Biodivers & Ecol Marine & Cont, Aix Marseille Univ, CNRS,IRD, Technopole Arbois Mediterranee,Batiment Villemin, F-13545 Aix En Provence 04, France. [Chini, L. P.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Fader, M.] German Fed Inst Hydrol, Int Ctr Water Resources & Global Change, Mainzer Tor 1, D-56068 Koblenz, Germany. [Friedlingstein, P.] Univ Exeter, Coll Engn Math & Phys Sci, Exeter EX4 4QE, Devon, England. [Kato, E.] Inst Appl Energy, Minato Ku, Tokyo 1050003, Japan. [Lindeskog, M.] Lund Univ, Dept Phys Geog & Ecosyst Sci, Solvegatan 12, S-22362 Lund, Sweden. [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. [Robertson, E.] Hadley Ctr, Met Off, FitzRoy Rd, Exeter EX1 3PB, Devon, England. [Zaehle, S.] Max Planck Inst Biogeochem, Hans Knoll Str, D-07701 Jena, Germany. RP Arneth, A (reprint author), Karlsruhe Inst Technol, Deptartment Atmospher Environm Res, Kreuzeckbahnstr 19, D-82467 Garmisch Partenkirchen, Germany. EM Almut.arneth@kit.edu RI Pugh, Thomas/A-3790-2010 OI Pugh, Thomas/0000-0002-6242-7371 FU EU FP7 grants LUC4C [603542]; OPERAS [308393]; Helmholtz Association in its ATMO programme; LUC4C; German Research Foundation's Emmy Noether Programme [PO 1751/1-1]; Environment Research and Technology Development Fund (ERTDF) from the Ministry of the Environment, Japan [S-10]; Joint UK DECC/Defra Met Office Hadley Centre Climate Programme [GA01101]; European Research Council (ERC) under the European Union [647204]; Swiss National Science Foundation; ERC SyG project IMBALANCE-P: 'Effects of phosphorus limitations on Life, Earth system and Society' grant [610028]; FP7 through project EMBRACE [282672] FX A.A., A.D.B. and T.A.M.P. acknowledge support from EU FP7 grants LUC4C (grant no. 603542), OPERAS (grant no. 308393), and the Helmholtz Association in its ATMO programme and its impulse and networking fund. M.F., W.L., C.Y. and S.S. were also funded by LUC4C. J.P. and J.E. M.S.N. were supported by the German Research Foundation's Emmy Noether Programme (PO 1751/1-1). E.K. was supported by the Environment Research and Technology Development Fund (ERTDF) (S-10) from the Ministry of the Environment, Japan. E.R. was funded by LUC4C and by the Joint UK DECC/Defra Met Office Hadley Centre Climate Programme (GA01101). S.Z. has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement no. 647204; QUINCY). B.D.S. is supported by the Swiss National Science Foundation and FP7 funding through project EMBRACE (282672). P.C. received support from the ERC SyG project IMBALANCE-P: 'Effects of phosphorus limitations on Life, Earth system and Society' grant agreement no. 610028. This is paper number 24 of the Birmingham Institute of Forest Research. NR 69 TC 1 Z9 1 U1 6 U2 6 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 FEB PY 2017 VL 10 IS 2 BP 79 EP + DI 10.1038/NGEO2882 PG 8 WC Geosciences, Multidisciplinary SC Geology GA EK7RB UT WOS:000394121800008 ER PT J AU McColl, KA Alemohammad, SH Akbar, R Konings, AG Yueh, S Entekhabi, D AF McColl, Kaighin A. Alemohammad, Seyed Hamed Akbar, Ruzbeh Konings, Alexandra G. Yueh, Simon Entekhabi, Dara TI The global distribution and dynamics of surface soil moisture SO NATURE GEOSCIENCE LA English DT Article ID LAND; PRECIPITATION; VARIABILITY; SCALES; MEMORY; MODELS AB Surface soil moisture has a direct impact on food security, human health and ecosystem function. It also plays a key role in the climate system, and the development and persistence of extreme weather events such as droughts, floods and heatwaves. However, sparse and uneven observations have made it difficult to quantify the global distribution and dynamics of surface soil moisture. Here we introduce a metric of soil moisture memory and use a full year of global observations from NASA's Soil Moisture Active Passive mission to show that surface soil moisture-a storage believed to make up less than 0.001% of the global freshwater budget by volume, and equivalent to an, on average, 8-mm thin layer of water covering all land surfaces-plays a significant role in the water cycle. Specifically, we find that surface soil moisture retains a median 14% of precipitation falling on land after three days. Furthermore, the retained fraction of the surface soil moisture storage after three days is highest over arid regions, and in regions where drainage to groundwater storage is lowest. We conclude that lower groundwater storage in these regions is due not only to lower precipitation, but also to the complex partitioning of the water cycle by the surface soil moisture storage layer at the land surface. C1 [McColl, Kaighin A.; Alemohammad, Seyed Hamed; Akbar, Ruzbeh; Konings, Alexandra G.; Entekhabi, Dara] MIT, Dept Civil & Environm Engn, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [McColl, Kaighin A.] Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. [Konings, Alexandra G.] Stanford Univ, Dept Earth Syst Sci, Stanford, CA 94305 USA. [Yueh, Simon] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Entekhabi, Dara] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. RP Entekhabi, D (reprint author), MIT, Dept Civil & Environm Engn, 77 Massachusetts Ave, Cambridge, MA 02139 USA.; Entekhabi, D (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. EM darae@mit.edu OI Alemohammad, Seyed Hamed/0000-0001-5662-3643; Konings, Alexandra/0000-0002-2810-1722 FU National Science Foundation; Harvard University's Center for the Environment FX K.A.M. is funded by a National Science Foundation Graduate Research Fellowship and a Ziff Environmental Fellowship from Harvard University's Center for the Environment. The parts of this work performed by the Massachusetts Institute of Technology and by the Jet Propulsion Laboratory, California Institute of Technology were conducted under contracts with the National Aeronautics and Space Administration. The authors thank S. Seneviratne for comments on earlier drafts of the manuscript. NR 45 TC 0 Z9 0 U1 7 U2 7 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 FEB PY 2017 VL 10 IS 2 BP 100 EP + DI 10.1038/NGEO2868 PG 8 WC Geosciences, Multidisciplinary SC Geology GA EK7RB UT WOS:000394121800012 ER PT J AU Asoka, A Gleeson, T Wada, Y Mishra, V AF Asoka, Akarsh Gleeson, Tom Wada, Yoshihide Mishra, Vimal TI Relative contribution of monsoon precipitation and pumping to changes in groundwater storage in India SO NATURE GEOSCIENCE LA English DT Article ID SUMMER MONSOON; MULTIPLE-REGRESSION; DOMINANCE ANALYSIS; WATER; IRRIGATION; DEPLETION; PREDICTORS; RAINFALL; CLIMATE; CANALS AB The depletion of groundwater resources threatens food and water security in India. However, the relative influence of groundwater pumping and climate variability on groundwater availability and storage remains unclear. Here we show from analyses of satellite and local well data spanning the past decade that long-term changes in monsoon precipitation are driving groundwater storage variability in most parts of India either directly by changing recharge or indirectly by changing abstraction. We find that groundwater storage has declined in northern India at the rate of 2 cm yr(-1) and increased by 1 to 2 cm yr(-1) in southern India between 2002 and 2013. We find that a large fraction of the total variability in groundwater storage in north-central and southern India can be explained by changes in precipitation. Groundwater storage variability in northwestern India can be explained predominantly by variability in abstraction for irrigation, which is in turn influenced by changes in precipitation. Declining precipitation in northern India is linked to Indian Ocean warming, suggesting a previously unrecognized teleconnection between ocean temperatures and groundwater storage. C1 [Asoka, Akarsh; Mishra, Vimal] IIT, Civil Engn & Earth Sci, Gandhinagar 382355, India. [Gleeson, Tom] Univ Victoria, Dept Civil Engn, Victoria, BC V8P 5C2, Canada. [Gleeson, Tom] Univ Victoria, Sch Earth & Ocean Sci, Victoria, BC V8P 5C2, Canada. [Wada, Yoshihide] NASA Goddard Inst Space Studies, New York, NY 10025 USA. [Wada, Yoshihide] Columbia Univ, Ctr Climate Syst Res, New York, NY 10027 USA. [Wada, Yoshihide] Univ Utrecht, Dept Phys Geog, Domplein 29, NL-3512 JE Utrecht, Netherlands. [Wada, Yoshihide] Int Inst Appl Syst Anal, Schlosspl 1, A-2361 Laxenburg, Austria. RP Mishra, V (reprint author), IIT, Civil Engn & Earth Sci, Gandhinagar 382355, India. EM vmishra@iitgn.ac.in FU ITRA-Water project FX The authors acknowledge funding from the ITRA-Water project. Data availability from the Central Ground Water Board (CGWB), Gravity Recovery and Climate Experiment (GRACE), and India Meteorological Department (IMD) is greatly appreciated. NR 50 TC 1 Z9 1 U1 1 U2 1 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 FEB PY 2017 VL 10 IS 2 BP 109 EP + DI 10.1038/NGEO2869 PG 11 WC Geosciences, Multidisciplinary SC Geology GA EK7RB UT WOS:000394121800014 ER PT J AU Behrenfeld, MJ Hu, YX O'Malley, RT Boss, ES Hostetler, CA Siegel, DA Sarmiento, JL Schulien, J Hair, JW Lu, XM Rodier, S Scarino, AJ AF Behrenfeld, Michael J. Hu, Yongxiang O'Malley, Robert T. Boss, Emmanuel S. Hostetler, Chris A. Siegel, David A. Sarmiento, Jorge L. Schulien, Jennifer Hair, Johnathan W. Lu, Xiaomei Rodier, Sharon Scarino, Amy Jo TI Annual boom-bust cycles of polar phytoplankton biomass revealed by space-based lidar SO NATURE GEOSCIENCE LA English DT Article ID MARINE-PHYTOPLANKTON; OPTICAL-PROPERTIES; GLOBAL-SCALE; OCEAN; CHLOROPHYLL; SUBSURFACE; GROWTH; LIGHT; SEA; PLANKTON AB Polar plankton communities are among the most productive, seasonally dynamic and rapidly changing ecosystems in the global ocean. However, persistent cloud cover, periods of constant night and prevailing low solar elevations in polar regions severely limit traditional passive satellite ocean colour measurements and leave vast areas unobserved for many consecutive months each year. Consequently, our understanding of the annual cycles of polar plankton and their interannual variations is incomplete. Here we use space-borne lidar observations to overcome the limitations of historical passive sensors and report a decade of uninterrupted polar phytoplankton biomass cycles. We find that polar phytoplankton dynamics are categorized by 'boom-bust' cycles resulting from slight imbalances in plankton predator-prey equilibria. The observed seasonal-to-interannual variations in biomass are predicted by mathematically modelled rates of change in phytoplankton division. Furthermore, we find that changes in ice cover dominated variability in Antarctic phytoplankton stocks over the past decade, whereas ecological processes were the predominant drivers of change in the Arctic. We conclude that subtle and environmentally driven imbalances in polar food webs underlie annual phytoplankton boom-bust cycles, which vary interannually at each pole. C1 [Behrenfeld, Michael J.; O'Malley, Robert T.; Schulien, Jennifer] Oregon State Univ, Dept Bot & Plant Pathol, Cordley Hall 2082, Corvallis, OR 97331 USA. [Hu, Yongxiang; Hostetler, Chris A.; Hair, Johnathan W.; Lu, Xiaomei; Rodier, Sharon; Scarino, Amy Jo] NASA Langley Res Ctr, MS 420, Hampton, VA 23681 USA. [Boss, Emmanuel S.] Univ Maine, Sch Marine Sci, 5706 Aubert Hall, Orono, ME 04469 USA. [Siegel, David A.] Univ Calif Santa Barbara, Earth Res Inst, Santa Barbara, CA 93106 USA. [Siegel, David A.] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA. [Sarmiento, Jorge L.] Princeton Univ, Atmospher & Ocean Sci Program, 300 Forrestal Rd,Sayre Hall, Princeton, NJ 08544 USA. RP Behrenfeld, MJ (reprint author), Oregon State Univ, Dept Bot & Plant Pathol, Cordley Hall 2082, Corvallis, OR 97331 USA. EM mjb@science.oregonstate.edu RI Hu, Yongxiang/K-4426-2012 FU National Aeronautics and Space Administration's Ocean Biology and Biogeochemistry Program; North Atlantic Aerosol and Marine Ecosystems Study (NAAMES) FX This work was supported by the National Aeronautics and Space Administration's Ocean Biology and Biogeochemistry Program and the North Atlantic Aerosol and Marine Ecosystems Study (NAAMES). NR 41 TC 1 Z9 1 U1 4 U2 4 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 FEB PY 2017 VL 10 IS 2 BP 118 EP + DI 10.1038/NGEO2861 PG 7 WC Geosciences, Multidisciplinary SC Geology GA EK7RB UT WOS:000394121800015 ER PT J AU Lisse, CM Christian, DJ Wolk, SJ Gunther, HM Chen, CH Grady, CA AF Lisse, C. M. Christian, D. J. Wolk, S. J. Gunther, H. M. Chen, C. H. Grady, C. A. TI CHANDRA CHARACTERIZATION OF X-RAY EMISSION IN THE YOUNG F-STAR BINARY SYSTEM HD 113766 SO ASTRONOMICAL JOURNAL LA English DT Article DE astrochemistry; protoplanetary disks; planets and satellites: formation; techniques: spectroscopic; X-rays: stars ID CENTAURUS OB ASSOCIATION; VISUAL DOUBLE STARS; CLASS-I PROTOSTARS; DEBRIS DISKS; SCORPIUS-CENTAURUS; PHOTOMETRIC VARIABILITY; SOLAR NEIGHBORHOOD; PLANET FORMATION; STELLAR CORONAE; CHI-PERSEI AB Using Chandra, we have obtained imaging X-ray spectroscopy of the 10-16 Myr old F-star binary HD 113766. We individually resolve the 1(.)"4 separation binary components for the first time in the X-ray and find a total 0.3-2.0 keV luminosity of 2.2 x 10(29) erg s(-1), consistent with previous RASS estimates. We find emission from the easternmost, infrared-bright, dusty member HD 113766A to be only similar to 10% that of the western, infrared-faint member HD 113766B. There is no evidence for a 3rd late-type stellar or substellar member of HD 113766 with L-x > 6 x 10(25) erg s(-1) within 2' of the binary pair. The ratio of the two stars' X-ray luminosity is consistent with their assignments as F2V and F6V by Pecaut et al. The emission is soft for both stars, kT(Apec) = 0.30-0.50 keV, suggesting X-rays produced by stellar rotation and/or convection in young dynamos, but not accretion or outflow shocks, which we rule out. A possible 2.8 +/- 0.15 (2 sigma) hr modulation in the HD 113766B X-ray emission is seen, but at very low confidence and of unknown provenance. Stellar wind drag models corresponding to L-x similar to 2 x 10(29) erg s(-1) argue for a 1 mm dust particle lifetime around HD 113766B of only similar to 90,0000 years, suggesting that dust around HD 113766B is quickly removed, whereas 1 mm sized dust around HD 113766A can survive for > 1.5 x 10(6) years. At 10(28) -10(29) erg s(-1) X-ray luminosity, astrobiologically important effects, like dust warming and X-ray photolytic organic synthesis, are likely for any circumstellar material in the HD 113766 systems. C1 [Lisse, C. M.] Johns Hopkins Univ, Appl Phys Lab, Space Explorat Sect, Planetary Explorat Branch, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. [Christian, D. J.] Calif State Univ Northridge, Dept Phys & Astron, 18111 Nordhoff St, Northridge, CA 91330 USA. [Wolk, S. J.] Harvard Smithsonian Ctr Astrophys, Chandra Xray Ctr, 60 Garden St, Cambridge, MA 02138 USA. [Gunther, H. M.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave,NE83-569, Cambridge, MA 02139 USA. [Chen, C. H.] STScI, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Grady, C. A.] NASA, Eureka Sci & Goddard Space Flight Ctr, GSFC, Code 667, Greenbelt, MD 20771 USA. RP Lisse, CM (reprint author), Johns Hopkins Univ, Appl Phys Lab, Space Explorat Sect, Planetary Explorat Branch, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM carey.lisse@jhuapl.edu; damian.christian@csun.edu; swolk@cfa.harvard.edu; hgunther@mit.edu; cchen@stsci.edu; carol.a.grady@nasa.gov OI Wolk, Scott/0000-0002-0826-9261; Lisse, Carey/0000-0002-9548-1526; Christian, Damian/0000-0003-1746-3020 FU National Aeronautics and Space Administration through Chandra Award [GO1-12028X]; National Aeronautics Space Administration [NAS8-03060] FX The authors would like to thank J. Kastner, E. Mamajek, and J. Raymond for many useful discussions concerning X-ray emission from young stellar sources. C.M. Lisse gratefully acknowledges support for this work provided by the National Aeronautics and Space Administration through Chandra Award Number GO1-12028X issued by the Chandra X-ray Observatory Center (CXC). The CXC is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. NR 73 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD FEB PY 2017 VL 153 IS 2 AR 62 DI 10.3847/1538-3881/153/2/62 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EK2WU UT WOS:000393788400006 ER PT J AU Shvartzvald, Y Bryden, G Gould, A Henderson, CB Howell, SB Beichman, C AF Shvartzvald, Y. Bryden, G. Gould, A. Henderson, C. B. Howell, S. B. Beichman, C. TI UKIRT MICROLENSING SURVEYS AS A PATHFINDER FOR WFIRST: THE DETECTION OF FIVE HIGHLY EXTINGUISHED LOW-|b| EVENTS SO ASTRONOMICAL JOURNAL LA English DT Article DE Galaxy: bulge; gravitational lensing: micro ID GALACTIC BULGE; OPTICAL DEPTH; POPULATION; SEXTRACTOR; BINARY; SYSTEM; FIELD AB Optical microlensing surveys are restricted from detecting events near the Galactic plane and center, where the event rate is thought to be the highest due to the high optical extinction of these fields. In the near-infrared (NIR), however, the lower extinction leads to a corresponding increase in event detections and is a primary driver for the wavelength coverage of the WFIRST microlensing survey. During the 2015 and 2016 bulge observing seasons, we conducted NIR microlensing surveys with UKIRT in conjunction with and in support of the Spitzer and Kepler microlensing campaigns. Here, we report on five highly extinguished (A(H) = 0.81-1.97), low-Galactic latitude (-0.98 <= b <= -0.36) microlensing events discovered from our 2016 survey. Four of them were monitored with an hourly cadence by optical surveys but were not reported as discoveries, likely due to the high extinction. Our UKIRT surveys and suggested future NIR surveys enable the first measurement of the microlensing event rate in the NIR. This wavelength regime overlaps with the bandpass of the filter in which the WFIRST microlensing survey will conduct its highest-cadence observations, making this event rate derivation critically important for optimizing its yield. C1 [Shvartzvald, Y.; Bryden, G.; Henderson, C. B.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Gould, A.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Gould, A.] Korea Astron & Space Sci Inst, Daejon 305348, South Korea. [Gould, A.] Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. [Howell, S. B.] NASA, Kepler & Missions K2, Ames Res Ctr, POB 1,M-S 244-30, Moffett Field, CA 94035 USA. [Beichman, C.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. RP Shvartzvald, Y (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU NSF [AST-1516842]; NASA; ESO Telescopes at the La Silla Paranal Observatory [179.B-2002] FX Work by Y.S. and C.B.H. was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Universities Space Research Association through a contract with NASA. Work by A.G. was supported by NSF grant AST-1516842. The United Kingdom Infrared Telescope (UKIRT) is supported by NASA and operated under an agreement among the University of Hawaii, the University of Arizona, and Lockheed Martin Advanced Technology Center; operations are enabled through the cooperation of the Joint Astronomy Centre of the Science and Technology Facilities Council of the U.K. We acknowledge the support from NASA HQ for the UKIRT observations in connection with K2C9. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 179.B-2002. NR 27 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 FEB PY 2017 VL 153 IS 2 AR 61 DI 10.3847/1538-3881/153/2/61 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EK2WU UT WOS:000393788400005 ER PT J AU Diosady, LT Murman, SM AF Diosady, Laslo T. Murman, Scott M. TI Tensor-product preconditioners for higher-order space-time discontinuous Galerkin methods SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE Higher-order; Discontinuous Galerkin; Space-time; Compressible Navier-Stokes; Preconditioning ID NAVIER-STOKES EQUATIONS; FORMULATION; ALGORITHM; SYSTEMS AB A space-time discontinuous-Galerkin spectral-element discretization is presented for direct numerical simulation of the compressible Navier-Stokes equations. An efficient solution technique based on a matrix-free Newton-Krylov method is developed in order to overcome the stiffness associated with high solution order. The use of tensor-product basis functions is key to maintaining efficiency at high-order. Efficient preconditioning methods are presented which can take advantage of the tensor-product formulation. A diagonalized Alternating-Direction-Implicit (ADI) scheme is extended to the space-time discontinuous Galerkin discretization. A new preconditioner for the compressible Euler/Navier-Stokes equations based on the fast-diagonalization method is also presented. Numerical results demonstrate the effectiveness of these preconditioners for the direct numerical simulation of subsonic turbulent flows. (C) 2016 Elsevier Inc. All rights reserved. C1 [Diosady, Laslo T.] NASA, Ames Res Ctr, Sci & Technol Corp, Mountain View, CA 94035 USA. [Murman, Scott M.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. RP Diosady, LT (reprint author), NASA, Ames Res Ctr, Sci & Technol Corp, Mountain View, CA 94035 USA. EM laslo.diosady@nasa.gov; scott.murman@nasa.gov FU Revolutionary Computational Aerosciences sub-project within NASA's Aeronautics Sciences project FX This work was partially funded by the Revolutionary Computational Aerosciences sub-project within NASA's Aeronautics Sciences project. NR 25 TC 0 Z9 0 U1 1 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9991 EI 1090-2716 J9 J COMPUT PHYS JI J. Comput. Phys. PD FEB 1 PY 2017 VL 330 BP 296 EP 318 DI 10.1016/j.jcp.2016.11.022 PG 23 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA EL1VG UT WOS:000394408900017 ER PT J AU Ho, K deWeck, OL Hoffman, JA Shishko, R AF Ho, Koki deWeck, Olivier L. Hoffman, Jeffrey A. Shishko, Robert TI Dynamic modeling and optimization for space logistics using time-expanded networks (vol 105, pg 428, 2014) SO ACTA ASTRONAUTICA LA English DT Correction C1 [Ho, Koki; deWeck, Olivier L.; Hoffman, Jeffrey A.] MIT, Cambridge, MA 02139 USA. [Shishko, Robert] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Ho, K (reprint author), MIT, Cambridge, MA 02139 USA. EM koki_ho@mit.edu NR 1 TC 0 Z9 0 U1 1 U2 1 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 FEB PY 2017 VL 131 BP 226 EP 226 DI 10.1016/j.actaastro.2016.12.017 PG 1 WC Engineering, Aerospace SC Engineering GA EJ2CU UT WOS:000393018300025 ER PT J AU Chembo, YK Baumgartel, L Yu, N AF Chembo, Yanne K. Baumgartel, Lukas Yu, Nan TI Neutral Mounting of Ultrahigh Q Whispering Gallery Mode disc-Resonators for Metrological Applications SO IEEE PHOTONICS JOURNAL LA English DT Article DE Whispering gallery mode resonator; microwave photonic oscillators; time-frequency metrology ID FREQUENCY COMB GENERATION; BILLION QUALITY-FACTOR; OPTICAL CAVITY; STABILIZATION; OSCILLATOR; MICRORESONATORS; REFERENCES AB Whispering gallery mode resonators find key applications in microwave photonic oscillators for aerospace engineering, frequency synthesis, and time-frequency metrology. However, their elastic mechanical deformations induce undesirable shifts for their optical eigenfrequencies, which should ideally be immune to vibrations. We propose a mounting configuration that provides strong immunity against external vibrations and mechanical fluctuations. Numerical simulations confirm the analytical study. C1 [Chembo, Yanne K.] CNRS, Opt Dept, FEMTO ST Inst, F-25030 Besancon, France. [Chembo, Yanne K.] Univ Bourgogne Franche Comte, F-25030 Besancon, France. [Baumgartel, Lukas; Yu, Nan] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Chembo, YK (reprint author), CNRS, Opt Dept, FEMTO ST Inst, F-25030 Besancon, France.; Chembo, YK (reprint author), Univ Bourgogne Franche Comte, F-25030 Besancon, France. EM yanne.chembo@femto-st.fr FU Jet Propulsion Laboratory, California Institute of Technology; NASA FX This work was supported by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 40 TC 0 Z9 0 U1 5 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1943-0655 EI 1943-0647 J9 IEEE PHOTONICS J JI IEEE Photonics J. PD FEB PY 2017 VL 9 IS 1 AR 6800308 DI 10.1109/JPHOT.2016.2638041 PG 8 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA EK2NS UT WOS:000393764600001 ER PT J AU Kim, J Oh, H Kim, J Meyyappan, M Lee, JS AF Kim, Jungsik Oh, Hyeongwan Kim, Jiwon Meyyappan, M. Lee, Jeong-Soo TI Electrical characteristics of tunneling field-effect transistors with asymmetric channel thickness SO JAPANESE JOURNAL OF APPLIED PHYSICS LA English DT Article ID QUANTUM CONFINEMENT; PERFORMANCE; FET; MOBILITY; MOSFETS; IMPACT; TFETS AB Effects of using asymmetric channel thickness in tunneling field-effect transistors (TFET) are investigated in sub-50 nm channel regime using two-dimensional (2D) simulations. As the thickness of the source side becomes narrower in narrow-source wide-drain (NSWD) TFETs, the threshold voltage (V-th) and the subthreshold swing (SS) decrease due to enhanced gate controllability of the source side. The narrow source thickness can make the band-to-band tunneling (BTBT) distance shorter and induce much higher electric field near the source junction at the on-state condition. In contrast, in a TFET with wide-source narrow-drain (WSND), the SS shows almost constant values and the V-th slightly increases with narrowing thickness of the drain side. In addition, the ambipolar current can rapidly become larger with smaller thickness on the drain side because of the shorter BTBT distance and the higher electric-field at the drain junction. The on-current of the asymmetric channel TFET is lower than that of conventional TFETs due to the volume limitation of the NSWD TFET and high series resistance of the WSND TFET. The on-current is almost determined by the channel thickness of the source side. (C) 2017 The Japan Society of Applied Physics C1 [Kim, Jungsik; Lee, Jeong-Soo] Pohang Univ Sci & Technol POSETCH, Div IT Convergence Engn, Pohang 37673, Gyeongbuk, South Korea. [Oh, Hyeongwan; Kim, Jiwon; Lee, Jeong-Soo] Pohang Univ Sci & Technol POSETCH, Dept Elect Engn, Pohang 37673, Gyeongbuk, South Korea. [Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Kim, J (reprint author), Pohang Univ Sci & Technol POSETCH, Div IT Convergence Engn, Pohang 37673, Gyeongbuk, South Korea. FU National Research Foundation of Korea (NRF) grant - Korean government (MSIP) [2013R1A1A2007094]; agency for Defense Development [ADD-14-02-06-20]; POSTECH; Samsung Electronics; Samsung Display; Electronic Design Automation (EDA) tool program of IC Design Education Center (IDEC) in Republic of Korea FX This work was supported by the National Research Foundation of Korea (NRF) grant funded by the Korean government (MSIP) (No. 2013R1A1A2007094), and by the agency for Defense Development (ADD-14-02-06-20), and by Semiconductor Industry Collaborative Project between POSTECH and Samsung Electronics, and by Semiconductor Industry Collaborative Project between POSTECH and Samsung Display. TCAD Sentaurus simulation tool is supported by Electronic Design Automation (EDA) tool program of IC Design Education Center (IDEC) in Republic of Korea. NR 34 TC 0 Z9 0 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0021-4922 EI 1347-4065 J9 JPN J APPL PHYS JI Jpn. J. Appl. Phys. PD FEB PY 2017 VL 56 IS 2 AR 024201 DI 10.7567/JJAP.56.024201 PG 5 WC Physics, Applied SC Physics GA EK5IT UT WOS:000393960800001 ER PT J AU Ghods, M Lauer, M Grugel, RN Tewari, SN Poirier, DR AF Ghods, M. Lauer, M. Grugel, R. N. Tewari, S. N. Poirier, D. R. TI Convection and macrosegregation in Al-19Cu alloy directionally solidified through an abrupt contraction in cross-section: A comparison with Al-7Si SO JOURNAL OF CRYSTAL GROWTH LA English DT Article DE Computer simulation; Convection; Cross-section decrease; Directional solidification; Segregation; Aluminum alloys ID DENDRITIC SOLIDIFICATION; NATURAL-CONVECTION; METALLIC ALLOYS; BINARY-ALLOYS; SIMULATION; FLOW; CONSERVATION; SUPERALLOYS; INTERFACE; MODEL AB Hypoeutectic Al-19 wt. % Cu alloys were directionally solidified in cylindrical molds that featured an abrupt cross-section decrease 9.5 to 3.2 mm in diameter). Thermo-solutal convection and cross-section-change induced shrinkage flow effects on macrosegregation were investigated. Dendrite clustering and extensive radial macrosegregation was seen, particularly in the larger cross-section before contraction. This alloy shows positive longitudinal macrosegregation near the contraction followed by negative macrosegregation right after it; the extent of macrosegregation, however, decreases with increasing growth speed. The degree of thermo-solutal convection was compared to another study investigating directional solidification of Al-7 wt. % Si [1] in order to study the effect of solutal expansion coefficient on macrosegregation. An interesting change of the radial macrosegregation profile, attributable to the area-change-induced-shrinkage flow, was observed very close to the contraction. A two-dimensional model accounting for both shrinkage and thermo-solutal convection was used to simulate solidification, the resulting steepling as well as axial and radial macrosegregation. The experimentally observed macrosegregation associated with the contraction during directional solidification was well predicted by the numerical simulations. C1 [Ghods, M.; Tewari, S. N.] Cleveland State Univ, Chem & Biomed Engn Dept, Cleveland, OH 44114 USA. [Lauer, M.; Poirier, D. R.] Univ Arizona, Mat Sci & Engn Dept, Tucson, AZ 85721 USA. [Grugel, R. N.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35811 USA. [Lauer, M.] ME Elecmet 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-19% Cu and Al-7% Si alloys for this 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 33 TC 0 Z9 0 U1 1 U2 1 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 FEB 1 PY 2017 VL 459 BP 135 EP 145 DI 10.1016/j.jcrysgro.2016.11.111 PG 11 WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied SC Crystallography; Materials Science; Physics GA EJ1XT UT WOS:000393004600022 ER PT J AU Lim, H Kim, J Min, J Carvajal, NA Lloyd, CW Wang, YF AF Lim, Hyunjung Kim, JiEun Min, Jungwon Carvajal, Nubia A. Lloyd, Charles W. Wang, Youfa TI Child health promotion program in South Korea in collaboration with US National Aeronautics and Space Administration: Improvement in dietary and nutrition knowledge of young children (vol 10, pg 555, 2016) SO NUTRITION RESEARCH AND PRACTICE LA English DT Correction C1 [Lim, Hyunjung; Kim, JiEun] Kyung Hee Univ, Grad Sch East West Med Sci, Res Inst Med Nutr, Dept Med Nutr, Yongin 17104, South Korea. [Min, Jungwon; Wang, Youfa] Univ Buffalo State Univ New York, Dept Epidemiol & Environm Hlth, Syst Oriented Global Childhood Obes Intervent, 816 Kimball Tower, Buffalo, NY 14214 USA. [Min, Jungwon] Korea Inst Child Care & Educ, Seoul 06750, South Korea. [Carvajal, Nubia A.] NASA Informat Technol & Multimedia Serv Contract, MEI Technol, Houston, TX 77058 USA. [Lloyd, Charles W.] NASA, Johnson Space Ctr, Human Res Program, Houston, TX 77058 USA. RP Lim, H (reprint author), Kyung Hee Univ, Grad Sch East West Med Sci, Res Inst Med Nutr, Dept Med Nutr, Yongin 17104, South Korea. NR 1 TC 0 Z9 0 U1 0 U2 0 PU KOREAN NUTRITION SOC PI SEOUL PA 804 KST CTR, 635-4 YEOGSAM-SONG KANGNAM-KU, SEOUL, 135-703, SOUTH KOREA SN 1976-1457 EI 2005-6168 J9 NUTR RES PRACT JI Nutr. Res. Pract. PD FEB PY 2017 VL 11 IS 1 BP 76 EP 76 DI 10.4162/nrp.2017.11.1.76 PG 1 WC Nutrition & Dietetics SC Nutrition & Dietetics GA EJ8AZ UT WOS:000393445900011 PM 28194269 ER PT J AU Langlois, A Johnson, CA Montpetit, B Royer, A Blukacz-Richards, EA Neave, E Dolant, C Roy, A Arhonditsis, G Kim, DK Kaluskar, S Brucker, L AF Langlois, A. Johnson, C. -A. Montpetit, B. Royer, A. Blukacz-Richards, E. A. Neave, E. Dolant, C. Roy, A. Arhonditsis, G. Kim, D. -K. Kaluskar, S. Brucker, L. TI Detection of rain-on-snow (ROS) events and ice layer formation using passive microwave radiometry: A context for Peary caribou habitat in the Canadian Arctic SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Rain-on-snow; Ice layers; Snow; Arctic; Passive microwave; Peary caribou ID QUEEN ELIZABETH ISLANDS; WATER EQUIVALENT; SVALBARD REINDEER; EMISSION MODEL; AMPLIFICATION; POPULATION; IMPACTS; TRENDS AB Over the past four decades, amplified warming in the Arctic has led to numerous consequences. Of particular relevance, negative anomalies of snow and sea ice cover, glacier retreat, and the extended melt of Greenland combined with increasing temperature at double the rate of the rest of the planet have been observed in the Arctic. Several studies have suggested that another response to the current arctic warming could be an increase in rain-on-snow (ROS) events followed by subsequent freezing and the creation of ice layers. We use recently developed detection algorithms of ROS and ice events using passive microwave retrieval approaches to examine the spatial and temporal trends in rain-on-snow and ice layer creation for 18 islands across the Canadian Arctic Archipelago (CAA) over the last two decades. Results show that both icing and ROS event occurrence tripled between the periods of 1979-1995 and 1996-2011, with very active years in winters 1993-1994,1998-1999 and 2002-2003. The areas with the most combined occurrences are the Boothia Peninsula and Axel Heiberg, Cornwallis, Banks and Victoria Islands. We then compare the rain-on-snow and icing events to Peary caribou estimates to test whether the algorithms can detect weather events associated with population declines. There has been an important reduction in population numbers of Peary caribou, the northernmost caribou population in Canada, over the last three generations. The major hypothesis for the decline is that severe weather events lead to more difficult winter grazing conditions. The comparison with the Peary caribou population estimates suggest that caribou numbers decrease with increased occurrence of ROS and icing events, where 3-4 ROS events and 12 icing events in one winter season are sufficient to have a negative impact on Peary caribou. Crown Copyright (C) 2016 Published by Elsevier Inc. All rights reserved. C1 [Langlois, A.; Montpetit, B.; Royer, A.; Dolant, C.; Roy, A.] Univ Sherbrooke, Ctr Applicat & Rech Teledetect, Sherbrooke, PQ J1K 2R1, Canada. [Langlois, A.; Royer, A.; Dolant, C.; Roy, A.] Univ Laval, Ctr Etud Nord, Quebec City, PQ G1K 7P4, Canada. [Johnson, C. -A.; Neave, E.] Environm & Climate Change Canada, Landscape Sci & Technol, Ottawa, ON, Canada. [Blukacz-Richards, E. A.] Environm & Climate Change Canada, Climate Res Div, Toronto, ON, Canada. [Arhonditsis, G.; Kim, D. -K.; Kaluskar, S.] Univ Toronto, Dept Phys & Environm Sci, Toronto, ON M5S 1A1, Canada. [Brucker, L.] NASA, Goddard Space Flight Ctr, Cryospher Lab, Code 615, Greenbelt, MD USA. RP Langlois, A (reprint author), Univ Sherbrooke, Ctr Applicat & Rech Teledetect CARTEL, Dept Geomat Appl, Sherbrooke, PQ J1K 2R1, Canada. EM a.langlois2@USherbrooke.ca RI Brucker, Ludovic/A-8029-2010; OI Brucker, Ludovic/0000-0001-7102-8084; Arhonditsis, George/0000-0001-5359-8737 NR 54 TC 0 Z9 0 U1 5 U2 5 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD FEB PY 2017 VL 189 BP 84 EP 95 DI 10.1016/j.rse.2016.11.006 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA EJ1YB UT WOS:000393005400007 ER PT J AU Lievens, H Martens, B Verhoest, NEC Hahn, S Reichle, RH Miralles, DG AF Lievens, H. Martens, B. Verhoest, N. E. C. Hahn, S. Reichle, R. H. Miralles, D. G. TI Assimilation of global radar backscatter and radiometer brightness temperature observations to improve soil moisture and land evaporation estimates SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE ASCAT backscatter; SMOS brightness temperature; Data assimilation; GLEAM; Soil moisture; Land evaporation ID L-BAND; PASSIVE MICROWAVE; SURFACE-ROUGHNESS; SMOS OBSERVATIONS; WESTERN DENMARK; BIAS CORRECTION; CARBON-DIOXIDE; TRANSFER MODEL; DATA SETS; AMSR-E AB Active radar backscatter (sigma degrees) observations from the Advanced Scatterometer (ASCAT) and passive radiometer brightness temperature (TB) observations from the Soil Moisture Ocean Salinity (SMOS) mission are assimilated either individually or jointly into the Global Land Evaporation Amsterdam Model (GLEAM) to improve its simulations of soil moisture and land evaporation. To enable sigma degrees and TB assimilation, GLEAM is coupled to the Water Cloud Model and the L -band Microwave Emission from the Biosphere (L-MEB) model. The innovations, i.e. differences between observations and simulations, are mapped onto the model soil moisture states through an Ensemble Kalman Filter. The validation of surface (0-10 cm) soil moisture simulations over the period 2010-2014 against in situ measurements from the International Soil Moisture Network (ISMN) shows that assimilating sigma degrees or TB alone improves the average correlation of seasonal anomalies (R-an) from 0.514 to 0.547 and 0.548, respectively. The joint assimilation further improves Ran to 0.559. Associated enhancements in daily evaporative flux simulations by GLEAM are validated based on measurements from 22 FLUXNET stations. Again, the singular assimilation improves R-an from 0.502 to 0.536 and 0.533, respectively for sigma degrees and TB, whereas the best performance is observed for the joint assimilation (R-an = 0.546). These results demonstrate the complementary value of assimilating radar backscatter observations together with brightness temperatures for improving estimates of hydrological variables, as their joint assimilation outperforms the assimilation of each observation type separately. (C) 2016 Elsevier Inc. All rights reserved. C1 [Lievens, H.; Martens, B.; Verhoest, N. E. C.; Miralles, D. G.] Univ Ghent, Lab Hydrol & Water Management, Ghent, Belgium. [Lievens, H.; Reichle, R. H.] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD USA. [Hahn, S.] Vienna Univ Technol, Dept Geodesy & Geoinformat, Vienna, Austria. [Miralles, D. G.] Vrije Univ Amsterdam, Dept Earth Sci, Amsterdam, Netherlands. RP Lievens, H (reprint author), Univ Ghent, Lab Hydrol & Water Management, Ghent, Belgium. EM Hans.Lievens@UGent.be RI Verhoest, Niko/C-9726-2010; Reichle, Rolf/E-1419-2012; OI Verhoest, Niko/0000-0003-4116-8881; Martens, Brecht/0000-0002-7368-7953 FU Belgian Science Policy (BELSPO) [SR/00/302]; ESA [IPL-POE-2015-723-LG-cb-LE]; Netherlands Organization for Scientific Research [863.14.004]; CDIAC; OzFlux office; ChinaFlux office; AsiaFlux office FX The study is performed in the framework of the HYDRAS+ project (SR/00/302) financed by the Belgian Science Policy (BELSPO), and the ESA 's Support To Science Element SMOS+ET II project (IPL-POE-2015-723-LG-cb-LE). Hans Lievens is a postdoctoral research fellow of the Research Foundation Flanders (FWO). Rolf H. Reichle was supported by funding for the SMAP Science Team. Diego G. Miralles acknowledges the financial support from The Netherlands Organization for Scientific Research through grant 863.14.004. The SMOS data were obtained from the "Centre Aval de Traitement des Donnees SMOS" (CATDS), operated for the "Centre National d'Etudes Spatiales" (CNES, France) by IFREMER (Brest, France). The authors would like to thank the principal investigators of the International Soil Moisture Network (ISMN). This work used eddy-covariance data acquired and shared by the FLUXNET community, including these networks: AmeriFlux, AfriFlux, AsiaFlux, CarboAfrica, CarboEuropeIP, CarboItaly, CarboMont, ChinaFlux, Fluxnet-Canada, Green Grass, ICOS, KoFlux, LBA, NECC, TERN OzFlux, TCOS-Siberia, and USCCC. The FLUXNET eddy-covariance data processing and harmonization was carried out by the ICOS Ecosystem Thematic Center, AmeriFlux Management Project and Fluxdata project of FLUXNET, with the support of CDIAC, and the OzFlux, ChinaFlux and AsiaFlux offices. GLEAM description and data can be found at www.gleam.eu. We thank the Associate Editor and reviewers for their valuable contribution to this paper. NR 118 TC 0 Z9 0 U1 12 U2 12 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD FEB PY 2017 VL 189 BP 194 EP 210 DI 10.1016/j.rse.2016.11.022 PG 17 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA EJ1YB UT WOS:000393005400015 ER PT J AU Lei, Y Siqueira, P Treuhaft, R AF Lei, Yang Siqueira, Paul Treuhaft, Robert TI A physical scattering model of repeat-pass InSAR correlation for vegetation SO WAVES IN RANDOM AND COMPLEX MEDIA LA English DT Article ID POLARIMETRIC SAR INTERFEROMETRY; SYNTHETIC-APERTURE RADAR; TEMPORAL DECORRELATION; L-BAND; CORRELATION MAGNITUDE; FOREST; QUANTIFICATION AB A physical scattering model of repeat-pass InSAR correlation over forested areas is derived by accounting for the changes in the dielectric properties and positions of the scatterers in the scene between overpasses. This derivation is based on the discrete representation of a sparse random medium (such as forest canopy) along with the solution to the Foldy-Lax multiple scattering equations. In addition to taking into account the random motion of scatterers, which has been investigated in previous work, the derived repeat-pass InSAR correlation model in this paper includes the effects of moisture-induced dielectric fluctuations. This is accomplished by incorporating a separate correlation profile that takes into account these fluctuations into the framework. Once constructed, the mathematical formulation of this scattering model is cast into a modified version of the Random Volume over Ground model such that it can separately take into account dielectric fluctuations in the ground and volume components. This model is then validated using a modified version of ESA's PolSARproSim simulation to show that similar results can be obtained from both the simulation and the theoretical model. C1 [Lei, Yang; Siqueira, Paul] Univ Massachusetts Amherst, Amherst, MA 01003 USA. [Treuhaft, Robert] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Siqueira, P (reprint author), Univ Massachusetts Amherst, Amherst, MA 01003 USA. EM siqueira@ecs.umass.edu FU NASA Headquarters under the NASA Earth and Space Science Fellowship (NESSF) Program; NASA [NNX12AO23G] FX This work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship (NESSF) Program and NASA grant number NNX12AO23G for supporting the DESDynI-R (now called NISAR) mission. NR 28 TC 0 Z9 0 U1 3 U2 3 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND SN 1745-5030 EI 1745-5049 J9 WAVE RANDOM COMPLEX JI Waves Random Complex Media PD FEB PY 2017 VL 27 IS 1 BP 129 EP 152 DI 10.1080/17455030.2016.1209594 PG 24 WC Physics, Multidisciplinary SC Physics GA EK4DA UT WOS:000393876100010 ER PT J AU Jeong, U Kim, J Lee, H Lee, YG AF Jeong, Ukkyo Kim, Jhoon Lee, Hahlim Lee, Yun Gon TI Assessing the effect of long-range pollutant transportation on air quality in Seoul using the conditional potential source contribution function method SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Long-range transport; PM10; SO2; CO; NO2; Potential source contribution function ID DATA ASSIMILATION; SOURCE REGIONS; ASIAN DUST; EAST-ASIA; SOURCE APPORTIONMENT; ATMOSPHERIC AEROSOL; PARTICULATE MATTER; UNITED-STATES; INTEX-B; CHINA AB It is important to estimate the effects of the long-range transport of atmospheric pollutants for efficient and effective strategies to control air quality. In this study, the contributions of trans-boundary transport to the mean concentrations of SO2, NO2, CO, and PK in Seoul, Korea from 2001 to 2014 were estimated based on the conditional potential source contribution function (CPSCF) method. Eastern China was found to be the major source of trans-boundary pollution in Seoul, but moderate sources were also located in northeastern China. The contribution of long-range transport from Japan was negligible. The spatial distributions of the potential source contribution function (PSCF) values of each pollutant showed reasonable consistency with their emission inventory and satellite products. The PSCF values of SO2 and PM10 from eastern China were higher than those of NO2 and CO. The mean concentrations of SO2, NO2, CO, and PM10 in Seoul for the period from 2001 to 2014 were 534, 37.0, and 619.1 ppb, and 57.4 4 mu g/m(3), respectively. The contributions of long-range transport to the mean concentrations of SO2, NO2, CO, and PM10 in Seoul were 0.74, 3.4, and 39.0 ppb, and 12.1 mu g/m(3), respectively, which are 14%, 9%, 6%, and 21% of the mean concentrations, respectively. The annual mean concentrations of SO2 and NO2 followed statistically significant increasing linear trends (0.5 and 1.6 ppb per decade, respectively), whereas the trends in the annual mean concentrations of CO and PM10 were statistically insignificant. The trends in the ratio of the increased concentrations associated with long-range transport to the annual mean concentrations of the pollutants were statistically insignificant. However, the results indicate that the trans-boundary transport of 502, NO2, CO, and Milio from eastern China consistently affected air quality in Seoul over the study period (2001-2014). Regionally, the effects of the long-range transport of pollutants from Beijing and Harbin-Changchun on air quality in Seoul have become more significant over this period. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Jeong, Ukkyo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Jeong, Ukkyo] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Kim, Jhoon] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Lee, Hahlim] Pukyong Natl Univ, Dept Spatial Informat Engn, Busan, South Korea. [Lee, Yun Gon] Chungnam Natl Univ, Res Inst Basic Sci, Daejeon, South Korea. RP Kim, J (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.; Kim, J (reprint author), Harvard Smithonian Ctr Astrophys, Cambridge, MA 02138 USA. EM jkim2@yonsei.ac.kr FU Korean Ministry of Environment as part of the Eco-Innovation Program of KEITI [ARQ201204015] FX This work was supported by the Korean Ministry of Environment as part of the Eco-Innovation Program of KEITI (ARQ201204015). The authors thank NOAA ARL for providing the HYSPLIT model backward trajectory data; NIER for providing SO2, NO2, CO, and PM10 data; NASA and ESA for providing OMI and MODIS data; and NCAR and NASA for providing MOPITT data. NR 84 TC 0 Z9 0 U1 9 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD FEB PY 2017 VL 150 BP 33 EP 44 DI 10.1016/j.atmosenv.2016.11.017 PG 12 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA EI8PU UT WOS:000392770700004 ER PT J AU Hsiao, TC Chen, WN Ye, WC Lin, NH Tsay, SC Lin, TH Lee, CT Chuang, MT Pantina, P Wang, SH AF Hsiao, Ta-Chih Chen, Wei-Nai Ye, Wei-Cheng Lin, Neng-Huei Tsay, Si-Chee Lin, Tang-Huang Lee, Chung-Te Chuang, Ming-Tung Pantina, Peter Wang, Sheng-Hsiang TI Aerosol optical properties at the Lulin Atmospheric Background Station in Taiwan and the influences of long-range transport of air pollutants SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Aerosol optical properties; Lulin Atmospheric Background Station; Long-range transport; Biomass burning ID BIOMASS-BURNING AEROSOLS; FILTER-BASED MEASUREMENTS; VISIBLE-LIGHT ABSORPTION; BOUNDARY-LAYER DYNAMICS; IN-SITU; SOUTHERN AFRICA; EAST-ASIA; RADIATIVE PROPERTIES; ANGSTROM EXPONENT; FREE TROPOSPHERE AB The Lulin Atmospheric Background Station (LABS, 23.47 degrees N 120.87 degrees E, 2862 m ASL) in Central Taiwan was constructed in 2006 and is the only high-altitude background station in the western Pacific region for studying the influence of continental outflow. In this study, extensive optical properties of aerosols, including the aerosol light scattering coefficient (sigma(s)) and light absorption coefficient (sigma(a)), were collected from 2013 to 2014. The intensive optical properties, including mass scattering efficiency (alpha(s)), mass absorption efficiency (alpha(a)), single scattering albedo (omega), scattering Angstrom exponent (angstrom), and backscattering fraction (b), were determined and investigated, and the distinct seasonal cycle was observed. The value of as began to increase in January and reached a maximum in April; the mean in spring was 5.89 m(2) g(-1) with a standard deviation (SD) of 4.54 m(2) g(-1) and a 4.48 m(2) g(-1) interquartile range (IQR: 2.95-7.43 m(2) g(-1)). The trend was similar in alpha(a), with a maximum in March and a monthly mean of 0.84 m(2) g(-1). The peak values of omega (Mean = 0.92, SD = 0.03, IQR: 0.90-0.93) and angstrom (Mean = 2.22, SD = 0.61, IQR: 2.12-2.47) occurred in autumn. These annual patterns of optical properties were associated with different long-range transport patterns of air pollutants such as biomass burning (BB) aerosol in spring and potential anthropogenic emissions in autumn. The optical measurements performed at LABS during spring in 2013 were compared with those simultaneously performed at the Doi Ang Kang Meteorology Station, Chiang Mai Province, Thailand (DAK, 19.93 degrees N, 99.05 degrees E, 1536 m a.s.l.), which is located in the Southeast Asia BB source region. Furthermore, the relationships among alpha(s), alpha(a), and b were used to characterize the potential aerosol types transported to LABS during different seasons, and the data were inspected according to the HYSPLIT 5-day backward trajectories, which differentiate between different regions of air mass origin. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Hsiao, Ta-Chih; Ye, Wei-Cheng; Lee, Chung-Te] Natl Cent Univ, Grad Inst Environm Engn, Taoyuan, Taiwan. [Chen, Wei-Nai] Acad Sinica, Res Ctr Environm Changes, Taipei, Taiwan. [Lin, Neng-Huei; Wang, Sheng-Hsiang] Natl Cent Univ, Dept Atmospher Sci, Taoyuan, Taiwan. [Tsay, Si-Chee; Pantina, Peter] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Lin, Tang-Huang] Natl Cent Univ, Ctr Space & Remote Sensing Res, Taoyuan, Taiwan. [Chuang, Ming-Tung] Natl Cent Univ, Grad Inst Energy Engn, Taoyuan, Taiwan. RP Hsiao, TC (reprint author), Natl Cent Univ, Grad Inst Environm Engn, Taoyuan, Taiwan. EM tchsiao@ncu.edu.tw OI Hsiao, Ta-Chih/0000-0003-4103-6272 FU National Science Council of Taiwan [NSC 102-2221-E-008-004-MY3]; Taiwan EPA [EPA-103-U1L1-02-101, EPA-102-FA11-03-A217] FX This work was supported by the National Science Council of Taiwan under grants No. NSC 102-2221-E-008-004-MY3 and by the Taiwan EPA under contracts No. EPA-103-U1L1-02-101 and EPA-102-FA11-03-A217. Deployment of 7-SEAS/BASELInE in Southeast Asia was supported by NASA Radiation Sciences Program, managed by Dr. Hal B. Maring. We also thank all assistants from the region and many graduate students involved in the site operations, data analyses, and technical support for making the 7-SEAS/BASELInE campaign a success. NR 83 TC 0 Z9 0 U1 4 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD FEB PY 2017 VL 150 BP 366 EP 378 DI 10.1016/j.atmosenv.2016.11.031 PG 13 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA EI8PU UT WOS:000392770700035 ER PT J AU Carroll, ML DiMiceli, CM Townshend, JRG Sohlberg, RA Elders, AI Devadiga, S Sayer, AM Levy, RC AF Carroll, M. L. DiMiceli, C. M. Townshend, J. R. G. Sohlberg, R. A. Elders, A. I. Devadiga, S. Sayer, A. M. Levy, R. C. TI Development of an operational land water mask for MODIS Collection 6, and influence on downstream data products SO INTERNATIONAL JOURNAL OF DIGITAL EARTH LA English DT Article DE Earth observation; image processing; land cover; remote sensing; water resources ID SPLIT-WINDOW ALGORITHM; SURFACE TEMPERATURE; AEROSOL; RESOLUTION AB Data from the Moderate Resolution Imaging Spectro-radiometer (MODIS) on-board the Earth Observing System Terra and Aqua satellites are processed using a land water mask to determine when an algorithm no longer needs to be run or when an algorithm needs to follow a different pathway. Entering the fourth reprocessing (Collection 6 (C6)) the MODIS team replaced the 1 km water mask with a 500 m water mask for improved representation of the continental surfaces. The new water mask represents more small water bodies for an overall increase in water surface from 1% to 2% of the continental surface. While this is still a small fraction of the overall global surface area the increase is more dramatic in certain areas such as the Arctic and Boreal regions where there are dramatic increases in water surface area in the new mask. MODIS products generated by the on-going C6 reprocessing using the new land water mask show significant impact in areas with high concentrations of change in the land water mask. Here differences between the Collection 5 (C5) and C6 water masks and the impact of these differences on the MOD04 aerosol product and the MOD11 land surface temperature product are shown. C1 [Carroll, M. L.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Carroll, M. L.; Devadiga, S.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [DiMiceli, C. M.; Townshend, J. R. G.; Sohlberg, R. A.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Elders, A. I.] George Mason Univ, Atmospher Ocean & Earth Sci, Fairfax, VA 22030 USA. [Devadiga, S.] NASA, Goddard Space Flight Ctr, Terr Informat Syst Lab, Greenbelt, MD USA. [Sayer, A. M.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Greenbelt, MD USA. [Sayer, A. M.; Levy, R. C.] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD USA. RP Carroll, ML (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.; Carroll, ML (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA. EM mark.carroll@nasa.gov RI Levy, Robert/M-7764-2013 OI Levy, Robert/0000-0002-8933-5303 FU National Aeronautics and Space Administration (NASA) Terrestrial Ecology program [NNX08AT97A]; NASA MEaSURES program [NNX13AJ35A]; NASA EOS [NNX14AJ33G] FX This work was funded in part by National Aeronautics and Space Administration (NASA) Terrestrial Ecology program Grant/Cooperative Agreement Number: #NNX08AT97A; NASA MEaSURES program Grant/Cooperative Agreement Number: #NNX13AJ35A; and NASA EOS Grant/Cooperative Agreement Number: #NNX14AJ33G. NR 16 TC 1 Z9 1 U1 1 U2 1 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND SN 1753-8947 EI 1753-8955 J9 INT J DIGIT EARTH JI Int. J. Digit. Earth PD FEB PY 2017 VL 10 IS 2 BP 207 EP 218 DI 10.1080/17538947.2016.1232756 PG 12 WC Geography, Physical; Remote Sensing SC Physical Geography; Remote Sensing GA EJ4JU UT WOS:000393183700005 ER PT J AU Mishchenko, MI Yurkin, MA AF Mishchenko, Michael I. Yurkin, Maxim A. TI On the concept of random orientation in far-field electromagnetic scattering by nonspherical particles SO OPTICS LETTERS LA English DT Article ID T-MATRIX; LIGHT-SCATTERING AB Although the model of randomly oriented nonspherical particles has been used in a great variety of applications of far-field electromagnetic scattering, it has never been defined in strict mathematical terms. In this Letter, we use the formalism of Euler rigid-body rotations to clarify the concept of statistically random particle orientations and derive its immediate corollaries in the form of the most general mathematical properties of the orientation-averaged extinction and scattering matrices. Our results serve to provide a rigorous mathematical foundation for numerous publications in which the notion of randomly oriented particles and its light-scattering implications have been considered intuitively obvious. (C) 2017 Optical Society of America C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. [Yurkin, Maxim A.] SB RAS, Voevodsky Inst Chem Kinet & Combust, Inst Skaya Str 3, Novosibirsk 630090, Russia. [Yurkin, Maxim A.] Novosibirsk State Univ, Pirogova 2, Novosibirsk 630090, Russia. RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM michael.i.mishchenko@nasa.gov RI Yurkin, Maxim/A-7583-2008 OI Yurkin, Maxim/0000-0002-3524-0093 FU National Aeronautics and Space Administration (NASA); Russian Science Foundation (RSF) [14-15-00155] FX National Aeronautics and Space Administration (NASA) (Remote Sensing Theory Program and ACE Project); Russian Science Foundation (RSF) (14-15-00155). NR 30 TC 0 Z9 0 U1 2 U2 2 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 EI 1539-4794 J9 OPT LETT JI Opt. Lett. PD FEB 1 PY 2017 VL 42 IS 3 BP 494 EP 497 DI 10.1364/OL.42.000494 PG 4 WC Optics SC Optics GA EJ6CZ UT WOS:000393307500032 PM 28146510 ER PT J AU Amavizca, E Bashan, Y Ryu, CM Farag, MA Bebout, BM de-Bashan, LE AF Amavizca, Edgar Bashan, Yoav Ryu, Choong-Min Farag, Mohamed A. Bebout, Brad M. de-Bashan, Luz E. TI Enhanced performance of the microalga Chlorella sorokiniana remotely induced by the plant growth-promoting bacteria Azospirillum brasilense and Bacillus pumilus SO SCIENTIFIC REPORTS LA English DT Article ID ROOT-SURFACE COLONIZATION; ALGINATE BEADS; SYSTEMIC RESISTANCE; POPULATION-SIZE; WHEAT ROOTS; WASTE-WATER; FATTY-ACIDS; GC-MS; VULGARIS; VOLATILES AB Remote effects (occurring without physical contact) of two plant growth-promoting bacteria (PGPB) Azospirillum brasilense Cd and Bacilus pumilus ES4 on growth of the green microalga Chlorella sorokiniana UTEX 2714 were studied. The two PGPB remotely enhanced the growth of the microalga, up to six-fold, and its cell volume by about three-fold. In addition to phenotypic changes, both bacteria remotely induced increases in the amounts of total lipids, total carbohydrates, and chlorophyll a in the cells of the microalga, indicating an alteration of the microalga's physiology. The two bacteria produced large amounts of volatile compounds, including CO2, and the known plant growth-promoting volatile 2,3-butanediol and acetoin. Several other volatiles having biological functions in other organisms, as well as numerous volatile compounds with undefined biological roles, were detected. Together, these bacteria-derived volatiles can positively affect growth and metabolic parameters in green microalgae without physical attachment of the bacteria to the microalgae. This is a new paradigm on how PGPB promote growth of microalgae which may serve to improve performance of Chlorella spp. for biotechnological applications. C1 [Amavizca, Edgar; Bashan, Yoav; de-Bashan, Luz E.] Northwestern Ctr Biol Res CIBNOR, Environm Microbiol Grp, Av IPN 195, La Paz 23096, Bcs, Mexico. [Bashan, Yoav; de-Bashan, Luz E.] Bashan Inst Sci, 1730 Post Oak Court, Auburn, AL 36830 USA. [Bashan, Yoav; de-Bashan, Luz E.] Auburn Univ, Dept Entomol & Plant Pathol, 301 Funchess Hall, Auburn, AL 36849 USA. [Ryu, Choong-Min] KRIBB, Mol Phytobacteriol Lab, Daejeon 305600, South Korea. [Farag, Mohamed A.] Cairo Univ, Dept Pharmacognosy, Fac Pharm, Cairo 11562, Egypt. [Bebout, Brad M.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. RP de-Bashan, LE (reprint author), Northwestern Ctr Biol Res CIBNOR, Environm Microbiol Grp, Av IPN 195, La Paz 23096, Bcs, Mexico.; de-Bashan, LE (reprint author), Bashan Inst Sci, 1730 Post Oak Court, Auburn, AL 36830 USA.; de-Bashan, LE (reprint author), Auburn Univ, Dept Entomol & Plant Pathol, 301 Funchess Hall, Auburn, AL 36849 USA. EM luz@bashanfoundation.org FU Consejo Nacional de Ciencia y Tecnologia of Mexico (CONACYT) [251102]; CONACYT [321403]; Bashan Foundation USA; Alexander von Humboldt Foundation, Germany; Next-Generation BioGreen 21 Program (SSAC grant) - RDA [PJ009524]; KRIBB Research Initiative Program of South Korea FX We thank Soohyun Lee of the Korean Research Institute of Bioscience and Biotechnology (KRIBB) in Daejeon, South Korea and Kyungseok Park of the Rural Development Administration (RDA) in Suwon, South Korea for ideas and technical support. At CIBNOR, we thank Manuel Moreno for technical assistance and Ira Fogel for editorial services. We thank Mike Kubo and Angela Detweiler, NASA Ames Research Center, for assistance with CO2 headspace concentration analysis. At Auburn University, we thank Esther Ngumbi for providing information related to VOCs. This study was supported by Consejo Nacional de Ciencia y Tecnologia of Mexico (CONACYT-Basic Science-2015, contract 251102) and time for writing by The Bashan Foundation, USA. E.A. was mainly supported by a graduate fellowship from CONACYT (321403) and small periodic grants from The Bashan Foundation USA. M.A.F. received financial support from the Alexander von Humboldt Foundation, Germany. This work was supported by the Next-Generation BioGreen 21 Program (SSAC grant PJ009524) funded by the RDA and the KRIBB Research Initiative Program of South Korea. This is a contribution 2017-18 of The Bashan Institute of Science, USA. NR 75 TC 0 Z9 0 U1 6 U2 6 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2045-2322 J9 SCI REP-UK JI Sci Rep PD FEB 1 PY 2017 VL 7 AR 41310 DI 10.1038/srep41310 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EJ6AH UT WOS:000393300200001 PM 28145473 ER PT J AU Schieber, J Bish, D Coleman, M Reed, M Hausrath, EM Cosgrove, J Gupta, S Minitti, ME Edgett, KS Malin, M AF Schieber, Juergen Bish, David Coleman, Max Reed, Mark Hausrath, Elisabeth M. Cosgrove, John Gupta, Sanjeev Minitti, Michelle E. Edgett, Kenneth S. Malin, Mike TI Encounters with an unearthly mudstone: Understanding the first mudstone found on Mars SO SEDIMENTOLOGY LA English DT Review DE Burial history; deposition; diagenesis; Mars; mudstone ID FORSTERITE DISSOLUTION RATES; GREEN RIVER FORMATION; GALE CRATER; CARBONATE CONCRETIONS; OLIVINE DISSOLUTION; GLASS DISSOLUTION; SEDIMENTARY-ROCKS; SHRINKAGE CRACKS; CLAY-MINERALS; RED BEDS AB The Sheepbed mudstone forms the base of the strata examined by the Curiosity rover in Gale Crater on Mars, and is the first bona fide mudstone known on another planet. From images and associated data, this contribution proposes a holistic interpretation of depositional regime, diagenesis and burial history. A lake basin probably received sediment pulses from alluvial fans. Bed cross-sections show millimetre to centimetre-scale layering due to distal pulses of fluvial sediment injections (fine-grained hyperpycnites), fall-out from river plumes, and some aeolian supply. Diagenetic features include mineralized synaeresis cracks and millimetre-scale nodules, as well as stratiform cementation. Clay minerals were initially considered due to insitu alteration, but bulk rock chemistry and mineralogy suggests that sediments were derived from variably weathered source rocks that probably contained pre-existing clay minerals. X-ray diffraction analyses show contrasting clay mineralogy in closely spaced samples, consistent with at least partial detrital supply of clay minerals. A significant (ca 30 wt%) amorphous component is consistent with little post-depositional alteration. Theoretical modelling of diagenetic reactions, as well as kinetic considerations, suggest that the bulk of diagenetic clay mineral formation occurred comparatively late in diagenesis. Diagenetic features (synaeresis cracks and nodules) were previously thought to reflect early diagenetic gas formation, but an alternative scenario of synaeresis crack formation via fabric collapse of flocculated clays appears more likely. The observed diagenetic features, such as solid nodules, hollow nodules, matrix cement and raised ridges' (synaeresis cracks) can be explained with progressive alteration of olivine/glass in conjunction with centrifugal and counter diffusion of reactive species. Anhydrite-filled fractures in the Sheepbed mudstone occurred late in diagenesis when fluid pressures built up to exceed lithostatic pressure. Generating fluid overpressure by burial to facilitate hydraulic fracturing suggests a burial depth of at least 1000m for the underlying strata that supplied these fluids. C1 [Schieber, Juergen; Bish, David] Indiana Univ, Dept Geol Sci, 1001 East 10th St, Bloomington, IN 47405 USA. [Coleman, Max] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Coleman, Max] NASA, Astrobiol Inst, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Reed, Mark] Univ Oregon, Dept Geol Sci, 1585 East 13th Ave, Eugene, OR 97403 USA. [Hausrath, Elisabeth M.] Univ Nevada, Dept Geosci, 4505 South Maryland Pkwy, Las Vegas, NV 89154 USA. [Cosgrove, John; Gupta, Sanjeev] Imperial Coll, Dept Earth Sci & Engn, London SW7 2AZ, England. [Minitti, Michelle E.] Planetary Sci Inst, 1700 East Ft Lowell Rd 106, Tucson, AZ 85719 USA. [Edgett, Kenneth S.; Malin, Mike] Malin Space Sci Syst, 5880 Pacific Ctr Blvd, San Diego, CA 92121 USA. RP Schieber, J (reprint author), Indiana Univ, Dept Geol Sci, 1001 East 10th St, Bloomington, IN 47405 USA. EM jschiebe@indiana.edu NR 137 TC 2 Z9 2 U1 4 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0037-0746 EI 1365-3091 J9 SEDIMENTOLOGY JI Sedimentology PD FEB PY 2017 VL 64 IS 2 BP 311 EP 358 DI 10.1111/sed.12318 PG 48 WC Geology SC Geology GA EK4ID UT WOS:000393889400001 ER PT J AU Herring, J VanDyke, MS Cummins, RG Melton, F AF Herring, Jamie VanDyke, Matthew S. Cummins, R. Glenn Melton, Forrest TI Communicating Local Climate Risks Online Through an Interactive Data Visualization SO ENVIRONMENTAL COMMUNICATION-A JOURNAL OF NATURE AND CULTURE LA English DT Article DE ClimateData; US; climate change; interactivity; data visualization; digital tools; attitudes ID PERCEPTIONS; EXPERIENCE; IMAGERY; MEDIA; US AB Literature suggests a need to develop climate communication tools that focus on the impacts of climate change at local scales to increase proximity and communicate the risks on a more personal level. However, the nature of raw climate projection data makes accessibility by the lay audience a challenge and necessitates the need for innovative technological approaches to its distribution. ClimateData.US was created as an interactive visualization tool based on downscaled climate projection data to increase proximity and render climate change as salient and personally relevant. This experiment evaluated whether interacting with ClimateData.US influenced participants' climate change attitudes and concern and whether this effect varied as a function of geographic proximity. Findings revealed strong effectsregardless of geographic proximityfor interacting with the website on participants' perceived reality of climate change, attitude certainty, and concern for climate change. C1 [Herring, Jamie] HabitatSeven, Ottawa, ON, Canada. [VanDyke, Matthew S.] Appalachian State Univ, Dept Commun, ASU Box 32039, Boone, NC 28608 USA. [Cummins, R. Glenn] Texas Tech Univ, Coll Media & Commun, Lubbock, TX 79409 USA. [Melton, Forrest] NASA, Ames Res Ctr, Cooperat Res Earth Sci & Technol, Moffett Field, CA 94035 USA. EM matthewvandyke.research@gmail.com OI VanDyke, Matthew/0000-0002-2905-3099 NR 47 TC 0 Z9 0 U1 6 U2 6 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 1752-4032 EI 1752-4040 J9 ENVIRON COMMUN JI Environ. Commun. PD FEB PY 2017 VL 11 IS 1 BP 90 EP 105 DI 10.1080/17524032.2016.1176946 PG 16 WC Communication; Environmental Studies SC Communication; Environmental Sciences & Ecology GA EI4UU UT WOS:000392489800006 ER PT J AU Xu, KM Wong, TK Dong, ST Chen, F Kato, SJ Taylor, PC AF Xu, Kuan-Man Wong, Takmeng Dong, Shengtao Chen, Feng Kato, Seiji Taylor, Patrick C. TI Cloud object analysis of CERES Aqua observations of tropical and subtropical cloud regimes: Evolution of cloud object size distributions during the Madden-Julian Oscillation SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Madden-Julian Oscillation; Cloud size distribution; Aqua observations; CERES; Cloud regimes ID 1998 EL-NINO; MULTIVARIATE MJO INDEX; STATISTICAL-ANALYSES; INTRASEASONAL VARIABILITY; SCALE CIRCULATION; DEEP CONVECTION; PART I; SATELLITE; METHODOLOGY; RAINFALL AB In this study, we analyze cloud object data from the Aqua satellite between July 2006 and June 2010 that are matched with the real-time multivariate Madden-Julian Oscillation (MJO) index to examine the impact of MJO evolution on the evolutions of the size distributions of cloud object types. These types include deep convective (DC), cirrostratus, shallow cumulus, stratocumulus and overcast-stratus. A cloud object is a contiguous region of the earth with a single dominant cloud-system type. It is found that the cloud object size distributions of some phases depart greatly from the 8-phase combined distribution at large cloud-object diameters. The large-size group of cloud objects contributes to most of the temporal variations during the MJO evolution. For deep convective and cirrostratus cloud objects, there is a monotonic increase in both the number and footprint of large objects from the depressed to mature phases, which is attributed to the development and maturing of deep convection and anvils. The largest increase in the mean diameter during the mature phases that lasts to the early dissipating phase is related to growth of anvil clouds and is accompanied by moderate decreases in small-size objects. For shallow cumulus, the large objects decrease in number at the mature phases, but increase in number for both sizes before the mature phase. The opposite is true for the large overcast-stratus objects. The temporal evolution of large stratocumulus objects is similar to that of deep convective and cirrostratus object types except for peaking slightly earlier. Published by Elsevier Ltd. C1 [Xu, Kuan-Man; Wong, Takmeng; Kato, Seiji; Taylor, Patrick C.] NASA, Langley Res Ctr, Climate Sci Branch, Stop 420, Hampton, VA 23681 USA. [Dong, Shengtao; Chen, Feng] Sci Syst & Applicat Inc, Hampton, VA USA. EM Kuan-Man.Xu@nasa.gov RI Xu, Kuan-Man/B-7557-2013 OI Xu, Kuan-Man/0000-0001-7851-2629 FU NASA Energy and Water cycle Study (NEWS); Interdisciplinary Study (IDS); Science of Terra program; Aqua program FX This work has been supported by NASA Energy and Water cycle Study (NEWS), Interdisciplinary Study (IDS) and Science of Terra and Aqua programs. NR 42 TC 0 Z9 0 U1 5 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD FEB PY 2017 VL 188 SI SI BP 148 EP 158 DI 10.1016/j.jqsrt.2016.06.008 PG 11 WC Optics; Spectroscopy SC Optics; Spectroscopy GA EI5WF UT WOS:000392566300017 ER PT J AU Yang, YK Marshak, A Han, M Palm, SP Harding, DJ AF Yang, Yuekui Marshak, Alexander Han, Mei Palm, Stephen P. Harding, David J. TI Snow grain size retrieval over the polar ice sheets with the Ice, Cloud, and land Elevation Satellite (ICESat) observations SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE ICESat; GLAS; Snow grain size; Greenland; Antarctica; Surface albedo ID MODIS; ALBEDO; REFLECTANCE; ANTARCTICA; ALGORITHM; GREENLAND; MISSION AB Snow grain size is an important parameter for cryosphere studies. As a proof of concept, this paper presents an approach to retrieve this parameter over Greenland, East and West Antarctica ice sheets from surface reflectances observed with the Geoscience Laser Altimeter System (GLAS) onboard the Ice, Cloud, and land Elevation Satellite (ICESat) at 1064 nm. Spaceborne lidar observations overcome many of the disadvantages in passive remote sensing, including difficulties in cloud screening and low sun angle limitations and hence tend to provide more accurate and stable retrievals. Results from the GLAS L2A campaign, which began on 25 September and lasted until 19 November, 2003, show that the mode of the grain size distribution over Greenland is the largest (similar to 300 mu m) among the three, West Antarctica is the second (similar to 220 mu m) and East Antarctica is the smallest (similar to 190 mu m). Snow grain sizes are larger over the coastal regions compared to inland the ice sheets. These results are consistent with previous studies. Applying the broadband snow surface albedo parameterization scheme developed by Garder and Sharp (2010) to the retrieved snow grain size, ice sheet surface albedo is also derived. In the future, more accurate retrievals can be achieved with multiple wavelengths lidar observations. Published by Elsevier Ltd. C1 [Yang, Yuekui] Univ Space Res Assoc, Columbia, MD 21046 USA. [Yang, Yuekui; Marshak, Alexander; Han, Mei; Palm, Stephen P.; Harding, David J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Han, Mei] Morgan State Univ, Baltimore, MD 21239 USA. [Palm, Stephen P.] Sci Syst & Applicat Inc, Lanham, MD USA. EM yuekui.yang@nasa.gov FU NASA ICESat-2 Science Definition Program [NNX15AE87G] FX This study is supported by the NASA ICESat-2 Science Definition Program under the Grant NNX15AE87G. The authors thank Dr. Alexander Kokhanovsky for helpful discussions. We also appreciate the helpful comments and suggestions from two anonymous reviewers. NR 25 TC 0 Z9 0 U1 6 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD FEB PY 2017 VL 188 SI SI BP 159 EP 164 DI 10.1016/j.jqsrt.2016.03.033 PG 6 WC Optics; Spectroscopy SC Optics; Spectroscopy GA EI5WF UT WOS:000392566300018 ER PT J AU Jin, ZH Sun, MG AF Jin, Zhonghai Sun, Moguo TI Errors in spectral fingerprints and their effects on climate fingerprinting accuracy in the solar spectrum SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Climate change fingerprinting; Spectral fingerprint; Radiative transfer ID INFRARED-SPECTRA; REFLECTANCE; MODELS AB Using the Earth's reflected solar spectrum for climate change fingerprinting is an emerging research area. The spectral fingerprinting approach directly retrieves the changes in climate variables from the mean spectral data averaged across large space and time scales. To investigate this fingerprinting concept, we use ten years of satellite data to simulate the monthly and annual mean reflected solar spectra and the associated spectral fingerprints for different regions over the ocean. The interannual variations in the spectral data are derived and attributed to the interannual variations in the relevant climate variables. The fingerprinting retrieved changes in climate variables are then compared with the actual underlying variable changes from the observational data to evaluate the fingerprinting retrieval accuracy. Two important errors related to the fingerprinting approach, the nonlinearity error and the averaging error in the mean fingerprints, and their impact on the retrieval accuracy, are investigated. It is found that the averaging error increases but the nonlinearity error decreases as the region size increases. The averaging error has minimal effect on the fingerprinting retrieval accuracy in small regions but has more of an impact in large regions. In comparison, the effect of nonlinearity error on the retrieval accuracy decreases as the region size increases. It is also found that the fingerprinting retrieval accuracy is more sensitive to the nonlinearity error than to the averaging error. In addition, we compare the fingerprinting accuracy between using the monthly mean data and the annual mean data. The results show that on average higher retrieval accuracy is achieved when the annual mean data are used for the fingerprinting retrieval. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Jin, Zhonghai] Anhui Inst Opt & Fine Mech, Lab Remote Sensing, Hefei 230031, Anhui, Peoples R China. [Sun, Moguo] Sci Syst & Applicat, 1 Enterprise PKWY,STE 200, Hampton, VA 23666 USA. [Jin, Zhonghai; Sun, Moguo] NASA, Climate Sci Branch, Langley Res Ctr, Hampton, VA 23681 USA. EM Zhonghai.jin@nasa.gov FU NASA [NNH14ZDA001N-ACSCS]; CLARREO project of NASA FX We thank the NASA CERES group for the SSF data, Dr. Sky Yang and Dr. Shuntai Zhou for the ozone data, and Rosemary Baize and Amber Richards for help in editing. This research is supported by the NASA Grant NNH14ZDA001N-ACSCS and the CLARREO project of NASA. NR 18 TC 0 Z9 0 U1 1 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD FEB PY 2017 VL 188 SI SI BP 165 EP 175 DI 10.1016/j.jqsrt.2016.06.029 PG 11 WC Optics; Spectroscopy SC Optics; Spectroscopy GA EI5WF UT WOS:000392566300019 ER PT J AU Zhang, TP Stackhouse, PW Gupta, SK Cox, SJ Mikovitz, JC AF Zhang, Taiping Stackhouse, Paul W., Jr. Gupta, Shashi K. Cox, Stephen J. Mikovitz, J. Colleen TI A generalized formulation for downscaling data based on Fourier Transform and inversion: Mathematical rationale and application to the Max-Planck-Institute aerosol climatology data SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Downscaling; Fourier transform; GEWEX SRB; Aerosol climatology ID BOUNDARY-CONDITIONS; BSRN MEASUREMENTS; VALIDATION AB Occasionally, a need arises to downscale a time series of data from a coarse temporal resolution to a finer one, a typical example being from monthly means to daily means. For this case, daily means derived as such are used as inputs of climatic or atmospheric models so that the model results may exhibit variance on the daily time scale and retain the monthly mean of the original data set without an abrupt change from the end of one month to the beginning of the next. Different methods have been developed which often need assumptions, free parameters and the solution of simultaneous equations. Here we derive a generalized formulation by means of Fourier transform and inversion so that it can be used to directly compute daily means from a series of an arbitrary number of monthly means. The formulation can be used to transform any coarse temporal resolution to a finer one. From the derived results, the original data can be recovered almost identically. As a real application, we use this method to derive the daily counterpart of the MAC-v1 aerosol climatology that provides monthly mean aerosol properties for 18 shortwave bands and 12 longwave bands for the years from 1860 to 2100. The derived daily means are to be used as inputs of the shortwave and longwave algorithms of the NASA GEWEX SRB project. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Zhang, Taiping; Gupta, Shashi K.; Cox, Stephen J.; Mikovitz, J. Colleen] NASA, SSAI, Langley Res Ctr, One Enterprise Pkwy,Suite 200, Hampton, VA 23666 USA. [Stackhouse, Paul W., Jr.] NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. EM Taiping.Zhang@NASA.gov FU NASA Earth Science Mission, Radiation Science Program; Earth Science Mission FX This work was funded under the NASA Earth Science Mission, Radiation Science Program, Dr. Hal Maring, program manager. Additional funding for data production and archival came from the Earth Science Mission, Dr. Jack Kaye. NR 8 TC 0 Z9 0 U1 1 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD FEB PY 2017 VL 188 SI SI BP 176 EP 180 DI 10.1016/j.jqsrt.2016.08.019 PG 5 WC Optics; Spectroscopy SC Optics; Spectroscopy GA EI5WF UT WOS:000392566300020 ER PT J AU Lin, B Min, QL AF Lin, Bing Min, Qilong TI Optimal frequency selection of multi-channel O-2-band different absorption barometric radar for air pressure measurements SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article ID 3-DIMENSIONAL DATA ASSIMILATION; VECTOR RADIATIVE-TRANSFER; MICROWAVE; SIMULATIONS; SYSTEM; MODEL AB Through theoretical analysis, optimal selection of frequencies for O-2 differential absorption radar systems on air pressure field measurements is achieved. The required differential absorption optical depth between a radar frequency pair is 0.5. With this required value and other considerations on water vapor absorption and the contamination of radio wave transmission, frequency pairs of present considered radar system are obtained. Significant impacts on general design of differential absorption remote sensing systems are expected from current results. (C) Published by Elsevier Ltd. C1 [Lin, Bing] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Min, Qilong] SUNY Albany, Atmospher Sci Res Ctr, Albany, NY 12222 USA. EM bing.lin@nasa.gov NR 11 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 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD FEB PY 2017 VL 188 SI SI BP 188 EP 191 DI 10.1016/j.jqsrt.2016.06.019 PG 4 WC Optics; Spectroscopy SC Optics; Spectroscopy GA EI5WF UT WOS:000392566300022 ER PT J AU Sun, WB Hu, YX Weimer, C Ayers, K Baize, RR Lee, T AF Sun, Wenbo Hu, Yongxiang Weimer, Carl Ayers, Kirk Baize, Rosemary R. Lee, Tsengdar TI A FDTD solution of scattering of laser beam with orbital angular momentum by dielectric particles: Far-field characteristics SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Electromagnetic beams; Orbital angular momentum; Scattering; Remote sensing ID TIME-DOMAIN SOLUTION; SCREW DISLOCATIONS; LIGHT-SCATTERING; WAVE-FRONTS; MODES AB Electromagnetic (EM) beams with orbital angular momentum (OAM) may have great potential applications in communication technology and in remote sensing of the Earth atmosphere system and outer planets. Study of their interaction with optical lenses and dielectric or metallic objects, or scattering of them by particles in the Earth-atmosphere system, is a necessary step to explore the advantage of the OAM EM beams. In this study, the 3-dimensional (3D) scattered-field (SF) finite-difference time domain (FDTD) technique with the convolutional perfectly matched layer (CPML) absorbing boundary conditions (ABC) is applied to calculate the scattering of the purely azimuthal (the radial mode number is assumed to be zero) Laguerre-Gaussian (IC) beams with the OAM by dielectric particles. We found that for OAM beam's interaction with dielectric particles, the forward-scattering peak in the conventional phase function (P11) disappears, and light scattering peak occurs at a scattering angle of similar to 15 degrees to 45 degrees. The disappearance of forward-scattering peak means that, in laser communications most of the particle-scattered noise cannot enter the receiver, thus the received light is optimally the original OAM-encoded signal. This feature of the OAM beam also implies that in lidar remote sensing of the atmospheric particulates, most of the multiple-scattering energy will be off lidar sensors, and this may result in an accurate profiling of particle layers in the atmosphere or in the oceans by lidar, or even in the ground when a ground penetration radar (GPR) with the OAM is applied. This far-field characteristics of the scattered OAM light also imply that the optical theorem, which is derived from plane parallel wave scattering case and relates the forward scattering amplitude to the total cross section of the scatterer, is invalid for the scattering of OAM beams by dielectric particles. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Sun, Wenbo; Ayers, Kirk] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Hu, Yongxiang; Baize, Rosemary R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Weimer, Carl] Ball Aerosp & Technol Corp, Boulder, CO 80301 USA. [Lee, Tsengdar] NASA Headquarters, Washington, DC 20546 USA. EM wenbo.sun-1@nasa.gov RI Hu, Yongxiang/K-4426-2012 FU NASA ESTO ACT project "Lidar Orbital Angular Momentum Sensor" FX This work is supported by NASA ESTO ACT project "Lidar Orbital Angular Momentum Sensor". NR 28 TC 1 Z9 1 U1 10 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD FEB PY 2017 VL 188 SI SI BP 200 EP 213 DI 10.1016/j.jqsrt.2016.02.006 PG 14 WC Optics; Spectroscopy SC Optics; Spectroscopy GA EI5WF UT WOS:000392566300024 ER PT J AU Romoser, AA Scully, RR Limero, TF De Vera, V Cheng, PF Hand, JJ James, JT Ryder, VE AF Romoser, Amelia A. Scully, Robert R. Limero, Thomas F. De Vera, Vanessa Cheng, Patti F. Hand, Jennifer J. James, John T. Ryder, Valerie E. TI Predicting Air Quality at First Ingress into Vehicles Visiting the International Space Station SO AEROSPACE MEDICINE AND HUMAN PERFORMANCE LA English DT Article DE confined spaces; offgas toxicity; air quality; risk determination AB INTRODUCTION: NASA regularly performs ground-based offgas tests (OGTs), which allow prediction of accumulated volatile pollutant concentrations at first entry on orbit, on whole modules and vehicles scheduled to connect to the International Space Station (ISS). These data guide crew safety operations and allow for estimation of ISS air revitalization systems impact from additional pollutant load. Since volatiles released from vehicle, module, and payload materials can affect crew health and performance, prediction of first ingress air quality is important. METHODS: To assess whether toxicological risk is typically over or underpredicted, OGT and first ingress samples from 10 vehicles and modules were compared. Samples were analyzed by gas chromatography and gas chromatography-mass spectrometry. The rate of pollutant accumulation was extrapolated over time. Ratios of analytical values and Spacecraft Maximum Allowable Concentrations were used to predict total toxicity values (T-values) at first entry. Results were also compared by compound. RESULTS: Frequently overpredicted was 2-butanone (9/10), whereas propanal (6/10) and ethanol (8/10) were typically underpredicted, but T-values were not substantially affected. Ingress sample collection delay (estimated by octafluoropropane introduced from ISS atmosphere) and T-value prediction accuracy correlated well (R-2 = 0.9008), highlighting the importance of immediate air sample collection and accounting for ISS air dilution. DISCUSSION: Importantly,T-value predictions were conservative 70% of the time. Results also suggest that T-values can be normalized to octafluoropropane levels to adjust for ISS air dilution at first ingress. Finally, OGT and ingress sampling has allowed small leaks in vehicle fluid systems to be recognized and addressed. C1 [Romoser, Amelia A.; Scully, Robert R.; Limero, Thomas F.; De Vera, Vanessa; Cheng, Patti F.; Hand, Jennifer J.] Wyle Sci Technol & Engn Grp, 2101 NASA Pkwy, Houston, TX 77058 USA. [James, John T.] Univ Space Res Assoc, Houston, TX USA. [Ryder, Valerie E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Romoser, AA (reprint author), Wyle Sci Technol & Engn Grp, 2101 NASA Pkwy, Houston, TX 77058 USA. EM amelia.a.romoser@nasa.gov NR 29 TC 0 Z9 0 U1 0 U2 0 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 2375-6314 EI 2375-6322 J9 AEROSP MED HUM PERF JI Aerosp. Med.Hum. Perform. PD FEB PY 2017 VL 88 IS 2 BP 104 EP 113 DI 10.3357/AMHP.4702.2017 PG 10 WC Biophysics; Public, Environmental & Occupational Health; Medicine, Research & Experimental SC Biophysics; Public, Environmental & Occupational Health; Research & Experimental Medicine GA EI1TZ UT WOS:000392262300005 PM 28095954 ER PT J AU Oliveira, DM AF Oliveira, D. M. TI Magnetohydrodynamic Shocks in the Interplanetary Space: a Theoretical Review SO BRAZILIAN JOURNAL OF PHYSICS LA English DT Review DE Space physics; Plasma physics; MHD discontinuities; Interplanetary shocks ID RANKINE-HUGONIOT PROBLEM; IMPACT ANGLE CONTROL; SOLAR-WIND; MAGNETIC-FIELD; SLOW SHOCKS; ROTATIONAL DISCONTINUITIES; BOW SHOCK; EVOLUTION; AU; GEOEFFECTIVENESS AB I discuss in this brief review some properties of magnetohydrodynamic (MHD) discontinuities in the interplanetary space. My emphasis is on a special case of MHD discontinuity, namely interplanetary (IP) shocks, and those that are found at 1 AU. I derive the Rankine-Hugoniot (RH) equations to evaluate plasma parameters in the downstream region (shocked plasma) in relation to the upstream region (unshocked plasma). These properties are used to classify IP shocks in terms of their geometry and their direction of propagation in relation to the Sun. The shock geometry is determined in terms of two angles: , the angle between the upstream magnetic field and the shock normal, and , the angle between the shock normal and the Sun-Earth line. Sources of IP shocks frequently found in the solar wind at Earth's orbit are presented. Then the RH equations are solved for two categories of IP shocks in a special case: perpendicular shocks, when is 90 (ay), and oblique shocks, when that angle is 45 (ay). Finally, I highlight the importance of knowing the shock geometry, mainly the impact angle , specially whether the shock is frontal or inclined, for space weather-related investigations. IP shocks are known to be more geoeffective if they strike the Earth's magnetosphere frontally, or with impact angle nearly null. These results have been reported both by modeling and experimental studies in the literature. C1 [Oliveira, D. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Oliveira, D. M.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA. RP Oliveira, DM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Oliveira, DM (reprint author), Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA. EM denny.m.deoliveira@nasa.gov RI Oliveira, Denny/B-9818-2015 OI Oliveira, Denny/0000-0003-2078-7229 FU National Science Foundation [AGS-1143895]; Air Force Office of Sponsored Research [FA-9550-120264]; National Aeronautics and Space Administration (NASA) [NNX13AK31G, NNG11PL02A] FX This work was supported by grant AGS-1143895 from the National Science Foundation, grant FA-9550-120264 from the Air Force Office of Sponsored Research, and grants NNX13AK31G and NNG11PL02A from the National Aeronautics and Space Administration (NASA). I thank the Wind and ACE teams for the solar wind data and CDAWeb interface for data availability. I also thank the SOHO/LASCO team for the coronagraph image used in this review. The LASCO data can be downloaded from the website http://lasco-www.nrl.navy.mil. Finally, I would like to thank an anonymous reviewer for carefully evaluating this paper. NR 74 TC 0 Z9 1 U1 2 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0103-9733 EI 1678-4448 J9 BRAZ J PHYS JI Braz. J. Phys. PD FEB PY 2017 VL 47 IS 1 BP 81 EP 95 DI 10.1007/s13538-016-0472-x PG 15 WC Physics, Multidisciplinary SC Physics GA EI1HJ UT WOS:000392227400011 ER PT J AU Kelbe, D van Aardt, J Romanczyk, P van Leeuwen, M Cawse-Nicholson, K AF Kelbe, David van Aardt, Jan Romanczyk, Paul van Leeuwen, Martin Cawse-Nicholson, Kerry TI Multiview Marker-Free Registration of Forest Terrestrial Laser Scanner Data With Embedded Confidence Metrics SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Forestry; image registration; laser radar ID RANGE-IMAGE REGISTRATION; AUTOMATIC REGISTRATION; POINT-CLOUDS; LIDAR; INVENTORY; SURFACES; SCENES; TREES; ATTRIBUTES; MODELS AB Terrestrial laser scanning has demonstrated increasing potential for rapid comprehensive measurement of forest structure, especially when multiple scans are spatially registered in order to reduce the limitations of occlusion. Although marker-based registration techniques (based on retroreflective spherical targets) are commonly used in practice, a blind marker-free approach is preferable, insofar as it supports rapid operational data acquisition. To support these efforts, we extend the pairwise registration approach of our earlier work, and develop a graph-theoretical framework to perform blind marker-free global registration of multiple point cloud data sets. Pairwise pose estimates are weighted based on their estimated error, in order to overcome pose conflict while exploiting redundant information and improving precision. The proposed approach was tested for eight diverse New England forest sites, with 25 scans collected at each site. Quantitative assessment was provided via a novel embedded confidence metric, with a mean estimated root-mean-square error of 7.2 cm and 89% of scans connected to the reference node. This paper assesses the validity of the embedded multiview registration confidence metric and evaluates the performance of the proposed registration algorithm. C1 [Kelbe, David; van Aardt, Jan; Romanczyk, Paul; van Leeuwen, Martin; Cawse-Nicholson, Kerry] Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. [Kelbe, David] Oak Ridge Natl Lab, Oak Ridge, TN 37831 USA. [Romanczyk, Paul] Aerosp Corp, El Segundo, CA 90009 USA. [van Leeuwen, Martin] UCL, London WC1E 6BT, England. [Cawse-Nicholson, Kerry] Jet Prop Lab, Pasadena, CA 91109 USA. RP Kelbe, D (reprint author), Oak Ridge Natl Lab, Oak Ridge, TN 37831 USA. EM dave.kelbe@gmail.com FU National Science Foundation [DGE-1102937]; National Aeronautics and Space Administration [NNX12AQ24G]; Chester F. Carlson Center for Imaging Science at the Rochester Institute of Technology FX This work was supported in part by the National Science Foundation Graduate Research Fellowship under Grant DGE-1102937, in part by the National Aeronautics and Space Administration under Grant NNX12AQ24G, and in part by the Chester F. Carlson Center for Imaging Science at the Rochester Institute of Technology. (Corresponding author: David Kelbe.) NR 56 TC 0 Z9 0 U1 14 U2 14 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 FEB PY 2017 VL 55 IS 2 BP 729 EP 741 DI 10.1109/TGRS.2016.2614251 PG 13 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA EI3LI UT WOS:000392391800009 ER PT J AU Fattahi, H Agram, P Simons, M AF Fattahi, Heresh Agram, Piyush Simons, Mark TI A Network-Based Enhanced Spectral Diversity Approach for TOPS Time-Series Analysis SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Coregistration; interferometric synthetic aperture radar (InSAR); spectral diversity; terrain observation by progressive scan (TOPS) ID ILLAPEL EARTHQUAKE CHILE; SYNTHETIC APERTURE RADAR; TERRASAR-X; SENTINEL-1 MISSION; M(W)8.3 ILLAPEL; SAR SYSTEMS; WIDE-BAND; INTERFEROMETRY; INTERFEROGRAMS; REGISTRATION AB For multitemporal analysis of synthetic aperture radar (SAR) images acquired with a terrain observation by progressive scan (TOPS) mode, all acquisitions from a given satellite track must be coregistered to a reference coordinate system with accuracies better than 0.001 of a pixel (assuming full SAR resolution) in the azimuth direction. Such a high accuracy can be achieved through geometric coregistration, using precise satellite orbits and a digital elevation model, followed by a refinement step using a time-series analysis of coregistration errors. These errors represent the misregistration between all TOPS acquisitions relative to the reference coordinate system. We develop a workflow to estimate the time series of azimuth misregistration using a network-based enhanced spectral diversity (NESD) approach, in order to reduce the impact of temporal decorrelation on coregistration. Example time series of misregistration inferred for five tracks of Sentinel-1 TOPS acquisitions indicates a maximum relative azimuth misregistration of less than 0.01 of the full azimuth resolution between the TOPS acquisitions in the studied areas. Standard deviation of the estimated misregistration time series for different stacks varies from 1.1e-3 to 2e-3 of the azimuth resolution, equivalent to 1.6-2.8 cm orbital uncertainty in the azimuth direction. These values fall within the 1-sigma orbital uncertainty of the Sentinel-1 orbits and imply that orbital uncertainty is most likely the main source of the constant azimuth misregistration between different TOPS acquisitions. We propagate the uncertainty of individual misregistration estimated with ESD to the misregistration time series estimated with NESD and investigate the different challenges for operationalizing NESD. C1 [Fattahi, Heresh; Simons, Mark] CALTECH, Pasadena, CA 91125 USA. [Agram, Piyush] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Fattahi, H (reprint author), CALTECH, Pasadena, CA 91125 USA. EM hfattahi@gps.caltech.edu FU National Aeronautics and Space Administration [NNX16AK58G] FX The work of M. Simons was supported by the National Aeronautics and Space Administration under Grant NNX16AK58G. NR 37 TC 1 Z9 1 U1 7 U2 7 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 FEB PY 2017 VL 55 IS 2 BP 777 EP 786 DI 10.1109/TGRS.2016.2614925 PG 10 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA EI3LI UT WOS:000392391800013 ER PT J AU Kroodsma, RA McKague, DS Ruf, CS AF Kroodsma, Rachael A. McKague, Darren S. Ruf, Christopher S. TI Vicarious Cold Calibration for Conical Scanning Microwave Imagers SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE AMSR2; calibration; intercalibration; Microwave radiometry; TMI ID RADIOMETERS AB Vicarious cold calibration (VCC) for spaceborne microwave radiometers is analyzed and modified for application to conical scanning microwave imagers at frequencies from 6 to 90 GHz. The details of the algorithm are modified to account for additional frequencies and polarizations that were not included in the development of the original algorithm. The modified algorithm is shown to produce a more stable cold reference brightness temperature (TB) than the original algorithm. An analysis is performed of this updated algorithm to show the global regions that contribute to the derivation of the cold reference TB and to show which geophysical parameters contribute to the coldest TBs. The analysis suggests that water vapor variability has the largest impact on the TBs in the VCC algorithm. The modified VCC algorithm is applied to microwave imager data and is used as an intercalibration method. It is shown to agree well with other intercalibration methods, demonstrating that it is a valid and accurate method for calibration of microwave imagers. C1 [Kroodsma, Rachael A.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. [Kroodsma, Rachael A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McKague, Darren S.; Ruf, Christopher S.] Univ Michigan, Ann Arbor, MI 48109 USA. RP Kroodsma, RA (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. EM rachael.a.kroodsma@nasa.gov; dmckague@umich.edu; cruf@umich.edu NR 16 TC 1 Z9 1 U1 1 U2 1 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 FEB PY 2017 VL 55 IS 2 BP 816 EP 827 DI 10.1109/TGRS.2016.2615552 PG 12 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA EI3LI UT WOS:000392391800016 ER PT J AU Beauchamp, RM Tanelli, S Peral, E Chandrasekar, V AF Beauchamp, Robert M. Tanelli, Simone Peral, Eva Chandrasekar, V. TI Pulse Compression Waveform and Filter Optimization for Spaceborne Cloud and Precipitation Radar SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Meteorological radar; optimization; pulse compression methods; radar remote sensing; radar clutter; radar cross-sections; spaceborne radar ID SURFACE CLUTTER; CROSS-SECTIONS; SEA-SURFACE; BAND; DESIGN AB The optimal design of pulse compression waveform/filter pairs for use with near-nadir spaceborne radar in low earth orbit for the observation of clouds and precipitation is discussed. An optimization technique is introduced that considers performance metrics specific to the remote sensing of clouds and precipitation from such platforms. Specifically, the sensitivity of the radar to precipitation and clouds is maximized as close to the ground as required. The sensitivity of the radar near the surface is typically limited by the pulse compression range sidelobes from the surface's echo. Optimization of the waveform/filter pair's performance is facilitated by a time-domain radar scattering model to simulate radar reflectivity range profiles. The presented radar-scattering model accounts for the radar's configuration constraints and platform motion, as well as the spatial distribution and relative motion of the scatterers. In this paper, the optimization of both linear frequency modulation (LFM) and nonlinear frequency modulation (NLFM) waveforms is considered. It is demonstrated that the LFM waveforms provide superior performance over NLFM waveforms for application subject to unmitigated Doppler shifts. C1 [Beauchamp, Robert M.; Chandrasekar, V.] Colorado State Univ, Ft Collins, CO 80523 USA. [Tanelli, Simone; Peral, Eva] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Beauchamp, RM (reprint author), Colorado State Univ, Ft Collins, CO 80523 USA. FU ACE mission FX 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. The first author's participation was enabled by the Jet Propulsion Laboratory Summer Internship Program. Support from Dr. Hal Maring and the ACE mission concept study funding are gratefully acknowledged. NR 26 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 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD FEB PY 2017 VL 55 IS 2 BP 915 EP 931 DI 10.1109/TGRS.2016.2616898 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 EI3LI UT WOS:000392391800025 ER PT J AU Colle, BA Naeger, AR Molthan, A AF Colle, Brian A. Naeger, Aaron R. Molthan, Andrew TI Structure and Evolution of a Warm Frontal Precipitation Band during the GPM Cold Season Precipitation Experiment (GCPEx) SO MONTHLY WEATHER REVIEW LA English DT Article ID CONTINENTAL WINTER CYCLONES; COMMA HEAD REGION; NORTHEASTERN UNITED-STATES; MOIST SYMMETRIC STABILITY; MID-LATITUDE CYCLONES; MICROSCALE STRUCTURE; GENERATING CELLS; MICROPHYSICAL PROPERTIES; EXTRATROPICAL CYCLONES; MIDLATITUDE CYCLONES AB This paper describes the evolution of an intense precipitation band associated with a relatively weak warm front observed during the Global Precipitation Measurement (GPM) Mission Cold Season Precipitation Experiment (GCPEx) over southern Ontario, Canada, on 18 February 2012. The warm frontal precipitation band went through genesis, maturity, and decay over a 5-6-h period. The Weather Research and Forecasting (WRF) Model nested down to 1-km grid spacing was able to realistically predict the precipitation band evolution, albeit somewhat weaker and slightly farther south than observed. Band genesis began in an area of precipitation with embedded convection to the north of the warm front in a region of weak frontogenetical forcing at low levels and a weakly positive to slightly negative moist potential vorticity (MPV*) from 900 to 650 hPa. A midlevel dry intrusion helped reduce the midlevel stability, while the precipitation band intensified as the low-level frontogenesis intensified in a sloping layer with the warm front. Aggregates of unrimed snow occurred within the band during early maturity, while more supercooled water and graupel occurred as the upward motion increased because of the frontogenetical circulation. As the low-level cyclone moved east, the low-level deformation decreased and the column stabilized for vertical and slantwise ascent, and the warm frontal band weakened. A WRF experiment turning off latent heating resulted in limited precipitation band development and a weaker warm front, while turning off latent cooling only intensified the frontal precipitation band as additional midlevel instability compensated for the small decrease in frontogenetical forcing. C1 [Colle, Brian A.] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA. [Naeger, Aaron R.] Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35899 USA. [Molthan, Andrew] NASA, Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL USA. RP Colle, BA (reprint author), SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA. EM brian.colle@stonybrook.edu FU National Aeronautics and Space Administration [NNX13AF88G] FX This work was supported by National Aeronautics and Space Administration Grant NNX13AF88G. We appreciate the comments and suggestions made by the Editor (Dr. David Schultz) and three anonymous reviewers, who helped improve several aspects of this paper. NR 64 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 FEB PY 2017 VL 145 IS 2 BP 473 EP 493 DI 10.1175/MWR-D-16-0072.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EI3TS UT WOS:000392415000004 ER PT J AU Li, SB Villeneuve, DL Berninger, JP Blackwell, BR Cavallin, JE Hughes, MN Jensen, KM Jorgenson, Z Kahl, MD Schroeder, AL Stevens, KE Thomas, LM Weberg, MA Ankley, GT AF Li, Shibin Villeneuve, Daniel L. Berninger, Jason P. Blackwell, Brett R. Cavallin, Jenna E. Hughes, Megan N. Jensen, Kathleen M. Jorgenson, Zachary Kahl, Michael D. Schroeder, Anthony L. Stevens, Kyle E. Thomas, Linnea M. Weberg, Matthew A. Ankley, Gerald T. TI An integrated approach,for identifying priority contaminant in the Great Lakes Basin - Investigations in the Lower Green Bay/Fox River and Milwaukee Estuary areas of concern SO SCIENCE OF THE TOTAL ENVIRONMENT LA English DT Article DE Mixture; Screening; Chemical-biomolecule interactions; ToxCast (TM); Contaminants of emerging concern; Risk assessment ID MINNOW PIMEPHALES-PROMELAS; FATHEAD MINNOW; BIOANALYTICAL TOOLS; ORGANIC MICROPOLLUTANTS; STABLY EXPRESSES; TOXCAST PROGRAM; RECYCLED WATER; DRINKING-WATER; WASTE-WATER; CELL-LINE AB Environmental assessment of complex mixtures typically requires integration of chemical and biological measurements. This study demonstrates the use of a combination of instrumental chemical analyses, effects-based monitoring, and bio-effects prediction approaches to help identify potential hazards and priority contaminants in two Great Lakes Areas of Concern (AOCs), the Lower Green Bay/Fox River located near Green Bay, WI, USA and the Milwaukee Estuary, located near Milwaukee, WI, USA. Fathead minnows were caged at four sites within each AOC (eight sites total). Following 4 d of in situ exposure, tissues and biofluids were sampled and used for targeted biological effects analyses. Additionally, 4 d composite water samples were collected concurrently at each caged fish site and analyzed for 132 analytes as well as evaluated for total estrogenic and androgenic activity using cell-based bioassays. Of the analytes examined, 75 were detected in composite samples from at least one site. Based on multiple analyses, one site in the East River and another site near a paper mill discharge in the Lower Green Bay/Fox River AOC, were prioritized due to their estrogenic and androgenic activity, respectively. The water samples from other sites generally did not exhibit significant estrogenic or androgenic activity, nor was there evidence for endocrine disruption in the fish exposed at these sites as indicated by the lack of alterations in ex vivo steroid production, circulating steroid concentrations, or vitellogenin mRNA expression in males. Induction of hepatic cyp1a mRNA expression was detected at several sites, suggesting the presence of chemicals that activate the aryl hydrocarbon receptor. To expand the scope beyond targeted investigation of endpoints selected a priori, several bio-effects prediction approaches were employed to identify other potentially disturbed biological pathways and related chemical constituents that may warrant future monitoring at these sites. For example, several chemicals such as diethylphthalate and naphthalene, and genes and related pathways, such as cholinergic receptor muscarinic 3 (CHRM3), estrogen receptor alpha1 (esr1), chemokine ligand 10 protein (OCCL10), tumor protein p53 (p53), and monoamine oxidase B (Maob), were identified as candidates for future assessments at these AOCs. Overall, this study demonstrates that a better prioritization of contaminants and associated hazards can be achieved through integrated evaluation of multiple lines of evidence. Such prioritization can guide more comprehensive follow-up risk assessment efforts. (C) 2016 Elsevier B.V. All rights reserved. C1 [Li, Shibin; Villeneuve, Daniel L.; Berninger, Jason P.; Blackwell, Brett R.; Cavallin, Jenna E.; Hughes, Megan N.; Jensen, Kathleen M.; Kahl, Michael D.; Stevens, Kyle E.; Thomas, Linnea M.; Weberg, Matthew A.; Ankley, Gerald T.] US EPA, Natl Hlth & Environm Effects Res Lab, Mid Continent Ecol Div, 6201 Congdon Blvd, Duluth, MN 55804 USA. [Li, Shibin; Berninger, Jason P.] US EPA, Natl Res Council, 6201 Congdon Blvd, Duluth, MN 55804 USA. [Jorgenson, Zachary] US Fish & Wildlife Serv, Twin Cities Ecol Field Serv Field Off, 4101 Amer Blvd East, Bloomington, MN 55425 USA. [Schroeder, Anthony L.] Univ Minnesota Crookston, Math Sci & Technol Dept, 2900 Univ Ave, Crookston, MN 56716 USA. RP Li, SB (reprint author), US EPA, Natl Hlth & Environm Effects Res Lab, Mid Continent Ecol Div, 6201 Congdon Blvd, Duluth, MN 55804 USA. EM lishibin1116@gmail.com FU National Research Council Research Associateship Awards at the U.S. Environmental Protection Agency, Mid-Continent Ecology Division FX The present study was performed while two of the authors, Shibin Li and Jason P. Benninger, held National Research Council Research Associateship Awards at the U.S. Environmental Protection Agency, Mid-Continent Ecology Division. The authors also thank the following team members who have been critical in the implementation and success of the program that this study is a part of: Kathy lee (USGS), JoAnn Banda (USFWS), Steve Choy (USFWS), Dan Gefell (USFWS), and Jeremy Moore (USFWS). This document has been subjected to review by the National Health and Environmental Effects Research Laboratory and approved for publication. Approval does not signify that the contents reflect the views of the Agency nor does mention of trade names or commercial products constitute endorsement or recommendation for use. The findings and conclusions in this article are those of the authors and do not necessarily represent the views or policies of the corresponding agencies. NR 60 TC 0 Z9 0 U1 9 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0048-9697 EI 1879-1026 J9 SCI TOTAL ENVIRON JI Sci. Total Environ. PD FEB 1 PY 2017 VL 579 BP 825 EP 837 DI 10.1016/j.scitotenv.2016.11.021 PG 13 WC Environmental Sciences SC Environmental Sciences & Ecology GA EH6QA UT WOS:000391897800085 PM 27866739 ER PT J AU Kast, J Schuck, EL Deitchman, AN Putcha, L Derendorf, H AF Kast, J. Schuck, E. L. Deitchman, A. N. Putcha, L. Derendorf, H. TI ANTIBIOTICS IN SPACE: POTENTIAL IMPACT OF THE SPACEFLIGHT ENVIRONMENT ON CIPROFLOXACIN EFFICACY AGAINST E. COLI. SO CLINICAL PHARMACOLOGY & THERAPEUTICS LA English DT Meeting Abstract CT Annual Meeting of the American-Society-for-Clinical-Pharmacology-and-Therapeutics (ASCPT) CY MAR 15-18, 2017 CL Washington, DC SP Amer Soc Clin Pharmacol & Therapeut C1 [Kast, J.; Schuck, E. L.; Deitchman, A. N.; Derendorf, H.] Univ Florida, Gainesville, FL USA. [Putcha, L.] NASA Johnson Space Ctr, Houston, TX USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0009-9236 EI 1532-6535 J9 CLIN PHARMACOL THER JI Clin. Pharmacol. Ther. PD FEB PY 2017 VL 101 IS S1 MA PI-050 BP S33 EP S33 PG 1 WC Pharmacology & Pharmacy SC Pharmacology & Pharmacy GA EH7EM UT WOS:000391935700102 ER PT J AU Stevenazzi, S Bonfanti, M Masetti, M Nghiem, SV Sorichetta, A AF Stevenazzi, Stefania Bonfanti, Marianna Masetti, Marco Nghiem, Son V. Sorichetta, Alessandro TI A versatile method for groundwater vulnerability projections in future scenarios SO JOURNAL OF ENVIRONMENTAL MANAGEMENT LA English DT Article DE Groundwater vulnerability; Time dimension; Statistical method; Land use management ID CONTAMINATION; RISKS AB Water scarcity and associated risks are serious societal problems. A major challenge for the future will be to ensure the short-term and long-term provision of accessible and safe freshwater to meet the needs of the rapidly growing human population and changes in land cover and land use, where conservation and protection play a key role. Through a Bayesian spatial statistical method, a time-dependent approach for groundwater vulnerability assessment is developed to account for both the recent status of groundwater contamination and its evolution, as required by the European Union (Groundwater Directive, 2006/118/EC). This approach combines natural and anthropogenic factors to identify areas with a critical combination of high levels and increasing trends of nitrate concentrations, together with a quantitative evaluation of how different future scenarios would impact the quality of groundwater resources in a given area. In particular, the proposed approach can determine potential impacts on groundwater resources if policies are maintained at the status quo or if new measures are implemented for safeguarding groundwater quality, as natural factors are changing under climatic or anthropogenic stresses. (C) 2016 Elsevier B.V. All rights reserved. C1 [Stevenazzi, Stefania; Bonfanti, Marianna; Masetti, Marco] Univ Milan, Dipartimento Sci Terra A Desio, Via Luigi Mangiagalli 34, I-20133 Milan, Italy. [Nghiem, Son V.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 300-235, Pasadena, CA 91109 USA. [Sorichetta, Alessandro] Univ Southampton, Geog & Environm, Highfield Campus,Bldg 54, Southampton SO17 1BJ, Hants, England. [Sorichetta, Alessandro] Flowminder Fdn, Roslagsgatan 17, SE-11355 Stockholm, Sweden. RP Stevenazzi, S (reprint author), Univ Milan, Dipartimento Sci Terra A Desio, Via Luigi Mangiagalli 34, I-20133 Milan, Italy. EM stefania.stevenazzi@unimi.it RI Masetti, Marco/N-6823-2013 FU NASA Land-Cover and Land-Use Change (LCLUC) Program FX The research carried out at the Jet Propulsion Laboratory, California Institute of Technology, was supported by the NASA Land-Cover and Land-Use Change (LCLUC) Program. The research carried out at the Department of Geography and Environment, University of Southampton (UK), was done in the framework of the WorldPop Project (www.worldpop.org) and Flowminder Foundation (www.flowminder.org). NR 31 TC 0 Z9 0 U1 9 U2 9 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0301-4797 EI 1095-8630 J9 J ENVIRON MANAGE JI J. Environ. Manage. PD FEB 1 PY 2017 VL 187 BP 365 EP 374 DI 10.1016/j.jenvman.2016.10.057 PG 10 WC Environmental Sciences SC Environmental Sciences & Ecology GA EH8QN UT WOS:000392037500038 PM 27836560 ER PT J AU Nunez, PD ten Brummelaar, T Mennesson, B Scott, NJ AF Nunez, Paul D. ten Brummelaar, Theo Mennesson, Bertrand Scott, Nicholas J. TI Visibility Estimation for the CHARA/JouFLU Exozodi Survey SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE methods: data analysis; methods: statistical; techniques: high angular resolution; (stars:) circumstellar matter ID INFRARED INTERFEROMETRIC SURVEY; OPTICAL INTERFEROMETER; STELLAR INTERFEROMETER; CIRCUMSTELLAR MATERIAL; BEAM COMBINER; CHARA ARRAY; STARS; CHARA/FLUOR; VLTI; VEGA AB We discuss the estimation of the interferometric visibility (fringe contrast) for the Exozodi survey conducted at the CHARA array with the JouFLU beam combiner. We investigate the use of the statistical median to estimate the uncalibrated visibility from an ensemble of fringe exposures. Under a broad range of operating conditions, numerical simulations indicate that this estimator has a smaller bias compared with other estimators. We also propose an improved method for calibrating visibilities, which not only takes into account the time interval between observations of calibrators and science targets, but also the uncertainties of the calibrators' raw visibilities. We test our methods with data corresponding to stars that do not display the exozodi phenomenon. The results of our tests show that the proposed method yields smaller biases and errors. The relative reduction in bias and error is generally modest, but can be as high as similar to 20%-40% for the brightest stars of the CHARA data and statistically significant at the 95% confidence level (CL). C1 [Nunez, Paul D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [ten Brummelaar, Theo; Scott, Nicholas J.] Mt Wilson Observ, CHARA Array, Mt Wilson, CA 91023 USA. [Mennesson, Bertrand] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Scott, Nicholas J.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. RP Nunez, PD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM paul.nunez@jpl.nasa.gov OI Scott, Nicholas/0000-0003-1038-9702 FU NASA [NNN13D460T]; National Science Foundation [AST-1211929] FX This research was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory administered by Universities Space Research Association under contract with NASA. P.N. and B.M. are grateful for support from the NASA Exoplanet Research Program element, though grant number NNN13D460T. This work is based upon observations obtained with the Georgia State University Center for High Angular Resolution Astronomy Array at Mount Wilson Observatory. The CHARA Array is supported by the National Science Foundation under Grant No. AST-1211929. Institutional support was provided from the GSU College of Arts and Sciences and the GSU Office of the Vice President for Research and Economic Development. We also thank the anonymous referee for the valuable comments which improved the quality of this manuscript. NR 30 TC 0 Z9 0 U1 5 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD FEB 1 PY 2017 VL 129 IS 972 AR 024002 DI 10.1088/1538-3873/129/972/024002 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EH3NV UT WOS:000391679600001 ER PT J AU Righter, K Nickodem, K Pando, K Danielson, L Boujibar, A Righter, M Lapen, TJ AF Righter, K. Nickodem, K. Pando, K. Danielson, L. Boujibar, A. Righter, M. Lapen, T. J. TI Distribution of Sb, As, Ge, and In between metal and silicate during accretion and core formation in the Earth SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article DE Siderophile; Core formation; Volatiles; Activity coefficient; Metal ID TERRESTRIAL MAGMA OCEAN; SIDEROPHILE ELEMENTS; HIGH-PRESSURE; PARTITION-COEFFICIENTS; OXYGEN FUGACITY; MELT COMPOSITION; OXIDATION-STATE; LIQUID-METAL; TEMPERATURE; MANTLE AB A large number of siderophile (iron-loving) elements are also volatile, thus offering constraints on the origin of volatile elements in differentiated bodies such as Earth, Moon, Mars and Vesta. Metal-silicate partitioning data for many of these elements is lacking, making their overall mantle concentrations in these bodies difficult to model and origin difficult to distinguish between core formation and volatile depletion. To address this gap in understanding, we have undertaken systematic studies of four volatile siderophile elements - Sb, As, Ge and In - at variable temperature and variable Si content of metal. Several series were carried out at 1 GPa, and between 1500 and 1900 degrees C, for both C saturated and C-free conditions. The results show that temperature causes a decrease in the metal/silicate partition coefficient for all four elements. In addition, activity coefficients for each element have been determined and show a very strong dependence on Si content of Fe alloy. Si dissolved in metal significantly decreases the metal/silicate partition coefficients, at both 1600 and 1800 degrees C. The combination of temperature and Si content of the metal causes reduction of the metal-silicate partition coefficient to values that are close to those required for an origin of mantle As, Sb, Ge, and In concentrations by metal-silicate equilibrium processes. Combining these new results with previous studies on As, Sb, Ge, and In, allowed derivation of predictive expressions for metal/silicate partition coefficients for these elements which can then be applied to Earth. The expressions are applied to two scenarios for continuous accretion of Earth; specifically for constant and increasing fO(2) during accretion. The results indicate that mantle concentrations of As, Sb, Ge, and In can be explained by metal-silicate equilibrium during an accretion scenario. The modeling is not especially sensitive to either scenario, although all element concentrations are explained better by a model with variable fO(2). The specific effect of Si is important and calculations that include only S and C (and no Si) cannot reproduce the mantle As, Sb, Ge, and In concentrations. The final core composition in the variable fO2 model is 10.2% Si, 2% S, and 1.1% C (or X-Si = 0.18, X-S = 0.03, and X-C = 0.04. These results suggest that core formation (involving a Si, S, and C-bearing metallic liquid) and accretion were the most important processes establishing many of Earth's mantle volatile elements (indigenous), while post-core formation addition or re-equilibration (exogenous) was of secondary or minor importance. Published by Elsevier Ltd. C1 [Righter, K.; Boujibar, A.] NASA, Johnson Space Ctr, Mailcode KT,2101 NASA Pkwy, Houston, TX 77058 USA. [Nickodem, K.] Univ Notre Dame, Dept Civil Engn & Geol Sci, Notre Dame, IN 46556 USA. [Pando, K.; Danielson, L.] NASA Johnson Space Ctr, Jacobs JETS, 2101 NASA Pkwy, Houston, TX 77058 USA. [Righter, M.; Lapen, T. J.] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA. [Nickodem, K.] Syracuse Univ, Dept Geog, 144 Eggers Hall, Syracuse, NY 13244 USA. RP Righter, K (reprint author), NASA, Johnson Space Ctr, Mailcode KT,2101 NASA Pkwy, Houston, TX 77058 USA. EM kevin.righter-1@nasa.gov FU NASA Cosmochemistry program; NASA LASER program; LPI summer internship FX This work was supported by RTOPs from the NASA Cosmochemistry and LASER programs to KR. KN was supported by an LPI summer internship. We thank A. Peslier and K. Ross for their assistance with the electron microprobe at JSC, C.-T. Lee and P. Luffi for access to and assistance with the LA-ICP-MS at Rice University, and Yongjun Gao for assistance with the Q-ICP-MS at Univ. of Houston. We thank R. Dasgupta for loan of the carbon standard for microprobe analysis. Discussions with M. Humayun, F. Moynier, M. Rutherford, D. Kring, and colleagues with the LPI-JSC NLSI team helped to formulate the ideas and issues discussed in this paper. Early versions of the manuscript benefitted greatly from comments and suggestions of M. Norman, C. Ballhaus, and E. Cottrell. The two anonymous journal reviews and comments of the AE W. van Westrenen also improved the clarity of the presentation. NR 86 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 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD FEB 1 PY 2017 VL 198 BP 1 EP 16 DI 10.1016/j.gca.2016.10.045 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EG4BH UT WOS:000390987900001 ER PT J AU Martins, JA Brand, VS Capucim, MN Felix, RR Martins, LD Freitas, ED Goncalves, FLT Hallak, R Dias, MAFS Cecil, DJ AF Martins, Jorge A. Brand, Veronika S. Capucim, Mauricio N. Felix, Rafael R. Martins, Leila D. Freitas, Edmilson D. Goncalves, Fabio L. T. Hallak, Ricardo Silva Dias, Maria A. F. Cecil, Daniel J. TI Climatology of destructive hailstorms in Brazil SO ATMOSPHERIC RESEARCH LA English DT Article DE Hail report; Destructive hailstorm; Hail annual cycle; Hail diurnal cycle; Hail geographical distribution ID MESOSCALE CONVECTIVE COMPLEXES; SOUTHEASTERN SOUTH-AMERICA; CONTIGUOUS UNITED-STATES; FRIULI-VENEZIA GIULIA; HAIL KINETIC-ENERGY; LOW-LEVEL JET; SOUTHWESTERN FRANCE; LIGHTNING ACTIVITY; CROP DAMAGE; NWP MODEL AB Hail is considered to be among the most complex extreme weather phenomena of the atmosphere. Every year, notably in the southern Brazilian States, destructive hailstorms result in serious economic losses and cause a great social impact destroying crops, homes, medical facilities and schools. The aim of this study is to document the spatial, annual, and diurnal variation in destructive hailstorm frequency during a 22 year period from 1991 to 2012 in Brazil. The analysis is based on a collection of reports released by the Brazilian National Civil Protection Secretariat-SEDEC. Based on reports of emergency assistance given to the population affected by a disaster, the information discussed in this work is assumed as representative only of destructive hailstorms. The analysis reveals a large spatial variability, with the majority of hailstorm occurrences distributed in the three southern-most Brazilian States. Within those states, the number of hail reports was observed to increase with increasing population density in rural areas. Hailstorms were reported most often in the late afternoon and evening of the winter/spring transition, in agreement with a few other areas in the subtropics with available studies, but different from the majority of studies for temperate zones, which suggest spring/summer as the hail season. Although the results show some discrepancies compared to satellite hail signatures, the findings of this work confirm that southern Brazil is a region prone to the development of strong convective storms, with high annual numbers of destructive hail events. (C) 2016 Elsevier B.V. All rights reserved. C1 [Martins, Jorge A.; Capucim, Mauricio N.; Felix, Rafael R.; Martins, Leila D.] Univ Tecnol Fed Parana, Av Pioneiros 3131, BR-86047125 Londrina, PR, Brazil. [Brand, Veronika S.; Freitas, Edmilson D.; Goncalves, Fabio L. T.; Hallak, Ricardo; Silva Dias, Maria A. F.] Univ Sao Paulo, Dept Atmospher Sci, Inst Astron Geophys & Atmospher Sci, Rua Mattao 1226, BR-05508090 Sao Paulo, SP, Brazil. [Cecil, Daniel J.] NASA, Marshall Space Flight Ctr, 320 Sparkman Dr NW, Huntsville, AL 35805 USA. RP Martins, JA (reprint author), Univ Tecnol Fed Parana, Av Pioneiros 3131, BR-86047125 Londrina, PR, Brazil. EM jmartins@utfpr.edu.br NR 153 TC 0 Z9 0 U1 6 U2 6 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 FEB 1 PY 2017 VL 184 BP 126 EP 138 DI 10.1016/j.atmosres.2016.10.012 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EF7GW UT WOS:000390499100012 ER PT J AU Davila, CG Bisagni, C AF Davila, Carlos G. Bisagni, Chiara TI Fatigue life and damage tolerance of postbuckled composite stiffened structures with initial delamination SO COMPOSITE STRUCTURES LA English DT Article DE Composite structures; Postbuckling; Damage tolerance; Fatigue; Delamination; Tests ID CYCLIC BUCKLING TESTS; CURVED PANELS; PROGRESSIVE FAILURE; COMPRESSION; BEHAVIOR; SHEAR; PREDICTION; SPECIMEN AB The durability and damage tolerance of postbuckled composite structures are issues that are not completely understood and remain difficult to predict due to the nonlinearity of the geometric response and its interaction with local damage modes. A research effort was undertaken to investigate experimentally the quasi-static and fatigue damage progression in single-stringer compression specimens. Three specimens were manufactured with a co-cured hat stringer, and an initial defect was introduced with a Teflon film inserted between one flange of the stringer and the skin. Pre-test finite element analyses were conducted using the virtual crack closure technique to select the range of defect sizes to be considered and the load levels to be applied during the fatigue tests. The tests were monitored with digital image correlation, passive thermography, and ultrasound systems. After an initial opening and extension of the Teflon-induced embedded defect, the specimens sustained a high number of cycles. It was observed that when the skin/stringer separation develops in the opposite flange, it propagates rapidly within a small number of cycles and causes the collapse of the specimen. These test results contribute to a better understanding of the complex response phenomena exhibited by postbuckled stiffened structures subjected to fatigue loads in the postbuckling range. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Davila, Carlos G.] NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA. [Bisagni, Chiara] Delft Univ Technol, Fac Aerosp Engn, NL-2629 HS Delft, Netherlands. RP Bisagni, C (reprint author), Delft Univ Technol, Fac Aerosp Engn, NL-2629 HS Delft, Netherlands. EM Carlos.G.Davila@nasa.gov; C.Bisagni@tudelft.nl RI Bisagni, Chiara/G-7158-2012 OI Bisagni, Chiara/0000-0002-8713-9763 NR 32 TC 0 Z9 0 U1 7 U2 7 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0263-8223 EI 1879-1085 J9 COMPOS STRUCT JI Compos. Struct. PD FEB 1 PY 2017 VL 161 BP 73 EP 84 DI 10.1016/j.compstruct.2016.11.033 PG 12 WC Materials Science, Composites SC Materials Science GA EF6WK UT WOS:000390471700008 ER PT J AU Lynch, SD Marcek, BJ Marshall, HM Bushnell, PG Bernal, D Brill, RW AF Lynch, Scott D. Marcek, Benjamin J. Marshall, Heather M. Bushnell, Peter G. Bernal, Diego Brill, Richard W. TI The effects of pop-up satellite archival tags (PSATs) on the metabolic rate and swimming kinematics of juvenile sandbar shark Carcharhinus plumbeus SO FISHERIES RESEARCH LA English DT Article DE Cost of transport; Drag; Hydrodynamics; Metabolic rate; Stride length; Strouhal number; Tail beat ID ATLANTIC BLUEFIN TUNA; WESTERN NORTH-ATLANTIC; MARLIN MAKAIRA-NIGRICANS; FISH AGGREGATING DEVICES; PELAGIC LONGLINE GEAR; POSTRELEASE SURVIVAL; WHITE MARLIN; RECREATIONAL FISHERY; HABITAT UTILIZATION; OXYGEN-CONSUMPTION AB Pop-up satellite archival tags (PSATs) have been used since the 1990s to document the movements and post-release survival of numerous fish species. The effects of PSAT attachment on metabolic rate, cost of transport, and swimming kinematics have, however, not been broadly investigated. We therefore quantified the acute effects of PSAT attachment on these parameters in juvenile (47-87 cm fork length) sandbar shark Carcharhinus plumbeus. Using a water tunnel, we also measured the lift and drag forces of PSATs from three manufacturers which allowed us to calculate the theoretical power costs of towing these devices. We found no evidence that PSAT attachment results in increases in metabolic rate or cost of transport, or influences swimming kinematics of juvenile sandbar shark at volitional swimming speeds. Applying drag force measurements obtained for PSATs to our data showed that the predicted fractional increase in metabolic rate engendered by towing one of these devices at a specified velocity, normalized by the metabolic rate when swimming at that velocity minus the standard metabolic rate, would be below 5%. Our results are therefore congruent and suggest that PSAT attachment does not negatively impact juvenile sandbar shark (and by extension other elasmobranch species of equivalent or larger body sizes and employing a similar swimming mode). (C) 2016 Elsevier B.V. All rights reserved. C1 [Lynch, Scott D.; Bernal, Diego] Univ Massachusetts Dartmouth, Dept Biol, 285 Old Westport Rd, N Dartmouth, MA 02747 USA. [Marcek, Benjamin J.] Virginia Inst Marine Sci, Dept Fisheries Sci, Coll William & Mary, POB 1346, Gloucester Point, VA 23062 USA. [Marshall, Heather M.] Mote Marine Lab, 1600 Ken Thompson Pkwy, Sarasota, FL 34236 USA. [Bushnell, Peter G.] Indiana Univ, Dept Biol Sci, 1700 Mishawaka Ave, South Bend, IN 46615 USA. [Brill, Richard W.] NOAA, James J Howard Marine Sci Lab, Northeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, 74 Magruder Rd, Highlands, NJ 07732 USA. RP Marcek, BJ (reprint author), Virginia Inst Marine Sci, Dept Fisheries Sci, Coll William & Mary, POB 1346, Gloucester Point, VA 23062 USA. EM slynch@umassd.edu; bmarcek@vims.edu; hmmarshall@gmail.com; PBushnel@iusb.edu; dbernal@umassd.edu; rbrill@vims.edu FU University of Massachusetts Dartmouth (UMD); Indiana University South Bend; Northeast Fisheries Science Center, National Marine Fisheries Service, NOAA [NSF-IOS-1354593] FX We thank the staff of the Virginia Institute of Marine Science Eastern Shore Laboratory for their continuing and genuine hospitality and technical support. This is contribution 3578 from the Virginia Institute of Marine Science. Financial support was provided by the University of Massachusetts Dartmouth (UMD), Indiana University South Bend; and the Northeast Fisheries Science Center, National Marine Fisheries Service, NOAA and NSF-IOS-1354593. We also recognize Ashley Stoehr (Department of Biology, UMD) for her help; and especially John Steffensen and Morten Svendsen (University of Copenhagen) for their review and helpful comments on an earlier draft of this manuscript. The views expressed herein are those of the authors and do not necessarily reflect the views of their agencies or funding bodies. Likewise, mention of trade names or commercial companies is for identification purposes only and does not imply endorsement by the National Marine Fisheries Service, NOAA, or any of its subagencies. NR 51 TC 0 Z9 0 U1 14 U2 14 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 FEB PY 2017 VL 186 BP 205 EP 215 DI 10.1016/j.fishres.2016.08.013 PN 1 PG 11 WC Fisheries SC Fisheries GA EF7FG UT WOS:000390494900021 ER PT J AU Petro, NE Keller, JW Gaddis, LR AF Petro, Noah E. Keller, John W. Gaddis, Lisa R. TI Editorial Introduction: Lunar Reconnaissance Orbiter, part II SO ICARUS LA English DT Editorial Material C1 [Petro, Noah E.; Keller, John W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gaddis, Lisa R.] USGS, Astrogeol Sci Ctr, Flagstaff, AZ USA. RP Petro, NE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD FEB PY 2017 VL 283 SI SI BP 1 EP 1 DI 10.1016/j.icarus.2016.11.018 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF8XX UT WOS:000390616400001 ER PT J AU Patterson, GW Stickle, AM Turner, FS Jensen, JR Bussey, DBJ Spudis, P Espiritu, RC Schulze, RC Yocky, DA Wahl, DE Zimmerman, M Cahill, JTS Nolan, M Carter, L Neish, CD Raney, RK Thomson, BJ Kirk, R Thompson, TW Tise, BL Erteza, IA Jakowatz, CV AF Patterson, G. W. Stickle, A. M. Turner, F. S. Jensen, J. R. Bussey, D. B. J. Spudis, P. Espiritu, R. C. Schulze, R. C. Yocky, D. A. Wahl, D. E. Zimmerman, M. Cahill, J. T. S. Nolan, M. Carter, L. Neish, C. D. Raney, R. K. Thomson, B. J. Kirk, R. Thompson, T. W. Tise, B. L. Erteza, I. A. Jakowatz, C. V. TI Bistatic radar observations of the Moon using Mini-RF on LRO and the Arecibo Observatory SO ICARUS LA English DT Article DE Moon; Radar observations; Ices; Regoliths; Impact processes ID LUNAR SOUTH-POLE; BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; ICY GALILEAN SATELLITES; REMOTE-SENSING DATA; COHERENT-BACKSCATTER; WATER ICE; REGOLITH PROPERTIES; PHASE-ANGLE; CRATERS; DEPOSITS AB The Miniature Radio Frequency (Mini-RF) instrument aboard NASA's Lunar Reconnaissance Orbiter (LRO) is a hybrid dual-polarized synthetic aperture radar (SAR) that operated in concert with the Arecibo Observatory to collect bistatic radar data of the lunar nearside from 2012 to 2015. The purpose of this bistatic campaign was to characterize the radar scattering properties of the surface and near-surface, as a function of bistatic angle, for a variety of lunar terrains and search for a coherent bacicscatter opposition effect indicative of the presence of water ice. A variety of lunar terrain types were sampled over a range of incidence and bistatic angles; including mare, highland, pyroclastic, crater ejecta, and crater floor materials. Responses consistent with an opposition effect were observed for the ejecta of several Copernican-aged craters and the floor of the south-polar crater Cabeus. The responses of ejecta material varied by crater in a manner that suggests a relationship with crater age. The response for Cabeus was observed within the portion of its floor that is not in permanent shadow. The character of the response differs from that of crater ejecta and appears unique with respect to all other lunar terrains observed. Analysis of data for this region suggests that the unique nature of the response may indicate the presence of near-surface deposits of water ice. (C) 2016 Elsevier Inc. All rights reserved. C1 [Patterson, G. W.; Stickle, A. M.; Turner, F. S.; Jensen, J. R.; Bussey, D. B. J.; Espiritu, R. C.; Schulze, R. C.; Zimmerman, M.; Cahill, J. T. S.; Raney, R. K.] Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. [Spudis, P.] Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA. [Yocky, D. A.; Wahl, D. E.; Tise, B. L.; Erteza, I. A.; Jakowatz, C. V.] Sandia Natl Labs, Albuquerque, NM 87815 USA. [Nolan, M.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Carter, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Neish, C. D.] Univ Western Ontario, 1151 Richmond St, London, ON N6A 5B7, Canada. [Thomson, B. J.] Boston Univ, Ctr Remote Sensing, 725 Commonwealth Ave, Boston, MA 02215 USA. [Kirk, R.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Thompson, T. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Patterson, GW (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM Wes.Patterson@jhuapl.edu FU LRO project; NASA FX We thank the LRO project and LROC team for their efforts and flexibility in accommodating the non-trivial operations involved in the Mini-RF bistatic campaign. We also thank the Mini-RF team for their efforts in processing and calibrating the data into the form presented here. The authors would also like to thank Paul Lucey and an anonymous reviewer, whose insightful comments helped to improve the manuscript. This work was supported by the LRO project, under contract with NASA. NR 93 TC 2 Z9 2 U1 5 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD FEB PY 2017 VL 283 SI SI BP 2 EP 19 DI 10.1016/j.icarus.2016.05.017 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF8XX UT WOS:000390616400002 ER PT J AU Sanin, AB Mitrofanov, IG Litvak, ML Bakhtin, BN Bodnarik, JG Boynton, WV Chin, G Evans, LG Harshman, K Fedosov, F Golovin, DV Kozyrev, AS Livengood, TA Malakhov, AV McClanahan, TP Mokrousov, MI Starr, RD Sagdeev, RZ Tret'yakov, VI Vostrukhin, AA AF Sanin, A. B. Mitrofanov, I. G. Litvak, M. L. Bakhtin, B. N. Bodnarik, J. G. Boynton, W. V. Chin, G. Evans, L. G. Harshman, K. Fedosov, F. Golovin, D. V. Kozyrev, A. S. Livengood, T. A. Malakhov, A. V. McClanahan, T. P. Mokrousov, M. I. Starr, R. D. Sagdeev, R. Z. Tret'yakov, V. I. Vostrukhin, A. A. TI Hydrogen distribution in the lunar polar regions SO ICARUS LA English DT Article DE Moon; surface; Regoliths; Ices ID WATER ICE; RECONNAISSANCE ORBITER; GAMMA-RAY; MOON; SURFACE; POLES; PROSPECTOR; DEPOSITS; VOLATILES; HYDRATION AB We present a method of conversion of the lunar neutron counting rate measured by the Lunar Reconnaissance Orbiter (LRO) Lunar Exploration Neutron Detector (LEND) instrument collimated neutron detectors, to water equivalent hydrogen (WEH) in the top 1 m layer of lunar regolith. Polar maps of the Moon's inferred hydrogen abundance are presented and discussed. (C) 2016 Elsevier Inc. All rights reserved. C1 [Sanin, A. B.; Mitrofanov, I. G.; Litvak, M. L.; Bakhtin, B. N.; Fedosov, F.; Golovin, D. V.; Kozyrev, A. S.; Malakhov, A. V.; Mokrousov, M. I.; Tret'yakov, V. I.; Vostrukhin, A. A.] Russian Acad Sci, Inst Space Res, Moscow 117997, Russia. [Bodnarik, J. G.; Boynton, W. V.; Harshman, K.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85719 USA. [Chin, G.; Evans, L. G.; Livengood, T. A.; McClanahan, T. P.; Starr, R. D.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Evans, L. G.] Comp Sci Corp, Lanham, MD 20706 USA. [Livengood, T. A.; Sagdeev, R. Z.] Univ Maryland, College Pk, MD 20742 USA. [Starr, R. D.] Catholic Univ Amer, Washington, DC 20064 USA. RP Sanin, AB (reprint author), Russian Acad Sci, Inst Space Res, Moscow 117997, Russia. EM sanin@np.cosmos.ru FU Russian Science Foundation [14-22-00249]; NASA grant [NNX09AW01G] FX This work is supported by the grant # 14-22-00249 from Russian Science Foundation and by NASA grant NNX09AW01G. NR 41 TC 0 Z9 0 U1 3 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD FEB PY 2017 VL 283 SI SI BP 20 EP 30 DI 10.1016/j.icarus.2016.06.002 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF8XX UT WOS:000390616400003 ER PT J AU Hurley, DM Cook, JC Retherford, KD Greathouse, T Gladstone, GR Mandt, K Grava, C Kaufmann, D Hendrix, A Feldman, PD Pryor, W Stickle, A Killen, RM Stern, SA AF Hurley, Dana M. Cook, Jason C. Retherford, Kurt D. Greathouse, Thomas Gladstone, G. Randall Mandt, Kathleen Grava, Cesare Kaufmann, David Hendrix, Amanda Feldman, Paul D. Pryor, Wayne Stickle, Angela Killen, Rosemary M. Stern, S. Alan TI Contributions of solar wind and micrometeoroids to molecular hydrogen in the lunar exosphere SO ICARUS LA English DT Article DE Moon Atmospheres; Dynamics Solar wind Impact processes ID POLAR-REGIONS; SURFACE; MOON; ATMOSPHERE; IMPLANTATION; BOMBARDMENT; TEMPERATURE; DETECTIONS; RETENTION; RELEASE AB We investigate the density and spatial distribution of the H-2 exosphere of the Moon assuming various source mechanisms. Owing to its low mass, escape is non-negligible for H-2. For high-energy source mechanisms, a high percentage of the released molecules escape lunar gravity. Thus, the H-2 spatial distribution for high-energy release processes reflects the spatial distribution of the source. For low energy release mechanisms, the escape rate decreases and the H-2 redistributes itself predominantly to reflect a thermally accommodated exosphere. However, a small dependence on the spatial distribution of the source is superimposed on the thermally accommodated distribution in model simulations, where density is locally enhanced near regions of higher source rate. For an exosphere accommodated to the local surface temperature, a source rate of 2.2 g s(-1) is required to produce a steady state density at high latitude of 1200 cm(-3). Greater source rates are required to produce the same density for more energetic release mechanisms. Physical sputtering by solar wind and direct delivery of H-2 through micrometeoroid bombardment can be ruled out as mechanisms for producing and liberating H-2 into the lunar exosphere. Chemical sputtering by the solar wind is the most plausible as a source mechanism and would require 10-50% of the solar wind H+ inventory to be converted to H-2 to account for the observations. (C) 2016 Elsevier Inc. All rights reserved. C1 [Hurley, Dana M.; Stickle, Angela] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Cook, Jason C.; Kaufmann, David; Stern, S. Alan] Southwest Res Inst, Boulder, CO 80302 USA. [Retherford, Kurt D.; Greathouse, Thomas; Gladstone, G. Randall; Mandt, Kathleen; Grava, Cesare] Southwest Res Inst, San Antonio, TX 78228 USA. [Hendrix, Amanda] Planetary Sci Inst, Tucson, AZ USA. [Feldman, Paul D.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Pryor, Wayne] Cent Arizona Coll, Coolidge, AZ 85128 USA. [Killen, Rosemary M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hurley, DM (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. EM dana.hurley@jhuapl.edu OI Hurley, Dana/0000-0003-1052-1494; Mandt, Kathleen/0000-0001-8397-3315 FU NASA; Lunar Reconnaissance Orbiter; Southwest Research Institute FX This work was supported by NASA, the Lunar Reconnaissance Orbiter, and the Southwest Research Institute. D.M.H. thanks Nancy Chabot and Joshua Cahill for helpful discussions and inputs that improved the paper. NR 46 TC 0 Z9 0 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD FEB PY 2017 VL 283 SI SI BP 31 EP 37 DI 10.1016/j.icarus.2016.04.019 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF8XX UT WOS:000390616400004 ER PT J AU Bauer, S Hussmann, H Oberst, J Dirkx, D Mao, D Neumann, GA Mazarico, E Torrence, MH McGarry, JF Smith, DE Zuber, MT AF Bauer, S. Hussmann, H. Oberst, J. Dirkx, D. Mao, D. Neumann, G. A. Mazarico, E. Torrence, M. H. McGarry, J. F. Smith, D. E. Zuber, M. T. TI Analysis of one-way laser ranging data to LRO, time transfer and clock characterization SO ICARUS LA English DT Article DE Laser ranging; One-way; Lunar Reconnaissance Orbiter; time transfer ID LUNAR RECONNAISSANCE ORBITER AB We processed and analyzed one-way laser ranging data from International Laser Ranging Service ground stations to NASA's Lunar Reconnaissance Orbiter (LRO), obtained from June 13, 2009 until September 30, 2014. We pair and analyze the one-way range observables from station laser fire and spacecraft laser arrival times by using nominal LRO orbit models based on the GRAIL gravity field. We apply corrections for instrument range walk, as well as for atmospheric and relativistic effects. In total we derived a tracking data volume of approximate to 3000 hours featuring 64 million Full Rate and 1.5 million Normal Point observations. From a statistical analysis of the dataset we evaluate the experiment and the ground station performance. We observe a laser ranging measurement precision of 12.3 cm in case of the Full Rate data which surpasses the LOLA timestamp precision of 15 cm. The averaging to Normal Point data further reduces the measurement precision to 5.6 cm. We characterized the LRO clock with fits throughout the mission time and estimated the rate to 6.9 x 10(-8), the aging to 1.6 x 10(-12) /day and the change of aging to 2.3 x 10(-14) /day(2) over all mission phases. The fits also provide referencing of onboard time to the TDB time scale at a precision of 166 ns over two and 256 ns over all mission phases, representing ground to space time transfer. Furthermore we measure ground station clock differences from the fits as well as from simultaneous passes which we use for ground to ground time transfer from common view observations. We observed relative offsets ranging from 33 to 560 ns and relative rates ranging from 2 x 10(-13) to 6 x 10(-12) between the ground station clocks during selected mission phases. We study the results from the different methods and discuss their applicability for time transfer. (C) 2016 Elsevier Inc. All rights reserved. C1 [Bauer, S.; Hussmann, H.; Oberst, J.] German Aerosp Ctr DLR, Berlin, Germany. [Oberst, J.] TU Berlin, Berlin, Germany. [Oberst, J.] Moscow State Univ Geodesy & Cartog MIIGAiK, Moscow, Russia. [Dirkx, D.] Delft Univ Technol, Delft, Netherlands. [Dirkx, D.] Joint Inst VLBI ERIC, Dwingeloo, Netherlands. [Mao, D.] Sigma Space Corp, Lanham, MD USA. [Neumann, G. A.; Mazarico, E.; McGarry, J. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Torrence, M. H.] Stinger Ghaffarian Technol Inc, Greenbelt, MD USA. [Smith, D. E.; Zuber, M. T.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA. RP Bauer, S (reprint author), German Aerosp Ctr DLR, Berlin, Germany. EM sven.bauer@dlr.de RI Neumann, Gregory/I-5591-2013; OI Neumann, Gregory/0000-0003-0644-9944; Dirkx, Dominic/0000-0003-2069-0603 FU ESPaCE project, EC FP7 Grant [263466]; Russian Science Foundation [14-22-00197] FX S. Bauer, H. Hussmann, and D. Dirkx were supported by the ESPaCE project, EC FP7 Grant Agreement 263466. Major parts of this work were carried out while the first author very much enjoyed a research visit at NASA Goddard Space Flight Center (GSFC). J.O. was hosted by MIIGAiK and supported by the Russian Science Foundation, project #14-22-00197. We thank two anonymous reviewers for their very constructive comments. NR 36 TC 0 Z9 0 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 FEB PY 2017 VL 283 SI SI BP 38 EP 54 DI 10.1016/j.icarus.2016.09.026 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF8XX UT WOS:000390616400005 ER PT J AU Mao, DD McGarry, JF Mazarico, E Neumann, GA Sun, XL Torrence, MH Zagwodzki, TW Rowlands, DD Hoffman, ED Horvath, JE Golder, JE Barker, MK Smith, DE Zuber, MT AF Mao, Dandan McGarry, Jan F. Mazarico, Erwan Neumann, Gregory A. Sun, Xiaoli Torrence, Mark H. Zagwodzki, Thomas W. Rowlands, David D. Hoffman, Evan D. Horvath, Julie E. Golder, James E. Barker, Michael K. Smith, David E. Zuber, Maria T. TI The laser ranging experiment of the Lunar Reconnaissance Orbiter: Five years of operations and data analysis SO ICARUS LA English DT Article DE Moon; Orbit determination; Experimental techniques ID GRAVITY-FIELD; MISSION; ALTIMETER; RECOVERY; PHOBOS; MOON AB We describe the results of the Laser Ranging (LR) experiment carried out from June 2009 to September 2014 in order to make one-way time-of-flight measurements of laser pulses between Earth-based laser ranging stations and the Lunar Reconnaissance Orbiter (LRO) orbiting the Moon. Over 4,000 h of successful LR data are obtained from 10 international ground stations. The 20-30 cm precision of the full-rate LR data is further improved to 5-10 cm after conversion into normal points. The main purpose of LR is to utilize the high accuracy normal point data to improve the quality of the LRO orbits, which are nominally determined by the radiometric S-band tracking data. When independently used in the LRO precision orbit determination process with the high-resolution GRAIL gravity model, LR data provide good orbit solutions, with an average difference of similar to 50 m in total position, and similar to 20 cm in radial direction, compared to the definitive LRO trajectory. When used in combination with the S-band tracking data, LR data help to improve the orbit accuracy in the radial direction to similar to 15 cm. In order to obtain highly accurate LR range measurements for precise orbit determination results, it is critical to closely model the behavior of the clocks both at the ground stations and on the spacecraft. LR provides a unique data set to calibrate the spacecraft clock. The LRO spacecraft clock is characterized by the LR data to a timing knowledge of 0.015 ms over the entire 5 years of LR operation. We here present both the engineering setup of the LR experiments and the detailed analysis results of the LR data. (C) 2016 Elsevier Inc. All rights reserved. C1 [Mao, Dandan; Zagwodzki, Thomas W.; Golder, James E.; Barker, Michael K.] Sigma Space Corp, Lanham, MD 20706 USA. [McGarry, Jan F.; Mazarico, Erwan; Neumann, Gregory A.; Sun, Xiaoli; Rowlands, David D.; Hoffman, Evan D.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Torrence, Mark H.] Stinger Ghaffarian Technol Inc, Greenbelt, MD 20770 USA. [Horvath, Julie E.] Honeywell Technol Solut Inc, Columbia, MD 21046 USA. [Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. RP Mao, DD (reprint author), Sigma Space Corp, Lanham, MD 20706 USA. EM dandan.mao@sigmaspace.com RI Neumann, Gregory/I-5591-2013 OI Neumann, Gregory/0000-0003-0644-9944 NR 53 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 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD FEB PY 2017 VL 283 SI SI BP 55 EP 69 DI 10.1016/j.icarus.2016.07.003 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF8XX UT WOS:000390616400006 ER PT J AU Smith, DE Zuber, MT Neumann, GA Mazarico, E Lemoine, FG Head, JW Lucey, PG Aharonson, O Robinson, MS Sun, XL Torrence, MH Barker, MK Oberst, J Duxbury, TC Mao, DD Barnouin, OS Jha, K Rowlands, DD Goossens, S Baker, D Bauer, S Glaser, P Lemelin, M Rosenburg, M Sori, MM Whitten, J Mcclanahan, T AF Smith, David E. Zuber, Maria T. Neumann, Gregory A. Mazarico, Erwan Lemoine, Frank G. Head, James W., III Lucey, Paul G. Aharonson, Oded Robinson, Mark S. Sun, Xiaoli Torrence, Mark H. Barker, Michael K. Oberst, Juergen Duxbury, Thomas C. Mao, Dandan Barnouin, Olivier S. Jha, Kopal Rowlands, David D. Goossens, Sander Baker, David Bauer, Sven Glaeser, Philipp Lemelin, Myriam Rosenburg, Margaret Sori, Michael M. Whitten, Jennifer Mcclanahan, Timothy TI Summary of the results from the lunar orbiter laser altimeter after seven years in lunar orbit SO ICARUS LA English DT Article DE Moon; surface; orbit determination ID SOUTH-POLE; RECONNAISSANCE ORBITER; ILLUMINATION CONDITIONS; GLOBAL SHAPE; LOLA DATA; MOON; SURFACE; MISSION; TOPOGRAPHY; CRATERS AB In June 2009 the Lunar Reconnaissance Orbiter (LRO) spacecraft was launched to the Moon. The payload consists of 7 science instruments selected to characterize sites for future robotic and human missions. Among them, the Lunar Orbiter Laser Altimeter (LOLA) was designed to obtain altimetry, surface roughness, and reflectance measurements. The primary phase of lunar exploration lasted one year, following a 3-month commissioning phase. On completion of its exploration objectives, the LRO mission transitioned to a science mission. After 7 years in lunar orbit, the LOLA instrument continues to map the lunar surface. The LOLA dataset is one of the foundational datasets acquired by the various LRO instruments. LOLA provided a high-accuracy global geodetic reference frame to which past, present and future lunar observations can be referenced. It also obtained high-resolution and accurate global topography that were used to determine regions in permanent shadow at the lunar poles. LOLA further contributed to the study of polar volatiles through its unique measurement of surface brightness at zero phase, which revealed anomalies in several polar craters that may indicate the presence of water ice. In this paper, we describe the many LOLA accomplishments to date and its contribution to lunar and planetary science. (C) 2016 Elsevier Inc. All rights reserved. C1 [Smith, David E.; Zuber, Maria T.; Sori, Michael M.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Neumann, Gregory A.; Mazarico, Erwan; Lemoine, Frank G.; Sun, Xiaoli; Rowlands, David D.; Baker, David; Mcclanahan, Timothy] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Head, James W., III] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA. [Lucey, Paul G.; Lemelin, Myriam] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Aharonson, Oded] Weizmann Inst Sci, Dept Earth & Planetary Sci, IL-76100 Rehovot, Israel. [Robinson, Mark S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Torrence, Mark H.] Stinger Ghaffarian Technol Inc, Greenbelt, MD 20770 USA. [Barker, Michael K.; Mao, Dandan; Jha, Kopal] Sigma Space Corp, Lanham, MD 20706 USA. [Oberst, Juergen; Bauer, Sven] German Aerosp Ctr DLR, Rutherfordstr 2, D-12489 Berlin, Germany. [Oberst, Juergen; Glaeser, Philipp] Tech Univ Berlin, D-10623 Berlin, Germany. [Duxbury, Thomas C.] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA. [Barnouin, Olivier S.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA. [Goossens, Sander] Univ Maryland Baltimore Cty, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21250 USA. [Rosenburg, Margaret] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Sori, Michael M.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Whitten, Jennifer] Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, Washington, DC 20560 USA. RP Smith, DE (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. EM smithde@mit.edu RI Neumann, Gregory/I-5591-2013; OI Neumann, Gregory/0000-0003-0644-9944; Sori, Michael/0000-0002-6191-2447 FU Lunar Reconnaissance Orbiter spacecraft and operations teams; Project Science Office FX We would like to acknowledge the LOLA Engineering Team for the design and development of an outstanding instrument. We also recognize the support of the Lunar Reconnaissance Orbiter spacecraft and operations teams, and the Project Science Office without whom the LOLA investigation would not have been possible. In addition, we gratefully acknowledge the contributions of Mikhail A. Kreslaysky, Caleb Fassett, Debra Hurwitz and Lauren Jozwiak toward making LOLA a success through their scientific utilization of the data to address important scientific problems. NR 92 TC 2 Z9 2 U1 4 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD FEB PY 2017 VL 283 SI SI BP 70 EP 91 DI 10.1016/j.icarus.2016.06.006 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF8XX UT WOS:000390616400007 ER PT J AU Wagner, RV Nelson, DM Plescia, JB Robinson, MS Speyerer, EJ Mazarico, E AF Wagner, R. V. Nelson, D. M. Plescia, J. B. Robinson, M. S. Speyerer, E. J. Mazarico, E. TI Coordinates of anthropogenic features on the Moon SO ICARUS LA English DT Article DE Moon, surface; Image processing; Data reduction techniques ID LUNAR ATMOSPHERE; LANDING SITE; SPACECRAFT; TRAVERSE; IMPACTS; MISSION; MODEL AB High-resolution images from the Lunar Reconnaissance Orbiter Camera (LROC) Narrow Angle Camera (NAC) reveal the landing locations of recent and historic spacecraft and associated impact sites across the lunar surface. Using multiple images of each site acquired between 2009 and 2015, an improved Lunar Reconnaissance Orbiter (LRO) ephemeris, and a temperature-dependent camera orientation model, we derived accurate coordinates (<12 m) for each soft-landed spacecraft, rover, deployed scientific payload, and spacecraft impact crater that we have identified. Accurate coordinates enhance the scientific interpretations of data returned by the surface instruments and of returned samples of the Apollo and Luna sites. In addition, knowledge of the sizes and positions of craters formed as the result of impacting spacecraft provides key benchmarks into the relationship between energy and crater size, as well as calibration points for reanalyzing seismic measurements acquired during the Apollo program. We identified the impact craters for the three spacecraft that impacted the surface during the LRO mission by comparing before and after NAC images. (C) 2016 Elsevier Inc. All rights reserved. C1 [Wagner, R. V.; Nelson, D. M.; Robinson, M. S.; Speyerer, E. J.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Plescia, J. B.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Mazarico, E.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. RP Wagner, RV (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. EM rvwagner@asu.edu OI Wagner, Robert/0000-0001-5999-0721; Speyerer, Emerson/0000-0001-9354-1858 FU LRO project [NNG07EK00C] FX We thank the LRO Mission Operations Team at Goddard Space Flight Center and LROC Science Operations Team at Arizona State University for acquiring the many images that made this work possible. We thank Bob Craddock and two anonymous reviewers for their help in improving this manuscript. We also thank Zachary Davis for assistance with proofreading. This work was funded by the LRO project, grant #NNG07EK00C. NR 54 TC 1 Z9 1 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD FEB PY 2017 VL 283 SI SI BP 92 EP 103 DI 10.1016/j.icarus.2016.05.011 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF8XX UT WOS:000390616400008 ER PT J AU Kreslavsky, MA Head, JW Neumann, GA Zuber, MT Smith, DE AF Kreslavsky, Mikhail A. Head, James W. Neumann, Gregory A. Zuber, Maria T. Smith, David E. TI Low-amplitude topographic features and textures on the Moon: Initial results from detrended Lunar Orbiter Laser Altimeter (LOLA) topography SO ICARUS LA English DT Article DE Moon, surface; Volcanism; Tectonics; Data reduction techniques ID MARS AB Global lunar topographic data derived from ranging measurements by the Lunar Oribter Laser Altimeter (LOLA) onboard LRO mission to the Moon have extremely high vertical precision. We use detrended topography as a means for utilization of this precision in geomorphological analysis. The detrended topography was calculated as a difference between actual topography and a trend surface defined as a median topography in a circular sliding window. We found that despite complicated distortions caused by the non-linear nature of the detrending procedure, visual inspection of these data facilitates identification of low-amplitude gently-sloping geomorphic features. We present specific examples of patterns of lava flows forming the lunar maria and revealing compound flow fields, a new class of lava flow complex on the Moon. We also highlight the identification of linear tectonic features that otherwise are obscured in the images and topographic data processed in a more traditional manner. (C) 2016 Published by Elsevier Inc. C1 [Kreslavsky, Mikhail A.] Univ Calif Santa Cruz, Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Kreslavsky, Mikhail A.] Moscow State Univ Geodesy & Cartog MIIGAiK, MExLab, Moscow, Russia. [Head, James W.] Brown Univ, Earth Environm & Planetary Sci, Providence, RI 02912 USA. [Neumann, Gregory A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD USA. [Zuber, Maria T.; Smith, David E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. RP Kreslavsky, MA (reprint author), Univ Calif Santa Cruz, Earth & Planetary Sci, Santa Cruz, CA 95064 USA. EM mkreslav@ucsc.edu RI Neumann, Gregory/I-5591-2013 OI Neumann, Gregory/0000-0003-0644-9944 FU NASA Lunar Reconnaissance Orbiter Lunar Orbiter Laser Altimeter (LOLA) experiment [NNX09AM54G, NNX11AK29G]; NASA Solar System Exploration Research Virtual Institute (SSERVI) grant [NNA14AB01A]; Russian Science Foundation [14-22-00197] FX We acknowledge financial support from the NASA Lunar Reconnaissance Orbiter Lunar Orbiter Laser Altimeter (LOLA) experiment (NNX09AM54G and NNX11AK29G to JWH) and the NASA Solar System Exploration Research Virtual Institute (SSERVI) grant for Evolution and Environment of Exploration Destinations under cooperative Agreement No. NNA14AB01A at Brown University. All work on data processing and analysis was carried out by MAK at MIIGAiK under Russian Science Foundation support, project 14-22-00197. NR 26 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 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD FEB PY 2017 VL 283 SI SI BP 138 EP 145 DI 10.1016/j.icarus.2016.07.017 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF8XX UT WOS:000390616400011 ER PT J AU Jozwiak, LM Head, JW Neumann, GA Wilson, L AF Jozwiak, L. M. Head, J. W., III Neumann, G. A. Wilson, L. TI Observational constraints on the identification of shallow lunar magmatism: Insights from floor-fractured craters SO ICARUS LA English DT Article DE Moon; Geophysics; Volcanism ID GRAVITY-ANOMALIES; GRAIL; MOON; MISSION; GENERATION; INTRUSIONS; INTERIOR; GLASSES AB Floor-fractured craters are a class of lunar crater hypothesized to form in response to the emplacement of a shallow magmatic intrusion beneath the crater floor. The emplacement of a shallow magmatic body should result in a positive Bouguer anomaly relative to unaltered complex craters, a signal which is observed for the average Bouguer anomaly interior to the crater walls. We observe the Bouguer anomaly of floor-fractured craters on an individual basis using the unfiltered Bouguer gravity solution from GRAIL and also a degree 100-600 band-filtered Bouguer gravity solution. The low-magnitude of anomalies arising from shallow magmatic intrusions makes identification using unfiltered Bouguer gravity solutions inconclusive. The observed anomalies in the degree 100-600 Bouguer gravity solution are spatially heterogeneous, although there is spatial correlation between volcanic surface morphologies and positive Bouguer anomalies. We interpret these observations to mean that the spatial heterogeneity observed in the Bouguer signal is the result of variable degrees of magmatic degassing within the intrusions. (C) 2016 Elsevier Inc. All rights reserved. C1 [Jozwiak, L. M.; Head, J. W., III] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA. [Neumann, G. A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20768 USA. [Wilson, L.] Univ Lancaster, Lancaster Environm Ctr, Lancaster LA1 4YQ, England. RP Jozwiak, LM (reprint author), Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA. EM lauren_jozwiak@brown.edu RI Neumann, Gregory/I-5591-2013 OI Neumann, Gregory/0000-0003-0644-9944 FU NASA [NNX13AR86H]; NASA Lunar Reconnaissance Orbiter (LRO) Mission, Lunar Orbiter Laser Altimeter (LOLA) Experiment Team [NNX11AK29G, NNX13AO77G]; NASA Gravity Recovery and Interior Laboratory (GRAIL) Mission Guest Scientist Program [NNX12AL07G]; NASA Solar System Exploration Research Virtual Institute (SSERVI) [NNA14AB01A] FX We gratefully acknowledge the support of NASA Harriett G. Jenkins Fellowship (Grant NNX13AR86H) to L.M. Jozwiak. We also gratefully acknowledge financial support from the NASA Lunar Reconnaissance Orbiter (LRO) Mission, Lunar Orbiter Laser Altimeter (LOLA) Experiment Team (Grants NNX11AK29G and NNX13AO77G), the NASA Gravity Recovery and Interior Laboratory (GRAIL) Mission Guest Scientist Program (Grant NNX12AL07G) and the NASA Solar System Exploration Research Virtual Institute (SSERVI) grant for Evolution and Environment of Exploration Destinations under cooperative agreement number NNA14AB01A at Brown University. Additionally, we acknowledge Jay Dickson for his invaluable assistance in data processing. NR 33 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 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD FEB PY 2017 VL 283 SI SI BP 224 EP 231 DI 10.1016/j.icarus.2016.04.020 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF8XX UT WOS:000390616400014 ER PT J AU Bandfield, JL Cahill, JTS Carter, LM Neish, CD Patterson, GW Williams, JP Paige, DA AF Bandfield, Joshua L. Cahill, Joshua T. S. Carter, Lynn M. Neish, Catherine D. Patterson, G. Wesley Williams, Jean-Pierre Paige, David A. TI Distal ejecta from lunar impacts: Extensive regions of rocky deposits SO ICARUS LA English DT Article DE Moon, surface; Impact processes; Infrared observations; Radar observations ID RADIOMETER EXPERIMENT; CRATER; MOON; TEMPERATURES; CONSTRAINTS; MERCURY AB Lunar Reconnaissance Orbiter (LRO) Diviner Radiometer, Mini-RF, and LRO Camera data were used to identify and characterize rocky lunar deposits that appear well separated from any potential source crater. Two regions are described: 1) A similar to 18,000 km(2) area with elevated rock abundance and extensive melt ponds and veneers near the antipode of Tycho crater (167.5 degrees E, 42.5 degrees N). This region has been identified previously, using radar and imaging data. 2) A much larger and more diffuse region, covering 730,000 km(2), centered near 310 degrees E, 35 degrees S, containing elevated rock abundance and numerous granular flow deposits on crater walls. The rock distributions in both regions favor certain slope azimuths over others, indicating a directional component to the formation of these deposits. The spatial distribution of rocks is consistent with the arrival of ejecta from the west and northwest at low angles (similar to 10-30 degrees) above the horizon in both regions. The derived age and slope orientations of the deposits indicate that the deposits likely originated as ejecta from the Tycho impact event. Despite their similar origin, the deposits in the two regions show significant differences in the datasets. The Tycho crater antipode deposit covers a smaller area, but the deposits are pervasive and appear to be dominated by impact melts. By contrast, the nearside deposits cover a much larger area and numerous granular flows were triggered. However, the features in this region are less prominent with no evidence for the presence of impact melts. The two regions appear to be surface expressions of a distant impact event that can modify surfaces across wide regions, resulting in a variety of surface morphologies. The Tycho impact event may only be the most recent manifestation of these processes, which likely have played a role in the development of the regolith throughout lunar history. (C) 2016 Elsevier Inc. All rights reserved. C1 [Bandfield, Joshua L.] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA. [Cahill, Joshua T. S.; Patterson, G. Wesley] Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. [Carter, Lynn M.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. [Neish, Catherine D.] Univ Western Ontario, Dept Earth Sci, 1151 Richmond St, London, ON N6A 3K7, Canada. [Williams, Jean-Pierre; Paige, David A.] Univ Calif Los Angeles, Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. RP Bandfield, JL (reprint author), Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA. EM jbandfield@spacescience.org RI Williams, Jean-Pierre/C-3531-2009; Carter, Lynn/D-2937-2012 OI Williams, Jean-Pierre/0000-0003-4163-2760; FU Lunar Reconnaissance Orbiter program FX We would like to thank the LRO, LROC, Mini-RF, and Diviner operations teams for the collection of high quality datasets used in this work. We would also like to thank Sam Lawrence and Julie Stopar for helpful discussions. The Lunar Reconnaissance Orbiter program provided support for this work. We also thank two anonymous reviewers, who provided helpful and constructive comments that significantly improved this manuscript. NR 41 TC 0 Z9 0 U1 6 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD FEB PY 2017 VL 283 SI SI BP 282 EP 299 DI 10.1016/j.icarus.2016.05.013 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF8XX UT WOS:000390616400018 ER PT J AU Lucey, PG Greenhagen, BT Song, E Arnold, JA Lemelin, M Hanna, KD Bowles, NE Glotch, TD Paige, DA AF Lucey, Paul G. Greenhagen, Benjamin T. Song, Eugenie Arnold, Jessica A. Lemelin, Myriam Hanna, Kerri Donaldson Bowles, Neil E. Glotch, Timothy D. Paige, David A. TI Space weathering effects in Diviner Lunar Radiometer multispectral infrared measurements of the lunar Christiansen Feature: Characteristics and mitigation SO ICARUS LA English DT Article DE Moon; Solar wind; Infrared observations; Moon, surface ID MAGNETIC-ANOMALIES; IRON CONCENTRATION; OPTICAL-PROPERTIES; EMISSION-SPECTRA; SURFACE; MOON; SOILS; ORIGIN; SELENE; CRATER AB Multispectral infrared measurements by the Diviner Lunar Radiometer Experiment on the Lunar Renaissance Orbiter enable the characterization of the position of the Christiansen Feature, a thermal infrared spectral feature that laboratory work has shown is proportional to the bulk silica content of lunar surface materials. Diviner measurements show that the position of this feature is also influenced by the changes in optical and physical properties of the lunar surface with exposure to space, the process known as space weathering. Large rayed craters and lunar swirls show corresponding Christiansen Feature anomalies. The space weathering effect is likely due to differences in thermal gradients in the optical surface imposed by the space weathering control of albedo. However, inspected at high resolution, locations with extreme compositions and Christiansen Feature wavelength positions - silica-rich and olivine-rich areas do not have extreme albedos, and fall off the albedo- Christiansen Feature wavelength position trend occupied by most of the Moon. These areas demonstrate that the Christiansen Feature wavelength position contains compositional information and is not solely dictated by albedo. An optical maturity parameter derived from near-IR measurements is used to partly correct Diviner data for space weathering influences. (C) 2016 The Authors. Published by Elsevier Inc. C1 [Lucey, Paul G.; Lemelin, Myriam] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, 1680 East West Rd, Honolulu, HI 96822 USA. [Greenhagen, Benjamin T.] Johns Hopkins Univ, Appl Phys Lab, 11101 Johns Hopkins Rd, Laurel, MD 20723 USA. [Song, Eugenie] Jet Prop Lab, 4800 Oak Grove Dr,Pasadena Mail Stop 264-623, Pasadena, CA 91109 USA. [Arnold, Jessica A.; Hanna, Kerri Donaldson; Bowles, Neil E.] Univ Oxford, Atmospher Ocean & Planetary Phys, Parks Rd, Oxford OX1 3PU, England. [Lemelin, Myriam] Univ Hawaii Manoa, Dept Geol & Geophys, 1680 East West Rd, Honolulu, HI 96822 USA. [Glotch, Timothy D.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. [Paige, David A.] Univ Calif Los Angeles, Deptartment Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. RP Lucey, PG (reprint author), Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, 1680 East West Rd, Honolulu, HI 96822 USA. EM lucey@higp.hawaii.edu FU National Aeronautics and Space Administration's Lunar Reconnaissance Orbiter project FX Work described in this paper was sponsored by the National Aeronautics and Space Administration's Lunar Reconnaissance Orbiter project under a contract to the University of California at Los Angeles, David A. Paige, Principal Investigator. This is Hawaii Institute of Geophysics and Planetology Publication Number 2192 and School of Ocean and Earth Sciences and Technology Publication Number 9630. The authors thank Douglas Hemingway and David Blewett for thoughtful reviews. The sponsor was not involved in the study design, in the collection, analysis or interpretation of data, in the writing of the report, or in the decision to submit the article for publication. NR 43 TC 1 Z9 1 U1 4 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD FEB PY 2017 VL 283 SI SI BP 343 EP 351 DI 10.1016/j.icarus.2016.05.010 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF8XX UT WOS:000390616400021 ER PT J AU Jordan, AP Stubbs, TJ Wilson, JK Schwadron, NA Spence, HE AF Jordan, A. P. Stubbs, T. J. Wilson, J. K. Schwadron, N. A. Spence, H. E. TI The rate of dielectric breakdown weathering of lunar regolith in permanently shadowed regions SO ICARUS LA English DT Article DE Moon; Regoliths; Cosmic rays ID RECONNAISSANCE ORBITER MISSION; PROTON FLUENCE MODEL; DESTRUCTIVE BREAKDOWN; DISCHARGES; COMPLEX; EVENTS; UPDATE; FILMS; WATER; MOON AB Large solar energetic particle events may cause dielectric breakdown in the upper 1 mm of regolith in permanently shadowed regions (PSRs). We estimate how the resulting breakdown weathering compares to meteoroid impact weathering. Although the SEP event rates measured by the Cosmic Ray Telescope for the Effects of Radiation (CRaTER) on the Lunar Reconnaissance Orbiter (LRO) are too low for breakdown to have significantly affected the regolith over the duration of the LRO mission, regolith gardened by meteoroid impacts has been exposed to SEPs for similar to 10(6) yr. Therefore, we estimate that breakdown weathering's production rate of vapor and melt in the coldest PSRs is up to 1.8- 3.5 x 10(-7) kg m(-2) yr(-1), which is comparable to that produced by meteoroid impacts. Thus, in PSRs, up to 10-25% of the regolith may have been melted or vaporized by dielectric breakdown. Breakdown weathering could also be consistent with observations of the increased porosity ("fairy castles") of PSR regolith. We also show that it is conceivable that breakdown-weathered material is present in Apollo soil samples. Consequently, breakdown weathering could be an important process within PSRs, and it warrants further investigation. (C) 2016 Elsevier Inc. All rights reserved. C1 [Jordan, A. P.; Wilson, J. K.; Schwadron, N. A.; Spence, H. E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Jordan, A. P.; Stubbs, T. J.; Wilson, J. K.; Schwadron, N. A.; Spence, H. E.] NASA, Ames Res Ctr, Solar Syst Explorat Res Virtual Inst, Moffett Field, CA 94035 USA. [Stubbs, T. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Jordan, AP (reprint author), Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.; Jordan, AP (reprint author), NASA, Ames Res Ctr, Solar Syst Explorat Res Virtual Inst, Moffett Field, CA 94035 USA. EM a.p.jordan@unh.edu RI Stubbs, Timothy/I-5139-2013 OI Stubbs, Timothy/0000-0002-5524-645X FU NASA grant [NNG11PA03C, NNX14AG13A] FX This work was supported by NASA grant NNG11PA03C and NNX14AG13A. The authors wish to thank Carle Pieters, Jay Melosh, and Joe Dwyer for helpful discussions. The authors also thank Paul Lucey and an anonymous reviewer for their helpful comments and suggestions. NR 60 TC 0 Z9 0 U1 1 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD FEB PY 2017 VL 283 SI SI BP 352 EP 358 DI 10.1016/j.icarus.2016.08.027 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF8XX UT WOS:000390616400022 ER PT J AU Zawodny, NS Liu, F Cattafesta, L AF Zawodny, Nikolas S. Liu, Fei Cattafesta, Louis TI Transfer matrix modeling of a recessed microphone for unsteady surface pressure measurements SO APPLIED ACOUSTICS LA English DT Article DE Transfer matrices; Recessed microphone; Frequency response; Microphone calibration ID NOISE AB Recessed microphones are commonly used for unsteady surface pressure measurements, either due to space limitations or to satisfy performance requirements. A technique is developed using transfer matrices to design a configuration by modeling its frequency response. This.technique is beneficial since it provides guidance to optimize the recessed configuration prior to fabrication. The recessed nature also allows for utilization of closely-spaced pressure ports on a surface, thus providing an inexpensive means for measuring unsteady surface pressures with high spatial resolution. A tube-branch design capable of achieving a 10-kHz bandwidth is presented and validated experimentally using an acoustic plane wave tube. Published by Elsevier Ltd. C1 [Zawodny, Nikolas S.; Liu, Fei] Univ Florida, Interdisciplinary Microsyst Grp, Gainesville, FL 32611 USA. [Cattafesta, Louis] Florida State Univ, FCAAP, Tallahassee, FL 32310 USA. [Liu, Fei] Ford Motor Co, Program NVH, 20800 Oakwood Blvd, Dearborn, MI 48121 USA. RP Zawodny, NS (reprint author), Univ Florida, Interdisciplinary Microsyst Grp, Gainesville, FL 32611 USA.; Zawodny, NS (reprint author), NASA, Langley Res Ctr, Aeroacoust Branch, Mail Stop 461, Hampton, VA 23681 USA. EM nikolas.s.zawodny@nasa.gov; fliu40@ford.com; lcattafesta@fsu.edu FU NASA Aeronautics Scholarship Program FX The authors gratefully acknowledge Sam Yang for his assistance with system model development, Derek Dussault for his assistance with recessed sensor packaging and experimental characterization, and Dylan Alexander for his assistance with isolated electret microphone experimental characterization. Partial financial assistance for this work was provided by the NASA Aeronautics Scholarship Program. NR 13 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0003-682X EI 1872-910X J9 APPL ACOUST JI Appl. Acoust. PD FEB PY 2017 VL 117 BP 185 EP 190 DI 10.1016/j.apacoust.2016.10.013 PN A PG 6 WC Acoustics SC Acoustics GA EF1HD UT WOS:000390075000023 ER EF