FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Martens, B Lievens, H Colliander, A Jackson, TJ Verhoest, NEC AF Martens, Brecht Lievens, Hans Colliander, Andreas Jackson, Thomas J. Verhoest, Niko E. C. TI Estimating Effective Roughness Parameters of the L-MEB Model for Soil Moisture Retrieval Using Passive Microwave Observations From SMAPVEX12 SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Passive Active L-band Sensor (PALS); passive microwave remote sensing; roughness modeling; soil moisture ID L-BAND RADIOMETER; DISCHARGE PREDICTIONS; SURFACE-ROUGHNESS; OCEAN SALINITY; SIMPLEX-METHOD; CROP FIELDS; CALIBRATION; EMISSION; RADAR; SCALE AB Despite the continuing efforts to improve existing soil moisture retrieval algorithms, the ability to estimate soil moisture from passive microwave observations is still hampered by problems in accurately modeling the observed microwave signal. This paper focuses on the estimation of effective surface roughness parameters of the L-band Microwave Emission from the Biosphere (L-MEB) model in order to improve soil moisture retrievals from passive microwave observations. Data from the SMAP Validation Experiment 2012 conducted in Canada are used to develop and validate a simple model for the estimation of effective roughness parameters. Results show that the L-MEB roughness parameters can be empirically related to the observed brightness temperatures and the leaf area index of the vegetation. These results indicate that the roughness parameters are compensating for both roughness and vegetation effects. It is also shown, using a leave-one-out cross validation, that the model is able to accurately estimate the roughness parameters necessary for the inversion of the L-MEB model. In order to demonstrate the usefulness of the roughness parameterization, the performance of the model is compared to more traditional roughness formulations. Results indicate that the soil moisture retrieval error can be reduced to 0.054 m(3)/m(3) if the roughness formulation proposed in this study is implemented in the soil moisture retrieval algorithm. C1 [Martens, Brecht; Lievens, Hans; Verhoest, Niko E. C.] Univ Ghent, Lab Hydrol & Water Management, B-9000 Ghent, Belgium. [Colliander, Andreas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Jackson, Thomas J.] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA. RP Martens, B (reprint author), Univ Ghent, Lab Hydrol & Water Management, B-9000 Ghent, Belgium. EM Brecht.Martens@ugent.be RI Verhoest, Niko/C-9726-2010; OI Verhoest, Niko/0000-0003-4116-8881; Martens, Brecht/0000-0002-7368-7953 FU National Aeronautics and Space Administration FX The authors would like to thank the SMAPVEX12 investigators for making the data of the campaigns publicly available to the scientific community and the anonymous reviewers for their significant contribution to this paper. The second author is a Postdoctoral Research Fellow with the Research Foundation Flanders (FWO). Part of the work described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 49 TC 5 Z9 6 U1 4 U2 38 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 JUL PY 2015 VL 53 IS 7 BP 4091 EP 4103 DI 10.1109/TGRS.2015.2390259 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 CD9ZO UT WOS:000351461000042 ER PT J AU Wallace, JK Rider, S Serabyn, E Kuhn, J Liewer, K Deming, J Showalter, G Lindensmith, C Nadeau, J AF Wallace, J. Kent Rider, Stephanie Serabyn, Eugene Kuehn, Jonas Liewer, Kurt Deming, Jody Showalter, Gordon Lindensmith, Chris Nadeau, Jay TI Robust, compact implementation of an off-axis digital holographic microscope SO OPTICS EXPRESS LA English DT Article ID PHASE-CONTRAST MICROSCOPY; NUMERICAL RECONSTRUCTION; TUMOR-CELLS; RESOLUTION; ALGORITHM; MOTILITY; BEHAVIOR AB Recent advances in digital technologies, such as high-speed computers and large-format digital imagers, have led to a burgeoning interest in the science and engineering of digital holographic microscopy (DHM). Here we report on a novel off-axis DHM, based on a twin-beam optical design, which avoids the limitations of prior systems, and provides many advantages, including compactness, intrinsic stability, robustness against misalignment, ease of use, and cost. These advantages are traded for a physically constrained sample volume, as well as a fixed fringe spacing. The first trade is not overly restrictive for most applications, and the latter provides for a pre-set assembly alignment that optimizes the spatial frequency sampling. Moreover, our new design supports use in both routine laboratory settings as well as extreme environments without any sacrifice in performance, enabling ready observation of microbial species in the field. The instrument design is presented in detail here, along with a demonstration of bacterial video imaging at sub-micrometer resolution at temperatures down to -15 degrees C. (C) 2015 Optical Society of America C1 [Wallace, J. Kent; Serabyn, Eugene; Kuehn, Jonas; Liewer, Kurt; Lindensmith, Chris] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rider, Stephanie; Nadeau, Jay] CALTECH, Div Aerosp Engn, Pasadena, CA 91125 USA. [Showalter, Gordon] Univ Washington, Dept Biol Oceanog, Seattle, WA 98105 USA. [Nadeau, Jay] McGill Univ, Dept Biomed Engn, Montreal, PQ H3A 2B4, Canada. RP Wallace, JK (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM james.k.wallace@jpl.nasa.gov FU Gordon and Betty Moore Foundation [4037, 4038] FX This work was funded by the Gordon and Betty Moore Foundation through grants 4037 to McGill University and 4038 to the California Institute of Technology. We also thank the Keck Institute for Space Studies for allowing us use of the Tolman/Bacher House, which served as a meeting location for our team on the Caltech campus. We appreciate the contribution of Asphericon, Inc. for fabricating customized optical elements to meet the packaging needs. This work was partially carried out by the Jet Propulsion Laboratory, California Institute of Technology. NR 31 TC 6 Z9 6 U1 1 U2 10 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD JUN 29 PY 2015 VL 23 IS 13 BP 17367 EP 17378 DI 10.1364/OE.23.017367 PG 12 WC Optics SC Optics GA CN6KI UT WOS:000358543300086 PM 26191746 ER PT J AU Ingersoll, MA Lyons, AS Muniyan, S D'Cunha, N Robinson, T Hoelting, K Dwyer, JG Bu, XR Batra, SK Lin, MF AF Ingersoll, Matthew A. Lyons, Anastesia S. Muniyan, Sakthivel D'Cunha, Napoleon Robinson, Tashika Hoelting, Kyle Dwyer, Jennifer G. Bu, Xiu R. Batra, Surinder K. Lin, Ming-Fong TI Novel Imidazopyridine Derivatives Possess Anti-Tumor Effect on Human Castration-Resistant Prostate Cancer Cells SO PLOS ONE LA English DT Article ID PHOSPHATIDYLINOSITOL 3-KINASE INHIBITOR; ANDROGEN RECEPTOR; ACID-PHOSPHATASE; IN-VIVO; TYROSINE-PHOSPHATASE; INCREASED SURVIVAL; P66(SHC) PROTEIN; GROWTH; EXPRESSION; APOPTOSIS AB Prostate cancer (PCa) is the second leading cause of cancer-related death afflicting United States males. Most treatments to-date for metastatic PCa include androgen-deprivation therapy and second-generation anti-androgens such as abiraterone acetate and enzalutamide. However, a majority of patients eventually develop resistance to these therapies and relapse into the lethal, castration-resistant form of PCa to which no adequate treatment option remains. Hence, there is an immediate need to develop effective therapeutic agents toward this patient population. Imidazopyridines have recently been shown to possess Akt kinase inhibitory activity; thus in this study, we investigated the inhibitory effect of novel imidazopyridine derivatives HIMP, M-Mel, OMP, and EtOP on different human castration-resistant PCa cells. Among these compounds, HIMP and M-MeI were found to possess selective dose-and time-dependent growth inhibition: they reduced castration-resistant PCa cell proliferation and spared benign prostate epithelial cells. Using LNCaP C-81 cells as the model system, these compounds also reduced colony formation as well as cell adhesion and migration, and M-MeI was the most potent in all studies. Further investigation revealed that while HIMP primarily inhibits PCa cell growth via suppression of PI3K/Akt signaling pathway, M-MeI can inhibit both PI3K/Akt and androgen receptor pathways and arrest cell growth in the G2 phase. Thus, our results indicate the novel compound M-MeI to be a promising candidate for castration-resistant PCa therapy, and future studies investigating the mechanism of imidazopyridine inhibition may aid to the development of effective anti-PCa agents. C1 [Ingersoll, Matthew A.; Muniyan, Sakthivel; Dwyer, Jennifer G.; Batra, Surinder K.; Lin, Ming-Fong] Univ Nebraska Med Ctr, Dept Biochem & Mol Biol, Omaha, NE USA. [Lyons, Anastesia S.; D'Cunha, Napoleon; Bu, Xiu R.] Clark Atlanta Univ, Dept Chem, Atlanta, GA 30314 USA. [Robinson, Tashika] Clark Atlanta Univ, Dept Biol Sci, Atlanta, GA 30314 USA. [Hoelting, Kyle] Univ Nebraska Med Ctr, Coll Pharm, Omaha, NE USA. [Dwyer, Jennifer G.; Lin, Ming-Fong] Univ Nebraska Med Ctr, Urol Sect, Dept Surg, Omaha, NE USA. [Bu, Xiu R.] Clark Atlanta Univ, Lab Electopt Mat, Atlanta, GA USA. [Bu, Xiu R.] Clark Atlanta Univ, NASA, Ctr High Performance Polymers & Composites, Atlanta, GA USA. [Batra, Surinder K.; Lin, Ming-Fong] Univ Nebraska Med Ctr, Eppley Inst Res Canc & Allied Dis, Omaha, NE USA. [Lin, Ming-Fong] Kaohsiung Med Univ, Coll Pharm, Kaohsiung 807, Taiwan. RP Bu, XR (reprint author), Clark Atlanta Univ, Dept Chem, Atlanta, GA 30314 USA. EM JBu@cau.edu; mlin@unmc.edu OI Muniyan, Sakthivel/0000-0001-9405-7857 FU National Cancer Institute, National Institutes of Health [CA88184, CA138791]; Department of Defense PCa Training Grants [PC094594, PC121645]; University of Nebraska Medical Center Bridge Fund; UNMC Eppley Cancer Center grant [CA036727] FX This work was supported in part by the National Cancer Institute, National Institutes of Health [CA88184 (MFL), CA138791 (SKB)], Department of Defense PCa Training Grants [PC094594 (MFL), PC121645 (MFL)], and the University of Nebraska Medical Center Bridge Fund (MFL). The cell cycle analysis was performed at the UNMC Flow Cytometry Core Facility in part supported by UNMC Eppley Cancer Center grant [CA036727] (Ken Cowan). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 54 TC 1 Z9 2 U1 1 U2 2 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 JUN 29 PY 2015 VL 10 IS 6 AR e0131811 DI 10.1371/journal.pone.0131811 PG 20 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN1BL UT WOS:000358150400159 PM 26121643 ER PT J AU Restano, M Plaut, JJ Campbell, BA Gim, Y Nunes, D Bernardini, F Egan, A Seu, R Phillips, RJ AF Restano, Marco Plaut, Jeffrey J. Campbell, Bruce A. Gim, Yonggyu Nunes, Daniel Bernardini, Fabrizio Egan, Anthony Seu, Roberto Phillips, Roger J. TI Effects of the passage of Comet C/2013 A1 (Siding Spring) observed by the Shallow Radar (SHARAD) on Mars Reconnaissance Orbiter SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Comet Siding Spring; SHARAD ID IONS AB The close passage of Comet C/2013 A1 (Siding Spring) to Mars provided a unique opportunity to observe the interaction of cometary materials with the Martian ionosphere and atmosphere using the sounding radar SHARAD (SHAllow RADar) aboard Mars Reconnaissance Orbiter. In two nightside observations, acquired in the 10h following the closest approach, the SHARAD data reveal a significant increase of the total electron content (TEC). The observed TEC values are typical for daylight hours just after dawn or before sunset but are unprecedented this deep into the night. Results support two predictions indicating that cometary pickup O+ ions, or ions generated from the ablation of cometary dust, are responsible for the creation of an additional ion layer. C1 [Restano, Marco; Bernardini, Fabrizio; Seu, Roberto] Univ Roma La Sapienza, Dipartimento DIET, I-00185 Rome, Italy. [Plaut, Jeffrey J.; Gim, Yonggyu; Nunes, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Campbell, Bruce A.] Smithsonian Inst, Washington, DC 20560 USA. [Egan, Anthony] Southwest Res Inst, Space Operat Dept, Boulder, CO USA. [Phillips, Roger J.] Southwest Res Inst, Planetary Sci Directorate, Boulder, CO USA. RP Restano, M (reprint author), Univ Roma La Sapienza, Dipartimento DIET, Piazzale Aldo Moro 5, I-00185 Rome, Italy. EM marco.res@inwind.it FU ASI FX The Shallow Subsurface Radar (SHARAD) was provided by the Italian Space Agency (ASI), and its operations are led by the DIET Department, University of Rome "La Sapienza" under an ASI science contract. The Mars Reconnaissance Orbiter mission is managed by the Jet Propulsion Laboratory, California Institute of Technology, for the NASA Science Mission Directorate, Washington, DC. SHARAD data become available on the Geosciences Node of NASA's Planetary Data System (http://pds-geosciences.wustl.edu/) 6 months after the collection of the observations. NR 22 TC 9 Z9 9 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 28 PY 2015 VL 42 IS 12 BP 4663 EP 4669 DI 10.1002/2015GL064150 PG 7 WC Geosciences, Multidisciplinary SC Geology GA CM9CB UT WOS:000358002500001 ER PT J AU Benna, M Mahaffy, PR Grebowsky, JM Plane, JMC Yelle, RV Jakosky, BM AF Benna, M. Mahaffy, P. R. Grebowsky, J. M. Plane, J. M. C. Yelle, R. V. Jakosky, B. M. TI Metallic ions in the upper atmosphere of Mars from the passage of comet C/2013 A1 (Siding Spring) SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Comet Siding Spring; Mars; atmosphere; metal ion ID IONOSPHERE; DUST AB We report the first in situ detection of metal ions in the upper atmosphere of Mars resulting from the ablation of dust particles from comet Siding Spring. This detection was carried out by the Neutral Gas and Ion Mass Spectrometer on board the Mars Atmosphere and Volatile Evolution Mission. Metal ions of Na, Mg, Al, K, Ti, Cr, Mn, Fe, Co, Ni, Cu, and Zn, and possibly of Si, and Ca, were identified in the ion spectra collected at altitudes of similar to 185km. The measurements revealed that Na+ was the most abundant species, and that the remaining metals were depleted with respect to the CI (type 1 carbonaceous Chondrites) abundance of Na+. The temporal profile and abundance ratios of these metal ions suggest that the combined effects of dust composition, partial ablation, differential upward transport, and differences in the rates of formation and removal of these metal ions are responsible for the observed depletion. C1 [Benna, M.; Mahaffy, P. R.; Grebowsky, J. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Benna, M.] Univ Maryland Baltimore Cty, CSST, Baltimore, MD 21228 USA. [Plane, J. M. C.] Univ Leeds, Fac Math & Phys Sci, Leeds, W Yorkshire, England. [Yelle, R. V.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Jakosky, B. M.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. RP Benna, M (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM mehdi.benna@nasa.gov RI Plane, John/C-7444-2015; Benna, Mehdi/F-3489-2012 OI Plane, John/0000-0003-3648-6893; FU NASA; European Research Council [291332-CODITA] FX The MAVEN/NGIMS investigation was supported by NASA. Instrument testing and calibrations were completed at the Planetary Environment laboratory of NASA's Goddard Space Flight Center. We are grateful for the engineering/technical support especially from T. King (Instrument Manager), E. Weidner, E. Lyness, K. Patel, (Instrument Operations), and E. Raaen and M. Elrod (Calibration). J.M.C.P. acknowledges funding from the European Research Council (project 291332-CODITA). The NGIMS data supporting this article are provided in the supporting information Dataset S1. NR 30 TC 15 Z9 15 U1 0 U2 7 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 JUN 28 PY 2015 VL 42 IS 12 BP 4670 EP 4675 DI 10.1002/2015GL064159 PG 6 WC Geosciences, Multidisciplinary SC Geology GA CM9CB UT WOS:000358002500002 ER PT J AU Samsonov, AA Sergeev, VA Kuznetsova, MM Sibeck, DG AF Samsonov, A. A. Sergeev, V. A. Kuznetsova, M. M. Sibeck, D. G. TI Asymmetric magnetospheric compressions and expansions in response to impact of inclined interplanetary shock SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE inclined interplanetary shocks; sudden impulse; asymmetric magnetopause motion ID GEOMAGNETIC SUDDEN COMMENCEMENT; WIND; PROPAGATION; MOTION; MODEL AB We use global MHD simulations to model the magnetospheric response to an inclined shock that first strikes the duskside magnetosphere. The simulations predict several phenomena related specifically to the inclined shocks. The magnetospheric compression on the duskside exceeds that on the dawnside, and the geocentric distance to the dusk magnetopause varies in a simple step-like form. The compression on the dawnside is preceded and followed by expansions. For a moderately strong shock, the expansion magnitude reaches several R-E behind the terminator plane. The magnetopause and cross-tail currents in the magnetotail are significantly deformed during and after the shock passage. The position of the magnetotail magnetopause moves by more than 10R(E). This asymmetric magnetopause deformation is mainly related to a strong |V-y| downstream from the inclined shock. The magnetospheric expansion results in a decrease in the horizontal magnetic field at low-latitude stations, as confirmed by observations. C1 [Samsonov, A. A.; Sergeev, V. A.] St Petersburg State Univ, St Petersburg 199034, Russia. [Kuznetsova, M. M.; Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Samsonov, AA (reprint author), St Petersburg State Univ, St Petersburg 199034, Russia. EM andre.samsonov@gmail.com RI Samsonov, Andrey/I-7057-2012 OI Samsonov, Andrey/0000-0001-8243-1151 FU Russian Science Foundation [14-17-00072] FX Simulation results have been provided by the Community Coordinated Modeling Center (http://ccmc.gsfc.nasa.gov) at Goddard Space Flight Center. We have used results of the runs Andrey_Samsonov_041714_1, Andrey_Samsonov_020515_1, Andrey_Samsonov_030315_1, and Andrey_Samsonov_030315_1a. The SWMF was developed at the University of Michigan. Wind data are available from the Coordinated Data Analysis Web (CDAWeb). Ground magnetometer data are available from the World Data Center for Geomagnetism at Kyoto (http://wdc.kugi.kyoto-u.ac.jp/). This work was supported by the Russian Science Foundation grant 14-17-00072. A.A.S. thanks Gabor Toth for valuable comments. NR 27 TC 2 Z9 2 U1 1 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 JUN 28 PY 2015 VL 42 IS 12 BP 4716 EP 4722 DI 10.1002/2015GL064294 PG 7 WC Geosciences, Multidisciplinary SC Geology GA CM9CB UT WOS:000358002500008 ER PT J AU Meng, X Komjathy, A Verkhoglyadova, OP Yang, YM Deng, Y Mannucci, AJ AF Meng, X. Komjathy, A. Verkhoglyadova, O. P. Yang, Y. -M. Deng, Y. Mannucci, A. J. TI A new physics-based modeling approach for tsunami-ionosphere coupling SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE traveling ionospheric disturbance; ionospheric modeling; gravity wave; tsunami ID INTERNAL GRAVITY-WAVES; ATMOSPHERE; THERMOSPHERE AB Tsunamis can generate gravity waves propagating upward through the atmosphere, inducing total electron content (TEC) disturbances in the ionosphere. To capture this process, we have implemented tsunami-generated gravity waves into the Global Ionosphere-Thermosphere Model (GITM) to construct a three-dimensional physics-based model WP (Wave Perturbation)-GITM. WP-GITM takes tsunami wave properties, including the wave height, wave period, wavelength, and propagation direction, as inputs and time-dependently characterizes the responses of the upper atmosphere between 100km and 600km altitudes. We apply WP-GITM to simulate the ionosphere above the West Coast of the United States around the time when the tsunami associated with the March 2011 Tohuku-Oki earthquke arrived. The simulated TEC perturbations agree with Global Positioning System observations reasonably well. For the first time, a fully self-consistent and physics-based model has reproduced the GPS-observed traveling ionospheric signatures of an actual tsunami event. C1 [Meng, X.; Komjathy, A.; Verkhoglyadova, O. P.; Yang, Y. -M.; Mannucci, A. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Komjathy, A.] Univ New Brunswick, Dept Geodesy & Geomat Engn, Fredericton, NB, Canada. [Deng, Y.] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA. RP Meng, X (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM Xing.Meng@jpl.nasa.gov RI Meng, Xing/A-1929-2016; OI Verkhoglyadova, Olga/0000-0002-9295-9539 FU NASA; NASA's Science Mission Directorate in Washington [ROSES NNH10ZDA001N-GEOIM, NNH07ZDA001N-ESI] FX Portions of this work were done at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Funding for the research came from NASA's Science Mission Directorate in Washington (ROSES NNH10ZDA001N-GEOIM and NNH07ZDA001N-ESI). The authors would like to acknowledge Aaron Ridley at the University of Michigan for beneficial discussions during the model development. The authors also thank J. H. King, N. Papatashvilli at AdnetSystems, NASA GSFC, and CDAWeb for providing the OMNI data (http://cdaweb.gsfc.nasa.gov/istp\_public/). GPS measurements used for this research were obtained from stations in the Plate Boundary Observation network. The computational resources were provided by the JPL high-performance computing. NR 29 TC 6 Z9 6 U1 1 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 28 PY 2015 VL 42 IS 12 BP 4736 EP 4744 DI 10.1002/2015GL064610 PG 9 WC Geosciences, Multidisciplinary SC Geology GA CM9CB UT WOS:000358002500011 ER PT J AU Gurnett, DA Morgan, DD Persoon, AM Granroth, LJ Kopf, AJ Plaut, JJ Green, JL AF Gurnett, D. A. Morgan, D. D. Persoon, A. M. Granroth, L. J. Kopf, A. J. Plaut, J. J. Green, J. L. TI An ionized layer in the upper atmosphere of Mars caused by dust impacts from comet Siding Spring SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE cometary dust; comet Siding Spring; comet Siding Spring encounter with Mars; meteor impacts with Mars' atmosphere ID C/2013; IONOSPHERE AB We report the detection of a dense ionized layer in the upper atmosphere of Mars caused by the impact of dust from comet Siding Spring. The observations were made by the ionospheric radar sounder on the Mars Express spacecraft during two low-altitude passes approximately 7h and 14h after closest approach of the comet to Mars. During these passes an unusual transient layer of ionization was detected at altitudes of about 80 to 100km with peak electron densities of (1.5 to 2.5)x10(5)cm(-3), much higher than normally observed in the Martian ionosphere. From comparisons to previously observed ionization produced by meteors at Earth and Mars, we conclude that the layer was produced by dust from the comet impacting and ionizing the upper atmosphere of Mars. C1 [Gurnett, D. A.; Morgan, D. D.; Persoon, A. M.; Granroth, L. J.; Kopf, A. J.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Plaut, J. J.] Jet Prop Lab, Pasadena, CA USA. [Green, J. L.] NASA Headquarters, Washington, DC USA. RP Gurnett, DA (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. EM donald-gurnett@uiowa.edu FU NASA [1224107]; Jet Propulsion Laboratory FX All the data used in this study are available at http://www-pw.physics.uiowa.edu/marsx/Gurnett_etal_GRL_2015. The research at the University of Iowa was supported by NASA through contract 1224107 with the Jet Propulsion Laboratory. We thank the many members of the scientific, technical, and management teams at NASA Headquarters, the Jet Propulsion Laboratory, the European Space Agency, and the Italian Space Agency for their effort in planning the spacecraft operations required to successfully obtain these data. NR 17 TC 9 Z9 9 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 28 PY 2015 VL 42 IS 12 BP 4745 EP 4751 DI 10.1002/2015GL063726 PG 7 WC Geosciences, Multidisciplinary SC Geology GA CM9CB UT WOS:000358002500012 ER PT J AU Lundgren, P Samsonov, SV Velez, CML Ordonez, M AF Lundgren, Paul Samsonov, Sergey V. Lopez Velez, Cristian Mauricio Ordonez, Milton TI Deep source model for Nevado del Ruiz Volcano, Colombia, constrained by interferometric synthetic aperture radar observations SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Nevado del Ruiz Volcano; volcano deformation; InSAR ID LOCAL STRESSES; 1985 ERUPTION; NOVEMBER 13; DEFORMATION; INVERSION; ALGORITHM; CALDERA; ANDES AB Nevado del Ruiz is part of a large volcano complex in the northern Andes of Colombia. Interferometric synthetic aperture radar observations from the RADARSAT-2 satellite since 2011 show steady inflation of the volcano since 2012 at 3-4cm/yr. The broad (>20km) deformation pattern from both ascending and descending track data constrain source models for either point or spheroidal sources, both located at >14km beneath the surface (mean elevation 4.2km) and 10km SW of Nevado del Ruiz, below nearby Santa Isabel Volcano. Stress change computations for both sources in the context of a compressive regional stress indicate that dikes propagating from the source should become trapped in sills, possibly leading to a more complex pathway to the surface and explaining the significant lateral separation of the source and Nevado del Ruiz Volcano. C1 [Lundgren, Paul] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Samsonov, Sergey V.] Nat Resources Canada, Canada Ctr Mapping & Earth Observat, Ottawa, ON, Canada. [Lopez Velez, Cristian Mauricio; Ordonez, Milton] Colombian Geol Serv, Dept Geol Hazards, Manizales, Colombia. RP Lundgren, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM paul.lundgren@jpl.nasa.gov OI Samsonov, Sergey/0000-0002-6798-4847 FU National Aeronautics and Space Administration FX We thank the Canadian Space Agency for providing RADARSAT-2 data. We thank Freysteinn Sigmundsson for a thorough review. 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. Data used in the modeling and modeling software may be obtained at request by contacting the authors. NR 35 TC 4 Z9 4 U1 6 U2 19 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 JUN 28 PY 2015 VL 42 IS 12 BP 4816 EP 4823 DI 10.1002/2015GL063858 PG 8 WC Geosciences, Multidisciplinary SC Geology GA CM9CB UT WOS:000358002500022 ER PT J AU Mackie, CJ Candian, A Huang, XC Lee, TJ Tielens, AGGM AF Mackie, Cameron J. Candian, Alessandra Huang, Xinchuan Lee, Timothy J. Tielens, Alexander G. G. M. TI Linear transformation of anharmonic molecular force constants between normal and Cartesian coordinates SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID POTENTIAL-ENERGY SURFACE; VIBRATIONAL FREQUENCIES; SPECTROSCOPIC CONSTANTS; FIELD; C3H3+; CODE AB A full derivation of the analytic transformation of the quadratic, cubic, and quartic force constants from normal coordinates to Cartesian coordinates is given. Previous attempts at this transformation have resulted in non-linear transformations; however, for the first time, a simple linear transformation is presented here. Two different approaches have been formulated and implemented, one of which does not require prior knowledge of the translation-rotation eigenvectors from diagonalization of the Hessian matrix. The validity of this method is tested using two molecules H2O and c-C3H2D+. (C) 2015 AIP Publishing LLC. C1 [Mackie, Cameron J.; Candian, Alessandra; Tielens, Alexander G. G. M.] Leiden Observ, NL-2333 CA Leiden, Netherlands. [Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA. [Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Mackie, CJ (reprint author), Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands. EM mackie@strw.leidenuniv.nl RI Lee, Timothy/K-2838-2012; HUANG, XINCHUAN/A-3266-2013; OI Mackie, Cameron/0000-0003-2885-2021; Candian, Alessandra/0000-0002-5431-4449 FU European Research Council [246976]; Spinoza award; NASA [12-APRA12-0107]; NASA/SETI [NNX12AG96A]; SARA supercomputer center in Almere (NL) [MP-270-13] FX Helpful discussions with Dr. David Schwenke (NASA Ames), Professor Joel Bowman (Emory) and Professor Dr. Walter Thiel (Max-Planck) are gratefully acknowledged by the authors of this work. Studies of interstellar chemistry at Leiden Observatory that are supported through advanced European Research Council Grant No. 246976 and a Spinoza award. X.H. and T.J.L. gratefully acknowledge support from the NASA 12-APRA12-0107 grant. X.H. acknowledges the support from NASA/SETI Co-operative Agreement NNX12AG96A. The calculations were performed at the SARA supercomputer center in Almere (NL) under Project No. MP-270-13. NR 25 TC 5 Z9 5 U1 0 U2 4 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD JUN 28 PY 2015 VL 142 IS 24 AR 244107 DI 10.1063/1.4922891 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA CM3WE UT WOS:000357615100011 PM 26133410 ER PT J AU Jacobson, MZ Nghiem, SV Sorichetta, A Whitney, N AF Jacobson, Mark Z. Nghiem, Son V. Sorichetta, Alessandro Whitney, Natasha TI Ring of impact from the mega-urbanization of Beijing between 2000 and 2009 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE heat island; urban climate; urbanization; ozone ID URBAN HEAT-ISLAND; SHALLOW-WATER EQUATIONS; POTENTIAL ENSTROPHY; SIZE DISTRIBUTIONS; UNITED-STATES; GATOR-GCMM; SEA-ICE; LAND; MODEL; OPENSTREETMAP AB The transient climate, soil, and air quality impacts of the rapid urbanization of Beijing between 2000 and 2009 are investigated with three-dimensional computer model simulations. The simulations integrate a new satellite data set for urban extent and a geolocated crowd-sourced data set for road surface area and consider differences only in urban land cover and its physical properties. The simulations account for changes in meteorologically driven natural emissions but do not include changes in anthropogenic emissions resulting from urbanization and road network variations. The astounding urbanization, which quadrupled Beijing urban extent between 2000 and 2009 in terms of physical infrastructure change, created a ring of impact that decreased surface albedo, increased ground and near-surface air temperatures, increased vertical turbulent kinetic energy, and decreased the near-surface relative humidity and wind speed. The meteorological changes alone decreased near-surface particulate matter, nitrogen oxides (NOx), and many other chemicals due to vertical dilution but increased near-surface ozone due to the higher temperature and lower NO. Vertical dilution and wind stagnation increased elevated pollution layers and column aerosol extinction. In sum, the ring of impact around Beijing may have increased urban heating, dried soil, mixed pollutants vertically, aggravated air stagnation, and increased near-surface oxidant pollution even before accounting for changes in anthropogenic emissions. C1 [Jacobson, Mark Z.; Whitney, Natasha] Stanford Univ, Dept Civil & Environm Engn, Stanford, CA 94305 USA. [Nghiem, Son V.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Sorichetta, Alessandro] Univ Southampton, Geog & Environm, Southampton, Hants, England. [Sorichetta, Alessandro] Univ Southampton, Inst Life Sci, Southampton, Hants, England. RP Jacobson, MZ (reprint author), Stanford Univ, Dept Civil & Environm Engn, Stanford, CA 94305 USA. EM jacobson@stanford.edu FU NASA SMD Earth Sciences Division; National Aeronautics and Space Administration (NASA) Land-Cover and Land-Use Change (LCLUC) Program; Bill & Melinda Gates Foundation [OPP1106427, 1032350] FX This project received funding from the NASA SMD Earth Sciences Division and computer support from the NASA high-end computing center. The research carried out at the Jet Propulsion Laboratory, California Institute of Technology, was supported under a contract with the National Aeronautics and Space Administration (NASA) Land-Cover and Land-Use Change (LCLUC) Program. The research carried out at the Department of Geography and Environment, University of Southampton, was done in the framework of the WorldPop Project (www.worldpop.org.uk) and supported by funding from the Bill & Melinda Gates Foundation (OPP1106427 and 1032350). Data used to generate figures and the table for this paper are available freely from the corresponding author at jacobson@stanford.edu. NR 77 TC 2 Z9 2 U1 4 U2 37 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 JUN 27 PY 2015 VL 120 IS 12 BP 5740 EP 5756 DI 10.1002/2014JD023008 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CM8MX UT WOS:000357956800002 ER PT J AU Vogelmann, AM Fridlind, AM Toto, T Endo, S Lin, WY Wang, J Feng, S Zhang, YY Turner, DD Liu, YG Li, ZJ Xie, SC Ackerman, AS Zhang, MH Khairoutdinov, M AF Vogelmann, Andrew M. Fridlind, Ann M. Toto, Tami Endo, Satoshi Lin, Wuyin Wang, Jian Feng, Sha Zhang, Yunyan Turner, David D. Liu, Yangang Li, Zhijin Xie, Shaocheng Ackerman, Andrew S. Zhang, Minghua Khairoutdinov, Marat TI RACORO continental boundary layer cloud investigations: 1. Case study development and ensemble large-scale forcings SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE continental boundary layer cloud; observation-based modeling case studies; large-eddy simulation or LES; ensemble large-scale forcing; in situ aerosol size distribution and hygroscopicity; RACORO aircraft observations ID SOUTHERN GREAT-PLAINS; SINGLE-COLUMN MODELS; SHALLOW CUMULUS CONVECTION; OPERATIONAL RAMAN LIDAR; SGP CENTRAL FACILITY; LIQUID WATER PATH; DIURNAL-CYCLE; ECMWF MODEL; ATMOSPHERIC RADIATION; AEROSOL ACTIVATION AB Observation-based modeling case studies of continental boundary layer clouds have been developed to study cloudy boundary layers, aerosol influences upon them, and their representation in cloud- and global-scale models. Three 60 h case study periods span the temporal evolution of cumulus, stratiform, and drizzling boundary layer cloud systems, representing mixed and transitional states rather than idealized or canonical cases. Based on in situ measurements from the Routine AAF (Atmospheric Radiation Measurement (ARM) Aerial Facility) CLOWD (Clouds with Low Optical Water Depth) Optical Radiative Observations (RACORO) field campaign and remote sensing observations, the cases are designed with a modular configuration to simplify use in large-eddy simulations (LES) and single-column models. Aircraft measurements of aerosol number size distribution are fit to lognormal functions for concise representation in models. Values of the aerosol hygroscopicity parameter, , are derived from observations to be similar to 0.10, which are lower than the 0.3 typical over continents and suggestive of a large aerosol organic fraction. Ensemble large-scale forcing data sets are derived from the ARM variational analysis, European Centre for Medium-Range Weather Forecasts, and a multiscale data assimilation system. The forcings are assessed through comparison of measured bulk atmospheric and cloud properties to those computed in trial large-eddy simulations, where more efficient run times are enabled through modest reductions in grid resolution and domain size compared to the full-sized LES grid. Simulations capture many of the general features observed, but the state-of-the-art forcings were limited at representing details of cloud onset, and tight gradients and high-resolution transients of importance. Methods for improving the initial conditions and forcings are discussed. The cases developed are available to the general modeling community for studying continental boundary clouds. C1 [Vogelmann, Andrew M.; Toto, Tami; Endo, Satoshi; Lin, Wuyin; Wang, Jian; Liu, Yangang] Brookhaven Natl Lab, Upton, NY 11973 USA. [Fridlind, Ann M.; Ackerman, Andrew S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Feng, Sha; Li, Zhijin] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. [Feng, Sha; Li, Zhijin] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Zhang, Yunyan; Xie, Shaocheng] Lawrence Livermore Natl Lab, Livermore, CA USA. [Turner, David D.] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA. [Zhang, Minghua; Khairoutdinov, Marat] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA. RP Vogelmann, AM (reprint author), Brookhaven Natl Lab, Upton, NY 11973 USA. EM vogelmann@bnl.gov RI Xie, Shaocheng/D-2207-2013; Vogelmann, Andrew/M-8779-2014; Zhang, Yunyan/F-9783-2011; Liu, Yangang/H-6154-2011; Wang, Jian/G-9344-2011 OI Xie, Shaocheng/0000-0001-8931-5145; Vogelmann, Andrew/0000-0003-1918-5423; FU U.S. Department of Energy Science Office of Biological and Environmental Research Program; Earth System Modeling Program via the FASTER Project; Atmospheric System Research Program [SC00112704, DE-SC0006988, DE-SC0006898]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center; NASA Radiation Sciences Program; DOE ARM program; U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344] FX Data used in this article are from the U.S. Department of Energy SGP ARM Climate Research Facility (available from http://www.archive.arm.gov) and the AAF RACORO Campaign (available from http://www.arm.gov/campaigns/aaf2009racoro#data). We thank the entire RACORO team: the RACORO scientific steering committee, Haf Jonsson for the analysis and processing of the Twin Otter flight data and recalibration of the PCASP, the instrument mentors for their analysis and processing of data, and the DOE ARM Aerial Facility for its coordination of RACORO. We also especially acknowledge Don Collins for guidance using the SMPS data, David Cook provided informative discussions regarding the surface roughness length over the SGP, Krista Gaustad and Laura Riihimaki for special processing of MWRRET data for 8 May, and the Raman lidar mentor team of Chris Martin, John Goldsmith, and Rob Newsom for their efforts in maintaining the Raman lidar. Ozone measurements from the Ozone Monitoring Instrument (OMI) were provided by the NASA/GSFC TOMS Ozone Processing Team (OPT) and obtained via the ARM External Data Center. We would like to thank three anonymous reviewers for their thoughtful comments on the manuscript. This research was supported by the U.S. Department of Energy Science Office of Biological and Environmental Research Program under the following grants/contracts: the Earth System Modeling Program via the FASTER Project (A.M.V., T.T., W.L., S.E., Y.L., S.F., Z.L., M.Z., and M.K.), and the Atmospheric System Research Program via DE-SC00112704 (A.M.V., Y.L., and J.W.), DE-SC0006988 (A.M.F. and A.S.A.), and DE-SC0006898 (D.D.T.). A.M.F. and A.S.A. used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under contract DE-AC02-05CH11231, and the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center, and received additional support from the NASA Radiation Sciences Program. Work at LLNL was supported by the DOE ARM program and performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under contract DE-AC52-07NA27344 (Y.Z. and S.X.). NR 99 TC 6 Z9 6 U1 1 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 27 PY 2015 VL 120 IS 12 BP 5962 EP 5992 DI 10.1002/2014JD022713 PG 31 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CM8MX UT WOS:000357956800015 ER PT J AU Endo, S Fridlind, AM Lin, WY Vogelmann, AM Toto, T Ackerman, AS McFarquhar, GM Jackson, RC Jonsson, HH Liu, YG AF Endo, Satoshi Fridlind, Ann M. Lin, Wuyin Vogelmann, Andrew M. Toto, Tami Ackerman, Andrew S. McFarquhar, Greg M. Jackson, Robert C. Jonsson, Haflidi H. Liu, Yangang TI RACORO continental boundary layer cloud investigations: 2. Large-eddy simulations of cumulus clouds and evaluation with in situ and ground-based observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE LES; cumulus; cloud physics; RACORO; aircraft observations; boundary layer ID GENERAL HYDRODYNAMIC THEORY; ATMOSPHERIC RADIATION; AEROSOL ACTIVATION; FALL SPEED; PART I; PARAMETERIZATION; MICROPHYSICS; CONVECTION; PHASE; MODEL AB A 60h case study of continental boundary layer cumulus clouds is examined using two large-eddy simulation (LES) models. The case is based on observations obtained during the RACORO Campaign (Routine Atmospheric Radiation Measurement (ARM) Aerial Facility (AAF) Clouds with Low Optical Water Depths (CLOWD) Optical Radiative Observations) at the ARM Climate Research Facility's Southern Great Plains site. The LES models are driven by continuous large-scale and surface forcings and are constrained by multimodal and temporally varying aerosol number size distribution profiles derived from aircraft observations. We compare simulated cloud macrophysical and microphysical properties with ground-based remote sensing and aircraft observations. The LES simulations capture the observed transitions of the evolving cumulus-topped boundary layers during the three daytime periods and generally reproduce variations of droplet number concentration with liquid water content (LWC), corresponding to the gradient between the cloud centers and cloud edges at given heights. The observed LWC values fall within the range of simulated values; the observed droplet number concentrations are commonly higher than simulated, but differences remain on par with potential estimation errors in the aircraft measurements. Sensitivity studies examine the influences of bin microphysics versus bulk microphysics, aerosol advection, supersaturation treatment, and aerosol hygroscopicity. Simulated macrophysical cloud properties are found to be insensitive in this nonprecipitating case, but microphysical properties are especially sensitive to bulk microphysics supersaturation treatment and aerosol hygroscopicity. C1 [Endo, Satoshi; Lin, Wuyin; Vogelmann, Andrew M.; Toto, Tami; Liu, Yangang] Brookhaven Natl Lab, Upton, NY 11973 USA. [Fridlind, Ann M.; Ackerman, Andrew S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [McFarquhar, Greg M.; Jackson, Robert C.] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA. [Jonsson, Haflidi H.] Naval Postgrad Sch, Ctr Interdisciplinary Remotely Piloted Aircraft S, Monterey, CA USA. RP Endo, S (reprint author), Brookhaven Natl Lab, Upton, NY 11973 USA. EM sendo@bnl.gov RI Vogelmann, Andrew/M-8779-2014; Liu, Yangang/H-6154-2011; OI Vogelmann, Andrew/0000-0003-1918-5423; McFarquhar, Greg/0000-0003-0950-0135 FU U.S. Department of Energy Science Office of Biological and Environmental Research Program under the Earth System Modeling Program via the FASTER Project; U.S. Department of Energy Science Office of Biological and Environmental Research Program under the Atmospheric System Research Program [DE-SC00112704] FX This research was supported by the U.S. Department of Energy Science Office of Biological and Environmental Research Program under the Earth System Modeling Program via the FASTER Project (http://www.bnl.gov/faster/) and the Atmospheric System Research Program via DE-SC00112704. Observational data sets were obtained from the U.S. Department of Energy ARM Climate Research Facility (https://www.arm.gov/) and Oklahoma Mesonet (https://www.mesonet.org/). Processed forcing and observational data sets used for the 3 day case study are also aggregated as an ARM PI data product (http://iop.archive.arm.gov/arm-iop/0pi-data/vogelmann/racoro/case_studi es). The research utilized resources at the New York Center for Computational Sciences. Authors appreciate Marat Khairoutdinov for his helpful comments on LES configurations, Kwinten Van Weverberg and Hugh Morrison for providing and helping to use the two-moment microphysics scheme, and Peter Blossey for providing the interface to RRTM radiation scheme in WRF-FASTER. NR 60 TC 7 Z9 7 U1 1 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 27 PY 2015 VL 120 IS 12 BP 5993 EP 6014 DI 10.1002/2014JD022525 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CM8MX UT WOS:000357956800016 ER PT J AU Lin, WY Liu, YG Vogelmann, AM Fridlind, A Endo, S Song, H Feng, S Toto, T Li, ZJ Zhang, MH AF Lin, Wuyin Liu, Yangang Vogelmann, Andrew M. Fridlind, Ann Endo, Satoshi Song, Hua Feng, Sha Toto, Tami Li, Zhijin Zhang, Minghua TI RACORO continental boundary layer cloud investigations: 3. Separation of parameterization biases single-column model CAM5 simulations of shallow cumulus SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE continental shallow cumulus; single-column model; RACORO ID COMMUNITY ATMOSPHERE MODEL; FINE-RESOLUTION ANALYSES; DIURNAL CYCLE; CLIMATE SENSITIVITY; PART I; TROPICAL CONVECTION; SGP SITE; LAND; IMPACT; FLUX AB Climatically important low-level clouds are commonly misrepresented in climate models. The FAst-physics System TEstbed and Research (FASTER) Project has constructed case studies from the Atmospheric Radiation Measurement Climate Research Facility's Southern Great Plain site during the RACORO aircraft campaign to facilitate research on model representation of boundary-layer clouds. This paper focuses on using the single-column Community Atmosphere Model version 5 (SCAM5) simulations of a multi-day continental shallow cumulus case to identify specific parameterization causes of low-cloud biases. Consistent model biases among the simulations driven by a set of alternative forcings suggest that uncertainty in the forcing plays only a relatively minor role. In-depth analysis reveals that the model's shallow cumulus convection scheme tends to significantly under-produce clouds during the times when shallow cumuli exist in the observations, while the deep convective and stratiform cloud schemes significantly over-produce low-level clouds throughout the day. The links between model biases and the underlying assumptions of the shallow cumulus scheme are further diagnosed with the aid of large-eddy simulations and aircraft measurements, and by suppressing the triggering of the deep convection scheme. It is found that the weak boundary layer turbulence simulated is directly responsible for the weak cumulus activity and the simulated boundary layer stratiform clouds. Increased vertical and temporal resolutions are shown to lead to stronger boundary layer turbulence and reduction of low-cloud biases. C1 [Lin, Wuyin; Liu, Yangang; Vogelmann, Andrew M.; Endo, Satoshi; Song, Hua; Toto, Tami] Brookhaven Natl Lab, Biol Environm & Climate Sci Dept, Upton, NY 11973 USA. [Fridlind, Ann] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Feng, Sha; Li, Zhijin] Univ Calif Los Angeles, JIFRESSE, Los Angeles, CA USA. [Feng, Sha; Li, Zhijin] Jet Prop Lab, Pasadena, CA USA. [Feng, Sha; Li, Zhijin] JIFRESSE, Pasadena, CA USA. [Zhang, Minghua] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA. RP Lin, WY (reprint author), Brookhaven Natl Lab, Biol Environm & Climate Sci Dept, Upton, NY 11973 USA. EM wlin@bnl.gov RI Vogelmann, Andrew/M-8779-2014; Liu, Yangang/H-6154-2011 OI Vogelmann, Andrew/0000-0003-1918-5423; FU U.S. Department of Energy Science Office of Biological and Environmental Research Program under the Earth System Modeling Program via the FASTER Project; U.S. Department of Energy Science Office of Biological and Environmental Research Program under the Atmospheric System Research Program [DE-SC0012704] FX This research was supported by the U.S. Department of Energy Science Office of Biological and Environmental Research Program under the Earth System Modeling Program via the FASTER Project (http://www.bnl.gov/faster), and the Atmospheric System Research Program via DE-SC0012704. Data from the DOE's SGP ARM Climate Research Facility (http://www.archive.arm.gov/) are used in this work. His-Yen Ma and Shaocheng Xie provided the RACORO period CAPT simulations. NR 69 TC 3 Z9 3 U1 0 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 27 PY 2015 VL 120 IS 12 BP 6015 EP 6033 DI 10.1002/2014JD022524 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CM8MX UT WOS:000357956800017 ER PT J AU Kneifel, S von Lerber, A Tiira, J Moisseev, D Kollias, P Leinonen, J AF Kneifel, Stefan von Lerber, Annakaisa Tiira, Jussi Moisseev, Dmitri Kollias, Pavlos Leinonen, Jussi TI Observed relations between snowfall microphysics and triple-frequency radar measurements SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE triple-frequency radar; snowfall microphysics ID RAYLEIGH-GANS APPROXIMATION; ICE PARTICLES; SCATTERING PROPERTIES; AGGREGATE SNOWFLAKES; SOLID PRECIPITATION; FALLING SNOW; 225 GHZ; MICROWAVE; REFLECTIVITY; MODELS AB Recently published studies of triple-frequency radar observations of snowfall have demonstrated that naturally occurring snowflakes exhibit scattering signatures that are in some cases consistent with spheroidal particle models and in others can only be explained by complex aggregates. Until recently, no in situ observations have been available to investigate links between microphysical snowfall properties and their scattering properties. In this study, we investigate for the first time relations between collocated ground-based triple-frequency observations with in situ measurements of snowfall at the ground. The three analyzed snowfall cases obtained during a recent field campaign in Finland cover light to moderate snowfall rates with transitions from heavily rimed snow to open-structured, low-density snowflakes. The observed triple-frequency signatures agree well with the previously published findings from airborne radar observations. A rich spatiotemporal structure of triple-frequency observations throughout the cloud is observed during the three cases, which often seems to be related to riming and aggregation zones within the cloud. The comparison of triple-frequency signatures from the lowest altitudes with the ground-based in situ measurements reveals that in the presence of large (>5mm) snow aggregates, a bending away in the triple-frequency space from the curve of classical spheroid scattering models is always observed. Rimed particles appear along an almost horizontal line in the triple-frequency space, which was not observed before. Overall, the three case studies indicate a close connection of triple-frequency signatures and snow particle structure, bulk snowfall density, and characteristic size of the particle size distribution. C1 [Kneifel, Stefan; Kollias, Pavlos] McGill Univ, Dept Atmospher & Ocean Sci, Montreal, PQ, Canada. [von Lerber, Annakaisa; Moisseev, Dmitri] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. [Tiira, Jussi; Moisseev, Dmitri] Univ Helsinki, Dept Phys, Helsinki, Finland. [Leinonen, Jussi] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Kneifel, S (reprint author), McGill Univ, Dept Atmospher & Ocean Sci, Montreal, PQ, Canada. EM skneifel@meteo.uni-koeln.de RI Moisseev, Dmitri/A-3288-2008; Kneifel, Stefan/A-2044-2015; OI Moisseev, Dmitri/0000-0002-4575-0409; Kneifel, Stefan/0000-0003-2220-2968; Leinonen, Jussi/0000-0002-6560-6316; Tiira, Jussi/0000-0003-0851-3989 FU German Academic Exchange Service (DAAD); U.S. Department of Energy Atmospheric System Research (ASR) program; Finnish Funding Agency for Technology and Innovation (TEKES) [3155/31/2009]; Academy of Finland [255718]; Academy of Finland Finnish Center of Excellence program [272041]; Cluster for Energy and Environment through the Measurement, Monitoring, and Environmental Assessment (MMEA) research program; National Aeronautics and Space Administration FX We gratefully acknowledge the work of the Hyytiala station and ARM AMF2 personnel for the daily tasks with measurements, especially mentioning Matti Leskinen and Janne Levula (UH). We thank the NASA GPM ground validation program and Walter Petersen for providing ground-based precipitation instrumentation used in this study. We also thank Larry Bliven from NASA GSFC/Wallops Flight Facility for advices with PIP data interpretation and Jarmo Koistinen from Finnish Meteorological Institute (FMI) for his assistance with the synoptic analysis of the case studies. Work carried out by S.K. was supported by a Postdoctoral Fellowship from the German Academic Exchange Service (DAAD); additional funding for S.K. and P.K. was provided by the U.S. Department of Energy Atmospheric System Research (ASR) program. The research of A.L. was funded by grants 3155/31/2009 of the Finnish Funding Agency for Technology and Innovation (TEKES) and 255718 of the Academy of Finland. D.M. and J.T. were supported by the Academy of Finland Finnish Center of Excellence program (grant 272041) and the Cluster for Energy and Environment through the Measurement, Monitoring, and Environmental Assessment (MMEA) research program. The research of J.L. described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Peter Rodriguez from Environment Canada is acknowledged for sharing his ideas on snow measurement setup. We further thank Robin Hogan for his fruitful discussion and for providing his code to compute DWR using SSRG. We also acknowledge valuable discussions with Chris Westbrook, Jani Tyynela, and Maria Cadeddu. All remote sensing and in situ data from the BAECC campaign used in this study are available from the ARM data archive at http://www.archive.arm.gov. NR 49 TC 11 Z9 11 U1 2 U2 16 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 JUN 27 PY 2015 VL 120 IS 12 BP 6034 EP 6055 DI 10.1002/2015JD023156 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CM8MX UT WOS:000357956800018 ER PT J AU Ulbricht, G Mazin, BA Szypryt, P Walter, AB Bockstiegel, C Bumble, B AF Ulbricht, Gerhard Mazin, Benjamin A. Szypryt, Paul Walter, Alex B. Bockstiegel, Clint Bumble, Bruce TI Highly multiplexible thermal kinetic inductance detectors for x-ray imaging spectroscopy SO APPLIED PHYSICS LETTERS LA English DT Article AB For X-ray imaging spectroscopy, high spatial resolution over a large field of view is often as important as high energy resolution, but current X-ray detectors do not provide both in the same device. Thermal Kinetic Inductance Detectors (TKIDs) are being developed as they offer a feasible way to combine the energy resolution of transition edge sensors with pixel counts approaching CCDs and thus promise significant improvements for many X-ray spectroscopy applications. TKIDs are a variation of Microwave Kinetic Inductance Detectors (MKIDs) and share their multiplexibility: working MKID arrays with 2024 pixels have recently been demonstrated and much bigger arrays are under development. In this work, we present a TKID prototype, which is able to achieve an energy resolution of 75 eV at 5.9 keV, even though its general design still has to be optimized. We further describe TKID fabrication, characterization, multiplexing, and working principle and demonstrate the necessity of a data fitting algorithm in order to extract photon energies. With further design optimizations, we expect to be able to improve our TKID energy resolution to less than 10 eV at 5.9 keV. (C) 2015 AIP Publishing LLC. C1 [Ulbricht, Gerhard; Mazin, Benjamin A.; Szypryt, Paul; Walter, Alex B.; Bockstiegel, Clint] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Bumble, Bruce] NASA, Jet Prop Lab, Pasadena, CA 91125 USA. RP Ulbricht, G (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. EM ulbricht@physics.ucsb.edu RI Mazin, Ben/B-8704-2011; Ulbricht, Gerhard/P-7487-2016 OI Mazin, Ben/0000-0003-0526-1114; Ulbricht, Gerhard/0000-0002-6497-3763 FU NASA Space Technology Research Fellowship (NSTRF) program [NNX13AL70H]; NASA ROSES-APRA [NNX13AH34G, NNX14AI79G]; NSF FX The authors would like to thank the NASA Space Technology Research Fellowship (NSTRF) program (Grant No. NNX13AL70H) for funding graduate student P.S. The work was funded by the NASA ROSES-APRA detectors program Grant Nos. NNX13AH34G and NNX14AI79G. Devices were made at the UC Santa Barbara Nanofabrication Facility; a part of the NSF funded National Nanotechnology Infrastructure Network. NR 25 TC 5 Z9 5 U1 3 U2 9 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD JUN 22 PY 2015 VL 106 IS 25 AR 251103 DI 10.1063/1.4923096 PG 4 WC Physics, Applied SC Physics GA CL5XG UT WOS:000357036600003 ER PT J AU Ackermann, M Ajello, M Albert, A Anderson, B Atwood, WB Baldini, L Barbiellini, G Bastieri, D Bellazzini, R Bissaldi, E Blandford, RD Bloom, ED Bonino, R Bottacini, E Brandt, TJ Bregeon, J Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caputo, R Caragiulo, M Caraveo, PA Cecchi, C Charles, E Chekhtman, A Chiang, J Chiaro, G Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Cuoco, A Cutini, S D'Ammando, F de Angelis, A de Palma, F Desiante, R Digel, SW Di Venere, L Drell, PS Drlica-Wagner, A Favuzzi, C Fegan, SJ Franckowiak, A Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Giglietto, N Giordano, F Giroletti, M Godfrey, G Gomez-Vargas, GA Grenier, IA Grove, JE Guiriec, S Gustafsson, M Hewitt, JW Hill, AB Horan, D Johannesson, G Johnson, RP Kuss, M Larsson, S Latronico, L Li, J Li, L Longo, F Loparco, F Lovellette, MN Lubrano, P Malyshev, D Mayer, M Mazziotta, MN McEnery, JE Michelson, PF Mizuno, T Moiseev, AA Monzani, ME Morselli, A Murgia, S Nuss, E Ohsugi, T Orienti, M Orlando, E Ormes, JF Paneque, D Pesce-Rollins, M Piron, F Pivato, G Raino, S Rando, R Razzano, M Reimer, A Reposeur, T Ritz, S Sanchez-Conde, M Schulz, A Sgro, C Siskind, EJ Spada, F Spandre, G Spinelli, P Tajima, H Takahashi, H Thayer, JB Tibaldo, L Torres, DF Tosti, G Troja, E Vianello, G Werner, M Winer, BL Wood, KS Wood, M Zaharijas, G Zimmer, S AF Ackermann, M. Ajello, M. Albert, A. Anderson, B. Atwood, W. B. Baldini, L. Barbiellini, G. Bastieri, D. Bellazzini, R. Bissaldi, E. Blandford, R. D. Bloom, E. D. Bonino, R. Bottacini, E. Brandt, T. J. Bregeon, J. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caputo, R. Caragiulo, M. Caraveo, P. A. Cecchi, C. Charles, E. Chekhtman, A. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Cuoco, A. Cutini, S. D'Ammando, F. de Angelis, A. de Palma, F. Desiante, R. Digel, S. W. Di Venere, L. Drell, P. S. Drlica-Wagner, A. Favuzzi, C. Fegan, S. J. Franckowiak, A. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Giglietto, N. Giordano, F. Giroletti, M. Godfrey, G. Gomez-Vargas, G. A. Grenier, I. A. Grove, J. E. Guiriec, S. Gustafsson, M. Hewitt, J. W. Hill, A. B. Horan, D. Johannesson, G. Johnson, R. P. Kuss, M. Larsson, S. Latronico, L. Li, J. Li, L. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Malyshev, D. Mayer, M. Mazziotta, M. N. McEnery, J. E. Michelson, P. F. Mizuno, T. Moiseev, A. A. Monzani, M. E. Morselli, A. Murgia, S. Nuss, E. Ohsugi, T. Orienti, M. Orlando, E. Ormes, J. F. Paneque, D. Pesce-Rollins, M. Piron, F. Pivato, G. Raino, S. Rando, R. Razzano, M. Reimer, A. Reposeur, T. Ritz, S. Sanchez-Conde, M. Schulz, A. Sgro, C. Siskind, E. J. Spada, F. Spandre, G. Spinelli, P. Tajima, H. Takahashi, H. Thayer, J. B. Tibaldo, L. Torres, D. F. Tosti, G. Troja, E. Vianello, G. Werner, M. Winer, B. L. Wood, K. S. Wood, M. Zaharijas, G. Zimmer, S. TI Updated search for spectral lines from Galactic dark matter interactions with pass 8 data from the Fermi Large Area Telescope SO PHYSICAL REVIEW D LA English DT Article ID CANDIDATES; GALAXIES; DENSITY AB Dark matter in the Milky Way may annihilate directly into. rays, producing a monoenergetic spectral line. Therefore, detecting such a signature would be strong evidence for dark matter annihilation or decay. We search for spectral lines in the Fermi Large Area Telescope observations of the Milky Way halo in the energy range 200 MeV-500 GeV using analysis methods from our most recent line searches. The main improvements relative to previous works are our use of 5.8 years of data reprocessed with the Pass 8 event-level analysis and the additional data resulting from the modified observing strategy designed to increase exposure of the Galactic center region. We search in five sky regions selected to optimize sensitivity to different theoretically motivated dark matter scenarios and find no significant detections. In addition to presenting the results from our search for lines, we also investigate the previously reported tentative detection of a line at 133 GeV using the new Pass 8 data. C1 [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA. [Albert, A.; Baldini, L.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chekhtman, A.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Franckowiak, A.; Funk, S.; Godfrey, G.; Hill, A. B.; Malyshev, D.; Michelson, P. F.; Monzani, M. E.; Orlando, E.; Paneque, D.; Reimer, A.; Tajima, H.; Thayer, J. B.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Albert, A.; Baldini, L.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Franckowiak, A.; Funk, S.; Godfrey, G.; Hill, A. B.; Malyshev, D.; Michelson, P. F.; Monzani, M. E.; Orlando, E.; Paneque, D.; Reimer, A.; Tajima, H.; Thayer, J. B.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Atwood, W. B.; Caputo, R.; Johnson, R. P.; Ritz, S.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Atwood, W. B.; Caputo, R.; Johnson, R. P.; Ritz, S.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Baldini, L.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Barbiellini, G.; Desiante, R.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Chiaro, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bellazzini, R.; Kuss, M.; Pesce-Rollins, M.; Pivato, G.; Razzano, M.; Sgro, C.; Spada, F.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Bissaldi, E.; Caragiulo, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bonino, R.; Cuoco, A.; Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Bonino, R.; Cuoco, A.] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy. [Brandt, T. J.; Guiriec, S.; McEnery, J. E.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bregeon, J.; Cohen-Tanugi, J.; Nuss, E.; Piron, F.] Univ Montpellier, CNRS, IN2P3, Lab Univ & Particules Montpellier, Montpellier, France. [Bruel, P.; Fegan, S. J.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Caliandro, G. A.] CIFS, I-10133 Turin, Italy. [Caraveo, P. A.] INAF, Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Cecchi, C.; Ciprini, S.; Cutini, S.; Gasparrini, D.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Cecchi, C.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, 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.] ASI Sci Data Ctr, I-00133 Rome, Italy. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Roma, Italy. [Anderson, B.; Conrad, J.; Larsson, S.; Sanchez-Conde, M.; Zimmer, S.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Anderson, B.; Conrad, J.; Cuoco, A.; Larsson, S.; Li, L.; Sanchez-Conde, M.; Zimmer, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden. [D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF, Ist Radioastron, I-40129 Bologna, Italy. [D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.] Ist Nazl Fis Nucl, Grp Collegato Udine, Sez Trieste, I-33100 Udine, Italy. [de Palma, F.] Univ Telemat Pegaso, I-80132 Naples, Italy. [Desiante, R.] Univ Udine, I-33100 Udine, Italy. [Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Drlica-Wagner, A.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA. [Fukazawa, Y.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Gomez-Vargas, G. A.; Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Gomez-Vargas, G. A.] Pontificia Univ Catolica Chile, Dept Fis, Santiago, Chile. [Grenier, I. A.] CEA Saclay, Univ Paris Diderot, CNRS, IRFU,Serv Astrophys,Lab AIM, F-91191 Gif Sur Yvette, France. [Grove, J. E.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Gustafsson, M.] Univ Gottingen, Fac Phys, Inst Theoret Phys, D-37077 Gottingen, Germany. [Hewitt, J. W.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Hewitt, J. W.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Hewitt, J. W.; Moiseev, A. A.] CRESST, Greenbelt, MD 20771 USA. [Hewitt, J. W.; Moiseev, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Li, J.; Torres, D. F.] CSIC, IEEC, Inst Space Sci, E-08193 Barcelona, Spain. [Li, L.] AlbaNova, KTH Royal Inst Technol, Dept Phys, SE-10691 Stockholm, Sweden. [McEnery, J. E.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [Murgia, S.] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Reimer, A.; Werner, M.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Werner, M.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Reposeur, T.] Univ Bordeaux 1, CNRS, Ctr Etud Nucl Bordeaux Gradignan, IN2P3, F-33175 Gradignan, France. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Torres, D. F.] ICREA, Barcelona, Spain. [Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Dept Phys, Columbus, OH 43210 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 Gor, Lab Astroparticle Phys, SI-5000 Nova Gorica, Slovenia. RP Ackermann, M (reprint author), DESY, D-15738 Zeuthen, Germany. EM aalbert@slac.stanford.edu; rcaputo@ucsc.edu RI Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Bonino, Raffaella/S-2367-2016; Di Venere, Leonardo/C-7619-2017; Morselli, Aldo/G-6769-2011; Funk, Stefan/B-7629-2015; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Sgro, Carmelo/K-3395-2016; Bissaldi, Elisabetta/K-7911-2016; OI Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; Zaharijas, Gabrijela/0000-0001-8484-7791; SPINELLI, Paolo/0000-0001-6688-8864; Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; Bonino, Raffaella/0000-0002-4264-1215; Torres, Diego/0000-0002-1522-9065; Di Venere, Leonardo/0000-0003-0703-824X; Morselli, Aldo/0000-0002-7704-9553; Funk, Stefan/0000-0002-2012-0080; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Bissaldi, Elisabetta/0000-0001-9935-8106; Hill, Adam/0000-0003-3470-4834 FU Royal Swedish Academy of Sciences through the K. A. Wallenberg Foundation; NASA postdoctoral fellowship; Marie Curie International Outgoing Fellowship for Career Development through the FP7 Programme [257861]; 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), the High Energy Accelerator Research Organization (KEK), and the 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. B. Anderson is supported by the Royal Swedish Academy of Sciences through a grant from the K. A. Wallenberg Foundation. S. G. received support from a NASA postdoctoral fellowship. A. B. H. is supported by the Marie Curie International Outgoing Fellowship for Career Development through the FP7/20072013 Programme (Grant No. 257861). M. R. received funding from the Italian Ministry of Education, University and Research (MIUR) through Contract No. FIRB-2012-RBFR12PM1F. NR 38 TC 66 Z9 66 U1 0 U2 9 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 JUN 22 PY 2015 VL 91 IS 12 AR 122002 DI 10.1103/PhysRevD.91.122002 PG 19 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA CK9TY UT WOS:000356583600002 ER PT J AU Clementel, N Madura, TI Kruip, CJH Paardekooper, JP AF Clementel, N. Madura, T. I. Kruip, C. J. H. Paardekooper, J. -P. TI 3D radiative transfer simulations of Eta Carinae's inner colliding winds - II. Ionization structure of helium at periastron SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE hydrodynamics; radiative transfer; binaries: close; stars: individual: Eta Carinae; stars: mass-loss; stars: winds, outflows ID SIMPLEX ALGORITHM; COMPANION; EVENTS; VARIABILITY; PARAMETERS; COLLISION; EMISSION AB Spectral observations of the massive colliding wind binary Eta Carinae show phase-dependent variations, in intensity and velocity, of numerous helium emission and absorption lines throughout the entire 5.54-yr orbit. Approaching periastron, the 3D structure of the wind-wind interaction region (WWIR) gets highly distorted due to the eccentric (e similar to 0.9) binary orbit. The secondary star (eta(B)) at these phases is located deep within the primary's dense wind photosphere. The combination of these effects is thought to be the cause of the particularly interesting features observed in the helium lines at periastron. We perform 3D radiative transfer simulations of eta Car's interacting winds at periastron. Using the SIMPLEX radiative transfer algorithm, we post-process output from 3D smoothed particle hydrodynamic simulations of the inner 150 au of the eta Car system for two different primary star mass-loss rates (M-eta A)(.) Using previous results from simulations at apastron as a guide for the initial conditions, we compute 3D helium ionization maps. We find that, for higher. M-eta A, (eta B) He0+-ionizing photons are not able to penetrate into the pre-shock primary wind. He+ due to eta(B) is only present in a thin layer along the leading arm of the WWIR and in a small region close to the stars. Lowering. M-eta A allows eta(B)'s ionizing photons to reach the expanding unshocked secondary wind on the apastron side of the system, and create a low fraction of He+ in the pre-shock primary wind. With apastron on our side of the system, our results are qualitatively consistent with the observed variations in strength and radial velocity of eta Car's helium emission and absorption lines, which helps better constrain the regions where these lines arise. C1 [Clementel, N.; Kruip, C. J. H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Clementel, N.] S African Astron Observ, ZA-7935 Observatory, South Africa. [Madura, T. I.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Paardekooper, J. -P.] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Paardekooper, J. -P.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. RP Clementel, N (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM clementel@saao.ac.za FU NASA FX TIM is supported by an appointment to the NASA Postdoctoral Programme at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 34 TC 8 Z9 8 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 21 PY 2015 VL 450 IS 2 BP 1388 EP 1398 DI 10.1093/mnras/stv696 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6LB UT WOS:000356338500018 ER PT J AU Russell, TD Miller-Jones, JCA Curran, PA Soria, R Altamirano, D Corbel, S Coriat, M Moin, A Russell, DM Sivakoff, GR Slaven-Blair, TJ Belloni, TM Fender, RP Heinz, S Jonker, PG Krimm, HA Kording, EG Maitra, D Markoff, S Middleton, M Migliari, S Remillard, RA Rupen, MP Sarazin, CL Tetarenko, AJ Torres, MAP Tudose, V Tzioumis, AK AF Russell, T. D. Miller-Jones, J. C. A. Curran, P. A. Soria, R. Altamirano, D. Corbel, S. Coriat, M. Moin, A. Russell, D. M. Sivakoff, G. R. Slaven-Blair, T. J. Belloni, T. M. Fender, R. P. Heinz, S. Jonker, P. G. Krimm, H. A. Koerding, E. G. Maitra, D. Markoff, S. Middleton, M. Migliari, S. Remillard, R. A. Rupen, M. P. Sarazin, C. L. Tetarenko, A. J. Torres, M. A. P. Tudose, V. Tzioumis, A. K. TI Radio monitoring of the hard state jets in the 2011 outburst of MAXI J1836-194 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE proper motions; stars: individual: MAXI J1836; 194; ISM: jets and outflows; radio continuum: stars; X-rays: binaries ID BLACK-HOLE CANDIDATE; X-RAY BINARIES; VLBA CALIBRATOR SURVEY; SPECTRAL ENERGY-DISTRIBUTION; COMPACT OBJECT FORMATION; ACTIVE GALACTIC NUCLEUS; BROAD-BAND SPECTRUM; GX 339-4; RELATIVISTIC JETS; INTERNAL SHOCKS AB MAXI J1836-194 is a Galactic black hole candidate X-ray binary that was discovered in 2011 when it went into outburst. In this paper, we present the full radio monitoring of this system during its 'failed' outburst, in which the source did not complete a full set of state changes, only transitioning as far as the hard intermediate state. Observations with the Karl G. Jansky Very Large Array (VLA) and Australia Telescope Compact Array (ATCA) show that the jet properties changed significantly during the outburst. The VLA observations detected linearly polarized emission at a level of similar to 1 per cent early in the outburst, increasing to similar to 3 per cent as the outburst peaked. High-resolution images with the Very Long Baseline Array (VLBA) show an similar to 15 mas jet along the position angle -21 +/- 2 degrees, in agreement with the electric vector position angle found from our polarization results (-21 +/- 4 degrees), implying that the magnetic field is perpendicular to the jet. Astrometric observations suggest that the system required an asymmetric natal kick to explain its observed space velocity. Comparing quasisimultaneous X-ray monitoring with the 5 GHz VLA observations from the 2011 outburst shows an unusually steep hard-state radio/X-ray correlation of L-R alpha L-X(1.8 +/- 0.2), where L-R and LX denote the radio and X-ray luminosities, respectively. With ATCA and Swift monitoring of the source during a period of re-brightening in 2012, we show that the system lay on the same steep correlation. Due to the low inclination of this system, we then investigate the possibility that the observed correlation may have been steepened by variable Doppler boosting. C1 [Russell, T. D.; Miller-Jones, J. C. A.; Curran, P. A.; Soria, R.; Slaven-Blair, T. J.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Altamirano, D.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Corbel, S.] Univ Paris Diderot, CNRS INSU, Lab AIM CEA IRFU, CEA DSM IRFU SAp, F-91191 Gif Sur Yvette, France. [Corbel, S.] Univ Orleans, CNRS INSU, Stn Radioastron Nancay, Observ Paris,USR 704,OSUC, F-18330 Nancay, France. [Coriat, M.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa. [Moin, A.; Russell, D. M.] New York Univ Abu Dhabi, Abu Dhabi, U Arab Emirates. [Moin, A.] Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Sivakoff, G. R.; Tetarenko, A. J.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Belloni, T. M.] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. [Fender, R. P.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Heinz, S.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Jonker, P. G.; Torres, M. A. P.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonker, P. G.; Koerding, E. G.; Torres, M. A. P.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Krimm, H. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krimm, H. A.] USRA, Columbia, MD 21044 USA. [Maitra, D.] Wheaton Coll, Dept Phys & Astron, Norton, MA 02766 USA. [Markoff, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Middleton, M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Migliari, S.] Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Spain. [Migliari, S.] Univ Barcelona, Inst Cosm Sci, E-08028 Barcelona, Spain. [Remillard, R. A.] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Rupen, M. P.] Herzberg Astron & Astrophys, Natl Res Council, Penticton, BC V2A 6J9, Canada. [Rupen, M. P.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Tudose, V.] Inst Space Sci, RO-077125 Bucharest, Romania. [Tzioumis, A. K.] CSIRO Astron & Space Sci, ATNF, Epping, NSW 1710, Australia. RP Russell, TD (reprint author), Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia. EM thomas.russell@icrar.org RI Miller-Jones, James/B-2411-2013; Sivakoff, Gregory/G-9602-2011; Tudose, Valeriu/F-8976-2010; OI Miller-Jones, James/0000-0003-3124-2814; Sivakoff, Gregory/0000-0001-6682-916X; Russell, David/0000-0002-3500-631X; Russell, Thomas/0000-0001-6958-8891 FU Australian Research Council [DP 120102393]; Royal Society; French Research National Agency: CHAOS project [ANR-12-BS05-0009]; Uni-vEarthS Labex program of Sorbonne Paris Cite [ANR-10-LABX-0023, ANR-11-IDEX-0005-02]; NSERC Discovery Grant; INAF-PRIN [2012-6]; Spanish Ministerio de Economia y Competitividad; European Social Funds through a Ramon y Cajal Fellowship; Spanish Ministerio de Ciencia e Innovacion [AYA2013-47447-C03-1-P]; state government of Western Australia; Commonwealth of Australia FX We would like to thank the anonymous referee for their helpful comments and suggestions. We also thank Tom Maccarone for useful discussions. This research was supported under the Australian Research Council's Discovery Projects funding scheme (project number DP 120102393). DA acknowledges support from the Royal Society. SC acknowledges funding support from the French Research National Agency: CHAOS project ANR-12-BS05-0009 (http://www.chaos-project.fr) and financial support from the Uni-vEarthS Labex program of Sorbonne Paris Cite (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02). GRS and AJT are supported by an NSERC Discovery Grant. TMB acknowledges support from INAF-PRIN 2012-6. SM acknowledges support by the Spanish Ministerio de Economia y Competitividad and European Social Funds through a Ramon y Cajal Fellowship and the Spanish Ministerio de Ciencia e Innovacion (SM; grant AYA2013-47447-C03-1-P). This research has made use of NASA's Astrophysics Data System. The International Centre for Radio Astronomy Research is a joint venture between Curtin University and the University of Western Australia, funded by the state government of Western Australia and the joint venture partners. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The ATCA is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. NR 118 TC 9 Z9 9 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 21 PY 2015 VL 450 IS 2 BP 1745 EP 1759 DI 10.1093/mnras/stv723 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6LB UT WOS:000356338500047 ER PT J AU Tregloan-Reed, J Southworth, J Burgdorf, M Novati, SC Dominik, M Finet, F Jorgensen, UG Maier, G Mancini, L Prof, S Ricci, D Snodgrass, C Bozza, V Browne, P Dodds, P Gerner, T Harpsoe, K Hinse, TC Hundertmark, M Kains, N Kerins, E Liebig, C Penny, MT Rahvar, S Sahu, K Scarpetta, G Schafer, S Schonebeck, F Skottfelt, J Surdej, J AF Tregloan-Reed, Jeremy Southworth, John Burgdorf, M. Novati, S. Calchi Dominik, M. Finet, F. Jorgensen, U. G. Maier, G. Mancini, L. Prof, S. Ricci, D. Snodgrass, C. Bozza, V. Browne, P. Dodds, P. Gerner, T. Harpsoe, K. Hinse, T. C. Hundertmark, M. Kains, N. Kerins, E. Liebig, C. Penny, M. T. Rahvar, S. Sahu, K. Scarpetta, G. Schaefer, S. Schoenebeck, F. Skottfelt, J. Surdej, J. TI Transits and starspots in the WASP-6 planetary system SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; stars: fundamental parameters; stars: individual: WASP-6; planetary systems; starspots ID SPIN-ORBIT ALIGNMENT; HIGH-PRECISION PHOTOMETRY; EXTRASOLAR PLANETS; DIFFERENTIAL EVOLUTION; TRANSMISSION SPECTRUM; EXOPLANETARY SYSTEM; CIRCUMBINARY PLANET; PHYSICAL-PROPERTIES; HABITABLE ZONE; HOT JUPITERS AB We present updates to PRISM, a photometric transit-starspot model, and GEMC, a hybrid optimization code combining MCMC and a genetic algorithm. We then present high-precision photometry of four transits in the WASP-6 planetary system, two of which contain a starspot anomaly. All four transits were modelled using PRISM and GEMC, and the physical properties of the system calculated. We find the mass and radius of the host star to be 0.836 +/- 0.063 M-circle dot and 0.864 +/- 0.024 R-circle dot, respectively. For the planet, we find a mass of 0.485 +/- 0.027M(Jup), a radius of 1.230 +/- 0.035 R-Jup and a density of 0.244 +/- 0.014 rho(Jup). These values are consistent with those found in the literature. In the likely hypothesis that the two spot anomalies are caused by the same starspot or starspot complex, we measure the stars rotation period and velocity to be 23.80 +/- 0.15 d and 1.78 +/- 0.20 km s(-1), respectively, at a colatitude of 75.8 degrees. We find that the sky-projected angle between the stellar spin axis and the planetary orbital axis is lambda = 7.2 degrees +/- 3.7 degrees, indicating axial alignment. Our results are consistent with and more precise than published spectroscopic measurements of the Rossiter-McLaughlin effect. These results suggest thatWASP-6 b formed at amuch greater distance from its host star and suffered orbital decay through tidal interactions with the protoplanetary disc. C1 [Tregloan-Reed, Jeremy] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. [Tregloan-Reed, Jeremy; Southworth, John] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Burgdorf, M.] Univ Hamburg, Meteorol Inst, D-20146 Hamburg, Germany. [Novati, S. Calchi] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Novati, S. Calchi; Bozza, V.; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, I-84084 Fisciano, SA, Italy. [Novati, S. Calchi; Scarpetta, G.] IIASS, I-84019 Vietri Sul Mare, SA, Italy. [Dominik, M.; Browne, P.; Dodds, P.; Hundertmark, M.; Liebig, C.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Finet, F.; Surdej, J.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Finet, F.] Aryabhatta Res Inst Observat Sci ARIES, Naini Tal 263129, Uttarakhand, India. [Jorgensen, U. G.; Harpsoe, K.; Skottfelt, J.] Univ Copenhagen, Niels Bohr Inst, DK-1350 Copenhagen K, Denmark. [Jorgensen, U. G.; Harpsoe, K.; Skottfelt, J.] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Maier, G.; Prof, S.; Gerner, T.; Schoenebeck, F.] Heidelberg Univ, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany. [Mancini, L.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Ricci, D.] Univ Nacl Autonoma Mexico, Inst Astron, Observ Astron Nacl, Ensenada 22860, Baja California, Mexico. [Ricci, D.] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Ricci, D.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Snodgrass, C.] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England. [Bozza, V.; Scarpetta, G.] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy. [Hinse, T. C.] Korea Astron & Space Sci Inst, Daejeon 305348, South Korea. [Hinse, T. C.] Armagh Observ, Armagh BT61 9DG, North Ireland. [Kains, N.; Sahu, K.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kerins, E.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Penny, M. T.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran, Iran. [Schaefer, S.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. RP Tregloan-Reed, J (reprint author), NASA Ames Res Ctr, Moffett Field, CA 94035 USA. EM jeremy.j.tregloan-reed@nasa.gov RI Hundertmark, Markus/C-6190-2015; Rahvar, Sohrab/A-9350-2008; OI Hundertmark, Markus/0000-0003-0961-5231; Rahvar, Sohrab/0000-0002-7084-5725; Dominik, Martin/0000-0002-3202-0343; Ricci, Davide/0000-0002-9790-0552; Snodgrass, Colin/0000-0001-9328-2905 FU The Danish Council for Independent Research (FNU); Department of Culture, Arts Leisure (DCAL); STFC; ORAU (Oak Ridge Associated Universities); NASA; Spanish Ministry of Economy and Competitiveness (MINECO) [MINECO SEV-2011-0187]; Communaute francaise de Belgique - Actions de recherche concertees - Academie Wallonie-Europe FX We like to thank the anonymous referee for the helpful comments on the manuscript. The operation of the Danish 1.54-m telescope at ESOs La Silla observatory is financed by a grant to UGJ from The Danish Council for Independent Research (FNU). Research at the Armagh Observatory is funded by the Department of Culture, Arts & Leisure (DCAL). JTR acknowledges financial support from STFC in the form of a PhD Studentship (the majority of this work) and also acknowledges financial support from ORAU (Oak Ridge Associated Universities) and NASA in the form of a Post-Doctoral Programme (NPP) Fellowship. JS acknowledges financial support from STFC in the form of an Advanced Fellowship. DR acknowledges financial support from the Spanish Ministry of Economy and Competitiveness (MINECO) under the 2011 Severo Ochoa Programme MINECO SEV-2011-0187. FF, DR (boursier FRIA) and J Surdej acknowledge support from the Communaute francaise de Belgique - Actions de recherche concertees - Academie Wallonie-Europe. NR 67 TC 9 Z9 9 U1 0 U2 8 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 21 PY 2015 VL 450 IS 2 BP 1760 EP 1769 DI 10.1093/mnras/stv730 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6LB UT WOS:000356338500048 ER PT J AU Ade, PAR Aikin, RW Barkats, D Benton, SJ Bischoff, CA Bock, JJ Bradford, KJ Brevik, JA Buder, I Bullock, E Dowell, CD Duband, L Filippini, JP Fliescher, S Golwala, SR Halpern, M Hasselfield, M Hildebrandt, SR Hilton, GC Hui, H Irwin, KD Kang, JH Karkare, KS Kaufman, JP Keating, BG Kefeli, S Kernasovskiy, SA Kovac, JM Kuo, CL Leitch, EM Lueker, M Megerian, KG Netterfield, CB Nguyen, HT O'Brient, R Ogburn, RW Orlando, A Pryke, C Richter, S Schwarz, R Sheehy, CD Staniszewski, ZK Sudiwala, RV Teply, GP Thompson, K Tolan, JE Turner, AD Vieregg, AG Weber, AC Wong, CL Yoon, KW AF Ade, P. A. R. Aikin, R. W. Barkats, D. Benton, S. J. Bischoff, C. A. Bock, J. J. Bradford, K. J. Brevik, J. A. Buder, I. Bullock, E. Dowell, C. D. Duband, L. Filippini, J. P. Fliescher, S. Golwala, S. R. Halpern, M. Hasselfield, M. Hildebrandt, S. R. Hilton, G. C. Hui, H. Irwin, K. D. Kang, J. H. Karkare, K. S. Kaufman, J. P. Keating, B. G. Kefeli, S. Kernasovskiy, S. A. Kovac, J. M. Kuo, C. L. Leitch, E. M. Lueker, M. Megerian, K. G. Netterfield, C. B. Nguyen, H. T. O'Brient, R. Ogburn, R. W. Orlando, A. Pryke, C. Richter, S. Schwarz, R. Sheehy, C. D. Staniszewski, Z. K. Sudiwala, R. V. Teply, G. P. Thompson, K. Tolan, J. E. Turner, A. D. Vieregg, A. G. Weber, A. C. Wong, C. L. Yoon, K. W. CA BICEP2 Keck Array Collaborations TI BICEP2/KECK ARRAY. IV. OPTICAL CHARACTERIZATION AND PERFORMANCE OF THE BICEP2 AND KECK ARRAY EXPERIMENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; gravitational waves; inflation; polarization ID GRAVITY-WAVES; POLARIZATION; POLARIMETER AB BICEP2. and the Keck Array. are polarization-sensitive microwave telescopes that observe the cosmic microwave background (CMB) from the South Pole at degree angular scales in search of a signature of inflation imprinted as B-mode polarization in the CMB. BICEP2. was deployed in late 2009, observed for three years until the end of 2012 at 150 GHz with 512 antenna-coupled transition edge sensor bolometers, and has reported a detection of B-mode polarization on degree angular scales. The Keck Array. was first deployed in late 2010 and will observe through 2016 with five receivers at several frequencies (95, 150, and 220 GHz). BICEP2. and the Keck Array. share a common optical design and employ the field-proven BICEP1. strategy of using small-aperture, cold, on-axis refractive optics, providing excellent control of systematics while maintaining a large field of view. This design allows for full characterization of far-field optical performance using microwave sources on the ground. Here we describe the optical design of both instruments and report a full characterization of the optical performance and beams of BICEP2. and the Keck Array. at 150 GHz. C1 [Ade, P. A. R.; Sudiwala, R. V.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Aikin, R. W.; Bock, J. J.; Brevik, J. A.; Filippini, J. P.; Golwala, S. R.; Hildebrandt, S. R.; Hui, H.; Kefeli, S.; Lueker, M.; Staniszewski, Z. K.; Teply, G. P.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [Barkats, D.] ESO, Joint ALMA Observ, Santiago, Chile. [Benton, S. J.; Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON, Canada. [Bischoff, C. A.; Bradford, K. J.; Buder, I.; Karkare, K. S.; Kovac, J. M.; Richter, S.; Wong, C. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bock, J. J.; Dowell, C. D.; Hildebrandt, S. R.; Megerian, K. G.; Nguyen, H. T.; O'Brient, R.; Turner, A. D.; Weber, A. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bullock, E.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. [Duband, L.] Univ Grenoble Alpes, CEA INAC SBT, F-38000 Grenoble, France. [Filippini, J. P.] Univ Illinois, Dept Phys, Urbana, IL 61820 USA. [Fliescher, S.; Pryke, C.; Schwarz, R.; Sheehy, C. D.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Halpern, M.; Hasselfield, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Hilton, G. C.; Irwin, K. D.] Natl Inst Stand & Technol, Boulder, CO 80305 USA. [Irwin, K. D.; Kang, J. H.; Kernasovskiy, S. A.; Kuo, C. L.; Ogburn, R. W.; Thompson, K.; Tolan, J. E.; Yoon, K. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Irwin, K. D.; Kuo, C. L.; Ogburn, R. W.; Yoon, K. W.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Kaufman, J. P.; Keating, B. G.; Orlando, A.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Leitch, E. M.; Sheehy, C. D.; Vieregg, A. G.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Vieregg, A. G.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. RP Ade, PAR (reprint author), Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. EM avieregg@kicp.uchicago.edu OI Orlando, Angiola/0000-0001-8004-5054; Karkare, Kirit/0000-0002-5215-6993; Barkats, Denis/0000-0002-8971-1954 FU National Science Foundation (NSF) (Caltech/Harvard) [ANT-0742818, ANT-1044978]; National Science Foundation (NSF) (Chicago/Minnesota) [ANT-0742592, ANT-1110087]; NSF (Harvard) [ANT-1145172]; NSF (Minnesota) [ANT-1145143]; NSF (Stanford) [ANT-1145248]; W. M. Keck Foundation (Caltech); JPL Research and Technology Development Fund; NASA [06-ARPA206-0040, 10-SAT10-0017]; Gordon and Betty Moore Foundation at Caltech; Canada Foundation for Innovation; FAS Science Division Research Computing Group at Harvard; U.S. Department of Energy Office of Science; W. M. Keck Foundation FX BICEP2 was supported by the National Science Foundation (NSF) under grants ANT-0742818 and ANT-1044978 (Caltech/Harvard) and ANT-0742592 and ANT-1110087 (Chicago/Minnesota). The Keck Array. was supported by the NSF under grants ANT-1145172 (Harvard), ANT-1145143 (Minnesota), and ANT-1145248 (Stanford), and by the W. M. Keck Foundation (Caltech). The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and grants 06-ARPA206-0040 and 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. Computations presented in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard. The analysis effort at Stanford and SLAC was partially suported by the U.S. Department of Energy Office of Science. The receiver development was supported in part by a grant from the W. M. Keck Foundation. Tireless administrative support was provided by Irene Coyle and Kathy Deniston. NR 29 TC 8 Z9 8 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2015 VL 806 IS 2 AR 206 DI 10.1088/0004-637X/806/2/206 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500061 ER PT J AU An, HJ Bellm, E Bhalerao, V Boggs, SE Christensen, FE Craig, WW Fuerst, F Hailey, CJ Harrison, FA Kaspi, VM Natalucci, L Stern, D Tomsick, JA Zhang, WW AF An, Hongjun Bellm, Eric Bhalerao, Varun Boggs, Steven E. Christensen, Finn E. Craig, William W. Fuerst, Felix Hailey, Charles J. Harrison, Fiona A. Kaspi, Victoria M. Natalucci, Lorenzo Stern, Daniel Tomsick, John A. Zhang, William W. TI BROADBAND X-RAY PROPERTIES OF THE GAMMA-RAY BINARY 1FGL J1018.6-5856 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; gamma rays: stars; stars: individual (1FGL J1018.6-5856); X-rays: binaries ID HIGH-ENERGY EMISSION; LS 5039; TIMING-EXPLORER; PULSAR; I+61-DEGREES-303; MICROQUASARS; PSR-1259-63; RADIATION; SYSTEMS; MODEL AB We report on NuSTAR, XMM-Newton, and Swift observations of the gamma-ray binary 1FGL J1018.6-5856. We measure the orbital period to be 16.544 +/- 0.008 days using Swift data spanning 1900 days. The orbital period is different from the 2011 gamma-ray measurement which was used in the previous X-ray study of An et al. using similar to 400 days of Swift data, but is consistent with a new gamma-ray solution reported in 2014. The light curve folded on the new period is qualitatively similar to that reported previously, having a spike at phase 0 and broad sinusoidal modulation. The X-ray flux enhancement at phase 0 occurs more regularly in time than was previously suggested. A spiky structure at this phase seems to be a persistent feature, although there is some variability. Furthermore, we find that the source flux clearly correlates with the spectral hardness throughout all orbital phases, and that the broadband X-ray spectra measured with NuSTAR, XMM-Newton, and Swift are well fit with an unbroken power-law model. This spectrum suggests that the system may not be accretion-powered. C1 [An, Hongjun; Zhang, William W.] Stanford Univ, Dept Phys KIPAC, Stanford, CA 94305 USA. [An, Hongjun; Kaspi, Victoria M.; Zhang, William W.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Bellm, Eric; Fuerst, Felix; Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Bhalerao, Varun] Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Boggs, Steven E.; Craig, William W.; Tomsick, John A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Kaspi, Victoria M.] McGill Space Inst, Montreal, PQ H3A 2T8, Canada. [Natalucci, Lorenzo] INAFIAPS, Ist Nazl Astrofis, I-00133 Rome, Italy. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP An, HJ (reprint author), Stanford Univ, Dept Phys KIPAC, Stanford, CA 94305 USA. RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Bellm, Eric/0000-0001-8018-5348; Bhalerao, Varun/0000-0002-6112-7609; An, Hongjun/0000-0002-6389-9012 FU NASA [NNG08FD60C, NAS5-00147]; National Aeronautics and Space Administration; Kavli Institute for Particle Astrophysics and Cosmology (KIPAC); ASI/INAF [I/037/12/0-011/13] FX We thank R. W. Romani for useful discussions. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. H.A. acknowledges supports provided by the NASA sponsored Fermi Contract NAS5-00147 and by Kavli Institute for Particle Astrophysics and Cosmology (KIPAC). LN wishes to acknowledge the Italian Space Agency (ASI) for financial support by ASI/INAF grant I/037/12/0-011/13. NR 37 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2015 VL 806 IS 2 AR 166 DI 10.1088/0004-637X/806/2/166 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500021 ER PT J AU D'Angelo, G Podolak, M AF D'Angelo, Gennaro Podolak, Morris TI CAPTURE AND EVOLUTION OF PLANETESIMALS IN CIRCUMJOVIAN DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; hydrodynamics; methods: numerical; planet-disk interactions; planets and satellites: formation; protoplanetary disks ID PRIMORDIAL SOLAR NEBULA; GAS GIANT PLANETS; ACCRETION DISKS; PROTOPLANETARY DISKS; MASS PLANETS; CIRCUMPLANETARY DISKS; MECHANICAL-PROPERTIES; GALILEAN SATELLITES; CORE ACCRETION; BINARY-SYSTEMS AB We study the evolution of planetesimals in evolved gaseous disks that orbit a solar-mass star and harbor a Jupitermass planet at a(p) approximate to 5 AU. The gas dynamics are modeled with a three-dimensional hydrodynamics code that employs nested grids and achieves a resolution of one Jupiter radius in the circumplanetary disk. The code models solids as individual particles. Planetesimals are subjected to gravitational forces by the star and the planet, a drag force by the gas, disruption via ram pressure, and mass loss through ablation. The mass evolution of solids is calculated self-consistently with their temperature, velocity, and position. We consider icy and icy/rocky bodies of radius 0.1-100 km, initially deployed on orbits around the star within a few Hill radii (R-H) of the planet's orbit. Planetesimals are scattered inward, outward, and toward disk regions of radius r >> a(p). Scattering can relocate significant amounts of solids, provided that regions |r - a(p)| similar to 3R(H) are replenished with planetesimals. Scattered bodies can be temporarily captured on planetocentric orbits. Ablation consumes nearly all solids at gas temperatures greater than or similar to 220 K. Super-Keplerian rotation around and beyond the outer edge of the gas gap can segregate less than or similar to 0.1 km bodies, producing solid gap edges at size-dependent radial locations. Capture, break-up, and ablation of solids result in a dust-laden circumplanetary disk with low surface densities of kilometer sized planetesimals, implying relatively long timescales for satellite formation. After a giant planet acquires most of its mass, accretion of solids is unlikely to significantly alter its heavy element content. The luminosity generated by accretion of solids and the contraction luminosity can be of similar orders of magnitude. C1 [D'Angelo, Gennaro] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [D'Angelo, Gennaro] SETI Inst, Mountain View, CA 94043 USA. [Podolak, Morris] Tel Aviv Univ, Dept Geosci, IL-69978 Ramat Aviv, Israel. RP D'Angelo, G (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA. EM gennaro.dangelo@nasa.gov; morris@post.tau.ac.il OI D'Angelo, Gennaro/0000-0002-2064-0801; Podolak, Morris/0000-0003-4801-8691 FU NASA Outer Planets Research Program [202844.02.02.01.75]; NASA Origins of Solar Systems Program [NNX11AD20G, NNX11AK54G, NNX14AG92G] FX We wish to express our gratitude to Jack Lissauer and Peter Bodenheimer for their valuable feedback. We thank an anonymous referee for prompt and constructive comments. G. D. acknowledges support from NASA Outer Planets Research Program grant 202844.02.02.01.75 and from NASA Origins of Solar Systems Program grants NNX11AD20G, NNX11AK54G, and NNX14AG92G. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. NR 118 TC 5 Z9 5 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 JUN 20 PY 2015 VL 806 IS 2 AR 203 DI 10.1088/0004-637X/806/2/203 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500058 ER PT J AU Gao, P Hu, RY Robinson, TD Li, C Yung, YL AF Gao, Peter Hu, Renyu Robinson, Tyler D. Li, Cheng Yung, Yuk L. TI STABILITY OF CO2 ATMOSPHERES ON DESICCATED M DWARF EXOPLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: atmospheres; planets and satellites: physical evolution; planets and satellites: terrestrial planets ID IDEAL-GAS STATE; MARTIAN ATMOSPHERE; CARBON-DIOXIDE; HETEROGENEOUS CHEMISTRY; THERMODYNAMIC FUNCTIONS; EARTH OBSERVATIONS; PLANETS; ABSORPTION; OXYGEN; OZONE AB We investigate the chemical stability of CO2-dominated atmospheres of desiccated M dwarf terrestrial exoplanets using a one-dimensional photochemical model. Around Sun-like stars, CO2 photolysis by Far-UV (FUV) radiation is balanced by recombination reactions that depend on water abundance. Planets orbiting M dwarf stars experience more FUV radiation, and could be depleted in water due to M dwarfs' prolonged, high-luminosity pre-main sequences. We show that, for water-depleted M dwarf terrestrial planets, a catalytic cycle relying on H2O2 photolysis can maintain a CO2 atmosphere. However, this cycle breaks down for atmospheric hydrogen mixing ratios < 1 ppm, resulting in similar to 40% of the atmospheric CO2 being converted to CO and O-2 on a timescale of 1 Myr. The increased O-2 abundance leads to high O-3 concentrations, the photolysis of which forms another CO(2)regenerating catalytic cycle. For atmospheres with < 0.1 ppm hydrogen, CO2 is produced directly from the recombination of CO and O. These catalytic cycles place an upper limit of similar to 50% on the amount of CO2 that can be destroyed via photolysis, which is enough to generate Earth-like abundances of (abiotic) O-2 and O-3. The conditions that lead to such high oxygen levels could be widespread on planets in the habitable zones of M dwarfs. Discrimination between biological and abiotic O-2 and O-3 in this case can perhaps be accomplished by noting the lack of water features in the reflectance and emission spectra of these planets, which necessitates observations at wavelengths longer than 0.95 mu m. C1 [Gao, Peter; Hu, Renyu; Li, Cheng; Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Gao, Peter] NASA, Astrobiol Inst, Virtual Planetary Lab, Seattle, WA 98195 USA. [Hu, Renyu] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Robinson, Tyler D.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. [Robinson, Tyler D.] Oak Ridge Associated Univ, Oak Ridge, TN 37830 USA. RP Gao, P (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM pgao@caltech.edu OI Gao, Peter/0000-0002-8518-9601; Li, Cheng/0000-0002-8280-3119 FU Venus Express program via NASA [NNX10AP80G]; NASA through the NASA Astrobiology Institute [NNH12ZDA002C]; NASA [NNA13AA93A, 51332, NAS 5-26555]; Space Telescope Science Institute; National Aeronautics and Space Administration FX We thank K. Willacy, M. Allen, and R. L. Shia for assistance with the setting up and running of the KinetgenX code. We thank V. Meadows and R. Barnes for their valuable inputs. This research was supported in part by the Venus Express program via NASA NNX10AP80G grant to the California Institute of Technology, and was performed as part of the NASA Astrobiology Institute's Virtual Planetary Laboratory Lead Team, supported by NASA through the NASA Astrobiology Institute under solicitation NNH12ZDA002C and Cooperative Agreement Number NNA13AA93A. Support for R.H.'s work was provided in part by NASA through Hubble Fellowship grant #51332 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. 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. NR 57 TC 4 Z9 4 U1 2 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2015 VL 806 IS 2 AR 249 DI 10.1088/0004-637X/806/2/249 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500104 ER PT J AU Guo, F Liu, YH Daughton, W Li, H AF Guo, Fan Liu, Yi-Hsin Daughton, William Li, Hui TI PARTICLE ACCELERATION AND PLASMA DYNAMICS DURING MAGNETIC RECONNECTION IN THE MAGNETICALLY DOMINATED REGIME SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; galaxies: jets; gamma-ray burst: general; magnetic reconnection; pulsars: general; relativistic processes ID GAMMA-RAY BURSTS; HYPERBOLIC FLUX TUBES; ELECTRON ACCELERATION; CRAB-NEBULA; PULSAR WIND; MAGNETOHYDRODYNAMIC SIMULATIONS; RELATIVISTIC RECONNECTION; NONTHERMAL PARTICLES; EXTRAGALACTIC JETS; SIGMA-PROBLEM AB Magnetic reconnection is thought to be the driver for many explosive phenomena in the universe. The energy release and particle acceleration during reconnection have been proposed as a mechanism for producing high-energy emissions and cosmic rays. We carry out two- and three-dimensional (3D) kinetic simulations to investigate relativistic magnetic reconnection and the associated particle acceleration. The simulations focus on electron-positron plasmas starting with a magnetically dominated, force-free current sheet (sigma equivalent to B-2/(4 pi n(e)m(e)c(2)) >> 1). For this limit, we demonstrate that relativistic reconnection is highly efficient at accelerating particles through a first-order Fermi process accomplished by the curvature drift of particles along the electric field induced by the relativistic flows. This mechanism gives rise to the formation of hard power-law spectra f proportional to (gamma - 1)(-p) and approaches p = 1 for sufficiently large sigma and system size. Eventually most of the available magnetic free energy is converted into nonthermal particle kinetic energy. An analytic model is presented to explain the key results and predict a general condition for the formation of power-law distributions. The development of reconnection in these regimes leads to relativistic inflow and outflow speeds and enhanced reconnection rates relative to nonrelativistic regimes. In the 3D simulation, the interplay between secondary kink and tearing instabilities leads to strong magnetic turbulence, but does not significantly change the energy conversion, reconnection rate, or particle acceleration. This study suggests that relativistic reconnection sites are strong sources of nonthermal particles, which may have important implications for a variety of high-energy astrophysical problems. C1 [Guo, Fan; Daughton, William; Li, Hui] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Liu, Yi-Hsin] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Guo, F (reprint author), Los Alamos Natl Lab, Los Alamos, NM 87545 USA. EM guofan.ustc@gmail.com RI Daughton, William/L-9661-2013; Guo, Fan/H-1723-2013; OI Guo, Fan/0000-0003-4315-3755 FU DOE through LDRD program at LANL; DOE/OFES; CMSO; NASA through Heliospheric Theory Program; NSF [OCI 07-25070] FX We gratefully acknowledge useful discussions with and comments from Andrey Beresnyak, Xuhui Chen, Wei Cui, Wei Deng, Brenda Dingus, Jim Drake, Joe Giacalone, Dimitrios Giannios, Serguei Komissarov, Pawan Kumar, Xiaocan Li, Maxim Lyutikov, Rob Preece, Marc Swisdak, Alexander Tchekhovskoy, Dmitri Uzdensky, Yajie Yuan, Gary Zank, Bing Zhang, and Haocheng Zhang. This work is supported by the DOE through the LDRD program at LANL and DOE/OFES support to LANL in collaboration with CMSO, and by NASA through the Heliospheric Theory Program. The research is part of the Blue Waters sustained-petascale computing project, which is supported by the NSF (Grant No. OCI 07-25070) and the state of Illinois. Additional simulations were performed at the National Center for Computational Sciences at ORNL and with LANL institutional computing. NR 101 TC 40 Z9 41 U1 2 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2015 VL 806 IS 2 AR 167 DI 10.1088/0004-637X/806/2/167 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500022 ER PT J AU Haynes, K Mandell, AM Madhusudhan, N Deming, D Knutson, H AF Haynes, Korey Mandell, Avi M. Madhusudhan, Nikku Deming, Drake Knutson, Heather TI SPECTROSCOPIC EVIDENCE FOR A TEMPERATURE INVERSION IN THE DAYSIDE ATMOSPHERE OF HOT JUPITER WASP-33b SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; planetary systems; techniques: photometric; techniques: spectroscopic ID HUBBLE-SPACE-TELESCOPE; COLLISION-INDUCED ABSORPTION; HD 209458B; THERMAL INVERSIONS; GIANT PLANETS; TRANSMISSION SPECTRUM; INFRARED-EMISSION; SECONDARY ECLIPSE; C/O RATIO; EXOPLANET AB We present observations of two occultations of the extrasolar planet WASP-33b using the Wide Field Camera 3 (WFC3) on the Hubble Space Telescope, which allow us to constrain the temperature structure and composition of its dayside atmosphere. WASP-33b is the most highly irradiated hot Jupiter discovered to date, and the only exoplanet known to orbit a delta-Scuti star. We observed in spatial scan mode to decrease instrument systematic effects in the data, and removed fluctuations in the data due to stellar pulsations. The rms for our final, binned spectrum is 1.05 times the photon noise. We compare our final spectrum, along with previously published photometric data, to atmospheric models of WASP-33b spanning a wide range in temperature profiles and chemical compositions. We find that the data require models with an oxygen-rich chemical composition and a temperature profile that increases at high altitude. We find that our measured spectrum displays an excess in the measured flux toward short wavelengths that is best explained as emission from TiO. If confirmed by additional measurements at shorter wavelengths, this planet would become the first hot Jupiter with a thermal inversion that can be definitively attributed to the presence of TiO in its dayside atmosphere. C1 [Haynes, Korey; Mandell, Avi M.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Haynes, Korey] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA. [Mandell, Avi M.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [Madhusudhan, Nikku] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Knutson, Heather] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Haynes, K (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. EM khaynes0112@gmail.com FU NASA [NAS 5-26555]; NASA through Space Telescope Science Institute; NASA Astrophysics Data Analysis Program; [GO-12495] FX The authors would like to thank the anonymous referee for thoughtful comments that improved the paper. This work is based on observations made with the NASA/ESA Hubble Space Telescope that were obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program GO-12495. Support for this work was provided by NASA through a grant from the Space Telescope Science Institute, with additional support for data analysis provided by a grant from the NASA Astrophysics Data Analysis Program (for K.H. and A.M.M.). NR 55 TC 14 Z9 14 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2015 VL 806 IS 2 AR 146 DI 10.1088/0004-637X/806/2/146 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500001 ER PT J AU Keck, ML Brenneman, LW Ballantyne, DR Bauer, F Boggs, SE Christensen, FE Craig, WW Dauser, T Elvis, M Fabian, AC Fuerst, F Garcia, J Grefenstette, BW Hailey, CJ Harrison, FA Madejski, G Marinucci, A Matt, G Reynolds, CS Stern, D Walton, DJ Zoghbi, A AF Keck, M. L. Brenneman, L. W. Ballantyne, D. R. Bauer, F. Boggs, S. E. Christensen, F. E. Craig, W. W. Dauser, T. Elvis, M. Fabian, A. C. Fuerst, F. Garcia, J. Grefenstette, B. W. Hailey, C. J. Harrison, F. A. Madejski, G. Marinucci, A. Matt, G. Reynolds, C. S. Stern, D. Walton, D. J. Zoghbi, A. TI NUSTAR AND SUZAKU X-RAY SPECTROSCOPY OF NGC 4151: EVIDENCE FOR REFLECTION FROM THE INNER ACCRETION DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies: active; galaxies: individual (NGC 4151); galaxies: Seyfert; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; SEYFERT-GALAXY NGC-4151; BLACK-HOLE SPIN; BROAD-BAND SPECTRUM; NARROW-LINE REGION; DEEP CHANDRA ACIS; XMM-NEWTON; SWIFT J2127.4+5654; EMISSION-LINES; IRON LINES AB We present X-ray timing and spectral analyses of simultaneous 150 ks Nuclear Spectroscopic Telescope Array (NuSTAR) and Suzaku X-ray observations of the Seyfert 1.5 galaxy NGC 4151. We disentangle the continuum emission, absorption, and reflection properties of the active galactic nucleus (AGN) by applying inner accretion disk reflection and absorption-dominated models. With a time-averaged spectral analysis, we find strong evidence for relativistic reflection from the inner accretion disk. We find that relativistic emission arises from a highly ionized inner accretion disk with a steep emissivity profile, which suggests an intense, compact illuminating source. We find a preliminary, near-maximal black hole spin a > 0.9 accounting for statistical and systematic modeling errors. We find a relatively moderate reflection fraction with respect to predictions for the lamp post geometry, in which the illuminating corona is modeled as a point source. Through a time-resolved spectral analysis, we find that modest coronal and inner disk reflection (IDR) flux variation drives the spectral variability during the observations. We discuss various physical scenarios for the IDR model and we find that a compact corona is consistent with the observed features. C1 [Keck, M. L.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Keck, M. L.; Brenneman, L. W.; Elvis, M.; Garcia, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Bauer, F.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, F.] Millennium Inst Astrophys, Santiago 7820436, Chile. [Bauer, F.] Space Sci Inst, Boulder, CO 80301 USA. [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Dauser, T.] Dr Karl Remeis Observ, D-96049 Bamberg, Germany. [Dauser, T.] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Fuerst, F.; Grefenstette, B. W.; Harrison, F. A.; Walton, D. J.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Madejski, G.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Marinucci, A.; Matt, G.] Univ Rome Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Stern, D.; Walton, D. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zoghbi, A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Keck, ML (reprint author), Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA. EM keckm@bu.edu RI XRAY, SUZAKU/A-1808-2009; Boggs, Steven/E-4170-2015; Zoghbi, Abderahmen/A-8445-2017; OI Boggs, Steven/0000-0001-9567-4224; Zoghbi, Abderahmen/0000-0002-0572-9613; Ballantyne, David/0000-0001-8128-6976 FU NASA [NNG08FD60C, NNX13AE90G]; National Aeronautics and Space Administration; Italian Space Agency under ASI/INAF [I/037/12/0-011/13]; European Union [n.312789]; NASA-ADAP [NNX14AF86G, NNX14AF89G]; CONICYT-Chile (Basal-CATA) [PFB-06/2007]; CONICYT-Chile (FONDECYT) [1141218]; CONICYT-Chile (Anillo) [ACT1101]; ICM [IC120009] FX This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research made use of the NuSTAR Data Analysis Software (NuSTAR-DAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). M.L.K. gratefully acknowledges support through NASA grant #NNX13AE90G. G.M. and A.M. acknowledge financial support from Italian Space Agency under grant ASI/INAF I/037/12/0-011/13 and from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement n.312789. C.S.R. acknowledges support from the NASA-ADAP program under grants NNX14AF86G and NNX14AF89G. F.E.B. acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT 1141218, Anillo ACT1101) and ICM grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. We thank Alan Marscher for helpful discussions. We thank the anonymous referee for comments, which have improved this manuscript. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013), and Matplotlib (Hunter 2007). NR 87 TC 16 Z9 16 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2015 VL 806 IS 2 AR 149 DI 10.1088/0004-637X/806/2/149 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500004 ER PT J AU Kogut, A Dwek, E Moseley, SH AF Kogut, A. Dwek, E. Moseley, S. H. TI SPECTRAL CONFUSION FOR COSMOLOGICAL SURVEYS OF REDSHIFTED C II EMISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: high-redshift; galaxies: luminosity function, mass function; galaxies: star formation; line: identification ID FINE-STRUCTURE LINES; STAR-FORMATION RATE; CII EMISSION; SUBMILLIMETER GALAXY; EARLY UNIVERSE; MU-M; INTENSITY; REIONIZATION; INDICATOR; CARBON AB Far-infrared cooling lines are ubiquitous features in the spectra of star-forming galaxies. Surveys of redshifted finestructure lines provide a promising new tool to study structure formation and galactic evolution at redshifts including the epoch of reionization as well as the peak of star formation. Unlike neutral hydrogen surveys, where the 21 cm line is the only bright line, surveys of redshifted fine-structure lines suffer from confusion generated by line broadening, spectral overlap of different lines, and the crowding of sources with redshift. We use simulations to investigate the resulting spectral confusion and derive observing parameters to minimize these effects in pencilbeam surveys of redshifted far-IR line emission. We generate simulated spectra of the 17 brightest far-IR lines in galaxies, covering the 150-1300 mu m wavelength region corresponding to redshifts 0 < z < 7, and develop a simple iterative algorithm that successfully identifies the 158 mu m [C II] line and other lines. Although the [C II] line is a principal coolant for the interstellar medium, the assumption that the brightest observed lines in a given line of sight are always [C II] lines is a poor approximation to the simulated spectra once other lines are included. Blind line identification requires detection of fainter companion lines from the same host galaxies, driving survey sensitivity requirements. The observations require moderate spectral resolution 700 < R < 4000 with angular resolution between 20 ''. and 10 ', sufficiently narrow to minimize confusion yet sufficiently large to include a statistically meaningful number of sources. C1 [Kogut, A.; Dwek, E.; Moseley, S. H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kogut, A (reprint author), NASA, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA. EM Alan.J.Kogut@nasa.gov OI Kogut, Alan/0000-0001-9835-2351 FU NASA's Science Innovation Fund FX We thank D. Leisawitz for encouraging the development of the simulations. Support for this research came from NASA's Science Innovation Fund. NR 37 TC 3 Z9 3 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2015 VL 806 IS 2 AR 234 DI 10.1088/0004-637X/806/2/234 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500089 ER PT J AU Lien, A Sakamoto, T Gehrels, N Palmer, DM Barthelmy, SD Graziani, C Cannizzo, JK AF Lien, Amy Sakamoto, Takanori Gehrels, Neil Palmer, David M. Barthelmy, Scott D. Graziani, Carlo Cannizzo, John K. TI PROBING THE COSMIC GAMMA-RAY BURST RATE WITH TRIGGER SIMULATIONS OF THE SWIFT BURST ALERT TELESCOPE (vol 783, pg 24, 2014) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Lien, Amy; Cannizzo, John K.] CRESST, Greenbelt, MD 20771 USA. [Lien, Amy; Gehrels, Neil; Barthelmy, Scott D.; Cannizzo, John K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lien, Amy; Cannizzo, John K.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Sakamoto, Takanori] Aoyama Gakuin Univ, Coll Sci & Engn, Dept Math & Phys, Chuo Ku, Sagamihara, Kanagawa 2525258, Japan. [Palmer, David M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Graziani, Carlo] Univ Chicago, Dept Astron, Chicago, IL 60637 USA. [Graziani, Carlo] Univ Chicago, Flash Ctr Computat Sci, Chicago, IL 60637 USA. RP Lien, A (reprint author), CRESST, Greenbelt, MD 20771 USA. NR 3 TC 2 Z9 2 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2015 VL 806 IS 2 AR 276 DI 10.1088/0004-637X/806/2/276 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500131 ER PT J AU Matson, RA Gies, DR Guo, Z Quinn, SN Buchhave, LA Latham, DW Howell, SB Rowe, JF AF Matson, Rachel A. Gies, Douglas R. Guo, Zhao Quinn, Samuel N. Buchhave, Lars A. Latham, David W. Howell, Steve B. Rowe, Jason F. TI HST/COS DETECTION OF THE SPECTRUM OF THE SUBDWARF COMPANION OF KOI-81 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: spectroscopic; stars: evolution; stars: individual (KOI-81); subdwarfs ID MASS WHITE-DWARFS; TOMOGRAPHIC SEPARATION; ULTRAVIOLET DETECTION; COMPOSITE SPECTRA; COMPACT OBJECTS; MAIN-SEQUENCE; BINARY-SYSTEM; PHI-PERSEI; STARS; DISCOVERY AB KOI-81 is a totally eclipsing binary discovered by the Kepler mission that consists of a rapidly rotating B-type star and a small, hot companion. The system was forged through large-scale mass transfer that stripped the mass donor of its envelope and spun up the mass gainer star. We present an analysis of UV spectra of KOI-81 that were obtained with the Cosmic Origins Spectrograph on the Hubble Space Telescope that reveal for the first time the spectral features of the faint, hot companion. We present a double-lined spectroscopic orbit for the system that yields mass estimates of 2.92 M-circle dot and 0.19 M-circle dot for the B-star and hot subdwarf, respectively. We used a Doppler tomography algorithm to reconstruct the UV spectra of the components, and a comparison of the reconstructed and model spectra yields effective temperatures of 12 and 19-27 kK for the B-star and hot companion, respectively. The B-star is pulsating, and we identified a number of peaks in the Fourier transform of the light curve, including one that may indicate an equatorial rotation period of 11.5 hr. The B-star has an equatorial velocity that is 74% of the critical velocity where centrifugal and gravitational accelerations balance at the equator, and we fit the transit light curve by calculating a rotationally distorted model for the photosphere of the B-star. C1 [Matson, Rachel A.; Gies, Douglas R.; Guo, Zhao; Quinn, Samuel N.] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA. [Matson, Rachel A.; Gies, Douglas R.; Guo, Zhao; Quinn, Samuel N.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. [Buchhave, Lars A.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Howell, Steve B.; Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA. RP Matson, RA (reprint author), Georgia State Univ, Ctr High Angular Resolut Astron, POB 5060, Atlanta, GA 30302 USA. EM rmatson@chara.gsu.edu; gies@chara.gsu.edu; guo@chara.gsu.edu; quinn@astro.gsu.edu; lbuchhave@cfa.harvard.edu; dlatham@cfa.harvard.edu; steve.b.howell@nasa.gov; Jason.Rowe@nasa.gov OI Buchhave, Lars A./0000-0003-1605-5666; Gies, Douglas/0000-0001-8537-3583; Latham, David/0000-0001-9911-7388 FU NASA through Space Telescope Science Institute [12288]; NASA [NAS 5-26555]; National Science Foundation [AST-1411654]; GSU ACI Fellowship; GSU College of Arts and Sciences; Research Program Enhancement fund of the Board of Regents of the University System of Georgia FX We are grateful to Charles Proffitt and Denise Taylor of STScI for their aid in planning the observations with HST. Support for program #12288 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. This material is also based upon work supported by the National Science Foundation under Grant No. AST-1411654. Institutional support has been provided from a GSU ACI Fellowship (RAM), the GSU College of Arts and Sciences, and the Research Program Enhancement fund of the Board of Regents of the University System of Georgia, administered through the GSU Office of the Vice President for Research and Economic Development. NR 50 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2015 VL 806 IS 2 AR 155 DI 10.1088/0004-637X/806/2/155 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500010 ER PT J AU Nitta, NV Mason, GM Wang, LH Cohen, CMS Wiedenbeck, ME AF Nitta, Nariaki V. Mason, Glenn M. Wang, Linghua Cohen, Christina M. S. Wiedenbeck, Mark E. TI SOLAR SOURCES OF He-3-RICH SOLAR ENERGETIC PARTICLE EVENTS IN SOLAR CYCLE 24 SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun: flares; Sun: magnetic fields; Sun: particle emission; Sun: UV radiation ID CORONAL MASS EJECTIONS; ADVANCED COMPOSITION EXPLORER; IMPULSIVE ELECTRON EVENTS; III RADIO-BURSTS; MAGNETIC-FIELD; ISOTOPE SPECTROMETER; WIND SPACECRAFT; FLARES; ACCELERATION; PLASMA AB Using high-cadence EUV images obtained by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory, we investigate the solar sources of 26 He-3-rich solar energetic particle events at. less than or similar to 1 MeV nucleon(-1) that were well-observed by the Advanced Composition Explorer during solar cycle 24. Identification of the solar sources is based on the association of He-3-rich events with type III radio bursts and electron events as observed by Wind. The source locations are further verified in EUV images from the Solar and Terrestrial Relations Observatory, which provides information on solar activities in the regions not visible from the Earth. Based on AIA observations, He-3-rich events are not only associated with coronal jets as emphasized in solar cycle 23 studies, but also with more spatially extended eruptions. The properties of the He-3-rich events do not appear to be strongly correlated with those of the source regions. As in the previous studies, the magnetic connection between the source region and the observer is not always reproduced adequately by the simple potential field source surface model combined with the Parker spiral. Instead, we find a broad longitudinal distribution of the source regions extending well beyond the west limb, with the longitude deviating significantly from that expected from the observed solar wind speed. C1 [Nitta, Nariaki V.] Lockheed Martin Adv Technol Ctr, Dept A021S, Palo Alto, CA 94304 USA. [Mason, Glenn M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Wang, Linghua] Peking Univ, Inst Space Phys & Appl Technol, Beijing 100871, Peoples R China. [Cohen, Christina M. S.] CALTECH, Pasadena, CA 91125 USA. [Wiedenbeck, Mark E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Nitta, NV (reprint author), Lockheed Martin Adv Technol Ctr, Dept A021S, B-252,3251 Hanover St, Palo Alto, CA 94304 USA. EM nitta@lmsal.com; glenn.mason@jhuapl.edu; wanglhwang@gmail.com; cohen@srl.caltech.edu; mark.e.wiedenbeck@jpl.nasa.gov RI Wang, Linghua/C-4938-2014 OI Wang, Linghua/0000-0001-7309-4325 FU NSF [AGS-1259549, 1156138/112111]; NASA [NNX10AQ68G, NNX10AT75G, 44A-1089749, NNX11A075G, NNX13AH66G]; NASA AIA contract [NNG04EA00C]; NASA STEREO mission under NRL [N00173-02-C-2035]; UC Berkeley under NASA [SA2715-26309, NAS5-03131 T] FX We thank the referee for finding and correcting some problems in the original manuscript. This work has been supported by the NSF grant AGS-1259549, NASA grant NNX10AQ68G, NASA AIA contract NNG04EA00C and the NASA STEREO mission under NRL Contract No. N00173-02-C-2035. GMM acknowledges NASA grant NNX10AT75G, 44A-1089749, and NSF grant 1156138/112111. C.M.S.C. and M.E.W. acknowledge support at Caltech and JPL from subcontract SA2715-26309 from UC Berkeley under NASA contract NAS5-03131 T, and by NASA grants NNX11A075G and NNX13AH66G. NR 56 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2015 VL 806 IS 2 AR 235 DI 10.1088/0004-637X/806/2/235 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500090 ER PT J AU Schnittman, JD AF Schnittman, Jeremy D. TI THE DISTRIBUTION AND ANNIHILATION OF DARK MATTER AROUND BLACK HOLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE astroparticle physics; black hole physics; relativistic processes ID PENROSE MECHANISM; CONSTRAINTS; RADIATION; GALAXIES AB We use a Monte Carlo code to calculate the geodesic orbits of test particles around Kerr black holes, generating a distribution function of both bound and unbound populations of dark matter (DM) particles. From this distribution function, we calculate annihilation rates and observable gamma-ray spectra for a few simple DM models. The features of these spectra are sensitive to the black hole spin, observer inclination, and detailed properties of the DM annihilation cross-section and density profile. Confirming earlier analytic work, we find that for rapidly spinning black holes, the collisional Penrose process can reach efficiencies exceeding 600%, leading to a high-energy tail in the annihilation spectrum. The high particle density and large proper volume of the region immediately surrounding the horizon ensures that the observed flux from these extreme events is non-negligible. C1 [Schnittman, Jeremy D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Schnittman, Jeremy D.] Joint Space Sci Inst, College Pk, MD 20742 USA. RP Schnittman, JD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM jeremy.schnittman@nasa.gov FU NASA [ATP12-0139, ATP13-0077] FX This work was partially supported by NASA grants ATP12-0139 and ATP13-0077. We thank Alessandra Buonanno, Francesc Ferrer, Ted Jacobson, Henric Krawczynski, Tzvi Piran, Laleh Sadeghian, and Joe Silk for helpful comments and discussion. NR 43 TC 4 Z9 4 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2015 VL 806 IS 2 AR 264 DI 10.1088/0004-637X/806/2/264 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500119 ER PT J AU Ursino, E Galeazzi, M Gupta, A Kelley, RL Mitsuishi, I Ohashi, T Sato, K AF Ursino, E. Galeazzi, M. Gupta, A. Kelley, R. L. Mitsuishi, I. Ohashi, T. Sato, K. TI EXPLORING THE BRIDGE BETWEEN A3556 AND A3558 IN THE SHAPLEY SUPERCLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: abundances; intergalactic medium; large-scale structure of universe; X-rays: diffuse background ID HOT INTERGALACTIC MEDIUM; X-RAY-ABSORPTION; GALAXY CLUSTERS; MISSING BARYONS; MASS; CHANDRA; FILAMENT; ABSORBERS; CORE; GAS AB Looking at the region connecting two clusters is a promising way to identify and study the Warm-Hot Intergalactic Medium. Observations show that the spectrum of the bridge between A3556 and A3558 has a stronger soft X-ray emission than the nearby region. Suzaku. observations could not discriminate the origin of the extra emission. In this work we analyze a dedicated Chandra. observation of the same target to identify point sources and characterize the background emission in the bridge. We find that the count number of the point sources is much higher than average field population (using CDFS 4Ms as a reference). Moreover, the shape of the cumulative distribution resembles that of galaxy distribution suggesting that the point sources are galaxies in a filament. The Suzaku. extra emission is well explained by the high abundance of point sources identified by Chandra. Furthermore, we used optical/ IR observations of point sources in the same field to estimate the density of the putative filament as rho approximate to 150 rho(b), below Suzaku. sensitivity. C1 [Ursino, E.; Galeazzi, M.] Univ Miami, Dept Phys, Coral Gables, FL 33155 USA. [Gupta, A.] Columbus State Community Coll, Dept Biol & Phys Sci, Columbus, OH 43215 USA. [Gupta, A.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Kelley, R. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mitsuishi, I.] Nagoya Univ, Div Particle & Astrophys Sci, Nagoya, Aichi 4648602, Japan. [Ohashi, T.] Tokyo Metropolitan Univ, Dept Phys, Tokyo 1920397, Japan. [Sato, K.] Tokyo Univ Sci, Dept Phys, Tokyo 1628601, Japan. RP Ursino, E (reprint author), Univ Miami, Dept Phys, Coral Gables, FL 33155 USA. EM galeazzi@physics.miami.edu RI XRAY, SUZAKU/A-1808-2009; OI Ursino, Eugenio /0000-0002-2567-2036 FU SAO award [GO1-12179X] FX This work has been supported in part by SAO award #GO1-12179X. The authors would like to thank R. K. Smith and W. Liu for the useful discussion and suggestions. NR 45 TC 0 Z9 0 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2015 VL 806 IS 2 AR 211 DI 10.1088/0004-637X/806/2/211 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500066 ER PT J AU Furst, F Pottschmidt, K Miyasaka, H Bhalerao, V Bachetti, M Boggs, SE Christensen, FE Craig, WW Grinberg, V Hailey, CJ Harrison, FA Kennea, JA Rahoui, F Stern, D Tendulkar, SP Tomsick, JA Walton, DJ Wilms, J Zhang, WW AF Fuerst, F. Pottschmidt, K. Miyasaka, H. Bhalerao, V. Bachetti, M. Boggs, S. E. Christensen, F. E. Craig, W. W. Grinberg, V. Hailey, C. J. Harrison, F. A. Kennea, J. A. Rahoui, F. Stern, D. Tendulkar, S. P. Tomsick, J. A. Walton, D. J. Wilms, J. Zhang, W. W. TI DISTORTED CYCLOTRON LINE PROFILE IN CEP X-4 AS OBSERVED BY NuSTAR SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; radiation: dynamics; stars: neutron; X-rays: binaries; X-rays: individual (Cep X-4) ID X-RAY PULSAR; CEPHEUS X-4; RESONANCE FEATURE; GX 304-1; DISCOVERY; ENERGY; OUTBURST; TELESCOPE; HERCULES-X-1; ABSORPTION AB We present spectral analysis of Nuclear Spectroscopic Telescope Array and Swift observations of Cep X-4 during its outburst in 2014. We observed the source once during the peak of the outburst and once during the decay, finding good agreement in the spectral shape between the observations. We describe the continuum using a power law with a Fermi-Dirac cutoff at high energies. Cep X-4 has a very strong cyclotron resonant scattering feature (CRSF) around 30 keV. A simple absorption-like line with a Gaussian optical depth or a pseudo-Lorentzian profile both fail to describe the shape of the CRSF accurately, leaving significant deviations at the red side of the line. We characterize this asymmetry with a second absorption feature around 19 keV. The line energy of the CRSF, which is not influenced by the addition of this feature, shows a small but significant positive luminosity dependence. With luminosities between (1-6) x 10(36) erg s(-1), Cep X-4 is below the theoretical limit where such a correlation is expected. This behavior is similar to Vela X-1 and we discuss parallels between the two systems. C1 [Fuerst, F.; Miyasaka, H.; Harrison, F. A.; Tendulkar, S. P.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Pottschmidt, K.] UMBC, CRESST, Dept Phys, Baltimore, MD 21250 USA. [Pottschmidt, K.] UMBC, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Pottschmidt, K.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bhalerao, V.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Bachetti, M.] Osservatorio Astron Cagliari, I-09047 Selargius, CA, Italy. [Boggs, S. E.; Craig, W. W.; Tomsick, J. A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Grinberg, V.] MIT, Kavli Inst Astrophys, Cambridge, MA 02139 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Rahoui, F.] European So Observ, D-85748 Garching, Germany. [Rahoui, F.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & ECAP, D-96049 Bamberg, Germany. RP Fuerst, F (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RI Wilms, Joern/C-8116-2013; Boggs, Steven/E-4170-2015; OI Wilms, Joern/0000-0003-2065-5410; Boggs, Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337; Bhalerao, Varun/0000-0002-6112-7609 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration FX We thank the anonymous referee for valuable 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). NR 36 TC 3 Z9 3 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 JUN 20 PY 2015 VL 806 IS 2 AR L24 DI 10.1088/2041-8205/806/2/L24 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2KO UT WOS:000356772700003 ER PT J AU Pulkkinen, A Bernabeu, E Eichner, J Viljanen, A Ngwira, C AF Pulkkinen, Antti Bernabeu, Emanuel Eichner, Jan Viljanen, Ari Ngwira, Chigomezyo TI Regional-scale high-latitude extreme geoelectric fields pertaining to geomagnetically induced currents SO EARTH PLANETS AND SPACE LA English DT Article DE Geomagnetically induced currents; Extreme events; Spatial scales ID ELECTRIC-FIELDS; SURFACE; STORM; EARTH AB Motivated by the needs of the high-voltage power transmission industry, we use data from the high-latitude IMAGE magnetometer array to study characteristics of extreme geoelectric fields at regional scales. We use 10-s resolution data for years 1993-2013, and the fields are characterized using average horizontal geoelectric field amplitudes taken over station groups that span about 500-km distance. We show that geoelectric field structures associated with localized extremes at single stations can be greatly different from structures associated with regionally uniform geoelectric fields, which are well represented by spatial averages over single stations. Visual extrapolation and rigorous extreme value analysis of spatially averaged fields indicate that the expected range for 1-in-100-year extreme events are 3-8 V/km and 3.4-7.1 V/km, respectively. The Quebec reference ground model is used in the calculations. C1 [Pulkkinen, Antti; Ngwira, Chigomezyo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bernabeu, Emanuel] PJM Interconnect, Audubon, PA USA. [Eichner, Jan] Munich Re, Geo Risks Res, Munich, Germany. [Viljanen, Ari] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. [Ngwira, Chigomezyo] Catholic Univ Amer, Washington, DC 20064 USA. RP Pulkkinen, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM antti.a.pulkkinen@nasa.gov FU EU's 7th Framework Programme (FP7) [260330 (EURISGIC)] FX We thank the institutes who maintain the IMAGE magnetometer array. The IMAGE array data used in this paper are publicly available at http://space.fmi.fi/image. We acknowledge discussions with Drs L. Marti (Hydro One), R. Horton (Southern Company), as well as with Mr. F. Koza (PJM) and Mr M. Olson (NERC). The work of A.V. was partially supported from the EU's 7th Framework Programme (FP7/2007-2013) under grant agreement no. 260330 (EURISGIC). NR 22 TC 8 Z9 8 U1 0 U2 2 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1880-5981 J9 EARTH PLANETS SPACE JI Earth Planets Space PD JUN 19 PY 2015 VL 67 BP 1 EP 8 AR 93 DI 10.1186/s40623-015-0255-6 PG 8 WC Geosciences, Multidisciplinary SC Geology GA CL4HX UT WOS:000356914300001 ER PT J AU Werner, MW Soifer, BT Lombardi, LS Helou, G AF Werner, M. W. Soifer, B. T. Lombardi, L. Storrie Helou, G. TI Spitzer's stellar work SO SCIENCE LA English DT Letter C1 [Werner, M. W.] CALTECH, Jet Prop Lab, Spitzer Space Telescope, Pasadena, CA 91109 USA. [Soifer, B. T.; Lombardi, L. Storrie; Helou, G.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Werner, MW (reprint author), CALTECH, Jet Prop Lab, Spitzer Space Telescope, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mww@ipac.caltech.edu NR 0 TC 0 Z9 0 U1 0 U2 1 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 JUN 19 PY 2015 VL 348 IS 6241 BP 1326 EP 1326 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CK7XK UT WOS:000356449500036 PM 26089504 ER PT J AU Jontof-Hutter, D Rowe, JF Lissauer, JJ Fabrycky, DC Ford, EB AF Jontof-Hutter, Daniel Rowe, Jason F. Lissauer, Jack J. Fabrycky, Daniel C. Ford, Eric B. TI The mass of the Mars-sized exoplanet Kepler-138 b from transit timing SO NATURE LA English DT Article ID LOW-DENSITY PLANETS; CHAIN MONTE-CARLO; SUN-LIKE STAR; 1ST 16 MONTHS; LIGHT-CURVE; DIFFERENTIAL EVOLUTION; EXTRASOLAR PLANETS; CANDIDATES; SYSTEM; ORBITS AB Extrasolar planets that pass in front of their host star (transit) cause a temporary decrease in the apparent brightness of the star, providing a direct measure of the planet's size and orbital period. In some systems with multiple transiting planets, the times of the transits are measurably affected by the gravitational interactions between neighbouring planets(1,2). In favourable cases, the departures from Keplerian orbits (that is, unaffected by gravitational effects) implied by the observed transit times permit the planetary masses to be measured, which is key to determining their bulk densities(3). Characterizing rocky planets is particularly difficult, because they are generally smaller and less massive than gaseous planets. Therefore, few exoplanets near the size of Earth have had their masses measured. Here we report the sizes and masses of three planets orbiting Kepler-138, a star much fainter and cooler than the Sun. We determine that the mass of the Mars-sized inner planet, Kepler-138 b, is 0.066(-0.037)(+0.059) Earth masses. Its density is 2.6(-1.5)(+2.4) grams per cubic centimetre. The middle and outer planets are both slightly larger than Earth. The middle planet's density (6.2(-3.4)(+5.8) grams per cubic centimetre) is similar to that of Earth, and the outer planet is less than half as dense at 2.1(-1.2)(+2.2) grams per cubic centimetre, implying that it contains a greater portion of low-density components such as water and hydrogen. C1 [Jontof-Hutter, Daniel; Ford, Eric B.] Penn State Univ, Dept Astron, Davey Lab, University Pk, PA 16802 USA. [Jontof-Hutter, Daniel; Rowe, Jason F.; Lissauer, Jack J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA. [Fabrycky, Daniel C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. RP Jontof-Hutter, D (reprint author), Penn State Univ, Dept Astron, Davey Lab, University Pk, PA 16802 USA. EM dxj14@psu.edu OI Fabrycky, Daniel/0000-0003-3750-0183 FU NASA Postdoctoral Program; Center for Exoplanets and Habitable Worlds; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium; NASA [NNX14AB92G]; Kepler Participating Scientist Program award [NNX14AB87G]; NASA Kepler Participating Scientist Program award [NNX14AN76G]; NASA Exoplanet Research Program award [NNX15AE21G] FX D.J-H. acknowledges support through the NASA Postdoctoral Program and funding from the Center for Exoplanets and Habitable Worlds. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science and the Pennsylvania Space Grant Consortium. J.F.R. acknowledges NASA grant NNX14AB92G issued through the Kepler Participating Scientist Program. D.C.F. is an Alfred P. Sloane Fellow and was supported by the Kepler Participating Scientist Program award NNX14AB87G. E.B.F. was supported in part by NASA Kepler Participating Scientist Program award NNX14AN76G and NASA Exoplanet Research Program award NNX15AE21G, as well as the Center for Exoplanets and Habitable Worlds. NR 56 TC 19 Z9 19 U1 1 U2 9 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 JUN 18 PY 2015 VL 522 IS 7556 BP 321 EP + DI 10.1038/nature14494 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CK7PU UT WOS:000356425400048 PM 26085271 ER PT J AU Hornbuckle, BC Sasaki, TT Bigelow, GS Noebe, RD Weaver, ML Thompson, GB AF Hornbuckle, B. C. Sasaki, T. T. Bigelow, G. S. Noebe, R. D. Weaver, M. L. Thompson, G. B. TI Structure-property relationships in a precipitation strengthened Ni-29.7Ti-20Hf (at%) shape memory alloy SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article DE Nitinol; Precipitation strengthening; NiTiHf; Microstructural characterization; Atom probe tomography ID MARTENSITIC-TRANSFORMATION; PHASE; NITI; MICROSTRUCTURE; BEHAVIOR AB The martensitic transformation temperatures, load-biased thermomechanical properties, and microstructure (characterized by transmission electron microscopy and atom probe tomography) were investigated for a Ni-29.7Ti-20Hf (at%) alloy aged at 550 degrees C for 0-300 h. Aging for three hours and longer resulted in the precipitation of a face-centered orthorhombic phase, previously denoted as the H-phase. The number density, size, and composition of this phase did not change significantly upon aging from 3 to 30 h. However, continued aging to 300 h resulted in a decrease in the number density and significant coarsening of the precipitates at 550 degrees C. The alloy exhibited near optimum response for shape memory behavior and dimensional stability after aging for three hours, though transformation temperatures continued to increase with aging time. (C) 2015 Elsevier B.V. All rights reserved. C1 [Hornbuckle, B. C.; Sasaki, T. T.; Weaver, M. L.; Thompson, G. B.] Univ Alabama, Dept Met & Mat Engn, Tuscaloosa, AL 35487 USA. [Bigelow, G. S.; Noebe, R. D.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA. RP Thompson, GB (reprint author), Univ Alabama, Dept Met & Mat Engn, Tuscaloosa, AL 35487 USA. EM gthompson@eng.ua.edu FU NASA [NNX09AO61A]; Transformative Aeronautics Concepts Program, Transformational Tools & Technologies Project FX The authors gratefully acknowledge funding for this research under the NASA Grant NNX09AO61A and from the Transformative Aeronautics Concepts Program, Transformational Tools & Technologies Project (Dale Hopkins, Technical Lead for Structures & Materials Discipline). UA's Central Analytical Facility (www.caf.ua.edu) is recognized for additional support and access to the microscopes used in this study. Also, Dr. M. Moody is thanked for helpful discussions on atom probe analysis. NR 34 TC 6 Z9 6 U1 5 U2 14 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0921-5093 EI 1873-4936 J9 MAT SCI ENG A-STRUCT JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process. PD JUN 18 PY 2015 VL 637 BP 63 EP 69 DI 10.1016/j.msea.2015.03.123 PG 7 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA CK4QF UT WOS:000356207600008 ER PT J AU Gopalswamy, N Tsurutani, B Yan, YH AF Gopalswamy, Nat Tsurutani, Bruce Yan, Yihua TI Short-term variability of the Sun-Earth system: an overview of progress made during the CAWSES-II period SO PROGRESS IN EARTH AND PLANETARY SCIENCE LA English DT Review DE Solar activity; Space weather; Coronal mass ejections; Flares; Solar energetic particle events; Geospace impact; Geomagnetic storms ID CORONAL MASS EJECTIONS; SOLAR-CYCLE 24; ENERGETIC PARTICLE EVENTS; GROUND-LEVEL ENHANCEMENT; EXTREME-ULTRAVIOLET WAVE; MAGNETIC-FLUX ROPES; RELATIVISTIC ELECTRON ACCELERATION; DST LESS-THAN-OR-EQUAL-TO-50 NT; PARALLEL INTERPLANETARY SHOCK; ACTIVITY HILDCAA EVENTS AB This paper presents an overview of results obtained during the CAWSES-II period on the short-term variability of the Sun and how it affects the near-Earth space environment. CAWSES-II was planned to examine the behavior of the solar-terrestrial system as the solar activity climbed to its maximum phase in solar cycle 24. After a deep minimum following cycle 23, the Sun climbed to a very weak maximum in terms of the sunspot number in cycle 24 (MiniMax24), so many of the results presented here refer to this weak activity in comparison with cycle 23. The short-term variability that has immediate consequence to Earth and geospace manifests as solar eruptions from closed-field regions and high-speed streams from coronal holes. Both electromagnetic (flares) and mass emissions (coronal mass ejections - CMEs) are involved in solar eruptions, while coronal holes result in high-speed streams that collide with slow wind forming the so-called corotating interaction regions (CIRs). Fast CMEs affect Earth via leading shocks accelerating energetic particles and creating large geomagnetic storms. CIRs and their trailing high-speed streams (HSSs), on the other hand, are responsible for recurrent small geomagnetic storms and extended days of auroral zone activity, respectively. The latter leads to the acceleration of relativistic magnetospheric 'killer' electrons. One of the major consequences of the weak solar activity is the altered physical state of the heliosphere that has serious implications for the shock-driving and storm-causing properties of CMEs. Finally, a discussion is presented on extreme space weather events prompted by the 23 July 2012 super storm event that occurred on the backside of the Sun. Many of these studies were enabled by the simultaneous availability of remote sensing and in situ observations from multiple vantage points with respect to the Sun-Earth line. C1 [Gopalswamy, Nat] NASA, Goddard Space Flight Ctr, Heliophys Div, Solar Phys Lab, Greenbelt, MD 20771 USA. [Tsurutani, Bruce] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Yan, Yihua] Chinese Acad Sci, Key Lab Solar Act, Natl Astron Observ, Beijing 100012, Peoples R China. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Div, Solar Phys Lab, Code 671, Greenbelt, MD 20771 USA. EM nat.gopalswamy@nasa.gov NR 356 TC 7 Z9 7 U1 1 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 2197-4284 J9 PROG EARTH PLANET SC JI Prog. Earth Planet. Sci. PD JUN 17 PY 2015 VL 2 AR UNSP 13 DI 10.1186/s40645-015-0043-8 PG 41 WC Geosciences, Multidisciplinary SC Geology GA CV0MF UT WOS:000363944100001 ER PT J AU Clement, GP Bukley, AP Paloski, WH AF Clement, Gilles P. Bukley, Angelia P. Paloski, William H. TI Artificial gravity as a countermeasure for mitigating physiological deconditioning during long-duration space missions SO FRONTIERS IN SYSTEMS NEUROSCIENCE LA English DT Review DE gravity; adaptation; international space station; microgravity; centrifuge; countermeasure ID DOWN BED REST; SHORT-RADIUS CENTRIFUGATION; NEGATIVE-PRESSURE EXERCISE; INDUCED BONE LOSS; SIMULATED MICROGRAVITY; ORTHOSTATIC INTOLERANCE; ROTATING ENVIRONMENT; LINEAR ACCELERATION; TREADMILL EXERCISE; UPRIGHT EXERCISE AB In spite of the experience gained in human space flight since Yuri Gagarin's historical flight in 1961, there has yet to be identified a completely effective countermeasure for mitigating the effects of weightlessness on humans. Were astronauts to embark upon a journey to Mars today, the 6-month exposure to weightlessness en route would leave them considerably debilitated, even with the implementation of the suite of piece meal countermeasures currently employed. Continuous or intermittent exposure to simulated gravitational states on board the spacecraft while traveling to and from Mars, also known as artificial gravity, has the potential for enhancing adaptation to Mars gravity and re adaptation to Earth gravity. Many physiological functions are adversely affected by the weightless environment of spaceflight because they are calibrated for normal, Earth's gravity. Hence, the concept of artificial gravity is to provide a broad-spectrum replacement for the gravitational forces that naturally occur on the Earth's surface, thereby avoiding the physiological deconditioning that takes place in weightlessness. Because researchers have long been concerned by the adverse sensorimotor effects that occur in weightlessness as well as in rotating environments, additional study of the complex interactions among sensorimotor and other physiological systems in rotating environments must be undertaken both on Earth and in space before artificial gravity can be implemented. C1 [Clement, Gilles P.] Wyle Sci & Engn Grp, Houston, TX 77058 USA. [Bukley, Angelia P.] Int Space Univ, Arlincton, VA USA. [Paloski, William H.] NASA, Johnson Space Ctr, Houston, TX USA. RP Clement, GP (reprint author), Wyle Sci & Engn Grp, 1290 Hercules Ave, Houston, TX 77058 USA. EM gilles.r.clement@nasa.gov NR 66 TC 5 Z9 6 U1 1 U2 6 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 JUN 17 PY 2015 VL 9 AR 92 DI 10.3389/fnsys.2015.00092 PG 11 WC Neurosciences SC Neurosciences & Neurology GA CU9CY UT WOS:000363841800001 PM 26136665 ER PT J AU Ritchie, LE Taddeo, SS Weeks, BR Lima, F Bloomfield, SA Azcarate-Peril, MA Zwart, SR Smith, SM Turner, ND AF Ritchie, Lauren E. Taddeo, Stella S. Weeks, Brad R. Lima, Florence Bloomfield, Susan A. Azcarate-Peril, M. Andrea Zwart, Sara R. Smith, Scott M. Turner, Nancy D. TI Space Environmental Factor Impacts upon Murine Colon Microbiota and Mucosal Homeostasis SO PLOS ONE LA English DT Article ID INFLAMMATORY-BOWEL-DISEASE; LONG-DURATION SPACEFLIGHT; TOLL-LIKE RECEPTORS; INTESTINAL MICROBIOTA; GUT MICROBIOTA; ULCERATIVE-COLITIS; GENE-EXPRESSION; IMMUNE-SYSTEM; RADIATION; IRRADIATION AB Astronaut intestinal health may be impacted by microgravity, radiation, and diet. The aim of this study was to characterize how high and low linear energy transfer (LET) radiation, microgravity, and elevated dietary iron affect colon microbiota (determined by 16S rDNA pyrosequencing) and colon function. Three independent experiments were conducted to achieve these goals: 1) fractionated low LET. radiation (Cs-137, 3 Gy, RAD), high Fe diet (IRON) (650 mg/kg diet), and a combination of low LET. radiation and high Fe diet (IRON+RAD) in male Sprague-Dawley rats; 2) high LET Si-38 particle exposure (0.050 Gy), 1/6 G partial weight bearing (PWB), and a combination of high (LETSi)-Si-38 particle exposure and PWB in female BalbC/ByJ mice; and 3) 13 d spaceflight in female C57BL/6 mice. Low LET radiation, IRON and spaceflight increased Bacteroidetes and decreased Firmicutes. RAD and IRON+RAD increased Lactobacillales and lowered Clostridiales compared to the control (CON) and IRON treatments. Low LET radiation, IRON, and spaceflight did not significantly affect diversity or richness, or elevate pathogenic genera. Spaceflight increased Clostridiales and decreased Lactobacillales, and similar trends were observed in the experiment using a ground-based model of microgravity, suggesting altered gravity may affect colonic microbiota. Although we noted no differences in colon epithelial injury or inflammation, spaceflight elevated TGF beta gene expression. Microbiota and mucosal characterization in these models is a first step in understanding the impact of the space environment on intestinal health. C1 [Ritchie, Lauren E.; Turner, Nancy D.] Texas A&M Univ, Intercollegiate Fac Genet, College Stn, TX 77843 USA. [Taddeo, Stella S.; Turner, Nancy D.] Texas A&M Univ, Nutr & Food Sci Dept, College Stn, TX USA. [Weeks, Brad R.] Texas A&M Univ, Dept Vet Pathobiol, College Stn, TX USA. [Lima, Florence] Univ Kentucky, Dept Med, Div Nephrol, Lexington, KY 40506 USA. [Bloomfield, Susan A.] Texas A&M Univ, Dept Hlth & Kinesiol, College Stn, TX USA. [Azcarate-Peril, M. Andrea] Univ N Carolina, Sch Med, Dept Cell Biol & Physiol, Chapel Hill, NC USA. [Zwart, Sara R.; Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Human Hlth & Performance Directorate, Houston, TX 77058 USA. RP Turner, ND (reprint author), Texas A&M Univ, Intercollegiate Fac Genet, College Stn, TX 77843 USA. EM n-turner@tamu.edu FU NASA; National Institutes of Health/National Institute of Diabetes and Digestive and Kidney Diseases [P30 DK34987]; National Space Biomedical Research Institute [NCC 9-58] FX This study was funded by the NASA Human Research Program's Human Health Countermeasures Element by a grant to SRZ, SMS, and NDT; a National Institutes of Health/National Institute of Diabetes and Digestive and Kidney Diseases grant (P30 DK34987) to MAAP, and a National Space Biomedical Research Institute grant (NCC 9-58) to NDT. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 69 TC 1 Z9 1 U1 0 U2 7 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 JUN 17 PY 2015 VL 10 IS 6 AR UNSP e0125792 DI 10.1371/journal.pone.0125792 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CK9NS UT WOS:000356567400004 PM 26083373 ER PT J AU Schwalm, CR Huntzinger, DN Fisher, JB Michalak, AM Bowman, K Ciais, P Cook, R El-Masri, B Hayes, D Huang, MY Ito, A Jain, A King, AW Lei, HM Liu, JJ Lu, CQ Mao, JF Peng, SS Poulter, B Ricciuto, D Schaefer, K Shi, XY Tao, B Tian, HQ Wang, WL Wei, YX Yang, J Zeng, N AF Schwalm, Christopher R. Huntzinger, Deborah N. Fisher, Joshua B. Michalak, Anna M. Bowman, Kevin Ciais, Philippe Cook, Robert El-Masri, Bassil Hayes, Daniel Huang, Maoyi Ito, Akihiko Jain, Atul King, Anthony W. Lei, Huimin Liu, Junjie Lu, Chaoqun Mao, Jiafu Peng, Shushi Poulter, Benjamin Ricciuto, Daniel Schaefer, Kevin Shi, Xiaoying Tao, Bo Tian, Hanqin Wang, Weile Wei, Yaxing Yang, Jia Zeng, Ning TI Toward "optimal" integration of terrestrial biosphere models SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE modeling; carbon cycle; model integration ID PROGRAM MULTISCALE SYNTHESIS; AIR CO2 ENRICHMENT; CLIMATE-CHANGE; CARBON STORAGE; INTERCOMPARISON PROJECT; NITROGEN-CYCLE; FOREST BIOMASS; LAND-USE; PREDICTION; UNCERTAINTY AB Multimodel ensembles (MME) are commonplace in Earth system modeling. Here we perform MME integration using a 10-member ensemble of terrestrial biosphere models (TBMs) from the Multiscale synthesis and Terrestrial Model Intercomparison Project (MsTMIP). We contrast optimal (skill based for present-day carbon cycling) versus naive (one model-one vote) integration. MsTMIP optimal and naive mean land sink strength estimates (-1.16 versus -1.15 Pg C per annum respectively) are statistically indistinguishable. This holds also for grid cell values and extends to gross uptake, biomass, and net ecosystem productivity. TBM skill is similarly indistinguishable. The added complexity of skill-based integration does not materially change MME values. This suggests that carbon metabolism has predictability limits and/or that all models and references are misspecified. Resolving this issue requires addressing specific uncertainty types (initial conditions, structure, and references) and a change in model development paradigms currently dominant in the TBM community. C1 [Schwalm, Christopher R.] No Arizona Univ, Ctr Ecosyst Sci & Soc, Flagstaff, AZ 86011 USA. [Schwalm, Christopher R.; Huntzinger, Deborah N.] No Arizona Univ, Sch Earth Sci & Environm Sustainabil, Flagstaff, AZ 86011 USA. [Huntzinger, Deborah N.] No Arizona Univ, Dept Civil Engn Construct Management & Environm E, Flagstaff, AZ 86011 USA. [Fisher, Joshua B.; Bowman, Kevin; Liu, Junjie] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Michalak, Anna M.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA USA. [Ciais, Philippe; Peng, Shushi; Tao, Bo] Lab Sci Climat & Environm, Gif Sur Yvette, France. [Cook, Robert; Hayes, Daniel; King, Anthony W.; Mao, Jiafu; Ricciuto, Daniel; Shi, Xiaoying; Wei, Yaxing] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. [El-Masri, Bassil; Jain, Atul] Univ Illinois, Dept Atmospher Sci, Urbana, IL USA. [Huang, Maoyi] Pacific NW Natl Lab, Atmospher Sci & Global Change Div, Richland, WA 99352 USA. [Ito, Akihiko] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan. [Lei, Huimin] Tsinghua Univ, Dept Hydraul Engn, Beijing 100084, Peoples R China. [Lu, Chaoqun; Tian, Hanqin; Yang, Jia] Auburn Univ, Int Ctr Climate & Global Change Res, Auburn, AL 36849 USA. [Lu, Chaoqun; Tian, Hanqin; Yang, Jia] Auburn Univ, Sch Forestry & Wildlife Sci, Auburn, AL 36849 USA. [Poulter, Benjamin] Montana State Univ, Dept Ecol, Bozeman, MT 59717 USA. [Schaefer, Kevin] Natl Snow & Ice Data Ctr, Boulder, CO USA. [Wang, Weile] Ames Res Ctr, Natl Aeronaut & Space Adm, Moffett Field, CA USA. [Zeng, Ning] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. RP Schwalm, CR (reprint author), No Arizona Univ, Ctr Ecosyst Sci & Soc, Flagstaff, AZ 86011 USA. EM christopher.schwalm@nau.edu RI Mao, Jiafu/B-9689-2012; Lei, Huimin/H-9596-2015; Tian, Hanqin/A-6484-2012; Wei, Yen/H-5329-2012; Peng, Shushi/J-4779-2014; Ricciuto, Daniel/I-3659-2016; Zeng, Ning/A-3130-2008; Yang, Jia/A-6483-2012; Jain, Atul/D-2851-2016 OI Fisher, Joshua/0000-0003-4734-9085; Poulter, Benjamin/0000-0002-9493-8600; Huang, Maoyi/0000-0001-9154-9485; Mao, Jiafu/0000-0002-2050-7373; Lei, Huimin/0000-0002-1175-2334; Tian, Hanqin/0000-0002-1806-4091; Peng, Shushi/0000-0001-5098-726X; Ricciuto, Daniel/0000-0002-3668-3021; Cook, Robert/0000-0001-7393-7302; Zeng, Ning/0000-0002-7489-7629; Yang, Jia/0000-0003-2019-9603; Jain, Atul/0000-0002-4051-3228 FU National Aeronautics and Space Administration (NASA) [NNX12AP74G, NNX10AG01A, NNX11AO08A]; Multiscale synthesis and Terrestrial Model Intercomparison Project (MsTMIP); NASA ROSES [NNX10AG01A, NNH10AN681]; Modeling and Synthesis Thematic Data Center at Oak Ridge National Laboratory (ORNL); DOE [DE-AC05-00OR22725]; U.S. Department of Energy (DOE), Office of Science, Biological and Environmental Research (BER) through the Earth System Modeling program; Environmental Molecular Sciences Laboratory(EMSL); U.S. DOE-BER; U.S. DOE-BER through the Subsurface Biogeochemical Research Program (SBR) as part of the SBR Scientific Focus Area (SFA) at the Pacific Northwest National Laboratory (PNNL); U.S. DOE [DE-AC05-76RLO1830]; NASA Interdisciplinary Science Program (IDS); NASA Land Cover/Land Use Change Program (LCLUC); NASA Terrestrial Ecology Program; NASA Atmospheric Composition Modeling and Analysis Program (ACMAP); NSF Dynamics of Coupled Natural-Human System Program (CNH); Decadal and Regional Climate Prediction using Earth System Models (EaSM); DOE National Institute for Climate Change Research; USDA AFRI Program; EPA STAR Program; U.S. National Science Foundation [NSF-AGS-12-43071, NSF-EFRI083598]; USDA National Institute of Food and Agriculture (NIFA) [2011-68002-30220]; U.S. Department of Energy (DOE) Office of Science [DOE-DE-SC0006706]; NASA Land Cover and Land Use Change Program [NNX14AD94G]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; National Science Foundation [OCI-0725070, ACI-1238993]; GhG Europe FP7 FX C.R.S. was supported by National Aeronautics and Space Administration (NASA) grants NNX12AP74G, NNX10AG01A, and NNX11AO08A. J.B.F. carried out this research at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Funding for the Multiscale synthesis and Terrestrial Model Intercomparison Project (MsTMIP; http://nacp.ornl.gov/MsTMIP.shtml) activity was provided through NASA ROSES grant NNX10AG01A. Data management support for preparing, documenting, and distributing model driver and output data was performed by the Modeling and Synthesis Thematic Data Center at Oak Ridge National Laboratory (ORNL; http://nacp.ornl.gov), with funding through NASA ROSES grant NNH10AN681. Finalized MsTMIP data products are archived at the ORNL DAAC (http://daac.ornl.gov). This is MsTMIP contribution 5. Acknowledgments for specific MsTMIP participating models: Biome-BGC: Biome-BGC code was provided by the Numerical Terradynamic Simulation Group at the University of Montana. The computational facilities provided by NASA Earth Exchange at NASA Ames Research Center. CLM: This research is supported in part by the U.S. Department of Energy (DOE), Office of Science, Biological and Environmental Research. Oak Ridge National Laboratory is managed by UT-BATTELLE for DOE under contract DE-AC05-00OR22725. CLM4VIC: CLM4VIC simulations were supported in part by the U.S. Department of Energy (DOE), Office of Science, Biological and Environmental Research (BER) through the Earth System Modeling program and performed using the Environmental Molecular Sciences Laboratory(EMSL), a national scientific user facility sponsored by the U.S. DOE-BER and located at Pacific Northwest National Laboratory (PNNL). Participation of M. Huang in the MsTMIP synthesis is supported by the U.S. DOE-BER through the Subsurface Biogeochemical Research Program (SBR) as part of the SBR Scientific Focus Area (SFA) at the Pacific Northwest National Laboratory (PNNL). PNNL is operated for the U.S. DOE by BATTELLE Memorial Institute under contract DE-AC05-76RLO1830. DLEM: The Dynamic Land Ecosystem Model (DLEM) developed in the International Center for Climate and Global Change Research at Auburn University has been supported by NASA Interdisciplinary Science Program (IDS), NASA Land Cover/Land Use Change Program (LCLUC), NASA Terrestrial Ecology Program, NASA Atmospheric Composition Modeling and Analysis Program (ACMAP); NSF Dynamics of Coupled Natural-Human System Program (CNH), Decadal and Regional Climate Prediction using Earth System Models (EaSM); DOE National Institute for Climate Change Research; USDA AFRI Program; and EPA STAR Program. Integrated Science Assessment Model (ISAM) simulations were supported by the U.S. National Science Foundation (NSF-AGS-12-43071 and NSF-EFRI083598), the USDA National Institute of Food and Agriculture (NIFA) (2011-68002-30220), the U.S. Department of Energy (DOE) Office of Science (DOE-DE-SC0006706), and the NASA Land Cover and Land Use Change Program (NNX14AD94G). ISAM simulations were carried out at the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the U.S. Department of Energy under contract DE-AC02-05CH11231, and at the Blue Waters sustained-petascale computing, University of Illinois at Urbana-Champaign, which is supported by the National Science Foundation (awards OCI-0725070 and ACI-1238993) and the state of Illinois. LPJ-wsl: This work was conducted at LSCE, France, using a modified version of the LPJ version 3.; 1 model, originally made available by the Potsdam Institute for Climate Impact Research. ORCHIDEE-LSCE: ORCHIDEE is a global land surface model developed at the IPSL institute in France. The simulations were performed with the support of the GhG Europe FP7 grant with computing facilities provided by LSCE (Laboratoire des Sciences du Climat et de l'Environnement) or TGCC (Tres Grand Centre de Calcul). VISIT: VISIT was developed at the National Institute for Environmental Studies, Japan. This work was mostly conducted during a visiting stay at Oak Ridge National Laboratory. NR 95 TC 7 Z9 7 U1 4 U2 30 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 JUN 16 PY 2015 VL 42 IS 11 BP 4418 EP 4428 DI 10.1002/2015GL064002 PG 11 WC Geosciences, Multidisciplinary SC Geology GA CM2LI UT WOS:000357511200022 ER PT J AU Forrister, H Liu, J Scheuer, E Dibb, J Ziemba, L Thornhill, KL Anderson, B Diskin, G Perring, AE Schwarz, JP Campuzano-Jost, P Day, DA Palm, BB Jimenez, JL Nenes, A Weber, RJ AF Forrister, Haviland Liu, Jiumeng Scheuer, Eric Dibb, Jack Ziemba, Luke Thornhill, Kenneth L. Anderson, Bruce Diskin, Glenn Perring, Anne E. Schwarz, Joshua P. Campuzano-Jost, Pedro Day, Douglas A. Palm, Brett B. Jimenez, Jose L. Nenes, Athanasios Weber, Rodney J. TI Evolution of brown carbon in wildfire plumes SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE brown carbon; biomass burning; lifetime; plume evolution; photooxidation; bleaching ID SOUTHEASTERN UNITED-STATES; AEROSOL MASS-SPECTROMETRY; LIGHT-ABSORPTION; ORGANIC AEROSOL; OPTICAL-PROPERTIES; BLACK CARBON; SOLAR-RADIATION; HIGH-RESOLUTION; SECONDARY; COMBUSTION AB Particulate brown carbon (BrC) in the atmosphere absorbs light at subvisible wavelengths and has poorly constrained but potentially large climate forcing impacts. BrC from biomass burning has virtually unknown lifecycle and atmospheric stability. Here, BrC emitted from intense wildfires was measured in plumes transported over 2days from two main fires, during the 2013 NASA SEAC4RS mission. Concurrent measurements of organic aerosol (OA) and black carbon (BC) mass concentration, BC coating thickness, absorption angstrom ngstrom exponent, and OA oxidation state reveal that the initial BrC emitted from the fires was largely unstable. Using back trajectories to estimate the transport time indicates that BrC aerosol light absorption decayed in the plumes with a half-life of 9 to 15 h, measured over day and night. Although most BrC was lost within a day, possibly through chemical loss and/or evaporation, the remaining persistent fraction likely determines the background BrC levels most relevant for climate forcing. C1 [Forrister, Haviland; Liu, Jiumeng; Nenes, Athanasios; Weber, Rodney J.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Scheuer, Eric; Dibb, Jack] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Ziemba, Luke; Thornhill, Kenneth L.; Anderson, Bruce; Diskin, Glenn] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Perring, Anne E.; Schwarz, Joshua P.] Natl Ocean & Atmospher Adm, Earth Syst Res Lab, Div Chem Sci, Boulder, CO USA. [Perring, Anne E.; Schwarz, Joshua P.; Campuzano-Jost, Pedro; Day, Douglas A.; Palm, Brett B.; Jimenez, Jose L.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Campuzano-Jost, Pedro; Day, Douglas A.; Palm, Brett B.; Jimenez, Jose L.] Univ Colorado, Dept Chem & Biogeochem, Boulder, CO 80309 USA. [Nenes, Athanasios] Georgia Inst Technol, Sch Chem & Biomol Engn, Atlanta, GA 30332 USA. RP Weber, RJ (reprint author), Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. EM rodney.weber@eas.gatech.edu RI Liu, Jiumeng/K-2024-2012; Perring, Anne/G-4597-2013; Jimenez, Jose/A-5294-2008; schwarz, joshua/G-4556-2013; Manager, CSD Publications/B-2789-2015 OI Liu, Jiumeng/0000-0001-7238-593X; Perring, Anne/0000-0003-2231-7503; Jimenez, Jose/0000-0001-6203-1847; schwarz, joshua/0000-0002-9123-2223; FU GIT NASA [NNX12AB83G, NNX14AP74G]; UNH NASA [NNX12AB80G]; NASA [NNX12AC03G] FX All data used in this paper were collected as part of the NASA SEAC4RS mission and became available to the general public on 15 October 2014 through the NASA data archive. This project was funded by GIT NASA contracts NNX12AB83G and NNX14AP74G and UNH NASA contract NNX12AB80G. P.C.J., D.A.D., and J.L.J. were supported by NASA NNX12AC03G. NR 47 TC 21 Z9 21 U1 12 U2 83 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 JUN 16 PY 2015 VL 42 IS 11 BP 4623 EP 4630 DI 10.1002/2015GL063897 PG 8 WC Geosciences, Multidisciplinary SC Geology GA CM2LI UT WOS:000357511200046 ER PT J AU Wallace, WT Gazda, DB Limero, TF Minton, JM Macatangay, AV Dwivedi, P Fernandez, FM AF Wallace, William T. Gazda, Daniel B. Limero, Thomas F. Minton, John M. Macatangay, Ariel V. Dwivedi, Prabha Fernandez, Facundo M. TI Electrothermal Vaporization Sample Introduction for Spaceflight Water Quality Monitoring via Gas Chromatography-Differential Mobility Spectrometry SO ANALYTICAL CHEMISTRY LA English DT Article ID MASS-SPECTROMETRY; DIMETHYLSILANEDIOL AB In the history of manned spaceflight, environmental monitoring has relied heavily on archival sampling. However, with the construction of the International Space Station (ISS) and the subsequent extension in mission duration up to one year, an enhanced, real-time method for environmental monitoring is necessary. The station air is currently monitored for trace volatile organic compounds (VOCs) using gas chromatography-differential mobility spectrometry (GC-DMS) via the Air Quality Monitor (AQM), while water is analyzed to measure total organic carbon and biocide concentrations using the Total Organic Carbon Analyzer (TOCA) and the Colorimetric Water Quality Monitoring Kit (CWQMK), respectively. As mission scenarios extend beyond low Earth orbit, a convergence in analytical instrumentation to analyze both air and water samples is highly desirable. Since the AQM currently provides quantitative, compound-specific information for air samples and many of the targets in air are also common to water, this platform is a logical starting point for developing a multimatrix monitor. Here, we report on the interfacing of an electrothermal vaporization (ETV) sample introduction unit with a ground-based AQM for monitoring target analytes in water. The results show that each of the compounds tested from water have similar GC-DMS parameters as the compounds tested in air. Moreover, the ETV enabled AQM detection of dimethlsilanediol (DMSD), a compound whose analysis had proven challenging using other sample introduction methods. Analysis of authentic ISS water samples using the ETV-AQM showed that DMSD could be successfully quantified, while the concentrations obtained for the other compounds also agreed well with laboratory results. C1 [Wallace, William T.; Gazda, Daniel B.; Limero, Thomas F.] Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA. [Minton, John M.] Univ Arkansas, Little Rock, AR 72204 USA. [Macatangay, Ariel V.] NASA Johnson Space Ctr, Houston, TX 77058 USA. [Dwivedi, Prabha] Ctr Dis Control & Prevent, Atlanta, GA 30341 USA. [Fernandez, Facundo M.] Georgia Inst Technol, Sch Chem & Biochem, Atlanta, GA 30332 USA. RP Wallace, WT (reprint author), Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA. EM william.wallace-1@nasa.gov; facundo.fernandez@chemistry.gatech.edu FU NASA [NAS 9-02078, NNX13AF51G S02]; Arkansas Space Grant Consortium FX W.T.W., D.B.G., and T.F.L. acknowledge funding under NASA contract # NAS 9-02078. The work of J.M.M. was supported through the Arkansas Space Grant Consortium. W.T.W. would like to thank Sarah Castro (NASA Johnson Space Center) for critical editing and Zachary Pickett for his work on our early DMSD studies. F.M.F. thanks NASA for award number NNX13AF51G S02. NR 30 TC 2 Z9 2 U1 9 U2 22 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0003-2700 EI 1520-6882 J9 ANAL CHEM JI Anal. Chem. PD JUN 16 PY 2015 VL 87 IS 12 BP 5981 EP 5988 DI 10.1021/acs.analchem.5b00055 PG 8 WC Chemistry, Analytical SC Chemistry GA CL2DZ UT WOS:000356755100019 PM 25971650 ER PT J AU Del Genio, AD Chen, YH AF Del Genio, Anthony D. Chen, Yonghua TI Cloud-radiative driving of the Madden-Julian oscillation as seen by the A-Train SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Madden-Julian oscillation; clouds; radiative heating; convection ID STATIC ENERGY BUDGET; TROPICAL INTRASEASONAL OSCILLATION; MOISTURE-CONVECTION FEEDBACKS; TROPOPAUSE TRANSITION LAYER; COUPLED EQUATORIAL WAVES; STRATIFORM INSTABILITY; CLIMATE MODELS; PART I; MJO; VARIABILITY AB Cloud and water vapor radiative heating anomalies associated with convection may be an effective source of moist static energy driving the Madden-Julian Oscillation (MJO). In this paper 5years of radiative heating profiles derived from CloudSat radar and Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation data are analyzed to document radiative heating anomalies during the MJO. Atmospheric shortwave absorption and surface longwave radiation anomalies are of opposite sign and 10-20% as large as top-of-atmosphere outgoing longwave radiation (OLR) anomalies, confirming that OLR provides a useful estimate of the total column radiative heating anomaly. Positive anomalies generally peak about 1week before the MJO peak and are smallest over the Indian Ocean. Anomalies over the Maritime Continent are strongest and coincident with the MJO peak. Shortwave heating profile anomalies are weaker than longwave anomalies in the active region of the MJO but generally of opposite sign; thus, shortwave heating damps the longwave destabilization of the lower troposphere. The exception is the onset phase of the MJO, where shortwave and longwave heating anomalies due to thin cirrus are both positive in the upper troposphere and exert a stabilizing influence. Specific humidity anomalies in the middle troposphere reach 0.5gkg(-1), but the associated clear-sky heating anomaly is small. Radiative enhancement of column moist static energy becomes significant as precipitation increases before the MJO peak and remains high after the MJO peak as precipitation begins to decline. Elevated radiative heating after the peak may contribute to destabilizing the MJO. C1 [Del Genio, Anthony D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Chen, Yonghua] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. RP Del Genio, AD (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM anthony.d.delgenio@nasa.gov FU NASA CloudSat-CALIPSO Mission; NASA Modeling and Analysis Program FX The authors thank three anonymous reviewers for their constructive comments that improved the manuscript. The A-Train data used in this paper are available from the CloudSat Data Processing Center (http://www.cloudsat.cira.colostate.edu/dataHome.php). The Wheeler-Hendon MJO index is available at http://www.cawcr.gov.au/staff/mwheeler/maproom/. The NOAA Climate Prediction Center MJO indices are available at http://www.cpc.ncep.noaa.gov/products/precip/CWlink/daily_mjo_index/pent ad.html. The specific subsets of data used in our analysis are available from Y. Chen (yonghuachen@gmail.com). This research was supported by the NASA CloudSat-CALIPSO Mission and the NASA Modeling and Analysis Program. NR 60 TC 4 Z9 4 U1 2 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 16 PY 2015 VL 120 IS 11 BP 5344 EP 5356 DI 10.1002/2015JD023278 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CL5BV UT WOS:000356975700004 ER PT J AU Shindell, DT Faluvegi, G Rotstayn, L Milly, G AF Shindell, Drew T. Faluvegi, Greg Rotstayn, Leon Milly, George TI Spatial patterns of radiative forcing and surface temperature response SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE aerosols; climate; regional climate; aerosol forcing ID CLIMATE-CHANGE; ANTHROPOGENIC AEROSOLS; MODEL; SENSITIVITY; SPREAD; OZONE; CMIP5 AB Examination of effective radiative forcing (ERF), a measure of changes in Earth's energy balance, facilitates understanding the role of various drivers of climate change. For short-lived compounds, ERF can be highly inhomogeneous geographically. The relationship between the spatial patterns of ERF and surface temperature response is poorly characterized, however. We examine that relationship in the latest generation of global climate models. We find that the uneven distribution of historical aerosol, ozone, and land use forcing leads to substantial differences compared to the well-mixed greenhouse gases (WMGHG). There is a stronger response per unit global mean forcing to historical inhomogeneous forcing than to WMGHG both globally and in much of the Northern Hemisphere (NH) extratropics, in fairly good agreement with results inferred from observations. Our results indicate that the enhanced global mean response is attributable to the concentration of inhomogeneous forcing in the NH extratropics, where there is strongest sensitivity to forcing, rather than to processes specific to the inhomogeneous forcers. In many regions, inclusion of inhomogeneous forcing greatly increases the spread in historical temperature changes simulated by the models, suggesting that better forcing characterization could play an important role in improving modeling of decadal-scale regional climate change. Finally, incorporating observed temperatures, the results provide estimates of global historical aerosol forcing (-1.00.4Wm(-2)) consistent with other studies (though with narrower uncertainties) and also provide constraints on NH and NH extratropical historical aerosol forcing (-1.40.6 and -1.20.6Wm(-2), respectively) and aerosol+ozone forcing. C1 [Shindell, Drew T.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. [Faluvegi, Greg; Milly, George] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Rotstayn, Leon] CSIRO, Oceans & Atmosphere Flagship, Aspendale, Vic, Australia. RP Shindell, DT (reprint author), Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. EM drew.shindell@duke.edu RI Shindell, Drew/D-4636-2012; Rotstayn, Leon/A-1756-2012 OI Rotstayn, Leon/0000-0002-2385-4223 FU NASA FX We thank the World Climate Research Programme's Working Group on Coupled Modelling, the U.S. Department of Energy's Program for Climate Model Diagnosis and Intercomparison, and the climate modeling groups from CMIP and the Atmospheric Chemistry and Climate Model Intercomparison Project for making available their model output. Data used in this analysis are available via the CMIP5 or ACCMIP archives (models; http://cmip-pcmdi.llnl.gov/cmip5/data_portal.html and http://www.giss.nasa.gov/projects/accmip/) and from the University of York (observations; http://www-users.york.ac.uk/similar to kdc3/papers/coverage2013/series.html). We also thank David Considine for support via NASA's Modeling, Analysis and Prediction Program, and Piers Forster and two anonymous reviewers for comments. Computational resources supporting this work were provided by the NASA High-End Computing Program through the NASA Center for Climate Simulation at Goddard Space Flight Center. NR 44 TC 8 Z9 8 U1 3 U2 22 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 JUN 16 PY 2015 VL 120 IS 11 BP 5385 EP 5403 DI 10.1002/2014JD022752 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CL5BV UT WOS:000356975700007 ER PT J AU Garfinkel, CI Hurwitz, MM Oman, LD AF Garfinkel, C. I. Hurwitz, M. M. Oman, L. D. TI Effect of recent sea surface temperature trends on the Arctic stratospheric vortex SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Arctic stratosphere; SST trends; ozone trends; ozone loss ID PACIFIC DECADAL OSCILLATION; OZONE-DEPLETING SUBSTANCES; ATMOSPHERIC CIRCULATION; NORTHERN-HEMISPHERE; PROPAGATION; MODEL; TROPOSPHERE; EVENTS; MSU AB Comprehensive chemistry-climate model experiments and observational data are used to show that up to half of the satellite era early springtime cooling trend in the Arctic lower stratosphere was caused by changing sea surface temperatures (SSTs). An ensemble of experiments forced only by changing SSTs is compared to an ensemble of experiments in which both the observed SSTs and chemically and radiatively active trace species are changing. By comparing the two ensembles, it is shown that warming of Indian Ocean, North Pacific, and North Atlantic SSTs and cooling of the tropical Pacific have strongly contributed to recent polar stratospheric cooling in late winter and early spring. When concentrations of ozone-depleting substances and greenhouse gases are fixed, polar ozone concentrations show a small but robust decline due to changing SSTs. Ozone loss is larger in the presence of changing concentrations of ozone-depleting substances and greenhouse gases. The stratospheric changes can be understood by examining the tropospheric height and heat flux anomalies generated by the anomalous SSTs. Finally, recent SST changes have contributed to a decrease in the frequency of late winter stratospheric sudden warmings. C1 [Garfinkel, C. I.] Hebrew Univ Jerusalem, Fredy & Nadine Herrmann Inst Earth Sci, Jerusalem, Israel. [Hurwitz, M. M.; Oman, L. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hurwitz, M. M.] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21239 USA. RP Garfinkel, CI (reprint author), Hebrew Univ Jerusalem, Fredy & Nadine Herrmann Inst Earth Sci, Jerusalem, Israel. EM chaim.garfinkel@mail.huji.ac.il RI Oman, Luke/C-2778-2009 OI Oman, Luke/0000-0002-5487-2598 FU Hebrew University of Jerusalem; Israel Science Foundation [1558/14]; NASA ACMAP program FX This work was supported by a startup grant from Hebrew University of Jerusalem and by the Israel Science Foundation (grant 1558/14). M.M.H. acknowledges support from the NASA ACMAP program. We would also like to thank those involved in model development at GSFC and the high-performance computing resources that were provided by NASA's Advanced Supercomputing Division. We would also like to thank Feng Li for making available the coupled ocean-atmosphere integration. We thank the three anonymous reviewers for their helpful comments. We would like to thank Greg Bodeker of Bodeker Scientific for providing the combined total column ozone database available at http://www.bodekerscientific.com/data/total-column-ozone. All data necessary to understand, evaluate, replicate, and build upon the reported research will be made available and accessible upon request to C.I.G. (chaim.garfinkel@mail.huji.ac.il). NR 60 TC 8 Z9 8 U1 2 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 16 PY 2015 VL 120 IS 11 BP 5404 EP 5416 DI 10.1002/2015JD023284 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CL5BV UT WOS:000356975700008 ER PT J AU Yasunari, TJ Koster, RD Lau, WKM Kim, KM AF Yasunari, Teppei J. Koster, Randal D. Lau, William K. M. Kim, Kyu-Myong TI Impact of snow darkening via dust, black carbon, and organic carbon on boreal spring climate in the Earth system SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE snow darkening; dust; black carbon; organic carbon; climate; global model ID ASIAN SUMMER MONSOON; LIGHT-ABSORBING IMPURITIES; CATCHMENT-BASED APPROACH; LAND-SURFACE PROCESSES; HIMALAYAN GLACIERS; TIBETAN PLATEAU; GOCART MODEL; ICE CORE; PREMONSOON SEASON; WATER EQUIVALENT AB Dust, black carbon (BC), and organic carbon (OC) aerosols, when deposited onto snow, are known to reduce the albedo of the snow (i.e., snow darkening effect (SDE)). Here using the NASA Goddard Earth Observing System Model, Version 5 (GEOS-5) with aerosol tracers and a state-of-the-art snow darkening module (GOddard SnoW Impurity Module: GOSWIM) for the land surface, we examine the role of SDE on climate in the boreal spring snowmelt season. SDE is found to produce significant surface warming (over 15Wm(-2)) over broad areas in midlatitudes, with dust being the most important contributor to the warming in central Asia and the western Himalayas and with BC having larger impact in the Europe, eastern Himalayas, East Asia, and North America. The contribution of OC to the warming is generally low but still significant mainly over southeastern Siberia, northeastern East Asia, and western Canada (similar to 19% of the total solar visible absorption by these snow impurities). The simulations suggest that SDE strengthens the boreal spring water cycle in East Asia through water recycling and moisture advection from the ocean and contributes to the maintenance of dry conditions in parts of a region spanning Europe to central Asia, partially through feedback on the model's background climatology. Overall, our study suggests that the existence of SDE in the Earth system associated with dust, BC, and OC contributes significantly to enhanced surface warming over continents in northern hemisphere midlatitudes during boreal spring, raising the surface skin temperature by approximately 3-6K near the snowline. C1 [Yasunari, Teppei J.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21046 USA. [Yasunari, Teppei J.; Koster, Randal D.; Lau, William K. M.; Kim, Kyu-Myong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lau, William K. M.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. RP Yasunari, TJ (reprint author), Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21046 USA. EM teppei.j.yasunari@nasa.gov RI Kim, Kyu-Myong/G-5398-2014; Koster, Randal/F-5881-2012; Yasunari, Teppei/E-5374-2010; Lau, William /E-1510-2012 OI Koster, Randal/0000-0001-6418-6383; Yasunari, Teppei/0000-0002-9896-9404; Lau, William /0000-0002-3587-3691 FU NASA Modeling, Analysis, and Prediction (MAP) Program by NASA Headquarters FX The NASA Modeling, Analysis, and Prediction (MAP) Program by NASA Headquarters supported this work. We thank the MODIS snow and ice team for the development of the snow cover fraction data product; NASA Center for Climate Simulation for the GEOS-5 simulations; the NASA Global Modeling and Assimilation Office (GMAO) for the development of GEOS-5, producing the initial conditions and the MERRA data product; and the NASA GES DISC for the online provision of MERRA data. We also thank Lawrence L. Takacs (Science Systems and Applications, Inc.), Arlindo da Silva (NASA), and Peter R. Colarco (NASA) at NASA Goddard Space Flight Center for helping us in this work. Useful information on our discussion was obtained from Taichu Y. Tanaka (Japan Meteorological Agency), Teruo Aoki (Meteorological Research Institute), and Ritesh Gautam (Indian Institute of Technology). The GEOS-5 outputs and/or other data used in this study are available via contact with Teppei J. Yasunari (teppei.j.yasunari@nasa.gov or t.j.yasunari@eng.hokudai.ac.jp, as of 1 July 2015) and/or Kyu-Myong Kim (kyu-myong.kim-1@nasa.gov). NR 116 TC 9 Z9 9 U1 4 U2 22 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 JUN 16 PY 2015 VL 120 IS 11 BP 5485 EP 5503 DI 10.1002/2014JD022977 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CL5BV UT WOS:000356975700013 ER PT J AU Meyer, K Platnick, S Zhang, ZB AF Meyer, Kerry Platnick, Steven Zhang, Zhibo TI Simultaneously inferring above-cloud absorbing aerosol optical thickness and underlying liquid phase cloud optical and microphysical properties using MODIS SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Clouds; Aerosols; Remote Sensing ID CALIPSO LIDAR MEASUREMENTS; SATELLITE-OBSERVATIONS; MULTIPLE-SCATTERING; RADIATIVE-TRANSFER; C-130 AIRCRAFT; SAFARI 2000; CALIOP; DEPTH; RETRIEVAL; ALGORITHM AB The regional haze over the southeast (SE) Atlantic Ocean induced by biomass burning in southern Africa can be problematic for passive imager-based retrievals of the underlying quasi-permanent marine boundary layer (MBL) clouds and for estimates of top-of-atmosphere (TOA) aerosol direct radiative effect (DRE). Here an algorithm is introduced to simultaneously retrieve above-cloud aerosol optical thickness (AOT), the cloud optical thickness (COT), and cloud effective particle radius (CER) of the underlying MBL clouds while also providing pixel-level estimates of retrieval uncertainty. This approach utilizes reflectance measurements at six Moderate Resolution Imaging Spectroradiometer (MODIS) channels from the visible to the shortwave infrared. Retrievals are run under two aerosol model assumptions on 8years (2006-2013) of June-October Aqua MODIS data over the SE Atlantic, from which a regional cloud and above-cloud aerosol climatology is produced. The cloud retrieval methodology is shown to yield COT and CER consistent with those from the MODIS operational cloud product (MOD06) when forcing AOT to zero, while the full COT-CER-AOT retrievals that account for the above-cloud aerosol attenuation increase regional monthly mean COT and CER by up to 9% and 2%, respectively. Retrieved AOT is roughly 3 to 5 times larger than the collocated 532nm Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) retrievals, though closer agreement is observed with the CALIOP 1064nm retrievals, a result consistent with previous case study analyses. Regional cloudy-sky above-cloud aerosol DRE calculations are also performed that illustrate the importance of the aerosol model assumption and underlying cloud retrievals. C1 [Meyer, Kerry] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21046 USA. [Meyer, Kerry; Platnick, Steven] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zhang, Zhibo] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21228 USA. RP Meyer, K (reprint author), Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21046 USA. EM kerry.meyer@nasa.gov RI Meyer, Kerry/E-8095-2016; Platnick, Steven/J-9982-2014 OI Meyer, Kerry/0000-0001-5361-9200; Platnick, Steven/0000-0003-3964-3567 FU NASA Radiation Sciences Program; NASA [NNH14CK44C, NNX14AI35G] FX The authors would like to thank Rob Levy for his expertise with the MODIS Dark Target aerosol models, and Nandana Amarasinghe for his efforts toward enhancing our forward radiative transfer modeling capabilities. The authors would also like to thank Robert J. Swap for invaluable discussions about aerosol transport over the southern Atlantic Ocean. This research was supported by the NASA Radiation Sciences Program and by funding from NASA CloudSat and CALIPSO Science Team grant NNH14CK44C managed by David Considine; Z. Zhang acknowledges funding support from the NASA New Investigator Program (NNX14AI35G) managed by Ming-Ying Wei. The MODIS data used in this study are publically available from the NASA Level 1 and Atmosphere Archive and Distribution System (LAADS) (http://ladsweb.nascom.nasa.gov); the CALIOP data are publically available from the NASA Langley Research Center's Atmospheric Science Data Center (ASDC) CALIPSO Search and Subsetting web application (https://www-calipso.larc.nasa.gov/search/login.php). NR 73 TC 8 Z9 8 U1 5 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 16 PY 2015 VL 120 IS 11 BP 5524 EP 5547 DI 10.1002/2015JD023128 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CL5BV UT WOS:000356975700015 ER PT J AU Haddad, ZS Steward, JL Tseng, HC Vukicevic, T Chen, SH Hristova-Veleva, S AF Haddad, Z. S. Steward, J. L. Tseng, H. -C. Vukicevic, T. Chen, S. -H. Hristova-Veleva, S. TI A data assimilation technique to account for the nonlinear dependence of scattering microwave observations of precipitation SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE precipitation; data assimilation; microwave ID SATELLITE DATA ASSIMILATION; CLOUD; IMPLEMENTATION; RETRIEVAL; SYSTEM; MODEL AB Satellite microwave observations of rain, whether from radar or passive radiometers, depend in a very crucial way on the vertical distribution of the condensed water mass and on the types and sizes of the hydrometeors in the volume resolved by the instrument. This crucial dependence is nonlinear, with different types and orders of nonlinearity that are due to differences in the absorption/emission and scattering signatures at the different instrument frequencies. Because it is not monotone as a function of the underlying condensed water mass, the nonlinearity requires great care in its representation in the observation operator, as the inevitable uncertainties in the numerous precipitation variables are not directly convertible into an additive white uncertainty in the forward calculated observations. In particular, when attempting to assimilate such data into a cloud-permitting model, special care needs to be applied to describe and quantify the expected uncertainty in the observations operator in order not to turn the implicit white additive uncertainty on the input values into complicated biases in the calculated radiances. One approach would be to calculate the means and covariances of the nonlinearly calculated radiances given an a priori joint distribution for the input variables. This would be a very resource-intensive proposal if performed in real time. We propose a representation of the observation operator based on performing this moment calculation off line, with a dimensionality reduction step to allow for the effective calculation of the observation operator and the associated covariance in real time during the assimilation. The approach is applicable to other remotely sensed observations that depend nonlinearly on model variables, including wind vector fields. The approach has been successfully applied to the case of tropical cyclones, where the organization of the system helps in identifying the dimensionality-reducing variables. C1 [Haddad, Z. S.; Steward, J. L.; Hristova-Veleva, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Haddad, Z. S.; Steward, J. L.; Hristova-Veleva, S.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. [Tseng, H. -C.; Chen, S. -H.] Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA. [Vukicevic, T.] NOAA, AOML, Miami, FL USA. RP Haddad, ZS (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM zhaddad@jifresse.ucla.edu RI Chen, Hua/B-7664-2014 OI Chen, Hua/0000-0002-9493-6939 FU National Aeronautics and Space Administration; National Oceanic and Atmospheric Administration through Hurricane Forecasting Improvement Project FX This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The research was supported by a grant from the National Oceanic and Atmospheric Administration through the Hurricane Forecasting Improvement Project. The TRMM data and our forward simulations can be found at http://trmm.jpl.nasa.gov/2015JD023107_data/. NR 19 TC 3 Z9 3 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 16 PY 2015 VL 120 IS 11 BP 5548 EP 5563 DI 10.1002/2015JD023107 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CL5BV UT WOS:000356975700016 ER PT J AU Rong, PP Yue, J Russell, JM Lumpe, JD Gong, J Wu, DL Randall, CE AF Rong, P. P. Yue, J. Russell, J. M., III Lumpe, J. D. Gong, J. Wu, D. L. Randall, C. E. TI Horizontal winds derived from the polar mesospheric cloud images as observed by the CIPS instrument on the AIM satellite SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE CIPS; PMCs; horizontal winds; pattern matching ID PARTICLE-SIZE EXPERIMENT; NOCTILUCENT CLOUDS; GRAVITY-WAVES; MODEL; ICE; THERMOSPHERE; TEMPERATURE; NLC AB A cloud pattern matching technique is applied to polar mesospheric cloud (PMC) images taken by the Cloud Imaging and Particle Size instrument (CIPS) to infer the wind velocities in the mesopause region. CIPS measurements are analyzed to detect patterns that repeat from one orbit to the next but are displaced in location; the displacement provides a measure of the wind velocity. Pattern matching is achieved by resampling the CIPS data to longitude and latitude grids with the grid-box size forced at similar to 5km in both directions. The correlated patterns are searched within a geographic region referred to as a frame of similar to 500km in longitudex400km in latitude. The histograms of the derived velocities indicate that easterly winds prevail, with a mean zonal wind of -20 to -15m/s. Mean meridional winds are overall small, but in late summer the histogram indicated a poleward wind of similar to 20-30m/s. The variability of CIPS cloud albedo on consecutive orbits is also examined at fixed geolocations. The statistical results suggest that similar to 86% of pairs underwent mean cloud albedo variation of < 50% on consecutive orbits, suggesting a moderate change. It is also found that the correlation of the cloud structures between two consecutive orbits at a fixed location is generally poor. These findings suggest that cloud patterns are subject to wind advection, but the cloud patches are more extended in size than the movement that occurs. Cloud voids are found to be more likely to remain at the same geolocations. C1 [Rong, P. P.; Yue, J.; Russell, J. M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. [Lumpe, J. D.] Computat Phys Inc, Boulder, CO USA. [Gong, J.] Univ Space Res Assoc, Greenbelt, MD USA. [Wu, D. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Randall, C. E.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. RP Rong, PP (reprint author), Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. EM ppr@jhu.edu RI Yue, Jia/D-8177-2011; Wu, Dong/D-5375-2012; Randall, Cora/L-8760-2014 OI Randall, Cora/0000-0002-4313-4397 FU NASA Small Explorer Program [NAS5-03132] FX This work was supported by the NASA Small Explorer Program through contract NAS5-03132. We acknowledge all members of AIM science team, especially the CIPS team, for the consistent support on this project over a 2 year period. CIPS data can be accessed through website http://lasp.colorado.edu/aim/download-data.html. The data used in this study were processed by Jerry Lumpe (lumpe@cpi.com) from Computational Physics, Inc., Boulder, Colorado. NR 42 TC 2 Z9 2 U1 1 U2 3 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 JUN 16 PY 2015 VL 120 IS 11 BP 5564 EP 5584 DI 10.1002/2014JD022813 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CL5BV UT WOS:000356975700017 ER PT J AU Marchenko, S Krotkov, NA Lamsal, LN Celarier, EA Swartz, WH Bucsela, EJ AF Marchenko, S. Krotkov, N. A. Lamsal, L. N. Celarier, E. A. Swartz, W. H. Bucsela, E. J. TI Revising the slant column density retrieval of nitrogen dioxide observed by the Ozone Monitoring Instrument SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE remote sensing; instruments and techniques; atmosphere: composition and chemistry ID ABSORPTION CROSS-SECTION; TROPOSPHERIC NO2; SATELLITE RETRIEVALS; RAMAN-SCATTERING; EMISSIONS; OMI; MODEL; SCIAMACHY; CHEMISTRY; SPACE AB Nitrogen dioxide retrievals from the Aura/Ozone Monitoring Instrument (OMI) have been used extensively over the past decade, particularly in the study of tropospheric air quality. Recent comparisons of OMI NO2 with independent data sets and models suggested that the OMI values of slant column density (SCD) and stratospheric vertical column density (VCD) in both the NASA OMNO2 and Royal Netherlands Meteorological Institute DOMINO products are too large, by around 10-40%. We describe a substantially revised spectral fitting algorithm, optimized for the OMI visible light spectrometer channel. The most important changes comprise a flexible adjustment of the instrumental wavelength shifts combined with iterative removal of the ring spectral features; the multistep removal of instrumental noise; iterative, sequential estimates of SCDs of the trace gases in the 402-465nm range. These changes reduce OMI SCD(NO2) by 10-35%, bringing them much closer to SCDs retrieved from independent measurements and models. The revised SCDs, submitted to the stratosphere-troposphere separation algorithm, give tropospheric VCDs approximate to 10-15% smaller in polluted regions, and up to approximate to 30% smaller in unpolluted areas. Although the revised algorithm has been optimized specifically for the OMI NO2 retrieval, our approach could be more broadly applicable. C1 [Marchenko, S.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Marchenko, S.; Krotkov, N. A.; Lamsal, L. N.; Celarier, E. A.; Swartz, W. H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lamsal, L. N.; Celarier, E. A.] Univ Space Res Assoc, Columbia, MD USA. [Swartz, W. H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Bucsela, E. J.] SRI Int, Menlo Pk, CA 94025 USA. RP Marchenko, S (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA. EM sergey_marchenko@ssaihq.com RI Krotkov, Nickolay/E-1541-2012; Swartz, William/A-1965-2010 OI Krotkov, Nickolay/0000-0001-6170-6750; Swartz, William/0000-0002-9172-7189 FU NASA's Earth Science Division FX We thank A. Richter for kindly providing us with the preliminary SCD(NO2) fitting results for the OMI orbits #03610 and #03622 (both from 20 March 2005). The OMI OMNO2 data used in this analysis are publicly available at http://disc.sci.gsfc.nasa.gov/Aura/data-holdings/OMI, and the DOMINO product is available at http://www.temis.nl. The SCIAMACHY data were obtained from the Aura Validation Data Center, http://avdc.gsfc.nasa.gov. This work was supported by NASA's Earth Science Division through an Aura science team grant. The Dutch-and Finnish-built OMI instrument is part of the NASA EOS Aura satellite payload. The OMI instrument is managed by KNMI and the Netherlands Agency for Aerospace Programs. We wish to thank the referees for their constructive, helpful criticism. NR 69 TC 9 Z9 9 U1 2 U2 16 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 JUN 16 PY 2015 VL 120 IS 11 BP 5670 EP 5692 DI 10.1002/2014JD022913 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CL5BV UT WOS:000356975700023 PM 27708989 ER PT J AU Prather, MJ Hsu, J DeLuca, NM Jackman, CH Oman, LD Douglass, AR Fleming, EL Strahan, SE Steenrod, SD Sovde, OA Isaksen, ISA Froidevaux, L Funke, B AF Prather, Michael J. Hsu, Juno DeLuca, Nicole M. Jackman, Charles H. Oman, Luke D. Douglass, Anne R. Fleming, Eric L. Strahan, Susan E. Steenrod, Stephen D. Sovde, O. Amund Isaksen, Ivar S. A. Froidevaux, Lucien Funke, Bernd TI Measuring and modeling the lifetime of nitrous oxide including its variability SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE nitrous oxide; atmospheric lifetime; perturbation lifetime; stratospheric photochemistry; models and measurements; anthropogenic emissions ID ATMOSPHERIC CHEMISTRY; TIME SCALES; STRATOSPHERIC OZONE; TRANSPORT; N2O; NOY; CFC-12; GASES; CYCLE AB The lifetime of nitrous oxide, the third-most-important human-emitted greenhouse gas, is based to date primarily on model studies or scaling to other gases. This work calculates a semiempirical lifetime based on Microwave Limb Sounder satellite measurements of stratospheric profiles of nitrous oxide, ozone, and temperature; laboratory cross-section data for ozone and molecular oxygen plus kinetics for O(D-1); the observed solar spectrum; and a simple radiative transfer model. The result is 1169years. The observed monthly-to-biennial variations in lifetime and tropical abundance are well matched by four independent chemistry-transport models driven by reanalysis meteorological fields for the period of observation (2005-2010), but all these models overestimate the lifetime due to lower abundances in the critical loss region near 32km in the tropics. These models plus a chemistry-climate model agree on the nitrous oxide feedback factor on its own lifetime of 0.940.01, giving N2O perturbations an effective residence time of 109years. Combining this new empirical lifetime with model estimates of residence time and preindustrial lifetime (123years) adjusts our best estimates of the human-natural balance of emissions today and improves the accuracy of projected nitrous oxide increases over this century. C1 [Prather, Michael J.; Hsu, Juno; DeLuca, Nicole M.] Univ Calif Irvine, Earth Syst Sci, Irvine, CA 92697 USA. [Jackman, Charles H.; Oman, Luke D.; Douglass, Anne R.; Fleming, Eric L.; Steenrod, Stephen D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fleming, Eric L.; Strahan, Susan E.] Sci Syst & Applicat Inc, Lanham, MD USA. [Steenrod, Stephen D.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res Ctr, Columbia, MD USA. [Sovde, O. Amund] Ctr Int Climate & Environm Res Oslo, Oslo, Norway. [Isaksen, Ivar S. A.] Univ Oslo, Dept Geosci, Oslo, Norway. [Froidevaux, Lucien] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Funke, Bernd] CSIC, Inst Astrofis Andalucia, Granada, Spain. RP Prather, MJ (reprint author), Univ Calif Irvine, Earth Syst Sci, Irvine, CA 92697 USA. EM mprather@uci.edu RI Jackman, Charles/D-4699-2012; Douglass, Anne/D-4655-2012; Funke, Bernd/C-2162-2008; Oman, Luke/C-2778-2009; Sovde Haslerud, Amund/H-2850-2016; OI Funke, Bernd/0000-0003-0462-4702; Oman, Luke/0000-0002-5487-2598; Sovde Haslerud, Amund/0000-0002-3812-3837; Prather, Michael/0000-0002-9442-8109 FU NASA [NNX09AJ47G, NNX13AL12G]; DOE [DE-SC0007021, DE-SC0012536]; UCI NSF REU [1005042]; NASA MAP program; Spanish MCINN [AYA2011-23552]; EC FEDER funds; NASA FX Tabulated data sets used in the figures here will be posted at ftp://halo.ess.uci.edu or are otherwise available from the corresponding author (mprather@uci.edu). Research at UCI was supported by NASA grants NNX09AJ47G and NNX13AL12G and DOE awards DE-SC0007021 and DE-SC0012536. N.M.D. was supported by UCI NSF REU 1005042. The GEOSCCM contribution was supported by the NASA MAP program. B.F. was supported by the Spanish MCINN under grant AYA2011-23552 and EC FEDER funds. Work at the Jet Propulsion Laboratory was performed under contract with NASA. The assistance of Ryan Fuller (at JPL) for the creation of MLS data sets used here is acknowledged. The GSFC 2-D model contribution was supported by the NASA Atmospheric Composition: Modeling and Analysis Program. NR 54 TC 3 Z9 3 U1 2 U2 22 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 JUN 16 PY 2015 VL 120 IS 11 BP 5693 EP 5705 DI 10.1002/2015JD023267 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CL5BV UT WOS:000356975700024 ER PT J AU Bernard, F McGillen, MR Fleming, EL Jackman, CH Burkholder, JB AF Bernard, Francois McGillen, Max R. Fleming, Eric L. Jackman, Charles H. Burkholder, James B. TI CBrF3 (Halon-1301): UV absorption spectrum between 210 and 320 K, atmospheric lifetime, and ozone depletion potential SO JOURNAL OF PHOTOCHEMISTRY AND PHOTOBIOLOGY A-CHEMISTRY LA English DT Article DE Bromotrifluoromethane; ozone depletion potential; UV absorption spectrum; temperature dependence; photolysis lifetime ID TEMPERATURE-DEPENDENCE; CROSS-SECTIONS; ULTRAVIOLET; METHANE; IMPACT; PHASE; BR AB CBrF3 (Halon-1301) is a man-made ozone depleting substance that is a major source of bromine in the Earth's stratosphere. Halon-1301 is predominantly removed from the atmosphere by UV photolysis in the stratosphere at wavelengths between 200 and 225 nm. The existing level of uncertainty in the Halon-1301 UV absorption spectrum temperature-dependence directly impacts the ability to model stratospheric ozone chemistry and climate change. In this work, the UV absorption spectrum of Halon-1301 between 195 and 235 nm was measured over the temperature range 210-320 K. An empirical parameterization of the spectrum and its temperature dependence is presented. The present results are critically compared with results from previous studies and the current recommendation for use in atmospheric models. A global annually averaged lifetime for Halon-1301 of 74.6 (73.7-75.5) years was calculated using a 2-D atmospheric model and the present results. The range of lifetimes given in parenthesis represents the possible values due solely to the 2 sigma uncertainty in the Halon-1301 UV spectrum obtained in this work. In addition, the CBrF3 ozone depletion potential was calculated using the 2-D model to be 18.6 (+/- 0.1) using the UV spectrum and 2 sigma uncertainty from this work. Published by Elsevier B.V. C1 [Bernard, Francois; McGillen, Max R.; Burkholder, James B.] NOAA, Earth Syst Res Lab, Div Chem Sci, Dept Commerce, Boulder, CO 80305 USA. [Bernard, Francois; McGillen, Max R.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Fleming, Eric L.; Jackman, Charles H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fleming, Eric L.] Sci Syst & Applicat Inc, Lanham, MD USA. RP Burkholder, JB (reprint author), NOAA, Earth Syst Res Lab, Div Chem Sci, Dept Commerce, Boulder, CO 80305 USA. EM james.b.burkholder@noaa.gov RI Jackman, Charles/D-4699-2012; McGillen, Max/G-5196-2011; BERNARD, Francois/F-2864-2014; Manager, CSD Publications/B-2789-2015 OI McGillen, Max/0000-0002-1623-5985; BERNARD, Francois/0000-0002-6116-3167; FU NOAA's Atmospheric Chemistry, Carbon Cycle, and Climate (AC4) Program; NASA's Atmospheric Composition Program FX This work was supported in part by NOAA's Atmospheric Chemistry, Carbon Cycle, and Climate (AC4) Program and NASA's Atmospheric Composition Program. NR 19 TC 3 Z9 3 U1 0 U2 8 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 1010-6030 J9 J PHOTOCH PHOTOBIO A JI J. Photochem. Photobiol. A-Chem. PD JUN 15 PY 2015 VL 306 BP 13 EP 20 DI 10.1016/j.jphotochem.2015.03.012 PG 8 WC Chemistry, Physical SC Chemistry GA CK3JJ UT WOS:000356112100002 ER PT J AU Yavasli, DD Tucker, CJ Melocik, KA AF Yavasli, Dogukan Dogu Tucker, Compton J. Melocik, Katherine A. TI Change in the glacier extent in Turkey during the Landsat Era SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Mountain glaciers; Satellite data; Climate change; Turkey; Landsat; ASTER ID NORTH-ATLANTIC OSCILLATION; TRENDS; VARIABILITY; PRECIPITATION; NUMBERS; COVER AB We report the latest study for small glaciers, using Turkey as an example, and update previous studies of glaciers in Turkey from the 1970s to 2012-2013. We used seventy-two Landsat scenes from the Multispectral Scanner (MSS), Return Beam Vidicon-3 (RBV-3), Thematic Mapper (TM), Enhanced Thematic Mapper plus (ETM+), and Operational Land Imager (OLI); five Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) images; and forty-one commercial satellite images. IKONOS, Quickbird-2, GeoEye-1, and WorldView-1 and -2 commercial satellite images were used to evaluate mapping accuracies, to understand debris-covered glacial margins, to map glacier margins in shadows, and to better determine the area of the smaller glaciers in Turkey. We also used nine Landsat-5 simultaneously acquired TM and MSS images to more accurately process MSS imagery from the 1970s. The area of the glaciers in Turkey decreased from 25 km(2) in the 1970s to 10.85 km(2) in 2012-2013. By 2012-2013, five glaciers had disappeared, six were less than 0.5 km(2), one was 0.8 km(2), and only two were 3.0 km(2) or larger. No trends in 1980 to 2012 annual precipitation, 1980 to 2012 winter precipitation, and 1980 to 2008 cloud cover extent were found, while surface temperatures increased, with summer minimum temperatures showing the greatest increases. We attribute glacier recession in Turkey from the 1970s to 2012-2013 to increasing summer minimum temperatures with no changes in precipitation or cloud cover over this time period. (C) 2015 Elsevier Inc. All rights reserved. C1 [Yavasli, Dogukan Dogu] Ege Univ, Dept Geog, Izmir, Turkey. [Tucker, Compton J.] NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. RP Yavasli, DD (reprint author), Ege Univ, Dept Geog, Izmir, Turkey. EM dogukan.yavasli@ege.edu.tr; compton.j.tucker@nasa.gov; katherine.a.melocik@nasa.gov RI Yavasli, Dogukan/D-7623-2015 OI Yavasli, Dogukan/0000-0002-0150-867X NR 26 TC 4 Z9 4 U1 1 U2 8 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 JUN 15 PY 2015 VL 163 BP 32 EP 41 DI 10.1016/j.rse.2015.03.002 PG 10 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA CJ8RN UT WOS:000355771300004 ER PT J AU Sorek-Hamer, M Kloog, I Koutrakis, P Strawa, AW Chatfield, R Cohen, A Ridgway, WL Broday, DM AF Sorek-Hamer, Meytar Kloog, Itai Koutrakis, Petros Strawa, Anthony W. Chatfield, Robert Cohen, Ayala Ridgway, William L. Broday, David M. TI Assessment of PM2.5 concentrations over bright surfaces using MODIS satellite observations SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Dark Target; Deep Blue; Aerosol optical depth (AOD); MODIS; PM2.5; Mixed effects models ID AEROSOL OPTICAL DEPTH; GROUND-LEVEL PM2.5; PARTICULATE MATTER CONCENTRATIONS; IMAGING SPECTRORADIOMETER MODIS; AIR-QUALITY; UNITED-STATES; RETRIEVALS; MORTALITY; THICKNESS; PRODUCTS AB Exposure to particles with an aerodynamic diameter smaller than 2.5 mu m (PM2.5) adversely impacts human health. In many geographical regions where ground PM2.5 monitoring is spatially sparse and unsuitable for environmental health inference, satellite remote sensing can potentially be used for estimating human exposure to PM2.5. However, retrieval of the aerosol optical depth (AOD) using the Dark Target (DT) algorithm is uncertain in many regions worldwide (e.g. western USA, the Middle East and central Asia) due to low signal-to-noise ratio as a result of high surface reflectivity in the spectral bands used by the algorithm. In this study we use the Deep Blue (DB) algorithm as well as a combined DB-DT algorithm for AOD retrievals. The AOD products are used to predict ground PM2.5 using mixed effects models and the daily calibration approach. Models for the two study areas (Israel and San Joaquin Valley, Central California) were developed independently and then compared to each other. Using the AOD(DB) within a mixed effects model considerably improved PM2.5 prediction in high reflectance regions, revealing in both study areas enhanced model performance (in terms of both R-2 and the root mean square prediction error), significant increase in the spatiotemporal availability of the AOD product, and improved PM2.5 prediction relative to using AOD(DT) retrievals. (C) 2015 Elsevier Inc. All rights reserved. C1 [Sorek-Hamer, Meytar; Broday, David M.] Civil & Environm Engn, Haifa, Israel. [Kloog, Itai] Ben Gurion Univ Negev, Dept Geog & Environm Dev, Beer Sheva, Israel. [Koutrakis, Petros] Harvard Univ, Sch Publ Hlth, Dept Environm Hlth, Boston, MA 02115 USA. [Strawa, Anthony W.; Chatfield, Robert] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Cohen, Ayala] Technion Israel Inst Technol, Ind & Management Engn, Haifa, Israel. [Ridgway, William L.] Sci Syst & Applicat Inc, Lanham, MD 20771 USA. RP Broday, DM (reprint author), Technion Israel Inst Technol, Civil & Environm Engn, Haifa, Israel. EM dbroday@tx.technion.acil OI Broday, David/0000-0002-6525-3979 FU Environment and Health Fund, Israel FX M.S.H. would like to thank the Environment and Health Fund, Israel, for supporting her studies with a doctoral fellowship, and NASA AMES Research Center, CA, USA for hosting her in summer 2012. The research was done at the Technion Center of Excellence in Exposure Science and Environmental Health (TCEEH). The authors thank the reviewers for their valuable comments. NR 37 TC 9 Z9 9 U1 5 U2 38 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 JUN 15 PY 2015 VL 163 BP 180 EP 185 DI 10.1016/j.rse.2015.03.014 PG 6 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA CJ8RN UT WOS:000355771300016 ER PT J AU Schrijver, CJ Kauristie, K Aylward, AD Denardini, CM Gibson, SE Glover, A Gopalswamy, N Grande, M Hapgood, M Heynderickx, D Jakowski, N Kalegaev, VV Lapenta, G Linker, JA Liu, SP Mandrini, CH Mann, IR Nagatsuma, T Nandy, D Obara, T O'Brien, TP Onsager, T Opgenoorth, HJ Terkildsen, M Valladares, CE Vilmer, N AF Schrijver, Carolus J. Kauristie, Kirsti Aylward, Alan D. Denardini, Clezio M. Gibson, Sarah E. Glover, Alexi Gopalswamy, Nat Grande, Manuel Hapgood, Mike Heynderickx, Daniel Jakowski, Norbert Kalegaev, Vladimir V. Lapenta, Giovanni Linker, Jon A. Liu, Siqing Mandrini, Cristina H. Mann, Ian R. Nagatsuma, Tsutomu Nandy, Dibyendu Obara, Takahiro O'Brien, T. Paul Onsager, Terrance Opgenoorth, Hermann J. Terkildsen, Michael Valladares, Cesar E. Vilmer, Nicole TI Understanding space weather to shield society: A global road map for 2015-2025 commissioned by COSPAR and ILWS SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Space weather; COSPAR/ILWS road map panel ID INTERPLANETARY SCINTILLATION AB There is a growing appreciation that the environmental conditions that we call space weather impact the technological infrastructure that powers the coupled economies around the world. With that comes the need to better shield society against space weather by improving forecasts, environmental specifications, and infrastructure design. We recognize that much progress has been made and continues to be made with a powerful suite of research observatories on the ground and in space, forming the basis of a Sun Earth system observatory. But the domain of space weather is vast extending from deep within the Sun to far outside the planetary orbits and the physics complex including couplings between various types of physical processes that link scales and domains from the microscopic to large parts of the solar system. Consequently, advanced understanding of space weather requires a coordinated international approach to effectively provide awareness of the processes within the Sun Earth system through observation-driven models. This roadmap prioritizes the scientific focus areas and research infrastructure that are needed to significantly advance our understanding of space weather of all intensities and of its implications for society. Advancement of the existing system observatory through the addition of small to moderate state-of-the-art capabilities designed to fill observational gaps will enable significant advances. Such a strategy requires urgent action: key instrumentation needs to be sustained, and action needs to be taken before core capabilities are lost in the aging ensemble. We recommend advances through priority focus (1) on observation-based modeling throughout the Sun Earth system, (2) on forecasts more than 12 h ahead of the magnetic structure of incoming coronal mass ejections, (3) on understanding the geospace response to variable solar-wind stresses that lead to intense geomagnetically-induced currents and ionospheric and radiation storms, and (4) on developing a comprehensive specification of space climate, including the characterization of extreme space storms to guide resilient and robust engineering of technological infrastructures. The roadmap clusters its implementation recommendations by formulating three action pathways, and outlines needed instrumentation and research programs and infrastructure for each of these. An executive summary provides an overview of all recommendations. (C) 2015 COSPAR. Published by Elsevier Ltd. C1 [Schrijver, Carolus J.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Kauristie, Kirsti] Finnish Meteorol Inst, FI-00560 Helsinki, Finland. [Aylward, Alan D.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Denardini, Clezio M.] Inst Nacl Pesquisas Espaciais, Sao Jose Dos Campos, SP, Brazil. [Gibson, Sarah E.] HAO NCAR, Boulder, CO 80307 USA. [Glover, Alexi] RHEA Syst, D-64293 Darmstadt, Germany. [Glover, Alexi] ESA SSA Programme Off, D-64293 Darmstadt, Germany. [Gopalswamy, Nat] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Grande, Manuel] Aberystwyth Univ, Penglais STY23 3B, Scotland. [Hapgood, Mike] RAL Space, Didcot OX11 0QX, Oxon, England. [Hapgood, Mike] STFC, Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Heynderickx, Daniel] DH Consultancy BVBA, B-3000 Leuven, Belgium. [Jakowski, Norbert] German Aerosp Ctr, D-17235 Neustrelitz, Germany. [Kalegaev, Vladimir V.] Moscow MV Lomonosov State Univ, Skobeltsyn Inst Nucl Phys, Moscow 119991, Russia. [Lapenta, Giovanni] Katholieke Univ Leuven, B-3001 Leuven, Belgium. [Linker, Jon A.] Predict Sci Inc, San Diego, CA 92121 USA. [Liu, Siqing] Chinese Acad Sci, Natl Space Sci Ctr, Beijing 100190, Peoples R China. [Mandrini, Cristina H.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. [Mann, Ian R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2J1, Canada. [Nagatsuma, Tsutomu] Natl Inst Informat & Commun Technol, Space Weather & Environm Informat Lab, Tokyo 1848795, Japan. [Nandy, Dibyendu] Ctr Excellence Space Sci, Kolkata 74125, Mohanpur, India. [Nandy, Dibyendu] Indian Inst Sci Educ & Res, Kolkata 74125, Mohanpur, India. Tohoku Univ, Planetary Plasma & Atmospher Res Ctr, Aoba Ku, Sendai, Miyagi 9808578, Japan. [O'Brien, T. Paul] Aerosp Corp, Dept Space Sci, Chantilly, Chantilly, VA 20151 USA. [Onsager, Terrance] NOAA, Space Weather Predict Ctr, Boulder, CO 80305 USA. [Opgenoorth, Hermann J.] Swedish Inst Space Phys, S-75121 Uppsala, Sweden. [Terkildsen, Michael] Space Weather Serv, Bur Meteorol, Surry Hills, NSW, Australia. [Valladares, Cesar E.] Boston Coll, Inst Sci Res, Newton, MA 02459 USA. [Vilmer, Nicole] Univ Paris Diderot, CNRS, Observ Paris, LENA, F-92195 Meudon, France. RP Schrijver, CJ (reprint author), Lockheed Martin Solar & Astrophys Lab, 3251 Hanover St, Palo Alto, CA 94304 USA. EM schrijver@lmsal.com RI De Nardin, Clezio/C-4103-2012; Grande, Manuel/C-2242-2013; OI De Nardin, Clezio/0000-0002-3624-2461; Grande, Manuel/0000-0002-2233-2618; Nagatsuma, Tsutomu/0000-0002-9334-0738; Lapenta, Giovanni/0000-0002-3123-4024 NR 48 TC 22 Z9 22 U1 2 U2 16 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 JUN 15 PY 2015 VL 55 IS 12 BP 2745 EP 2807 DI 10.1016/j.asr.2015.03.023 PG 63 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA CJ3FA UT WOS:000355367600001 ER PT J AU Vaisberg, O Artemyev, A Avanov, L AF Vaisberg, O. Artemyev, A. Avanov, L. TI Nonadiabatic ion acceleration at the nightside highlatitude magnetopause: Fine structure of the velocity distribution function SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Magnetopause; Magnetic reconnection; Ion acceleration ID SHEARED MAGNETIC-FIELD; CURRENT SHEET ACCELERATION; INTERBALL TAIL PROBE; GEOMAGNETIC TAIL; EARTHS MAGNETOPAUSE; PARTICLE MOTION; RECONNECTION; MAGNETOTAIL; PLASMA; MODEL AB In this paper we use Interball-tail observations and numerical modeling to investigate ion acceleration in reconnected nightside magnetopause. We consider magnetic field configuration corresponding to the superposition of the magnetopause current sheet and reconnected fluxtube, which moves tailward. This fluxtube creates normal component of the magnetic field and the transverse electric field component. Initial current sheet geometry includes tangential and shear components of the magnetic field. Interaction of cold magnetosheath ions with the reconnected current sheet results in particle acceleration and transition through the magnetopause. Reflected and transited ions form velocity distributions with a halo in the (v(parallel to),v(perpendicular to)) plane. Numerical modeling reproduce these velocity distributions quite well. Comparison of numerical results and spacecraft observation indicates that nonadibatic ion acceleration plays essential role in formation of such velocity distributions. (C) 2015 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Vaisberg, O.] RAS, Space Res Inst, Moscow, Russia. [Artemyev, A.; Avanov, L.] Univ Maryland, NASA, Goddard Space Flight Ctr, Baltimore, MD USA. RP Vaisberg, O (reprint author), RAS, Space Res Inst, Moscow, Russia. EM olegv@iki.rssi.ru; ante0226@gmail.com NR 46 TC 0 Z9 0 U1 1 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD JUN 15 PY 2015 VL 55 IS 12 BP 2840 EP 2850 DI 10.1016/j.asr.2015.02.036 PG 11 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA CJ3FA UT WOS:000355367600005 ER PT J AU Joseph, OO Yamazak, Y Cilliers, P Baki, P Ngwira, CM Mito, C AF Joseph, Olwendo Ouko Yamazak, Yosuke Cilliers, Pierre Baki, Paul Ngwira, Chigomezyo M. Mito, Collins TI A study on the response of the Equatorial Ionization Anomaly over the East Africa sector during the geomagnetic storm of November 13, 2012 SO ADVANCES IN SPACE RESEARCH LA English DT Article DE IGS; Ionospheric ionization anomaly; East African region; Geomagnetic storm ID TOTAL ELECTRON-CONTENT; IONOSPHERIC DISTURBANCE DYNAMO; INSTRUMENTAL BIASES; REGION; TEC; SATELLITE; PERIODS; FIELDS; MODEL; JAPAN AB Using a set of up to 12 International GNSS Services (IGS) receivers around the East African region, we present the formation of the peak of ionospheric Equatorial Ionization Anomaly during the geomagnetic storm of 13th November 2012. The diurnal pattern of total electron content (TEC) shows a strong negative storm during the main phase of the storm. Latitudinal variation of TEC shows development of strong Equatorial Ionization Anomaly (EIA) on the recovery phase. Evidence in terms of magnetic variations during the storm period, indicates that the penetration of interplanetary electric fields is the main cause of the negative ionospheric effect during the main phase of the storm. Observation shows the occurrence of very strong westward electric fields arising from the IMF Bz turning southward a few hours after sunset local time. TEC enhancement during the recovery phase on the 16th are attributed to the increased ionospheric disturbance dynamo electric fields. In addition the EIA crest was found to intensify in amplitude as well as expand in latitudinal extent. (C) 2015 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Joseph, Olwendo Ouko] Pwani Univ, Sch Pure & Appl Sci, Dept Math & Phys, Kilifi, Kenya. [Yamazak, Yosuke] Univ Lancaster, Dept Phys, Lancaster, England. [Cilliers, Pierre] South African Natl Space Agcy, Space Sci Directorate, Hermanus, South Africa. [Baki, Paul] Kenya Tech Univ, Sch Pure & Appl Sci, Dept Phys, Nairobi, Kenya. [Ngwira, Chigomezyo M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Ngwira, Chigomezyo M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. [Mito, Collins] Univ Nairobi, Dept Phys, Nairobi, Kenya. RP Joseph, OO (reprint author), Pwani Univ, Sch Pure & Appl Sci, Dept Math & Phys, POB 195-80108, Kilifi, Kenya. EM castrajoseph@yahoo.com; y.yamaza-ki@lancaster.ac.uk; pjcilliers@sansa.org.za; paul.baki@gmail.com; Collins@uonbi.ac.ke NR 32 TC 5 Z9 5 U1 2 U2 6 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 JUN 15 PY 2015 VL 55 IS 12 BP 2863 EP 2872 DI 10.1016/j.asr.2015.03.011 PG 10 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA CJ3FA UT WOS:000355367600007 ER PT J AU Harpold, AA Molotch, NP Musselman, KN Bales, RC Kirchner, PB Litvak, M Brooks, PD AF Harpold, Adrian A. Molotch, Noah P. Musselman, Keith N. Bales, Roger C. Kirchner, Peter B. Litvak, Marcy Brooks, Paul D. TI Soil moisture response to snowmelt timing in mixed-conifer subalpine forests SO HYDROLOGICAL PROCESSES LA English DT Article DE snowmelt; soil moisture; snow-vegetation interactions; cross-site comparison ID SURFACE-ENERGY EXCHANGES; WESTERN UNITED-STATES; HIGH-ELEVATION; SIERRA-NEVADA; NEW-MEXICO; STREAMFLOW GENERATION; WATER RETENTION; BOREAL FOREST; ACCUMULATION; COVER AB Western US forest ecosystems and downstream water supplies are reliant on seasonal snowmelt. Complex feedbacks govern forest-snow interactions in which forests influence the distribution of snow and the timing of snowmelt but are also sensitive to snow water availability. Notwithstanding, few studies have investigated the influence of forest structure on snow distribution, snowmelt and soil moisture response. Using a multi-year record from co-located observations of snow depth and soil moisture, we evaluated the influence of forest-canopy position on snow accumulation and snow depth depletion, and associated controls on the timing of soil moisture response at Boulder Creek, Colorado, Jemez River Basin, New Mexico, and the Wolverton Basin, California. Forest-canopy controls on snow accumulation led to 12-42cm greater peak snow depths in open versus under-canopy positions. Differences in accumulation and melt across sites resulted in earlier snow disappearance in open positions at Jemez and earlier snow disappearance in under-canopy positions at Boulder and Wolverton sites. Irrespective of net snow accumulation, we found that peak annual soil moisture was nearly synchronous with the date of snow disappearance at all sites with an average deviation of 12, 3 and 22days at Jemez, Boulder and Wolverton sites, respectively. Interestingly, sites in the Sierra Nevada showed peak soil moisture prior to snow disappearance at both our intensive study site and the nearby snow telemetry stations. Our results imply that the duration of soil water stress may increase as regional warming or forest disturbance lead to earlier snow disappearance and soil moisture recession in subalpine forests. Copyright (c) 2014 John Wiley & Sons, Ltd. C1 [Harpold, Adrian A.; Molotch, Noah P.] Univ Nevada, Insitutute Arctic & Alpine Res, Boulder, CO 80304 USA. [Harpold, Adrian A.] Univ Nevada, Dept Nat Resources & Environm Sci, Reno, NV 89557 USA. [Molotch, Noah P.] CALTECH, Jet Prop Lab, Boulder, CO 80304 USA. [Molotch, Noah P.] Univ Colorado, Dept Geog, Boulder, CO 80304 USA. [Molotch, Noah P.] Univ Colorado, INSTAAR, Boulder, CO 80304 USA. [Musselman, Keith N.] Univ Calif Los Angeles, Civil & Environm Engn, Los Angeles, CA 90095 USA. [Bales, Roger C.; Kirchner, Peter B.] Univ Calif, Sierra Nevada Res Inst, Merced, CA 95343 USA. [Litvak, Marcy] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Brooks, Paul D.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. RP Harpold, AA (reprint author), Univ Nevada, Dept Nat Resources & Environm Sci, Reno, NV 89557 USA. EM aharpold@cabnr.unr.edu RI Molotch, Noah/C-8576-2009; OI Harpold, Adrian/0000-0002-2566-9574 FU NSF EAR Postdoctoral Fellowship [EAR 1144894]; Office of Science (BER) at DOE; NSF CZO [EAR 724960, EAR 725097, EAR 724958] FX The first author was supported by an NSF EAR Postdoctoral Fellowship (EAR 1144894). The Office of Science (BER) at DOE and the NSF CZO (EAR 724960, EAR 725097 and EAR 724958) also provided support for this study. NR 74 TC 8 Z9 8 U1 8 U2 39 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0885-6087 EI 1099-1085 J9 HYDROL PROCESS JI Hydrol. Process. PD JUN 15 PY 2015 VL 29 IS 12 BP 2782 EP 2798 DI 10.1002/hyp.10400 PG 17 WC Water Resources SC Water Resources GA CJ7TD UT WOS:000355701700010 ER PT J AU Lin, YN Jolivet, R Simons, M Agram, PS Martens, HR Li, Z Lodi, SH AF Lin, Y. N. Jolivet, R. Simons, M. Agram, P. S. Martens, H. R. Li, Z. Lodi, S. H. TI High interseismic coupling in the Eastern Makran (Pakistan) subduction zone SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Makran subduction zone; interseismic coupling; InSAR ID CURRENT PLATE VELOCITIES; ACCRETIONARY WEDGE; CRUSTAL DEFORMATION; GPS MEASUREMENTS; OKI EARTHQUAKE; MOTION MODEL; CHILE; FAULT; SLIP; IRAN AB Estimating the extent of interseismic coupling along subduction zone megathrusts is essential for quantitative assessments of seismic and tsunami hazards. Up to now, quantifying the seismogenic potential of the eastern Makran subduction zone at the northern edge of the Indian ocean has remained elusive due to a paucity of geodetic observations. Furthermore, non-tectonic processes obscure the signature of accumulating elastic strain. Historical earthquakes of magnitudes greater than 7 have been reported. In particular, the 1945 Mw 8.1 earthquake resulted in a significant tsunami that swept the shores of the Arabian Sea and the Indian Ocean. A quantitative estimate of elastic strain accumulation along the subduction plate boundary in eastern Makran is needed to confront previous indirect and contradictory conclusions about the seismic potential in the region. Here, we infer the distribution of interseismic coupling on the eastern Makran megathrust from time series of satellite Interferometric Synthetic Aperture Radar (InSAR) images acquired between 2003 and 2010, applying a consistent series of corrections to extract the low amplitude, long wavelength deformation signal associated with elastic strain on the megathrust We find high interseismic coupling (i.e. the megathrust does not slip and elastic strain accumulates) in the central section of eastern Makran, where the 1945 earthquake occurred, while lower coupling coincides spatially with the subduction of the Sonne Fault Zone. The inferred accumulation of elastic strain since the 1943 earthquake is consistent with the future occurrence of magnitude 7+ earthquakes and we cannot exclude the possibility of a multi-segment rupture (Mw 8+). However, the likelihood for such scenarios might be modulated by partitioning of plate convergence between slip on the megathrust and internal deformation of the overlying, actively deforming, accretionary wedge. (C) 2015 Elsevier B.V. All rights reserved. C1 [Lin, Y. N.; Jolivet, R.; Simons, M.; Martens, H. R.] CALTECH, Seismol Lab, Geol & Planetary Sci, Pasadena, CA 91125 USA. [Agram, P. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Li, Z.] Newcastle Univ, Sch Civil Engn & Geosci, COMET, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. [Lodi, S. H.] NED Univ Engn & Technol, Dept Civil Engn, Karachi 75270, Pakistan. [Jolivet, R.] Univ Cambridge, Dept Earth Sci, COMET, Bullard Labs, Cambridge CB3 0EZ, England. RP Jolivet, R (reprint author), CALTECH, Seismol Lab, Geol & Planetary Sci, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM rpj29@cam.ac.uk RI Li, Zhenhong/F-8705-2010; OI Li, Zhenhong/0000-0002-8054-7449; Jolivet, Romain/0000-0002-9896-3651; Simons, Mark/0000-0003-1412-6395 NR 73 TC 4 Z9 4 U1 2 U2 13 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 JUN 15 PY 2015 VL 420 BP 116 EP 126 DI 10.1016/j.epsl.2015.03.037 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CH6LU UT WOS:000354148900012 ER PT J AU Bhattacharjee, AK Balakrishnan, K Garcia, AL Bell, JB Donev, A AF Bhattacharjee, Amit Kumar Balakrishnan, Kaushik Garcia, Alejandro L. Bell, John B. Donev, Aleksandar TI Fluctuating hydrodynamics of multi-species reactive mixtures SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID STOCHASTIC DIFFERENTIAL-EQUATIONS; CHEMICAL LANGEVIN EQUATION; REACTION-DIFFUSION MODEL; MONTE-CARLO METHOD; MASTER-EQUATION; NONEQUILIBRIUM FLUCTUATIONS; MICROSCOPIC SIMULATION; HOMOGENEOUS SYSTEMS; PATTERN-FORMATION; COMPLEX FLUIDS AB We formulate and study computationally the fluctuating compressible Navier-Stokes equations for reactive multi-species fluid mixtures. We contrast two different expressions for the covariance of the stochastic chemical production rate in the Langevin formulation of stochastic chemistry, and compare both of them to predictions of the chemical master equation for homogeneous well-mixed systems close to and far from thermodynamic equilibrium. We develop a numerical scheme for inhomogeneous reactive flows, based on our previous methods for non-reactive mixtures [Balakrishnan, Phys. Rev. E 89, 013017 (2014)]. We study the suppression of non-equilibrium long-ranged correlations of concentration fluctuations by chemical reactions, as well as the enhancement of pattern formation by spontaneous fluctuations. Good agreement with available theory demonstrates that the formulation is robust and a useful tool in the study of fluctuations in reactive multi-species fluids. At the same time, several problems with Langevin formulations of stochastic chemistry are identified, suggesting that future work should examine combining Langevin and master equation descriptions of hydrodynamic and chemical fluctuations. (C) 2015 AIP Publishing LLC. C1 [Bhattacharjee, Amit Kumar; Donev, Aleksandar] NYU, Courant Inst Math Sci, New York, NY 10012 USA. [Balakrishnan, Kaushik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Garcia, Alejandro L.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Bell, John B.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Res Div, Berkeley, CA 94720 USA. RP Bhattacharjee, AK (reprint author), NYU, Courant Inst Math Sci, 251 Mercer St, New York, NY 10012 USA. RI Bhattacharjee, Amit/A-5596-2013 OI Bhattacharjee, Amit/0000-0002-1475-743X FU U.S. Department of Energy Office of Science, Office of Advanced Scientific Computing Research, Applied Mathematics program [DE-SC0008271, DE-AC02-05CH11231] FX We would like to thank M. Malek-Mansour, Jonathan Goodman, Eric Vanden-Eijnden, Samuel Isaacson, Hans Christian Ottinger, Dick Bedeaux, Annie Lemarchand, Florence Baras, John Pearson, Sorin Tanase Nicola, and Signe Kjelstrup for informative discussions. This material is based upon work supported by the U.S. Department of Energy Office of Science, Office of Advanced Scientific Computing Research, Applied Mathematics program under Award No. DE-SC0008271 and under Contract No. DE-AC02-05CH11231. NR 142 TC 9 Z9 9 U1 6 U2 12 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD JUN 14 PY 2015 VL 142 IS 22 AR 224107 DI 10.1063/1.4922308 PG 21 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA CK4FG UT WOS:000356176600009 PM 26071701 ER PT J AU Rozo, E Rykoff, ES Bartlett, JG Melin, JB AF Rozo, E. Rykoff, E. S. Bartlett, James G. Melin, Jean-Baptiste TI redMaPPer - III. A detailed comparison of the Planck 2013 and SDSS DR8 redMaPPer cluster catalogues SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: groups: general ID MASSIVE GALAXY CLUSTERS; ALL-SKY SURVEY; X-RAY SEARCH; SCALING RELATIONS; COSMOLOGICAL CONSTRAINTS; DATA RELEASE; MILKY-WAY; SZ; PERFORMANCE; CHANDRA AB We compare the Planck Sunyaev-Zeldovich (SZ) cluster sample (PSZ1) to the Sloan Digital Sky Survey (SDSS) redMaPPer catalogue, finding that all Planck clusters within the redMaPPer mask and within the redshift range probed by redMaPPer are contained in the redMaPPer cluster catalogue. These common clusters define a tight scaling relation in the richness-SZ mass (lambda-M-SZ) plane, with an intrinsic scatter in richness of sigma(lambda vertical bar MSZ) = 0.266 +/- 0.017. The corresponding intrinsic scatter in true cluster halo mass at fixed richness is approximate to 21 per cent. The regularity of this scaling relation is used to identify failures in both catalogues. The failure rates for redMaPPer and PSZ1 1.2 per cent and 14.7 per cent, respectively. The PSZ1 failure rates decreases to 9.8 per cent after removing incorrect redshifts that were drawn from the literature. We note the failure rates in the PSZ1 from this analysis are specific to the SDSS overlap region, and may not be indicative of failure rates over the full Planck survey. We have further identified five PSZ1 sources that suffer from projection effects (multiple rich systems along the line of sight of the SZ detection) and 17 new high-redshift (z greater than or similar to 0.6) cluster candidates of varying degrees of confidence. C1 [Rozo, E.; Rykoff, E. S.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Rozo, E.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. [Bartlett, James G.] Univ Paris Diderot, Sorbonne Paris Cite, CEA Lrfu Observat Paris, APC,CNRS IN2P3, F-75205 Paris 13, France. [Bartlett, James G.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Melin, Jean-Baptiste] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. RP Rozo, E (reprint author), SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. EM erozo@email.arizona.edu FU US Department of Energy [DE-AC02-76SF00515]; Institut Universitaire de France; National Aeronautics and Space Administration FX The authors wish to thank the anonymous referee for comments that helped improved the presentation of this work. We thank August Evrard for comments on an early draft of this manuscript. We also thank Nabila Aghanim for help with accessing the full Planck cluster catalogue and validation table. This work was supported in part by the US Department of Energy contract to SLAC no. DE-AC02-76SF00515. JGB gratefully acknowledges support from the Institut Universitaire de France. A portion 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 52 TC 15 Z9 15 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 JUN 11 PY 2015 VL 450 IS 1 BP 592 EP 605 DI 10.1093/mnras/stv605 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6BA UT WOS:000356311600043 ER PT J AU Sutton, AD Roberts, TP Gladstone, JC Walton, DJ AF Sutton, Andrew D. Roberts, Timothy P. Gladstone, Jeanette C. Walton, Dominic J. TI The hyperluminous X-ray source candidate in IC 4320: another HLX bites the dust SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; X-rays: binaries; X-rays: galaxies ID MASS BLACK-HOLE; ACTIVE GALACTIC NUCLEI; ESO 243-49 HLX-1; HOLMBERG IX X-1; GALAXY NGC 2276; XMM-NEWTON; CARTWHEEL RING; OPTICAL IDENTIFICATIONS; ULTRALUMINOUS STATE; ACCRETION FLOWS AB The known members of the class of hyperluminous X-ray sources (HLXs) are few in number, yet they are of great interest as they are regarded as the likeliest intermediate-mass black hole (IMBH) candidates amongst the wider population of ultraluminous X-ray sources (ULXs). Here we report optical photometry and spectroscopy of an HLX candidate associated with the galaxy IC 4320, that reveal it is a background AGN. We discuss the implications of the exclusion of this object from the small number of well-studied HLXs, that appears to accentuate the difference in characteristics between the good IMBH candidate ESO 243-49 HLX-1 and the small handful of other HLXs. C1 [Sutton, Andrew D.; Roberts, Timothy P.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Sutton, Andrew D.] NASA, George C Marshall Space Flight Ctr, Astrophys Off, Huntsville, AL 35812 USA. [Gladstone, Jeanette C.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Walton, Dominic J.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. RP Sutton, AD (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England. EM andrew.d.sutton@nasa.gov FU Science and Technology Facilities Council [ST/K000861/1, ST/L00075X/1]; ESO telescopes at the La Silla Paranal Observatory [090.D-0300(A), 092.D-0212(A)] FX ADS and TPR acknowledge funding from the Science and Technology Facilities Council as part of the consolidated grants ST/K000861/1 and ST/L00075X/1. This work is based on observations made with ESO telescopes at the La Silla Paranal Observatory under programme IDs 090.D-0300(A) and 092.D-0212(A). It is also based in part on observations made by the Chandra X-ray Observatory, and made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. NR 63 TC 7 Z9 7 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 11 PY 2015 VL 450 IS 1 BP 787 EP 793 DI 10.1093/mnras/stv505 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6BA UT WOS:000356311600054 ER PT J AU Aasi, J Abadie, J Abbott, BP Abbott, R Abbott, T Abernathy, MR Accadia, T Acernese, F Adams, C Adams, T Adhikari, RX Affeldt, C Agathos, M Aggarwal, N Aguiar, OD Ajith, P Allen, B Allocca, A Ceron, EA Amariutei, D Anderson, RA Anderson, SB Anderson, WG Arai, K Araya, MC Arceneaux, C Areeda, J Ast, S Aston, SM Astone, P Aufmuth, P Aulbert, C Austin, L Aylott, BE Babak, S Baker, PT Ballardin, G Ballmer, SW Barayoga, JC Barker, D Barnum, SH Barone, F Barr, B Barsotti, L Barsuglia, M Barton, MA Bartos, I Bassiri, R Basti, A Batch, J Bauchrowitz, J Bauer, TS Bebronne, M Behnke, B Bejger, M Beker, MG Bell, AS Bell, C Belopolski, I Bergmann, G Berliner, JM Bertolini, A Bessis, D Betzwieser, J Beyersdorf, PT Bhadbhade, T Bilenko, IA Billingsley, G Birch, J Bitossi, M Bizouard, MA Black, E Blackburn, JK Blackburn, L Blair, D Blom, M Bock, O Bodiya, TP Boer, M Bogan, C Bond, C Bondu, F Bonelli, L Bonnand, R Bork, R Born, M Bose, S Bosi, L Bowers, J Bradaschia, C Brady, PR Braginsky, VB Branchesi, M Brannen, CA Brau, JE Breyer, J Briant, T Bridges, DO Brillet, A Brinkmann, M Brisson, V Britzger, M Brooks, AF Brown, DA Brown, DD Bruckner, F Bulik, T Bulten, HJ Buonanno, A Buskulic, D Buy, C Byer, RL Cadonati, L Cagnoli, G Bustillo, JC Calloni, E Camp, JB Campsie, P Cannon, KC Canuel, B Cao, J Capano, CD Carbognani, F Carbone, L Caride, S Castiglia, A Caudill, S Cavaglia, M Cavalier, F Cavalieri, R Cella, G Cepeda, C Cesarini, E Chakraborty, R Chalermsongsak, T Chao, S Charlton, P Chassande-Mottin, E Chen, X Chen, Y Chincarini, A Chiummo, A Cho, HS Chow, J Christensen, N Chu, Q Chua, SSY Chung, S Ciani, G Clara, F Clark, DE Clark, JA Cleva, F Coccia, E Cohadon, PF Colla, A Colombini, M Constancio, M Conte, A Conte, R Cook, D Corbitt, TR Cordier, M Cornish, N Corsi, A Costa, CA Coughlin, MW Coulon, JP Countryman, S Couvares, P Coward, DM Cowart, M Coyne, DC Craig, K Creighton, JDE Creighton, TD Crowder, SG Cumming, A Cunningham, L Cuoco, E Dahl, K Dal Canton, T Damjanic, M Danilishin, SL D'Antonio, S Danzmann, K Dattilo, V Daudert, B Daveloza, H Davier, M Davies, GS Daw, EJ Day, R Dayanga, T Debreczeni, G Degallaix, J Deleeuw, E Deleglise, S Del Pozzo, W Denker, T Dent, T Dereli, H Dergachev, V De Rosa, R DeRosa, RT DeSalvo, R Dhurandhar, S Di az, M Dietz, A Di Fiore, L Di Lieto, A Di Palma, I Di Virgilio, A Dmitry, K Donovan, F Dooley, KL Doravari, S Drago, M Drever, RWP Driggers, JC Du, Z Dumas, JC Dwyer, S Eberle, T Edwards, M Effler, A Ehrens, P Eichholz, J Eikenberry, SS Endroczi, G Essick, R Etzel, T Evans, K Evans, M Evans, T Factourovich, M Fafone, V Fairhurst, S Fang, Q Farr, B Farr, W Favata, M Fazi, D Fehrmann, H Feldbaum, D Ferrante, I Ferrini, F Fidecaro, F Finn, LS Fiori, I Fisher, R Flaminio, R Foley, E Foley, S Forsi, E Forte, LA Fotopoulos, N Fournier, JD Franco, S Frasca, S Frasconi, F Frede, M Frei, M Frei, Z Freise, A Frey, R Fricke, TT Fritschel, P Frolov, VV Fujimoto, MK Fulda, P Fyffe, M Gair, J Gammaitoni, L Garcia, J Garufi, F Gehrels, N Gemme, G Genin, E Gennai, A Gergely, L Ghosh, S Giaime, JA Giampanis, S Giardina, KD Giazotto, A Gil-Casanova, S Gill, C Gleason, J Goetz, E Goetz, R Gondan, L Gonzalez, G Gordon, N Gorodetsky, ML Gossan, S Gossler, S Gouaty, R Graef, C Graff, PB Granata, M Grant, A Gras, S Gray, C Greenhalgh, RJS Gretarsson, AM Griffo, C Grote, H Grover, K Grunewald, S Guidi, GM Guido, C Gushwa, KE Gustafson, EK Gustafson, R Hall, B Hall, E Hammer, D Hammond, G Hanke, M Hanks, J Hanna, C Hanson, J Harms, J Harry, GM Harry, IW Harstad, ED Hartman, MT Haughian, K Hayama, K Heefner, J Heidmann, A Heintze, M Heitmann, H Hello, P Hemming, G Hendry, M Heng, IS Heptonstall, AW Heurs, M Hild, S Hoak, D Hodge, KA Holt, K Hong, T Hooper, S Horrom, T Hosken, DJ Hough, J Howell, EJ Hu, Y Hua, Z Huang, V Huerta, EA Hughey, B Husa, S 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B Lewis, JB Lhuillier, V Li, TGF Lin, AC Littenberg, TB Litvine, V Liu, F Liu, H Liu, Y Liu, Z Lloyd, D Lockerbie, NA Lockett, V Lodhia, D Loew, K Logue, J Lombardi, AL Lorenzini, M Loriette, V Lormand, M Losurdo, G Lough, J Luan, J Lubinski, MJ Luck, H Lundgren, AP Macarthur, J Macdonald, E Machenschalk, B MacInnis, M Macleod, DM Magana-Sandoval, F Mageswaran, M Mailand, K Majorana, E Maksimovic, I Malvezzi, V Man, N Manca, GM Mandel, I Mandic, V Mangano, V Mantovani, M Marchesoni, F Marion, F Marka, S Marka, Z Markosyan, A Maros, E Marque, J Martelli, F Martellini, L Martin, IW Martin, RM Martynov, D Marx, JN Mason, K Masserot, A Massinger, TJ Matichard, F Matone, L Matzner, RA Mavalvala, N May, G Mazumder, N Mazzolo, G McCarthy, R McClelland, DE McGuire, SC McIntyre, G McIver, J Meacher, D Meadors, GD Mehmet, M Meidam, J Meier, T Melatos, A Mendell, G Mercer, RA Meshkov, S Messenger, C Meyer, MS Miao, H Michel, C Mikhailov, EE Milano, L Miller, J Minenkov, Y Mingarelli, CMF Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Moe, B Mohan, M Mohapatra, SRP Mokler, F Moraru, D Moreno, G Morgado, N Mori, T Morriss, SR Mossavi, K Mours, B Mow-Lowry, CM Mueller, CL Mueller, G Mukherjee, S Mullavey, A Munch, J Murphy, D Murray, PG Mytidis, A Nagy, MF Nardecchia, I Nash, T Naticchioni, L Nayak, R Necula, V Neri, I Newton, G Nguyen, T Nishida, E Nishizawa, A Nitz, A Nocera, F Nolting, D Normandin, ME Nuttall, LK Ochsner, E O'Dell, J Oelker, E Ogin, GH Oh, JJ Oh, SH Ohme, F Oppermann, P O'Reilly, B Larcher, WO O'Shaughnessy, R Osthelder, C Ott, CD Ottaway, DJ Ottens, RS Ou, J Overmier, H Owen, BJ Padilla, C Pai, A Palomba, C Pan, Y Pankow, C Paoletti, F Paoletti, R Papa, MA Paris, H Pasqualetti, A Passaquieti, R Passuello, D Pedraza, M Peiris, P Penn, S Perreca, A Phelps, M Pichot, M Pickenpack, M Piergiovanni, F Pierro, V Pinard, L Pindor, B Pinto, IM Pitkin, M Poeld, J Poggiani, R Poole, V Poux, C Predoi, V Prestegard, T Price, LR Prijatelj, M Principe, M Privitera, S 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TI Characterization of the LIGO detectors during their sixth science run SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article DE LIGO; gravitational waves; detector characterization ID GRAVITATIONAL-WAVE DETECTOR; THERMAL NOISE; INTERFEROMETER; READOUT; LASER AB In 2009-2010, the Laser Interferometer Gravitational-Wave Observatory (LIGO) operated together with international partners Virgo and GEO600 as a network to search for gravitational waves (GWs) of astrophysical origin. The sensitivity of these detectors was limited by a combination of noise sources inherent to the instrumental design and its environment, often localized in time or frequency, that couple into the GW readout. Here we review the performance of the LIGO instruments during this epoch, the work done to characterize the detectors and their data, and the effect that transient and continuous noise artefacts have on the sensitivity of LIGO to a variety of astrophysical sources. C1 [Aasi, J.; Abadie, J.; Abbott, B. 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D.; Taylor, R.; Thirugnanasambandam, M. P.; Thrane, E.; Torrie, C. I.; Vass, S.; Wallace, L.; Weinstein, A. J.; Whitcomb, S. E.; Williams, R.; Yamamoto, H.; Yeaton-Massey, D.; Zhang, F.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Abbott, T.; Bowers, J.; Corbitt, T. R.; DeRosa, R. T.; Effler, A.; Giaime, J. A.; Gonzalez, G.; Iafrate, J.; Johnson, W. W.; Kokeyama, K.; Kudla, S.; May, G.; Mullavey, A.; Walker, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA. [Accadia, T.; Bebronne, M.; Gouaty, R.; Letendre, N.; Marion, F.; Masserot, A.; Mours, B.; Rolland, L.; Verkindt, D.; Yvert, M.] Univ Savoie, CNRS IN2P3, Lab Annecy le Vieux Phys Particules LAPP, F-74941 Annecy Le Vieux, France. [Acernese, F.; Barone, F.; Calloni, E.; De Rosa, R.; Di Fiore, L.; Forte, L. A.; Garufi, F.; Milano, L.; Romano, R.] Complesso Univ Monte S Angelo, Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy. [Acernese, F.; Barone, F.; Romano, R.] Univ Salerno, I-84084 Salerno, Italy. 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RI Vecchio, Alberto/F-8310-2015; Ferrante, Isidoro/F-1017-2012; McClelland, David/E-6765-2010; Losurdo, Giovanni/K-1241-2014; Travasso, Flavio/J-9595-2016; Bartos, Imre/A-2592-2017; Punturo, Michele/I-3995-2012; Cella, Giancarlo/A-9946-2012; Cesarini, Elisabetta/C-4507-2017; Costa, Cesar/G-7588-2012; Chow, Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Ciani, Giacomo/G-1036-2011; Miao, Haixing/O-1300-2013; Howell, Eric/H-5072-2014; M, Manjunath/N-4000-2014; Gammaitoni, Luca/B-5375-2009; Gorodetsky, Michael/C-5938-2008; Prokhorov, Leonid/I-2953-2012; Heidmann, Antoine/G-4295-2016; Ott, Christian/G-2651-2011; Marchesoni, Fabio/A-1920-2008; Zhu, Xingjiang/E-1501-2016; Frasconi, Franco/K-1068-2016; Kumar, Prem/B-6691-2009; Pinto, Innocenzo/L-3520-2016; Deleglise, Samuel/B-1599-2015; Neri, Igor/F-1482-2010; Aggarwal, Nancy/M-7203-2015; Steinlechner, Sebastian/D-5781-2013; Chen, Yanbei/A-2604-2013; Shaddock, Daniel/A-7534-2011; Strigin, Sergey/I-8337-2012; Vicere, Andrea/J-1742-2012; Rocchi, Alessio/O-9499-2015; Martelli, Filippo/P-4041-2015; Branchesi, Marica/P-2296-2015; Gehring, Tobias/A-8596-2016; Strain, Kenneth/D-5236-2011; Graef, Christian/J-3167-2015; Hild, Stefan/A-3864-2010; Bell, Angus/E-7312-2011; Iyer, Bala R./E-2894-2012; Gemme, Gianluca/C-7233-2008; Ottaway, David/J-5908-2015; Leonardi, Matteo/G-9694-2015; prodi, giovanni/B-4398-2010; Danilishin, Stefan/K-7262-2012; Sigg, Daniel/I-4308-2015; Puppo, Paola/J-4250-2012; Tacca, Matteo/J-1599-2015; Garufi, Fabio/K-3263-2015; Di Virgilio, Angela Dora Vittoria/E-9078-2015; Sergeev, Alexander/F-3027-2017; Harms, Jan/J-4359-2012; Ward, Robert/I-8032-2014; OI Vecchio, Alberto/0000-0002-6254-1617; Ferrante, Isidoro/0000-0002-0083-7228; McClelland, David/0000-0001-6210-5842; Losurdo, Giovanni/0000-0003-0452-746X; Travasso, Flavio/0000-0002-4653-6156; Punturo, Michele/0000-0001-8722-4485; Cella, Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167; Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Ciani, Giacomo/0000-0003-4258-9338; Miao, Haixing/0000-0003-4101-9958; Howell, Eric/0000-0001-7891-2817; M, Manjunath/0000-0001-8710-0730; Gammaitoni, Luca/0000-0002-4972-7062; Gorodetsky, Michael/0000-0002-5159-2742; Heidmann, Antoine/0000-0002-0784-5175; Ott, Christian/0000-0003-4993-2055; Marchesoni, Fabio/0000-0001-9240-6793; Zhu, Xingjiang/0000-0001-7049-6468; Frasconi, Franco/0000-0003-4204-6587; Deleglise, Samuel/0000-0002-8680-5170; Neri, Igor/0000-0002-9047-9822; Steinlechner, Sebastian/0000-0003-4710-8548; Shaddock, Daniel/0000-0002-6885-3494; Vicere, Andrea/0000-0003-0624-6231; Rocchi, Alessio/0000-0002-1382-9016; Martelli, Filippo/0000-0003-3761-8616; Gehring, Tobias/0000-0002-4311-2593; Strain, Kenneth/0000-0002-2066-5355; Graef, Christian/0000-0002-4535-2603; Bell, Angus/0000-0003-1523-0821; Iyer, Bala R./0000-0002-4141-5179; Gemme, Gianluca/0000-0002-1127-7406; prodi, giovanni/0000-0001-5256-915X; Danilishin, Stefan/0000-0001-7758-7493; Sigg, Daniel/0000-0003-4606-6526; Puppo, Paola/0000-0003-4677-5015; Tacca, Matteo/0000-0003-1353-0441; Garufi, Fabio/0000-0003-1391-6168; Murphy, David/0000-0002-8538-815X; Pitkin, Matthew/0000-0003-4548-526X; Veitch, John/0000-0002-6508-0713; Davies, Gareth/0000-0002-4289-3439; Principe, Maria/0000-0002-6327-0628; Del Pozzo, Walter/0000-0003-3978-2030; Allen, Bruce/0000-0003-4285-6256; Granata, Massimo/0000-0003-3275-1186; Kanner, Jonah/0000-0001-8115-0577; Freise, Andreas/0000-0001-6586-9901; Nitz, Alexander/0000-0002-1850-4587; Mandel, Ilya/0000-0002-6134-8946; Whiting, Bernard F/0000-0002-8501-8669; Denker, Timo/0000-0003-1259-5315; Naticchioni, Luca/0000-0003-2918-0730; calloni, enrico/0000-0003-4819-3297; Scott, Jamie/0000-0001-6701-6515; Sorazu, Borja/0000-0002-6178-3198; Bondu, Francois/0000-0001-6487-5197; Zweizig, John/0000-0002-1521-3397; Husa, Sascha/0000-0002-0445-1971; Papa, M.Alessandra/0000-0002-1007-5298; Vocca, Helios/0000-0002-1200-3917; Aulbert, Carsten/0000-0002-1481-8319; Pinto, Innocenzo M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200; Guidi, Gianluca/0000-0002-3061-9870; Drago, Marco/0000-0002-3738-2431; Pierro, Vincenzo/0000-0002-6020-5521; Coccia, Eugenio/0000-0002-6669-5787; Vetrano, Flavio/0000-0002-7523-4296; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Swinkels, Bas/0000-0002-3066-3601; Ward, Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447; O'Shaughnessy, Richard/0000-0001-5832-8517; Vedovato, Gabriele/0000-0001-7226-1320; Matichard, Fabrice/0000-0001-8982-8418 FU United States National Science Foundation for the construction and operation of the LIGO Laboratory; Science and Technology Facilities Council of the United Kingdom; Max-Planck-Society; State of Niedersachsen/Germany; Italian Istituto Nazionale di Fisica Nucleare; French Centre National de la Recherche Scientifique; Australian Research Council; International Science Linkages program of the Commonwealth of Australia; Council of Scientific and Industrial Research of India; Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de Economia y Competitividad; Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears; Foundation for Fundamental Research on Matter by the Netherlands Organization for Scientific Research; Polish Ministry of Science and Higher Education; FOCUS Programme of Foundation for Polish Science; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; National Aeronautics and Space Administration; National Research Foundation of Korea; Industry Canada; Province of Ontario through the Ministry of Economic Development and Innovation; National Science and Engineering Research Council Canada; Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation; Alfred P Sloan Foundation FX The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector, and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Economia y Competitividad, the Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organization for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the National Science and Engineering Research Council Canada, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P Sloan Foundation. NR 60 TC 59 Z9 59 U1 13 U2 87 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 JUN 11 PY 2015 VL 32 IS 11 AR 115012 DI 10.1088/0264-9381/32/11/115012 PG 30 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA CJ1IX UT WOS:000355238400013 ER PT J AU Ghisellini, G Tagliaferri, G Sbarrato, T Gehrels, N AF Ghisellini, G. Tagliaferri, G. Sbarrato, T. Gehrels, N. TI SDSS J013127.34-032100.1: a candidate blazar with an 11 billion solar mass black hole at z=5.18 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE quasars: general; X-rays: general ID ACTIVE GALACTIC NUCLEI; RADIO-LOUD QUASARS; X-RAY; FERMI BLAZARS; DATA RELEASE; LINE REGION; SKY SURVEY; SWIFT; TELESCOPE; EMISSION AB The radio-loud quasar SDSS J013127.34-032100.1 at a redshift z = 5.18 is one of the most distant radio-loud objects. The radio to optical flux ratio (i.e. the radio-loudness) of the source is large, making it a promising blazar candidate. Its overall spectral energy distribution, completed by the X-ray flux and spectral slope derived through Target of Opportunity Swift/X-ray Telescope observations, is interpreted by a non-thermal jet plus an accretion disc and molecular torus model. We estimate that its black hole mass is (1.1 +/- A 0.2) x 10(10) M-aS (TM) for an accretion efficiency eta = 0.08, scaling roughly linearly with eta. Although there is a factor a parts per thousand(3)2 of systematic uncertainty, this black hole mass is the largest found at these redshifts. We derive a viewing angle between 3 and 5 deg. This implies that there must be other (hundreds) sources with the same black hole mass of SDSS J013127.34-032100.1, but whose jets are pointing away from Earth. We discuss the problems posed by the existence of such large black hole masses at such redshifts, especially in jetted quasars. In fact, if they are associated with rapidly spinning black holes, the accretion efficiency is high, implying a slower pace of black hole growth with respect to radio-quiet quasars. C1 [Ghisellini, G.; Tagliaferri, G.] Osserv Astron Brera, INAF, I-23807 Merate, Italy. [Sbarrato, T.] Univ Milano Bicocca, Dip Fis G Occhialini, I-20126 Milan, Italy. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Ghisellini, G (reprint author), Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, Italy. EM gabriele.ghisellini@brera.inaf.it OI Ghisellini, Gabriele/0000-0002-0037-1974; Sbarrato, Tullia/0000-0002-3069-9399 FU NASA; National Science Foundation FX This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/Caltech, funded by NASA. It also 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/Caltech, funded by NASA and the National Science Foundation. Part of this work is based on archival data and online service provided by the ASI Science Data Center (ASDC). NR 41 TC 3 Z9 3 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 11 PY 2015 VL 450 IS 1 BP L34 EP L38 DI 10.1093/mnrasl/slv042 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2WS UT WOS:000355346000008 ER PT J AU Ackermann, M Ajello, M Allafort, A Antolini, E Atwood, WB Axelsson, M Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Berenji, B Blandford, RD Bloom, ED Bonamente, E Borgland, AW Bottacini, E Bouvier, A Bregeon, J Brigida, M Bruel, P Buehler, R Burnett, TH Buson, S Caliandro, GA Cameron, RA Caraveo, PA Casandjian, JM Cavazzuti, E Cecchi, C Charles, E Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Costamante, L Cutini, S De Angelis, A De Palma, F Dermer, CD Digel, SW Silva, EDCE Drell, PS Dubois, R Escande, L Favuzzi, C Fegan, SJ Ferrara, EC Finke, J Focke, WB Fortin, P Frailis, M Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giebels, B Giglietto, N Giommi, P Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grove, JE Guiriec, S Gustafsson, M Hadasch, D Hayashida, M Hays, E Healey, SE Horan, D Hou, X Hughes, RE Iafrate, G Johannesson, G Johnson, AS Johnson, WN Kamae, T Katagiri, H Kataoka, J Knodlseder, J Kuss, M Lande, J Larsson, S Latronico, L Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Madejski, GM Mazziotta, MN McConville, W McEnery, JE Michelson, PF Mitthumsiri, W Mizuno, T Moiseev, AA Monte, C Monzani, ME Moretti, E Morselli, A Moskalenko, IV Murgia, S Nakamori, T Naumann-Godo, M Nolan, PL Norris, P Nuss, E Ohno, M Ohsugi, T Okumura, A Omodei, N Orienti, M Orlando, E Ormes, JF Ozaki, M Paneque, D Parent, D Pesce-Rollins, M Pierbattista, M Piranomonte, S Piron, F Pivato, G Porter, TA Raino, S Rando, R Razzano, M Razzaque, S Reimer, A Reimer, O Ritz, S Rochester, LS Romani, RW Roth, M Sanchez, DA Sbarra, C Scargle, JD Schalk, TL Sgro, C Shaw, MS Siskind, EJ Spandre, G Spinelli, P Strong, AW Suson, DJ Tajima, H Takahashi, H Takahashi, T Tanaka, T Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tinivella, M Torres, DF Tosti, G Troja, E Uchiyama, Y Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Waite, AP Wallace, E Wang, P Winer, BL Wood, DL Wood, KS Zimmer, S AF Ackermann, M. Ajello, M. Allafort, A. Antolini, E. Atwood, W. B. Axelsson, M. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Berenji, B. Blandford, R. D. Bloom, E. D. Bonamente, E. Borgland, A. W. Bottacini, E. Bouvier, A. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Burnett, T. H. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Casandjian, J. M. Cavazzuti, E. Cecchi, C. Charles, E. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Costamante, L. Cutini, S. De Angelis, A. De Palma, F. Dermer, C. D. Digel, S. W. Silva, E. Do Couto E. Drell, P. S. Dubois, R. Escande, L. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Finke, J. Focke, W. B. Fortin, P. Frailis, M. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giebels, B. Giglietto, N. Giommi, P. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guiriec, S. Gustafsson, M. Hadasch, D. Hayashida, M. Hays, E. Healey, S. E. Horan, D. Hou, X. Hughes, R. E. Iafrate, G. Johannesson, G. Johnson, A. S. Johnson, W. N. Kamae, T. Katagiri, H. Kataoka, J. Knodlseder, J. Kuss, M. Lande, J. Larsson, S. Latronico, L. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Madejski, G. M. Mazziotta, M. N. McConville, W. McEnery, J. E. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Moretti, E. Morselli, A. Moskalenko, I. V. Murgia, S. Nakamori, T. Naumann-Godo, M. Nolan, P. L. Norris, P. Nuss, E. Ohno, M. Ohsugi, T. Okumura, A. Omodei, N. Orienti, M. Orlando, E. Ormes, J. F. Ozaki, M. Paneque, D. Parent, D. Pesce-Rollins, M. Pierbattista, M. Piranomonte, S. Piron, F. Pivato, G. Porter, T. A. Raino, S. Rando, R. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Ritz, S. Rochester, L. S. Romani, R. W. Roth, M. Sanchez, D. A. Sbarra, C. Scargle, J. D. Schalk, T. L. Sgro, C. Shaw, M. S. Siskind, E. J. Spandre, G. Spinelli, P. Strong, A. W. Suson, D. J. Tajima, H. Takahashi, H. Takahashi, T. Tanaka, T. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tinivella, M. Torres, D. F. Tosti, G. Troja, E. Uchiyama, Y. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Waite, A. P. Wallace, E. Wang, P. Winer, B. L. Wood, D. L. Wood, K. S. Zimmer, S. TI SECOND CATALOG OF ACTIVE GALACTIC NUCLEI DETECTED BY THE FERMI LARGE AREA TELESCOPE (vol 743, 171, 2011) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Ackermann, M.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; Silva, E. Do Couto E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Healey, S. E.; Johnson, A. S.; Kamae, T.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Shaw, M. S.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Ackermann, M.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; Silva, E. Do Couto E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Healey, S. E.; Johnson, A. S.; Kamae, T.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Shaw, M. S.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. 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[Brigida, M.; De Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ & Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; De Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Fortin, P.; Giebels, B.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Burnett, T. H.; Roth, M.; Wallace, E.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Caliandro, G. A.; Hadasch, D.; Torres, D. F.] CSIC, Inst Ciencies Espai IEEE, Barcelona 08193, Spain. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Cavazzuti, E.; Cutini, S.; Gasparrini, D.; Giommi, P.] ASI Sci Data Ctr, I-00044 Rome, Italy. [Cheung, C. C.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Ciprini, S.] ASI Sci Data Ctr, I-00044 Rome, Italy. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Universe & Particules Montpellier, Montpellier, France. [Conrad, J.; Larsson, S.; Zimmer, S.] Stockholm Univ, AlbaNova, Dept Phys, S-10691 Stockholm, Sweden. [De Angelis, A.; Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [De Angelis, A.; Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Dermer, C. D.; Finke, J.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Escande, L.; Lott, B.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Ferrara, E. C.; Gehrels, N.; Hays, E.; McConville, W.; McEnery, J. E.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Frailis, M.; Iafrate, G.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Fukazawa, Y.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Hou, X.] Univ Bordeaux 1, IN2P3, CNRS, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Hughes, R. E.; Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Katagiri, H.] Ibaraki Univ, Coll Sci, Bunkyo Ku, Mito, Ibaraki 3108512, Japan. [Kataoka, J.; Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Knodlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France. [Knodlseder, J.] Univ Toulouse, GAHEC, IRAP, UPS OMP, Toulouse, France. [McConville, W.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McConville, W.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Moiseev, A. A.] CRESST, Greenbelt, MD 20771 USA. [Moiseev, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Norris, P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA. [Ohno, M.; Okumura, A.; Ozaki, M.; Takahashi, T.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [Orlando, E.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Parent, D.; Razzaque, S.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Piranomonte, S.] Osserv Astron Roma, I-00040 Rome, 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. [Sanchez, D. A.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Torres, D. F.] ICREA, Barcelona, Spain. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Wood, D. L.] Praxis Inc, Alexandria, VA 22303 USA. RP Ackermann, M (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. EM elisabetta.cavazzuti@asdc.asi.it; sarac@slac.stanford.edu; charles.dermer@nrl.navy.mil; lott@cenbg.in2p3.fr; gasparrini@asdc.asi.it RI Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Reimer, Olaf/A-3117-2013; Funk, Stefan/B-7629-2015; Johannesson, Gudlaugur/O-8741-2015 OI Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; Torres, Diego/0000-0002-1522-9065; Reimer, Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080; Johannesson, Gudlaugur/0000-0003-1458-7036 NR 1 TC 1 Z9 1 U1 1 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 144 DI 10.1088/0004-637X/806/1/144 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300144 ER PT J AU Arai, T Matsuura, S Bock, J Cooray, A Kim, MG Lanz, A Lee, DH Lee, HM Sano, K Smidt, J Matsumoto, T Nakagawa, T Onishi, Y Korngut, P Shirahata, M Tsumura, K Zemcov, M AF Arai, T. Matsuura, S. Bock, J. Cooray, A. Kim, M. G. Lanz, A. Lee, D. H. Lee, H. M. Sano, K. Smidt, J. Matsumoto, T. Nakagawa, T. Onishi, Y. Korngut, P. Shirahata, M. Tsumura, K. Zemcov, M. TI MEASUREMENTS OF THE MEAN DIFFUSE GALACTIC LIGHT SPECTRUM IN THE 0.95-1.65 mu m BAND FROM CIBER SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: general; scattering ID INFRARED-BACKGROUND-EXPERIMENT; LOW-RESOLUTION SPECTRUM; 100 MICRON CIRRUS; ZODIACAL LIGHT; MILKY-WAY; INTERSTELLAR GRAINS; SIZE DISTRIBUTION; RED CAMERA; DUST CLOUD; H-I AB We report measurements of the diffuse galactic light (DGL) spectrum in the near-infrared, spanning the wavelength range 0.95-1.65 mu m by the Cosmic Infrared Background ExpeRiment. Using the low-resolution spectrometer calibrated for absolute spectro-photometry, we acquired long-slit spectral images of the total diffuse sky brightness toward six high-latitude fields spread over four sounding rocket flights. To separate the DGL spectrum from the total sky brightness, we correlated the spectral images with a 100 mu m intensity map, which traces the dust column density in optically thin regions. The measured DGL spectrum shows no resolved features and is consistent with other DGL measurements in the optical and at near-infrared wavelengths longer than 1.8 mu m. Our result implies that the continuum is consistently reproduced by models of scattered starlight in the Rayleigh scattering regime with a few large grains. C1 [Arai, T.; Matsuura, S.; Sano, K.; Matsumoto, T.; Nakagawa, T.; Onishi, Y.] Japan Aerosp Explorat Agcy JAXA, Inst Space & Astronaut Sci, Dept Space Astron & Astrophys, Sagamihara, Kanagawa 2525210, Japan. [Arai, T.; Tsumura, K.] Tohoku Univ, Frontier Res Inst Interdisciplinary Sci, Sendai, Miyagi 9808578, Japan. [Bock, J.; Lanz, A.; Korngut, P.; Zemcov, M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Bock, J.; Korngut, P.; Zemcov, M.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Cooray, A.; Smidt, J.] Univ Calif Irvine, Ctr Cosmol, Irvine, CA 92697 USA. [Kim, M. G.; Lee, H. M.] Seoul Natl Univ, Dept Phys & Astron, Seoul 151742, South Korea. [Lee, D. H.] Korea Astron & Space Sci Inst KASI, Taejon 305348, South Korea. [Matsumoto, T.] Natl Taiwan Univ, Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Shirahata, M.] Natl Astron Observ Japan, Natl Inst Nat Sci, Tokyo 1818588, Japan. [Smidt, J.] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA. [Matsuura, S.] Kwansei Gakuin Univ, Dept Phys, Kobe, Hyogo 6691337, Japan. RP Arai, T (reprint author), Japan Aerosp Explorat Agcy JAXA, Inst Space & Astronaut Sci, Dept Space Astron & Astrophys, Sagamihara, Kanagawa 2525210, Japan. RI Matsuura, Shuji/B-5658-2016 OI Matsuura, Shuji/0000-0002-5698-9634 FU NASA APRA research grants [NNX07AI54G, NNG05WC18G, NNX07AG43G, NNX07AJ24G, NNX10AE12G]; Jet Propulsion Laboratory's Director's Research and Development Fund; KAKENHI from the Japan Society for the Promotion of Science (JSPS) [2034, 18204018, 19540250, 21340047, 21111004, 26800112]; Ministry of Education, Culture, Sports, Science, and Technology (MEXT); Pioneer Project from the Korea Astronomy and Space Science Institute (KASI); NASA Postdoctoral Fellowship; NSF CAREER award [AST-0645427]; JSPS Research Fellowship; NSF [AST-1313319]; [2012R1A4A1028713] FX This work was supported by NASA APRA research grants NNX07AI54G, NNG05WC18G, NNX07AG43G, NNX07AJ24G, and NNX10AE12G. Initial support was provided by an award to J.B. from the Jet Propulsion Laboratory's Director's Research and Development Fund. CIBER was supported by KAKENHI (2034, 18204018, 19540250, 21340047, 21111004, and 26800112) from the Japan Society for the Promotion of Science (JSPS), and the Ministry of Education, Culture, Sports, Science, and Technology (MEXT). Korean participation in CIBER was supported by the Pioneer Project from the Korea Astronomy and Space Science Institute (KASI). We would like to acknowledge the dedicated efforts of the sounding rocket staff at the NASA Wallops Flight Facility and the White Sands Missile Range. P.K. and M.Z. acknowledge support from a NASA Postdoctoral Fellowship, A.C. acknowledges support from an NSF CAREER award, and T.A. acknowledges support from the JSPS Research Fellowship for Young Scientists. A.C. acknowledges support from an NSF CAREER award AST-0645427 and NSF AST-1313319. H.M.L acknowledges support from grant 2012R1A4A1028713. We thank T.D. Brandt for kindly providing data and models. NR 48 TC 8 Z9 8 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 69 DI 10.1088/0004-637X/806/1/69 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300069 ER PT J AU Boersma, C Bregman, J Allamandola, LJ AF Boersma, C. Bregman, J. Allamandola, L. J. TI PROPERTIES OF POLYCYCLIC AROMATIC HYDROCARBONS IN THE NORTHWEST PHOTON DOMINATED REGION OF NGC 7023. III. QUANTIFYING THE TRADITIONAL PROXY FOR PAH CHARGE AND ASSESSING ITS ROLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; infrared: ISM; ISM: individual objects (NGC 7023); techniques: spectroscopic ID INFRARED-EMISSION BANDS; SPITZER-SPACE-TELESCOPE; BLIND SIGNAL SEPARATION; HERBIG AE/BE STARS; SPECTROSCOPIC DATABASE; FEATURES; EXCITATION; NGC-7023; GALAXIES; SPECTRUM AB Polycyclic aromatic hydrocarbon (PAH) emission in the Spitzer/IRS spectral map of the northwest photon dominated region (PDR) in NGC 7023 is analyzed. Here, results from fitting the 5.2-14.5 mu m spectrum at each pixel using exclusively PAH spectra from the NASA Ames PAH IR Spectroscopic Database (www.astrochem.org/pahdb/) and observed PAH band strength ratios, determined after isolating the PAH bands, are combined. This enables the first quantitative and spectrally consistent calibration of PAH charge proxies. Calibration is straightforward because the 6.2/11.2 mu m PAH band strength ratio varies linearly with the ionized fraction (PAH ionization parameter) as determined from the intrinsic properties of the individual PAHs comprising the database. This, in turn, can be related to the local radiation field, electron density, and temperature. From these relations diagnostic templates are developed to deduce the PAH ionization fraction and astronomical environment in other objects. The commonly used 7.7/11.2 mu m PAH band strength ratio fails as a charge proxy over a significant fraction of the nebula. The 11.2/12.7 mu m PAH band strength ratio, commonly used as a PAH erosion indicator, is revealed to be a better tracer for PAH charge across NGC 7023. Attempting to calibrate the 12.7/11.2 mu m PAH band strength ratio against the PAH hydrogen adjacency ratio (duo+trio)/solo is, unexpectedly, anti-correlated. This work both validates and extends the results from Paper I and Paper II. C1 [Boersma, C.; Bregman, J.; Allamandola, L. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Boersma, C (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA. EM Christiaan.Boersma@nasa.gov FU NASA [1407]; NASA's Laboratory Astrophysics, Carbon in the Galaxy/ consortium grant [NNH10ZDA001N]; NASA's Astrobiology; Astronomy + Physics Research and Analysis (APRA) [NNX07AH02G]; Spitzer Space Telescope Support Programs [50082] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. Support from NASA's Laboratory Astrophysics, Carbon in the Galaxy/ consortium grant (NNH10ZDA001N); and NASA's Astrobiology; Astronomy + Physics Research and Analysis (APRA; NNX07AH02G), and Spitzer Space Telescope Support Programs (50082) are greatly acknowledged. C.B. is grateful for an appointment at NASA Ames Research Center through the San Jose State University Research Foundation (NNX14AG80A). NR 37 TC 10 Z9 10 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 121 DI 10.1088/0004-637X/806/1/121 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300121 ER PT J AU Bowler, BP Shkolnik, EL Liu, MC Schlieder, JE Mann, AW Dupuy, TJ Hinkley, S Crepp, JR Johnson, JA Howard, AW Flagg, L Weinberger, AJ Aller, KM Allers, KN Best, WMJ Kotson, MC Montet, BT Herczeg, GJ Baranec, C Riddle, R Law, NM Nielsen, EL Wahhaj, Z Biller, BA Hayward, TL AF Bowler, Brendan P. Shkolnik, Evgenya L. Liu, Michael C. Schlieder, Joshua E. Mann, Andrew W. Dupuy, Trent J. Hinkley, Sasha Crepp, Justin R. Johnson, John Asher Howard, Andrew W. Flagg, Laura Weinberger, Alycia J. Aller, Kimberly M. Allers, Katelyn N. Best, William M. J. Kotson, Michael C. Montet, Benjamin T. Herczeg, Gregory J. Baranec, Christoph Riddle, Reed Law, Nicholas M. Nielsen, Eric L. Wahhaj, Zahed Biller, Beth A. Hayward, Thomas L. TI PLANETS AROUND LOW-MASS STARS (PALMS). V. AGE-DATING LOW-MASS COMPANIONS TO MEMBERS AND INTERLOPERS OF YOUNG MOVING GROUPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: spectroscopic; brown dwarfs; stars: individual (2MASS J02155892, 0929121, 2MASS J15594729+4403595, HD 23514) ID TW-HYDRAE ASSOCIATION; DIGITAL SKY SURVEY; VERY-LOW MASS; BRIGHT SOURCE CATALOG; X-RAY SOURCES; SOUTHERN SPECTROPHOTOMETRIC STANDARDS; CANDIDATE SUBSTELLAR COMPANION; SUPERNOVA FACTORY OBSERVATIONS; FINDING CAMPAIGN DISCOVERY; EXTRASOLAR GIANT PLANETS AB We present optical and near-infrared adaptive optics (AO) imaging and spectroscopy of 13 ultracool (>M6) companions to late-type stars (K7-M4.5), most of which have recently been identified as candidate members of nearby young moving groups (YMGs; 8-120 Myr) in the literature. Three of these are new companions identified in our AO imaging survey, and two others are confirmed to be comoving with their host stars for the first time. The inferred masses of the companions (similar to 10-100 M-Jup) are highly sensitive to the ages of the primary stars; therefore we critically examine the kinematic and spectroscopic properties of each system to distinguish bona fide YMG members from old field interlopers. The new M7 substellar companion 2MASS J02155892-0929121 C (40-60 M-Jup) shows. clear spectroscopic signs of low gravity and, hence, youth. The primary, possibly a member of the similar to 40 Myr Tuc-Hor moving group, is visually resolved into three components, making it a young low-mass quadruple system in a compact (less than or similar to 100 AU) configuration. In addition, LiI lambda 6708 absorption in the intermediate-gravity M7.5 companion 2MASS J15594729+4403595 B provides unambiguous evidence that it is young (less than or similar to 200 Myr) and resides below the hydrogen-burning limit. Three new close-separation (<1 '') companions (2MASS J06475229-2523304 B, PYC J11519+0731 B, and GJ 4378 Ab) orbit stars previously reported as candidate YMG members, but instead are likely old (greater than or similar to 1Gyr) tidally locked spectroscopic binaries without convincing kinematic associations with any known moving group. The high rate of false positives in the form of old active stars with YMG-like kinematics underscores the importance of radial velocity and parallax measurements to validate candidate young stars identified via proper motion and activity selection alone. Finally, we spectroscopically confirm the cool temperature and substellar nature of HD 23514 B, a recently discovered M8 benchmark brown dwarf orbiting the dustiest-known member of the Pleiades. C1 [Bowler, Brendan P.; Montet, Benjamin T.; Riddle, Reed] CALTECH, Pasadena, CA 91125 USA. [Shkolnik, Evgenya L.; Flagg, Laura] Lowell Observ, Flagstaff, AZ 86001 USA. [Liu, Michael C.; Howard, Andrew W.; Aller, Kimberly M.; Best, William M. J.; Kotson, Michael C.; Baranec, Christoph] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Schlieder, Joshua E.] NASA, Ames Res Ctr, Postdoctoral Program Fellow, Moffett Field, CA 94035 USA. [Mann, Andrew W.; Dupuy, Trent J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Hinkley, Sasha] Univ Exeter, Phys & Astron, Exeter EX4 4QL, Devon, England. [Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Johnson, John Asher; Montet, Benjamin T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Flagg, Laura] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. [Weinberger, Alycia J.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Allers, Katelyn N.] Bucknell Univ, Dept Phys & Astron, Lewisburg, PA 17837 USA. [Herczeg, Gregory J.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Law, Nicholas M.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. [Nielsen, Eric L.] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA. [Nielsen, Eric L.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA USA. [Wahhaj, Zahed] European So Observ, Santiago, Chile. [Biller, Beth A.] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Hayward, Thomas L.] Southern Operat Ctr AURA, Gemini Observ, La Serena, Chile. RP Bowler, BP (reprint author), CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM bpbowler@caltech.edu OI Montet, Benjamin/0000-0001-7516-8308; Nielsen, Eric/0000-0001-6975-9056; Herczeg, Gregory/0000-0002-7154-6065 FU NASA Grant [NNX11AC31G]; NSF Grant [AST09-09222]; National Science Foundation [AST-0906060, AST-0960343, AST-1207891]; Mt. Cuba Astronomical Foundation; Alfred P. Sloan Foundation; National Science Foundation Graduate Research Fellowship [DGE1144469]; National Aeronautics and Space Administration; National Science Foundation FX We thank the referee for their helpful suggestions and Niall Deacon for obtaining some of the IRTF observations presented here. M.C.L. has been supported by NASA Grant NNX11AC31G and NSF Grant AST09-09222. This paper is based on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory (NOAO Prop. ID: 2014B-0083; PI: Bowler), which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. This research is also based in part on observations obtained at the Gemini Observatory, which is operated by AURA under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil) and CONICET (Argentina). The Robo-AO system was developed by collaborating partner institutions, the California Institute of Technology and the Inter-University Centre for Astronomy and Astrophysics, and with the support of the National Science Foundation under Grants AST-0906060, AST-0960343, and AST-1207891, the Mt. Cuba Astronomical Foundation, and by a gift from Samuel Oschin. Ongoing science operation support of Robo-AO is provided by the California Institute of Technology and the University of Hawai'i. C.B. acknowledges support from the Alfred P. Sloan Foundation. B.T.M. is supported by a National Science Foundation Graduate Research Fellowship under Grant DGE1144469. We utilized 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. NASA's Astrophysics Data System Bibliographic Services together with the VizieR catalog access tool and SIMBAD database operated at CDS, Strasbourg, France, were invaluable resources for this work. This research has made use of the Washington Double Star Catalog maintained at the U.S. Naval Observatory. Finally, mahalo nui loa to the kama'aina of Hawai'i for their support of Keck and the Maunakea observatories. We are grateful to conduct observations from this mountain. NR 203 TC 7 Z9 7 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 62 DI 10.1088/0004-637X/806/1/62 PG 36 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300062 ER PT J AU Brodwin, M Greer, CH Leitch, EM Stanford, SA Gonzalez, AH Gettings, DP Abdulla, Z Carlstrom, JE Decker, B Eisenhardt, PR Lin, HW Mantz, AB Marrone, DP McDonald, M Stalder, B Stern, D Wylezalek, D AF Brodwin, M. Greer, C. H. Leitch, E. M. Stanford, S. A. Gonzalez, A. H. Gettings, D. P. Abdulla, Z. Carlstrom, J. E. Decker, B. Eisenhardt, P. R. Lin, H. W. Mantz, A. B. Marrone, D. P. McDonald, M. Stalder, B. Stern, D. Wylezalek, D. TI THE MASSIVE AND DISTANT CLUSTERS OF WISE SURVEY. III. SUNYAEV-ZEL'DOVICH MASSES OF GALAXY CLUSTERS AT z similar to 1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: clusters: general; galaxies: clusters: intracluster medium; galaxies: high-redshift; infrared: galaxies ID SOUTH-POLE TELESCOPE; 720 SQUARE DEGREES; X-RAY-PROPERTIES; SPECTROSCOPIC CONFIRMATION; STAR-FORMATION; COSMOLOGICAL IMPLICATIONS; SKY SURVEY; DISCOVERY; SAMPLE; CATALOG AB We present CARMA 30 GHz Sunyaev-Zel'dovich (SZ) observations of five high-redshift (z greater than or similar to 1), infrared-selected galaxy clusters discovered as part of the all-sky Massive and Distant Clusters of WISE Survey (MaDCoWS). The SZ decrements measured toward these clusters demonstrate that the MaDCoWS selection is discovering evolved, massive galaxy clusters with hot intracluster gas. Using the SZ scaling relation calibrated with South Pole Telescope clusters at similar masses and redshifts, we find these MaDCoWS clusters have masses in the range M-200 approximate to 2-6 x 10(14) M-circle dot. Three of these are among the most massive clusters found to date at z greater than or similar to 1, demonstrating that MaDCoWS is sensitive to the most massive clusters to at least z = 1.3. The added depth of the AllWISE data release will allow all-sky infrared cluster detection to z approximate to 1.5 and beyond. C1 [Brodwin, M.; Decker, B.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Greer, C. H.; Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85121 USA. [Leitch, E. M.; Abdulla, Z.; Carlstrom, J. E.; Mantz, A. B.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Leitch, E. M.; Abdulla, Z.; Carlstrom, J. E.; Mantz, A. B.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Stanford, S. A.] Univ Calif Davis, Davis, CA 95616 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. [Gonzalez, A. H.; Gettings, D. P.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Eisenhardt, P. R.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lin, H. W.; Stalder, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Wylezalek, D.] European So Observ, Garching, Germany. RP Brodwin, M (reprint author), Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. OI Marrone, Daniel/0000-0002-2367-1080 FU Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris Foundation; James S. McDonnell Foundation; Associates of the California Institute of Technology; University of Chicago; state of California; state of Illinois; state of Maryland; National Science Foundation; CARMA partner universities; NSF [AST-1140019]; National Aeronautics and Space Administration; NASA Astrophysics Data Analysis Program (ADAP) [NNX12AE15G]; NASA Keck PI Data Award; W. M. Keck Foundation; [PHY-0114422]; [GN-2013A-Q-44]; [GN-2013B-Q-8] FX We thank the anonymous referee for helpful comments that improved the paper. We thank L. Bleem for providing the code and data to produce Figure 4 and B. Benson for helpful conversations. Support for CARMA construction was derived from the Gordon and Betty Moore Foundation; the Kenneth T. and Eileen L. Norris Foundation; the James S. McDonnell Foundation; the Associates of the California Institute of Technology; the University of Chicago; the states of California, Illinois, and Maryland; and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement and by the CARMA partner universities; the work at Chicago was supported by NSF grant AST-1140019. Additional support was provided by PHY-0114422. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. M.B., D.P.G., A.H.G., and S.A.S. acknowledge support for this research from the NASA Astrophysics Data Analysis Program (ADAP) through grant NNX12AE15G. This work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. 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 work is based in part on data 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. Based in part on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). Data were obtained in Program IDs GN-2013A-Q-44 and GN-2013B-Q-8. This paper includes data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile. NR 52 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 26 DI 10.1088/0004-637X/806/1/26 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300026 ER PT J AU Cohen, O Ma, Y Drake, JJ Glocer, A Garraffo, C Bell, JM Gombosi, TI AF Cohen, O. Ma, Y. Drake, J. J. Glocer, A. Garraffo, C. Bell, J. M. Gombosi, T. I. TI THE INTERACTION OF VENUS-LIKE, M-DWARF PLANETS WITH THE STELLAR WIND OF THEIR HOST STAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); planets and satellites: atmospheres; planets and satellites: magnetic fields; planets and satellites: terrestrial planets ID RESISTIVE MHD SIMULATIONS; EARTH-LIKE EXOPLANETS; EJECTION CME ACTIVITY; CLOSE-IN EXOPLANETS; MASS M-STARS; HABITABLE ZONES; HOT JUPITERS; GANYMEDES MAGNETOSPHERE; TERRESTRIAL EXOPLANETS; ATMOSPHERIC ESCAPE AB We study the interaction between the atmospheres of Venus-like, non-magnetized exoplanets orbiting an M-dwarf star, and the stellar wind using a multi-species MHD model. We focus our investigation on the effect of enhanced stellar wind and enhanced EUV flux as the planetary distance from the star decreases. Our simulations reveal different topologies of the planetary space environment for sub- and super-Alfvenic stellar wind conditions, which could lead to dynamic energy deposition into the atmosphere during the transition along the planetary orbit. We find that the stellar wind penetration for non-magnetized planets is very deep, up to a few hundreds of kilometers. We estimate a lower limit for the atmospheric mass-loss rate and find that it is insignificant over the lifetime of the planet. However, we predict that when accounting for atmospheric ion acceleration, a significant amount of the planetary atmosphere could be eroded over the course of a billion years. C1 [Cohen, O.; Drake, J. J.; Garraffo, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ma, Y.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Glocer, A.] NASA, GSFC, Greenbelt, MD 20771 USA. [Bell, J. M.] NIA, Ctr Planetary Atmospheres & Flight Sci, Hampton, VA 23666 USA. [Gombosi, T. I.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA. RP Cohen, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Gombosi, Tamas/G-4238-2011; OI Gombosi, Tamas/0000-0001-9360-4951; Cohen, Ofer/0000-0003-3721-0215 FU Smithsonian Institution Consortium; Smithsonian Institute Competitive Grants Program for Science (CGPS) grant "Can Exoplanets Around Red Dwarfs Maintain Habitable Atmospheres?"; NASA Astrobiology Institute grant [NNX15AE05G]; NASA ESS; NASA ESTO-CT; NSF KDI; DoD MURI; NASA [NAS8-03060] FX We thank an anonymous referee for his/her useful comments. The work presented here was funded by the Smithsonian Institution Consortium for Unlocking the Mysteries of the Universe grant "Lessons from Mars: Are Habitable Atmospheres on Planets around M Dwarfs Viable?", by the Smithsonian Institute Competitive Grants Program for Science (CGPS) grant "Can Exoplanets Around Red Dwarfs Maintain Habitable Atmospheres?", and by NASA Astrobiology Institute grant NNX15AE05G. Simulation results were obtained using the Space Weather Modeling Framework, developed by the Center for Space Environment Modeling, at the University of Michigan with funding support from NASA ESS, NASA ESTO-CT, NSF KDI, and DoD MURI. The simulations were performed on the Smithsonian Institute HYDRA cluster. J.J.D. was supported by NASA contract NAS8-03060 to the Chandra X-ray Center during the course of this research and thanks the Director, B. Wilkes, for continuing support and encouragement. NR 69 TC 7 Z9 7 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 41 DI 10.1088/0004-637X/806/1/41 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300041 ER PT J AU Czakon, NG Sayers, J Mantz, A Golwala, SR Downes, TP Koch, PM Lin, KY Molnar, SM Moustakas, LA Mroczkowski, T Pierpaoli, E Shitanishi, JA Siegel, S Umetsu, K AF Czakon, N. G. Sayers, J. Mantz, A. Golwala, S. R. Downes, T. P. Koch, P. M. Lin, K. -Y. Molnar, S. M. Moustakas, L. A. Mroczkowski, T. Pierpaoli, E. Shitanishi, J. A. Siegel, S. Umetsu, K. TI GALAXY CLUSTER SCALING RELATIONS BETWEEN BOLOCAM SUNYAEV-ZEL'DOVICH EFFECT AND CHANDRA X-RAY MEASUREMENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: intracluster medium ID SOUTH-POLE TELESCOPE; WEAK-LENSING MASSES; 720 SQUARE DEGREES; COSMOLOGICAL CONSTRAINTS; MACS J0717.5+3745; SECONDARY CALIBRATORS; TEMPERATURE RELATION; OBSERVED GROWTH; RICH CLUSTERS; XMM-NEWTON AB We present scaling relations between the integrated Sunyaev-Zel'dovich effect (SZE) signal, Y-SZ, its X-ray analogue, Y-X = MgasTX, and total mass, M-tot, for the 45 galaxy clusters in the Bolocam X-ray SZ (BOXSZ) sample. All parameters are integrated within r(2500). Y-2500 values are measured using SZE data collected with Bolocam, operating at 140 GHz at the Caltech Submillimeter Observatory. The temperature, T-X, and mass, M-gas,M- 2500, of the intracluster medium are determined using X-ray data collected with Chandra, and M-tot is derived from M-gas assuming a constant gas mass fraction. Our analysis accounts for several potential sources of bias, including selection effects, contamination from radio point sources, and the loss of SZE signal due to noise filtering and beam-smoothing effects. We measure the Y-2500-Y-X scaling to have a power-law index of 0.84 +/- 0.07, and a fractional intrinsic scatter in Y-2500 of (21 +/- 7)% at fixed Y-X, both of which are consistent with previous analyses. We also measure the scaling between Y-2500 and M-2500, finding a power-law index of 1.06 +/- 0.12 and a fractional intrinsic scatter in Y-2500 at fixed mass of (25 +/- 9)%. While recent SZE scaling relations using X-ray mass proxies have found power-law indices consistent with the self-similar prediction of 5/3, our measurement stands apart by differing from the self-similar prediction by approximately 5 sigma. Given the good agreement between the measured Y-2500-Y-X scalings, much of this discrepancy appears to be caused by differences in the calibration of the X-ray mass proxies adopted for each particular analysis. C1 [Czakon, N. G.; Koch, P. M.; Lin, K. -Y.; Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Sayers, J.; Golwala, S. R.; Downes, T. P.; Siegel, S.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Mantz, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Molnar, S. M.] Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan. [Moustakas, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mroczkowski, T.] Naval Res Lab, Washington, DC 20375 USA. [Pierpaoli, E.; Shitanishi, J. A.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA. RP Czakon, NG (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. EM czakon@asiaa.sinica.edu.tw OI Mroczkowski, Tony/0000-0003-3816-5372; Umetsu, Keiichi/0000-0002-7196-4822; Moustakas, Leonidas/0000-0003-3030-2360; Pierpaoli, Elena/0000-0002-7957-8993 FU Gordon and Betty Moore Foundation; Jet Propulsion Laboratory Research and Technology Development Program; National Science Council of Taiwan [NSC100-2112-M-001-008-MY3]; NASA Graduate Student Research Fellowship; NASA Postdoctoral Program; Norris Foundation CCAT Postdoctoral Fellowship; NSF [AST-0838187, AST-1140019]; NASA - Chandra X-ray Center [PF0-110077]; NASA [NAS8-03060]; National Research Council Fellowship; Academia Sinica Career Development Award; [NSF/AST-9618798]; [NSF/AST-0098737]; [NSF/AST-9980846]; [NSF/AST-0229008]; [NSF/AST-0206158]; [NASA/NNX07AH59G] FX This material is based upon work at the CSO, which, when the data used in this analysis were taken, was operated by the California Institute of Technology under cooperative agreement with the National Science Foundation. Bolocam was constructed and commissioned using funds from NSF/AST-9618798, NSF/AST-0098737, NSF/AST-9980846, NSF/AST-0229008, and NSF/AST-0206158. Bolocam observations were partially supported by the Gordon and Betty Moore Foundation, the Jet Propulsion Laboratory Research and Technology Development Program, as well as the National Science Council of Taiwan grant NSC100-2112-M-001-008-MY3. We acknowledge the assistance of: the Bolocam instrument team: P.A.R. Ade, J.E. Aguirre, J.J. Bock, S.F. Edgington, J. Glenn, A. Goldin, S.R. Golwala, D. Haig, A.E. Lange, G.T. Laurent, P.D. Mauskopf, H.T. Nguyen, P. Rossinot, and J. Sayers; Matt Ferry, who helped collect the data for Abell 1835 and MS 1054.4-0321; the day crew and Hilo staff of the CSO, who provided invaluable assistance during commissioning and data-taking for this survey data set; and Kathy Deniston, Barbara Wertz, and Diana Bisel, who provided effective administrative support at Caltech and in Hilo. This research made extensive use of high performance computing resources at the U.S. Planck Data Center, which is a part of the Infrared Processing and Analysis Center at Caltech. We also thank an anonymous referee for a detailed report that substantially improved the quality of this paper. N.C. was partially supported by a NASA Graduate Student Research Fellowship; J.S. was partially supported by a NASA Graduate Student Research Fellowship, a NASA Postdoctoral Program fellowship, and a Norris Foundation CCAT Postdoctoral Fellowship; A.M. was funded by NSF AST-0838187 and AST-1140019. The work of L.A.M. was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA; support for T.M. was provided by NASA through Einstein Fellowship Program grant No. PF0-110077 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060, and by a National Research Council Fellowship. E.P. and J.A.S. were partially supported by NASA/NNX07AH59G. K.U. acknowledges partial support from the Academia Sinica Career Development Award. NR 109 TC 13 Z9 13 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 JUN 10 PY 2015 VL 806 IS 1 AR 18 DI 10.1088/0004-637X/806/1/18 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300018 ER PT J AU De Rosa, G Peterson, BM Ely, J Kriss, GA Crenshaw, DM Horne, K Korista, KT Netzer, H Pogge, RW Arevalo, P Barth, AJ Bentz, MC Brandt, WN Breeveld, AA Brewer, BJ Bonta, ED De Lorenzo-Caceres, A Denney, KD Dietrich, M Edelson, R Evans, PA Fausnaugh, MM Gehrels, N Gelbord, JM Goad, MR Grier, CJ Grupe, D Hall, PB Kaastra, J Kelly, BC Kennea, JA Kochanek, CS Lira, P Mathur, S McHardy, IM Nousek, JA Pancoast, A Papadakis, I Pei, L Schimoia, JS Siegel, M Starkey, D Treu, T Uttley, P Vaughan, S Vestergaard, M Villforth, C Yan, H Young, S Zu, Y AF De Rosa, G. Peterson, B. M. Ely, J. Kriss, G. A. Crenshaw, D. M. Horne, Keith Korista, K. T. Netzer, H. Pogge, R. W. Arevalo, P. Barth, A. J. Bentz, M. C. Brandt, W. N. Breeveld, A. A. Brewer, B. J. Bonta, E. Dalla De Lorenzo-Caceres, A. Denney, K. D. Dietrich, M. Edelson, R. Evans, P. A. Fausnaugh, M. M. Gehrels, N. Gelbord, J. M. Goad, M. R. Grier, C. J. Grupe, D. Hall, P. B. Kaastra, J. Kelly, B. C. Kennea, J. A. Kochanek, C. S. Lira, P. Mathur, S. McHardy, I. M. Nousek, J. A. Pancoast, A. Papadakis, I. Pei, L. Schimoia, J. S. Siegel, M. Starkey, D. Treu, T. Uttley, P. Vaughan, S. Vestergaard, M. Villforth, C. Yan, H. Young, S. Zu, Y. TI SPACE TELESCOPE AND OPTICAL REVERBERATION MAPPING PROJECT. I. ULTRAVIOLET OBSERVATIONS OF THE SEYFERT 1 GALAXY NGC 5548 WITH THE COSMIC ORIGINS SPECTROGRAPH ON HUBBLE SPACE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 5548); galaxies: nuclei; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; BROAD-LINE REGION; BLACK-HOLE MASS; RADIUS-LUMINOSITY RELATIONSHIP; PEAKED EMISSION-LINES; TERM PROFILE VARIABILITY; VELOCITY-DELAY MAPS; H-BETA EMISSION; IONIZED ABSORPTION; QUASAR VARIABILITY AB We describe the first results from a six-month long reverberation-mapping experiment in the ultraviolet based on 171 observations of the Seyfert 1 galaxy NGC 5548 with the Cosmic Origins Spectrograph on the Hubble Space Telescope. Significant correlated variability is found in the continuum and broad emission lines, with amplitudes ranging from similar to 30% to a factor of two in the emission lines and a factor of three in the continuum. The variations of all the strong emission lines lag behind those of the continuum, with He II lambda 1640 lagging behind the continuum by similar to 2.5 days and Ly alpha lambda 1215, CIV lambda 1550, and Si IV lambda 1400 lagging by similar to 5-6 days. The relationship between the continuum and emission lines is complex. In particular, during the second half of the campaign, all emission-line lags increased by a factor of 1.3-2 and differences appear in the detailed structure of the continuum and emission-line light curves. Velocity-resolved cross-correlation analysis shows coherent structure in lag versus line of sight velocity for the emission lines; the high-velocity wings of C-IV respond to continuum variations more rapidly than the line core, probably indicating higher velocity broad-line region clouds at smaller distances from the central engine. The velocity-dependent response of Ly alpha, however, is more complex and will require further analysis. C1 [De Rosa, G.; Peterson, B. M.; Pogge, R. W.; Fausnaugh, M. M.; Grier, C. J.; Kochanek, C. S.; Mathur, S.; Schimoia, J. S.; Zu, Y.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [De Rosa, G.; Peterson, B. M.; Pogge, R. W.; Kochanek, C. S.; Mathur, S.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA. [De Rosa, G.; Ely, J.; Kriss, G. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kriss, G. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Crenshaw, D. M.; Bentz, M. C.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Horne, Keith; De Lorenzo-Caceres, A.; Starkey, D.; Villforth, C.] Univ St Andrews, SUPA Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Korista, K. T.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. [Netzer, H.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile. [Barth, A. J.; Pei, L.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Brandt, W. N.; Grier, C. J.; Kennea, J. A.; Nousek, J. A.; Siegel, M.] Penn State Univ, Dept Astron & Astrophys, Eberly Coll Sci, University Pk, PA 16802 USA. [Breeveld, A. A.; Denney, K. D.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Brewer, B. J.] Univ Auckland, Dept Stat, Auckland 1142, New Zealand. [Bonta, E. Dalla] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35122 Padua, Italy. [Bonta, E. Dalla] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Dietrich, M.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. [Dietrich, M.] Worcester State Univ, Dept Earth Environm & Phys, Worcester, MA 01602 USA. [Edelson, R.; Young, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Evans, P. A.; Goad, M. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Gehrels, N.; Vaughan, S.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Gelbord, J. M.] Spectral Sci Inc, Burlington, MA 01803 USA. [Gelbord, J. M.] Eureka Sci Inc, Oakland, CA 94602 USA. [Grupe, D.] Morehead State Univ, Ctr Space Sci, Morehead, KY 40351 USA. [Hall, P. B.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. [Kaastra, J.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Kaastra, J.] Univ Utrecht, Dept Phys & Astron, NL-3508 Utrecht, Netherlands. [Kaastra, J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Kelly, B. C.; Pancoast, A.; Treu, T.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Lira, P.] Univ Chile, Dept Astron, Camino Observ 1515, Santiago, Chile. [McHardy, I. M.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [Papadakis, I.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece. [Papadakis, I.] Univ Crete, Inst Theoret & Computat Phys, GR-71003 Iraklion, Greece. [Papadakis, I.] Fdn Res & Technol, IESL, GR-71110 Iraklion, Greece. [Schimoia, J. S.] Univ Fed Rio Grande do Sul, Inst Fis, Porto Alegre, RS, Brazil. [Treu, T.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Uttley, P.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Vestergaard, M.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Vestergaard, M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Yan, H.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. [Zu, Y.] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Denney, K. D.] NSF, Arlington, VA USA. [Treu, T.] Packard, Detroit, MI USA. RP De Rosa, G (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. RI Brandt, William/N-2844-2015; Papadakis, Iossif/C-3235-2011; Lira, Paulina/G-8536-2016; OI Brandt, William/0000-0002-0167-2453; Vestergaard, Marianne/0000-0001-9191-9837; Zu, Ying/0000-0001-6966-6925; Peterson, Bradley/0000-0001-6481-5397; Pogge, Richard/0000-0003-1435-3053; Barth, Aaron/0000-0002-3026-0562 FU NASA from the Space Telescope Science Institute [GO-13330]; NASA [NAS5-26555, NNX13AC26G, NNX13AC63G, NNX13AE99G, NNH13CH61C]; National Science Foundation [AST-1008882]; NSF [AST-1412693, AST-1009756, AST-1412315, AST-1253702, AST-1302093]; NSERC; NWO; Netherlands Organization for Scientific Research; UC Center for Galaxy Evolution; Fondecyt grant [1120328]; NSF; UCSB; CNPq; National Council for Scientific and Technological Development (Brazil); Packard Foundation; Danish National Research Foundation; Danish Council for Independent Research [DFF 4002-00275] FX Support for HST program number GO-13330 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. We are grateful for the dedication and hard work by the Institute staff to make this program a success. G.D.R., B.M.P.,C.J.G., M.M.F., and R.W.P. are grateful for the support of the National Science Foundation through grant AST-1008882 to The Ohio State University. A.J.B. and L.P. have been supported by NSF grant AST-1412693. M.C.B. gratefully acknowledges support through NSF CAREER grant AST-1253702 to Georgia State University. K.D.D. is supported by an NSF Fellowship awarded under grant AST-1302093. R.E. gratefully acknowledges support from NASA under awards NNX13AC26G, NNX13AC63G, and NNX13AE99G. J.M.G. gratefully acknowledges support from NASA under award NNH13CH61C. P.B.H. is supported by NSERC. SRON is financially supported by NWO, the Netherlands Organization for Scientific Research. B.C.K. is partially supported by the UC Center for Galaxy Evolution. C.S.K. acknowledges the support of NSF grant AST-1009756. P.L. acknowledges support from Fondecyt grant #1120328. A.P. acknowledges support from a NSF graduate fellowship and a UCSB Dean's Fellowship. J.S.S. acknowledges CNPq, National Council for Scientific and Technological Development (Brazil) for partial support and The Ohio State University for warm hospitality. T.T. has been supported by NSF grant AST-1412315. T.T. and B.C.K. acknowledge support from the Packard Foundation in the form of a Packard Research Fellowship to T.T. T.T. thanks the American Academy in Rome and thee Observatory of Monteporzio Catone for kind hospitality. The Dark Cosmology Centre is funded by the Danish National Research Foundation. MV gratefully acknowledges support from the Danish Council for Independent Research via grant No. DFF 4002-00275. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The authors acknowledge with great sadness the loss of our longtime collaborator in the planning phases of this project, Professor David J. Axon, who passed away on 2012 April 5. NR 124 TC 23 Z9 23 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 128 DI 10.1088/0004-637X/806/1/128 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300128 ER PT J AU Dressler, A Henry, A Martin, CL Sawicki, M McCarthy, P Villaneuva, E AF Dressler, Alan Henry, Alaina Martin, Crystal L. Sawicki, Marcin McCarthy, Patrick Villaneuva, Edward TI CONFIRMATION OF A STEEP LUMINOSITY FUNCTION FOR Ly alpha EMITTERS AT z=5.7: A MAJOR COMPONENT OF REIONIZATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift ID LYMAN-BREAK GALAXIES; ULTRA-DEEP-FIELD; STAR-FORMATION RATE; 7 CANDIDATE GALAXIES; SIMILAR-TO 8; ESCAPE FRACTION; COSMIC REIONIZATION; KECK SPECTROSCOPY; FORMATION HISTORY; IONIZING PHOTONS AB We report the first direct and robust measurement of the faint-end slope of the Ly alpha emitter (LAE) luminosity function (LF) at z = 5.7. Candidate LAEs from a low-spectral-resolution blind search with IMACS on Magellan-Baade were targeted at higher resolution to distinguish high-redshift LAEs from foreground galaxies. All but 2 of our 42 single-emission-line systems have flux F < 2.0x10(-17) ergs s(-1) cm(-2), making these the faintest emission-lines observed for a z = 5.7 sample with known completeness, an essential property for determining the faint end slope of the LAE LF. We find 13 LAEs as compared to 29 foreground galaxies, in very good agreement with the modeled foreground counts predicted in Dressler et al. that had been used to estimate a faint-end slope of alpha = -2.0 for the LAE LF. A 32% LAE fraction, LAE/(LAE+foreground) within the flux interval F = 2-20 x 10(-18) ergs s(-1) cm(-2) constrains the faint end slope of the LF to -2.35 < alpha < -1.95 (1 sigma). We show how this steep LF should provide, to the limit of our observations, M-UV similar to -16, more than 20% of the flux necessary to maintain ionization at z = 5.7, with a factor of 10 extrapolation in flux reaching more than 50%. This is in addition to the comparable contribution by brighter Lyman Break Galaxies M-UV less than or similar to -18. We suggest that this bodes well for a sufficient supply of Lyman continuum photons by similar, low-mass star-forming galaxies within the reionization epoch at z approximate to 7, only 250 Myr earlier. C1 [Dressler, Alan; McCarthy, Patrick; Villaneuva, Edward] Carnegie Observ, Pasadena, CA 91101 USA. [Henry, Alaina] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Martin, Crystal L.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Sawicki, Marcin] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. RP Dressler, A (reprint author), Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA. EM dressler@obs.carnegiescience.edu; alaina.henry@nasa.gov; cmartin@physics.ucsb.edu; sawicki@ap.smu.ca; pmc2@obs.carnegiescience.edu; edwardv@obs.carnegiescience.edu NR 55 TC 13 Z9 13 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 JUN 10 PY 2015 VL 806 IS 1 AR 19 DI 10.1088/0004-637X/806/1/19 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300019 ER PT J AU Edelson, R Gelbord, JM Horne, K McHardy, IM Peterson, BM Arevalo, P Breeveld, AA De Rosa, G Evans, PA Goad, MR Kriss, GA Brandt, WN Gehrels, N Grupe, D Kennea, JA Kochanek, CS Nousek, JA Papadakis, I Siegel, M Starkey, D Uttley, P Vaughan, S Young, S Barth, AJ Bentz, MC Brewer, BJ Crenshaw, DM Bonta, ED De Lorenzo-Caceres, A Denney, KD Dietrich, M Ely, J Fausnaugh, MM Grier, CJ Hall, PB Kaastra, J Kelly, BC Korista, KT Lira, P Mathur, S Netzer, H Pancoast, A Pei, L Pogge, RW Schimoia, JS Treu, T Vestergaard, M Villforth, C Yan, H Zu, Y AF Edelson, R. Gelbord, J. M. Horne, K. McHardy, I. M. Peterson, B. M. Arevalo, P. Breeveld, A. A. De Rosa, G. Evans, P. A. Goad, M. R. Kriss, G. A. Brandt, W. N. Gehrels, N. Grupe, D. Kennea, J. A. Kochanek, C. S. Nousek, J. A. Papadakis, I. Siegel, M. Starkey, D. Uttley, P. Vaughan, S. Young, S. Barth, A. J. Bentz, M. C. Brewer, B. J. Crenshaw, D. M. Bonta, E. Dalla De Lorenzo-Caceres, A. Denney, K. D. Dietrich, M. Ely, J. Fausnaugh, M. M. Grier, C. J. Hall, P. B. Kaastra, J. Kelly, B. C. Korista, K. T. Lira, P. Mathur, S. Netzer, H. Pancoast, A. Pei, L. Pogge, R. W. Schimoia, J. S. Treu, T. Vestergaard, M. Villforth, C. Yan, H. Zu, Y. TI SPACE TELESCOPE AND OPTICAL REVERBERATION MAPPING PROJECT. II. SWIFT AND HST REVERBERATION MAPPING OF THE ACCRETION DISK OF NGC 5548 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 5548); galaxies: nuclei; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; BROAD-LINE REGION; RADIUS-LUMINOSITY RELATIONSHIP; X-RAY; CONTINUUM EMISSION; SEYFERT-GALAXIES; ULTRAVIOLET/OPTICAL TELESCOPE; EMITTING REGIONS; MR 2251-178; VARIABILITY AB Recent intensive Swift monitoring of the Seyfert 1 galaxy NGC 5548 yielded 282 usable epochs over 125 days across six UV/optical bands and the X-rays. This is the densest extended active galactic nucleus (AGN) UV/optical continuum sampling ever obtained, with a mean sampling rate <0.5 day. Approximately daily Hubble Space Telescope UV sampling was also obtained. The UV/optical light curves show strong correlations (r(max) = 0.57 - 0.90) and the clearest measurement to date of interband lags. These lags are well-fit by a tau alpha lambda(4/3) wavelength dependence, with a normalization that indicates an unexpectedly large disk radius of similar to 0.35 +/- 0.05 lt-day at 1367 angstrom, assuming a simple face-on model. The U band shows a marginally larger lag than expected from the fit and surrounding bands, which could be due to Balmer continuum emission from the broad-line region as suggested by Korista and Goad. The UV/X-ray correlation is weaker (r(max) < 0.45) and less consistent over time. This indicates that while Swift is beginning to measure UV/optical lags in general agreement with accretion disk theory (although the derived size is larger than predicted), the relationship with X-ray variability is less well understood. Combining this accretion disk size estimate with those from quasar microlensing studies suggests that AGN disk sizes scale approximately linearly with central black hole mass over a wide range of masses. C1 [Edelson, R.; Young, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Gelbord, J. M.] Spectral Sci Inc, Burlington, MA 01803 USA. [Gelbord, J. M.] Eureka Sci Inc, Oakland, CA 94602 USA. [Horne, K.; Starkey, D.; De Lorenzo-Caceres, A.; Villforth, C.] Univ St Andrews, SUPA Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [McHardy, I. M.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [Peterson, B. M.; De Rosa, G.; Kochanek, C. S.; Denney, K. D.; Fausnaugh, M. M.; Grier, C. J.; Mathur, S.; Pogge, R. W.; Schimoia, J. S.; Zu, Y.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Peterson, B. M.; De Rosa, G.; Kochanek, C. S.; Denney, K. D.; Mathur, S.; Pogge, R. W.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA. [Breeveld, A. A.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile. [Breeveld, A. A.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [De Rosa, G.; Kriss, G. A.; Ely, J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Evans, P. A.; Goad, M. R.; Vaughan, S.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Kriss, G. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Brandt, W. N.; Kennea, J. A.; Nousek, J. A.; Siegel, M.; Grier, C. J.] Penn State Univ, Dept Astron & Astrophys, Eberly Coll Sci, Davey Lab 525, University Pk, PA 16802 USA. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Grupe, D.] Morehead State Univ, Ctr Space Sci, Morehead, KY 40351 USA. [Papadakis, I.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece. [Papadakis, I.] Univ Crete, Inst Theoret & Computat Phys, GR-71003 Iraklion, Greece. [Papadakis, I.] Fdn Res & Technol, IESL, GR-71110 Iraklion, Greece. [Uttley, P.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Barth, A. J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Bentz, M. C.; Crenshaw, D. M.; Pei, L.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Brewer, B. J.] Univ Auckland, Dept Stat, Auckland 1142, New Zealand. [Bonta, E. Dalla] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35122 Padua, Italy. [Bonta, E. Dalla] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Dietrich, M.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. [Dietrich, M.] Worcester State Univ, Dept Phys & Earth Sci, Worcester, MA 01602 USA. [Hall, P. B.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. [Kaastra, J.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Kaastra, J.] Univ Utrecht, Dept Phys & Astron, NL-3508 Utrecht, Netherlands. [Kaastra, J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Kelly, B. C.; Pancoast, A.; Treu, T.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Korista, K. T.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. [Lira, P.] Univ Chile, Dept Astron, Camino Observ 1515, Santiago, Chile. [Netzer, H.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Schimoia, J. S.] Univ Fed Rio Grande do Sul, Inst Fis, Porto Alegre, RS, Brazil. [Treu, T.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Vestergaard, M.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Vestergaard, M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Yan, H.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. [Yan, H.] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Denney, K. D.] NSF, Arlington, VA USA. [Treu, T.] Packard, Detroit, MI USA. RP Edelson, R (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RI Brandt, William/N-2844-2015; Papadakis, Iossif/C-3235-2011; Lira, Paulina/G-8536-2016; OI Brandt, William/0000-0002-0167-2453; Barth, Aaron/0000-0002-3026-0562; Vestergaard, Marianne/0000-0001-9191-9837; Zu, Ying/0000-0001-6966-6925 FU NASA from the Space Telescope Science Institute [GO-13330]; NASA [NAS5-26555, NNX13AC26G, NNX13AC63G, NNX13AE99G, NNH13CH61C]; National Science Foundation [AST-1008882]; NSF grant [AST-1412693]; NSF CAREER grant [AST-1253702]; NSF Fellowship [AST-1302093]; NSERC; NWO, the Netherlands Organization for Scientific Research; UC Center for Galaxy Evolution; NSF [AST-1009756, AST-1412315]; Fondecyt grant [1120328]; NSF graduate fellowship; UCSB Dean's Fellowship; CNPq; National Council for Scientific and Technological Development (Brazil); Packard Foundation in the form of a Packard Research Fellowship; Danish National Research Foundation; Danish Council for Independent Research [DFF 4002-00275]; National Aeronautics and Space Administration FX Support for HST program number GO-13330 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. R.E. gratefully acknowledges support from NASA under awards NNX13AC26G, NNX13AC63G, and NNX13AE99G. J.M.G. gratefully acknowledges support from NASA under award NNH13CH61C. B.M.P., G.D.R., C.J.G., M.M.F., and R.W.P. are grateful for the support of the National Science Foundation through grant AST-1008882 to The Ohio State University. A.J.B. and L.P. have been supported by NSF grant AST-1412693. M.C.B. gratefully acknowledges support through NSF CAREER grant AST-1253702 to Georgia State University. K.D.D. is supported by an NSF Fellowship awarded under grant AST-1302093. P.B.H. is supported by NSERC. SRON is financially supported by NWO, the Netherlands Organization for Scientific Research. B.C.K. is partially supported by the UC Center for Galaxy Evolution. C.S.K. acknowledges the support of NSF grant AST-1009756. P.L. acknowledges support from Fondecyt grant #1120328. A.P. acknowledges support from a NSF graduate fellowship and a UCSB Dean's Fellowship. J.S.S. acknowledges CNPq, National Council for Scientific and Technological Development (Brazil) for the partial support and The Ohio State University for warm hospitality. T.T. has been supported by NSF grant AST-1412315. T.T. and B.C.K. acknowledge support from the Packard Foundation in the form of a Packard Research Fellowship to T.T. T.T. thanks the American Academy in Rome and the Observatory of Monteporzio Catone for kind hospitality. The Dark Cosmology Centre is funded by the Danish National Research Foundation. M.V. gratefully acknowledges support from the Danish Council for Independent Research via grant No. DFF 4002-00275. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 65 TC 36 Z9 36 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 129 DI 10.1088/0004-637X/806/1/129 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300129 ER PT J AU Gopalswamy, N Makela, P Akiyama, S Yashiro, S Xie, H Thakur, N Kahler, SW AF Gopalswamy, N. Maekelae, P. Akiyama, S. Yashiro, S. Xie, H. Thakur, N. Kahler, S. W. TI LARGE SOLAR ENERGETIC PARTICLE EVENTS ASSOCIATED WITH FILAMENT ERUPTIONS OUTSIDE ACTIVE REGIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE shock waves; Sun: coronal mass ejections (CMEs); Sun: filaments, prominences; Sun: flares; Sun: particle emission; Sun: radio radiation ID CORONAL MASS EJECTIONS; SHOCK FORMATION; SOHO MISSION; CYCLE 24; RADIO; SPACE; WAVES; ACCELERATION; SPECTRA; BURSTS AB We report on four large filament eruptions (FEs) from solar cycles 23 and 24 that were associated with large solar energetic particle (SEP) events and interplanetary type II radio bursts. The post-eruption arcades corresponded mostly to C-class soft X-ray enhancements, but an M1.0 flare was associated with one event. However, the associated coronal mass ejections (CMEs) were fast (speeds similar to 1000 km s(-1)) and appeared as halo CMEs in the coronagraph field of view. The interplanetary type II radio bursts occurred over a wide wavelength range, indicating the existence of strong shocks throughout the inner heliosphere. No metric type II bursts were present in three events, indicating that the shocks formed beyond 2-3 Rs. In one case, there was a metric type II burst with low starting frequency, indicating a shock formation height of similar to 2 Rs. The FE-associated SEP events did have softer spectra (spectral index >4) in the 10-100 MeV range, but there were other low-intensity SEP events with spectral indices >= 4. Some of these events are likely FE-SEP events, but were not classified as such in the literature because they occurred close to active regions. Some were definitely associated with large active region flares, but the shock formation height was large. We definitely find a diminished role for flares and complex type III burst durations in these large SEP events. Fast CMEs and shock formation at larger distances from the Sun seem to be the primary characteristics of the FE-associated SEP events. C1 [Gopalswamy, N.; Maekelae, P.; Akiyama, S.; Yashiro, S.; Xie, H.; Thakur, N.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Maekelae, P.; Akiyama, S.; Yashiro, S.; Xie, H.; Thakur, N.] Catholic Univ Amer, Washington, DC 20064 USA. [Kahler, S. W.] Air Force Res Lab, Albuquerque, NM 87117 USA. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. EM nat.gopalswamy@nasa.gov FU NASA/LWS program; NSF [AGS-1358274]; NASA [NNX15AB77G, NNX15AB70G] FX We thank the Big Bear Solar Observatory and the Hida Observatory for making their H-alpha data available on line. We thank NOAA/NGDC for making the GOES proton data available. This work benefitted greatly from the open data policy of NASA. STEREO is a mission in NASA's Solar Terrestrial Probes program. SOHO is a project of international collaboration between ESA and NASA. The work of N.G., S.Y., S.A., and N.T. was supported by NASA/LWS program. P. M. was partially supported by NSF grant AGS-1358274 and NASA grant NNX15AB77G. H.X. was partially supported by NASA grant NNX15AB70G. NR 45 TC 15 Z9 15 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 JUN 10 PY 2015 VL 806 IS 1 AR 8 DI 10.1088/0004-637X/806/1/8 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300008 ER PT J AU Huffenberger, KM Araujo, D Bischoff, C Buder, I Chinone, Y Cleary, K Kusaka, A Monsalve, R Naess, SK Newburgh, LB Reeves, R Ruud, TM Wehus, IK Zwart, JTL Dickinson, C Eriksen, HK Gaier, T Gundersen, JO Hasegawa, M Hazumi, M Miller, AD Radford, SJE Readhead, ACS Staggs, ST Tajima, O Thompson, KL AF Huffenberger, K. M. Araujo, D. Bischoff, C. Buder, I. Chinone, Y. Cleary, K. Kusaka, A. Monsalve, R. Naess, S. K. Newburgh, L. B. Reeves, R. Ruud, T. M. Wehus, I. K. Zwart, J. T. L. Dickinson, C. Eriksen, H. K. Gaier, T. Gundersen, J. O. Hasegawa, M. Hazumi, M. Miller, A. D. Radford, S. J. E. Readhead, A. C. S. Staggs, S. T. Tajima, O. Thompson, K. L. CA QUIET Collaboration TI THE Q/U IMAGING EXPERIMENT: POLARIZATION MEASUREMENTS OF RADIO SOURCES AT 43 AND 95 GHz SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; galaxies: active; galaxies: individual (Cen A, Pict A); methods: statistical; polarization ID ACTIVE GALACTIC NUCLEI; MICROWAVE BACKGROUND POLARIZATION; PROBE WMAP OBSERVATIONS; SCALE ROTATION MEASURES; HIGH-FREQUENCY; POINT SOURCES; EXTRAGALACTIC SOURCES; SOURCE CATALOG; FARADAYS FOG; BRIGHT AB We present polarization measurements of extragalactic radio sources observed during the cosmic microwave background polarization survey of the Q/U Imaging Experiment (QUIET), operating at 43 GHz (Q-band) and 95GHz (W-band). We examine sources selected at 20 GHz from the public, >40 mJy catalog of the Australia Telescope (AT20G) survey. There are similar to 480 such sources within QUIET's four low-foreground survey patches, including the nearby radio galaxies Centaurus A and Pictor A. The median error on our polarized flux density measurements is 30-40 mJy per Stokes parameter. At signal-to-noise ratio >3 significance, we detect linear polarization for seven sources in Q-band and six in W-band; only 1.3 +/- 1.1 detections per frequency band are expected by chance. For sources without a detection of polarized emission, we find that half of the sources have polarization amplitudes below 90 mJy (Q-band) and 106 mJy (W-band), at 95% confidence. Finally, we compare our polarization measurements to intensity and polarization measurements of the same sources from the literature. For the four sources with WMAP and Planck intensity measurements >1 Jy, the polarization fractions are above 1% in both QUIET bands. At high significance, we compute polarization fractions as much as 10%-20% for some sources, but the effects of source variability may cut that level in half for contemporaneous comparisons. Our results indicate that simple models-ones that scale a fixed polarization fraction with frequency-are inadequate to model the behavior of these sources and their contributions to polarization maps. C1 [Huffenberger, K. M.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Huffenberger, K. M.; Gundersen, J. O.] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA. [Araujo, D.; Zwart, J. T. L.; Miller, A. D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Araujo, D.; Zwart, J. T. L.; Miller, A. D.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Buder, I.; Tajima, O.] Univ Chicago, Kavli Inst Cosmol Phys, Dept Phys, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bischoff, C.; Buder, I.; Tajima, O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bischoff, C.; Buder, I.] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki 3050801, Japan. [Chinone, Y.; Hasegawa, M.; Hazumi, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Chinone, Y.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Kusaka, A.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Kusaka, A.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Kusaka, A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Monsalve, R.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. [Naess, S. K.; Ruud, T. M.; Eriksen, H. K.] Univ Toronto, Dunlap Inst, Toronto, ON M5S 3H4, Canada. [Newburgh, L. B.] Univ Concepcion, Dept Astron, CePIA, Concepcion, Chile. [Reeves, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wehus, I. K.; Gaier, T.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. [Zwart, J. T. L.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Dickinson, C.] Univ Oslo, Ctr Math Applicat, NO-0316 Oslo, Norway. [Thompson, K. L.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Thompson, K. L.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. RP Huffenberger, KM (reprint author), Florida State Univ, Dept Phys, POB 3064350, Tallahassee, FL 32306 USA. EM huffenbe@physics.fsu.edu OI radford, simon/0000-0001-9113-1660; Huffenberger, Kevin/0000-0001-7109-0099; Bischoff, Colin/0000-0001-9185-6514; Zwart, Jonathan/0000-0002-4967-946X FU NSF [AST-0506648, PHY-0855887, PHY-0355328, AST-0448909, AST-1010016, PHY-0551142]; KAKENHI [20244041, 20740158, 21111002]; PRODEX [C90284]; KIPAC Enterprise grant; Strategic Alliance for the Implementation of New Technologies (SAINT); Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; Fermilab; Kavli Institute for Cosmological Physics; University of Chicago; JPL RTD program; ERC [307209] FX Bruce Winstein, who led the QUIET project, died in 2011, soon after observations concluded. The project's success owes a great debt to his intellectual and scientific leadership. Support for the QUIET instrument and operation was provided through the NSF cooperative agreement AST-0506648. Support was also provided by NSF awards PHY-0855887, PHY-0355328, AST-0448909, AST-1010016, and PHY-0551142; KAKENHI 20244041, 20740158, and 21111002; PRODEX C90284; a KIPAC Enterprise grant; and by the Strategic Alliance for the Implementation of New Technologies (SAINT). This research used resources of the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231.; Some work was performed on the Joint Fermilab-KICP Supercomputing Cluster, supported by grants from Fermilab, the Kavli Institute for Cosmological Physics, and the University of Chicago. Some work was performed on the Abel Cluster, owned and maintained by the University of Oslo and NOTUR (the Norwegian High Performance Computing Consortium), and on the Central Computing System, owned and operated by the Computing Research Center at KEK. Portions of this work were performed at the Jet Propulsion Laboratory (JPL) and California Institute of Technology, operating under a contract with the National Aeronautics and Space Administration. The Q-band modules were developed using funding from the JPL R&TD program. We acknowledge the Northrop Grumman Corporation for collaboration in the development and fabrication of HEMT-based cryogenic temperature-compatible MMICs.; C.D. acknowledges an STFC Advanced Fellowship, an EU Marie-Curie IRG grant under the FP7 and an ERC Starting Grant (No. 307209). H. K. E. acknowledges an ERC Starting Grant under FP7. A. D. M. acknowledges a Sloan foundation fellowship. J. Z. gratefully acknowledges a South Africa National Research Foundation Square Kilometre Array Research Fellowship. NR 72 TC 1 Z9 1 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 112 DI 10.1088/0004-637X/806/1/112 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300112 ER PT J AU Johnson, TJ Ray, PS Roy, J Cheung, CC Harding, AK Pletsch, HJ Fort, S Camilo, F Deneva, J Bhattacharyya, B Stappers, BW Kerr, M AF Johnson, T. J. Ray, P. S. Roy, J. Cheung, C. C. Harding, A. K. Pletsch, H. J. Fort, S. Camilo, F. Deneva, J. Bhattacharyya, B. Stappers, B. W. Kerr, M. TI DISCOVERY OF GAMMA-RAY PULSATIONS FROM THE TRANSITIONAL REDBACK PSR J1227-4853 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: individual (J1227-4853); binaries: eclipsing; gamma rays: stars ID LARGE-AREA TELESCOPE; BINARY MILLISECOND PULSAR; HIGH-ENERGY EMISSION; BLACK-WIDOW PULSARS; X-RAY; XSS J12270-4859; LIGHT CURVES; NEUTRON-STARS; STATE CHANGE; SLOT GAPS AB The 1.69 ms spin period of PSR J1227-4853 was recently discovered in radio observations of the low-mass X-ray binary XSS J12270-4859 following the announcement of a possible transition to a rotation-powered millisecond pulsar state, inferred from decreases in optical, X-ray, and gamma-ray flux from the source. We report the detection of significant (5s) gamma-ray pulsations after the transition, at the known spin period, using similar to 1 year of data from the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope. The gamma-ray light curve of PSR J1227-4853 can be fit by one broad peak, which occurs at nearly the same phase as the main peak in the 1.4 GHz radio profile. The partial alignment of light-curve peaks in different wavebands suggests that at least some of the radio emission may originate at high altitude in the pulsar magnetosphere, in extended regions co-located with the gamma-ray emission site. We folded the LAT data at the orbital period, both pre- and post-transition, but find no evidence for significant modulation of the gamma-ray flux. Analysis of the gamma-ray flux over the mission suggests an approximate transition time of 2012 November 30. Continued study of the pulsed emission and monitoring of PSR J1227-4853, and other known redback systems, for subsequent flux changes will increase our knowledge of the pulsar emission mechanism and transitioning systems. C1 [Johnson, T. J.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Ray, P. S.; Cheung, C. C.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Roy, J.; Bhattacharyya, B.; Stappers, B. W.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Roy, J.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Harding, A. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pletsch, H. J.; Fort, S.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. [Pletsch, H. J.; Fort, S.] Leibniz Univ Hannover, D-30167 Hannover, Germany. [Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Deneva, J.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Kerr, M.] CSIRO, Australia Telescope Natl Facil, Astron & Space Sci, Epping, NSW 1710, Australia. [Deneva, J.] Naval Res Lab, Washington, DC 20375 USA. RP Johnson, TJ (reprint author), George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. EM tyrel.j.johnson@gmail.com; Paul.Ray@nrl.navy.mil; jayanta.roy@manchester.ac.uk OI Ray, Paul/0000-0002-5297-5278 FU Commonwealth Government; NASA [DPR S-15633 Y] FX The Parkes radio telescope is part of the Australia Telescope which is funded by the Commonwealth Government for operation as a National Facility managed by CSIRO.; Portions of this research performed at the Naval Research Laboratory are sponsored by NASA DPR S-15633 Y. NR 63 TC 6 Z9 6 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 91 DI 10.1088/0004-637X/806/1/91 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300091 ER PT J AU Jun, HD Im, M Lee, HM Ohyama, Y Woo, JH Fan, XH Goto, T Kim, D Kim, JH Kim, M Lee, MG Nakagawa, T Pearson, C Serjeant, S AF Jun, Hyunsung David Im, Myungshin Lee, Hyung Mok Ohyama, Youichi Woo, Jong-Hak Fan, Xiaohui Goto, Tomotsugu Kim, Dohyeong Kim, Ji Hoon Kim, Minjin Lee, Myung Gyoon Nakagawa, Takao Pearson, Chris Serjeant, Stephen TI REST-FRAME OPTICAL SPECTRA AND BLACK HOLE MASSES OF 3 < z < 6 QUASARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; quasars: emission lines; quasars: supermassive black holes ID DIGITAL-SKY-SURVEY; ACTIVE GALACTIC NUCLEI; NEAR-INFRARED SPECTROSCOPY; HIGH-REDSHIFT QUASARS; EMISSION-LINE PROPERTIES; WIDE-FIELD CAMERA; LUMINOSITY FUNCTION; DATA RELEASE; Z-GREATER-THAN-5.7 QUASARS; ADDITIONAL QUASARS AB We present the rest-frame optical spectral properties of 155 luminous quasars at 3.3 < z < 6.4 taken with the AKARI space telescope, including the first detection of the Ha emission line as far out as z similar to 6. We extend the scaling relation between the rest-frame optical continuum and the line luminosity of active galactic nuclei (AGNs) to the high-luminosity, high-redshift regime that has rarely been probed before. Remarkably, we find that a single log-linear relation can be applied to the 5100 angstrom and H alpha AGN luminosities over a wide range of luminosity (10(42) < L-5100 < 10(47) ergs s(-1)) or redshift (0 < z < 6), suggesting that the physical mechanism governing this relation is unchanged from z = 0 to. 6, over five decades in luminosity. Similar scaling relations are found between the optical and the UV continuum luminosities or line widths. Applying the scaling relations to the H beta black hole (BH) mass (MBH) estimator of local AGNs, we derive the MBH estimators based on the H alpha, Mg (II), and C (IV) lines, finding that the UV-line-based masses are overall consistent with the Balmer-line-based, but with a large intrinsic scatter of 0.40 dex for the C (IV) estimates. Our 43 MBH estimates from Ha confirm the existence of BHs as massive as similar to 10(10) M-circle dot out to z similar to 5. and provide a secure footing for previous results from Mg (II)-line-based studies that a rapid MBH growth has occurred in the early universe. C1 [Jun, Hyunsung David] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Jun, Hyunsung David; Im, Myungshin; Kim, Dohyeong; Kim, Ji Hoon] Seoul Natl Univ, Dept Phys & Astron, Astron Program, CEOU, Seoul 151742, South Korea. [Im, Myungshin; Lee, Hyung Mok; Woo, Jong-Hak; Kim, Dohyeong; Lee, Myung Gyoon] Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul 151742, South Korea. [Ohyama, Youichi] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Fan, Xiaohui] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Goto, Tomotsugu] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. [Goto, Tomotsugu] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. [Kim, Ji Hoon] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Kim, Minjin] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Kim, Minjin] Univ Sci & Technol, Taejon 305350, South Korea. [Nakagawa, Takao] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan. [Pearson, Chris; Serjeant, Stephen] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Pearson, Chris] CCLRC Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England. [Pearson, Chris] Univ Oxford, Oxford Astrophys, Oxford OX1 3RH, England. RP Im, M (reprint author), Seoul Natl Univ, Dept Phys & Astron, Astron Program, CEOU, Seoul 151742, South Korea. EM hyunsung.jun@jpl.nasa.gov; mim@astro.snu.ac.kr RI Kim, Ji Hoon/A-8989-2009; OI Kim, Ji Hoon/0000-0002-1418-3309; Im, Myungshin/0000-0002-8537-6714 FU NASA Postdoctoral Program at the Jet Propulsion Laboratory; NASA; National Research Foundation of Korea (NRF) [2008-0060544, 2012R1A2A2A01006087, 2012R1A4A1028713]; NRF-2014-Fostering Core Leaders of Future Program - Korea government (MSIP) [2014-009728]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; 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; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University; National Aeronautics and Space Administration; [MOST100-2112-M-001-001-MY3] FX We thank Todd Boroson, Jenny Greene, Lisa Storrie-Lombardi, Celine Peroux, and Donald Schneider for kindly providing the iron template derived from I Zw 1, the rest-frame optical luminosities and line widths of local AGNs, and the optical spectra of APM-UKST quasars and Q0000-26. Also, we thank Eduardo Banados, Hyunjin Shim, and Doosoo Yoon for useful communication. This research was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. This work was supported by the National Research Foundation of Korea (NRF) grant. No. 2008-0060544 (H.D.J. and M.I.), 2012R1A2A2A01006087 (J.H.W), 2012R1A4A1028713 (H.M.L. and M.G.L.), and NRF-2014-Fostering Core Leaders of Future Program, No. 2014-009728 (D.K.), funded by the Korea government (MSIP). This work was supported by grant MOST100-2112-M-001-001-MY3 (Y.O.).; This research is based on observations with AKARI, a JAXA project with the participation of ESA. 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 publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This publication makes use of data products from the United Kingdom Infrared Deep Sky Survey. The UKIDSS project is defined in Lawrence et al. (2007). UKIDSS uses the UKIRT Wide Field Camera (WFCAM; Casali et al. 2007). The photometric system is described in Hewett et al. (2006), and the calibration is described in Hodgkin et al. (2009). The pipeline processing and science archive are described in M.J. Irwin et al. (2009, in preparation) and Hambly et al. (2008). This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. NR 134 TC 12 Z9 12 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 109 DI 10.1088/0004-637X/806/1/109 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300109 ER PT J AU Kastner, JH Qi, CH Gorti, U Hily-Blant, P Oberg, K Forveille, T Andrews, S Wilner, D AF Kastner, Joel H. Qi, Chunhua Gorti, Uma Hily-Blant, Pierre Oberg, Karin Forveille, Thierry Andrews, Sean Wilner, David TI A RING OF C2H IN THE MOLECULAR DISK ORBITING TW Hya SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; protoplanetary disks; stars: individual (TW Hya); stars: pre-main sequence ID PROTOPLANETARY DISKS; SUBMILLIMETER ARRAY; HYDRAE; LINE; CHEMISTRY; CO; EXCITATION; ACCRETION AB We have used the Submillimeter Array to image, at similar to 1.'' 5 resolution, C2H N = 3 -> 2 emission from the circumstellar disk orbiting the nearby (D = 54 pc), similar to 8 Myr-old, similar to 0.8 M-circle dot classical T Tauri star TW Hya. The SMA imaging reveals that the C2H emission exhibits a ring-like morphology. Based on a model in which the C2H column density follows a truncated radial power-law distribution, we find that the inner edge of the ring lies at similar to 45 AU, and that the ring extends to at least similar to 120 AU. Comparison with previous (single-dish) observations of C2H N = 4 -> 3 emission indicates that the C2H molecules are subthermally excited and, hence, that the emission arises from the relatively warm (T greater than or similar to 40 K), tenuous (n << 10(7) cm(-3)) upper atmosphere of the disk. Based on these results and comparisons of the SMA C2H map with previous submillimeter and scattered-light imaging, we propose that the C2H emission most likely traces particularly efficient photo-destruction of small grains and/or photodesorption and photodissociation of hydrocarbons derived from grain ice mantles in the surface layers of the outer disk. The presence of a C2H ring in the TW Hya disk hence likely serves as a marker of dust grain processing and radial and vertical grain size segregation within the disk. C1 [Kastner, Joel H.] Rochester Inst Technol, Sch Phys & Astron, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. [Kastner, Joel H.] Rochester Inst Technol, Lab Multiwavelength Astrophys, Rochester, NY 14623 USA. [Qi, Chunhua; Oberg, Karin; Andrews, Sean; Wilner, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gorti, Uma] SETI Inst, Mountain View, CA 94043 USA. [Gorti, Uma] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hily-Blant, Pierre; Forveille, Thierry] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. [Hily-Blant, Pierre; Forveille, Thierry] CNRS, IPAG, F-38000 Grenoble, France. [Hily-Blant, Pierre] Inst Univ France, F-38000 Grenoble, France. RP Kastner, JH (reprint author), Rochester Inst Technol, Sch Phys & Astron, Chester F Carlson Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14623 USA. EM jhk@cis.rit.edu OI Kastner, Joel/0000-0002-3138-8250 FU Smithsonian Institution; Academia Sinica; National Science Foundation [AST-1108950]; NASA Origins of Solar Systems grant [NNX11AK63] FX The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. We gratefully acknowledge Alexander Faure for providing electron impact rates for C2H, and we thank the anonymous referee for helpful comments and suggestions. This research is supported by National Science Foundation grant AST-1108950 to RIT and NASA Origins of Solar Systems grant NNX11AK63 to SAO. NR 34 TC 9 Z9 9 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 JUN 10 PY 2015 VL 806 IS 1 AR 75 DI 10.1088/0004-637X/806/1/75 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300075 ER PT J AU Lehmer, BD Tyler, JB Hornschemeier, AE Wik, DR Yukita, M Antoniou, V Boggs, S Christensen, FE Craig, WW Hailey, CJ Harrison, FA Maccarone, TJ Ptak, A Stern, D Zezas, A Zhang, WW AF Lehmer, B. D. Tyler, J. B. Hornschemeier, A. E. Wik, D. R. Yukita, M. Antoniou, V. Boggs, S. Christensen, F. E. Craig, W. W. Hailey, C. J. Harrison, F. A. Maccarone, T. J. Ptak, A. Stern, D. Zezas, A. Zhang, W. W. TI THE 0.3-30 keV SPECTRA OF POWERFUL STARBURST GALAXIES: NuSTAR AND CHANDRA OBSERVATIONS OF NGC 3256 AND NGC 3310 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 3256 and NGC 3310); galaxies: starburst; galaxies: star formation; X-rays: galaxies ID X-RAY-EMISSION; STAR-FORMING GALAXIES; LUMINOUS INFRARED GALAXIES; XMM-NEWTON OBSERVATIONS; INITIAL MASS FUNCTION; MERGER NGC-3256; FORMATION HISTORY; CLUSTER FORMATION; SPIRAL GALAXIES; LOW-METALLICITY AB We present nearly simultaneous Chandra and NuSTAR observations of two actively star-forming galaxies within 50 Mpc: NGC 3256 and NGC 3310. Both galaxies are significantly detected by both Chandra and NuSTAR, which together provide the first-ever spectra of these two galaxies spanning 0.3-30 keV. The X-ray emission from both galaxies is spatially resolved by Chandra; we find that hot gas dominates the E < 1-3 keV emission while ultraluminous X-ray sources (ULXs) provide majority contributions to the emission at E > 1-3 keV. The NuSTAR galaxy-wide spectra of both galaxies follow steep power-law distributions with Gamma approximate to 2.6 at E > 5-7 keV. Using new and archival Chandra data, we search for signatures of heavily obscured or low luminosity active galactic nuclei (AGNs). We find that both NGC 3256 and NGC 3310 have X-ray detected sources coincident with nuclear regions; however, the steep NuSTAR spectra of both galaxies restricts these sources to be either low luminosity AGNs (L2-10 keV/L-Edd less than or similar to 10(-5)) or non-AGNs in nature (e.g., ULXs or crowded X-ray sources that reach L2-10 keV similar to 10(40) erg s(-1) cannot be ruled out). Combining our constraints on the 0.3-30 keV spectra of NGC 3256 and NGC 3310 with equivalent measurements for nearby star-forming galaxies M83 and NGC 253, we analyze the star formation rate (SFR) normalized spectra of these starburst galaxies. The spectra of all four galaxies show sharply declining power-law slopes at energies above 3-6 keV primarily due to ULX populations. Our observations therefore constrain the average spectral shape of galaxy-wide populations of luminous accreting binaries (i.e., ULXs). Interestingly, despite a completely different galaxy sample selection, emphasizing here a range of SFRs and stellar masses, these properties are similar to those of super-Eddington accreting ULXs that have been studied individually in a targeted NuSTAR ULX program. We also find that NGC 3310 exhibits a factor of approximate to 3-10 elevation of X-ray emission over the other star-forming galaxies due to a corresponding overabundance of ULXs. We argue that the excess of ULXs in NGC 3310 is most likely explained by the relatively low metallicity of the young stellar population in this galaxy, a property that is expected to produce an excess of luminous X-ray binaries for a given SFR. C1 [Lehmer, B. D.; Wik, D. R.; Yukita, M.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Lehmer, B. D.; Tyler, J. B.; Hornschemeier, A. E.; Wik, D. R.; Yukita, M.; Ptak, A.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tyler, J. B.] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Antoniou, V.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Boggs, S.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94720 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Harrison, F. A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Maccarone, T. J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zezas, A.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece. [Zezas, A.] Univ Crete, Inst Theoret & Computat Phys, Iraklion 71003, Crete, Greece. [Zezas, A.] Fdn Res & Technol Hellas, Iraklion 71110, Crete, Greece. RP Lehmer, BD (reprint author), Johns Hopkins Univ, Homewood Campus, Baltimore, MD 21218 USA. RI Boggs, Steven/E-4170-2015; Yukita, Mihoko/E-4135-2017; Zezas, Andreas/C-7543-2011; Antoniou, Vallia/E-3837-2013 OI Boggs, Steven/0000-0001-9567-4224; Zezas, Andreas/0000-0001-8952-676X; Antoniou, Vallia/0000-0001-7539-1593 FU Chandra X-ray Center grant [GO4-15086 Z]; NASA ADAP grant [NNX13AI48G]; European Research Council under the European Union's Seventh Framework Programme (FP)/ERC Grant [617001]; NASA [NNG08FD60C]; National Aeronautics and Space Administration FX We thank the anonymous referee for helpful comments, which have improved the quality of this paper. We gratefully acknowledge financial support from Chandra X-ray Center grant GO4-15086 Z (B.D.L., J.B.T.) and NASA ADAP grant NNX13AI48G (B.D.L.). A. Z. acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement n. 617001. 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. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (Italy) and the California Institute of Technology (USA). NR 88 TC 3 Z9 3 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 126 DI 10.1088/0004-637X/806/1/126 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300126 ER PT J AU Makela, P Gopalswamy, N Akiyama, S Xie, H Yashiro, S AF Maekelae, P. Gopalswamy, N. Akiyama, S. Xie, H. Yashiro, S. TI ESTIMATING THE HEIGHT OF CMEs ASSOCIATED WITH A MAJOR SEP EVENT AT THE ONSET OF THE METRIC TYPE II RADIO BURST DURING SOLAR CYCLES 23 AND 24 SO ASTROPHYSICAL JOURNAL LA English DT Article DE shock waves; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: radio radiation ID CORONAL MASS EJECTIONS; ENERGETIC PARTICLE EVENTS; MAGNETIC RECONNECTION; OUTER CORONA; SHOCK-WAVES; LARGE-ANGLE; EXPANSION; EMISSION; ERUPTION; FLARES AB We studied the coronal mass ejection (CME) height at the onset of 59 metric type II radio bursts associated with major solar energetic particle (SEP) events, excluding ground level enhancements (GLEs), during solar cycles 23 and 24. We calculated CME heights using a simple flare-onset method used by Gopalswamy et al. to estimate CME heights at the metric type II onset for cycle 23 GLEs. We found the mean CME height for non-GLE events (1.72 R-circle dot) to be similar to 12% greater than that (1.53 R-circle dot) for cycle 23 GLEs. The difference could be caused by more impulsive acceleration of the GLE-associated CMEs. For cycle 24 non-GLE events, we compared the CME heights obtained using the flare-onset method and the three-dimensional spherical-shock fitting method and found the correlation to be good (CC = 0.68). We found the mean CME height for cycle 23 non-GLE events (1.79 R-circle dot) to be greater than that for cycle 24 non-GLE events (1.58 R-circle dot), but statistical tests do not definitely reject the possibility of coincidence. We suggest that the lower formation height of the shocks during cycle 24 indicates a change in the Alfven speed profile because solar magnetic fields are weaker and plasma density levels are closer to the surface than usual during cycle 24. We also found that complex type III bursts showing diminution of type III emission in the 7-14 MHz frequency range are more likely associated with events with a CME height at the type II onset above 2 R-circle dot, supporting suggestions that the CME/shock structure causes the feature. C1 [Maekelae, P.; Akiyama, S.; Xie, H.; Yashiro, S.] Catholic Univ Amer, Washington, DC 20064 USA. [Maekelae, P.; Gopalswamy, N.; Akiyama, S.; Xie, H.; Yashiro, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Makela, P (reprint author), Catholic Univ Amer, Washington, DC 20064 USA. EM pertti.makela@nasa.gov OI Gopalswamy, Nat/0000-0001-5894-9954 FU NASA [NNX10AL50A, NNG11PL10A] FX We thank the Wind/WAVES, SDO/AIA, and STEREO/SECCHI teams for providing data. This research was done as part of the LWS Focused Science Topic, "SEP Variability" supported by NASA grants NNX10AL50A and NNG11PL10A. SOHO is a project of international cooperation between ESA and NASA. The authors thank the anonymous referee for helpful comments. NR 61 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 13 DI 10.1088/0004-637X/806/1/13 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300013 ER PT J AU McCauliff, SD Jenkins, JM Catanzarite, J Burke, CJ Coughlin, JL Twicken, JD Tenenbaum, P Seader, S Li, J Cote, M AF McCauliff, Sean D. Jenkins, Jon M. Catanzarite, Joseph Burke, Christopher J. Coughlin, Jeffrey L. Twicken, Joseph D. Tenenbaum, Peter Seader, Shawn Li, Jie Cote, Miles TI AUTOMATIC CLASSIFICATION OF KEPLER PLANETARY TRANSIT CANDIDATES SO ASTROPHYSICAL JOURNAL LA English DT Article DE astronomical databases: miscellaneous; binaries: eclipsing; catalogs; methods: statistical; planets and satellites: detection; techniques: photometric ID ERROR-CORRECTION; FALSE POSITIVES; VARIABLE-STARS; LIGHT CURVES; IDENTIFICATION; MISSION AB In the first three years of operation, the Kepler mission found 3697 planet candidates (PCs) from a set of 18,406 transit-like features detected on more than 200,000 distinct stars. Vetting candidate signals manually by inspecting light curves and other diagnostic information is a labor intensive effort. Additionally, this classification methodology does not yield any information about the quality of PCs; all candidates are as credible as any other. The torrent of exoplanet discoveries will continue after Kepler, because a number of exoplanet surveys will have an even broader search area. This paper presents the application of machine-learning techniques to the classification of the exoplanet transit-like signals present in the Kepler light curve data. Transit-like detections are transformed into a uniform set of real-numbered attributes, the most important of which are described in this paper. Each of the known transit-like detections is assigned a class of PC; astrophysical false positive; or systematic, instrumental noise. We use a random forest algorithm to learn the mapping from attributes to classes on this training set. The random forest algorithm has been used previously to classify variable stars; this is the first time it has been used for exoplanet classification. We are able to achieve an overall error rate of 5.85% and an error rate for classifying exoplanets candidates of 2.81%. C1 [McCauliff, Sean D.] NASA, Ames Res Ctr, Wyle, Moffett Field, CA 94035 USA. [Jenkins, Jon M.; Cote, Miles] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Catanzarite, Joseph; Burke, Christopher J.; Coughlin, Jeffrey L.; Twicken, Joseph D.; Tenenbaum, Peter; Seader, Shawn; Li, Jie] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP McCauliff, SD (reprint author), NASA, Ames Res Ctr, Wyle, Moffett Field, CA 94035 USA. EM sean.d.mccauliff@nasa.gov FU NASA's Space Mission Directorate FX Kepler was competitively selected as NASA's 10th Discovery mission. We would like to thank Abhishek Jaiantilal for use of the randomforest-matlab code. This paper would not be possible without the work of the members of the Kepler TCE Review Team. Funding for the Kepler mission is provided by NASA's Space Mission Directorate. 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. NR 37 TC 8 Z9 8 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 6 DI 10.1088/0004-637X/806/1/6 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300006 ER PT J AU Merten, J Meneghetti, M Postman, M Umetsu, K Zitrin, A Medezinski, E Nonino, M Koekemoer, A Melchior, P Gruen, D Moustakas, LA Bartelmann, M Host, O Donahue, M Coe, D Molino, A Jouvel, S Monna, A Seitz, S Czakon, N Lemze, D Sayers, J Balestra, I Rosati, P Benitez, N Biviano, A Bouwens, R Bradley, L Broadhurst, T Carrasco, M Ford, H Grillo, C Infante, L Kelson, D Lahav, O Massey, R Moustakas, J Rasia, E Rhodes, J Vega, J Zheng, W AF Merten, J. Meneghetti, M. Postman, M. Umetsu, K. Zitrin, A. Medezinski, E. Nonino, M. Koekemoer, A. Melchior, P. Gruen, D. Moustakas, L. A. Bartelmann, M. Host, O. Donahue, M. Coe, D. Molino, A. Jouvel, S. Monna, A. Seitz, S. Czakon, N. Lemze, D. Sayers, J. Balestra, I. Rosati, P. Benitez, N. Biviano, A. Bouwens, R. Bradley, L. Broadhurst, T. Carrasco, M. Ford, H. Grillo, C. Infante, L. Kelson, D. Lahav, O. Massey, R. Moustakas, J. Rasia, E. Rhodes, J. Vega, J. Zheng, W. TI CLASH: THE CONCENTRATION-MASS RELATION OF GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: clusters: general; gravitational lensing: strong; gravitational lensing: weak ID HUBBLE-SPACE-TELESCOPE; WEAK-LENSING ANALYSIS; DARK-MATTER HALOES; OBSERVATIONS COSMOLOGICAL INTERPRETATION; ACT-CL J0102-4915; LINE-OF-SIGHT; X-RAY; LAMBDA-CDM; PHOTOMETRIC REDSHIFTS; RXC J2248.7-4431 AB We present a new determination of the concentration-mass (c-M) relation for galaxy clusters based on our comprehensive lensing analysis of 19 X-ray selected galaxy clusters from the Cluster Lensing and Supernova Survey with Hubble (CLASH). Our sample spans a redshift range between 0.19 and 0.89. We combine weak-lensing constraints from the Hubble Space Telescope (HST) and from ground-based wide-field data with strong lensing constraints from HST. The results are reconstructions of the surface-mass density for all CLASH clusters on multi-scale grids. Our derivation of Navarro-Frenk-White parameters yields virial masses between 0.53 x 10(15) M-circle dot/h and 1.76 x 10(15) M-circle dot/h and the halo concentrations are distributed around c(200c) similar to 3.7 with a 1 sigma significant negative slope with cluster mass. We find an excellent 4% agreement in the median ratio of our measured concentrations for each cluster and the respective expectation from numerical simulations after accounting for the CLASH selection function based on X-ray morphology. The simulations are analyzed in two dimensions to account for possible biases in the lensing reconstructions due to projection effects. The theoretical c-M relation from our X-ray selected set of simulated clusters and the c-M relation derived directly from the CLASH data agree at the 90% confidence level. C1 [Merten, J.; Meneghetti, M.; Moustakas, L. A.; Rhodes, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Merten, J.; Zitrin, A.; Sayers, J.; Rhodes, J.] CALTECH, Pasadena, CA 91125 USA. [Merten, J.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Meneghetti, M.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Meneghetti, M.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy. [Postman, M.; Koekemoer, A.; Coe, D.; Bradley, L.; Zheng, W.] Space Telescope Sci Inst, Baltimore, MD 21208 USA. [Umetsu, K.; Czakon, N.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Medezinski, E.; Lemze, D.; Ford, H.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Nonino, M.; Balestra, I.; Biviano, A.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy. [Melchior, P.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Melchior, P.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Gruen, D.; Monna, A.; Seitz, S.] Univ Munich, D-81679 Munich, Germany. [Gruen, D.; Monna, A.; Seitz, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Bartelmann, M.; Carrasco, M.] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Host, O.; Grillo, C.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Donahue, M.; Benitez, N.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Molino, A.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Jouvel, S.; Lahav, O.] CSIC, IEEC, Inst Ciencies Espai, E-08193 Bellaterra, Barcelona, Spain. [Jouvel, S.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Balestra, I.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Rosati, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy. [Bouwens, R.] Leiden Univ, Leiden Observ, NL-2333 Leiden, Netherlands. [Broadhurst, T.] Univ Basque Country, UPV EHU, Dept Theoret Phys & Hist Sci, E-48080 Bilbao, Spain. [Broadhurst, T.] Basque Fdn Sci, Ikerbasque, Santiago 48011, Chile. [Carrasco, M.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofs, Santiago 22, Chile. [Infante, L.] Pontificia Univ Catolica Chile, Ctr Astroingn, Dept Astron & Astrofis, Santiago, Chile. [Kelson, D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Massey, R.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Moustakas, J.] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. [Rasia, E.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Vega, J.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain. [Zitrin, A.; Vega, J.] Observ Paris, CNRS, LERMA, UMR 8112, F-75014 Paris, France. RP Merten, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM jmerten@caltech.edu RI Meneghetti, Massimo/O-8139-2015; OI Meneghetti, Massimo/0000-0003-1225-7084; Nonino, Mario/0000-0001-6342-9662; Balestra, Italo/0000-0001-9660-894X; Vega Ferrero, Jesus/0000-0003-2338-5567; rasia, elena/0000-0003-4175-002X; Umetsu, Keiichi/0000-0002-7196-4822; Biviano, Andrea/0000-0002-0857-0732; Moustakas, Leonidas/0000-0003-3030-2360; Koekemoer, Anton/0000-0002-6610-2048; Benitez, Narciso/0000-0002-0403-7455 FU People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme (FP7) under REA grant [627288]; ORAU; NASA; National Science Council of Taiwan [NSC100-2112-M-001-008-MY3]; Academia Sinica Career Development Award; NASA - STScI [HST-HF-51334.01 A]; Deutsche Forschungsgemeinschaft (DFG) [SFB Transregio 33]; DFG cluster of excellence "Origin and Structure of the universe"; Baden Wurttemberg Stiftung; DNRF; Norris Foundation CCAT Postdoctoral Fellowship; National Science Foundation [AST-1210973, SAO TM3-14008X]; NASA [NAS8-03060]; MIUR; [ASI/INAF I/023/12/0]; [INFN/PD51]; [NSF/AST1313447]; [NASA/NNX11AB07G] FX The research was in part carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. J. M. has received funding from the People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme (FP7/2007-2013) under REA grant agreement number 627288. M. M. thanks ORAU and NASA for supporting his research at JPL and acknowledges support from the contract ASI/INAF I/023/12/0, INFN/PD51, and the PRIN MIUR 20102011 "The dark universe and the cosmic evolution of baryons: from current surveys to Euclid." K. U. acknowledges support from the National Science Council of Taiwan (grant NSC100-2112-M-001-008-MY3) and from the Academia Sinica Career Development Award. Support for A.Z. is provided by NASA through Hubble Fellowship grant #HST-HF-51334.01 A awarded by STScI. D.G., S.S. and P.R. were supported by SFB Transregio 33 "The Dark universe" by the Deutsche Forschungsgemeinschaft (DFG) and the DFG cluster of excellence "Origin and Structure of the universe." This work was supported in part by contract research "Internationale Spitzenforschung II/2-6" of the Baden Wurttemberg Stiftung. The Dark Cosmology Centre is funded by the DNRF. J. S. was supported by NSF/AST1313447, NASA/NNX11AB07G, and the Norris Foundation CCAT Postdoctoral Fellowship. E.R. acknowledges support from the National Science Foundation AST-1210973, SAO TM3-14008X (issued under NASA Contract No. NAS8-03060) NR 154 TC 40 Z9 40 U1 2 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 4 DI 10.1088/0004-637X/806/1/4 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300004 ER PT J AU Moore, RL Sterling, AC Falconer, DA AF Moore, Ronald L. Sterling, Alphonse C. Falconer, David A. TI MAGNETIC UNTWISTING IN SOLAR JETS THAT GO INTO THE OUTER CORONA IN POLAR CORONAL HOLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun: activity; Sun: chromosphere; Sun: corona; Sun: magnetic fields ID X-RAY JETS; EXTREME-ULTRAVIOLET; ALFVENIC WAVES; II SPICULES; BLOWOUT JETS; HINODE; TELESCOPE; WIND; REGION; ENERGY AB We study 14 large solar jets observed in polar coronal holes. In EUV movies from the Solar Dynamics Observatory/Atmospheric Imaging Assembly (AIA), each jet appears similar to most X-ray jets and EUV jets that erupt in coronal holes; but each is exceptional in that it goes higher than most, so high that it is observed in the outer corona beyond 2.2 R-Sun in images from the Solar and Heliospheric Observatory/Large Angle Spectroscopic Coronagraph (LASCO)/C2 coronagraph. From AIA He II 304 angstrom movies and LASCO/C2 running-difference images of these high-reaching jets, we find: (1) the front of the jet transits the corona below 2.2 RSun at a speed typically several times the sound speed; (2) each jet displays an exceptionally large amount of spin as it erupts; (3) in the outer corona, most of the jets display measureable swaying and bending of a few degrees in amplitude; in three jets the swaying is discernibly oscillatory with a period of order 1 hr. These characteristics suggest that the driver in these jets is a magnetic-untwisting wave that is basically a large-amplitude (i.e., nonlinear) torsional Alfven wave that is put into the reconnected open field in the jet by interchange reconnection as the jet erupts. From the measured spinning and swaying, we estimate that the magnetic-untwisting wave loses most of its energy in the inner corona below 2.2 RSun. We point out that the torsional waves observed in Type-II spicules might dissipate in the corona in the same way as the magnetic-untwisting waves in our big jets, and thereby power much of the coronal heating in coronal holes. C1 [Moore, Ronald L.; Sterling, Alphonse C.; Falconer, David A.] Marshall Space Flight Ctr, Heliophys & Planetary Sci Off, Huntsville, AL 35812 USA. [Moore, Ronald L.; Falconer, David A.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. RP Moore, RL (reprint author), Marshall Space Flight Ctr, Heliophys & Planetary Sci Off, ZP13, Huntsville, AL 35812 USA. EM ron.moore@nasa.gov FU Heliophysics Division of NASA's Science Mission Directorate through the Living With a Star Targeted Research and Technology Program FX This work was funded by the Heliophysics Division of NASA's Science Mission Directorate through the Living With a Star Targeted Research and Technology Program. ACS benefited from discussions held at the International Space Science Institute's (ISSI; Bern, Switzerland) International Team on Solar Coronal Jets. NR 54 TC 7 Z9 7 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 11 DI 10.1088/0004-637X/806/1/11 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300011 ER PT J AU Petrosian, V Kitanidis, E Kocevski, D AF Petrosian, Vahe Kitanidis, Ellie Kocevski, Daniel TI COSMOLOGICAL EVOLUTION OF LONG GAMMA-RAY BURSTS AND THE STAR FORMATION RATE SO ASTROPHYSICAL JOURNAL LA English DT Article DE early universe; gamma-ray burst: general; methods: statistical; stars: formation ID OPTICAL LUMINOSITY EVOLUTION; REDSHIFT DISTRIBUTION; FORMATION HISTORY; TRUNCATED DATA; QUASARS; SELECTION; RADIO; PEAK; AFTERGLOWS; TESTS AB Gamma-ray bursts (GRBs), by virtue of their high luminosities, can be detected up to very high redshifts. and therefore can be excellent probes of the early universe. This task is hampered by the fact that most of their characteristics have a broad range,. so we first need to obtain an accurate description of the distribution of these characteristics. and,. especially, their cosmological evolution. We use a sample of about 200 Swift long GRBs with known redshifts to determine the evolution of the. luminosity, formation rate, and the general shape of the luminosity function (LF). In contrast to most other forward-fitting methods of treating this problem, we use the Efron-Petrosian methods, which allow a non-parametric determination of the above quantities. We find a relatively strong luminosity evolution, an LF that can be fitted to a broken power law, and an unusually high formation rate at low redshifts, a rate more than one order of magnitude higher than the star formation rate (SFR). On the other hand, our results seem to agree with the almost constant SFR in redshifts 1-3 and the decline above this redshift. C1 [Petrosian, Vahe] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Petrosian, Vahe] Stanford Univ, KIPAC, Stanford, CA 94305 USA. [Petrosian, Vahe] Stanford Univ, Dept Appl Phys, Stanford, CA 94305 USA. [Kitanidis, Ellie] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Kocevski, Daniel] NASA, Goddard Space Flight Ctr, College Pk, MD USA. RP Petrosian, V (reprint author), Stanford Univ, Dept Phys, Stanford, CA 94305 USA. OI Petrosian, Vahe'/0000-0002-2670-8942 FU Swift [NASA NNX12AE74G] FX This work was partially supported by Swift guest investigator grant NASA NNX12AE74G and is based on Ellie Kitanidis's senior honor thesis at Stanford University (see http://purl.stanford.edu/xp981bq5003). NR 53 TC 9 Z9 9 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 44 DI 10.1088/0004-637X/806/1/44 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300044 ER PT J AU Rangwala, N Maloney, PR Wilson, CD Glenn, J Kamenetzky, J Spinoglio, L AF Rangwala, Naseem Maloney, Philip R. Wilson, Christine D. Glenn, Jason Kamenetzky, Julia Spinoglio, Luigi TI MORPHOLOGY AND KINEMATICS OF WARM MOLECULAR GAS IN THE NUCLEAR REGION OF ARP 220 AS REVEALED BY ALMA SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: ISM; galaxies: kinematics and dynamics; techniques: interferometric ID HERSCHEL-SPIRE SPECTROSCOPY; STAR-FORMATION; INTERSTELLAR-MEDIUM; NGC 1068; LINE; CO; EMISSION; GALAXIES; ARP-220; SHOCKS AB We present Atacama Large Millimeter Array (ALMA) Cycle-0 observations of the CO J = 6-5 line in the advanced galaxy merger Arp 220. This line traces warm molecular gas, which dominates the total CO luminosity. The CO emission from the two nuclei is well resolved by the 0 ''.39x0 ''.22 beam and the exceptional sensitivity and spatial/spectral resolution reveal new complex features in the morphology and kinematics of the warm gas. The line profiles are asymmetric between the red and blue sides of the nuclear disks and the peak of the line emission is offset from the peak of the continuum emission in both nuclei by about 100 pc in the same direction. CO self-absorption is detected at the centers of both nuclei but it is much deeper in the eastern nucleus. We also clearly detect strong, highly redshifted CO absorption located near the southwest side of each nucleus. For the eastern nucleus, we reproduce the major line profile features with a simple kinematic model of a highly turbulent, rotating disk with a substantial line center optical depth and a large gradient in the excitation temperature. The red/blue asymmetries and line-to-continuum offset are likely produced by absorption of the blue (SW) sides of the two nuclei by blueshifted, foreground molecular gas; the mass of the absorber is comparable to the nuclear warm gas mass (similar to 10(8) M-circle dot). We measure an unusually high L-CO/L-FIR ratio in the eastern nucleus, suggesting there is an additional energy source, such as mechanical energy from shocks, present in this nucleus. C1 [Rangwala, Naseem; Maloney, Philip R.; Glenn, Jason; Kamenetzky, Julia] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80303 USA. [Rangwala, Naseem] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Wilson, Christine D.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Spinoglio, Luigi] INAF, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy. RP Rangwala, N (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, 1255 38th St, Boulder, CO 80303 USA. FU NASA ROSES grant [NNX13AL16G]; NASA grant [1487846, 1472566]; Natural Sciences and Engineering Research Council of Canada FX The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: ADS/JAO. ALMA2011.0.00403.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. We are very grateful to Adam Leroy for doing a custom reduction for our observations and providing very useful recommendations. We thank Kazushi Sakamoto for sharing his CO J = 3-2 data cube observed by the Submillimeter Array. The research of Naseem Rangwala is supported by NASA ROSES grant NNX13AL16G. The research of Philip R. Maloney is supported by NASA grant 1487846. The research of Christine D. Wilson (C.D.W.) is supported by grants from the Natural Sciences and Engineering Research Council of Canada. C.D.W. also thanks the European Southern Observatory and the National Radio Astronomy Observatory for visitor support. The research of Jason Glenn is supported by NASA grant 1472566. NR 33 TC 9 Z9 9 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 17 DI 10.1088/0004-637X/806/1/17 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300017 ER PT J AU Schnittman, JD Krolik, JH AF Schnittman, Jeremy D. Krolik, Julian H. TI EVOLUTION OF A BINARY BLACK HOLE WITH A RETROGRADE CIRCUMBINARY ACCRETION DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; gravitational waves ID ACTIVE GALACTIC NUCLEI; MERGER RATE; SUPERMASSIVE BINARY; RADIATION-PRESSURE; MASSIVE GALAXIES; OBSCURING TORI; CENTRAL CAVITY; GAS; SIMULATIONS; DUSTY AB We consider the evolution of a supermassive black hole binary (SMBHB) surrounded by a retrograde accretion disk. Assuming the disk is exactly in the binary plane and transfers energy and angular momentum to the binary via direct gas accretion, we calculate the time evolution of the binary's semimajor axis a and eccentricity e. Because the gas is predominantly transferred when the binary is at apocenter, we find the eccentricity grows rapidly while maintaining constant a (1+e). After accreting only a fraction of the secondary's mass, the eccentricity grows to nearly unity; from then on, gravitational wave (GW) emission dominates the evolution, preserving constant a (1-e). The high-eccentricity waveforms redistribute the peak GW power from the nHz to mu Hz bands, substantially affecting the signal that might be detected with pulsar timing arrays. We also estimate the torque coupling binaries of arbitrary eccentricity with obliquely aligned circumbinary disks. If the outer edge of the disk is not an extremely large multiple of the binary separation, retrograde accretion can drive the binary into the GW-dominated state before these torques align the binary with the angular momentum of the mass supply. C1 [Schnittman, Jeremy D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krolik, Julian H.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Schnittman, JD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. OI Krolik, Julian/0000-0002-2995-7717 FU National Science Foundation [AST-1028111]; NASA [ATP12-0139] FX This work was partially supported by National Science Foundation grant AST-1028111 and NASA grant ATP12-0139. We thank Cole Miller for helpful comments and discussion. We also thank the referee for leading us to pursue the properties of binary-circumbinary disk (counter) alignment much further than we had initially. NR 61 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 88 DI 10.1088/0004-637X/806/1/88 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300088 ER PT J AU Singer, LP Kasliwal, MM Cenko, SB Perley, DA Anderson, GE Anupama, GC Arcavi, I Bhalerao, V Bue, BD Cao, Y Connaughton, V Corsi, A Cucchiara, A Fender, RP Fox, DB Gehrels, N Goldstein, A Gorosabel, J Horesh, A Hurley, K Johansson, J Kann, DA Kouveliotou, C Huang, K Kulkarni, SR Masci, F Nugent, P Rau, A Rebbapragada, UD Staley, TD Svinkin, D Thone, CC Postigo, ADU Urata, Y Weinstein, A AF Singer, Leo P. Kasliwal, Mansi M. Cenko, S. Bradley Perley, Daniel A. Anderson, Gemma E. Anupama, G. C. Arcavi, Iair Bhalerao, Varun Bue, Brian D. Cao, Yi Connaughton, Valerie Corsi, Alessandra Cucchiara, Antonino Fender, Rob P. Fox, Derek B. Gehrels, Neil Goldstein, Adam Gorosabel, J. Horesh, Assaf Hurley, Kevin Johansson, Joel Kann, D. A. Kouveliotou, Chryssa Huang, Kuiyun Kulkarni, S. R. Masci, Frank Nugent, Peter Rau, Arne Rebbapragada, Umaa D. Staley, Tim D. Svinkin, Dmitry Thoene, C. C. Postigo, A. De Ugarte Urata, Yuji Weinstein, Alan TI THE NEEDLE IN THE 100 deg(2) HAYSTACK: UNCOVERING AFTERGLOWS OF FERMI GRBs. WITH THE PALOMAR TRANSIENT FACTORY SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: individual (GRB 130702A, GRB 140606B); gravitational waves; methods: observational; supernovae: general; surveys ID GAMMA-RAY BURST AB The Fermi Gamma-ray Space Telescope has greatly expanded the number and energy window of observations of gamma-ray bursts (GRBs). However, the coarse localizations of tens to a hundred square degrees provided by the Fermi GRB Monitor instrument have posed a formidable obstacle to locating the bursts' host galaxies, measuring their redshifts, and tracking their panchromatic afterglows. We have built a target-of-opportunity mode for the intermediate Palomar Transient Factory in order to perform targeted searches for Fermi afterglows. Here, we present the results of one year of this program: 8 afterglow discoveries out of 35 searches. Two of the bursts with detected afterglows (GRBs 130702A and 140606B) were at low redshift (z = 0.145 and 0.384, respectively) and had spectroscopically confirmed broad-line Type Ic supernovae. We present our broadband follow-up including spectroscopy as well as X-ray, UV, optical, millimeter, and radio observations. We study possible selection effects in the context of the total Fermi and Swift GRB samples. We identify one new outlier on the Amati relation. We find that two bursts are consistent with a mildly relativistic shock breaking out from the progenitor star rather than the ultra-relativistic internal shock mechanism that powers standard cosmological bursts. Finally, in the context of the Zwicky Transient Facility, we discuss how we will continue to expand this effort to find optical counterparts of binary neutron star. mergers that may soon be detected by Advanced LIGO and Virgo. C1 [Singer, Leo P.; Weinstein, Alan] CALTECH, LIGO Lab, Pasadena, CA 91125 USA. [Singer, Leo P.; Cenko, S. Bradley; Cucchiara, Antonino; Gehrels, Neil] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Kasliwal, Mansi M.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Perley, Daniel A.; Cao, Yi; Kulkarni, S. R.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Anderson, Gemma E.; Fender, Rob P.] Univ Oxford, Dept Phys, Astrophys, Oxford OX1 3RH, England. [Anderson, Gemma E.; Fender, Rob P.] Univ Southampton, Phys & Astron, Southampton SO17 1BJ, Hants, England. [Anupama, G. C.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Arcavi, Iair] Las Cumbres Observ, Global Telescope Network, Goleta, CA 93117 USA. [Arcavi, Iair] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Bhalerao, Varun] IUCAA, Pune 411007, Maharashtra, India. [Bue, Brian D.; Rebbapragada, Umaa D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Connaughton, Valerie; Rebbapragada, Umaa D.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Connaughton, Valerie] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Corsi, Alessandra] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Fox, Derek B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Goldstein, Adam; Kouveliotou, Chryssa] NASA, Marshall Space Flight Ctr, Astrophys Off, ZP12, Huntsville, AL 35812 USA. [Gorosabel, J.; Thoene, C. C.; Postigo, A. De Ugarte] CSIC, IAA, E-18008 Granada, Spain. [Gorosabel, J.] Univ Basque Country, UPV EHU, Unidad Asociada Grp Ciencia Planetarias, Dept Fis Aplicada 1,ETS Ingn,IAA,CSIC, E-48013 Bilbao, Spain. [Gorosabel, J.] Ikerbasque, Basque Fdn Sci, E-48008 Bilbao, Spain. [Horesh, Assaf] Benoziyo Ctr Astrophys, Weizmann Inst Sci, IL-76100 Rehovot, Israel. [Hurley, Kevin] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Johansson, Joel] Oskar Klein Ctr, Dept Phys, SE-10691 Stockholm, Sweden. [Kann, D. A.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Kann, D. A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Huang, Kuiyun] Natl Taiwan Normal Univ, Dept Math & Sci, New Taipei City 24449, Taiwan. [Masci, Frank] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Nugent, Peter] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Nugent, Peter] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Svinkin, Dmitry] Ioffe Phys Tech Inst, St Petersburg 194021, Russia. [Postigo, A. De Ugarte] Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Urata, Yuji] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan. RP Singer, LP (reprint author), CALTECH, LIGO Lab, Pasadena, CA 91125 USA. EM leo.p.singer@nasa.gov RI Horesh, Assaf/O-9873-2016; OI Horesh, Assaf/0000-0002-5936-1156; Thone, Christina/0000-0002-7978-7648; Singer, Leo/0000-0001-9898-5597; Anderson, Gemma/0000-0001-6544-8007; Staley, Tim/0000-0002-4474-5253; Bhalerao, Varun/0000-0002-6112-7609; de Ugarte Postigo, Antonio/0000-0001-7717-5085 FU National Science Foundation (NSF); Swift Guest Investigator Program Cycle 9 award 10522 (NASA grant) [NNX14AC24G]; Cycle 10 award 10553 (NASA grant) [NNX14AI99G]; W.M. Keck Foundation; European Research Council Advanced Grant [267697]; Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris Foundation; James S. McDonnell Foundation; Associates of the California Institute of Technology; University of Chicago; state of California; state of Illinois; states of Maryland; NSF; Discovery Communications; NSF [AST-1005313]; Spanish research project [AYA2012-39362-C0202]; European Commission under the Marie Curie Career Integration Grant programme (FP7-PEOPLE-CIG 322307); Research and Technology Development Grant; NASA [NNX07AR71G, NNX13AP09G, NNX11AP96G, NNX13AI54G]; Russian Space Agency contract; RFBR [15-02-00532, 13-02-12017-ofi-m]; NASA FX L.P.S. thanks generous support from the National Science Foundation (NSF) in the form of a Graduate Research Fellowship. The National Radio Astronomy Observatory is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. This paper is based on observations obtained with the Palomar 48 inch Oschin telescope and the Palomar 60 inch telescope at the Palomar Observatory as part of the Intermediate Palomar Transient Factory 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 present work is partly funded by Swift Guest Investigator Program Cycle 9 award 10522 (NASA grant NNX14AC24G) and Cycle 10 award 10553 (NASA grant NNX14AI99G). 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 NASA; the Observatory was made possible by the generous financial support of the W.M. Keck Foundation. We thank Thomas Kruhler for reducing the X-shooter spectrum of GRB 131011A/iPTF13dsw. We thank the staff of the Mullard Radio Astronomy Observatory for their invaluable assistance in the operation of AMI. G.E.A., R.P.F., and T.D.S. acknowledge the support of the European Research Council Advanced Grant 267697, "4 Pi Sky: Extreme Astrophysics with Revolutionary Radio Telescopes." Support for CARMA construction was derived from the Gordon and Betty Moore Foundation; the Kenneth T. and Eileen L. Norris Foundation; the James S. McDonnell Foundation; the Associates of the California Institute of Technology; the University of Chicago; the states of California, Illinois, and Maryland; and the NSF. Ongoing CARMA development and operations are supported by the NSF under a cooperative agreement. and by the CARMA partner universities. These results made use of Lowell Observatory's DCT. Lowell operates the DCT in partnership with Boston University, Northern Arizona University, the University of Maryland, and the University of Toledo. Partial support of the DCT was provided by Discovery Communications. LMI was built by Lowell Observatory using funds from the NSF (AST-1005313). This work is partly based on observations made with GTC, at the Roque de los Muchachos Observatory (La Palma, Spain). The research activity of A.d.U.P., C.T., and J.G. is supported by Spanish research project AYA2012-39362-C0202. A.d.U.P. acknowledges support by the European Commission under the Marie Curie Career Integration Grant programme (FP7-PEOPLE-2012-CIG 322307). A portion of this work was carried out at the Jet Propulsion Laboratory under a Research and Technology Development Grant, under contract with NASA. US Government Support Acknowledged. K.H. acknowledges support for the IPN under the following NASA grants: NNX07AR71G, NNX13AP09G, NNX11AP96G, and NNX13AI54G. The Konus-Wind experiment is partially supported by a Russian Space Agency contract and RFBR grants 15-02-00532 and 13-02-12017-ofi-m. IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the NSF.; This research has made use of data, software, and/or web tools obtained from HEASARC, a service of the Astrophysics Science Division at NASA/GSFC and of the Smithsonian Astrophysical Observatory's High Energy Astrophysics Division. This research has made use of NED, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester including the Swift XRT GRB catalog and light-curve repository (Evans et al. 2007, 2009; Goad et al. 2007). This research made use of Astropy49 (Robitaille et al. 2013), a community-developed core Python package for Astronomy. Some of the results in this paper have been derived using HEALPix (Gorski et al. 2005). NR 215 TC 12 Z9 12 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 52 DI 10.1088/0004-637X/806/1/52 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300052 ER PT J AU Snowden, SL Koutroumpa, D Kuntz, KD Lallement, R Puspitarini, L AF Snowden, S. L. Koutroumpa, D. Kuntz, K. D. Lallement, R. Puspitarini, L. TI THE NORTH GALACTIC POLE RIFT AND THE LOCAL HOT BUBBLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: bubbles; ISM: clouds; ISM: magnetic fields; solar neighborhood; X-rays: diffuse background ID SOFT-X-RAY; SENSITIVITY HI SURVEY; WIND CHARGE-EXCHANGE; SOLAR-WIND; INTERSTELLAR-MEDIUM; MOLECULAR CLOUD; URSA-MAJOR; CHANDRA OBSERVATIONS; ROSAT SURVEY; MAPS AB The North Galactic Pole Rift (NGPR) is one of the few distinct neutral hydrogen clouds at high Galactic latitudes that have well-defined distances. It is located at the edge of the Local Cavity (LC) and provides an important test case for understanding the Local Hot Bubble (LHB), the presumed location for the hot diffuse plasma responsible for much of the observed 1/4 keV emission originating in the solar neighborhood. Using data from the ROSAT All-Sky Survey and the Planck reddening map, we find the path length within the LC (LHB plus Complex of Local Interstellar Clouds) to be 98 +/- 27 pc, in excellent agreement with the distance to the NGPR of 98 +/- 6 pc. In addition, we examine another 14 directions that are distributed over the sky where the LC wall is apparently optically thick at 1/4 keV. We find that the data in these directions are also consistent with the LHB model and a uniform emissivity plasma filling most of the LC. C1 [Snowden, S. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Koutroumpa, D.] Univ Paris 06, Sorbonne Univ, Univ Versailles St Quentin, LATMOS IPSL,CNRS INSU, F-78280 Guyancourt, France. [Kuntz, K. D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. [Lallement, R.] Univ Paris Diderot, CNRS UMR8111, GEPI, Observ Paris, F-92190 Meudon, France. [Puspitarini, L.] Inst Teknol Bandung, FMIPA, Bosscha Observ, Bandung 40132, Indonesia. [Puspitarini, L.] Inst Teknol Bandung, FMIPA, Dept Astron, Bandung 40132, Indonesia. RP Snowden, SL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. FU l'Observatoire de Paris-Meudon GEPI; French National Program "Physique Chimie du Milieu Interstellaire" of the Institut National des Sciences de l'Univers (INSU); French National Research Agency (ANR) through the STILISM project FX S.L.S. would like to thank the l'Observatoire de Paris-Meudon GEPI for their hospitality and support as this paper is based on work which took place while he was a Visiting Scientist in 2014 October-November. D.K. and R.L. would like to acknowledge financial support from the French National Program "Physique Chimie du Milieu Interstellaire" of the Institut National des Sciences de l'Univers (INSU). R.L. and L.P. acknowledge support from the French National Research Agency (ANR) through the STILISM project. The ROSAT PSPC data used in the MBM 12 analysis were acquired from the HEASARC archive. The OMNI data were obtained from the GSFC/SPDF OMNIWeb interface at http://omniweb.gsfc.nasa.gov. NR 49 TC 2 Z9 2 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 JUN 10 PY 2015 VL 806 IS 1 AR 120 DI 10.1088/0004-637X/806/1/120 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300120 ER PT J AU Snowden, SL Heiles, C Koutroumpa, D Kuntz, KD Lallement, R McCammon, D Peek, JEG AF Snowden, S. L. Heiles, C. Koutroumpa, D. Kuntz, K. D. Lallement, R. McCammon, D. Peek, J. E. G. TI REVISITING THE LOCAL LEO COLD CLOUD AND REVISED CONSTRAINTS ON THE LOCAL HOT BUBBLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: bubbles; ISM: clouds; ISM: magnetic fields; solar neighborhood; X-rays: diffuse background ID SOFT-X-RAY; WIND CHARGE-EXCHANGE; SOUTHERN GALACTIC HEMISPHERE; SENSITIVITY HI SURVEY; ALL-SKY SURVEY; INTERSTELLAR-MEDIUM; PHYSICAL-PROPERTIES; SUPERNOVA REMNANT; MOLECULAR CLOUDS; CROSS-SECTIONS AB The Local Leo Cold Cloud (LLCC, at a distance of 11-24 pc) was studied in its relation to the Local Hot Bubble (LHB) and the result suggested that much of the observed 1/4 keV emission in that direction originates in front of the cloud. This placed a strong constraint on the distribution of X-ray emission within the LHB and called into question the assumption of a uniform distribution of X-ray emitting plasma within the Local Cavity. However, recent work has quantified the contribution of heliospheric solar wind charge exchange (SWCX) emission to the diffuse X-ray background measured by the ROSAT All-Sky Survey (RASS) at 1/4 keV, and led to the consistency of pressure measurements between the LHB and the local cloud component of the complex of local interstellar clouds (CLICs) surrounding the Sun. In this paper we revisit the LLCC and improve the previous analysis by using higher resolution RASS data, a serendipitous ROSAT pointed observation, a rigorous treatment of the band-averaged X-ray absorption cross section, and models for the heliospheric and magnetospheric SWCX contributions. We find that the foreground emission to the cloud is in excess of the expected heliospheric (interplanetary plus near Earth) SWCX contribution but that it is marginally consistent with the range of possible LHB plasma path lengths between the LLCC and the CLICs given the currently understood plasma emissivity. C1 [Snowden, S. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Heiles, C.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Koutroumpa, D.] Univ Paris 06, Sorbonne Univ, Univ Versailles St Quentin, LATMOS IPSL,CNRS INSU, F-78280 Guyancourt, France. [Kuntz, K. D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. [Lallement, R.] Univ Paris Diderot, CNRS, GEPI, Observ Paris,UMR8111, F-92190 Meudon, France. [McCammon, D.] Univ Wisconsin, Madison, WI 53706 USA. [Peek, J. E. G.] Space Telescope Sci Inst, Baltimore, MD 21210 USA. RP Snowden, SL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. OI McCammon, Dan/0000-0001-5170-4567 FU French National Program "Physique Chimie du Milieu Interstellaire" of the Institut National des Sciences de l'Univers (INSU); l'Observatoire de Paris-Meudon GEPI FX S.L.S. would like to thank the l'Observatoire de Paris-Meudon GEPI for their hospitality and support as much of the analysis in this paper took place while he was a Visiting Scientist in 2014 October-November. D.K. and R.L. would like to acknowledge financial support from the French National Program "Physique Chimie du Milieu Interstellaire" of the Institut National des Sciences de l'Univers (INSU). The ROSAT PSPC data used in the LLCC analysis were acquired from the HEASARC archive. The IMP-8 data were obtained from the GSFC/SPDF OMNIWeb interface at http://omniweb.gsfc.nasa.gov. NR 78 TC 4 Z9 4 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 119 DI 10.1088/0004-637X/806/1/119 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300119 ER PT J AU Sonnentrucker, P Wolfire, M Neufeld, DA Flagey, N Gerin, M Goldsmith, P Lis, D Monje, R AF Sonnentrucker, P. Wolfire, M. Neufeld, D. A. Flagey, N. Gerin, M. Goldsmith, P. Lis, D. Monje, R. TI A HERSCHEL/HIFI LEGACY SURVEY OF HF AND H2O IN THE GALAXY: PROBING DIFFUSE MOLECULAR CLOUD CHEMISTRY SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; cosmic rays; ISM: abundances; ISM: clouds; ISM: lines and bands; ISM: molecules ID STAR-FORMING REGIONS; RAY IONIZATION RATE; FINE-STRUCTURE EXCITATION; TRANSLUCENT SIGHT LINES; HYDROGEN-FLUORIDE; INTERSTELLAR-MEDIUM; TRIGONOMETRIC PARALLAXES; GALACTIC-CENTER; G10.6-0.4 W31C; SAGITTARIUS B2(M) AB We combine Herschel observations for a total of 12 sources to construct the most uniform survey of HF and H2O in our Galactic disk. Both molecules are detected in absorption along all sight lines. The high spectral resolution of the Heterodyne Instrument for the Far-infrared (HIFI) allows us to compare the HF and H2O distributions in 47 diffuse cloud components sampling the disk. We find that the HF and H2O velocity distributions follow each other almost perfectly and establish that HF and H2O probe the same gas-phase volume. Our observations corroborate theoretical predictions that HF is a sensitive tracer of H-2 in diffuse clouds, down to molecular fractions of only a few percent. Using HF to trace H-2 in our sample, we find that the N(H2O)-to-N(HF) ratio shows a narrow distribution with a median value of 1.51. Our results further suggest that H2O might be used as a tracer of H-2-within a factor of 2.5-in the diffuse interstellar medium (ISM). We show that the measured factor of similar to 2.5 variation around the median is driven by true local variations in the H2O abundance relative to H-2 throughout the disk. The latter variability allows us to test our theoretical understanding of the chemistry of oxygen-bearing molecules in the diffuse gas. We show that both gas-phase and grain-surface chemistry are required to reproduce our H2O observations. This survey thus confirms that grain surface reactions can play a significant role in the chemistry occurring in the diffuse ISM (n(H) <= 1000 cm(-3)). C1 [Sonnentrucker, P.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Sonnentrucker, P.] European Space Agcy, F-75738 Paris 15, France. [Wolfire, M.] Univ Maryland, College Pk, MD 20742 USA. [Neufeld, D. A.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Flagey, N.] Inst Astron, Hilo, HI 96720 USA. [Gerin, M.; Lis, D.] Univ Paris 06, Sorbonne Univ, Observ Paris, CNRS,UMR 8112,LERMA, Paris, France. [Gerin, M.; Lis, D.] PSL Res Univ, LERMA, Observ Paris, CNRS,UMR 8112, F-75014 Paris, France. [Goldsmith, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lis, D.; Monje, R.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RP Sonnentrucker, P (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM sonnentr@stsci.edu FU NASA [NNN12AA01C]; NSF grant [AST-1411827] FX We thank the referee for very useful comments that improved the manuscript significantly. We thank David Hollenbach for useful comments on grain surface chemistry. P.S. acknowledges support for this work from NASA through award NNN12AA01C issued by JPL/Caltech. M.G.W. was supported in part by NSF grant AST-1411827. M.G. thanks CNES and PCMI/INSU for support for the analysis of the Herschel data. This work was carried out in part at the Jet Propulsion Laboratory, which is operated for NASA by the California Institute of Technology. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada, and the United States under the leadership of SRON Netherlands, Institute for Space Research, Groningen, The Netherlands, and with major contributions from Germany, France, and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland: NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologa (CSIC-INTA). Sweden: Chalmers University of Technology-MC2, RSS, & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University-Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. NR 72 TC 7 Z9 7 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 49 DI 10.1088/0004-637X/806/1/49 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300049 ER PT J AU Walton, DJ Middleton, MJ Rana, V Miller, JM Harrison, FA Fabian, AC Bachetti, M Barret, D Boggs, SE Christensen, FE Craig, WW Fuerst, F Grefenstette, BW Hailey, CJ Madsen, KK Stern, D Zhang, W AF Walton, D. J. Middleton, M. J. Rana, V. Miller, J. M. Harrison, F. A. Fabian, A. C. Bachetti, M. Barret, D. Boggs, S. E. Christensen, F. E. Craig, W. W. Fuerst, F. Grefenstette, B. W. Hailey, C. J. Madsen, K. K. Stern, D. Zhang, W. TI NUSTAR, XMM-NEWTON, AND SUZAKU OBSERVATIONS OF THE ULTRALUMINOUS X-RAY SOURCE HOLMBERG II X-1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; X-rays: binaries; X-rays: individual (Holmberg II X-1) ID MASS BLACK-HOLES; BROAD-BAND; ACCRETION DISKS; STATE TRANSITIONS; NEARBY GALAXIES; SPECTRAL STATE; EMISSION-LINE; SOLAR MASSES; ESO 243-49; IX X-1 AB We present the first broadband 0.3-25.0 keV X-ray observations of the bright ultraluminous X-ray source (ULX) Holmberg II X-1, performed by NuSTAR, XMM-Newton, and Suzaku in 2013 September. The NuSTAR data provide the first observations of Holmberg II X-1 above 10 keV and reveal a very steep high-energy spectrum, similar to other ULXs observed by NuSTAR to date. These observations further demonstrate that ULXs exhibit spectral states that are not typically seen in Galactic black hole binaries. Comparison with other sources implies that Holmberg II X-1 accretes at a high fraction of its Eddington accretion rate and possibly exceeds it. The soft X-ray spectrum (E < 10 keV) appears to be dominated by two blackbody-like emission components, the hotter of which may be associated with an accretion disk. However, all simple disk models under-predict the NuSTAR data above similar to 10 keV and require an additional emission component at the highest energies probed, implying the NuSTAR data does not fall away with a Wien spectrum. We investigate physical origins for such an additional high-energy emission component and favor a scenario in which the excess arises from Compton scattering in a hot corona of electrons with some properties similar to the very high state seen in Galactic binaries. The observed broadband 0.3-25.0 keV luminosity inferred from these epochs is L-X = (8.1 +/- 0.1) x 10(39) erg s(-1), typical for Holmberg II X-1, with the majority of this flux (similar to 90%) emitted below 10 keV. C1 [Walton, D. J.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Walton, D. J.; Rana, V.; Harrison, F. A.; Fuerst, F.; Grefenstette, B. W.; Madsen, K. K.] CALTECH, Space Radiat Lab, Pasadena, CA 91109 USA. [Middleton, M. J.; Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 49109 USA. [Bachetti, M.; Barret, D.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Bachetti, M.; Barret, D.] CNRS, IRAP, F-31028 Toulouse 4, France. [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Zhang, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Walton, DJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI XRAY, SUZAKU/A-1808-2009; Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337; Rana, Vikram/0000-0003-1703-8796 FU French Space Agency (CNES); NASA; ESA; space agency of Japan (JAXA); space agency of USA (NASA) FX The authors would like to thank the referee for the positive feedback, which helped improve the clarity of the final manuscript. M.B. and D.B. acknowledge financial support from the French Space Agency (CNES). This research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by NASA/JPL and has utilized the NUSTARDAS software package, jointly developed by the ASDC (Italy) and Caltech (USA). This research has also made use of data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States, and with Suzaku, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). NR 69 TC 15 Z9 15 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 65 DI 10.1088/0004-637X/806/1/65 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300065 ER PT J AU Williams, BF Dalcanton, JJ Dolphin, AE Weisz, DR Lewis, AR Lang, DT Bell, EF Boyer, M Fouesneau, M Gilbert, KM Monachesi, A Skillman, E AF Williams, Benjamin F. Dalcanton, Julianne J. Dolphin, Andrew E. Weisz, Daniel R. Lewis, Alexia R. Lang, Dustin Bell, Eric F. Boyer, Martha Fouesneau, Morgan Gilbert, Karoline M. Monachesi, Antonela Skillman, Evan TI A GLOBAL STAR-FORMING EPISODE IN M31 2-4 GYR AGO SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: individual (M31); galaxies: interactions ID LOCAL GROUP GALAXIES; ANDROMEDA GALAXY; FORMATION HISTORY; STELLAR CONTENT; DWARF GALAXIES; SPIRAL GALAXY; GIANT STREAM; THIN PLANE; OUTER DISK; MILKY-WAY AB We have identified a major global enhancement of star formation in the inner M31 disk that occurred between 2-4 Gyr ago, producing similar to 60% of the stellar mass formed in the past 5 Gyr. The presence of this episode in the inner disk was discovered by modeling the optical resolved star color-magnitude diagrams of low extinction regions in the main disk of M31 (3 < R < 20 kpc) as part of the Panchromatic Hubble Andromeda Treasury. This measurement confirms and extends recent measurements of a widespread star formation enhancement of similar age in the outer disk, suggesting that this burst was both massive and global. Following the galaxy-wide burst, the star formation rate of M31 has significantly declined. We briefly discuss possible causes for these features of the M31 evolutionary history, including interactions with M32, M33, and/or a merger. C1 [Williams, Benjamin F.; Dalcanton, Julianne J.; Weisz, Daniel R.; Lewis, Alexia R.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Dolphin, Andrew E.] Raytheon Co, Tucson, AZ 85706 USA. [Lang, Dustin] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Boyer, Martha] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Fouesneau, Morgan] MPIA, Heidelberg, Germany. [Gilbert, Karoline M.] STScI, Baltimore, MD 21218 USA. [Monachesi, Antonela] MPA, Garching, Germany. [Skillman, Evan] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. RP Williams, BF (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM ben@astro.washington.edu; jd@astro.washington.edu; adolphin@raytheon.com; dweisz@astro.washington.edu; dstn@cmu.edu; ericbell@umich.edu; martha.boyer@nasa.gov; fouesneau@mpia-hd.mpg.de; kgilbert@stsci.edu; antonela@mpa-garching.mpg.de; skillman@astro.umn.edu OI Bell, Eric/0000-0002-5564-9873 FU NASA through grant from the Space Telescope Science Institute [GO-12055]; NASA - Space Telescope Science Institute [HST-HF-51331.01]; NASA [NAS5-26555] FX Support for this work was provided by NASA through grant GO-12055 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. Support for DRW is provided by NASA through Hubble Fellowship grants HST-HF-51331.01 awarded by the Space Telescope Science Institute. We thank Amazon cloud services, for donating some of the computing time necessary to make these measurements. NR 61 TC 5 Z9 5 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 48 DI 10.1088/0004-637X/806/1/48 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300048 ER PT J AU Zhang, BB van Eerten, H Burrows, DN Ryan, GS Evans, PA Racusin, JL Troja, E MacFadyen, A AF Zhang, Bin-Bin van Eerten, Hendrik Burrows, David N. Ryan, Geoffrey Scott Evans, Philip A. Racusin, Judith L. Troja, Eleonora MacFadyen, Andrew TI AN ANALYSIS OF CHANDRA DEEP FOLLOW-UP GAMMA-RAY BURSTS: IMPLICATIONS FOR OFF-AXIS JETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; methods: numerical ID AFTERGLOW LIGHT CURVES; SWIFT XRT DATA; BROAD-BAND OBSERVATIONS; X-RAY; COMPREHENSIVE ANALYSIS; ELECTRON ACCELERATION; COLLISIONLESS SHOCKS; SPECTRAL PROPERTIES; OPTICAL AFTERGLOW; RELATIVISTIC JET AB We present a sample of 27 gamma-ray bursts (GRBs) with detailed Swift. light curves supplemented by late-time Chandra. observations. To answer the missing jet-break problem in general, we develop a numerical-simulationbased model that can be directly fit to the data using Monte Carlo methods. Our numerical model takes into account all the factors that can shape a jet break: (i) lateral expansion, (ii) edge effects, and (iii) off-axis effects. Our results provide improved fits to the light curves and constraints on physical parameters. More importantly, our results suggest that off-axis effects are important and must be included in interpretations of GRB jet breaks. C1 [Zhang, Bin-Bin; Burrows, David N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Zhang, Bin-Bin] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Zhang, Bin-Bin] CSIC, IAA, E-18080 Granada, Spain. [van Eerten, Hendrik] Max Planck Inst Extraterrestrial Phys MPE, D-85741 Garching, Germany. [van Eerten, Hendrik; Ryan, Geoffrey Scott; MacFadyen, Andrew] NYU, Ctr Cosmol & Particle Phys, Dept Phys, New York, NY 10003 USA. [Evans, Philip A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Racusin, Judith L.; Troja, Eleonora] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Troja, Eleonora] Univ Maryland, CRESST, Dept Astron, College Pk, MD 20742 USA. RP Zhang, BB (reprint author), Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. EM binbin.zhang@uah.edu RI Zhang, Binbin/C-9035-2013; OI Zhang, Binbin/0000-0003-2002-116X; Zhang, Binbin/0000-0003-4111-5958; MacFadyen, Andrew/0000-0002-0106-9013 FU NASA [NAS5-00136, TM3-14005X, NNX13AO93G]; SAO [SV4-74018, AR3-14005X, GO1-12102X, GO3-14067X] FX We thank the anonymous referee for detailed and thoughtful comments that greatly improved the paper. We thank Peter Veres, Peter Meszaros, Kazumi Kashiyama, Xiao-Hong Zhao, Xue-Wen Liu, Valerie Connaughton, Dirk Grupe, Derek Fox, Abe Falcone, Leisa Townsley, Eveline Helder, He Gao, Liang Li, Fangkun Peng, Enwei Liang, Neil Gehrels, and Bing Zhang for helpful comments and suggestions. We thank Tyson Littenberg and Dan Foreman-Mackey for discussion on the MCMC method. B.B.Z. thanks Johannes Buchner and Farhan Feroz for help on the MULTINEST codes. This work was supported by SAO contract SV4-74018, NASA contract NAS5-00136, and by SAO grants AR3-14005X, GO1-12102X, and GO3-14067X. H.V.E., G.S.R., and A.M. acknowledge the support by NASA TM3-14005X and NNX13AO93G. We acknowledge the use of public data from the Swift and Chandra data archive. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. NR 101 TC 13 Z9 13 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2015 VL 806 IS 1 AR 15 DI 10.1088/0004-637X/806/1/15 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300015 ER PT J AU Schiemangk, M Lampmann, K Dinkelaker, A Kohfeldt, A Krutzik, M Kurbis, C Sahm, A Spiessberger, S Wicht, A Erbert, G Trankle, G Peters, A AF Schiemangk, Max Lampmann, Kai Dinkelaker, Aline Kohfeldt, Anja Krutzik, Markus Kuerbis, Christian Sahm, Alexander Spiessberger, Stefan Wicht, Andreas Erbert, Goetz Traenkle, Guenther Peters, Achim TI High-power, micro-integrated diode laser modules at 767 and 780 nm for portable quantum gas experiments SO APPLIED OPTICS LA English DT Article ID ATOM INTERFEROMETRY; LINEWIDTH AB We present micro-integrated diode laser modules operating at wavelengths of 767 and 780 nm for cold quantum gas experiments on potassium and rubidium. The master-oscillator-power-amplifier concept provides both narrow linewidth emission and high optical output power. With a linewidth (10 mu s) below 1 MHz and an output power of up to 3W, these modules are specifically suited for quantum optics experiments and feature the robustness required for operation at a drop tower or on-board a sounding rocket. This technology development hence paves the way toward precision quantum optics experiments in space. (C) 2015 Optical Society of America C1 [Schiemangk, Max; Lampmann, Kai; Dinkelaker, Aline; Krutzik, Markus; Wicht, Andreas; Peters, Achim] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. [Schiemangk, Max; Lampmann, Kai; Dinkelaker, Aline; Kohfeldt, Anja; Kuerbis, Christian; Sahm, Alexander; Spiessberger, Stefan; Wicht, Andreas; Erbert, Goetz; Traenkle, Guenther; Peters, Achim] Leibniz Inst Hochstfrequenztech, Ferdinand Braun Inst, D-12489 Berlin, Germany. [Lampmann, Kai] Johannes Gutenberg Univ Mainz, Inst Phys, D-55128 Mainz, Germany. [Krutzik, Markus] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Schiemangk, M (reprint author), Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. EM max.schiemangk@physik.hu-berlin.de FU German Space Agency (DLR) [DLR 50WM0940, DLR 50WM1132, DLR 50WM1134, DLR 50WM1240]; European Commission (EC) [250072]; European Union FX German Space Agency (DLR) (DLR 50WM0940, DLR 50WM1132, DLR 50WM1134, DLR 50WM1240); European Commission (EC) (250072).; The authors thank H. Ahlers, H. Muntinga, and A. Wenzlawski from the QUANTUS-I team for providing their experiment for the test of the MOPA module. C. K. and A. W. acknowledge financial support from the European Union's Seventh Framework Programme for research, technological development and demonstration. NR 22 TC 8 Z9 8 U1 1 U2 10 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD JUN 10 PY 2015 VL 54 IS 17 BP 5332 EP 5338 DI 10.1364/AO.54.005332 PG 7 WC Optics SC Optics GA CK3FE UT WOS:000356101200010 PM 26192832 ER PT J AU Brasunas, J Mamoutkine, A Gorius, N AF Brasunas, J. Mamoutkine, A. Gorius, N. TI Identifying sampling comb changes in Fourier transform spectrometers with significant self-emission and beam splitter absorption SO APPLIED OPTICS LA English DT Article ID CALIBRATION; MODE AB For accurate calibration of Fourier transform spectrometers we must constrain or resample the interferogram data to an invariant sampling comb. This can become challenging when instrument self-emission is significant and beam splitter absorption is present. The originally-sampled interferogram center-burst position can move due not only to sampling comb changes, but also to an interaction between the strength of an external target and the so-called anomalous phase (the two ports of the interferometer contribute center-bursts at different locations, and the relative weighting of the two ports varies with the strength of the external target). We present a model of the anomalous phase to enable partitioning of changes in observed center-burst location between sampling comb changes and anomalous phase effects. C1 [Brasunas, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mamoutkine, A.] Adnet Syst, Greenbelt, MD 20771 USA. [Gorius, N.] Catholic Univ, Greenbelt, MD 20771 USA. RP Brasunas, J (reprint author), NASA, Goddard Space Flight Ctr, Code 693, Greenbelt, MD 20771 USA. EM john.c.brasunas@nasa.gov NR 13 TC 1 Z9 1 U1 1 U2 7 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD JUN 10 PY 2015 VL 54 IS 17 BP 5461 EP 5468 DI 10.1364/AO.54.005461 PG 8 WC Optics SC Optics GA CK3FE UT WOS:000356101200026 PM 26192848 ER PT J AU de Leon, J Takami, M Karr, JL Hashimoto, J Kudo, T Sitko, M Mayama, S Kusakabe, N Akiyama, E Liu, HB Usuda, T Abe, L Brandner, W Brandt, TD Carson, J Currie, T Egner, SE Feldt, M Follette, K Grady, CA Goto, M Guyon, O Hayano, Y Hayashi, M Hayashi, S Henning, T Ishii, KWHM Ishii, M Iye, M Janson, M Kandori, R Knapp, GR Kuzuhara, M Kwon, J Matsuo, T McElwain, MW Miyama, S Morino, JI Moro-Martin, A Nishimura, T Pyo, TS Serabyn, E Suenaga, T Suto, H Suzuki, R Takahashi, Y Takato, N Terada, H Thalmann, C Tomono, D Turner, EL Watanabe, M Wisniewski, JP Yamada, T Takami, H Tamura, M AF de Leon, Jerome Takami, Michihiro Karr, Jennifer L. Hashimoto, Jun Kudo, Tomoyuki Sitko, Michael Mayama, Satoshi Kusakabe, Nobuyuki Akiyama, Eiji Liu, Hauyu Baobab Usuda, Tomonori Abe, Lyu Brandner, Wolfgang Brandt, Timothy D. Carson, Joseph Currie, Thayne Egner, Sebastian E. Feldt, Markus Follette, Katherine Grady, Carol A. Goto, Miwa Guyon, Olivier Hayano, Yutaka Hayashi, Masahiko Hayashi, Saeko Henning, Thomas Hodapp, Klaus W. Ishii, Miki Iye, Masanori Janson, Markus Kandori, Ryo Knapp, Gillian R. Kuzuhara, Masayuki Kwon, Jungmi Matsuo, Taro McElwain, Michael W. Miyama, Shoken Morino, Jun-Ichi Moro-Martin, Amaya Nishimura, Tetsuo Pyo, Tae-Soo Serabyn, Eugene Suenaga, Takuya Suto, Hiroshi Suzuki, Ryuji Takahashi, Yasuhiro Takato, Naruhisa Terada, Hiroshi Thalmann, Christian Tomono, Daigo Turner, Edwin L. Watanabe, Makoto Wisniewski, John P. Yamada, Toru Takami, Hideki Tamura, Motohide TI NEAR-IR HIGH-RESOLUTION IMAGING POLARIMETRY OF THE SU Aur DISK: CLUES FOR TIDAL TAILS? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE polarization; protoplanetary disks; stars: individual (SU Aur); stars: pre-main sequence ID T-TAURI STARS; PROTOPLANETARY DISK; CIRCUMSTELLAR DISK; PROTOSTELLAR ENVELOPES; STELLAR ENCOUNTERS; ADAPTIVE OPTICS; FORMING REGIONS; SCATTERED-LIGHT; GIANT PLANETS; YOUNG STARS AB We present new high-resolution (similar to 0."09) H-band imaging observations of the circumstellar disk around the T Tauri star SU Aur. Our observations with Subaru-HiCIAO have revealed the presence of scattered light as close as 0."15 (similar to 20 AU) to the star. Within our image, we identify bright emission associated with a disk with a minimum radius of similar to 90 AU, an inclination of similar to 35 degrees from the plane of the sky, and an approximate PA of 15 degrees for the major axis. We find a brightness asymmetry between the northern and southern sides of the disk due to a non-axisymmetric disk structure. We also identify a pair of asymmetric tail structures extending east and west from the disk. The western tail extends at least 2."5 (350 AU) from the star, and is probably associated with a reflection nebula previously observed at optical and near-IR wavelengths. The eastern tail extends at least 1. (140 AU) at the present signal-to-noise. These tails are likely due to an encounter with an unseen brown dwarf, but our results do not exclude the explanation that these tails are outflow cavities or jets. C1 [de Leon, Jerome; Takami, Michihiro; Karr, Jennifer L.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [de Leon, Jerome; Mayama, Satoshi; Suenaga, Takuya] Grad Univ Adv Studies SOKENDAI, Ctr Promot Integrated Sci, Miura, Kanagawa 2400193, Japan. [Hashimoto, Jun; Wisniewski, John P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Hashimoto, Jun; Kusakabe, Nobuyuki; Akiyama, Eiji; Usuda, Tomonori; Hayashi, Masahiko; Ishii, Miki; Iye, Masanori; Kandori, Ryo; Morino, Jun-Ichi; Suto, Hiroshi; Suzuki, Ryuji; Tamura, Motohide] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Kudo, Tomoyuki; Currie, Thayne; Egner, Sebastian E.; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko; Nishimura, Tetsuo; Pyo, Tae-Soo; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daigo; Tamura, Motohide] Subaru Telescope, Hilo, HI 96720 USA. [Sitko, Michael] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA. [Abe, Lyu] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR 7293, F-06108 Nice 2, France. [Brandner, Wolfgang; Feldt, Markus; Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Brandt, Timothy D.; Turner, Edwin L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Carson, Joseph] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA. [Follette, Katherine] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Grady, Carol A.] Eureka Sci, Oakland, CA 96402 USA. [Grady, Carol A.; McElwain, Michael W.] Goddard Space Flight Ctr, ExoPlanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. Univ Sternwarte, D-81679 Munich, Germany. [Hodapp, Klaus W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [Janson, Markus] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Kuzuhara, Masayuki] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan. [Kwon, Jungmi; Takahashi, Yasuhiro; Tamura, Motohide] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Matsuo, Taro] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto, Kyoto 6068502, Japan. [Miyama, Shoken] Hiroshima Univ, Higashihiroshima 7398511, Japan. [Moro-Martin, Amaya] CSIC, CAB, INTA, Dept Astrophys, E-28850 Madrid, Spain. [Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Takahashi, Yasuhiro] MEXT, Tokyo, Tokyo 1008959, Japan. [Thalmann, Christian] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Turner, Edwin L.] Univ Tokyo, Kavli Inst Phys & Math Univ, Kashiwa, Chiba 2778568, Japan. [Watanabe, Makoto] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan. [Yamada, Toru] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. RP de Leon, J (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. EM jpdeleon.bsap@gmail.com RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016; OI Watanabe, Makoto/0000-0002-3656-4081; Feldt, Markus/0000-0002-4188-5242 FU Ministry of Science and Technology (MoST) of Taiwan [103-2112-M-001-029]; NSF AST [1008440] FX We thank the Subaru Telescope staff for their support, especially Michael Lemmen for making our observations successful. We also thank Drs. Kazushi Sakamoto, Shigehisa Takakuwa, Lihwai Lin, Yoichi Ohyama, Pin-Gao Gu, and Henry Hsieh for useful discussions. M. T. is supported from Ministry of Science and Technology (MoST) of Taiwan (Grant No. 103-2112-M-001-029). C.A.G. acknowledges support under NSF AST 1008440. This research made use of the Simbad database operated at CDS, Strasbourg, France, and the NASA's Astrophysics Data System Abstract Service. NR 42 TC 2 Z9 2 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 10 PY 2015 VL 806 IS 1 AR L10 DI 10.1088/2041-8205/806/1/L10 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL0LH UT WOS:000356633700010 ER PT J AU Fransson, C Larsson, J Migotto, K Pesce, D Challis, P Chevalier, RA France, K Kirshner, RP Leibundgut, B Lundqvist, P McCray, R Spyromilio, J Taddia, F Jerkstrand, A Mattila, S Smith, N Sollerman, J Wheeler, JC Crotts, A Garnavich, P Heng, K Lawrence, SS Panagia, N Pun, CSJ Sonneborn, G Sugerman, B AF Fransson, Claes Larsson, Josefin Migotto, Katia Pesce, Dominic Challis, Peter Chevalier, Roger A. France, Kevin Kirshner, Robert P. Leibundgut, Bruno Lundqvist, Peter McCray, Richard Spyromilio, Jason Taddia, Francesco Jerkstrand, Anders Mattila, Seppo Smith, Nathan Sollerman, Jesper Wheeler, J. Craig Crotts, Arlin Garnavich, Peter Heng, Kevin Lawrence, Stephen S. Panagia, Nino Pun, Chun S. J. Sonneborn, George Sugerman, Ben TI THE DESTRUCTION OF THE CIRCUMSTELLAR RING OF SN 1987A SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; shock waves; supernovae: individual (SN 1987A) ID SUPERNOVA 1987A; RADIO REMNANT; SPECTROSCOPY; SIMULATIONS; EVOLUTION; SN-1987A; NEBULA; EJECTA; SHOCK AB We present imaging and spectroscopic observations with Hubble Space Telescope and Very Large Telescope of the ring of SN 1987A from 1994 to 2014. After an almost exponential increase of the shocked emission from the hotspots up to day similar to 8000 (similar to 2009), both this and the unshocked emission are now fading. From the radial positions of the hotspots we see an acceleration of these up to 500-1000 km s(-1), consistent with the highest spectroscopic shock velocities from the radiative shocks. In the most recent observations (2013 and 2014), we find several new hotspots outside the inner ring, excited by either X-rays from the shocks or by direct shock interaction. All of these observations indicate that the interaction with the supernova ejecta is now gradually dissolving the hotspots. We predict, based on the observed decay, that the inner ring will be destroyed by similar to 2025. C1 [Fransson, Claes; Migotto, Katia; Lundqvist, Peter; Taddia, Francesco; Sollerman, Jesper] AlbaNova Univ Ctr, Stockholm Univ, Oskar Klein Ctr, Dept Astron, SE-10691 Stockholm, Sweden. [Larsson, Josefin] AlbaNova, KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Larsson, Josefin] AlbaNova, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Pesce, Dominic; Chevalier, Roger A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Challis, Peter; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [France, Kevin] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [France, Kevin] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Leibundgut, Bruno; Spyromilio, Jason] European So Observ, D-85748 Garching, Germany. [McCray, Richard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Jerkstrand, Anders] Queens Univ, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. [Mattila, Seppo] Turku Univ, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland. [Mattila, Seppo] Turku Univ, Tuorla Observ, Dept Phys & Astron, FI-21500 Piikkio, Finland. [Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Wheeler, J. Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Crotts, Arlin] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Garnavich, Peter] Univ Notre Dame, Nieuwland Sci 25, Notre Dame, IN 46556 USA. [Heng, Kevin] Univ Bern, Ctr Space & Habitabil, CH-3012 Bern, Switzerland. [Lawrence, Stephen S.] Hofstra Univ, Dept Phys & Astron, Hempstead, NY 11549 USA. [Panagia, Nino] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Panagia, Nino] Osserv Astron Capodimonte, INAF NA, I-80131 Naples, Italy. [Panagia, Nino] Supernova Ltd, Virgin Gorda VG 1150, Virgin Islands, England. [Pun, Chun S. J.] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Sonneborn, George] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Sugerman, Ben] Goucher Coll, Dept Phys & Astron, Baltimore, MD 21204 USA. RP Fransson, C (reprint author), AlbaNova Univ Ctr, Stockholm Univ, Oskar Klein Ctr, Dept Astron, SE-10691 Stockholm, Sweden. RI Jerkstrand, Anders/K-9648-2015; OI Jerkstrand, Anders/0000-0001-8005-4030; Sollerman, Jesper/0000-0003-1546-6615; Lundqvist, Peter/0000-0002-3664-8082; /0000-0003-0065-2933; Fransson, Claes/0000-0001-8532-3594; Heng, Kevin/0000-0003-1907-5910 FU Swedish Research Council; Swedish National Space Board, NASA [NNX12AF90G]; NSF [AST-1109801]; NASA through a grant from the Space Telescope Science Institute; ESO Programmes [080.D-0727, 082.D-0273, 086.D-0713, 088.D-0638, 090.D-645, 092.D0119, 094.D-0505] FX We are grateful to the referee for detailed comments. This work was supported by the Swedish Research Council and the Swedish National Space Board, NASA grant NNX12AF90G, NSF grant AST-1109801. Support for the HST observing program was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. Partially based on observations collected at the European Southern Observatory, Chile (ESO Programmes 080.D-0727, 082.D-0273, 086.D-0713, 088.D-0638, 090.D-645, 092.D0119, 094.D-0505). NR 23 TC 9 Z9 9 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 10 PY 2015 VL 806 IS 1 AR L19 DI 10.1088/2041-8205/806/1/L19 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL0LH UT WOS:000356633700019 ER PT J AU Morales-Juberias, R Sayanagi, KM Simon, AA Fletcher, LN Cosentino, RG AF Morales-Juberias, R. Sayanagi, K. M. Simon, A. A. Fletcher, L. N. Cosentino, R. G. TI MEANDERING SHALLOW ATMOSPHERIC JET AS A MODEL OF SATURN'S NORTH-POLAR HEXAGON SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planets and satellites: atmospheres; planets and satellites: general; planets and satellites: physical evolution ID GULF-STREAM; EQUILIBRIA; STABILITY; EASTWARD; ANNULUS; WAVES AB The Voyager flybys of Saturn in 1980-1981 revealed a circumpolar Hexagon at similar to 78 degrees north planetographic latitude that has persisted for over 30 Earth years, more than one Saturn year, and has been observed by ground-based telescopes, Hubble Space Telescope and multiple instruments on board the Cassini orbiter. Its average phase speed is very slow with respect to the System III rotation rate, defined by the primary periodicity in the Saturn Kilometric Radiation during the Voyager era. Cloud tracking wind measurements reveal the presence of a prograde jet-stream whose path traces the Hexagon's shape. Previous numerical models have produced large-amplitude, n = 6, wavy structures with westward intrinsic phase propagation (relative to the jet). However, the observed net phase speed has proven to be more difficult to achieve. Here we present numerical simulations showing that instabilities in shallow jets can equilibrate as meanders closely resembling the observed morphology and phase speed of Saturn's northern Hexagon. We also find that the winds at the bottom of the model are as important as the winds at the cloud level in matching the observed Hexagon's characteristics. C1 [Morales-Juberias, R.; Cosentino, R. G.] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA. [Sayanagi, K. M.] Hampton Univ, Atmospher & Planetary Sci Dept, Hampton, VA 23668 USA. [Simon, A. A.] NASA, GSFC, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Fletcher, L. N.] Univ Oxford, Clarendon Lab, Atmospher Ocean & Planetary Phys, Oxford OX1 3PU, England. RP Morales-Juberias, R (reprint author), New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA. EM rmjuberias@gmail.com RI Simon, Amy/C-8020-2012; Fletcher, Leigh/D-6093-2011 OI Simon, Amy/0000-0003-4641-6186; Fletcher, Leigh/0000-0001-5834-9588 FU NASA [NNX14AH47G, NNX12AR38G]; NSF [1212216]; Royal Society Research Fellowship at the University of Oxford FX This work was partially supported by NASA PATM grant number NNX14AH47G to A.S., and NASA OPR grant NNX12AR38G and NSF A&A grant 1212216 to K.M.S. L.N.F. was supported by a Royal Society Research Fellowship at the University of Oxford. Computational resources were provided by New Mexico Tech. NR 26 TC 0 Z9 0 U1 4 U2 12 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 JUN 10 PY 2015 VL 806 IS 1 AR L18 DI 10.1088/2041-8205/806/1/L18 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL0LH UT WOS:000356633700018 ER PT J AU Scott, JM Haykowsky, MJ AF Scott, Jessica M. Haykowsky, Mark J. TI Letter by Scott and Haykowsky Regarding Articles, "Can Intensive Exercise Harm the Heart? The Benefits of Competitive Endurance Training for Cardiovascular Structure and Function" and "Can Intensive Exercise Harm the Heart? You Can Get Too Much of a Good Thing" SO CIRCULATION LA English DT Letter C1 [Scott, Jessica M.] NASA, Lyndon B Johnson Space Ctr, Univ Space Res Assoc, Houston, TX 77058 USA. [Haykowsky, Mark J.] Univ Alberta, Edmonton, AB, Canada. RP Scott, JM (reprint author), NASA, Lyndon B Johnson Space Ctr, Univ Space Res Assoc, Houston, TX 77058 USA. NR 6 TC 0 Z9 0 U1 0 U2 1 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA TWO COMMERCE SQ, 2001 MARKET ST, PHILADELPHIA, PA 19103 USA SN 0009-7322 EI 1524-4539 J9 CIRCULATION JI Circulation PD JUN 9 PY 2015 VL 131 IS 23 BP E523 EP E523 DI 10.1161/CIRCULATIONAHA.114.013457 PG 1 WC Cardiac & Cardiovascular Systems; Peripheral Vascular Disease SC Cardiovascular System & Cardiology GA DC5IJ UT WOS:000369254400002 PM 26056349 ER PT J AU Lecoutre, C Guillaument, R Marre, S Garrabos, Y Beysens, D Hahn, I AF Lecoutre, C. Guillaument, R. Marre, S. Garrabos, Y. Beysens, D. Hahn, I. TI Weightless experiments to probe universality of fluid critical behavior SO PHYSICAL REVIEW E LA English DT Article ID LIQUID CRITICAL-POINT; CRITICAL ISOCHORE; LIGHT-SCATTERING; XENON; HEAT; SF6 AB Near the critical point of fluids, critical opalescence results in light attenuation, or turbidity increase, that can be used to probe the universality of critical behavior. Turbidity measurements in SF6 under weightlessness conditions on board the International Space Station are performed to appraise such behavior in terms of both temperature and density distances from the critical point. Data are obtained in a temperature range, far (1 K) from and extremely close (a few mu K) to the phase transition, unattainable from previous experiments on Earth. Data are analyzed with renormalization-group matching classical-to-critical crossover models of the universal equation of state. It results that the data in the unexplored region, which is a minute deviant from the critical density value, still show adverse effects for testing the true asymptotic nature of the critical point phenomena. C1 [Lecoutre, C.; Guillaument, R.; Marre, S.; Garrabos, Y.] CNRS, ICMCB, ESEME, UPR 9048, F-33600 Pessac, France. [Lecoutre, C.; Guillaument, R.; Marre, S.; Garrabos, Y.] Univ Bordeaux, ICMCB, UPR 9048, F-33600 Pessac, France. [Beysens, D.] Univ Paris Diderot, Univ Paris 06, CNRS ESPCI, Phys & Mecan Milieux Heterogenes,UMR 7636, F-75005 Paris, France. [Beysens, D.] CEA Grenoble, Serv Basses Temp, F-38000 Grenoble, France. [Beysens, D.] Univ Grenoble 1, F-38000 Grenoble, France. [Hahn, I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lecoutre, C (reprint author), CNRS, ICMCB, ESEME, UPR 9048, F-33600 Pessac, France. EM carole.lecoutre@icmcb.cnrs.fr RI Lecoutre, Carole/H-3367-2013; Garrabos, Yves/H-5404-2013; Marre, Samuel/H-3377-2013 FU CNES; NASA FX We thank the DECLIC CNES-NASA teams, and associated industrial teams, involved in the ALI-DECLIC project development and achievement and in particular the NASA and CADMOS teams for operational managing and control of the facility onboard the ISS. C.L., R.G., S.M., Y.G., and D.B. are grateful to CNES for financial support. The research of I.H. was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 23 TC 5 Z9 5 U1 0 U2 8 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1539-3755 EI 1550-2376 J9 PHYS REV E JI Phys. Rev. E PD JUN 8 PY 2015 VL 91 IS 6 AR 060101 DI 10.1103/PhysRevE.91.060101 PG 5 WC Physics, Fluids & Plasmas; Physics, Mathematical SC Physics GA CJ8BY UT WOS:000355725400001 PM 26172640 ER PT J AU Sola, F Dynys, FW AF Sola, F. Dynys, F. W. TI Probing the mechanical properties and microstructure of WSi2/SixGe1-x multiphase thermoelectric material by nanoindentation, electron and focused ion beam microscopy methods SO JOURNAL OF ALLOYS AND COMPOUNDS LA English DT Article DE SEM; TEM; FIB; Nanoindentation; Fracture toughness; Thermoelectric material ID ELASTIC PROPERTIES; SILICON; GERMANIUM; ALLOY; NANOCOMPOSITES; INDENTATION; TRANSITION; HARDNESS; STEEL; FILMS AB Thermoelectric (TE) materials such as silicon germanium (SiGe) alloys have been traditionally used in radioisotope thermoelectric generators (RTG) NASA applications. Beyond traditional RTG applications, we are exploring other applications in the energy harvesting arena. There is still a need to increment the TE figure of merit (ZT) of SiGe based TE alloys and we have been working on ways to improve it by incorporating tungsten di-silicide (WSi2) phases into the matrix by directional solidification (DS) process. Considerable efforts have been focused until now in microstructural engineering methods that lead to ZT improvement by microstructure optimization of TE materials. Although critical for the previous mentioned applications, work pertinent to the mechanical integrity of this type of WSi2/SiGe based TE materials is lacking. In this work, we explored for the first time the local mechanical properties and microstructure of WSi2/SixGe1-x multiphase thermoelectric material by nanoindentation, scanning electron microscopy (SEM), focused ion beam (FIB) and transmission electron microscopy (TEM) methods. We report hardness (H), modulus (E) and fracture toughness (k(c)) data for all phases. We obtained average H (and E) values (in GPa) of 12.94 (464.95) for the WSi2 phase, 19.49 (214.52) for the matrix, 14.95 (142.84) for the Si rich phase, and 13.98 (138.56) for the Ge rich phase respectively; while average k(c) values (in MPa m(0.5)) were 1.37 for theWSi(2), 0.52 for the matrix, 0.36 for the Si rich and 0.24 for the Ge rich phases respectively. FIB serial sectioning and cross-sectional TEM analysis is also included which provided insights on the deformation process below the nanoindentation area. Published by Elsevier B.V. C1 [Sola, F.; Dynys, F. W.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA. RP Sola, F (reprint author), NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA. EM francisco.sola-lopez@nasa.gov FU NASA FX This work was supported by the NASA Advanced Thermoelectric Project. The authors would like to acknowledge Dr. R. Rogers for the XRD work and Ms. J. Buehler for polishing of the samples. NR 32 TC 2 Z9 3 U1 2 U2 49 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0925-8388 EI 1873-4669 J9 J ALLOY COMPD JI J. Alloy. Compd. PD JUN 5 PY 2015 VL 633 BP 165 EP 169 DI 10.1016/j.jallcom.2015.01.246 PG 5 WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering GA CD2MF UT WOS:000350911800026 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 Dietary Exposure to Individual Polybrominated Diphenyl Ether Congeners BDE-47 and BDE-99 Alters Innate Immunity and Disease Susceptibility in Juvenile Chinook Salmon SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID PERSISTENT ORGANIC POLLUTANTS; TROUT ONCORHYNCHUS-MYKISS; RESPIRATORY BURST; RAINBOW-TROUT; VIBRIO-ANGUILLARUM; FLAME RETARDANTS; GENE-EXPRESSION; THYROID-HORMONE; TELEOST FISH; IN-VITRO AB Polybrominated diphenyl ethers (PBDEs), used as commercial flame-retardants, are bioaccumulating in threatened Pacific salmon. However, little is known of PBDE effects on critical physiological functions required for optimal health and survival. BDE-47 and BDE-99 are the predominant PBDE congeners found in Chinook salmon collected from the Pacific Northwest. In the present study, both innate immunity (phagocytosis and production of superoxide anion) and pathogen challenge were used to evaluate health and survival in groups of juvenile Chinook salmon exposed orally to either BDE-47 or BDE-99 at environmentally relevant concentrations. Head kidney macrophages from Chinook salmon exposed to BDE-99, but not those exposed to BDE-47, were found to have a reduced ability in vitro to engulf foreign particles. However, both congeners increased the in vitro production of superoxide anion in head kidney macrophages. Salmon exposed to either congener had reduced survival during challenge with the pathogenic marine bacteria Listonella anguillarum. The concentration response curves generated for these end points were nonmonotonic and demonstrated a requirement for using multiple environmentally relevant PBDE concentrations for effect studies. Consequently, predicting risk from toxicity reference values traditionally generated with monotonic concentration responses may underestimate PBDE effect on critical physiological functions required for optimal health and survival in salmon. C1 [Arkoosh, Mary R.; Dietrich, Joseph P.] NOAA, Environm & Fisheries Sci Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. [Van Gaest, Ahna L.; Strickland, Stacy A.; Hutchinson, Greg P.; Krupkin, Alex B.] NOAA, Frank Orth & Associates, Under Contract Northwest Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. RP Arkoosh, MR (reprint author), NOAA, Environm & Fisheries Sci Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2032 South East OSU Dr, Newport, OR 97365 USA. EM mary.arkoosh@noaa.gov FU National Oceanic and Atmospheric Administration; US Environmental Protection Agency, 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 the National Oceanic and Atmospheric Administration and the US Environmental Protection Agency, Region 10, Puget Sound Science and Technical Studies Assistance Program (EPA-R10-PS-1004, federal grant no. 13-923270-01). We thank Gina Ylitalo and Lyndal Johnson from NOAA's Northwest Fisheries Science Center as well as Sandra O'Neill from the Washington Department of Fish and Wildlife for their thoughtful comments on the study and review of the manuscript. We thank Carla Stehr for the scanning electron microscopy photo of teleost macrophages engulfing foreign particles used for the TOC art. NR 62 TC 5 Z9 5 U1 13 U2 41 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 JUN 2 PY 2015 VL 49 IS 11 BP 6974 EP 6981 DI 10.1021/acs.est.5b01076 PG 8 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA CJ8UN UT WOS:000355779100072 PM 25938634 ER PT J AU Chapel, J Stancliffe, D Bevacqua, T Winkler, S Clapp, B Rood, T Gaylor, D Freesland, D Krimchansky, A AF Chapel, Jim Stancliffe, Devin Bevacqua, Tim Winkler, Stephen Clapp, Brian Rood, Tim Gaylor, David Freesland, Doug Krimchansky, Alexander TI Guidance, navigation, and control performance for the GOES-R spacecraft SO CEAS SPACE JOURNAL LA English DT Article DE Spacecraft attitude control; Spacecraft pointing; Spacecraft jitter; GPS at GEO ID ATTITUDE AB The Geostationary Operational Environmental Satellite-R series (GOES-R) is the first of the next generation geostationary weather satellites. The series represents a dramatic increase in Earth observation capabilities, with 4 times the resolution, 5 times the observation rate, and 3 times the number of spectral bands. GOES-R also provides unprecedented availability, with less than 120 min per year of lost observation time. This paper presents the guidance navigation & control (GN&C) requirements necessary to realize the ambitious pointing, knowledge, and image navigation and registration (INR) objectives of GOES-. Because the suite of instruments is sensitive to disturbances over a broad spectral range, a high-fidelity simulation of the vehicle has been created with modal content over 500 Hz to assess the pointing stability requirements. Simulation results are presented showing acceleration, shock response spectra, and line-of-sight (LOS) responses for various disturbances from 0 to 512 Hz. Simulation results demonstrate excellent performance relative to the pointing and pointing stability requirements, with LOS jitter for the isolated instrument platform of approximately 1 micro-rad. Attitude and attitude rate knowledge are provided directly to the instrument with an accuracy defined by the integrated rate error requirements. The data are used internally for motion compensation. The final piece of the INR performance is orbit knowledge, which GOES- achieves with GPS navigation. Performance results are shown demonstrating compliance with the 50-75 m orbit position accuracy requirements. As presented in this paper, the GN&C performance supports the challenging mission objectives of GOES-R. C1 [Chapel, Jim; Stancliffe, Devin; Bevacqua, Tim; Winkler, Stephen; Clapp, Brian] Lockheed Martin Space Syst, Denver, CO USA. [Rood, Tim] Adv Solut Inc, Littleton, CO USA. [Gaylor, David] Emergent Space Technol, Greenbelt, MD USA. [Freesland, Doug] ACS Engn, Columbia, MD USA. [Krimchansky, Alexander] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Chapel, J (reprint author), Lockheed Martin Space Syst, Denver, CO USA. EM jim.d.chapel@lmco.com NR 18 TC 4 Z9 5 U1 0 U2 0 PU SPRINGER WIEN PI WIEN PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA SN 1868-2502 EI 1868-2510 J9 CEAS Space J JI CEAS Space J. PD JUN PY 2015 VL 7 IS 2 SI SI BP 87 EP 104 DI 10.1007/s12567-015-0077-1 PG 18 WC Engineering, Aerospace SC Engineering GA DG9YI UT WOS:000372439300003 ER PT J AU San Martin, M Mendeck, GF Brugarolas, PB Singh, G Serricchio, F Lee, SW Wong, EC Essmiller, JC AF San Martin, Miguel Mendeck, Gavin F. Brugarolas, Paul B. Singh, Gurkirpal Serricchio, Frederick Lee, Steven W. Wong, Edward C. Essmiller, John C. TI In-flight experience of the Mars Science Laboratory Guidance, Navigation, and Control system for Entry, Descent, and Landing SO CEAS SPACE JOURNAL LA English DT Article DE EDL; GN&C; Mars; NASA; MSL; Curiosity AB The Mars Science Laboratory (MSL) project successfully landed the rover Curiosity in Gale crater in August 5, 2012, thus demonstrating and validating a series of technical innovations and advances which resulted in a quantum leap in Entry, Descent, and Landing (EDL) performance relative to previous missions. These included the first use at Mars of Entry Guidance to reduce the size of the landing ellipse and the first use of the SkyCrane landing architecture to enable the placement of a 1 ton class rover on the surface of the red planet. Both of these advances required innovations in the design, analysis and testing of the Guidance, Navigation, and Control system. This paper will start with a high-level description of the MSL EDL/GN&C system design and performance requirements, followed by a brief discussion of the risks and uncertainties as they were understood prior to landing, and the actual in-flight GN&C performance as reconstructed from telemetry. Finally, this paper will address areas of improvements for future Mars EDL missions. C1 [San Martin, Miguel; Brugarolas, Paul B.; Singh, Gurkirpal; Serricchio, Frederick; Lee, Steven W.; Wong, Edward C.; Essmiller, John C.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Mendeck, Gavin F.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. RP San Martin, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM alejandro.m.sanmartin@jpl.nasa.gov OI San Martin, Alejandro/0000-0001-6883-3568 NR 17 TC 1 Z9 1 U1 0 U2 1 PU SPRINGER WIEN PI WIEN PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA SN 1868-2502 EI 1868-2510 J9 CEAS Space J JI CEAS Space J. PD JUN PY 2015 VL 7 IS 2 SI SI BP 119 EP 142 DI 10.1007/s12567-015-0091-3 PG 24 WC Engineering, Aerospace SC Engineering GA DG9YI UT WOS:000372439300005 ER PT J AU SunSpiral, V Trimmer, B AF SunSpiral, Vytas Trimmer, Barry TI An Interview with NASA Principal Investigator Vytas SunSpiral: Expert Opinion on the Advantages and Limitations of Soft Robotics SO SOFT ROBOTICS LA English DT Editorial Material AB Vytas SunSpiral is an entrepreneurial researcher moving fluidly between leading startups and building research labs to explore cutting edge robotic technologies. During the last 20 years, he has been the founder and CTO of multiple startups and launched a number of robotics projects at NASA. He has served as an advisor and consultant to startups, and he is currently the Principle Investigator of the Dynamic Tensegrity Robotics Lab (DTRL) at NASA Ames Research Center and is a Fellow of the NASA Innovative Advanced Concepts (NIAC) program. Vytas graduated from Stanford University (1998) with a BA in Symbolic Systems and an MS in Computer Science, with a robotics focus in both. C1 [SunSpiral, Vytas] NASA, Moffett Field, CA USA. [SunSpiral, Vytas] NASA Innovat Adv Concepts NIAC Program, Moffett Field, CA USA. RP SunSpiral, V (reprint author), NASA Ames Res Ctr, Intelligent Syst Div, Intelligent Robot Grp, Dynam Tensegr Robot Lab, Moffett Field, CA 94035 USA. EM vytas.sunspiral@nasa.gov NR 0 TC 0 Z9 0 U1 3 U2 5 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 JUN PY 2015 VL 2 IS 2 BP 51 EP 58 DI 10.1089/soro.2015.28999.btr PG 8 WC Robotics SC Robotics GA CV8XG UT WOS:000364571000002 ER PT J AU Loeffler, MJ Hudson, RL AF Loeffler, Mark J. Hudson, Reggie L. TI Descent without Modification? The Thermal Chemistry of H2O2 on Europa and Other Icy Worlds SO ASTROBIOLOGY LA English DT Article ID WATER-ICE; HYDROGEN-PEROXIDE; CHEMICAL-COMPOSITION; INFRARED SPECTRUM; CRYSTALLINE WATER; SUBSURFACE OCEAN; SULFURIC-ACID; GAS-PHASE; SURFACE; SATELLITES AB The strong oxidant H2O2 is known to exist in solid form on Europa and is suspected to exist on several other Solar System worlds at temperatures below 200 K. However, little is known of the thermal chemistry that H2O2 might induce under these conditions. Here, we report new laboratory results on the reactivity of solid H2O2 with eight different compounds in H2O-rich ices. Using infrared spectroscopy, we monitored compositional changes in ice mixtures during warming. The compounds CH4 (methane), C3H4 (propyne), CH3OH (methanol), and CH3CN (acetonitrile) were unaltered by the presence of H2O2 in ices, showing that exposure to either solid H(2)O(2)or frozen H2O+H2O2 at cryogenic temperatures will not oxidize these organics, much less convert them to CO2. This contrasts strongly with the much greater reactivity of organics with H2O2 at higher temperatures, and particularly in the liquid and gas phases. Of the four inorganic compounds studied, CO, H2S, NH3, and SO2, only the last two reacted in ices containing H2O2, NH3 making NH4+ and SO2 making SO42- by H+ and e(-) transfer, respectively. An important astrobiological conclusion is that formation of surface H2O2 on Europa and that molecule's downward movement with H2O-ice do not necessarily mean that all organics encountered in icy subsurface regions will be destroyed by H2O2 oxidation. Key Words: Europa-Laboratory investigations-Icy moons-Infrared spectroscopy-H2O2 resistance. C1 [Loeffler, Mark J.; Hudson, Reggie L.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. RP Hudson, RL (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Code 691, Greenbelt, MD 20771 USA. EM reggie.hudson@nasa.gov RI Loeffler, Mark/C-9477-2012 FU NASA's Planetary Geology and Geophysics and Outer Planets Research programs; NASA Astrobiology Institute FX The support of NASA's Planetary Geology and Geophysics and Outer Planets Research programs is gratefully acknowledged. The authors particularly acknowledge support from the NASA Astrobiology Institute through a grant to the Goddard Center for Astrobiology. Perry Gerakines is thanked for assistance in day-to-day operations of the equipment in our laboratory. NR 56 TC 0 Z9 0 U1 5 U2 14 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD JUN 1 PY 2015 VL 15 IS 6 BP 453 EP 461 DI 10.1089/ast.2014.1195 PG 9 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA CV0MM UT WOS:000363944800005 PM 26060983 ER PT J AU Schuerger, AC Lee, P AF Schuerger, Andrew C. Lee, Pascal TI Microbial Ecology of a Crewed Rover Traverse in the Arctic: Low Microbial Dispersal and Implications for Planetary Protection on Human Mars Missions SO ASTROBIOLOGY LA English DT Article ID ANTARCTIC RESEARCH STATION; SCIENCE ANALYSIS GROUP; SPACECRAFT SURFACES; BACILLUS-SUBTILIS; UV-IRRADIATION; SURVIVAL; CONTAMINATION; MICROORGANISMS; REGIONS; ENVIRONMENTS AB Between April 2009 and July 2011, the NASA Haughton-Mars Project (HMP) led the Northwest Passage Drive Expedition (NWPDX), a multi-staged long-distance crewed rover traverse along the Northwest Passage in the Arctic. In April 2009, the HMP Okarian rover was driven 496km over sea ice along the Northwest Passage, from Kugluktuk to Cambridge Bay, Nunavut, Canada. During the traverse, crew members collected samples from within the rover and from undisturbed snow-covered surfaces around the rover at three locations. The rover samples and snow samples were stored at subzero conditions (-20 degrees C to -1 degrees C) until processed for microbial diversity in labs at the NASA Kennedy Space Center, Florida. The objective was to determine the extent of microbial dispersal away from the rover and onto undisturbed snow. Interior surfaces of the rover were found to be associated with a wide range of bacteria (69 unique taxa) and fungi (16 unique taxa). In contrast, snow samples from the upwind, downwind, uptrack, and downtrack sample sites exterior to the rover were negative for both bacteria and fungi except for two colony-forming units (cfus) recovered from one downwind (1 cfu; site A4) and one uptrack (1 cfu; site B6) sample location. The fungus, Aspergillus fumigatus (GenBank JX517279), and closely related bacteria in the genus Brevibacillus were recovered from both snow (B. agri, GenBank JX517278) and interior rover surfaces. However, it is unknown whether the microorganisms were deposited onto snow surfaces at the time of sample collection (i.e., from the clothing or skin of the human operator) or via airborne dispersal from the rover during the 12-18h layovers at the sites prior to collection. Results support the conclusion that a crewed rover traveling over previously undisturbed terrain may not significantly contaminate the local terrain via airborne dispersal of propagules from the vehicle. Key Words: Planetary protectionContaminationHabitabilityHaughton CraterMars. Astrobiology 15, xxx-xxx. C1 [Schuerger, Andrew C.] Univ Florida, Space Life Sci Lab, Kennedy Space Ctr, FL 32899 USA. [Lee, Pascal] Mars Inst, Moffett Field, CA USA. [Lee, Pascal] SETI Inst, Moffett Field, CA USA. [Lee, Pascal] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Schuerger, AC (reprint author), Univ Florida, Space Life Sci Lab, Bldg M6-1025, Kennedy Space Ctr, FL 32899 USA. EM schuerg@ufl.edu FU NASA's Planetary Protection Office [NNX12AJ84G, NNX08AQ81A]; NASA's Human Exploration and Operations Mission Directorate (HEOMD) [NNX08AO59A]; Mars Institute; SETI Institute; National Aeronautics and Space Administration (NASA); California Air National Guard; AM General Corporation; Cornell University; Simon Fraser University; University of Alberta; National Space Biomedical Research Institute; Canadian Space Agency; Bombardier, Inc.; First Air, Inc.; Hamilton Sundstrand Corporation; Nunavut Research Institute; Aboriginal Affairs and Northern Development Canada; Polar Continental Shelf Project of Natural Resources Canada; Nunavut community of Kugluktuk; Nunavut community of Cambridge Bay; Nunavut community of Gjoa Haven; Nunavut community of Resolute Bay; Nunavut community of Grise Fiord FX The research was supported by two research grants (NNX12AJ84G and NNX08AQ81A) from NASA's Planetary Protection Office and through a Cooperative Agreement (NNX08AO59A) by NASA's Human Exploration and Operations Mission Directorate (HEOMD). The NASA Haughton-Mars Project and the Northwest Passage Drive Expedition (NWPDX) were sponsored by the Mars Institute, the SETI Institute, and the National Aeronautics and Space Administration (NASA). We would like to thank W.L. Nicholson for his suggestions on 16S and 18S sequencing protocols and the loan of specialized equipment for a portion of the lab work described herein. Thanks are also owed to the many other sponsors and supporters of the NWPDX expedition including the California Air National Guard; AM General Corporation; Cornell University; Simon Fraser University; University of Alberta; the National Space Biomedical Research Institute; the Canadian Space Agency, Bombardier, Inc.; First Air, Inc.; Hamilton Sundstrand Corporation; the Nunavut Research Institute; Aboriginal Affairs and Northern Development Canada; the Polar Continental Shelf Project of Natural Resources Canada; and the Nunavut communities of Kugluktuk, Cambridge Bay, Gjoa Haven, Resolute Bay, and Grise Fiord. Pascal Lee expresses special thanks to NWPDX-2009 field team members John W. Schutt, Joe Amarualik, Jesse T. Weaver, and Mark Carroll for the excellent support and enthusiasm during the NWPDX-2009 traverse. Kira Lorber and Stephen Braham are thanked for logistics and communications support, respectively. NR 49 TC 3 Z9 3 U1 3 U2 17 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD JUN 1 PY 2015 VL 15 IS 6 BP 478 EP 491 DI 10.1089/ast.2015.1289 PG 14 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA CV0MM UT WOS:000363944800007 PM 26060984 ER PT J AU Alwood, JS Shahnazari, M Chicana, B Schreurs, AS Kumar, A Bartolini, A Shirazi-Fard, Y Globus, RK AF Alwood, Joshua S. Shahnazari, Mohammad Chicana, Betsabel Schreurs, A. S. Kumar, Akhilesh Bartolini, Alana Shirazi-Fard, Yasaman Globus, Ruth K. TI Ionizing Radiation Stimulates Expression of Pro-Osteoclastogenic Genes in Marrow and Skeletal Tissue SO JOURNAL OF INTERFERON AND CYTOKINE RESEARCH LA English DT Article ID LONG-DURATION SPACEFLIGHT; KAPPA-B LIGAND; BONE-RESORPTION; MUSCULOSKELETAL DISUSE; RECEPTOR ACTIVATOR; OXIDATIVE STRESS; CANCELLOUS BONE; MURINE MODEL; T-CELLS; DIFFERENTIATION AB Exposure to ionizing radiation can cause rapid mineral loss and increase bone-resorbing osteoclasts within metabolically active, cancellous bone tissue leading to structural deficits. To better understand mechanisms involved in rapid, radiation-induced bone loss, we determined the influence of total body irradiation on expression of select cytokines known both to stimulate osteoclastogenesis and contribute to inflammatory bone disease. Adult (16 week), male C57BL/6J mice were exposed to either 2Gy gamma rays (Cs-137, 0.8Gy/min) or heavy ions (Fe-56, 600MeV, 0.50-1.1Gy/min); this dose corresponds to either a single fraction of radiotherapy (typical total dose is 10Gy) or accumulates over long-duration interplanetary missions. Serum, marrow, and mineralized tissue were harvested 4h7 days later. Gamma irradiation caused a prompt (2.6-fold within 4h) and persistent (peaking at 4.1-fold within 1 day) rise in the expression of the obligate osteoclastogenic cytokine, receptor activator of nuclear factor kappa-B ligand (Rankl), within marrow cells over controls. Similarly, Rankl expression peaked in marrow cells within 3 days of iron exposure (9.2-fold). Changes in Rankl expression induced by gamma irradiation preceded and overlapped with a rise in expression of other pro-osteoclastic cytokines in marrow (eg, monocyte chemotactic protein-1 increased by 11.9-fold, and tumor necrosis factor-alpha increased by 1.7-fold over controls). The ratio, Rankl/Opg, in marrow increased by 1.8-fold, a net pro-resorption balance. In the marrow, expression of the antioxidant transcription factor, Nfe2l2, strongly correlated with expression levels of Nfatc1, Csf1, Tnf, and Rankl. Radiation exposure increased a serum marker of bone resorption (tartrate-resistant acid phosphatase) and led to cancellous bone loss (16% decrement after 1 week). We conclude that total body irradiation (gamma or heavy-ion) caused temporal elevations in the concentrations of specific genes expressed within marrow and mineralized tissue related to bone resorption, including select cytokines that lead to osteoclastogenesis and elevated resorption; this is likely to account for rapid and progressive deterioration of cancellous microarchitecture following exposure to ionizing radiation. C1 [Alwood, Joshua S.; Shahnazari, Mohammad; Chicana, Betsabel; Schreurs, A. S.; Kumar, Akhilesh; Bartolini, Alana; Shirazi-Fard, Yasaman; Globus, Ruth K.] NASA, Ames Res Ctr, Bone & Signaling Lab, Space Biosci Div, Moffett Field, CA 94035 USA. RP Globus, RK (reprint author), NASA, Ames Res Ctr, Bone & Signaling Lab, Space Biosci Div, Mail Stop 236-7, Moffett Field, CA 94035 USA. EM ruth.k.globus@nasa.gov FU National Space Biomedical Research Institute under NASA [MA02501, NCC 9-58]; DOE-NASA - Office of Science (Biological and Environmental Research), U.S. Department of Energy [DE-SC0001507]; 2 NASA Postdoctoral Program fellowships from NASA's Space Biology Program FX This research was supported by the National Space Biomedical Research Institute grant No. MA02501 under NASA cooperative agreement NCC 9-58 (R.K.G., J.S.A.), a DOE-NASA Interagency Award No. DE-SC0001507, supported by the Office of Science (Biological and Environmental Research), U.S. Department of Energy (R.K.G.), and 2 NASA Postdoctoral Program fellowships from NASA's Space Biology Program (J.S.A., A.K). The authors thank P. Guida, A. Rusek, L. Loudenslager, and A. Kim of the NASA Space Radiation Laboratory at BNL for experimental support and S. Choi and T. Truong for microcomputed tomography support and C. Tahimic for manuscript review. NR 46 TC 1 Z9 1 U1 4 U2 8 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1079-9907 EI 1557-7465 J9 J INTERF CYTOK RES JI J. Interferon Cytokine Res. PD JUN 1 PY 2015 VL 35 IS 6 BP 480 EP 487 DI 10.1089/jir.2014.0152 PG 8 WC Biochemistry & Molecular Biology; Cell Biology; Immunology SC Biochemistry & Molecular Biology; Cell Biology; Immunology GA CU9RR UT WOS:000363883100008 PM 25734366 ER PT J AU Price, H Baker, J Naderi, F AF Price, Hoppy Baker, John Naderi, Firouz TI A Minimal Architecture for Human Journeys to Mars SO NEW SPACE LA English DT Article AB Proposed architectures for human journeys to Mars need to take note of the two competing constraints of an executable program: the annual NASA human spaceflight budget will likely remain constrained (possibly growing with inflation), and going to Mars and landing on Mars need to happen within the interest horizon of the various stakeholders, including the public. In this article we describe a stepwise approach for human journeys to Mars using a minimal architecture. We refer to this architecture as minimal because it would minimize large new development efforts and rely largely on elements currently being developed or planned by NASA, such as SLS, Orion, a deep space habitat, and a 100-kWe-class SEP tug. In the architecture proposed here, human missions to Mars would begin with a crewed landing on Phobos in 2033, followed by a short-stay landing on Mars in 2039, and continue with a one-year stay in 2043. Each mission campaign would build on previous campaigns, leaving a legacy and new capabilities for those that follow. A first look independent cost assessment by the Aerospace Corporation suggests that this example could plausibly fit within an inflation-adjusted budget. Furthermore, although not considered here, international contributions could offset some of the cost. C1 [Price, Hoppy; Baker, John; Naderi, Firouz] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Price, H (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-170S, Pasadena, CA 91109 USA. EM Humphrey.W.Price@jpl.nasa.gov NR 2 TC 3 Z9 3 U1 2 U2 6 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 2168-0256 EI 2168-0264 J9 NEW SPACE JI New Space PD JUN 1 PY 2015 VL 3 IS 2 BP 73 EP 81 DI 10.1089/space.2015.0018 PG 9 WC Engineering, Aerospace SC Engineering GA CV0ID UT WOS:000363933100002 ER PT J AU Lee, JH Lin, KC Eklund, D AF Lee, Jinho Lin, Kuo-Cheng Eklund, Dean TI Challenges in Fuel Injection for High-Speed Propulsion Systems SO AIAA JOURNAL LA English DT Article ID SUPERSONIC CROSS-FLOWS; INDUCED IODINE FLUORESCENCE; LARGE-EDDY SIMULATION; LIQUID JETS; TRANSVERSE INJECTION; AEROSPACE PROPULSION; TURBULENT PRANDTL; SCRAMJET ENGINES; SCHMIDT NUMBERS; PRIMARY BREAKUP C1 [Lee, Jinho] NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA. [Lin, Kuo-Cheng] Taitech Inc, Beavercreek, OH 45430 USA. [Eklund, Dean] US Air Force, Res Lab, Wright Patterson AFB, OH 45433 USA. RP Lee, JH (reprint author), NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA. FU Hypersonic Propulsion Element of Fundamental Hypersonic Program; U.S. Air Force Research Laboratory's Robust Scramjet Program FX This work was sponsored by the Hypersonic Propulsion Element of the Fundamental Hypersonic Program under the leadership of A. Auslander and R. Gaffney (Associate Principal Investigators) and J. Pittman (Principal Investigator). The sponsorship of T. Jackson and R. Mercier under the auspices of the U.S. Air Force Research Laboratory's Robust Scramjet Program is also gratefully acknowledged. NR 121 TC 0 Z9 0 U1 2 U2 6 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 JUN PY 2015 VL 53 IS 6 BP 1405 EP 1423 DI 10.2514/1.J053280 PG 19 WC Engineering, Aerospace SC Engineering GA CH9WD UT WOS:000354386200001 ER PT J AU Jones, MG Watson, WR Howerton, BM Busse-Gerstengarbe, S AF Jones, M. G. Watson, W. R. Howerton, B. M. Busse-Gerstengarbe, S. TI Effects of Mean Flow Assumption and Harmonic Distortion on Impedance Eduction Methods SO AIAA JOURNAL LA English DT Article ID GRAZING FLOW; BOUNDARY-CONDITION; LINER IMPEDANCE; VALIDATION; DUCT AB This investigation uses methods based on the Pridmore-Brown and convected Helmholtz equations to study the acoustic behavior of a single-layer, conventional liner fabricated by DLR, German Aerospace Center and tested in the NASA Langley Grazing Flow Impedance Tube. Two key assumptions are explored in this investigation. First, a comparison of results achieved with uniform-flow and shear-flow impedance eduction methods is considered. Second, an approach based on the Prony method is used to extend these methods from single-mode to multimode implementations. In addition, a detailed study into the effects of harmonic distortion on the educed impedance is performed, and the results are used to develop guidelines regarding acceptable levels of harmonic distortion. C1 [Jones, M. G.; Howerton, B. M.] NASA, Langley Res Ctr, Struct Acoust Branch, Res Directorate, Hampton, VA 23681 USA. [Watson, W. R.] NASA, Langley Res Ctr, Computat AeroSci Branch, Res Directorate, Hampton, VA 23681 USA. [Busse-Gerstengarbe, S.] Tech Univ Berlin, Inst Fluid Mech & Engn Acoust, D-10623 Berlin, Germany. RP Jones, MG (reprint author), NASA, Langley Res Ctr, Struct Acoust Branch, Res Directorate, Hampton, VA 23681 USA. FU NASA; German Research Foundation [TH 288/35-1] FX The authors wish to express their appreciation to Carl Gerhold and Chris Jasinski for their support in the implementation of the multimode impedance eduction method and to Jason June for his support with implementation of the shear-flow assumption. This research was funded by the Fixed Wing Project of NASA's Fundamental Aeronautics Program. Support for S. Busse-Gerstengarbe was provided by the German Research Foundation as part of the UNLIMITED Project (TH 288/35-1). NR 20 TC 1 Z9 1 U1 0 U2 0 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD JUN PY 2015 VL 53 IS 6 BP 1503 EP 1514 DI 10.2514/1.J053399 PG 12 WC Engineering, Aerospace SC Engineering GA CH9WD UT WOS:000354386200009 ER PT J AU Mankbadi, MR Georgiadis, NJ AF Mankbadi, M. R. Georgiadis, N. J. TI Examination of Parameters Affecting Large-Eddy Simulations of Flow Past a Square Cylinder SO AIAA JOURNAL LA English DT Article C1 [Mankbadi, M. R.; Georgiadis, N. J.] NASA, John H Glenn Res Ctr, Inlet & Nozzle Branch, Cleveland, OH 44135 USA. RP Mankbadi, MR (reprint author), NASA, John H Glenn Res Ctr, Inlet & Nozzle Branch, 21000 Brookpk Rd, Cleveland, OH 44135 USA. FU Rotary Wing Project; Aeronautical Sciences Project under the Fundamental Aeronautics Program FX This work was supported by the Rotary Wing Project and the Aeronautical Sciences Project under the Fundamental Aeronautics Program. Special thanks to J. R. DeBonis, D. A. Yoder, and G. E. Welch for their advice. NR 7 TC 2 Z9 2 U1 1 U2 3 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD JUN PY 2015 VL 53 IS 6 BP 1706 EP 1711 DI 10.2514/1.J053684 PG 6 WC Engineering, Aerospace SC Engineering GA CH9WD UT WOS:000354386200024 ER PT J AU Bouhenni, R Dunmire, J Liu, Y Rafiq, Q Gothard, D King, J Naiman, M Ansari, R Edward, DP AF Bouhenni, Rachida Dunmire, Jeffrey Liu, Ying Rafiq, Qundeel Gothard, David King, James Naiman, Melissa Ansari, Rafat Edward, Deepak P. TI Identification of Molecular Signatures in Vitreous Humor Following Laser Exposure using Dynamic Light Scattering SO INVESTIGATIVE OPHTHALMOLOGY & VISUAL SCIENCE LA English DT Meeting Abstract CT Annual Meeting of the Association-for-Research-in-Vision-and-Ophthalmology (ARVO) CY MAY 03-07, 2015 CL Denver, CO SP Assoc Res Vis & Ophthalmol C1 [Bouhenni, Rachida; Dunmire, Jeffrey] Summa Hlth Syst, Ophthalmol, Akron, OH USA. [Liu, Ying; Rafiq, Qundeel; Edward, Deepak P.] Johns Hopkins Univ, Baltimore, MD USA. [Gothard, David] BIOSTATS, Akron, OH USA. [King, James; Ansari, Rafat] NASA, Glenn Res Ctr, Cleveland, OH USA. [Naiman, Melissa] Univ Illinois, Chicago, IL USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU ASSOC RESEARCH VISION OPHTHALMOLOGY INC PI ROCKVILLE PA 12300 TWINBROOK PARKWAY, ROCKVILLE, MD 20852-1606 USA SN 0146-0404 EI 1552-5783 J9 INVEST OPHTH VIS SCI JI Invest. Ophthalmol. Vis. Sci. PD JUN PY 2015 VL 56 IS 7 MA 4630 PG 3 WC Ophthalmology SC Ophthalmology GA CT5ZY UT WOS:000362891103411 ER PT J AU Ethier, CR Feola, A Raykin, J Mulugeta, L Gleason, R Myers, JG Nelson, ES Samuels, B AF Ethier, C. Ross Feola, Andrew Raykin, Julia Mulugeta, Lealem Gleason, Rudy Myers, Jerry G. Nelson, Emily S. Samuels, Brian TI Modeling the Effects of Spaceflight on the Posterior Eye in VIIP SO INVESTIGATIVE OPHTHALMOLOGY & VISUAL SCIENCE LA English DT Meeting Abstract CT Annual Meeting of the Association-for-Research-in-Vision-and-Ophthalmology (ARVO) CY MAY 03-07, 2015 CL Denver, CO SP Assoc Res Vis & Ophthalmol C1 [Ethier, C. Ross; Feola, Andrew; Raykin, Julia; Gleason, Rudy] Georgia Inst Technol, Biomed Engn, Atlanta, GA 30332 USA. [Mulugeta, Lealem] Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA. [Myers, Jerry G.; Nelson, Emily S.] NASA Glenn Res Ctr, Cleveland, OH USA. [Samuels, Brian] Univ Alabama Birmingham, Ophthalmol, Birmingham, AL USA. NR 0 TC 0 Z9 0 U1 2 U2 2 PU ASSOC RESEARCH VISION OPHTHALMOLOGY INC PI ROCKVILLE PA 12300 TWINBROOK PARKWAY, ROCKVILLE, MD 20852-1606 USA SN 0146-0404 EI 1552-5783 J9 INVEST OPHTH VIS SCI JI Invest. Ophthalmol. Vis. Sci. PD JUN PY 2015 VL 56 IS 7 MA 4825 PG 3 WC Ophthalmology SC Ophthalmology GA CT5ZY UT WOS:000362891104183 ER PT J AU Parsons-Wingerter, PA Radhakrishnan, K Chalam, KV Grant, MB AF Parsons-Wingerter, Patricia A. Radhakrishnan, Krishnan Chalam, K. V. Grant, Maria B. TI VESGEN Analysis of Generational Branching Patterns in Arteries and Veins for Investigating Diabetic Retinopathy by Spectralis Angiographic Imaging SO INVESTIGATIVE OPHTHALMOLOGY & VISUAL SCIENCE LA English DT Meeting Abstract CT Annual Meeting of the Association-for-Research-in-Vision-and-Ophthalmology (ARVO) CY MAY 03-07, 2015 CL Denver, CO SP Assoc Res Vis & Ophthalmol C1 [Parsons-Wingerter, Patricia A.] NASA, Ames Res Ctr, Space Biosci Res Branch, Moffett Field, CA 94035 USA. [Radhakrishnan, Krishnan] Univ Kentucky, Internal Med, Lexington, KY USA. [Chalam, K. V.] Univ Florida, Ophthalmol, Jacksonville, FL USA. [Grant, Maria B.] Indiana Univ, Glick Eye Inst, Ophthalmol, Indianapolis, IN 46204 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASSOC RESEARCH VISION OPHTHALMOLOGY INC PI ROCKVILLE PA 12300 TWINBROOK PARKWAY, ROCKVILLE, MD 20852-1606 USA SN 0146-0404 EI 1552-5783 J9 INVEST OPHTH VIS SCI JI Invest. Ophthalmol. Vis. Sci. PD JUN PY 2015 VL 56 IS 7 MA 5960 PG 2 WC Ophthalmology SC Ophthalmology GA CT5ZY UT WOS:000362891107029 ER PT J AU Youngquist, RC Nurge, MA Johnson, WL Starr, SO AF Youngquist, Robert C. Nurge, Mark A. Johnson, Wesley L. Starr, Stanley O. TI Modeling Transmission Effects on Multilayer Insulation SO JOURNAL OF THERMAL SCIENCE AND ENGINEERING APPLICATIONS LA English DT Article ID REFLECTANCE; ALUMINUM AB Multilayer insulation (MLI), commonly used in cryogenics, is typically composed of many layers of thin polymer sheets each coated with a thin film of highly reflective metal. The primary purpose of this insulation is to block radiative energy transfer. However, at very low temperatures where blackbody radiation occurs at long wavelengths, some energy may be transmitted through these layers, degrading the performance of the insulation. Traditional modeling techniques assume that the films are opaque and are not easily extended to include radiative transmission through the layers. In order to model the effect of wavelength dependent transmission on the thermal performance of MLI, an L1-norm energy vector is defined and combined with a square energy distribution matrix. The key here is that the energy distribution matrix describes one time step of the radiation-one set of reflections, transmissions, and absorptions-and since this matrix is square, it can be easily raised to a large power, describing the final state of the system quickly. This approach removes the need to track every reflected and transmitted radiation element, but instead determines the eventual location where the thermal radiation energy is deposited. This method can be generalized to model dependence of the reflection and transmission of the radiation on wavelength or angle of propagation, to include thermal conduction effects, and to model transient behavior. The results of this work predict the degree of transmission dependent degradation expected to be seen when using state-of-the-art MLI in low temperature cryogenic systems. C1 [Youngquist, Robert C.; Nurge, Mark A.; Starr, Stanley O.] NASA, KSC Appl Phys Lab NE L5, Kennedy Space Ctr, FL 32899 USA. [Johnson, Wesley L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Nurge, MA (reprint author), NASA, KSC Appl Phys Lab NE L5, Kennedy Space Ctr, FL 32899 USA. EM robert.c.youngquist@nasa.gov; mark.a.nurge@nasa.gov; wesley.l.johnson@nasa.gov; stanley.o.starr@nasa.gov FU NASA's Advanced Exploration Systems Program FX This work was funded by NASA's Advanced Exploration Systems Program. NR 13 TC 2 Z9 2 U1 3 U2 5 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 JUN PY 2015 VL 7 IS 2 AR 021007 DI 10.1115/1.4028570 PG 7 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA CU2WP UT WOS:000363384700007 ER PT J AU Zhu, YQ Toon, OB Lambert, A Kinnison, DE Brakebusch, M Bardeen, CG Mills, MJ English, JM AF Zhu, Yunqian Toon, Owen B. Lambert, Alyn Kinnison, Douglas E. Brakebusch, Matthias Bardeen, Charles G. Mills, Michael J. English, Jason M. TI Development of a Polar Stratospheric Cloud Model within the Community Earth System Model using constraints on Type I PSCs from the 2010-2011 Arctic winter SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS LA English DT Article ID NITRIC-ACID TRIHYDRATE; LARGE HNO3-CONTAINING PARTICLES; CHEMICAL-TRANSPORT MODEL; OZONE LOSS; ATMOSPHERIC CHEMISTRY; H2SO4/HNO3/H2O SOLUTIONS; HETEROGENEOUS REACTIONS; TOMOGRAPHIC APPROACH; CHLORINE ACTIVATION; PHYSICAL PROCESSES AB Polar stratospheric clouds (PSCs) are critical elements of Arctic and Antarctic ozone depletion. We establish a PSC microphysics model using coupled chemistry, climate, and microphysics models driven by specific dynamics. We explore the microphysical formation and evolution of STS (Supercooled Ternary Solution) and NAT (Nitric Acid Trihydrate). Characteristics of STS particles dominated by thermodynamics compare well with observations. For example, the mass of STS is close to the thermodynamic equilibrium assumption when the particle surface area is >4 mu m(2)/cm(3). We derive a new nucleation rate equation for NAT based on observed denitrification in the 2010-2011 Arctic winter. The homogeneous nucleation scheme leads to supermicron NAT particles as observed. We also find that as the number density of NAT particles increases, the denitrification also increases. Simulations of the PSC lidar backscatter, denitrification, and gas phase species are generally within error bars of the observations. However, the simulations are very sensitive to temperature, which limits our ability to fully constrain some parameters (e.g., denitrification, ozone amount) based on observations. C1 [Zhu, Yunqian; Toon, Owen B.; Brakebusch, Matthias; English, Jason M.] Univ Colorado, Lab Atmospher & Space Phys, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA. [Lambert, Alyn] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Kinnison, Douglas E.; Bardeen, Charles G.; Mills, Michael J.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. RP Zhu, YQ (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA. EM yunqian.zhu@colorado.edu RI Mills, Michael/B-5068-2010; English, Jason/E-9365-2015 OI Mills, Michael/0000-0002-8054-1346; English, Jason/0000-0001-9700-6860 FU NASA [NNX09AK71G]; AURA satellite project; National Science Foundation; National Science Foundation [CNS-0821794]; University of Colorado Boulder FX MIPAS data are from the MIPAS2D database (www.isac.cnr.it/similar to rss/mipas2d.htm). We thank E. Arnone for his help with the MIPAS data. Data are provided courtesy of the National Centre for Earth Observation via the NERC Earth Observation Data Centre (NEODC). The work at the University of Colorado was supported by NASA grant NNX09AK71G, as well as a grant from the AURA satellite project. Work at the Jet Propulsion Laboratory, California Institute of Technology, was carried out under a contract with the National Aeronautics and Space Administration. We thank Lynn Harvey for her help with the MLS data. We thank Michael Pitts for his help with the CALIPSO PSC cloud coverage retrieval. We thank Stephan Borrmann and his group for their help with the PSC size data from the RECONCILE campaign. This work utilized the Yellowstone and Janus supercomputer. We would like to acknowledge high-performance computing support from Yellowstone (ark:/85065/d7wd3xhc) provided by NCAR's Computational and Information Systems Laboratory, sponsored by the National Science Foundation. Janus is supported by the National Science Foundation (award CNS-0821794) and the University of Colorado Boulder. The Janus supercomputer is a joint effort of the University of Colorado Boulder, the University of Colorado Denver and the National Center for Atmospheric Research. NR 135 TC 3 Z9 3 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1942-2466 J9 J ADV MODEL EARTH SY JI J. Adv. Model. Earth Syst. PD JUN PY 2015 VL 7 IS 2 BP 551 EP 585 DI 10.1002/2015MS000427 PG 35 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CQ7ZH UT WOS:000360825000010 ER PT J AU Borghesi, G Mastorakos, E AF Borghesi, Giulio Mastorakos, Epaminondas TI Spontaneous ignition of isolated n-heptane droplets at low, intermediate, and high ambient temperatures from a mixture-fraction perspective SO COMBUSTION AND FLAME LA English DT Article DE Single droplet; Detailed numerical simulation; Complex chemistry; Microgravity; Autoignition ID DETAILED NUMERICAL SIMULATIONS; CONDITIONAL MOMENT CLOSURE; MICROGRAVITY EXPERIMENTS; SPRAY COMBUSTION; AUTOIGNITION; FLAMES; METHANOL; EVAPORATION; CHEMISTRY; TRANSPORT AB Detailed numerical simulations of isolated n-heptane droplets autoignition have been conducted at pressures of 5 and 10 atm for several values of the initial ambient gas temperature. The ignition modes considered included low-, intermediate-, and high-temperature ignition. The analysis was conducted from a mixture-fraction perspective. For sufficiently low values of the ambient gas temperature, two-stage ignition was observed. Under these conditions, low-temperature reactions played an important role in the transition of the system to a fully burning state. As the initial value of the ambient gas temperature increased, the influence of the low-temperature reactions on the ignition process decreased and eventually became marginal for temperatures above 900 K. Comparisons against homogeneous reactor calculations showed that the ignition location in mixture fraction space could be reasonably predicted for the high-temperature case, whereas discrepancies occurred for the intermediate- and low-temperature ones due to the shift in the maximum reactivity of the system caused by the cool flame appearance. The dependence of the ignition process on the initial droplet diameter was also studied for different values of the initial ambient gas temperature. It was found that, for all cases investigated, a value of the droplet diameter existed for which ignition took the least time to occur. For smaller droplets, the ignition transient was longer and eventually a burning flame did no longer appear when the droplet was initially too small. For the low-temperature case, the minimum ignition delay time was determined by the competition between the quicker ignition of the cool flame and the longer second induction time resulting from the decrease in the droplet size: for the high-temperature case, it was the results of phenomena occurring early during the droplet lifetime. (C) 2015 The Combustion Institute. Published by Elsevier Inc. All rights reserved. C1 [Borghesi, Giulio] CALTECH, Dept Civil & Mech Engn, Pasadena, CA 91125 USA. [Mastorakos, Epaminondas] Univ Cambridge, Dept Engn, Cambridge CB2 1PZ, England. RP Borghesi, G (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 125-130, Pasadena, CA 91109 USA. EM Giulio.Borghesi@jpl.nasa.gov OI Mastorakos, Epaminondas/0000-0001-8245-5188 NR 46 TC 4 Z9 4 U1 3 U2 21 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 JUN PY 2015 VL 162 IS 6 BP 2544 EP 2560 DI 10.1016/j.combustflame.2015.03.003 PG 17 WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary; Engineering, Chemical; Engineering, Mechanical SC Thermodynamics; Energy & Fuels; Engineering GA CQ4RP UT WOS:000360592600021 ER PT J AU Shaver, DJ Caillouet, CW AF Shaver, Donna J. Caillouet, Charles W., Jr. TI REINTRODUCTION OF KEMP'S RIDLEY (LEPIDOCHELYS KEMPII) SEA TURTLE TO PADRE ISLAND NATIONAL SEASHORE, TEXAS AND ITS CONNECTION TO HEAD-STARTING SO HERPETOLOGICAL CONSERVATION AND BIOLOGY LA English DT Article DE conservation; head-start; Lepidochelys kempii; nesting; satellite tracking ID GULF-OF-MEXICO; NORTHWESTERN GULF; HEADSTART PROJECT; RANCHO-NUEVO; CONSERVATION; MANAGEMENT; RECOVERY; MODELS; COAST; WILD AB Kemp's Ridley (Lepidochelys kempii) is the most endangered of the sea turtles. Most nesting is on the Gulf of Mexico coastline from Texas, USA, through Veracruz, Mexico, with greatest numbers near Playa de Rancho Nuevo (RN), Tamaulipas, Mexico. The Mexican government began protecting nesters, eggs, and hatchlings at RN in 1966, but annual numbers of nests continued to decline. In January 1978, the U.S. National Park Service (NPS), Fish and Wildlife Service (FWS), and National Marine Fisheries Service (NMFS), the Texas Parks and Wildlife Department (TPWD), and the Instituto Nacional de Pesca (INP) of Mexico implemented a bi-national Kemp's Ridley restoration and enhancement program (KRREP) for the NPS Padre Island National Seashore (PAIS) near Corpus Christi, Texas, and RN. Its planned goals were to reintroduce Kemp's Ridley to PAIS, which included head-starting, and to enhance protection of Kemp's Ridley nesters, eggs, and hatchlings at RN. This paper summarizes collecting, transporting, and incubating eggs, attempted imprinting of eggs and hatchlings, transporting hatchlings, tracking nesters, and documenting nestings in the wild. Through 2014, 20 Padre Island imprinted head-started turtles (n = 69 nests) and 39 RN imprinted head-started turtles (n = 64 nests) were recorded nesting in Texas (n = 125 nests) and near RN (n = 8 nests). C1 [Shaver, Donna J.] Natl Pk Serv, Padre Isl Natl Seashore, Corpus Christi, TX 78480 USA. [Caillouet, Charles W., Jr.] Natl Marine Fisheries Serv, Galveston Lab, Galveston, TX 77551 USA. RP Shaver, DJ (reprint author), Natl Pk Serv, Padre Isl Natl Seashore, POB 181300, Corpus Christi, TX 78480 USA. EM donna_shaver@nps.gov; waxmanjr@aol.com FU NPS; NMFS; FWS; TPWD; INP; CONANP; SEMARNAT; Animal Rehabilitation Keep (ARK); City of Corpus Christi; Friends of Aransas and Matagorda Island National Wildlife Refuges (FAMI); Gladys Porter Zoo, HEART/Sea Turtle Restoration Project; National Fish and Wildlife Foundation; National Park Foundation; Natural Resource Damage Assessment (NRDA); Norcross Wildlife Foundation; Sea Turtle, Inc.; Shell Oil Company Foundation; Texas General Land Office; TAMUG; Texas Master Naturalists, Unilever HPC-USA; U.S. Geological Survey; University of Alabama at Birmingham; University of Charleston; University of Texas FX Various components of the work were funded and permitted by NPS, NMFS, FWS, TPWD, and INP (and its successor agencies including CONANP and SEMARNAT). Bryan Arroyo, Richard Byles, Kelsey Gocke, Mike Ray, Tom Shearer, Catherine Yeargan, and others aided with FWS and TPWD permitting and support. Work by PAIS personnel was authorized under FWS Permit TE840727-3, TPWD Scientific Permit SPR-0190-122, and NPS Institutional Animal Care Protocols NPS IACUC 2011-15.; Animal Rehabilitation Keep (ARK), City of Corpus Christi, Friends of Aransas and Matagorda Island National Wildlife Refuges (FAMI), Gladys Porter Zoo, HEART/Sea Turtle Restoration Project, National Fish and Wildlife Foundation, National Park Foundation, Natural Resource Damage Assessment (NRDA), Norcross Wildlife Foundation, Sea Turtle, Inc., Shell Oil Company Foundation, Texas General Land Office, TAMUG, Texas Master Naturalists, Unilever HPC-USA, U.S. Geological Survey, University of Alabama at Birmingham, University of Charleston, University of Texas, and others provided assistance or funding for activities in Texas. NR 188 TC 5 Z9 6 U1 2 U2 17 PU HERPETOLOGICAL CONSERVATION & BIOLOGY PI CORVALLIS PA C/O R BRUCE BURY, USGS FOREST & RANGELAND, CORVALLIS, OR 00000 USA SN 2151-0733 EI 1931-7603 J9 HERPETOL CONSERV BIO JI Herpetol. Conserv. Biol. PD JUN PY 2015 VL 10 IS 1 BP 378 EP 435 PG 58 WC Zoology SC Zoology GA CQ1QK UT WOS:000360373100026 ER PT J AU Sundaresan, A Marriott, K Mao, J Bhuiyan, S Denkins, P AF Sundaresan, A. Marriott, K. Mao, J. Bhuiyan, S. Denkins, P. TI The Effects of Benzofuran-2-Carboxylic Acid Derivatives as Countermeasures in Immune Modulation and Cancer Cell Inhibition SO MICROGRAVITY SCIENCE AND TECHNOLOGY LA English DT Article DE Immune suppression; Microgravity; Benzofurans; Countermeasures; Radiation; Apoptosis ID INDUCED GENOMIC INSTABILITY; IONIZING-RADIATION; ANTITUMOR-ACTIVITY; MICROGRAVITY; EXPRESSION; ANALOGS; INCREASES AB Microgravity and radiation exposure experienced during space flights result in immune system suppression. In long-term spaceflight, the crew is exposed to space radiation, microgravity, infectious agents from other crew members, and microbial contamination, all of which have a significant impact on the body's immune system and may contribute to the development of autoimmune diseases, allergic reactions, and/or cancer initiation. Many studies have revealed strong effects of microgravity on immune cell function, and microgravity is now considered as one of the major causes of immune dysfunction during space flight (Sundaresan, Int. J. Transp. Phenom. 12(1-2), 93-100, 2011; Martinelli et al., IEEE Eng. Biol. Med. 28(4), 85-90, 2009). We screened two newly synthetized derivatives of benzofuran 2-carboxylic acid, KMEG and KM12. The former KMEG was assessed for lymphoproliferative activities while the latter, KM12, was used in an array of cancer cell lines for testing its cancer inhibiting effects. For ground-based studies, synthetic benzofuran-2-carboxylic acid derivatives were assessed for biological effects in several scenarios, which involved exposure to modeled microgravity and radiation, as well as their immune enhancement and anti-cancer effects. Initial findings indicate that the benzofuran-2-carboxylic acid derivatives possibly have immune enhancing and anti-tumor properties in human lymphocytes and cancer cells exposed to analog spaceflight conditions modeled microgravity and gamma-radiation). C1 [Sundaresan, A.] Texas So Univ, Houston, TX 77004 USA. [Marriott, K.] Savannah State Univ, Savannah, GA 31404 USA. [Mao, J.] Tougaloo Coll, Jackson, MS 39174 USA. [Bhuiyan, S.] Jarvis Christian Coll, Hawkins, TX 75765 USA. [Denkins, P.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Sundaresan, A (reprint author), Texas So Univ, Houston, TX 77004 USA. EM sundaresana@TSU.EDU NR 32 TC 0 Z9 0 U1 1 U2 7 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 JUN PY 2015 VL 27 IS 3 BP 129 EP 140 DI 10.1007/s12217-014-9408-7 PG 12 WC Engineering, Aerospace; Thermodynamics; Mechanics SC Engineering; Thermodynamics; Mechanics GA CP0FA UT WOS:000359550000001 ER PT J AU DiLisi, G Dempsey, R Rarick, R Rosenblatt, C AF DiLisi, Gregory Dempsey, Robert Rarick, Richard Rosenblatt, Charles TI Using Parabolic Flights to Examine Quantitatively the Stability of Liquid Bridges under Varying Total Body Force SO MICROGRAVITY SCIENCE AND TECHNOLOGY LA English DT Article DE Bond number; Liquid bridges; Microgravity; Parabolic flights ID ARBITRARY VOLUME; MINIMUM VOLUME; EQUAL DISKS; GRAVITY; DYNAMICS; FIELDS; LIMIT; LONG AB Liquid bridges were flown aboard a Boeing 727-200 aircraft in a series of parabolic arcs that produced multiple periods of microgravity. During the microgravity portion of each arc, g(eff), the effective total body acceleration due to external forces became negligibly small so that cylindrical liquid bridges could be suspended across two coaxial support posts. Near the bottom of each arc, g(eff) slowly increased to a maximum of 1.84g, causing the liquid bridges to deform and in some cases collapse. Although the physics of liquid bridges subject to varying total body force is well-established and has been analyzed extensively both theoretically and experimentally, specific hardware was designed to vary g(eff) in a precise way that overcomes the gravity-related limitations and high g-jitter associated with parabolic flights. Bridge-stability was examined for axial and lateral orientations with respect to g(eff) by measuring the slenderness ratio as a function of Bond number at the instant of bridge collapse. Results exhibit remarkable agreement with theory as well as with the experimental results obtained in a magnetic levitation-based experiment. The parabolic flight method offers technical originality and provides experimental insights for researchers in the microgravity field. Here we present hardware development, experimental considerations, and results, and demonstrate that parabolic flight is a viable alternative to extant techniques for quantitative experiments on fluids. C1 [DiLisi, Gregory] John Carroll Univ, University Hts, OH 44118 USA. [Dempsey, Robert] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Rarick, Richard] Cleveland State Univ, Cleveland, OH 44115 USA. [Rosenblatt, Charles] Case Western Reserve Univ, Cleveland, OH 44106 USA. RP DiLisi, G (reprint author), John Carroll Univ, University Hts, OH 44118 USA. EM gdilisi@jcu.edu FU National Aeronautics and Space Administration under Reduced Gravity Student Flight Program FX This work was supported by the National Aeronautics and Space Administration under the Reduced Gravity Student Flight Program. The authors also wish to acknowledge the undergraduate students from John Carroll University and Baldwin Wallace University who performed several of the in-flight measurements. NR 32 TC 0 Z9 0 U1 2 U2 3 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 JUN PY 2015 VL 27 IS 3 BP 145 EP 153 DI 10.1007/s12217-015-9423-3 PG 9 WC Engineering, Aerospace; Thermodynamics; Mechanics SC Engineering; Thermodynamics; Mechanics GA CP0FA UT WOS:000359550000003 ER PT J AU LeNoble, C Peritz, J Weber, E Adaryukov, J Dodson, C Svec, L AF LeNoble, Chelsea Peritz, Jonathan Weber, Erica Adaryukov, James Dodson, Catherine Svec, Leedjia TI The Application of Multipurpose Efficiently Engineered Tabling Outcomes (MEETO) for Improved Networks SO NAVAL ENGINEERS JOURNAL LA English DT Article AB From continuous operations (CONOPS) to speed networking events, there are numerous applications within the military environment in which a systematic arrangement of people is required. Shifts must be scheduled to minimize sleep disturbance, teams must be created to maximize diversity, and individuals seek to network with as many new individuals as possible. While planned rotation within groups can improve functions within military operations, there are significant logistical challenges to ensure equitable distribution of personnel, balanced teams, or efficient social networking events. This experiment created and tested different algorithms that sought to solve the challenge of rotating personnel so that an individual would not engage in the same condition more than once for a set period. The successful solution comprised a matrix allowing for multiples of five in systematic rearrangements of stepwise patterns. The solution utilized six rounds of five people per table to achieve the intended result that each person in a group of 100 people meets 24 other people without meeting the same person twice. The algorithm may be adjusted in other situations, for example smaller or larger numbers, even numbers, or unexpected conditions. C1 [LeNoble, Chelsea] Florida Inst Technol, Melbourne, FL 32901 USA. [Peritz, Jonathan] Coral Springs Charter Sch, Coral Springs, FL 33065 USA. [Weber, Erica] Melbourne Cent Catholic High Sch, Melbourne, FL 32901 USA. [Dodson, Catherine] Michigan State Univ, Social Psychol, E Lansing, MI 48824 USA. [Adaryukov, James] Satellite High Sch, Satellite Beach, FL 32937 USA. [Svec, Leedjia] NASA, Houston, TX USA. RP LeNoble, C (reprint author), Florida Inst Technol, Melbourne, FL 32901 USA. NR 8 TC 0 Z9 0 U1 1 U2 1 PU AMER SOC NAVAL ENG INC PI ALEXANDRIA PA 1452 DUKE STREET, ALEXANDRIA, VA 22314-3458 USA SN 0028-1425 EI 1559-3584 J9 NAV ENG J JI Nav. Eng. J. PD JUN PY 2015 VL 127 IS 2 BP 101 EP 104 PG 4 WC Engineering, Marine; Engineering, Civil; Oceanography SC Engineering; Oceanography GA CO5CV UT WOS:000359178100005 ER PT J AU Alexeyev, SO Rannu, KA Dyadina, PI Latosh, BN Turyshev, SG AF Alexeyev, S. O. Rannu, K. A. Dyadina, P. I. Latosh, B. N. Turyshev, S. G. TI Observational limits on Gauss-Bonnet and Randall-Sundrum gravities SO JOURNAL OF EXPERIMENTAL AND THEORETICAL PHYSICS LA English DT Article ID SPHERICALLY SYMMETRIC-SOLUTIONS; EXTENDED EINSTEIN EQUATIONS; DILATONIC BLACK-HOLES; F R THEORIES; GENERAL-RELATIVITY; HAWKING RADIATION; BACKGROUND FIELDS; QUANTUM-GRAVITY; STRING GRAVITY; TENSOR AB We discuss the possibilities of experimental search for the new physics predicted by the Gauss-Bonnet and the Randall-Sundrum theories of gravity. The effective four-dimensional spherically symmetrical solutions of these theories are analyzed. We consider these solutions in the weak-field limit and in the process of the primordial black hole evaporation. We show that the predictions of the discussed models are the same as of general relativity. Hence, current experiments are not applicable for such search, and therefore different methods of observation and higher accuracy are required. C1 [Alexeyev, S. O.; Rannu, K. A.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119991, Russia. [Dyadina, P. I.] Moscow MV Lomonosov State Univ, Dept Phys, Moscow 119991, Russia. [Latosh, B. N.] Dubna Int Univ, Fac Nat & Engn Sci, Dubna 141980, Moscow Oblast, Russia. [Latosh, B. N.] Ural Fed Univ, Inst Nat Sci, Dept Phys, Ekaterinburg 620002, Russia. [Turyshev, S. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Alexeyev, SO (reprint author), Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119991, Russia. EM salexeyev@gmail.com RI Latosh, Boris/E-8252-2017 OI Latosh, Boris/0000-0001-7099-0861 FU Federal Agency on Science and Innovations of Russian Federation [02.740.11.0575]; D. Zimin's "Dynasty" Foundation FX This paper was supported by the Federal Agency on Science and Innovations of Russian Federation, state contract 02.740.11.0575. S. A. and B. L. were also supported by individual grants from D. Zimin's "Dynasty" Foundation. The authors thank S. Capozziello, M. Smolyakov, and D. Levkov for the useful discussions on the subject of this work. This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 84 TC 0 Z9 0 U1 0 U2 1 PU MAIK NAUKA/INTERPERIODICA/SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA SN 1063-7761 EI 1090-6509 J9 J EXP THEOR PHYS+ JI J. Exp. Theor. Phys. PD JUN PY 2015 VL 120 IS 6 BP 966 EP 973 DI 10.1134/S1063776115060011 PG 8 WC Physics, Multidisciplinary SC Physics GA CN7YB UT WOS:000358650800005 ER PT J AU Capotondi, A Wittenberg, AT Newman, M Di Lorenzo, E Yu, JY Braconnot, P Cole, J Dewitte, B Giese, B Guilyardi, E Jin, FF Karnauskas, K Kirtman, B Lee, T Schneider, N Xue, Y Yeh, SW AF Capotondi, Antonietta Wittenberg, Andrew T. Newman, Matthew Di Lorenzo, Emanuele Yu, Jin-Yi Braconnot, Pascale Cole, Julia Dewitte, Boris Giese, Benjamin Guilyardi, Eric Jin, Fei-Fei Karnauskas, Kristopher Kirtman, Benjamin Lee, Tong Schneider, Niklas Xue, Yan Yeh, Sang-Wook TI Understanding ENSO Diversity SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID SEA-SURFACE TEMPERATURE; NINO-SOUTHERN-OSCILLATION; CENTRAL EQUATORIAL PACIFIC; WESTERLY WIND BURSTS; COUPLED CLIMATE MODELS; TONGUE EL-NINO; TROPICAL PACIFIC; OCEAN-ATMOSPHERE; DECADAL VARIABILITY; REANALYSIS PROJECT AB El Nino-Southern Oscillation (ENSO) is a naturally occurring mode of tropical Pacific variability, with global impacts on society and natural ecosystems. While it has long been known that El Nino events display a diverse range of amplitudes, triggers, spatial patterns, and life cycles, the realization that ENSO's impacts can be highly sensitive to this event-to-event diversity is driving a renewed interest in the subject. This paper surveys our current state of knowledge of ENSO diversity, identifies key gaps in understanding, and outlines some promising future research directions. C1 [Capotondi, Antonietta; Newman, Matthew] Univ Colorado, Boulder, CO 80309 USA. [Capotondi, Antonietta; Newman, Matthew] NOAA, ESRL, Boulder, CO 80305 USA. [Wittenberg, Andrew T.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. [Di Lorenzo, Emanuele] Georgia Inst Technol, Atlanta, GA 30332 USA. [Yu, Jin-Yi] Univ Calif Irvine, Irvine, CA USA. [Braconnot, Pascale] Lab Sci Climat & Environm, Gif Sur Yvette, France. [Cole, Julia] Univ Arizona, Tucson, AZ USA. [Dewitte, Boris] LEGOS, Toulouse, France. [Giese, Benjamin] Texas A&M, College Stn, TX USA. [Guilyardi, Eric] IPSL, LOCEAN, Paris, France. [Guilyardi, Eric] Univ Reading, Reading, Berks, England. [Jin, Fei-Fei; Schneider, Niklas] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Karnauskas, Kristopher] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. [Kirtman, Benjamin] Univ Miami, Miami, FL USA. [Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Xue, Yan] Climate Predict Ctr, College Pk, MD USA. [Yeh, Sang-Wook] Hanyang Univ, Ansan, South Korea. RP Capotondi, A (reprint author), NOAA, ESRL, PSD1, 325 Broadway, Boulder, CO 80305 USA. EM antonietta.capotondi@noaa.gov RI Newman, Matthew /F-8336-2010; Wittenberg, Andrew/G-9619-2013; Guilyardi, Eric/D-4868-2011; Di Lorenzo, Emanuele/E-9107-2012 OI Newman, Matthew /0000-0001-5348-2312; Wittenberg, Andrew/0000-0003-1680-8963; Guilyardi, Eric/0000-0002-2255-8625; Di Lorenzo, Emanuele/0000-0002-1935-7363 FU U.S. CLIVAR office; NASA; NOAA; NSF; DOE; National Science Foundation FX The authors of this paper are members of the U.S. CLIVAR ENSO Diversity Working Group, sponsored by U.S. CLIVAR. The working group wishes to acknowledge the U.S. CLIVAR office for its support, and the U.S. CLIVAR funding agencies, NASA, NOAA, NSF, and DOE, for their sponsorship. The authors would also like to thank Drs. M. McPhaden and D. Dommenget, as well as two anonymous reviewers, for their careful readings of the manuscript, excellent suggestions, and constructive criticism, which have considerably improved the paper. 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. AC acknowledges support from the National Science Foundation for this study. NR 133 TC 63 Z9 64 U1 15 U2 71 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 JUN PY 2015 VL 96 IS 6 BP 921 EP 938 DI 10.1175/BAMS-D-13-00117.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CN1WZ UT WOS:000358212700001 ER PT J AU Walsh, KJE Camargo, SJ Vecchi, GA Daloz, AS Elsner, J Emanuel, K Horn, M Lim, YK Roberts, M Patricola, C Scoccimarro, E Sobel, AH Strazzo, S Villarini, G Wehner, M Zhao, M Kossin, JP Larow, T Oouchi, K Schubert, S Wang, H Bacmeister, J Chang, P Chauvin, F Jablonowski, C Kumar, A Murakami, H Ose, T Reed, KA Saravanan, R Yamada, Y Zarzycki, CM Vidale, PL Jonas, JA Henderson, N AF Walsh, Kevin J. E. Camargo, Suzana J. Vecchi, Gabriel A. Daloz, Anne Sophie Elsner, James Emanuel, Kerry Horn, Michael Lim, Young-Kwon Roberts, Malcolm Patricola, Christina Scoccimarro, Enrico Sobel, Adam H. Strazzo, Sarah Villarini, Gabriele Wehner, Michael Zhao, Ming Kossin, James P. LaRow, Tim Oouchi, Kazuyoshi Schubert, Siegfried Wang, Hui Bacmeister, Julio Chang, Ping Chauvin, Fabrice Jablonowski, Christiane Kumar, Arun Murakami, Hiroyuki Ose, Tomoaki Reed, Kevin A. Saravanan, Ramalingam Yamada, Yohei Zarzycki, Colin M. Vidale, Pier Luigi Jonas, Jeffrey A. Henderson, Naomi TI HURRICANES AND CLIMATE The US CLIVAR Working Group on Hurricanes SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID TROPICAL CYCLONE ACTIVITY; GENERAL-CIRCULATION MODELS; RADIATIVE-CONVECTIVE EQUILIBRIUM; SEA-SURFACE TEMPERATURES; GENESIS POTENTIAL INDEX; CMIP5 MODELS; FUTURE CHANGES; 20-1ST-CENTURY PROJECTIONS; MAXIMUM INTENSITY; ATMOSPHERIC MODEL AB While a quantitative climate theory of tropical cyclone formation remains elusive, considerable progress has been made recently in our ability to simulate tropical cyclone climatologies and to understand the relationship between climate and tropical cyclone formation. Climate models are now able to simulate a realistic rate of global tropical cyclone formation, although simulation of the Atlantic tropical cyclone climatology remains challenging unless horizontal resolutions finer than 50 km are employed. This article summarizes published research from the idealized experiments of the Hurricane Working Group of U.S. Climate and Ocean: Variability, Predictability and Change (CLIVAR). This work, combined with results from other model simulations, has strengthened relationships between tropical cyclone formation rates and climate variables such as midtropospheric vertical velocity, with decreased climatological vertical velocities leading to decreased tropical cyclone formation. Systematic differences are shown between experiments in which only sea surface temperature is increased compared with experiments where only atmospheric carbon dioxide is increased. Experiments where only carbon dioxide is increased are more likely to demonstrate a decrease in tropical cyclone numbers, similar to the decreases simulated by many climate models for a future, warmer climate. Experiments where the two effects are combined also show decreases in numbers, but these tend to be less for models that demonstrate a strong tropical cyclone response to increased sea surface temperatures. Further experiments are proposed that may improve our understanding of the relationship between climate and tropical cyclone formation, including experiments with two-way interaction between the ocean and the atmosphere and variations in atmospheric aerosols. C1 [Walsh, Kevin J. E.; Horn, Michael] Univ Melbourne, Parkville, Vic 3010, Australia. [Camargo, Suzana J.; Sobel, Adam H.; Henderson, Naomi] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Vecchi, Gabriel A.; Zhao, Ming; Murakami, Hiroyuki] Geophys Fluid Dynam Lab, Princeton, NJ USA. [Daloz, Anne Sophie] Univ Wisconsin, Space Sci & Engn Ctr, Madison, WI USA. [Elsner, James; Strazzo, Sarah; LaRow, Tim] Florida State Univ, Tallahassee, FL 32306 USA. [Emanuel, Kerry] MIT, Cambridge, MA 02139 USA. [Lim, Young-Kwon] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Lim, Young-Kwon] Goddard Earth Sci Technol & Res, Greenbelt, MD USA. [Lim, Young-Kwon] IM Syst Grp, Greenbelt, MD USA. [Roberts, Malcolm] Met Off, Exeter, Devon, England. [Patricola, Christina; Chang, Ping; Saravanan, Ramalingam] Texas A&M Univ, College Stn, TX USA. [Scoccimarro, Enrico] Ist Nazl Geofis & Vulcanol, Bologna, Italy. [Scoccimarro, Enrico] Ctr Euromediterraneo Cambiamenti Climat, Bologna, Italy. [Villarini, Gabriele] Univ Iowa, Iowa City, IA USA. [Wehner, Michael] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Kossin, James P.] NOAA, NCDC, Asheville, NC USA. [Oouchi, Kazuyoshi; Yamada, Yohei] JAMSTEC, Yokohama, Kanagawa, Japan. [Schubert, Siegfried] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Wang, Hui; Kumar, Arun] NOAA, NCEP, College Pk, MD USA. [Bacmeister, Julio; Reed, Kevin A.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Chauvin, Fabrice] Meteo France, Toulouse, France. [Zarzycki, Colin M.] Univ Michigan, Ann Arbor, MI 48109 USA. [Ose, Tomoaki] Japan Meteorol Agcy, Meteorol Res Inst, Tsukuba, Ibaraki, Japan. [Vidale, Pier Luigi] Univ Reading, Reading, Berks, England. [Jonas, Jeffrey A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Jonas, Jeffrey A.] Columbia Univ, New York, NY USA. RP Walsh, KJE (reprint author), Univ Melbourne, Sch Earth Sci, Parkville, Vic 3010, Australia. EM kevin.walsh@unimelb.edu.au RI Vecchi, Gabriel/A-2413-2008; Camargo, Suzana/C-6106-2009; Reed, Kevin/C-4466-2012; Murakami, Hiroyuki/L-5745-2015; Zarzycki, Colin/E-5691-2014; Zhao, Ming/C-6928-2014; Jablonowski, Christiane/I-9068-2012; Kossin, James/C-2022-2016; Chang, Ping /A-1642-2013; Villarini, Gabriele/F-8069-2016; Sobel, Adam/K-4014-2015; Patricola, Christina/L-9902-2016 OI Strazzo, Sarah/0000-0003-1332-3135; Vidale, Pier Luigi/0000-0002-1800-8460; Walsh, Kevin/0000-0002-1860-510X; Vecchi, Gabriel/0000-0002-5085-224X; Camargo, Suzana/0000-0002-0802-5160; Reed, Kevin/0000-0003-3741-7080; Jablonowski, Christiane/0000-0003-0407-0092; Kossin, James/0000-0003-0461-9794; Chang, Ping /0000-0002-9085-0759; Villarini, Gabriele/0000-0001-9566-2370; Sobel, Adam/0000-0003-3602-0567; Patricola, Christina/0000-0002-3387-0307 FU NASA; NOAA; NSF; DOE; ARC Centre of Excellence for Climate System Science [CE110001028]; U.S. DOE [DE-SC0006824, DE-SC0006684, DE-SC0004966]; NOAA [NA11OAR4310154, NA11OAR4310092]; NSF AGS [1143959]; NASA [NNX09AK34G]; Italian Ministry of Education, Universities and Research; Italian Ministry of Environment, Land and Sea under the GEMINA project; Ministry of Education, Culture, Sports, Science and Technology (MEXT), Japan FX We wish to take this opportunity to recognize the essential contributions from participating modeling groups (U.S. DOE-NCAR CAM5.1, CMCC ECHAM5, CNRM, FSU COAPS, NOAA GFDL HiRAM, NASA GISS-Columbia University, NASA GSFC GEOS-5, Hadley Centre HadGEM3, JAMSTEC NICAM, MRI CGCM3, NCEP GFS, and WRF) that ran model experiments and furnished their data for analysis. We also appreciate the contributions of NOAA GFDL for hosting the meeting that led to this paper, the U.S. CLIVAR Project Office and UCAR JOSS for logistics support, and the U.S. CLIVAR funding agencies-NASA, NOAA, NSF, and DOE for their sponsorship. The Texas Advanced Computing Center (TACC) at The University of Texas at Austin and the Texas A&M Supercomputing Facility provided supercomputing resources used to perform portions of the simulations described in this paper. Portions of the work described in this paper were funded in part by the ARC Centre of Excellence for Climate System Science (Grant CE110001028); the U.S. DOE Grants DE-SC0006824, DE-SC0006684, and DE-SC0004966; the NOAA Grants NA11OAR4310154 and NA11OAR4310092; NSF AGS 1143959; and NASA Grant NNX09AK34G. E. Scoccimarro received funding from the Italian Ministry of Education, Universities and Research and the Italian Ministry of Environment, Land and Sea under the GEMINA project. The numerical experiments for NICAM and MRI-AGCM were performed on the Earth Simulator of JAMSTEC under the framework of the KAKUSHIN project funded by the Ministry of Education, Culture, Sports, Science and Technology (MEXT), Japan. NR 126 TC 33 Z9 33 U1 6 U2 31 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 JUN PY 2015 VL 96 IS 6 BP 997 EP 1017 DI 10.1175/BAMS-D-13-00242.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CN1XE UT WOS:000358213200002 ER PT J AU Holt, B Johnson, MP Perkovic-Martin, D Panzer, B AF Holt, Benjamin Johnson, Michael P. Perkovic-Martin, Dragana Panzer, Ben TI Snow depth on Arctic sea ice derived from radar: In situ comparisons and time series analysis SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE snow on sea Ice ID ULTRA-WIDE-BAND; THICKNESS; VARIABILITY; OCEAN AB The snow radar being flown on NASA's Operation IceBridge, ongoing aircraft campaigns to the Arctic and the Antarctic are providing unique observations of the depth of snow on the sea ice cover. In this paper, we focus on the radar-derived snow depth results from the 2009-2012 Arctic campaigns. We develop and evaluate the use of a distinct snow layer tracker to measure snow depth based on a Support Vector Machine (SVM) supervised learning algorithm. The snow radar is designed to detect both the air-snow and snow-ice interfaces using ultrawideband frequencies from 2 to 8 GHz. The quality, errors, and repeatability of the snow radar snow depth estimates are examined, based on comparisons with in situ data obtained during two separate sea ice field campaigns, the GreenArc 2009 and the CryoVEx 2011 campaigns off Greenland in the Lincoln Sea. Finally, we analyze 4 years (2009-2012) of three annually repeated sea ice flight lines obtained in early spring, located off Greenland and the Canadian Arctic. We examine the annual variations of snow depth differences between perennial and seasonal ice when available. Overall, the snow layer tracker produced consistent, accurate results for snow depths between 0.10 and approximate to 0.60 m. This was confirmed with comparisons with the two data sets from the in situ measurement campaigns as well as with the time series analysis, and is consistent with other published results. C1 [Holt, Benjamin; Johnson, Michael P.; Perkovic-Martin, Dragana] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Panzer, Ben] Sandia Natl Labs, Albuquerque, NM 87185 USA. RP Holt, B (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Benjamin.M.Holt@jpl.nasa.gov FU National Aeronautics and Space Administration FX This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, and at Kansas University, under contract with the National Aeronautics and Space Administration. Ben Panzer performed this work while at the University of Kansas. The authors wish to thank the following for valuable discussions: Christian Haas (York University) regarding the CryoVEx field measurements, Ron Kwok (JPL), and Prasad Gogineni and Carl Leuschen (University of Kansas). We also wish to thank Jackie Richter-Menge and Bruce Elder (CRREL) as well as Sinead Farrell (University of Maryland) for providing the GreenArc 2009 data. The snow radar raw data utilized for this study were produced by CReSIS and made available, along with the ATM, CAMBOT, and DMS imagery through the National Snow and Ice Data Center IceBridge data portal (http://nsidc.org/icebridge/portal/). To identify snow depths for different sea ice types, we utilized derived sea ice type output data available from the EUMETSAT Ocean and Sea Ice Processing Centre (http://saf.met.no/p/ice/#type). NR 43 TC 3 Z9 3 U1 1 U2 5 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 JUN PY 2015 VL 120 IS 6 BP 4260 EP 4287 DI 10.1002/2015JC010815 PG 28 WC Oceanography SC Oceanography GA CN0SP UT WOS:000358124100021 ER PT J AU Boardsen, SA Kim, EH Raines, JM Slavin, JA Gershman, DJ Anderson, BJ Korth, H Sundberg, T Schriver, D Travnicek, P AF Boardsen, S. A. Kim, E. -H. Raines, J. M. Slavin, J. A. Gershman, D. J. Anderson, B. J. Korth, H. Sundberg, T. Schriver, D. Travnicek, P. TI Interpreting similar to 1Hz magnetic compressional waves in Mercury's inner magnetosphere in terms of propagating ion-Bernstein waves SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE ion-Bernstein mode; ray tracing; Mercury's magnetosphere; planetary loss cone instability ID MESSENGERS 1ST FLYBY; ULF WAVES; CYCLOTRON WAVES; PLASMA SHEET; FIELD; DISTRIBUTIONS; GENERATION; FREQUENCY; MAGNETOMETER; ABSORPTION AB We show that similar to 1Hz magnetic compressional waves observed in Mercury's inner magnetosphere could be interpreted as ion-Bernstein waves in a moderate proton beta similar to 0.1 plasma. An observation of a proton distribution with a large planetary loss cone is presented, and we show that this type of distribution is highly unstable to the generation of ion-Bernstein waves with low magnetic compression. Ray tracing shows that as these waves propagate back and forth about the magnetic equator; they cycle between a state of low and high magnetic compression. The group velocity decreases during the high-compression state leading to a pileup of compressional wave energy, which could explain the observed dominance of the highly compressional waves. This bimodal nature is due to the complexity of the index of refraction surface in a warm plasma whose upper branch has high growth rate with low compression, and its lower branch has low growth/damping rate with strong compression. Two different cycles are found: one where the compression maximum occurs at the magnetic equator and one where the compression maximum straddles the magnetic equator. The later cycle could explain observations where the maximum in compression straddles the equator. Ray tracing shows that this mode is confined within 12 degrees magnetic latitude which can account for the bulk of the observations. We show that the Doppler shift can account for the difference between the observed and model wave frequency, if the wave vector direction is in opposition to the plasma flow direction. We note that the Wentzel-Kramers-Brillouin approximation breaks down during the pileup of compressional energy and that a study involving full wave solutions is required. C1 [Boardsen, S. A.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA. [Boardsen, S. A.] NASA Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD USA. [Kim, E. -H.] Princeton Univ, Princeton Ctr Heliophys, Princeton, NJ 08544 USA. [Kim, E. -H.] Princeton Univ, Princeton Plasma Phys Lab, Princeton, NJ 08543 USA. [Raines, J. M.; Slavin, J. A.; Gershman, D. J.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Gershman, D. J.] NASA Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD USA. [Anderson, B. J.; Korth, H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Sundberg, T.] Queen Mary Univ London, Sch Phys & Astron, London, England. [Schriver, D.] Univ Calif Los Angeles, Dept Phys, Los Angeles, CA 90024 USA. [Travnicek, P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Boardsen, SA (reprint author), Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA. EM Scott.A.Boardsen@nasa.gov RI Travnicek, Pavel/G-8608-2014; Slavin, James/H-3170-2012 OI Slavin, James/0000-0002-9206-724X FU NASA Planetary Data Analysis Program [NNX10AU26G]; Geoscience [NNX08AJ78G]; NASA [NNH09AK63I, NNH11AQ46I]; DOE [DEAC02-09CH11466]; NASA Discovery Program [NAS5-97271]; NASA Heliophysics Supporting Research Program [NNX15AJ68G] FX We thank K. Ronnmark at Umea University in Sweden for providing us with the warm plasma instability code WHAMP and the warm plasma ray tracing code RATRACE. The data used in this study are publicly available at the Planetary Data System (http://pds.nasa.gov/). This research was supported by NASA Planetary Data Analysis Program grant NNX10AU26G and Geoscience grant NNX08AJ78G. The work at the Princeton University was supported by NASA grants NNH09AK63I and NNH11AQ46I, and DOE contract DEAC02-09CH11466. The MESSENGER project is supported by the NASA Discovery Program under contracts NAS5-97271 to the Johns Hopkins University Applied Physics Laboratory. This work was also supported by the NASA Heliophysics Supporting Research Program under grant NNX15AJ68G. NR 55 TC 5 Z9 5 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2015 VL 120 IS 6 BP 4213 EP 4228 DI 10.1002/2014JA020910 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN1RZ UT WOS:000358199100010 ER PT J AU Hwang, J Choi, EJ Park, JS Fok, MC Lee, DY Kim, KC Shin, DK Usanova, ME Reeves, GD AF Hwang, J. Choi, E. -J. Park, J. -S. Fok, M. -C. Lee, D. -Y. Kim, K. -C. Shin, D. -K. Usanova, M. E. Reeves, G. D. TI Comprehensive analysis of the flux dropout during 7-8 November 2008 storm using multisatellite observations and RBE model SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE flux dropout; RBE model; magneopause shadowing; atmospheric precipitation; geomagnetic storm; radiation belt ID OUTER RADIATION BELT; PITCH-ANGLE SCATTERING; ION-CYCLOTRON WAVES; ELECTRON ACCELERATION; INNER MAGNETOSPHERE; MAGNETIC STORMS; CHORUS WAVES; 30 SEPTEMBER; PHASE-SPACE; DIFFUSION AB We investigate an electron flux dropout during a weak storm on 7-8 November 2008, with Dst minimum value being - 37 nT. During this period, two clear dropouts were observed on GOES 11>2MeV electrons. We also find a simultaneous dropout in the subrelativistic electrons recorded by Time History of Events and Macroscale Interactions during Substorms probes in the outer radiation belt. Using the Radiation Belt Environment model, we try to reproduce the observed dropout features in both relativistic and subrelativistic electrons. We found that there are local time dependences in the dropout for both observation and simulation in subrelativistic electrons: ( 1) particle loss begins from nightside and propagates into dayside and (2) resupply starts from near dawn magnetic local time and propagates into the dayside following electron drift direction. That resupply of the particles might be caused by substorm injections due to enhanced convection. We found a significant precipitation in hundreds keV electrons during the dropout. We observe electromagnetic ion cyclotron and chorus waves both on the ground and in space. We find the drift shells are opened near the beginning of the first dropout. The dropout in MeV electrons at GEO might therefore be initiated due to the magnetopause shadowing, and the followed dropout in hundreds keV electrons might be the result of the combination of magnetopause shadowing and precipitation loss into the Earth's atmosphere. C1 [Hwang, J.; Kim, K. -C.] Korea Astron & Space Sci Inst, Taejon, South Korea. [Hwang, J.] Korea Univ Sci & Technol, Dept Astron & Space Sci, Taejon, South Korea. [Choi, E. -J.] Korea Adv Inst Sci & Technol, Dept Phys, Taejon 305701, South Korea. [Park, J. -S.] Kyung Hee Univ, Sch Space Res, Yongin, South Korea. [Fok, M. -C.] NASA GSFC, Greenbelt, MD USA. [Lee, D. -Y.; Shin, D. -K.] Chungbuk Natl Univ, Dept Astron & Space Sci, Cheongju, South Korea. [Usanova, M. E.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Reeves, G. D.] Los Alamos Natl Lab, Space Sci & Applicat Grp, Los Alamos, NM USA. RP Hwang, J (reprint author), Korea Astron & Space Sci Inst, Taejon, South Korea. EM jahwang@kasi.re.kr OI Reeves, Geoffrey/0000-0002-7985-8098 FU Planetary system research for space exploration project; KASI; NSL [20110030742]; Canadian Space Agency; NASA [NAS5-02099] FX This work was supported by "Planetary system research for space exploration" project and the basic research funding from KASI. This work at Chungbuk National University was supported by an NSL grant (20110030742) of the National Research Foundation of Korea. We are thankful to the THEMIS team (http://themis.ssl.berkeley.edu/data_retrieval. index); NASA's CDAWeb ( http://cdaweb.gsfc.nasa.gov/), OMNI ( http://omniweb.gsfc.nasa.gov/); and NOAA's GOES (http://www.goes.noaa.gov/), POES (ftp://virbo.org/POES), NGDC http://www.ngdc.noaa.gov/ngdcinfo/onlineaccess.html),and LANL GEO data ( by personal contact to G.D. Reeves) for providing online data access and data analysis tools. The authors thank I.R. Mann, D.K. Milling, and the rest of the CARISMA team for the data. CARISMA is operated by the University of Alberta, funded by the Canadian Space Agency. We acknowledge NASA contract NAS5-02099 for the use of data from the THEMIS mission. NR 55 TC 3 Z9 3 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2015 VL 120 IS 6 BP 4298 EP 4312 DI 10.1002/2015JA021085 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN1RZ UT WOS:000358199100015 ER PT J AU Welling, DT Jordanova, VK Glocer, A Toth, G Liemohn, MW Weimer, DR AF Welling, D. T. Jordanova, V. K. Glocer, A. Toth, G. Liemohn, M. W. Weimer, D. R. TI The two-way relationship between ionospheric outflow and the ring current SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE magnetosphere; ring current; ionospheric outflow ID ALLEN PROBES OBSERVATIONS; SHEET ION COMPOSITION; FIELD-ALIGNED CURRENT; POLAR WIND; PLASMA SHEET; NEAR-EARTH; INNER MAGNETOSPHERE; MAGNETIC-FIELD; STORM-TIME; PROTON PRECIPITATION AB It is now well established that the ionosphere, because it acts as a significant source of plasma, plays a critical role in ring current dynamics. However, because the ring current deposits energy into the ionosphere, the inverse may also be true: the ring current can play a critical role in the dynamics of ionospheric outflow. This study uses a set of coupled, first-principles-based numerical models to test the dependence of ionospheric outflow on ring current-driven region 2 field-aligned currents (FACs). A moderate magnetospheric storm event is modeled with the Space Weather Modeling Framework using a global MHD code (Block Adaptive Tree Solar wind Roe-type Upwind Scheme, BATS-R-US), a polar wind model (Polar Wind Outflow Model), and a bounce-averaged kinetic ring current model (ring current atmosphere interaction model with self-consistent magnetic field, RAM-SCB). Initially, each code is two-way coupled to all others except for RAM-SCB, which receives inputs from the other models but is not allowed to feed back pressure into the MHD model. The simulation is repeated with pressure coupling activated, which drives strong pressure gradients and region 2 FACs in BATS-R-US. It is found that the region 2 FACs increase heavy ion outflow by up to 6 times over the noncoupled results. The additional outflow further energizes the ring current, establishing an ionosphere-magnetosphere mass feedback loop. This study further demonstrates that ionospheric outflow is not merely a plasma source for the magnetosphere but an integral part in the nonlinear ionosphere-magnetosphere-ring current system. C1 [Welling, D. T.; Toth, G.; Liemohn, M. W.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Jordanova, V. K.] Los Alamos Natl Lab, Los Alamos, NM USA. [Glocer, A.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Weimer, D. R.] Virginia Polytech Inst & State Univ, Bradley Dept Elect & Comp Engn, Ctr Space Sci & Engn Res, Blacksburg, VA 24061 USA. RP Welling, DT (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. EM dwelling@umich.edu RI Toth, Gabor/B-7977-2013; OI Toth, Gabor/0000-0002-5654-9823; Jordanova, Vania/0000-0003-0475-8743 FU NSF [AGS 1202984]; NASA [NNH13AV48I, NNH14AX90I, NNX11AO60G, NNX13AD69G]; Los Alamos National Laboratory Directed Research and Development (LDRD) Program FX The authors acknowledge the use of data from the ACE satellite MAG and SWEPAM instruments provided by NASA GSFC Space Physics Data Facility. Dst index was obtained via the World Data Center for Geomagnetism, Kyoto. This work was supported by NSF award AGS 1202984; NASA awards NNH13AV48I, NNH14AX90I, NNX11AO60G, and NNX13AD69G; and the Los Alamos National Laboratory Directed Research and Development (LDRD) Program. Models used in this study can be freely obtained from http://csem.engin.umich.edu; simulation data can be obtained by contacting the authors. NR 114 TC 6 Z9 6 U1 1 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2015 VL 120 IS 6 BP 4338 EP 4353 DI 10.1002/2015JA021231 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN1RZ UT WOS:000358199100018 ER PT J AU Gershman, DJ Raines, JM Slavin, JA Zurbuchen, TH Sundberg, T Boardsen, SA Anderson, BJ Korth, H Solomon, SC AF Gershman, Daniel J. Raines, Jim M. Slavin, James A. Zurbuchen, Thomas H. Sundberg, Torbjoern Boardsen, Scott A. Anderson, Brian J. Korth, Haje Solomon, Sean C. TI MESSENGER observations of multiscale Kelvin-Helmholtz vortices at Mercury SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Kelvin-Helmholtz; Mercury; MESSENGER; finite gyroradius ID EARTHS MAGNETOSPHERE; PLANETARY IONS; PLASMA SHEET; SOLAR-WIND; MAGNETOPAUSE; MAGNETOSHEATH; MAGNETOTAIL; INSTABILITIES; MAGNETOMETER; ENVIRONMENT AB Observations by the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft in Mercury's magnetotail demonstrate for the first time that Na+ ions exert a dynamic influence on Mercury's magnetospheric system. Na+ ions are shown to contribute up to similar to 30% of the ion thermal pressure required to achieve pressure balance in the premidnight plasma sheet. High concentrations of planetary ions should lead to Na+ dominance of the plasma mass density in these regions. On orbits with northward-oriented interplanetary magnetic field and high (i.e., >1cm(-3)) Na+ concentrations, MESSENGER has often recorded magnetic field fluctuations near the Na+ gyrofrequency associated with the Kelvin-Helmholtz (K-H) instability. These nightside K-H vortices are characteristically different from those observed on Mercury's dayside that have a nearly constant wave frequency of similar to 0.025Hz. Collectively, these observations suggest that large spatial gradients in the hot planetary ion population at Mercury may result in a transition from a fluid description to a kinetic description of vortex formation across the dusk terminator, providing the first set of truly multiscale observations of the K-H instability at any of the diverse magnetospheric environments explored in the solar system. C1 [Gershman, Daniel J.] NASA Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Gershman, Daniel J.; Raines, Jim M.; Slavin, James A.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Sundberg, Torbjoern] Queen Mary Univ London, Sch Phys & Astron, London, England. [Boardsen, Scott A.] NASA Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD USA. [Boardsen, Scott A.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA. [Anderson, Brian J.; Korth, Haje] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA. RP Gershman, DJ (reprint author), NASA Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. EM djgersh@umich.edu RI Slavin, James/H-3170-2012 OI Slavin, James/0000-0002-9206-724X FU NASA Discovery Program [NAS5-97271]; Carnegie Institution of Washington [NASW-00002]; NASA Postdoctoral Program at Goddard Space Flight Center FX We thank two anonymous reviewers for their thoughtful comments on an earlier draft. The data used in this work can be obtained from the Planetary Data System (http://pds.nasa.gov/). The MESSENGER project is supported by the NASA Discovery Program under contracts NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of Washington. D.J.G. is supported by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities. NR 64 TC 8 Z9 8 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2015 VL 120 IS 6 BP 4354 EP 4368 DI 10.1002/2014JA020903 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN1RZ UT WOS:000358199100019 ER PT J AU Fatemi, S Lue, C Holmstrom, M Poppe, AR Wieser, M Barabash, S Delory, GT AF Fatemi, Shahab Lue, Charles Holmstrom, Mats Poppe, Andrew R. Wieser, Martin Barabash, Stas Delory, Gregory T. TI Solar wind plasma interaction with Gerasimovich lunar magnetic anomaly SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Interaction with lunar crustal fields; Hybrid modeling of plasma ID MHD SIMULATION; MOON; SURFACE; FIELDS; PROSPECTOR; MAGNETOMETER; ENVIRONMENT; REGIONS; CAVITY; MODEL AB We present the results of the first local hybrid simulations (particle ions and fluid electrons) for the solar wind plasma interaction with realistic lunar crustal fields. We use a three-dimensional hybrid model of plasma and an empirical model of the Gerasimovich magnetic anomaly based on Lunar Prospector observations. We examine the effects of low and high solar wind dynamic pressures on this interaction when the Gerasimovich magnetic anomaly is located at nearly 20 degrees solar zenith angle. We find that for low solar wind dynamic pressure, the crustal fields mostly deflect the solar wind plasma, form a plasma void at very close distances to the Moon (below 20km above the surface), and reflect nearly 5% of the solar wind in charged form. In contrast, during high solar wind dynamic pressure, the crustal fields are more compressed, the solar wind is less deflected, and the lunar surface is less shielded from impinging solar wind flux, but the solar wind ion reflection is more locally intensified (up to 25%) compared to low dynamic pressures. The difference is associated with an electrostatic potential that forms over the Gerasimovich magnetic anomaly as well as the effects of solar wind plasma on the crustal fields during low and high dynamic pressures. Finally, we show that an antimoonward Hall electric field is the dominant electric field for similar to 3km altitude and higher, and an ambipolar electric field has a noticeable contribution to the electric field at close distances (<3km) to the Moon. C1 [Fatemi, Shahab; Poppe, Andrew R.; Delory, Gregory T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Fatemi, Shahab; Poppe, Andrew R.; Delory, Gregory T.] NASA, Ames Res Ctr, Solar Syst Explorat Res Virtual Inst, Moffett Field, CA 94035 USA. [Lue, Charles; Holmstrom, Mats; Wieser, Martin; Barabash, Stas] Swedish Inst Space Phys, S-98128 Kiruna, Sweden. [Lue, Charles] Umea Univ, Dept Phys, Umea, Sweden. RP Fatemi, S (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM shahab@ssl.berkeley.edu OI Holmstrom, Mats/0000-0001-5494-5374 FU NASA's Solar System Exploration Research Virtual Institute (SSERVI) [NNX14AG16A]; SSERVI [SSERVI-2015-026] FX S. Fatemi, A. R. Poppe, and G. T. Delory gratefully acknowledge support from NASA's Solar System Exploration Research Virtual Institute (SSERVI), grant NNX14AG16A. This publication is SSERVI contribution SSERVI-2015-026. This research was conducted using resources provided by the Swedish National Infrastructure for Computing (SNIC) at the High Performance Computing Center North (HPC2N), Umea University, Sweden. The software used in this work was developed in part by the DOE NNSA ASC- and DOE Office of Science ASCR-supported Flash Center for Computational Science at the University of Chicago. The visualization tools we developed for our model data analysis are based on python Matplotlib and Mayavi open libraries. The authors thank the International Space Science Institute (ISSI) Bern, Switzerland, for organizing a meeting when the topic of this paper was extensively discussed. We thank the teams who created and provided Wind magnetic field and plasma data used in this analysis, including K. W. Ogilvie, A. J. Lazarus, and R. Lepping. The Wind data used for this paper is available at Comprehensive Solar Wind Laboratory For Long-Term Solar Wind Measurements at NASA website wind. nasa.gov. Data set name: WIND SWE 92-sec and MFI Magnetic Field. Selection period is 17 June 2009 between 16: 30 UT and 21: 50 UT. NR 54 TC 8 Z9 8 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2015 VL 120 IS 6 BP 4719 EP 4735 DI 10.1002/2015JA021027 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN1RZ UT WOS:000358199100048 ER PT J AU Dai, L Takahashi, K Lysak, R Wang, C Wygant, JR Kletzing, C Bonnell, J Cattell, CA Smith, CW MacDowall, RJ Thaller, S Breneman, A Tang, XW Tao, X Chen, LJ AF Dai, Lei Takahashi, Kazue Lysak, Robert Wang, Chi Wygant, John R. Kletzing, Craig Bonnell, John Cattell, Cynthia A. Smith, Charles W. MacDowall, Robert J. Thaller, Scott Breneman, Aaron Tang, Xiangwei Tao, Xin Chen, Lunjin TI Storm time occurrence and spatial distribution of Pc4 poloidal ULF waves in the inner magnetosphere: A Van Allen Probes statistical study SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Pc4 ULF waves; poloidal waves; geomagnetic storm; Van Allen Probe; solar wind dynamic pressure; ring current ID GIANT PULSATIONS; MAGNETIC-FIELD; AMPTE CCE; HYDROMAGNETIC-WAVES; SYNCHRONOUS ORBIT; ALFVEN WAVES; CONE ANGLE; SOLAR-WIND; ACCELERATION; ELECTRONS AB Poloidal ULF waves are capable of efficiently interacting with energetic particles in the ring current and the radiation belt. Using Van Allen Probes (Radiation Belt Storm Probes (RBSP)) data from October 2012 to July 2014, we investigate the spatial distribution and storm time occurrence of Pc4 (7-25mHz) poloidal waves in the inner magnetosphere. Pc4 poloidal waves are sorted into two categories: waves with and without significant magnetic compressional components. Two types of poloidal waves have comparable occurrence rates, both of which are much higher during geomagnetic storms. The noncompressional poloidal waves mostly occur in the late recovery phase associated with an increase of Dst toward 0, suggesting that the decay of the ring current provides their free energy source. The occurrence of dayside compressional Pc4 poloidal waves is found correlated with the variation of the solar wind dynamic pressure, indicating their origin in the solar wind. Both compressional and noncompressional waves preferentially occur on the dayside near noon at L similar to 5-6. In addition, compressional poloidal waves are observed at magnetic local time 18-24 on the nightside. The location of the Pc4 poloidal waves relative to the plasmapause is investigated. The RBSP statistical results may shed light on the in-depth investigations of the generation and propagation of Pc4 poloidal waves. C1 [Dai, Lei; Wang, Chi] Chinese Acad Sci, State Key Lab Space Weather, Ctr Space Sci & Appl Res, Beijing, Peoples R China. [Dai, Lei; Lysak, Robert; Wygant, John R.; Cattell, Cynthia A.; Thaller, Scott; Breneman, Aaron; Tang, Xiangwei] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Takahashi, Kazue] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Kletzing, Craig] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Bonnell, John] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Smith, Charles W.] Univ New Hampshire, Inst Earth Oceans & Space, Dept Phys, Durham, NH 03824 USA. [MacDowall, Robert J.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Tao, Xin] Univ Sci & Technol China, Dept Geophys & Planetary Sci, Hefei 230026, Peoples R China. [Chen, Lunjin] Univ Texas Dallas, Dept Phys, Richardson, TX USA. RP Dai, L (reprint author), Chinese Acad Sci, State Key Lab Space Weather, Ctr Space Sci & Appl Res, Beijing, Peoples R China. EM ldai@spaceweather.ac.cn OI Cattell, Cynthia/0000-0002-3805-320X; Kletzing, Craig/0000-0002-4136-3348 FU NASA [NNX14AB97G]; NNSFC [41231067]; Specialized Research Fund for State Key Laboratories of China; APL for the development of RBSP/EFW; JHU/APL [921647] FX Work by L.D. and K.T. was supported by NASA grant NNX14AB97G. This work was supported by NNSFC grant 41231067 and in part by the Specialized Research Fund for State Key Laboratories of China. Work at UMN was supported by a contract from APL for the development of RBSP/EFW.EMFISIS is supported by a JHU/APL contract 921647. The RBSP EMFISIS data are available at http://emfisis.physics.uiowa.edu/Flight/. The RBSP EFW data are available at http://rbsp.space.umn.edu/data/rbsp/. The OMNI data are available at CDAWeb. The Dst data are provided by the World Data Center for Geomagnetism, Kyoto. NR 63 TC 12 Z9 13 U1 2 U2 18 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 JUN PY 2015 VL 120 IS 6 BP 4748 EP 4762 DI 10.1002/2015JA021134 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN1RZ UT WOS:000358199100050 ER PT J AU Chi, PJ Le, G AF Chi, P. J. Le, G. TI Observations of magnetospheric high-m poloidal waves by ST-5 satellites in low Earth orbit during geomagnetically quiet times SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE high-m waves; poloidal mode; drift Alfven ballooning mode ID ALFVEN-BALLOONING MODES; KINETIC-THEORY; PULSATIONS; PLASMAPAUSE AB The poloidal waves with large azimuthal wave numbers (m similar to 100) in the magnetosphere are known to be generated by drift or drift-bounce resonance with energetic ring current particles, and these waves may play a role in modulating the energetic particles in the inner magnetosphere. When examining the magnetic field data collected by the NASA Space Technology 5 (ST-5) satellites in the low Earth orbit, Le et al. (2011) discovered many wave events with frequencies of 30-200 mHz (in the Pc2 and Pc3 bands), and they proposed that these waves should, in fact, be Doppler-shifted high-m poloidal waves in the magnetosphere with frequencies at only a few millihertz (in the Pc5 band). Using a new method that examines the differences in wave phase detected by the three ST-5 satellites, we confirm that the frequencies in the Earth frame for the poloidal waves observed are mainly between 3 and 5 mHz. Not only were poloidal waves observed frequently by ST-5 in the dayside magnetosphere but they were also occasionally seen in the nightside when the satellites passed through the same L shells. In each wave event, the azimuthal wave number may change with L, but the wave frequency in the Earth frame remains the same. We also find that poloidal waves can last more than 9 h during geomagnetically quiet conditions, suggesting that even a very weak ring current can supply enough energetic particles to excite poloidal waves. C1 [Chi, P. J.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90024 USA. [Le, G.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. RP Chi, PJ (reprint author), Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90024 USA. EM pchi@igpp.ucla.edu RI Le, Guan/C-9524-2012 OI Le, Guan/0000-0002-9504-5214 NR 22 TC 2 Z9 2 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2015 VL 120 IS 6 BP 4776 EP 4783 DI 10.1002/2015JA021145 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN1RZ UT WOS:000358199100052 ER PT J AU Ni, BB Zou, ZY Gu, XD Zhou, C Thorne, RM Bortnik, J Shi, R Zhao, ZY Baker, DN Kanekal, SG Spence, HE Reeves, GD Li, XL AF Ni, Binbin Zou, Zhengyang Gu, Xudong Zhou, Chen Thorne, Richard M. Bortnik, Jacob Shi, Run Zhao, Zhengyu Baker, Daniel N. Kanekal, Shrikhanth G. Spence, Harlan E. Reeves, Geoffrey D. Li, Xinlin TI Variability of the pitch angle distribution of radiation belt ultrarelativistic electrons during and following intense geomagnetic storms: Van Allen Probes observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE radiation belt ultrarelativistic electrons; pitch angle distribution; decay time scales; geomagnetic storms; resonant wave-particle interactions ID MARCH 2013 STORM; RELATIVISTIC ELECTRONS; EMIC WAVES; STATISTICAL-ANALYSIS; RESONANT SCATTERING; MAGNETIC STORM; ACCELERATION; CHORUS; RING; SIMULATIONS AB Fifteen months of pitch angle resolved Van Allen Probes Relativistic Electron-Proton Telescope (REPT) measurements of differential electron flux are analyzed to investigate the characteristic variability of the pitch angle distribution of radiation belt ultrarelativistic (>2MeV) electrons during storm conditions and during the long-term poststorm decay. By modeling the ultrarelativistic electron pitch angle distribution as sin(n)alpha, where alpha is the equatorial pitch angle, we examine the spatiotemporal variations of the n value. The results show that, in general, n values increase with the level of geomagnetic activity. In principle, ultrarelativistic electrons respond to geomagnetic storms by becoming more peaked at 90 degrees pitch angle with n values of 2-3 as a supportive signature of chorus acceleration outside the plasmasphere. High n values also exist inside the plasmasphere, being localized adjacent to the plasmapause and exhibiting energy dependence, which suggests a significant contribution from electromagnetic ion cyclotron (EMIC) wave scattering. During quiet periods, n values generally evolve to become small, i.e., 0-1. The slow and long-term decays of the ultrarelativistic electrons after geomagnetic storms, while prominent, produce energy and L-shell-dependent decay time scales in association with the solar and geomagnetic activity and wave-particle interaction processes. At lower L shells inside the plasmasphere, the decay time scales tau(d) for electrons at REPT energies are generally larger, varying from tens of days to hundreds of days, which can be mainly attributed to the combined effect of hiss-induced pitch angle scattering and inward radial diffusion. As L shell increases to L similar to 3.5, a narrow region exists (with a width of similar to 0.5L), where the observed ultrarelativistic electrons decay fastest, possibly resulting from efficient EMIC wave scattering. As L shell continues to increase, tau(d) generally becomes larger again, indicating an overall slower loss process by waves at high L shells. Our investigation based upon the sin(n)alpha function fitting and the estimate of decay time scale offers a convenient and useful means to evaluate the underlying physical processes that play a role in driving the acceleration and loss of ultrarelativistic electrons and to assess their relative contributions. C1 [Ni, Binbin; Zou, Zhengyang; Gu, Xudong; Zhou, Chen; Shi, Run; Zhao, Zhengyu] Wuhan Univ, Sch Elect Informat, Dept Space Phys, Wuhan 430072, Peoples R China. [Ni, Binbin] Chinese Acad Sci, State Key Lab Space Weather, Beijing, Peoples R China. [Thorne, Richard M.; Bortnik, Jacob] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. [Baker, Daniel N.; Li, Xinlin] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Kanekal, Shrikhanth G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Spence, Harlan E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Reeves, Geoffrey D.] Los Alamos Natl Lab, Space Sci & Applicat Grp, Los Alamos, NM USA. RP Ni, BB (reprint author), Wuhan Univ, Sch Elect Informat, Dept Space Phys, Wuhan 430072, Peoples R China. EM bbni@whu.edu.cn RI Reeves, Geoffrey/E-8101-2011; OI Reeves, Geoffrey/0000-0002-7985-8098; zou, zhengyang/0000-0003-1273-4573 FU NSFC [41204120, 41474141]; Fundamental Research Funds for the Central Universities [2042014kf0251]; Specialized Research Fund for State Key Laboratories; JHU/APL under NASA [967399, 921647, NAS5-01072]; ECT sub-award [13-041]; NASA [NNX11AR64G] FX This work was supported by the NSFC grants 41204120 and 41474141, the Fundamental Research Funds for the Central Universities grant 2042014kf0251, and the Project Supported by the Specialized Research Fund for State Key Laboratories. This work was also supported by JHU/APL contracts 967399 and 921647 under NASA's prime contract NAS5-01072. The analysis at UCLA was supported by the ECT sub-award 13-041 and NASA grant NNX11AR64G. Van Allen Probes REPT data were obtained from http://www.rbsp-ect.lanl.gov/science/DataDirectories.php. NR 48 TC 8 Z9 9 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2015 VL 120 IS 6 BP 4863 EP 4876 DI 10.1002/2015JA021065 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN1RZ UT WOS:000358199100058 ER PT J AU Lindkvist, J Holmstrom, M Khurana, KK Fatemi, S Barabash, S AF Lindkvist, Jesper Holmstrom, Mats Khurana, Krishan K. Fatemi, Shahab Barabash, Stas TI Callisto plasma interactions: Hybrid modeling including induction by a subsurface ocean SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Callisto; plasma interaction; hybrid model; subsurface ocean; Galileo flyby; magnetosphere ID MAGNETIC-FIELD; WAVE OBSERVATIONS; EUROPA; MAGNETOSPHERE; SATELLITES; ABSENCE AB By using a hybrid plasma solver (ions as particles and electrons as a fluid), we have modeled the interaction between Callisto and Jupiter's magnetosphere for variable ambient plasma parameters. We compared the results with the magnetometer data from flybys (C3, C9, and C10) by the Galileo spacecraft. Modeling the interaction between Callisto and Jupiter's magnetosphere is important to establish the origin of the magnetic field perturbations observed by Galileo and thought to be related to a subsurface ocean. Using typical upstream magnetospheric plasma parameters and a magnetic dipole corresponding to the inductive response inside the moon, we show that the model results agree well with observations for the C3 and C9 flybys, but agrees poorly with the C10 flyby close to Callisto. The study does support the existence of a subsurface ocean at Callisto. C1 [Lindkvist, Jesper; Holmstrom, Mats; Barabash, Stas] Swedish Inst Space Phys, S-98128 Kiruna, Sweden. [Lindkvist, Jesper] Umea Univ, Dept Phys, Umea, Sweden. [Khurana, Krishan K.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. [Fatemi, Shahab] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Fatemi, Shahab] NASA, Ames Res Ctr, Solar Syst Explorat Res Virtual Inst, Moffett Field, CA 94035 USA. RP Lindkvist, J (reprint author), Swedish Inst Space Phys, S-98128 Kiruna, Sweden. EM jesper@irf.se OI Holmstrom, Mats/0000-0001-5494-5374 FU Swedish National Space Board (SNSB) FX This research was conducted using resources provided by the Swedish National Infrastructure for Computing (SNIC) at the High Performance Computing Center North (HPC2N), Umea University, Sweden. The software used in this work was in part developed by the DOE NNSA-ASC OASCR Flash Center at the University of Chicago. The hybrid solver is part of the openly available FLASH code and can be downloaded from http://flash.uchicago.edu/. The simulation results are available from the corresponding author on request. MAG data from the Galileo orbiter is publicly available via the NASA Planetary Data System (PDS) archive. Jesper Lindkvist is funded by the Swedish National Space Board (SNSB). NR 19 TC 8 Z9 8 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2015 VL 120 IS 6 BP 4877 EP 4889 DI 10.1002/2015JA021212 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN1RZ UT WOS:000358199100059 ER PT J AU Connor, HK Raeder, J Sibeck, DG Trattner, KJ AF Connor, H. K. Raeder, J. Sibeck, D. G. Trattner, K. J. TI Relation between cusp ion structures and dayside reconnection for four IMF clock angles: OpenGGCM-LTPT results SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE cusp ion dispersions; dayside reconnection; MHD simulation; test particle simulation ID INTERPLANETARY MAGNETIC-FIELD; MAGNETOPAUSE RECONNECTION; MAGNETOSPHERIC CUSPS; MIDALTITUDE CUSP; PRECIPITATION; SIMULATIONS; CONVECTION; MODEL AB When, where, and which type of reconnection (antiparallel or component) happens on the dayside magnetopause are long-standing unsolved questions due to insufficient in situ observation of reconnection sites. Previous studies showed that the dispersed ion signatures observed in the magnetospheric cusps depend on the reconnection mechanism, suggesting that cusp ion signatures can be a good tool to investigate the locations and properties of dayside reconnection. We investigate this close relation between cusp signatures and magnetopause reconnection for four different interplanetary magnetic field (IMF) clock angles (CA) using the Open Global Geospace Circulation Model (OpenGGCM) and the Liouville Theorem Particle Tracer(LTPT). OpenGGCM produces dayside reconnection under the resistive MHD theory, and LTPT calculates cusp ion signatures caused by the simulated reconnection. Our model results show that for CA = 0 degrees, antiparallel reconnection at both the northern and southern lobes causes a reverse dispersion in which ion energies increase with increasing latitude. For CA = 60 degrees, unsteady antiparallel reconnection at both the northern and southern lobes causes double reverse dispersions. For CA = 120 degrees, component reconnection near the subsolar point produces a dispersionless signature in the low-latitude cusp, and antiparallel reconnection on the duskside northern magnetopause produces a normal dispersion in the high-latitude cusp in which ion energies decrease with increasing latitude. For CA = 180 degrees, antiparallel reconnection near the subsolar point causes a normal dispersion. C1 [Connor, H. K.; Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Raeder, J.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Trattner, K. J.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. RP Connor, HK (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. EM hyunju.k.connor@nasa.gov FU National Aeronautics and Space Administration [NNX10AL07G]; NSF MRI program [PHY-1229408] FX The simulation data of this paper are available upon request. This work was supported by grant NNX10AL07G from the National Aeronautics and Space Administration, and an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. Computations were performed on Trillian, a Cray XE6m-200 super-computer at UNH supported by the NSF MRI program under grant PHY-1229408. NR 38 TC 1 Z9 1 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2015 VL 120 IS 6 BP 4890 EP 4906 DI 10.1002/2015JA021156 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN1RZ UT WOS:000358199100060 ER PT J AU Qian, XS Wu, S Furman, E Zhang, QM Su, J AF Qian, Xiaoshi Wu, Shan Furman, Eugene Zhang, Q. M. Su, Ji TI Ferroelectric polymers as multifunctional electroactive materials: recent advances, potential, and challenges SO MRS COMMUNICATIONS LA English DT Article ID POLY(VINYLIDENE FLUORIDE-TRIFLUOROETHYLENE) COPOLYMER; HIGH-DIELECTRIC-CONSTANT; ENHANCED ENERGY-STORAGE; ELECTROCALORIC REFRIGERATION; ELECTROMECHANICAL PROPERTIES; VINYLIDENE FLUORIDE; ROOM-TEMPERATURE; WORKING BODY; BEHAVIOR; NANOCOMPOSITES AB As multifunctional electroactive materials, ferroelectric polymers are unique owing to their exceptionally high dielectric strength (>600 MV/m), high flexibility, and easy and low-temperature fabrication into required shapes. Although polyvinylidene difluoride (PVDF)-based ferroelectric polymers have been known for several decades, recent findings reveal the potential of this class of electroactive polymers (EAPs) to achieve giant electroactive responses by tuning the molecular, nano, and meso-structures. This paper presents these advances, including giant electrocaloric effect, giant electroactuation, and large, hysteresis-free polarization response. New developments in materials benefit applications, such as environmentally benign and potentially highly energy-efficient electrical field controlled solid-state refrigeration, artificial muscles, and high-energy and power density electric energy storage devices. The challenges in developing these materials to realize these applications, and strategies to further improve the responses of EAPs will be also discussed. C1 [Qian, Xiaoshi; Wu, Shan; Furman, Eugene; Zhang, Q. M.] Penn State Univ, Dept Elect Engn, University Pk, PA 16802 USA. [Qian, Xiaoshi; Wu, Shan; Furman, Eugene; Zhang, Q. M.] Penn State Univ, Mat Res Inst, University Pk, PA 16802 USA. [Su, Ji] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Qian, XS (reprint author), Penn State Univ, Dept Elect Engn, University Pk, PA 16802 USA. EM xyq5004@psu.edu; qxz1@psu.edu FU U.S. DoE, Office of Basic Energy Sciences, Division of Materials Science and Engineering [DE-FG02-07ER46410]; Office of Naval Research [N00014-14-1-0109] FX The research of ECE in modified ferroelectric PVDF-based polymers was supported by U.S. DoE, Office of Basic Energy Sciences, Division of Materials Science and Engineering under Award No. DE-FG02-07ER46410. The research of PVDF based polymers for capacitor application was supported by the Office of Naval Research, under grant No. N00014-14-1-0109. NR 118 TC 1 Z9 1 U1 9 U2 44 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 2159-6859 EI 2159-6867 J9 MRS COMMUN JI MRS Commun. PD JUN PY 2015 VL 5 IS 2 BP 115 EP 129 DI 10.1557/mrc.2015.20 PG 15 WC Materials Science, Multidisciplinary SC Materials Science GA CN1AK UT WOS:000358147300003 ER PT J AU AghaKouchak, A Farahmand, A Melton, FS Teixeira, J Anderson, MC Wardlow, BD Hain, CR AF AghaKouchak, A. Farahmand, A. Melton, F. S. Teixeira, J. Anderson, M. C. Wardlow, B. D. Hain, C. R. TI Remote sensing of drought: Progress, challenges and opportunities SO REVIEWS OF GEOPHYSICS LA English DT Review DE drought; remote sensing ID LAND-SURFACE TEMPERATURE; SNOW WATER EQUIVALENT; MONITORING METEOROLOGICAL DROUGHT; POLARIZATION DIFFERENCE INDEX; VEGETATION CONDITION INDEX; PASSIVE MICROWAVE SENSORS; NINO SOUTHERN-OSCILLATION; EUCALYPTUS-MACULATA HOOK; AMAZON RAIN-FORESTS; SOIL-MOISTURE INDEX AB This review surveys current and emerging drought monitoring approaches using satellite remote sensing observations from climatological and ecosystem perspectives. We argue that satellite observations not currently used for operational drought monitoring, such as near-surface air relative humidity data from the Atmospheric Infrared Sounder mission, provide opportunities to improve early drought warning. Current and future satellite missions offer opportunities to develop composite and multi-indicator drought models. While there are immense opportunities, there are major challenges including data continuity, unquantified uncertainty, sensor changes, and community acceptability. One of the major limitations of many of the currently available satellite observations is their short length of record. A number of relevant satellite missions and sensors (e.g., the Gravity Recovery and Climate Experiment) provide only a decade of data, which may not be sufficient to study droughts from a climate perspective. However, they still provide valuable information about relevant hydrologic and ecological processes linked to this natural hazard. Therefore, there is a need for models and algorithms that combine multiple data sets and/or assimilate satellite observations into model simulations to generate long-term climate data records. Finally, the study identifies a major gap in indicators for describing drought impacts on the carbon and nitrogen cycle, which are fundamental to assessing drought impacts on ecosystems. C1 [AghaKouchak, A.; Farahmand, A.] Univ Calif Irvine, Ctr Hydrometeorol & Remote Sensing, Irvine, CA 92697 USA. [Melton, F. S.] NASA Ames Res Ctr Cooperat Res Earth Sci & Techno, Moffett Field, CA USA. [Teixeira, J.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91125 USA. [Anderson, M. C.] ARS, USDA, Beltsville, MD USA. [Wardlow, B. D.] Univ Nebraska, Sch Nat Resources, Lincoln, NE USA. [Hain, C. R.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. RP AghaKouchak, A (reprint author), Univ Calif Irvine, Ctr Hydrometeorol & Remote Sensing, Irvine, CA 92697 USA. EM amir.a@uci.edu RI Anderson, Martha/C-1720-2015 OI Anderson, Martha/0000-0003-0748-5525 FU National Aeronautics and Space Administration (NASA) [NNX15AC27G] FX This study is supported by the National Aeronautics and Space Administration (NASA) award NNX15AC27G. The input data sets and final outputs presented in this paper are all freely available through the Global Integrated Drought Monitoring and Prediction System (GIDMaPS; http://drought.eng.uci.edu/), and the NOAA/NIDIS Global Vegetation Health data (http://www.star.nesdis.noaa.gov/smcd/emb/vci/VH/). NR 329 TC 29 Z9 30 U1 26 U2 107 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 8755-1209 EI 1944-9208 J9 REV GEOPHYS JI Rev. Geophys. PD JUN PY 2015 VL 53 IS 2 BP 452 EP 480 DI 10.1002/2014RG000456 PG 29 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN3JO UT WOS:000358322200008 ER PT J AU Richardson, IG von Rosenvinge, TT Cane, HV AF Richardson, I. G. von Rosenvinge, T. T. Cane, H. V. TI The Properties of Solar Energetic Particle Event-Associated Coronal Mass Ejections Reported in Different CME Catalogs SO SOLAR PHYSICS LA English DT Article DE Coronal mass ejections; Solar energetic particles; STEREO; SOHO ID ASYMMETRIC CONE MODEL; PEAK INTENSITIES; AUTOMATIC DETECTION; PROTON EVENTS; HALO CMES; CYCLE 23; EARTH; SHOCK; ACCELERATION; DEPENDENCE AB We compare estimates of the speed and width of coronal mass ejections (CMEs) in several catalogs for the CMEs associated with similar to 200 solar energetic particle (SEP) events in 2006 - 2013 that included 25 MeV protons. The catalogs used are: CDAW, CACTUS, SEEDS, and CORIMP, all derived from observations by the LASCO coronagraphs on the SOHO spacecraft, the CACTUS catalog derived from the COR2 coronagraphs on the STEREO-A and -B spacecraft, and the DONKI catalog, which uses observations from SOHO and the STEREO spacecraft. We illustrate how, for this set of events, CME parameters can differ considerably in each catalog. The well-known correlation between CME speed and proton event intensity is shown to be similar for most catalogs, but this is largely because it is determined by a few large particle events associated with fast CMEs, and small events associated with slow CMEs. Intermediate particle events "shuffle" in position when speeds from different catalogs are used. Quadrature spacecraft CME speeds do not improve the correlation. CME widths also vary widely between catalogs, and they are influenced by plane-of-the-sky projection and how the width is inferred from the coronagraph images. The high degree of association (similar to 50 %) between the 25 MeV proton events and "full halo" (360 degrees-width) CMEs as defined in the CDAW catalog is removed when other catalogs are considered. Using CME parameters from the quadrature spacecraft, the SEP intensity is correlated with CME width, which is also correlated with CME speed. C1 [Richardson, I. G.; von Rosenvinge, T. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Richardson, I. G.] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Richardson, I. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Cane, H. V.] Bruny Isl Radio Spectrometer, Bruny Isl, Tas, Australia. RP Richardson, IG (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM ian.g.richardson@nasa.gov; tycho.t.vonrosenvinge@nasa.gov; hcane@utas.edu.au OI Richardson, Ian/0000-0002-3855-3634 FU NASA FX We thank the many individuals who have contributed to the development of the CME catalogs used in this study. The LASCO CME catalog is compiled at the CDAW Data Center by NASA and The Catholic University of America in cooperation with the Naval Research Laboratory. The CACTUS CME catalog is maintained by the Solar Influences Data Analysis Center at the Royal Observatory of Belgium. SEEDS is compiled at the Space Weather Laboratory of George Mason University and is supported by the NASA Living With a Star Program and NASA Applied Information Systems Research Program. The Institute for Astronomy of the University of Hawaii produces the CORIMP catalog. DONKI is developed at the Community Coordinated Modeling Center, NASA Goddard Space Flight Center. SOHO is a project of international cooperation between ESA and NASA. We thank Leila Mays for information about the DONKI database. This work was supported by the NASA Living With a Star Program as part of the activities of the Focussed Science Team studying the variability of solar energetic particle events. NR 47 TC 2 Z9 2 U1 1 U2 8 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 JUN PY 2015 VL 290 IS 6 BP 1741 EP 1759 DI 10.1007/s11207-015-0701-4 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM9YX UT WOS:000358068200012 ER PT J AU Mays, ML Taktakishvili, A Pulkkinen, A MacNeice, PJ Rastatter, L Odstrcil, D Jian, LK Richardson, IG LaSota, JA Zheng, Y Kuznetsova, MM AF Mays, M. L. Taktakishvili, A. Pulkkinen, A. MacNeice, P. J. Rastaetter, L. Odstrcil, D. Jian, L. K. Richardson, I. G. LaSota, J. A. Zheng, Y. Kuznetsova, M. M. TI Ensemble Modeling of CMEs Using the WSA-ENLIL plus Cone Model SO SOLAR PHYSICS LA English DT Article DE Coronal mass ejections, modeling; Coronal mass ejections, interplanetary; Coronal mass ejections, forecasting ID CORONAL MASS EJECTIONS; ENERGETIC PARTICLE EVENT; 2013 APRIL 11; SOLAR-WIND; 3-DIMENSIONAL PROPAGATION; INTERPLANETARY SHOCKS; INNER HELIOSPHERE; WHITE-LIGHT; FORECASTS; EVOLUTION AB Ensemble modeling of coronal mass ejections (CMEs) provides a probabilistic forecast of CME arrival time that includes an estimation of arrival-time uncertainty from the spread and distribution of predictions and forecast confidence in the likelihood of CME arrival. The real-time ensemble modeling of CME propagation uses the Wang-Sheeley-Arge (WSA)-ENLIL+Cone model installed at the Community Coordinated Modeling Center (CCMC) and executed in real-time at the CCMC/Space Weather Research Center. The current implementation of this ensemble-modeling method evaluates the sensitivity of WSA-ENLIL+Cone model simulations of CME propagation to initial CME parameters. We discuss the results of real-time ensemble simulations for a total of 35 CME events that occurred between January 2013 -aEuro parts per thousand July 2014. For the 17 events where the CME was predicted to arrive at Earth, the mean absolute arrival-time prediction error was 12.3 hours, which is comparable to the errors reported in other studies. For predictions of CME arrival at Earth, the correct-rejection rate is 62 %, the false-alarm rate is 38 %, the correct-alarm ratio is 77 %, and the false-alarm ratio is 23 %. The arrival time was within the range of the ensemble arrival predictions for 8 out of 17 events. The Brier Score for CME arrival-predictions is 0.15 (where a score of 0 on a range of 0 to 1 is a perfect forecast), which indicates that on average, the predicted probability, or likelihood, of CME arrival is fairly accurate. The reliability of ensemble CME-arrival predictions is heavily dependent on the initial distribution of CME input parameters (e.g. speed, direction, and width), particularly the median and spread. Preliminary analysis of the probabilistic forecasts suggests undervariability, indicating that these ensembles do not sample a wide-enough spread in CME input parameters. Prediction errors can also arise from ambient-model parameters, the accuracy of the solar-wind background derived from coronal maps, or other model limitations. Finally, predictions of the K (P) geomagnetic index differ from observed values by less than one for 11 out of 17 of the ensembles and K (P) prediction errors computed from the mean predicted K (P) show a mean absolute error of 1.3. C1 [Mays, M. L.; Taktakishvili, A.] Catholic Univ Amer, Washington, DC 20064 USA. [Mays, M. L.; Taktakishvili, A.; Pulkkinen, A.; MacNeice, P. J.; Rastaetter, L.; Odstrcil, D.; Jian, L. K.; Zheng, Y.; Kuznetsova, M. M.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Odstrcil, D.] George Mason Univ, Fairfax, VA 22030 USA. [Jian, L. K.; Richardson, I. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Richardson, I. G.] Univ Maryland, Dept Astron, CRESST, College Pk, MD 20742 USA. [LaSota, J. A.] Univ Illinois, Champaign, IL USA. RP Mays, ML (reprint author), Catholic Univ Amer, Washington, DC 20064 USA. EM m.leila.mays@nasa.gov RI Jian, Lan/B-4053-2010; OI Jian, Lan/0000-0002-6849-5527; Richardson, Ian/0000-0002-3855-3634 FU NSF [AGS 1242798, 1321493] FX The work was carried out as a part of NASA's Game Changing Development Program Advanced Radiation Protection Integrated Solar Energetic Proton (ISEP) project. L.K. Jian acknowledges the support of NSF grants AGS 1242798 and 1321493. M.L. Mays thanks T. Nieves-Chinchilla and B.J. Thompson for useful discussions. We gratefully acknowledge the participants of the CME Arrival Time Scoreboard (kauai.ccmc.gsfc.nasa.gov/CMEscoreboard). The ACE and Wind solar-wind plasma and magnetic-field data were obtained at NASA's CDAWeb (cdaweb.gsfc.nasa.gov). OMNI data were obtained from NASA's COHOWeb (omniweb.gsfc.nasa.gov/coho). The Dst geomagnetic index was obtained from the World Data Center for Geomagnetism in Kyoto, Japan. Estimated real-time planetary KP indices are from NOAA and the NGDC, and final definitive KP indices are from the Helmholtz Center Potsdam GFZ German Research Centre for Geosciences. The SOHO/LASCO CME catalog is generated and maintained at the CDAW Data Center by NASA and the Catholic University of America in cooperation with the Naval Research Laboratory. SOHO is a mission of international cooperation between the European Space Agency and NASA. The STEREO/SECCHI data are produced by an international consortium of the NRL, LMSAL and NASA GSFC (USA), RAL and University of Birmingham (UK), MPS (Germany), CSL (Belgium), IOTA and IAS (France). Some figure colors are based on ColorBrewer.org. NR 69 TC 28 Z9 28 U1 1 U2 3 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 JUN PY 2015 VL 290 IS 6 BP 1775 EP 1814 DI 10.1007/s11207-015-0692-1 PG 40 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM9YX UT WOS:000358068200014 ER PT J AU Aleksi, J Ansoldi, S Antonelli, LA Antoranz, P Babic, A Bangale, P de Almeida, UB Barrio, JA Gonzalez, JB Bednarek, W Bernardini, E Biasuzzi, B Biland, A Blanch, O Boller, A Bonnefoy, S Bonnoli, G Borracci, F Bretz, T Carmona, E Carosi, A Colin, P Colombo, E Contreras, JL Cortina, J Covino, S Da Vela, P Dazzi, F De Angelis, A De Caneva, G De Lotto, B Wilhelmi, ED Mendez, CD Prester, DD Dorner, D Doro, M Einecke, S Eisenacher, D Elsaesser, D Fonseca, MV Font, L Frantzen, K Fruck, C Galindo, D Lopez, RJG Garczarczyk, M Terrats, DG Gaug, M Godinovic, N Munoz, AG Gozzini, SR Hadasch, D Hanabata, Y Hayashida, M Herrera, J Hildebrand, D Hose, J Hrupec, D Hughes, G Idec, W Kadenius, V Kellermann, H Knoetig, ML Kodani, K Konno, Y Krause, J Kubo, H Kushida, J La Barbera, A Lelas, D Lewandowska, N Lindfors, E Lombardi, S Lopez, M Lopez-Coto, R Lopez-Oramas, A Lorenz, E Lozano, I Makariev, M Mallot, K Maneva, G Mankuzhiyil, N Mannheim, K Maraschi, L Marcote, B Mariotti, M Martinez, M Mazin, D Menzel, U Miranda, JM Mirzoyan, R Moralejo, A Munar-Adrover, P Nakajima, D Niedzwiecki, A Nilsson, K Nishijima, K Noda, K Orito, R Overkemping, A Paiano, S Palatiello, M Paneque, D Paoletti, R Paredes, JM Paredes-Fortuny, X Persic, M Moroni, PGP Prandini, E Puljak, I Reinthal, R Rhode, W Ribo, M Rico, J Garcia, JR Rugamer, S Saito, T Saito, K Satalecka, K Scalzotto, V Scapin, V Schultz, C Schweizer, T Sun, S Shore, SN Sillanpaa, A Sitarek, J Snidaric, I Sobczynska, D Spanier, F Stamatescu, V Stamerra, A Steinbring, T Steinke, B Storz, J Strzys, M Takalo, L Takami, H Tavecchio, F Temnikov, P Terzic, T Tescaro, D Teshima, M Thaele, J Tibolla, O Torres, DF Toyama, T Treves, A Uellenbeck, M Vogler, P Zanin, R Archambault, S Archer, A Beilicke, M Benbow, W Berger, K Bird, R Biteau, J Buckley, JH Bugaev, V Cerruti, M Chen, X Ciupik, L Collins-Hughes, E Cui, W Eisch, JD Falcone, A Feng, Q Finley, JP Fortin, P Fortson, L Furniss, A Galante, N Gillanders, GH Griffin, S Gyuk, G Hakansson, N Holder, J Johnson, CA Kaaret, P Kar, P Kertzman, M Kieda, D Lang, MJ McArthur, S McCann, A Meagher, K Millis, J Moriarty, P Ong, RA Otte, AN Perkins, JS Pichel, A Pohl, M Popkow, A Prokoph, H Pueschel, E Ragan, K Reyes, LC Reynolds, PT Richards, GT Roache, E Rovero, AC Sembroski, GH Shahinyan, K Staszak, D Telezhinsky, I Tucci, JV Tyler, J Varlotta, A Wakely, SP Welsing, R Wilhelm, A Williams, DA Buson, S Finke, J Villata, M Raiteri, C Aller, HD Aller, MF Cesarini, A Chen, WP Gurwell, MA Jorstad, SG Kimeridze, GN Koptelova, E Kurtanidze, OM Kurtanidze, SO Lahteenmaki, A Larionov, VM Larionova, EG Lin, HC McBreen, B Moody, JW Morozova, DA Marscher, AP Max-Moerbeck, W Nikolashvili, MG Perri, M Readhead, ACS Richards, JL Ros, JA Sadun, AC Sakamoto, T Sigua, LA Smith, PS Tornikoski, M Troitsky, IS Wehrle, AE Jordan, B AF Aleksi, J. Ansoldi, S. Antonelli, L. A. Antoranz, P. Babic, A. Bangale, P. de Almeida, U. Barres Barrio, J. A. Gonzalez, J. Becerra Bednarek, W. Bernardini, E. Biasuzzi, B. Biland, A. Blanch, O. Boller, A. Bonnefoy, S. Bonnoli, G. Borracci, F. Bretz, T. Carmona, E. Carosi, A. Colin, P. Colombo, E. Contreras, J. L. Cortina, J. Covino, S. Da Vela, P. Dazzi, F. De Angelis, A. De Caneva, G. De Lotto, B. Wilhelmi, E. de Ona Mendez, C. Delgado Prester, D. Dominis Dorner, D. Doro, M. Einecke, S. Eisenacher, D. Elsaesser, D. Fonseca, M. V. Font, L. Frantzen, K. Fruck, C. Galindo, D. Lopez, R. J. Garcia Garczarczyk, M. Terrats, D. Garrido Gaug, M. Godinovic, N. Munoz, A. Gonzalez Gozzini, S. R. Hadasch, D. Hanabata, Y. Hayashida, M. Herrera, J. Hildebrand, D. Hose, J. Hrupec, D. Hughes, G. Idec, W. Kadenius, V. Kellermann, H. Knoetig, M. L. Kodani, K. Konno, Y. Krause, J. Kubo, H. Kushida, J. La Barbera, A. Lelas, D. Lewandowska, N. Lindfors, E. Lombardi, S. Lopez, M. Lopez-Coto, R. Lopez-Oramas, A. Lorenz, E. Lozano, I. Makariev, M. Mallot, K. Maneva, G. Mankuzhiyil, N. Mannheim, K. Maraschi, L. Marcote, B. Mariotti, M. Martinez, M. Mazin, D. Menzel, U. Miranda, J. M. Mirzoyan, R. Moralejo, A. Munar-Adrover, P. Nakajima, D. Niedzwiecki, A. Nilsson, K. Nishijima, K. Noda, K. Orito, R. Overkemping, A. Paiano, S. Palatiello, M. Paneque, D. Paoletti, R. Paredes, J. M. Paredes-Fortuny, X. Persic, M. Moroni, P. G. Prada Prandini, E. Puljak, I. Reinthal, R. Rhode, W. Ribo, M. Rico, J. Garcia, J. Rodriguez Rugamer, S. Saito, T. Saito, K. Satalecka, K. Scalzotto, V. Scapin, V. Schultz, C. Schweizer, T. Sun, S. Shore, S. N. Sillanpaa, A. Sitarek, J. Snidaric, I. Sobczynska, D. Spanier, F. Stamatescu, V. Stamerra, A. Steinbring, T. Steinke, B. Storz, J. Strzys, M. Takalo, L. Takami, H. Tavecchio, F. Temnikov, P. Terzic, T. Tescaro, D. Teshima, M. Thaele, J. Tibolla, O. Torres, D. F. Toyama, T. Treves, A. Uellenbeck, M. Vogler, P. Zanin, R. Archambault, S. Archer, A. Beilicke, M. Benbow, W. Berger, K. Bird, R. Biteau, J. Buckley, J. H. Bugaev, V. Cerruti, M. Chen, X. Ciupik, L. Collins-Hughes, E. Cui, W. Eisch, J. D. Falcone, A. Feng, Q. Finley, J. P. Fortin, P. Fortson, L. Furniss, A. Galante, N. Gillanders, G. H. Griffin, S. Gyuk, G. Hakansson, N. Holder, J. Johnson, C. A. Kaaret, P. Kar, P. Kertzman, M. Kieda, D. Lang, M. J. McArthur, S. McCann, A. Meagher, K. Millis, J. Moriarty, P. Ong, R. A. Otte, A. N. Perkins, J. S. Pichel, A. Pohl, M. Popkow, A. Prokoph, H. Pueschel, E. Ragan, K. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Rovero, A. C. Sembroski, G. H. Shahinyan, K. Staszak, D. Telezhinsky, I. Tucci, J. V. Tyler, J. Varlotta, A. Wakely, S. P. Welsing, R. Wilhelm, A. Williams, D. A. Buson, S. Finke, J. Villata, M. Raiteri, C. Aller, H. D. Aller, M. F. Cesarini, A. Chen, W. P. Gurwell, M. A. Jorstad, S. G. Kimeridze, G. N. Koptelova, E. Kurtanidze, O. M. Kurtanidze, S. O. Lahteenmaki, A. Larionov, V. M. Larionova, E. G. Lin, H. C. McBreen, B. Moody, J. W. Morozova, D. A. Marscher, A. P. Max-Moerbeck, W. Nikolashvili, M. G. Perri, M. Readhead, A. C. S. Richards, J. L. Ros, J. A. Sadun, A. C. Sakamoto, T. Sigua, L. A. Smith, P. S. Tornikoski, M. Troitsky, I. S. Wehrle, A. E. Jordan, B. CA MAGIC Collaboration VERITAS Collaboration TI Unprecedented study of the broadband emission of Mrk 421 during flaring activity in March 2010 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radiation mechanisms: non-thermal; galaxies: active; BL Lacertae objects: individual: Mrk 421; gamma rays: galaxies ID LARGE-AREA TELESCOPE; BL LACERTAE OBJECTS; GAMMA-RAY OUTBURST; SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS; ATMOSPHERIC CHERENKOV TELESCOPES; EXTRAGALACTIC BACKGROUND LIGHT; SPECTRAL ENERGY-DISTRIBUTION; SELF-COMPTON MODEL; X-RAY; TEV BLAZARS AB Context. Because of its proximity, Mrk 421 is one of the best sources on which to study the nature of BL Lac objects. Its proximity allows us to characterize its broadband spectral energy distribution (SED). Aims. The goal is to better understand the mechanisms responsible for the broadband emission and the temporal evolution of Mrk 421. These mechanisms may also apply to more distant blazars that cannot be studied with the same level of detail. Methods. A flare occurring in March 2010 was observed for 13 consecutive days (from MJD 55 265 to MJD 55 277) with unprecedented wavelength coverage from radio to very high energy (VHE; E > 100 GeV) gamma-rays with MAGIC, VERITAS, Whipple, Fermi-LAT, MAXI, RXTE, Swift, GASP-WEBT, and several optical and radio telescopes. We modeled the day-scale SEDs with one-zone and two-zone synchrotron self-Compton (SSC) models, investigated the physical parameters, and evaluated whether the observed broadband SED variability can be associated with variations in the relativistic particle population. Results. The activity of Mrk 421 initially was high and then slowly decreased during the 13-day period. The flux variability was remarkable at the X-ray and VHE bands, but it was minor or not significant at the other bands. The variability in optical polarization was also minor. These observations revealed an almost linear correlation between the X-ray flux at the 2-10 keV band and the VHE gamma-ray flux above 200 GeV, consistent with the gamma-rays being produced by inverse-Compton scattering in the Klein-Nishina regime in the framework of SSC models. The one-zone SSC model can describe the SED of each day for the 13 consecutive days reasonably well, which once more shows the success of this standard theoretical scenario to describe the SEDs of VHE BL Lacs such as Mrk 421. This flaring activity is also very well described by a two-zone SSC model, where one zone is responsible for the quiescent emission, while the other smaller zone, which is spatially separated from the first, contributes to the daily variable emission occurring at X-rays and VHE gamma-rays. The second blob is assumed to have a smaller volume and a narrow electron energy distribution with 3 x 10(4) < gamma < 6 x 10(5), where. is the Lorentz factor of the electrons. Such a two-zone scenario would naturally lead to the correlated variability at the X-ray and VHE bands without variability at the optical/UV band, as well as to shorter timescales for the variability at the X-ray and VHE bands with respect to the variability at the other bands. Conclusions. Both the one-zone and the two-zone SSC models can describe the daily SEDs via the variation of only four or five model parameters, under the hypothesis that the variability is associated mostly with the underlying particle population. This shows that the particle acceleration and cooling mechanism that produces the radiating particles might be the main mechanism responsible for the broadband SED variations during the flaring episodes in blazars. The two-zone SSC model provides a better agreement with the observed SED at the narrow peaks of the low-and high-energy bumps during the highest activity, although the reported one-zone SSC model could be further improved by varying the parameters related to the emitting region itself (delta, B and R), in addition to the parameters related to the particle population. C1 [Aleksi, J.; Blanch, O.; Cortina, J.; Munoz, A. Gonzalez; Lopez-Coto, R.; Lopez-Oramas, A.; Martinez, M.; Moralejo, A.; Rico, J.; Sitarek, J.; Stamatescu, V.] Campus UAB, IFAE, Bellaterra 08193, Spain. [Ansoldi, S.; Biasuzzi, B.; De Angelis, A.; De Lotto, B.; Mankuzhiyil, N.; Palatiello, M.; Persic, M.] Univ Udine, I-33100 Udine, Italy. 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EM dpaneque@mpp.mpg.de; sysun@mpp.mpg.de; takami@post.kek.jp RI Fonseca Gonzalez, Maria Victoria/I-2004-2015; Temnikov, Petar/L-6999-2016; Maneva, Galina/L-7120-2016; Makariev, Martin/M-2122-2016; Torres, Diego/O-9422-2016; Delgado, Carlos/K-7587-2014; Barrio, Juan/L-3227-2014; Martinez Rodriguez, Manel/C-2539-2017; Cortina, Juan/C-2783-2017; Lahteenmaki, Anne/L-5987-2013; Larionov, Valeri/H-1349-2013; Font, Lluis/L-4197-2014; Contreras Gonzalez, Jose Luis/K-7255-2014; Lopez Moya, Marcos/L-2304-2014; Morozova, Daria/H-1298-2013; Larionova, Elena/H-7287-2013; Troitskiy, Ivan/K-7979-2013; Jorstad, Svetlana/H-6913-2013; GAug, Markus/L-2340-2014; Miranda, Jose Miguel/F-2913-2013; Stamatescu, Victor/C-9945-2016 OI Bonnoli, Giacomo/0000-0003-2464-9077; Antonelli, Lucio Angelo/0000-0002-5037-9034; Stamerra, Antonio/0000-0002-9430-5264; Prandini, Elisa/0000-0003-4502-9053; Becerra Gonzalez, Josefa/0000-0002-6729-9022; Bird, Ralph/0000-0002-4596-8563; Doro, Michele/0000-0001-9104-3214; Covino, Stefano/0000-0001-9078-5507; de Ona Wilhelmi, Emma/0000-0002-5401-0744; LA BARBERA, ANTONINO/0000-0002-5880-8913; Cesarini, Andrea/0000-0002-8611-8610; Villata, Massimo/0000-0003-1743-6946; Fonseca Gonzalez, Maria Victoria/0000-0003-2235-0725; De Lotto, Barbara/0000-0003-3624-4480; Perri, Matteo/0000-0003-3613-4409; Persic, Massimo/0000-0003-1853-4900; Raiteri, Claudia Maria/0000-0003-1784-2784; Temnikov, Petar/0000-0002-9559-3384; Torres, Diego/0000-0002-1522-9065; Delgado, Carlos/0000-0002-7014-4101; Barrio, Juan/0000-0002-0965-0259; Cortina, Juan/0000-0003-4576-0452; Pueschel, Elisa/0000-0002-0529-1973; Prada Moroni, Pier Giorgio/0000-0001-9712-9916; Larionov, Valeri/0000-0002-4640-4356; Font, Lluis/0000-0003-2109-5961; Contreras Gonzalez, Jose Luis/0000-0001-7282-2394; Lopez Moya, Marcos/0000-0002-8791-7908; Morozova, Daria/0000-0002-9407-7804; Larionova, Elena/0000-0002-2471-6500; Troitskiy, Ivan/0000-0002-4218-0148; Jorstad, Svetlana/0000-0001-9522-5453; GAug, Markus/0000-0001-8442-7877; Miranda, Jose Miguel/0000-0002-1472-9690; Stamatescu, Victor/0000-0001-9030-7513 FU German BMBF; German MPG; Italian INFN; Italian INAF; Swiss National Fund SNF; ERDF under the Spanish MINECO; Japanese JSPS; Japanese MEXT; Centro de Excelencia Severo Ochoa project of the Spanish Consolider-Ingenio programme [SEV-2012-0234]; CPAN project of the Spanish Consolider-Ingenio programme [CSD2007-00042]; MultiDark project of the Spanish Consolider-Ingenio programme [CSD2009-00064]; Academy of Finland [268740, 212656, 210338, 121148]; Croatian Science Foundation (HrZZ) Project [09/176]; University of Rijeka [13.12.1.3.02]; DFG Collaborative Research Centers [SFB823/C4, SFB876/C3]; Polish MNiSzW [745/N-HESS-MAGIC/2010/0]; US Department of Energy Office of Science; US National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the UK; NASA [NNX11AQ03G, NNX08AW31G, NNX11A043G]; Academia Sinica; NSF [AST-0808050, AST-1109911]; Russian RFBR [12-02-00452]; St. Petersburg University [6.0.163.2010, 6.38.71.2012]; Georgian National Science Foundation [GNSF/ST07/4-180]; Shota Rustaveli National Science Foundation [FR/577/6-320/13] FX The authors thank the anonymous referee for providing a very detailed and constructive list of remarks that helped us to improve the manuscript. The MAGIC collaboration would like to thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO, and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Centro de Excelencia Severo Ochoa SEV-2012-0234, CPAN CSD2007-00042, and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 268740 of the Academy of Finland, by the Croatian Science Foundation (HrZZ) Project 09/176 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. The VERITAS collaboration acknowledges supports from the grants from the US Department of Energy Office of Science, the US National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748) and by STFC in the UK. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. 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 research at Boston University was funded in part by NASA Fermi Guest Investigator grant NNX11AQ03G. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The OVRO 40-m monitoring program is supported in part by NASA grants NNX08AW31G and NNX11A043G, and NSF grants AST-0808050 and AST-1109911. The Metsahovi team acknowledges the support from the Academy of Finland to our observing projects (numbers 212656, 210338, 121148, and others). This work was partly supported by Russian RFBR grant 12-02-00452 and St. Petersburg University research grants 6.0.163.2010, 6.38.71.2012. The Abastumani Observatory team acknowledges financial support by the Georgian National Science Foundation through grant GNSF/ST07/4-180 and by the Shota Rustaveli National Science Foundation through the grant FR/577/6-320/13.; We acknowledge the use of public data from the Swift and RXTE data archive. NR 98 TC 11 Z9 11 U1 4 U2 26 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 JUN PY 2015 VL 578 AR A22 DI 10.1051/0004-6361/201424811 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM2IF UT WOS:000357502600034 ER PT J AU Azulay, R Guirado, JC Marcaide, JM Marti-Vidal, I Ros, E Jauncey, DL Lestrade, JF Preston, RA Reynolds, JE Tognelli, E Ventura, P AF Azulay, R. Guirado, J. C. Marcaide, J. M. Marti-Vidal, I. Ros, E. Jauncey, D. L. Lestrade, J. -F. Preston, R. A. Reynolds, J. E. Tognelli, E. Ventura, P. TI Dynamical masses of the low-mass stellar binary AB Doradus B SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrometry; binaries: close; stars: fundamental parameters; stars: pre-main sequence ID MAIN-SEQUENCE TRACKS; EVOLUTIONARY MODELS; MOVING GROUP; ECLIPSING BINARY; QUADRUPLE SYSTEM; AGE; STARS; CONSTRAINTS; PHOTOMETRY; DWARFS AB Context. AB Doradus is the main system of the AB Doradus moving group. It is a quadruple system formed by two widely separated binaries of pre-main-sequence (PMS) stars: AB DorA/C and AB Dor Ba/Bb. The pair AB DorA/C has been extensively studied and its dynamical masses have been determined with high precision, thus making AB DorC a benchmark for calibrating PMS stellar models. If the orbit and dynamical masses of the pair AB Dor Ba/Bb could be determined, they could play a similar role to that of AB DorC in calibrating PMS models, and would also help to better understand the dynamics of the whole AB Doradus system. Aims. We aim to determine the individual masses of the pair AB Dor Ba/Bb using VLBI observations and archive infrared data as part of a larger program that monitors binary systems in the AB Doradus moving group. Methods. We observed the system AB Dor B between 2007 and 2013 with the Australian Long Baseline Array (LBA) at a frequency of 8.4 GHz in phase-reference mode. Results. We detected, for the first time, compact radio emission from both stars in the binary, AB Dor Ba and AB Dor Bb. This result allowed us to determine the orbital parameters of both the relative and absolute orbits and, consequently, their individual dynamical masses: 0 : 28 +/- 0 : 05 M-circle dot and 0 : 25 +/- 0 : 05 M-circle dot, respectively. Conclusions. Comparisons of the dynamical masses with the prediction of PMS evolutionary models show that the models under-predict the dynamical masses of the binary components Ba and Bb by 10-30% and 10-40%, respectively, although they still agree at the 2 sigma level. Some of the stellar models considered favor an age between 50 and 100 Myr for this system, while others predict older ages. We also discuss the evolutionary status of AB Dor Ba/Bb in terms of an earlier double-double star scenario that might explain the strong radio emission detected in both components. C1 [Azulay, R.; Guirado, J. C.; Marcaide, J. M.; Ros, E.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain. [Azulay, R.; Ros, E.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Guirado, J. C.; Ros, E.] Univ Valencia, Obser Astron, Valencia 46980, Spain. [Marti-Vidal, I.] Onsala Space Observ, Chalmers Univ Technol, S-43992 Onsala, Sweden. [Jauncey, D. L.; Reynolds, J. E.] CSIRO Astron & Space Sci, Canberra, ACT 2122, Australia. [Jauncey, D. L.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 0200, Australia. [Lestrade, J. -F.] Observ Paris LERMA, F-75014 Paris, France. [Preston, R. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tognelli, E.] Univ Roma Tor Vergata, Dept Phys, I-00133 Rome, Italy. [Tognelli, E.] INFN, Sect Pisa, I-56127 Pisa, Italy. [Ventura, P.] INAF Observ Rome, I-00040 Monte Porzio Catone, RM, Italy. RP Azulay, R (reprint author), Univ Valencia, Dept Astron & Astrofis, C Dr Moliner 50, E-46100 Valencia, Spain. EM Rebecca.Azulay@uv.es RI Marti-Vidal, Ivan/A-8799-2017; OI Marti-Vidal, Ivan/0000-0003-3708-9611; Ventura, Paolo/0000-0002-5026-6400; Ros, Eduardo/0000-0001-9503-4892 FU Spanish MINECO [AYA2009-13036-C02-02, AYA2012-38491-C02-01]; Generalitat Valenciana [PROMETEO/2009/104, PROMETEOII/2014/057]; Commonwealth of Australia FX This work has been partially supported by the Spanish MINECO projects AYA2009-13036-C02-02 and AYA2012-38491-C02-01 and by the Generalitat Valenciana projects PROMETEO/2009/104 and PROMETEOII/2014/057. The Long Baseline Array is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. We thank J. Montalban for providing the PMS models and for the guidance to use them appropriately. The data used in this study were acquired as part of NASA's Earth Science Data Systems and archived and distributed by the Crustal Dynamics Data Information System (CDDIS). This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. R.A. acknowledges the Max-Planck-Institute fur Radioastronomie for its hospitality and especially J. A. Zensus for support. NR 37 TC 1 Z9 1 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2015 VL 578 AR A16 DI 10.1051/0004-6361/201525704 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM2IF UT WOS:000357502600028 ER PT J AU Benisty, M Juhasz, A Boccaletti, A Avenhaus, H Milli, J Thalmann, C Dominik, C Pinilla, P Buenzli, E Pohl, A Beuzit, JL Birnstiel, T de Boer, J Bonnefoy, M Chauvin, G Christiaens, V Garufi, A Grady, C Henning, T Huelamo, N Isella, A Langlois, M Menard, F Mouillet, D Olofsson, J Pantin, E Pinte, C Pueyo, L AF Benisty, M. Juhasz, A. Boccaletti, A. Avenhaus, H. Milli, J. Thalmann, C. Dominik, C. Pinilla, P. Buenzli, E. Pohl, A. Beuzit, J. -L. Birnstiel, T. de Boer, J. Bonnefoy, M. Chauvin, G. Christiaens, V. Garufi, A. Grady, C. Henning, T. Huelamo, N. Isella, A. Langlois, M. Menard, F. Mouillet, D. Olofsson, J. Pantin, E. Pinte, C. Pueyo, L. TI Asymmetric features in the protoplanetary disk MWC 758 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques: high angular resolution; protoplanetary disks ID HD 142527; IMAGING POLARIMETRY; TRANSITIONAL DISKS; DUST FILTRATION; SPIRAL ARMS; GAP EDGES; PLANET; EVOLUTION; VLT/NACO; MWC-758 AB Context. The study of dynamical processes in protoplanetary disks is essential to understand planet formation. In this context, transition disks are prime targets because they are at an advanced stage of disk clearing and may harbor direct signatures of disk evolution. Aims. We aim to derive new constraints on the structure of the transition disk MWC 758, to detect non-axisymmetric features and understand their origin. Methods. We obtained infrared polarized intensity observations of the protoplanetary disk MWC 758 with VLT/SPHERE at 1.04 mu m to resolve scattered light at a smaller inner working angle (0.093 '') and a higher angular resolution (0.027 '') than previously achieved. Results. We observe polarized scattered light within 0.53 '' (148 au) down to the inner working angle (26 au) and detect distinct non-axisymmetric features but no fully depleted cavity. The two small-scale spiral features that were previously detected with HiCIAO are resolved more clearly, and new features are identified, including two that are located at previously inaccessible radii close to the star. We present a model based on the spiral density wave theory with two planetary companions in circular orbits. The best model requires a high disk aspect ratio (H/r similar to 0.20 at the planet locations) to account for the large pitch angles which implies a very warm disk. Conclusions. Our observations reveal the complex morphology of the disk MWC 758. To understand the origin of the detected features, the combination of high-resolution observations in the submillimeter with ALMA and detailed modeling is needed. C1 [Benisty, M.; Beuzit, J. -L.; Bonnefoy, M.; Chauvin, G.; Menard, F.; Mouillet, D.; Pinte, C.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. [Benisty, M.; Beuzit, J. -L.; Bonnefoy, M.; Chauvin, G.; Menard, F.; Mouillet, D.; Pinte, C.] CNRS, IPAG, F-38000 Grenoble, France. [Juhasz, A.] Inst Astron, Cambridge CB3 OHA, England. [Boccaletti, A.] Univ Paris 07, Univ Paris 06, CNRS, LESIA,Observ Paris, F-92195 Meudon, France. [Avenhaus, H.; Christiaens, V.] Univ Chile, Dept Astron, Santiago, Chile. [Milli, J.; de Boer, J.] ESO, Santiago, Chile. [Thalmann, C.; Garufi, A.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Dominik, C.] Sterrenkundig Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Pinilla, P.; de Boer, J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Buenzli, E.; Pohl, A.; Henning, T.; Olofsson, J.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Pohl, A.] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Birnstiel, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Grady, C.] Eureka Sci, Greenbelt, MD 20771 USA. [Grady, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Huelamo, N.] Ctr Astrobiol INTA CSIC, Villanueva De La Canada 28691, Spain. [Isella, A.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. [Langlois, M.] Univ Lyon 1, CNRS, Ecole Normale Super Lyon, Observ Lyon,Ctr Rech Astrophys Lyon,UMR 5574, F-69230 St Genis Laval, France. [Menard, F.; Pinte, C.] Univ Chile, CNRS INSU, UMI FCA, France UMI 3386, Santiago, Chile. [Menard, F.; Pinte, C.] Univ Chile, Dept Astron, Santiago, Chile. [Pantin, E.] Univ Paris Diderot, CNRS, CEA DSM, Lab AIM,IRFU SAp, F-91191 Gif Sur Yvette, France. [Pueyo, L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Benisty, M (reprint author), Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. EM Myriam.Benisty@obs.ujf-grenoble.fr RI Huelamo, Nuria/C-3042-2017; OI Huelamo, Nuria/0000-0002-2711-8143; Buenzli, Esther/0000-0003-3306-1486; Birnstiel, Tilman/0000-0002-1899-8783 FU "Programme National de Physique Stellaire" (PNPS) of CNRS/INSU, France; NASA Origins of Solar Systems program [NNG13PB64P]; NASA Origins of Solar Systems [NNX12AJ04G] FX We acknowledge the SVT team at ESO HQ for their help during the preparation of the OBs and the VLT team for conducting the observations. We thank C. P. Dullemond, G. Lesur, M. Min, and M. Tauras for fruitful discussions, and the referee for providing useful comments. M.B. acknowledges financial support from "Programme National de Physique Stellaire" (PNPS) of CNRS/INSU, France. C.G. was supported under the NASA Origins of Solar Systems program on NNG13PB64P. T.B. acknowledges support from NASA Origins of Solar Systems grant NNX12AJ04G. NR 41 TC 46 Z9 46 U1 1 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2015 VL 578 AR L6 DI 10.1051/0004-6361/201526011 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM2IF UT WOS:000357502600007 ER PT J AU Couturier-Tamburelli, I Pietri, N Gudipati, MS AF Couturier-Tamburelli, Isabelle Pietri, Nathalie Gudipati, Murthy S. TI Simulation of Titan's atmospheric photochemistry Formation of non-volatile residue from polar nitrile ices SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planets and satellites: surfaces; ultraviolet: planetary systems; astrochemistry; planets and satellites: atmospheres ID ELECTRONICALLY EXCITED-STATES; OPTICAL-CONSTANTS; ABSORPTION-SPECTRA; AEROSOLS ANALOGS; ACETYLENE; CHEMISTRY; THOLINS; HAZE; MOLECULES; HC5N AB We studied the photochemistry of frozen ice of a polar Titan's atmospheric molecule cyanodiacetylene (HC5N) to determine the possible contribution of this compound to the lower altitude photochemistry of haze layers found on Titan. We used infrared analysis to examine the residue produced by irradiation of solid HC5N at lambda > 300 nm. The resulting polymer is orange-brown in color. Based on theoretical analysis and the general tendency of HC5N and C4N2 to undergo similar ice photochemistry at longer wavelengths accessible in Titan's lower atmosphere, we conclude that Titan's lower atmosphere is photochemically active in the regions of cloud, ice, and aerosol formation. C4N2 is a symmetric molecule with no net dipole moment whereas, HC5N has a large dipole moment of similar to 4 D. Consequently, though both these molecules have very similar molecular weight and size, their sublimation temperatures are different, HC5N subliming around 170K compared to 160K for C4N2. Based on our studies we conclude that in Titan's atmosphere the cyanoacetylene class of molecules (HCN, HC3N, HC5N, etc.) would condense first followed by the dicyanoacetylenes (C2N2, C4N2, C6N2, etc.), leading to fractionation of different class of molecules. From the fluxes used in the laboratory and depletion of the original HC5N signals, we estimate Titan's haze ice photochemistry involving polar nitriles to be significant and very similar to their non-polar counterparts. C1 [Couturier-Tamburelli, Isabelle; Pietri, Nathalie] Aix Marseille Univ, CNRS, UMR 7345, PIIM, F-13013 Marseille, France. [Gudipati, Murthy S.] CALTECH, Jet Prop Lab, Ice Spect Lab, Div Sci, Pasadena, CA 91109 USA. RP Couturier-Tamburelli, I (reprint author), Aix Marseille Univ, CNRS, UMR 7345, PIIM, F-13013 Marseille, France. EM isabelle.couturier@univ-amu.fr; gudipati@jpl.nasa.gov RI Gudipati, Murthy/F-7575-2011 FU French National Program Environnements Planetaires et Origines de la Vie (EPOV); NASA Astrobiology Institute; Jet Propulsion Laboratory Director's Research and Development Fund; JPL Research and Technology Development funding for the infrastructure of the ice spectroscopy laboratory (ISL); Titan organic aerosol spectroscopy and chemistry (TOAST) laboratory at JPL; National Aeronautics and Space Administration FX This work was funded by the French National Program Environnements Planetaires et Origines de la Vie (EPOV). The JPL part of the work is partly supported by several of the following funding sources: NASA Astrobiology Institute team "Titan as a Prebiotic Chemical System", the Jet Propulsion Laboratory Director's Research and Development Fund, and the JPL Research and Technology Development funding for the infrastructure of the ice spectroscopy laboratory (ISL) and Titan organic aerosol spectroscopy and chemistry (TOAST) laboratory at JPL. Research carried out at the Jet Propulsion Laboratory, California Institute of Technology was under a contract with the National Aeronautics and Space Administration. We thank Mr. Tim Hempel for helping in preparing the manuscript to be suitable for the A&A format. NR 57 TC 0 Z9 0 U1 5 U2 27 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2015 VL 578 AR A111 DI 10.1051/0004-6361/201425518 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM2IF UT WOS:000357502600123 ER PT J AU Hoyer, D Rauch, T Werner, K Hauschildt, PH Kruk, JW AF Hoyer, D. Rauch, T. Werner, K. Hauschildt, P. H. Kruk, J. W. TI Search with UVES and X-Shooter for signatures of the low-mass secondary in the post common-envelope binary AA Doradus SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: abundances; binaries: eclipsing; stars: low-mass; stars: individual: AA Dor; virtual observatory tools ID WHITE-DWARFS G191-B2B; BALMER LINE PROBLEM; HOT SUBDWARF STARS; SDOB PRIMARY; STELLAR LABORATORIES; OSCILLATOR-STRENGTHS; BROWN DWARF; LB 3459; ELEMENTAL COMPOSITION; RE 0503-289 AB Context. AA Dor is a close, totally eclipsing, post common-envelope binary with an sdOB-type primary star and an extremely low-mass secondary star, located close to the mass limit of stable central hydrogen burning. Within error limits, it may either be a brown dwarf or a late M-type dwarf. Aims. We aim to extract the secondary's contribution to the phase-dependent composite spectra. The spectrum and identified lines of the secondary decide on its nature. Methods. In January 2014, we measured the phase-dependent spectrum of AA Dor with X-Shooter over one complete orbital period. Since the secondary's rotation is presumable synchronized with the orbital period, its surface strictly divides into a day and night side. Therefore, we may obtain the spectrum of its cool side during its transit and of its hot, irradiated side close to its occultation. We developed the Virtual Observatory (VO) tool TLISA to search for weak lines of a faint companion in a binary system. We successfully applied it to the observations of AA Dor. Results. We identified 53 spectral lines of the secondary in the ultraviolet-blue, visual, and near-infrared X-Shooter spectra that are strongest close to its occultation. We identified 57 (20 additional) lines in available Ultraviolet and Visual Echelle Spectrograph (UVES) spectra from 2001. The lines are mostly from CII-III and OII, typical for a low-mass star that is irradiated and heated by the primary. We verified the orbital period of P = 22 597.033201 +/- 0.00007 s and determined the orbital velocity K-sec = 232.9(-6.5)(+16.6) km s(-1) of the secondary. The mass of the secondary is M-sec = 0.081(-0.010)(+0.018) M-circle dot and, hence, it is not possible to reliably determine a brown dwarf or an M-type dwarf nature. Conclusions. Although we identified many emission lines of the secondary's irradiated surface, the resolution and signal-to-noise ratio of our UVES and X-Shooter spectra are not good enough to extract a good spectrum of the secondary's nonirradiated hemisphere. C1 [Hoyer, D.; Rauch, T.; Werner, K.] Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, D-72076 Tubingen, Germany. [Hauschildt, P. H.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Kruk, J. W.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hoyer, D (reprint author), Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, Sand 1, D-72076 Tubingen, Germany. EM rauch@astro.uni-tuebingen.de FU German Aerospace Center (DLR) [50 OR 1501, 05 OR 1402]; Federal Ministry of Education and Research (BMBF) [05 AC 6VTB, 05 AC 11VTB]; ESO Service [066.D-1800, 092.C-0692]; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G] FX D.H. and T.R. are supported by the German Aerospace Center (DLR, grants 50 OR 1501 and 05 OR 1402, respectively). The GAVO project at Tubingen was supported by the Federal Ministry of Education and Research (BMBF, grants 05 AC 6VTB, 05 AC 11VTB). The TLISA tool (http://astro.uni-tuebingen.de/similar to TLISA) used for this paper was constructed as part of the activities of the German Astrophysical Virtual Observatory. The UVES and X-Shooter spectra used in this analysis were obtained as parts of ESO Service Mode runs, programs 066.D-1800 and 092.C-0692, respectively. We thank David Kilkenny for his help in determining the exact time of the secondary's occultation during our X-Shooter observations, Roger Wesson who had performed these observations and successfully covered this critical time, and Travis Barman who put the irradiated spectrum of the secondary at our disposal. 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 NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. This research has made use of NASA's Astrophysics Data System and the SIMBAD database, operated at CDS, Strasbourg, France. NR 62 TC 2 Z9 2 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2015 VL 578 AR A125 DI 10.1051/0004-6361/201526229 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM2IF UT WOS:000357502600137 ER PT J AU Kennedy, MB Milligan, RO Allred, JC Mathioudakis, M Keenan, FP AF Kennedy, Michael B. Milligan, Ryan O. Allred, Joel C. Mathioudakis, Mihalis Keenan, Francis P. TI Radiative hydrodynamic modelling and observations of the X-class solar flare on 2011 March 9 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: atmosphere; Sun: chromosphere; Sun: flares; Sun: X-rays, gamma rays ID WHITE-LIGHT FLARES; NONTHERMAL ELECTRONS; IMPULSIVE PHASE; ULTRAVIOLET OBSERVATIONS; SPECTROSCOPIC-IMAGER; CHROMOSPHERIC FLARES; EMISSION MEASURES; ATOMIC DATABASE; SOURCE SIZES; RAY AB Aims. We investigated the response of the solar atmosphere to non-thermal electron beam heating using the radiative transfer and hydrodynamics modelling code RADYN. The temporal evolution of the parameters that describe the non-thermal electron energy distribution were derived from hard X-ray observations of a particular flare, and we compared the modelled and observed parameters. Methods. The evolution of the non-thermal electron beam parameters during the X1.5 solar flare on 2011 March 9 were obtained from analysis of RHESSI X-ray spectra. The RADYN flare model was allowed to evolve for 110 s, after which the electron beam heating was ended, and was then allowed to continue evolving for a further 300 s. The modelled flare parameters were compared to the observed parameters determined from extreme-ultraviolet spectroscopy. Results. The model produced a hotter and denser flare loop than that observed and also cooled more rapidly, suggesting that additional energy input in the decay phase of the flare is required. In the explosive evaporation phase a region of high-density cool material propagated upward through the corona. This material underwent a rapid increase in temperature as it was unable to radiate away all of the energy deposited across it by the non-thermal electron beam and via thermal conduction. A narrow and high-density (n(e) <= 10(15) cm(-3)) region at the base of the flare transition region was the source of optical line emission in the model atmosphere. The collision-stopping depth of electrons was calculated throughout the evolution of the flare, and it was found that the compression of the lower atmosphere may permit electrons to penetrate farther into a flaring atmosphere compared to a quiet Sun atmosphere. C1 [Kennedy, Michael B.; Milligan, Ryan O.; Mathioudakis, Mihalis; Keenan, Francis P.] Queens Univ Belfast, Astrophys Res Ctr, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. [Milligan, Ryan O.; Allred, Joel C.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Milligan, Ryan O.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Kennedy, MB (reprint author), Queens Univ Belfast, Astrophys Res Ctr, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. EM mkennedy29@qub.ac.uk FU Northern Ireland Department of Employment and Learning; International Space Science Institute; Leverhulme Trust [F/00203/X]; NASA [NNX11AQ53G, NNX14AE07G]; UK STFC; European Community [606862] FX M.B.K. thanks the Northern Ireland Department of Employment and Learning for the award of a Ph.D. studentship and acknowledges support from the International Space Science Institute to attend a team meeting led by L. Fletcher on "Observations and Modelling of Flare Chromospheres", where helpful discussions regarding the manuscript took place. R.O.M. is grateful to the Leverhulme Trust for financial support from grant F/00203/X, and to NASA for LWS/TR&T grant NNX11AQ53G and LWS/SDO Data Analysis grant NNX14AE07G. M.M. and F.P.K. acknowledge financial support from the UK STFC. The research leading to these results has received funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 606862 (F-CHROMA). CHIANTI is a collaborative project involving George Mason University, the University of Michigan (USA) and the University of Cambridge (UK). Data are provided courtesy of NASA/SDO and RHESSI, and the EVE, HMI, and RHESSI science teams. This research has made use of NASA's Astrophysics Data System. We thank the anonymous referee for their comments that helped to improve the quality and clarity of the manuscript. NR 54 TC 8 Z9 8 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2015 VL 578 AR A72 DI 10.1051/0004-6361/201425144 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM2IF UT WOS:000357502600084 ER PT J AU Maneva, YG Ofman, L Vinas, A AF Maneva, Y. G. Ofman, L. Vinas, A. TI Relative drifts and temperature anisotropies of protons and alpha particles in the expanding solar wind: 2.5D hybrid simulations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE solar wind; plasmas; turbulence; waves; instabilities; acceleration of particles ID ALFVEN-CYCLOTRON WAVES; DIFFERENTIAL FLOW; ALFVEN/CYCLOTRON FLUCTUATIONS; VELOCITY DISTRIBUTIONS; ULYSSES OBSERVATIONS; INSTABILITY-DRIVEN; HE++ IONS; PLASMA; CORONA; ACCELERATION AB Context. We perform 2.5D hybrid simulations to investigate the origin and evolution of relative drift speeds between protons and a particles in the collisionless turbulent low-(beta) over tilde $ solar wind plasma. Aims. We study the generation of differential streaming by wave-particle interactions and absorption of turbulent wave spectra. Next we focus on the role of the relative drifts for the turbulent heating and acceleration of ions in the collisionless fast solar wind streams. Methods. The energy source is given by an initial broad-band spectrum of parallel propagating Alfven-cyclotron waves, which coexists with the plasma and is self-consistently coupled to the perpendicular ion bulk velocities. We include the effect of a gradual solar wind expansion, which cools and decelerates the minor ions. We here consider for the first time the combined effect of self-consistently initialized dispersive turbulent Alfvenic spectra with differentially streaming protons and alpha particles in the expanding solar wind outflows within a 2.5D hybrid simulation study. Results. For differential streaming of V-ap < 0.5V(A), the selected initial wave spectrum accelerates the minor ions in the non-expanding wind. At V-ap = 0.5V(A) the relative drift speed remains nearly steady. For ions that stream below this threshold value, the waves act to increase the magnitude of the relative drift speed. Ions that stream faster than the threshold value become subject to a nonlinear streaming instability, and as the system evolves, their bulk velocities decrease. We find that the solar wind expansion strongly affects the relative drift speed and significantly slows down both ion species for all values of the relative drift speeds considered in this study. The initial nonresonant wave spectra interact with the particles, resulting in preferential and anisotropic heating for the minor ions with a prominent increase of their perpendicular temperature, which overcomes the effect of the double-adiabatic cooling that is due to the solar wind expansion. Finally, the initial parallel spectra undergo a micro-turbulent nonlinear cascade during which oblique waves are generated, whose intensity depends on the value of the relative drift speed. C1 [Maneva, Y. G.] Katholieke Univ Leuven, Ctr Math Plasma Astrophys, B-3001 Leuven, Belgium. [Maneva, Y. G.; Ofman, L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Ofman, L.; Vinas, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Maneva, YG (reprint author), Katholieke Univ Leuven, Ctr Math Plasma Astrophys, B-3001 Leuven, Belgium. EM yana.maneva@wis.kuleuven.be FU NASA [NNX10AC56G]; F+ fellowship at KU Leuven under SOLSPANET [269299]; ESA Prodex [C 90347]; Wind/SWE project FX This work was supported by NASA, grant NNX10AC56G. Y. G. Maneva would like to acknowledge the F+ fellowship at KU Leuven, (FP7/2007-2013) under the grant agreement SOLSPANET (project 269299) and C 90347 (ESA Prodex) for partial support. A. F. Vinas would like to acknowledge the Wind/SWE project for partial support. Fruitful discussions with P. Hunana are highly appreciated. NR 52 TC 7 Z9 7 U1 2 U2 8 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2015 VL 578 AR A85 DI 10.1051/0004-6361/201424401 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM2IF UT WOS:000357502600097 ER PT J AU Melin, JB Bartlett, JG AF Melin, Jean-Baptiste Bartlett, James G. TI Measuring cluster masses with CMB lensing: a statistical approach SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE large-scale structure of Universe; galaxies: clusters: general; cosmic background radiation; methods: data analysis; gravitational lensing: weak; methods: statistical ID GALAXY CLUSTERS; X-RAY; COSMOLOGICAL CONSTRAINTS; SCALING RELATIONS; SAMPLE; CALIBRATION; PARAMETERS; EVOLUTION; RICHNESS; VELOCITY AB We present a method for measuring the masses of galaxy clusters using the imprint of their gravitational lensing signal on the cosmic microwave background (CMB) temperature anisotropies. The method first reconstructs the projected gravitational potential with a quadratic estimator and then applies a matched filter to extract cluster mass. The approach is well-suited for statistical analyses that bin clusters according to other mass proxies. We find that current experiments, such as Planck, the South Pole Telescope and the Atacama Cosmology Telescope, can practically implement such a statistical methodology, and that future experiments will reach sensitivities sufficient for individual measurements of massive systems. As illustration, we use simulations of Planck observations to demonstrate that it is possible to constrain the mass scale of a set of 62 massive clusters with prior information from X-ray observations, similar to the published Planck ESZ-XMM sample. We examine the effect of the thermal (tSZ) and kinetic (kSZ) Sunyaev-Zeldovich (SZ) signals, finding that the impact of the kSZ remains small in this context. The stronger tSZ signal, however, must be actively removed from the CMB maps by component separation techniques prior to reconstruction of the gravitational potential. Our study of two such methods highlights the importance of broad frequency coverage for this purpose. A companion paper presents application to the Planck data on the ESZ-XMM sample. C1 [Melin, Jean-Baptiste] CEA Saclay, DSM, Irfu, SPP, F-91191 Gif Sur Yvette, France. [Bartlett, James G.] Univ Paris Diderot, Sorbonne Paris Cite, AstroParticule & Cosmol, APC,CNRS,IN2P3,CEA,lrfu, F-75205 Paris 13, France. [Bartlett, James G.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Melin, JB (reprint author), CEA Saclay, DSM, Irfu, SPP, F-91191 Gif Sur Yvette, France. EM jean-baptiste.melin@cea.fr FU National Aeronautics and Space Administration FX The authors would like to thank the anonymous referee for useful comments which helped to clarify some important aspects of this work. A portion 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 59 TC 9 Z9 9 U1 1 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2015 VL 578 AR A21 DI 10.1051/0004-6361/201424720 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM2IF UT WOS:000357502600033 ER PT J AU Ryan, EL Mizuno, DR Shenoy, SS Woodward, CE Carey, SJ Noriega-Crespo, A Kraemer, KE Price, SD AF Ryan, E. L. Mizuno, D. R. Shenoy, S. S. Woodward, C. E. Carey, S. J. Noriega-Crespo, A. Kraemer, K. E. Price, S. D. TI The kilometer-sized Main Belt asteroid population revealed by Spitzer SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE minor planets,asteroids: general; infrared: general ID NEAR-EARTH ASTEROIDS; DIGITAL SKY SURVEY; MULTIBAND IMAGING PHOTOMETER; INFRARED-SURVEY-EXPLORER; INNER GALACTIC PLANE; THERMAL INERTIA; ION IRRADIATION; OBJECTS; MAGNITUDE; DIAMETERS AB Aims. Multi-epoch Spitzer Space Telescope 24 mu m data is utilized from the MIPSGAL and Taurus Legacy surveys to detect asteroids based on their relative motion. Methods. Infrared detections are matched to known asteroids and average diameters and albedos are derived using the near Earth asteroid thermal model (NEATM) for 1865 asteroids ranging in size from 0.2 to 169 km. A small subsample of these objects was also detected by IRAS or MSX and the single wavelength albedo and diameter fits derived from these data are within the uncertainties of the IRAS and/or MSX derived albedos and diameters and available occultation diameters, which demonstrates the robustness of our technique. Results. The mean geometric albedo of the small Main Belt asteroids in this sample is p(V) = 0.134 with a sample standard deviation of 0.106. The albedo distribution of this sample is far more diverse than the IRAS or MSX samples. The cumulative size-frequency distribution of asteroids in the Main Belt at small diameters is directly derived and a 3 sigma deviation from the fitted size-frequency distribution slope is found near 8 km. Completeness limits of the optical and infrared surveys are discussed. C1 [Ryan, E. L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Ryan, E. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mizuno, D. R.] Boston Coll, Inst Sci Res, Chestnut Hill, MA USA. [Shenoy, S. S.] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Woodward, C. E.] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. [Carey, S. J.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Noriega-Crespo, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kraemer, K. E.; Price, S. D.] Boston Coll, Inst Sci Res, Newton, MA 02459 USA. RP Ryan, EL (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM erin.l.ryan@nasa.gov OI Kraemer, Kathleen/0000-0002-2626-7155 FU National Science Foundation [AST-0706980]; NASA; JPL/Caltech FX E.L.R. and C.E.W. acknowledge support from National Science Foundation grant AST-0706980 to conduct this research. This research was supported by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. This work is based, in part, on archival data obtained with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by an award issued by JPL/Caltech. We thank an anonymous referee for helpful comments which greatly improved this paper. NR 59 TC 2 Z9 2 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2015 VL 578 AR A42 DI 10.1051/0004-6361/201321375 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM2IF UT WOS:000357502600054 ER PT J AU Sandell, G Mookerjea, B Gusten, R Requena-Torres, MA Riquelme, D Okada, Y AF Sandell, G. Mookerjea, B. Guesten, R. Requena-Torres, M. A. Riquelme, D. Okada, Y. TI High spectral and spatial resolution observations of the PDR emission in the NGC 2023 reflection nebula with SOFIA and APEX SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: clouds; submillimeter: ISM; ISM: lines and bands; ISM: individual objects: NGC 2023; ISM: molecules; photon-dominated region (PDR) ID MOLECULAR-HYDROGEN EMISSION; CLUMPY PHOTODISSOCIATION REGIONS; STAR-FORMING REGIONS; MU-M EMISSION; C-II; VIBRATIONAL FLUORESCENCE; PHYSICAL CONDITIONS; H-2; NGC-2023; HERSCHEL AB We have mapped the NGC 2023 reflection nebula in [CII] and CO(11-10) with the heterodyne receiver GREAT on SOFIA and obtained slightly smaller maps in (CO)-C-13(3-2), CO(3-2), CO(4-3), CO(6-5), and CO(7-6) with APEX in Chile. We use these data to probe the morphology, kinematics, and physical conditions of the C II region, which is ionized by FUV radiation from the B2 star HD37903. The [CII] emission traces an ellipsoidal shell-like region at a position angle of similar to-50 degrees, and is surrounded by a hot molecular shell. In the southeast, where the C II region expands into a dense, clumpy molecular cloud ridge, we see narrow and strong line emission from high-J CO lines, which comes from a thin, hot molecular shell surrounding the [C II] emission. The [CII] lines are broader and show photo evaporating gas flowing into the C II region. Based on the strength of the [(CII)-C-13] F = 2-1 line, the [CII] line appears to be somewhat optically thick over most of the nebula with an optical depth of a few. We model the physical conditions of the surrounding molecular cloud and the PDR emission using both RADEX and simple PDR models. The temperature of the CO emitting PDR shell is similar to 90-120 K, with densities of 10(5)-10(6) cm(-3), as deduced from RADEX modeling. Our PDR modeling indicates that the PDR layer where [C II] emission dominates has somewhat lower densities, 10(4) to a few times 10(5) cm(-3). C1 [Sandell, G.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. [Mookerjea, B.] Tata Inst Fundamental Res, Mumbai 400005, Maharashtra, India. [Guesten, R.; Requena-Torres, M. A.; Riquelme, D.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Okada, Y.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. RP Sandell, G (reprint author), NASA, Ames Res Ctr, SOFIA USRA, MS 232-12,Bldg N232,Rm 146,POB 1, Moffett Field, CA 94035 USA. EM Goran.H.Sandell@nasa.gov; bhaswati@tifr.res.in FU NASA [NAS2-97001]; Deutsches SOFIA Institut (DSI) under DLR [50 OK 0901] FX The NASA/DLR Stratospheric Observatory for Infrared Astronomy (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. NR 48 TC 0 Z9 0 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2015 VL 578 AR A41 DI 10.1051/0004-6361/201525881 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM2IF UT WOS:000357502600053 ER PT J AU Velusamy, T Langer, WD Goldsmith, PF Pineda, JL AF Velusamy, T. Langer, W. D. Goldsmith, P. F. Pineda, J. L. TI Internal structure of spiral arms traced with [C II]: Unraveling the warm ionized medium, H I, and molecular emission lanes SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: structure; Galaxy: structure; Galaxy: general; submillimeter: ISM; ISM: general ID GALACTIC PLANE SURVEY; MILKY-WAY GALAXY; INTERSTELLAR-MEDIUM; CLOUDS; GAS; LINES; GHZ AB Context. The spiral arm tangencies are ideal lines of sight in which to determine the distribution of interstellar gas components in the spiral arms and study the influence of spiral density waves on the interarm gas in the Milky Way. [CII] emission in the tangencies delineates the warm ionized component and the photon-dominated regions and is thus an important probe of spiral arm structure and dynamics. Aims. We aim to use [C II], Hi, and (CO)-C-12 spectral line maps of the Crux, Norma, and Perseus tangencies to analyze the internal structure of the spiral arms in different gas layers. Methods. We used [C II] l-V maps along with those for HI and (CO)-C-12 to derive the average spectral line intensity profiles over the longitudinal range of each tangency. Using the V-LSR of the emission features, we located the [CII], HI, and (CO)-C-12 emissions along a cross cut of the spiral arm. We used the [CII] velocity profile to identify the compressed warm ionized medium (WIM) in the spiral arm. Results. We present a large-scale (similar to 15 degrees) position-velocity map of the Galactic plane in [CII] from l = 326.degrees 6 to 341.degrees 4 observed with Herschel HIFI. In the spectral line profiles at the tangencies, [C II] has two emission peaks, one associated with the compressed WIM and the other the molecular gas photon-dominated regions. When represented as a cut across the inner to outer edge of the spiral arm, the [C II]-WIM peak appears closest to the inner edge while (CO)-C-12 and [C II] associated with molecular gas are at the outermost edge. Hi has broader emission with an intermediate peak located nearer to that of (CO)-C-12. Conclusions. The velocity-resolved spectral line data of the spiral arm tangencies unravel the internal structure in the arms locating the emission lanes within them. We interpret the excess [Cii] near the tangent velocities as shock compression of the WIM induced by the spiral density waves and as the innermost edge of spiral arms. For the Norma and Perseus arms, we estimate widths of similar to 250 pc in [C II]-WIM and similar to 400 pc in (CO)-C-12 and overall spiral arm widths of similar to 500 pc in [CII] and (CO)-C-12 emissions; in HI the widths are similar to 400 pc and similar to 620 pc for Perseus and Norma, respectively. The electron densities in the WIM are similar to 0.5 cm(-3), about an order of magnitude higher than the average for the disk. The enhanced electron density in the WIM is a result of compression of the WIM by the spiral density wave potential. C1 [Velusamy, T.; Langer, W. D.; Goldsmith, P. F.; Pineda, J. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Velusamy, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Thangasamy.Velusamy@jpl.nasa.gov RI Goldsmith, Paul/H-3159-2016 FU National Aeronautics and Space Administration FX We thank the staffs of the ESA Herschel Science Centre and NASA Herschel Science Center, and the HIFI, Instrument Control Centre (ICC) for their help with the data reduction routines. In addition, we owe special thanks to David Teyssier for clarifications regarding the hebCorrection tool. This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 38 TC 2 Z9 2 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2015 VL 578 AR A135 DI 10.1051/0004-6361/201525902 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM2IF UT WOS:000357502600147 ER PT J AU Roman, MO Stokes, EC AF Roman, Miguel O. Stokes, Eleanor C. TI Holidays in lights: Tracking cultural patterns in demand for energy services SO EARTHS FUTURE LA English DT Article DE Energy Use; Climate Change Mitigation; Human Dimensions; Remote Sensing ID DAY/NIGHT BAND; LOW-CARBON; CONSUMPTION; ELECTRICITY; VEGETATION; IMAGERY; URBANIZATION; POPULATION; SATURATION; ALGORITHM AB Successful climate change mitigation will involve not only technological innovation, but also innovation in how we understand the societal and individual behaviors that shape the demand for energy services. Traditionally, individual energy behaviors have been described as a function of utility optimization and behavioral economics, with price restructuring as the dominant policy lever. Previous research at the macro-level has identified economic activity, power generation and technology, and economic role as significant factors that shape energy use. However, most demand models lack basic contextual information on how dominant social phenomenon, the changing demographics of cities, and the sociocultural setting within which people operate, affect energy decisions and use patterns. Here we use high-quality Suomi-NPP VIIRS nighttime environmental products to: (1) observe aggregate human behavior through variations in energy service demand patterns during the Christmas and New Year's season and the Holy Month of Ramadan and (2) demonstrate that patterns in energy behaviors closely track sociocultural boundaries at the country, city, and district level. These findings indicate that energy decision making and demand is a sociocultural process as well as an economic process, often involving a combination of individual price-based incentives and societal-level factors. While nighttime satellite imagery has been used to map regional energy infrastructure distribution, tracking daily dynamic lighting demand at three major scales of urbanization is novel. This methodology can enrich research on the relative importance of drivers of energy demand and conservation behaviors at fine scales. Our initial results demonstrate the importance of seating energy demand frameworks in a social context. C1 [Roman, Miguel O.] NASA, Goddard Space Flight Ctr, Terr Informat Syst Lab, Greenbelt, MD 20771 USA. [Stokes, Eleanor C.] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. RP Roman, MO (reprint author), NASA, Goddard Space Flight Ctr, Terr Informat Syst Lab, Greenbelt, MD 20771 USA. EM miguel.o.roman@nasa.gov; eleanor.stokes@yale.edu FU NASA's Office of the Chief Scientist under the Science Innovation Fund (SIF); NASA's Minority University Research and Education Program [NASA-NNX13AR88H] FX The authors would like to thank Peter Ma and Jesse Allen (NASA/GSFC/SSAI) for their support on the figures; to Virginia Kalb (NASA/GSFC) and Zhuosen Wang (NASA/GSFC/ORAU) for their advice on the Suomi-NPP VIIRS Day/Night Band algorithms; and to Adi Grief, Qingling Zhang, and Karen Seto (YALE/FES) for much useful discussions. The authors gratefully acknowledge support provided by NASA's Office of the Chief Scientist under the Science Innovation Fund (SIF); as well as NASA's Minority University Research and Education Program under grant NASA-NNX13AR88H. NR 62 TC 4 Z9 4 U1 2 U2 21 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2328-4277 J9 EARTHS FUTURE JI Earth Future PD JUN PY 2015 VL 3 IS 6 BP 182 EP 205 DI 10.1002/2014EF000285 PG 24 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA CN0YU UT WOS:000358142500002 PM 27819010 ER PT J AU Hui, HJ Peslier, AH Rudnick, RL Simonetti, A Neal, CR AF Hui, Hejiu Peslier, Anne H. Rudnick, Roberta L. Simonetti, Antonio Neal, Clive R. TI Plume-cratonic lithosphere interaction recorded by water and other trace elements in peridotite xenoliths from the Labait volcano, Tanzania SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS LA English DT Article DE Tanzanian craton; nominally anhydrous mineral; Fourier transform infrared spectroscopy; laser-ablation inductively coupled plasma mass spectrometry; water; craton; mantle plume ID EAST-AFRICAN RIFT; NOMINALLY ANHYDROUS MINERALS; DISLOCATION CREEP REGIME; UPPER-MANTLE MINERALS; MAGMA ASCENT RATES; CONTINENTAL LITHOSPHERE; GREENSTONE-BELT; HYDROGEN DIFFUSION; NORTHERN TANZANIA; BASALTIC GLASSES AB Water and other trace element concentrations in olivine (1-39 ppm H2O), orthopyroxene (10-150 ppm H2O), and clinopyroxene (16-340 ppm H2O) of mantle xenoliths from the Labait volcano, located on the edge of the Tanzanian craton along the eastern branch of the East African Rift, record melting and subsequent refertilization by plume magmas in a stratified lithosphere. These water contents are at the lower end of the range observed in other cratonic mantle lithospheres. Despite correlations between water content and indices of melting in orthopyroxene from the shallow peridotites, and in both olivine and orthopyroxene from the deep peridotites, water concentrations are too high for the peridotites to be simple residues. Instead, the Labait water contents are best explained as reflecting interaction between residual peridotite with a melt having relatively low water content (<1 wt.% H2O). Plume-derived melts are the likely source of water and other trace element enrichments in the Labait peridotites. Only garnet may have undergone addition of water from the host magma as evidenced by water content increasing toward the kelyphite rim in one otherwise homogeneous garnet. Based on modeling of the diffusion profile, magma ascent occurred at 4-28 m/s. In summary, plume-craton interaction appears to result in only moderate water enrichment of the lithosphere. C1 [Hui, Hejiu] Nanjing Univ, Sch Earth Sci & Engn, State Key Lab Mineral Deposits Res, Nanjing 210008, Jiangsu, Peoples R China. [Hui, Hejiu; Simonetti, Antonio; Neal, Clive R.] Univ Notre Dame, Dept Civil & Environm Engn & Earth Sci, Notre Dame, IN 46556 USA. [Hui, Hejiu] USRA Houston, Lunar & Planetary Inst, Houston, TX USA. [Peslier, Anne H.] NASA Johnson Space Ctr, Houston, TX USA. [Rudnick, Roberta L.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. RP Hui, HJ (reprint author), Nanjing Univ, Sch Earth Sci & Engn, State Key Lab Mineral Deposits Res, Nanjing 210008, Jiangsu, Peoples R China. EM hhui@nju.edu.cn RI Hui, Hejiu/D-2912-2011; Simonetti, Antonio/E-4187-2016 OI Hui, Hejiu/0000-0003-2733-5794; Simonetti, Antonio/0000-0002-4025-2283 FU NSF [EAR 0802652, EAR 1118335, EAR 9506510] FX This project was supported by NSF grants EAR 0802652 and EAR 1118335 to AHP and EAR 9506510 to RLR. We thank Cin-Ty Lee for invaluable discussions. We are grateful for the comments from two anonymous reviewers that greatly improved the manuscript and for efficient editing by T. Becker. Supporting data are provided in the tables and figures, including those in an SI file. NR 165 TC 5 Z9 7 U1 6 U2 29 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1525-2027 J9 GEOCHEM GEOPHY GEOSY JI Geochem. Geophys. Geosyst. PD JUN PY 2015 VL 16 IS 6 BP 1687 EP 1710 DI 10.1002/2015GC005779 PG 24 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CM9DV UT WOS:000358007800001 ER PT J AU Tian, HQ Lu, CQ Yang, J Banger, K Huntzinger, DN Schwalm, CR Michalak, AM Cook, R Ciais, P Hayes, D Huang, MY Ito, A Jain, AK Lei, HM Mao, JF Pan, SF Post, WM Peng, SS Poulter, B Ren, W Ricciuto, D Schaefer, K Shi, XY Tao, B Wang, WL Wei, YX Yang, QC Zhang, BW Zeng, N AF Tian, Hanqin Lu, Chaoqun Yang, Jia Banger, Kamaljit Huntzinger, Deborah N. Schwalm, Christopher R. Michalak, Anna M. Cook, Robert Ciais, Philippe Hayes, Daniel Huang, Maoyi Ito, Akihiko Jain, Atul K. Lei, Huimin Mao, Jiafu Pan, Shufen Post, Wilfred M. Peng, Shushi Poulter, Benjamin Ren, Wei Ricciuto, Daniel Schaefer, Kevin Shi, Xiaoying Tao, Bo Wang, Weile Wei, Yaxing Yang, Qichun Zhang, Bowen Zeng, Ning TI Global patterns and controls of soil organic carbon dynamics as simulated by multiple terrestrial biosphere models: Current status and future directions SO GLOBAL BIOGEOCHEMICAL CYCLES LA English DT Article DE soil organic carbon (SOC); heterotrophic respiration (Rh); mean residence time (MRT); soil carbon dynamics model; belowground processes; uncertainty ID PROGRAM MULTISCALE SYNTHESIS; EARTH SYSTEM MODELS; LAND-USE CHANGE; INTERCOMPARISON PROJECT; NITROGEN INTERACTIONS; AGRICULTURAL LAND; VEGETATION MODEL; CLIMATE-CHANGE; WHITE SPRUCE; TEMPERATURE AB Soil is the largest organic carbon (C) pool of terrestrial ecosystems, and C loss from soil accounts for a large proportion of land-atmosphere C exchange. Therefore, a small change in soil organic C (SOC) can affect atmospheric carbon dioxide (CO2) concentration and climate change. In the past decades, a wide variety of studies have been conducted to quantify global SOC stocks and soil C exchange with the atmosphere through site measurements, inventories, and empirical/process-based modeling. However, these estimates are highly uncertain, and identifying major driving forces controlling soil C dynamics remains a key research challenge. This study has compiled century-long (1901-2010) estimates of SOC storage and heterotrophic respiration (Rh) from 10 terrestrial biosphere models (TBMs) in the Multi-scale Synthesis and Terrestrial Model Intercomparison Project and two observation-based data sets. The 10 TBM ensemble shows that global SOC estimate ranges from 425 to 2111Pg C (1Pg=10(15)g) with a median value of 1158Pg C in 2010. The models estimate a broad range of Rh from 35 to 69PgCyr(-1) with a median value of 51PgCyr(-1) during 2001-2010. The largest uncertainty in SOC stocks exists in the 40-65 degrees N latitude whereas the largest cross-model divergence in Rh are in the tropics. The modeled SOC change during 1901-2010 ranges from -70Pg C to 86Pg C, but in some models the SOC change has a different sign from the change of total C stock, implying very different contribution of vegetation and soil pools in determining the terrestrial C budget among models. The model ensemble-estimated mean residence time of SOC shows a reduction of 3.4years over the past century, which accelerate C cycling through the land biosphere. All the models agreed that climate and land use changes decreased SOC stocks, while elevated atmospheric CO2 and nitrogen deposition over intact ecosystems increased SOC stockseven though the responses varied significantly among models. Model representations of temperature and moisture sensitivity, nutrient limitation, and land use partially explain the divergent estimates of global SOC stocks and soil C fluxes in this study. In addition, a major source of systematic error in model estimations relates to nonmodeled SOC storage in wetlands and peatlands, as well as to old C storage in deep soil layers. C1 [Tian, Hanqin; Lu, Chaoqun; Yang, Jia; Banger, Kamaljit; Pan, Shufen; Ren, Wei; Tao, Bo; Yang, Qichun; Zhang, Bowen] Auburn Univ, Int Ctr Climate & Global Change Res, Sch Forestry & Wildlife Sci, Auburn, AL 36849 USA. [Huntzinger, Deborah N.] No Arizona Univ, Sch Earth Sci & Environm Sustainabil, Flagstaff, AZ 86011 USA. [Huntzinger, Deborah N.; Schwalm, Christopher R.] No Arizona Univ, Dept Civil Engn Construct Management & Environm E, Flagstaff, AZ 86011 USA. [Schwalm, Christopher R.] No Arizona Univ, Ctr Ecosyst Sci & Soc, Flagstaff, AZ 86011 USA. [Michalak, Anna M.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA USA. [Cook, Robert; Hayes, Daniel; Mao, Jiafu; Post, Wilfred M.; Ricciuto, Daniel; Shi, Xiaoying; Wei, Yaxing] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. [Cook, Robert; Hayes, Daniel; Mao, Jiafu; Post, Wilfred M.; Ricciuto, Daniel; Shi, Xiaoying; Wei, Yaxing] Oak Ridge Natl Lab, Climate Change Sci Inst, Oak Ridge, TN 37831 USA. [Ciais, Philippe; Peng, Shushi] Lab Sci Climat & Environm, Gif Sur Yvette, France. [Huang, Maoyi] Pacific NW Natl Lab, Atmospher Sci & Global Change Div, Richland, WA 99352 USA. [Ito, Akihiko] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan. [Jain, Atul K.] Univ Illinois, Dept Atmospher Sci, Urbana, IL USA. [Lei, Huimin] Tsinghua Univ, Dept Hydraul Engn, Beijing 100084, Peoples R China. [Poulter, Benjamin] Montana State Univ, Dept Ecol, Bozeman, MT 59717 USA. [Schaefer, Kevin] Natl Snow & Ice Data Ctr, Boulder, CO USA. [Wang, Weile] NASA, Ames Res Ctr, Mountain View, CA USA. [Zeng, Ning] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. RP Tian, HQ (reprint author), Auburn Univ, Int Ctr Climate & Global Change Res, Sch Forestry & Wildlife Sci, Auburn, AL 36849 USA. EM tianhan@auburn.edu; czl0003@auburn.edu RI Lei, Huimin/H-9596-2015; Tian, Hanqin/A-6484-2012; Peng, Shushi/J-4779-2014; Ren, Wei/G-8317-2016; Ren, Wei/I-4048-2014; Banger, Kamaljit/B-3215-2016; Mao, Jiafu/B-9689-2012; Ricciuto, Daniel/I-3659-2016; Zeng, Ning/A-3130-2008; Yang, Jia/A-6483-2012; Jain, Atul/D-2851-2016 OI Cook, Robert/0000-0001-7393-7302; Poulter, Benjamin/0000-0002-9493-8600; Huang, Maoyi/0000-0001-9154-9485; Zhang, Bowen/0000-0002-8370-0509; Lei, Huimin/0000-0002-1175-2334; Tian, Hanqin/0000-0002-1806-4091; Peng, Shushi/0000-0001-5098-726X; Ren, Wei/0000-0002-4840-4835; Mao, Jiafu/0000-0002-2050-7373; Ricciuto, Daniel/0000-0002-3668-3021; Zeng, Ning/0000-0002-7489-7629; Yang, Jia/0000-0003-2019-9603; Jain, Atul/0000-0002-4051-3228 FU NASA ROSES [NNX10AG01A, NNH10AN68I]; U.S. Department of Energy (DOE), Office of Science, Biological and Environmental Research; DOE [DE-AC05-00OR22725]; U.S. DOE-BER; U.S. DOE-BER through the Subsurface Biogeochemical Research Program (SBR) as part of the SBR Scientific Focus Area (SFA) at the Pacific Northwest National Laboratory (PNNL); U.S. DOE by BATTELLE Memorial Institute [DE-AC05-76RLO1830]; NASA Interdisciplinary Science Program [NNX10AU06G, NNX11AD47G, NNX14AF93G, NNG04GM39C]; NASA Land Cover/Land Use Change Program [NNX08AL73G]; NASA Carbon Monitoring System Program [NNX14AO73G]; National Science Foundation Dynamics of Coupled Natural-Human System Program [1210360]; Decadal and Regional Climate Prediction using Earth System Models [AGS-1243220]; DOE National Institute for Climate Change Research [DUKE-UN-07-SC-NICCR-1014]; EPA STAR program [2004-STAR-L1]; U.S. National Science Foundation [NSF-AGS-12-43071, NSF-EFRI-083598]; USDA National Institute of Food and Agriculture (NIFA) [2011-68002-30220]; U.S. Department of Energy (DOE) Office of Science [DOE-DE-SC0006706]; NASA Land cover and Land Use Change Program [NNX14AD94G]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; National Science Foundation [OCI-0725070, ACI-1238993] FX Funding for the Multi-scale Synthesis and Terrestrial Model Intercomparison Project (MsTMIP; http://nacp.ornl.gov/MsTMIP.shtml) was provided through NASA ROSES grant NNX10AG01A. Data management support for preparing, documenting, and distributing model driver and output data were performed by the Modeling and Synthesis Thematic Data Center at Oak Ridge National Laboratory (http://nacp.ornl.gov), with funding through NASA ROSES grant NNH10AN68I. Finalized MsTMIP data products will be archived at the ORNL DAAC (http://daac.ornl.gov). This is MsTMIP contribution 4. Acknowledgments for specific MsTMIP participating models are as follows. (1) Biome-BGC. Biome-BGC code was provided by the Numerical Terradynamic Simulation Group at University of Montana. The computational facilities were provided by NASA Earth Exchange at NASA Ames Research Center. (2) CLM and GTEC. Simulations were supported in part by the U.S. Department of Energy (DOE), Office of Science, Biological and Environmental Research. Oak Ridge National Laboratory is managed by UTBATTELLE for DOE under contract DE-AC05-00OR22725. (3) CLM4-VIC. This research is supported in part by the U.S. Department of Energy (DOE), Office of Science, Biological and Environmental Research (BER) through the Earth System Modeling program and performed using the Environmental Molecular Sciences Laboratory (EMSL), a national scientific user facility sponsored by the U.S. DOE-BER and located at Pacific Northwest National Laboratory (PNNL). Participation of M. Huang in the MsTMIP synthesis is supported by the U.S. DOE-BER through the Subsurface Biogeochemical Research Program (SBR) as part of the SBR Scientific Focus Area (SFA) at the Pacific Northwest National Laboratory (PNNL). PNNL is operated for the U.S. DOE by BATTELLE Memorial Institute under contract DE-AC05-76RLO1830. (4) DLEM. The Dynamic Land Ecosystem Model (DLEM) developed in International Center for Climate and Global Change Research at Auburn University has been supported by NASA Interdisciplinary Science Program (NNX10AU06G, NNX11AD47G, NNX14AF93G, and NNG04GM39C), NASA Land Cover/Land Use Change Program (NNX08AL73G), NASA Carbon Monitoring System Program (NNX14AO73G), National Science Foundation Dynamics of Coupled Natural-Human System Program(1210360), Decadal and Regional Climate Prediction using Earth System Models (AGS-1243220), DOE National Institute for Climate Change Research (DUKE-UN-07-SC-NICCR-1014), and EPA STAR program (2004-STAR-L1). (5) ISAM. The simulations were supported by the U.S. National Science Foundation (NSF-AGS-12-43071 and NSF-EFRI-083598), the USDA National Institute of Food and Agriculture (NIFA) (2011-68002-30220), the U.S. Department of Energy (DOE) Office of Science (DOE-DE-SC0006706), and the NASA Land cover and Land Use Change Program (NNX14AD94G). ISAM simulations were carried out at the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the U.S. Department of Energy under contract DE-AC02-05CH11231, and at the Blue Waters sustained-petascale computing, University of Illinois at Urbana-Champaign, which is supported by the National Science Foundation (awards OCI-0725070 and ACI-1238993) and the state of Illinois. (6) LPJ-wsl. This work was conducted at LSCE, France, using a modified version of the LPJ version 3.1 model, originally made available by the Potsdam Institute for Climate Impact Research. (7) ORCHIDEE-LSCE. ORCHIDEE is developed at the IPSL institute in France.; The simulations were performed with the support of the GHG-Europe FP7 grant with computing facilities provided by LSCE (Laboratoire des Sciences du Climat et de l'Environnement) or TGCC (Tres Grand Centre de Calcul). (8) VISIT. VISIT was developed at the National Institute for Environmental Studies, Japan. This work was mostly conducted during a visiting stay at Oak Ridge National Laboratory. NR 66 TC 17 Z9 17 U1 18 U2 107 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 JUN PY 2015 VL 29 IS 6 BP 775 EP 792 DI 10.1002/2014GB005021 PG 18 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA CM8NE UT WOS:000357957600004 ER PT J AU Wierzchos, K Cancilla, JC Torrecilla, JS Diaz-Rodriguez, P Davila, AF Ascaso, C Nienow, J McKay, CP Wierzchos, J AF Wierzchos, K. Cancilla, J. C. Torrecilla, J. S. Diaz-Rodriguez, P. Davila, A. F. Ascaso, C. Nienow, J. McKay, C. P. Wierzchos, J. TI Application of artificial neural networks as a tool for moisture prediction in microbially colonized halite in the Atacama Desert SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article DE Atacama Desert; halite; microbial endolithic communities; artificial neural network ID IONIC LIQUIDS; HYPERARID CORE; WATER-CONTENT; WASTE; LIFE AB The Atacama Desert is the driest and one of the most life-limiting places on Earth. Despite the extreme conditions, microbial endolithic communities have been found inside halite rocks. The presence of these microbial communities is possible due to the hygroscopic properties of evaporitic rocks composed of sodium chloride. It is important to elucidate every possible water source in such a hyperarid environment. Therefore, in the present study, an artificial neural network (ANN) based model has been designed to predict the presence of liquid water on the surface of halite pinnacles. The model predicts the moisture formation using two basic meteorological variables, air temperature, and air relative humidity. ANNs have been successfully employed for the first time as a tool for predicting the appearance of liquid water, a key factor for the endolithic microbial communities living in the driest part of the Atacama Desert. The model developed is able to correctly predict the formation of water on the surface of the halite pinnacles 83% of the cases. We anticipate the future application of this model as an important tool for the prediction of the water availability and therefore potential habitability of lithic substrates in extreme environments on Earth and perhaps elsewhere. C1 [Wierzchos, K.; Cancilla, J. C.; Torrecilla, J. S.; Diaz-Rodriguez, P.] Univ Complutense Madrid, Dept Chem Engn, Madrid, Spain. [Davila, A. F.] SETI Inst, Mountain View, CA USA. [Ascaso, C.; Wierzchos, J.] Museo Nacl Ciencias Nat CSIC, Madrid, Spain. [Nienow, J.] Valdosta State Univ, Dept Biol, Valdosta, GA USA. [McKay, C. P.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. RP Wierzchos, K (reprint author), Univ Complutense Madrid, Dept Chem Engn, Madrid, Spain. EM kacperwierzchos@gmail.com RI Torrecilla, Jose/L-6525-2014 OI Torrecilla, Jose/0000-0003-1209-203X FU MINECO (Spain) [CGL2013-42509P]; European Union [HEALTH-F4-2011-258868]; NASA [NNX12AD61G] FX This work was supported by MINECO (Spain) grant CGL2013-42509P, the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement HEALTH-F4-2011-258868, and by grant NNX12AD61G from NASA Exobiology program. All the data used for this work can be obtained via email from the corresponding author at kacperwierzchos@gmail.com. NR 30 TC 0 Z9 0 U1 3 U2 14 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 JUN PY 2015 VL 120 IS 6 BP 1018 EP 1026 DI 10.1002/2014JG002837 PG 9 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA CM8LM UT WOS:000357952400003 ER PT J AU MacGregor, JA Li, JL Paden, JD Catania, GA Clow, GD Fahnestock, MA Gogineni, SP Grimm, RE Morlighem, M Nandi, S Seroussi, H Stillman, DE AF MacGregor, Joseph A. Li, Jilu Paden, John D. Catania, Ginny A. Clow, Gary D. Fahnestock, Mark A. Gogineni, S. Prasad Grimm, Robert E. Morlighem, Mathieu Nandi, Soumyaroop Seroussi, Helene Stillman, David E. TI Radar attenuation and temperature within the Greenland Ice Sheet SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE LA English DT Article ID GEOTHERMAL HEAT-FLUX; ECHO SOUNDING DATA; ANTARCTIC ICE; WEST ANTARCTICA; PENETRATING RADAR; EAST ANTARCTICA; BASAL MELT; RADIOFREQUENCY ATTENUATION; ELECTRICAL-CONDUCTIVITY; NORTHEAST GREENLAND AB The flow of ice is temperature-dependent, but direct measurements of englacial temperature are sparse. The dielectric attenuation of radio waves through ice is also temperature-dependent, and radar sounding of ice sheets is sensitive to this attenuation. Here we estimate depth-averaged radar-attenuation rates within the Greenland Ice Sheet from airborne radar-sounding data and its associated radiostratigraphy. Using existing empirical relationships between temperature, chemistry, and radar attenuation, we then infer the depth-averaged englacial temperature. The dated radiostratigraphy permits a correction for the confounding effect of spatially varying ice chemistry. Where radar transects intersect boreholes, radar-inferred temperature is consistently higher than that measured directly. We attribute this discrepancy to the poorly recognized frequency dependence of the radar-attenuation rate and correct for this effect empirically, resulting in a robust relationship between radar-inferred and borehole-measured depth-averaged temperature. Radar-inferred englacial temperature is often lower than modern surface temperature and that of a steady state ice-sheet model, particularly in southern Greenland. This pattern suggests that past changes in surface boundary conditions (temperature and accumulation rate) affect the ice sheet's present temperature structure over a much larger area than previously recognized. This radar-inferred temperature structure provides a new constraint for thermomechanical models of the Greenland Ice Sheet. C1 [MacGregor, Joseph A.; Catania, Ginny A.] Univ Texas Austin, Inst Geophys, Austin, TX 78712 USA. [Li, Jilu; Paden, John D.; Gogineni, S. Prasad; Nandi, Soumyaroop] Univ Kansas, Ctr Remote Sensing Ice Sheets, Lawrence, KS 66045 USA. [Catania, Ginny A.] Univ Texas Austin, Dept Geol Sci, Austin, TX USA. [Clow, Gary D.] US Geol Survey, Lakewood, CO 80225 USA. [Clow, Gary D.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. [Fahnestock, Mark A.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. [Grimm, Robert E.; Stillman, David E.] Southwest Res Inst, Dept Space Studies, Boulder, CO USA. [Morlighem, Mathieu] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. [Seroussi, Helene] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP MacGregor, JA (reprint author), Univ Texas Austin, Inst Geophys, Austin, TX 78712 USA. EM joemac@ig.utexas.edu RI Catania, Ginny/B-9787-2008; Morlighem, Mathieu/O-9942-2014; OI Morlighem, Mathieu/0000-0001-5219-1310; Grimm, Robert/0000-0002-7588-1194 FU NSF [ARC 1107753, 1108058, ANT 0424589]; NASA [NNX12AB71G] FX NSF (ARC 1107753 and 1108058; ANT 0424589) and NASA (NNX12AB71G) supported this work. We thank the organizations (Program for Arctic Regional Climate Assessment, Center for Remote Sensing of Ice Sheets, and Operation IceBridge) and innumerable individuals that both supported and performed the collection and processing of the radar data used in this study. We thank S. Anandakrishnan, K. Matsuoka, and D.P. Winebrenner for the inspiration for this work; the Centre for Ice and Climate for the DEP data; and L.C. Andrews, K. A. Christianson, C. Grima, J.C. Hiester, N. Holschuh, K. Thirumalai, and D. A. Young for valuable discussions. We thank Associate Editor J.N. Bassis, D.M. Schroeder, and an anonymous referee for valuable comments that improved this manuscript. Echo-intensity data will be archived at the National Snow and Ice Data Center (NSIDC; http://www.nsidc.org). NR 90 TC 13 Z9 13 U1 2 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9003 EI 2169-9011 J9 J GEOPHYS RES-EARTH JI J. Geophys. Res.-Earth Surf. PD JUN PY 2015 VL 120 IS 6 BP 983 EP 1008 DI 10.1002/2014JF003418 PG 26 WC Geosciences, Multidisciplinary SC Geology GA CM8ZQ UT WOS:000357994400003 ER PT J AU Dow, CF Kulessa, B Rutt, IC Tsai, VC Pimentel, S Doyle, SH van As, D Lindback, K Pettersson, R Jones, GA Hubbard, A AF Dow, C. F. Kulessa, B. Rutt, I. C. Tsai, V. C. Pimentel, S. Doyle, S. H. van As, D. Lindback, K. Pettersson, R. Jones, G. A. Hubbard, A. TI Modeling of subglacial hydrological development following rapid supraglacial lake drainage SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE LA English DT Article DE Greenland ice sheet; subglacial hydrology; lake drainage; modeling ID GREENLAND ICE-SHEET; OUTBURST FLOODS; WEST GREENLAND; OUTLET GLACIER; SEASONAL-CHANGES; WATER STORAGE; SURFACE MELT; EVOLUTION; SYSTEM; MOTION AB The rapid drainage of supraglacial lakes injects substantial volumes of water to the bed of the Greenland ice sheet over short timescales. The effect of these water pulses on the development of basal hydrological systems is largely unknown. To address this, we develop a lake drainage model incorporating both (1) a subglacial radial flux element driven by elastic hydraulic jacking and (2) downstream drainage through a linked channelized and distributed system. Here we present the model and examine whether substantial, efficient subglacial channels can form during or following lake drainage events and their effect on the water pressure in the surrounding distributed system. We force the model with field data from a lake drainage site, 70 km from the terminus of Russell Glacier in West Greenland. The model outputs suggest that efficient subglacial channels do not readily form in the vicinity of the lake during rapid drainage and instead water is evacuated primarily by a transient turbulent sheet and the distributed system. Following lake drainage, channels grow but are not large enough to reduce the water pressure in the surrounding distributed system, unless preexisting channels are present throughout the domain. Our results have implications for the analysis of subglacial hydrological systems in regions where rapid lake drainage provides the primary mechanism for surface-to-bed connections. C1 [Dow, C. F.; Kulessa, B.; Rutt, I. C.; Jones, G. A.] Swansea Univ, Coll Sci, Glaciol Grp, Swansea, W Glam, Wales. [Dow, C. F.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Tsai, V. C.] CALTECH, Seismol Lab, Pasadena, CA 91125 USA. [Pimentel, S.] Trinity Western Univ, Fac Nat & Appl Sci, Dept Math, Langley, BC, Canada. [Doyle, S. H.; Hubbard, A.] Aberystwyth Univ, Inst Geog & Earth Sci, Aberystwyth, Dyfed, Wales. [van As, D.] Geol Survey Denmark & Greenland, Copenhagen, Denmark. [Lindback, K.; Pettersson, R.] Uppsala Univ, Dept Earth Sci, Uppsala, Sweden. RP Dow, CF (reprint author), Swansea Univ, Coll Sci, Glaciol Grp, Swansea, W Glam, Wales. EM christine.f.dow@nasa.gov RI Tsai, Victor/J-8405-2012; OI Tsai, Victor/0000-0003-1809-6672; Kulessa, Bernd/0000-0002-4830-4949; Hubbard, Alun/0000-0002-0503-3915 FU NERC [NE/G007195/1]; Greenland Analogue Project; NERC doctoral scholarship; NASA Postdoctoral Program fellowship at the Goddard Space Flight Center FX For further information on the modeling methodology see the supporting information and/or contact C.F. Dow. This project was funded with NERC grant NE/G007195/1 and the Greenland Analogue Project. C.F.D. was funded by a NERC doctoral scholarship and a NASA Postdoctoral Program fellowship at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities. The authors would like to thank Mauro Werder and Ian Hewitt for helpful discussions about the modeling approach. Three anonymous reviewers and the Associate Editor are thanked for their helpful suggestions that have improved this manuscript. NR 73 TC 7 Z9 7 U1 5 U2 19 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9003 EI 2169-9011 J9 J GEOPHYS RES-EARTH JI J. Geophys. Res.-Earth Surf. PD JUN PY 2015 VL 120 IS 6 BP 1127 EP 1147 DI 10.1002/2014JF003333 PG 21 WC Geosciences, Multidisciplinary SC Geology GA CM8ZQ UT WOS:000357994400010 PM 26640746 ER PT J AU Chemtob, SM Nickerson, RD Morris, RV Agresti, DG Catalano, JG AF Chemtob, Steven M. Nickerson, Ryan D. Morris, Richard V. Agresti, David G. Catalano, Jeffrey G. TI Synthesis and structural characterization of ferrous trioctahedral smectites: Implications for clay mineral genesis and detectability on Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE clay mineralogy; smectite; X-ray diffraction; VNIR; X-ray spectroscopy; Mars ID RESOLUTION REFLECTANCE SPECTROSCOPY; HYDROTHERMAL ALTERATION; MOSSBAUER-SPECTROSCOPY; SILICATE MINERALS; HYDROUS MINERALS; OCTAHEDRAL SHEET; OXIDATION-STATE; POLARIZED EXAFS; OXYGEN FUGACITY; IRON AB Widespread detections of phyllosilicates in Noachian terrains on Mars imply a history of near-surface fluid-rock interaction. Ferrous trioctahedral smectites are thermodynamically predicted products of basalt weathering on early Mars, but to date only Fe3+-bearing dioctahedral smectites have been identified from orbital observations. In general, the physicochemical properties of ferrous smectites are poorly studied because they are susceptible to air oxidation. In this study, eight Fe2+-bearing smectites were synthesized from Fe2+-Mg-Al silicate gels at 200 degrees C under anoxic conditions. Samples were characterized by inductively coupled plasma optical emission spectrometry, powder X-ray diffraction, Fe K-edge X-ray absorption spectroscopy (XAS), Mossbauer spectroscopy, and visible/near-infrared (VNIR) reflectance spectroscopy. The range of redox states was Fe3+/sigma Fe=0 to 0.060.01 as determined by both XAS and, for short integration times, Mossbauer. The smectites have 060 distances (d((060))) between 1.53 and 1.56 angstrom, indicating a trioctahedral structure.d((060)) and XAS-derived interatomic Fe-(Fe,Mg,Al) distance scaled with Fe content. Smectite VNIR spectra feature OH/H2O absorption bands at 1.4 and 1.9 mu m, (Fe2+,Mg,Al)(3)-OH stretching bands near 1.4 mu m, and Fe2+Fe2+Fe2+-OH, MgMgMg-OH, AlAl(Mg,Fe2+)-OH, and AlAl-OH combination bands at 2.36 mu m, 2.32 mu m 2.25 mu m, and 2.20 mu m, respectively. The spectra for ferrous saponites are distinct from those for dioctahedral ferric smectites, permitting their differentiation from orbital observations. X-ray diffraction patterns for synthetic high-Mg ferrosaponite and high-Mg ferrian saponite are both consistent with the Sheepbed saponite detected by the chemistry and mineralogy (CheMin) instrument at Gale Crater, Mars, suggesting that anoxic basalt alteration was a viable pathway for clay mineral formation on early Mars. C1 [Chemtob, Steven M.; Nickerson, Ryan D.; Catalano, Jeffrey G.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Chemtob, Steven M.; Catalano, Jeffrey G.] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO USA. [Morris, Richard V.] NASA, Lyndon B Johnson Space Ctr, EIS Directorate, Houston, TX 77058 USA. [Agresti, David G.] Univ Alabama Birmingham, Dept Phys, Birmingham, AL 35294 USA. RP Chemtob, SM (reprint author), Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. EM chemtob@levee.wustl.edu RI Catalano, Jeffrey/A-8322-2013 OI Catalano, Jeffrey/0000-0001-9311-977X FU NASA [NX11AH09G, NNX14AJ95G]; McDonnell Center for the Space Sciences at Washington University; National Science Foundation [EAR-1161543]; DOE Office of Science [DE-AC02-06CH11357] FX This research was supported by the NASA Mars Fundamental Research Program under awards NX11AH09G and NNX14AJ95G. Additional support was provided to S.M.C. by the McDonnell Center for the Space Sciences at Washington University. Use of the XRD facility at Washington University is supported by the National Science Foundation under award EAR-1161543. This research used resources of the Advanced Photon Source, a U.S. Department of Energy (DOE) Office of Science User Facility operated for the DOE Office of Science by Argonne National Laboratory under contract DE-AC02-06CH11357. We thank Chris Gorski for collecting preliminary Mossbauer spectra on two samples. We thank Qing Ma (5-BM-D), Sungsik Lee (12-BM-B), and Matt Newville (13-BM-D) for their assistance with XAFS data collection at the Advanced Photon Source. We thank Abigail Fraeman for her assistance with VNIR reflectance spectra collection. We thank M. Darby Dyar and Joseph Michalski for their reviews that greatly improved the quality of the manuscript. Data sets presented in this manuscript are available by e-mail requests directed to the corresponding author (S.M.C.). NR 84 TC 1 Z9 1 U1 3 U2 29 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 JUN PY 2015 VL 120 IS 6 BP 1119 EP 1140 DI 10.1002/2014JE004763 PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CM8LB UT WOS:000357951300005 ER PT J AU Wordsworth, RD Kerber, L Pierrehumbert, RT Forget, F Head, JW AF Wordsworth, Robin D. Kerber, Laura Pierrehumbert, Raymond T. Forget, Francois Head, James W. TI Comparison of "warm and wet" and "cold and icy" scenarios for early Mars in a 3-D climate model SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE paleoclimate; early Mars; atmospheres; hydrology; valley networks; astrobiology ID GENERAL-CIRCULATION MODEL; EARLY MARTIAN CLIMATE; LONG-TERM EVOLUTION; CO2; CLOUDS; GREENHOUSE; VALLEYS; SURFACE; OCEAN; WATER AB We use a 3-D general circulation model to compare the primitive Martian hydrological cycle in warm and wet and cold and icy scenarios. In the warm and wet scenario, an anomalously high solar flux or intense greenhouse warming artificially added to the climate model are required to maintain warm conditions and an ice-free northern ocean. Precipitation shows strong surface variations, with high rates around Hellas basin and west of Tharsis but low rates around Margaritifer Sinus (where the observed valley network drainage density is nonetheless high). In the cold and icy scenario, snow migration is a function of both obliquity and surface pressure, and limited episodic melting is possible through combinations of seasonal, volcanic, and impact forcing. At surface pressures above those required to avoid atmospheric collapse (approximate to 0.5bar) and moderate to high obliquity, snow is transported to the equatorial highland regions where the concentration of valley networks is highest. Snow accumulation in the Aeolis quadrangle is high, indicating an ice-free northern ocean is not required to supply water to Gale crater. At lower surface pressures and obliquities, both H2O and CO2 are trapped as ice at the poles and the equatorial regions become extremely dry. The valley network distribution is positively correlated with snow accumulation produced by the cold and icy simulation at 41.8 degrees obliquity but uncorrelated with precipitation produced by the warm and wet simulation. Because our simulations make specific predictions for precipitation patterns under different climate scenarios, they motivate future targeted geological studies. C1 [Wordsworth, Robin D.] Harvard Univ, Paulson Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Wordsworth, Robin D.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Kerber, Laura] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Pierrehumbert, Raymond T.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Forget, Francois] Inst Pierre Simon Laplace, Lab Meterol Dynam, Paris, France. [Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. RP Wordsworth, RD (reprint author), Harvard Univ, Paulson Sch Engn & Appl Sci, Cambridge, MA 02138 USA. EM rwordsworth@seas.harvard.edu OI Pierrehumbert, Raymond/0000-0002-5887-1197 NR 76 TC 22 Z9 22 U1 9 U2 37 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 JUN PY 2015 VL 120 IS 6 BP 1201 EP 1219 DI 10.1002/2015JE004787 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CM8LB UT WOS:000357951300009 ER PT J AU Cook-Hallett, C Barnes, JW Kattenhorn, SA Hurford, T Radebaugh, J Stiles, B Beuthe, M AF Cook-Hallett, Casey Barnes, Jason W. Kattenhorn, Simon A. Hurford, Terry Radebaugh, Jani Stiles, Bryan Beuthe, Mikael TI Global contraction/expansion and polar lithospheric thinning on Titan from patterns of tectonism SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Titan; global stress fields; tectonics ID CASSINI RADAR; VIMS OBSERVATIONS; GROOVED TERRAIN; DESPUN PLANET; XANADU REGION; FEATURES; SURFACE; RECONNAISSANCE; ENCELADUS; EVOLUTION AB We investigate the underlying physical processes that govern the formation and evolution of Titan's tectonic features. This is done by mapping mountain chains and hills using Cassini RADAR data obtained during Titan flybys T3 to T69. Our mapping of mountain chains and hills reveals a global pattern: east-west orientations within 30 degrees of the equator and north-south between 60 degrees latitude and the poles. This result makes Titan one of the few solar system bodies where global processes, rather than regional processes, dominate tectonism. After comparison with five global stress models showing theoretical mountain chain orientations, we suggest that either global contraction coupled with spin-up or global expansion coupled with despinning could explain our observations if coupled with a lithosphere thinner in Titan's polar regions. C1 [Cook-Hallett, Casey; Barnes, Jason W.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA. [Cook-Hallett, Casey] North Idaho Coll, Div Nat Sci, Coeur Dalene, ID USA. [Kattenhorn, Simon A.] Univ Idaho, Dept Geol Sci, Moscow, ID 83843 USA. [Hurford, Terry] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Radebaugh, Jani] Brigham Young Univ, Dept Geol, Provo, UT 84602 USA. [Stiles, Bryan] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Beuthe, Mikael] Royal Observ Belgium, Brussels, Belgium. RP Cook-Hallett, C (reprint author), Univ Idaho, Dept Phys, Moscow, ID 83844 USA. EM cook6924@vandals.uidaho.edu RI Barnes, Jason/B-1284-2009; Hurford, Terry/F-2625-2012 OI Barnes, Jason/0000-0002-7755-3530; FU NASA [NNX10AQ10G]; PRODEX program; Belgian Federal Science Policy Office; National Aeronautics and Space Administration FX Thanks to Alex Patthoff and Emily Martin for discussions and lessons on ArcGIS. The authors acknowledge support from NASA Outer Planets Research Program grant NNX10AQ10G. M. Beuthe is supported by the PRODEX program managed by the European Space Agency and the Belgian Federal Science Policy Office. The portion of this research carried out by B. Stiles was done so at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The data to support this article are from the National Aeronautics and Space Administration (NASA). ArcGIS shapefiles are available at the following website:r5d4. barnesos.net/GlobalPatternsofTectonism. NR 59 TC 6 Z9 6 U1 2 U2 6 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 JUN PY 2015 VL 120 IS 6 BP 1220 EP 1236 DI 10.1002/2014JE004645 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CM8LB UT WOS:000357951300010 ER PT J AU Nastula, J Gross, R AF Nastula, J. Gross, R. TI Chandler wobble parameters from SLR and GRACE SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE Chandler wobble parameters; SLR; GRACE ID POLAR MOTION; OCEANIC EXCITATION; GRAVITATIONAL CHANGES; ANGULAR-MOMENTUM; EARTH ROTATION; SERIES; MODELS; PERIOD AB The period and quality factor Q of the Chandler wobble are functions of the internal structure and dissipation processes of the Earth. Better estimates of the period and Q of the Chandler wobble can therefore be used to better understand these properties of the Earth. Here the period and Q of the Chandler wobble are estimated by finding those values that minimize the power in the Chandler frequency band of the difference between observed and modeled polar motion excitation functions. The observations of the polar motion excitation functions that we used are derived from both space-geodetic polar motion observations and from satellite laser ranging (SLR) and Gravity Recovery and Climate Experiment (GRACE) observations of the degree-2 coefficients of the Earth's time-varying gravitational field. The models of the polar motion excitation functions that we used are derived from general circulation models of the atmosphere and oceans and from hydrologic models. Our preferred values for the period and Q of the Chandler wobble that we estimated using this approach are 430.90.7 solar days and 127 (56, 255), respectively. C1 [Nastula, J.] Polish Acad Sci, Space Res Ctr, PL-01237 Warsaw, Poland. [Gross, R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Nastula, J (reprint author), Polish Acad Sci, Space Res Ctr, PL-01237 Warsaw, Poland. EM nastula@cbk.waw.pl FU Ministry of Scientific Research and Information Technology [2012/05/B/ST10/02132, 2014/13/B/ST10/04975]; National Aeronautics and Space Administration; Earth Surface and Interior Focus Area of NASA's Science Mission Directorate FX J. Nastula was supported by the Ministry of Scientific Research and Information Technology through projects 2012/05/B/ST10/02132 and 2014/13/B/ST10/04975. J. Nastula thanks Waldemar Popinski for writing the Multitaper computer procedures used in the numerical computations. The work of R. Gross described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Support for that work was provided by the Earth Surface and Interior Focus Area of NASA's Science Mission Directorate. The data series is accessible from the following: The x, y COMB polar motion data series are available from: http://keof.jpl.nasa.gov. The Atmospheric Angular Momentum (AAM), Oceanic Angular Momentum (OAM), and Hydrospheric Angular momentum (HAM) data series are available from http://www.gfz-potsdam.de/en/research/organizational-units/departments/d epartment-1/earth-system-modelling/services/eam/. The Delta C21 and Delta S21 data series estimated from the GRACE observations are available from http:/podaac.jpl.nasa.gov/dataacces. The Delta C21 and Delta S21 data series denoted as SLR2 are available from http:/grace.jpl.nasa.gov/data/weekly5x5gravityharmonicsdata/. The Delta C21 and Delta S21 data series denoted as SLR1 were made available by M. Cheng and are available from him upon request (cs21.801110 series, Minkang Cheng, Ph.D Research Scientist, Center for Space Research, 3925 W. Braker Ln. Ste. 200 Austin, Texas 78759 Phone: 512-471-7818 FAX: 512-232-2443 cheng@csr.utexas.edu. NR 49 TC 6 Z9 6 U1 2 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD JUN PY 2015 VL 120 IS 6 BP 4474 EP 4483 DI 10.1002/2014JB011825 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CM8ZG UT WOS:000357993000026 ER PT J AU Zwieback, S Hensley, S Hajnsek, I AF Zwieback, Simon Hensley, Scott Hajnsek, Irena TI A Polarimetric First-Order Model of Soil Moisture Effects on the DInSAR Coherence SO REMOTE SENSING LA English DT Article DE DInSAR; InSAR; interferometry; electromagnetic model; soil moisture; deformations; displacement ID RADAR INTERFEROMETRY; SAR INTERFEROMETRY; PENETRATION; RETRIEVALS; VEGETATION AB Changes in soil moisture between two radar acquisitions can impact the observed coherence in differential interferometry: both coherence magnitude || and phase phi are affected. The influence on the latter potentially biases the estimation of deformations. These effects have been found to be variable in magnitude and sign, as well as dependent on polarization, as opposed to predictions by existing models. Such diversity can be explained when the soil is modelled as a half-space with spatially varying dielectric properties and a rough interface. The first-order perturbative solution achieves-upon calibration with airborne L band data-median correlations at HH polarization of 0.77 for the phase phi, of 0.50 for ||, and for the phase triplets of 0.56. The predictions are sensitive to the choice of dielectric mixing model, in particular the absorptive properties; the differences between the mixing models are found to be partially compensatable by varying the relative importance of surface and volume scattering. However, for half of the agricultural fields the Hallikainen mixing model cannot reproduce the observed sensitivities of the phase to soil moisture. In addition, the first-order expansion does not predict any impact on the HV coherence, which is however empirically found to display similar sensitivities to soil moisture as the co-pol channels HH and VV. These results indicate that the first-order solution, while not able to reproduce all observed phenomena, can capture some of the more salient patterns of the effect of soil moisture changes on the HH and VV DInSAR signals. Hence it may prove useful in separating the deformations from the moisture signals, thus yielding improved displacement estimates or new ways for inferring soil moisture. C1 [Zwieback, Simon; Hajnsek, Irena] ETH, Inst Environm Engn, CH-8093 Zurich, Switzerland. [Hensley, Scott] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hajnsek, Irena] German Aerosp Ctr DLR, Microwaves & Radar Inst, D-82230 Wessling, Germany. RP Zwieback, S (reprint author), ETH, Inst Environm Engn, Stefano Franscini Pl 3, CH-8093 Zurich, Switzerland. EM zwieback@ifu.baug.ethz.ch; scott.hensley@jpl.nasa.gov; irena.hajnsek@dlr.de FU Helmholtz Alliance [HA310] FX The authors would like to thank the reviewers for their insightful comments and suggestions. The study has been conducted under the support of the Helmholtz Alliance HA310 "Remote Sensing and Earth System Dynamics". NR 42 TC 6 Z9 6 U1 3 U2 12 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD JUN PY 2015 VL 7 IS 6 BP 7571 EP 7596 DI 10.3390/rs70607571 PG 26 WC Remote Sensing SC Remote Sensing GA CM3NX UT WOS:000357590300003 ER PT J AU Jung, HC Jasinski, MF AF Jung, Hahn Chul Jasinski, Michael F. TI Sensitivity of a Floodplain Hydrodynamic Model to Satellite- Based DEM Scale and Accuracy: Case Study-The Atchafalaya Basin SO REMOTE SENSING LA English DT Article DE Atchafalaya; digital elevation model; floodplain; hydrodynamic model; Surface Water and Ocean Topography (SWOT) mission ID RASTER-BASED MODEL; INUNDATION SIMULATION; MESH RESOLUTION; RIVER-BASIN; PRONE AREAS; FLOW; REPRESENTATION; DELINEATION; ALTIMETRY; AMAZON AB The hydrodynamics of low-lying riverine floodplains and wetlands play a critical role in hydrology and ecosystem processes. Because small topographic features affect floodplain storage and flow velocity, a hydrodynamic model setup of these regions imposes more stringent requirements on the input Digital Elevation Model (DEM) compared to upland regions with comparatively high slopes. This current study provides a systematic approach to evaluate the required relative vertical accuracy and spatial resolution of current and future satellite-based altimeters within the context of DEM requirements for 2-D floodplain hydrodynamic models. A case study is presented for the Atchafalaya Basin with a model domain of 1190 km(2). The approach analyzes the sensitivity of modeled floodplain water elevation and velocity to typical satellite-based DEM grid-box scale and vertical error, using a previously calibrated version of the physically-based flood inundation model (LISFLOOD-ACC). Results indicate a trade-off relationship between DEM relative vertical error and grid-box size. Higher resolution models are the most sensitive to vertical accuracy, but the impact diminishes at coarser resolutions because of spatial averaging. The results provide guidance to engineers and scientists when defining the observation scales of future altimetry missions such as the Surface Water and Ocean Topography (SWOT) mission from the perspective of numerical modeling requirements for large floodplains of O[10(3)] km(2) and greater. C1 [Jung, Hahn Chul] Sci Syst & Applicat Inc SSAI, Lanham, MD 20706 USA. [Jung, Hahn Chul] NASA, Goddard Space Flight Ctr, Off Appl Sci, Greenbelt, MD 20771 USA. [Jasinski, Michael F.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. RP Jung, HC (reprint author), Sci Syst & Applicat Inc SSAI, 10210 Greenbelt Rd, Lanham, MD 20706 USA. EM hahnchul.jung@nasa.gov; michael.f.jasinski@nasa.gov FU NASA; NASA's Terrestrial Hydrology Program; Goddard Space Flight Center (GSFC) FX This research was supported by an appointment to the NASA Postdoctoral Program (NPP) at the Goddard Space Flight Center (GSFC), administered by Oak Ridge Associated Universities (ORAU) through a contract with NASA, and by NASA's Terrestrial Hydrology Program. We gratefully acknowledge Paul Bates for use of the LISFLOOD-ACC model. LiDAR data were obtained from the USGS National Geospatial Program and USGS Coastal and Marine Geology Program archives. NR 47 TC 2 Z9 2 U1 4 U2 16 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD JUN PY 2015 VL 7 IS 6 BP 7938 EP 7958 DI 10.3390/rs70607938 PG 21 WC Remote Sensing SC Remote Sensing GA CM3NX UT WOS:000357590300020 ER PT J AU Savani, NP Vourlidas, A Szabo, A Mays, ML Richardson, IG Thompson, BJ Pulkkinen, A Evans, R Nieves-Chinchilla, T AF Savani, N. P. Vourlidas, A. Szabo, A. Mays, M. L. Richardson, I. G. Thompson, B. J. Pulkkinen, A. Evans, R. Nieves-Chinchilla, T. TI Predicting the magnetic vectors within coronal mass ejections arriving at Earth: 1. Initial architecture SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE CMEs; Bz forecasts ID STRUCTURED SOLAR-WIND; IN-SITU OBSERVATIONS; CLOUDS; FIELD; FLUX; EVOLUTION; PROPAGATION; SPACE; CMES; AU AB The process by which the Sun affects the terrestrial environment on short timescales is predominately driven by the amount of magnetic reconnection between the solar wind and Earth's magnetosphere. Reconnection occurs most efficiently when the solar wind magnetic field has a southward component. The most severe impacts are during the arrival of a coronal mass ejection (CME) when the magnetosphere is both compressed and magnetically connected to the heliospheric environment. Unfortunately, forecasting magnetic vectors within coronal mass ejections remain elusive. Here we report how, by combining a statistically robust helicity rule for a CME's solar origin with a simplified flux rope topology, the magnetic vectors within the Earth-directed segment of a CME can be predicted. In order to test the validity of this proof-of-concept architecture for estimating the magnetic vectors within CMEs, a total of eight CME events (between 2010 and 2014) have been investigated. With a focus on the large false alarm of January 2014, this work highlights the importance of including the early evolutionary effects of a CME for forecasting purposes. The angular rotation in the predicted magnetic field closely follows the broad rotational structure seen within the in situ data. This time-varying field estimate is implemented into a process to quantitatively predict a time-varying Kp index that is described in detail in paper II. Future statistical work, quantifying the uncertainties in this process, may improve the more heuristic approach used by early forecasting systems. C1 [Savani, N. P.; Vourlidas, A.] Univ Maryland Baltimore Cty, GPHI, Baltimore, MD 21228 USA. [Savani, N. P.; Szabo, A.; Mays, M. L.; Richardson, I. G.; Thompson, B. J.; Pulkkinen, A.; Nieves-Chinchilla, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mays, M. L.; Nieves-Chinchilla, T.] Catholic Univ Amer, IACS, Washington, DC 20064 USA. [Richardson, I. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Evans, R.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. RP Savani, NP (reprint author), Univ Maryland Baltimore Cty, GPHI, Baltimore, MD 21228 USA. EM neel.savani02@imperial.ac.uk RI Nieves-Chinchilla, Teresa/F-3482-2016; Thompson, Barbara/C-9429-2012; Vourlidas, Angelos/C-8231-2009; OI Nieves-Chinchilla, Teresa/0000-0003-0565-4890; Vourlidas, Angelos/0000-0002-8164-5948; Richardson, Ian/0000-0002-3855-3634 FU NASA [NNH14AX40I, S-136361-Y] FX This work was supported by NASA grant NNH14AX40I and NASA contract S-136361-Y to NRL. We thank Y.-M. Wang (NRL) for constructive comments about active region helicity, and M. Stockman (SWPC) and B. Murtagh (SWPC) for clarifying the forecasting policy and procedures at SWPC. We thank M. Shankar for his lively debates throughout the process. The OMNI data were obtained from the GSFC/SPDF OMNIWeb interface at http://omniweb.gsfc.nasa.gov. NR 60 TC 13 Z9 13 U1 0 U2 8 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 JUN PY 2015 VL 13 IS 6 BP 374 EP 385 DI 10.1002/2015SW001171 PG 12 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA CM8NT UT WOS:000357959400007 ER PT J AU Kong, AYY Rosenzweig, C Arky, J AF Kong, Angela Y. Y. Rosenzweig, Cynthia Arky, Joshua TI Nitrogen Dynamics Associated with Organic and Inorganic Inputs to Substrate Commonly Used on Rooftop Farms SO HORTSCIENCE LA English DT Article DE compost; leachate; organic matter; potential mineralizable nitrogen; rooftop farm; urban agriculture ID MINERALIZABLE NITROGEN; QUALITY PERFORMANCE; MICROBIAL BIOMASS; SWISS-CHARD; RUNOFF; SOILS; SYSTEMS; ECOSYSTEMS; MANAGEMENT; FERTILIZER AB Employing rooftops for the cultivation of crops in limited urban space has garnered interest in densely populated cities in the United States, where there is a growing demand for locally sourced vegetable products. Fertility management recommendations for rooftop farming, however, are scant. With insufficient research on nutrient cycling within rooftop farming systems, which tend to use soilless substrates with low organic matter content, the potential tradeoffs between the negative impacts (e.g., nutrient runoff) and the benefits (e.g., increased locally produced vegetables, stormwater retention, etc.) associated with rooftop farms are unclear. The objective of this study was to evaluate the effects of organic and inorganic nitrogen (N) inputs on the N dynamics within substrate typically used on rooftop farms. Substrate without added N inputs (control) was compared with substrates receiving N sources that are both realistic for and/or reflective of amendments currently applied on urban rooftop farms: a synthetic fertilizer (Osmocote (R) 14N-4.2P-11.6K), and three organic N inputs composted poultry manure, municipal green waste (MGW) compost, and vermicompost. Aboveground crop biomass and yields of Beta vulgaris (swiss chard), along with inorganic N availability (ammonium: NH4+ and nitrate: NOD, potentially mineralizable nitrogen (PMN), leachate-inorganic N concentrations, and pH and electrical conductivity (EC) levels were measured during an 8-week greenhouse experiment. Despite differences in carbon-to-nitrogen ratios (C:N), few differences in N cycling and yields were found among the treatments receiving organic N inputs. Crop yields from the synthetic fertilizer and MGW compost treatments were higher than the other organic N input treatments. Inorganic N levels in the synthetic fertilizer treatment decreased from 129 mg N/L at the start of the season to 113 mg N/L at the end of the season, while nearly 10-fold decreases of inorganic N concentrations in the substrate of the control and organic N input treatments from week 0 (79.5-117.8 mg N/L) to week 8 (12.8-16.6 mg N/L) were observed. Greater N availability at critical periods during the season may have promoted greater crop N uptake efficiency and, therefore, higher yields in the system receiving synthetic fertilizer. However, the greatest losses of NH4+ and NO3- via leachate were also measured from this treatment. Our results show that the type of N input influenced plant-available N and yields and that the MGW compost treatment best achieved the balance between higher yields and reduced N losses to potential roof runoff. Furthermore, additional N inputs to these systems, particularly to the treatments receiving organic composts, will likely be necessary if a high N-demanding crop (such as swiss chard) is to be grown in the same substrates for more than 8 weeks. Rooftop farming is an emergent component of urban agriculture; regulations and guidelines for nutrient management of rooftop farms are necessary to optimize productivity and long-term benefits and to minimize negative environmental impacts. C1 [Kong, Angela Y. Y.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10021 USA. [Rosenzweig, Cynthia] NASA, Goddard Inst Space Studies, New York, NY 10021 USA. [Arky, Joshua] Columbia Univ, Off Acad & Res Programs, Earth Inst, Sustainable Dev, New York, NY 10021 USA. RP Kong, AYY (reprint author), Columbia Univ, Ctr Climate Syst Res, 545 West 112th St, New York, NY 10021 USA. EM ak3132@columbia.edu NR 50 TC 1 Z9 1 U1 5 U2 39 PU AMER SOC HORTICULTURAL SCIENCE PI ALEXANDRIA PA 113 S WEST ST, STE 200, ALEXANDRIA, VA 22314-2851 USA SN 0018-5345 EI 2327-9834 J9 HORTSCIENCE JI Hortscience PD JUN PY 2015 VL 50 IS 6 BP 806 EP 813 PG 8 WC Horticulture SC Agriculture GA CM5YY UT WOS:000357766100008 ER PT J AU Andersson, AJ Kline, DI Edmunds, PJ Archer, SD Bednarsek, N Carpenter, RC Chadsey, M Goldstein, P Grottoli, AG Hurst, TP King, AL Kubler, JE Kuffner, IB Mackey, KRM Menge, BA Paytan, A Riebesell, U Schnetzer, A Warner, ME Zimmerman, RC AF Andersson, Andreas J. Kline, David I. Edmunds, Peter J. Archer, Stephen D. Bednarsek, Nina Carpenter, Robert C. Chadsey, Meg Goldstein, Philip Grottoli, Andrea G. Hurst, Thomas P. King, Andrew L. Kuebler, Janet E. Kuffner, Ilsa B. Mackey, Katherine R. M. Menge, Bruce A. Paytan, Adina Riebesell, Ulf Schnetzer, Astrid Warner, Mark E. Zimmerman, Richard C. TI Understanding Ocean Acidification Impacts on Organismal to Ecological Scales SO OCEANOGRAPHY LA English DT Editorial Material ID CARBON-DIOXIDE; CORAL-REEFS; ANTHROPOGENIC CO2; MARINE ORGANISMS; CALCIFICATION; PHOTOSYNTHESIS; ECOSYSTEM; PH; METAANALYSIS; MESOCOSM AB Ocean acidification (OA) research seeks to understand how marine ecosystems and global elemental cycles will respond to changes in seawater carbonate chemistry in combination with other environmental perturbations such as warming, eutrophication, and deoxygenation. Here, we discuss the effectiveness and limitations of current research approaches used to address this goal. A diverse combination of approaches is essential to decipher the consequences of OA to marine organisms, communities, and ecosystems. Consequently, the benefits and limitations of each approach must be considered carefully. Major research challenges involve experimentally addressing the effects of OA in the context of large natural variability in seawater carbonate system parameters and other interactive variables, integrating the results from different research approaches, and scaling results across different temporal and spatial scales. C1 [Andersson, Andreas J.; Kline, David I.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Edmunds, Peter J.; Carpenter, Robert C.; Kuebler, Janet E.] Calif State Univ Northridge, Northridge, CA 91330 USA. [Archer, Stephen D.] Bigelow Lab Ocean Sci, East Boothbay, ME USA. [Bednarsek, Nina] NOAA, Pacific Marine Environm Lab, Newport, OR USA. [Chadsey, Meg] Washington Sea Grant, Seattle, WA USA. [Goldstein, Philip] Univ Colorado, Boulder, CO 80309 USA. [Grottoli, Andrea G.] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA. [Hurst, Thomas P.] NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Hatfield Marine Sci Ctr, Newport, OR USA. [King, Andrew L.] NOAA, Northeast Fisheries Sci Ctr, Silver Spring, MD USA. [Kuffner, Ilsa B.] US Geol Survey, St Petersburg, FL USA. [Mackey, Katherine R. M.] Univ Calif Irvine, Earth Syst Sci, Irvine, CA USA. [Menge, Bruce A.] Oregon State Univ, Integrat Biol, Corvallis, OR 97331 USA. [Menge, Bruce A.] Oregon State Univ, Marine Biol, Corvallis, OR 97331 USA. [Paytan, Adina] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Riebesell, Ulf] GEOMAR Helmholtz Ctr Ocean Res, Biol Oceanog, Kiel, Germany. [Schnetzer, Astrid] N Carolina State Univ, Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA. [Warner, Mark E.] Univ Delaware, Coll Earth Ocean & Environm, Newark, DE USA. [Zimmerman, Richard C.] Old Dominion Univ, Earth Ocean & Atmospher Sci, Norfolk, VA USA. RP Andersson, AJ (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. EM aandersson@ucsd.edu; dkline@ucsd.edu OI Kuffner, Ilsa/0000-0001-8804-7847 NR 88 TC 12 Z9 12 U1 9 U2 94 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD JUN PY 2015 VL 28 IS 2 SI SI BP 16 EP 27 PG 12 WC Oceanography SC Oceanography GA CL8NP UT WOS:000357231700005 ER PT J AU Busch, DS O'Donnell, MJ Hauri, C Mach, KJ Poach, M Doney, SC Signorini, SR AF Busch, D. Shallin O'Donnell, Michael J. Hauri, Claudine Mach, Katharine J. Poach, Matthew Doney, Scott C. Signorini, Sergio R. TI Understanding, Characterizing, and Communicating Responses to Ocean Acidification CHALLENGES AND UNCERTAINTIES SO OCEANOGRAPHY LA English DT Article ID MARINE ORGANISMS; CLIMATE-CHANGE; CORAL-REEFS; ECOSYSTEM; IMPACTS; SCIENCE; CO2; COMMUNITIES; ADAPTATION; STRESSORS AB Over the past decade, ocean acidification (OA) has emerged as a major concern in ocean science. The field of OA is based on certainties-update of carbon dioxide into the global ocean alters its carbon chemistry, and many marine organisms, especially calcifiers, are sensitive to this change. However, the field must accommodate uncertainties about the seriousness of these impacts as it synthesizes and draws conclusions from multiple disciplines. There is pressure from stakeholders to expeditiously inform society about the extent to which OA will impact marine ecosystems and the people who depend on them. Ultimately, decisions about actions related to OA require evaluating risks about the likelihood and magnitude of these impacts. As the scientific literature accumulates, some of the uncertainty related to single-species sensitivity to OA is diminishing. Difficulties remain in scaling laboratory results to species and ecosystem responses in nature, though modeling exercises provide useful insight. As recognition of OA grows scientists' ability to communicate the certainties and uncertainties of our knowledge on OA is crucial for interaction with decision makers. In this regard, there are a number of valuable practices that can be drawn from other fields, especially the global climate change community. A generally accepted set of best practices that scientists follow in their discussions of uncertainty would be helpful for the community engaged in ocean acidification. C1 [Busch, D. Shallin] NOAA, Ocean Acidificat Program, Silver Spring, MD USA. [Busch, D. Shallin] NOAA, Natl Marine Fisheries Serv, Off Sci & Technol, Silver Spring, MD USA. [O'Donnell, Michael J.] Calif Ocean Sci Trust, Oakland, CA USA. [Hauri, Claudine] Univ Hawaii, Sch Ocean & Earth Sci & Technol, Int Pacific Res Ctr, Honolulu, HI 96822 USA. [Hauri, Claudine] Univ Alaska Fairbanks, Int Arctic Res Ctr, Fairbanks, AK USA. [Mach, Katharine J.] Carnegie Inst Sci, IPCC Working Grp Tech Support Unit 2, Dept Global Ecol, Sci, Stanford, CA USA. [Poach, Matthew] NOAA, James J Howard Marine Sci Lab, Northeast Fisheries Sci Ctr, NMFS, Highlands, NJ USA. [Doney, Scott C.] Woods Hole Oceanog Inst, Dept Marine Chem & Geochem, Woods Hole, MA 02543 USA. [Signorini, Sergio R.] Sci Applicat Int Corp, Mclean, VA 22102 USA. [Signorini, Sergio R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Busch, DS (reprint author), NOAA, Ocean Acidificat Program, Seattle, WA 98115 USA. EM shallin.busch@noaa.gov RI Doney, Scott/F-9247-2010 OI Doney, Scott/0000-0002-3683-2437 FU NOAA Ocean Acidification Program; National Marine Fisheries Service; NSF-supported Center for Climate and Energy Decision Making; NASA Ocean Biology and Biogeochemistry Program FX We thank the organizers of the 2013 OA Principal Investigators Meeting for their efforts to build a community of OA researchers and for their foresight in providing us the venue to develop the themes discussed in this paper. W. Balch, F. Dobbs, H. Galindo, J. Grear, F. Morel, S. Palumbi, M. Saito, and C. Zakroff contributed to the initial discussions around uncertainty. R. Brainard and an anonymous reviewer provided comments that improved the manuscript The following funding sources supported our work on this manuscript: NOAA Ocean Acidification Program and National Marine Fisheries Service (DSB, MP), NSF-supported Center for Climate and Energy Decision Making (SCD), and NASA Ocean Biology and Biogeochemistry Program (SS). The content of this manuscript does not reflect any position of the US Government or of NOAA. NR 65 TC 5 Z9 5 U1 7 U2 43 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD JUN PY 2015 VL 28 IS 2 SI SI BP 30 EP 39 DI 10.5670/oceanog.2015.29 PG 10 WC Oceanography SC Oceanography GA CL8NP UT WOS:000357231700007 ER PT J AU Alin, SR Brainard, RE Price, NN Newton, JA Cohen, A Peterson, WT DeCarlo, EH Shadwick, EH Noakes, S Bednarsek, N AF Alin, Simone R. Brainard, Russell E. Price, Nichole N. Newton, Jan A. Cohen, Anne Peterson, William T. DeCarlo, Eric H. Shadwick, Elizabeth H. Noakes, Scott Bednarsek, Nina TI Characterizing the Natural System: Toward Sustained, Integrated Coastal Ocean Acidification Observing Networks to Facilitate Resource Management and Decision Support SO OCEANOGRAPHY LA English DT Article ID CONTINENTAL-SHELF; ECOSYSTEMS; SATURATION; PACIFIC; IMPACTS; CARBON AB Coastal ocean ecosystems have always served human populations they provide food security, livelihoods, coastal protection, and defense. Ocean acidification is a global threat to these ecosystem services, particularly when other local and regional stressors combine with it to jeopardize coastal health. Monitoring efforts call for a coordinated global approach toward sustained, integrated coastal ocean health observing networks to address the region-specific mix of factors while also adhering to global ocean acidification observing network principles to facilitate comparison among regions for increased utility and understanding. Here, we generalize guidelines for scoping and designing regional coastal ocean acidification observing networks and provide examples of existing efforts. While challenging in the early stages of coordinating the design and prioritizing the implementation Of these observing networks, it is essential to actively engage all of the relevant stakeholder groups from the outset, including private industries, public agencies, regulatory bodies, decision makers, and the general public. The long-term sustainability of these critical observing networks will rely on leveraging of resources and the strength of partnerships across the consortium of stakeholders and those implementing coastal ocean health observing networks. C1 [Alin, Simone R.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. [Brainard, Russell E.] NOAA, Coral Reef Ecosyst Div, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI USA. [Price, Nichole N.] Bigelow Lab Ocean Sci, East Boothbay, ME USA. [Newton, Jan A.] Univ Washington, Washington Ocean Acidificat Ctr, Seattle, WA 98195 USA. [Cohen, Anne] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. [Peterson, William T.] NOAA, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR USA. [DeCarlo, Eric H.] Univ Hawaii Manoa, Dept Oceanog, Marine Geol & Geochem Div, Honolulu, HI 96822 USA. [Shadwick, Elizabeth H.] Virginia Inst Marine Sci, Coll William & Mary, Gloucester Point, VA 23062 USA. [Noakes, Scott] Univ Georgia, Ctr Appl Isotope Studies, Athens, GA 30602 USA. [Bednarsek, Nina] Univ Washington, Sch Marine & Environm Affairs, Seattle, WA 98195 USA. RP Alin, SR (reprint author), NOAA, Pacific Marine Environm Lab, 7600 Sand Point Way Ne, Seattle, WA 98115 USA. EM simone.r.alin@noaa.gov FU National Science Foundation; National Aeronautics and Space Administration; National Oceanic and Atmospheric Administration FX The authors wish to thank the Ocean Carbon and Biogeochemistry Program and its Ocean Acidification Subcommittee for organizing and hosting the Second Ocean Acidification Principal Investigators' Meeting, where the foundation for this article was laid. We also thank the National Science Foundation, National Aeronautics and Space Administration, and the National Oceanic and Atmospheric Administration for funding the meeting, as well as much of the science that informed our productive discussions. We thank Jon Hare for discussion that particularly improved the manuscript, as well as Richard Feely, the editors, and two anonymous reviewers for constructive reviews on earlier versions. Alin thanks NOAAs Ocean Acidification Program and Pacific Marine Environmental Laboratory (PMEL contribution number 4267) for supporting her role in the meeting and paper. NR 43 TC 3 Z9 3 U1 4 U2 24 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD JUN PY 2015 VL 28 IS 2 SI SI BP 92 EP 107 DI 10.5670/oceanog.2015.34 PG 16 WC Oceanography SC Oceanography GA CL8NP UT WOS:000357231700012 ER PT J AU Salisbury, J Vandemark, D Jonsson, B Balch, W Chakraborty, S Lohrenz, S Chapron, B Hales, B Mannino, A Mathis, JT Reul, N Signorini, SR Wanninkhof, R Yates, KK AF Salisbury, Joseph Vandemark, Douglas Joensson, Bror Balch, William Chakraborty, Sumit Lohrenz, Steven Chapron, Bertrand Hales, Burke Mannino, Antonio Mathis, Jeremy T. Reul, Nicolas Signorini, Sergio R. Wanninkhof, Rik Yates, Kimberly K. TI How Can Present and Future Satellite Missions Support Scientific Studies that Address Ocean Acidification? SO OCEANOGRAPHY LA English DT Article ID NEURAL-NETWORK TECHNIQUES; SEA-SURFACE TEMPERATURE; CONTINENTAL-SHELF; UPWELLING SYSTEM; TOTAL ALKALINITY; NORTH-ATLANTIC; RIVER PLUME; CO2; PHYTOPLANKTON; CARBON AB Space-based observations offer unique capabilities for studying spatial and temporal dynamics of the upper ocean inorganic carbon cycle and, in turn, supporting research tied to ocean acidification (OA). Satellite sensors measuring sea surface temperature, color, salinity, wind, waves, currents, and sea level enable a fuller understanding of a range of physical, chemical, and biological phenomena that drive regional OA dynamics as well as the potentially varied impacts of carbon cycle change on a broad range of ecosystems. Here, we update and expand on previous work that addresses the benefits of space-based' assets for OA and carbonate system studies. Carbonate chemistry and the key processes controlling surface ocean OA variability are reviewed. Synthesis of present satellite data streams and their utility in this arena are discussed, as are opportunities on the horizon for using new satellite sensors with increased spectral, temporal, and/or spatial resolution. We outline applications that include the ability to track the biochemically dynamic nature of water masses, to map coral reefs at higher resolution, to discern functional phytoplankton groups and their relationships to acid perturbations, and to track processes that contribute to acid variation near the land-ocean interface. C1 [Salisbury, Joseph; Vandemark, Douglas] Univ New Hampshire, Ocean Proc Anal Lab, Durham, NH 03824 USA. [Joensson, Bror] Princeton Univ, Geosci, Princeton, NJ 08544 USA. [Balch, William] Bigelow Lab Ocean Sci, East Boothbay, ME USA. [Chakraborty, Sumit; Lohrenz, Steven] Univ Massachusetts Dartmouth, Sch Marine Sci & Technol, New Bedford, MA USA. [Chapron, Bertrand] IFREMER, Lab Oceanog Spatiale, Plouzane, France. [Hales, Burke] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA. [Mannino, Antonio] NASA, Goddard Space Flight Ctr, Ocean Ecol Div, Greenbelt, MD 20771 USA. [Mathis, Jeremy T.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. [Reul, Nicolas] IFREMER, Lab Oceanog Spatiale, La Seyne Sur Mer, France. [Signorini, Sergio R.] Sci Applicat Int Corp, Mclean, VA 22102 USA. [Signorini, Sergio R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wanninkhof, Rik] NOAA, Atlantic Oceanog & Meteorol Lab, Miami, FL 33149 USA. [Yates, Kimberly K.] US Geol Survey, St Petersburg, FL USA. RP Salisbury, J (reprint author), Univ New Hampshire, Ocean Proc Anal Lab, Durham, NH 03824 USA. EM joe.salisbury@unh.edu RI Chapron, Bertrand/O-6527-2015; reul, nicolas/C-4895-2009; Mannino, Antonio/I-3633-2014; OI Lohrenz, Steven/0000-0003-3811-2975; Reul, Nicolas/0000-0003-4881-2967 FU NASA Ocean Biology & Biogeochemistry program [NNX14AL84G]; NOAA Ocean Acidification Program and Integrated Ocean Observing System programs, Northeastern Regional Association of Coastal Ocean Observing Systems (NERACOOS) [A002004, USM-GR05194-001]; National Oceanic and Atmospheric Administration (NOAA)'s Ocean Acidification Program; NOAA's Pacific Marine Environmental Laboratory (PMEL) [4303]; Pathfinder ESA-STSE Ocean Acidification; National Science Foundation FX We gratefully acknowledge our sponsors whose grants made this collaboration possible. The NASA Ocean Biology & Biogeochemistry program (particularly NNX14AL84G), the NOAA Ocean Acidification Program and Integrated Ocean Observing System programs, including Northeastern Regional Association of Coastal Ocean Observing Systems (NERACOOS) grants A002004 and USM-GR05194-001, Pathfinder ESA-STSE Ocean Acidification, and the National Science Foundation. Background and satellite images in Figure 1 are courtesy of NASA, except the GOCI satellite image, which is courtesy of the Korea Ocean Satellite Research Center and the SMOS satellite image, which is courtesy of the European Space Agency. Aquarius is a joint mission shared by NASA and CONAE. We appreciate the insightful critiques of Frank Muller-Karger, Nick Hardman-Mountford, and one anonymous reviewer, and thank Amy Ehntholt and Kristy Donahue for valuable help. References to non-USGS products and services are provided for information only and do not constitute endorsement or warranty, expressed or implied, by the US Government, as to their suitability, content, usefulness, functioning, completeness, or accuracy. We acknowledge funding support from the National Oceanic and Atmospheric Administration (NOAA)'s Ocean Acidification Program and NOAA's Pacific Marine Environmental Laboratory (PMEL contribution number 4303). NR 90 TC 1 Z9 1 U1 2 U2 17 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD JUN PY 2015 VL 28 IS 2 SI SI BP 108 EP 121 DI 10.5670/oceanog.2015.35 PG 14 WC Oceanography SC Oceanography GA CL8NP UT WOS:000357231700013 ER PT J AU Boehm, AB Jacobson, MZ O'Donnell, MJ Sutula, M Wakefield, WW Weisberg, SB Whiteman, E AF Boehm, Alexandria B. Jacobson, Mark Z. O'Donnell, Michael J. Sutula, Martha Wakefield, W. Waldo Weisberg, Stephen B. Whiteman, Elizabeth TI Ocean Acidification Science Needs for Natural Resource Managers of the North American West Coast SO OCEANOGRAPHY LA English DT Article ID CALIFORNIA CURRENT SYSTEM; SEAWATER PH; CHEMISTRY; IMPACT; EUTROPHICATION; ADAPTATION; ORGANISMS; ECOSYSTEM; CO2 AB Natural circulation patterns along the west coast of North America periodically draw subthermocline, low pH waters into shallow coastal areas. The presence of corrosive, low pH waters, caused by ocean acidification (OA), is frequently observed along the North American west coast. Reduction of global atmospheric CO, inputs is the appropriate management focus for decreasing OA, but there are also many management decisions made at regional to local spatial scales that can lessen the exposure to or limit the effects of atmospheric CO,. Here, we describe these local management actions and identify the science needs that would assist local managers in deciding whether, and how best, to address local OA. Science needs are diverse, but three commonalities emerge. First, managers need a comprehensive monitoring program that expands understanding of spatial and temporal OA patterns and how OA changes influence marine ecosystems. Second, they require mechanistic, process-based models that differentiate natural from anthropogenically driven OA patterns and the extent to which local actions would affect OA conditions in context of what is largely a global atmospheric-driven phenomenon. Models present the opportunity to visualize outcomes with and without the changes in management actions included in model scenarios. Third, managers need models that identify which locales are most and least vulnerable to future changes due to OA. Understanding vulnerability will assist managers in better siting facilities (e.g., aquaria) or protecting marine resources. The required monitoring and modeling are all achievable, with much of the necessary research and development already underway. The challenge will be to ensure good and continuing communication between the management community that requires the information and the scientific community that is often hesitant to provide recommendations while uncertainty remains high. C1 [Boehm, Alexandria B.; Jacobson, Mark Z.] Stanford Univ, Environm & Water Studies Civil & Environm Engn, Stanford, CA 94305 USA. [O'Donnell, Michael J.; Whiteman, Elizabeth] Calif Ocean Sci Trust, Oakland, CA USA. [Sutula, Martha] Southern Calif Coastal Water Res Project, Dept Biochem, Costa Mesa, CA USA. [Wakefield, W. Waldo] NOAA, Fishery Resource Anal & Monitoring Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR USA. [Weisberg, Stephen B.] Southern Calif Coastal Water Res Project, Costa Mesa, CA USA. RP Boehm, AB (reprint author), Stanford Univ, Environm & Water Studies Civil & Environm Engn, Stanford, CA 94305 USA. EM aboehm@stanford.edu RI Weisberg, Stephen/B-2477-2008 OI Weisberg, Stephen/0000-0002-0655-9425 FU California Ocean Protection Council; California Ocean Science Trust; Institute of Natural Resources, Oregon FX This paper is a product of the West Coast Ocean Acidification and Hypoxia Science Panel. It was developed by a working group that included panel members and relevant external experts, and it has received input from the full panel. The Panel is convened by the California Ocean Science Trust and is supported by the California Ocean Protection Council, the California Ocean Science Trust, and the Institute of Natural Resources, Oregon. The authors acknowledge Meg Caldwell, who provided input to an early version of the manuscript. NR 49 TC 7 Z9 7 U1 3 U2 18 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD JUN PY 2015 VL 28 IS 2 SI SI BP 170 EP 181 DI 10.5670/oceanog.2015.40 PG 12 WC Oceanography SC Oceanography GA CL8NP UT WOS:000357231700018 ER PT J AU Gledhill, DK White, MM Salisbury, J Thomas, H Mlsna, I Liebman, M Mook, B Grear, J Candelmo, AC Chambers, RC Gobler, CJ Hunt, CW King, AL Price, NN Signorini, SR Standoff, E Stymiest, C Wahle, RA Waller, JD Rebuck, ND Wang, ZHA Capson, TL Morrison, JR Cooley, SR Doney, SC AF Gledhill, Dwight K. White, Meredith M. Salisbury, Joseph Thomas, Helmuth Mlsna, Ivy Liebman, Matthew Mook, Bill Grear, Jason Candelmo, Allison C. Chambers, R. Christopher Gobler, Christopher J. Hunt, Christopher W. King, Andrew L. Price, Nichole N. Signorini, Sergio R. Standoff, Esperanza Stymiest, Cassie Wahle, Richard A. Waller, Jesica D. Rebuck, Nathan D. Wang, Zhaohui A. Capson, Todd L. Morrison, J. Ruairidh Cooley, Sarah R. Doney, Scott C. TI Ocean and Coastal Acidification off New England and Nova Scotia SO OCEANOGRAPHY LA English DT Article ID ELEVATED CARBON-DIOXIDE; CALANUS-FINMARCHICUS GUNNERUS; COD GADUS-MORHUA; ARGOPECTEN-IRRADIANS; JUVENILE BIVALVES; SATURATION STATE; MARINE ORGANISMS; NORTH-ATLANTIC; CLIMATE-CHANGE; UNITED-STATES AB New England coastal and adjacent Nova Scotia shelf waters have a reduced buffering capacity because of significant freshwater input, making the regions waters potentially more vulnerable to coastal acidification. Nutrient loading and heavy precipitation events further acidify the regions poorly buffered coastal waters. Despite the apparent vulnerability of these waters, and fisheries and maricultures significant dependence on calcifying species, the community lacks the ability to confidently predict how the regions ecosystems will respond to continued ocean and coastal acidification. Here, we discuss ocean and coastal acidification processes specific to New England coastal and Nova Scotia shelf waters and review current understanding of the biological consequences most relevant to the region. We also identify key research and monitoring needs to be addressed and highlight existing capacities that should be leveraged to advance a regional understanding of ocean and coastal acidification. C1 [Gledhill, Dwight K.] NOAA, Ocean Acidificat Program, Silver Spring, MD 20910 USA. [White, Meredith M.; Price, Nichole N.; Waller, Jesica D.] Bigelow Lab Ocean Sci, East Boothbay, ME USA. [Salisbury, Joseph] Univ New Hampshire, Ocean Proc Anal Lab, Durham, NH 03824 USA. [Thomas, Helmuth] Dalhousie Univ, Dept Oceanog, Halifax, NS, Canada. [Mlsna, Ivy] US EPA, Off Water, Oak Ridge Inst Sci Educ, Boston, MA USA. [Liebman, Matthew] US EPA, Boston, MA USA. [Mook, Bill] Mook Seafarm Inc, Walpole, ME USA. [Grear, Jason] US EPA, Populat Ecol Branch, Narragansett, RI USA. [Candelmo, Allison C.] NOAA, Northeast Fisheries Sci Ctr NEFSC, Sandy Hook, NJ USA. [Chambers, R. Christopher] NOAA, NEFSC, Sandy Hook, NJ USA. [Gobler, Christopher J.] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA. [Hunt, Christopher W.] Univ New Hampshire, Nat Resources & Earth Syst Sci PhD Program, Durham, NH 03824 USA. [King, Andrew L.] Norwegian Inst Water Res, Oslo, Norway. [Signorini, Sergio R.] NASA, Sci Applicat Int Corp, Goddard Space Flight Ctr, Crofton, MD USA. [Standoff, Esperanza] Univ Maine Cooperat Extens & Sea Grant, Waldoboro, ME USA. [Stymiest, Cassie] Northeast Reg Assoc Coastal Ocean Observing Syst, Portsmouth, Hants, England. [Wahle, Richard A.] Univ Maine, Darling Marine Ctr, Sch Marine Sci, Walpole, ME 04573 USA. [Waller, Jesica D.] Univ Maine, Sch Marine Sci, Walpole, ME USA. [Rebuck, Nathan D.] NOAA, NEFSC, Narragansett, RI USA. [Wang, Zhaohui A.] Woods Hole Oceanog Inst, Dept Marine Chem & Geochem, Woods Hole, MA 02543 USA. [Capson, Todd L.] Sustainable Fisheries Partnership, Washington, DC USA. [Morrison, J. Ruairidh] NERACOOS, Portsmouth, NH USA. [Cooley, Sarah R.] Ocean Conservancy, Washington, DC USA. [Doney, Scott C.] WHOI, Marine Chem & Geochem, Woods Hole, MA USA. RP Gledhill, DK (reprint author), NOAA, Ocean Acidificat Program, Silver Spring, MD 20910 USA. EM dwight.gledhill@noaa.gov RI Doney, Scott/F-9247-2010; OI Doney, Scott/0000-0002-3683-2437; White, Meredith/0000-0001-8113-9618; Hunt, Christopher/0000-0001-8061-4560 FU National Oceanic and Atmospheric Administration (NOAA) US Integrated Ocean Observing System (IOOS) Award [NA11NOS0120034]; Internship/Research Participation Program at the Office of Water, US Environmental Protection Agency (EPA); NASA [NNX14AL84G NASA-CCS] FX NECAN thanks the presenters of the NECAN webinar series and participants at the state-of-science workshop for thoughtful insights. For a complete listing of participants and contributors, please consult the NECAN website (http://www.neracoos.org/necan). NECAN is coordinated in part by NERACOOS (http://www.neracoos.org), with funding from the National Oceanic and Atmospheric Administration (NOAA) US Integrated Ocean Observing System (IOOS) Award #NA11NOS0120034. This project was supported in part by an appointment to the Internship/Research Participation Program at the Office of Water, US Environmental Protection Agency (EPA), administered by the Oak Ridge Institute for Science and Education through an interagency agreement between the US Department of Energy and the EPA. JS acknowledges support from NASA grant from NNX14AL84G NASA-CCS. The scientific results and conclusions, as well as any views or opinions expressed herein, are those of the authors and do not necessarily reflect the views of any of the federal agencies with which any of the contributing authors may be affiliated. NR 94 TC 5 Z9 5 U1 8 U2 50 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD JUN PY 2015 VL 28 IS 2 SI SI BP 182 EP 197 DI 10.5670/oceanog.2015.41 PG 16 WC Oceanography SC Oceanography GA CL8NP UT WOS:000357231700019 ER PT J AU Choi, CR Woo, MH Dokgo, K Choi, EJ Min, KW Hwang, J Park, YD Lee, DY AF Choi, C. -R. Woo, M. -H. Dokgo, K. Choi, E. -J. Min, K. -W. Hwang, J. Park, Y. -D. Lee, D. -Y. TI Pitch-angle diffusion of electrons through growing and propagating along a magnetic field electromagnetic wave in Earth's radiation belts SO PHYSICS OF PLASMAS LA English DT Article ID ION-CYCLOTRON WAVES; STOCHASTIC ACCELERATION; PARTICLE INTERACTIONS; GEOMAGNETIC STORMS; PRECIPITATION; SCATTERING; MAGNETOSPHERE; GROWTH AB The diffusion of electrons via a linearly polarized, growing electromagnetic (EM) wave propagating along a uniform magnetic field is investigated. The diffusion of electrons that interact with the growing EM wave is investigated through the autocorrelation function of the parallel electron acceleration in several tens of electron gyration timescales, which is a relatively short time compared with the bounce time of electrons between two mirror points in Earth's radiation belts. Furthermore, the pitch-angle diffusion coefficient is derived for the resonant and non-resonant electrons, and the effect of the wave growth on the electron diffusion is discussed. The results can be applied to other problems related to local acceleration or the heating of electrons in space plasmas, such as in the radiation belts. (C) 2015 AIP Publishing LLC. C1 [Choi, C. -R.; Dokgo, K.; Choi, E. -J.; Min, K. -W.] Korea Adv Inst Sci & Technol, Dept Phys, Daejeon 305701, South Korea. [Woo, M. -H.] Natl Fus Res Inst, Taejon 305333, South Korea. [Hwang, J.; Park, Y. -D.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Lee, D. -Y.] Chungbuk Natl Univ, Dept Astron & Space Sci, Cheongju 361763, South Korea. [Choi, E. -J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. RP Choi, CR (reprint author), Korea Adv Inst Sci & Technol, Dept Phys, Daejeon 305701, South Korea. EM crchoi@kaist.ac.kr RI Min, Kyoung Wook/C-1948-2011 FU Korea Astronomy and Space Science Institute (KASI) under an RD program [2013-1-600-01]; "Planetary system research for space exploration" project; KASI; National Research Foundation of Korea [2014M1A3A3A02034585] FX This research was supported by the Korea Astronomy and Space Science Institute (KASI) under an R&D program (Project No. 2013-1-600-01) supervised by the Ministry of Science, ICT and Future Planning (Korea). This work was also supported by "Planetary system research for space exploration," project and the basic research funding from KASI. C.-R. Choi acknowledges the support of the National Research Foundation of Korea through Grant No. 2014M1A3A3A02034585. NR 34 TC 1 Z9 1 U1 0 U2 4 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 JUN PY 2015 VL 22 IS 6 AR 062903 DI 10.1063/1.4923267 PG 6 WC Physics, Fluids & Plasmas SC Physics GA CM4XN UT WOS:000357689500052 ER PT J AU Yang, JS Barrila, J Roland, KL Kilbourne, J Ott, CM Forsyth, RJ Nickerson, CA AF Yang, Jiseon Barrila, Jennifer Roland, Kenneth L. Kilbourne, Jacquelyn Ott, C. Mark Forsyth, Rebecca J. Nickerson, Cheryl A. TI Characterization of the Invasive, Multidrug Resistant Non-typhoidal Salmonella Strain D23580 in a Murine Model of Infection SO PLOS NEGLECTED TROPICAL DISEASES LA English DT Article ID ENTERICA SEROVAR TYPHIMURIUM; NONTYPHOIDAL SALMONELLA; SEROTYPE ENTERITIDIS; ESCHERICHIA-COLI; ACID RESISTANCE; SIGMA-FACTOR; FLAGELLA; AFRICA; VIRULENCE; ADULTS AB A distinct pathovar of Salmonella enterica serovar Typhimurium, ST313, has emerged in sub-Saharan Africa as a major cause of fatal bacteremia in young children and HIV-infected adults. D23580, a multidrug resistant clinical isolate of ST313, was previously shown to have undergone genome reduction in a manner that resembles that of the more human-restricted pathogen, Salmonella enterica serovar Typhi. It has since been shown through tissue distribution studies that D23580 is able to establish an invasive infection in chickens. However, it remains unclear whether ST313 can cause lethal disease in a non-human host following a natural course of infection. Herein we report that D23580 causes lethal and invasive disease in a murine model of infection following peroral challenge. The LD50 of D23580 in female BALB/c mice was 4.7 x 10(5) CFU. Tissue distribution studies performed 3 and 5 days post-infection confirmed that D23580 was able to more rapidly colonize the spleen, mesenteric lymph nodes and gall bladder in mice when compared to the well-characterized S. Typhimurium strain SL1344. D23580 exhibited enhanced resistance to acid stress relative to SL1344, which may lend towards increased capability to survive passage through the gastrointestinal tract as well as during its intracellular lifecycle. Interestingly, D23580 also displayed higher swimming motility relative to SL1344, S. Typhi strain Ty2, and the ST313 strain A130. Biochemical tests revealed that D23580 shares many similar metabolic features with SL1344, with several notable differences in the Voges-Proskauer and catalase tests, as well alterations in melibiose, and inositol utilization. These results represent the first full duration infection study using an ST313 strain following the entire natural course of disease progression, and serve as a benchmark for ongoing and future studies into the pathogenesis of D23580. C1 [Yang, Jiseon; Barrila, Jennifer; Roland, Kenneth L.; Kilbourne, Jacquelyn; Forsyth, Rebecca J.; Nickerson, Cheryl A.] Arizona State Univ, Biodesign Inst, Ctr Infect Dis & Vaccinol, Tempe, AZ 85281 USA. [Ott, C. Mark] NASA, Lyndon B Johnson Space Ctr, Biomed Res & Environm Sci Div, Houston, TX 77058 USA. [Nickerson, Cheryl A.] Arizona State Univ, Sch Life Sci, Tempe, AZ USA. RP Yang, JS (reprint author), Arizona State Univ, Biodesign Inst, Ctr Infect Dis & Vaccinol, Tempe, AZ 85281 USA. EM Cheryl.Nickerson@asu.edu FU NASA [NNX09AH40G]; Graduate Student Facilities Award, School of Life Sciences, Arizona State University; NIH [R01 AI60557, R21 AI105479] FX This research was funded by NASA grant NNX09AH40G (CAN), Graduate Student Facilities Award, School of Life Sciences, Arizona State University (JY), NIH grants R01 AI60557 and R21 AI105479 (KLR). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 66 TC 8 Z9 8 U1 3 U2 9 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1935-2735 J9 PLOS NEGLECT TROP D JI Plos Neglect. Trop. Dis. PD JUN PY 2015 VL 9 IS 6 AR e0003839 DI 10.1371/journal.pntd.0003839 PG 17 WC Infectious Diseases; Parasitology; Tropical Medicine SC Infectious Diseases; Parasitology; Tropical Medicine GA CM0VX UT WOS:000357398100041 PM 26091096 ER PT J AU Acero, F Ackermann, M Ajello, M Albert, A Atwood, WB Axelsson, M Baldini, L Ballet, J Barbiellini, G Bastieri, D Belfiore, A Bellazzini, R Bissaldi, E Blandford, RD Bloom, ED Bogart, JR Bonino, R Bottacini, E Bregeon, J Britto, RJ Bruel, P Buehler, R Burnett, TH Buson, S Caliandro, GA Cameron, RA Caputo, R Caragiulo, M Caraveo, PA Casandjian, JM Cavazzuti, E Charles, E Chaves, RCG Chekhtman, A Cheung, CC Chiang, J Chiaro, G Ciprini, S Claus, R Cohen-Tanugi, J Cominsky, LR Conrad, J Cutini, S D'Ammando, F de Angelis, A DeKlotz, M de Palma, F Desiante, R Digel, SW Di Venere, L Drell, PS Dubois, R Dumora, D Favuzzi, C Fegan, SJ Ferrara, EC Finke, J Franckowiak, A Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Giebels, B Giglietto, N Giommi, P Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grondin, MH Grove, JE Guillemot, L Guiriec, S Hadasch, D Harding, AK Hays, E Hewitt, JW Hill, AB Horan, D Iafrate, G Jogler, T Johannesson, G Johnson, RP Johnson, AS Johnson, TJ Johnson, WN Kamae, T Kataoka, J Katsuta, J Kuss, M La Mura, G Landriu, D Larsson, S Latronico, L Lemoine-Goumard, M Li, J Li, L Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Madejski, GM Massaro, F Mayer, M Mazziotta, MN McEnery, JE Michelson, PF Mirabal, N Mizuno, T Moiseev, AA Mongelli, M Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nuss, E Ohno, M Ohsugi, T Omodei, N Orienti, M Orlando, E Ormes, JF Paneque, D Panetta, JH Perkins, JS Pesce-Rollins, M Piron, F Pivato, G Porter, TA Racusin, JL Rando, R Razzano, M Razzaque, S Reimer, A Reimer, O Reposeur, T Rochester, LS Romani, RW Salvetti, D Sanchez-Conde, M Parkinson, PMS Schulz, A Siskind, EJ Smith, DA Spada, F Spandre, G Spinelli, P Stephens, TE Strong, AW Suson, DJ Takahashi, H Takahashi, T Tanaka, Y Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tibolla, O Torres, DF Torresi, E Tosti, G Troja, E Van Klaveren, B Vianello, G Winer, BL Wood, KS Wood, M Zimmer, S AF Acero, F. Ackermann, M. Ajello, M. Albert, A. Atwood, W. B. Axelsson, M. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Belfiore, A. Bellazzini, R. Bissaldi, E. Blandford, R. D. Bloom, E. D. Bogart, J. R. Bonino, R. Bottacini, E. Bregeon, J. Britto, R. J. Bruel, P. Buehler, R. Burnett, T. H. Buson, S. Caliandro, G. A. Cameron, R. A. Caputo, R. Caragiulo, M. Caraveo, P. A. Casandjian, J. M. Cavazzuti, E. Charles, E. Chaves, R. C. G. Chekhtman, A. Cheung, C. C. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. Cohen-Tanugi, J. Cominsky, L. R. Conrad, J. Cutini, S. D'Ammando, F. de Angelis, A. DeKlotz, M. de Palma, F. Desiante, R. Digel, S. W. Di Venere, L. Drell, P. S. Dubois, R. Dumora, D. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Finke, J. Franckowiak, A. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Giebels, B. Giglietto, N. Giommi, P. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grondin, M. -H. Grove, J. E. Guillemot, L. Guiriec, S. Hadasch, D. Harding, A. K. Hays, E. Hewitt, J. W. Hill, A. B. Horan, D. Iafrate, G. Jogler, T. Johannesson, G. Johnson, R. P. Johnson, A. S. Johnson, T. J. Johnson, W. N. Kamae, T. Kataoka, J. Katsuta, J. Kuss, M. La Mura, G. Landriu, D. Larsson, S. Latronico, L. Lemoine-Goumard, M. Li, J. Li, L. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Madejski, G. M. Massaro, F. Mayer, M. Mazziotta, M. N. McEnery, J. E. Michelson, P. F. Mirabal, N. Mizuno, T. Moiseev, A. A. Mongelli, M. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nuss, E. Ohno, M. Ohsugi, T. Omodei, N. Orienti, M. Orlando, E. Ormes, J. F. Paneque, D. Panetta, J. H. Perkins, J. S. Pesce-Rollins, M. Piron, F. Pivato, G. Porter, T. A. Racusin, J. L. Rando, R. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Reposeur, T. Rochester, L. S. Romani, R. W. Salvetti, D. Sanchez-Conde, M. Parkinson, P. M. Saz Schulz, A. Siskind, E. J. Smith, D. A. Spada, F. Spandre, G. Spinelli, P. Stephens, T. E. Strong, A. W. Suson, D. J. Takahashi, H. Takahashi, T. Tanaka, Y. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tibolla, O. Torres, D. F. Torresi, E. Tosti, G. Troja, E. Van Klaveren, B. Vianello, G. Winer, B. L. Wood, K. S. Wood, M. Zimmer, S. TI FERMI LARGE AREA TELESCOPE THIRD SOURCE CATALOG SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; gamma-rays: general ID GAMMA-RAY EMISSION; PULSAR WIND NEBULA; ALL-SKY SURVEY; ACTIVE GALACTIC NUCLEI; PSR B1259-63/LS 2883; SUPERNOVA REMNANT; RADIO-SOURCES; UNASSOCIATED SOURCES; GLOBULAR-CLUSTERS; WMAP OBSERVATIONS AB We present the third Fermi Large Area Telescope (LAT) source catalog (3FGL) of sources in the 100 MeV-300 GeV range. Based on the first 4 yr of science data from the Fermi Gamma-ray Space Telescope mission, it is the deepest yet in this energy range. Relative to the Second Fermi LAT catalog, the 3FGL catalog incorporates twice as much data, as well as a number of analysis improvements, including improved calibrations at the event reconstruction level, an updated model for Galactic diffuse.-ray emission, a refined procedure for source detection, and improved methods for associating LAT sources with potential counterparts at other wavelengths. The 3FGL catalog includes 3033 sources above 4 sigma significance, with source location regions, spectral properties, and monthly light curves for each. Of these, 78 are flagged as potentially being due to imperfections in the model for Galactic diffuse emission. Twenty-five sources are modeled explicitly as spatially extended, and overall 238 sources are considered as identified based on angular extent or correlated variability (periodic or otherwise) observed at other wavelengths. For 1010 sources we have not found plausible counterparts at other wavelengths. More than 1100 of the identified or associated sources are active galaxies of the blazar class; several other classes of non-blazar active galaxies are also represented in the 3FGL. Pulsars represent the largest Galactic source class. From source counts of Galactic sources we estimate that the contribution of unresolved sources to the Galactic diffuse emission is similar to 3% at 1 GeV. C1 [Acero, F.; Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Landriu, D.] CEA IRFU CNRS Univ Paris Diderot, Lab AIM, CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Clemson Univ, Kinard Lab Phys, Dept Phys & Astron, Clemson, SC 29634 USA. [Albert, A.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Dubois, R.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Kamae, T.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Van Klaveren, B.; Vianello, G.; Wood, M.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Albert, A.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Dubois, R.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Kamae, T.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Van Klaveren, B.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Atwood, W. B.; Caputo, R.; Johnson, R. P.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Atwood, W. B.; Caputo, R.; Johnson, R. P.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Axelsson, M.; Conrad, J.; Larsson, S.; Sanchez-Conde, M.; Zimmer, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Axelsson, M.; Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Axelsson, M.; Conrad, J.; Larsson, S.; Li, L.; Sanchez-Conde, M.; Zimmer, S.] Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Baldini, L.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.; Bellazzini, R.; Kuss, M.; Pesce-Rollins, M.; Pivato, G.; Razzano, M.; Spada, F.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Barbiellini, G.; Desiante, R.; Iafrate, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Chiaro, G.; La Mura, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Belfiore, A.; Caraveo, P. A.; Salvetti, D.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Bissaldi, E.; Caragiulo, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Mongelli, M.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bonino, R.; Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Bonino, R.] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy. [Bregeon, J.; Chaves, R. C. G.; Cohen-Tanugi, J.; Nuss, E.; Piron, F.] Univ Montpellier, Lab Univers & Particules Montpellier, CNRS IN2P3, F-34059 Montpellier, France. [Britto, R. J.; Razzaque, S.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa. [Bruel, P.; Fegan, S. J.; Giebels, B.; Horan, D.] Ecole Polytech, CNRS IN2P3, Lab Leprince Ringuet, Palaiseau, France. [Burnett, T. H.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Caliandro, G. A.] CIFS, I-10133 Turin, Italy. [Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.; Giommi, P.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00133 Rome, Italy. [Chekhtman, A.; Johnson, T. J.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Cheung, C. C.; Finke, J.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Ciprini, S.; Cutini, S.; Gasparrini, D.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Ciprini, S.; Cutini, S.; Gasparrini, D.] INAF Osservatorio Astron Roma, I-00040 Rome, Italy. [Cominsky, L. R.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA. [Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden. [D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.] Ist Nazl Fis Nucl, Grp Collegato Udine, Sez Trieste, I-33100 Udine, Italy. [DeKlotz, M.] Stellar Solut Inc, Palo Alto, CA 94306 USA. [de Palma, F.] Univ Telemat Pegaso, I-80132 Naples, Italy. [Desiante, R.] Univ Udine, I-33100 Udine, Italy. [Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Dumora, D.; Grondin, M. -H.; Lemoine-Goumard, M.; Lott, B.; Reposeur, T.; Smith, D. A.] Univ Bordeaux 1, IN2P3 CNRS, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Ferrara, E. C.; Guiriec, S.; Harding, A. K.; Hays, E.; Hewitt, J. W.; McEnery, J. E.; Mirabal, N.; Moiseev, A. A.; Perkins, J. S.; Racusin, J. L.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fukazawa, Y.; Katsuta, J.; Ohno, M.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Guillemot, L.] Univ Orleans CNRS, Lab Phys & Chim Environm & Espace, F-45071 Orleans 02, France. Observ Paris, CNRS INSU, Stn Radioastron Nancay, F-18330 Nancay, France. [Hadasch, D.; La Mura, G.; Reimer, A.; Reimer, O.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Hadasch, D.; La Mura, G.; Reimer, A.; Reimer, O.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Hewitt, J. W.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Hewitt, J. W.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Hewitt, J. W.; Moiseev, A. A.] CRESST, Greenbelt, MD 20771 USA. [Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Iafrate, G.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Li, J.; Torres, D. F.] Inst Space Sci IEEC CSIC, E-08193 Barcelona, Spain. [Li, L.] KTH Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Massaro, F.] Yale Univ, Dept Astron, Dept Phys, New Haven, CT 06520 USA. [Massaro, F.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [McEnery, J. E.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mizuno, T.; Ohsugi, T.; Tanaka, Y.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Murgia, S.] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Parkinson, P. M. Saz] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Stephens, T. E.] Brigham Young Univ, Harold B Lee Lib, Provo, UT 84602 USA. [Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Takahashi, T.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan. [Tibolla, O.] Univ Autonoma Chiapas UNACH, MCTP, Tuxtla Gutierrez 29050, Chiapas, Mexico. [Torres, D. F.] ICREA, Barcelona, Spain. [Torresi, E.] INAF IASF Bologna, I-40129 Bologna, Italy. [Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. RP Acero, F (reprint author), CEA IRFU CNRS Univ Paris Diderot, Lab AIM, CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. EM jean.ballet@cea.fr; tburnett@u.washington.edu; elisabetta.cavazzuti@asdc.asi.it; digel@stanford.edu RI Di Venere, Leonardo/C-7619-2017; Bissaldi, Elisabetta/K-7911-2016; Massaro, Francesco/L-9102-2016; Morselli, Aldo/G-6769-2011; Reimer, Olaf/A-3117-2013; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Funk, Stefan/B-7629-2015; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Bonino, Raffaella/S-2367-2016 OI Giroletti, Marcello/0000-0002-8657-8852; Baldini, Luca/0000-0002-9785-7726; TORRESI, ELEONORA/0000-0002-5201-010X; Di Venere, Leonardo/0000-0003-0703-824X; Stephens, Thomas/0000-0003-3065-6871; Iafrate, Giulia/0000-0002-6185-8292; Giordano, Francesco/0000-0002-8651-2394; giommi, paolo/0000-0002-2265-5003; Bonino, Raffaella/0000-0002-4264-1215; Caraveo, Patrizia/0000-0003-2478-8018; Hill, Adam/0000-0003-3470-4834; Bastieri, Denis/0000-0002-6954-8862; Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094; Axelsson, Magnus/0000-0003-4378-8785; Bissaldi, Elisabetta/0000-0001-9935-8106; Massaro, Francesco/0000-0002-1704-9850; Morselli, Aldo/0000-0002-7704-9553; Reimer, Olaf/0000-0001-6953-1385; Torres, Diego/0000-0002-1522-9065; Funk, Stefan/0000-0002-2012-0080; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; FU National Aeronautics and Space Administration FX This work made extensive use of the ATNF pulsar catalog98 (Manchester et al. 2005). This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration, and of archival data, software, and online services provided by the ASI Science Data Center (ASDC), operated by the Italian Space Agency. NR 116 TC 257 Z9 258 U1 20 U2 34 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 JUN PY 2015 VL 218 IS 2 AR 23 DI 10.1088/0067-0049/218/2/23 PG 41 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7AO UT WOS:000357122200009 ER PT J AU Daly, AM Bermudez, C Kolesnikova, L Alonso, JL AF Daly, A. M. Bermudez, C. Kolesnikova, L. Alonso, J. L. TI COMPREHENSIVE ANALYSIS OF PREBIOTIC PROPENAL UP TO 660 GHz SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; ISM: molecules; molecular data; techniques: spectroscopic ID S-TRANS-ACROLEIN; VIBRATIONALLY EXCITED-STATES; MICROWAVE-SPECTRUM; LABORATORY CHARACTERIZATION; ASTROPHYSICAL DETECTION; INTERSTELLAR-MOLECULES; GALACTIC-CENTER; DIPOLE-MOMENT; WAVE SPECTRUM; CIS-ACROLEIN AB Since interstellar detection of propenal is only based on two rotational transitions in the centimeter wave region, its high resolution rotational spectrum has been measured up to 660 GHz and fully characterized by assignment of more than 12,000 transitions to provide direct laboratory data to the astronomical community. Spectral assignments and analysis include transitions from the ground state of the trans and cis isomers, three trans-C-13 isotopologues, and ten excited vibrational states of the trans form. Combining new millimeter and submillimeter data with those from the far-infrared region has yielded the most precise set of spectroscopic constants of trans-propenal obtained to date. Newly determined rotational constants, centrifugal distortion constants, vibrational energies, and Coriolis and Fermi interaction constants are given with high accuracy and were used to predict transition frequencies and intensities over a wide frequency range. Results of this work should facilitate astronomers further observation of propenal in the interstellar medium. C1 [Daly, A. M.; Bermudez, C.; Kolesnikova, L.; Alonso, J. L.] Univ Valladolid, Unidad Asociada CSIC, Labs Espectroscopia & Bioespectroscopia, Area Quim Fis,GEM, E-47011 Valladolid, Spain. [Daly, A. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Daly, AM (reprint author), Univ Valladolid, Unidad Asociada CSIC, Labs Espectroscopia & Bioespectroscopia, Area Quim Fis,GEM, Edificio Quifima,Parque Cient UVa, E-47011 Valladolid, Spain. EM Adam.M.Daly@jpl.nasa.gov FU Ministerio de Ciencia e Innovacion [CTQ 2013-40717 P, CTQ 2010-19008, CSD 2009-00038]; Junta de Castilla y Leon [VA070A08, VA175U13]; Minisiterio de Ciencia e Innovacion [BES 2011-047695] FX This research has been supported by the "Ministerio de Ciencia e Innovacion" (grant numbers CTQ 2013-40717 P, CTQ 2010-19008 and CONSOLIDER-Ingenio program "ASTROMOL," CSD 2009-00038) and Junta de Castilla y Leon (Grants VA070A08 and VA175U13). C.B. wishes to thank the Minisiterio de Ciencia e Innovacion for an FPI grant (BES 2011-047695). NR 35 TC 4 Z9 4 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2015 VL 218 IS 2 AR 30 DI 10.1088/0067-0049/218/2/30 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7AO UT WOS:000357122200016 ER PT J AU Kriek, M Shapley, AE Reddy, NA Siana, B Coil, AL Mobasher, B Freeman, WR de Groot, L Price, SH Sanders, R Shivaei, I Brammer, GB Momcheva, IG Skelton, RE van Dokkum, PG Whitaker, KE Aird, J Azadi, M Kassis, M Bullock, JS Conroy, C Dave, R Keres, D Krumholz, M AF Kriek, Mariska Shapley, Alice E. Reddy, Naveen A. Siana, Brian Coil, Alison L. Mobasher, Bahram Freeman, William R. de Groot, Laura Price, Sedona H. Sanders, Ryan Shivaei, Irene Brammer, Gabriel B. Momcheva, Ivelina G. Skelton, Rosalind E. van Dokkum, Pieter G. Whitaker, Katherine E. Aird, James Azadi, Mojegan Kassis, Marc Bullock, James S. Conroy, Charlie Dave, Romeel Keres, Dusan Krumholz, Mark TI THE MOSFIRE DEEP EVOLUTION FIELD (MOSDEF) SURVEY: REST-FRAME OPTICAL SPECTROSCOPY FOR similar to 1500 H-SELECTED GALAXIES AT 1.37 <= z <= 3.8 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: distances and redshifts; galaxies: evolution; galaxies: formation; galaxies: high-redshift; surveys ID STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; ACTIVE GALACTIC NUCLEI; EXTRAGALACTIC LEGACY SURVEY; MASS-METALLICITY RELATION; POST-STARBURST GALAXIES; HUBBLE-SPACE-TELESCOPE; DIGITAL SKY SURVEY; MEDIUM-BAND SURVEY; QUIESCENT GALAXIES AB In this paper we present the MOSFIRE Deep Evolution Field (MOSDEF) survey. The MOSDEF survey aims to obtain moderate-resolution (R = 3000-3650) rest-frame optical spectra (similar to 3700-7000 angstrom) for similar to 1500 galaxies at 1.37 <= z <= 3.80 in three well-studied CANDELS fields: AEGIS, COSMOS, and GOODS-N. Targets are selected in three redshift intervals: 1.37 <= z <= 1.70, 2.09 <= z <= 2.61, and 2.95 <= z <= 3.80, down to fixed H-AB (F160W) magnitudes of 24.0, 24.5, and 25.0, respectively, using the photometric and spectroscopic catalogs from the 3D-HST survey. We target both strong nebular emission lines (e.g., [O II] lambda lambda 3727, 3730, H beta, [O III] lambda lambda 4960, 5008, Ha, [N II] lambda lambda 6550, 6585, and [S II] lambda lambda 6718, 6733) and stellar continuum and absorption features (e.g., Balmer lines, Ca-II H and K, Mgb, 4000 angstrom break). Here we present an overview of our survey, the observational strategy, the data reduction and analysis, and the sample characteristics based on spectra obtained during the first 24 nights. To date, we have completed 21 masks, obtaining spectra for 591 galaxies. For similar to 80% of the targets we derive a robust redshift from either emission or absorption lines. In addition, we confirm 55 additional galaxies, which were serendipitously detected. The MOSDEF galaxy sample includes unobscured star-forming, dusty star-forming, and quiescent galaxies and spans a wide range in stellar mass (similar to 10(9)-10(11.5) M-circle dot) and star formation rate (similar to 10(0)-10(3) M-circle dot yr(-1)). The spectroscopically confirmed sample is roughly representative of an H-band limited galaxy sample at these redshifts. With its large sample size, broad diversity in galaxy properties, and wealth of available ancillary data, MOSDEF will transform our understanding of the stellar, gaseous, metal, dust, and black hole content of galaxies during the time when the universe was most active. C1 [Kriek, Mariska; Price, Sedona H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Shapley, Alice E.; Sanders, Ryan] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Reddy, Naveen A.; Siana, Brian; Mobasher, Bahram; Freeman, William R.; de Groot, Laura; Shivaei, Irene] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Coil, Alison L.; Keres, Dusan] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Brammer, Gabriel B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Momcheva, Ivelina G.; van Dokkum, Pieter G.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Skelton, Rosalind E.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa. [Whitaker, Katherine E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Aird, James] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Kassis, Marc] WM Keck Observ, Kamuela, HI 96743 USA. [Bullock, James S.] Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA. [Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Conroy, Charlie; Krumholz, Mark] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Dave, Romeel] Univ Western Cape, ZA-7535 Cape Town, South Africa. RP Kriek, M (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. RI Bullock, James/K-1928-2015; Skelton, Rosalind/S-1845-2016 OI Bullock, James/0000-0003-4298-5082; Skelton, Rosalind/0000-0001-7393-3336 FU NSF AAG [AST-1312780, 1312547, 1312764, 1313171]; NASA through the Space Telescope Science Institute [AR-13907]; Committee Faculty Research Grant; Hellmann Fellowship; Alfred P. Sloan Research Fellowship; NSF CAREER [AST-1055081]; W.M. Keck Foundation; NASA/ESA Hubble Space Telescope [12177, 12328, 12060-12064, 12440-12445, 13056]; NASA [NAS 5-26555] FX We thank the MOSFIRE instrument team for building this powerful instrument and for taking data for us during their commissioning runs. M. Kriek acknowledges valuable discussions with N. Konidaris about the reduction of MOSFIRE data and with M. Franx regarding the noise properties of the data. We thank the referee for a constructive report. This work would not have been possible without the 3D-HST collaboration, who provided to us the spectroscopic and photometric catalogs used to select our targets and to derive stellar population parameters. We are grateful to I. McLean, K. Kulas, and G. Mace for taking observations for us in 2013 May and June. We acknowledge support from an NSF AAG collaborative grant AST-1312780, 1312547, 1312764, and 1313171, and archival grant AR-13907, provided by NASA through a grant from the Space Telescope Science Institute. M. Kriek acknowledges support from a Committee Faculty Research Grant and a Hellmann Fellowship. N.A.R. is supported by an Alfred P. Sloan Research Fellowship. A.L.C. acknowledges funding from NSF CAREER grant AST-1055081. The data presented in this paper 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 on observations made with the NASA/ESA Hubble Space Telescope (programs 12177, 12328, 12060-12064, 12440-12445, 13056), which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. NR 97 TC 45 Z9 45 U1 1 U2 4 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 JUN PY 2015 VL 218 IS 2 AR 15 DI 10.1088/00647-0049/218/2/15 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7AO UT WOS:000357122200001 ER PT J AU Tyler, RH Henning, WG Hamilton, CW AF Tyler, Robert H. Henning, Wade G. Hamilton, Christopher W. TI TIDAL HEATING IN A MAGMA OCEAN WITHIN JUPITER'S MOON Io SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE planets and satellites: dynamical evolution and stability; planets and satellites: general; planets and satellites: interiors ID PLANET-PLANET SCATTERING; TERRESTRIAL EXOPLANETS; VISCOELASTIC MODELS; GIANT PLANETS; CONVECTION; EARTH; FLOW; DISSIPATION; EVOLUTION; GALILEO AB Active volcanism observed on Io is thought to be driven by the temporally periodic, spatially differential projection of Jupiter's gravitational field over the moon. Previous theoretical estimates of the tidal heat have all treated Io as essentially a solid, with fluids addressed only through adjustment of rheological parameters rather than through appropriate extension of the dynamics. These previous estimates of the tidal response and associated heat generation on Io are therefore incomplete and possibly erroneous because dynamical aspects of the fluid behavior are not permitted in the modeling approach. Here we address this by modeling the partial-melt asthenosphere as a global layer of fluid governed by the Laplace Tidal Equations. Solutions for the tidal response are then compared with solutions obtained following the traditional solid-material approach. It is found that the tidal heat in the solid can match that of the average observed heat flux (nominally 2.25 W m(-2)), though only over a very restricted range of plausible parameters, and that the distribution of the solid tidal heat flux cannot readily explain a longitudinal shift in the observed (inferred) low-latitude heat fluxes. The tidal heat in the fluid reaches that observed over a wider range of plausible parameters, and can also readily provide the longitudinal offset. Finally, expected feedbacks and coupling between the solid/fluid tides are discussed. Most broadly, the results suggest that both solid and fluid tidal-response estimates must be considered in exoplanet studies, particularly where orbital migration under tidal dissipation is addressed. C1 [Tyler, Robert H.; Henning, Wade G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Tyler, Robert H.; Henning, Wade G.] NASA Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Hamilton, Christopher W.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Tyler, RH (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM robert.h.tyler@nasa.gov FU NASA [NNX13AG01G, NNX11AM38G]; NASA; OPR Program [NNX14AR42G] FX The authors thank Bill Moore for helpful discussions, as well as access to and training in the use of the TideLab suite of code. R.H.T. acknowledges support by NASA Outer Planets Research (OPR) Program (through awards NNX13AG01G, NNX11AM38G). W.G.H. and C.W.H. acknowledge support of the NASA Post-doctoral Fellowship Program. All authors acknowledge a new award from the OPR Program (NNX14AR42G) specifically directed at the topic of this paper. NR 59 TC 3 Z9 3 U1 2 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2015 VL 218 IS 2 AR 22 DI 10.1088/0067-0049/218/2/22 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7AO UT WOS:000357122200008 ER PT J AU Bi, J Knyazikhin, Y Choi, SH Park, T Barichivich, J Ciais, P Fu, R Ganguly, S Hall, F Hilker, T Huete, A Jones, M Kimball, J Lyapustin, AI Mottus, M Nemani, RR Piao, SL Poulter, B Saleska, SR Saatchi, SS Xu, L Zhou, LM Myneni, RB AF Bi, Jian Knyazikhin, Yuri Choi, Sungho Park, Taejin Barichivich, Jonathan Ciais, Philippe Fu, Rong Ganguly, Sangram Hall, Forrest Hilker, Thomas Huete, Alfredo Jones, Matthew Kimball, John Lyapustin, Alexei I. Mottus, Matti Nemani, Ramakrishna R. Piao, Shilong Poulter, Benjamin Saleska, Scott R. Saatchi, Sassan S. Xu, Liang Zhou, Liming Myneni, Ranga B. TI Sunlight mediated seasonality in canopy structure and photosynthetic activity of Amazonian rainforests SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE Amazonian rainforests; seasonality; remote sensing; MISR; MODIS ID LEAF-AREA INDEX; TROPICAL FOREST; DRY SEASON; MODIS; CARBON; PRODUCTIVITY; VARIABILITY; SENSITIVITY; ALGORITHM; PHENOLOGY AB Resolving the debate surrounding the nature and controls of seasonal variation in the structure and metabolism of Amazonian rainforests is critical to understanding their response to climate change. In situ studies have observed higher photosynthetic and evapotranspiration rates, increased litterfall and leaf flushing during the Sunlight-rich dry season. Satellite data also indicated higher greenness level, a proven surrogate of photosynthetic carbon fixation, and leaf area during the dry season relative to the wet season. Some recent reports suggest that rainforests display no seasonal variations and the previous results were satellite measurement artefacts. Therefore, here we re-examine several years of data from three sensors on two satellites under a range of sun positions and satellite measurement geometries and document robust evidence for a seasonal cycle in structure and greenness of wet equatorial Amazonian rainforests. This seasonal cycle is concordant with independent observations of solar radiation. Weattribute alternative conclusions to an incomplete study of the seasonal cycle, i. e. the dry season only, and to prognostications based on a biased radiative transfer model. Consequently, evidence of dry season greening in geometry corrected satellite data was ignored and the absence of evidence for seasonal variation in lidar data due to noisy and saturated signals was misinterpreted as evidence of the absence of changes during the dry season. Our results, grounded in the physics of radiative transfer, buttress previous reports of dry season increases in leaf flushing, litterfall, photosynthesis and evapotranspiration in well-hydrated Amazonian rainforests. C1 [Bi, Jian; Knyazikhin, Yuri; Choi, Sungho; Park, Taejin; Myneni, Ranga B.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA. [Barichivich, Jonathan] Univ E Anglia, Sch Environm Sci, Climat Res Unit, Norwich NR4 7TJ, Norfolk, England. [Ciais, Philippe] UVSQ, CEA, CNRS, IPSL,LSCE, F-91191 Gif Sur Yvette, France. [Fu, Rong] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA. [Ganguly, Sangram] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hall, Forrest] NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hilker, Thomas] Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA. [Huete, Alfredo] Univ Technol Sydney, Plant Funct Biol & Climate Change Cluster, Sydney, NSW 2007, Australia. [Jones, Matthew; Kimball, John] Univ Montana, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA. [Lyapustin, Alexei I.] NASA, Climate & Radiat Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mottus, Matti] Univ Helsinki, Dept Geosci & Geog, FI-00014 Helsinki, Finland. [Nemani, Ramakrishna R.] NASA, Adv Supercomp Div, Ames Res Ctr, Moffett Field, CA 94035 USA. [Piao, Shilong] Peking Univ, Dept Ecol, Beijing 100871, Peoples R China. [Piao, Shilong] Chinese Acad Sci, Inst Tibetan Plateau Res, Beijing 100085, Peoples R China. [Poulter, Benjamin] Montana State Univ, Dept Ecol, Bozeman, MT 59717 USA. [Saleska, Scott R.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. [Saatchi, Sassan S.; Xu, Liang] Univ Calif Los Angeles, Inst Environm & Sustainabil, Los Angeles, CA 90095 USA. [Saatchi, Sassan S.] CALTECH, Jet Prop Lab, Radar Sci & Engn Sect, Pasadena, CA 91109 USA. [Zhou, Liming] SUNY Albany, Dept Atmospher & Environm Sci, Albany, NY 12222 USA. RP Bi, J (reprint author), Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA. EM jknjazi@bu.edu RI Myneni, Ranga/F-5129-2012; Mottus, Matti/A-4130-2009; Huete, Alfredo/C-1294-2008; Zhou, Liming/A-2688-2012; OI Mottus, Matti/0000-0002-2745-1966; Huete, Alfredo/0000-0003-2809-2376; Poulter, Benjamin/0000-0002-9493-8600 FU NASA Earth Science Division FX This study was supported by NASA Earth Science Division. NR 36 TC 11 Z9 11 U1 4 U2 55 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 JUN PY 2015 VL 10 IS 6 AR 064014 DI 10.1088/1748-9326/10/6/064014 PG 6 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA CL3FK UT WOS:000356835600016 ER PT J AU Doyle, PM Jogo, K Nagashima, K Krot, AN Wakita, S Ciesla, FJ Hutcheon, ID AF Doyle, Patricia M. Jogo, Kaori Nagashima, Kazuhide Krot, Alexander N. Wakita, Shigeru Ciesla, Fred J. Hutcheon, Ian D. TI Early aqueous activity on the ordinary and carbonaceous chondrite parent bodies recorded by fayalite SO NATURE COMMUNICATIONS LA English DT Article ID EARLY SOLAR-SYSTEM; OXYGEN-ISOTOPE FRACTIONATION; PROTOPLANETARY DISK; RATIO ESTIMATION; ORGANIC-MATTER; ASTEROID BELT; CHRONOLOGY; CHONDRULES; EVOLUTION; ALLENDE AB Chronology of aqueous activity on chondrite parent bodies constrains their accretion times and thermal histories. Radiometric Mn-53-Cr-53 dating has been successfully applied to aqueously formed carbonates in CM carbonaceous chondrites. Owing to the absence of carbonates in ordinary (H, L and LL), and CV and CO carbonaceous chondrites, and the lack of proper standards, there are no reliable ages of aqueous activity on their parent bodies. Here we report the first Mn-53-Cr-53 ages of aqueously formed fayalite in the L3 chondrite Elephant Moraine 90161 as 2.4(-1.3)(+1.8) Myr after calcium-aluminium-rich inclusions (CAIs), the oldest Solar System solids. In addition, measurements using our synthesized fayalite standard show that fayalite in the CV3 chondrite Asuka 881317 and CO3-like chondrite MacAlpine Hills 88107 formed 4.2(-0.7)(+0.8) and 5.1(-0.4)(+0.5) Myr after CAIs, respectively. Thermal modelling, combined with the inferred conditions (temperature and water/rock ratio) and Mn-53-Cr-53 ages of aqueous alteration, suggests accretion of the L, CV and CO parent bodies similar to 1.8 - 2.5 Myr after CAIs. C1 [Doyle, Patricia M.; Jogo, Kaori; Nagashima, Kazuhide; Krot, Alexander N.] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Doyle, Patricia M.; Jogo, Kaori; Krot, Alexander N.] Univ Hawaii, NASA Astrobiol Inst, Honolulu, HI 96822 USA. [Wakita, Shigeru] Natl Astron Observ Japan, Ctr Computat Astrophys, Mitaka, Tokyo 1818588, Japan. [Ciesla, Fred J.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Hutcheon, Ian D.] Lawrence Livermore Natl Lab, Glenn Seaborg Inst, Livermore, CA 94551 USA. RP Doyle, PM (reprint author), Univ Cape Town, Dept Geol Sci, ZA-7701 Rondebosch, South Africa. EM pdoyle@higp.hawaii.edu; sasha@higp.hawaii.edu OI Wakita, Shigeru/0000-0002-3161-3454 NR 66 TC 12 Z9 12 U1 5 U2 20 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD JUN PY 2015 VL 6 AR 7444 DI 10.1038/ncomms8444 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CL7UH UT WOS:000357176700010 PM 26100451 ER PT J AU Sun, T Socki, RA Bish, DL Harvey, RP Bao, HM Niles, PB Cavicchioli, R Tonui, E AF Sun, Tao Socki, Richard A. Bish, David L. Harvey, Ralph P. Bao, Huiming Niles, Paul B. Cavicchioli, Ricardo Tonui, Eric TI Lost cold Antarctic deserts inferred from unusual sulfate formation and isotope signatures SO NATURE COMMUNICATIONS LA English DT Article ID ICE-SHEET; TRANSANTARCTIC MOUNTAINS; ATMOSPHERIC SULFATES; SULFUR ISOTOPES; VICTORIA LAND; DRY VALLEYS; OXYGEN; REDUCTION; FRACTIONATION; BACTERIAL AB The Antarctic ice cap significantly affects global ocean circulation and climate. Continental glaciogenic sedimentary deposits provide direct physical evidence of the glacial history of the Antarctic interior, but these data are sparse. Here we investigate a new indicator of ice sheet evolution: sulfates within the glaciogenic deposits from the Lewis Cliff Ice Tongue of the central Transantarctic Mountains. The sulfates exhibit unique isotope signatures, including delta S-34 up to + 50% for mirabilite evaporites, Delta O-17 up to + 2.3% for dissolved sulfate within contemporary melt-water ponds, and extremely negative delta O-18 as low as -22.2%. The isotopic data imply that the sulfates formed under environmental conditions similar to today's McMurdo Dry Valleys, suggesting that ice-free cold deserts may have existed between the South Pole and the Transantarctic Mountains since the Miocene during periods when the ice sheet size was smaller than today, but with an overall similar to modern global hydrological cycle. C1 [Sun, Tao; Bao, Huiming] Louisiana State Univ, Baton Rouge, LA 70803 USA. [Sun, Tao; Niles, Paul B.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Socki, Richard A.] NASA, Johnson Space Ctr, ESCG, Houston, TX 77058 USA. [Bish, David L.] Indiana Univ, Indianapolis, IN 47405 USA. [Harvey, Ralph P.] Case Western Reserve Univ, Cleveland, OH 44106 USA. [Cavicchioli, Ricardo] Univ New S Wales, Sydney, NSW 2052, Australia. [Tonui, Eric] BP Amer, Upstream Technol, Houston, TX 77079 USA. RP Sun, T (reprint author), Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA. EM tsun9@central.uh.edu FU NASA's Mars Fundamental Research Program [NNF05GL75G]; National Science Foundation's Office of Polar Programs, Division of Infrastructure and Logistics; Economic Development Assistantship from Louisiana State Board of Regents; NASA Postdoctoral Fellowship; Australian Research Council; Australian Antarctic Science program FX We acknowledge funding from NASA's Mars Fundamental Research Program (grant #NNF05GL75G) to conduct this research. The National Science Foundation's Office of Polar Programs, Division of Infrastructure and Logistics provided outstanding field support. T.S. is supported by Economic Development Assistantship from Louisiana State Board of Regents and a NASA Postdoctoral Fellowship. The research performed by R.C. is supported by the Australian Research Council and the Australian Antarctic Science program. We also thank Michael Kaplan and Sarah Feakins for helpful discussions. NR 59 TC 1 Z9 1 U1 4 U2 15 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD JUN PY 2015 VL 6 AR 7579 DI 10.1038/ncomms8579 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CL7VX UT WOS:000357181300001 PM 26119082 ER PT J AU Du, XM Cao, DY Mishra, D Bernardes, S Jordan, TR Madden, M AF Du, Xiaomin Cao, Daiyong Mishra, Deepak Bernardes, Sergio Jordan, Thomas R. Madden, Marguerite TI Self-Adaptive Gradient-Based Thresholding Method for Coal Fire Detection Using ASTER Thermal Infrared Data, Part I: Methodology and Decadal Change Detection SO REMOTE SENSING LA English DT Article ID LAND-SURFACE-TEMPERATURE; JHARIA COALFIELD; SPONTANEOUS COMBUSTION; NORTHERN CHINA; TM DATA; EMISSIVITY; INDIA; WUDA; RADIOMETER; RESOLUTION AB Coal fires that are induced by natural spontaneous combustion or result from human activities occurring on the surface and in underground coal seams destroy coal resources and cause serious environmental degradation. Thermal infrared image data, which directly measure surface temperature, can be an important tool to map coal fires over large areas. As the first of two parts introducing our coal fire detection method, this paper proposes a self-adaptive threshold-based approach for coal fire detection using ASTER thermal infrared data: the self-adaptive gradient-based thresholding method (SAGBT). This method is based on an assumption that the attenuation of temperature along the coal fire's boundaries generates considerable numbers of spots with extremely high gradient values. The SAGBT method applied mathematical morphology thinning to skeletonize the potential high gradient buffers into the extremely high gradient lines, which provides a self-adaptive mechanism to generate thresholds according to the thermal spatial patterns of the images. The final threshold was defined as an average temperature value reading from the high temperature buffers (segmented by 1.0 sigma from the mean) and along a sequence of extremely high gradient lines (thinned from the potential high gradient buffers and segmented within the lower bounds, ranging from 0.5 sigma to 1.5 sigma and with an upper bound of 3.2 sigma, where sigma is the standard deviation), marking the coal fire areas. The SAGBT method used the basic outer boundary of the coal-bearing strata to simply exclude false alarms. The intermediate thresholds reduced the coupling with the temperature and converged by changing the potential high gradient buffers. This simple approach can be economical and accurate in identifying coal fire areas. In addition, it allows for the identification of thresholds using multiple ASTER TIR scenes in a consistent and uniform manner, and supports long-term coal fire change analyses using historical images in local areas. This paper focuses on the introduction of the methodology. Furthermore, an improvement to SAGBT is proposed. In a subsequent paper, subtitled "Part 2, Validation and Sensitivity Analysis," we address satellite-field simultaneous observations and report comparisons between the retrieved thermal anomalies and field measurements in different aspects to prove that the coal fires are separable by the SAGBT method. These comparisons allowed us to estimate the accuracy and biases of the SAGBT method. As an application of the SAGBT, a relationship between coal fires' decadal variation and coal production was also examined. Our work documented a total area increase in the beginning of 2003, which correlates with increased mining activities and the rapid increase of energy consumption in China during the decade (2001-2011). Additionally, a decrease in the total coal fire area is consistent with the nationally sponsored fire suppression efforts during 2007-2008. It demonstrated the applicability of SAGBT method for long-term change detection with multi-temporal images. C1 [Du, Xiaomin; Cao, Daiyong] China Univ Min & Technol, Sch Geosci & Surveying Engn, Beijing 100083, Peoples R China. [Du, Xiaomin; Mishra, Deepak; Bernardes, Sergio; Jordan, Thomas R.; Madden, Marguerite] Univ Georgia, Dept Geog, Ctr Geospatial Res, Athens, GA 30602 USA. [Bernardes, Sergio] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. RP Mishra, D (reprint author), Univ Georgia, Dept Geog, Ctr Geospatial Res, Athens, GA 30602 USA. EM xiaomin@uga.edu; cdy@cumtb.edu.cn; dmishra@uga.edu; sergio.bernardes@nasa.gov; tombob@uga.edu; mmadden@uga.edu FU Strategic Priority Research Program of the Chinese Academy of Sciences, Carbon Emission from Coal Spontaneous Combustion [XDA05030200]; China Scholarship Council FX Funding for this work was provided by a Strategic Priority Research Program of the Chinese Academy of Sciences, Carbon Emission from Coal Spontaneous Combustion (Grant No. XDA05030200). The first author's visiting study at the University of Georgia (UGA) was sponsored by the China Scholarship Council. We thank Guang Yang and Zhipeng Li for collection of field data. The authors wish to thank the anonymous reviewers for their constructive suggestions that improved the paper. Image acquisition was granted by the Land Processes Distributed Active Archive Center (LP DAAC) of the National Aeronautics and Space Administration (NASA), including the tasking of the ASTER orbital sensor to acquire images during field activities in China. ASTER images were accessed through the Earth Resources Observation Systems (EROS) Data Center of the U.S. Geological Survey (USGS). Special thanks to UGA's international student internship program for facilitating collaboration between the two institutes. NR 59 TC 2 Z9 2 U1 2 U2 19 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 JUN PY 2015 VL 7 IS 6 BP 6576 EP 6610 DI 10.3390/rs70606576 PG 35 WC Remote Sensing SC Remote Sensing GA CM3NS UT WOS:000357589800004 ER PT J AU Heidinger, AK Li, Y Baum, BA Holz, RE Platnick, S Yang, P AF Heidinger, Andrew K. Li, Yue Baum, Bryan A. Holz, Robert E. Platnick, Steven Yang, Ping TI Retrieval of Cirrus Cloud Optical Depth under Day and Night Conditions from MODIS Collection 6 Cloud Property Data SO REMOTE SENSING LA English DT Article ID PARTICLES; SATELLITE; MODEL AB This paper presents a technique to generate cirrus optical depth and particle effective size estimates from the cloud emissivities at 8.5, 11 and 12 mu m contained in the Collection-6 (C6) MYD06 cloud product. This technique employs the latest scattering models and scattering radiative transfer approximations to estimate cloud optical depth and particle effective size using efficient analytical formulae. Two scattering models are tested. The first is the same scattering model as that used in the C6 MYD06 solar reflectance products. The second model is an empirical model derived from radiometric consistency. Both models are shown to generate optical depths that compare well to those from constrained CALIPSO retrievals and MYD06. In terms of effective radius retrievals, the results from the radiometric empirical model agree more closely with MYD06 than those from the C6 model. This analysis is applied to AQUA/MODIS data collocated with CALIPSO/CALIOP during January 2010. C1 [Heidinger, Andrew K.] NOAA Satellite & Informat Serv NESDIS, Ctr Satellite Applicat & Res, Madison, WI 53706 USA. [Li, Yue; Baum, Bryan A.; Holz, Robert E.] Univ Wisconsin, SSEC, Madison, WI 53706 USA. [Platnick, Steven] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. RP Heidinger, AK (reprint author), NOAA Satellite & Informat Serv NESDIS, Ctr Satellite Applicat & Res, 1225 West Dayton St, Madison, WI 53706 USA. EM andrew.heidinger@noaa.gov; yue.li@ssec.wisc.edu; bryan.baum@ssec.wisc.edu; reholz@ssec.wisc.edu; steven.e.platnick@nasa.gov; pyang@tamu.edu RI Yang, Ping/B-4590-2011; Baum, Bryan/B-7670-2011; Platnick, Steven/J-9982-2014; Heidinger, Andrew/F-5591-2010 OI Baum, Bryan/0000-0002-7193-2767; Platnick, Steven/0000-0003-3964-3567; Heidinger, Andrew/0000-0001-7631-109X FU NASA [NNX11AR06G] FX This work was supported by Hal Maring of the NASA ROSES Program. Bryan Baum and Ping Yang also gratefully acknowledge the support from NASA grant NNX11AR06G. The NPP Atmospheric PEATE at the University of Wisconsin provided the data for this paper. NR 21 TC 5 Z9 5 U1 1 U2 9 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD JUN PY 2015 VL 7 IS 6 BP 7257 EP 7271 DI 10.3390/rs70607257 PG 15 WC Remote Sensing SC Remote Sensing GA CM3NS UT WOS:000357589800032 ER PT J AU Clewley, D Whitcomb, J Moghaddam, M McDonald, K Chapman, B Bunting, P AF Clewley, Daniel Whitcomb, Jane Moghaddam, Mahta McDonald, Kyle Chapman, Bruce Bunting, Peter TI Evaluation of ALOS PALSAR Data for High-Resolution Mapping of Vegetated Wetlands in Alaska SO REMOTE SENSING LA English DT Article ID LAND-COVER DATABASE; METHANE EMISSIONS; INVENTORY MAPS; RANDOM FORESTS; CLIMATE-CHANGE; CLASSIFICATION; SUCCESSION; IMPACTS; PROJECT; EXTENT AB As the largest natural source of methane, wetlands play an important role in the carbon cycle. High-resolution maps of wetland type and extent are required to quantify wetland responses to climate change. Mapping northern wetlands is particularly important because of a disproportionate increase in temperatures at higher latitudes. Synthetic aperture radar data from a spaceborne platform can be used to map wetland types and dynamics over large areas. Following from earlier work by Whitcomb et al. (2009) using Japanese Earth Resources Satellite (JERS-1) data, we applied the "random forests" classification algorithm to variables from L-band ALOS PALSAR data for 2007, topographic data (e.g., slope, elevation) and locational information (latitude, longitude) to derive a map of vegetated wetlands in Alaska, with a spatial resolution of 50 m. We used the National Wetlands Inventory and National Land Cover Database (for upland areas) to select training and validation data and further validated classification results with an independent dataset that we created. A number of improvements were made to the method of Whitcomb et al. (2009): (1) more consistent training data in upland areas; (2) better distribution of training data across all classes by taking a stratified random sample of all available training pixels; and (3) a more efficient implementation, which allowed classification of the entire state as a single entity (rather than in separate tiles), which eliminated discontinuities at tile boundaries. The overall accuracy for discriminating wetland from upland was 95%, and the accuracy at the level of wetland classes was 85%. The total area of wetlands mapped was 0.59 million km(2), or 36% of the total land area of the state of Alaska. The map will be made available to download from NASA's wetland monitoring website. C1 [Clewley, Daniel; Whitcomb, Jane; Moghaddam, Mahta] Univ So Calif, Viterbi Sch Engn, Los Angeles, CA 90089 USA. [McDonald, Kyle] CUNY City Coll, New York, NY 10031 USA. [Chapman, Bruce] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bunting, Peter] Aberystwyth Univ, Dept Geog & Earth Sci, Aberystwyth SY23 3DB, Ceredigion, Wales. RP Clewley, D (reprint author), Univ So Calif, Viterbi Sch Engn, Los Angeles, CA 90089 USA. EM daniel.clewley@gmail.com; jbwhitco@usc.edu; mahta@usc.edu; kmcdonald2@ccny.cuny.edu; bruce.d.chapman@jpl.nasa.gov; pfb@aber.ac.uk RI Bunting, Pete/B-8678-2013; OI Bunting, Pete/0000-0002-7435-0148; Clewley, Daniel/0000-0003-1243-3711 FU NASA's Making Earth System Data Records for Use in Research Environments (MEaSUREs) Program; National Aeronautics and Space Administration FX This work was supported through NASA's Making Earth System Data Records for Use in Research Environments (MEaSUREs) Program. This work was undertaken in part within the framework of the JAXA Kyoto & Carbon Initiative. ALOS PALSAR data were provided through the Alaska Satellite Facility. Portions of this work were undertaken at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 61 TC 4 Z9 4 U1 1 U2 13 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD JUN PY 2015 VL 7 IS 6 BP 7272 EP 7297 DI 10.3390/rs70607272 PG 26 WC Remote Sensing SC Remote Sensing GA CM3NS UT WOS:000357589800033 ER PT J AU Bellini, A Renzini, A Anderson, J Bedin, LR Piotto, G Soto, M Brown, TM Milone, AP Sohn, ST Sweigart, AV AF Bellini, A. Renzini, A. Anderson, J. Bedin, L. R. Piotto, G. Soto, M. Brown, T. M. Milone, A. P. Sohn, S. T. Sweigart, A. V. TI UV INSIGHTS INTO THE COMPLEX POPULATIONS OF M87 GLOBULAR CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M87); galaxies: star clusters: general; (Galaxy:) globular clusters: general; Hertzsprung-Russell and C-M diagrams; techniques: photometric ID MULTIPLE STELLAR POPULATIONS; SPACE-TELESCOPE OBSERVATIONS; DOUBLE MAIN-SEQUENCE; EARLY-TYPE GALAXIES; OMEGA-CENTAURI; ADVANCED CAMERA; STAR-CLUSTERS; ACS SURVEY; WIDE-FIELD; NGC 6397 AB We have imaged with Hubble Space Telescope WFC3/UVIS the central 2.'7 x 2.'7 region of the giant elliptical galaxy M87, using the ultraviolet filter F275W. In combination with archival ACS/WFC data taken through the F606W and F814W filters, covering the same field, we have constructed integrated-light UV-optical colors and magnitudes for 1460 objects, most of which are believed to be globular clusters (GCs) belonging to M87. The purpose was to ascertain whether the multiple-populations syndrome, ubiquitous among Galactic GCs, also exists among the M87 family of clusters. To achieve this goal, we sought those GCs with exceptionally blue UV-tooptical colors because helium-enriched sub-populations produce a horizontal-branch morphology that is well populated at high effective temperature. For comparison, integrated, synthetic UV-optical and purely optical colors and magnitudes have been constructed for 45 Galactic GCs, starting from individual-star photometry obtained with the same instruments and the same filters. We identify a small group of M87 clusters exhibiting a radial UV-optical color gradient, representing our best candidate GCs hosting multiple populations with extreme helium content. We also find that the central spatial distribution of the bluer GCs is flattened in a direction parallel to the jet, while the distribution of redder GCs is more spherical. We release to the astronomical community our photometric catalog in F275W, F606W, and F814W bands and the high-quality image stacks in the same bands. C1 [Bellini, A.; Anderson, J.; Soto, M.; Brown, T. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Renzini, A.; Bedin, L. R.; Piotto, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Piotto, G.] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, Mt Stromlo Observ, I-35122 Padua, Italy. [Milone, A. P.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Weston, ACT 2611, Australia. [Sohn, S. T.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Sweigart, A. V.] NASA, Goddard Space Flight Ctr, Explorat Univ Div, Greenbelt, MD 20771 USA. RP Bellini, A (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM bellini@stsci.edu OI Piotto, Giampaolo/0000-0002-9937-6387; bedin, luigi/0000-0003-4080-6466; Brown, Thomas/0000-0002-1793-9968 FU STScI grant [GO-12989, GO-13297]; Australian Research Council [DP120100475]; Becas Chile de Postdoctorado en el Extranjero project [74150088] FX The authors gratefully thank the anonymous referee for his/her useful suggestions that helped improving the manuscript, and Thomas Puzia for a critical reading of the manuscript. A. B. and J. A. acknowledge support from STScI grant GO-12989. A. P. M. acknowledges the financial support from the Australian Research Council through Discovery Project grant DP120100475. M. S. acknowledges support from STScI grant GO-13297 and Becas Chile de Postdoctorado en el Extranjero project 74150088. NR 63 TC 4 Z9 4 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2015 VL 805 IS 2 AR 178 DI 10.1088/0004-637X/805/2/178 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400093 ER PT J AU Chakraborti, S Soderberg, A Chomiuk, L Kamble, A Yadav, N Ray, A Hurley, K Margutti, R Milisavljevic, D Bietenholz, M Brunthaler, A Pignata, G Pian, E Mazzali, P Fransson, C Bartel, N Hamuy, M Levesque, E MacFadyen, A Dittmann, J Krauss, M Briggs, MS Connaughton, V Yamaoka, K Takahashi, T Ohno, M Fukazawa, Y Tashiro, M Terada, Y Murakami, T Goldsten, J Barthelmy, S Gehrels, N Cummings, J Krimm, H Palmer, D Golenetskii, S Aptekar, R Frederiks, D Svinkin, D Cline, T Mitrofanov, IG Golovin, D Litvak, ML Sanin, AB Boynton, W Fellows, C Harshman, K Enos, H von Kienlin, A Rau, A Zhang, X Savchenko, V AF Chakraborti, Sayan Soderberg, Alicia Chomiuk, Laura Kamble, Atish Yadav, Naveen Ray, Alak Hurley, Kevin Margutti, Raffaella Milisavljevic, Dan Bietenholz, Michael Brunthaler, Andreas Pignata, Giuliano Pian, Elena Mazzali, Paolo Fransson, Claes Bartel, Norbert Hamuy, Mario Levesque, Emily MacFadyen, Andrew Dittmann, Jason Krauss, Miriam Briggs, M. S. Connaughton, V. Yamaoka, K. Takahashi, T. Ohno, M. Fukazawa, Y. Tashiro, M. Terada, Y. Murakami, T. Goldsten, J. Barthelmy, S. Gehrels, N. Cummings, J. Krimm, H. Palmer, D. Golenetskii, S. Aptekar, R. Frederiks, D. Svinkin, D. Cline, T. Mitrofanov, I. G. Golovin, D. Litvak, M. L. Sanin, A. B. Boynton, W. Fellows, C. Harshman, K. Enos, H. von Kienlin, A. Rau, A. Zhang, X. Savchenko, V. TI A MISSING-LINK IN THE SUPERNOVA-GRB CONNECTION: THE CASE OF SN 2012ap SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; radiation mechanisms: non-thermal; shock waves; supernovae: individual (SN 2012ap); techniques: interferometric ID GAMMA-RAY BURSTS; RELATIVISTIC BLAST WAVES; 25 APRIL 1998; EMISSION; MODEL; SYNCHROTRON AB Gamma-ray bursts (GRBs) are characterized by ultra-relativistic outflows, while supernovae are generally characterized by non-relativistic ejecta. GRB afterglows decelerate rapidly, usually within days, because their low-mass ejecta rapidly sweep up a comparatively larger mass of circumstellar material. However, supernovae with heavy ejecta can be in nearly free expansion for centuries. Supernovae were thought to have non-relativistic outflows except for a few relativistic ones accompanied by GRBs. This clear division was blurred by SN 2009bb, the first supernova with a relativistic outflow without an observed GRB. However, the ejecta from SN 2009bb was baryon loaded and in nearly free expansion for a year, unlike GRBs. We report the first supernova discovered without a GRB but with rapidly decelerating mildly relativistic ejecta, SN 2012ap. We discovered a bright and rapidly evolving radio counterpart driven by the circumstellar interaction of the relativistic ejecta. However, we did not find any coincident GRB with an isotropic fluence of more than one-sixth of the fluence from GRB 980425. This shows for the first time that central engines in SNe Ic, even without an observed GRB, can produce both relativistic and rapidly decelerating outflows like GRBs. C1 [Chakraborti, Sayan; Soderberg, Alicia; Kamble, Atish; Margutti, Raffaella; Milisavljevic, Dan; Dittmann, Jason] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Chakraborti, Sayan] Harvard Univ, Cambridge, MA 02138 USA. [Chomiuk, Laura] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Yadav, Naveen; Ray, Alak] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. [Hurley, Kevin] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Bietenholz, Michael] York Univ, Dept Phys & Astron, N York, ON M3J 1P3, Canada. [Brunthaler, Andreas] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdrop, South Africa. [Brunthaler, Andreas] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Pignata, Giuliano] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. [Pian, Elena] Scuola Normale Super Pisa, I-56126 Pisa, Italy. [Mazzali, Paolo] Liverpool John Moores Univ, Liverpool L3 5UX, Merseyside, England. [Mazzali, Paolo] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Fransson, Claes] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Hamuy, Mario] Univ Chile, Dept Astron, Santiago, Chile. [Levesque, Emily] Univ Colorado, C327A, Boulder, CO 80309 USA. [MacFadyen, Andrew] NYU, New York, NY 10003 USA. [Krauss, Miriam] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Briggs, M. S.; Connaughton, V.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. [Yamaoka, K.] Nagoya Univ, Grad Sch Sci, Nagoya, Aichi 4648602, Japan. [Takahashi, T.] ISAS JAXA, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Ohno, M.; Fukazawa, Y.] Hiroshima Univ, Higashihiroshima, Hiroshima 7398526, Japan. [Tashiro, M.; Terada, Y.] Saitama Univ, Sakura Ku, Saitama, Saitama 3388570, Japan. [Murakami, T.] Kanazawa Univ, Kanazawa, Ishikawa 9201192, Japan. [Goldsten, J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Barthelmy, S.; Gehrels, N.; Cummings, J.; Krimm, H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cummings, J.] UMBC, Dept Phys, Baltimore, MD 21250 USA. [Krimm, H.] Univ Space Res Assoc, Columbia, MD 20144 USA. [Palmer, D.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Golenetskii, S.; Aptekar, R.; Frederiks, D.; Svinkin, D.] AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia. [Cline, T.] NASA, Goddard Space Flight Ctr, Emeritus, Greenbelt, MD 20771 USA. [Mitrofanov, I. G.; Golovin, D.; Litvak, M. L.; Sanin, A. B.] Space Res Inst, Moscow 117997, Russia. [Boynton, W.; Fellows, C.; Harshman, K.; Enos, H.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [von Kienlin, A.; Rau, A.; Zhang, X.] MPE, D-85748 Garching, Germany. [Savchenko, V.] Observ Paris, F-75205 Paris 13, France. RP Chakraborti, S (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM schakraborti@fas.harvard.edu RI Hamuy, Mario/G-7541-2016; OI Frederiks, Dmitry/0000-0002-1153-6340; MacFadyen, Andrew/0000-0002-0106-9013; Margutti, Raffaella/0000-0003-4768-7586; Pian, Elena/0000-0001-8646-4858 FU Science and Technology Facilities Council [ST/L00061X/1] NR 36 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2015 VL 805 IS 2 AR 187 DI 10.1088/0004-637X/805/2/187 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400102 ER PT J AU Deming, D Knutson, H Kammer, J Fulton, BJ Ingalls, J Carey, S Burrows, A Fortney, JJ Todorov, K Agol, E Cowan, N Desert, JM Fraine, J Langton, J Morley, C Showman, AP AF Deming, Drake Knutson, Heather Kammer, Joshua Fulton, Benjamin J. Ingalls, James Carey, Sean Burrows, Adam Fortney, Jonathan J. Todorov, Kamen Agol, Eric Cowan, Nicolas Desert, Jean-Michel Fraine, Jonathan Langton, Jonathan Morley, Caroline Showman, Adam P. TI SPITZER SECONDARY ECLIPSES OF THE DENSE, MODESTLY-IRRADIATED, GIANT EXOPLANET HAT-P-20b USING PIXEL-LEVEL DECORRELATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; infrared: planetary systems; planetary systems; planets and satellites: atmospheres ID HOT JUPITERS; WARM-SPITZER; THERMAL EMISSION; LIGHT CURVES; BROWN DWARF; HD 209458B; MU-M; ATMOSPHERIC CIRCULATION; TRANSITING PLANET; PHASE VARIATIONS AB HAT-P-20b is a giant metal-rich exoplanet orbiting a metal-rich star. We analyze two secondary eclipses of the planet in each of the 3.6 and 4.5 mu m bands of Warm Spitzer. We have developed a simple, powerful, and radically different method to correct the intra-pixel effect for Warm Spitzer data, which we call pixel-level decorrelation ( PLD). PLD corrects the intra-pixel effect very effectively, but without explicitly using-or even measuring-the fluctuations in the apparent position of the stellar image. We illustrate and validate PLD using synthetic and real data and comparing the results to previous analyses. PLD can significantly reduce or eliminate red noise in Spitzer secondary eclipse photometry, even for eclipses that have proven to be intractable using other methods. Our successful PLD analysis of four HAT-P-20b eclipses shows a best-fit blackbody temperature of 1134 +/- 29 K, indicating inefficient longitudinal transfer of heat, but lacking evidence for strong molecular absorption. We find sufficient evidence for variability in the 4.5 mu m band that the eclipses should be monitored at that wavelength by Spitzer, and this planet should be a high priority for James Webb Space Telescope spectroscopy. All four eclipses occur about 35 minutes after orbital phase 0.5, indicating a slightly eccentric orbit. A joint fit of the eclipse and transit times with extant RV data yields e cos omega = 0.01352(-0.00057)(+0.00054) and establishes the small eccentricity of the orbit to high statistical confidence. HAT-P-20b is another excellent candidate for orbital evolution via Kozai migration or other three-body mechanisms. C1 [Deming, Drake; Fraine, Jonathan] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Deming, Drake; Agol, Eric] NASA, Astrobiol Inst, Virtual Planetary Lab, Pasadena, CA 91125 USA. [Knutson, Heather; Kammer, Joshua] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Fulton, Benjamin J.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Ingalls, James; Carey, Sean] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Fortney, Jonathan J.; Morley, Caroline] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Todorov, Kamen] ETH, Inst Astron, CH-8092 Zurich, Switzerland. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Cowan, Nicolas] Amherst Coll, Dept Phys & Astron, Amherst, MA 01002 USA. [Desert, Jean-Michel] Univ Colorado, CASA, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Langton, Jonathan] Principia Coll, Dept Phys, Elsah, IL 62028 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. RP Deming, D (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM ddeming@astro.umd.edu OI /0000-0002-0802-9145 FU NASA FX We thank Jasmina Blecic, Patricio Cubillos, and Joseph Harrington for sending us the digital version of their results, used in Figures 5-7, and we thank Julie Moses for comments on this paper. This work is based on observations made with Spitzer, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 56 TC 25 Z9 25 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2015 VL 805 IS 2 AR 132 DI 10.1088/0004-637X/805/2/132 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400047 ER PT J AU Kay, C Opher, M Evans, RM AF Kay, C. Opher, M. Evans, R. M. TI GLOBAL TRENDS OF CME DEFLECTIONS BASED ON CME AND SOLAR PARAMETERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun: coronal mass ejections (CMEs) ID CORONAL MASS EJECTIONS; SELF-SIMILAR MAGNETOHYDRODYNAMICS; MAGNETIC-FLUX ROPE; INTERPLANETARY SPACE; ERUPTING PROMINENCES; MHD SIMULATION; PROPAGATION; WIND; STEREO; MODEL AB Accurate space weather forecasting requires. knowledge. of the trajectory of coronal mass ejections (CMEs), including any deflections. close to the Sun or through interplanetary space. Kay et al. introduced ForeCAT, a model of CME deflection resulting from the background solar magnetic field. For a magnetic field solution corresponding to Carrington Rotation (CR) 2029 (declining phase, 2005 April-May), the majority of the CMEs deflected to the Heliospheric Current Sheet, the minimum in magnetic pressure on global scales. Most of the deflection occurred below 4 R-circle dot. Here we extend ForeCAT to include a three-dimensional description of the deflecting CME. We attempt to answer the following questions: (1) do all CMEs deflect to the magnetic minimum? and (2) does most deflection occur within the first few solar radii (4 R-circle dot)? Results for solar minimum and declining-phase CMEs show that not every CME deflects to the magnetic minimum and that typically the majority of the deflection occurs below 10 R-circle dot. Slow, wide, low-mass CMEs in declining-phase solar backgrounds with strong magnetic field and magnetic gradients exhibit the largest deflections. Local gradients related to active regions tend to cause the largest deviations from the deflection predicted by global magnetic gradients, but variations can also be seen for CMEs in the quiet-Sun regions of the declining-phase CR. We show the torques due to differential forces along the CME can cause rotation about the CME's toroidal axis. C1 [Kay, C.; Opher, M.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Evans, R. M.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. RP Kay, C (reprint author), Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. EM ckay@bu.edu OI Kay, Christina/0000-0002-2827-6012 NR 73 TC 11 Z9 11 U1 2 U2 12 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 JUN 1 PY 2015 VL 805 IS 2 AR 168 DI 10.1088/0004-637X/805/2/168 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400083 ER PT J AU Linford, JD Ribeiro, VARM Chomiuk, L Nelson, T Sokoloski, JL Rupen, MP Mukai, K O'Brien, TJ Mioduszewski, AJ Weston, J AF Linford, J. D. Ribeiro, V. A. R. M. Chomiuk, L. Nelson, T. Sokoloski, J. L. Rupen, M. P. Mukai, K. O'Brien, T. J. Mioduszewski, A. J. Weston, J. TI THE DISTANCE TO NOVA V959 MON FROM VLA IMAGING SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: stars; novae, cataclysmic variables; radio continuum: stars; stars: individual (V959 Mon); white dwarfs ID GAMMA-RAY EMISSION; CLASSICAL NOVAE; WHITE-DWARF; MONOCEROTIS 2012; RS OPHIUCHI; V407 CYGNI; OUTBURST; RADIO; REMNANTS; SHELL AB Determining reliable distances to classical novae is a challenging but crucial step in deriving their ejected masses and explosion energetics. Here we combine radio expansion measurements from the Karl G. Jansky Very Large Array with velocities derived from optical spectra to estimate an expansion parallax for nova V959 Mon, the first nova discovered through its gamma-ray emission. We spatially resolve the nova at frequencies of 4.5-36.5 GHz in nine different imaging epochs. The first five epochs cover the expansion of the ejecta from 2012 October to 2013 January, while the final four epochs span 2014 February-May. These observations correspond to days 126 through 199 and days 615 through 703 after the first detection of the nova. The images clearly show a non-spherical ejecta geometry. Utilizing ejecta velocities derived from three-dimensional modeling of optical spectroscopy, the radio expansion implies a distance between 0.9 +/- 0.2 and 2.2 +/- 0.4 kpc, with a most probable distance of 1.4 +/- 0.4 kpc. This distance implies a gamma-ray luminosity of 0.6 x 10(35) erg s(-1), which is much less than the prototype gamma-ray-detected nova, V407 Cyg, possibly due to the lack of a red giant companion in the V959 Mon system. V959 Mon also has a much lower gamma-ray luminosity than other classical novae detected in gamma-rays to date, indicating a range of at least a factor of 10 in the gamma-ray luminosities for these explosions. C1 [Linford, J. D.; Chomiuk, L.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Ribeiro, V. A. R. M.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Ribeiro, V. A. R. M.] Univ Cape Town, Astrophys Cosmol & Grav Ctr, Dept Astron, ZA-7701 Rondebosch, South Africa. [Nelson, T.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Sokoloski, J. L.; Weston, J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Rupen, M. P.] Natl Res Council Canada, Herzberg Inst Astrophys, Penticton, BC, Canada. [Mukai, K.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Mukai, K.] NASA, GSFC, CRESST, Greenbelt, MD 20771 USA. [Mukai, K.] NASA, GSFC, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [O'Brien, T. J.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Mioduszewski, A. J.] Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Linford, JD (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. EM jlinford@.msu.edu OI Roberts Machado Ribeiro, Valerio Alipio/0000-0003-3617-4400 FU NASA Fermi Guest Investigator grant [NNH13ZDA001N-FERMI]; Radboud Excellence Initiative; South Africa SKA Project; NASA [NNX13A091G]; NSF [AST-1211778] FX The authors thank the anonymous referee for their constructive (and extremely pleasant) criticism. The authors thank W. Steffen and N. Koning for useful discussions on the use of SHAPE, and T. Finzell for useful discussions on V1324 Sco. J. L. and L. C. were supported in part by NASA Fermi Guest Investigator grant NNH13ZDA001N-FERMI. V. A. R. M. R. was supported in part by the Radboud Excellence Initiative and the South Africa SKA Project. T. N. was supported in part by NASA award NNX13A091G. J. L. S. and J. W. were funded in part by NSF award AST-1211778. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. NR 53 TC 7 Z9 7 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 JUN 1 PY 2015 VL 805 IS 2 AR 136 DI 10.1088/0004-637X/805/2/136 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400051 ER PT J AU Margutti, R Guidorzi, C Lazzati, D Milisavljevic, D Kamble, A Laskar, T Parrent, J Gehrels, NC Soderberg, AM AF Margutti, R. Guidorzi, C. Lazzati, D. Milisavljevic, D. Kamble, A. Laskar, T. Parrent, J. Gehrels, N. C. Soderberg, A. M. TI DUST IN THE WIND: THE ROLE OF RECENT MASS LOSS IN LONG GAMMA-RAY BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; gamma-ray burst: individual (GRBs 060218, 100316D, 980425, 130925A); supernovae: general ID GRB 130925A; RADIO OBSERVATIONS; SCATTERING MODEL; SUPERNOVAE; AFTERGLOW; EVOLUTION; STARS; TELESCOPE; ENVIRONMENT; EXPLOSIONS AB We study the late-time (t > 0.5 days) X-ray afterglows of nearby (z < 0.5) long gamma-ray bursts (GRBs) with Swift and identify a population of explosions with slowly decaying, super-soft (photon index Gamma(x) > 3) X-ray emission that is inconsistent with forward shock synchrotron radiation associated with the afterglow. These explosions also show larger-than-average intrinsic absorption (NHx,i > 6 x 10(21) cm(-2)) and prompt gamma-ray emission with extremely long duration (T-90 > 1000 s). The chance association of these three rare properties (i.e., large NHx,i, super-soft Gamma(x), and extreme duration) in the same class of explosions is statistically unlikely. We associate these properties with the turbulent mass-loss history of the progenitor star that enriched and shaped the circumburst medium. We identify a natural connection between NHx,i, Gamma(x), and T-90 in these sources by suggesting that the late-time super-soft X-rays originate from radiation reprocessed by material lost to the environment by the stellar progenitor before exploding (either in the form of a dust echo or as reprocessed radiation from a long-lived GRB remnant), and that the interaction of the explosion's shock/jet with the complex medium is the source of the extremely long prompt emission. However, current observations do not allow us to exclude the possibility that super-soft X-ray emitters originate from peculiar stellar progenitors with large radii that only form in very dusty environments. C1 [Margutti, R.; Milisavljevic, D.; Kamble, A.; Laskar, T.; Parrent, J.; Soderberg, A. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Guidorzi, C.] Univ Ferrara, Dept Phys & Earth Sci, I-44122 Ferrara, Italy. [Lazzati, D.] Oregon State Univ, Dept Phys, Corvallis, OR 97331 USA. [Gehrels, N. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Margutti, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Lazzati, Davide/0000-0002-9190-662X; Margutti, Raffaella/0000-0003-4768-7586 FU NSF [1066293]; David and Lucile Packard Foundation Fellowship for Science and Engineering award FX We thank the referee for helpful comments that improved the quality of our work. R.M. is grateful to the Aspen Center for Physics and the NSF Grant #1066293 for hospitality during the completion of this work and for providing a stimulating environment that inspired this project. Support for this work was provided by the David and Lucile Packard Foundation Fellowship for Science and Engineering awarded to A.M.S. NR 62 TC 8 Z9 8 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2015 VL 805 IS 2 AR 159 DI 10.1088/0004-637X/805/2/159 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400074 ER PT J AU Meyer, ET Georganopoulos, M Sparks, WB Godfrey, L Lovell, JEJ Perlman, E AF Meyer, Eileen T. Georganopoulos, Markos Sparks, William B. Godfrey, Leith Lovell, James E. J. Perlman, Eric TI RULING OUT IC/CMB X-RAYS IN PKS 0637-752 AND THE IMPLICATIONS FOR TEV EMISSION FROM LARGE-SCALE QUASAR JETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; quasars: individual (PKS 0637-752, 3C 273) ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; INVERSE-COMPTON MODEL; EXTENDED RADIO JETS; 3C 273; CHANDRA OBSERVATIONS; COSMOLOGICAL IMPACT; EXTRAGALACTIC JETS; SYNCHROTRON; 3C-273 AB The Chandra X-ray observatory has discovered dozens of resolved, kiloparsec-scale jets associated with powerful quasars in which the X-ray fluxes are observed to be much higher than the expected level based on the radio-optical synchrotron spectrum. The most popular explanation for the anomalously high and hard X-ray fluxes is that these jets do not decelerate significantly by the kiloparsec scale, but rather remain highly relativistic (Lorentz factors Gamma similar to 10). By adopting a small angle to the line of sight, the X-rays can thus be explained by inverse Compton upscattering of cosmic microwave background (CMB) photons (IC/CMB), where the observed emission is strongly Doppler boosted. Using over six years of Fermi monitoring data, we show that the expected hard, steady gamma-ray emission implied by the IC/CMB model is not seen in PKS 0637-752, the prototype jet for which this model was first proposed. IC/CMB emission is thus ruled out as the source of the X-rays, joining recent results for the jets in 3C 273 (using the same method) and PKS 1136-135 (using UV polarization). We further show that the Fermi observations give an upper limit of delta < 6.5 for the four brightest X-ray knots of PKS 0637-752, and derive an updated limit of delta < 7.8 for knots A and B1 of 3C 273 (assuming equipartition). Finally, we discuss the fact that high levels of synchrotron X-ray emission in a slow jet will unavoidably lead to a level of angle-integrated TeV emission which exceeds that of the TeV BL Lac class. C1 [Meyer, Eileen T.; Sparks, William B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Meyer, Eileen T.; Georganopoulos, Markos] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Georganopoulos, Markos] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Godfrey, Leith] ASTRON, Netherlands Inst Radio Astron, NL-7990 AA Dwingeloo, Netherlands. [Lovell, James E. J.] Univ Tasmania, Sch Phys Sci, Hobart, Tas 7001, Australia. [Perlman, Eric] Florida Inst Technol, Melbourne, FL 32901 USA. RP Meyer, ET (reprint author), Space Telescope Sci Inst, Baltimore, MD 21218 USA. EM meyer@stsci.edu OI Perlman, Eric/0000-0002-3099-1664 FU Fermi Grant [NNX13AO88G] FX E. T. M. acknowledges Fermi Grant NNX13AO88G. NR 46 TC 11 Z9 11 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 JUN 1 PY 2015 VL 805 IS 2 AR 154 DI 10.1088/0004-637X/805/2/154 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400069 ER PT J AU Miceli, M Sciortino, S Troja, E Orlando, S AF Miceli, M. Sciortino, S. Troja, E. Orlando, S. TI SPATIAL DISTRIBUTION OF X-RAY EMITTING EJECTA IN TYCHO'S SNR: INDICATIONS OF SHOCKED TITANIUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (Tycho's SNR); ISM: supernova remnants; X-rays: ISM ID SUPERNOVA REMNANT W49B; IA SUPERNOVAE; CORE-COLLAPSE; EMISSION; PROGENITOR; SPECTRUM; MODELS; LINE; SPECTROPOLARIMETRY; NUCLEOSYNTHESIS AB Young supernova remnants (SNRs) show characteristic ejecta-dominated X-ray emission that allows us to probe the products of explosive nucleosynthesis processes and to ascertain important information about the physics of supernova explosions. Hard X-ray observations have recently revealed the presence of the radioactive decay lines of Ti-44 at similar to 67.9 and similar to 78.4 keV in Tycho's SNR. Here, we analyze a set of XMM-Newton archive observations of Tycho's SNR. We produce equivalent width (EW) maps of the Fe K and Ca XIX emission lines and find indications for a stratification of the abundances of these elements and significant anisotropies. We then perform spatially resolved spectral analysis by identifying five different regions characterized by high/low values of the Fe K EW. We find that the spatial distribution of the Fe K emission is correlated with that of Cr XXII. We also detect the Ti K line complex in the spectra extracted from the two regions with the highest values of Fe and Cr EWs. The Ti line emission remains undetected in regions where Fe and Cr EWs are low. Our results indicate that the post-shock Ti is spatially colocated with other iron-peak nuclei in Tycho's SNR, in agreement with the predictions of multi-D models of SNe Ia. C1 [Miceli, M.] Univ Palermo, Dipartimento Fis & Chim, I-90134 Palermo, Italy. [Miceli, M.; Sciortino, S.; Orlando, S.] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Miceli, M (reprint author), Univ Palermo, Dipartimento Fis & Chim, Piazza Parlamento 1, I-90134 Palermo, Italy. EM miceli@astropa.unipa.it OI Troja, Eleonora/0000-0002-1869-7817; Miceli, Marco/0000-0003-0876-8391; Orlando, Salvatore/0000-0003-2836-540X FU PRIN INAF grant FX We thank the anonymous referee for comments and suggestions. This paper was partially funded by the PRIN INAF 2014 grant. M.M. thanks M. Dadina for discussions about the X-IFU instrumental background. NR 40 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2015 VL 805 IS 2 AR 120 DI 10.1088/0004-637X/805/2/120 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400035 ER PT J AU Plavchan, P Chen, X Pohl, G AF Plavchan, Peter Chen, Xi Pohl, Garrett TI WHAT IS THE MASS OF alpha CEN B b? SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: dynamical evolution and stability; planets and satellites: formation; planets and satellites: individual (alpha Centauri) ID TERRESTRIAL PLANET FORMATION; BINARY STAR SYSTEMS; CENTAURI-B; TIDAL DISSIPATION; STELLAR ACTIVITY; ROTATION; KEPLER; DISCS; CIRCULARIZATION; COPLANARITY AB We investigate the possibility of constraining the sin i degeneracy of alpha Cen B b-with orbital period P = 3.24 days; a = 0.042 AU; m sin i = 1.1 M-circle plus-to estimate the true mass of the newly reported terrestrial exoplanet in the nearest stellar system to our Sun. We present detailed numerical simulations of the dynamical stability of the exoplanet in the alpha Cen AB binary system for a range of initial inclinations, eccentricities, and semimajor axes. The system represents a benchmark case for the interplay of the Kozai mechanism with general relativistic and tidal forces. From our simulations, there is only a small boundary in initial inclinations and initial semimajor axes which result in the migration via the Kozai mechanism of alpha Cen B b to its present location. Inside this boundary, the planet orbit is stable for up to 1 Gyr against the Kozai mechanism, and outside this boundary the planet collides with alpha Cen B or is ejected. In our three simulations where the planet migrates in toward the star via the Kozai mechanism, the final inclination is 46 degrees-53 degrees relative to the AB orbital plane, lower than the initial inclination of 75 degrees in each case. We discuss inclination constraints from the formation of alpha Cen B b in situ at its present location, migration in a proto-planetary disk, or migration in resonance with additional planets. We conclude that alpha Cen B b probably has a mass of less than 2.7 M-circle plus, implying a likely terrestrial composition warranting future confirmation. C1 [Plavchan, Peter; Pohl, Garrett] Dept Phys Astron & Mat Sci, 901 South Natl Ave, Springfield, MO 65897 USA. [Chen, Xi] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. RP Plavchan, P (reprint author), Dept Phys Astron & Mat Sci, 901 South Natl Ave, Springfield, MO 65897 USA. EM peterplavchan@missouristate.edu OI Plavchan, Peter/0000-0002-8864-1667 FU National Aeronautics and Space Administration under Exoplanet Exploration Program; NASA JPL Research and Technology Development program; Missouri SpaceGrant Consortium FX We thank the anonymous referee for a thoughtful review that improved the clarity and presentation of this manuscript. The authors acknowledge Thayne Currie, Dave Latham, and David Ciardi for their encouragement in writing this paper. 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. P.P. acknowledges support from a NASA JPL Research and Technology Development program, and the Missouri SpaceGrant Consortium. NR 67 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2015 VL 805 IS 2 AR 174 DI 10.1088/0004-637X/805/2/174 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400089 ER PT J AU Sadykov, VM Dominguez, SV Kosovichev, AG Sharykin, IN Struminsky, AB Zimovets, I AF Sadykov, Viacheslav M. Dominguez, Santiago Vargas Kosovichev, Alexander G. Sharykin, Ivan N. Struminsky, Alexei B. Zimovets, Ivan TI PROPERTIES OF CHROMOSPHERIC EVAPORATION AND PLASMA DYNAMICS OF A SOLAR FLARE FROM IRIS OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic fields; Sun: activity; Sun: atmosphere; Sun: flares; Sun: UV radiation ID LOOP RADIATIVE HYDRODYNAMICS; REGION-IMAGING-SPECTROGRAPH; HIGH TIME RESOLUTION; EXTREME-ULTRAVIOLET; SPECTROSCOPIC OBSERVATIONS; NONTHERMAL ELECTRONS; HINODE; SPECTROMETER; TRANSPORT; EVENTS AB The dynamics of hot chromospheric plasma of solar flares is a key to understanding the mechanisms of flare energy release and particle acceleration. A moderate M1.0 class flare of 2014 June 12, (SOL2014-06-12T21:12) was simultaneously observed by NASA's Interface Region Imaging Spectrograph (IRIS) and. other spacecraft, and also by the New Solar Telescope at the BBSO. This paper presents the first part of our investigation focused on analysis of the IRIS data. Our analysis of the IRIS data in different spectral lines reveals a strong redshifted jet-like flow with a speed of similar to 100 km s(-1) of the chromospheric material before the flare. Strong nonthermal emission of the C II k 1334.5 angstrom line, formed in the chromosphere-corona transition region, is observed at the beginning of the impulsive phase in several small (with a size of similar to 1 '') points. It is also found that the C II k line is redshifted across the flaring region before, during, and after the impulsive phase. A peak of integrated emission of the hot (1.1 . 10(7) K) plasma in the Fe XXI 1354.1 angstrom line is detected approximately five minutes after the integrated emission peak of the lower temperature C II k. A strong blueshift of the Fe XXI line across the flaring region corresponds to evaporation flows of the hot chromospheric plasma with a speed of 50 km s-1. Additional analysis of the RHESSI data supports the idea that the upper chromospheric dynamics observed by IRIS has features of "gentle" evaporation driven by heating of the solar chromosphere by accelerated electrons and by a heat flux from the flare energy release site. C1 [Sadykov, Viacheslav M.; Dominguez, Santiago Vargas; Kosovichev, Alexander G.] New Jersey Inst Technol, Big Bear Solar Observ, Big Bear City, CA 92314 USA. [Sadykov, Viacheslav M.; Kosovichev, Alexander G.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Sadykov, Viacheslav M.; Sharykin, Ivan N.; Struminsky, Alexei B.; Zimovets, Ivan] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia. [Sadykov, Viacheslav M.; Struminsky, Alexei B.] MIPT, Dolgoprudnyi 141700, Moscow Region, Russia. [Dominguez, Santiago Vargas] Univ Nacl Colombia, Observatorio Astron, Bogota, Colombia. RP Sadykov, VM (reprint author), New Jersey Inst Technol, Big Bear Solar Observ, Big Bear City, CA 92314 USA. RI Zimovets, Ivan/E-4431-2017 OI Zimovets, Ivan/0000-0001-6995-3684 FU NASA Ames Research Center; NASA [NNX14AB68G, NNX14AB70G, NNX11AO736]; NSF [AGS-1250818]; RFBR grant [15-32-21078]; NJIT grant FX The authors acknowledge the Big Bear Solar Observatory (BBSO) observing and technical team, and the IRIS mission team and the NASA Ames Research Center for their contributions and support. The authors thank the referee for very useful comments. The work was partially supported by NASA grants NNX14AB68G, NNX14AB70G, and NNX11AO736; NSF grant AGS-1250818; RFBR grant 15-32-21078; and an NJIT grant. NR 41 TC 8 Z9 8 U1 2 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2015 VL 805 IS 2 AR 167 DI 10.1088/0004-637X/805/2/167 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400082 ER PT J AU Seo, YM Shirley, YL Goldsmith, P Ward-Thompson, D Kirk, JM Schmalzl, M Lee, JE Friesen, R Langston, G Masters, J Garwood, RW AF Seo, Young Min Shirley, Yancy L. Goldsmith, Paul Ward-Thompson, Derek Kirk, Jason M. Schmalzl, Markus Lee, Jeong-Eun Friesen, Rachel Langston, Glen Masters, Joe Garwood, Robert W. TI AN AMMONIA SPECTRAL MAP OF THE L1495-B218 FILAMENTS IN THE TAURUS MOLECULAR CLOUD. I. PHYSICAL PROPERTIES OF FILAMENTS AND DENSE CORES SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: molecules; radio lines: ISM; stars: formation ID GOULD BELT SURVEY; STAR-FORMATION; PRESTELLAR CORES; CO DEPLETION; PIPE NEBULA; DARK CLOUDS; GRAVITATIONAL COLLAPSE; INTERSTELLAR AMMONIA; (CO)-O-18 DEPLETION; VLBA DETERMINATION AB We present deep NH3 observations of the L1495-B218 filaments in the Taurus molecular cloud covering over a 3 degrees angular range using the K-band focal plane array on the 100 m Green Bank Telescope. The L1495-B218 filaments form an interconnected, nearby, large complex extending over 8 pc. We observed NH3 (1, 1) and (2, 2) with a spectral resolution of 0.038 km s(-1) and a spatial resolution of 31 ''. Most of the ammonia peaks coincide with intensity peaks in dust continuum maps at 350 and 500 mu m. We deduced physical properties by fitting a model to the observed spectra. We find gas kinetic temperatures of 8-15 K, velocity dispersions of 0.05-0.25 km s(-1), and NH3 column densities of 5 x 10(12) to 1 x 10(14) cm(-2). The CSAR algorithm, which is a hybrid of seeded-watershed and binary dendrogram algorithms, identifies a total of 55 NH3 structures, including 39 leaves and 16 branches. The masses of the NH3 sources range from 0.05 to 9.5 M-circle dot. The masses of NH3 leaves are mostly smaller than their corresponding virial mass estimated from their internal and gravitational energies, which suggests that these leaves are gravitationally unbound structures. Nine out of 39 NH3 leaves are gravitationally bound, and seven out of nine gravitationally bound NH3 leaves are associated with star formation. We also found that 12 out of 30 gravitationally unbound leaves are pressure. confined. Our data suggest that a dense core may form as a pressure-confined structure, evolve to a gravitationally bound core, and undergo collapse to form a protostar. C1 [Seo, Young Min; Shirley, Yancy L.] Univ Arizona, Dept Astron Steward Observ, Tucson, AZ 85721 USA. [Goldsmith, Paul] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ward-Thompson, Derek; Kirk, Jason M.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Schmalzl, Markus] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Lee, Jeong-Eun] Kyung Hee Univ, Dept Astron & Space Sci, Yongin 446701, Gyeonggi Do, South Korea. [Friesen, Rachel] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Langston, Glen] Natl Sci Fdn, Astron, Arlington, VA 22230 USA. [Masters, Joe; Garwood, Robert W.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Seo, YM (reprint author), Univ Arizona, Dept Astron Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. FU NRAO Observer's Grant [GBT/13A-126]; NSF Grant [AST-1008577, AST-1410190] FX We are grateful to the anonymous referee for helpful suggestions. We are also grateful to A. Hacar and M. Tafalla for providing C18O data. Y. Seo was support by a NRAO Observer's Grant (GBT/13A-126) and partially by NSF Grant AST-1008577. Y. Shirley was partially supported by NSF Grants AST-1008577 and AST-1410190. This work was carried out in part at the Jet Propulsion Laboratory, which is operated for NASA by the California Institute of Technology. NR 97 TC 5 Z9 5 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2015 VL 805 IS 2 AR 185 DI 10.1088/0004-637X/805/2/185 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400100 ER PT J AU Tsai, CW Eisenhardt, PRM Wu, JW Stern, D Assef, RJ Blain, AW Bridge, CR Benford, DJ Cutri, RM Griffith, RL Jarrett, TH Lonsdale, CJ Masci, FJ Moustakas, LA Petty, SM Sayers, J Stanford, SA Wright, EL Yan, L Leisawitz, DT Liu, FC Mainzer, AK McLean, IS Padgett, DL Skrutskie, MF Gelino, CR Beichman, CA Juneau, S AF Tsai, Chao-Wei Eisenhardt, Peter R. M. Wu, Jingwen Stern, Daniel Assef, Roberto J. Blain, Andrew W. Bridge, Carrie R. Benford, Dominic J. Cutri, Roc M. Griffith, Roger L. Jarrett, Thomas H. Lonsdale, Carol J. Masci, Frank J. Moustakas, Leonidas A. Petty, Sara M. Sayers, Jack Stanford, S. Adam Wright, Edward L. Yan, Lin Leisawitz, David T. Liu, Fengchuan Mainzer, Amy K. McLean, Ian S. Padgett, Deborah L. Skrutskie, Michael F. Gelino, Christopher R. Beichman, Charles A. Juneau, Stephanie TI THE MOST LUMINOUS GALAXIES DISCOVERED BY WISE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; infrared: galaxies; quasars: supermassive black holes ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; DUST-OBSCURED GALAXIES; DIGITAL SKY SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; ADAPTIVE OPTICS SYSTEM; STAR-FORMING GALAXIES; INFRARED GALAXIES; DATA RELEASE; SUBMILLIMETER GALAXIES AB We present 20 Wide-field Infrared Survey Explorer (WISE)-selected galaxies with bolometric luminosities L-bol > 10(14) L-circle dot, including five with infrared luminosities L-IR equivalent to L(rest 8-1000 mu m) > 10(14) L-circle dot. These "extremely luminous infrared galaxies," or ELIRGs, were discovered using the "W1W2-dropout" selection criteria which requires marginal or non-detections at 3.4 and 4.6 mu m (W1 and W2, respectively) but strong detections at 12 and 22 mu m in the WISE survey. Their spectral energy distributions are dominated by emission at rest-frame 4-10 mu m, suggesting that hot dust with T-d similar to 450 K is responsible for the high luminosities. These galaxies are likely powered by highly obscured active galactic nuclei (AGNs), and there is no evidence suggesting these systems are beamed or lensed. We compare this WISE-selected sample with 116 optically selected quasars that reach the same L-bol level, corresponding to the most luminous unobscured quasars in the literature. We find that the rest-frame 5.8 and 7.8 mu m luminosities of the WISE-selected ELIRGs can be 30%-80% higher than that of the unobscured quasars. The existence of AGNs with L-bol > 10(14) L-circle dot at z > 3 suggests that these supermassive black holes are born with large mass, or have very rapid mass assembly. For black hole seed masses similar to 10(3) M-circle dot, either sustained super-Eddington accretion is needed, or the radiative efficiency must be <15%, implying a black hole with slow spin, possibly due to chaotic accretion. C1 [Tsai, Chao-Wei; Eisenhardt, Peter R. M.; Stern, Daniel; Moustakas, Leonidas A.; Liu, Fengchuan; Mainzer, Amy K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wu, Jingwen; Wright, Edward L.; McLean, Ian S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Assef, Roberto J.] Univ Diego Port, Fac Ingn, Nucl Astron, Santiago, Chile. [Blain, Andrew W.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Bridge, Carrie R.; Sayers, Jack] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Benford, Dominic J.; Leisawitz, David T.; Padgett, Deborah L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cutri, Roc M.; Masci, Frank J.; Yan, Lin; Gelino, Christopher R.; Beichman, Charles A.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Griffith, Roger L.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Jarrett, Thomas H.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa. [Lonsdale, Carol J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Petty, Sara M.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Stanford, S. Adam] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Skrutskie, Michael F.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Juneau, Stephanie] CEA Saclay, DSM IRFU SAp, F-91191 Gif Sur Yvette, France. RP Tsai, CW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Chao-Wei.Tsai@jpl.nasa.gov RI Benford, Dominic/D-4760-2012; OI Benford, Dominic/0000-0002-9884-4206; Moustakas, Leonidas/0000-0003-3030-2360 FU National Aeronautics and Space Administration [13-ADAP13-0092]; NASA; W.M. Keck Foundation; NASA Postdoctoral Program at the Jet Propulsion Laboratory; Gemini-CONICYT [32120009] FX The authors thank the anonymous referee for the constructive comments and for encouraging a more thorough discussion of gravitational lensing in this paper. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, and NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology. WISE and NEOWISE are funded by the National Aeronautics and Space Administration. This work is also 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. 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. Part of this research has made use of the Keck Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration. This research has made use of the NASA/IPAC Infrared Science Archive and the NASA/IPAC Extragalactic Database (NED), which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under contracts with the National Aeronautics and Space Administration. This material is based upon work supported by the National Aeronautics and Space Administration under Proposal No. 13-ADAP13-0092 issued through the Astrophysics Data Analysis Program. C.-W. T. was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. R. J. A. was supported by Gemini-CONICYT grant number 32120009. NR 119 TC 29 Z9 29 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2015 VL 805 IS 2 AR 90 DI 10.1088/0004-637X/805/2/90 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400005 ER PT J AU Walton, DJ Reynolds, MT Miller, JM Reis, RC Stern, D Harrison, FA AF Walton, D. J. Reynolds, M. T. Miller, J. M. Reis, R. C. Stern, D. Harrison, F. A. TI BROAD IRON EMISSION FROM GRAVITATIONALLY LENSED QUASARS OBSERVED BY CHANDRA SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: active ID ACTIVE GALACTIC NUCLEI; XMM-NEWTON OBSERVATIONS; SPINNING BLACK-HOLE; X-RAY REFLECTION; EMITTING REGIONS; NGC 4151; ACCRETION; EVOLUTION; LINES; GALAXIES AB Recent work has demonstrated the potential of gravitationally lensed quasars to extend measurements of black hole spin out to high redshift with the current generation of X-ray observatories. Here we present an analysis of a large sample of 27 lensed quasars in the redshift range 1.0 less than or similar to z less than or similar to 4.5 observed with Chandra, utilizing over 1.6 Ms of total observing time, focusing on the rest-frame iron K emission from these sources. Although the X-ray signal-to-noise ratio (S/N) currently available does not permit the detection of iron emission from the inner accretion disk in individual cases in our sample, we find significant structure in the stacked residuals. In addition to the narrow core, seen almost ubiquitously in local active galactic nuclei (AGNs), we find evidence for an additional underlying broad component from the inner accretion disk, with a clear red wing to the emission profile. Based on simulations, we find the detection of this broader component to be significant at greater than the 3 sigma level. This implies that iron emission from the inner disk is relatively common in the population of lensed quasars, and in turn further demonstrates that, with additional observations, this population represents an opportunity to significantly extend the sample of AGN spin measurements out to high redshift. C1 [Walton, D. J.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Walton, D. J.; Harrison, F. A.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Reynolds, M. T.; Miller, J. M.; Reis, R. C.] Univ Michigan, Dept Astron, Ann Arbor, MI 49109 USA. RP Walton, DJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU NASA FX The authors would like to thank the reviewer for providing feedback which helped improve this paper, and Julian Merten for useful discussions. The work of D.J.W./D.S. was performed at JPL/Caltech, under contract with NASA. NR 53 TC 3 Z9 3 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2015 VL 805 IS 2 AR 161 DI 10.1088/0004-637X/805/2/161 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400076 ER PT J AU Luo, T Wang, ZE Ferrare, RA Hostetler, CA Yuan, RM Zhang, DM AF Luo, Tao Wang, Zhien Ferrare, Richard A. Hostetler, Chris A. Yuan, Renmin Zhang, Damao TI Vertically resolved separation of dust and other aerosol types by a new lidar depolarization method SO OPTICS EXPRESS LA English DT Article ID SPECTRAL-RESOLUTION LIDAR; OPTICAL-PROPERTIES; SAHARAN DUST; RETRIEVALS AB This paper developed a new retrieval framework of external mixing of the dust and non-dust aerosol to predict the lidar ratio of the external mixing aerosols and to separate the contributions of non-spherical aerosols by using different depolarization ratios among dust, sea salt, smoke, and polluted aerosols. The detailed sensitivity tests and case study with the new method showed that reliable dust information could be retrieved even without prior information about the non-dust aerosol types. This new method is suitable for global dust retrievals with satellite observations, which is critical for better understanding global dust transportation and for model improvements. (C)2015 Optical Society of America C1 [Luo, Tao; Wang, Zhien; Zhang, Damao] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82070 USA. [Ferrare, Richard A.; Hostetler, Chris A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Luo, Tao; Yuan, Renmin] Univ Sci & Technol China, Sch Earth & Space Sci, Hefei 230031, Anhui, Peoples R China. RP Wang, ZE (reprint author), Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82070 USA. EM zwang@uwyo.edu RI zhang, damao/A-2900-2016; Wang, Zhien/F-4857-2011 OI zhang, damao/0000-0002-3518-292X; FU NASA grant [NNX13AQ41G]; NASA/JPL FX The CALIPSO data set was obtained from the NASA Langley Research Center Atmospheric Science Data Center (eosweb.larc.nasa.gov). The CloudSat 2B-GEOPROF and ECMWF-AUX products were obtained from CloudSat Data Processing Center (cloudsat.cira.colostate.edu). The HSRL data was obtained from NASA (science.larc.nasa.gov/hsrl/). This research was funded by NASA grant NNX13AQ41G and a contract from NASA/JPL. NR 39 TC 1 Z9 1 U1 9 U2 20 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD JUN 1 PY 2015 VL 23 IS 11 BP 14095 EP 14107 DI 10.1364/OE.23.014095 PG 13 WC Optics SC Optics GA CL4DI UT WOS:000356902400069 PM 26072778 ER PT J AU Lin, B Nehrir, AR Harrison, FW Browell, EV Ismail, S Obland, MD Campbell, J Dobler, J Meadows, B Fan, TF Kooi, S AF Lin, Bing Nehrir, Amin R. Harrison, F. Wallace Browell, Edward V. Ismail, Syed Obland, Michael D. Campbell, Joel Dobler, Jeremy Meadows, Byron Fan, Tai-Fang Kooi, Susan TI Atmospheric CO2 column measurements in cloudy conditions using intensity-modulated continuous-wave lidar at 1.57 micron SO OPTICS EXPRESS LA English DT Article ID ABSORPTION AB This study evaluates the capability of atmospheric CO2 column measurements under cloudy conditions using an airborne intensity-modulated continuous-wave integrated-path-differential-absorption lidar operating in the 1.57-mu m CO2 absorption band. The atmospheric CO2 column amounts from the aircraft to the tops of optically thick cumulus clouds and to the surface in the presence of optically thin clouds are retrieved from lidar data obtained during the summer 2011 and spring 2013 flight campaigns, respectively. For the case of intervening thin cirrus clouds with an average cloud optical depth of about 0.16 over an arid/semi-arid area, the CO2 column measurements from 12.2 km altitude were found to be consistent with the cloud free conditions with a lower precision due to the additional optical attenuation of the thin clouds. The clear sky precision for this flight campaign case was about 0.72% for a 0.1-s integration, which was close to previously reported flight campaign results. For a vegetated area and lidar path lengths of 8 to 12 km, the precision of the measured differential absorption optical depths to the surface was 1.3 - 2.2% for 0.1-s integration. The precision of the CO2 column measurements to thick clouds with reflectance about 1/10 of that of the surface was about a factor of 2 to 3 lower than that to the surface owing to weaker lidar returns from clouds and a smaller CO2 differential absorption optical depth compared to that for the entire column. (C) 2015 Optical Society of America C1 [Lin, Bing; Nehrir, Amin R.; Harrison, F. Wallace; Ismail, Syed; Obland, Michael D.; Campbell, Joel; Meadows, Byron] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Browell, Edward V.] NASA, Langley Res Ctr, STARSS II Affiliate, Hampton, VA 23681 USA. [Dobler, Jeremy] Exelis Inc, Ft Wayne, IN 46818 USA. [Fan, Tai-Fang; Kooi, Susan] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. RP Lin, B (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM bing.lin@nasa.gov FU NASA ASCENDS Mission Study and NASA Langley Research Center FX The authors would like to express their appreciation to D. MacDonnell, D. Garber, D. McGregor, and Y. Hu for their valuable comments and encouragement. This research was supported by the NASA ASCENDS Mission Study and NASA Langley Research Center. NR 12 TC 3 Z9 3 U1 3 U2 11 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD JUN 1 PY 2015 VL 23 IS 11 BP A582 EP A593 PG 12 WC Optics SC Optics GA CL4DI UT WOS:000356902400019 PM 26072883 ER PT J AU Jiang, JZ Hofmann, D Jarvis, DJ Fecht, HJ AF Jiang, Jian-Zhong Hofmann, Douglas Jarvis, David John Fecht, Hans-J. TI Low-Density High-Strength Bulk Metallic Glasses and Their Composites: A Review SO ADVANCED ENGINEERING MATERIALS LA English DT Review ID HIGH MECHANICAL STRENGTH; CA-MG-ZN; SUPERCOOLED LIQUID REGION; AMORPHOUS MATRIX COMPOSITES; HIGH-TENSILE STRENGTH; MOLD CASTING METHOD; SHAPED COPPER MOLD; FCC-AL PARTICLES; FORMING ABILITY; THERMAL-STABILITY AB This review gives an overview of the field of low-density (<6gcm(-3)) bulk metallic glasses/composites and their potential engineering and space applications. The review focuses on four systems, Al-, Mg-, Ca-, and Ti-based metallic glass-forming systems. In the following sections, glass forming ability, mechanical properties, thermal stability, and corrosion resistance of the four metallic glass systems and their composites are presented. C1 [Fecht, Hans-J.] Univ Ulm, Inst Micro & Nanomat, Fac Engn & Comp Sci, D-89081 Ulm, Germany. [Jiang, Jian-Zhong] Zhejiang Univ, Dept Mat Sci & Engn, ICNSM, Hangzhou 310027, Zhejiang, Peoples R China. [Jiang, Jian-Zhong] Zhejiang Univ, Lab New Struct Mat, Hangzhou 310027, Zhejiang, Peoples R China. [Hofmann, Douglas] CALTECH, Jet Prop Lab, Engn & Sci Directorate, Pasadena, CA 91109 USA. [Jarvis, David John] ESA ESTEC, Noordwijk, Netherlands. RP Jiang, JZ (reprint author), Zhejiang Univ, Dept Mat Sci & Engn, ICNSM, Hangzhou 310027, Zhejiang, Peoples R China. EM hans.fecht@uni-ulm.de FU European Space Agency ESA (AccMet project); European Space Agency ESA (ThermoLab-ISS); National Key Basic Research Program of China [2012CB825700]; National Natural Science Foundation of China [51371157, 10979002]; Zhejiang University-Helmholtz Cooperation fund; Fundamental Research Funds for the Central Universities; Air Force Office of Scientific Research [RF01152700/PO60020925] FX The authors gratefully acknowledge the useful discussions with Dr. A.L. Greer (University of Cambridge UK) and the technical support by Dr. L. Y. Chen (International Center for New-Structured Materials (ICNSM), Zhejiang University P. R. China), Dr. B. O. Malomo (Department of Mechanical Engineering, Obafemi Awolowo University, Ile-Ife, Nigeria), Dr. R. K. Wunderlich, Dr. K. Bruhne, and Dr. A. Sommer (University of Ulm). The authors like to thank the funding agencies supporting this work, in particular the European Space Agency ESA (AccMet project and ThermoLab-ISS) and the National Key Basic Research Program of China (2012CB825700), National Natural Science Foundation of China (grants 51371157 and 10979002), Zhejiang University-Helmholtz Cooperation fund and the Fundamental Research Funds for the Central Universities. D. H. acknowledges financial support from the Air Force Office of Scientific Research under Grant No. RF01152700/PO60020925. NR 177 TC 5 Z9 5 U1 17 U2 91 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 1438-1656 EI 1527-2648 J9 ADV ENG MATER JI Adv. Eng. Mater. PD JUN PY 2015 VL 17 IS 6 BP 761 EP 780 DI 10.1002/adem.201400252 PG 20 WC Materials Science, Multidisciplinary SC Materials Science GA CK6XQ UT WOS:000356372500004 ER PT J AU Hanisch, RJ Berriman, GB Lazio, TJW Bunn, SE Evans, J McGlynn, TA Plante, R AF Hanisch, R. J. Berriman, G. B. Lazio, T. J. W. Bunn, S. Emery Evans, J. McGlynn, T. A. Plante, R. TI The Virtual Astronomical Observatory: Re-engineering access to astronomical data SO ASTRONOMY AND COMPUTING LA English DT Article DE Catalogs; Surveys; Virtual observatory tools; Data discovery; Data access; Applications ID TOOL; VO; SOFTWARE; SYSTEM; IRIS AB The US Virtual Astronomical Observatory was a software infrastructure and development project designed both to begin the establishment of an operational Virtual Observatory (VU) and to provide the US coordination with the international VU effort. The concept of the VU is to provide the means by which an astronomer is able to discover, access, and process data seamlessly, regardless of its physical location. This paper describes the origins of the VAO, including the predecessor efforts within the US National Virtual Observatory, and summarizes its main accomplishments. These accomplishments include the development of both scripting toolkits that allow scientists to incorporate VU data directly into their reduction and analysis environments and high-level science applications for data discovery, integration, analysis, and catalog cross-comparison. Working with the international community, and based on the experience from the software development, the VAO was a major contributor to international standards within the International Virtual Observatory Alliance. The VAO also demonstrated how an operational virtual observatory could be deployed, providing a robust operational environment in which VU services worldwide were routinely checked for aliveness and compliance with international standards. Finally, the VAO engaged in community outreach, developing a comprehensive web site with on-line tutorials, announcements, links to both US and internationally developed tools and services, and exhibits and hands-on training at annual meetings of the American Astronomical Society and through summer schools and community days. All digital products of the VAO Project, including software, documentation, and tutorials, are stored in a repository for community access. The enduring legacy of the VAO is an increasing expectation that new telescopes and facilities incorporate VU capabilities during the design of their data management systems. Published by Elsevier B.V. C1 [Hanisch, R. J.] Virtual Astron Observ, Washington, DC 20036 USA. [Hanisch, R. J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Berriman, G. B.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bunn, S. Emery] CALTECH, Ctr Adv Comp Res, Pasadena, CA 91125 USA. [Evans, J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [McGlynn, T. A.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Sci Arch Res Ctr, Greenbelt, MD 20771 USA. [Plante, R.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA. RP Lazio, TJW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM robert.hanisch@nist.gov; gbb@ipac.caltech.edu; joseph.lazio@jpl.nasa.gov; janet@cfa.harvard.edu; thomas.a.mcglynn@nasa.gov; rplante@illinois.edu FU National Science Foundation [AST-0834235]; NASA [NNX13AC07G]; NASA/HEASARC; National Aeronautics & Space Administration (NASA) FX The VAO program would not have been possible without the financial support of the National Science Foundation (AST-0834235) and NASA (NNX13AC07G to STScI/MAST), and it was supported NASA/HEASARC. Funding at IPAC has been provided by a grant from the National Aeronautics & Space Administration (NASA) to the Jet Propulsion Laboratory, operated by the California Institute of Technology under contract to NASA. We appreciate the wise guidance of the Board of Directors of the VAO, LLC, and the VAO Science Council, and we are grateful for feedback from the astronomical community that helped us improve our science tools and infrastructure. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 47 TC 3 Z9 3 U1 1 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 2213-1337 EI 2213-1345 J9 ASTRON COMPUT JI Astron. Comput. PD JUN PY 2015 VL 11 SI SI BP 190 EP 209 DI 10.1016/j.ascom.2015.03.007 PN B PG 20 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA CK9FV UT WOS:000356546900015 ER PT J AU Gerakines, PA Hudson, RL AF Gerakines, Perry A. Hudson, Reggie L. TI INFRARED SPECTRA AND OPTICAL CONSTANTS OF ELUSIVE AMORPHOUS METHANE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: abundances; ISM: molecules ID ICES RELEVANT; INTENSITY MEASUREMENTS; INTERSTELLAR ICE; PURE ICES; CH4; MIXTURES; ETHANE; PLUTO; ION; SPECTROSCOPY AB New and accurate laboratory results are reported for amorphous methane (CH4) ice near 10 K for the study of the interstellar medium (ISM) and the outer solar system. Near-and mid-infrared (IR) data, including spectra, band strengths, absorption coefficients, and optical constants, are presented for the first time for this seldom-studied amorphous solid. The apparent IR band strength near 1300 cm(-1) (7.69 mu m) for amorphous CH4 is found to be about 33% higher than the value long used by IR astronomers to convert spectral observations of interstellar CH4 into CH4 abundances. Although CH4 is most likely to be found in an amorphous phase in the ISM, a comparison of results from various laboratory groups shows that the earlier CH4 band strength at 1300 cm(-1) (7.69 mu m) was derived from IR spectra of ices that were either partially or entirely crystalline CH4. Applications of the new amorphous-CH4 results are discussed, and all optical constants are made available in electronic form. C1 [Gerakines, Perry A.; Hudson, Reggie L.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. RP Gerakines, PA (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. EM Reggie.Hudson@NASA.gov RI Gerakines, Perry/D-2226-2012 OI Gerakines, Perry/0000-0002-9667-5904 FU NASA Astrobiology Institute through the Goddard Center for Astrobiology; NASA FX NASA funding through the Outer Planets Research and Cassini Data Analysis programs is acknowledged. Both authors received partial support from the NASA Astrobiology Institute through the Goddard Center for Astrobiology. The experimental assistance of Marla Moore, Mark Loeffler, and Robert Ferrante is acknowledged. NR 35 TC 8 Z9 8 U1 3 U2 13 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 JUN 1 PY 2015 VL 805 IS 2 AR L20 DI 10.1088/2041-8205/805/2/L20 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL0IY UT WOS:000356626900010 ER PT J AU Saito, T Kurita, M Okamoto, H Uchida, I Parker, D Balazs, G AF Saito, Tomomi Kurita, Masanori Okamoto, Hitoshi Uchida, Itaru Parker, Denise Balazs, George TI Tracking Male Loggerhead Turtle Migrations Around Southwestern Japan Using Satellite Telemetry SO CHELONIAN CONSERVATION AND BIOLOGY LA English DT Article DE Reptilia; Testudines: Cheloniidae; Caretta caretta; male; migration; sea surface temperature ID CENTRAL NORTH PACIFIC; CARETTA-CARETTA; SEA-TURTLES; ADULT FEMALE; HABITAT USE; OCEAN AB Three satellite-tagged male loggerhead turtles (Caretta caretta) were released from the coastal waters of Satsuma Peninsula, Kyusyu, southwestern Japan (lat 31 degrees 42'N, long 130 degrees 18'E), and their movements were tracked for up to 449 d. Total distance traveled by the turtles ranged from 1540 to 5519 km. The turtles remained mainly along the coast and islands of the East China Sea and the Sea of Japan, except for spending a brief period of time (1-30 d) in the open ocean. The long-distance movement followed a seasonal pattern, evidently triggered by fluctuations in sea surface temperature. C1 [Saito, Tomomi; Kurita, Masanori; Okamoto, Hitoshi; Uchida, Itaru] Port Nagoya Publ Aquarium, Minato Ku, Nagoya, Aichi 4550033, Japan. [Parker, Denise] Joint Inst Marine & Atmospher Res, Newport, OR 97365 USA. [Balazs, George] NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96818 USA. RP Saito, T (reprint author), Kochi Univ, Usa Marine Biol Inst, Tosa, Kochi 7811164, Japan. EM t-saito@kochi-u.ac.jp; m-kurita@nagoyaminato.or.jp; h-nakamura@nagoyaminato.or.jp; itsahonuworldinhawaii@hotmail.com; Denise.Parker@noaa.gov NR 32 TC 2 Z9 3 U1 7 U2 24 PU CHELONIAN RESEARCH FOUNDATION PI LUNENBURG PA 168 GOODRICH ST., LUNENBURG, MA USA SN 1071-8443 EI 1943-3956 J9 CHELONIAN CONSERV BI JI Chelonian Conserv. Biol. PD JUN PY 2015 VL 14 IS 1 BP 82 EP 87 PG 6 WC Zoology SC Zoology GA CK8ZM UT WOS:000356529000011 ER PT J AU Salas, E Tannenbaum, SI Kozlowski, SWJ Miller, CA Mathieu, JE Vessey, WB AF Salas, Eduardo Tannenbaum, Scott I. Kozlowski, Steve W. J. Miller, Christopher A. Mathieu, John E. Vessey, William B. TI Teams in Space Exploration: A New Frontier for the Science of Team Effectiveness SO CURRENT DIRECTIONS IN PSYCHOLOGICAL SCIENCE LA English DT Article DE teams; teamwork; team training; team cohesion ID DYNAMICS; ORGANIZATIONS; PERFORMANCE; MODELS; METAANALYSIS AB Researchers from a variety of disciplines are currently working with NASA to prepare for human exploration of Mars in the next decades. Such exploration will take scientific discovery to new heights, providing unprecedented information about the geology, atmosphere, and potential for life on Mars, including previous life, current life, and perhaps even our own lives in the future. To make these unparalleled discoveries, however, astronauts will need to undertake a novel and unprecedented journey. Moreover, the mission to Mars will require a team of crew members who will have to endure and sustain team performance requirements never seen before. Multidisciplinary teams of scientists have begun to provide the needed steps to address this challenge. The purpose of this article is (a) to illustrate the kinds of new conceptual frameworks and paradigms needed for teams in space exploration, (b) to delineate promising research paths to ensure that a robust team science can emerge for long-duration space exploration (LDSE), (c) to showcase initial findings and insights from studying astronauts now, and (d) to outline a plan of action for team-effectiveness research in LDSE. C1 [Salas, Eduardo] Rice Univ, Dept Psychol, Houston, TX 77005 USA. [Tannenbaum, Scott I.] Grp Org Effectiveness, Albany, NY USA. [Kozlowski, Steve W. J.] Michigan State Univ, Dept Psychol, E Lansing, MI 48824 USA. [Miller, Christopher A.] Smart Informat Flow Technol, Minneapolis, MN USA. [Mathieu, John E.] Univ Connecticut, Dept Management, Storrs, CT USA. [Vessey, William B.] NASA Johnson Space Ctr, Wyle Sci Technol & Engn Grp, Houston, TX USA. RP Salas, E (reprint author), Rice Univ, Dept Psychol, MS-25,Sewall Hall 464, Houston, TX 77005 USA. EM esalas@ist.ucf.edu OI KOZLOWSKI, STEVE/0000-0002-5123-3424 NR 60 TC 5 Z9 5 U1 3 U2 19 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 0963-7214 EI 1467-8721 J9 CURR DIR PSYCHOL SCI JI Curr. Dir. Psychol. PD JUN PY 2015 VL 24 IS 3 BP 200 EP 207 DI 10.1177/0963721414566448 PG 8 WC Psychology, Multidisciplinary SC Psychology GA CK6AH UT WOS:000356309600007 ER PT J AU Chan, C Albright, S Gorius, N Brasunas, J Jennings, D Flasar, FM Carlson, R Guandique, E Nixon, C AF Chan, Cheong Albright, Shane Gorius, Nicolas Brasunas, John Jennings, Don Flasar, F. Michael Carlson, Ronald Guandique, Ever Nixon, Conor TI Electrical interferences observed in the Cassini CIRS spectrometer SO EXPERIMENTAL ASTRONOMY LA English DT Article DE Fourier transform spectrometer; Electrical noise; Engineering; Spacecraft instrumentation AB The Composite Infrared Spectrometer (CIRS) carried onboard the Cassini spacecraft has now operated successfully for 17 years, following launch in 1997. Following insertion into Saturnian orbit in July 2004, the instrument has taken data nearly continuously, returning over 100 million interferograms (spectra) to date. Although of generally high quality, and resulting in more than 100 peer-reviewed scientific articles, the spectra are afflicted with several types of instrumental electrical (non-random) noise artifacts. These noise artifacts require either mitigation strategies (prevention), removal from the observed data, or else awareness of the affected spectral areas which must be excluded from scientific analysis. The sources and nature of these varied noise types were not readily identified until after launch. The purpose of this article is to inform users of the noise in the CIRS dataset and to serve as a 'lesson-learned' guide for designers of future instruments. C1 [Chan, Cheong; Albright, Shane; Gorius, Nicolas; Brasunas, John; Jennings, Don; Flasar, F. Michael] NASA, Goddard Space Flight Ctr, Sch Aerosp Engn, Atlanta, GA 30332 USA. [Carlson, Ronald; Guandique, Ever; Nixon, Conor] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Guandique, Ever] ADNET Syst Inc, Bethesda, MD 20817 USA. RP Chan, C (reprint author), NASA, Goddard Space Flight Ctr, Sch Aerosp Engn, Atlanta, GA 30332 USA. EM cheongyuchan@gmail.com; conor.a.nixon@nasa.gov RI Flasar, F Michael/C-8509-2012; Nixon, Conor/A-8531-2009 OI Nixon, Conor/0000-0001-9540-9121 FU NASA Education office FX The authors would like to thank the CIRS team for their cooperation and the NASA Education office for funding the internship. NR 33 TC 1 Z9 1 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0922-6435 EI 1572-9508 J9 EXP ASTRON JI Exp. Astron. PD JUN PY 2015 VL 39 IS 2 BP 367 EP 386 DI 10.1007/s10686-015-9452-3 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6VA UT WOS:000356365200009 ER PT J AU Lai, QZ Wu, LG She, CL AF Lai Qiao-zhen Wu Li-guang She Chung-lin TI SEA SURFACE TEMPERATURE RESPONSE TO TYPHOON MORAKOT (2009) AND ITS INFLUENCE SO JOURNAL OF TROPICAL METEOROLOGY LA English DT Article DE sea surface temperature; typhoon; ocean response; typhoon track forecast ID TROPICAL CYCLONE; HURRICANE; MODEL; SIMULATIONS; INTENSITY; PACIFIC; LAYER AB While previous studies indicate that typhoons can decrease sea surface temperature (SST) along their tracks, a few studies suggest that the cooling patterns in coastal areas are different from those in the open sea. However, little is known about how the induced cooling coupled with the complex ocean circulation in the coastal areas can affect tropical cyclone track and intensity. The sea surface responses to the land falling process of Typhoon Morakot (2009) are examined observationally and its influences on the activity of the typhoon are numerically simulated with the WRF model. The present study shows that the maximum SST cooling associated with Morakot occurred on the left-hand side of the typhoon track during its landfall. Numerical simulations show that, together with the SST gradients associated with the coastal upwelling and mesoscale oceanic vortices, the resulting SST cooling can cause significant difference in the typhoon track, comparable to the current 24-hour track forecasting error. It is strongly suggested that it is essential to include the non-uniform SST distribution in the coastal areas for further improvement in typhoon track forecast. C1 [Lai Qiao-zhen] Longyan Meteorol Off Fujian Prov, Longyan 364000, Peoples R China. [Wu Li-guang] Nanjing Univ Informat Sci & Technol, Minist Educ, Key Lab Meteorol Disaster, Nanjing 210044, Jiangsu, Peoples R China. [She Chung-lin] NASA, Goddard Space Flight Ctr, UMBC Goddard Earth & Sci Technol Ctr, Greenbelt, MD 20771 USA. RP Wu, LG (reprint author), Nanjing Univ Informat Sci & Technol, Minist Educ, Key Lab Meteorol Disaster, Nanjing 210044, Jiangsu, Peoples R China. EM liguang@nuist.edu.cn FU National Key Technology Research and Development Program of China [2009CB421503]; New Recruitment Graduate Project of the Fujian Province Meteorological Bureau [2012G01] FX Foundation item: National Key Technology Research and Development Program of China (2009CB421503); New Recruitment Graduate Project of the Fujian Province Meteorological Bureau (2012G01) NR 25 TC 0 Z9 0 U1 3 U2 8 PU JOURNAL OF TROPICAL METEOROLOGICAL PRESS PI GUANGZHOU PA 6 FU JIN RD, GUANGZHOU, 510080, PEOPLES R CHINA SN 1006-8775 J9 J TROP METEOROL JI J. Trop. Meteorol. PD JUN PY 2015 VL 21 IS 2 BP 111 EP 120 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CK9KA UT WOS:000356557800002 ER PT J AU Kokhanovsky, AA Davis, AB Cairns, B Dubovik, O Hasekamp, OP Sano, I Mukai, S Rozanov, VV Litvinov, P Lapyonok, T Kolomiets, IS Oberemok, YA Savenkov, S Martin, W Wasilewski, A Di Noia, A Stap, FA Rietjens, J Xu, F Natraj, V Duan, M Cheng, T Munro, R AF Kokhanovsky, A. A. Davis, A. B. Cairns, B. Dubovik, O. Hasekamp, O. P. Sano, I. Mukai, S. Rozanov, V. V. Litvinov, P. Lapyonok, T. Kolomiets, I. S. Oberemok, Y. A. Savenkov, S. Martin, W. Wasilewski, A. Di Noia, A. Stap, F. A. Rietjens, J. Xu, F. Natraj, V. Duan, M. Cheng, T. Munro, R. TI Space-based remote sensing of atmospheric aerosols: The multi-angle spectro-polarimetric frontier SO EARTH-SCIENCE REVIEWS LA English DT Article DE Aerosol; Remote sensing; Polarimetry; Optical instrumentation; Radiative transfer; Climate change ID VECTOR RADIATIVE-TRANSFER; MARKOV-CHAIN FORMALISM; CLOUD-TOP PRESSURE; OXYGEN-A-BAND; BIDIRECTIONAL REFLECTANCE MODEL; MOLECULAR LINE ABSORPTION; SKY RADIANCE MEASUREMENTS; POINT-SPREAD FUNCTION; DISCRETE RANDOM-MEDIA; OPTICAL-PROPERTIES AB The review of optical instrumentation, forward modeling, and inverse problem solution for the polarimetric aerosol remote sensing from space is presented. The special emphasis is given to the description of current airborne and satellite imaging polarimeters and also to modern satellite aerosol retrieval algorithms based on the measurements of the Stokes vector of reflected solar light as detected on a satellite. Various underlying surface reflectance models are discussed and evaluated. (C) 2015 Elsevier B.V. All rights reserved. C1 [Kokhanovsky, A. A.; Munro, R.] EUMETSAT, D-64367 Darmstadt, Germany. [Davis, A. B.; Xu, F.; Natraj, V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cairns, B.; Martin, W.; Wasilewski, A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Dubovik, O.; Litvinov, P.; Lapyonok, T.] Univ Lille 1, CNRS, Lab Opt Atmospher, Lille, France. [Hasekamp, O. P.; Di Noia, A.; Stap, F. A.; Rietjens, J.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Sano, I.] Kinki Univ, Fac Sci & Technol, Higashiosaka, Osaka 6778502, Japan. [Mukai, S.] Kyoto Coll Grad Studies Informat, Sakyo Ku, Kyoto 6068225, Japan. [Rozanov, V. V.] Univ Bremen, Inst Remote Sensing, D-28359 Bremen, Germany. [Kolomiets, I. S.; Oberemok, Y. A.; Savenkov, S.] Kiev Taras Shevchenko Univ, Radiophys Dept, UA-01601 Kiev, Ukraine. [Duan, M.] Chinese Acad Sci, Inst Atmospher Phys, Beijing, Peoples R China. [Duan, M.; Cheng, T.] Chinese Acad Sci, Inst Remote Sensing & Digital Earth RADI, Beijing, Peoples R China. [Stap, F. A.] Univ Utrecht, Inst Marine & Atmospher Res, NL-3508 TA Utrecht, Netherlands. RP Kokhanovsky, AA (reprint author), EUMETSAT, Eumetsat Allee 1, D-64367 Darmstadt, Germany. EM Alexander.kokhanovsky@eumetsat.int RI Cheng, Tianhai/H-1113-2013; Kokhanovsky, Alexander/C-6234-2016; Xu, Feng/G-3673-2013; OI Cheng, Tianhai/0000-0001-7889-9579; Kokhanovsky, Alexander/0000-0001-7370-1164; Cairns, Brian/0000-0002-1980-1022; Di Noia, Antonio/0000-0002-5052-0763 FU International Space Science Institute (ISSI) in Bern (Switzerland); EUMETSAT; JAXA's Global Change Observation Mission - Climate 1 (GCOM-C1) [JX-PSPC-40059]; JSPS KAKENHI [25340019]; NASA; ESA; DFG; SRON; CNRS; Bremen University; Lille University FX This work was supported financially by the International Space Science Institute (ISSI) in Bern (Switzerland), by EUMETSAT, by JAXA's Global Change Observation Mission - Climate 1 (GCOM-C1) project (JX-PSPC-40059), by JSPS KAKENHI (25340019), and by NASA, ESA, DFG, SRON, CNRS, as well as Bremen University and Lille University. The authors extend special thanks to Vladimir Budak, Dave Diner, Mike Garay, Ya. Ilyushin, Ralph Kahn, Olga Kalashnikova, Rob Levy, Anton Lopatin, John Martonchik, Michael Mishchenko, Lorraine Remer, Felix Seidel, Robert Spurr, Knut Stamnes, Didier Tanre, and Elenora Zege for the many useful discussions related to the topic of this paper, at ISSI and elsewhere. We thank K. Tanaka and H. Murakami of the JAXA (Japan) for providing us with detailed information about S-GLI. Part of this research was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 221 TC 10 Z9 11 U1 8 U2 23 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 JUN PY 2015 VL 145 BP 85 EP 116 DI 10.1016/j.earscirev.2015.01.012 PG 32 WC Geosciences, Multidisciplinary SC Geology GA CK0HC UT WOS:000355885300007 ER PT J AU Seager, R Hooks, A Williams, AP Cook, B Nakamura, J Henderson, N AF Seager, Richard Hooks, Allison Williams, A. Park Cook, Benjamin Nakamura, Jennifer Henderson, Naomi TI Climatology, Variability, and Trends in the US Vapor Pressure Deficit, an Important Fire-Related Meteorological Quantity* SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID WESTERN UNITED-STATES; DATA ASSIMILATION SYSTEM; NORTH-AMERICA; WILDFIRE; DROUGHT; FORESTS; US; TEMPERATURE; MECHANISMS; REANALYSIS AB Unlike the commonly used relative humidity, vapor pressure deficit (VPD) is an absolute measure of the difference between the water vapor content of the air and its saturation value and an accurate metric of the ability of the atmosphere to extract moisture from the land surface. VPD has been shown to be closely related to variability in burned forest areas in the western United States. Here, the climatology, variability, and trends in VPD across the United States are presented. VPD reaches its climatological maximum in summer in the interior southwest United States because of both high temperatures and low vapor pressure under the influence of the northerly, subsiding eastern flank of the Pacific subtropical anticyclone. Maxima of variance of VPD are identified in the Southwest and southern plains in spring and summer and are to a large extent driven by temperature variance, but vapor pressure variance is also important in the Southwest. La Nina-induced circulation anomalies cause subsiding, northerly flow that drives down actual vapor pressure and increases saturation vapor pressure from fall through spring. High spring and summer VPDs can also be caused by reduced precipitation in preceding months, as measured by Bowen ratio anomalies. Case studies of 2002 (the Rodeo-Chediski and Hayman fires, which occurred in Arizona and Colorado, respectively) and 2007 (the Murphy Complex fire, which occurred in Idaho and Nevada) show very high VPDs caused by antecedent surface drying and subsidence warming and drying of the atmosphere. VPD has increased in the southwest United States since 1961, driven by warming and a drop in actual vapor pressure, but has decreased in the northern plains and Midwest, driven by an increase in actual vapor pressure. C1 [Seager, Richard; Williams, A. Park; Nakamura, Jennifer; Henderson, Naomi] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Hooks, Allison] Columbia Univ, Columbia Coll, New York, NY USA. [Cook, Benjamin] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Seager, R (reprint author), Columbia Univ, Lamont Doherty Earth Observ, 61 Rte 9W, Palisades, NY 10964 USA. EM seager@ldeo.columbia.edu RI Cook, Benjamin/H-2265-2012; Williams, Park/B-8214-2016 OI Williams, Park/0000-0001-8176-8166 FU NSF [AGS-1243204]; Earth Institute at Columbia University undergraduate research internship FX This work was supported by NSF Award AGS-1243204 (Linking Near-term Future Changes in Weather and Hydroclimate in Western North America to Adaptation for Ecosystem and Water Management). Author AH was supported by an Earth Institute at Columbia University undergraduate research internship. The GLDAS data used in this study were acquired as part of NASA's Earth-Sun System Division and were archived and distributed by the Goddard Earth Sciences (GES) Data and Information Services Center (DISC) Distributed Active Archive Center (DAAC). We thank three reviewers for their helpful comments and criticisms. NR 43 TC 9 Z9 9 U1 7 U2 26 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 JUN PY 2015 VL 54 IS 6 BP 1121 EP 1141 DI 10.1175/JAMC-D-14-0321.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CK6VY UT WOS:000356367900001 ER PT J AU Leppert, KD Cecil, DJ AF Leppert, Kenneth D., II Cecil, Daniel J. TI Signatures of Hydrometeor Species from Airborne Passive Microwave Data for Frequencies 10-183 GHz SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID PHYSICAL PRECIPITATION RETRIEVAL; MESOSCALE CONVECTIVE SYSTEMS; CLOUD-RADIATION MODEL; POLARIMETRIC RADAR; SATELLITE MEASUREMENTS; VIDEO DISDROMETER; ICE CLOUDS; RAIN; CLASSIFICATION; IDENTIFICATION AB Passive microwave brightness temperatures (BTs) collected above severe thunderstorms using the Advanced Microwave Precipitation Radiometer and Conical Scanning Millimeter-Wave Imaging Radiometer during the Midlatitude Continental Convective Clouds Experiment are compared with a hydrometeor identification applied to dual-polarimetric Weather Surveillance Radar-1988 Doppler radar data collected at Vance Air Force Base, Oklahoma (KVNX). The goal of this work is to determine the signatures of various hydrometeor species in terms of BTs measured at frequencies used by the Global Precipitation Measurement mission Microwave Imager. Results indicate that hail is associated with an ice-scattering signature at all frequencies examined, including 10.7 GHz. However, it appears that frequencies <= 37.1 GHz are most useful for identifying hail. Low-level (below 2.5 km) hail becomes probable for a BT below 240 K at 19.4 GHz, 170 K at 37.1 GHz, 90 K at 85.5 GHz, 80 K at 89.0 GHz, 100 K at 165.5 GHz, and 100 K at 183.3 +/- 7 GHz. Graupel may be distinguished from hail and profiles without any hydrometeor species by its strong scattering signature at higher frequencies (e.g., 165.5 GHz) and its relative lack of scattering at frequencies <= 19.4 GHz. There is a clearer distinction between profiles that contain liquid precipitation and profiles without any hydrometeors when the liquid is associated above with hail and/or graupel (i.e., a hydrometeor category with a strong scattering signature) than when the liquid is associated with smaller ice. Near-surface precipitation is much more likely for a 19.4-GHz BT < 250 K, 37.1-GHz BT < 240 K, 89.0-GHz BT < 220 K, and 165.5-GHz BT < 140 K. C1 [Leppert, Kenneth D., II] Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35899 USA. [Cecil, Daniel J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Leppert, KD (reprint author), NSSTC, Rm 4074,320 Sparkman Dr, Huntsville, AL 35805 USA. EM leppert@nsstc.uah.edu RI Measurement, Global/C-4698-2015 FU NASA Precipitation Measurement Missions Science Team FX Funding for this research was generously provided through the NASA Precipitation Measurement Missions Science Team. The authors thank Dr. Brenda Dolan for providing the code used for the hydrometeor identification and her help in running the code. The authors also thank Dr. Timothy Lang for his helpful suggestions for this work and three anonymous reviewers for providing thoughtful and helpful suggestions for improving the manuscript. In addition, the authors gratefully acknowledge the NASA EOSDIS Global Hydrology Resource Center DAAC for providing the AMPR, CoSMIR, and KVNX radar data. NR 36 TC 4 Z9 4 U1 2 U2 5 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 JUN PY 2015 VL 54 IS 6 BP 1313 EP 1334 DI 10.1175/JAMC-D-14-0145.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CK6VY UT WOS:000356367900013 ER PT J AU Carey, LD Petersen, WA AF Carey, Lawrence D. Petersen, Walter A. TI Sensitivity of C-Band Polarimetric Radar-Based Drop Size Estimates to Maximum Diameter SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID DUAL-POLARIZATION RADAR; 2D VIDEO DISDROMETER; SMALL RAINDROP DISTORTION; AXIS RATIOS; DIFFERENTIAL REFLECTIVITY; LABORATORY MEASUREMENTS; DISTRIBUTION TRUNCATION; DISTRIBUTION PARAMETERS; DISTRIBUTION RETRIEVAL; RAINFALL ESTIMATION AB Estimating raindrop size has been a long-standing objective of polarimetric radar-based precipitation retrieval methods. The relationship between the differential reflectivity Z(dr) and the median volume diameter D-0 is typically derived empirically using raindrop size distribution observations from a disdrometer, a raindrop physical model, and a radar scattering model. Because disdrometers are known to undersample large raindrops, the maximum drop diameter D-max is often an assumed parameter in the rain physical model. C-band Z(dr) is sensitive to resonance scattering at drop diameters larger than 5 mm, which falls in the region of uncertainty for D-max. Prior studies have not accounted for resonance scattering at C band and D-max uncertainty in assessing potential errors in drop size retrievals. As such, a series of experiments are conducted that evaluate the effect of D-max parameterization on the retrieval error of D-0 from a fourth-order polynomial function of C-band Z(dr) by varying the assumed D-max through the range of assumptions found in the literature. Normalized bias errors for estimating D-0 from C-band Z(dr) range from -8% to 15%, depending on the postulated error in D-max. The absolute normalized bias error increases with C-band Z(dr), can reach 10% for Z(dr) as low as 1-1.75 dB, and can increase from there to values as large as 15%-45% for larger Z(dr), which is a larger potential bias error than is found at S and X band. Uncertainty in D-max assumptions and the associated potential D-0 retrieval errors should be noted and accounted for in future C-band polarimetric radar studies. C1 [Carey, Lawrence D.] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA. [Petersen, Walter A.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. RP Carey, LD (reprint author), Univ Alabama, Dept Atmospher Sci, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM larry.carey@nsstc.uah.edu FU NASA [NNM05AA22A, NNM11AA01A, NNX13AI89G] FX This research is funded by Dr. Ramesh Kakar, NASA Precipitation Measurement Mission (PMM), Dr. Gail Skofronick-Jackson, NASA GPM Project Scientist, and Dr. Mathew Schwaller, NASA GPM Project Office under the following NASA Contracts: NNM05AA22A, NNM11AA01A, and NNX13AI89G. We also acknowledge the late Dr. Arthur Hou, whose leadership as the former NASA GPM Project Scientist was essential to the success of the GPM program and the realization of this study. We thank Patrick Gatlin, Matt Wingo, and Chris Schultz for their careful operation and maintenance of the 2DVD units at the NSSTC berm in Huntsville over many years. We thank Dr. V. N. Bringi for the use of the CSU 2DVD data, close collaboration, scientific leadership in the retrieval of raindrop characteristics from polarimetric radar, and his insight into this research. We acknowledge the many members of the NASA PMM DSD Working Group who have provided ideas, insightful comments, and encouragement during the conduct of this research, including Mr. Patrick Gatlin, Dr. Ali Tokay, Dr. Merhala Thurai, and Dr. Chris Williams. Constructive comments from four anonymous reviewers greatly improved the clarity of the text and figures. NR 67 TC 4 Z9 4 U1 3 U2 6 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 JUN PY 2015 VL 54 IS 6 BP 1352 EP 1371 DI 10.1175/JAMC-D-14-0079.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CK6VY UT WOS:000356367900015 ER PT J AU Rutan, DA Kato, S Doelling, DR Rose, FG Nguyen, LT Caldwell, TE Loeb, NG AF Rutan, David A. Kato, Seiji Doelling, David R. Rose, Fred G. Le Trang Nguyen Caldwell, Thomas E. Loeb, Norman G. TI CERES Synoptic Product: Methodology and Validation of Surface Radiant Flux SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID RESEARCH MOORED ARRAY; ENERGY SYSTEM CERES; DIURNAL-VARIATIONS; RADIATIVE PROPERTIES; CLEAR SKIES; ISCCP DATA; CLOUD; IRRADIANCE; MODEL; TOP AB The Clouds and the Earth's Radiant Energy System Synoptic (SYN1deg), edition 3, product provides climate-quality global 3-hourly 1 degrees x 1 degrees gridded top of atmosphere, in-atmosphere, and surface radiant fluxes. The in-atmosphere surface fluxes are computed hourly using a radiative transfer code based upon inputs from Terra and Aqua Moderate Resolution Imaging Spectroradiometer (MODIS), 3-hourly geostationary (GEO) data, and meteorological assimilation data from the Goddard Earth Observing System. The GEO visible and infrared imager calibration is tied to MODIS to ensure uniform MODIS-like cloud properties across all satellite cloud datasets. Computed surface radiant fluxes are compared to surface observations at 85 globally distributed land (37) and ocean buoy (48) sites as well as several other publicly available global surface radiant flux data products. Computed monthly mean downward fluxes from SYN1deg have a bias (standard deviation) of 3.0 W m(-2) (5.7%) for shortwave and -4.0 W m(-2) (2.9%) for longwave compared to surface observations. The standard deviation between surface downward shortwave flux calculations and observations at the 3-hourly time scale is reduced when the diurnal cycle of cloud changes is explicitly accounted for. The improvement is smaller for surface downward longwave flux owing to an additional sensitivity to boundary layer temperature/humidity, which has a weaker diurnal cycle compared to clouds. C1 [Rutan, David A.; Rose, Fred G.; Le Trang Nguyen; Caldwell, Thomas E.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Kato, Seiji; Doelling, David R.; Loeb, Norman G.] SSAI, Hampton, VA USA. RP Rutan, DA (reprint author), Sci Syst & Applicat Inc, 1 Enterprise Pkwy,Suite 200, Hampton, VA 23666 USA. EM david.a.rutan@nasa.gov FU NASA CERES project FX This work was funded by the NASA CERES project. The products and the validation could not have been accomplished without the help of the CERES TISA team. Data were obtained from the NASA Langley Research Center EOSDIS Distributed Active Archive Center. We also wish to acknowledge the hard work by the many dedicated scientists maintaining surface instrumentation in diverse climates to obtain high-quality observations of downwelling shortwave and longwave surface flux. Those groups are noted in appendix B. We also thank the reviewers, whose close read of the paper greatly improved the end result. NR 57 TC 15 Z9 15 U1 6 U2 20 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 JUN PY 2015 VL 32 IS 6 BP 1121 EP 1143 DI 10.1175/JTECH-D-14-00165.1 PG 23 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA CK6WN UT WOS:000356369500001 ER PT J AU Marvel, K Zelinka, M Klein, SA Bonfils, C Caldwell, P Doutriaux, C Santer, BD Taylor, KE AF Marvel, Kate Zelinka, Mark Klein, Stephen A. Bonfils, Celine Caldwell, Peter Doutriaux, Charles Santer, Benjamin D. Taylor, Karl E. TI External Influences on Modeled and Observed Cloud Trends SO JOURNAL OF CLIMATE LA English DT Article ID 20TH-CENTURY TEMPERATURE; ATMOSPHERIC CIRCULATION; GENERAL-CIRCULATION; FEEDBACK PROCESSES; CLIMATE-CHANGE; TROPICAL BELT; OCEAN; ISCCP; PACIFIC; CMIP5 AB Understanding the cloud response to external forcing is a major challenge for climate science. This crucial goal is complicated by intermodel differences in simulating present and future cloud cover and by observational uncertainty. This is the first formal detection and attribution study of cloud changes over the satellite era. Presented herein are CMIP5 model-derived fingerprints of externally forced changes to three cloud properties: the latitudes at which the zonally averaged total cloud fraction (CLT) is maximized or minimized, the zonal average CLT at these latitudes, and the height of high clouds at these latitudes. By considering simultaneous changes in all three properties, the authors define a coherent multivariate fingerprint of cloud response to external forcing and use models from phase 5 of CMIP (CMIP5) to calculate the average time to detect these changes. It is found that given perfect satellite cloud observations beginning in 1983, the models indicate that a detectable multivariate signal should have already emerged. A search is then made for signals of external forcing in two observational datasets: ISCCP and PATMOS-x. The datasets are both found to show a poleward migration of the zonal CLT pattern that is incompatible with forced CMIP5 models. Nevertheless, a detectable multivariate signal is predicted by models over the PATMOS-x time period and is indeed present in the dataset. Despite persistent observational uncertainties, these results present a strong case for continued efforts to improve these existing satellite observations, in addition to planning for new missions. C1 [Marvel, Kate; Zelinka, Mark; Klein, Stephen A.; Bonfils, Celine; Caldwell, Peter; Doutriaux, Charles; Santer, Benjamin D.; Taylor, Karl E.] Lawrence Livermore Natl Lab, Livermore, CA USA. [Marvel, Kate] Columbia Univ, NASA Goddard Inst Space Studies, New York, NY 10025 USA. [Marvel, Kate] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA. RP Marvel, K (reprint author), Columbia Univ, NASA Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM katherine.d.marvel@nasa.gov RI Taylor, Karl/F-7290-2011; Santer, Benjamin/F-9781-2011; Klein, Stephen/H-4337-2016; Zelinka, Mark/C-4627-2011 OI Taylor, Karl/0000-0002-6491-2135; Klein, Stephen/0000-0002-5476-858X; Zelinka, Mark/0000-0002-6570-5445 FU Regional and Global Climate Modeling Program of the U.S. Department of Energy (DOE) Office of Science; DOE Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; Laboratory Directed Research and Development award [13-ERD-032]; DOE/OBER Early Career Research Program [SCW1295] FX CMIP5 data processing was enabled by the CDAT analysis package. The EOF analysis was performed using the eofs software package available from http://ajdawson.github.io/eofs/. This work was supported by the Regional and Global Climate Modeling Program of the U.S. Department of Energy (DOE) Office of Science and was performed under the auspices of the DOE Lawrence Livermore National Laboratory (Contract DE-AC52-07NA27344). KM was supported by a Laboratory Directed Research and Development award (13-ERD-032). CB was supported by the DOE/OBER Early Career Research Program Award SCW1295. We acknowledge the World Climate Research Programme's Working Group on Coupled Modelling, which is responsible for CMIP, and we thank the climate modeling groups (listed in Table A1 of this paper) for producing and making available their model output. For CMIP the U.S. Department of Energy's Program for Climate Model Diagnosis and Intercomparison provides coordinating support and led development of software infrastructure in partnership with the Global Organization for Earth System Science Portals. NR 66 TC 3 Z9 3 U1 1 U2 17 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 JUN PY 2015 VL 28 IS 12 BP 4820 EP 4840 DI 10.1175/JCLI-D-14-00734.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CK5RR UT WOS:000356283900012 ER PT J AU Orbe, C Newman, PA Waugh, DW Holzer, M Oman, LD Li, F Polvani, LM AF Orbe, Clara Newman, Paul A. Waugh, Darryn W. Holzer, Mark Oman, Luke D. Li, Feng Polvani, Lorenzo M. TI Airmass Origin in the Arctic. Part I: Seasonality SO JOURNAL OF CLIMATE LA English DT Article ID WARM CONVEYOR BELTS; AIR-POLLUTION; STORM TRACKS; TROPOSPHERIC TRANSPORT; GLOBAL CLIMATOLOGY; WATER-VAPOR; STRATOSPHERE; ANTICYCLONE; TROPOPAUSE; EXCHANGE AB The first climatology of airmass origin in the Arctic is presented in terms of rigorously defined airmass fractions that partition air according to where it last contacted the planetary boundary layer (PBL). Results from a present-day climate integration of the Goddard Earth Observing System Chemistry-Climate Model (GEOSCCM) reveal that the majority of air in the Arctic below 700 mb last contacted the PBL poleward of 60 degrees N. By comparison, 62% (+/- 0.8%) of the air above 700 mb originates over Northern Hemisphere midlatitudes (i.e., "midlatitude air"). Seasonal variations in the airmass fractions above 700 mb reveal that during boreal winter air from midlatitudes originates primarily over the oceans, with 26% (+/- 1.9%) last contacting the PBL over the eastern Pacific, 21% (+/- 0.87%) over the Atlantic, and 16% (+/- 1.2%) over the western Pacific. During summer, by comparison, midlatitude air originates primarily over land, overwhelmingly so over Asia [41% (+/- 1.0%)] and, to a lesser extent, over North America [24% (+/- 1.5%)]. Seasonal variations in the airmass fractions are interpreted in terms of changes in the large-scale ventilation of the midlatitude boundary layer and the midlatitude tropospheric jet. C1 [Orbe, Clara; Newman, Paul A.; Oman, Luke D.] NASA, Goddard Space Flight Ctr, Lab Atmospher Chem & Dynam, Greenbelt, MD 20771 USA. [Waugh, Darryn W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Holzer, Mark; Polvani, Lorenzo M.] Univ New S Wales, Sch Math & Stat, Dept Appl Math, Sydney, NSW, Australia. [Holzer, Mark] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. [Li, Feng] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA. [Polvani, Lorenzo M.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. RP Orbe, C (reprint author), NASA, Goddard Space Flight Ctr, Lab Atmospher Chem & Dynam, Greenbelt, MD 20771 USA. EM clara.orbe@nasa.gov RI Oman, Luke/C-2778-2009; Waugh, Darryn/K-3688-2016 OI Oman, Luke/0000-0002-5487-2598; Waugh, Darryn/0000-0001-7692-2798 FU NASA; ARC [DP120100674]; NSF [AGS-1403676, AGS-1402931] FX This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. The authors also acknowledge support from ARC Grant DP120100674 (M.H.) and NSF Grants AGS-1403676 (D.W.) and AGS-1402931 (M.H. and L.M.P.). NR 66 TC 5 Z9 5 U1 3 U2 9 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 JUN PY 2015 VL 28 IS 12 BP 4997 EP 5014 DI 10.1175/JCLI-D-14-00720.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CK5RR UT WOS:000356283900023 ER PT J AU Thomas, BF Vogel, RM Famiglietti, JS AF Thomas, Brian F. Vogel, Richard M. Famiglietti, James S. TI Objective hydrograph baseflow recession analysis SO JOURNAL OF HYDROLOGY LA English DT Article DE Hydromorphology; Groundwater/surface water interaction; Quantile regression; Numerical derivative; Linear reservoir; Water withdrawal ID SMOOTHING NOISY DATA; SPLINE FUNCTIONS; FLOW RECESSION; STREAMFLOW; HYDROLOGY; WATER; RAINFALL; SYSTEMS; STORAGE; CURVES AB A streamflow hydrograph recession curve expresses the theoretical relationship between aquifer structure and groundwater outflow to a stream channel. That theoretical relationship is often portrayed empirically using a recession plot defined as a plot of ln(-dQ/dt) versus ln(Q), where Q is streamflow discharge. Such hydrograph recession plots are commonly used to estimate recession parameters, aquifer properties and for evaluating alternative hydrologic hypotheses. We introduce a comprehensive and objective approach to analyze baseflow recessions with innovations including the use of quantile regression, efficient and objective numerical estimation of dQ/dt, inclusion of groundwater withdrawals, and incorporation of seasonal effects. We document that these innovations when all combined, lead to significant improvements, over previous studies, in our ability to discern the theoretical behavior of stream aquifer systems. A case study reveals that our methodology enables us to reject the simple linear reservoir hypothesis of stream aquifer interactions for watersheds in New Jersey and results in improved correlations between low flow statistics and aquifer properties for those same watersheds. (C) 2015 Elsevier B.V. All rights reserved. C1 [Thomas, Brian F.; Famiglietti, James S.] Univ Calif Irvine, Ctr Hydrol Modeling, Irvine, CA 92697 USA. [Thomas, Brian F.; Famiglietti, James S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Thomas, Brian F.; Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Vogel, Richard M.] Tufts Univ, Dept Civil & Environm Engn, Medford, MA 02155 USA. [Famiglietti, James S.] Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA 92697 USA. RP Thomas, BF (reprint author), 4800 Oak Grove Dr,Mail Stop 300-329, Pasadena, CA 91109 USA. EM Brian.F.Thomas@jpl.nasa.gov RI Vogel, Richard/A-8513-2008 OI Vogel, Richard/0000-0001-9759-0024 FU Tufts Institute for the Environment (TIE); University of California Office of the President Multicampus Research and Programs Initiative; National Aeronautics and Space Administration FX Project support was provided by a fellowship awarded to the first author by the Tufts Institute for the Environment (TIE); and by the University of California Office of the President Multicampus Research and Programs Initiative. A portion 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. The authors also express their appreciation to Charles Kroll for helpful comments, two anonymous reviewers and Editor Peter Kitanidis whose comments contributed to substantial improvements to the original manuscript. NR 70 TC 5 Z9 5 U1 5 U2 26 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 JUN PY 2015 VL 525 BP 102 EP 112 DI 10.1016/j.jhydrol.2015.03.028 PG 11 WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA CK0HF UT WOS:000355885600008 ER PT J AU Li, BL Rodell, M Famiglietti, JS AF Li, Bailing Rodell, Matthew Famiglietti, James S. TI Groundwater variability across temporal and spatial scales in the central and northeastern US SO JOURNAL OF HYDROLOGY LA English DT Article DE Spatial and temporal variability of; groundwater storage anomalies; Scale dependency of groundwater storage; Groundwater recharge ID CLIMATE EXPERIMENT GRACE; SOIL-MOISTURE; GRAVITY RECOVERY; WATER; SURFACE; DEPLETION; RECHARGE; STORAGE; ASSIMILATION; ILLINOIS AB Depth-to-water measurements from 181 monitoring wells in unconfined or semi-confined aquifers in nine regions of the central and northeastern U.S. were analyzed. Groundwater storage exhibited strong seasonal variations in all regions, with peaks in spring and lows in autumn, and its interannual variability was nearly unbounded, such that the impacts of droughts, floods, and excessive pumping could persist for many years. We found that the spatial variability of groundwater storage anomalies (deviations from the long term mean) increases as a power function of extent scale (square root of area). That relationship, which is linear on a log-log graph, is common to other hydrological variables but had never before been shown with groundwater data. We describe how the derived power function can be used to determine the number of wells needed to estimate regional mean groundwater storage anomalies with a desired level of accuracy, or to assess uncertainty in regional mean estimates from a set number of observations. We found that the spatial variability of groundwater storage anomalies within a region often increases with the absolute value of the regional mean anomaly, the opposite of the relationship between soil moisture spatial variability and mean. Recharge (drainage from the lowest model soil layer) simulated by the Variable Infiltration Capacity (VIC) model was compatible with observed monthly groundwater storage anomalies and month-to-month changes in groundwater storage. (C) 2015 Elsevier B.V. All rights reserved. C1 [Li, Bailing] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Li, Bailing; Rodell, Matthew] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Famiglietti, James S.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA USA. [Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. [Famiglietti, James S.] Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA USA. RP Li, BL (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. EM bailing.li@nasa.gov RI Rodell, Matthew/E-4946-2012 OI Rodell, Matthew/0000-0003-0106-7437 FU NASA's Terrestrial Hydrology Program FX This research was funded by NASA's Terrestrial Hydrology Program. We thank the USGS and the Illinois State Water Survey for providing the groundwater data, David Mocko for providing monthly NLDAS-2 VIC model output and anonymous reviewers for their comments that have helped improve the quality of this paper. NR 42 TC 2 Z9 2 U1 4 U2 30 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 JUN PY 2015 VL 525 BP 769 EP 780 DI 10.1016/j.jhydrol.2015.04.033 PG 12 WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA CK0HF UT WOS:000355885600065 ER PT J AU Yasuda, T Iwakiri, WB Tashiro, MS Terada, Y Kouzu, T Enoto, T Nakagawa, YE Bamba, A Urata, Y Yamaoka, K Ohno, M Shibata, S Makishima, K AF Yasuda, Tetsuya Iwakiri, Wataru B. Tashiro, Makoto S. Terada, Yukikatsu Kouzu, Tomomi Enoto, Teruaki Nakagawa, Yujin E. Bamba, Aya Urata, Yuji Yamaoka, Kazutaka Ohno, Masanori Shibata, Shinpei Makishima, Kazuo TI Sub-MeV band observation of a hard burst from AXP 1E 1547.0-5408 with the Suzaku Wide-band All-sky Monitor SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE stars: magnetars; X-rays: bursts; X-rays: individual (AXP 1E 1547.0-5408, SGR J1550-5418, PSR J1550-5418) ID X-RAY-DETECTOR; MAGNETIZED NEUTRON-STARS; SGR J1550-5418 BURSTS; IN-ORBIT PERFORMANCE; 1998 AUGUST 27; GIANT FLARE; BOARD SUZAKU; RADIATIVE MECHANISM; SGR-1806-20; SGR-1900+14 AB The 2.1-s anomalous X-ray pulsar 1E 1547.0-5408 exhibited an X-ray outburst on 2009 January 22, emitting a large number of short bursts. The wide-band all-sky monitor (WAM) on-board Suzaku detected at least 254 bursts in the 160 keV-6.2MeV band over the period of January 22 00: 57-17: 02 UT from the direction of 1E 1547.0-5408. One of these bursts, which occurred at 06: 45: 13, produced the brightest fluence in the 0.5-6.2 MeV range, with an averaged 0.16-6.2 MeV flux and extrapolated 25 keV-2 MeV fluence of about 1x10(-5) erg cm(-2) s(-1) and about 3x10(-4) erg cm(-2), respectively. After pile-up corrections, the time-resolved WAM spectra of this burst were well-fitted in the 0.16-6.2 MeV range by two-component models; specifically, a blackbody plus an optically thin thermal bremsstrahlung or a combination of a blackbody and a power-law component with an exponential cut-off. These results are compared with previous works reporting the persistent emission and weaker short bursts followed by the same outburst. C1 [Yasuda, Tetsuya; Tashiro, Makoto S.; Terada, Yukikatsu; Kouzu, Tomomi] Saitama Univ, Grad Sch Sci & Engn, Saitama, Saitama 3388570, Japan. [Iwakiri, Wataru B.; Enoto, Teruaki] RIKEN Nishina Ctr, Wako, Saitama 3510198, Japan. [Enoto, Teruaki] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nakagawa, Yujin E.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Bamba, Aya] Aoyama Gakuin Univ, Dept Phys & Math, Chuo Ku, Sagamihara, Kanagawa 2525258, Japan. [Urata, Yuji] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan. [Yamaoka, Kazutaka] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan. [Yamaoka, Kazutaka] Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Ohno, Masanori] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Shibata, Shinpei] Yamagata Univ, Dept Phys, Yamagata 9908560, Japan. [Makishima, Kazuo] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. RP Yasuda, T (reprint author), Saitama Univ, Grad Sch Sci & Engn, 255 Shimo Okubo, Saitama, Saitama 3388570, Japan. EM yasuda@heal.phy.saitama-u.ac.jp RI XRAY, SUZAKU/A-1808-2009 FU Ministry of Education, Culture, Sports, Science, and Technology (MEXT) of Japan [24-10233, 23340055, 22340039]; MEXT [22684012]; JSPS [24540309] FX This work was supported in part by Grant-in-Aid for the Japan Society for the Promotion of Science (JSPS) Fellows (No. 24-10233, T.Y.), Grants-in-Aid for Scientific Research (B) from the Ministry of Education, Culture, Sports, Science, and Technology (MEXT) of Japan (No. 23340055, Y.T.; No. 22340039, M.S.T.), a Grant-in-Aid for Young Scientists (A) from MEXT (No. 22684012, A. B.), and JSPS KAKENHI (No. 24540309, Y.E.N.). NR 51 TC 0 Z9 0 U1 0 U2 1 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 JUN PY 2015 VL 67 IS 3 AR 41 DI 10.1093/pasj/psv011 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK4GQ UT WOS:000356182500012 ER PT J AU Perrone, JA Liston, DB AF Perrone, John A. Liston, Dorion B. TI Redundancy reduction explains the expansion of visual direction space around the cardinal axes SO VISION RESEARCH LA English DT Article DE Oblique effect; Visual motion; Redundancy reduction; Surround inhibition; MT; MSTd ID PURSUIT EYE-MOVEMENTS; AREA MT; MACAQUE MONKEY; ORIENTATION SELECTIVITY; RECEPTIVE-FIELD; MOTION SENSOR; MT/V5 NEURONS; SELF-MOTION; MST NEURONS; OWL MONKEY AB Motion direction discrimination in humans is worse for oblique directions than for the cardinal directions (the oblique effect). For some unknown reason, the human visual system makes systematic errors in the estimation of particular motion directions; a direction displacement near a cardinal axis appears larger than it really is whereas the same displacement near an oblique axis appears to be smaller. Although the perceptual effects are robust and are clearly measurable in smooth pursuit eye movements, all attempts to identify the neural underpinnings for the oblique effect have failed. Here we show that a model of image velocity estimation based on the known properties of neurons in primary visual cortex (V1) and the middle temporal (MT) visual area of the primate brain produces the oblique effect. We also provide an explanation for the unusual asymmetric patterns of inhibition that have been found surrounding MT neurons. These patterns are consistent with a mechanism within the visual system that prevents redundant velocity signals from being passed onto the next motion-integration stage, (dorsal Medial superior temporal, MSTd). We show that model redundancy-reduction mechanisms within the MT-MSTd pathway produce the oblique effect. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Perrone, John A.] Univ Waikato, Sch Psychol, Hamilton 3240, New Zealand. [Liston, Dorion B.] San Jose State Univ, San Jose, CA 95192 USA. [Liston, Dorion B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Perrone, JA (reprint author), Univ Waikato, Sch Psychol, Hamilton 3240, New Zealand. EM jpnz@waikato.ac.nz FU Marsden Fund Council; Office of Naval Research, USA FX J.P. and D.L. supported by the Marsden Fund Council from Government funding, administered by the Royal Society of New Zealand. DL supported by Office of Naval Research, USA. There is no conflict of interest. NR 53 TC 0 Z9 0 U1 2 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0042-6989 EI 1878-5646 J9 VISION RES JI Vision Res. PD JUN PY 2015 VL 111 BP 31 EP 42 DI 10.1016/j.visres.2015.03.020 PN A PG 12 WC Neurosciences; Ophthalmology SC Neurosciences & Neurology; Ophthalmology GA CK2FW UT WOS:000356027200004 PM 25888929 ER PT J AU Cunnane, D Kawamura, JH Wolak, MA Acharya, N Tan, T Xi, XX Karasik, BS AF Cunnane, D. Kawamura, J. H. Wolak, M. A. Acharya, N. Tan, T. Xi, X. X. Karasik, B. S. TI Characterization of MgB2 Superconducting Hot Electron Bolometers SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Hot electron bolometers (HEBs); MgB2; superconducting devices; terahertz mixers ID THIN-FILMS; MIXERS AB Hot-Electron Bolometer (HEB) mixers have proven to be the best tool for high-resolution spectroscopy at the Terahertz frequencies. However, the current state of the art NbN mixers suffer from a small intermediate frequency (IF) bandwidth as well as a low operating temperature. MgB2 is a promising material for HEB mixer technology in view of its high critical temperature and fast thermal relaxation allowing for a large IF bandwidth. In this work, we have fabricated and characterized thin-film (similar to 15 nm) MgB2-based spiral antenna-coupled HEB mixers on SiC substrate. We achieved the IF bandwidth greater than 8 GHz at 25 K and the device noise temperature < 4000 K at 9 K using a 600 GHz source. Using temperature dependencies of the radiation power dissipated in the device we have identified the optical loss in the integrated microantenna responsible as a cause of the limited sensitivity of the current mixer devices. From the analysis of the current-voltage (IV) characteristics, we have derived the effective thermal conductance of the mixer device and estimated the required local oscillator power in an optimized device to be similar to 1 mu W. C1 [Cunnane, D.; Kawamura, J. H.; Karasik, B. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wolak, M. A.; Acharya, N.; Tan, T.; Xi, X. X.] 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 FU National Space and Aeronautics Administration; NASA Astrophysics Research and Analysis Program through a contract from JPL; NASA FX This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Space and Aeronautics Administration. The work at Temple University was supported by the NASA Astrophysics Research and Analysis Program through a contract from JPL. The work of D. Cunnane was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. NR 20 TC 13 Z9 13 U1 4 U2 20 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 2015 VL 25 IS 3 AR 2300206 DI 10.1109/TASC.2014.2369353 PG 6 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA CJ7IN UT WOS:000355668500001 ER PT J AU McDermott, SP Bransome, NC Sutton, SE Smith, BE Link, JS Miller, TJ AF McDermott, S. P. Bransome, N. C. Sutton, S. E. Smith, B. E. Link, J. S. Miller, T. J. TI Quantifying alosine prey in the diets of marine piscivores in the Gulf of Maine SO JOURNAL OF FISH BIOLOGY LA English DT Article DE alewife; demersal fish; Gulf of Maine; river herring; trophic interaction ID HUDSON RIVER ESTUARY; ATLANTIC COD; STRIPED BASS; POMATOMUS-SALTATRIX; TROPHIC ECOLOGY; AGE-0 BLUEFISH; CHESAPEAKE-BAY; DELAWARE BAY; SALMO-SALAR; FOOD WEBS AB The objectives of this work were to quantify the spatial and temporal distribution of the occurrence of anadromous fishes (alewife Alosa pseudoharengus, blueback herring Alosa aestivalis and American shad Alosa sapidissima) in the stomachs of demersal fishes in coastal waters of the north-west Atlantic Ocean. Results show that anadromous fishes were detectable and quantifiable in the diets of common marine piscivores for every season sampled. Even though anadromous fishes were not the most abundant prey, they accounted for c. 5-10% of the diet by mass for several marine piscivores. Statistical comparisons of these data with fish diet data from a broad-scale survey of the north-west Atlantic Ocean indicate that the frequency of this trophic interaction was significantly higher within spatially and temporally focused sampling areas of this study than in the broad-scale survey. Odds ratios of anadromous predation were as much as 460 times higher in the targeted sampling as compared with the broad-scale sampling. Analyses indicate that anadromous prey consumption was more concentrated in the near-coastal waters compared with consumption of a similar, but more widely distributed species, the Atlantic herring Clupea harengus. In the context of ecosystem-based fisheries management, the results suggest that even low-frequency feeding events may be locally important, and should be incorporated into ecosystem models. (C) 2015 The Fisheries Society of the British Isles C1 [McDermott, S. P.] Natl Marine Fisheries Serv, Greater Atlantic Reg Off, Gloucester, MA 01930 USA. [Bransome, N. C.; Miller, T. J.] Univ Maryland, Ctr Environm Sci, Chesapeake Biol Lab, Solomons, MD 20688 USA. [Sutton, S. E.; Smith, B. E.; Link, J. S.] NOAA, Northeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Woods Hole, MA 02543 USA. RP McDermott, SP (reprint author), Natl Marine Fisheries Serv, Greater Atlantic Reg Off, 55 Great Republ Dr, Gloucester, MA 01930 USA. EM sean.mcdermott@noaa.gov RI Miller, Thomas/C-2129-2008 OI Miller, Thomas/0000-0001-8427-1614 FU NOAA Fisheries Greater Atlantic Regional Fisheries Office Habitat Conservation Programme; NOAA Cooperative Institute for North Atlantic Research [CINAR NA09OAR4320129]; NSF-NOAA CAMEO project [OCE-0961-632] FX This work was funded through an award from NOAA Fisheries Greater Atlantic Regional Fisheries Office Habitat Conservation Programme and via a student fellowship to N.B. from the NOAA Cooperative Institute for North Atlantic Research (CINAR NA09OAR4320129). T.J.M. is supported in part by an NSF-NOAA CAMEO project (OCE-0961-632). We thank the crew of NOAA R.V. Gloria Michelle, staff from NEFSC who assisted with fieldwork, Maine Department of Marine Resources staff and crew of F.V. Robert Michael. Also, we thank the many scientists who have contributed to the NEFSC food habits database, without whom, these analyses would not have been possible. This is contribution 5000 from the University of Maryland Center for Environmental Science. NR 63 TC 2 Z9 2 U1 3 U2 13 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-1112 EI 1095-8649 J9 J FISH BIOL JI J. Fish Biol. PD JUN PY 2015 VL 86 IS 6 BP 1811 EP 1829 DI 10.1111/jfb.12692 PG 19 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA CJ6UD UT WOS:000355628700009 PM 25943427 ER PT J AU Muller, HSP Brown, LR Drouin, BJ Pearson, JC Kleiner, I Sams, RL Sung, K Ordu, MH Lewen, F AF Mueller, Holger S. P. Brown, Linda R. Drouin, Brian J. Pearson, John C. Kleiner, Isabelle Sams, Robert L. Sung, Keeyoon Ordu, Matthias H. Lewen, Frank TI Rotational spectroscopy as a tool to investigate interactions between vibrational polyads in symmetric top molecules: Low-lying states v(8) <= 2 of methyl cyanide, CH3CN SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE Rotational spectroscopy; Infrared spectroscopy; Vibration-rotation interaction; Methyl cyanide; Interstellar molecule ID SPECTRAL-LINE CATALOG; ETHYL CYANIDE; GROUND-STATE; INTERSTELLAR-MEDIUM; HIGH-RESOLUTION; SAGITTARIUS B2(N); INFRARED-SPECTRUM; COLOGNE DATABASE; EXCITED-STATES; WAVE SPECTRUM AB Rotational and rovibrational spectra of methyl cyanide were recorded to analyze interactions in low-lying vibrational states and to construct line lists for radio astronomical observations as well as for infrared spectroscopic investigations of planetary atmospheres. The rotational spectra cover large portions of the 36-1627 GHz region. In the infrared (IR), a spectrum was recorded for this study in the region of 2v(8) around 717 cm(-1) with assignments covering 684-765 cm-1. Additional spectra in the vs region were used to validate the analysis. Information on the K level structure of CH3CN is almost exclusively obtained from IR spectra, as are basics of the J level structure. The large amount and the high accuracy of the rotational data improves knowledge of the J level structure considerably. Moreover, since these data extend to much higher and K quantum numbers, they allowed us to investigate for the first time in depth local interactions between these states which occur at high K values. In particular, we have detected several interactions between v(8) = 1 and 2. Notably, there is a strong Delta v(8) = +/- 1, Delta K = 0, Delta l = +/- 3 Fermi resonance between v(8) = 1(-1) and v(8) = 2(+2) at K = 14. Pronounced effects in the spectrum are also caused by resonant Delta v(8) = +/- 1, Delta K = -/+ 2, Delta l = +/- 1 interactions between v(8) = 1 and 2 at K = 13, l = 1/K = 11, l = 0 and at K = 15, l = +1/K = 13, l = +2. An equivalent resonant interaction occurs between K = 14 of the ground vibrational state and K = 12, l = +1 of v(8) = 1 for which we present the first detailed account. A preliminary account was given in an earlier study on the ground vibrational state. Similar resonances were found for CH3CCH and, more recently, for CH3NC, warranting comparison of the results. From data pertaining to v(8) = 2, we also investigated rotational interactions with v(4) = 1 as well as Delta v(8) = +/- 1, Delta K = 0, Delta l = +/- 3 Fermi interactions between v(8) = 2 and 3. We have derived N-2- and self-broadening coefficients for the v(8), 2v(8) - v(8), and 2v(8) bands from previously determined v(4) values. Subsequently, we determined transition moments and intensities for the three IR bands. (C) 2015 Elsevier Inc. All rights reserved. C1 [Mueller, Holger S. P.; Ordu, Matthias H.; Lewen, Frank] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Brown, Linda R.; Drouin, Brian J.; Pearson, John C.; Sung, Keeyoon] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kleiner, Isabelle] Univ Paris Est Creteil & Paris Diderot, LISA, Inst Pierre Simon Laplace, CNRS,UMR 7583, F-94010 Creteil, France. [Sams, Robert L.] Pacific NW Natl Lab, Richland, WA 99352 USA. RP Muller, HSP (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. EM hspm@ph1.uni-koeln.de RI Sung, Keeyoon/I-6533-2015; OI Mueller, Holger/0000-0002-0183-8927 FU Bundesministerium fur Bildung und Forschung (BMBF) [FKZ 50OF0901]; Deutsche Forschungsgemeinschaft (DFG) [SFB 494, SFB 956]; Department of Energy's Office of Biological and Environmental Research located at the Pacific Northwest National Laboratory (PNNL); United States Department of Energy [DE-AC05-76RLO1830] FX H.S.P.M. is grateful to the Bundesministerium fur Bildung und Forschung (BMBF) for financial support through project FKZ 50OF0901 (ICC HIFI Herschel) during part of the present investigation. The measurements in Koln were supported by the Deutsche Forschungsgemeinschaft (DFG) through the collaborative research grants SFB 494 initially, and later SFB 956, project area B3. The portion of this work, which was carried out at the Jet Propulsion Laboratory, California Institute of Technology, was performed under contract with the National Aeronautics and Space Administration. The infrared spectra analyzed in the present study were recorded at the W.R. Wiley Environmental Molecular Sciences Laboratory, a national scientific user facility sponsored by the Department of Energy's Office of Biological and Environmental Research located at the Pacific Northwest National Laboratory (PNNL). PNNL is operated for the United States Department of Energy by the Battelle Memorial Institute under Contract DE-AC05-76RLO1830. NR 86 TC 7 Z9 7 U1 2 U2 13 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 EI 1096-083X J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD JUN PY 2015 VL 312 BP 22 EP 37 DI 10.1016/j.jms.2015.02.009 PG 16 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA CJ6XR UT WOS:000355639000004 ER PT J AU Elliott, BM Sung, K Miller, CE AF Elliott, Ben M. Sung, Keeyoon Miller, Charles E. TI FT-IR spectra of O-18-, and C-13-enriched CO2 in the v(3) region: High accuracy frequency calibration and spectroscopic constants for (OCO)-O-16-C-12-O-18, (OCO)-O-18-C-12-O-18, and (OCO)-O-16-C-13-O-16 SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE O-18-enriched; C-13-enriched; CO2; FT-IR; Absolute wavenumber accuracy; Remote sensing ID SENSITIVITY CAVITY RING; ENRICHED CARBON-DIOXIDE; CONSTRAINED MULTISPECTRUM ANALYSIS; 4.3 MU-M; INFRARED-SPECTROSCOPY; 7000 CM(-1); LINE POSITIONS; MOLECULAR-CONSTANTS; ABSORPTION-BANDS; SPEED DEPENDENCE AB In this report, we extend our Fourier transform infrared (FT-IR) spectroscopy measurements of CO2 in the v(3) region (2200-2450 cm(-1), 65-75 THz) to the O-18-, and C-13-substituted isotopologues, using the JPL Bruker IFS-125HR Fourier Transform Spectrometer (JPL-FTS). High quality (S/N similar to 2000) spectra were obtained separately for each of the 180-, and 13C-isotopically enriched samples. The absolute wavenumber accuracies were better than 3 x 10(-6) cm(-1) (similar to 100 kHz) for strong, isolated transitions, calibrated against the highest accuracy reported CO and (OCO)-O-16-C-12-O-16 (626) frequency measurements. The JPL-FTS performance and calibration procedure is shown to be reliable and consistent, achievable through vigorous maintenance of the optical alignment and regular monitoring of its instrumental line shape function. Effective spectroscopic constant fits of the 00011 <- 00001 fundamental bands for 18012080 (628), (OCO)-O-18-C-12-O-18 (828), and (OCO)-O-16-C-13-O-16 (636) were obtained with RMS residuals of 2.9 x 10(-6) cm(-1), 2.8 x 10(-6) cm(-1), and 2.9 x 10(-6) cm(-1), respectively. The observed bands encompassed 79 lines over the J(max) range of P67/R67, 47 lines over P70/R62, and 60 lines over P70/R70 for 628, 828, and 636, respectively. These results complement our recent work on the O-17-enriched isotopologues (Elliott et al., 2014), providing additional high-quality frequency measurements for atmospheric remote sensing applications. (C) 2015 Elsevier Inc. All rights reserved. C1 [Elliott, Ben M.; Sung, Keeyoon; Miller, Charles E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Miller, CE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM benm.elliott@epss.ucla.edu; keeyoon.sung@jpl.nasa.gov; charles.e.miller@jpl.nasa.gov RI Sung, Keeyoon/I-6533-2015 FU NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology FX BM Elliott was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Oak Ridge Associated Universities through a contract with NASA. The authors thank Timothy Crawford for his professional assistance in maintaining the JPL-FTS and all the peripheral apparatus. K. Sung thanks Baron Vazindel from Bruker Optics, Inc. for his professional on-site service performance, especially on the optics alignment for the Bruker IFS-125HR at JPL since its installation in 2006. 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. Copyright 2014 California Institute of Technology. Government sponsorship acknowledged. NR 37 TC 0 Z9 0 U1 1 U2 13 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 EI 1096-083X J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD JUN PY 2015 VL 312 BP 78 EP 86 DI 10.1016/j.jms.2015.02.007 PG 9 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA CJ6XR UT WOS:000355639000011 ER PT J AU Kogut, A Fixsen, DJ Hill, RS AF Kogut, Alan Fixsen, Dale J. Hill, Robert S. TI Polarization properties of a broadband multi-moded concentrator SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA A-OPTICS IMAGE SCIENCE AND VISION LA English DT Article ID NONIMAGING CONCENTRATORS; FLUX AB We present the design and performance of a non-imaging concentrator for use in broadband polarimetry at millimeter through submillimeter wavelengths. A rectangular geometry preserves the input polarization state as the concentrator couples f/2 incident optics to a 2 pi sr detector. Measurements of the co-polar and cross-polar beams in both the few-mode and highly over-moded limits agree with a simple model based on mode truncation. The measured co-polar beam pattern is nearly independent of frequency in both linear polarizations. The cross-polar beam pattern is dominated by a uniform term corresponding to polarization efficiency of 94%. After correcting for efficiency, the remaining cross-polar response is -18 dB. C1 [Kogut, Alan; Fixsen, Dale J.; Hill, Robert S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kogut, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Alan.J.Kogut@nasa.gov NR 14 TC 3 Z9 3 U1 1 U2 3 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1084-7529 EI 1520-8532 J9 J OPT SOC AM A JI J. Opt. Soc. Am. A-Opt. Image Sci. Vis. PD JUN PY 2015 VL 32 IS 6 BP 1040 EP 1045 DI 10.1364/JOSAA.32.001040 PG 6 WC Optics SC Optics GA CJ6VM UT WOS:000355633300004 PM 26367036 ER PT J AU Massey, R Williams, L Smit, R Swinbank, M Kitching, TD Harvey, D Jauzac, M Israel, H Clowe, D Edge, A Hilton, M Jullo, E Leonard, A Liesenborgs, J Merten, J Mohammed, I Nagai, D Richard, J Robertson, A Saha, P Santana, R Stott, J Tittley, E AF Massey, Richard Williams, Liliya Smit, Renske Swinbank, Mark Kitching, Thomas D. Harvey, David Jauzac, Mathilde Israel, Holger Clowe, Douglas Edge, Alastair Hilton, Matt Jullo, Eric Leonard, Adrienne Liesenborgs, Jori Merten, Julian Mohammed, Irshad Nagai, Daisuke Richard, Johan Robertson, Andrew Saha, Prasenjit Santana, Rebecca Stott, John Tittley, Eric TI The behaviour of dark matter associated with four bright cluster galaxies in the 10 kpc core of Abell 3827 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE astroparticle physics; gravitational lensing: strong; galaxies: clusters: individual: Abell 3827; dark matter ID HUBBLE-SPACE-TELESCOPE; LENSING MASS RECONSTRUCTION; STELLAR POPULATION SYNTHESIS; CHARGE-TRANSFER INEFFICIENCY; PIXEL-BASED CORRECTION; LARGE-SCALE STRUCTURE; ADVANCED CAMERA; NONPARAMETRIC INVERSION; GENETIC ALGORITHM; CROSS-SECTION AB Galaxy cluster Abell 3827 hosts the stellar remnants of four almost equally bright elliptical galaxies within a core of radius 10 kpc. Such corrugation of the stellar distribution is very rare, and suggests recent formation by several simultaneous mergers. We map the distribution of associated dark matter, using new Hubble Space Telescope imaging and Very Large Telescope/Multi-Unit Spectroscopic Explorer integral field spectroscopy of a gravitationally lensed system threaded through the cluster core. We find that each of the central galaxies retains a dark matter halo, but that (at least) one of these is spatially offset from its stars. The best-constrained offset is 1.62(-0.49)(+0.47) kpc, where the 68 per cent confidence limit includes both statistical error and systematic biases in mass modelling. Such offsets are not seen in field galaxies, but are predicted during the long infall to a cluster, if dark matter self-interactions generate an extra drag force. With such a small physical separation, it is difficult to definitively rule out astrophysical effects operating exclusively in dense cluster core environments - but if interpreted solely as evidence for self-interacting dark matter, this offset implies a cross-section sigma(DM)/(m) similar to (1.7 +/- 0.7) x 10(-4) cm(2) g(-1) x (t(infall)/10(9) yr)(-2), where t(infall) is the infall duration. C1 [Massey, Richard; Jauzac, Mathilde; Israel, Holger] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Massey, Richard; Smit, Renske; Swinbank, Mark; Edge, Alastair; Leonard, Adrienne; Robertson, Andrew; Stott, John] Univ Durham, Ctr Extragalact Astron, Durham DH1 3LE, England. [Williams, Liliya] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Kitching, Thomas D.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Harvey, David] Ecole Polytech Fed Lausanne, Observ Sauverny, CH-1290 Versoix, Switzerland. [Jauzac, Mathilde; Hilton, Matt] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Clowe, Douglas; Santana, Rebecca] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. [Jullo, Eric] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Leonard, Adrienne] UCL, London WC1E 6BT, England. [Liesenborgs, Jori] Univ Hasselt, Expertisectr Digitale Media, B-3590 Diepenbeek, Belgium. [Merten, Julian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Merten, Julian] CALTECH, Pasadena, CA 91125 USA. [Mohammed, Irshad; Saha, Prasenjit] Univ Zurich, Inst Phys, CH-8057 Zurich, Switzerland. [Nagai, Daisuke] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Richard, Johan] Univ Lyon 1, Observ Lyon, F-69561 St Genis Laval, France. [Tittley, Eric] Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. RP Massey, R (reprint author), Univ Durham, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England. EM r.j.massey@durham.ac.uk OI Mohammed, Irshad/0000-0003-0784-5447; Robertson, Andrew/0000-0002-0086-0524; Leonard, Adrienne/0000-0002-5976-0405; Edge, Alastair/0000-0002-3398-6916; Stott, John/0000-0002-1679-9983 FU Royal Society University Research Fellowships; Science and Technology Facilities Council [ST/L00075X/1, ST/H005234/1, ST/I001573/1]; Leverhulme Trust [PLP-2011-003]; NASA; NASA [NAS 5-26555]; ESO Telescopes at the La Silla Paranal Observatory [093.A-0237, 294.A-5014]; BIS National E-infrastructure capital grant [ST/K00042X/1]; STFC capital grant [ST/H008519/1]; STFC DiRAC Operations grant [ST/K003267/1]; Durham University FX The authors are pleased to thank Jay Anderson for advice with CTI correction for HST/WFC3, Jean-Paul Kneib for advice using LENSTOOL, and the anonymous referee whose suggestions improved the manuscript. RM and TDK are supported by Royal Society University Research Fellowships. This work was supported by the Science and Technology Facilities Council (grant numbers ST/L00075X/1, ST/H005234/1 and ST/I001573/1) and the Leverhulme Trust (grant number PLP-2011-003). This research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA.; Facilities: This paper uses data from observations GO-12817 (PI: R. Massey) with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA Inc, under NASA contract NAS 5-26555. This paper also uses data from observations made with ESO Telescopes at the La Silla Paranal Observatory under programmes 093.A-0237 and 294.A-5014 (PI: R. Massey). We thank the Director General for granting discretionary time, and Paranal Science Operations for running the observations. The LENSTOOL analysis 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. LLRW would like to acknowledge the Minnesota Supercomputing Institute, without whose computational support GRALE work would not have been possible. NR 82 TC 53 Z9 53 U1 0 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2015 VL 449 IS 4 BP 3393 EP 3406 DI 10.1093/mnras/stv467 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2VE UT WOS:000355342000005 ER PT J AU Davis, TA Rowlands, K Allison, JR Shabala, SS Ting, YS Lagos, CDP Kaviraj, S Bourne, N Dunne, L Eales, S Ivison, RJ Maddox, S Smith, DJB Smith, MWL Temi, P AF Davis, Timothy A. Rowlands, Kate Allison, James R. Shabala, Stanislav S. Ting, Yuan-Sen Lagos, Claudia del P. Kaviraj, Sugata Bourne, Nathan Dunne, Loretta Eales, Steve Ivison, Rob. J. Maddox, Steve Smith, Daniel J. B. Smith, Matthew W. L. Temi, Pasquale TI Molecular and atomic gas in dust lane early-type galaxies - I. Low star formation efficiencies in minor merger remnants SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM: molecules; galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: interactions; galaxies: ISM ID CO-TO-H-2 CONVERSION FACTOR; SCIENCE DEMONSTRATION PHASE; MASS-METALLICITY RELATION; DIGITAL-SKY-SURVEY; ATLAS(3D) PROJECT; HERSCHEL-ATLAS; FORMING GALAXIES; ELLIPTIC GALAXIES; SAURON PROJECT; COLD GAS AB In this work we present IRAM 30-m telescope observations of a sample of bulge-dominated galaxies with large dust lanes, which have had a recent minor merger. We find these galaxies are very gas rich, with H-2 masses between 4 x 10(8) and 2 x 10(10) M-circle dot. We use these molecular gas masses, combined with atomic gas masses from an accompanying paper, to calculate gas-to-dust and gas-to-stellar-mass ratios. The gas-to-dust ratios of our sample objects vary widely (between approximate to 50 and 750), suggesting many objects have low gas-phase metallicities, and thus that the gas has been accreted through a recent merger with a lower mass companion. We calculate the implied minor companion masses and gas fractions, finding a median predicted stellar mass ratio of approximate to 40:1. The minor companion likely had masses between approximate to 10(7) and 10(10) M-circle dot. The implied merger mass ratios are consistent with the expectation for low-redshift gas-rich mergers from simulations. We then go on to present evidence that (no matter which star formation rate indicator is used) our sample objects have very low star formation efficiencies (star formation rate per unit gas mass), lower even than the early-type galaxies from ATLAS(3D) which already show a suppression. This suggests that minor mergers can actually suppress star formation activity. We discuss mechanisms that could cause such a suppression, include dynamical effects induced by the minor merger. C1 [Davis, Timothy A.; Lagos, Claudia del P.; Ivison, Rob. J.] European So Observ, D-85748 Garching, Germany. [Davis, Timothy A.; Kaviraj, Sugata; Smith, Daniel J. B.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL1 9AB, Herts, England. [Rowlands, Kate] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Allison, James R.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Shabala, Stanislav S.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Ting, Yuan-Sen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lagos, Claudia del P.] Univ Western Australia, Int Ctr Radio Astron ICRAR, Crawley, WA 6009, Australia. [Bourne, Nathan; Dunne, Loretta] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Dunne, Loretta; Maddox, Steve] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand. [Eales, Steve; Smith, Matthew W. L.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Temi, Pasquale] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. RP Davis, TA (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM t.davis4@herts.ac.uk RI Ivison, R./G-4450-2011; OI Ivison, R./0000-0001-5118-1313; Smith, Daniel/0000-0001-9708-253X; Lagos, Claudia/0000-0003-3021-8564; Davis, Timothy/0000-0003-4932-9379; Maddox, Stephen/0000-0001-5549-195X; Ting, Yuan-Sen/0000-0001-5082-9536 FU Science and Technology Facilities Council Ernest Rutherford Fellowship; European Research Council Starting Grant SEDmorph; Australian Research Council [DE130101399]; European Research Council Advanced grant COSMICISM; European Community [229517, 283393]; INSU/CNRS (France); MPG (Germany); IGN (Spain); STFC (UK); ARC (Australia); AAO; National Aeronautics and Space Administration FX TAD acknowledges support from a Science and Technology Facilities Council Ernest Rutherford Fellowship, and thanks Maarten Baes, Gianfranco De Zotti, Ivan Oteo Gomez, Michal Michalowski and Catherine Vlahakis for comments which improved the paper. KR acknowledges support from the European Research Council Starting Grant SEDmorph (PI: V. Wild). SSS thanks the Australian Research Council for an Early Career Fellowship (DE130101399). LD, RJI and SM acknowledge support from the European Research Council Advanced grant COSMICISM. The research leading to these results has received funding from the European Community's Seventh Framework Programme (/FP7/2007-2013/) under grant agreement No. 229517 and No. 283393 (RadioNet3). This paper is based on observations carried out with the IRAM 30-m telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain).; The H-ATLAS is a project with Herschel, which is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The H-ATLAS website is http://www.h-atlas.org/. 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 programs including GALEX MIS, VST KIDS, VISTA VIKING, WISE, H-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/. This publication makes use of data products from the WISE, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 92 TC 10 Z9 10 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 JUN 1 PY 2015 VL 449 IS 4 BP 3503 EP 3516 DI 10.1093/mnras/stv597 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2VE UT WOS:000355342000014 ER PT J AU Marocco, F Jones, HRA Day-Jones, AC Pinfield, DJ Lucas, PW Burningham, B Zhang, ZH Smart, RL Gomes, JI Smith, L AF Marocco, F. Jones, H. R. A. Day-Jones, A. C. Pinfield, D. J. Lucas, P. W. Burningham, B. Zhang, Z. H. Smart, R. L. Gomes, J. I. Smith, L. TI A large spectroscopic sample of L and T dwarfs from UKIDSS LAS: peculiar objects, binaries, and space density SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: spectroscopic; brown dwarfs; stars: low-mass; stars: luminosity function, mass function ID LOW-MASS STARS; DIGITAL SKY SURVEY; VERY-LOW MASS; YOUNG KINEMATIC GROUPS; PROPER MOTION SURVEY; LARGE-AREA SURVEY; BROWN DWARF; ULTRACOOL DWARFS; LUMINOSITY-FUNCTION; L/T TRANSITION AB We present the spectroscopic analysis of a large sample of late-M, L, and T dwarfs from the United Kingdom Deep Infrared Sky Survey. Using the YJHK photometry from the Large Area Survey and the red-optical photometry from the Sloan Digital Sky Survey we selected a sample of 262 brown dwarf candidates and we have followed-up 196 of them using the echelle spectrograph X-shooter on the Very Large Telescope. The large wavelength coverage (0.30-2.48 mu m) and moderate resolution (R similar to 5000-9000) of X-shooter allowed us to identify peculiar objects including 22 blue L dwarfs, 2 blue T dwarfs, and 2 low-gravity M dwarfs. Using a spectral indices-based technique, we identified 27 unresolved binary candidates, for which we have determined the spectral type of the potential components via spectral deconvolution. The spectra allowed us to measure the equivalent width of the prominent absorption features and to compare them to atmospheric models. Cross-correlating the spectra with a radial velocity standard, we measured the radial velocity of our targets, and we determined the distribution of the sample, which is centred at -1.7 +/- 1.2 km s(-1) with a dispersion of 31.5 km s(-1). Using our results, we estimated the space density of field brown dwarfs and compared it with the results of numerical simulations. Depending on the binary fraction, we found that there are (0.85 +/- 0.55) x 10(-3) to (1.00 +/- 0.64) x 10(-3) objects per cubic parsec in the L4-L6.5 range, (0.73 +/- 0.47) x 10(-3) to (0.85 +/- 0.55) x 10(-3) objects per cubic parsec in the L7-T0.5 range, and (0.74 +/- 0.48) x 10(-3) to (0.88 +/- 0.56) x 10(-3) objects per cubic parsec in the T1-T4.5 range. We notice that there seems to be an excess of objects in the L-T transition with respect to the late-T dwarfs, a discrepancy that could be explained assuming a higher binary fraction than expected for the L-T transition, or that objects in the high-mass end and low-mass end of this regime form in different environments, i.e. following different initial mass functions. C1 [Marocco, F.; Jones, H. R. A.; Day-Jones, A. C.; Pinfield, D. J.; Lucas, P. W.; Burningham, B.; Zhang, Z. H.; Gomes, J. I.; Smith, L.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Burningham, B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Zhang, Z. H.] IAC, E-38200 Tenerife, Spain. [Smart, R. L.] INAF Osservatorio Astrofis Torino, I-10025 Pino Torinese, Italy. RP Marocco, F (reprint author), Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. EM f.marocco@herts.ac.uk OI Marocco, Federico/0000-0001-7519-1700; Burningham, Ben/0000-0003-4600-5627; Smart, Richard/0000-0002-4424-4766 FU European Organisation for Astronomical Research in the Southern Hemisphere, Chile [086.C-0450, 087.C-0639, 088.C-0048, 091.C-0452]; Marie Curie 7th European Community Framework Programme [247593]; European Science Foundation (ESF) [4641] FX This research is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile programs 086.C-0450, 087.C-0639, 088.C-0048, and 091.C-0452.; The authors would like to acknowledge the Marie Curie 7th European Community Framework Programme grant no. 247593 Interpretation and Parametrization of Extremely Red COOL dwarfs (IPERCOOL) International Research Staff Exchange Scheme. FM would like to acknowledge the support received from the European Science Foundation (ESF) within the framework of the ESF activity entitled 'Gaia Research for European Astronomy Training', Exchange Grant number 4641. NR 109 TC 6 Z9 6 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 JUN 1 PY 2015 VL 449 IS 4 BP 3651 EP 3692 DI 10.1093/mnras/stv530 PG 42 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2VE UT WOS:000355342000030 ER PT J AU Madura, TI Clementel, N Gull, TR Kruip, CJH Paardekooper, JP AF Madura, T. I. Clementel, N. Gull, T. R. Kruip, C. J. H. Paardekooper, J. -P. TI 3D printing meets computational astrophysics: deciphering the structure of eta Carinae's inner colliding winds SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE hydrodynamics; binaries: close; stars: individual: Eta Carinae; stars: mass-loss; stars: winds, outflows ID SMOOTHED PARTICLE HYDRODYNAMICS; RADIATIVE-TRANSFER; MASSIVE STARS; BINARY; SIMULATIONS; SPH; INSTABILITIES; COMPANION; EMISSION; MODELS AB We present the first 3D prints of output from a supercomputer simulation of a complex astrophysical system, the colliding stellar winds in the massive (greater than or similar to 120 M-circle dot), highly eccentric (e similar to 0.9) binary star system eta Carinae. We demonstrate the methodology used to incorporate 3D interactive figures into a PDF (Portable Document Format) journal publication and the benefits of using 3D visualization and 3D printing as tools to analyse data from multidimensional numerical simulations. Using a consumer-grade 3D printer (MakerBot Replicator 2X), we successfully printed 3D smoothed particle hydrodynamics simulations of eta Carinae's inner (r similar to 110 au) wind-wind collision interface at multiple orbital phases. The 3D prints and visualizations reveal important, previously unknown 'finger-like' structures at orbital phases shortly after periastron (phi similar to 1.045) that protrude radially outwards from the spiral wind-wind collision region. We speculate that these fingers are related to instabilities (e.g. thin-shell, Rayleigh-Taylor) that arise at the interface between the radiatively cooled layer of dense post-shock primary-star wind and the fast (3000 km s(-1)), adiabatic post-shock companion-star wind. The success of our work and easy identification of previously unrecognized physical features highlight the important role 3D printing and interactive graphics can play in the visualization and understanding of complex 3D time-dependent numerical simulations of astrophysical phenomena. C1 [Madura, T. I.; Gull, T. R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Clementel, N.; Kruip, C. J. H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Paardekooper, J. -P.] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Paardekooper, J. -P.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. RP Madura, TI (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 667, Greenbelt, MD 20771 USA. EM thomas.i.madura@nasa.gov FU NASA FX TIM is supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. We thank Frederic Vogt for very useful discussions on the incorporation of 3D interactive graphics into PDFs and 3D printing. We thank an anonymous referee for helpful comments. NR 49 TC 6 Z9 6 U1 3 U2 11 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 JUN 1 PY 2015 VL 449 IS 4 BP 3780 EP 3794 DI 10.1093/mnras/stv422 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2VE UT WOS:000355342000038 ER PT J AU Kirk, B Hilton, M Cress, C Crawford, SM Hughes, JP Battaglia, N Bond, JR Burke, C Gralla, MB Hajian, A Hasselfield, M Hincks, AD Infante, L Kosowsky, A Marriage, TA Menanteau, F Moodley, K Niemack, MD Sievers, JL Sifon, C Wilson, S Wollack, EJ Zunckel, C AF Kirk, Brian Hilton, Matt Cress, Catherine Crawford, Steven M. Hughes, John P. Battaglia, Nicholas Bond, J. Richard Burke, Claire Gralla, Megan B. Hajian, Amir Hasselfield, Matthew Hincks, Adam D. Infante, Leopoldo Kosowsky, Arthur Marriage, Tobias A. Menanteau, Felipe Moodley, Kavilan Niemack, Michael D. Sievers, Jonathan L. Sifon, Cristobal Wilson, Susan Wollack, Edward J. Zunckel, Caroline TI SALT spectroscopic observations of galaxy clusters detected by ACT and a type II quasar hosted by a brightest cluster galaxy SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual: ACT-CL J0320.4+0032; quasars: general; cosmology: observations ID DIGITAL SKY SURVEY; SOUTH-POLE TELESCOPE; BLACK-HOLES; DATA RELEASE; COSMOLOGICAL CONSTRAINTS; VELOCITY DISPERSION; PHYSICAL-PROPERTIES; SCALING RELATIONS; GALACTIC NUCLEI; REDSHIFT SURVEY AB We present Southern African Large Telescope follow-up observations of seven massive clusters detected by the Atacama Cosmology Telescope (ACT) on the celestial equator using the Sunyaev-Zel'dovich (SZ) effect. We conducted multi-object spectroscopic observations with the Robert Stobie Spectrograph in order to measure galaxy redshifts in each cluster field, determine the cluster line-of-sight velocity dispersions, and infer the cluster dynamical masses. We find that the clusters, which span the redshift range 0.3 < z < 0.55, range in mass from (5-20) x 10(14) M-circle dot (M-200c). Their masses, given their SZ signals, are similar to those of Southern hemisphere ACT clusters previously observed using Gemini and the VLT. We note that the brightest cluster galaxy in one of the systems studied, ACT-CL J0320.4+0032 at z = 0.38, hosts a type II quasar. Only a handful of such systems are currently known, and therefore ACT-CL J0320.4+0032 may be a rare example of a very massive halo in which quasar-mode feedback is actively taking place. C1 [Kirk, Brian; Hilton, Matt; Burke, Claire; Moodley, Kavilan; Wilson, Susan] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Kirk, Brian; Cress, Catherine] Ctr High Performance Comp, ZA-7700 Cape Town, South Africa. [Hilton, Matt] Univ Nottingham, Sch Phys & Astron, Ctr Astron & Particle Theory, Nottingham NG7 2RD, England. [Cress, Catherine] Univ Western Cape, Dept Phys, ZA-7530 Cape Town, South Africa. [Crawford, Steven M.] South African Astron Observ, ZA-7935 Cape Town, South Africa. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Battaglia, Nicholas] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Bond, J. Richard; Hajian, Amir] Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Gralla, Megan B.; Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Hasselfield, Matthew] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Hincks, Adam D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Infante, Leopoldo] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Menanteau, Felipe] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA. [Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Sievers, Jonathan L.; Zunckel, Caroline] Univ KwaZulu Natal, Sch Chem & Phys, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Sifon, Cristobal] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kirk, B (reprint author), Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. EM bmarshallk@gmail.com; hiltonm@ukzn.ac.za RI Wollack, Edward/D-4467-2012; OI Wollack, Edward/0000-0002-7567-4451; Sievers, Jonathan/0000-0001-6903-5074; Menanteau, Felipe/0000-0002-1372-2534; Sifon, Cristobal/0000-0002-8149-1352 FU Rutgers University; National Research Foundation; University of KwaZulu-Natal; US National Science Foundation [AST-0408698, AST-0965625, PHY-0855887, PHY-1214379, AST-0955810, AST-1312380]; Princeton University; University of Pennsylvania; Canada Foundation for Innovation (CFI); Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT); CFI under the Compute Canada; Government of Ontario; Ontario Research Fund - Research Excellence; University of Toronto; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science FX We thank the anonymous referee for a number of suggestions that improved the quality of this paper. We thank Alastair Edge for useful discussions about known BCG quasar hosts. This work is based in large part on observations obtained with the SALT. Funding for SALT is provided in part by Rutgers University, a founding member of the SALT consortium. BK, MHi and KM acknowledge financial support from the National Research Foundation and the University of KwaZulu-Natal. This work was supported by the US National Science Foundation through awards AST-0408698 and AST-0965625 for the ACT project, as well as awards PHY-0855887 and PHY-1214379, along with awards AST-0955810 to AJB and AST-1312380 to AK. Funding was also provided by Princeton University, the University of Pennsylvania, and a Canada Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque Astronomico Atacama in northern Chile under the auspices of the Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT). Computations were performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by the CFI under the auspices of Compute Canada, the Government of Ontario, the Ontario Research Fund - Research Excellence; and the University of Toronto. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration (see the SDSS-III web site for details). NR 73 TC 6 Z9 6 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2015 VL 449 IS 4 BP 4010 EP 4026 DI 10.1093/mnras/stv595 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2VE UT WOS:000355342000051 ER PT J AU Holwerda, BW Baldry, IK Alpaslan, M Bauer, A Bland-Hawthorn, J Brough, S Brown, MJI Cluver, ME Conselice, C Driver, SP Hopkins, AM Jones, DH Lopez-Sanchez, AR Loveday, J Meyer, MJ Moffett, A AF Holwerda, B. W. Baldry, I. K. Alpaslan, M. Bauer, A. Bland-Hawthorn, J. Brough, S. Brown, M. J. I. Cluver, M. E. Conselice, C. Driver, S. P. Hopkins, A. M. Jones, D. H. Lopez-Sanchez, A. R. Loveday, J. Meyer, M. J. Moffett, A. TI Galaxy And Mass Assembly (GAMA) blended spectra catalogue: strong galaxy-galaxy lens and occulting galaxy pair candidates SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: strong; catalogues; dust, extinction; galaxies: distances and redshifts; galaxies: statistics ID DIGITAL-SKY-SURVEY; SPECTROSCOPICALLY SELECTED SAMPLE; BACKLIT SPIRAL GALAXIES; SYNTHETIC FIELD METHOD; DUST ENERGY-BALANCE; ACS SURVEY; SEEING GALAXIES; NGC 891; OVERLAPPING GALAXIES; INTERNAL STRUCTURE AB We present the catalogue of blended galaxy spectra from the Galaxy And Mass Assembly (GAMA) survey. These are cases where light from two galaxies are significantly detected in a single GAMA fibre. Galaxy pairs identified from their blended spectrum fall into two principal classes: they are either strong lenses, a passive galaxy lensing an emission-line galaxy; or occulting galaxies, serendipitous overlaps of two galaxies, of any type. Blended spectra can thus be used to reliably identify strong lenses for follow-up observations (high-resolution imaging) and occulting pairs, especially those that are a late-type partly obscuring an early-type galaxy which are of interest for the study of dust content of spiral and irregular galaxies. The GAMA survey setup and its AUTOZ automated redshift determination were used to identify candidate blended galaxy spectra from the cross-correlation peaks. We identify 280 blended spectra with a minimum velocity separation of 600 km s(-1), of which 104 are lens pair candidates, 71 emission-line-passive pairs, 78 are pairs of emission-line galaxies and 27 are pairs of galaxies with passive spectra. We have visually inspected the candidates in the Sloan Digital Sky Survey (SDSS) and Kilo Degree Survey (KiDS) images. Many blended objects are ellipticals with blue fuzz (Ef in our classification). These latter 'Ef' classifications are candidates for possible strong lenses, massive ellipticals with an emission-line galaxy in one or more lensed images. The GAMA lens and occulting galaxy candidate samples are similar in size to those identified in the entire SDSS. This blended spectrum sample stands as a testament of the power of this highly complete, second-largest spectroscopic survey in existence and offers the possibility to expand e.g. strong gravitational lens surveys. C1 [Holwerda, B. W.] Leiden Univ, Sterrenwacht Leiden, NL-2333 CA Leiden, Netherlands. [Baldry, I. K.] Liverpool John Moores Univ, Astrophys Res Inst, IC2, Liverpool L3 5RF, Merseyside, England. [Alpaslan, M.] NASA, Ames Res Ctr, Mountain View, CA 94034 USA. [Bauer, A.; Brough, S.; Hopkins, A. M.; Lopez-Sanchez, A. R.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Bland-Hawthorn, J.] Sydney Inst Astron, Sch Phys A28, Sydney, NSW 2006, Australia. [Brown, M. J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Cluver, M. E.] Univ Western Cape, Dept Phys, ZA-7530 Bellville, South Africa. [Conselice, C.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Driver, S. P.; Meyer, M. J.; Moffett, A.] Univ Western Australia, ICRAR M468, Crawley, WA 6009, Australia. [Driver, S. P.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Lopez-Sanchez, A. R.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia. [Loveday, J.] Univ Sussex, Astron Ctr, Brighton BN1 9QH, E Sussex, England. RP Holwerda, BW (reprint author), Leiden Univ, Sterrenwacht Leiden, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands. EM benne.holwerda@gmail.com RI Driver, Simon/H-9115-2014; Brown, Michael/B-1181-2015; OI Driver, Simon/0000-0001-9491-7327; Brown, Michael/0000-0002-1207-9137; Alpaslan, Mehmet/0000-0003-0321-1033; Baldry, Ivan/0000-0003-0719-9385 FU European Space Agency; STFC (UK); ARC (Australia); AAO; Australian Research Council [FT100100280]; National Aeronautics and Space Administration FX The authors thank the referee for his or her comments and suggestions. The lead author thanks the European Space Agency for the support of the Research Fellowship programme and the whole GAMA team for a magnificent observational effort. 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 SDSS and the United Kingdom Infrared Telescope Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programmes including GALEX MIS, VST KiDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT and ASKAP providing UV to radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO, and the participating institutions. The GAMA website is www.gamasurvey.org/. MJIB acknowledges financial support from the Australian Research Council (FT100100280) This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of NASA's Astrophysics Data System. NR 71 TC 2 Z9 2 U1 1 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2015 VL 449 IS 4 BP 4277 EP 4287 DI 10.1093/mnras/stv589 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2VE UT WOS:000355342000069 ER PT J AU Wang, LY Viero, M Ross, NP Asboth, V Bethermin, M Bock, J Clements, D Conley, A Cooray, A Farrah, D Hajian, A Han, JX Lagache, G Marsden, G Myers, A Norberg, P Oliver, S Page, M Symeonidis, M Schulz, B Wang, WT Zemcov, M AF Wang, Lingyu Viero, Marco Ross, Nicholas P. Asboth, Viktoria Bethermin, Matthieu Bock, Jamie Clements, Dave Conley, Alex Cooray, Asantha Farrah, Duncan Hajian, Amir Han, Jiaxin Lagache, Guilaine Marsden, Gaelen Myers, Adam Norberg, Peder Oliver, Seb Page, Mat Symeonidis, Myrto Schulz, Bernhard Wang, Wenting Zemcov, Mike TI Co-evolution of black hole growth and star formation from a cross-correlation analysis between quasars and the cosmic infrared background SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: haloes; galaxies: high-redshift; quasars: general; submillimetre: galaxies ID DIGITAL-SKY-SURVEY; OSCILLATION SPECTROSCOPIC SURVEY; ACTIVE GALACTIC NUCLEI; BARYON ACOUSTIC-OSCILLATIONS; HERSCHEL-SPIRE INSTRUMENT; 7TH DATA RELEASE; 9TH DATA RELEASE; 100 MU-M; SDSS-III; LUMINOSITY FUNCTION AB We present the first cross-correlation measurement between Sloan Digital Sky Survey type 1 quasars and the cosmic infrared background (CIB) measured by Herschel. The quasars cover the redshift range 0.15 < z < 3.5 where most of the CIB originates. We detect the sub-millimetre emission of the quasars, which dominates on small scales, and correlated emission from dusty star-forming galaxies (DSFGs) dominant on larger scales. The mean flux of the Data Release 7 (DR7) quasars (median redshift < z > = 1.4) is 11.1, 7.1 and 3.6 mJy at 250, 350 and 500 mu m, respectively, while the mean flux of the DR9 quasars (< z > = 2.5) is 5.7, 5.0 and 1.8 mJy at 250, 350 and 500 mu m, respectively. Assuming a modified blackbody spectral energy distribution with a power law in the mid-infrared, we infer that the mean infrared luminosity of the DR7 and DR9 quasars is 10(12.4) and 10(12.8) L-circle dot, respectively. The correlated emission arises from DSFGs in the same halo as the quasar (the one-halo term) and DSFGs in separate haloes correlated with the quasar-hosting halo (the two-halo term). Using a simple halo model, we find that most quasars are hosted by central galaxies. The host halo mass scale of the DR7 central and satellite quasars is 10(12.4 +/- 0.9) and 10(13.6 +/- 0.4) M-circle dot, respectively. The host halo mass scale of the DR9 central and satellite quasars is 10(12.3 +/- 0.6) and 10(12.8 +/- 0.4) M-circle dot, respectively. Thus, the halo environment of the central quasars is similar to that of the most actively star-forming galaxies, which supports the view that dusty starburst and quasar activity are evolutionarily linked. C1 [Wang, Lingyu; Han, Jiaxin; Norberg, Peder; Wang, Wenting] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. [Viero, Marco; Bock, Jamie; Zemcov, Mike] CALTECH, Pasadena, CA 91125 USA. [Ross, Nicholas P.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Asboth, Viktoria; Marsden, Gaelen] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Bethermin, Matthieu] European So Observ, D-85748 Garching, Germany. [Bock, Jamie; Schulz, Bernhard; Zemcov, Mike] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Clements, Dave] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2BZ, England. [Conley, Alex] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA. [Cooray, Asantha] Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA. [Farrah, Duncan] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Hajian, Amir] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Lagache, Guilaine] Inst Astrophys Spatiale, F-91405 Orsay, France. [Lagache, Guilaine] Univ Paris 11, Paris, France. [Lagache, Guilaine] CNRS, UMR 8617, F-75700 Paris, France. [Myers, Adam] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Oliver, Seb; Symeonidis, Myrto] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Page, Mat] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Schulz, Bernhard] CALTECH, JPL, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. RP Wang, LY (reprint author), Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. EM lingyu.wang25@gmail.com OI Bethermin, Matthieu/0000-0002-3915-2015 FU ERC StG grant [DEGAS-259586]; CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); NASA (USA); Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington; US Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New York University; Pennsylvania State University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; Yale University FX LW and PN acknowledge support from an ERC StG grant (DEGAS-259586).; SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA).; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS website is http://www.sdss.org/.; The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory and the University of Washington.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the US Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/.; 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. NR 86 TC 4 Z9 4 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 JUN 1 PY 2015 VL 449 IS 4 BP 4476 EP 4493 DI 10.1093/mnras/stv559 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2VE UT WOS:000355342000082 ER PT J AU Mamajanov, I Callahan, MP Dworkin, JP Cody, GD AF Mamajanov, Irena Callahan, Michael P. Dworkin, Jason P. Cody, George D. TI Prebiotic Alternatives to Proteins: Structure and Function of Hyperbranched Polyesters SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES LA English DT Article; Proceedings Paper CT Conference on Origins of Life and Evolution of Biospheres (OLEB) CY JUL 06-11, 2014 CL Nara, JAPAN DE Hyperbranched polymer; Polyester; Smart material; Protein; Size exclusion chromatography ID MOLECULAR-SIZE DISTRIBUTION; CITRIC-ACID; 3-DIMENSIONAL POLYMERS; AQUEOUS-SOLUTION; DRUG-DELIVERY; AMINO-ACIDS; CARBONACEOUS METEORITES; THERMAL SYNTHESIS; PEPTIDE FORMATION; FORMOSE REACTION AB Proteins are responsible multiple biological functions, such as ligand binding, catalysis, and ion channeling. This functionality is enabled by proteins' three-dimensional structures that require long polypeptides. Since plausibly prebiotic synthesis of functional polypeptides has proven challenging in the laboratory, we propose that these functions may have been initially performed by alternative macromolecular constructs, namely hyperbranched polymers (HBPs), during early stages of chemical evolution. HBPs can be straightforwardly synthesized in one-pot processes, possess globular structures determined by their architecture as opposed to folding in proteins, and have documented ligand binding and catalytic properties. Our initial study focuses on glycerol-citric acid HBPs synthesized via moderate heating in the dry state. The polymerization products consisted of a mixture of isomeric structures of varying molar mass as evidenced by NMR, mass spectrometry and size-exclusion chromatography. Addition of divalent cations during polymerization resulted in increased incorporation of citric acid into the HBPs and the possible formation of cation-oligomer complexes. The chelating properties of citric acid govern the makeup of the resulting polymer, turning the polymerization system into a rudimentary smart material. C1 [Mamajanov, Irena; Cody, George D.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. [Callahan, Michael P.; Dworkin, Jason P.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Callahan, Michael P.; Dworkin, Jason P.] NASA, Goddard Ctr Astrobiol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Mamajanov, I (reprint author), Carnegie Inst Sci, Geophys Lab, 5251 Broad Branch Rd NW, Washington, DC 20015 USA. EM imamajanov@ciw.edu RI Dworkin, Jason/C-9417-2012 OI Dworkin, Jason/0000-0002-3961-8997 NR 61 TC 0 Z9 0 U1 1 U2 22 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 JUN PY 2015 VL 45 IS 1-2 SI SI BP 123 EP 137 DI 10.1007/s11084-015-9430-9 PG 15 WC Biology SC Life Sciences & Biomedicine - Other Topics GA CJ9KC UT WOS:000355820100014 PM 25990933 ER PT J AU Wei, CY Pohorille, A AF Wei, Chenyu Pohorille, Andrew TI M2 Proton Channel: Toward a Model of a Primitive Proton Pump SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES LA English DT Article; Proceedings Paper CT Conference on Origins of Life and Evolution of Biospheres (OLEB) CY JUL 06-11, 2014 CL Nara, JAPAN DE Proton pump; Proton transport; Energy transduction; Ion channels; Membrane proteins ID INFLUENZA-A VIRUS; F0F1 ATP SYNTHASE; ION-CHANNEL; WEAK ACIDS; MECHANISM; TRANSPORT; BACTERIORHODOPSIN; SELECTIVITY; ACTIVATION; LIPOSOMES AB Transmembrane proton transfer was essential to early cellular systems in order to transduce energy for metabolic functions. The reliable, efficient and controlled generation of proton gradients became possible only with the emergence of active proton pumps. On the basis of features shared by most modern proton pumps we identify the essential mechanistic steps in active proton transport. Further, we discuss the mechanism of action of a small, transmembrane M2 proton channel from influenza A virus as a model for proton transport in protocells. The M2 channel is a 94-residue long, alpha-helical tetramer that is activated at low pH and exhibits high selectivity and directionality. A shorter construct, built of transmembrane fragments that are only 24 amino acids in length, exhibits very similar proton transport properties. Molecular dynamics simulations on the microsecond time-scale carried out for the M2 channel provided atomic level details on the activation of the channel in response to protonation of the histidine residue, His37. The pathway of proton conduction is mediated by His37, which accepts and donates protons at different interconverting conformation states when pH is lower than 6.5. The Val27 and Trp41 gates and the salt bridge between Asp44 and Arg45 further enhance the directionality of proton transport. It is argued that the architecture and the mechanism of action similar to that found in the M2 channel might have been the perfect starting point for evolution towards the earliest proton pumps, indicating that active proton transport could have readily emerged from simple, passive proton channels. C1 [Wei, Chenyu; Pohorille, Andrew] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Wei, Chenyu; Pohorille, Andrew] UCSF, Dept Pharmaceut Chem, San Francisco, CA 94143 USA. RP Pohorille, A (reprint author), NASA, Ames Res Ctr, Mail Stop 239-4, Moffett Field, CA 94035 USA. EM Andrew.Pohorille@nasa.gov NR 42 TC 2 Z9 2 U1 4 U2 20 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 JUN PY 2015 VL 45 IS 1-2 SI SI BP 241 EP 248 DI 10.1007/s11084-015-9421-x PG 8 WC Biology SC Life Sciences & Biomedicine - Other Topics GA CJ9KC UT WOS:000355820100025 PM 25777465 ER PT J AU Wallis, DD Miles, DM Narod, BB Bennest, JR Murphy, KR Mann, IR Yau, AW AF Wallis, D. D. Miles, D. M. Narod, B. B. Bennest, J. R. Murphy, K. R. Mann, I. R. Yau, A. W. TI The CASSIOPE/e-POP Magnetic Field Instrument (MGF) SO SPACE SCIENCE REVIEWS LA English DT Review DE Magnetometer; Fluxgate; Satellite; Field-aligned currents ID ALIGNED CURRENTS; BIRKELAND CURRENTS; MAGNETOMETER DATA; ARRAY AB Field-aligned currents couple energy between the Earth's magnetosphere and ionosphere and are responsible for driving both micro and macro motions of plasma and neutral atoms in both regimes. These currents are believed to be a contributing energy source for ion acceleration in the polar ionosphere and may be detected via measurements of magnetic gradients along the track of a polar orbiting spacecraft, usually the north-south gradients of the east-west field component. The detection of such gradients does not require observatory class measurements of the geomagnetic field. The Magnetic Field instrument (MGF) measures the local magnetic field onboard the Enhanced Polar Outflow Probe (e-POP) satellite by using two ring-core fluxgate sensors to characterize and remove the stray spacecraft field. The fluxgate sensors have their heritage in the MAGSAT design, are double wound for reduced mass and cross-field dependence, and are mounted on a modest 0.9 m carbon-fiber boom. The MGF samples the magnetic field 160 times per sec (similar to 50 meters) to a resolution of 0.0625 nT and outputs data at 1952 bytes per second including temperature measurements. Its power consumption is 2.2 watts, and its noise level is 7 pT per root Hz at 1 Hz. C1 [Wallis, D. D.] Magnametrics, Ottawa, ON, Canada. [Wallis, D. D.; Yau, A. W.] Univ Calgary, Calgary, AB, Canada. [Miles, D. M.; Mann, I. R.] Univ Alberta, Edmonton, AB, Canada. [Narod, B. B.] Narod Geophys Ltd, Vancouver, BC, Canada. [Narod, B. B.] Univ British Columbia, Vancouver, BC V5Z 1M9, Canada. [Bennest, J. R.] Bennest Enterprises Ltd, Summerland, BC, Canada. [Murphy, K. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Miles, DM (reprint author), Univ Alberta, Edmonton, AB, Canada. EM David.Miles@ualberta.ca OI Miles, David/0000-0002-4714-5966 FU NSERC; Canadian Space Agency; Canadian NSERC PGSD2 graduate scholarship; NSERC Industrial Research Chair and Discovery Grant programs FX We acknowledge the support from the Canadian Space Agency for the development and operation of the CASSIOPE/e-POP mission. The authors are grateful for the support and guidance of R. Hum. We thank J. Schmidt of Minerva Technology Inc. for his contributions to the flight firmware, W. Lunscher and his team at COM DEV for their technical assistance, and the technical team at Magellan Aerospace Corporation for the boom development. K.R. Murphy is supported by an NSERC Postdoctoral fellowship. D.M. Miles is supported by grants from the Canadian Space Agency and a Canadian NSERC PGSD2 graduate scholarship. I. R. Mann is supported by an NSERC Discovery Grant. A. W. Yau is supported by grants from the Canadian Space Agency and the NSERC Industrial Research Chair and Discovery Grant programs. NR 18 TC 4 Z9 4 U1 0 U2 12 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD JUN PY 2015 VL 189 IS 1-4 BP 27 EP 39 DI 10.1007/s11214-014-0105-z PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK1PU UT WOS:000355980100004 ER PT J AU Bedka, KM Wang, C Rogers, R Carey, LD Feltz, W Kanak, J AF Bedka, Kristopher M. Wang, Cecilia Rogers, Ryan Carey, Lawrence D. Feltz, Wayne Kanak, Jan TI Examining Deep Convective Cloud Evolution Using Total Lightning, WSR-88D, and GOES-14 Super Rapid Scan Datasets* SO WEATHER AND FORECASTING LA English DT Article ID SEVERE WEATHER; DETECTION NETWORK; UNITED-STATES; ENHANCED-V; GOES-R; SATELLITE; TOP AB The Geostationary Operational Environmental Satellite-14 (GOES-14) Imager operated in 1-min Super Rapid Scan Operations for GOES-R (SRSOR) mode during summer and fall of 2012 to emulate the high temporal resolution sampling of the GOES-R Advanced Baseline Imager (ABI). The current GOES operational scan interval is 15-30 min, which is too coarse to capture details important for severe convective storm forecasting including 1) when indicators of a severe storm such as rapid cloud-top cooling, overshooting tops, and above-anvil cirrus plumes first appear; 2) how satellite-observed cloud tops truly evolve over time; and 3) how satellite cloud-top observations compare with radar and lightning observations at high temporal resolution. In this paper, SRSOR data, radar, and lightning observations are used to analyze five convective storms, four of which were severe, to address these uncertainties. GOES cloud-top cooling, increased lightning flash rates, and peak precipitation echo tops often preceded severe weather, signaling rapid intensification of the storm updraft. Near the time of several severe hail or damaging wind events, GOES cloud-top temperatures and radar echo tops were warming rapidly, which indicated variability in the storm updraft that could have allowed the hail and wind gusts to reach the surface. Above-anvil cirrus plumes were another prominent indicator of impending severe weather. Detailed analysis of storms throughout the 2012 SRSOR period indicates that 57% of the plume-producing storms were severe and 85% of plumes from severe storms appeared before a severe weather report with an average lead time of 18 min, 9 min earlier than what would be observed by GOES operational scanning. C1 [Bedka, Kristopher M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Wang, Cecilia] Sci Syst & Applicat Inc, Hampton, VA USA. [Rogers, Ryan; Carey, Lawrence D.] Univ Alabama, Huntsville, AL 35899 USA. [Feltz, Wayne] Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI USA. [Kanak, Jan] Slovak Hydrometeorol Inst, Bratislava, Slovakia. RP Bedka, KM (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. EM kristopher.m.bedka@nasa.gov FU GOES-R Risk Reduction Research (R3) program FX This research has been supported by the GOES-R Risk Reduction Research (R3) program. In particular, we thank Dr. Steven Goodman, senior (chief) scientist, GOES-R System Program, for his guidance and support throughout this effort. The authors would also like to thank Tim Schmit (NOAA/NESDIS) and Martin Setvak (CHMI) for their valuable comments on this work. An additional thank you goes to NOAA/NESDIS for collecting the GOES-14 SRSOR data. NR 37 TC 11 Z9 11 U1 2 U2 17 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 JUN PY 2015 VL 30 IS 3 BP 571 EP 590 DI 10.1175/WAF-D-14-00062.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CJ7FG UT WOS:000355659300004 ER PT J AU Sasso, JP Eves, ND Christensen, JF Koelwyn, GJ Scott, J Jones, LW AF Sasso, John P. Eves, Neil D. Christensen, Jesper F. Koelwyn, Graeme J. Scott, Jessica Jones, Lee W. TI A framework for prescription in exercise-oncology research SO JOURNAL OF CACHEXIA SARCOPENIA AND MUSCLE LA English DT Editorial Material ID RANDOMIZED CONTROLLED-TRIAL; OPERABLE BREAST-CANCER; QUALITY-OF-LIFE; PHYSICAL-ACTIVITY; HEART-RATE; AEROBIC EXERCISE; CLINICAL-TRIALS; FUTURE-RESEARCH; SURVIVORS; METAANALYSIS AB The field of exercise-oncology has increased dramatically over the past two decades, with close to 100 published studies investigating the efficacy of structured exercise training interventions in patients with cancer. Of interest, despite considerable differences in study population and primary study end point, the vast majority of studies have tested the efficacy of an exercise prescription that adhered to traditional guidelines consisting of either supervised or home-based endurance (aerobic) training or endurance training combined with resistance training, prescribed at a moderate intensity (50-75% of a predetermined physiological parameter, typically age-predicted heart rate maximum or reserve), for two to three sessions per week, for 10 to 60 min per exercise session, for 12 to 15 weeks. The use of generic exercise prescriptions may, however, be masking the full therapeutic potential of exercise treatment in the oncology setting. Against this background, this opinion paper provides an overview of the fundamental tenets of human exercise physiology known as the principles of training, with specific application of these principles in the design and conduct of clinical trials in exercise-oncology research. We contend that the application of these guidelines will ensure continued progress in the field while optimizing the safety and efficacy of exercise treatment following a cancer diagnosis. C1 [Sasso, John P.; Jones, Lee W.] Mem Sloan Kettering Canc Ctr, New York, NY 10021 USA. [Eves, Neil D.] Univ British Columbia Okanagan, Sch Hlth & Exercise Sci, Ctr Heart Lung & Vasc Hlth, Kelowna, BC, Canada. [Christensen, Jesper F.] Rigshosp, Dept Infect Dis, Ctr Inflammat & Metab, DK-2100 Copenhagen, Denmark. [Christensen, Jesper F.] Rigshosp, Dept Infect Dis, Ctr Phys Act Res CIM CFAS, DK-2100 Copenhagen, Denmark. [Koelwyn, Graeme J.] NYU, Sch Med, Sackler Inst Grad Biomed Sci, New York, NY USA. [Scott, Jessica] NASA, Lyndon B Johnson Space Ctr, Univ Space Res Assoc, Houston, TX 77058 USA. RP Sasso, JP (reprint author), Mem Sloan Kettering Canc Ctr, 1275 York Ave, New York, NY 10021 USA. FU NCI NIH HHS [P30 CA008748] NR 50 TC 14 Z9 14 U1 0 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2190-5991 EI 2190-6009 J9 J CACHEXIA SARCOPENI JI J. Caxhexia Sarcopenia Muscle PD JUN PY 2015 VL 6 IS 2 BP 115 EP 124 DI 10.1002/jcsm.12042 PG 10 WC Medicine, General & Internal SC General & Internal Medicine GA CJ2UP UT WOS:000355340500001 PM 26136187 ER PT J AU Tompson, SR AF Tompson, Sara R. TI Applied Minds: How Engineers Think. SO LIBRARY JOURNAL LA English DT Book Review C1 [Tompson, Sara R.] Jet Prop Lab Lib, Arch & Records Sect, Pasadena, CA 91109 USA. RP Tompson, SR (reprint author), Jet Prop Lab Lib, Arch & Records Sect, Pasadena, CA 91109 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 1 PY 2015 VL 140 IS 10 BP 130 EP 130 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA CJ3MK UT WOS:000355387900221 ER PT J AU Horz, F Archer, PD Niles, PB Zolensky, ME Evans, M AF Hoerz, F. Archer, P. D., Jr. Niles, P. B. Zolensky, M. E. Evans, M. TI Devolatilization or melting of carbonates at Meteor Crater, AZ? SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID SILICATE LIQUID IMMISCIBILITY; IMPACT-MELT; SHOCK METAMORPHISM; TERRESTRIAL IMPACT; RIES CRATER; ROCKS; GEOCHEMISTRY; SUEVITE; GLASS; ARIZONA AB We have investigated the carbonates in the impact melts and in a monolithic clast of highly shocked Coconino sandstone of Meteor Crater, AZ to evaluate whether melting or devolatilization is the dominant response of carbonates during high-speed meteorite impact. Both melt- and clast-carbonates are calcites that have identical crystal habits and that contain anomalously high SiO2 and Al2O3. Also, both calcite occurrences lack any meteoritic contamination, such as Fe or Ni, which is otherwise abundantly observed in all other impact melts and their crystallization products at Meteor Crater. The carbon and oxygen isotope systematics for both calcite deposits suggest a low temperature environment (<100 degrees C) for their precipitation from an aqueous solution, consistent with caliche. We furthermore subjected bulk melt beads to thermogravimetric analysis and monitored the evolving volatiles with a quadrupole mass spectrometer. CO2 yields were <5wt%, with typical values in the 2wt% range; also total CO2 loss is positively correlated with H2O loss, an indication that most of these volatiles derive from the secondary calcite. Also, transparent glasses, considered the most pristine impact melts, yield 100 wt% element totals by EMPA, suggesting complete loss of CO2. The target dolomite decomposed into MgO, CaO, and CO2; the CO2 escaped and the CaO and MgO combined with SiO2 from coexisting quartz and FeO from the impactor to produce the dominant impact melt at Meteor Crater. Although confined to Meteor Crater, these findings are in stark contrast to Osinski etal. (2008) who proposed that melting of carbonates, rather than devolatilization, is the dominant process during hypervelocity impact into carbonate-bearing targets, including Meteor Crater. C1 [Hoerz, F.] LZ Technol Inc, Houston, TX 77058 USA. [Archer, P. D., Jr.] NASA, Johnson Space Ctr, Jacobs, Houston, TX 77058 USA. [Niles, P. B.; Zolensky, M. E.; Evans, M.] NASA, Johnson Space Ctr, ARES, Houston, TX 77058 USA. [Evans, M.] Texas A&M Univ, College Stn, TX 77843 USA. RP Horz, F (reprint author), LZ Technol Inc, 1110 NASA Pkwy, Houston, TX 77058 USA. EM friedrich.p.horz@nasa.gov FU NASA's Planetary Geology and Geophysics Program; Mars Fundamental Research Program; Cosmochemistry Program FX We thank Anne Peslier (EMPA), Kent D. Ross (SEM), and James Martinez (EBSD) for their assistance in generating some of the analyses reported here. The Meteor Crater samples were generously provided from Nininger's original "impactite" collection by the Center for Meteorite Studies, ASU, Tempe, AZ (all MCxx samples) and by J. Haggerty, USGS Flagstaff, AZ (MCH samples), or collected in the field by the senior author (COC5). Fruitful discussions with M. J. Cintala, D. Mittlefehldt, T. H. See, and D. Stoffler shaped our thinking. Constructive reviews by Alex Deutsch, Boris Ivanov, and AE Uwe Reimold lead to a much improved article. This work was supported by NASA's Planetary Geology and Geophysics (F.H), Mars Fundamental Research (D. A.), and Cosmochemistry Programs (PBN and MEZ). NR 68 TC 6 Z9 6 U1 3 U2 12 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUN PY 2015 VL 50 IS 6 BP 1050 EP 1070 DI 10.1111/maps.12453 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CJ1WQ UT WOS:000355276100004 ER PT J AU Keil, K Zucolotto, ME Krot, AN Doyle, PM Telus, M Krot, TV Greenwood, RC Franchi, IA Wasson, JT Welten, KC Caffee, MW Sears, DWG Riebe, M Wieler, R dos Santos, E Scorzelli, RB Gattacceca, J Lagroix, F Laubenstein, M Mendes, JC Schmitt-Kopplin, P Harir, M Moutinho, ALR AF Keil, Klaus Zucolotto, Maria E. Krot, Alexander N. Doyle, Patricia M. Telus, Myriam Krot, Tatiana V. Greenwood, Richard C. Franchi, Ian A. Wasson, John T. Welten, Kees C. Caffee, Marc W. Sears, Derek W. G. Riebe, My Wieler, Rainer dos Santos, Edivaldo Scorzelli, Rosa B. Gattacceca, Jerome Lagroix, France Laubenstein, Matthias Mendes, Julio C. Schmitt-Kopplin, Philippe Harir, Mourad Moutinho, Andre L. R. TI The Vicencia meteorite fall: A new unshocked (S1) weakly metamorphosed (3.2) LL chondrite SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID UNEQUILIBRATED ORDINARY CHONDRITES; STONY METEORITES; ORGANIC-MATTER; EXPOSURE AGES; NOBLE-GASES; CARBONACEOUS CHONDRITES; COSMOGENIC NUCLIDES; PRODUCTION-RATES; OXYGEN-ISOTOPE; PARENT-BODY AB The Vicencia meteorite, a stone of 1.547kg, fell on September 21, 2013, at the village Borracha, near the city of Vicencia, Pernambuco, Brazil. It was recovered immediately after the fall, and our consortium study showed it to be an unshocked (S1) LL3.2 ordinary chondrite. The LL group classification is based on the bulk density (3.13gcm(-3)); the chondrule mean apparent diameter (0.9mm); the bulk oxygen isotopic composition (O-17=3.768 +/- 0.042 parts per thousand, O-18=5.359 +/- 0.042 parts per thousand, O-17=0.981 +/- 0.020 parts per thousand); the content of metallic Fe,Ni (1.8 vol%); the Co content of kamacite (1.73 wt%); the bulk contents of the siderophile elements Ir and Co versus Au; and the ratios of metallic Fe-0/total iron (0.105) versus total Fe/Mg (1.164), and of Ni/Mg (0.057) versus total Fe/Mg. The petrologic type 3.2 classification is indicated by the beautifully developed chondritic texture, the standard deviation (similar to 0.09) versus mean Cr2O3 content (similar to 0.14 wt%) of ferroan olivine, the TL sensitivity and the peak temperature and peak width at half maximum, the cathodoluminescence properties of chondrules, the content of trapped Xe-132(tr) (0.317x10(-8)cm(3)STPg(-1)), and the Raman spectra for organic material in the matrix. The cosmic ray exposure age is similar to 72Ma, which is at the upper end of the age distribution of LL group chondrites. The meteorite is unusual in that it contains relatively large, up to nearly 100m in size, secondary fayalite grains, defined as olivine with Fa(>75), large enough to allow insitu measurement of oxygen and Mn-Cr isotope systematics with SIMS. Its oxygen isotopes plot along a mass-dependent fractionation line with a slope of similar to 0.5 and O-17 of 4.0 +/- 0.3 parts per thousand, and are similar to those of secondary fayalite and magnetite in the unequilibrated chondrites EET 90161, MET 96503, and Ngawi. These data suggest that secondary fayalite in Vicencia was in equilibrium with a fluid with a O-17 of similar to 4 parts per thousand, consistent with the composition of the fluid in equilibrium with secondary magnetite and fayalite in other unequilibrated ordinary chondrites. Secondary fayalite and the chondrule olivine phenocrysts in Vicencia are not in isotopic equilibrium, consistent with low-temperature formation of fayalite during aqueous alteration on the LL parent body. That alteration, as dated by the Mn-53-Cr-53 chronology age of secondary fayalite, took place 4.0-1.1+1.4 Ma after formation of CV CAIs when anchored to the quenched angrite D'Orbigny. C1 [Keil, Klaus; Krot, Alexander N.; Doyle, Patricia M.; Telus, Myriam; Krot, Tatiana V.] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Zucolotto, Maria E.] Museu Nacl UFRJ, Quinta da Boa Vista RJ, BR-20940040 Rio De Janeiro, Brazil. [Greenwood, Richard C.; Franchi, Ian A.] Open Univ, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England. [Wasson, John T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [Wasson, John T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Dept Chem & Biochem, Los Angeles, CA 90095 USA. [Welten, Kees C.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Caffee, Marc W.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Caffee, Marc W.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Riebe, My; Wieler, Rainer] ETH, Dept Earth Sci, CH-8092 Zurich, Switzerland. [dos Santos, Edivaldo; Scorzelli, Rosa B.] Ctr Brasileiro Pesquisas Fis, BR-22290180 Rio De Janeiro, Brazil. [Gattacceca, Jerome] Aix Marseille Univ, CNRS, CEREGE 34, F-13545 Aix En Provence, France. [Lagroix, France] IPGP, Paris, France. [Laubenstein, Matthias] Ist Nazl Fis Nucl, Lab Nazl Gran Sasso, I-67100 Assergi, AQ, Italy. [Mendes, Julio C.] Univ Fed Rio de Janeiro, Dept Geol, Rio de Janeiro, Brazil. [Schmitt-Kopplin, Philippe; Harir, Mourad] Helmholtz Zentrum Munchen, DES, D-85764 Neuherberg, Germany. RP Keil, K (reprint author), Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. EM keil@hawaii.edu RI Schmitt-Kopplin, Philippe/H-6271-2011; Caffee, Marc/K-7025-2015; Laubenstein, Matthias/C-4851-2013; Lagroix, France/A-6112-2011; OI Schmitt-Kopplin, Philippe/0000-0003-0824-2664; Caffee, Marc/0000-0002-6846-8967; Laubenstein, Matthias/0000-0001-5390-4343; Lagroix, France/0000-0003-2873-2767; Wasson, John/0000-0002-7253-2300 FU NASA Cosmochemistry Program [NNX10AH76G]; NASA [NNX10AG98G]; Swiss National Science Foundation; SSERVI FX The research of ANK, PMD, TVK, MT, and KK was supported in part by grant NNX10AH76G from the NASA Cosmochemistry Program (A. N. Krot, PI), that of JTW by NASA grant NNX10AG98G, that of KW by the NASA Cosmochemistry Program, and that of MR and RW by the Swiss National Science Foundation. DWGS is grateful to Chris McKay for support and Hazel Sears for assistance in the laboratory. The TL laboratory is supported by a SSERVI grant to the FINESSE project (PI: Jennifer Heldmann). We thank Alan Rubin, Addi Bischoff, and an anonymous reviewer for most valuable and constructive comments that have improved the manuscript considerably. "This is Hawai'i Institute of Geophysics and Planetology publication number 2169 and School of Ocean and Earth Science and Technology publication number 9424". NR 66 TC 4 Z9 4 U1 2 U2 19 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUN PY 2015 VL 50 IS 6 BP 1089 EP 1111 DI 10.1111/maps.12456 PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CJ1WQ UT WOS:000355276100006 ER PT J AU Hall, DK Crawford, CJ DiGirolamo, NE Riggs, GA Foster, JL AF Hall, Dorothy K. Crawford, Christopher J. DiGirolamo, Nicolo E. Riggs, George A. Foster, James L. TI Detection of earlier snowmelt in the Wind River Range, Wyoming, using Landsat imagery, 1972-2013 SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Wind River Range; Snowmelt; Snow-cover depletion curves; Landsat; MODIS ID WESTERN UNITED-STATES; NORTH-AMERICA; CONTINENTAL GLACIER; COVER; SNOWPACK; MODIS; VARIABILITY; STREAMFLOW; USA; PRECIPITATION AB In the western United States snow has been melting earlier in recent decades due to warmer winter and spring weather. This is particularly noticeable in the Pacific Northwest and coastal areas, yet has been less obvious in locations farther inland. Using the historical Landsat image archive, snow cover was mapped in the Wind River Range (WRR) in northwestern Wyoming, from 1972-2013. The objective of this work was to estimate the temporal change in the rate of snowmelt in the Fremont Lake basin of the WRR for the 42-year study period. Much of the streamflow in Wyoming originates from melting snow in the WRR. Streamflow is a significant contributor to the water resources for the north-central part of the state and has tremendous societal and economic impacts especially during the prolonged drought that is affecting the western U.S. Consistent with the ongoing and severe drought, data from the Pine Creek Above Fremont Lake gauge show a striking reduction in cumulative stream discharge in the 2000s vs. the decades of the 1970s, 1980s and 1990s. Snow-cover depletion curves derived from snow maps created from Landsat imagery were generated for the period 1972-2013. MODerate-Resolution Imaging Spectroradiometer (MODIS)-derived standard snow-cover maps were also used to generate snow-cover depletion curves, from 2000-2013, to provide an accuracy assessment of the Landsat technique. Landsat-derived mean snow-cover depletion curves from 2000-2013 and from the three previous decades, show that snow cover in the Fremont lake basin is melting 16 +/- 10 days earlier, on average, in the 2000s compared to the period from 1972-1999. Increasing spring and summer nighttime air temperature is the likely driver of the earlier snowmelt documented in the Landsat record. (C) 2015 Published by Elsevier Inc. C1 [Hall, Dorothy K.] NASA, Cryospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Crawford, Christopher J.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. [DiGirolamo, Nicolo E.; Riggs, George A.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Foster, James L.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. RP Hall, DK (reprint author), NASA, Cryospher Sci Lab, Goddard Space Flight Ctr, Code 615, Greenbelt, MD 20771 USA. FU NASA through the MODIS Science Team and Earth Observing System Program; NASA Postdoctoral Program [NNH06CC03B] FX The research conducted at Goddard Space Flight Center (GSFC) was supported by NASA through the MODIS Science Team and Earth Observing System Program. Christopher J. Crawford was funded through a NASA Postdoctoral Program (NNH06CC03B) appointment at the Goddard Space Flight Center administrated by Oak Ridge Associated Universities. Valuable discussions were held with personnel at the Pinedale Ranger District in Wyoming providing much useful information that inspired this work. NR 44 TC 3 Z9 3 U1 5 U2 26 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 JUN 1 PY 2015 VL 162 BP 45 EP 54 DI 10.1016/j.rse.2015.01.032 PG 10 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA CI8WI UT WOS:000355052000004 ER PT J AU Muller, D Krasemann, H Brewin, RJW Brockmann, C Deschamps, PY Doerffer, R Fomferra, N Franz, BA Grant, MG Groom, SB Melin, F Platt, T Regner, P Sathyendranath, S Steinmetz, F Swinton, J AF Mueller, Dagmar Krasemann, Hajo Brewin, Robert J. W. Brockmann, Carsten Deschamps, Pierre-Yves Doerffer, Roland Fomferra, Norman Franz, Bryan A. Grant, Mike G. Groom, Steve B. Melin, Frederic Platt, Trevor Regner, Peter Sathyendranath, Shubha Steinmetz, Francois Swinton, John TI The Ocean Colour Climate Change Initiative: II. Spatial and temporal homogeneity of satellite data retrieval due to systematic effects in atmospheric correction processors SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE OC-CCI; CCI; Ocean-Colour; Climate Change; Atmospheric correction; Algorithm comparison; Angular dependency; Systematic error ID MULTIPLE-SCATTERING; ALGORITHM; AEROSOLS; MERIS; RADIANCE; WATERS AB The established procedure to access the quality of atmospheric correction processors and their underlying algorithms is the comparison of satellite data products with related in-situ measurements. Although this approach addresses the accuracy of derived geophysical properties in a straight forward fashion, it is also limited in its ability to catch systematic sensor and processor dependent behaviour of satellite products along the scan-line, which might impair the usefulness of the data in spatial analyses. The Ocean Colour Climate Change Initiative (OC-CCI) aims to create an ocean colour dataset on a global scale to meet the demands of the ecosystem modelling community. The need for products with increasing spatial and temporal resolution that also show as little systematic and random errors as possible, increases. Due to cloud cover, even temporal means can be influenced by along-scanline artefacts if the observations are not balanced and effects cannot be cancelled out mutually. These effects can arise from a multitude of results which are not easily separated, if at all. Among the sources of artefacts, there are some sensor-specific calibration issues which should lead to similar responses in all processors, as well as processor-specific features which correspond with the individual choices in the algorithms. A set of methods is proposed and applied to MERIS data over two regions of interest in the North Atlantic and the South Pacific Gyre. The normalised water leaving reflectance products of four atmospheric correction processors, which have also been evaluated in match-up analysis, is analysed in order to find and interpret systematic effects across track. These results are summed up with a semi-objective ranking and are used as a complement to the match-up analysis in the decision for the best Atmospheric Correction (AC) processor. Although the need for discussion remains concerning the absolutes by which to judge an AC processor, this example demonstrates clearly, that relying on the match-up analysis alone can lead to misjudgement (C) 2015 Elsevier Inc All rights reserved. C1 [Mueller, Dagmar; Krasemann, Hajo; Doerffer, Roland] Helmholtz Zentrum Geesthacht, D-21502 Geesthacht, Germany. [Brewin, Robert J. W.; Grant, Mike G.; Groom, Steve B.; Platt, Trevor; Sathyendranath, Shubha] Plymouth Marine Lab, Plymouth PL1 3DH, Devon, England. [Brockmann, Carsten; Fomferra, Norman] Brockmann Consult, D-21502 Geesthacht, Germany. [Deschamps, Pierre-Yves; Steinmetz, Francois] HYGEOS, F-59000 Lille, France. [Franz, Bryan A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Melin, Frederic] European Commiss, Joint Res Ctr, Inst Environm & Sustainabil, I-21027 Ispra, Italy. [Regner, Peter] European Space Agcy, ESRIN, I-00044 Frascati, Italy. [Swinton, John] Telespazio VEGA UK Ltd, Luton LU1 3LU, Beds, England. RP Muller, D (reprint author), Helmholtz Zentrum Geesthacht, Max Planck Str 1, D-21502 Geesthacht, Germany. EM dagmar.mueller@hzg.de RI Franz, Bryan/D-6284-2012; OI Franz, Bryan/0000-0003-0293-2082; Brewin, Robert/0000-0001-5134-8291 NR 20 TC 2 Z9 2 U1 0 U2 10 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 JUN 1 PY 2015 VL 162 BP 257 EP 270 DI 10.1016/j.rse.2015.01.033 PG 14 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA CI8WI UT WOS:000355052000020 ER PT J AU Brewin, RJW Sathyendranath, S Muller, D Brockrnann, C Deschamps, PY Devred, E Doerffer, R Fomferra, N Franz, B Grant, M Groom, S Horseman, A Hu, C Krasemann, H Lee, Z Maritorena, S Meelin, F Peters, M Platt, T Regner, P Smyth, T Steinmetz, F Swinton, J Werdell, J White, GN AF Brewin, Robert J. W. Sathyendranath, Shubha Mueller, Dagmar Brockrnann, Carsten Deschamps, Pierre-Yves Devred, Emmanuel Doerffer, Roland Fomferra, Norman Franz, Bryan Grant, Mike Groom, Steve Horseman, Andrew Hu, Chuanmin Krasemann, Hajo Lee, ZhongPing Maritorena, Stephane Melin, Frederic Peters, Marco Platt, Trevor Regner, Peter Smyth, Tim Steinmetz, Francois Swinton, John Werdell, Jeremy White, George N., III TI The Ocean Colour Climate Change Initiative: III. A round-robin comparison on in-water bio-optical algorithms SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Phytoplankton; Ocean colour; Inherent Optical Properties; Remote sensing; Chlorophyll-a ID INHERENT OPTICAL-PROPERTIES; DISSOLVED ORGANIC-MATTER; SATELLITE DATA; SEMIANALYTICAL MODEL; MULTISENSOR APPROACH; SHALLOW WATERS; PACIFIC-OCEAN; DATA PRODUCTS; PHYTOPLANKTON; OPTIMIZATION AB Satellite-derived remote-sensing reflectance (R-rs) can be used for mapping biogeochemically relevant variables, such as the chlorophyll concentration and the Inherent Optical Properties (IOPs) of the water, at global scale for use in climate-change studies. Prior to generating such products, suitable algorithms have to be selected that are appropriate for the purpose. Algorithm selection needs to account for both qualitative and quantitative requirements. In this paper we develop an objective methodology designed to rank the quantitative performance of a suite of bio-optical models. The objective classification is applied using the NASA bio-Optical Marine Algorithm Dataset (NOMAD). Using in situ Rrs as input to the models, the performance of eleven semi-analytical models, as well as five empirical chlorophyll algorithms and an empirical diffuse attenuation coefficient algorithm, is ranked for spectrally-resolved IOPs, chlorophyll concentration and the diffuse attenuation coefficient at 489 nm. The sensitivity of the objective classification and the uncertainty in the ranking are tested using a Monte-Carlo approach (bootstrapping). Results indicate that the performance of the semi-analytical models varies depending on the product and wavelength of interest. For chlorophyll retrieval, empirical algorithms perform better than semi-analytical models, in general. The performance of these empirical models reflects either their immunity to scale errors or instrument noise in R data, or simply that the data used for model parameterisation were not independent of NOMAD. Nonetheless, uncertainty in the classification suggests that the performance of some semi-analytical algorithms at retrieving chlorophyll is comparable with the empirical algorithms. For phytoplankton absorption at 443 nm, some semi-analytical models also perform with similar accuracy to an empirical model: We discuss the potential biases, limitations and uncertainty in the approach, as well as additional qualitative considerations for algorithm selection for climate-change studies. Our classification has the potential to be routinely implemented, such that the performance of emerging algorithms can be compared with existing algorithms as they become available. In the long-term, such an approach will further aid algorithm development for ocean-colour studies. (C) 2013 Elsevier Inc All rights reserved. C1 [Brewin, Robert J. W.; Sathyendranath, Shubha; Grant, Mike; Groom, Steve; Horseman, Andrew; Platt, Trevor; Smyth, Tim] Plymouth Marine Lab, Plymouth PL1 3DH, Devon, England. [Brewin, Robert J. W.; Sathyendranath, Shubha] Plymouth Marine Lab, Natl Ctr Earth Observat, Plymouth PL1 3DH, Devon, England. [Mueller, Dagmar; Doerffer, Roland; Krasemann, Hajo] Helmholtz Zentrum Geesthacht, D-21502 Geesthacht, Germany. [Brockrnann, Carsten; Fomferra, Norman; Peters, Marco] Brockmann Consult, D-21502 Geesthacht, Germany. [Deschamps, Pierre-Yves; Steinmetz, Francois] HYGEOS, F-59000 Lille, France. [Devred, Emmanuel] Univ Laval, Quebec City, PQ G1V 0A6, Canada. [Franz, Bryan; Werdell, Jeremy] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hu, Chuanmin] Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA. [Lee, ZhongPing] Univ Massachusetts, Coll Sci & Math, Boston, MA 02125 USA. [Maritorena, Stephane] Univ Calif Santa Barbara, Earth Res Inst, Santa Barbara, CA 93106 USA. [Melin, Frederic] European Commiss, Joint Res Ctr, Inst Environm & Sustainabil, I-21027 Ispra, Italy. [Regner, Peter] European Space Agcy, ESRIN, I-00044 Frascati, Italy. [Swinton, John] Telespazio VEGA UK Ltd, Luton LU1 3LU, Beds, England. [White, George N., III] Bedford Inst Oceanog, Ocean Sci Div, Dartmouth, NS B2Y 4A2, Canada. RP Brewin, RJW (reprint author), Plymouth Marine Lab, Prospect Pl, Plymouth PL1 3DH, Devon, England. EM robr@pml.ac.uk OI Brewin, Robert/0000-0001-5134-8291 FU NASA SIMBIOS Program [NRA-96-MTPE-04, NRA-99-OES-09]; UK National Centre for Earth Observation FX NOMAD data were contributed by participants in the NASA SIMBIOS Program (NRA-96-MTPE-04 and NRA-99-OES-09) and by voluntary contributors. A cruise name accompanies each data record. Cruise details, including contributors' names, are available online (http://seabass.gsfc.nasa.gov/seabasscgi/nomad.cgi) using the General Search and Cruise Search utilities to facilitate communication, collaboration, and acknowledgement. NASA should be commended for the development of the NOMAD dataset and for on-going in situ activities. This work is a contribution to the Ocean Colour Climate Change Initiative of the European Space Agency and was supported by the UK National Centre for Earth Observation. NR 72 TC 21 Z9 21 U1 3 U2 30 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 JUN 1 PY 2015 VL 162 BP 271 EP 294 DI 10.1016/j.rse.2013.09.016 PG 24 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA CI8WI UT WOS:000355052000021 ER PT J AU Laeng, A Hubert, D Verhoelst, T von Clarmann, T Dinelli, BM Dudhia, A Raspollini, P Stiller, G Grabowski, U Keppens, A Kiefer, M Sofieva, V Froidevaux, L Walker, KA Lambert, JC Zehner, C AF Laeng, A. Hubert, D. Verhoelst, T. von Clarmann, T. Dinelli, B. M. Dudhia, A. Raspollini, P. Stiller, G. Grabowski, U. Keppens, A. Kiefer, M. Sofieva, V. Froidevaux, L. Walker, K. A. Lambert, J. -C. Zehner, C. TI The ozone climate change initiative: Comparison of four Level-2 processors for the Michelson Interferometer for Passive Atmospheric Sounding (MIPAS) SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE MIPAS; Ozone ID LIMB EMISSION-SPECTRA; MIPAS/ENVISAT MEASUREMENTS; TOMOGRAPHIC RETRIEVAL; REGULARIZATION METHOD; RADIATIVE-TRANSFER; VERTICAL PROFILES; AURA SATELLITE; TECHNICAL NOTE; EOS MLS; VALIDATION AB The MIPAS spectrometer onboard the Envisat platform observed infrared emission from the Earth's limb between 2002 and 2012. It recorded high-resolution spectra during day and night, from pole to pole and between 6 and 70 km altitude in the nominal measurement mode or up to 170 km in special measurement modes, producing daily more than 1000 vertical profiles of various trace gases. The operational Level-2 data are processed by ESA/DLR but there exist three other, independent research Level-2 processors that are hosted by ISAC-CNR/University of Bologna, Oxford University, and KIT IMK/IAA. All four Level-2 processors rely on the same Level-1b data provided by ESA but their retrieval schemes differ. As part of ESA's Ozone Climate Change Initiative project, an intercomparison of the four MIPAS processors took place, in which vertical ozone profiles retrieved by these four processors from MIPAS nominal mode measurements were compared for 2007 and 2008. We present the results of this comparison exercise, which consisted of five parts: an information content study of the vertical averaging kernels, an intercomparison of zonal seasonal means and spreads, a determination of biases through comparison to ozonesonde and lidar measurements, a comparison to other satellite records (bias estimation and precision assessment with respect to ACE-FTS and Aura-MLS data), and a geophysical validation of the provided error bars using MIPAS MIPAS collocations. The four processors demonstrate similar performance. All processors use the same Level-1b data from ESA, apply global fits, and use microwindows instead of the full spectrum. The main differences in the processing schemes include the choice of microwindows, the regularization approach, the treatment of negative retrieved values, and the cloud detection threshold. The different regularization schemes lead to a different trade-off between noise and resolution, but without a clear average advantage for any particular data set. The vertical resolution is typically 3-5 km and the single profile precision is about 2-3%. In the middle and upper stratosphere, at 25-45 km, all four MIPAS processors clearly show a high bias of 2 to 5% relative to all reference instruments. The similarity of the structure and magnitude of the bias among the MIPAS data sets indicates that the bias is most likely linked to the use of microwindows of the MIPAS AB band. The satellite intercomparisons show furthermore that for the KIT dataset, the onset of the high bias starts at a somewhat higher altitude (only above 35 km) than for the other three datasets. This is likely due to the more restrictive use of the AB band by the KIT processor, which comes at the cost of a coarser vertical resolution near the ozone volume mixing ratio (vmr) peak. In the troposphere, the Level-2 algorithms that suppress negative ozone values in the iterative retrieval process produce a larger positive bias than the algorithm that does not follow such a strategy. Our main conclusion is that the four MIPAS processors are more similar to each other than to any other reference instrument. This indicates that the observed biases are very likely instrument-related. (C) 2014 Elsevier Inc. All rights reserved. C1 [Laeng, A.; von Clarmann, T.; Stiller, G.; Grabowski, U.; Kiefer, M.] Karlsruhe Inst Technol, Inst Meteorol & Klimaforsch, D-76021 Karlsruhe, Germany. [Hubert, D.; Verhoelst, T.; Keppens, A.; Lambert, J. -C.] Belgian Inst Space Aeron BIRA IASB, Brussels, Belgium. [Dinelli, B. M.] CNR, ISAC, I-40126 Bologna, Italy. [Dudhia, A.] Univ Oxford, Oxford OX1 2JD, England. [Raspollini, P.] CNR, IFAC, Florence, Italy. [Sofieva, V.] Finnish Meteorol Inst, Helsinki, Finland. [Froidevaux, L.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Walker, K. A.] Univ Toronto, Toronto, ON M5S 1A1, Canada. [Zehner, C.] ESA, ESRIN, Frascati, Italy. RP Laeng, A (reprint author), Karlsruhe Inst Technol, Inst Meteorol & Klimaforsch, D-76021 Karlsruhe, Germany. EM alexandra.laeng@kit.edu RI Sofieva, Viktoria/E-1958-2014; OI Sofieva, Viktoria/0000-0002-9192-2208; Dinelli, Bianca Maria/0000-0002-1218-0008; Hubert, Daan/0000-0002-4365-865X FU Canadian Space Agency; National Aeronautics and Space Administration FX This work was performed in the frame of European Space Agency (ESA) project Ozone_cci. All four MIPAS teams acknowledge ESA for providing MIPAS Lib data. The ACE mission is supported primarily by the Canadian Space Agency. Work at the Jet Propulsion Laboratory was performed under contract with the National Aeronautics and Space Administration. NR 73 TC 5 Z9 5 U1 2 U2 13 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 JUN 1 PY 2015 VL 162 BP 316 EP 343 DI 10.1016/j.rse.2014.12.013 PG 28 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA CI8WI UT WOS:000355052000023 ER PT J AU Buchwitz, M Reuter, M Schneising, O Boesch, H Guerlet, S Dils, B Aben, I Armante, R Bergamaschi, P Blumenstock, T Bovensmann, H Brunner, D Buchmann, B Burrows, JP Butz, A Chedin, A Chevallier, F Crevoisier, CD Deutscher, NM Frankenberg, C Hase, F Hasekamp, OP Heymann, J Kaminski, T Laeng, A Lichtenberg, G De Maziere, M Noel, S Notholt, J Orphal, J Popp, C Parker, R Scholze, M Sussmann, R Stiller, GP Warneke, T Zehner, C Bril, A Crisp, D Griffith, DWT Kuze, A O'Dell, C Oshchepkov, S Sherlock, V Suto, H Wennberg, P Wunch, D Yokota, T Yoshida, Y AF Buchwitz, M. Reuter, M. Schneising, O. Boesch, H. Guerlet, S. Dils, B. Aben, I. Armante, R. Bergamaschi, P. Blumenstock, T. Bovensmann, H. Brunner, D. Buchmann, B. Burrows, J. P. Butz, A. Chedin, A. Chevallier, F. Crevoisier, C. D. Deutscher, N. M. Frankenberg, C. Hase, F. Hasekamp, O. P. Heymann, J. Kaminski, T. Laeng, A. Lichtenberg, G. De Maziere, M. Noel, S. Notholt, J. Orphal, J. Popp, C. Parker, R. Scholze, M. Sussmann, R. Stiller, G. P. Warneke, T. Zehner, C. Bril, A. Crisp, D. Griffith, D. W. T. Kuze, A. O'Dell, C. Oshchepkov, S. Sherlock, V. Suto, H. Wennberg, P. Wunch, D. Yokota, T. Yoshida, Y. TI The Greenhouse Gas Climate Change Initiative (GHG-CCI): Comparison and quality assessment of near-surface-sensitive satellite-derived CO2 and CH4 global data sets SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE SCIAMACHY; GOSAT; Greenhouse gases; Carbon dioxide; Methane; Climate change ID COLUMN OBSERVING NETWORK; HYPERSPECTRAL INFRARED OBSERVATIONS; ATMOSPHERIC CO2; RETRIEVAL ALGORITHM; CARBON-DIOXIDE; METHANE EMISSIONS; SOLAR OCCULTATION; THIN CLOUDS; 1ST YEAR; PART 1 AB The GHG-CCI project is one of several projects of the European Space Agency's (ESA) Climate Change Initiative (CCI). The goal of the CCI is to generate and deliver data sets of various satellite-derived Essential Climate Variables (ECVs) in line with GCOS (Global Climate Observing System) requirements. The "ECV Greenhouse Gases" (ECV GHG) is the global distribution of important climate relevant gases - atmospheric CO2 and CH4 - with a quality sufficient to obtain information on regional CO2 and CH4 sources and sinks. Two satellite instruments deliver the main input data for GHG-CCI: SCIAMACHY/ENVISAT and TANSO-FTS/GOSAT. The first order priority goal of GHG-CCI is the further development of retrieval algorithms for near-surface-sensitive column-averaged dry air mole fractions of CO2 and CH4, denoted XCO2 and XCH4, to meet the demanding user requirements. GHG-CCI focuses on four core data products: XCO2 from SCIAMACHY and TANSO and XCH4 from the same two sensors. For each of the four core data products at least two candidate retrieval algorithms have been independently further developed and the corresponding data products have been quality-assessed and inter-compared. This activity is referred to as "Round Robin" (RR) activity within the CCI. The main goal of the RR was to identify for each of the four core products which algorithms should be used to generate the Climate Research Data Package (CRDP). The CRDP will essentially be the first version of the ECV GHG. This manuscript gives an overview of the GHG-CCI RR and related activities. This comprises the establishment of the user requirements, the improvement of the candidate retrieval algorithms and comparisons with ground-based observations and models. The manuscript summarizes the final RR algorithm selection decision and its justification. Comparison with ground-based Total Carbon Column Observing Network (TCCON) data indicates that the "breakthrough" single measurement precision requirement has been met for SCIAMACHY and TANSO XCO2 (<3 ppm) and TANSO XCH4 (<17 ppb). The achieved relative accuracy for XCH4 is 3-15 ppb for SCIAMACHY and 2-8 ppb for TANSO depending on algorithm and time period. Meeting the 0.5 ppm systematic error requirement for XCO2 remains a challenge: approximately 1 ppm has been achieved at the validation sites but also larger differences have been found in regions remote from TCCON. More research is needed to identify the causes for the observed differences. In this context GHG-CCI suggests taking advantage of the ensemble of existing data products, for example, via the EnseMble Median Algorithm (EMMA). (C) 2013 Elsevier Inc All rights reserved. C1 [Buchwitz, M.; Reuter, M.; Schneising, O.; Bovensmann, H.; Burrows, J. P.; Deutscher, N. M.; Heymann, J.; Noel, S.; Notholt, J.; Warneke, T.] Univ Bremen, Inst Environm Phys IUP, D-28334 Bremen, Germany. [Boesch, H.] Univ Leicester, Leicester, Leics, England. [Guerlet, S.; Aben, I.; Hasekamp, O. P.] SRON Netherlands Inst Space Res, Utrecht, Netherlands. [Dils, B.; De Maziere, M.] Belgian Inst Space Aeron BIRA, Brussels, Belgium. [Lichtenberg, G.] Deutsch Zentrum Luft & Raumfahrt DLR, Oberpfaffenhofen, Germany. [Armante, R.; Chedin, A.; Crevoisier, C. D.] Meteorol Dynam Lab, Palaiseau, France. [Blumenstock, T.; Butz, A.; Hase, F.; Laeng, A.; Orphal, J.; Sussmann, R.; Stiller, G. P.] Karlsruhe Inst Technol, D-76021 Karlsruhe, Germany. [Blumenstock, T.; Butz, A.; Hase, F.; Laeng, A.; Orphal, J.; Sussmann, R.; Stiller, G. P.] Karlsruhe Inst Technol, Garmisch Partenkirchen, Germany. [Brunner, D.; Buchmann, B.; Popp, C.] Swiss Fed Labs Mat Sci & Technol Empa, Dubendorf, Switzerland. [Chevallier, F.] Lab Sci Climat & Environm, Gif Sur Yvette, France. [Bergamaschi, P.] European Commiss Joint Res Ctr EC JRC, Inst Environm & Sustainabil, Air & Climate Unit, Ispra, Italy. [Frankenberg, C.; Crisp, D.] Jet Prop Lab, Pasadena, CA USA. [Kaminski, T.; Scholze, M.] FastOpt GmbH, Hamburg, Germany. [Scholze, M.] Univ Bristol, Bristol, Avon, England. [Zehner, C.] European Space Agcy, ESRIN, Frascati, Italy. [Bril, A.; Oshchepkov, S.; Yokota, T.; Yoshida, Y.] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan. [Deutscher, N. M.; Griffith, D. W. T.] Univ Wollongong, Wollongong, NSW, Australia. [Kuze, A.; Suto, H.] Japan Aerosp Explorat Agcy JAXA, Tsukuba, Ibaraki, Japan. [O'Dell, C.] Colorado State Univ, Ft Collins, CO 80523 USA. [Sherlock, V.] Natl Inst Water & Atmospher Res NIWA, Lauder, New Zealand. [Wennberg, P.; Wunch, D.] CALTECH, Pasadena, CA 91125 USA. RP Buchwitz, M (reprint author), Univ Bremen, Inst Environm Phys IUP, FB1,Otto Hahn Allee 1, D-28334 Bremen, Germany. EM Michael.Buchwitz@iup.physik.uni-bremen.de RI Deutscher, Nicholas/E-3683-2015; Brunner, Dominik/A-1255-2009; Butz, Andre/A-7024-2013; Boesch, Hartmut/G-6021-2012; Chevallier, Frederic/E-9608-2016; Scholze, Marko/N-4573-2014; Reuter, Maximilian/L-3752-2014; KUZE, AKIHIKO/J-2074-2016; Bovensmann, Heinrich/P-4135-2016; Sussmann, Ralf/K-3999-2012; Frankenberg, Christian/A-2944-2013; Notholt, Justus/P-4520-2016; Burrows, John/B-6199-2014 OI Deutscher, Nicholas/0000-0002-2906-2577; Brunner, Dominik/0000-0002-4007-6902; Butz, Andre/0000-0003-0593-1608; Chevallier, Frederic/0000-0002-4327-3813; Scholze, Marko/0000-0002-3474-5938; Reuter, Maximilian/0000-0001-9141-3895; KUZE, AKIHIKO/0000-0001-5415-3377; Bovensmann, Heinrich/0000-0001-8882-4108; Frankenberg, Christian/0000-0002-0546-5857; Notholt, Justus/0000-0002-3324-885X; Burrows, John/0000-0002-6821-5580 FU ESA/ESRIN (GHG-CCI); EU (MACC-II) [283576]; DLR (SADOS); State of Bremen; University of Bremen; NASA [NNX11AG01G, NAG5-12247, NNG05-GD07G]; NASA Orbiting Carbon Observatory Program; DOE ARM program; Australian Research Council [DP0879468, LP0562346]; EU project IMECC; EU project GEOmon; Senate of Bremen FX This work was primarily funded by ESA/ESRIN (GHG-CCI) but also received funding from EU FP7 (grant agreement No. 283576, MACC-II), DLR (SADOS), and the State and the University of Bremen. We thank the members of the GOSAT Project (JAM, NIES, and Ministry of the Environment (MoE), Japan) for providing GOSAT Level 1B and Level 2 data products (GOSAT RA1 PI project CONSCIGO). The ACOS v2.9 data were produced by the ACOS/OCO-2 project at the Jet Propulsion Laboratory, California Institute of Technology, and obtained from the ACOS/OCO-2 data archive maintained at the NASA Goddard Earth Science Data and Information Services Center. We thank NOAA for making available the CarbonTracker CO2 fields. We also thank TCCON and related funding organizations (NASA grants NNX11AG01G, NAG5-12247, NNG05-GD07G, NASA Orbiting Carbon Observatory Program, DOE ARM program, the Australian Research Council, DP0879468 and LP0562346, the EU projects IMECC and GEOmon, the Senate of Bremen). Last but not least we would like to thank the two referees for helpful comments. NR 72 TC 20 Z9 20 U1 10 U2 80 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 JUN 1 PY 2015 VL 162 BP 344 EP 362 DI 10.1016/j.rse.2013.04.024 PG 19 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA CI8WI UT WOS:000355052000024 ER PT J AU Gates, M Stich, S McDonald, M Muirhead, B Mazanek, D Abell, P Lopez, P AF Gates, Michele Stich, Steve McDonald, Mark Muirhead, Brian Mazanek, Dan Abell, Paul Lopez, Pedro TI The Asteroid Redirect Mission and sustainable human exploration SO ACTA ASTRONAUTICA LA English DT Article DE Asteroid Redirect Mission; Human Space Exploration; Human exploration AB We present the importance of the Asteroid Redirect Mission (ARM) in the context of the Global Exploration Roadmap and NASA's strategy for sustainable human exploration. We also provide status toward baseline of the ARM, including evolution of concept development based on internal NASA analysis and risk reduction, as well as external inputs received. This includes development of mission concept options, key trade studies, and analysis of drivers for both the robotic and crewed mission segments. Published by Elsevier Ltd. on behalf of IAA. C1 [Gates, Michele] NASA Headquarters, Washington, DC 20546 USA. [Stich, Steve; McDonald, Mark; Abell, Paul; Lopez, Pedro] NASA, Lyndon B Johnson Space Ctr, Washington, DC USA. [Muirhead, Brian] NASA, Jet Prop Lab, Washington, DC USA. [Mazanek, Dan] NASA, Langley Res Ctr, Washington, DC USA. RP Gates, M (reprint author), NASA Headquarters, Washington, DC 20546 USA. EM michele.m.gates@nasa.gov; j.s.stich@nasa.gov; mark.a.mcdonald@nasa.gov; brian.k.muirhead@nasa.gov; daniel.d.mazanek@nasa.gov; paul.a.abell@nasa.gov; pedro.lopez-1@nasa.gov NR 7 TC 2 Z9 2 U1 1 U2 5 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 JUN-JUL PY 2015 VL 111 BP 29 EP 36 DI 10.1016/j.actaastro.2015.01.025 PG 8 WC Engineering, Aerospace SC Engineering GA CI2NY UT WOS:000354585500003 ER PT J AU Summerer, L Wilcox, RE Bechtel, R Harbison, S AF Summerer, L. Wilcox, R. E. Bechtel, R. Harbison, S. TI The International Safety Framework for nuclear power source applications in outer space-Useful and substantial guidance SO ACTA ASTRONAUTICA LA English DT Article DE Nuclear power sources; Safety; Safety framework; COPUOS; STSC AB In 2009, the International Safety Framework for Nuclear Power Source Applications in Outer Space was adopted, following a multi-year process that involved all major space faring nations under the auspices of a partnership between the UN Committee on the Peaceful Uses of Outer Space and the International Atomic Energy Agency. The Safety Framework reflects an international consensus on best practices to achieve safety. Following the 1992 UN Principles Relevant to the Use of Nuclear Power Sources in Outer Space, it is the second attempt by the international community to draft guidance promoting the safety of applications of nuclear power sources in space missions. NPS applications in space have unique safety considerations compared with terrestrial applications. Mission launch and outer space operational requirements impose size, mass and other space environment limitations not present for many terrestrial nuclear facilities. Potential accident conditions could expose nuclear power sources to extreme physical conditions. The Safety Framework is structured to provide guidance for both the programmatic and technical aspects of safety. In addition to sections containing specific guidance for governments and for management, it contains technical guidance pertinent to the design, development and all mission phases of space NPS applications. All sections of the Safety Framework contain elements directly relevant to engineers and space mission designers for missions involving space nuclear power sources. The challenge for organisations and engineers involved in the design and development processes of space nuclear power sources and applications is to implement the guidance provided in the Safety Framework by integrating it into the existing standard space mission infrastructure of design, development and operational requirements, practices and processes. This adds complexity to the standard space mission and launch approval processes. The Safety Framework is deliberately generic to remain relevantly independent of technological progress, of national organisational setups and of space mission types. Implementing its guidance therefore leaves room for interpretation and adaptation. Relying on reported practices, we analyse the guidance particularly relevant to engineers and space mission designers. (C) 2015 IAA. Published by Elsevier Ltd. All rights reserved. C1 [Summerer, L.] European Space Agcy, Adv Concepts Team, NL-2201 AZ Noordwijk, Netherlands. [Wilcox, R. E.] CALTECH, Jet Prop Lab, Project Support Off, Pasadena, CA 91109 USA. [Bechtel, R.] US DOE, Off Space & Def Power Syst, Washington, DC 20585 USA. [Harbison, S.] COPUOS STSC, NPS Working Grp, Vienna, Austria. RP Summerer, L (reprint author), European Space Agcy, Adv Concepts Team, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. EM leopold.summerer@esa.int; rwilcox@jpl.nasa.gov; ryan.bechtel@nuclear.energy.gov; SHarb67909@aol.com OI Summerer, Leopold/0000-0001-7742-5216 FU Jet Propulsion Laboratory, California Institute of Technology; National Aeronautics and Space Administration FX The paper has greatly benefited from information shared within the 2010-2015 work-plan of the Working Group on Space Nuclear Power Sources in Outer Space within the Scientific and Technical Subcommittee of the Committee on the Peaceful Uses of Outer Space. The views expressed in the paper are those of the authors and do not necessarily reflect the view of any entities with which the authors may be affiliated. Part of this work was supported by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 27 TC 1 Z9 1 U1 2 U2 3 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 JUN-JUL PY 2015 VL 111 BP 89 EP 101 DI 10.1016/j.actaastro.2015.02.007 PG 13 WC Engineering, Aerospace SC Engineering GA CI2NY UT WOS:000354585500009 ER PT J AU Boll, NJ Salazar, D Stelter, CJ Landis, GA Colozza, AJ AF Boll, Nathan J. Salazar, Denise Stelter, Christopher J. Landis, Geoffrey A. Colozza, Anthony J. TI Venus high temperature atmospheric dropsonde and extreme-environment seismometer (HADES) SO ACTA ASTRONAUTICA LA English DT Article DE Venus; Lander; Geology; Atmosphere; Seismometer; High-temperature ID FLUX RADIOMETER EXPERIMENT; PIONEER VENUS; MAGNETOMETER; ORBITER AB The atmospheric composition and geologic structure of Venus have been identified by the US National Research Council's Decadal Survey for Planetary Science as priority targets for scientific exploration; however, the high temperature and pressure at the surface, along with the highly corrosive chemistry of the Venus atmosphere, present significant obstacles to spacecraft design that have severely limited past and proposed landed missions. Following the methodology of the NASA Innovative Advanced Concepts (NIAC) proposal regime and the Collaborative Modeling and Parametric Assessment of Space Systems (COMPASS) design protocol, this paper presents a conceptual study and initial feasibility analysis for a Discovery-class Venus lander capable of an extended-duration mission at ambient temperature and pressure, incorporating emerging technologies within the field of high temperature electronics in combination with novel configurations of proven, high Technology Readiness Level (TRL) systems. Radioisotope Thermal Power (RTG) systems and silicon carbide (SiC) communications and data handling are examined in detail, and various high-temperature instruments are proposed, including a seismometer and an advanced photodiode imager. The study combines this technological analysis with proposals for a descent instrument package and a relay orbiter to demonstrate the viability of an integrated atmospheric and in-situ geologic exploratory mission that differs from previous proposals by greatly reducing the mass, power requirements, and cost, while achieving important scientific goals. Published by Elsevier Ltd. on behalf of IAA. C1 [Boll, Nathan J.] Univ Michigan, Ann Arbor, MI 48109 USA. [Salazar, Denise] Univ Texas Austin, Austin, TX 78712 USA. [Stelter, Christopher J.] NASA, Langley Res Ctr, Washington, DC USA. [Landis, Geoffrey A.; Colozza, Anthony J.] NASA, John H Glenn Res Ctr, Washington, DC USA. RP Boll, NJ (reprint author), Univ Michigan, Ann Arbor, MI 48109 USA. EM njboll@umich.edu; denise.salazar.1210@gmail.com; christopherstelter@gmail.com; geoffrey.landis@nasa.gov; anthony.j.colozza@nasa.gov NR 39 TC 1 Z9 1 U1 2 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JUN-JUL PY 2015 VL 111 BP 146 EP 159 DI 10.1016/j.actaastro.2015.02.008 PG 14 WC Engineering, Aerospace SC Engineering GA CI2NY UT WOS:000354585500013 ER PT J AU Barshi, I AF Barshi, Immanuel TI From Healy's Training Principles to Training Specifications: The Case of the Comprehensive LOFT SO AMERICAN JOURNAL OF PSYCHOLOGY LA English DT Article ID LEARNING CURRICULA; MEDICAL-EDUCATION; INSTRUCTION; CHALLENGE; SCHOOL AB Alice Healy has dedicated much of her work to questions of skill acquisition, retention, and transfer. In the process, she has come to identify numerous training principles that have been shown to promote the acquisition, retention, and transfer of knowledge and skills in laboratory studies. The goal of this article is to translate some of the training principles offered by Healy and her colleagues (Healy, Schneider, & Bourne, 2012) into real-world, practical training specifications for the particular context of pilot training at the airline level. The training approach described here suggests structuring all of airline pilot training as line-oriented flight training (LOFT), where the notion of "line" refers to the air-line drawn on a map between a departure airport and a destination airport. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Barshi, I (reprint author), NASA, Ames Res Ctr, Mail Stop 262-4, Moffett Field, CA 94035 USA. EM Immanuel.Barshi@nasa.gov NR 37 TC 0 Z9 0 U1 2 U2 3 PU UNIV ILLINOIS PRESS PI CHAMPAIGN PA 1325 S OAK ST, CHAMPAIGN, IL 61820-6903 USA SN 0002-9556 EI 1939-8298 J9 AM J PSYCHOL JI Am. J. Psychol. PD SUM PY 2015 VL 128 IS 2 BP 219 EP 227 PG 9 WC Psychology, Multidisciplinary SC Psychology GA CI4WF UT WOS:000354753900008 PM 26255441 ER PT J AU Lim, YK AF Lim, Young-Kwon TI The East Atlantic/West Russia (EA/WR) teleconnection in the North Atlantic: climate impact and relation to Rossby wave propagation SO CLIMATE DYNAMICS LA English DT Article DE Teleconnection; EA/WR; Climate impact; Rossby wave; Stationary wave model ID ATMOSPHERIC CIRCULATION; GEOPOTENTIAL HEIGHT; HEMISPHERE WINTER; DECADAL TRENDS; OSCILLATION; PATTERNS; PRECIPITATION; VARIABILITY; FREQUENCY; BLOCKING AB Large-scale winter teleconnection of the East Atlantic/West Russia (EA/WR) over the Atlantic and surrounding regions is examined in order to quantify its impacts on temperature and precipitation and identify the physical mechanisms responsible for its existence. A rotated empirical orthogonal function analysis of the upper-tropospheric monthly height field captures successfully the EA/WR pattern and its interannual variation, with the North Atlantic Oscillation (NAO) as the first mode. EA/WR's climate impact extends from eastern North America to Eurasia. The positive (negative) EA/WR produces positive (negative) temperature anomalies over the eastern US, western Europe and Russia east of Caspian Sea, with negative (positive) anomalies over eastern Canada, eastern Europe including Ural Mountains, northeastern Africa and the Middle East. These anomalies are largely explained by lower-tropospheric temperature advections. Positive (negative) precipitation anomalies are found over the mid-latitude Atlantic and central Russia around similar to 60 degrees anomaly is dominant. Eastern Canada and western Europe including the Mediterranean region are characterized by negative (positive) precipitation anomalies. The EA/WR is found to be closely associated with Rossby wave propagation. Wave activity fluxes show that it is strongly tied to large-scale stationary waves. Furthermore, a stationary wave model (SWM) forced with vorticity transients in the mid-latitude Atlantic (similar to 40 degrees N) or diabatic heat source over the subtropical Atlantic near the Caribbean Sea produces well-organized EA/WR-like wave patterns, respectively. Sensitivity tests with the SWM indicate enhancement of EA/WR-like blocking over west of Scandinavia when the mean state is modified to have a positive NAO component that enhances upper-level westerlies between 40 and 60 degrees N. C1 NASA, Goddard Space Flight Ctr, Goddard Earth Sci Technol & Res, IM Syst Grp,Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Lim, YK (reprint author), NASA, Goddard Space Flight Ctr, Goddard Earth Sci Technol & Res, IM Syst Grp,Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. EM Young-Kwon.Lim@nasa.gov NR 35 TC 9 Z9 9 U1 2 U2 16 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 EI 1432-0894 J9 CLIM DYNAM JI Clim. Dyn. PD JUN PY 2015 VL 44 IS 11-12 BP 3211 EP 3222 DI 10.1007/s00382-014-2381-4 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CI4GH UT WOS:000354705700019 ER PT J AU Wild, M Folini, D Hakuba, MZ Schar, C Seneviratne, SI Kato, S Rutan, D Ammann, C Wood, EF Konig-Langlo, G AF Wild, Martin Folini, Doris Hakuba, Maria Z. Schaer, Christoph Seneviratne, Sonia I. Kato, Seiji Rutan, David Ammann, Christof Wood, Eric F. Koenig-Langlo, Gert TI The energy balance over land and oceans: an assessment based on direct observations and CMIP5 climate models SO CLIMATE DYNAMICS LA English DT Article DE Global energy balance; Radiation budget; Global climate models; Surface and satellite observations; CMIP5 ID GENERAL-CIRCULATION MODELS; DOWNWARD LONGWAVE RADIATION; ANNUAL CYCLE; SATELLITE-OBSERVATIONS; OBSERVING SYSTEM; SURFACE; BUDGET; ATMOSPHERE; SHORTWAVE; TRANSPORTS AB The energy budgets over land and oceans are still afflicted with considerable uncertainties, despite their key importance for terrestrial and maritime climates. We evaluate these budgets as represented in 43 CMIP5 climate models with direct observations from both surface and space and identify substantial biases, particularly in the surface fluxes of downward solar and thermal radiation. These flux biases in the various models are then linearly related to their respective land and ocean means to infer best estimates for present day downward solar and thermal radiation over land and oceans. Over land, where most direct observations are available to constrain the surface fluxes, we obtain 184 and 306 Wm(-2) for solar and thermal downward radiation, respectively. Over oceans, with weaker observational constraints, corresponding estimates are around 185 and 356 Wm(-2). Considering additionallysurface albedo and emissivity, we infer a surface absorbed solar and net thermal radiation of 136 and -66 Wm(-2) over land, and 170 and -53 Wm(-2) over oceans, respectively. The surface net radiation is thus estimated at 70 Wm(-2) over land and 117 Wm(-2) over oceans, which may impose additional constraints on the poorly known sensible/latent heat flux magnitudes, estimated here near 32/38 Wm(-2) over land, and 16/100 Wm(-2) over oceans. Estimated uncertainties are on the order of 10 and 5 Wm(-2) for most surface and TOA fluxes, respectively. By combining these surface budgets with satellite-determined TOA budgets we quantify the atmospheric energy budgets as residuals (including ocean to land transports), and revisit the global mean energy balance. C1 [Wild, Martin; Folini, Doris; Hakuba, Maria Z.; Schaer, Christoph; Seneviratne, Sonia I.] Swiss Fed Inst Technol, Inst Atmospher & Climate Sci, CH-8092 Zurich, Switzerland. [Kato, Seiji; Rutan, David] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Ammann, Christof] Res Stn Agroscope, Climate & Air Pollut Grp, CH-8046 Zurich, Switzerland. [Wood, Eric F.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. [Koenig-Langlo, Gert] Alfred Wegener Inst, D-27570 Bremerhaven, Germany. RP Wild, M (reprint author), Swiss Fed Inst Technol, Inst Atmospher & Climate Sci, Univ Str 16, CH-8092 Zurich, Switzerland. EM martin.wild@env.ethz.ch RI Seneviratne, Sonia/G-8761-2011; Schar, Christoph/A-1033-2008; Wild, Martin/J-8977-2012; Konig-Langlo, Gert/K-5048-2012 OI Seneviratne, Sonia/0000-0001-9528-2917; Schar, Christoph/0000-0002-4171-1613; Konig-Langlo, Gert/0000-0002-6100-4107 FU Swiss National Science Foundation [135395]; National Centre for Competence in Climate Research (NCCR Climate) of the Swiss National Science Foundation as part of the NCCR Project HyClim; Office of Science, U.S. Department of Energy FX This study got support from the Swiss National Science Foundation Grant No. 135395 "Towards an improved understanding of the global energy balance: absorption of solar radiation" and from the National Centre for Competence in Climate Research (NCCR Climate) of the Swiss National Science Foundation as part of the NCCR Project HyClim. We highly appreciate the valuable review comments of Dr. Kevin Trenberth on this manuscript. We are grateful to Prof. Atsumu Ohmura for numerous discussions and for his leadership in the establishment of GEBA and BSRN. We would like to thank Dr. Guido Mueller for processing the BSRN data, Dr. Urs Beyerle and Prof. Reto Knutti for their efforts to download the immense CMIP5 dataset and Dr. Gabriela Schaepmann-Strub for advice on the albedo issues. We highly acknowledge Barbara Schar for the design of the global energy balance figures, and an anonymous reviewer for useful comments. We acknowledge the international modeling groups for providing their data for analysis, the Program for Climate Model Diagnosis and Intercomparison (PCMDI) for collecting and archiving the model data, the JSC/CLIVAR Working Group on Coupled Modeling (WGCM) and their Coupled Model Intercomparison Project (CMIP) and Climate Simulation Panel for organizing the model data analysis activity, and the IPCC WG1 TSU for technical support. The IPCC Data Archive at Lawrence Livermore National Laboratory is supported by the Office of Science, U.S. Department of Energy. NR 74 TC 33 Z9 33 U1 5 U2 45 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 EI 1432-0894 J9 CLIM DYNAM JI Clim. Dyn. PD JUN PY 2015 VL 44 IS 11-12 BP 3393 EP 3429 DI 10.1007/s00382-014-2430-z PG 37 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CI4GH UT WOS:000354705700029 ER PT J AU Obaza, A Hoffman, R Clausing, R AF Obaza, A. Hoffman, R. Clausing, R. TI Long-term stability of eelgrass fish assemblages in two highly developed coastal estuaries SO FISHERIES MANAGEMENT AND ECOLOGY LA English DT Article DE eelgrass; estuary; fish assemblage; stability; urbanisation ID SOUTHERN-CALIFORNIA; DIEL VARIATION; ENVIRONMENTAL-INFLUENCES; HABITAT UTILIZATION; COMMUNITY ECOLOGY; SHALLOW SEAGRASS; NURSERY FUNCTION; ZOSTERA-MARINA; PREDATION RISK; CLIMATE-CHANGE AB Changes in fish assemblages were tracked in representative eelgrass (Zostera marina L.) beds within two estuaries on the urbanised coast of southern California, USA, San Diego Bay and Mission Bay, from 1987 to 2010. Assemblages were sampled twice yearly (spring and summer) at day and night using beach seines. Assemblage stability was examined over time along with changes in assemblage structure across time of day and season, including the influence of temporally variable abiotic variables. Only the occasionally occurring fish, those present in <70% of samples, in Mission Bay appeared to be shifting to a new assemblage. Although season and sampling time significantly affected assemblages, correlations with abiotic factors were low. Given the long history of urban development of these estuaries, community shifts may have occurred prior to the onset of sampling, giving the appearance of stability. Alternatively, eelgrass habitat may be providing a refuge from long-term disturbances. C1 [Obaza, A.] Ocean Associates Inc, Arlington, VA USA. [Obaza, A.] Natl Marine Fisheries Serv, West Coast Reg Off, Long Beach, CA 90802 USA. [Hoffman, R.] Natl Marine Fisheries Serv, Southwest Reg Off, Long Beach, CA 90802 USA. [Clausing, R.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA USA. RP Obaza, A (reprint author), Natl Marine Fisheries Serv, West Coast Reg Off, 501 West Ocean Blvd,Suite 4200, Long Beach, CA 90802 USA. EM Adam.Obaza@noaa.gov NR 88 TC 2 Z9 2 U1 1 U2 30 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0969-997X EI 1365-2400 J9 FISHERIES MANAG ECOL JI Fisheries Manag. Ecol. PD JUN PY 2015 VL 22 IS 3 BP 224 EP 238 DI 10.1111/fme.12119 PG 15 WC Fisheries SC Fisheries GA CI1GR UT WOS:000354492100004 ER PT J AU Stevenazzi, S Masetti, M Nghiem, SV Sorichetta, A AF Stevenazzi, Stefania Masetti, Marco Nghiem, Son V. Sorichetta, Alessandro TI Groundwater vulnerability maps derived from a time-dependent method using satellite scatterometer data SO HYDROGEOLOGY JOURNAL LA English DT Article DE Vulnerability mapping; Urban areas; Remote sensing; Nitrate; Italy ID UNITED-STATES; AQUIFER SUSCEPTIBILITY; NITRATE CONTAMINATION; PROBABILITY; AUSTRALIA; AREAS; WATER; GIS AB Introducing the time variable in groundwater vulnerability assessment is an innovative approach to study the evolution of contamination by non-point sources and to forecast future trends. This requires a determination of the relationship between temporal changes in groundwater contamination and in land use. Such effort will enable breakthrough advances in mapping hazardous areas, and in assessing the efficacy of land-use planning for groundwater protection. Through a Bayesian spatial statistical approach, time-dependent vulnerability maps are derived by using hydrogeological variables together with three different time-dependent datasets: population density, high-resolution urban survey, and satellite QuikSCAT (QSCAT) data processed with the innovative dense sampling method (DSM). This approach is demonstrated extensively over the Po Plain in Lombardy region (northern Italy). Calibrated and validated maps show physically consistent relations between the hydrogeological variables and nitrate trends. The results indicate that changes of urban nitrate sources are strongly related to groundwater deterioration. Among the different datasets, QSCAT-DSM is proven to be the most efficient dataset to represent urban nitrate sources of contamination, with major advantages: a worldwide coverage, a continuous decadal data collection, and an adequate resolution without spatial gaps. This study presents a successful approach that, for the first time, allows the inclusion of the time dimension in groundwater vulnerability assessment by using innovative satellite remote sensing data for quantitative statistical analyses of groundwater quality changes. C1 [Stevenazzi, Stefania; Masetti, Marco] Univ Milan, Dipartimento Sci Terra A Desio, I-20133 Milan, Italy. [Nghiem, Son V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sorichetta, Alessandro] Univ Southampton, Geog & Environm, Southampton SO17 1BJ, Hants, England. 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; marco.masetti@unimi.it; son.v.nghiem@jpl.nasa.gov; A.Sorichetta@soton.ac.uk RI Masetti, Marco/N-6823-2013 FU National Aeronautics and Space Administration (NASA) Land-Cover and Land-Use Change (LCLUC) Program; Bill & Melinda Gates Foundation [OPP1106427, 1032350] FX The research carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology, was supported by the National Aeronautics and Space Administration (NASA) Land-Cover and Land-Use Change (LCLUC) Program. We thank Gregory Neumann of JPL for processing satellite QSCAT-DSM data. 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.uk) and supported by funding from the Bill & Melinda Gates Foundation (OPP1106427, 1032350). NR 51 TC 4 Z9 4 U1 2 U2 18 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1431-2174 EI 1435-0157 J9 HYDROGEOL J JI Hydrogeol. J. PD JUN PY 2015 VL 23 IS 4 BP 631 EP 647 DI 10.1007/s10040-015-1236-3 PG 17 WC Geosciences, Multidisciplinary; Water Resources SC Geology; Water Resources GA CI3AW UT WOS:000354620800003 ER PT J AU Petropoulos, GP Ireland, G Cass, A Srivastava, PK AF Petropoulos, George P. Ireland, Gareth Cass, Alexander Srivastava, Prashant K. TI Performance Assessment of the SEVIRI Evapotranspiration Operational Product: Results Over Diverse Mediterranean Ecosystems SO IEEE SENSORS JOURNAL LA English DT Article DE Evapotranspiration; Earth Observation; operational products; SEVIRI; validation; Europe ID LAND-SURFACE MODEL; ENERGY-BALANCE CLOSURE; EDDY-COVARIANCE; VEGETATION INDEX; SOIL-MOISTURE; VALIDATION; MODIS; SATELLITE; AFRICA; ALGORITHM AB Evapotranspiration (ET) is an important variable in weather systems and hydrometeorological modeling. In this paper, an extensive validation was carried out on the spinning enhanced visible and infrared imager (SEVIRI) ET operational product, evaluating its accuracy at selected European sites. Validation was performed through comparisons with in-situ eddy covariance measurements belonging to the CarboEurope IP network. Comparisons were performed for selected cloud-free days with a satisfactory energy balance ratio in 2011. A total of nine sites covering six land covers were used in validating the ET retrieval accuracy from the operational product. A series of statistical metrics was computed to evaluate the agreement, which also included explored the variability of site characteristics and influence of land cover on ET performances. Overall, a good agreement was reported between the satellite-derived ET estimates and the ground measurements (d-index = 0.755, root mean square deviation (RMSD) = 0.107 mm h(-1)). A minor negative bias of -0.015 mm h(-1) suggested only slight underestimation of the in-situ data. In terms of land cover, the highest agreement in ET was reported for the olive orchards and open shrubland sites (d-index = 0.893/0.867, RMSD = 0.041/0.050 mm h(-1)). A systematic ET underestimation by SEVIRI was found for all land cover types. Results of this study are largely in agreement to previous analogous validation studies of the product. Our findings support the potential value of the SEVIRI ET product for regional to mesoscale studies and practical applications. The latter is of particular importance for water limiting environments such as those found in the Mediterranean basin, as accurate information on ET rates can provide tremendous support in sustainable water resource management as well as policy and decision making. C1 [Petropoulos, George P.; Ireland, Gareth; Cass, Alexander] Aberystwyth Univ, Dept Geog & Earth Sci, Aberystwyth SY23 3FL, Dyfed, Wales. [Srivastava, Prashant K.] NASA, Goddard Space Flight Ctr, Hydrol Sci, Greenbelt, MD 20771 USA. [Srivastava, Prashant K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. RP Petropoulos, GP (reprint author), Aberystwyth Univ, Dept Geog & Earth Sci, Aberystwyth SY23 3FL, Dyfed, Wales. EM petropoulos.george@gmail.com; gai2@aber.ac.uk; alc32@aber.ac.uk; prashant.k.srivastava@nasa.gov RI Petropoulos, George/F-2384-2013 OI Petropoulos, George/0000-0003-1442-1423 FU European Commission Marie Curie Re-Integration Gran TRANSFORM-EO; High Performance Computing Facilities of Wales PREMIER-EO projects FX The work of G. Petropoulos's contribution was supported by the European Commission Marie Curie Re-Integration Gran TRANSFORM-EO and the High Performance Computing Facilities of Wales PREMIER-EO projects. The associate editor coordinating the review of this paper and approving it for publication was Prof. Octavian Postolache. (Corresponding author: George P. Petropoulos.) NR 41 TC 5 Z9 5 U1 2 U2 8 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 JUN PY 2015 VL 15 IS 6 BP 3412 EP 3423 DI 10.1109/JSEN.2015.2390031 PG 12 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Physics, Applied SC Engineering; Instruments & Instrumentation; Physics GA CI7OV UT WOS:000354954500010 ER PT J AU Stevenson, A Cray, JA Williams, JP Santos, R Sahay, R Neuenkirchen, N McClure, CD Grant, IR Houghton, JDR Quinn, JP Timson, DJ Patil, SV Singhal, RS Anton, J Dijksterhuis, J Hocking, AD Lievens, B Rangel, DEN Voytek, MA Gunde-Cimerman, N Oren, A Timmis, KN McGenity, TJ Hallsworth, JE AF Stevenson, Andrew Cray, Jonathan A. Williams, Jim P. Santos, Ricardo Sahay, Richa Neuenkirchen, Nils McClure, Colin D. Grant, Irene R. Houghton, Jonathan D. R. Quinn, John P. Timson, David J. Patil, Satish V. Singhal, Rekha S. Anton, Josefa Dijksterhuis, Jan Hocking, Ailsa D. Lievens, Bart Rangel, Drauzio E. N. Voytek, Mary A. Gunde-Cimerman, Nina Oren, Aharon Timmis, Kenneth N. McGenity, Terry J. Hallsworth, John E. TI Is there a common water-activity limit for the three domains of life? SO ISME JOURNAL LA English DT Article ID EXTREMELY HALOPHILIC BACTERIUM; SP-NOV.; GEN. NOV.; XEROPHILIC FUNGI; SALINIBACTER-RUBER; TETRAGENOCOCCUS-HALOPHILUS; ENTOMOPATHOGENIC FUNGI; TEMPERATURE RELATIONS; EMENDED DESCRIPTION; COMPATIBLE SOLUTES AB Archaea and Bacteria constitute a majority of life systems on Earth but have long been considered inferior to Eukarya in terms of solute tolerance. Whereas the most halophilic prokaryotes are known for an ability to multiply at saturated NaCl (water activity (a(w)) 0.755) some xerophilic fungi can germinate, usually at high-sugar concentrations, at values as low as 0.650-0.605 a(w). Here, we present evidence that halophilic prokayotes can grow down to water activities of <0.755 for Halanaerobium lacusrosei (0.748), Halobacterium strain 004.1 (0.728), Halobacterium sp. NRC-1 and Halococcus morrhuae (0.717), Haloquadratum walsbyi (0.709), Halococcus salifodinae (0.693), Halobacterium noricense (0.687), Natrinema pallidum (0.681) and haloarchaeal strains GN-2 and GN-5 (0.635 a(w)). Furthermore, extrapolation of growth curves (prone to giving conservative estimates) indicated theoretical minima down to 0.611 a(w) for extreme, obligately halophilic Archaea and Bacteria. These were compared with minima for the most solute-tolerant Bacteria in high-sugar (or other non-saline) media (Mycobacterium spp., Tetragenococcus halophilus, Saccharibacter floricola, Staphylococcus aureus and so on) and eukaryotic microbes in saline (Wallemia spp., Basipetospora halophila, Dunaliella spp. and so on) and high-sugar substrates (for example, Xeromyces bisporus, Zygosaccharomyces rouxii, Aspergillus and Eurotium spp.). We also manipulated the balance of chaotropic and kosmotropic stressors for the extreme, xerophilic fungi Aspergillus penicilloides and X. bisporus and, via this approach, their established water-activity limits for mycelial growth (similar to 0.65) were reduced to 0.640. Furthermore, extrapolations indicated theoretical limits of 0.632 and 0.636 aw for A. penicilloides and X. bisporus, respectively. Collectively, these findings suggest that there is a common water-activity limit that is determined by physicochemical constraints for the three domains of life. C1 [Stevenson, Andrew; Cray, Jonathan A.; Williams, Jim P.; Santos, Ricardo; McClure, Colin D.; Grant, Irene R.; Houghton, Jonathan D. R.; Quinn, John P.; Timson, David J.; Hallsworth, John E.] Queens Univ Belfast, Sch Biol Sci, MBC, Inst Global Food Secur, Belfast BT9 7BL, Antrim, North Ireland. [Santos, Ricardo] Inst Super Tecn, Lab Anal, Lisbon, Portugal. [Sahay, Richa; Neuenkirchen, Nils; Timmis, Kenneth N.; McGenity, Terry J.; Hallsworth, John E.] Univ Essex, Sch Biol Sci, Colchester CO4 3SQ, Essex, England. [Patil, Satish V.] North Maharashtra Univ, Sch Life Sci, Jalgaon, Maharashtra, India. [Singhal, Rekha S.] Inst Chem Technol, Dept Food Engn & Technol, Mumbai, Maharashtra, India. [Anton, Josefa] Univ Alicante, Dept Physiol Genet & Microbiol, E-03080 Alicante, Spain. [Dijksterhuis, Jan] CBS Fungal Biodivers Ctr, Utrecht, Netherlands. [Hocking, Ailsa D.] CSIRO Food & Nutr, N Ryde, NSW, Australia. [Lievens, Bart] Scientia Terrae Res Inst, Microbial Ecol & Biorat Control, St Katelijne Waver, Belgium. [Rangel, Drauzio E. N.] Univ Vale Paraiba, Inst Pesquisa Desenvolvimento, Sao Jose dos Campos, SP, Brazil. [Voytek, Mary A.] NASA Headquarters, Washington, DC USA. [Gunde-Cimerman, Nina] Univ Ljubljana, Biotech Fac, Ljubljana, Slovenia. [Oren, Aharon] Hebrew Univ Jerusalem, Alexander Silberman Inst Life Sci, Dept Plant & Environm Sci, Jerusalem, Israel. [Timmis, Kenneth N.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Microbiol, D-38106 Braunschweig, Germany. RP Hallsworth, JE (reprint author), Queens Univ Belfast, Sch Biol Sci, 97 Lisburn Rd, Belfast BT9 7BL, Antrim, North Ireland. EM j.hallsworth@qub.ac.uk RI Rangel, Drauzio/C-2711-2012; Hallsworth, John/K-7876-2013; OI Rangel, Drauzio/0000-0001-7188-100X; McGenity, Terence/0000-0002-1497-8822; Timson, David/0000-0002-0985-8818 FU Research (Northern Ireland); Enterprise Directorate of Queen's University Belfast; Department of Agriculture and Rural Development (Northern Ireland); Department for Employment and Learning (Northern Ireland); Biotechnology and Biological Sciences Research Council (BBSRC, UK) [BBF/003471/1, BBF/00351X/1]; Beaufort Marine Research Award for Marine Biodiscovery; Marine Institute, Ireland; State of Sao Paulo Research Foundation (FAPESP) [2010/06374-1] FX We are grateful to Peter N Golyshin and Olga V Golyshina (Bangor University, UK), Barbara J Javor (Southwest Fisheries Science Center, USA) and Tom L Kieft (New Mexico Tech., USA) for fruitful discussions, and to Helga Stan-Lotter (University of Salzburg, Austria) for providing Halobacterium sp. NRC-1. Funding was received from the Research (Northern Ireland) and Enterprise Directorate of Queen's University Belfast; Department of Agriculture and Rural Development and the Department for Employment and Learning (Northern Ireland); Biotechnology and Biological Sciences Research Council (BBSRC, UK) Projects BBF/003471/1 and BBF/00351X/1; and the Beaufort Marine Research Award for Marine Biodiscovery that is carried out under the Sea Change Strategy and the Strategy for Science Technology and Innovation (2006-2013), with the support of the Marine Institute, Ireland. This work was also supported by the State of Sao Paulo Research Foundation (FAPESP) via a grant awarded to Drauzio EN Rangel (#2010/06374-1). NR 147 TC 33 Z9 33 U1 11 U2 64 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1751-7362 EI 1751-7370 J9 ISME J JI ISME J. PD JUN PY 2015 VL 9 IS 6 BP 1333 EP 1351 DI 10.1038/ismej.2014.219 PG 19 WC Ecology; Microbiology SC Environmental Sciences & Ecology; Microbiology GA CI5HR UT WOS:000354786700006 PM 25500507 ER PT J AU Lievens, H Al Bitar, A Verhoest, NEC Cabot, F De Lannoy, GJM Drusch, M Dumedah, G Franssen, HJH Kerr, Y Tomer, SK Martens, B Merlin, O Pan, M van den Berg, MJ Vereecken, H Walker, JP Wood, EF Pauwels, VRN AF Lievens, H. Al Bitar, A. Verhoest, N. E. C. Cabot, F. De Lannoy, G. J. M. Drusch, M. Dumedah, G. Franssen, H-J. Hendricks Kerr, Y. Tomer, S. K. Martens, B. Merlin, O. Pan, M. van den Berg, M. J. Vereecken, H. Walker, J. P. Wood, E. F. Pauwels, V. R. N. TI Optimization of a Radiative Transfer Forward Operator for Simulating SMOS Brightness Temperatures over the Upper Mississippi Basin SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID SURFACE SOIL-MOISTURE; ASSIMILATION SYSTEM NLDAS; INTEGRATED FORECAST SYSTEM; BAND MICROWAVE EMISSION; TRANSFER MODEL; DISCHARGE PREDICTIONS; RETRIEVAL ALGORITHM; GLOBAL SIMULATION; UNITED-STATES; LAND AB The Soil Moisture Ocean Salinity (SMOS) satellite mission routinely provides global multiangular observations of brightness temperature TB at both horizontal and vertical polarization with a 3-day repeat period. The assimilation of such data into a land surface model (LSM) may improve the skill of operational flood forecasts through an improved estimation of soil moisture SM. To accommodate for the direct assimilation of the SMOS TB data, the LSM needs to be coupled with a radiative transfer model (RTM), serving as a forward operator for the simulation of multiangular and multipolarization top of the atmosphere TBs. This study investigates the use of the Variable Infiltration Capacity model coupled with the Community Microwave Emission Modelling Platform for simulating SMOS TB observations over the upper Mississippi basin, United States. For a period of 2 years (2010-11), a comparison between SMOS TBs and simulations with literature-based RTM parameters reveals a basin-averaged bias of 30 K. Therefore, time series of SMOS TB observations are used to investigate ways for mitigating these large biases. Specifically, the study demonstrates the impact of the LSM soil moisture climatology in the magnitude of TB biases. After cumulative distribution function matching the SM climatology of the LSM to SMOS retrievals, the average bias decreases from 30 K to less than 5 K. Further improvements can be made through calibration of RTM parameters related to the modeling of surface roughness and vegetation. Consequently, it can be concluded that SM rescaling and RTM optimization are efficient means for mitigating biases and form a necessary preparatory step for data assimilation. C1 [Lievens, H.; Verhoest, N. E. C.; Martens, B.; van den Berg, M. J.] Univ Ghent, Lab Hydrol & Water Management, B-9000 Ghent, Belgium. [Al Bitar, A.; Cabot, F.; Kerr, Y.; Tomer, S. K.; Merlin, O.] Ctr Etud Spatiales Biosphere, Toulouse, France. [De Lannoy, G. J. M.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Drusch, M.] European Space Agcy, NL-2200 AG Noordwijk, Netherlands. [Dumedah, G.; Walker, J. P.; Pauwels, V. R. N.] Monash Univ, Dept Civil Engn, Clayton, Vic 3168, Australia. [Franssen, H-J. Hendricks; Vereecken, H.] Forschungszentrum Julich, D-52425 Julich, Germany. [Pan, M.; Wood, E. F.] Princeton Univ, Land Surface Hydrol Grp, Princeton, NJ 08544 USA. RP Lievens, H (reprint author), Univ Ghent, Lab Hydrol & Water Management, Coupure Links 653, B-9000 Ghent, Belgium. EM hans.lievens@ugent.be RI Verhoest, Niko/C-9726-2010; Pan, Ming/B-6841-2011; OI Verhoest, Niko/0000-0003-4116-8881; Pan, Ming/0000-0003-3350-8719; Hendricks-Franssen, Harrie-Jan/0000-0002-0004-8114; Pauwels, Valentijn/0000-0002-1290-9313; Martens, Brecht/0000-0002-7368-7953; Al Bitar, Ahmad/0000-0002-1756-1096 FU Belgian Science Policy (BELSPO) [SR/00/302]; CNES Terre, Ocean, Surfaces continentales, Atmosphere (TOSCA) program; Australian Research Council FX The work has been performed in the framework of the ESA-STSE project "SMOS + Hydrology Study" and was partly funded through project SR/00/302 (Hydras+) financed by the Belgian Science Policy (BELSPO), and the CNES Terre, Ocean, Surfaces continentales, Atmosphere (TOSCA) program. Furthermore, we would like to acknowledge the Julich Supercomputing Center for granting computation time on JUROPA. Hans Lievens is a postdoctoral research fellow of the Research Foundation Flanders (FWO). Valentijn Pauwels is currently a Future Fellow funded by the Australian Research Council. NR 74 TC 8 Z9 8 U1 4 U2 14 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 JUN PY 2015 VL 16 IS 3 BP 1109 EP 1134 DI 10.1175/JHM-D-14-0052.1 PG 26 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CI9YI UT WOS:000355126500010 ER PT J AU Lawston, PM Santanello, JA Zaitchik, BF Rodell, M AF Lawston, Patricia M. Santanello, Joseph A., Jr. Zaitchik, Benjamin F. Rodell, Matthew TI Impact of Irrigation Methods on Land Surface Model Spinup and Initialization of WRF Forecasts SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID SOUTHERN GREAT-PLAINS; ATMOSPHERIC RESPONSE; UNITED-STATES; WATER; PRECIPITATION; FLUXES; TEMPERATURE; CLIMATE; AGRICULTURE; FRAMEWORK AB In the United States, irrigation represents the largest consumptive use of freshwater and accounts for approximately one-third of total water usage. Irrigation impacts soil moisture and can ultimately influence clouds and precipitation through land-planetary boundary layer (PBL) coupling processes. This study utilizes NASA's Land Information System (LIS) and the NASA Unified Weather Research and Forecasting Model (NU-WRF) framework to investigate the effects of drip, flood, and sprinkler irrigation methods on land-atmosphere interactions, including land-PBL coupling and feedbacks at the local scale. To initialize 2-day, 1-km WRF forecasts over the central Great Plains in a drier-than-normal (2006) and a wetter-than-normal year (2008), 5-yr irrigated LIS spinups were used. The offline and coupled simulation results show that regional irrigation impacts are sensitive to time, space, and method and that irrigation cools and moistens the surface over and downwind of irrigated areas, ultimately resulting in both positive and negative feedbacks on the PBL depending on the time of day and background climate conditions. Furthermore, the results portray the importance of both irrigation method physics and correct representation of several key components of land surface models, including accurate and timely land-cover and crop-type classification, phenology (greenness), and soil moisture anomalies (through a land surface model spinup) in coupled prediction models. C1 [Lawston, Patricia M.] Univ Delaware, Dept Geog, Newark, DE 19716 USA. [Lawston, Patricia M.; Santanello, Joseph A., Jr.; Rodell, Matthew] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Zaitchik, Benjamin F.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. RP Lawston, PM (reprint author), Univ Delaware, Dept Geog, 216 Pearson Hall, Newark, DE 19716 USA. EM pmlawsto@udel.edu RI Rodell, Matthew/E-4946-2012; Santanello, Joseph/D-4438-2012 OI Rodell, Matthew/0000-0003-0106-7437; Santanello, Joseph/0000-0002-0807-6590 FU NASA Energy and Water Cycle Study (NEWS); LIS-WRF and LVT FX Much of this work was conducted as part of the NASA GSFC Intern Program and supported by the NASA Energy and Water Cycle Study (NEWS). Many thanks to the LIS team, especially Sujay Kumar, for providing feedback and support with LIS-WRF and LVT, and to Hiroko Beaudoing, Kristi Arsenault, and Eric Hunt for sharing their knowledge of irrigation and land-cover datasets. The MET analysis included data from the Research Data Archive (RDA; available via http://rda.ucar.edu/datasets/ds337.0), which is maintained by the Computational and Information Systems Laboratory (CISL) at the National Center for Atmospheric Research (NCAR). NR 57 TC 7 Z9 7 U1 0 U2 14 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 JUN PY 2015 VL 16 IS 3 BP 1135 EP 1154 DI 10.1175/JHM-D-14-0203.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CI9YI UT WOS:000355126500011 ER PT J AU Demir, I Conover, H Krajewski, WF Seo, BC Goska, R He, YB McEniry, MF Graves, SJ Petersen, W AF Demir, Ibrahim Conover, Helen Krajewski, Witold F. Seo, Bong-Chul Goska, Radoslaw He, Yubin McEniry, Michael F. Graves, Sara J. Petersen, Walter TI Data-Enabled Field Experiment Planning, Management, and Research Using Cyberinfrastructure SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID RADAR-RAINFALL; BEAM BLOCKAGE; UNIDATA; ACCESS; FLOOD; GIS AB In the spring of 2013, NASA conducted a field campaign known as Iowa Flood Studies (IFloodS) as part of the Ground Validation (GV) program for the Global Precipitation Measurement (GPM) mission. The purpose of IFloodS was to enhance the understanding of flood-related, space-based observations of precipitation processes in events that transpire worldwide. NASA used a number of scientific instruments such as ground-based weather radars, rain and soil moisture gauges, stream gauges, and disdrometers to monitor rainfall events in Iowa. This article presents the cyberinfrastructure tools and systems that supported the planning, reporting, and management of the field campaign and that allow these data and models to be accessed, evaluated, and shared for research. The authors describe the collaborative informatics tools, which are suitable for the network design, that were used to select the locations in which to place the instruments. How the authors used information technology tools for instrument monitoring, data acquisition, and visualizations after deploying the instruments and how they used a different set of tools to support data analysis and modeling after the campaign are also explained. All data collected during the campaign are available through the Global Hydrology Resource Center (GHRC), a NASA Distributed Active Archive Center (DAAC). C1 [Demir, Ibrahim; Krajewski, Witold F.; Seo, Bong-Chul; Goska, Radoslaw] Univ Iowa, IIHR Hydrosci & Engn, Iowa City, IA USA. [Conover, Helen; He, Yubin; McEniry, Michael F.; Graves, Sara J.] Univ Alabama, Informat Technol & Syst Ctr, Huntsville, AL 35899 USA. [Petersen, Walter] NASA, Goddard Space Flight Ctr, Off Field Support, Wallops Isl, VA 23337 USA. RP Demir, I (reprint author), IIHR Hydrosci & Engn, Iowa Flood Ctr, 207 C Maxwell Stanley Hydraul Lab, Iowa City, IA 52242 USA. EM ibrahim-demir@uiowa.edu RI Measurement, Global/C-4698-2015 FU NASA's Cooperative Agreement [NNM11AA01A, NNX13AD83G, NNX13AG94G]; Iowa Flood Center; National Science Foundation [1327830]; NASA GPM program; Precipitation Measurement Mission program FX Funding for this work was provided by NASA's Cooperative Agreement NNM11AA01A and Grants NNX13AD83G and NNX13AG94G, the Iowa Flood Center, and the National Science Foundation Award 1327830. We also gratefully acknowledge funding and management support from the NASA GPM and Precipitation Measurement Mission programs. NR 27 TC 4 Z9 4 U1 0 U2 5 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 JUN PY 2015 VL 16 IS 3 BP 1155 EP 1170 DI 10.1175/JHM-D-14-0163.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CI9YI UT WOS:000355126500012 ER PT J AU Bringi, VN Tolstoy, L Thurai, M Petersen, WA AF Bringi, V. N. Tolstoy, L. Thurai, M. Petersen, W. A. TI Estimation of Spatial Correlation of Drop Size Distribution Parameters and Rain Rate Using NASA's S-Band Polarimetric Radar and 2D Video Disdrometer Network: Two Case Studies from MC3E SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID SMALL-SCALE RAINFALL; DIFFERENT CLIMATIC REGIMES; DUAL-POLARIZED RADAR; PRECIPITATION RADAR; VARIABILITY; VALIDATION; PROFILER; EVENTS; HAIL AB Polarimetric radar data obtained at high spatial and temporal resolutions offer a distinct advantage in estimating the spatial correlation function of drop size distribution (DSD) parameters and rain rate compared with a fixed gauge-disdrometer network. On two days during the 2011 Midlatitude Continental Convective Clouds Experiment (MC3E) campaign in Oklahoma, NASA's S-band polarimetric radar (NPOL) performed repeated PPI scans every 40 s over six 2D video disdrometer (2DVD) sites, located 20-30 km from the radar. The two cases were 1) a rapidly evolving multicell rain event (with large drops) and 2) a long-duration stratiform rain event. From the time series at each polar pixel, the Pearson correlation coefficient is computed as a function of distance along each radial in the PPI scan. Azimuthal dependence is found, especially for the highly convective event. A pseudo-1D spatial correlation is computed that is fitted to a modified-exponential function with two parameters (decorrelation distance R-0 and shape F). The first event showed significantly higher spatial variability in rain rate (shorter decorrelation distance R-0 = 3.4 km) compared with the second event with R-0 = 10.2 km. Further, for the second event, the spatial correlation of the DSD parameters and rain rate from radar showed good agreement with 2DVD-based spatial correlations over distances ranging from 1.5 to 7 km. The NPOL also performed repeated RHI scans every 40 s along one azimuth centered over the 2DVD network. Vertical correlations of the DSD parameters as well as the rainwater content were determined below the melting level, with the first event showing more variability compared with the second event. C1 [Bringi, V. N.; Tolstoy, L.; Thurai, M.] Colorado State Univ, Dept Elect & Comp Engn, Ft Collins, CO 80523 USA. [Petersen, W. A.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. RP Bringi, VN (reprint author), Colorado State Univ, Dept Elect & Comp Engn, Campus Mail 1373, Ft Collins, CO 80523 USA. EM bringi@engr.colostate.edu RI Measurement, Global/C-4698-2015 FU NASA GPM program offices FX We thank the NPOL scientists and technicians as well as the disdrometer field technicians during MC3E for collecting the data used in this study. We would also like to thank Dr. R. Kakar of the NASA Precipitation Measurement Mission and Dr. A. Hou and Dr. M. Schwaller of the NASA GPM program offices for providing funding for this study. The S-band profiler data shown in Figs. 2b and 2d were provided by Dr. C. R. Williams. NR 39 TC 6 Z9 6 U1 0 U2 4 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 JUN PY 2015 VL 16 IS 3 BP 1207 EP 1221 DI 10.1175/JHM-D-14-0204.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CI9YI UT WOS:000355126500015 ER PT J AU Best, MJ Abramowitz, G Johnson, HR Pitman, AJ Balsamo, G Boone, A Cuntz, M Decharme, B Dirmeyer, PA Dong, J Ek, M Guo, Z Haverd, V Van den Hurk, BJJ Nearing, GS Pak, B Peters-Lidard, C Santanello, JA Stevens, L Vuichard, N AF Best, M. J. Abramowitz, G. Johnson, H. R. Pitman, A. J. Balsamo, G. Boone, A. Cuntz, M. Decharme, B. Dirmeyer, P. A. Dong, J. Ek, M. Guo, Z. Haverd, V. Van den Hurk, B. J. J. Nearing, G. S. Pak, B. Peters-Lidard, C. Santanello, J. A., Jr. Stevens, L. Vuichard, N. TI The Plumbing of Land Surface Models: Benchmarking Model Performance SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID ATMOSPHERE COUPLING EXPERIMENT; SOIL WETNESS PROJECT; PARAMETERIZATION SCHEMES; CLIMATE MODELS; PHASE; HYDROLOGY; MOISTURE; SYSTEM; IMPACT; ENERGY AB The Protocol for the Analysis of Land Surface Models (PALS) Land Surface Model Benchmarking Evaluation Project (PLUMBER) was designed to be a land surface model (LSM) benchmarking intercomparison. Unlike the traditional methods of LSM evaluation or comparison, benchmarking uses a fundamentally different approach in that it sets expectations of performance in a range of metrics a priori-before model simulations are performed. This can lead to very different conclusions about LSM performance. For this study, both simple physically based models and empirical relationships were used as the benchmarks. Simulations were performed with 13 LSMs using atmospheric forcing for 20 sites, and then model performance relative to these benchmarks was examined. Results show that even for commonly used statistical metrics, the LSMs' performance varies considerably when compared to the different benchmarks. All models outperform the simple physically based benchmarks, but for sensible heat flux the LSMs are themselves outperformed by an out-of-sample linear regression against downward shortwave radiation. While moisture information is clearly central to latent heat flux prediction, the LSMs are still outperformed by a three-variable nonlinear regression that uses instantaneous atmospheric humidity and temperature in addition to downward shortwave radiation. These results highlight the limitations of the prevailing paradigm of LSM evaluation that simply compares an LSM to observations and to other LSMs without a mechanism to objectively quantify the expectations of performance. The authors conclude that their results challenge the conceptual view of energy partitioning at the land surface. C1 [Best, M. J.; Johnson, H. R.] Met Off, Exeter EX1 3PB, Devon, England. [Abramowitz, G.; Pitman, A. J.] Univ New S Wales, ARC Ctr Excellence Climate Syst Sci, Sydney, NSW, Australia. [Balsamo, G.] ECMWF, Reading, Berks, England. [Boone, A.; Decharme, B.] Meteo France, CNRM GAME, Toulouse, France. [Cuntz, M.] UFZ Helmholtz Ctr Environm Res, Leipzig, Germany. [Dirmeyer, P. A.; Guo, Z.] George Mason Univ, Ctr Ocean Land Atmosphere Studies, Fairfax, VA 22030 USA. [Dong, J.; Ek, M.] NOAA, NCEP, EMC, College Pk, MD USA. [Haverd, V.] CSIRO, Oceans & Atmosphere Flagship, Canberra, ACT, Australia. [Van den Hurk, B. J. J.] KNMI, De Bilt, Netherlands. [Nearing, G. S.; Peters-Lidard, C.; Santanello, J. A., Jr.] NASA GSFC, Hydrol Sci Lab, Greenbelt, MD USA. [Pak, B.; Stevens, L.] CSIRO, Oceans & Atmosphere Flagship, Aspendale, Vic, Australia. [Vuichard, N.] CEA CNRS UVSQ, IPSL LSCE, UMR 8212, Lab Sci Climat & Environm, Gif Sur Yvette, France. RP Best, MJ (reprint author), Met Off, Fitzroy Rd, Exeter EX1 3PB, Devon, England. EM martin.best@metoffice.gov.uk RI Pitman, Andrew/A-7353-2011; haverd, vanessa/G-8683-2011; Santanello, Joseph/D-4438-2012; Dirmeyer, Paul/B-6553-2016; Vuichard, Nicolas/A-6629-2011; Peters-Lidard, Christa/E-1429-2012; Stevens, Lauren/I-4183-2016; OI Pitman, Andrew/0000-0003-0604-3274; Santanello, Joseph/0000-0002-0807-6590; Dirmeyer, Paul/0000-0003-3158-1752; Peters-Lidard, Christa/0000-0003-1255-2876; Best, Martin/0000-0003-4468-876X FU Joint DECC/Defra Met Office Hadley Centre Climate Programme [CA01101]; Australian Research Council Centre of Excellence for Climate System Science [CE110001028]; U.S. Department of Energy, Biological and Environmental Research, Terrestrial Carbon Program [DE-FG02-04ER63917, DE-FG02-04ER63911]; CFCAS; NSERC; BIOCAP; Environment Canada; NRCan; CarboEuropeIP; FAO-GTOS-TCO; iLEAPS; Max Planck Institute for Biogeochemistry; National Science Foundation; Tuscia University; Universite Laval and Environment Canada; U.S. Department of Energy FX M. Best and H. Johnson were supported by the Joint DECC/Defra Met Office Hadley Centre Climate Programme (CA01101). We acknowledge the support of the Australian Research Council Centre of Excellence for Climate System Science (CE110001028). This work used eddy covariance data acquired by the FLUXNET community and in particular by the following networks: AmeriFlux [U.S. Department of Energy, Biological and Environmental Research, Terrestrial Carbon Program (DE-FG02-04ER63917 and DE-FG02-04ER63911)], AfriFlux, AsiaFlux, CarboAfrica, CarboEuropeIP, CarboItaly, CarboMont, ChinaFlux, FLUXNET-Canada (supported by CFCAS, NSERC, BIOCAP, Environment Canada, and NRCan), GreenGrass, KoFlux, LBA, NECC, OzFlux, TCOS-Siberia, and USCCC. We acknowledge the financial support to the eddy covariance data harmonization provided by CarboEuropeIP, FAO-GTOS-TCO, iLEAPS, Max Planck Institute for Biogeochemistry, the National Science Foundation, Tuscia University, Universite Laval and Environment Canada, and the U.S. Department of Energy and the database development and technical support from Berkeley Water Center; Lawrence Berkeley National Laboratory; Microsoft Research eScience; Oak Ridge National Laboratory; University of California, Berkeley; and University of Virginia. NR 52 TC 27 Z9 27 U1 5 U2 35 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 JUN PY 2015 VL 16 IS 3 BP 1425 EP 1442 DI 10.1175/JHM-D-14-0158.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CI9YI UT WOS:000355126500028 ER PT J AU Owusu-Danquah, JS Saleeb, AF Dhakal, B Padula, SA AF Owusu-Danquah, J. S. Saleeb, A. F. Dhakal, B. Padula, S. A., II TI A Comparative Study of Ni49.9Ti50.1 and Ni50.3Ti29.7Hf20 Tube Actuators (vol 24, pg 1726, 2015) SO JOURNAL OF MATERIALS ENGINEERING AND PERFORMANCE LA English DT Correction C1 [Owusu-Danquah, J. S.; Saleeb, A. F.; Dhakal, B.] Univ Akron, Dept Civil Engn, Akron, OH 44325 USA. [Padula, S. A., II] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Saleeb, AF (reprint author), Univ Akron, Dept Civil Engn, 302 Buchtel Common, Akron, OH 44325 USA. EM saleeb@uakron.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1059-9495 EI 1544-1024 J9 J MATER ENG PERFORM JI J. Mater. Eng. Perform. PD JUN PY 2015 VL 24 IS 6 SI SI BP 2577 EP 2577 DI 10.1007/s11665-015-1500-7 PG 1 WC Materials Science, Multidisciplinary SC Materials Science GA CI6SF UT WOS:000354890800050 ER PT J AU Mader, TH Gibson, CR Lee, AG Patel, NB Hart, SF Pettit, DR AF Mader, Thomas H. Gibson, C. Robert Lee, Andrew G. Patel, Nimesh B. Hart, Steven F. Pettit, Donald R. TI Unilateral Loss of Spontaneous Venous Pulsations in an Astronaut SO JOURNAL OF NEURO-OPHTHALMOLOGY LA English DT Letter ID DURATION SPACE-FLIGHT; OPTIC DISC EDEMA C1 [Mader, Thomas H.] US Army, Cooper Landing, AK 99572 USA. [Gibson, C. Robert] Coastal Eye Associates, Webster, TX USA. [Lee, Andrew G.] Methodist Hosp, Dept Ophthalmol, Houston, TX 77030 USA. [Patel, Nimesh B.] Univ Houston, Univ Eye Inst, Houston, TX USA. [Hart, Steven F.] NASA, Johnson Space Ctr, Space Med, Houston, TX USA. [Pettit, Donald R.] NASA, Johnson Space Ctr, Houston, TX USA. RP Mader, TH (reprint author), US Army, Cooper Landing, AK 99572 USA. NR 5 TC 3 Z9 3 U1 0 U2 0 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA TWO COMMERCE SQ, 2001 MARKET ST, PHILADELPHIA, PA 19103 USA SN 1070-8022 EI 1536-5166 J9 J NEURO-OPHTHALMOL JI J. Neuro-Ophthal. PD JUN PY 2015 VL 35 IS 2 BP 226 EP 227 PG 2 WC Clinical Neurology; Ophthalmology SC Neurosciences & Neurology; Ophthalmology GA CI7ZO UT WOS:000354986600029 PM 25756457 ER PT J AU Jiang, B Woodell, GA Jobson, DJ AF Jiang, Bo Woodell, Glenn A. Jobson, Daniel J. TI Novel multi-scale retinex with color restoration on graphics processing unit SO JOURNAL OF REAL-TIME IMAGE PROCESSING LA English DT Article DE Multi-scale Retinex; Image enhancement; Autolevels; Real time; GPU ID IMAGE-ENHANCEMENT; VISION; GPU AB The multi-scale retinex with color restoration (MSRCR) was developed as a general-purpose image enhancement algorithm that provides simultaneous dynamic range compression, local lightness/contrast enhancement, and good color rendition, and has been successfully used for a wide variety of imagery from diverse fields. While the MSRCR performs good enhancement in most images, the output image can sometimes be further visually optimized during our experiments. An improved MSRCR+Autolevels (AL) algorithm is presented, which can eliminate the impact of a small number of outliers in the histogram of the image and further improve the contrast of an image. New extension significantly improves the visual performance of the MSRCR algorithm. However, the MSRCR+AL containing a large number of complex calculations is computationally expensive, limiting real-time applications. In this paper, a parallel application of the MSRCR+AL algorithm on a graphics processing unit (GPU) is presented. For the various configurations in our test, the GPU-accelerated MSRCR+AL shows a scalable speedup as the resolution of an image increases. The up to 45x speedup (1,024 x 1,024) over the single-threaded CPU counterpart shows a promising direction of using the GPU-based MSRCR+AL in large-scale, time-critical applications. We also achieved 17 frames per second in video processing (1,280 x 720). C1 [Jiang, Bo] NIA, Hampton, VA 23666 USA. [Woodell, Glenn A.; Jobson, Daniel J.] NASA, Langley Res Ctr, Electromagnet & Sensors Branch, Hampton, VA 23665 USA. RP Jiang, B (reprint author), NIA, 100 Explorat Way, Hampton, VA 23666 USA. EM bjiang07@gmail.com FU NASA [NNL09AA00A] FX The authors wish to thank the NASA Aviation Safety Program, External Hazards Sensing and Mitigation for the funding which made this work possible. In particular, Dr. Jiang was funded by NASA Grant#NNL09AA00A to the National Institute of Aerospace. NR 37 TC 2 Z9 3 U1 2 U2 20 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1861-8200 EI 1861-8219 J9 J REAL-TIME IMAGE PR JI J. Real-Time Image Process. PD JUN PY 2015 VL 10 IS 2 SI SI BP 239 EP 253 DI 10.1007/s11554-014-0399-9 PG 15 WC Computer Science, Artificial Intelligence; Engineering, Electrical & Electronic; Imaging Science & Photographic Technology SC Computer Science; Engineering; Imaging Science & Photographic Technology GA CI4JU UT WOS:000354715300005 ER PT J AU Jiang, X Olsen, ET Pagano, TS Su, H Yung, YL AF Jiang, Xun Olsen, Edward T. Pagano, Thomas S. Su, Hui Yung, Yuk L. TI Modulation of Midtropospheric CO2 by the South Atlantic Walker Circulation* SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID ATMOSPHERIC CARBON-DIOXIDE; MAUNA-LOA; EL-NINO; OSCILLATION; VARIABILITY; CLIMATE; REANALYSIS; MISSION; MODEL; CYCLE AB Midtropospheric CO2 data from the Atmospheric Infrared Sounder (AIRS) are used in this study to explore the variability of CO2 over the South Atlantic Ocean. It was found that the area-averaged CO2 over the South Atlantic Ocean is less than that over South America by about 1 ppm during December-March. This CO2 contrast is due to the large-scale vertical circulation over this region. During December-March, there is sinking motion over the South Atlantic Ocean. The sinking motion brings high-altitude air with a slightly lower concentration of CO2 to the midtroposphere. Meanwhile, air rising over South America brings near-surface air with a higher concentration of CO2 to the midtroposphere. As a result, the AIRS midtropospheric CO2 concentration is lower over the South Atlantic Ocean than over South America during December-March. The detrended AIRS midtropospheric CO2 difference correlates well with the inverted and detrended 400-hPa vertical pressure velocity difference between the South Atlantic and South America. Results obtained from this study demonstrate the strong impact of large-scale circulation on the vertical distribution of CO2 in the free troposphere and suggest that midtropospheric CO2 measurements can be used as an innovative observational constraint on the simulation of large-scale circulations in climate models. C1 [Jiang, Xun] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77004 USA. [Olsen, Edward T.; Pagano, Thomas S.; Su, Hui] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA USA. [Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Jiang, X (reprint author), Univ Houston, Dept Earth & Atmospher Sci, 4800 Calhoun Rd, Houston, TX 77004 USA. EM xjiang7@uh.edu FU AIRS project; OCO-2 project; NASA [NNX13AC04G]; Caltech; National Aeronautics and Space Administration FX We thank two anonymous reviewers for helpful comments. XJ and YLY were supported by the AIRS project, OCO-2 project, and NASA Grant NNX13AC04G to UH and Caltech. 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 39 TC 1 Z9 1 U1 0 U2 9 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 EI 1520-0469 J9 J ATMOS SCI JI J. Atmos. Sci. PD JUN PY 2015 VL 72 IS 6 BP 2241 EP 2247 DI 10.1175/JAS-D-14-0340.1 PG 7 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CI9RW UT WOS:000355108500003 ER PT J AU Chao, WC AF Chao, Winston C. TI Correction of Excessive Precipitation over Steep and High Mountains in a GCM: A Simple Method of Parameterizing the Thermal Effects of Subgrid Topographic Variation SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID MODEL AB The excessive precipitation over steep and high mountains (EPSM) in GCMs and mesoscale models is due to a lack of parameterization of the thermal effects of subgrid-scale topographic variation. These thermal effects drive subgrid-scale heated-slope-induced vertical circulations (SHVC). SHVC provide a ventilation effect of removing heat from the boundary layer of resolvable-scale mountain slopes and depositing it higher up. The lack of SHVC parameterization is the cause of EPSM. The author has previously proposed a method of parameterizing SHVC, here termed SHVC.1. Although this has been successful in avoiding EPSM, the drawback is that it suppresses convective-type precipitation in the regions where it is applied. In this article, the author proposes a new method of parameterizing SHVC, here termed SHVC.2. In SHVC.2, the potential temperature and mixing ratio of the boundary layer are changed when used as input to the cumulus parameterization scheme over mountainous regions. This allows the cumulus parameterization to assume the additional function of SHVC parameterization. SHVC.2 has been tested in NASA Goddard's GEOS-5 GCM. It achieves the primary goal of avoiding EPSM while also avoiding the suppression of convective-type precipitation in the regions where it is applied. C1 [Chao, Winston C.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Chao, WC (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 610-1, Greenbelt, MD 20771 USA. EM winston.c.chao@nasa.gov FU NASA [WBS 432938.11.01.04.01.06, WBS 802678.02.17.01.25] FX Help from Larry Takacs, Matt Thompson, Joe Stassi, Danifan Barahona, and Purnendu Chakraborty of NASA GSFC GMAO in using the GEOS-5 GCM and programming advices is gratefully acknowledged. Discussion with Max Suarez was useful. Jim Gass provided graphics support. This work was supported by NASA under WBS 432938.11.01.04.01.06 and WBS 802678.02.17.01.25. Computing resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Center for Climate Studies (NCCS) at the Goddard Space Flight Center. Maharaj Bhat of NASA/NCCS helped with setting up the Fortran code for the Student's t test. NR 16 TC 1 Z9 1 U1 1 U2 2 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 JUN PY 2015 VL 72 IS 6 BP 2366 EP 2378 DI 10.1175/JAS-D-14-0336.1 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CI9RW UT WOS:000355108500011 ER PT J AU Zhang, GJ Fan, JW Xu, KM AF Zhang, Guang J. Fan, Jiwen Xu, Kuan-Man TI Comments on "A Unified Representation of Deep Moist Convection in Numerical Modeling of the Atmosphere. Part I" SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Editorial Material C1 [Zhang, Guang J.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Fan, Jiwen] Pacific NW Natl Lab, Richland, WA 99352 USA. [Xu, Kuan-Man] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Zhang, GJ (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, CASPO, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM gzhang@ucsd.edu RI Fan, Jiwen/E-9138-2011; Xu, Kuan-Man/B-7557-2013 OI Xu, Kuan-Man/0000-0001-7851-2629 NR 3 TC 2 Z9 2 U1 0 U2 6 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 JUN PY 2015 VL 72 IS 6 BP 2562 EP 2565 DI 10.1175/JAS-D-14-0246.1 PG 4 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CI9RW UT WOS:000355108500022 ER PT J AU Frederick, MA Banks, DW Garzon, GA Matisheck, JR AF Frederick, M. A. Banks, D. W. Garzon, G. A. Matisheck, J. R. TI Flight tests of a supersonic natural laminar flow airfoil SO MEASUREMENT SCIENCE AND TECHNOLOGY LA English DT Article; Proceedings Paper CT 16th International Symposium on Flow Visualization (ISFV) CY JUL 24-27, 2014 CL Okinawa, JAPAN DE supersonic natural laminar flow; boundary layer transition; boundary layer; laminar flow; infrared thermography; flight test; airfoil AB A flight test campaign of a supersonic natural laminar flow airfoil has been recently completed. The test surface was an 80 inch (203 cm) chord and 40 inch (102 cm) span article mounted on the centerline store location of an F-15B airplane. The test article was designed with a leading edge sweep of effectively 0 degrees to minimize boundary layer crossflow. The test article surface was coated with an insulating material to avoid significant heat transfer to and from the test article structure to maintain a quasi-adiabatic wall. An aircraft-mounted infrared camera system was used to determine boundary layer transition and the extent of laminar flow. The tests were flown up to Mach 2.0 and chord Reynolds numbers in excess of 30 million. The objectives of the tests were to determine the extent of laminar flow at high Reynolds numbers and to determine the sensitivity of the flow to disturbances. Both discrete (trip dots) and 2D disturbances (forward-facing steps) were tested. A series of oblique shocks, of yet unknown origin, appeared on the surface, which generated sufficient crossflow to affect transition. Despite the unwanted crossflow, the airfoil performed well. The results indicate that the sensitivity of the flow to the disturbances, which can translate into manufacturing tolerances, was similar to that of subsonic natural laminar flow wings. C1 [Frederick, M. A.; Banks, D. W.] NASA, Armstrong Flight Res Ctr, Edwards AFB, CA 93523 USA. [Garzon, G. A.; Matisheck, J. R.] Aerion Corp, Reno, NV 89502 USA. RP Frederick, MA (reprint author), NASA, Armstrong Flight Res Ctr, Edwards AFB, CA 93523 USA. EM mike.frederick-1@nasa.gov FU NASA High Speed Fundamental Aeronautics Project; Aerion Corporation FX Funding for this research was provided by the NASA High Speed Fundamental Aeronautics Project and the Aerion Corporation. NR 15 TC 0 Z9 0 U1 1 U2 11 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 JUN PY 2015 VL 26 IS 6 AR 064003 DI 10.1088/0957-0233/26/6/064003 PG 18 WC Engineering, Multidisciplinary; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA CI4VR UT WOS:000354752500004 ER PT J AU Roundy, JK Yuan, X Schaake, J Wood, EF AF Roundy, Joshua K. Yuan, Xing Schaake, John Wood, Eric F. TI A Framework for Diagnosing Seasonal Prediction through Canonical Event Analysis SO MONTHLY WEATHER REVIEW LA English DT Article ID CLIMATE FORECAST SYSTEM; UNITED-STATES; PRECIPITATION; DROUGHT; FLOODS AB Hydrologic extremes in the form of flood and drought have large impacts on society that can be reduced through preparations made possible by seasonal prediction. However, the skill of seasonal predictions from global climate models is uncertain, which severely limits their practical use. In the past, the skill assessment has been limited to a single temporal or spatial resolution for a short hindcast period, which is prone to sampling errors, and noise that leads to uncertainty. In this work a framework that uses "canonical" forecast events, or averages in space-time, to provide a more certain assessment of when and where models are skillful is developed. This framework is demonstrated by using NCEP's Climate Forecast System, version 2, hindcast dataset for precipitation and temperature over the contiguous United States (CONUS). As part of the canonical event analyses, the probabilistic predictability metric (PPM) is used to define spatial and seasonal variability of forecast skill and its attribution to El Nino-Southern Oscillation (ENSO) over the CONUS. The PPM indicates that there are clear seasonal and spatial patterns of model skill that provide a better understanding of when and where to have confidence in model predictions as compared to a skill metric based on a single temporal and spatial scale. Furthermore, the canonical event analysis also facilitates the attribution of spatiotemporal variations of precipitation predictive skill to the antecedent ENSO conditions. This work illustrates the importance of using canonical event analysis to diagnose seasonal predictions and discusses its extensions for model development. C1 [Roundy, Joshua K.; Yuan, Xing; Wood, Eric F.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. RP Roundy, JK (reprint author), NASA, Goddard Space Flight Ctr, Bldg 33,Room G209, Greenbelt, MD 20771 USA. EM joshua.roundy@nasa.gov RI Yuan, Xing/G-8392-2011; Roundy, Joshua/H-9377-2016 OI Yuan, Xing/0000-0001-6983-7368; Roundy, Joshua/0000-0003-0328-3248 FU NASA Earth and Space Science Fellowship [NNX08AU28H]; NOAA Climate Program Office [NA10OAR4310246, NA12OAR4310090] FX J. K. Roundy was supported through NASA Earth and Space Science Fellowship NNX08AU28H (Understanding Hydrologic Sensitivity and Land-Atmosphere Coupling through Space-Based Remote Sensing), and through support from the NOAA Climate Program Office (Grants NA10OAR4310246 and NA12OAR4310090). The support for this research is gratefully acknowledged. We would also like to thank the three anonymous reviewers for their helpful comments. NR 25 TC 3 Z9 3 U1 0 U2 7 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 JUN PY 2015 VL 143 IS 6 BP 2404 EP 2418 DI 10.1175/MWR-D-14-00190.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CJ0TL UT WOS:000355190900023 ER PT J AU Lamsal, LN Duncan, BN Yoshida, Y Krotkov, NA Pickering, KE Streets, DG Lu, ZF AF Lamsal, Lok N. Duncan, Bryan N. Yoshida, Yasuko Krotkov, Nickolay A. Pickering, Kenneth E. Streets, David G. Lu, Zifeng TI U.S. NO2 trends (2005-2013): EPA Air Quality System (AQS) data versus improved observations from the Ozone Monitoring Instrument (OMI) SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Nitrogen dioxide; Troposphere; Air quality; Trend; Aura OMI ID TROPOSPHERIC NITROGEN-DIOXIDE; UNITED-STATES; SATELLITE RETRIEVALS; ECONOMIC RECESSION; COLUMN RETRIEVAL; POWER-PLANTS; INTEX-B; EMISSIONS; SPACE; INVENTORY AB Emissions of nitrogen oxides (NOx) and, subsequently, atmospheric levels of nitrogen dioxide (NO2) have decreased over the U.S. due to a combination of environmental policies and technological change. Consequently, NO2 levels have decreased by 30-40% in the last decade. We quantify NO2 trends (2005 -2013) over the U.S. using surface measurements from the U.S. Environmental Protection Agency (EPA) Air Quality System (AQS) and an improved tropospheric NO2 vertical column density (VCD) data product from the Ozone Monitoring Instrument (OMI) on the Aura satellite. We demonstrate that the current OMI NO2 algorithm is of sufficient maturity to allow a favorable correspondence of trends and variations in OMI and AQS data. Our trend model accounts for the non-linear dependence of NO2 concentration on emissions associated with the seasonal variation of the chemical lifetime, including the change in the amplitude of the seasonal cycle associated with the significant change in NOx emissions that occurred over the last decade. The direct relationship between observations and emissions becomes more robust when one accounts for these non-linear dependencies. We improve the OMI NO2 standard retrieval algorithm and, subsequently, the data product by using monthly vertical concentration profiles, a required algorithm input, from a high-resolution chemistry and transport model (CTM) simulation with varying emissions (2005-2013). The impact of neglecting the time-dependence of the profiles leads to errors in trend estimation, particularly in regions where emissions have changed substantially. For example, trends calculated from retrievals based on time-dependent profiles offer 18% more instances of significant trends and up to 15% larger total NO2 reduction versus the results based on profiles for 2005. Using a CTM, we explore the theoretical relation of the trends estimated from NO2 VCDs to those estimated from ground-level concentrations. The model-simulated trends in VCDs strongly correlate with those estimated from surface concentrations (r = 0.83, N = 355). We then explore the observed correspondence of trends estimated from OMI and AQS data. We find a significant, but slightly weaker, correspondence (i.e., r = 0.68, N = 208) than predicted by the model and discuss some of the important factors affecting the relationship, including known problems (e.g., NOz interferents) associated with the AQS data. This significant correspondence gives confidence in trend and surface concentration estimates from OMI VCDs for locations, such as the majority of the U.S. and globe, that are not covered by surface monitoring networks. Using our improved trend model and our enhanced OMI data product, we find that both OMI and AQS data show substantial downward trends from 2005 to 2013, with an average reduction of 38% for each over the U.S. The annual reduction rates inferred from OMI and AQS measurements are larger (-4.8 +/- 1.9%/yr, -3.7 +/- 1.5%/yr) from 2005 to 2008 than 2010 to 2013 (-1.2 +/- 1.2%/yr, -2.1 +/- 1.4%/yr). We quantify NO2 trends for major U.S. cities and power plants; the latter suggest larger negative trend (-4.0 +/- 1.5%/yr) between 2005 and 2008 and smaller or insignificant changes (-0.5 +/- 1.2%/yr) during 2010-2013. (C) 2015 The Authors. Published by Elsevier Ltd. C1 [Lamsal, Lok N.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA. [Lamsal, Lok N.; Duncan, Bryan N.; Yoshida, Yasuko; Krotkov, Nickolay A.; Pickering, Kenneth E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Yoshida, Yasuko] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Streets, David G.; Lu, Zifeng] Argonne Natl Lab, Decis & Informat Sci Div, Argonne, IL 60439 USA. RP Lamsal, LN (reprint author), NASA, GESTAR USRA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM lok.lamsal@nasa.gov RI Krotkov, Nickolay/E-1541-2012; Pickering, Kenneth/E-6274-2012; Duncan, Bryan/A-5962-2011 OI Krotkov, Nickolay/0000-0001-6170-6750; FU NASA Air Quality Applied Science Team (AQAST); NASA's Earth Science Directorate Atmospheric Composition Programs FX Heather Simon, Paul Miller, and two anonymous reviewers provided helpful comments that improved this manuscript. This work was supported by the NASA Air Quality Applied Science Team (AQAST) and NASA's Earth Science Directorate Atmospheric Composition Programs. NR 89 TC 21 Z9 22 U1 11 U2 76 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 JUN PY 2015 VL 110 BP 130 EP 143 DI 10.1016/j.atmosenv.2015.03.055 PG 14 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA CI2QG UT WOS:000354591500015 ER PT J AU Streit, K Bennett, SA Van Dover, CL Coleman, M AF Streit, Kathrin Bennett, Sarah A. Van Dover, Cindy L. Coleman, Max TI Sources of organic carbon for Rimicaris hybisae: Tracing individual fatty acids at two hydrothermal vent fields in the Mid-Cayman rise SO DEEP-SEA RESEARCH PART I-OCEANOGRAPHIC RESEARCH PAPERS LA English DT Article DE Chemosynthetic carbon source; Photosynthetic carbon source; Hydrothermal vent chemistry; Piccard; Von Damm; Ectosymbionts ID DEEP-SEA VENT; EXOCULATA; COMMUNITY; SHRIMPS; FRACTIONATION; BIOSYNTHESIS; BIOLOGY; LIPIDS; RIDGE; LIFE AB Hydrothermal vents harbor ecosystems mostly decoupled from organic carbon synthesized with the energy of sunlight (photosynthetic carbon source) but fueled instead by oxidation of reduced compounds to generate a chemosynthetic carbon source. Our study aimed to disentangle photosynthetic and chemosynthetic organic carbon sources for the shrimp species Rimicaris hybisae, a primary consumer presumed to obtain its organic carbon mainly from ectosymbiotic chemoautotrophic bacteria living on its gill cover membrane. To provide ectosymbionts with ideal conditions for chemosynthesis, these shrimp live in dense clusters around vent chimneys; they are, however, also found sparsely distributed adjacent to diffuse vent flows, where they might depend on alternative food sources. Densely and sparsely distributed shrimp were sampled and dissected into abdominal tissue and gill cover membrane, covered with ectosymbiotic bacteria, at two hydrothermal vent fields in the Mid-Cayman rise that differ in vent chemistry. Fatty acids (FA) were extracted from shrimp tissues and their carbon isotopic compositions assessed. The FA data indicate that adult R. hybisae predominantly rely on bacteria for their organic carbon needs. Their FA composition is dominated by common bacterial FA of the n7 family (similar to 41%). Bacterial FA of the n4 FA family are also abundant and found to constitute good biomarkers for gill ectosymbionts. Sparsely distributed shrimp contain fractions of n4 FA in gill cover membranes similar to 4% lower than densely packed ones (similar to 18%) and much higher fractions of photosynthetic FA in abdominal tissues, similar to 4% more (compared with 1.6%), suggesting replacement of ectosymbionts along with exoskeletons (molt), while they take up alternative diets of partly photosynthetic organic carbon. Abdominal tissues also contain photosynthetic FA from a second source taken up presumably during an early dispersal phase and still present to c. 3% in adult shrimp. The contribution of photosynthetic carbon to the FA pool of adult R. hybisae is, however, overall small (max. 8%). Significant differences in carbon isotopic values of chemosynthetically derived FA between vent fields suggest that different dominant C fixation pathways are being used. (C) 2015 Published by Elsevier Ltd. C1 [Streit, Kathrin; Bennett, Sarah A.; Coleman, Max] NASA, Jet Prop Lab, CALTECH, Pasadena, CA 91109 USA. [Van Dover, Cindy L.] Duke Univ, Marine Lab, Nicholas Sch Environm, Beaufort, NC 28516 USA. RP Coleman, M (reprint author), NASA, Jet Prop Lab, CALTECH, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM max.coleman@jpl.nasa.gov FU National Science Foundation [OCE-1061863, OCE-1061881]; NASA's Astrobiology Science and Technology for Exploring Planets Program [NNX09AB75G]; ASTEP grant [NNX09AB75G]; NSF [OCE-221061881] FX We thank the R/V Atlantis crew (AT18-16), the ROV Jason Operations Team and the OASES 2012 Science Party, Chief Scientist Chris German, for help during the cruise, which was supported jointly by grants to CRG from the National Science Foundation (OCE-1061863) and NASA's Astrobiology Science and Technology for Exploring Planets Program (NNX09AB75G) and to MC from the National Science Foundation (OCE-1061881). The post-cruise contributions of KS, SAB and MC were supported through the same ASTEP grant (NNX09AB75G) and one of the NSF grants (OCE-221061881) and were carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). The authors would like to thank E. Versteegh, B. Theiling, R. Kidd, K. Williford and R. Mielke (JPL) for their assistance in the laboratory, A. Sessions (Caltech) for giving inputs on the GC-IRMS technique and the JPL Planetary Surface Instruments Group led by M. Darrach for many fruitful discussions. NR 41 TC 1 Z9 1 U1 5 U2 19 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0637 EI 1879-0119 J9 DEEP-SEA RES PT I JI Deep-Sea Res. Part I-Oceanogr. Res. Pap. PD JUN PY 2015 VL 100 BP 13 EP 20 DI 10.1016/j.dsr.2015.02.003 PG 8 WC Oceanography SC Oceanography GA CI2PG UT WOS:000354588900002 ER PT J AU Anderson, RL AF Anderson, Rodney L. TI Approaching Moons from Resonance via Invariant Manifolds SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article; Proceedings Paper CT 22nd AAS/AIAA Space Flight Mechanics Meeting CY JAN 29-FEB 02, 2012 CL Charleston, SC SP AAS, Space Flight Mech Comm, AIAA, Astrodynam Techn Comm ID RESTRICTED 3-BODY PROBLEM; DYNAMICAL-SYSTEMS ANALYSIS; EUROPA ORBITER MISSION; TRAJECTORY DESIGN; HALO ORBITS; TRANSFERS; CAPTURE; COMETS; FLYBYS; CONNECTIONS AB In this work, the final approach typical of a trajectory traveling from the last resonance of an endgame scenario in a tour down to a moon is examined within the context of invariant manifolds. Previous analyses have usually solved this problem either by using numerical techniques or by computing a catalog of suitable trajectories. The invariant manifolds of a selected set of libration orbits and unstable resonant orbits are computed here to serve as guides for desirable approach trajectories. The analysis focuses on designing an approach phase that may be tied into the final resonance in the endgame sequence while also targeting desired conditions at the moon. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Anderson, RL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 301-121, Pasadena, CA 91109 USA. NR 68 TC 3 Z9 3 U1 1 U2 1 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 JUN PY 2015 VL 38 IS 6 BP 1097 EP 1109 DI 10.2514/1.G000286 PG 13 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA CI2ZC UT WOS:000354615900010 ER PT J AU Narayan, SR Manohar, AK Mukerjee, S AF Narayan, S. R. Manohar, Aswin K. Mukerjee, Sanjeev TI Bi-Functional Oxygen Electrodes - Challenges and Prospects SO ELECTROCHEMICAL SOCIETY INTERFACE LA English DT Article ID REGENERATIVE FUEL-CELLS; CARBON-BLACK ANODES; ELECTROCATALYTIC ACTIVITY; ALKALINE ELECTROLYTE; REDUCTION REACTION; CATHODE CATALYSTS; PEROVSKITE OXIDES; LI-O-2 BATTERIES; AIR; EVOLUTION C1 [Narayan, S. R.] NASA Jet Prop Lab, Pasadena, CA 91109 USA. [Narayan, S. R.; Manohar, Aswin K.] Univ So Calif, Los Angeles, CA 90089 USA. [Mukerjee, Sanjeev] Northeastern Univ, Dept Chem & Chem Biol, Boston, MA USA. [Mukerjee, Sanjeev] Northeastern Univ, Renewable Energy Technol, New York, NY USA. [Mukerjee, Sanjeev] LEAP, New York, NY USA. RP Narayan, SR (reprint author), NASA Jet Prop Lab, Pasadena, CA 91109 USA. EM sri.narayan@usc.edu; aswinkam@usc.edu; s.mukerjee@neu.edu NR 52 TC 1 Z9 1 U1 7 U2 11 PU ELECTROCHEMICAL SOC INC PI PENNINGTON PA 65 SOUTH MAIN STREET, PENNINGTON, NJ 08534 USA SN 1064-8208 EI 1944-8783 J9 ELECTROCHEM SOC INTE JI Electrochem. Soc. Interface PD SUM PY 2015 VL 24 IS 2 BP 65 EP 69 DI 10.1149/2.F06152IF PG 5 WC Electrochemistry SC Electrochemistry GA DM7SO UT WOS:000376560500013 ER PT J AU Bowers, ML Gao, Y Yang, L Gaydosh, DJ De Graef, M Noebe, RD Wang, Y Mills, MJ AF Bowers, M. L. Gao, Y. Yang, L. Gaydosh, D. J. De Graef, M. Noebe, R. D. Wang, Y. Mills, M. J. TI Austenite grain refinement during load-biased thermal cycling of a Ni49.9Ti50.1 shape memory alloy SO ACTA MATERIALIA LA English DT Article DE SMA; Microstructural evolution; Actuation; Orientation mapping; Defect analysis ID SITU NEUTRON-DIFFRACTION; SELF-ACCOMMODATION; B19' MARTENSITE; NITI; TRANSFORMATION; STRESS; DEFORMATION; EVOLUTION; BEHAVIOR; MICROCRYSTALS AB A near-equiatomic NiTi shape memory alloy was subjected to a variety of thermomechanical treatments including pure thermal cycling and load-biased thermal cycling to investigate microstructural evolution of the material under actuating conditions. In situ and post mortem scanning transmission electron microscopy (STEM) was used to study the effects of stress on the development of defect substructures during cycling through the martensitic transformation. High temperature observations of the austenite phase show rapid accumulation of dislocations and moderate deformation twinning upon thermomechanical cycling. Additionally, TEM-based orientation mapping suggests the emergence of fine crystallites from the original coarse austenite grain structure. A possible mechanism is proposed for the observed grain refinement based on the crystallographic theory of martensite transformation. (C) 2015 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved. C1 [Bowers, M. L.; Gao, Y.; Yang, L.; Wang, Y.; Mills, M. J.] Ohio State Univ, Dept Mat Sci & Engn, Columbus, OH 43210 USA. [De Graef, M.] Carnegie Mellon Univ, Dept Mat Sci & Engn, Pittsburgh, PA USA. [Gaydosh, D. J.; Noebe, R. D.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA. [Gaydosh, D. J.] Ohio Aerosp Inst, Cleveland, OH 44142 USA. RP Bowers, ML (reprint author), Ohio State Univ, Dept Mat Sci & Engn, Columbus, OH 43210 USA. RI Wang, Yunzhi/B-2557-2010 FU DOE Basic Energy Sciences award [DE-SC0001258]; NSF [DMR-1207494, DMR-1410322]; NASA ARMD Aeronautical Sciences and Transformational Tools & Technologies Projects FX This work was supported in part by DOE Basic Energy Sciences award #DE-SC0001258, NSF awards #DMR-1207494 and #DMR-1410322, and the NASA ARMD Aeronautical Sciences and Transformational Tools & Technologies Projects (technical discipline lead Dale Hopkins). The authors gratefully acknowledge Noel T. Nuhfer at CMU for assisting with the ASTAR data acquisition. We would also like to thank Dr. Othmane Benafan for providing the as-tested 100 MPa-20cycle NiTi sample for ASTAR analysis. NR 36 TC 5 Z9 5 U1 3 U2 34 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 JUN 1 PY 2015 VL 91 BP 318 EP 329 DI 10.1016/j.actamat.2015.03.017 PG 12 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA CH6NX UT WOS:000354154400028 ER PT J AU Urschel, MR Kubo, MD Hoehler, TM Peters, JW Boyd, ES AF Urschel, Matthew R. Kubo, Michael D. Hoehler, Tori M. Peters, John W. Boyd, Eric S. TI Carbon Source Preference in Chemosynthetic Hot Spring Communities SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID YELLOWSTONE-NATIONAL-PARK; STREAMER BIOFILM COMMUNITIES; GEOTHERMAL SPRINGS; SP-NOV.; HYDROTHERMAL ECOSYSTEMS; ESCHERICHIA-COLI; ENERGY; AQUIFICALES; GROWTH; ACID AB Rates of dissolved inorganic carbon (DIC), formate, and acetate mineralization and/or assimilation were determined in 13 high-temperature (> 73 degrees C) hot springs in Yellowstone National Park (YNP), Wyoming, in order to evaluate the relative importance of these substrates in supporting microbial metabolism. While 9 of the hot spring communities exhibited rates of DIC assimilation that were greater than those of formate and acetate assimilation, 2 exhibited rates of formate and/or acetate assimilation that exceeded those of DIC assimilation. Overall rates of DIC, formate, and acetate mineralization and assimilation were positively correlated with spring pH but showed little correlation with temperature. Communities sampled from hot springs with similar geochemistries generally exhibited similar rates of substrate transformation, as well as similar community compositions, as revealed by 16S rRNA gene-tagged sequencing. Amendment of microcosms with small (micromolar) amounts of formate suppressed DIC assimilation in short-term (< 45min) incubations, despite the presence of native DIC concentrations that exceeded those of added formate by 2 to 3 orders of magnitude. The concentration of added formate required to suppress DIC assimilation was similar to the affinity constant (Km) for formate transformation, as determined by community kinetic assays. These results suggest that dominant chemoautotrophs in high-temperature communities are facultatively autotrophic or mixotrophic, are adapted to fluctuating nutrient availabilities, and are capable of taking advantage of energy-rich organic substrates when they become available. C1 [Urschel, Matthew R.; Boyd, Eric S.] Montana State Univ, Dept Microbiol & Immunol, Bozeman, MT 59717 USA. [Urschel, Matthew R.; Peters, John W.; Boyd, Eric S.] Montana State Univ, Thermal Biol Inst, Bozeman, MT 59717 USA. [Kubo, Michael D.; Hoehler, Tori M.] NASA, Ames Res Ctr, Mountain View, CA USA. [Peters, John W.] Montana State Univ, Dept Chem & Biochem, Bozeman, MT 59717 USA. RP Boyd, ES (reprint author), Montana State Univ, Dept Microbiol & Immunol, Bozeman, MT 59717 USA. EM eboyd@montana.edu OI Peters, John/0000-0001-9117-9568 FU NASA Exobiology and Evolutionary Biology award [NNX10AT31G]; NSF Partnerships in International Research and Education award [PIRE-0968421] FX This work was supported by NASA Exobiology and Evolutionary Biology award NNX10AT31G (to T.M.H. and E.S.B.) and NSF Partnerships in International Research and Education award PIRE-0968421 (to J.W.P.). NR 54 TC 4 Z9 4 U1 1 U2 13 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 EI 1098-5336 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD JUN PY 2015 VL 81 IS 11 BP 3834 EP 3847 DI 10.1128/AEM.00511-15 PG 14 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA CH3FA UT WOS:000353912000029 PM 25819970 ER PT J AU Hultquist, G Graham, MJ Kodra, O Moisa, S Liu, R Bexell, U Smialek, JL AF Hultquist, G. Graham, M. J. Kodra, O. Moisa, S. Liu, R. Bexell, U. Smialek, J. L. TI Corrosion of copper in distilled water without O-2 and the detection of produced hydrogen SO CORROSION SCIENCE LA English DT Article DE Copper; AES; XPS; SIMS; Oxidation; Hydrogen absorption ID PURE WATER; FUNDAMENTAL-ASPECTS; SOLID-SURFACES; SPECTROSCOPY; OXIDATION AB This paper reports on hydrogen pressures measured during similar to 19,000 h immersion of copper in oxygen-free liquid distilled water. Copper corrosion products have been examined ex-situ by SEM and characterized by XPS and SIMS. XPS strongly indicates a corrosion product containing both oxygen and hydrogen. SIMS shows that oxygen is mainly present in the outer 0.3 mu m surface region and that hydrogen penetrates to depths well below the corrosion product. Thermal desorption spectroscopy shows that the reaction product formed near room-temperature is less stable than that formed in air at 350 degrees C. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Hultquist, G.] Royal Inst Technol, Surface & Corros Sci, SE-10044 Stockholm, Sweden. [Graham, M. J.] Natl Res Council Canada, Aerosp, Ottawa, ON K1A 0R6, Canada. [Kodra, O.; Moisa, S.] Natl Res Council Canada, Elect & Photon Mat, Ottawa, ON K1A 0R6, Canada. [Liu, R.] Natl Univ Singapore, Fac Sci, Singapore 117551, Singapore. [Bexell, U.] Dalarna Univ, SE-79188 Falun, Sweden. [Smialek, J. L.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA. RP Hultquist, G (reprint author), Royal Inst Technol, Surface & Corros Sci, SE-10044 Stockholm, Sweden. EM gunnarh@kth.se FU Swedish Radiation Safety Authority (SSM) FX The Swedish Radiation Safety Authority (SSM) is gratefully acknowledged for financial support. NR 17 TC 9 Z9 9 U1 3 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0010-938X EI 1879-0496 J9 CORROS SCI JI Corrosion Sci. PD JUN PY 2015 VL 95 BP 162 EP 167 DI 10.1016/j.corsci.2015.03.009 PG 6 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA CH4KC UT WOS:000354001400017 ER PT J AU Khazendar, A Borstad, CP Scheuchl, B Rignot, E Seroussi, H AF Khazendar, Ala Borstad, Christopher P. Scheuchl, Bernd Rignot, Eric Seroussi, Helene TI The evolving instability of the remnant Larsen B Ice Shelf and its tributary glaciers SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Antarctica; Larsen Ice Shelf; ice-shelf instability; laser altimetry; InSAR ice flow speeds; numerical ice modeling ID PINE ISLAND GLACIER; ANTARCTIC PENINSULA; RADAR INTERFEROMETRY; ELEVATION CHANGES; LASER ALTIMETRY; COLLAPSE; SHEET; THICKNESS; FLOW; DISINTEGRATION AB Following the 2002 disintegration of the northern and central parts of the Larsen B Ice Shelf, the tributary glaciers of the southern surviving part initially appeared relatively unchanged and hence assumed to be buttressed sufficiently by the remnant ice shelf. Here, we modify this perception with observations from IceBridge altimetry and InSAR-inferred ice flow speeds. Our analyses show that the surfaces of Leppard and Flask glaciers directly upstream from their grounding lines lowered by 15 to 20 m in the period 2002-2011. The thinning appears to be dynamic as the flow of both glaciers and the remnant ice shelf accelerated in the same period. Flask Glacier started accelerating even before the 2002 disintegration, increasing its flow speed by similar to 55% between 1997 and 2012. Starbuck Glacier meanwhile did not change much. We hypothesize that the different evolutions of the three glaciers are related to their dissimilar bed topographies and degrees of grounding. We apply numerical modeling and data assimilation that show these changes to be accompanied by a reduction in the buttressing afforded by the remnant ice shelf, a weakening of the shear zones between its flow units and an increase in its fracture. The fast flowing northwestern part of the remnant ice shelf exhibits increasing fragmentation, while the stagnant southeastern part seems to be prone to the formation of large rifts, some of which we show have delimited successive calving events. A large rift only 12 km downstream from the grounding line is currently traversing the stagnant part of the ice shelf, defining the likely front of the next large calving event. We propose that the flow acceleration, ice front retreat and enhanced fracture of the remnant Larsen B Ice Shelf presage its approaching demise. (C) 2015 Elsevier B.V. All rights reserved. C1 [Khazendar, Ala; Borstad, Christopher P.; Rignot, Eric; Seroussi, Helene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Scheuchl, Bernd; Rignot, Eric] Univ Calif Irvine, Earth Syst Sci, Irvine, CA 92697 USA. RP Khazendar, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ala@jpl.nasa.gov RI Rignot, Eric/A-4560-2014; OI Rignot, Eric/0000-0002-3366-0481; Borstad, Christopher/0000-0001-6992-1770 FU NASA's Cryospheric Sciences Program; NASA's MEaSuREs Program; NASA's Modeling, Analysis and Prediction Program; National Aeronautics and Space Administration FX This work was supported by NASA's Cryospheric Sciences Program (A.K., C.B. and H.S.), NASA's MEaSuREs Program (B.S. and E.R.) and NASA's Modeling, Analysis and Prediction Program (C.B.). Spaceborne SAR data collection post 2005 was coordinated by the Space Task Group and its successor, the Polar Space Task Group. The authors are grateful to L. Padman for providing the ocean tide model. The authors much appreciate the highly constructive and helpful comments made by three anonymous reviewers.; This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 62 TC 8 Z9 8 U1 6 U2 39 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 JUN 1 PY 2015 VL 419 BP 199 EP 210 DI 10.1016/j.eps1.2015.03.014 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CH2JW UT WOS:000353852500019 ER PT J AU Rhodes, KL Warren-Rhodes, KA Sweet, S Helgenberger, M Joseph, E Boyle, LN Hopkins, KD AF Rhodes, Kevin L. Warren-Rhodes, Kimberley A. Sweet, Scott Helgenberger, Mike Joseph, Eugene Boyle, Linda Ng Hopkins, Kevin D. TI Marine ecological footprint indicates unsustainability of the Pohnpei (Micronesia) coral reef fishery SO ENVIRONMENTAL CONSERVATION LA English DT Article DE biocapacity; consumption; ecological overshoot; marine ecological footprint; Micronesia; overfishing ID ECOSYSTEM APPROPRIATION; PACIFIC; ISLAND; CATCH; COMMUNITIES; MANAGEMENT; DIVERSITY; DYNAMICS; SERVICES; BIOMASS AB Throughout the tropics, developing countries and territories are highly dependent on nearshore marine resources for food and income, however information on the sustainability and proper management of these fisheries is lacking. In Pohnpei, Micronesia, the sustainability of a coral reef finfishery was assessed by comparing coral reef fish demand to coral reef biocapacity using a marine ecological footprint (MEF) analysis. Based on geo-referenced satellite and aerial imagery, Pohnpei and surrounding atolls have 184.2 km(2) of coral reef habitat with a sustainable finfish yield of 573-1118 t yr(-1), however total harvest was estimated at 4068 t yr(-1), exceeding biocapacity by 360-710%. The MEF was supported by observed impacts to coral reef resources, including (1) long-term declines in fish spawning aggregation density, (2) reductions in mean size, age and fecundity of key commercial species, (3) reliance on undersized fish, and (4) decadal declines in mean size and abundance of fishes of iconic value and critical to ecosystem maintenance. The commercial fishery was responsible for 68% of finfish catch volume, while reef fish consumption, at 93 kg person(-1) yr(-1), was among the highest in the region. To sustainably meet current demand, up to 833 km(2) of additional reef area would be required. The study illustrates the MEF, at least rudimentarily, reflects biological reality on local reefs and represents a valuable analytical tool in a marine policymaker's toolbox. C1 [Rhodes, Kevin L.; Hopkins, Kevin D.] Univ Hawaii, Coll Forestry Agr & Nat Resource Management, Hilo, HI 96720 USA. [Warren-Rhodes, Kimberley A.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Sweet, Scott] TerraUnda, Dumaguete 6200, Negros Oriental, Philippines. [Helgenberger, Mike] Off Fisheries & Aquaculture, FM-96941 Kolonia, Pohnpei, Micronesia. [Joseph, Eugene] Conservat Soc Pohnpei, Kolonia 96941, Pohnpei, Micronesia. [Boyle, Linda Ng] Univ Washington, Dept Ind & Syst Engn, Seattle, WA 98195 USA. RP Rhodes, KL (reprint author), Univ Hawaii, Coll Forestry Agr & Nat Resource Management, 200 W Kawili St, Hilo, HI 96720 USA. EM klrhodes_grouper@yahoo.com FU US Department of Interior; NOAA Coral Reef Conservation [NA08NMF4630458, NA05NMF4631049]; Micronesia Conservation Trust through the Margaret A. Cargill Foundation; Nature Conservancy FX We thank survey participants, the Pohnpei State Department of Lands and Natural Resources, and the College of Micronesia. Surveys were conducted and compiled by J. Amor, J. Hadley, M. Ioanis, E. John, C. Wichilmel and M. Obispo. Administrative assistance was provided by M. Albert, L. Yamada and P. Shed of the Conservation Society of Pohnpei, with logistical support from D. David and the Pohnpei Office of Fisheries and Aquaculture. Multi-year funding for fish monitoring at Kehpara was provided to the Conservation Society of Pohnpei through the US Department of Interior. Additional funding was made available through NOAA Coral Reef Conservation grants to Kevin Hopkins (NA08NMF4630458), M. Tupper (University of Guam) (NA05NMF4631049) and the Micronesia Conservation Trust through the Margaret A. Cargill Foundation. Additional funding was supplied by The Nature Conservancy to Scott Sweet. NR 70 TC 1 Z9 1 U1 7 U2 39 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0376-8929 EI 1469-4387 J9 ENVIRON CONSERV JI Environ. Conserv. PD JUN PY 2015 VL 42 IS 2 BP 182 EP 190 DI 10.1017/S037689291400023X PG 9 WC Biodiversity Conservation; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CH5AW UT WOS:000354047300011 ER PT J AU Rittweger, J Bareille, MP Clement, G Linnarsson, D Paloski, WH Wuyts, F Zange, J Angerer, O AF Rittweger, Joern Bareille, Marie-Pierre Clement, Gilles Linnarsson, Dag Paloski, William H. Wuyts, Floris Zange, Jochen Angerer, Oliver TI Short-arm centrifugation as a partially effective musculoskeletal countermeasure during 5-day head-down tilt bed rest-results from the BRAG1 study SO EUROPEAN JOURNAL OF APPLIED PHYSIOLOGY LA English DT Article DE Bed rest; Human physiology; Artificial gravity; Space flight; De-conditioning; Countermeasures ID FLYWHEEL RESISTIVE EXERCISE; LONG-DURATION SPACEFLIGHT; ARTIFICIAL GRAVITY; BONE LOSS; RESISTANCE EXERCISE; VERTICAL JUMP; PERFORMANCE; POWER; MICROGRAVITY; ASTRONAUTS AB Human centrifugation, also called artificial gravity (AG), is proposed as a combined strategy against detrimental effects of microgravity in long-term space missions. This study scrutinized human short-arm centrifugation as countermeasure against musculoskeletal de-conditioning. Eleven healthy male subjects [mean age of 34 (SD 7) years] completed the cross-over trial, including three campaigns of -6A degrees head-down tilt bed rest (HDT) for 5 days, with preceding baseline data collection and recovery phases. Bed rest without AG was used as control condition (Ctrl), and AG with 1 g at the center of mass applied once per day for 30 min in one bout (AG(1x30)) and in 6 bouts of 5 min (AG(6x5), 3-min rest between bouts) as experimental conditions. End-points were muscle strength, vertical jump performance, and biomarkers of bone and protein metabolism. AG(6x5) was better tolerated than AG(1x30). Bone resorption markers CTX, NTX, and DPD all increased by approximately 25 % toward the end of bed rest (P < 0.001), and nitrogen balance decreased by approximately 3 g/day (P < 0.001), without any protection by AG (P > 0.4). Decreases in vertical jump height by 2.1 (SE 0.6) cm after Ctrl bed rest was prevented by either of the AG protocols (P = 0.039). The present study yielded succinct catabolic effects upon muscle and bone metabolism that were un-prevented by AG. The preservation of vertical jump performance by AG in this study is likely caused by central nervous rather than by peripheral musculoskeletal effects. C1 [Rittweger, Joern; Zange, Jochen] German Aerosapce Ctr DLR, Inst Aerosp Med, D-51147 Cologne, Germany. [Bareille, Marie-Pierre] MEDES IMPS, F-31405 Toulouse 4, France. [Clement, Gilles] CNRS, Lyon Neurosci Res Ctr, UMR5292, F-69500 Lyon, France. [Linnarsson, Dag] Royal Inst Technol, Stockholm, Sweden. [Paloski, William H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Wuyts, Floris] Univ Antwerp, Dept Biomed Phys, B-2020 Antwerp, Belgium. [Angerer, Oliver] German Aerosp Ctr DLR, Space Adm, D-53227 Bonn, Germany. RP Rittweger, J (reprint author), German Aerosapce Ctr DLR, Inst Aerosp Med, Linder Hohe 1, D-51147 Cologne, Germany. EM joern.rittweger@dlr.de RI Rittweger, Jorn/A-4308-2009 FU ESA [22 127/08]; CNES [70686]; German Aerospace Center (DLR) within the project 'Artificial Gravity' FX This study was funded by ESA contract no. 22 127/08 and by a CNES framework agreement no. 70686. J Rittweger and J Zange were supported by internal funding from the German Aerospace Center (DLR) within the project 'Artificial Gravity'. In addition, J. Rittweger used private funds to participate in the study in its planning phase (2006-2009). We are grateful to the staff of MEDES for their excellent work and support of this study. Special thanks go to Dr. Petra Frings-Meuthen and Gaby Kraus from the DLR Institute of Aerospace Medicine for the assessment of serum and urine markers of bone metabolism. Last but not least, we are deeply indebted to the study participants-without their selfless contribution, this work would not have been possible. NR 38 TC 1 Z9 2 U1 1 U2 7 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1439-6319 EI 1439-6327 J9 EUR J APPL PHYSIOL JI Eur. J. Appl. Physiol. PD JUN PY 2015 VL 115 IS 6 BP 1233 EP 1244 DI 10.1007/s00421-015-3120-1 PG 12 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA CH9ZS UT WOS:000354395900006 PM 25667067 ER PT J AU Holgate, TC Bennett, R Hammel, T Caillat, T Keyser, S Sievers, B AF Holgate, Tim C. Bennett, Russell Hammel, Tom Caillat, Thierry Keyser, Steve Sievers, Bob TI Increasing the Efficiency of the Multi-mission Radioisotope Thermoelectric Generator SO JOURNAL OF ELECTRONIC MATERIALS LA English DT Article; Proceedings Paper CT International Conference on Thermoelectrics (ICT) CY JUL 06-10, 2014 CL Nashville, TN DE Thermoelectrics; RTG; radioisotope; generator; skutterudite ID MECHANICAL-PROPERTIES; SKUTTERUDITES AB The National Aeronautics and Space Administration's Mars Science Laboratory terrestrial rover, Curiosity, has recently completed its first Martian year (687 Earth days) during which it has provided a wealth of information and insight into the red planet's atmosphere and geology. The success of this mission was made possible in part by the reliable electrical power provided by its onboard thermoelectric power source-the multi-mission radioisotope thermoelectric generator (MMRTG). In an effort to increase the output power and efficiency of these generators, a newly designed enhanced MMRTG (eMMRTG) that will utilize the more efficient skutterudite-based thermoelectric materials has been conceptualized and modeled, and is now being developed. A discussion of the motivations, modeling results and key design factors are presented and discussed. C1 [Holgate, Tim C.; Bennett, Russell; Hammel, Tom; Keyser, Steve; Sievers, Bob] TESI, Hunt Valley, MD 21031 USA. [Caillat, Thierry] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Holgate, TC (reprint author), TESI, Hunt Valley, MD 21031 USA. EM Tim.holgate@teledyne.com NR 15 TC 2 Z9 2 U1 3 U2 38 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 JUN PY 2015 VL 44 IS 6 BP 1814 EP 1821 DI 10.1007/s11664-014-3564-9 PG 8 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA CH1WT UT WOS:000353813700065 ER PT J AU Hendricks, TJ AF Hendricks, Terry J. TI Perturbation Methods for Real-Time In Situ Evaluation of Hot-Side Thermal Resistances in Thermoelectric Energy Recovery Systems SO JOURNAL OF ELECTRONIC MATERIALS LA English DT Article; Proceedings Paper CT International Conference on Thermoelectrics (ICT) CY JUL 06-10, 2014 CL Nashville, TN DE Thermal resistance monitoring; perturbation; thermoelectric energy recovery AB Thermoelectric (TE) power systems in high-temperature industrial, transportation, and military energy systems require high-performance hot-side and cold-side heat transfer to provide the critical temperature differential and transfer the required thermal energy to create the power output. Hot- and cold-side heat transfer performance is typically characterized by the hot-side and cold-side thermal resistance, R (h,th) and R (c,th), respectively. This heat transfer performance determines the hot-side temperature, T (h), and cold-side temperature, T (c), conditions when operating in energy recovery environments with available temperature differentials characterized by an external driving temperature, T (src), and ambient temperature, T (amb). It is crucial to monitor and track the hot-side thermal performance at all times during TE energy recovery system operation, thereby allowing one to track the system "health," predict future expected system performance, and anticipate/prevent system failures. This paper describes the use of a perturbation methodology and a direct coupling between the TE current, voltage, and hot-side energy flow to extract a real-time in situ evaluation of hot-side thermal resistances. External measurable TE parameters, either system current or T (src), can be perturbed during system operation, and the resulting TE system response can then be coupled mathematically to the hot-side thermal transfer performance (i.e., thermal resistance). This paper discusses the mathematical formalism of this technique, and TE module experimental data showing successful application of real-time current perturbation. This technique provides a pathway for developing faster, real-time system monitoring and diagnostics to alleviate system performance degradation, or prevent system damage from dramatic changes in hot-side thermal transfer conditions in industrial, transportation, and spacecraft TE power systems. C1 CALTECH, NASA Jet Prop Lab, Thermal Energy Convers Grp, Power & Sensors Sect, Pasadena, CA 91125 USA. RP Hendricks, TJ (reprint author), CALTECH, NASA Jet Prop Lab, Thermal Energy Convers Grp, Power & Sensors Sect, Pasadena, CA 91125 USA. EM terry.j.hendricks@jpl.nasa.gov FU NASA [43-17508]; US Department of Energy, at the Jet Propulsion Laboratory, California Institute of Technology FX This work was carried out under NASA Space Act Agreement No. 43-17508, a contract between NASA and General Motors with funding from the US Department of Energy, at the Jet Propulsion Laboratory, California Institute of Technology, under a contract to the National Aeronautics and Space Administration. NR 17 TC 0 Z9 0 U1 2 U2 4 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 JUN PY 2015 VL 44 IS 6 BP 1909 EP 1918 DI 10.1007/s11664-014-3591-6 PG 10 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA CH1WT UT WOS:000353813700078 ER PT J AU Goldstein, ML Escoubet, P Hwang, KJ Wendel, DE Vinas, AF Fung, SF Perri, S Servidio, S Pickett, JS Parks, GK Sahraoui, F Gurgiolo, C Matthaeus, W Weygand, JM AF Goldstein, M. L. Escoubet, P. Hwang, K. -Joo Wendel, D. E. Vinas, A. -F. Fung, S. F. Perri, S. Servidio, S. Pickett, J. S. Parks, G. K. Sahraoui, F. Gurgiolo, C. Matthaeus, W. Weygand, J. M. TI Multipoint observations of plasma phenomena made in space by Cluster SO JOURNAL OF PLASMA PHYSICS LA English DT Article ID AURORAL KILOMETRIC RADIATION; SOLAR-WIND TURBULENCE; KELVIN-HELMHOLTZ INSTABILITY; ELECTRON-DISTRIBUTION FUNCTIONS; PERPENDICULAR BOW SHOCK; WHISTLER-MODE CHORUS; 3-DIMENSIONAL MAGNETIC RECONNECTION; SPECTROMETRY CIS EXPERIMENT; WAVE-PARTICLE INTERACTIONS; STORM-TIME CHORUS AB Plasmas are ubiquitous in nature, surround our local geospace environment, and permeate the universe. Plasma phenomena in space give rise to energetic particles, the aurora, solar flares and coronal mass ejections, as well as many energetic phenomena in interstellar space. Although plasmas can be studied in laboratory settings, it is often difficult, if not impossible, to replicate the conditions (density, temperature, magnetic and electric fields, etc.) of space. Single-point space missions too numerous to list have described many properties of near-Earth and heliospheric plasmas as measured both in situ and remotely (see http://www.nasa.gov/missions/#. U1mcVmeweRY for a list of NASA-related missions). However, a full description of our plasma environment requires three-dimensional spatial measurements. Cluster is the first, and until data begin flowing from the Magnetospheric Multiscale Mission (MMS), the only mission designed to describe the three-dimensional spatial structure of plasma phenomena in geospace. In this paper, we concentrate on some of the many plasma phenomena that have been studied using data from Cluster. To date, there have been more than 2000 refereed papers published using Cluster data but in this paper we will, of necessity, refer to only a small fraction of the published work. We have focused on a few basic plasma phenomena, but, for example, have not dealt with most of the vast body of work describing dynamical phenomena in Earth's magnetosphere, including the dynamics of current sheets in Earth's magnetotail and the morphology of the dayside high latitude cusp. Several review articles and special publications are available that describe aspects of that research in detail and interested readers are referred to them (see for example, Escoubet et al. 2005 Multiscale Coupling of Sun-Earth Processes, p. 459, Keith et al. 2005 Sur. Geophys. 26, 307-339, Paschmann et al. 2005 Outer Magnetospheric Boundaries: Cluster Results, Space Sciences Series of ISSI. Berlin: Springer, Goldstein et al. 2006 Adv. Space Res. 38, 21-36, Taylor et al. 2010 The Cluster Mission: Space Plasma in Three Dimensions, Springer, pp. 309-330 and Escoubet et al. 2013 Ann. Geophys. 31, 1045-1059). C1 [Goldstein, M. L.; Hwang, K. -Joo; Wendel, D. E.; Vinas, A. -F.; Fung, S. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Escoubet, P.] Estec, ESA, Noordwijk, Netherlands. [Hwang, K. -Joo] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Perri, S.; Servidio, S.] Univ Calabria, Dipartimento Fis, I-87036 Arcavacata Di Rende, Italy. [Pickett, J. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Parks, G. K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Sahraoui, F.] UPMC, Observ St Maur, Ecole Polytech, CNRS,Lab Phys Plasmas, F-94107 St Maur Des Fosses, France. [Gurgiolo, C.] Bitterroot Basic Res, Hamilton, MT 59840 USA. [Matthaeus, W.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Weygand, J. M.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. RP Goldstein, ML (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM melvyn.l.goldstein@nasa.gov RI Wendel, Deirdre/D-4429-2012; NASA MMS, Science Team/J-5393-2013 OI Wendel, Deirdre/0000-0002-1925-9413; NASA MMS, Science Team/0000-0002-9504-5214 FU NASA headquarters; MMS Interdisciplinary Science Team at the Goddard Space Flight Center; NSF [AGS-1155841]; project POR Calabria FSE; Marie Curie Project 'Turboplasmas' [FP7 PIRSES-2010-269297] FX The authors would like to thank the Cluster experiment teams for making available their data. J. S. Pickett, S. Fung, G. K. Parks, and M. L. Goldstein would like to acknowledge the support of NASA headquarters to the Cluster mission. A. F. Vinas, D. E. Wendell, K.-J. Hwang, and MLG also acknowledge support from the MMS Interdisciplinary Science Team at the Goddard Space Flight Center for its support. J. M. Weygand was supported, in part, by NSF grant AGS-1155841, and S. Servidio acknowledges support by the project POR Calabria FSE 2007/2013 and the Marie Curie Project FP7 PIRSES-2010-269297 'Turboplasmas'. NR 377 TC 6 Z9 6 U1 4 U2 16 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-3778 EI 1469-7807 J9 J PLASMA PHYS JI J. Plasma Phys. PD JUN PY 2015 VL 81 AR UNSP 325810301 DI 10.1017/S0022377815000185 PN 3 PG 74 WC Physics, Fluids & Plasmas SC Physics GA CH8MS UT WOS:000354291100021 ER PT J AU Schneider, VI Healy, AF Barshi, I Bourne, LE AF Schneider, Vivian I. Healy, Alice F. Barshi, Immanuel Bourne, Lyle E., Jr. TI Effects of difficulty, specificity, and variability on training to follow navigation instructions SO PSYCHONOMIC BULLETIN & REVIEW LA English DT Article DE Transfer and retention; Cognitive training; Human memory and learning ID RETENTION AB To study the relative merits of three training principles - difficulty of training, specificity of training, and variability of training - subjects were trained to follow navigation instructions to move in a grid on a computer screen. Subjects repeated and then followed the instructions by mouse clicking on the grid. They were trained, given a short distractor task, and then tested. There were three groups, each receiving different message lengths during training: easy (short lengths), hard (long lengths), and mixed (all lengths), with all subjects given all lengths at test. At test, the mixed group was best on most lengths, the easy group was better than the hard group on short lengths, and the hard group was better than the easy group on long lengths. The results support the advantages of both specificity and variability of training but do not support the hypothesis that difficult training of the form used here would lead to overall best performance at test. C1 [Schneider, Vivian I.; Healy, Alice F.; Bourne, Lyle E., Jr.] Univ Colorado, Dept Psychol & Neurosci, Boulder, CO 80309 USA. [Barshi, Immanuel] NASA, Human Syst Integrat Div, Ames Res Ctr, Moffett Field, CA USA. RP Schneider, VI (reprint author), Univ Colorado, Dept Psychol & Neurosci, Muenzinger Bldg,345 UCB, Boulder, CO 80309 USA. EM vivian.schneider@colorado.edu FU National Aeronautics and Space Administration [NNA07CN59A, NNX10AC87A, NNX14AB75A]; Army Research Institute [DASW01-03-K-0002]; Army Research Office [W911NF-05-1-0153] FX This research was supported in part by National Aeronautics and Space Administration Grants NNA07CN59A, NNX10AC87A, and NNX14AB75A; Army Research Institute Contract DASW01-03-K-0002; and Army Research Office Grant W911NF-05-1-0153 to the University of Colorado. A preliminary version of this experiment was reported at the 2007 meeting of the Psychonomic Society, Long Beach, California, USA. Special thanks are due to James A. Kole for insightful comments leading to the design of this experiment and to Henry L. Roediger III and Mark Steyvers for thoughtful suggestions concerning an earlier version of this manuscript. NR 25 TC 0 Z9 0 U1 1 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1069-9384 EI 1531-5320 J9 PSYCHON B REV JI Psychon. Bull. Rev. PD JUN PY 2015 VL 22 IS 3 BP 856 EP 862 DI 10.3758/s13423-014-0715-1 PG 7 WC Psychology, Mathematical; Psychology, Experimental SC Psychology GA CH7FA UT WOS:000354199800029 PM 25128209 ER PT J AU Pernice, MF De Carvalho, NV Ratcliffe, JG Hallett, SR AF Pernice, Maria Francesca De Carvalho, Nelson V. Ratcliffe, James G. Hallett, Stephen R. TI Experimental study on delamination migration in composite laminates SO COMPOSITES PART A-APPLIED SCIENCE AND MANUFACTURING LA English DT Article DE Delamination; Transverse cracking; Mechanical testing; Finite element analysis (FEA) ID SUBSEQUENT MIGRATION; FRACTURE-TOUGHNESS; INTERFACE; CRACK; GROWTH; SPECIMENS; DCB AB The transition of delamination growth between different ply interfaces in composite tape laminates, known as migration, was investigated experimentally. The test method used promotes delamination growth initially along a 0/theta ply interface, which eventually migrates to a neighbouring theta/0 ply interface. Specimens with theta = 60 degrees and 75 degrees were tested. Migration occurs in two main stages: (1) the initial 0/theta interface delamination turns, transforming into intraply cracks that grow through the theta plies; this process occurs at multiple locations across the width of a specimen, (2) one or more of these cracks growing through the theta plies reaches and turns into the theta/0 ply interface, where it continues to grow as a delamination. A correlation was established between these experimental observations and the shear stress sign at the delamination front, obtained by finite element analyses. Overall, the experiments provide insight into the key mechanisms that govern delamination growth and migration. (C) 2015 The Authors. Published by Elsevier Ltd. This is an open access article under the CC BY license (http://creativecommons.org/licenses/by/4.0/). C1 [Pernice, Maria Francesca; Hallett, Stephen R.] Univ Bristol, ACCIS, Bristol BS8 1TR, Avon, England. [De Carvalho, Nelson V.] NASA, Langley Res Ctr, Natl Inst Aerosp, Resident Durabil Damage Tolerance & Reliabil Bran, Hampton, VA 23681 USA. [Ratcliffe, James G.] NASA, Langley Res Ctr, Durabil Damage Tolerance & Reliabil Branch, Hampton, VA 23681 USA. RP Pernice, MF (reprint author), Univ Bristol, ACCIS, Bristol BS8 1TR, Avon, England. EM aemfp@my.bristol.ac.uk RI Hallett, Stephen/D-2573-2011; OI Hallett, Stephen/0000-0003-0751-8323; Pernice, Maria Francesca/0000-0002-1945-8834 FU National Aeronautics and Space Administration (NASA), Langley Research Center, United States [NNL09AA00A]; Engineering and Physical Sciences Research Council (EPSRC), United Kingdom, through the Centre for Doctoral Training in Advanced Composites [EP/G036772/1] FX This material is based on work supported by the National Aeronautics and Space Administration (NASA), Langley Research Center, United States, under Research Cooperative Agreement No. NNL09AA00A. The first author is supported by the Engineering and Physical Sciences Research Council (EPSRC), United Kingdom, through the Centre for Doctoral Training in Advanced Composites [grant number EP/G036772/1]. Special thanks to Drs. T.K. O'Brien, J. Reeder, M. Czabaj and W. Jackson of NASA and Prof P. Weaver of ACCIS, for the invaluable technical discussions. NR 33 TC 5 Z9 5 U1 0 U2 9 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1359-835X EI 1878-5840 J9 COMPOS PART A-APPL S JI Compos. Pt. A-Appl. Sci. Manuf. PD JUN PY 2015 VL 73 BP 20 EP 34 DI 10.1016/j.compositesa.2015.02.018 PG 15 WC Engineering, Manufacturing; Materials Science, Composites SC Engineering; Materials Science GA CH0SQ UT WOS:000353733100003 ER PT J AU Hartwig, JW Darr, SR McQuillen, JB Rame, E Chato, DJ AF Hartwig, J. W. Darr, S. R. McQuillen, J. B. Rame, E. Chato, D. J. TI A steady state pressure drop model for screen channel liquid acquisition devices (vol 64, pg 260, 2014) SO CRYOGENICS LA English DT Correction C1 [Hartwig, J. W.; Chato, D. J.] Glenn Res Ctr, Prop & Propellants Branch, Cleveland, OH USA. [Darr, S. R.] Univ Florida, Gainesville, FL 32611 USA. [McQuillen, J. B.] Glenn Res Ctr, Fluid Phys & Transport Branch, Cleveland, OH USA. [Rame, E.] Glenn Res Ctr, Natl Ctr Micrograv Res, Cleveland, OH USA. RP Hartwig, JW (reprint author), NASA, Glenn Res Ctr, M-S 301-3, Cleveland, OH 44135 USA. EM Jason.W.Hartwig@nasa.gov RI Chato, David/B-2698-2013 OI Chato, David/0000-0003-2990-0646 NR 1 TC 0 Z9 0 U1 0 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0011-2275 EI 1879-2235 J9 CRYOGENICS JI Cryogenics PD JUN PY 2015 VL 68 BP 67 EP 67 DI 10.1016/j.cryogenics.2015.04.001 PG 1 WC Thermodynamics; Physics, Applied SC Thermodynamics; Physics GA CH0YB UT WOS:000353747200007 ER PT J AU Quick, LC Marsh, BD AF Quick, Lynnae C. Marsh, Bruce D. TI Constraining the thickness of Europa's water-ice shell: Insights from tidal dissipation and conductive cooling SO ICARUS LA English DT Article DE Europa; Geophysics; Interiors; Tides, solid body; Jupiter, satellites ID ART. NO. 1233; GALILEAN SATELLITES; SUBSURFACE OCEAN; LIQUID-WATER; GEOLOGICAL EVIDENCE; INTERIOR STRUCTURE; INTERNAL STRUCTURE; THERMAL EVOLUTION; CHAOTIC TERRAIN; SOUTH-POLE AB The time of crystallization of a 100 km thick ocean on Europa is estimated using a Stefan-style solidification solution. This solution is then extended to estimate the present thickness of the ice shell. It is assumed that the shell is initially in a steady-state conductive regime, and the ocean is taken to be an infinite liquid half space cooling from above. We find that in the absence of tidal heating and without the presence of low-eutectic impurities to serve as anti-freezes, a 100 km thick ocean solidifies in about 64 Myr. Conversely, when considering the present thickness of Europa's ice shell, if tidal heating is included at a global dissipation rate of similar to 1 TW, the shell is found to be, on average, approximately 28 km thick. However, if this dissipative heating is solely restricted to the shell, the local rate of heating may vary significantly due to crustal compositional heterogeneities and it is shown that this process may, in turn, produce thermal maxima in the crust, which could lead to local melting and structural instabilities, perhaps associated with the formation of chaos regions. Our approach is also extended to Ganymede and Callisto in order to estimate the time of solidification of their putative subsurface oceans and the current thicknesses of their ice-I shells. (C) 2015 Elsevier Inc. All rights reserved. C1 [Quick, Lynnae C.] Johns Hopkins Univ, Earth & Planetary Sci Dept, Baltimore, MD 21218 USA. [Quick, Lynnae C.; Marsh, Bruce D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Quick, LC (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab Code 698, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM lynnae.c.quick@nasa.gov FU Johns Hopkins University Bromery Fellowship; Johns Hopkins University Applied Physics Laboratory Graduate Student Fellowship FX L.C.Q. gratefully acknowledges funding from the Johns Hopkins University Bromery Fellowship and the Johns Hopkins University Applied Physics Laboratory Graduate Student Fellowship. The authors wish to thank Dr. Amy Barr and Dr. Julie Rathbun for helpful suggestions that improved the quality of this manuscript. We also thank Dr. James Roberts for helpful discussions. NR 70 TC 2 Z9 2 U1 6 U2 25 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUN PY 2015 VL 253 BP 16 EP 24 DI 10.1016/j.icarus.2015.02.016 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH1BD UT WOS:000353755200002 ER PT J AU Dohm, JM Hare, TM Robbins, SJ Williams, JP Soare, RJ El-Maarry, MR Conway, SJ Buczkowski, DL Kargel, JS Banks, ME Fairen, AG Schulze-Makuch, D Komatsu, G Miyamoto, H Anderson, RC Davila, AF Mahaney, WC Fink, W Cleaves, KJ Yan, J Hynek, B Maruyama, S AF Dohm, J. M. Hare, T. M. Robbins, S. J. Williams, J. -P. Soare, R. J. El-Maarry, M. R. Conway, S. J. Buczkowski, D. L. Kargel, J. S. Banks, M. E. Fairen, A. G. Schulze-Makuch, D. Komatsu, G. Miyamoto, H. Anderson, R. C. Davila, A. F. Mahaney, W. C. Fink, W. Cleaves, K. J. Yan, J. Hynek, B. Maruyama, S. TI Geological and hydrological histories of the Argyre province, Mars SO ICARUS LA English DT Article DE Mars; Geological processes; Astrobiology; Tectonics ID SURFACE GROUND ICE; MAGNETIC-FIELD; ANTARCTIC PALEOSOLS; VALLES MARINERIS; NORTHERN PLAINS; CLIMATE-CHANGE; SLOPE STREAKS; IMPACT BASIN; EVOLUTION; SYSTEM AB The geologic history of the multi-ringed Argyre impact basin and surroundings has been reconstructed on the basis of geologic mapping and relative-age dating of rock materials and structures. The impact formed a primary basin, rim materials, and a complex basement structural fabric including faults and valleys that are radial and concentric about the primary basin, as well as structurally-controlled local basins. Since its formation, the basin has been a regional catchment for volatiles and sedimentary materials as well as a dominant influence on the flow of surface ice, debris flows, and groundwater through and over its basement structures. The basin is interpreted to have been occupied by lakes, including a possible Mediterranean-sized sea that formed in the aftermath of the Argyre impact event The hypothesized lakes froze and diminished through time, though liquid water may have remained beneath the ice cover and sedimentation may have continued for some time. At its deepest, the main Argyre lake may have taken more than a hundred thousand years to freeze to the bottom even absent any heat source besides the Sun, but with impact-induced hydrothermal heat, geothermal heat flow due to long-lived radioactivities in early martian history, and concentration of solutes in sub-ice brine, liquid water may have persisted beneath thick ice for many millions of years. Existence of an ice-covered sea perhaps was long enough for life to originate and evolve with gradually colder and more hypersaline conditions. The Argyre rock materials, diverse in origin and emplacement mechanisms, have been modified by impact, magmatic, eolian, fluvial, lacustrine, glacial, periglacial, alluvial, colluvial, and tectonic processes. Post-impact adjustment of part of the impact-generated basement structural fabric such as concentric faults is apparent. Distinct basin-stratigraphic units are interpreted to be linked to large-scale geologic activity far from the basin, including growth of the Tharsis magmatic-tectonic complex and the growth into southern middle latitudes of south polar ice sheets. Along with the migration of surface and sub-surface volatiles towards the central part of the primaiy basin, the substantial difference in elevation with respect to the surrounding highlands and Tharsis and the Thaumasia highlands result in the trapping of atmospheric volatiles within the basin in the form of fog and regional or local precipitation, even today. In addition, the impact event caused long-term (millions of years) hydrothermal activity, as well as deep-seated basement structures that have tapped the internal heat of Mars, as conduits, for far greater time, possibly even today. This possibility is raised by the observation of putative open-system pingos and nearby gullies that occur in linear depressions with accompanying systems of faults and fractures. Long-term water and heat energy enrichment, complemented by the interaction of the nutrient-enriched primordial crustal and mantle materials favorable to life excavated to the surface and near-surface environs through the Argyre impact event, has not only resulted in distinct geomorphology, but also makes the Argyre basin a potential site of exceptional astrobiological significance. (C) 2015 Elsevier Inc. All rights reserved. C1 [Dohm, J. M.; Miyamoto, H.] Univ Tokyo, Univ Museum, Bunkyo Ku, Tokyo 1130033, Japan. [Hare, T. M.] US Geol Survey, Flagstaff, AZ 86001 USA. [Robbins, S. J.] SW Res Inst, Boulder, CO 80302 USA. [Williams, J. -P.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. [Soare, R. J.] Dawson Coll, Dept Geog, Montreal, PQ H3Z 1A4, Canada. [El-Maarry, M. R.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Conway, S. J.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Buczkowski, D. L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Kargel, J. S.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. [Banks, M. E.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Banks, M. E.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Fairen, A. G.] Ctr Astrobiol, Dept Planetol & Habitabil, Madrid 28850, Spain. [Fairen, A. G.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Schulze-Makuch, D.] Tech Univ Berlin, Ctr Astron & Astrophys, D-10623 Berlin, Germany. [Komatsu, G.] Univ Annunzio, Int Res Sch Planetary Sci, I-65421 Pescara, Italy. [Anderson, R. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Davila, A. F.] SETI Inst, Mountain View, CA 94043 USA. [Mahaney, W. C.] Quaternary Surveys, Thornhill, ON L4J 1J4, Canada. [Fink, W.] Univ Arizona, Dept Elect & Comp Engn, Coll Engn, Tucson, AZ 85721 USA. [Cleaves, K. J.; Maruyama, S.] Tokyo Inst Technol, Earth Life Sci Inst, Tokyo 1528551, Japan. [Cleaves, K. J.] Inst Adv Study, Princeton, NJ 08540 USA. [Yan, J.] Natl Astron Observ Japan, RISE Project Off, Oshu 0230861, Japan. [Hynek, B.] Univ Colorado, Lab Atmospher & Space Phys & Geol Sci, Boulder, CO 80309 USA. RP Dohm, JM (reprint author), Univ Tokyo, Univ Museum, Bunkyo Ku, Hongo 7-3-1, Tokyo 1130033, Japan. EM jmd@um.u-tokyo.ac.jp RI Williams, Jean-Pierre/C-3531-2009; Komatsu, Goro/I-7822-2012; Miyamoto, Hideaki/B-9666-2008; Maruyama, Shigenori/C-8288-2009; OI Williams, Jean-Pierre/0000-0003-4163-2760; Komatsu, Goro/0000-0003-4155-108X; Conway, Susan/0000-0002-0577-2312; EL-MAARRY, MOHAMED RAMY/0000-0002-8262-0320; Hare, Trent/0000-0001-8842-389X; Schulze-Makuch, Dirk/0000-0002-1923-9746; Cleaves, Henderson/0000-0003-4101-0654 FU National Aeronautics and Space Administration (NASA) Planetary Geology & Geophysics Program; Tokyo Dome Corporation; European Research Council under the European Union's Seventh Framework Programme (FP7), ERC [307496] FX J.M. Dohm was supported by the National Aeronautics and Space Administration (NASA) Planetary Geology & Geophysics Program. Professors Dohm and Miyamoto express their gratitude to the Tokyo Dome Corporation for their support of the TeNQ exhibit and the branch of Space Exploration Education & Discovery, the University Museum, the University of Tokyo. Work by A.G. Fairen was supported by the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013), ERC Grant agreement No. 307496. We are grateful for the thoughtful reviews by T. Ohman and an anonymous reviewer which ultimately resulted in an improved manuscript. NR 195 TC 9 Z9 9 U1 3 U2 42 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 JUN PY 2015 VL 253 BP 66 EP 98 DI 10.1016/j.icarus.2015.02.017 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH1BD UT WOS:000353755200007 ER PT J AU Khayat, AS Villanueva, GL Mumma, MJ Tokunaga, AT AF Khayat, A. S. Villanueva, G. L. Mumma, M. J. Tokunaga, A. T. TI A search for SO2, H2S and SO above Tharsis and Syrtis volcanic districts on Mars using ground-based high-resolution submillimeter spectroscopy SO ICARUS LA English DT Article DE Mars, atmosphere; Abundances, atmospheres; Atmospheres, structure; Radiative transfer; Volcanism ID MARTIAN ATMOSPHERE; ROTATIONAL TRANSITIONS; METHANE; DETECTABILITY; SPECTROMETER; MILLIMETER; PLANETARY; EMISSION; DATABASE; SURFACE AB We surveyed the Tharsis and Syrtis volcanic regions on Mars during 23 November 2011 to 13 May 2012 which correspOnded to its mid Northern Spring and early Northern Summer seasons (L-s = 34-110 degrees). Strong submillimeter rotational transitions of sulfur dioxide (SO2), sulfur monoxide (SO) and hydrogen sulfide (H2S) were targeted. No active release was detected, and we infer 2 sigma upper limits across the disk of the planet of 1.1 ppb, 0.7 ppb and 1.3 ppb for SO2, SO and H2S, respectively. Our derived upper limit for SO2 is comparable to previously reported limits, whereas for H2S we set a more stringent upper limit than previously measured, and we establish a limit for SO. Among the targeted molecules, SO2 is the strongest indicator for volcanic outgassing. Assuming a photochemical lifetime of 2 years for SO2, our upper limit of 1.1 ppb implies an outgassing rate less than 55 metric tons/day. This rate limits the daily amount of degassing magma to less than 12,000 m(3). Our sensitivity is sufficient to detect a volcanic release on Mars that is 4% the SO2 released continuously from Kilauea volcano in Hawaii or 5% that of the Masaya volcano in Nicaragua. The non-detection of the sulfur compounds in the atmosphere of Mars indicates the absence of major volcanic outgassing. Published by Elsevier Inc. C1 [Khayat, A. S.; Tokunaga, A. T.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Villanueva, G. L.; Mumma, M. J.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Villanueva, G. L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Khayat, AS (reprint author), Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. EM Khayat@ifa.hawaii.edu FU National Science Foundation [AST-0838261]; NASA Planetary Astronomy Program [NNX08AE38A]; NASA [NNH14CK55B]; RTOP [344-32-07]; NASA's Astrobiology Program [RTOP 344-53-51] FX We are grateful to the staff at the Caltech Submillimeter Observatory (CSO), Simon Radford, Timm Riesen and Louis Scuderi for their support during the Mars observing runs. This material is based upon work at the CSO, which is operated by the California Institute of Technology under cooperative agreement with the National Science Foundation, Grant No. AST-0838261. We gratefully acknowledge the support from the NASA Planetary Astronomy Program under Cooperative Agreement NNX08AE38A, NASA contract NNH14CK55B, RTOP 344-32-07 and NASA's Astrobiology Program (RTOP 344-53-51) that supported M.J.M., and G.L.V. A.J.K. would like to thank Norbert Schorghofer who provided valuable ideas to the writing and undertaking of the research summarized here. 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 56 TC 5 Z9 5 U1 0 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUN PY 2015 VL 253 BP 130 EP 141 DI 10.1016/j.icarus.2015.02.028 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH1BD UT WOS:000353755200010 ER PT J AU Rhoden, AR Hurford, TA Roth, L Retherford, K AF Rhoden, Alyssa Rose Hurford, Terry A. Roth, Lorenz Retherford, Kurt TI Linking Europa's plume activity to tides, tectonics, and liquid water SO ICARUS LA English DT Article DE Europa; Tectonics; Jupiter, satellites; Satellites, surfaces ID NONSYNCHRONOUS ROTATION; TIDAL STRESSES; SOUTH-POLE; ENCELADUS; FRACTURES; OBLIQUITY; EARTH; OSCILLATIONS; SATELLITES; ATMOSPHERE AB Much of the geologic activity preserved on Europa's icy surface has been attributed to tidal deformation, mainly due to Europa's eccentric orbit. Although the surface is geologically young (30-80 Myr), there is little information as to whether tidally-driven surface processes are ongoing. However, a recent detection of water vapor near Europa's south pole suggests that it may be geologically active. Initial observations indicated that Europa's plume eruptions are time-variable and may be linked to its tidal cycle. Saturn's moon, Enceladus, which shares many similar traits with Europa, displays tidally-modulated plume eruptions, which bolstered this interpretation. However, additional observations of Europa at the same time in its orbit failed to yield a plume detection, casting doubt on the tidal control hypothesis. The purpose of this study is to analyze the timing of plume eruptions within the context of Europa's tidal cycle to determine whether such a link exists and examine the inferred similarities and differences between plume activity on Europa and Enceladus. To do this, we determine the locations and orientations of hypothetical tidally-driven fractures that best match the temporal variability of the plumes observed at Europa. Specifically, we identify model faults that are in tension at the time in Europa's orbit when a plume was detected and in compression at times when the plume was not detected. We find that tidal stress driven solely by eccentricity is incompatible with the observations unless additional mechanisms are controlling the eruption timing or restricting the longevity of the plumes. The addition of obliquity tides, and corresponding precession of the spin pole, can generate a number of model faults that are consistent with the pattern of plume detections. The locations and orientations of these hypothetical source fractures are robust across a broad range of precession rates and spin pole directions. Analysis of the stress variations across the fractures suggests that the plumes would be best observed earlier in the orbit (true anomaly similar to 120 degrees). Our results indicate that Europa's plumes, if confirmed, differ in many respects from the Enceladean plumes and that either active fractures or volatile sources are rare. (C) 2015 Elsevier Inc. All rights reserved. C1 [Rhoden, Alyssa Rose; Hurford, Terry A.] NASA, Goddard Space Flight Ctr, Code 693, Greenbelt, MD 20771 USA. [Rhoden, Alyssa Rose] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Roth, Lorenz; Retherford, Kurt] SW Res Inst, San Antonio, TX 78238 USA. [Roth, Lorenz] Royal Inst Technol, Sch Elect Engn, Stockholm, Sweden. RP Rhoden, AR (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. EM Alyssa.Rhoden@jhuapl.edu RI Hurford, Terry/F-2625-2012 FU NASA through Space Telescope Science Institute [13619]; NASA [NAS5-26555] FX The authors would like to thank G. Collins and P. Geissler for thoughtful reviews that improved this manuscript. A. Rhoden was partially supported through an appointment to the NASA Postdoctoral Program, administered by ORAU. L. Roth and K. Retherford were supported through HST Program number 13619 provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. NR 48 TC 2 Z9 2 U1 9 U2 25 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUN PY 2015 VL 253 BP 169 EP 178 DI 10.1016/j.icarus.2015.02.023 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH1BD UT WOS:000353755200015 ER PT J AU Deau, E AF Deau, Estelle TI The opposition effect in Saturn's main rings as seen by Cassini ISS: 2. Constraints on the ring particles and their regolith with analytical radiative transfer models SO ICARUS LA English DT Article DE Planetary rings; Saturn, rings; Photometry ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; DENSE PLANETARY RINGS; SELF-GRAVITY WAKES; THEORETICAL PHOTOMETRIC FUNCTION; HEAD-ON COLLISIONS; COHERENT BACKSCATTERING; B-RING; STELLAR OCCULTATION; LIGHT-SCATTERING; NUMERICAL-SIMULATION AB The opposition effect in Saturn's main rings is characterized by a surge in ring brightness, when the phase angle approaches zero degree. This effect can be used to derive: physical properties of the ring particles and the ring layer, via the shadow hiding mechanism; and physical properties of the regolith grains that cover the ring particles, via the coherent backscattering mechanism. Since the exact origin of this effect is still a matter of debate, we try different combinations of the physical mechanisms cited above to derive constraints on the nature, the texture, and the disposition of the ring particles. In particular, we derive regolith grain sizes, particle sizes, differential power law indices, filling factors, and vertical thicknesses; and we compare them with independent works to validate or invalidate the assumptions of the opposition effect models used. Our coherent backscattering model provides grain sizes similar to the sizes estimated from water ice band depth modeling in the near infrared. Our shadow hiding model assuming a power law size distribution provides vertical thickness consistent with previous estimates from density waves measurements and N-body simulations. We show that the assumption of an homogeneous medium is a key parameter in the shadow hiding modeling. In the case of the B ring, we demonstrate that all previous photometric models assuming an homogeneous ring layer (i.e. uniform particle size distribution, random spacing of the particles and small filling factor) have led to a set of unconfirmed solutions. This result reinforces the idea that the Saturn's main rings should be modeled as an heterogeneous medium. (C) 2013 Elsevier Inc. All rights reserved. C1 [Deau, Estelle] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. [Deau, Estelle] CEA Saclay, IRFU, Serv Astrophys, Lab AIM,UMR 7158, F-91191 Gif Sur Yvette, France. RP Deau, E (reprint author), NASA, Jet Prop Lab, 4800 Oak Grove Dr,M-S 230-207G, Pasadena, CA 91109 USA. EM Estelle.Deau@jpl.nasa.gov FU Conseil Regional de la Martinique; CNES (Centre National d'Etudes Spatiales); CNRS (Centre National de la Recherche Scientifique); Postdoctoral Program of NASA [09-CDAP09-0033] FX This study was originally performed at CEA Saclay, and was initially funded by the Conseil Regional de la Martinique, from E. Deau's funding; the CNES (Centre National d'Etudes Spatiales), and the CNRS (Centre National de la Recherche Scientifique), from A. Brahic's funding. A part of this study was performed at JPL (Jet Propulsion Laboratory), under contract with NASA (National Aeronautics and Space Administration) and California Institute of Technology, and was funded by the Postdoctoral Program of NASA, led by ORAU (OakRidge Associated Universities), and the Cassini Project (09-CDAP09-0033). Government sponsorships acknowledged. NR 190 TC 3 Z9 3 U1 0 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 JUN PY 2015 VL 253 BP 311 EP 345 DI 10.1016/j.icarus.2013.08.031 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH1BD UT WOS:000353755200024 ER PT J AU Reese, DC Brodeur, RD AF Reese, Douglas C. Brodeur, Richard D. TI Species associations and redundancy in relation to biological hotspots within the northern California Current ecosystem SO JOURNAL OF MARINE SYSTEMS LA English DT Article DE Hotspots; Community composition; Species associations; Redundancy; Ecosystem resilience; Nekton; Jellyfish; California Current ID OCEANOGRAPHIC CONDITIONS; COMMUNITY STRUCTURE; SPATIAL OVERLAP; CLIMATE-CHANGE; OCEAN; PACIFIC; ZOOPLANKTON; IMPACTS; OREGON; FISH AB The dynamic nature of biological hotspots, while well recognized, is not well understood. We hypothesize that the persistence of hotspots in the northern California Current System (CCS), despite seasonal and annual changes in the nekton community species composition, is related to associations among species and their functional redundancy. To address this hypothesis, sampling was conducted during June and August of 2000 and 2002 within two hotspots occurring between Newport, Oregon and Crescent City, California in the coastal CCS. Associations were examined to identify potentially complementary and redundant species. The strongest negative associations were between jellyfish and fish species, with strong positive associations evident among several fish species. Dominant species varied seasonally and annually, although evidence indicated replacement of dominant species by other similar species with respect to functional group and preferred habitat. This finding suggests that the persistence of these biological hotspots is related to species redundancy and is an important attribute contributing to stability within this highly variable system. (C) 2014 Elsevier B.V. All rights reserved. C1 [Reese, Douglas C.] Oregon State Univ, Dept Fisheries & Wildlife, Corvallis, OR 97331 USA. [Brodeur, Richard D.] Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Fish Ecol Div, Newport, OR 97365 USA. RP Reese, DC (reprint author), Oregon State Univ, Dept Fisheries & Wildlife, 104 Nash Hall, Corvallis, OR 97331 USA. EM Doug.Reese@oregonstate.edu FU U.S. GLOBEC Northeast Pacific Program FX We thank the crew and scientists who assisted in the collection of samples at sea, especially B. Emmett, J. Fisher, and T. Miller. T. Miller was especially helpful in providing the information from diet analyses used in the classification of species by functional group. We also thank B. Pearcy, B. McCune, D. Ainley, and two anonymous reviewers for providing valuable comments on the manuscript. Funding for this study was provided by the U.S. GLOBEC Northeast Pacific Program. NR 56 TC 4 Z9 4 U1 2 U2 14 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 JUN PY 2015 VL 146 SI SI BP 3 EP 16 DI 10.1016/j.jmarsys.2014.10.009 PG 14 WC Geosciences, Multidisciplinary; Marine & Freshwater Biology; Oceanography SC Geology; Marine & Freshwater Biology; Oceanography GA CG8ZP UT WOS:000353604500002 ER PT J AU Kaynak, Y Karaca, HE Noebe, RD Jawahir, IS AF Kaynak, Yusuf Karaca, Haluk E. Noebe, Ronald D. Jawahir, I. S. TI The Effect of Active Phase of the Work Material on Machining Performance of a NiTi Shape Memory Alloy SO METALLURGICAL AND MATERIALS TRANSACTIONS A-PHYSICAL METALLURGY AND MATERIALS SCIENCE LA English DT Article; Proceedings Paper CT Bulk Metallic Glasses 11 Symposium CY FEB 16-20, 2014 CL TMS Annual Meeting & Exhibit, San Diego, CA SP Bulk Met Glasses Symposia HO TMS Annual Meeting & Exhibit ID TOOL-WEAR; TI-6AL-4V; TRANSFORMATION; EVOLUTION; TITANIUM AB Poor machinability with conventional machining processes is a major shortcoming that limits the manufacture of NiTi components. To better understand the effects of phase state on the machining performance of NiTi alloys, cutting temperature, tool-wear behavior, cutting force components, tool-chip contact length, chip thickness, and machined surface quality data were generated from a NiTi alloy using precooled cryogenic, dry, minimum quantity lubrication (MQL), and preheated machining conditions. Findings reveal that machining NiTi in the martensite phase, which was achieved through precooled cryogenic machining, profoundly improved the machining performance by reducing cutting force components, notch wear, and surface roughness. Machining in the austenite state, achieved through preheating, did not provide any benefit over dry and MQL machining, and these processes were, in general, inferior to cryogenic machining in terms of machining performance, particularly at higher cutting speeds. C1 [Kaynak, Yusuf] Marmara Univ, Fac Technol, Dept Mech Engn, TR-34722 Istanbul, Turkey. [Karaca, Haluk E.; Jawahir, I. S.] Univ Kentucky, Coll Engn, Dept Mech Engn, Lexington, KY 40506 USA. [Noebe, Ronald D.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. [Jawahir, I. S.] Univ Kentucky, ISM, Lexington, KY 40506 USA. EM yusuf.kaynak@marmara.edu.tr FU NASA EPSCOR Program [NNX11AQ31A]; NASA FAP Aeronautical Sciences; TACP Transformational Tools & Technologies Projects (Dale Hopkins, Technical Lead) FX Support from the NASA EPSCOR Program under Grant No. NNX11AQ31A and the NASA FAP Aeronautical Sciences and TACP Transformational Tools & Technologies Projects (Dale Hopkins, Technical Lead) are gratefully acknowledged. NR 29 TC 4 Z9 4 U1 2 U2 8 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1073-5623 EI 1543-1940 J9 METALL MATER TRANS A JI Metall. Mater. Trans. A-Phys. Metall. Mater. Sci. PD JUN PY 2015 VL 46A IS 6 BP 2625 EP 2636 DI 10.1007/s11661-015-2828-1 PG 12 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA CG4EQ UT WOS:000353236700034 ER PT J AU Pollak, L Mehta, SK Pierson, DL Sacagiu, T Kalmanovich, SA Cohrs, RJ AF Pollak, L. Mehta, S. K. Pierson, D. L. Sacagiu, T. Kalmanovich, S. Avneri Cohrs, R. J. TI Varicella-zoster DNA in saliva of patients with meningoencephalitis: a preliminary study SO ACTA NEUROLOGICA SCANDINAVICA LA English DT Article DE varicella zoster; meningoencephalitis; saliva ID HERPES-SIMPLEX-VIRUS; RELIABLE DETECTION; CLINICAL-FEATURES; ORAL FLUID; REACTIVATION; INFECTIONS; DISEASE; PRESENTATIONS; COMPLICATIONS; ENCEPHALITIS AB ObjectivesSince the routine use of polymerase chain reaction testing (PCR) in diagnosing herpes infections, varicella-zoster virus is increasingly recognized as a cause of varicella-zoster meningoencephalitis (VZV ME) among immunocompetent patients. We were interested to determine whether patients with VZV ME had VZV DNA in their saliva during the acute phase of the illness. Materials and methodsForty-five consecutive patients who underwent a lumbar puncture for diagnostic purposes were included in the study. The cerebrospinal fluid was examined for the presence of VZV DNA by PCR, and patients with positive findings were treated with acyclovir. The saliva was later analyzed in a blinded fashion for the presence of VZV DNA. ResultsVZV DNA was found in saliva in four of five (80%) patients with PCR confirmed VZV ME (sensitivity 0.8, specificity 0.84, and likelihood ratio 5). This was significantly more than in patients with non-zoster viral ME (0%, P=0.009), parainfectious headache (12%, P=0.03) and controls (9.5%, P=0.007). In immunocompromised patients with systemic lymphoma and AIDS, VZV DNA was present at a similar rate (67%, P=0.6). ConclusionsWe have found VZV DNA in saliva of patients with PCR confirmed VZV ME at a higher proportion than in controls and patients with non-VZV viral ME. This finding might be of clinical importance, especially in immunocompetent individuals with suspected VZV ME where the results of genetic and immunological testing are not conclusive. C1 [Pollak, L.; Sacagiu, T.; Kalmanovich, S. Avneri] Tel Aviv Univ, Sackler Fac Med, Assaf Harofeh Med Ctr, Dept Neurol, Zerifin, Israel. [Mehta, S. K.; Pierson, D. L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Cohrs, R. J.] Univ Colorado, Sch Med, Dept Neurol, Aurora, CO USA. [Cohrs, R. J.] Univ Colorado, Sch Med, Dept Microbiol, Aurora, CO USA. RP Pollak, L (reprint author), Kibutz Galuyot 4, IL-74012 Ness Ziona, Israel. EM lea.pollak@gmail.com NR 23 TC 0 Z9 0 U1 1 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0001-6314 EI 1600-0404 J9 ACTA NEUROL SCAND JI Acta Neurol. Scand. PD JUN PY 2015 VL 131 IS 6 BP 417 EP 421 DI 10.1111/ane.12335 PG 5 WC Clinical Neurology SC Neurosciences & Neurology GA CF4NH UT WOS:000352525500011 PM 25314141 ER PT J AU Sen Gupta, A Tarboton, DG Hummel, P Brown, ME Habib, S AF Sen Gupta, A. Tarboton, D. G. Hummel, P. Brown, M. E. Habib, S. TI Integration of an energy balance snowmelt model into an open source modeling framework SO ENVIRONMENTAL MODELLING & SOFTWARE LA English DT Article DE Model integration; Data model; Energy balance; Snow melt; Glacier melt ID SURFACE-TEMPERATURE; INTERFACE; SYSTEM; COVER; PRECIPITATION; SIMULATIONS; PREDICTION; DESIGN; NETCDF; MODIS AB This paper presents a data model for organizing the inputs and outputs of an energy balance snowmelt model (the Utah Energy Balance Model, UEB) that provides a foundation for its integration into the EPA BASINS modeling framework and enables its coupling with other hydrologic models in this system. Having UEB as a BASINS component has facilitated its coupling with the Geospatial Streamflow Forecast Model (GeoSFM) to compute the melting of glaciers and subsequent streamflow in the Himalayas. The data model uses a combination of structured text and network Common Data Form (netCDF) files to represent parameters, geographical, time series, and gridded space-time data. We describe the design and structure of this data model, integration methodology of UEB and GeoSFM and illustrate the effectiveness of the resulting coupled models for the computation of surface water input and streamflow for a glaciated watershed in Nepal Himalayas. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Sen Gupta, A.; Tarboton, D. G.] Utah State Univ, Dept Civil & Environm Engn, Logan, UT 84322 USA. [Hummel, P.] AQUA TERRA Consultants, Decatur, GA USA. [Brown, M. E.; Habib, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sen Gupta, A (reprint author), Utah State Univ, Utah Water Res Lab, Civil & Environm Engn, 4110 Old Main Hill, Logan, UT 84322 USA. EM avirup.sengupta@aggiemail.usu.edu RI Sen Gupta, Avirup/L-8938-2014; Brown, Molly/E-2724-2010; OI Sen Gupta, Avirup/0000-0001-5972-5186; Brown, Molly/0000-0001-7384-3314; Tarboton, David/0000-0002-1998-3479 FU NASA [NNX11AK036] FX This research was supported by NASA award NNX11AK036. The authors are thankful to Dr. Adina Racoviteanu from Laboratoire de Glaciologie et Geophysique de l'Environnement for providing glacier mapping and substrate albedo data for the Langtang Khola Watershed. We would also like to thank HKH Cryosphere Monitoring Project implemented by ICIMOD and ICIMOD's glacier hydrologist Dr. Joseph Michael Shea for providing monthly temperature lapse rate data for Langtang Khola watershed. NR 75 TC 1 Z9 1 U1 2 U2 21 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1364-8152 EI 1873-6726 J9 ENVIRON MODELL SOFTW JI Environ. Modell. Softw. PD JUN PY 2015 VL 68 BP 205 EP 218 DI 10.1016/j.envsoft.2015.02.017 PG 14 WC Computer Science, Interdisciplinary Applications; Engineering, Environmental; Environmental Sciences SC Computer Science; Engineering; Environmental Sciences & Ecology GA CG1ZC UT WOS:000353073700017 ER PT J AU Walsh, WA Brodziak, J AF Walsh, William A. Brodziak, Jon TI Billfish CPUE standardization in the Hawaii longline fishery: Model selection and multimodel inference SO FISHERIES RESEARCH LA English DT Article; Proceedings Paper CT 5th International Billfish Symposium CY NOV 04-08, 2013 CL Taipei, TAIWAN DE Istiophoridae; Incidental catches; CPUE standardization; Model selection; Zero-inflation; Negative binomial ID MARLIN MAKAIRA-NIGRICANS; PACIFIC-OCEAN; BLUE MARLIN; ABUNDANCE; CATCH AB This paper presents catch per unit effort (CPUE) standardizations and model selection procedures for four billfish species (Family Istiophoridae) caught primarily as bycatch in the Hawaii-based pelagic longline fishery during 1995-2011: Blue marlin Makaira nigricans; Striped marlin Kajikia audax;,Shortbill spearfish Tetrapturus angustirostris; and Sailfish Istiophorus platypterus. The first three species were analyzed on a fishery-wide basis. For sailfish, the fishery data came exclusively from tuna-targeted longline sets in the deep-set sector of the Hawaii-based fishery. We used fishery observer data from the NOAA Fisheries Pacific Islands Regional Observer Program to fit the CPUE standardization models. In this context, our objective was to investigate the quality of model fit for five types of generalized linear models (GLMs: Poisson; negative binomial; zero-inflated Poisson; zero-inflated negative binomial; delta-Gamma). Each of these models represented a different hypothesis about the capture process for a bycatch species for which the catch data primarily consisted of zero catch observations. The five GLMs were fitted by forward entry variable selection, and the best fitting GLM for each species was selected on the basis of Akaike Information Criterion values and calculated Akaike weights. The best-fitting model selected for each species was a zero-inflated negative binomial GLM (ZINB). The ZINB model was comprised of a negative binomial counts model for expected zero catch sets and a positive catch per set distribution along with a binomial inflation model to account for excess zeros. For each species, the important explanatory variables for standardizing CPUE were fishing year, fishing (i.e., calendar) quarter, and fishing region. The best-fitting models indicated that standardized CPUE for striped and blue marlins decreased significantly during the study period. Because the ZINB model was selected as the best fitting model for all species, we suggest that longline CPUE for incidentally caught billfishes is best represented as a process characterized by zero inflation and overdispersion in the positive catches and expected zero catches. We therefore recommend that ZINB models be considered as an a priori model for CPUE standardizations of billfishes and other bycatch species in longline fisheries. (C) 2014 Elsevier B.V. All rights reserved. C1 [Walsh, William A.] Univ Hawaii, Joint Inst Marine & Atmospher Res, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96818 USA. [Brodziak, Jon] Natl Marine Fisheries Serv, NOAA Fisheries, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96818 USA. RP Walsh, WA (reprint author), Univ Hawaii, Joint Inst Marine & Atmospher Res, Pacific Isl Fisheries Sci Ctr, 1845 Wasp Blvd, Honolulu, HI 96818 USA. EM William.Walsh@noaa.gov NR 29 TC 2 Z9 2 U1 4 U2 26 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 JUN PY 2015 VL 166 SI SI BP 151 EP 162 DI 10.1016/j.fishres.2014.07.015 PG 12 WC Fisheries SC Fisheries GA CG2AN UT WOS:000353077400017 ER PT J AU Sankararaman, S Mahadevanb, S AF Sankararaman, Shankar Mahadevanb, Sankaran TI Integration of model verification, validation, and calibration for uncertainty quantification in engineering systems SO RELIABILITY ENGINEERING & SYSTEM SAFETY LA English DT Article DE Multi-level system; Uncertainty quantification; Bayesian network; Calibration; Validation; Verification ID COMPUTATIONAL MODELS; ERROR ESTIMATION; EPISTEMIC UNCERTAINTY; FINITE-ELEMENTS; CODE; SIMULATION; NETWORKS; DYNAMICS; BAYES AB This paper proposes a Bayesian methodology to integrate model verification, validation, and calibration activities for the purpose of overall uncertainty quantification in different types of engineering systems. The methodology is first developed for single-level models, and then extended to systems that are studied using multi-level models that interact with each other. Two types of interactions amongst multilevel models are considered: (1) Type-I, where the output of a lower-level model (component and/or subsystem) becomes an input to a higher level system model, and (2) Type-II, where parameters of the system model are inferred using lower-level models and tests (that describe simplified components and/ or isolated physics). The various models, their inputs, parameters, and outputs, experimental data, and various sources of model error are connected through a Bayesian network. The results of calibration, verification, and validation with respect to each individual model are integrated using the principles of conditional probability and total probability, and propagated through the Bayesian network in order to quantify the overall system-level prediction uncertainty. The proposed methodology is illustrated with numerical examples that deal with heat conduction and structural dynamics. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Sankararaman, Shankar] SGT Inc, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Mahadevanb, Sankaran] Vanderbilt Univ, Dept Civil & Environm Engn, Nashville, TN 37235 USA. RP Sankararaman, S (reprint author), SGT Inc, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM shankar.sankararaman@nasa.gov FU Sandia National Laboratories [BG-7732] FX The study in this paper was supported by funds from Sandia National Laboratories through Contract no. BG-7732 (Technical Monitor: Dr. Angel Urbina). The support is gratefully acknowledged. NR 80 TC 4 Z9 4 U1 8 U2 28 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0951-8320 EI 1879-0836 J9 RELIAB ENG SYST SAFE JI Reliab. Eng. Syst. Saf. PD JUN PY 2015 VL 138 BP 194 EP 209 DI 10.1016/j.ress.2015.01.023 PG 16 WC Engineering, Industrial; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA CF6IR UT WOS:000352660900018 ER PT J AU Beck, BS Schiller, NH Jones, MG AF Beck, Benjamin S. Schiller, Noah H. Jones, Michael G. TI Impedance assessment of a dual-resonance acoustic liner SO APPLIED ACOUSTICS LA English DT Article DE Acoustic liners; Absorption; Noise control ID MICRO-PERFORATED PANEL; SOUND-ABSORPTION; DETAILED ANALYSIS; ABSORBERS; SYSTEMS; CAVITY; GAPS AB Acoustic liners are commonly used to reduce noise from commercial aircraft engines. Engine liners are placed in the nacelle inlet and aft bypass duct to attenuate the noise radiated from the engine. Traditional engine liners are constructed of a perforated facesheet over a honeycomb structure to create a quarter-wave absorber. With this design, the low frequency performance of the liner is limited by the depth of the honeycomb. However, with advances in engine design, lower frequency sound absorption is becoming more critical while liner depth must be minimized. Acoustic metamaterials can exhibit unique acoustic behavior using periodically arranged sub-wavelength resonators. Researchers have shown that acoustic metamaterials can effectively block the propagation of low-frequency acoustic waves. Therefore, acoustic metamaterial-inspired concepts are being investigated to improve the low frequency performance of engine liners. A proposed dual-resonance liner is presented here that combines the idea of a Helmholtz resonator metamaterial with a traditional quarter-wave acoustic liner. The low frequency acoustic absorption of a traditional liner can be significantly increased by adding a second, low frequency resonance to the system. The normal incidence absorption coefficient of the proposed liner is more than 10 times larger than a conventional honeycomb liner at the designed Helmholtz resonance frequency while retaining similar performance at higher frequencies. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Beck, Benjamin S.] Natl Inst Aerosp, Hampton, VA 23666 USA. [Schiller, Noah H.; Jones, Michael G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Beck, BS (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA. EM ben.beck@nasa.gov NR 27 TC 0 Z9 0 U1 6 U2 51 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 JUN PY 2015 VL 93 BP 15 EP 22 DI 10.1016/j.apacoust.2015.01.011 PG 8 WC Acoustics SC Acoustics GA CF0QL UT WOS:000352249200003 ER PT J AU Moreno-Madrinan, MJ Rickman, DL Ogashawara, I Irwin, DE Ye, J Al-Hamdan, MZ AF Moreno-Madrinan, Max J. Rickman, Douglas L. Ogashawara, Igor Irwin, Daniel E. Ye, Jun Al-Hamdan, Mohammad Z. TI Using remote sensing to monitor the influence of river discharge on watershed outlets and adjacent coral Reefs: Magdalena River and Rosario Islands, Colombia SO INTERNATIONAL JOURNAL OF APPLIED EARTH OBSERVATION AND GEOINFORMATION LA English DT Article DE Remote sensing; MODIS; TRMM; Water quality; Suspended sediments ID TOTAL SUSPENDED MATTER; TAMPA-BAY; MONTASTRAEA-ANNULARIS; CARIBBEAN SEA; 250-M IMAGERY; TURBIDITY; IMPACT; USA AB Worldwide, coral reef ecosystems are being increasingly threatened by sediments loads from river discharges, which in turn are influenced by changing rainfall patterns due to climate change and by growing human activity in their watersheds. In this case study, we explored the applicability of using remote sensing (RS) technology to estimate and monitor the relationship between water quality at the coral reefs around the Rosario Islands, in the Caribbean Sea, and the rainfall patterns in the Magdalena River watershed. From the Moderate Resolution Imaging Spectroradiometer (MODIS), this study used the water surface reflectance product (MOD09GQ) to estimate water surface reflectance as a proxy for sediment concentration and the land cover product (MCD12Q1 V51) to characterize land cover of the watershed. Rainfall was estimated by using the 3B43 V7 product from the Tropical Rainforest Measuring Mission (TRMM). For the first trimester of each year, we investigated the inter-annual temporal variation in water surface reflectance at the Rosario Islands and at the three main mouths of the Magdalena River watershed. No increasing or decreasing trends of water surface reflectance were detected for any of the sites for the study period 2001-2014 (p > 0.05) but significant correlations were detected among the trends of each site at the watershed mouths (r = 0.57-0.90, p < 0.05) and between them and the inter-annual variation in rainfall on the watershed (r = 0.63-0.67,p < 0.05). Those trimesters with above-normal water surface reflectance at the mouths and above-normal rainfall at the watershed coincided with La Nina conditions while the opposite was the case during El Nino conditions. Although, a preliminary analysis of inter-annual land cover trends found only cropland cover in the watershed to be significantly correlated with water surface reflectance at two of the watershed mouths (r = 0.58 and 0.63, p < 0.05), the validation analysis draw only a 40.7% of accuracy in this land cover classification. This requires further analysis to confirm the impact of the cropland on the water quality at the watershed outlets. Spatial analysis with MOD09GQ imagery detected the overpass of river plumes from Barbacoas Bay over the Rosario Islands waters. (C) 2015 The Authors. Published by Elsevier B.V. C1 [Moreno-Madrinan, Max J.] Indiana Univ, Fairbanks Sch Publ Hlth, Dept Environm Hlth, IUPUI, Indianapolis, IN 46202 USA. [Rickman, Douglas L.] NASA, Marshall Space Flight Ctr, Global Hydrol & Climate Ctr, Earth Sci Off, Huntsville, AL 35805 USA. [Ogashawara, Igor] Indiana Univ Purdue Univ, Sch Sci, Dept Earth Sci, IUPUI, Indianapolis, IN 46202 USA. [Irwin, Daniel E.] NASA, Earth Sci Off, SERVIR, Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Ye, Jun] Univ Akron, Dept Stat, Akron, OH 44325 USA. [Al-Hamdan, Mohammad Z.] Univ Space Res Assoc, NASA, Inst Sci & Technol, Marshall Space Flight Ctr, Huntsville, AL 35805 USA. RP Moreno-Madrinan, MJ (reprint author), Indiana Univ, Fairbanks Sch Publ Hlth, Dept Environm Hlth, IUPUI, Indianapolis, IN 46202 USA. EM mmorenom@iu.edu OI Rickman, Doug/0000-0003-3409-2882 FU NASA Postdoctoral Program (NPP); SERVIR/MSFC through the NPP under contract with Oak Ridge Associated Universities FX This research was conceived and initiated while the main author was working with SERVIR at the Marshall Space Flight Center (MSFC) during his fellowship with the NASA Postdoctoral Program (NPP). Partial funds were provided by SERVIR/MSFC through the NPP under contract with Oak Ridge Associated Universities. We thank Africa Flores-Cordova from University of Alabama in Huntsville (UAH) for her help with SRTM data and delineating the watershed and Dr. Ashutosh Limaye from NASA/MSFC for his advice with the use of TRMM data. We also thank Damien Jules Sulla-Menashe from Boston University for his advice regarding use and limitations of the land cover product, MCD12Q1. NR 39 TC 7 Z9 7 U1 3 U2 41 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 JUN PY 2015 VL 38 BP 204 EP 215 DI 10.1016/j.jag.2015.01.008 PG 12 WC Remote Sensing SC Remote Sensing GA CE6TC UT WOS:000351970100021 ER PT J AU Abrams, M Tsu, H Hulley, G Iwao, K Pieri, D Cudahy, T Kargel, J AF Abrams, Michael Tsu, Hiroji Hulley, Glynn Iwao, Koki Pieri, David Cudahy, Tom Kargel, Jeffrey TI The Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) after fifteen years: Review of global products SO INTERNATIONAL JOURNAL OF APPLIED EARTH OBSERVATION AND GEOINFORMATION LA English DT Review DE ASTER; Terra; Earth Observing System; Global data ID MULTISPECTRAL SATELLITE DATA; LAND-SURFACE TEMPERATURE; DEM; METHODOLOGY AB The Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) is a 15-channel imaging instrument operating on NASA's Terra satellite. A joint project between the U.S. National Aeronautics and Space Administration and Japan's Ministry of Economy, Trade, and Industry, ASTER has been acquiring data for 15 years, since March 2000. The archive now contains over 2.8 million scenes; for the majority of them, a stereo pair was collected using nadir and backward telescopes imaging in the NIR wavelength. The majority of users require only a few to a few dozen scenes for their work. Studies have ranged over numerous scientific disciplines, and many practical applications have benefited from ASTER's unique data. A few researchers have been able to mine the entire ASTER archive, that is now global in extent due to the long duration of the mission. Six examples of global products are described in this contribution: the ASTER Global Digital Elevation Model (GDEM), the most complete, highest resolution DEM available to all users; the ASTER Emissivity Database (ASTER GED), a global 5-band emissivity map of the land surface; the ASTER Global Urban Area Map (AGURAM), a 15-m resolution database of over 3500 cities; the ASTER Volcano Archive (AVA), an archive of over 1500 active volcanoes; ASTER Geoscience products of the continent of Australia; and the Global Ice Monitoring from Space (GUMS) project. (C) 2015. Elsevier B.V. All rights reserved. C1 [Abrams, Michael; Hulley, Glynn; Pieri, David] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Tsu, Hiroji] Japan Space Syst, Tokyo, Japan. [Iwao, Koki] Natl Inst Adv Ind Sci & Technol, Tsukuba, Ibaraki, Japan. [Cudahy, Tom] CSIRO, Perth, WA, Australia. [Kargel, Jeffrey] Univ Arizona, Tucson, AZ USA. RP Abrams, M (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 40 TC 11 Z9 11 U1 4 U2 25 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 JUN PY 2015 VL 38 BP 292 EP 301 DI 10.1016/j.jag.2015.01.013 PG 10 WC Remote Sensing SC Remote Sensing GA CE6TC UT WOS:000351970100029 ER PT J AU Parsani, M Carpenter, MH Nielsen, EJ AF Parsani, Matteo Carpenter, Mark H. Nielsen, Eric J. TI Entropy stable discontinuous interfaces coupling for the three-dimensional compressible Navier-Stokes equations SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE Entropy stability; Discontinuous interface coupling; Summation-by-parts (SBP) operators; Compressible Navier-Stokes equations; High order discontinuous methods ID CONSERVATION-LAWS; SCHEMES; SYSTEMS; EULER; FORM C1 [Parsani, Matteo; Carpenter, Mark H.; Nielsen, Eric J.] NASA Langley Res Ctr LaRC, Computat AeroSci Branch, Hampton, VA 23681 USA. RP Parsani, M (reprint author), NASA Langley Res Ctr LaRC, Computat AeroSci Branch, Hampton, VA 23681 USA. EM matteo.parsani@nasa.gov; mark.h.carpenter@nasa.gov; eric.j.nielsen@nasa.gov OI Parsani, Matteo/0000-0001-7300-1280 FU NASA Postdoctoral Program at the Langley Research Center; NASA FX Special thanks are extended to Dr. Mujeeb Malik for funding this work as part of the "Revolutionary Computational Aerosciences" project. This research was also supported by an appointment to the NASA Postdoctoral Program at the Langley Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. The authors are also grateful to Professor Magnus Svard for the fruitful discussions on entropy stability. NR 16 TC 5 Z9 5 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9991 EI 1090-2716 J9 J COMPUT PHYS JI J. Comput. Phys. PD JUN 1 PY 2015 VL 290 BP 132 EP 138 DI 10.1016/j.jcp.2015.02.042 PG 7 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA CE4XK UT WOS:000351833400007 ER PT J AU Beyer, AD Shaw, MD Marsili, F Allman, MS Lita, AE Verma, VB Resta, GV Stern, JA Mirin, RP Nam, SW Farr, WH AF Beyer, Andrew D. Shaw, Matthew D. Marsili, Francesco Allman, M. Shane Lita, Adriana E. Verma, Varun B. Resta, Giovanni V. Stern, Jeffrey A. Mirin, Richard P. Nam, Sae Woo Farr, William H. TI Tungsten Silicide Superconducting Nanowire Single-Photon Test Structures Fabricated Using Optical Lithography SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Nanolithography; optical detectors; superconducting detectors; superconducting materials ID DETECTOR AB Single-pixel fiber-coupled superconducting nanowire single-photon detectors (SNSPDs) operating at 1550 nm and utilizing amorphous superconducting tungsten silicide (WSi) films have proven ability to detect photons with: high system-detection efficiency (SDE) of up to 93%, low-jitter on the order of similar to 150 ps, dark count rates of similar to 1 kcps, and fast reset times on the order of tens of nanoseconds. Additionally, WSi SNSPD devices with 12-pixels have recently demonstrated downlink data rates of 79 Mbps between a terminal in orbit around the moon and a terminal on earth, as part of the Lunar Laser Communication Demonstration (LLCD) at the Lunar Lasercomm OCTL Terminal (LLOT). To further extend the performance of SNSPD devices for optical and quantum communication for terrestrial and space-based applications, the next generation of devices will need to incorporate hundreds to thousands of SNSPD pixels and to be free-space coupled. The wire widths necessary for optimal performance of WSi (similar to 120-220 nm) devices have to date been achieved using electron-beam lithography (EBL) to pattern photoresists for etch-back fabrication methods. The high cost and time to fabricate kilo-pixel arrays of SNSPDs using EBL will become prohibitive in producing such devices. Here, we report fabrication of a WSi SNSPD test structure with 64 pixels using optical lithography instead of EBL. Specifically, we used Canon EX3 and EX6 deep-UV (DUV) steppers with KrF excimer lasers (lambda = 248 nm) in the Micro Devices Laboratory at the Jet Propulsion Laboratory to fabricate the array. Dies with 8 x 8 pixels with 166-nm-wide wires were produced, with pixels having a 100 mu m pitch in the vertical and horizontal directions. Two improvements were observed: 1) the time to pattern the 8 x 8 SNSPD pixels on 3.5 mm x 3.5 mm dies filling a 4-in Si wafer required similar to 24 hours using EBL while optical lithography wrote the same dies in approximately 15 minutes; and 2) the cost to write one 4-in wafer using EBL was comparable to the cost for one optical mask for use in the stepper to write many 4-in wafers. While fabrication times and costs will vary from facility to facility, the improvements in speed and cost for optical lithography versus EBL are apparent, and this technological advance should scale and enable fast and rapid production of kilo-pixel arrays in the future. C1 [Beyer, Andrew D.; Shaw, Matthew D.; Marsili, Francesco; Resta, Giovanni V.; Stern, Jeffrey A.; Farr, William H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Allman, M. Shane; Lita, Adriana E.; Verma, Varun B.; Mirin, Richard P.; Nam, Sae Woo] NIST, Boulder, CO 80305 USA. RP Beyer, AD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Andrew.d.beyer@jpl.nasa.gov; gvresta@gmail.com OI Mirin, Richard/0000-0002-4472-4655 FU National Aeronautics and Space Administration; DARPA FX This work was supported in part by a contract with the National Aeronautics and Space Administration and by DARPA. NR 12 TC 1 Z9 1 U1 6 U2 50 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 2015 VL 25 IS 3 AR 2200805 DI 10.1109/TASC.2014.2378232 PG 5 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA CE0AZ UT WOS:000351465400010 ER PT J AU Fore, AG Chapman, BD Hawkins, BP Hensley, S Jones, CE Michel, TR Muellerschoen, RJ AF Fore, Alexander G. Chapman, Bruce D. Hawkins, Brian P. Hensley, Scott Jones, Cathleen E. Michel, Thierry R. Muellerschoen, Ronald J. TI UAVSAR Polarimetric Calibration SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Airborne radar; radar cross-sections; radar imaging; radar measurements; radar polarimetry; radar remote sensing; synthetic aperture radar (SAR); polarimetric SAR ID SAR CALIBRATION; ALGORITHM AB Uninhabited aerial vehicle synthetic aperture radar (UAVSAR) is a reconfigurable polarimetric L-band SAR that operates in quad-polarization mode and is specifically designed to acquire airborne repeat-track SAR data for interferometric measurements. In this paper, we present details of the UAVSAR radar performance, the radiometric calibration, and the polarimetric calibration. For the radiometric calibration, we employ an array of trihedral corner reflectors, as well as distributed targets. We show that UAVSAR is a well-calibrated SAR system for polarimetric applications, with absolute radiometric calibration bias better than 1 dB, residual root-mean-square (RMS) errors of similar to 0.7 dB, and RMS phase errors similar to 5.3 degrees. For the polarimetric calibration, we have evaluated the methods of Quegan and Ainsworth et al. for crosstalk calibration and find that the method of Quegan gives crosstalk estimates that depend on target type, whereas the method of Ainsworth et al. gives more stable crosstalk estimates. We find that both methods estimate leakage of the copolarizations into the cross-polarizations to be on the order of -30 dB. C1 [Fore, Alexander G.; Chapman, Bruce D.; Hawkins, Brian P.; Hensley, Scott; Jones, Cathleen E.; Michel, Thierry R.; Muellerschoen, Ronald J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Fore, AG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Alexander.Fore@jpl.nasa.gov FU National Aeronautics and Space Administration at the Jet Propulsion Laboratory, California Institute of Technology FX This work was supported under contract with the National Aeronautics and Space Administration at the Jet Propulsion Laboratory, California Institute of Technology. NR 13 TC 6 Z9 9 U1 0 U2 12 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 JUN PY 2015 VL 53 IS 6 BP 3481 EP 3491 DI 10.1109/TGRS.2014.2377637 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 CD4OV UT WOS:000351063800037 ER PT J AU Narvekar, PS Entekhabi, D Kim, SB Njoku, EG AF Narvekar, Parag S. Entekhabi, Dara Kim, Seung-Bum Njoku, Eni G. TI Soil Moisture Retrieval Using L-Band Radar Observations SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Radar roughness (RR); radar soil moisture; radar vegetation ID INTEGRAL-EQUATION MODEL; POWER-LAW SPECTRUM; SURFACE-ROUGHNESS; BACKSCATTERING MODEL; ERS SCATTEROMETER; SAR DATA; C-BAND; VEGETATION; SCATTERING; SENSITIVITY AB An algorithm for surface soil moisture estimation using L-band radar observations is introduced. The formulation envelops a wide range of land surface conditions based on three limiting cases defined in terms of end-members: smooth bare soil, rough bare soil, and a maximum vegetation covered soil. Parameterizations for these end-members are obtained using forward electromagnetic scattering models. Modulation due to soil surface roughness and overlying vegetation scattering effects between end-members are accounted using the radar vegetation index and the newly introduced radar roughness index. Hence, the retrieval algorithm developed here does not depend on ancillary vegetation or roughness information. The algorithm is tested with ground-based truck-mounted bare soil observations and observations from several airborne field campaigns that represent a wide range of surface conditions. C1 [Narvekar, Parag S.; Entekhabi, Dara] MIT, Dept Civil & Environm Engn, Cambridge, MA 02139 USA. [Kim, Seung-Bum; Njoku, Eni G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Narvekar, PS (reprint author), MIT, Dept Civil & Environm Engn, 77 Massachusetts Ave, Cambridge, MA 02139 USA. NR 50 TC 8 Z9 8 U1 1 U2 31 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 JUN PY 2015 VL 53 IS 6 BP 3492 EP 3506 DI 10.1109/TGRS.2014.2377714 PG 15 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA CD4OV UT WOS:000351063800038 ER PT J AU Wolak, MA Acharya, N Tan, T Cunnane, D Karasik, BS Xi, XX AF Wolak, Matthaeus A. Acharya, Narendra Tan, Teng Cunnane, Daniel Karasik, Boris S. Xi, Xiaoxing TI Fabrication and Characterization of Ultrathin MgB2 Films for Hot-Electron Bolometer Applications SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Hot electron bolometers; HPCVD; magnesium diboride; superconducting thin films ID CHEMICAL VAPOR-DEPOSITION; THIN-FILMS; SINGLE-CRYSTALS; RESISTIVITY; BANDWIDTH; RESISTANCE; MIXERS AB Hot-electron bolometer mixers employing thin films of conventional superconducting materials have already been successfully fabricated in the past. Magnesium diboride (MgB2) is a promising alternative to conventional superconductors, and we report the fabrication and study of ultrathin MgB, films of down to 10 nm deposited by hybrid physical-chemical vapor deposition technique. The MgB2 films showed T-c of above 36 K, while residual resistivities of up to 26 mu Omega . cm were achieved. Critical currents of more than 6 x 10(6) A . cm(-2) at 20 K have been measured for the films with thicknesses ranging from 10 to 100 nm. Fishtail structures have been observed in the magnetic field dependence of the critical current density for the thinnest of these films, indicating the presence of defects, which act as vortex pinning centers. From the magnetic field dependence, an average distance between adjacent pinning centers of 35 nm has been obtained for the thinnest films. C1 [Wolak, Matthaeus A.; Acharya, Narendra; Tan, Teng; Xi, Xiaoxing] Temple Univ, Dept Phys, Philadelphia, PA 19122 USA. [Cunnane, Daniel; Karasik, Boris S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wolak, MA (reprint author), Temple Univ, Dept Phys, Philadelphia, PA 19122 USA. EM matthaeus.wolak@temple.edu FU DoD DURIP Award from the Office of Naval Research [N0014-12-1-0777] FX This work made use of the CoE-NIC facility at Temple University supported by the DoD DURIP Award N0014-12-1-0777 from the Office of Naval Research. NR 36 TC 0 Z9 0 U1 5 U2 37 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 2015 VL 25 IS 3 AR 7500005 DI 10.1109/TASC.2015.2390415 PG 5 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA CD5PE UT WOS:000351139500006 ER PT J AU Szypryt, P Mazin, BA Bumble, B Leduc, HG Baker, L AF Szypryt, P. Mazin, B. A. Bumble, B. Leduc, H. G. Baker, L. TI Ultraviolet, Optical, and Near-IR Microwave Kinetic Inductance Detector Materials Developments SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Infrared imaging; optical imaging; superconducting device fabrication; superconducting microwave devices; superconducting resonators ID ARCONS AB We have fabricated 2024 pixel microwave kinetic inductance detector (MKID) arrays in the ultraviolet/optical/ near-IR (UVOIR) regime that are currently in use in astronomical instruments. In order to make MKIDs desirable for novel instruments, larger arrays with nearly perfect yield need to be fabricated. As array size increases, however, the percent yield often decreases due to frequency collisions in the readout. The per-pixel performance must also be improved, namely, the energy resolution. We are investigating ways to reduce frequency collisions and to improve the per-pixel performance of our devices through new superconducting material systems and fabrication techniques. There are two main routes that we are currently exploring. First, we are attempting to create more uniform titanium nitride films through the use of atomic layer deposition rather than the more traditional sputtering method. In addition, we are experimenting with completely new material systems for MKIDs, such as platinum silicide. C1 [Szypryt, P.; Mazin, B. A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Bumble, B.; Leduc, H. G.; Baker, L.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Szypryt, P (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. EM pszypryt@physics.ucsb.edu; bmazin@physics.ucsb.edu RI Mazin, Ben/B-8704-2011 OI Mazin, Ben/0000-0003-0526-1114 FU NASA Space Technology Research Fellowship FX This work was supported by a NASA Space Technology Research Fellowship. NR 15 TC 3 Z9 3 U1 2 U2 29 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 2015 VL 25 IS 3 AR 2400604 DI 10.1109/TASC.2014.2377598 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA CB4UV UT WOS:000349624700002 ER PT J AU O'Neill, S Ortega, S AF O'Neill, Sean Ortega, Sam TI 3D print a home on Mars SO NEW SCIENTIST LA English DT Editorial Material C1 [Ortega, Sam] NASA, Centennial Challenges, Washington, DC USA. [Ortega, Sam] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. NR 0 TC 1 Z9 1 U1 1 U2 10 PU REED BUSINESS INFORMATION LTD PI SUTTON PA QUADRANT HOUSE THE QUADRANT, SUTTON SM2 5AS, SURREY, ENGLAND SN 0262-4079 J9 NEW SCI JI New Sci. PD MAY 30 PY 2015 VL 226 IS 2023 BP 27 EP 27 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CJ6BU UT WOS:000355578800016 ER PT J AU Polk, JE Capece, AM AF Polk, James E. Capece, Angela M. TI Materials characterization of impregnated W and W-Ir cathodes after oxygen poisoning SO APPLIED SURFACE SCIENCE LA English DT Article DE Cathodes; Oxygen poisoning; Barium tungstate AB Electric thrusters use hollow cathodes as the electron source for generating the plasma discharge and for beam neutralization. These cathodes contain porous tungsten emitters impregnated with BaO material to achieve a lower surface work function and are operated with xenon propellant. Oxygen contaminants in the xenon plasma can poison the emitter surface, resulting in a higher work function and increased operating temperature. This could lead directly to cathode failure by preventing discharge ignition or could accelerate evaporation of the BaO material. Exposures over hundreds of hours to very high levels of oxygen can result in increased temperatures, oxidation of the tungsten substrate, and the formation of surface layers of barium tungstates. In this work, we present results of a cathode test in which impregnated tungsten and tungsten-iridium emitters were operated with 100 ppm of oxygen in the xenon plasma for several hundred hours. The chemical and morphological changes were studied using scanning electron microscopy, energy dispersive spectroscopy, and laser profilometry. The results provide strong evidence that high concentrations of oxygen accelerate the formation of tungstate layers in both types of emitters, a phenomenon not inherent to normal cathode operation. Deposits of pure tungsten were observed on the W-Ir emitter, indicating that tungsten is preferentially removed from the surface and transported in the insert plasma. A W-Ir cathode surface will therefore evolve to a pure W composition, eliminating the work function benefit of W-Ir. However, the W-Ir emitter exhibited less erosion and redeposition at the upstream end than the pure W emitter. (C) 2015 Elsevier B.V. All rights reserved. C1 [Polk, James E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Capece, Angela M.] CALTECH, Pasadena, CA 91125 USA. RP Polk, JE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM james.e.polk@jpl.nasa.gov OI Capece, Angela/0000-0003-4147-7174 FU National Aeronautics and Space Administration FX The authors would like to thank Al Owens, Ray Swindlehurst, and Ron Watkins for their assistance in preparing the test facility and Ron Ruiz and Jim Kulleck for their contributions in electron microscopy. The research described in this paper was carried out by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 17 TC 2 Z9 2 U1 0 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-4332 EI 1873-5584 J9 APPL SURF SCI JI Appl. Surf. Sci. PD MAY 30 PY 2015 VL 338 BP 27 EP 34 DI 10.1016/j.apsusc.2015.02.116 PG 8 WC Chemistry, Physical; Materials Science, Coatings & Films; Physics, Applied; Physics, Condensed Matter SC Chemistry; Materials Science; Physics GA CE2EL UT WOS:000351626700004 ER PT J AU Meyer, ET Georganopoulos, M Sparks, WB Perlman, E van der Marel, RP Anderson, J Sohn, ST Biretta, J Norman, C Chiaberge, M AF Meyer, Eileen T. Georganopoulos, Markos Sparks, William B. Perlman, Eric van der Marel, Roeland P. Anderson, Jay Sohn, Sangmo Tony Biretta, John Norman, Colin Chiaberge, Marco TI A kiloparsec-scale internal shock collision in the jet of a nearby radio galaxy SO NATURE LA English DT Article ID GAMMA-RAY BURSTS; HUBBLE-SPACE-TELESCOPE; M87 JET; 3C 264; EMISSION; MOTION; MODEL AB Jets of highly energized plasma with relativistic velocities are associated with black holes ranging in mass from a few times that of the Sun to the billion-solar-mass black holes at the centres of galaxies(1). A popular but unconfirmed hypothesis to explain how the plasma is energized is the 'internal shock model', in which the relativistic flow is unsteady(2). Faster components in the jet catch up to and collide with slower ones, leading to internal shocks that accelerate particles and generate magnetic fields(3). This mechanism can explain the variable, high-energy emission from a diverse set of objects(4-7), with the best indirect evidence being the unseen fast relativistic flow inferred to energize slower components in X-ray binary jets(8,9). Mapping of the kinematic profiles in resolved jets has revealed precessing and helical patterns in X-ray binaries(10,11), apparent superluminal motions(12,13), and the ejection of knots (bright components) from standing shocks in the jets of active galaxies(14,15). Observations revealing the structure and evolution of an internal shock in action have, however, remained elusive, hindering measurement of the physical parameters and ultimate efficiency of the mechanism. Here we report observations of a collision between two knots in the jet of nearby radio galaxy 3C 264. Abright knot with an apparent speed of (7.0 +/- 0.8)c, where c is the speed of light in a vacuum, is in the incipient stages of a collision with a slower-moving knot of speed (1.8 +/- 0.5)c just downstream, resulting in brightening of both knots-as seen in the most recent epoch of imaging. C1 [Meyer, Eileen T.; Sparks, William B.; van der Marel, Roeland P.; Anderson, Jay; Biretta, John; Norman, Colin; Chiaberge, Marco] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Meyer, Eileen T.; Georganopoulos, Markos] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Georganopoulos, Markos] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Perlman, Eric] Florida Inst Technol, Melbourne, FL 32901 USA. [Sohn, Sangmo Tony; Norman, Colin; Chiaberge, Marco] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Chiaberge, Marco] Ist Radio Astron, Ist Nazl Astrofis, I-40129 Bologna, Italy. RP Meyer, ET (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM eileen.meyer@gmail.com FU HST [GO-13327] FX E.T.M. acknowledges HST grant GO-13327. NR 28 TC 2 Z9 2 U1 0 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 MAY 28 PY 2015 VL 521 IS 7553 BP 495 EP + DI 10.1038/nature14481 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DF8BN UT WOS:000371582000002 PM 26017450 ER PT J AU Case, NA MacDonald, EA Heavner, M Tapia, AH Lalone, N AF Case, N. A. MacDonald, E. A. Heavner, M. Tapia, A. H. Lalone, N. TI Mapping auroral activity with Twitter SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE aurora; mapping; Twitter; citizen science ID GEOMAGNETIC STORMS; EARTHQUAKE AB Twitter is a popular, publicly accessible, social media service that has proven useful in mapping large-scale events in real time. In this study, for the first time, the use of Twitter as a measure of auroral activity is investigated. Peaks in the number of aurora-related tweets are found to frequently coincide with geomagnetic disturbances (detection rate of 91%). Additionally, the number of daily aurora-related tweets is found to strongly correlate with several auroral strength proxies (r(avg)approximate to 0.7). An examination is made of the bias for location and time of day within Twitter data, and a first-order correction of these effects is presented. Overall, the results suggest that Twitter can provide both specific details about an individual aurora and accurate real-time indication of when, and even from where, an aurora is visible. C1 [Case, N. A.; MacDonald, E. A.; Heavner, M.] New Mexico Consortium, Los Alamos, NM 87544 USA. [Case, N. A.; MacDonald, E. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Heavner, M.] Los Alamos Natl Lab, Los Alamos, NM USA. [Tapia, A. H.; Lalone, N.] Penn State Univ, Coll Informat Sci & Technol, University Pk, PA 16802 USA. RP Case, NA (reprint author), New Mexico Consortium, Los Alamos, NM 87544 USA. EM nathan.a.case@nasa.gov OI Case, Nathan/0000-0003-0692-1778 FU National Science Foundation (NSF) [1344296] FX This material is based upon work supported, in part, by the National Science Foundation (NSF) under grant 1344296. 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 NSF. The OMNI data were obtained from the GSFC/SPDF OMNIWeb interface at http://omniweb.gsfc.nasa.gov. The Hemispheric Power data were provided by the National Oceanic and Atmosphere Administration (NOAA) POES satellites and were obtained through the Space Weather Prediction Center (http://www.swpc.noaa.gov/). NR 25 TC 5 Z9 5 U1 0 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2015 VL 42 IS 10 BP 3668 EP 3676 DI 10.1002/2015GL063709 PG 9 WC Geosciences, Multidisciplinary SC Geology GA CL0KJ UT WOS:000356631300006 ER PT J AU Mlynczak, MG Hunt, LA Marshall, BT Russell, JM Mertens, CJ Thompson, RE Gordley, LL AF Mlynczak, Martin G. Hunt, Linda A. Marshall, B. Thomas Russell, James M., III Mertens, Christopher J. Thompson, R. Earl Gordley, Larry L. TI A combined solar and geomagnetic index for thermospheric climate SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Sun-Earth connection; space climate; thermosphere; nitric oxide AB Infrared radiation from nitric oxide (NO) at 5.3 mu m is a primary mechanism by which the thermosphere cools to space. The Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument on the NASA Thermosphere-Ionosphere-Mesosphere Energetics and Dynamics satellite has been measuring thermospheric cooling by NO for over 13years. In this letter we show that the SABER time series of globally integrated infrared power (watts) radiated by NO can be replicated accurately by a multiple linear regression fit using the F-10.7, Ap, and Dst indices. This allows reconstruction of the NO power time series back nearly 70years with extant databases of these indices. The relative roles of solar ultraviolet and geomagnetic processes in determining the NO cooling are derived and shown to vary significantly over the solar cycle. The NO power is a fundamental integral constraint on the thermospheric climate, and the time series presented here can be used to test upper atmosphere models over seven different solar cycles. C1 [Mlynczak, Martin G.; Mertens, Christopher J.] NASA Langley Res Ctr, Hampton, VA USA. [Hunt, Linda A.] SSAI, Hampton, VA USA. [Marshall, B. Thomas; Thompson, R. Earl; Gordley, Larry L.] GATS, Newport News, VA USA. [Russell, James M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. RP Mlynczak, MG (reprint author), NASA Langley Res Ctr, Hampton, VA USA. EM m.g.mlynczak@nasa.gov OI Hunt, Linda/0000-0002-5330-541X FU NASA Heliophysics Division Thermosphere-Ionosphere-Mesosphere Energetics and Dynamics mission FX The authors acknowledge support from the NASA Heliophysics Division Thermosphere-Ionosphere-Mesosphere Energetics and Dynamics mission. The Ap and F10.7 solar flux are obtained from the daily geomagnetic and daily solar data sets prepared by the NOAA Space Weather Prediction Center. The Dst data are obtained from the Data Analysis Center for geomagnetism and Space Magnetism at the World Data Center for Geomagnetism in Kyoto, Japan. The daily sunspot data are downloaded from the WDC-SILSO (World Data Center for Sunspot Index and Long-term Solar Observations) at the Royal Observatory of Belgium, Brussels. The NO power data are available by contacting the first author of this article. NR 6 TC 3 Z9 3 U1 0 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 MAY 28 PY 2015 VL 42 IS 10 BP 3677 EP 3682 DI 10.1002/2015GL064038 PG 6 WC Geosciences, Multidisciplinary SC Geology GA CL0KJ UT WOS:000356631300007 ER PT J AU Sun, WJ Slavin, JA Fu, SY Raines, JM Zong, QG Imber, SM Shi, QQ Yao, ZH Poh, G Gershman, DJ Pu, ZY Sundberg, T Anderson, BJ Korth, H Baker, DN AF Sun, Wei-Jie Slavin, James A. Fu, Suiyan Raines, Jim M. Zong, Qiu-Gang Imber, Suzanne M. Shi, Quanqi Yao, Zhonghua Poh, Gangkai Gershman, Daniel J. Pu, Zuyin Sundberg, Torbjoern Anderson, Brian J. Korth, Haje Baker, Daniel N. TI MESSENGER observations of magnetospheric substorm activity in Mercury's near magnetotail SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE magnetospheric substorm; Mercury; dipolarization; field-aligned current ID SOLAR-WIND CONDITIONS; MAGNETIC-FIELD; MAGNETOPAUSE; RECONNECTION; MODEL; ACCELERATION; INSTRUMENT; PARTICLES; FLYBY; TAIL AB MErcury Surface, Space ENviroment, GEochemistry, and Ranging (MESSENGER) magnetic field and plasma measurements taken during crossings of Mercury's magnetotail from 2011 to 2014 have been examined for evidence of substorms. A total of 26 events were found during which an Earth-like growth phase was followed by clear near-tail expansion phase signatures. During the growth phase, just as at Earth, the thinning of the plasma sheet and the increase of the magnetic field intensity in the lobe are observed, but the fractional increase in field intensity could be approximate to 3 to 5 times that at Earth. The average timescale of the growth phase is approximate to 1min. The dipolarization that marks the initiation of the substorm expansion phase is only a few seconds in duration. During the expansion phase, lasting approximate to 1min, the plasma sheet is observed to thicken and engulf the spacecraft. The duration of the substorm observed in this paper is consistent with previous observations of Mercury's Dungey cycle. The reconfiguration of the magnetotail during Mercury's substorm is very similar to that at Earth despite its very compressed timescale. C1 [Sun, Wei-Jie; Fu, Suiyan; Zong, Qiu-Gang; Pu, Zuyin] Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China. [Sun, Wei-Jie; Slavin, James A.; Raines, Jim M.; Poh, Gangkai] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Imber, Suzanne M.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Shi, Quanqi] Shandong Univ, Sch Space Sci & Phys, Shandong Prov Key Lab Opt Astron & Solar Terr Env, Weihai, Peoples R China. [Yao, Zhonghua] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Gershman, Daniel J.] NASA Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD USA. [Sundberg, Torbjoern] Queen Mary Univ London, Sch Phys & Astron, London, England. [Anderson, Brian J.; Korth, Haje] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Baker, Daniel N.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. RP Sun, WJ (reprint author), Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China. EM weijiesun@pku.edu.cn RI Poh, Gangkai/O-5378-2016; Slavin, James/H-3170-2012; OI Poh, Gangkai/0000-0002-5775-2006; Slavin, James/0000-0002-9206-724X; Sun, Weijie/0000-0001-5260-658X; Yao, Zhonghua/0000-0001-6826-2486 FU NASA [NASW-00002, NAS5-97271, NNX15AJ68G]; Chinese Scholarship Council; National Nature Science Foundation of China [41474139, 41322031, 41421003]; Major Project of Chinese National Programs for Fundamental Research and Development [2012CB825603] FX The data used in this study were available from the Planetary Data System (PDS): http://pds.jpl.nasa.gov. The MESSENGER project is supported by the NASA Discovery Program under contracts NASW-00002 to the Carnegie Institution of Washington and NAS5-97271 to the Johns Hopkins University Applied Physics Laboratory. Wei-Jie Sun is supported by the State Scholarship Fund of Chinese Scholarship Council. This work is supported by the National Nature Science Foundation of China (grants 41474139, 41322031, and 41421003) and Major Project of Chinese National Programs for Fundamental Research and Development (2012CB825603). This work is also supported by the NASA Heliophysics Supporting Research Program under grant NNX15AJ68G. NR 38 TC 8 Z9 8 U1 2 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2015 VL 42 IS 10 BP 3692 EP 3699 DI 10.1002/2015GL064052 PG 8 WC Geosciences, Multidisciplinary SC Geology GA CL0KJ UT WOS:000356631300009 ER PT J AU Benna, M Mahaffy, PR Halekas, JS Elphic, RC Delory, GT AF Benna, M. Mahaffy, P. R. Halekas, J. S. Elphic, R. C. Delory, G. T. TI Variability of helium, neon, and argon in the lunar exosphere as observed by the LADEE NMS instrument SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Moon; exosphere; helium; neon; argon; variability ID GAMMA-RAY SPECTROMETER; SOLAR-WIND; ATMOSPHERE; SIMULATION; SURFACE; MOON AB The Neutral Mass Spectrometer (NMS) onboard the Lunar Atmosphere and Dust Environment Explorer (LADEE) provided the first global characterization of He and Ar along with the discovery of Ne in the lunar exosphere. The mapping of the equatorial distribution of these noble gases revealed new selenographic and temporal variations. Helium was found to be controlled by the supply of solar wind alpha particles and by the presence of an endogenous source that supplies the exosphere at a rate of 1.9x10(23)atomss(-1). Neon was detected over the nightside at levels comparable to He and was found to exhibit the spatial distribution of a surface accommodated noncondensable gas. The global measurements of NMS revealed the presence of a localized Ar enhancement that has never been identified before at the western maria. The variability resulting from this local enhancement is coupled to a more global but transient source. C1 [Benna, M.; Mahaffy, P. R.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Benna, M.] Univ Maryland Baltimore Cty, CSST, Baltimore, MD 21228 USA. [Halekas, J. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Elphic, R. C.; Delory, G. T.] NASA Ames Res Ctr, Moffett Field, CA USA. RP Benna, M (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM mehdi.benna@nasa.gov RI Benna, Mehdi/F-3489-2012; OI Halekas, Jasper/0000-0001-5258-6128 FU NASA; NASA [NAS5-02099] FX The LADEE/NMS investigation was supported by NASA. Tests and calibrations were done at the Planetary Environment Laboratory of NASA's Goddard Space Flight Center. We are grateful for engineering/technical support especially from T. King (Instrument Manager), E. Weidner, E. Lyness, K. Patel, M. Nagaraja (Instrument Operations), and E. Raaen (Calibration). We acknowledge NASA contract NAS5-02099 and V. Angelopoulos for use of data from the ARTEMIS Mission, and specifically C. W. Carlson and J.P. McFadden for use of ESA data. The NMS data supporting this article are publicly available at the Planetary Data System (http://pds-atmospheres.nmsu.edu/data_and_services/atmospheres_data/LADE E/nms.html). NR 29 TC 10 Z9 10 U1 2 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2015 VL 42 IS 10 BP 3723 EP 3729 DI 10.1002/2015GL064120 PG 7 WC Geosciences, Multidisciplinary SC Geology GA CL0KJ UT WOS:000356631300013 ER PT J AU Heavens, NG Cantor, BA Hayne, PO Kass, DM Kleinbohl, A McCleese, DJ Piqueux, S Schofield, JT Shirley, JH AF Heavens, N. G. Cantor, B. A. Hayne, P. O. Kass, D. M. Kleinboehl, A. McCleese, D. J. Piqueux, S. Schofield, J. T. Shirley, J. H. TI Extreme detached dust layers near Martian volcanoes: Evidence for dust transport by mesoscale circulations forced by high topography SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE topographic circulation; dust; Mars; volcanoes; mesoscale ID ORBITER CAMERA OBSERVATIONS; MARS CLIMATE SOUNDER; WATER-VAPOR; VERTICAL-DISTRIBUTION; SOLAR OCCULTATIONS; ATMOSPHERE; CLOUDS; STORMS; SPECTROMETER; THARSIS AB Modeling suggests that thermal circulations over Mars's highest volcanoes transport water vapor and dust from the surface into the middle atmosphere, forming detached layers in these constituents. Intense vertical mixing also takes place in regional and global dust storms, which can generate detached layers that are extreme in both altitude and magnitude. Here we employ observations by the Mars Climate Sounder (MCS) on board Mars Reconnaissance Orbiter, taking advantage of improved vertical coverage in MCS's aerosol retrievals, to discover a new class of extreme detached dust layers (EDDLs). Observed during minimal dust storm activity and furthermore distinguished by their potentially large and measurable horizontal extent (>1000km), these EDDLs cluster near Olympus Mons and the Tharsis Montes, from which they likely originate. The existence of these EDDLs suggests that vertical mixing by topographic circulations can be much stronger than previously modeled and more frequent than previously observed. C1 [Heavens, N. G.] Hampton Univ, Dept Atmospher & Planetary Sci, Hampton, VA 23668 USA. [Cantor, B. A.] Malin Space Sci Syst, San Diego, CA USA. [Hayne, P. O.; Kass, D. M.; Kleinboehl, A.; McCleese, D. J.; Piqueux, S.; Schofield, J. T.; Shirley, J. H.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91125 USA. RP Heavens, NG (reprint author), Hampton Univ, Dept Atmospher & Planetary Sci, Hampton, VA 23668 USA. EM Nicholas.Heavens@hamptonu.edu OI Heavens, Nicholas/0000-0001-7654-503X FU NASA Jet Propulsion Laboratory; Caltech [1471216]; NASA [NNX14AM32G] FX N.G. Heavens acknowledges support from the NASA Jet Propulsion Laboratory, Caltech (subcontract 1471216) and NASA's Mars Data Analysis Program (NNX14AM32G). We thank an anonymous reviewer and Jim Murphy for their helpful comments. All MRO-MCS data used here are freely available from NASA's Planetary Data System (PDS). Any analytical code is available from the first author by request. NR 37 TC 6 Z9 6 U1 1 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2015 VL 42 IS 10 BP 3730 EP 3738 DI 10.1002/2015GL064004 PG 9 WC Geosciences, Multidisciplinary SC Geology GA CL0KJ UT WOS:000356631300014 ER PT J AU Neish, CD Barnes, JW Sotin, C MacKenzie, S Soderblom, JM Le Mouelic, S Kirk, RL Stiles, BW Malaska, MJ Le Gall, A Brown, RH Baines, KH Buratti, B Clark, RN Nicholson, PD AF Neish, C. D. Barnes, J. W. Sotin, C. MacKenzie, S. Soderblom, J. M. Le Mouelic, S. Kirk, R. L. Stiles, B. W. Malaska, M. J. Le Gall, A. Brown, R. H. Baines, K. H. Buratti, B. Clark, R. N. Nicholson, P. D. TI Spectral properties of Titan's impact craters imply chemical weathering of its surface SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE erosion and weathering; impact cratering; Titan ID CASSINI VIMS; HUYGENS PROBE; LANDING SITE; RADAR; ATMOSPHERE; TRANSMISSION; CONSTRAINTS; TOPOGRAPHY; EVAPORITE; IMAGES AB We examined the spectral properties of a selection of Titan's impact craters that represent a range of degradation states. The most degraded craters have rims and ejecta blankets with spectral characteristics that suggest that they are more enriched in water ice than the rims and ejecta blankets of the freshest craters on Titan. The progression is consistent with the chemical weathering of Titan's surface. We propose an evolutionary sequence such that Titan's craters expose an intimate mixture of water ice and organic materials, and chemical weathering by methane rainfall removes the soluble organic materials, leaving the insoluble organics and water ice behind. These observations support the idea that fluvial processes are active in Titan's equatorial regions. C1 [Neish, C. D.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Barnes, J. W.; MacKenzie, S.] Univ Idaho, Dept Phys, Moscow, ID USA. [Sotin, C.; Stiles, B. W.; Malaska, M. J.; Baines, K. H.; Buratti, B.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Soderblom, J. M.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. [Le Mouelic, S.] Univ Nantes, Lab Planetol & Geodynam, LPGNantes, CNRS UMR 6112, Nantes, France. [Kirk, R. L.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Le Gall, A.] Univ Versailles St Quentin, Lab Atmospheres, Milieux, Observat Spatiales LATMOS, Paris, France. [Brown, R. H.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Clark, R. N.] US Geol Survey, Denver, CO 80225 USA. [Nicholson, P. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Neish, CD (reprint author), Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. EM cneish@fit.edu RI Barnes, Jason/B-1284-2009; OI Barnes, Jason/0000-0002-7755-3530; Malaska, Michael/0000-0003-0064-5258 FU NASA [NNH11ZDA001N-OPR, NNH13ZDA001N-OPR]; NASA FX We wish to acknowledge the Cassini VIMS and RADAR teams for acquiring and processing the data presented here. Data from the Cassini mission are made publicly available through the Planetary Data System (pds.nasa.gov). We also wish to thank E. Turtle and an anonymous individual for their careful reviews and J. Lunine for input that helped to improve the manuscript. C.N. and C.S. acknowledge support from the NASA Outer Planets Research Program (NNH11ZDA001N-OPR and NNH13ZDA001N-OPR). Part of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. NR 52 TC 6 Z9 6 U1 0 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2015 VL 42 IS 10 BP 3746 EP 3754 DI 10.1002/2015GL063824 PG 9 WC Geosciences, Multidisciplinary SC Geology GA CL0KJ UT WOS:000356631300016 ER PT J AU Han, SC Sauber, J Pollitz, F AF Han, Shin-Chan Sauber, Jeanne Pollitz, Fred TI Coseismic compression/dilatation and viscoelastic uplift/subsidence following the 2012 Indian Ocean earthquakes quantified from satellite gravity observations SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE gravity change; strike-slip earthquake; GPS; viscoelastic relaxation; elastic deformation ID DEFORMATION; SEISMICITY; RELAXATION; AFTERSLIP; EARTH AB The 2012 Indian Ocean earthquake sequence (M-w 8.6, 8.2) is a rare example of great strike-slip earthquakes in an intraoceanic setting. With over a decade of Gravity Recovery and Climate Experiment (GRACE) data, we were able to measure and model the unanticipated large coseismic and postseismic gravity changes of these events. Using the approach of normal mode decomposition and spatial localization, we computed the gravity changes corresponding to five moment tensor components. Our analysis revealed that the gravity changes are produced predominantly by coseismic compression and dilatation within the oceanic crust and upper mantle and by postseismic vertical motion. Our results suggest that the postseismic positive gravity and the postseismic uplift measured with GPS within the coseismic compressional quadrant are best fit by ongoing uplift associated with viscoelastic mantle relaxation. Our study demonstrates that the GRACE data are suitable for analyzing strike-slip earthquakes as small as M-w 8.2 with the noise characteristics of this region. C1 [Han, Shin-Chan] Univ Newcastle, Sch Engn, Callaghan, NSW 2308, Australia. [Sauber, Jeanne] NASA Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD USA. [Pollitz, Fred] US Geol Survey, Menlo Pk, CA 94025 USA. RP Han, SC (reprint author), Univ Newcastle, Sch Engn, Callaghan, NSW 2308, Australia. EM shin-chan.han@newcastle.edu.au NR 23 TC 5 Z9 5 U1 1 U2 7 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 MAY 28 PY 2015 VL 42 IS 10 BP 3764 EP 3772 DI 10.1002/2015GL063819 PG 9 WC Geosciences, Multidisciplinary SC Geology GA CL0KJ UT WOS:000356631300018 ER PT J AU Wu, WY Lan, CW Lo, MH Reager, JT Famiglietti, JS AF Wu, Wen-Ying Lan, Chia-Wei Lo, Min-Hui Reager, John T. Famiglietti, James S. TI Increases in the annual range of soil water storage at northern middle and high latitudes under global warming SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE annual range; CMIP5; global warming ID CLIMATE-CHANGE; CMIP5; PRECIPITATION; AVAILABILITY; GRACE; SIMULATIONS; IMPACTS; DROUGHT; RUNOFF; MODELS AB Soil water storage is a fundamental signal in the land hydrological cycle and changes in soil moisture can affect regional climate. In this study, we used simulations from Coupled Model Intercomparison Project Phase 5 archives to investigate changes in the annual range of soil water storage under global warming at northern middle and high latitudes. Results show that future warming could lead to significant declines in snowfall, and a corresponding lack of snowmelt water recharge to the soil, which makes soil water less available during spring and summer. Conversely, more precipitation as rainfall results in higher recharge to soil water during its accumulating season. Thus, the wettest month of soil water gets wetter, and the driest month gets drier, resulting in an increase of the annual range and suggesting that stronger heterogeneity in global water distribution (changing extremes) could occur under global warming; this has implications for water management and water security under a changing climate. C1 [Wu, Wen-Ying; Lan, Chia-Wei; Lo, Min-Hui] Natl Taiwan Univ, Dept Atmospher Sci, Taipei 10764, Taiwan. [Reager, John T.; Famiglietti, James S.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91125 USA. [Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. [Famiglietti, James S.] Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA USA. RP Lo, MH (reprint author), Natl Taiwan Univ, Dept Atmospher Sci, Taipei 10764, Taiwan. EM minhuilo@ntu.edu.tw OI LO, MIN-HUI/0000-0002-8653-143X FU MOST [103-2111-M-002-006, 104-2923-M-002-002-MY4]; NASA FX We acknowledge the World Climate Research Programme's Working Group on Coupled Modelling, which is responsible for CMIP, and we thank the climate modeling groups for producing and making available their model output. For CMIP, the U.S. Department of Energy's Program for Climate Model Diagnosis and Intercomparison provides coordinating support and led development of software infrastructure in partnership with the Global Organization for Earth System Science Portals. GRACE land data were processed by Sean Swenson, supported by the NASA MEaSUREs Program, and are available at http://grace.jpl.nasa.gov. This study was supported by the MOST 103-2111-M-002-006 and MOST 104-2923-M-002-002-MY4 to National Taiwan University. A portion of this research was conducted at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 32 TC 2 Z9 2 U1 5 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2015 VL 42 IS 10 BP 3903 EP 3910 DI 10.1002/2015GL064110 PG 8 WC Geosciences, Multidisciplinary SC Geology GA CL0KJ UT WOS:000356631300035 ER PT J AU Thompson, DR Seidel, FC Gao, BC Gierach, MM Green, RO Kudela, RM Mouroulis, P AF Thompson, David R. Seidel, Felix C. Gao, Bo Cai Gierach, Michelle M. Green, Robert O. Kudela, Raphael M. Mouroulis, Pantazis TI Optimizing irradiance estimates for coastal and inland water imaging spectroscopy SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE imaging spectroscopy; phytoplankton; atmospheric correction; solar irradiance ID HYPERSPECTRAL IMAGER; SPECTROMETER; CALIBRATION; AIRBORNE; DESIGN; ATLAS AB Next generation orbital imaging spectrometers, with advanced global remote sensing capabilities, propose to address outstanding ocean science questions related to coastal and inland water environments. These missions require highly accurate characterization of solar irradiance in the critical 380-600nm spectral range. However, the irradiance in this spectral region is temporally variable and difficult to measure directly, leading to considerable variance between different models. Here we optimize an irradiance estimate using data from the NASA airborne Portable Remote Imaging Spectrometer (PRISM), leveraging spectrally smooth in-scene targets. We demonstrate improved retrievals for both PRISM and the Next Generation Airborne Visible Infrared Imaging Spectrometer. C1 [Thompson, David R.; Seidel, Felix C.; Gierach, Michelle M.; Green, Robert O.; Mouroulis, Pantazis] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Gao, Bo Cai] US Naval Res Lab, Washington, DC USA. [Kudela, Raphael M.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. RP Thompson, DR (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM david.r.thompson@jpl.nasa.gov OI Seidel, Felix/0000-0002-4282-2198; Thompson, David/0000-0003-1100-7550 FU JPL Earth System Science Formulation office FX The optimized irradiance spectrum and all PRISM and AVIRIS-NG radiance spectra are available at http://prism.jpl.nasa.gov and http://aviris-ng.jpl.nasa.gov. Data for Figures 3-6 are provided as supporting information. This research was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We thank the JPL PRISM team: D. Cohen, K. Balasubramanian, S. Leland, F. Loya, D. Moore, D. Randall, J. Rodriguez, C. Sarture, E. Urquiza, V. White, and K. Yee. We thank D. A. Roberts, E. Pennington, and B. Bue for assistance with AVIRIS-NG ground truth data. K. Hayashi Negrey of the University of California, Santa Cruz provided invaluable support with the collection of in situ reflectance data. We thank J. M. Fontenla for his counsel and assistance. We also thank B. Mateer, I. McCubbin, and C. V. White, and acknowledge the financial support of the JPL Earth System Science Formulation office. Copyright 2015 California Institute of Technology. All Rights Reserved. NR 18 TC 3 Z9 3 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2015 VL 42 IS 10 BP 4116 EP 4123 DI 10.1002/2015GL063287 PG 8 WC Geosciences, Multidisciplinary SC Geology GA CL0KJ UT WOS:000356631300061 ER PT J AU Tian, BJ AF Tian, Baijun TI Spread of model climate sensitivity linked to double-Intertropical Convergence Zone bias SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE global climate models (GCMs); double-ITCZ bias; equilibrium climate sensitivity (ECS); Coupled Model Intercomparison Project (CMIP5); emergent constraint ID GENERAL-CIRCULATION MODELS; DOUBLE-ITCZ PROBLEM; FUTURE; CMIP5; TEMPERATURE; PACIFIC; OCEAN AB Despite decades of climate research and model development, two outstanding problems still plague the latest global climate models (GCMs): the double-Intertropical Convergence Zone (ITCZ) bias and the 2-5 degrees C spread of equilibrium climate sensitivity (ECS). Here we show that the double-ITCZ bias and ECS in 44 GCMs from Coupled Model Intercomparison Project Phases 3/5 are negatively correlated. The models with weak (strong) double-ITCZ biases have high (low)-ECS values of similar to 4.1(2.2)degrees C. This indicates that the double-ITCZ bias is a new emergent constraint for ECS based on which ECS might be in the higher end of its range (similar to 4.0 degrees C) and most models might have underestimated ECS. In addition, we argue that the double-ITCZ bias can physically affect both cloud and water vapor feedbacks (thus ECS) and is a more easily measured emergent constraint for ECS than previous ones. It can be used as a performance metric for evaluating and comparing different GCMs. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Tian, BJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM baijun.tian@jpl.nasa.gov RI Tian, Baijun/A-1141-2007 OI Tian, Baijun/0000-0001-9369-2373 FU AIRS project at JPL FX I thank Jonathan Jiang for providing the HadGEM2-ES model precipitation data, Eric Fetzer, Brian Kahn, Graeme Stephens, Hui Su, Duane Waliser, Steven Sherwood, Sandrine Bony, Brian Soden, and two anonymous reviewers for comments. This research was performed at Jet Propulsion Laboratory (JPL) under a contract with National Aeronautics and Space Administration (NASA). It was supported by the AIRS project at JPL. I acknowledge the World Climate Research Program's (WCRP) Working Group on Coupled Modeling (WGCM), which is responsible for CMIP, and the U.S. Department of Energy's (DOE) Program for Climate Model Diagnosis and Intercomparison (PCMDI), which provides coordinating support and leads development of software infrastructure in partnership with the Global Organization for Earth System Science Portals. I thank the climate modeling groups around the world for producing and making available their model output. The observational data used in this work were provided by the Obs4MIPs project, initiated by NASA and DOE, with governance provided by the WCRP's Data Advisory Council (WDAC). Copyright 2015. All rights reserved. NR 32 TC 9 Z9 9 U1 3 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2015 VL 42 IS 10 BP 4133 EP 4141 DI 10.1002/2015GL064119 PG 9 WC Geosciences, Multidisciplinary SC Geology GA CL0KJ UT WOS:000356631300063 ER PT J AU Strahan, SE Oman, LD Douglass, AR Coy, L AF Strahan, S. E. Oman, L. D. Douglass, A. R. Coy, L. TI Modulation of Antarctic vortex composition by the quasi-biennial oscillation SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE stratospheric chlorine; stratospheric transport; quasi-biennial oscillation; Antarctic ozone ID STRATOSPHERIC POLAR VORTEX; INTERANNUAL VARIABILITY; OZONESONDE MEASUREMENTS; TROPICAL STRATOSPHERE; TRACE GASES; SOUTH-POLE; CIRCULATION; QBO; TRANSPORT; DESCENT AB Using a decade of Aura Microwave Limb Sounder observations, we show distinctly different N2O distributions in Southern Hemisphere winter that depend on the phase of the quasi-biennial oscillation (QBO). Composites of the nitrous oxide (N2O) anomalies calculated for westerly and easterly phases show that QBO-generated variability originating in the subtropical middle stratosphere fills the midlatitude surf zone by late winter. After the spring vortex breakup, the anomaly is transported to the Antarctic where it remains until the next vortex forms in fall. Trapped in the newly formed vortex, the anomaly descends in isolation through fall and winter, arriving in the Antarctic lower stratosphere in Septemberabout 1year after it formed. This transport pathway explains previously reported variability of N2O and inorganic chlorine (Cl-y) inside the Antarctic vortex and demonstrates that the middle stratosphere QBO affects ozone depletion by modulating Antarctic Cl-y. C1 [Strahan, S. E.] Univ Space Res Assoc, Columbia, MD 21046 USA. [Strahan, S. E.; Oman, L. D.; Douglass, A. R.; Coy, L.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA. [Coy, L.] Sci Syst & Applicat Inc, Lanham, MD USA. RP Strahan, SE (reprint author), Univ Space Res Assoc, Columbia, MD 21046 USA. EM susan.e.strahan@nasa.gov RI Douglass, Anne/D-4655-2012; Oman, Luke/C-2778-2009 OI Oman, Luke/0000-0002-5487-2598 FU NASA Atmospheric Composition Modeling and Analysis Program FX This work was supported by the NASA Atmospheric Composition Modeling and Analysis Program. MLS data are available at http://mls.jpl.nasa.gov. The MERRA reanalysis can be obtained from the Goddard Earth Science Data and Information Services Center, http://disc.sci.gsfc.nasa.gov/daac-bin/DataHoldings.pl. We thank Darryn Waugh and Paul Newman for their helpful discussions. NR 41 TC 2 Z9 2 U1 2 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2015 VL 42 IS 10 BP 4216 EP 4223 DI 10.1002/2015GL063759 PG 8 WC Geosciences, Multidisciplinary SC Geology GA CL0KJ UT WOS:000356631300073 ER PT J AU Orbe, C Waugh, DW Newman, PA AF Orbe, Clara Waugh, Darryn W. Newman, Paul A. TI Air-mass origin in the tropical lower stratosphere: The influence of Asian boundary layer air SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE boundary layer origin; troposphere-stratosphere transport; asian monsoon ID WATER-VAPOR; CIRCULATION MODELS; MONSOON TRANSPORT; AEROSOL LAYER; TRANSIT-TIME; PIPE MODEL; AGE; CLIMATE; OZONE; DISTRIBUTIONS AB A climatology of air-mass origin in the tropical lower stratosphere is presented for the Goddard Earth Observing System Chemistry Climate Model. During late boreal summer and fall, air-mass fractions reveal that as much as 20% of the air in the tropical lower stratosphere last contacted the planetary boundary layer (PBL) over Asia; by comparison, the air-mass fractions corresponding to last PBL contact over North America and over Europe are negligible. Asian air reaches the extratropical tropopause within a few days of leaving the boundary layer and is quasi-horizontally transported into the tropical lower stratosphere, where it persists until January. The rapid injection of Asian air into the lower stratosphereand its persistence in the deep tropics through late (boreal) winteris important as industrial emissions over East Asia continue to increase. Hence, the Asian monsoon may play an increasingly important role in shaping stratospheric composition. C1 [Orbe, Clara; Newman, Paul A.] NASA, Goddard Space Flight Ctr, Lab Atmospher Chem & Dynam, Greenbelt, MD 20771 USA. [Waugh, Darryn W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. RP Orbe, C (reprint author), NASA, Goddard Space Flight Ctr, Lab Atmospher Chem & Dynam, Greenbelt, MD 20771 USA. EM clara.orbe@nasa.gov RI Waugh, Darryn/K-3688-2016 OI Waugh, Darryn/0000-0001-7692-2798 FU Goddard Space Flight Center; NSF [AGS-1403676]; NASA [NNX14AP58G] FX This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. The authors also acknowledge support from NSF grant AGS-1403676 (D.W.W.) and NASA grant NNX14AP58G (D.W.W.). The authors are thankful for the discussions with Bill Randel, Laura Pan, and Mijeong Park. All data presented in this paper are available from the corresponding author upon direct request. NR 51 TC 7 Z9 7 U1 1 U2 7 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 MAY 28 PY 2015 VL 42 IS 10 BP 4240 EP 4248 DI 10.1002/2015GL063937 PG 9 WC Geosciences, Multidisciplinary SC Geology GA CL0KJ UT WOS:000356631300076 ER PT J AU Vega-Rodriguez, M Muller-Karger, FE Hallock, P Quiles-Perez, GA Eakin, CM Colella, M Jones, DL Li, J Soto, I Guild, L Lynds, S Ruzicka, R AF Vega-Rodriguez, M. Mueller-Karger, F. E. Hallock, P. Quiles-Perez, G. A. Eakin, C. M. Colella, M. Jones, D. L. Li, J. Soto, I. Guild, L. Lynds, S. Ruzicka, R. TI Influence of water-temperature variability on stony coral diversity in Florida Keys patch reefs SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Coral reef; Florida Keys; Sea surface temperature; Degree Heating Weeks; Species richness; Shannon diversity ID CLIMATE-CHANGE; THERMAL TOLERANCE; ACROPORA-PALMATA; LONG-TERM; STRESS; PATTERNS; DISEASE; FUTURE; HETEROGENEITY; ZOOXANTHELLAE AB Annual surveys conducted by the Coral Reef Evaluation and Monitoring Project (CREMP) reported that average benthic cover of stony corals in the Florida Keys National Marine Sanctuary, USA declined from similar to 13% in 1996 to 8% in 2009. Keys-wide, mean species richness (SR) declined by similar to 2.3 species per station. Stress due to temperature extremes is suspected to be a major driver of this trend. We tested the potential for sea surface temperature (SST) variability and acute warm-temperature events (assessed with Degree Heating Weeks) to affect stony coral diversity in the Florida Keys. Benthic cover of 43 stony coral species was examined with respect to SST variability and habitat type (patch, offshore shallow, and offshore deep reefs). For each CREMP site, SST annual variance was classified as low (<7.0 degrees C-2), intermediate (7.0 to 10.9 degrees C-2), or high (>= 11.0 degrees C-2). Nonparametric MANOVA analyses showed that in the Upper, Middle, and Lower Keys regions, massive-type stony coral species (e.g. Siderastrea siderea, Pseudodiploria strigosa, Orbicella annularis complex, Montastraea cavernosa, and Colpophyllia natans) were prevalent in the patch reef habitats exposed to intermediate to high SST variability. Intermediate SST variability was also correlated with higher Shannon diversity means in patch reefs in the Upper Keys and higher SR means in the Middle Keys, indicating either that the stony coral species in these habitats are adapted to an intermediate temperature range or that individual colonies have acclimatized to that range. No significant relationships were found between stony coral diversity and SST variability in the Dry Tortugas region. C1 [Vega-Rodriguez, M.; Mueller-Karger, F. E.; Hallock, P.; Quiles-Perez, G. A.; Jones, D. L.; Soto, I.] Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA. [Eakin, C. M.; Li, J.] NOAA, Coral Reef Watch, Ctr Satellite Applicat & Res, Natl Environm Satellite Data & Informat Serv, College Pk, MD 20740 USA. [Colella, M.; Ruzicka, R.] Florida Fish & Wildlife Conservat Commiss, Fish & Wildlife Res Inst, St Petersburg, FL 33701 USA. [Guild, L.] NASA, Ames Res Ctr, Earth Sci Div, Moffett Field, CA 94035 USA. [Lynds, S.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. RP Vega-Rodriguez, M (reprint author), Univ S Florida, Coll Marine Sci, 140 Seventh Ave South, St Petersburg, FL 33701 USA. EM mariavegarod@mail.usf.edu RI Eakin, C. Mark/F-5585-2010 FU NOAA Coral Reef Conservation Program; NASA Ames Research Center; University of South Florida's Institute for Marine Remote Sensing by NASA Grant [NNX09AV24G]; NASA [NNX12AN94H]; NSF FG-LSAMP Bridge to the Doctorate (HRD) [0929435]; USF-CMS Bridge to the Doctorate Endowed; Alfred P. Sloan Fellowship; ARCS; USEPA Water Quality Protection Program [X7-97468002]; State of Florida Marine Resource Conservation Trust Fund; NOAA; US Army Corps of Engineers [MOA-2001-683]; National Science Foundation [NSF-1015342] FX This work was possible thanks to a collaboration among the NOAA Coral Reef Watch program funded by the NOAA Coral Reef Conservation Program, the NASA Ames Research Center, and the University of South Florida's Institute for Marine Remote Sensing funded by NASA Grant NNX09AV24G to F.E.M.K., C.M.E., L.G., C. Hu, and S.L. We thank W. Turner for the NASA support. Additional funding was provided to M.V.R. by NASA headquarters under the NASA Earth and Science Fellowship Program (NNX12AN94H), the NSF FG-LSAMP Bridge to the Doctorate (HRD # 0929435), USF-CMS Bridge to the Doctorate Endowed and Alfred P. Sloan Fellowship, and ARCS (Tampa Bay Chapter). Funding to support the CREMP program is achieved through the USEPA Water Quality Protection Program (X7-97468002), the State of Florida Marine Resource Conservation Trust Fund, NOAA, the US Army Corps of Engineers (MOA-2001-683), and the National Science Foundation (NSF-1015342). The authors thank S. Donahue (FKNMS) for providing the thermograph data, N. Melo for support with the Surfer software, and the Editor and anonymous reviewers for providing helpful comments which led to the improvement of the manuscript. The manuscript contents are solely the opinions of the authors and do not constitute a statement of policy, decision, or position on behalf of NOAA or the US government. IMaRS contribution 167. NR 60 TC 2 Z9 2 U1 10 U2 38 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 MAY 28 PY 2015 VL 528 BP 173 EP 186 DI 10.3354/meps11268 PG 14 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA CK2WR UT WOS:000356075600013 ER PT J AU Klimchuk, JA AF Klimchuk, James A. TI Key aspects of coronal heating SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Article DE corona; coronal heating; magnetic fields ID SOLAR ACTIVE-REGION; HI-C; MAGNETIC-FIELDS; LOOP MODELS; FLUX-TUBE; DYNAMICS; NANOFLARES; EMISSION; RECONNECTION; RESOLUTION AB We highlight 10 key aspects of coronal heating that must be understood before we can consider the problem to be solved. (1) All coronal heating is impulsive. (2) The details of coronal heating matter. (3) The corona is filled with elemental magnetic stands. (4) The corona is densely populated with current sheets. (5) The strands must reconnect to prevent an infinite build-up of stress. (6) Nanoflares repeat with different frequencies. (7) What is the characteristic magnitude of energy release? (8) What causes the collective behaviour responsible for loops? (9) What are the onset conditions for energy release? (10) Chromospheric nanoflares are not a primary source of coronal plasma. Significant progress in solving the coronal heating problem will require coordination of approaches: observational studies, field-aligned hydrodynamic simulations, large-scale and localized three-dimensional magnetohydrodynamic simulations, and possibly also kinetic simulations. There is a unique value to each of these approaches, and the community must strive to coordinate better. C1 NASA, Goddard Space Flight Ctr, Heliophys Div, Greenbelt, MD 20771 USA. RP Klimchuk, JA (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Div, Code 661, Greenbelt, MD 20771 USA. EM james.a.klimchuk@nasa.gov RI Klimchuk, James/D-1041-2012 OI Klimchuk, James/0000-0003-2255-0305 FU NASA FX This work was supported by the NASA Heliophysics Guest Investigator and Supporting Research and Technology Programs. NR 65 TC 11 Z9 11 U1 1 U2 3 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1364-503X EI 1471-2962 J9 PHILOS T R SOC A JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci. PD MAY 28 PY 2015 VL 373 IS 2042 AR UNSP 20140256 DI 10.1098/rsta.2014.0256 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CG5BL UT WOS:000353304600001 ER PT J AU Schmelz, JT Winebarger, AR AF Schmelz, J. T. Winebarger, A. R. TI What can observations tell us about coronal heating? SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Review DE solar corona; coronal loops; hot plasma ID X-RAY TELESCOPE; EUV IMAGING SPECTROMETER; ACTIVE-REGION LOOPS; EMISSION MEASURE DISTRIBUTIONS; TRANSITION-REGION; TEMPERATURE-MEASUREMENTS; SOLAR CORONA; DIAGNOSTIC SPECTROMETER; MULTITHERMAL ANALYSIS; DENSITY-MEASUREMENTS AB The actual source of coronal heating is one of the longest standing unsolved mysteries in all of astrophysics, but it is only in recent years that observations have begun making significant contributions. Coronal loops, their structure and sub-structure, their temperature and density details, and their evolution with time, may hold the key to solving this mystery. Because spatial resolution of current observatories cannot resolve fundamental scale lengths, information about the heating of the corona must be inferred from indirect observations. Loops with unexpectedly high densities and multi-thermal cross-field temperatures were not consistent with results expected from steady uniform heating models. The hot (T > 5 MK) plasma component of loops may also be a key observation; a new sounding rocket instrument called the Marshall Grazing Incidence X-ray Spectrometer will specifically target this observable. Finally, a loop is likely to be a tangle of magnetic strands. The High Resolution Coronal Imager observed magnetic braids untwisting and reconnecting, dispersing enough energy to heat the surrounding plasma. The existence of multi-thermal, cooling loops and hot plasma provides observational constraints that all viable coronal heating models will need to explain. C1 [Schmelz, J. T.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA. [Winebarger, A. R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Schmelz, JT (reprint author), Univ Memphis, Dept Phys, Memphis, TN 38152 USA. EM jschmelz@memphis.edu NR 75 TC 2 Z9 2 U1 0 U2 1 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1364-503X EI 1471-2962 J9 PHILOS T R SOC A JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci. PD MAY 28 PY 2015 VL 373 IS 2042 AR UNSP 20140257 DI 10.1098/rsta.2014.0257 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CG5BL UT WOS:000353304600002 ER PT J AU Wang, HL Su, WY AF Wang, Hailan Su, Wenying TI The ENSO effects on tropical clouds and top-of-atmosphere cloud radiative effects in CMIP5 models SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE global climate models; cloud; cloud radiative effect; El Nino-Southern Oscillation ID GENERAL-CIRCULATION MODELS; 1997/98 EL-NINO; DIURNAL CYCLE; INTERCOMPARISON PROJECT; CLIMATE MODEL; OCEAN; PACIFIC; ISCCP; SIMULATION; CONVECTION AB The El Nino-Southern Oscillation (ENSO) effects on tropical clouds and top-of-atmosphere (TOA) cloud radiative effects (CREs) in Coupled Model Intercomparison Project Phase 5 (CMIP5) models are evaluated using satellite-based observations and International Satellite Cloud Climatology Project satellite simulator output. Climatologically, most CMIP5 models produce considerably less total cloud amount with higher cloud top and notably larger reflectivity than observations in tropical Indo-Pacific (60 degrees E-200 degrees E; 10 degrees S-10 degrees N). During ENSO, most CMIP5 models strongly underestimate TOA CRE and cloud changes over western tropical Pacific. Over central tropical Pacific, while the multi-model mean resembles observations in TOA CRE and cloud amount anomalies, it notably overestimates cloud top pressure (CTP) decreases; there are also substantial inter-model variations. The relative effects of changes in cloud properties, temperature, and humidity on TOA CRE anomalies during ENSO in the CMIP5 models are assessed using cloud radiative kernels. The CMIP5 models agree with observations in that their TOA shortwave CRE anomalies are primarily contributed by total cloud amount changes, and their TOA longwave CRE anomalies are mostly contributed by changes in both total cloud amount and CTP. The model biases in TOA CRE anomalies particularly the strong underestimations over western tropical Pacific are, however, mainly explained by model biases in CTP and cloud optical thickness () changes. Despite the distinct model climatological cloud biases particularly in regime, the TOA CRE anomalies from total cloud amount changes are comparable between the CMIP5 models and observations, because of the strong compensations between model underestimation of TOA CRE anomalies from thin clouds and overestimation from medium and thick clouds. C1 [Wang, Hailan; Su, Wenying] NASA Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. [Wang, Hailan] Sci Syst & Applicat Inc, Hampton, VA USA. RP Wang, HL (reprint author), NASA Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. EM Hailan.Wang@nasa.gov FU NASA CLOUDSAT and CALIPSO Science Team Recompete program [NNH09ZDA001N-CCST] FX This study is supported by the NASA CLOUDSAT and CALIPSO Science Team Recompete program (NNH09ZDA001N-CCST). We acknowledge the World Climate Research Programme's Working Group on Coupled Modeling, which is responsible for CMIP, and we thank the climate modeling groups (listed in Table 1 of this paper) for producing and making available their model output. For CMIP, the U.S. Department of Energy's Program for Climate Model Diagnosis and Intercomparison provides coordinating support and led development of software infrastructure in partnership with the Global Organization for Earth System Science Portals. The CERES EBAF Edition 2.7 data were obtained from the NASA Langley Research Center CERES ordering tool at http://ceres.larc.nasa.gov/cmip5_data.php/. The ISCCP data were obtained from the website http://climserv.ipsl.polytechnique.fr/cfmip-obs/. We thank Mark Zelinka and two anonymous reviewers for their constructive comments and suggestions which have significantly improved this paper. NR 60 TC 1 Z9 1 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2015 VL 120 IS 10 BP 4443 EP 4465 DI 10.1002/2014JD022337 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CL1IT UT WOS:000356696800002 ER PT J AU Klingaman, NP Jiang, XA Xavier, PK Petch, J Waliser, D Woolnough, SJ AF Klingaman, Nicholas P. Jiang, Xianan Xavier, Prince K. Petch, Jon Waliser, Duane Woolnough, Steven J. TI Vertical structure and physical processes of the Madden-Julian oscillation: Synthesis and summary SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Madden-Julian oscillation; diabatic processes; tropical convection; general circulation models ID MOIST STATIC ENERGY; COMMUNITY ATMOSPHERE MODEL; INTRASEASONAL VARIABILITY; EASTWARD PROPAGATION; MJO SIMULATION; CLIMATE MODELS; CONVECTION; BUDGET; PARAMETERIZATION; ORGANIZATION AB The Vertical structure and physical processes of the Madden-Julian oscillation (MJO) project comprises three experiments, designed to evaluate comprehensively the heating, moistening, and momentum associated with tropical convection in general circulation models (GCMs). We consider here only those GCMs that performed all experiments. Some models display relatively higher or lower MJO fidelity in both initialized hindcasts and climate simulations, while others show considerable variations in fidelity between experiments. Fidelity in hindcasts and climate simulations are not meaningfully correlated. The analysis of each experiment led to the development of process-oriented diagnostics, some of which distinguished between GCMs with higher or lower fidelity in that experiment. We select the most discriminating diagnostics and apply them to data from all experiments, where possible, to determine if correlations with MJO fidelity hold across scales and GCM states. While normalized gross moist stability had a small but statistically significant correlation with MJO fidelity in climate simulations, we find no link with fidelity in medium-range hindcasts. Similarly, there is no association between time step to time step rainfall variability, identified from short hindcasts and fidelity in medium-range hindcasts or climate simulations. Two metrics that relate precipitation to free-tropospheric moisturethe relative humidity for extreme daily precipitation and variations in the height and amplitude of moistening with rain ratesuccessfully distinguish between higher-fidelity and lower fidelity GCMs in hindcasts and climate simulations. To improve the MJO, developers should focus on relationships between convection and both total moisture and its rate of change. We conclude by offering recommendations for further experiments. C1 [Klingaman, Nicholas P.; Woolnough, Steven J.] Univ Reading, Dept Meteorol, Natl Ctr Atmospher Sci, Reading, Berks, England. [Jiang, Xianan; Waliser, Duane] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. [Jiang, Xianan; Waliser, Duane] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Xavier, Prince K.; Petch, Jon] Met Off, Exeter, Devon, England. RP Klingaman, NP (reprint author), Univ Reading, Dept Meteorol, Natl Ctr Atmospher Sci, Reading, Berks, England. EM n.p.klingaman@reading.ac.uk RI Klingaman, Nicholas/H-4610-2012 OI Klingaman, Nicholas/0000-0002-2927-9303 FU National Centre for Atmospheric Science, a collaborative center of the Natural Environment Research Council [R8/H12/83/001]; NSF Climate and Large-Scale Dynamics Program [AGS-1228302]; NOAA MAPP program [NA12OAR4310075]; Office of Naval Research [ONRBAA12-001]; NSF [AGS-1221013]; Jet Propulsion Laboratory, California Institute of Technology under National Aeronautics and Space Administration FX All data from all experiments in this project are freely available through http://earthsystemcog.org/projects/gass-yotc-mip. The authors express their gratitude to the nine modeling centers that contributed GCM data to all three experiments in this project, each of which was demanding enough on its own. Comments from Chidong Zhang and an anonymous reviewer helped us to improve the manuscript. Nicholas Klingaman and Steven Woolnough were funded by the National Centre for Atmospheric Science, a collaborative center of the Natural Environment Research Council, under contract R8/H12/83/001. Xianan Jiang acknowledges support by NSF Climate and Large-Scale Dynamics Program under award AGS-1228302 and NOAA MAPP program under award NA12OAR4310075. Duane Waliser acknowledges support from the Office of Naval Research under Project ONRBAA12-001 and NSF AGS-1221013, and the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 55 TC 14 Z9 14 U1 1 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2015 VL 120 IS 10 BP 4671 EP 4689 DI 10.1002/2015JD023196 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CL1IT UT WOS:000356696800015 ER PT J AU Klingaman, NP Woolnough, SJ Jiang, XN Waliser, D Xavier, PK Petch, J Caian, M Hannay, C Kim, D Ma, HY Merryfield, WJ Miyakawa, T Pritchard, M Ridout, JA Roehrig, R Shindo, E Vitart, F Wang, HL Cavanaugh, NR Mapes, BE Shelly, A Zhang, GJ AF Klingaman, Nicholas P. Woolnough, Steven J. Jiang, Xianan Waliser, Duane Xavier, Prince K. Petch, Jon Caian, Mihaela Hannay, Cecile Kim, Daehyun Ma, Hsi-Yen Merryfield, William J. Miyakawa, Tomoki Pritchard, Mike Ridout, James A. Roehrig, Romain Shindo, Eiki Vitart, Frederic Wang, Hailan Cavanaugh, Nicholas R. Mapes, Brian E. Shelly, Ann Zhang, Guang J. TI Vertical structure and physical processes of the Madden-Julian oscillation: Linking hindcast fidelity to simulated diabatic heating and moistening SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Madden-Julian oscillation; tropical convection; diabatic heating; model evaluation; hindcasts; diabatic moistening ID TEMPERATURE-GRADIENT APPROXIMATION; TROPICAL INTRASEASONAL OSCILLATION; COMMUNITY ATMOSPHERE MODEL; MULTIVARIATE MJO INDEX; 30-50 DAY VARIABILITY; GLOBAL CLIMATE MODEL; PART I; SYSTEMATIC-ERRORS; FORECAST SYSTEM; SUMMER MONSOON AB Many theories for the Madden-Julian oscillation (MJO) focus on diabatic processes, particularly the evolution of vertical heating and moistening. Poor MJO performance in weather and climate models is often blamed on biases in these processes and their interactions with the large-scale circulation. We introduce one of the three components of a model evaluation project, which aims to connect MJO fidelity in models to their representations of several physical processes, focusing on diabatic heating and moistening. This component consists of 20day hindcasts, initialized daily during two MJO events in winter 2009-2010. The 13 models exhibit a range of skill: several have accurate forecasts to 20days lead, while others perform similarly to statistical models (8-11days). Models that maintain the observed MJO amplitude accurately predict propagation, but not vice versa. We find no link between hindcast fidelity and the precipitation-moisture relationship, in contrast to other recent studies. There is also no relationship between models' performance and the evolution of their diabatic heating profiles with rain rate. A more robust association emerges between models' fidelity and net moistening: the highest-skill models show a clear transition from low-level moistening for light rainfall to midlevel moistening at moderate rainfall and upper level moistening for heavy rainfall. The midlevel moistening, arising from both dynamics and physics, may be most important. Accurately representing many processes may be necessary but not sufficient for capturing the MJO, which suggests that models fail to predict the MJO for a broad range of reasons and limits the possibility of finding a panacea. C1 [Klingaman, Nicholas P.; Woolnough, Steven J.] Univ Reading, Natl Ctr Atmospher Sci, Reading, Berks, England. [Klingaman, Nicholas P.; Woolnough, Steven J.] Univ Reading, Dept Meteorol, Reading, Berks, England. [Jiang, Xianan; Waliser, Duane] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. [Jiang, Xianan; Waliser, Duane] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Xavier, Prince K.; Petch, Jon; Shelly, Ann] UK Met Off, Exeter, Devon, England. [Caian, Mihaela] Swedish Meteorol & Hydrol Inst, Rossby Ctr, S-60176 Norrkoping, Sweden. [Hannay, Cecile] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Kim, Daehyun] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Ma, Hsi-Yen] Lawrence Livermore Natl Lab, Program Climate Model Diag & Intercomparison, Livermore, CA USA. [Merryfield, William J.] Environm Canada, Canadian Ctr Climate Modelling & Anal, Victoria, BC, Canada. [Miyakawa, Tomoki] Japan Agcy Marine Earth Sci & Technol, Dept Coupled Ocean Atmosphere Land Proc Res, Yokosuka, Kanagawa 2370061, Japan. [Miyakawa, Tomoki] Univ Tokyo, Atmosphere & Ocean Res Inst, Tokyo, Japan. [Pritchard, Mike] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. [Ridout, James A.] Naval Res Lab, Monterey, CA USA. [Roehrig, Romain] Meteo France, CNRM GAME, Toulouse, France. [Roehrig, Romain] CNRS, Toulouse, France. [Shindo, Eiki] Meteorol Res Inst, Tsukuba, Ibaraki 305, Japan. [Vitart, Frederic] European Ctr Medium Range Weather Forecasts, Reading, Berks, England. [Wang, Hailan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cavanaugh, Nicholas R.; Zhang, Guang J.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Mapes, Brian E.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Coral Gables, FL 33124 USA. RP Klingaman, NP (reprint author), Univ Reading, Natl Ctr Atmospher Sci, Reading, Berks, England. EM n.p.klingaman@reading.ac.uk RI Klingaman, Nicholas/H-4610-2012; Ma, Hsi-Yen/K-1019-2013 OI Klingaman, Nicholas/0000-0002-2927-9303; FU National Centre for Atmospheric Science, a collaborative center of the Natural Environment Research Council [R8/H12/83/001]; NSF Climate and Large-Scale Dynamics program [AGS-1228302]; NOAA MAPP program [NA12OAR4310075]; Office of Naval Research [ONRBAA12-001, 0601153N]; NSF [AGS-1221013, OCI-1053575, AGS-1015964]; Jet Propulsion Laboratory, California Institute of Technology under National Aeronautics and Space Administration; National Science Foundation; NASA [NNX13AM18G]; Korea Meteorological Administration Research and Development Program [CATER 2013-3142]; U.S. DOE as part of the CAPT; U.S. DOE by LLNL [DE-AC52-07NA27344]; NOAA CGC postdoctoral fellowship; NOAA [NA11OAR4310098]; DOE [DE-SC0008880]; [ATM-0425247] FX The complete archive of data produced by this project and analyzed in this manuscript is freely available for download from https://earthsystemcog.org/projects/gass-yotc-mip/. The authors are grateful to Chindong Zhang and three anonymous reviewers for their comments and suggestions on this manuscript. Nicholas Klingaman and Steven Woolnough were funded by the National Centre for Atmospheric Science, a collaborative center of the Natural Environment Research Council, under contract R8/H12/83/001. Xianan Jiang acknowledges support by NSF Climate and Large-Scale Dynamics program under award AGS-1228302 and NOAA MAPP program under award NA12OAR4310075. Duane Waliser acknowledges support from the Office of Naval Research under project ONRBAA12-001, and NSF AGS-1221013, and the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The National Center for Atmospheric Research is sponsored by the National Science Foundation. Daehyun Kim appreciates the NASA/GISS modeling group, especially Maxwell Kelley, Mao-Sung Yao, and Anthony Del Genio, for their invaluable and unlimited support. Daehyun Kim was supported by the NASA grant NNX13AM18G and the Korea Meteorological Administration Research and Development Program under grant CATER 2013-3142. The effort of Hsi-Yen Ma was funded by the RGCM and ASR programs of the U.S. DOE as part of the CAPT. This work was performed under the auspices of the U.S. DOE by LLNL under contract DE-AC52-07NA27344. William Merryfield acknowledges Jason Cole and Mike Lazare for their roles in producing CanCM4 data and Woo-Sung Lee for performing the CanCM4 simulations. Tomoki Miyakawa acknowledges the NICAM and MIROC teams for developing the models; M. Watanabe, H. Miura, and T. Nasuno for supervising the simulations; N. Hirota and T. Hashino for assistance in data processing; and a grant of supercomputing resources from the Earth Simulator Center. Mike Pritchard was supported by a NOAA CGC postdoctoral fellowship; he thanks Marat Khairoutdinov for developing and making SPCAM3 available through the Center for Multiscale Modeling of Atmospheric Processes, a National Science Foundation (NSF) Science and Technology Center managed by Colorado State University under cooperative agreement ATM-0425247. Computing resources for SPCAM3 simulations were provided courtesy of the Extreme Science and Engineering Discovery Environment, supported by NSF grant OCI-1053575 under allocation TG-ATM120034. James Ridout gratefully acknowledges support from the Office of Naval Research program element 0601153N, a grant of computing time from the United States Department of Defense High Performance Computing Modernization Program, and assistance from Maria Flatau in preparing the NavGEM1 hindcasts. Frederic Vitart acknowledges Peter Bechtold for assisting in producing tendency output from the ECMWF IFS hindcasts. Guang Zhang was supported by NSF AGS-1015964, NOAA NA11OAR4310098, and DOE DE-SC0008880. NR 103 TC 16 Z9 16 U1 2 U2 21 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2015 VL 120 IS 10 BP 4690 EP 4717 DI 10.1002/2014JD022374 PG 28 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CL1IT UT WOS:000356696800016 ER PT J AU Jiang, X Waliser, DE Xavier, PK Petch, J Klingaman, NP Woolnough, SJ Guan, B Bellon, G Crueger, T DeMott, C Hannay, C Lin, H Hu, WT Kim, D Lappen, CL Lu, MM Ma, HY Miyakawa, T Ridout, JA Schubert, SD Scinocca, J Seo, KH Shindo, E Song, XL Stan, C Tseng, WL Wang, WQ Wu, TW Wu, XQ Wyser, K Zhang, GJ Zhu, HY AF Jiang, Xianan Waliser, Duane E. Xavier, Prince K. Petch, Jon Klingaman, Nicholas P. Woolnough, Steven J. Guan, Bin Bellon, Gilles Crueger, Traute DeMott, Charlotte Hannay, Cecile Lin, Hai Hu, Wenting Kim, Daehyun Lappen, Cara-Lyn Lu, Mong-Ming Ma, Hsi-Yen Miyakawa, Tomoki Ridout, James A. Schubert, Siegfried D. Scinocca, John Seo, Kyong-Hwan Shindo, Eiki Song, Xiaoliang Stan, Cristiana Tseng, Wan-Ling Wang, Wanqiu Wu, Tongwen Wu, Xiaoqing Wyser, Klaus Zhang, Guang J. Zhu, Hongyan TI Vertical structure and physical processes of the Madden-Julian oscillation: Exploring key model physics in climate simulations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Madden-Julian oscillation; general circulation model; moist convection; multiscale interaction ID TROPICAL INTRASEASONAL OSCILLATION; CONVECTIVE MOMENTUM TRANSPORT; GENERAL-CIRCULATION MODEL; MOIST STATIC ENERGY; COUPLED EQUATORIAL WAVES; TEMPERATURE-GRADIENT APPROXIMATION; SEA-SURFACE TEMPERATURES; ASIAN SUMMER MONSOON; 1997-98 EL-NINO; TOGA COARE IOP AB Aimed at reducing deficiencies in representing the Madden-Julian oscillation (MJO) in general circulation models (GCMs), a global model evaluation project on vertical structure and physical processes of the MJO was coordinated. In this paper, results from the climate simulation component of this project are reported. It is shown that the MJO remains a great challenge in these latest generation GCMs. The systematic eastward propagation of the MJO is only well simulated in about one fourth of the total participating models. The observed vertical westward tilt with altitude of the MJO is well simulated in good MJO models but not in the poor ones. Damped Kelvin wave responses to the east of convection in the lower troposphere could be responsible for the missing MJO preconditioning process in these poor MJO models. Several process-oriented diagnostics were conducted to discriminate key processes for realistic MJO simulations. While large-scale rainfall partition and low-level mean zonal winds over the Indo-Pacific in a model are not found to be closely associated with its MJO skill, two metrics, including the low-level relative humidity difference between high- and low-rain events and seasonal mean gross moist stability, exhibit statistically significant correlations with the MJO performance. It is further indicated that increased cloud-radiative feedback tends to be associated with reduced amplitude of intraseasonal variability, which is incompatible with the radiative instability theory previously proposed for the MJO. Results in this study confirm that inclusion of air-sea interaction can lead to significant improvement in simulating the MJO. C1 [Jiang, Xianan; Waliser, Duane E.; Guan, Bin] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90089 USA. [Jiang, Xianan; Waliser, Duane E.; Guan, Bin] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Xavier, Prince K.; Petch, Jon] UK Met Off, Exeter, Devon, England. [Klingaman, Nicholas P.; Woolnough, Steven J.] Natl Ctr Atmospher Sci, Reading, Berks, England. [Klingaman, Nicholas P.; Woolnough, Steven J.] Univ Reading, Dept Meteorol, Reading, Berks, England. [Bellon, Gilles] CNRS, Meteo France, CNRM GAME, Toulouse, France. [Crueger, Traute] Max Planck Inst Meteorol, Hamburg, Germany. [DeMott, Charlotte] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Hannay, Cecile] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Lin, Hai] Environm Canada, Dorval, PQ, Canada. [Hu, Wenting] Chinese Acad Sci, Inst Atmospher Phys, State Key Lab Numer Modeling Atmospher Sci & Geop, Beijing, Peoples R China. [Kim, Daehyun] Columbia Univ, Lamont Doherty Earth Observ, New York, NY USA. [Lappen, Cara-Lyn] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX USA. [Lu, Mong-Ming] Cent Weather Bur, Taipei, Taiwan. [Ma, Hsi-Yen] Lawrence Livermore Natl Lab, Livermore, CA USA. [Miyakawa, Tomoki] Japan Agcy Marine Earth Sci & Technol, Dept Coupled Ocean Atmosphere Land Proc Res, Yokosuka, Kanagawa 2370061, Japan. [Ridout, James A.] Naval Res Lab, Monterey, CA USA. [Schubert, Siegfried D.] NASA GSFC, Global Modeling & Assimilat Off, Greenbelt, MD USA. [Scinocca, John] Environm Canada, Canadian Ctr Climate Modelling & Anal, Victoria, BC, Canada. [Seo, Kyong-Hwan] Pusan Natl Univ, Dept Atmospher Sci, Pusan 609735, South Korea. [Shindo, Eiki] Meteorol Res Inst, Climate Res Dept, Tsukuba, Ibaraki 305, Japan. [Song, Xiaoliang; Zhang, Guang J.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Stan, Cristiana] George Mason Univ, Dept Atmospher Ocean & Earth Sci, Fairfax, VA 22030 USA. [Tseng, Wan-Ling] Acad Sinica, Univ Res Ctr Environm Changes, Taipei 115, Taiwan. [Wang, Wanqiu] NOAA, Natl Ctr Environm Predict, Climate Predict Ctr, Camp Springs, MD USA. [Wu, Tongwen] China Meteorol Adm, Beijing Climate Ctr, Beijing, Peoples R China. [Wu, Xiaoqing] Iowa State Univ, Dept Geol & Atmospher Sci, Ames, IA USA. [Wyser, Klaus] Swedish Meteorol & Hydrol Inst, Rossby Ctr, S-60176 Norrkoping, Sweden. [Zhu, Hongyan] Bur Meteorol, Ctr Australian Weather & Climate Res, Melbourne, Vic, Australia. RP Jiang, XA (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90089 USA. EM xianan@ucla.edu RI Stan, Cristiana/B-4376-2009; Klingaman, Nicholas/H-4610-2012; DeMott, Charlotte/L-7414-2015; Ma, Hsi-Yen/K-1019-2013; Guan, Bin/F-6735-2010; OI Stan, Cristiana/0000-0002-0076-0574; Klingaman, Nicholas/0000-0002-2927-9303; DeMott, Charlotte/0000-0002-3975-1288; Bellon, Gilles/0000-0003-3981-1225 FU National Science Foundation (NSF) Climate and Large-Scale Dynamics Program [AGS-1228302]; NOAA MAPP program [NA12OAR4310075]; Office of Naval Research [ONRBAA12-001, 0601153N]; NSF [AGS-1221013, AGS-1211848, ATM-0935263]; Jet Propulsion Laboratory, California Institute of Technology under NASA; National Centre for Atmospheric Science, a National Environment Research Council collaborative center [R8/H12/83/001]; Joint DECC/Defra Met Office Hadley Centre Climate Programme [GA01101]; NASA [NNX13AM18G]; Korea Meteorological Administration Research and Development Program [CATER 2013-3142]; National Science Foundation; European Union [244067]; U.S. DOE as part of the CAPT; U.S. DOE by LLNL [DE-AC52-07NA27344]; National Research Foundation of Korea - Ministry of Education, Science and Technology [2011-0015486] FX The multimodel output collected by this project and analyzed in this study is available for free download from https://earthsystemcog.org/projects/gassyotc-mip/. We acknowledge the insightful comments from the Editor, C. Zhang, and J. Lin and other two reviewers, which greatly helped improve this manuscript. We would like to thank E. Maloney and J. Benedict for their help with the calculation of gross moist stability. We are indebted to E. Maloney, A. Del Genio, B. Wang, B. Mapes, M. Moncrieff, A. Majda, C. Zhang, T. Li, and WGNE MJO Task Force members for stimulating discussions during the course of this study. X. Jiang acknowledges support by National Science Foundation (NSF) Climate and Large-Scale Dynamics Program under awards AGS-1228302, and NOAA MAPP program under award NA12OAR4310075. D. Waliser acknowledges the Office of Naval Research under Project ONRBAA12-001, NSF AGS-1221013, and the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the NASA. N. Klingaman and S. Woolnough were supported by the National Centre for Atmospheric Science, a National Environment Research Council collaborative center, under contract R8/H12/83/001. P. Xavier and J. Petch are supported by the Joint DECC/Defra Met Office Hadley Centre Climate Programme (GA01101). D. Kim was supported by the NASA grant NNX13AM18G and the Korea Meteorological Administration Research and Development Program under grant CATER 2013-3142, and he appreciates the NASA/GISS modeling group, especially M. Kelley, M.-S. Yao, and A. Del Genio for their invaluable and unlimited supports. J. Ridout gratefully acknowledges support from the Office of Naval Research Program Element 0601153N, a grant of computing time from the United States Department of Defense High Performance Computing Modernization Program. The SMHI simulations were performed on resources provided by the Swedish National Infrastructure for Computing (SNIC) at the Parallel Computing Centre (PDC). The National Center for Atmospheric Research is sponsored by the National Science Foundation. Some of this research by T. Crueger has received funding from the European Union, Seventh Framework Programme (FP7/2007-2013) under grant agreement 244067. The effort of H.-Y. Ma was funded by the RGCM and ASR programs of the U.S. DOE as part of the CAPT. This work was performed under the auspices of the U.S. DOE by LLNL under contract DE-AC52-07NA27344. C. Stan was supported by NSF grant AGS-1211848. K.-H. Seo is supported by the National Research Foundation of Korea grant (2011-0015486) funded by the Ministry of Education, Science and Technology. X. Wu is supported by the NSF under grant ATM-0935263. T. Miyakawa acknowledges M. Watanabe and N. Hirota for their support in providing MIROC data set, and the Earth Simulator (JIMSTEC) for the computation. W-L Tseng was supported by the German BMBF NORDATLANTIK project, and the Norddeutscher Verbund fur Hoch- und Hochstleistungsrechnen for the computation. NR 204 TC 39 Z9 39 U1 7 U2 40 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 MAY 27 PY 2015 VL 120 IS 10 BP 4718 EP 4748 DI 10.1002/2014JD022375 PG 31 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CL1IT UT WOS:000356696800017 ER PT J AU Xavier, PK Petch, JC Klingaman, NP Woolnough, SJ Jiang, XA Waliser, DE Caian, M Cole, J Hagos, SM Hannay, C Kim, D Miyakawa, T Pritchard, MS Roehrig, R Shindo, E Vitart, F Wang, HL AF Xavier, Prince K. Petch, Jon C. Klingaman, Nicholas P. Woolnough, Steve J. Jiang, Xianan Waliser, Duane E. Caian, Mihaela Cole, Jason Hagos, Samson M. Hannay, Cecile Kim, Daehyun Miyakawa, Tomoki Pritchard, Michael S. Roehrig, Romain Shindo, Eiki Vitart, Frederic Wang, Hailan TI Vertical structure and physical processes of the Madden-Julian Oscillation: Biases and uncertainties at short range SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE diabatic processes; Madden-Julian Oscillation; modeling; convection; Year of Tropical convection; uncertainties ID CONVECTIVE MOMENTUM TRANSPORT; GLOBAL CLIMATE MODEL; TOGA COARE; INTRASEASONAL OSCILLATION; POTENTIAL PREDICTABILITY; TROPICAL CONVECTION; WEATHER PREDICTION; SYSTEMATIC-ERRORS; ACTIVE CONVECTION; PART II AB An analysis of diabatic heating and moistening processes from 12 to 36h lead time forecasts from 12 Global Circulation Models are presented as part of the Vertical structure and physical processes of the Madden-Julian Oscillation (MJO) project. A lead time of 12-36h is chosen to constrain the large-scale dynamics and thermodynamics to be close to observations while avoiding being too close to the initial spin-up of the models as they adjust to being driven from the Years of Tropical Convection (YOTC) analysis. A comparison of the vertical velocity and rainfall with the observations and YOTC analysis suggests that the phases of convection associated with the MJO are constrained in most models at this lead time although the rainfall in the suppressed phase is typically overestimated. Although the large-scale dynamics is reasonably constrained, moistening and heating profiles have large intermodel spread. In particular, there are large spreads in convective heating and moistening at midlevels during the transition to active convection. Radiative heating and cloud parameters have the largest relative spread across models at upper levels during the active phase. A detailed analysis of time step behavior shows that some models show strong intermittency in rainfall and differences in the precipitation and dynamics relationship between models. The wealth of model outputs archived during this project is a very valuable resource for model developers beyond the study of the MJO. In addition, the findings of this study can inform the design of process model experiments, and inform the priorities for field experiments and future observing systems. C1 [Xavier, Prince K.; Petch, Jon C.] Met Off, Exeter, Devon, England. [Klingaman, Nicholas P.; Woolnough, Steve J.] Univ Reading, Natl Ctr Atmospher Sci Climate, Reading, Berks, England. [Jiang, Xianan; Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Caian, Mihaela] Swedish Meteorol & Hydrol Inst, Rossby Ctr, S-60176 Norrkoping, Sweden. [Cole, Jason] Environm Canada, Canadian Ctr Climate Modelling & Anal, Victoria, BC, Canada. [Hagos, Samson M.] Pacific NW Natl Lab, Richland, WA 99352 USA. [Hannay, Cecile] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Kim, Daehyun] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Miyakawa, Tomoki] Japan Agcy Marine Earth Sci & Technol, Res Inst Global Change, Yokosuka, Kanagawa, Japan. [Pritchard, Michael S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. [Roehrig, Romain] Meteo France, CNRM, GAME, Toulouse, France. [Roehrig, Romain] CNRS, Toulouse, France. [Shindo, Eiki] Meteorol Res Inst, Climate Res Dept, Ibaraki, Japan. [Vitart, Frederic] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England. [Wang, Hailan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Xavier, PK (reprint author), Met Off, Exeter, Devon, England. EM prince.xavier@metoffice.gov.uk RI Klingaman, Nicholas/H-4610-2012; OI Klingaman, Nicholas/0000-0002-2927-9303; Cole, Jason/0000-0003-0450-2748 FU Joint DECC/Defra Met Office Hadley Centre Climate Programme [GA01101]; U.S. National Science Foundation (NSF); NASA Modeling, Analysis and Prediction (MAP) program; National Aeronautics and Space Administration; NSF Climate and Large-Scale Dynamics Program [AGS-1228302]; NOAA MAPP program [NA12OAR4310075]; National Centre for Atmospheric Science, a Natural Environment Research Council collaborative center; Office of Biological and Environmental Research of the U. S. Department of Energy as part of the Atmospheric Systems Research Program; NASA [NNX13AM18G]; Korea Meteorological Administration Research and Development Program [CATER 2013-3142]; U.S. National Science Foundation; NOAA CGC postdoctoral fellowship; NSF [OCI-1053575]; [ATM-0425247] FX The GASS-YoTC Vertical Structure and Physical Processes Multi-model Experiment was supported by the World Climate Research Program and World Weather Research Program and organized by the GEWEX Global Atmospheric System Studies (GASS) subproject and the YoTC/WGNE MJO Task Force. IT support and data services hosted by the NASA Jet Propulsion Laboratory. P. Xavier and J. Petch are supported by the Joint DECC/Defra Met Office Hadley Centre Climate Programme (GA01101). Support for D. Waliser was provided by the U.S. National Science Foundation (NSF) and the NASA Modeling, Analysis and Prediction (MAP) program with his research carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. X. Jiang acknowledges support by NSF Climate and Large-Scale Dynamics Program under award AGS-1228302 and NOAA MAPP program under award NA12OAR4310075. Support for N. Klingaman and S. Woolnough was provided by the National Centre for Atmospheric Science, a Natural Environment Research Council collaborative center. T. Miyakawa acknowledges the MIROC team (for developing the model), M. Watanabe (for supervising the simulations), N. Hirota and T. Hashino (for their support in data processing), and the Earth simulator (for computation). S. Hagos acknowledges support from the Office of Biological and Environmental Research of the U. S. Department of Energy as part of the Atmospheric Systems Research Program. D. Kim appreciates the NASA/GISS modeling group, especially M. Kelley, M.-S. Yao, and A. Del Genio for their invaluable and unlimited support. D. Kim was supported by the NASA grant NNX13AM18G and the Korea Meteorological Administration Research and Development Program under grant CATER 2013-3142. NCAR is sponsored by the U.S. National Science Foundation. M. Pritchard was supported by a NOAA CGC postdoctoral fellowship; he thanks M. Khairoutdinov for developing and making SPCAM3 available through the Center for Multiscale Modeling of Atmospheric Processes, a NSF Science and Technology Center managed by Colorado State University under Cooperative agreement ATM-0425247. Computing resources for SPCAM3 simulations were provided courtesy of the Extreme Science and Engineering Discovery Environment, supported by NSF grant OCI-1053575 under allocation TG-ATM120034. We acknowledge the insightful comments from C. Zhang and three anonymous reviewers which helped improve the manuscript. M. Webb and A. Bodas-Salcedo are acknowledged for providing information on cloud radiative heating. Quality-controlled model data from all three experiments are archived at Earth System Grid (https://earthsystemcog.org/projects/gass-yotc-mip/) and are available for download. NR 75 TC 13 Z9 13 U1 2 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2015 VL 120 IS 10 BP 4749 EP 4763 DI 10.1002/2014JD022718 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CL1IT UT WOS:000356696800018 ER PT J AU Painemal, D Minnis, P Nordeen, M AF Painemal, David Minnis, Patrick Nordeen, Michele TI Aerosol variability, synoptic-scale processes, and their link to the cloud microphysics over the northeast Pacific during MAGIC SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE aerosol indirect effect; boundary layer clouds; northeast Pacific; satellite clouds microphysics; MAGIC campaign ID DATA ASSIMILATION SYSTEM; MARINE STRATOCUMULUS; CALIFORNIA COAST; BOUNDARY-LAYER; OPTICAL DEPTH; VOCALS-REX; SATELLITE; REANALYSIS; CLIMATE AB Shipborne aerosol measurements collected from October 2012 to September 2013 along 36 transects between the port of Los Angeles, California (33.7 degrees N, 118.2 degrees), and Honolulu, Hawaii (21.3 degrees N, 157.8 degrees W), during the Marine ARM GPCI (Global Energy and Water Cycle Experiment (GEWEX)-Cloud System Study (GCSS)-Pacific Cross-section Intercomparison) Investigation of Clouds campaign are analyzed to determine the circulation patterns that modulate the synoptic and monthly variability of cloud condensation nuclei (CCN) in the boundary layer. Seasonal changes in CCN are evident, with low magnitudes during autumn/winter, and high CCN during spring/summer accompanied with a characteristic westward decrease. CCN monthly evolution is consistent with satellite-derived cloud droplet number concentration N-d from the Moderate Resolution Imaging Spectroradiometer. One-point correlation (r) analysis between the 1000hPa zonal wind time series over a region between 125 degrees W and 135 degrees W, 35 degrees N and 45 degrees N, and the N-d field yields a negative r (up to -0.55) over a domain that covers a zonal extent of at least 20 degrees from the California shoreline, indicating that N-d decreases when the zonal wind intensifies. The negative r expands southwestward as the zonal wind precedes N-d by up to 3days, suggesting a transport mechanism from the coast of North America mediated by the California low-coastal jet, which intensifies in summer when the aerosol concentration and N-d reach a maximum. A first assessment of aerosol-cloud interaction (ACI) is performed by combining CCN and satellite N-d values from the Fifteenth Geostationary Operational Environmental Satellite. The CCN-N-d correlation is 0.66-0.69, and the ACI metric defined as ACI=ln(N-d)/ln(CCN) is high at 0.9, similar to other aircraft-based studies and substantially greater than those inferred from satellites and climate models. C1 [Painemal, David; Nordeen, Michele] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Painemal, David; Minnis, Patrick; Nordeen, Michele] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Painemal, D (reprint author), Sci Syst & Applicat Inc, Hampton, VA 23666 USA. EM david.painemal@nasa.gov FU U.S. Department of Energy, Office of Biological and Environmental Research, Atmospheric System Research Program [DE-FOA-0000885] FX This research was supported by the U.S. Department of Energy, Office of Biological and Environmental Research, Atmospheric System Research Program grant DE-FOA-0000885. The MAGIC data set was downloaded from the ARM archive available at http://www.archive.arm.gov/. MODIS retrievals are available at http://ceres.larc.nasa.gov/order_data.php and GOES 15 at http://www-pm.larc.nasa.gov or upon request. The authors thank the NOAA Air Resources Laboratory for making available the HYSPLIT online application used to perform the back trajectory analysis (http://www.ready.noaa.gov). We acknowledge Horizon Lines and the Captain and crew of the Horizon Spirit, as well as the leadership of MAGIC PI Ernie Lewis and the work of scientists and technicians involved in the data collection and postprocessing. NR 45 TC 4 Z9 4 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2015 VL 120 IS 10 BP 5122 EP 5139 DI 10.1002/2015JD023175 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CL1IT UT WOS:000356696800038 ER PT J AU Sun, K Cady-Pereira, K Miller, DJ Tao, L Zondlo, MA Nowak, JB Neuman, JA Mikoviny, T Muller, M Wisthaler, A Scarino, AJ Hostetler, CA AF Sun, Kang Cady-Pereira, Karen Miller, David J. Tao, Lei Zondlo, Mark A. Nowak, John B. Neuman, J. A. Mikoviny, Tomas Mueller, Markus Wisthaler, Armin Scarino, Amy J. Hostetler, Chris A. TI Validation of TES ammonia observations at the single pixel scale in the San Joaquin Valley during DISCOVER-AQ SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE TES; ammonia; validation; NH3 ID IASI SATELLITE-OBSERVATIONS; QUANTUM CASCADE-LASER; ATMOSPHERIC AMMONIA; OPEN-PATH; PARTICULATE MATTER; EMISSIONS; NH3; RESOLUTION; MODEL; CALIBRATION AB Ammonia measurements from a vehicle-based, mobile open-path sensor and those from aircraft were compared with Tropospheric Emission Spectrometer (TES) NH3 columns at the pixel scale during the NASA Deriving Information on Surface conditions from Column and Vertically Resolved Observations Relevant to Air Quality field experiment. Spatial and temporal mismatches were reduced by having the mobile laboratory sample in the same areas as the TES footprints. To examine how large heterogeneities in the NH3 surface mixing ratios may affect validation, a detailed spatial survey was performed within a single TES footprint around the overpass time. The TES total NH3 column above a single footprint showed excellent agreement with the in situ total column constructed from surface measurements with a difference of 2% (within the combined measurement uncertainties). The comparison was then extended to a TES transect of nine footprints where aircraft data (5-80ppbv) were available in a narrow spatiotemporal window (<10km, <1h). The TES total NH3 columns above the nine footprints agreed to within 6% of the in situ total columns derived from the aircraft-based measurements. Finally, to examine how TES captures surface spatial gradients at the interpixel scale, ground-based, mobile measurements were performed directly underneath a TES transect, covering nine footprints within 1.5h of the overpass. The TES total columns were strongly correlated (R-2=0.82) with the median NH3 mixing ratios measured at the surface. These results provide the first in situ validation of the TES total NH3 column product, and the methodology is applicable to other satellite observations of short-lived species at the pixel scale. C1 [Sun, Kang; Miller, David J.; Tao, Lei; Zondlo, Mark A.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. [Sun, Kang; Miller, David J.; Tao, Lei; Zondlo, Mark A.] ERC, NSF, Infrared Technol Hlth & Environm, Ctr Mid, Princeton, NJ USA. [Cady-Pereira, Karen] Atmospher & Environm Res, Lexington, MA USA. [Nowak, John B.] Aerodyne Res Inc, Billerica, MA USA. [Neuman, J. A.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Neuman, J. A.] NOAA Earth Syst Res Lab, Boulder, CO 80309 USA. [Mikoviny, Tomas; Wisthaler, Armin] Inst Ionenphys & Angew Phys, Innsbruck, Austria. [Mikoviny, Tomas; Wisthaler, Armin] Univ Oslo, Dept Chem, Oslo, Norway. [Mueller, Markus] Oak Ridge Associated Univ, Oak Ridge, TN USA. [Scarino, Amy J.] Sci Syst & Applications Inc, Hampton, VA USA. [Hostetler, Chris A.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Zondlo, MA (reprint author), Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. EM mzondlo@princeton.edu RI Nowak, John/B-1085-2008; Muller, Markus/L-1699-2014; Neuman, Andy/A-1393-2009; Zondlo, Mark/R-6173-2016; Manager, CSD Publications/B-2789-2015 OI Nowak, John/0000-0002-5697-9807; Muller, Markus/0000-0003-4110-8950; Neuman, Andy/0000-0002-3986-1727; Zondlo, Mark/0000-0003-2302-9554; FU Center for Mid-Infrared Technologies for Health and the Environment under National Science Foundation [EEC-0540832]; NASA Earth and Space Science Fellowship [NN12AN64H]; NASA Jet Propulsion Laboratory; Austrian Federal Ministry for Transport, Innovation and Technology (bmvit) through Austrian Space Applications Programme of the Austrian Research Promotion Agency (FFG) [9, 840086]; National Institute of Aerospace; NASA FX We acknowledge the support of the NASA DISCOVER-AQ California 2013 science team, as well as Trent Proctor of the U.S. Forest Service for providing work and storage space in Porterville, California. We thank Michael Shook, Jennifer Olson, and Gao Chen for providing the merged airborne NH3 data set and PBL heights derived from P-3B data and Robert Herman for providing the TES footprint coordinates before the overpass. The sensor development was supported by the Center for Mid-Infrared Technologies for Health and the Environment under National Science Foundation grant EEC-0540832. Kang Sun acknowledges support by NASA Earth and Space Science Fellowship (NN12AN64H). Work at AER was funded through a contract with the NASA Jet Propulsion Laboratory. The CRDS NH3 measurements were made possible by the generous support from the DISCOVER-AQ program. NH3 measurements by the PTR-ToF-MS aboard the NASA P-3B were supported by the Austrian Federal Ministry for Transport, Innovation and Technology (bmvit) through the Austrian Space Applications Programme 9 of the Austrian Research Promotion Agency (FFG) (840086). The measurement instrument was developed in joint work with Ionicon Analytik GmbH (Innsbruck, Austria). Armin Wisthaler received support from the Visiting Scientist Program at the National Institute of Aerospace. Tomas Mikoviny was supported by an appointment to the NASA Postdoctoral Program at the Langley Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. The aircraft measurement teams acknowledge NASA B-200 King Air and P-3B flight crew for their outstanding work supporting these flights. All data used in this study are available at DISCOVER-AQ data archive (http://www-air.larc.nasa.gov/cgi-bin/ArcView/discover-aq.ca-2013). NR 42 TC 8 Z9 8 U1 2 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2015 VL 120 IS 10 BP 5140 EP 5154 DI 10.1002/2014JD022846 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CL1IT UT WOS:000356696800039 ER PT J AU Liu, JJ Bowman, KW Henze, DK AF Liu, Junjie Bowman, Kevin W. Henze, Daven K. TI Source-receptor relationships of column-average CO2 and implications for the impact of observations on flux inversions SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE adjoint sensitivity; local versus nonlocal flux contributions; observation impact; GOSAT column CO2 ID VARIATIONAL DATA ASSIMILATION; ENSEMBLE KALMAN FILTER; ATMOSPHERIC CO2; FIRE EMISSIONS; MODEL; OCEAN; ADJOINT; COMMUNITIES; INFORMATION; TRANSPORT AB Source-receptor relationships are the fundamental quantities used in atmosphere CO2 flux inversions. In this study, we systematically investigate the global source-receptor relationships of column CO2 (X-CO2) in 12 continental-scale receptors in terms of transport and local versus nonlocal flux contributions using the GEOS-Chem adjoint model. Using simulated Greenhouse gases Observing Satellite (GOSAT) X-CO2, we quantify the impact of inclusion (add-on) or exclusion of observations (data-denial) within a receptor region on flux inversion. We discuss the connections between the observation impact and the underlying source-receptor relationships. The strong sensitivity of X-CO2 to nonlocal fluxes makes the X-CO2 observations have strong impact on nonlocal flux estimation. On an annual mean, the impact of GOSAT X-CO2 over Europe on North America flux estimation is 10%-39% of the full observation impact. Because the Southern Hemisphere midlatitude X-CO2 are most sensitive to local and tropical fluxes, the mean impact of GOSAT X-CO2 over Southern South America on Northern South America (N-S-America) flux estimation is 30%-59% of the full observation impact. Because of the strong sensitivity of the X-CO2 over N-S-America to Central Africa (C-Africa) fluxes, the mean impact on C-Africa flux estimation is between 14% and 31% of the full observation impact in spite of the sparse observation coverage. The results also show that X-CO2 have similar sensitivity to local and nonlocal fluxes occurring 3 months before, which indicates that X-CO2 observations cannot differentiate any fluxes occurring beyond 3 months. C1 [Liu, Junjie; Bowman, Kevin W.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Henze, Daven K.] Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA. RP Liu, JJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM junjie.liu@jpl.nasa.gov RI Chem, GEOS/C-5595-2014; OI LIu, Junjie/0000-0002-7184-6594 FU OCO-2 science team grant [11-OCO211-24]; NASA Carbon Monitoring System program FX Data to support this article can be obtained by contacting the corresponding author by email (junjie.liu@jpl.nasa.gov). We appreciate the constructive comments from the three anonymous reviewers. We acknowledge the funding support from OCO-2 science team grant (11-OCO211-24) and NASA Carbon Monitoring System program. The GOSAT-ACOS XCO2 data were produced by the ACOS/OCO-2 project at the Jet Propulsion Laboratory, California Institute of Technology, and obtained from the ACOS/OCO-2 data archive maintained at the NASA Goddard Earth Science Data and Information Services Center. The GOSAT spectra were provided to the ACOS Team through a GOSAT Research Announcement (RA) agreement between the California Institute of Technology and the three parties, JAXA, NIES, and the MOE. A portion 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. All the computations were performed in NASA AMES supercomputers. NR 47 TC 7 Z9 7 U1 3 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2015 VL 120 IS 10 BP 5214 EP 5236 DI 10.1002/2014JD022914 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CL1IT UT WOS:000356696800042 ER PT J AU Houweling, S Baker, D Basu, S Boesch, H Butz, A Chevallier, F Deng, F Dlugokencky, EJ Feng, L Ganshin, A Hasekamp, O Jones, D Maksyutov, S Marshall, J Oda, T O'Dell, CW Oshchepkov, S Palmer, PI Peylin, P Poussi, Z Reum, F Takagi, H Yoshida, Y Zhuravlev, R AF Houweling, S. Baker, D. Basu, S. Boesch, H. Butz, A. Chevallier, F. Deng, F. Dlugokencky, E. J. Feng, L. Ganshin, A. Hasekamp, O. Jones, D. Maksyutov, S. Marshall, J. Oda, T. O'Dell, C. W. Oshchepkov, S. Palmer, P. I. Peylin, P. Poussi, Z. Reum, F. Takagi, H. Yoshida, Y. Zhuravlev, R. TI An intercomparison of inverse models for estimating sources and sinks of CO2 using GOSAT measurements SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE carbon cycle; carbon dioxide; inverse modeling; model intercomparison; satellite remote sensing ID ATMOSPHERIC CO2; TRANSPORT SIMULATIONS; RETRIEVAL ALGORITHM; REGIONAL CO2; GLOBAL CO2; ENSEMBLE; FLUXES; XCO2; VALIDATION; CHEMISTRY AB This study presents the outcome of an inverse modeling intercomparison experiment on the use of total column CO2 retrievals from Greenhouse Gas Observing Satellite (GOSAT) for quantifying global sources and sinks of CO2. Eight research groups submitted inverse modeling results for the first year of GOSAT measurements. Inversions were carried out using only GOSAT data, a combination of GOSAT and surface measurements, and using only surface measurements. As expected, the most robust flux estimates are obtained at large scales (e.g., within 20% of the annual flux at the global scale), and they quickly diverge toward the scale of the subcontinental TRANSCOM regions and beyond (to >100% of the annual flux). We focus our analysis on a shift in the CO2 uptake over land from the Tropics toward the Northern Hemisphere Extra tropics of approximate to 1 PgC/yr when GOSAT data are used in the inversions. This shift is largely driven by TRANSCOM regions Europe and Northern Africa, showing, respectively, an increased uptake and release of 0.7 and 0.9 PgC/yr. Inversions using GOSAT data show a reduced gradient between midlatitudes of the Northern Hemisphere and the Tropics, consistent with the latitudinal shift in carbon uptake. However, the reduced gradients degrade the agreement with background aircraft and surface measurements. To narrow the range of inversion-derived flux, estimates will require further efforts to understand the differences not only between the retrieval schemes but also between inverse models, as their contributions to the overall uncertainty are estimated to be of similar magnitude. C1 [Houweling, S.; Hasekamp, O.] SRON Netherlands Inst Space Res, Utrecht, Netherlands. [Houweling, S.] Inst Marine & Atmospher Res Utrecht, Utrecht, Netherlands. [Baker, D.] Colorado State Univ, CIRA, Boulder, CO USA. [Basu, S.; Dlugokencky, E. J.; Oda, T.] NOAA ESRL, Boulder, CO USA. [Boesch, H.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Butz, A.] Karlsruhe Inst Technol, D-76021 Karlsruhe, Germany. [Chevallier, F.; Peylin, P.] Lab Sci Climat & Environm, Gif Sur Yvette, France. [Deng, F.; Jones, D.] Univ Toronto, Dept Phys, Toronto, ON, Canada. [Feng, L.; Palmer, P. I.] Univ Edinburgh, Sch GeoSci, Edinburgh, Midlothian, Scotland. [Ganshin, A.; Zhuravlev, R.] Cent Aerol Observ, Dolgoprudnyi, Russia. [Maksyutov, S.; Oshchepkov, S.; Takagi, H.; Yoshida, Y.] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan. [Marshall, J.; Reum, F.] Max Planck Inst Biogeochem, D-07745 Jena, Germany. [Oda, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Oda, T.] GESTAR, Columbia, MD USA. [O'Dell, C. W.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Poussi, Z.] Climmod, Orsay, France. RP Houweling, S (reprint author), SRON Netherlands Inst Space Res, Utrecht, Netherlands. EM s.houweling@sron.nl RI Maksyutov, Shamil/G-6494-2011; Butz, Andre/A-7024-2013; Boesch, Hartmut/G-6021-2012; Ganshin, Alexander/C-1626-2014; Vuichard, Nicolas/A-6629-2011; Chevallier, Frederic/E-9608-2016; Jones, Dylan/O-2475-2014; OI Maksyutov, Shamil/0000-0002-1200-9577; Butz, Andre/0000-0003-0593-1608; Ganshin, Alexander/0000-0002-2835-3145; Chevallier, Frederic/0000-0002-4327-3813; Jones, Dylan/0000-0002-1935-3725; Deng, Feng/0000-0002-1381-0243 FU ESA via the GHG-CCI project FX This study made use of several measurement data sets that were kindly made available to us and are essential for our research, including: HIPPO (http://hippo.ucar.edu), CONTRAIL (http://www.cger.nies.go.jp/contrail/contrail.html), NOAA aircraft profiles (http://www.esrl.noaa.gov/gmd/ccgg/aircraft/), TCCON (http://www.tccon.caltech.edu), and various surface measurement networks (CSIRO, EC, Niwa, JMA, and LSCE) who make their data available through the World Data Centre for Greenhouse Gases (http://ds.data.jma.go.jp/gmd/wdcgg/). We would like to thank the GOSAT project for making the GOSAT-observed spectral radiances freely available. In addition, we thank the organizers of GOSAT RA to stimulate international collaboration by organizing meetings, which initiated this intercomparison initiative. University of Leicester, SRON and KIT received funding from ESA via the GHG-CCI project. NR 42 TC 11 Z9 12 U1 3 U2 34 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 MAY 27 PY 2015 VL 120 IS 10 BP 5253 EP 5266 DI 10.1002/2014JD022962 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CL1IT UT WOS:000356696800044 ER PT J AU Fleming, EL George, C Heard, DE Jackman, CH Kurylo, MJ Mellouki, W Orkin, VL Swartz, WH Wallington, TJ Wine, PH Burkholder, JB AF Fleming, Eric L. George, Christian Heard, Dwayne E. Jackman, Charles H. Kurylo, Michael J. Mellouki, Wahid Orkin, Vladimir L. Swartz, William H. Wallington, Timothy J. Wine, Paul H. Burkholder, James B. TI The impact of current CH4 and N2O atmospheric loss process uncertainties on calculated ozone abundances and trends SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE stratospheric ozone; chemical uncertainties; laboratory measurements ID LASER-INDUCED FLUORESCENCE; OH RADICAL REACTIONS; GAS-PHASE REACTIONS; RATE CONSTANTS; TEMPERATURE-DEPENDENCE; FLASH-PHOTOLYSIS; BRANCHING RATIOS; ULTRAVIOLET-ABSORPTION; DEPLETING SUBSTANCES; SUBSTITUTED METHANES AB The atmospheric loss processes of N2O and CH4, their estimated uncertainties, lifetimes, and impacts on ozone abundance and long-term trends are examined using atmospheric model calculations and updated kinetic and photochemical parameters and uncertainty factors from Stratospheric Processes and their Role in Climate (SPARC) (2013). The uncertainty ranges in calculated N2O and CH4 global lifetimes computed using the SPARC estimated uncertainties are reduced by nearly a factor of 2 compared with uncertainties from Sander et al. (2011). Uncertainties in CH4 loss due to reaction with OH and O(D-1) have relatively small impacts on present-day global total ozone (0.2-0.5%). Uncertainty in the Cl+CH4 reaction affects the amount of chlorine in radical versus reservoir forms and has a modest impact on present-day southern hemisphere (SH) polar ozone (similar to 6%) and on the rate of past ozone decline and future recovery. Uncertainty in the total rate coefficient for the O(D-1)+N2O reaction results in a substantial range in present-day stratospheric odd nitrogen (20-25%) and global total ozone (1.5-2.5%). Uncertainty in the O(D-1)+N2O reaction branching ratio for the O-2+N-2 and 2NO product channels results in moderate impacts on odd nitrogen (+/- 10%) and global ozone (+/- 1%), with uncertainty in N2O photolysis resulting in relatively small impacts (+/- 5% in odd nitrogen, +/- 0.5% in global ozone). Uncertainties in the O(D-1)+N2O reaction and its branching ratio also affect the rate of past global total ozone decline and future recovery, with a range in future ozone projections of +/- 1-1.5% by 2100, relative to present day. C1 [Fleming, Eric L.; Jackman, Charles H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fleming, Eric L.] Sci Syst & Applicat Inc, Lanham, MD USA. [George, Christian] Univ Lyon 1, CNRS, IRCELYON, CRNS, F-69365 Lyon, France. [Heard, Dwayne E.] Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England. [Kurylo, Michael J.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res Program, Greenbelt, MD USA. [Mellouki, Wahid] CNRS, Inst Combust Aerotherm Reactivite & Environm, Orleans 02, France. [Orkin, Vladimir L.] NIST, Gaithersburg, MD 20899 USA. [Swartz, William H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Wallington, Timothy J.] Ford Motor Co, Syst Analyt & Environm Sci Dept, Dearborn, MI 48121 USA. [Wine, Paul H.] Georgia Inst Technol, Sch Chem & Biochem, Atlanta, GA 30332 USA. [Wine, Paul H.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Burkholder, James B.] NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO USA. RP Fleming, EL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM eric.l.fleming@nasa.gov; James.B.Burkholder@noaa.gov RI Jackman, Charles/D-4699-2012; Wine, Paul/J-4820-2015; Swartz, William/A-1965-2010; Mellouki, Abdelwahid/H-5219-2011; Manager, CSD Publications/B-2789-2015 OI Wine, Paul/0000-0002-5537-4304; Swartz, William/0000-0002-9172-7189; Mellouki, Abdelwahid/0000-0002-6594-5262; FU NOAAs Climate Goal and NASAs Atmospheric Composition Program FX We thank Susan Strahan and Steve Steenrod of the Global Modeling Initiative project for running the GMI CTM simulations used in this work. We also thank four anonymous reviewers for their helpful comments and suggestions. This work was supported in part by NOAAs Climate Goal and NASAs Atmospheric Composition Program. GSFC 2-D model output used in this manuscript will be provided to interested individuals upon request to E. Fleming (eric.l.fleming@nasa.gov). NR 78 TC 1 Z9 1 U1 1 U2 23 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 MAY 27 PY 2015 VL 120 IS 10 BP 5267 EP 5293 DI 10.1002/2014JD022067 PG 27 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CL1IT UT WOS:000356696800045 ER PT J AU Thebault, E Finlay, CC Beggan, CD Alken, P Aubert, J Barrois, O Bertrand, F Bondar, T Boness, A Brocco, L Canet, E Chambodut, A Chulliat, A Coisson, P Civet, F Du, A Fournier, A Fratter, I Gillet, N Hamilton, B Hamoudi, M Hulot, G Jager, T Korte, M Kuang, W Lalanne, X Langlais, B Leger, JM Lesur, V Lowes, FJ Macmillan, S Mandea, M Manoj, C Maus, S Olsen, N Petrov, V Ridley, V Rother, M Sabaka, TJ Saturnino, D Schachtschneider, R Sirol, O Tangborn, A Thomson, A Toffner-Clausen, L Vigneron, P Wardinski, I Zvereva, T AF Thebault, Erwan Finlay, Christopher C. Beggan, Ciaran D. Alken, Patrick Aubert, Julien Barrois, Olivier Bertrand, Francois Bondar, Tatiana Boness, Axel Brocco, Laura Canet, Elisabeth Chambodut, Aude Chulliat, Arnaud Coisson, Pierdavide Civet, Francois Du, Aimin Fournier, Alexandre Fratter, Isabelle Gillet, Nicolas Hamilton, Brian Hamoudi, Mohamed Hulot, Gauthier Jager, Thomas Korte, Monika Kuang, Weijia Lalanne, Xavier Langlais, Benoit Leger, Jean-Michel Lesur, Vincent Lowes, Frank J. Macmillan, Susan Mandea, Mioara Manoj, Chandrasekharan Maus, Stefan Olsen, Nils Petrov, Valeriy Ridley, Victoria Rother, Martin Sabaka, Terence J. Saturnino, Diana Schachtschneider, Reyko Sirol, Olivier Tangborn, Andrew Thomson, Alan Toffner-Clausen, Lars Vigneron, Pierre Wardinski, Ingo Zvereva, Tatiana TI International Geomagnetic Reference Field: the 12th generation SO EARTH PLANETS AND SPACE LA English DT Article DE Geomagnetism; Field modeling; IGRF ID MODELS; IGRF AB The 12th generation of the International Geomagnetic Reference Field (IGRF) was adopted in December 2014 by the Working Group V-MOD appointed by the International Association of Geomagnetism and Aeronomy (IAGA). It updates the previous IGRF generation with a definitive main field model for epoch 2010.0, a main field model for epoch 2015.0, and a linear annual predictive secular variation model for 2015.0-2020.0. Here, we present the equations defining the IGRF model, provide the spherical harmonic coefficients, and provide maps of the magnetic declination, inclination, and total intensity for epoch 2015.0 and their predicted rates of change for 2015.0-2020.0. We also update the magnetic pole positions and discuss briefly the latest changes and possible future trends of the Earth's magnetic field. C1 [Thebault, Erwan; Civet, Francois; Langlais, Benoit; Saturnino, Diana] Univ Nantes, CNRS, Lab Planetol & Geodynam Nantes, UMR 6112, F-44322 Nantes, France. [Finlay, Christopher C.; Olsen, Nils; Toffner-Clausen, Lars] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Beggan, Ciaran D.; Hamilton, Brian; Macmillan, Susan; Ridley, Victoria; Thomson, Alan] British Geol Survey, Edinburgh EH9 3LA, Midlothian, Scotland. [Alken, Patrick; Chulliat, Arnaud; Manoj, Chandrasekharan; Maus, Stefan] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Alken, Patrick; Chulliat, Arnaud; Manoj, Chandrasekharan] NOAA, NCEI, Boulder, CO 80305 USA. [Aubert, Julien; Brocco, Laura; Coisson, Pierdavide; Fournier, Alexandre; Hulot, Gauthier; Lalanne, Xavier; Sirol, Olivier; Vigneron, Pierre] Univ Paris Diderot, CNRS, Inst Phys Globe Paris, Sorbonne Paris Cite, F-75005 Paris, France. [Barrois, Olivier; Gillet, Nicolas] Univ Grenoble Alpes, CNRS, ISTerre, F-38041 Grenoble, France. [Bertrand, Francois; Boness, Axel; Jager, Thomas; Leger, Jean-Michel] Univ Grenoble Alpes, F-38000 Grenoble, France. [Bertrand, Francois; Boness, Axel; Jager, Thomas; Leger, Jean-Michel] CEA, LETI, F-38054 Grenoble, France. [Bondar, Tatiana; Petrov, Valeriy; Zvereva, Tatiana] IZMIRAN, Pushkov Inst Terr Magnetism Ionosphere & Radio Wa, Moscow, Russia. [Canet, Elisabeth] ETH, Inst Geophys, Earth & Planetary Magnetism Grp, CH-8093 Zurich, Switzerland. [Chambodut, Aude] Univ Strasbourg, CNRS, EOST, Inst Phys Globe Strasbourg,UMR 7516, Strasbourg, France. [Du, Aimin] Chinese Acad Sci, Inst Geol & Geophys, Key Lab Earth & Planetary Phys, Beijing 100029, Peoples R China. [Fratter, Isabelle] Ctr Natl Etudes Spati, F-31400 Toulouse, France. [Hamoudi, Mohamed; Korte, Monika; Lesur, Vincent; Rother, Martin; Schachtschneider, Reyko; Wardinski, Ingo] GFZ German Res Ctr Geosci Telegrafenberg, D-14473 Potsdam, Germany. [Sabaka, Terence J.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Lowes, Frank J.] Newcastle Univ, Sch Chem, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. [Mandea, Mioara] CNES, F-75001 Paris, France. [Hamoudi, Mohamed] Univ Algiers, USTHB, Dept Geophys, Algiers, Algeria. [Tangborn, Andrew] UMBC, Joint Ctr Earth Syst Technol, Baltimore, MD USA. RP Thebault, E (reprint author), Univ Nantes, CNRS, Lab Planetol & Geodynam Nantes, UMR 6112, 1 Chem Houssiniere, F-44322 Nantes, France. EM erwan.thebault@univ-nantes.fr RI MANDEA, Mioara/E-4892-2012; CHAMBODUT, Aude/E-9615-2017; Thebault, Erwan/A-5670-2011; Aubert, Julien/A-5616-2011; Hulot, Gauthier/A-5627-2011; Korte, Monika/A-6086-2009; Chulliat, Arnaud/A-5747-2011; Coisson, Pierdavide/C-5942-2012; Lesur, Vincent/H-1031-2012; Olsen, Nils/H-1822-2011; Finlay, Christopher/B-5062-2014; Langlais, Benoit/K-5366-2012; Fournier, Alexandre/A-5774-2011; Kuang, Weijia/K-5141-2012 OI CHAMBODUT, Aude/0000-0001-8793-1315; Toffner-Clausen, Lars/0000-0003-4314-3776; Aubert, Julien/0000-0002-2756-0724; Korte, Monika/0000-0003-2970-9075; Chulliat, Arnaud/0000-0001-7414-9631; Coisson, Pierdavide/0000-0003-4155-2111; Lesur, Vincent/0000-0003-2568-320X; Olsen, Nils/0000-0003-1132-6113; Finlay, Christopher/0000-0002-4592-2290; Langlais, Benoit/0000-0001-5207-304X; Fournier, Alexandre/0000-0003-3276-0496; Kuang, Weijia/0000-0001-7786-6425 FU CHAMP mission by the German Aerospace Center (DLR); Federal Ministry of Education and Research; Danish Government; NASA; ESA; CNES; DARA; Thomas B. Thriges Foundation; Centre National des Etudes Spatiales (CNES) within the context of the project of the 'Travaux preparatoires et exploitation de la mission Swarm'; NSF; French 'Agence Nationale de la Recherche' [ANR-11-BS56-011]; Region Pays de Loire, France; DFG [SPP 1488] FX The institutes that support magnetic observatories together with INTERMAGNET are thanked for promoting high standards of observatory practice and prompt reporting. The support of the CHAMP mission by the German Aerospace Center (DLR) and the Federal Ministry of Education and Research is gratefully acknowledged. The Orsted Project was made possible by extensive support from the Danish Government, NASA, ESA, CNES, DARA, and the Thomas B. Thriges Foundation. The authors also acknowledge ESA for providing access to the Swarm L1b data. E. Canet acknowledges the support of ESA through the Support to Science Element (STSE) program. This work was partly funded by the Centre National des Etudes Spatiales (CNES) within the context of the project of the 'Travaux preparatoires et exploitation de la mission Swarm.' W. Kuang and A. Tangborn were funded by NASA and the NSF. This work was partly supported by the French 'Agence Nationale de la Recherche' under the grant ANR-11-BS56-011 and by the Region Pays de Loire, France. I. Wardinski was supported by the DFG through SPP 1488. The IGRF-12 task force finally wishes to express their gratitude to C. Manoj and A. Woods for maintaining the IGRF web pages at NGDC. This is IPGP contribution no. 3625. NR 32 TC 48 Z9 49 U1 8 U2 39 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY EI 1880-5981 J9 EARTH PLANETS SPACE JI Earth Planets Space PD MAY 27 PY 2015 VL 67 AR 79 DI 10.1186/s40623-015-0228-9 PG 19 WC Geosciences, Multidisciplinary SC Geology GA CK2IR UT WOS:000356034500001 ER PT J AU Zhang, RY Wang, GH Guo, S Zarnora, ML Ying, Q Lin, Y Wang, WG Hu, M Wang, Y AF Zhang, Renyi Wang, Gehui Guo, Song Zarnora, Misti L. Ying, Qi Lin, Yun Wang, Weigang Hu, Min Wang, Yuan TI Formation of Urban Fine Particulate Matter SO CHEMICAL REVIEWS LA English DT Review ID SECONDARY ORGANIC AEROSOL; IONIZATION MASS-SPECTROMETRY; MASTER CHEMICAL MECHANISM; PROTON-TRANSFER-REACTION; MILAGRO 2006 CAMPAIGN; CATALYZED HETEROGENEOUS REACTIONS; OH-INITIATED REACTIONS; AIR-POLLUTION SOURCES; ATMOSPHERIC NANOPARTICLE GROWTH; THERMODYNAMIC-EQUILIBRIUM MODEL C1 [Zhang, Renyi; Wang, Gehui; Guo, Song; Zarnora, Misti L.; Lin, Yun; Wang, Weigang] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. [Zhang, Renyi; Wang, Gehui; Guo, Song; Zarnora, Misti L.; Lin, Yun; Wang, Weigang] Texas A&M Univ, Dept Chem, College Stn, TX 77843 USA. [Zhang, Renyi; Guo, Song; Hu, Min] Peking Univ, Coll Environm Sci & Engn, State Key Joint Lab Environm Simulat & Pollut Con, Beijing 100871, Peoples R China. [Wang, Gehui] Chinese Acad Sci, Inst Earth Environm, State Key Lab Loess & Quaternary Geol, Key Lab Aerosol Phys & Chem, Beijing 100864, Peoples R China. [Wang, Weigang] Chinese Acad Sci, Inst Chem, State Key Lab Struct Chem Unstable & Stable Spec, BNLMS, Beijing 100864, Peoples R China. [Wang, Yuan] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Zhang, RY (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. EM Renyi-zhang@tamu.edu RI Wang, Weigang/L-1786-2013; Guo, Song/D-9218-2012; Zhang, Renyi/A-2942-2011; OI Guo, Song/0000-0002-9661-2313; Lin, Yun/0000-0001-8222-0346 FU Robert A. Welch Foundation [A-1417]; Ministry of Science and Technology of China [2013CB955800]; collaborative research program by Texas AM University; National Natural Science Foundation of China [41227805, 21190052]; Texas A&M University-Weizmann Collaborative Program; Strategic Priority Research Program of the Chinese Academy of Sciences [41325014, XDA05100103, XDB05020401]; Visiting Scholar Program by the Chinese Academy of Science; National Basic Research Program, China Ministry of Science and Technology [2013CB228503]; NASA ROSES10-COUND program FX This work was supported by the Robert A. Welch Foundation (Grant A-1417), the Ministry of Science and Technology of China (Grant 2013CB955800), a collaborative research program by Texas A&M University and the National Natural Science Foundation of China, and a Texas A&M University-Weizmann Collaborative Program. G.W. acknowledged the National Natural Science Foundation of China and the Strategic Priority Research Program of the Chinese Academy of Sciences for financial support (Grants 41325014, XDA05100103, and XDB05020401). W.W. acknowledged financial support for the Visiting Scholar Program by the Chinese Academy of Science and the National Natural Science Foundation of China (Grant 41227805). M.H. was supported by the National Basic Research Program, China Ministry of Science and Technology (Grant 2013CB228503), and National Natural Science Foundation of China (21190052). Y.W. was supported by the NASA ROSES10-COUND program. We were grateful to Professor A. R. Ravishankara of Colorado State University, Professor of Robert D. Kuchta of University of Colorado at Boulder, and Dr. Sasha Madronich of NCAR for helpful suggestions and discussions. NR 485 TC 76 Z9 79 U1 72 U2 289 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0009-2665 EI 1520-6890 J9 CHEM REV JI Chem. Rev. PD MAY 27 PY 2015 VL 115 IS 10 BP 3803 EP 3855 DI 10.1021/acs.chemrev.5b00067 PG 53 WC Chemistry, Multidisciplinary SC Chemistry GA CJ3KZ UT WOS:000355383900005 PM 25942499 ER PT J AU Fujishima, K Venter, C Wang, K Ferreira, R Rothschild, LJ AF Fujishima, Kosuke Venter, Chris Wang, Kendrick Ferreira, Raphael Rothschild, Lynn J. TI An overhang-based DNA block shuffling method for creating a customized random library SO SCIENTIFIC REPORTS LA English DT Article ID IN-VITRO SELECTION; PROTEINS; EVOLUTION; DISPLAY; REPEATS; DESIGN; GALAXY AB We present an overhang-based DNA block shuffling method to create a customized random DNA library with flexible sequence design and length. Our method enables the efficient and seamless assembly of short DNA blocks with dinucleotide overhangs through a simple ligation process. Next generation sequencing analysis of the assembled DNA library revealed that ligation was accurate, directional and unbiased. This straightforward DNA assembly method should fulfill the versatile needs of both in vivo and in vitro functional screening of random peptides and RNA created with a desired amino acid and nucleotide composition, as well as making highly repetitive gene constructs that are difficult to synthesize de novo. C1 [Fujishima, Kosuke] Univ Affiliated Res Ctr, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Venter, Chris; Wang, Kendrick] NASA, Ames Res Ctr, NASA Educ Associates Program EAP, Moffett Field, CA 94035 USA. [Wang, Kendrick] Stanford Univ, Dept Bioengn, Stanford, CA 94305 USA. [Ferreira, Raphael] Univ Paris 07, Diderot, France. [Rothschild, Lynn J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Fujishima, K (reprint author), Univ Affiliated Res Ctr, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM kosuke.fujishima@nasa.gov; lynn.j.rothschild@nasa.gov OI Fujishima, Kosuke/0000-0002-8844-812X FU NASA Ames Directors Discretionary Fund; NASA Ames Science Innovation Fund FX We thank Russell Durrett for helping the DNA sequence analysis and Ryan Kent for reviewing the final manuscript. We are grateful to the NASA Ames Directors Discretionary Fund and the NASA Ames Science Innovation Fund for support. NR 17 TC 0 Z9 0 U1 1 U2 12 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 MAY 26 PY 2015 VL 5 AR 9740 DI 10.1038/srep09740 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CJ5KT UT WOS:000355527000001 PM 26010273 ER PT J AU Bahr, CJ Zawodny, NS Bertolucci, B Li, J Sheplak, M Cattafesta, LN AF Bahr, Christopher J. Zawodny, Nikolas S. Bertolucci, Brandon Li, Jian Sheplak, Mark Cattafesta, Louis N. TI A plasma-based non-intrusive point source for acoustic beamforming applications SO JOURNAL OF SOUND AND VIBRATION LA English DT Article ID SHEAR-LAYER; SPACE; SOUND AB A laser-generated plasma acoustic point source is used to directly measure the point spread function (PSF) of a microphone phased array. In beamforming analysis of microphone phased array data, the true acoustic field is convolved with the array's PSF. By directly measuring the PSF, corrections to the array analysis can be computed and applied. The acoustic source is measured in an open-jet aeroacoustic facility to evaluate the effects of sampling rate, microphone installation, source shift, reflections, shear layer refraction and model presence. Results show that measurements exhibit behavior consistent with theory with regard to source shift and shear layer refraction. Application of a measured PSF in beamforming analysis shows that the process provides an effective in situ method for array calibration both with and without flow and allows for corrections to incorporate reflections and scattering. The technique improves the agreement of beamforming results with the true spectrum of a known source, especially in the presence of reflections. Published by Elsevier Ltd. C1 [Bahr, Christopher J.; Zawodny, Nikolas S.] NASA, Langley Res Ctr, Aeroacoust Branch, Hampton, VA 23665 USA. [Bertolucci, Brandon] Boeing Aircraft Co, Boeing ANP Labs, Seattle, WA USA. [Li, Jian] Univ Florida, Dept Elect & Comp Engn, Gainesville, FL USA. [Sheplak, Mark] Univ Florida, Dept Mech & Aerosp Engn, Gainesville, FL USA. [Cattafesta, Louis N.] Florida State Univ, Dept Mech Engn, Tallahassee, FL 32306 USA. RP Bahr, CJ (reprint author), NASA, Langley Res Ctr, Aeroacoust Branch, Hampton, VA 23665 USA. EM christophor.j.bahr@nasa.gov OI Bahr, Christopher/0000-0002-3095-4265 FU Florida Center for Advanced Aero-Propulsion FX The authors acknowledge the financial support provided by the Florida Center for Advanced Aero-Propulsion. They thank Dr. Fei Liu, Kyle Woolwine, and Derek Dussault for their efforts in this research, along with James Underbrink for extensive discussion of array measurement techniques and his input on this body of work. NR 33 TC 4 Z9 4 U1 1 U2 11 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0022-460X EI 1095-8568 J9 J SOUND VIB JI J. Sound Vibr. PD MAY 26 PY 2015 VL 344 BP 59 EP 80 DI 10.1016/j.jsv.2015.01.023 PG 22 WC Acoustics; Engineering, Mechanical; Mechanics SC Acoustics; Engineering; Mechanics GA CD3RJ UT WOS:000350997600005 ER PT J AU Johnson, CL Phillips, RJ Purucker, ME Anderson, BJ Byrne, PK Denevi, BW Feinberg, JM Hauck, SA Head, JW Korth, H James, PB Mazarico, E Neumann, GA Philpott, LC Siegler, MA Tsyganenko, NA Solomon, SC AF Johnson, Catherine L. Phillips, Roger J. Purucker, Michael E. Anderson, Brian J. Byrne, Paul K. Denevi, Brett W. Feinberg, Joshua M. Hauck, Steven A., II Head, James W., III Korth, Haje James, Peter B. Mazarico, Erwan Neumann, Gregory A. Philpott, Lydia C. Siegler, Matthew A. Tsyganenko, Nikolai A. Solomon, Sean C. TI Low-altitude magnetic field measurements by MESSENGER reveal Mercury's ancient crustal field SO SCIENCE LA English DT Article ID THERMOCHEMICAL EVOLUTION; GLOBAL CONTRACTION; ORIGIN; SURFACE; PLAINS; ORBIT AB Magnetized rocks can record the history of the magnetic field of a planet, a key constraint for understanding its evolution. From orbital vector magnetic field measurements of Mercury taken by the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft at altitudes below 150 kilometers, we have detected remanent magnetization in Mercury's crust. We infer a lower bound on the average age of magnetization of 3.7 to 3.9 billion years. Our findings indicate that a global magnetic field driven by dynamo processes in the fluid outer core operated early in Mercury's history. Ancient field strengths that range from those similar to Mercury's present dipole field to Earth-like values are consistent with the magnetic field observations and with the low iron content of Mercury's crust inferred from MESSENGER elemental composition data. C1 [Johnson, Catherine L.; Philpott, Lydia C.] Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V6T 1Z4, Canada. [Johnson, Catherine L.; Siegler, Matthew A.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Phillips, Roger J.] Southwest Res Inst, Planetary Sci Directorate, Boulder, CO 80302 USA. [Purucker, Michael E.; Mazarico, Erwan; Neumann, Gregory A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Anderson, Brian J.; Denevi, Brett W.; Korth, Haje] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Byrne, Paul K.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Feinberg, Joshua M.] Univ Minnesota, Inst Rock Magnetism, Dept Earth Sci, Minneapolis, MN 55455 USA. [Hauck, Steven A., II] Case Western Reserve Univ, Dept Earth Environm & Planetary Sci, Cleveland, OH 44106 USA. [Head, James W., III] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA. [James, Peter B.; Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Siegler, Matthew A.] So Methodist Univ, Dept Earth Sci, Dallas, TX 75205 USA. [Tsyganenko, Nikolai A.] St Petersburg State Univ, Inst & Fac Phys, St Petersburg 199034, Russia. [Byrne, Paul K.; Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. RP Johnson, CL (reprint author), Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V6T 1Z4, Canada. EM cjohnson@eos.ubc.ca RI Denevi, Brett/I-6502-2012; Mazarico, Erwan/N-6034-2014; Neumann, Gregory/I-5591-2013; Hauck, Steven/A-7865-2008; Tsyganenko, Nikolai/J-7377-2012; OI Denevi, Brett/0000-0001-7837-6663; Mazarico, Erwan/0000-0003-3456-427X; Neumann, Gregory/0000-0003-0644-9944; Hauck, Steven/0000-0001-8245-146X; Tsyganenko, Nikolai/0000-0002-5938-1579; Philpott, Lydia/0000-0002-5286-8528 FU NASA Discovery Program; MESSENGER Participating Scientist Program; Natural Sciences and Engineering Research Council of Canada FX We thank the MESSENGER operations and engineering teams for enabling the low-altitude observations reported here. We are also grateful for the contributions of our friend and colleague M. H. Acuna whose expertise was critical to the Magnetometer development. The MESSENGER mission is supported by the NASA Discovery Program and the MESSENGER Participating Scientist Program. C.L.J. and L.C.P. also acknowledge support from the Natural Sciences and Engineering Research Council of Canada. Data from the MESSENGER mission are archived with the NASA Planetary Data System. We thank three reviewers for thoughtful comments that improved the manuscript. NR 29 TC 15 Z9 15 U1 4 U2 20 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 MAY 22 PY 2015 VL 348 IS 6237 BP 892 EP 895 DI 10.1126/science.aaa8720 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CI6NW UT WOS:000354877900039 PM 25953822 ER PT J AU Kuin, NPM Landsman, W Breeveld, AA Page, MJ Lamoureux, H James, C Mehdipour, M Still, M Yershov, V Brown, PJ Carter, M Mason, KO Kennedy, T Marshall, F Roming, PWA Siegel, M Oates, S Smith, PJ De Pasquale, M AF Kuin, N. P. M. Landsman, W. Breeveld, A. A. Page, M. J. Lamoureux, H. James, C. Mehdipour, M. Still, M. Yershov, V. Brown, P. J. Carter, M. Mason, K. O. Kennedy, T. Marshall, F. Roming, P. W. A. Siegel, M. Oates, S. Smith, P. J. De Pasquale, M. TI Calibration of the Swift-UVOT ultraviolet and visible grisms SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE instrumentation: spectrographs; space vehicles: instruments; techniques: imaging spectroscopy ID WOLF-RAYET STARS; DYNAMIC-RANGE; TELESCOPE; SPECTROPHOTOMETRY; SPECTROSCOPY; PERFORMANCE; MISSION; CATALOG; ATLAS AB We present the calibration of the Swift Ultraviolet and Optical Telescope (UVOT) grisms, of which there are two, providing low-resolution field spectroscopy in the ultraviolet and optical bands, respectively. The UV grism covers the range lambda 1700-5000 angstrom with a spectral resolution (lambda/Delta lambda) of 75 at lambda 2600 angstrom for source magnitudes of u= 10-16 mag, while the visible grism covers the range lambda 2850-6600 angstrom with a spectral resolution of 100 at lambda 4000 angstrom for source magnitudes of b=12-17 mag. This calibration extends over all detector positions, for all modes used during operations. The wavelength accuracy (1 sigma) is 9 angstrom in the UV grism clocked mode, 17 angstrom in the UV grism nominal mode and 22 angstrom in the visible grism. The range below lambda 2740 angstrom in the UV grism and lambda 5200 angstrom in the visible grism never suffers from overlapping by higher spectral orders. The flux calibration of the grisms includes a correction we developed for coincidence loss in the detector. The error in the coincidence loss correction is less than 20 per cent. The position of the spectrum on the detector only affects the effective area (sensitivity) by a fewper cent in the nominal modes, but varies substantially in the clocked modes. The error in the effective area is from 9 per cent in the UV grism clocked mode to 15 per cent in the visible grism clocked mode C1 [Kuin, N. P. M.; Breeveld, A. A.; Page, M. J.; Lamoureux, H.; James, C.; Mehdipour, M.; Yershov, V.; Carter, M.; Kennedy, T.; Oates, S.; De Pasquale, M.] Univ Coll London, Mullard Space Sci Lab, Surrey RH5 6NT, England. [Landsman, W.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Still, M.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. [Brown, P. J.] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Mason, K. O.] Harwell Oxford, Satellite Applicat Catapult, Harwell OX11 0QR, Berks, England. [Marshall, F.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Roming, P. W. A.; Siegel, M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Roming, P. W. A.] Southwest Res Inst, Space Sci & Engn Div, San Antonio, TX 78228 USA. [Roming, P. W. A.] Univ Texas San Antonio, Phys & Astron Dept, San Antonio, TX 78249 USA. [Oates, S.] Inst Astrofs Andalucia IAA CSIC, E-18008 Granada, Spain. [De Pasquale, M.] IASF Palermo, I-90146 Palermo, Italy. RP Kuin, NPM (reprint author), Univ Coll London, Mullard Space Sci Lab, Surrey RH5 6NT, England. EM npkuin@gmail.com FU UK Space Agency; PSU by NASA [NAS5-00136] FX Throughout the calibration many people provided feedback and helped refine the understanding of what was possible and what could be improved through their use of the grisms for observational studies. We wish to thank all of them for their efforts, help and patience. A special thanks goes to all the Swift planners who through their effort ensured the success of this calibration. The optical design of the grisms was by the late Richard Bingham. We are grateful to Fred Walter, Ed Sion, and Greg Schwartz for sharing their HST and optical spectra, some of which were taken during several Swift-HST observing campaigns, which helped the calibration effort. This work was supported by the UK Space Agency through a grant for Swift Post Launch Support at UCL-MSSL. This work is sponsored at PSU by NASA contract NAS5-00136. We acknowledge the use of data from the SIMBAD and Vizier data bases at the CDS in Strassbourg, the online WR spectra from Hamann, the STScI MAST and HLA archive, the ESA INES IUE archive, the HEASARC archives, and the NIST atomic data base on the WWW. We used 'Astropy', a community-developed core PYTHON package for Astronomy (Astropy Collaboration, 2013). NR 32 TC 6 Z9 6 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 21 PY 2015 VL 449 IS 3 BP 2514 EP 2538 DI 10.1093/mnras/stv408 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2TP UT WOS:000355337800025 ER PT J AU Gullberg, B De Breuck, C Vieira, JD Weiss, A Aguirre, JE Aravena, M Bethermin, M Bradford, CM Bothwell, MS Carlstrom, JE Chapman, SC Fassnacht, CD Gonzalez, AH Greve, TR Hezaveh, Y Holzapfel, WL Husband, K Ma, J Malkan, M Marrone, DP Menten, K Murphy, EJ Reichardt, CL Spilker, JS Stark, AA Strandet, M Welikala, N AF Gullberg, B. De Breuck, C. Vieira, J. D. Weiss, A. Aguirre, J. E. Aravena, M. Bethermin, M. Bradford, C. M. Bothwell, M. S. Carlstrom, J. E. Chapman, S. C. Fassnacht, C. D. Gonzalez, A. H. Greve, T. R. Hezaveh, Y. Holzapfel, W. L. Husband, K. Ma, J. Malkan, M. Marrone, D. P. Menten, K. Murphy, E. J. Reichardt, C. L. Spilker, J. S. Stark, A. A. Strandet, M. Welikala, N. TI The nature of the [C II] emission in dusty star-forming galaxies from the SPT survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: high-redshift; galaxies: ISM; galaxies: starburst; infrared: galaxies; submillimetre: galaxies ID 158 MU-M; ULTRALUMINOUS INFRARED GALAXIES; SOUTH-POLE TELESCOPE; LUMINOUS SUBMILLIMETER GALAXIES; SPACE-OBSERVATORY MEASUREMENTS; ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT GALAXIES; MICRON LINE DEFICIT; HUBBLE DEEP FIELD; SIMILAR-TO 1-2 AB We present [C II] observations of 20 strongly lensed dusty star-forming galaxies at 2.1 < z < 5.7 using Atacama Pathfinder EXperiment and Herschel. The sources were selected on their 1.4 mm flux (S-1.4mm > 20 mJy) from the South Pole Telescope (SPT) survey, with far-infrared (FIR) luminosities determined from extensive photometric data. The [CII] line is robustly detected in 17 sources, all but one being spectrally resolved. 11 out of 20 sources observed in [C II] also have low-J CO detections from Australia Telescope Compact Array. A comparison with mid-and high-J CO lines from Atacama Large Millimeter/submillimeter Array reveals consistent [C II] and CO velocity profiles, suggesting that there is little differential lensing between these species. The [C II], low-J CO and FIR data allow us to constrain the properties of the interstellar medium. We find [C II] to CO(1-0) luminosity ratios in the SPT sample of 5200 +/- 1800, with significantly less scatter than in other samples. This line ratio can be best described by a medium of [C II] and CO emitting gas with a higher [C II] than CO excitation temperature, high CO optical depth tau(CO)(1-0) >> 1, and low to moderate [CII] optical depth tau[C II] less than or similar to 1. The geometric structure of photodissociation regions allows for such conditions. C1 [Gullberg, B.; De Breuck, C.; Bethermin, M.] European So Observ, D-85748 Garching, Germany. [Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Vieira, J. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Weiss, A.; Menten, K.; Strandet, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Aguirre, J. E.] Univ Penn, Philadelphia, PA 19104 USA. [Aravena, M.] European So Observ, Santiago 19, Chile. [Aravena, M.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile. [Bradford, C. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bothwell, M. S.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HA, England. [Carlstrom, J. E.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Carlstrom, J. E.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Chapman, S. C.] Dalhousie Univ, Halifax, NS B3H 4R2, Canada. [Fassnacht, C. D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Gonzalez, A. H.; Ma, J.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Greve, T. R.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Hezaveh, Y.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Holzapfel, W. L.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Husband, K.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Marrone, D. P.; Spilker, J. S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Murphy, E. J.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Welikala, N.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. RP Gullberg, B (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM bgullber@eso.org RI Holzapfel, William/I-4836-2015; OI Marrone, Daniel/0000-0002-2367-1080; De Breuck, Carlos/0000-0002-6637-3315; Stark, Antony/0000-0002-2718-9996 FU National Aeronautics and Space Administration; Commonwealth of Australia; US National Science Foundation [AST-1312950]; National Science Foundation [PLR-1248097]; NSF Physics Frontier Center [PHY-1125897]; Kavli Foundation; Gordon and Betty Moore Foundation [GBMF 947] FX This publication is based on data acquired with the APEX. APEX is a collaboration between the Max-Planck-Institut fur Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory. This paper makes use of the following ALMA data: ADS/JAO. ALMA#2011.0.00957.S, ADS/JAO.ALMA#2011.0.00958.S and ADS/JAO. ALMA#2012.1.00844.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 Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The ATCA is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. This research has made use of the NED which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of NASA's Astrophysics Data System Bibliographic Services; This material is based on work supported by the US National Science Foundation under grant no. AST-1312950. The SPT is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation grant GBMF 947. NR 126 TC 18 Z9 18 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 21 PY 2015 VL 449 IS 3 BP 2883 EP 2900 DI 10.1093/mnras/stv372 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2TP UT WOS:000355337800055 ER PT J AU Littlejohns, OM Butler, NR Cucchiara, A Watson, AM Fox, OD Lee, WH Kutyrev, AS Richer, MG Klein, CR Prochaska, JX Bloom, JS Troja, E Ramirez-Ruiz, E de Diego, JA Georgiev, L Gonzalez, J Roman-Zuniga, CG Gehrels, N Moseley, H AF Littlejohns, O. M. Butler, N. R. Cucchiara, A. Watson, A. M. Fox, O. D. Lee, W. H. Kutyrev, A. S. Richer, M. G. Klein, C. R. Prochaska, J. X. Bloom, J. S. Troja, E. Ramirez-Ruiz, E. de Diego, J. A. Georgiev, L. Gonzalez, J. Roman-Zuniga, C. G. Gehrels, N. Moseley, H. TI A detailed study of the optical attenuation of gamma-ray bursts in the Swift era SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gamma-ray bursts: general; galaxies: distances and redshifts; galaxies: ISM ID DIGITAL SKY SURVEY; WIDE-FIELD CAMERA; X-RAY; COLUMN DENSITIES; COMPLETE SAMPLE; LIGHT CURVES; PHOTOMETRIC REDSHIFT; INTERSTELLAR-MEDIUM; AFTERGLOW EMISSION; GLOBULAR-CLUSTERS AB We present optical and near-infrared (NIR) photometry of 28 gamma-ray bursts (GRBs) detected by the Swift satellite and rapidly observed by the Reionization and Transients Infrared/Optical (RATIR) camera. We compare the optical flux at fiducial times of 5.5 and 11 h after the high-energy trigger to that in the X-ray regime to quantify optical darkness. 46 +/- 9 per cent (13/28) of all bursts in our sample and 55 +/- 10 per cent (13/26) of long GRBs are optically dark, which is statistically consistently with previous studies. Fitting RATIR optical and NIR spectral energy distributions of 19 GRBs, most (6/7) optically dark GRBs either occur at high redshift (z > 4.5) or have a high dust content in their host galaxies (A(V) > 0.3). Performing Kolmogorov-Smirnov tests, we compare the RATIR sample to those previously presented in the literature, finding our distributions of redshift, optical darkness, host dust extinction and X-ray-derived column density to be consistent. The one reported discrepancy is with host galaxy dust content in the BAT6 sample, which appears inconsistent with our sample and other previous literature. Comparing X-ray-derived host galaxy hydrogen column densities to host galaxy dust extinction, we find that GRBs tend to occur in host galaxies with a higher metal-to-dust ratio than our own Galaxy, more akin to the Large and Small Magellanic Clouds. Finally, to mitigate time evolution of optical darkness, we measure beta(OX, rest) at a fixed rest-frame time, t(rest) = 1.5 h and fixed rest-frame energies in the X-ray and optical regimes. Choosing to evaluate optical flux at lambda(rest) = 0.25 mu m, we remove high redshift as a source of optical darkness, demonstrating that optical darkness must result from either high redshift, dust content in the host galaxy along the GRB sight line, or a combination of the two. C1 [Littlejohns, O. M.; Butler, N. R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Cucchiara, A.; Kutyrev, A. S.; Troja, E.; Gehrels, N.; Moseley, H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Watson, A. M.; Lee, W. H.; de Diego, J. A.; Georgiev, L.; Gonzalez, J.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Fox, O. D.; Klein, C. R.; Bloom, J. S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Richer, M. G.; Roman-Zuniga, C. G.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico. [Prochaska, J. X.; Ramirez-Ruiz, E.] Univ Calif Santa Cruz, UCO Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Littlejohns, OM (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. EM owenlittlejohns@gmail.com; natbutler@asu.edu RI Roman-Zuniga, Carlos/F-6602-2016; Gonzalez, Jose/L-6687-2014 OI Roman-Zuniga, Carlos/0000-0001-8600-4798; Gonzalez, Jose/0000-0002-3724-1583 FU NASA [NNX09AH71G, NNX09AT02G, NNX10AI27G, NNX12AE66G]; CONACyT [INFR-2009-01-122785, CB-2008-101958]; UNAM PAPIIT [IN113810]; UC MEXUS-CONACyT [CN 09-283]; NASA Postdoctoral Programme at the Goddard Space Flight Center; NASA FX We thank Pall Jakobsson for useful comments and suggestions on the manuscript. We also thank Jochen Greiner for supplying us with detailed data related to Greiner et al. (2011). We thank the RATIR project team and the staff of the Observatorio Astronomico Nacional on Sierra San Pedro Martir. RATIR is a collaboration between the University of California, the Universidad Nacional Autonoma de Mexico, NASA Goddard Space Flight Center and Arizona State University, benefiting from the loan of an H2RG detector and hardware and software support from Teledyne Scientific and Imaging. RATIR, the automation of the Harold L. Johnson Telescope of the Observatorio Astronomico Nacional on Sierra San Pedro Martir, and the operation of both are funded through NASA grants NNX09AH71G, NNX09AT02G, NNX10AI27G and NNX12AE66G, CONACyT grants INFR-2009-01-122785 and CB-2008-101958, UNAM PAPIIT grant IN113810 and UC MEXUS-CONACyT grant CN 09-283. AC is supported by the NASA Postdoctoral Programme at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. This work made use of data supplied by the UKSSDC at the University of Leicester. NR 107 TC 4 Z9 4 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 21 PY 2015 VL 449 IS 3 BP 2919 EP 2936 DI 10.1093/mnras/stv479 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2TP UT WOS:000355337800058 ER PT J AU Littlefield, C Mukai, K Mumme, R Cain, R Magno, KC Corpuz, T Sandefur, D Boyd, D Cook, M Ulowetz, J Martinez, L AF Littlefield, Colin Mukai, Koji Mumme, Raymond Cain, Ryan Magno, Katrina C. Corpuz, Taylor Sandefur, Davis Boyd, David Cook, Michael Ulowetz, Joseph Martinez, Luis TI Periodic eclipse variations in asynchronous polar V1432 Aql: evidence of a shifting threading region SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; stars: individual: V1432 Aql; stars: individual: RX J1940.1-1025; stars: magnetic field; novae, cataclysmic variables; white dwarfs ID NEAR-SYNCHRONOUS POLAR; ACCRETION GEOMETRY; RX J1940.1-1025; HU AQUARII; OLD NOVA; SYNCHRONIZATION; AM; AQUILAE; DWARF; CYGNI AB We report the results of a 28-month photometric campaign studying V1432 Aql, the only known eclipsing, asynchronous polar. Our data show that both the residual eclipse flux and eclipse O-C timings vary strongly as a function of the spin-orbit beat period. Relying upon a new model of the system, we show that cyclical changes in the location of the threading region along the ballistic trajectory of the accretion stream could produce both effects. This model predicts that the threading radius is variable, in contrast to previous studies which have assumed a constant threading radius. Additionally, we identify a very strong photometric maximum which is only visible for half of the beat cycle. The exact cause of this maximum is unclear, but we consider the possibility that it is the optical counterpart of the third accreting polecap proposed by Rana et al. Finally, the rate of change of the white dwarf's spin period is consistent with it being proportional to the difference between the spin and orbital periods, implying that the spin period is approaching the orbital period asymptotically. C1 [Littlefield, Colin; Mumme, Raymond; Cain, Ryan; Magno, Katrina C.; Corpuz, Taylor; Sandefur, Davis] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Littlefield, Colin] Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA. [Mukai, Koji] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Mukai, Koji] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Mukai, Koji] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. [Boyd, David] CBA Oxford, W Challow OX12 9TX, Wantage, England. [Cook, Michael] Newcastle Observ, CBA Ontario, Newcastle, ON L1B 1M5, Canada. [Ulowetz, Joseph] CBA Illinois, Northbrook, IL 60062 USA. [Martinez, Luis] Lenomiya Observ, Casa Grande, AZ 85122 USA. RP Littlefield, C (reprint author), Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. EM clittlef@alumni.nd.edu; koji.mukai@nasa.gov NR 36 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 MAY 21 PY 2015 VL 449 IS 3 BP 3107 EP 3120 DI 10.1093/mnras/stv462 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2TP UT WOS:000355337800070 ER PT J AU Kennedy, GM Matra, L Marmier, M Greaves, JS Wyatt, MC Bryden, G Holland, W Lovis, C Matthews, BC Pepe, F Sibthorpe, B Udry, S AF Kennedy, Grant M. Matra, Luca Marmier, Maxime Greaves, Jane S. Wyatt, Mark C. Bryden, Geoffrey Holland, Wayne Lovis, Christophe Matthews, Brenda C. Pepe, Francesco Sibthorpe, Bruce Udry, Stephane TI Kuiper belt structure around nearby super-Earth host stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE planet-disc interactions; circumstellar matter; stars: individual: 61 Vir; stars: individual: HD 20794; stars: individual: HD 38858; stars: individual: HD 69830 ID INFRARED INTERFEROMETRIC SURVEY; GENEVA-COPENHAGEN SURVEY; STEADY-STATE EVOLUTION; NEPTUNE-MASS PLANETS; MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; SUN-LIKE STARS; DEBRIS DISKS; CIRCUMSTELLAR DISK; BETA-PICTORIS AB We present new observations of the Kuiper belt analogues around HD 38858 and HD 20794, hosts of super-Earth mass planets within 1 au. As two of the four nearby G-type stars (with HD 69830 and 61 Vir) that form the basis of a possible correlation between low-mass planets and debris disc brightness, these systems are of particular interest. The disc around HD 38858 is well resolved with Herschel and we constrain the disc geometry and radial structure. We also present a probable James Clerk Maxwell Telescope sub-mm continuum detection of the disc and a CO J = 2-1 upper limit. The disc around HD 20794 is much fainter and appears marginally resolved with Herschel, and is constrained to be less extended than the discs around 61 Vir and HD 38858. We also set limits on the radial location of hot dust recently detected around HD 20794 with near-IR interferometry. We present High Accuracy Radial velocity Planet Searcher upper limits on unseen planets in these four systems, ruling out additional super-Earths within a few au, and Saturn-mass planets within 10 au. We consider the disc structure in the three systems with Kuiper belt analogues (HD 69830 has only a warm dust detection), concluding that 61 Vir and HD 38858 have greater radial disc extent than HD 20794. We speculate that the greater width is related to the greater minimum planet masses (10-20 M-circle plus versus 3-5 M-circle plus), arising from an eccentric planetesimal population analogous to the Solar system's scattered disc. We discuss alternative scenarios and possible means to distinguish among them. C1 [Kennedy, Grant M.; Matra, Luca; Wyatt, Mark C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Matra, Luca] ESO Vitacura, Santiago 19001, Chile. [Marmier, Maxime; Lovis, Christophe; Pepe, Francesco; Udry, Stephane] Univ Geneva, Dept Astron, CH-1290 Versoix, Switzerland. [Greaves, Jane S.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Bryden, Geoffrey] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Holland, Wayne] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Holland, Wayne] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Matthews, Brenda C.] Natl Res Council Canada, Victoria, BC V9E 2E7, Canada. [Matthews, Brenda C.] Univ Victoria, Victoria, BC V8W 3P6, Canada. [Sibthorpe, Bruce] SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. RP Kennedy, GM (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM gkennedy@ast.cam.ac.uk OI Kennedy, Grant/0000-0001-6831-7547 FU European Union through ERC [279973]; STFC; ESO; Swiss National Science Foundation (SNSF) FX We thank the referee for a thoughtful review. This work was supported by the European Union through ERC grant number 279973 (GMK, LM, and MCW). LM also acknowledges support by both STFC and ESO through graduate studentships. MM, CL, FP, and SU acknowledge the Swiss National Science Foundation (SNSF) for the continuous support of the RV research programmes. NR 94 TC 5 Z9 5 U1 1 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 21 PY 2015 VL 449 IS 3 BP 3121 EP 3136 DI 10.1093/mnras/stv511 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2TP UT WOS:000355337800071 ER PT J AU Cao, Y Kulkarni, SR Howell, DA Gal-Yam, A Kasliwal, MM Valenti, S Johansson, J Amanullah, R Goobar, A Sollerman, J Taddia, F Horesh, A Sagiv, I Cenko, SB Nugent, PE Arcavi, I Surace, J Wozniak, PR Moody, DI Rebbapragada, UD Bue, BD Gehrels, N AF Cao, Yi Kulkarni, S. R. Howell, D. Andrew Gal-Yam, Avishay Kasliwal, Mansi M. Valenti, Stefano Johansson, J. Amanullah, R. Goobar, A. Sollerman, J. Taddia, F. Horesh, Assaf Sagiv, Ilan Cenko, S. Bradley Nugent, Peter E. Arcavi, Iair Surace, Jason Wozniak, P. R. Moody, Daniela I. Rebbapragada, Umaa D. Bue, Brian D. Gehrels, Neil TI A strong ultraviolet pulse from a newborn type Ia supernova SO NATURE LA English DT Article ID TIME OPTICAL-SPECTRA; SN 2011FE; COMPANION STAR; LOW-RESOLUTION; DATA RELEASE; SWIFT; PROGENITOR; TELESCOPE; SPECTROGRAPH; CONSTRAINTS AB Type Ia supernovae(1) are destructive explosions of carbon-oxygen white dwarfs(2,3). Although they are used empirically to measure cosmological distances(4-6), the nature of their progenitors remains mysterious(3). One of the leading progenitor models, called the single degenerate channel, hypothesizes that a white dwarf accretes matter from a companion star and the resulting increase in its central pressure and temperature ignites thermonuclear explosion(3,7,8). Here we report observations with the Swift Space Telescope of strong but declining ultraviolet emission from a type Ia supernova within four days of its explosion. This emission is consistent with theoretical expectations of collision between material ejected by the supernova and a companion star(9), and therefore provides evidence that some type Ia supernovae arise from the single degenerate channel. C1 [Cao, Yi; Kulkarni, S. R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Kulkarni, S. R.] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA. [Howell, D. Andrew; Valenti, Stefano; Arcavi, Iair] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Howell, D. Andrew; Valenti, Stefano] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Gal-Yam, Avishay; Horesh, Assaf; Sagiv, Ilan] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Kasliwal, Mansi M.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Johansson, J.; Amanullah, R.; Goobar, A.] Stockholm Univ, Dept Phys, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Sollerman, J.; Taddia, F.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Cenko, S. Bradley; Gehrels, Neil] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Nugent, Peter E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Arcavi, Iair] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Surace, Jason] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Wozniak, P. R.; Moody, Daniela I.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Rebbapragada, Umaa D.; Bue, Brian D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Cao, Y (reprint author), CALTECH, Dept Astron, Pasadena, CA 91125 USA. EM ycao@astro.caltech.edu RI Horesh, Assaf/O-9873-2016; OI Horesh, Assaf/0000-0002-5936-1156; Sollerman, Jesper/0000-0003-1546-6615; Wozniak, Przemyslaw/0000-0002-9919-3310 FU W. M. Keck Foundation; National Science Foundation; EU/FP7 via an ERC grant; "Quantum Universe" I-Core programme; ISF; Minerva and Weizmann-UK grants; Kimmel Award; Carnegie-Princeton fellowship; Swedish Research Council; Knut and Alice Wallenberg Foundation; Office of Science of the US Department of Energy [DE-AC02-05CH11231]; US Department of Energy as part of the Laboratory Directed Research and Development programme; National Aeronautics and Space Administration FX We thank A. L. Piro, M. Kromer and J. Cohen for discussions. We also thank A. Waszczak, A. Rubin, O. Yaron, A. De Cia, D. A. Perley, G. E. Duggan, O. Smirnova, S. Papadogiannakis, A. Nyholm, Y. F. Martinez and the staff at the Nordic Optical Telescope and Gemini for observation and data reduction. Some of the data presented here were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and NASA. The observatory was made possible by the generous financial support of the W. M. Keck Foundation. Some data were obtained with the Nordic Optical Telescope, which is operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain. This work also makes use of observations from the Las Cumbres Observatory Global Telescope (LCOGT) network. Research at California Institute of Technology is supported by the National Science Foundation. D.A.H. acknowledges support from the National Science Foundation. A.G.-Y. acknowledges support from the EU/FP7 via an ERC grant, the "Quantum Universe" I-Core programme, the ISF, Minerva and Weizmann-UK grants, and the Kimmel Award. M.M.K. acknowledges generous support from the Carnegie-Princeton fellowship. Supernova research at the Oskar Klein Centre is supported by the Swedish Research Council and by the Knut and Alice Wallenberg Foundation. The National Energy Research Scientific Computing Center, which is supported by the Office of Science of the US Department of Energy under contract number DE-AC02-05CH11231, provided staff, computational resources, and data storage for this project. The participation of the Los Alamos National Laboratory (LANL) in iPTF is supported by the US Department of Energy as part of the Laboratory Directed Research and Development programme. A portion of this work was carried out at the Jet Propulsion Laboratory under a Research and Technology Development Grant, under contract with the National Aeronautics and Space Administration. NR 62 TC 33 Z9 33 U1 1 U2 5 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 MAY 21 PY 2015 VL 521 IS 7552 BP 328 EP + DI 10.1038/nature14440 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CI5RM UT WOS:000354816500050 PM 25993962 ER PT J AU Brightman, M Balokovic, M Stern, D Arevalo, P Ballantyne, DR Bauer, FE Boggs, SE Craig, WW Christensen, FE Comastri, A Fuerst, F Gandhi, P Hailey, CJ Harrison, FA Hickox, RC Koss, M LaMassa, S Puccetti, S Rivers, E Vasudevan, R Walton, DJ Zhang, WW AF Brightman, M. Balokovic, M. Stern, D. Arevalo, P. Ballantyne, D. R. Bauer, F. E. Boggs, S. E. Craig, W. W. Christensen, F. E. Comastri, A. Fuerst, F. Gandhi, P. Hailey, C. J. Harrison, F. A. Hickox, R. C. Koss, M. LaMassa, S. Puccetti, S. Rivers, E. Vasudevan, R. Walton, D. J. Zhang, W. W. TI DETERMINING THE COVERING FACTOR OF COMPTON-THICK ACTIVE GALACTIC NUCLEI WITH NuSTAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 424, NGC 1068, NGC 4945, Circinus); X-rays: galaxies ID X-RAY-SPECTRA; SEYFERT 2 GALAXIES; H2O MASER EMISSION; SWIFT-BAT SURVEY; XMM-NEWTON; NGC 4945; CIRCINUS GALAXY; LUMINOSITY DEPENDENCE; OBSCURED FRACTION; TORUS MODELS AB The covering factor of Compton-thick (CT) obscuring material associated with the torus in active galactic nuclei (AGNs) is at present best understood through the fraction of sources exhibiting CT absorption along the line of sight (N-H > 1.5 x 10(24) cm(-2)) in the X-ray band, which reveals the average covering factor. Determining this CT fraction is difficult, however, due to the extreme obscuration. With its spectral coverage at hard X-rays (>10 keV), Nuclear Spectroscopic Telescope Array (NuSTAR). is sensitive to the AGNs covering factor since Compton scattering of X-rays off optically thick material dominates at these energies. We present a spectral analysis of 10 AGNs observed with NuSTAR. where the obscuring medium is optically thick to Compton scattering, so-called CT AGNs. We use the torus models of Brightman & Nandra that predict the X-ray spectrum from reprocessing in a torus and include the torus opening angle as a free parameter and aim to determine the covering factor of the CT gas in these sources individually. Across the sample we find mild to heavy CT columns, with N-H measured from 10(24) to 10(26) cm(-2), and a wide range of covering factors, where individual measurements range from 0.2 to 0.9. We find that the covering factor, f(c), is a strongly decreasing function of the intrinsic 2-10 keV luminosity, L-X, where f(c) = (-0.41 +/- 0.13) log(10)(L-X/erg s(-1))+18.31 +/- 5.33, across more than two orders of magnitude in L-X (10(41.5) - 10(44) erg s-1). The covering factors measured here agree well with the obscured fraction as a function of L-X as determined by studies of local AGNs with L-X > 10(42.5) erg s(-1) C1 [Brightman, M.; Balokovic, M.; Harrison, F. A.; Rivers, E.; Walton, D. J.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Brightman, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Stern, D.; Walton, D. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, F. E.] Millennium Inst Astrophys, Santiago, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Comastri, A.] INAF Osserv Astron Bologna, I-40127 Bologna, Italy. [Gandhi, P.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Gandhi, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Koss, M.] ETH, Dept Phys, Inst Astron, SNSF Ambiz Fellow, CH-8093 Zurich, Switzerland. [LaMassa, S.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Puccetti, S.] ASDC ASI, I-00133 Rome, Italy. [Puccetti, S.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Vasudevan, R.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Brightman, M (reprint author), CALTECH, Cahill Ctr Astrophys, 1216 East Calif Blvd, Pasadena, CA 91125 USA. RI Koss, Michael/B-1585-2015; Comastri, Andrea/O-9543-2015; Boggs, Steven/E-4170-2015; OI Koss, Michael/0000-0002-7998-9581; Comastri, Andrea/0000-0003-3451-9970; Boggs, Steven/0000-0001-9567-4224; Puccetti, Simonetta/0000-0002-2734-7835 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; NASA Headquarters under the NASA Earth and Space Science Fellowship Program [NNX14AQ07H]; NSF [AST 1008067]; STFC [ST/J003697/1]; Swiss National Science Foundation (SNSF) through the Ambizione fellowship grant [PZ00P2 154799/1]; Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo [IC120009]; CONICYT-Chile grants Basal-CATA [PFB-06/2007]; FONDECYT [1141218]; "EMBIGGEN" Anillo [ACT1101]; "Millennium Institute of Astrophysics (MAS)" of the Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo [IC120009] FX This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The work presented here was also based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This research has also made use of data and software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. Furthermore, this research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. M. Balokovic acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. D.R.B. acknowledges support from NSF award AST 1008067; P.G. acknowledges support from STFC (grant reference ST/J003697/1), M.K. acknowledges support from the Swiss National Science Foundation (SNSF) through the Ambizione fellowship grant PZ00P2 154799/1. We also acknowledge support from CONICYT-Chile grants Basal-CATA PFB-06/2007 (FEB), FONDECYT 1141218 (FEB), "EMBIGGEN" Anillo ACT1101 (FEB), Project IC120009 "Millennium Institute of Astrophysics (MAS)" of the Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo (FEB). NR 73 TC 22 Z9 22 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2015 VL 805 IS 1 AR 41 DI 10.1088/0004-637X/805/1/41 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8BA UT WOS:000354991300041 ER PT J AU Ciardi, DR Beichman, CA Horch, EP Howell, SB AF Ciardi, David R. Beichman, Charles A. Horch, Elliott P. Howell, Steve B. TI UNDERSTANDING THE EFFECTS OF STELLAR MULTIPLICITY ON THE DERIVED PLANET RADII FROM TRANSIT SURVEYS: IMPLICATIONS FOR KEPLER, K2, AND TESS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; planetary systems ID SOLAR-TYPE STARS; CANDIDATES; MISSION; OBJECTS; SAMPLE; AU; COMPANIONS; VALIDATION; SYSTEMS AB We present a study on the effect of undetected stellar companions on the derived planetary radii for Kepler Objects of Interest (KOIs). The current production of the KOI list assumes that each KOI is a single star. Not accounting for stellar multiplicity statistically biases the planets toward smaller radii. The bias toward smaller radii depends on the properties of the companion stars and whether the planets orbit the primary or the companion stars. Defining a planetary radius correction factor, X-R, we find that if the KOIs are assumed to be single, then, on average, the planetary radii may be underestimated by a factor of < X-R > approximate to 1.5. If typical radial velocity and high-resolution imaging observations are performed and no companions are detected, then this factor reduces to < X-R > approximate to 1.2. The correction factor < X-R > is dependent on the primary star properties and ranges from < X-R > approximate to 1.6 for A and F stars to < X-R > approximate to 1.2 for K and M stars. For missions like K2 and TESS where the stars may be closer than the stars in the Kepler target sample, observational vetting (primary imaging) reduces the radius correction factor to < X-R > approximate to 1.1. Finally, we show that if the stellar multiplicity rates are not accounted for correctly, then occurrence rate calculations for Earth-sized planets may overestimate the frequency of small planets by as much as 15%-20%. C1 [Ciardi, David R.; Beichman, Charles A.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Horch, Elliott P.] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA. [Howell, Steve B.] NASA, Ames Res Ctr, Mountain View, CA USA. RP Ciardi, DR (reprint author), CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. EM ciardi@ipac.caltech.edu OI Ciardi, David/0000-0002-5741-3047 NR 37 TC 13 Z9 13 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 MAY 20 PY 2015 VL 805 IS 1 AR 16 DI 10.1088/0004-637X/805/1/16 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8BA UT WOS:000354991300016 ER PT J AU Dangi, BB Kim, YS Krasnokutski, SA Kaiser, RI Bauschlicher, CW AF Dangi, Beni B. Kim, Yong S. Krasnokutski, Serge A. Kaiser, Ralf I. Bauschlicher, Charles W., Jr. TI TOWARD THE FORMATION OF CARBONACEOUS REFRACTORY MATTER IN HIGH TEMPERATURE HYDROCARBON-RICH ATMOSPHERES OF EXOPLANETS UPON MICROMETEOROID IMPACT SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; planets and satellites: atmospheres; solid state: refractory; techniques: imaging spectroscopy ID GJ 1214B; RAMAN-SPECTRA; TRANSMISSION SPECTRUM; HD 189733B; METHANE; SPECTROSCOPY; DISEQUILIBRIUM; APPROXIMATION; CHEMISTRY; GRAPHITE AB We report on laboratory simulation experiments mimicking the chemical processing of model atmospheres of exoplanets containing C3 and C4 hydrocarbons at moderate temperatures of 400 K upon interaction of catalytic surfaces of micrometeoroids. By utilizing an ultrasonic levitator device and heating singly levitated particles under simulated microgravity conditions, Raman spectroscopy is utilized as a non-invasive tool to probe on line and in situ the conversion of C3 and C4 hydrocarbons to refractory carbonaceous matter on the surfaces of levitated particles. Secondary Ion Mass Spectrometry and electron microscopic imaging were also conducted to gain further insight into the elementary composition and structures of the refractories formed. Our results provide compelling evidence that in the presence of a catalytic surface, which can be supplied in the form of micrometeoroids and atmospheric dust particles, hydrocarbon gases present in the atmospheres of exoplanets can be converted to refractory, carbon-rich carbonaceous matter of mainly graphitic structure with a carbon content of at least 90% at elevated temperatures. This finding might explain the low methane to carbon monoxide (CH4-CO) ratio in the hot Neptune GJ 436b, where the abundant methane photochemically converts to higher order hydrocarbons and ultimately to refractory graphite-like carbon in the presence of a silicon surface. C1 [Dangi, Beni B.; Kim, Yong S.; Krasnokutski, Serge A.; Kaiser, Ralf I.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA. [Bauschlicher, Charles W., Jr.] NASA Ames Res Ctr, Entry Syst & Technol Div, Moffett Field, CA 94035 USA. RP Kaiser, RI (reprint author), Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA. FU National Science Foundation [CHE-1360658] FX The authors thank Tina Carvalho of the University of Hawaii Biological Electron Microscope Facility for help with the SEM and TEM image acquisition. Funding for the research from the National Science Foundation (CHE-1360658) is greatly acknowledged. They would also would like to thank Dr. Anupam Mishra and Tayro Acosta of the Hawaiian Institute of Geophysics and Planetology (HIGP) for the use of micro-Raman systems and Professor Yuk L. Yung (California Institute of Technology) for helpful discussions. NR 40 TC 1 Z9 1 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2015 VL 805 IS 1 AR 76 DI 10.1088/0004-637X/805/1/76 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8BA UT WOS:000354991300076 ER PT J AU Fukumura, K Tombesi, F Kazanas, D Shrader, C Behar, E Contopoulos, I AF Fukumura, Keigo Tombesi, Francesco Kazanas, Demosthenes Shrader, Chris Behar, Ehud Contopoulos, Ioannis TI MAGNETICALLY DRIVEN ACCRETION DISK WINDS AND ULTRA-FAST OUTFLOWS IN PG 1211+143 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: individual (PG1211+143); galaxies: Seyfert; methods: numerical; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; HIGH-VELOCITY OUTFLOW; X-RAY ABSORBERS; RADIATION-MAGNETOHYDRODYNAMIC SIMULATIONS; HUBBLE-SPACE-TELESCOPE; BROAD ABSORPTION-LINES; K-SHELL ABSORPTION; SEYFERT 1 GALAXIES; PDS 456; PHYSICAL CONDITIONS AB We present a study of X-ray ionization of MHD accretion-disk winds in an effort to constrain the physics underlying the highly ionized ultra-fast outflows (UFOs) inferred by X-ray absorbers often detected in various sub. classes of Seyfert active galactic nuclei (AGNs). Our primary focus is to show that magnetically driven outflows are indeed physically plausible candidates for the observed outflows accounting for the AGN absorption properties of the present X-ray spectroscopic observations. Employing a stratified MHD wind launched across the entire AGN accretion disk, we calculate its X-ray ionization and the ensuing X-ray absorption-line spectra. Assuming an appropriate ionizing AGN spectrum, we apply our MHD winds to model the absorption features in an XMM-Newton/EPIC spectrum of the narrow-line Seyfert, PG 1211+143. We find, through identifying the detected features with Fe K alpha transitions, that the absorber has a characteristic ionization parameter of log (xi(c)[erg cm s(-1)]) similar or equal to 5-6 and a column density on the order of N-H similar or equal to 10(23) cm(-2) outflowing at a characteristic velocity of v(c)/c similar or equal to 0.1-0.2 (where c is the speed of light). The best-fit model favors its radial location at r(c) similar or equal to 200 R-o (R-o is the black hole's innermost stable circular orbit), with an inner wind truncation radius at R-t similar or equal to 30 R-o. The overall K-shell feature in the data is suggested to be dominated by Fe XXV with very little contribution from Fe XXVI and weakly ionized iron, which is in good agreement with a series of earlier analyses of the UFOs in various AGNs, including PG 1211+143. C1 [Fukumura, Keigo] James Madison Univ, Harrisonburg, VA 22807 USA. [Tombesi, Francesco; Kazanas, Demosthenes; Shrader, Chris] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Tombesi, Francesco] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Tombesi, Francesco] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Shrader, Chris] Univ Space Res Assoc, Columbia, MD 21046 USA. [Behar, Ehud] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. [Contopoulos, Ioannis] Acad Athens, Res Ctr Astron, Athens 11527, Greece. RP Fukumura, K (reprint author), James Madison Univ, Harrisonburg, VA 22807 USA. EM fukumukx@jmu.edu NR 90 TC 12 Z9 12 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 MAY 20 PY 2015 VL 805 IS 1 AR 17 DI 10.1088/0004-637X/805/1/17 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8BA UT WOS:000354991300017 ER PT J AU Ly, C Rigby, JR Cooper, M Yan, RB AF Ly, Chun Rigby, Jane R. Cooper, Michael Yan, Renbin TI METAL-POOR, STRONGLY STAR-FORMING GALAXIES IN THE DEEP2 SURVEY: THE RELATIONSHIP BETWEEN STELLAR MASS, TEMPERATURE-BASED METALLICITY, AND STAR FORMATION RATE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: abundances; galaxies: distances and redshifts; galaxies: evolution; galaxies: ISM; galaxies: photometry; galaxies: starburst ID EMISSION-LINE GALAXIES; DIGITAL SKY SURVEY; SIMILAR-TO 2; SPECTROSCOPIC PARALLEL SURVEY; HIGH-REDSHIFT GALAXIES; NEWH-ALPHA SURVEY; PHYSICAL CONDITIONS; FUNDAMENTAL PLANE; LENSED GALAXIES; DWARF GALAXIES AB We report on the discovery of 28 z approximate to 0.8 metal-poor galaxies in DEEP2. These galaxies were selected for their detection of the weak [O III] lambda 4363 emission line, which provides a "direct" measure of the gas-phase metallicity. A primary goal for identifying these rare galaxies is to examine whether the fundamental metallicity relation (FMR) between stellar mass, gas metallicity, and star formation rate (SFR) holds for low stellar mass and high SFR galaxies. The FMR suggests that higher SFR galaxies have lower metallicity (at fixed stellar mass). To test this trend, we combine spectroscopic measurements of metallicity and dust-corrected SFR with stellar mass estimates from modeling the optical photometry. We find that these galaxies are 1.05 +/- 0.61 dex above the z similar to 1 stellar mass-SFR relation and 0.23 +/- 0.23 dex below the local mass-metallicity relation. Relative to the FMR, the latter offset is reduced to 0.01 dex, but significant dispersion remains (0.29 dex with 0.16 dex due to measurement uncertainties). This dispersion suggests that gas accretion, star formation, and chemical enrichment have not reached equilibrium in these galaxies. This is evident by their short stellar mass doubling timescale of approximate to 100(-75)(+310) Myr, which suggests stochastic star formation. Combining our sample with other z similar to 1 metal-poor galaxies, we find a weak positive SFR-metallicity dependence (at fixed stellar mass) that is significant at 94.4% confidence. We interpret this positive correlation as recent star formation that has enriched the gas but has not had time to drive the metal-enriched gas out with feedback mechanisms. C1 [Ly, Chun; Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Cooper, Michael] UCI, Dept Phys & Astron, Ctr Galaxy Evolut, Irvine, CA USA. [Yan, Renbin] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. RP Ly, C (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM chun.ly@nasa.gov OI Ly, Chun/0000-0002-4245-2318; Yan, Renbin/0000-0003-1025-1711 FU NSF [AST-9509298, AST-0071048, AST-0507428, AST-0507483]; NASA LTSA grant [NNG04GC89G]; NASA Postdoctoral Program FX Based on observations taken at the W. M. Keck Observatory, which is operated jointly by the National Aeronautics and Space Administration (NASA), the University of California, and the California Institute of Technology. Funding for the DEEP2 Galaxy Redshift Survey has been provided by NSF grants AST-9509298, AST-0071048, AST-0507428, and AST-0507483, as well as NASA LTSA grant NNG04GC89G. C.L. is funded through the NASA Postdoctoral Program. We thank Jeffrey Newman, Alaina Henry, Massimo Ricotti, and Kate Whitaker for insightful discussions, and the anonymous referee for insightful comments that improved the paper. NR 72 TC 7 Z9 7 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2015 VL 805 IS 1 AR 45 DI 10.1088/0004-637X/805/1/45 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8BA UT WOS:000354991300045 ER PT J AU Pasham, DR Cenko, SB Levan, AJ Bower, GC Horesh, A Brown, GC Dolan, S Wiersema, K Filippenko, AV Fruchter, AS Greiner, J O'Brien, PT Page, KL Rau, A Tanvir, NR AF Pasham, Dheeraj R. Cenko, S. Bradley Levan, Andrew J. Bower, Geoffrey C. Horesh, Assaf Brown, Gregory C. Dolan, Stephen Wiersema, Klaas Filippenko, Alexei V. Fruchter, Andrew S. Greiner, Jochen O'Brien, Paul T. Page, Kim L. Rau, Arne Tanvir, Nial R. TI A MULTIWAVELENGTH STUDY OF THE RELATIVISTIC TIDAL DISRUPTION CANDIDATE SWIFT J2058.4+0516 AT LATE TIMES SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion; accretion disks; astrometry; black hole physics; relativistic processes ID MASSIVE BLACK-HOLES; GAMMA-RAY BURST; PHOTON IMAGING CAMERA; FUNDAMENTAL PLANE; ACCRETION FLOWS; RADIO-EMISSION; SOLAR MASSES; XMM-NEWTON; GALAXY; EVENT AB We report a multiwavelength (X-ray, ultraviolet/optical/infrared (UVOIR), radio) analysis of the relativistic tidal disruption event (TDE) candidate Sw J2058+05 from 3 months to 3 yr post-discovery in order to study its properties and compare its behavior with that of Sw J1644+57. Our main results are as follows: (1) The long-term X-ray light curve of Sw J2058+05 shows a remarkably similar trend to that of Sw J1644+57. After a prolonged power-law decay, the X-ray flux drops off rapidly by a factor of greater than or similar to 160 within a span of Delta t/t <= 0.95. Associating this sudden decline with the transition from super-Eddington to sub-Eddington accretion, we estimate the black hole mass to be in the range of 10(4-6) M-circle dot. (2) We detect rapid (less than or similar to 500 s) X-ray variability before the drop-off, suggesting that, even at late times, the X-rays originate from close to the black hole (ruling out a forward-shock origin). (3) We confirm using Hubble Space Telescope and Very Long Baseline Array astrometry that the location of the source coincides with the galaxy's center to within less than or similar to 400 pc (in projection). (4) We modeled Sw J2058+05's UVOIR spectral energy distribution with a single-temperature blackbody and find that while the radius remains more or less constant at a value of 63.4 +/- 4.5 AU (similar to 10(15) cm) at all times during the outburst, the blackbody temperature drops significantly from similar to 30,000 K at early times to a value of similar to 15,000 K at late times (before the Xray drop-off). Our results strengthen Sw J2058+05's interpretation as a TDE similar to Sw J1644+57. C1 [Pasham, Dheeraj R.; Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 661, Greenbelt, MD 20771 USA. [Pasham, Dheeraj R.; Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Levan, Andrew J.; Brown, Gregory C.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Bower, Geoffrey C.] Acad Sinica, Inst Astron & Astrophys, Hilo, HI 96720 USA. [Horesh, Assaf] Weizmann Inst Sci, Fac Phys, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Dolan, Stephen] Oxford Astrophys, Oxford OX1 3RH, England. [Wiersema, Klaas; O'Brien, Paul T.; Page, Kim L.; Tanvir, Nial R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Fruchter, Andrew S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Greiner, Jochen; Rau, Arne] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Pasham, DR (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 661, Greenbelt, MD 20771 USA. EM dheerajrangareddy.pasham@nasa.gov RI Horesh, Assaf/O-9873-2016 OI Horesh, Assaf/0000-0002-5936-1156 FU NSF Grant [1066293]; UK Space Agency; National Aeronautics and Space Administration (NASA) through Chandra Award [GO3-14107X]; NASA [NAS8-03060, NAS 5-26555]; HST [GO-13611-006 A]; NSF [AST-1211916]; ESA Member States; NASA; W. M. Keck Foundation FX We thank the XMM-Newton and HST teams, in particular Project Scientist N. Schartel and STScI director M. Mountain, for the approval and prompt scheduling of our DD requests. We are also grateful to James Guillochon and Ryan Chornock for valuable discussions. D.R.P. is grateful for valuable discussions with Sjoert van Velzen and Nick Stone. S.B.C. thanks the Aspen Center for Physics and NSF Grant #1066293 for hospitality during the preparation of this manuscript. K.L.P. acknowledges support from the UK Space Agency. Support for this work was provided by the National Aeronautics and Space Administration (NASA) through Chandra Award Number GO3-14107X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. D.R.P. and S.B.C. also acknowledge support from HST grant GO-13611-006 A. The work of A.V.F. was made possible by NSF grant AST-1211916, the TABASGO Foundation, and the Christopher R. Redlich Fund. A.V.F. and S.B.C. also acknowledge the support of Gary and Cynthia Bengier. Finally, we would like to thank the referee for his/her careful comments and suggestions. The scientific results reported in this article are based in part on observations made by the Chandra X-ray Observatory, NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555, and XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. 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 NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. Also, observations were obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). Also, based on observations made with ESO Telescopes at the La Silla or Paranal Observatories. We acknowledge the use of public data from the Swift data archive. NR 76 TC 11 Z9 11 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2015 VL 805 IS 1 AR 68 DI 10.1088/0004-637X/805/1/68 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8BA UT WOS:000354991300068 ER PT J AU Pontin, DI Wyper, PF AF Pontin, D. I. Wyper, P. F. TI THE EFFECT OF RECONNECTION ON THE STRUCTURE OF THE SUN'S OPEN-CLOSED FLUX BOUNDARY SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic reconnection; solar wind; Sun: corona; Sun: magnetic fields ID SLOW SOLAR-WIND; OPEN MAGNETIC-FIELD; CORONAL NULL-POINT; FLARE RIBBONS; MODEL; PSEUDOSTREAMERS; TOPOLOGY; CONNECTIVITY; TRANSPORT; DYNAMICS AB Global magnetic field extrapolations are now revealing the huge complexity of the Sun's corona, and in particular the structure of the boundary between open and closed magnetic flux. Moreover, recent developments indicate that magnetic reconnection in the corona likely occurs in highly fragmented current layers, and that this typically leads to a dramatic increase in the topological complexity beyond that of the equilibrium field. In this paper we use static models to investigate the consequences of reconnection at the open-closed flux boundary ("interchange reconnection") in a fragmented current layer. We demonstrate that it leads to efficient mixing of magnetic flux (and therefore plasma) from open and closed field regions. This corresponds to an increase in the length and complexity of the open-closed boundary. Thus, whenever reconnection occurs at a null point or separator of this open-closed boundary, the associated separatrix arc of the so-called S-web in the high corona becomes not a single line but a band of finite thickness within which the open-closed boundary is highly structured. This has significant implications for the acceleration of the slow solar wind, for which the interaction of open and closed field is thought to be important, and may also explain the coronal origins of certain solar energetic particles. The topological structures examined contain magnetic null points, separatrices and separators, and include a model for a pseudo-streamer. The potential for understanding both the large scale morphology and fine structure observed in flare ribbons associated with coronal nulls is also discussed. C1 [Pontin, D. I.] Univ Dundee, Div Math, Dundee, Scotland. [Wyper, P. F.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP Pontin, DI (reprint author), Univ Dundee, Div Math, Dundee, Scotland. EM dpontin@maths.dundee.ac.uk; peter.f.wyper@nasa.gov RI Wyper, Peter/H-9166-2013; Pontin, David/E-2313-2011 OI Pontin, David/0000-0002-1089-9270 FU UK's STFC [ST/K000993]; Leverhulme Trust; appointment to the NASA Postdoctoral Program at Goddard Space Flight Center; NASA FX D.P. acknowledges financial support from the UK's STFC (grant number ST/K000993) and the Leverhulme Trust. P.W. acknowledges support from an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 63 TC 3 Z9 3 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2015 VL 805 IS 1 AR 39 DI 10.1088/0004-637X/805/1/39 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8BA UT WOS:000354991300039 ER PT J AU Shariff, K Cuzzi, JN AF Shariff, Karim Cuzzi, Jeffrey N. TI THE SPHERICALLY SYMMETRIC GRAVITATIONAL COLLAPSE OF A CLUMP OF SOLIDS IN A GAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: formation; protoplanetary disks ID PROTOPLANETARY DISKS; SOLAR NEBULA; PLANETESIMAL FORMATION; PREFERENTIAL CONCENTRATION; STREAMING INSTABILITIES; ISOTROPIC TURBULENCE; PAIR DISPERSION; PARTICLES; DUST; DYNAMICS AB In the subject of planetesimal formation, several mechanisms have been identified that create dense particle clumps in the solar nebula. The present work is concerned with the gravitational collapse of such clumps, idealized as being spherically symmetric. Fully nonlinear simulations using the two-fluid model are carried out (almost) up to the time when a central density singularity forms. We refer to this as the collapse time. The end result of the study is a parametrization of the collapse time, in order that it may be compared with timescales for various disruptive effects to which clumps may be subject in a particular situation. An important effect that determines the collapse time is that as the clump compresses, it also compresses the gas due to drag. This increases gas pressure, which retards particle collapse and can lead to oscillation in the size and density of the clump. In the limit of particles perfectly coupled to the gas, the characteristic ratio of gravitational force to gas pressure becomes relevant and defines a two-phase Jeans parameter, Jt, which is the classical Jeans parameter with the speed of sound replaced by an effective wave speed in the coupled two-fluid medium. The parameter J(t) remains useful even away from the perfect coupling limit because it makes the simulation results insensitive to the initial density ratio of particles to gas (Phi(0)) as a separate parameter. A simple ordinary differential equation model is developed. It takes the form of two coupled non-linear oscillators and reproduces key features of the simulations. Finally, a parametric study of the time to collapse is performed and a formula (fit to the simulations) is developed. In the incompressible limit J(t) -> 0, collapse time equals the self-sedimentation time, which is inversely proportional to the Stokes number. As J(t) increases, the collapse time decreases with J(t) and eventually becomes approximately equal to the dynamical time. Values of collapse time versus clump size are given for a minimum-mass solar nebula. Finally, the timescale of clump erosion due to turbulent strain is estimated. C1 [Shariff, Karim; Cuzzi, Jeffrey N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Shariff, K (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. OI Shariff, Karim/0000-0002-7256-2497 NR 47 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2015 VL 805 IS 1 AR 42 DI 10.1088/0004-637X/805/1/42 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8BA UT WOS:000354991300042 ER PT J AU Zhang, K Crockett, N Salyk, C Pontoppidan, K Turner, NJ Carpenter, JM Blake, GA AF Zhang, Ke Crockett, Nathan Salyk, Colette Pontoppidan, Klaus Turner, Neal J. Carpenter, John M. Blake, Geoffrey A. TI DIMMING AND CO ABSORPTION TOWARD THE AA TAU PROTOPLANETARY DISK: AN INFALLING FLOW CAUSED BY DISK INSTABILITY? SO ASTROPHYSICAL JOURNAL LA English DT Article DE protoplanetary disks; stars: individual (AA Tau); stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be ID X-RAY-ABSORPTION; MAGNETOSPHERIC ACCRETION; PROTOSTELLAR DISKS; CHEMICAL-PROCESSES; INNER DISK; EMISSION; SPECTROSCOPY; CONSTRAINTS; VARIABILITY; STARS AB AA Tau, a classical T Tauri star in the Taurus cloud, has been the subject of intensive photometric monitoring for more than two decades due to its quasi-cyclic variation in optical brightness. Beginning in 2011, AA Tau showed another peculiar variation-its median optical though near-IR flux dimmed significantly, a drop consistent with a 4-mag increase in visual extinction. It has stayed in the faint state since. Here we present 4.7 mu m CO rovibrational spectra of AA Tau over eight epochs, covering an 11 yr time span, that reveal enhanced (CO)-C-12 and (CO)-C-13 absorption features in the J(low) <= 13 transitions after the dimming. These newly appeared absorptions require molecular gas along the line of sight with T similar to 500 K and a column density of log (N (CO)-C-12) similar to 18.5 cm(-2), with line centers that show a constant 6 km s(-1) redshift. The properties of the molecular gas confirm an origin in the circumstellar material. We suggest that the dimming and absorption are caused by gas and dust lifted to large heights by a magnetic buoyancy instability. This material is now propagating inward, and on reaching the star within a few years will be observed as an accretion outburst. C1 [Zhang, Ke; Carpenter, John M.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Crockett, Nathan; Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Salyk, Colette] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Pontoppidan, Klaus] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Turner, Neal J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Zhang, K (reprint author), CALTECH, Div Phys Math & Astron, MC 249-17, Pasadena, CA 91125 USA. EM kzhang@astro.caltech.edu OI Salyk, Colette/0000-0003-3682-6632 FU NSF AAG program; NOAO Leo Goldberg Fellowship program; Origins of Solar Systems Program [13-OSS13-0114]; NSF award [AST-1140063]; W. M. Keck Foundation; NASA Origins of Solar Systems program; [179.C-0151] FX We thank Jerome Bouvier and Konstantin Grankin for sharing their AA Tau photometric data, and the anonymous referee for helpful comments. K.Z., N.C. and G.A.B. gratefully acknowledge support from the NSF AAG and NASA Origins of Solar Systems programs. C.S. acknowledges the financial support of the NOAO Leo Goldberg Fellowship program. N.J.T.'s contributions were made at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA and with support from Origins of Solar Systems Program grant 13-OSS13-0114. J.M.C. acknowledges support from NSF award AST-1140063. The spectra presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and NASA. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The VLT data presented were acquired under program ID 179.C-0151. Finally, the authors wish to acknowledge the significant cultural role of the summit of Mauna Kea. NR 47 TC 3 Z9 3 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2015 VL 805 IS 1 AR 55 DI 10.1088/0004-637X/805/1/55 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8BA UT WOS:000354991300055 ER PT J AU Zhao, L DeVore, CR Antiochos, SK Zurbuchen, TH AF Zhao, L. DeVore, C. R. Antiochos, S. K. Zurbuchen, T. H. TI NUMERICAL SIMULATIONS OF HELICITY CONDENSATION IN THE SOLAR CORONA SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic reconnection; Sun: corona; Sun: magnetic fields ID MAGNETIC-FLUX TUBES; RECONNECTION; FIELDS; RELAXATION; FILAMENTS; SUPERGRANULATION; DISSIPATION; COALESCENCE; CHIRALITY; PATTERNS AB The helicity condensation model has been proposed by Antiochos to explain the observed smoothness of coronal loops and the observed buildup of magnetic shear at filament channels. The basic hypothesis of the model is that magnetic reconnection in the corona causes the magnetic stress injected by photospheric motions to collect only at those special locations where prominences are observed to form. In this work we present the first detailed quantitative MHD simulations of the reconnection evolution proposed by the helicity condensation model. We use the well-known ansatz of modeling the closed corona as an initially uniform field between two horizontal photospheric plates. The system is driven by applying photospheric rotational flows that inject magnetic helicity into the corona. The flows are confined to a finite region on the photosphere so as to mimic the finite flux system of a bipolar active region, for example. The calculations demonstrate that, contrary to common belief, opposite helicity twists do not lead to significant reconnection in such a coronal system, whereas twists with the same sense of helicity do produce substantial reconnection. Furthermore, we find that for a given amount of helicity injected into the corona, the evolution of the magnetic shear is insensitive to whether the pattern of driving photospheric motions is fixed or quasi-random. In all cases, the shear propagates via reconnection to the boundary of the flow region while the total magnetic helicity is conserved, as predicted by the model. We discuss the implications of our results for solar observations and for future, more realistic simulations of the helicity condensation process. C1 [Zhao, L.; Zurbuchen, T. H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48105 USA. [DeVore, C. R.; Antiochos, S. K.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP Zhao, L (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48105 USA. RI DeVore, C/A-6067-2015; OI DeVore, C/0000-0002-4668-591X; Zhao, Liang/0000-0002-5975-7476 FU NASA Earth and Space Science Fellowship Program-Grant [NNX09AV13H]; TRT Program; SRT Program; LWS [NNX10AQ61G, NNX13AH66G]; NSF [AGS-1432100] FX We gratefully acknowledge financial support for our research from NASA Earth and Space Science Fellowship Program-Grant NNX09AV13H (L.Z.), TR&T and SR&T Programs (C.R.D. and S.K.A.), LWS NNX10AQ61G and NNX13AH66G (T.H.Z.), and NSF AGS-1432100 (L.Z.). Also, we thank the DoD High Performance Computing and Modernization Program for providing computer resources for our large-scale numerical simulations during the time that C.R.D. held a staff position at the Naval Research Laboratory. NR 40 TC 4 Z9 4 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2015 VL 805 IS 1 AR 61 DI 10.1088/0004-637X/805/1/61 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8BA UT WOS:000354991300061 ER PT J AU Zhu, W Udalski, A Gould, A Dominik, M Bozza, V Han, C Yee, JC Novati, SC Beichman, CA Carey, S Poleski, R Skowron, J Kozlowski, S Mroz, P Pietrukowicz, P Pietrzynski, G Szymanski, MK Soszynski, I Ulaczyk, K Wyrzykowski, L Gaudi, BS Pogge, RW DePoy, DL Jung, YK Choi, JY Hwang, KH Shin, IG Park, H Jeong, J AF Zhu, Wei Udalski, A. Gould, A. Dominik, M. Bozza, V. Han, C. Yee, J. C. Novati, S. Calchi Beichman, C. A. Carey, S. Poleski, R. Skowron, J. Kozlowski, S. Mroz, P. Pietrukowicz, P. Pietrzynski, G. Szymanski, M. K. Soszynski, I. Ulaczyk, K. Wyrzykowski, L. Gaudi, B. S. Pogge, R. W. DePoy, D. L. Jung, Y. K. Choi, J. -Y. Hwang, K. -H. Shin, I. -G. Park, H. Jeong, J. CA OGLE Collaboration FUN Collaboration TI SPITZER AS A MICROLENS PARALLAX SATELLITE: MASS AND DISTANCE MEASUREMENTS OF BINARY LENS SYSTEM OGLE-2014-BLG-1050L SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; gravitational lensing: micro ID GALACTIC BULGE; ISOLATED STAR; HOST STAR; OGLE-III; EVENTS; MAGNIFICATION; DWARF; PREDICTIONS; DISCOVERY; MOTIONS AB We report the first mass and distance measurements of a caustic-crossing binary system OGLE-2014-BLG-1050 L using the space-based microlens parallax method. Spitzer captured the second caustic. crossing of the event, which occurred similar to 10 days before that seen from Earth. Due to the coincidence that the source-lens relative motion was almost parallel to the direction of the binary-lens axis, the fourfold degeneracy, which was known before only to occur in single-lens events, persists in this case, leading to either a lower-mass (0.2 and 0.07 M-circle dot) binary at similar to 1.1 kpc or a higher-mass (0.9 and 0.35 M-circle dot) binary at similar to 3.5 kpc. However, the latter solution is strongly preferred for reasons including blending and lensing probability. OGLE-2014-BLG-1050 L demonstrates the power of microlens parallax in probing stellar and substellar binaries. C1 [Zhu, Wei; Gould, A.; Poleski, R.; Gaudi, B. S.; Pogge, R. W.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Udalski, A.; Poleski, R.; Skowron, J.; Kozlowski, S.; Mroz, P.; Pietrukowicz, P.; Pietrzynski, G.; Szymanski, M. K.; Soszynski, I.; Ulaczyk, K.; Wyrzykowski, L.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Dominik, M.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Bozza, V.; Novati, S. Calchi] Univ Salerno, Dipartimento Fis ER Caianiello, I-84084 Fisciano, SA, Italy. [Bozza, V.] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy. [Han, C.; Jung, Y. K.; Choi, J. -Y.; Hwang, K. -H.; Shin, I. -G.; Park, H.; Jeong, J.] Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Cheongju 371763, South Korea. [Yee, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Novati, S. Calchi; Beichman, C. A.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Novati, S. Calchi] IIASS, I-84019 Vietri Sul Mare, SA, Italy. [Carey, S.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [DePoy, D. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. RP Zhu, W (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. RI Skowron, Jan/M-5186-2014; Kozlowski, Szymon/G-4799-2013; OI Skowron, Jan/0000-0002-2335-1730; Kozlowski, Szymon/0000-0003-4084-880X; ZHU, WEI/0000-0003-4027-4711 FU NSF [AST 1103471]; JPL [1500811]; NASA [NNX12AB99G]; Creative Research Initiative Program of the National Research Foundation of Korea [2009-0081561]; NASA through the Sagan Fellowship Program; European Research Council under the European Community's Seventh Framework Programme (FP7)/ERC [246678] FX Work by W.Z., A.G., and B.S.G. was supported by NSF grant AST 1103471. Work by J.C.Y., A.G., and S.C. was supported by JPL grant 1500811. A.G., B.S.G., and R.W.P. were supported by NASA grant NNX12AB99G. Work by C.H. was supported by the Creative Research Initiative Program (2009-0081561) of the National Research Foundation of Korea. Work by J.C.Y. was performed under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. Work by C.A.B. was carried out in part at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The OGLE project has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no. 246678 to AU. 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. NR 56 TC 17 Z9 17 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2015 VL 805 IS 1 AR 8 DI 10.1088/0004-637X/805/1/8 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8BA UT WOS:000354991300008 ER PT J AU Lin, Y Han, XG Campbell, CJ Kim, JW Zhao, B Luo, W Dai, JQ Hu, LB Connell, JW AF Lin, Yi Han, Xiaogang Campbell, Caroline J. Kim, Jae-Woo Zhao, Bin Luo, Wei Dai, Jiaqi Hu, Liangbing Connell, John W. TI Holey Graphene Nanomanufacturing: Structure, Composition, and Electrochemical Properties SO ADVANCED FUNCTIONAL MATERIALS LA English DT Article ID ENERGY-STORAGE; NANOMESH; CARBON; LITHOGRAPHY; OXIDE AB Topology is critical for properties and function of 2D nanomaterials. Membranes and films from 2D nanomaterials usually suffer from large tortuosity as a result from dense restacking of the nanosheets and thus have limited utility in applications such as electrodes for supercapacitor and batteries, which require ion transport through the nanosheet thickness. In comparison with conventional porous 2D nanomaterials, introducing holes through the nanosheets to create holey 2D nanomaterials with retention of the 2D-related properties is a more viable approach to improve molecular transport. Here, graphene is used as a model to study the fundamental structure-property relationship as a result from defect-enabled hole creation. Specifically, the correlation of electrochemical capacitive properties with structure and composition for holey graphene materials is prepared using a highly scalable controlled air oxidation process. The presence of holes on graphene sheets is not sufficient to account for the observed capacitance improvement. Rather, the improvement is achieved through the combination of an enhanced mesopore fraction with simultaneous oxygen doping while retaining the graphitic carbon network with minimal damage. The detailed understanding might be further applied to other 2D materials toward a broader range of both energy-related and other applications. C1 [Lin, Yi; Campbell, Caroline J.; Kim, Jae-Woo] Natl Inst Aerosp, Hampton, VA 23666 USA. [Lin, Yi] Coll William & Mary, Dept Appl Sci, Williamsburg, VA 23185 USA. [Han, Xiaogang; Zhao, Bin; Luo, Wei; Dai, Jiaqi; Hu, Liangbing] Univ Maryland, Dept Mat Sci & Engn, College Pk, MD 20742 USA. [Connell, John W.] NASA Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. RP Lin, Y (reprint author), Natl Inst Aerosp, 100 Exploration Way, Hampton, VA 23666 USA. EM yi.lin-1@nasa.gov; binghu@umd.edu RI Kim, Jae-Woo/A-8314-2008; Luo, Wei/E-1582-2011 OI Luo, Wei/0000-0002-4019-4634 FU Leading Edge Aeronautics Research for NASA (LEARN) program [NNX13AB88A]; NSF-CBET [1335944, 1335979]; LEARN FX The authors would like to thank M. Funk, L. Garcia, P. Tiemsin, and C. Chamberlain for experimental assistance. Y.L. acknowledges the financial support from the Leading Edge Aeronautics Research for NASA (LEARN) program (Grant No. NNX13AB88A). L.H. gratefully acknowledge the support from NSF-CBET (Grant Nos. 1335944 and 1335979), respectively. C.J.C. was a Langley Aerospace Research Summer Scholars (LARSS) Program scholar supported by LEARN. NR 21 TC 22 Z9 22 U1 28 U2 205 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 1616-301X EI 1616-3028 J9 ADV FUNCT MATER JI Adv. Funct. Mater. PD MAY 20 PY 2015 VL 25 IS 19 BP 2920 EP 2927 DI 10.1002/adfm.201500321 PG 8 WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA CI3DC UT WOS:000354626800015 ER PT J AU Laslandes, M Patterson, K Pellegrino, S AF Laslandes, Marie Patterson, Keith Pellegrino, Sergio TI Optimized actuators for ultrathin deformable primary mirrors SO APPLIED OPTICS LA English DT Article ID OPTICS AB A novel design and selection scheme for surface-parallel actuators for ultrathin, lightweight mirrors is presented. The actuation system consists of electrodes printed on a continuous layer of piezoelectric material bonded to an optical-quality substrate. The electrodes provide almost full coverage of the piezoelectric layer, in order to maximize the amount of active material that is available for actuation, and their shape is optimized to maximize the correctability and stroke of the mirror for a chosen number of independent actuators and for a dominant imperfection mode. The starting point for the design of the electrodes is the observation that the correction of a figure error that has at least two planes of mirror symmetry is optimally done with twin actuators that have the same optimized shape but are rotated through a suitable angle. Additional sets of optimized twin actuators are defined by considering the intersection between the twin actuators, and hence an arbitrarily fine actuation pattern can be generated. It is shown that this approach leads to actuator systems with better performance than simple, geometrically based actuators. Several actuator patterns to correct third-order astigmatism aberrations are presented, and an experimental demonstration of a 41-actuator mirror is also presented. (C) 2015 Optical Society of America C1 [Laslandes, Marie; Pellegrino, Sergio] CALTECH, Pasadena, CA 91125 USA. [Patterson, Keith] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Pellegrino, S (reprint author), CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM sergiop@caltech.edu FU Defense Advanced Research Projects Agency (DARPA) [W31P4Q-14-1-0008]; French Defence procurement agency (DGA) through Aix-Marseille University, France; Keck Institute of Space Studies; Dow Resnick Bridge program at Caltech; National Aeronautics and Space Administration (NASA) FX Defense Advanced Research Projects Agency (DARPA) (W31P4Q-14-1-0008); National Aeronautics and Space Administration (NASA).; We thank Xin Ning (Caltech) for help with the optimization algorithm and John Steeves (Caltech) for advice on mirror fabrication. We thank Dr. Harish Manohara (JPL) for providing access to the Microdevices Lab (MDL) cleanroom facilities for sample fabrication. We thank Dr. Risaku Toda (JPL) and Mr. Victor White (JPL) for processing equipment training and usage advice at the MDL. ML acknowledges the support of a postdoctoral grant from the French Defence procurement agency (DGA) held through Aix-Marseille University, France. Financial support from the Keck Institute of Space Studies and the Dow Resnick Bridge program at Caltech is gratefully acknowledged. A part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with National Aeronautics and Space Administration (NASA). NR 30 TC 0 Z9 0 U1 1 U2 13 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD MAY 20 PY 2015 VL 54 IS 15 BP 4937 EP 4952 DI 10.1364/AO.54.004937 PG 16 WC Optics SC Optics GA CI6UL UT WOS:000354898100042 PM 26192533 ER PT J AU Aartsen, MG Ackermann, M Adams, J Aguilar, JA Ahlers, M Ahrens, M Altmann, D Anderson, T Arguelles, C Arlen, TC Auffenberg, J Bai, X Barwick, SW Baum, V Bay, R Beatty, JJ Tjus, JB Becker, KH BenZvi, S Berghaus, P Berley, D Bernardini, E Bernhard, A Besson, DZ Binder, G Bindig, D Bissok, M Blaufuss, E Blumenthal, J Boersma, DJ Bohm, C Bos, F Bose, D Boser, S Botner, O Brayeur, L Bretz, HP Brown, AM Buzinsky, N Casey, J Casier, M Cheung, E Chirkin, D Christov, A Christy, B Clark, K Classen, L Clevermann, F Coenders, S Cowen, DF Silva, AHC Daughhetee, J Davis, JC Day, M de Andre, JPAM De Clercq, C De Ridder, S Desiati, P de Vries, KD de With, M DeYoung, T Diaz-Velez, JC Dunkman, M Eagan, R Eberhardt, B Ehrhardt, T Eichmann, B Eisch, J Euler, S Evenson, PA Fadiran, O Fazely, AR Fedynitch, A Feintzeig, J Felde, J Filimonov, K Finley, C Fischer-Wasels, T Flis, S Frantzen, K Fuchs, T Gaisser, TK Gaior, R Gallagher, J Gerhardt, L Gier, D Gladstone, L Glusenkamp, T Goldschmidt, A Golup, G Gonzalez, JG Goodman, JA Gora, D Grant, D Gretskov, P Groh, JC Gross, A Ha, C Haack, C Ismail, AH Hallen, P Hallgren, A Halzen, F Hanson, K Hebecker, D Heereman, D Heinen, D Helbing, K Hellauer, R Hellwig, D Hickford, S Hill, GC Hoffman, KD Hoffmann, R Homeier, A Hoshina, K Huang, F Huelsnitz, W Hulth, PO Hultqvist, K Ishihara, A Jacobi, E Jacobsen, J Japaridze, GS Jero, K Jlelati, O Jurkovic, M Kaminsky, B Kappes, A Karg, T Karle, A Kauer, M Keivani, A Kelley, JL Kheirandish, A Kiryluk, J Klas, J Klein, SR Kohne, JH Kohnen, G Kolanoski, H Koob, A Kopke, L Kopper, C Kopper, S Koskinen, DJ Kowalski, M Kriesten, A Krings, K Kroll, G Kroll, M Kunnen, J Kurahashi, N Kuwabara, T Labare, M Lanfranchi, JL Larsen, DT Larson, MJ Lesiak-Bzdak, M Leuermann, M Lunemann, J Madsen, J Maggi, G Maruyama, R Mase, K Matis, HS Maunu, R McNally, F Meagher, K Medici, M Meli, A Meures, T Miarecki, S Middell, E Middlemas, E Milke, N Miller, J Mohrmann, L Montaruli, T Morse, R Nahnhauer, R Naumann, U Niederhausen, H Nowicki, SC Nygren, DR Obertacke, A Odrowski, S Olivas, A Omairat, A O'Murchadha, A Palczewski, T Paul, L Penke, O Pepper, JA de los Heros, CP Pfendner, C Pieloth, D Pinat, E Posselt, J Price, PB Przybylski, GT Putz, J Quinnan, M Radel, L Rameez, M Rawlins, K Redl, P Rees, I Reimann, R Relich, M Resconi, E Rhode, W Richman, M Riedel, B Robertson, S Rodrigues, JP Rongen, M Rott, C Ruhe, T Ruzybayev, B Ryckbosch, D Saba, SM Sander, HG Sandroos, J Santander, M Sarkar, S Schatto, K Scheriau, F Schmidt, T Schmitz, M Schoenen, S Schoneberg, S Schonwald, A Schukraft, A Schulte, L Schulz, O Seckel, D Sestayo, Y Seunarine, S Shanidze, R Smith, MWE Soldin, D Spiczak, GM Spiering, C Stamatikos, M Stanev, T Stanisha, NA Stasik, A Stezelberger, T Stokstad, RG Stossl, A Strahler, EA Strom, R Strotjohann, NL Sullivan, GW Taavola, H Taboada, I Tamburro, A Tepe, A Ter-Antonyan, S Terliuk, A Tesic, G Tilav, S Toale, PA Tobin, MN Tosi, D Tselengidou, M Unger, E Usner, M Vallecorsa, S van Eijndhoven, N Vandenbroucke, J van Santen, J Vehring, M Voge, M Vraeghe, M Walck, C Wallraff, M Weaver, C Wellons, M Wendt, C Westerhoff, S Whelan, BJ Whitehorn, N Wichary, C Wiebe, K Wiebusch, CH Williams, DR Wissing, H Wolf, M Wood, TR Woschnagg, K Xu, DL Xu, XW Xu, Y Yanez, JP Yodh, G Yoshida, S Zarzhitsky, P Ziemann, J Zoll, M AF Aartsen, M. G. Ackermann, M. Adams, J. Aguilar, J. A. Ahlers, M. Ahrens, M. Altmann, D. Anderson, T. Arguelles, C. Arlen, T. C. Auffenberg, J. Bai, X. Barwick, S. W. Baum, V. Bay, R. Beatty, J. J. Tjus, J. Becker Becker, K. -H. BenZvi, S. Berghaus, P. Berley, D. Bernardini, E. Bernhard, A. Besson, D. Z. Binder, G. Bindig, D. Bissok, M. Blaufuss, E. Blumenthal, J. Boersma, D. J. Bohm, C. Bos, F. Bose, D. Boeser, S. Botner, O. Brayeur, L. Bretz, H. -P. Brown, A. M. Buzinsky, N. Casey, J. Casier, M. Cheung, E. Chirkin, D. Christov, A. Christy, B. Clark, K. Classen, L. Clevermann, F. Coenders, S. Cowen, D. F. Silva, A. H. Cruz Daughhetee, J. Davis, J. C. Day, M. de Andre, J. P. A. M. De Clercq, C. De Ridder, S. Desiati, P. de Vries, K. D. de With, M. DeYoung, T. Diaz-Valez, J. C. Dunkman, M. Eagan, R. Eberhardt, B. Ehrhardt, T. Eichmann, B. Eisch, J. Euler, S. Evenson, P. A. Fadiran, O. Fazely, A. R. Fedynitch, A. Feintzeig, J. Felde, J. Filimonov, K. Finley, C. Fischer-Wasels, T. Flis, S. Frantzen, K. Fuchs, T. Gaisser, T. K. Gaior, R. Gallagher, J. Gerhardt, L. Gier, D. Gladstone, L. Gluesenkamp, T. Goldschmidt, A. Golup, G. Gonzalez, J. G. Goodman, J. A. Gora, D. Grant, D. Gretskov, P. Groh, J. C. Gross, A. Ha, C. Haack, C. Ismail, A. Haj Hallen, P. Hallgren, A. Halzen, F. Hanson, K. Hebecker, D. Heereman, D. Heinen, D. Helbing, K. Hellauer, R. Hellwig, D. Hickford, S. Hill, G. C. Hoffman, K. D. Hoffmann, R. Homeier, A. Hoshina, K. Huang, F. Huelsnitz, W. Hulth, P. O. Hultqvist, K. Ishihara, A. Jacobi, E. Jacobsen, J. Japaridze, G. S. Jero, K. Jlelati, O. Jurkovic, M. Kaminsky, B. Kappes, A. Karg, T. Karle, A. Kauer, M. Keivani, A. Kelley, J. L. Kheirandish, A. Kiryluk, J. Klaes, J. Klein, S. R. Koehne, J. -H. Kohnen, G. Kolanoski, H. Koob, A. Koepke, L. Kopper, C. Kopper, S. Koskinen, D. J. Kowalski, M. Kriesten, A. Krings, K. Kroll, G. Kroll, M. Kunnen, J. Kurahashi, N. Kuwabara, T. Labare, M. Lanfranchi, J. L. Larsen, D. T. Larson, M. J. Lesiak-Bzdak, M. Leuermann, M. Luenemann, J. Madsen, J. Maggi, G. Maruyama, R. Mase, K. Matis, H. S. Maunu, R. McNally, F. Meagher, K. Medici, M. Meli, A. Meures, T. Miarecki, S. Middell, E. Middlemas, E. Milke, N. Miller, J. Mohrmann, L. Montaruli, T. Morse, R. Nahnhauer, R. Naumann, U. Niederhausen, H. Nowicki, S. C. Nygren, D. R. Obertacke, A. Odrowski, S. Olivas, A. Omairat, A. O'Murchadha, A. Palczewski, T. Paul, L. Penke, O. Pepper, J. A. de los Heros, C. Perez Pfendner, C. Pieloth, D. Pinat, E. Posselt, J. Price, P. B. Przybylski, G. T. Puetz, J. Quinnan, M. Raedel, L. Rameez, M. Rawlins, K. Redl, P. Rees, I. Reimann, R. Relich, M. Resconi, E. Rhode, W. Richman, M. Riedel, B. Robertson, S. Rodrigues, J. P. Rongen, M. Rott, C. Ruhe, T. Ruzybayev, B. Ryckbosch, D. Saba, S. M. Sander, H. -G. Sandroos, J. Santander, M. Sarkar, S. Schatto, K. Scheriau, F. Schmidt, T. Schmitz, M. Schoenen, S. Schoeneberg, S. Schoenwald, A. Schukraft, A. Schulte, L. Schulz, O. Seckel, D. Sestayo, Y. Seunarine, S. Shanidze, R. Smith, M. W. E. Soldin, D. Spiczak, G. M. Spiering, C. Stamatikos, M. Stanev, T. Stanisha, N. A. Stasik, A. Stezelberger, T. Stokstad, R. G. Stoessl, A. Strahler, E. A. Stroem, R. Strotjohann, N. L. Sullivan, G. W. Taavola, H. Taboada, I. Tamburro, A. Tepe, A. Ter-Antonyan, S. Terliuk, A. Tesic, G. Tilav, S. Toale, P. A. Tobin, M. N. Tosi, D. Tselengidou, M. Unger, E. Usner, M. Vallecorsa, S. van Eijndhoven, N. Vandenbroucke, J. van Santen, J. Vehring, M. Voge, M. Vraeghe, M. Walck, C. Wallraff, M. Weaver, Ch. Wellons, M. Wendt, C. Westerhoff, S. Whelan, B. J. Whitehorn, N. Wichary, C. Wiebe, K. Wiebusch, C. H. Williams, D. R. Wissing, H. Wolf, M. Wood, T. R. Woschnagg, K. Xu, D. L. Xu, X. W. Xu, Y. Yanez, J. P. Yodh, G. Yoshida, S. Zarzhitsky, P. Ziemann, J. Zoll, M. TI SEARCH FOR PROMPT NEUTRINO EMISSION FROM GAMMA-RAY BURSTS WITH ICECUBE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma-ray burst: general; neutrinos ID HIGH-ENERGY NEUTRINOS; 1ST 2 YEARS; COSMIC-RAYS; SPECTRAL CATALOG; MUON NEUTRINOS; ACCELERATION; TELESCOPE; MISSION; SIMULATIONS; FIREBALLS AB We present constraints derived from a search of four years of IceCube data for a prompt neutrino flux from gammaray bursts (GRBs). A single low-significance neutrino, compatible with the atmospheric neutrino background, was found in coincidence with one of the 506 observed bursts. Although GRBs have been proposed as candidate sources for ultra-high-energy cosmic rays, our limits on the neutrino flux disfavor much of the parameter space for the latest models. We also find that no more than similar to 1% of the recently observed astrophysical neutrino flux consists of prompt emission from GRBs that are potentially observable by existing satellites. C1 [Aartsen, M. G.; Hill, G. C.; Robertson, S.; Whelan, B. J.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. [Ackermann, M.; Berghaus, P.; Bernardini, E.; Bernhard, A.; Bretz, H. -P.; Silva, A. H. Cruz; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Kaminsky, B.; Karg, T.; Kowalski, M.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Schoenwald, A.; Shanidze, R.; Spiering, C.; Stasik, A.; Stoessl, A.; Strotjohann, N. L.; Terliuk, A.; Usner, M.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany. [Adams, J.; Brown, A. M.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [Aguilar, J. A.; Hanson, K.; Heereman, D.; Meures, T.; O'Murchadha, A.; Pinat, E.] Univ Libre Bruxelles, Fac Sci, B-1050 Brussels, Belgium. [Ahlers, M.; Arguelles, C.; BenZvi, S.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Valez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; Larsen, D. T.; McNally, F.; Middlemas, E.; Morse, R.; Rees, I.; Rodrigues, J. P.; Santander, M.; Tobin, M. N.; Tosi, D.; Vandenbroucke, J.; van Santen, J.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Ahlers, M.; Arguelles, C.; BenZvi, S.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Valez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; Larsen, D. T.; McNally, F.; Middlemas, E.; Morse, R.; Rees, I.; Rodrigues, J. P.; Santander, M.; Tobin, M. N.; Tosi, D.; Vandenbroucke, J.; van Santen, J.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA. [Ahrens, M.; Bohm, C.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Ahrens, M.; Bohm, C.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Altmann, D.; Classen, L.; Kappes, A.; Tselengidou, M.] Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany. [Anderson, T.; Arlen, T. C.; Cowen, D. F.; Dunkman, M.; Eagan, R.; Groh, J. C.; Huang, F.; Keivani, A.; Lanfranchi, J. L.; Quinnan, M.; Smith, M. W. E.; Stanisha, N. A.; Tesic, G.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Auffenberg, J.; Bissok, M.; Blumenthal, J.; Gier, D.; Gretskov, P.; Haack, C.; Hallen, P.; Heinen, D.; Hellwig, D.; Koob, A.; Kriesten, A.; Leuermann, M.; Paul, L.; Penke, O.; Puetz, J.; Raedel, L.; Reimann, R.; Rongen, M.; Schoenen, S.; Schukraft, A.; Vehring, M.; Wallraff, M.; Wichary, C.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys, D-52056 Aachen, Germany. [Bai, X.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA. [Barwick, S. W.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Baum, V.; Boeser, S.; Eberhardt, B.; Ehrhardt, T.; Koepke, L.; Kroll, G.; Luenemann, J.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany. [Bay, R.; Binder, G.; Filimonov, K.; Gerhardt, L.; Ha, C.; Klein, S. R.; Miarecki, S.; Price, P. B.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA. [Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Tjus, J. Becker; Bos, F.; Eichmann, B.; Fedynitch, A.; Kroll, M.; Saba, S. M.; Schoeneberg, S.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany. [Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Helbing, K.; Hickford, S.; Hoffmann, R.; Klaes, J.; Kopper, S.; Naumann, U.; Obertacke, A.; Omairat, A.; Posselt, J.; Soldin, D.; Tepe, A.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany. [Berley, D.; Blaufuss, E.; Cheung, E.; Christy, B.; Felde, J.; Goodman, J. A.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Maunu, R.; Meagher, K.; Olivas, A.; Redl, P.; Richman, M.; Schmidt, T.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Bernhard, A.; Coenders, S.; Gross, A.; Jurkovic, M.; Krings, K.; Resconi, E.; Schulz, O.; Sestayo, Y.] Tech Univ Munich, D-85748 Garching, Germany. [Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Binder, G.; Gerhardt, L.; Goldschmidt, A.; Ha, C.; Klein, S. R.; Matis, H. S.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Boersma, D. J.; Botner, O.; Euler, S.; Hallgren, A.; de los Heros, C. Perez; Stroem, R.; Taavola, H.; Unger, E.] Uppsala Univ, Dept Phys & Astron, SE-75120 Uppsala, Sweden. [Bose, D.; Rott, C.] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea. [Brayeur, L.; Casier, M.; De Clercq, C.; de Vries, K. D.; Golup, G.; Kunnen, J.; Maggi, G.; Miller, J.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium. [Buzinsky, N.; Grant, D.; Kopper, C.; Nowicki, S. C.; Odrowski, S.; Riedel, B.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Christov, A.; Montaruli, T.; Rameez, M.; Vallecorsa, S.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland. [Clark, K.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Clevermann, F.; Frantzen, K.; Fuchs, T.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.; Scheriau, F.; Schmitz, M.; Ziemann, J.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany. [Cowen, D. F.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [de Andre, J. P. A. M.; DeYoung, T.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [De Ridder, S.; Ismail, A. Haj; Jlelati, O.; Labare, M.; Meli, A.; Ryckbosch, D.; Vraeghe, M.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium. [de With, M.; Hebecker, D.; Kolanoski, H.; Kowalski, M.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. [Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA. [Gaior, R.; Ishihara, A.; Kuwabara, T.; Mase, K.; Relich, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Homeier, A.; Schulte, L.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany. [Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA. [Kauer, M.; Maruyama, R.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.; Xu, Y.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Kohnen, G.] Univ Mons, B-7000 Mons, Belgium. [Koskinen, D. J.; Larson, M. J.; Medici, M.; Sarkar, S.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Kurahashi, N.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Madsen, J.; Seunarine, S.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA. [Palczewski, T.; Pepper, J. A.; Toale, P. A.; Williams, D. R.; Xu, D. L.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA. [Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England. [Hoshina, K.] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, Tokyo 1130032, Japan. [Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Aartsen, MG (reprint author), Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. RI Koskinen, David/G-3236-2014; Maruyama, Reina/A-1064-2013; Tjus, Julia/G-8145-2012; Sarkar, Subir/G-5978-2011; Beatty, James/D-9310-2011; Wiebusch, Christopher/G-6490-2012; OI Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Koskinen, David/0000-0002-0514-5917; Maruyama, Reina/0000-0003-2794-512X; Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952; Wiebusch, Christopher/0000-0002-6418-3008; Schukraft, Anne/0000-0002-9112-5479; Groh, John/0000-0001-9880-3634; Larsen, Dag Toppe/0000-0002-9898-2174; Maunu, Ryan/0000-0002-5755-3437; Perez de los Heros, Carlos/0000-0002-2084-5866; Strotjohann, Nora Linn/0000-0002-4667-6730; Arguelles Delgado, Carlos/0000-0003-4186-4182 FU U.S. National Science Foundation-office of Polar Programs; U.S. National Science Foundation-physics Division; University of Wisconsin Alumni Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin-Madison; Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy; National Energy Research Scientific Computing Center; Louisiana Optical Network Initiative (LONI) grid computing resources; Natural Sciences and Engineering Research Council of Canada; WestGrid and Compute/Calcul Canada; Swedish Research Council; Swedish Polar Research Secretariat; Swedish National Infrastructure for Computing (SNIC); Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Helmholtz Alliance for Astroparticle Physics (HAP); Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO Odysseus programme; Flanders Institute to encourage scientific and technological research in industry (IWT); Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF); Danish National Research Foundation, Denmark (DNRF) FX We acknowledge the support from the following agencies: U.S. National Science Foundation-office of Polar Programs, U.S. National Science Foundation-physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; Natural Sciences and Engineering Research Council of Canada, WestGrid and Compute/Calcul Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF); Danish National Research Foundation, Denmark (DNRF). NR 44 TC 27 Z9 28 U1 0 U2 15 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 MAY 20 PY 2015 VL 805 IS 1 AR L5 DI 10.1088/2041-8205/805/1/L5 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI4VS UT WOS:000354752600005 ER PT J AU Schopf, JW Kudryavtsev, AB Walter, MR Van Kranendonk, MJ Williford, KH Kozdon, R Valley, JW Gallardo, VA Espinoza, C Flannery, DT AF Schopf, J. William Kudryavtsev, Anatoliy B. Walter, Malcolm R. Van Kranendonk, Martin J. Williford, Kenneth H. Kozdon, Reinhard Valley, John W. Gallardo, Victor A. Espinoza, Carola Flannery, David T. TI Reply to Dvorak et al.: Apparent evolutionary stasis of ancient subseafloor sulfur cycling biocoenoses SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter C1 [Schopf, J. William] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. [Schopf, J. William; Kudryavtsev, Anatoliy B.] Univ Calif Los Angeles, Ctr Study Evolut & Origin Life, Los Angeles, CA 90095 USA. [Schopf, J. William] Univ Calif Los Angeles, Inst Mol Biol, Los Angeles, CA 90095 USA. [Schopf, J. William; Kudryavtsev, Anatoliy B.] Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA. [Schopf, J. William; Kudryavtsev, Anatoliy B.; Williford, Kenneth H.; Kozdon, Reinhard; Valley, John W.] Univ Wisconsin, Astrobiol Res Consortium, Madison, WI 53706 USA. [Williford, Kenneth H.; Kozdon, Reinhard; Valley, John W.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Walter, Malcolm R.; Van Kranendonk, Martin J.; Flannery, David T.] Univ New S Wales, Australian Ctr Astrobiol, Randwick, NSW 2052, Australia. [Walter, Malcolm R.; Van Kranendonk, Martin J.; Flannery, David T.] Univ New S Wales, Sch Biol Earth & Environm Sci, Randwick, NSW 2052, Australia. [Van Kranendonk, Martin J.] Univ New S Wales, Australian Res Council Ctr Excellence, Core Crust Fluid Syst, Randwick, NSW 2052, Australia. [Williford, Kenneth H.; Flannery, David T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gallardo, Victor A.; Espinoza, Carola] Univ Concepcion, Fac Ciencias Nat & Oceanog, Dept Oceanog, Concepcion, Chile. RP Schopf, JW (reprint author), Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. EM schopf@ess.ucla.edu NR 5 TC 0 Z9 0 U1 1 U2 7 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAY 19 PY 2015 VL 112 IS 20 BP E2560 EP E2560 DI 10.1073/pnas.1503754112 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CI4OD UT WOS:000354729500004 PM 25902537 ER PT J AU Beebe, M Wang, L Madaras, SE Klopf, JM Li, Z Brantley, D Heimburger, M Wincheski, RA Kittiwatanakul, S Lu, J Wolf, SA Lukaszew, RA AF Beebe, M. Wang, L. Madaras, S. E. Klopf, J. M. Li, Z. Brantley, D. Heimburger, M. Wincheski, R. A. Kittiwatanakul, S. Lu, J. Wolf, S. A. Lukaszew, R. A. TI Surface plasmon resonance modulation in nanopatterned Au gratings by the insulator-metal transition in vanadium dioxide films SO OPTICS EXPRESS LA English DT Article ID THIN-FILMS; VO2; METAMATERIALS AB Correlated experimental and simulation studies on the modulation of Surface Plasmon Polaritons (SPP) in Au/VO2 bilayers are presented. The modification of the SPP wave vector by the thermallyinduced insulator-to-metal phase transition (IMT) in VO2 was investigated by measuring the optical reflectivity of the sample. Reflectivity changes are observed for VO2 when transitioning between the insulating and metallic states, enabling modulation of the SPP in the Au layer by the thermally induced IMT in the VO2 layer. Since the IMT can also be optically induced using ultrafast laser pulses, we postulate the viability of SPP ultrafast modulation for sensing or control. (C)2015 Optical Society of America C1 [Beebe, M.; Wang, L.; Madaras, S. E.; Klopf, J. M.; Li, Z.; Brantley, D.; Heimburger, M.; Lukaszew, R. A.] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. [Wincheski, R. A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Kittiwatanakul, S.; Lu, J.; Wolf, S. A.] Univ Virginia, Dept Mat Sci & Engn, Charlottesville, VA 22904 USA. [Wolf, S. A.] Univ Virginia, Dept Phys, Charlottesville, VA 22904 USA. RP Beebe, M (reprint author), Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. EM mrbeebe@email.wm.edu FU National Science Foundation [NSF-DMR-1006013]; Virginia Microelectronics Consortium (VMEC) FX Aspects of this work were supported by a grant from the National Science Foundation (NSF-DMR-1006013) and by the Virginia Microelectronics Consortium (VMEC). NR 19 TC 1 Z9 1 U1 10 U2 66 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD MAY 18 PY 2015 VL 23 IS 10 BP 13222 EP 13229 DI 10.1364/OE.23.013222 PG 8 WC Optics SC Optics GA CI4GQ UT WOS:000354706800072 PM 26074574 ER PT J AU Goldstein, R Burch, JL Mokashi, P Broiles, T Mandt, K Hanley, J Cravens, T Rahmati, A Samara, M Clark, G Hassig, M Webster, JM AF Goldstein, R. Burch, J. L. Mokashi, P. Broiles, T. Mandt, K. Hanley, J. Cravens, T. Rahmati, A. Samara, M. Clark, G. Haessig, M. Webster, J. M. TI The Rosetta Ion and Electron Sensor (IES) measurement of the development of pickup ions from comet 67P/Churyumov-Gerasimenko SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE comets; plasma; pickup ID SOLAR-WIND; PLASMA CONSORTIUM; CHARGE-EXCHANGE; HALLEY; RPC AB The Rosetta Ion and Electron Sensor (IES) has been measuring solar wind ions intermittently since exiting from hibernation in May 2014. On 19 August, when Rosetta was similar to 80km from the comet 67P/Churyumov-Gerasimenko, which was similar to 3.5AU from the Sun, IES began to see ions at its lowest energy range, similar to 4-10eV. We identify these as ions created from neutral species emitted by the comet nucleus, photoionized by solar UV radiation in the neighborhood of the Rosetta spacecraft (S/C), and attracted by the small negative potential of the S/C resulting from the population of thermal electrons. Later, IES began to see higher-energy ions that we identify as having been picked up and accelerated by the solar wind. IES continues to measure changes in the solar wind and the development of the pickup ion structure. C1 [Goldstein, R.; Burch, J. L.; Mokashi, P.; Broiles, T.; Mandt, K.; Hanley, J.; Haessig, M.; Webster, J. M.] Southwest Res Inst, San Antonio, TX 78227 USA. [Cravens, T.; Rahmati, A.] Univ Kansas, Phys & Astron, Lawrence, KS 66045 USA. [Samara, M.; Clark, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Haessig, M.] Univ Bern, Inst Phys, Bern, Switzerland. RP Goldstein, R (reprint author), Southwest Res Inst, San Antonio, TX 78227 USA. EM rgoldstein@swri.edu RI Clark, George/L-6433-2015; OI Broiles, Thomas/0000-0001-6910-2724; Mandt, Kathleen/0000-0001-8397-3315 FU U.S. National Aeronautics and Space Administration [1345493]; Jet Propulsion Laboratory, California Institute of Technology FX The data for this work are available from ESA's PSA archive or NASA's PDS Small Bodies Archive. The work on IES was supported, in part, by the U.S. National Aeronautics and Space Administration through contract 1345493 with the Jet Propulsion Laboratory, California Institute of Technology. We thank the teams at Imperial College London and ESA who have been responsible for the operation of IES. NR 14 TC 18 Z9 18 U1 0 U2 7 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 MAY 16 PY 2015 VL 42 IS 9 BP 3093 EP 3099 DI 10.1002/2015GL063939 PG 7 WC Geosciences, Multidisciplinary SC Geology GA CK0EM UT WOS:000355878300004 ER PT J AU Farrell, WM Hurley, DM Zimmerman, MI AF Farrell, W. M. Hurley, D. M. Zimmerman, M. I. TI Spillage of lunar polar crater volatiles onto adjacent terrains: The case for dynamic processes SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Moon; volatiles; craters; water ID WATER; MOON; ICE AB We present an investigation of the release and transport of lunar polar crater volatiles onto topside regions surrounding the cold traps. The volatiles are liberated via surface energization processes associated with the harsh space environment, including solar wind plasma sputtering and impact vaporization. We find that some fraction of these volatiles can migrate from crater floors onto topside regions (those regions directly adjacent to and above the polar crater floors), and that these surrounding terrains should contain a sampling of the material originating within the crater itself. It is concluded that the nature of the volatile content on crater floors can be obtained by sampling the surface volatiles that have migrated or spilled out onto the adjacent terrain. This spillage effect could make human or robotic prospecting for crater resources significantly easier, since an assessment may not require direct entry into the very harsh polar crater environment. We also suggest that there are dynamic processes actively operating on the crater floors, and we estimate their source rates assuming dynamic equilibrium of the observed water frost and our modeled loss rates. C1 [Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Farrell, W. M.; Hurley, D. M.; Zimmerman, M. I.] NASA, Solar Syst Explorat Res Virtual Inst, Ames Res Ctr, Moffett Field, CA USA. [Hurley, D. M.; Zimmerman, M. I.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Farrell, WM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM william.m.farrell@nasa.gov RI Hurley, Dana/F-4488-2015; Farrell, William/I-4865-2013 OI Hurley, Dana/0000-0003-1052-1494; FU Solar System Exploration Research Virtual Institute (SSERVI) FX The data presented is from a set of Interactive Data Language (IDL) custom-coded models that are maintained by the authors and available upon request. We gratefully acknowledge funding for this work from the Solar System Exploration Research Virtual Institute (SSERVI) and encouragement from its director Yvonne Pendleton. We also thank David Goldstein and Raul Baragiola who generously provided thoughtful discussion following our presentation to "SSERVI's Friends of Lunar Volatiles" focus group. NR 18 TC 1 Z9 1 U1 1 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 MAY 16 PY 2015 VL 42 IS 9 BP 3160 EP 3165 DI 10.1002/2015GL063200 PG 6 WC Geosciences, Multidisciplinary SC Geology GA CK0EM UT WOS:000355878300012 ER PT J AU Mazarico, E Genova, A Neumann, GA Smith, DE Zuber, MT AF Mazarico, Erwan Genova, Antonio Neumann, Gregory A. Smith, David E. Zuber, Maria T. TI Simulated recovery of Europa's global shape and tidal Love numbers from altimetry and radio tracking during a dedicated flyby tour SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Europa; tide; altimetry; flyby; gravity ID GRAVITY-FIELD; LASER ALTIMETRY; ICE SHELL; TOPOGRAPHY; TITAN; MARS; MERCURY AB The fundamental scientific objectives for future spacecraft exploration of Jupiter's moon Europa include confirmation of the existence of subsurface ocean beneath the surface ice shell and constraints on the physical properties of the ocean. Here we conduct a comprehensive simulation of a multiple-flyby mission. We demonstrate that radio tracking data can provide an estimate of the gravitational tidal Love number k(2) with sufficient precision to confirm the presence of a liquid layer. We further show that a capable long-range laser altimeter can improve determination of the spacecraft position, improve the k(2) determination (<1% error), and enable the estimation of the planetary shape and Love number h(2) (3-4% error), which is directly related to the amplitude of the surface tidal deformation. These measurements, in addition to the global shape accurately constrained by the long altimetric profiles, can yield further constraints on the interior structure of Europa. C1 [Mazarico, Erwan; Genova, Antonio; Neumann, Gregory A.] NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Genova, Antonio; Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. RP Mazarico, E (reprint author), NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM erwan.m.mazarico@nasa.gov RI Neumann, Gregory/I-5591-2013; Mazarico, Erwan/N-6034-2014; Genova, Antonio/M-1400-2016 OI Neumann, Gregory/0000-0003-0644-9944; Mazarico, Erwan/0000-0003-3456-427X; Genova, Antonio/0000-0001-5584-492X FU NASA FX We acknowledge the NASA support of the simulation effort by the Europa Pre-Project, through a grant to MIT. We thank F. Nimmo (UCSC) for providing the topographic models. The simulation was performed using the trajectory made available for the ICEE proposal (http://solarsystem.nasa.gov/europa/iceedocs.cfm). NR 41 TC 1 Z9 1 U1 2 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 16 PY 2015 VL 42 IS 9 BP 3166 EP 3173 DI 10.1002/2015GL063224 PG 8 WC Geosciences, Multidisciplinary SC Geology GA CK0EM UT WOS:000355878300013 ER PT J AU Hand, KP Carlson, RW AF Hand, K. P. Carlson, R. W. TI Europa's surface color suggests an ocean rich with sodium chloride SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE planetary science; Europa; Jupiter; astrobiology ID GALILEAN SATELLITES; SUBSURFACE OCEAN; EXCESS ELECTRONS; RADIATION-DAMAGE; HALIDE CLUSTERS; MU-M; NACL; CONSTRAINTS; ABSORPTION; FLUXES AB The composition of Europa's surface may be representative of the subsurface ocean; however, considerable debate persists regarding the endogenous or exogenous nature of a hydrated sulfate feature on Europa. Direct evidence of oceanic salts on Europa's surface has been largely inconclusive. We show that the observed color within geologically young features on Europa's surface can be explained by sodium chloride delivered from the ocean below. We find that sodium chloride, when exposed to Europa surface conditions, accumulates electrons in F and M centers, yielding a yellow-brown discoloration comparable to Europa's surface. Irradiation of sodium chloride from Europa's ocean thus provides a simple and elegant solution to the color of the non-ice material observed on Europa. This evidence for endogenous salts suggests that Europa's ocean is interacting with a silicate seafloor, a critical consideration for assessing habitability. C1 [Hand, K. P.; Carlson, R. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Hand, KP (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM khand@jpl.nasa.gov FU National Aeronautics and Space Administration; internal Research and Technology Development program; Instrument Concepts for Europa Exploration program within the National Aeronautics and Space Administration FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration and funded in part through the internal Research and Technology Development program. R.W.C. and K.P.H. acknowledge support from the Instrument Concepts for Europa Exploration program within the National Aeronautics and Space Administration. Data presented in this manuscript, including spectra and images from our laboratory experiments, are freely available by contacting K.P. Hand at khand@jpl.nasa.gov. NR 29 TC 14 Z9 14 U1 3 U2 27 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 MAY 16 PY 2015 VL 42 IS 9 BP 3174 EP 3178 DI 10.1002/2015GL063559 PG 5 WC Geosciences, Multidisciplinary SC Geology GA CK0EM UT WOS:000355878300014 ER PT J AU Schnepf, NR Kuvshinov, A Sabaka, T AF Schnepf, N. R. Kuvshinov, A. Sabaka, T. TI Can we probe the conductivity of the lithosphere and upper mantle using satellite tidal magnetic signals? SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE geomagnetic induction; electrical properties; satellite magnetics; marine electromagnetics; ocean tides; composition of the crust and mantle ID ELECTRICAL-CONDUCTIVITY; WATER-CONTENT; ELECTROMAGNETIC INDUCTION; GLOBAL INDUCTION; OBSERVATORY DATA; DOMAIN APPROACH; EARTHS MANTLE; INVERSION; PACIFIC; FIELDS AB A few studies convincingly demonstrated that the magnetic fields induced by the lunar semidiurnal (M2) ocean flow can be identified in satellite observations. This result encourages using M2 satellite magnetic data to constrain subsurface electrical conductivity in oceanic regions. Traditional satellite-based induction studies using signals of magnetospheric origin are mostly sensitive to conducting structures because of the inductive coupling between primary and induced sources. In contrast, galvanic coupling from the oceanic tidal signal allows for studying less conductive, shallower structures. We perform global 3-D electromagnetic numerical simulations to investigate the sensitivity of M2 signals to conductivity distributions at different depths. The results of our sensitivity analysis suggest it will be promising to use M2 oceanic signals detected at satellite altitude for probing lithospheric and upper mantle conductivity. Our simulations also suggest that M2 seafloor electric and magnetic field data may provide complementary details to better constrain lithospheric conductivity. C1 [Schnepf, N. R.] MIT, Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Kuvshinov, A.] ETH, Inst Geophys, CH-8093 Zurich, Switzerland. [Sabaka, T.] NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Schnepf, NR (reprint author), MIT, Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. EM nschnepf@mit.edu FU NSF FX N.R.S. would like to thank the NSF Graduate Research Fellowship Program for support. The CM5 data used here may be obtained by contacting T. J. Sabaka (terence.j.sabaka@nasa.gov) and the model output may be obtained by contacting N. R. Schnepf (nschnepf@mit.edu). NR 36 TC 4 Z9 4 U1 1 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 16 PY 2015 VL 42 IS 9 BP 3233 EP 3239 DI 10.1002/2015GL063540 PG 7 WC Geosciences, Multidisciplinary SC Geology GA CK0EM UT WOS:000355878300022 ER PT J AU Hall, T Hereid, K AF Hall, Timothy Hereid, Kelly TI The frequency and duration of US hurricane droughts SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE hurricanes; statistical modeling; risk analysis ID TROPICAL CYCLONE TRACKS; RISK AB As of the end of the 2014 hurricane season, the U.S. has experienced no major hurricane landfall since Hurricane Wilma in 2005, a drought that currently stands at 9years. Here we use a stochastic tropical cyclone model to calculate the mean waiting time for multiyear landfall droughts. We estimate that the mean time to wait for a 9year drought is 177years. We also find that the average probability of ending the drought with a major landfall in the next year is 0.39 and is independent of the drought duration, as one would expect for a Bernoulli process. C1 [Hall, Timothy] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Hereid, Kelly] ACE Tempest Re, Stamford, CT USA. RP Hall, T (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM timothy.m.hall@nasa.gov OI Hereid, Kelly/0000-0003-0322-2664 FU NASA National Climate Assessment Award FX This work was supported in part by a NASA National Climate Assessment Award. Data used for the analysis are publicly available and maintained by the Hurricane Research Division of NOAA. NR 10 TC 4 Z9 4 U1 2 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 16 PY 2015 VL 42 IS 9 BP 3482 EP 3485 DI 10.1002/2015GL063652 PG 4 WC Geosciences, Multidisciplinary SC Geology GA CK0EM UT WOS:000355878300052 ER PT J AU Saide, PE Peterson, DA da Silva, A Anderson, B Ziemba, LD Diskin, G Sachse, G Hair, J Butler, C Fenn, M Jimenez, JL Campuzano-Jost, P Perring, AE Schwarz, JP Markovic, MZ Russell, P Redemann, J Shinozuka, Y Streets, DG Yan, F Dibb, J Yokelson, R Toon, OB Hyer, E Carmichael, GR AF Saide, Pablo E. Peterson, David A. da Silva, Arlindo Anderson, Bruce Ziemba, Luke D. Diskin, Glenn Sachse, Glen Hair, Johnathan Butler, Carolyn Fenn, Marta Jimenez, Jose L. Campuzano-Jost, Pedro Perring, Anne E. Schwarz, Joshua P. Markovic, Milos Z. Russell, Phil Redemann, Jens Shinozuka, Yohei Streets, David G. Yan, Fang Dibb, Jack Yokelson, Robert Toon, O. Brian Hyer, Edward Carmichael, Gregory R. TI Revealing important nocturnal and day-to-day variations in fire smoke emissions through a multiplatform inversion SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE inversion; fire emissions; biomass burning; SEAC4RS; WRF-Chem; AERONET ID BIOMASS BURNING EMISSIONS; AEROSOL OPTICAL DEPTH; HIGH-RESOLUTION; ORGANIC AEROSOL; UNITED-STATES; MODEL; FOREST; CARBON; WILDFIRES; INDONESIA AB We couple airborne, ground-based, and satellite observations; conduct regional simulations; and develop and apply an inversion technique to constrain hourly smoke emissions from the Rim Fire, the third largest observed in California, USA. Emissions constrained with multiplatform data show notable nocturnal enhancements (sometimes over a factor of 20), correlate better with daily burned area data, and are a factor of 2-4 higher than a priori estimates, highlighting the need for improved characterization of diurnal profiles and day-to-day variability when modeling extreme fires. Constraining only with satellite data results in smaller enhancements mainly due to missing retrievals near the emissions source, suggesting that top-down emission estimates for these events could be underestimated and a multiplatform approach is required to resolve them. Predictions driven by emissions constrained with multiplatform data present significant variations in downwind air quality and in aerosol feedback on meteorology, emphasizing the need for improved emissions estimates during exceptional events. C1 [Saide, Pablo E.; Carmichael, Gregory R.] Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA 52242 USA. [Peterson, David A.] CNR, Monterey, CA USA. [da Silva, Arlindo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Anderson, Bruce; Ziemba, Luke D.; Diskin, Glenn; Hair, Johnathan; Butler, Carolyn; Fenn, Marta] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Sachse, Glen] Natl Inst Aerosp, Hampton, VA USA. [Jimenez, Jose L.; Campuzano-Jost, Pedro] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA. [Jimenez, Jose L.; Campuzano-Jost, Pedro] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Perring, Anne E.; Schwarz, Joshua P.; Markovic, Milos Z.] NOAA, Earth Syst Res Lab, Boulder, CO USA. [Russell, Phil; Redemann, Jens] NASA Ames, Moffett Field, CA USA. [Shinozuka, Yohei] NASA, Ames Res Ctr, Cooperat Res Earth Sci & Technol, Moffett Field, CA 94035 USA. [Shinozuka, Yohei] Bay Area Environm Res Inst, Petaluma, CA USA. [Streets, David G.; Yan, Fang] Argonne Natl Lab, Div Energy Syst, Argonne, IL 60439 USA. [Dibb, Jack] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Yokelson, Robert] Univ Montana, Dept Chem, Missoula, MT 59812 USA. [Toon, O. Brian] Univ Colorado, Lab Atmospher & Space Phys, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA. [Hyer, Edward] Naval Res Lab, Marine Meteorol Div, Monterey, CA USA. RP Saide, PE (reprint author), Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA 52242 USA. EM pablo-saide@uiowa.edu RI Yokelson, Robert/C-9971-2011; Hyer, Edward/E-7734-2011; Perring, Anne/G-4597-2013; Jimenez, Jose/A-5294-2008; peterson, david/L-2350-2016; schwarz, joshua/G-4556-2013; Manager, CSD Publications/B-2789-2015 OI Yokelson, Robert/0000-0002-8415-6808; Hyer, Edward/0000-0001-8636-2026; Perring, Anne/0000-0003-2231-7503; Jimenez, Jose/0000-0001-6203-1847; schwarz, joshua/0000-0002-9123-2223; FU NSF [1049140 NCE]; NASA [NNX11AI52G, NNH12AT27i, NNX12AC03G, NNX12AC20G, NNX12AC64G]; EPA [83503701]; National Center for Research Resources, a part of the National Institutes of Health [UL1RR024979] FX We thank all SEAC4RS participants that made the field experiment possible, especially Project Manager Hal Maring. We also thank Brent Holben, Patrick Arnott, Min Hao, Craig Coburn, Adriana Predoi-Cross, and their staff for establishing and maintaining the AERONET sites used in this investigation. This work was carried out with the aid of NSF grant 1049140 NCE; NASA grants NNX11AI52G, NNH12AT27i, NNX12AC03G, NNX12AC20G, and NNX12AC64G; EPA grant 83503701; and grant number UL1RR024979 from the National Center for Research Resources, a part of the National Institutes of Health. Its contents are solely the responsibility of the authors and do not necessarily represent the official views of the funding institutions. Contact P. E. Saide (pablo-saide@uiowa.edu) or G. R. Carmichael (gregory-carmichael@uiowa.edu) for data requests. NR 50 TC 10 Z9 10 U1 8 U2 44 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 MAY 16 PY 2015 VL 42 IS 9 BP 3609 EP 3618 DI 10.1002/2015GL063737 PG 10 WC Geosciences, Multidisciplinary SC Geology GA CK0EM UT WOS:000355878300069 ER PT J AU He, Y Risi, C Gao, J Masson-Delmotte, V Yao, TD Lai, CT Ding, YJ Worden, J Frankenberg, C Chepfer, H Cesana, G AF He, You Risi, Camille Gao, Jing Masson-Delmotte, Valerie Yao, Tandong Lai, Chun-Ta Ding, Yongjian Worden, John Frankenberg, Christian Chepfer, Helene Cesana, Gregory TI Impact of atmospheric convection on south Tibet summer precipitation isotopologue composition using a combination of in situ measurements, satellite data, and atmospheric general circulation modeling SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE precipitation isotopic composition; Tibetan Plateau; Indian monsoon; Rayleigh distillation; atmospheric general circulation modeling ID WATER-VAPOR; ICE CORES; DELTA-D; ISOTOPIC COMPOSITION; STABLE-ISOTOPES; DEEP CONVECTION; ASIAN MONSOON; PLATEAU; CLIMATE; RESOLUTION AB Precipitation isotopologues recorded in natural archives from the southern Tibetan Plateau may document past variations of Indian monsoon intensity. The exact processes controlling the variability of precipitation isotopologue composition must therefore first be deciphered and understood. This study investigates how atmospheric convection affects the summer variability of O-18 in precipitation (O-18(p)) and D in water vapor (D-v) at the daily scale. This is achieved using isotopic data from precipitation samples at Lhasa, isotopic measurements of water vapor retrieved from satellites (Tropospheric Emission Spectrometer (TES), GOSAT) and atmospheric general circulation modeling. We reveal that both O-18(p) and D-v at Lhasa are well correlated with upstream convective activity, especially above northern India. First, during days of strong convection, northern India surface air contains large amounts of vapor with relatively low D-v. Second, when this low-D-v moisture is uplifted toward southern Tibet, this initial depletion in HDO is further amplified by Rayleigh distillation as the vapor moves over the Himalayan. The intraseasonal variability of the isotopologue composition of vapor and precipitation over the southern Tibetan Plateau results from these processes occurring during air mass transportation. C1 [He, You; Ding, Yongjian] Chinese Acad Sci, Cold & Arid Reg Environm & Engn Res Inst, Beijing, Peoples R China. [He, You; Gao, Jing; Yao, Tandong] Chinese Acad Sci, Inst Tibetan Plateau Res, Key Lab Tibetan Environm Changes & Land Surface, Beijing, Peoples R China. [He, You; Risi, Camille; Chepfer, Helene; Cesana, Gregory] CNRS, Inst Pierre Simon Laplace, Lab Meteorol Dynam, Paris, France. [Gao, Jing; Yao, Tandong] Chinese Acad Sci, CAS Ctr Excellence Tibetan Plateau Earth Sci, Beijing, Peoples R China. [Masson-Delmotte, Valerie] CEA, CNRS, Lab Sci Climat & Environm, Inst Pierre Simon Laplace,UVSQ,UMR 8212, F-91198 Gif Sur Yvette, France. [Lai, Chun-Ta] San Diego State Univ, Dept Biol, San Diego, CA 92182 USA. [Worden, John; Frankenberg, Christian] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Gao, J (reprint author), Chinese Acad Sci, Inst Tibetan Plateau Res, Key Lab Tibetan Environm Changes & Land Surface, Beijing, Peoples R China. EM JingGao@itpcas.ac.cn RI Masson-Delmotte, Valerie/G-1995-2011; Frankenberg, Christian/A-2944-2013 OI Masson-Delmotte, Valerie/0000-0001-8296-381X; Frankenberg, Christian/0000-0002-0546-5857 FU CAS [XDB03030100]; National Natural Science Foundation of China [41471053, 41190080]; China-France Caiyuanpei Program; National Aeronautics and Space Administration; U.S. National Science Foundation, Division of Atmospheric and Geo-space Sciences [AGS-0956425] FX This work is supported by CAS Strategic Priority Research Program(B)-Interactions among Multiple Geo-spheres on Tibetan Plateau and their Resource-Environment Effects (grant XDB03030100), by the National Natural Science Foundation of China (grants 41471053 and 41190080), and by the China-France Caiyuanpei Program. This work was finished in Laboratoire de Meteorologie Dynamique, Institut Pierre Simon Laplace, CNRS, Paris, France. LMDZ simulations were performed on the supercomputer of the IDRIS computing center. 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. C.-T Lai was supported by the U.S. National Science Foundation, Division of Atmospheric and Geo-space Sciences under Grant AGS-0956425. We thank Laurent Li and Pang Hongxi for their constructive comments. We also thank the staffs from Tibet observation stations for collecting the samples and staffs for measuring the samples, and all those who contributed to the field work. Part of in situ delta18Op data are from Third Pole Environment Database (http://en.tpedatabase.cn/). The back trajectories and the OLR (Outgoing Longwave Radiation) are computed using National Centers for Environmental Prediction (NCEP) reanalysis data. LMDZiso data can be acquired by contacting Camille Risi (Camille.Risi@lmd.jussieu.fr). TES and GOSAT satellite data can also be acquired by contacting John Worden (john.r.worden@jpl.nasa.gov). CALIPSO data can also be acquired by contacting Gregory Cesana (gregory.cesana@lmd.polytechnique.fr). In situ delta18Op data can also be acquired by contacting Gao Jing (gaojing@itpcas.ac.cn). NR 80 TC 15 Z9 15 U1 3 U2 34 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 MAY 16 PY 2015 VL 120 IS 9 BP 3852 EP 3871 DI 10.1002/2014JD022180 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CJ8IY UT WOS:000355744800016 ER PT J AU Battaglia, A Tanelli, S Mroz, K Tridon, F AF Battaglia, A. Tanelli, S. Mroz, K. Tridon, F. TI Multiple scattering in observations of the GPM dual-frequency precipitation radar: Evidence and impact on retrievals SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE radar; GPM-DPR; multiple scattering; graupel ID SURFACE REFERENCE TECHNIQUE; RAIN-PROFILING ALGORITHM; PART II; APPROXIMATION; ATTENUATION; CONVECTION; RANGE; OCEAN AB This paper illustrates how multiple scattering signatures affect Global Precipitation Measuring (GPM) Mission Dual-Frequency Precipitation Radar (DPR) Ku and Ka band reflectivity measurements and how they are consistent with prelaunch assessments based on theoretical considerations and confirmed by airborne observations. In particular, in the presence of deep convection, certain characteristics of the dual-wavelength reflectivity profiles cannot be explained with single scattering, whereas they are readily explained by multiple-scattering theory. Examples of such signatures are the absence of surface reflectivity peaks and anomalously small reflectivity slopes in the lower troposphere. These findings are relevant for DPR-based rainfall retrievals and stratiform/convective classification algorithms when dealing with deep convective regions. A path to refining the rainfall inversion problem is proposed by adopting a methodology based on a forward operator which accounts for multiple scattering. A retrieval algorithm based on this methodology is applied to a case study over Africa, and it is compared to the standard DPR products obtained with the at-launch version of the standard algorithms. C1 [Battaglia, A.] Univ Leicester, Natl Ctr Earth Observat, Leicester, Leics, England. [Battaglia, A.; Mroz, K.; Tridon, F.] Univ Leicester, Dept Phys & Astron, Earth Observat Sci, Leicester LE1 7RH, Leics, England. [Tanelli, S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Battaglia, A (reprint author), Univ Leicester, Natl Ctr Earth Observat, Leicester, Leics, England. EM a.battaglia@leicester.ac.uk RI Measurement, Global/C-4698-2015; Tridon, Frederic/M-4127-2013; OI Tridon, Frederic/0000-0002-0436-283X; Battaglia, Alessandro/0000-0001-9243-3484 FU project "Calibration and validation studies over the North Atlantic and UK for the Global Precipitation Mission," by the UK NERC [NE/L007169/1]; National Aeronautics and Space Administration FX The work done by A. Battaglia and F. Tridon was funded by the project "Calibration and validation studies over the North Atlantic and UK for the Global Precipitation Mission," which was funded by the UK NERC (NE/L007169/1). The work done by S. Tanelli 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 carried out for the GPM mission under the Precipitation Measurement Missions program, and support by Ramesh Kakar is gratefully acknowledged. V03B-GPM and MSG data were downloaded from the Precipitation Processing System (DOI 10.5067/GPM/DPR/DPR/2A, 10.5067/GPM/DPR/Ku/2A, and 10.5067/GPM/DPR/Ka/2A for the 2A-DPR, 2A-Ku, and 2A-Ka, respectively) and the EumetSat Earth Observation Portal, respectively. The forward radar model code was courteously provided by R. Hogan (http://www.met.rdg.ac.uk/clouds/multiscatter/). NR 35 TC 7 Z9 7 U1 4 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 16 PY 2015 VL 120 IS 9 BP 4090 EP 4101 DI 10.1002/2014JD022866 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CJ8IY UT WOS:000355744800030 ER PT J AU Cho, HM Zhang, ZB Meyer, K Lebsock, M Platnick, S Ackerman, AS Di Girolamo, L C-Labonnote, L Cornet, C Riedi, J Holz, RE AF Cho, Hyoun-Myoung Zhang, Zhibo Meyer, Kerry Lebsock, Matthew Platnick, Steven Ackerman, Andrew S. Di Girolamo, Larry C-Labonnote, Laurent Cornet, Celine Riedi, Jerome Holz, Robert E. TI Frequency and causes of failed MODIS cloud property retrievals for liquid phase clouds over global oceans SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE MODIS; cloud; failure; inhomogeneity; drizzle; A-Train ID CALIPSO LIDAR MEASUREMENTS; VIEW-ANGLE DEPENDENCE; SOLAR ZENITH ANGLE; SATELLITE-OBSERVATIONS; OPTICAL-THICKNESS; ATTENUATED BACKSCATTER; INSTRUMENT SIMULATORS; WATER CLOUDS; AEROSOLS; DEPOLARIZATION AB Moderate Resolution Imaging Spectroradiometer (MODIS) retrieves cloud droplet effective radius (r(e)) and optical thickness () by projecting observed cloud reflectances onto a precomputed look-up table (LUT). When observations fall outside of the LUT, the retrieval is considered failed because no combination of and r(e) within the LUT can explain the observed cloud reflectances. In this study, the frequency and potential causes of failed MODIS retrievals for marine liquid phase (MLP) clouds are analyzed based on 1year of Aqua MODIS Collection 6 products and collocated CALIOP and CloudSat observations. The retrieval based on the 0.86 mu m and 2.1 mu m MODIS channel combination has an overall failure rate of about 16% (10% for the 0.86 mu m and 3.7 mu m combination). The failure rates are lower over stratocumulus regimes and higher over the broken trade wind cumulus regimes. The leading type of failure is the r(e) too large failure accounting for 60%-85% of all failed retrievals. The rest is mostly due to the r(e) too small or retrieval failures. Enhanced retrieval failure rates are found when MLP cloud pixels are partially cloudy or have high subpixel inhomogeneity, are located at special Sun-satellite viewing geometries such as sunglint, large viewing or solar zenith angles, or cloudbow and glory angles, or are subject to cloud masking, cloud overlapping, and/or cloud phase retrieval issues. The majority (more than 84%) of failed retrievals along the CALIPSO track can be attributed to at least one or more of these potential reasons. The collocated CloudSat radar reflectivity observations reveal that the remaining failed retrievals are often precipitating. It remains an open question whether the extremely large r(e) values observed in these clouds are the consequence of true cloud microphysics or still due to artifacts not included in this study. C1 [Cho, Hyoun-Myoung; Zhang, Zhibo] Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. [Zhang, Zhibo] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21228 USA. [Meyer, Kerry; Platnick, Steven] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Meyer, Kerry] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA. [Lebsock, Matthew] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Ackerman, Andrew S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Di Girolamo, Larry] Univ Illinois, Dept Atmospher Sci, Urbana, IL USA. [C-Labonnote, Laurent; Cornet, Celine; Riedi, Jerome] Univ Sci & Technol Lille, Lab Opt Atmospher, CNRS, Villeneuve Dascq, France. [Holz, Robert E.] Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI USA. RP Zhang, ZB (reprint author), Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. EM zhibo.zhang@umbc.edu RI Zhang, Zhibo/D-1710-2010; Meyer, Kerry/E-8095-2016; Platnick, Steven/J-9982-2014 OI Zhang, Zhibo/0000-0001-9491-1654; Meyer, Kerry/0000-0001-5361-9200; Platnick, Steven/0000-0003-3964-3567 FU NASA [NNX11AI98G, NNX14AJ25G]; U.S. National Science Foundation through the MRI program [CNS-0821258, CNS-1228778]; SCREMS program [DMS-0821311]; UMBC FX This research is supported by NASA grants NNX11AI98G and NNX14AJ25G managed by Richard Eckman. Zhibo Zhang would like to thank Gala Wind, Thomas Arnold, and Nandana Amarasinghe for their help on MODIS C6 data. The computations in this study were performed on 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 MODIS data are obtained from NASA's Level 1 and Atmosphere Archive and Distribution System (LAADS http://ladsweb.nascom.nasa.gov/). The CALIOP data are obtained from NASA' Atmospheric Science Data Center (ASDC, https://eosweb.larc.nasa.gov/). The CloudSat data are obtained from CloudSat data processing center (http://www.cloudsat.cira.colostate.edu/dataHome.php). NR 65 TC 11 Z9 12 U1 3 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 16 PY 2015 VL 120 IS 9 BP 4132 EP 4154 DI 10.1002/2015JD023161 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CJ8IY UT WOS:000355744800033 ER PT J AU Huang, L Jiang, JH Wang, Z Su, H Deng, M Massie, S AF Huang, Lei Jiang, Jonathan H. Wang, Zhien Su, Hui Deng, Min Massie, Steven TI Climatology of cloud water content associated with different cloud types observed by A-Train satellites SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE cloud climatology; cloud water content; cloud type; cloud fraction; cloud profile ID TRANSPORT PATHWAYS; UPPER TROPOSPHERE; PRECIPITATION; DISTRIBUTIONS; VALIDATION; PRODUCTS; CAMPAIGN; RADAR; CO AB This study investigates the climatology of vertical distributions of cloud liquid water content, ice water content, and cloud fraction (CFR) associated with eight different cloud types, by utilizing the combined CloudSat radar and Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations lidar measurements. The geographical and seasonal variations of these cloud properties for each cloud type are also analyzed. The cloud water content (CWC) of each cloud type is sorted by three parameters obtained from colocated satellite observations to investigate the relationships between large-scale conditions and the vertical structure of clouds. Results show that different cloud types have different altitudes of CWC and CFR peaks, and the altitude of CFR peak does not always overlap with that of CWC peak. Each type of cloud shows a clear asymmetric pattern of spatial distribution between Northern Hemisphere (NH) and Southern Hemisphere (SH). Stratocumulus and stratus clouds make the greatest contribution to the liquid water path, while the ice water path is mostly contributed by deep convective cloud over the tropics and nimbostratus over the middle and high latitudes. Over both middle and high latitudes, clouds have larger seasonal variation in the NH than in the SH. Over ocean, large CWCs of deep convective cloud, cirrus, and altostratus are above 7 km, and are associated with high convective available potential energy (>2000J/kg), warm sea surface temperature (>303 K), and relatively high precipitation (>1mm/h). Over land, most of the middle and high clouds have similar CWC distributions compared to those over ocean, but altocumulus and low clouds are quite different from those over ocean. C1 [Huang, Lei; Jiang, Jonathan H.; Su, Hui] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wang, Zhien; Deng, Min] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA. [Massie, Steven] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. RP Huang, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Lei.Huang@jpl.nasa.gov RI Wang, Zhien/F-4857-2011 FU NASA AST program; NASA MAP program; NASA CloudSat/CALIPSO program FX This research is supported by the NASA AST, MAP, and CloudSat/CALIPSO programs. The study was performed at NASA Jet Propulsion Laboratory (JPL) at the California Institute of Technology, under contract with NASA. We thank Gerald G. Mace for useful discussions. We also appreciate the comments from three anonymous reviewers that led to significant improvements of this paper. The CloudSat Level 2 data sets are obtained from the CloudSat Data Processing Center, located at the Cooperative Institute for Research in the Atmosphere at Colorado State University. The SST data are obtained from the Remote Sensing Systems (http://www.remss.com). AIRS Level 3 products are obtained from AIRS Data Server (http://disc.sci.gsfc.nasa.gov/AIRS/data-holdings/by-data-product-v5/air sL3_STD_AIRS_AMSU.shtml). TRMM precipitation data are obtained from GES DISC (http://mirador.gsfc.nasa.gov/cgi-bin/mirador/homepageAlt.pl?keyword=3B4 2). NR 49 TC 2 Z9 2 U1 1 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 16 PY 2015 VL 120 IS 9 BP 4196 EP 4212 DI 10.1002/2014JD022779 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CJ8IY UT WOS:000355744800036 ER PT J AU Kahn, RA Gaitley, BJ AF Kahn, Ralph A. Gaitley, Barbara J. TI An analysis of global aerosol type as retrieved by MISR SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE aerosol remote sensing; aerosol type; multiangle imaging; MISR; particle pollution; desert dust ID SKY RADIANCE MEASUREMENTS; OPTICAL-PROPERTIES; SIZE DISTRIBUTIONS; IN-SITU; DUST; SENSITIVITY; AERONET; COMPONENT; NETWORK; MODELS AB In addition to aerosol optical depth (AOD), aerosol type is required globally for climate forcing calculations, constraining aerosol transport models and other applications. However, validating satellite aerosol-type retrievals is more challenging than testing AOD results, because aerosol type is a more complex quantity, and ground truth data are far less numerous and generally not as robust. We evaluate the Multiangle Imaging Spectroradiometer (MISR) Version 22 aerosol-type retrievals by assessing product self-consistency on a regional basis and by making comparisons with general expectation and with the Aerosol Robotic Network aerosol-type climatology, as available. The results confirm and add detail to the observation that aerosol-type discrimination improves dramatically where midvisible AOD exceeds about 0.15 or 0.2. When the aerosol-type information content of the observations is relatively low, increased scattering-angle range improves particle-type sensitivity. The MISR standard, operational product discriminates among small, medium, and large particles and exhibits qualitative sensitivity to single-scattering albedo (SSA) under good aerosol-type retrieval conditions, providing a categorical aerosol-type classification. MISR angstrom ngstrom exponent deviates systematically from ground truth where particle types missing from the algorithm climatology are present, or where cloud contamination is likely to occur, and SSA tends to be overestimated where absorbing particles are found. We determined that the number of mixtures passing the algorithm acceptance criteria (#SuccMix) represents aerosol-type retrieval quality effectively, providing a useful aerosol-type quality flag. C1 [Kahn, Ralph A.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Gaitley, Barbara J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Kahn, RA (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. EM Ralph.Kahn@nasa.gov FU NASA; EOS-MISR FX We thank our colleagues on the Jet Propulsion Laboratory's MISR instrument team and at the NASA Langley Research Center's Atmospheric Sciences Data Center for their roles in producing the MISR data sets (available from http://eosweb.larc.nasa.gov), and Brent Holben, Tom Eck, and the AERONET scientists for the validation data sets used in this study (available from http://aeronet.gsfc.nasa.gov). We also thank Tom Eck, James Limbacher, Lauren Zamora, David Diner, Michael Garay, and two anonymous reviewers for their comments on early versions of the manuscript. The work of R. Kahn is supported in part by NASA's Climate and Radiation Research and Analysis Program, under H. Maring, NASA's Atmospheric Composition Program under R. Eckman, and the EOS-MISR project. NR 70 TC 14 Z9 14 U1 4 U2 28 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 MAY 16 PY 2015 VL 120 IS 9 BP 4248 EP 4281 DI 10.1002/2015JD023322 PG 34 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CJ8IY UT WOS:000355744800039 ER PT J AU de Gouw, JA McKeen, SA Aikin, KC Brock, CA Brown, SS Gilman, JB Graus, M Hanisco, T Holloway, JS Kaiser, J Keutsch, FN Lerner, BM Liao, J Markovic, MZ Middlebrook, AM Min, KE Neuman, JA Nowak, JB Peischl, J Pollack, IB Roberts, JM Ryerson, TB Trainer, M Veres, PR Warneke, C Welti, A Wolfe, GM AF de Gouw, J. A. McKeen, S. A. Aikin, K. C. Brock, C. A. Brown, S. S. Gilman, J. B. Graus, M. Hanisco, T. Holloway, J. S. Kaiser, J. Keutsch, F. N. Lerner, B. M. Liao, J. Markovic, M. Z. Middlebrook, A. M. Min, K. -E. Neuman, J. A. Nowak, J. B. Peischl, J. Pollack, I. B. Roberts, J. M. Ryerson, T. B. Trainer, M. Veres, P. R. Warneke, C. Welti, A. Wolfe, G. M. TI Airborne measurements of the atmospheric emissions from a fuel ethanol refinery SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE fuel ethanol ID ORGANIC-COMPOUND EMISSIONS; LAND-USE CHANGE; CELLULOSIC ETHANOL; GASOLINE VEHICLES; OZONE FORMATION; BIOFUEL CROPS; AIR-QUALITY; IMPACTS; CULTIVATION; REDUCTION AB Ethanol made from corn now constitutes approximately 10% of the fuel used in gasoline vehicles in the U.S. The ethanol is produced in over 200 fuel ethanol refineries across the nation. We report airborne measurements downwind from Decatur, Illinois, where the third largest fuel ethanol refinery in the U.S. is located. Estimated emissions are compared with the total point source emissions in Decatur according to the 2011 National Emissions Inventory (NEI-2011), in which the fuel ethanol refinery represents 68.0% of sulfur dioxide (SO2), 50.5% of nitrogen oxides (NOx=NO+NO2), 67.2% of volatile organic compounds (VOCs), and 95.9% of ethanol emissions. Emissions of SO2 and NOx from Decatur agreed with NEI-2011, but emissions of several VOCs were underestimated by factors of 5 (total VOCs) to 30 (ethanol). By combining the NEI-2011 with fuel ethanol production numbers from the Renewable Fuels Association, we calculate emission intensities, defined as the emissions per ethanol mass produced. Emission intensities of SO2 and NOx are higher for plants that use coal as an energy source, including the refinery in Decatur. By comparing with fuel-based emission factors, we find that fuel ethanol refineries have lower NOx, similar VOC, and higher SO2 emissions than from the use of this fuel in vehicles. The VOC emissions from refining could be higher than from vehicles, if the underestimated emissions in NEI-2011 downwind from Decatur extend to other fuel ethanol refineries. Finally, chemical transformations of the emissions from Decatur were observed, including formation of new particles, nitric acid, peroxyacyl nitrates, aldehydes, ozone, and sulfate aerosol. C1 [de Gouw, J. A.; McKeen, S. A.; Aikin, K. C.; Brock, C. A.; Brown, S. S.; Gilman, J. B.; Graus, M.; Holloway, J. S.; Lerner, B. M.; Liao, J.; Markovic, M. Z.; Middlebrook, A. M.; Min, K. -E.; Neuman, J. A.; Nowak, J. B.; Peischl, J.; Pollack, I. B.; Roberts, J. M.; Ryerson, T. B.; Trainer, M.; Veres, P. R.; Warneke, C.] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA. [de Gouw, J. A.; McKeen, S. A.; Aikin, K. C.; Gilman, J. B.; Graus, M.; Holloway, J. S.; Lerner, B. M.; Liao, J.; Markovic, M. Z.; Min, K. -E.; Neuman, J. A.; Nowak, J. B.; Peischl, J.; Pollack, I. B.; Veres, P. R.; Warneke, C.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [de Gouw, J. A.] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA. [Graus, M.] Univ Innsbruck, Inst Meteorol & Geophys, A-6020 Innsbruck, Austria. [Hanisco, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kaiser, J.] Univ Wisconsin, Madison, WI USA. [Keutsch, F. N.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Markovic, M. Z.] Environm Canada, Air Qual Proc Res Div, Toronto, ON, Canada. [Min, K. -E.] Gwangju Inst Sci & Technol, Gwangju, South Korea. [Nowak, J. B.] Aerodyne Res Inc, Billerica, MA USA. [Welti, A.] ETH, Zurich, Switzerland. [Wolfe, G. M.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. RP de Gouw, JA (reprint author), NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA. EM Joost.deGouw@noaa.gov RI Kaiser, Jennifer/N-7732-2014; Lerner, Brian/H-6556-2013; Brown, Steven/I-1762-2013; Trainer, Michael/H-5168-2013; Gilman, Jessica/E-7751-2010; Manager, CSD Publications/B-2789-2015; Pollack, Ilana/F-9875-2012; Roberts, James/A-1082-2009; Warneke, Carsten/E-7174-2010; Aikin, Kenneth/I-1973-2013; Middlebrook, Ann/E-4831-2011; Veres, Patrick/E-7441-2010; Neuman, Andy/A-1393-2009; Nowak, John/B-1085-2008; Ryerson, Tom/C-9611-2009; Peischl, Jeff/E-7454-2010; Graus, Martin/E-7546-2010; Wolfe, Glenn/D-5289-2011; de Gouw, Joost/A-9675-2008 OI Lerner, Brian/0000-0001-8721-8165; Gilman, Jessica/0000-0002-7899-9948; Roberts, James/0000-0002-8485-8172; Middlebrook, Ann/0000-0002-2984-6304; Veres, Patrick/0000-0001-7539-353X; Neuman, Andy/0000-0002-3986-1727; Nowak, John/0000-0002-5697-9807; Peischl, Jeff/0000-0002-9320-7101; Graus, Martin/0000-0002-2025-9242; de Gouw, Joost/0000-0002-0385-1826 FU STAR grant program of the U.S. Environmental Protection Agency; U.S. Weather Research Program within NOAA/OAR Office of Weather and Air Quality FX Data used in this work are archived at http://www.esrl.noaa.gov/csd/groups/csd7/measurements/2013senex/P3/DataD ownload/. The formaldehyde measurements were made possible with financial support from the STAR grant program of the U.S. Environmental Protection Agency. Some of this material (S.A. McKeen) is based upon work supported by the U.S. Weather Research Program within NOAA/OAR Office of Weather and Air Quality. We are thankful for the staff at the NOAA Aircraft Operations Center and the WP-3D flight crew for the help in instrumenting the aircraft and for conducting the flights. NR 50 TC 5 Z9 5 U1 12 U2 52 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 MAY 16 PY 2015 VL 120 IS 9 BP 4385 EP 4397 DI 10.1002/2015JD023138 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CJ8IY UT WOS:000355744800046 ER PT J AU Norris, KJ Garrett, MP Zhang, J Coleman, E Tompa, GS Kobayashi, NP AF Norris, Kate J. Garrett, Matthew P. Zhang, Junce Coleman, Elane Tompa, Gary S. Kobayashi, Nobuhiko P. TI Silicon nanowire networks for multi-stage thermoelectric modules SO ENERGY CONVERSION AND MANAGEMENT LA English DT Article DE Nanowire network; Plasma Enhanced Chemical Vapor Deposition (PECVD); Silicon; TiN nucleation layer; Copper substrate ID THERMAL-CONDUCTIVITY; POWER; GENERATOR; HEAT; DEVICES AB We present the fabrication and characterization of single, double, and quadruple stacked flexible silicon nanowire network based thermoelectric modules. From double to quadruple stacked modules, power production increased 27%, demonstrating that stacking multiple nanowire thermoelectric devices in series is a scalable method to generate power by supplying larger temperature gradient. We present a vertically scalable multi-stage thermoelectric module design using semiconducting nanowires, eliminating the need for both n-type and p-type semiconductors for modules. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Norris, Kate J.; Garrett, Matthew P.; Zhang, Junce; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. [Norris, Kate J.; Garrett, Matthew P.; Zhang, Junce; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Nanostruct Energy Convers Technol & Res NECTAR, Adv Studies Labs, NASA Ames Res Ctr, Moffett Field, CA 94035 USA. [Coleman, Elane; Tompa, Gary S.] Struct Mat Ind Inc, Piscataway, NJ USA. RP Norris, KJ (reprint author), Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. EM katejeannenorris@gmail.com FU NASA SBIR [NNX11CE14P]; National Science Foundation Graduate Research Fellowship [DGE-0809125]; Semiconductor Research Corporation CSR fund FX This work was supported by NASA SBIR NNX11CE14P. The authors are grateful to HP labs (Palo Alto, California), specifically Stanley Williams and the HP Quantum Science Research (QSR) group. We would also like to thank the MACS facility (Moffett Field, California) at Advanced Studies Laboratories, University of California Santa Cruz, and NASA Ames Research Center for continuous support on analytical equipment. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-0809125. Support by Semiconductor Research Corporation CSR fund (Dr. Victor Zhirnov) is also highly appreciated. NR 31 TC 5 Z9 5 U1 4 U2 35 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0196-8904 EI 1879-2227 J9 ENERG CONVERS MANAGE JI Energy Conv. Manag. PD MAY 15 PY 2015 VL 96 BP 100 EP 104 DI 10.1016/j.enconman.2015.02.050 PG 5 WC Thermodynamics; Energy & Fuels; Mechanics SC Thermodynamics; Energy & Fuels; Mechanics GA CH0RD UT WOS:000353729200011 ER PT J AU Alexander, C AF Alexander, Claudia TI We Could Not Fail The First African Americans in the Space Program SO SCIENCE LA English DT Book Review C1 [Alexander, Claudia] Jet Prop Lab, Pasadena, CA 91740 USA. RP Alexander, C (reprint author), Jet Prop Lab, Pasadena, CA 91740 USA. EM claudia.j.alexander@jpl.nasa.gov NR 3 TC 0 Z9 0 U1 0 U2 1 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 MAY 15 PY 2015 VL 348 IS 6236 BP 764 EP 764 DI 10.1126/science.aaa8008 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CI0LN UT WOS:000354428700025 ER PT J AU Sanders, GB AF Sanders, Gerald B. TI Preface: Terrestrial Fieldwork to Support in situ Resource Utilization (ISRU) and Robotic Resource Prospecting for Future Activities in Space SO ADVANCES IN SPACE RESEARCH LA English DT Editorial Material C1 NASA, Lyndon B Johnson Space Ctr, Div Energy Syst, Houston, TX 77058 USA. RP Sanders, GB (reprint author), NASA, Lyndon B Johnson Space Ctr, Div Energy Syst, 2101 NASA Pkwy, Houston, TX 77058 USA. EM gerald.b.sanders@nasa.gov NR 0 TC 0 Z9 0 U1 2 U2 4 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 MAY 15 PY 2015 VL 55 IS 10 BP 2379 EP 2380 DI 10.1016/j.asr.2015.03.018 PG 2 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA CH0ZC UT WOS:000353749900001 ER PT J AU Sanders, GB Larson, WE AF Sanders, Gerald B. Larson, William E. TI Final review of analog field campaigns for In Situ Resource Utilization technology and capability maturation SO ADVANCES IN SPACE RESEARCH LA English DT Review DE Analog testing; In Situ Resource Utilization; Lunar human exploration; Field testing AB A key aspect of enabling an affordable and sustainable program of human exploration beyond low Earth orbit is the ability to locate, extract, and harness the resources found in space to reduce what needs to be launched from Earth's deep gravity well and to minimize the risk of dependence on Earth for survival. Known as In Situ Resource Utilization or ISRU, the ability to convert space resources into useful and mission critical products has been shown in numerous studies to be mission and architecture enhancing or enabling. However at the time of the release of the US Vision for Space Exploration in 2004, only concept feasibility hardware for ISRU technologies and capabilities had been built and tested in the laboratory; no ISRU hardware had ever flown in a mission to the Moon or Mars. As a result, an ISRU development project was established with phased development of multiple generations of hardware and systems. To bridge the gap between past ISRU feasibility hardware and future hardware needed for space missions, and to increase confidence in mission and architecture planners that ISRU capabilities would meet exploration needs, the ISRU development project incorporated extensive ground and analog site testing to mature hardware, operations, and interconnectivity with other exploration systems linked to ISRU products. This report documents the series of analog test activities performed from 2008 to 2012, the stepwise progress achieved, and the end-to-end system and mission demonstrations accomplished in this test program. Published by Elsevier Ltd. on behalf of COSPAR. C1 [Sanders, Gerald B.] NASA, Lyndon B Johnson Space Ctr, Div Energy Syst, Houston, TX 77058 USA. [Larson, William E.] NASA, Kennedy Space Ctr, Kennedy Space Ctr, FL 32899 USA. RP Sanders, GB (reprint author), NASA, Lyndon B Johnson Space Ctr, Div Energy Syst, 2101 NASA Pkwy, Houston, TX 77058 USA. EM gerald.b.sanders@nasa.gov; william.e.larson@nasa.gov NR 31 TC 4 Z9 4 U1 2 U2 10 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 MAY 15 PY 2015 VL 55 IS 10 BP 2381 EP 2404 DI 10.1016/j.asr.2014.12.024 PG 24 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA CH0ZC UT WOS:000353749900002 ER PT J AU Graham, L Graff, TG Yingst, RA ten Kate, IL Russell, P AF Graham, Lee Graff, Trevor G. Yingst, R. Aileen ten Kate, Inge L. Russell, Patrick TI 2012 Moon Mars Analog Mission Activities on Mauna Kea, Hawai'i SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Geology; Moon; Mars; Rover ID GROUND-PENETRATING RADAR; MOSSBAUER SPECTROMETER AB Rover-based 2012 Moon and Mars Analog Mission Activities (MMAMA) scientific investigations were completed at Mauna Kea, Hawaii. Scientific investigations, scientific input, and science operations constraints were tested in the context of an existing project and protocols for the field activities designed to help NASA achieve the Vision for Space Exploration. Four separate science investigations were integrated in a Martian analog environment with initial science operations planned based on a model similar to the operations control of the Mars Exploration Rovers (MER). However, evolution of the operations process occurred during the initial planning sessions and as the analog mission progressed. We review here the overall program of the investigation into the origin of the valley including preliminary sensor data results, an applicable methodology for developing an optimum science input based on productive engineering, and science trades and the science operations approach for an investigation into the valley on the upper slopes of Mauna Kea identified as "Apollo Valley". Published by Elsevier Ltd. on behalf of COSPAR. C1 [Graham, Lee] NASA, Lyndon B Johnson Space Ctr, Explorat Integrat & Sci, Houston, TX 77058 USA. [Graff, Trevor G.] NASA, Lyndon B Johnson Space Ctr, Dept Sci, JACOBS, Houston, TX 77058 USA. [Yingst, R. Aileen] Planetary Sci Inst, Tucson, AZ 85719 USA. [ten Kate, Inge L.] Univ Utrecht, Dept Earth Sci, NL-3584 CD Utrecht, Netherlands. [Russell, Patrick] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20013 USA. RP Graham, L (reprint author), NASA, Lyndon B Johnson Space Ctr, Explorat Integrat & Sci, Mail Code X14,2101 NASA Pkwy, Houston, TX 77058 USA. EM lee.d.graham@nasa.gov NR 14 TC 4 Z9 4 U1 4 U2 9 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 MAY 15 PY 2015 VL 55 IS 10 BP 2405 EP 2413 DI 10.1016/j.asr.2015.01.024 PG 9 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA CH0ZC UT WOS:000353749900003 ER PT J AU Heldmann, JL Colaprete, A Elphic, RC Mattes, G Ennico, K Fritzler, E Marinova, MM McMurray, R Morse, S Roush, TL Stoker, CR AF Heldmann, Jennifer L. Colaprete, Anthony Elphic, Richard C. Mattes, Greg Ennico, Kimberly Fritzler, Erin Marinova, Margarita M. McMurray, Robert Morse, Stephanie Roush, Ted L. Stoker, Carol R. TI Real-time science operations to support a lunar polar volatiles rover mission SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Moon; Volatiles; Rover; Missions AB Future human exploration of the Moon will likely rely on in situ resource utilization (ISRU) to enable long duration lunar missions. Prior to utilizing ISRU on the Moon, the natural resources (in this case lunar volatiles) must be identified and characterized, and ISRU demonstrated on the lunar surface. To enable future uses of ISRU, NASA and the CSA are developing a lunar rover payload that can (1) locate near subsurface volatiles, (2) excavate and analyze samples of the volatile-bearing regolith, and (3) demonstrate the form, extractability and usefulness of the materials. Such investigations are important both for ISRU purposes and for understanding the scientific nature of these intriguing lunar volatile deposits. Temperature models and orbital data suggest near surface volatile concentrations may exist at briefly lit lunar polar locations outside persistently shadowed regions. A lunar rover could be remotely operated at some of these locations for the similar to 2-14 days of expected sunlight at relatively low cost. Due to the limited operational time available, both science and rover operations decisions must be made in real time, requiring immediate situational awareness, data analysis, and decision support tools. Given these constraints, such a mission requires a new concept of operations. In this paper we outline the results and lessons learned from an analog field campaign in July 2012 which tested operations for a lunar polar rover concept. A rover was operated in the analog environment of Hawaii by an off-site Flight Control Center, a rover navigation center in Canada, a Science Backroom at NASA Ames Research Center in California, and support teams at NASA Johnson Space Center in Texas and NASA Kennedy Space Center in Florida. We find that this type of mission requires highly efficient, real time, remotely operated rover operations to enable low cost, scientifically relevant exploration of the distribution and nature of lunar polar volatiles. The field demonstration illustrated the need for science operations personnel in constant communications with the flight mission operators and the Science Backroom to provide immediate and continual science support and validation throughout the mission. Specific data analysis tools are also required to enable immediate data monitoring, visualization, and decision making. The field campaign demonstrated that this novel methodology of real-time science operations is possible and applicable to providing important new insights regarding lunar polar volatiles for both science and exploration. Published by Elsevier Ltd. on behalf of COSPAR. C1 [Heldmann, Jennifer L.; Colaprete, Anthony; Elphic, Richard C.; Ennico, Kimberly; Roush, Ted L.; Stoker, Carol R.] NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94035 USA. [Mattes, Greg] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Fritzler, Erin; McMurray, Robert; Morse, Stephanie] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Marinova, Margarita M.] BAER Inst, Sonoma, CA 95476 USA. RP Heldmann, JL (reprint author), NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94035 USA. EM jennifer.heldmann@nasa.gov NR 6 TC 5 Z9 5 U1 2 U2 6 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 MAY 15 PY 2015 VL 55 IS 10 BP 2427 EP 2437 DI 10.1016/j.asr.2014.07.037 PG 11 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA CH0ZC UT WOS:000353749900005 ER PT J AU Elphic, RC Heldmann, JL Marinova, MM Colaprete, A Fritzler, EL McMurray, RE Morse, S Roush, TL Stoker, CR Deans, MC Smith, TF AF Elphic, Richard C. Heldmann, Jennifer L. Marinova, Margarita M. Colaprete, Anthony Fritzler, Erin L. McMurray, Robert E. Morse, Stephanie Roush, Ted L. Stoker, Carol R. Deans, Matthew C. Smith, Trey F. TI Simulated real-time lunar volatiles prospecting with a rover-borne neutron spectrometer SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Moon; Volatiles; Rover; Neutron spectroscopy ID GAMMA-RAY; EXPLORATION; DETECTOR; WATER AB In situ resource utilization (ISRU) may one day enable long duration lunar missions. But the efficacy of such an approach greatly depends on (1) physical and chemical makeup of the resource, and (2) the logistical cost of exploiting the resource. Establishing these key strategic factors requires prospecting: the capability of locating and characterizing potential resources. There is already considerable evidence from orbital and impact missions that the lunar poles harbor plausibly rich reservoirs of volatiles. The next step is to land on the Moon and assess the nature, "ore-grade", and extractability of water ice and other materials. In support of this next step, a mission simulation was carried out on the island of Hawai'i in July of 2012. A robotic rover, provided by the Canadian Space Agency, carried several NASA ISRU-supporting instruments in a field test to address how such a mission might be carried out. This exercise was meant to test the ability to (a) locate and characterize volatiles, (b) acquire subsurface samples in a volatile-rich location, and (c) analyze the form and composition of the volatiles to determine their utility. This paper describes the successful demonstration of neutron spectroscopy as a prospecting and decision support system to locate and evaluate potential ISRU targets in the field exercise. Published by Elsevier Ltd. on behalf of COSPAR. C1 [Elphic, Richard C.; Heldmann, Jennifer L.; Colaprete, Anthony; Roush, Ted L.; Stoker, Carol R.] NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94035 USA. [Marinova, Margarita M.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Fritzler, Erin L.; McMurray, Robert E.; Morse, Stephanie] NASA, Ames Res Ctr, Engn Syst Div, Moffett Field, CA 94035 USA. [Deans, Matthew C.; Smith, Trey F.] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA. RP Elphic, RC (reprint author), NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94035 USA. EM richard.c.elphic@nasa.gov NR 19 TC 3 Z9 3 U1 0 U2 3 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 MAY 15 PY 2015 VL 55 IS 10 BP 2438 EP 2450 DI 10.1016/j.asr.2015.01.035 PG 13 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA CH0ZC UT WOS:000353749900006 ER PT J AU Roush, TL Colaprete, A Elphic, R Ennico-Smith, K Heldmann, J Stoker, C Marinova, M McMurray, R Fritzler, E Morse, S AF Roush, Ted L. Colaprete, Anthony Elphic, Richard Ennico-Smith, Kimberly Heldmann, Jennifer Stoker, Carol Marinova, Margarita McMurray, Robert Fritzler, Erin Morse, Stephanie TI In Situ Resource Utilization (ISRU) field expedition 2012: Near-Infrared Volatile Spectrometer System (NIRVSS) science measurements compared to site knowledge SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Lunar; Volatile; Prospecting; Rover AB The scientific information collected and evaluated using the Near-Infrared Volatile Spectrometer System (NIRVSS) during the 2012 In Situ Resource Utilization (ISRU) field campaign, exhibits variations related to differing surface materials and presence of volatiles during both rover traverses and auger activities demonstrating the promise of using NIRVSS for volatile prospecting on the lunar surface. Published by Elsevier Ltd. on behalf of COSPAR. C1 [Roush, Ted L.; Colaprete, Anthony; Elphic, Richard; Ennico-Smith, Kimberly; Heldmann, Jennifer; Stoker, Carol] NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94035 USA. [Marinova, Margarita] BAER Inst, Petaluma, CA 94952 USA. [McMurray, Robert] NASA, Ames Res Ctr, Engn Syst Div, Moffett Field, CA 94035 USA. [Fritzler, Erin; Morse, Stephanie] NASA, Ames Res Ctr, Strateg Management & Anal Div, Lockheed Martin Space, Moffett Field, CA 94035 USA. RP Roush, TL (reprint author), NASA, Ames Res Ctr, Div Space Sci & Astrobiol, MS 245-3, Moffett Field, CA 94035 USA. EM ted.l.roush@nasa.gov FU NASA's Human Exploration and Operations Mission Directorate FX We thank NASA's Human Exploration and Operations Mission Directorate for their support of the July 2012 Hawaii ISRU field campaign. We thank the many individuals from NASA KSC, JSC, ARC, Glenn, the Canadian Space Agency, and Pacific International Space Center for Exploration Systems for their assistance in organizing and supporting the Hawaii 2012 field test. Without their efforts this work would not have been possible. We acknowledge the Gemini Observatory for the atmospheric transmission spectrum for Mauna Kea shown in Fig. 3. We thank two anonymous reviewers for their comments that helped to improve the original manuscript. NR 11 TC 4 Z9 4 U1 1 U2 5 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 MAY 15 PY 2015 VL 55 IS 10 BP 2451 EP 2456 DI 10.1016/j.asr.2014.08.033 PG 6 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA CH0ZC UT WOS:000353749900007 ER PT J AU Captain, JE Weis, K Cryderman, K Coan, M Lance, L Levine, L Loftin, KB Santiago-Maldonado, E Bauer, B Quinn, J AF Captain, Janine E. Weis, Kyle Cryderman, Katherine Coan, Mary Lance, Lucas Levine, Lanfang Loftin, Kathleen Brooks Santiago-Maldonado, Edgardo Bauer, Brint Quinn, Jaqueline TI Design and development of volatile analysis system for analog field test of lunar exploration mission SO ADVANCES IN SPACE RESEARCH LA English DT Article DE In Situ Resource Utilization; Field test; Volatile analysis; Lunar regolith; Lunar resources AB The recent evidence of water in the lunar crater Cabeus from the LCROSS mission (Colaprete et al., 2010) provides confirmation of a valuable resource on the lunar surface. To understand this resource and the impact it can have on future exploration, further information is needed on the distribution and availability of the water ice. The Lunar Advanced Volatile Analysis (LAVA) subsystem is a part of the Regolith & Environment Science and Oxygen & Lunar Volatile Extraction (RESOLVE) payload, designed to provide ground truth to the volatile distribution near the permanently shadowed regions on the lunar surface. The payload is designed to drill and extract a regolith core sample, heat the regolith to drive off the volatiles, and identify and quantify the volatile resources. The LAVA subsystem is specifically responsible for processing and analyzing the volatile gas sample from the lunar regolith sample. The main objective of this paper is to provide insight into the operations and hardware for volatile analysis developed and deployed at the 2012 RESOLVE Field Test on the slopes of Mauna Kea. The vision of employing Commercial Off the Shelf (COTS) and modified COTS hardware to lower the cost for mission-enabling field tests will be highlighted. This paper will discuss how the LAVA subsystem hardware supported several high level RESOLVE mission objectives to demonstrate the challenging lunar mission concept proposed. Published by Elsevier Ltd. on behalf of COSPAR. C1 [Captain, Janine E.; Cryderman, Katherine; Coan, Mary; Lance, Lucas; Loftin, Kathleen Brooks; Santiago-Maldonado, Edgardo; Quinn, Jaqueline] NASA, Kennedy Space Ctr, FL 32899 USA. [Weis, Kyle; Levine, Lanfang; Bauer, Brint] QinetiQ, Kennedy Space Ctr, FL 32899 USA. RP Captain, JE (reprint author), NASA, Kennedy Space Ctr, FL 32899 USA. EM Janine.E.Captain@nasa.gov FU National Aeronautics and Space Administration FX The authors would like to thank the Pacific International Space Center for Exploration System (PISCES), the Canadian Space Agency (CSA) and numerous volunteers involved in this field test. This work was funded by the National Aeronautics and Space Administration. NR 31 TC 1 Z9 1 U1 1 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD MAY 15 PY 2015 VL 55 IS 10 BP 2457 EP 2471 DI 10.1016/j.asr.2014.11.006 PG 15 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA CH0ZC UT WOS:000353749900008 ER PT J AU Chao, Y Farrara, JD Schumann, G Andreadis, KM Moller, D AF Chao, Yi Farrara, John D. Schumann, Guy Andreadis, Konstantinos M. Moller, Delwyn TI Sea surface salinity variability in response to the Congo river discharge SO CONTINENTAL SHELF RESEARCH LA English DT Article DE Sea surface salinity variability; River discharge; Hydrological forcing; Freshwater budget ID ATLANTIC-OCEAN; AQUARIUS; CIRCULATION; SENSOR; SPACE; PLUME; GULF; SMOS AB Sea surface salinity (SSS) variability associated with the Congo River discharge is examined using Aquarius satellite-retrieved SSS data and vertical profiles of salinity measured by the Argo floats. The Congo River and its adjacent coastal ocean region are selected for study because of their global importance in ocean-freshwater dynamics undermined by the lack of observational data and coordinated efforts to make in situ measurements in this region. With a weekly repeat orbit, Aquarius provides a unique opportunity to routinely map the SSS in this relatively remote and understudied region. The Congo River plume can be clearly identified in the Aquarius SSS data with a northwestward extension of 500-1000 km off the coast of the Democratic Republic of Congo (DRC). The peak amplitude of the SSS variability associated with the Congo River discharge exceeds 3.0 psu, significantly greater than the designed Aquarius SSS retrieval accuracy of 0.2 psu. Using the first two years of Aquarius data from September 2011 to August 2013, a well-defined seasonal cycle is described: maximum freshwater anomalies are found in the boreal winter and spring seasons. The anomalies during the 2012-2013 winter and spring seasons are significantly fresher than the 2011-2012 winter and spring seasons, suggesting a strong year-to-year variability. A strong correlation is found between month-to-month variations in upper ocean salinity (as revealed by Aquarius satellite and Argo observations) and month-to-month variations in the freshwater discharge from the Congo River over a region off the coast of West Africa that is large enough to be easily observed by the Aquarius satellite. Vertical profiles of salinity derived from Argo floats reveal that these freshwater anomalies can be traced to 30 m below the sea surface. Combining the spatial area characterized by strong negative correlations between Aquarius SSS data and Congo discharge with the Argo vertical profiles of salinity, the volume of the freshwater anomalies is inferred and used to estimate the Congo River discharge. Reasonably good agreement is found between the Congo River discharge as observed by a stream gauge at Brazzaville and that estimated from the combined Aquarius and Argo data, especially during the freshening portion of the seasonal cycle (during this phase the correlation is 0.84, implying similar to 70% of the variance can be explained). The precipitation minus evaporation portion of the freshwater flux is found to play a secondary role in this region. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Chao, Yi; Farrara, John D.; Moller, Delwyn] Remote Sensing Solut Inc, Pasadena, CA 91107 USA. [Chao, Yi; Farrara, John D.; Schumann, Guy] Univ Calif Los Angeles, Los Angeles, CA USA. [Andreadis, Konstantinos M.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Farrara, JD (reprint author), Remote Sensing Solut Inc, Pasadena, CA 91107 USA. EM jfarrara@jifresse.ucla.edu FU JPL Aquarius project [1425025B]; Ocean Salinity Science Team (OSST) grant from Oregon State University [NS235A-A]; National Aeronautics and Space Administration (NASA) [NNX12AF67G]; UCLA Joint Institute for Regional Earth System Science and Engineering (JIFRESSE); NOAA Climate Observations and Monitoring (COM) program FX The research of Y. Chao at Remote Sensing Solutions, Inc. is supported by the JPL Aquarius project through a subcontract (1425025B). The research of Y. Chao and J. Farrara at the University of California at Los Angeles (UCLA) is supported by the Ocean Salinity Science Team (OSST) grant through a subcontract (NS235A-A) from Oregon State University. The research of K. Andreadis and G. Schumann was carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA) (Grant no. NNX12AF67G). Staff support from the UCLA Joint Institute for Regional Earth System Science and Engineering (JIFRESSE) is also acknowledged. Thanks go to Raphael Tshimanga from the Congo Basin Network for Research and Capacity Development in Water Resources (CB-Hydronet) for providing the Congo River discharge data at Brazzaville station and to Fiachra O'Loughlin at the School of Geographical Sciences at the University of Bristol (UK) for providing the GRDC discharge data at Kinshasa station. Discussions with a number of OSST team members (Ricardo Matano, Alberto Piola, Raul Guerrero, Elbio Palma, Martin Saraceno, Ted Strub) on the South Atlantic ocean circulation and variability are acknowledged. The global ocean evaporation products were provided by the WHOI OAFlux project (http://oaflux.whoi.edu) funded by the NOAA Climate Observations and Monitoring (COM) program. The GPCP data provided by the NOAA/OAR/ESRL PSD, Boulder, Colorado, USA, from their Web site at http://www.esrl.noaa.gov/psd/. The GPCP combined precipitation data were developed and computed by the NASA/Goddard Space Flight Center's Laboratory for Atmospheres as a contribution to the GEWEX Global Precipitation Climatology Project. NR 26 TC 1 Z9 1 U1 5 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0278-4343 EI 1873-6955 J9 CONT SHELF RES JI Cont. Shelf Res. PD MAY 15 PY 2015 VL 99 BP 35 EP 45 DI 10.1016/j.csr.2015.03.005 PG 11 WC Oceanography SC Oceanography GA CH2PE UT WOS:000353866300004 ER PT J AU Li, WQ Beard, BL Li, CX Xu, HF Johnson, CM AF Li, Weiqiang Beard, Brian L. Li, Chengxiang Xu, Huifang Johnson, Clark M. TI Experimental calibration of Mg isotope fractionation between dolomite and aqueous solution and its geological implications SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID MAGNESIUM-ISOTOPE; HIGH-TEMPERATURE; DISORDERED DOLOMITE; SEAWATER CHEMISTRY; SEDIMENTARY DOLOMITE; CARBONATE MINERALOGY; WESTERN NEWFOUNDLAND; SALT-SOLUTIONS; DOLOMITIZATION; CALCITE AB Hydrothermal experiments at 220, 160, and 130 degrees C were performed to calibrate the Mg isotope fractionation factor between dolomite and aqueous Mg. Hydrothermal experiments included synthesis of dolomite using different starting materials, as well as exchange experiments that used poorly-ordered proto-dolomite. The morphology of synthesized dolomite was dependent on starting mineralogy, suggesting that dolomite was synthesized by different pathways. Hydrothermally synthesized dolomite was initially fine-grained disordered or poorly-ordered dolomite that, with time, recrystallized to coarser-grained ordered dolomite. Isotopic exchange was monitored using Sr-87/Sr-86 ratios and Mg-25 tracers, and these indicated near-complete isotope exchange between dolomite and aqueous solutions at the end of most hydrothermal experiments. The Mg isotope fractionation factor between dolomite and aqueous solution obtained from synthesis and exchange experiments converged with time and was independent of dolomite morphology, suggesting attainment of isotopic equilibrium. Combining results from synthesis and exchange experiments, the temperature dependent Mg isotope fractionation factor for ordered dolomite is: Delta Mg-26(dolo-aq) = -0.1554(+/- 0.0096) x 10(6)/T-2 where T is in Kelvin. In contrast, poorly-ordered dolomite has a Delta Mg-26(dolo-aq) fractionation factor that is up to 0.25 parts per thousand lower than that of ordered dolomite, and this is attributed to longer Mg-O bonds in imperfectly ordered dolomite. The experimentally calibrated Delta Mg-26(dolo-aq) fractionation factors lie between those calculated by Schauble (2011) and Rustad et al. (2010). The Delta Mg-26(dolo-aq) fractionation factor extrapolated to lower temperatures using the Delta Mg-26-T function of this study matches the Delta Mg-26(dolo-aq) fractionation factor obtained by modeling of Mg isotope compositions of ODP drill core samples. This study shows that significant Mg isotope fractionation occurs during dolomite precipitation. These results collectively demonstrate that Mg isotopes in dolomite are a useful tool for studying Mg global cycling and dolomitization. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Li, Weiqiang; Beard, Brian L.; Xu, Huifang; Johnson, Clark M.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Li, Weiqiang; Beard, Brian L.; Xu, Huifang; Johnson, Clark M.] NASA, Astrobiol Inst, Washington, DC USA. [Li, Weiqiang; Li, Chengxiang] Nanjing Univ, Sch Earth Sci & Engn, State Key Lab Mineral Deposits Res, Nanjing 210093, Jiangsu, Peoples R China. RP Li, WQ (reprint author), Nanjing Univ, Sch Earth Sci & Engn, Nanjing 210093, Jiangsu, Peoples R China. EM liweiqiang@nju.edu.cn RI Li, Weiqiang/D-2975-2011 OI Li, Weiqiang/0000-0003-2648-7630 FU NASA Astrobiology Institute of United States; National Science Foundation of China [41473002] FX This paper benefited from discussions with Or Bialik, Fangfu Zhang and Zhizhang Shen, and constructive comments from John Higgins and Josh Wimpenny, as well as editorial comments by Jeff Alt. This study was supported by the NASA Astrobiology Institute of United States. W. Li is supported by the National Science Foundation of China (41473002). NR 70 TC 17 Z9 19 U1 5 U2 44 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 MAY 15 PY 2015 VL 157 BP 164 EP 181 DI 10.1016/j.gca.2015.02.024 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CG3XX UT WOS:000353214100010 ER PT J AU Peters, TJ Simon, JI Jones, JH Usui, T Moriwaki, R Economos, RC Schmitt, AK McKeegan, KD AF Peters, T. J. Simon, J. I. Jones, J. H. Usui, T. Moriwaki, R. Economos, R. C. Schmitt, A. K. McKeegan, K. D. TI Tracking the source of the enriched martian meteorites in olivine-hosted melt inclusions of two depleted shergottites, Yamato 980459 and Tissint SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE martian mantle melting; mantle depletion; olivine-phyric shergottites; olivine-hosted melt inclusions; Rare Earth Elements; crustal recycling ID MANTLE; MARS; YAMATO-980459; PETROGENESIS; CONSTRAINTS; ORIGIN; CLINOPYROXENE; SYSTEMATICS; MAGMATISM; EVOLUTION AB The apparent lack of plate tectonics on all terrestrial planets other than Earth has been used to support the notion that for most planets, once a primitive crust forms, the crust and mantle evolve geochemically-independent through time. This view has had a particularly large impact on models for the evolution of Mars and its silicate interior. Recent data indicating a greater potential that there may have been exchange between the martian crust and mantle has led to a search for additional geochemical evidence to support the alternative hypothesis, that some mechanism of crustal recycling may have operated early in the history of Mars. In order to study the most juvenile melts available to investigate martian mantle source(s) and melting processes, the trace element compositions of olivine-hosted melt inclusions for two incompatible-element-depleted olivine-phyric shergottites, Yamato 980459 (Y98) and Tissint, and the interstitial glass of Y98, have been measured by Secondary Ionization Mass Spectrometry (SIMS). Chondrite-normalized Rare Earth Element (REE) patterns for both Y98 and Tissint melt inclusions, and the Y98 interstitial glass, are characteristically light-REE depleted and parallel those of their host rock. For Y98, a clear flattening and upward inflection of La and Ce, relative to predictions based on middle and heavier REE, provides evidence for involvement of an enriched component early in their magmatic history; either inherited from a metasomatized mantle or crustal source, early on and prior to extensive host crystallization. Comparing these melt inclusion and interstitial glass analyses to existing melt inclusion and whole-rock data sets for the shergottite meteorite suite, defines mixing relationships between depleted and enriched end members, analogous to mixing relationships between whole rock Sr and Nd isotopic measurements. When considered in light of their petrologic context, the origin of these trace element enriched and isotopically evolved signatures represents either (1) crustal assimilation during the final few km of melt ascent towards the martian surface, or (2) assimilation soon after melt segregation, through melt-rock interaction with a portion of the martian crust recycled back into the mantle. (C) 2015 Elsevier B.V. All rights reserved. C1 [Peters, T. J.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Peters, T. J.; Simon, J. I.; Jones, J. H.] NASA, Johnson Space Ctr, Astromat Res & Explorat Sci, Houston, TX 77058 USA. [Peters, T. J.; Simon, J. I.] NASA, Johnson Space Ctr, Ctr Isotope Cosmochem & Geochronol, Houston, TX 77058 USA. [Usui, T.; Moriwaki, R.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Tokyo 1528551, Japan. [Economos, R. C.; Schmitt, A. K.; McKeegan, K. D.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. RP Peters, TJ (reprint author), Lunar & Planetary Inst, 3303 NASA Rd 1, Houston, TX 77058 USA. EM Peterstj2313@gmail.com RI McKeegan, Kevin/A-4107-2008; UCLA, SIMS/A-1459-2011; OI McKeegan, Kevin/0000-0002-1827-729X; Schmitt, Axel/0000-0002-9029-4211 FU NASA [NNX11AF57G]; Instrumentation and Facilities Program, Division of Earth Sciences, National Science Foundation FX We are grateful to Dr. Anne Peslier at Johnson Space Center (JSC) for assistance with Electron Microprobe analyses (EMPA), and Dr. Kent Ross and Dr. Eve Berger for assistance with the JSC Field Emission Scanning Electron Microscope. Editorial handling and suggestions by Tamsin Mather, and comments by David Baratoux and Jon Wade, significantly improved upon the original manuscript. NASA funding comes from the Mars Fundamental Research Program (NNX11AF57G). The ion microprobe facility at UCLA is partly supported by a grant from the Instrumentation and Facilities Program, Division of Earth Sciences, National Science Foundation. NR 59 TC 5 Z9 5 U1 1 U2 14 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 MAY 15 PY 2015 VL 418 BP 91 EP 102 DI 10.1016/j.epsl.2015.02.033 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CF6KI UT WOS:000352665200009 ER PT J AU Pankine, AA Tamppari, LK AF Pankine, Alexey A. Tamppari, Leslie K. TI Constraints on water vapor vertical distribution at the Phoenix landing site during summer from MGS TES day and night observations SO ICARUS LA English DT Article DE Mars; Mars, atmosphere; Infrared observations; Atmospheres, structure ID THERMAL EMISSION SPECTROMETER; MARS GLOBAL SURVEYOR; CONVECTIVE BOUNDARY-LAYER; ATMOSPHERIC TEMPERATURES; INTERANNUAL VARIABILITY; MARTIAN ATMOSPHERE; ICE CLOUDS; EXPRESS; SIMULATIONS; OCCULTATION AB We present a new method to retrieve column abundances and vertical extent of the water vapor from the Mars Global Surveyor (MGS) Thermal Emission Spectrometer (TES) spectra. The new method enables retrievals from the nighttime TES spectra. The retrieval algorithm employs a new model of the vertical distribution of water vapor in the martian atmosphere. In this model water vapor is confined to a layer of finite height in the lower atmosphere. The atmosphere is dry above this 'wet' layer. Within the 'wet' layer the water vapor has a constant mixing ratio below the water ice cloud condensation height and is saturated above that height. The new retrieval method simultaneously fits the daytime and nighttime TES spectra for a given location using a single mixing ratio profile. We apply this new method to the TES spectra collected over the site of the Phoenix spacecraft landing during late northern spring and summer. Retrieved daytime column abundances are similar to 1-5 pr-mu m higher than in the previous TES retrieval. Nighttime column abundances are lower than the daytime abundances by similar to 5-10 pr-mu m due to assumed exchange with soil and predicted water ice cloud formation. The height of the 'wet' layer varies with season, reaching similar to 18 km around L-s = 80-100 degrees and decreasing to 7-10 km by L-s = 140 degrees. Changes in the vertical extent of vapor are consistent with seasonal changes in the intensity of the turbulent mixing in the lower atmosphere and in the water ice cloud condensation height. Water vapor extends by several kilo-meters above the top of the boundary layer at similar to 4 km, suggesting that vertical transport of vapor is not limited to the boundary layer. (C) 2015 Elsevier Inc. All rights reserved. C1 [Pankine, Alexey A.] Space Sci Inst, Boulder, CO 80301 USA. [Tamppari, Leslie K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Pankine, AA (reprint author), Space Sci Inst, Boulder, CO 80301 USA. EM apankine@spacescience.com FU NASA Mars Data Analysis program [NNX13AE53G]; Jet Propulsion Laboratory FX This research was carried out at the Space Science Institute and Jet Propulsion Laboratory, California Institute of Technology, with funding from the NASA Mars Data Analysis program grant NNX13AE53G and Jet Propulsion Laboratory subcontract to Space Science Institute. NR 57 TC 2 Z9 2 U1 1 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 MAY 15 PY 2015 VL 252 BP 107 EP 120 DI 10.1016/j.icarus.2015.01.008 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CE8TW UT WOS:000352118000007 ER PT J AU Rodriguez, JAP Leonard, GJ Platz, T Tanaka, KL Kargel, JS Fairen, AG Gulick, V Baker, VR Glines, N Miyamoto, H Yan, JG Oguma, M AF Rodriguez, J. Alexis P. Leonard, Gregory J. Platz, Thomas Tanaka, Kenneth L. Kargel, Jeffrey S. Fairen, Alberto G. Gulick, Virginia Baker, Victor R. Glines, Natalie Miyamoto, Hideaki Yan Jianguo Oguma, Midori TI New insights into the Late Amazonian zonal shrinkage of the Martian south polar plateau (vol 248, pg 407, 2015) SO ICARUS LA English DT Correction C1 [Rodriguez, J. Alexis P.; Gulick, Virginia; Glines, Natalie] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rodriguez, J. Alexis P.; Platz, Thomas] Planetary Sci Inst, Tucson, AZ 85719 USA. [Leonard, Gregory J.; Kargel, Jeffrey S.; Baker, Victor R.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. [Platz, Thomas] Free Univ Berlin, Inst Geol Sci, Planetary Sci & Remote Sensing, D-12249 Berlin, Germany. [Tanaka, Kenneth L.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Fairen, Alberto G.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Gulick, Virginia] SETI Inst, Mountain View, CA 94043 USA. [Miyamoto, Hideaki; Oguma, Midori] Univ Tokyo, Univ Museum, Tokyo 1130033, Japan. [Yan Jianguo] Wuhan Univ, State Key Lab Informat Engn Surveying Mapping & R, Wuhan 430070, Peoples R China. RP Rodriguez, JAP (reprint author), NASA, Ames Res Ctr, Mail Stop 239-20, Moffett Field, CA 94035 USA. EM alexis@psi.edu RI Platz, Thomas/F-7539-2013; Miyamoto, Hideaki/B-9666-2008 OI Platz, Thomas/0000-0002-1253-2034; NR 1 TC 0 Z9 0 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAY 15 PY 2015 VL 252 BP 228 EP 228 DI 10.1016/j.icarus.2015.01.009 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CE8TW UT WOS:000352118000018 ER PT J AU Robinson, MS Boyd, AK Denevi, BW Lawrence, SJ McEwen, AS Moser, DE Povilaitis, RZ Stelling, RW Suggs, RM Thompson, SD Wagner, RV AF Robinson, Mark S. Boyd, Aaron K. Denevi, Brett W. Lawrence, Samuel J. McEwen, Alfred S. Moser, Danielle E. Povilaitis, Reinhold Z. Stelling, Richard W. Suggs, Robert M. Thompson, Shane D. Wagner, Robert V. TI New crater on the Moon and a swarm of secondaries SO ICARUS LA English DT Article DE Impact processes; Geological processes; Moon, surface; Moon; Regoliths ID ACCRETION RATE; LUNAR; METEORITES; DENSITY; FLUX AB Lunar Reconnaissance Orbiter Camera images acquired both before and after the formation of an 18.8 m diameter crater on 17 March 2013 reveal intricate details of ejecta distribution and the structure of the top two meters of the regolith. Our observations indicate that (I) the regolith is mature down to several tens of cm and immature below one meter, (2) surface reflectivity properties are affected for distances greater than fifty crater radii, and (3) large numbers of secondary impacts (splotches) formed up to 30 km distant from this new primary crater. These observations provide new knowledge of the distribution of ejected materials from small impact craters on the Moon, the modification of the top few cm of the regolith by micrometeorite impacts, and potential hazards to future explorers. (C) 2015 Elsevier Inc. All rights reserved. C1 [Robinson, Mark S.; Boyd, Aaron K.; Lawrence, Samuel J.; Povilaitis, Reinhold Z.; Stelling, Richard W.; Thompson, Shane D.; Wagner, Robert V.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Denevi, Brett W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [McEwen, Alfred S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Moser, Danielle E.] Marshall Space Flight Ctr, Meteoroid Environm Off, MITS Dynet, Huntsville, AL 35812 USA. [Suggs, Robert M.] Marshall Space Flight Ctr, Meteoroid Environm Off, Huntsville, AL 35812 USA. RP Robinson, MS (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. EM robinson@ser.asu.edu RI Denevi, Brett/I-6502-2012 OI Denevi, Brett/0000-0001-7837-6663 FU NASA LRO project FX We thank the NASA LRO and LROC operations team for acquiring the images that made this study possible; the NASA LRO project supported this study. NR 25 TC 10 Z9 10 U1 1 U2 12 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAY 15 PY 2015 VL 252 BP 229 EP 235 DI 10.1016/j.icarus.2015.01.019 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CE8TW UT WOS:000352118000019 ER PT J AU Vokrouhlicky, D Farnocchia, D Capek, D Chesley, SR Pravec, P Scheirich, P Muller, TG AF Vokrouhlicky, David Farnocchia, Davide Capek, David Chesley, Steven R. Pravec, Petr Scheirich, Petr Mueller, Thomas G. TI The Yarkovsky effect for 99942 Apophis SO ICARUS LA English DT Article DE Celestial mechanics; Asteroids, dynamics; Asteroids, rotation ID SPIN-STATE; ASTEROIDS; YORP; EARTH; ITOKAWA; MODEL; ASTROMETRY; STANDARDS; HAYABUSA; DENSITY AB We use the recently determined rotation state, shape, size and thermophysical model of Apophis to predict the strength of the Yarkovsky effect in its orbit. Apophis does not rotate about the shortest principal axis of the inertia tensor, rather its rotational angular momentum vector wobbles at an average angle of similar or equal to 37 degrees from the body axis. Therefore, we pay special attention to the modeling of the Yarkovsky effect for a body in such a tumbling state, a feature that has not been described in detail so far. Our results confirm that the Yarkovsky effect is not significantly weakened by the tumbling state. The previously stated rule that the Yarkovsky effect for tumbling kilometer-size asteroids is well represented by a simple model assuming rotation about the shortest body axis in the direction of the rotational angular momentum and with rotation period close to the precession period is confirmed. Taking into account uncertainties of the model parameters, as well as the expected density distribution for Apophis' spectral class, we predict the secular change in the semimajor axis is (-12.8 +/- 3.6) x 10(-4) au/Myr (formal 1 cr uncertainty). The currently available astrometric data for Apophis do not allow an unambiguous direct detection of the Yarkovsky effect. However, the fitted secular change in semimajor axis of (-23 +/- 13) x 10(-4) au/Myr is compatible with the model prediction. We revise the Apophis' impact probability information in the second half of this century by extending the orbital uncertainty derived from the current astrometric data and by taking into account the uncertainty in the dynamical model due to the thermal recoil accelerations. This is done by mapping the combined uncertainty to the close encounter in 2029 and by determining the statistical weight of the known keyholes leading to resonant impact orbits. Whereas collision with the Earth before 2060 is ruled out, impacts are still possible from 2060 with probabilities up to a few parts in a million. More definitive analysis will be available after the Apophis apparition in 2020-2021. (C) 2015 Elsevier Inc. All rights reserved. C1 [Vokrouhlicky, David] Charles Univ Prague, Inst Astron, CZ-18000 Prague 8, Czech Republic. [Farnocchia, Davide; Chesley, Steven R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Capek, David; Pravec, Petr; Scheirich, Petr] Acad Sci Czech Republic, Astron Inst, CZ-25165 Ondrejov, Czech Republic. [Mueller, Thomas G.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. RP Vokrouhlicky, D (reprint author), Charles Univ Prague, Inst Astron, V Holesovickach 2, CZ-18000 Prague 8, Czech Republic. EM vokrouhl@cesnet.cz RI Pravec, Petr/G-9037-2014; Scheirich, Peter/H-4331-2014; Capek, David/G-9005-2014 OI Scheirich, Peter/0000-0001-8518-9532; FU Czech Grant Agency [P209/12/0229, P209-13-01308S] FX We thank the anonymous referees for suggestions that helped to improve the original version of this paper. This work was supported by the Czech Grant Agency (Grants P209/12/0229 and P209-13-01308S). D. Farnocchia and S.R. Chesley conducted this research at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 45 TC 6 Z9 6 U1 0 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 MAY 15 PY 2015 VL 252 BP 277 EP 283 DI 10.1016/j.icarus.2015.01.011 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CE8TW UT WOS:000352118000023 ER PT J AU Ore, CMD Barucci, MA Emery, JP Cruikshank, DP de Bergh, C Roush, TL Perna, D Merlin, F Ore, LVD AF Ore, C. Morea Dalle Barucci, M. A. Emery, J. P. Cruikshank, D. P. de Bergh, C. Roush, T. L. Perna, D. Merlin, F. Ore, L. V. Dalle TI The composition of "ultra-red" TNOs and centaurs SO ICARUS LA English DT Article DE Trans-neptunian objects; Centaurs; Ices, IR spectroscopy; Photometry ID KUIPER-BELT OBJECTS; TRANS-NEPTUNIAN OBJECTS; ESO LARGE PROGRAM; OUTER SOLAR-SYSTEM; NEAR-INFRARED SPECTROSCOPY; 47171 1999 TC36; TRANSNEPTUNIAN OBJECTS; 5145 PHOLUS; 90377 SEDNA; MU-M AB We present an analysis of the colors available for seven trans-neptunian objects (TNOs) and three centaurs among the reddest known, aimed at characterizing their surface chemical properties. In particular we seek to obtain evidence in support of the proposed correlation between the visible coloration of the surface of TNOs and their surface compositions (Brown, M.E., Schaller, EL., Fraser, W.C. [2011]. Astrophys. J. 739, L60). The analysis focuses on nine available colors in the visible-near IR (0.3-4.5 gm) spectral range scaled to the V albedo to provide a proxy for the spectral shape of the objects. The colors include Spitzer IRAC data never published before, key in providing an effective constraint in the discrimination of ices contributing to the surface composition of the objects. Compositions are obtained by comparing the data to a grid of radiative transfer models convolved by the filter response functions of the colors adopted in the spectrum-proxies to match the resolution of the observations. We find evidence suggesting the presence of hydrocarbons and/or methanol on the surfaces of most objects in our sample, supporting the hypothesis by Brown et al. (Brown, M.E., Schaller, E.L., Fraser, W.C. [2011]. Astrophys. J. 739, L60) that the coloration of red TNOs could be linked to their methanol content. From our finding of methanol/hydrocarbon ices on the surfaces of the objects in our sample of very red TNOs and centaurs we infer that ultra-red objects in general might contain these ices and therefore might have formed in the outer part of the Solar System. We also deduce that the surfaces of most of the very red TNOs in our dataset are probably still quite pristine, and that their organic materials could have been produced by irradiation of the volatile ices whose traces are still present on their surface. Although our sample is small, we infer that the irradiation process is still in progress, as hinted by the centaurs' slightly elevated organic amounts at smaller perihelion distances. However, considering the relatively similar amounts of organics found in our data at a wide variety of perihelion distances, we also infer that it could have started before Neptune's migration. The technique used to constrain the composition described as part of this study introduces a new approach at investigating the surface chemistry of the very small and numerous objects that constitute the bulk of the TNO and centaur populations. This innovative method has the potential to provide constraints for irradiation theories and for models of dynamical and chemical evolution of the Solar System. (C) 2015 Elsevier Inc. All rights reserved. C1 [Ore, C. Morea Dalle] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Ore, C. Morea Dalle; Cruikshank, D. P.; Roush, T. L.; Ore, L. V. Dalle] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Barucci, M. A.; de Bergh, C.; Perna, D.; Merlin, F.] Univ Paris Diderot, Univ Paris 06, LESIA Observ Paris, CNRS, F-92195 Meudon, France. [Emery, J. P.] Univ Tennessee, Earth & Planetary Sci Dept, Knoxville, TN 37919 USA. RP Ore, CMD (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA. EM Cristina.M.DalleOre@nasa.gov FU Outer Planets Research grant [NASA NNX12AM75G]; NASA Planetary Astronomy grant [NNX10AB23G]; NASA FX CMDO and JPE acknowledge support from the Outer Planets Research grant NASA NNX12AM75G and NASA Planetary Astronomy grant NNX10AB23G. This work is based [in part] on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 138 TC 1 Z9 1 U1 0 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAY 15 PY 2015 VL 252 BP 311 EP 326 DI 10.1016/j.icarus.2015.01.014 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CE8TW UT WOS:000352118000026 ER PT J AU Estrada, PR Durisen, RH Cuzzi, JN Morgan, DA AF Estrada, Paul R. Durisen, Richard H. Cuzzi, Jeffrey N. Morgan, Demitri A. TI Combined structural and compositional evolution of planetary rings due to micrometeoroid impacts and ballistic transport SO ICARUS LA English DT Article DE Planetary rings; Saturn, rings; Impact processes; Disks ID PARTICLE EROSION MECHANISMS; SATURNS MAIN RINGS; SELF-GRAVITY WAKES; CASSINI VIMS; NUMERICAL SIMULATIONS; VELOCITY DISPERSION; SIZE DISTRIBUTIONS; METEOROID IMPACTS; B-RING; INSTABILITY AB We introduce improved numerical techniques for simulating the structural and compositional evolution of planetary rings due to micrometeoroid bombardment and subsequent ballistic transport of impact ejecta. Our current, robust code is capable of modeling structural changes and pollution transport simultaneously over long times on both local and global scales. In this paper, we describe the methodology based on the original structural code of Durisen et al. (Durisen, RH. et al. [1989]. Icarus 80,136-166) and on the pollution transport code of Cuzzi and Estrada (Cuzzi, J.N., Estrada, P.R. [1998]. Icarus 132, 1-35). We provide demonstrative simulations to compare with, and extend upon previous work, as well as examples of how ballistic transport can maintain the observed structure in Saturn's rings using available Cassini occultation optical depth data. In particular, we explicitly verify the claim that the inner B (and presumably A) ring edge can be maintained over long periods of time due to an ejecta distribution that is heavily biased in the prograde direction through a balance between the sharpening effects of ballistic transport and the broadening effects of viscosity. We also see that a "ramp"-like feature forms over time just inside that edge. However, it does not remain linear for the duration of the runs presented here unless a less steep ejecta velocity distribution is adopted. We also model the C ring plateaus and find that their outer edges can be maintained at their observed sharpness for long periods due to ballistic transport. We hypothesize that the addition of a significant component of a retrograde-biased ejecta distribution may help explain the linearity of the ramp and could provide a mechanism for maintaining the sharpness of C ring plateau inner edges. This component would arise for the subset of micrometeoroid impacts which are destructive rather than merely cratering. Such a distribution will be introduced in future work. (C) 2015 Elsevier Inc. All rights reserved. C1 [Estrada, Paul R.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Durisen, Richard H.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. [Cuzzi, Jeffrey N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Morgan, Demitri A.] NASA, USRA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Estrada, PR (reprint author), SETI Inst, Carl Sagan Ctr, 189 N Bernardo Ave 100, Mountain View, CA 94043 USA. EM Paul.R.Estrada@nasa.gov FU NASA's Cassini Data Analysis Program; Cassini IDS grant FX The authors warmly thank Henrik Latter and Jurgen Schmidt for their thoughtful and thorough reviews of this work which has led to great improvement in its exposition. We thank Josh Colwell and Glen Stewart for useful discussions. This work was supported by a grant from NASA's Cassini Data Analysis Program (PRE), and a Cassini IDS grant to JNC. NR 78 TC 2 Z9 2 U1 0 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 MAY 15 PY 2015 VL 252 BP 415 EP 439 DI 10.1016/j.icarus.2015.02.005 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CE8TW UT WOS:000352118000034 ER PT J AU Gerakines, PA Hudson, RL AF Gerakines, Perry A. Hudson, Reggie L. TI The radiation stability of glycine in solid CO2 - In situ laboratory measurements with applications to Mars SO ICARUS LA English DT Article DE Astrobiology; Cosmochemistry; Ices, IR spectroscopy; Mars ID SOLAR-SYSTEM BODIES; AMINO-ACIDS; ULTRAVIOLET PHOTOLYSIS; WATER; ICE; SURFACE; SPACE; RADIOLYSIS; MATRIX AB The detection of biologically important, organic molecules on Mars is an important goal that may soon be reached. However, the current small number of organic detections at the martian surface may be due to the harsh UV and radiation conditions there. It seems likely that a successful search will require probing the subsurface of Mars, where penetrating cosmic rays and solar energetic particles dominate the radiation environment, with an influence that weakens with depth. Toward the goal of understanding the survival of organic molecules in cold radiation-rich environments on Mars, we present new kinetics data on the radiolytic destruction of glycine diluted in frozen carbon dioxide. Rate constants were measured in situ with infrared spectroscopy, without additional sample manipulation, for irradiations at 25, 50, and 75 K with 0.8-MeV protons. The resulting half-lives for glycine in CO2-ice are compared to previous results for glycine in H2O-ice and show that glycine in CO2-ice is much less stable in a radiation environment, with destruction rate constants similar to 20-40 times higher than glycine in H2O-ice. Extrapolation of these results to conditions in the martian subsurface results in half-lives estimated to be less than 100-200 Myr even at depths of a few meters. Published by Elsevier C1 [Gerakines, Perry A.; Hudson, Reggie L.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. RP Gerakines, PA (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Code 691, Greenbelt, MD 20771 USA. EM perty.a.gerakines@nasa.gov RI Gerakines, Perry/D-2226-2012 OI Gerakines, Perry/0000-0002-9667-5904 NR 30 TC 3 Z9 3 U1 4 U2 20 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 MAY 15 PY 2015 VL 252 BP 466 EP 472 DI 10.1016/j.icarus.2015.02.008 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CE8TW UT WOS:000352118000037 ER PT J AU Hume, KL Bayes, KD Sander, SP AF Hume, Kelly L. Bayes, Kyle D. Sander, Stanley P. TI Equilibrium Constant for the Reaction ClO plus ClO <-> ClOOCl Between 250 and 206 K SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID CHLORINE PEROXIDE; ULTRAVIOLET-ABSORPTION; SELF-REACTION; NM; TEMPERATURE; KINETICS; OZONE; SPECTRUM; BAND; CHLOROFLUOROMETHANES AB The chlorine peroxide molecule, ClOOCl is an important participant in the chlorine-catalyzed destruction of ozone in the stratosphere. Very few laboratory measurements have been made for the partitioning between monomer ClO and dimer ClOOCl at temperatures lower than 280 K. This paper reports absorption spectra for both ClO and ClOOCl when they are in equilibrium at 1 atm and temperatures down to 206 K. The very low ClO concentrations involved requires measuring and calibrating a differential cross section, Delta sigma(ClO), for the 10-0 band Of ClO. A third law fit of the new results gives K-eq = [(2.01 +/- 0.17) 10(-27) cm(3) molecule(-1)] e((8554 -/+ 21)K/T), where the error limits reflect the uncertainty in the entropy change. The resulting equilibrium constants. are slightly lower than currently recommended. The slope of the van't Hoff plot yields a value for the enthalpy of formation of ClOOCl at 298 K, Delta H-f(o) of 129.8 +/- 0.6 kJ mol(-1). Uncertainties in the absolute ultraviolet cross sections of ClOOCl and ClO appear to be the limiting factors in these measurements. The new K-eq parameters are consistent with the measurements of Santee et al.(42) in the stratosphere. C1 [Hume, Kelly L.; Bayes, Kyle D.; Sander, Stanley P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bayes, KD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Kyle.D.Bayes@jpl.nasa.gov FU National Aeronautics and Space Administration; Upper Atmosphere Research and Tropospheric Chemistry programs; JPL Postdoctoral Program FX This work acknowledges the pioneering contributions of Mario Molina and his colleagues in elucidating the role of ClOOCl in the catalytic destruction of ozone in the polar stratosphere. We thank John Barker, University of Michigan, for access to his entropy calculations for ClO and ClOOCl and for several useful discussions. This research was carried out by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This work was supported by the Upper Atmosphere Research and Tropospheric Chemistry programs and the JPL Postdoctoral Program. NR 40 TC 2 Z9 2 U1 3 U2 14 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD MAY 14 PY 2015 VL 119 IS 19 BP 4473 EP 4481 DI 10.1021/jp510100n PG 9 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA CI6YV UT WOS:000354911000020 PM 25560546 ER PT J AU Hwang, SA Crucian, B Sams, C Actor, JK AF Hwang, Shen-An Crucian, Brian Sams, Clarence Actor, Jeffrey K. TI Post-Spaceflight (STS-135) Mouse Splenocytes Demonstrate Altered Activation Properties and Surface Molecule Expression SO PLOS ONE LA English DT Article ID IMMUNE-SYSTEM DYSREGULATION; EPSTEIN-BARR-VIRUS; PERIPHERAL-BLOOD LEUKOCYTES; SHORT-DURATION SPACEFLIGHT; SPACE-FLIGHT; HUMAN-LYMPHOCYTES; LACTOFERRIN MODULATION; CYTOKINE PRODUCTION; EPIGENETIC CHANGES; APPLIED PHYSIOLOGY AB Alterations in immune function have been documented during or post-spaceflight and in ground based models of microgravity. Identification of immune parameters that are dysregulated during spaceflight is an important step in mitigating crew health risks during deep space missions. The in vitro analysis of leukocyte activity post-spaceflight in both human and animal species is primarily focused on lymphocytic function. This report completes a broader spectrum analysis of mouse lymphocyte and monocyte changes post 13 days orbital flight (mission STS-135). Analysis includes an examination in surface markers for cell activation, and antigen presentation and co-stimulatory molecules. Cytokine production was measured after stimulation with T-cell mitogen or TLR-2, TLR-4, or TLR-5 agonists. Splenocyte surface marker analysis immediate post-spaceflight and after in vitro culture demonstrated unique changes in phenotypic populations between the flight mice and matched treatment ground controls. Post-spaceflight splenocytes (flight splenocytes) had lower expression intensity of CD4(+)CD25(+) and CD8(+)CD25(+) cells, lower percentage of CD11c(+)MHC II+ cells, and higher percentage of CD11c(+)MHC I+ populations compared to ground controls. The flight splenocytes demonstrated an increase in phagocytic activity. Stimulation with ConA led to decrease in CD4(+) population but increased CD4(+)CD25(+) cells compared to ground controls. Culturing with TLR agonists led to a decrease in CD11c(+) population in splenocytes isolated from flight mice compared to ground controls. Consequently, flight splenocytes with or without TLR-agonist stimulation showed a decrease in CD11c+MHC I+, CD11c(+)MHC II+, and CD11c(+)CD86(+) cells compared to ground controls. Production of IFN-gamma was decreased and IL-2 was increased from ConA stimulated flight splenocytes. This study demonstrated that expression of surface molecules can be affected by conditions of spaceflight and impaired responsiveness persists under culture conditions in vitro. C1 [Hwang, Shen-An; Actor, Jeffrey K.] Univ Texas Houston, Sch Med, Dept Pathol & Lab Med, Houston, TX 77030 USA. [Crucian, Brian] NASA, Lyndon B Johnson Space Ctr, Div Biomed & Environm Sci, Houston, TX 77058 USA. [Sams, Clarence] NASA, Lyndon B Johnson Space Ctr, Space & Clin Operat Div, Houston, TX 77058 USA. RP Actor, JK (reprint author), Univ Texas Houston, Sch Med, Dept Pathol & Lab Med, Houston, TX 77030 USA. EM Jeffrey.K.Actor@uth.tmc.edu OI Actor, Jeffrey/0000-0002-9265-7012 NR 63 TC 3 Z9 5 U1 0 U2 4 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 MAY 13 PY 2015 VL 10 IS 5 AR e0124380 DI 10.1371/journal.pone.0124380 PG 19 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CI1ZP UT WOS:000354544200037 PM 25970640 ER PT J AU Goldstein, ML Wicks, RT Perri, S Sahraoui, F AF Goldstein, M. L. Wicks, R. T. Perri, S. Sahraoui, F. TI Kinetic scale turbulence and dissipation in the solar wind: key observational results and future outlook SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Review DE solar wind; turbulence; plasma heating; turbulent dissipation ID ION-CYCLOTRON WAVES; INTERPLANETARY MAGNETIC-FIELD; OUTWARD PROPAGATING WAVES; ELECTRON HEAT-CONDUCTION; FREQUENCY ALFVEN WAVES; 1 AU; MAGNETOHYDRODYNAMIC TURBULENCE; SHELL-MODEL; HALL MAGNETOHYDRODYNAMICS; HOMOGENEOUS TURBULENCE AB Turbulence is ubiquitous in the solar wind. Turbulence causes kinetic and magnetic energy to cascade to small scales where they are eventually dissipated, adding heat to the plasma. The details of how this occurs are not well understood. This article reviews the evidence for turbulent dissipation and examines various diagnostics for identifying solar wind regions where dissipation is occurring. We also discuss how future missions will further enhance our understanding of the importance of turbulence to solar wind dynamics. C1 [Goldstein, M. L.; Wicks, R. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wicks, R. T.] Univ Maryland, Dept Astron, GPHI, College Pk, MD 20742 USA. [Perri, S.] Univ Calabria, Dipartimento Fis, I-87036 Arcavacata Di Rende, Italy. [Sahraoui, F.] Ecole Polytech, CNRS UPMC, Lab Phys Plasmas, F-91128 Palaiseau, France. RP Goldstein, ML (reprint author), NASA, Goddard Space Flight Ctr, Code 672, Greenbelt, MD 20771 USA. EM melvyn.l.goldstein@nasa.gov RI Wicks, Robert/A-1180-2009 OI Wicks, Robert/0000-0002-0622-5302 FU NASA GI grant; NASA HSR grant at Goddard Space Flight Center; Borsa Postdoc POR Calabria FSE; project THESOW - L'Agence Nationale de la Recherche (ANR, France) FX R.T.W. is funded by a NASA GI grant and a NASA HSR grant at Goddard Space Flight Center. S.P.'s research is supported by 'Borsa Postdoc POR Calabria FSE 2007/2013'. F.S. was supported, in part, by the project THESOW funded by L'Agence Nationale de la Recherche (ANR, France). NR 150 TC 10 Z9 10 U1 2 U2 25 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1364-503X EI 1471-2962 J9 PHILOS T R SOC A JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci. PD MAY 13 PY 2015 VL 373 IS 2041 AR 20140147 DI 10.1098/rsta.2014.0147 PG 21 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CG5BK UT WOS:000353304500004 ER PT J AU Roytershteyn, V Karimabadi, H Roberts, A AF Roytershteyn, Vadim Karimabadi, Homa Roberts, Aaron TI Generation of magnetic holes in fully kinetic simulations of collisionless turbulence SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Article DE plasma turbulence; magnetic holes; fully kinetic simulations ID SOLAR-WIND; PLASMA; FIELD AB The results of three-dimensional fully kinetic simulations of decaying turbulence with the amplitude of the fluctuating magnetic field comparable to that of the mean field are presented. Coherent structures in the form of localized depressions in the magnitude of the magnetic field are observed to form self-consistently in the simulations. These depressions bear considerable resemblance to the so-called magnetic holes frequently reported in spacecraft observations. The structures are pressure-balanced and tend to be aligned with the local magnetic field. In the smallest structures observed, the decrease in the magnetic field strength is compensated by an increase in the electron perpendicular pressure, such that the transverse size of these structures is comparable to the electron gyroradius inside the depression. It is suggested that the structures evolve self-consistently out of the depressions in the fluctuating magnetic field, rather than being the consequence of instability growth and saturation. This is confirmed by additional, small-scale simulations, including those with realistic mass ratio between protons and electrons. C1 [Roytershteyn, Vadim; Karimabadi, Homa] SciberQuest Inc, Del Mar, CA 92014 USA. [Roytershteyn, Vadim] Space Sci Inst, Boulder, CO 80301 USA. [Roberts, Aaron] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Roytershteyn, V (reprint author), SciberQuest Inc, Del Mar, CA 92014 USA. EM vroytershteyn@spacescience.org OI Roytershteyn, Vadim/0000-0003-1745-7587 FU NASA at SSI [NNX14AI63G]; National Science Foundation [OCI-0725070, ACI-1238993]; State of Illinois FX We gratefully acknowledge support from NASA grant NNX14AI63G at SSI. This research is part of the Blue Waters sustained-petascale computing project, which is supported by the National Science Foundation (awards OCI-0725070 and ACI-1238993) and the State of Illinois. Blue Waters is a joint effort of the University of Illinois at Urbana-Champaign and its National Center for Supercomputing Applications. Additional simulations were performed on the Pleiades supercomputer provided by the NASA HEC program. NR 21 TC 9 Z9 9 U1 1 U2 5 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1364-503X EI 1471-2962 J9 PHILOS T R SOC A JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci. PD MAY 13 PY 2015 VL 373 IS 2041 AR 20140151 DI 10.1098/rsta.2014.0151 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CG5BK UT WOS:000353304500008 ER PT J AU Papadopoulos, A D'Andrea, CB Sullivan, M Nichol, RC Barbary, K Biswas, R Brown, PJ Covarrubias, RA Finley, DA Fischer, JA Foley, RJ Goldstein, D Gupta, RR Kessler, R Kovacs, E Kuhlmann, SE Lidman, C March, M Nugent, PE Sako, M Smith, RC Spinka, H Wester, W Abbott, TMC Abdalla, F Allam, SS Banerji, M Bernstein, JP Bernstein, RA Carnero, A da Costa, LN DePoy, DL Desai, S Diehl, HT Eifler, T Evrard, AE Flaugher, B Frieman, JA Gerdes, D Gruen, D Honscheid, K James, D Kuehn, K Kuropatkin, N Lahav, O Maia, MAG Makler, M Marshall, JL Merritt, KW Miller, CJ Miquel, R Ogando, R Plazas, AA Roe, NA Romer, AK Rykoff, E Sanchez, E Santiago, BX Scarpine, V Schubnell, M Sevilla, I Soares-Santos, M Suchyta, E Swanson, M Tarle, G Thaler, J Tucker, LD Wechsler, RH Zuntz, J AF Papadopoulos, A. D'Andrea, C. B. Sullivan, M. Nichol, R. C. Barbary, K. Biswas, R. Brown, P. J. Covarrubias, R. A. Finley, D. A. Fischer, J. A. Foley, R. J. Goldstein, D. Gupta, R. R. Kessler, R. Kovacs, E. Kuhlmann, S. E. Lidman, C. March, M. Nugent, P. E. Sako, M. Smith, R. C. Spinka, H. Wester, W. Abbott, T. M. C. Abdalla, F. Allam, S. S. Banerji, M. Bernstein, J. P. Bernstein, R. A. Carnero, A. da Costa, L. N. DePoy, D. L. Desai, S. Diehl, H. T. Eifler, T. Evrard, A. E. Flaugher, B. Frieman, J. A. Gerdes, D. Gruen, D. Honscheid, K. James, D. Kuehn, K. Kuropatkin, N. Lahav, O. Maia, M. A. G. Makler, M. Marshall, J. L. Merritt, K. W. Miller, C. J. Miquel, R. Ogando, R. Plazas, A. A. Roe, N. A. Romer, A. K. Rykoff, E. Sanchez, E. Santiago, B. X. Scarpine, V. Schubnell, M. Sevilla, I. Soares-Santos, M. Suchyta, E. Swanson, M. Tarle, G. Thaler, J. Tucker, L. D. Wechsler, R. H. Zuntz, J. TI DES13S2cmm: the first superluminous supernova from the Dark Energy Survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; supernovae: general; supernovae: individual: DES13S2cmm ID BARYON ACOUSTIC-OSCILLATIONS; HUBBLE-SPACE-TELESCOPE; IA SUPERNOVAE; HIGH-REDSHIFT; LUMINOUS SUPERNOVAE; PAIR-INSTABILITY; LIGHT-CURVE; COSMOLOGICAL CONSTRAINTS; ULTRALUMINOUS SUPERNOVAE; IC SUPERNOVAE AB We present DES13S2cmm, the first spectroscopically-confirmed superluminous supernova (SLSN) from the Dark Energy Survey (DES). We briefly discuss the data and search algorithm used to find this event in the first year of DES operations, and outline the spectroscopic data obtained from the European Southern Observatory (ESO) Very Large Telescope to confirm its redshift (z = 0.663 +/- 0.001 based on the host-galaxy emission lines) and likely spectral type (Type I). Using this redshift, we find M-U(peak) = -21.05(-0.09)(+0.10) for the peak, rest-frame U-band absolute magnitude, and find DES13S2cmm to be located in a faint, low-metallicity (subsolar), low stellar-mass host galaxy (log (M/M-circle dot) = 9.3 +/- 0.3), consistent with what is seen for other SLSNe-I. We compare the bolometric light curve of DES13S2cmm to 14 similarly well-observed SLSNe-I in the literature and find that it possesses one of the slowest declining tails (beyond +30 d rest-frame past peak), and is the faintest at peak. Moreover, we find the bolometric light curves of all SLSNe-I studied herein possess a dispersion of only 0.2-0.3 mag between +25 and +30 d after peak (rest frame) depending on redshift range studied; this could be important for 'standardizing' such supernovae, as is done with the more common Type Ia. We fit the bolometric light curve of DES13S2cmm with two competing models for SLSNe-I-the radioactive decay of Ni-56, and a magnetar - and find that while the magnetar is formally a better fit, neither model provides a compelling match to the data. Although we are unable to conclusively differentiate between these two physical models for this particular SLSN-I, further DES observations of more SLSNe-I should break this degeneracy, especially if the light curves of SLSNe-I can be observed beyond 100 d in the rest frame of the supernova. C1 [Papadopoulos, A.; D'Andrea, C. B.; Nichol, R. C.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Sullivan, M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Barbary, K.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Biswas, R.; Gupta, R. R.; Kovacs, E.; Kuhlmann, S. E.; Spinka, H.; Bernstein, J. P.] Argonne Natl Lab, Argonne, IL 60439 USA. [Brown, P. J.; DePoy, D. L.; Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX USA. [Covarrubias, R. A.; Allam, S. S.; Swanson, M.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA. [Covarrubias, R. A.; Foley, R. J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Finley, D. A.; Wester, W.; Diehl, H. T.; Flaugher, B.; Frieman, J. A.; Kuropatkin, N.; Merritt, K. W.; Scarpine, V.; Soares-Santos, M.; Tucker, L. D.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Fischer, J. A.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Foley, R. J.; Thaler, J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Goldstein, D.; Nugent, P. E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Goldstein, D.; Nugent, P. E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Kessler, R.; Frieman, J. A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Kessler, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Lidman, C.] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Smith, R. C.; Abbott, T. M. C.; James, D.] Natl Optic Astron Observ, Ctr Tololo Interamer Observ, La Serena, Chile. [Abdalla, F.; Banerji, M.; Lahav, O.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Allam, S. S.] Space Telescope Sci Inst STScI, Baltimore, MD 21218 USA. [Bernstein, R. A.] Carnegie Observ, Pasadena, CA 91101 USA. [Carnero, A.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carnero, A.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.; Santiago, B. X.] Lab Interinst E Astron LIneA, BR-20921400 Rio De Janeiro, RJ, Brazil. [Desai, S.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Desai, S.] Excellence Cluster Universe, D-85748 Garching, Germany. [Eifler, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Evrard, A. E.; Gerdes, D.; Miller, C. J.; Schubnell, M.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Evrard, A. E.; Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Gruen, D.] Univ Observ Munich, D-81679 Munich, Germany. [Gruen, D.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Honscheid, K.; Suchyta, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Makler, M.] Ctr Brasileiro Pesquisas Fis, ICRA, BR-22290180 Rio De Janeiro, RJ, Brazil. [Miquel, R.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain. [Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Plazas, A. A.] Brookhaven Natl Lab, Dept Phys, Upton, NY 11973 USA. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Rykoff, E.; Sevilla, I.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Sanchez, E.] Ctr Invest Energet Medioambientales & Tecnol CIEM, E-28040 Madrid, Spain. [Santiago, B. X.] Univ Fed Rio Grande do Sul, Inst Fis, BR-91501970 Porto Alegre, RS, Brazil. [Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Zuntz, J.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. RP Papadopoulos, A (reprint author), Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg,Burnaby Rd, Portsmouth PO1 3FX, Hants, England. EM andreas.papadopoulos@port.ac.uk RI Ogando, Ricardo/A-1747-2010; Sanchez, Eusebio/H-5228-2015; Makler, Martin/G-2639-2012; OI Ogando, Ricardo/0000-0003-2120-1154; Sanchez, Eusebio/0000-0002-9646-8198; Makler, Martin/0000-0003-2206-2651; Suchyta, Eric/0000-0002-7047-9358; Evrard, August/0000-0002-4876-956X; Abdalla, Filipe/0000-0003-2063-4345; Sullivan, Mark/0000-0001-9053-4820 FU SEPnet; Faculty of Technology of the University of Portsmouth; Royal Society; EU/FP7-ERC [615929]; NASA; ESO telescopes at the La Silla Paranal Observatory under DDT programme [ID 292.D-5013]; 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; 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; 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; associated Excellence Cluster Universe; University of Michigan; National Optical Astronomy Observatory; University of Nottingham; Ohio State University; University of Pennsylvania; University of Portsmouth; SLAC National Accelerator Laboratory; Stanford University; University of Sussex; Texas AM University FX We wish to thank Kate Maguire for her assistance with the ESO VLT Directors Discretionary Time proposal. We also thank Cosimo Inserra and Stephen Smartt for helpful discussions regarding the classification, standardization and k-corrections of superluminous supernovae. AP acknowledges the financial support of SEPnet (www.sepnet.ac.uk) and the Faculty of Technology of the University of Portsmouth. Likewise, CD and RN thank the support of the Faculty of Technology of the University of Portsmouth during this research, and MS acknowledges support from the Royal Society and EU/FP7-ERC grant no [615929]. Part of TE's research was carried out at JPL/Caltech, under a contract with NASA.; Based on observations made with ESO telescopes at the La Silla Paranal Observatory under DDT programme ID 292.D-5013.; We are grateful for the extraordinary contributions of our CTIO colleagues and the DES Camera, 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 organization. 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, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia e Tecnologia, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey.; The 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 67 TC 17 Z9 17 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 11 PY 2015 VL 449 IS 2 BP 1215 EP 1227 DI 10.1093/mnras/stv174 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2TN UT WOS:000355337500003 ER PT J AU Shimwell, TW Markevitch, M Brown, S Feretti, L Gaensler, BM Johnston-Hollitt, M Lage, C Srinivasan, R AF Shimwell, Timothy W. Markevitch, Maxim Brown, Shea Feretti, Luigina Gaensler, B. M. Johnston-Hollitt, M. Lage, Craig Srinivasan, Raghav TI Another shock for the Bullet cluster, and the source of seed electrons for radio relics SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE acceleration of particles; radiation mechanisms: non-thermal; shock waves; galaxies: clusters: individual: 1E 0657-55.8; galaxies: clusters: intracluster medium; radio continuum general ID MERGING GALAXY CLUSTER; X-RAY OBSERVATIONS; HOTTEST KNOWN CLUSTER; CHANDRA OBSERVATION; COMA CLUSTER; 1E 0657-56; PARTICLE-ACCELERATION; INTRACLUSTER MEDIUM; CIZA J2242.8+5301; ABELL 2146 AB With Australia Telescope Compact Array observations, we detect a highly elongated Mpc-scale diffuse radio source on the eastern periphery of the Bullet cluster 1E 0657-55.8, which we argue has the positional, spectral and polarimetric characteristics of a radio relic. This powerful relic (2.3 +/- 0.1 x 10(25) W Hz(-1)) consists of a bright northern bulb and a faint linear tail. The bulb emits 94 per cent of the observed radio flux and has the highest surface brightness of any known relic. Exactly coincident with the linear tail, we find a sharp X-ray surface brightness edge in the deep Chandra image of the cluster - a signature of a shock front in the hot intracluster medium (ICM), located on the opposite side of the cluster to the famous bow shock. This new example of an X-ray shock coincident with a relic further supports the hypothesis that shocks in the outer regions of clusters can form relics via diffusive shock (re-) acceleration. Intriguingly, our new relic suggests that seed electrons for reacceleration are coming from a local remnant of a radio galaxy, which we are lucky to catch before its complete disruption. If this scenario, in which a relic forms when a shock crosses a well-defined region of the ICM polluted with aged relativistic plasma - as opposed to the usual assumption that seeds are uniformly mixed in the ICM - is also the case for other relics, this may explain a number of peculiar properties of peripheral relics. C1 [Shimwell, Timothy W.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Shimwell, Timothy W.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Markevitch, Maxim] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Brown, Shea] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Feretti, Luigina] INAF Ist Radioastron, I-40129 Bologna, Italy. [Gaensler, B. M.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Johnston-Hollitt, M.; Srinivasan, Raghav] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6014, New Zealand. [Lage, Craig] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. RP Shimwell, TW (reprint author), CSIRO Astron & Space Sci, Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia. EM tws29@mrao.cam.ac.uk FU Commonwealth of Australia; Australian Research Council [FL100100114]; Marsden Fund FX The ATCA is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. BMG acknowledges the support of Australian Laureate Fellowship FL100100114 from the Australian Research Council. MJH acknowledges support from the Marsden Fund. MJH acknowledges support from the Marsden Fund. We thank Douglas Clowe for kindly providing the R-band image and we thank the anonymous referee for comments. NR 61 TC 23 Z9 23 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 11 PY 2015 VL 449 IS 2 BP 1486 EP 1494 DI 10.1093/mnras/stv334 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2TN UT WOS:000355337500027 ER PT J AU Smith, N Mauerhan, JC Cenko, SB Kasliwal, MM Silverman, JM Filippenko, AV Gal-Yam, A Clubb, KI Graham, ML Leonard, DC Horst, JC Williams, GG Andrews, JE Kulkarni, SR Nugent, P Sullivan, M Maguire, K Xu, D Ben-Ami, S AF Smith, Nathan Mauerhan, Jon C. Cenko, S. Bradley Kasliwal, Mansi M. Silverman, Jeffrey M. Filippenko, Alexei V. Gal-Yam, Avishay Clubb, Kelsey I. Graham, Melissa L. Leonard, Douglas C. Horst, J. Chuck Williams, G. Grant Andrews, Jennifer E. Kulkarni, Shrinivas R. Nugent, Peter Sullivan, Mark Maguire, Kate Xu, Dong Ben-Ami, Sagi TI PTF11iqb: cool supergiant mass-loss that bridges the gap between Type IIn and normal supernovae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE circumstellar matter; stars: evolution; supernovae: general; supernovae: individual: PTF11iqb; stars: winds, outflows ID SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; SN 2009IP CONSTRAINTS; DIGITAL SKY SURVEY; CIRCUMSTELLAR INTERACTION; DUST FORMATION; IA SUPERNOVAE; LIGHT CURVES; PHOTOMETRIC CALIBRATION; LUMINOUS SUPERNOVAE; STANDARD STARS AB The supernova (SN) PTF11iqb was initially classified as a Type IIn event caught very early after explosion. It showed narrowWolf-Rayet (WR) spectral features on day 2 (as in SN 1998S and SN 2013cu), but the narrow emission weakened quickly and the spectrum morphed to resemble Types II-L and II-P. At late times, H alpha exhibited a complex, multipeaked profile reminiscent of SN 1998S. In terms of spectroscopic evolution, we find that PTF11iqb was a near twin of SN 1998S, although with somewhat weaker interaction with circumstellar material (CSM) at early times, and stronger interaction at late times. We interpret the spectral changes as caused by early interaction with asymmetric CSM that is quickly (by day 20) enveloped by the expanding SN ejecta photosphere, but then revealed again after the end of the plateau when the photosphere recedes. The light curve can be matched with a simple model for CSM interaction (with a mass-loss rate of roughly 10(-4) M-circle dot yr(-1)) added to the light curve of a normal SN II-P. The underlying plateau requires a progenitor with an extended hydrogen envelope like a red supergiant at the moment of explosion, consistent with the slow wind speed (<80 km s(-1)) inferred from narrow H alpha emission. The cool supergiant progenitor is significant because PTF11iqb showed WR features in its early spectrum - meaning that the presence of such WR features does not necessarily indicate a WR-like progenitor. Overall, PTF11iqb bridges SNe IIn with weaker pre-SN mass-loss seen in SNe II-L and II-P, implying a continuum between these types. C1 [Smith, Nathan; Mauerhan, Jon C.; Williams, G. Grant; Andrews, Jennifer E.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Mauerhan, Jon C.; Filippenko, Alexei V.; Clubb, Kelsey I.; Graham, Melissa L.; Nugent, Peter] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Cenko, S. Bradley] NASA Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Kasliwal, Mansi M.; Kulkarni, Shrinivas R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Silverman, Jeffrey M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Gal-Yam, Avishay; Xu, Dong; Ben-Ami, Sagi] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Leonard, Douglas C.; Horst, J. Chuck] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Williams, G. Grant] Univ Arizona, Multiple Mirror Telescope Observ, Tucson, AZ 85721 USA. [Nugent, Peter] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Res Div, Berkeley, CA 94720 USA. [Sullivan, Mark] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Maguire, Kate] European Southern Observ Astron Res Southern Hemi, D-85748 Garching, Germany. RP Smith, N (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM nathans@as.arizona.edu OI Sullivan, Mark/0000-0001-9053-4820 FU W.M. Keck Foundation; NSF [AST-1210599, AST-1312221, AST-1211916, AST-1009571, AST-1210311]; Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ); Israeli Ministry of Science; Israel Science Foundation; Minerva; I-CORE Program of the Planning and Budgeting Committee; EU/FP7 via ERC [307260]; Quantum Universe I-Core program by the Israeli Committee; ISF; WIS-UK 'making connections'; Kimmel and ARCHES awards; Gary & Cynthia Bengier; Richard & Rhoda Goldman Fund; Christopher R. Redlich Fund; TABASGO Foundation; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302771]; Marie Curie Intra-European Fellowship, within the 7th European Community Framework Programme (FP7); Royal Society FX We thank Iair Arcavi, Peter Blanchard, Yi Cao, Ori Fox, Paul Groot, Asaf Horesh, Michael Kandrashoff, Pat Kelly, Nick Konidaris, Rubina Kotak, David Levitan, Adam Miller, Yen-Chen Pan, Jarod Parrent, Paul Smith, and WeiKang Zheng for assistance with some of the observations and data reduction. We thank Eran Ofek for helpful discussions and assistance with the PTF photometric data. We thank the referee, Max Stritzinger, for a careful reading of the manuscript and helpful comments. We thank the staffs at Lick, MMT, LBT, Keck, Palomar, and WHT for their assistance with the observations. Observations using Steward Observatory facilities were obtained as part of the observing program AZTEC: Arizona Transient Exploration and Characterization. Some observations reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution. This research was based in part on observations made with the LBT. The LBT is an international collaboration among institutions in the United States, Italy and Germany. The LBT Corporation partners are: the University of Arizona on behalf of the Arizona university system; the Istituto Nazionale di Astrofisica, Italy; the LBT Beteiligungsgesellschaft, Germany, representing the Max-Planck Society, the Astrophysical Institute Potsdam and Heidelberg University; the Ohio State University and the Research Corporation, on behalf of the University of Notre Dame, University of Minnesota and University of Virginia. The WHT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de AstrofAsica de Canarias. 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 NASA; 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.; NS received partial support from NSF grants AST-1210599 and AST-1312221. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful to support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), Israeli Ministry of Science, Israel Science Foundation, Minerva and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation. AGY is supported by the EU/FP7 via ERC grant no. 307260, the Quantum Universe I-Core program by the Israeli Committee for planning and funding, and the ISF, Minerva and ISF grants, WIS-UK 'making connections,' and Kimmel and ARCHES awards. The supernova research of AVF's group at U.C. Berkeley is supported by Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. JMS is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. KM is supported by a Marie Curie Intra-European Fellowship, within the 7th European Community Framework Programme (FP7). MS acknowledges support from the Royal Society. DCL and JCH are grateful for support from NSF grants AST-1009571 and AST-1210311, under which part of this research (photometry collected at MLO) was carried out. NR 120 TC 25 Z9 25 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 11 PY 2015 VL 449 IS 2 BP 1876 EP 1896 DI 10.1093/mnras/stv354 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2TN UT WOS:000355337500060 ER PT J AU Kobayashi, MIN Leauthaud, A More, S Okabe, N Laigle, C Rhodes, J Takeuchi, TT AF Kobayashi, Masato I. N. Leauthaud, Alexie More, Surhud Okabe, Nobuhiro Laigle, Clotilde Rhodes, Jason Takeuchi, Tsutomu T. TI Can we use weak lensing to measure total mass profiles of galaxies on 20 kpc scales? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: weak; galaxies: haloes; galaxies: stellar content; galaxies: structure; cosmology: observations; large-scale structure of Universe ID DARK-MATTER HALOS; HUBBLE-SPACE-TELESCOPE; STELLAR POPULATION SYNTHESIS; DENSITY PROFILES; COSMIC EVOLUTION; COSMOLOGICAL SIMULATIONS; SHAPE MEASUREMENT; BARYONIC INFALL; ADVANCED CAMERA; ACS SURVEY AB Current constraints on dark matter density profiles from weak lensing are typically limited to radial scales greater than 50-100 kpc. In this paper, we explore the possibility of probing the very inner regions of galaxy/halo density profiles by measuring stacked weak lensing on scales of only a few tens of kpc. Our forecasts focus on scales smaller than the 'equality radius' (R-eq), where the stellar component and the dark matter component contribute equally to the lensing signal. We compute the evolution of R-eq as a function of lens stellar mass and redshift and show that R-eq = 7-34 kpc for galaxies with M-* = 10(9.5)-10(11.5) M-circle dot. Unbiased shear measurements will be challenging on these scales. We introduce a simple metric to quantify how many source galaxies overlap with their neighbours and for which shear measurements will be challenging. Rejecting source galaxies with close-by companions results in an similar to 20 per cent decrease in the overall source density. Despite this decrease, we show that Euclid and Wide Field Infrared Survey Telescope will be able to constrain galaxy/halo density profiles at R-eq with S/N > 20 for M-* > 10(10) M-circle dot. Weak lensing measurements at R-eq, in combination with stellar kinematics on smaller scales, will be a powerful means by which to constrain both the inner slope of the dark matter density profile as well as the mass and redshift dependence of the stellar initial mass function. C1 [Kobayashi, Masato I. N.; Takeuchi, Tsutomu T.] Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Nagoya, Aichi 4648602, Japan. [Leauthaud, Alexie; More, Surhud; Okabe, Nobuhiro] Univ Tokyo, WPI, Kavli IPMU, Chiba 2778582, Japan. [Laigle, Clotilde] Inst Astrophys Paris, UMR 7095, CNRS, F-75014 Paris, France. [Laigle, Clotilde] Univ Paris 06, Sorbonne Univ, UMR 7095, Inst Astrophys Paris, F-75005 Paris, France. [Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rhodes, Jason] CALTECH, Pasadena, CA 91125 USA. RP Kobayashi, MIN (reprint author), Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Nagoya, Aichi 4648602, Japan. EM masato.kobayashi@nagoya-u.jp OI Kobayashi, Masato/0000-0003-3990-1204 FU World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan; Ministry of Education, Culture, Sports, Science, and Technology of Japan [25287057, 26800097]; ILP LABEX [ANR-10-LABX-63, ANR-11-IDEX-0004-02]; JPL, under a contract for NASA by Caltech; [23340046] FX We are grateful to the referee for a careful reading of the manuscript and for providing thoughtful comments. We thank Robert Lupton for useful discussions during the preparation of this paper and Naoshi Sugiyama for practical advice during the data analysis. This work, AL, and SM are supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. MINK acknowledges the financial support from N. Sugiyama (25287057) by Grants-in-Aid from the Ministry of Education, Culture, Sports, Science, and Technology of Japan. NO (26800097) is supported by Grants-in-Aid from the Ministry of Education, Culture, Sports, Science, and Technology of Japan. CL is supported by the ILP LABEX (under reference ANR-10-LABX-63 and ANR-11-IDEX-0004-02). JR was supported by JPL, run under a contract for NASA by Caltech. TTT has been supported by the Grant-in-Aid for the Scientific Research Fund (23340046), for the Global COE Program Request for Fundamental Principles in the Universe: from Particles to the Solar system and the Cosmos, and for the JSPS Strategic Young Researcher Overseas Visits Program for Accelerating Brain Circulation, commissioned by the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan. NR 85 TC 3 Z9 3 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 11 PY 2015 VL 449 IS 2 BP 2128 EP 2143 DI 10.1093/mnras/stv424 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2TN UT WOS:000355337500078 ER PT J AU Allman, MS Verma, VB Stevens, M Gerrits, T Horansky, RD Lita, AE Marsili, F Beyer, A Shaw, MD Kumor, D Mirin, R Nam, SW AF Allman, M. S. Verma, V. B. Stevens, M. Gerrits, T. Horansky, R. D. Lita, A. E. Marsili, F. Beyer, A. Shaw, M. D. Kumor, D. Mirin, R. Nam, S. W. TI A near-infrared 64-pixel superconducting nanowire single photon detector array with integrated multiplexed readout SO APPLIED PHYSICS LETTERS LA English DT Article ID CIRCUIT; SPECTROPHOTOMETER; EFFICIENCY AB We demonstrate a 64-pixel free-space-coupled array of superconducting nanowire single photon detectors optimized for high detection efficiency in the near-infrared range. An integrated, readily scalable, multiplexed readout scheme is employed to reduce the number of readout lines to 16. The cryogenic, optical, and electronic packaging to read out the array as well as characterization measurements are discussed. (C) 2015 AIP Publishing LLC. C1 [Allman, M. S.; Verma, V. B.; Stevens, M.; Gerrits, T.; Horansky, R. D.; Lita, A. E.; Mirin, R.; Nam, S. W.] NIST, Boulder, CO 80305 USA. [Marsili, F.; Beyer, A.; Shaw, M. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kumor, D.] Purdue Univ, W Lafayette, IN 47907 USA. RP Allman, MS (reprint author), NIST, 325 Broadway, Boulder, CO 80305 USA. EM shane.allman@boulder.nist.gov OI Mirin, Richard/0000-0002-4472-4655 FU NIST; DARPA INPHO program FX This work was supported by NIST and the DARPA INPHO program. NR 27 TC 16 Z9 16 U1 6 U2 24 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD MAY 11 PY 2015 VL 106 IS 19 AR 192601 DI 10.1063/1.4921318 PG 4 WC Physics, Applied SC Physics GA CI8GI UT WOS:000355008100024 ER PT J AU Stoffle, N Pinsky, L Kroupa, M Hoang, S Idarraga, J Amberboy, C Rios, R Hauss, J Keller, J Bahadori, A Semones, E Turecek, D Jakubek, J Vykydal, Z Pospisil, S AF Stoffle, Nicholas Pinsky, Lawrence Kroupa, Martin Hoang, Son Idarraga, John Amberboy, Clif Rios, Ryan Hauss, Jessica Keller, John Bahadori, Amir Semones, Edward Turecek, Daniel Jakubek, Jan Vykydal, Zdenek Pospisil, Stanislav TI Timepix-based radiation environment monitor measurements aboard the International Space Station SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article DE Timepix; Medipix; International Space Station; Ionizing radiation; Pixel detector; Active dosimeter ID DETECTOR AB A number of small, single element radiation detectors, employing the CERN-based Medipix2 Collaboration's Timepix Application Specific Integrated Circuit (ASIC) coupled to a specially modified version of the USB-Lite interface for that ASIC providecl by the Institute for Experimental and Applied Physics (LEAP) at the Czech Technical University in Prague, have been developed at the University of Houston and NASA Johnson Space Center. These detectors, officially designated by NASA as Radiation Environment Monitors (REMs), were deployed aboard the International Space Station in late 2012. Six REM units are currently operating on Station Support Computers (SSCs) and returning data on a daily basis. The associated data acquisition software on the SSCs provides both automated data collection and transfer, as well as algorithms to handle adjustment of acquisition rates and recovery and restart of the acquisition software. A suite of ground software analysis tools has been developed to allow rapid analysis of the data and provides a ROOT-based framework for extending data analysis capabilities. (C) 2015 Elsevier B.V. All rights reserved, C1 [Stoffle, Nicholas; Pinsky, Lawrence; Kroupa, Martin; Hoang, Son; Idarraga, John] Univ Houston, Houston, TX 77251 USA. [Stoffle, Nicholas; Amberboy, Clif; Rios, Ryan; Hauss, Jessica] Lockheed Martin, Houston, TX USA. [Keller, John] Wyle Labs, Houston, TX USA. [Bahadori, Amir; Semones, Edward] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Turecek, Daniel; Jakubek, Jan; Vykydal, Zdenek; Pospisil, Stanislav] Czech Tech Univ, Inst Expt & Appl Phys, CR-16635 Prague, Czech Republic. RP Stoffle, N (reprint author), Univ Houston, 3700 Calhoun, Houston, TX 77251 USA. RI Vykydal, Zdenek/H-6426-2016 OI Vykydal, Zdenek/0000-0003-2329-0672 NR 17 TC 6 Z9 6 U1 3 U2 21 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 MAY 11 PY 2015 VL 782 BP 143 EP 148 DI 10.1016/j.nima.2015.02.016 PG 6 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA CD4PL UT WOS:000351065600020 ER PT J AU Badnell, NR Ferland, GJ Gorczyca, TW Nikolic, D Wagle, GA AF Badnell, N. R. Ferland, G. J. Gorczyca, T. W. Nikolic, D. Wagle, G. A. TI BOOTSTRAPPING DIELECTRONIC RECOMBINATION FROM SECOND-ROW ELEMENTS AND THE ORION NEBULA SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; atomic processes; galaxies: abundances; ISM: abundances ID FINITE-DENSITY PLASMAS; MODEL ATMOSPHERES; RATE COEFFICIENTS; CHARGE-TRANSFER; STARS; IONS; ABUNDANCES; RADIATION; REGIONS; CLOUDY AB Dielectronic recombination (DR) is the dominant recombination process for most heavy elements in photoionized clouds. Accurate DR rates for a species can be predicted when the positions of autoionizing states are known. Unfortunately such data are not available for most third-and higher-row elements. This introduces an uncertainty that is especially acute for photoionized clouds, where the low temperatures mean that DR occurs energetically through very low-lying autoionizing states. This paper discusses S2+ -> S+ DR, the process that is largely responsible for establishing the [S III]/[S II] ratio in nebulae. We derive an empirical rate coefficient using a novel method for second-row ions, which do have accurate data. Photoionization models are used to reproduce the [O III]/ [O II]/[O I]/[Ne III] intensity ratios in central regions of the Orion Nebula. O and Ne have accurate atomic data and can be used to derive an empirical S2+ -> S+ DR rate coefficient at similar to 10(4) K. We present new calculations of the DR rate coefficient for S2+ -> S+ and quantify how uncertainties in the autoionizing level positions affect it. The empirical and theoretical results are combined and we derive a simple fit to the resulting rate coefficient at all temperatures for incorporation into spectral synthesis codes. This method can be used to derive empirical DR rates for other ions, provided that good observations of several stages of ionization of O and Ne are available. C1 [Badnell, N. R.] Univ Strathclyde, Glasgow G4 0NG, Lanark, Scotland. [Ferland, G. J.; Wagle, G. A.] Univ Kentucky, Lexington, KY 40506 USA. [Ferland, G. J.] Queens Univ Belfast, Belfast BT7 1NN, Antrim, North Ireland. [Gorczyca, T. W.] Western Michigan Univ, Kalamazoo, MI 49008 USA. [Nikolic, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Badnell, NR (reprint author), Univ Strathclyde, Glasgow G4 0NG, Lanark, Scotland. RI Nikolic, Dragan/N-8346-2015; OI Nikolic, Dragan/0000-0002-3810-7984; Ferland, Gary/0000-0003-4503-6333 FU NSF [1108928, 1109061, 1412155]; NASA [10-ATP10-0053, 10-ADAP10-0073, NNX12AH73G, ATP13-0153]; STScI [HST-AR- 13245, GO-12560, HST-GO-12309, GO-13310.002 A, HST-AR- 13914]; Leverhulme Trust via the award of a Visiting Professorship at The Queen's University of Belfast [VP1-2012-025]; NASA APRA grant [NNX11AF32G]; STFC UK APAP Network grant [ST/J000892/1] FX G.J.F. acknowledges support by NSF (1108928, 1109061, and 1412155), NASA (10-ATP10-0053, 10-ADAP10-0073, NNX12AH73G, and ATP13-0153), STScI (HST-AR- 13245, GO-12560, HST-GO-12309, GO-13310.002 A, and HST-AR- 13914) and is grateful to the Leverhulme Trust for support via the award of a Visiting Professorship at The Queen's University of Belfast (VP1-2012-025). T.W.G. was supported in part by the NASA APRA grant NNX11AF32G. N.R.B. was supported in part the STFC UK APAP Network grant ST/J000892/1. NR 33 TC 1 Z9 1 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2015 VL 804 IS 2 AR 100 DI 10.1088/0004-637X/804/2/100 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6WR UT WOS:000354905000022 ER PT J AU Banados, E Venemans, BP Morganson, E Hodge, J Decarli, R Walter, F Stern, D Schlafly, E Farina, EP Greiner, J Chambers, KC Fan, X Rix, HW Burgett, WS Draper, PW Flewelling, J Kaiser, N Metcalfe, N Morgan, JS Tonry, JL Wainscoat, RJ AF Banados, E. Venemans, B. P. Morganson, E. Hodge, J. Decarli, R. Walter, F. Stern, D. Schlafly, E. Farina, E. P. Greiner, J. Chambers, K. C. Fan, X. Rix, H-W Burgett, W. S. Draper, P. W. Flewelling, J. Kaiser, N. Metcalfe, N. Morgan, J. S. Tonry, J. L. Wainscoat, R. J. TI CONSTRAINING THE RADIO-LOUD FRACTION OF QUASARS AT z > 5.5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; quasars: general ID DIGITAL SKY SURVEY; SIMILAR-TO 6; SOUTHERN SPECTROPHOTOMETRIC STANDARDS; OPTICALLY SELECTED QUASARS; ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASSES; LUMINOSITY FUNCTION; HIGH-REDSHIFT; Z-SIMILAR-TO-6 QUASARS; HIGH-RESOLUTION AB Radio-loud active galactic nuclei at z similar to 2-4 are typically located in dense environments and their host galaxies are among the most massive systems at those redshifts, providing key insights for galaxy evolution. Finding radio-loud quasars at the highest accessible redshifts (z similar to 6) is important to the study of their properties and environments at even earlier cosmic time. They could also serve as background sources for radio surveys intended to study the intergalactic medium beyond the epoch of reionization in HI 21 cm absorption. Currently, only five radio-loud (R= f(v,5) (GHz)/f(v,4400) (angstrom) > 10) quasars are known at z similar to 6. In this paper we search for 5.5 less than or similar to z less than or similar to 7.2 quasars by cross-matching the optical Panoramic Survey Telescope & Rapid Response System 1 and radio Faint Images of the Radio Sky at Twenty cm surveys. The radio information allows identification of quasars missed by typical color-based selections. While we find no good 6.4 less than or similar to z less than or similar to 7.2 quasar candidates at the sensitivities of these surveys, we discover two new radio-loud quasars at z similar to 6. Furthermore, we identify two additional z similar to 6 radio-loud quasars that were not previously known to be radio-loud, nearly doubling the current z similar to 6 sample. We show the importance of having infrared photometry for z > 5.5 quasars to robustly classify them as radio-quiet or radioloud. Based on this, we reclassify the quasar J0203+0012 (z = 5.72), previously considered radio-loud, to be radio-quiet. Using the available data in the literature, we constrain the radio-loud fraction of quasars at z similar to 6, using the Kaplan-Meier estimator, to be 8.1(-3.2)(+5.0)%. This result is consistent with there being no evolution of the radio-loud fraction with redshift, in contrast to what has been suggested by some studies at lower redshifts. C1 [Banados, E.; Venemans, B. P.; Decarli, R.; Walter, F.; Schlafly, E.; Farina, E. P.; Rix, H-W] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Morganson, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hodge, J.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Greiner, J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Chambers, K. C.; Burgett, W. S.; Flewelling, J.; Kaiser, N.; Morgan, J. S.; Tonry, J. L.; Wainscoat, R. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Fan, X.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Draper, P. W.; Metcalfe, N.] Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Banados, E (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM banados@mpia.de OI Farina, Emanuele Paolo/0000-0002-6822-2254; Banados, Eduardo/0000-0002-2931-7824; Chambers, Kenneth /0000-0001-6965-7789; Schlafly, Edward Ford/0000-0002-3569-7421 FU ERC grant "Cosmic Dawn"; National Aeronautics and Space Administration through Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; National Science Foundation [AST-1238877]; NSF [AST-9987045]; NSF Telescope System Instrumentation Program (TSIP); Ohio Board of Regents; Ohio State University Office of Research; DFG [HA 1850/28-1]; National Aeronautics and Space Administration FX We thank the anonymous referee for providing excellent suggestions and comments that improved the manuscript. E. B. thanks the IMPRS for Astronomy & Cosmic Physics at the University of Heidelberg. E. P. F. and B. P. V. acknowledge funding through the ERC grant "Cosmic Dawn." We thank F. Ardila, M. Balokovic J. Larson, E. Manjavacas, M. Maseda, T. Minear, A. Place, S. Schmidl, and C. Steinhardt for their important participation in some of our follow-up observations. 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 No. NNX08AR22G 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, Eotvos Lorand University (ELTE), and the Los Alamos National Laboratory. This work is based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programs ID 092.A-0150, 093.A-0863, and 093.A-0574. The LBT is an international collaboration among institutions in the United States, Italy and Germany. The LBT Corporation partners are: The University of Arizona on behalf of the Arizona university system; Istituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany, representing the Max Planck Society, the Astrophysical Institute Potsdam, and Heidelberg University; The Ohio State University; The Research Corporation, on behalf of The University of Notre Dame, University of Minnesota and University of Virginia. This paper used data obtained with the MODS spectrographs built with funding from NSF grant AST-9987045 and the NSF Telescope System Instrumentation Program (TSIP), with additional funds from the Ohio Board of Regents and the Ohio State University Office of Research. Part of the funding for GROND (both hardware as well as personnel) was generously granted from the Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. We used the Milliquas Quasar Catalog to cross match our candidates with known quasars (http://quasars.org/milliquas.htm; Flesch 2015) This research made use of Astropy, a community-developed core Python package for Astronomy (Robitaille & Tollerud 2013; http://www.astropy.org). We used the python package Lifelines (Davidson-Pilon 2015) https://github.com/camdavidsonpilon/lifelines) to perform the Kaplan-Meier estimates. This publication made use of TOPCAT (Taylor et al. 2005, http://www.starlink.ac.uk/topcat). The plots in this publication were produced using Matplotlib (Hunter 2007, http://www.matplotlib.org). NR 101 TC 9 Z9 9 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2015 VL 804 IS 2 AR 118 DI 10.1088/0004-637X/804/2/118 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6WR UT WOS:000354905000040 ER PT J AU Berry, CPL Mandel, I Middleton, H Singer, LP Urban, AL Vecchio, A Vitale, S Cannon, K Farr, B Farr, WM Graff, PB Hanna, C Haster, CJ Mohapatra, S Pankow, C Price, LR Sidery, T Veitch, J AF Berry, Christopher P. L. Mandel, Ilya Middleton, Hannah Singer, Leo P. Urban, Alex L. Vecchio, Alberto Vitale, Salvatore Cannon, Kipp Farr, Ben Farr, Will M. Graff, Philip B. Hanna, Chad Haster, Carl-Johan Mohapatra, Satya Pankow, Chris Price, Larry R. Sidery, Trevor Veitch, John TI PARAMETER ESTIMATION FOR BINARY NEUTRON-STAR COALESCENCES WITH REALISTIC NOISE DURING THE ADVANCED LIGO ERA SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational waves; methods: data analysis; stars: neutron; surveys ID GRAVITATIONAL-WAVE OBSERVATIONS; ELECTROMAGNETIC FOLLOW-UP; MASS-DISTRIBUTION; BLACK-HOLES; BAYESIAN-INFERENCE; COMPACT BINARIES; ASTRONOMY; MERGERS; GALAXY; TRANSIENTS AB Advanced ground-based gravitational-wave (GW) detectors begin operation imminently. Their intended goal is not only to make the first direct detection of GWs, but also to make inferences about the source systems. Binary neutron-star mergers are among the most promising sources. We investigate the performance of the parameter-estimation (PE) pipeline that will be used during the first observing run of the Advanced Laser Interferometer Gravitational-wave Observatory (aLIGO) in 2015: we concentrate on the ability to reconstruct the source location on the sky, but also consider the ability to measure masses and the distance. Accurate, rapid sky localization is necessary to alert electromagnetic (EM) observatories so that they can perform follow-up searches for counterpart transient events. We consider PE accuracy in the presence of non-stationary, non-Gaussian noise. We find that the character of the noise makes negligible difference to the PE performance at a given signal-to-noise ratio. The source luminosity distance can only be poorly constrained, since the median 90% (50%) credible interval scaled with respect to the true distance is 0.85 (0.38). However, the chirp mass is well measured. Our chirp-mass estimates are subject to systematic error because we used gravitational-waveform templates without component spin to carry out inference on signals with moderate spins, but the total error is typically less than 10(-3) M-circle dot. The median 90% (50%) credible region for sky localization is similar to 600 deg(2) (similar to 150 deg(2)), with 3% (30%) of detected events localized within 100 deg(2). Early aLIGO, with only two detectors, will have a sky-localization accuracy for binary neutron stars of hundreds of square degrees; this makes EM follow-up challenging, but not impossible. C1 [Berry, Christopher P. L.; Mandel, Ilya; Middleton, Hannah; Vecchio, Alberto; Farr, Ben; Farr, Will M.; Haster, Carl-Johan; Sidery, Trevor; Veitch, John] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Singer, Leo P.; Price, Larry R.] CALTECH, LIGO Lab, Pasadena, CA 91125 USA. [Singer, Leo P.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Urban, Alex L.; Pankow, Chris] Univ Wisconsin, Leonard E Parker Ctr Gravitat Cosmol & Astrophys, Milwaukee, WI 53201 USA. [Vitale, Salvatore; Mohapatra, Satya] MIT, Cambridge, MA 02139 USA. [Cannon, Kipp] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Farr, Ben] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Farr, Ben] Northwestern Univ, Ctr Interdisciplinary Explorat & Res Astrophys CI, Evanston, IL 60208 USA. [Farr, Ben] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Graff, Philip B.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Graff, Philip B.] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA. [Hanna, Chad] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [Hanna, Chad] Penn State Univ, University Pk, PA 16802 USA. [Mohapatra, Satya] Syracuse Univ, Syracuse, NY 13244 USA. RP Berry, CPL (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. EM cplb@star.sr.bham.ac.uk RI Vecchio, Alberto/F-8310-2015; OI Vecchio, Alberto/0000-0002-6254-1617; Farr, Ben/0000-0002-2916-9200; Berry, Christopher/0000-0003-3870-7215; Mandel, Ilya/0000-0002-6134-8946; Veitch, John/0000-0002-6508-0713 FU Science and Technology Facilities Council; NASA grant [NNX12AN10G]; National Science Foundation; LIGO Laboratory; STFC grant [ST/K005014/1]; National Science Foundation [PHY-0757058]; NSF [PHY-0923409, PHY-0600953] FX This work was supported by the Science and Technology Facilities Council. P.B.G. acknowledges NASA grant NNX12AN10G. S.V. acknowledges the support of the National Science Foundation and the LIGO Laboratory. J.V. was supported by STFC grant ST/K005014/1. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation and operates under cooperative agreement PHY-0757058.; Results were produced using the computing facilities of the LIGO DataGrid including: the Nemo computing cluster at the Center for Gravitation and Cosmology at the University of Wisconsin-Milwauke under NSF Grants PHY-0923409 and PHY-0600953; the Atlas computing cluster at the Albert Einstein Institute, Hannover; the LIGO computing clusters at Caltech, and the facilities of the Advanced Research Computing @ Cardiff (ARCCA) Cluster at Cardiff University. We are especially grateful to Paul Hopkins of ARCCA for assistance. NR 88 TC 39 Z9 39 U1 2 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2015 VL 804 IS 2 AR 114 DI 10.1088/0004-637X/804/2/114 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6WR UT WOS:000354905000036 ER PT J AU Brambilla, G Kalapotharakos, C Harding, AK Kazanas, D AF Brambilla, Gabriele Kalapotharakos, Constantinos Harding, Alice K. Kazanas, Demosthenes TI TESTING DISSIPATIVE MAGNETOSPHERE MODEL LIGHT CURVES AND SPECTRA WITH FERMI PULSARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; pulsars: general; radiation mechanisms: non-thermal ID LARGE-AREA TELESCOPE; GAMMA-RAY PULSARS; SLOT GAPS; PARTICLE-ACCELERATION; PAIR CREATION; STRIPED WIND; CRAB PULSAR; POLAR CAPS; EMISSION; SIMULATIONS AB We explore the emission properties of a dissipative pulsar magnetosphere model introduced by Kalapotharakos et al. comparing its high-energy light curves and spectra, due to curvature radiation, with data collected by the Fermi LAT. The magnetosphere structure is assumed to be near the force-free solution. The accelerating electric field, inside the light cylinder (LC), is assumed to be negligible, while outside the LC it rescales with a finite conductivity (sigma). In our approach we calculate the corresponding high-energy emission by integrating the trajectories of test particles that originate from the stellar surface, taking into account both the accelerating electric field components and the radiation reaction forces. First, we explore the parameter space assuming different value sets for the stellar magnetic field, stellar period, and conductivity. We show that the general properties of the model are in a good agreement with observed emission characteristics of young gamma-ray pulsars, including features of the phase-resolved spectra. Second, we find model parameters that fit each pulsar belonging to a group of eight bright pulsars that have a published phase-resolved spectrum. The sigma values that best describe each of the pulsars in this group show an increase with the spin-down rate (E) and a decrease with the pulsar age, expected if pair cascades are providing the magnetospheric conductivity. Finally, we explore the limits of our analysis and suggest future directions for improving such models. C1 [Brambilla, Gabriele] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy. [Brambilla, Gabriele; Kalapotharakos, Constantinos; Harding, Alice K.; Kazanas, Demosthenes] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kalapotharakos, Constantinos] Univ Maryland, Coll Pk UMDCP CRESST, College Pk, MD 20742 USA. RP Brambilla, G (reprint author), Univ Milan, Dipartimento Fis, Via Celoria 16, I-20133 Milan, Italy. EM gabriele.brambilla@nasa.gov OI BRAMBILLA, GABRIELE/0000-0002-3692-1974 NR 40 TC 9 Z9 9 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 MAY 10 PY 2015 VL 804 IS 2 AR 84 DI 10.1088/0004-637X/804/2/84 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6WR UT WOS:000354905000006 ER PT J AU Holman, GD Foord, A AF Holman, Gordon D. Foord, Adi TI DIRECT SPATIAL ASSOCIATION OF AN X-RAY FLARE WITH THE ERUPTION OF A SOLAR QUIESCENT FILAMENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: filaments, prominences; Sun: flares; Sun: magnetic fields; Sun: UV radiation; Sun: X-rays, gamma-rays ID CORONAL MASS EJECTIONS; MICROFLARES; EVENTS; RHESSI; FLUX AB Solar flares primarily occur in active regions. Hard X-ray flares have been found to occur only in active regions. They are often associated with the eruption of active region filaments and coronal mass ejections (CMEs). CMEs can also be associated with the eruption of quiescent filaments, not located in active regions. Here we report the first identification of a solar X-ray flare outside an active region observed by the Ramaty High Energy Solar Spectroscopic Imager (RHESSI). The X-ray emission was directly associated with the eruption of a long, quiescent filament and fast CME. Images from RHESSI show this flare emission to be located along a section of the western ribbon of the expanding, post-eruption arcade. EUV images from the Solar Dynamics Observatory Atmospheric Imaging Assembly show no connection between this location and nearby active regions. Therefore the flare emission is found not to be located in or associated with an active region. However, a nearby, small, magnetically strong dipolar region provides a likely explanation for the existence and location of the flare X-ray emission. This emerging dipolar region may have also triggered the filament eruption. C1 [Holman, Gordon D.; Foord, Adi] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Foord, Adi] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Holman, GD (reprint author), NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA. EM gordon.d.holman@nasa.gov FU NASA; RHESSI project FX We thank the referee and Karin Muglach for helpful comments that led to improvements in the paper, and Brian Dennis, Richard Schwartz, and Kim Tolbert for their continuing help and support with the RHESSI data analysis. G.H. was supported by NASA Heliophysics Guest Investigator and Living with a Star TR & T Grants and the RHESSI project. A.F. was supported by the RHESSI project. NR 16 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2015 VL 804 IS 2 AR 108 DI 10.1088/0004-637X/804/2/108 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6WR UT WOS:000354905000030 ER PT J AU Kashlinsky, A Mather, JC Helgason, K Arendt, RG Bromm, V Moseley, SH AF Kashlinsky, A. Mather, J. C. Helgason, K. Arendt, R. G. Bromm, V. Moseley, S. H. TI RECONSTRUCTING EMISSION FROM PRE-REIONIZATION SOURCES WITH COSMIC INFRARED BACKGROUND FLUCTUATION MEASUREMENTS BY THE JWST SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; early universe; infrared: diffuse background; large-scale structure of universe ID POPULATION-III STARS; COBE DIRBE MAPS; SPITZER-SPACE-TELESCOPE; ORIGINS DEEP SURVEY; GAMMA-RAY BURSTS; 1ST BLACK-HOLES; ALL-SKY SURVEY; PHOTOMETRIC CALIBRATION; EXPERIMENT SEARCH; INTERPLANETARY DUST AB We present new methodology to use cosmic infrared background (CIB) fluctuations to probe sources at 10 less than or similar to z less than or similar to 30 from a James Webb Space Telescope (JWST)/NIRCam configuration that will isolate known galaxies to 28 AB mag at 0.5-5 mu m. At present significant mutually consistent source-subtracted CIB fluctuations have been identified in the Spitzer and AKARI data at similar to 2-5 mu m, but we demonstrate internal inconsistencies at shorter wavelengths in the recent CIBER data. We evaluate CIB contributions from remaining galaxies and show that the bulk of the high-z sources will be in the confusion noise of the NIRCam beam, requiring CIB studies. The accurate measurement of the angular spectrum of the fluctuations and probing the dependence of its clustering component on the remaining shot noise power would discriminate between the various currently proposed models for their origin and probe the flux distribution of its sources. We show that the contribution to CIB fluctuations from remaining galaxies is large at visible wavelengths for the current instruments precluding probing the putative Lyman-break of the CIB fluctuations. We demonstrate that with the proposed JWST configuration such measurements will enable probing the Lyman-break. We develop a Lyman-break tomography method to use the NIRCam wavelength coverage to identify or constrain, via the adjacent two-band subtraction, the history of emissions over 10 less than or similar to z less than or similar to 30 as the universe comes out of the "Dark Ages." We apply the proposed tomography to the current Spitzer/IRAC measurements at 3.6 and 4.5 mu m, to find that it already leads to interestingly low upper limit on emissions at z greater than or similar to 30. C1 [Kashlinsky, A.; Mather, J. C.; Arendt, R. G.; Moseley, S. H.] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kashlinsky, A.] SSAI, Lanham, MD 20770 USA. [Mather, J. C.; Moseley, S. H.] NASA, Greenbelt, MD USA. [Helgason, K.] MPA, D-85748 Garching, Germany. [Arendt, R. G.] CRESST UMBC, Baltimore, MD USA. [Bromm, V.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Kashlinsky, A (reprint author), NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA. EM Alexander.Kashlinsky@nasa.gov OI Arendt, Richard/0000-0001-8403-8548 NR 103 TC 8 Z9 8 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2015 VL 804 IS 2 AR 99 DI 10.1088/0004-637X/804/2/99 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6WR UT WOS:000354905000021 ER PT J AU Mei, S Scarlata, C Pentericci, L Newman, JA Weiner, BJ Ashby, MLN Castellano, M Conselice, CJ Finkelstein, SL Galametz, A Grogin, NA Koekemoer, AM Huertas-Company, M Lani, C Lucas, RA Papovich, C Rafelski, M Teplitz, HI AF Mei, Simona Scarlata, Claudia Pentericci, Laura Newman, Jeffrey A. Weiner, Benjamin J. Ashby, Matthew L. N. Castellano, Marco Conselice, Chistopher J. Finkelstein, Steven L. Galametz, Audrey Grogin, Norman A. Koekemoer, Anton M. Huertas-Company, Marc Lani, Caterina Lucas, Ray A. Papovich, Casey Rafelski, Marc Teplitz, Harry I. TI STAR-FORMING BLUE ETGS IN TWO NEWLY DISCOVERED GALAXY OVERDENSITIES IN THE HUDF AT z=1.84 AND 1.9: UNVEILING THE PROGENITORS OF PASSIVE ETGS IN CLUSTER CORES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: evolution ID COLOR-MAGNITUDE RELATION; MASS-SIZE RELATION; ULTRA DEEP FIELD; HUBBLE-SPACE-TELESCOPE; SIMILAR-TO 1; EXTRAGALACTIC LEGACY SURVEY; FORMATION-DENSITY RELATION; LARGE-SCALE ENVIRONMENT; HIGH-REDSHIFT CLUSTERS; LYMAN-BREAK GALAXIES AB We present the discovery of two galaxy overdensities in the Hubble Space Telescope UDF: a proto-cluster, HUDFJ0332.4-2746.6 at z = 1.84 +/- 0.01, and a group, HUDFJ0332.5-2747.3 at z = 1.90 +/- 0.01. Assuming viralization, the velocity dispersion of HUDFJ0332.4-2746.6 implies a mass of M-200 = (2.2 +/- 1.8) x 10(14) M-circle dot, consistent with the lack of extended X-ray emission. Neither overdensity shows evidence of a red sequence. About 50% of their members show interactions and/or disturbed morphologies, which are signatures of merger remnants or disk instability. Most of their ETGs have blue colors and show recent star formation. These observations reveal for the first time large fractions of spectroscopically confirmed star-forming blue ETGs in proto-clusters at z approximate to 2. These star-forming ETGs are most likely among the progenitors of the quiescent population in clusters at more recent epochs. Their mass-size relation is consistent with that of passive ETGs in clusters at z similar to 0.7-1.5. If these galaxies are the progenitors of cluster ETGs at these lower redshifts, their size would evolve according to a similar mass-size relation. It is noteworthy that quiescent ETGs in clusters at z = 1.8-2 also do not show any significant size evolution over this redshift range, contrary to field ETGs. The ETG fraction is less than or similar to 50%, compared to the typical quiescent ETG fraction of approximate to 80% in cluster cores at z < 1. The fraction, masses, and colors of the newly discovered ETGs imply that other cluster ETGs will be formed/accreted at a later time. C1 [Mei, Simona; Huertas-Company, Marc] Univ Paris Diderot, GEPI, Observ Paris, CNRS,PSL, F-75014 Paris, France. [Mei, Simona; Huertas-Company, Marc] Univ Paris Sorbonne Cite PSC, Univ Paris Denis Diderot, F-75205 Paris 13, France. [Mei, Simona; Rafelski, Marc; Teplitz, Harry I.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Scarlata, Claudia] Univ Minnesota, Minnesota Inst Astrophys, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Pentericci, Laura; Castellano, Marco] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Newman, Jeffrey A.] Univ Pittsburgh, Pittsburgh, PA 15260 USA. [Weiner, Benjamin J.; Ashby, Matthew L. N.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Conselice, Chistopher J.; Lani, Caterina] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Grogin, Norman A.; Koekemoer, Anton M.; Lucas, Ray A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Finkelstein, Steven L.] Univ Texas Austin, Austin, TX 78712 USA. [Papovich, Casey] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 78743 USA. [Rafelski, Marc] NASA, Postdoctoral Program Fellow, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lani, Caterina] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Galametz, Audrey] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. RP Mei, S (reprint author), Univ Paris Diderot, GEPI, Observ Paris, CNRS,PSL, 61 Ave Observ, F-75014 Paris, France. OI Castellano, Marco/0000-0001-9875-8263; Weiner, Benjamin/0000-0001-6065-7483; Koekemoer, Anton/0000-0002-6610-2048 FU NASA [NAS526555]; Institut Universitaire de France (IUF) FX This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program and the 3D-HST Treasury Program (GO 12177 and 12328) with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS526555. 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. S.M. acknowledges financial support from the Institut Universitaire de France (IUF), of which she is a senior member. We thank the referee for very useful comments that improved the paper. NR 152 TC 17 Z9 17 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2015 VL 804 IS 2 AR 117 DI 10.1088/0004-637X/804/2/117 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6WR UT WOS:000354905000039 ER PT J AU Richert, AJW Lyra, W Boley, A Mac Low, MM Turner, N AF Richert, Alexander J. W. Lyra, Wladimir Boley, Aaron Mac Low, Mordecai-Mark Turner, Neal TI ON SHOCKS DRIVEN BY HIGH-MASS PLANETS IN RADIATIVELY INEFFICIENT DISKS. I. TWO-DIMENSIONAL GLOBAL DISK SIMULATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; planet-disk interactions; planets and satellites: formation; protoplanetary disks; shock waves; turbulence ID DIFFERENTIALLY ROTATING-DISKS; ROSSBY-WAVE INSTABILITY; BAROCLINIC VORTICITY PRODUCTION; PRIMORDIAL SOLAR NEBULA; PROTOPLANETARY DISKS; MAGNETOROTATIONAL TURBULENCE; TIDAL INTERACTION; ANGULAR-MOMENTUM; ACCRETION DISKS; MAGNETIZED ACCRETION AB Recent observations of gaps and non-axisymmetric features in the dust distributions of transition disks have been interpreted as evidence of embedded massive protoplanets. However, comparing the predictions of planet-disk interaction models to the observed features has shown far from perfect agreement. This may be due to the strong approximations used for the predictions. For example, spiral arm fitting typically uses results that are based on low-mass planets in an isothermal gas. In this work, we describe two-dimensional, global, hydrodynamical simulations of disks with embedded protoplanets, with and without the assumption of local isothermality, for a range of planet-to-star mass ratios 1-10 M-J for a 1 M-circle dot star. We use the PENCIL CODE in polar coordinates for our models. We find that the inner and outer spiral wakes of massive protoplanets (M greater than or similar to 5 M-J) produce significant shock heating that can trigger buoyant instabilities. These drive sustained turbulence throughout the disk when they occur. The strength of this effect depends strongly on the mass of the planet and the thermal relaxation timescale; for a 10 M-J planet embedded in a thin, purely adiabatic disk, the spirals, gaps, and vortices typically associated with planet-disk interactions are disrupted. We find that the effect is only weakly dependent on the initial radial temperature profile. The spirals that form in disks heated by the effects we have described may fit the spiral structures observed in transition disks better than the spirals predicted by linear isothermal theory. C1 [Richert, Alexander J. W.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Richert, Alexander J. W.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Richert, Alexander J. W.; Lyra, Wladimir; Turner, Neal] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Richert, Alexander J. W.; Lyra, Wladimir] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Boley, Aaron] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Mac Low, Mordecai-Mark] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. RP Richert, AJW (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM ajr327@psu.edu; wlyra@jpl.nasa.gov; acboley@phas.ubc.ca; mordecai@amnh.org; neal.j.turner@jpl.nasa.gov OI Richert, Alexander/0000-0002-9613-6863; Mac Low, Mordecai-Mark/0000-0003-0064-4060 FU NSF AAG grant [AST10-09802]; Center for Exoplanets and Habitable Worlds (PSU); National Aeronautics and Space Administration (NASA); Canada Research Chairs program; University of British Columbia; NASA OSS grant [NNX14AJ56G]; California Institute of Technology (Caltech) FX A. R. is funded by NSF AAG grant AST10-09802, and by the Center for Exoplanets and Habitable Worlds (PSU). W. L. is funded by the National Aeronautics and Space Administration (NASA) through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. A. B. is funded, in part, by the Canada Research Chairs program and The University of British Columbia. M.-M. M. L. is funded, in part, by NASA OSS grant NNX14AJ56G. This work was performed in part at the Jet Propulsion Laboratory, under contract with the California Institute of Technology (Caltech). The authors acknowledge discussions with Sijme-Jan Paardekooper, Axel Brandenburg, Dhrubaditya Mitra, Thayne Currie, and Wilhelm Kley. NR 71 TC 4 Z9 4 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2015 VL 804 IS 2 AR 95 DI 10.1088/0004-637X/804/2/95 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6WR UT WOS:000354905000017 ER PT J AU Rivers, E Risaliti, G Walton, DJ Harrison, F Arevalo, P Baur, FE Boggs, SE Brenneman, LW Brightman, M Christensen, FE Craig, WW Furst, F Hailey, CJ Hickox, RC Marinucci, A Reeves, J Stern, D Zhang, WW AF Rivers, E. Risaliti, G. Walton, D. J. Harrison, F. Arevalo, P. Baur, F. E. Boggs, S. E. Brenneman, L. W. Brightman, M. Christensen, F. E. Craig, W. W. Fuerst, F. Hailey, C. J. Hickox, R. C. Marinucci, A. Reeves, J. Stern, D. Zhang, W. W. TI THE MULTI-LAYER VARIABLE ABSORBERS IN NGC 1365 REVEALED BY XMM-NEWTON AND NuSTAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 1365); X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; SPECTRAL VARIABILITY; ACCRETION DISK; ABSORPTION; WIND; SUZAKU; AGN AB Between 2012 July and 2013 February, NuSTAR and XMM-Newton performed four long-look joint observations of the type 1.8 Seyfert, NGC 1365. We have analyzed the variable absorption seen in these observations in order to characterize the geometry of the absorbing material. Two of the observations caught NGC 1365 in an unusually low absorption state, revealing complexity in the multi-layer absorber that had previously been hidden. We find the need for three distinct zones of neutral absorption in addition to the two zones of ionized absorption and the Compton-thick torus previously seen in this source. The most prominent absorber is likely associated with broad-line region clouds with column densities of around similar to 10(23) cm(-2) and a highly clumpy nature as evidenced by an occultation event in 2013 February. We also find evidence of a patchy absorber with a variable column around similar to 10(22) cm(-2) and a line-of-sight covering fraction of 0.3-0.9, which responds directly to the intrinsic source flux, possibly due to a wind geometry. A full-covering, constant absorber with a low column density of similar to 1 x 10(22) cm(-2) is also present, though the location of this low density haze is unknown. C1 [Rivers, E.; Walton, D. J.; Harrison, F.; Brightman, M.; Fuerst, F.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Risaliti, G.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Risaliti, G.; Brenneman, L. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Walton, D. J.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile. [Baur, F. E.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 22, Chile. [Baur, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, DTU Space, Natl Space Inst, DK-2800 Lyngby, Denmark. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Marinucci, A.] Univ Rome Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Reeves, J.] Keele Univ, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Rivers, E (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Risaliti, Guido/0000-0002-3556-977X FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; NASA/GSFC; NASA/IPAC; NASA FX This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This work has also made use of HEASARC online services, supported by NASA/GSFC, and the NASA/IPAC Extragalactic Database, operated by JPL/California Institute of Technology under contract with NASA. This work also made use of data from the XMM-Newton observatory. NR 31 TC 5 Z9 5 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2015 VL 804 IS 2 AR 107 DI 10.1088/0004-637X/804/2/107 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6WR UT WOS:000354905000029 ER PT J AU Romani, RW Filippenko, AV Cenko, SB AF Romani, Roger W. Filippenko, Alexei V. Cenko, S. Bradley TI A SPECTROSCOPIC STUDY OF THE EXTREME BLACK WIDOW PSR J1311-3430 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: stars; pulsars: general ID MILLISECOND PULSARS; DISCOVERY; COMPANION; MODEL; STAR AB We report on a series of spectroscopic observations of PSR J1311-3430, an extreme black-widow gamma-ray pulsar with a helium-star companion. In a previous study we estimated the neutron star mass as M-NS = 2.68 +/- 0.14 M-circle dot (statistical error), based on limited spectroscopy and a basic (direct heating) light-curve model; however, much larger model-dependent systematics dominate the mass uncertainty. Our new spectroscopy reveals a range of complex source behavior. The variable He I companion wind emission lines can dominate broadband photometry, especially in red filters or near minimum brightness, and the wind flux should complete companion evaporation in a spin-down time. The heated companion face also undergoes dramatic flares, reaching similar to 40,000 K over similar to 20% of the star; this is likely powered by a magnetic field generated in the companion. The companion center-of-light radial velocity is now well measured with K-CoL = 615.4 +/- 5.1 km s(-1). We detect non-sinusoidal velocity components due to the heated face flux distribution. Using our spectra to excise flares and wind lines, we generate substantially improved light curves for companion continuum fitting. We show that the inferred inclination and neutron star mass, however, remain sensitive to the poorly constrained heating pattern. The neutron star's mass, M-NS, is likely less than the direct heating value and could range as low as 1.8 M-circle dot for extreme equatorial heating concentration. While we cannot yet pin down M-NS, our data imply that an intrabinary shock reprocesses the pulsar emission and heats the companion. Improved spectra and, especially, models that include such shock heating are needed for precise parameter measurement. C1 [Romani, Roger W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Cenko, S. Bradley] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. RP Romani, RW (reprint author), Stanford Univ, Dept Phys, Stanford, CA 94305 USA. EM rwr@astro.stanford.edu FU NASA [NNX11AO44G, NNX12A068G]; Richard and Rhoda Goldman Fund; Christopher R. Redlich Fund; TABASGO Foundation; NSF grant [AST-1211916]; W. M. Keck Foundation; Gary and Cynthia Bengier FX We thank Kelsey Clubb, Ori Fox, and Melissa Graham for assistance with some of the Keck observations, as well as German Gimeno for help with the Gemini campaign. We also thank the referee for many detailed comments. This work was partially supported by NASA grants NNX11AO44G and NNX12A068G. A.V.F. and S.B.C. were supported by Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. 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 NASA; the Observatory was made possible by the generous financial support of the W. M. Keck Foundation. NR 21 TC 6 Z9 6 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2015 VL 804 IS 2 AR 115 DI 10.1088/0004-637X/804/2/115 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6WR UT WOS:000354905000037 ER PT J AU Schneider, AC Cushing, MC Kirkpatrick, JD Gelino, CR Mace, GN Wright, EL Eisenhardt, PR Skrutskie, MF Griffith, RL Marsh, KA AF Schneider, Adam C. Cushing, Michael C. Kirkpatrick, J. Davy Gelino, Christopher R. Mace, Gregory N. Wright, Edward L. Eisenhardt, Peter R. Skrutskie, M. F. Griffith, Roger L. Marsh, Kenneth A. TI HUBBLE SPACE TELESCOPE SPECTROSCOPY OF BROWN DWARFS DISCOVERED WITH THE WIDE-FIELD INFRARED SURVEY EXPLORER SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: low-mass; brown dwarfs ID Y DWARFS; T-DWARFS; WATER CLOUDS; WISE; PHOTOMETRY; SPECTRA; MASS; ATMOSPHERES; TRANSITION; BINARIES AB We present a sample of brown dwarfs identified with the Wide-field Infrared Survey Explorer (WISE) for which we have obtained Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) near-infrared grism spectroscopy. The sample (22 in total) was observed with the G141 grism covering 1.10-1.70 mu m, while 15 were also observed with the G102 grism, which covers 0.90-1.10 mu m. The additional wavelength coverage provided by the G102 grism allows us to (1) search for spectroscopic features predicted to emerge at low effective temperatures (e.g., ammonia bands) and (2) construct a smooth spectral sequence across the T/Y boundary. We find no evidence of absorption due to ammonia in the G102 spectra. Six of these brown dwarfs are new discoveries, three of which are found to have spectral types of T8 or T9. The remaining three, WISE J082507.35+280548.5 (Y0.5), WISE J120604.38+840110.6 (Y0), and WISE J235402.77+024015.0 (Y1), are the 19th, 20th, and 21st spectroscopically confirmed Y dwarfs to date. We also present HST grism spectroscopy and reevaluate the spectral types of five brown dwarfs for which spectral types have been determined previously using other instruments. C1 [Schneider, Adam C.; Cushing, Michael C.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Kirkpatrick, J. Davy; Gelino, Christopher R.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Gelino, Christopher R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Mace, Gregory N.; Wright, Edward L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Mace, Gregory N.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Eisenhardt, Peter R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Skrutskie, M. F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Griffith, Roger L.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Marsh, Kenneth A.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. RP Schneider, AC (reprint author), Univ Toledo, Dept Phys & Astron, 2801 W Bancroft St, Toledo, OH 43606 USA. EM Adam.Schneider@Utoledo.edu FU National Aeronautics and Space Administration FX We wish to thank Caroline Morley and Didier Saumon for useful discussions regarding low-temperature models. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, and NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology. WISE and NEOWISE are funded by the National Aeronautics and Space Administration. This research has benefitted from the M, L, T, and Y dwarf compendium housed at dwarfarchives.org. This research has benefitted from the SpeX Prism Spectral Libraries, maintained by Adam Burgasser at http://pono.ucsd.edu/similar to adam/browndwarfs/spexprism. HST acknowledgement needed. We thank the STSCI help desk for useful discussions and resolution suggestions regarding WFC3 IR photometry. The authors wish to thank Caroline Morley for providing spectroscopic models via the webpage http://ucolick.org/similar to cmorley/cmorley/Models.html. NR 44 TC 7 Z9 7 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2015 VL 804 IS 2 AR 92 DI 10.1088/0004-637X/804/2/92 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6WR UT WOS:000354905000014 ER PT J AU Taquet, V Lopez-Sepulcre, A Ceccarelli, C Neri, R Kahane, C Charnley, SB AF Taquet, Vianney Lopez-Sepulcre, Ana Ceccarelli, Cecilia Neri, Roberto Kahane, Claudine Charnley, Steven B. TI CONSTRAINING THE ABUNDANCES OF COMPLEX ORGANICS IN THE INNER REGIONS OF SOLAR-TYPE PROTOSTARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: abundances; ISM: individual objects (NGC 1333-IRAS 2A, NGC 1333-IRAS 4A); ISM: molecules; stars: formation ID LOW-MASS PROTOSTARS; STAR-FORMING REGIONS; GRAIN-SURFACE-CHEMISTRY; EXTRAORDINARY SOURCES ANALYSIS; SUBMILLIMETER-WAVE SPECTRUM; INTERSTELLAR ICE ANALOGS; YOUNG STELLAR OBJECTS; MOLECULAR LINE SURVEY; HOT-CORE; IRAS 16293-2422 AB The high abundances of Complex Organic Molecules (COMs) with respect to methanol, the most abundant COM, detected toward low-mass protostars, tend to be underpredicted by astrochemical models. This discrepancy might come from the large beam of the single-dish telescopes, encompassing several components of the studied protostar, commonly used to detect COMs. To address this issue, we have carried out multi-line observations of methanol and several COMs toward the two low-mass protostars NGC 1333-IRAS 2A and -IRAS 4A with the Plateau de Bure interferometer at an angular resolution of 2 '', resulting in the first multi-line detection of the O-bearing species glycolaldehyde and ethanol and of the N-bearing species ethyl cyanide toward low-mass protostars other than IRAS 16293. The high number of detected transitions from COMs (more than 40 methanol transitions for instance) allowed us to accurately derive the source size of their emission and the COM column densities. The COM abundances with respect to methanol derived toward IRAS 2A and IRAS 4A are slightly, but not substantitally, lower than those derived from previous single-dish observations. The COM abundance ratios do not vary significantly with the protostellar luminosity, over five orders of magnitude, implying that low-mass hot corinos are quite chemically rich as high-mass hot cores. Astrochemical models still underpredict the abundances of key COMs, such as methyl formate or di-methyl ether, suggesting that our understanding of their formation remains incomplete. C1 [Taquet, Vianney; Charnley, Steven B.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. [Taquet, Vianney; Charnley, Steven B.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD USA. [Taquet, Vianney] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Lopez-Sepulcre, Ana; Ceccarelli, Cecilia; Kahane, Claudine] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. [Lopez-Sepulcre, Ana; Ceccarelli, Cecilia; Kahane, Claudine] CNRS, IPAG, F-38000 Grenoble, France. [Lopez-Sepulcre, Ana] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Neri, Roberto] Inst Radioastron Millimetr, Grenoble, France. RP Taquet, V (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Mailstop 691,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM taquet@strw.leidenuniv.nl FU NASA's Origins of Solar Systems and Exobiology Programs; NASA postdoctoral program; French space agency CNES FX The authors are grateful to the anonymous referee whose comments contributed to improving the quality of the present paper. This work was supported by NASA's Origins of Solar Systems and Exobiology Programs. V.T. acknowledges support from the NASA postdoctoral program. A.L.-S. and C.C. acknowledge financing from the French space agency CNES. NR 97 TC 15 Z9 15 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2015 VL 804 IS 2 AR 81 DI 10.1088/0004-637X/804/2/81 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6WR UT WOS:000354905000003 ER PT J AU Webber, MW Lewis, NK Marley, M Morley, C Fortney, JJ Cahoy, K AF Webber, Matthew W. Lewis, Nikole K. Marley, Mark Morley, Caroline Fortney, Jonathan J. Cahoy, Kerri TI EFFECT OF LONGITUDE-DEPENDENT CLOUD COVERAGE ON EXOPLANET VISIBLE WAVELENGTH REFLECTED-LIGHT PHASE CURVES SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; radiative transfer; stars: individual (Kepler-7); techniques: photometric ID EXTRASOLAR GIANT PLANETS; HUBBLE-SPACE-TELESCOPE; HD 189733B; HOT JUPITERS; TRANSMISSION SPECTRUM; DWARF ATMOSPHERES; THERMAL STRUCTURE; MEAN OPACITIES; ALBEDO; MODELS AB We use a planetary albedo model to investigate variations in visible wavelength phase curves of exoplanets. Thermal and cloud properties for these exoplanets are derived using one-dimensional radiative-convective and cloud simulations. The presence of clouds on these exoplanets significantly alters their planetary albedo spectra. We confirm that non-uniform cloud coverage on the dayside of tidally locked exoplanets will manifest as changes to the magnitude and shift of the phase curve. In this work, we first investigate a test case of our model using a Jupiter-like planet, at temperatures consistent to 2.0 AU insolation from a solar type star, to consider the effect of H2O clouds. We then extend our application of the model to the exoplanet Kepler-7b and consider the effect of varying cloud species, sedimentation efficiency, particle size, and cloud altitude. We show that, depending on the observational filter, the largest possible shift of the phase curve maximum will be similar to 2 degrees-10 degrees for a Jupiter-like planet, and up to similar to 30 degrees (similar to 0.08 in fractional orbital phase) for hot-Jupiter exoplanets at visible wavelengths as a function of dayside cloud distribution with a uniformly averaged thermal profile. The models presented in this work can be adapted for a variety of planetary cases at visible wavelengths to include variations in planet-star separation, gravity, metallicity, and source-observer geometry. Finally, we tailor our model for comparison with, and confirmation of, the recent optical phase-curve observations of Kepler-7b with the Kepler space telescope. The average planetary albedo can vary between 0.1 and 0.6 for the 1300 cloud scenarios that were compared to the observations. Many of these cases cannot produce a high enough albedo to match the observations. We observe that smaller particle size and increasing cloud altitude have a strong effect on increasing albedo. In particular, we show that a set of models where Kepler-7b has roughly half of its dayside covered in small-particle clouds high in the atmosphere, made of bright minerals like MgSiO3 and Mg2SiO4, provide the best fits to the observed offset and magnitude of the phase-curve, whereas Fe clouds are found to be too dark to fit the observations. C1 [Webber, Matthew W.; Lewis, Nikole K.; Cahoy, Kerri] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Lewis, Nikole K.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Marley, Mark] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Morley, Caroline; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Cahoy, Kerri] MIT, Dept Aeronaut & Astronaut, Cambridge, MA 02139 USA. RP Webber, MW (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. OI Marley, Mark/0000-0002-5251-2943 FU NASA; Jet Propulsion Laboratory (JPL) FX The authors thank Brice-Olivier Demory for his helpful discussion and for providing the Kepler-7b phase curve data. 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. NR 62 TC 9 Z9 9 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2015 VL 804 IS 2 AR 94 DI 10.1088/0004-637X/804/2/94 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6WR UT WOS:000354905000016 ER PT J AU Burlaga, LF Florinski, V Ness, NF AF Burlaga, L. F. Florinski, V. Ness, N. F. TI IN SITU OBSERVATIONS OF MAGNETIC TURBULENCE IN THE LOCAL INTERSTELLAR MEDIUM SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: magnetic fields ID GALACTIC COSMIC-RAYS; VOYAGER 1; ASTROPHYSICAL BODIES; FIELD; SCALE; GENERATION; SPECTRA; MODELS; GALAXY AB We present the first in situ observations of turbulence in the local interstellar magnetic field B, measured by Voyager 1 from 2013.36 to 2014.64. The fluctuations of the components of B, the rms of the fluctuations of the components of B, and magnitude of B have a Kolmogorov k(-5/3) spectrum in the range from 4 x 10(-6) to 3 x 10(-7) Hz. The turbulence is compressible; the variance is primarily along the average magnetic field. The turbulence is weak, the ratio of the turbulent fluctuations to the average field being 0.023. A small linear increase in the azimuthal angle lambda of B and a small linear decrease in the elevation angle delta were observed during the 468 day interval under consideration, which might be related to magnetic draping. C1 [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Florinski, V.] Univ Alabama, Dept Space Sci, Huntsville, AL 35899 USA. [Ness, N. F.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Code 673, Greenbelt, MD 20771 USA. EM lburlagahsp@verizon.net; vaf000@uah.edu; nfnudel@yahoo.com FU NASA [NNX12AC63G, NNG14PN24P, NNX10AE46, NNX12AH44G]; NSF [AGS-0955700]; NASA Marshall Space Flight Center [NNM11AA01A] FX We thank R. Jokipii for notes on the spectrum of the interstellar turbulence. T. McClanahan, S. Kramer, and D. Berdichevsky provided support in the processing of the data. N. F. Ness was supported by NASA grant NNX12AC63G to the Catholic University of America. L. F. Burlaga was supported by NASA Contract NNG14PN24P. V. Florinski was supported by NASA grants NNX10AE46 and NNX12AH44G, by NSF grant AGS-0955700, and a cooperative agreement with NASA Marshall Space Flight Center NNM11AA01A. NR 23 TC 15 Z9 15 U1 2 U2 8 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 MAY 10 PY 2015 VL 804 IS 2 AR L31 DI 10.1088/2041-8205/804/2/L31 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH8NN UT WOS:000354293200005 ER PT J AU Jennings, DE Achterberg, RK Cottini, V Anderson, CM Flasar, FM Nixon, CA Bjoraker, GL Kunde, VG Carlson, RC Guandique, E Kaelberer, MS Tingley, JS Albright, SA Segura, ME de Kok, R Coustenis, A Vinatier, S Bampasidis, G Teanby, NA Calcutt, S AF Jennings, Donald E. Achterberg, R. K. Cottini, V. Anderson, C. M. Flasar, F. M. Nixon, C. A. Bjoraker, G. L. Kunde, V. G. Carlson, R. C. Guandique, E. Kaelberer, M. S. Tingley, J. S. Albright, S. A. Segura, M. E. de Kok, R. Coustenis, A. Vinatier, S. Bampasidis, G. Teanby, N. A. Calcutt, S. TI EVOLUTION OF THE FAR-INFRARED CLOUD AT TITAN'S SOUTH POLE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE molecular processes; planets and satellites: atmospheres; planets and satellites: composition; planets and satellites: individual (Titan); radiation mechanisms: thermal ID CASSINI/CIRS OBSERVATIONS; STRATOSPHERIC AEROSOLS; TEMPORAL VARIATIONS; HCN POLYMER; ATMOSPHERE; SPECTRA; WINTER AB A condensate cloud on Titan identified by its 220 cm(-1) far-infrared signature continues to undergo seasonal changes at both the north and south poles. In the north, the cloud, which extends from 55 N to the pole, has been gradually decreasing in emission intensity since the beginning of the Cassini mission with a half-life of 3.8 years. The cloud in the south did not appear until 2012 but its intensity has increased rapidly, doubling every year. The shape of the cloud at the south pole is very different from that in the north. Mapping in 2013 December showed that the condensate emission was confined to a ring with a maximum at 80 S. The ring was centered 4 degrees from Titan's pole. The pattern of emission from stratospheric trace gases like nitriles and complex hydrocarbons (mapped in 2014 January) was also offset by 4 degrees, but had a central peak at the pole and a secondary maximum in a ring at about 70 S with a minimum at 80 S. The shape of the gas emission distribution can be explained by abundances that are high at the atmospheric pole and diminish toward the equator, combined with correspondingly increasing temperatures. We discuss possible causes for the condensate ring. The present rapid build up of the condensate cloud at the south pole is likely to transition to a gradual decline from 2015 to 2016. C1 [Jennings, Donald E.; Achterberg, R. K.; Cottini, V.; Anderson, C. M.; Flasar, F. M.; Nixon, C. A.; Bjoraker, G. L.; Kunde, V. G.; Carlson, R. C.; Guandique, E.; Kaelberer, M. S.; Tingley, J. S.; Albright, S. A.; Segura, M. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Achterberg, R. K.; Cottini, V.; Kunde, V. G.; Segura, M. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Carlson, R. C.] Catholic Univ Amer, IACS, Washington, DC 20064 USA. [Guandique, E.; Kaelberer, M. S.; Tingley, J. S.] ADNET Syst Inc, Rockville, MD 20852 USA. [Albright, S. A.] Syst & Software Designers Inc, Columbia, MD 21045 USA. [de Kok, R.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [de Kok, R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Coustenis, A.; Vinatier, S.; Bampasidis, G.] Univ Paris Diderot, Univ Paris 06, CNRS, Observ Paris,LESIA, F-92195 Meudon, France. [Bampasidis, G.] Univ Athens, Fac Phys, GR-15783 Athens, Greece. [Teanby, N. A.] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England. [Calcutt, S.] Univ Oxford, Dept Phys, Oxford OX1 3PU, England. RP Jennings, DE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM donald.e.jennings@nasa.gov RI Flasar, F Michael/C-8509-2012; Nixon, Conor/A-8531-2009; OI Nixon, Conor/0000-0001-9540-9121; Cottini, Valeria/0000-0003-0839-5855; Calcutt, Simon/0000-0002-0102-3170; Teanby, Nicholas/0000-0003-3108-5775 FU NASA's Cassini mission and Cassini Data Analysis Program FX We acknowledge support from NASA's Cassini mission and Cassini Data Analysis Program. NR 26 TC 3 Z9 3 U1 2 U2 12 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 MAY 10 PY 2015 VL 804 IS 2 AR L34 DI 10.1088/2041-8205/804/2/L34 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH8NN UT WOS:000354293200008 ER PT J AU Boggs, SE Harrison, FA Miyasaka, H Grefenstette, BW Zoglauer, A Fryer, CL Reynolds, SP Alexander, DM An, H Barret, D Christensen, FE Craig, WW Forster, K Giommi, P Hailey, CJ Hornstrup, A Kitaguchi, T Koglin, JE Madsen, KK Mao, PH Mori, K Perri, M Pivovaroff, MJ Puccetti, S Rana, V Stern, D Westergaard, NJ Zhang, WW AF Boggs, S. E. Harrison, F. A. Miyasaka, H. Grefenstette, B. W. Zoglauer, A. Fryer, C. L. Reynolds, S. P. Alexander, D. M. An, H. Barret, D. Christensen, F. E. Craig, W. W. Forster, K. Giommi, P. Hailey, C. J. Hornstrup, A. Kitaguchi, T. Koglin, J. E. Madsen, K. K. Mao, P. H. Mori, K. Perri, M. Pivovaroff, M. J. Puccetti, S. Rana, V. Stern, D. Westergaard, N. J. Zhang, W. W. TI Ti-44 gamma-ray emission lines from SN1987A reveal an asymmetric explosion SO SCIENCE LA English DT Article ID CORE-COLLAPSE SUPERNOVAE; SN 1987A; LIGHT-CURVE; CHANDRA OBSERVATIONS; NEUTRINO BURST; SN-1987A; EJECTA; PROFILES; SPECTRUM AB In core-collapse supernovae, titanium-44 (Ti-44) is produced in the innermost ejecta, in the layer of material directly on top of the newly formed compact object. As such, it provides a direct probe of the supernova engine. Observations of supernova 1987A (SN1987A) have resolved the 67.87- and 78.32-kilo-electron volt emission lines from decay of Ti-44 produced in the supernova explosion. These lines are narrow and redshifted with a Doppler velocity of similar to 700 kilometers per second, direct evidence of large-scale asymmetry in the explosion. C1 [Boggs, S. E.; Zoglauer, A.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Harrison, F. A.; Miyasaka, H.; Grefenstette, B. W.; Forster, K.; Madsen, K. K.; Mao, P. H.; Rana, V.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Fryer, C. L.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Reynolds, S. P.] NC State Univ, Dept Phys, Raleigh, NC 27695 USA. [Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [An, H.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Barret, D.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Barret, D.] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France. [Christensen, F. E.; Hornstrup, A.; Westergaard, N. J.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, W. W.; Pivovaroff, M. J.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Giommi, P.; Perri, M.; Puccetti, S.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00133 Rome, Italy. [Hailey, C. J.; Mori, K.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Kitaguchi, T.] RIKEN Nishina Ctr, Wako, Saitama 3510198, Japan. [Koglin, J. E.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Perri, M.; Puccetti, S.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Boggs, SE (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM boggs@berkeley.edu RI Boggs, Steven/E-4170-2015 OI Boggs, Steven/0000-0001-9567-4224 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; French Space Agency (CNES); Japan Society for the Promotion of Science [24740185]; Technical University of Denmark FX This work was supported under NASA Contract no. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). D.B. acknowledges funding from the French Space Agency (CNES). T.K. was supported by Japan Society for the Promotion of Science Grant-in-Aid for Young Scientists (B) (no. 24740185). N.J.W. acknowledges funding from the Technical University of Denmark. NuSTAR data are accessible from NASA's High Energy Astrophysics Science Archive Research Center (HEASARC, http://heasarc.gsfc.nasa.gov/). NR 32 TC 20 Z9 20 U1 2 U2 4 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 MAY 8 PY 2015 VL 348 IS 6235 BP 670 EP 671 DI 10.1126/science.aaa2259 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CH5AI UT WOS:000354045700039 PM 25954004 ER PT J AU Muratov, CB Osipov, VV Vanden-Eijnden, E AF Muratov, C. B. Osipov, V. V. Vanden-Eijnden, E. TI Energy barriers for bit-encoding states based on 360 degrees domain walls in ultrathin ferromagnetic nanorings SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID RANDOM-ACCESS MEMORY; MICROMAGNETICS; PATH AB A numerical thermal stability study of the bit-encoding states in a proposed multi-level magnetic storage element based on an ultrathin ferromagnetic nanoring is presented. The material parameters and the ring dimensions for which there are five distinct metastable magnetization configurations separated by energy barriers exceeding 50k(B)T at room temperature are identified. The results are obtained, using the string method for the study of rare events to locate the transition states separating the metastable states and to identify the most likely thermally activated pathways. (c) 2015 AIP Publishing LLC. C1 [Muratov, C. B.] New Jersey Inst Technol, Dept Math Sci, Newark, NJ 07102 USA. [Osipov, V. V.] NASA, Intelligent Syst Div, D&SH Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. [Vanden-Eijnden, E.] New York Univ, Courant Inst Math Sci, New York, NY 10012 USA. RP Muratov, CB (reprint author), New Jersey Inst Technol, Dept Math Sci, Newark, NJ 07102 USA. EM muratov@njit.edu FU NSF [DMS-0908279, DMS-1313687, DMS-0708140]; ONR [N00014-11-1-0345] FX The work of C.B.M. was supported by NSF via Grant Nos. DMS-0908279 and DMS-1313687. E. V.-E. was supported in part by NSF Grant No. DMS-0708140 and ONR Grant No. N00014-11-1-0345. NR 35 TC 1 Z9 1 U1 2 U2 16 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 MAY 7 PY 2015 VL 117 IS 17 AR 17D118 DI 10.1063/1.4914341 PG 4 WC Physics, Applied SC Physics GA CI7YW UT WOS:000354984100341 ER PT J AU Song, XP Huang, CQ Saatchi, SS Hansen, MC Townshend, JR AF Song, Xiao-Peng Huang, Chengquan Saatchi, Sassan S. Hansen, Matthew C. Townshend, John R. TI Annual Carbon Emissions from Deforestation in the Amazon Basin between 2000 and 2010 SO PLOS ONE LA English DT Article ID FOREST COVER CHANGE; BRAZILIAN AMAZON; TROPICAL DEFORESTATION; LAND-USE; INTERANNUAL VARIABILITY; UNITED-STATES; DENSITY MAPS; TREE COVER; BIOMASS; CLOUD AB Reducing emissions fromdeforestation and forest degradation (REDD+) is considered one of themost cost-effective strategies for mitigating climate change. However, historical deforestation and emission rates. critical inputs for setting reference emission levels for REDD+. are poorly understood. Here we use multi-source, time-series satellite data to quantify carbon emissions from deforestation in the Amazon basin on a year-to-year basis between 2000 and 2010. We first derive annual deforestation indicators by using the Moderate Resolution Imaging Spectroradiometer Vegetation Continuous Fields (MODIS VCF) product. MODIS indicators are calibrated by using a large sample of Landsat data to generate accurate deforestation rates, which are subsequently combined with a spatially explicit biomass dataset to calculate committed annual carbon emissions. Across the study area, the average deforestation and associated carbon emissions were estimated to be 1.59 +/- 0.25M ha.yr(-1) and 0.18 +/- 0.07 Pg C.yr(-1) respectively, with substantially different trends and inter-annual variability in different regions. Deforestation in the Brazilian Amazon increased between 2001 and 2004 and declined substantially afterwards, whereas deforestation in the Bolivian Amazon, the Colombian Amazon, and the Peruvian Amazon increased over the study period. The average carbon density of lost forests after 2005 was 130 Mg C.ha(-1), similar to 11% lower than the average carbon density of remaining forests in year 2010 (144 Mg C.ha(-1)). Moreover, the average carbon density of cleared forests increased at a rate of 7 Mg C.ha(-1).yr(-1) from 2005 to 2010, suggesting that deforestation has been progressively encroaching into high-biomass lands in the Amazon basin. Spatially explicit, annual deforestation and emission estimates like the ones derived in this study are useful for setting baselines for REDD+ and other emission mitigation programs, and for evaluating the performance of such efforts. C1 [Song, Xiao-Peng; Huang, Chengquan; Hansen, Matthew C.; Townshend, John R.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Song, Xiao-Peng; Huang, Chengquan; Townshend, John R.] Univ Maryland, Global Land Cover Facil, College Pk, MD 20742 USA. [Saatchi, Sassan S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Song, XP (reprint author), Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. EM xpsong@umd.edu RI Song, Xiao-Peng/F-4894-2014 OI Song, Xiao-Peng/0000-0002-5514-0321 FU NASA's Earth and Space Science Fellowship (NESSF) Program [NNX12AN92H]; Making Earth System Data Records for Use in Research Environments (MEaSUREs) Program [NNX08AP33A]; Land Cover and Land Use Change Program [NNH07ZDA001N-LCLUC]; NASA's FX This study was funded by NASA's Earth and Space Science Fellowship (NESSF) Program (NNX12AN92H), Making Earth System Data Records for Use in Research Environments (MEaSUREs) Program (NNX08AP33A), and Land Cover and Land Use Change Program (NNH07ZDA001N-LCLUC). Additional support was provided by NASA's NR 91 TC 14 Z9 14 U1 8 U2 45 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 MAY 7 PY 2015 VL 10 IS 5 AR e0126754 DI 10.1371/journal.pone.0126754 PG 21 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CH7KF UT WOS:000354214400108 PM 25951328 ER PT J AU Spitale, JN Hurford, TA Rhoden, AR Berkson, EE Platts, SS AF Spitale, Joseph N. Hurford, Terry A. Rhoden, Alyssa R. Berkson, Emily E. Platts, Symeon S. TI Curtain eruptions from Enceladus' south-polar terrain SO NATURE LA English DT Article ID PLUME; JETS AB Observations of the south pole of the Saturnian moon Enceladus revealed large rifts in the south-polar terrain, informally called 'tiger stripes', named Alexandria, Baghdad, Cairo and Damascus Sulci. These fractures have been shown to be the sources of the observed jets of water vapour and icy particles(1-4) and to exhibit higher temperatures than the surrounding terrain(5,6). Subsequent observations have focused on obtaining close-up imaging of this region to better characterize these emissions. Recent work(7) examined those newer data sets and used triangulation of discrete jets3 to produce maps of jetting activity at various times. Here we show that much of the eruptive activity can be explained by broad, curtain-like eruptions. Optical illusions in the curtain eruptions resulting from a combination of viewing direction and local fracture geometry produce image features that were probably misinterpreted previously as discrete jets. We present maps of the total emission along the fractures, rather than just the jet-like component, for five times during an approximately one-year period in 2009 and 2010. An accurate picture of the style, timing and spatial distribution of the south-polar eruptions is crucial to evaluating theories for the mec(h)anism controlling the eruptions. C1 [Spitale, Joseph N.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Hurford, Terry A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rhoden, Alyssa R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Berkson, Emily E.] Rochester Inst Technol, Rochester, NY 14623 USA. [Platts, Symeon S.] Univ Arizona, Film & Televis Dept, Tucson, AZ 85721 USA. RP Spitale, JN (reprint author), Planetary Sci Inst, 1700 East Ft Lowell Rd,Suite 106, Tucson, AZ 85719 USA. EM jnspitale@psi.edu RI Hurford, Terry/F-2625-2012 FU Cassini Data Analysis and Participating Scientists Program [NNX13AG45G] FX This work was funded by grant number NNX13AG45G of the Cassini Data Analysis and Participating Scientists Program. We thank M. Hedman, P. Thomas and C. Howett for conversations on this topic. NR 7 TC 12 Z9 12 U1 1 U2 12 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 MAY 7 PY 2015 VL 521 IS 7550 BP 57 EP U368 DI 10.1038/nature14368 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CH4YS UT WOS:000354040900031 PM 25951283 ER PT J AU Luneva, MV Clayson, CA Dubovikov, MS AF Luneva, M. V. Clayson, C. A. Dubovikov, M. S. TI Effects of mesoscale eddies in the active mixed layer: test of the parametrisation in eddy resolving simulations SO GEOPHYSICAL AND ASTROPHYSICAL FLUID DYNAMICS LA English DT Article; Proceedings Paper CT Workshop on the Dynamics of Shelf Seas CY OCT 23-24, 2013 CL Univ Liverpool, Liverpool, ENGLAND HO Univ Liverpool DE Mesoscale parametrisation; Active mixed layer; Eddy resolving simulations; Restratification; Eddy diffusivity; omega-equation ID VERTICAL VELOCITY; OCEAN; CIRCULATION; MODEL; SEA; PARAMETERIZATION; SURFACE; FRONTS; FLUXES; DIAGNOSIS AB In eddy resolving simulations, we test a mixed layer mesoscale parametrisation, developed recently by Canuto and Dubovikov [Ocean Model., 2011, 39, 200-207]. With no adjustable parameters, the parametrisation yields the horizontal and vertical mesoscale fluxes in terms of coarse-resolution fields and eddy kinetic energy (EKE). We compare terms of the parametrisation diagnosed from coarse-grained fields with the eddy mesoscale fluxes diagnosed directly from the high resolution model. An expression for the EKE in terms of mean fields has also been found to get a closed parametrisation in terms of the mean fields only. In 40 numerical experiments we simulated two types of flows: idealised flows driven by baroclinic instabilities only, and more realistic flows, driven by wind and surface fluxes as well as by inflow-outflow. The diagnosed quasi-instantaneous horizontal and vertical mesoscale buoyancy fluxes (averaged over 1 degrees - 2 degrees and 10 days) demonstrate a strong scatter typical for turbulent flows, however, the fluxes are positively correlated with the parametrisation with higher (0.5-0.74) correlations at the experiments with larger baroclinic radius Rossby. After being averaged over 3-4 months, diffusivities diagnosed from the eddy resolving simulations are consistent with the parametrisation for a broad range of parameters. Diagnosed vertical mesoscale fluxes restratify mixed layer and are in a good agreement with the parametrisation unless vertical turbulent mixing in the upper layer becomes strong enough in comparison with mesoscale advection. In the latter case, numerical simulations demonstrate that the deviation of the fluxes from the parametrisation is controlled by dimensionless parameter estimating the ratio of vertical turbulent mixing term to mesoscale advection. An analysis using a modified omega-equation reveals that the effects of the vertical mixing of vorticity is responsible for the two-three fold amplification of vertical mesoscale flux. Possible physical mechanisms, responsible for the amplification of vertical mesoscale flux are discussed. C1 [Luneva, M. V.] Natl Oceanog Ctr, Liverpool L3 5DA, Merseyside, England. [Clayson, C. A.] Woods Hole Oceanog Inst, Phys Oceanog, Woods Hole, MA 02543 USA. [Dubovikov, M. S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Dubovikov, M. S.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. RP Luneva, MV (reprint author), Natl Oceanog Ctr, 6 Brownlow St, Liverpool L3 5DA, Merseyside, England. EM mane1@noc.ac.uk FU UK Natural Environment Research Council (NERC); Office of Naval Research [N00014-03-1-0989, N00014-12-10188]; NASA High-End Computing (HEC) Program through the NASA Center for Climate Simulation (NCCS) at the Goddard Space Flight Center FX The work has been dedicated to Professor John Huthnance on the occasion of his retirement. We thank Professor V.M. Canuto for a useful discussion of the manuscript and an anonymous reviewers for detailed analysis of our paper and valuable criticisms. The authors acknowledge the National Capability funding provided by the UK Natural Environment Research Council (NERC), the Office of Naval Research under grants N00014-03-1-0989 and N00014-12-10188, and the NASA High-End Computing (HEC) Program through the NASA Center for Climate Simulation (NCCS) at the Goddard Space Flight Center. NR 44 TC 0 Z9 0 U1 1 U2 6 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND SN 0309-1929 EI 1029-0419 J9 GEOPHYS ASTRO FLUID JI Geophys. Astrophys. Fluid Dyn. PD MAY 4 PY 2015 VL 109 IS 3 SI SI BP 281 EP 310 DI 10.1080/03091929.2015.1041023 PG 30 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Mechanics SC Astronomy & Astrophysics; Geochemistry & Geophysics; Mechanics GA CL6QW UT WOS:000357093200006 ER PT J AU Wei, JW Lee, ZP Lewis, M Pahlevan, N Ondrusek, M Armstrong, R AF Wei, Jianwei Lee, Zhongping Lewis, Marlon Pahlevan, Nima Ondrusek, Michael Armstrong, Roy TI Radiance transmittance measured at the ocean surface SO OPTICS EXPRESS LA English DT Article ID WATER-LEAVING RADIANCE; IN-WATER; COLOR; MODEL; REFLECTANCE; FIELD AB The radiance transmittance (T-r) is the ratio of the water-leaving radiance (L-w(0(+))) to the sub-surface upwelling radiance (L-u(0(-))), which is an important optical parameter for ocean optics and ocean color remote sensing. Historically, a constant value (similar to 0.54) based on theoretical presumptions has been adopted for Tr and is widely used. This optical parameter, however, has never been measured in the aquatic environments. With a robust setup to measure both L-u(0(-)) and L-w(0(+)) simultaneously in the field, this study presents Tr in the zenith direction between 350 and 700 nm measured in a wide range of oceanic waters. It is found that the measured T-r values are generally consistent with the long-standing theoretical value of 0.54, with mean relative difference less than 10%. In particular, the agreement within the spectral domain of 400-600 nm is found to be the best (with the averaged difference less than 5%). The largest difference is observed for wavelengths longer than 600 nm with the average difference less than 15%, which is related to the generally very small values in both L-u(0(-)) and L-w(0(+)) and rough environmental conditions. These results provide a validation of the setup for simultaneous measurements of upwelling radiance and water-leaving radiance and confidence in the theoretical T-r value used in ocean optics studies at least for oceanic waters. (C) 2015 Optical Society of America C1 [Wei, Jianwei; Lee, Zhongping] Univ Massachusetts, Sch Environm, Opt Oceanog Lab, Boston, MA 02125 USA. [Lewis, Marlon] Dalhousie Univ, Dept Oceanog, Halifax, NS B3H 4J1, Canada. [Pahlevan, Nima] NASA Goddard Space Flight Ctr, Terr Informat Syst Lab, Greenbelt, MD 20771 USA. [Pahlevan, Nima] SSAI, Lanham, MD 20706 USA. [Ondrusek, Michael] NOAA Ctr Weather & Climate Predict NCWCP, College Pk, MD 20740 USA. [Armstrong, Roy] Univ Puerto Rico, Bioopt Oceanog Lab, Mayaguez, PR 00681 USA. RP Wei, JW (reprint author), Univ Massachusetts, Sch Environm, Opt Oceanog Lab, Boston, MA 02125 USA. EM jianwei.wei@umb.edu RI Ondrusek, Michael/F-5617-2010; wei, Jianwei/E-8031-2016; OI Ondrusek, Michael/0000-0002-5311-9094; wei, Jianwei/0000-0002-6872-3534; Pahlevan, Nima/0000-0002-5454-5212 FU National Aeronautic and Space Administration (NASA) Ocean Biology and Biogeochemistry and Water and Energy Cycle Programs; National Oceanic and Atmospheric Administration (NOAA) JPSS VIIRS Ocean Color Cal/Val Project; NOAA CREST Grant [NA06OAR480162] FX This study is funded by the National Aeronautic and Space Administration (NASA) Ocean Biology and Biogeochemistry and Water and Energy Cycle Programs and the National Oceanic and Atmospheric Administration (NOAA) JPSS VIIRS Ocean Color Cal/Val Project. Field measurements in Puerto Rico were partially supported by NOAA CREST Grant # NA06OAR480162. We thank Dr. Giuseppe Zibordi for assistance in the field campaign. Three anonymous reviewers are thanked for their comments and suggestions. NR 23 TC 5 Z9 5 U1 0 U2 5 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD MAY 4 PY 2015 VL 23 IS 9 BP 11826 EP 11837 DI 10.1364/OE.23.011826 PG 12 WC Optics SC Optics GA CH9EB UT WOS:000354337700091 PM 25969274 ER PT J AU DellaCorte, C AF DellaCorte, Christopher TI REMEMBERING EDWARD T. HANEY SO TRIBOLOGY & LUBRICATION TECHNOLOGY LA English DT Letter C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP DellaCorte, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU SOC TRIBOLOGISTS & LUBRICATION ENGINEERS PI PARK RIDGE PA 840 BUSSE HIGHWAY, PARK RIDGE, IL 60068 USA SN 1545-858X J9 TRIBOL LUBR TECHNOL JI Tribol. Lubr. Technol. PD MAY PY 2015 VL 71 IS 5 BP 7 EP 7 PG 1 WC Engineering, Mechanical SC Engineering GA CG6UF UT WOS:000353437200011 ER PT J AU Nayagam, V Dietrich, DL Hicks, MC Williams, FA AF Nayagam, Vedha Dietrich, Daniel L. Hicks, Michael C. Williams, Forman A. TI Cool-flame, extinction during n-alkane droplet combustion in microgravity SO COMBUSTION AND FLAME LA English DT Article DE Cool flame extinction; Droplet combustion; Microgravity; Normal alkane ID SPHERICAL DIFFUSION FLAMES; SYSTEMS; HEPTANE; HYDROCARBON; OXIDATION; IGNITION AB Recent droplet-combustion experiments onboard the International Space Station (ISS) have revealed that large n-alkane droplets, following radiative extinction of the visible flame, can continue to burn quasisteadily in a low-temperature regime, characterized by negative-temperature-coefficient (NTC) chemistry. In this study we report experimental observations of n-heptane, n-octane, and n-decane droplets of varying initial size burning in oxygen/nitrogen, oxygen/nitrogen/carbon dioxide, and oxygen/nitrogen/helium environments at pressures from 0.5 to 1.0 atm, with oxygen concentrations from 14% to 25% by volume. These large n-alkane droplets exhibited radiative extinction of the hot flame, followed by quasi-steady low-temperature burning, which terminated with diffusive extinction accompanied by the formation of a vapor cloud, while small droplets did not exhibit radiative extinction but instead burned to completion or disruptively extinguished. Results for droplet burning rates in both the hot-flame and cool-flame regimes, as well as droplet extinction diameters at the end of each stage, are presented. The cool-flame extinction diameters for all three n-alkanes are shown to follow a similar trend as functions of the oxygen concentration, predicted here from a simplified theoretical model that is based on the reaction-rate parameters for the oxygen molecule addition to the alkyl radical and for ketohydroperoxide decomposition. (C) 2015 The Combustion Institute. Published by Elsevier Inc. All rights reserved. C1 [Nayagam, Vedha] Case Western Reserve Univ, Dept Mech & Aerosp Engn, Cleveland, OH 44106 USA. [Dietrich, Daniel L.; Hicks, Michael C.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Williams, Forman A.] Univ Calif San Diego, Dept Mech & Aerosp Engn, La Jolla, CA 92093 USA. RP Nayagam, V (reprint author), Case Western Reserve Univ, Dept Mech & Aerosp Engn, Cleveland, OH 44106 USA. EM v.nayagam@grc.nasa.gov FU NASA Space Life and Physical Sciences Research and Applications Program; International Space Station Program FX The authors would like to thank the FLEX team members Profs. T. Avedisian, M.Y. Choi, T. Farouk, F. Dryer, and B. Shaw. This work was supported by the NASA Space Life and Physical Sciences Research and Applications Program and the International Space Station Program. Mr. J. Mark Hickman served as the project manager. NR 19 TC 11 Z9 11 U1 4 U2 16 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 MAY PY 2015 VL 162 IS 5 BP 2140 EP 2147 DI 10.1016/j.combustflame.2015.01.012 PG 8 WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary; Engineering, Chemical; Engineering, Mechanical SC Thermodynamics; Energy & Fuels; Engineering GA CN6RI UT WOS:000358561500045 ER PT J AU Detweiler, AM Mioni, CE Hellier, KL Allen, JJ Carter, SA Bebout, BM Fleming, EE Corrado, C Prufert-Bebout, LE AF Detweiler, Angela M. Mioni, Cecile E. Hellier, Katie L. Allen, Jordan J. Carter, Sue A. Bebout, Brad M. Fleming, Erich E. Corrado, Carley Prufert-Bebout, Leslie E. TI Evaluation of wavelength selective photovoltaic panels on microalgae growth and photosynthetic efficiency SO ALGAL RESEARCH-BIOMASS BIOFUELS AND BIOPRODUCTS LA English DT Article DE Microalgae cultivation; Growth rate; Wavelength selective luminescent solar concentrators; Photovoltaic cells; Greenhouse ID LIGHT-EMITTING-DIODES; NITROGEN LIMITATION; SOLAR CONCENTRATORS; ENERGY-CONVERSION; DUNALIELLA-SALINA; ALGAE; ENHANCEMENT; IRRADIANCE; RADIATION; CULTURE AB Large-scale cultivation of microalgal biomass in open systems can benefit fromthe lowcost of using natural sun-light, as opposed to artificial light, but may encounter problems with photoinhibition, high evaporation rates, potential contamination and high energy demand. Wavelength selective luminescent solar concentrator (LSC) panels can solve some of these problems when incorporated into low-cost sheltered structures for algal biomass production that concurrently produce their own electricity by harnessing select portions of solar energy, not used for algal growth. The LSC panels in this study contained a fluorescent dye, Lumogen Red 305, which transmits blue and red wavelengths used for photosynthesis with high efficiency, while absorbing the green wavelengths and re-emitting them as red wavelengths. The fluorescently generated red wavelengths are either transmitted to boost algal growth, or waveguided and captured by photovoltaic cells to be converted into electricity. We found that different strains of microalgae (currently used commercially) grew equally well under the altered spectral conditions created by the luminescent panels, compared to growth under the full solar spectrum. Thus this technology presents a new approach wherein algae can be grown under protected, controlled conditions, while the cost of operations is offset by the structure's internal electrical production, without any loss to algal growth rate or achievable biomass density. Published by Elsevier B.V. C1 [Detweiler, Angela M.; Bebout, Brad M.; Prufert-Bebout, Leslie E.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. [Detweiler, Angela M.] Bay Area Environm Res Inst, Petaluma, CA 94952 USA. [Mioni, Cecile E.] Calif State Univ Monterey Bay, Sci & Environm Policy Div, Seaside, CA 93955 USA. [Hellier, Katie L.; Carter, Sue A.; Corrado, Carley] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Allen, Jordan J.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Fleming, Erich E.] Calif State Univ Channel Islands, Dept Biol, Camarillo, CA 93012 USA. RP Prufert-Bebout, LE (reprint author), NASA, Ames Res Ctr, Mail Stop 239-4,Bldg 239,Room 334,POB 1, Moffett Field, CA 94035 USA. EM leslie.e.bebout@nasa.gov OI Hellier, Kaitlin/0000-0002-6328-1167 FU UC Discovery Grant "Lowcost, high efficiency luminescent solar greenhouse" [192864]; Abengoa Solar FX This study was funded by the UC Discovery Grant "Lowcost, high efficiency luminescent solar greenhouse" (grant # 192864) to Dr. Sue Carter in collaboration with the Algae for Exploration (AlEx) working group in the Exobiology Branch at NASA ARC. Dr. Carter received additional funding from Abengoa Solar. The authors would like to thank Glenn Alers for making available the LSC panels used in this study, Stuart Pilorz for the help with data analysis, and Craig Everroad and Thomas Murphy for their insightful comments in reviewing this manuscript. NR 34 TC 3 Z9 3 U1 7 U2 49 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 2211-9264 J9 ALGAL RES JI Algal Res. PD MAY PY 2015 VL 9 BP 170 EP 177 DI 10.1016/j.algal.2015.03.003 PG 8 WC Biotechnology & Applied Microbiology SC Biotechnology & Applied Microbiology GA CM8YF UT WOS:000357988700021 ER PT J AU Ciceri, S Mancini, L Southworth, J Bruni, I Nikolov, N D'Ago, G Schroder, T Bozza, V Tregloan-Reed, J Henning, T AF Ciceri, S. Mancini, L. Southworth, J. Bruni, I. Nikolov, N. D'Ago, G. Schroeder, T. Bozza, V. Tregloan-Reed, J. Henning, Th. TI Physical properties of the HAT-P-23 and WASP-48 planetary systems from multi-colour photometry SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary systems; stars: fundamental parameters; techniques: photometric; stars: individual: HAT-P-23; stars: individual: WASP-48 ID TRANSITING EXTRASOLAR PLANETS; STELLAR EVOLUTION DATABASE; HIGH-PRECISION PHOTOMETRY; LIMB-DARKENING LAW; TRANSMISSION SPECTRUM; SURFACE GRAVITIES; LIGHT-CURVE; ATMOSPHERE MODELS; TIDAL-EVOLUTION; PARAMETERS AB Context. Accurate and repeated photometric follow-up observations of planetary transit events are important to precisely characterize the physical properties of exoplanets. A good knowledge of the main characteristics of the exoplanets is fundamental in order to trace their origin and evolution. Multi-band photometric observations play an important role in this process. Aims. By using new photometric data, we computed precise estimates of the physical properties of two transiting planetary systems at equilibrium temperatures of similar to 2000 K. Methods. We present new broadband, multi-colour photometric observations obtained using three small class telescopes and the telescope-defocussing technique. In particular we obtained 11 and 10 light curves covering 8 and 7 transits of HAT-P-23 and WASP-48, respectively. For each of the two targets, one transit event was simultaneously observed through four optical filters. One transit of WASP-48 b was monitored with two telescopes from the same observatory. The physical parameters of the systems were obtained by fitting the transit light curves with JKTEBOP and from published spectroscopic measurements. Results. We have revised the physical parameters of the two planetary systems, finding a smaller radius for both HAT-P-23 b and WASP-48 b, R-b = 1.224 +/- 0.037 R-Jup and R-b = 1.396 +/- 0.051 R-Jup, respectively, than those measured in the discovery papers (R-b = 1.368 +/- 0.090 R-Jup and R-b = 1.67 +/- 0.10 R-Jup). The density of the two planets are higher than those previously published (rho(b) similar to 1.1 and similar to 0.3 rho(jup) for HAT-P-23 and WASP-48, respectively) hence the two hot Jupiters are no longer located in a parameter space region of highly inflated planets. An analysis of the variation of the planet's measured radius as a function of optical wavelength reveals flat transmission spectra within the experimental uncertainties. We also confirm the presence of the eclipsing contact binary NSVS-3071474 in the same field of view of WASP-48, for which we refine the value of the period to be 0.459 d. C1 [Ciceri, S.; Mancini, L.; Schroeder, T.; Henning, Th.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Bruni, I.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Nikolov, N.] Univ Exeter, Astrophys Grp, Exeter EX4 4QL, Devon, England. [D'Ago, G.; Bozza, V.] Univ Salerno, Dept Phys, I-84084 Fisciano, SA, Italy. [D'Ago, G.; Bozza, V.] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy. [Tregloan-Reed, J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Ciceri, S (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM ciceri@mpia.de RI D'Ago, Giuseppe/N-8318-2016; OI D'Ago, Giuseppe/0000-0001-9697-7331; Bruni, Ivan/0000-0002-1560-4590 NR 53 TC 4 Z9 4 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2015 VL 577 AR A54 DI 10.1051/0004-6361/201425449 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM0CN UT WOS:000357345900006 ER PT J AU Guo, JN Zeitlin, C Wimmer-Schweingruber, RF Hassler, DM Posner, A Heber, B Kohler, J Rafkin, S Ehresmann, B Appel, JK Bohm, E Bottcher, S Burmeister, S Brinza, DE Lohf, H Martin, C Reitz, G AF Guo, Jingnan Zeitlin, Cary Wimmer-Schweingruber, Robert F. Hassler, Donald M. Posner, Arik Heber, Bernd Koehler, Jan Rafkin, Scot Ehresmann, Bent Appel, Jan K. Boehm, Eckart Boettcher, Stephan Burmeister, Soenke Brinza, David E. Lohf, Henning Martin, Cesar Reitz, Goenther TI Variations of dose rate observed by MSL/RAD in transit to Mars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE instrumentation: detectors; space vehicles: instruments; solar-terrestrial relations ID GALACTIC COSMIC-RAYS; RADIATION; MODULATION AB Aims. To predict the cruise radiation environment related to future human missions to Mars, the correlation between solar modulation potential and the dose rate measured by the Radiation Assessment Detector (RAD) has been analyzed and empirical models have been employed to quantify this correlation. Methods. The instrument RAD, onboard Mars Science Laboratory's (MSL) rover Curiosity, measures a broad spectrum of energetic particles along with the radiation dose rate during the 253-day cruise phase as well as on the surface of Mars. With these first ever measurements inside a spacecraft from Earth to Mars, RAD observed the impulsive enhancement of dose rate during solar particle events as well as a gradual evolution of the galactic cosmic ray (GCR) induced radiation dose rate due to the modulation of the primary GCR flux by the solar magnetic field, which correlates with long-term solar activities and heliospheric rotation. Results. We analyzed the dependence of the dose rate measured by RAD on solar modulation potentials and estimated the dose rate and dose equivalent under different solar modulation conditions. These estimations help us to have approximate predictions of the cruise radiation environment, such as the accumulated dose equivalent associated with future human missions to Mars. Conclusions. The predicted dose equivalent rate during solar maximum conditions could be as low as one-fourth of the current RAD cruise measurement. However, future measurements during solar maximum and minimum periods are essential to validate our estimations. C1 [Guo, Jingnan; Wimmer-Schweingruber, Robert F.; Heber, Bernd; Koehler, Jan; Appel, Jan K.; Boehm, Eckart; Boettcher, Stephan; Burmeister, Soenke; Lohf, Henning; Martin, Cesar] Univ Kiel, Inst Expt & Appl Phys, D-24118 Kiel, Germany. [Zeitlin, Cary] SW Res Inst, Earth Oceans & Space Dept, Durham, NH USA. [Hassler, Donald M.; Rafkin, Scot; Ehresmann, Bent] SW Res Inst, Space Sci & Engn Div, Boulder, CO 80302 USA. [Posner, Arik] NASA Headquarters, Sci Miss Directorate, Washington, DC 20546 USA. [Brinza, David E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Reitz, Goenther] Deutsch Zentrum Luft & Raumfahrt, Aerosp Med, D-51147 Cologne, Germany. RP Guo, JN (reprint author), Univ Kiel, Inst Expt & Appl Phys, Olshaussenstr 40, D-24118 Kiel, Germany. EM guo@physik.uni-kiel.de FU National Aeronautics and Space Administration (NASA, HEOMD) under Jet Propulsion Laboratory (JPL) [1273039]; DLR; DLR's Space Administration [50QM0501, 50QM1201]; NASA FX RAD is supported by the National Aeronautics and Space Administration (NASA, HEOMD) under Jet Propulsion Laboratory (JPL) sub-contract #1273039 to Southwest Research Institute and in Germany by DLR and DLR's Space Administration grant numbers 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 thank Shawn Kang at JPL for his work on the shielding model of the spacecraft during the cruise phase. The sunspot data has been obtained from Source: WDC-SILSO, Royal Observatory of Belgium, Brussels. 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 the following URL: http://ppi.pds.nasa.gov/ NR 22 TC 6 Z9 6 U1 3 U2 8 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2015 VL 577 AR A58 DI 10.1051/0004-6361/201525680 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM0CN UT WOS:000357345900010 ER PT J AU Peretz, U Behar, E Drake, SA AF Peretz, Uria Behar, Ehud Drake, Stephen A. TI Coronae of stars with supersolar elemental abundances SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: abundances; stars: coronae; stars: general ID X-RAY SPECTROSCOPY; SOLAR-TYPE STARS; PHOTOSPHERIC ABUNDANCES; ATMOSPHERIC PARAMETERS; ENERGETIC PARTICLES; ALPHA-CENTAURI; ACTIVITY CYCLE; BINARY-SYSTEM; CHANDRA; DWARFS AB Coronal elemental abundances are known to deviate from the photospheric values of their parent star, with the degree of deviation depending on the first ionization potential (FIP). This study focuses on the coronal composition of stars with supersolar photospheric abundances. We present the coronal abundances of six such stars: 11 LMi, iota Hor, HR 7291, tau Boo, and alpha Cen A and B. These stars all have high-statistics X-ray spectra, three of which are presented for the first time. The abundances we measured were obtained using the line-resolved spectra of the Reflection Grating Spectrometer (RGS) in conjunction with the higher throughput EPIC-pn camera spectra onboard the XMM-Newton observatory. A collisionally ionized plasma model with two or three temperature components is found to represent the spectra well. All elements are found to be consistently depleted in the coronae compared to their respective photospheres. For 11 LMi and tau Boo no FIP effect is present, while iota Hor, HR 7291, and alpha Cen A and B show a clear FIP trend. These conclusions hold whether the comparison is made with solar abundances or the individual stellar abundances. Unlike the solar corona, where low-FIP elements are enriched, in these stars the FIP effect is consistently due to a depletion of high-FIP elements with respect to actual photospheric abundances. A comparison with solar (instead of stellar) abundances yields the same fractionation trend as on the Sun. In both cases, a similar FIP bias is inferred, but different fractionation mechanisms need to be invoked. C1 [Peretz, Uria; Behar, Ehud] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. [Drake, Stephen A.] USRA, CRESST, Greenbelt, MD 20771 USA. [Drake, Stephen A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Peretz, U (reprint author), Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. EM uperetz@tx.technion.ac.il FU I-CORE program of the Planning and Budgeting Committee; Israel Science Foundation [1937/12, 1163/10]; Israel's Ministry of Science and Technology; National Science Foundation [PHYS-1066293] FX The authors are grateful to an anonymous referee for useful comments that led us to broaden the sample of the paper. This research is supported by the I-CORE program of the Planning and Budgeting Committee and the Israel Science Foundation (grant numbers 1937/12 and 1163/10), and by a grant from Israel's Ministry of Science and Technology. This work was supported in part by the National Science Foundation under Grant No. PHYS-1066293 and the hospitality of the Aspen Center for Physics. NR 43 TC 1 Z9 1 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2015 VL 577 AR A93 DI 10.1051/0004-6361/201424769 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM0CN UT WOS:000357345900045 ER PT J AU Pon, A Caselli, P Johnstone, D Kaufman, M Butler, MJ Fontani, F Jimenez-Serra, I Tan, JC AF Pon, A. Caselli, P. Johnstone, D. Kaufman, M. Butler, M. J. Fontani, F. Jimenez-Serra, I. Tan, J. C. TI Mid-J CO shock tracing observations of infrared dark clouds. I. SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: clouds; stars: formation; turbulence; shock waves; ISM: molecules ID MASSIVE-STAR-FORMATION; MOLECULAR CLOUDS; MAGNETOHYDRODYNAMIC TURBULENCE; DISSIPATION; CORES; DEUTERATION; CHEMISTRY; EMISSION; VELOCITY; OUTFLOWS AB Infrared dark clouds (IRDCs) are dense, molecular structures in the interstellar medium that can harbour sites of high-mass star formation. IRDCs contain supersonic turbulence, which is expected to generate shocks that locally heat pockets of gas within the clouds. We present observations of the CO J = 8-7, 9-8, and 10-9 transitions, taken with the Herschel Space Observatory, towards four dense, starless clumps within IRDCs (C1 in G028.37+00.07, F1 and F2 in G034.43+0007, and G2 in G034.77-0.55). We detect the CO J = 8-7 and 9-8 transitions towards three of the clumps (C1, F1, and F2) at intensity levels greater than expected from photodissociation region (PDR) models. The average ratio of the 8-7 to 9-8 lines is also found to be between 1.6 and 2.6 in the three clumps with detections, significantly smaller than expected from PDR models. These low line ratios and large line intensities strongly suggest that the C1, F1, and F2 clumps contain a hot gas component not accounted for by standard PDR models. Such a hot gas component could be generated by turbulence dissipating in low velocity shocks. C1 [Pon, A.; Caselli, P.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Johnstone, D.] Joint Astron Ctr, Hilo, HI 96720 USA. [Johnstone, D.] NRC Herzberg Astron & Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. [Kaufman, M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Kaufman, M.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Butler, M. J.] Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland. [Fontani, F.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Jimenez-Serra, I.] European So Observ, D-85748 Garching, Germany. [Tan, J. C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Tan, J. C.] Univ Florida, Dept Phys, Gainesville, FL 32611 USA. RP Pon, A (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. EM andyrpon@mpe.mpg.de RI Fontani, Francesco/R-5351-2016 OI Fontani, Francesco/0000-0003-0348-3418 FU European Research Council (ERC) [PALs 320620]; Natural Sciences and Engineering Research Council (NSERC) Discovery Grant; European Union [PIIF-GA-2011-301538] FX We would like to thank our referee, Dr. Goldsmith, for helping us improve the quality of this paper. The authors would like to thank Dr. N. Bailey, Dr. J. Bailey, and Dr. J. D. Henshaw for many insightful conversations regarding the data presented in this paper. The authors also thank Dr. C. McCoey and Dr. S. Beaulieu for help with HIPE. A.P. and P.C. acknowledge the financial support of the European Research Council (ERC; project PALs 320620). D. J. acknowledges support from a Natural Sciences and Engineering Research Council (NSERC) Discovery Grant. I. J. S. acknowledges the funding received from the People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme (FP7/2007-2013) under REA grant agreement PIIF-GA-2011-301538. This research has made use of the Smithsonian Astrophysical Observatory (SAO)/National Aeronautics and Space Administration's (NASA's) Astrophysics Data System (ADS). HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. This research has made use of the astro-ph archive. Some spectral line data were taken from the Spectral Line Atlas of Interstellar Molecules (SLAIM; Available at http://www.splatalogue.net); (Lovas, priv. comm.; Remijan et al. 2007). NR 38 TC 8 Z9 8 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2015 VL 577 AR A75 DI 10.1051/0004-6361/201525681 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM0CN UT WOS:000357345900027 ER PT J AU Vinas, AF Moya, PS Navarro, RE Valdivia, JA Araneda, JA Munoz, V AF Vinas, Adolfo F. Moya, Pablo S. Navarro, Roberto E. Valdivia, J. Alejandro Araneda, Jaime A. Munoz, Victor TI Electromagnetic fluctuations of the whistler-cyclotron and firehose instabilities in a Maxwellian and Tsallis-kappa-like plasma SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SOLAR-WIND; THERMAL NOISE; ELECTRONS; DISTRIBUTIONS; STATISTICS; ION AB Observed electron velocity distributions in the Earth's magnetosphere and the solar wind exhibit a variety of nonthermal features which deviate from thermal equilibrium, for example, in the form of temperature anisotropies, suprathermal tail extensions, and field-aligned beams. The state close to thermal equilibrium and its departure from it provides a source for spontaneous emissions of electromagnetic fluctuations, such as the whistler. Here we present a comparative analysis of the electron whistler-cyclotron and firehose fluctuations based upon anisotropic plasma modeled with Maxwellian and Tsallis-kappa-like particle distributions, to explain the correspondence relationship of the magnetic fluctuations as a function of the electron temperature and thermal anisotropy in the solar wind and magnetosphere plasmas. The analysis presented here considers correlation theory of the fluctuation-dissipation theorem and the dispersion relation of transverse fluctuations, with wave vectors parallel to the uniform background magnetic field, in a finite temperature anisotropic thermal bi-Maxwellian and nonthermal Tsallis-kappa-like magnetized electron-proton plasma. Dispersion analysis and stability thresholds are derived for these thermal and nonthermal distributions using plasma and field parameters relevant to the solar wind and magnetosphere environments. Our results indicate that there is an enhancement of the fluctuations level in the case of nonthermal distributions due to the effective higher temperature and the excess of suprathermal particles. These results suggest that a comparison of the electromagnetic fluctuations due to thermal and nonthermal distributions provides a diagnostic signature by which inferences about the nature of the particle velocity distribution function can be ascertained without in situ particle measurements. C1 [Vinas, Adolfo F.; Moya, Pablo S.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Moya, Pablo S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Moya, Pablo S.; Navarro, Roberto E.; Valdivia, J. Alejandro; Munoz, Victor] Univ Chile, Fac Ciencias, Dept Fis, Santiago, Chile. [Navarro, Roberto E.; Araneda, Jaime A.] Univ Concepcion, Fac Ciencias Fis & Matemat, Dept Fis, Concepcion, Chile. RP Vinas, AF (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. EM adolfo.vinas@nasa.gov RI Moya, Pablo/C-3163-2011; Valdivia, Juan/A-3631-2008; Araneda, Jaime/J-9245-2015; Navarro, Roberto/F-7045-2014; Munoz, Victor/A-2255-2008 OI Moya, Pablo/0000-0002-9161-0888; Valdivia, Juan/0000-0003-3381-9904; Navarro, Roberto/0000-0003-0782-1904; FU NASA's Wind/SWE program; Comision Nacional de Ciencia y Tecnologia (CONICyT, Chile); FONDECYT [1110880, 3150262, 1121144, 1110135, 1110729, 1130273] FX A. F. Vinas would like to thank the NASA's Wind/SWE program for the support of this research. We also thank the Comision Nacional de Ciencia y Tecnologia (CONICyT, Chile) by providing financial support for postdoctoral (P. S. Moya) and doctoral (R. Navarro) fellows. We would like to thank FONDECYT 1110880 (J. A. Araneda), 3150262 (R. E. Navarro), 1121144 (V. Munoz), and 1110135, 1110729, and 1130273 (J. A. Valdivia) for providing financial support. The results of this paper do not require any spacecraft data analysis, but the numerical data generated to reproduce all the figures will be made available upon request. NR 40 TC 19 Z9 19 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAY PY 2015 VL 120 IS 5 BP 3307 EP 3317 DI 10.1002/2014JA020554 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM7KA UT WOS:000357869600003 ER PT J AU Tang, XW Cattell, C Lysak, R Wilson, LB Dai, L Thaller, S AF Tang, Xiangwei Cattell, Cynthia Lysak, Robert Wilson, Lynn B., III Dai, Lei Thaller, Scott TI THEMIS observations of electrostatic ion cyclotron waves and associated ion heating near the Earth's dayside magnetopause SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID FIELD-ALIGNED CURRENTS; HYDROGEN CYCLOTRON; PLASMA-WAVES; POLAR MAGNETOSPHERE; INSTABILITY; EXCITATION; DIFFUSION; BEAMS; MAGNETOTAIL; INSTRUMENT AB We present the first observations of large-amplitude electrostatic ion cyclotron (EIC) waves near the Earth's dayside magnetopause at MLT of similar to 14 using data from Time History of Events and Macroscale Interactions during Substorms (THEMIS) satellites. The EIC waves were identified in a boundary layer in the magnetosphere adjacent to the magnetopause where reconnection was occurring. The EIC wave power was primarily at 2f(cH) (where f(cH) is the hydrogen cyclotron frequency) and simultaneously observed with perpendicular ion heating. The EIC waves had electric field amplitudes as large as 30 mV/m peak to peak with significant power both perpendicular and parallel to the magnetic field. These amplitudes were greater than those of previously observed ion cyclotron harmonics at the nightside magnetopause. The EIC waves occurred during an interval of enhancements in the quasi-static electric field and fluctuations in the background magnetic field, plasma density, and temperatures. The observations indicate that a plasma density gradient is a possible source of free energy for the EIC waves. The observed flow shears are not large enough to drive the waves. Whistler mode waves were identified near the EIC wave region but closer to the magnetopause in a region with slightly higher ion and electron temperatures. C1 [Tang, Xiangwei; Cattell, Cynthia; Lysak, Robert; Dai, Lei; Thaller, Scott] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Wilson, Lynn B., III] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA. RP Tang, XW (reprint author), Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. EM xtang@physics.umn.edu RI Wilson III, Lynn/D-4425-2012; OI Wilson III, Lynn/0000-0002-4313-1970; Cattell, Cynthia/0000-0002-3805-320X FU Leonard Burlaga/Arctowski Medal Fellowship; NASA [NAS5-02099]; German Ministry for Economy and Technology; German Center for Aviation and Space (DLR) [50 OC 0302]; [NNX08AF28]; [NNX13AE16G] FX At the University of Minnesota, this work was supported by NNX08AF28 and NNX13AE16G. X. Tang was partially supported by a Leonard Burlaga/Arctowski Medal Fellowship. The data for this paper are available at http://themis.ssl.berkeley.edu/index.shtml. The authors acknowledge NASA contract NAS5-02099 and V. Angelopoulos for the use of data from the THEMIS Mission, specifically: J. W. Bonnell and F. S. Mozer for the use of EFI data; D. Larson and R. P. Lin for the use of SST data; C. W. Carlson and J. P. McFadden for the use of ESA data; A. Roux and O. LeContel for the use of SCM data; and K. H. Glassmeier, U. Auster, and W. Baumjohann for the use of FGM data provided under the lead of the Technical University of Braunschweig and with financial support through the German Ministry for Economy and Technology and the German Center for Aviation and Space (DLR) under contract 50 OC 0302. The authors are grateful for discussion and comments from S. J. Monson, A. Breneman, and J. Dombeck. NR 48 TC 2 Z9 2 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAY PY 2015 VL 120 IS 5 BP 3380 EP 3392 DI 10.1002/2015JA020984 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM7KA UT WOS:000357869600008 ER PT J AU Collinson, GA Grebowsky, J Sibeck, DG Jian, LK Boardsen, S Espley, J Hartle, D Zhang, TLL Barabash, S Futaana, Y Kollmann, P AF Collinson, Glyn A. Grebowsky, Joseph Sibeck, David G. Jian, Lan K. Boardsen, Scott Espley, Jared Hartle, Dick Zhang, Tielong L. Barabash, Stas Futaana, Yoshifumi Kollmann, Peter TI The impact of a slow interplanetary coronal mass ejection on Venus SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ONE-HERTZ WAVES; BOW SHOCK; MAGNETIC-FIELD; SOLAR-WIND; IONOSPHERIC HOLES; EXPRESS MISSION; SPACE PLASMAS; MARS EXPRESS; UPSTREAM; NIGHTSIDE AB We present Venus Express observations of the impact of a slow interplanetary coronal mass ejection (ICME), which struck Venus on 23 December 2006, creating unusual quasi steady state upstream conditions for the 2 h close to periapsis: an enhanced (similar to 20 nT) interplanetary magnetic field (IMF), radially aligned with the Sun-Venus line; and a dense (similar to 10 cm(-3)) solar wind. Contrary to our current understanding and expectations, the ionosphere became partially demagnetized. We also find evidence for shocked sheathlike solar wind protons and electrons in the wake of Venus, and powerful (approximate to 100 nT(2)/Hz) foreshock whistler mode waves radiating from the bow shock at an unexpectedly low frequency (0.6 Hz). Given the abnormally high density of escaping heavy ions at the magnetopause boundary (295 cm(-3), one of the highest of the whole mission) and the enhanced density of escaping heavy ions in the wake, we find that even weak ICMEs with no driving shocks can increase atmospheric loss rates at Venus and suggests that the Bx component of the IMF may be a factor in atmospheric escape rates. C1 [Collinson, Glyn A.; Grebowsky, Joseph; Sibeck, David G.; Jian, Lan K.; Boardsen, Scott; Espley, Jared; Hartle, Dick] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Collinson, Glyn A.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Collinson, Glyn A.] Lab Gwyddoniaeth Gofod, Cricieth, Gwynedd, Wales. [Jian, Lan K.] Univ Maryland, College Pk, MD 20742 USA. [Boardsen, Scott] Univ Maryland Baltimore Cty, Catonsville, MD USA. [Zhang, Tielong L.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. [Barabash, Stas; Futaana, Yoshifumi] Swedish Inst Space Phys, Inst Rymdfys, S-98128 Kiruna, Sweden. [Kollmann, Peter] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Collinson, GA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM glyn.a.collinson@nasa.gov RI Jian, Lan/B-4053-2010; Kollmann, Peter/C-2583-2016; OI Jian, Lan/0000-0002-6849-5527; Kollmann, Peter/0000-0002-4274-9760; Futaana, Yoshifumi/0000-0002-7056-3517 NR 54 TC 2 Z9 2 U1 2 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAY PY 2015 VL 120 IS 5 BP 3489 EP 3502 DI 10.1002/2014JA020616 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM7KA UT WOS:000357869600016 ER PT J AU Delzanno, GL Borovsky, JE Thomsen, MF Moulton, JD MacDonald, EA AF Delzanno, G. L. Borovsky, J. E. Thomsen, M. F. Moulton, J. D. MacDonald, E. A. TI Future beam experiments in the magnetosphere with plasma contactors: How do we get the charge off the spacecraft? SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ARTIFICIAL AURORAL STREAKS; ELECTRON-BEAM; POTENTIAL CONTROL; ACTIVE SPACECRAFT; SOUNDING ROCKET; CODE; EMISSIONS; ORBIT AB The idea of using a high-voltage electron beam with substantial current to actively probe magnetic field line connectivity in space has been discussed since the 1970s. However, its experimental realization onboard a magnetospheric spacecraft has never been accomplished because the tenuous magnetospheric plasma cannot provide the return current necessary to keep spacecraft charging under control. In this work, we perform Particle-In-Cell simulations to investigate the conditions under which a high-voltage electron beam can be emitted from a spacecraft and explore solutions that can mitigate spacecraft charging. The electron beam cannot simply be compensated for by an ion beam of equal current, because the Child-Langmuir space charge limit is violated under conditions of interest. On the other hand, releasing a high-density neutral contactor plasma prior and during beam emission is critical in aiding beam emission. We show that after an initial transient controlled by the size of the contactor cloud where the spacecraft potential rises, the spacecraft potential can settle into conditions that allow for electron beam emission. A physical explanation of this result in terms of ion emission into spherical geometry from the surface of the plasma cloud is presented, together with scaling laws of the peak spacecraft potential varying the ion mass and beam current. These results suggest that a strategy where the contactor plasma and the electron beam operate simultaneously might offer a pathway to perform beam experiments in the magnetosphere. C1 [Delzanno, G. L.; Moulton, J. D.] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA. [Borovsky, J. E.] Space Sci Inst, Boulder, CO USA. [Borovsky, J. E.] Univ Michigan, AOSS, Ann Arbor, MI 48109 USA. [Thomsen, M. F.] Los Alamos Natl Lab, Intelligence & Space Res Div, Los Alamos, NM USA. [MacDonald, E. A.] Nasa Goddard, Greenbelt, MD USA. RP Delzanno, GL (reprint author), Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA. EM delzanno@lanl.gov FU Laboratory Directed Research and Development program (LDRD), U.S. Department of Energy Office of Science, Office of Fusion Energy Sciences, under National Nuclear Security Administration of the U.S. Department of Energy by Los Alamos National Laboratory [DE-AC52-06NA25396]; NASA magnetospheric GI program; NASA Geospace SRT program; NASA LWS TRT program FX The data used for this paper were obtained from numerical calculations and are available from the corresponding author upon request. The authors wish to thank Patrick Colestock and Eric Dors for useful discussions and Ira Katz and Myron Mandell for providing useful references on the SCATHA experiments. This work was funded by the Laboratory Directed Research and Development program (LDRD), U.S. Department of Energy Office of Science, Office of Fusion Energy Sciences, under the auspices of the National Nuclear Security Administration of the U.S. Department of Energy by Los Alamos National Laboratory, operated by Los Alamos National Security LLC under contract DE-AC52-06NA25396. This research used resources provided by the Los Alamos National Laboratory Institutional Computing Program. J. E. B. was funded by the NASA magnetospheric GI program, the NASA Geospace SRT program, and by the NASA LWS TRT program. NR 46 TC 2 Z9 2 U1 4 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAY PY 2015 VL 120 IS 5 BP 3647 EP 3664 DI 10.1002/2014JA020608 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM7KA UT WOS:000357869600028 ER PT J AU Kempf, Y Pokhotelov, D Gutynska, O Wilson, LB Walsh, BM von Alfthan, S Hannuksela, O Sibeck, DG Palmroth, M AF Kempf, Yann Pokhotelov, Dimitry Gutynska, Olga Wilson, Lynn B., III Walsh, Brian M. von Alfthan, Sebastian Hannuksela, Otto Sibeck, David G. Palmroth, Minna TI Ion distributions in the Earth's foreshock: Hybrid-Vlasov simulation and THEMIS observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID LOW-FREQUENCY WAVES; COLLISIONLESS BOW SHOCKS; UPSTREAM SOLAR-WIND; FIELD-ALIGNED BEAM; PERPENDICULAR COLLISIONLESS; GYRATING IONS; TERRESTRIAL FORESHOCK; ULF WAVES; MAGNETOSHEATH; MACROSTRUCTURE AB We present the ion distribution functions in the ion foreshock upstream of the terrestrial bow shock obtained with Vlasiator, a new hybrid-Vlasov simulation geared toward large-scale simulations of the Earth's magnetosphere (http://vlasiator.fmi.fi). They are compared with the distribution functions measured by the multispacecraft Time History of Events and Macroscale Interactions during Substorms (THEMIS) mission. The known types of ion distributions in the foreshock are well reproduced by the hybrid-Vlasov model. We show that Vlasiator reproduces the decrease of the backstreaming beam speed with increasing distance from the foreshock edge, as well as the beam speed increase and density decrease with increasing radial distance from the bow shock, which have been reported before and are visible in the THEMIS data presented here. We also discuss the process by which wave-particle interactions cause intermediate foreshock distributions to lose their gyrotropy. This paper demonstrates the strength of the hybrid-Vlasov approach which lies in producing uniformly sampled ion distribution functions with good resolution in velocity space, at every spatial grid point of the simulation and at any instant. The limitations of the hybrid-Vlasov approach are also discussed. C1 [Kempf, Yann; von Alfthan, Sebastian; Hannuksela, Otto; Palmroth, Minna] Finnish Meteorol Inst, Earth Observat Unit, FIN-00101 Helsinki, Finland. [Kempf, Yann; Pokhotelov, Dimitry; Hannuksela, Otto] Univ Helsinki, Dept Phys, Helsinki, Finland. [Pokhotelov, Dimitry] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Gutynska, Olga; Wilson, Lynn B., III; Sibeck, David G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Walsh, Brian M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Kempf, Y (reprint author), Finnish Meteorol Inst, Earth Observat Unit, FIN-00101 Helsinki, Finland. EM yann.kempf@fmi.fi RI Wilson III, Lynn/D-4425-2012; Pokhotelov, Dimitry/H-6969-2014; OI Wilson III, Lynn/0000-0002-4313-1970; Pokhotelov, Dimitry/0000-0002-3712-0597; Pfau-Kempf, Yann/0000-0001-5793-7070 FU European Research Council under the European Community's Seventh Framework Programme (FP-7/ERC) [200141-QuESpace]; Academy of Finland; Science and Technology Facilities Council (STFC) [ST/L000563/1] FX Y.K. acknowledges fruitful discussions with H.E.J. Koskinen and B. Lembege. We acknowledge that the results of this research have been achieved using the PRACE (Partnership for Advanced Computing in Europe) Tier-0 Research Infrastructure resource Hermit based in Germany at the High Performance Computing Center Stuttgart (HLRS) and the PRACE Tier-1 Research Infrastructure resource Abel owned by the University of Oslo and the Norwegian metacenter for High Performance Computing (NOTUR) and operated by the Department for Research Computing at USIT, the University of Oslo IT department. The Quantifying Energy circulation in Space plasmas (QuESpace) project, in which Vlasiator was initially developed, has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP-7/2007-2013/ERC) agreement 200141-QuESpace. The work of Y.K., D.P., S.A., O.H., and M.P. has been supported by the Academy of Finland. The work of D.P. has been supported by Science and Technology Facilities Council (STFC) grant ST/L000563/1. Simulation figures in this paper were made using VisIt [Childs et al., 2012]. THEMIS data are available through http://themis.ssl.berkeley.edu. Visit http://vlasiator.fmi.fi. NR 52 TC 6 Z9 6 U1 2 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAY PY 2015 VL 120 IS 5 BP 3684 EP 3701 DI 10.1002/2014JA020519 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM7KA UT WOS:000357869600030 ER PT J AU Taguchi, S Tawara, A Hairston, MR Slavin, JA Le, G Matzka, J Stolle, C AF Taguchi, S. Tawara, A. Hairston, M. R. Slavin, J. A. Le, G. Matzka, J. Stolle, C. TI Response of reverse convection to fast IMF transitions SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID INTERPLANETARY MAGNETIC-FIELD; ALIGNED CURRENT REGIONS; NORTH-SOUTH COMPONENT; IONOSPHERIC CONVECTION; ELECTRIC-FIELDS; SUDDEN CHANGES; SOLAR-WIND; POLAR; CURRENTS; TIME AB The nature of the transition that high-latitude reverse convection makes in response to fast interplanetary magnetic field (IMF) changes is investigated using observations from multiple spacecraft and a ground magnetometer array. We focused on two fast IMF-transition events on 22 April 2006. Immediately after the first event, three ST5 spacecraft identified a clear change in the distribution of the polar cap field-aligned current. Coordinate observations with the Greenland magnetometer chain showed that the near-noon Hall current distribution, which is closely related to the polar cap field-aligned current or reverse convection, was in a transition state for about 10 min. For the second event, the Greenland magnetic perturbations also showed that a transition state occurred in the near-noon sector for 10-15 min. Three DMSP spacecraft that traversed the polar cap provided evidence showing that variations of the ground magnetic perturbations were produced by the transition from clockwise plasma circulation to the anticlockwise circulation over the polar cap. A simple calculation based on the Biot-Savart law shows that the near-noon transition state is consistent with the approach of a new convection region to the near-noon sector at the speed of 0.5-1 kms(-1), which is coupled with the moving away of the old convection region at a similar speed. For the higher-latitude sunward flow region, it is found that the convection takes a transition state almost simultaneously (within 1 min) with that in the near-noon sector, i.e., quasi-instantaneous response. C1 [Taguchi, S.] Kyoto Univ, Dept Geophys, Grad Sch Sci, Kyoto, Japan. [Tawara, A.] Univ Electrocommun, Dept Commun Engn & Informat, Tokyo, Japan. [Hairston, M. R.] Univ Texas Dallas, William B Hanson Ctr Space Sci, Richardson, TX 75083 USA. [Slavin, J. A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Le, G.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Matzka, J.; Stolle, C.] Tech Univ Denmark, DTU Space, DK-2800 Lyngby, Denmark. RP Taguchi, S (reprint author), Kyoto Univ, Dept Geophys, Grad Sch Sci, Kyoto, Japan. EM taguchi@kugi.kyoto-u.ac.jp RI Le, Guan/C-9524-2012; Slavin, James/H-3170-2012; OI Le, Guan/0000-0002-9504-5214; Slavin, James/0000-0002-9206-724X; Hairston, Marc/0000-0003-4524-4837; Taguchi, Satoshi/0000-0001-7419-5531 NR 36 TC 1 Z9 1 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAY PY 2015 VL 120 IS 5 BP 4020 EP 4037 DI 10.1002/2015JA021002 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM7KA UT WOS:000357869600056 ER PT J AU Gruen, D Bernstein, GM Jarvis, M Rowe, B Vikram, V Plazas, AA Seitz, S AF Gruen, D. Bernstein, G. M. Jarvis, M. Rowe, B. Vikram, V. Plazas, A. A. Seitz, S. TI Characterization and correction of charge-induced pixel shifts in DECam SO JOURNAL OF INSTRUMENTATION LA English DT Article DE Photon detectors for UV, visible and IR photons (solid-state) (PIN diodes, APDs, Si-PMTs, G-APDs, CCDs, EBCCDs, EMCCDs etc); Image processing ID COUPLED-DEVICES; DARK; SEXTRACTOR; FIELD AB Interaction of charges in CCDs with the already accumulated charge distribution causes both a flux dependence of the point-spread function (an increase of observed size with flux, also known as the brighter/fatter effect) and pixel-to-pixel correlations of the Poissonian noise in flat fields. We describe these effects in the Dark Energy Camera (DECam) with charge dependent shifts of effective pixel borders, i.e. the Antilogus et al. (2014) model, which we fit to measurements of flat-field Poissonian noise correlations. The latter fall off approximately as a power-law r(-2.5) with pixel separation r, are isotropic except for an asymmetry in the direct neighbors along rows and columns, are stable in time, and are weakly dependent on wavelength. They show variations from chip to chip at the 20% level that correlate with the silicon resistivity. The charge shifts predicted by the model cause biased shape measurements, primarily due to their effect on bright stars, at levels exceeding weak lensing science requirements. We measure the flux dependence of star images and show that the effect can be mitigated by applying the reverse charge shifts at the pixel level during image processing. Differences in stellar size, however, remain significant due to residuals at larger distance from the centroid. C1 [Gruen, D.; Seitz, S.] Univ Observ Munich, D-81679 Munich, Germany. [Gruen, D.; Seitz, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Bernstein, G. M.; Jarvis, M.; Vikram, V.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Rowe, B.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Vikram, V.] Argonne Natl Lab, Lemont, IL 60439 USA. [Plazas, A. A.] Brookhaven Natl Lab, Upton, NY 11973 USA. [Plazas, A. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gruen, D (reprint author), Univ Observ Munich, Scheinerstr 1, D-81679 Munich, Germany. EM dgruen@usm.uni-muenchen.de OI Rowe, Barnaby/0000-0002-7042-9174 FU Deutsche Forschungsgemeinschaft (DFG) [SFB-Transregio 33]; DFG cluster of excellence 'Origin and Structure of the Universe' [DE-SC007901]; NSF [AST-1311924]; DOE [DE-AC02-98CH10886]; JPL; NASA by Caltech; 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; 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; 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; associated Excellence Cluster Universe; University of Michigan; National Optical Astronomy Observatory; University of Nottingham; Ohio State University; University of Pennsylvania; University of Portsmouth; SLAC National Accelerator Laboratory, Stanford University; University of Sussex; Texas AM University FX This project was supported by SFB-Transregio 33 'The Dark Universe' by the Deutsche Forschungsgemeinschaft (DFG) and the DFG cluster of excellence 'Origin and Structure of the Universe'. DG thanks Pierre Astier, Thomas Diehl, Augustin Guyonnet, Stephen Holland, Mihael Kodric, Ralf Kosyra, and Andy Rasmussen for helpful discussions. GMB acknowledges support for this work from NSF grant AST-1311924 and DOE grant DE-SC007901. AAP is supported by DOE grant DE-AC02-98CH10886 and JPL, which is run under a contract for NASA by Caltech.; 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, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia e Tecnologia, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey.; The 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 31 TC 7 Z9 7 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 MAY PY 2015 VL 10 AR C05032 DI 10.1088/1748-0221/10/05/C05032 PG 22 WC Instruments & Instrumentation SC Instruments & Instrumentation GA CM8ZI UT WOS:000357993300032 ER PT J AU Varnai, T Marshak, A AF Varnai, Tamas Marshak, Alexander TI Effect of Cloud Fraction on Near-Cloud Aerosol Behavior in the MODIS Atmospheric Correction Ocean Color Product SO REMOTE SENSING LA English DT Article ID CALIPSO OBSERVATIONS; PARTICLES; VICINITY; CERES; MODEL; AQUA; AIR AB Characterizing the way satellite-based aerosol statistics change near clouds is important for better understanding both aerosol-cloud interactions and aerosol direct radiative forcing. This study focuses on the question of whether the observed near-cloud increases in aerosol optical thickness and particle size may be explained by a combination of two factors: (i) Near-cloud data coming from areas with higher cloud fractions than far-from-cloud data and (ii) Cloud fraction being correlated with aerosol optical thickness and particle size. This question is addressed through a statistical analysis of aerosol parameters included in the MODIS (MODerate resolution Imaging Spectroradiometer) ocean color product. Results from ten Septembers (2002-2011) over part of the northeast Atlantic Ocean confirm that the combination of these two factors working together explains a significant but not dominant part (in our case, 15%-30%) of mean optical thickness changes near clouds. Overall, the findings show that cloud fraction plays a large role in shaping the way aerosol statistics change with distance to clouds. This implies that both cloud fraction and distance to clouds are important to consider when aerosol-cloud interactions or aerosol direct radiative effects are examined in satellite or modeling studies. C1 [Varnai, Tamas] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. [Varnai, Tamas; Marshak, Alexander] NASA Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD 20771 USA. RP Varnai, T (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, 1000 Hilltop Circle, Baltimore, MD 21250 USA. EM varnai@umbc.edu; alexander.marshak@nasa.gov RI Marshak, Alexander/D-5671-2012 FU NASA Radiation Sciences Program; NASA CALIPSO project FX We gratefully acknowledge support for this research by the NASA Radiation Sciences Program managed by Hal Maring and by the NASA CALIPSO project supervised by Charles Trepte as the technical officer. We also thank Ziauddin Ahmad, Bryan Franz, Gerhard Meister, and other members of the MODIS ocean color team, as well as Bob Charlson, Larry Di Girolamo, Robert Levy, Alexei Lyapustin, Guoyong Wen, Rob Wood, and Weidong Yang for insightful discussions and help. We are also grateful to the three anonymous reviewers, who helped greatly to improve the manuscript. NR 34 TC 3 Z9 4 U1 0 U2 3 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD MAY PY 2015 VL 7 IS 5 BP 5283 EP 5299 DI 10.3390/rs70505283 PG 17 WC Remote Sensing SC Remote Sensing GA CM3PW UT WOS:000357596200015 ER PT J AU Chapman, B McDonald, K Shimada, M Rosenqvist, A Schroeder, R Hess, L AF Chapman, Bruce McDonald, Kyle Shimada, Masanobu Rosenqvist, Ake Schroeder, Ronny Hess, Laura TI Mapping Regional Inundation with Spaceborne L-Band SAR SO REMOTE SENSING LA English DT Article ID SYNTHETIC-APERTURE RADAR; SOUTH FLORIDA WETLANDS; AMAZON FLOODPLAIN; SLOPE CORRECTION; WATER STORAGE; ALOS PALSAR; VEGETATION; DYNAMICS; IMAGES; BASIN AB Shortly after the launch of ALOS PALSAR L-band SAR by the Japan Space Exploration Agency (JAXA), a program to develop an Earth Science Data Record (ESDR) for inundated wetlands was funded by NASA. Using established methodologies, extensive multi-temporal L-band ALOS ScanSAR data acquired bi-monthly by the PALSAR instrument onboard ALOS were used to classify the inundation state for South America for delivery as a component of this Inundated Wetlands ESDR (IW-ESDR) and in collaboration with JAXA's ALOS Kyoto and Carbon Initiative science programme. We describe these methodologies and the final classification of the inundation state, then compared this with results derived from dual-season data acquired by the JERS-1 L-band SAR mission in 1995 and 1996, as well as with estimates of surface water extent measured globally every 10 days by coarser resolution sensors. Good correspondence was found when comparing open water extent classified from multi-temporal ALOS ScanSAR data with surface water fraction identified from coarse resolution sensors, except in those regions where there may be differences in sensitivity to widespread and shallow seasonal flooding event, or in areas that could be excluded through use of a continental-scale inundatable mask. It was found that the ALOS ScanSAR classification of inundated vegetation was relatively insensitive to inundated herbaceous vegetation. Inundation dynamics were examined using the multi-temporal ALOS ScanSAR acquisitions over the Pacaya-Samiria and surrounding areas in the Peruvian Amazon. C1 [Chapman, Bruce; McDonald, Kyle; Schroeder, Ronny] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [McDonald, Kyle] CUNY City Coll, CUNY Environm Crossrd Initiat, New York, NY 10031 USA. [McDonald, Kyle] CUNY City Coll, CREST Inst, New York, NY 10031 USA. [Shimada, Masanobu] Japan Aerosp & Explorat Agcy, Earth Observat Res Ctr, Tsukuba, Ibaraki 3058505, Japan. [Rosenqvist, Ake] SoloEO, Tokyo 3058505, Japan. [Schroeder, Ronny] Univ Hohenheim, Inst Bot, D-70593 Stuttgart, Germany. [Hess, Laura] Univ Calif Santa Barbara, Earth Res Inst, Santa Barbara, CA 93106 USA. RP Chapman, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM bruce.d.chapman@jpl.nasa.gov; kmcdonald2@ccny.cuny.edu; shimada.masanobu@jaxa.jp; ake.rosenqvist@soloEO.com; ronny.schroder@gmail.com; lola@eri.ucsb.edu FU NASA MEaSUREs program; National Aeronautics and Space Administration FX We thank the NASA MEaSUREs program and Martha Maiden for funding this work, the NASDA/JAXA GRFM project for the JERS-1 imagery, the Alaska Satellite Facility ALOS Data node for ancillary ALOS data, the global classification from ESA's GlobClover land cover classification product, and the NASA SRTM project for its near global DEM. This research was undertaken within the framework of the ALOS Kyoto & Carbon Initiative. The ALOS data were provided by JAXA EORC. 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. We also thank the editor and the reviewers for their advice and suggestions for the improvement of this paper.; This work was partially performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. U.S. Government sponsorship acknowledged. NR 41 TC 5 Z9 5 U1 5 U2 18 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 MAY PY 2015 VL 7 IS 5 BP 5440 EP 5470 DI 10.3390/rs70505440 PG 31 WC Remote Sensing SC Remote Sensing GA CM3PW UT WOS:000357596200022 ER PT J AU Ibrahim, YZ Balzter, H Kaduk, J Tucker, CJ AF Ibrahim, Yahaya Z. Balzter, Heiko Kaduk, Joerg Tucker, Compton J. TI Land Degradation Assessment Using Residual Trend Analysis of GIMMS NDVI3g, Soil Moisture and Rainfall in Sub-Saharan West Africa from 1982 to 2012 SO REMOTE SENSING LA English DT Article ID DIFFERENCE VEGETATION INDEX; TIME-SERIES; SOUTH-AFRICA; EAST-AFRICA; NOAA-AVHRR; SAHEL; DESERTIFICATION; CLIMATE; PRODUCTS; VARIABILITY AB Areas affected by land degradation in Sub-Saharan West Africa between 1982 and 2012 are identified using time-series analysis of vegetation index data derived from satellites. The residual trend (RESTREND) of a Normalized Difference Vegetation Index (NDVI) time-series is defined as the fraction of the difference between the observed NDVI and the NDVI predicted from climate data. It has been widely used to study desertification and other forms of land degradation in drylands. The method works on the assumption that a negative trend of vegetation photosynthetic capacity is an indication of land degradation if it is independent from climate variability. In the past, many scientists depended on rainfall data as the major climatic factor controlling vegetation productivity in drylands when applying the RESTREND method. However, the water that is directly available to vegetation is stored as soil moisture, which is a function of cumulative rainfall, surface runoff, infiltration and evapotranspiration. In this study, the new NDVI third generation (NDVI3g), which was generated by the National Aeronautics and Space Administration-Goddard Space Flight Center Global Inventory Modeling and Mapping Studies (NASA-GSFC GIMMS) group, was used as a satellite-derived proxy of vegetation productivity, together with the soil moisture index product from the Climate Prediction Center (CPC) and rainfall data from the Climate Research Unit (CRU). The results show that the soil moisture/NDVI pixel-wise residual trend indicates land degraded areas more clearly than rainfall/NDVI. The spatial and temporal trends of the RESTREND in the region follow the patterns of drought episodes, reaffirming the difficulties in separating the impacts of drought and land degradation on vegetation photosynthetic capacity. Therefore, future studies of land degradation and desertification in drylands should go beyond using rainfall as a sole predictor of vegetation condition, and include soil moisture index datasets in the analysis. C1 [Ibrahim, Yahaya Z.; Balzter, Heiko; Kaduk, Joerg] Univ Leicester, Ctr Landscape & Climate Res, Dept Geog, Leicester LE1 7RH, Leics, England. [Tucker, Compton J.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ibrahim, YZ (reprint author), Univ Leicester, Ctr Landscape & Climate Res, Dept Geog, Leicester LE1 7RH, Leics, England. EM yzii1@le.ac.uk; hb91@le.ac.uk; jk61@le.ac.uk; compton.j.tucker@nasa.gov OI Kaduk, Jorg/0000-0003-4051-3081 FU Royal Society, Wolfson Research Merit Award FX The authors are grateful and wish to acknowledge the use of the new NDVI3g provided by Jim Tucker and Jorge E. Pinzon of NASA. Special thanks to CRU for providing the CRU v3.21 rainfall data and NOAA-NCEP for CPC soil moisture (v2) data. Finally to R development team for making various library packages available which were used for the data analyses. H. Balzter was supported by the Royal Society, Wolfson Research Merit Award. NR 72 TC 13 Z9 13 U1 6 U2 37 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD MAY PY 2015 VL 7 IS 5 BP 5471 EP 5494 DI 10.3390/rs70505471 PG 24 WC Remote Sensing SC Remote Sensing GA CM3PW UT WOS:000357596200023 ER PT J AU Fagan, ME DeFries, RS Sesnie, SE Arroyo-Mora, JP Soto, C Singh, A Townsend, PA Chazdon, RL AF Fagan, Matthew E. DeFries, Ruth S. Sesnie, Steven E. Arroyo-Mora, J. Pablo Soto, Carlomagno Singh, Aditya Townsend, Philip A. Chazdon, Robin L. TI Mapping Species Composition of Forests and Tree Plantations in Northeastern Costa Rica with an Integration of Hyperspectral and Multitemporal Landsat Imagery SO REMOTE SENSING LA English DT Article ID MAP ACCURACY ASSESSMENT; OIL PALM; IMAGING SPECTROSCOPY; SATELLITE IMAGERY; RAIN-FORESTS; COVER CHANGE; TIME-SERIES; ETM PLUS; RADIOMETRIC NORMALIZATION; DISCRIMINANT-ANALYSIS AB An efficient means to map tree plantations is needed to detect tropical land use change and evaluate reforestation projects. To analyze recent tree plantation expansion in northeastern Costa Rica, we examined the potential of combining moderate-resolution hyperspectral imagery (2005 HyMap mosaic) with multitemporal, multispectral data (Landsat) to accurately classify (1) general forest types and (2) tree plantations by species composition. Following a linear discriminant analysis to reduce data dimensionality, we compared four Random Forest classification models: hyperspectral data (HD) alone; HD plus interannual spectral metrics; HD plus a multitemporal forest regrowth classification; and all three models combined. The fourth, combined model achieved overall accuracy of 88.5%. Adding multitemporal data significantly improved classification accuracy (p < 0.0001) of all forest types, although the effect on tree plantation accuracy was modest. The hyperspectral data alone classified six species of tree plantations with 75% to 93% producer's accuracy; adding multitemporal spectral data increased accuracy only for two species with dense canopies. Non-native tree species had higher classification accuracy overall and made up the majority of tree plantations in this landscape. Our results indicate that combining occasionally acquired hyperspectral data with widely available multitemporal satellite imagery enhances mapping and monitoring of reforestation in tropical landscapes. C1 [Fagan, Matthew E.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [DeFries, Ruth S.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. [Sesnie, Steven E.] US Fish & Wildlife Serv, Southwest Reg Off, Albuquerque, NM 87102 USA. [Arroyo-Mora, J. Pablo; Soto, Carlomagno] McGill Univ, Dept Geog, Montreal, PQ H3A 2K6, Canada. [Singh, Aditya; Townsend, Philip A.] Univ Wisconsin, Dept Forest & Wildlife Ecol, Madison, WI 53706 USA. [Chazdon, Robin L.] Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA. RP Fagan, ME (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. EM matthew.e.fagan@nasa.gov; rd2402@columbia.edu; Steven_Sesnie@fws.gov; pablo.arroyo@mcgill.ca; carlo.soto.castro@gmail.com; singh22@wisc.edu; ptownsend@wisc.edu; robin.chazdon@uconn.edu RI Singh, Aditya/I-3628-2013; Townsend, Philip/B-5741-2008; OI Singh, Aditya/0000-0001-5559-9151; Townsend, Philip/0000-0001-7003-8774; Chazdon, Robin/0000-0002-7349-5687 FU National Aeronautics and Space Administration Earth System Science Fellowship [NNX10AP49H]; ASPRS Ta Liang Memorial Award; Earth Institute; Columbia Institute of Latin American Studies; NASA FX This work was supported by National Aeronautics and Space Administration Earth System Science Fellowship NNX10AP49H, the ASPRS Ta Liang Memorial Award, The Earth Institute, the Columbia Institute of Latin American Studies, and by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. The authors would like to thank Margaret Kalacska for an insightful and helpful early review of this manuscript, and to thank Chris Small for countless hours of great remote sensing advice in small restaurants. Field research was made possible by logistical support provided by FUNDECOR and the staff at the Organization for Tropical Studies La Selva Biological Station, and we would like to thank Andres Sanchun, Jose Miranda, Marvin Paniagua, and Mauricio Gaitan for assistance in the field. We thank CENAT and Carlos Andres Campos for providing geospatial data on Costa Rica and would like to express our appreciation to Bonnie Tice and Sue Pirkle. Finally, the authors wish to thank the three anonymous reviewers for their insightful comments, which led to marked improvements in the original manuscript. NR 136 TC 9 Z9 9 U1 7 U2 29 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD MAY PY 2015 VL 7 IS 5 BP 5660 EP 5696 DI 10.3390/rs70505660 PG 37 WC Remote Sensing SC Remote Sensing GA CM3PW UT WOS:000357596200031 ER PT J AU Ting, DZY Chang, YC Rafol, SB Liu, JK Hill, CJ Keo, SA Mumolo, J Gunapala, SD Bandara, SV AF Ting, David Z. -Y. Chang, Yia-Chung Rafol, Sir B. Liu, John K. Hill, Cory J. Keo, Sam A. Mumolo, Jason Gunapala, Sarath D. Bandara, Sumith V. TI The sub-monolayer quantum dot infrared photodetector revisited SO INFRARED PHYSICS & TECHNOLOGY LA English DT Article; Proceedings Paper CT 8th International Workshop on Quantum Structure Infrared Photodetectors (QSIP) CY JUN 29-JUL 03, 2014 CL Santa Fe, NM SP Univ New Mexico, Georgia State Univ, NASA Jet Propuls Lab, AF Res Lab, Army Res Off DE Infrared detector; Quantum dot; Submonolayer ID ISLANDS; ARRAYS; WELL AB The sub-monolayer quantum dot infrared photodetector (SML-QDIP) was proposed as an alternative to the standard QDIP based on Stranski-Krastanow (SK) quantum dots. Theoretical modeling indicates that the normal-incidence photo-response observed in the initial SML-QDIP devices, originally attributed to 3D quantum confinement effect, is most likely the result of optical cavity scattering. Modeling results also suggest candidate SML-QDIP structures with improved intrinsic normal incidence absorption. (C) 2014 Elsevier B.V. All rights reserved. C1 [Ting, David Z. -Y.; Rafol, Sir B.; Liu, John K.; Hill, Cory J.; Keo, Sam A.; Mumolo, Jason; Gunapala, Sarath D.; Bandara, Sumith V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chang, Yia-Chung] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. RP Ting, DZY (reprint author), CALTECH, Jet Prop Lab, M-S 302-307,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM David.Z.Ting@jpl.nasa.gov NR 25 TC 0 Z9 0 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1350-4495 EI 1879-0275 J9 INFRARED PHYS TECHN JI Infrared Phys. Technol. PD MAY PY 2015 VL 70 BP 20 EP 24 DI 10.1016/j.infrared.2014.09.028 PG 5 WC Instruments & Instrumentation; Optics; Physics, Applied SC Instruments & Instrumentation; Optics; Physics GA CL8OM UT WOS:000357234000005 ER PT J AU Sun, J Choi, KK Jhabvala, MD Jhabvala, CA Waczynski, A Olver, K AF Sun, J. Choi, K. K. Jhabvala, M. D. Jhabvala, C. A. Waczynski, A. Olver, K. TI Advanced inductively coupled plasma etching processes for fabrication of resonator-quantum well infrared photodetector SO INFRARED PHYSICS & TECHNOLOGY LA English DT Article; Proceedings Paper CT 8th International Workshop on Quantum Structure Infrared Photodetectors (QSIP) CY JUN 29-JUL 03, 2014 CL Santa Fe, NM SP Univ New Mexico, Georgia State Univ, NASA Jet Propuls Lab, AF Res Lab, Army Res Off DE Inductively coupled plasma etching; Resonator-quantum well infrared; photodetectors focal plane array; GaAs substrate removal ID DAMAGE; GAAS; SICL4; TIME; INP AB Resonator-quantum well infrared photodetectors (R-QWIPs) are the next generation of QWIP detectors that use resonances to increase the quantum efficiency (QE). To achieve the expected performance, the detector geometry must be produced in precise specification. In particular, the height of the diffractive elements (DE) and the thickness of the active resonator must be uniformly and accurately realized to within 0.05 mu m accuracy and the substrates of the detectors have to be removed totally. To achieve these specifications, two optimized inductively coupled plasma (ICP) etching processes are developed. Using these etching techniques, we have fabricated a number of R-QWIP test detectors and FPAs with the required dimensions and completely removed the substrates of the test detectors and FPAs. Their QE spectra were tested to be in close agreement with the theoretical predictions. The operability and spectral non-uniformity of the FPA is about 99.57% and 3% respectively. Published by Elsevier B.V. C1 [Sun, J.] US Army, Res Lab, Adelphi, MD 20783 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sun, J (reprint author), US Army, Res Lab, Adelphi, MD 20783 USA. NR 14 TC 3 Z9 3 U1 4 U2 11 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1350-4495 EI 1879-0275 J9 INFRARED PHYS TECHN JI Infrared Phys. Technol. PD MAY PY 2015 VL 70 BP 25 EP 29 DI 10.1016/j.infrared.2014.09.022 PG 5 WC Instruments & Instrumentation; Optics; Physics, Applied SC Instruments & Instrumentation; Optics; Physics GA CL8OM UT WOS:000357234000006 ER PT J AU Baril, N Bandara, S Hoeglund, L Henry, N Brown, A Billman, C Maloney, P Nallon, E Tidrow, M Pellegrino, J AF Baril, Neil Bandara, Sumith Hoeglund, Linda Henry, Nathan Brown, Alexander Billman, Curtis Maloney, Patrick Nallon, Eric Tidrow, Meimei Pellegrino, Joseph TI Low operating bias InAs/GaSb strain layer superlattice LWIR detector SO INFRARED PHYSICS & TECHNOLOGY LA English DT Article; Proceedings Paper CT 8th International Workshop on Quantum Structure Infrared Photodetectors (QSIP) CY JUN 29-JUL 03, 2014 CL Santa Fe, NM SP Univ New Mexico, Georgia State Univ, NASA Jet Propuls Lab, AF Res Lab, Army Res Off DE Superlattice; Infrared detector; Heterojunction; Band offset; InAs/GaSb; Barrier AB Minimization of operating bias and generation-recombination dark current in long wavelength infrared (LWIR) strained layer superlattice (SLS) detectors, consisting of a lightly doped p-type absorber layer and a wide band gap hole barrier, are investigated with respect to the band alignment between the wide band gap barrier and absorber layers. Dark current vs. bias, photoresponse, quantum efficiency, lifetime, and modeling are used to correlate device performance with the wide gap barrier composition. Decreases in dark current density and operating bias were observed as the conduction band of the wide gap barrier was lowered with respect to the absorber layer. The device achieved 95% of its maximum quantum efficiency at 0 V bias, and 100% by 0.05 V. This study demonstrates key device design parameters responsible for optimal performance of heterojunction based SLS LWIR detectors. Published by Elsevier B.V. C1 [Baril, Neil; Bandara, Sumith; Billman, Curtis; Maloney, Patrick; Nallon, Eric; Tidrow, Meimei; Pellegrino, Joseph] US Army RDECOM CERDEC NVESD, Ft Belvoir, VA 22060 USA. [Hoeglund, Linda] Corbin Co, Alexandria, VA 22314 USA. [Henry, Nathan; Brown, Alexander] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Baril, N (reprint author), 10221 Burbeck Rd, Ft Belvoir, VA 22060 USA. EM info@nvl.army.mil NR 8 TC 2 Z9 2 U1 5 U2 19 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1350-4495 EI 1879-0275 J9 INFRARED PHYS TECHN JI Infrared Phys. Technol. PD MAY PY 2015 VL 70 BP 58 EP 61 DI 10.1016/j.infrared.2014.10.013 PG 4 WC Instruments & Instrumentation; Optics; Physics, Applied SC Instruments & Instrumentation; Optics; Physics GA CL8OM UT WOS:000357234000013 ER PT J AU Hoglund, L Ting, DZ Soibel, A Fisher, A Khoshakhlagh, A Hill, CJ Baker, L Keo, S Mumolo, J Gunapala, SD AF Hoeglund, L. Ting, D. Z. Soibel, A. Fisher, A. Khoshakhlagh, A. Hill, C. J. Baker, L. Keo, S. Mumolo, J. Gunapala, S. D. TI Influence of carrier concentration on the minority carrier lifetime in mid-wavelength infrared InAs/InAsSb superlattices SO INFRARED PHYSICS & TECHNOLOGY LA English DT Article; Proceedings Paper CT 8th International Workshop on Quantum Structure Infrared Photodetectors (QSIP) CY JUN 29-JUL 03, 2014 CL Santa Fe, NM SP Univ New Mexico, Georgia State Univ, NASA Jet Propuls Lab, AF Res Lab, Army Res Off DE Infrared; Superlattice; InAs/InAsSb; Minority carrier lifetime; Capacitance-voltage ID DETECTORS AB The influence of carrier concentration on the minority carrier lifetime was studied in mid-wavelength infrared InAs/InAsSb superlattices. A significant correlation between the carrier concentration and the minority carrier lifetime was observed, with lifetime decreasing from 3.6 mu s to 1 mu s when increasing the carrier concentration from 2 x 10(15) cm(-3) to 4.4 x 10(15) cm(-3). From temperature dependence studies of the minority carrier lifetime, radiative recombination has been identified as the main recombination mechanism in these superlattices. The radiative recombination rate increases with carrier concentration which is consistent with our observations. (C) 2014 Elsevier B.V. All rights reserved. C1 [Hoeglund, L.; Ting, D. Z.; Soibel, A.; Fisher, A.; Khoshakhlagh, A.; Hill, C. J.; Baker, L.; Keo, S.; Mumolo, J.; Gunapala, S. D.] CALTECH, Jet Prop Lab, Ctr Infrared Photodetectors, Pasadena, CA 91109 USA. RP Hoglund, L (reprint author), CALTECH, Jet Prop Lab, Ctr Infrared Photodetectors, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 12 TC 3 Z9 3 U1 2 U2 18 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1350-4495 EI 1879-0275 J9 INFRARED PHYS TECHN JI Infrared Phys. Technol. PD MAY PY 2015 VL 70 BP 62 EP 65 DI 10.1016/j.infrared.2014.10.011 PG 4 WC Instruments & Instrumentation; Optics; Physics, Applied SC Instruments & Instrumentation; Optics; Physics GA CL8OM UT WOS:000357234000014 ER PT J AU Gunapala, SD Rafol, SB Ting, DZ Soibel, A Hoglund, L Hill, CJ Khoshakhlagh, A Liu, JK Mumolo, JM Keo, SA AF Gunapala, S. D. Rafol, S. B. Ting, D. Z. Soibel, A. Hoeglund, L. Hill, C. J. Khoshakhlagh, A. Liu, J. K. Mumolo, J. M. Keo, S. A. TI 1/f Noise QWIPs and nBn detectors SO INFRARED PHYSICS & TECHNOLOGY LA English DT Article; Proceedings Paper CT 8th International Workshop on Quantum Structure Infrared Photodetectors (QSIP) CY JUN 29-JUL 03, 2014 CL Santa Fe, NM SP Univ New Mexico, Georgia State Univ, NASA Jet Propuls Lab, AF Res Lab, Army Res Off DE Infrared detector; QWIP; nBn; Focal plane array; 1/f Noise ID WELL INFRARED PHOTODETECTORS AB The low-frequency noise is a ubiquitous phenomenon and the spectral power density of this fluctuation process is inversely proportional to the frequency of the signal. We have measured the 1/f noise of a 640 x 512 pixel quantum well infrared photodetector (QWIP) focal plane array (FPA) with 6.2 mu m peak wavelength. Our experimental observations show that this QWIP FPA's 1/f noise corner frequency is about 0.1 mHz. With this kind of low frequency stability, QWIPs could unveil a new class of infrared applications that have never been imagined before. Furthermore, we present the results from a similar 1/f noise measurement of bulk InAsSb absorber (lattice matched to GaSb substrate) nBn detector array with 4.0 mu m cutoff wavelength. (C) 2014 Elsevier B.V. All rights reserved. C1 [Gunapala, S. D.; Rafol, S. B.; Ting, D. Z.; Soibel, A.; Hoeglund, L.; Hill, C. J.; Khoshakhlagh, A.; Liu, J. K.; Mumolo, J. M.; Keo, S. A.] CALTECH, Jet Prop Lab, Ctr Infrared Photodetectors, Pasadena, CA 91109 USA. RP Gunapala, SD (reprint author), Jet Prop Lab, M-S 302-306,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Sarath.d.Gunapala@jpl.nasa.gov NR 20 TC 0 Z9 0 U1 3 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1350-4495 EI 1879-0275 J9 INFRARED PHYS TECHN JI Infrared Phys. Technol. PD MAY PY 2015 VL 70 BP 115 EP 120 DI 10.1016/j.infrared.2014.09.031 PG 6 WC Instruments & Instrumentation; Optics; Physics, Applied SC Instruments & Instrumentation; Optics; Physics GA CL8OM UT WOS:000357234000025 ER PT J AU Soibel, A Hill, CJ Keo, SA Hoglund, L Rosenberg, R Kowalczyk, R Khoshakhlagh, A Fisher, A Ting, DZY Gunapala, SD AF Soibel, Alexander Hill, Cory J. Keo, Sam A. Hoglund, Linda Rosenberg, Robert Kowalczyk, Robert Khoshakhlagh, Arezou Fisher, Anita Ting, David Z. -Y. Gunapala, Sarath D. TI Room temperature performance of mid-wavelength infrared InAsSb nBn detectors SO INFRARED PHYSICS & TECHNOLOGY LA English DT Article; Proceedings Paper CT 8th International Workshop on Quantum Structure Infrared Photodetectors (QSIP) CY JUN 29-JUL 03, 2014 CL Santa Fe, NM SP Univ New Mexico, Georgia State Univ, NASA Jet Propuls Lab, AF Res Lab, Army Res Off DE Infrared detectors; Semiconductor detectors; BIRD detectors; Sb-based detectors ID PHOTODETECTORS; DESIGN AB In this work we investigate the high temperature performance of mid-wavelength infrared InAsSb-AlAsSb nBn detectors with cut-off wavelengths near 4.5 mu m. The quantum efficiency of these devices is 35% without antireflection coatings and does not change with temperature in the 77-325 K temperature range, indicating potential for room temperature operation. The device dark current stays diffusion limited in the 150-325 K temperature range and becomes dominated by generation-recombination processes at lower temperatures. Detector detectivities of D*(lambda) = 1 x 10(9) (cm Hz(0.5)/W) at T= 300 K and D*(lambda)= 5 x 10(9) (cm Hz(0.5)/W) at T= 250 K, which is easily achievable with a one stage TE cooler. (C) 2014 Elsevier B.V. All rights reserved. C1 [Soibel, Alexander; Hill, Cory J.; Keo, Sam A.; Hoglund, Linda; Rosenberg, Robert; Kowalczyk, Robert; Khoshakhlagh, Arezou; Fisher, Anita; Ting, David Z. -Y.; Gunapala, Sarath D.] CALTECH, Jet Prop Lab, Pasadena, CA 91030 USA. RP Soibel, A (reprint author), JPL, 4800 Oak Grove Dr,M-S 302-205, Pasadena, CA 91109 USA. NR 16 TC 1 Z9 1 U1 5 U2 15 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1350-4495 EI 1879-0275 J9 INFRARED PHYS TECHN JI Infrared Phys. Technol. PD MAY PY 2015 VL 70 BP 121 EP 124 DI 10.1016/j.infrared.2014.09.030 PG 4 WC Instruments & Instrumentation; Optics; Physics, Applied SC Instruments & Instrumentation; Optics; Physics GA CL8OM UT WOS:000357234000026 ER PT J AU De Groeve, T Thielen-del Pozo, J Brakenridge, R Adler, R Alfieri, L Kull, D Lindsay, F Imperiali, O Pappenberger, F Rudari, R Salamon, P Villars, N Wyjad, K AF De Groeve, T. Thielen-del Pozo, J. Brakenridge, R. Adler, R. Alfieri, L. Kull, D. Lindsay, F. Imperiali, O. Pappenberger, F. Rudari, R. Salamon, P. Villars, N. Wyjad, K. TI JOINING FORCES IN A GLOBAL FLOOD PARTNERSHIP SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article C1 [De Groeve, T.; Thielen-del Pozo, J.; Alfieri, L.; Salamon, P.] Commiss European Communities, JRC, I-21027 Ispra, VA, Italy. [Brakenridge, R.] Dartmouth Flood Observ, Boulder, CO USA. [Adler, R.] Univ Maryland, College Pk, MD 20742 USA. [Alfieri, L.; Pappenberger, F.] European Ctr Medium Range Weather Forecasts, Forecast Dept, Reading RG2 9AX, Berks, England. [Kull, D.] World Bank Grp, Global Facil Disaster Reduct & Recovery, Geneva, Switzerland. [Lindsay, F.] NASA, Washington, DC 20546 USA. [Imperiali, O.] Commiss European Communities, European Community Humanitarian Off, B-1049 Brussels, Belgium. [Pappenberger, F.] Hohai Univ, Coll Hydrol & Water Resources, Nanjing, Jiangsu, Peoples R China. [Pappenberger, F.] Univ Bristol, Dept Geog, Bristol BS8 1TH, Avon, England. [Rudari, R.] CIMA Res Fdn, Savona, Italy. [Villars, N.] Deltares, Delft, Netherlands. [Wyjad, K.] United Nations World Food Programme, Rome, Italy. RP Thielen-del Pozo, J (reprint author), Commiss European Communities, JRC, Via E Fermi 2479,TP122, I-21027 Ispra, VA, Italy. RI Pappenberger, Florian/A-2839-2009; OI Pappenberger, Florian/0000-0003-1766-2898; Alfieri, Lorenzo/0000-0002-3616-386X NR 3 TC 4 Z9 4 U1 3 U2 5 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD MAY PY 2015 VL 96 IS 5 BP ES97 EP ES100 DI 10.1175/BAMS-D-14-00147.1 PG 4 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CL3SL UT WOS:000356870800001 ER PT J AU Flexas, MM Schodlok, MP Padman, L Menemenlis, D Orsi, AH AF Flexas, M. M. Schodlok, M. P. Padman, L. Menemenlis, D. Orsi, A. H. TI Role of tides on the formation of the Antarctic Slope Front at the Weddell-Scotia Confluence SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article; Proceedings Paper CT Open Science Symposium on Western Pacific Ocean Circulation and Climate CY OCT 15-17, 2012 CL Qingdao, PEOPLES R CHINA SP NW Pacific Ocean Circulat & Climate Expt DE Antarctic Slope Front; Antarctic Slope Current; tides; Scotia sea; numerical model; SASSI ID SEA CONTINENTAL-SLOPE; BOTTOM WATER PRODUCTION; ROSS SEA; OVERTURNING CIRCULATION; SOUTHERN-OCEAN; YERMAK PLATEAU; DIURNAL TIDES; SHELF BREAK; DEEP-OCEAN; MODEL AB The structure of the Antarctic Slope Front (ASF) and the associated Antarctic Slope Current (ASC) on the Scotia Sea side of the Weddell-Scotia Confluence (WSC) is described using data from a hydrographic survey and three 1 year long moorings across the continental slope. The ASC in this region flows westward along isobaths with an annual mean speed of approximate to 0.2 m s(-1), with time variability dominated by the K-1 and O-1 tidal diurnal constituents, a narrowband oscillation with approximate to 2-week period attributable to the spring/neap tidal cycle, and seasonal variability. Realistic and idealized high-resolution numerical simulations are used to determine the contribution of tides to the structure of the ASF and the speed of the ASC. Two simulations forced by realistic atmospheric forcing and boundary conditions integrated with and without tidal forcing show that tidal forcing is essential to reproduce the measured ASF/ASC cross-slope structure, the time variability at our moorings, and the reduced stratification within the WSC. Two idealized simulations run with tide-only forcing, one with a homogeneous ocean and the other with initial vertical stratification that is laterally homogeneous, show that tides can generate the ASC and ASF through volume flux convergence along the slope initiated by effects including the Lagrangian component of tidal rectification and mixing at the seabed and in the stratified ocean interior. Climate models that exclude the effects of tides will not correctly represent the ASF and ASC or their influence on the injection of intermediate and dense waters from the WSC to the deep ocean. C1 [Flexas, M. M.; Schodlok, M. P.; Menemenlis, D.] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91125 USA. [Flexas, M. M.] UIB CSIC, IMEDEA, Palma De Mallorca, Spain. [Schodlok, M. P.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. [Padman, L.] Earth & Space Res, Corvallis, OR USA. [Orsi, A. H.] Texas A&M Univ, Dept Oceanog, College Stn, TX 77843 USA. RP Flexas, MM (reprint author), CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91125 USA. EM msbert@jpl.nasa.gov FU Spanish Research and Innovation (I+D+i) National Plan [CGL2007-28783-E/ ANT, CTM2008-04623-E/ANT, CTM2009-08287-E/ANT, CTM2011-14056-E]; National Science Foundation [ANT-0818061, ANT-0830398, OCE-0961405]; National Aeronautics and Space Administration [NNX08AN67G]; National Aeronautics and Space Administration (ECCO2 project); NASA Postdoctoral Program; NASA FX We thank everyone who made the oceanographic cruises successful, especially the scientists, technicians, officers, and crew onboard the RV Hesperides and RV Puerto Deseado. We are grateful for the assistance of John Walpert, Agusti Julia, Joan Puigdefabregas, and Jordi Cateura with the mooring design, construction, and deployment. Hong Zhang kindly provided the ECCO2 adjoint boundary conditions, and Xiaochun (Adam) Wang helped implementing the tidal forcing. Conversations with Gary Egbert, Eberhard Fahrbach, Andrew Thompson, and Victor Zlotnicki improved this work. This research was supported by the Spanish Research and Innovation (I+D+i) National Plan (CGL2007-28783-E/ ANT, CTM2008-04623-E/ANT, CTM2009-08287-E/ANT, and CTM2011-14056-E), the National Science Foundation (ANT-0818061, ANT-0830398, and OCE-0961405), the National Aeronautics and Space Administration (NNX08AN67G and ECCO2 project), and the NASA Postdoctoral Program administered by Oak Ridge Associated Universities. Data and products are available through the Spanish Polar Database website (http://hielo.igme.es/index.php/en/), NSF website (http://www.nsf.gov/), and ECCO2 website (http://ecco2.jpl.nasa.gov/). This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This is ESR contribution number 155. This work is dedicated to Agusti Julia (1940-2009) and Eberhard Fahrbach (1948-2013). We are grateful to Matthew Mazloff and one anonymous reviewer whose many perceptive comments greatly improved this manuscript. NR 72 TC 3 Z9 3 U1 0 U2 7 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 MAY PY 2015 VL 120 IS 5 BP 3658 EP 3680 DI 10.1002/2014JC010372 PG 23 WC Oceanography SC Oceanography GA CL0JI UT WOS:000356628100027 ER PT J AU Seo, KW Wilson, CR Scambos, T Kim, BM Waliser, DE Tian, B Kim, BH Eom, J AF Seo, Ki-Weon Wilson, Clark R. Scambos, Ted Kim, Baek-Min Waliser, Duane E. Tian, Baijun Kim, Byeong-Hoon Eom, Jooyoung TI Surface mass balance contributions to acceleration of Antarctic ice mass loss during 2003-2013 SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE ice mass balance; Antarctica; GRACE ID SEA-LEVEL RISE; WEST ANTARCTICA; GRACE DATA; SNOW ACCUMULATION; SHEET; GREENLAND; GLACIER; VARIABILITY; INCREASE; RADAR AB Recent observations from satellite gravimetry (the Gravity Recovery and Climate Experiment (GRACE) mission) suggest an acceleration of ice mass loss from the Antarctic Ice Sheet (AIS). The contribution of surface mass balance changes (due to variable precipitation) is compared with GRACE-derived mass loss acceleration by assessing the estimated contribution of snow mass from meteorological reanalysis data. We find that over much of the continent, the acceleration can be explained by precipitation anomalies. However, on the Antarctic Peninsula and other parts of West Antarctica, mass changes are not explained by precipitation and are likely associated with ice discharge rate increases. The total apparent GRACE acceleration over all of the AIS between 2003 and 2013 is -13.67.2Gt/yr(2). Of this total, we find that the surface mass balance component is -8.22.0Gt/yr(2). However, the GRACE estimate appears to contain errors arising from the atmospheric pressure fields used to remove air mass effects. The estimated acceleration error from this effect is about 9.85.8Gt/yr(2). Correcting for this yields an ice discharge acceleration of -15.16.5Gt/yr(2). C1 [Seo, Ki-Weon; Kim, Byeong-Hoon; Eom, Jooyoung] Seoul Natl Univ, Dept Earth Educ, Seoul, South Korea. [Wilson, Clark R.] Univ Texas Austin, Dept Geol Sci, Jackson Sch Geosci, Austin, TX USA. [Wilson, Clark R.] Univ Texas Austin, Ctr Space Res, Austin, TX 78712 USA. [Scambos, Ted] Univ Colorado, Nat Snow & Ice Data Ctr, Boulder, CO 80309 USA. [Kim, Baek-Min] Korea Polar Res Inst, Div Polar Earth Syst Sci, Inchon, South Korea. [Waliser, Duane E.; Tian, Baijun] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Seo, KW (reprint author), Seoul Natl Univ, Dept Earth Educ, Seoul, South Korea. EM seokiweon@snu.ac.kr RI Tian, Baijun/A-1141-2007 OI Tian, Baijun/0000-0001-9369-2373 FU National Research Foundation [NRF-2013R1A1A2008368]; Korea Polar Research Institute [PM14020]; NASA FX This work was supported by National Research Foundation grant NRF-2013R1A1A2008368 and Korea Polar Research Institute research grant PM14020. D.W. and B.T.'s contributions were carried out on behalf of the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. GRACE, ERA Interim, MERRA, and NCEP/DOE data are available from GRACE Tellus site (http://grace.jpl.nasa.gov), ECMWF data server (http://data-portal.ecmwf.int), Goddard Earth Sciences Data and Information Services Center (http://disc.sci.gsfc.nasa.gov), and Earth System Research Laboratory (http://www.esrl.noaa.gov), respectively. RACMO2.3 data are available upon request in Institute for Marine and Atmospheric Research Utrecht (http://www.projects.science.uu.nl/ice-climate/models/antarctica.php). NR 36 TC 4 Z9 4 U1 2 U2 22 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 MAY PY 2015 VL 120 IS 5 BP 3617 EP 3627 DI 10.1002/2014JB011755 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CK7YV UT WOS:000356454500041 PM 27708992 ER PT J AU Xue, L Schwartz, S Liu, Z Feng, LJ AF Xue, Lian Schwartz, Susan Liu, Zhen Feng, Lujia TI Interseismic megathrust coupling beneath the Nicoya Peninsula, Costa Rica, from the joint inversion of InSAR and GPS data SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE interseismic deformaion; subduction zone; InSAR and GPS ID SAN-ANDREAS FAULT; SUBDUCTION ZONE; STRAIN ACCUMULATION; SLOW-SLIP; RADAR INTERFEROMETRY; SURFACE DEFORMATION; EARTHQUAKE RUPTURE; SEISMOGENIC ZONE; SATELLITE RADAR; P-WAVE AB The Nicoya Peninsula, Costa Rica, was struck by a long-anticipated and gap-filling M-w 7.6 earthquake in 2012. To study interseismic strain accumulation on the megathrust beneath the Nicoya Peninsula, we present an improved interseismic coupling model by integrating interferometric synthetic aperture radar (InSAR) and GPS data. Our model reveals three strongly coupled patches. The first strongly coupled patch locates beneath the Nicoya Peninsula and ruptured during the 2012 earthquake. The second strongly coupled patch locates offshore the central Nicoya Peninsula and remained largely unbroken. However, this region is close to and possibly intermingled with shallow slow slip and tremor, suggesting that accumulated strain in this region may be released both seismically and aseismically. The third strongly coupled patch offshore of the southeastern end of Nicoya overlaps part of the coseismic rupture of the 1990 M-w 7.0 Nicoya Gulf earthquake, indicating that significant strain has re-accumulated since this event. Incorporating InSAR data provides a more refined interseismic coupling model than using GPS alone and allows for a more reliable comparison with local seismic and aseismic activities. This comparison indicates that strongly locked regions during the interseismic stage are the loci of coseismic slip, and deep slow slip and low-frequency earthquakes occur in regions of low coupling or transition zones from low to high coupling, while shallow slow slip and tremor commingle with strongly coupled regions. Our study demonstrates that InSAR data can be used to recover small long-wavelength deformation signals with refined resolution in challenging subduction zone environments when integrated with GPS observations. C1 [Xue, Lian; Schwartz, Susan] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Liu, Zhen] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Feng, Lujia] Nanyang Technol Univ, Earth Observ Singapore, Singapore 639798, Singapore. RP Xue, L (reprint author), Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. EM lxue3@ucsc.edu RI Feng, Lujia/F-2523-2012; Liu, Zhen/D-8334-2017 OI Feng, Lujia/0000-0002-3736-5025; FU National Aeronautics and Space Administration; [OCE-0841061]; [EAR-1321550] FX This study was supported by OCE-0841061 and EAR-1321550. ALOS PALSAR data are copyright JAXA/METI and were provided by the GEO Supersites and the U.S. Government Research Consortium Data pool at the Alaska Satellite Facility (https://www.asf.alaska.edu/). The research described in this paper was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We greatly appreciate the support of Emily Brodsky, and thank all the people who provided advice on this project. Figures were created using Generic Mapping Tools [Wessel and Smith, 1991]. We thank M.E. Prichard and an anonymous reviewer for their very helpful comments that greatly improved this paper as well Scott Baker, Tim Dixon, Rowena Lohman and Isabelle Ryder for their early guidance on this project. NR 69 TC 1 Z9 1 U1 1 U2 3 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 MAY PY 2015 VL 120 IS 5 BP 3707 EP 3722 DI 10.1002/2014JB011844 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CK7YV UT WOS:000356454500046 ER PT J AU Wu, X Abbondanza, C Altamimi, Z Chin, TM Collilieux, X Gross, RS Heflin, MB Jiang, Y Parker, JW AF Wu, Xiaoping Abbondanza, Claudio Altamimi, Zuheir Chin, T. Mike Collilieux, Xavier Gross, Richard S. Heflin, Michael B. Jiang, Yan Parker, Jay W. TI KALREFA Kalman filter and time series approach to the International Terrestrial Reference Frame realization SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE terrestrial reference frame; Kalman filter; geodetic techniques; time series; data combination; geocenter motion ID MASS REDISTRIBUTION; GEODETIC DATA; SEA-LEVEL; MOTION; SYSTEM; GPS; ITRF2008; SPACE; NOISE AB The current International Terrestrial Reference Frame is based on a piecewise linear site motion model and realized by reference epoch coordinates and velocities for a global set of stations. Although linear motions due to tectonic plates and glacial isostatic adjustment dominate geodetic signals, at today's millimeter precisions, nonlinear motions due to earthquakes, volcanic activities, ice mass losses, sea level rise, hydrological changes, and other processes become significant. Monitoring these (sometimes rapid) changes desires consistent and precise realization of the terrestrial reference frame (TRF) quasi-instantaneously. Here, we use a Kalman filter and smoother approach to combine time series from four space geodetic techniques to realize an experimental TRF through weekly time series of geocentric coordinates. In addition to secular, periodic, and stochastic components for station coordinates, the Kalman filter state variables also include daily Earth orientation parameters and transformation parameters from input data frames to the combined TRF. Local tie measurements among colocated stations are used at their known or nominal epochs of observation, with comotion constraints applied to almost all colocated stations. The filter/smoother approach unifies different geodetic time series in a single geocentric frame. Fragmented and multitechnique tracking records at colocation sites are bridged together to form longer and coherent motion time series. While the time series approach to TRF reflects the reality of a changing Earth more closely than the linear approximation model, the filter/smoother is computationally powerful and flexible to facilitate incorporation of other data types and more advanced characterization of stochastic behavior of geodetic time series. C1 [Wu, Xiaoping; Abbondanza, Claudio; Chin, T. Mike; Gross, Richard S.; Heflin, Michael B.; Jiang, Yan; Parker, Jay W.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Abbondanza, Claudio] Univ Calif Los Angeles, Reg Earth Syst Sci & Engn, Joint Inst, Los Angeles, CA USA. [Altamimi, Zuheir; Collilieux, Xavier] Inst Natl Informat Geog & Forestiere, Paris, France. [Jiang, Yan] Geol Survey Canada, Sidney, BC, Canada. RP Wu, X (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Xiaoping.Wu@jpl.nasa.gov FU National Aeronautics and Space Administration (NASA) FX Part of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). All data used in this study are freely available from the ITRF Web site http://itrf.ensg.fr and NASA's Archive of Space Geodesy Data site http://cddis.nasa.gov. The Generic MappingTools areusedto create Figures 4 and 5. We thank two anonymous reviewers for their constructive comments and suggestions. NR 53 TC 5 Z9 5 U1 1 U2 7 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 MAY PY 2015 VL 120 IS 5 BP 3775 EP 3802 DI 10.1002/2014JB011622 PG 28 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CK7YV UT WOS:000356454500049 ER PT J AU Fukumori, I Wang, O Llovel, W Fenty, I Forget, G AF Fukumori, Ichiro Wang, Ou Llovel, William Fenty, Ian Forget, Gael TI A near-uniform fluctuation of ocean bottom pressure and sea level across the deep ocean basins of the Arctic Ocean and the Nordic Seas SO PROGRESS IN OCEANOGRAPHY LA English DT Review ID GENERAL-CIRCULATION; DATA ASSIMILATION; ALTIMETER DATA; WIND; ATLANTIC; MODEL; VARIABILITY; SENSITIVITY; PERFORMANCE; TRANSPORT AB Across the Arctic Ocean and the Nordic Seas, a basin-wide mode of ocean bottom pressure and sea level fluctuation is identified using satellite and in situ observations in conjunction with a global ocean circulation model and its adjoint. The variation extends across the interconnected deep ocean basins of these semi-enclosed Arctic seas, collectively called the Arctic Mediterranean, with spatially near-uniform amplitude and phase. The basin-wide fluctuation is barotropic and dominates the region's large-scale variability from sub-monthly to interannual timescales. The fluctuation results from bifurcating coastally trapped waves generated by winds along the continental slopes of the Arctic Mediterranean and its neighboring seas, including the North Atlantic Ocean. The winds drive Ekman transport across the large bathymetric gradients, forcing mass divergence between the shallow coastal area and the deep ocean basins and creating ocean bottom pressure anomalies of opposite signs in the two regions. The anomalies rapidly propagate away as barotropic coastally trapped waves with the coast and continental slope as respective boundaries. The waves subsequently bifurcate at the shallow straits connecting the Arctic Mediterranean with the rest of the globe. The straits transmit the shallow anomalies but not the deep variations, thereby inhibiting the anomalies' mutual cancelation by geographically separating the two. Anomalies that enter the deep Arctic basins equilibrate uniformly across the domain characterized by a homogeneous depth-integrated planetary potential vorticity distribution. The potential vorticity's steep gradient that borders the basins shields the region from neighboring shallow variations, giving rise to the observed spatially confined fluctuation. Compensating anomalies outside the Arctic adjust similarly across the rest of the globe but are comparatively negligible in amplitude because of the global ocean's larger area relative to that of the deep Arctic Mediterranean. The study, from a technical perspective, illustrates the utility of a model's adjoint in identifying causal mechanisms underlying a complex system. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Fukumori, Ichiro; Wang, Ou; Llovel, William; Fenty, Ian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Llovel, William] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. [Forget, Gael] MIT, Cambridge, MA 02139 USA. RP Fukumori, I (reprint author), CALTECH, Jet Prop Lab, Mail Stop 300-323,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM fukumori@jpl.nasa.gov RI LLOVEL, William/G-6930-2016 FU National Aeronautics and Space Administration (NASA); National Science Foundation FX 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). GRACE mascons solutions were kindly made available by M. Watkins, D. Wiese, C. Boening, and V. Zlotnicki. Ocean bottom pressure data in the Beaufort Sea were collected and made available by the Beaufort Gyre Exploration Program based at the Woods Hole Oceanographic Institution (http://www.whoi.edu/beaufortgyre) in collaboration with researchers from Fisheries and Oceans Canada at the Institute of Ocean Sciences. The North Pole Bottom Pressure Records were provided by NCAR/EOL under sponsorship of the National Science Foundation, http://data.eol.ucar.edu/. The authors thank Don Chambers and other anonymous reviewers for providing valuable comments on this manuscript. NR 49 TC 8 Z9 8 U1 1 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0079-6611 J9 PROG OCEANOGR JI Prog. Oceanogr. PD MAY PY 2015 VL 134 BP 152 EP 172 DI 10.1016/j.pocean.2015.01.013 PG 21 WC Oceanography SC Oceanography GA CK9IN UT WOS:000356553900008 ER PT J AU Williams, KE McKay, CP AF Williams, Kaj E. McKay, Christopher P. TI Comparing flow-through and static ice cave models for Shoshone Ice Cave SO INTERNATIONAL JOURNAL OF SPELEOLOGY LA English DT Article DE ice cave; latent heat; airflow; Shoshone Ice Cave; USA ID AUSTRIA; BALANCE; MASS AB In this paper we suggest a new ice cave type: the "flow-through" ice cave. In a flow-through ice cave external winds blow into the cave and wet cave walls chill the incoming air to the wet-bulb temperature, thereby achieving extra cooling of the cave air. We have investigated an ice cave in Idaho, located in a lava tube that is reported to have airflow through porous wet end-walls and could therefore be a flow-through cave. We have instrumented the site and collected data for one year. In order to determine the actual ice cave type present at Shoshone, we have constructed numerical models for static and flow-through caves (dynamic is not relevant here). The models are driven with exterior measurements of air temperature, relative humidity and wind speed. The model output is interior air temperature and relative humidity. We then compare the output of both models to the measured interior air temperatures and relative humidity. While both the flow-through and static cave models are capable of preserving ice year-round (a net zero or positive ice mass balance), both models show very different cave air temperature and relative humidity output. We find the empirical data support a hybrid model of the static and flow-through models: permitting a static ice cave to have incoming air chilled to the wet-bulb temperature fits the data best for the Shoshone ice cave. C1 [Williams, Kaj E.; McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94035 USA. [Williams, Kaj E.] Montana State Univ, Dept Earth Sci, Bozeman, MT 59717 USA. RP Williams, KE (reprint author), NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Mail Stop 245-3, Moffett Field, CA 94035 USA. EM kaj.williams@montana.edu FU NASA; Idaho Space Grant Consortium FX The authors would like to thank Fred Cheslik and the Shoshone Indian Ice Caves for permitting us to instrument the cave, and for their hospitality. We thank three anonymous reviewers who provided useful comments and improvements to the manuscript. We also thank NASA and the Idaho Space Grant Consortium for partial support. NR 23 TC 0 Z9 0 U1 3 U2 3 PU SOCIETA SPELEOLOGICA ITALIANA PI BOLOGNA PA VIA ZAMBONI 67, BOLOGNA, 40126, ITALY SN 0392-6672 EI 1827-806X J9 INT J SPELEOL JI Int. J. Speleol. PD MAY PY 2015 VL 44 IS 2 BP 115 EP 123 DI 10.5038/1827-806X.44.2.2 PG 9 WC Geology; Geosciences, Multidisciplinary SC Geology GA CK4CP UT WOS:000356167600002 ER PT J AU Genova, A Goossens, S Lemoine, FG Mazarico, E Fricke, SK Smith, DE Zuber, MT AF Genova, Antonio Goossens, Sander Lemoine, Frank G. Mazarico, Erwan Fricke, Susan K. Smith, David E. Zuber, Maria T. TI Long-term variability of CO2 and O in the Mars upper atmosphere from MRO radio science data SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE MRO; Mars Upper Atmosphere; Radio Science ID GLOBAL SURVEYOR; SPACECRAFT; THERMOSPHERE; ORIENTATION; AEROBRAKING; EPHEMERIS; TRACKING; GRAVITY; ORBITS; PHOBOS AB We estimate the annual variability of CO2 and O partial density using approximately 6years of Mars Reconnaissance Orbiter (MRO) radio science data from August 2006 to January 2012, which cover three full Martian years (from the northern hemisphere summer of 28 to the northern hemisphere summer of 31). These two elements are the dominant species at the MRO periapsis altitude, constituting about 70-80% of the total density. We report the recovered annual cycle of CO2 and the annual and seasonal cycle of O in the upper atmosphere. Although no other observations are available at those altitudes, our results are in good agreement with the density measurements of the Mars Express Spectroscopy for Investigation of Characteristics of the Atmosphere of Mars, which uses stellar occultations between 60 and 130km to determine the CO2 variability, and with the Mars Global Reference Atmospheric Model 2010 for the O annual and seasonal variabilities. Furthermore, the updated model provides more reasonable MRO drag coefficients (C-D), which are estimated to absorb mismodeling in the atmospheric density prediction. The higher content of dust in the atmosphere due to dust storms increases the density, so the C(D)s should compensate for this effect. The correlation between the drag coefficient and the dust optical depth, measured by the Mars Odyssey Thermal Emission Imaging System (THEMIS) instrument, increases from 0.4 to 0.8 with the a priori and adjusted models, respectively. The trend of C(D)s not only confirms a substantial improvement in the prediction of the atmospheric density with the updated model but also provides useful information for local dust storms, near MRO periapsis, that cannot be measured by the opacity level since THEMIS does not always sample the southern hemisphere evenly. C1 [Genova, Antonio; Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Genova, Antonio; Goossens, Sander; Lemoine, Frank G.; Mazarico, Erwan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Goossens, Sander] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21228 USA. [Fricke, Susan K.] SGT Inc, Greenbelt, MD USA. RP Genova, A (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. EM antonio.genova@nasa.gov RI Lemoine, Frank/D-1215-2013; Goossens, Sander/K-2526-2015; Mazarico, Erwan/N-6034-2014; Genova, Antonio/M-1400-2016 OI Goossens, Sander/0000-0002-7707-1128; Mazarico, Erwan/0000-0003-3456-427X; Genova, Antonio/0000-0001-5584-492X NR 51 TC 1 Z9 1 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAY PY 2015 VL 120 IS 5 BP 849 EP 868 DI 10.1002/2014JE004770 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CK7TB UT WOS:000356434600002 ER PT J AU Crow-Willard, EN Pappalardo, RT AF Crow-Willard, Emma N. Pappalardo, Robert T. TI Structural mapping of Enceladus and implications for formation of tectonized regions SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Enceladus; tectonics; mapping ID SOUTH-POLAR FRACTURES; UNSTABLE EXTENSION; TIGER STRIPES; ICE SHELL; HEAT-FLUX; ORIGIN; CONVECTION; MIRANDA; GEOLOGY; SURFACE AB Global structural mapping of high-resolution Cassini images of Enceladus reveals a richly varied surface. Most notable are three main regions of deformation each containing multiple structural units. In addition to the well known South Polar Terrain (SPT), there are two other large regions of deformation that we term Leading Hemisphere Terrain (LHT) and Trailing Hemisphere Terrain (THT). Each of these three terrains includes a circumferential belt that encloses one or more other structurally deformed units. Areal extents range from about 80,000km(2) (SPT) to 195,000km(2) (LHT) or 160 to 250km equivalent circular radius. Based on relative crater densities, the THT is inferred to be older than the LHT; the geologically active SPT is the youngest. The overall similarities in shape and dimension of the three tectonized terrains suggest similar formational processes, plausibly related to broad loading of a thin elastic shell. A viable scenario is that each tectonized terrain formed above a large-scale region of warm upwelling ice, with subsequent downwarping triggered by cooling and/or subsurface melting. However, differences in morphological detail suggest that the specific evolution of each tectonized terrain has been different. C1 [Crow-Willard, Emma N.] Occidental Coll, Dept Geol, Los Angeles, CA 90041 USA. [Crow-Willard, Emma N.; Pappalardo, Robert T.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Pappalardo, RT (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM robert.pappalardo@jpl.nasa.gov FU National Aeronautics and Space Administration; NASA [NNG06GF44G]; Jupiter Europa Orbiter Pre-Project FX 5The Cassini ISS team's global image mosaic of Enceladus is available from the Planetary Data System or from the ISS team website . Our ArcGIS map is available by email request from the corresponding author . This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Funding was provided by the NASA Outer Planets Research Program (NNG06GF44G) and the (former) Jupiter Europa Orbiter Pre-Project. We are grateful to Geoff Collins for useful discussion and assistance, to Simon Kattenhorn and Wes Patterson for reviews that greatly improved this manuscript, and to D. Alex Patthoff for invaluable assistance in revision of the manuscript. NR 53 TC 8 Z9 8 U1 4 U2 9 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 MAY PY 2015 VL 120 IS 5 BP 928 EP 950 DI 10.1002/2015JE004818 PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CK7TB UT WOS:000356434600006 ER PT J AU Jian, LK MacNeice, PJ Taktakishvili, A Odstrcil, D Jackson, B Yu, HS Riley, P Sokolov, IV Evans, RM AF Jian, L. K. MacNeice, P. J. Taktakishvili, A. Odstrcil, D. Jackson, B. Yu, H. -S. Riley, P. Sokolov, I. V. Evans, R. M. TI Validation for solar wind prediction at Earth: Comparison of coronal and heliospheric models installed at the CCMC SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE models; solar wind; space weather forecasting ID COROTATING INTERACTION REGIONS; MAGNETIC-FIELD DIRECTION; EJECTION IMAGER SMEI; MASS EJECTIONS; INTERPLANETARY SCINTILLATION; SPACE WEATHER; 3-DIMENSIONAL PROPAGATION; INNER HELIOSPHERE; FLUX TRANSPORT; ALFVEN WAVES AB Multiple coronal and heliospheric models have been recently upgraded at the Community Coordinated Modeling Center (CCMC), including the Wang-Sheeley-Arge (WSA)-Enlil model, MHD-Around-a-Sphere (MAS)-Enlil model, Space Weather Modeling Framework (SWMF), and heliospheric tomography using interplanetary scintillation data. To investigate the effects of photospheric magnetograms from different sources, different coronal models, and different model versions on the model performance, we run these models in 10 combinations. Choosing seven Carrington rotations in 2007 as the time window, we compare the modeling results with the Operating Mission as Nodes on the Internet data for near-Earth space environment during the late declining phase of solar cycle 23. Visual comparison is proved to be a necessary addition to the quantitative assessment of the models' capabilities in reproducing the time series and statistics of solar wind parameters. The MAS-Enlil model captures the time patterns of solar wind parameters better, while the WSA-Enlil model matches with the time series of normalized solar wind parameters better. Models generally overestimate slow wind temperature and underestimate fast wind temperature and magnetic field. Using improved algorithms, we have identified magnetic field sector boundaries (SBs) and slow-to-fast stream interaction regions (SIRs) as focused structures. The success rate of capturing them and the time offset vary largely with models. For this quiet period, the new version of MAS-Enlil model works best for SBs, while heliospheric tomography works best for SIRs. The new version of SWMF with more physics added needs more development. General strengths and weaknesses for each model are diagnosed to provide an unbiased reference to model developers and users. C1 [Jian, L. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Jian, L. K.; MacNeice, P. J.; Taktakishvili, A.; Odstrcil, D.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Taktakishvili, A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Odstrcil, D.; Evans, R. M.] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA. [Jackson, B.; Yu, H. -S.] Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92103 USA. [Riley, P.] Predictive Sci Inc, San Diego, CA USA. [Sokolov, I. V.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP Jian, LK (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM lan.jian@nasa.gov RI Sokolov, Igor/H-9860-2013; Jian, Lan/B-4053-2010; OI Sokolov, Igor/0000-0002-6118-0469; Jian, Lan/0000-0002-6849-5527; Riley, Pete/0000-0002-1859-456X FU NSF [AGS 1242798, 1321493, 1259549, AGS 1257519] FX This work is supported by NSF grants AGS 1242798, 1321493 and 1259549. A.T. and I.V.S. are supported by NSF grant AGS 1257519. Simulation results have been provided by the CCMC at NASA/GSFC through their public Runs on Request system (http://ccmc.gsfc.nasa.gov/requests/requests.php). The results of IPS tomography are available upon request from Bernard Jackson at UCSD. The simulation results of other models are available to the public at http://ccmc.gsfc.nasa.gov/ungrouped/SH/Helio_main.php by searching "Jian" as run requestor's last name and choosing 2056-2062 as the Carrington rotation number. The CCMC is a multiagency partnership between NASA, AFMC, AFOSR, AFRL, AFWA, NOAA, NSF, and ONR. We are grateful to the CCMC team for their work. We thank the GONG, SOHO/MDI, MWO, and NSO teams for providing the photospheric magnetograms. We appreciate Nick Arge for providing the WSA coronal model at the CCMC and thank all the other modeling teams (see section 2) for providing their models at the CCMC and for their consultation. We acknowledge the Space Physics Data Facility at NASA/GSFC for providing OMNI data (see http://omniweb.gsfc.nasa.gov/). L.K.J. thanks Janet Luhmann and Christopher Russell for helpful discussion. NR 94 TC 7 Z9 7 U1 0 U2 11 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 MAY PY 2015 VL 13 IS 5 BP 316 EP 338 DI 10.1002/2015SW001174 PG 23 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA CL0HX UT WOS:000356623500009 ER PT J AU Cervini-Silva, J Antonio-Nieto-Camacho Ramirez-Apan, MT Gomez-Vidales, V Palacios, E Montoya, A de Jesus, ER AF Cervini-Silva, Javiera Antonio-Nieto-Camacho Teresa Ramirez-Apan, Maria Gomez-Vidales, Virginia Palacios, Eduardo Montoya, Ascencion Ronquillo de Jesus, Elba TI Anti-inflammatory, anti-bacterial, and cytotoxic activity of fibrous clays SO COLLOIDS AND SURFACES B-BIOINTERFACES LA English DT Article DE Early anti-inflammatory response; Frequency of inversion sites; Silanol groups ID TRIBOLIUM-CASTANEUM; POWDER DIFFRACTION; MOUSE EAR; MAYA BLUE; SEPIOLITE; PALYGORSKITE; EFFICACY; HALLOYSITE; AGENTS; INDIGO AB Produced worldwide at 1.2 m tons per year, fibrous clays are used in the production of pet litter, animal feed stuff to roof parcels, construction and rheological additives, and other applications needing to replace long-fiber length asbestos. To the authors' knowledge, however, information on the beneficial effects of fibrous clays on health remains scarce. This paper reports on the anti-inflammatory, antibacterial, and cytotoxic activity by sepiolite (Vallecas, Spain) and palygorskite (Torrejon El Rubio, Spain). The anti-inflammatory activity was determined using the 12-O-tetradecanoylphorbol-13-acetate (TPA) and myeloperoxidase (MPO) methods. Histological cuts were obtained for quantifying leukocytes found in the epidermis. Palygorkite and sepiolite caused edema inhibition and migration of neutrophils ca. 68.64 and 45.54%, and 80 and 65%, respectively. Fibrous clays yielded high rates of infiltration, explained by cleavage of polysomes and exposure of silanol groups. Also, fibrous clays showed high inhibition of myeloperoxidase contents shortly after exposure, but decreased sharply afterwards. In contrast, tubular clays caused an increasing inhibition of myeloperoxidase with time. Thus, clay structure restricted the kinetics and mechanism of myeloperoxidase inhibition. Fibrous clays were screened in vitro against human cancer cell lines. Cytotoxicity was determined using the protein-binding dye sulforhodamine B (SRB). Exposing cancer human cells to sepiolite or palygorskite showed growth inhibition varying with cell line. This study shows that fibrous clays served as an effective anti-inflammatory, limited by chemical transfer and cellular-level signals responding exclusively to an early exposure to clay, and cell viability decreasing significantly only after exposure to high concentrations of sepiolite. (C) 2015 Elsevier B.V. All rights reserved. C1 [Cervini-Silva, Javiera; Ronquillo de Jesus, Elba] Univ Autonoma Metropolitana, Dept Proc & Tecnol, Unidad Cuajimalpa, Mexico City 05348, DF, Mexico. [Cervini-Silva, Javiera] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Earth Sci, Berkeley, CA 94720 USA. [Cervini-Silva, Javiera] NASA, Astrobiol Inst, Mountain View, CA USA. [Antonio-Nieto-Camacho; Teresa Ramirez-Apan, Maria] Univ Nacl Autonoma Mexico, Inst Quim, Lab Pruebas Biol, Mexico City 04510, DF, Mexico. [Gomez-Vidales, Virginia] Univ Nacl Autonoma Mexico, Inst Quim, Lab Resonancia Paramagnet Elect, Mexico City 04510, DF, Mexico. [Palacios, Eduardo; Montoya, Ascencion] Inst Mexicano Petr, Direcc Invest & Posgrad, Ciuadad Mexico, DF, Mexico. RP Cervini-Silva, J (reprint author), Univ Autonoma Metropolitana, Dept Proc & Tecnol, Unidad Cuajimalpa, Av Vasco de Quiroga 4871, Mexico City 05348, DF, Mexico. EM jcervini@correo.cua.uam.mx FU Universidad Autonoma Metropolitana Unidad Cuajimalpa [33678] FX The authors thank Maria del Rocio Galindo Ortega and Carolina Lopez Pacheco (UAM-Cuajimalpa), and Daniela Rodriguez Montano (Unidad de Histologia, Instituto de Fisiologia Celular, UNAM) for technical assistance; and Drs. Georgios D. Chyssikos (Theoretical and Physical Chemistry Institute, National Hellenic Research Foundation, Athens, 11635, Greece), Vassilis Gionis (Institute of Materials Science, N.C.S.R. "Demokritos", 15310, Aghia Paraskevi, Attiki, Greece); and Stephan Kaufhold (BGR Bundensansaltfur Geowissenschaften und Rohstoffe, Hannover, Germany) for providing insightful comments during the preparation of this manuscript. This project was supported in part by Universidad Autonoma Metropolitana Unidad Cuajimalpa (Grant No. 33678). NR 35 TC 9 Z9 9 U1 6 U2 35 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-7765 EI 1873-4367 J9 COLLOID SURFACE B JI Colloid Surf. B-Biointerfaces PD MAY 1 PY 2015 VL 129 BP 1 EP 6 DI 10.1016/j.colsurfb.2015.03.019 PG 6 WC Biophysics; Chemistry, Physical; Materials Science, Biomaterials SC Biophysics; Chemistry; Materials Science GA CJ3AQ UT WOS:000355356200001 PM 25819359 ER PT J AU Shaver, I Chain-Guadarrama, A Cleary, KA Sanfiorenzo, A Santiago-Garcia, RJ Finegan, B Hormel, L Sibelet, N Vierling, LA Bosque-Perez, NA DeClerck, F Fagan, ME Waits, LP AF Shaver, Irene Chain-Guadarrama, Adina Cleary, Katherine A. Sanfiorenzo, Andre Santiago-Garcia, Ricardo J. Finegan, Bryan Hormel, Leontina Sibelet, Nicole Vierling, Lee A. Bosque-Perez, Nilsa A. DeClerck, Fabrice Fagan, Matthew E. Waits, Lisette P. TI Coupled social and ecological outcomes of agricultural intensification in Costa Rica and the future of biodiversity conservation in tropical agricultural regions SO GLOBAL ENVIRONMENTAL CHANGE-HUMAN AND POLICY DIMENSIONS LA English DT Article DE Agricultural intensification; Biodiversity; Non-traditional agricultural export; Smallholder; Pineapple; Costa Rica ID ENVIRONMENTAL SERVICE PAYMENTS; LAND-USE CHANGE; RAIN-FOREST; AGROFORESTRY SYSTEMS; DIPTERYX-PANAMENSIS; TREE COVER; LANDSCAPES; MANAGEMENT; SECONDARY; GLOBALIZATION AB Tropical ecosystem conversion to agriculture has caused widespread habitat loss and created fragmented landscapes composed of remnant forest patches embedded in a matrix of agricultural land uses. Non-traditional agricultural export (NTAE) crops such as pineapple are rapidly replacing multiuse landscapes characterized by a diverse matrix of pasture and smallholder crops with intensive, large-scale, monoculture plantations. Using an interdisciplinary approach, we conduct a case study to examine the coupled social and ecological implications of agricultural intensification in this region, with larger application to regions experiencing similar patterns of agricultural intensification. Guided by frameworks from both political and landscape ecology, we: (1) describe the social and economic implications of pineapple expansion, specifically the concentration of land, labor and financial resources, (2) quantify pineapple cultivation's spatial characteristics, and (3) assess the effects of pineapple expansion on surrounding forest ecosystems, on the agricultural matrix and on biodiversity conservation. Our results indicate that pineapple production concentrates land, labor, and financial resources, which has a homogenizing effect on the agricultural economy in the study region. This constrains farm-based livelihoods, with larger implications for food security and agricultural diversity. Landscape ecology analyses further reveal how pineapple production simplifies and homogenizes the agricultural matrix between forest patches, which is likely to have a negative effect on biodiversity. To offset the effects of pineapple expansion on social and environmental systems, we recommend developing landscape level land use planning capacity. Furthermore, agricultural and conservation policy reform is needed to promote landscape heterogeneity and economic diversity within the agricultural sector. Our interdisciplinary research provides a detailed examination of the social and ecological impacts of agricultural intensification in a tropical landscape, and offers recommendations for improvement relevant not only to our study region but to the many other tropical landscapes currently undergoing non-traditional agricultural export driven agricultural intensification. (c) 2015 Elsevier Ltd. All rights reserved. C1 [Shaver, Irene; Sanfiorenzo, Andre; Santiago-Garcia, Ricardo J.] Univ Idaho, Environm Sci Program, Moscow, ID 83844 USA. [Chain-Guadarrama, Adina; Vierling, Lee A.] Univ Idaho, Dept Forest Rangeland & Fire Sci, Idaho Falls, ID 83441 USA. [Shaver, Irene; Chain-Guadarrama, Adina; Cleary, Katherine A.; Sanfiorenzo, Andre; Santiago-Garcia, Ricardo J.] Trop Agr Res & Higher Educ Ctr CATIE, Grad Sch, Turrialba 30501, Costa Rica. [Cleary, Katherine A.; Waits, Lisette P.] Univ Idaho, Dept Fish & Wildlife Sci, Moscow, ID 83844 USA. [Bosque-Perez, Nilsa A.] Univ Idaho, Dept Plant Soil & Entomol Sci, Moscow, ID 83844 USA. [DeClerck, Fabrice] CGIAR, Biodivers Int, Agrobiodivers & Ecosyst Serv Program, F-34950 Montpellier, France. [Finegan, Bryan] Trop Agr Res & Higher Educ Ctr CATIE, Prod & Conservat Forests Program, Turrialba 30501, Costa Rica. [Hormel, Leontina] Univ Idaho, Dept Sociol & Anthropol, Moscow, ID 83844 USA. [Sibelet, Nicole] CIRAD, UMR Innovat, F-34398 Montpellier, France. [Sibelet, Nicole] Trop Agr Res & Higher Educ Ctr CATIE, Econ & Environm Dev IDEA, Turrialba 30501, Costa Rica. [Fagan, Matthew E.] NASA, Goddard Space Flight Ctr, Postdoctoral Program, Greenbelt, MD 20771 USA. RP Shaver, I (reprint author), 13775 Nisula Rd, McCall, ID 83638 USA. EM shaverirene@gmail.com RI Chain-Guadarrama, Adina/K-1167-2016; Guadarrama, Mercedes/K-1155-2016 OI Chain-Guadarrama, Adina/0000-0002-6944-2064; Guadarrama, Mercedes/0000-0002-6944-2064 FU National Science Foundation under IGERT [0903479]; National Science Foundation under CNH [1313824] FX This material is based upon work supported by the National Science Foundation under IGERT grant number Award No. 0903479 and CNH grant Award No. 1313824. Fabrice DeClerck was supported by the CGIAR research program on Water Land and Ecosystems. NR 121 TC 3 Z9 3 U1 21 U2 80 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0959-3780 EI 1872-9495 J9 GLOBAL ENVIRON CHANG JI Glob. Environ. Change-Human Policy Dimens. PD MAY PY 2015 VL 32 BP 74 EP 86 DI 10.1016/j.gloenvcha.2015.02.006 PG 13 WC Environmental Sciences; Environmental Studies; Geography SC Environmental Sciences & Ecology; Geography GA CJ8RH UT WOS:000355770700008 ER PT J AU Kara, E Fabian, AC Lohfink, AM Parker, ML Walton, DJ Boggs, SE Christensen, FE Hailey, CJ Harrison, FA Matt, G Reynolds, CS Stern, D Zhang, WW AF Kara, E. Fabian, A. C. Lohfink, A. M. Parker, M. L. Walton, D. J. Boggs, S. E. Christensen, F. E. Hailey, C. J. Harrison, F. A. Matt, G. Reynolds, C. S. Stern, D. Zhang, W. W. TI The Compton hump and variable blue wing in the extreme low-flux NuSTAR observations of 1H0707-495 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; galaxies: active; galaxies: individual: 1H0707-495; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; X-RAY REVERBERATION; LINE SEYFERT-1 GALAXY-1H-0707-495; ACCRETING BLACK-HOLES; NARROW-LINE; XMM-NEWTON; 1H 0707-495; IRON-K; SPECTRAL VARIABILITY; GALAXY MCG-6-30-15 AB The narrow-line Seyfert I galaxy, 1H0707-495, has been well observed in the 0.3-10 keV band, revealing a dramatic drop in flux in the iron K alpha band, a strong soft excess, and short time-scale reverberation lags associated with these spectral features. In this paper, we present the first results of a deep 250-ks NuSTAR (Nuclear Spectroscopic Telescope Array) observation of 1H0707-495, which includes the first sensitive observations above 10 keV. Even though the NuSTAR observations caught the source in an extreme low-flux state, the Compton hump is still significantly detected. NuSTAR, with its high effective area above 7 keV, clearly detects the drop in flux in the iron Ka band, and by comparing these observations with archival XMM-Newton observations, we find that the energy of this drop increases with increasing flux. We discuss possible explanations for this, the most likely of which is that the drop in flux is the blue wing of the relativistically broadened iron K alpha emission line. When the flux is low, the coronal source height is low, thus enhancing the most gravitationally redshifted emission. C1 [Kara, E.; Fabian, A. C.; Lohfink, A. M.; Parker, M. L.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. [Walton, D. J.; Harrison, F. A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Matt, G.] Univ Rome Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Reynolds, C. S.] Joint Space Sci Inst JSI, College Pk, MD 20742 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kara, E (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 OHA, England. EM ekara@ast.cam.ac.uk RI Boggs, Steven/E-4170-2015 OI Boggs, Steven/0000-0001-9567-4224 FU Gates Cambridge Scholarship; European Union [312789]; Italian Space Agency [ASI/INAF I/037/12/0-011/13]; National Aeronautics and Space Administration (NASA) [NNG08FD60C]; NASA FX EK thanks Javier Garcia and Thomas Dauser for interesting discussions on the RELXILLLP modelling. EK is supported by the Gates Cambridge Scholarship. ACF thanks the Royal Society. EK, ACF, AML, and GM acknowledge support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312789, StrongGravity. AML and GM acknowledge financial support from Italian Space Agency under grant ASI/INAF I/037/12/0-011/13. This work was supported under National Aeronautics and Space Administration (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 NASA. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. NR 50 TC 8 Z9 8 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 1 PY 2015 VL 449 IS 1 BP 234 EP 242 DI 10.1093/mnras/stv304 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2WO UT WOS:000355345600019 ER PT J AU Nemmen, RS Tchekhovskoy, A AF Nemmen, Rodrigo S. Tchekhovskoy, Alexander TI On the efficiency of jet production in radio galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; galaxies: active; galaxies: jets; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE SPIN; RADIATIVELY INEFFICIENT ACCRETION; ADVECTION-DOMINATED ACCRETION; BLANDFORD-ZNAJEK PROCESS; RELATIVISTIC JETS; SAGITTARIUS-A; ELECTROMAGNETIC EXTRACTION; OBSERVATIONAL CONSTRAINTS; NUMERICAL SIMULATIONS AB The mechanisms that produce and power relativistic jets are fundamental open questions in black hole (BH) astrophysics. In order to constrain these mechanisms, we analyse the energy efficiency of jet production eta based on archival Chandra observations of 27 nearby, low-luminosity active galactic nuclei. We obtain eta as the ratio of the jet power, inferred from the energetics of jet powered X-ray emitting cavities, to the BH mass accretion rate. (M) over dot(BH). The standard assumption in estimating (M) over dot(BH) is that all the gas from the Bondi radius r(B) makes it down to the BH. It is now clear, however, that only a small fraction of the gas reaches the hole. To account for this effect, we use the standard disc mass-loss scaling, (M) over dot (r) alpha (r/r(B))(s) (M) over dot(Bondi). This leads to much lower values of (M) over dot(BH) and higher values of eta than in previous studies. If hot accretion flows are characterized by 0.5 <= s <= 0.6 - on the lower end of recent theoretical and observational studies - then dynamically important magnetic fields near rapidly spinning BHs are necessary to account for the high eta approximate to 100-300 per cent in the sample. Moreover, values of s > 0.6 are essentially ruled out, or there would be insufficient energy to power the jets. We discuss the implications of our results for the distribution of massive BH spins and the possible impact of a significant extra cold gas supply on our estimates. C1 [Nemmen, Rodrigo S.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508090 Sao Paulo, SP, Brazil. [Nemmen, Rodrigo S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nemmen, Rodrigo S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Nemmen, Rodrigo S.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA. [Tchekhovskoy, Alexander] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Tchekhovskoy, Alexander] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Tchekhovskoy, Alexander] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. RP Nemmen, RS (reprint author), Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508090 Sao Paulo, SP, Brazil. EM rodrigo.nemmen@iag.usp.br FU NASA Postdoctoral Program (NPP) at Goddard Space Flight Center; NASA [NNH10ZDA001N, NAS8-03060]; FAPESP; NASA through Einstein Postdoctoral Fellowship - Chandra X-ray Center [PF3-140115] FX We acknowledge useful discussions with Mihoko Yukita, Ka-Wah Wong, Aleksander Sadowski, Helen Russell, Jonathan C. McKinney, Jeremy Schnittman, Markos Georganopoulos, Ramesh Narayan, Jeff McClintock, Feng Yuan and Sylvain Guiriec. RSN was partially supported by the NASA Postdoctoral Program (NPP) at Goddard Space Flight Center, administered by Oak Ridge Associated Universities with NASA, as well as the NASA grant NNH10ZDA001N and FAPESP. AT was supported by NASA through Einstein Postdoctoral Fellowship grant number PF3-140115 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060, and NASA support via High-End Computing (HEC) Program through the NASA Advanced Super-computing (NAS) Division at Ames Research Center that provided access to the Pleiades supercomputer, as well as NSF support through an XSEDE computational time allocation TG-AST100040 on NICS Kraken, Nautilus, TACC Stampede, Maverick and Ranch. This project made considerable use of IPYTHON (Perez & Granger 2007) and the ASTROPY and MCERP libraries. NR 114 TC 6 Z9 6 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 1 PY 2015 VL 449 IS 1 BP 316 EP 327 DI 10.1093/mnras/stv260 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2WO UT WOS:000355345600024 ER PT J AU Hensley, B Murphy, E Staguhn, J AF Hensley, Brandon Murphy, Eric Staguhn, Johannes TI Characterizing extragalactic anomalous microwave emission in NGC 6946 with CARMA SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms: general; ISM: general; radio continuum: ISM ID SPINNING DUST EMISSION; ANISOTROPY-PROBE; GALACTIC EMISSION; NEARBY GALAXIES; STAR-FORMATION; IMAGE ATLAS; SPITZER; RADIO; WMAP; CONTINUUM AB Using 1 cm and 3 mm observations from the Combined Array for Research in Millimeter-wave Astronomy and 2 mm observations from the Goddard IRAM Superconducting 2 Millimeter Observer observations, we follow up the first extragalactic detection of anomalous microwave emission (AME) reported by Murphy et al. in an extranuclear region (Enuc. 4) of the nearby face-on spiral galaxy NGC 6946. We find the spectral shape and peak frequency of AME in this region to be consistent with models of spinning dust emission. However, the strength of the emission far exceeds the Galactic AME emissivity given the abundance of polycyclic aromatic hydrocarbons (PAHs) in that region. Using our galaxy-wide 1 cm map (21 arcsec resolution), we identify a total of eight 21 arcsec x 21 arcsec regions in NGC 6946 that harbour AME at > 95 per cent significance at levels comparable to that observed in Enuc. 4. The remainder of the galaxy has 1 cm emission consistent with or below the observed Galactic AME emissivity per PAH surface density. We probe relationships between the detected AME and dust surface density, PAH emission, and radiation field, though no environmental property emerges to delineate regions with strong versus weak or non-existent AME. On the basis of these data and other AME observations in the literature, we determine that the AME emissivity per unit dust mass is highly variable. We argue that the spinning dust hypothesis, which predicts the AME power to be approximately proportional to the PAH mass, is therefore incomplete. C1 [Hensley, Brandon] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Murphy, Eric] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Staguhn, Johannes] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. [Staguhn, Johannes] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hensley, B (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. EM bhensley@princeton.edu OI Hensley, Brandon/0000-0001-7449-4638 FU NSF Graduate Research Fellowship [DGE-0646086]; NSF [AST-1408723]; NSF ATI [1020981, 1106284] FX BH acknowledges support from the NSF Graduate Research Fellowship under Grant no. DGE-0646086 and NSF grant AST-1408723. The GISMO observations and JS were supported through NSF ATI grants 1020981 and 1106284. NR 54 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 MAY 1 PY 2015 VL 449 IS 1 BP 809 EP 819 DI 10.1093/mnras/stv287 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2WO UT WOS:000355345600059 ER PT J AU De Pasquale, M Kuin, NPM Oates, S Schulze, S Cano, Z Guidorzi, C Beardmore, A Evans, PA Uhm, ZL Zhang, B Page, M Kobayashi, S Castro-Tirado, A Gorosabel, J Sakamoto, T Fatkhullin, T Pandey, SB Im, M Chandra, P Frail, D Gao, H Kopac, D Jeon, Y Akerlof, C Huang, KY Pak, S Park, WK Gomboc, A Melandri, A Zane, S Mundell, CG Saxton, CJ Holland, ST Virgili, F Urata, Y Steele, I Bersier, D Tanvir, N Sokolov, VV Moskvitin, AS AF De Pasquale, Massimiliano Kuin, N. P. M. Oates, S. Schulze, S. Cano, Z. Guidorzi, C. Beardmore, A. Evans, P. A. Uhm, Z. L. Zhang, B. Page, M. Kobayashi, S. Castro-Tirado, A. Gorosabel, J. Sakamoto, T. Fatkhullin, T. Pandey, S. B. Im, M. Chandra, P. Frail, D. Gao, H. Kopac, D. Jeon, Y. Akerlof, C. Huang, K. Y. Pak, S. Park, W. -K. Gomboc, A. Melandri, A. Zane, S. Mundell, C. G. Saxton, C. J. Holland, S. T. Virgili, F. Urata, Y. Steele, I. Bersier, D. Tanvir, N. Sokolov, V. V. Moskvitin, A. S. TI The optical rebrightening of GRB100814A: an interplay of forward and reverse shocks? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanism: non-thermal; shock waves; gamma-ray burst: general ID GAMMA-RAY BURST; AFTERGLOW LIGHT CURVES; CONTINUOUS ENERGY INJECTION; RELATIVISTIC BLAST WAVES; SWIFT XRT DATA; X-RAY; JET BREAKS; THEORETICAL IMPLICATIONS; COMPREHENSIVE ANALYSIS; PHOTOMETRIC SYSTEM AB We present a wide data set of gamma-ray, X-ray, UV/Opt/IR (UVOIR), and radio observations of the Swift GRB100814A. At the end of the slow decline phase of the X-ray and optical afterglow, this burst shows a sudden and prominent rebrightening in the optical band only, followed by a fast decay in both bands. The optical rebrightening also shows chromatic evolution. Such a puzzling behaviour cannot be explained by a single component model. We discuss other possible interpretations, and we find that a model that incorporates a long-lived reverse shock and forward shock fits the temporal and spectral properties of GRB100814 the best. C1 [De Pasquale, Massimiliano; Kuin, N. P. M.; Oates, S.; Page, M.; Zane, S.; Saxton, C. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [De Pasquale, Massimiliano; Uhm, Z. L.; Zhang, B.; Gao, H.] Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. [De Pasquale, Massimiliano] INAF IASF, I-90146 Palermo, Italy. [Oates, S.; Castro-Tirado, A.; Gorosabel, J.] Inst Astrofis Andalucia CSIC, E-18080 Granada, Spain. [Schulze, S.; Cano, Z.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland. [Schulze, S.] Pontificia Univ Catolica Chile, Dept Astronom & Astrofis, Santiago 22, Chile. [Schulze, S.] Millennium Inst Astrophys, Santiago 7820436, Chile. [Cano, Z.; Kopac, D.; Mundell, C. G.; Virgili, F.; Steele, I.; Bersier, D.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Guidorzi, C.] Univ Ferrara, Dept Phys & Earth Sci, I-44122 Ferrara, Italy. [Beardmore, A.; Evans, P. A.; Kobayashi, S.; Tanvir, N.] Univ Leicester, Leicester LE1 7RH, Leics, England. [Gorosabel, J.] Basque Fdn Sci, Ikerbasque, E-48008 Bilbao, Spain. [Gorosabel, J.] Univ Pais Vasco UPV EHU, Unidad Asociada Grp Ciencia Planetarias UPV EHU I, Dept Fis Aplicada 1, ETS Ingn, E-48013 Bilbao, Spain. [Sakamoto, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fatkhullin, T.; Sokolov, V. V.; Moskvitin, A. S.] Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz 369167, Russia. [Pandey, S. B.] ARIES, Naini Tal 263129, Uttarakhand, India. [Im, M.; Jeon, Y.; Park, W. -K.] Seoul Natl Univ, FPRD, Dept Phys & Astron, CEOU Astron Program, Seoul 151742, South Korea. [Chandra, P.] Pune Univ, Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Frail, D.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Akerlof, C.] Univ Michigan, Ann Arbor, MI 48109 USA. [Huang, K. Y.] Natl Taiwan Normal Univ, Dept Math & Sci, New Taipei City 24449, Taiwan. [Pak, S.] Kyung Hee Univ, Yongin 446701, Gyeonggi Do, South Korea. [Park, W. -K.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Gomboc, A.] Univ Ljubljana, Fac Math & Phys, SI-1000 Ljubljana, Slovenia. [Gomboc, A.] Ctr Excellence Space SI, SI-1000 Ljubljana, Slovenia. [Melandri, A.] INAF Brera Astron Observ, I-23807 Merate, LC, Italy. [Saxton, C. J.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. [Holland, S. T.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Urata, Y.] Natl Cent Univ, Insti Astron, Chungli 32054, Taiwan. RP De Pasquale, M (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM m.depasquale@ucl.ac.uk OI Castro-Tirado, A. J./0000-0003-2999-3563; Im, Myungshin/0000-0002-8537-6714; Schulze, Steve/0000-0001-6797-1889 FU United Kingdom Space Agency (UKSA); Royal Society; Wolfson Foundation; Science and Technology Facilities Council (STFC); STFC; UKSA; Slovenian Research Agency; Centre of Excellence for Space Sciences and Technologies SPACE-SI; European Union; European Regional Development Fund; Republic of Slovenia; Creative Initiative programme of the National Research Foundation of Korea (NRF) - Korea government (MSIP) [2008-0060544]; Grant of Excellence from the Icelandic; Iniciativa Cientifica Milenio (Millennium Center for Supernova Science) [P10-064-F]; Basal-CATA [PFB-06/2007]; 'Fondo de Innovacion para la Competitividad, del Ministerio de Economia, Fomento y Turismo de Chile'; Dill Faulkes Educational Trust FX MDP, MJP, NPK, and SRO acknowledge United Kingdom Space Agency (UKSA) funding. MDP thanks M. A. Aloy, F. Daigne, and A. Mizuta for insightful discussions at 'Supernovae and Gamma-Ray Burst 2013' conference, Kyoto. CGM thanks the Royal Society, the Wolfson Foundation and the Science and Technology Facilities Council (STFC) for support. FG acknowledges support from STFC. APB and PAE acknowledge UKSA support. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. AG acknowledges funding from the Slovenian Research Agency and from the Centre of Excellence for Space Sciences and Technologies SPACE-SI, an operation partly financed by the European Union, European Regional Development Fund and Republic of Slovenia. MI, YJ, and S. Pak acknowledge the support from the Creative Initiative programme, grant No. 2008-0060544 of the National Research Foundation of Korea (NRF), funded by the Korea government (MSIP). SS acknowledges financial support from support by a Grant of Excellence from the Icelandic and the Iniciativa Cientifica Milenio grant P10-064-F (Millennium Center for Supernova Science), with input from 'Fondo de Innovacion para la Competitividad, del Ministerio de Economia, Fomento y Turismo de Chile', and Basal-CATA (PFB-06/2007). The Liverpool Telescope is operated by Liverpool John Moores University at the Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The Faulkes Telescopes, now owned by the Las Cumbres Observatory Global Telescope network, are operated with support from the Dill Faulkes Educational Trust. NR 100 TC 5 Z9 5 U1 0 U2 9 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 MAY 1 PY 2015 VL 449 IS 1 BP 1024 EP 1042 DI 10.1093/mnras/stv267 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2WO UT WOS:000355345600074 ER PT J AU Arbabi, A Horie, Y Ball, AJ Bagheri, M Faraon, A AF Arbabi, Amir Horie, Yu Ball, Alexander J. Bagheri, Mahmood Faraon, Andrei TI Subwavelength-thick lenses with high numerical apertures and large efficiency based on high-contrast transmitarrays SO NATURE COMMUNICATIONS LA English DT Article ID MICRO-FRESNEL LENSES; GRATING REFLECTORS; ORDER GRATINGS; METASURFACES; ELEMENTS; MIRROR; NM AB Flat optical devices thinner than a wavelength promise to replace conventional free-space components for wavefront and polarization control. Transmissive flat lenses are particularly interesting for applications in imaging and on-chip optoelectronic integration. Several designs based on plasmonic metasurfaces, high-contrast transmitarrays and gratings have been recently implemented but have not provided a performance comparable to conventional curved lenses. Here we report polarization-insensitive, micron-thick, high-contrast transmitarray micro-lenses with focal spots as small as 0.57 lambda. The measured focusing efficiency is up to 82%. A rigorous method for ultrathin lens design, and the trade-off between high efficiency and small spot size (or large numerical aperture) are discussed. The micro-lenses, composed of silicon nano-posts on glass, are fabricated in one lithographic step that could be performed with high-throughput photo or nanoimprint lithography, thus enabling widespread adoption. C1 [Arbabi, Amir; Horie, Yu; Ball, Alexander J.; Faraon, Andrei] CALTECH, Thomas J Watson Lab Appl Phys, Pasadena, CA 91125 USA. [Bagheri, Mahmood] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Faraon, A (reprint author), CALTECH, Thomas J Watson Lab Appl Phys, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM faraon@caltech.edu FU Caltech/JPL president and director fund (PDF); DARPA; JASSO; 'Light-Material Interactions in Energy Conversion' Energy Frontier Research Center - US Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-SC0001293]; Summer Undergraduate Research Fellowship (SURF) at Caltech FX This work was supported by the Caltech/JPL president and director fund (PDF). A.A. was also supported by DARPA. Y.H. was supported by the JASSO fellowship and the 'Light-Material Interactions in Energy Conversion' Energy Frontier Research Center funded by the US Department of Energy, Office of Science, Office of Basic Energy Sciences under Award no. DE-SC0001293. Alexander Ball was supported by the Summer Undergraduate Research Fellowship (SURF) at Caltech. The device nanofabrication was performed in the Kavli Nanoscience Institute at Caltech. We thank David Fattal and Sonny Vo for useful discussion. NR 33 TC 53 Z9 54 U1 13 U2 56 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD MAY PY 2015 VL 6 AR 7069 DI 10.1038/ncomms8069 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CJ5MG UT WOS:000355531100005 PM 25947118 ER PT J AU Georgiou, CD Sun, HJ Mckay, CP Grintzalis, K Papapostolou, I Zisimopoulos, D Panagiotidis, K Zhang, GS Koutsopoulou, E Christidis, GE Margiolaki, I AF Georgiou, Christos D. Sun, Henry J. Mckay, Christopher P. Grintzalis, Konstantinos Papapostolou, Ioannis Zisimopoulos, Dimitrios Panagiotidis, Konstantinos Zhang, Gaosen Koutsopoulou, Eleni Christidis, George E. Margiolaki, Irene TI Evidence for photochemical production of reactive oxygen species in desert soils SO NATURE COMMUNICATIONS LA English DT Article ID SINGLET OXYGEN; ATACAMA DESERT; MARTIAN SOIL; MOLECULAR-OXYGEN; OXIDE SURFACES; HYDROGEN-PEROXIDE; SUPEROXIDE IONS; MOJAVE-DESERT; PERCHLORATE; TIO2 AB The combination of intense solar radiation and soil desiccation creates a short circuit in the biogeochemical carbon cycle, where soils release significant amounts of CO2 and reactive nitrogen oxides by abiotic oxidation. Here we show that desert soils accumulate metal superoxides and peroxides at higher levels than non-desert soils. We also show the photogeneration of equimolar superoxide and hydroxyl radical in desiccated and aqueous soils, respectively, by a photo-induced electron transfer mechanism supported by their mineralogical composition. Reactivity of desert soils is further supported by the generation of hydroxyl radical via aqueous extracts in the dark. Our findings extend to desert soils the photogeneration of reactive oxygen species by certain mineral oxides and also explain previous studies on desert soil organic oxidant chemistry and microbiology. Similar processes driven by ultraviolet radiation may be operating in the surface soils on Mars. C1 [Georgiou, Christos D.; Grintzalis, Konstantinos; Papapostolou, Ioannis; Zisimopoulos, Dimitrios; Panagiotidis, Konstantinos; Margiolaki, Irene] Univ Patras, Dept Biol, Patras 26504, Greece. [Sun, Henry J.] Desert Res Inst, Las Vegas, NV 89119 USA. [Mckay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Zhang, Gaosen] Chinese Acad Sci, Cold & Arid Reg Environm & Engn Res Inst, Lanzhou 73000, Peoples R China. [Koutsopoulou, Eleni] Univ Patras, Lab Elect Microscopy & Microanal, Patras 26500, Greece. [Christidis, George E.] Tech Univ Crete, Dept Mineral Resources Engn, Khania 73100, Greece. RP Georgiou, CD (reprint author), Univ Patras, Dept Biol, Patras 26504, Greece. EM c.georgiou@upatras.gr RI Georgiou, Christos/B-8354-2013; Grintzalis, Konstantinos/I-5124-2014 OI Georgiou, Christos/0000-0001-9707-0109; Grintzalis, Konstantinos/0000-0002-6276-495X FU Greek Ministry of Education; NASA Astrobiology Program [NNX07AT65]; National Science Foundation [IIA-1301726]; NASA Planetary Protection Program FX C.D.G. was financially supported by the Greek Ministry of Education. H.J.S. and G.Z. were supported by a grant from the NASA Astrobiology Program NNX07AT65. H.J.S was also in part supported by the National Science Foundation under grant number IIA-1301726. He thanks R. Kreidberg for editorial assistance. C.P.M. acknowledges the support from the NASA Planetary Protection Program. We thank the ESRF for the provision of synchrotron X-ray beamtime at the high-resolution powder diffraction beamline (ID31). We are grateful to Professor P.V. Ioannou (Department of Chemistry) and Associate Professor M. Kornaros (Department of Chemical Engineering) at the University of Patras, Greece, for HTPA synthesis and HPLC-MS identification in samples, respectively. NR 70 TC 5 Z9 5 U1 12 U2 53 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD MAY PY 2015 VL 6 AR 7100 DI 10.1038/ncomms8100 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CJ5MN UT WOS:000355531800001 PM 25960012 ER PT J AU Mostl, C Rollett, T Frahm, RA Liu, YD Long, DM Colaninno, RC Reiss, MA Temmer, M Farrugia, CJ Posner, A Dumbovic, M Janvier, M Demoulin, P Boakes, P Devos, A Kraaikamp, E Mays, ML Vrsnak, B AF Mostl, Christian Rollett, Tanja Frahm, Rudy A. Liu, Ying D. Long, David M. Colaninno, Robin C. Reiss, Martin A. Temmer, Manuela Farrugia, Charles J. Posner, Arik Dumbovic, Mateja Janvier, Miho Demoulin, Pascal Boakes, Peter Devos, Andy Kraaikamp, Emil Mays, Mona L. Vrsnak, Bojan TI Strong coronal channelling and interplanetary evolution of a solar storm up to Earth and Mars SO NATURE COMMUNICATIONS LA English DT Article ID IN-SITU OBSERVATIONS; MASS EJECTIONS; MAGNETIC CLOUD; ARRIVAL TIMES; WIND; PROPAGATION; SHOCK; CMES; SUN; DEFLECTION AB The severe geomagnetic effects of solar storms or coronal mass ejections (CMEs) are to a large degree determined by their propagation direction with respect to Earth. There is a lack of understanding of the processes that determine their non-radial propagation. Here we present a synthesis of data from seven different space missions of a fast CME, which originated in an active region near the disk centre and, hence, a significant geomagnetic impact was forecasted. However, the CME is demonstrated to be channelled during eruption into a direction + 37 +/- 10 degrees (longitude) away from its source region, leading only to minimal geomagnetic effects. In situ observations near Earth and Mars confirm the channelled CME motion, and are consistent with an ellipse shape of the CME-driven shock provided by the new Ellipse Evolution model, presented here. The results enhance our understanding of CME propagation and shape, which can help to improve space weather forecasts. C1 [Mostl, Christian; Rollett, Tanja] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria. [Mostl, Christian; Reiss, Martin A.; Temmer, Manuela; Boakes, Peter] Graz Univ, Inst Phys, IGAM Kanzelhohe Observ, A-8010 Graz, Austria. [Frahm, Rudy A.] Southwest Res Inst, San Antonio, TX 78238 USA. [Liu, Ying D.] Chinese Acad Sci, Natl Space Sci Ctr, State Key Lab Space Weather, Beijing 100190, Peoples R China. [Long, David M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Colaninno, Robin C.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Farrugia, Charles J.] Univ New Hampshire, Dept Phys, Ctr Space Sci, Durham, NH 03824 USA. [Posner, Arik] NASA Headquarters, Washington, DC 20546 USA. [Dumbovic, Mateja; Vrsnak, Bojan] Univ Zagreb, Fac Geodesy, Hvar Observ, Zagreb 10000, Croatia. [Janvier, Miho] Univ Dundee, Dept Math, Dundee DD1 4HN, Scotland. [Demoulin, Pascal] CNRS, UMR 8109, LESIA, Observ Paris, F-92195 Meudon, France. [Devos, Andy; Kraaikamp, Emil] Royal Observ Belgium, Solar Terr Ctr Excellence SIDC, B-1180 Brussels, Belgium. [Mays, Mona L.] Catholic Univ Amer, Washington, DC 20064 USA. [Mays, Mona L.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP Mostl, C (reprint author), Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria. EM christian.moestl@oeaw.ac.at RI Long, David/J-3227-2013; OI Long, David/0000-0003-3137-0277; Dumbovic, Mateja/0000-0002-8680-8267; Demoulin, Pascal/0000-0001-8215-6532; Liu, Ying/0000-0002-3483-5909 FU Austrian Science Fund (FWF) [P26174-N27, V195-N16]; Leverhulme Trust; Croatian Science Foundation [6212]; Recruitment Program of Global Experts of China; NSFC [41374173]; Specialized Research Fund for State Key Laboratories of China; European Union Seventh Framework Programme (FP7) [606692, 284461]; NASA [NNX13AP39G, NNX10AQ29G, NASW-00003]; STEREO Farside Grant; National Aeronautics and Space Administration (NASA, HEOMD) under Jet Propulsion Laboratory (JPL) [1273039]; DLR and DLR's Space Administration [50QM0501, 50QM1201]; Belgian Federal Science Policy Office through the ESA-PRODEX program [4000103240]; European Commission's Seventh Framework Programme (FP7) [263506, 263252] FX This study was supported by the Austrian Science Fund (FWF): [P26174-N27, V195-N16]. T.R. gratefully acknowledges the JungforscherInnenfonds of the Council of the University Graz. D.M.L. is a Leverhulme Early-Career Fellow funded by the Leverhulme Trust. M.D. and B.V. acknowledge financial support by the Croatian Science Foundation under the project 6212 SOLSTEL. Y.D.L. was supported by the Recruitment Program of Global Experts of China, NSFC under grant 41374173 and the Specialized Research Fund for State Key Laboratories of China. The presented work has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 606692 [HELCATS] and No. 284461 [eHEROES]. Part of this work was supported by NASA grants NNX13AP39G, NNX10AQ29G and STEREO Farside Grant to UNH. MEX/ASPERA-3 is supported in the United States of America by NASA contract NASW-00003. RAD is supported by the National Aeronautics and Space Administration (NASA, HEOMD) under Jet Propulsion Laboratory (JPL) subcontract #1273039 to the Southwest Research Institute and in Germany by DLR and DLR's Space Administration grant numbers 50QM0501 and 50QM1201 to the Christian Albrechts University, Kiel. A.D. acknowledges support from the Belgian Federal Science Policy Office through the ESA-PRODEX program, grant No. 4000103240. E.K. acknowledges support from the European Commission's Seventh Framework Programme (FP7/2007-2014) under the grant agreement nr. 263506 (AFFECTS project), and grant agreement nr. 263252 (COMESEP project). This research has made use of the Heliophysics Event Knowledge database and the ESA JHelioviewer software. We thank Janet G. Luhmann and Julia K. Thalmann for discussions, and the Center for Geomagnetism in Kyoto for providing the Dst indices. NR 63 TC 20 Z9 20 U1 0 U2 5 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD MAY PY 2015 VL 6 AR 7135 DI 10.1038/ncomms8135 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CJ5MZ UT WOS:000355533300005 PM 26011032 ER PT J AU Dunning, PD Stanford, BK Kim, HA AF Dunning, Peter D. Stanford, Bret K. Kim, H. Alicia TI Coupled aerostructural topology optimization using a level set method for 3D aircraft wings SO STRUCTURAL AND MULTIDISCIPLINARY OPTIMIZATION LA English DT Article DE Level set method; 3D unstructured mesh; Topology optimization; Multi-disciplinary optimization ID STRUCTURAL OPTIMIZATION; SENSITIVITY; DESIGN; VEHICLES; FEM AB The purpose of this work is to develop a level set topology optimization method for an unstructured three-dimensional mesh and apply it to wing box design for coupled aerostructural considerations. The paper develops fast marching and upwind schemes suitable for unstructured meshes, which make the level set method robust and efficient. The method is applied to optimize a representative wing box internal structure for the NASA Common Research Model. The objective is to minimize the total compliance of the wing box. The trim condition that aerodynamic lift must balance the total weight of the aircraft is enforced by allowing the root angle of attack to change. The adjoint method is used to obtain the coupled shape sensitivities required to perform aerostructural optimization of the wing box. Optimum solutions for several aerodynamic and body force load cases, as well as a ground load case, are presented. C1 [Dunning, Peter D.] Natl Inst Aerosp, Hampton, VA 23666 USA. [Stanford, Bret K.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Kim, H. Alicia] Univ Bath, Bath BA2 7AY, Avon, England. RP Dunning, PD (reprint author), Natl Inst Aerosp, Hampton, VA 23666 USA. EM en2pdd@bath.ac.uk OI Kim, Hyunsun Alicia/0000-0002-5629-2466; Dunning, Peter/0000-0002-7645-7598 FU Fixed Wing project under the National Aeronautics and Space Administration's (NASA) Fundamental Aeronautics Program FX This work is funded by the Fixed Wing project under the National Aeronautics and Space Administration's (NASA) Fundamental Aeronautics Program. The authors would like to thank Dr. Maxwell Blair for his example DLM code and the Numerical Analysis Group at the Rutherford Appleton Laboratory for their FORTRAN HSL packages (HSL, a collection of Fortran codes for large-scale scientific computation. See http://www.hsl.rl.ac.uk/). NR 44 TC 5 Z9 5 U1 3 U2 23 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1615-147X EI 1615-1488 J9 STRUCT MULTIDISCIP O JI Struct. Multidiscip. Optim. PD MAY PY 2015 VL 51 IS 5 BP 1113 EP 1132 DI 10.1007/s00158-014-1200-1 PG 20 WC Computer Science, Interdisciplinary Applications; Engineering, Multidisciplinary; Mechanics SC Computer Science; Engineering; Mechanics GA CJ8NP UT WOS:000355760000010 ER PT J AU Montanaro, M Gerace, A Rohrbach, S AF Montanaro, Matthew Gerace, Aaron Rohrbach, Scott TI Toward an operational stray light correction for the Landsat 8 Thermal Infrared Sensor SO APPLIED OPTICS LA English DT Article ID RADIOMETRIC CALIBRATION; SURFACE TEMPERATURE; TIRS AB The Thermal Infrared Sensor (TIRS) onboard Landsat 8 was tasked with continuing thermal band measurements of Earth as part of the Landsat program. From first light in early 2013, there were obvious indications, such as non-uniform banding and varying absolute calibration errors, that stray light was contaminating the thermal image data collected from the instrument. Stray light in this case refers to unwanted radiance from outside the field-of-view entering the optical system and being recorded by the focal plane. Standard calibration techniques used to flat-field and radiometrically correct the data were not sufficient to adjust the image products to within the accuracy that the Landsat community has come to expect. The development of an operational technique to remove the effects of the stray light in the TIRS data has become a high priority. A methodology is presented that makes use of a stray light optical model developed for the instrument along with knowledge of the out-of-field area surrounding the TIRS earth scene. Two versions of the algorithm are proposed in which one method utilizes near-coincident image data from an external sensor while another novel method is proposed that makes use of TIRS image data itself without the need for external data. Preliminary results of the algorithm indicate that banding artifacts due to stray light are significantly reduced when the methods are applied. Additionally, initial absolute calibration error estimates of over 9K are reduced to within 2K when applying the correction methods. Although both variations of the proposed algorithm have significantly reduced the stray light effects, the fact that the latter method utilizing TIRS image data itself does not rely on any external data is a significant advantage toward the development of an operational stray light correction solution. Ongoing work is focused on operationalizing the algorithm and identifying and quantifying potential sources of error when applying the method. (C) 2015 Optical Society of America C1 [Montanaro, Matthew; Gerace, Aaron] Rochester Inst Technol, Rochester, NY 14623 USA. [Rohrbach, Scott] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Montanaro, M (reprint author), Rochester Inst Technol, 54 Lomb Mem Dr, Rochester, NY 14623 USA. EM montanaro@cis.rit.edu FU Goddard Space Flight Center (GSFC), National Aeronautics and Space Administration (NASA) [NNG09HP18C, NNX09AQ57A, NNX14AP40G] FX Goddard Space Flight Center (GSFC), National Aeronautics and Space Administration (NASA) (NNG09HP18C, NNX09AQ57A,NNX14AP40G). NR 16 TC 4 Z9 4 U1 0 U2 7 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD MAY 1 PY 2015 VL 54 IS 13 BP 3963 EP 3978 DI 10.1364/AO.54.003963 PG 16 WC Optics SC Optics GA CH4DC UT WOS:000353980900037 ER PT J AU Zhai, PW Hu, YX Trepte, CR Winker, DM Lucker, PL Lee, ZP Josset, DB AF Zhai, Peng-Wang Hu, Yongxiang Trepte, Charles R. Winker, David M. Lucker, Patricia L. Lee, Zhongping Josset, Damien B. TI Uncertainty in the bidirectional reflectance model for oceanic waters SO APPLIED OPTICS LA English DT Article ID ATMOSPHERIC CORRECTION; COLOR IMAGERY; DIFFUSE-REFLECTANCE; LEAVING RADIANCE; PHASE FUNCTION; DETAILED VALIDATION; COUPLED ATMOSPHERE; LIGHT-SCATTERING; SEAWIFS IMAGERY; MUELLER MATRIX AB We study the impacts of the bio-optical model variations on the angular distribution (f/Q factor) of the upwelling radiance field in ocean waters. An ocean water bio-optical model has been combined with a vector radiative transfer model to calculate the f/Q factors systematically. The f/Q factors are compared to those in [Appl. Opt. 41, 6289 (2002)] and the differences are found to be within +/- 10% for 81% of the total number of cases covering all wavelengths, chlorophyll a concentrations, and solar and viewing geometries. The differences are attributed to the choice of ocean water scattering function and scattering coefficient biases. In addition, we study the uncertainty of f/Q factor due to three factors: (I) the absorption coefficient of the colored dissolved organic matter (CDOM), (II) the particle scattering coefficient, and (III) the ocean water depolarization. The impacts of ocean water depolarization on the f/Q variation is found to be negligible. If we perturb the CDOM absorption coefficient by a factor ranging from 0.1 to 10, the f/Q values vary within +/- 5% of the average behavior of ocean waters for 93% of the cases. If we perturb the scattering coefficients by a factor ranging from 0.5 to 2.0, the f/Q variation is within +/- 5% for 81% of the cases studied. This work contributes to understanding the uncertainty of ocean color remote sensing. (C) 2015 Optical Society of America C1 [Zhai, Peng-Wang] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. [Hu, Yongxiang; Trepte, Charles R.; Winker, David M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Lucker, Patricia L.] NASA, Langley Res Ctr, SSAI, Hampton, VA 23681 USA. [Lee, Zhongping] Univ Massachusetts, Sch Environm, Boston, MA 02125 USA. [Josset, Damien B.] NRL SSC, Stennis Space Ctr, MS 39529 USA. RP Zhai, PW (reprint author), Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. EM pwzhai@umbc.edu RI Hu, Yongxiang/K-4426-2012 FU NASA Radiation Science Program FX This work was supported by the NASA Radiation Science Program administrated by Hal Maring and the Biogeochemistry Program administrated by Paula Bontempi. We appreciate the three anonymous reviewers for their constructive comments. NR 50 TC 4 Z9 4 U1 2 U2 8 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD MAY 1 PY 2015 VL 54 IS 13 BP 4061 EP 4069 DI 10.1364/AO.54.004061 PG 9 WC Optics SC Optics GA CH4DC UT WOS:000353980900048 ER PT J AU Saif, B Chaney, D Smith, WS Greenfield, P Hack, W Bluth, J Van Otten, A Bluth, M Sanders, J Keski-Kuha, R Feinberg, L North-Morris, M Millerd, J AF Saif, Babak Chaney, David Smith, W. Scott Greenfield, Perry Hack, Warren Bluth, Josh Van Otten, Austin Bluth, Marcel Sanders, James Keski-Kuha, Ritva Feinberg, Lee North-Morris, Michael Millerd, James TI Nanometer level characterization of the James Webb Space Telescope optomechanical systems using high-speed interferometry SO APPLIED OPTICS LA English DT Article AB The James Webb Space Telescope (JWST) Optical Telescope Element is a three mirror anastigmat consisting of a 6.5 m segmented primary mirror (PM), a secondary mirror, and a tertiary mirror. The primary mirror comprises 18 individual hexagonal segments. The telescope and instruments will be assembled at Goddard Space Flight Center (GSFC) to build the Optical Telescope Element-Integrated Science Instrument Module (OTIS). While at GSFC, the OTIS will go through a series of environmental tests. In these tests the OTIS will be exposed to launch level acoustics and vibrations. To assure that OTIS's performance has not changed due to these environmental tests, the assembly will be tested optically at the center of curvature of the PM. A high-speed interferometer has been designed and built to characterize both static and dynamic changes due to environmental exposure. This paper describes the details of these measurement techniques. To validate and develop the techniques that will be used on OTIS assembly two spare JWST PM segments were measured and the results presented here. (C) 2015 Optical Society of America C1 [Saif, Babak; Keski-Kuha, Ritva; Feinberg, Lee] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Chaney, David] Ball Aerosp & Technol Corp, Boulder, CO 80301 USA. [Smith, W. Scott] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Greenfield, Perry; Hack, Warren] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Bluth, Josh; Van Otten, Austin; Bluth, Marcel] ATK Space Syst, Magna, UT 84044 USA. [Sanders, James] GSFC Vantage Syst Inc, Lanham, MD 20706 USA. [North-Morris, Michael; Millerd, James] 4D Technol, Tucson, AZ 85706 USA. RP Millerd, J (reprint author), 4D Technol, 3280 E Hemisphere Loop,Ste 146, Tucson, AZ 85706 USA. EM james.millerd@4dtechnology.com FU NASA's James Webb Space Telescope project FX NASA's James Webb Space Telescope project. NR 5 TC 2 Z9 2 U1 2 U2 8 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD MAY 1 PY 2015 VL 54 IS 13 BP 4285 EP 4298 DI 10.1364/AO.54.004285 PG 14 WC Optics SC Optics GA CH4DC UT WOS:000353980900080 ER PT J AU Gundy-Burlet, K AF Gundy-Burlet, Karen TI The Use of Standards on the LADEE Mission SO COMPUTER LA English DT Article AB The Lunar Atmosphere Dust Environment Explorer (LADEE) software developers incorporated IEEE and other standards to achieve high reliability while adhering to strict budget and schedule guidelines. C1 NASA, Washington, DC 20546 USA. RP Gundy-Burlet, K (reprint author), NASA, Washington, DC 20546 USA. EM karen.gundy-burlet@nasa.gov NR 4 TC 0 Z9 0 U1 1 U2 2 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 0018-9162 EI 1558-0814 J9 COMPUTER JI Computer PD MAY PY 2015 VL 48 IS 5 BP 92 EP 95 PG 4 WC Computer Science, Hardware & Architecture; Computer Science, Software Engineering SC Computer Science GA CJ0WV UT WOS:000355201000018 ER PT J AU Yasumiishi, EM Criddle, KR Hillgruber, N Mueter, FJ Helle, JH AF Yasumiishi, Ellen M. Criddle, Keith R. Hillgruber, Nicola Mueter, Franz J. Helle, John H. TI Chum salmon (Oncorhynchus keta) growth and temperature indices as indicators of the year-class strength of age-1 walleye pollock (Gadus chalcogrammus) in the eastern Bering Sea SO FISHERIES OCEANOGRAPHY LA English DT Article DE indicators; recruitment; salmon; walleye pollock ID OSCILLATING CONTROL HYPOTHESIS; NORTH PACIFIC-OCEAN; THERAGRA-CHALCOGRAMMA; PINK SALMON; CLIMATE-CHANGE; SOCKEYE-SALMON; BRISTOL BAY; ENVIRONMENT; VARIABILITY; GORBUSCHA AB Ecosystem-based fisheries management requires the development of physical and biological time series that index ocean productivity for stock assessment and recruitment forecasts for commercially important species. As recruitment in marine fish is related to ocean condition, we developed proxies for ocean conditions based on sea surface temperature (SST) and biometric measurements of chum salmon (Oncorhynchus keta) captured in the walleye pollock (Gadus chalcogrammus) fishery in the eastern Bering Sea in three periods (July 16-30, September 1-15 and September 16-30). The main purpose of this paper was to evaluate Pacific salmon (Oncorhynchus spp.) growth as a possible indicator of ocean conditions that, in turn, may affect age-1 walleye pollock recruitment. Marine growth rates of Pacific salmon are the result of a complex interplay of physical, biological and population-based factors that fish experience as they range through oceanic habitats. These growth rates can, therefore, be viewed as indicators of recent ocean productivity. Thus, our hypothesis was that estimated intra-annual growth in body weight of immature and maturing age-4 male and female chum salmon may be used as a biological indicator of variations in rearing conditions also experienced by age-0 walleye pollock; consequently, they may be used to predict the recruitment to age-1 in walleye pollock. Summer SSTs and chum salmon growth at the end of July and September explained the largest amount of variability in walleye pollock recruitment indicating that physical and biological indices of ocean productivity can index fish recruitment. C1 [Yasumiishi, Ellen M.; Criddle, Keith R.; Hillgruber, Nicola; Mueter, Franz J.; Helle, John H.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Juneau, AK 99801 USA. [Yasumiishi, Ellen M.] NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv,Ted Stevens Marine Res, Juneau, AK 99801 USA. [Hillgruber, Nicola] Thunen Inst Fisheries Ecol, D-22926 Ahrensburg, Germany. RP Yasumiishi, EM (reprint author), Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, 17101 Point Lena Loop Rd, Juneau, AK 99801 USA. EM ellen.yasumiishi@noaa.gov RI Criddle, Keith/P-7080-2016 OI Criddle, Keith/0000-0001-9347-2944 FU Auke Bay Laboratories; National Marine Fisheries, National Oceanic and Atmospheric Administration (NOAA); NOAA Advanced Studies Program, Professional Development program FX Funding for this project was provided by the Auke Bay Laboratories, National Marine Fisheries, National Oceanic and Atmospheric Administration (NOAA) and the NOAA Advanced Studies Program, Professional Development program. We greatly appreciate the time and effort to collect samples made by the observers onboard the commercial fishing vessels. We also thank the anonymous reviewers for their comments. NR 52 TC 0 Z9 0 U1 2 U2 9 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1054-6006 EI 1365-2419 J9 FISH OCEANOGR JI Fish Oceanogr. PD MAY PY 2015 VL 24 IS 3 BP 242 EP 256 DI 10.1111/fog.12108 PG 15 WC Fisheries; Oceanography SC Fisheries; Oceanography GA CJ1WH UT WOS:000355275100004 ER PT J AU Brune, AJ West, TK Hosder, S Edquist, KT AF Brune, Andrew J. West, Thomas K. Hosder, Serhat Edquist, Karl T. TI Uncertainty Analysis of Mars Entry Flows over a Hypersonic Inflatable Aerodynamic Decelerator SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID POLYNOMIAL CHAOS; SENSITIVITY-ANALYSIS; EARTH ENTRY AB A detailed uncertainty analysis for high-fidelity flowfield simulations over a fixed aeroshell of hypersonic inflatable aerodynamic decelerator scale for Mars entry is presented for fully laminar and turbulent flows at peak stagnation-point heating conditions. This study implements a sparse-collocation approach based on stochastic expansions for efficient and accurate uncertainty quantification under a large number of uncertainty sources in the computational model. The convective and radiative heating and shear stress uncertainties are computed over the hypersonic inflatable aerodynamic decelerator surface and are shown to vary due to a small fraction of 65 flowfield and radiation modeling parameters considered in the uncertainty analysis. The main contributors to the convective heating uncertainty near the stagnation point are the CO2-CO2, CO2-O, and CO-O binary collision interactions, freestream density, and freestream velocity for both boundary-layer flows. In laminar flow, exothermic recombination reactions are more important at the shoulder. The main contributors to radiative heating at the nose and flank were the CO2 dissociation rate and CO heavy-particle excitation rates, whereas the freestream density showed importance toward the shoulder. The CO2-CO2 interaction and freestream velocity and density control the wall shear stress uncertainty. C1 [Brune, Andrew J.; West, Thomas K.] Missouri Univ Sci & Technol, Dept Aerosp & Mech Engn, Rolla, MO 65409 USA. [Hosder, Serhat] Missouri Univ Sci & Technol, Dept Aerosp & Mech Engn, Aerosp Engn, Rolla, MO 65409 USA. [Edquist, Karl T.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Engn Directorate, Hampton, VA 23681 USA. RP Brune, AJ (reprint author), Missouri Univ Sci & Technol, Dept Aerosp & Mech Engn, Rolla, MO 65409 USA. FU NASA Space Technology Research Fellowship [NNX13AL58H] FX This work was supported by a NASA Space Technology Research Fellowship under training project grant NNX13AL58H (Serhat Hosder, principal investigator, and Karl Edquist, research collaborator). The authors would like to thank Christopher O. Johnston for his expert opinion and discussions of the shock-layer radiation modeling for the current project. NR 19 TC 2 Z9 2 U1 0 U2 3 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY PY 2015 VL 52 IS 3 BP 776 EP 788 DI 10.2514/1.A33131 PG 13 WC Engineering, Aerospace SC Engineering GA CI8DC UT WOS:000354997900013 ER PT J AU Milos, FS Gasch, MJ Prabhu, DK AF Milos, Frank S. Gasch, Matthew J. Prabhu, Dinesh K. TI Conformal Phenolic Impregnated Carbon Ablator Arcjet Testing, Ablation, and Thermal Response SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article AB A new conformal type of phenolic impregnated carbon ablator was manufactured by resin impregnation of carbon felt. Based on property measurements of the conformal material and the existing model for a standard, rigid phenolic impregnated carbon ablator, a midfidelity material response model for the conformal material was developed. The rigid and conformal materials were arcjet tested simultaneously on a sphere-cone geometry in several environments with frustum heat flux up to 380W/cm2. Good agreement between the predictions and data was obtained for recession, surface temperature, and in-depth temperatures. The conformal material has a slightly greater ablation rate but significantly lower thermal diffusivity than the rigid material. C1 [Milos, Frank S.; Gasch, Matthew J.] NASA, Ames Res Ctr, Thermal Protect Mat Branch, Moffett Field, CA 94035 USA. [Prabhu, Dinesh K.] ERC Inc, Entry Syst Technol Div, Moffett Field, CA 94035 USA. RP Milos, FS (reprint author), NASA, Ames Res Ctr, Thermal Protect Mat Branch, Mail Stop 234-1, Moffett Field, CA 94035 USA. FU Fundamental Aeronautics Program; Space Technology Program FX This work was supported by both the Fundamental Aeronautics Program and the Space Technology Program. The authors thank Parul Agrawal for the arcjet test data, Robin Beck for overall management, and Mairead Stackpoole for laboratory data. NR 7 TC 1 Z9 1 U1 1 U2 17 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY PY 2015 VL 52 IS 3 BP 804 EP 812 DI 10.2514/1.A33216 PG 9 WC Engineering, Aerospace SC Engineering GA CI8DC UT WOS:000354997900015 ER PT J AU Osipov, V Khasin, M Hafiychuk, H Muratov, C Watson, M Smelyanskiy, V AF Osipov, Viatcheslav Khasin, Michael Hafiychuk, Halyna Muratov, Cyrill Watson, Michael Smelyanskiy, Vadim TI Mitigation of Solid Booster Ignition over Pressure by Water Aerosol Sprays SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID LIQUID SHEETS; OVERPRESSURE; DROP; SIZE; SUSPENSIONS; RELAXATION; BREAKUP; SOUND AB Interaction of acoustic waves with water aerosol layers is analyzed in the context of the problem of solid booster ignition overpressure suppression. In contrast to the conventional approach to ignition overpressure suppression, which aims at using water to quench the sources of the ignition overpressure waves, this study focuses on blocking the ignition overpressure wave propagation, using reflection and attenuation of the wave by the water aerosol layers. The study considers interaction of the waves with aerosol layers of large mass loading for varying sizes of the droplets. The size of the droplets is shown to substantially affect the mechanisms of interaction with the waves. The criteria for the crossover between different mechanisms are established as functions of the droplet size and the ignition overpressure wave parameters. The optimal parameters and designs for water aerosol sprays are proposed that maximize the ignition overpressure suppression. These results were obtained using the nozzle and the exhaust hole geometries similar to those of the space shuttle. Remarkably, it is found that various a priori reasonable designs of the aerosol and water sprays may increase the ignition overpressure impact on the vehicle, increasing the risk of vehicle damage. C1 [Osipov, Viatcheslav; Khasin, Michael; Hafiychuk, Halyna] NASA, Stinger Ghaffarian Technol Inc, Ames Res Ctr, Appl Phys Grp, Moffett Field, CA 94035 USA. [Muratov, Cyrill] New Jersey Inst Technol, Appl Phys Grp, Newark, NJ 07102 USA. [Watson, Michael] NASA, George C Marshall Space Flight Ctr, Dept Math Sci, Huntsville, AL 35812 USA. [Smelyanskiy, Vadim] NASA, Ames Res Ctr, Syst Engn, Moffett Field, CA 94035 USA. RP Osipov, V (reprint author), NASA, Stinger Ghaffarian Technol Inc, Ames Res Ctr, Appl Phys Grp, Moffett Field, CA 94035 USA. NR 32 TC 0 Z9 0 U1 0 U2 2 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY PY 2015 VL 52 IS 3 BP 928 EP 943 DI 10.2514/1.A33110 PG 16 WC Engineering, Aerospace SC Engineering GA CI8DC UT WOS:000354997900025 ER PT J AU Qian, J Wang, Y Song, HJ Pant, K Peabody, H Ku, JT Butler, CD AF Qian, Jing Wang, Yi Song, Hongjun Pant, Kapil Peabody, Hume Ku, Jentung Butler, Charles D. TI Projection-Based Reduced-Order Modeling for Spacecraft Thermal Analysis SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID PIECEWISE-LINEAR APPROACH; REDUCTION; SYSTEMS; APPROXIMATIONS; DEVICES; DESIGN; LISA AB This paper presents a mathematically rigorous, subspace projection-based reduced-order modeling methodology and an integrated framework to automatically generate reduced-order models for spacecraft thermal analysis. Two key steps in the reduced-order modeling procedure are described: first, the acquisition of a full-scale spacecraft model in the ordinary differential equation, and differential algebraic equation, forms to resolve its dynamic thermal behavior; and second, reduced-order modeling to markedly reduce the dimension of the full-scale model. Specifically, proper orthogonal decomposition in conjunction with a discrete empirical interpolation method and trajectory piecewise-linear methods are developed to address the strong nonlinear thermal effects due to coupled conductive and radiative heat transfer in the spacecraft environment. Case studies using NASA-relevant satellite models are undertaken to verify the capability and to assess the computational performance of the reduced-order modeling technique in terms of speedup and error relative to the full-scale model. Reduced-order modeling exhibits excellent agreement in spatiotemporal thermal profiles (less than 0.5% relative error in pertinent timescales) along with salient computational acceleration (up to two orders of magnitude speedup) over the full-scale analysis. These findings establish the feasibility of reduced-order modeling to perform rational and computationally affordable thermal analysis, develop reliable thermal control strategies for spacecraft, and greatly reduce the development cycle times and costs. C1 [Qian, Jing; Wang, Yi; Song, Hongjun; Pant, Kapil] CFD Res Corp, Biomed & Energy Technol, Huntsville, AL 35806 USA. [Peabody, Hume; Ku, Jentung; Butler, Charles D.] NASA, Goddard Space Flight Ctr, Thermal Engn Branch, Greenbelt, MD 20771 USA. RP Wang, Y (reprint author), CFD Res Corp, Biomed & Energy Technol, 701 McMillian Way, Huntsville, AL 35806 USA. EM yi.wang@cfdrc.com FU NASA [NNX11CB02C] FX This research is sponsored by NASA under contract number NNX11CB02C. NR 24 TC 2 Z9 2 U1 3 U2 7 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY PY 2015 VL 52 IS 3 BP 978 EP 989 DI 10.2514/1.A33117 PG 12 WC Engineering, Aerospace SC Engineering GA CI8DC UT WOS:000354997900029 ER PT J AU Bykov, AM Churazov, EM Ferrari, C Forman, WR Kaastra, JS Klein, U Markevitch, M de Plaa, J AF Bykov, A. M. Churazov, E. M. Ferrari, C. Forman, W. R. Kaastra, J. S. Klein, U. Markevitch, M. de Plaa, J. TI Structures and Components in Galaxy Clusters: Observations and Models SO SPACE SCIENCE REVIEWS LA English DT Review DE Clusters of galaxies; Radiation mechanisms: non-thermal; Radio continuum; X-rays: galaxies: clusters ID ACTIVE GALACTIC NUCLEI; DIFFUSIVE SHOCK ACCELERATION; X-RAY-LINES; MAGNETIC-FIELD AMPLIFICATION; XMM-NEWTON OBSERVATIONS; MASSIVE BLACK-HOLES; COOLING FLOWS; PERSEUS CLUSTER; RESONANT SCATTERING; ELLIPTIC GALAXIES AB Clusters of galaxies are the largest gravitationally bounded structures in the Universe dominated by dark matter. We review the observational appearance and physical models of plasma structures in clusters of galaxies. Bubbles of relativistic plasma which are inflated by supermassive black holes of AGNs, cooling and heating of the gas, large scale plasma shocks, cold fronts, non-thermal halos and relics are observed in clusters. These constituents are reflecting both the formation history and the dynamical properties of clusters of galaxies. We discuss X-ray spectroscopy as a tool to study the metal enrichment in clusters and fine spectroscopy of Fe X-ray lines as a powerful diagnostics of both the turbulent plasma motions and the energetics of the non-thermal electron populations. The knowledge of the complex dynamical and feedback processes is necessary to understand the energy and matter balance as well as to constrain the role of the non-thermal components of clusters. C1 [Bykov, A. M.] AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia. [Bykov, A. M.] St Petersburg State Politecn Univ, St Petersburg, Russia. [Bykov, A. M.] Int Space Sci Inst, Bern, Switzerland. [Churazov, E. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Churazov, E. M.] Space Res Inst IKI, Moscow 117997, Russia. [Ferrari, C.] Univ Nice Sophia Antipolis, Lab Lagrange, Observ Cote Azur, CNRS,UMR7293, F-06300 Nice, France. [Forman, W. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kaastra, J. S.; de Plaa, J.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Klein, U.] Univ Bonn, Argelander Inst Astron, Bonn, Germany. [Markevitch, M.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Bykov, AM (reprint author), AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia. EM byk@astro.ioffe.ru; churazov@mpa-garching.mpg.de; chiara.ferrari@oca.eu; forman@cfa.harvard.edu; j.kaastra@sron.nl; uklein@astro.uni-bonn.de; maxim.markevitch@nasa.gov; J.de.Plaa@sron.nl RI Bykov, Andrei/E-3131-2014; Churazov, Eugene/A-7783-2013; OI Forman, William/0000-0002-9478-1682 FU NASA [NASA-03060]; Chandra HRC project; Chandra archive grant [AR1-12007X]; NASA observing grant [GO2-13005X]; NWO (the Netherlands Organization for Scientific Research) FX We would like to thank the referee for useful comments and the ISSI staff for providing an inspiring atmosphere favorable for intense discussions. We thank Hiroki Akamatsu for providing us with Fig. 21 before publication. W. Forman acknowledges support from NASA contract NASA-03060 that funds the Chandra HRC project, the Chandra archive grant AR1-12007X, and the NASA observing grant GO2-13005X. SRON is financially supported by NWO (the Netherlands Organization for Scientific Research). NR 202 TC 3 Z9 3 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD MAY PY 2015 VL 188 IS 1-4 BP 141 EP 185 DI 10.1007/s11214-014-0129-4 PG 45 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ0FO UT WOS:000355151400005 ER PT J AU Fletcher, L Cargill, PJ Antiochos, SK Gudiksen, BV AF Fletcher, L. Cargill, P. J. Antiochos, S. K. Gudiksen, B. V. TI Structures in the Outer Solar Atmosphere SO SPACE SCIENCE REVIEWS LA English DT Review DE Sun; Corona; Hard X-rays ID CORONAL MAGNETIC-FIELDS; X-RAY-EMISSION; FREQUENCY ACOUSTIC-WAVES; MASS EJECTIONS; ENERGY-RELEASE; ACTIVE-REGION; FLUX ROPES; QUIET SUN; PARTICLE-ACCELERATION; FILAMENT ERUPTIONS AB The structure and dynamics of the outer solar atmosphere are reviewed with emphasis on the role played by the magnetic field. Contemporary observations that focus on high resolution imaging over a range of temperatures, as well as UV, EUV and hard X-ray spectroscopy, demonstrate the presence of a vast range of temporal and spatial scales, mass motions, and particle energies present. By focusing on recent developments in the chromosphere, corona and solar wind, it is shown that small scale processes, in particular magnetic reconnection, play a central role in determining the large-scale structure and properties of all regions. This coupling of scales is central to understanding the atmosphere, yet poses formidable challenges for theoretical models. C1 [Fletcher, L.] Univ Glasgow, SUPA Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. [Cargill, P. J.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Space & Atmospher Phys, London SW7 2BZ, England. [Cargill, P. J.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. [Antiochos, S. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gudiksen, B. V.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Gudiksen, B. V.] Univ Oslo, Ctr Math Applicat, N-0316 Oslo, Norway. RP Fletcher, L (reprint author), Univ Glasgow, SUPA Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. EM lyndsay.fletcher@glasgow.ac.uk FU STFC [ST/I001808/1]; NASA TRT Program; NASA SRT Program FX We thank Andre Balogh for organizing this workshop and ISSI staff for their hospitality. The work of L. Fletcher has been supported by STFC grant ST/I001808/1 and that of S. Antiochos has been supported by the NASA TR&T and SR&T Programs. NR 202 TC 6 Z9 6 U1 2 U2 5 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD MAY PY 2015 VL 188 IS 1-4 BP 211 EP 249 DI 10.1007/s11214-014-0111-1 PG 39 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ0FO UT WOS:000355151400007 ER PT J AU Nathal, M AF Nathal, Mike TI ADVANCED TURBINE AIRFOIL DEVELOPMENT STRATEGIES: HARVESTING LOW-HANGING FRUIT SO ADVANCED MATERIALS & PROCESSES LA English DT Article ID TENSILE PROPERTIES; BARRIER COATINGS; ALLOYS; CREEP; BEHAVIOR C1 [Nathal, Mike] NASA Glenn Res Ctr, Adv Metall Branch, Struct & Mat Div, Cleveland, OH USA. EM miken345@wowway.com NR 31 TC 0 Z9 0 U1 0 U2 1 PU ASM INT PI MATERIALS PARK PA SUBSCRIPTIONS SPECIALIST CUSTOMER SERVICE, MATERIALS PARK, OH 44073-0002 USA SN 0882-7958 EI 2161-9425 J9 ADV MATER PROCESS JI Adv. Mater. Process. PD MAY PY 2015 VL 173 IS 5 BP 21 EP 24 PG 4 WC Materials Science, Multidisciplinary SC Materials Science GA CI3OL UT WOS:000354657000003 ER PT J AU Righter, K AF Righter, Kevin TI Modeling siderophile elements during core formation and accretion, and the role of the deep mantle and volatiles SO AMERICAN MINERALOGIST LA English DT Article DE Core; mantle; magma ocean; siderophile; volatile; accretion ID SILICATE PARTITION-COEFFICIENTS; TERRESTRIAL MAGMA OCEAN; HIGH-PRESSURE; EARTHS CORE; OXYGEN FUGACITY; NITROGEN SOLUBILITY; TRACE-ELEMENTS; LIQUID-METAL; SULFIDE MELT; REDOX STATE AB The last decade has seen general agreement that moderately siderophile elements (MSE) in Earth's primitive upper mantle (PUM) can be explained by metal-silicate equilibrium at mid-mantle depths in an early Earth magma ocean environment. Despite the agreement, there are some differences in the detailed modeling that has been carried out. This paper will examine siderophile element metal/silicate partitioning with respect to three different topics: (1) an examination of aspects of the modeling that one might suspect leads to differences in outcomes or in comparison between models, but actually are in agreement with experimental data and between models; (2) a discussion of the role of the deep mantle in modeling efforts; and (3) the role and/or fate of volatiles in magma ocean scenarios with an emphasis on where data are lacking. C1 NASA JSC, Mailcode KT, Houston, TX 77058 USA. RP Righter, K (reprint author), NASA JSC, Mailcode KT, 2101 NASA Pkwy, Houston, TX 77058 USA. EM kevin.righter-1@nasa.gov FU NASA Cosmochemistry program through an RTOP FX The author thanks H. Watson and T. Rushmer for the invitation to write this manuscript for the special issue. K.R. is funded by the NASA Cosmochemistry program through an RTOP. Comments and suggestions of an anonymous reviewer and A. Bouhifd helped improve the presentation of this work. NR 113 TC 5 Z9 6 U1 3 U2 21 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD MAY-JUN PY 2015 VL 100 IS 5-6 BP 1098 EP 1109 DI 10.2138/am-2015-5052 PG 12 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA CI3RS UT WOS:000354665700013 ER PT J AU Martin, AM Medard, E Devouard, B Keller, LP Righter, K Devidal, JL Rahman, Z AF Martin, Audrey M. Medard, Etienne Devouard, Bertrand Keller, Lindsay P. Righter, Kevin Devidal, Jean-Luc Rahman, Zia TI Fayalite oxidation processes in Obsidian Cliffs rhyolite flow, Oregon SO AMERICAN MINERALOGIST LA English DT Article DE Olivine; fayalite; laihunite; oxyfayalite; rhyolite; lithophysae; oxidation ID TEMPERATURE CRYSTAL-CHEMISTRY; ELECTRON-MICROPROBE; OXIDIZED OLIVINE; TOPAZ RHYOLITES; KINETICS; STABILITY; LAIHUNITE; ENERGY; IRON; SPECTROSCOPY AB This study investigates the oxidation of fayalite Fe22+SiO4 that is present in lithophysae from a rhyolite flow (Obsidian Cliffs, Oregon). Textural, chemical, and structural analyses of the successive oxidation zones are used to constrain: ( I) the oxidation processes of olivine, and (2) the role of temperature, chemical diffusion, and meteoric infiltration. Petrologic analyses and thermodynamic modeling show that the rhyolite flow emplaced at 800-950 degrees C. Fayalite-bearing lithophysae formed only in the core of the lava flow. Variations in the gas composition inside the lithophysae induced the oxidation of fayalite to a laihunite-1M zone Fe12+Fe23+square(1)(SiO4)(2). This zone is made of nano-lamellae of amorphous silica SiO2 and laihunite-3MFe(1.6)(2+)Fe(1.6)(3+)square(0.8)(SiO4)(2)+ hematite Fe2O3. It probably formed by a nucleation and growth process in the fayalite fractures and defects and at fayalite crystal edges. The laihunite-1M zone then oxidized into an "oxyfayalite" zone with the composition Fe0.522+Fe2.323+square(1.16)(SiO4)(2). This second oxidation zone is made of lamellae of amorphous silica SiO2 and hematite Fe2O3, with a possible small amount of ferrosilite Fe2+SiO3. A third and outer zone, composed exclusively of hematite, is also present. The successive oxidation zones suggest that there may be a mineral in the olivine group with higher Fe3+ content than laihunite-1M. The transformation of laihunite-1M to this "oxyfayalite" phase could occur by a reaction such as 0.24Fe(M1)(2+laihunite-1M) + 0.06O(2) = 0.16 Fe-M1(3+"oxyfayalite") + 0.08 square("oxyfayalite") + 0.04 (Fe23+O3hematite) This would imply that Fe3+ can also be incorporated in the M1 site of olivine. C1 [Martin, Audrey M.; Keller, Lindsay P.; Righter, Kevin; Rahman, Zia] NASA, Johnson Space Ctr, Mailcode KT, Houston, TX 77058 USA. [Martin, Audrey M.] Case Western Reserve Univ, Earth Environm & Planetary Sci, Cleveland, OH 44118 USA. [Medard, Etienne; Devouard, Bertrand; Devidal, Jean-Luc] Univ Clermont Ferrand, CNRS, IRD, Lab Magmas & Volcans, F-63038 Clermont Ferrand, France. [Devouard, Bertrand] CNRS, IRD, AMU, CEREGE,UM34, F-13545 Aix En Provence, France. RP Martin, AM (reprint author), NASA, Johnson Space Ctr, Mailcode KT, 2101 NASA Pkwy, Houston, TX 77058 USA. EM audrey.martin@case.edu OI Martin, Audrey/0000-0002-1165-8866; Medard, Etienne/0000-0002-7040-7442; DEVOUARD, Bertrand/0000-0002-8774-1842 FU Johnson Space Center FX The authors thank D. Howard for providing some of the Obsidian Cliffs rhyolites samples. Yann Morizet, Jonathan Castro, and an anonymous reviewer are gratefully acknowledged for their insightful and constructive comments. This research was supported by an appointment to the NASA Postdoctoral Program at the Johnson Space Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 72 TC 1 Z9 1 U1 6 U2 14 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD MAY-JUN PY 2015 VL 100 IS 5-6 BP 1153 EP 1164 DI 10.2138/am-2015-5042 PG 12 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA CI3RS UT WOS:000354665700017 ER PT J AU Collazzi, AC Kouveliotou, C van der Horst, AJ Younes, GA Kaneko, Y Gogus, E Lin, L Granot, J Finger, MH Chaplin, VL Huppenkothen, D Watts, AL von Kienlin, A Baring, MG Gruber, D Bhat, PN Gibby, MH Gehrels, N McEnery, J van der Klis, M Wijers, RAMJ AF Collazzi, A. C. Kouveliotou, C. van der Horst, A. J. Younes, G. A. Kaneko, Y. Gogus, E. Lin, L. Granot, J. Finger, M. H. Chaplin, V. L. Huppenkothen, D. Watts, A. L. von Kienlin, A. Baring, M. G. Gruber, D. Bhat, P. N. Gibby, M. H. Gehrels, N. McEnery, J. van der Klis, M. Wijers, R. A. M. J. TI THE FIVE YEAR FERMI/GBM MAGNETAR BURST CATALOG SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; pulsars: individual (SGR J1550-5418, SGR J0501+4516, 1E1841-045, SGR J0418+5729, SGR 1806-20, SGR J1822.3-1606, AXP 4U 0142+61, AXP 1E 2259+586, 3XMM J185246.6+0033.7); stars: neutron; X-rays: bursts ID SOFT GAMMA REPEATER; X-RAY PULSAR; QUASI-PERIODIC OSCILLATIONS; SGR J1550-5418 BURSTS; HIGH-ENERGY TRANSIENT; 1E 1547.0-5408; ACTIVE EPISODE; MONITOR; DISCOVERY; EMISSION AB Since launch in 2008, the Fermi Gamma-ray Burst Monitor (GBM) has detected many hundreds of bursts from magnetar sources. While the vast majority of these bursts have been attributed to several known magnetars, there is also a small sample of magnetar-like bursts of unknown origin. Here, we present the Fermi/GBM magnetar catalog, providing the results of the temporal and spectral analyses of 440 magnetar bursts with high temporal and spectral resolution. This catalog covers the first five years of GBM magnetar observations, from 2008 July to 2013 June. We provide durations, spectral parameters for various models, fluences, and peak fluxes for all the bursts, as well as a detailed temporal analysis for SGR J1550-5418 bursts. Finally, we suggest that some of the bursts of unknown origin are associated with the newly discovered magnetar 3XMM J185246.6+0033.7. C1 [Collazzi, A. C.] SciTec Inc, Princeton, NJ 08540 USA. [Kouveliotou, C.; van der Horst, A. J.; Younes, G. A.] George Washington Univ, Dept Phys, Washington, DC 20052 USA. [Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, ZP12, Huntsville, AL 35812 USA. [Younes, G. A.; Finger, M. H.] Univ Space Res Assoc, NSSTC, Huntsville, AL 35805 USA. [Kaneko, Y.; Gogus, E.] Sabanci Univ, TR-34956 Istanbul, Turkey. [Lin, L.] APC, Francois Arago Ctr, F-75205 Paris, France. [Granot, J.] Open Univ Israel, Dept Nat Sci, IL-43537 Raanana, Israel. [Chaplin, V. L.] Vanderbilt Univ, Sch Med, Nashville, TN 37232 USA. [Huppenkothen, D.] NYU, Ctr Data Sci, New York, NY 10003 USA. [Huppenkothen, D.] NYU, Ctr Cosmol & Particle Phys, Dept Phys, New York, NY 10003 USA. [Watts, A. L.; van der Klis, M.; Wijers, R. A. M. J.] Univ Amsterdam, Anton Pannekoek Inst, NL-1090 GE Amsterdam, Netherlands. [von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. [Gruber, D.] Planetarium Sudtirol, I-39053 Karneid, Italy. [Bhat, P. N.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Gibby, M. H.] Jacobs Technol Inc, Huntsville, AL USA. [Gehrels, N.; McEnery, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Collazzi, AC (reprint author), SciTec Inc, 100 Wall St, Princeton, NJ 08540 USA. EM acollazzi@scitec.com OI Wijers, Ralph/0000-0002-3101-1808 FU NASA [NNH07ZDA001-GLAST]; NASA Postdoctoral Program at the Marshall Space Flight Center; Moore-Sloan Data Science Environment at New York University; Netherlands Organization for Scientific Research (NWO) Vidi Fellowship; Bundesministeriums fur Wirtschaft und Technologie (BMWi) through DLR [50 OG 1101]; Netherlands Organisation for Scientific Research (NWO); Royal Netherlands Academy of Arts and Sciences (KNAW) FX This publication is part of the GBM/Magnetar Key Project (NASA grant NNH07ZDA001-GLAST, PI: C. Kouveliotou). A.C.C. was supported by an appointment to the NASA Postdoctoral Program at the Marshall Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. C.K. and G.A.Y. acknowledge support from NASA grant NNH07ZDA001-GLAST. D.H. was supported by the Moore-Sloan Data Science Environment at New York University. A.L.W. acknowledges support from a Netherlands Organization for Scientific Research (NWO) Vidi Fellowship. A.v.K. was supported by the Bundesministeriums fur Wirtschaft und Technologie (BMWi) through DLR grant 50 OG 1101. M.v.d.K. acknowledges support from the Netherlands Organisation for Scientific Research (NWO) and the Royal Netherlands Academy of Arts and Sciences (KNAW). NR 71 TC 7 Z9 7 U1 1 U2 4 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 MAY PY 2015 VL 218 IS 1 AR 11 DI 10.1088/0067-0049/218/1/11 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8DN UT WOS:000354999200011 ER PT J AU Sacchi, C Bhasin, K Kadowaki, N Vong, F AF Sacchi, Claudio Bhasin, Kul Kadowaki, Naoto Vong, Fred TI TECHNOLOGIES AND APPLICATIONS OF FUTURE SATELLITE NETWORKING SO IEEE COMMUNICATIONS MAGAZINE LA English DT Editorial Material C1 [Sacchi, Claudio] Univ Trento, Fac Engn, Trento, Italy. [Bhasin, Kul] NASA Glenn Res Ctr, Cleveland, OH USA. [Bhasin, Kul] Space Commun Projects NASA GRC, San Diego, CA USA. [Bhasin, Kul] AIAA, San Diego, CA USA. [Bhasin, Kul] SPIE, Bellingham, WA USA. [Kadowaki, Naoto] Strateg Planning Dept NICT, Koganei, Tokyo, Japan. [Kadowaki, Naoto] Wireless Network Res Inst NICT, Yokosuka, Kanagawa, Japan. [Vong, Fred] Asia Satellite Telecommun Co Ltd, Engn, Hong Kong, Hong Kong, Peoples R China. RP Sacchi, C (reprint author), Univ Trento, Dept Comp Sci & Informat Engn, Trento, Italy. EM sacchi@disi.unitn.it NR 0 TC 0 Z9 0 U1 3 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0163-6804 EI 1558-1896 J9 IEEE COMMUN MAG JI IEEE Commun. Mag. PD MAY PY 2015 VL 53 IS 5 BP 154 EP 155 PG 2 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA CI1CV UT WOS:000354479400018 ER PT J AU Chen, TY Vakilinia, K Divsalar, D Wesel, RD AF Chen, Tsung-Yi Vakilinia, Kasra Divsalar, Dariush Wesel, Richard D. TI Protograph-Based Raptor-Like LDPC Codes SO IEEE TRANSACTIONS ON COMMUNICATIONS LA English DT Article DE Channel coding; low-density parity-check codes ID PARITY-CHECK CODES; DESIGN; COMPLEXITY; CAPACITY; CONSTRUCTION; PERFORMANCE AB This paper proposes protograph-based Raptor-like (PBRL) codes as a class of rate-compatible low-density parity-check codes for binary-input AWGN channels. As with the Raptor codes, exclusive-OR operations on precoded bits produce additional parity bits providing extensive rate compatibility. Unlike Raptor codes, each additional parity bit in the protograph is explicitly designed to optimize the density evolution threshold. During the lifting process, approximate cycle extrinsic message degree (ACE) and circulant progressive edge growth (CPEG) constraints are used to avoid undesirable graphical structures. Some density-evolution performance is sacrificed to obtain lower error floors, particularly at short blocklengths. Simulation results are shown for information block sizes of k = 1032 and 16 384. For a target frame error rate of 10(-5), at each rate, the k = 1032 and 16 384 code families perform within 1 dB and 0.4 dB of both the Gallager bound and the normal approximation, respectively. The 16 384 code family outperforms the best known standardized code family, namely, the AR4JA codes. The PBRL codes also outperform DVB-S2 codes that have the advantages of longer blocklengths and outer BCH codes. Performance is similar to RC code families designed by Nguyen et al. that do not constrain codes to have the PBRL structure and involve simulation in the optimization process at each rate. C1 [Chen, Tsung-Yi] SpiderCloud Wireless Inc, San Jose, CA 95134 USA. [Vakilinia, Kasra; Divsalar, Dariush; Wesel, Richard D.] Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA. [Wesel, Richard D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Chen, TY (reprint author), SpiderCloud Wireless Inc, San Jose, CA 95134 USA. EM tsungyi.chen@engineering.ucla.edu; vakiliniak@ucla.edu; Dariush.Divsalar@jpl.nasa.gov; wesel@ee.ucla.edu FU National Science Foundation [1162501, 1161822, 82-17473] FX This material is based upon work supported by the National Science Foundation under Grants 1162501 and 1161822 (JPL Task Plan 82-17473). 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. This research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Parts of this work were presented at the Global Communications Conference 2011 and the International Conference on Communications 2012. The editor coordinating the review of this paper and approving it for publication was M. Lentmaier. (Tsung-Yi Chen and Kasra Vakilinia contributed equally to this work.) NR 56 TC 13 Z9 13 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0090-6778 EI 1558-0857 J9 IEEE T COMMUN JI IEEE Trans. Commun. PD MAY PY 2015 VL 63 IS 5 BP 1522 EP 1532 DI 10.1109/TCOMM.2015.2404842 PG 11 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA CI7LE UT WOS:000354944100003 ER PT J AU Choi, S Mulfinger, DG Robinson, JE Capozzi, BJ AF Choi, Seongim Mulfinger, Daniel G. Robinson, John E., III Capozzi, Brian J. TI Design of an Optimal Route Structure Using Heuristics-Based Stochastic Schedulers SO JOURNAL OF AIRCRAFT LA English DT Article AB The purpose of the current study is to identify key parameters and provide reasonable guidelines for the design of an efficient route structure in the extended terminal airspace area under dense air traffic flows. First, various scheduling algorithms, including a first-come/first-served and mixed-integer linear programming, are compared in terms of efficiency and optimality of scheduling performance. To further improve the efficiency of the scheduling algorithms, heuristics based on the first-come/first-served and genetic algorithms are adopted and quickly predetermine the aircraft sequences at the scheduling point. Subsequently, a dynamic planning framework is constructed to provide a more practical scheduling strategy for realistic operation, and it effectively handles the dynamic situations of traffic flows under uncertainties in weather and operations. It is an integrated framework that iteratively executes a flight trajectory model and the scheduling algorithms. As a practical application of the proposed scheduling strategy to the dense terminal environment, a design of an optimal route structure is carried out where the terminal airspace is represented in Cartesian coordinates. The sensitivities of the scheduling performance with respect to the uncertainty quantification and propagation models are investigated in more general airspace topology by varying merge point locations and their numbers. C1 [Choi, Seongim] Virginia Polytech Inst & State Univ, Dept Aerosp & Ocean Engn, Blacksburg, VA 24060 USA. [Mulfinger, Daniel G.; Robinson, John E., III] NASA, Ames Res Ctr, Airspace Syst Div, Moffett Field, CA 94035 USA. [Capozzi, Brian J.] Mosa ATM, Leesburg, VA 20175 USA. RP Choi, S (reprint author), Virginia Polytech Inst & State Univ, Dept Aerosp & Ocean Engn, Blacksburg, VA 24060 USA. NR 18 TC 0 Z9 0 U1 3 U2 6 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD MAY-JUN PY 2015 VL 52 IS 3 BP 764 EP 777 DI 10.2514/1.C032645 PG 14 WC Engineering, Aerospace SC Engineering GA CI4VH UT WOS:000354751400004 ER PT J AU Wu, MHG Green, SM Jones, J AF Wu, Minghong G. Green, Steven M. Jones, James TI Strategies for Choosing Descent Flight-Path Angles for Small Jets SO JOURNAL OF AIRCRAFT LA English DT Article ID INTERNATIONAL-AIRPORT; ARRIVALS; DESIGN AB A standard descent procedure with a fixed flight-path angle is proposed to improve trajectory predictability for arriving small jets in the transition airspace into congested terminal area. Three candidate strategies for selecting fuel-efficient and flyable descent flight-path angles are proposed. The three strategies vary in operational complexity and fuel-burn merits. To mitigate variation of wind among flights, the two simpler strategies are adapted to airport, directions of arrival, and time. Three major U.S. airports with different degrees of wind variation and disparate arrival traffic flows are analyzed. Results show that, when compared to the simple airport-static adaptation, the finest adaptation of the simpler strategies recover up to 50-75% of the extra fuel burn relative to the minimum-fuel strategy. Wind variation, descent altitude restrictions, arrival directions, and fleet composition all affect the fuel efficiency of the simple strategies. Tradeoffs between fuel burn and planned speed-brake usage in the choice of the flight-path angle are discussed. Fuel efficiency of simple strategies for the entire national airspace in the United States is estimated. Considerations and implications for air navigation service providers are discussed. C1 [Wu, Minghong G.] Univ Calif Santa Cruz, Santa Cruz, CA 94035 USA. [Green, Steven M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Jones, James] Univ Maryland, Dept Civil & Environm Engn, College Pk, MD 20742 USA. RP Wu, MHG (reprint author), Univ Calif Santa Cruz, Santa Cruz, CA 94035 USA. NR 34 TC 0 Z9 0 U1 0 U2 2 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD MAY-JUN PY 2015 VL 52 IS 3 BP 847 EP 866 DI 10.2514/1.C032835 PG 20 WC Engineering, Aerospace SC Engineering GA CI4VH UT WOS:000354751400011 ER PT J AU Bui, TT AF Bui, Trong T. TI Analysis of Stall Aerodynamics of a Swept Wing with Laminar-Flow Glove SO JOURNAL OF AIRCRAFT LA English DT Article AB Reynolds-averaged Navier-Stokes computational-fluid-dynamics analysis was conducted to study the low-speed stall aerodynamics of a business jet's swept wing modified with a laminar-flow wing glove. The stall aerodynamics of the gloved wing were analyzed and compared with the unmodified wing for the flight speed of 120 kt and altitude of 2300 ft above mean sea level. A polyhedral finite-volume unstructured Navier-Stokes computational-fluid-dynamics code was used in the analysis. This computational-fluid-dynamics code was first validated for wing stall predictions using the wing-body geometry from the First AIAA Computational Fluid Dynamics High-Lift Prediction Workshop. It was found that the computational-fluid-dynamics code under consideration can produce results that are within the scattering of other computational-fluid-dynamics codes considered at the workshop. In particular, the polyhedral computational-fluid-dynamics code was able to predict wing stall for the AIAA wing-body geometry to within 1 deg of angle of attack as compared to benchmark wind-tunnel test data. Computational-fluid-dynamics results show that the addition of the laminar-flow wing glove causes the gloved wing to stall much earlier than the unmodified wing. Furthermore, the gloved wing has a different stall characteristic than the clean wing, with no sharp lift dropoff at stall for the gloved wing. C1 NASA, Armstrong Flight Res Ctr, Aerodynam & Prop Branch, Edwards AFB, CA 93523 USA. RP Bui, TT (reprint author), NASA, Armstrong Flight Res Ctr, Aerodynam & Prop Branch, POB 273-MS 4840B, Edwards AFB, CA 93523 USA. NR 6 TC 0 Z9 0 U1 1 U2 2 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD MAY-JUN PY 2015 VL 52 IS 3 BP 867 EP 871 DI 10.2514/1.C032883 PG 5 WC Engineering, Aerospace SC Engineering GA CI4VH UT WOS:000354751400012 ER PT J AU Landman, D Toro, KG Commo, SA Lynn, KC AF Landman, Drew Toro, Kenneth G. Commo, Sean A. Lynn, Keith C. TI Prediction Interval Development for Wind-Tunnel Balance Check-Loading SO JOURNAL OF AIRCRAFT LA English DT Article AB The current approach used to apply uncertainty intervals to balance estimated loads is based on the root mean square error from calibration. Using the root mean square error, a constant interval is applied around the estimated load and it is expected that a predetermined percentage of the check-loads applied fall within this constant uncertainty interval. However, this approach ignores additional sources of uncertainty and assumes constant uncertainty regardless of the load combination and magnitude applied to the balance. Rigorous prediction interval theory permits varying interval widths but fails to account for the additional error sources that are unrelated to the mathematical modeling. An engineered solution is proposed that combines prediction interval theory and the need to account for the additional sources of uncertainty from calibration and check loading. Results from a case study using the in-situ load system show improved probabilistic behavior in terms of uncertainty interval capture percentage when compared with the current root mean square error method. C1 [Landman, Drew; Toro, Kenneth G.] Old Dominion Univ, Dept Mech & Aerosp Engn, Norfolk, VA 23529 USA. [Commo, Sean A.] NASA, Langley Res Ctr, Syst Engn & Engn Methods Branch, Hampton, VA 23681 USA. [Lynn, Keith C.] NASA, Langley Res Ctr, Adv Measurements & Data Syst Branch, Hampton, VA 23681 USA. RP Landman, D (reprint author), Old Dominion Univ, Dept Mech & Aerosp Engn, 1300 Elkhorn Ave, Norfolk, VA 23529 USA. FU National Force Measurement Technology Capability under NASA's Aeronautics Test Program FX This work has been supported and funded by the National Force Measurement Technology Capability under NASA's Aeronautics Test Program. The authors would like to express their sincere appreciation to the individuals who have contributed to the many aspects of this project. In particular, the authors would like to recognize the following for the critical contributions: J. Greg Jones for his extensive expertise, knowledge, and dedication to balance calibrations; Ray Rhew for his valuable input on force measurement system design and characterization; Peter Parker for his insight on the Single-Vector Calibration System and consultation during the development of the in-situ load system (ILS); and Michael Acheson and Mark Cagle for their initial work with the ILS. NR 9 TC 0 Z9 0 U1 3 U2 4 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD MAY-JUN PY 2015 VL 52 IS 3 BP 884 EP 889 DI 10.2514/1.C032930 PG 6 WC Engineering, Aerospace SC Engineering GA CI4VH UT WOS:000354751400015 ER PT J AU Ordaz, I Geiselhart, KA Fenbert, JW AF Ordaz, Irian Geiselhart, Karl A. Fenbert, James W. TI Conceptual Design of Low-Boom Aircraft with Flight Trim Requirement SO JOURNAL OF AIRCRAFT LA English DT Article AB A new low-boom target generation approach is presented that allows the introduction of a trim requirement during the early conceptual design of supersonic aircraft. The formulation provides an approximation of the center of pressure for an aircraft configuration with a reversed equivalent area matching a low-boom equivalent area target. The center of pressure is approximated from a surrogate lift distribution that is based on the lift component of the classical equivalent area. The assumptions of the formulation are verified to be sufficiently accurate for a supersonic aircraft of high fineness ratio through three case studies. The first two quantify and verify the accuracy and the sensitivity of the surrogate center of pressure corresponding to shape deformation of lifting components. The third verification case shows the capability of the approach to achieve a trim state while maintaining the low-boom characteristics of a previously untrimmed configuration. Finally, the new low-boom target generation approach is demonstrated through the early conceptual design of a demonstrator concept that is low-boom feasible, trimmed, and stable in cruise. C1 [Ordaz, Irian; Geiselhart, Karl A.] NASA, Langley Res Ctr, Aeronaut Syst Anal Branch, Hampton, VA 23681 USA. [Fenbert, James W.] Analytical Mech Associates Inc, Aeronaut Syst Anal Branch, Hampton, VA 23681 USA. RP Ordaz, I (reprint author), NASA, Langley Res Ctr, Aeronaut Syst Anal Branch, Mail Stop 442, Hampton, VA 23681 USA. NR 18 TC 0 Z9 0 U1 0 U2 2 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD MAY-JUN PY 2015 VL 52 IS 3 BP 932 EP 939 DI 10.2514/1.C033160 PG 8 WC Engineering, Aerospace SC Engineering GA CI4VH UT WOS:000354751400022 ER PT J AU Grauer, JA AF Grauer, Jared A. TI Real-Time Data-Compatibility Analysis Using Output-Error Parameter Estimation SO JOURNAL OF AIRCRAFT LA English DT Article ID IDENTIFICATION AB Output-error parameter estimation, normally a postflight batch technique, was applied to solve the data-compatibility problem in real time. Short segments of data were sequentially processed to enable real-time estimation, and variations on the algorithm were used to expedite convergence from arbitrary starting values of the unknown model parameters. The method was applied to flight-test data to correct the data for systematic instrumentation errors. Results showed that the method produced accurate estimates of the data-compatibility correction parameters at a rate of 0.5 Hz. A sensor fault was also introduced into the flight data, and the use of a data-forgetting algorithm showed that the method was capable of quickly adapting to the data in a way that could enable sensor fault detection. C1 NASA, Langley Res Ctr, Dynam Syst & Control Branch, Hampton, VA 23681 USA. RP Grauer, JA (reprint author), NASA, Langley Res Ctr, Dynam Syst & Control Branch, MS 308, Hampton, VA 23681 USA. FU NASA Aviation Safety Program; Vehicle Systems Safety Technologies project; Subsonic Fixed-Wing Project FX This research was funded by the NASA Aviation Safety Program, Vehicle Systems Safety Technologies project, and the Subsonic Fixed-Wing Project. Conversations with Eugene Morelli at NASA Langley Research Center are acknowledged and appreciated. NR 18 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD MAY-JUN PY 2015 VL 52 IS 3 BP 940 EP 947 DI 10.2514/1.C033182 PG 8 WC Engineering, Aerospace SC Engineering GA CI4VH UT WOS:000354751400023 ER PT J AU Rodriguez-Fonseca, B Mohino, E Mechoso, CR Caminade, C Biasutti, M Gaetani, M Garcia-Serrano, J Vizy, EK Cook, K Xue, YK Polo, I Losada, T Druyan, L Fontaine, B Bader, J Doblas-Reyes, FJ Goddard, L Janicot, S Arribas, A Lau, W Colman, A Vellinga, M Rowell, DP Kucharski, F Voldoire, A AF Rodriguez-Fonseca, Belen Mohino, Elsa Mechoso, Carlos R. Caminade, Cyril Biasutti, Michela Gaetani, Marco Garcia-Serrano, J. Vizy, Edward K. Cook, Kerry Xue, Yongkang Polo, Irene Losada, Teresa Druyan, Leonard Fontaine, Bernard Bader, Juergen Doblas-Reyes, Francisco J. Goddard, Lisa Janicot, Serge Arribas, Alberto Lau, William Colman, Andrew Vellinga, M. Rowell, David P. Kucharski, Fred Voldoire, Aurore TI Variability and Predictability of West African Droughts: A Review on the Role of Sea Surface Temperature Anomalies SO JOURNAL OF CLIMATE LA English DT Article ID TROPICAL NORTH-AFRICA; GENERAL-CIRCULATION MODELS; IDEALIZED 2-DIMENSIONAL FRAMEWORK; ATLANTIC CLIMATE VARIABILITY; EASTERN EQUATORIAL ATLANTIC; SAHEL RAINFALL VARIABILITY; INTERANNUAL VARIABILITY; REGIONAL CLIMATE; SUMMER RAINFALL; DECADAL PREDICTION AB The Sahel experienced a severe drought during the 1970s and 1980s after wet periods in the 1950s and 1960s. Although rainfall partially recovered since the 1990s, the drought had devastating impacts on society. Most studies agree that this dry period resulted primarily from remote effects of sea surface temperature (SST) anomalies amplified by local land surface-atmosphere interactions. This paper reviews advances made during the last decade to better understand the impact of global SST variability on West African rainfall at interannual to decadal time scales. At interannual time scales, a warming of the equatorial Atlantic and Pacific/Indian Oceans results in rainfall reduction over the Sahel, and positive SST anomalies over the Mediterranean Sea tend to be associated with increased rainfall. At decadal time scales, warming over the tropics leads to drought over the Sahel, whereas warming over the North Atlantic promotes increased rainfall. Prediction systems have evolved from seasonal to decadal forecasting. The agreement among future projections has improved from CMIP3 to CMIP5, with a general tendency for slightly wetter conditions over the central part of the Sahel, drier conditions over the western part, and a delay in the monsoon onset. The role of the Indian Ocean, the stationarity of teleconnections, the determination of the leader ocean basin in driving decadal variability, the anthropogenic role, the reduction of the model rainfall spread, and the improvement of some model components are among the most important remaining questions that continue to be the focus of current international projects. C1 [Rodriguez-Fonseca, Belen; Mohino, Elsa] Univ Complutense Madrid, Fac Ciencias Fis, Dept Fis Tierra Astron & Astrofis 1, E-28040 Madrid, Spain. [Rodriguez-Fonseca, Belen] CSIC, Inst Geociencias, Madrid, Spain. [Rodriguez-Fonseca, Belen] Univ Complutense Madrid, E-28040 Madrid, Spain. [Mechoso, Carlos R.; Xue, Yongkang] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. [Caminade, Cyril] Univ Liverpool, Inst Infect & Global Hlth, Sch Environm Sci, Liverpool L69 3BX, Merseyside, England. [Biasutti, Michela] Columbia Univ, Lamont Doherty Earth Observ, New York, NY USA. [Gaetani, Marco] CNR, Ist Biometeorol, Rome, Italy. [Garcia-Serrano, J.; Doblas-Reyes, Francisco J.] Inst Catala Ciencies Clima, Barcelona, Spain. [Vizy, Edward K.; Cook, Kerry] Univ Texas Austin, Jackson Sch Geosci, Dept Geol Sci, Austin, TX USA. [Polo, Irene] Univ Reading, Dept Meteorol, NCAS Climate, Reading, Berks, England. [Losada, Teresa] Univ Castilla La Mancha, Inst Ciencias Ambientales, Toledo, Spain. [Druyan, Leonard] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Druyan, Leonard] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Fontaine, Bernard] Univ Bourgogne, CNRS, Ctr Rech Climatol, Dijon, France. [Bader, Juergen] Max Planck Inst Meteorol, D-20146 Hamburg, Germany. [Doblas-Reyes, Francisco J.] Inst Catalana Recerca & Estudis Avancats, Barcelona, Spain. [Goddard, Lisa] Columbia Univ, Int Res Inst Climate & Soc, New York, NY USA. [Janicot, Serge] UPMC, LOCEAN IPSL, IRD, Paris, France. [Arribas, Alberto; Colman, Andrew; Vellinga, M.; Rowell, David P.] Met Off Hadley Ctr, Exeter, Devon, England. [Lau, William] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Kucharski, Fred] Abdus Salam Int Ctr Theoret Phys, Trieste, Italy. [Voldoire, Aurore] CNRS, Meteo France, Grp Etud Atmosphere Meteorol, Ctr Natl Rech Meteorol, Toulouse, France. RP Rodriguez-Fonseca, B (reprint author), Univ Complutense Madrid, Fac Ciencias Fis, Dept Fis Tierra Astron & Astrofis 1, Ciudad Univ,Plaza Ciencias,1, E-28040 Madrid, Spain. EM brfonsec@ucm.es RI Mohino, Elsa/G-8620-2015; Garcia-Serrano, Javier/I-5058-2015; Biasutti, Michela/G-3804-2012; Losada, Teresa/O-8739-2015; Vizy, Edward/A-1577-2009; OI Mohino, Elsa/0000-0002-4342-6349; Garcia-Serrano, Javier/0000-0003-3913-0876; Biasutti, Michela/0000-0001-6681-1533; Losada, Teresa/0000-0002-8430-1745; cyril, caminade/0000-0002-3846-7082 FU Spanish projects [MINECO CGL2011-13564-E, GL2012-38923-C02-01]; U.S. National Science Foundation [SES-1048946, ATM-1036604, AGS-1041477, AGS-1115506]; European Commission [243964, 603521, 308378]; European Community FX This work was supported by Spanish projects MINECO CGL2011-13564-E and GL2012-38923-C02-01. Support from the U.S. National Science Foundation (Awards SES-1048946, ATM-1036604, AGS-1041477, and AGS-1115506) is gratefully acknowledged. Also gratefully acknowledged are the GCM modeling groups, the Program for Climate Model Diagnosis and Intercomparison (PCMDI), and the World Climate Research Programme's Working Group on Coupled Modeling (WGCM) for their roles in making available the WCRP CMIP5 multimodel dataset. Support of this dataset is provided by the Office of Science, U.S. Department of Energy (DOE). We acknowledge the EU QWECI, PREFACE, and SPECS projects both funded by the European Commission's Seventh Framework Research Programme under Grant Agreements 243964, 603521, and 308378 respectively. Based on a French initiative, AMMA was built by an international scientific group and is currently funded by a large number of agencies, especially from France, the United Kingdom, the United States, and Africa. It has been the beneficiary of a major financial contribution from the European Community's Sixth Framework Research Programme. The authors are grateful to Ashlynn Fiss for her help in improving this manuscript. NR 197 TC 13 Z9 13 U1 4 U2 35 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 MAY PY 2015 VL 28 IS 10 BP 4034 EP 4060 DI 10.1175/JCLI-D-14-00130.1 PG 27 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CH9QE UT WOS:000354370100009 ER PT J AU Lahsen, M Mathews, A Dove, MR Orlove, B Puri, R Barnes, J McElwee, P Moore, F O'Reilly, J Yager, K AF Lahsen, Myanna Mathews, Andrew Dove, Michael R. Orlove, Ben Puri, Rajindra Barnes, Jessica McElwee, Pamela Moore, Frances O'Reilly, Jessica Yager, Karina TI Strategies for changing the intellectual climate SO NATURE CLIMATE CHANGE LA English DT Letter C1 [Lahsen, Myanna] Brazilian Inst Space Res INPE, Ctr Earth Syst Sci, BR-12227010 Sao Paulo, Brazil. [Mathews, Andrew] Univ Calif Santa Cruz, Anthropol, Santa Cruz, CA 95064 USA. [Dove, Michael R.] Yale Univ, Yale Sch Forestry & Environm Studies, New Haven, CT 06511 USA. [Orlove, Ben] Columbia Univ, Earth & Environm Sci, New York, NY 10027 USA. [Puri, Rajindra] Univ Kent, Sch Anthropol & Conservat, Canterbury CT2 7NZ, Kent, England. [Barnes, Jessica] Univ S Carolina, Dept Geog, Columbia, SC 29208 USA. [McElwee, Pamela] Rutgers State Univ, Dept Human Ecol, Newark, NJ 07102 USA. [Moore, Frances] Stanford Univ, Sch Earth Sci, Stanford, CA 94305 USA. [O'Reilly, Jessica] St Johns Univ, Coll St Benedict, Anthropol & Sociol Dept, St Joseph, MN 56321 USA. [O'Reilly, Jessica] St Johns Univ, Coll St Benedict, Anthropol & Sociol Dept, Collegeville, MN 56321 USA. [Yager, Karina] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lahsen, M (reprint author), Brazilian Inst Space Res INPE, Ctr Earth Syst Sci, BR-12227010 Sao Paulo, Brazil. EM myannal@gmail.com RI Lahsen, Myanna/E-3697-2013; OI Puri, Rajindra/0000-0002-3442-8537; McElwee, Pamela/0000-0003-3525-9285 NR 5 TC 3 Z9 3 U1 3 U2 14 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 MAY PY 2015 VL 5 IS 5 BP 391 EP 392 PG 3 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA CI6SO UT WOS:000354891900005 ER PT J AU Kok, M Smith, JG Wohl, CJ Siochi, EJ Young, TM AF Kok, Mariana Smith, Joseph G., Jr. Wohl, Christopher J. Siochi, Emilie J. Young, Trevor M. TI Critical considerations in the mitigation of insect residue contamination on aircraft surfaces - A review SO PROGRESS IN AEROSPACE SCIENCES LA English DT Review DE Laminar flow; Insect mitigation; Coatings; Engineered surface testing ID LAMINAR-FLOW CONTROL; INTERMITTENCY TRANSPORT-EQUATION; LEADING-EDGE SURFACES; IMPACT DYNAMICS; DROSOPHILA-MELANOGASTER; MECHANICAL-PROPERTIES; TURBULENT TRANSITION; BYPASS TRANSITION; BOUNDARY-LAYER; DROP IMPACT AB Mitigation of insect residue contamination on next generation aircraft is vital for the commercial exploitation of laminar flow technologies. A review of the critical entomological, meteorological and aeronautical factors affecting insect residue accumulation on aircraft leading edge surfaces is herein presented. An evaluation of a passive mitigation strategy, namely the use of anti-contamination coatings, has been conducted and the key issues in the use of these coatings highlighted. A summary of the variations in major experiments, including laboratory, wind tunnel and flight testing, is outlined. The effects of surface and material characteristics on insect residue adhesion were also investigated, with topographical features of the surface and surface chemistry shown as influential factors. The use of a substitute as an alternative to live insect testing has shown promise. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Kok, Mariana; Young, Trevor M.] Univ Limerick, Dept Mech Aeronaut & Biomed Engn, Limerick, Ireland. [Kok, Mariana; Young, Trevor M.] Univ Limerick, Mat & Surface Sci Inst, Limerick, Ireland. [Smith, Joseph G., Jr.; Wohl, Christopher J.; Siochi, Emilie J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Young, TM (reprint author), Univ Limerick, Dept Mech Aeronaut & Biomed Engn, Limerick, Ireland. EM Trevor.Young@ul.ie NR 165 TC 3 Z9 3 U1 2 U2 15 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0376-0421 J9 PROG AEROSP SCI JI Prog. Aeosp. Sci. PD MAY PY 2015 VL 75 BP 1 EP 14 DI 10.1016/j.paerosci.2015.02.001 PG 14 WC Engineering, Aerospace SC Engineering GA CI8UE UT WOS:000355046400001 ER PT J AU Motagh, M Bahroudi, A Haghighi, MH Samsonov, S Fielding, E Wetzel, HU AF Motagh, Mahdi Bahroudi, Abbas Haghighi, Mahmud Haghshenas Samsonov, Sergey Fielding, Eric Wetzel, Hans-Ulrich TI The 18 August 2014 M-w 6.2 Mormon, Iran, Earthquake: A Thin-Skinned Faulting in the Zagros Mountain Inferred from lnSAR Measurements SO SEISMOLOGICAL RESEARCH LETTERS LA English DT Article ID SIMPLY FOLDED BELT; MICROEARTHQUAKE SEISMICITY; CONTINENTAL COLLISION; SPATIAL-DISTRIBUTION; SURFACE DEFORMATION; BAYESIAN INVERSION; SOURCE PARAMETERS; QESHM EARTHQUAKE; GPS MEASUREMENTS; GEODETIC DATA C1 [Motagh, Mahdi; Haghighi, Mahmud Haghshenas; Wetzel, Hans-Ulrich] GFZ German Res Ctr Geosci, D-14473 Potsdam, Germany. [Bahroudi, Abbas] Univ Tehran, Fac Engn, Sch Min Engn, Explorat Dept, Tehran 51514395, Iran. [Samsonov, Sergey] Nat Resources Canada, Canada Ctr Mapping & Earth Observat, Ottawa, ON K1A 0E4, Canada. [Fielding, Eric] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Motagh, M (reprint author), GFZ German Res Ctr Geosci, Telegrafenberg Haus A17, D-14473 Potsdam, Germany. EM motagh@gfz-potsdam.de FU Initiative and Networking Fund of the Helmholtz Association FX Original RADARSAT-2 data are copyright 2013-2014 MacDonald, Dettwiler and Associates Ltd (MDA). Part of this research was supported by the National Aeronautics and Space Administration's Earth Surface and Interior focus area and performed at the Jet Propulsion Laboratory, California Institute of Technology. We would like to thank Ziyadin Cakir, an anonymous reviewer and the Editor in Chief, Zhigang Peng, for their helpful comments on the original version of the manuscript. This study was supported by the Initiative and Networking Fund of the Helmholtz Association in the frame of Helmholtz Alliance "Remote Sensing and Earth System Dynamics." NR 43 TC 4 Z9 4 U1 0 U2 5 PU SEISMOLOGICAL SOC AMER PI ALBANY PA 400 EVELYN AVE, SUITE 201, ALBANY, CA 94706-1375 USA SN 0895-0695 EI 1938-2057 J9 SEISMOL RES LETT JI Seismol. Res. Lett. PD MAY-JUN PY 2015 VL 86 IS 3 BP 775 EP 782 DI 10.1785/0220140222 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CI3RX UT WOS:000354666200004 ER PT J AU Marubashi, K Akiyama, S Yashiro, S Gopalswamy, N Cho, KS Park, YD AF Marubashi, K. Akiyama, S. Yashiro, S. Gopalswamy, N. Cho, K. -S. Park, Y. -D. TI Geometrical Relationship Between Interplanetary Flux Ropes and Their Solar Sources SO SOLAR PHYSICS LA English DT Article DE Coronal mass ejection (CME); Interplanetary coronal mass ejection (ICME); Interplanetary magnetic flux rope; Magnetic cloud; Solar wind magnetic field ID CORONAL MASS EJECTIONS; MAGNETIC CLOUDS; WIND; MODEL; RECONNECTION; DECREASES; FILAMENTS; ROTATION; HELIOS; SPACE AB We investigated the physical connection between interplanetary flux ropes (IFRs) near Earth and coronal mass ejections (CMEs) by comparing the magnetic field structures of IFRs and CME source regions. The analysis is based on the list of 54 pairs of ICMEs (interplanetary coronal mass ejections) and CMEs that are taken to be the most probable solar source events. We first attempted to identify the flux rope structure in each of the 54 ICMEs by fitting models with a cylinder and torus magnetic field geometry, both with a force-free field structure. This analysis determined the possible geometries of the identified flux ropes. Then we compared the flux rope geometries with the magnetic field structure of the solar source regions. We obtained the following results: (1) Flux rope structures are seen in 51 ICMEs out of the 54. The result implies that all ICMEs have an intrinsic flux rope structure, if the three exceptional cases are attributed to unfavorable observation conditions. (2) It is possible to find flux rope geometries with the main axis orientation close to the orientation of the magnetic polarity inversion line (PIL) in the solar source regions, the differences being less than 25A degrees. (3) The helicity sign of an IFR is strongly controlled by the location of the solar source: flux ropes with positive (negative) helicity are associated with sources in the southern (northern) hemisphere (six exceptions were found). (4) Over two-thirds of the sources in the northern hemisphere are concentrated along PILs with orientations of 45A degrees A +/- 30A degrees (measured clockwise from the east), and over two-thirds in the southern hemisphere along PILs with orientations of 135A degrees A +/- 30A degrees, both corresponding to the Hale boundaries. These results strongly support the idea that a flux rope with the main axis parallel to the PIL erupts in a CME and that the erupted flux rope propagates through the interplanetary space with its orientation maintained and is observed as an IFR. C1 [Akiyama, S.; Yashiro, S.; Gopalswamy, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Akiyama, S.; Yashiro, S.] Catholic Univ Amer, Washington, DC 20064 USA. [Cho, K. -S.; Park, Y. -D.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. EM kmaru_bg@kzh.biglobe.ne.jp FU "Development of Korean Space Weather Center" of KASI; KASI basic research funds FX This work benefited from the NASA/LWS Coordinated Data Analysis Workshops on CME flux ropes in 2010 and 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 Innovacion (Reference number AYA2010-12439-E), Spain. We thank the ACE, Wind, SOHO, and Yohkoh teams for providing the data on line. SOHO is a project of international collaboration between ESA and NASA. The Yohkoh mission was developed and launched by ISAS/JAXA, Japan, with NASA and SERC/PPARC (UK) as international partners. We also thank the BBSO, the MLSO, the Meudon Observatory, The Hida Obserbatory of Kyoto University, and the Catania Astrophysical Observatory teams for providing their H alpha data. K.M., K.-S.C., and Y.-D. Park were supported by the "Development of Korean Space Weather Center" of KASI and the KASI basic research funds. NR 54 TC 9 Z9 9 U1 0 U2 5 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 MAY PY 2015 VL 290 IS 5 BP 1371 EP 1397 DI 10.1007/s11207-015-0681-4 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI1GB UT WOS:000354490200005 ER PT J AU Lin, Y Kim, JW Connell, JW Lebron-Colon, M Siochi, EJ AF Lin, Yi Kim, Jae-Woo Connell, John W. Lebron-Colon, Marisabel Siochi, Emilie J. TI Purification of Carbon Nanotube Sheets SO ADVANCED ENGINEERING MATERIALS LA English DT Article ID SHEET/BISMALEIMIDE NANOCOMPOSITES; FIBERS; PERFORMANCE; YARNS; TRANSPARENT; FILMS AB Large volumes of carbon nanotube (CNT) sheets and yarns are required to enable practical applications such as structural reinforcements, electrical conductors, electromagnetic interference shielding, and energy storage. Although these macroscopic assemblages of CNTs are commercially available, reports on their handling and processing have been quite limited. In this article, we report a systematic study of the purification of commercially available CNT sheets produced directly from as-grown nanotubes. These CNT sheets contain residual metal catalysts encapsulated in graphitic carbon nanoparticles known to contaminate common powdery pristine CNT materials. Although many purification methods effective for powdery CNTs are known, they cannot be directly applied to CNT sheets because these processes often involve sonication and/or reflux, which are too aggressive and deleterious to the integrity of the sheets. Therefore, alternative physically benign processes were chosen and evaluated in detail. Assessment of the purification method included characterization of parameters such as residual metal content, weight retention, and changes in the Raman D-to-G intensity ratio. Importantly, the purification methodology was also placed in the context of the targeted application as a structural reinforcement in advanced composites. In this application, the mechanical properties of the CNT sheets are crucial, thus specific strength and modulus were evaluated and compared for the purified CNT sheets and the nanocomposites produced therefrom. Several important processing parameters were identified that resulted in purified CNT sheets with not only low catalyst content but also reasonable retention of mechanical properties. In addition, the scalability of the purification method and a procedure to prevent CNT sheet wrinkling after purification were demonstrated. Assessment criteria of CNT sheet purification techniques toward other potential applications are also discussed. C1 [Lin, Yi; Kim, Jae-Woo] Natl Inst Aerosp, Hampton, VA 23666 USA. [Lin, Yi] Coll William & Mary, Dept Appl Sci, Williamsburg, VA 23185 USA. [Connell, John W.; Siochi, Emilie J.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. [Lebron-Colon, Marisabel] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. RP Lin, Y (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA. EM yi.lin@nianet.org; emilie.j.siochi@nasa.gov RI Kim, Jae-Woo/A-8314-2008 FU NASA Game Changing Development Program FX The financial support from the NASA Game Changing Development Program is gratefully acknowledged. We thank C. Chamberlain (NASA LaRC) for assistance in thermogravimetric measurements, and Dr. W. Cao and Prof. H. E. Elsayed-Ali (Applied Research Center at Old Dominion University) for HR-TEM/EDS acquisitions. NR 31 TC 2 Z9 2 U1 3 U2 42 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 1438-1656 EI 1527-2648 J9 ADV ENG MATER JI Adv. Eng. Mater. PD MAY PY 2015 VL 17 IS 5 BP 674 EP 688 DI 10.1002/adem.201400306 PG 15 WC Materials Science, Multidisciplinary SC Materials Science GA CI0HI UT WOS:000354417300014 ER PT J AU Xiong, MY Shelobolina, ES Roden, EE AF Xiong, Mai Yia Shelobolina, Evgenya S. Roden, Eric E. TI Potential for Microbial Oxidation of Ferrous Iron in Basaltic Glass SO ASTROBIOLOGY LA English DT Article ID FE-OXIDIZING BACTERIA; NEUTRAL PH; WATER ENVIRONMENTS; OCEAN CRUST; NITRATE; FE(II); SEQUENCES; MINERALS; ROCKS; MARS AB Basaltic glass (BG) is an amorphous ferrous iron [Fe(II)]-containing material present in basaltic rocks, which are abundant on rocky planets such as Earth and Mars. Previous research has suggested that Fe(II) in BG can serve as an energy source for chemolithotrophic microbial metabolism, which has important ramifications for potential past and present microbial life on Mars. However, to date there has been no direct demonstration of microbially catalyzed oxidation of Fe(II) in BG. In this study, three different culture systems were used to investigate the potential for microbial oxidation of Fe(II) in BG, including (1) the chemolithoautotrophic Fe(II)-oxidizing, nitrate-reducing "Straub culture"; (2) the mixotrophic Fe(II)-oxidizing, nitrate-reducing organism Desulfitobacterium frappieri strain G2; and (3) indigenous microorganisms from a streambed Fe seep in Wisconsin. The BG employed consisted of clay and silt-sized particles of freshly quenched lava from the TEB flow in Kilauea, Hawaii. Soluble Fe(II) or chemically reduced NAu-2 smectite (RS) were employed as positive controls to verify Fe(II) oxidation activity in the culture systems. All three systems demonstrated oxidation of soluble Fe(II) and/or structural Fe(II) in RS, whereas no oxidation of Fe(II) in BG material was observed. The inability of the Straub culture to oxidize Fe(II) in BG was particularly surprising, as this culture can oxidize other insoluble Fe(II)-bearing minerals such as biotite, magnetite, and siderite. Although the reason for the resistance of the BG toward enzymatic oxidation remains unknown, it seems possible that the absence of distinct crystal faces or edge sites in the amorphous glass renders the material resistant to such attack. These findings have implications with regard to the idea that Fe(II)-Si-rich phases in basalt rocks could provide a basis for chemolithotrophic microbial life on Mars, specifically in neutral-pH environments where acid-promoted mineral dissolution and utilization of dissolved Fe(II) as an energy source is not likely to take place. Key Words: Basaltic glass-Chemolithotrophic-Microbial-Iron oxidation-Mars. Astrobiology 15, 331-340. C1 [Roden, Eric E.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. Univ Wisconsin, NASA Astrobiol Inst, Madison, WI USA. RP Roden, EE (reprint author), Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. EM eroden@geology.wisc.edu FU NASA Astrobiology Institute FX This work was supported by the NASA Astrobiology Institute. We gratefully acknowledge B. Converse for assistance with the 16S rRNA gene pyrosequencing analysis and Tao Wu for assistance with mineralogical analysis. NR 59 TC 0 Z9 0 U1 7 U2 29 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD MAY 1 PY 2015 VL 15 IS 5 BP 331 EP 340 DI 10.1089/ast.2014.1233 PG 10 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA CI2XV UT WOS:000354612400002 PM 25915449 ER PT J AU Assef, RJ Eisenhardt, PRM Stern, D Tsai, CW Wu, J Wylezalek, D Blain, AW Bridge, CR Donoso, E Gonzales, A Griffith, RL Jarrett, TH AF Assef, R. J. Eisenhardt, P. R. M. Stern, D. Tsai, C. -W. Wu, J. Wylezalek, D. Blain, A. W. Bridge, C. R. Donoso, E. Gonzales, A. Griffith, R. L. Jarrett, T. H. TI HALF OF THE MOST LUMINOUS QUASARS MAY BE OBSCURED: INVESTIGATING THE NATURE OF WISE-SELECTED HOT DUST-OBSCURED GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: high-redshift; infrared: galaxies; quasars: general ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASS; STELLAR POPULATION SYNTHESIS; SIMILAR-TO 2; INFRARED-SURVEY-EXPLORER; SPITZER-SPACE-TELESCOPE; LY-ALPHA EMITTERS; LESS-THAN 3.2; HIGH-REDSHIFT; SUBMILLIMETER GALAXIES AB The Wide-field Infrared Survey Explorer mission has unveiled a rare population of high-redshift (z = 1-4.6), dusty, hyper-luminous galaxies, with infrared luminosities L-IR > 10(13) L-circle dot, and sometimes exceeding 10(14) L-circle dot. Previous work has shown that their dust temperatures and overall far-infrared spectral energy distributions (SEDs) are significantly hotter than expected to be powered by star formation. We present here an analysis of the rest-frame optical through mid-infrared SEDs for a large sample of these so-called "hot, dust-obscured galaxies" (Hot DOGs). We find that the SEDs of Hot DOGs are generally well modeled by the combination of a luminous, yet obscured active galactic nuclei (AGNs) that dominates the rest-frame emission at lambda > 1 mu m and the bolometric luminosity output, and a less luminous host galaxy that is responsible for the bulk of the rest optical/UV emission. Even though the stellar mass of the host galaxies may be as large as 10(11) - 10(12) M-circle dot, the AGN emission, with a range of luminosities comparable to those of the most luminous QSOs known, require that either Hot DOGs have black hole masses significantly in excess of the local relations, or that they radiate significantly above the Eddington limit, at a level at least 10 times more efficiently than z similar to 2 QSOs. We show that, while rare, the number density of Hot DOGs is comparable to that of equally luminous but unobscured (i.e., Type 1) QSOs. This may be at odds with the trend suggested at lower luminosities for the fraction of obscured AGNs to decrease with increasing luminosity. That trend may, instead, reverse at higher luminosities. Alternatively, Hot DOGs may not be the torus-obscured counterparts of the known optically selected, largely unobscured, hyper-luminous QSOs, and may represent a new component of the galaxy evolution paradigm. Finally, we discuss the environments of Hot DOGs and statistically show that these objects are in regions as dense as those of known high-redshift protoclusters. C1 [Assef, R. J.] Univ Diego Port, Nucl Astron Fac Ingn, Santiago, Chile. [Eisenhardt, P. R. M.; Stern, D.; Tsai, C. -W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wu, J.] Univ Calif Los Angeles, Astron, Los Angeles, CA 90095 USA. [Wylezalek, D.] European So Observ, D-85748 Garching, Germany. [Blain, A. W.] Univ Leicester, Phys & Astron, Leicester LE1 7RH, Leics, England. [Bridge, C. R.; Gonzales, A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Donoso, E.] ICATE, RA-5400 San Juan, Argentina. [Gonzales, A.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Gonzales, A.] Scripps Coll, Claremont, CA 91711 USA. [Griffith, R. L.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Jarrett, T. H.] Univ Cape Town, Dept Astron, ACGC, ZA-7701 Rondebosch, South Africa. RP Assef, RJ (reprint author), Univ Diego Port, Nucl Astron Fac Ingn, Av Ejercito Libertador 441, Santiago, Chile. EM roberto.assef@mail.udp.cl FU Gemini-CONICYT [32120009]; National Aeronautics and Space Administration [13-ADAP13-0092] FX We are indebted to all WISE team members. We thank the anonymous referee for comments and suggestions that helped to improve this article. RJA was supported by Gemini-CONICYT grant number 32120009. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. 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. Kitt Peak National Observatory and CTIO, National Optical Astronomy Observatory, are operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. The WIYN Observatory is a joint facility of the University of Wisconsin-Madison, Indiana University, Yale University, and the National Optical Astronomy Observatory. The SOAR Telescope is a joint project of: Conselho Nacional de Pesquisas Cientificas e Tecnologicas CNPq-Brazil, The University of North Carolina at Chapel Hill, Michigan State University, and the National Optical Astronomy Observatory. Based partly on observations obtained at the Hale Telescope, Palomar Observatory as part of a continuing collaboration between the California Institute of Technology, NASA/JPL, NOAO, Oxford University, Stony Brook University, and the National Astronomical Observatories of China. This material is based upon work supported by the National Aeronautics and Space Administration under Proposal No. 13-ADAP13-0092 issued through the Astrophysics Data Analysis Program. NR 84 TC 32 Z9 32 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2015 VL 804 IS 1 AR 27 DI 10.1088/0004-637X/804/1/27 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH7BB UT WOS:000354189500027 ER PT J AU Crossfield, IJM Petigura, E Schlieder, JE Howard, AW Fulton, BJ Aller, KM Ciardi, DR Lepine, S Barclay, T De Pater, I De Kleer, K Quintana, EV Christiansen, JL Schlafly, E Kaltenegger, L Crepp, JR Henning, T Obermeier, C Deacon, N Weiss, LM Isaacson, HT Hansen, BMS Liu, MC Greene, T Howell, SB Barman, T Mordasini, C AF Crossfield, Ian J. M. Petigura, Erik Schlieder, Joshua E. Howard, Andrew W. Fulton, B. J. Aller, Kimberly M. Ciardi, David R. Lepine, Sebastien Barclay, Thomas De Pater, Imke De Kleer, Katherine Quintana, Elisa V. Christiansen, Jessie L. Schlafly, Eddie Kaltenegger, Lisa Crepp, Justin R. Henning, Thomas Obermeier, Christian Deacon, Niall Weiss, Lauren M. Isaacson, Howard T. Hansen, Brad M. S. Liu, Michael C. Greene, Tom Howell, Steve B. Barman, Travis Mordasini, Christoph TI A NEARBY M STAR WITH THREE TRANSITING SUPER-EARTHS DISCOVERED BY K2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; stars: individual (EPIC 201367065); techniques: photometric; techniques: spectroscopic ID DIGITAL SKY SURVEY; MAIN-SEQUENCE STARS; M-DWARFS; LOW-MASS; LIGHT CURVES; SPECTROSCOPIC SURVEY; PLANET CANDIDATES; KINEMATIC GROUPS; FALSE POSITIVES; BLEND SCENARIOS AB Small, cool planets represent the typical end-products of planetary formation. Studying the architectures of these systems, measuring planet masses and radii, and observing these planets' atmospheres during transit directly informs theories of planet assembly, migration, and evolution. Here we report the discovery of three small planets orbiting a bright (K-s = 8.6 mag) M0 dwarf using data collected as part of K2, the new ecliptic survey using the repurposed Kepler spacecraft. Stellar spectroscopy and K2 photometry indicate that the system hosts three transiting planets with radii 1.5-2.1 R-circle plus, straddling the transition region between rocky and increasingly volatile-dominated compositions. With orbital periods of 10-45 days the planets receive just 1.5-10x the flux incident on Earth, making these some of the coolest small planets known orbiting a nearby star; planet d is located near the inner edge of the system's habitable zone. The bright, low-mass star makes this system an excellent laboratory to determine the planets' masses via Doppler spectroscopy and to constrain their atmospheric compositions via transit spectroscopy. This discovery demonstrates the ability of K2 and future space-based transit searches to find many fascinating objects of interest. C1 [Crossfield, Ian J. M.; Barman, Travis] Univ Arizona Lunar, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Petigura, Erik; De Pater, Imke; De Kleer, Katherine; Weiss, Lauren M.; Isaacson, Howard T.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Schlieder, Joshua E.; Barclay, Thomas; Quintana, Elisa V.; Greene, Tom; Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Howard, Andrew W.; Fulton, B. J.; Aller, Kimberly M.; Liu, Michael C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Ciardi, David R.; Christiansen, Jessie L.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Lepine, Sebastien] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Schlafly, Eddie; Henning, Thomas; Obermeier, Christian; Mordasini, Christoph] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Deacon, Niall] Univ Hertfordshire, Coll Lane, Hatfield AL10 9AB, Herts, England. [Hansen, Brad M. S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA. [Kaltenegger, Lisa] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Crossfield, Ian J. M.; Mordasini, Christoph] Inst Phys, CH-3012 Bern, Switzerland. RP Crossfield, IJM (reprint author), Univ Arizona Lunar, Lunar & Planetary Lab, 1629 E Univ Blvd, Tucson, AZ 85721 USA. EM ianc@lpl.arizona.edu OI Weiss, Lauren/0000-0002-3725-3058; Ciardi, David/0000-0002-5741-3047; Schlafly, Edward Ford/0000-0002-3569-7421 FU NASA [NNX12AJ23G, NNH14CK55B]; NSF [AST 09-08419] FX We thank Geoff Marcy, Evan Sinukoff, and Charles Beichman for helpful conversations; Vishnu Reddy for swapping SpeX time; and Steve Bryson and our referee Don Pollacco for useful comments that improved the quality of this manuscript. A. W.H. acknowledges NASA grant No. NNX12AJ23G, and S.L. acknowledges NSF grant No. AST 09-08419. This work made use of the SIMBAD database (operated at CDS, Strasbourg, France); NASA's Astrophysics Data System Bibliographic Services; the Authorea collaborative writing website; the NASA Exoplanet Archive; and Infrared Science Archive, and data products from the Two Micron All Sky Survey (2MASS), the APASS database, the SDSS-III project, the Digitized Sky Survey, and the Wide-Field Infrared Survey Explorer. Portions of this work were performed at the California Institute of Technology under contract with the National Aeronautics and Space Administration. Some of the data presented herein were obtained at the W. M. Keck Observatory (which is operated as a scientific partnership among Caltech, UC, and NASA) and at the Infrared Telescope Facility (IRTF, operated by UH under NASA contract NNH14CK55B). The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 84 TC 47 Z9 47 U1 2 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2015 VL 804 IS 1 AR 10 DI 10.1088/0004-637X/804/1/10 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH7BB UT WOS:000354189500010 ER PT J AU Cucchiara, A Fumagalli, M Rafelski, M Kocevski, D Prochaska, JX Cooke, RJ Becker, GD AF Cucchiara, A. Fumagalli, M. Rafelski, M. Kocevski, D. Prochaska, J. X. Cooke, R. J. Becker, G. D. TI UNVEILING THE SECRETS OF METALLICITY AND MASSIVE STAR FORMATION USING DLAS ALONG GAMMA-RAY BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: general; galaxies: ISM; gamma-ray burst: general; quasars: absorption lines; techniques: imaging spectroscopy ID DAMPED LY-ALPHA; GRB AFTERGLOW SPECTRA; HIGH-RESOLUTION SPECTROSCOPY; VLT/X-SHOOTER SPECTROSCOPY; COSMIC CHEMICAL EVOLUTION; MAGELLAN UNIFORM SURVEY; HUBBLE-SPACE-TELESCOPE; HIGH COLUMN DENSITY; SIMILAR-TO 5; HOST GALAXY AB We present the largest, publicly available sample of damped Ly alpha systems (DLAs) along the lines of sight of Swift-discovered gamma-ray bursts (GRBs). in order to investigate the environmental properties of long GRB hosts in the z = 1.8-6 redshift range. Compared with the most recent quasar DLA sample (QSO-DLA), our analysis shows that GRB-DLAs probe a more metal-enriched environment at z greater than or similar to 3, up to [X/H] similar to -0.5. In the z = 2-3 redshift range, despite the large number of lower limits, there are hints that the two populations may be more similar (only at a 90% significance level) than at higher redshifts. Also, at high-z, the GRB-DLA average metallicity seems to decline at a lower rate than the QSO-DLAs: GRB-DLA hosts may be polluted with metals at least as far as similar to 2 kpc from the GRB explosion site, probably due to previous star formation episodes and/or supernova explosions. This shallow metallicity trend, now extended up to z similar to 5, confirms previous results that GRB hosts are star-forming and have, on average, higher metallicities. than the general QSO-DLA population. Finally, our host metallicity measurements are broadly consistent with the predictions derived from the hypothesis of two channels of GRB progenitors, one of which is mildly affected by a metallicity bias, although more data are needed to constrain the models at z greater than or similar to 4. C1 [Cucchiara, A.; Rafelski, M.; Kocevski, D.] NASA, Goddard Space Flight Ctr, Postdoctoral Program, Greenbelt, MD 20771 USA. [Fumagalli, M.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. [Fumagalli, M.] Carnegie Observ, Pasadena, CA 91101 USA. [Prochaska, J. X.; Cooke, R. J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Becker, G. D.] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Becker, G. D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Cucchiara, A (reprint author), NASA, Goddard Space Flight Ctr, Postdoctoral Program, Greenbelt, MD 20771 USA. EM antonino.cucchiara@nasa.gov RI Fumagalli, Michele/K-9510-2015 OI Fumagalli, Michele/0000-0001-6676-3842 FU NASA Postdoctoral Program at the Goddard Space Flight Center; Science and Technology Facilities Council [ST/L00075X/1] FX This research was supported by the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. A.C. thanks M.F. and M.R. for the incredible support and useful discussions during the writing of this work. A.C. also thanks M.T. for fundamental discussion as well for providing the models' curves. M.F. acknowledges support by the Science and Technology Facilities Council (Grant #ST/L00075X/1). A.C. thanks P. D'Avanzo for providing the spectrum of GRB 090205A. NR 158 TC 20 Z9 20 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 MAY 1 PY 2015 VL 804 IS 1 AR 51 DI 10.1088/0004-637X/804/1/51 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH7BB UT WOS:000354189500051 ER PT J AU Desert, JM Charbonneau, D Torres, G Fressin, F Ballard, S Bryson, ST Knutson, HA Batalha, NM Borucki, WJ Brown, TM Deming, D Ford, EB Fortney, JJ Gilliland, RL Latham, DW Seager, S AF Desert, Jean-Michel Charbonneau, David Torres, Guillermo Fressin, Francois Ballard, Sarah Bryson, Stephen T. Knutson, Heather A. Batalha, Natalie M. Borucki, William J. Brown, Timothy M. Deming, Drake Ford, Eric B. Fortney, Jonathan J. Gilliland, Ronald L. Latham, David W. Seager, Sara TI LOW FALSE POSITIVE RATE OF KEPLER CANDIDATES ESTIMATED FROM A COMBINATION OF SPITZER AND FOLLOW-UP OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; eclipses; planetary systems; planets and satellites: detection; techniques: polarimetric ID TRANSIT TIMING VARIATIONS; SUN-LIKE STAR; INFRARED ARRAY CAMERA; MULTIPLE-PLANET SYSTEMS; EXOPLANET HD 189733B; CIRCLE-PLUS PLANET; HABITABLE-ZONE; SPACE-TELESCOPE; ECLIPSING BINARIES; EXTRASOLAR PLANET AB NASA's Kepler mission has provided several thousand transiting planet candidates during the 4 yr of its nominal mission, yet only a small subset of these candidates have been confirmed as true planets. Therefore, the most fundamental question about these candidates is the fraction of bona fide planets. Estimating the rate of false positives of the overall Kepler sample is necessary to derive the planet occurrence rate. We present the results from two large observational campaigns that were conducted with the Spitzer Space Telescope during the the Kepler mission. These observations are dedicated to estimating the false positive rate (FPR) among the Kepler candidates. We select a sub-sample of 51 candidates, spanning wide ranges in stellar, orbital, and planetary parameter space, and we observe their transits with Spitzer at 4.5 mu m. We use these observations to measures the candidate's transit depths and infrared magnitudes. An authentic planet produces an achromatic transit depth (neglecting the modest effect of limb darkening). Conversely a bandpass-dependent depth alerts us to the potential presence of a blending star that could be the source of the observed eclipse: a false positive scenario. For most of the candidates (85%), the transit depths measured with Kepler are consistent with the transit depths measured with Spitzer as expected for planetary objects, while we find that the most discrepant measurements are due to the presence of unresolved stars that dilute the photometry. The Spitzer constraints on their own yield FPRs between 5% and depending on the Kepler Objects of Interest. By considering the population of the Kepler field stars, and by combining follow-up observations (imaging) when available, we find that the overall FPR of our sample is low. The measured upper limit on the FPR of our sample is 8.8% at a confidence level of 3 sigma. This observational result, which uses the achromatic property of planetary transit signals that is not investigated by the Kepler observations, provides an independent indication that Kepler's FPR is low. C1 [Desert, Jean-Michel; Brown, Timothy M.] Univ Colorado, CASA, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Desert, Jean-Michel; Knutson, Heather A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Charbonneau, David; Torres, Guillermo; Fressin, Francois; Ballard, Sarah; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ballard, Sarah] Univ Washington, Seattle, WA 98195 USA. [Bryson, Stephen T.; Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Batalha, Natalie M.] San Jose State Univ, San Jose, CA 95192 USA. [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Ford, Eric B.] Univ Florida, Gainesville, FL 32611 USA. [Ford, Eric B.; Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Seager, Sara] MIT, Cambridge, MA 02159 USA. RP Desert, JM (reprint author), Univ Colorado, CASA, Dept Astrophys & Planetary Sci, 389-UCB, Boulder, CO 80309 USA. EM desert@colorado.edu OI /0000-0001-6545-639X FU NASA's Science Mission Directorate; NASA; NASA Kepler Mission Participating Scientist Program [NNX09AB53G, NNX12AC77G, NNX12AC75G, NNX14AB83G]; John Templeton Foundation; National Aeronautics and Space Administration FX We thank the anonymous reviewer for the careful reading of our manuscript and the valuable comments. This work is based on observations made with Kepler, which was competitively selected as the 10th Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. The authors would like to thank the many people who generously gave so much of their time to make this mission a success. This work is also based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. D.C. acknowledges support for this work from grants NNX09AB53G and NNX12AC77G, and G.T. acknowledges support from grants NNX12AC75G and NNX14AB83G, each from the NASA Kepler Mission Participating Scientist Program. D.C. acknowledges the support of a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. We would like to thank the Spitzer staff at IPAC and in particular Nancy Silbermann for scheduling the Spitzer observations of this program. J.-M.D. and S.B. acknowledge the Sagan Exoplanet Fellowship program supported by the National Aeronautics and Space Administration and administered by the NASA Exoplanet Science Institute (NExScI). We thank Samaya Nissanke for careful reading of the manuscript. NR 108 TC 15 Z9 15 U1 4 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2015 VL 804 IS 1 AR 59 DI 10.1088/0004-637X/804/1/59 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH7BB UT WOS:000354189500059 ER PT J AU Gorti, U Hollenbach, D Dullemond, CP AF Gorti, U. Hollenbach, D. Dullemond, C. P. TI THE IMPACT OF DUST EVOLUTION AND PHOTOEVAPORATION ON DISK DISPERSAL SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: formation; protoplanetary disks; stars: formation; stars: winds; outflows ID T-TAURI STARS; TURBULENT PROTOPLANETARY DISKS; GIANT-PLANET FORMATION; HERBIG AE STARS; X-RAY-RADIATION; CIRCUMSTELLAR DISKS; FAR-ULTRAVIOLET; EXTREME-ULTRAVIOLET; MOLECULE FORMATION; INFRARED-EMISSION AB Protoplanetary disks are dispersed by viscous evolution and photoevaporation in a few million years; in the interim small, sub-micron-sized dust grains must grow and form planets. The time-varying abundance of small grains in an evolving disk directly affects gas heating by far-ultraviolet (FUV) photons, while dust evolution affects photoevaporation by changing the disk opacity and resulting penetration of FUV photons in the disk. Photoevaporative flows, in turn, selectively carry small dust grains, leaving the larger particles-which decouple, from the gas-behind in the disk. We study these effects by investigating the evolution of a disk subject to viscosity, photoevaporation by EUV, FUV, and X-rays, dust evolution, and radial drift using a one-dimensional (1D) multi-fluid approach (gas + different dust grain sizes) to solve for the evolving surface density distributions. The 1D evolution is augmented by 1+1D models constructed at each epoch to obtain the instantaneous disk structure and determine photoevaporation rates. The implementation of a dust coagulation/fragmentation model results in a marginal decrease in disk lifetimes when compared to models with no dust evolution; the disk lifetime is thus found to be relatively insensitive to the evolving dust opacity. We find that photoevaporation can cause significant reductions in the gas/dust mass ratio in the planet-forming regions of the disk as it evolves, and may result in a corresponding increase in heavy element abundances relative to hydrogen. We discuss implications for theories of planetesimal formation and giant planet formation, including the formation of gas-poor giants. After gas disk dispersal, similar to 3 x 10(-4) M-circle dot of mass in solids typically remain, comparable to the solids inventory of our solar system. C1 [Gorti, U.; Hollenbach, D.] SETI Inst, Mountain View, CA 94043 USA. [Gorti, U.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Dullemond, C. P.] Heidelberg Univ, D-69115 Heidelberg, Germany. RP Gorti, U (reprint author), SETI Inst, Mountain View, CA 94043 USA. OI Dullemond, Cornelis/0000-0002-7078-5910 FU NASA [NNX09AO42G]; DFG [DU 414/9-1] FX U.G. acknowledges several helpful discussions with Jeff Cuzzi, Chris Ormel and Til Birnstiel. U.G. and D.H. acknowledge funding from NASA Award NNX09AO42G which made this work possible. This project made use of NASA HEC supercomputing resources. C.P.D. acknowledges funding from DFG grant DU 414/9-1. NR 114 TC 29 Z9 29 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2015 VL 804 IS 1 AR 29 DI 10.1088/0004-637X/804/1/29 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH7BB UT WOS:000354189500029 ER EF