FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Simoes, F Pfaff, R Freudenreich, H Klenzing, J Rowland, D Bromund, K Kepko, L Le, G Liebrecht, MC Martin, S Uribe, P AF Simoes, Fernando Pfaff, Robert Freudenreich, Henry Klenzing, Jeffrey Rowland, Douglas Bromund, Kenneth Kepko, Larry Le, Guan Liebrecht, Maria Carmen Martin, Steven Uribe, Paulo TI Equatorial ionosphere semiannual oscillation investigated from Schumann resonance measurements on board the C/NOFS satellite SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TROPICAL MIDDLE ATMOSPHERE; SOLAR-CYCLE VARIATIONS; SEASONAL-VARIATIONS; ELECTRON-DENSITY; FREQUENCY; TEMPERATURE; VARIABILITY; INTENSITY; REGION; MODEL AB Detection of Schumann resonance signatures in the equatorial ionosphere offers remote sensing capabilities for the investigation of tropospheric and space weather effects in the ionosphere. Schumann resonances are electromagnetic oscillations in the earth-ionosphere cavity produced by lightning activity. Analysis of AC electric field measurements gathered by the Communications/Navigation Outage Forecasting System satellite reveals a semiannual pattern in Schumann resonance data recorded during nighttime in the equatorial ionosphere. This pattern observed in the Schumann resonance amplitude is expected to help validate-or at least constrain-potential mechanisms proposed to explain the semiannual oscillation observed in different geophysical records, such as those reported in a variety of tropospheric, ionospheric/thermospheric, and magnetospheric observations. C1 [Simoes, Fernando; Pfaff, Robert; Freudenreich, Henry; Klenzing, Jeffrey; Rowland, Douglas; Bromund, Kenneth; Kepko, Larry; Le, Guan; Martin, Steven; Uribe, Paulo] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Space Weather Lab, Greenbelt, MD 20771 USA. [Freudenreich, Henry; Martin, Steven] ADNET Syst Inc, Rockville, MD USA. [Liebrecht, Maria Carmen] Sigma Space Corp, Lanham, MD USA. RP Simoes, F (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Space Weather Lab, Code 674,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM fernando.a.simoes.nasa@gmail.com RI Kepko, Larry/D-7747-2012; Rowland, Douglas/F-5589-2012; Klenzing, Jeff/E-2406-2011; Le, Guan/C-9524-2012 OI Kepko, Larry/0000-0002-4911-8208; Rowland, Douglas/0000-0003-0948-6257; Klenzing, Jeff/0000-0001-8321-6074; Le, Guan/0000-0002-9504-5214 FU USAF Space Test Program; Air Force Office of Scientific Research FX The Communication/Navigation Outage Forecast System (C/NOFS) mission, conceived and developed by the U.S. Air Force Research Laboratory, is sponsored and executed by the USAF Space Test Program. We acknowledge support from the Air Force Office of Scientific Research. FS is supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 37 TC 1 Z9 1 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 16 PY 2013 VL 118 IS 21 BP 12045 EP 12051 DI 10.1002/jgrd.50797 PG 7 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 302NS UT WOS:000330611800009 ER PT J AU Christensen, MW Stephens, GL Lebsock, MD AF Christensen, Matthew W. Stephens, Graeme L. Lebsock, Matthew D. TI Exposing biases in retrieved low cloud properties from CloudSat: A guide for evaluating observations and climate data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID LIQUID WATER PATH; RADIATIVE IMPACTS; WARM RAIN; PART II; MICROPHYSICS; PRECIPITATION; SYSTEM; MODIS; MACROPHYSICS; AEROSOLS AB This study provides an assessment of low cloud properties retrieved from CloudSat, MODIS (Moderate Resolution Imaging Spectroradiometer), and Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation with the goal of exposing biases that hinder meaningful comparisons with the simulated cloud properties in global climate models (GCMs). Being pertinent to GCM comparisons, CloudSat is the only satellite that can provide the vertical structure of cloud water and ice content from space. Biases in CloudSat low cloud properties are found to be tied to problems involving cloud detection and algorithm retrieval failures related to precipitation and strict cloud screening procedures. We show that MODIS and CloudSat cloud liquid water path (LWP) data agree when carefully screened for lack of precipitation but significantly depart in precipitating clouds due to rain water contamination of LWP in the CloudSat retrieval algorithm. The presence of drizzle and rain (occurring about 20% of the time) is associated with different mean LWP, mean particle sizes, and optical depths of all low clouds and therefore the radiative properties of the oceanic low clouds. Another more significant source of the LWP bias stems from the apparent lack of cloud detection. On average, the Cloud Profiling Radar misses clouds with adequate liquid and ice water retrievals as detected by MODIS in approximately 45% of warm clouds with the bulk of the bias occurring in clouds below 1 km in the so-called "ground clutter zone." By incorporating additional sensors such as MODIS, the following results suggest that this LWP bias can be greatly reduced. C1 [Christensen, Matthew W.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Stephens, Graeme L.; Lebsock, Matthew D.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Christensen, MW (reprint author), Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. EM chrismat@atmos.colostate.edu RI Christensen, Matthew/C-5733-2013 FU NASA [NNN13D771T] FX We would like to thank the reviewers for their helpful input and comments in writing this paper. This research was supported by NASA grant NNN13D771T. 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 42 TC 15 Z9 15 U1 1 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 NOV 16 PY 2013 VL 118 IS 21 BP 12120 EP 12131 DI 10.1002/2013JD020224 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 302NS UT WOS:000330611800015 ER PT J AU Yang, ZF Wang, J Ichoku, C Hyer, E Zeng, J AF Yang, Zhifeng Wang, Jun Ichoku, Charles Hyer, Edward Zeng, Jing TI Mesoscale modeling and satellite observation of transport and mixing of smoke and dust particles over northern sub-Saharan African region SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID PIXEL-BASED CALCULATION; AEROSOL OPTICAL DEPTH; FIRE RADIATIVE ENERGY; INITIAL ASSESSMENT; DATA ASSIMILATION; MINERAL DUST; WEST-AFRICA; NILE DELTA; MODIS; ALGORITHM AB The transport and vertical distribution of smoke and dust aerosols over the northern sub-Saharan African region are simulated in the Weather Research and Forecasting model with Chemistry (WRF-Chem), which uses hourly dynamic smoke emissions from the Fire Locating and Modeling of Burning Emissions database derived from the Moderate Resolution Imaging Spectroradiometer (MODIS) fire products. Model performance for February 2008 is evaluated using MODIS true color images, aerosol optical depth (AOD) measurements from the Aerosol Robotic Network, MODIS AOD retrievals, and the Cloud-Aerosol Lidar data with Orthogonal Polarization (CALIOP) atmospheric backscattering and extinction products. Specification of smoke injection height of 650m in WRF-Chem yields aerosol vertical profiles that are most consistent with CALIOP observations of aerosol layer height. Between the equator and 10 degrees N, Saharan dust is often mixed with smoke near the surface, and their transport patterns manifest the interplay of trade winds, subtropical highs, precipitation associated with the Intertropical Convergence Zone, and the high mountains located near the Great Rift Valley region. At the 700 hPa level and above, smoke layers spread farther to the north and south and are often above the dust layers over the Sahel region. In some cases, transported smoke can also be mixed with dust over the Saharan region. Statistically, 5% of the CALIOP valid measurements in February 2007-2011 show aerosol layers either above or between the clouds, reinforcing the importance of the aerosol vertical distribution for quantifying aerosol impact on climate in the Sahel region. C1 [Yang, Zhifeng; Wang, Jun; Zeng, Jing] Univ Nebraska, Lincoln, NE 68588 USA. [Ichoku, Charles] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD 20771 USA. [Hyer, Edward] Naval Res Lab, Marine Meteorol Div, Monterey, CA USA. RP Wang, J (reprint author), Univ Nebraska, Lincoln, NE 68588 USA. EM jwang7@unl.edu RI Ichoku, Charles/E-1857-2012; Hyer, Edward/E-7734-2011; Yang, Zhifeng/I-8253-2015; Wang, Jun/A-2977-2008 OI Ichoku, Charles/0000-0003-3244-4549; Hyer, Edward/0000-0001-8636-2026; Wang, Jun/0000-0002-7334-0490 FU Science Mission Directorate of the National Aeronautics and Space Administration (NASA) as part of the Interdisciplinary Studies (IDS) FX This research was supported by the Science Mission Directorate of the National Aeronautics and Space Administration (NASA) as part of the Interdisciplinary Studies (IDS) conducted through the Radiation Sciences Program managed by Hal B. Maring. Part of the computational support in this research is also provided by the Holland Computing Center of the University of Nebraska. J. Wang also thank Dr. Robert Oglesby and Dr. Qi (Steve) Hu at the University of Nebraska-Lincoln for their constructive comments. NR 67 TC 14 Z9 14 U1 0 U2 20 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 NOV 16 PY 2013 VL 118 IS 21 BP 12139 EP 12157 DI 10.1002/2013JD020644 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 302NS UT WOS:000330611800017 ER PT J AU Shinozuka, Y Johnson, RR Flynn, CJ Russell, PB Schmid, B Redemann, J Dunagan, SE Kluzek, CD Hubbe, JM Segal-Rosenheimer, M Livingston, JM Eck, TF Wagener, R Gregory, L Chand, D Berg, LK Rogers, RR Ferrare, RA Hair, JW Hostetler, CA Burton, SP AF Shinozuka, Y. Johnson, R. R. Flynn, C. J. Russell, P. B. Schmid, B. Redemann, J. Dunagan, S. E. Kluzek, C. D. Hubbe, J. M. Segal-Rosenheimer, M. Livingston, J. M. Eck, T. F. Wagener, R. Gregory, L. Chand, D. Berg, L. K. Rogers, R. R. Ferrare, R. A. Hair, J. W. Hostetler, C. A. Burton, S. P. TI Hyperspectral aerosol optical depths from TCAP flights SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID AIRBORNE SUN PHOTOMETER; SPECTRAL-RESOLUTION LIDAR; COLUMNAR WATER-VAPOR; LOWER TROPOSPHERIC AEROSOL; GROUND-BASED MEASUREMENTS; SOLVE-II; IN-SITU; SUNPHOTOMETER MEASUREMENTS; SATELLITE MEASUREMENTS; SOLAR IRRADIANCE AB The 4STAR (Spectrometer for Sky-Scanning, Sun-Tracking Atmospheric Research), a hyperspectral airborne Sun photometer, acquired aerosol optical depths (AOD) at 1 Hz during all July 2012 flights of the Two-Column Aerosol Project. Root-mean-square differences from Aerosol Robotic Network ground-based observations were 0.01 at wavelengths between 500-1020 nm, 0.02 at 380 and 1640 nm, and 0.03 at 440 nm in four clear-sky fly-over events, and similar in ground side-by-side comparisons. Changes in the above-aircraft AOD across 3 km deep spirals were typically consistent with integrals of coincident in situ (on Department of Energy Gulfstream 1 with 4STAR) and lidar (on NASA B200) extinction measurements within 0.01, 0.03, 0.01, 0.02, 0.02, and 0.02 at 355, 450, 532, 550, 700, and 1064 nm, respectively, despite atmospheric variations and combined measurement uncertainties. Finer vertical differentials of the 4STAR measurements matched the in situ ambient extinction profile within 14% for one homogeneous column. For the AOD observed between 350 and 1660 nm, excluding strong water vapor and oxygen absorption bands, estimated uncertainties were similar to 0.01 and dominated by (then) unpredictable throughput changes, up to +/-0.8%, of the fiber optic rotary joint. The favorable intercomparisons herald 4STAR's spatially resolved high-frequency hyperspectral products as a reliable tool for climate studies and satellite validation. C1 [Shinozuka, Y.] NASA ARC CREST, Moffett Field, CA USA. [Shinozuka, Y.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Johnson, R. R.; Russell, P. B.; Redemann, J.; Dunagan, S. E.; Segal-Rosenheimer, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Flynn, C. J.; Schmid, B.; Kluzek, C. D.; Hubbe, J. M.; Chand, D.; Berg, L. K.] Pacific NW Natl Lab, Richland, WA 99352 USA. [Livingston, J. M.] SRI Int, Menlo Pk, CA 94025 USA. [Eck, T. F.] Univ Space Res Assoc, Columbia, MD USA. [Eck, T. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wagener, R.; Gregory, L.] Brookhaven Natl Lab, Upton, NY 11973 USA. [Rogers, R. R.; Ferrare, R. A.; Hair, J. W.; Hostetler, C. A.; Burton, S. P.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Shinozuka, Y (reprint author), Bay Area Environm Res Inst, 596 1st St W, Sonoma, CA 95476 USA. EM Yohei.Shinozuka@nasa.gov RI Wagener, Richard/B-5445-2008; Berg, Larry/A-7468-2016 OI Wagener, Richard/0000-0003-3892-1182; Berg, Larry/0000-0002-3362-9492 FU NASA Radiation Science Program; Ames Instrument Working Group; NOAA Office of Global Programs; DOE ARM program FX We would like to thank the DOE ARM aerial facility staff Mike Hubbell, Bill Svancara, Dick Hone, Jason Tomlinson, and Gene Dukes for carrying out the G-1 research flights; the NASA Langley King Air flight crew Mike Wusk, Dale Bowser, Dean Riddick, Scott Sims, Rick Yasky, Greg Slover, and Leslie Kagey for their outstanding work supporting the B-200 flights and measurements; Meloe Kacenelenbogen for her contribution during the calibration of AATS-14; and Qin Zhang for assistance with preparing the figures. The 4STAR hardware and science algorithm development were funded by the NASA Radiation Science Program, the Ames Instrument Working Group, and the NOAA Office of Global Programs. Further maturation of 4STAR as well as the participation of 4STAR in TCAP and subsequent analyses was funded by the DOE ARM program. Analysis and interpretation of data collected on board the G-1 were supported by the DOE ARM and DOE Atmospheric System Research (ASR) Programs. NR 56 TC 9 Z9 9 U1 2 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 16 PY 2013 VL 118 IS 21 BP 12180 EP 12194 DI 10.1002/2013JD020596 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 302NS UT WOS:000330611800020 ER PT J AU Tegtmeier, S Hegglin, MI Anderson, J Bourassa, A Brohede, S Degenstein, D Froidevaux, L Fuller, R Funke, B Gille, J Jones, A Kasai, Y Kruger, K Kyrola, E Lingenfelser, G Lumpe, J Nardi, B Neu, J Pendlebury, D Remsberg, E Rozanov, A Smith, L Toohey, M Urban, J von Clarmann, T Walker, KA Wang, RHJ AF Tegtmeier, S. Hegglin, M. I. Anderson, J. Bourassa, A. Brohede, S. Degenstein, D. Froidevaux, L. Fuller, R. Funke, B. Gille, J. Jones, A. Kasai, Y. Krueger, K. Kyrola, E. Lingenfelser, G. Lumpe, J. Nardi, B. Neu, J. Pendlebury, D. Remsberg, E. Rozanov, A. Smith, L. Toohey, M. Urban, J. von Clarmann, T. Walker, K. A. Wang, R. H. J. TI SPARC Data Initiative: A comparison of ozone climatologies from international satellite limb sounders SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID QUASI-BIENNIAL OSCILLATION; TECHNICAL NOTE; STRATOSPHERIC AEROSOL; RETRIEVAL ALGORITHM; ANTARCTIC OZONE; ERROR ANALYSIS; WATER-VAPOR; DATA SET; VALIDATION; O-3 AB A comprehensive quality assessment of the ozone products from 18 limb-viewing satellite instruments is provided by means of a detailed intercomparison. The ozone climatologies in form of monthly zonal mean time series covering the upper troposphere to lower mesosphere are obtained from LIMS, SAGE I/II/III, UARS-MLS, HALOE, POAM II/III, SMR, OSIRIS, MIPAS, GOMOS, SCIAMACHY, ACE-FTS, ACE-MAESTRO, Aura-MLS, HIRDLS, and SMILES within 1978-2010. The intercomparisons focus on mean biases of annual zonal mean fields, interannual variability, and seasonal cycles. Additionally, the physical consistency of the data is tested through diagnostics of the quasi-biennial oscillation and Antarctic ozone hole. The comprehensive evaluations reveal that the uncertainty in our knowledge of the atmospheric ozone mean state is smallest in the tropical and midlatitude middle stratosphere with a 1 sigma multi-instrument spread of less than +/-5%. While the overall agreement among the climatological data sets is very good for large parts of the stratosphere, individual discrepancies have been identified, including unrealistic month-to-month fluctuations, large biases in particular atmospheric regions, or inconsistencies in the seasonal cycle. Notable differences between the data sets exist in the tropical lower stratosphere (with a spread of +/-30%) and at high latitudes (+/-15%). In particular, large relative differences are identified in the Antarctic during the time of the ozone hole, with a spread between the monthly zonal mean fields of +/-50%. The evaluations provide guidance on what data sets are the most reliable for applications such as studies of ozone variability, model-measurement comparisons, detection of long-term trends, and data-merging activities. C1 [Tegtmeier, S.; Krueger, K.; Toohey, M.] GEOMAR Helmholtz Ctr Ocean Res Kiel, D-24105 Kiel, Germany. [Hegglin, M. I.] Univ Reading, Reading, Berks, England. [Anderson, J.] Hampton Univ, Hampton, VA 23668 USA. [Bourassa, A.; Degenstein, D.] Univ Saskatchewan, Saskatoon, SK, Canada. [Brohede, S.; Urban, J.] Chalmers, S-41296 Gothenburg, Sweden. [Froidevaux, L.; Fuller, R.; Neu, J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Funke, B.] Inst Astrofis Andalucia, E-18080 Granada, Spain. [Gille, J.] Univ Colorado, Boulder, CO 80309 USA. [Jones, A.; Pendlebury, D.; Walker, K. A.] Univ Toronto, Toronto, ON, Canada. [Kasai, Y.] NICT, Koganei, Tokyo, Japan. [Kyrola, E.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. [Lingenfelser, G.; Remsberg, E.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Lumpe, J.] Computat Phys Inc, Boulder, CO USA. [Nardi, B.; Smith, L.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Rozanov, A.] Univ Bremen, Inst Environm Phys IUP, D-28359 Bremen, Germany. [von Clarmann, T.] Karlsruhe Inst Technol, D-76021 Karlsruhe, Germany. [Wang, R. H. J.] Georgia Inst Technol, Atlanta, GA 30332 USA. RP Tegtmeier, S (reprint author), GEOMAR Helmholtz Ctr Ocean Res Kiel, Dusternbrooker Weg 20, D-24105 Kiel, Germany. EM stegtmeier@geomar.de RI Urban, Jo/F-9172-2010; Kyrola, Erkki/E-1835-2014; Funke, Bernd/C-2162-2008; Toohey, Matthew/G-3129-2010; Hegglin, Michaela/D-7528-2017 OI Urban, Jo/0000-0001-7026-793X; Funke, Bernd/0000-0003-0462-4702; Toohey, Matthew/0000-0002-7070-405X; Hegglin, Michaela/0000-0003-2820-9044 FU WGL project TransBrom; European Union [226224-SHIVA]; National Aeronautics and Space Administration; CSA; Canadian Foundation for Climate and Atmospheric Sciences; Swedish National Space Board (SNSB); National Technology Agency of Finland (Tekes); Centre National d'Etudes Spatiales (CNES) in France; ESA; Academy of Finland [MIDAT (134325)]; German Aerospace Agency (DLR) within the project SADOS [50EE1105]; State and University of Bremen; National Oceanic and Atmospheric Administration's Educational Partnership Program Cooperative Remote Sensing Science and Technology Center (NOAA EPP CREST) FX These climatological comparisons have resulted from the work of the SPARC Data Initiative team which has been ongoing since 2009. The authors thank the relevant instrument teams, the various space agencies (CSA, ESA, NASA, JAXA and other national space agencies), and organizations such as CEOS-ACC and IGACO. We particularly thank the ISSI in Bern for facilitating two successful team meetings in Bern as part of the ISSI International Team activity program and SPARC and WCRP for travel support. The work from S. T. was funded from the WGL project TransBrom and the European Union's Seventh Framework Programme FP7/2007-2013 under grant agreement no 226224-SHIVA. M. I. H. thanks the CSA and ESA for supporting her work for the SPARC Data Initiative. Work at the Jet Propulsion Laboratory, California Institute of Technology, was performed under contract with the National Aeronautics and Space Administration. The ACE is a Canadian-led mission mainly supported by the CSA. Development of the ACE climatologies was supported by grants from the Canadian Foundation for Climate and Atmospheric Sciences and the CSA. Odin is a Swedish-led satellite project funded jointly by the Swedish National Space Board (SNSB), the CSA, the National Technology Agency of Finland (Tekes), the Centre National d'Etudes Spatiales (CNES) in France, and the third party mission programme of ESA. The work of E. K. was supported by the Academy of Finland through the project MIDAT (134325). The work of the University Bremen team was funded in part by the German Aerospace Agency (DLR) within the project SADOS (50EE1105) and by the State and University of Bremen. The work from Hampton University was partially funded under the National Oceanic and Atmospheric Administration's Educational Partnership Program Cooperative Remote Sensing Science and Technology Center (NOAA EPP CREST). We thank ECMWF for service and support and the German Weather Service (DWD) for providing access to the ECMWF data base. NR 53 TC 30 Z9 30 U1 2 U2 24 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 NOV 16 PY 2013 VL 118 IS 21 BP 12229 EP 12247 DI 10.1002/2013JD019877 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 302NS UT WOS:000330611800025 ER PT J AU Strode, SA Pawson, S AF Strode, Sarah A. Pawson, Steven TI Detection of carbon monoxide trends in the presence of interannual variability SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID BIOMASS BURNING EMISSIONS; AIR-POLLUTION TRANSPORT; NORTH-AMERICA; EARTHS ATMOSPHERE; MAUNA-LOA; CO; CHEMISTRY; MOPITT; TROPOSPHERE; MISSION AB Trends in fossil fuel emissions are a major driver of changes in atmospheric CO, but detection of trends in CO from anthropogenic sources is complicated by the presence of large interannual variability (IAV) in biomass burning. We use a multiyear model simulation of CO with year-specific biomass burning to predict the number of years needed to detect the impact of changes in Asian anthropogenic emissions on downwind regions. Our study includes two cases for changing anthropogenic emissions: a stepwise change of 15% and a linear trend of 3% yr(-1). We first examine how well the model reproduces the observed IAV of CO over the North Pacific, since this variability impacts the time needed to detect significant anthropogenic trends. The modeled IAV over the North Pacific correlates well with that seen from the Measurements of Pollution in the Troposphere (MOPITT) instrument but underestimates the magnitude of the variability. The model predicts that a 3% yr(-1) trend in Asian anthropogenic emissions would lead to a statistically significant trend in CO surface concentration in the western United States within 12 years, and accounting for Siberian boreal biomass-burning emissions greatly reduces the number of years needed for trend detection. Combining the modeled trend with the observed MOPITT variability at 500 hPa, we estimate that the 3% yr(-1) trend could be detectable in satellite observations over Asia in approximately a decade. Our predicted timescales for trend detection highlight the importance of long-term measurements of CO from satellites. C1 [Strode, Sarah A.] Univ Space Res Assoc, Columbia, MD USA. [Strode, Sarah A.; Pawson, Steven] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Strode, SA (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Code 614, Greenbelt, MD 20771 USA. EM Sarah.a.strode@nasa.gov RI Strode, Sarah/H-2248-2012; Pawson, Steven/I-1865-2014 OI Strode, Sarah/0000-0002-8103-1663; Pawson, Steven/0000-0003-0200-717X FU NASA FX This research was supported by NASA, including substantial computing resources provided by the High-Performance Computing Program. We thank Eric Nielsen and Lesley Ott for assistance with the model. We thank Paul Novelli for useful discussions on the GMD data and Merritt Deeter for helpful discussions of the MOPITT data. NR 77 TC 3 Z9 4 U1 0 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 NOV 16 PY 2013 VL 118 IS 21 BP 12257 EP 12273 DI 10.1002/2013JD020258 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 302NS UT WOS:000330611800027 ER PT J AU Atreya, SK Trainer, MG Franz, HB Wong, MH Manning, HLK Malespin, CA Mahaffy, PR Conrad, PG Brunner, AE Leshin, LA Jones, JH Webster, CR Owen, TC Pepin, RO Navarro-Gonzalez, R AF Atreya, Sushil K. Trainer, Melissa G. Franz, Heather B. Wong, Michael H. Manning, Heidi L. K. Malespin, Charles A. Mahaffy, Paul R. Conrad, Pamela G. Brunner, Anna E. Leshin, Laurie A. Jones, John H. Webster, Christopher R. Owen, Tobias C. Pepin, Robert O. Navarro-Gonzalez, R. TI Primordial argon isotope fractionation in the atmosphere of Mars measured by the SAM instrument on Curiosity and implications for atmospheric loss SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE planetary atmospheres; argon isotopes; solar system; Mars; habitability; atmospheric loss ID MARTIAN ATMOSPHERE; GAS COMPONENTS; NOBLE-GASES; SOLAR-WIND; EVOLUTION; VOLATILES; RATIOS; SHERGOTTITES; ABUNDANCE; SURFACE AB The quadrupole mass spectrometer of the Sample Analysis at Mars (SAM) instrument on Curiosity rover has made the first high-precision measurement of the nonradiogenic argon isotope ratio in the atmosphere of Mars. The resulting value of Ar-36/Ar-38=4.20.1 is highly significant for it provides excellent evidence that Mars meteorites are indeed of Martian origin, and it points to a significant loss of argon of at least 50% and perhaps as high as 85-95% from the atmosphere of Mars in the past 4 billion years. Taken together with the isotopic fractionations in N, C, H, and O measured by SAM, these results imply a substantial loss of atmosphere from Mars in the posthydrodynamic escape phase. C1 [Atreya, Sushil K.; Wong, Michael H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Trainer, Melissa G.; Franz, Heather B.; Malespin, Charles A.; Mahaffy, Paul R.; Conrad, Pamela G.; Brunner, Anna E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Manning, Heidi L. K.] Concordia Coll, Moorhead, MN USA. [Leshin, Laurie A.] Rensselaer Polytech Inst, Sch Sci, Troy, NY USA. [Jones, John H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Webster, Christopher R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Owen, Tobias C.] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Pepin, Robert O.] Univ Minnesota, Minneapolis, MN USA. [Navarro-Gonzalez, R.] Univ Nacl Autonoma Mexico, Mexico City 04510, DF, Mexico. RP Atreya, SK (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. EM atreya@umich.edu RI Gonzalez, Rafael/D-1748-2009; Trainer, Melissa/E-1477-2012 FU NASA Mars Science Laboratory Project FX We thank John Grotzinger, Alexander Pavlov, Richard Becker, Andrew Steele, Paul Niles, and Susanne Schwenzer for comments on the manuscript and the MSL Team for successful operation of the mission. This research was supported by the NASA Mars Science Laboratory Project. NR 27 TC 17 Z9 17 U1 2 U2 21 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD NOV 16 PY 2013 VL 40 IS 21 BP 5605 EP 5609 DI 10.1002/2013GL057763 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 263LT UT WOS:000327810800008 ER PT J AU Potter, RWK Kring, DA Collins, GS AF Potter, Ross W. K. Kring, David A. Collins, Gareth S. TI Quantifying the attenuation of structural uplift beneath large lunar craters SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE structural uplift; impact basins; complex craters; numerical modeling; moon ID CHICXULUB IMPACT CRATER; HYDROCODE SIMULATIONS; DEFORMATION; VOLCANISM; PRESSURE; FRACTURE; COLLAPSE; TARGET; BASIN; MOON AB Terrestrial crater observations and laboratory experiments demonstrate that target material beneath complex impact craters is uplifted relative to its preimpact position. Current estimates suggest maximum uplift is one tenth of the final crater diameter for terrestrial complex craters and one tenth to one fifth for lunar central peak craters. These latter values are derived from an analytical model constrained by observations from small craters and may not be applicable to larger complex craters and basins. Here, using numerical modeling, we produce a set of relatively simple analytical equations that estimate the maximum amount of structural uplift and quantify the attenuation of uplift with depth beneath large lunar craters. C1 [Potter, Ross W. K.; Kring, David A.] Lunar & Planetary Inst, Ctr Lunar Sci & Explorat, Houston, TX 77058 USA. [Potter, Ross W. K.; Kring, David A.] NASA, Lunar Sci Inst, Washington, DC 20546 USA. [Collins, Gareth S.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London, England. RP Potter, RWK (reprint author), Lunar & Planetary Inst, Ctr Lunar Sci & Explorat, 3303 NASA Rd 1, Houston, TX 77058 USA. EM potter@lpi.usra.edu OI Collins, Gareth/0000-0002-6087-6149 FU NASA Lunar Science Institute [NNA09DB33A]; UK Science & Technology Facilities Council [ST/J001260/1] FX We thank Boris Ivanov, Jay Melosh, Kai Wunnemann and Dirk Elbeshausen for their work developing iSALE. We also thank Jay Melosh and an anonymous reviewer for their comments. This work was partially supported by NASA Lunar Science Institute contract NNA09DB33A (PI David A. Kring). GSC was supported by UK Science & Technology Facilities Council grant ST/J001260/1. This is LPI contribution number 1760. NR 38 TC 4 Z9 4 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 NOV 16 PY 2013 VL 40 IS 21 BP 5615 EP 5620 DI 10.1002/2013GL057829 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 263LT UT WOS:000327810800010 ER PT J AU Hofton, MA Luthcke, SB Blair, JB AF Hofton, M. A. Luthcke, S. B. Blair, J. B. TI Estimation of ICESat intercampaign elevation biases from comparison of lidar data in East Antarctica SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE ICESat; elevation biases; mass balance ID SHEET MASS-BALANCE AB The Ice, Cloud, and land Elevation Satellite (ICESat) laser campaign elevation biases are estimated from an analysis of ICESat and airborne Land, Vegetation, and Ice Sensor lidar intrasensor and intersensor elevation differences from two regions of the Antarctic ice sheet that experienced minimal surface elevation change. Elevation observations are corrected for a combination of accumulation, melting, and firn densification processes and glacial isostatic adjustment. ICESat elevations are adjusted for the saturation and Gaussian-Centroid corrections. Relative to laser campaign L3I, biases are found to be less than approximate to 8cm, except for campaign L2E at 14.72cm corresponding to the time of a significant accumulation anomaly in East Antarctica. The intercampaign bias trend estimated from intersensor elevation differences computed over campaigns L2A to L2F (September 2003 to October 2009) excluding L2E is 1.040.48cm/yr. The intercampaign bias trend represents a correction to ICESat derived Antarctica mass balance of 11753Gt/yr. C1 [Hofton, M. A.] Univ Maryland, Dept Geog Sci, College Pk, MD 20741 USA. [Luthcke, S. B.; Blair, J. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hofton, MA (reprint author), Univ Maryland, Dept Geog Sci, Lefrak Hall, College Pk, MD 20741 USA. EM mhofton@umd.edu RI Blair, James/D-3881-2013 FU [NNX11AH69G] FX The authors would like to thank S. Ligtenberg, E. Ivins, M. Beckley, C. Shuman, an anonymous reviewer, and J. Stroeve for their input and reviews. M.H. was supported by grant NNX11AH69G. NR 13 TC 18 Z9 19 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 NOV 16 PY 2013 VL 40 IS 21 BP 5698 EP 5703 DI 10.1002/2013GL057652 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 263LT UT WOS:000327810800025 ER PT J AU Russell, GL Lacis, AA Rind, DH Colose, C Opstbaum, RF AF Russell, Gary L. Lacis, Andrew A. Rind, David H. Colose, Christopher Opstbaum, Roger F. TI Fast atmosphere-ocean model runs with large changes in CO2 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE climate sensitivity; CO2 AB How does climate sensitivity vary with the magnitude of climate forcing? This question was investigated with the use of a modified coupled atmosphere-ocean model, whose stability was improved so that the model would accommodate large radiative forcings yet be fast enough to reach rapid equilibrium. Experiments were performed in which atmospheric CO2 was multiplied by powers of 2, from 1/64 to 256 times the 1950 value. From 8 to 32 times, the 1950 CO2, climate sensitivity for doubling CO2 reaches 8 degrees C due to increases in water vapor absorption and cloud top height and to reductions in low level cloud cover. As CO2 amount increases further, sensitivity drops as cloud cover and planetary albedo stabilize. No water vapor-induced runaway greenhouse caused by increased CO2 was found for the range of CO2 examined. With CO2 at or below 1/8 of the 1950 value, runaway sea ice does occur as the planet cascades to a snowball Earth climate with fully ice covered oceans and global mean surface temperatures near -30 degrees C. C1 [Russell, Gary L.; Lacis, Andrew A.; Rind, David H.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Colose, Christopher] SUNY Albany, Albany, NY 12222 USA. [Opstbaum, Roger F.] Bergen Community Coll, Paramus, NJ USA. RP Russell, GL (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM Gary.L.Russell@nasa.gov FU NASA Earth Science Research Division; NASA; Goddard Space Flight Center's Science Innovation Fund (SIF) Program FX We thank James Hansen for helpful suggestions in regard to the FAOM modeling approach and analysis and Makiko Sato for assistance with graphics display. The NASA Center for Climate Simulations provided computer resources for this paper's calculations. We also express our thanks to NASA Earth Science Research Division, managed by J. Kaye and D. Considine, for support, and we thank the NASA Modeling Analysis and Prediction (MAP) Program for support. We also thank J. Garvin for support for G. Russell and A. Lacis as part of Goddard Space Flight Center's Science Innovation Fund (SIF) Program. NR 13 TC 9 Z9 9 U1 0 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 NOV 16 PY 2013 VL 40 IS 21 BP 5787 EP 5792 DI 10.1002/2013GL056755 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 263LT UT WOS:000327810800040 ER PT J AU Waquet, F Peers, F Ducos, F Goloub, P Platnick, S Riedi, J Tanre, D Thieuleux, F AF Waquet, F. Peers, F. Ducos, F. Goloub, P. Platnick, S. Riedi, J. Tanre, D. Thieuleux, F. TI Global analysis of aerosol properties above clouds SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE aerosol; climate; cloud; satellite; global; aerosol; climate; cloud; satellite; global ID POLARIZATION MEASUREMENTS; ABSORBING AEROSOLS; OPTICAL DEPTH; SAFARI 2000; RETRIEVAL; SATELLITE; POLDER; MODIS; ATMOSPHERE; CLIMATE AB The seasonal and spatial variability of Aerosol Above Cloud (AAC) properties are derived from passive satellite data for the year 2008. A significant amount of aerosols are transported above liquid water clouds on the global scale. For particles in the fine mode (i.e., radius smaller than 0.3 mu m), including both clear-sky and AAC, retrievals increase the global mean aerosol optical thickness by 25(6)%. The two main regions of originated anthropogenic AAC are the tropical Southeast Atlantic, for biomass-burning aerosols, and the North Pacific, mainly for pollutants. Man-made AAC are also detected over the Arctic during the spring. Mineral dust particles are detected above clouds within the so-called dust belt region (5-40 degrees N). AAC may cause a warming effect and bias the retrieval of the cloud properties. This study will then help to better quantify the impacts of aerosols on clouds and climate. C1 [Waquet, F.; Peers, F.; Ducos, F.; Goloub, P.; Riedi, J.; Tanre, D.; Thieuleux, F.] Univ Lille 1, Opt Atmospher Lab, CNRS INSU UMR8518, F-59655 Villeneuve Dascq, France. [Platnick, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Waquet, F (reprint author), Univ Lille 1, Opt Atmospher Lab, CNRS INSU UMR8518, F-59655 Villeneuve Dascq, France. EM fabien.waquet@univ-lille1.fr RI Platnick, Steven/J-9982-2014 OI Platnick, Steven/0000-0003-3964-3567 FU Programme National de Teledetection Spatiale (PNTS) [PNTS-2013-10] FX This work has been supported by the Programme National de Teledetection Spatiale (PNTS, http://www.insu.cnrs.fr/actions-sur-projets/pnts-programme-national-de-t eledetection-spatiale), grant no PNTS-2013-10. The authors are grateful to CNES, NASA, and the ICARE data and services center. NR 40 TC 9 Z9 9 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 NOV 16 PY 2013 VL 40 IS 21 BP 5809 EP 5814 DI 10.1002/2013GL057482 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 263LT UT WOS:000327810800044 ER PT J AU Rousselet, E Levin, M Gebhard, E Higgins, BM DeGuise, S Godard-Codding, CAJ AF Rousselet, Estelle Levin, Milton Gebhard, Erika Higgins, Benjamin M. DeGuise, Sylvain Godard-Codding, Celine A. J. TI Evaluation of immune functions in captive immature loggerhead sea turtles (Caretta caretta) SO VETERINARY IMMUNOLOGY AND IMMUNOPATHOLOGY LA English DT Article DE Caretta caretta; Lymphocyte proliferation; Mitogen; Natural killer; Phagocytosis; Respiratory burst; Sea turtle ID WHALES DELPHINAPTERUS-LEUCAS; KILLER-CELL-ACTIVITY; IN-VITRO EXPOSURE; HYPAQUE DISCONTINUOUS GRADIENTS; PERIPHERAL-BLOOD; CHELONIA-MYDAS; GREEN TURTLES; LYMPHOCYTE-PROLIFERATION; AVIAN HETEROPHILS; HEALTH PARAMETERS AB Sea turtles face numerous environmental challenges, such as exposure to chemical pollution and biotoxins, which may contribute to immune system impairment, resulting in increased disease susceptibility. Therefore, a more thorough assessment of the host's immune response and its susceptibility is needed for these threatened and endangered animals. In this study, the innate and acquired immune functions of sixty-five clinically healthy, immature, captive loggerhead sea turtles (Caretta caretta) were assayed using non-lethal blood sample collection. Functional immune assays were developed and/or optimized for this species, including mitogen-induced lymphocyte proliferation, natural killer (NK) cell activity, phagocytosis, and respiratory burst. Peripheral blood mononuclear cells (PBMC) and phagocytes were isolated by density gradient centrifugation on Ficoll-Paque and discontinuous Percoll gradients, respectively. The T lymphocyte mitogens ConA significantly induced lymphocyte proliferation at 1 and 2 mu g/mL while PHA significantly induced lymphocyte proliferation at 5 and 10 mu g/mL. The B lymphocyte mitogen LPS significantly induced proliferation at 1 mu g/mL. Monocytes demonstrated higher phagocytic activity than eosinophils. In addition, monocytes exhibited respiratory burst. Natural killer cell activity was higher against YAC-1 than K-562 target cells. These optimized assays may help to evaluate the integrity of loggerhead sea turtle's immune system upon exposure to environmental contaminants, as well as part of a comprehensive health assessment and monitoring program. (C) 2013 Elsevier B.V. All rights reserved. C1 [Rousselet, Estelle; Godard-Codding, Celine A. J.] Texas Tech Univ, Inst Environm & Human Hlth, Dept Environm Toxicol, Lubbock, TX 79416 USA. [Levin, Milton; Gebhard, Erika; DeGuise, Sylvain] Univ Connecticut, Dept Pathobiol & Vet Sci, Storrs, CT 06269 USA. [Higgins, Benjamin M.] NOAA, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Galveston, TX 77551 USA. RP Rousselet, E (reprint author), VetAgroSup Campus Vet Lyon, 1 Ave Bourgelat, F-69280 Marcy Letoile, France. EM estelle.rousselet@vetagro-sup.fr FU Rotary Foundation; Texas Tech University FX The staff at the NOAA Fisheries Service Galveston Sea Turtle Facility is gratefully acknowledged. The authors specially acknowledge Dr. Carol Norris (Flow Cytometry/Confocal Microscopy Facility of the Biotechnology/Bioservices Center, University of Connecticut) for her technical support. This project was performed under Florida Fish and Wildlife Conservation Commission MTP# 10-015-A, and U.S. Fish and Wildlife Service TE676379-4. Funding and logistic support for this project was provided by the Rotary Foundation and Texas Tech University. NR 65 TC 4 Z9 4 U1 1 U2 23 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-2427 EI 1873-2534 J9 VET IMMUNOL IMMUNOP JI Vet. Immunol. Immunopathol. PD NOV 15 PY 2013 VL 156 IS 1-2 BP 43 EP 53 DI 10.1016/j.vetimm.2013.09.004 PG 11 WC Immunology; Veterinary Sciences SC Immunology; Veterinary Sciences GA 260CL UT WOS:000327572500004 PM 24094689 ER PT J AU Klenzing, J Simoes, F Ivanov, S Bilitza, D Heelis, RA Rowland, D AF Klenzing, J. Simoes, F. Ivanov, S. Bilitza, D. Heelis, R. A. Rowland, D. TI Performance of the IRI-2007 model for equatorial topside ion density in the African sector for low and extremely low solar activity SO ADVANCES IN SPACE RESEARCH LA English DT Article DE African equatorial ionosphere; CINDI; C/NOFS; IRI-2007; Solar minimum; Aeronomy ID INTERNATIONAL REFERENCE IONOSPHERE; ELECTRON-DENSITY; INDEX; FOF2; IRI AB The recent availability of new data sets during the recent extreme solar minimum provides an opportunity for testing the performance of the International Reference Ionosphere in historically undersampled regions. This study presents averages and variability of topside ionospheric densities over Africa as a function of season, local time, altitude, and magnetic dip latitude as measured by the Communication/Navigation Outage Forecast System (C/NOFS) satellite. The results are compared to the three topside model options available in IRI-2007. Overall, the NeQuick model is found to have the best performance, though during the deepest part of the solar minimum all three options significantly overestimate density. Published by Elsevier Ltd. on behalf of COSPAR. C1 [Klenzing, J.; Simoes, F.; Rowland, D.] NASA GSFC, Space Weather Lab Code 674, Greenbelt, MD 20771 USA. [Ivanov, S.] Georgia Inst Technol, Dept Phys, Atlanta, GA 30332 USA. [Bilitza, D.] NASA GSFC, Heliophys Lab Code 672, Greenbelt, MD 20771 USA. [Bilitza, D.] George Mason Univ, Dept Phys, Fairfax, VA 22030 USA. [Heelis, R. A.] Univ Texas Dallas, Ctr Space Sci, Richardson, TX 75083 USA. RP Klenzing, J (reprint author), NASA GSFC, Space Weather Lab Code 674, Greenbelt, MD 20771 USA. EM jeffrey.klenzing@nasa.gov; fernando.a.simoes@nasa.gov; ctoyan2400@gmail.com; dieter.bilitza-1@nasa.gov; heelis@utdallas.edu; douglas.e.rowland@nasa.gov RI Klenzing, Jeff/E-2406-2011; Rowland, Douglas/F-5589-2012 OI Klenzing, Jeff/0000-0001-8321-6074; Rowland, Douglas/0000-0003-0948-6257 FU NASA [NNX09AJ74G S04, NAS5-01068, NNX10AM94G] FX The work performed by JK and FS was supported by appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. The work performed by SI at Goddard Space Flight Center was made possible by the NASA Education Office through the Undergraduate Student Research Program managed by the Universities Space Research Association. DB is supported through NASA Grant NNX09AJ74G S04. The work at the University of Texas at Dallas is supported by NASA Grant NAS5-01068 and NASA Grant NNX10AM94G. Ri12 and IG12 are provided by the UK World Data Center, and Kp is provided through CDA-Web/GSFC. CINDI data can be obtained through http://cindispace.utdallas.edu/. NR 27 TC 9 Z9 9 U1 0 U2 11 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 NOV 15 PY 2013 VL 52 IS 10 BP 1780 EP 1790 DI 10.1016/j.asr.2012.09.030 PG 11 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 252HO UT WOS:000326996000009 ER PT J AU Tompson, SR AF Tompson, Sara R. TI Cracking the Particle Code of the Universe: The Hunt for the Higgs Boson SO LIBRARY JOURNAL LA English DT Book Review C1 [Tompson, Sara R.] Jet Prop Lab Lib, Arch & Records Sect, Pasadena, CA USA. RP Tompson, SR (reprint author), Jet Prop Lab Lib, Arch & Records Sect, Pasadena, CA USA. NR 1 TC 0 Z9 0 U1 0 U2 3 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 NOV 15 PY 2013 VL 138 IS 19 BP 109 EP 110 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 253PT UT WOS:000327102500232 ER PT J AU Park, J Bogard, DD Nyquist, LE Garrison, DH Mikouchi, T AF Park, Jisun Bogard, Donald D. Nyquist, Laurence E. Garrison, Daniel H. Mikouchi, Takashi TI Ar-Ar ages and trapped Ar components in Martian shergottites RBT 04262 and LAR 06319 SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID IMPLANTED NOBLE-GASES; DECAY CONSTANTS; EXCESS AR-40; PARENT BODY; METEORITES; CHASSIGNY; OLIVINE; ORIGIN; BASALTS; XENON AB We made Ar-39-Ar-40 (Ar-Ar) analyses of whole rock (WR) and mineral samples of two Martian shergottites, RBT 04262 (RBT) and LAR 06319 (LAR), in order to determine their Ar-Ar ages and the Ar-40/Ar-36 ratios of the trapped Martian Ar they contain. All samples released trapped (excess) Ar-40 and Ar-36 and suggested Ar-Ar ages older than their formation ages. Because trapped Ar components having different Ar-40/Ar-36 were released at different extraction temperatures, we utilized only a portion of the data to derive preferred Ar-Ar ages. We obtain Ar-Ar ages of 171 +/- 8 Ma for RBT plagioclase and 163 +/- 13 Ma for LAR whole rock. We identify two trapped Ar components. At low temperatures, particularly for plagioclase, Trapped-A with Ar-40/Ar-36 285 +/- 3 was released, and we believe this is most likely absorbed terrestrial air. At high extraction temperatures, particularly for pyroxene, Trapped-B with Ar-40/Ar-36 1813 +/- 127 was released. The poikilitic/non-poikilitic texture of RBT and the presence of large pyroxene oikocrysts allowed a clear definition of Trapped-B. This Ar component is Martian, and its isotopic similarity to the Martian atmospheric composition suggests that it may represent Martian atmospheric Ar incorporated into the shergottite melt via crustal rocks. Trapped-B partitioned into pyroxene at a constant molar ratio of K/Ar-36(Tr) = 33.2 +/- 9.5 x 10(6) for RBT 04262, and 80 +/- 21 x 10(6) for LAR 06319. Trapped-A mixed in different proportions with Trapped-B could give apparently intermediate trapped Ar-40/Ar-36 compositions commonly observed in shergottites. (c) 2013 Elsevier Ltd. All rights reserved. C1 [Park, Jisun; Bogard, Donald D.; Nyquist, Laurence E.; Garrison, Daniel H.] ARES, NASA Johnson Space Ctr, Houston, TX 77058 USA. [Park, Jisun; Bogard, Donald D.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Park, Jisun] Rutgers State Univ, Dept Chem & Chem Biol, Piscataway, NJ 08854 USA. [Garrison, Daniel H.] ESCG Barrios, Houston, TX 77058 USA. [Mikouchi, Takashi] Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan. RP Park, J (reprint author), Rutgers State Univ, Dept Chem & Chem Biol, Piscataway, NJ 08854 USA. EM park@lpi.usra.edu; bogard@lpi.usra.edu; laurence.e.nyquist@nasa.gov; dan.h.garrison@nasa.gov; mikouchi@eps.s.u-tokyo.ac.jp FU NASA Cosmochemistry Program; NASA Mars Fundamental Research Program; NASA; Lunar & Planetary Institute; Japanese Ministry of Education, Culture, Sports, Science and Technology [20740305]; NIPR Research Project Funds, P-9 (Evolution of the early Solar System materials) FX We thank K. Nagao (University of Tokyo) for the unirradiated RBT and LAR noble gas data, and G. F. Herzog (Rutgers University) for the CRE age discussion. We also thank C.-Y. Shih (NASA JSC/ESCG) for the RBT and LAR sample mineral separation. Discussions with M. N. Rao (NASA JSC/ESCG) have provided insights into the possible mechanisms by which terrestrial air might be trapped into shergottite plagioclase. Financial support has been supplied by the NASA Cosmochemistry and Mars Fundamental Research Programs (J.P. and L.E.N). D.D.B. was supported by NASA and the Lunar & Planetary Institute. T.M. was supported in part by a Grant-in-Aid for Young Scientists (B) by the Japanese Ministry of Education, Culture, Sports, Science and Technology No. 20740305 and by NIPR Research Project Funds, P-9 (Evolution of the early Solar System materials). The SEM work was performed in the Electron Microbeam Analysis Facility for Mineralogy at the Department of Earth and Planetary Science, University of Tokyo. We thank Susanne Schwenzer, Rainer Wieler, and an anonymous reviewer for constructive reviews, as well as Associate Editor J.N. Goswami and Executive Editor Marc Norman for editorial handling of the paper. NR 64 TC 3 Z9 3 U1 1 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD NOV 15 PY 2013 VL 121 BP 546 EP 570 DI 10.1016/j.gca.2013.06.045 PG 25 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 226ZR UT WOS:000325077100033 ER PT J AU Shibuya, T Yoshizaki, M Masaki, Y Suzuki, K Takai, K Russell, MJ AF Shibuya, Takazo Yoshizaki, Motoko Masaki, Yuka Suzuki, Katsuhiko Takai, Ken Russell, Michael J. TI Reactions between basalt and CO2-rich seawater at 250 and 350 degrees C, 500 bars: Implications for the CO2 sequestration into the modern oceanic crust and the composition of hydrothermal vent fluid in the CO2-rich early ocean SO CHEMICAL GEOLOGY LA English DT Article DE Experiment; CO2 sequestration; Archean hydrothermal alteration; Carbonatization; Alkaline hydrothermal fluid; Iron cycle ID MOLAL THERMODYNAMIC PROPERTIES; EAST PACIFIC RISE; MID-ATLANTIC RIDGE; DE-FUCA RIDGE; CARBON-DIOXIDE; WESTERN-AUSTRALIA; PILBARA CRATON; MIDOCEAN RIDGES; HIGH-PRESSURES; ELEVATED-TEMPERATURES AB This study aims to understand how basaltic rocks absorb CO2 in high-temperature alteration zones in the subseafloor, and to reconstruct hydrothermal alteration processes such as carbonatization of Archean greenstones. To this end, we conducted two laboratory experiments, simulating hydrothermal reactions between basalt (synthesized under quartz-fayalite-magnetite oxygen fugacity) and CO2-rich NaCl fluid (pH = 6.5 at 25 degrees C) at high temperature and pressure. As the water/rock reactions progressed at 250 degrees C and 350 degrees C, 500 bars, total carbonic acid concentration (Sigma CO2) reduced from its initial 400 mmol/kg to near 0 and 100 mmol/kg, respectively, meanwhile calcite was formed in the basalt as an alteration mineral. This indicates that calcite destabilizes as temperature increases in the H2O-CO2-basalt system and that crustal basalts can absorb almost all CO2 in the fluid as calcite, at least at temperatures and initial CO2 concentrations below 250 degrees C and 400 mmol/kg, respectively. Although the second aim was realized in the experiments, minerals such as sericite, dolomite, ankerite, and siderite present in Archean greenstones were not identified in the alteration products, possibly because K, Mg, and Fe were lacking in the initial solutions. Steady-state concentrations of SiO2, Mg, and K in the fluids during water/rock reactions were similar to those of high-temperature fluids (>250 degrees C) in modern basalt-hosted hydrothermal systems. However, the final experimental pH(in-situ) was 6.6 and 7.2 at 250 degrees C and 350 degrees C, respectively, higher than that in modern hydrothermal fluids (approximately 5) and higher than the neutral pH (5.5-5.6) at 250-350 degrees C, 500 bars. The results suggest that the presence of abundant CO2 in the initial fluid induced carbonatization of basalt; consequently, pH was buffered by precipitation and dissolution of calcite. Because pH(in-situ) was elevated, the dissolved Fe and Mn concentrations in the fluid were two to three orders of magnitude lower than those of modern hydrothermal fluids. In modern oceans, high-temperature hydrothermal vent fluids are the second-largest iron source (after riverine input). However, because alkaline, metal-poor hydrothermal fluids are generated in CO2-rich systems, CO2-rich seafloor hydrothermal systems may have behaved as iron sinks in early oceans. (C) 2013 Elsevier B. V. All rights reserved. C1 [Shibuya, Takazo; Yoshizaki, Motoko; Suzuki, Katsuhiko; Takai, Ken] Japan Agcy Marine Earth Sci & Technol JAMSTEC, Precambrian Ecosyst Lab, Yokosuka, Kanagawa 2370061, Japan. [Shibuya, Takazo; Takai, Ken] Japan Agcy Marine Earth Sci & Technol JAMSTEC, Submarine Hydrothermal Syst Res Grp, Yokosuka, Kanagawa 2370061, Japan. [Masaki, Yuka; Suzuki, Katsuhiko] Japan Agcy Marine Earth Sci & Technol JAMSTEC, Inst Res Earth Evolut IFREE, Yokosuka, Kanagawa 2370061, Japan. [Takai, Ken] Japan Agcy Marine Earth Sci & Technol JAMSTEC, Subsurface Geobiol Adv Res SUGAR Project, Yokosuka, Kanagawa 2370061, Japan. [Yoshizaki, Motoko] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan. [Shibuya, Takazo; Russell, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Shibuya, T (reprint author), Japan Agcy Marine Earth Sci & Technol JAMSTEC, Precambrian Ecosyst Lab, 2-15 Natsushima Cho, Yokosuka, Kanagawa 2370061, Japan. EM takazos@jamstec.go.jp FU Trans-crustal Advection and In-situ biogeochemical processes of Global sub-seafloor Aquifer (TAIGA) project; Japanese Ministry of Education, Culture, Sports, Science and Technology [22740333]; NASA's Astrobiology Institute (Icy Worlds) FX We thank Kenji Shimizu for the assistance of the preparation of synthetic basalt. We are also grateful to Kentaro Nakamura for discussion about the reactions between basalt and seawater under CO2-rich conditions. XRD analyses were helped by Tatsuo Nozaki. The authors appreciate the editorial handling by Jeremy Fein and the helpful comments of John Walther and an anonymous reviewer on the manuscript. This work was partially supported by the Trans-crustal Advection and In-situ biogeochemical processes of Global sub-seafloor Aquifer (TAIGA) project and the Grants-in-Aid for Scientific Research from the Japanese Ministry of Education, Culture, Sports, Science and Technology (No. 22740333). MJR's research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration: Exobiology and Evolutionary Biology and supported by NASA's Astrobiology Institute (Icy Worlds). NR 108 TC 10 Z9 10 U1 6 U2 52 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2541 EI 1878-5999 J9 CHEM GEOL JI Chem. Geol. PD NOV 14 PY 2013 VL 359 BP 1 EP 9 DI 10.1016/j.chemgeo.2013.08.044 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 254QA UT WOS:000327179000001 ER PT J AU Brown, PG Assink, JD Astiz, L Blaauw, R Boslough, MB Borovicka, J Brachet, N Brown, D Campbell-Brown, M Ceranna, L Cooke, W de Groot-Hedlin, C Drob, DP Edwards, W Evers, LG Garces, M Gill, J Hedlin, M Kingery, A Laske, G Le Pichon, A Mialle, P Moser, DE Saffer, A Silber, E Smets, P Spalding, RE Spurny, P Tagliaferri, E Uren, D Weryk, RJ Whitaker, R Krzeminski, Z AF Brown, P. G. Assink, J. D. Astiz, L. Blaauw, R. Boslough, M. B. Borovicka, J. Brachet, N. Brown, D. Campbell-Brown, M. Ceranna, L. Cooke, W. de Groot-Hedlin, C. Drob, D. P. Edwards, W. Evers, L. G. Garces, M. Gill, J. Hedlin, M. Kingery, A. Laske, G. Le Pichon, A. Mialle, P. Moser, D. E. Saffer, A. Silber, E. Smets, P. Spalding, R. E. Spurny, P. Tagliaferri, E. Uren, D. Weryk, R. J. Whitaker, R. Krzeminski, Z. TI A 500-kiloton airburst over Chelyabinsk and an enhanced hazard from small impactors SO NATURE LA English DT Article ID EARTH; ASTEROIDS; INFRASOUND; EXPLOSION; COMETS AB Most large (over a kilometre in diameter) near-Earth asteroids are now known, but recognition that airbursts (or fireballs resulting from nuclear-weapon-sized detonations of meteoroids in the atmosphere) have the potential to do greater damage(1) than previously thought has shifted an increasing portion of the residual impact risk (the risk of impact from an unknown object) to smaller objects(2). Above the threshold size of impactor at which the atmosphere absorbs sufficient energy to prevent a ground impact, most of the damage is thought to be caused by the airburst shock wave(3), but owing to lack of observations this is uncertain(4,5). Here we report an analysis of the damage from the airburst of an asteroid about 19 metres (17 to 20 metres) in diameter southeast of Chelyabinsk, Russia, on 15 February 2013, estimated to have an energy equivalent of approximately 500 (+/- 100) kilotons of trinitrotoluene (TNT, where 1 kiloton of TNT = 4.185x10(12) joules). We show that a widely referenced technique(4-6) of estimating airburst damage does not reproduce the observations, and that the mathematical relations(7) based on the effects of nuclear weapons-almost always used with this technique-overestimate blast damage. This suggests that earlier damage estimates(5,6) near the threshold impactor size are too high. We performed a global survey of airbursts of a kiloton or more (including Chelyabinsk), and find that the number of impactors with diameters of tens of metres may be an order of magnitude higher than estimates based on other techniques(8,9). This suggests a non-equilibrium(if the population were in a long-term collisional steady state the size-frequency distribution would either follow a single power law or there must be a size-dependent bias in other surveys) in the near-Earth asteroid population for objects 10 to 50 metres in diameter, and shifts more of the residual impact risk to these sizes. C1 [Brown, P. G.; Campbell-Brown, M.; Gill, J.; Silber, E.; Uren, D.; Weryk, R. J.; Krzeminski, Z.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Brown, P. G.] Univ Western Ontario, Ctr Planetary Sci & Explorat, London, ON N6A 5B7, Canada. [Assink, J. D.; Brachet, N.; Le Pichon, A.] Commissariat Energie Atom, Dept Anal Surveillance Environm CEA DAM DIF, F-91297 Bruyeres Le Chatel, Arpajon, France. [Astiz, L.; de Groot-Hedlin, C.; Hedlin, M.; Laske, G.] Univ Calif San Diego, Inst Geophys & Planetary Phys, Lab Atmospher Acoust, La Jolla, CA 92093 USA. [Blaauw, R.; Moser, D. E.] NASA, Marshall Informat Technol Serv MITS, Dynet Tech Serv, Marshall Space Flight Ctr, Huntsville, CA 35812 USA. [Boslough, M. B.; Spalding, R. E.] Sandia Natl Labs, Albuquerque, NM 87185 USA. [Borovicka, J.; Spurny, P.] Acad Sci Czech Republic, Astron Inst, CZ-25165 Ondrejov, Czech Republic. [Brown, D.; Mialle, P.] Comprehens Test Ban Treaty Org, Provis Tech Secretariat, Int Data Ctr, A-1400 Vienna, Austria. [Ceranna, L.] Bundesanstalt Geowissensch & Rohstoffe, D-30655 Hannover, Germany. [Cooke, W.; Saffer, A.] Marshall Space Flight Ctr, Meteoroid Environm Off, Space Environm Team, Huntsville, AL 35812 USA. [Drob, D. P.] Naval Res Lab, Space Sci Div, Washington, DC 20375 USA. [Edwards, W.] Nat Resources Canada, Canadian Hazard Informat Serv, Ottawa, ON K1A 0Y3, Canada. [Evers, L. G.; Smets, P.] Royal Netherlands Meteorol Inst, Seismol Div, NL-3732 GK De Bilt, Netherlands. [Evers, L. G.; Smets, P.] Delft Univ Technol, Fac Civil Engn & Geosci, Dept Geosci & Engn, NL-2628 CN Delft, Netherlands. [Garces, M.] Univ Hawaii, Infrasound Lab, Honolulu, HI 96740 USA. [Kingery, A.] NASA, ERC Inc Jacobs ESSSA Grp, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Tagliaferri, E.] ET Space Syst, Camarillo, CA 93012 USA. [Whitaker, R.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Brown, PG (reprint author), Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. EM pbrown@uwo.ca RI Evers, Laslo/E-5707-2011; Drob, Douglas/G-4061-2014; Borovicka, Jiri/F-4257-2014; Spurny, Pavel/G-9044-2014; OI Evers, Laslo/0000-0003-2825-6211; Drob, Douglas/0000-0002-2045-7740; Smets, Pieter/0000-0003-0394-0973 FU NASA [NNX11AB76A]; Office of Naval Research; [67985815] FX Funding was provided by the NASA co-operative agreement NNX11AB76A and the Czech institutional project RVO:67985815. D. P. D. acknowledges support from the Office of Naval Research. We appreciate discussions with F. Gilbert (of UCSD), J. Stevens (of SAIC), P. Earle and J. Bellini (of USGS). D. Dearborn provided assistance with video reductions. NR 26 TC 98 Z9 100 U1 2 U2 41 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 NOV 14 PY 2013 VL 503 IS 7475 BP 238 EP 241 DI 10.1038/nature12741 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 250YX UT WOS:000326894200046 PM 24196713 ER PT J AU Velazquez, JM Baskaran, S Gaikwad, AV Ngo-Duc, TT He, XT Oye, MM Meyyappan, M Rout, TK Fu, JY Banerjee, S AF Velazquez, Jesus M. Baskaran, Sivapalan Gaikwad, Anil V. Tam-Triet Ngo-Duc He, Xiangtong Oye, Michael M. Meyyappan, M. Rout, Tapan K. Fu, John Y. Banerjee, Sarbajit TI Effective Piezoelectric Response of Substrate-Integrated ZnO Nanowire Array Devices on Galvanized Steel SO ACS APPLIED MATERIALS & INTERFACES LA English DT Article DE electromechanical devices; functional coatings; galvanized steel; nanowire array; piezoelectric coefficient; zinc oxide ID GROWTH; NANOGENERATORS; DRIVEN AB Harvesting waste energy through electromechanical coupling in practical devices requires combining device design with the development of synthetic strategies for large-area controlled fabrication of active piezoelectric materials. Here, we show a facile route to the large-area fabrication of ZnO nanostructured arrays using commodity galvanized steel as the Zn precursor as well as the substrate. The ZnO nanowires are further integrated within a device construct and the effective piezoelectric response is deduced based on a novel experimental approach involving induction of stress in the nanowires through pressure wave propagation along with phase-selective lock-in detection of the induced current. The robust methodology for measurement of the effective piezoelectric coefficient developed here allows for interrogation of piezoelectric functionality for the entire substrate under bending-type deformation of the ZnO nanowires. C1 [Velazquez, Jesus M.; Banerjee, Sarbajit] SUNY Buffalo, Dept Chem, Buffalo, NY 14260 USA. [Baskaran, Sivapalan; He, Xiangtong; Fu, John Y.] SUNY Buffalo, Dept Mech & Aerosp Engn, Buffalo, NY 14260 USA. [Gaikwad, Anil V.; Rout, Tapan K.] Tata Steel Grp Europe, NL-1760 Ijmuiden, Netherlands. [Tam-Triet Ngo-Duc; Oye, Michael M.; Meyyappan, M.] NASA, Ctr Nanotechnol, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Banerjee, S (reprint author), SUNY Buffalo, Dept Chem, Buffalo, NY 14260 USA. EM sb244@buffalo.edu FU Tata Steel Group; National Science Foundation [DMR 0847169]; NASA Harriet G. Jenkins Fellowship FX This work was primarily funded by the Tata Steel Group. We also acknowledge partial support from the National Science Foundation under DMR 0847169. J.M.V. acknowledges partial support through a NASA Harriet G. Jenkins Fellowship. We appreciate helpful guidance from Dr. Debashish Bhattacharya. NR 23 TC 10 Z9 10 U1 2 U2 27 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1944-8244 J9 ACS APPL MATER INTER JI ACS Appl. Mater. Interfaces PD NOV 13 PY 2013 VL 5 IS 21 BP 10650 EP 10657 DI 10.1021/am402679w PG 8 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Science & Technology - Other Topics; Materials Science GA 253QD UT WOS:000327103500033 ER PT J AU Della Gaspera, E Tucker, R Star, K Lan, EH Ju, YS Dunn, B AF Della Gaspera, Enrico Tucker, Ryan Star, Kurt Lan, Esther H. Ju, Yongho Sungtaek Dunn, Bruce TI Copper-Based Conductive Composites with Tailored Thermal Expansion SO ACS APPLIED MATERIALS & INTERFACES LA English DT Article DE nanoparticles; colloidal synthesis; negative thermal expansion; zirconium tungstate; sintering; electrical properties ID METAL-MATRIX COMPOSITES; ZIRCONIUM TUNGSTATE; GOLD NANOPARTICLES; THIN-FILMS; ZRW2O8; TEMPERATURE; PARTICLES; PRESSURE; TRANSFORMATION; NANOCRYSTALS AB We have devised a moderate temperature hot-pressing route for preparing metal matrix composites which possess tunable thermal expansion. coefficients in combination with high electrical and thermal conductivities. The composites are based on incorporating ZrW2O8, a material with a negative coefficient of thermal expansion (CTE), within a continuous copper matrix. The ZrW2O8 enables us to tune the CTE in a predictable manner, while the copper phase is responsible for the electrical and thermal conductivity properties. An important consideration in the processing of these materials is to avoid the decomposition of the ZrW2O8 phase. This is accomplished by using relatively mild hot-pressing conditions of 500 degrees C for 1 h at 40 MPa. To ensure that these conditions enable sintering of the copper, we developed a synthesis route for the preparation of Cu nanoparticles (NPs) based on the reduction of a common copper salt in aqueous solution in the presence of a size control agent. Upon hot pressing these nanoparticles at 500 degrees C, we are able to achieve 92-93% of the theoretical density of copper. The resulting materials exhibit a CTE which can be tuned between the value of pure copper (16.5 ppm/degrees C) and less than 1 ppm/degrees C. Thus, by adjusting the relative amount of the two components, the properties of the composite can be designed so that a material with high electrical conductivity and a CTE that matches the relatively low CTE values of semiconductor or thermoelectric materials can be achieved. This unique combination of electrical and thermal properties enables these Cu-based metal matrix composites to be used as electrical contacts to a variety of semiconductor and thermoelectric devices which offer stable operation under thermal cycling conditions. C1 [Della Gaspera, Enrico; Tucker, Ryan; Star, Kurt; Lan, Esther H.; Dunn, Bruce] Univ Calif Los Angeles, Dept Mat Sci & Engn, Los Angeles, CA 90095 USA. [Star, Kurt] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ju, Yongho Sungtaek] Univ Calif Los Angeles, Dept Mech & Aerosp Engn, Los Angeles, CA 90095 USA. RP Dunn, B (reprint author), Univ Calif Los Angeles, Dept Mat Sci & Engn, 420 Westwood Plaza, Los Angeles, CA 90095 USA. EM bdunn@ucla.edu RI SPIEL, CSIRO/C-2809-2013; Della Gaspera, Enrico/H-3085-2013 OI Della Gaspera, Enrico/0000-0001-9948-5893 FU National Science Foundation; Department of Energy [CBET-1048726] FX This material is based upon work supported by the National Science Foundation and the Department of Energy under Grant No. CBET-1048726. The authors would like to thank Hyungseok Kim and Jesse Ko for TEM images and XRD measurements. NR 60 TC 6 Z9 6 U1 10 U2 66 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1944-8244 J9 ACS APPL MATER INTER JI ACS Appl. Mater. Interfaces PD NOV 13 PY 2013 VL 5 IS 21 BP 10966 EP 10974 DI 10.1021/am403227c PG 9 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Science & Technology - Other Topics; Materials Science GA 253QD UT WOS:000327103500074 PM 24175870 ER PT J AU Choi, KK Jhabvala, MD Sun, J Jhabvala, CA Waczynski, A Olver, K AF Choi, K. K. Jhabvala, M. D. Sun, J. Jhabvala, C. A. Waczynski, A. Olver, K. TI Resonator-quantum well infrared photodetectors SO APPLIED PHYSICS LETTERS LA English DT Article AB We applied a recent electromagnetic model to design the resonator-quantum well infrared photodetector (R-QWIP). In this design, we used an array of rings as diffractive elements to diffract normal incident light into parallel propagation and used the pixel volume as a resonator to intensify the diffracted light. With a proper pixel size, the detector resonates at certain optical wavelengths and thus yields a high quantum efficiency (QE). To test this detector concept, we fabricated a number of R-QWIPs with different quantum well materials and detector geometries. The experimental result agrees satisfactorily with the prediction, and the highest QE achieved is 71%. C1 [Choi, K. K.; Sun, J.; Olver, K.] US Army Res Lab, Electopt & Photon Div, Adelphi, MD 20783 USA. [Jhabvala, M. D.; Jhabvala, C. A.; Waczynski, A.] NASA, Goddard Space Flight Ctr, Instrument Syst & Technol Div, Greenbelt, MD 20771 USA. RP Choi, KK (reprint author), US Army Res Lab, Electopt & Photon Div, Adelphi, MD 20783 USA. EM kwong.k.choi.civ@mail.mil NR 11 TC 11 Z9 11 U1 0 U2 38 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD NOV 11 PY 2013 VL 103 IS 20 AR 201113 DI 10.1063/1.4831797 PG 4 WC Physics, Applied SC Physics GA 263OU UT WOS:000327818700013 ER PT J AU Barnes, JW Clark, RN Sotin, C Adamkovics, M Appere, T Rodriguez, S Soderblom, JM Brown, RH Buratti, BJ Baines, KH Le Mouelic, S Nicholson, PD AF Barnes, Jason W. Clark, Roger N. Sotin, Christophe Adamkovics, Mate Appere, Thomas Rodriguez, Sebastien Soderblom, Jason M. Brown, Robert H. Buratti, Bonnie J. Baines, Kevin H. Le Mouelic, Stephane Nicholson, Philip D. TI A TRANSMISSION SPECTRUM OF TITAN'S NORTH POLAR ATMOSPHERE FROM A SPECULAR REFLECTION OF THE SUN SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: individual (Titan); radiative transfer; techniques: spectroscopic ID GIANT PLANET TRANSITS; METHANE; CASSINI/VIMS; SURFACE; LIQUID; CM(-1); LAKES; NITROGEN; ETHANE; MODEL AB Cassini/VIMS T85 observations of a solar specular reflection off of Kivu Lacus (87 degrees.4N 241 degrees.1E) provide an empirical transmission spectrum of Titan's atmosphere. Because this observation was acquired from short range (33,000 km), its intensity makes it visible within the 2.0, 2.7, and 2.8 mu m atmospheric windows in addition to the 5 mu m window where all previous specular reflections have been seen. The resulting measurement of the total one- way normal atmospheric optical depth (corresponding to haze scattering plus haze and gas absorption) provides strong empirical constraints on radiative transfer models. Using those models, we find that the total haze column abundance in our observation is 20% higher than the Huygens equatorial value. Ours is the first measurement in the 2-5 mu m wavelength range that probes all the way to the surface in Titan's arctic, where the vast majority of surface liquids are located. The specular technique complements other probes of atmospheric properties such as solar occultations and the direct measurements from Huygens. In breaking the degeneracy between surface and atmospheric absorptions, our measured optical depths will help to drive future calculations of deconvolved surface albedo spectra. C1 [Barnes, Jason W.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA. [Clark, Roger N.] US Geol Survey, Denver, CO 80225 USA. [Sotin, Christophe; Buratti, Bonnie J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Adamkovics, Mate] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Appere, Thomas; Rodriguez, Sebastien] Univ Paris 07, Lab AIM, CNRS, CEA Saclay,DSM,IRFU SAp, F-91191 Gif Sur Yvette, France. [Soderblom, Jason M.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Brown, Robert H.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Baines, Kevin H.] Univ Wisconsin, Space Sci & Engn Ctr, Madison, WI 53706 USA. [Le Mouelic, Stephane] Univ Nantes, Lab Planetol & Geodynam, F-44322 Nantes, France. [Nicholson, Philip D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Barnes, JW (reprint author), Univ Idaho, Dept Phys, Moscow, ID 83844 USA. EM jwbarnes@uidaho.edu RI Barnes, Jason/B-1284-2009; Rodriguez, Sebastien/H-5902-2016; OI Barnes, Jason/0000-0002-7755-3530; Rodriguez, Sebastien/0000-0003-1219-0641; Soderblom, Jason/0000-0003-3715-6407 FU NASA/ESA Cassini mission; NASA CDAPS Program [NNX12AC28G]; NSF planetary astronomy grant [AST-1008788]; Agence Nationale de la Recherche (ANR projects "APOSTIC", France) [11BS56002] FX The authors acknowledge the support of the NASA/ESA Cassini mission. J.W.B. acknowledges support from the NASA CDAPS Program, grant No. NNX12AC28G. M.A'. is supported in part by NSF planetary astronomy grant AST-1008788. T. A. and S. R. benefited from the support by the Agence Nationale de la Recherche (ANR projects "APOSTIC" No. 11BS56002, France). NR 50 TC 2 Z9 2 U1 1 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2013 VL 777 IS 2 AR 161 DI 10.1088/0004-637X/777/2/161 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800080 ER PT J AU Brosius, JW AF Brosius, Jeffrey W. TI RAPID EVOLUTION OF THE SOLAR ATMOSPHERE DURING THE IMPULSIVE PHASE OF A MICROFLARE OBSERVED WITH THE EXTREME-ULTRAVIOLET IMAGING SPECTROMETER ABOARD HINODE: HINTS OF CHROMOSPHERIC MAGNETIC RECONNECTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: flares; Sun: transition region; Sun: UV radiation ID CORONAL DIAGNOSTIC SPECTROMETER; HIGH TIME RESOLUTION; LOOP RADIATIVE HYDRODYNAMICS; BRAGG CRYSTAL SPECTROMETER; X-RAY SPECTROSCOPY; XIX RESONANCE LINE; CA-XIX; ENERGY-TRANSPORT; ATOMIC DATABASE; EMISSION-LINES AB We obtained rapid cadence (11.2 s) EUV stare spectra of a solar microflare with the Extreme-ultraviolet Imaging Spectrometer aboard Hinode. The intensities of lines formed at temperatures too cool to be found in the corona brightened by factors around 16 early during this event, indicating that we observed a site of energy deposition in the chromosphere. We derive the density evolution of the flare plasma at temperature around 2 MK from the intensity ratio of Fe XIV lines at 264.789 angstrom and 274.204 angstrom. From both lines we removed the bright pre-flare quiescent emission, and from 274.204 we removed the blended emission of Si VII lambda 274.180 based on the Si VII lambda 274.180/275.361 intensity ratio, which varies only slightly with density. In this way the flare electron density is derived with emission from only the flare plasma. The density increased by an order of magnitude from its pre-flare quiescent average of (3.43 +/- 0.19) x 109 cm(-3) to its maximum impulsive phase value of (3.04 +/- 0.57) x 10(10) cm(-3) in 2 minutes. The fact that this rapid increase in density is not accompanied by systematic, large upward velocities indicates that the density increase is not due to the filling of loops with evaporated chromospheric material, but rather due to material being directly heated in the chromosphere, likely by magnetic reconnection. The density increase may be due to a progression of reconnection sites to greater depths in the chromosphere, where it has access to larger densities, or it may be due to compression of 2 MK plasma by the 10 MK plasma as it attempts to expand against the high-density chromospheric plasma. C1 Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. RP Brosius, JW (reprint author), Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Solar Phys Lab, Code 671, Greenbelt, MD 20771 USA. EM Jeffrey.W.Brosius@nasa.gov FU NASA [NNX10AC08G] FX J.W.B. acknowledges NASA support through SR&T grant NNX10AC08G. CHIANTI is a collaborative project involving George Mason University, the University of Michigan (USA), and the University of Cambridge (UK). Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners; it is operated by these agencies in cooperation with ESA and NSC (Norway). The AIA data used are provided courtesy of NASA/SDO and the AIA science team. We thank the referee for a thorough review of the manuscript and for helpful, constructive comments. NR 64 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 NOV 10 PY 2013 VL 777 IS 2 AR 135 DI 10.1088/0004-637X/777/2/135 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800054 ER PT J AU Cassano, R Ettori, S Brunetti, G Giacintucci, S Pratt, GW Venturi, T Kale, R Dolag, K Markevitch, M AF Cassano, R. Ettori, S. Brunetti, G. Giacintucci, S. Pratt, G. W. Venturi, T. Kale, R. Dolag, K. Markevitch, M. TI REVISITING SCALING RELATIONS FOR GIANT RADIO HALOS IN GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; radiation mechanisms: non-thermal; radio continuum: general; X-rays: galaxies: clusters ID DARK-MATTER HALOES; X-RAY-CLUSTERS; VLA SKY SURVEY; DEEP 1.4 GHZ; SUNYAEV-ZELDOVICH; COMA CLUSTER; T RELATION; FOLLOW-UP; REACCELERATION MODEL; LINEAR-REGRESSION AB Many galaxy clusters host megaparsec-scale radio halos, generated by ultrarelativistic electrons in the magnetized intracluster medium. Correlations between the synchrotron power of radio halos and the thermal properties of the hosting clusters were established in the last decade, including the connection between the presence of a halo and cluster mergers. The X-ray luminosity and redshift-limited Extended GMRT Radio Halo Survey provides a rich and unique dataset for statistical studies of the halos. We uniformly analyze the radio and X-ray data for the GMRT cluster sample, and use the new Planck Sunyaev-Zel'dovich (SZ) catalog to revisit the correlations between the power of radio halos and the thermal properties of galaxy clusters. We find that the radio power at 1.4 GHz scales with the cluster X-ray (0.1- 2.4 keV) luminosity computed within R-500 as P-1.4 similar to L-500(2.1 +/- 0.2). Our bigger and more homogenous sample confirms that the X-ray luminous (L-500 > 5 x 10(44) erg s(-1)) clusters branch into two populations-radio halos lie on the correlation, while clusters without radio halos have their radio upper limits well below that correlation. This bimodality remains if we excise cool cores from the X-ray luminosities. We also find that P-1.4 scales with the cluster integrated SZ signal within R-500, measured by Planck, as P-1.4 similar to Y-500(2.05 +/- 0.28), in line with previous findings. However, contrary to previous studies that were limited by incompleteness and small sample size, we find that "SZ-luminous" Y-500 > 6 x 10(-5) Mpc(2) clusters show a bimodal behavior for the presence of radio halos, similar to that in the radio-X-ray diagram. Bimodality of both correlations can be traced to clusters dynamics, with radio halos found exclusively in merging clusters. These results confirm the key role of mergers for the origin of giant radio halos, suggesting that they trigger the relativistic particle acceleration. C1 [Cassano, R.; Brunetti, G.; Venturi, T.; Kale, R.] INAF IRA, I-40129 Bologna, Italy. [Ettori, S.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Ettori, S.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy. [Giacintucci, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Giacintucci, S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Pratt, G. W.] Univ Paris Diderot, DSM CNRS, CEA Saclay, Lab AIM,IRFU,Serv Astrophys,CEA, F-91191 Gif Sur Yvette, France. [Dolag, K.] Univ Observ Munich, D-81679 Munich, Germany. [Dolag, K.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Markevitch, M.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Cassano, R (reprint author), INAF IRA, Via Gobetti 101, I-40129 Bologna, Italy. RI Ettori, Stefano/N-5004-2015; OI Ettori, Stefano/0000-0003-4117-8617; Brunetti, Gianfranco/0000-0003-4195-8613; Cassano, Rossella/0000-0003-4046-0637; Venturi, Tiziana/0000-0002-8476-6307 FU DFG; NASA [PF0-110071]; Chandra X-ray Center (CXC) FX We thank the referee for the useful comments. R. C. thanks Nemmen Rodrigo for providing the patched BCES routine running with gfortran in Mac, and N. Aghanim, D. Dallacasa, J. Donnert, C. Giocoli, P. Mazzotta, and F. Vazza, for useful discussions. We thank H. Bourdin for supplying additional data. K. D. acknowledges the support by the DFG Cluster of Excellence "Origin and Structure of the Universe." S.G. acknowledges the support of NASA through Einstein Postdoctoral Fellowship PF0-110071 awarded by the Chandra X-ray Center (CXC), which is operated by SAO. NR 94 TC 49 Z9 49 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 NOV 10 PY 2013 VL 777 IS 2 AR 141 DI 10.1088/0004-637X/777/2/141 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800060 ER PT J AU Cucchiara, A Prochaska, JX Perley, D Cenko, SB Werk, J Cardwell, A Turner, J Cao, Y Bloom, JS Cobb, BE AF Cucchiara, A. Prochaska, J. X. Perley, D. Cenko, S. B. Werk, J. Cardwell, A. Turner, J. Cao, Y. Bloom, J. S. Cobb, B. E. TI GEMINI SPECTROSCOPY OF THE SHORT-HARD GAMMA-RAY BURST GRB 130603B AFTERGLOW AND HOST GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: individual (GRB 130603B); techniques: imaging spectroscopy ID OPTICAL AFTERGLOWS; STAR-FORMATION; BINARY MERGER; REDSHIFT; TELESCOPE; PROGENITOR; LONG; IDENTIFICATION; METALLICITIES; SPECTROGRAPH AB We present early optical photometry and spectroscopy of the afterglow and host galaxy of the bright short-duration gamma-ray burst GRB 130603B discovered by the Swift satellite. Using our Target of Opportunity program on the Gemini South telescope, our prompt optical spectra reveal a strong trace from the afterglow superimposed on continuum and emission lines from the z = 0.3568 +/- 0.0005 host galaxy. The combination of a relatively bright optical afterglow (r' = 21.52 at Delta t = 8.4 hr), together with an observed offset of 0 ''.9 from the host nucleus (4.8 kpc projected distance at z = 0.3568), allow us to extract a relatively clean spectrum dominated by afterglow light. Furthermore, the spatially resolved spectrum allows us to constrain the properties of the explosion site directly, and compare these with the host galaxy nucleus, as well as other short-duration GRB host galaxies. We find that while the host is a relatively luminous (L approximate to 0.8 L-B*), star-forming (SFR = 1.84 M-circle dot yr(-1)) galaxy with almost solar metallicity, the spectrum of the afterglow exhibits weak Ca II absorption features but negligible emission features. The explosion site therefore lacks evidence of recent star formation, consistent with the relatively long delay time distribution expected in a compact binary merger scenario. The star formation rate (SFR; both in an absolute sense and normalized to the luminosity) and metallicity of the host are both consistent with the known sample of short-duration GRB hosts and with recent results which suggest GRB 130603B emission to be the product of the decay of radioactive species produced during the merging process of a neutron-star-neutron-star binary ("kilonova"). Ultimately, the discovery of more events similar to GRB 130603B and their rapid follow-up from 8 m class telescopes will open new opportunities for our understanding of the final stages of compact-objects binary systems and provide crucial information (redshift, metallicity, and chemical content of their explosion site) to characterize the environment of one of the most promising gravitational wave sources. C1 [Cucchiara, A.; Prochaska, J. X.; Werk, J.] Univ Calif Santa Cruz, Lick Observ, UCO, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Perley, D.; Cao, Y.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Cenko, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Cardwell, A.; Turner, J.] AURA, Gemini South Observ, La Serena, Chile. [Bloom, J. S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Cobb, B. E.] George Washington Univ, Washington, DC USA. RP Cucchiara, A (reprint author), Univ Calif Santa Cruz, Lick Observ, UCO, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA. EM acucchia@ucolick.org FU NASA [HST-HF-51296.01-A]; Space Telescope Science Institute [NAS 5-26555] FX A.C. thanks the anonymous referee for the valuable comments and suggestions which have helped significantly to improve the manuscript. A. C., also, thanks D. A. Kann and S. Savaglio for the valuable discussions and comments. Gemini results are based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the 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). Partial support for this work was provided by NASA through Hubble Fellowship grant HST-HF-51296.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. NR 75 TC 14 Z9 15 U1 0 U2 13 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 NOV 10 PY 2013 VL 777 IS 2 AR 94 DI 10.1088/0004-637X/777/2/94 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800013 ER PT J AU Gelfand, JD Castro, D Slane, PO Temim, T Hughes, JP Rakowski, C AF Gelfand, Joseph D. Castro, Daniel Slane, Patrick O. Temim, Tea Hughes, John P. Rakowski, Cara TI SUPERNOVA REMNANT KES 17: AN EFFICIENT COSMIC RAY ACCELERATOR INSIDE A MOLECULAR CLOUD SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; gamma rays: ISM; ISM: individual objects (Kes 17); ISM: supernova remnants; X-rays: individual (Kes 17) ID LARGE-AREA TELESCOPE; MAGNETIC-FIELD AMPLIFICATION; PARTICLE-ACCELERATION; INTERSTELLAR-MEDIUM; X-RAY; NONTHERMAL EMISSION; INFRARED SURVEY; GALACTIC PLANE; CASSIOPEIA-A; HIGH-ENERGY AB The supernova remnant Kes 17 (SNR G304.6+ 0.1) is one of a few but growing number of remnants detected across the electromagnetic spectrum. In this paper, we analyze recent radio, X-ray, and gamma-ray observations of this object, determining that efficient cosmic ray acceleration is required to explain its broadband non-thermal spectrum. These observations also suggest that Kes 17 is expanding inside a molecular cloud, though our determination of its age depends on whether thermal conduction or clump evaporation is primarily responsible for its center-filled thermal X-ray morphology. Evidence for efficient cosmic ray acceleration in Kes 17 supports recent theoretical work concluding that the strong magnetic field, turbulence, and clumpy nature of molecular clouds enhance cosmic ray production in supernova remnants. While additional observations are needed to confirm this interpretation, further study of Kes 17 is important for understanding how cosmic rays are accelerated in supernova remnants. C1 [Gelfand, Joseph D.] NYU Abu Dhabi, New York, NY 10276 USA. [Castro, Daniel] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Slane, Patrick O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Temim, Tea] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Rakowski, Cara] US Patent & Trademark Off, Alexandria, VA USA. RP Gelfand, JD (reprint author), NYU Abu Dhabi, POB 903, New York, NY 10276 USA. EM jg168@cosmo.nyu.edu; cara.rakowski@gmail.com RI Gelfand, Joseph/F-1110-2015; OI Gelfand, Joseph/0000-0003-4679-1058; Temim, Tea/0000-0001-7380-3144 FU NASA [NNX10AR51G, NAS8-03060]; NSF Astronomy and Astrophysics Postdoctoral Fellowship grant [AST-0702957]; Commonwealth of Australia FX The authors thank the anonymous referee for usual comments and suggestions. J.D.G. acknowledges the support of NASA grant NNX10AR51G, and NSF Astronomy and Astrophysics Postdoctoral Fellowship grant AST-0702957, as well as the hospitality of the Center for Cosmology and Particle Physics at New York University where much of this work was conducted. P.O.S. acknowledges support from NASA contract NAS8-03060. The Australia Telescope is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. This research has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). NR 85 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 NOV 10 PY 2013 VL 777 IS 2 AR 148 DI 10.1088/0004-637X/777/2/148 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800067 ER PT J AU Gjerlow, E Mikkelsen, K Eriksen, HK Gorski, KM Huey, G Jewell, JB Naess, SK Rocha, G Seljebotn, DS Wehus, IK AF Gjerlow, E. Mikkelsen, K. Eriksen, H. K. Gorski, K. M. Huey, G. Jewell, J. B. Naess, S. K. Rocha, G. Seljebotn, D. S. Wehus, I. K. TI COSMIC MICROWAVE BACKGROUND LIKELIHOOD APPROXIMATION FOR BANDED PROBABILITY DISTRIBUTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; methods: data analysis; methods: numerical; methods: statistical ID PROBE WMAP OBSERVATIONS; POWER SPECTRUM ESTIMATION; MAPS; ESTIMATOR AB We investigate sets of random variables that can be arranged sequentially such that a given variable only depends conditionally on its immediate predecessor. For such sets, we show that the full joint probability distribution may be expressed exclusively in terms of uni- and bivariate marginals. Under the assumption that the cosmic microwave background (CMB) power spectrum likelihood only exhibits correlations within a banded multipole range, Delta l(C), we apply this expression to two outstanding problems in CMB likelihood analysis. First, we derive a statistically well-defined hybrid likelihood estimator, merging two independent (e.g., low- and high-l) likelihoods into a single expression that properly accounts for correlations between the two. Applying this expression to the WilkinsonMicrowave Anisotropy Probe (WMAP) likelihood, we verify that the effect of correlations on cosmological parameters in the transition region is negligible in terms of cosmological parameters for WMAP; the largest relative shift seen for any parameter is 0.06s. However, because this may not hold for other experimental setups (e. g., for different instrumental noise properties or analysis masks), but must rather be verified on a case-by-case basis, we recommend our new hybridization scheme for future experiments for statistical self-consistency reasons. Second, we use the same expression to improve the convergence rate of the Blackwell-Rao likelihood estimator, reducing the required number of Monte Carlo samples by several orders of magnitude, and thereby extend it to high-l applications. C1 [Gjerlow, E.; Mikkelsen, K.; Eriksen, H. K.; Naess, S. K.; Seljebotn, D. S.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Gorski, K. M.; Huey, G.; Jewell, J. B.; Rocha, G.; Wehus, I. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Naess, S. K.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Rocha, G.] CALTECH, Pasadena, CA 91109 USA. RP Gjerlow, E (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0315 Oslo, Norway. EM eirik.gjerlow@astro.uio.no FU ERC Starting Grant [StG2010-257080]; Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA FX This project was supported by the ERC Starting Grant StG2010-257080. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Some of the results in this paper have been derived using the HEALPix (Gorski et al. 2005) software and analysis package. NR 22 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 NOV 10 PY 2013 VL 777 IS 2 AR 150 DI 10.1088/0004-637X/777/2/150 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800069 ER PT J AU Haghighipour, N Kaltenegger, L AF Haghighipour, Nader Kaltenegger, Lisa TI CALCULATING THE HABITABLE ZONE OF BINARY STAR SYSTEMS. II. P-TYPE BINARIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; planetary systems; planets and satellites: atmospheres; planets and satellites: terrestrial planets ID TRANSITING CIRCUMBINARY PLANET; MAIN-SEQUENCE STARS; ORBITAL STABILITY; HU AQUARII; EARTH-MASS; KEPLER-16 AB We have developed a comprehensive methodology for calculating the circumbinary habitable zone (HZ) in planethosting P-type binary star systems. We present a general formalism for determining the contribution of each star of the binary to the total flux received at the top of the atmosphere of an Earth-like planet and use the Sun's HZ to calculate the inner and outer boundaries of the HZ around a binary star system. We apply our calculations to the Kepler's currently known circumbinary planetary systems and show the combined stellar flux that determines the boundaries of their HZs. We also show that the HZ in P-type systems is dynamic and, depending on the luminosity of the binary stars, their spectral types, and the binary eccentricity, its boundaries vary as the stars of the binary undergo their orbital motion. We present the details of our calculations and discuss the implications of the results. C1 [Haghighipour, Nader] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Haghighipour, Nader] Univ Hawaii, NASA, Astrobiol Inst, Honolulu, HI 96822 USA. [Haghighipour, Nader] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Kaltenegger, Lisa] MPIA, D-69117 Heidelberg, Germany. [Kaltenegger, Lisa] CfA, Cambridge, MA 02138 USA. RP Haghighipour, N (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. FU NASA Astrobiology Institute [NNA09DA77]; HST grant [HST-GO-12548.06-A]; Alexander von Humboldt Foundation [HST-GO-12548.06-A]; NASA through a grant from the Space Telescope Science Institute; NASA [NAS5-26555]; NAI; DFG [3142/1-1] FX We are grateful to Tobias Muller at the Computational Physics group at the Institute for Astronomy and Astrophysics, University of Tubingen for making the movies and graphs of HZs. N. H. acknowledges support from the NASA Astrobiology Institute under cooperative agreement NNA09DA77 at the Institute for Astronomy, University of Hawaii, HST grant HST-GO-12548.06-A, and Alexander von Humboldt Foundation. Support for program HST-GO-12548.06-A was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. N. H. is also thankful to the Computational Physics group at the Institute for Astronomy and Astrophysics, University of Tubingen for their kind hospitality during the course of this project. L. K. acknowledges support from NAI and DFG funding ENP Ka 3142/1-1. NR 33 TC 16 Z9 17 U1 0 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 NOV 10 PY 2013 VL 777 IS 2 AR 166 DI 10.1088/0004-637X/777/2/166 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800085 ER PT J AU Inami, H Armus, L Charmandaris, V Groves, B Kewley, L Petric, A Stierwalt, S Diaz-Santos, T Surace, J Rich, J Haan, S Howell, J Evans, AS Mazzarella, J Marshall, J Appleton, P Lord, S Spoon, H Frayer, D Matsuhara, H Veilleux, S AF Inami, H. Armus, L. Charmandaris, V. Groves, B. Kewley, L. Petric, A. Stierwalt, S. Diaz-Santos, T. Surace, J. Rich, J. Haan, S. Howell, J. Evans, A. S. Mazzarella, J. Marshall, J. Appleton, P. Lord, S. Spoon, H. Frayer, D. Matsuhara, H. Veilleux, S. TI MID-INFRARED ATOMIC FINE-STRUCTURE EMISSION-LINE SPECTRA OF LUMINOUS INFRARED GALAXIES: SPITZER/IRS SPECTRA OF THE GOALS SAMPLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: ISM; galaxies: starburst; infrared: galaxies ID HUBBLE-SPACE-TELESCOPE; STAR-FORMING GALAXIES; HIGH-RESOLUTION SPECTROSCOPY; ACTIVE GALACTIC NUCLEI; SKY LIRG SURVEY; STARBURST GALAXIES; NEARBY GALAXIES; STELLAR POPULATIONS; SUPERNOVA-REMNANTS; OXYGEN ABUNDANCES AB We present the data and our analysis of mid-infrared atomic fine-structure emission lines detected in Spitzer/Infrared Spectrograph high-resolution spectra of 202 local Luminous Infrared Galaxies (LIRGs) observed as part of the Great Observatories All-sky LIRG Survey (GOALS). We readily detect emission lines of [S IV], [Ne II], [Ne v], [Ne III], [S III] 18.7 mu m, [OIV], [Fe II], [S III] 33.5, and [Si II]. More than 75% of these galaxies are classified as starburst-dominated sources in the mid-infrared, based on the [Ne v]/[Ne II] line flux ratios and equivalent width of the 6.2 mu m polycyclic aromatic hydrocarbon feature. We compare ratios of the emission-line fluxes to those predicted from stellar photo-ionization and shock-ionization models to constrain the physical and chemical properties of the gas in the starburst LIRG nuclei. Comparing the [S III]/[Ne II] and [Ne III]/[Ne II] line ratios to the Starburst-99-Mappings III models with an instantaneous burst history, the emission-line ratios suggest that the nuclear starbursts in our LIRGs have ages of 1-4.5 Myr, metallicities of 1-2 Z(circle dot), and ionization parameters of 2-8x10(7) cm s(-1). Based on the [S III](33.5 mu m)/[S III] 18.7 mu m ratios, the electron density in LIRG nuclei is typically one to a few hundred cm-3, with a median electron density of similar to 300 cm(-3), for those sources above the low density limit for these lines. We also find that strong shocks are likely present in 10 starburst-dominated sources of our sample. A significant fraction of the GOALS sources (80) have resolved neon emission-line profiles (FWHM >= 600 km s(-1)) and five show clear differences in the velocities of the [Ne III] or [Nev] emission lines, relative to [Ne II], of more than 200 km s-1. Furthermore, six starburst and five active galactic nucleus dominated LIRGs show a clear trend of increasing line width with ionization potential, suggesting the possibility of a compact energy source and stratified interstellar medium in their nuclei. We confirm a strong correlation between the sum of the [Ne II] 12.8 mu m and [Ne III] 15.5 mu m emission, as well as [S III] 33.5 mu m, with both the infrared luminosity and the 24 mu m warm dust emission measured from the spectra, consistent with all three lines tracing ongoing star formation. Finally, we find no correlation between the hardness of the radiation field or the emission-line width and the ratio of the total infrared to 8 mu m emission (IR8), a measure of the strength of the starburst and the distance of the LIRGs from the star-forming main sequence. This may be a function of the fact that the infrared luminosity and the mid-infrared fine-structure lines are sensitive to different timescales over the starburst, or that IR8 is more sensitive to the geometry of the region emitting the warm dust than the radiation field producing the Hii region emission. C1 [Inami, H.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Inami, H.; Armus, L.; Stierwalt, S.; Diaz-Santos, T.; Surace, J.; Howell, J.; Marshall, J.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Charmandaris, V.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece. [Charmandaris, V.] Univ Crete, Inst Theoret & Computat Phys, GR-71003 Iraklion, Greece. [Charmandaris, V.] IESL Fdn Res & Technol Hellas, GR-71110 Iraklion, Greece. [Charmandaris, V.] Observ Paris, Chercheur Associe, F-75014 Paris, France. [Groves, B.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kewley, L.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Petric, A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Stierwalt, S.; Evans, A. S.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Rich, J.] Carnegie Inst Sci, Pasadena, CA 91101 USA. [Haan, S.] CSIRO Astron & Space Sci, Marsfield, NSW 2122, Australia. [Evans, A. S.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Mazzarella, J.; Lord, S.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Appleton, P.] NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. [Spoon, H.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Frayer, D.] Natl Radio Astron Observ, Green Bank, WV 24944 USA. [Matsuhara, H.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Tokyo, Japan. [Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Inami, H (reprint author), Natl Opt Astron Observ, Tucson, AZ 85719 USA. EM inami@noao.edu RI Charmandaris, Vassilis/A-7196-2008; OI Charmandaris, Vassilis/0000-0002-2688-1956; Rich, Jeffrey/0000-0002-5807-5078; Mazzarella, Joseph/0000-0002-8204-8619; Appleton, Philip/0000-0002-7607-8766 NR 76 TC 22 Z9 21 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 NOV 10 PY 2013 VL 777 IS 2 AR 156 DI 10.1088/0004-637X/777/2/156 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800075 ER PT J AU Kaltenegger, L Haghighipour, N AF Kaltenegger, Lisa Haghighipour, Nader TI CALCULATING THE HABITABLE ZONE OF BINARY STAR SYSTEMS. I. S-TYPE BINARIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; planets and satellites: atmospheres; planets and satellites: dynamical evolution and stability; planets and satellites: terrestrial planets; planet-star interactions ID ALPHA-CENTAURI-B; MAIN-SEQUENCE STARS; EXTRA-SOLAR PLANETS; ORBITS; DETECTABILITY; STABILITY AB We have developed a comprehensive methodology for calculating the boundaries of the habitable zone (HZ) of planet-hosting S-type binary star systems. Our approach is general and takes into account the contribution of both stars to the location and extent of the binary HZ with different stellar spectral types. We have studied how the binary eccentricity and stellar energy distribution affect the extent of the HZ. Results indicate that in binaries where the combination of mass-ratio and orbital eccentricity allows planet formation around a star of the system to proceed successfully, the effect of a less luminous secondary on the location of the primary's HZ is generally negligible. However, when the secondary is more luminous, it can influence the extent of the HZ. We present the details of the derivations of our methodology and discuss its application to the binary HZ around the primary and secondary main-sequence stars of an FF, MM, and FM binary, as well as two known planet-hosting binaries a Cen AB and HD 196886. C1 [Kaltenegger, Lisa] MPIA, D-69117 Heidelberg, Germany. [Kaltenegger, Lisa] CfA, Cambridge, MA 02138 USA. [Haghighipour, Nader] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Haghighipour, Nader] Univ Hawaii Manoa, NASA, Astrobiol Inst, Honolulu, HI 96822 USA. [Haghighipour, Nader] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. RP Kaltenegger, L (reprint author), MPIA, Koenigstuhl 17, D-69117 Heidelberg, Germany. EM kaltenegger@mpia.de FU NAI at the Institute for Astronomy [NNA09DA77]; DFG [Ka 3142/1-1]; University of Hawaii; NASA EXOB [NNX09AN05G]; HST grant [HST-GO-12548.06-A]; Alexander von Humboldt Foundation; NASA through a grant from the Space Telescope Science Institute [HST-GO-12548.06-A]; NASA [NAS5-26555] FX L. K. acknowledges support from NAI and DFG funding ENP Ka 3142/1-1. N. H. acknowledges support from the NAI under Cooperative Agreement NNA09DA77 at the Institute for Astronomy, the University of Hawaii, NASA EXOB grant NNX09AN05G, HST grant HST-GO-12548.06-A, and the Alexander von Humboldt Foundation. Support for program HST-GO-12548.06-A was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. NR 33 TC 21 Z9 22 U1 0 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 NOV 10 PY 2013 VL 777 IS 2 AR 165 DI 10.1088/0004-637X/777/2/165 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800084 ER PT J AU Mason, RE Almeida, CR Levenson, NA Nemmen, R Alonso-Herrero, A AF Mason, R. E. Ramos Almeida, C. Levenson, N. A. Nemmen, R. Alonso-Herrero, A. TI THE ROLE OF THE ACCRETION DISK, DUST, AND JETS IN THE IR EMISSION OF LOW-LUMINOSITY ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion; accretion disks; galaxies: active; galaxies: individual (NGC 1052, NGC 3031, NGC 3998, NGC 4374, NGC 4486, NGC 4579, NGC 4594); galaxies: nuclei; infrared: galaxies ID RADIATIVELY INEFFICIENT ACCRETION; SPECTRAL ENERGY-DISTRIBUTIONS; ADVECTION-DOMINATED ACCRETION; CLUMPY TORUS MODELS; SEYFERT-GALAXIES; NEARBY GALAXIES; NGC 4258; AGN; SPECTROSCOPY; FLOW AB We use recent high-resolution infrared (IR; 1-20 mu m) photometry to examine the origin of the IR emission in low-luminosity active galactic nuclei (LLAGN). The data are compared with published model fits that describe the spectral energy distribution (SED) of LLAGN in terms of an advection-dominated accretion flow, truncated thin accretion disk, and jet. The truncated disk in these models is usually not luminous enough to explain the observed IR emission, and in all cases its spectral shape is much narrower than the broad IR peaks in the data. Synchrotron radiation from the jet appears to be important in very radio-loud nuclei, but the detection of strong silicate emission features in many objects indicates that dust must also contribute. We investigate this point by fitting the IR SED of NGC 3998 using dusty torus and optically thin (tau(mid-IR) similar to 1) dust shell models. While more detailed modeling is necessary, these initial results suggest that dust may account for the nuclear mid-IR emission of many LLAGN. C1 [Mason, R. E.] Northern Operat Ctr, Gemini Observ, Hilo, HI 96720 USA. [Ramos Almeida, C.] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Ramos Almeida, C.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain. [Levenson, N. A.] Southern Operat Ctr, Gemini Observ, La Serena, Chile. [Nemmen, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Alonso-Herrero, A.] CSIC UC, Inst Fis Cantabria, E-39005 Santander, Spain. RP Mason, RE (reprint author), Northern Operat Ctr, Gemini Observ, 670 N Aohoku Pl, Hilo, HI 96720 USA. EM rmason@gemini.edu RI Nemmen, Rodrigo/O-6841-2014; Alonso-Herrero, Almudena/H-1426-2015; OI Alonso-Herrero, Almudena/0000-0001-6794-2519; Levenson, Nancy A./0000-0003-4209-639X FU Spanish Plan Nacional de Astronomia y Astrofisica [AYA2009-05705-E]; CRA [PN-AYA2010-21887-C04.04]; NASA FX We thank the referee for a useful report that helped improve this work. Supported by the Gemini Observatory, operated by the Association of Universities for Research in Astronomy, Inc., on behalf of the international Gemini partnership of Argentina, Australia, Brazil, Canada, Chile, and the USA. A. A.-H. acknowledges support from the Spanish Plan Nacional de Astronomia y Astrofisica under grant AYA2009-05705-E, CRA from PN-AYA2010-21887-C04.04. R.N. 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. NR 53 TC 9 Z9 9 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 NOV 10 PY 2013 VL 777 IS 2 AR 164 DI 10.1088/0004-637X/777/2/164 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800083 ER PT J AU Mirocha, J Harker, GJA Burns, JO AF Mirocha, Jordan Harker, Geraint J. A. Burns, Jack O. TI INTERPRETING THE GLOBAL 21 cm SIGNAL FROM HIGH REDSHIFTS. I. MODEL-INDEPENDENT CONSTRAINTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark ages, reionization, first stars; diffuse radiation ID PROBE WMAP OBSERVATIONS; 1ST COSMOLOGICAL OBJECTS; SUPERMASSIVE BLACK-HOLES; POPULATION III GALAXIES; SQUARE KILOMETER ARRAY; STAR-FORMING GALAXIES; WEBB-SPACE-TELESCOPE; DEEP FIELD CAMPAIGN; SPIN-EXCHANGE RATES; LY-ALPHA EMITTERS AB The sky-averaged (global) 21 cm signal is a powerful probe of the intergalactic medium (IGM) prior to the completion of reionization. However, so far it has been unclear whether it will provide more than crude estimates of when the universe's first stars and black holes formed, even in the best case scenario in which the signal is accurately extracted from the foregrounds. In contrast to previous work, which has focused on predicting the 21 cm signatures of the first luminous objects, we investigate an arbitrary realization of the signal and attempt to translate its features to the physical properties of the IGM. Within a simplified global framework, the 21 cm signal yields quantitative constraints on the Ly alpha background intensity, net heat deposition, ionized fraction, and their time derivatives without invoking models for the astrophysical sources themselves. The 21 cm absorption signal is most easily interpreted, setting strong limits on the heating rate density of the universe with a measurement of its redshift alone, independent of the ionization history or details of the Ly alpha background evolution. In a companion paper, we extend these results, focusing on the confidence with which one can infer source emissivities from IGM properties. C1 [Mirocha, Jordan; Harker, Geraint J. A.; Burns, Jack O.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Mirocha, Jordan; Harker, Geraint J. A.; Burns, Jack O.] NASA, Ames Res Ctr, NASA Lunar Sci Inst, Moffett Field, CA 94035 USA. RP Mirocha, J (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, Campus Box 389, Boulder, CO 80309 USA. EM jordan.mirocha@colorado.edu OI Harker, Geraint/0000-0002-7894-4082 FU NASA Lunar Science Institute [NNA09DB30A] FX The authors thank the anonymous referee, whose suggestions helped improve the quality of this manuscript, and acknowledge the LUNAR consortium,12 headquartered at the University of Colorado, which is funded by the NASA Lunar Science Institute (via Cooperative Agreement NNA09DB30A) to investigate concepts for astrophysical observatories on the Moon. NR 104 TC 16 Z9 16 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 NOV 10 PY 2013 VL 777 IS 2 AR 118 DI 10.1088/0004-637X/777/2/118 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800037 ER PT J AU Neill, JL Crockett, NR Bergin, EA Pearson, JC Xu, LH AF Neill, Justin L. Crockett, Nathan R. Bergin, Edwin A. Pearson, John C. Xu, Li-Hong TI DEUTERATED MOLECULES IN ORION KL FROM HERSCHEL/HIFI SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: abundances; ISM: individual objects (Orion KL); ISM: molecules ID STAR-FORMING REGIONS; TORSION-ROTATION TRANSITIONS; EXTRAORDINARY SOURCES HEXOS; GRAIN SURFACE-CHEMISTRY; O1 HALE-BOPP; GROUND-STATE; LINE SURVEY; COLLISIONAL EXCITATION; HOT CORE; SPECTROSCOPIC PARAMETERS AB We present a comprehensive study of the deuterated molecules detected in the fullband HIFI survey of the Orion Kleinmann-Low nebula (Orion KL) region. Ammonia, formaldehyde, and methanol and their singly deuterated isotopologues are each detected through numerous transitions in this survey with a wide range in optical depths and excitation conditions. In conjunction with a recent study of the abundance of HDO and H2O in Orion KL, this study yields the best constraints on deuterium fractionation in an interstellar molecular cloud to date. As previous studies have found, both the Hot Core and Compact Ridge regions within Orion KL contain significant abundances of deuterated molecules, suggesting an origin in cold grain mantles. In the Hot Core, we find that ammonia is roughly a factor of two more fractionated than water. In the Compact Ridge, meanwhile, we find similar deuterium fractionation in water, formaldehyde, and methanol, with D/H ratios of (2-8) x 10(-3). The [CH2DOH]/[CH3OD] ratio in the Compact Ridge is found to be 1.2+/-0.3. The Hot Core generally has lower deuterium fractionation than the Compact Ridge, suggesting a slightly warmer origin, or a greater contribution from warm gas phase chemistry. C1 [Neill, Justin L.; Crockett, Nathan R.; Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Pearson, John C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Xu, Li-Hong] Univ New Brunswick, Dept Phys, CLAMS, St John, NB E2L 4L5, Canada. RP Neill, JL (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM jneill@umich.edu RI Xu, Li-Hong/J-5095-2015 FU NASA through JPL/Caltech; Natural Sciences and Engineering Research Council of Canada FX 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 U.S. 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 Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. Author L. H. X. thanks the Natural Sciences and Engineering Research Council of Canada for financial support of this research program. NR 94 TC 20 Z9 20 U1 0 U2 11 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 NOV 10 PY 2013 VL 777 IS 2 AR 85 DI 10.1088/0004-637X/777/2/85 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800004 ER PT J AU Nesvold, ER Kuchner, MJ Rein, H Pan, M AF Nesvold, Erika R. Kuchner, Marc J. Rein, Hanno Pan, Margaret TI SMACK: A NEW ALGORITHM FOR MODELING COLLISIONS AND DYNAMICS OF PLANETESIMALS IN DEBRIS DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE celestial mechanics; circumstellar matter; interplanetary medium; methods: numerical; planet-disk interactions; planetary systems ID BETA-PICTORIS; KUIPER-BELT; RESONANT SIGNATURES; SIZE DISTRIBUTIONS; PLANETARY SYSTEM; EPSILON-ERIDANI; DUSTY DEBRIS; EVOLUTION; CASCADES; RINGS AB We present the Superparticle-Method/Algorithm for Collisions in Kuiper belts and debris disks (SMACK), a new method for simultaneously modeling, in three dimensions, the collisional and dynamical evolution of planetesimals in a debris disk with planets. SMACK can simulate azimuthal asymmetries and how these asymmetries evolve over time. We show that SMACK is stable to numerical viscosity and numerical heating over 10(7) yr and that it can reproduce analytic models of disk evolution. We use SMACK to model the evolution of a debris ring containing a planet on an eccentric orbit. Differential precession creates a spiral structure as the ring evolves, but collisions subsequently break up the spiral, leaving a narrower eccentric ring. C1 [Nesvold, Erika R.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Kuchner, Marc J.; Pan, Margaret] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 21230 USA. [Rein, Hanno] Inst Adv Study, Princeton, NJ 08540 USA. [Rein, Hanno] Univ Toronto Scarborough, Toronto, ON M1C 1A4, Canada. RP Nesvold, ER (reprint author), Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA. EM Erika.Nesvold@umbc.edu; Marc.Kuchner@nasa.gov; rein@ias.edu; Margaret.Pan@nasa.gov FU NASA Planetary Geology and Geophysics Program [11-PGG11-0032] FX We thank the NASA High-End Computing Program for granting us time on the Discover cluster. This research was supported in part by the NASA Planetary Geology and Geophysics Program, grant No. 11-PGG11-0032. NR 57 TC 18 Z9 18 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 NOV 10 PY 2013 VL 777 IS 2 AR 144 DI 10.1088/0004-637X/777/2/144 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800063 ER PT J AU Pajola, M Lazzarin, M Ore, CMD Cruikshank, DP Roush, TL Magrin, S Bertini, I La Forgia, F Barbieri, C AF Pajola, M. Lazzarin, M. Ore, C. M. Dalle Cruikshank, D. P. Roush, T. L. Magrin, S. Bertini, I. La Forgia, F. Barbieri, C. TI PHOBOS AS A D-TYPE CAPTURED ASTEROID, SPECTRAL MODELING FROM 0.25 TO 4.0 mu m SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: individual (Phobos); planets and satellites: surfaces; techniques: imaging spectroscopy ID TAGISH LAKE METEORITE; HUBBLE-SPACE-TELESCOPE; CARBONACEOUS CHONDRITE; ROSETTA-ALICE; 21 LUTETIA; OPTICAL-PROPERTIES; HST OBSERVATIONS; MARS PATHFINDER; 4 VESTA; ULTRAVIOLET AB This paper describes the spectral modeling of the surface of Phobos in the wavelength range between 0.25 and 4.0 mu m. We use complementary data to cover this spectral range: the OSIRIS (Optical, Spectroscopic, and Infrared Remote Imaging System on board the ESA Rosetta spacecraft) reflectance spectrum that Pajola et al. merged with the VSK-KRFM-ISM (Videospectrometric Camera (VSK)-Combined Radiometer and Photometer for Mars (KRFM)-Imaging Spectrometer for Mars (ISM) on board the USSR Phobos 2 spacecraft) spectra by Murchie & Erard and the IRTF (NASA Infrared Telescope Facility, Hawaii, USA) spectra published by Rivkin et al. The OSIRIS data allow the characterization of an area of Phobos covering from 86 degrees.8 N to 90 degrees S in latitude and from 126 degrees W to 286 degrees W in longitude. This corresponds chiefly to the trailing hemisphere, but with a small sampling of the leading hemisphere as well. We compared the OSIRIS results with the Trojan D-type asteroid 624 Hektor and show that the overall slope and curvature of the two bodies over the common wavelength range are very similar. This favors Phobos being a captured D-type asteroid as previously suggested. We modeled the OSIRIS data using two models, the first one with a composition that includes organic carbonaceous material, serpentine, olivine, and basalt glass, and the second one consisting of Tagish Lake meteorite and magnesium-rich pyroxene glass. The results of these models were extended to longer wavelengths to compare the VSK-KRFM-ISM and IRTF data. The overall shape of the second model spectrum between 0.25 and 4.0 mu m shows curvature and an albedo level that match both the OSIRIS and Murchie & Erard data and the Rivkin et al. data much better than the first model. The large interval fit is encouraging and adds weight to this model, making it our most promising fit for Phobos. Since Tagish Lake is commonly used as a spectral analog for D-type asteroids, this provides additional support for compositional similarities between Phobos and D-type asteroids. C1 [Pajola, M.; Magrin, S.; Bertini, I.; Barbieri, C.] Univ Padua, Ctr Studies & Act Space, CISAS, I-35131 Padua, Italy. [Lazzarin, M.; La Forgia, F.; Barbieri, C.] Univ Padua, Dept Phys & Astron, I-35131 Padua, Italy. [Ore, C. M. Dalle] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Ore, C. M. Dalle; Cruikshank, D. P.; Roush, T. L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Pajola, M (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM maurizio.pajola@studenti.unipd.it RI La Forgia, Fiorangela/F-3107-2015 OI La Forgia, Fiorangela/0000-0003-3924-1867 NR 48 TC 8 Z9 8 U1 0 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 NOV 10 PY 2013 VL 777 IS 2 AR 127 DI 10.1088/0004-637X/777/2/127 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800046 ER PT J AU Sahai, R Vlemmings, WHT Huggins, PJ Nyman, LA Gonidakis, I AF Sahai, R. Vlemmings, W. H. T. Huggins, P. J. Nyman, L-A Gonidakis, I. TI ALMA OBSERVATIONS OF THE COLDEST PLACE IN THE UNIVERSE: THE BOOMERANG NEBULA SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary nebulae: individual (Boomerang Nebula); radio lines: stars; stars: AGB and post-AGB; stars: mass-loss; stars: winds, outflows ID MORPHOLOGICAL CLASSIFICATION-SYSTEM; OH-IR STARS; MASS-LOSS; DISKS AB The Boomerang Nebula is the coldest known object in the universe, and an extreme member of the class of pre-planetary nebulae, objects which represent a short-lived transitional phase between the asymptotic giant branch and planetary nebula evolutionary stages. Previous single-dish CO (J = 1-0) observations (with a 45 '' beam) showed that the high-speed outflow in this object has cooled to a temperature significantly below the temperature of the cosmic background radiation. Here we report the first observations of the Boomerang Nebula with ALMA in the CO J = 2-1 and J = 1-0 lines to resolve the structure of this ultra-cold nebula. We find a central hourglass-shaped nebula surrounded by a patchy, but roughly round, cold high-velocity outflow. We compare the ALMA data with visible-light images obtained with the Hubble Space Telescope and confirm that the limb-brightened bipolar lobes seen in these data represent hollow cavities with dense walls of molecular gas and dust producing both the molecular-emission-line and scattered-light structures seen at millimeter and visible wavelengths. The large diffuse biconical shape of the nebula seen in the visible wavelength range is likely due to preferential illumination of the cold, high-velocity outflow. We find a compact source of millimeter-wave continuum in the nebular waist-these data, together with sensitive upper limits on the radio continuum using observations with ATCA, indicate the presence of a substantial mass of very large (millimeter-sized) grains in the waist of the nebula. Another unanticipated result is the detection of CO emission regions beyond the ultra-cold region which indicate the re-warming of the cold gas, most likely due to photoelectric grain heating. C1 [Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Vlemmings, W. H. T.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden. [Huggins, P. J.] NYU, Dept Phys, New York, NY 10003 USA. [Nyman, L-A] JAO, Santiago, Chile. [Nyman, L-A] European So Observ, Santiago 19, Chile. [Gonidakis, I.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Marsfield, NSW 2122, Australia. RP Sahai, R (reprint author), CALTECH, Jet Prop Lab, MS 183-900, Pasadena, CA 91109 USA. EM raghvendra.sahai@jpl.nasa.gov OI /0000-0002-2700-9916 FU NASA; Deutsche Forschungsgemeinschaft (DFG) [VL 61/3-1]; Marie Curie Career Integration Grant [321691]; NSF [AST 08-06910]; internal Research and Technology Development program FX This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00510. S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC, and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. R.S.'s contribution to the research described here was carried out at JPL, California Institute of Technology, under a contract with NASA and partially funded through the internal Research and Technology Development program. W. V. acknowledges support by the Deutsche Forschungsgemeinschaft (DFG; through the Emmy Noether Research grant VL 61/3-1) and Marie Curie Career Integration Grant 321691. This work was supported in part by NSF grant AST 08-06910 (to P.J.H.). NR 14 TC 8 Z9 8 U1 0 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 NOV 10 PY 2013 VL 777 IS 2 AR 92 DI 10.1088/0004-637X/777/2/92 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800011 ER PT J AU Sbarrato, T Tagliaferri, G Ghisellini, G Perri, M Puccetti, S Balokovic, M Nardini, M Stern, D Boggs, SE Brandt, WN Christensen, FE Giommi, P Greiner, J Hailey, CJ Harrison, FA Hovatta, T Madejski, GM Rau, A Schady, P Sudilovsky, V Urry, CM Zhang, WW AF Sbarrato, T. Tagliaferri, G. Ghisellini, G. Perri, M. Puccetti, S. Balokovic, M. Nardini, M. Stern, D. Boggs, S. E. Brandt, W. N. Christensen, F. E. Giommi, P. Greiner, J. Hailey, C. J. Harrison, F. A. Hovatta, T. Madejski, G. M. Rau, A. Schady, P. Sudilovsky, V. Urry, C. M. Zhang, W. W. TI NuSTAR DETECTION OF THE BLAZAR B2 1023+25 AT REDSHIFT 5.3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; quasars: general; quasars: individual (B2 1023+25); X-rays: general ID ACTIVE GALACTIC NUCLEI; RAY SPECTRAL PROPERTIES; RADIO-LOUD QUASARS; X-RAY; BLACK-HOLES; SNAPSHOT OBSERVATIONS; DISTANT BLAZAR; FERMI BLAZARS; SKY SURVEY; TELESCOPE AB B2 1023+ 25 is an extremely radio-loud quasar at z = 5.3 that was first identified as a likely high-redshift blazar candidate in the SDSS+ FIRST quasar catalog. Here, we use the Nuclear Spectroscopic Telescope Array (NuSTAR) to investigate its non-thermal jet emission, whose high-energy component we detected in the hard X-ray energy band. The X-ray flux is similar to 5.5 x 10(-14) erg cm(-2) s(-1) (5-10 keV) and the photon spectral index is Gamma(X) similar or equal to 1.3-1.6. Modeling the full spectral energy distribution, we find that the jet is oriented close to the line of sight, with a viewing angle of similar to 3 degrees, and has significant Doppler boosting, with a large bulk Lorentz factor similar to 13, which confirms the identification of B2 1023+ 25 as a blazar. B2 1023+ 25 is the first object at redshift larger than 5 detected by NuSTAR, demonstrating the ability of NuSTAR to investigate the early X-ray universe and to study extremely active supermassive black holes located at very high redshift. C1 [Sbarrato, T.] Univ Insubria, Dipartimento Sci & Alta Tecnol, I-22100 Como, Italy. [Sbarrato, T.; Tagliaferri, G.; Ghisellini, G.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Perri, M.; Puccetti, S.; Giommi, P.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Perri, M.; Puccetti, S.; Giommi, P.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Balokovic, M.; Harrison, F. A.; Hovatta, T.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Nardini, M.] Univ Milano Bicocca, Dipartimento Fis G Occhialini, I-20126 Milan, Italy. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Christensen, F. E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Greiner, J.; Rau, A.; Schady, P.; Sudilovsky, V.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Madejski, G. M.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Urry, C. M.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sbarrato, T (reprint author), Univ Insubria, Dipartimento Sci & Alta Tecnol, Via Valleggio 11, I-22100 Como, Italy. EM tullia.sbarrato@brera.inaf.it RI Urry, Claudia/G-7381-2011; Boggs, Steven/E-4170-2015; Brandt, William/N-2844-2015; OI Tagliaferri, Gianpiero/0000-0003-0121-0723; Puccetti, Simonetta/0000-0002-2734-7835; Urry, Claudia/0000-0002-0745-9792; Boggs, Steven/0000-0001-9567-4224; Brandt, William/0000-0002-0167-2453; giommi, paolo/0000-0002-2265-5003; Perri, Matteo/0000-0003-3613-4409; Ghisellini, Gabriele/0000-0002-0037-1974; Sbarrato, Tullia/0000-0002-3069-9399 FU ASI-INAF grant [I/037/12/0]; NASA [NNG08FD60C]; National Aeronautics and Space Administration; DFG [HA 1850/28-1]; National Science Foundation; International Fulbright Science and Technology Award FX We thank the anonymous referee for useful comments. We acknowledge financial support from the ASI-INAF grant I/037/12/0. 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 also use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). The scientific results reported in this article are based in part on observations made by the Chandra X-ray Observatory and published previously in cited articles. 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. Part of this work is based on archival data, software, or on-line services provided by the ASDC. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASDC, Italy. Part of the funding for GROND (both hardware as well as personnel) was generously granted from the Leibniz Prize to Professor G. Hasinger (DFG grant HA 1850/28-1). 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 operation of the OVRO 40 m telescope is supported by NASA awards NNX08AW31G and NNX11AO43G and NSF awards AST-0808050 and AST-1109911. M. B. acknowledges support from an International Fulbright Science and Technology Award. NR 46 TC 15 Z9 15 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 NOV 10 PY 2013 VL 777 IS 2 AR 147 DI 10.1088/0004-637X/777/2/147 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800066 ER PT J AU Brown, TM Landsman, WB Randall, SK Sweigart, AV Lanz, T AF Brown, Thomas M. Landsman, Wayne B. Randall, Suzanna K. Sweigart, Allen V. Lanz, Thierry TI THE DISCOVERY OF PULSATING HOT SUBDWARFS IN NGC 2808 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE globular clusters: individual (NGC 2808); stars: horizontal-branch; stars: oscillations; ultraviolet: stars ID HORIZONTAL-BRANCH STARS; CLUSTER OMEGA-CENTAURI; DOUBLE MAIN-SEQUENCE; DWARF COOLING CURVE; GLOBULAR-CLUSTERS; B-STARS; ELLIPTIC GALAXIES; CLOSE BINARIES; MASS-LOSS; ORIGIN AB We present the results of a Hubble Space Telescope program to search for pulsating hot subdwarfs in the core of NGC 2808. These observations were motivated by the recent discovery of such stars in the outskirts of omega Cen. Both NGC 2808 and omega Cen are massive globular clusters exhibiting complex stellar populations and large numbers of extreme horizontal branch stars. Our far-UV photometric monitoring of over 100 hot evolved stars has revealed six pulsating subdwarfs with periods ranging from 85 to 149 s and UV amplitudes of 2.0%-6.8%. In the UV color-magnitude diagram of NGC 2808, all six of these stars lie immediately below the canonical horizontal branch, a region populated by the subluminous "blue-hook" stars. For three of these six pulsators, we also have low-resolution far-UV spectroscopy that is sufficient to broadly constrain their atmospheric abundances and effective temperatures. Curiously, and in contrast to the omega Cen pulsators, the NGC 2808 pulsators do not exhibit the spectroscopic or photometric uniformity one might expect from a well-defined instability strip, although they all fall within a narrow band (0.2 mag) of far-UV luminosity. C1 [Brown, Thomas M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Landsman, Wayne B.; Sweigart, Allen V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Randall, Suzanna K.] European So Observ, D-85748 Garching, Germany. [Lanz, Thierry] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR7293, F-06304 Nice, France. RP Brown, TM (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM tbrown@stsci.edu; Wayne.Landsman@nasa.gov; srandall@eso.org; allen.sweigart@gmail.com; Thierry.Lanz@oca.eu OI Brown, Thomas/0000-0002-1793-9968 FU NASA through STScI [12954]; NASA [NAS 5-26555] FX Support for Program 12954 was provided by NASA through a grant from STScI, which is operated by AURA, Inc., under NASA contract NAS 5-26555. The authors are grateful to Marc Rafelski, who graciously used his software to calculate the orbital variation in the Sun and target limb angles for the planned observation date, so that we could confirm the observing window would not suffer from unusually high O I emission. NR 41 TC 4 Z9 4 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 10 PY 2013 VL 777 IS 2 AR L22 DI 10.1088/2041-8205/777/2/L22 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242TY UT WOS:000326266500004 ER PT J AU Moor, A Juhasz, A Kospal, A Abraham, P Apai, D Csengeri, T Grady, C Henning, T Hughes, AM Kiss, C Pascucci, I Schmalzl, M Gabanyi, K AF Moor, A. Juhasz, A. Kospal, A. Abraham, P. Apai, D. Csengeri, T. Grady, C. Henning, Th. Hughes, A. M. Kiss, Cs. Pascucci, I. Schmalzl, M. Gabanyi, K. TI ALMA CONTINUUM OBSERVATIONS OF A 30 Myr OLD GASEOUS DEBRIS DISK AROUND HD 21997 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; infrared: stars; stars: individual (HD 21997) ID MOLECULAR GAS; CIRCUMSTELLAR DISK; PLANET FORMATION; BETA-PICTORIS; TW HYDRAE; DUST; STARS; PERFORMANCE; EVOLUTION; MISSION AB Circumstellar disks around stars older than 10 Myr are expected to be gas-poor. There are, however, two examples of old (30-40 Myr) debris-like disks containing a detectable amount of cold CO gas. Here we present Atacama Large Millimeter/Submillimeter Array (ALMA) and Herschel Space Observatory observations of one of these disks, around HD 21997, and study the distribution and origin of the dust and its connection to the gas. Our ALMA continuum images at 886 mu m clearly resolve a broad ring of emission within a diameter of similar to 4 ''.5, adding HD 21997 to the dozen debris disks resolved at (sub) millimeter wavelengths. Modeling the morphology of the ALMA image with a radiative transfer code suggests inner and outer radii of similar to 55 and similar to 150 AU, and a dust mass of 0.09 M-circle plus. Our data and modeling hints at an extended cold outskirt of the ring. Comparison with the morphology of the CO gas in the disk reveals an inner dust-free hole where gas nevertheless can be detected. Based on dust grain lifetimes, we propose that the dust content of this gaseous disk is of secondary origin and is produced by planetesimals. Since the gas component is probably primordial, HD 21997 is one of the first known examples of a hybrid circumstellar disk, a thus-far little studied late phase of circumstellar disk evolution. C1 [Moor, A.; Abraham, P.; Kiss, Cs.; Gabanyi, K.] Hungarian Acad Sci, Konkoly Observ, Res Ctr Astron & Earth Sci, H-1525 Budapest, Hungary. [Juhasz, A.; Schmalzl, M.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands. [Kospal, A.] SRE SA, European Space Agcy ESA ESTEC, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. [Apai, D.; Pascucci, I.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Apai, D.; Pascucci, I.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Csengeri, T.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Grady, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Grady, C.] Eureka Sci, Oakland, CA 94602 USA. [Henning, Th.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Hughes, A. M.] Wesleyan Univ, Dept Astron, Van Vleck Observ, Middletown, CT 06457 USA. RP Moor, A (reprint author), Hungarian Acad Sci, Konkoly Observ, Res Ctr Astron & Earth Sci, POB 67, H-1525 Budapest, Hungary. EM moor@konkoly.hu FU Hungarian OTKA [K101393/K104607, NN102014]; European Space Agency (ESA) [PECS-98073]; Bolyai Fellowship FX We thank our anonymous referee whose comments improved the manuscript. This Letter makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00780. S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This research was partly funded by the Hungarian OTKA grants K101393/K104607 and the PECS-98073 program of the European Space Agency (ESA). A. M. and C. K. acknowledge the support of the Bolyai Fellowship. K. G. acknowledges support from the Hungarian OTKA grant NN102014. NR 34 TC 16 Z9 16 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 10 PY 2013 VL 777 IS 2 AR L25 DI 10.1088/2041-8205/777/2/L25 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242TY UT WOS:000326266500007 ER PT J AU Williams, SC Bode, MF Darnley, MJ Evans, A Zubko, V Shafter, AW AF Williams, S. C. Bode, M. F. Darnley, M. J. Evans, A. Zubko, V. Shafter, A. W. TI RAPID DUST FORMATION IN NOVAE: THE SPEED CLASS-FORMATION TIMESCALE CORRELATION EXPLAINED SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE novae, cataclysmic variables ID INFRARED-SPECTROSCOPY; CASSIOPEIAE 1993; CO EMISSION; MAXIMUM; NUCLEOSYNTHESIS; PHASE; M31 AB Observations show that the time of onset of dust formation in classical novae depends strongly on their speed class, with dust typically taking longer to form in slower novae. Using empirical relationships between speed class, luminosity and ejection velocity, it can be shown that dust formation timescale is expected to be essentially independent of speed class. However, following a nova outburst the spectrum of the central hot source evolves, with an increasing proportion of the radiation being emitted short-ward of the Lyman limit. The rate at which the spectrum evolves also depends on the speed class. We have therefore refined the simple model by assuming photons at energies higher than the Lyman limit are absorbed by neutral hydrogen gas internal to the dust formation sites, therefore preventing these photons reaching the nucleation sites. With this refinement the dust formation timescale is theoretically dependent on speed class and the results of our theoretical modification agree well with the observational data. We consider two types of carbon-based dust, graphite and amorphous carbon, with both types producing similar relationships. Our results can be used to predict when dust will form in a nova of a given speed class and hence when observations should optimally be taken to detect the onset of dust formation. C1 [Williams, S. C.; Bode, M. F.; Darnley, M. J.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Evans, A.] Keele Univ, Lennard Jones Lab, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Zubko, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Shafter, A. W.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. RP Williams, SC (reprint author), Liverpool John Moores Univ, Astrophys Res Inst, IC2,Liverpool Sci Pk,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England. EM S.C.Williams@2010.ljmu.ac.uk OI Williams, Steven/0000-0001-8178-0202 FU STFC; NSF [AST-1009566] FX S.C.W. is supported by an STFC research studentship. A. W. S. is grateful for financial support through NSF grant AST-1009566. We thank an anonymous referee for valuable comments on the initial submitted version of this Letter. NR 35 TC 2 Z9 2 U1 0 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 NOV 10 PY 2013 VL 777 IS 2 AR L32 DI 10.1088/2041-8205/777/2/L32 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242TY UT WOS:000326266500014 ER PT J AU Miljkovic, K Wieczorek, MA Collins, GS Laneuville, M Neumann, GA Melosh, HJ Solomon, SC Phillips, RJ Smith, DE Zuber, MT AF Miljkovic, Katarina Wieczorek, Mark A. Collins, Gareth S. Laneuville, Matthieu Neumann, Gregory A. Melosh, H. Jay Solomon, Sean C. Phillips, Roger J. Smith, David E. Zuber, Maria T. TI Asymmetric Distribution of Lunar Impact Basins Caused by Variations in Target Properties SO SCIENCE LA English DT Article ID INNER SOLAR-SYSTEM; MOON; EVOLUTION; ORIGIN; CRUST; DEFORMATION; SIMULATIONS; BOMBARDMENT; CHRONOLOGY; SURFACE AB Maps of crustal thickness derived from NASA's Gravity Recovery and Interior Laboratory (GRAIL) mission revealed more large impact basins on the nearside hemisphere of the Moon than on its farside. The enrichment in heat-producing elements and prolonged volcanic activity on the lunar nearside hemisphere indicate that the temperature of the nearside crust and upper mantle was hotter than that of the farside at the time of basin formation. Using the iSALE-2D hydrocode to model impact basin formation, we found that impacts on the hotter nearside would have formed basins with up to twice the diameter of similar impacts on the cooler farside hemisphere. The size distribution of lunar impact basins is thus not representative of the earliest inner solar system impact bombardment. C1 [Miljkovic, Katarina; Wieczorek, Mark A.; Laneuville, Matthieu] Univ Paris Diderot, Inst Phys Globe Paris, Sorbonne Paris Cite, F-75205 Paris 13, France. [Collins, Gareth S.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London SW7 2AZ, England. [Neumann, Gregory A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Melosh, H. Jay] Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Phillips, Roger J.] SW Res Inst, Planetary Sci Directorate, Boulder, CO 80302 USA. [Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. RP Miljkovic, K (reprint author), Univ Paris Diderot, Inst Phys Globe Paris, Sorbonne Paris Cite, Case 7011,Lamarck A 5,35 Rue Helene Brion, F-75205 Paris 13, France. EM miljkovic@ipgp.fr RI Wieczorek, Mark/G-6427-2010; Miljkovic, Katarina/D-4844-2013; Neumann, Gregory/I-5591-2013; Laneuville, Matthieu/F-8523-2010; OI Wieczorek, Mark/0000-0001-7007-4222; Miljkovic, Katarina/0000-0001-8644-8903; Neumann, Gregory/0000-0003-0644-9944; Laneuville, Matthieu/0000-0001-6022-0046; Collins, Gareth/0000-0002-6087-6149 FU UnivEarthS LabEx project of the University of Sorbonne Paris Cite [ANR-10-LABX-0023, ANR-11-IDEX-0005-02]; UK Science & Technology Facilities Council [ST/J001260/1]; French Space Agency (CNES); Discovery Program of NASA FX Supported by UnivEarthS LabEx project of the University of Sorbonne Paris Cite grants ANR-10-LABX-0023 and ANR-11-IDEX-0005-02 (K.M.), UK Science & Technology Facilities Council grant ST/J001260/1 (G.S.C.), and the French Space Agency (CNES). The GRAIL mission is supported by the Discovery Program of NASA and is performed under contract to the Massachusetts Institute of Technology and the Jet Propulsion Laboratory, California Institute of Technology. We gratefully acknowledge the developers of iSALE-2D/3D (www.isale-code.de). NR 32 TC 25 Z9 25 U1 3 U2 21 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 NOV 8 PY 2013 VL 342 IS 6159 BP 724 EP 726 DI 10.1126/science.1243224 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 247UK UT WOS:000326647600039 PM 24202170 ER PT J AU Bera, PP Head-Gordon, M Lee, TJ AF Bera, Partha P. Head-Gordon, Martin Lee, Timothy J. TI Relative energies, structures, vibrational frequencies, and electronic spectra of pyrylium cation, an oxygen-containing carbocyclic ring isoelectronic with benzene, and its isomers SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID BASIS-SETS; CHEMISTRY; DENSITY; OXIDATION; KINETICS; IONS AB We have studied relative energies, structures, rotational, vibrational, and electronic spectra of the pyrylium cation, an oxygen-containing six-membered carbocyclic ring, and its six isomers, using ab initio quantum chemical methods. Isoelectronic with benzene, the pyrylium cation has a benzenoid structure and is the global minimum on the singlet potential energy surface of C5H5O+. The second lowest energy isomer, the furfuryl cation, has a five membered backbone akin to a sugar, and is only 16 kcal mol(-1) above the global minimum computed using coupled cluster theory with singles, doubles, and perturbative triple excitations (CCSD(T)) with the correlation consistent cc-pVTZ basis set. Other isomers are 25, 26, 37, 60, and 65 kcal mol(-1) above the global minimum, respectively, at the same level of theory. Lower level methods such as density functional theory (B3LYP) and second order Moller-Plesset perturbation theory performed well when tested against the CCSD(T) results. The pyrylium and furfuryl cations, although separated by only 16 kcal mol(-1), are not easily interconverted, as multiple bonds must be broken and formed, and the existence of more than one transition state is likely. Additionally, we have also investigated the asymptotes for the barrierless ion-molecule association of molecules known to exist in the interstellar medium that may lead to formation of the pyrylium cation. (C) 2013 AIP Publishing LLC. C1 [Bera, Partha P.; Lee, Timothy J.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. [Head-Gordon, Martin] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA. [Head-Gordon, Martin] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Chem Sci, Berkeley, CA 94720 USA. RP Lee, TJ (reprint author), NASA, Ames Res Ctr, MS 245-1, Mountain View, CA 94035 USA. EM Timothy.J.Lee@nasa.gov RI Lee, Timothy/K-2838-2012; Bera, Partha /K-8677-2012 FU NASA [10-APRA10-167]; NASA Laboratory astrophysics "Carbon in the Galaxy" consortium grant [NNH10ZDA001N]; BAER Institute FX P.P.B. would like the thank Dr. Xinchuan Huang for helpful discussions. The authors gratefully acknowledge support from the NASA grant 10-APRA10-167, and NASA Laboratory astrophysics "Carbon in the Galaxy" consortium grant (NNH10ZDA001N). P. P. B. is also thankful to BAER Institute for their support. NR 28 TC 2 Z9 2 U1 0 U2 12 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD NOV 7 PY 2013 VL 139 IS 17 AR 174302 DI 10.1063/1.4826138 PG 9 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 251IT UT WOS:000326922300016 PM 24206293 ER PT J AU Qi, TT Bauschlicher, CW Lawson, JW Desai, TG Reed, EJ AF Qi, Tingting Bauschlicher, Charles W., Jr. Lawson, John W. Desai, Tapan G. Reed, Evan J. TI Comparison of ReaxFF, DFTB, and DFT for Phenolic Pyrolysis. 1. Molecular Dynamics Simulations SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID REACTIVE FORCE-FIELD; CARBON/PHENOLIC COMPOSITE; RESIN; CARBONIZATION; SOLIDS; ATOMS AB A systematic comparison of atomistic modeling methods including density functional theory (DFT), the self-consistent charge density-functional tight-binding (SCC-DFTB), and ReaxFF is presented for simulating the initial stages of phenolic polymer pyrolysis. A phenolic polymer system is simulated for several hundred picoseconds within a temperature range of 2500 to 3500 K. The time evolution of major pyrolysis products including small-molecule species and char is examined. Two temperature zones are observed which demark cross-linking versus fragmentation. The dominant chemical products for all methods are similar, but the yields for each product differ. At 3500 K, DFTB overestimates CO production (300-400%) and underestimates free H (similar to 30%) and small CmHnO molecules (similar to 70%) compared with DFT. At 3500 K, ReaxFF underestimates free H (similar to 60%) and fused carbon rings (similar to 70%) relative to DFT. Heterocyclic oxygen-containing five- and six-membered carbon rings are observed at 2500 K. Formation mechanisms for H2O, CO, and char are discussed. Additional calculations using a semiclassical method for incorporating quantum nuclear energies of molecules were also performed. These results suggest that chemical equilibrium can be affected by quantum nuclear effects at temperatures of 2500 K and below. Pyrolysis reaction mechanisms and energetics are examined in detail in a companion manuscript. C1 [Qi, Tingting; Reed, Evan J.] Stanford Univ, Dept Mat Sci & Engn, Stanford, CA 94305 USA. [Bauschlicher, Charles W., Jr.] NASA, Entry Syst & Technol Div, Ames Res Ctr, Moffett Field, CA 94035 USA. [Lawson, John W.] NASA, Thermal Protect Mat Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. [Desai, Tapan G.] Adv Cooling Technol Inc, Lancaster, PA 17601 USA. RP Lawson, JW (reprint author), NASA, Thermal Protect Mat Branch, Ames Res Ctr, Mail Stop 234, Moffett Field, CA 94035 USA. EM john.w.lawson@nasa.gov; evanreed@stanford.edu FU NASA Ames Center Innovation Fund FX This work was supported by a NASA Ames Center Innovation Fund grant. We also gratefully acknowledge the computational resources from the National Energy Research Scientific Computing Center (NERSC) and the Stanford NNIN Computing Facility (SNCF). NR 24 TC 26 Z9 26 U1 6 U2 81 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 NOV 7 PY 2013 VL 117 IS 44 BP 11115 EP 11125 DI 10.1021/jp4081096 PG 11 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 250ID UT WOS:000326845300001 PM 24094313 ER PT J AU Bauschlicher, CW Qi, TT Reed, EJ Lenfant, A Lawson, JW Desai, TG AF Bauschlicher, Charles W., Jr. Qi, Tingting Reed, Evan J. Lenfant, Antonin Lawson, John W. Desai, Tapan G. TI Comparison of ReaxFF, DFTB, and DFT for Phenolic Pyrolysis. 2. Elementary Reaction Paths SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID MOLECULAR-DYNAMICS SIMULATIONS; GAUSSIAN-BASIS SETS; ELECTRON CORRELATION; FORCE-FIELD; EXCHANGE; ATOMS AB Reaction paths for the loss of CO, H-2, and H2O from atomistic models of phenolic resin are determined using the hybrid B3LYP approach. B3LYP energetics are confirmed using CCSD(T). The energetics along the B3LYP paths are also evaluated using the PW91 generalized gradient approximation (GGA), the more approximate self-consistent charge density functional tight binding (SCC-DFTB), and the reactive force field (ReaxFF). Compared with the CCSD(T)/cc-pVTZ level for bond and reaction energies and barrier heights, the B3LYP, PW91, DFTB(mio), DFTB(pbc), and ReaxFF have average absolute errors of 3.8, 5.1, 17.4, 13.2, and 19.6 kcal/mol, respectively. The PW91 is only slightly less accurate than the B3LYP approach, while the more approximate approaches yield somewhat larger errors. The SCC-DFTB paths are in better agreement with B3LYP than are those obtained with ReaxFF. C1 [Bauschlicher, Charles W., Jr.] NASA, Entry Syst & Technol Div, Ames Res Ctr, Moffett Field, CA 94035 USA. [Qi, Tingting; Reed, Evan J.; Lenfant, Antonin] Stanford Univ, Dept Mat Sci & Engn, Stanford, CA 94305 USA. [Lenfant, Antonin] Inst Super Elect Paris, Dept Comp Sci, F-75006 Paris, France. [Lawson, John W.] NASA, Thermal Protect Mat Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. [Desai, Tapan G.] Adv Cooling Technol Inc, Lancaster, PA 17601 USA. RP Bauschlicher, CW (reprint author), NASA, Entry Syst & Technol Div, Ames Res Ctr, Mail Stop 230-3, Moffett Field, CA 94035 USA. EM charles.w.bauschlicher@nasa.gov FU Ames Center Innovation Fund FX This work was partly supported by the Ames Center Innovation Fund. NR 16 TC 11 Z9 11 U1 9 U2 46 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 NOV 7 PY 2013 VL 117 IS 44 BP 11126 EP 11135 DI 10.1021/jp406786a PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 250ID UT WOS:000326845300002 PM 24093151 ER PT J AU Fortenberry, RC Crawford, TD Lee, TJ AF Fortenberry, Ryan C. Crawford, T. Daniel Lee, Timothy J. TI Vibrational Frequencies and Spectroscopic Constants for 1 (3)A ' HNC and 1 (3)A ' HOC plus from High-Accuracy Quartic Force Fields SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID SHELL HARTREE-FOCK; ABUNDANCE RATIO; WAVE-FUNCTIONS; BASIS-SETS; MOLECULES; ENERGIES; HYDROGEN; HCN; GRADIENTS; CLOUDS AB The spectroscopic constants and vibrational frequencies for the 1 (3)A' states of HNC, DNC, HOC+, and DOC+ are computed and discussed in this work. The reliable CcCR quartic force field based on high-level coupled cluster ab initio quantum chemical computations is exclusively utilized to provide the anharmonic potential. Then, second-order vibrational perturbation theory and vibrational configuration interaction methods are employed to treat the nuclear Schrodinger equation. Second-order perturbation theory is also employed to provide spectroscopic data for all molecules examined. The relationship between these molecules and the corresponding 1 (3)A' HCN and HCO+ isomers is further developed here. These data are applicable to laboratory studies involving formation of HNC and HOC+ as well as astronomical observations of chemically active astrophysical environments. C1 [Fortenberry, Ryan C.] Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA. [Fortenberry, Ryan C.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Crawford, T. Daniel] Virginia Tech, Dept Chem, Blacksburg, VA 24061 USA. RP Fortenberry, RC (reprint author), Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA. EM rfortenberry@georgiasouthern.edu; Timothy.J.Lee@nasa.gov RI Lee, Timothy/K-2838-2012; Crawford, Thomas/A-9271-2017 OI Crawford, Thomas/0000-0002-7961-7016 FU R.C.F; National Science Foundation (NSF) Multi-User Chemistry Research Instrumentation and Facility (CRIF:MU) Award; NSF [CHE-1058420]; NASA [10-APRA10-0167]; NASA's Laboratory Astrophysics 'Carbon in the Galaxy' Consortium [NNH1OZDA001N] FX The NASA Postdoctoral Program administered by Oak Ridge Associated Universities through a contract with NASA as well as funds provided by Georgia Southern University financially supported the work done by R.C.F. The National Science Foundation (NSF) Multi-User Chemistry Research Instrumentation and Facility (CRIF:MU) Award CHE-0741927 provided the necessary computer hardware employed in this work. T.D.C. and R.C.F. gratefully acknowledge this support. Additionally, T.D.C. received NSF Award CHE-1058420 and is thankful for this support. T.J.L. was funded by NASA Grant 10-APRA10-0167. T.J.L. and R.C.F. also acknowledge support from NASA's Laboratory Astrophysics 'Carbon in the Galaxy' Consortium Grant (NNH1OZDA001N). Creation of the figures employed the CheMVP program developed at the University of Georgia's Center for Computational Quantum Chemistry. NR 50 TC 6 Z9 6 U1 1 U2 13 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 NOV 7 PY 2013 VL 117 IS 44 BP 11339 EP 11345 DI 10.1021/jp408750 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 250ID UT WOS:000326845300025 PM 24102307 ER PT J AU Bielefeld, J Wu, WLK Caldwell, RR Dore, O AF Bielefeld, Jannis Wu, W. L. Kimmy Caldwell, Robert R. Dore, Olivier TI Freezing out early dark energy SO PHYSICAL REVIEW D LA English DT Article ID MICROWAVE BACKGROUND ANISOTROPIES; HUBBLE-SPACE-TELESCOPE; SOUTH-POLE TELESCOPE; COSMOLOGICAL CONSTANT; COSMIC COINCIDENCE; QUINTESSENCE; MODELS; LIGHT; PROBE AB A phenomenological model of dark energy that tracks the baryonic and cold dark matter at early times but resembles a cosmological constant at late times is explored. In the transition between these two regimes, the dark energy density drops rapidly as if it were a relic species that freezes out, during which time the equation of state peaks at +1. Such an adjustment in the dark energy density, as it shifts from scaling to potential domination, could be the signature of a trigger mechanism that helps explain the late-time cosmic acceleration. We show that the non-negligible dark energy density at early times, and the subsequent peak in the equation of state at the transition, leave an imprint on the cosmic microwave background anisotropy pattern and the rate of growth of large scale structure. The model introduces two new parameters, consisting of the present-day equation of state and the redshift of the freeze-out transition. A Monte Carlo Markov chain analysis of a ten-dimensional parameter space is performed to compare the model with pre-Planck cosmic microwave background, large scale structure and supernova data and measurements of the Hubble constant. We find that the transition described by this model could have taken place as late as a redshift z similar to 250. We explore the capability of future cosmic microwave background and weak lensing experiments to put tighter constraints on this model. The viability of this model may suggest new directions in dark-energy model building that address the coincidence problem. C1 [Bielefeld, Jannis; Caldwell, Robert R.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Wu, W. L. Kimmy] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Wu, W. L. Kimmy] Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Dore, Olivier] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA. [Dore, Olivier] CALTECH, Pasadena, CA 91125 USA. RP Bielefeld, J (reprint author), Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. OI Caldwell, Robert/0000-0001-7490-7463 FU JPL Strategic University Research Partnership (SURP) Program; Keck Institute of Space Studies; Stanford Graduate Fellowship FX This research was carried out in part at the Jet Propulsion Laboratory, run by the California Institute of Technology under a contract from NASA, and Dartmouth College and was funded through the JPL Strategic University Research Partnership (SURP) Program. Part of this work was supported by the Keck Institute of Space Studies and we thank colleagues at the "CMB Polarization Cosmology in the Coming Decade" for stimulating discussions. W. L. K. W. acknowledges support from a Stanford Graduate Fellowship. NR 59 TC 4 Z9 4 U1 0 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD NOV 7 PY 2013 VL 88 IS 10 AR 103004 DI 10.1103/PhysRevD.88.103004 PG 11 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 250CS UT WOS:000326828400002 ER PT J AU Wei, CY Pohorille, A AF Wei, Chenyu Pohorille, Andrew TI Activation and Proton Transport Mechanism in Influenza A M2 Channel SO BIOPHYSICAL JOURNAL LA English DT Article ID MOLECULAR-DYNAMICS SIMULATION; M-2 ION-CHANNEL; SOLID-STATE NMR; PH-DEPENDENT CONFORMATION; VIRUS M2; TRANSMEMBRANE DOMAIN; CONDUCTION MECHANISM; AROMATIC INTERACTION; TRYPTOPHAN RESIDUE; AMANTADINE BINDING AB Molecular dynamics trajectories 2 mu s in length have been generated for the pH-activated, tetrameric M2 proton channel of the influenza A virus in all protonation states of the pH sensor located at the His(37) tetrad. All simulated structures are in very good agreement with high-resolution structures. Changes in the channel caused by progressive protonation of His(37) provide insight into the mechanism of proton transport. The channel is closed at both His(37) and Trp(41) sites in the singly and doubly protonated states, but it opens at Trp(41) upon further protonation. Anions access the charged His(37) and by doing so stabilize the protonated states of the channel. The narrow opening at the His(37) site, further blocked by anions, is inconsistent with the water-wire mechanism of proton transport. Instead, conformational interconversions of His(37) correlated with hydrogen bonding to water molecules indicate that these residues shuttle protons in high-protonation states. Hydrogen bonds between charged and uncharged histidines are rare. The valve at Val(27) remains on average quite narrow in all protonation states but fluctuates sufficiently to support water and proton transport. A proton transport mechanism in which the channel, depending on pH, opens at either the histidine or valine gate is only partially supported by the simulations. C1 [Wei, Chenyu; Pohorille, Andrew] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Wei, Chenyu; Pohorille, Andrew] Univ Calif San Francisco, Dept Pharmaceut Chem, San Francisco, CA USA. RP Wei, CY (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM chenyu.wei@nasa.gov; andrew.pohorille@nasa.gov FU NASA Exobiology Program FX This work was supported by the NASA Exobiology Program. NR 72 TC 15 Z9 15 U1 2 U2 21 PU CELL PRESS PI CAMBRIDGE PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA SN 0006-3495 EI 1542-0086 J9 BIOPHYS J JI Biophys. J. PD NOV 5 PY 2013 VL 105 IS 9 BP 2036 EP 2045 DI 10.1016/j.bpj.2013.08.030 PG 10 WC Biophysics SC Biophysics GA 250NB UT WOS:000326858400013 PM 24209848 ER PT J AU Van Doornik, DM Berejikian, BA Campbell, LA AF Van Doornik, Donald M. Berejikian, Barry A. Campbell, Lance A. TI Gene Flow between Sympatric Life History Forms of Oncorhynchus mykiss Located above and below Migratory Barriers SO PLOS ONE LA English DT Article ID CROSS-SPECIES AMPLIFICATION; RESIDENT RAINBOW-TROUT; FRESH-WATER; POPULATION-STRUCTURE; MICROSATELLITE LOCI; STEELHEAD TROUT; OTOLITH MICROCHEMISTRY; ANADROMOUS STEELHEAD; REPRODUCTIVE SUCCESS; HATCHERY PROGRAMS AB Oncorhynchus mykiss have a diverse array of life history types, and understanding the relationship among types is important for management of the species. Patterns of gene flow between sympatric freshwater resident O. mykiss, commonly known as rainbow trout, and anadromous O. mykiss, commonly known as steelhead, populations are complex and poorly understood. In this study, we attempt to determine the occurrence and pathways of gene flow and the degree of genetic similarity between sympatric resident and anadromous O. mykiss in three river systems, and investigate whether resident O. mykiss are producing anadromous offspring in these rivers, two of which have complete barriers to upstream migration. We found that the population structure of the O. mykiss in these rivers appears to be influenced more by the presence of a barrier to upstream migration than by life history type. The sex ratio of resident O. mykiss located above a barrier, and smolts captured in screw traps was significantly skewed in favor of females, whereas the reverse was true below the barriers, suggesting that male resident O. mykiss readily migrate downstream over the barrier, and that precocious male maturation may be occurring in the anadromous populations. Through paternity analyses, we also provide direct confirmation that resident O. mykiss can produce offspring that become anadromous. Most (89%) of the resident O. mykiss that produced anadromous offspring were males. Our results add to the growing body of evidence that shows that gene flow does readily occur between sympatric resident and anadromous O. mykiss life history types, and indicates that resident O. mykiss populations may be a potential repository of genes for the anadromous life history type. C1 [Van Doornik, Donald M.; Berejikian, Barry A.] NOAA, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Manchester, WA 98353 USA. [Campbell, Lance A.] Washington Dept Fish & Wildlife, Olympia, WA USA. RP Van Doornik, DM (reprint author), NOAA, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Manchester, WA 98353 USA. EM don.vandoornik@noaa.gov FU National Oceanic and Atmospheric Administration; Hood Canal Salmon Enhancement Group, Long Live the Kings; Skokomish Tribal Nation; U.S. Fish and Wildlife Service; Washington Department of Fish and Wildlife FX Primary funding for this work was provided by the National Oceanic and Atmospheric Administration. Additional support was provided by the Hood Canal Salmon Enhancement Group, Long Live the Kings, the Skokomish Tribal Nation, the U.S. Fish and Wildlife Service, and the Washington Department of Fish and Wildlife. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 69 TC 5 Z9 5 U1 3 U2 19 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 NOV 5 PY 2013 VL 8 IS 11 AR e79931 DI 10.1371/journal.pone.0079931 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 247EE UT WOS:000326597400096 PM 24224023 ER PT J AU Aides, A Schechner, YY Holodovsky, V Garay, MJ Davis, AB AF Aides, Amit Schechner, Yoav Y. Holodovsky, Vadim Garay, Michael J. Davis, Anthony B. TI Multi sky-view 3D aerosol distribution recovery SO OPTICS EXPRESS LA English DT Article AB Aerosols affect climate, health and aviation. Currently, their retrieval assumes a plane-parallel atmosphere and solely vertical radiative transfer. We propose a principle to estimate the aerosol distribution as it really is: a three dimensional (3D) volume. The principle is a type of tomography. The process involves wide angle integral imaging of the sky on a very large scale. The imaging can use an array of cameras in visible light. We formulate an image formation model based on 3D radiative transfer. Model inversion is done using optimization methods, exploiting a closed-form gradient which we derive for the model-fit cost function. The tomography model is distinct, as the radiation source is unidirectional and uncontrolled, while off-axis scattering dominates the images. (c) 2013 Optical Society of America C1 [Aides, Amit; Schechner, Yoav Y.; Holodovsky, Vadim] Technion Israel Inst Technol, Dept Elect Engn, IL-32000 Haifa, Israel. [Garay, Michael J.; Davis, Anthony B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Aides, A (reprint author), Technion Israel Inst Technol, Dept Elect Engn, IL-32000 Haifa, Israel. EM amitibo@tx.technion.ac.il FU Taub Foundation; US-Israel Binational Science Foundation (BSF) [2012202]; BMBF; NASA's Earth Science Technology Office Advanced Information Systems Technology Program FX We are grateful to David J. Diner for fruitful discussions and his support at all levels. We thank the reviewers for useful comments. Yoav Schechner is a Landau Fellow - supported by the Taub Foundation. This work is supported by the US-Israel Binational Science Foundation (BSF grant 2012202) and conducted in the Ollendorff Minerva Center. Minerva is funded through the BMBF. Part of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA and with support by NASA's Earth Science Technology Office Advanced Information Systems Technology Program. NR 26 TC 11 Z9 11 U1 1 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 NOV 4 PY 2013 VL 21 IS 22 BP 25820 EP 25833 DI 10.1364/OE.21.025820 PG 14 WC Optics SC Optics GA 252LZ UT WOS:000327007800043 PM 24216808 ER PT J AU Grudinin, IS Baumgartel, L Yu, N AF Grudinin, Ivan S. Baumgartel, Lukas Yu, Nan TI Impact of cavity spectrum on span in microresonator frequency combs SO OPTICS EXPRESS LA English DT Article ID GENERATION; DISPERSION; DYNAMICS; LASER AB We experimentally study the factors that limit the span in frequency combs derived from the crystalline whispering gallery mode resonators. We observe that cavity dispersion is the key property that governs the parameters of the combs resulting from cascaded four wave mixing process. Two different regimes of comb generation are observed depending on the precise cavity dispersion behavior at the pump wavelength. In addition, the comb generation efficiency is found to be affected by the crossing of modes of different families. The influence of Raman lasing and its dependence on temperature is discussed. (C) 2013 Optical Society of America C1 [Grudinin, Ivan S.; Baumgartel, Lukas; Yu, Nan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Baumgartel, Lukas] Univ So Calif, Los Angeles, CA 90089 USA. RP Grudinin, IS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM grudinin@jpl.nasa.gov NR 27 TC 25 Z9 25 U1 4 U2 27 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 NOV 4 PY 2013 VL 21 IS 22 BP 26929 EP 26935 DI 10.1364/OE.21.026929 PG 7 WC Optics SC Optics GA 252LZ UT WOS:000327007800150 PM 24216915 ER PT J AU Hoyt, DP AF Hoyt, Diana P. TI Culturematic SO RESEARCH-TECHNOLOGY MANAGEMENT LA English DT Book Review C1 [Hoyt, Diana P.] NASA, Off Chief Technologist, Washington, DC 20546 USA. RP Hoyt, DP (reprint author), NASA, Off Chief Technologist, Washington, DC 20546 USA. EM diana.hoyt@nasa.gov NR 1 TC 0 Z9 0 U1 0 U2 0 PU INDUSTRIAL RESEARCH INST, INC PI ARLINGTON PA 2200 CLARENDON BLVD, STE 1102, ARLINGTON, VA 22201 USA SN 0895-6308 EI 1930-0166 J9 RES TECHNOL MANAGE JI Res.-Technol. Manage. PD NOV-DEC PY 2013 VL 56 IS 6 BP 63 EP 64 PG 2 WC Business; Engineering, Industrial; Management SC Business & Economics; Engineering GA AI8XV UT WOS:000337211200015 ER PT J AU Evans, JM Mohney, L Wang, SQ Moore, RK Elayi, SC Stenger, MB Moore, FB Knapp, CF AF Evans, Joyce M. Mohney, Lindsay Wang, Siqi Moore, Rachel K. Elayi, Samy-Claude Stenger, Michael B. Moore, Fritz B. Knapp, Charles F. TI Cardiovascular Regulation During Body Unweighting by Lower Body Positive Pressure SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE blood pressure; stroke volume; body segment impedance; LBPP; alter-G; reduced gravity; spectral power; baroreflex ID HEART-RATE-VARIABILITY; NEGATIVE-PRESSURE; RESPONSES; BAROREFLEX; EXERCISE; REFLEXES; POSTURE; HUMANS; GENDER; REST AB Background: We hypothesized that human cardiovascular responses to standing in reduced gravity environments, as on the Moon or Mars, could be modeled using a lower body positive pressure (LBPP) chamber. Methods: Heart rate, blood pressure, body segment fluid shifts, ECG, indexes of sympathetic, parasympathetic balance, and baroreflex control of the heart and periphery plus echocardiographic measures of cardiac function were recorded from seven men and seven women supine and standing at 100% (Earth), 40% (similar to Mars), and 20% (similar to Moon) bodyweights (BW). Results: The fluid shifted from the chest was greater when standing at 100% BW than at 20% and 40% BW, while fluid pooled in the abdomen was similar at all BWs. Compared to moving from supine to standing at 100% BW, moving to 20% and 40% BW resulted in smaller decreases in stroke volume and pulse pressure, smaller increases in heart rate and smaller decreases in parasympathetic control of heart rate, baroreflex slope, numbers of blood pressure ramps, and much reduced indexes of sympathetic drive to the heart and periphery. However, peripheral vascular resistance, systolic pressure, and baroreflex effectiveness were elevated during 20% and 40% BW, compared to supine and standing at 100% BW. Discussion: Standing at reduced bodyweight suppressed indexes of sympathetic control of heart rate and peripheral vasomotion. Regulatory responses indicated a combination of arterial and cardiopulmonary baroreflex control: mean heart rate, vasomotion, and baroreflex sensitivity appeared to be more under cardiopulmonary control while baroreflex effectiveness appeared to be driven more by the arterial baroreflex. C1 [Evans, Joyce M.] Lake Erie Coll Osteopath Med, Bradenton, FL USA. [Wang, Siqi; Knapp, Charles F.] Univ Kentucky, Ctr Biomed Engn, Lexington, KY 40506 USA. [Elayi, Samy-Claude] Univ Kentucky, Lexington, KY 40506 USA. [Moore, Rachel K.] Georgia Inst Technol, Atlanta, GA 30332 USA. [Stenger, Michael B.] Wyle Sci Technol & Engn Grp, Houston, TX USA. [Moore, Fritz B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Evans, JM (reprint author), Univ Kentucky, Ctr Biomed Engn, Room 1, Lexington, KY 40506 USA. EM jevans1@uky.edu FU KY NASA EPSCoR [516204] FX The authors would like to acknowledge Tim Matz, Wyle Houston, for his skill in acquiring and analyzing ultrasound images of the heart and blood vessels. We also wish to thank Rebecca Schneider for study set up; Adam Lindstrom, of the UK SSTARS Center, who guided our statistical analysis; Dr. David Brown, Biomedical Engineering, University of Kentucky, who wrote the program for R wave detection; and Natalia Arzeno, NASA Johnson Space Center Cardiovascular Laboratory, who developed the software used for beat-to-beat analysis. This study was supported by KY NASA EPSCoR Grant 516204. NR 20 TC 4 Z9 4 U1 1 U2 4 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 EI 1943-4448 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD NOV PY 2013 VL 84 IS 11 BP 1140 EP 1146 DI 10.3357/ASEM.3576.2013 PG 7 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA AD1LY UT WOS:000332996700003 PM 24279226 ER PT J AU Reyes, DA Girimaji, SS Pandya, MJ Abdol-Hamid, KS AF Reyes, Dasia A. Girimaji, Sharath S. Pandya, Mohagna J. Abdol-Hamid, Khaled S. TI Computations of High-Lift Wing Configuration on Unstructured Grids Using k-omega Models SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT 49th AIAA Aerospace Sciences Meeting including the New Horizons Forum and Aerospace Exposition CY JAN 03-07, 2011 CL Orlando, FL SP AIAA ID AVERAGED NAVIER-STOKES; TURBULENCE MODEL; FLOWS; EQUATION AB Turbulent flow computations of the NASA "trap-wing" high-lift configuration are performed at various angles of attack using a k-omega family of models to assess their capabilities for high-lift design and optimization applications. The four k-omega model variants used are: 1) Wilcox's 1988 baseline model; 2) variable-beta* model consistent with the rapidly strained limit; 3) variable-beta* model consistent with the explicit algebraic Reynolds stress model; and 4) Wilcox's 2006 enhanced model. Subject to the conditions of this test, the variable-beta* model consistent with the rapidly strained limit not only performs the best but is also numerically more robust and does not require the use of a production-to-dissipation limiter. Overall, our findings indicate that variable-beta* makes an important difference. In the proximity of stall, a low-Reynolds-number correction to eddy viscosity may be needed to accurately capture experimental behavior. The results provide much needed insight into the models' predictive capabilities and identify areas for future k-omega model improvements. C1 [Reyes, Dasia A.; Girimaji, Sharath S.] Texas A&M Univ, College Stn, TX 77843 USA. [Pandya, Mohagna J.; Abdol-Hamid, Khaled S.] NASA, Langley Res Ctr, Configurat Aerodynam Branch, Hampton, VA 23681 USA. RP Reyes, DA (reprint author), Texas A&M Univ, Mail Stop 3141, College Stn, TX 77843 USA. NR 31 TC 0 Z9 0 U1 1 U2 5 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 NOV-DEC PY 2013 VL 50 IS 6 BP 1682 EP 1695 DI 10.2514/1.C031492 PG 14 WC Engineering, Aerospace SC Engineering GA AA8VQ UT WOS:000331373500002 ER PT J AU Zeng, J Kukreja, SL AF Zeng, Jie Kukreja, Sunil L. TI Flutter Prediction for Flight/Wind-Tunnel Flutter Test Under Atmospheric Turbulence Excitation SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT International Forum of Aeroelasticity and Structural Dynamics CY JUN 26-30, 2011 CL Paris, FRANCE ID IDENTIFICATION; SYSTEMS; TOOL AB In this paper, a flutter-boundary prediction technique for an aeroelastic/aeroservoelastic structure is introduced. This approach uses time-series flight/wind-tunnel flutter test data to compute an accurate estimate of the flutter speed. The flutter-boundary prediction tool discussed in this paper can be categorized into three steps. 1) Signal preprocessing techniques are introduced to estimate the frequency-response function if the external excitation signal is measurable or compute the autopower spectrum when only responses from sensors can be measured due to a strong turbulence perturbation during flight flutter test. 2) A frequency-domain system-identification methodology combined with a stabilization diagram is implemented to extract the elastic modes of a flexible structure. Accuracy of modes estimated in the second step directly affects the robustness of flutter prediction. 3) The flutter-prediction analysis can therefore be performed with the implementation of an appropriate flutter-prediction tool such as the Zimmerman-Weissenburger flutter margin and/or damping trends extrapolation methods. Application of the proposed flutter-boundary prediction method to the Aeroelastic Test Wing I and SuperSonic SemiSpan Transport model demonstrates that it is an efficient tool for flutter-boundary prediction of aeroelastic/aeroservoelastic structures. C1 [Zeng, Jie] ZONATechnol Inc, Scottsdale, AZ 85258 USA. [Kukreja, Sunil L.] NASA, Dryden Flight Res Ctr, Edwards AFB, CA 93523 USA. RP Zeng, J (reprint author), Commercial Aircraft Corp China Ltd, Beijing Aeronaut Sci & Technol Res Inst, Beijing, Peoples R China. EM zengjie@comac.cc; sunil.l.kukreja@nasa.gov NR 17 TC 1 Z9 4 U1 0 U2 1 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD NOV-DEC PY 2013 VL 50 IS 6 BP 1696 EP 1709 DI 10.2514/1.C031710 PG 14 WC Engineering, Aerospace SC Engineering GA AA8VQ UT WOS:000331373500003 ER PT J AU Broeren, AP Riley, JT AF Broeren, Andy P. Riley, James T. TI Scaling of Lift Degradation Due to Antiicing Fluids SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT 4th AIAA Atmospheric and Space Environments Conference CY JUN 25-28, 2012 CL New Orleans, LA SP AIAA ID AERODYNAMICS AB In recent years, North American civil airworthiness authorities have conducted research to develop the allowance times for aircraft operations in ice-pellet precipitation. These allowance times are critical to ensure the safety and efficient operation of commercial and cargo flights. Wind-tunnel testing with uncontaminated antiicing fluids and fluids contaminated with simulated ice pellets has been carried out to better understand the flowoff characteristics and resulting aerodynamic effects. The percent lift loss was determined at an 8 deg angle of attack and used as one of the evaluation criteria in determining the allowance times. This paper describes how the lift loss was related to the loss in the maximum lift of a Boeing 737-200ADV airplane through the aerodynamic acceptance test performed for fluids qualification. A loss in the maximum lift coefficient of 5.24% on the B737-200ADV airplane (which was adopted as the threshold in the aerodynamic acceptance test) corresponds to a lift loss of 7.3% on the test model at an 8 deg angle of attack. A statistical analysis was performed to account for data scatter in the correlation and indicated that the upper limit of lift loss on the test model was 9.2%. Therefore, for cases resulting in lift loss from 7.3 to 9.2%, extra scrutiny of the visual observations is required for evaluating fluid performance with contamination and establishing appropriate allowance times. C1 [Broeren, Andy P.] NASA, John H Glenn Res Ctr Lewis Field, Icing Branch, Cleveland, OH 44135 USA. [Riley, James T.] FAA, Aircraft Icing Res Program, Atlantic City, NJ 08405 USA. RP Broeren, AP (reprint author), NASA, John H Glenn Res Ctr Lewis Field, Icing Branch, 21000 Brookpark Rd,MS 11-2, Cleveland, OH 44135 USA. NR 29 TC 1 Z9 1 U1 1 U2 1 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD NOV-DEC PY 2013 VL 50 IS 6 BP 1886 EP 1895 DI 10.2514/1.C032259 PG 10 WC Engineering, Aerospace SC Engineering GA AA8VQ UT WOS:000331373500019 ER PT J AU Zelinski, SJ AF Zelinski, Shannon J. TI Benefits of Precision Scheduling and Spacing for Arrival Operations SO JOURNAL OF AIRCRAFT LA English DT Article AB Advances in arrival scheduling and controller aids for spacing have the potential benefits of reducing aircraft delays and increasing airport arrival throughput. Schedulers use fixed arrival paths to estimate aircraft's time-to-fly and assign them arrival slots based on the required separation with a buffer. Concepts that reduce arrival time uncertainty can take advantage of advanced scheduling with smaller spacing buffers. These concepts have been successfully demonstrated with a handful of near- to midterm traffic demand scenarios and technologies using spacing buffers as low as 0.3 n mile. The analysis published here characterizes the observed arrival spacing behavior of 29 runways at 15 airports in eight of the busiest terminal areas across the United States during 32-60 days worth of traffic. The typical observed instrument arrival buffers ranging from 0.5 to 1.5 n mile would equate to roughly a 10-20% increase in runway arrival capacity if buffers were reduced to 0.3 n mile. The effect of fixed arrival routing on terminal area flight time was also studied. Most runways studied had a significant path stretch delay. This work estimates that 1-2 min of this delay could be reduced with precision scheduling, and most of the remaining delay could be absorbed by speed control. C1 NASA, Ames Res Ctr, Aerosp High Dens Operat Branch, Moffett Field, CA 94035 USA. RP Zelinski, SJ (reprint author), NASA, Ames Res Ctr, Aerosp High Dens Operat Branch, Mail Stop 210-06,Bldg 210,Rm 207,POB 1, Moffett Field, CA 94035 USA. FU Concept and Technology Development Project, NASA's Airspace Systems Program FX This work was funded by the Concept and Technology Development Project, which is a part of NASA's Airspace Systems Program. NR 21 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 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD NOV-DEC PY 2013 VL 50 IS 6 BP 1923 EP 1932 DI 10.2514/1.C032352 PG 10 WC Engineering, Aerospace SC Engineering GA AA8VQ UT WOS:000331373500022 ER PT J AU Brown, AM DeHaye, M DeLessio, S AF Brown, Andrew M. DeHaye, Michael DeLessio, Steven TI Probabilistic Methods to Determine Resonance Risk and Damping for Rocket Turbine Blades SO JOURNAL OF PROPULSION AND POWER LA English DT Article AB The liquid oxygen-hydrogen J-2X rocket engine, which powers the upper stage of the NASA Space Launch System, is presently undergoing hot-fire testing. Analysis revealed numerous potential resonance issues with hardware in the turbomachinery flowpath, which could be catastrophic for the launch vehicle. This paper describes a series of probabilistic analyses incorporating nondeterministic characteristics of mistuning amplification, blade damping, natural frequency, and speed to assess the risk of failure of turbine blades due to resonance during past and present tests and to determine an appropriate value of damping to use in deterministic forced response analysis. The analyses are the first reported in the literature combining these critical nondeterministic parameters. The new damping determination technique developed here indicates that combining a damping value in the lower 1.5 sigma range with a 3 sigma mistuning amplification value results in a desired total 3 sigma probability of failure. These risk calculations were invaluable for determining high-cycle-fatigue margins of safety and in determining if risk-reduction methods such as dampers were necessary immediately, or if tests could be performed before risk-reduction hardware was ready. C1 [Brown, Andrew M.; DeHaye, Michael] NASA, George C Marshall Space Flight Ctr, ER41, Huntsville, AL 35812 USA. [DeLessio, Steven] Jacobs Inc, Jacobs ESTS, NASA MSFC ER41, Huntsville, AL 35812 USA. RP Brown, AM (reprint author), NASA, George C Marshall Space Flight Ctr, ER41, Huntsville, AL 35812 USA. NR 22 TC 1 Z9 1 U1 4 U2 10 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 EI 1533-3876 J9 J PROPUL POWER JI J. Propul. Power PD NOV-DEC PY 2013 VL 29 IS 6 BP 1367 EP 1373 DI 10.2514/1.B34834 PG 7 WC Engineering, Aerospace SC Engineering GA AA8VB UT WOS:000331372000014 ER PT J AU Peuget, JW Frendi, A AF Peuget, John W. Frendi, Abdelkader TI Toward the Understanding of Flow-Induced Vibrations in a Rocket-Engine Manifold SO JOURNAL OF PROPULSION AND POWER LA English DT Article ID ACOUSTIC EXCITATION; SIMULATION; RADIATION AB Results from two unsteady, turbulent flow computations using a hybrid Reynolds-averaged Navier-Stokes/large-eddy-simulation turbulence model are presented. One computation deals with flow in a complex rocket-engine cooling manifold and the other with a simpler T-junction flow. Results from the T-junction flow computations show that, for a for a critical flow velocity in the side branches, an acoustic resonance is excited. The reduced velocity at resonance was found to be in the range 1.5 to 1.7, which is in good agreement with experimental measurements. In addition, the pressure profile exhibits a node on the axis of the T junction with antinodes of opposite signs in the side branches. For the rocket-engine cooling manifold, results show that vortex shedding and pressure fluctuations within the manifold significantly influence the stability of shear layers and flow through exit cooling tubes. In some cooling tubes near the inflow region, the shear layer blocks the entrance to the tubes, whereas in some other regions, flow reversal is observed. C1 [Peuget, John W.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Frendi, Abdelkader] Univ Alabama, Huntsville, AL 35899 USA. RP Peuget, JW (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. FU Launch Services Program at NASA Kennedy Space Center; Propulsion Systems Department at NASA Marshall Space Flight Center FX The first author would like to acknowledge the support of the Launch Services Program at NASA Kennedy Space Center and the Propulsion Systems Department at NASA Marshall Space Flight Center. NR 25 TC 2 Z9 2 U1 1 U2 7 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 EI 1533-3876 J9 J PROPUL POWER JI J. Propul. Power PD NOV-DEC PY 2013 VL 29 IS 6 BP 1468 EP 1477 DI 10.2514/1.B34728 PG 10 WC Engineering, Aerospace SC Engineering GA AA8VB UT WOS:000331372000024 ER PT J AU Johansen, CT Novak, L Bathel, BF Ashcraft, SW Danehy, PM AF Johansen, C. T. Novak, L. Bathel, B. F. Ashcraft, S. W. Danehy, P. M. TI Mars Science Laboratory Reaction Control System Jet Computations with Visualization and Velocimetry SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT 50th AIAA Aerospace Sciences Meeting and Exhibit including the New Horizons Forum and Aerospace Exposition CY JAN 06-13, 2012 CL Nashville, TN SP AIAA, US AF Off Sci Res ID FLOWS AB Numerical predictions of the Mars Science Laboratory reaction control system jets interacting with a Mach 10 hypersonic flow are compared to experimental nitric oxide planar laser-induced fluorescence data. The steady Reynolds-averaged Navier-Stokes equations using the Baldwin-Barth one-equation turbulence model were solved using the OVERFLOW code. The experimental fluorescence data used for comparison consist of qualitative two-dimensional visualization images, qualitative reconstructed three-dimensional flow structures, and quantitative two-dimensional distributions of streamwise velocity. Through modeling of the fluorescence signal equation, computational flow images were produced and directly compared to the qualitative fluorescence data. Post processing of the experimental and simulation data enabled the jet trajectory to be extracted for a more quantitative comparison. The two-dimensional velocity fields were reconstructed through interpolation of a series of single-component velocity profiles. Each distribution of single-component velocity was obtained using molecular tagging velocimetry. After validating the numerical model, the numerical solution was further examined to gain insight into hypersonic jet-in- crossflow interaction. Novel nitric oxide planar laser induced fluorescence experiments are proposed based on this analysis. C1 [Johansen, C. T.] Univ Calgary, Calgary, AB T2N 1N4, Canada. [Novak, L.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Bathel, B. F.; Ashcraft, S. W.; Danehy, P. M.] NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23681 USA. RP Johansen, CT (reprint author), Univ Calgary, Calgary, AB T2N 1N4, Canada. NR 23 TC 2 Z9 2 U1 0 U2 2 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD NOV-DEC PY 2013 VL 50 IS 6 BP 1183 EP 1195 DI 10.2514/1.A32496 PG 13 WC Engineering, Aerospace SC Engineering GA AA8VG UT WOS:000331372500007 ER PT J AU Dutta, S Braun, RD Russell, RP Striepe, SA Clark, IG AF Dutta, Soumyo Braun, Robert D. Russell, Ryan P. Striepe, Scott A. Clark, Ian G. TI Comparison of Statistical Estimation Techniques for Mars Entry, Descent, and Landing Reconstruction SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT 50th AIAA Aerospace Sciences Meeting and Exhibit including the New Horizons Forum and Aerospace Exposition CY JAN 06-13, 2012 CL Nashville, TN SP AIAA, US AF Off Sci Res ID PATHFINDER ENTRY; SMOOTHER; FILTERS AB Flight data from an entry, descent, and landing sequence can be used to reconstruct the vehicle's trajectory, aerodynamic coefficients, and the atmospheric profile experienced by the vehicle. Past Mars missions have not contained instrumentation that would allow for the separation of uncertainties in the atmosphere and the aerodynamic database. The 2012 Mars Science Laboratory took measurements of the pressure distribution on the aeroshell forebody during entry and allows freestream atmospheric conditions to be partially observable. Methods to estimate the flight performance statistically using onboard measurements are demonstrated here through the use of simulated Mars data. A range of statistical estimators, specifically the extended Kalman filter and unscented Kalman filter, are used to demonstrate which estimator best quantifies the states and the uncertainties in the flight parameters. The techniques demonstrated herein are planned for application to the Mars Science Laboratory flight dataset. C1 [Dutta, Soumyo; Braun, Robert D.] Georgia Inst Technol, Daniel Guggenheim Sch Aerosp Engn, Atlanta, GA 30332 USA. [Russell, Ryan P.] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA. [Striepe, Scott A.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA. [Clark, Ian G.] CALTECH, Jet Prop Lab, Entry Descent & Landing Syst & Adv Technol Grp, Pasadena, CA 91109 USA. RP Dutta, S (reprint author), Georgia Inst Technol, Daniel Guggenheim Sch Aerosp Engn, 270 Ferst Dr, Atlanta, GA 30332 USA. NR 39 TC 4 Z9 5 U1 1 U2 1 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 NOV-DEC PY 2013 VL 50 IS 6 BP 1207 EP 1221 DI 10.2514/1.A32459 PG 15 WC Engineering, Aerospace SC Engineering GA AA8VG UT WOS:000331372500009 ER PT J AU Huang, J Chu, XL Lyons, TW Sun, T Feng, LJ Zhang, QR Chang, HJ AF Huang, Jing Chu, Xuelei Lyons, Timothy W. Sun, Tao Feng, Lianjun Zhang, Qirui Chang, Huajin TI The sulfur isotope signatures of Marinoan deglaciation captured in Neoproterozoic shallow-to-deep cap carbonate from South China SO PRECAMBRIAN RESEARCH LA English DT Article DE Neoproterozoic; South China; Doushantuo Formation; Cap carbonate; Sulfur isotope ID EDIACARAN DOUSHANTUO FORMATION; PB ZIRCON AGE; SNOWBALL EARTH; METHANE SEEPS; HYDRATE DESTABILIZATION; HYDROTHERMAL ORIGIN; YANGTZE PLATFORM; DEATH-VALLEY; ICE AGES; GLACIATION AB We present high-resolution sulfur and carbon isotope records from the cap carbonate of the Doushantuo Formation, South China, a unique suite of depositional facies spanning across a pronounced paleooceanic depth gradient. The delta S-34 of carbonate-associated sulfate (CAS) decreases across a shelf-to-slope depth transect. We propose that the deeper-water slope profile represents syn-glacial sulfur isotope compositions of the seawater sulfates with impact of S-34-depleted hydrothermal sulfur inputs, while the delta S-34 of the shallow inner-shelf were dominantly controlled by the S-34-enriched terrigenous input. We suggest that the terrigenous sulfur inputs were mainly from weathering and erosion of the pre-Marinoan Datangpo Formation glacially ground and then freshly exposed during rapid deglaciation. The widespread Datangpo Formation, deposited between the Sturtian and Marinoan glacial intervals, is noted for the unusually high delta S-34 values of its pyrite. The low sulfate conditions in the ocean allowed for strong local controls and consequent heterogeneities in seawater chemistry. The post-Marinoan ocean was stratified in the immediate wake of glaciation, with anoxic deep waters overlain by an oxic, melt-water layer. During the transgression, the shallow water was disturbed by upwelling. The oxidation of dissolved organic carbon (DOG) from deep water would lead to transiently enhanced C-13 depletions but S-34 enrichments in the shallow waters. (C) 2013 Elsevier B.V. All rights reserved. C1 [Huang, Jing] Univ Sci & Technol China, Sch Earth & Space Sci, CAS Key Lab Crust Mantle Mat & Environm, Hefei 230026, Peoples R China. [Chu, Xuelei; Feng, Lianjun; Zhang, Qirui] Chinese Acad Sci, Inst Geol & Geophys, State Key Lab Lithospher Evolut, Beijing 100029, Peoples R China. [Chu, Xuelei] NW Univ Xian, State Key Lab Continental Dynam, Xian 710069, Peoples R China. [Lyons, Timothy W.] Univ Calif Riverside, Dept Earth Sci, Riverside, CA 92521 USA. [Sun, Tao] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Chang, Huajin] Qinghai Normal Univ, Sch Life & Geog Sci, Xining 810008, Peoples R China. RP Chu, XL (reprint author), Chinese Acad Sci, Inst Geol & Geophys, Beijing 100029, Peoples R China. EM xlchu@mail.iggcas.ac.cn RI Feng, Lianjun/E-4570-2014 OI Feng, Lianjun/0000-0002-0325-3789 FU Ministry of Science and Technology of China [2011CB808805]; Natural Science Foundation of China [41172029, 41003034, 41025011]; State Key Laboratory of Continental Dynamics, Northwest University in China; U.S. National Science Foundation; NASA Astrobiology Institute FX This research is funded by the Ministry of Science and Technology of China (Grant 2011CB808805), the Natural Science Foundation of China (Grants 41172029, 41003034, 41025011), and the State Key Laboratory of Continental Dynamics, Northwest University in China. Funds were provided to TWL by the U.S. National Science Foundation and the NASA Astrobiology Institute. We thank Dr. G. Jiang and Dr. Y. Li for constructive comments and F. Zhang for laboratory assistant. We are grateful for the constructive suggestions and comments of two anonymous reviewers. NR 75 TC 3 Z9 4 U1 9 U2 31 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0301-9268 EI 1872-7433 J9 PRECAMBRIAN RES JI Precambrian Res. PD NOV PY 2013 VL 238 BP 42 EP 51 DI 10.1016/j.precamres.2013.09.002 PG 10 WC Geosciences, Multidisciplinary SC Geology GA AA0WT UT WOS:000330818800003 ER PT J AU Yue, Q Fetzer, EJ Kahn, BH Wong, S Manipon, G Guillaume, A Wilson, B AF Yue, Qing Fetzer, Eric J. Kahn, Brian H. Wong, Sun Manipon, Gerald Guillaume, Alexandre Wilson, Brian TI Cloud-State-Dependent Sampling in AIRS Observations Based on CloudSat Cloud Classification SO JOURNAL OF CLIMATE LA English DT Article DE Clouds; Temperature; Water vapor; Climate records; Satellite observations ID ATMOSPHERIC INFRARED SOUNDER; TROPICAL WESTERN PACIFIC; 1998 EL-NINO; WATER-VAPOR; STATISTICAL-ANALYSES; CLIMATE-CHANGE; OBJECT DATA; SATELLITE; TEMPERATURE; VALIDATION AB The precision, accuracy, and potential sampling biases of temperature T and water vapor q vertical profiles obtained by satellite infrared sounding instruments are highly cloud-state dependent and poorly quantified. The authors describe progress toward a comprehensive T and q climatology derived from the Atmospheric Infrared Sounder (AIRS) suite that is a function of cloud state based on collocated CloudSat observations. The AIRS sampling rates, biases, and center root-mean-square differences (CRMSD) are determined through comparisons of pixel-scale collocated ECMWF model analysis data. The results show that AIRS provides a realistic representation of most meteorological regimes in most geographical regions, including those dominated by high thin cirrus and shallow boundary layer clouds. The mean AIRS observational biases relative to the ECMWF analysis between the surface and 200 hPa are within +/- 1 K in T and from -1 to +0.5 g kg(-1) in q. Biases because of cloud-state-dependent sampling dominate the total biases in the AIRS data and are largest in the presence of deep convective (DC) and nimbostratus (Ns) clouds. Systematic cold and dry biases are found throughout the free troposphere for DC and Ns. Somewhat larger biases are found over land and in the midlatitudes than over the oceans and in the tropics, respectively. Tropical and oceanic regions generally have a smaller CRMSD than the midlatitudes and over land, suggesting agreement of T and q variability between AIRS and ECMWF in these regions. The magnitude of CRMSD is also strongly dependent on cloud type. C1 [Yue, Qing; Fetzer, Eric J.; Kahn, Brian H.; Wong, Sun; Manipon, Gerald; Guillaume, Alexandre; Wilson, Brian] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Yue, Qing] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Pasadena, CA 91109 USA. RP Yue, Q (reprint author), Univ Calif Los Angeles, Jet Prop Lab, Joint Inst Reg Earth Syst Sci & Engn, 4800 Oak Grove Dr,Mail Stop 233-301F, Pasadena, CA 91109 USA. EM qing.yue@jpl.nasa.gov RI Yue, Qing/F-4619-2017 OI Yue, Qing/0000-0002-3559-6508 FU National Aeronautics and Space Administration; NASA's Making Earth Science Data Records for Use in Research Environments (MEASURES) program; AIRS Project at JPL FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This project was supported by NASA's Making Earth Science Data Records for Use in Research Environments (MEASURES) program. We acknowledge the support of the AIRS Project at JPL. The authors thank Baijun Tian, Bjorn Lambrigsten, Ed Olsen, and Joel Susskind for useful feedback during the preparation of this manuscript. We also thank the anonymous reviewers for their helpful suggestions and comments. NR 63 TC 16 Z9 16 U1 1 U2 7 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 NOV PY 2013 VL 26 IS 21 BP 8357 EP 8377 DI 10.1175/JCLI-D-13-00065.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 296OF UT WOS:000330193800007 ER PT J AU Hall, T Yonekura, E AF Hall, Timothy Yonekura, Emmi TI North American Tropical Cyclone Landfall and SST: A Statistical Model Study SO JOURNAL OF CLIMATE LA English DT Article DE Hurricanes; typhoons; Stochastic models; Risk assessment ID SEA-SURFACE TEMPERATURE; POTENTIAL INTENSITY; ATLANTIC HURRICANES; RISK-ASSESSMENT; CLIMATE-CHANGE; CMIP5 MODELS; TRACKS; TRENDS; IMPACT AB A statistical-stochastic model of the complete life cycle of North Atlantic (NA) tropical cyclones (TCs) is used to examine the relationship between climate and landfall rates along the North American Atlantic and Gulf Coasts. The model draws on archived data of TCs throughout the North Atlantic to estimate landfall rates at high geographic resolution as a function of the ENSO state and one of two different measures of sea surface temperature (SST): 1) SST averaged over the NA subtropics and the hurricane season and 2) this SST relative to the seasonal global subtropical mean SST (termed relSST). Here, the authors focus on SST by holding ENSO to a neutral state. Jackknife uncertainty tests are employed to test the significance of SST and relSST landfall relationships. There are more TC and major hurricane landfalls overall in warm years than cold, using either SST or relSST, primarily due to a basinwide increase in the number of storms. The signal along the coast, however, is complex. Some regions have large and significant sensitivity (e.g., an approximate doubling of annual major hurricane landfall probability on Texas from -2 to +2 standard deviations in relSST), while other regions have no significant sensitivity (e.g., the U.S. mid-Atlantic and Northeast coasts). This geographic structure is due to both shifts in the regions of primary TC genesis and shifts in TC propagation. C1 [Hall, Timothy] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Yonekura, Emmi] Columbia Univ, New York, NY USA. RP Hall, T (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM timothy.m.hall@nasa.gov FU NASA; NOAA [NA11OAR4310093] FX We are grateful to Dr. Thomas Jagger for discussion concerning extreme value theory. We also thank three anonymous reviewers for helpful comments on the manuscript. This work was supported by a NASA National Climate Assessment Award and NOAA Grant NA11OAR4310093. NR 37 TC 7 Z9 7 U1 0 U2 18 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 NOV PY 2013 VL 26 IS 21 BP 8422 EP 8439 DI 10.1175/JCLI-D-12-00756.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 296OF UT WOS:000330193800011 ER PT J AU Taylor, PC Cai, M Hu, AX Meehl, GA Washington, W Zhang, GJ AF Taylor, Patrick C. Cai, Ming Hu, Aixue Meehl, Gerald A. Washington, Warren Zhang, Guang J. TI A decomposition of feedback contributions to polar warming amplification (vol 26, pg 7023, 2013) SO JOURNAL OF CLIMATE LA English DT Correction C1 [Taylor, Patrick C.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Cai, Ming] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA. [Hu, Aixue; Meehl, Gerald A.; Washington, Warren] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Zhang, Guang J.] Univ Calif San Diego, Scripps Inst Oceanog, San Diego, CA 92103 USA. RP Cai, M (reprint author), Florida State Univ, Dept Earth Ocean & Atmospher Sci, 1017 Acad Way, Tallahassee, FL 32306 USA. EM mcai@fsu.edu RI Hu, Aixue/E-1063-2013 OI Hu, Aixue/0000-0002-1337-287X NR 1 TC 0 Z9 0 U1 0 U2 6 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 NOV PY 2013 VL 26 IS 21 BP 8706 EP 8706 DI 10.1175/JCLI-D-13-00511.1 PG 1 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 296OF UT WOS:000330193800029 ER PT J AU Salzmann, U Dolan, AM Haywood, AM Chan, WL Voss, J Hill, DJ Abe-Ouchi, A Otto-Bliesner, B Bragg, FJ Chandler, MA Contoux, C Dowsett, HJ Jost, A Kamae, Y Lohmann, G Lunt, DJ Pickering, SJ Pound, MJ Ramstein, G Rosenbloom, NA Sohl, L Stepanek, C Ueda, H Zhang, ZS AF Salzmann, Ulrich Dolan, Aisling M. Haywood, Alan M. Chan, Wing-Le Voss, Jochen Hill, Daniel J. Abe-Ouchi, Ayako Otto-Bliesner, Bette Bragg, Frances J. Chandler, Mark A. Contoux, Camille Dowsett, Harry J. Jost, Anne Kamae, Youichi Lohmann, Gerrit Lunt, Daniel J. Pickering, Steven J. Pound, Matthew J. Ramstein, Gilles Rosenbloom, Nan A. Sohl, Linda Stepanek, Christian Ueda, Hiroaki Zhang, Zhongshi TI Challenges in quantifying Pliocene terrestrial warming revealed by data-model discord SO NATURE CLIMATE CHANGE LA English DT Article ID POLAR AMPLIFICATION; MIDDLE PLIOCENE; CLIMATE-CHANGE; RECONSTRUCTION; TEMPERATURE; VEGETATION; OCEAN AB Comparing simulations of key warm periods in Earth history with contemporaneous geological proxy data is a useful approach for evaluating the ability of climate models to simulate warm, high-CO2 climates that are unprecedented in the more recent past(1-3). Here we use a global data set of confidence-assessed, proxy-based temperature estimates and biome reconstructions to assess the ability of eight models to simulate warm terrestrial climates of the Pliocene epoch. The Late Pliocene, 3.6-2.6 million years ago, is an accessible geological interval to understand climate processes of a warmer world(4). We show that model-predicted surface air temperatures reveal a substantial cold bias in the Northern Hemisphere. Particularly strong data-model mismatches in mean annual temperatures (up to 18 degrees C) exist in northern Russia. Our model sensitivity tests identify insufficient temporal constraints hampering the accurate configuration of model boundary conditions as an important factor impacting on data-model discrepancies. We conclude that to allow a more robust evaluation of the ability of present climate models to predict warm climates, future Pliocene data-model comparison studies should focus on orbitally defined time slices(5). C1 [Salzmann, Ulrich] Northumbria Univ, Fac Engn & Environm, Dept Geog, Newcastle Upon Tyne NE1 8ST, Tyne & Wear, England. [Dolan, Aisling M.; Haywood, Alan M.; Pickering, Steven J.] Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. [Chan, Wing-Le; Abe-Ouchi, Ayako] Univ Tokyo, Atmosphere & Ocean Res Inst, Kashiwa, Chiba 2778564, Japan. [Voss, Jochen] Univ Leeds, Sch Math, Leeds LS2 9JT, W Yorkshire, England. [Hill, Daniel J.] British Geol Survey, Nottingham NG12 5GG, England. [Abe-Ouchi, Ayako] Japan Agcy Marine Earth Sci & Technol, Yokohama, Kanagawa 2360001, Japan. [Otto-Bliesner, Bette; Rosenbloom, Nan A.] Natl Ctr Atmospher Res, Boulder, CO 80305 USA. [Bragg, Frances J.; Lunt, Daniel J.] Univ Bristol, Sch Geol Sci, Bristol BS8 1SS, Avon, England. [Chandler, Mark A.; Sohl, Linda] Columbia Univ, NASA GISS, New York, NY 10025 USA. [Contoux, Camille; Ramstein, Gilles] CNRS CEA UVSQ, LSCE IPSL, F-91191 Gif Sur Yvette, France. [Contoux, Camille; Jost, Anne] Univ Paris 06, CNRS, Sisyphe, F-75005 Paris, France. [Dowsett, Harry J.] US Geol Survey, Eastern Geol & Paleoclimate Sci Ctr, Reston, VA 20192 USA. [Kamae, Youichi; Ueda, Hiroaki] Univ Tsukuba, Grad Sch Life & Environm Sci, Tsukuba, Ibaraki 3058506, Japan. [Lohmann, Gerrit; Stepanek, Christian] Alfred Wegener Inst Polar & Marine Res, D-27570 Bremerhaven, Germany. [Zhang, Zhongshi] Chinese Acad Sci, Inst Atmospher Phys, Beijing 100029, Peoples R China. [Zhang, Zhongshi] Bjerknes Ctr Climate Res, N-5007 Bergen, Norway. RP Salzmann, U (reprint author), Northumbria Univ, Fac Engn & Environm, Dept Geog, Newcastle Upon Tyne NE1 8ST, Tyne & Wear, England. EM Ulrich.Salzmann@northumbria.ac.uk RI Kamae, Youichi/L-6694-2013; Voss, Jochen/F-9638-2012; Lunt, Daniel/G-9451-2011; Ramstein, Gilles/L-3328-2014; Zhang, Zhongshi/L-2891-2013; Bragg, Fran/C-6198-2015; OI Pound, Matthew/0000-0001-8029-9548; Hill, Daniel/0000-0001-5492-3925; Abe-Ouchi, Ayako/0000-0003-1745-5952; Kamae, Youichi/0000-0003-0461-5718; Voss, Jochen/0000-0002-2323-3814; Lunt, Daniel/0000-0003-3585-6928; Ramstein, Gilles/0000-0002-1522-917X; Zhang, Zhongshi/0000-0002-2354-1622; Bragg, Fran/0000-0002-8179-4214; Dolan, Aisling/0000-0002-9585-9648; Lohmann, Gerrit/0000-0003-2089-733X; Dowsett, Harry/0000-0003-1983-7524 FU Natural Environment Research Council, NERC [NE/I016287/1]; European Research Council under the European Union [278636]; NERC [NE/H006273/1]; Japan Society for the Promotion of Science; Leverhulme Trust; National Centre for Atmospheric Science; British Geological Survey; Helmholtz research programme PACES; Helmholtz Climate Initiative REKLIM; Helmholtz Graduate School for Polar and Marine Research; REKLIM; US National Science Foundation; National Science Foundation FX Financial support was provided by grants to U.S. and A.M.H. from the Natural Environment Research Council, NERC (NE/I016287/1). A.M.D. and A.M.H. acknowledge financial support from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no. 278636. D.J.L. and F.J.B. acknowledge the NERC grant NE/H006273/1. U.S., A.M.D., H.J.D. and A.M.H. thank the US Geological Survey John Wesley Powell Center for Analysis and Synthesis. W-L.C. and A.A-O. acknowledge financial support from the Japan Society for the Promotion of Science and computing resources at the Earth Simulator Center, JAMSTEC. H.J.D. acknowledges the continued support of the US Geological Survey Climate and Land Use Change Research and Development Program; D.J.H. acknowledges the Leverhulme Trust for the award of an Early Career Fellowship and the National Centre for Atmospheric Science and the British Geological Survey for financial support. G.L. received financial support through the Helmholtz research programme PACES and the Helmholtz Climate Initiative REKLIM. C.S. acknowledges financial support from the Helmholtz Graduate School for Polar and Marine Research and from REKLIM. B.O-B. and N.A.R. recognize the National Center for Atmospheric Research is sponsored by the US National Science Foundation and computing resources were provided by the Climate Simulation Laboratory at the National Center for Atmospheric Research's Computational and Information Systems Laboratory sponsored by the National Science Foundation and other agencies. NR 27 TC 39 Z9 39 U1 5 U2 32 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 NOV PY 2013 VL 3 IS 11 BP 969 EP 974 DI 10.1038/NCLIMATE2008 PG 6 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 295OJ UT WOS:000330125100015 ER PT J AU White, JC Wulder, MA Varhola, A Vastaranta, M Coops, NC Cook, BD Pitt, D Woods, M AF White, Joanne C. Wulder, Michael A. Varhola, Andres Vastaranta, Mikko Coops, Nicholas C. Cook, Bruce D. Pitt, Doug Woods, Murray TI A best practices guide for generating forest inventory attributes from airborne laser scanning data using an area-based approach SO FORESTRY CHRONICLE LA English DT Editorial Material ID LIDAR C1 [White, Joanne C.; Wulder, Michael A.; Vastaranta, Mikko] Forestry Canada, Pacific Forestry Ctr, Canadian Forest Serv, Nat Resources Canada, Victoria, BC V8Z 1M5, Canada. [Varhola, Andres; Coops, Nicholas C.] Univ British Columbia, Fac Forestry, Dept Forest Resources Management, Integrated Remote Sensing Studio, Vancouver, BC V6T 1W5, Canada. [Vastaranta, Mikko] Univ Helsinki, Dept Forest Sci, Helsinki, Finland. [Cook, Bruce D.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Pitt, Doug] Canadian Wood Fibre Ctr, Canadian Forest Serv, Nat Resources Canada, Sault Ste Marie, ON, Canada. [Woods, Murray] Ontario Minist Nat Resources, Prov Serv, Sci & Res Branch, North Bay, ON, Canada. RP White, JC (reprint author), Forestry Canada, Pacific Forestry Ctr, Canadian Forest Serv, Nat Resources Canada, 506 W Burnside Rd, Victoria, BC V8Z 1M5, Canada. RI Coops, Nicholas/J-1543-2012; Wulder, Michael/J-5597-2016; OI Coops, Nicholas/0000-0002-0151-9037; Wulder, Michael/0000-0002-6942-1896; Vastaranta, Mikko/0000-0001-6552-9122 NR 3 TC 20 Z9 21 U1 3 U2 13 PU CANADIAN INST FORESTRY PI MATTAWA PA C/O CANADIAN ECOLOGY CENTRE, PO BOX 430, 6905 HWY 17 W, MATTAWA, ONTARIO P0H 1V0, CANADA SN 0015-7546 EI 1499-9315 J9 FOREST CHRON JI For. Chron. PD NOV-DEC PY 2013 VL 89 IS 6 BP 722 EP 723 DI 10.5558/tfc2013-132 PG 2 WC Forestry SC Forestry GA 293PT UT WOS:000329986200003 ER PT J AU Thomson, J D'Asaro, EA Cronin, MF Rogers, WE Harcourt, RR Shcherbina, A AF Thomson, J. D'Asaro, E. A. Cronin, M. F. Rogers, W. E. Harcourt, R. R. Shcherbina, A. TI Waves and the equilibrium range at Ocean Weather Station P SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE waves; equilibrium; wind stress ID DOPPLER-VELOCIMETER DATA; SEA-SURFACE ROUGHNESS; WIND STRESS; DRAG COEFFICIENT; GRAVITY-WAVES; DISSIPATION; SPECTRA; FLUX; DEPENDENCE; STEEPNESS AB Wave and wind measurements at Ocean Weather Station P (OWS-P, 50 degrees N 145 degrees W) are used to evaluate the equilibrium range of surface wave energy spectra. Observations are consistent with a local balance between wind input and breaking dissipation, as described by Philips (1985). The measurements include direct covariance wind stress estimates and wave breaking dissipation rate estimates during a 3 week research cruise to OWS-P. The analysis is extended to a wider range of conditions using observations of wave energy spectra and wind speed during a 2 year mooring deployment at OWS-P. At moderate wind speeds (5-15 m/s), mooring wave spectra are in agreement, within 5% uncertainty, with the forcing implied by standard drag laws and mooring wind measurements. At high wind speeds (>15 m/s), mooring wave spectra are biased low, by 13%, relative to the forcing implied by standard drag laws and mooring wind measurements. Deviations from equilibrium are associated with directionality and variations at the swell frequencies. A spectral wave hindcast accurately reproduces the mooring observations, and is used to examine the wind input. C1 [Thomson, J.; D'Asaro, E. A.; Harcourt, R. R.; Shcherbina, A.] Univ Washington, Appl Phys Lab, Seattle, WA 98105 USA. [Cronin, M. F.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. [Rogers, W. E.] Stennis Space Ctr, Naval Res Lab, Stennis Space Ctr, MS USA. RP Thomson, J (reprint author), Univ Washington, Appl Phys Lab, 1013 NE 40th St, Seattle, WA 98105 USA. EM jthomson@apl.uw.edu FU National Science Foundation [OCE-0850551, OCE-0960778] FX Joe Talbert (APL-UW) designed and built the waverider mooring, with guidance from Christian Meinig (PMEL-NOAA) and assistance from Alex deKlerk (APL-UW) and Stephanie Downey (APL-UW). Marie Roberts (IOS Canada) and the crew of the R/V Tully deployed the original mooring. Julie Thomas and Grant Cameron (CDIP-SIO) provided the waverider data telemetry and data archiving. Wind data were provided by the PMEL-NOAA Ocean Climate Stations group, with assistance from Keith Ronnholm. The crew of the R/V New Horizon (SIO) helped with the October 2012 mooring turnaround. Michael Schwendeman (APL-UW) and Johannes Gemmrich (U. Victoria) have contributed many discussions on equilibrium waves. Two anonymous reviewers improved the analysis and discussion of results. Funding was provided the National Science Foundation (OCE-0850551 and OCE-0960778). NR 55 TC 15 Z9 15 U1 1 U2 10 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 NOV PY 2013 VL 118 IS 11 BP 5951 EP 5962 DI 10.1002/2013JC008837 PG 12 WC Oceanography SC Oceanography GA 291YD UT WOS:000329867900007 ER PT J AU Ilie, R Skoug, RM Valek, P Funsten, HO Glocer, A AF Ilie, R. Skoug, R. M. Valek, P. Funsten, H. O. Glocer, A. TI Global view of inner magnetosphere composition during storm time SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE inner magnetosphere; modeling; TWINS data; magnetic storm ID RING CURRENT DEVELOPMENT; ION COMPOSITION; DISTANT MAGNETOTAIL; GEOMAGNETIC STORM; POLAR WIND; MODEL; IONOSPHERE; PLASMA; BULK; O+ AB Plasma dynamics in the inner magnetosphere are greatly affected by variations in the ion composition. The ratio of hydrogen to oxygen has been shown to be highly dependent on geomagnetic activity. To investigate this dependence, we examine the timing of the injection and subsequent evolution of O+ in the ring current during the storm of 6 August 2011 as observed by Two Wide-angle Imaging Neutral-atom Spectrometers (TWINS) instruments. To help interpret magnetospheric evolution using the global O Energetic Neutral Atom (ENA) emission measured by TWINS, we have employed a multidomain modeling of the global magnetosphere using the Space Weather Modeling Framework. TWINS Energetic Neutral Atom (ENA) imagers have the capability to distinguish between H and O emission and thus the major ion constituents of the ring current. Global composition measurements from TWINS spacecraft show intensifications of the oxygen ENA emission and thus an increase in the transport of ionospheric oxygen into the ring current that occur during the main phase of the storm. Both the observations and the simulation suggests that the peak in O ENA emission is correlated with the substorm injections that occurred during this time. The model also shows a very dynamic magnetosphere that allows for loss of oxygen from the Earth-magnetosphere system through plasmoids capable of transporting oxygen down the tail throughout the magnetic storm. This can possibly be a predominant pathway for loss of oxygen from the magnetosphere. C1 [Ilie, R.; Skoug, R. M.; Funsten, H. O.] Los Alamos Natl Lab, Los Alamos, NM USA. [Valek, P.] SW Res Inst, San Antonio, TX USA. [Glocer, A.] NASA, GSFC, Greenbelt, MD USA. RP Ilie, R (reprint author), Los Alamos Natl Lab, Alamos, NM 87545 USA. EM rilie@lanl.gov RI Glocer, Alex/C-9512-2012; Funsten, Herbert/A-5702-2015; OI Glocer, Alex/0000-0001-9843-9094; Funsten, Herbert/0000-0002-6817-1039; Valek, Philip/0000-0002-2318-8750 FU U.S. Department of Energy; NSF [NSF AGS 1027008]; NASA TWINS project FX Work at Los Alamos was performed under the auspices of the U.S. Department of Energy with financial support from the NSF grant NSF AGS 1027008 and the NASA TWINS project. We gratefully acknowledge Natasha Buzulukova and Mei-Ching Fok from NASA Goddard for providing the ENA tool as well as the whole SWMF team at University of Michigan. We would like to thank Sorin Zaharia from Los Alamos National Laboratory for valuable comments. NR 62 TC 6 Z9 6 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 NOV PY 2013 VL 118 IS 11 BP 7074 EP 7084 DI 10.1002/2012JA018468 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 293SB UT WOS:000329992900024 ER PT J AU He, F Zhang, XX Chen, B Fok, MC Zou, YL AF He, Fei Zhang, Xiao-Xin Chen, Bo Fok, Mei-Ching Zou, Yong-Liao TI Moon-based EUV imaging of the Earth's Plasmasphere: Model simulations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE earth's plasmasphere; EUV emission; moon-based imaging; magnetic storm; global dynamics ID EXTREME-ULTRAVIOLET IMAGER; ELECTRIC-FIELD; OUTER MAGNETOSPHERE; INTERPLANETARY GAS; SOLAR-WIND; NIGHT-SKY; PLANET-B; HE-II; RADIATION; SCANNER AB The EUV imager on board the Chang'E-3 lunar lander will image the Earth's plasmasphere from a lunar perspective to focus on some of the open questions in plasmaspheric researches (i.e., global structures, erosion, and refilling of plasmasphere). In order to achieve the understanding of the plasmaspheric dynamics in relation to these EUV images in lunar perspective, the He+ 30.4nm emission intensities and global structures of the plasmasphere viewed from the moon are investigated using a dynamic global core plasma model embedded with TS07 magnetic field model and W05 electric field model. Two typical storms observed by the IMAGE EUV imager are systematically simulated from the perspectives of the moon. It is found from the simulations that the maximum emission intensity of the plasmasphere is similar to 12.3 R which is greater than that detected from polar orbit, and the global shapes and temporal evolutions of large-scale plasmaspheric structures (plasmapause, shoulder, and plume) also have different patterns in moon-based simulated images. It is also shown that the plasmaspheric structures extracted from moon-based EUV images are in agreement with those from IMAGE EUV images. Systematic simulations demonstrate that specific latitudinal distribution of the plasmaspheric structures can only be imaged at specific positions in lunar orbit. It is expected that this investigation provides us with an overall understanding on moon-based EUV images and helps to identify the plasmaspheric structures and evolution patterns in future moon-based EUV imaging. C1 [He, Fei; Chen, Bo] Chinese Acad Sci, Changchun Inst Opt Fine Mech & Phys, Changchun, Peoples R China. [Zhang, Xiao-Xin] China Meteorol Adm, Natl Ctr Space Weather, Beijing 100081, Peoples R China. [Fok, Mei-Ching] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zou, Yong-Liao] Chinese Acad Sci, Natl Astron Observ, Beijing, Peoples R China. RP Zhang, XX (reprint author), China Meteorol Adm, Natl Ctr Space Weather, Beijing 100081, Peoples R China. EM xxzhang@cma.gov.cn RI Fok, Mei-Ching/D-1626-2012; OI Zhang, XiaoXin/0000-0002-7759-7402; HE, Fei/0000-0003-0542-2686 FU National Basic Research Program of China [2012CB957800, 2011CB811400]; National Natural Science Foundation of China [41204102, 41274147]; National Hi-Tech Research and Development Program of China [2012AA121000]; Chinese Academy of Sciences FX The authors would like to thank D. R. Weimer for providing the W05 electric field model. The authors would like to thank NASA-CCMC for providing the code of IGRF and Tsyganenko model and T. Forrester of IMAGE EUV team for the EUV data and relevant processing software. The authors also thank the ACE Science Center for the MAG and SWEPAM data and the Kyoto World Data Center for the Geomagnetic Index (AL, Kp, Dst). We also thank two reviewers for very valuable comments that helped us to improve the paper. This work was supported by the National Basic Research Program of China (2012CB957800 and 2011CB811400), the National Natural Science Foundation of China (41204102 and 41274147), the National Hi-Tech Research and Development Program of China (2012AA121000), and the Key Development Project of Chinese Academy of Sciences: Application research on the scientific data from Chang'E-3 mission. NR 57 TC 10 Z9 12 U1 2 U2 13 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 NOV PY 2013 VL 118 IS 11 BP 7085 EP 7103 DI 10.1002/2013JA018962 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 293SB UT WOS:000329992900025 ER PT J AU Gershman, DJ Slavin, JA Raines, JM Zurbuchen, TH Anderson, BJ Korth, H Baker, DN Solomon, SC AF Gershman, Daniel J. Slavin, James A. Raines, Jim M. Zurbuchen, Thomas H. Anderson, Brian J. Korth, Haje Baker, Daniel N. Solomon, Sean C. TI Magnetic flux pileup and plasma depletion in Mercury's subsolar magnetosheath SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE plasma depletion; magnetic flux pile-up; magnetosheath; Mercury ID ELECTRON-DISTRIBUTION FUNCTIONS; HIGH-LATITUDE MAGNETOPAUSE; FIELD DRAPING ENHANCEMENT; SOLAR-WIND INTERACTION; DAYSIDE MAGNETOPAUSE; MESSENGER OBSERVATIONS; TEMPERATURE ANISOTROPY; ISEE OBSERVATIONS; LAYER UPSTREAM; BOUNDARY-LAYER AB Measurements from the Fast Imaging Plasma Spectrometer (FIPS) and Magnetometer (MAG) on the MErcury Surface, Space ENvironment, GEochemistry, and Ranging spacecraft during 40 orbits about Mercury are used to characterize the plasma depletion layer just exterior to the planet's dayside magnetopause. A plasma depletion layer forms at Mercury as a result of piled-up magnetic flux that is draped around the magnetosphere. The low average upstream Alfvenic Mach number (M-A similar to 3-5) in the solar wind at Mercury often results in large-scale plasma depletion in the magnetosheath between the subsolar magnetopause and the bow shock. Flux pileup is observed to occur downstream under both quasi-perpendicular and quasi-parallel shock geometries for all orientations of the interplanetary magnetic field (IMF). Furthermore, little to no plasma depletion is seen during some periods with stable northward IMF. The consistently low value of plasma , the ratio of plasma pressure to magnetic pressure, at the magnetopause associated with the low average upstream M-A is believed to be the cause for the high average reconnection rate at Mercury, reported to be nearly 3 times that observed at Earth. Finally, a characteristic depletion length outward from the subsolar magnetopause of similar to 300km is found for Mercury. This value scales among planetary bodies as the average standoff distance of the magnetopause. C1 [Gershman, Daniel J.; Slavin, James A.; Raines, Jim M.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Gershman, Daniel J.] NASA, Geospace Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [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. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. RP Gershman, DJ (reprint author), NASA, Geospace Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM djgersh@umich.edu RI Slavin, James/H-3170-2012 OI Slavin, James/0000-0002-9206-724X FU NASA Postdoctoral Program at Goddard Space Flight Center; NASA Graduate Student Research Program; MESSENGER mission; NASA [NAS5-97271, NASW-00002] FX D.J.G. is supported by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities. In addition, this work was supported by the NASA Graduate Student Research Program (J.M.R.) and the MESSENGER mission. 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. NR 81 TC 25 Z9 25 U1 0 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 NOV PY 2013 VL 118 IS 11 BP 7181 EP 7199 DI 10.1002/2013JA019244 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 293SB UT WOS:000329992900031 ER PT J AU Oberheide, J Mlynczak, MG Mosso, CN Schroeder, BM Funke, B Maute, A AF Oberheide, J. Mlynczak, M. G. Mosso, C. N. Schroeder, B. M. Funke, B. Maute, A. TI Impact of tropospheric tides on the nitric oxide 5.3 mu m infrared cooling of the low-latitude thermosphere during solar minimum conditions SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE nonmigrating tides; thermospheric energy budget; nitric oxide cooling; volume emission rates; SABER ID NONMIGRATING DIURNAL TIDES; UPPER-ATMOSPHERE; APRIL 2002; ART.; EMISSION; STORMS; MODEL AB This paper explores the impact of diurnal tides that begin near the surface as heat is released by evaporation and condensation on Earth's upper atmosphere natural thermostat: the nitric oxide (NO) infrared cooling of the thermosphere at 5.3 m. Equatorial NO volume emission rate measurements from 100 to 180 km made by Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) on TIMED during the solar minimum year 2008 are analyzed on two important nonmigrating tides, the DE2 and DE3 components. DE3 (DE2) amplitudes maximize around 125 km altitude and, depending on season, are on the order of 0.18 (0.16) nW/m(3). This represents a substantial modulation of the mean NO emission that maximizes in the same altitude range with a value of about 0.8nW/m(3). Tropospheric tides are therefore important not only for the dynamics and electrodynamics of the ionosphere-thermosphere system but also for modulating the thermospheric energy budget. Supporting photochemical tidal modeling indicates that the main tidal coupling mechanism is the temperature dependence of the collisional excitation of the NO (=1) vibrational state. However, the response to vertical tidal advection is also important. It is in-phase with the response to temperature and contributes as much as 50% to the NO tides at and above the emission maximum. Neutral density tidal variations contribute about 25% but with a 9 h phase offset resulting in a net damping. These results imply that NO 5.3 m emissions are a suitable proxy for studying tidal dynamics in the thermosphere where no global temperature measurements are available. C1 [Oberheide, J.; Mosso, C. N.; Schroeder, B. M.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Mlynczak, M. G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Funke, B.] CSIC, Inst Astrofis Andalucia, Granada, Spain. [Maute, A.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. RP Oberheide, J (reprint author), Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. EM joberhe@clemson.edu RI Oberheide, Jens/C-6156-2011; Funke, Bernd/C-2162-2008 OI Oberheide, Jens/0000-0001-6721-2540; Funke, Bernd/0000-0003-0462-4702 FU National Science Foundation (NSF) [AGS1112704, AGS1139048]; NASA TIMED Project; NASA Living with a Star program; Spanish MINECO [AYA2011-23552]; EC FEDER funds; NSF [AGS1138784]; NASA [NNX13AAF77G]; National Science Foundation FX We thank Linda A. Hunt for helpful discussions and Wenbin Wang for comments on an initial draft of the manuscript. J.O., C.N.M., and B. M. S. were supported by grants from the National Science Foundation (NSF), AGS1112704 and AGS1139048. M. G. M. acknowledges support from the NASA TIMED Project and the NASA Living with a Star program. B. F. was supported by the Spanish MINECO under grant AYA2011-23552 and EC FEDER funds. A. M. was supported in part by NSF grant AGS1138784 and NASA grant NNX13AAF77G. The National Center for Atmospheric Research is operated by the University Corporation for Atmospheric Research under the sponsorship of the National Science Foundation. NR 43 TC 5 Z9 5 U1 1 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 NOV PY 2013 VL 118 IS 11 BP 7283 EP 7293 DI 10.1002/2013JA019278 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 293SB UT WOS:000329992900041 ER PT J AU Peterson, WK Brain, DA Mitchell, DL Bailey, SM Chamberlin, PC AF Peterson, W. K. Brain, D. A. Mitchell, D. L. Bailey, S. M. Chamberlin, P. C. TI Correlations between variations in solar EUV and soft X-ray irradiance and photoelectron energy spectra observed on Mars and Earth SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE photoelectrons; Mars; solar irradiance variability; Earth ID AE-E MEASUREMENTS; ATMOSPHERE EXPLORER; IONOSPHERIC STORMS; MINIMUM CONDITIONS; ELECTRON; DENSITY; REFLECTOMETER; MODELS; FIELDS; PEAKS AB Solar extreme ultraviolet (EUV; 10-120nm) and soft X-ray (XUV; 0-10nm) radiation are major heat sources for the Mars thermosphere as well as the primary source of ionization that creates the ionosphere. In investigations of Mars thermospheric chemistry and dynamics, solar irradiance models are used to account for variations in this radiation. Because of limited proxies, irradiance models do a poor job of tracking the significant variations in irradiance intensity in the EUV and XUV ranges over solar rotation time scales when the Mars-Sun-Earth angle is large. Recent results from Earth observations show that variations in photoelectron energy spectra are useful monitors of EUV and XUV irradiance variability. Here we investigate photoelectron energy spectra observed by the Mars Global Surveyor (MGS) Electron Reflectometer (ER) and the FAST satellite during the interval in 2005 when Earth, Mars, and the Sun were aligned. The Earth photoelectron data in selected bands correlate well with calculations based on 1nm resolution observations above 27nm supplemented by broadband observations and a solar model in the 0-27nm range. At Mars, we find that instrumental and orbital limitations to the identifications of photoelectron energy spectra in MGS/ER data preclude their use as a monitor of solar EUV and XUV variability. However, observations with higher temporal and energy resolution obtained at lower altitudes on Mars might allow the separation of the solar wind and ionospheric components of electron energy spectra so that they could be used as reliable monitors of variations in solar EUV and XUV irradiance than the time shifted, Earth-based, F-10.7 index currently used. C1 [Peterson, W. K.; Brain, D. A.] Univ Colorado, LASP, Boulder, CO 80303 USA. [Mitchell, D. L.] Univ Calif Berkeley, SSL, Berkeley, CA 94720 USA. [Bailey, S. M.] Virginia Polytech Inst & State Univ, Baradley Sch Engn, Blacksburg, VA 24061 USA. [Chamberlin, P. C.] NASA Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD USA. RP Peterson, WK (reprint author), Univ Colorado, LASP, Boulder, CO 80303 USA. EM bill.peterson@lasp.colorado.edu RI Chamberlin, Phillip/C-9531-2012; Peterson, WK/A-8706-2009 OI Chamberlin, Phillip/0000-0003-4372-7405; Peterson, WK/0000-0002-1513-6096 FU NASA [NNX12AD25G] FX We thank Ian Stewart, Jane Fox, Jim McFadden, and Phil Richards for data, models, and discussions. We thank the SOHO EIT team for images used in Figure 1. The GOES X-ray observations and indices in Figure 2 are from the NOAA SPIDR web site. We thank one of the reviewers for his/her constructive comments. W. K. P. was supported by NASA Grant NNX12AD25G. NR 35 TC 8 Z9 8 U1 0 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 NOV PY 2013 VL 118 IS 11 BP 7338 EP 7347 DI 10.1002/2013JA019251 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 293SB UT WOS:000329992900046 ER PT J AU Coustenis, A Atreya, S Castillo, J Coll, P Mueller-Wodarg, I Spilker, L AF Coustenis, A. Atreya, S. Castillo, J. Coll, P. Mueller-Wodarg, I. Spilker, L. TI Surfaces, atmospheres and magnetospheres of the outer planets and their satellites and ring systems: Part IX SO PLANETARY AND SPACE SCIENCE LA English DT Editorial Material C1 [Coustenis, A.] Observ Paris, LESIA, F-92195 Meudon, France. [Atreya, S.] Univ Michigan, Ann Arbor, MI 48109 USA. [Castillo, J.; Spilker, L.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Coll, P.] Univ Paris 07, LISA, Paris Est Creteil, France. [Coll, P.] Hop Henri Mondor, CNRS, F-94010 Creteil, France. [Mueller-Wodarg, I.] Univ London Imperial Coll Sci Technol & Med, London, England. RP Coustenis, A (reprint author), Observ Paris, LESIA, F-92195 Meudon, France. EM athena.coustenis@obspm.fr RI Mueller-Wodarg, Ingo/M-9945-2014 OI Mueller-Wodarg, Ingo/0000-0001-6308-7826 NR 0 TC 1 Z9 1 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD NOV PY 2013 VL 88 SI SI BP 1 EP 2 DI 10.1016/j.pss.2013.10.010 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 287KI UT WOS:000329540300001 ER PT J AU Zhang, X Nixon, CA Shia, RL West, RA Irwin, PGJ Yelle, RV Allen, MA Yung, YL AF Zhang, X. Nixon, C. A. Shia, R. L. West, R. A. Irwin, P. G. J. Yelle, R. V. Allen, M. A. Yung, Y. L. TI Radiative forcing of the stratosphere of Jupiter, Part I: Atmospheric cooling rates from Voyager to Cassini SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Jupiter atmosphere; Outer planets; Abundance retrieval; Radiative transfer; Energy balance ID COLLISION-INDUCED ABSORPTION; INDUCED INFRARED-SPECTRA; PROBE MASS-SPECTROMETER; H-2-HE PAIRS; JOVIAN STRATOSPHERE; THERMAL STRUCTURE; GRAVITY-WAVES; TEMPERATURES; METHANE; GALILEO AB We developed a line-by-line heating and cooling rate model for the stratosphere of Jupiter, based on two complete sets of global maps of temperature. C2H2 and C2H6, retrieved from the Cassini and Voyager observations in the latitude and vertical plane, with a careful error analysis. The non-LTE effect is found unimportant on the thermal cooling rate below the 0.01 mbar pressure level. The most important coolants are molecular hydrogen between 10 and 100 mbar, and hydrocarbons, including ethane (C2H6), acetylene (C2H2) and methane (CH4), in the region above. The two-dimensional cooling rate maps are influenced primarily by the temperature structure, and also by the meridional distributions of C2H2 and C2H6. The temperature anomalies at the 1 mbar pressure level in the Cassini data and the strong C2H6 latitudinal contrast in the Voyager epoch are the two most prominent features influencing the cooling rate patterns, with the effect from the 'quasi-quadrennial oscillation (QQO)' thermal structures at -20 mbar. The globally averaged CH4 heating and cooling rates are not balanced, clearly in the lower stratosphere under 10 mbar, and possibly in the upper stratosphere above the 1 mbar pressure level. Possible heating sources from the gravity wave breaking and aerosols are discussed. The radiative relaxation timescale in the lower stratosphere implies that the temperature profile might not be purely radiatively controlled. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Zhang, X.; Shia, R. L.; Allen, M. A.; Yung, Y. L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Nixon, C. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [West, R. A.; Allen, M. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Irwin, P. G. J.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. [Yelle, R. V.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. RP Zhang, X (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM xiz@gps.caltech.edu RI Nixon, Conor/A-8531-2009; OI Nixon, Conor/0000-0001-9540-9121; Irwin, Patrick/0000-0002-6772-384X FU Outer Planets Research program via NASA [JPL.1452240]; NASA Cassini Mission; NASA [NNX09AB72G]; United Kingdom Science and Technology Facilities Council FX We thank V. Meadows for the latest CH4 absorption data, G. Orton for the updated hydrogen-brodened C2H2 and C2H6 line list, T. Greathouse, T. Dowling, L Brown, R. Morales-Juberias, and M. Line for discussions and two anonymous refrees for helpful reviews. This research was supported by the Outer Planets Research program via NASA grant JPL.1452240 to the California Institute of Technology. CAN was supported in part by NASA Cassini Mission. RLS and YLY were supported in part by NASA NNX09AB72G grant to the California Institute of Technology. PGJI was supported in part by the United Kingdom Science and Technology Facilities Council. The digital data files of the retrieved temperatures, gas abundances, and cooling rates are available in the online supplementary materials. NR 84 TC 6 Z9 6 U1 0 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD NOV PY 2013 VL 88 SI SI BP 3 EP 25 DI 10.1016/j.pss.2013.07.005 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 287KI UT WOS:000329540300002 ER PT J AU Sittler, EC Cooper, JF Hartle, RE Paterson, WR Christian, ER Lipatov, AS Mahaffy, PR Paschalidis, NP Coplan, MA Cassidy, TA Richardson, JD Fegley, B Andre, N AF Sittler, E. C., Jr. Cooper, J. F. Hartle, R. E. Paterson, W. R. Christian, E. R. Lipatov, A. S. Mahaffy, P. R. Paschalidis, N. P. Coplan, M. A. Cassidy, T. A. Richardson, J. D. Fegley, B., Jr. Andre, N. TI Plasma ion composition measurements for Europa SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Europa Magnetospheric interaction; Ionospheric currents; Surface composition; Oceanic fields ID INFRARED MAPPING SPECTROMETER; ELECTRIC-FIELD MEASUREMENTS; NEUTRAL MASS-SPECTROMETER; SUBSURFACE OCEAN; JOVIAN MAGNETOSPHERE; INNER MAGNETOSPHERE; VOLCANIC GASES; SULFURIC-ACID; ENERGETIC ION; DOUBLE PROBES AB Jupiter magnetospheric interactions and surface composition, both important to subsurface ocean detection for the Galilean icy moons Europa, Ganymede, and Callisto, can be measured using plasma ion mass spectrometry on either an orbiting spacecraft or one designed for multiple flybys of these moons. Detection of emergent oceanic materials at the Europa surface is more likely than at Ganymede and Callisto. A key challenge is to resolve potential intrinsic Europan materials from the space weathering patina of iogenic species implanted onto the sensible surface by magnetospheric interactions. Species-resolved measurements of pickup ion currents are also critical to extraction of oceanic induced magnetic fields from magnetospheric interaction background dominated by these currents. In general the chemical astrobiological potential of Europa should be determined through the combination of surface, ionospheric, and pickup ion composition measurements. The requisite Ion Mass Spectrometer (IMS) for these measurements would need to work in the high radiation environment of Jupiter's magnetosphere between the orbits of Europa and Ganymede, and beyond. A 3D hybrid model of the moon-magnetosphere interaction is also needed to construct a global model of the electric and magnetic fields, and the plasma environment, around Europa. Europa's ionosphere is probably usually dominated by hot pickup ions with 100-1000 eV temperatures, excursions to a "classical" cold ionosphere likely being infrequent. A field aligned ionospheric wind driven by the electron polarization electric field should arise and be measurable. Published by Elsevier Ltd. C1 [Sittler, E. C., Jr.; Cooper, J. F.; Hartle, R. E.; Paterson, W. R.; Christian, E. R.; Mahaffy, P. R.; Paschalidis, N. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lipatov, A. S.] Univ Maryland Baltimore Cty, GPHI, Baltimore, MD 21228 USA. [Coplan, M. A.] Univ Maryland, College Pk, MD 20742 USA. [Cassidy, T. A.] Univ Colorado, LASP, Boulder, CO 80309 USA. [Richardson, J. D.] MIT, Cambridge, MA 02139 USA. [Fegley, B., Jr.] Washington Univ, St Louis, MO USA. [Andre, N.] CESR IRAP, Toulouse, France. RP Sittler, EC (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Edward.C.Sittler@nasa.gov RI Cooper, John/D-4709-2012 FU NASA Astrobiology Instrument Development (ASTID); Outer Planets Research (OPR) FX This work has been supported under the NASA Astrobiology Instrument Development (ASTID) and Outer Planets Research (OPR) programs. NR 96 TC 5 Z9 5 U1 0 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD NOV PY 2013 VL 88 SI SI BP 26 EP 41 DI 10.1016/j.pss.2013.01.013 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 287KI UT WOS:000329540300003 ER PT J AU Kharuk, VI Ranson, KJ Im, ST Oskorbin, PA Dvinskaya, ML Ovchinnikov, DV AF Kharuk, Viacheslav I. Ranson, Kenneth J. Im, Sergey T. Oskorbin, Pavel A. Dvinskaya, Maria L. Ovchinnikov, Dmitriy V. TI Tree-Line Structure and Dynamics at the Northern Limit of the Larch Forest: Anabar Plateau, Siberia, Russia SO ARCTIC ANTARCTIC AND ALPINE RESEARCH LA English DT Article ID GLACIER-NATIONAL-PARK; SWEDISH SCANDES; CLIMATE-CHANGE; SOUTHERN SIBERIA; PINUS-SYLVESTRIS; POLAR URALS; USA; 20TH-CENTURY; TEMPERATURE; PERSPECTIVE AB The goal of the study was to provide an analysis of climate impact before, during, and after the Little Ice Age (LIA) on the larch (Larix gmelinii) tree line at the northern extreme of Siberian forests. Recent decadal climate change impacts on the tree line, regeneration abundance, and age structure were analyzed. The location of the study area was within the forest-tundra ecotone (elevation range 170-450 m) in the Anabar Plateau, northern Siberia. Field studies were conducted along elevational transects. Tree natality/mortality and radial increment were determined based on dendrochronology analyses. Tree morphology, number of living and subfossil trees, regeneration abundance, and age structure were studied. Locations of pre-LIA, LIA, and post-LIA tree lines and refugia boundaries were established. Long-term climate variables and drought index were included in the analysis. It was found that tree mortality from the 16th century through the beginning of the 19th century caused a downward tree line recession. Sparse larch stands experienced deforestation, transforming into tundra with isolated relict trees. The maximum tree mortality and radial growth decrease were observed to have occurred at the beginning of 18th century. Now larch, at its northern boundary in Siberia, is migrating into tundra areas. Upward tree migration was induced by warming in the middle of the 19th century. Refugia played an important role in repopulation of the forest-tundra ecotone by providing a seed source and shelter for recruitment of larch regeneration. Currently this ecotone is being repopulated mainly by tree cohorts that were established after the 1930s. The last two decades of warming did not result in an acceleration of regeneration recruitment because of increased drought conditions. The regeneration line reached (but did not exceed) the pre-LIA tree line location, although contemporary tree heights and stand densities are comparatively lower than in the pre-LIA period. The mean rate of tree line upward migration has been about 0.35 m yr(-1) (with a range of 0.21-0.58), which translates to a tree line response to temperature of about 55 m degrees C-1. C1 [Kharuk, Viacheslav I.; Im, Sergey T.; Oskorbin, Pavel A.; Dvinskaya, Maria L.; Ovchinnikov, Dmitriy V.] VN Sukachev Inst Forest, Krasnoyarsk 660036, Russia. [Ranson, Kenneth J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kharuk, VI (reprint author), VN Sukachev Inst Forest, Krasnoyarsk 660036, Russia. EM kharuk@ksc.krasn.ru RI Ranson, Kenneth/G-2446-2012; Im, Sergei/J-2736-2016 OI Ranson, Kenneth/0000-0003-3806-7270; Im, Sergei/0000-0002-5794-7938 FU Siberian Branch of the Russian Academy of Sciences [30.33]; NASA's Earth Science Division FX This work was supported in part by the Siberian Branch of the Russian Academy of Sciences (#30.33) and NASA's Earth Science Division. Thanks to Joanne Howl for assistance with editing the manuscript. NR 44 TC 7 Z9 8 U1 3 U2 23 PU INST ARCTIC ALPINE RES PI BOULDER PA UNIV COLORADO, BOULDER, CO 80309 USA SN 1523-0430 EI 1938-4246 J9 ARCT ANTARCT ALP RES JI Arct. Antarct. Alp. Res. PD NOV PY 2013 VL 45 IS 4 BP 526 EP 537 DI 10.1657/1938-4246-45.4.526 PG 12 WC Environmental Sciences; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 287HT UT WOS:000329533400009 ER PT J AU Balestra, I Vanzella, E Rosati, P Monna, A Grillo, C Nonino, M Mercurio, A Biviano, A Bradley, L Coe, D Fritz, A Postman, M Seitz, S Scodeggio, M Tozzi, P Zhengll, W Ziegler, B Zitrin, A Annunziatella, M Bartelmann, M Benitez, N Broadhurst, T Bouwens, R Czoske, O Donahue, M Ford, H Girardi, M Infante, L Jouvel, S Kelson, D Koekemoer, A Kuchner, U Lemze, D Lombardi, M Maier, C Medezinski, E Melchior, P Meneghetti, M Merten, J Molino, A Moustakas, L Presotto, V Smit, R Umetsu, K AF Balestra, I. Vanzella, E. Rosati, P. Monna, A. Grillo, C. Nonino, M. Mercurio, A. Biviano, A. Bradley, L. Coe, D. Fritz, A. Postman, M. Seitz, S. Scodeggio, M. Tozzi, P. Zhengll, W. Ziegler, B. Zitrin, A. Annunziatella, M. Bartelmann, M. Benitez, N. Broadhurst, T. Bouwens, R. Czoske, O. Donahue, M. Ford, H. Girardi, M. Infante, L. Jouvel, S. Kelson, D. Koekemoer, A. Kuchner, U. Lemze, D. Lombardi, M. Maier, C. Medezinski, E. Melchior, P. Meneghetti, M. Merten, J. Molino, A. Moustakas, L. Presotto, V. Smit, R. Umetsu, K. TI CLASH-VLT: spectroscopic confirmation of z=6.11 quintuply lensed galaxy in the Frontier Fields cluster RXC J2248.7-4431 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gravitational lensing: strong; galaxies: high-redshift ID LYMAN-BREAK GALAXIES; STAR-FORMING GALAXIES; SIMILAR-TO 8; EXTRAGALACTIC LEGACY SURVEY; GOODS-SOUTH FIELD; LUMINOSITY FUNCTION; ESCAPE FRACTION; BRIGHT END; REDSHIFT; CONSTRAINTS AB We present VIsible Multi-Object Spectrograph (VIMOS) observations of a z similar to 6 galaxy quintuply imaged by the Frontier Fields galaxy cluster RXC J2248.7-4431 (z = 0.348). This sub-L*, high-z galaxy has been recently discovered by Monna et al. (2013) using dropout techniques with the 16-band HST photometry acquired as part of the Cluster Lensing And Supernova survey with Hubble (CLASH). Obtained as part of the CLASH-VLT survey, the VIMOS medium-resolution spectra of this source show a very faint continuum between similar to 8700 angstrom and similar to 9300 angstrom and a prominent emission line at 8643 angstrom, which can be readily identified with Lyman-alpha at z = 6.110 +/- 0.002. The emission line exhibits an asymmetric profile, with a more pronounced red wing. The rest-frame equivalent width of the line is EW = 79 +/- 10 angstrom, relatively well constrained thanks to the detection of the UV continuum, which is rarely achieved for a sub-L* galaxy at this redshift. After correcting for magnification, the star formation rate (SFR) estimated from the Ly alpha line is SFR(Ly alpha) = 11 M-circle dot yr(-l) and that estimated from the UV data is SFR(UV) = 3 M-circle dot yr(-1). We estimate that the effective radius of the source is R-e less than or similar to 0.4 kpc, which implies a star formation surface mass density Sigma(SFR) > 6 M(circle dot)yr(-1) kpc(-2) and, using the Kennicutt-Schmidt relation, a gas surface mass density Sigma(gas) > 10(3) M(circle dot)pc(-2). Our results support the idea that this magnified, distant galaxy is a young and compact object with luminosity 0.4 L* at z = 6, when the Universe was just 1 Gyr old, with a similar amount of mass in gas and stars. In the spirit of the Frontier Fields initiative, we also publish the redshifts of several multiply imaged sources and other background objects, which will help improving the strong-lensing model of this galaxy cluster. C1 [Balestra, I.; Nonino, M.; Biviano, A.; Annunziatella, M.; Girardi, M.] INAF Osservatorio Astron Trieste, I-34131 Trieste, Italy. [Balestra, I.; Mercurio, A.] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy. [Vanzella, E.; Meneghetti, M.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Rosati, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy. [Monna, A.; Seitz, S.] Univ Observ Munich, D-81679 Munich, Germany. [Grillo, C.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Bradley, L.; Coe, D.; Postman, M.; Koekemoer, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Fritz, A.; Scodeggio, M.] INAF IASF Milano, I-20133 Milan, Italy. [Tozzi, P.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Seitz, S.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Zhengll, W.; Ford, H.; Lemze, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Ziegler, B.; Czoske, O.; Kuchner, U.; Maier, C.] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Zitrin, A.; Bartelmann, M.] Heidelberg Univ, D-69120 Heidelberg, Germany. [Annunziatella, M.; Girardi, M.; Presotto, V.] Univ Trieste, Dipartimento Fis, I-34143 Trieste, Italy. [Benitez, N.; Molino, A.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Broadhurst, T.] Univ Basque Country, Dept Theoret Phys, Bilbao 48080, Spain. [Bouwens, R.; Smit, R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Kelson, D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Meneghetti, M.] INFN Bologna, I-40127 Bologna, Italy. [Lombardi, M.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy. [Medezinski, E.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Jouvel, S.] CSIC, Inst Ciencies Espai IEEC, Bellaterra 08193, Barcelona, Spain. [Infante, L.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Melchior, P.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Merten, J.; Moustakas, L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. RP Balestra, I (reprint author), INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34131 Trieste, Italy. EM italobale@gmail.com RI Molino Benito, Alberto/F-5298-2014; Grillo, Claudio/E-6223-2015; Meneghetti, Massimo/O-8139-2015; OI Tozzi, Paolo/0000-0003-3096-9966; Benitez, Narciso/0000-0002-0403-7455; Grillo, Claudio/0000-0002-5926-7143; Meneghetti, Massimo/0000-0003-1225-7084; Balestra, Italo/0000-0001-9660-894X; Maier, Christian/0000-0001-6405-2182; Vanzella, Eros/0000-0002-5057-135X; Umetsu, Keiichi/0000-0002-7196-4822; Biviano, Andrea/0000-0002-0857-0732; LOMBARDI, MARCO/0000-0002-3336-4965; Moustakas, Leonidas/0000-0003-3030-2360; Koekemoer, Anton/0000-0002-6610-2048 FU DFG Cluster of Excellence Origin Structure of the Universe; Baden-Wurttemberg Stiftung FX We thank the anonymous referee for the valuable comments and suggestions. We acknowledge partial support by the DFG Cluster of Excellence Origin Structure of the Universe. A.Z. is supported by contract research "Internationale Spitzenforschung II/2-6" of the Baden-Wurttemberg Stiftung. NR 31 TC 21 Z9 21 U1 1 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 NOV PY 2013 VL 559 AR L9 DI 10.1051/0004-6361/201322620 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263ZR UT WOS:000327847200147 ER PT J AU de Val-Borro, M Kuppers, M Hartogh, P Rezac, L Biver, N Bockelee-Morvan, D Crovisier, J Jarchow, C Villanueva, GL AF de Val-Borro, M. Kueppers, M. Hartogh, P. Rezac, L. Biver, N. Bockelee-Morvan, D. Crovisier, J. Jarchow, C. Villanueva, G. L. TI A survey of volatile species in Oort cloud comets C/2001 Q4 (NEAT) and C/2002 T7 (LINEAR) at millimeter wavelengths SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE comets: individual: C/2002 T7 (LINEAR); comets: individual: C/2001 Q4 (NEAT); submillimeter: planetary systems; techniques: spectroscopic; molecular processes ID CHIRP TRANSFORM SPECTROMETER; WATER OUTGASSING RATE; HALE-BOPP; RADIO OBSERVATIONS; 103P/HARTLEY 2; DEEP IMPACT; FORMALDEHYDE EMISSION; RADIATIVE-TRANSFER; PARENT MOLECULES; UPPER LIMIT AB Context. The chemical composition of comets can be inferred using spectroscopic observations in submillimeter and radio wavelengths. Aims. We aim to compare the production rates ratio of several volatiles in two comets, C/2001 Q4 (NEAT) and C/2002 T7 (LINEAR), which are generally regarded as dynamically new and likely to originate in the Oort cloud. This type of comets is considered to be composed of primitive material that has not undergone considerable thermal processing. Methods. The line emission in the coma was measured in the comets, C/2001 Q4 (NEAT) and C/2002 T7 (LINEAR), that were observed on five consecutive nights, 7-11 May 2004, at heliocentric distances of 1.0 and 0.7 AU, respectively, by means of high-resolution spectroscopy using the 10-m Submillimeter Telescope at the Arizona Radio Observatory. Both objects became very bright and reached naked-eye visibility during their perihelion passage in the spring of 2004. Results. We present a search for six parent-and product-volatile species (HCN, H2CO, CO, CS, CH3OH, and HNC) in both comets. Multiline observations of the CH3OH J = 5-4 series allow us to estimate the rotational temperature using the rotation diagram technique. We derive rotational temperatures of 54(9) K for C/2001 Q4 (NEAT) and 119(34) K for C/2002 T7 (LINEAR). The gas production rates are computed using the level distribution obtained with a spherically symmetric molecular excitation code that includes collisions between neutrals and electrons. The effects of radiative pumping of the fundamental vibrational levels by infrared photons from the Sun are considered for the case of HCN. We find an HCN production rate of 2.96(5) x 10(26) molec.s(-1) for comet C/2001 Q4 (NEAT), corresponding to a mixing ratio with respect to H2O of 1.12(2) x 10(-3). The mean HCN production rate during the observing period is 4.54(10) x 10(26) molec.s(-1) for comet C/2002 T7 (LINEAR), which gives a mixing ratio of 1.51(3) x 10(-3). Relative abundances of CO, CH3OH, H2CO, CS, and HNC with respect to HCN are 3.05(83) x 10(1), 1.50(25) x 10(1), 1.16(27), 7.02(30) x 10(1), and 5.75(73) x 10(-2) in comet C/2001 Q4 (NEAT) and < 4.12 x 10(1), 4.07(44) x 10(1), 4.72(73), 1.32(6), and 1.09(8) x 10(1) in comet C/2002 T7 (LINEAR). Conclusions. With systematically lower mixing ratios in comet C/2001 Q4 (NEAT), production rate ratios of the observed species with respect to H2O lie within the typical ranges of dynamically new comets in both objects. We find a relatively low abundance of CO in C/2001 Q4 (NEAT) compared to the observed range in other comets based on millimeter/submillimeter observations, and a significant upper limit on the CO production in C/2002 T7 (LINEAR) is derived. Depletion of CO suggests partial evaporation from the surface layers during previous visits to the outer solar system and agrees with previous measurements of dynamically new comets. Rotational temperatures derived from CH3OH rotational diagrams in both C/2001 Q4 (NEAT) and C/2002 T7 (LINEAR) are roughly consistent with observations of other comets at similar distances from the Sun. C1 [de Val-Borro, M.; Hartogh, P.; Rezac, L.; Jarchow, C.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [de Val-Borro, M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Kueppers, M.] European Space Agcy, European Space Astron Ctr, Rosetta Sci Operat Ctr, Villanueva De La Canada 28691, Spain. [Biver, N.; Bockelee-Morvan, D.; Crovisier, J.] Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris, F-92195 Meudon, France. [Villanueva, G. L.] 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 de Val-Borro, M (reprint author), Max Planck Inst Solar Syst Res, Max Planck Str 2, D-37191 Katlenburg Lindau, Germany. EM valborro@princeton.edu; michael.kueppers@sciops.esa.int; hartogh@mps.mpg.de; rezac@mps.mpg.de; nicolas.biver@obspm.fr; dominique.bockelee@obspm.fr; jacques.crovisier@obspm.fr; jarchow@mps.mpg.de; Geronimo.Villanueva@nasa.gov FU German Science Foundation; NSF [AST-1108686]; NASA [NNX12AH91H] FX Results presented in this paper are based on observations at the SMT which is operated by the Arizona Radio Observatory (ARO), Steward Observatory, University of Arizona. We are grateful to the ARO staff for their expertise and support during these observations, and to M. Drahus for valuable comments that improved the manuscript. We gratefully acknowledge useful discussions about the spectroscopic analysis package pyspeckit with Adam G. Ginsburg. The anonymous referee is thanked for useful and positive feedback. MdVB acknowledges support from the Special Priority Program 1488 (PlanetMag, http://www.planetmag.de) of the German Science Foundation and partial support from grants NSF AST-1108686 and NASA NNX12AH91H. NR 81 TC 2 Z9 2 U1 0 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2013 VL 559 AR A48 DI 10.1051/0004-6361/201322284 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263ZR UT WOS:000327847200048 ER PT J AU Galametz, A Stern, D Pentericcil, L De Breuck, C Vernet, J Wylezalek, D Fassbender, R Hatch, N Kurk, J Overzier, R Rettura, A Seymour, N AF Galametz, Audrey Stern, Daniel Pentericcil, Laura De Breuck, Carlos Vernet, Joel Wylezalek, Dominika Fassbender, Rene Hatch, Nina Kurk, Jaron Overzier, Roderik Rettura, Alessandro Seymour, Nick TI A large-scale galaxy structure at z=2.02 associated with the radio galaxy MRC 0156-252 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual: MRC 0156-252; large-scale structure of Universe; galaxies: individual: MRC 0156-252 ID ACTIVE GALACTIC NUCLEI; X-RAY-EMISSION; LY-ALPHA EMITTERS; HIGH-REDSHIFT; PROTO-CLUSTER; SPECTROSCOPIC CONFIRMATION; MIDINFRARED SELECTION; ELLIPTIC GALAXIES; DISTANT CLUSTER; RED GALAXIES AB We present the spectroscopic confirmation of a structure of galaxies surrounding the radio galaxy MRC 0156-252 at z = 2.02. The structure was initially discovered as an overdensity of both near-infrared selected z > 1.6 and mid-infrared selected z > 1.2 galaxy candidates. We used the VLT/FORS2 multi-object spectrograph to target similar to 80 high-redshift galaxy candidates, and obtain robust spectroscopic redshifts for more than half the targets. The majority of the confirmed sources are star-forming galaxies at z > 1.5. In addition to the radio galaxy, two of its close-by companions (<6 '') also show AGN signatures. Ten sources, including the radio galaxy, lie within vertical bar z - 2.020 vertical bar < 0.015 (i.e., velocity offsets < 1500 km s(-1)) and within projected 2 Mpc comoving of the radio galaxy. Additional evidence suggests not only that the galaxy structure associated with MRC 0156-252 is a forming galaxy cluster but also that this structure is most probably embedded in a larger-scale structure. C1 [Galametz, Audrey; Pentericcil, Laura; Fassbender, Rene] INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [De Breuck, Carlos; Vernet, Joel; Wylezalek, Dominika] European So Observ, D-85748 Garching, Germany. [Hatch, Nina] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Fassbender, Rene; Kurk, Jaron] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Overzier, Roderik] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil. [Overzier, Roderik] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Rettura, Alessandro] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Seymour, Nick] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. RP Galametz, A (reprint author), INAF Osservatorio Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy. EM galametz@oa-roma.inaf.it OI Fassbender, Rene/0000-0001-7489-0702; Hatch, Nina/0000-0001-5600-0534; Vernet, Joel/0000-0002-8639-8560; Seymour, Nicholas/0000-0003-3506-5536; De Breuck, Carlos/0000-0002-6637-3315 FU European Southern Observatory using the Very Large Telescope on Cerro Paranal through ESO programme [090.A-0734] FX Based on observations obtained at the European Southern Observatory using the Very Large Telescope on Cerro Paranal through ESO programme 090.A-0734 (P.I. A. Galametz). NR 69 TC 21 Z9 21 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2013 VL 559 AR UNSP A2 DI 10.1051/0004-6361/201322345 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263ZR UT WOS:000327847200002 ER PT J AU Luna, GJM Sokoloski, JL Mukai, K Nelson, T AF Luna, G. J. M. Sokoloski, J. L. Mukai, K. Nelson, T. TI Symbiotic stars in X-rays SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE binaries: symbiotic; accretion, accretion disks; X-rays: binaries ID ACCRETING WHITE-DWARFS; RADIATION-DRIVEN WINDS; DISK BOUNDARY-LAYERS; NOVA RS OPHIUCHI; CATACLYSMIC VARIABLES; IA SUPERNOVAE; BI-CRUCIS; CH-CYGNI; S-STARS; SPECTROSCOPIC OBSERVATIONS AB Until recently, symbiotic binary systems in which a white dwarf accretes from a red giant were thought to be mainly a soft X-ray population. Here we describe the detection with the X-ray Telescope (XRT) on the Swift satellite of nine white dwarf symbiotics that were not previously known to be X-ray sources and one that had previously been detected as a supersoft X-ray source. The nine new X-ray detections were the result of a survey of 41 symbiotic stars, and they increase the number of symbiotic stars known to be X-ray sources by approximately 30%. The Swift/XRT telescope detected all of the new X-ray sources at energies greater than 2 keV. Their X-ray spectra are consistent with thermal emission and fall naturally into three distinct groups. The first group contains those sources with a single, highly absorbed hard component that we identify as probably coming from an accretion-disk boundary layer. The second group is composed of those sources with a single, soft X-ray spectral component that probably originates in a region where low-velocity shocks produce X-ray emission, i.e., a colliding-wind region. The third group consists of those sources with both hard and soft X-ray spectral components. We also find that unlike in the optical, where rapid, stochastic brightness variations from the accretion disk typically are not seen, detectable UV flickering is a common property of symbiotic stars. Supporting our physical interpretation of the two X-ray spectral components, simultaneous Swift UV photometry shows that symbiotic stars with harder X-ray emission tend to have stronger UV flickering, which is usually associated with accretion through a disk. To place these new observations in the context of previous work on X-ray emission from symbiotic stars, we modified and extended the alpha/beta/gamma classification scheme for symbiotic-star X-ray spectra that was introduced by Muerset et al. based upon observations with the ROSAT satellite, to include a new 6 classification for sources with hard X-ray emission from the innermost accretion region. Because we have identified the elusive accretion component in the emission from a sample of symbiotic stars, our results have implications for the understanding of wind-fed mass transfer in wide binaries, and the accretion rate in one class of candidate progenitors of type Ia supernovae. C1 [Luna, G. J. M.] Inst Astron & Fis Espacio, Buenos Aires, DF, Argentina. [Sokoloski, J. L.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Mukai, K.] NASA GSFC, CRESST & Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Mukai, K.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. [Nelson, T.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55409 USA. RP Luna, GJM (reprint author), Inst Astron & Fis Espacio, CC 67 Suc 28,C1428ZAA Caba, Buenos Aires, DF, Argentina. EM gjmluna@iafe.uba.ar FU PIP-Conicet [D4598]; FONCyT/PICT [269]; SAO [GO1-12041A]; NASA [NNX10AK31G, NNX11AD77G] FX We thank the anonymous referee for comments and suggestions which improved the final quality of this article. We acknowledge the Swift team for planning these observations. G. J. M. Luna is a member of the CIC-CONICET (Argentina) and acknowledges support from grants PIP-Conicet/2011 #D4598 and FONCyT/PICT/2011 #269. J. L. Sokoloski acknowledges support from grants SAO GO1-12041A, NASA NNX10AK31G, and NASA NNX11AD77G. We thank N. Masetti and P. Evans for useful comments that helped to improve the manuscript. NR 108 TC 12 Z9 12 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2013 VL 559 AR UNSP A6 DI 10.1051/0004-6361/201220792 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263ZR UT WOS:000327847200006 ER PT J AU Maturi, M Merten, J AF Maturi, Matteo Merten, Julian TI Weak-lensing detection of intracluster filaments with ground-based data SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: numerical; galaxies: clusters: general; cosmology: observations; large-scale structure of Universe; dark matter ID PRIMORDIAL NON-GAUSSIANITY; DARK-MATTER; COSMIC WEB; NUMBER COUNTS; SHEAR PEAKS; UNIVERSE; GALAXIES; CLUSTERS; SIMULATIONS; PROFILE AB According to the current standard model of cosmology, matter in the Universe arranges itself along a network of filamentary structure. These filaments connect the main nodes of this so-called "cosmic web", which are clusters of galaxies. Although its large-scale distribution is clearly characterized by numerical simulations, constraining the dark-matter content of the cosmic web in reality turns out to be difficult. The natural method of choice is gravitational lensing. However, the direct detection and mapping of the elusive filament signal is challenging and in this work we present two methods that are specifically tailored to achieve this task. A linear matched filter aims at detecting the smooth mass-component of filaments and is optimized to perform a shear decomposition that follows the anisotropic component of the lensing signal. Filaments clearly inherit this property due to their morphology. At the same time, the contamination arising from the central massive cluster is controlled in a natural way. The filament lo-detection is of about kappa similar to 0.01-0.005 according to the filter's template width and length, enabling the detection of structures beyond reach with other approaches. The second, complementary method seeks to detect the clumpy component of filaments. The detection is determined by the number density of subclump identifications in an area enclosing the potential filament, as was found within the observed field with the filter approach. We tested both methods against mocked observations based on realistic N-body simulations of filamentary structure and proved the feasibility of detecting filaments with ground-based data. C1 [Maturi, Matteo] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, D-69120 Heidelberg, Germany. [Merten, Julian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Maturi, M (reprint author), Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, Philosophenweg 12, D-69120 Heidelberg, Germany. EM maturi@uni-heidelberg.de; jmerten@caltech.edu FU Transregional Collaborative Research Centre TRR 33; NASA FX We are grateful to Klaus Dolag for providing us the N-body numerical simulation used in this work and to Massimo Meneghetti for his help in extracting its lensing properties. This work was supported by the Transregional Collaborative Research Centre TRR 33 (M.M.). This research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 37 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 NOV PY 2013 VL 559 AR A112 DI 10.1051/0004-6361/201322007 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263ZR UT WOS:000327847200112 ER PT J AU Morabito, DD D'Addario, LR Acosta, RJ Nessel, JA AF Morabito, David D. D'Addario, Larry R. Acosta, Roberto J. Nessel, James A. TI Tropospheric delay statistics measured by two site test interferometers at Goldstone, California SO RADIO SCIENCE LA English DT Article DE interferometry ID SEEING MONITOR AB Site test interferometers (STIs) have been deployed at two locations within the NASA Deep Space Network tracking complex in Goldstone, California. An STI measures the difference of atmospheric delay fluctuations over a distance comparable to the separations of microwave antennas that could be combined as phased arrays for communication and navigation. The purpose of the Goldstone STIs is to assess the suitability of Goldstone as an uplink array site and to statistically characterize atmosphere-induced phase delay fluctuations for application to future arrays. Each instrument consists of two similar to 1m diameter antennas and associated electronics separated by similar to 200m. The antennas continuously observe signals emitted by geostationary satellites and produce measurements of the phase difference between the received signals. The two locations at Goldstone are separated by 12.5km and differ in elevation by 119m. We find that their delay fluctuations are statistically similar but do not appear as shifted versions of each other, suggesting that the length scale for evolution of the turbulence pattern is shorter than the separation between instruments. We also find that the fluctuations are slightly weaker at the higher altitude site. C1 [Morabito, David D.; D'Addario, Larry R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Acosta, Roberto J.; Nessel, James A.] NASA, Glenn Res Ctr, Cleveland, OH USA. RP Morabito, DD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM David.D.Morabito@jpl.nasa.gov NR 39 TC 7 Z9 7 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0048-6604 EI 1944-799X J9 RADIO SCI JI Radio Sci. PD NOV PY 2013 VL 48 IS 6 BP 729 EP 738 DI 10.1002/2013RS005268 PG 10 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA 290EY UT WOS:000329737900007 ER PT J AU Durrieu, S Nelson, RF AF Durrieu, Sylvie Nelson, Ross F. TI Earth observation from space - The issue of environmental sustainability SO SPACE POLICY LA English DT Article DE Space remote sensing; Earth observation systems; Space junk; Sustainability; Sustainable management; Lidar; Forest; Biomass; Life cycle assessment ID AIRBORNE LASER; FOREST INVENTORY; LIDAR; BIOMASS; RESOURCES; CARBON; INFORMATION; ICESAT/GLAS; INDICATORS; PROTECTION AB Remote sensing scientists work under assumptions that should not be taken for granted and should, therefore, be challenged. These assumptions include the following: 1. Space, especially Low Earth Orbit (LEO), will always be available to governmental and commercial space entities that launch Earth remote sensing missions. 2. Space launches are benign with respect to environmental impacts. 3. Minimization of Type 1 error, which provides increased confidence in the experimental outcome, is the best way to assess the significance of environmental change. 4. Large-area remote sensing investigations, i.e. national, continental, global studies, are best done from space. 5. National space missions should trump international, cooperative space missions to ensure national control and distribution of the data products. At best, all of these points are arguable, and in some cases, they're wrong. Development of observational space systems that are compatible with sustainability principles should be a primary concern when Earth remote sensing space systems are envisioned, designed, and launched. The discussion is based on the hypothesis that reducing the environmental impacts of the data acquisition step, which is at the very beginning of the information stream leading to decision and action, will enhance coherence in the information stream and strengthen the capacity of measurement processes to meet their stated functional goal, i.e. sustainable management of Earth resources. We suggest that unconventional points of view should be adopted and when appropriate, remedial measures considered that could help to reduce the environmental footprint of space remote sensing and of Earth observation and monitoring systems in general. This article discusses these five assumptions in the context of sustainable management of Earth's resources. Taking each assumption in turn, we find the following: (1) Space debris may limit access to Low Earth Orbit over the next decades. (2) Relatively speaking, given that they're rare event, space launches may be benign, but study is merited on upper stratospheric and exospheric layers given the chemical activity associated with rocket combustion by-products. (3) Minimization of Type II error should be considered in situations where minimization of Type I error greatly hampers or precludes our ability to correct the environmental condition being studied. (4) In certain situations, airborne collects may be less expensive and more environmentally benign, and comparative studies should be done to determine which path is wisest. (5) International cooperation and data sharing will reduce instrument and launch costs and mission redundancy. Given fiscal concerns of most of the major space agencies - e.g. NASA, ESA, CNES - it seems prudent to combine resources. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Durrieu, Sylvie] Maison Teledetect Languedoc Roussillon, UMR TETIS Irstea Cirad AgroParisTech ENGREF, F-34196 Montpellier, France. [Nelson, Ross F.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA. RP Durrieu, S (reprint author), Maison Teledetect Languedoc Roussillon, UMR TETIS Irstea Cirad AgroParisTech ENGREF, 500,Rue J F Breton BP 5095, F-34196 Montpellier, France. EM sylvie.durrieu@teledetection.fr; ross.f.nelson@nasa.gov NR 79 TC 3 Z9 3 U1 2 U2 26 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0265-9646 EI 1879-338X J9 SPACE POLICY JI Space Policy PD NOV PY 2013 VL 29 IS 4 BP 238 EP 250 DI 10.1016/j.spacepol.2013.07.003 PG 13 WC International Relations; Social Sciences, Interdisciplinary SC International Relations; Social Sciences - Other Topics GA 287KN UT WOS:000329540800006 ER PT J AU Memarsadeghi, N Rincon, R AF Memarsadeghi, Nargess Rincon, Rafael TI NASA COMPUTATIONAL CASE STUDY: SAR DATA PROCESSING-GROUND-RANGE PROJECTION SO COMPUTING IN SCIENCE & ENGINEERING LA English DT Article C1 [Memarsadeghi, Nargess] NASA, Goddard Space Flight Ctr, Sci Data Syst Branch, Washington, DC USA. [Rincon, Rafael] NASA, Goddard Space Flight Ctr, Microwave Instruments Technol Branch, Greenbelt, MD USA. RP Memarsadeghi, N (reprint author), NASA, Global Learning & Observat Benefit Environm GLOBE, Washington, DC 20546 USA. EM memarsadeghi@nasa.gov; rafael.f.rincon@nasa.gov NR 5 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 1521-9615 EI 1558-366X J9 COMPUT SCI ENG JI Comput. Sci. Eng. PD NOV-DEC PY 2013 VL 15 IS 6 BP 92 EP 95 PG 4 WC Computer Science, Interdisciplinary Applications SC Computer Science GA 275XA UT WOS:000328711500011 ER PT J AU Russell, CT Raymond, CA Jaumann, R McSween, HY De Sanctis, MC Nathues, A Prettyman, TH Ammannito, E Reddy, V Preusker, F O'Brien, DP Marchi, S Denevi, BW Buczkowski, DL Pieters, CM McCord, TB Li, JY Mittlefehldt, DW Combe, JP Williams, DA Hiesinger, H Yingst, RA Polanskey, CA Joy, SP AF Russell, C. T. Raymond, C. A. Jaumann, R. McSween, H. Y. De Sanctis, M. C. Nathues, A. Prettyman, T. H. Ammannito, E. Reddy, V. Preusker, F. O'Brien, D. P. Marchi, S. Denevi, B. W. Buczkowski, D. L. Pieters, C. M. McCord, T. B. Li, J. -Y. Mittlefehldt, D. W. Combe, J. -P. Williams, D. A. Hiesinger, H. Yingst, R. A. Polanskey, C. A. Joy, S. P. TI Dawn completes its mission at 4 Vesta SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID CARBONACEOUS CHONDRITE CLASTS; SURFACE-COMPOSITION; DARK MATERIAL; PARENT BODY; CERES; HETEROGENEITY; MINERALOGY; EVOLUTION; REGOLITH; ORIGIN AB The Dawn mission was designed to test our hypothesis about the origin and evolution of the early solar system by visiting the largest differentiated basaltic asteroid, 4 Vesta, believed to be a survivor from the earliest times of rocky body formation. Observations from orbit show that Vesta is the parent body of the Howardite, Eucrite, Diogenite meteorites. Vesta has an iron core and a eucritic-diogenitic crust. Its surface is characterized by abundant impact craters but with no evident volcanic features. It has two ancient impact basins in the southern hemisphere that are associated with circum-planetary troughs. The northern hemisphere is the more heavily cratered and contains the oldest terrains. The surface of Vesta is diverse, with north-south and east-west dichotomies in the eucrite-to-diogenite ratio. Its surface contains both very bright and very dark material, and its color varies strongly from region to region. Both the mineralogical and the elemental compositions agree with that expected for the HED parent body. Significant OH or H may be present in the upper crust and the presence of pits in fresh craters is consistent with the devolatilization of the surface after a collision either brought to or tapped a source of water on Vesta. The presence of dark material on the surface of Vesta suggests efficient transport pathways for organic material, and the mixing of the dark material with the more pristine pyroxene explains the varying albedo across the surface. Vesta has proven to be a reliable witness to the formation of the solar system. C1 [Russell, C. T.; Joy, S. P.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90096 USA. [Raymond, C. A.; Polanskey, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Jaumann, R.; Preusker, F.] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Planetary Res, D-12489 Berlin, Germany. [McSween, H. Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [De Sanctis, M. C.; Ammannito, E.] Ist Nazl Astrofis, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy. [Nathues, A.; Reddy, V.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Prettyman, T. H.; O'Brien, D. P.; Yingst, R. A.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Marchi, S.] NASA, Lunar Sci Inst, Ctr Lunar Origin & Evolut, Boulder, CO 80302 USA. [Denevi, B. W.; Buczkowski, D. L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Pieters, C. M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [McCord, T. B.; Combe, J. -P.] Bear Fight Inst, Winthrop, WA 98862 USA. [Li, J. -Y.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mittlefehldt, D. W.] NASA, Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA. [Williams, D. A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Hiesinger, H.] Univ Munster, Inst Planetol, D-48149 Munster, Germany. RP Russell, CT (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, 603 Charles Young Dr,3845 Slichter Hall, Los Angeles, CA 90096 USA. EM ctrussell@igpp.ucla.edu RI Denevi, Brett/I-6502-2012; OI Denevi, Brett/0000-0001-7837-6663; De Sanctis, Maria Cristina/0000-0002-3463-4437; Prettyman, Thomas/0000-0003-0072-2831; Reddy, Vishnu/0000-0002-7743-3491 FU Max Planck Society; DLR; NASA/JPL; ASI; Italian Space Agency, Rome; NASA's Dawn at Vesta Participating Scientist program; [NNM05AA86C] FX The success of the Dawn mission is due to the efforts of a large team of engineers, scientists, and administrators in industry and government laboratories both in the United States and abroad. Orbital Sciences Corporation played a major role in the development, integration, and testing of the flight system. The Dawn mission is managed by NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate, Washington DC. UCLA is responsible for overall Dawn mission science. The Dawn framing cameras have been developed and built under the leadership of the Max Planck Institute for Solar System Research, Katlenburg-Lindau, Germany, with significant contributions by DLR German Aerospace Center; Institute of Planetary Research, Berlin; and in coordination with the Institute of Computer and Communication Network Engineering, Braunschweig. The framing camera project is funded by the Max Planck Society, DLR, and NASA/JPL. The VIR visible and infrared mapping spectrometer was developed under the leadership of the Institute for Space Astrophysics and Planetology, Rome, belonging to the Italian National Institute for Astrophysics (INAF), Italy. The instrument was built by Selex-Galileo, Florence, Italy. The VIR project is funded by ASI, the Italian Space Agency, Rome. The GRaND instrument was built by Los Alamos National Laboratory and is operated by the Planetary Science Institute. Several of the co-authors are supported by NASA's Dawn at Vesta Participating Scientist program. C. T. R., H. Y. M., C. M. P., T. B. M., and J. P. C. are supported by the Discovery program through contract NNM05AA86C to the University of California, Los Angeles. A portion of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Dawn data are archived with the NASA Planetary Data System. We thank the Dawn team for the development, cruise, orbital insertion, and operations of the Dawn spacecraft at Vesta. NR 56 TC 30 Z9 31 U1 2 U2 15 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 NOV PY 2013 VL 48 IS 11 BP 2076 EP 2089 DI 10.1111/maps.12091 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 273NY UT WOS:000328543300002 ER PT J AU McSween, HY Binzel, RP De Sanctis, MC Ammannito, E Prettyman, TH Beck, AW Reddy, V Le Corre, L Gaffey, MJ McCord, TB Raymond, CA Russell, CT AF McSween, Harry Y., Jr. Binzel, Richard P. De Sanctis, M. Cristina Ammannito, Eleonora Prettyman, Thomas H. Beck, Andrew W. Reddy, Vishnu Le Corre, Lucille Gaffey, Michael J. McCord, Thomas B. Raymond, Carol A. Russell, Christopher T. CA Dawn Sci Team TI Dawn; the Vesta-HED connection; and the geologic context for eucrites, diogenites, and howardites SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID ASTEROID 4 VESTA; EARLY SOLAR-SYSTEM; PARENT BODY; MN-53-CR-53 SYSTEMATICS; BASALTIC ACHONDRITES; IMPACT SPHERULES; ORTHO-PYROXENE; DARK MATERIAL; METEORITES; ORIGIN AB The Dawn mission has provided new evidence strengthening the identification of asteroid Vesta as the parent body of the howardite, eucrite, and diogenite (HED) meteorites. The evidence includes Vesta's petrologic complexity, detailed spectroscopic characteristics, unique space weathering, diagnostic geochemical abundances and neutron absorption characteristics, chronology of surface units and impact history, occurrence of exogenous carbonaceous chondritic materials in the regolith, and dimensions of the core, all of which are consistent with HED observations and constraints. Global mapping of the distributions of HED lithologies by Dawn cameras and spectrometers provides the missing geologic context for these meteorites, thereby allowing tests of petrogenetic models and increasing their scientific value. C1 [McSween, Harry Y., Jr.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA. [McSween, Harry Y., Jr.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Binzel, Richard P.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [De Sanctis, M. Cristina; Ammannito, Eleonora] Ist Nazl Astrofis, Ist Astrofis & Planetol Spaziali, Rome, Italy. [Prettyman, Thomas H.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Beck, Andrew W.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Reddy, Vishnu; Le Corre, Lucille] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Gaffey, Michael J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA. [McCord, Thomas B.] Bear Fight Inst, Winthrop, WA 98862 USA. [Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. RP McSween, HY (reprint author), Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA. EM mcsween@utk.edu RI Beck, Andrew/J-7215-2015; OI Beck, Andrew/0000-0003-4455-2299; De Sanctis, Maria Cristina/0000-0002-3463-4437; Prettyman, Thomas/0000-0003-0072-2831; Reddy, Vishnu/0000-0002-7743-3491; Le Corre, Lucille/0000-0003-0349-7932 FU NASA's Discovery Program; NASA's Dawn at Vesta Participating Scientists Program; Italian Space Agency; Max Planck Society; German Space Agency (DLR); Planetary Science Institute under Jet Propulsion Laboratory, California Institute of Technology FX This work was funded by NASA's Discovery Program through a contract to the University of California, Los Angeles, by NASA's Dawn at Vesta Participating Scientists Program, by the Italian Space Agency, by the Max Planck Society and German Space Agency (DLR), and by the Planetary Science Institute under contract with the Jet Propulsion Laboratory, California Institute of Technology. We appreciate reviews by K. Keil, G. Consolmagno, and an anonymous reviewer. NR 113 TC 43 Z9 44 U1 4 U2 25 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 NOV PY 2013 VL 48 IS 11 BP 2090 EP 2104 DI 10.1111/maps.12108 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 273NY UT WOS:000328543300003 ER PT J AU Mittlefehldt, DW Herrin, JS Quinn, JE Mertzman, SA Cartwright, JA Mertzman, KR Peng, ZX AF Mittlefehldt, David W. Herrin, Jason S. Quinn, Julie E. Mertzman, Stanley A. Cartwright, Julia A. Mertzman, Karen R. Peng, Zhan X. TI Composition and petrology of HED polymict breccias: The regolith of (4) Vesta SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID CARBONACEOUS CHONDRITE CLASTS; PARENT BODY; BASALTIC ACHONDRITES; ANTARCTIC EUCRITES; CUMULATE EUCRITES; KAPOETA HOWARDITE; TREND EUCRITES; IMPACT MELTS; DIOGENITES; METEORITES AB We have done petrologic and compositional studies on a suite of polymict eucrites and howardites to better understand regolith processes on their parent asteroid, which we accept is (4) Vesta. Taking into account noble gas results from companion studies, we interpret five howardites to represent breccias assembled from the true regolith: Elephant Moraine (EET) 87513, Grosvenor Mountains (GRO) 95535, GRO 95602, Lewis Cliff (LEW) 85313, and Meteorite Hills (MET) 00423. We suggest that EET 87503 is paired with EET 87513, and thus is also regolithic. Pecora Escarpment (PCA) 02066 is dominated by melt-matrix clasts, which may have been formed from true regolith by impact melting. These meteorites display a range in eucrite:diogenite mixing ratio from 55:45 to 76:24. There is no correlation between degree of regolith character and Ni content. The Ni contents of howardite, eucrite, and diogenites (HEDs) are mostly controlled by the distribution of coarse chondritic clasts and metal grains, which in some cases resulted from individual, low-velocity accretion events, rather than extensive regolith gardening. Trace element compositions indicate that the mafic component of HED polymict breccias is mostly basalt similar to main-group eucrites; Stannern-trend basaltic debris is less common. Pyroxene compositions show that some trace element-rich howardites contain abundant debris from evolved basalts, and that cumulate gabbro debris is present in some breccias. The scale of heterogeneity varies considerably; regolithic howardite EET 87513 is more homogeneous than fragmental howardite Queen Alexandra Range (QUE) 97001. Individual samples of a given howardite can have different compositions even at roughly 5g masses, indicating that obtaining representative meteorite compositions requires multiple or large samples. C1 [Mittlefehldt, David W.] NASA, KR Astromat Res Off, Astromat Res & Explorat Sci Directorate, Johnson Space Ctr, Houston, TX 77058 USA. [Herrin, Jason S.; Quinn, Julie E.; Peng, Zhan X.] Engn & Sci Contract Grp, Houston, TX 77258 USA. [Mertzman, Stanley A.; Mertzman, Karen R.] Franklin & Marshall Coll, Dept Geosci, Lancaster, PA 17604 USA. [Cartwright, Julia A.] Max Planck Inst Chem, D-55128 Mainz, Germany. RP Mittlefehldt, DW (reprint author), NASA, KR Astromat Res Off, Astromat Res & Explorat Sci Directorate, Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. EM david.w.mittlefehldt@nasa.gov RI Cartwright, Julia/A-8470-2013; OI Herrin, Jason/0000-0002-2452-244X FU National Science Foundation; NASA Cosmochemistry Program FX We thank the National Science Foundation for funding the ANSMET collecting teams that brought back the Antarctic samples studied here, and the Meteorite Working Group, NASA-Johnson Space Center and the National Museum of Natural History (Smithsonian Institution) for allocation of the samples. We thank K. M. McBride and C. E. Satterwhite for providing photodocumentation and details of sample allocations for select howardites, J. Schutt for providing the map of Elephant Moraine polymict breccia to find locations (Fig. S3), and D. K. Ross for help acquiring all BSE images except for Fig. S5a. Editorial handling by H. Y. McSween Jr., and reviews by A. W. Beck, J. S. Delaney, and R. G. Mayne resulted in considerable improvement in the article; we thank them for their efforts. Funding for this research was provided to DWM from the NASA Cosmochemistry Program. NR 127 TC 16 Z9 17 U1 1 U2 11 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 NOV PY 2013 VL 48 IS 11 BP 2105 EP 2134 DI 10.1111/maps.12182 PG 30 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 273NY UT WOS:000328543300004 ER PT J AU De Sanctis, MC Ammannito, E Capria, MT Capaccioni, F Combe, JP Frigeri, A Longobardo, A Magni, G Marchi, S McCord, TB Palomba, E Tosi, F Zambon, F Carraro, F Fonte, S Li, YJ McFadden, LA Mittlefehldt, DW Pieters, CM Jaumann, R Stephan, K Raymond, CA Russell, CT AF De Sanctis, M. Cristina Ammannito, Eleonora Capria, M. Teresa Capaccioni, Fabrizio Combe, Jean-Philippe Frigeri, Alessandro Longobardo, Andrea Magni, Gianfranco Marchi, Simone McCord, Tom B. Palomba, Ernesto Tosi, Federico Zambon, Francesca Carraro, Francesco Fonte, Sergio Li, Y. J. McFadden, Lucy A. Mittlefehldt, David W. Pieters, Carle M. Jaumann, Ralf Stephan, Katrin Raymond, Carol A. Russell, Christopher T. TI Vesta's mineralogical composition as revealed by the visible and infrared spectrometer on Dawn SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID ASTEROID 4 VESTA; EUCRITE PARENT BODY; MAIN-BELT; IMAGING SPECTROMETER; BASALTIC ACHONDRITE; HED METEORITES; ORTHO-PYROXENE; DIOGENITES; SURFACE; MISSION AB The Dawn spacecraft mission has provided extensive new and detailed data on Vesta that confirm and strengthen the Vesta-howardite-eucrite-diogenite (HED) meteorite link and the concept that Vesta is differentiated, as derived from earlier telescopic observations. Here, we present results derived by newly calibrated spectra of Vesta. The comparison between data from the Dawn imaging spectrometerVIRand the different class of HED meteorites shows that average spectrum of Vesta resembles howardite spectra. Nevertheless, the Vesta spectra at high spatial resolution reveal variations in the distribution of HED-like mineralogies on the asteroid. The data have been used to derive HED distribution on Vesta, reported in Ammannito etal. (2013), and to compute the average Vestan spectra of the different HED lithologies, reported here. The spectra indicate that, not only are all the different HED lithologies present on Vesta, but also carbonaceous chondritic material, which constitutes the most abundant inclusion type found in howardites, is widespread. However, the hydration feature used to identify carbonaceous chondrite material varies significantly on Vesta, revealing different band shapes. The characteristic of these hydration features cannot be explained solely by infalling of carbonaceous chondrite meteorites and other possible origins must be considered. The relative proportion of HEDs on Vesta's surface is computed, and results show that most of the vestan surface is compatible with eucrite-rich howardites and/or cumulate or polymict eucrites. A very small percentage of surface is covered by diogenite, and basaltic eucrite terrains are relatively few compared with the abundance of basaltic eucrites in the HED suite. The largest abundance of diogenitic material is found in the Rheasilvia region, a deep basin, where it clearly occurs below a basaltic upper crust. However, diogenite is also found elsewhere; although the depth to diogenite is consistent with one magma ocean model, its lateral extent is not well constrained. C1 [De Sanctis, M. Cristina; Ammannito, Eleonora; Capria, M. Teresa; Capaccioni, Fabrizio; Frigeri, Alessandro; Longobardo, Andrea; Magni, Gianfranco; Marchi, Simone; Palomba, Ernesto; Tosi, Federico; Zambon, Francesca; Carraro, Francesco; Fonte, Sergio] INAF, Ist Astrofis & Planetol Spaziali, Rome, Italy. [Combe, Jean-Philippe; McCord, Tom B.] Bear Fight Inst, Winthrop, WA 98862 USA. [Marchi, Simone] NASA, Lunar Sci Inst, Boulder, CO USA. [Li, Y. J.] Planetary Sci Inst, Tucson, AZ 85719 USA. [McFadden, Lucy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mittlefehldt, David W.] NASA, Astromat Res Off, Johnson Space Ctr, Houston, TX 77058 USA. [Pieters, Carle M.] Brown Univ, Providence, RI 02912 USA. [Jaumann, Ralf; Stephan, Katrin] DLR, Inst Planetary Res, D-80302 Berlin, Germany. [Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. RP De Sanctis, MC (reprint author), INAF, Ist Astrofis & Planetol Spaziali, Rome, Italy. EM mariacristina.desanctis@iaps.inaf.it RI De Sanctis, Maria Cristina/G-5232-2013; Frigeri, Alessandro/F-2151-2010; OI Tosi, Federico/0000-0003-4002-2434; De Sanctis, Maria Cristina/0000-0002-3463-4437; Zambon, Francesca/0000-0002-4190-6592; Frigeri, Alessandro/0000-0002-9140-3977; capria, maria teresa/0000-0002-9814-9588; McFadden, Lucy/0000-0002-0537-9975; Capaccioni, Fabrizio/0000-0003-1631-4314; Palomba, Ernesto/0000-0002-9101-6774 FU Italian Space Agency; NASA's Dawn at Vesta Participating Scientists Program FX VIR is funded by the Italian Space Agency and was developed under the leadership of INAF-Istituto di Astrofisica e Planetologia Spaziali, Rome, Italy. The instrument was built by Selex-Galileo, Florence, Italy. The authors acknowledge the support of the Dawn Science, Instrument, and Operations Teams. We also acknowledge H. Y. McSween, T. Hiroi, and R. Binzel for their helpful comments. This work was supported by the Italian Space Agency and NASA's Dawn at Vesta Participating Scientists Program. A portion of this work was performed at the Jet Propulsion Laboratory under contract with NASA. This research utilizes spectra of the NASA RELAB facility at Brown University. NR 86 TC 39 Z9 39 U1 3 U2 18 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 NOV PY 2013 VL 48 IS 11 BP 2166 EP 2184 DI 10.1111/maps.12138 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 273NY UT WOS:000328543300007 ER PT J AU Ammannito, E De Sanctis, MC Capaccioni, F Capria, MT Carraro, F Combe, JP Fonte, S Frigeri, A Joy, SP Longobardo, A Magni, G Marchi, S McCord, TB McFadden, LA McSween, HY Palomba, E Pieters, CM Polanskey, CA Raymond, CA Sunshine, JM Tosi, F Zambon, F Russell, CT AF Ammannito, Eleonora De Sanctis, M. Cristina Capaccioni, Fabrizio Capria, M. Teresa Carraro, F. Combe, Jean-Philippe Fonte, Sergio Frigeri, Alessandro Joy, Steven P. Longobardo, Andrea Magni, Gianfranco Marchi, Simone McCord, Thomas B. McFadden, Lucy A. McSween, Harry Y. Palomba, Ernesto Pieters, Carle M. Polanskey, Carol A. Raymond, Carol A. Sunshine, Jessica M. Tosi, Federico Zambon, Francesca Russell, Christopher T. TI Vestan lithologies mapped by the visual and infrared spectrometer on Dawn SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID ASTEROID 4 VESTA; SPACE-TELESCOPE IMAGES; DIOGENITE PARENT BODY; IMAGING SPECTROMETER; REFLECTANCE SPECTRA; HED METEORITES; ORTHO-PYROXENE; ROSETTA MISSION; HOWARDITE; SPECTROSCOPY AB We present global lithological maps of the Vestan surface based on Dawn mission's Visible InfraRed (VIR) Spectrometer acquisitions with a spatial sampling of 200m. The maps confirm the results obtained with the data set acquired by VIR with a spatial sampling of 700m, that the reflectance spectra of Vesta's surface are dominated by pyroxene absorptions that can be interpreted within the context of the distribution of howardites, eucrites, and diogenites (HEDs). The maps also partially agree with the ground and Hubble Space Telescope observations: they confirm the background surface being an assemblage of howardite or polymict eucrite, as well as the location of a diogenitic-rich spot; however, there is no evidence of extended olivine-rich regions in the equatorial latitudes. Diogenite is revealed on the Rheasilvia basin floor, indicating that material of the lower crust/mantle was exposed. VIR also detected diogenites along the scarp of Matronalia Rupes, and the rims of Severina and a nearby, unnamed crater, and as ejecta of Antonia crater. The diogenite distribution is fully consistent with petrological constraints; although the mapped distribution does not provide unambiguous constraints, it favors the hypothesis of a magma ocean. C1 [Ammannito, Eleonora; De Sanctis, M. Cristina; Capaccioni, Fabrizio; Capria, M. Teresa; Carraro, F.; Fonte, Sergio; Frigeri, Alessandro; Longobardo, Andrea; Magni, Gianfranco; Palomba, Ernesto; Tosi, Federico; Zambon, Francesca] INAF, Ist Astrofis & Planetol Spaziali, Rome, Italy. [Combe, Jean-Philippe; McCord, Thomas B.] Bear Fight Inst, Winthrop, WA 98862 USA. [Joy, Steven P.; Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Marchi, Simone] NASA, Lunar Sci Inst, Southwest Res Inst, Boulder, CO 80302 USA. [McFadden, Lucy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McSween, Harry Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Pieters, Carle M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Polanskey, Carol A.; Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sunshine, Jessica M.] Univ Maryland, College Pk, MD 20742 USA. RP Ammannito, E (reprint author), INAF, Ist Astrofis & Planetol Spaziali, Rome, Italy. EM eleonora.ammannito@iaps.inaf.it RI Frigeri, Alessandro/F-2151-2010; OI Frigeri, Alessandro/0000-0002-9140-3977; McFadden, Lucy/0000-0002-0537-9975; De Sanctis, Maria Cristina/0000-0002-3463-4437; Capaccioni, Fabrizio/0000-0003-1631-4314; Palomba, Ernesto/0000-0002-9101-6774; Tosi, Federico/0000-0003-4002-2434; Zambon, Francesca/0000-0002-4190-6592 FU ASI (Italian Space Agency); Italian Space Agency; NASA FX The VIR spectrometer is funded by ASI (Italian Space Agency). It was built by Selex-Galileo, Florence, Italy and is now managed by INAF-Istituto di Astrofisica e Planetologia Spaziali, Rome, Italy. This work was supported by the Italian Space Agency, and NASA's Dawn at Vesta Participating Scientists Program. A portion of this work was performed at the Jet Propulsion Laboratory under contract with NASA. The authors acknowledge the support of the Dawn Science, Instrument, and Operations Teams. We also acknowledge Sharon Uy for her careful review of the manuscript. NR 68 TC 40 Z9 40 U1 2 U2 10 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 NOV PY 2013 VL 48 IS 11 BP 2185 EP 2198 DI 10.1111/maps.12192 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 273NY UT WOS:000328543300008 ER PT J AU Thangjam, G Reddy, V Le Corre, L Nathues, A Sierks, H Hiesinger, H Li, JY Sanchez, JA Russell, CT Gaskell, R Raymond, C AF Thangjam, Guneshwar Reddy, Vishnu Le Corre, Lucille Nathues, Andreas Sierks, Holger Hiesinger, Harald Li, Jian-Yang Sanchez, Juan A. Russell, Christopher T. Gaskell, Robert Raymond, Carol TI Lithologic mapping of HED terrains on Vesta using Dawn Framing Camera color data SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID ASTEROID 4 VESTA; PARENT BODY; SPECTRAL REFLECTANCE; DARK MATERIAL; SOLAR-SYSTEM; LUNAR CRUST; SOUTH-POLE; DIOGENITES; METEORITES; SURFACE AB The surface composition of Vesta, the most massive intact basaltic object in the asteroid belt, is interesting because it provides us with an insight into magmatic differentiation of planetesimals that eventually coalesced to form the terrestrial planets. The distribution of lithologic and compositional units on the surface of Vesta provides important constraints on its petrologic evolution, impact history, and its relationship with vestoids and howardite-eucrite-diogenite (HED) meteorites. Using color parameters (band tilt and band curvature) originally developed for analyzing lunar data, we have identified and mapped HED terrains on Vesta in Dawn Framing Camera (FC) color data. The average color spectrum of Vesta is identical to that of howardite regions, suggesting an extensive mixing of surface regolith due to impact gardening over the course of solar system history. Our results confirm the hemispherical dichotomy (east-west and north-south) in albedo/color/composition that has been observed by earlier studies. The presence of diogenite-rich material in the southern hemisphere suggests that it was excavated during the formation of the Rheasilvia and Veneneia basins. Our lithologic mapping of HED regions provides direct evidence for magmatic evolution of Vesta with diogenite units in Rheasilvia forming the lower crust of a differentiated object. C1 [Thangjam, Guneshwar; Reddy, Vishnu; Le Corre, Lucille; Nathues, Andreas; Sierks, Holger; Sanchez, Juan A.] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany. [Reddy, Vishnu] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58201 USA. [Le Corre, Lucille; Gaskell, Robert] Planetary Sci Inst, Tucson, AZ USA. [Hiesinger, Harald] Univ Munster, Inst Planetol, D-48149 Munster, Germany. [Li, Jian-Yang] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Raymond, Carol] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Thangjam, G (reprint author), Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany. EM thangjam@mps.mpg.de OI Reddy, Vishnu/0000-0002-7743-3491; Le Corre, Lucille/0000-0003-0349-7932 FU Max Planck Society; German Space Agency, DLR; Dawn at Vesta Participating Scientist Program; NASA FX We thank the Dawn team for the development, cruise, orbital insertion, and operations of the Dawn spacecraft at Vesta. The Framing Camera project is financially supported by the Max Planck Society and the German Space Agency, DLR. We also thank the Dawn at Vesta Participating Scientist Program for funding the research. A portion of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Dawn data are archived with the NASA Planetary Data System. This study uses 239 HED meteorite spectra from the RELAB spectral database at Brown University and we acknowledge the concerned PIs and the RELAB team for their effort. We thank Thomas Burbine, the anonymous reviewer, and Harry Y. McSween Jr. for their helpful and constructive comments. NR 73 TC 14 Z9 14 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD NOV PY 2013 VL 48 IS 11 BP 2199 EP 2210 DI 10.1111/maps.12132 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 273NY UT WOS:000328543300009 ER PT J AU Prettyman, TH Mittlefehldt, DW Yamashita, N Beck, AW Feldman, WC Hendricks, JS Lawrence, DJ McCoy, TJ McSween, HY Peplowski, PN Reedy, RC Toplis, MJ Le Corre, L Mizzon, H Reddy, V Titus, TN Raymond, CA Russell, CT AF Prettyman, Thomas H. Mittlefehldt, David W. Yamashita, Naoyuki Beck, Andrew W. Feldman, William C. Hendricks, John S. Lawrence, David J. McCoy, Timothy J. McSween, Harry Y. Peplowski, Patrick N. Reedy, Robert C. Toplis, Michael J. Le Corre, Lucille Mizzon, Hugau Reddy, Vishnu Titus, Timothy N. Raymond, Carol A. Russell, Christopher T. TI Neutron absorption constraints on the composition of 4 Vesta SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID LUNAR PROSPECTOR; GAMMA-RAY; DAWN MISSION; PARENT BODY; MARS ODYSSEY; WATER-ICE; EPITHERMAL NEUTRONS; HED METEORITES; DARK MATERIAL; SOUTH-POLE AB Global maps of the macroscopic thermal neutron absorption cross section of Vesta's regolith by the Gamma Ray and Neutron Detector (GRaND) on board the NASA Dawn spacecraft provide constraints on the abundance and distribution of Fe, Ca, Al, Mg, and other rock-forming elements. From a circular, polar low-altitude mapping orbit, GRaND sampled the regolith to decimeter depths with a spatial resolution of about 300km. At this spatial scale, the variation in neutron absorption is about seven times lower than that of the Moon. The observed variation is consistent with the range of absorption for howardite whole-rock compositions, which further supports the connection between Vesta and the howardite, eucrite, and diogenite meteorites. We find a strong correlation between neutron absorption and the percentage of eucritic materials in howardites and polymict breccias, which enables petrologic mapping of Vesta's surface. The distribution of basaltic eucrite and diogenite determined from neutron absorption measurements is qualitatively similar to that indicated by visible and near infrared spectroscopy. The Rheasilvia basin and ejecta blanket has relatively low absorption, consistent with Mg-rich orthopyroxene. Based on a combination of Fe and neutron absorption measurements, olivine-rich lithologies are not detected on the spatial scales sampled by GRaND. The sensitivity of GRaND to the presence of mantle material is described and implications for the absence of an olivine signature are discussed. High absorption values found in Vesta's dark hemisphere, where exogenic hydrogen has accumulated, indicate that this region is richer in basaltic eucrite, representative of Vesta's ancient upper crust. C1 [Prettyman, Thomas H.; Yamashita, Naoyuki; Feldman, William C.; Reedy, Robert C.; Le Corre, Lucille; Reddy, Vishnu] Planetary Sci Inst, Tucson, AZ 85719 USA. [Mittlefehldt, David W.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Beck, Andrew W.; McCoy, Timothy J.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Hendricks, John S.] TechSource Inc, Los Alamos, NM 87544 USA. [Lawrence, David J.; Peplowski, Patrick N.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [McSween, Harry Y.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA. [McSween, Harry Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Toplis, Michael J.; Mizzon, Hugau] Univ Toulouse, CNRS, Observ Midi Pyrenees, IRAP,UMR 5277, Toulouse, France. [Le Corre, Lucille; Reddy, Vishnu] Max Planck Inst Solar Syst Res, Lindau, Germany. [Titus, Timothy N.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. RP Prettyman, TH (reprint author), Planetary Sci Inst, 1700 East Ft Lowell,Suite 106, Tucson, AZ 85719 USA. EM prettyman@psi.edu RI Beck, Andrew/J-7215-2015; Peplowski, Patrick/I-7254-2012; Lawrence, David/E-7463-2015; OI Beck, Andrew/0000-0003-4455-2299; Peplowski, Patrick/0000-0001-7154-8143; Lawrence, David/0000-0002-7696-6667; Reedy, Robert/0000-0002-2189-1303; Prettyman, Thomas/0000-0003-0072-2831; Reddy, Vishnu/0000-0002-7743-3491; Le Corre, Lucille/0000-0003-0349-7932 FU NASA Jet Propulsion Laboratory; NASA Discovery Program; NASA Dawn at Vesta Participating Scientist Program FX This work was carried out under contract with the NASA Jet Propulsion Laboratory. GRaND is operated by the Planetary Science Institute. The Dawn mission is led by the University of California, Los Angeles under the auspices of the NASA Discovery Program. Funding for U.S. Participating Scientists was provided by the NASA Dawn at Vesta Participating Scientist Program. Contributions by members of the Dawn Science, Spacecraft and Instrument-Operations teams at JPL and UCLA, including Carol Polanskey, Steve Joy, Joe Mafi, and Marc Rayman, are greatly appreciated. In addition, we are grateful for technical support provided by Joe Makowski and Mike Violet of Orbital Sciences Corporation. GRaND data are archived by the NASA Planetary Data System Small Bodies Node. Comments by the reviewers, Brad Jolliff and Josef Masarik, and the associate editor, Ingo Leya, helped improve the manuscript. Tomo Usui provided a portion of the HED whole-rock compositions used in this study. NR 108 TC 20 Z9 20 U1 1 U2 10 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 NOV PY 2013 VL 48 IS 11 BP 2211 EP 2236 DI 10.1111/maps.12244 PG 26 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 273NY UT WOS:000328543300010 ER PT J AU Yamashita, N Prettyman, TH Mittlefehldt, DW Toplis, MJ McCoy, TJ Beck, AW Reedy, RC Feldman, WC Lawrence, DJ Peplowski, PN Forni, O Mizzon, H Raymond, CA Russell, CT AF Yamashita, N. Prettyman, T. H. Mittlefehldt, D. W. Toplis, M. J. McCoy, T. J. Beck, A. W. Reedy, R. C. Feldman, W. C. Lawrence, D. J. Peplowski, P. N. Forni, O. Mizzon, H. Raymond, C. A. Russell, C. T. TI Distribution of iron on Vesta SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID GAMMA-RAY SPECTROMETER; LUNAR-SURFACE; DAWN MISSION; MARS ODYSSEY; GLOBAL DISTRIBUTION; NEUTRON DETECTOR; HED METEORITES; DARK MATERIAL; PROSPECTOR; SPECTRA AB We have completed a mapping study of 7.6MeV gamma rays produced by neutron capture by Fe at the surface of the main belt asteroid 4 Vesta as measured by the bismuth germanate scintillator of the Gamma Ray and Neutron Detector (GRaND) on the Dawn spacecraft. The procedures used to determine Fe counting rates are presented, along with a global map, constituting the necessary initial step to quantify Fe abundances. While the final calibration of orbital data to absolute concentrations has not been determined, the range of fully corrected Fe counting rates is compared with that of Fe in howardites. We find that the global distribution of corrected Fe counting rates is generally consistent with mineralogy and composition determined independently by other instruments on the Dawn spacecraft, including measurements of pyroxene absorption bands by the Visible and Infrared Spectrometer and Framing Camera, and an index of diogenitic materials provided by neutron absorption measurements by GRaND. In addition, there is a distinctive low Fe region in the western hemisphere that was not reported by reflectance or optical observations, possibly indicating the presence of a cumulate eucrite component in Vesta's regolith. C1 [Yamashita, N.; Prettyman, T. H.; Reedy, R. C.; Feldman, W. C.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Mittlefehldt, D. W.] NASA, Astromat Res Off, Johnson Space Ctr, Houston, TX 77058 USA. [Toplis, M. J.; Forni, O.; Mizzon, H.] Univ Toulouse, UPS OMP, Inst Rech Astrophys & Planetol, Toulouse, France. [Toplis, M. J.; Forni, O.; Mizzon, H.] CNRS, IRAP, Toulouse, France. [McCoy, T. J.; Beck, A. W.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Lawrence, D. J.; Peplowski, P. N.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. RP Yamashita, N (reprint author), Planetary Sci Inst, Tucson, AZ 85719 USA. EM yamashita@psi.edu RI Beck, Andrew/J-7215-2015; Peplowski, Patrick/I-7254-2012; Lawrence, David/E-7463-2015; OI Beck, Andrew/0000-0003-4455-2299; Peplowski, Patrick/0000-0001-7154-8143; Lawrence, David/0000-0002-7696-6667; Reedy, Robert/0000-0002-2189-1303; Prettyman, Thomas/0000-0003-0072-2831 FU NASA Discovery Program Office; JPL; NASA; NASA's Dawn at Vesta Participating Scientist program FX We thank T. Usui and two anonymous reviewers for their valuable comments and suggestions that led to improvements in this manuscript. The Dawn mission is led by the University of California, Los Angeles, and managed by Jet Propulsion Laboratory (JPL) under the auspices of the NASA Discovery Program Office. A portion of this work was carried out by the Planetary Science Institute under contract with JPL, by JPL under contract with NASA, and by NASA's Dawn at Vesta Participating Scientist program. Science experimental data records and housekeeping data acquired by GRaND during Vesta encounter and used in this study are available from NASA's Planetary Data System. NR 61 TC 17 Z9 17 U1 1 U2 8 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 NOV PY 2013 VL 48 IS 11 BP 2237 EP 2251 DI 10.1111/maps.12139 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 273NY UT WOS:000328543300011 ER PT J AU Lawrence, DJ Peplowski, PN Prettyman, TH Feldman, WC Bazell, D Mittlefehldt, DW Reedy, RC Yamashita, N AF Lawrence, David J. Peplowski, Patrick N. Prettyman, Thomas H. Feldman, William C. Bazell, David Mittlefehldt, David W. Reedy, Robert C. Yamashita, Naoyuki TI Constraints on Vesta's elemental composition: Fast neutron measurements by Dawn's gamma ray and neutron detector SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID LUNAR PROSPECTOR; HED METEORITES; MARS ODYSSEY; WATER ICE; SPECTROMETER; MISSION; SPECTRA; MOON AB Surface composition information from Vesta is reported using fast neutron data collected by the gamma ray and neutron detector on the Dawn spacecraft. After correcting for variations due to hydrogen, fast neutrons show a compositional dynamic range and spatial variability that is consistent with variations in average atomic mass from howardite, eucrite, and diogenite (HED) meteorites. These data provide additional compositional evidence that Vesta is the parent body to HED meteorites. A subset of fast neutron data having lower statistical precision show spatial variations that are consistent with a 400ppm variability in hydrogen concentrations across Vesta and supports the idea that Vesta's hydrogen is due to long-term delivery of carbonaceous chondrite material. C1 [Lawrence, David J.; Peplowski, Patrick N.; Bazell, David] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Prettyman, Thomas H.; Feldman, William C.; Reedy, Robert C.; Yamashita, Naoyuki] Planetary Sci Inst, Tucson, AZ USA. [Mittlefehldt, David W.] NASA, Johnson Space Ctr, Houston, TX USA. RP Lawrence, DJ (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. EM david.j.lawrence@jhuapl.edu RI Peplowski, Patrick/I-7254-2012; Lawrence, David/E-7463-2015; OI Peplowski, Patrick/0000-0001-7154-8143; Lawrence, David/0000-0002-7696-6667; Reedy, Robert/0000-0002-2189-1303; Prettyman, Thomas/0000-0003-0072-2831 FU NASA Discovery Program Office; Dawn mission program; NASA's Dawn at Vesta Participating Scientist program FX The authors thank two anonymous reviewers who provided helpful and constructive comments, which resulted in a much improved manuscript. The Dawn mission is led by the University of California, Los Angeles, and managed by the Jet Propulsion Laboratory, Pasadena, California under the auspices of the NASA Discovery Program Office. Support for this work was provided by the Dawn mission program and by NASA's Dawn at Vesta Participating Scientist program. Science experimental data records and housekeeping data acquired by GRaND during Vesta encounter and used in this study are available from NASA's Planetary Data System. NR 27 TC 10 Z9 10 U1 2 U2 7 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 NOV PY 2013 VL 48 IS 11 BP 2271 EP 2288 DI 10.1111/maps.12187 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 273NY UT WOS:000328543300013 ER PT J AU Toplis, MJ Mizzon, H Monnereau, M Forni, O McSween, HY Mittlefehldt, DW McCoy, TJ Prettyman, TH De Sanctis, MC Raymond, CA Russell, CT AF Toplis, M. J. Mizzon, H. Monnereau, M. Forni, O. McSween, H. Y. Mittlefehldt, D. W. McCoy, T. J. Prettyman, T. H. De Sanctis, M. C. Raymond, C. A. Russell, C. T. TI Chondritic models of 4 Vesta: Implications for geochemical and geophysical properties SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID METEORITE PARENT BODIES; EARLY SOLAR-SYSTEM; MELT MIGRATION; CORE FORMATION; DIFFERENTIATED ASTEROIDS; PARTITION-COEFFICIENTS; EUCRITIC METEORITES; PHASE-RELATIONS; SILICATE MELTS; DIOGENITES AB Simple mass-balance and thermodynamic constraints are used to illustrate the potential geochemical and geophysical diversity of a fully differentiated Vesta-sized parent body with a eucrite crust (e.g., core size and density, crustal thickness). The results of this analysis are then combined with data from the howardite-eucrite-diogenite (HED) meteorites and the Dawn mission to constrain Vesta's bulk composition. Twelve chondritic compositions are considered, comprising seven carbonaceous, three ordinary, and two enstatite chondrite groups. Our analysis excludes CI and LL compositions as plausible Vesta analogs, as these are predicted to have a negative metal fraction. Second, the MELTS thermodynamic calculator is used to show that the enstatite chondrites, the CV, CK and L-groups cannot produce Juvinas-like liquids, and that even for the other groups, depletion in sodium is necessary to produce liquids of appropriate silica content. This conclusion is consistent with the documented volatile-poor nature of eucrites. Furthermore, carbonaceous chondrites are predicted to have a mantle too rich in olivine to produce typical howardites and to have Fe/Mn ratios generally well in excess of those of the HEDs. On the other hand, an Na-depleted H-chondrite bulk composition is capable of producing Juvinas-like liquids, has a mantle rich enough in pyroxene to produce abundant howardite/diogenite, and has a Fe/Mn ratio compatible with eucrites. In addition, its predicted bulk-silicate density is within 100kgm(-3) of solutions constrained by data of the Dawn mission. However, oxidation state and oxygen isotopes are not perfectly reproduced and it is deduced that bulk Vesta may contain approximately 25% of a CM-like component. Values for the bulk-silicate composition of Vesta and a preliminary phase diagram are proposed. C1 [Toplis, M. J.; Mizzon, H.; Monnereau, M.; Forni, O.] Univ Toulouse, Observ Midi Pyrenees, UMR 5277, IRAP,CNRS, F-31400 Toulouse, France. [McSween, H. Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Mittlefehldt, D. W.] NASA, Astromat Res Off, Johnson Space Ctr, Houston, TX 77058 USA. [McCoy, T. J.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. [Prettyman, T. H.] Planetary Sci Inst, Tucson, AZ 85719 USA. [De Sanctis, M. C.] Ist Astrofis & Planetol Spaziali INAF, I-00133 Rome, Italy. [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. RP Toplis, MJ (reprint author), Univ Toulouse, Observ Midi Pyrenees, UMR 5277, IRAP,CNRS, 14 Ave E Belin, F-31400 Toulouse, France. EM mtoplis@irap.omp.eu RI De Sanctis, Maria Cristina/G-5232-2013; OI De Sanctis, Maria Cristina/0000-0002-3463-4437; Forni, Olivier/0000-0001-6772-9689; Prettyman, Thomas/0000-0003-0072-2831 FU Centre National d'Etudes Spatiales (CNES) FX Enlightening discussions with J.-A. Barrat and formal reviews by H. Takeda and G. J. Taylor are gratefully acknowledged. MT thanks the Centre National d'Etudes Spatiales (CNES) for their financial support, which enabled participation in this work and the Dawn mission. NR 92 TC 19 Z9 19 U1 1 U2 17 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 NOV PY 2013 VL 48 IS 11 BP 2300 EP 2315 DI 10.1111/maps.12195 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 273NY UT WOS:000328543300015 ER PT J AU Polychronaki, A Gitas, IZ Veraverbeke, S Debien, A AF Polychronaki, Anastasia Gitas, Ioannis Z. Veraverbeke, Sander Debien, Annekatrien TI Evaluation of ALOS PALSAR Imagery for Burned Area Mapping in Greece Using Object-Based Classification SO REMOTE SENSING LA English DT Article DE fire severity; Mediterranean landscape; multi-temporal SAR ID LAND-COVER CLASSIFICATION; BOREAL FOREST ECOSYSTEMS; SURFACE SOIL-MOISTURE; ERS-2 SAR IMAGES; RADAR DATA; INTERIOR ALASKA; HIGH-RESOLUTION; FIRE SCARS; IDENTIFICATION; PELOPONNESE AB In this work, the potential of Advanced Land Observing Satellite (ALOS) Phased Array type L-band Synthetic Aperture Radar (PALSAR) imagery to map burned areas was evaluated in two study areas in Greece. For this purpose, we developed an object-based classification scheme to map the fire-disturbed areas using the PALSAR imagery acquired before and shortly after fire events. The advantage of employing an object-based approach was not only the use of the temporal variation of the backscatter coefficient, but also the incorporation in the classification of topological features, such as neighbor objects, and class related features, such as objects classified as burned. The classification scheme resulted in mapping the burned areas with satisfactory results: 0.71 and 0.82 probabilities of detection for the two study areas. Our investigation revealed that the pre-fire vegetation conditions and fire severity should be taken in consideration when mapping burned areas using PALSAR in Mediterranean regions. Overall, findings suggest that the developed scheme could be applied for rapid burned area assessment, especially to areas where cloud cover and fire smoke inhibit accurate mapping of burned areas when optical data are used. C1 [Polychronaki, Anastasia; Gitas, Ioannis Z.] Aristotle Univ Thessaloniki, Lab Forest Management & Remote Sensing, GR-54124 Thessaloniki, Greece. [Veraverbeke, Sander] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Debien, Annekatrien] KSAT, N-9291 Tromso, Norway. RP Polychronaki, A (reprint author), Aristotle Univ Thessaloniki, Lab Forest Management & Remote Sensing, POB 248, GR-54124 Thessaloniki, Greece. EM anpolych@for.auth.gr; igitas@for.auth.gr; Sander.S.Veraverbeke@jpl.nasa.gov; annekatrien.debien@gmail.com RI Gitas, Ioannis/C-3329-2008; Veraverbeke, Sander/H-2301-2012 OI Gitas, Ioannis/0000-0003-0056-5629; Veraverbeke, Sander/0000-0003-1362-5125 FU ESA [7204, 7882]; National Aeronautics and Space Administration FX We thank ESA for providing access to the ALOS PALSAR and SPOT data (cat-1 project IDs 7204 and 7882). We appreciate Niko Theofanous and Spyro Papakonstantinou from the Forest Service of Rhodes for providing valuable information about the burned areas. We are grateful to the anonymous reviewers for their constructive comments, which helped to improve the manuscript. 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. The JPL author's copyright for this publication is held by the California Institute of Technology. NR 52 TC 5 Z9 6 U1 0 U2 18 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD NOV PY 2013 VL 5 IS 11 BP 5680 EP 5701 DI 10.3390/rs5115680 PG 22 WC Remote Sensing SC Remote Sensing GA 274SQ UT WOS:000328626900015 ER PT J AU Forman, BA Reichle, RH AF Forman, B. A. Reichle, R. H. TI The spatial scale of model errors and assimilated retrievals in a terrestrial water storage assimilation system SO WATER RESOURCES RESEARCH LA English DT Article DE hydrology; modeling; remote sensing; snow; data assimilation; synthetic experiment ID LAND DATA ASSIMILATION; SNOW COVER; GRACE AB Synthetic satellite observations (or retrievals) of terrestrial water storage (TWS) in the Mackenzie River basin located in northwestern Canada were assimilated into the Catchment land surface model to evaluate the impact (i) assimilating TWS retrievals at subbasin (approximate to 10(5) km(2)) or basin (approximate to 10(6) km(2)) scales and (ii) incorrectly specifying the model error correlation length that is used for the perturbation of model forcing and prognostic variables in the ensemble-based assimilation system. Specifically, a total of 16 experiments were conducted over a 9 year study period using different combinations of the spatial scale of the assimilated TWS retrievals and the horizontal model error correlation length. In general, assimilation of the TWS retrievals at the subbasin scale (approximate to 2.7 x 10(5) km(2) on average) yielded the best agreement relative to the synthetic truth. Greater improvement in TWS and snow water equivalent, in general, was witnessed as the (designed) horizontal model error correlation length increased. Conversely, subsurface soil water, evaporation, and runoff estimates typically improved (or remained unchanged) as the horizontal model error correlation length decreased. As the scale of the assimilated TWS retrieval decreased, more mass was effectively transferred from snow water equivalent into the subsurface, thereby dampening the hydrologic runoff response in the study area and correcting for improper model physics related to the runoff routing scheme. In general, TWS retrievals should be assimilated at the smallest spatial scale for which the observation errors can be considered uncorrelated while the specification of the horizontal error correlation length scale is of secondary importance. C1 [Forman, B. A.] Univ Maryland, Dept Civil & Environm Engn, College Pk, MD 20742 USA. [Reichle, R. H.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Forman, BA (reprint author), Univ Maryland, Dept Civil & Environm Engn, 1173 Glenn Martin Hall, College Pk, MD 20742 USA. EM baforman@umd.edu RI Reichle, Rolf/E-1419-2012 FU NASA [NNH06CC03B] FX Partial funding provided by the NASA Post-doctoral Program (contract NNH06CC03B). Computing was supported by the NASA High End Computing Program. We thank the anonymous reviewers and the Associate Editor for their insights and feedback that led to an improved manuscript. Additional thanks go to Gabrielle De Lannoy for many useful conversations related to this work. NR 31 TC 6 Z9 6 U1 1 U2 20 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD NOV PY 2013 VL 49 IS 11 BP 7457 EP 7468 DI 10.1002/2012WR012885 PG 12 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 275NJ UT WOS:000328683800021 ER PT J AU Otto, KA Jaumann, R Krohn, K Matz, KD Preusker, F Roatsch, T Schenk, P Scholten, F Stephan, K Raymond, CA Russell, CT AF Otto, Katharina A. Jaumann, Ralf Krohn, Katrin Matz, Klaus-Dieter Preusker, Frank Roatsch, Thomas Schenk, Paul Scholten, Frank Stephan, Katrin Raymond, Carol A. Russell, Christopher T. TI Mass-wasting features and processes in Vesta's south polar basin Rheasilvia SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Vesta; Rheasilvia; mass wasting; landslides; slumping; flow-like features ID ASTEROID 4 VESTA; INDUCED SEISMIC ACTIVITY; OBLIQUE IMPACT; PARENT BODY; DAWN; SURFACE; HETEROGENEITY; TOPOGRAPHY; MORPHOLOGY; MINERALOGY AB The Rheasilvia crater is Vesta's largest impact basin. It is a 500km diameter complex crater centered near the south pole and overlying the 400km diameter impact basin Veneneia. Using Framing Camera (FC) data from the Dawn spacecraft's Low Altitude Mapping Orbit (20m/pixel) and a digital terrain model derived from High Altitude Mapping Orbit stereo data, we identified various mass-wasting features within the south polar region. These features include intra-crater mass movements, flow-like and creep-like structures, slumping areas, landslides, and curved radial and concentric ridges. Intra-crater mass-wasting features are represented by lobate slides, talus material, dark patches on the crater wall, spurs along the crater rim and boulders. Slumping areas develop in compact material, whereas landslides form in relatively loose material. Both may be triggered by seismic shaking induced by impacts. Intra-crater mass wasting and slid and slumped materials are homogeneously distributed throughout the basin. Slumping and sliding processes have contributed most efficiently to basin degradation. Flow-like and creep-like features originate from granular material and cluster between 0 degrees E and 90 degrees E, an area exposing shocked and fractured material from the Rheasilvia impact event. The radial curved ridges are likely to be remnants of the early Rheasilvia collapse process, when radially moving masses were deflected by the Coriolis Effect. The concentric ridges are artifacts from the crater rim collapse. Curved ridges at the intersection of Rheasilvia and Veneneia, and on Rheasilvia's central peak, may also have been influenced by the Rheasilvia basin relaxation process, and an oblique impact, respectively. C1 [Otto, Katharina A.; Jaumann, Ralf; Krohn, Katrin; Matz, Klaus-Dieter; Preusker, Frank; Roatsch, Thomas; Scholten, Frank; Stephan, Katrin] German Aerosp Ctr, D-12489 Berlin, Germany. [Jaumann, Ralf] Free Univ Berlin, Inst Geosci, Berlin, Germany. [Schenk, Paul] Lunar & Planetary Sci Inst, Houston, TX USA. [Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. RP Otto, KA (reprint author), German Aerosp Ctr, Rutherfordstr 2, D-12489 Berlin, Germany. EM katharina.otto@dlr.de NR 47 TC 12 Z9 12 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD NOV PY 2013 VL 118 IS 11 BP 2279 EP 2294 DI 10.1002/2013JE004333 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 270YJ UT WOS:000328355300002 ER PT J AU Han, SC AF Han, Shin-Chan TI Determination and localized analysis of intersatellite line of sight gravity difference: Results from the GRAIL primary mission SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE GRAIL; gravity; topography; crustal density ID TO-SATELLITE TRACKING; ELASTIC THICKNESS; MARTIAN GRAVITY; FIELD; VENUS; CRUST; MOON; TOPOGRAPHY; RESOLUTION; ANOMALIES AB The line of sight (LOS) gravity difference between two coorbiting spacecrafts is determined in terms of intersatellite range-acceleration measurements available from the Gravity Recovery and Interior Laboratory (GRAIL). The precise orbit data are crucial for retrieving gravity difference from range acceleration and aligning the LOS data particularly in altitude. A relative orbit error of a few centimeters in position and a few tens mu m/s in velocity is commensurate with the GRAIL-ranging instrument noise at a few Gal in LOS gravity difference. The power spectrum, as well as the topography correlation and admittance, is quantified by upward continuing the topographic potential, forward modeling the LOS gravity along the spacecraft trajectory (i.e., Bouguer correction) and comparing with the GRAIL LOS observations. Based on the data analysis from the primary GRAIL mission, I found that the LOS gravity difference observation produced near unity correlation with topography potential out to degree 550, higher than the global estimate, over the areas covered by the low-altitude orbit (similar to 20 km). The crustal density was estimated to be 2500-2600 kg/m(3) with regional variations of about 10%, by minimizing the Bouguer coherence of the GRAIL data at the degree band 150-300. Systematic decrease in the density estimates by 3-4% or 100 kg/m(3) was observed at shorter wavelengths (degree band 300-500). It implies the inadequacy of a uniform density model across the entire lithosphere and suggests radial stratification of the bulk density (or porosity). Due to spatially localized characteristic, the LOS gravity difference data are well suited to regional analysis at the highest-possible resolution. C1 NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. RP Han, SC (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Code 698, Greenbelt, MD 20771 USA. EM shin-chan.han@nasa.gov RI Han, Shin-Chan/A-2022-2009 FU NASA's LASER program; GRACE projects FX This work was supported by NASA's LASER program and GRACE projects. I thank Sander Goossens, Dave Rowlands, Greg Neumann, and Frank Lemoine for their technical advice and help to process GRAIL L1B data available from PDS Geosciences Node. Sander Goossens provided the estimate of LGRS time tag bias, 1.0207 s, for the primary mission. This bias should be applied for processing the KBR1B data from PDS. Greg Neumann provided the spherical harmonic coefficients of LOLA topography in the principal axis coordinate system (also available in PDS). I thank JPL colleagues for producing the high-quality Level-1B data products and orbits. I gratefully acknowledge GRAIL PI and the team for making the L1B data available publicly only in 6 months after the end of the primary mission. A Generic Mapping Tools (GMT) program, spectrum1d, written by Walter Smith and Paul Wessel, was used to compute power and cross-power spectra of the time series. A few FORTRAN subroutines written by Mark Wieczorek, available via SHTOOLS, were used. Constructive comments by Mark Wieczorek (editor in chief) and meticulous reviews by two anonymous reviewers greatly improved the manuscript. I thank Dave Rowlands and Nick Schmerr for proofreading the manuscript. NR 41 TC 4 Z9 4 U1 0 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 NOV PY 2013 VL 118 IS 11 BP 2323 EP 2337 DI 10.1002/2013JE004402 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 270YJ UT WOS:000328355300005 ER PT J AU Minitti, ME Kah, LC Yingst, RA Edgett, KS Anderson, RC Beegle, LW Carsten, JL Deen, RG Goetz, W Hardgrove, C Harker, DE Herkenhoff, KE Hurowitz, JA Jandura, L Kennedy, MR Kocurek, G Krezoski, GM Kuhn, SR Limonadi, D Lipkaman, L Madsen, MB Olson, TS Robinson, ML Rowland, SK Rubin, DM Seybold, C Schieber, J Schmidt, M Sumner, DY Tompkins, VV Van Beek, JK Van Beek, T AF Minitti, M. E. Kah, L. C. Yingst, R. A. Edgett, K. S. Anderson, R. C. Beegle, L. W. Carsten, J. L. Deen, R. G. Goetz, W. Hardgrove, C. Harker, D. E. Herkenhoff, K. E. Hurowitz, J. A. Jandura, L. Kennedy, M. R. Kocurek, G. Krezoski, G. M. Kuhn, S. R. Limonadi, D. Lipkaman, L. Madsen, M. B. Olson, T. S. Robinson, M. L. Rowland, S. K. Rubin, D. M. Seybold, C. Schieber, J. Schmidt, M. Sumner, D. Y. Tompkins, V. V. Van Beek, J. K. Van Beek, T. TI MAHLI at the Rocknest sand shadow: Science and science-enabling activities SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE aeolian; Mars Science Laboratory; Rocknest; MAHLI ID CHEMCAM INSTRUMENT SUITE; ROVER LANDING SITE; GALE CRATER; MERIDIANI-PLANUM; AEOLIAN BEDFORMS; MARS; EVOLUTION; SYSTEM; STRATIGRAPHY; EXPLORATION AB During Martian solar days 57-100, the Mars Science Laboratory Curiosity rover acquired and processed a solid (sediment) sample and analyzed its mineralogy and geochemistry with the Chemistry and Mineralogy and Sample Analysis at Mars instruments. An aeolian depositherein referred to as the Rocknest sand shadowwas inferred to represent a global average soil composition and selected for study to facilitate integration of analytical results with observations from earlier missions. During first-time activities, the Mars Hand Lens Imager (MAHLI) was used to support both science and engineering activities related to sample assessment, collection, and delivery. Here we report on MAHLI activities that directly supported sample analysis and provide MAHLI observations regarding the grain-scale characteristics of the Rocknest sand shadow. MAHLI imaging confirms that the Rocknest sand shadow is one of a family of bimodal aeolian accumulations on Marssimilar to the coarse-grained ripples interrogated by the Mars Exploration Rovers Spirit and Opportunityin which a surface veneer of coarse-grained sediment stabilizes predominantly fine-grained sediment of the deposit interior. The similarity in grain size distribution of these geographically disparate deposits support the widespread occurrence of bimodal aeolian transport on Mars. We suggest that preservation of bimodal aeolian deposits may be characteristic of regions of active deflation, where winnowing of the fine-sediment fraction results in a relatively low sediment load and a preferential increase in the coarse-grained fraction of the sediment load. The compositional similarity of Martian aeolian deposits supports the potential for global redistribution of fine-grained components, combined with potential local contributions. C1 [Minitti, M. E.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Kah, L. C.; Hardgrove, C.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN USA. [Yingst, R. A.] Planetary Sci Inst, Tucson, AZ USA. [Edgett, K. S.; Harker, D. E.; Kennedy, M. R.; Krezoski, G. M.; Lipkaman, L.; Van Beek, J. K.; Van Beek, T.] Malin Space Sci Syst, San Diego, CA USA. [Anderson, R. C.; Beegle, L. W.; Carsten, J. L.; Deen, R. G.; Jandura, L.; Kuhn, S. R.; Limonadi, D.; Robinson, M. L.; Seybold, C.; Tompkins, V. V.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Goetz, W.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Herkenhoff, K. E.] US Geol Survey, Flagstaff, AZ 86001 USA. [Hurowitz, J. A.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. [Kocurek, G.] Univ Texas Austin, Jackson Sch Geosci, Austin, TX 78712 USA. [Madsen, M. B.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Olson, T. S.] Salish Kootenai Coll, Dept Informat Technol & Comp Engn, Pablo, MT USA. [Rowland, S. K.] Univ Hawaii Manoa, Dept Geol & Geophys, Honolulu, HI 96822 USA. [Rubin, D. M.] US Geol Survey, Menlo Pk, CA 94025 USA. [Schieber, J.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA. [Schmidt, M.] Brock Univ, Dept Earth Sci, St Catharines, ON L2S 3A1, Canada. [Sumner, D. Y.] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. RP Minitti, ME (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM minitti@me.com OI Edgett, Kenneth/0000-0001-7197-5751 FU Jet Propulsion Laboratory, California Institute of Technology, under National Aeronautics and Space Administration FX This work results from MSL science activities performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Our thanks are extended to the entire MSL Science team, and particularly R.J. Sullivan, for the enthusiastic discussion and thought-provoking comments; we accept all errors as our own. We also thank the entire MSL Mastcam/MAHLI/MARDI operations and science teams for their endless generosity and expertise. We particularly acknowledge the efforts of J.N. Maki, M.A. Caplinger, M.A. Ravine, K.D. Supulver, and B. Duston for assistance with data collection and analyses related to motor count/range characterization. Constructive reviews by Lori Fenton, Jim Zimbelman, David Baratoux, and an anonymous reviewer improved the paper. NR 88 TC 19 Z9 19 U1 1 U2 12 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 NOV PY 2013 VL 118 IS 11 BP 2338 EP 2360 DI 10.1002/2013JE004426 PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 270YJ UT WOS:000328355300006 ER PT J AU Yingst, RA Kah, LC Palucis, M Williams, RME Garvin, J Bridges, JC Bridges, N Deen, RG Farmer, J Gasnault, O Goetz, W Hamilton, VE Hipkin, V Jensen, JK King, PL Koefoed, A Le Mouelic, SP Madsen, MB Mangold, N Martinez-Frias, J Maurice, S McCartney, EM Newsom, H Pariser, O Sautter, VH Wiens, RC AF Yingst, R. A. Kah, L. C. Palucis, M. Williams, R. M. E. Garvin, J. Bridges, J. C. Bridges, N. Deen, R. G. Farmer, J. Gasnault, O. Goetz, W. Hamilton, V. E. Hipkin, V. Jensen, J. K. King, P. L. Koefoed, A. Le Mouelic, S. P. Madsen, M. B. Mangold, N. Martinez-Frias, J. Maurice, S. McCartney, E. M. Newsom, H. Pariser, O. Sautter, V. H. Wiens, R. C. TI Characteristics of pebble- and cobble-sized clasts along the Curiosity rover traverse from Bradbury Landing to Rocknest SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; transport properties; fluvial processes; surface materials ID GALE-CRATER; EARLY MARS; SITE; SURFACE; VENTIFACTS; ROCKS; VENUS; SHAPE AB We have assessed the characteristics of clasts along Curiosity's traverse to shed light on the processes important in the genesis, modification, and transportation of surface materials. Pebble- to cobble-sized clasts at Bradbury Landing, and subsequently along Curiosity's traverse to Yellowknife Bay, reflect a mixing of two end-member transport mechanisms. The general clast population likely represents material deposited via impact processes, including meteorite fragments, ejecta from distant craters, and impactites consisting of shocked and shock-melted materials from within Gale Crater, which resulted predominantly in larger, angular clasts. A subset of rounded pebble-sized clasts has likely been modified by intermittent alluvial or fluvial processes. The morphology of this rounded clast population indicates that water was a more important transporting agent here than at other Mars sites that have been studied in situ. Finally, we identified populations of basalt clasts and porphyritic clasts of undetermined composition by their morphologic and textural characteristics; basalts are confirmed by geochemical data provided by ChemCam. C1 [Yingst, R. A.; Williams, R. M. E.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Kah, L. C.] Univ Tennessee, Knoxville, TN USA. [Palucis, M.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Garvin, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bridges, J. C.] Univ Leicester, Dept Phys & Astron, Space Res Ctr, Leicester LE1 7RH, Leics, England. [Bridges, N.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Deen, R. G.; Pariser, O.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Farmer, J.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Gasnault, O.; Le Mouelic, S. P.; Mangold, N.; Maurice, S.] CNRS, UMR 6112, Lab Planetol & Geodynam Nantes, Nantes, France. [Gasnault, O.; Le Mouelic, S. P.; Mangold, N.; Maurice, S.] Univ Nantes, Nantes, France. [Goetz, W.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Hamilton, V. E.] SW Res Inst, Dept Space Studies, Boulder, CO USA. [Hipkin, V.] Canadian Space Agcy, St Hubert, PQ, Canada. [Jensen, J. K.; Koefoed, A.; Madsen, M. B.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [King, P. L.] Australian Natl Univ, Res Sch Earth Sci, Coll Phys & Math Sci, Canberra, ACT, Australia. [Martinez-Frias, J.] CSIC UCM, Inst Geosci, Fac Ciencias Geol, Madrid, Spain. [McCartney, E. M.] Malin Space Sci Syst, San Diego, CA USA. [Newsom, H.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. [Sautter, V. H.] MNHN, LMCM, Paris, France. [Wiens, R. C.] Los Alamos Natl Lab, Los Alamos, NM USA. RP Yingst, RA (reprint author), Planetary Sci Inst, 1700 E Ft Lowell,Ste 106, Tucson, AZ 85719 USA. EM yingst@psi.edu RI King, Penelope/A-1791-2011; OI King, Penelope/0000-0002-8364-9168; Gasnault, Olivier/0000-0002-6979-9012 FU Mars Science Laboratory Program through Malin Space Science Systems [08-0315]; Danish Council for Independent Research/Natural Sciences (FNU) [12-127126, 11-107019]; TICRA Foundation; Deutsche Forschungsgemeinschaft (DFG) [GO 2288/1-1]; National Aeronautics and Space Administration FX We gratefully acknowledge the constructive reviews whose comments improved this manuscript. This research was supported by the Mars Science Laboratory Program through Malin Space Science Systems contract 08-0315 to R.A.Y. We thank Hallie E. Gengl, JPL's OPGS team, for processing the standard clast survey images for stereo analysis by generating the 3-D local-level maps. Work in Denmark was funded by the Danish Council for Independent Research/Natural Sciences (FNU grants 12-127126 and 11-107019) and the TICRA Foundation. Work in Germany was funded by the Deutsche Forschungsgemeinschaft (DFG grant GO 2288/1-1). The work of R. Deen, O. Pariser, and Hallie Gengl was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 84 TC 16 Z9 16 U1 4 U2 20 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 NOV PY 2013 VL 118 IS 11 BP 2361 EP 2380 DI 10.1002/2013JE004435 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 270YJ UT WOS:000328355300007 ER PT J AU Jun, I Mitrofanov, I Litvak, ML Sanin, AB Kim, W Behar, A Boynton, WV DeFlores, L Fedosov, F Golovin, D Hardgrove, C Harshman, K Kozyrev, AS Kuzmin, RO Malakhov, A Mischna, M Moersch, J Mokrousov, M Nikiforov, S Shvetsov, VN Tate, C Tret'yakov, VI Vostrukhin, A AF Jun, I. Mitrofanov, I. Litvak, M. L. Sanin, A. B. Kim, W. Behar, A. Boynton, W. V. DeFlores, L. Fedosov, F. Golovin, D. Hardgrove, C. Harshman, K. Kozyrev, A. S. Kuzmin, R. O. Malakhov, A. Mischna, M. Moersch, J. Mokrousov, M. Nikiforov, S. Shvetsov, V. N. Tate, C. Tret'yakov, V. I. Vostrukhin, A. TI Neutron background environment measured by the Mars Science Laboratory's Dynamic Albedo of Neutrons instrument during the first 100 sols SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Martian neutron environment; DAN; MSL; MMRTG; GCR; Rocknest ID INTRANUCLEAR-CASCADE CALCULATION; GAMMA-RAY; DAN EXPERIMENT; SPECTROMETER; TRANSPORT; ONBOARD; MCNPX AB The Dynamic Albedo of Neutrons (DAN) instrument on board Mars Science Laboratory has been operating successfully since the landing and has been making measurements regularly along Curiosity's traverse at the surface. DAN measures thermal (E<0.4eV) and epithermal neutrons (0.4eV 5 mu m and diffusion charging for d < 2 mu m. The low E proportionally decreases both Pauthenier particle charging and the F = qE collection force. This greatly reduces the particle migration velocities (w), e. g., for d = 10 mu m, w = 0.01 m/s compared with 0.4 m/s on Earth. However, for small particles (d = 1 mu m), this is compensated by diffusion charging and reduced drag (w = 0.04 m/s on Mars, 0.05 m/s on Earth). The Martian atmosphere was simulated with 95% CO2/5% humid air at 9 mbar. Paschen curves were measured, and I-V curves (I similar to 5-300 mu A for V similar to 1.3-2.3 kV) were obtained for 5-10-cm-diameter wire/rod-cylinder ESPs. Only positive polarity yielded stable uniform corona. Charging of 0.5-1.3-cm-diameter spheres agreed with the Pauthenier theory. A Martian dust simulant collection efficiency test is in progress. C1 [Clements, J. Sidney; Thompson, Samuel M.; Cox, Nathanael D.] Appalachian State Univ, Dept Phys & Astron, Boone, NC 28608 USA. [Johansen, Michael R.; Hogue, Michael D.; Calle, Carlos I.] NASA, Electrostat & Surface Phys Lab, Kennedy Space Ctr, FL 32899 USA. [Williams, Blakeley S.] Univ S Alabama, Mobile, AL 36688 USA. [Lowder, M. Loraine] Atlanta Metropolitan Coll, Div Sci Math & Hlth Profess, Atlanta, GA 30310 USA. RP Clements, JS (reprint author), Appalachian State Univ, Dept Phys & Astron, Boone, NC 28608 USA. EM clementsjs@appstate.edu; samuelmaxton@gmail.com; nathanael.d.cox@gmail.com; michael.r.johansen@nasa.gov; blakeleyshay@gmail.com; michael.d.hogue@nasa.gov; mlowder@atlm.edu; carlos.i.calle@nasa.gov RI Cox, Nathanael/A-2564-2017 OI Cox, Nathanael/0000-0003-0843-9141 NR 24 TC 2 Z9 3 U1 2 U2 32 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0093-9994 EI 1939-9367 J9 IEEE T IND APPL JI IEEE Trans. Ind. Appl. PD NOV-DEC PY 2013 VL 49 IS 6 BP 2388 EP 2396 DI 10.1109/TIA.2013.2263782 PG 9 WC Engineering, Multidisciplinary; Engineering, Electrical & Electronic SC Engineering GA 259UT UT WOS:000327552500003 ER PT J AU Patel, VK Robinson, F Seyed-Yagoobi, J Didion, J AF Patel, Viral K. Robinson, Franklin Seyed-Yagoobi, Jamal Didion, Jeffrey TI Terrestrial and Microgravity Experimental Study of Microscale Heat-Transport Device Driven by Electrohydrodynamic Conduction Pumping SO IEEE TRANSACTIONS ON INDUSTRY APPLICATIONS LA English DT Article; Proceedings Paper CT Electrostatics Joint Conference CY JUN 12-14, 2012 CL Cambridge, CANADA DE Dielectric liquids; electrohydrodynamics (EHDs); microgravity; micropumps ID PIPES AB Research on heat transport in microscale has been generating much interest in the recent years due to the development of state-of-the-art high-powered electronics used in aerospace and terrestrial applications and the large amount of heat produced during their operation. Microscale two-phase-flow heat-transport devices are seen as one solution to this problem of high heat-flux removal. Microscale devices have extremely high heat fluxes due to the small heat-transfer surface area. In addition, the need for robust, nonmechanical, lightweight, low-noise, and low-vibration devices in specialized aerospace applications has led researchers to investigate electrically driven flow devices rather than their mechanical counterparts. This paper, for the first time, presents the results of an experimental study of a unique microscale heat-transport device that is driven by electrohydrodynamic (EHD) conduction pumping. Results from ground-based single-phase experiments with a microscale EHD pump are compared with experiments conducted on board a variable-gravity parabolic flight. Data show that the EHD pump functions well in both environments and can be potentially used in heat-transport devices in the absence of gravity. This is the first step in broader-scale future experimental work that will involve heat transfer, including phase change. C1 [Patel, Viral K.; Seyed-Yagoobi, Jamal] Worcester Polytech Inst, Dept Mech Engn, Worcester, MA 01609 USA. [Robinson, Franklin; Didion, Jeffrey] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Patel, VK (reprint author), Worcester Polytech Inst, Dept Mech Engn, Worcester, MA 01609 USA. EM vkpatel@wpi.edu; franklin.l.robinson@nasa.gov; jyagoobi@wpi.edu; jeffrey.r.didion@nasa.gov NR 13 TC 6 Z9 6 U1 2 U2 19 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0093-9994 EI 1939-9367 J9 IEEE T IND APPL JI IEEE Trans. Ind. Appl. PD NOV-DEC PY 2013 VL 49 IS 6 BP 2397 EP 2401 DI 10.1109/TIA.2013.2264042 PG 5 WC Engineering, Multidisciplinary; Engineering, Electrical & Electronic SC Engineering GA 259UT UT WOS:000327552500004 ER PT J AU Siegel, PH AF Siegel, P. H. TI SPECIAL ISSUE ON TERAHERTZ METAMATERIALS AND APPLICATIONS SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Editorial Material C1 [Siegel, P. H.] CALTECH, Pasadena, CA 91125 USA. [Siegel, P. H.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Siegel, PH (reprint author), CALTECH, Pasadena, CA 91125 USA. NR 0 TC 0 Z9 0 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD NOV PY 2013 VL 3 IS 6 SI SI BP 685 EP 688 DI 10.1109/TTHZ.2013.2285652 PG 4 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 262GZ UT WOS:000327723600003 ER PT J AU Siegel, PH AF Siegel, Peter H. TI Terahertz Pioneers SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Editorial Material C1 [Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91125 USA. [Siegel, Peter H.] CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA. [Siegel, Peter H.] NASA, Jet Prop Lab, Pasadena, CA USA. RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91125 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD NOV PY 2013 VL 3 IS 6 SI SI BP 692 EP 692 DI 10.1109/TTHZ.2013.2285321 PG 1 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 262GZ UT WOS:000327723600005 ER PT J AU Meringer, M Cleaves, HJ Freeland, SJ AF Meringer, Markus Cleaves, H. James, II Freeland, Stephen J. TI Beyond Terrestrial Biology: Charting the Chemical Universe of alpha-Amino Acid Structures SO JOURNAL OF CHEMICAL INFORMATION AND MODELING LA English DT Article ID SPARK DISCHARGE EXPERIMENT; GENETIC-CODE; INTERSTELLAR GLYCINE; SMALL MOLECULES; ORIGIN; EVOLUTION; ENUMERATION; GENERATION; CHEMISTRY; PEPTIDES AB alpha-Amino acids are fundamental to biochemistry as the monomeric building blocks with which cells construct proteins according to genetic instructions. However, the 20 amino acids of the standard genetic code represent a tiny fraction of the number of alpha-amino acid chemical structures that could plausibly play such a role, both from the perspective of natural processes by which life emerged and evolved, and from the perspective of human-engineered genetically coded proteins. Until now, efforts to describe the structures comprising this broader set, or even estimate their number, have been hampered by the complex combinatorial properties of organic molecules. Here, we use computer software based on graph theory and constructive combinatorics in order to conduct an efficient and exhaustive search of the chemical structures implied by two careful and precise definitions of the alpha-amino acids relevant to coded biological proteins. Our results include two virtual libraries of alpha-amino acid structures corresponding to these different approaches, comprising 121 044 and 3 846 structures, respectively, and suggest a simple approach to exploring much larger, as yet uncomputed, libraries of interest. C1 [Meringer, Markus] German Aerosp Ctr DLR, Earth Observat Ctr, D-82234 Oberpfaffenhofen, Germany. [Cleaves, H. James, II] Tokyo Inst Technol, Earth Life Sci Inst, Meguro Ku, Tokyo 1528550, Japan. [Cleaves, H. James, II] Inst Adv Study, Princeton, NJ 08540 USA. [Cleaves, H. James, II] Blue Marble Space Inst Sci, Washington, DC 20016 USA. [Cleaves, H. James, II] Georgia Inst Technol, Ctr Chem Evolut, Atlanta, GA 30332 USA. [Freeland, Stephen J.] Univ Hawaii, NASA, Astrobiol Inst, Honolulu, HI 96822 USA. RP Cleaves, HJ (reprint author), Tokyo Inst Technol, Earth Life Sci Inst, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528550, Japan. EM cleaves@ias.edu RI Meringer, Markus/F-8297-2010 OI Meringer, Markus/0000-0001-8526-2429 FU NASA Astrobiology Institute [NNA09DA77A] FX The authors would like to thank the University of Hawaii's NASA Astrobiology Institute and Institute for Astronomy for generous housing support for M.M. and H.J.C. The authors would also like to thank the NASA Astrobiology Institute's Director's Discretionary Fund for seed funding for this project as part of the NASA Astrobiology Institute under Cooperative Agreement No. NNA09DA77A issued through the Office of Space Science. NR 69 TC 6 Z9 6 U1 3 U2 19 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1549-9596 EI 1549-960X J9 J CHEM INF MODEL JI J. Chem Inf. Model. PD NOV PY 2013 VL 53 IS 11 BP 2851 EP 2862 DI 10.1021/ci400209n PG 12 WC Chemistry, Medicinal; Chemistry, Multidisciplinary; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Pharmacology & Pharmacy; Chemistry; Computer Science GA 262OX UT WOS:000327747200008 PM 24152173 ER PT J AU Delgado, L Prats, X Sridhar, B AF Delgado, Luis Prats, Xavier Sridhar, Banavar TI Cruise speed reduction for ground delay programs: A case study Cross Mark for San Francisco International Airport arrivals SO TRANSPORTATION RESEARCH PART C-EMERGING TECHNOLOGIES LA English DT Article DE Ground delay program; Speed reduction; Airborne delay; Delay recovery; Fuel consumption; K-means clustering ID TRAFFIC FLOW MANAGEMENT; HOLDING PROBLEM; CAPACITY AB Ground Delay Programs (GDP) are sometimes cancelled before their initial planned duration and for this reason aircraft are delayed when it is no longer needed. Recovering this delay usually leads to extra fuel consumption, since the aircraft will typically depart after having absorbed on ground their assigned delay and, therefore, they will need to cruise at more fuel consuming speeds. Past research has proposed speed reduction strategy aiming at splitting the GDP-assigned delay between ground and airborne delay, while using the same fuel as in nominal conditions. Being airborne earlier, an aircraft can speed up to nominal cruise speed and recover part of the GDP delay without incurring extra fuel consumption if the GDP is cancelled earlier than planned. In this paper, all GDP initiatives that occurred in San Francisco International Airport during 2006 are studied and characterised by a K-means algorithm into three different clusters. The centroids for these three clusters have been used to simulate three different GDPs at the airport by using a realistic set of inbound traffic and the Future Air Traffic Management Concepts Evaluation Tool (FACET). The amount of delay that can be recovered using this cruise speed reduction technique, as a function of the GDP cancellation time, has been computed and compared with the delay recovered with the current concept of operations. Simulations have been conducted in calm wind situation and without considering a radius of exemption. Results indicate that when aircraft depart early and fly at the slower speed they can recover additional delays, compared to current operations where all delays are absorbed prior to take-off, in the event the GDP cancels early. There is a variability of extra delay recovered, being more significant, in relative terms, for those GDPs with a relatively low amount of demand exceeding the airport capacity. C1 [Delgado, Luis] UPC, Off C3 120, Castelldefels Telecommun & Aeronaut Engn Sch EETA, Castelldefels 08860, Catalonia, Spain. [Prats, Xavier] UPC, Off C3 104, Castelldefels Telecommun & Aeronaut Engn Sch EETA, Castelldefels 08860, Catalonia, Spain. [Sridhar, Banavar] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. RP Delgado, L (reprint author), UPC, Off C3 120, Castelldefels Telecommun & Aeronaut Engn Sch EETA, Av Esteve Terradas 5, Castelldefels 08860, Catalonia, Spain. EM luis.delgado@upc.edu OI Delgado, Luis/0000-0003-4613-4277 NR 30 TC 5 Z9 5 U1 1 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0968-090X J9 TRANSPORT RES C-EMER JI Transp. Res. Pt. C-Emerg. Technol. PD NOV PY 2013 VL 36 BP 83 EP 96 DI 10.1016/j.trc.2013.07.011 PG 14 WC Transportation Science & Technology SC Transportation GA 264WX UT WOS:000327912800008 ER PT J AU Laurent, O Wu, J Li, LF Milesi, C AF Laurent, Olivier Wu, Jun Li, Lianfa Milesi, Cristina TI Green spaces and pregnancy outcomes in Southern California SO HEALTH & PLACE LA English DT Article DE Green space; Greenness; Premature birth; Birth weight; Preeclampsia ID AIR-POLLUTION; SURROUNDING GREENNESS; HEALTH; URBANITY; EXPOSURE; COHORT AB Little is known about the impacts of green spaces on pregnancy outcomes. The relationship between green space exposure and preeclampsia has never been studied. We used a hospital-based perinatal database including more than 80,000 births to study the relationships between greenness exposure and three pregnancy outcomes: birth weight in term born infants, preterm deliveries and preeclampsia. Greenness was characterized using the normalized difference vegetation index (NDVI) within circular buffers surrounding maternal homes. Analyses were conducted using generalized estimating equations, adjusted for potential confounders. We observed an increase in birth weight in term born infants and a reduced risk of preterm births associated with an increase in NDVI. No significant association was observed between greenness and preeclampsia. This study provides modest support for beneficial effects of greenness exposure on pregnancy outcomes and calls for confirmation in other study settings. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Laurent, Olivier; Wu, Jun; Li, Lianfa] Univ Calif Irvine, Program Publ Hlth, Irvine, CA 92697 USA. [Milesi, Cristina] Calif State Univ Monterey Bay, Dept Sci & Environm Policy, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Wu, J (reprint author), Univ Calif Irvine, Program Publ Hlth, Anteater Instruct & Res Bldg AIRB,653 East Peltas, Irvine, CA 92697 USA. EM olaurent@uci.edu; junwu@uci.edu; lianfal@uci.edu; cristina.milesi-1@nasa.gov FU Health Effect Institute [HEI 4787-RFA09-4110-3 WU]; National Institute of Environmental Health Sciences [NIEHS R21ES016379] FX The study was supported by the Health Effect Institute (HEI 4787-RFA09-4110-3 WU) and the National Institute of Environmental Health Sciences (NIEHS R21ES016379). The funding sources had no role in the study design, in the collection, analysis, NR 24 TC 24 Z9 24 U1 5 U2 23 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1353-8292 EI 1873-2054 J9 HEALTH PLACE JI Health Place PD NOV PY 2013 VL 24 BP 190 EP 195 DI 10.1016/j.healthplace.2013.09.016 PG 6 WC Public, Environmental & Occupational Health SC Public, Environmental & Occupational Health GA 252DO UT WOS:000326985300024 PM 24140704 ER PT J AU Meyers, VE Garcia, HD McMullin, TS Tobin, JM James, JT AF Meyers, Valerie E. Garcia, Hector D. McMullin, Tami S. Tobin, Joseph M. James, John T. TI Safe human exposure limits for airborne linear siloxanes during spaceflight SO INHALATION TOXICOLOGY LA English DT Article DE Inhalation; siloxane; spaceflight ID RISK-ASSESSMENT; LIVER-DISEASE; MECHANISMS; SILICONE; HEXAMETHYLDISILOXANE; RELEVANCE; IMPLANTS AB Background: Low molecular weight siloxanes are used in industrial processes and consumer products, and their vapors have been detected in the atmospheres of the Space Shuttle and International Space Station. Therefore, the National Aeronautics and Space Administration (NASA) developed spacecraft maximum allowable concentrations (SMACs) for siloxane vapors to protect astronaut health. Since publication of these original SMACs, new studies and new risk assessment approaches have been published that warrant re-examination of the SMACs. Objective: To reevaluate SMACs published for octamethyltrisiloxane (L3) for exposures ranging from 1 hour to 180 days, to develop a 1000-day SMAC, and to expand the applicability of those values to the family of linear siloxanes. Methods: A literature review was conducted to identify studies conducted since the SMACs for L3 were set in 1994. The updated data were reviewed to determine the sensitive toxicity endpoints, and current risk assessment approaches and methods for dosimetric adjustments were evaluated. Results: Recent data were used to update the original 1-hour, 24-hour, 30-day, and 180-day SMACs for L3, and a 1000-day SMAC was developed to protect crewmembers during future exploration beyond Earth orbit. Group SMACs for the linear siloxane family, including hexamethyldisiloxane (L2), L3, decamethyltetrasiloxane (L4), and dodecamethylpentasiloxane (L5), were set for exposures of 1-hour to 1000 days. Conclusion: New SMACs, based on acute pulmonary and neurotoxicity at high doses only achievable with L2 and potential liver effects following longer-term exposures to L2 and L3, were established to protect crewmembers from the adverse effects of exposure to linear siloxanes. C1 [Meyers, Valerie E.; James, John T.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Garcia, Hector D.] Wyle Sci Technol & Engn Grp, Houston, TX USA. [McMullin, Tami S.; Tobin, Joseph M.] Dow Corning Corp, Hlth & Environm Sci, Midland, MI USA. RP Meyers, VE (reprint author), NASA, Lyndon B Johnson Space Ctr, MC SK, 2010 NASA Pkwy, Houston, TX 77058 USA. EM valerie.e.meyers@nasa.gov FU NASA Johnson Space Center; Wyle Bioastronautics [NAS9-02078] FX This evaluation was supported by NASA Johnson Space Center and Wyle Bioastronautics Contract #NAS9-02078. Studies were provided by Dow Corning Corporation, a manufacturer of siloxanes, and technical input was provided by two employees of Dow Corning Corporation who are included as authors. NR 39 TC 1 Z9 1 U1 0 U2 11 PU INFORMA HEALTHCARE PI LONDON PA TELEPHONE HOUSE, 69-77 PAUL STREET, LONDON EC2A 4LQ, ENGLAND SN 0895-8378 EI 1091-7691 J9 INHAL TOXICOL JI Inhal. Toxicol. PD NOV PY 2013 VL 25 IS 13 BP 735 EP 746 DI 10.3109/08958378.2013.845629 PG 12 WC Toxicology SC Toxicology GA 258NF UT WOS:000327465300004 PM 24255951 ER PT J AU Mayr, HG Talaat, ER Wolven, BC AF Mayr, Hans G. Talaat, Elsayed R. Wolven, Brian C. TI Global propagation of gravity waves generated with the whole atmosphere transfer function model SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Review DE Theoretical spectral model; Global gravity wave propagation; Auroral gravity wave source; Thermospheric; Ducted; Earth reflected waves ID DISSIPATIVE MULTICONSTITUENT MEDIUM; DEEP TROPICAL CONVECTION; EARTHS THERMOSPHERE; MIDDLE ATMOSPHERE; IONOSPHERIC DISTURBANCES; NEUTRAL COMPOSITION; DYNAMICS EXPLORER; VERTICAL MOTIONS; AE-C; EXCITATION AB A brief review is presented of the Transfer Function Model (TFM) [e.g., Mayr et al., Space Science Reviews, 19901, which describes acoustic gravity waves (AGW) that propagate across the globe in a dissipative and static (no winds) background atmosphere with globally uniform temperature and density variations extending from the ground to 700 km. Unique among existing models, the TFM can be placed between the analytical approach on one end, and the rigorous numerical approach of general circulation models (GCM). The time consuming numerical integration of the conservation equations is restricted to compute the transfer function (TF) for a broad range of frequencies and spherical harmonics. Given TF, the atmospheric response for a chosen source configuration is then obtained in short order. Computationally efficient, the model is well suited to serve as experimental and educational tool for simulating propagating wave patterns across the globe. By design, the TFM is also semi-analytical and therefore well suited to explore the different wave modes that can be generated under different dynamical conditions. (C) 2013 The Authors. Published by Elsevier Ltd. All rights reserved. C1 [Mayr, Hans G.; Talaat, Elsayed R.; Wolven, Brian C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Mayr, Hans G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Mayr, HG (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM hans.mayr@jhuapl.edu OI Wolven, Brian/0000-0003-2858-2332 NR 51 TC 1 Z9 1 U1 0 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD NOV PY 2013 VL 104 BP 7 EP 17 DI 10.1016/j.jastp.2013.08.001 PG 11 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 255IH UT WOS:000327232100002 ER PT J AU Goldberg, RA Feofilov, AG Pesnell, WD Kutepov, AA AF Goldberg, R. A. Feofilov, A. G. Pesnell, W. D. Kutepov, A. A. TI Inter-hemispheric coupling during northern polar summer periods of 2002-2010 using TIMED/SABER measurements SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Inter-hemispheric-coupling; Polar summer; Stratospheric warming ID MACWAVE/MIDAS ROCKET; WAVE ACTIVITY; PROGRAM; CIRCULATION; MESOSPHERE; MODEL AB It has been found that for more than one polar summer season between 2002 and 2010, the northern polar mesospheric region near and above about 80 km was warmer than normal. The strongest warming effect of this type was observed to occur during northern summer 2002. Observational and theoretical studies imply that these "anomalies" were preceded by unusual dynamical processes in the southern hemisphere. We have analyzed temperature distributions measured by the SABER limb scanning infrared radiometer aboard the NASA TIMED satellite between 2002 and 2010 at altitudes from 15 to 110 km and for latitudes between 83 degrees S and 83 degrees N. We describe the approach to trace the spatial extent of inter-hemispheric temperature correlations demonstrating the global features that were unique for the "anomalous" northern polar summers. From our analysis of SABER data from 2002 to 2010, the anomalous heating for the northern mesopause region during northern summer was accompanied by stratospheric heating in the equatorial region. In the winter hemisphere it is accompanied by heating in the lower stratosphere and mesopause region, and cooling in the stratopause region. Also, all the elements of the temperature anomaly structure appear to develop and fade away nearly simultaneously, thereby suggesting either a global influence or a short lagging period (less than 7 days). Published by Elsevier Ltd. C1 [Goldberg, R. A.; Feofilov, A. G.; Pesnell, W. D.; Kutepov, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Feofilov, A. G.; Kutepov, A. A.] Catholic Univ Amer, Washington, DC 20064 USA. RP Goldberg, RA (reprint author), NASA, Goddard Space Flight Ctr, Mailcode 674,Greenbelt Rd, Greenbelt, MD 20771 USA. EM richard.a.goldberg@nasa.gov RI Pesnell, William/D-1062-2012; Feofilov, Artem/A-2271-2015 OI Pesnell, William/0000-0002-8306-2500; Feofilov, Artem/0000-0001-9924-4846 FU NASA [NNX08AL12G] FX The work of A Feofilov and A Kutepov was supported by NASA grant NNX08AL12G. The authors thank two anonymous reviewers for their thoughtful comments on the manuscript and Alexander Medvedev for the discussion on atmospheric circulation mechanisms. NR 20 TC 3 Z9 3 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD NOV PY 2013 VL 104 BP 277 EP 284 DI 10.1016/j.jastp.2012.11.018 PG 8 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 255IH UT WOS:000327232100027 ER PT J AU Liu, CH Kawata, T Zhou, GM Furusawa, Y Kota, R Kumabe, A Sutani, S Fukada, J Mishima, M Shigematsu, N George, K Cucinotta, F AF Liu, Cuihua Kawata, Tetsuya Zhou, Guangming Furusawa, Yoshiya Kota, Ryuichi Kumabe, Atsuhiro Sutani, Shinya Fukada, Junichi Mishima, Masayo Shigematsu, Naoyuki George, Kerry Cucinotta, Francis TI Comparison of the repair of potentially lethal damage after low- and high-LET radiation exposure, assessed from the kinetics and fidelity of chromosome rejoining in normal human fibroblasts SO JOURNAL OF RADIATION RESEARCH LA English DT Article DE heavy ion; PLDR (potentially lethal damage repair); premature chromosome condensation; FISH (fluorescence in situ hybridization); misrepair ID IRRADIATED HUMAN-CELLS; IN-SITU HYBRIDIZATION; X-RAY; EXCHANGE FORMATION; ENHANCED FIDELITY; HUMAN-LYMPHOCYTES; DNA-DAMAGE; HEAVY-IONS; BREAKS; CONDENSATION AB Potentially lethal damage (PLD) and its repair (PLDR) were studied in confluent human fibroblasts by analyzing the kinetics of chromosome break rejoining after X-ray or heavy-ion exposures. Cells were either held in the non-cycling G(0) phase of the cell cycle for 12 h, or forced to proliferate immediately after irradiation. Fusion premature chromosome condensation (PCC) was combined with fluorescence in situ hybridization (FISH) to study chromosomal aberrations in interphase. The culture condition had no impact on the rejoining kinetics of PCC breaks during the 12 h after X-ray or heavy-ion irradiation. However, 12 h after X-ray and silicon irradiation, cycling cells had more chromosome exchanges than non-cycling cells. After 6 Gy X-rays, the yield of exchanges in cycling cells was 2.8 times higher than that in non-cycling cells, and after 2 Gy of 55 keV/mu m silicon ions the yield of exchanges in cycling cells was twice that of non-cycling cells. In contrast, after exposure to 2 Gy 200-keV/mu m or 440-keV/mu m iron ions the yield of exchanges was similar in non-cycling and cycling cells. Since the majority of repair in G(0)/G(1) occurs via the non-homologous end joining process (NHEJ), increased PLDR in X-ray and silicon-ion irradiated cells may result from improved cell cycle-specific rejoining fidelity through the NHEJ pathway, which is not the case in high-LET iron-ion irradiated cells. C1 [Liu, Cuihua; Furusawa, Yoshiya] Natl Inst Radiol Sci, Res Ctr Charged Particle Therapy, Chiba 2638555, Japan. [Kawata, Tetsuya; Kota, Ryuichi; Kumabe, Atsuhiro; Sutani, Shinya; Fukada, Junichi; Mishima, Masayo; Shigematsu, Naoyuki] Keio Univ, Sch Med, Dept Radiol, Tokyo 1608582, Japan. [Zhou, Guangming] Chinese Acad Sci, Inst Modern Phys, Dept Space Radiobiol, Lanzhou 730000, Peoples R China. [George, Kerry] Wyle Integrated Sci & Engn Grp, Houston, TX USA. [Cucinotta, Francis] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Kawata, T (reprint author), Keio Univ, Sch Med, Dept Radiol, Tokyo 1608582, Japan. EM tkawata@rad.med.keio.ac.jp RI Shigematsu, Naoyuki/B-9374-2014; Furusawa, Yoshiya/A-4487-2012 OI Furusawa, Yoshiya/0000-0003-4213-7331 FU Heavy Ions at NIRS-HIMAC; NASA Radiation Health Program FX This study was supported by the research project with Heavy Ions at NIRS-HIMAC and the NASA Radiation Health Program. NR 37 TC 0 Z9 1 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0449-3060 EI 1349-9157 J9 J RADIAT RES JI J. Radiat. Res. PD NOV PY 2013 VL 54 IS 6 BP 989 EP 997 DI 10.1093/jrr/rrt031 PG 9 WC Biology; Radiology, Nuclear Medicine & Medical Imaging SC Life Sciences & Biomedicine - Other Topics; Radiology, Nuclear Medicine & Medical Imaging GA 258KT UT WOS:000327458900002 PM 23674607 ER PT J AU Mazin, BA Meeker, SR Strader, MJ Szypryt, P Marsden, D van Eyken, JC Duggan, GE Walter, AB Ulbricht, G Johnson, M Bumble, B O'Brien, K Stoughton, C AF Mazin, B. A. Meeker, S. R. Strader, M. J. Szypryt, P. Marsden, D. van Eyken, J. C. Duggan, G. E. Walter, A. B. Ulbricht, G. Johnson, M. Bumble, B. O'Brien, K. Stoughton, C. TI ARCONS: A 2024 Pixel Optical through Near-IR Cryogenic Imaging Spectrophotometer SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE Astronomical Instrumentation ID SUPERCONDUCTING TUNNEL-JUNCTIONS; RESOLUTION; DETECTOR; ARRAYS; ASTROPHYSICS; CRAB AB We present the design, construction, and commissioning results of ARCONS, the Array Camera for Optical to Near-IR Spectrophotometry. ARCONS is the first ground-based instrument in the optical through near-IR wavelength range based on microwave kinetic inductance detectors (MKIDs). MKIDs are revolutionary cryogenic detectors, capable of detecting single photons and measuring their energy without filters or gratings, similar to an X-ray microcalorimeter. MKIDs are nearly ideal, noiseless photon detectors, as they do not suffer from read noise or dark current and have nearly perfect cosmic ray rejection. ARCONS is an integral field spectrograph (IFS) containing a lens-coupled 2024 pixel MKID array yielding a 20xx20 field of view and has been deployed on the Palomar 200inch and Lick 120inch telescopes for 24 nights of observing. We present initial results showing that ARCONS and its MKID arrays are now a fully operational and powerful tool for astronomical observations. C1 [Mazin, B. A.; Meeker, S. R.; Strader, M. J.; Szypryt, P.; Marsden, D.; van Eyken, J. C.; Duggan, G. E.; Walter, A. B.; Ulbricht, G.; Johnson, M.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Bumble, B.] NASA Jet Prop Lab, Pasadena, CA 91125 USA. [O'Brien, K.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Stoughton, C.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. RP Mazin, BA (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. EM bmazin@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 [NNX11AD55G, NNX11AN29H]; NASA Office of the Chief Technologists Space Technology Research Fellowship; Keck Institute for Space Studies; Fermi Research Alliance, LLC [De-AC02-07CH11359]; United States Department of Energy FX The MKID detectors used in this work were developed under NASA grant NNX11AD55G. S. R. Meeker was supported by a NASA Office of the Chief Technologists Space Technology Research Fellowship, NASA grant NNX11AN29H. This work was partially supported by the Keck Institute for Space Studies. Fermilab is operated by Fermi Research Alliance, LLC under Contract No. De-AC02-07CH11359 with the United States Department of Energy. The authors would also like to thank Shri Kulkarni, Director of the Caltech Optical Observatories, and Jason Prochaska, Associate Director of Lick Observatory, for facilitating this project, as well as the excellent staffs of the Palomar and Lick Observatories for their assistance in getting ARCONS working. Jennifer Milburn's help with the guide camera software was invaluable. This project also greatly benefitted from the support of Mike Werner, Paul Goldsmith, and Jonas Zmuidzinas at JPL. Special thanks to Refree Stephen Shedman for valuable comments NR 40 TC 37 Z9 37 U1 0 U2 11 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD NOV 1 PY 2013 VL 125 IS 933 BP 1348 EP 1361 DI 10.1086/674013 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262DG UT WOS:000327713700007 ER PT J AU Herter, TL Vacca, WD Adams, JD Keller, LD Schoenwald, J Hirsch, L Wang, J De Buizer, JM Helton, LA Llorens, MC AF Herter, T. L. Vacca, W. D. Adams, J. D. Keller, L. D. Schoenwald, J. Hirsch, L. Wang, J. De Buizer, J. M. Helton, L. A. Llorens, M. C. TI Data Reduction and Early Science Calibration for FORCAST, A Mid-Infrared Camera for SOFIA SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE Data Analysis and Techniques ID MODEL ATMOSPHERES; INFRARED ASTRONOMY; OBSERVATORIES; STANDARDS; ASTEROIDS; SPECTRA; STARS AB FORCAST is a mid-infrared (5--40m) facility instrument for the Stratospheric Observatory for Infrared Astronomy (SOFIA). After achieving first light flight in 2010 May, FORCAST has completed two observatory characterization flights and thirteen science flights on SOFIA. In this paper we describe the photometric calibration of FORCAST which involves some subtleties in correction for array artifacts and uncertainties due to the airborne environment. At present FORCAST is able to achieve approximately 20% (3 sigma sigma) uncertainty in the calibration. C1 [Herter, T. L.; Adams, J. D.; Schoenwald, J.; Hirsch, L.; Wang, J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Vacca, W. D.; De Buizer, J. M.; Helton, L. A.; Llorens, M. C.] NASA, Univ Space Res Assoc, Ames Res Ctr, Moffett Field, CA 94035 USA. [Keller, L. D.] Ithaca Coll, Dept Phys, Ithaca, NY 14850 USA. RP Herter, TL (reprint author), Cornell Univ, Dept Astron, Space Sci Bldg, Ithaca, NY 14853 USA. OI Wang, Jason/0000-0003-0774-6502 FU Universities Space Research Association, Inc. (USRA), under NASA [NAS2-97001]; Deutsches SOFIA Institut (DSI) under DLR [50 OK 0901]; NASA [8500-98-014] FX This work is based on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). SOFIA science mission operations are conducted jointly 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. Financial support for FORCAST was provided by NASA through award 8500-98-014 issued by USRA. NR 25 TC 13 Z9 13 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD NOV 1 PY 2013 VL 125 IS 933 BP 1393 EP 1404 DI 10.1086/674144 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262DG UT WOS:000327713700011 ER PT J AU Dyar, MD Breves, E Jawin, E Marchand, G Nelms, M O'Connor, V Peel, S Rothstein, Y Sklute, EC Lane, MD Bishop, JL Mertzman, SA AF Dyar, M. Darby Breves, Elly Jawin, Erica Marchand, Gerard Nelms, Melissa O'Connor, Vanessa Peel, Samantha Rothstein, Yarrow Sklute, Elizabeth C. Lane, Melissa D. Bishop, Janice L. Mertzman, Stanley A. TI Mossbauer parameters of iron in sulfate minerals SO AMERICAN MINERALOGIST LA English DT Article DE Mossbauer; sulfate; jarosite; Mars ID HYDRATED FERRIC SULFATES; X-RAY-DIFFRACTION; SOLID-SOLUTION SERIES; CRYSTAL-STRUCTURE; CHEMICAL-COMPOSITION; MAGNETIC-PROPERTIES; BEARING MINERALS; MERIDIANI-PLANUM; HALOTRICHITE GROUP; ATOMIC-STRUCTURE AB Although Fe-sulfate minerals occur only rarely on Earth as alteration products of sulfidic basalts or in hydrothermal systems, multiple lines of evidence point to the importance of Fe- (and other) sulfate minerals on the surface of Mars. One such martian data set comes from the MIMOS II Mossbauer spectrometers on the Mars Exploration Rovers, which acquired hundreds of spectra from the martian surface at two locations. Interpretation of those spectra has been limited by the lack of a comprehensive set of laboratory analog spectra of the broad range of naturally occurring sulfate minerals. Accordingly, this study reports Mossbauer data of 98 samples representing 47 different sulfate mineral species, all containing six- or higher-coordinated Fe. The resultant Mossbauer parameters are related to the local polyhedral environment around the Fe cation in each mineral to explain variations in spectral characteristics. Results show that the size of the coordination polyhedron is the best predictor of quadrupole splitting, which increases with both octahedral volume and mean bond length. Species within groups of structurally similar minerals are shown to have comparable spectral peaks that generally fall within small ranges. Although coordination polyhedron geometry is not necessarily unique to any particular mineral species or group, Mossbauer data can be used to help constrain mineral identifications from martian spectra. The number of mineral species is large, but the range of crystal structures and hyperfine parameters may be small, so that in many cases, individual minerals cannot be uniquely fingerprinted. Examples would include quenstedtite, coquimbite, komelite, and lausenite, which have indistinguishable spectra, as do apjohnite, bilinite, dietrichite, and romerite. Overlap of Mossbauer parameters is a particular complication for identification of Fe3+-rich phases because the range of Mossbauer parameters for Fe3+ in any coordination number is so small. Previous analyses of martian Mossbauer spectra reported the presence of jarosite (Klingelhofer et al. 2004; Morris et al. 2004) and an unspecific ferric sulfate (Morris et al. 2008). New data presented here indicate that botryogen, metasideronatrite, and slavikite exhibit Mossbauer spectra similar to those attributed to jarosite at Meridiani Planum. Fibroferrite and rhomboclase have parameters similar to those observed at Arad Samra, and copiapite and parabutlerite could be present at Tyrone Mount Darwin and Berkner Island. Unique mineral identifications are generally not possible from Mossbauer data alone, particularly for paramagnetic phases, although combining Mossbauer results with other data sets enables a greater level of confidence in constraining mineralogy. This study provides a new expansive data set for future interpretation of iron sulfates on Mars. C1 [Dyar, M. Darby; Breves, Elly; Jawin, Erica; Marchand, Gerard; Nelms, Melissa; Peel, Samantha; Rothstein, Yarrow; Sklute, Elizabeth C.] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. [O'Connor, Vanessa] Smith Coll, Dept Geosci, Northampton, MA 01063 USA. [Lane, Melissa D.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Bishop, Janice L.] NASA, Ames Res Ctr, SETI Inst, Mountain View, CA 94043 USA. [Mertzman, Stanley A.] Franklin & Marshall Coll, Dept Earth & Environm, Lancaster, PA 17603 USA. RP Dyar, MD (reprint author), Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. EM mdyar@mtholyoke.eud OI Peel, Samantha/0000-0002-2285-6446 FU NSF [EAR-043907, EAR-0439161]; NASA [NNG04GG12G, NAG5-12687, NNX-11AF11G]; Massachusetts Space Grant Consortium FX We are grateful to Ed Cloutis, the Harvard Mineralogical Museum, and the NMNH for the loan of samples, and for support from NSF grants EAR-043907 and EAR-0439161 and NASA grants NNG04GG12G, NAG5-12687, and NNX-11AF11G. Student support for this project was provided by the Massachusetts Space Grant Consortium. Thoughtful suggestions from two anonymous reviewers and Juraj Majzlan were greatly appreciated. We thank David Palmer for help with the CrystalMaker models. This is PSI Contribution Number 605. NR 136 TC 7 Z9 8 U1 2 U2 37 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 NOV-DEC PY 2013 VL 98 IS 11-12 BP 1943 EP 1965 DI 10.2138/am.2013.4604 PG 23 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 252YP UT WOS:000327049100005 ER PT J AU Papike, JJ Burger, PV Bell, AS Le, L Shearer, CK Sutton, SR Jones, J Newville, M AF Papike, J. J. Burger, P. V. Bell, A. S. Le, L. Shearer, C. K. Sutton, S. R. Jones, J. Newville, M. TI Developing vanadium valence state oxybarometers (spinel-melt, olivine-melt, spinel-olivine) and V/(Cr plus Al) partitioning (spinet-melt) for martian olivine-phyric basalts SO AMERICAN MINERALOGIST LA English DT Article DE Vanadium; oxybarometry; Mars; Yamato 980459; spinel; olivine; XANES ID COMPARATIVE PLANETARY MINERALOGY; OXYGEN FUGACITY; UPPER-MANTLE; MARS; PETROGENESIS; CONSTRAINTS; SYSTEMATICS; REDOX; CRUST AB A spiked (with REE, V, Sc) martian basalt Yamato 980459 (Y98) composition was used to synthesize olivine, spinel, and pyroxene at 1200 degrees C at five oxygen fugacities: IW-1, IW, IW+1, IW+2, and QFM. These run products were analyzed by electron microprobe, ion microprobe, and X-ray absorption near-edge spectroscopy to establish four oxybarometers based on vanadium partitioning behavior between the following pairs of phases: V spinel-melt, V/(Cr+Al) spinel-melt, olivine-melt, and spinel-olivine. The results for the spinel-melt, olivine-melt, and V/(Cr+Al) spinel-melt are applicable for the entire oxygen fugacity range while the spinel-olivine oxybarometer is only applicable between IW-1 and IW+1. The oxybarometer based on V partitioning between spinel-olivine is restricted to basalts that crystallized under low oxygen fugacities, some martian, all lunar, as well as samples from 4 Vesta. The true potential and power of the new spinel-olivine oxybarometer is that it does not require samples representative of a melt composition or samples with some remnant of quenched melt present. It just requires that the spinel-olivine pairs were in equilibrium when the partitioning of V occurred. We have applied the V spinel-olivine oxybarometer to the Y98 meteorite as a test of the method. C1 [Papike, J. J.; Burger, P. V.; Bell, A. S.; Shearer, C. K.] Univ New Mexico, Inst Meteorit, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [Le, L.] NASA Johnson Space Ctr, JSC Engn Technol & Sci JETS, Houston, TX 77058 USA. [Newville, M.] Univ Chicago, Ctr Adv Radiat Sources, Chicago, IL 60637 USA. [Jones, J.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. RP Burger, PV (reprint author), Univ New Mexico, Inst Meteorit, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. EM pvburger@unm.edu FU NASA Cosmochemistry grants; National Science Foundation-Earth Sciences [EAR-1128799]; Department of Geosciences [DE-FG02-94ER14466]; U.S. Department of Energy, Office of Science, Office of Basic Energy Science [DE-AC02-06CH11357] FX This research was supported by NASA Cosmochemistry grants to C. Shearer and J. Jones. XANES spectra were collected at GeoSoilEnviroCARS (sector 13) Advanced Photon Source (APS), Argonne National Laboratory. We gratefully acknowledge the beamline award, as well as assistance of beamline staff. GeoSoilEnviroCARS is supported by the National Science Foundation-Earth Sciences (EAR-1128799) and Department of Geosciences (DE-FG02-94ER14466). Use of the Advanced Photon Source was supported by U.S. Department of Energy, Office of Science, Office of Basic Energy Science under contract no. DE-AC02-06CH11357. NR 18 TC 6 Z9 6 U1 1 U2 25 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 NOV-DEC PY 2013 VL 98 IS 11-12 BP 2193 EP 2196 DI 10.2138/am.2013.4622 PG 4 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 252YP UT WOS:000327049100028 ER PT J AU Hamilton, CW Glaze, LS James, MR Baloga, SM AF Hamilton, Christopher W. Glaze, Lori S. James, Mike R. Baloga, Stephen M. TI Topographic and stochastic influences on pahoehoe lava lobe emplacement SO BULLETIN OF VOLCANOLOGY LA English DT Article DE Topographic influences; Stochastic processes; Pahoehoe lava; Lobe emplacement ID KILAUEA VOLCANO; FLOOD LAVAS; MAUNA-ULU; FLOWS; HAWAII; MORPHOLOGY; INFLATION; MODEL; TUMULI; TUBES AB A detailed understanding of pahoehoe emplacement is necessary for developing accurate models of flow field development, assessing hazards, and interpreting the significance of lava morphology on Earth and other planetary surfaces. Active pahoehoe lobes on Kilauea Volcano, Hawai'i, were examined on 21-26 February 2006 using oblique time series stereo-photogrammetry and differential global positioning system measurements. During this time, the local discharge rate for peripheral lava lobes was generally constant at 0.0061 +/- 0.0019 m(3)/s, but the areal coverage rate of the lobes exhibited a periodic increase every 4.13 +/- 0.64 min. This periodicity is attributed to the time required for the pressure within the liquid lava core to exceed the cooling-induced strength of its margins. The pahoehoe flow advanced through a series of down-slope and cross-slope breakouts, which began as similar to 0.2-m-thick units (i.e., toes) that coalesced and inflated to become approximately meter-thick lobes. The lobes were thickest above the lowest points of the initial topography and above shallow to reverse-facing slopes, defined relative to the local flow direction. The flow path was typically controlled by high-standing topography, with the zone directly adjacent to the final lobe margin having an average relief that was a few centimeters higher than the lava-inundated region. This suggests that toe-scale topography can, at least temporarily, exert strong controls on pahoehoe flow paths by impeding the lateral spreading of the lobe. Observed cycles of enhanced areal spreading and inflated lobe morphology are also explored using a model that considers the statistical likelihood of sequential breakouts from active flow margins and the effects of topographic barriers. C1 [Hamilton, Christopher W.; Glaze, Lori S.] NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hamilton, Christopher W.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [James, Mike R.] Univ Lancaster, Lancaster Environm Ctr, Lancaster, England. [Baloga, Stephen M.] Proxemy Res, Laytonville, MD USA. RP Hamilton, CW (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM christopher.hamilton@nasa.gov RI James, Mike/C-6817-2008; Glaze, Lori/D-1314-2012 OI James, Mike/0000-0002-9177-2588; FU NASA [811073.02.01.04.44, 203959.02.03.17.56, NNX08AF16G, NNX10AP63G] FX We thank Benjamin Brooks and the Pacific GPS facility for providing access to DGPS survey equipment and post-processing resources, Samuel Hulme for his assistance with GMT, Richard Herd for kindly providing DGPS data for photogrammetry control, Andrew Harris for his assistance in the field making contemporaneous FLIR observations, Tim Orr for providing historical lava flow data shown in Fig. 1, as well as Sarah Fagents, Thorvaldur Thordarson, and Jacob Bleacher for many insightful discussions relating to lava flow emplacement. Prof. S. Robson and Prof. J. P. Muller are thanked for their ongoing support through the provision of VMS and GOTCHA, respectively. Christopher Kilburn and Jim Kauahikaua are sincerely thanked for their thorough and constructive reviews. Field work was conducted in Hawaii Volcanoes National Park under Scientific Research and Collecting Permit # HAVO-2006-SCI-0003. CWH 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. LSG and SMB research was supported by the NASA Planetary Geology and Geophysics and Mars Data Analysis programs (LSG, 811073.02.01.04.44 and 203959.02.03.17.56; SMB, NNX08AF16G and NNX10AP63G). NR 55 TC 8 Z9 8 U1 1 U2 13 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0258-8900 EI 1432-0819 J9 B VOLCANOL JI Bull. Volcanol. PD NOV PY 2013 VL 75 IS 11 AR 756 DI 10.1007/s00445-013-0756-8 PG 16 WC Geosciences, Multidisciplinary SC Geology GA 255LJ UT WOS:000327240200009 ER PT J AU Zacny, K Nagihara, S Hedlund, M Paulsen, G Shasho, J Mumm, E Kumar, N Szwarc, T Chu, P Craft, J Taylor, P Milam, M AF Zacny, K. Nagihara, S. Hedlund, M. Paulsen, G. Shasho, J. Mumm, E. Kumar, N. Szwarc, T. Chu, P. Craft, J. Taylor, P. Milam, M. TI Pneumatic and Percussive Penetration Approaches for Heat Flow Probe Emplacement on Robotic Lunar Missions SO EARTH MOON AND PLANETS LA English DT Article DE Moon; Heat flow; Heat flow probe; Drilling; Gas drilling; Percussive drilling; Penetrometer; Heat flow sensors; Heat flux; Lunar ID CONDUCTIVITY AB In this paper, the development of heat flow probes for measuring the geothermal gradient and conductivity of lunar regolith are presented. These two measurements are the required information for determining the heat flow of a planetary body. Considering the Moon as an example, heat flow properties are very important information for studying the radiogenic isotopes, the thermal evolution and differentiation history, and the mechanical properties of the interior. In order to obtain the best measurements, the sensors must be extended to a depth of at least 3 m, i.e. beyond the depth of significant thermal cycles. Two approaches to heat flow deployment and measurement are discussed in this paper: a percussive approach and a pneumatic approach. The percussive approach utilizes a high frequency hammer to drive a cone penetrometer into the lunar simulant. Ring-like thermal sensors (heaters and temperature sensors) on the penetrometer rod are deployed into the simulant every 30 cm as the penetrometer penetrates to the required 3 m depth. Once the target depth has been achieved, the deployment rod is removed from the simulant, eliminating any thermal path to the lander. The pneumatic approach relies on pressurized gas to excavate, using a cone-shaped nozzle to penetrate the simulant. The nozzle is attached to a coiled stem with thermal sensors embedded along the length of the stem. As the simulant is being lofted out of the hole by the escaping gas, the stem is progressively reeled out from a spool, thus moving the cone deeper into the hole. Thermal conductivity is measured using a needle probe attached to the end of the cone. Breadboard prototypes of these two heat flow probe systems have been constructed and successfully tested under lunar-like conditions to approximately 70 cm, which was the maximum possible depth allowed by the size of the test bin and the chamber. C1 [Zacny, K.; Hedlund, M.; Paulsen, G.; Chu, P.] Honeybee Robot, Pasadena, CA 91103 USA. [Nagihara, S.] Texas Tech Univ, Dept Geosci, Lubbock, TX 79409 USA. [Shasho, J.; Kumar, N.; Craft, J.] Honeybee Robot, New York, NY 10001 USA. [Mumm, E.] Honeybee Robot, Unit C, Longmont, CO 80501 USA. [Szwarc, T.] Stanford Univ, Stanford, CA 94035 USA. [Taylor, P.; Milam, M.] NASA GSFC, Greenbelt, MD 20771 USA. RP Zacny, K (reprint author), Honeybee Robot, 398 W Washington St,Suite 200, Pasadena, CA 91103 USA. EM zacny@honeybeerobotics.com; seiichi.nagihara@ttu.edu; hedlund@honeybeerobotics.com; paulsen@honeybeerobotics.com; Shasho@honeybeerobotics.com; mumm@honeybeerobotics.com; kumar@honeybeerobotics.com; tjs53@stanford.edu; chu@honeybeerobotics.com; craft@honeybeerobotics.com; patrick.t.taylor@nasa.gov; malcolm.b.milam@nasa.gov FU NASA through the Small Business innovative research (SBIR) program; NASA Planetary Instrument Definition and Development Program [10-PIDDP10-0028] FX Partial funding for the work presented in this paper has been provided by NASA through the Small Business innovative research (SBIR) program and the NASA Planetary Instrument Definition and Development Program (10-PIDDP10-0028). NR 39 TC 4 Z9 4 U1 3 U2 16 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 EI 1573-0794 J9 EARTH MOON PLANETS JI Earth Moon Planets PD NOV PY 2013 VL 111 IS 1-2 BP 47 EP 77 DI 10.1007/s11038-013-9423-5 PG 31 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 251RA UT WOS:000326946600004 ER PT J AU McLinden, ML Carswell, J Li, LH Heymsfield, G Emory, A Cervantes, JI Tian, L AF McLinden, Matthew L. Carswell, James Li, Lihua Heymsfield, Gerald Emory, Amber Cervantes, Jaime I. Tian, Lin TI Utilizing Versatile Transmission Waveforms to Mitigate Pulse-Compression Range Sidelobes With the HIWRAP Radar SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Pulse-compression methods; pulse-compression radar; radar; remote sensing AB The NASA Goddard Space Flight Center (GSFC) High-altitude Imaging Wind and Rain Airborne Profiler (HIWRAP) is a solid-state dual frequency Doppler radar funded by the NASA Instrument Incubator Program. It uses direct-digital-synthesizer devices to generate versatile waveforms including conventional pulses and linear frequency modulation (LFM) chirps. This letter describes a waveform used by the GSFC and the Remote Sensing Solutions to address the critical limitations of range sidelobes and blind ranges in airborne pulse-compression radar. By utilizing a frequency diversity waveform consisting of two pulses and an LFM chirp at each transmit cycle, this system provides the improved sensitivity and range resolution benefits of pulse compression on targets within the middle and high altitudes while maintaining conventional pulsed data near the radar and the surface. The data obtained by the HIWRAP during the NASA Midlatitude Continental Convective Clouds Experiment using this waveform scheme are presented. C1 [McLinden, Matthew L.; Li, Lihua; Heymsfield, Gerald; Emory, Amber] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Carswell, James] Remote Sensing Solut Inc, Barnstable, MA 02630 USA. [Cervantes, Jaime I.] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. [Tian, Lin] Morgan State Univ, Baltimore, MD 21251 USA. RP McLinden, ML (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Measurement, Global/C-4698-2015 FU NASA Global Precipitation Measurement Ground Validation FX This work was supported by the NASA Global Precipitation Measurement Ground Validation. NR 10 TC 1 Z9 1 U1 1 U2 10 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1545-598X EI 1558-0571 J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD NOV PY 2013 VL 10 IS 6 BP 1365 EP 1368 DI 10.1109/LGRS.2013.2241729 PG 4 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 251XI UT WOS:000326966700019 ER PT J AU Guillevic, PC Bork-Unkelbach, A Gottsche, FM Hulley, G Gastellu-Etchegorry, JP Olesen, FS Privette, JL AF Guillevic, Pierre C. Bork-Unkelbach, Annika Goettsche, Frank M. Hulley, Glynn Gastellu-Etchegorry, Jean-Philippe Olesen, Folke S. Privette, Jeffrey L. TI Directional Viewing Effects on Satellite Land Surface Temperature Products Over Sparse Vegetation Canopies-A Multisensor Analysis SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Field experiment; land surface temperature (LST); Moderate Resolution Imaging Spectroradiometer (MODIS); Spinning Enhanced Visible and Infrared Imager (SEVIRI); viewing directional effects ID EMISSIVITY PRODUCTS; RADIATIVE-TRANSFER; VALIDATION; ASTER AB Thermal infrared satellite observations of the Earth's surface are key components in estimating the surface skin temperature over global land areas. However, depending on sun illumination and viewing directional configurations, satellites measure different surface radiometric temperatures, particularly over sparsely vegetated regions where the radiometric contributions from soil and vegetation vary with the sun and viewing geometry. Over an oak tree woodland located near the town of Evora, Portugal, we compare different satellite-based land surface temperature (LST) products from the Moderate Resolution Imaging Spectroradiometer on board the Terra and Aqua polar-orbiting satellites and from the Spinning Enhanced Visible and Infrared Imager on board the geostationary Meteosat satellite with ground-based LST. The observed differences between LSTs derived from polar and geostationary satellites are up to 12 K due to directional effects. In this letter, we develop a methodology based on a radiative transfer model and dedicated field radiometric measurements to interpret and validate directional remote sensing measurements. The methodology is used to estimate the quantitative uncertainty in LST products derived from polar-orbiting satellites over a sparse vegetation canopy. C1 [Guillevic, Pierre C.] N Carolina State Univ, Cooperat Inst Climate & Satellites, Asheville, NC 28801 USA. [Bork-Unkelbach, Annika; Goettsche, Frank M.; Olesen, Folke S.] Karlsruhe Inst Technol, D-76021 Karlsruhe, Germany. [Hulley, Glynn] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gastellu-Etchegorry, Jean-Philippe] Ctr Etud Spati Biosphere, F-31401 Toulouse, France. [Privette, Jeffrey L.] Natl Ocean & Atmospher Adm, Natl Climat Data Ctr, Asheville, NC 28801 USA. RP Guillevic, PC (reprint author), N Carolina State Univ, Cooperat Inst Climate & Satellites, Asheville, NC 28801 USA. EM pierre.guillevic@noaa.gov RI Gottsche, Frank-Michael/A-7362-2013; Privette, Jeffrey/G-7807-2011 OI Gottsche, Frank-Michael/0000-0001-5836-5430; Privette, Jeffrey/0000-0001-8267-9894 FU Joint Polar Satellite System program; National Oceanic and Atmospheric Administration (NOAA)'s Climate Data Record project, through the Cooperative Institute for Climate and Satellites-North Carolina [NA09NES4400006] FX This work was supported in part by the Joint Polar Satellite System program, and by the National Oceanic and Atmospheric Administration (NOAA)'s Climate Data Record project, through the Cooperative Institute for Climate and Satellites-North Carolina under Cooperative Agreement NA09NES4400006. NR 21 TC 18 Z9 18 U1 0 U2 19 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1545-598X EI 1558-0571 J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD NOV PY 2013 VL 10 IS 6 BP 1464 EP 1468 DI 10.1109/LGRS.2013.2260319 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 251XI UT WOS:000326966700039 ER PT J AU Kokhanovsky, AA McBride, PJ Schmidt, KS Pilewskie, P AF Kokhanovsky, A. A. McBride, P. J. Schmidt, K. S. Pilewskie, P. TI The Determination of Cloud Optical Thickness and Effective Particle Size From Measurements of Transmitted Solar Diffuse Light SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Clouds; radiative transfer; remote sensing ID RADIUS AB A new dual-channel method for determining cloud optical thickness and cloud particle size is presented. The method is applied to both the experimental measurements of cloud transmittance and also to a synthetic data set derived from the numerical solution of the radiative transfer equation. The results of the validation show that the technique can be, indeed, applied to optically thick clouds. The technique is superior with respect to its speed and flexibility and with respect to existing up-to-date cloud retrieval methods based on the measurements of the transmitted solar light. C1 [Kokhanovsky, A. A.] Univ Bremen, Inst Remote Sensing, D-28334 Bremen, Germany. [McBride, P. J.] NASA, Goddard Space Flight Ctr, GESTAR, Greenbelt, MD 20771 USA. [Schmidt, K. S.; Pilewskie, P.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA. RP Kokhanovsky, AA (reprint author), Univ Bremen, Inst Remote Sensing, D-28334 Bremen, Germany. RI Kokhanovsky, Alexander/C-6234-2016; SCHMIDT, KONRAD SEBASTIAN/C-1258-2013 OI Kokhanovsky, Alexander/0000-0001-7370-1164; SCHMIDT, KONRAD SEBASTIAN/0000-0003-3899-228X FU German Aerospace Agency (DLR) via the GLOS project; National Oceanic and Atmospheric Administration [NA09OAR4310127]; National Aeronautics and Space Administration [NNX08AI83G] FX This work was supported by the German Aerospace Agency (DLR) via the GLOS project. The experimental data collection was supported by the National Oceanic and Atmospheric Administration under Award NA09OAR4310127 and the National Aeronautics and Space Administration under Award NNX08AI83G. NR 18 TC 1 Z9 1 U1 1 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1545-598X EI 1558-0571 J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD NOV PY 2013 VL 10 IS 6 BP 1512 EP 1516 DI 10.1109/LGRS.2013.2261274 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 251XI UT WOS:000326966700049 ER PT J AU Reck, TJ Chattopadhyay, G AF Reck, Theodore J. Chattopadhyay, Goutam TI A 600 GHz Asymmetrical Orthogonal Mode Transducer SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS LA English DT Article DE Metal machining; orthogonal mode transducer (OMT); terahertz AB Development of dual-polarization sensitive receivers offers significant advantages for future terahertz radiometers. The key to any such system is the orthogonal mode transducer (OMT) which separates two superimposed modes into two single-mode waveguides. This letter presents the design, fabrication and measurement of a split-block asymmetrical OMT operating from 500 to 600 GHz. C1 [Reck, Theodore J.; Chattopadhyay, Goutam] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Reck, TJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM theodore.reck@jpl.nasa.gov FU Jet Propulsion Laboratory, California Institute of Technology under National Aeronautics and Space Administration; National Aeronautics and Space Administration FX This work was supported by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 9 TC 3 Z9 3 U1 1 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1531-1309 EI 1558-1764 J9 IEEE MICROW WIREL CO JI IEEE Microw. Wirel. Compon. Lett. PD NOV PY 2013 VL 23 IS 11 BP 569 EP 571 DI 10.1109/LMWC.2013.2280642 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA 253MI UT WOS:000327090800001 ER PT J AU Ochsner, TE Cosh, MH Cuenca, RH Dorigo, WA Draper, CS Hagimoto, Y Kerr, YH Larson, KM Njoku, EG Small, EE Zreda, M AF Ochsner, Tyson E. Cosh, Michael H. Cuenca, Richard H. Dorigo, Wouter A. Draper, Clara S. Hagimoto, Yutaka Kerr, Yann H. Larson, Kristine M. Njoku, Eni G. Small, Eric E. Zreda, Marek TI State of the Art in Large-Scale Soil Moisture Monitoring SO SOIL SCIENCE SOCIETY OF AMERICA JOURNAL LA English DT Review ID LAND-SURFACE MODEL; HEAT-PULSE METHOD; APERTURE MICROWAVE RADIOMETER; BOUNDARY-LAYER DEVELOPMENT; GLOBAL VEGETATION MODEL; PLANT FUNCTIONAL TYPES; COSMIC-RAY NEUTRONS; WATER-CONTENT; IN-SITU; DATA ASSIMILATION AB Soil moisture is an essential climate variable influencing land-atmosphere interactions, an essential hydrologic variable impacting rainfall-runoff processes, an essential ecological variable regulating net ecosystem exchange, and an essential agricultural variable constraining food security. Large-scale soil moisture monitoring has advanced in recent years, creating opportunities to transform scientific understanding of soil moisture and related processes. These advances are being driven by researchers from a broad range of disciplines, but this complicates collaboration and communication; and, for some applications, the science required to utilize large-scale soil moisture data is poorly developed. In this review, we describe the state of the art in large-scale soil moisture monitoring and identify some critical needs for research to optimize the use of increasingly available soil moisture data. We review representative examples of (i) emerging in situ and proximal sensing techniques, (ii) dedicated soil moisture remote sensing missions, (iii) soil moisture monitoring networks, and (iv) applications of large-scale soil moisture measurements. Significant near-term progress seems possible in the use of large-scale soil moisture data for drought monitoring. Assimilation of soil moisture data for meteorological or hydrologic forecasting also shows promise, but significant challenges related to spatial variability and model structures remain. Little progress has been made in the use of large-scale soil moisture observations within the context of ecological or agricultural modeling. Opportunities abound to advance the science and practice of large-scale soil moisture monitoring for the sake of improved Earth system monitoring, modeling, and forecasting. C1 [Ochsner, Tyson E.] Oklahoma State Univ, Dept Plant & Soil Sci, Stillwater, OK 74078 USA. [Cosh, Michael H.] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. [Cuenca, Richard H.; Hagimoto, Yutaka] Oregon State Univ, Dep Biol & Ecol Engn, Corvallis, OR 97331 USA. [Dorigo, Wouter A.] Vienna Univ Technol, Dep Geodesy & Geoinformat, A-1040 Vienna, Austria. [Draper, Clara S.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Draper, Clara S.] Univ Space Res Assoc, GESTAR, Columbia, MD 21044 USA. [Kerr, Yann H.] Ctr Etudes Spatiales Biosphere, F-31401 Toulouse, France. [Larson, Kristine M.] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA. [Njoku, Eni G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Small, Eric E.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. [Zreda, Marek] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. RP Ochsner, TE (reprint author), Oklahoma State Univ, Dept Plant & Soil Sci, 368 Agr Hall, Stillwater, OK 74078 USA. EM tyson.ochsner@okstate.edu RI Cosh, MIchael/A-8858-2015; Small, eric/K-6007-2015; Draper, Clara/P-6097-2016; OI Cosh, MIchael/0000-0003-4776-1918; Draper, Clara/0000-0002-8299-4939; Dorigo, Wouter/0000-0001-8054-7572 FU SMOS Soil Moisture Network Study- Operational Phase (ESA ESTEC) [4000102722/10]; NASA [NNX10AU84G]; NSF [AGS 0935725]; U.S. National Science Foundation [ATM-0838491]; Jet Propulsion Laboratory, California Institute of Technology FX The contribution of Tyson Ochsner has been funded by the Oklahoma Agricultural Experiment Station. The contribution of Wouter Dorigo has been funded through the SMOS Soil Moisture Network Study- Operational Phase (ESA ESTEC Contract no.4000102722/10). The contributions of Eric Small and Kristine Larson were funded by grants from NASA (NNX10AU84G) and NSF (AGS 0935725). The contribution of Marek Zreda has been funded through the COSMOS project by the U.S. National Science Foundation (Grant no. ATM-0838491). The contribution of Eni Njoku was funded through the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. NR 230 TC 72 Z9 72 U1 15 U2 130 PU SOIL SCI SOC AMER PI MADISON PA 677 SOUTH SEGOE ROAD, MADISON, WI 53711 USA SN 0361-5995 EI 1435-0661 J9 SOIL SCI SOC AM J JI Soil Sci. Soc. Am. J. PD NOV-DEC PY 2013 VL 77 IS 6 BP 1888 EP 1919 DI 10.2136/sssaj2013.03.0093 PG 32 WC Soil Science SC Agriculture GA 252QS UT WOS:000327024500002 ER PT J AU Ackermann, M Ajello, M Asano, K Axelsson, M Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Bhat, PN Bissaldi, E Bloom, ED Bonamente, E Bonnell, J Bouvier, A Brandt, TJ Bregeon, J Brigida, M Bruel, P Buehler, R Burgess, JM Buson, S Byrne, D Caliandro, GA Cameron, RA Caraveo, PA Cecchi, C Charles, E Chaves, RCG Chekhtman, A Chiang, J Chiaro, G Ciprini, S Claus, R Cohen-Tanugi, J Connaughton, V Conrad, J Cutini, S D'Ammando, F de Angelis, A de Palma, F Dermer, CD Desiante, R Digel, SW Dingus, BL Di Venere, L Drell, PS Drlica-Wagner, A Dubois, R Favuzzi, C Ferrara, EC Fitzpatrick, G Foley, S Franckowiak, A Fukazawa, Y Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giglietto, N Giommi, P Giordano, F Giroletti, M Glanzman, T Godfrey, G Goldstein, A Granot, J Grenier, IA Grove, JE Gruber, D Guiriec, S Hadasch, D Hanabata, Y Hayashida, M Horan, D Hou, X Hughes, RE Inoue, Y Jackson, MS Jogler, T Johannesson, G Johnson, AS Johnson, WN Kamae, T Kataoka, J Kawano, T Kippen, RM Knodlseder, J Kocevski, D Kouveliotou, C Kuss, M Lande, J Larsson, S Latronico, L Lee, SH Longo, F Loparco, F Lovellette, MN Lubrano, P Massaro, F Mayer, M Mazziotta, MN McBreen, S McEnery, JE McGlynn, S Michelson, PF Mizuno, T Moiseev, AA Monte, C Monzani, ME Moretti, E Morselli, A Murgia, S Nemmen, R Nuss, E Nymark, T Ohno, M Ohsugi, T Omodei, N Orienti, M Orlando, E Paciesas, WS Paneque, D Panetta, JH Pelassa, V Perkins, JS Pesce-Rollins, M Piron, F Pivato, G Porter, TA Preece, R Racusin, JL Raino, S Rando, R Rau, A Razzano, M Razzaque, S Reimer, A Reimer, O Reposeur, T Ritz, S Romoli, C Roth, M Ryde, F Parkinson, PMS Schalk, TL Sgro, C Siskind, EJ Sonbas, E Spandre, G Spinelli, P Suson, DJ Tajima, H Takahashi, H Takeuchi, Y Tanaka, Y Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tierney, D Tinivella, M Torres, DF Tosti, G Troja, E Tronconi, V Usher, TL Vandenbroucke, J van der Horst, AJ Vasileiou, V Vianello, G Vitale, V von Kienlin, A Winer, BL Wood, KS Wood, M Xiong, S Yang, Z AF Ackermann, M. Ajello, M. Asano, K. Axelsson, M. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Bhat, P. N. Bissaldi, E. Bloom, E. D. Bonamente, E. Bonnell, J. Bouvier, A. Brandt, T. J. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Burgess, J. Michael Buson, S. Byrne, D. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cecchi, C. Charles, E. Chaves, R. C. G. Chekhtman, A. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. Cohen-Tanugi, J. Connaughton, V. Conrad, J. Cutini, S. D'Ammando, F. de Angelis, A. de Palma, F. Dermer, C. D. Desiante, R. Digel, S. W. Dingus, B. L. Di Venere, L. Drell, P. S. Drlica-Wagner, A. Dubois, R. Favuzzi, C. Ferrara, E. C. Fitzpatrick, G. Foley, S. Franckowiak, A. Fukazawa, Y. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giglietto, N. Giommi, P. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Goldstein, A. Granot, J. Grenier, I. A. Grove, J. E. Gruber, D. Guiriec, S. Hadasch, D. Hanabata, Y. Hayashida, M. Horan, D. Hou, X. Hughes, R. E. Inoue, Y. Jackson, M. S. Jogler, T. Johannesson, G. Johnson, A. S. Johnson, W. N. Kamae, T. Kataoka, J. Kawano, T. Kippen, R. M. Knoedlseder, J. Kocevski, D. Kouveliotou, C. Kuss, M. Lande, J. Larsson, S. Latronico, L. Lee, S. -H. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Massaro, F. Mayer, M. Mazziotta, M. N. McBreen, S. McEnery, J. E. McGlynn, S. Michelson, P. F. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Moretti, E. Morselli, A. Murgia, S. Nemmen, R. Nuss, E. Nymark, T. Ohno, M. Ohsugi, T. Omodei, N. Orienti, M. Orlando, E. Paciesas, W. S. Paneque, D. Panetta, J. H. Pelassa, V. Perkins, J. S. Pesce-Rollins, M. Piron, F. Pivato, G. Porter, T. A. Preece, R. Racusin, J. L. Raino, S. Rando, R. Rau, A. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Reposeur, T. Ritz, S. Romoli, C. Roth, M. Ryde, F. Parkinson, P. M. Saz Schalk, T. L. Sgro, C. Siskind, E. J. Sonbas, E. Spandre, G. Spinelli, P. Suson, D. J. Tajima, H. Takahashi, H. Takeuchi, Y. Tanaka, Y. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tierney, D. Tinivella, M. Torres, D. F. Tosti, G. Troja, E. Tronconi, V. Usher, T. L. Vandenbroucke, J. van der Horst, A. J. Vasileiou, V. Vianello, G. Vitale, V. von Kienlin, A. Winer, B. L. Wood, K. S. Wood, M. Xiong, S. Yang, Z. TI THE FIRST FERMI-LAT GAMMA-RAY BURST CATALOG SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; gamma-ray burst: general; methods: data analysis ID LARGE-AREA TELESCOPE; INTERNAL SHOCK MODEL; HIGH-ENERGY EMISSION; DELAYED GEV EMISSION; SPECTRAL COMPONENT; PROMPT EMISSION; GRB 100728A; LIKELIHOOD RATIO; FLARING ACTIVITY; PHOTON-EMISSION AB In three years of observations since the beginning of nominal science operations in 2008 August, the Large Area Telescope (LAT) on board the Fermi Gamma-Ray Space Telescope has observed high-energy (greater than or similar to 20 MeV) gamma-ray emission from 35 gamma-ray bursts (GRBs). Among these, 28 GRBs have been detected above 100 MeV and 7 GRBs above similar to 20 MeV. The first Fermi-LAT catalog of GRBs is a compilation of these detections and provides a systematic study of high-energy emission from GRBs for the first time. To generate the catalog, we examined 733 GRBs detected by the Gamma-Ray Burst Monitor (GBM) on Fermi and processed each of them using the same analysis sequence. Details of the methodology followed by the LAT collaboration for the GRB analysis are provided. We summarize the temporal and spectral properties of the LAT-detected GRBs. We also discuss characteristics of LAT-detected emission such as its delayed onset and longer duration compared with emission detected by the GBM, its power-law temporal decay at late times, and the fact that it is dominated by a power-law spectral component that appears in addition to the usual Band model. C1 [Ackermann, M.; Mayer, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Asano, K.] Tokyo Inst Technol, Interact Res Ctr Sci, Meguro, Tokyo 1528551, Japan. [Axelsson, M.; Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Axelsson, M.; Conrad, J.; Jackson, M. S.; Larsson, S.; Moretti, E.; Nymark, T.; Ryde, F.; Yang, Z.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Axelsson, M.; Jackson, M. S.; Moretti, E.; Nymark, T.; Ryde, F.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Baldini, L.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Chaves, R. C. G.; Grenier, I. A.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France. [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.; Pivato, G.; Rando, R.; Romoli, C.; Tronconi, V.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bechtol, K.; Bloom, E. D.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Di Venere, L.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Inoue, Y.; Jogler, T.; Johnson, A. S.; Kamae, T.; Kocevski, D.; Lande, J.; Massaro, F.; Michelson, P. F.; Monzani, M. E.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tajima, H.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Bechtol, K.; Bloom, E. D.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Di Venere, L.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Inoue, Y.; Jogler, T.; Johnson, A. S.; Kamae, T.; Kocevski, D.; Lande, J.; Massaro, F.; Michelson, P. F.; Monzani, M. E.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tajima, H.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Bhat, P. N.; Burgess, J. Michael; Connaughton, V.; Goldstein, A.; Pelassa, V.; Preece, R.; Xiong, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Bissaldi, E.; Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Bissaldi, E.; Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Bonnell, J.; Brandt, T. J.; Ferrara, E. C.; Gehrels, N.; Guiriec, S.; McEnery, J. E.; Nemmen, R.; Perkins, J. S.; Racusin, J. L.; Sonbas, E.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bonnell, J.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Bonnell, J.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Bouvier, A.; Razzano, M.; Ritz, S.; Parkinson, P. M. Saz; Schalk, T. L.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Bouvier, A.; Razzano, M.; Ritz, S.; Parkinson, P. M. Saz; Schalk, T. L.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ 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.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Byrne, D.; Fitzpatrick, G.; Foley, S.; McBreen, S.; Tierney, D.] Univ Coll Dublin, Dublin 4, Ireland. [Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Chekhtman, A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Ciprini, S.; Cutini, S.; Gasparrini, D.; Giommi, P.] Agenzia Spaziale Italiana Sci Data Ctr, I-00044 Rome, Italy. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Rome, Italy. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, Montpellier, France. [Conrad, J.; Larsson, S.; Yang, Z.] Stockholm Univ, AlbaNova, Dept 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. [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Dingus, B. L.; Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Foley, S.; Gruber, D.; McBreen, S.; Rau, A.; von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Fukazawa, Y.; Hanabata, Y.; Kawano, T.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Granot, J.] Open Univ Israel, Dept Nat Sci, IL-43537 Raanana, Israel. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Hou, X.; Reposeur, T.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Kataoka, J.; Takeuchi, Y.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France. [Kouveliotou, C.; Moiseev, A. A.; Perkins, J. S.; van der Horst, A. J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Lee, S. -H.] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan. [McGlynn, S.] Tech Univ Munich, Exzellenzcluster Universe, D-85748 Garching, Germany. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Moiseev, A. A.; Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Ohno, M.; Tanaka, Y.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Paciesas, W. S.; Sonbas, E.] USRA, Columbia, MD 21044 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Perkins, J. S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Perkins, J. S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Perkins, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Razzaque, S.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa. [Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Sonbas, E.] Adiyaman Univ, TR-02040 Adiyaman, Turkey. [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. RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. EM nicola.omodei@stanford.edu; piron@in2p3.fr; soebur.razzaque@gmail.com; vlasios.vasileiou@lupm.in2p3.fr RI Di Venere, Leonardo/C-7619-2017; 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; Massaro, Francesco/L-9102-2016; Torres, Diego/O-9422-2016; Johnson, Neil/G-3309-2014; Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Orlando, E/R-5594-2016; OI Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094; Axelsson, Magnus/0000-0003-4378-8785; Giroletti, Marcello/0000-0002-8657-8852; McBreen, Sheila/0000-0002-1477-618X; Moretti, Elena/0000-0001-5477-9097; Gasparrini, Dario/0000-0002-5064-9495; Di Venere, Leonardo/0000-0003-0703-824X; Inoue, Yoshiyuki/0000-0002-7272-1136; Giordano, Francesco/0000-0002-8651-2394; Dingus, Brenda/0000-0001-8451-7450; giommi, paolo/0000-0002-2265-5003; De Angelis, Alessandro/0000-0002-3288-2517; Preece, Robert/0000-0003-1626-7335; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; Burgess, James/0000-0003-3345-9515; 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; Massaro, Francesco/0000-0002-1704-9850; Torres, Diego/0000-0002-1522-9065; Reimer, Olaf/0000-0001-6953-1385; Morselli, Aldo/0000-0002-7704-9553; Baldini, Luca/0000-0002-9785-7726 FU National Aeronautics and Space Administration; Department of Energy in the United States; Commissariat a l'Energie Atom-ique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan; K. A. Wallenberg Foundation; Swedish Research Council; Swedish National Space Board in Sweden; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France FX The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States; the Commissariat a l'Energie Atom-ique 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. NR 297 TC 80 Z9 81 U1 1 U2 29 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 NOV PY 2013 VL 209 IS 1 AR UNSP 11 DI 10.1088/0067-0049/209/1/11 PG 90 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246WJ UT WOS:000326571000011 ER PT J AU Hasselfield, M Moodley, K Bond, JR Das, S Devlin, MJ Dunkley, J Dunner, R Fowler, JW Gallardo, P Gralla, MB Hajian, A Halpern, M Hincks, AD Marriage, TA Marsden, D Niemack, MD Nolta, MR Page, LA Partridge, B Schmitt, BL Sehgal, N Sievers, J Staggs, ST Swetz, DS Switzer, ER Wollack, EJ AF Hasselfield, Matthew Moodley, Kavilan Bond, J. Richard Das, Sudeep Devlin, Mark J. Dunkley, Joanna Duenner, Rolando Fowler, Joseph W. Gallardo, Patricio Gralla, Megan B. Hajian, Amir Halpern, Mark Hincks, Adam D. Marriage, Tobias A. Marsden, Danica Niemack, Michael D. Nolta, Michael R. Page, Lyman A. Partridge, Bruce Schmitt, Benjamin L. Sehgal, Neelima Sievers, Jon Staggs, Suzanne T. Swetz, Daniel S. Switzer, Eric R. Wollack, Edward J. TI THE ATACAMA COSMOLOGY TELESCOPE: BEAM MEASUREMENTS AND THE MICROWAVE BRIGHTNESS TEMPERATURES OF URANUS AND SATURN SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology: observations; planets and satellites: individual (Saturn, Uranus) ID PROBE WMAP OBSERVATIONS; CALIBRATION SOURCES; WINDOW FUNCTIONS; 148 GHZ; NEPTUNE; MAPS; SUBMILLIMETER; PROFILES; JUPITER; PLANETS AB We describe the measurement of the beam profiles and window functions for the Atacama Cosmology Telescope (ACT), which operated from 2007 to 2010 with kilopixel bolometer arrays centered at 148, 218, and 277 GHz. Maps of Saturn are used to measure the beam shape in each array and for each season of observations. Radial profiles are transformed to Fourier space in a way that preserves the spatial correlations in the beam uncertainty to derive window functions relevant for angular power spectrum analysis. Several corrections are applied to the resulting beam transforms, including an empirical correction measured from the final cosmic microwave background (CMB) survey maps to account for the effects of mild pointing variation and alignment errors. Observations of Uranus made regularly throughout each observing season are used to measure the effects of atmospheric opacity and to monitor deviations in telescope focus over the season. Using the WMAP-based calibration of the ACT maps to the CMB blackbody, we obtain precise measurements of the brightness temperatures of the Uranus and Saturn disks at effective frequencies of 149 and 219 GHz. For Uranus we obtain thermodynamic brightness temperatures T-U(149) = 106.7 +/- 2.2 K and T-U(219) = 100.1 +/- 3.1 K. For Saturn, we model the effects of the ring opacity and emission using a simple model and obtain resulting (unobscured) disk temperatures of T-S(149) = 137.3 +/- 3.2 K and T-S(219) = 137.3 +/- 4.7 K. C1 [Hasselfield, Matthew; Sievers, Jon] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Hasselfield, Matthew; Halpern, Mark] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. [Moodley, Kavilan] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Bond, J. Richard; Hajian, Amir; Hincks, Adam D.; Nolta, Michael R.; Sievers, Jon; Switzer, Eric R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Das, Sudeep] Argonne Natl Lab, Div High Energy Phys, Lemont, IL 60439 USA. [Das, Sudeep] Univ Calif Berkeley, LBL, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Devlin, Mark J.; Marsden, Danica; Schmitt, Benjamin L.; Swetz, Daniel S.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Dunkley, Joanna] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Duenner, Rolando; Gallardo, Patricio] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile. [Fowler, Joseph W.; Niemack, Michael D.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Fowler, Joseph W.; Gallardo, Patricio; Niemack, Michael D.; Page, Lyman A.; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Gralla, Megan B.; Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Marsden, Danica] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. [Sehgal, Neelima] Dept Phys & Astron, Stony Brook, NY 11794 USA. [Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hasselfield, M (reprint author), Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. RI Wollack, Edward/D-4467-2012; OI Wollack, Edward/0000-0002-7567-4451; Sievers, Jonathan/0000-0001-6903-5074 FU U.S. National Science Foundation [AST-0408698, AST-0965625]; Princeton University; University of Pennsylvania; Canada Foundation for Innovation (CFI) award; Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT); CFI under Compute Canada; Government of Ontario; Ontario Research Fund-Research Excellence; University of Toronto; [PHY-0855887]; [PHY-1214379] FX This work was supported by the U.S. National Science Foundation through awards AST-0408698 and AST-0965625 for the ACT project, as well as awards PHY-0855887 and PHY-1214379. Funding was also provided by Princeton University, the University of Pennsylvania, and a Canada Foundation for Innovation (CFI) award to the University of British Columbia. ACT operates in the Parque Astronomico Atacama in northern Chile under the auspices of the Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT). Computations were performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by the CFI under the auspices of Compute Canada, the Government of Ontario, the Ontario Research Fund-Research Excellence, and the University of Toronto. NR 30 TC 11 Z9 11 U1 0 U2 5 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 NOV PY 2013 VL 209 IS 1 AR UNSP 17 DI 10.1088/0067-0049/209/1/17 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246WJ UT WOS:000326571000017 ER PT J AU Krimm, HA Holland, ST Corbet, RHD Pearlman, AB Romano, P Kennea, JA Bloom, JS Barthelmy, SD Baumgartner, WH Cummings, JR Gehrels, N Lien, AY Markwardt, CB Palmer, DM Sakamoto, T Stamatikos, M Ukwatta, TN AF Krimm, H. A. Holland, S. T. Corbet, R. H. D. Pearlman, A. B. Romano, P. Kennea, J. A. Bloom, J. S. Barthelmy, S. D. Baumgartner, W. H. Cummings, J. R. Gehrels, N. Lien, A. Y. Markwardt, C. B. Palmer, D. M. Sakamoto, T. Stamatikos, M. Ukwatta, T. N. TI THE SWIFT/BAT HARD X-RAY TRANSIENT MONITOR SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE black hole physics; pulsars: general; surveys; X-rays: binaries; X-rays: general ID LARGE-AREA TELESCOPE; SOFT GAMMA-RAY; MILLISECOND PULSAR SWIFT-J1756.9-2508; ACTIVE GALACTIC NUCLEI; BLACK-HOLE; 2011 OUTBURST; MULTIWAVELENGTH OBSERVATIONS; SPECTRAL EVOLUTION; IGR J17544-2619; ALERT TELESCOPE AB The Swift/Burst Alert Telescope (BAT) hard X-ray transient monitor provides near real-time coverage of the X-ray sky in the energy range 15-50 keV. The BAT observes 88% of the sky each day with a detection sensitivity of 5.3 mCrab for a full-day observation and a time resolution as fine as 64 s. The three main purposes of the monitor are (1) the discovery of new transient X-ray sources, (2) the detection of outbursts or other changes in the flux of known X-ray sources, and (3) the generation of light curves of more than 900 sources spanning over eight years. The primary interface for the BAT transient monitor is a public Web site. Between 2005 February 12 and 2013 April 30, 245 sources have been detected in the monitor, 146 of them persistent and 99 detected only in outburst. Among these sources, 17 were previously unknown and were discovered in the transient monitor. In this paper, we discuss the methodology and the data processing and filtering for the BAT transient monitor and review its sensitivity and exposure. We provide a summary of the source detections and classify them according to the variability of their light curves. Finally, we review all new BAT monitor discoveries. For the new sources that are previously unpublished, we present basic data analysis and interpretations. C1 [Krimm, H. A.; Holland, S. T.; Corbet, R. H. D.; Pearlman, A. B.; Baumgartner, W. H.; Cummings, J. R.] CRESST, Greenbelt, MD 20771 USA. [Krimm, H. A.; Holland, S. T.; Corbet, R. H. D.; Pearlman, A. B.; Barthelmy, S. D.; Baumgartner, W. H.; Cummings, J. R.; Gehrels, N.; Lien, A. Y.; Markwardt, C. B.; Ukwatta, T. N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Holland, S. T.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Corbet, R. H. D.; Pearlman, A. B.; Baumgartner, W. H.; Cummings, J. R.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Corbet, R. H. D.; Pearlman, A. B.; Baumgartner, W. H.; Cummings, J. R.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Pearlman, A. B.] CALTECH, Dept Appl Phys, Pasadena, CA 91125 USA. [Romano, P.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-90146 Palermo, Italy. [Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Bloom, J. S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Palmer, D. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Sakamoto, T.] Aoyama Gakuin Univ, Coll Sci & Engn, Dept Math & Phys, Chuo Ku, Sagamihara, Kanagawa 2525258, Japan. [Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Ukwatta, T. N.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP Krimm, HA (reprint author), CRESST, Greenbelt, MD 20771 USA. FU NASA [NNX09AU85G, NNX12AD32G, NNX12AE57G, NNX13AC75G]; ASI-INAF grant [1/004/11/0] FX The Swift/BAT transient monitor is supported by NASA under Swift Guest Observer grants NNX09AU85G, NNX12AD32G, NNX12AE57G, and NNX13AC75G. H.A.K. also acknowledges these NASA grants for partial support. P. R. acknowledges ASI-INAF grant 1/004/11/0. We gratefully acknowledge the RXTE and Swift principal investigators for approving, and mission planners for scheduling, the many observations discussed in this work. 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 and from the UK Swift Science Data Centre at the University of Leicester. This research has also made use of the SIMBAD database, operated at CDS, Strasbourg, France. Finally, the authors acknowledge helpful comments from an anonymous referee. NR 218 TC 105 Z9 106 U1 0 U2 8 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 NOV PY 2013 VL 209 IS 1 AR UNSP 14 DI 10.1088/0067-0049/209/1/14 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246WJ UT WOS:000326571000014 ER PT J AU Mawet, D Pueyo, L Carlotti, A Mennesson, B Serabyn, E Wallace, JK AF Mawet, D. Pueyo, L. Carlotti, A. Mennesson, B. Serabyn, E. Wallace, J. K. TI RING-APODIZED VORTEX CORONAGRAPHS FOR OBSCURED TELESCOPES. I. TRANSMISSIVE RING APODIZERS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE brown dwarfs; instrumentation: adaptive optics; instrumentation: high angular resolution; stars: imaging; stars: low-mass; techniques: high angular resolution; telescopes ID PUPIL LYOT CORONAGRAPHS; PHASE-MASK CORONAGRAPH; LABORATORY DEMONSTRATION; ARBITRARY APERTURES; 1ST LIGHT; BEAMWIDTHS; COMPANION; CRYSTAL; DESIGN; STAR AB The vortex coronagraph (VC) is a new generation small inner working angle (IWA) coronagraph currently offered on various 8 m class ground-based telescopes. On these observing platforms, the current level of performance is not limited by the intrinsic properties of actual vortex devices, but by wavefront control residuals and incoherent background (e. g., thermal emission of the sky), or the light diffracted by the imprint of the secondary mirror and support structures on the telescope pupil. In the particular case of unfriendly apertures (mainly large central obscuration) when very high contrast is needed (e. g., direct imaging of older exoplanets with extremely large telescopes or space-based coronagraphs), a simple VC, like most coronagraphs, cannot deliver its nominal performance because of the contamination due to the diffraction from the obscured part of the pupil. Here, we propose a novel yet simple concept that circumvents this problem. We combine a vortex phase mask in the image plane of a high-contrast instrument with a single pupil-based amplitude ring apodizer, tailor-made to exploit the unique convolution properties of the VC at the Lyot-stop plane. We show that such a ring-apodized vortex coronagraph (RAVC) restores the perfect attenuation property of the VC regardless of the size of the central obscuration, and for any (even) topological charge of the vortex. More importantly, the RAVC maintains the IWA and conserves a fairly high throughput, which are signature properties of the VC. C1 [Mawet, D.] European So Observ, Santiago, Chile. [Pueyo, L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Carlotti, A.] Princeton Univ, Princeton, NJ 08544 USA. [Mawet, D.; Mennesson, B.; Serabyn, E.; Wallace, J. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mawet, D (reprint author), European So Observ, Alonso de Cordova 3107 Vitacura, Santiago, Chile. FU NASA [NNX12AG05G] FX This work was carried out at the European Southern Observatory (ESO) and at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This material is partially based on work supported by NASA under grant NNX12AG05G issued through the Astrophysics Research and Analysis (APRA) program. NR 46 TC 27 Z9 27 U1 1 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 NOV PY 2013 VL 209 IS 1 AR UNSP 7 DI 10.1088/0067-0049/209/1/7 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246WJ UT WOS:000326571000007 ER PT J AU Min, JB Duffy, KP Choi, BB Provenza, AJ Kray, N AF Min, James B. Duffy, Kirsten P. Choi, Benjamin B. Provenza, Andrew J. Kray, Nicholas TI Numerical modeling methodology and experimental study for piezoelectric vibration damping control of rotating composite fan blades SO COMPUTERS & STRUCTURES LA English DT Article DE Multiphysics piezoelectric finite element modeling; Forced vibration response; Piezoelectric vibration control; Blade rotational effects; Rotating blade base excitation model; Aircraft engine composite fan blades ID NETWORKS AB Resonant vibrations of aircraft engine blades cause blade fatigue problems in engines, which can lead to thicker and aerodynamically lower performing blade designs, increasing engine weight, fuel burn, and maintenance costs. In order to mitigate undesirable blade vibration levels, active piezoelectric vibration control has been investigated, potentially enabling thinner blade designs for higher performing blades and minimizing blade fatigue problems. While the piezoelectric damping idea has been investigated by other researchers over the years, very little study has been done including rotational effects. The present study attempts to fill this void. The particular objectives of this study were to: (a) develop a methodology to analyze a multiphysics piezoelectric finite element composite blade model for harmonic forced vibration response analysis coupled with a tuned RLC circuit for rotating engine blade conditions, (b) validate a numerical model with experimental test data, and (c) achieve a cost-effective numerical modeling capability which enables simulation of rotating blades within the NASA GRC Dynamic Spin Rig Facility. A numerical and experimental study for rotating piezoelectric composite subscale fan blades was performed. It was proved that the proposed numerical method is feasible and effective when applied to the rotating blade base excitation model. The experimental test and multiphysics finite element modeling technique described in this paper show that piezoelectric vibration damping can significantly reduce vibrations of aircraft engine composite fan blades. Published by Elsevier Ltd. C1 [Min, James B.; Choi, Benjamin B.; Provenza, Andrew J.] NASA, Glenn Res Ctr, Cleveland, OH USA. [Duffy, Kirsten P.] Univ Toledo, Toledo, OH 43606 USA. [Kray, Nicholas] Gen Elect Aviat, Cincinnati, OH USA. RP Min, JB (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. EM James.B.Min@nasa.gov FU NASA [SAA3-260] FX Authors express thanks to George Stefko and Milind Bakhle for valuable technical discussions; Carlos Morrison for a wireless inductive power transfer device development task during the course of the project; Karen Bartos helped for blade mesh modification; George Carlson for Ansys Multiphysics discussions; Greg Gemeinhardt for GE blade composite properties and ply-layup information; Ian Prentice for the original GE blade mesh; Karen Taminger, Ajay Misra, Leslie Greenbauer-Seng for the project support with the Subsonic Fixed Wing Project of the NASA Fundamental Aeronautics Program. This work was a collaborative effort between NASA GRC and GE Aviation through NASA Space Act Agreement SAA3-260. NR 21 TC 6 Z9 6 U1 5 U2 40 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0045-7949 EI 1879-2243 J9 COMPUT STRUCT JI Comput. Struct. PD NOV PY 2013 VL 128 BP 230 EP 242 DI 10.1016/j.compstruc.2013.06.001 PG 13 WC Computer Science, Interdisciplinary Applications; Engineering, Civil SC Computer Science; Engineering GA 248AZ UT WOS:000326667400020 ER PT J AU Sorek-Hamer, M Strawa, AW Chatfield, RB Esswein, R Cohen, A Broday, DM AF Sorek-Hamer, M. Strawa, A. W. Chatfield, R. B. Esswein, R. Cohen, A. Broday, D. M. TI Improved retrieval of PM2.5 from satellite data products using non-linear methods SO ENVIRONMENTAL POLLUTION LA English DT Article DE PM; MODIS; OMI; GAM; MARS ID GROUND-LEVEL PM2.5; IMAGING SPECTRORADIOMETER MODIS; GENERALIZED ADDITIVE-MODELS; ADAPTIVE REGRESSION SPLINES; AEROSOL OPTICAL-THICKNESS; AIR-QUALITY; PARTICULATE MATTER; UNITED-STATES; LAND; POLLUTION AB Satellite observations may improve the areal coverage of particulate matter (PM) air quality data that nowadays is based on surface measurements. Three statistical methods for retrieving daily PM2.5 concentrations from satellite products (MODIS-AOD, OMI-AAI) over the San Joaquin Valley (CA) are compared - Linear Regression (LR), Generalized Additive Models (GAM), and Multivariate Adaptive Regression Splines (MARS). Simple LRs show poor correlations in the western USA (R-2 congruent to 0.2). Both GAM and MARS were found to perform better than the simple LRs, with a slight advantage to the MARS over the GAM (R-2 = 0.71 and R-2 = 0.61, respectively). Since MARS is also characterized by a better computational efficiency than GAM, it can be used for improving PM2.5 retrievals from satellite aerosol products. Reliable PM2.5 retrievals can fill in missing surface measurements in areas with sparse ground monitoring coverage and be used for evaluating air quality models and as exposure metrics in epidemiological studies. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Sorek-Hamer, M.; Cohen, A.; Broday, D. M.] Technion Israel Inst Technol, Haifa, Israel. [Strawa, A. W.; Chatfield, R. B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Esswein, R.] Bay Area Environm Res Inst, Sonoma, CA USA. RP Broday, DM (reprint author), Technion Israel Inst Technol, Haifa, Israel. EM dbroday@tx.technion.ac.il OI Broday, David/0000-0002-6525-3979 FU Environment and Health Fund, Israel; NASA AMES Research Center, CA, USA 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. NR 43 TC 14 Z9 14 U1 3 U2 37 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0269-7491 EI 1873-6424 J9 ENVIRON POLLUT JI Environ. Pollut. PD NOV PY 2013 VL 182 BP 417 EP 423 DI 10.1016/j.envpol.2013.08.002 PG 7 WC Environmental Sciences SC Environmental Sciences & Ecology GA 247YU UT WOS:000326661700051 PM 23995022 ER PT J AU Di, LP Yue, P Ramapriyan, HK King, RL AF Di, Liping Yue, Peng Ramapriyan, Hampapuram K. King, Roger L. TI Introduction to the Special Issue on Geoscience Data Provenance SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Editorial Material C1 [Di, Liping] George Mason Univ, Ctr Spatial Informat Sci & Syst, Fairfax, VA 22030 USA. [Yue, Peng] Wuhan Univ, State Key Lab Informat Engn Surveying Mapping & R, Wuhan 430079, Peoples R China. [Ramapriyan, Hampapuram K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [King, Roger L.] Mississippi State Univ, Ctr Adv Vehicular Syst, Starkville, MS 39759 USA. RP Di, LP (reprint author), George Mason Univ, Ctr Spatial Informat Sci & Syst, Fairfax, VA 22030 USA. NR 0 TC 1 Z9 1 U1 0 U2 15 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 NOV PY 2013 VL 51 IS 11 SI SI BP 5062 EP 5064 DI 10.1109/TGRS.2013.2285999 PG 3 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 247DY UT WOS:000326596500001 ER PT J AU Di, LP Yue, P Ramapriyan, HK King, RL AF Di, Liping Yue, Peng Ramapriyan, Hampapuram K. King, Roger L. TI Geoscience Data Provenance: An Overview SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Cyberinfrastructure; geoprocessing workflow; geoscience data provenance; geospatial service; lineage; preservation ID EARTH-SCIENCE DATA; SEMANTIC PROVENANCE; SCIENTIFIC-DATA; SENSOR WEB; LINEAGE; PRESERVATION; ENVIRONMENT; TRACKING; SYSTEM AB The advancement of Earth observing sensors, data, and information systems enhances significantly the capabilities to access and process large volumes of geoscience data, which are often consumed by scientific workflows and processed in a distributed information environment. Consequently, data provenance becomes important since it allows users to determine the usability and reliability of data products. Motivation for capturing and sharing provenance also comes from the distributed data and information infrastructure that has been benefiting the Earth science community in the past decade, such as spatial data and information infrastructure, e-Science, and cyberinfrastructure. This paper provides an overview of geoscience data provenance in supporting provenance-aware geoscience data and information systems by summarizing state-of-the-art technologies and methodologies of geoscience data provenance and highlighting key considerations and possible solutions for geoscience data provenance. C1 [Di, Liping] George Mason Univ, Ctr Spatial Informat Sci & Syst, Fairfax, VA 22030 USA. [Yue, Peng] Wuhan Univ, State Key Lab Informat Engn Surveying Mapping & R, Wuhan 430079, Peoples R China. [Ramapriyan, Hampapuram K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [King, Roger L.] Mississippi State Univ, Ctr Adv Vehicular Syst, Starkville, MS 39762 USA. RP Di, LP (reprint author), George Mason Univ, Ctr Spatial Informat Sci & Syst, Fairfax, VA 22030 USA. EM ldi@gmu.edu; geopyue@gmail.com; hampapuram.k.ramapriyan@nasa.gov; rking@cavs.msstate.edu FU National Basic Research Program of China [2011CB707105]; U.S. Department of Energy [DE-NA0001123]; National Natural Science Foundation of China [41271397] FX This work was supported in part by the National Basic Research Program of China under Grant 2011CB707105, by the U. S. Department of Energy under Grant #DE-NA0001123, and by the National Natural Science Foundation of China (Project 41271397). NR 52 TC 7 Z9 7 U1 0 U2 32 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 NOV PY 2013 VL 51 IS 11 SI SI BP 5065 EP 5072 DI 10.1109/TGRS.2013.2242478 PG 8 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 247DY UT WOS:000326596500002 ER PT J AU Tilmes, C Fox, P Ma, XG McGuinness, DL Privette, AP Smith, A Waple, A Zednik, S Zheng, JG AF Tilmes, Curt Fox, Peter Ma, Xiaogang McGuinness, Deborah L. Privette, Ana Pinheiro Smith, Aaron Waple, Anne Zednik, Stephan Zheng, Jin Guang TI Provenance Representation for the National Climate Assessment in the Global Change Information System SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Data management; government information systems; knowledge representation AB The important topic of global climate change builds on a huge collection of scientific research. It is common for agencies releasing climate change information to be served with requests for all supporting materials resulting in a particular conclusion. Capturing and presenting global change provenance, linking to the research papers, data sets, models, analyses, observations, satellites, etc., that support the key research findings in this domain can increase understanding and aid in reproducibility of results and conclusions. The U. S. Global Change Research Program is now coordinating the production of a national climate assessment (NCA) that presents our best understanding of global change. We are now developing a global change information system that will present the content of that report and its provenance, including the scientific support for the findings of the assessment. We are using an approach that will present this information both through a human accessible Web site as well as a machine-readable interface for automated mining of the provenance graph. We plan to use the developing World Wide Web Consortium (W3C) PROV data model and ontology for this system. This paper will describe an overview of the process of developing the NCA and how the provenance trail of the report and each of the technical inputs can be captured and represented using the W3C PROV ontology. This will improve the visibility into the assessment process, increase understanding and possibility of reproducibility, and ultimately increase the credibility and trust of the resulting report. C1 [Tilmes, Curt] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fox, Peter; Ma, Xiaogang; McGuinness, Deborah L.; Zednik, Stephan; Zheng, Jin Guang] Rensselaer Polytech Inst, Tetherless World Constellat, Troy, NY 12180 USA. [Privette, Ana Pinheiro] N Carolina State Univ, Cooperat Inst Climate & Satellites, NOAA, Natl Climat Data Ctr, Asheville, NC 28801 USA. [Smith, Aaron] Univ Corp Atmospher Res, Boulder, CO 80301 USA. [Waple, Anne] NOAA, Natl Climat Data Ctr, Asheville, NC 28801 USA. RP Tilmes, C (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Curt.Tilmes@nasa.gov OI Zednik, Stephan/0000-0002-5635-9501; Ma, Xiaogang/0000-0002-9110-7369 NR 11 TC 9 Z9 9 U1 0 U2 9 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 NOV PY 2013 VL 51 IS 11 SI SI BP 5160 EP 5168 DI 10.1109/TGRS.2013.2262179 PG 9 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 247DY UT WOS:000326596500012 ER PT J AU Thurai, M Bringi, VN Petersen, WA Gatlin, PN AF Thurai, M. Bringi, V. N. Petersen, W. A. Gatlin, P. N. TI Drop Shapes and Fall Speeds in Rain: Two Contrasting Examples SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article DE Precipitation; Cloud microphysics ID VIDEO DISDROMETER; ERROR ANALYSIS; OSCILLATION FREQUENCIES; LABORATORY MEASUREMENTS; POLARIZATION RADAR; BACKSCATTER RATIOS; VERTICAL INCIDENCE; DOPPLER RADAR; WIND-TUNNEL; C-BAND AB Two rain events are analyzed using two collocated 2D-video disdrometers (2DVD) and a C-band polarimetric radar at 15-km distance. Both events had moderate-to-intense rainfall rates, but the second event had an embedded convective line. For the first event, the fall speed distribution for a given drop diameter interval showed a narrow and symmetric distribution with a mode at the expected value; the second event produced a wider distribution with a significant skewness toward lower fall speeds. The slower drops in the second event were detected while the convective line was directly over the 2DVD site. Drop shape information from the two 2DVD instruments showed that, during the passage of the convection line, around 30%-40% of the drops did not have an axis of rotational symmetry, whereas for event 1, it was only 5%. The implications are that for event 1 the dominant mode of drop oscillation is the axisymmetric mode, and that within the convective line of event 2 other fundamental modes were frequent. The radar data for the second event were analyzed in terms of the self-consistency among the radar-measured quantities. The K-dp/Z(h) versus Z(dr) variations within the line convection were not consistent with the corresponding variation determined from the scattering calculations using the measured 1-min drop size distributions and using the reference drop shapes. Also found were low (hv) regions within the line convection that were considerably lower than the scattering calculations. These findings are consistent with the asymmetric oscillation modes inferred from the 2DVD measurements for event 2 (probably collision induced) within the convective line. C1 [Thurai, M.; Bringi, V. N.] Colorado State Univ, Dept Elect & Comp Engn, Ft Collins, CO 80523 USA. [Petersen, W. A.] NASA, Wallops Flight Facil, Wallops Isl, VA USA. [Gatlin, P. N.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Thurai, M (reprint author), Colorado State Univ, Dept Elect & Comp Engn, Ft Collins, CO 80523 USA. EM merhala@engr.colostate.edu RI Measurement, Global/C-4698-2015; OI Gatlin, Patrick/0000-0001-9345-1457 FU National Science Foundation [AGS-0924622]; NASA [NNX10AJ12G]; Global Precipitation Measurement Mission Flight Project FX The work is primarily supported by the National Science Foundation via Grant AGS-0924622. Support from Dr. Ramesh Kakar, NASA Precipitation Measurement Mission (PMM), NASA Grant Award NNX10AJ12G, and the Global Precipitation Measurement Mission Flight Project, is also acknowledged. The authors also thank Dr. Ali Tokay and Dr. Larry Carey for helpful discussions. NR 54 TC 15 Z9 15 U1 1 U2 22 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 NOV PY 2013 VL 52 IS 11 BP 2567 EP 2581 DI 10.1175/JAMC-D-12-085.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 250FW UT WOS:000326836900013 ER PT J AU Garnier, A Pelon, J Dubuisson, P Yang, P Faivre, M Chomette, O Pascal, N Lucker, P Murray, T AF Garnier, Anne Pelon, Jacques Dubuisson, Philippe Yang, Ping Faivre, Michael Chomette, Olivier Pascal, Nicolas Lucker, Pat Murray, Tim TI Retrieval of Cloud Properties Using CALIPSO Imaging Infrared Radiometer. Part II: Effective Diameter and Ice Water Path SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article DE Cirrus clouds; Cloud microphysics; Algorithms; Cloud retrieval; Satellite observations ID OPERATIONAL VERTICAL SOUNDER; RADIATIVE-TRANSFER MODEL; MU-M WINDOW; CIRRUS CLOUDS; CLIMATE MODELS; ACCURATE PARAMETERIZATION; MICROPHYSICAL PROPERTIES; EFFECTIVE EMISSIVITY; STATISTICAL-ANALYSIS; OPTICAL-THICKNESS AB This paper describes the version-3 level-2 operational analysis of the Imaging Infrared Radiometer (IIR) data collected in the framework of the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) mission to retrieve cirrus cloud effective diameter and ice water path in synergy with the Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) collocated observations. The analysis uses a multisensor split-window technique relying on the concept of microphysical index applied to the two pairs of channels (12.05, 10.6 m) and (12.05, 8.65 m) to retrieve cirrus microphysical properties (effective diameter, ice water path) at 1-km pixel resolution. Retrievals are performed for three crystal families selected from precomputed lookup tables identified as representative of the main relationships between the microphysical indices. The uncertainties in the microphysical indices are detailed and quantified, and the impact on the retrievals is simulated. The possible biases have been assessed through consistency checks that are based on effective emissivity difference. It has been shown that particle effective diameters of single-layered cirrus clouds can be retrieved, for the first time, down to effective emissivities close to 0.05 when accurate measured background radiances can be used and up to 0.95 over ocean and land, as well as over low opaque clouds. The retrieval of the ice water path from the IIR effective optical depth and the effective diameter is discussed. Taking advantage of the cloud boundaries retrieved by CALIOP, an IIR power-law relationship between ice water content and extinction is established for four temperature ranges and shown to be consistent with previous results on average for the chosen dataset. C1 [Garnier, Anne; Lucker, Pat; Murray, Tim] Sci Syst & Applicat Inc, Hampton, VA USA. [Garnier, Anne; Lucker, Pat; Murray, Tim] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Garnier, Anne; Pelon, Jacques; Faivre, Michael] UPMC UVSQ CNRS, Lab Atmospheres, Paris, France. [Dubuisson, Philippe] Univ Lille 1, Opt Atmospher Lab, Lille, France. [Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX USA. [Chomette, Olivier] Ecole Polytech, Meteorol Dynam Lab, Palaiseau, France. [Pascal, Nicolas] Hygeos, Cloud Aerosol Water Radiat Interact ICARE, Lille, France. RP Garnier, A (reprint author), SSAI, 1 Enterprise Pkwy,Suite 200, Hampton, VA 23666 USA. EM anne.garnier@latmos.ipsl.fr RI Yang, Ping/B-4590-2011 FU CNES; Centre National de la Recherche Scientifique (CNRS); Institut National des Sciences de l'Univers (INSU); NASA FX The authors thank F. Parol, C. Stubenrauch, and S. Ackerman for fruitful discussions, the ICARE data center, and the CALIPSO team at NASA Langley Research Center for their help with the IIR level-2 algorithm. The products are processed at NASA/LaRC and are publicly available at NASA/LaRC (https://eosweb.larc.nasa.gov/) and ICARE (http://www.icare.univ-lille1.fr/) data centers. The authors are thankful to CNES, Centre National de la Recherche Scientifique (CNRS), Institut National des Sciences de l'Univers (INSU), and NASA for their support. NR 39 TC 11 Z9 11 U1 5 U2 17 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 NOV PY 2013 VL 52 IS 11 BP 2582 EP 2599 DI 10.1175/JAMC-D-12-0328.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 250FW UT WOS:000326836900014 ER PT J AU Korolev, AV Emery, EF Strapp, JW Cober, SG Isaac, GA AF Korolev, A. V. Emery, E. F. Strapp, J. W. Cober, S. G. Isaac, G. A. TI Quantification of the Effects of Shattering on Airborne Ice Particle Measurements SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article DE Clouds; Snow; Aircraft observations; Instrumentation; sensors ID OPTICAL ARRAY PROBES; WATER-CONTENT; CLOUDS; CRYSTALS; LIQUID; VOLUME; CIRRUS; FSSP AB Ice particle shattering poses a serious problem to the airborne characterization of ice cloud microstructure. Shattered ice fragments may contaminate particle measurements, resulting in artificially high concentrations of small ice. The ubiquitous observation of small ice particles has been debated over the last three decades. The present work is focused on the study of the effect of shattering based on the results of the Airborne Icing Instrumentation Evaluation (AIIE) experiment flight campaign. Quantitative characterization of the shattering effect was studied by comparing measurements from pairs of identical probes, one modified to mitigate shattering using tips designed for this study (K-tips) and the other in the standard manufacturer's configuration. The study focused on three probes: the forward scattering spectrometer probe (FSSP), the optical array probe (OAP-2DC), and the cloud imaging probe (CIP). It has been shown that the overestimation errors of the number concentration in size distributions measured by 2D probes increase with decreasing size, mainly affecting particles smaller than approximately 500 m. It was found that shattering artifacts may increase measured particle number concentration by 1 to 2 orders of magnitude. However, the associated increase of the extinction coefficient and ice water content derived from 2D data is estimated at only 20%-30%. Existing antishattering algorithms alone are incapable of filtering out all shattering artifacts from OAP-2DC and CIP measurements. FSSP measurements can be completely dominated by shattering artifacts, and it is not recommended to use this instrument for measurements in ice clouds, except in special circumstances. Because of the large impact of shattering on ice measurements, the historical data collected by FSSP and OAP-2DC should be reexamined by the cloud physics community. C1 [Korolev, A. V.; Strapp, J. W.; Cober, S. G.; Isaac, G. A.] Environm Canada, Cloud Phys & Severe Weather Res Sect, Toronto, ON M3H 5T4, Canada. [Emery, E. F.] NASA, Glenn Res Ctr, Cleveland, OH USA. [Strapp, J. W.] Met Analyt Inc, Aurora, ON, Canada. RP Korolev, AV (reprint author), Environm Canada, Cloud Phys & Severe Weather Sect, 4905 Dufferin St, Toronto, ON M3H 5T4, Canada. EM alexei.korolev@ec.gc.ca FU Environment Canada; Transport Canada; Federal Aviation Administration; NASA; DMT Inc. FX This work was funded by Environment Canada, Transport Canada, the Federal Aviation Administration, and NASA. Special thanks to Sara Lance (NOAA), Jorge Delgado (NOAA), and Dave Rogers (NCAR) for loaning their cloud particle probes for the AIIE project. We express our sincere gratitude to the NRC pilots Anthony Brown, John Aitken, and Tim Leslie for their outstanding cooperation during the AIIE flight operations. The efforts of the NRC Project Manager Dave Marcotte and NRC technicians in preparing and organizing the Convair-580 flights, and of the participants from DMT Inc. for their self-funded support during the AIIE project, are greatly appreciated. The support and analysis of 2D-S data by Brad Baker and Paul Lawson from SPEC Inc. are much appreciated. Authors express their gratitude to Darrel Baumgardner and two anonymous reviewers for their thoughtful comments. NR 31 TC 32 Z9 33 U1 2 U2 18 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 NOV PY 2013 VL 30 IS 11 BP 2527 EP 2553 DI 10.1175/JTECH-D-13-00115.1 PG 27 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 251SQ UT WOS:000326951400003 ER PT J AU Hoffman, RN Ardizzone, JV Leidner, SM Smith, DK Atlas, R AF Hoffman, Ross N. Ardizzone, Joseph V. Leidner, S. Mark Smith, Deborah K. Atlas, Robert TI Error Estimates for Ocean Surface Winds: Applying Desroziers Diagnostics to the Cross-Calibrated, Multiplatform Analysis of Wind Speed SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article DE Atmosphere-ocean interaction; Data quality control; Microwave observations; Satellite observations; Error analysis; Statistical techniques ID CURRENT SOUNDER RADIANCES; AMBIGUITY REMOVAL; ASSIMILATION AB The Desroziers diagnostics (DD) are applied to the cross-calibrated, multiplatform (CCMP) ocean surface wind datasets to estimate wind speed errors of the ECMWF background, the microwave satellite observations, and the resulting CCMP analysis. The DD confirm that the ECMWF operational surface wind speed error standard deviations vary with latitude in the range 0.8-1.3 m s(-1) and that the cross-calibrated Remote Sensing Systems (RSS) wind speed retrievals' standard deviations are in the range 0.5-0.7 m s(-1). Further, the estimated CCMP analysis wind speed standard deviations are in the range 0.2-0.3 m s(-1). The results suggest the need to revise the parameterization of the errors of the first guess at appropriate time (FGAT) procedure. Errors for wind speeds <16 m s(-1) are homogeneous; however, for the relatively rare but critical higher wind speed situations, errors are much larger. C1 [Hoffman, Ross N.; Leidner, S. Mark] Atmospher & Environm Res, Lexington, MA 02421 USA. [Ardizzone, Joseph V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Smith, Deborah K.] Remote Sensing Syst, Santa Rosa, CA USA. [Atlas, Robert] NOAA, Atlantic Oceanog & Meteorol Lab, Miami, FL 33149 USA. RP Hoffman, RN (reprint author), Atmospher & Environm Res, 131 Hartwell Ave, Lexington, MA 02421 USA. EM ross.n.hoffman@aer.com RI Atlas, Robert/A-5963-2011 OI Atlas, Robert/0000-0002-0706-3560 FU NASA Making Earth Science Data Records for Use in Research Environments (MEaSUREs) program; NASA ROSES [NNX11AO25A] FX This work was supported by grants made through the NASA Making Earth Science Data Records for Use in Research Environments (MEaSUREs) program and through NASA ROSES 2011 [Grant NNX11AO25A to Remote Sensing Systems (RSS), Santa Rosa, California]. NR 17 TC 5 Z9 5 U1 0 U2 4 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 NOV PY 2013 VL 30 IS 11 BP 2596 EP 2603 DI 10.1175/JTECH-D-13-00018.1 PG 8 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 251SQ UT WOS:000326951400007 ER PT J AU Raccanelli, A Bertacca, D Pietrobon, D Schmidt, F Samushia, L Bartolo, N Dore, O Matarrese, S Percival, WJ AF Raccanelli, Alvise Bertacca, Daniele Pietrobon, Davide Schmidt, Fabian Samushia, Lado Bartolo, Nicola Dore, Olivier Matarrese, Sabino Percival, Will J. TI Testing gravity using large-scale redshift-space distortions SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: analytical; cosmological parameters; cosmology: observations; large-scale structure of Universe ID DIGITAL SKY SURVEY; LUMINOUS RED GALAXIES; UNIFIED DARK-MATTER; SDSS-III; PECULIAR VELOCITIES; EVOLUTION; GROWTH; BIAS; COSMOLOGY; UNIVERSE AB We use luminous red galaxies from the Sloan Digital Sky Survey (SDSS) II to test the cosmological structure growth in two alternatives to the standard Lambda cold dark matter (Lambda CDM)+general relativity (GR) cosmological model. We compare observed three-dimensional clustering in SDSS Data Release 7 (DR7) with theoretical predictions for the standard vanilla Lambda CDM+GR model, unified dark matter (UDM) cosmologies and the normal branch Dvali-Gabadadze-Porrati (nDGP). In computing the expected correlations in UDM cosmologies, we derive a parametrized formula for the growth factor in these models. For our analysis we apply the methodology tested in Raccanelli et al. and use the measurements of Samushia et al. that account for survey geometry, non-linear and wide-angle effects and the distribution of pair orientation. We show that the estimate of the growth rate is potentially degenerate with wide-angle effects, meaning that extremely accurate measurements of the growth rate on large scales will need to take such effects into account. We use measurements of the zeroth and second-order moments of the correlation function from SDSS DR7 data and the Large Suite of Dark Matter Simulations (LasDamas), and perform a likelihood analysis to constrain the parameters of the models. Using information on the clustering up to r(max) = 120 h(-1) Mpc, and after marginalizing over the bias, we find, for UDM models, a speed of sound c(infinity) <= 6.1e-4, and, for the nDGP model, a cross-over scale r(c) >= 340 Mpc, at 95 per cent confidence level. C1 [Raccanelli, Alvise; Pietrobon, Davide; Dore, Olivier] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Raccanelli, Alvise; Schmidt, Fabian; Dore, Olivier] CALTECH, Pasadena, CA 91125 USA. [Bertacca, Daniele] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. [Bertacca, Daniele; Bartolo, Nicola; Matarrese, Sabino] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Samushia, Lado; Percival, Will J.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth P01 3FX, Hants, England. [Bartolo, Nicola; Matarrese, Sabino] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. RP Raccanelli, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM raccanelli@gmail.com OI Raccanelli, Alvise/0000-0001-6726-0438; Matarrese, Sabino/0000-0002-2573-1243 FU Gordon and Betty Moore Foundation at Caltech; European Research Council; STFC; Georgian National Science Foundation [ST08/4-442]; SNSF [128040]; National Aeronautics and Space Administration FX Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. AR would like to thank for the hospitality the Institute of Cosmology and Gravitation at the University of Portsmouth, where part of this work was carried out. FS is supported by the Gordon and Betty Moore Foundation at Caltech. WJP is grateful for support from the European Research Council and STFC. LS acknowledges support from European Research Council, Georgian National Science Foundation grant ST08/4-442 and SNSF (SCOPES grant No. 128040). NR 92 TC 17 Z9 17 U1 0 U2 3 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 NOV PY 2013 VL 436 IS 1 BP 89 EP 100 DI 10.1093/mnras/stt1517 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 245BY UT WOS:000326435100030 ER PT J AU Mason, E Orio, M Mukai, K Bianchini, A de Martino, D di Mille, F Williams, RE Abbot, T de Propris, R Luna, GJM AF Mason, E. Orio, M. Mukai, K. Bianchini, A. de Martino, D. di Mille, F. Williams, R. E. Abbot, T. de Propris, R. Luna, G. J. M. TI On the nature of CP Pup SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: individual: CP Pup; novae, cataclysmic variables ID CATACLYSMIC VARIABLES; OLD NOVA; INTERMEDIATE POLARS; DOPPLER TOMOGRAPHY; WHITE-DWARFS; T-PYXIDIS; ACCRETION; PERIOD; CAMELOPARDALIS; EMISSION AB We present new X-ray and optical spectra of the old nova CP Pup (nova Pup 1942) obtained with Chandra and the Cerro Tololo Inter American Observatory (CTIO) 4 m telescope. The X-ray spectrum reveals a multitemperature optically thin plasma reaching amaximum temperature of 36(-16)(+19) keV absorbed by local complex neutral material. The time-resolved optical spectroscopy confirms the presence of the similar to 1.47 h period, with cycle-to-cycle amplitude changes, as well as of an additional long-term modulation which is suggestive either of a longer period or of non-Keplerian velocities in the emission line regions. These new observational facts add further support to CP Pup as a magnetic cataclysmic variable (mCV). We compare the mCV and the non-mCV scenarios and, while we cannot conclude whether CP Pup is a long-period system, all pieces of observational evidence point at an intermediate polar-type CV. C1 [Mason, E.] Osserv Astron Trieste, INAF, I-14343 Trieste, Italy. [Mason, E.; Williams, R. E.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Orio, M.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Orio, M.] Univ Wisconsin, Dept Astron, Madison, WI 53704 USA. [Mukai, K.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Mukai, K.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Mukai, K.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Bianchini, A.; di Mille, F.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [de Martino, D.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [di Mille, F.] Carnegie Observ, Australian Astron Observ, La Serena, Chile. [Abbot, T.; de Propris, R.] AURA CTIO, La Serena, Chile. [Luna, G. J. M.] Inst Astron & Fis Espacio, Caba, Argentina. RP Mason, E (reprint author), Osserv Astron Trieste, INAF, Via GB Tiepolo 11, I-14343 Trieste, Italy. EM emason@oats.inaf.it OI mason, elena/0000-0003-3877-0484; de Martino, Domitilla/0000-0002-5069-4202 NR 43 TC 1 Z9 1 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 NOV PY 2013 VL 436 IS 1 BP 212 EP 221 DI 10.1093/mnras/stt1565 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 245BY UT WOS:000326435100039 ER PT J AU Roseboom, IG Dunlop, JS Cirasuolo, M Geach, JE Smail, I Halpern, M van der Werf, P Almaini, O Arumugam, V Asboth, V Auld, R Blain, A Bremer, MN Bock, J Bowler, RAA Buitrago, F Chapin, E Chapman, S Chrysostomou, A Clarke, C Conley, A Coppin, KEK Danielson, ALR Farrah, D Glenn, J Hatziminaoglou, E Ibar, E Ivison, RJ Jenness, T Van Kampen, E Karim, A Mackenzie, T Marsden, G Meijerink, R Michalowski, MJ Oliver, SJ Page, MJ Pearson, E Scott, D Simpson, JM Smith, DJB Spaans, M Swinbank, AM Symeonidis, M Targett, T Valiante, E Viero, M Wang, L Willott, CJ Zemcov, M AF Roseboom, I. G. Dunlop, J. S. Cirasuolo, M. Geach, J. E. Smail, I. Halpern, M. van der Werf, P. Almaini, O. Arumugam, V. Asboth, V. Auld, R. Blain, A. Bremer, M. N. Bock, J. Bowler, R. A. A. Buitrago, F. Chapin, E. Chapman, S. Chrysostomou, A. Clarke, C. Conley, A. Coppin, K. E. K. Danielson, A. L. R. Farrah, D. Glenn, J. Hatziminaoglou, E. Ibar, E. Ivison, R. J. Jenness, T. Van Kampen, E. Karim, A. Mackenzie, T. Marsden, G. Meijerink, R. Michalowski, M. J. Oliver, S. J. Page, M. J. Pearson, E. Scott, Douglas Simpson, J. M. Smith, D. J. B. Spaans, M. Swinbank, A. M. Symeonidis, M. Targett, T. Valiante, E. Viero, M. Wang, L. Willott, C. J. Zemcov, M. TI The SCUBA-2 Cosmology Legacy Survey: demographics of the 450-mu m population SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: starburst; submillimetre: galaxies ID STAR-FORMING GALAXIES; DEEP FIELD-SOUTH; ULTRALUMINOUS INFRARED GALAXIES; DEGREE EXTRAGALACTIC SURVEY; HIGH-REDSHIFT GALAXIES; EQUAL-TO 4; SUBMILLIMETER GALAXIES; MU-M; HERSCHEL-ATLAS; NUMBER COUNTS AB We investigate the multiwavelength properties of a sample of 450-mu m-selected sources from the SCUBA-2 Cosmology Legacy Survey. A total of 69 sources were identified above 4 sigma in deep SCUBA-2 450-mu m observations overlapping the UDS and COSMOS fields and covering 210 arcmin(2) to a typical depth of sigma(450) = 1.5 mJy. Reliable cross-identifications are found for 58 sources (84 per cent) in Spitzer and Hubble Space Telescope WFC3/IR data. The photometric redshift distribution (dN/dz) of 450-mu m-selected sources is presented, showing a broad peak in the redshift range 1 < z < 3 and a median of z = 1.4. Combining the SCUBA-2 photometry with Herschel SPIRE data from HerMES, the submm spectral energy distribution (SED) is examined via the use of modified blackbody fits, yielding aggregate values for the IR luminosity, dust temperature and emissivity of < L-IR > = 10(12 +/- 0.8) L-circle dot, < T-D > = 42 +/- 11 K and = 1.6 +/- 0.5, respectively. The relationship between these SED parameters and the physical properties of galaxies is investigated, revealing correlations between T-D and L-IR and between beta(D) and both stellar mass and effective radius. The connection between the star formation rate (SFR) and stellar mass is explored, with 24 per cent of 450-mu m sources found to be 'starbursts', i.e. displaying anomalously high specific SFRs. However, both the number density and observed properties of these 'starburst' galaxies are found to be consistent with the population of normal star-forming galaxies. C1 [Roseboom, I. G.; Dunlop, J. S.; Cirasuolo, M.; Bowler, R. A. A.; Buitrago, F.; Ivison, R. J.; Michalowski, M. J.; Targett, T.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Geach, J. E.; Coppin, K. E. K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Smail, I.; Danielson, A. L. R.; Karim, A.; Simpson, J. M.; Swinbank, A. M.; Wang, L.] Univ Durham, Inst Computat Cosmol, Dept Phys, Durham DH1 3LE, England. [Halpern, M.; Asboth, V.; Chapin, E.; Mackenzie, T.; Marsden, G.; Scott, Douglas] Univ British Columbia, Dept Phys Astron, Vancouver, BC V6T 1Z1, Canada. [van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Almaini, O.] Univ Nottingham, Sch Phys & Astron, Nottingham NG9 2RD, England. [Arumugam, V.; Ibar, E.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Auld, R.; Pearson, E.; Valiante, E.] Cardiff Univ, Cardiff Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Blain, A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Bremer, M. N.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Bock, J.; Viero, M.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chapin, E.] ESAC, XMM SOC, E-28691 Madrid, Spain. [Chapman, S.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. [Chrysostomou, A.; Smith, D. J. B.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Chrysostomou, A.; Jenness, T.] Joint Astron Ctr, Hilo, HI 96720 USA. [Clarke, C.; Oliver, S. J.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Conley, A.; Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA UCB 389, Boulder, CO 80309 USA. [Farrah, D.] Virginia Polytech Inst & State Univ, Dept Phys, Blacksburg, VA 24061 USA. [Hatziminaoglou, E.; Van Kampen, E.] ESO, D-85748 Garching, Germany. [Jenness, T.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Meijerink, R.; Spaans, M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Michalowski, M. J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium. [Page, M. J.; Symeonidis, M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Willott, C. J.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. RP Roseboom, IG (reprint author), Univ Edinburgh, Inst Astron, Royal Observ, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. EM igr@roe.ac.uk RI Smail, Ian/M-5161-2013; Ivison, R./G-4450-2011; OI Smail, Ian/0000-0003-3037-257X; Ivison, R./0000-0001-5118-1313; Scott, Douglas/0000-0002-6878-9840 FU Royal Society; European Research Council; STFC [ST/I001573/1]; Leverhulme Fellowship; ERC; Science and Technology Facilities Council [ST/I000976/1]; Canada Foundation for Innovation; CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA) FX JSD acknowledges the support of the Royal Society via a Wolfson Research Merit award and the support of the European Research Council via the award of an Advanced Grant.; IRS acknowledges support from STFC (ST/I001573/1), a Leverhulme Fellowship, the ERC Advanced Investigator programme DUSTYGAL and a Royal Society/Wolfson Merit Award.; LW and SJO were supported by the Science and Technology Facilities Council (grant number ST/I000976/1).; The James Clerk Maxwell Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the National Research Council of Canada and (until 2013 March 31) the Netherlands Organisation for Scientific Research. Additional funds for the construction of SCUBA-2 were provided by the Canada Foundation for Innovation.; SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK), 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); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). All the data used in this analysis are available through the JCMT, Herschel, HST and Spitzer archives. NR 102 TC 13 Z9 13 U1 1 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 NOV PY 2013 VL 436 IS 1 BP 430 EP 448 DI 10.1093/mnras/stt1577 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 245BY UT WOS:000326435100058 ER PT J AU Kennedy, GM Wyatt, MC Bryden, G Wittenmyer, R Sibthorpe, B AF Kennedy, G. M. Wyatt, M. C. Bryden, G. Wittenmyer, R. Sibthorpe, B. TI Star-planet-debris disc alignment in the HD 82943 system: is planetary system coplanarity actually the norm? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE planets and satellites: formation; circumstellar matter; stars: individual: HD 82943; planetary systems ID SPIN-ORBIT ALIGNMENT; SPITZER-SPACE-TELESCOPE; BETA-PICTORIS B; HR 8799; EXTRASOLAR PLANETS; EXOPLANETARY SYSTEMS; FOMALHAUT B; HERSCHEL; MISALIGNMENT; EVOLUTION AB Recent results suggest that the two planets in the HD 82943 system are inclined to the sky plane by 20 +/- 4 degrees. Here, we show that the debris disc in this system is inclined by 27 +/- 4 degrees, thus adding strength to the derived planet inclinations and suggesting that the planets and debris disc are consistent with being aligned at a level similar to the Solar system. Further, the stellar equator is inferred to be inclined by 28 +/- 4 degrees, suggesting that the entire star-planet-disc system is aligned, the first time such alignment has been tested for radial velocity discovered planets on similar to au wide orbits. We show that the planet-disc alignment is primordial, and not the result of planetary secular perturbations to the disc inclination. In addition, we note three other systems with planets at greater than or similar to 10 au discovered by direct imaging that already have good evidence of alignment, and suggest that empirical evidence of system-wide star-planet-disc alignment is therefore emerging, with the exception of systems that host hot Jupiters. While this alignment needs to be tested in a larger number of systems, and is perhaps unsurprising, it is a reminder that the system should be considered as a whole when considering the orientation of planetary orbits. C1 [Kennedy, G. M.; Wyatt, M. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Bryden, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wittenmyer, R.] Univ New S Wales, Sch Phys, Dept Astrophys, Sydney, NSW 2052, Australia. [Sibthorpe, B.] Univ Groningen, 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] FX We thank the referee for a concise review and help on transiting planet details. This work was supported by the European Union through ERC grant number 279973 (GMK & MCW). This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org. 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 NOV PY 2013 VL 436 IS 1 BP 898 EP 903 DI 10.1093/mnras/stt1657 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 245BY UT WOS:000326435100093 ER PT J AU King, OG Hovatta, T Max-Moerbeck, W Meier, DL Pearson, TJ Readhead, ACS Reeves, R Richards, JL Shepherd, MC AF King, O. G. Hovatta, T. Max-Moerbeck, W. Meier, D. L. Pearson, T. J. Readhead, A. C. S. Reeves, R. Richards, J. L. Shepherd, M. C. TI A quasi-periodic oscillation in the blazar J1359+4011 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; galaxies: active; galaxies: individual: J1359+4011; galaxies: jets ID LOW-FREQUENCY OSCILLATIONS; ACTIVE GALACTIC NUCLEI; BL-LACERTAE; BLACK-HOLE; SOURCE CATALOG; VARIABILITY; RADIO; ACCRETION; PRECESSION; WAVELETS AB The Owens Valley Radio Observatory 40-m telescope has been monitoring the 15-GHz radio flux density of over 1200 blazars since 2008. The 15-GHz light curve of the flat spectrum radio quasar J1359+4011 shows a strong and persistent quasi-periodic oscillation. The time-scale of the oscillation varies between 120 and 150 d over an similar to 4 year time span. We interpret this as the active galactic nucleus mass-scaled analogue of low-frequency quasi-periodic oscillations from Galactic microquasars or as evidence of modulation of the accretion flow by thermal instabilities in the 'inner' accretion disc. C1 [King, O. G.; Hovatta, T.; Pearson, T. J.; Readhead, A. C. S.; Reeves, R.; Shepherd, M. C.] CALTECH, Pasadena, CA 91125 USA. [Max-Moerbeck, W.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Meier, D. L.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Richards, J. L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. RP King, OG (reprint author), CALTECH, 1200 E Calif Blvd,MC 249-17, Pasadena, CA 91125 USA. EM ogk@astro.caltech.edu RI Reeves, Rodrigo/H-2812-2014; Pearson, Timothy/N-2376-2015 OI Reeves, Rodrigo/0000-0001-5704-271X; Pearson, Timothy/0000-0001-5213-6231 FU NASA [NNX08AW31G, NNX11A043G]; NSF [AST-0808050, AST-1109911]; Jenny and Antti Wihuri foundation; National Aeronautics and Space Administration FX We thank Russ Keeney for his support of observations at OVRO. The OVRO 40-m programme is supported in part by NASA grants NNX08AW31G and NNX11A043G and NSF grants AST-0808050 and AST-1109911. TH was supported by the Jenny and Antti Wihuri foundation. Support from MPIfR for upgrading the OVRO 40-m telescope receiver is acknowledged. We thank V. Pavlidou for useful discussions. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 39 TC 7 Z9 7 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 NOV PY 2013 VL 436 IS 1 BP L114 EP L117 DI 10.1093/mnrasl/slt125 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 245BY UT WOS:000326435100024 ER PT J AU Pearson, EA Eales, S Dunne, L Gonzalez-Nuevo, J Maddox, S Aguirre, JE Baes, M Baker, AJ Bourne, N Bradford, CM Clark, CJR Cooray, A Dariush, A De Zotti, G Dye, S Frayer, D Gomez, HL Harris, AI Hopwood, R Ibar, E Ivison, RJ Jarvis, M Krips, M Lapi, A Lupu, RE Michalowski, MJ Rosenman, M Scott, D Valiante, E Valtchanov, I van der Werf, P Vieira, JD AF Pearson, E. A. Eales, S. Dunne, L. Gonzalez-Nuevo, J. Maddox, S. Aguirre, J. E. Baes, M. Baker, A. J. Bourne, N. Bradford, C. M. Clark, C. J. R. Cooray, A. Dariush, A. De Zotti, G. Dye, S. Frayer, D. Gomez, H. L. Harris, A. I. Hopwood, R. Ibar, E. Ivison, R. J. Jarvis, M. Krips, M. Lapi, A. Lupu, R. E. Michalowski, M. J. Rosenman, M. Scott, D. Valiante, E. Valtchanov, I. van der Werf, P. Vieira, J. D. TI H-ATLAS: estimating redshifts of Herschel sources from sub-mm fluxes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: high-redshift; galaxies: photometry; submillimetre: galaxies ID STRONGLY LENSED GALAXIES; SUBMILLIMETER GALAXIES; STAR-FORMATION; SKY SURVEY; COLD DUST; POPULATION; UNIVERSE; EVOLUTION; ENERGY; SPIRE AB Upon its completion, the Herschel Astrophysics Terahertz Large Area Survey (H-ATLAS) will be the largest sub-millimetre survey to date, detecting close to half-a-million sources. It will only be possible to measure spectroscopic redshifts for a small fraction of these sources. However, if the rest-frame spectral energy distribution (SED) of a typical H-ATLAS source is known, this SED and the observed Herschel fluxes can be used to estimate the redshifts of the H-ATLAS sources without spectroscopic redshifts. In this paper, we use a sub-set of 40 H-ATLAS sources with previously measured redshifts in the range 0.5 < z < 4.2 to derive a suitable average template for high-redshift H-ATLAS sources. We find that a template with two dust components (T-c = 23.9 K, T-h = 46.9 K and ratio of mass of cold dust to mass of warm dust of 30.1) provides a good fit to the rest-frame fluxes of the sources in our calibration sample. We use a jackknife technique to estimate the accuracy of the redshifts estimated with this template, finding a root mean square of delta z/(1 + z) = 0.26. For sources for which there is prior information that they lie at z > 1, we estimate that the rms of delta z/(1 + z) = 0.12. We have used this template to estimate the redshift distribution for the sources detected in the H-ATLAS equatorial fields, finding a bimodal distribution with a mean redshift of 1.2, 1.9 and 2.5 for 250, 350 and 500 mu m selected sources, respectively. C1 [Pearson, E. A.; Eales, S.; Clark, C. J. R.; Gomez, H. L.; Valiante, E.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92617 USA. [Dunne, L.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [Gonzalez-Nuevo, J.] CSIC UC, Inst Fis Cantabria, E-39005 Santander, Spain. [Maddox, S.] Natl Radio Astron Observ, Green Bank, WV 24944 USA. [Aguirre, J. E.; Lupu, R. E.; Rosenman, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Baes, M.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium. [Baker, A. J.] State Univ New Jersey, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Bourne, N.; Dye, S.; Hopwood, R.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Bradford, C. M.] Jet Prop Lab, Pasadena, CA 91109 USA. [Dariush, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92617 USA. [De Zotti, G.] SISSA, I-34136 Trieste, Italy. [De Zotti, G.] INAF, Osservatorio Astronom Padova, I-35122 Padua, Italy. [Harris, A. I.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Ibar, E.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Jarvis, M.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Krips, M.] IRAM, F-38400 St Martin Hres, France. [Lapi, A.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Michalowski, M. J.] Univ Edinburgh, Inst Astron, Scottish Univ Phys Alliance, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Scott, D.] Univ British Columbia, Vancouver, BC V6T 1Z1, Canada. [Valtchanov, I.] SRE SDH, European Space Agcy, E-28691 Madrid, Spain. [van der Werf, P.] Leiden Univ, Leiden Observ, NL-23100 RA Leiden, Netherlands. [Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. RP Pearson, EA (reprint author), Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92617 USA. EM Elizabeth.Pearson@astro.cf.ac.uk RI Lupu, Roxana/P-9060-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Ivison, R./G-4450-2011; OI Lupu, Roxana/0000-0003-3444-5908; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Baes, Maarten/0000-0002-3930-2757; Ivison, R./0000-0001-5118-1313; De Zotti, Gianfranco/0000-0003-2868-2595; Maddox, Stephen/0000-0001-5549-195X; Scott, Douglas/0000-0002-6878-9840; Dye, Simon/0000-0002-1318-8343 FU STFC (UK); ARC (Australia); AAO; CSA (Canada); NAOC (China); CEA; CNES; CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); NASA (USA); National Radio Astronomy Observatory; Spanish CSIC for a JAE-DOC; Spanish Ministerio de Ciencia e Innovacion [AYA2010-21766-C03-01] FX The Herschel-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/. 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 UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programmes including GALEX MIS, VST KIDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT and ASKAP providing UV to radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO and the participating institutions. The GAMA website is http://www.gama-survey.org/. SPIRE has been developed by a consortium of institutes led by Cardiff University (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); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK) and NASA (USA). KSS is supported by the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. JGN acknowledges financial support from Spanish CSIC for a JAE-DOC fellowship and partial financial support from the Spanish Ministerio de Ciencia e Innovacion project AYA2010-21766-C03-01. NR 51 TC 9 Z9 9 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 NOV PY 2013 VL 435 IS 4 BP 2753 EP 2763 DI 10.1093/mnras/stt1369 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 236DP UT WOS:000325774700001 ER PT J AU Bernardini, F de Martino, D Mukai, K Falanga, M Andruchow, I Bonnet-Bidaud, JM Masetti, N Buitrago, DHG Mouchet, M Tovmassian, G AF Bernardini, F. de Martino, D. Mukai, K. Falanga, M. Andruchow, I. Bonnet-Bidaud, J. -M. Masetti, N. Gonzalez Buitrago, D. H. Mouchet, M. Tovmassian, G. TI On the nature of the hard X-ray sources SWIFT J1907.3-2050, IGR J12123-5802 and IGR J19552+0044 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE X-rays: individual: Swift J1907; 3-2050 (also known as: V1082 Sgr); X-rays: individual: Swift J1212; 3-5806 (also known as: IGR J12123-5802 and 1RXS J121222; 7-580118); X-rays: individual: IGR J19552+0044; X-rays: individual: WISE J195512; 47+004536; 6 ID MAGNETIC CATACLYSMIC VARIABLES; STATIONARY RADIATION HYDRODYNAMICS; OPTICAL SPECTROSCOPY; INTEGRAL OBJECTS; WHITE-DWARF; XMM-NEWTON; INTERMEDIATE POLARS; AM HERCULIS; LIMITING WINDOW; XSS J12270-4859 AB The INTEGRAL and Swift hard X-ray surveys have identified a large number of new sources, among which many are proposed as Cataclysmic Variables (CVs). Here, we present the first detailed study of three X-ray-selected CVs, Swift J1907.3-2050, IGR J12123-5802 and IGR J19552+0044 based on XMM-Newton, Suzaku, Swift observations and ground-based optical and archival (near-IR) nIR/IR data. Swift J1907.3-2050 is highly variable from hours to months-years at all wavelengths. No coherent X-ray pulses are detected but rather transient features. The X-ray spectrum reveals a multitemperature optically thin plasma absorbed by complex neutral material and a soft blackbody component arising from a small area. These characteristics are remarkably similar to those observed in magnetic CVs. A supra-solar abundance of nitrogen could arise from nuclear processed material from the donor star. Swift J1907.3-2050 could be a peculiar magnetic CV with the second longest (20.82 h) binary period. IGR J12123-5802 is variable in the X-rays on a time-scale of greater than or similar to 7.6 h. No coherent pulsations are detected, but its spectral characteristics suggest that it could be a magnetic CV of the Intermediate Polar (IP) type. IGR J19552+0044 shows two X-ray periods, similar to 1.38 h and similar to 1.69 h and an X-ray spectrum characterized by a multitemperature plasma with little absorption. We derive a low accretion rate, consistent with a CV below the orbital period gap. Its peculiar nIR/IR spectrum suggests a contribution from cyclotron emission. It could either be a pre-polar or an IP with the lowest degree of asynchronism. C1 [Bernardini, F.] Wayne State Univ, Detroit, MI 48201 USA. [Bernardini, F.; de Martino, D.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Mukai, K.] NASA, Goddard Space Flight Ctr, CRESST & X Ray Astrophys Lab, Greenbelt, MD 20771 USA. [Mukai, K.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Falanga, M.] ISSI, CH-3012 Bern, Switzerland. [Andruchow, I.] CONICET UNLP, Fac Ciencias Astron & Geofis, Buenos Aires, DF, Argentina. [Andruchow, I.] CONICET UNLP, Inst Astrofis La Plata, Buenos Aires, DF, Argentina. [Bonnet-Bidaud, J. -M.] CEA Saclay, DSM Irfu Serv Astrophys, F-91191 Gif Sur Yvette, France. [Masetti, N.] INAF Ist Astrofis Spaziale, I-40129 Bologna, Italy. [Gonzalez Buitrago, D. H.; Tovmassian, G.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico. [Mouchet, M.] Univ Paris 07, Lab APC, F-75005 Paris, France. [Mouchet, M.] Observ Paris, LUTH, Sect Meudon, F-92195 Meudon, France. RP Bernardini, F (reprint author), Wayne State Univ, 666 W Hancock St, Detroit, MI 48201 USA. EM bernardini@wayne.edu RI XRAY, SUZAKU/A-1808-2009; OI Bernardini, Federico/0000-0001-5326-2010; de Martino, Domitilla/0000-0002-5069-4202 FU ESA Member States; Swift; NASA; National Aeronautics and Space Administration; Two Micron All Sky Survey (2MASS); University of Massachusetts; Infrared Processing and Analysis Center (IPAC)/Caltech; NSF; Sloan Digital Sky Survey (SDSS) FX This work is based on observations obtained with XMM-Newton an ESA science mission with instruments and contributions directly funded by ESA Member States; with Swift, a NASA science mission with Italian participation; and Suzaku, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). This publication also 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; the Two Micron All Sky Survey (2MASS), a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center (IPAC)/Caltech, funded by NASA and the NSF; and the Sloan Digital Sky Survey (SDSS). NR 66 TC 7 Z9 7 U1 1 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 NOV PY 2013 VL 435 IS 4 BP 2822 EP 2834 DI 10.1093/mnras/stt1434 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 236DP UT WOS:000325774700005 ER PT J AU Koens, LA Maughan, BJ Jones, LR Ebeling, H Horner, DJ Perlman, ES Phillipps, S Scharf, CA AF Koens, L. A. Maughan, B. J. Jones, L. R. Ebeling, H. Horner, D. J. Perlman, E. S. Phillipps, S. Scharf, C. A. TI The WARPS Survey - VIII. Evolution of the galaxy cluster X-ray Luminosity Function SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: general; cosmology: observations; X-rays: galaxies: clusters ID MEDIUM-SENSITIVITY SURVEY; ECLIPTIC POLE SURVEY; FLUX-LIMITED SAMPLE; DIGITAL SKY SURVEY; COSMOLOGICAL CONSTRAINTS; OBSERVED GROWTH; SOURCE CATALOG; PARAMETERS; VARIANCE; IV AB We present measurements of the galaxy cluster X-ray Luminosity Function (XLF) from the Wide Angle ROSAT Pointed Survey (WARPS) and quantify its evolution. WARPS is a serendipitous survey of the central region of ROSAT pointed observations and was carried out in two phases (WARPS-I and WARPS-II). The results here are based on a final sample of 124 clusters, complete above a flux limit of 6.5 x 10(-14) erg cm(-2) s(-1), with members out to redshift z similar to 1.05, and a sky coverage of 70.9 deg(2). We find significant evidence for negative evolution of the XLF, which complements the majority of X-ray cluster surveys. To quantify the suggested evolution, we perform a maximum likelihood analysis and conclude that the evolution is driven by a decreasing number density of high-luminosity clusters with redshift, while the bulk of the cluster population remains nearly unchanged out to redshift z approximate to 1.1, as expected in a low-density universe. The results are found to be insensitive to a variety of sources of systematic uncertainty that affect the measurement of the XLF and determination of the survey selection function. We perform a Bayesian analysis of the XLF to fully account for uncertainties in the local XLF on the measured evolution, and find that the detected evolution remains significant at the 95 per cent level. We observe a significant excess of clusters in the WARPS at 0.1 < z < 0.3 and L-X approximate to 2 x 10(43) erg s(-1) compared with the reference low-redshift XLF, or our Bayesian fit to the WARPS data. We find that the excess cannot be explained by sample variance, or Eddington bias, and is unlikely to be due to problems with the survey selection function. C1 [Koens, L. A.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Koens, L. A.; Maughan, B. J.; Phillipps, S.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Jones, L. R.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Ebeling, H.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Horner, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Perlman, E. S.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Scharf, C. A.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. RP Koens, LA (reprint author), Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. EM lak@roe.ac.uk OI Phillipps, Steven/0000-0001-5991-3486 FU European Research Council under the EC [240185] FX We thank Chris Collins and Andy Young for useful discussions. LK acknowledges support from the European Research Council under the EC FP7 grant number 240185. 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. NR 61 TC 4 Z9 4 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 NOV PY 2013 VL 435 IS 4 BP 3231 EP 3242 DI 10.1093/mnras/stt1519 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 236DP UT WOS:000325774700037 ER PT J AU Simpson, JP Whitney, BA Hines, DC Schneider, G Burton, MG Colgan, SWJ Cotera, AS Erickson, EF Wolff, MJ AF Simpson, Janet P. Whitney, Barbara A. Hines, Dean C. Schneider, Glenn Burton, Michael G. Colgan, Sean W. J. Cotera, Angela S. Erickson, Edwin F. Wolff, Michael J. TI Aligned grains and inferred toroidal magnetic fields in the envelopes of massive young stellar objects(star) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: massive; stars: protostars; ISM: jets and outflows; ISM: magnetic fields; infrared: ISM; infrared: stars ID INFRARED IMAGING POLARIMETRY; BISPECTRUM SPECKLE INTERFEROMETRY; PROTOSTELLAR DISK FORMATION; SPECTRAL ENERGY-DISTRIBUTIONS; MODEL SCATTERING ENVELOPES; STAR-FORMING REGIONS; OPHIUCHI CLOUD CORE; MOLECULAR CLOUD; OUTFLOW SOURCE; MONOCEROS R2 AB Massive young stellar objects (YSOs), like low-mass YSOs, are thought to be surrounded by optically thick envelopes and/or discs and are observed to have associated regions that produce polarized light at near-infrared wavelengths. These polarized regions are thought to be lower density outflows along the polar axes of the YSO envelopes. Using the 0.2 arcsec spatial resolution of Near-Infrared Camera and Multi-Object Spectrometer on the Hubble Space Telescope, we are examining the structure of the envelopes and outflow regions of massive YSOs in star-forming regions within a few kpc of the Sun. Here, we report on 2 mu m polarimetry of Mon R2-IRS3, S140-IRS1 and AFGL 2591. All three sources contain YSOs with highly polarized monopolar outflows, with Mon R2-IRS3 containing at least two YSOs in a small cluster. The central stars of all four YSOs are also polarized, with position angles perpendicular to the directions of the outflows. We infer that this polarization is due to scattering and absorption by aligned grains. We have modelled our observations of S140-IRS1 and AFGL 2591 as light scattered and absorbed both by spherical grains and by elongated grains that are aligned by magnetic fields. Models that best reproduce the observations have a substantial toroidal component to the magnetic field in the equatorial plane. Moreover, the toroidal magnetic field in the model that best fits AFGL 2591 extends a large fraction of the height of the model cavity, which is 10(5) au. We conclude that the massive YSOs in this study all show evidence of the presence of a substantial toroidal magnetic field. C1 [Simpson, Janet P.; Cotera, Angela S.] SETI Inst, Mountain View, CA 94043 USA. [Whitney, Barbara A.] Univ Wisconsin, Madison, WI 53706 USA. [Hines, Dean C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Schneider, Glenn] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Burton, Michael G.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Colgan, Sean W. J.; Erickson, Edwin F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Wolff, Michael J.] Space Sci Inst, Boulder, CO 80301 USA. RP Simpson, JP (reprint author), SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA. EM jsimpson@seti.org RI Colgan, Sean/M-4742-2014; OI Burton, Michael/0000-0001-7289-1998 FU NASA through Space Telescope Science Institute [10519]; NASA [NAS5-26555] FX We thank the referee for his careful comments, which greatly improved the presentation. Support for programme 10519 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, under NASA contract NAS5-26555. NR 104 TC 2 Z9 2 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 NOV PY 2013 VL 435 IS 4 BP 3419 EP 3436 DI 10.1093/mnras/stt1534 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 236DP UT WOS:000325774700052 ER PT J AU Hilton, M Hasselfield, M Sifon, C Baker, AJ Barrientos, LF Battaglia, N Bond, JR Crichton, D Das, S Devlin, MJ Gralla, M Hajian, A Hincks, AD Hughes, JP Infante, L Irwin, KD Kosowsky, A Lin, YT Marriage, TA Marsden, D Menanteau, F Moodley, K Niemack, MD Nolta, MR Page, LA Reese, ED Sievers, J Spergel, DN Wollack, EJ AF Hilton, Matt Hasselfield, Matthew Sifon, Cristobal Baker, Andrew J. Felipe Barrientos, L. Battaglia, Nicholas Bond, J. Richard Crichton, Devin Das, Sudeep Devlin, Mark J. Gralla, Megan Hajian, Amir Hincks, Adam D. Hughes, John P. Infante, Leopoldo Irwin, Kent D. Kosowsky, Arthur Lin, Yen-Ting Marriage, Tobias A. Marsden, Danica Menanteau, Felipe Moodley, Kavilan Niemack, Michael D. Nolta, Mike R. Page, Lyman A. Reese, Erik D. Sievers, Jon Spergel, David N. Wollack, Edward J. TI The Atacama Cosmology Telescope: the stellar content of galaxy clusters selected using the Sunyaev-Zel'dovich effect SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: general; galaxies: luminosity function; mass function; galaxies: stellar content; cosmology: observations ID INITIAL MASS FUNCTION; COLOR-MAGNITUDE RELATION; BAND LUMINOSITY FUNCTION; X-RAY-CLUSTERS; TO-LIGHT RATIO; POPULATION SYNTHESIS; PHYSICAL-PROPERTIES; SCALING RELATIONS; INTRACLUSTER LIGHT; ELLIPTIC GALAXIES AB We present a first measurement of the stellar mass component of galaxy clusters selected via the Sunyaev-Zel'dovich (SZ) effect, using 3.6 and 4.5 mu m photometry from the Spitzer Space Telescope. Our sample consists of 14 clusters detected by the Atacama Cosmology Telescope (ACT), which span the redshift range 0.27 < z < 1.07 (median z = 0.50) and have dynamical mass measurements, accurate to about 30 per cent, with median M-500 = 6.9 x 10(14) M-circle dot. We measure the 3.6 and 4.5 mu m galaxy luminosity functions, finding the characteristic magnitude (m*) and faint-end slope (alpha) to be similar to those for infrared-selected cluster samples. We perform the first measurements of the scaling of SZ observables (Y-500 and y(0)) with both brightest cluster galaxy (BCG) stellar mass and total cluster stellar mass (M-500(star)). We find a significant correlation between BCG stellar mass and Y-500 (E(z)(-2/3) D-A(2) Y-500 proportional to M-*(1.2 +/- 0.6)), although we are not able to obtain a strong constraint on the slope of the relation due to the small sample size. Additionally, we obtain E(z)(-2/3) D-A(2) Y-500 proportional to M-500(star) (1.0 +/- 0.6) for the scaling with total stellar mass. The mass fraction in stars spans the range 0.006-0.034, with the second ranked cluster in terms of dynamical mass (ACT-CL J0237-4939) having an unusually low total stellar mass and the lowest stellar mass fraction. For the five clusters with gas mass measurements available in the literature, we see no evidence for a shortfall of baryons relative to the cosmic mean value. C1 [Hilton, Matt] Univ Nottingham, Sch Phys & Astron, Ctr Astron & Particle Theory, Nottingham NG7 2RD, England. [Hilton, Matt; Moodley, Kavilan] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Hasselfield, Matthew] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. [Sifon, Cristobal] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Baker, Andrew J.; Hughes, John P.; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Felipe Barrientos, L.; Infante, Leopoldo] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile. [Battaglia, Nicholas] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Battaglia, Nicholas; Bond, J. Richard; Hajian, Amir; Hincks, Adam D.; Nolta, Mike R.; Sievers, Jon] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Crichton, Devin; Gralla, Megan; Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Das, Sudeep] Argonne Natl Lab, Lemont, IL 60439 USA. [Das, Sudeep] Univ Calif Berkeley, LBL, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Devlin, Mark J.; Reese, Erik D.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Irwin, Kent D.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA. [Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Lin, Yen-Ting] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Marsden, Danica] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Page, Lyman A.; Sievers, Jon] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hilton, M (reprint author), Univ Nottingham, Sch Phys & Astron, Ctr Astron & Particle Theory, Nottingham NG7 2RD, England. EM hiltonm@ukzn.ac.za RI Hilton, Matthew James/N-5860-2013; Wollack, Edward/D-4467-2012; OI Wollack, Edward/0000-0002-7567-4451; Menanteau, Felipe/0000-0002-1372-2534; Sievers, Jonathan/0000-0001-6903-5074; Sifon, Cristobal/0000-0002-8149-1352 FU NASA; Leverhulme trust; US National Science Foundation [AST-0408698, AST-0965625, PHY-0855887, PHY-1214379, AST-0955810]; Princeton University; University of Pennsylvania; Canada Foundation for Innovation (CFI); Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT); CFI under Compute Canada; Government of Ontario; Ontario Research Fund - Research Excellence; University of Toronto FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. MH acknowledges financial support from the Leverhulme trust. 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 award AST-0955810 to AJB. 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. NR 101 TC 5 Z9 5 U1 0 U2 3 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 NOV PY 2013 VL 435 IS 4 BP 3469 EP 3480 DI 10.1093/mnras/stt1535 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 236DP UT WOS:000325774700056 ER PT J AU Wakeford, HR Sing, DK Deming, D Gibson, NP Fortney, JJ Burrows, AS Ballester, G Nikolov, N Aigrain, S Henry, G Knutson, H des Etangs, AL Pont, F Showman, AP Vidal-Madjar, A Zahnle, K AF Wakeford, H. R. Sing, D. K. Deming, D. Gibson, N. P. Fortney, J. J. Burrows, A. S. Ballester, G. Nikolov, N. Aigrain, S. Henry, G. Knutson, H. des Etangs, A. Lecavelier Pont, F. Showman, A. P. Vidal-Madjar, A. Zahnle, K. TI HST hot Jupiter transmission spectral survey: detection of water in HAT-P-1b from WFC3 near-IR spatial scan observations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: spectroscopic; planets and satellites: atmospheres; planetary systems ID HUBBLE-SPACE-TELESCOPE; EXOPLANET HD 189733B; TRANSITING EXTRASOLAR PLANET; MASS DWARF STARS; TIME-SERIES PHOTOMETRY; GIANT PLANETS; BROWN DWARFS; ATMOSPHERIC CHEMISTRY; MODEL ATMOSPHERES; C/O RATIO AB We present Hubble Space Telescope near-infrared transmission spectroscopy of the transiting hot-Jupiter HAT-P-1b. We observed one transit with Wide Field Camera 3 using the G141 low-resolution grism to cover the wavelength range 1.087-1.678 mu m. These time series observations were taken with the newly available spatial-scan mode that increases the duty cycle by nearly a factor of 2, thus improving the resulting photometric precision of the data. We measure a planet-to-star radius ratio of R-p/R-* = 0.117 09 +/- 0.000 38 in the white light curve with the centre of transit occurring at 245 6114.345 +/- 0.000 133 (JD). We achieve S/N levels per exposure of 1840 (0.061 per cent) at a resolution of delta lambda = 19.2 nm (R similar to 70) in the 1.1173-1.6549 mu m spectral region, providing the precision necessary to probe the transmission spectrum of the planet at close to the resolution limit of the instrument. We compute the transmission spectrum using both single target and differential photometry with similar results. The resultant transmission spectrum shows a significant absorption above the 5 Sigma level matching the 1.4 mu m water absorption band. In solar composition models, the water absorption is sensitive to the similar to 1 m bar pressure levels at the terminator. The detected absorption agrees with that predicted by a 1000 K isothermal model, as well as with that predicted by a planetary-averaged temperature model. C1 [Wakeford, H. R.; Sing, D. K.; Nikolov, N.; Pont, F.] Univ Exeter, Sch Phys, Astrophys Grp, Exeter EX4 4QL, Devon, England. [Deming, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Gibson, N. P.] ESO, D-85748 Garching, Germany. [Fortney, J. J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Burrows, A. S.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Ballester, G.; Showman, A. P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Aigrain, S.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Henry, G.] Tennessee State Univ, Nashville, TN 37203 USA. [Knutson, H.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [des Etangs, A. Lecavelier; Vidal-Madjar, A.] Inst Astrophys, CNRS, F-75014 Paris, France. [Zahnle, K.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Wakeford, HR (reprint author), Univ Exeter, Sch Phys, Astrophys Grp, Stocker Rd, Exeter EX4 4QL, Devon, England. EM hannah@astro.ex.ac.uk RI Nikolov, Nikolay/H-6183-2015; OI Nikolov, Nikolay/0000-0002-6500-3574; Sing, David /0000-0001-6050-7645; Fortney, Jonathan/0000-0002-9843-4354; Wakeford, Hannah/0000-0003-4328-3867; Gibson, Neale/0000-0002-9308-2353 FU STFC; Space Telescope Science Institute [HST-GO-12473] FX HRW and DKS acknowledge support from STFC. All US-based co-authors acknowledge support from the Space Telescope Science Institute under HST-GO-12473 grants to their respective institutions. This work is based on observations with the NASA/ESA Hubble Space Telescope. This research has made use of NASAs Astrophysics Data System and components of the IDL astronomy library. We thank the referee for their useful comments. NR 59 TC 33 Z9 33 U1 3 U2 7 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 NOV PY 2013 VL 435 IS 4 BP 3481 EP 3493 DI 10.1093/mnras/stt1536 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 236DP UT WOS:000325774700057 ER PT J AU Ines, AVM Das, NN Hansen, JW Njoku, EG AF Ines, Amor V. M. Das, Narendra N. Hansen, James W. Njoku, Eni G. TI Assimilation of remotely sensed soil moisture and vegetation with a crop simulation model for maize yield prediction SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Yield forecasting; Crop model; Data assimilation; Soil moisture; Leaf area index ID ENSEMBLE KALMAN FILTER; AMSR-E; GRAIN-YIELD; FORECASTS; INDEX; MANAGEMENT AB To improve the prediction of crop yields at an aggregate scale, we developed a data assimilation-crop modeling framework that incorporates remotely sensed soil moisture and leaf area index (LAI) into a crop model using sequential data assimilation. The core of the framework is an Ensemble Kalman Filter (EnKF) used to control crop model runs, assimilate remote sensing (RS) data and update model state variables. We modified the Decision Support System for Agro-technology Transfer - Cropping System Model (DSSAT-CSM)-Maize model (Jones et al., 2003) to be able to stop and start simulations at any given time in the growing season, such that the EnKF can update model state variables as RS data become available. The data assimilation-crop modeling framework was evaluated against 2003-2009 maize yields in Story County, Iowa, USA, assimilating AMSR-E soil moisture and MODIS-LAI data independently and simultaneously. Assimilating LAI or soil moisture independently slightly improved the correlation of observed and simulated yields (R = 0.51 and 0.50) compared to no data assimilation (open-loop; R = 0.47) but prediction errors improved with reductions in MBE and RMSE by 0.5 and 0.5 Mg ha(-1) respectively for LAI assimilation while these were reduced by 1.8 and 1.1 Mg ha(-1) for soil moisture assimilation. Yield correlation improved more when both soil moisture and LAI were assimilated (R = 0.65) suggesting a cause-effect interaction between soil moisture and LAI, prediction errors (MBE and RMSE) were also reduced by 1.7 and 1.8 Mg ha(-1) with respect to open-loop simulations. Results suggest that assimilation of LAI independently might be preferable when conditions are extremely wet while assimilation of soil moisture + LAI might be more suitable when conditions are more nominal. AMSR-E soil moisture tends to be more biased under the presence of high vegetation (i.e., when crops are fully developed) and that updating rootzone soil moisture by near-surface soil moisture assimilation under very wet conditions could increase the modeled percolation causing excessive nitrogen (N) leaching hence reducing crop yields even with water stress reduced at a minimum due to soil moisture assimilation. However, applying the data assimilation-crop modeling framework strategically by considering a-priori information on climate condition expected during the growing season may improve yield prediction performance substantially, in our case with higher correlation (R = 0.80) and more reductions in MBE and RMSE (2.5 and 3.3 Mg ha(-1)) compared to when there is no data assimilation. Scaling AMSR-E soil moisture to the climatology of the model did not improve our data assimilation results because the model is also biased. Better soil moisture products e.g., from Soil Moisture Active Passive (SMAP) mission, may solve the soil moisture data issue in the near future. (C) 2013 The Authors. Published by Elsevier Inc. All rights reserved. C1 [Ines, Amor V. M.; Hansen, James W.] Columbia Univ, Earth Inst, Int Res Inst Climate & Soc, Palisades, NY 10964 USA. [Das, Narendra N.; Njoku, Eni G.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ines, AVM (reprint author), Columbia Univ, Earth Inst, Int Res Inst Climate & Soc, 61 Route 9W, Palisades, NY 10964 USA. EM ines@iri.columbia.edu RI Hansen, James/M-1449-2015 OI Hansen, James/0000-0002-8599-7895 FU CGIAR Research Program on Climate Change, Agriculture and Food Security (CCAFS); European Union; United States Agency for International Development (USAID); Canadian International Development Agency (CIDA); New Zealand Ministry of Foreign Affairs and Trade; Danish International Development Agency (DANIDA); UK Department for International Development (DfID); Irish Aid; Instituto de Investigacao Cientifica Tropical, Portugal (IICT) FX This work was done with the support of the CGIAR Research Program on Climate Change, Agriculture and Food Security (CCAFS) with the financial assistance of the European Union, the United States Agency for International Development (USAID), Canadian International Development Agency (CIDA), New Zealand Ministry of Foreign Affairs and Trade, the Danish International Development Agency (DANIDA), the UK Department for International Development (DfID), Irish Aid, and Instituto de Investigacao Cientifica Tropical, Portugal (IICT) with technical support from IFAD. The views expressed in this document cannot be taken to reflect the official opinions of these agencies, nor the official position of the CGIAR. NR 41 TC 37 Z9 41 U1 10 U2 83 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 NOV PY 2013 VL 138 BP 149 EP 164 DI 10.1016/j.rse.2013.07.018 PG 16 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 249HC UT WOS:000326767300014 ER PT J AU Dlugach, ZM Mishchenko, MI AF Dlugach, Zh M. Mishchenko, M. I. TI Coherent backscattering and opposition effects observed in some atmosphereless bodies of the solar system SO SOLAR SYSTEM RESEARCH LA English DT Article ID SATURNS RINGS; WEAK-LOCALIZATION; ELECTROMAGNETIC-WAVES; MULTIPLE-SCATTERING; LIGHT-SCATTERING; T-MATRIX; POLARIZATION; OBJECTS; MEDIA; POLARIMETRY AB The results of photometric and polarimetric observations carried out for some bright atmosphere-less bodies of the Solar system near the zero phase angle reveal the simultaneous existence of two spectacular optical phenomena, the so-called brightness and polarization opposition effects. In a number of studies, these phenomena were explained by the influence of coherent backscattering. However, in general, the interference concept of coherent backscattering can be used only in the case where the particles are in the far-field zones of each other, i.e., when the scattering medium is rather rarefied. Because of this, it is important to prove rigorously and to demonstrate that the coherent backscattering effect may also exist in densely packed scattering media like regolith surface layers of celestial bodies. From the results of the computer modeling performed with the use of numerically exact solutions of the macroscopic Maxwell equations for discrete random media with different packing densities of particles, we studied the origin and evolution of all the opposition phenomena predicted by the coherent backscattering theory for low-packing-density media. It has been shown that the predictions of this theory remain valid for rather high packing densities of particles that are typical, in particular, of regolith surfaces of the Solar system bodies. The results allow us to conclude that both opposition effects observed simultaneously in some high-albedo atmosphereless bodies of the Solar system are caused precisely by coherent backscattering of solar light in the regolith layers composed of microscopic particles. C1 [Dlugach, Zh M.] Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine. [Mishchenko, M. I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Dlugach, ZM (reprint author), Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine. RI Mishchenko, Michael/D-4426-2012 FU National Academy of Sciences of Ukraine FX The work was supported by the National Academy of Sciences of Ukraine under the Main Astronomical Observatory GRAPE/GPU/GRID computing cluster project. The authors are grateful to the referee for a valuable comment. NR 42 TC 6 Z9 6 U1 0 U2 7 PU MAIK NAUKA/INTERPERIODICA/SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA SN 0038-0946 EI 1608-3423 J9 SOLAR SYST RES+ JI Solar Syst. Res. PD NOV PY 2013 VL 47 IS 6 BP 454 EP 462 DI 10.1134/S0038094613060014 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 248WF UT WOS:000326735600005 ER PT J AU Churchill, AM Lovell, DJ Mukherjee, A Ball, MO AF Churchill, Andrew M. Lovell, David J. Mukherjee, Avijit Ball, Michael O. TI Determining the Number of Airport Arrival Slots SO TRANSPORTATION SCIENCE LA English DT Article DE air traffic management; integer programming; airport slots; stochastic programming AB At many congested airports, access rights are governed by a system of slot controls. A slot conveys to its owner the right to schedule an operation (flight arrival or departure). In this paper, stochastic optimization models are developed to determine the numbers, of slots to make available over the course of a day, controlling for the long-term uncertainty induced in arrival or departure capacities because of weather conditions. Three related integer programming formulations for this problem are presented, which vary both in their computational properties and the economic trade-offs modeled. The models are compared both analytically and computationally. Experiments using data from New York's LaGaurdia Airport are reported to demonstrate the impact of these models on optimizing slot profiles while considering long-term capacity uncertainty and several policy objectives. C1 [Churchill, Andrew M.] Mosaic ATM Inc, Leesburg, VA 20175 USA. [Lovell, David J.] Univ Maryland, Dept Civil & Environm Engn, College Pk, MD 20742 USA. [Lovell, David J.; Ball, Michael O.] Univ Maryland, Syst Res Inst, College Pk, MD 20742 USA. [Mukherjee, Avijit] Univ Calif Santa Cruz, NASA Ames Res Ctr, Moffett Field, CA 94035 USA. [Ball, Michael O.] Univ Maryland, Robert H Smith Sch Business, College Pk, MD 20742 USA. RP Churchill, AM (reprint author), Mosaic ATM Inc, Leesburg, VA 20175 USA. EM achurchill@mosaicatm.com; lovell@umd.edu; avijit@ucsc.edu; mball@rhsmith.umd.edu FU National Center of Excellence for Aviation Operations Research under Federal Aviation Administration research [96-C-001, DFTA03-97-D00004] FX This work was supported by the National Center of Excellence for Aviation Operations Research, under Federal Aviation Administration research [Grant 96-C-001] and [Contract DFTA03-97-D00004]. Any opinions expressed herein do not necessarily reflect those of the Federal Aviation Administration or the Department of Transportation. NR 32 TC 2 Z9 2 U1 4 U2 14 PU INFORMS PI CATONSVILLE PA 5521 RESEARCH PARK DR, SUITE 200, CATONSVILLE, MD 21228 USA SN 0041-1655 J9 TRANSPORT SCI JI Transp. Sci. PD NOV PY 2013 VL 47 IS 4 BP 526 EP 541 DI 10.1287/trsc.1120.0438 PG 16 WC Operations Research & Management Science; Transportation; Transportation Science & Technology SC Operations Research & Management Science; Transportation GA 250JV UT WOS:000326850000005 ER PT J AU Romano, P Mangano, V Ducci, L Esposito, P Vercellone, S Bocchino, F Burrows, DN Kennea, JA Krimm, HA Gehrels, N Farinelli, R Ceccobello, C AF Romano, P. Mangano, V. Ducci, L. Esposito, P. Vercellone, S. Bocchino, F. Burrows, D. N. Kennea, J. A. Krimm, H. A. Gehrels, N. Farinelli, R. Ceccobello, C. TI The Swift Supergiant Fast X-ray Transients Project: A review, new results and future perspectives SO ADVANCES IN SPACE RESEARCH LA English DT Article DE X-rays:binaries; X-rays: individual ID XMM-NEWTON OBSERVATIONS; IGR J08408-4503; NEUTRON-STAR; INTEGRAL OBSERVATIONS; XTE J1739-302; SKY MONITOR; OUTBURST; BINARIES; TELESCOPE; CATALOG AB We present a review of the Supergiant Fast X-ray Transients (SFXT) Project, a systematic investigation of the properties of SFXTs with a strategy that combines Swift monitoring programs with outburst follow-up observations. This strategy has quickly tripled the available sets of broad-band data of SFXT outbursts, and gathered a wealth of out-of-outburst data, which have led us to a broad-band spectral characterization, an assessment of the fraction of the time these sources spend in each phase, and their duty cycle of inactivity. We present some new observational results obtained through our outburst follow-ups, as fitting examples of the exceptional capabilities of Swift in catching bright flares and monitor them panchromatically. (C) 2013 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Romano, P.; Mangano, V.; Vercellone, S.] INAF IASF Palermo, I-90146 Palermo, Italy. [Ducci, L.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Esposito, P.] INAF IASF Milano, I-20133 Milan, Italy. [Bocchino, F.] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Burrows, D. N.; Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Krimm, H. A.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Farinelli, R.; Ceccobello, C.] Univ Ferrara, Dept Phys, I-44122 Ferrara, Italy. RP Romano, P (reprint author), INAF IASF Palermo, Via U La Malfa 153, I-90146 Palermo, Italy. EM romano@ifc.inaf.it OI Bocchino, Fabrizio/0000-0002-2321-5616; Vercellone, Stefano/0000-0003-1163-1396; Esposito, Paolo/0000-0003-4849-5092 FU ASI-INAF [1/009/10/0, 1/004/11/0] FX We thank the Swift team duty scientists and science planners and the remainder of the Swift XRT and BAT teams, S. Barthelmy in particular, for their invaluable help and support. We also thank D. Grupe and M.M. Chester for helpful discussions. We also thank the anonymous referees for their insightful comments. We acknowledge financial contribution from the agreement ASI-INAF 1/009/10/0 and from contract ASI-INAF 1/004/11/0. This work made use of the results of the Swift/BAT hard X-ray transient monitor: http://swift.gsfc.nasa.gov/docs/swift/results/transients/ and of data supplied by the UK Swift Science Data Centre at the University of Leicester. NR 58 TC 9 Z9 9 U1 0 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 NOV 1 PY 2013 VL 52 IS 9 BP 1593 EP 1601 DI 10.1016/j.asr.2013.07.034 PG 9 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 244UH UT WOS:000326415200002 ER PT J AU Grimm, NB Chapin, FS Bierwagen, B Gonzalez, P Groffman, PM Luo, YQ Melton, F Nadelhoffer, K Pairis, A Raymond, PA Schimel, J Williamson, CE AF Grimm, Nancy B. Chapin, F. Stuart, III Bierwagen, Britta Gonzalez, Patrick Groffman, Peter M. Luo, Yiqi Melton, Forrest Nadelhoffer, Knute Pairis, Amber Raymond, Peter A. Schimel, Josh Williamson, Craig E. TI The impacts of climate change on ecosystem structure and function SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT LA English DT Article ID NORTH-AMERICA; UNITED-STATES; TEMPERATE STEPPE; COLORADO RIVER; GLOBAL-CHANGE; VEGETATION; RADIATION; INCREASE; DYNAMICS; SYSTEM AB Recent climate-change research largely confirms the impacts on US ecosystems identified in the 2009 National Climate Assessment and provides greater mechanistic understanding and geographic specificity for those impacts. Pervasive climate-change impacts on ecosystems are those that affect productivity of ecosystems or their ability to process chemical elements. Loss of sea ice, rapid warming, and higher organic inputs affect marine and lake productivity, while combined impacts of wildfire and insect outbreaks decrease forest productivity, mostly in the arid and semi-arid West. Forests in wetter regions are more productive owing to warming. Shifts in species ranges are so extensive that by 2100 they may alter biome composition across 5-20% of US land area. Accelerated losses of nutrients from terrestrial ecosystems to receiving waters are caused by both winter warming and intensification of the hydrologic cycle. Ecosystem feedbacks, especially those associated with release of carbon dioxide and methane release from wetlands and thawing permafrost soils, magnify the rate of climate change. C1 [Grimm, Nancy B.] Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. [Chapin, F. Stuart, III] Univ Alaska Fairbanks, Inst Arctic Biol, Fairbanks, AK USA. [Bierwagen, Britta] US EPA, Global Change Impacts & Assessment Grp, Off Res & Dev, Washington, DC 20460 USA. [Gonzalez, Patrick] Natl Pk Serv, Nat Resource Stewardship & Sci, Washington, DC USA. [Groffman, Peter M.] Cary Inst Ecosyst Studies, Millbrook, NY USA. [Luo, Yiqi] Univ Oklahoma, Dept Microbiol & Plant Biol, Norman, OK 73019 USA. [Melton, Forrest] NASA, Ames Res Ctr, Cooperat Res Earth Sci & Technol, Moffett Field, CA 94035 USA. [Nadelhoffer, Knute] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Pairis, Amber] Calif Dept Fish & Game, San Diego, CA USA. [Raymond, Peter A.] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. [Schimel, Josh] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. [Williamson, Craig E.] Miami Univ, Dept Zool, Oxford, OH 45056 USA. RP Grimm, NB (reprint author), Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. EM nbgrimm@asu.edu RI Raymond, Peter/C-4087-2009; Gonzalez, Patrick/B-9479-2013; Grimm, Nancy/D-2840-2009; OI Raymond, Peter/0000-0002-8564-7860; Gonzalez, Patrick/0000-0002-7105-0561; Grimm, Nancy/0000-0001-9374-660X; Chapin III, F Stuart/0000-0002-2558-9910 FU Gordon and Betty Moore Foundation; US Geological Survey; NASA FX This work resulted from an assessment workshop held in 2012. We thank the Gordon and Betty Moore Foundation, which provided a venue for the workshop and funding for this publication; the US Geological Survey, which provided funding for the workshop, the BEES report, and this issue; and NASA for helping fund this publication. We also thank M Bernstein, who contributed to the writing of the technical report upon which this paper is based. This paper was partially based on work performed while NBG and BB were working at the US National Science Foundation (NSF) and the US Environmental Protection Agency (EPA), respectively. Any opinions, findings, and conclusions expressed here are those of the authors and do not necessarily reflect the views of the NSF or the EPA. NR 59 TC 57 Z9 60 U1 17 U2 252 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1540-9295 EI 1540-9309 J9 FRONT ECOL ENVIRON JI Front. Ecol. Environ. PD NOV PY 2013 VL 11 IS 9 BP 474 EP 482 DI 10.1890/120282 PG 9 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 244CE UT WOS:000326363900004 ER PT J AU Nelson, EJ Kareiva, P Ruckelshaus, M Arkema, K Geller, G Girvetz, E Goodrich, D Matzek, V Pinsky, M Reid, W Saunders, M Semmens, D Tallis, H AF Nelson, Erik J. Kareiva, Peter Ruckelshaus, Mary Arkema, Katie Geller, Gary Girvetz, Evan Goodrich, Dave Matzek, Virginia Pinsky, Malin Reid, Walt Saunders, Martin Semmens, Darius Tallis, Heather TI Climate change's impact on key ecosystem services and the human well-being they support in the US SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT LA English DT Article ID SEA-LEVEL RISE; CALIFORNIA; DISPERSAL; FISHERIES; BENEFITS; OCEAN; TEMPERATURE; SNOWPACK; MARINE; YIELDS AB Climate change alters the functions of ecological systems. As a result, the provision of ecosystem services and the well-being of people that rely on these services are being modified. Climate models portend continued warming and more frequent extreme weather events across the US. Such weather-related disturbances will place a premium on the ecosystem services that people rely on. We discuss some of the observed and anticipated impacts of climate change on ecosystem service provision and livelihoods in the US. We also highlight promising adaptive measures. The challenge will be choosing which adaptive strategies to implement, given limited resources and time. We suggest using dynamic balance sheets or accounts of natural capital and natural assets to prioritize and evaluate national and regional adaptation strategies that involve ecosystem services. C1 [Nelson, Erik J.] Bowdoin Coll, Dept Econ, Brunswick, ME 04011 USA. [Kareiva, Peter; Girvetz, Evan] Nature Conservancy, Seattle, WA USA. [Ruckelshaus, Mary; Arkema, Katie; Tallis, Heather] Stanford Univ, Nat Capital Project, Dept Biol, Stanford, CA 94305 USA. [Ruckelshaus, Mary; Arkema, Katie; Tallis, Heather] Stanford Univ, Woods Inst Environm, Stanford, CA 94305 USA. [Ruckelshaus, Mary; Arkema, Katie; Girvetz, Evan] Univ Washington, Sch Environm & Forest Sci, Seattle, WA 98195 USA. [Geller, Gary] NASA, Ecol Forecasting Program, CALTECH, Jet Prop Lab, Pasadena, CA USA. [Goodrich, Dave] USDA ARS, Southwest Watershed Res Ctr, Tucson, AZ USA. [Matzek, Virginia; Saunders, Martin] Santa Clara Univ, Dept Environm Studies & Sci, Santa Clara, CA 95053 USA. [Pinsky, Malin] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Reid, Walt] David & Lucile Packard Fdn, Los Altos, CA USA. [Semmens, Darius] US Geol Survey, Geosci & Environm Change Sci Ctr, Denver, CO 80225 USA. RP Nelson, EJ (reprint author), Bowdoin Coll, Dept Econ, Brunswick, ME 04011 USA. EM enelson2@bowdoin.edu RI Pinsky, Malin/K-2884-2015; OI Pinsky, Malin/0000-0002-8523-8952; Geller, Gary/0000-0002-4490-6002 FU David H Smith Conservation Research Fellowship FX Part of the research described in this article was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. MLP's participation was supported by a David H Smith Conservation Research Fellowship. Any use of trade, firm, or product names is for descriptive purposes only and does not imply endorsement by the US Government. NR 69 TC 20 Z9 23 U1 7 U2 116 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1540-9295 EI 1540-9309 J9 FRONT ECOL ENVIRON JI Front. Ecol. Environ. PD NOV PY 2013 VL 11 IS 9 BP 483 EP 493 DI 10.1890/120312 PG 11 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 244CE UT WOS:000326363900005 ER PT J AU Staudt, A Leidner, AK Howard, J Brauman, KA Dukes, JS Hansen, LJ Paukert, C Sabo, J Solorzano, LA AF Staudt, Amanda Leidner, Allison K. Howard, Jennifer Brauman, Kate A. Dukes, Jeffrey S. Hansen, Lara J. Paukert, Craig Sabo, John Solorzano, Luis A. TI The added complications of climate change: understanding and managing biodiversity and ecosystems SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT LA English DT Article ID BUTTERFLY DIVERSITY; MELTING GLACIERS; GLOBAL CHANGE; LAND-USE; IMPACTS; TEMPERATURE; METAANALYSIS; IRRIGATION; SCENARIOS; DRIVERS AB Ecosystems around the world are already threatened by land-use and land-cover change, extraction of natural resources, biological disturbances, and pollution. These environmental stressors have been the primary source of ecosystem degradation to date, and climate change is now exacerbating some of their effects. Ecosystems already under stress are likely to have more rapid and acute reactions to climate change; it is therefore useful to understand how multiple stresses will interact, especially as the magnitude of climate change increases. Understanding these interactions could be critically important in the design of climate adaptation strategies, especially because actions taken by other sectors (eg energy, agriculture, transportation) to address climate change may create new ecosystem stresses. C1 [Staudt, Amanda] Natl Wildlife Federat, Reston, VA USA. [Leidner, Allison K.] NASA Headquarters, Div Earth Sci, Washington, DC USA. [Howard, Jennifer] NOAA, Silver Spring, MD USA. [Brauman, Kate A.] Univ Minnesota, Inst Environm, St Paul, MN 55108 USA. [Dukes, Jeffrey S.] Purdue Univ, Dept Forestry & Nat Resources, W Lafayette, IN 47907 USA. [Dukes, Jeffrey S.] Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA. [Hansen, Lara J.] EcoAdapt, Bainbridge Island, WA USA. [Paukert, Craig] Univ Missouri, USGS, Missouri Cooperat Fish & Wildlife Res Unit, Columbia, MO USA. [Sabo, John] Arizona State Univ, Tempe, AZ USA. [Solorzano, Luis A.] Gordon & Betty Moore Fdn, Palo Alto, CA USA. RP Staudt, A (reprint author), Natl Acad, Washington, DC USA. EM astaudt@nas.edu RI Dukes, Jeffrey/C-9765-2009; OI Dukes, Jeffrey/0000-0001-9482-7743; Brauman, Kate/0000-0002-8099-285X FU Missouri Department of Conservation; University of Missouri; USGS; US Fish and Wildlife Service; Wildlife Management Institute FX We thank K Johnson, J Riddell, and D Allen for helpful input to earlier versions of this manuscript. We acknowledge the US Geological Survey (USGS), the Gordon and Betty Moore Foundation, and the University of Missouri for supporting the workgroup meetings. The Missouri Cooperative Fish and Wildlife Research Unit is jointly sponsored by the Missouri Department of Conservation, the University of Missouri, the USGS, the US Fish and Wildlife Service, and the Wildlife Management Institute. NR 53 TC 37 Z9 37 U1 9 U2 72 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1540-9295 EI 1540-9309 J9 FRONT ECOL ENVIRON JI Front. Ecol. Environ. PD NOV PY 2013 VL 11 IS 9 BP 494 EP 501 DI 10.1890/120275 PG 8 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 244CE UT WOS:000326363900006 ER PT J AU Lee, H Mudawar, I Hasan, MM AF Lee, Hyoungsoon Mudawar, Issam Hasan, Mohammad M. TI Flow condensation in horizontal tubes SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER LA English DT Article DE Condensation; Horizontal flow; Interfacial waves ID CRITICAL HEAT-FLUX; FALLING LIQUID-FILMS; PARALLEL MICRO-CHANNELS; PRESSURE-DROP; TRANSFER COEFFICIENT; MOMENTUM TRANSPORT; UNIVERSAL APPROACH; COOLING SCHEME; JET; MICROGRAVITY AB This study examines condensation heat transfer in horizontal channels. Two separate condensation modules are tested using FC-72 as condensing fluid and water as coolant. The first module is dedicated to obtaining detailed heat transfer measurements of the condensing flow, and the second to video capture of the condensation film's interfacial behavior. Four dominant flow regimes are identified: smooth-annular, wavy-annular, stratified-wavy and stratified, whose boundaries show fair agreement with published flow regime maps. The film's interface is observed to feature an array of small ripples and relatively large waves, with the largest waves tending to merge into yet larger waves having greater liquid mass, amplitude and speed. This behavior is believed to influence condensation heat transfer, especially downstream. The local condensation heat transfer coefficient is highest near the inlet, where quality is near unity and the film thinnest, and decreases monotonically in the axial direction in response to the film thickening. This variation is very sensitive to the mass velocity of FC-72, and the heat transfer coefficient decreases sharply in the inlet region but this decrease slows significantly in the downstream region because of the combined effects of turbulence and interfacial waviness. The measured condensation heat transfer coefficient shows good agreement with a select number of correlations. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Lee, Hyoungsoon; Mudawar, Issam] Purdue Univ, Sch Mech Engn, BTPFL, W Lafayette, IN 47907 USA. [Hasan, Mohammad M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Mudawar, I (reprint author), Purdue Univ, Sch Mech Engn, BTPFL, 585 Purdue Mall, W Lafayette, IN 47907 USA. EM mudawar@ecn.purdue.edu FU National Aeronautics and Space Administration (NASA) [NNX13AB01G] FX The authors are grateful for the support of the National Aeronautics and Space Administration (NASA) under grant no. NNX13AB01G. NR 51 TC 9 Z9 9 U1 3 U2 26 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0017-9310 EI 1879-2189 J9 INT J HEAT MASS TRAN JI Int. J. Heat Mass Transf. PD NOV PY 2013 VL 66 BP 31 EP 45 DI 10.1016/j.ijheatmasstransfer.2013.06.044 PG 15 WC Thermodynamics; Engineering, Mechanical; Mechanics SC Thermodynamics; Engineering; Mechanics GA 242BF UT WOS:000326211700004 ER PT J AU D'Ambra, I Graham, WM Carmichael, RH Malej, A Onofri, V AF D'Ambra, Isabella Graham, William M. Carmichael, Ruth H. Malej, Alenka Onofri, Vladimir TI Predation patterns and prey quality of medusae in a semi-enclosed marine lake: implications for food web energy transfer in coastal marine ecosystems SO JOURNAL OF PLANKTON RESEARCH LA English DT Article DE gut content; stable isotope; SIAR; daily ration; Aurelia sp; jellyfish ID JELLYFISH AURELIA-AURITA; STABLE-ISOTOPE ANALYSES; POPULATION-DYNAMICS; ADRIATIC SEA; SP SCYPHOZOA; KIEL-BIGHT; SCYPHOMEDUSAE; ZOOPLANKTON; DIGESTION; CARBON AB Veliko Jezero (Mljet, Croatia) is a nearly enclosed karstic depression filled with saltwater, where jellyfish and prey exchange with the Adriatic Sea is negligible, making this small ecosystem ideal for the controlled study of medusae in food webs. Based on the analysis of their gut contents, medusae appeared to ingest less carbon than expected on the basis of their carbon content. To accurately define carbon ingestion by medusae, we determined the diet of Aurelia sp. 5 ( Dawson and Jacobs, 2001) (Scyphozoa: Semaeostomeae) from Veliko Jezero by combining gut content and stable isotope analyses. During daytime, gut contents identified a mix of small copepods as the dominant prey (62). In contrast, feeding models based on stable isotope values of medusae and their potential prey analyzed using Stable Isotope Analysis in R indicated appendicularians could have made the greatest contribution to Aurelia sp. 5 diet (1478), followed by calanoid copepods (050) and fish larvae (043). Because appendicularians and fish larvae are abundant with medusae at night near the bottom of the lake and contain more carbon than small copepods, we suggest diel movements of Aurelia sp. 5 and carbon content of prey determine the carbon assimilated by medusae, with night-time prey making a greater contribution to medusa diet than daytime prey. These data suggest medusae assimilate more carbon than previously estimated and suggest that jellyfish play an important role mediating carbon transfer in coastal food webs. C1 [D'Ambra, Isabella; Carmichael, Ruth H.] Dauphin Isl Sea Lab, Dauphin Isl, AL 36528 USA. [D'Ambra, Isabella; Carmichael, Ruth H.] Univ S Alabama, Dept Marine Sci, Mobile, AL 36668 USA. [Graham, William M.] Univ So Mississippi, Dept Marine Sci, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. [Malej, Alenka] Natl Inst Biol, Marine Biol Stn Piran, Forance 416330, Slovenia. [Onofri, Vladimir] Univ Dubrovnik, Inst Marine & Coastal Res, Dubrovnik 20000, Croatia. RP D'Ambra, I (reprint author), Via Santa Maria Cubito 687, I-80145 Naples, Italy. EM mikidambra@hotmail.com FU National Oceanographic and Atmospheric Agency-R.C. Shelby Center for Ecosystem-Based Fisheries Management FX This work was supported by the National Oceanographic and Atmospheric Agency-R.C. Shelby Center for Ecosystem-Based Fisheries Management to W.M.G. NR 41 TC 5 Z9 5 U1 1 U2 28 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0142-7873 EI 1464-3774 J9 J PLANKTON RES JI J. Plankton Res. PD NOV-DEC PY 2013 VL 35 IS 6 BP 1305 EP 1312 DI 10.1093/plankt/fbt065 PG 8 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 244IQ UT WOS:000326381800010 ER PT J AU Rothman, LS Gordon, IE Babikov, Y Barbe, A Benner, DC Bernath, PF Birk, M Bizzocchi, L Boudon, V Brown, LR Campargue, A Chance, K Cohen, EA Coudert, LH Devi, VM Drouin, BJ Fayt, A Flaud, JM Gamache, RR Harrison, JJ Hartmann, JM Hill, C Hodges, JT Jacquemart, D Jolly, A Lamouroux, J Le Roy, RJ Li, G Long, DA Lyulin, OM Mackie, CJ Massie, ST Mikhailenko, S Muller, HSP Naumenko, OV Nikitin, AV Orphal, J Perevalov, V Perrin, A Polovtseva, ER Richard, C Smith, MAH Starikova, E Sung, K Tashkun, S Tennyson, J Toon, GC Tyuterev, VG Wagner, G AF Rothman, L. S. Gordon, I. E. Babikov, Y. Barbe, A. Benner, D. Chris Bernath, P. F. Birk, M. Bizzocchi, L. Boudon, V. Brown, L. R. Campargue, A. Chance, K. Cohen, E. A. Coudert, L. H. Devi, V. M. Drouin, B. J. Fayt, A. Flaud, J. -M. Gamache, R. R. Harrison, J. J. Hartmann, J. -M. Hill, C. Hodges, J. T. Jacquemart, D. Jolly, A. Lamouroux, J. Le Roy, R. J. Li, G. Long, D. A. Lyulin, O. M. Mackie, C. J. Massie, S. T. Mikhailenko, S. Mueller, H. S. P. Naumenko, O. V. Nikitin, A. V. Orphal, J. Perevalov, V. Perrin, A. Polovtseva, E. R. Richard, C. Smith, M. A. H. Starikova, E. Sung, K. Tashkun, S. Tennyson, J. Toon, G. C. Tyuterev, Vl. G. Wagner, G. TI The HITRAN2012 molecular spectroscopic database SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE HITRAN; Spectroscopic database; Molecular spectroscopy; Molecular absorption; Spectroscopic line parameters; Absorption cross-sections; Aerosols ID MU-M REGION; ABSORPTION CROSS-SECTIONS; CW-CAVITY RING; COMPLEX REFRACTIVE-INDEXES; SPECTRAL-LINE PARAMETERS; O-2 A-BAND; INCLUDING TEMPERATURE DEPENDENCES; ELECTRIC QUADRUPOLE TRANSITIONS; ROTATIONAL-VIBRATIONAL SPECTRA; SUBMILLIMETER-WAVE SPECTRUM AB This paper describes the status of the 2012 edition of the HITRAN molecular spectroscopic compilation. The new edition replaces the previous HITRAN edition of 2008 and its updates during the intervening years. The HITRAN molecular absorption compilation is comprised of six major components structured into folders that are freely accessible on the internet. These folders consist of the traditional line-by-line spectroscopic parameters required for high-resolution radiative-transfer codes, infrared absorption cross-sections for molecules not yet amenable to representation in a line-by-line form, ultraviolet spectroscopic parameters, aerosol indices of refraction, collision-induced absorption data, and general tables such as partition sums that apply globally to the data. The new HITRAN is greatly extended in terms of accuracy, spectral coverage, additional absorption phenomena, and validity. Molecules and isotopologues have been added that address the issues of atmospheres beyond the Earth. Also discussed is a new initiative that casts HITRAN into a relational database format that offers many advantages over the long-standing sequential text-based structure that has existed since the initial release of HITRAN in the early 1970s. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Rothman, L. S.; Gordon, I. E.; Chance, K.; Li, G.; Mackie, C. J.; Richard, C.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Babikov, Y.; Lyulin, O. M.; Mikhailenko, S.; Naumenko, O. V.; Nikitin, A. V.; Perevalov, V.; Polovtseva, E. R.; Starikova, E.; Tashkun, S.] VE Zuev Inst Atmospher Opt SB RAS, Tomsk 634021, Russia. [Barbe, A.; Tyuterev, Vl. G.] Univ Reims, Grp Spectrometrie Mol & Atmospher, F-51062 Reims, France. [Benner, D. Chris; Devi, V. M.] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. [Bernath, P. F.] Old Dominion Univ, Dept Chem & Biochem, Norfolk, VA 23529 USA. [Birk, M.; Wagner, G.] DLR, Remote Sensing Technol Inst, D-82234 Wessling, Germany. [Bizzocchi, L.] Observ Astron Lisboa, CAAUL, Lisbon, Portugal. [Boudon, V.] Univ Bourgogne, CNRS, UMR 6303, Lab Interdisciplinaire Carnot Bourgogne, F-21078 Dijon, France. [Brown, L. R.; Cohen, E. A.; Drouin, B. J.; Sung, K.; Toon, G. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Campargue, A.] Univ Grenoble 1, CNRS, LIPhy UMR5588, F-38402 St Martin Dheres, France. [Coudert, L. H.; Flaud, J. -M.; Hartmann, J. -M.; Jolly, A.; Lamouroux, J.; Perrin, A.] Hop Henri Mondor, CNRS, F-94010 Creteil, France. [Coudert, L. H.; Flaud, J. -M.; Hartmann, J. -M.; Jolly, A.; Lamouroux, J.; Perrin, A.] Univ Paris 07, Lab Interuniv Syst Atmospher, F-94010 Creteil, France. [Fayt, A.] Catholic Univ Louvain, Lab Spect Mol, B-1348 Louvain, Belgium. [Gamache, R. R.; Lamouroux, J.] Univ Mass Lowell, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. [Harrison, J. J.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. [Hill, C.; Tennyson, J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Hodges, J. T.; Long, D. A.] NIST, Gaithersburg, MD 20899 USA. [Jacquemart, D.] Univ Paris 06, UMR 7075, Lab Dynam Interact & React, F-75252 Paris, France. [Le Roy, R. J.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. [Massie, S. T.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Mueller, H. S. P.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Orphal, J.] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-76344 Eggenstein Leopoldshafen, Germany. [Smith, M. A. H.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM LSR_JQSRT@verizon.net RI Tennyson, Jonathan/I-2222-2012; Bernath, Peter/B-6567-2012; BOUDON, Vincent/A-4504-2010; Orphal, Johannes/A-8667-2012; Starikova, Evgeniya/E-8680-2014; Nikitin, Andrei/K-2624-2013; Tashkun, Sergey/E-8682-2014; Babikov, Yurii/E-8686-2014; Li, Gang/P-2272-2015; Harrison, Jeremy/L-1073-2016; Sung, Keeyoon/I-6533-2015; OI Tennyson, Jonathan/0000-0002-4994-5238; Bernath, Peter/0000-0002-1255-396X; Orphal, Johannes/0000-0002-1943-4496; Nikitin, Andrei/0000-0002-4280-4096; Li, Gang/0000-0002-5605-7896; Harrison, Jeremy/0000-0001-5530-7104; Bizzocchi, Luca/0000-0002-9953-8593; Mueller, Holger/0000-0002-0183-8927; Chance, Kelly/0000-0002-7339-7577; Mackie, Cameron/0000-0003-2885-2021; Gordon, Iouli/0000-0003-4763-2841; Rothman, Laurence/0000-0002-3837-4847 FU NASA AURA [NNX11AF91G]; NASA [NNX10AB94G]; National Science Foundation; National Aeronautics and Space Administration FX The management and development of the HITRAN molecular database has been supported by NASA AURA mission Grant NNX11AF91G, and NASA Planetary Atmosphere Grant NNX10AB94G.; NCAR is sponsored by the National Science Foundation. Part of the research at the College of William and Mary, Langley Research Center, and the Jet Propulsion Laboratory an), California Institute of Technology was performed under contract with the National Aeronautics and Space Administration. NR 352 TC 988 Z9 1016 U1 36 U2 241 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV PY 2013 VL 130 SI SI BP 4 EP 50 DI 10.1016/j.jqsrt.2013.07.002 PG 47 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 245RS UT WOS:000326482100002 ER PT J AU Ma, Q Tipping, RH Lavrentieva, NN Dudaryonok, AS AF Ma, Q. Tipping, R. H. Lavrentieva, N. N. Dudaryonok, A. S. TI Verification of the H2O linelists with theoretically developed tools SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE HITRAN; Properties of the energy levels and wave functions of H2O states; The pair identity and the smooth variation rules ID MOLECULAR SPECTROSCOPIC DATABASE; BROADENED HALF-WIDTHS; HIGH-J STATES; WATER-VAPOR; LINE PARAMETERS; ENERGY-LEVELS; HITRAN; TRANSITIONS; SHIFTS; LIST AB Two basic rules (i.e., the pair identity and the smooth variation rules) resulting from the properties of the energy levels and wave functions of H2O states govern how the spectroscopic parameters vary with the H2O lines within the individually defined groups of lines. With these rules, for those lines involving high j states in the same groups, variations of all their spectroscopic parameters (i.e., the transition frequency, intensity, pressure broadened half-width, pressure-induced shift, and temperature exponent) can be well monitored. Thus, the rules can serve as simple and effective tools to screen the H2O spectroscopic data listed in the HITRAN database and verify the latter's accuracies. By checking violations of the rules occurring among the data within the individual groups, possible errors can be picked up and also possible missing lines in the linelist whose intensities are above the threshold can be identified. We have used these rules to check the accuracies of the spectroscopic parameters and the completeness of the linelists for several important H2O vibrational bands. Based on our results, the accuracy of the line frequencies in HITRAN 2008 is consistent. For the line intensity, we have found that there are a substantial number of lines whose intensity values are questionable. With respect to other parameters, many mistakes have been found. The above claims are consistent with a well known fact that values of these parameters in HITRAN contain larger uncertainties. Furthermore, supplements of the missing line list consisting of line assignments and positions can be developed from the screening results. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Ma, Q.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Ma, Q.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA. [Tipping, R. H.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Lavrentieva, N. N.; Dudaryonok, A. S.] VE Zuev Inst Atmospher Opt SB RAS, Tomsk 634021, Russia. RP Ma, Q (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM qma@giss.nasa.gov RI Lavrentieva, Nina/A-4010-2014 FU NSF [1228861]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231] FX Two of the authors (Q, Ma and R.H. Tipping) acknowledge financial support from NSF under Grant 1228861. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. NR 17 TC 1 Z9 1 U1 1 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV PY 2013 VL 130 SI SI BP 81 EP 99 DI 10.1016/j.jqsrt.2013.07.017 PG 19 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 245RS UT WOS:000326482100006 ER PT J AU Long, DA Truong, GW Hodges, JT Miller, CE AF Long, D. A. Truong, G-W Hodges, J. T. Miller, C. E. TI Absolute (CO2)-C-12-O-16 transition frequencies at the kHz-level from 1.6 to 7.8 mu m SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Carbon dioxide; Line positions; Transition frequencies; Optical frequency comb ID O-2 A-BAND; MOLECULAR-CONSTANTS; SPECTROSCOPIC DATABASE; LINE PARAMETERS; CAVITY RING; CO2; LASER; COMB; STABILIZATION; CM(-1) AB Absolute transition frequencies were measured for a series of transitions in the (30013)<-(00001) near-infrared (CO2)-C-12-O-16 band. These measurements were referenced to a cesium atomic clock through the use of an optical frequency comb. Combined standard uncertainties as low as 18 kHz (6 x 10(-7) cm(-1)) were achieved. Importantly, deviations as large as 5 MHz were observed relative to the HITRAN 2008 database. These measurements were then included in a global fit of 416 CO2 mid-infrared and near-infrared measurements each of which was absolute. The resulting spectroscopic parameters provide a series of secondary frequency standards with kHz-level uncertainties across a wide frequency range and should significantly improve spectroscopic retrieval algorithms for space-based measurements of atmospheric CO2. Published by Elsevier Ltd. C1 [Long, D. A.; Truong, G-W; Hodges, J. T.] NIST, Mat Measurement Lab, Gaithersburg, MD 20899 USA. [Truong, G-W] Univ Western Australia, Sch Phys, Frequency Stand & Metrol Res Grp, Nedlands, WA 6009, Australia. [Miller, C. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Long, DA (reprint author), NIST, Mat Measurement Lab, 100 Bur Dr, Gaithersburg, MD 20899 USA. EM david.long@nist.gov; charles.e.miller@jpl.nasa.gov FU NIST Greenhouse Gas Measurements and Climate Research Program; NIST Innovations in Measurement Science (IMS) award; Australian Fulbright Fellowship; Orbiting Carbon Observatory (OCO-2) mission; National Aeronautics and Space Administration (NASA) FX Support was provided by the NIST Greenhouse Gas Measurements and Climate Research Program and a NIST Innovations in Measurement Science (IMS) award. G.-W. Truong was supported at NIST by an Australian Fulbright Fellowship. Additional support was provided by the Orbiting Carbon Observatory (OCO-2) mission. The research performed at the Jet Propulsion Laboratory (JPL), California Institute of Technology was conducted under contract from the National Aeronautics and Space Administration (NASA). NR 32 TC 12 Z9 12 U1 3 U2 22 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV PY 2013 VL 130 SI SI BP 112 EP 115 DI 10.1016/j.jqsrt.2013.07.001 PG 4 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 245RS UT WOS:000326482100008 ER PT J AU Huang, XC Freedman, RS Tashkun, SA Schwenke, DW Lee, TJ AF Huang, Xinchuan Freedman, Richard S. Tashkun, Sergey A. Schwenke, David W. Lee, Timothy J. TI Semi-empirical (CO2)-C-12-O-16 IR line lists for simulations up to 1500 K and 20,000 cm(-1) SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE (CO2)-C-12-O-16; Infrared line list; High temperature; Theoretical spectroscopy; High energy ID RESOLUTION TRANSMISSION MEASUREMENTS; HIGH-TEMPERATURE; CARBON-DIOXIDE; CO2; INTENSITIES; NIGHTSIDE; WAVE AB New semi-empirical Infrared (IR) line lists for (CO2)-C-12-O-16, Ames-296 K and Ames-1000 K, have been computed using a newly updated ab initio CCSD(T)/aug-cc-pVQZ dipole moment surface (denoted DMS-N2) and an empirically refined potential energy surface (Ames-1). J=0-150 rovibrational levels are computed up to 30,000 cm(-1), and related transitions are cut off at 1E-42 cm molecule(-1) (296 K) and 1E-36 cm molecule(-1) (1000 K). These are the first line lists available to cover reliably the energy region as high as similar to 20,000 cm(-1). Recent experimental data at 1.1 mu m has confirmed the predicted intensities for the 50013-00001 and 50014-00001 band transitions have better than 90% agreement. Comparisons are made against the Wattson 750 K line list and HITEMP/HITRAN at 300 K, 500 K, 725 K, 1000 K, 1500 K, 2000 K and 3000 K. The temperature dependence and accuracy of the new Ames-296 K/1000 K line lists are investigated and we claim both line lists are capable of providing reliable opacities up to 18,00023,000 cm(-1), while the highest applicable wavenumber range drops as T rises. We suggest caution is used for T> 1000 K simulations. Comparison to recent experiments at 1000 K, 1550 K and 1773 K shows that the Ames-1000 K line list and HITEMP perform similarly in the 3200-3800 cm(-1) and 4600-5200 cm-1 ranges. In the 2000-2100 cm(-1) range, Ames-1000 K yields better agreement relative to experiment. Existing problems and possible future solutions in the new Ames-296 K/1000 K line lists for line positions and intensities are also discussed. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Huang, Xinchuan; Freedman, Richard S.] SETI Inst, Mountain View, CA 94043 USA. [Schwenke, David W.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Tashkun, Sergey A.] SB RAS, VE Zuev Inst Atmospher Opt, Tomsk 634021, Russia. RP Huang, XC (reprint author), SETI Inst, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA. EM xinchuan.huang-1@nasa.gov; Richard.S.Freedman@nasa.gov; Tashkun@rambler.ru; David.W.Schwenke@nasa.gov; Timothy.J.Lee@nasa.gov RI Lee, Timothy/K-2838-2012; Tashkun, Sergey/E-8682-2014; schwenke, david/I-3564-2013; HUANG, XINCHUAN/A-3266-2013 FU NASA; NASA ROSES [NN-H11ZDA001N11-OSS-0134, NNH11ZDA001N11-PATM-11-0014] FX DWS, TJL, and XH gratefully acknowledge financial support from the NASA Venus Express Supporting Investigator Program. X. Huang acknowledges the NASA/SETI Co-operative Agreement NNX09AI9A and NNX12AG96A. R.S. Freedman acknowledges the NASA/SETI Co-operative Agreement NNX12AJ19A and NASA ROSES funding NN-H11ZDA001N11-OSS-0134 and NNH11ZDA001N11-PATM-11-0014. TJL and XH thank Dr. Jeff Hollingsworth for helpful discussions. S.A. Tashkun thanks Dr. V.I. Perevalov for useful discussions. NR 25 TC 25 Z9 25 U1 0 U2 14 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV PY 2013 VL 130 SI SI BP 134 EP 146 DI 10.1016/j.jqsrt.2013.05.018 PG 13 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 245RS UT WOS:000326482100010 ER PT J AU Brown, LR Sung, K Benner, DC Devi, VM Boudon, V Gabard, T Wenger, C Campargue, A Leshchishina, O Kassi, S Mondelain, D Wang, L Daumont, L Regalia, L Rey, M Thomas, X Tyuterev, VG Lyulin, OM Nikitin, AV Niederer, HM Albert, S Bauerecker, S Quack, M O'Brien, JJ Gordon, IE Rothman, LS Sasada, H Coustenis, A Smith, MAH Carrington, T Wang, XG Mantz, AW Spickler, PT AF Brown, L. R. Sung, K. Benner, D. C. Devi, V. M. Boudon, V. Gabard, T. Wenger, C. Campargue, A. Leshchishina, O. Kassi, S. Mondelain, D. Wang, L. Daumont, L. Regalia, L. Rey, M. Thomas, X. Tyuterev, Vl G. Lyulin, O. M. Nikitin, A. V. Niederer, H. M. Albert, S. Bauerecker, S. Quack, M. O'Brien, J. J. Gordon, I. E. Rothman, L. S. Sasada, H. Coustenis, A. Smith, M. A. H. Carrington, T., Jr. Wang, X-G Mantz, A. W. Spickler, P. T. TI Methane line parameters in the HITRAN2012 database SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Methane; Line parameters; Remote sensing; Planets; Exoplanets; HITRAN database ID MOLECULAR SPECTROSCOPIC DATABASE; M TRANSPARENCY WINDOW; MULTISPECTRUM FITTING TECHNIQUE; INDUCED SHIFT COEFFICIENTS; LISTS 5852-7919 CM(-1); BROADENED HALF-WIDTHS; MIRS COMPUTER PACKAGE; MU-M REGION; NU(3) BAND; INFRARED-SPECTRUM AB The compilation of methane molecular line parameters was updated to include new global analyses and measurements for (CH4)-C-12, (CH4)-C-13 and (CH3D)-C-12. Over 70% of the methane parameters in HITRAN2008 were replaced; existing parameters retained were the microwave lines and the Dyad of (CH4)-C-13 near 7 mu m and nu(6) of (CH3D)-C-13 near 8.7 mu m, (CH3D)-C-12 (7-4076 cm(-1)), hot bands of (CH4)-C-12 (1887-3370 cm(-1)) and normal sample CH4 (4800-5550 cm(-1) and 8000-9200 cm(-1)). With a minimum intensity at 296 K in units of cm(-1)/(molecule cm(-2)) set to 10(-37) for the far-IR and 10(-29) for the mid- and near-IR, the methane database increased from 290,091 lines in HITRAN2008 to 468,013 lines, and three-fourths of these involved the main isotopologue. For (CH4)-C-12 and (CH4)-C-13, bands from the ground state were revised up to 4800 cm(-1). For the first time, (CH4)-C-13 and (CH3D)-C-12 line parameters near 2.3 mu m were included. Above 5550 cm(-1), the new compilation was based on empirical measurements. Prior laboratory results were replaced with extensive new measurements using FTIR (5550-5852 cm(-1)), differential absorption spectroscopy (DAS) and Cavity Ring Down Spectroscopy (CRDS) (5852-7912 cm(-1)). Ground state J values for nearly half of the measured lines in this range were obtained, either by confirming quantum assignments of analyses or by using spectra at 80 and 296 K. Finally, over 11,000 measured positions, intensities and empirical lower state energies (obtained using cold CH4) were also added for the first time between 10,923 and 11,502 cm(-1). Available pressure broadening measurements from HITRAN2008 were transferred into the new compilation, but 99% of the lines were given crudely-estimated coefficients. New measured intensities and broadening coefficients were included for far-IR transitions, and high accuracy line positions were inserted for the stronger P, Q and R branch transitions of nu(3) at 3.3 mu m and 2 nu(3) at 1.66 mu m. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Brown, L. R.; Sung, K.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Benner, D. C.; Devi, V. M.] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. [Boudon, V.; Gabard, T.; Wenger, C.] Univ Bourgogne, CNRS, UMR 6303, Lab Interdisciplinaire Carnot Bourgogne, F-21078 Dijon, France. [Campargue, A.; Leshchishina, O.; Kassi, S.; Mondelain, D.; Wang, L.] Univ Grenoble 1, CNRS, LIPhy UMR5588, F-38041 Grenoble, France. [Daumont, L.; Regalia, L.; Rey, M.; Thomas, X.; Tyuterev, Vl G.] Univ Reims, CNRS, UMR 7331, Grp Spectrometrie Mol & Atmospher, F-51687 Reims 2, France. [Lyulin, O. M.; Nikitin, A. V.] SB RAS, VE Zuev Inst Atmospher Opt, Lab Theoret Spect, Tomsk 634021, Russia. [Niederer, H. M.; Albert, S.; Bauerecker, S.; Quack, M.] ETH, Phys Chem Lab, CH-8093 Zurich, Switzerland. [O'Brien, J. J.] Univ Missouri, Dept Chem & Biochem, St Louis, MO 63121 USA. [Gordon, I. E.; Rothman, L. S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Sasada, H.] Keio Univ, Dept Phys, Fac Sci & Technol, Kohoku Ku, Yokohama, Kanagawa 2238522, Japan. [Coustenis, A.] Univ Paris Diderot, Univ Paris 06, CNRS, LESIA,Observ Paris, F-92195 Meudon, France. [Smith, M. A. H.] NASA, Sci Directorate, Langley Res Ctr, Hampton, VA 23681 USA. [Carrington, T., Jr.; Wang, X-G] Queens Univ, Dept Chem, Kingston, ON K7L 3N6, Canada. [Mantz, A. W.] Connecticut Coll, Dept Phys Astron & Geophys, New London, CT 06320 USA. [Spickler, P. T.] Bridgewater Coll, Dept Phys, Bridgewater, VA 22812 USA. RP Brown, LR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM linda.r.brown@jpl.nasa.gov RI BOUDON, Vincent/A-4504-2010; CARRINGTON, Tucker/I-6727-2012; Nikitin, Andrei/K-2624-2013; Quack, Martin/H-4457-2016; Sung, Keeyoon/I-6533-2015; OI CARRINGTON, Tucker/0000-0002-5200-2353; Nikitin, Andrei/0000-0002-4280-4096; Gordon, Iouli/0000-0003-4763-2841; Rothman, Laurence/0000-0002-3837-4847 FU ANR Project "CH4@Titan" [BLAN08-2_321467]; LEFE-Chat CNRS French; Groupement de Recherche International SAMIA [22]; fundamental problems of investigation and exploration of the Solar System of Russian Academia of Science; Ministry of Education, Culture, Sports, Science and Technology in Japan; Swiss National Science Foundation; ETH Zurich; Natural Sciences and Engineering Research Council of Canada; Canadian Space Agency and CAS (China); IDRIS/CINES computer centers of France; National Aeronautics and Space Administration; Martin Summer Science Research Institute; American Astronomical Society Small Research Grant FX This work is part of the ANR Project "CH4@Titan" (Ref: BLAN08-2_321467). The international funding support includes the LEFE-Chat CNRS French grant and the Groupement de Recherche International SAMIA between CNRS (France) and RFBR (Russia), Program Number 22: the fundamental problems of investigation and exploration of the Solar System of Russian Academia of Science; Grant in Aid for Scientific Research (A) and the Photon Frontier Network Program of the Ministry of Education, Culture, Sports, Science and Technology in Japan; the Swiss National Science Foundation, ETH Zurich; the Natural Sciences and Engineering Research Council of Canada, the Canadian Space Agency and CAS (China). We are grateful for the support from IDRIS/CINES computer centers of France and also the computer center Reims-Champagne-Ardenne.r Part of the research at the College of William and Mary, Connecticut College, Langley Research Center, the Harvard-Smithsonian Center for Astrophysics and the Jet Propulsion Laboratory (JPL) was performed under contract with National Aeronautics and Space Administration. Funding for research at Bridgewater College was provided by the Martin Summer Science Research Institute and from an American Astronomical Society Small Research Grant. NR 119 TC 51 Z9 52 U1 4 U2 44 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV PY 2013 VL 130 SI SI BP 201 EP 219 DI 10.1016/j.jqsrt.2013.06.020 PG 19 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 245RS UT WOS:000326482100015 ER PT J AU Down, MJ Hill, C Yurchenko, SN Tennyson, J Brown, LR Kleiner, I AF Down, Michael J. Hill, Christian Yurchenko, Sergei N. Tennyson, Jonathan Brown, Linda R. Kleiner, Isabelle TI Re-analysis of ammonia spectra: Updating the HITRAN (NH3)-N-14 database SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Ammonia; Line assignments; Atmospheric physics; Planetary atmospheres ID MOLECULAR SPECTROSCOPIC DATABASE; SELF-BROADENING COEFFICIENTS; PYRAMIDAL XY3 MOLECULES; MU-M; VIBRATIONAL SYSTEM; LINE POSITIONS; ENERGY-LEVELS; HOT BANDS; AB-INITIO; INTENSITIES AB The data incorporated in the HITRAN database for (NH3)-N-14 are analyzed using a comprehensive and consistent set of quantum numbers, empirical lower energy levels and the BYTe variationally calculated line list as reference points. Labelings are checked to ensure that they obey both the usual selection rules and the HITRAN labeling formalisms; the problems identified are corrected where possible. Further assignments are brought into question by combination difference (CD) checking of implied upper energy levels. The CD analysis yields an 89% complete (NH3)-N-14 energy level list up to 6610 cm(-1) and J=21, self-consistent to 0.1 cm(-1). In combination with the 1723 previously unassigned and unlabeled lines in HITRAN a total of 2529 problem lines were identified for re-analysis. The compiled energy level list was used to label and assign the set of problem transitions, resulting in a total of 249 new assignments and a further 368 new labelings. Assignment by comparison with the reference line list resulted in 111 further new line assignments and 14 new labelings. Intensities are checked against recent measurements and BYTe. New intensities are proposed for the nu(2) band with new intensities and line positions for the 2 nu(2)-nu(2) and new line lists are created for the nu(2)-nu(2), nu(2)-nu(4) and nu(4)-nu(4) bands. BYTe band intensities are analyzed to identify other regions of missing intensity. (C) 2013 The Authors. Published by Elsevier Ltd. All rights reserved. C1 [Down, Michael J.; Hill, Christian; Yurchenko, Sergei N.; Tennyson, Jonathan] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Brown, Linda R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kleiner, Isabelle] Hop Henri Mondor, CNRS, UMR 7583, LISA, F-94010 Creteil, France. RP Tennyson, J (reprint author), UCL, Dept Phys & Astron, Mortimer St, London WC1E 6BT, England. EM j.tennyson@ucl.ac.uk RI Tennyson, Jonathan/I-2222-2012; Yurchenko, Sergey/G-9929-2012 OI Tennyson, Jonathan/0000-0002-4994-5238; Yurchenko, Sergey/0000-0001-9286-9501 FU UK Natural Environmental Research Council (NERC); ERC [267219]; VAMDC; European Union [INFRA-2008-1.2.2, 239108]; National Aeronautics and Space Administration FX This work is supported by a the UK Natural Environmental Research Council (NERC) via a studentship to MJD, by ERC Advanced Investigator Project 267219 and the VAMDC project which is funded by the European Union INFRA-2008-1.2.2 Scientific Data Infrastructure program under Grant Agreement number 239108. Part of the research described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contracts and grants with the National Aeronautics and Space Administration. NR 62 TC 27 Z9 27 U1 4 U2 19 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV PY 2013 VL 130 SI SI BP 260 EP 272 DI 10.1016/j.jqsrt.2013.05.027 PG 13 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 245RS UT WOS:000326482100019 ER PT J AU Cho, KS Bong, SC Chae, J Kim, YH Park, YD Katsukawa, Y AF Cho, K. -S. Bong, S. -C. Chae, J. Kim, Y. -H. Park, Y. -D. Katsukawa, Y. TI FISS Observations of Vertical Motion of Plasma in Tiny Pores SO SOLAR PHYSICS LA English DT Article DE Chromosphere; Imaging spectroscopy; Photosphere; Pore; Surface magnetic field ID MAGNETIC-FLUX TUBES; SOLAR PORES; OPTICAL TELESCOPE; ACTIVE-REGION; FIELDS; INTENSIFICATION; CONVECTION; ELEMENTS; MISSION; LINES AB Pores can be exploited for the understanding of the interaction between small-scale vertical magnetic field and the surrounding convective motions as well as the transport of mechanical energy into the chromosphere along the magnetic field. For better understanding of the physics of pores, we investigate tiny pores in a new emerging active region (AR11117) that were observed on 26 October 2010 by the Solar Optical Telescope (SOT) on board Hinode and the Fast Imaging Solar Spectrograph (FISS) of the 1.6 meter New Solar Telescope (NST). The pores are compared with nearby small magnetic concentrations (SMCs), which have similar magnetic flux as the pores but do not appear dark. Magnetic flux density and Doppler velocities in the photosphere are estimated by applying the center-of-gravity method to the Hinode/Spectro-Polarimeter data. The line-of-sight motions in the lower chromosphere are determined by applying the bisector method to the wings of the H alpha and the Ca ii 8542 line simultaneously taken by the FISS. The coordinated observation reveals that the pores are filled with plasma which moves down slowly and are surrounded by stronger downflow in the photosphere. In the lower chromosphere, we found that the plasma flows upwards inside the pores while the plasma in the SMCs is always moving down. Our inspection of the Ca ii 8542 line from the wing to the core shows that the upflow in the pores slows down with height and turns into downflow in the upper chromosphere while the downflow in the SMCs gains its speed. Our results are in agreement with the numerical studies which suggest that rapid cooling of the interior of the pores drives a strong downflow, which collides with the dense lower layer below and rebounds into an upflow. C1 [Cho, K. -S.; Bong, S. -C.; Kim, Y. -H.; Park, Y. -D.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Cho, K. -S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cho, K. -S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Chae, J.] Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul 151747, South Korea. [Katsukawa, Y.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. RP Cho, KS (reprint author), Korea Astron & Space Sci Inst, Taejon 305348, South Korea. EM kscho@kasi.re.kr; chae@astro.snu.ac.kr; yukio.katsukawa@nao.ac.jp FU "Development of Korea Space Weather Center" of KASI; KASI; Korea Research Foundation; Korean Government [KRF-2008-220-C00022, 2011-0028102] FX We are grateful to the referee for helpful and constructive comments. This work was supported by the "Development of Korea Space Weather Center" of KASI and the KASI basic research funds and by the Korea Research Foundation Grant funded by the Korean Government (KRF-2008-220-C00022, 2011-0028102). One of the authors (K.-S.C.) is very thankful to R.J. Rutten for his valuable comments and to S. Tsuneta for supporting of collaborative visiting in NAOJ, where the part of present work has been carried out. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and NSC (Norway). NR 32 TC 5 Z9 5 U1 0 U2 1 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 NOV PY 2013 VL 288 IS 1 BP 23 EP 37 DI 10.1007/s11207-012-0196-1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242LK UT WOS:000326243200002 ER PT J AU BenMoussa, A Gissot, S Schuhle, U Del Zanna, G Auchere, F Mekaoui, S Jones, AR Walton, D Eyles, CJ Thuillier, G Seaton, D Dammasch, IE Cessateur, G Meftah, M Andretta, V Berghmans, D Bewsher, D Bolsee, D Bradley, L Brown, DS Chamberlin, PC Dewitte, S Didkovsky, LV Dominique, M Eparvier, FG Foujols, T Gillotay, D Giordanengo, B Halain, JP Hock, RA Irbah, A Jeppesen, C Judge, DL Kretzschmar, M McMullin, DR Nicula, B Schmutz, W Ucker, G Wieman, S Woodraska, D Woods, TN AF BenMoussa, A. Gissot, S. Schuehle, U. Del Zanna, G. Auchere, F. Mekaoui, S. Jones, A. R. Walton, D. Eyles, C. J. Thuillier, G. Seaton, D. Dammasch, I. E. Cessateur, G. Meftah, M. Andretta, V. Berghmans, D. Bewsher, D. Bolsee, D. Bradley, L. Brown, D. S. Chamberlin, P. C. Dewitte, S. Didkovsky, L. V. Dominique, M. Eparvier, F. G. Foujols, T. Gillotay, D. Giordanengo, B. Halain, J. P. Hock, R. A. Irbah, A. Jeppesen, C. Judge, D. L. Kretzschmar, M. McMullin, D. R. Nicula, B. Schmutz, W. Ucker, G. Wieman, S. Woodraska, D. Woods, T. N. TI On-Orbit Degradation of Solar Instruments SO SOLAR PHYSICS LA English DT Article DE Degradation; Solar instruments; Space environment; Calibration; Contamination; Solar mission ID CORONAL DIAGNOSTIC SPECTROMETER; ULTRAVIOLET IMAGING TELESCOPE; RADIOMETRIC CALIBRATION; PHOTOMETRIC CALIBRATION; IRRADIANCE OBSERVATIONS; HINODE MISSION; SOHO MISSION; CDS NIS; SUN; SUMER AB We present the lessons learned about the degradation observed in several space solar missions, based on contributions at the Workshop about On-Orbit Degradation of Solar and Space Weather Instruments that took place at the Solar Terrestrial Centre of Excellence (Royal Observatory of Belgium) in Brussels on 3 May 2012. The aim of this workshop was to open discussions related to the degradation observed in Sun-observing instruments exposed to the effects of the space environment. This article summarizes the various lessons learned and offers recommendations to reduce or correct expected degradation with the goal of increasing the useful lifespan of future and ongoing space missions. C1 [BenMoussa, A.; Bolsee, D.; Nicula, B.] Solar Terr Ctr Excellence, B-1180 Brussels, Belgium. [BenMoussa, A.; Gissot, S.; Seaton, D.; Dammasch, I. E.; Berghmans, D.; Dominique, M.; Giordanengo, B.; Nicula, B.] Observ Royal Belgique, B-1180 Brussels, Belgium. [Schuehle, U.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Del Zanna, G.] Univ Cambridge, DAMTP Ctr Math Sci, Cambridge CB3 0WA, England. [Auchere, F.] Univ Paris 11, Inst Astrophys Spatiale, CNRS, F-91405 Orsay, France. [Mekaoui, S.] Commiss European Communities, Joint Res Ctr, I-21020 Ispra, Italy. [Mekaoui, S.; Dewitte, S.] Royal Meteorol Inst Belgium, B-1180 Brussels, Belgium. [Jones, A. R.; Eparvier, F. G.; Jeppesen, C.; Ucker, G.; Woodraska, D.; Woods, T. N.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Walton, D.; Bradley, L.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Eyles, C. J.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. [Eyles, C. J.] Univ Valancia, ICMUV, Grp Astron & Ciencias Espacio, Valencia, Spain. [Thuillier, G.; Meftah, M.; Foujols, T.; Irbah, A.] Univ Versailles, Univ Paris 06, LATMOS CNRS UMR 8190, F-78000 Versailles, France. [Cessateur, G.; Schmutz, W.] PMOD WRC, CH-7260 Davos, Switzerland. [Andretta, V.] Osserv Astron Capodimonte, INAF, I-80141 Naples, Italy. [Bewsher, D.; Brown, D. S.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Bolsee, D.; Gillotay, D.] Belgium Inst Space Aeron, B-1180 Brussels, Belgium. [Chamberlin, P. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Didkovsky, L. V.; Judge, D. L.; Wieman, S.] Univ So Calif, Ctr Space Sci, Los Angeles, CA 90089 USA. [Halain, J. P.] Univ Liege, Ctr Spatial Liege, B-4013 Angleur, Belgium. [Hock, R. A.] Air Force Res Lab, Alburqueque, NM USA. [Kretzschmar, M.] Univ Orleans, LPC2E CNRS, UMR 7328, F-45071 Orleans 2, France. [McMullin, D. R.] Space Syst Res Corp, Alexandria, VA 22314 USA. RP Gissot, S (reprint author), Observ Royal Belgique, B-1180 Brussels, Belgium. EM ali.benmoussa@stce.be; samuel.gissot@oma.be RI Chamberlin, Phillip/C-9531-2012; Irbah, Abdanour/J-2408-2016; Schmutz, Werner/B-4153-2014; OI Chamberlin, Phillip/0000-0003-4372-7405; Irbah, Abdanour/0000-0003-3265-3148; Schmutz, Werner/0000-0003-1159-5639; Auchere, Frederic/0000-0003-0972-7022; Brown, Daniel/0000-0002-1618-8816; Bewsher, Danielle/0000-0002-6351-5170; SEATON, DANIEL/0000-0002-0494-2025; Andretta, Vincenzo/0000-0003-1962-9741 FU Belgian Federal Science Policy Office (BELSPO) through Solar Terrestrial Centre of Excellence (STCE) program FX The authors acknowledge the support from the Belgian Federal Science Policy Office (BELSPO) through the Solar Terrestrial Centre of Excellence (STCE) program. NR 75 TC 23 Z9 23 U1 0 U2 9 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD NOV PY 2013 VL 288 IS 1 BP 389 EP 434 DI 10.1007/s11207-013-0290-z PG 46 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242LK UT WOS:000326243200023 ER PT J AU Mauk, BH Fox, NJ Kanekal, SG Kessel, RL Sibeck, DG Ukhorskiy, A AF Mauk, B. H. Fox, N. J. Kanekal, S. G. Kessel, R. L. Sibeck, D. G. Ukhorskiy, A. TI Science Objectives and Rationale for the Radiation Belt Storm Probes Mission SO SPACE SCIENCE REVIEWS LA English DT Review DE Radiation belt; Magnetosphere; Geomagnetic storms; NASA mission ID RELATIVISTIC ELECTRONS; GEOMAGNETIC STORMS; PLASMA SHEET; RING CURRENT; GEM STORMS; ACCELERATION; FIELD; MODEL; MAGNETOSPHERE; ENERGIZATION AB The NASA Radiation Belt Storm Probes (RBSP) mission addresses how populations of high energy charged particles are created, vary, and evolve in space environments, and specifically within Earth's magnetically trapped radiation belts. RBSP, with a nominal launch date of August 2012, comprises two spacecraft making in situ measurements for at least 2 years in nearly the same highly elliptical, low inclination orbits (1.1x5.8 RE, 10(a similar to)). The orbits are slightly different so that 1 spacecraft laps the other spacecraft about every 2.5 months, allowing separation of spatial from temporal effects over spatial scales ranging from similar to 0.1 to 5 RE. The uniquely comprehensive suite of instruments, identical on the two spacecraft, measures all of the particle (electrons, ions, ion composition), fields (E and B), and wave distributions (d E and d B) that are needed to resolve the most critical science questions. Here we summarize the high level science objectives for the RBSP mission, provide historical background on studies of Earth and planetary radiation belts, present examples of the most compelling scientific mysteries of the radiation belts, present the mission design of the RBSP mission that targets these mysteries and objectives, present the observation and measurement requirements for the mission, and introduce the instrumentation that will deliver these measurements. This paper references and is followed by a number of companion papers that describe the details of the RBSP mission, spacecraft, and instruments. C1 [Mauk, B. H.; Fox, N. J.; Ukhorskiy, A.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Kanekal, S. G.; Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kessel, R. L.] NASA Headquarters, Heliophys Div, SMD, Washington, DC 20546 USA. RP Mauk, BH (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. EM Barry.Mauk@jhuapl.edu; mona.kessel@nasa.gov; david.g.sibeck@nasa.gov RI Ukhorskiy, Aleksandr/E-6429-2016; Fox, Nicola/P-6692-2016; Mauk, Barry/E-8420-2017 OI Ukhorskiy, Aleksandr/0000-0002-3326-4024; Fox, Nicola/0000-0003-3411-4228; Mauk, Barry/0000-0001-9789-3797 NR 64 TC 175 Z9 175 U1 2 U2 17 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 NOV PY 2013 VL 179 IS 1-4 BP 3 EP 27 DI 10.1007/s11214-012-9908-y PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 244IM UT WOS:000326381300002 ER PT J AU Kletzing, CA Kurth, WS Acuna, M MacDowall, RJ Torbert, RB Averkamp, T Bodet, D Bounds, SR Chutter, M Connerney, J Crawford, D Dolan, JS Dvorsky, R Hospodarsky, GB Howard, J Jordanova, V Johnson, RA Kirchner, DL Mokrzycki, B Needell, G Odom, J Mark, D Pfaff , R Phillips, JR Piker, CW Remington, SL Rowland, D Santolik, O Schnurr, R Sheppard, D Smith, CW Thorne, RM Tyler, J AF Kletzing, C. A. Kurth, W. S. Acuna, M. MacDowall, R. J. Torbert, R. B. Averkamp, T. Bodet, D. Bounds, S. R. Chutter, M. Connerney, J. Crawford, D. Dolan, J. S. Dvorsky, R. Hospodarsky, G. B. Howard, J. Jordanova, V. Johnson, R. A. Kirchner, D. L. Mokrzycki, B. Needell, G. Odom, J. Mark, D. Pfaff, R., Jr. Phillips, J. R. Piker, C. W. Remington, S. L. Rowland, D. Santolik, O. Schnurr, R. Sheppard, D. Smith, C. W. Thorne, R. M. Tyler, J. TI The Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) on RBSP SO SPACE SCIENCE REVIEWS LA English DT Review DE Radiation belt physics; Wave measurements; Magnetometer measurements; Space flight instruments; RBSP; Radiation belt storm probes; Van Allen probes; Whistler waves; Geomagnetic storms; Space weather AB The Electric and Magnetic Field Instrument and Integrated Science (EMFISIS) investigation on the NASA Radiation Belt Storm Probes (now named the Van Allen Probes) mission provides key wave and very low frequency magnetic field measurements to understand radiation belt acceleration, loss, and transport. The key science objectives and the contribution that EMFISIS makes to providing measurements as well as theory and modeling are described. The key components of the instruments suite, both electronics and sensors, including key functional parameters, calibration, and performance, demonstrate that EMFISIS provides the needed measurements for the science of the RBSP mission. The EMFISIS operational modes and data products, along with online availability and data tools provide the radiation belt science community with one the most complete sets of data ever collected. C1 [Kletzing, C. A.; Kurth, W. S.; Averkamp, T.; Bounds, S. R.; Crawford, D.; Dolan, J. S.; Dvorsky, R.; Hospodarsky, G. B.; Howard, J.; Johnson, R. A.; Kirchner, D. L.; Mokrzycki, B.; Phillips, J. R.; Piker, C. W.; Remington, S. L.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Acuna, M.; MacDowall, R. J.; Connerney, J.; Odom, J.; Schnurr, R.; Sheppard, D.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Torbert, R. B.; Bodet, D.; Chutter, M.; Needell, G.; Smith, C. W.; Tyler, J.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Torbert, R. B.; Bodet, D.; Chutter, M.; Needell, G.; Smith, C. W.; Tyler, J.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Thorne, R. M.] Univ Calif Los Angeles, Los Angeles, CA USA. [Jordanova, V.] Los Alamos Natl Lab, Los Alamos, NM USA. [Santolik, O.] Inst Atmospher Phys, Dept Space Phys, Prague, Czech Republic. [Santolik, O.] Charles Univ Prague, Fac Math & Phys, Prague, Czech Republic. [Mark, D.] Bison Aerosp Inc, Newcastle, WY USA. [Pfaff, R., Jr.; Rowland, D.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP Kletzing, CA (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. EM craig-kletzing@uiowa.edu RI Santolik, Ondrej/F-7766-2014; Rowland, Douglas/F-5589-2012; OI Rowland, Douglas/0000-0003-0948-6257; Kletzing, Craig/0000-0002-4136-3348; Hospodarsky, George/0000-0001-9200-9878; Kurth, William/0000-0002-5471-6202; Jordanova, Vania/0000-0003-0475-8743 FU JHU/APL under NASA Prime contract [921647, NAS5-01072] FX We would like to thank the entire Van Allen Probes team who have made this mission the success that it is. We would also like to thank the EFW team, in particular, for their work in supplying electric field signals to EMFISIS as well as supporting cross-calibration of the two sets of instruments. This work was performed under supported on JHU/APL contract no. 921647 under NASA Prime contract No. NAS5-01072. NR 145 TC 201 Z9 201 U1 2 U2 29 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 NOV PY 2013 VL 179 IS 1-4 BP 127 EP 181 DI 10.1007/s11214-013-9993-6 PG 55 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 244IM UT WOS:000326381300005 ER PT J AU Spence, HE Reeves, GD Baker, DN Blake, JB Bolton, M Bourdarie, S Chan, AA Claudepierre, SG Clemmons, JH Cravens, JP Elkington, SR Fennell, JF Friedel, RHW Funsten, HO Goldstein, J Green, JC Guthrie, A Henderson, MG Horne, RB Hudson, MK Jahn, JM Jordanova, VK Kanekal, SG Klatt, BW Larsen, BA Li, X MacDonald, EA Mann, IR Niehof, J O'Brien, TP Onsager, TG Salvaggio, D Skoug, RM Smith, SS Suther, LL Thomsen, MF Thorne, RM AF Spence, H. E. Reeves, G. D. Baker, D. N. Blake, J. B. Bolton, M. Bourdarie, S. Chan, A. A. Claudepierre, S. G. Clemmons, J. H. Cravens, J. P. Elkington, S. R. Fennell, J. F. Friedel, R. H. W. Funsten, H. O. Goldstein, J. Green, J. C. Guthrie, A. Henderson, M. G. Horne, R. B. Hudson, M. K. Jahn, J. -M. Jordanova, V. K. Kanekal, S. G. Klatt, B. W. Larsen, B. A. Li, X. MacDonald, E. A. Mann, I. R. Niehof, J. O'Brien, T. P. Onsager, T. G. Salvaggio, D. Skoug, R. M. Smith, S. S. Suther, L. L. Thomsen, M. F. Thorne, R. M. TI Science Goals and Overview of the Radiation Belt Storm Probes (RBSP) Energetic Particle, Composition, and Thermal Plasma (ECT) Suite on NASA's Van Allen Probes Mission SO SPACE SCIENCE REVIEWS LA English DT Review DE Radiation belts; Particle senors; Radiation detection; Space weather; Van Allen Probes ID INNER MAGNETOSPHERE; ACCELERATION; VARIABILITY; CONSISTENT; ELECTRONS; DYNAMICS; SAMPEX; DECAY AB The Radiation Belt Storm Probes (RBSP)-Energetic Particle, Composition, and Thermal Plasma (ECT) suite contains an innovative complement of particle instruments to ensure the highest quality measurements ever made in the inner magnetosphere and radiation belts. The coordinated RBSP-ECT particle measurements, analyzed in combination with fields and waves observations and state-of-the-art theory and modeling, are necessary for understanding the acceleration, global distribution, and variability of radiation belt electrons and ions, key science objectives of NASA's Living With a Star program and the Van Allen Probes mission. The RBSP-ECT suite consists of three highly-coordinated instruments: the Magnetic Electron Ion Spectrometer (MagEIS), the Helium Oxygen Proton Electron (HOPE) sensor, and the Relativistic Electron Proton Telescope (REPT). Collectively they cover, continuously, the full electron and ion spectra from one eV to 10's of MeV with sufficient energy resolution, pitch angle coverage and resolution, and with composition measurements in the critical energy range up to 50 keV and also from a few to 50 MeV/nucleon. All three instruments are based on measurement techniques proven in the radiation belts. The instruments use those proven techniques along with innovative new designs, optimized for operation in the most extreme conditions in order to provide unambiguous separation of ions and electrons and clean energy responses even in the presence of extreme penetrating background environments. The design, fabrication and operation of ECT spaceflight instrumentation in the harsh radiation belt environment ensure that particle measurements have the fidelity needed for closure in answering key mission science questions. ECT instrument details are provided in companion papers in this same issue. In this paper, we describe the science objectives of the RBSP-ECT instrument suite on the Van Allen Probe spacecraft within the context of the overall mission objectives, indicate how the characteristics of the instruments satisfy the requirements to achieve these objectives, provide information about science data collection and dissemination, and conclude with a description of some early mission results. C1 [Spence, H. E.; Smith, S. S.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Reeves, G. D.; Friedel, R. H. W.; Funsten, H. O.; Guthrie, A.; Henderson, M. G.; Jordanova, V. K.; Larsen, B. A.; MacDonald, E. A.; Niehof, J.; Skoug, R. M.; Thomsen, M. F.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Baker, D. N.; Bolton, M.; Elkington, S. R.; Li, X.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Blake, J. B.; Claudepierre, S. G.; Clemmons, J. H.; Fennell, J. F.; O'Brien, T. P.; Salvaggio, D.] Aerosp Corp, El Segundo, CA USA. [Chan, A. A.] Rice Univ, Houston, TX 77005 USA. [Cravens, J. P.] JPC LLC, Port Aransas, TX 78373 USA. [Goldstein, J.; Jahn, J. -M.] SW Res Inst, San Antonio, TX 78238 USA. [Green, J. C.; Onsager, T. G.] Natl Ocean & Atmospher Adm, Boulder, CO 80305 USA. [Horne, R. B.] British Antarctic Survey, Cambridge CB3 0ET, England. [Hudson, M. K.] Dartmouth Coll, Hanover, NH 03755 USA. [Kanekal, S. G.] NASA Goddard, Greenbelt, MD 20771 USA. [Klatt, B. W.] MIT, Cambridge, MA 02139 USA. [Mann, I. R.] Univ Alberta, Edmonton, AB T6G 2R3, Canada. [Bourdarie, S.] ONERA CERT, Toulouse 04, France. [Suther, L. L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Thorne, R. M.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. [Klatt, B. W.] Univ Calgary, Calgary, AB T2N 1N4, Canada. RP Spence, HE (reprint author), Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. EM Harlan.Spence@unh.edu RI Friedel, Reiner/D-1410-2012; Funsten, Herbert/A-5702-2015; Larsen, Brian/A-7822-2011; Reeves, Geoffrey/E-8101-2011; Henderson, Michael/A-3948-2011; OI Jordanova, Vania/0000-0003-0475-8743; Spence, Harlan/0000-0002-2526-2205; Friedel, Reiner/0000-0002-5228-0281; Funsten, Herbert/0000-0002-6817-1039; Larsen, Brian/0000-0003-4515-0208; Reeves, Geoffrey/0000-0002-7985-8098; Henderson, Michael/0000-0003-4975-9029; Horne, Richard/0000-0002-0412-6407; Clemmons, James/0000-0002-5298-5222 FU RBSP-ECT; JHU/APL under NASA's Prime Contract [967399, NAS5-01072] FX We gratefully acknowledge the Van Allen Probes mission team at the Johns Hopkins University (JHU)/Applied Physics Laboratory (APL) and the Project Science team at JHU/APL, NASA GSFC, and NASA HQ for their invaluable support during the design, development, testing, and early operations of the mission. This work was supported by RBSP-ECT funding provided by JHU/APL Contract No. 967399 under NASA's Prime Contract No. NAS5-01072. NR 49 TC 124 Z9 125 U1 1 U2 31 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 NOV PY 2013 VL 179 IS 1-4 BP 311 EP 336 DI 10.1007/s11214-013-0007-5 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 244IM UT WOS:000326381300009 ER PT J AU Baker, DN Kanekal, SG Hoxie, VC Batiste, S Bolton, M Li, X Elkington, SR Monk, S Reukauf, R Steg, S Westfall, J Belting, C Bolton, B Braun, D Cervelli, B Hubbell, K Kien, M Knappmiller, S Wade, S Lamprecht, B Stevens, K Wallace, J Yehle, A Spence, H Friedel, R AF Baker, D. N. Kanekal, S. G. Hoxie, V. C. Batiste, S. Bolton, M. Li, X. Elkington, S. R. Monk, S. Reukauf, R. Steg, S. Westfall, J. Belting, C. Bolton, B. Braun, D. Cervelli, B. Hubbell, K. Kien, M. Knappmiller, S. Wade, S. Lamprecht, B. Stevens, K. Wallace, J. Yehle, A. Spence, H. E. Friedel, R. TI The Relativistic Electron-Proton Telescope (REPT) Instrument on Board the Radiation Belt Storm Probes (RBSP) Spacecraft: Characterization of Earth's Radiation Belt High-Energy Particle Populations SO SPACE SCIENCE REVIEWS LA English DT Review DE Radiation detection; Particle sensors; Radiation belts; Space weather ID ACCELERATION; SOLAR; SIMULATION; INJECTIONS; SAMPEX; MAGNETOSPHERE; PREDICTION; MISSION; ZONE AB Particle acceleration and loss in the million electron Volt (MeV) energy range (and above) is the least understood aspect of radiation belt science. In order to measure cleanly and separately both the energetic electron and energetic proton components, there is a need for a carefully designed detector system. The Relativistic Electron-Proton Telescope (REPT) on board the Radiation Belt Storm Probe (RBSP) pair of spacecraft consists of a stack of high-performance silicon solid-state detectors in a telescope configuration, a collimation aperture, and a thick case surrounding the detector stack to shield the sensors from penetrating radiation and bremsstrahlung. The instrument points perpendicular to the spin axis of the spacecraft and measures high-energy electrons (up to similar to 20 MeV) with excellent sensitivity and also measures magnetospheric and solar protons to energies well above E=100 MeV. The instrument has a large geometric factor (g=0.2 cm(2) sr) to get reasonable count rates (above background) at the higher energies and yet will not saturate at the lower energy ranges. There must be fast enough electronics to avert undue dead-time limitations and chance coincidence effects. The key goal for the REPT design is to measure the directional electron intensities (in the range 10(-2)-10(6) particles/cm(2) s sr MeV) and energy spectra (Delta E/E similar to 25 %) throughout the slot and outer radiation belt region. Present simulations and detailed laboratory calibrations show that an excellent design has been attained for the RBSP needs. We describe the engineering design, operational approaches, science objectives, and planned data products for REPT. C1 [Baker, D. N.; Hoxie, V. C.; Batiste, S.; Bolton, M.; Li, X.; Elkington, S. R.; Monk, S.; Reukauf, R.; Steg, S.; Westfall, J.; Belting, C.; Braun, D.; Cervelli, B.; Hubbell, K.; Kien, M.; Knappmiller, S.; Wade, S.; Lamprecht, B.; Wallace, J.; Yehle, A.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. [Kanekal, S. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bolton, B.] Ball Aerosp, Boulder, CO 80301 USA. [Stevens, K.] Efficient Log Designs, Boulder, CO 80304 USA. [Spence, H. E.] Univ New Hampshire, Ctr Earth Oceans & Space, Durham, NH 03824 USA. [Friedel, R.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Baker, DN (reprint author), Univ Colorado, Atmospher & Space Phys Lab, 3665 Discovery Dr, Boulder, CO 80303 USA. EM daniel.baker@lasp.colorado.edu RI Friedel, Reiner/D-1410-2012; OI Friedel, Reiner/0000-0002-5228-0281; Spence, Harlan/0000-0002-2526-2205 FU NASA prime contract [NAS5-01072] FX This work has been supported by NASA prime contract NAS5-01072 to Johns Hopkins University Applied Physics Laboratory (JHU/APL). NR 55 TC 49 Z9 50 U1 0 U2 21 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 NOV PY 2013 VL 179 IS 1-4 BP 337 EP 381 DI 10.1007/s11214-012-9950-9 PG 45 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 244IM UT WOS:000326381300010 ER PT J AU Millan, RM McCarthy, MP Sample, JG Smith, DM Thompson, LD McGaw, DG Woodger, LA Hewitt, JG Comess, MD Yando, KB Liang, AX Anderson, BA Knezek, NR Rexroad, WZ Scheiman, JM Bowers, GS Halford, AJ Collier, AB Clilverd, MA Lin, RP Hudson, MK AF Millan, R. M. McCarthy, M. P. Sample, J. G. Smith, D. M. Thompson, L. D. McGaw, D. G. Woodger, L. A. Hewitt, J. G. Comess, M. D. Yando, K. B. Liang, A. X. Anderson, B. A. Knezek, N. R. Rexroad, W. Z. Scheiman, J. M. Bowers, G. S. Halford, A. J. Collier, A. B. Clilverd, M. A. Lin, R. P. Hudson, M. K. TI The Balloon Array for RBSP Relativistic Electron Losses (BARREL) SO SPACE SCIENCE REVIEWS LA English DT Review DE Radiation belts; Wave-particle interactions; Electron precipitation ID ION-CYCLOTRON WAVES; OUTER RADIATION BELT; X-RAYS; LOSS MECHANISMS; GEM STORMS; PRECIPITATION; MICROBURSTS; RESOLUTION; SAMPEX AB BARREL is a multiple-balloon investigation designed to study electron losses from Earth's Radiation Belts. Selected as a NASA Living with a Star Mission of Opportunity, BARREL augments the Radiation Belt Storm Probes mission by providing measurements of relativistic electron precipitation with a pair of Antarctic balloon campaigns that will be conducted during the Austral summers (January-February) of 2013 and 2014. During each campaign, a total of 20 small (similar to 20 kg) stratospheric balloons will be successively launched to maintain an array of similar to 5 payloads spread across similar to 6 hours of magnetic local time in the region that magnetically maps to the radiation belts. Each balloon carries an X-ray spectrometer to measure the bremsstrahlung X-rays produced by precipitating relativistic electrons as they collide with neutrals in the atmosphere, and a DC magnetometer to measure ULF-timescale variations of the magnetic field. BARREL will provide the first balloon measurements of relativistic electron precipitation while comprehensive in situ measurements of both plasma waves and energetic particles are available, and will characterize the spatial scale of precipitation at relativistic energies. All data and analysis software will be made freely available to the scientific community. C1 [Millan, R. M.; McGaw, D. G.; Woodger, L. A.; Anderson, B. A.; Knezek, N. R.; Scheiman, J. M.; Halford, A. J.; Hudson, M. K.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [McCarthy, M. P.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. [Sample, J. G.; Lin, R. P.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Sample, J. G.; Yando, K. B.; Lin, R. P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Smith, D. M.; Liang, A. X.; Rexroad, W. Z.; Bowers, G. S.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Thompson, L. D.] NASA, Wallops Flight Facil, Wallops Isl, VA 23337 USA. [Hewitt, J. G.] USAF Acad, Dept Phys DFP, Colorado Springs, CO 80840 USA. [Comess, M. D.] Space X, Hawthorne, CA 90250 USA. [Collier, A. B.] Univ Kwazulu Natal, Sch Phys, ZA-4001 Durban, South Africa. [Clilverd, M. A.] British Antarctic Survey, Cambridge CB3 0ET, England. [Lin, R. P.] Kyung Hee Univ, Sch Space Res, Yongin, South Korea. RP Millan, RM (reprint author), Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. EM Robyn.Millan@dartmouth.edu OI Anderson, Brett/0000-0001-5937-5497; Halford, Alexa/0000-0002-5383-4602 FU NASA Living With a Star program through NASA at Dartmouth College [NNX08AM58G]; Natural Environmental Research Council under the Antarctic Funding Initiative [AFI/11/22] FX BARREL is supported by the NASA Living With a Star program through NASA grant NNX08AM58G at Dartmouth College. Support for operations was provided by the Columbia Scientific Balloon Facility, the NASA Balloon Program Office, and the National Science Foundation's Office of Polar Programs. MAC has received funding from the Natural Environmental Research Council under the Antarctic Funding Initiative (AFI/11/22). The BARREL science campaigns were supported by NERC/British Antarctic Survey, SANSA Space Science, and the University of KwaZulu-Natal. NR 41 TC 21 Z9 21 U1 0 U2 10 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 NOV PY 2013 VL 179 IS 1-4 BP 503 EP 530 DI 10.1007/s11214-013-9971-z PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 244IM UT WOS:000326381300014 ER PT J AU Kessel, RL Fox, NJ Weiss, M AF Kessel, R. L. Fox, N. J. Weiss, M. TI The Radiation Belt Storm Probes (RBSP) and Space Weather SO SPACE SCIENCE REVIEWS LA English DT Review DE Space weather; Radiation Belt Storm Probes; RBSP; Geomagnetic storms ID TECHNOLOGIES AB Following the launch and commissioning of NASA's Radiation Belt Storm Probes (RBSP) in 2012, space weather data will be generated and broadcast from the spacecraft in near real-time. The RBSP mission targets one part of the space weather chain: the very high energy electrons and ions magnetically trapped within Earth's radiation belts. The understanding gained by RBSP will enable us to better predict the response of the radiation belts to solar storms in the future, and thereby protect space assets in the near-Earth environment. This chapter details the presently planned RBSP capabilities for generating and broadcasting near real-time space weather data, discusses the data products, the ground stations collecting the data, and the users/models that will incorporate the data into test-beds for radiation belt nowcasting and forecasting. C1 [Kessel, R. L.] NASA Headquarters, SMD, Heliophys Div, Washington, DC 20523 USA. [Fox, N. J.; Weiss, M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Fox, NJ (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM mona.kessel@nasa.gov; nicola.fox@jhuapl.edu RI Fox, Nicola/P-6692-2016 OI Fox, Nicola/0000-0003-3411-4228 NR 7 TC 18 Z9 18 U1 0 U2 6 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 NOV PY 2013 VL 179 IS 1-4 BP 531 EP 543 DI 10.1007/s11214-012-9953-6 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 244IM UT WOS:000326381300015 ER PT J AU DeWitt, C Bandyopadhyay, RM Eikenberry, SS Sellgren, K Blum, R Olsen, K Bauer, FE Sarajedini, A AF DeWitt, Curtis Bandyopadhyay, Reba M. Eikenberry, Stephen S. Sellgren, Kris Blum, Robert Olsen, Knut Bauer, Franz E. Sarajedini, Ata TI THREE NEW GALACTIC CENTER X-RAY SOURCES IDENTIFIED WITH NEAR-INFRARED SPECTROSCOPY SO ASTRONOMICAL JOURNAL LA English DT Article DE Galaxy: center; infrared: stars; X-rays: stars ID INTERSTELLAR EXTINCTION LAW; K-BAND SPECTROSCOPY; REPRESENTATIVE SAMPLE; COOL STARS; SPECTRAL CLASSIFICATION; SYMBIOTIC STARS; O SUPERGIANTS; POINT SOURCES; CENTER REGION; COUNTERPARTS AB We have conducted a near-infrared spectroscopic survey of 47 candidate counterparts to X-ray sources discovered by the Chandra X-Ray Observatory near the Galactic center (GC). Though a significant number of these astrometric matches are likely to be spurious, we sought out spectral characteristics of active stars and interacting binaries, such as hot, massive spectral types or emission lines, in order to corroborate the X-ray activity and certify the authenticity of the match. We present three new spectroscopic identifications, including a Be high-mass X-ray binary (HMXB) or a gamma Cassiopeiae (Cas) system, a symbiotic X-ray binary, and an O-type star of unknown luminosity class. The Be HMXB/gamma Cas system and the symbiotic X-ray binary are the first of their classes to be spectroscopically identified in the GC region. C1 [DeWitt, Curtis] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [DeWitt, Curtis] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [DeWitt, Curtis; Bandyopadhyay, Reba M.; Eikenberry, Stephen S.; Sarajedini, Ata] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Sellgren, Kris] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Blum, Robert; Olsen, Knut] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Bauer, Franz E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Bauer, Franz E.] Space Sci Inst, Boulder, CO 80301 USA. RP DeWitt, C (reprint author), Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. EM curtis.n.dewitt@nasa.gov FU CONICYT, Chile [FONDECYT 1101024, FONDAP (CATA) 15010003] FX F.E.B. acknowledges the support of CONICYT, Chile, under grants FONDECYT 1101024 and FONDAP (CATA) 15010003. NR 61 TC 2 Z9 2 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD NOV PY 2013 VL 146 IS 5 AR UNSP 109 DI 10.1088/0004-6256/146/5/109 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 238UK UT WOS:000325976200006 ER PT J AU Kane, SR Hinkel, NR Raymond, SN AF Kane, Stephen R. Hinkel, Natalie R. Raymond, Sean N. TI SOLAR SYSTEM MOONS AS ANALOGS FOR COMPACT EXOPLANETARY SYSTEMS SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: formation ID KEPLER PLANET CANDIDATES; SUN-LIKE STAR; IRREGULAR SATELLITES; SUPER-EARTHS; ECCENTRICITY DISTRIBUTION; GALILEAN SATELLITES; TERRESTRIAL PLANETS; TIMING VARIATIONS; TIDAL EVOLUTION; GIANT PLANETS AB The field of exoplanetary science has experienced a recent surge of new systems that is largely due to the precision photometry provided by the Kepler mission. The latest discoveries have included compact planetary systems in which the orbits of the planets all lie relatively close to the host star, which presents interesting challenges in terms of formation and dynamical evolution. The compact exoplanetary systems are analogous to the moons orbiting the giant planets in our solar system, in terms of their relative sizes and semimajor axes. We present a study that quantifies the scaled sizes and separations of the solar system moons with respect to their hosts. We perform a similar study for a large sample of confirmed Kepler planets in multi-planet systems. We show that a comparison between the two samples leads to a similar correlation between their scaled sizes and separation distributions. The different gradients of the correlations may be indicative of differences in the formation and/or long-term dynamics of moon and planetary systems. C1 [Kane, Stephen R.; Hinkel, Natalie R.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. [Kane, Stephen R.; Hinkel, Natalie R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Raymond, Sean N.] CNRS, UMR 5804, Lab Astrophys Bordeaux, F-33271 Floirac, France. [Raymond, Sean N.] Univ Bordeaux, Observ Aquitain Sci Univers, F-33271 Floirac, France. RP Kane, SR (reprint author), San Francisco State Univ, Dept Phys & Astron, 1600 Holloway Ave, San Francisco, CA 94132 USA. EM skane@ipac.caltech.edu FU National Science Foundation [AST-1109662] FX The authors would like to thank Jason Eastman, Gregory Laughlin, Philip Muirhead, and Jonathan Swift for insightful discussions. Thanks are also due to the anonymous referee, whose comments improved the quality of the 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. The authors acknowledge financial support from the National Science Foundation through grant AST-1109662. NR 77 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD NOV PY 2013 VL 146 IS 5 AR 122 DI 10.1088/0004-6256/146/5/122 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 238UK UT WOS:000325976200019 ER PT J AU Shaw, MS Filippenko, AV Romani, RW Cenko, SB Li, WD AF Shaw, Michael S. Filippenko, Alexei V. Romani, Roger W. Cenko, S. Bradley Li, Weidong TI PHOTOMETRICALLY TRIGGERED KECK SPECTROSCOPY OF FERMI BL LACERTAE OBJECTS SO ASTRONOMICAL JOURNAL LA English DT Article DE BL Lacertae objects: general; galaxies: active; gamma rays: galaxies; quasars: general; surveys ID OBSERVATORY SUPERNOVA SEARCH; LARGE-AREA TELESCOPE; AUTOMATIC IMAGING TELESCOPE; RAY BLAZAR CANDIDATES; SKY-SURVEY; OPTICAL SPECTROSCOPY; REDSHIFTS; SPECTRA; CATALOG; SAMPLE AB We report on Keck spectra of 10 Fermi blazars. J0622+3326, previously unobserved, is shown to be a flat-spectrum radio quasar at redshift z = 1.062. The others are known BL Lac type objects that have resisted previous attempts to secure redshifts. Using a photometric monitoring campaign with the 0.76m Katzman Automatic Imaging Telescope at Lick Observatory, we identified epochs when the relativistic jet emission was fainter than usual, thus triggering the Keck spectroscopy. This strategy gives improved sensitivity to stars and ionized gas in the host galaxy, thereby providing improved redshift constraints for seven of these sources. C1 [Shaw, Michael S.; Romani, Roger W.] Stanford Univ, Dept Phys, KIPAC, Stanford, CA 94305 USA. [Filippenko, Alexei V.; Cenko, S. Bradley; Li, Weidong] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Cenko, S. Bradley] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Shaw, MS (reprint author), Stanford Univ, Dept Phys, KIPAC, Stanford, CA 94305 USA. FU NASA [NNX10AU09G, GO-31089, NNX12AF12GA, NAS5-00147]; Richard and Rhoda Goldman Fund; TABASGO Foundation; NSF [AST-1211916] FX The work was supported in part by NASA grants NNX10AU09G, GO-31089, NNX12AF12GA, and NAS5-00147. A.V.F. and his group at U.C. Berkeley are also grateful for support from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia and Jim Katzman Foundation, and the TABASGO Foundation. 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 dedicate this paper to the memory of our dear friend and collaborator, Weidong Li, whose unfailing devotion to KAIT made this work possible; his premature, tragic passing has deeply saddened us. NR 34 TC 17 Z9 17 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD NOV PY 2013 VL 146 IS 5 AR UNSP 127 DI 10.1088/0004-6256/146/5/127 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 238UK UT WOS:000325976200024 ER PT J AU Appleton, PN Guillard, P Boulanger, F Cluver, ME Ogle, P Falgarone, E des Forets, GP O'Sullivan, E Duc, PA Gallagher, S Gao, Y Jarrett, T Konstantopoulos, I Lisenfeld, U Lord, S Lu, N Peterson, BW Struck, C Sturm, E Tuffs, R Valchanov, I van der Werf, P Xu, KC AF Appleton, P. N. Guillard, P. Boulanger, F. Cluver, M. E. Ogle, P. Falgarone, E. des Forets, G. Pineau O'Sullivan, E. Duc, P. -A. Gallagher, S. Gao, Y. Jarrett, T. Konstantopoulos, I. Lisenfeld, U. Lord, S. Lu, N. Peterson, B. W. Struck, C. Sturm, E. Tuffs, R. Valchanov, I. van der Werf, P. Xu, K. C. TI SHOCK-ENHANCED C+ EMISSION AND THE DETECTION OF H2O FROM THE STEPHAN'S QUINTET GROUP-WIDE SHOCK USING HERSCHEL SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: groups: individual (Stephan's Quintet); infrared: galaxies ID STAR-FORMING GALAXIES; SPECTRAL ENERGY-DISTRIBUTION; MOLECULAR-HYDROGEN EMISSION; RADIO-CONTINUUM EMISSION; INTERSTELLAR-MEDIUM; PHOTODISSOCIATION REGIONS; INFRARED-EMISSION; II LINE; X-RAY; TURBULENT DISSIPATION AB We present the first Herschel spectroscopic detections of the [O I] 63 mu m and [C II] 158 mu m fine-structure transitions, and a single para-H2O line from the 35 x 15 kpc(2) shocked intergalactic filament in Stephan's Quintet. The filament is believed to have been formed when a high-speed intruder to the group collided with a clumpy intergroup gas. Observations with the PACS spectrometer provide evidence for broad (>1000 km s(-1)) luminous [C II] line profiles, as well as fainter [O I] 63 mu m emission. SPIRE FTS observations reveal water emission from the p-H2O (1(11)-0(00)) transition at several positions in the filament, but no other molecular lines. The H2O line is narrow and may be associated with denser intermediate-velocity gas experiencing the strongest shock-heating. The [C II]/PAH(tot) and [C II]/FIR ratios are too large to be explained by normal photo-electric heating in photodissociation regions. H II region excitation or X-ray/cosmic-ray heating can also be ruled out. The observations lead to the conclusion that a large fraction the molecular gas is diffuse and warm. We propose that the [C II], [O I], and warm H-2 line emission is powered by a turbulent cascade in which kinetic energy from the galaxy collision with the intergalactic medium is dissipated to small scales and low velocities, via shocks and turbulent eddies. Low-velocity magnetic shocks can help explain both the [C II]/[O I] ratio, and the relatively high [C II]/H-2 ratios observed. The discovery that [C II] emission can be enhanced, in large-scale turbulent regions in collisional environments, has implications for the interpretation of [C II] emission in high-z galaxies. C1 [Appleton, P. N.; Lord, S.; Lu, N.; Xu, K. C.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. [Guillard, P.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Guillard, P.; Boulanger, F.; des Forets, G. Pineau] Univ Paris 11, Inst Astrophys Spatiale, Orsay, France. [Cluver, M. E.; Konstantopoulos, I.] Australian Astron Observ, Epping, NSW, Australia. [Ogle, P.] CALTECH, NASA Extragalact Database, IPAC, Pasadena, CA 91125 USA. [Falgarone, E.] Observ Paris, Ecole Normale Super, F-75231 Paris, France. [O'Sullivan, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Duc, P. -A.] Lab AIM, Paris, France. [Gallagher, S.] Univ Western Ontario, London, ON, Canada. [Gao, Y.] Purple Mt Observ, Nanjing, Jiangsu, Peoples R China. [Jarrett, T.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa. [Lisenfeld, U.] Univ Granada, Granada, Spain. [Peterson, B. W.] Univ Wisconsin Barron Cty, Rice Lake, WI 54868 USA. [Struck, C.] Iowa State Univ, Ames, IA 50011 USA. [Sturm, E.] Max Planck Inst Extraterr Phys, Munich, Germany. [Tuffs, R.] MPI Kernphys, Heidelberg, Germany. [Valchanov, I.] ESAC, Herschel Sci Ctr, Madrid, Spain. [van der Werf, P.] Leiden Univ, Leiden Observ, Leiden, Netherlands. RP Appleton, PN (reprint author), CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. EM apple@ipac.caltech.edu RI Lisenfeld, Ute/A-1637-2015; OI Lisenfeld, Ute/0000-0002-9471-5423; Konstantopoulos, Iraklis/0000-0003-2177-0146; Struck, Curtis/0000-0002-6490-2156; Appleton, Philip/0000-0002-7607-8766; Cluver, Michelle/0000-0002-9871-6490 FU NASA through JPL/Caltech FX P.N.A. acknowledges interesting discussions with P. Goldsmith and W. Langer (JPL) regarding [C II] emission in the Galaxy. This work is based on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. The authors thanks an anonymous referee for thoughtful comments on a previous version of the text. NR 79 TC 28 Z9 28 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 NOV 1 PY 2013 VL 777 IS 1 AR 66 DI 10.1088/0004-637X/777/1/66 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300066 ER PT J AU Boogert, ACA Chiar, JE Knez, C Oberg, KI Mundy, LG Pendleton, YJ Tielens, AGGM van Dishoeck, EF AF Boogert, A. C. A. Chiar, J. E. Knez, C. Oeberg, K. I. Mundy, L. G. Pendleton, Y. J. Tielens, A. G. G. M. van Dishoeck, E. F. TI INFRARED SPECTROSCOPIC SURVEY OF THE QUIESCENT MEDIUM OF NEARBY CLOUDS. I. ICE FORMATION AND GRAIN GROWTH IN LUPUS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: ISM; infrared: stars; ISM: abundances; ISM: molecules; stars: formation ID YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; LOW-MASS PROTOSTARS; MOLECULAR CLOUDS; DARK CLOUD; INTERSTELLAR EXTINCTION; SOLID CO; H-I; EVOLUTION; WATER AB Infrared photometry and spectroscopy (1-25 mu m) of background stars reddened by the Lupus molecular cloud complex are used to determine the properties of grains and the composition of ices before they are incorporated into circumstellar envelopes and disks. H2O ices form at extinctions of A(K) = 0.25 +/- 0.07 mag (A(V) = 2.1 +/- 0.6). Such a low ice formation threshold is consistent with the absence of nearby hot stars. Overall, the Lupus clouds are in an early chemical phase. The abundance of H2O ice (2.3 +/- 0.1 x 10(-5) relative to NH) is typical for quiescent regions, but lower by a factor of three to four compared to dense envelopes of young stellar objects. The low solid CH3OH abundance (<3%-8% relative to H2O) indicates a low gas phase H/CO ratio, which is consistent with the observed incomplete CO freeze out. Furthermore it is found that the grains in Lupus experienced growth by coagulation. The mid-infrared (>5 mu m) continuum extinction relative to A(K) increases as a function of A(K). Most Lupus lines of sight are well fitted with empirically derived extinction curves corresponding to R-V similar to 3.5 (A(K) = 0.71) and R-V similar to 5.0 (A(K) = 1.47). For lines of sight with A(K) > 1.0 mag, the tau(9.7)/A(K) ratio is a factor of two lower compared to the diffuse medium. Below 1.0 mag, values scatter between the dense and diffuse medium ratios. The absence of a gradual transition between diffuse and dense medium-type dust indicates that local conditions matter in the process that sets the tau(9.7)/A(K) ratio. This process is likely related to grain growth by coagulation, as traced by the A(7.4)/A(K) continuum extinction ratio, but not to ice mantle formation. Conversely, grains acquire ice mantles before the process of coagulation starts. C1 [Boogert, A. C. A.] CALTECH, NASA, Herschel Sci Ctr, IPAC, Pasadena, CA 91125 USA. [Chiar, J. E.] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA. [Knez, C.; Mundy, L. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Knez, C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Oeberg, K. I.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Oeberg, K. I.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Oeberg, K. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pendleton, Y. J.] NASA, Ames Res Ctr, Solar Syst Explorat Res Virtual Inst, Moffett Field, CA 94035 USA. [Tielens, A. G. G. M.; van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany. RP Boogert, ACA (reprint author), CALTECH, NASA, Herschel Sci Ctr, IPAC, Mail Code 100-22, Pasadena, CA 91125 USA. EM aboogert@ipac.caltech.edu FU National Aeronautics and Space Administration (NASA); NASA through JPL/Caltech; National Science Foundation FX We thank the anonymous referee for detailed comments that improved the presentation of the results. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory (JPL), California Institute of Technology (Caltech) under a contract with the National Aeronautics and Space Administration (NASA). Support for this work was provided by NASA through awards issued by JPL/Caltech to J.E.C. and C. K. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and JPL/Caltech, funded by NASA. 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/Caltech, funded by NASA and the National Science Foundation. NR 55 TC 12 Z9 12 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 NOV 1 PY 2013 VL 777 IS 1 AR 73 DI 10.1088/0004-637X/777/1/73 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300073 ER PT J AU Hemphill, PB Rothschild, RE Caballero, I Pottschmidt, K Kuhnel, M Furst, F Wilms, J AF Hemphill, Paul B. Rothschild, Richard E. Caballero, Isabel Pottschmidt, Katja Kuehnel, Matthias Fuerst, Felix Wilms, Joern TI MEASUREMENTS OF CYCLOTRON FEATURES AND PULSE PERIODS IN THE HIGH-MASS X-RAY BINARIES 4U 1538-522 AND 4U 1907+09 WITH THE INTERNATIONAL GAMMA-RAY ASTROPHYSICS LABORATORY SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: individual (4U 1538-522, 4U 1907+09); stars: magnetic field; stars: oscillations; X-rays: binaries; X-rays: stars ID OPTICAL SPECTROSCOPY; TORQUE REVERSAL; RESOLVED SPECTROSCOPY; SPIN-UP; ACCRETION; RXTE; 4U-1538-52; DISCOVERY; LINE; SPECTRUM AB We present a spectral and timing analysis of International Gamma-Ray Astrophysics Laboratory (INTEGRAL) observations of two high-mass X-ray binaries, 4U 1538-522 and 4U 1907+09. Our timing measurements for 4U 1538-522 find the pulse period to have exhibited a spin-up trend until approximately 2009, after which there is evidence for a torque reversal, with the source beginning to spin down to the most recently measured period of 525.407 +/- 0.001 s. The most recent INTEGRAL observations of 4U 1907+09 are not found to yield statistically significant pulse periods due to the significantly lower flux from the source compared with 4U 1538-522. A spectral model consisting of a power-law continuum with an exponential cutoff and modified by two cyclotron resonance scattering features is found to fit both sources well, with the cyclotron scattering features detected at similar to 22 and similar to 49 keV for 4U 1538-522 and at similar to 18 and similar to 36 keV for 4U 1907+09. The spectral parameters of 4U 1538-522 are generally not found to vary significantly with flux and there is little to no variation across the torque reversal. Examining our results in conjunction with previous work, we find no evidence for a correlation between cyclotron line energy and luminosity for 4U 1538-522. 4U 1907+09 shows evidence for a positive correlation between cyclotron line energy and luminosity, which would make it the fourth, and lowest luminosity, cyclotron line source to exhibit this relationship. C1 [Hemphill, Paul B.; Rothschild, Richard E.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Caballero, Isabel] Univ Paris 07, DSM IRFU SAp UMR AIM CNRS CEA 7158, CEA Saclay, F-91191 Gif Sur Yvette, France. [Pottschmidt, Katja] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Pottschmidt, Katja] CRESST, Greenbelt, MD 20771 USA. [Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Kuehnel, Matthias; Wilms, Joern] Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, D-96049 Bamberg, Germany. [Fuerst, Felix] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RP Hemphill, PB (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM pbhemphill@physics.ucsd.edu RI Wilms, Joern/C-8116-2013; OI Wilms, Joern/0000-0003-2065-5410; Hemphill, Paul/0000-0002-1676-6954 FU National Aeronautics and Space Administration [NNX09AT26G]; French Space Agency CNES though CNRS; ESA member states FX P.B.H. acknowledges support from the National Aeronautics and Space Administration grant NNX09AT26G. I. C. acknowledges financial support from the French Space Agency CNES though CNRS. This work is based on observations made by the INTEGRAL satellite, a European Space Agency (ESA) project funded by ESA member states. We also thank the Fermi GBM Pulsar Project for their extended monitoring of multiple pulsars. NR 64 TC 8 Z9 8 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 NOV 1 PY 2013 VL 777 IS 1 AR 61 DI 10.1088/0004-637X/777/1/61 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300061 ER PT J AU Inglis, AR Gilbert, HR AF Inglis, A. R. Gilbert, H. R. TI HARD X-RAY AND ULTRAVIOLET EMISSION DURING THE 2011 JUNE 7 SOLAR FLARE SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: flares; Sun: oscillations; Sun: X-rays, gamma rays ID QUASI-PERIODIC PULSATIONS; WHITE-LIGHT FLARES; MAGNETIC RECONNECTION; 2-RIBBON FLARES; OSCILLATORY RECONNECTION; SPECTROSCOPIC-IMAGER; PATCHY RECONNECTION; PROMINENCE MATERIAL; FOOTPOINT MOTIONS; ENERGY-RELEASE AB The relationship between X-ray and UV emission during flares, particularly in the context of quasi-periodic pulsations, remains unclear. To address this, we study the impulsive X-ray and UV emission during an eruptive flare on 2011 June 7 utilizing X-ray imaging from RHESSI and UV 1700 angstrom imaging from SDO/AIA. This event is associated with quasi-periodic pulsations in X-ray and possibly UV emission, as well as substantial parallel and perpendicular motion in the hard X-ray footpoints. The motion of the footpoints parallel to the flare ribbons is unusual; it reverses direction on at least two occasions. However, there is no associated short timescale motion of the UV bright regions. Over the same time interval, the footpoints also gradually move apart at v approximate to 12 km s(-1), consistent with the gradual outward expansion of the UV ribbons and the standard flare model. Additionally, we find that the locations of the brightest X-ray and UV regions are different, particularly during the early portion of the flare impulsive phase, despite their integrated emission being strongly correlated in time. Correlation analysis of measured flare properties, such as the footpoint separation, flare shear, photospheric magnetic field, and coronal reconnection rate, reveals that-in the impulsive phase-the 25-50 keV hard X-ray flux is only weakly correlated with these properties, in contrast with previous studies. We characterize this event in terms of long-term behavior, where the X-ray non-thermal, thermal, and UV emission sources appear temporally and spatially consistent, and short-term behavior, where the emission sources are inconsistent and quasi-periodic pulsations are a dominant feature requiring explanation. We suggest that the short timescale behavior of hard X-ray footpoints and the nature of the observed quasi-periodic pulsations are determined by fundamental, as yet unobserved properties of the reconnection region and particle acceleration sites. This presents a challenge for current three-dimensional flare reconnection models. C1 [Inglis, A. R.; Gilbert, H. R.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Solar Phys Lab, Greenbelt, MD 20771 USA. [Inglis, A. R.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Inglis, AR (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Solar Phys Lab, Greenbelt, MD 20771 USA. RI Inglis, Andrew/D-7674-2012 NR 71 TC 14 Z9 14 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2013 VL 777 IS 1 AR UNSP 30 DI 10.1088/0004-637X/777/1/30 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300030 ER PT J AU Jia, JJ Ptak, A Heckman, T Zakamska, NL AF Jia, Jianjun Ptak, Andrew Heckman, Timothy Zakamska, Nadia L. TI AN ARCHIVAL Chandra AND XMM-Newton SURVEY OF TYPE 2 QUASARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; quasars: general; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; SEYFERT 2 GALAXIES; HARD X-RAY; ULTRALUMINOUS INFRARED GALAXIES; II QUASARS; LUMINOSITY FUNCTION; OBSCURED QUASARS; HOST GALAXIES; EMISSION-LINE AB In order to investigate obscuration in high-luminosity type 2 active galactic nuclei (AGNs), we analyzed Chandra and XMM-Newton archival observations for 71 type 2 quasars detected at 0.05 < z < 0.73, which were selected based on their [O III] lambda 5007 emission lines. For 54 objects with good spectral fits, the observed hard X-ray luminosity ranges from 2 x 10(41) to 5.3 x 10(44) erg s(-1), with a median of 1.1 x 10(43) erg s(-1). We find that the means of the column density and photon index of our sample are log N-H = 22.9 cm(-2) and Gamma = 1.87, respectively. From simulations using a more physically realistic model, we find that the absorbing column density estimates based on simple power-law models significantly underestimate the actual absorption in approximately half of the sources. Eleven sources show a prominent Fe K alpha emission line (EW>100 eV in the rest frame) and we detect this line in the other sources through a joint fit (spectral stacking). The correlation between the Fe K alpha and [O III] fluxes and the inverse correlation of the equivalent width of the Fe K alpha line with the ratio of hard X-ray and [O III] fluxes is consistent with previous results for lower luminosity Seyfert 2 galaxies. We conclude that obscuration is the cause of the weak hard X-ray emission rather than intrinsically low X-ray luminosities. We find that about half of the population of optically selected type 2 quasars are likely to be Compton thick. We also find no evidence that the amount of X-ray obscuration depends on the AGN luminosity (over a range of more than three orders of magnitude in luminosity). C1 [Jia, Jianjun; Heckman, Timothy; Zakamska, Nadia L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Ptak, Andrew] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Jia, JJ (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. NR 69 TC 18 Z9 18 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 NOV 1 PY 2013 VL 777 IS 1 AR 27 DI 10.1088/0004-637X/777/1/27 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300027 ER PT J AU Lee, CF Sahai, R Contreras, CS Huang, PS Tay, JJH AF Lee, Chin-Fei Sahai, Raghvendra Sanchez Contreras, Carmen Huang, Po-Sheng Tay, Jeremy Jian Hao TI MULTIPLE FAST MOLECULAR OUTFLOWS IN THE PRE-PLANETARY NEBULA CRL 618 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary nebulae: general; stars: AGB and post-AGB; stars: individual (CRL 618); stars: mass-loss ID HUBBLE-SPACE-TELESCOPE; PLANETARY-NEBULAE; COLLIMATED OUTFLOWS; PHYSICAL STRUCTURE; PROTOPLANETARY; JETS; CRL-618; SPECTROSCOPY; EXPLOSIONS; ENVELOPE AB CRL 618 is a well-studied pre-planetary nebula. It has multiple highly collimated optical lobes, fast molecular outflows along the optical lobes, and an extended molecular envelope that consists of a dense torus in the equator and a tenuous round halo. Here we present our observations of this source in CO J = 3-2 and HCN J = 4-3 obtained with the Submillimeter Array at up to similar to 0 ''.3 resolutions. We spatially resolve the fast molecular outflow region previously detected in CO near the central star and find it to be composed of multiple outflows that have similar dynamical ages and are oriented along the different optical lobes. We also detect fast molecular outflows further away from the central star near the tips of the extended optical lobes and a pair of equatorial outflows inside the dense torus. We find that two episodes of bullet ejections in different directions are needed, one producing the fast molecular outflows near the central star and one producing the fast molecular outflows near the tips of the extended optical lobes. One possibility to launch these bullets is a magneto-rotational explosion of the stellar envelope. C1 [Lee, Chin-Fei; Huang, Po-Sheng] Acad Sinica Inst Astron & Astrophys, Taipei 106, Taiwan. [Sahai, Raghvendra] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sanchez Contreras, Carmen] Astrobiol Ctr CSIC INTA, E-28691 Madrid, Spain. [Tay, Jeremy Jian Hao] Natl Univ Singapore, Dept Phys, Singapore 117542, Singapore. RP Lee, CF (reprint author), Acad Sinica Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. RI Sanchez-Contreras, Carmen/N-3718-2015 OI Sanchez-Contreras, Carmen/0000-0002-6341-592X FU National Science Council of Taiwan [NSC 99-2112-M-001-007-MY2, NSC 101-2119-M-001-002-MY3]; Academia Sinica; NASA; Spanish MICINN/MINECO [AYA2009-07304, AYA2012-32032]; CONSOLIDER INGENIO [CDS2009-00038] FX We thank the anonymous referee for valuable suggestions. We thank the SMA staff for their efforts in running and maintaining the array. C.-F. Lee and P.-S. Huang acknowledge grants from the National Science Council of Taiwan (NSC 99-2112-M-001-007-MY2 and NSC 101-2119-M-001-002-MY3) and the Academia Sinica (Career Development Award). R.S.'s contribution to the research described here was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. C. S. C. has been partially supported by the Spanish MICINN/MINECO through grants AYA2009-07304, AYA2012-32032, and CONSOLIDER INGENIO 2010 for the team "Molecular Astrophysics: The Herschel and ALMA Era - ASTROMOL" (ref.: CDS2009-00038). NR 31 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 NOV 1 PY 2013 VL 777 IS 1 AR 37 DI 10.1088/0004-637X/777/1/37 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300037 ER PT J AU Leutenegger, MA Cohen, DH Sundqvist, JO Owocki, SP AF Leutenegger, Maurice A. Cohen, David H. Sundqvist, Jon O. Owocki, Stanley P. TI CONSTRAINTS ON POROSITY AND MASS LOSS IN O-STAR WINDS FROM MODELING OF X-RAY EMISSION LINE PROFILE SHAPES (vol 770, pg 80, 2013) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Leutenegger, Maurice A.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Leutenegger, Maurice A.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Leutenegger, Maurice A.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Cohen, David H.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [Sundqvist, Jon O.; Owocki, Stanley P.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Sundqvist, Jon O.] Univ Sternwarte Munchen, D-81679 Munich, Germany. RP Leutenegger, MA (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. EM Maurice.A.Leutenegger@nasa.gov NR 4 TC 0 Z9 0 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 NOV 1 PY 2013 VL 777 IS 1 AR 81 DI 10.1088/0004-637X/777/1/81 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300081 ER PT J AU Mace, GN Kirkpatrick, JD Cushing, MC Gelino, CR McLean, IS Logsdon, SE Wright, EL Skrutskie, MF Beichman, CA Eisenhardt, PR Kulas, KR AF Mace, Gregory N. Kirkpatrick, J. Davy Cushing, Michael C. Gelino, Christopher R. McLean, Ian S. Logsdon, Sarah E. Wright, Edward L. Skrutskie, Michael F. Beichman, Charles A. Eisenhardt, Peter R. Kulas, Kristin R. TI THE EXEMPLAR T8 SUBDWARF COMPANION OF WOLF 1130 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; brown dwarfs; stars: individual (Wolf 1130, WISE J200520.38+542433.9); stars: low-mass ID INFRARED-SURVEY-EXPLORER; SPITZER-SPACE-TELESCOPE; KECK II TELESCOPE; DWARF SPECTROSCOPIC SURVEY; EXOPLANET HOST STAR; COLD BROWN DWARFS; LARGE-AREA SURVEY; NEARBY M-DWARFS; ALL-SKY SURVEY; LOW-MASS STARS AB We have discovered a wide separation (188 ''.5) T8 subdwarf companion to the sdM1.5+WD binary Wolf 1130. Companionship of WISE J200520.38+ 542433.9 is verified through common proper motion over a similar to 3 yr baseline. Wolf 1130 is located 15.83 +/- 0.96 pc from the Sun, placing the brown dwarf at a projected separation of similar to 3000 AU. Near-infrared colors and medium resolution (R approximate to 2000-4000) spectroscopy establish the uniqueness of this system as a high-gravity, low-metallicity benchmark. Although there are a number of low-metallicity T dwarfs in the literature, WISE J200520.38+ 542433.9 has the most extreme inferred metallicity to date with [Fe/H] = -0.64 +/- 0.17 based on Wolf 1130. Model comparisons to this exemplar late-type subdwarf support it having an old age, a low metallicity, and a small radius. However, the spectroscopic peculiarities of WISE J200520.38+ 542433.9 underscore the importance of developing the low-metallicity parameter space of the most current atmospheric models. C1 [Mace, Gregory N.; McLean, Ian S.; Logsdon, Sarah E.; Wright, Edward L.; Kulas, Kristin R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Mace, Gregory N.; Kirkpatrick, J. Davy; Gelino, Christopher R.; Beichman, Charles A.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Cushing, Michael C.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Skrutskie, Michael F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Eisenhardt, Peter R.] NASA Jet Prop Lab, Pasadena, CA 91109 USA. RP Mace, GN (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, 430 Portola Plaza,Box 951547, Los Angeles, CA 90095 USA. EM gmace@astro.ucla.edu FU National Aeronautics and Space Administration; National Science Foundation (NASA); NASA [NAS 5-26555]; NASA through issued by JPL/Caltech [70062]; NASA through a grant from the STScI [12330]; W.M. Keck 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 (UC), Los Angeles, and the Jet Propulsion Laboratory (JPL)/California Institute of Technology (Caltech), funded by the National Aeronautics and Space Administration. We thank the Infrared Processing and Analysis Center (IRAC) at Caltech for funds provided by the Visiting Graduate Fellowship for G.N.M. This publication also makes use of data products from 2MASS. 2MASS is a joint project of the University of Massachusetts and IPAC/Caltech, funded by the National Aeronautics and Space Administration and the National Science Foundation (NASA). This research has made use of the NASA/IPAC Infrared Science Archive (IRSA), which is operated by JPL, Caltech, under contract with NASA. Our research has benefited from the M, L, and T dwarf compendium housed at http://DwarfArchives.org, whose server was funded by a NASA Small Research Grant, administered by the American Astronomical Society. The Brown Dwarf Spectroscopic Survey (BDSS) is hosted by UCLA and provided an essential comparison library for our moderate-resolution spectroscopy. This research has benefited from the SpeX Prism Spectral Libraries, maintained by Adam Burgasser at http://pono.ucsd.edu/similar to adam/browndwarfs/spexprism. We are also indebted to the SIMBAD database, operated at CDS, Strasbourg, France. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by JPL, Caltech, under a contract with NASA. Support for this work was provided by NASA through an award issued to program 70062 by JPL/Caltech. This work is also based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program 12330. Support for program 12330 was provided by NASA through a grant from the STScI. The Keck/OSIRIS observations were supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. The spectroscopic data presented herein were obtained at the Keck Observatory, which is operated as a scientific partnership among Caltech, UC and NASA. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. In acknowledgement of our observing time at Keck we further wish to recognize 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. We thank the anonymous referee for detailed and thoughtful recommendations to improve this paper prior to publication. NR 109 TC 14 Z9 14 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 NOV 1 PY 2013 VL 777 IS 1 AR 36 DI 10.1088/0004-637X/777/1/36 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300036 ER PT J AU Marion, GH Vinko, J Wheeler, JC Foley, RJ Hsiao, EY Brown, PJ Challis, P Filippenko, AV Garnavich, P Kirshner, RP Landsman, WB Parrent, JT Pritchard, TA Roming, PWA Silverman, JM Wang, XF AF Marion, G. H. Vinko, Jozsef Wheeler, J. Craig Foley, Ryan J. Hsiao, Eric Y. Brown, Peter J. Challis, Peter Filippenko, Alexei V. Garnavich, Peter Kirshner, Robert P. Landsman, Wayne B. Parrent, Jerod T. Pritchard, Tyler A. Roming, Peter W. A. Silverman, Jeffrey M. Wang, Xiaofeng TI HIGH-VELOCITY LINE FORMING REGIONS IN THE TYPE Ia SUPERNOVA 2009ig SO ASTROPHYSICAL JOURNAL LA English DT Article DE line: formation; line: identification; supernovae: general; supernovae: individual (SN 2009ig) ID HOBBY-EBERLY TELESCOPE; IMPROVED DISTANCES; SN 2001EL; SPECTRA; FEATURES; SPECTROSCOPY; EJECTA; RESOLUTION; SPECTROPOLARIMETRY; SPECTROGRAPH AB We report measurements and analysis of high-velocity (HVF) (>20,000 km s(-1)) and photospheric absorption features in a series of spectra of the Type Ia supernova (SN) 2009ig obtained between -14 days and +13 days with respect to the time of maximum B-band luminosity (B-max). We identify lines of Si II, Si III, S II, Ca II, and Fe II that produce both HVF and photospheric-velocity (PVF) absorption features. SN 2009ig is unusual for the large number of lines with detectable HVF in the spectra, but the light-curve parameters correspond to a slightly overluminous but unexceptional SN Ia (M-B = -19.46 mag and Delta m(15)(B) = 0.90 mag). Similarly, the Si II lambda 6355 velocity at the time of B-max is greater than "normal" for an SN Ia, but it is not extreme (upsilon(Si) = 13,400 km s(-1)). The -14 days and -13 days spectra clearly resolve HVF from Si II lambda 6355 as separate absorptions from a detached line forming region. At these very early phases, detached HVF are prevalent in all lines. From -12 days to -6 days, HVF and PVF are detected simultaneously, and the two line forming regions maintain a constant separation of about 8000 km s(-1). After -6 days all absorption features are PVF. The observations of SN 2009ig provide a complete picture of the transition from HVF to PVF. Most SNe Ia show evidence for HVF from multiple lines in spectra obtained before -10 days, and we compare the spectra of SN 2009ig to observations of other SNe. We show that each of the unusual line profiles for Si II lambda 6355 found in early-time spectra of SNe Ia correlate to a specific phase in a common development sequence from HVF to PVF. C1 [Marion, G. H.; Foley, Ryan J.; Challis, Peter; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marion, G. H.; Vinko, Jozsef; Wheeler, J. Craig; Silverman, Jeffrey M.] Univ Texas Austin, Austin, TX 78712 USA. [Vinko, Jozsef] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. [Hsiao, Eric Y.] Carnegie Observat, Campanas Observ, Colina El Pino, Casilla 601, Chile. [Brown, Peter J.; Wang, Xiaofeng] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, College Stn, TX 77843 USA. [Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Garnavich, Peter] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Landsman, Wayne B.] NASA, Goddard Space Flight Ctr, Adnet Syst, Greenbelt, MD 20771 USA. [Parrent, Jerod T.] Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Parrent, Jerod T.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Pritchard, Tyler A.; Roming, Peter W. A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Roming, Peter W. A.] SW Res Inst, Space Sci & Engn Div, San Antonio, TX 78228 USA. [Wang, Xiaofeng] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Wang, Xiaofeng] Tsinghua Univ, Tsinghua Ctr Astrophys THCA, Beijing 100084, Peoples R China. RP Marion, GH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gmarion@cfa.harvard.edu RI Wang, Xiaofeng/J-5390-2015 FU Hungarian OTKA Grants [K-76816, NN-107637]; NSF [AST-0707769, AST-1211196, AST-1008343, AST-1211916]; Texas Advanced Research Project [ARP-009]; Natural Science Foundation of China [NSFC 11178003, 11073013]; China-973 Program [2009CB824800]; TABASGO Foundation; Christopher R. Redlich Fund FX The authors wish to thank the Chairmen of the TACs from the University of Texas and Penn State University for providing Director's discretionary time for the HET/LRS observations. G. H. M. thanks Nick Suntzeff and Rob Robinson for insightful comments. G. H. M. also thanks Mark Phillips for providing perspective, as well as Michael Childress for helpful discussions and for sharing an advance copy of his paper on SN 2012fr. We thank Mark Sullivan, Isobel Hook, Peter Nugent, Andy Howell, and Bill Vacca for sharing their own data on line profiles in young SNe Ia. The authors make frequent use of David Bishop's excellent Web site listing recent supernovae and valuable references associated with them: http://www.rochesterastronomy.org/snimages/. J.V. is supported by Hungarian OTKA Grants K-76816 and NN-107637, NSF grant AST-0707769, and Texas Advanced Research Project ARP-009. The research of J.C.W. in supported in part by NSF grant AST-1109801. The CfA Supernova Program is supported by NSF grant AST-1211196 to the Harvard College Observatory. X. Wang is supported by the Natural Science Foundation of China (NSFC 11178003, 11073013), the China-973 Program 2009CB824800, and NSF grant AST-0708873 (through L. Wang). E.Y.H. is supported by NSF grant AST-1008343. A. V. F. is grateful for financial assistance from NSF grant AST-1211916, the TABASGO Foundation, and the Christopher R. Redlich Fund. We greatly appreciate the valuable assistance provided by staff members at the observatories where SN 2009ig was observed. NR 57 TC 20 Z9 20 U1 0 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 NOV 1 PY 2013 VL 777 IS 1 AR 40 DI 10.1088/0004-637X/777/1/40 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300040 ER PT J AU Medezinski, E Umetsu, K Nonino, M Merten, J Zitrin, A Broadhurst, T Donahue, M Sayers, J Waizmann, JC Koekemoer, A Coe, D Molino, A Melchior, P Mroczkowski, T Czakon, N Postman, M Meneghetti, M Lemze, D Ford, H Grillo, C Kelson, D Bradley, L Moustakas, J Bartelmann, M Benitez, N Biviano, A Bouwens, R Golwala, S Graves, G Infante, L Jimenez-Teja, Y Jouvel, S Lahav, O Moustakas, L Ogaz, S Rosati, P Seitz, S Zheng, W AF Medezinski, Elinor Umetsu, Keiichi Nonino, Mario Merten, Julian Zitrin, Adi Broadhurst, Tom Donahue, Megan Sayers, Jack Waizmann, Jean-Claude Koekemoer, Anton Coe, Dan Molino, Alberto Melchior, Peter Mroczkowski, Tony Czakon, Nicole Postman, Marc Meneghetti, Massimo Lemze, Doron Ford, Holland Grillo, Claudio Kelson, Daniel Bradley, Larry Moustakas, John Bartelmann, Matthias Benitez, Narciso Biviano, Andrea Bouwens, Rychard Golwala, Sunil Graves, Genevieve Infante, Leopoldo Jimenez-Teja, Yolanda Jouvel, Stephanie Lahav, Ofer Moustakas, Leonidas Ogaz, Sara Rosati, Piero Seitz, Stella Zheng, Wei TI CLASH: COMPLETE LENSING ANALYSIS OF THE LARGEST COSMIC LENS MACS J0717.5+3745 AND SURROUNDING STRUCTURES SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; dark matter; galaxies: clusters: individual (MACS J0717.5+3745); gravitational lensing: strong; gravitational lensing: weak ID MASSIVE GALAXY CLUSTERS; ZELDOVICH EFFECT OBSERVATIONS; EXTREME-VALUE STATISTICS; DEEP ADVANCED CAMERA; DARK-MATTER HALOS; X-RAY-CLUSTERS; SUNYAEV-ZELDOVICH; LAMBDA-CDM; OBSERVED GROWTH; MERGING CLUSTER AB The galaxy cluster MACS J0717.5+3745 (z = 0.55) is the largest known cosmic lens, with complex internal structures seen in deep X-ray, Sunyaev-Zel'dovich effect, and dynamical observations. We perform a combined weak-and strong-lensing analysis with wide-field BVR(c)i'z' Subaru/Suprime-Cam observations and 16-band Hubble Space Telescope observations taken as part of the Cluster Lensing And Supernova survey with Hubble. We find consistent weak distortion and magnification measurements of background galaxies and combine these signals to construct an optimally estimated radial mass profile of the cluster and its surrounding large-scale structure out to 5 Mpc h(-1). We find consistency between strong-lensing and weak-lensing in the region where these independent data overlap, <500 kpc h(-1). The two-dimensional weak-lensing map reveals a clear filamentary structure traced by distinct mass halos. We model the lensing shear field with nine halos, including the main cluster, corresponding to mass peaks detected above 2.5 sigma(kappa). The total mass of the cluster as determined by the different methods is M-vir approximate to (2.8 +/- 0.4) x 10(15) M-circle dot. Although this is the most massive cluster known at z > 0.5, in terms of extreme value statistics, we conclude that the mass of MACS J0717.5+3745 by itself is not in serious tension with Lambda CDM, representing only a similar to 2 sigma departure above the maximum simulated halo mass at this redshift. C1 [Medezinski, Elinor; Lemze, Doron; Ford, Holland; Zheng, Wei] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Umetsu, Keiichi] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Nonino, Mario; Biviano, Andrea] INAF Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Merten, Julian; Mroczkowski, Tony; Moustakas, Leonidas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zitrin, Adi; Bartelmann, Matthias] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Broadhurst, Tom; Jimenez-Teja, Yolanda] Univ Basque Country UPV EHU, Dept Theoret Phys & Hist Sci, E-48080 Bilbao, Spain. [Broadhurst, Tom] Basque Fdn Sci, Ikerbasque, E-48011 Bilbao, Spain. [Donahue, Megan] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Sayers, Jack; Mroczkowski, Tony; Czakon, Nicole; Golwala, Sunil] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Waizmann, Jean-Claude; Meneghetti, Massimo] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Koekemoer, Anton; Coe, Dan; Postman, Marc; Bradley, Larry; Ogaz, Sara] Space Telescope Sci Inst, Baltimore, MD 21208 USA. [Molino, Alberto; Benitez, Narciso] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Melchior, Peter] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Melchior, Peter] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Grillo, Claudio] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Kelson, Daniel] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Moustakas, John] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. [Bouwens, Rychard] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Graves, Genevieve] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Infante, Leopoldo] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Ctr Astroingn, Santiago 4860, Chile. [Jouvel, Stephanie] Inst Ciencies Espai IEEC CSIC, E-08193 Bellaterra, Barcelona, Spain. [Lahav, Ofer] Univ London Univ Coll, Dept Phys & Astron, London WC1E 6BT, England. [Rosati, Piero] European So Observ, D-85748 Garching, Germany. [Seitz, Stella] Univ Sternwarte, D-81679 Munich, Germany. RP Medezinski, E (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA. EM elinor@pha.jhu.edu RI Bartelmann, Matthias/A-5336-2014; Molino Benito, Alberto/F-5298-2014; Jimenez-Teja, Yolanda/D-5933-2011; Grillo, Claudio/E-6223-2015; Meneghetti, Massimo/O-8139-2015; OI Grillo, Claudio/0000-0002-5926-7143; Koekemoer, Anton/0000-0002-6610-2048; Meneghetti, Massimo/0000-0003-1225-7084; Nonino, Mario/0000-0001-6342-9662; Mroczkowski, Tony/0000-0003-3816-5372; Umetsu, Keiichi/0000-0002-7196-4822; Biviano, Andrea/0000-0002-0857-0732; Moustakas, Leonidas/0000-0003-3030-2360; Benitez, Narciso/0000-0002-0403-7455 FU NASA [NAS 5-26555, NAS 5-32864, HST-GO-12065.01-A, PF0-110077]; National Science Council of Taiwan [NSC100-2112-M-001-008-MY3]; Academia Sinica Career Development Award; Gordon and Betty Moore Foundation; NASA Graduate Student Research Fellowship; "Internationale Spitzenforschung II/2" of the Baden-Wurttemberg Stiftung; PRIN-INAF; [NSF/AST0838261]; [NASA/NNX11AB07G] FX The CLASH Multi-Cycle Treasury Program is based on observations made with the NASA/ESA Hubble Space Telescope. The Space Telescope Science Institute is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. ACS was developed under NASA contract NAS 5-32864. E. M. is supported by NASA grant HST-GO-12065.01-A. K. U. acknowledges partial support from the National Science Council of Taiwan (grant NSC100-2112-M-001-008-MY3) and from the Academia Sinica Career Development Award. The Bolocam observations were partially supported by the Gordon and Betty Moore Foundation. This material is based upon work at the Caltech Submillimeter Observatory, which is operated by the California Institute of Technology under cooperative agreement with the National Science Foundation (AST-0838261). J.S. is supported by NSF/AST0838261 and NASA/NNX11AB07G. N.C. is partially supported by a NASA Graduate Student Research Fellowship. A.Z. is supported by the "Internationale Spitzenforschung II/2" of the Baden-Wurttemberg Stiftung. T. M. is provided by NASA through the Einstein Fellowship Program, grant PF0-110077. This research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. M.N. acknowledges support from PRIN-INAF 2010. NR 152 TC 46 Z9 46 U1 1 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2013 VL 777 IS 1 AR 43 DI 10.1088/0004-637X/777/1/43 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300043 ER PT J AU Milligan, RO McElroy, SA AF Milligan, Ryan O. McElroy, Sarah A. TI CONTINUUM CONTRIBUTIONS TO THE SDO/AIA PASSBANDS DURING SOLAR FLARES SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: flares; Sun: UV radiation ID TRANSITION REGION; CORONAL EXPLORER; ATOMIC DATABASE; EMISSION-LINES; PLASMA; DIAGNOSTICS; ANGSTROM; RHESSI; SDO; WAVELENGTHS AB Data from the Multiple EUV Grating Spectrograph component of the Extreme-ultraviolet Variability Experiment (EVE) on board the Solar Dynamics Observatory (SDO) were used to quantify the contribution of continuum emission to each of the extreme ultraviolet (EUV) channels of the Atmospheric Imaging Assembly (AIA), also on SDO, during an X-class solar flare that occurred on 2011 February 15. Both the pre-flare-subtracted EVE spectra and fits to the associated free-free continuum were convolved with the AIA response functions of the seven EUV passbands at 10 s cadence throughout the course of the flare. It was found that 10%-25% of the total emission in the 94 angstrom, 131 angstrom, 193 angstrom, and 335 angstrom passbands throughout the main phase of the flare was due to free-free emission. Reliable measurements could not be made for the 171 angstrom channel, while the continuum contribution to the 304 angstrom channel was negligible due to the presence of the strong He II emission line. Up to 50% of the emission in the 211 angstrom channel was found to be due to free-free emission around the peak of the flare, while an additional 20% was due to the recombination continuum of He II. The analysis was extended to a number of M-and X-class flares and it was found that the level of free-free emission contributing to both the 171 angstrom and 211 angstrom passbands increased with increasing GOES class. These results suggest that the amount of continuum emission that contributes to AIA observations during flares is more significant than stated in previous studies which used synthetic, rather than observed, spectra. These findings highlight the importance of spectroscopic observations carried out in conjunction with those from imaging instruments so that the data are interpreted correctly. C1 [Milligan, Ryan O.; McElroy, Sarah A.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Milligan, Ryan O.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Milligan, Ryan O.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Solar Phys Lab Code 671, Greenbelt, MD 20771 USA. RP Milligan, RO (reprint author), Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Univ Rd, Belfast BT7 1NN, Antrim, North Ireland. EM r.milligan@qub.ac.uk FU Leverhulme Trust [F/00203/X]; NASA [NNX11AQ53G] FX The authors would like to thank Professor Mihalis Mathioudakis for useful and insightful discussions on this work, as well as financial support and constructive feedback on the manuscript, and to Dr. Dean Pesnell for informing us of the updated response functions. The anonymous referee also provided very constructive feedback which greatly improved the scope of this paper. 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. NR 27 TC 6 Z9 6 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 NOV 1 PY 2013 VL 777 IS 1 AR 12 DI 10.1088/0004-637X/777/1/12 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300012 ER PT J AU Sahraoui, F Huang, SY Belmont, G Goldstein, ML Retino, A Robert, P De Patoul, J AF Sahraoui, F. Huang, S. Y. Belmont, G. Goldstein, M. L. Retino, A. Robert, P. De Patoul, J. TI SCALING OF THE ELECTRON DISSIPATION RANGE OF SOLAR WIND TURBULENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE plasmas; solar wind; turbulence ID WEAKLY COLLISIONAL PLASMAS; CLUSTER MISSION; SCALES; FLUCTUATIONS; SPECTRUM; CASCADE; AU AB Electron scale solar wind (SW) turbulence has attracted great interest in recent years. Considerable evidence exists that the turbulence is not fully dissipated near the proton scale, but continues cascading down to electron scales. However, the scaling of the magnetic energy spectra as well as the nature of the plasma modes involved at those small scales are still not fully determined. Here we survey 10 yr of the Cluster STAFF search-coil magnetometer waveforms measured in the SW and perform a statistical study of the magnetic energy spectra in the frequency range [1, 180] Hz. We found that 75% of the analyzed spectra exhibit breakpoints near the electron gyroscale rho e, followed by steeper power-law-like spectra. We show that the scaling below the electron breakpoint cannot be determined unambiguously due to instrumental limitations that we discuss in detail. We compare our results to those reported in other studies and discuss their implications for the physical mechanisms involved and for theoretical modeling of energy dissipation in the SW. C1 [Sahraoui, F.; Belmont, G.; Retino, A.; Robert, P.; De Patoul, J.] UPMC, CNRS, Ecole Polytech, Lab Phys Plasmas, F-92120 Palaiseau, France. [Huang, S. Y.] Wuhan Univ, Sch Elect & Informat, Wuhan 430072, Peoples R China. [Goldstein, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sahraoui, F (reprint author), UPMC, CNRS, Ecole Polytech, Lab Phys Plasmas, Route Saclay, F-92120 Palaiseau, France. EM fouad.sahraoui@lpp.polytechnique.fr FU L'Agence Nationale de la Recherche (ANR, France); ANR grant FX This work is part of the project THESOW funded by L'Agence Nationale de la Recherche (ANR, France). J. De Patoul is funded through the ANR grant. The FGM, CIS, and PEACE data come from the CAA (ESA) and AMDA (CDPP, IRAP, France). FS thanks O. Gurcan and N. Cornilleau-Wehrlin for fruitful discussions and P. Canu for providing the WHISPER data. NR 41 TC 40 Z9 40 U1 1 U2 19 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2013 VL 777 IS 1 AR 15 DI 10.1088/0004-637X/777/1/15 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300015 ER PT J AU Sandstrom, KM Leroy, AK Walter, F Bolatto, AD Croxall, KV Draine, BT Wilson, CD Wolfire, M Calzetti, D Kennicutt, RC Aniano, G Meyer, JD Usero, A Bigiel, F Brinks, E de Blok, WJG Crocker, A Dale, D Engelbracht, CW Galametz, M Groves, B Hunt, LK Koda, J Kreckel, K Linz, H Meidt, S Pellegrini, E Rix, HW Roussel, H Schinnerer, E Schruba, A Schuster, KF Skibba, R van der Laan, T Appleton, P Armus, L Brandl, B Gordon, K Hinz, J Krause, O Montiel, E Sauvage, M Schmiedeke, A Smith, JDT Vigroux, L AF Sandstrom, K. M. Leroy, A. K. Walter, F. Bolatto, A. D. Croxall, K. V. Draine, B. T. Wilson, C. D. Wolfire, M. Calzetti, D. Kennicutt, R. C. Aniano, G. Meyer, J. Donovan Usero, A. Bigiel, F. Brinks, E. de Blok, W. J. G. Crocker, A. Dale, D. Engelbracht, C. W. Galametz, M. Groves, B. Hunt, L. K. Koda, J. Kreckel, K. Linz, H. Meidt, S. Pellegrini, E. Rix, H. -W. Roussel, H. Schinnerer, E. Schruba, A. Schuster, K. -F. Skibba, R. van der Laan, T. Appleton, P. Armus, L. Brandl, B. Gordon, K. Hinz, J. Krause, O. Montiel, E. Sauvage, M. Schmiedeke, A. Smith, J. D. T. Vigroux, L. TI THE CO-TO-H-2 CONVERSION FACTOR AND DUST-TO-GAS RATIO ON KILOPARSEC SCALES IN NEARBY GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies: ISM; infrared: ISM; ISM: molecules ID GIANT MOLECULAR CLOUDS; POLYCYCLIC AROMATIC-HYDROCARBONS; VIOLENT STAR-FORMATION; GAMMA-RAY EMISSION; SPIRAL GALAXIES; GALACTIC-CENTER; DWARF GALAXIES; X-FACTOR; PHOTODISSOCIATION REGIONS; INFRARED-EMISSION AB We present similar to kiloparsec spatial resolution maps of the CO-to-H-2 conversion factor (alpha(CO)) and dust-to-gas ratio (DGR) in 26 nearby, star-forming galaxies. We have simultaneously solved for alpha(CO) and the DGR by assuming that the DGR is approximately constant on kiloparsec scales. With this assumption, we can combine maps of dust mass surface density, CO-integrated intensity, and H I column density to solve for both alpha(CO) and the DGR with no assumptions about their value or dependence on metallicity or other parameters. Such a study has just become possible with the availability of high-resolution far-IR maps from the Herschel key program KINGFISH, (CO)-C-12 J = (2-1) maps from the IRAM 30 m large program HERACLES, and H I 21 cm line maps from THINGS. We use a fixed ratio between the (2-1) and (1-0) lines to present our alpha(CO) results on the more typically used (CO)-C-12 J = (1-0) scale and show using literature measurements that variations in the line ratio do not affect our results. In total, we derive 782 individual solutions for alpha(CO) and the DGR. On average, alpha(CO) = 3.1M(circle dot) pc(-2) (K km s(-1))(-1) for our sample with a standard deviation of 0.3 dex. Within galaxies, we observe a generally flat profile of alpha(CO) as a function of galactocentric radius. However, most galaxies exhibit a lower alpha(CO) value in the central kiloparsec-a factor of similar to 2 below the galaxy mean, on average. In some cases, the central alpha(CO) value can be factors of 5-10 below the standard Milky Way (MW) value of alpha(CO,MW) = 4.4 M-circle dot pc(-2) (K km s(-1))(-1). While for alpha(CO) we find only weak correlations with metallicity, the DGR is well-correlated with metallicity, with an approximately linear slope. Finally, we present several recommendations for choosing an appropriate alpha(CO) for studies of nearby galaxies. C1 [Sandstrom, K. M.; Walter, F.; Groves, B.; Kreckel, K.; Linz, H.; Meidt, S.; Rix, H. -W.; Schinnerer, E.; van der Laan, T.; Krause, O.; Schmiedeke, A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Leroy, A. K.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Bolatto, A. D.; Wolfire, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Croxall, K. V.; Crocker, A.; Pellegrini, E.; Smith, J. D. T.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Croxall, K. V.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Draine, B. T.; Aniano, G.] Princeton Univ Observ, Princeton, NJ 08544 USA. [Wilson, C. D.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Calzetti, D.; Crocker, A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Kennicutt, R. C.; Galametz, M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Aniano, G.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Aniano, G.] CNRS, UMR 8617, F-91405 Orsay, France. [Meyer, J. Donovan; Koda, J.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Usero, A.] Observ Astron Nacl, E-28014 Madrid, Spain. [Bigiel, F.] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, D-69120 Heidelberg, Germany. [Brinks, E.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [de Blok, W. J. G.] ASTRON, Netherlands Inst Radio Astron, NL-7990 AA Dwingeloo, Netherlands. [Dale, D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Engelbracht, C. W.; Skibba, R.; Hinz, J.; Montiel, E.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Engelbracht, C. W.] Raytheon Co, Tucson, AZ 85756 USA. [Hunt, L. K.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Roussel, H.; Vigroux, L.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Schruba, A.] CALTECH, Pasadena, CA 91125 USA. [Schuster, K. -F.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Skibba, R.] Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92093 USA. [Appleton, P.] CALTECH, NASA, Herschel Sci Ctr, IPAC, Pasadena, CA 91125 USA. [Armus, L.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Brandl, B.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Gordon, K.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Hinz, J.] MMT Observ, Tucson, AZ 85721 USA. [Montiel, E.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Sauvage, M.] CE Saclay, UMR AIM, CEA DSM DAPNIA, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Schmiedeke, A.] Univ Cologne, D-50937 Cologne, Germany. RP Sandstrom, KM (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM sandstrom@mpia.de RI Kreckel, Kathryn/C-3468-2012; OI Draine, Bruce/0000-0002-0846-936X; Appleton, Philip/0000-0002-7607-8766; Hunt, Leslie/0000-0001-9162-2371; Brinks, Elias/0000-0002-7758-9699 FU Marie Curie International Incoming Fellowship; CAREER grant [NSF-AST0955836, NASA-JPL1373858]; Research Corporation for Science Advancement Cottrell Scholar award; BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT(Spain); CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); NASA (USA); National Aeronautics and Space Administration FX We thank the referee for useful comments that helped to improve the quality of the manuscript. K. S. thanks R. Shetty, S. Glover, R. Klessen, D. Narayanan, and A. Stutz for helpful conversations. The authors thank R. Feldmann and N. Gnedin for helpful comments regarding the comparison of our measurements to their simulations. K. S. is supported by a Marie Curie International Incoming Fellowship. A. D. B. wishes to acknowledge partial support from a CAREER grant NSF-AST0955836, NASA-JPL1373858, and from a Research Corporation for Science Advancement Cottrell Scholar award.; This work is based on observations made with Herschel. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM(France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT(Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada); NAOC (China); CEA, LAM(France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK); and Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). HIPE is a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. 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 Bibliographic Services. NR 94 TC 110 Z9 110 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2013 VL 777 IS 1 AR 5 DI 10.1088/0004-637X/777/1/5 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300005 ER PT J AU Schnittman, JD Krolik, JH AF Schnittman, Jeremy D. Krolik, Julian H. TI A MONTE CARLO CODE FOR RELATIVISTIC RADIATION TRANSPORT AROUND KERR BLACK HOLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; X-rays: binaries ID ACTIVE GALACTIC NUCLEI; X-RAY-POLARIZATION; NO-HAIR THEOREM; COVARIANT MAGNETOIONIC THEORY; QUASI-PERIODIC OSCILLATIONS; STRONG-GRAVITY REGIME; ACCRETION DISKS; TETRAHEDRAL HOHLRAUMS; LINE-PROFILES; LIGHT CURVES AB We present a new code for radiation transport around Kerr black holes, including arbitrary emission and absorption mechanisms, as well as electron scattering and polarization. The code is particularly useful for analyzing accretion flows made up of optically thick disks and optically thin coronae. We give a detailed description of the methods employed in the code and also present results from a number of numerical tests to assess its accuracy and convergence. 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. EM jeremy.schnittman@nasa.gov; jhk@pha.jhu.edu FU NASA Chandra postdoctoral fellowship; NSF [AST-0507455, AST-0908336] FX We thank T. Kallman for helpful discussions and the anonymous referee for a very careful and constructive report. This work was partially supported by a NASA Chandra postdoctoral fellowship (J.D.S.) and NSF grants AST-0507455 and AST-0908336 (J.H.K.). NR 58 TC 11 Z9 11 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2013 VL 777 IS 1 AR 11 DI 10.1088/0004-637X/777/1/11 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300011 ER PT J AU Allafort, A Baldini, L Ballet, J Barbiellini, G Baring, MG Bastieri, D Bellazzini, R Bonamente, E Bottacini, E Brandt, TJ Bregeon, J Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Cecchi, C Chaves, RCG Chekhtman, A Chiang, J Chiaro, G Ciprini, S Claus, R D'Ammando, F de Palma, F Digel, SW Di Venere, L Drell, PS Favuzzi, C Ferrara, EC Franckowiak, A Fusco, P Gargano, F Gasparrini, D Giglietto, N Giroletti, M Glanzman, T Godfrey, G Grenier, IA Guiriec, S Hadasch, D Harding, AK Hayashida, M Hayashi, K Hays, E Hewitt, J Hill, AB Horan, D Hou, X Jogler, T Johnson, AS Johnson, TJ Kerr, M Knodlseder, J Kuss, M Lande, J Larsson, S Latronico, L Lemoine-Goumard, M Longo, F Loparco, F Lubrano, P Malyshev, D Marelli, M Mayer, M Mazziotta, MN Mehault, J Mizuno, T Monzani, ME Morselli, A Murgia, S Nemmen, R Nuss, E Ohsugi, T Omodei, N Orienti, M Orlando, E Paneque, D Pesce-Rollins, M Pierbattista, M Piron, F Pivato, G Porter, TA Raino, S Rando, R Ray, PS Razzano, M Reimer, O Reposeur, T Romani, RW Sartori, A Parkinson, PMS Sgro, C Siskind, EJ Smith, DA Spinelli, P Strong, AW Takahashi, H Thayer, JB Thompson, DJ Tibaldo, L Tinivella, M Torres, DF Tosti, G Uchiyama, Y Usher, TL Vandenbroucke, J Vasileiou, V Venter, C Vianello, G Vitale, V Winer, BL Wood, KS AF Allafort, A. Baldini, L. Ballet, J. Barbiellini, G. Baring, M. G. Bastieri, D. Bellazzini, R. Bonamente, E. Bottacini, E. Brandt, T. J. Bregeon, J. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cecchi, C. Chaves, R. C. G. Chekhtman, A. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. D'Ammando, F. de Palma, F. Digel, S. W. Di Venere, L. Drell, P. S. Favuzzi, C. Ferrara, E. C. Franckowiak, A. Fusco, P. Gargano, F. Gasparrini, D. Giglietto, N. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Guiriec, S. Hadasch, D. Harding, A. K. Hayashida, M. Hayashi, K. Hays, E. Hewitt, J. Hill, A. B. Horan, D. Hou, X. Jogler, T. Johnson, A. S. Johnson, T. J. Kerr, M. Knoedlseder, J. Kuss, M. Lande, J. Larsson, S. Latronico, L. Lemoine-Goumard, M. Longo, F. Loparco, F. Lubrano, P. Malyshev, D. Marelli, M. Mayer, M. Mazziotta, M. N. Mehault, J. Mizuno, T. Monzani, M. E. Morselli, A. Murgia, S. Nemmen, R. Nuss, E. Ohsugi, T. Omodei, N. Orienti, M. Orlando, E. Paneque, D. Pesce-Rollins, M. Pierbattista, M. Piron, F. Pivato, G. Porter, T. A. Raino, S. Rando, R. Ray, P. S. Razzano, M. Reimer, O. Reposeur, T. Romani, R. W. Sartori, A. Parkinson, P. M. Saz Sgro, C. Siskind, E. J. Smith, D. A. Spinelli, P. Strong, A. W. Takahashi, H. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tinivella, M. Torres, D. F. Tosti, G. Uchiyama, Y. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Venter, C. Vianello, G. Vitale, V. Winer, B. L. Wood, K. S. TI PSR J2021+4026 IN THE GAMMA CYGNI REGION: THE FIRST VARIABLE gamma-RAY PULSAR SEEN BY THE Fermi LAT SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma rays: stars; pulsars: individual (PSR J2021+4026); stars: neutron ID LARGE-AREA TELESCOPE; LIGHT CURVES; VELA PULSAR; X-RAY; SEARCH; VARIABILITY; MAGNETOSPHERE; DISCOVERY; ROTATION; SPECTRA AB Long-term monitoring of PSR J2021+4026 in the heart of the Cygnus region with the Fermi Large Area Telescope unveiled a sudden decrease in flux above 100 MeV over a timescale shorter than a week. The "jump" was near MJD 55850 (2011 October 16), with the flux decreasing from (8.33+/-0.08) x 10(-10) erg cm(-2) s(-1) to (6.86+/-0.13) x 10(-10) erg cm(-2) s(-1). Simultaneously, the frequency spindown rate increased from (7.8 +/- 0.1) x 10(-13) Hz s(-1) to (8.1 +/- 0.1) x 10(-13) Hz s(-1). Significant (>5 sigma) changes in the pulse profile and marginal (<3 sigma) changes in the emission spectrum occurred at the same time. There is also evidence for a small, steady flux increase over the 3 yr preceding MJD 55850. This is the first observation at gamma-ray energies of mode changes and intermittent behavior, observed at radio wavelengths for other pulsars. We argue that the change in pulsed gamma-ray emission is due to a change in emission beaming and we speculate that it is precipitated by a shift in the magnetic field structure, leading to a change of either effective magnetic inclination or effective current. C1 [Allafort, A.; Bottacini, E.; Cameron, R. A.; Chiang, J.; Claus, R.; Digel, S. W.; Di Venere, L.; Drell, P. S.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Kerr, M.; Lande, J.; Malyshev, D.; Monzani, M. E.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, O.; Romani, R. W.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, Stanford, CA 94305 USA. [Allafort, A.; Bottacini, E.; Cameron, R. A.; Chiang, J.; Claus, R.; Digel, S. W.; Di Venere, L.; Drell, P. S.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Kerr, M.; Lande, J.; Malyshev, D.; Monzani, M. E.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, O.; Romani, R. W.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Baldini, L.; Razzano, M.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Chaves, R. C. G.; Grenier, I. A.] Univ Paris Diderot, CNRS, CEA IRFU, Lab AIM,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Barbiellini, 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. [Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. [Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Chiaro, G.; Pivato, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bonamente, E.; Cecchi, C.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brandt, T. J.; Ferrara, E. C.; Guiriec, S.; Harding, A. K.; Hays, E.; Hewitt, J.; Nemmen, R.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bruel, P.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Buehler, R.; Mayer, M.] DESY, D-15738 Zeuthen, Germany. [Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, E-08193 Barcelona, Spain. [Caraveo, P. A.; Marelli, M.; Pierbattista, M.; Sartori, A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Chekhtman, A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Chekhtman, A.; Johnson, T. J.] Naval Res Lab, Washington, DC 20375 USA. [Ciprini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy. [Ciprini, S.; Gasparrini, D.] Ist Nazl Astrofis, Osservatorio Astron Roma, I-00040 Rome, Italy. [D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF, Ist Radioastron, I-40129 Bologna, Italy. [de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Hayashida, M.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Hayashi, K.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hou, X.; Lemoine-Goumard, M.; Mehault, J.; Reposeur, T.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Johnson, T. J.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Knoedlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, F-31100 Toulouse, France. [Larsson, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Larsson, S.] Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, F-34095 Montpellier, France. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Ray, P. S.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Parkinson, P. M. Saz] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Torres, D. F.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Venter, C.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa. [Vianello, G.] Consorzio Interuniv Fis Spaziale, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Dept Phys, Columbus, OH 43210 USA. RP Allafort, A (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, Stanford, CA 94305 USA. EM massimiliano.razzano@pi.infn.it; ltibaldo@slac.stanford.edu RI Di Venere, Leonardo/C-7619-2017; Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Venter, Christo/E-6884-2011; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; 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 OI Di Venere, Leonardo/0000-0003-0703-824X; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; Rando, Riccardo/0000-0001-6992-818X; Venter, Christo/0000-0002-2666-4812; Torres, Diego/0000-0002-1522-9065; Reimer, Olaf/0000-0001-6953-1385; Morselli, Aldo/0000-0002-7704-9553; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; FU NASA in the United States; DOE in the United States; CEA/Irfu in France; IN2P3/CNRS in France; ASI in Italy; INFN in Italy; MEXT in Japan; KEK in Japan; JAXA in Japan; K.A. Wallenberg Foundation in Sweden; Swedish Research Council in Sweden; National Space Board in Sweden; INAF in Italy; CNES in France FX The Fermi LAT Collaboration acknowledges support from a number of agencies and institutes for both the development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K.A. Wallenberg Foundation, the Swedish Research Council, and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged. NR 36 TC 20 Z9 20 U1 0 U2 18 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 NOV 1 PY 2013 VL 777 IS 1 AR L2 DI 10.1088/2041-8205/777/1/L2 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241SH UT WOS:000326187400002 ER PT J AU Tanaka, YT Cheung, CC Inoue, Y Stawarz, L Ajello, M Dermer, CD Wood, DL Chekhtman, A Fukazawa, Y Mizuno, T Ohno, M Paneque, D Thompson, DJ AF Tanaka, Y. T. Cheung, C. C. Inoue, Y. Stawarz, L. Ajello, M. Dermer, C. D. Wood, D. L. Chekhtman, A. Fukazawa, Y. Mizuno, T. Ohno, M. Paneque, D. Thompson, D. J. TI Fermi LARGE AREA TELESCOPE DETECTION OF TWO VERY-HIGH-ENERGY (E > 100 GeV) gamma-RAY PHOTONS FROM THE z=1.1 BLAZAR PKS 0426-380 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE acceleration of particles; galaxies: active; galaxies: jets; gamma rays: galaxies; quasars: individual (PKS 0426-380); radiation mechanisms: non-thermal ID EXTRAGALACTIC BACKGROUND LIGHT; ACTIVE GALACTIC NUCLEI; BL LACERTAE OBJECTS; HOST GALAXIES; EMISSION; QUASAR; DISCOVERY; EVOLUTION; UNIVERSE; CATALOG AB We report the Fermi Large Area Telescope (LAT) detection of two very-high-energy (VHE, E > 100 GeV) gamma-ray photons from the directional vicinity of the distant (redshift, z = 1.1) blazar PKS 0426-380. The null hypothesis that both the 134 and 122 GeV photons originate from unrelated sources can be rejected at the 5.5s confidence level. We therefore claim that at least one of the two VHE photons is securely associated with PKS 0426-380, making it the most distant VHE emitter known to date. The results are in agreement with recent Fermi-LAT constraints on the extragalactic background light (EBL) intensity, which imply a z similar or equal to 1 horizon for similar or equal to 100 GeV photons. The LAT detection of the two VHE gamma-rays coincided roughly with flaring states of the source, although we did not find an exact correspondence between the VHE photon arrival times and the flux maxima at lower gamma-ray energies. Modeling the gamma-ray continuum of PKS 0426-380 with daily bins revealed a significant spectral hardening around the time of the first VHE event detection (LAT photon index Gamma similar or equal to 1.4) but on the other hand no pronounced spectral changes near the detection time of the second one. This combination implies a rather complex variability pattern of the source in gamma-rays during the flaring epochs. An additional flat component is possibly present above several tens of GeV in the EBL-corrected Fermi-LAT spectrum accumulated over the similar to 8 month high state. C1 [Tanaka, Y. T.; Mizuno, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Cheung, C. C.; Dermer, C. D.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Inoue, Y.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Inoue, Y.; Paneque, D.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Stawarz, L.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Wood, D. L.] Praxis Inc, Alexandria, VA 22303 USA. [Chekhtman, A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Fukazawa, Y.; Ohno, M.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Tanaka, YT (reprint author), Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. EM ytanaka@hep01.hepl.hiroshima-u.ac.jp FU Kakenhi [24840031]; NASA [DPR S-15633-Y]; Polish NSC [DEC-2012/04/A/ST9/00083] FX We appreciate the referee's critical reading and valuable comments. Y.T.T. is supported by Kakenhi 24840031. Work by C. C. C. at NRL is supported in part by NASA DPR S-15633-Y. L. S. was supported by Polish NSC grant DEC-2012/04/A/ST9/00083. NR 43 TC 12 Z9 12 U1 0 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 NOV 1 PY 2013 VL 777 IS 1 AR L18 DI 10.1088/2041-8205/777/1/L18 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241SH UT WOS:000326187400018 ER PT J AU Gdoutos, E Shapiro, AA Daraio, C AF Gdoutos, E. Shapiro, A. A. Daraio, C. TI Thin and Thermally Stable Periodic Metastructures SO EXPERIMENTAL MECHANICS LA English DT Article DE Low thermal expansion; Thermally stable; Tunable CTE; Metastructures; bi-metallic array ID HIGH STIFFNESS; EXPANSION; COEFFICIENT AB We design, fabricate, and test thin thermally stable metastructures consisting of bi-metallic unit cells and show how the coefficient of thermal expansion (CTE) of these metastructures can be finely and coarsely tuned by varying the CTE of the constituent materials and the unit cell geometry. Planar and three-dimensional finite element method modeling (FEM) is used to drive our design and inform experiments, and predict the response of these metastructures. We develop a robust experimental fabrication procedure in order to fabricate thermally stable samples with high aspect ratios. We use digital image correlation (DIC) and an infrared camera to experimentally measure displacement and temperature during testing and compute the CTE of our samples. The samples, composed of an aluminum core and an external titanium frame, exhibit a CTE of 2.6 ppm/A degrees C, which is significantly lower than either constituent. These unit cells can be assembled over a large area to create thin low-CTE foils. Finally, we demonstrate how the approach developed in this work can be used to fabricate metastructures with CTE's ranging from -3.6 ppm/A degrees C to 8.4 ppm/A degrees C. C1 [Gdoutos, E.; Daraio, C.] CALTECH, Grad Aerosp Labs, Pasadena, CA 91125 USA. [Shapiro, A. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Daraio, C (reprint author), CALTECH, Grad Aerosp Labs, Pasadena, CA 91125 USA. EM daraio@caltech.edu RI Daraio, Chiara/N-2170-2015 OI Daraio, Chiara/0000-0001-5296-4440 FU Keck Institute for Space Studies at the California Institute of Technology; National Aeronautics and Space Administration FX This work was supported by the Keck Institute for Space Studies at the California Institute of Technology. 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. We thank Jerry Mulder for support with the laser welding process. We also thank Prof. Sergio Pellegrino and Dr. Namiko Yamamoto for valuable advice and assistance, and Prof. Craig A. Steeves for earlier discussions. NR 22 TC 8 Z9 8 U1 1 U2 20 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0014-4851 EI 1741-2765 J9 EXP MECH JI Exp. Mech. PD NOV PY 2013 VL 53 IS 9 BP 1735 EP 1742 DI 10.1007/s11340-013-9748-z PG 8 WC Materials Science, Multidisciplinary; Mechanics; Materials Science, Characterization & Testing SC Materials Science; Mechanics GA 239SN UT WOS:000326045800019 ER PT J AU Wichman, IS Olson, SL Miller, FJ Tanaya, SA AF Wichman, Indrek S. Olson, Sandra L. Miller, Fletcher J. Tanaya, Stefanus A. TI Experimental evaluation of flame and flamelet spread over cellulosic materials using the narrow channel apparatus SO FIRE AND MATERIALS LA English DT Article DE opposed flow flame spread; microgravity; narrow channel apparatus; thermally thin fuels; flamelets; transition phenomena ID FINGERING INSTABILITY; DIFFUSION FLAMES; MECHANISMS; COMBUSTION AB Originally conceived as an apparatus to study near-limit flames and their breakup into flamelets and later modified to function as a microgravity simulation apparatus, the narrow channel apparatus serves also as a facility for examining long time flame spread and material flammability in on-earth (terrestrial) applications. These applications include flame spread in narrow gaps, persistence of flame in heat-loss environments, and flame-to-flamelet front transition. The narrow channel apparatus tests described here measure behavior of the spreading flame and features of the flame-to-flamelet transition. Measured quantities include flow, flame and flamelet velocities in normal and inverted tests, flow deceleration and acceleration rates with associated flame or flamelet response, flame-to-flamelet transition times, and influences of fuel thickness. The principal goal of this research was to ascertain the capacity of the narrow channel apparatus to produce data for phenomena observed in both (1) simulated microgravity flame spread and (2) terrestrial flame spread in narrow gaps and channels. Copyright (c) 2012 John Wiley & Sons, Ltd. C1 [Wichman, Indrek S.] Michigan State Univ, Dept Mech Engn, E Lansing, MI 48824 USA. [Olson, Sandra L.] NASA Glenn Res Ctr Lewis Field, REC0, Combust & Reacting Syst Branch, Cleveland, OH 44135 USA. [Miller, Fletcher J.] San Diego State Univ, Dept Mech Engn, San Diego, CA 92182 USA. [Tanaya, Stefanus A.] Stant USA, Romeo, MI 48065 USA. RP Wichman, IS (reprint author), Michigan State Univ, Dept Mech Engn, E Lansing, MI 48824 USA. EM wichman@egr.msu.edu FU NASA [NNC04AA50A, NCC31053]; MSU FX This work was supported by NASA Cooperative Agreement NNC04AA50A and NCC31053 with MSU. I. S. W. acknowledges support during the compilation of this article from the MSU Strategic Partnership Grants (SPG) program. The authors wish to acknowledge the assistance of NASA summer interns Ms. Terri Williams and Ms. Rachel Morgan for the research leading to Figure 2, NASA engineer Mr. Jim Breuwer for making Figure 3, and MSU undergraduate summer intern Mr. Jiawei ("Johnny") Qin for modifying Figures 4-12 from S. Tanaya's thesis. NR 29 TC 4 Z9 4 U1 2 U2 12 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0308-0501 EI 1099-1018 J9 FIRE MATER JI Fire Mater. PD NOV PY 2013 VL 37 IS 7 BP 503 EP 519 DI 10.1002/fam.2143 PG 17 WC Materials Science, Multidisciplinary SC Materials Science GA 242WU UT WOS:000326276700002 ER PT J AU Callahan, MP Gerakines, PA Martin, MG Peeters, Z Hudson, RL AF Callahan, Michael P. Gerakines, Perry A. Martin, Mildred G. Peeters, Zan Hudson, Reggie L. TI Irradiated benzene ice provides clues to meteoritic organic chemistry SO ICARUS LA English DT Article DE Astrobiology; Cosmic rays; Cosmochemistry; Experimental techniques; Ices, IR spectroscopy ID POLYCYCLIC AROMATIC-HYDROCARBONS; ATMOSPHERIC-PRESSURE PHOTOIONIZATION; CARBONACEOUS METEORITES; MURCHISON METEORITE; ULTRAVIOLET PHOTOIRRADIATION; INTERSTELLAR-MEDIUM; LIQUID BENZENE; ION; RADIOLYSIS; RELEVANT AB Aromatic hydrocarbons account for a significant portion of the organic matter in carbonaceous chondrite meteorites, as a component of both the low molecular weight, solvent-extractable compounds and the insoluble organic macromolecular material. Previous work has suggested that the aromatic compounds in carbonaceous chondrites may have originated in the radiation-processed icy mantles of interstellar dust grains. Here we report new studies of the organic residue made from benzene irradiated at 19 K by 0.8 MeV protons. Polyphenyls with up to four rings were unambiguously identified in the residue by gas chromatography-mass spectrometry. Atmospheric pressure photoionization Fourier transform mass spectrometry was used to determine molecular composition, and accurate mass measurements suggested the presence of polyphenyls, partially hydrogenated polyphenyls, and other complex aromatic compounds. The profile of low molecular weight compounds in the residue compared well with extracts from the Murchison and Orgueil meteorites. These results are consistent with the possibility that solid phase radiation chemistry of benzene produced some of the complex aromatics found in meteorites. Published by Elsevier Inc. C1 [Callahan, Michael P.; Gerakines, Perry A.; Martin, Mildred G.; Hudson, Reggie L.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Callahan, Michael P.; Gerakines, Perry A.; Martin, Mildred G.; Hudson, Reggie L.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [Martin, Mildred G.] Catholic Univ Amer, Washington, DC 20064 USA. [Peeters, Zan] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. RP Callahan, MP (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. EM michael.p.callahan@nasa.gov RI Gerakines, Perry/D-2226-2012 OI Gerakines, Perry/0000-0002-9667-5904 FU NASA Postdoctoral Program fellowship; NASA; NASA Astrobiology Institute; Goddard Center of Astrobiology FX The authors thank Marla Moore (NASA GSFC), Jason Dworkin (NASA GSFC), Jim Cleaves (Institute for Advanced Study), and an anonymous reviewer for helpful suggestions regarding this research or manuscript. We also thank Cecilia Satterwhite (NASA JSC), Kevin Righter (NASA JSC), and the Meteorite Working Group for providing the RBT 04262 meteorite sample, Linda Welzenbach and Tim McCoy (Smithsonian National Museum of Natural History) for providing the Murchison meteorite sample, Pascale Ehrenfreund (The George Washington University) for providing the Orgueil meteorite sample, and Andrew Mattioda (NASA Ames) for providing some of the PAH standards used in this study. In addition, we thank Steve Brown, Tom Ward, and Eugene Gerashchenko (Radiation Effects Facility at NASA GSFC) for operation of the proton accelerator. M.P.C. was partially supported by a NASA Postdoctoral Program fellowship administered by Oak Ridge Associated Universities through a contract with NASA. This research was supported by the NASA Astrobiology Institute and the Goddard Center of Astrobiology. NR 50 TC 9 Z9 9 U1 1 U2 28 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 NOV-DEC PY 2013 VL 226 IS 2 BP 1201 EP 1209 DI 10.1016/j.icarus.2013.07.033 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 239DX UT WOS:000326003900003 ER PT J AU Li, JY Le Corre, L Schroder, SE Reddy, V Denevi, BW Buratti, BJ Mottola, S Hoffmann, M Gutierrez-Marques, P Nathues, A Russell, CT Raymond, CA AF Li, Jian-Yang Le Corre, Lucille Schroeder, Stefan E. Reddy, Vishnu Denevi, Brett W. Buratti, Bonnie J. Mottola, Stefano Hoffmann, Martin Gutierrez-Marques, Pablo Nathues, Andreas Russell, Christopher T. Raymond, Carol A. TI Global photometric properties of Asteroid (4) Vesta observed with Dawn Framing Camera SO ICARUS LA English DT Article DE Asteroid Vesta; Asteroids, surfaces; Photometry; Spectrophotometry ID HUBBLE-SPACE-TELESCOPE; BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; DISK-RESOLVED PHOTOMETRY; GALILEO PHOTOMETRY; DARK MATERIAL; SURFACE; IMAGES; HETEROGENEITY; REGOLITH; NUCLEUS AB Dawn spacecraft orbited Vesta for more than one year and collected a huge volume of multispectral, high-resolution data in the visible wavelengths with the Framing Camera. We present a detailed disk-integrated and disk-resolved photometric analysis using the Framing Camera images with the Minnaert model and the Hapke model, and report our results about the global photometric properties of Vesta. The photometric properties of Vesta show weak or no dependence on wavelengths, except for the albedo. At 554 nm, the global average geometric albedo of Vesta is 0.38 +/- 0.04, and the Bond albedo range is 0.20 +/- 0.02. The bolometric Bond albedo is 0.18 +/- 0.01. The phase function of Vesta is similar to those of S-type asteroids. Vesta's surface shows a single-peaked albedo distribution with a full-width-half-max similar to 17% relative to the global average. This width is much smaller than the full range of albedos (from similar to 0.55 x to >2 x global average) in localized bright and dark areas of a few tens of km in sizes, and is probably a consequence of significant regolith mixing on the global scale. Rheasilvia basin is similar to 10% brighter than the global average. The phase reddening of Vesta measured from Dawn Framing Camera images is comparable or slightly stronger than that of Eros as measured by the Near Earth Asteroid Rendezvous mission, but weaker than previous measurements based on ground-based observations of Vesta and laboratory measurements of HED meteorites. The photometric behaviors of Vesta are best described by the Hapke model and the Akimov disk-function, when compared with the Minnaert model, Lommel-Seeliger model, and Lommel-Seeliger-Lambertian model. The traditional approach for photometric correction is validated for Vesta for >99% of its surface where reflectance is within +/- 30% of global average. (C) 2013 Elsevier Inc. All rights reserved. C1 [Li, Jian-Yang; Le Corre, Lucille] Planetary Sci Inst, Tucson, AZ 85719 USA. [Schroeder, Stefan E.; Mottola, Stefano] Deutsch Zentrum Luft & Raumfahrt DLR, D-12489 Berlin, Germany. [Reddy, Vishnu; Hoffmann, Martin; Gutierrez-Marques, Pablo; Nathues, Andreas] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany. [Reddy, Vishnu] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA. [Denevi, Brett W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Buratti, Bonnie J.; Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. RP Li, JY (reprint author), Planetary Sci Inst, Tucson, AZ 85719 USA. EM jyli@psi.edu RI Denevi, Brett/I-6502-2012; Schroder, Stefan/D-9709-2013; OI Denevi, Brett/0000-0001-7837-6663; Schroder, Stefan/0000-0003-0323-8324; Reddy, Vishnu/0000-0002-7743-3491; Le Corre, Lucille/0000-0003-0349-7932 FU NASA's Dawn at Vesta Participating Scientist Program [NNX10AR56G, NNX13AB82G]; NASA's Dawn Mission through the Discovery Program; NASA; Max Planck Society; German Space Agency, DLR FX This work is supported by NASA's Dawn at Vesta Participating Scientist Program and NASA's Dawn Mission through the Discovery Program. JYL is supported by NASA's Dawn at Vesta Participating Scientist Program through Grants NNX10AR56G to University of Maryland at College Park and NNX13AB82G to Planetary Science Institute. Part of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. The Framing Camera project is financially supported by the Max Planck Society and the German Space Agency, DLR. The authors are extremely grateful to the wonderful engineering, operations, and instrument teams who made the Vesta phase of Dawn mission a great success. We thank Dr. Beth Clark and Dr. Paul Helfenstein for their careful and rigorous reviews, which helped improve the manuscript significantly. NR 82 TC 33 Z9 33 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 NOV-DEC PY 2013 VL 226 IS 2 BP 1252 EP 1274 DI 10.1016/j.icarus.2013.08.011 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 239DX UT WOS:000326003900008 ER PT J AU Koskinen, TT Sandel, BR Yelle, RV Capalbo, FJ Holsclaw, GM McClintock, WE Edgington, S AF Koskinen, T. T. Sandel, B. R. Yelle, R. V. Capalbo, F. J. Holsclaw, G. M. McClintock, W. E. Edgington, S. TI The density and temperature structure near the exobase of Saturn from Cassini UVIS solar occultations SO ICARUS LA English DT Article DE Saturn; Occultations; Atmospheres, Structure; Aeronomy ID EXTREME-ULTRAVIOLET OBSERVATIONS; UPPER-ATMOSPHERE; MOLECULAR-HYDROGEN; STELLAR OCCULTATIONS; BAND SYSTEM; THERMOSPHERE; VARIABILITY; MESOSPHERE; SPACECRAFT; ENCOUNTER AB We analyzed 15 solar occultations observed by the Cassini UVIS instrument to constrain the density and temperature structure near the exobase of Saturn. We retrieved the density of H-2 and thus the temperature at altitudes higher than 1900 km above the 1 bar level by analyzing the ionization continuum of H-2 at wavelengths shorter than 804 A. We find that the exospheric temperature ranges from 370 K to 540 K, with a typical uncertainty of less than 20 K. According to our data the temperature increases with latitude from the equator to the poles by 100-150 K At similar latitudes, the temperature varies by 20-50 K at different times with no evidence for any systematic diurnal trend so far. Based on our data, the exobase of Saturn is 2700-3000 km above the 1 bar level and the thermal escape parameter near the exobase ranges from 260 to 340, implying that thermal escape from Saturn is firmly in the Jeans regime. The mixing ratio of H-2 is close to unity at all altitudes below the exobase. We find that the pressure levels in the thermosphere deviate significantly from a simple spheroid predicted by potential theory. This is consistent with significant meridional temperature variations in the lower thermosphere. A global analysis of the temperature structure at different depths in the atmosphere is required to constrain both the shape and the deposition and redistribution of energy in the upper atmosphere further. (C) 2013 Elsevier Inc. All rights reserved. C1 [Koskinen, T. T.; Sandel, B. R.; Yelle, R. V.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Capalbo, F. J.] Univ Paris Est Creteil & Paris Diderot, Lab Interuniv Syst Atmospher, F-94010 Creteil, France. [Holsclaw, G. M.; McClintock, W. E.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. [Edgington, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Koskinen, TT (reprint author), Univ Arizona, Lunar & Planetary Lab, 1629 E Univ Blvd, Tucson, AZ 85721 USA. EM tommi@lpl.arizona.edu FU NASA CDAP Grant [NNX13AJ06G] FX We thank F.M. Flasar for useful correspondence regarding the shape of Saturn's atmosphere. T.T.K. acknowledges support by the NASA CDAP Grant NNX13AJ06G. NR 49 TC 10 Z9 10 U1 1 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD NOV-DEC PY 2013 VL 226 IS 2 BP 1318 EP 1330 DI 10.1016/j.icarus.2013.07.037 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 239DX UT WOS:000326003900012 ER PT J AU Deau, E Flandes, A Spilker, LJ Petazzoni, J AF Deau, Estelle Flandes, Alberto Spilker, Linda J. Petazzoni, Jerome TI Re-analysis of previous laboratory phase curves: 1. Variations of the opposition effect morphology with the textural properties, and an application to planetary surfaces SO ICARUS LA English DT Article DE Photometry; Radiative transfer; Regoliths ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; LIGHT-SCATTERING-DATABASE; SOLAR-SYSTEM OBJECTS; DISTANT ICY BODIES; COHERENT BACKSCATTERING; WEAK-LOCALIZATION; SPHERICAL-PARTICLES; DISORDERED MEDIA; REGOLITH ANALOGS; SATURNS RINGS AB Typical variations in the opposition effect morphology of laboratory samples at optical wavelengths are investigated to probe the role of the textural properties of the surface (roughness, porosity and grain size). A previously published dataset of 34 laboratory phase curves is re-analyzed and fit with several morphological models. The retrieved morphological parameters that characterize the opposition surge, amplitude, width and slope (A, HWHM and S respectively) are correlated to the single scattering albedo, the roughness, the porosity and the grain size of the samples. To test the universality of the laboratory samples' trends, we use previously published phase curves of planetary surfaces, including the Moon, satellites and rings of the giant planets. The morphological parameters of the surge (A and HWHM) for planetary surfaces are found to have a non-monotonic variation with the single scattering albedo, similar to that observed in asteroids (Belskaya, I.N., Shevchenko, V.G. [2000]. Icarus 147,94-105), which is unexplained so far. The morphological parameters of the surge (A and HWHM) for laboratory samples seem to exhibit the same non-monotonic variation with single scattering albedo. While the non-monotonic variation with albedo was already observed by Nelson et al. (Nelson, R.M., Hapke, B.W., Smythe, W.D., Hale, A.S., Piatek, J.L. [2004]. Planetary regolith microstructure: An unexpected opposition effect result. In: Mackwell, S., Stansbery, E. (Eds.), Proc. Lunar Sci. Conf. 35, p. 1089), we report here the same variation for the angular width. (C) 2013 Elsevier Inc. All rights reserved. C1 [Deau, Estelle; Spilker, Linda J.] NASA Jet Prop Lab, Pasadena, CA 91109 USA. [Flandes, Alberto] Univ Nacl Autonoma Mexico, Inst Geofis, Mexico City 04510, DF, Mexico. [Petazzoni, Jerome] DotCloud, San Francisco, CA 94104 USA. RP Deau, E (reprint author), NASA Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM estelle.deau@jpl.nasa.gov FU NASA; California Institute of Technology; NASA Postdoctoral Program; Cassini Program FX This study was performed at Jet Propulsion Laboratory (JPL), under contract with NASA and California Institute of Technology and was funded by the NASA Postdoctoral Program led by OakRidge Associated Universities (ORAU) and the Cassini Program. NR 127 TC 6 Z9 6 U1 0 U2 7 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 NOV-DEC PY 2013 VL 226 IS 2 BP 1465 EP 1488 DI 10.1016/j.icarus.2013.01.014 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 239DX UT WOS:000326003900020 ER PT J AU Sung, K Toon, GC Maltz, AW Smith, MAH AF Sung, Keeyoon Toon, Geoffrey C. Maltz, Arlan W. Smith, Mary Ann H. TI FT-IR measurements of cold C3H8 cross sections at 7-15 mu m for Titan atmosphere SO ICARUS LA English DT Article DE Titan atmosphere; Radiative transfer; IR spectroscopy; Atmospheric composition ID HIGH-RESOLUTION ANALYSIS; VOYAGER INFRARED OBSERVATIONS; BAND MODEL PARAMETERS; SPECTROSCOPIC DATABASE; NONMETHANE HYDROCARBONS; TEMPERATURE-DEPENDENCE; 748 CM-1; PROPANE; ABSORPTION; SPECTRUM AB We present absorption cross sections of propane (C3H8) at temperatures from 145 K to 297 K in the 690-1550 cm(-1) region. Pure and N-2-broadened spectra were measured at pressures from 3 Tort to 742 Torr using a Bruker IFS125 FT-IR spectrometer at JPL. The gas absorption cell, developed at Connecticut College, was cooled by a closed-cycle helium refrigerator. The cross sections were measured and compiled for individual spectra recorded at various experimental conditions covering the planetary atmosphere and Titan. In addition to the cross sections, a propane pseudoline list with a frequency grid of 0.005 cm(-1), was fitted to the 34 laboratory spectra. Line intensities and lower state energies were retrieved for each line, assuming a constant width. Validation tests showed that the pseudoline list reproduces discrete absorption features and continuum, the latter contributed by numerous weak and hot band features, in most of the observed spectra within 3%. Based on the pseudoline list, the total intensity in the 690-1550 cm(-1) region was determined to be 52.93 (+/- 3%) x 10(-19) cm(-1)/(molecule cm(-2)) at 296 K; this value is within 3% of the average from four earlier studies. Finally, the merit of the pseudoline approach is addressed for heavy polyatomic molecules in support of spectroscopic observation of atmospheres of Titan and other planets. The cold cross sections will be submitted to the HITRAN database (hitran.harvard.edu), and the list of C3H8 pseudolines will be available from a MK-IV website of JPL (http://mark4sun.jpl.nasa.gov/data/spec/Pseudo). (C) 2013 Elsevier Inc. All rights reserved. C1 [Sung, Keeyoon; Toon, Geoffrey C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Maltz, Arlan W.] Connecticut Coll, New London, CT 06320 USA. [Smith, Mary Ann H.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Sung, K (reprint author), CALTECH, Jet Prop Lab, M-S 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ksung@jpl.nasa.gov RI Sung, Keeyoon/I-6533-2015 FU National Aeronautics and Space Administration FX We thank J.-M. Flaud and C.A. Nixon for the C3H8 data in the 7 and 15 mu m regions. K. Sung appreciates insightful discussion and comments from Drs. Linda R. Brown (JPL) and Conor A. Nixon (GSFC). Research described in this article was performed at Connecticut College, NASA Langley Research Center and the Jet Propulsion Laboratory, California Institute of Technology, under contracts and cooperative agreements with the National Aeronautics and Space Administration. NR 61 TC 9 Z9 9 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 NOV-DEC PY 2013 VL 226 IS 2 BP 1499 EP 1513 DI 10.1016/j.icarus.2013.07.028 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 239DX UT WOS:000326003900022 ER PT J AU Le Corre, L Reddy, V Schmedemann, N Becker, KJ O'Brien, DP Yamashita, N Peplowski, PN Prettyman, TH Li, JY Cloutis, EA Denevi, BW Kneisl, T Palmer, E Gaskell, RW Nathues, A Gaffey, MJ Mittlefehldt, DW Garry, WB Sierks, H Russell, CT Raymond, CA De Sanctis, MC Ammanito, E AF Le Corre, Lucille Reddy, Vishnu Schmedemann, Nico Becker, Kris J. O'Brien, David P. Yamashita, Naoyuki Peplowski, Patrick N. Prettyman, Thomas H. Li, Jian-Yang Cloutis, Edward A. Denevi, Brett W. Kneisl, Thomas Palmer, Eric Gaskell, Robert W. Nathues, Andreas Gaffey, Michael J. Mittlefehldt, David W. Garry, William B. Sierks, Holger Russell, Christopher T. Raymond, Carol A. De Sanctis, Maria C. Ammanito, Eleonora TI Olivine or impact melt: Nature of the "Orange" material on Vesta from Dawn SO ICARUS LA English DT Article DE Asteroid Vesta; Asteroids, composition; Asteroids, surfaces; Mineralogy; Spectroscopy ID ASTEROID 4 VESTA; HUBBLE-SPACE-TELESCOPE; REFLECTANCE SPECTRA; HED METEORITES; GAMMA-RAY; NEUTRON-SPECTRA; PYROXENE BAND; TEMPERATURE; MISSION; SPECTROSCOPY AB NASA's Dawn mission observed a great variety of colored terrains on asteroid (4) Vesta during its survey with the Framing Camera (FC). Here we present a detailed study of the orange material on Vesta, which was first observed in color ratio images obtained by the FC and presents a red spectral slope. The orange material deposits can be classified into three types: (a) diffuse ejecta deposited by recent medium-size impact craters (such as Oppia), (b) lobate patches with well-defined edges (nicknamed "pumpkin patches"), and (c) ejecta rays from fresh-looking impact craters. The location of the orange diffuse ejecta from Oppia corresponds to the olivine spot nicknamed "Leslie feature" first identified by Gaffey (Gaffey, M.J. [1997]. Icarus 127, 130-157) from ground-based spectral observations. The distribution of the orange material in the FC mosaic is concentrated on the equatorial region and almost exclusively outside the Rheasilvia basin. Our in-depth analysis of the composition of this material uses complementary observations from FC, the visible and infrared spectrometer (VIR), and the Gamma Ray and Neutron Detector (GRaND). Several possible options for the composition of the orange material are investigated including, cumulate eucrite layer exposed during impact, metal delivered by impactor, olivine-orthopyroxene mixture and impact melt. Based on our analysis, the orange material on Vesta is unlikely to be metal or olivine (originally proposed by Gaffey (Gaffey, KJ. [1997]. Icarus 127, 130-157)). Analysis of the elemental composition of Oppia ejecta blanket with GRaND suggests that its orange material has similar to 25% cumulate eucrite component in a howarditic mixture, whereas two other craters with orange material in their ejecta, Octavia and Arruntia, show no sign of cumulate eucrites. Morphology and topography of the orange material in Oppia and Octavia ejecta and orange patches suggests an impact melt origin. A majority of the orange patches appear to be related to the formation of the Rheasilvia basin. Combining the interpretations from the topography, geomorphology, color and spectral parameters, and elemental abundances, the most probable analog for the orange material on Vesta is impact melt. (C) 2013 Elsevier Inc. All rights reserved. C1 [Le Corre, Lucille; Reddy, Vishnu; O'Brien, David P.; Yamashita, Naoyuki; Prettyman, Thomas H.; Li, Jian-Yang; Palmer, Eric; Gaskell, Robert W.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Le Corre, Lucille; Reddy, Vishnu; Nathues, Andreas; Sierks, Holger] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Schmedemann, Nico; Kneisl, Thomas] Free Univ Berlin, Inst Geol Sci, D-12249 Berlin, Germany. [Becker, Kris J.] USGS, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Peplowski, Patrick N.; Denevi, Brett W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Cloutis, Edward A.] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada. [Gaffey, Michael J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA. [Mittlefehldt, David W.] NASA, Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA. [Garry, William B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [De Sanctis, Maria C.; Ammanito, Eleonora] Ist Nazl Astrofis, Ist Astrofis & Planetol Spaziali, Rome, Italy. RP Le Corre, L (reprint author), Planetary Sci Inst, 1700 East Ft Lowell,Suite 106, Tucson, AZ 85719 USA. EM lecorre@psi.edu RI Denevi, Brett/I-6502-2012; Garry, Brent/I-5920-2013; Peplowski, Patrick/I-7254-2012; OI Le Corre, Lucille/0000-0003-0349-7932; Denevi, Brett/0000-0001-7837-6663; Peplowski, Patrick/0000-0001-7154-8143; De Sanctis, Maria Cristina/0000-0002-3463-4437; Prettyman, Thomas/0000-0003-0072-2831; Reddy, Vishnu/0000-0002-7743-3491 FU Dawn UCLA [2090-S-MB170]; NASA Dawn Participating Scientist Program [NNH09ZDA001N-DAVPS]; NASA Planetary Geology and Geophysics Grant [NNX07AP73G]; Dawn at Vesta Participating Scientist Program [NNX10AR21G]; German Space Agency (DLR) on behalf of the Federal Ministry of Economics and Technology [50OW1101]; NASA Discovery Program; Max Planck Society; German Space Agency, DLR; Italian Space Agency FX The authors would like to thank the Dawn Flight Operations team for a successful Dawn at Vesta mission. L.L. work is supported by Dawn UCLA subcontract# 2090-S-MB170. V.R. work is supported by NASA Dawn Participating Scientist Program Grant NNH09ZDA001N-DAVPS and NASA Planetary Geology and Geophysics Grant NNX07AP73G. D.P.O. is supported by Dawn at Vesta Participating Scientist Program Grant NNX10AR21G. NS and TK work is supported by the German Space Agency (DLR) on behalf of the Federal Ministry of Economics and Technology, Grant 50OW1101. The research utilizes spectra acquired with the NASA RELAB facility at Brown University. The authors would like to thank Guneshwar S. Thangjam for his help gathering laboratory spectral data from RELAB. E.A.C. thanks CSA, CFI, MRIF and the University of Winnipeg for supporting HOSERLab. The authors are grateful to Nicholas Moskovitz and Tom Burbine for their suggestions to improve the manuscript. The Dawn mission is led by the University of California, Los Angeles under the auspices of the NASA Discovery Program. The Framing Camera project is financially supported by the Max Planck Society and the German Space Agency, DLR. VIR is funded by the Italian Space Agency and was developed under the leadership of INAF-Istituto di Astrofisica e Planetologia Spaziali, Rome, Italy. GRaND is operated by the Planetary Science Institute. NR 97 TC 30 Z9 30 U1 1 U2 13 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD NOV-DEC PY 2013 VL 226 IS 2 BP 1568 EP 1594 DI 10.1016/j.icarus.2013.08.013 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 239DX UT WOS:000326003900028 ER PT J AU Rubincam, DP AF Rubincam, David Parry TI The solar Poynting-Robertson effect on particles orbiting Solar System bodies: Circular orbits SO ICARUS LA English DT Article DE Near-Earth objects; Interplanetary dust; Celestial mechanics; Planetary rings; Saturn, Rings ID RADIATION; ASTEROIDS; DYNAMICS; PRESSURE; FORCES; EARTH; RINGS AB The Poynting-Robertson effect from sunlight impinging directly on a particle which orbits a Solar System body (planet, asteroid, comet) is considered from the Sun's rest frame. There appear to be no significant first-order terms in V-b/c for circular orbits, where V-b is the body's speed in its orbit about the Sun and c is the speed of light, when the particle's orbital semimajor axis is much smaller than the body's orbital semimajor axis about the Sun as is mainly the case in the Solar System. Published by Elsevier Inc. C1 NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. RP Rubincam, DP (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Solar Syst Explorat Div, Code 661,Bldg 34,Room S280, Greenbelt, MD 20771 USA. EM David.P.Rubincam@nasa.gov FU NASA Advanced Exploration Systems and SALMON proposals FX I thank Joseph A. Burns and David Vokrouhlicky for correcting mistakes and making insightful comments which greatly improved the manuscript. The support of the NASA Advanced Exploration Systems and SALMON proposals is gratefully acknowledged. NR 18 TC 2 Z9 2 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD NOV-DEC PY 2013 VL 226 IS 2 BP 1618 EP 1623 DI 10.1016/j.icarus.2013.07.030 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 239DX UT WOS:000326003900031 ER PT J AU Ting, DZY Soibel, A Keo, SA Khoshakhlagh, A Hill, CJ Hoglund, L Mumolo, JM Gunapala, SD AF Ting, David Z. -Y. Soibel, Alexander Keo, Sam A. Khoshakhlagh, Arezou Hill, Cory J. Hoeglund, Linda Mumolo, Jason M. Gunapala, Sarath D. TI Superlattice and Quantum Dot Unipolar Barrier Infrared Detectors SO JOURNAL OF ELECTRONIC MATERIALS LA English DT Article DE Infrared detector; type II superlattice; quantum dot; unipolar barrier; mid-wavelength infrared; long-wavelength infrared ID PHOTODIODES; PERFORMANCE; PHOTODETECTORS; HGCDTE AB We report device performance and provide theoretical analysis of a modified long-wavelength complementary barrier infrared detector structure that incorporates a double tunnel junction contact designed for simpler material growth while retaining the robustness for processing. We also provide analysis of a mid-wavelength quantum dot barrier infrared detector and explain its spectral shape and turn-on characteristics. C1 [Ting, David Z. -Y.; Soibel, Alexander; Keo, Sam A.; Khoshakhlagh, Arezou; Hill, Cory J.; Hoeglund, Linda; Mumolo, Jason M.; Gunapala, Sarath D.] CALTECH, Jet Prop Lab, Ctr Infrared Sensors, Pasadena, CA 91109 USA. RP Ting, DZY (reprint author), CALTECH, Jet Prop Lab, Ctr Infrared Sensors, M-S 302-231,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM david.z.ting@jpl.nasa.gov RI Soibel, Alexander/A-1313-2007 FU National Aeronautics and Space Administration FX The authors thank S. Bandara, E. R. Blazejewski, D. R. Rhiger, R. E. deWames, and J.N. Schulman for helpful discussions. The authors thank R. Liang, M. Herman, E. Kolawa, and P. Dimotakis of JPL, and M. Tidrow of the US Army Night Vision Electronics Sensor Directorate for encouragement and support. The research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Government sponsorship acknowledged. NR 32 TC 6 Z9 6 U1 1 U2 16 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 NOV PY 2013 VL 42 IS 11 BP 3071 EP 3079 DI 10.1007/s11664-013-2641-9 PG 9 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA 239SW UT WOS:000326046800010 ER PT J AU Kumar, N Liang, D Comellas, A Chu, AD Abrams, T AF Kumar, Naresh Liang, Dong Comellas, Alejandro Chu, Allen D. Abrams, Thad TI Satellite-based PM concentrations and their application to COPD in Cleveland, OH SO JOURNAL OF EXPOSURE SCIENCE AND ENVIRONMENTAL EPIDEMIOLOGY LA English DT Article DE PM2.5 exposure; local time-space Kriging; aerosol optical depth; time-space lagged exposure; COPD ID PARTICULATE AIR-POLLUTION; AMBIENT PARTICULATE; LARGE DATASETS; TIME; ADMISSIONS; EXPOSURE; DISEASE; PATTERN; MATTER; CELLS AB A hybrid approach is proposed to estimate exposure to fine particulate matter (PM2.5) at a given location and time. This approach builds on satellite-based aerosol optical depth (AOD), air pollution data from sparsely distributed Environmental Protection Agency (EPA) sites and local time-space Kriging, an optimal interpolation technique. Given the daily global coverage of AOD data, we can develop daily estimate of air quality at any given location and time. This can assure unprecedented spatial coverage, needed for air quality surveillance and management and epidemiological studies. In this paper, we developed an empirical relationship between the 2 km AOD and PM2.5 data from EPA sites. Extrapolating this relationship to the study domain resulted in 2.3 million predictions of PM2.5 between 2000 and 2009 in Cleveland Metropolitan Statistical Area (MSA). We have developed local time-space Kriging to compute exposure at a given location and time using the predicted PM2.5. Daily estimates of PM2.5 were developed for Cleveland MSA between 2000 and 2009 at 2.5 km spatial resolution; 1.7 million (similar to 79.8%) of 2.13 million predictions required for multiyear and geographic domain were robust. In the epidemiological application of the hybrid approach, admissions for an acute exacerbation of chronic obstructive pulmonary disease (AECOPD) was examined with respect to time-space lagged PM2.5 exposure. Our analysis suggests that the risk of AECOPD increases 2.3% with a unit increase in PM2.5 exposure within 9 days and 0.05 degrees (similar to 5 km) distance lags. In the aggregated analysis, the exposed groups (who experienced exposure to PM2.5 > 15.4 mu g/m(3)) were 54% more likely to be admitted for AECOPD than the reference group. The hybrid approach offers greater spatiotemporal coverage and reliable characterization of ambient concentration than conventional in situ monitoring-based approaches. Thus, this approach can potentially reduce exposure misclassification errors in the conventional air pollution epidemiology studies. C1 [Kumar, Naresh] Univ Miami, Dept Publ Hlth Sci, Miami, FL 33136 USA. [Liang, Dong] Univ Iowa, Dept Epidemiol, Iowa City, IA USA. [Comellas, Alejandro] Univ Iowa, Dept Pulm Med, Iowa City, IA USA. [Chu, Allen D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Abrams, Thad] Iowa City VA Med Ctr, Iowa City, IA USA. RP Kumar, N (reprint author), Univ Miami, Dept Publ Hlth Sci, Miami, FL 33136 USA. EM nkumar@med.miami.edu RI Liang, Dong/J-3691-2016; OI Liang, Dong/0000-0002-0550-7324; Comellas, Alejandro/0000-0003-1521-7520 FU National Institute of Health [5R21ES014004-02]; EPA [RFQ-RT-10-00204] FX This work was funded in part by the National Institute of Health (5R21ES014004-02) and EPA (RFQ-RT-10-00204). NR 50 TC 16 Z9 16 U1 0 U2 15 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1559-0631 EI 1559-064X J9 J EXPO SCI ENV EPID JI J. Expo. Sci. Environ. Epidemiol. PD NOV-DEC PY 2013 VL 23 IS 6 BP 637 EP 646 DI 10.1038/jes.2013.52 PG 10 WC Environmental Sciences; Public, Environmental & Occupational Health; Toxicology SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Toxicology GA 240ID UT WOS:000326087900009 PM 24045428 ER PT J AU Zirbel, SA Lang, RJ Thomson, MW Sigel, DA Walkemeyer, PE Trease, BP Magleby, SP Howell, LL AF Zirbel, Shannon A. Lang, Robert J. Thomson, Mark W. Sigel, Deborah A. Walkemeyer, Phillip E. Trease, Brian P. Magleby, Spencer P. Howell, Larry L. TI Accommodating Thickness in Origami-Based Deployable Arrays SO JOURNAL OF MECHANICAL DESIGN LA English DT Article AB The purpose of this work is to develop approaches to accommodate thickness in origami-based deployable arrays with a high ratio of deployed-to-stowed diameter. The origami flasher model serves as a basis for demonstrating the approach. A thickness-accommodating mathematical model is developed to describe the flasher. Practical modifications are presented for the creation of physical models and two options are proposed: allowing the panels to fold along their diagonals or applying a membrane backing with specified widths at fold-lines. The mathematical model and hardware modifications are employed to create several physical models. The results are general and apply to a range of applications. An example is provided by the application that motivated the work: a deployable solar array for space applications. The model is demonstrated in hardware as a 1/20th scale prototype with a ratio of deployed-to-stowed diameter of 9.2 (or 1.25m deployed outer diameter to 0.136m stowed outer diameter). C1 [Zirbel, Shannon A.; Magleby, Spencer P.; Howell, Larry L.] Brigham Young Univ, Dept Mech Engn, Provo, UT 84602 USA. [Lang, Robert J.] Lang Origami, Alamo, CA 94507 USA. [Thomson, Mark W.; Sigel, Deborah A.; Walkemeyer, Phillip E.; Trease, Brian P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Howell, LL (reprint author), Brigham Young Univ, Dept Mech Engn, Provo, UT 84602 USA. EM lhowell@byu.edu RI Howell, Larry/A-6828-2008 OI Howell, Larry/0000-0001-8132-8822 FU NASA Office of the Chief Technologist's Space Technology Research Fellowship; National Science Foundation [1240417]; National Aeronautics and Space Administration; NSF EFRI-ODISSEI; Jet Propulsion Laboratory FX This work was supported by a NASA Office of the Chief Technologist's Space Technology Research Fellowship and the National Science Foundation through Award No. 1240417. 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. Author RJL would like to acknowledge support from NSF EFRI-ODISSEI and from Jet Propulsion Laboratory for the reported work. A special thanks to Mary Wilson and the Compliant Mechanisms Research Group at BYU for prototyping assistance, and to Dennis West at BYU for creating the computer animation. NR 21 TC 60 Z9 60 U1 8 U2 35 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 1050-0472 J9 J MECH DESIGN JI J. Mech. Des. PD NOV PY 2013 VL 135 IS 11 SI SI AR 111005 DI 10.1115/1.4025372 PG 11 WC Engineering, Mechanical SC Engineering GA 241NC UT WOS:000326172900006 ER PT J AU Chao, WC AF Chao, Winston C. TI Catastrophe-Concept-Based Cumulus Parameterization: Correction of Systematic Errors in the Precipitation Diurnal Cycle over Land in a GCM SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article DE Convective parameterization; Model errors; Parameterization ID MESOSCALE CONVECTIVE SYSTEM; HIGH-RESOLUTION SIMULATION; LARGE-SCALE ENVIRONMENT; GENERAL-CIRCULATION; DEEP CONVECTION; HYDROLOGIC-CYCLE; CLOUD ENSEMBLE; UNITED-STATES; MODEL; VARIABILITY AB The onset of cumulus convection in a grid column is a catastrophe, also known as a subcritical instability. Accordingly, in designing a cumulus parameterization scheme the onset of cumulus convection requires that a parameter crosses a critical value and the termination of cumulus convection requires that the same or a different parameter crosses a different critical value. Once begun, cumulus convection continues to exist, regardless of whether the onset criterion is still met, until the termination criterion is met. Also, the intensity of cumulus precipitation is related to how far the state is from the termination, not the onset, criterion.The cumulus parameterization schemes currently in use in GCMs, however, treat the onset of cumulus convection as a supercritical instability; namely, convection is turned on when a parameter exceeds a critical value and is turned off when the same parameter falls below the same critical value. Also, the intensity of cumulus precipitation is related to how far this critical value has been exceeded. Among the adverse consequences of the supercritical-instability-concept-based cumulus parameterization schemes are that over relatively flat land the precipitation peak occurs around noon4-6 h too soonand that the amplitude of the precipitation diurnal cycle is too weak.Based on the above-mentioned concept, a new cumulus parameterization scheme was designed by taking advantage of the existing infrastructure of the relaxed Arakawa-Schubert scheme (RAS), but replacing RAS's guiding principle with the catastrophe concept. Test results using NASA's Goddard Earth Observing System GCM, version 5 (GEOS-5), show dramatic improvement in the phase and amplitude of the precipitation diurnal cycle over relatively flat land. C1 NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Chao, WC (reprint author), NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Mail Code 610-1,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM winston.c.chao@nasa.gov FU NASA's Modeling, Analysis, and Prediction program [WBS 802678.02.17.01.25] FX Technical help from Larry Takacs and Max Suarez, both of NASA GSFC GMAO, in using the GEOS-5 GCM is gratefully acknowledged. Myong-In Lee generously provided Fig. 5 and the postprocessing computer program that produced Fig. 6. Suggestions from Michele Rienecker and Kay Cheney improved the manuscript writing. W. W. Grabowski and P. A. Dirmeyer and two anonymous reviewers provided helpful reviews of the manuscript. This work was supported by NASA's Modeling, Analysis, and Prediction program under 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 Simulation (NCCS) at Goddard Space Flight Center. NR 50 TC 11 Z9 11 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 NOV PY 2013 VL 70 IS 11 BP 3599 EP 3614 DI 10.1175/JAS-D-13-022.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 243YP UT WOS:000326354600014 ER PT J AU Pauluis, OM Mrowiec, AA AF Pauluis, Olivier M. Mrowiec, Agnieszka A. TI Isentropic Analysis of Convective Motions SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article DE Convection; Convective clouds; Deep convection; Lagrangian circulation; transport; Isentropic analysis ID GLOBAL ATMOSPHERIC CIRCULATION; SHALLOW CUMULUS CONVECTION; POTENTIAL VORTICITY; MEAN-FLOW; RESOLUTION; TROPOSPHERE; SIMULATION; WAVES AB This paper analyzes the convective mass transport by sorting air parcels in terms of their equivalent potential temperature to determine an isentropic streamfunction. By averaging the vertical mass flux at a constant value of the equivalent potential temperature, one can compute an isentropic mass transport that filters out reversible oscillatory motions such as gravity waves. This novel approach emphasizes the fact that the vertical energy and entropy transports by convection are due to the combination of ascending air parcels with high energy and entropy and subsiding air parcels with lower energy and entropy. Such conditional averaging can be extended to other dynamic and thermodynamic variables such as vertical velocity, temperature, or relative humidity to obtain a comprehensive description of convective motions. It is also shown how this approach can be used to determine the mean diabatic tendencies from the three-dimensional dynamic and thermodynamic fields.A two-stream approximation that partitions the isentropic circulation into a mean updraft and a mean downdraft is also introduced. This offers a straightforward way to identify the mean properties of rising and subsiding air parcels. The results from the two-stream approximation are compared with two other definitions of the cloud mass flux. It is argued that the isentropic analysis offers a robust definition of the convective mass transport that is not tainted by the need to arbitrarily distinguish between convection and its environment, and that separates the irreversible convective overturning from oscillations associated with gravity waves. C1 [Pauluis, Olivier M.] NYU, Ctr Atmosphere Ocean Sci, Courant Inst Math Sci, New York, NY 10012 USA. [Mrowiec, Agnieszka A.] Columbia Univ, New York, NY USA. [Mrowiec, Agnieszka A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Pauluis, OM (reprint author), NYU, Ctr Atmosphere Ocean Sci, Courant Inst Math Sci, 251 Mercer St, New York, NY 10012 USA. EM pauluis@cims.nyu.edu FU NSF [AGS-0944058]; New York University Abu Dhabi Research Institute; DOE Office of Science, Office of Biological and Environmental Research [DE-PS02-09ER09-01] FX We are thankful to the two anonymous reviewers and the editor for their constructive comments on the manuscript. Olivier Pauluis is supported by the NSF under Grant AGS-0944058 and by the New York University Abu Dhabi Research Institute. Agnieszka Mrowiec's contribution to this research was supported by the DOE Office of Science, Office of Biological and Environmental Research, through Contract DE-PS02-09ER09-01 within the scope of the FASTER Project. NR 32 TC 15 Z9 15 U1 0 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 EI 1520-0469 J9 J ATMOS SCI JI J. Atmos. Sci. PD NOV PY 2013 VL 70 IS 11 BP 3673 EP 3688 DI 10.1175/JAS-D-12-0205.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 243YP UT WOS:000326354600019 ER PT J AU Chu, DA Tsai, TC Chen, JP Chang, SC Jeng, YJ Chiang, WL Lin, NH AF Chu, D. Allen Tsai, Tzu-Chin Chen, Jen-Ping Chang, Shuenn-Chin Jeng, Yung-Jyh Chiang, Wei-Li Lin, Neng-Hui TI Interpreting aerosol lidar profiles to better estimate surface PM2.5 for columnar AOD measurements SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Taiwan; MODIS; Aerosol optical depth; Planetary boundary layer height; Haze layer height; Particulate matter ID IMAGING SPECTRORADIOMETER MODIS; PARTICULATE AIR-POLLUTION; LONG-RANGE TRANSPORT; OPTICAL DEPTH; ASIAN DUST; QUALITY ASSESSMENT; MICROPULSE LIDAR; TAIWAN; MATTER; URBAN AB Satellite aerosol optical depth (AOD) products have been used to estimate surface PM2.5 in different parts of the world. However, some revealed good but some relatively poorer relationship between AOD and PM2.5. The increasingly available lidar-based aerosol extinction profiles provide insights into the boundary layer as well as residual above it. Here we report a study in Taiwan using four-year (2006-2009) MPLNet data to characterize aerosol vertical distribution. We derived haze layer height (HLH) from MPLNet aerosol extinction profiles and classified profile differences by mean PBL extinction (MPE) and near-surface extinction (NSE). The former represents the mean extinction within boundary layer and the latter the closest extinction to surface. The comparison of MPE versus NSE leads to three distinct classifications of aerosol profiles to help interpret the relationship between AOD and PM2.5. The approximation of normalizing AOD AERONET by HLH closely follows MPE in correlating with PM2.5 (>= 0.8 with respect to season or >= 0.85 with respect to profile classification). The correlation resulted from AODmonis/HLH is systematically lower than that derived by AODAERONET/HLH. PM2.5 values are overall better estimated by profile classification than those derived by season. Better performance of PM2.5 is obtained with the approximation (i.e., normalizing AOD by HLH) than that using AOD only. The performance metrics used in quantifying the relationship reveal improvements in uncertainty by 2.9 mu g m(-3) (or 20%) with AODAERoNET/HLH and 2.3 mu g m(-3) (or 15%) with AODmonis/HLH in comparison to using ADD only. 2013 Elsevier Ltd. All rights reserved. C1 [Chu, D. Allen] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD USA. [Chu, D. Allen] NASA, Climate & Radiat Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tsai, Tzu-Chin; Chen, Jen-Ping; Jeng, Yung-Jyh] Natl Taiwan Univ, Dept Atmospher Sci, Taipei 10764, Taiwan. [Lin, Neng-Hui] Natl Cent Univ, Dept Atmospher Sci, Zhong Li, Taiwan. RP Chu, DA (reprint author), NASA, Climate & Radiat Lab, Goddard Space Flight Ctr, Code 613-2, Greenbelt, MD 20771 USA. EM allen.chu@nasa.gov; tzuchin@webmail2.as.ntu.edu.tw; jpchen@as.ntu.edu.tw; scchang@epa.gov.tw; yjjeng@webmail2.as.ntu.edu.tw; wlchiang@epa.gov.tw; nhlin@cc.ncu.edu.tw RI Chen, Jen-Ping/F-2947-2010; Xiongfei, Zhao/G-7690-2015 OI Chen, Jen-Ping/0000-0003-4188-6189; FU Taiwan EPA grant [EPA-100-FA11-03-A016]; NASA DISCOVERAQ grant [NNX1OAR41G] FX We would like to thank NASA Data Distribution and Archive Center for processing and providing MODIS AOD products. Data analysis and back trajectory modeling are performed under the Taiwan EPA grant (EPA-100-FA11-03-A016) while the development of the approximation theory is under the work of NASA DISCOVERAQ grant (NNX1OAR41G). NR 57 TC 15 Z9 15 U1 1 U2 34 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 NOV PY 2013 VL 79 BP 172 EP 187 DI 10.1016/j.atmosenv.2013.06.031 PG 16 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 236YF UT WOS:000325834700021 ER PT J AU Chew, BN Campbell, JR Salinas, SV Chang, CW Reid, JS Welton, EJ Holben, BN Liew, SC AF Chew, Boon Ning Campbell, James R. Salinas, Santo V. Chang, Chew Wai Reid, Jeffrey S. Welton, Ellsworth J. Holben, Brent N. Liew, Soo Chin TI Aerosol particle vertical distributions and optical properties over Singapore SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE AERONET; ENSO; MPLNET; Lidar; Maritime Continent; Southeast Asia ID SPECTRAL-RESOLUTION LIDAR; SUN-PHOTOMETER DATA; MARITIME CONTINENT; MICROPULSE LIDAR; SOUTHEAST-ASIA; FORECAST MODEL; BOUNDARY-LAYER; CLOUD; DEPTH; SENSITIVITY AB As part of the Seven Southeast Asian Studies (7SEAS) program, an Aerosol Robotic Network (AERONET) sun photometer and a Micro-Pulse Lidar Network (MPLNET) instrument have been deployed at Singapore to study the regional aerosol environment of the Maritime Continent (MC). Using coincident AERONET Level 2.0 and MPLNET Level 2.0a data from 24 September 2009 to 31 March 2011, the seasonal variability of aerosol particle vertical distributions and optical properties is examined. On average, the bulk (similar to 65%) of aerosol extinction is found below 1.5 km with substantial aerosol loading (similar to 35%) above. Possibly due to the transition from El Nifio to La Nifia conditions and subsequent reduction in fire events, the MPLNET mean integrated aerosol extinction is observed to be the lowest for July September 2010, which coincides with the typical MC biomass burning season. On the other hand, the highest mean integrated extinctions are derived for January March 2010 and 2011, which can be attributed to off-season MC biomass burning smoke and anthropogenic pollution. The seasonal lidar ratios also show higher occurrences >60 sr, which are indicative of biomass burning smoke, for October 2009 June 2010, but such occurrences decrease from July 2010 to March 2011 when La Nifia conditions prevail. In addition, principal component analysis (PCA) identifies five primary aerosol vertical profile types over Singapore, i.e. strongly-capped/deep near-surface layer (SCD; 0-1.35 km), enhanced mid-level layer (EML; 1.35-2.4 km), enhanced upper-level layer (EUL; 2.4-3.525 km), deep contiguous layer (DCL; 3.525-4.95 km) and deep multi-layer (DML; >4.95 km). PCA also identifies an off-season MC biomass burning smoke event from 22 February to 8 March 2010, which is subsequently examined in detail. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Chew, Boon Ning; Salinas, Santo V.; Chang, Chew Wai; Liew, Soo Chin] Natl Univ Singapore, Ctr Remote Imaging Sensing & Proc, Singapore 119076, Singapore. [Campbell, James R.; Reid, Jeffrey S.] Naval Res Lab, Marine Meteorol Div, Monterey, CA 93943 USA. [Welton, Ellsworth J.] NASA, Goddard Space Flight Ctr, Micro Pulse Lidar Network, Greenbelt, MD 20771 USA. [Holben, Brent N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Chew, BN (reprint author), Natl Univ Singapore, Ctr Remote Imaging Sensing & Proc, Block S17,Level 2,10 Lower Kent Ridge Rd, Singapore 119076, Singapore. EM crscbn@nus.edu.sg RI Campbell, James/C-4884-2012; Reid, Jeffrey/B-7633-2014; Liew, Soo Chin/C-9187-2011; Chew, Boon Ning/M-2405-2016 OI Campbell, James/0000-0003-0251-4550; Reid, Jeffrey/0000-0002-5147-7955; Liew, Soo Chin/0000-0001-8342-4682; Chew, Boon Ning/0000-0002-2933-7788 FU NASA Earth Observing System and Radiation Sciences Programs; Office of Naval Research (ONR); ONR Global and NASA; NASA Interagency Agreement NNG12HGO5I on behalf of NASA MPLNET FX AERONETand MPLNETare supported with funding from the NASA Earth Observing System and Radiation Sciences Programs. The AERONET and MPLNET instruments are deployed at Singapore as part of the Seven Southeast Asian Studies (7SEAS) field campaign, as sponsored by the Office of Naval Research (ONR), ONR Global and NASA. Dr. Campbell acknowledges the support of NASA Interagency Agreement NNG12HGO5I on behalf of NASA MPLNET. Dr. Reid's participation is supported by the NRL 6.1 Base Program. The authors would like to thank the Department of Civil and Environmental Engineering, and NUS Environmental Research Institute (NERI) at the National University of Singapore for hosting the 7SEAS atmospheric measurement supersite, and Singapore's National Environment Agency for collecting and archiving the surface air quality data. NR 68 TC 11 Z9 11 U1 1 U2 26 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD NOV PY 2013 VL 79 BP 599 EP 613 DI 10.1016/j.atmosenv.2013.06.026 PG 15 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 236YF UT WOS:000325834700068 ER PT J AU Turner, RT Iwaniec, UT Wong, CP Lindenmaier, LB Wagner, LA Branscum, AJ Menn, SA Taylor, J Zhang, Y Wu, HL Sibonga, JD AF Turner, Russell T. Iwaniec, Urszula T. Wong, Carmen P. Lindenmaier, Laurence B. Wagner, Lindsay A. Branscum, Adam J. Menn, Scott A. Taylor, James Zhang, Ye Wu, Honglu Sibonga, Jean D. TI Acute exposure to high dose gamma-radiation results in transient activation of bone lining cells SO BONE LA English DT Article DE Murine; Bone histomorphometry; Osteoblasts; Osteoclasts; Osteoporosis; Bone marrow ID WHOLE-BODY IRRADIATION; MARROW ABLATION; TRABECULAR BONE; GROWTH-FACTOR; GROWING RATS; X-RAYS; MICE; ESTROGEN; CANCER; HYPERPARATHYROIDISM AB The present studies investigated the cellular mechanisms for the detrimental effects of high dose whole body gamma-irradiation on bone. In addition, radioadaptation and bone marrow transplantation were assessed as interventions to mitigate the skeletal complications of irradiation. Increased trabecular thickness and separation and reduced cancellous bone volume fraction, connectivity density, and trabecular number were detected in proximal tibia and lumbar vertebra 14 days following gamma-irradiation with 6 Gy. To establish the cellular mechanism for the architectural changes, vertebrae were analyzed by histomorphometry 1, 3, and 14 days following irradiation. Marrow cell density decreased within 1 day (67% reduction, p < 0.0001), reached a minimum value after 3 days (86% reduction, p < 0.0001), and partially rebounded by 14 days (30% reduction, p = 0.0025) following irradiation. In contrast, osteoblast-lined bone perimeter was increased by 290% (1 day, p = 0.04), 1230% (3 days, p < 0.0001), and 530% (14 days, p = 0.003), respectively. There was a strong association between radiation-induced marrow cell death and activation of bone lining cells to express the osteoblast phenotype (Pearson correlation -0.85, p < 0.0001). An increase (p = 0.004) in osteoclast-lined bone perimeter was also detected with irradiation. A priming dose of gamma-radiation (0.5 mGy), previously shown to reduce mortality, had minimal effect on the cellular responses to radiation and did not prevent detrimental changes in bone architecture. Bone marrow transplantation normalized marrow cell density, bone turnover, and most indices of bone architecture following irradiation. In summary, radiation-induced death of marrow cells is associated with 1) a transient increase in bone formation due, at least in part, to activation of bone lining cells, and 2) an increase in bone resorption due to increased osteoclast perimeter. Bone marrow transplantation is effective in mitigating the detrimental effects of acute exposure to high dose whole body gamma-radiation on bone turnover. (C) 2013 Elsevier Inc. All rights reserved. C1 [Turner, Russell T.; Iwaniec, Urszula T.; Wong, Carmen P.; Lindenmaier, Laurence B.; Wagner, Lindsay A.] Oregon State Univ, Sch Biol & Populat Hlth Sci, Skeletal Biol Lab, Corvallis, OR 97331 USA. [Turner, Russell T.; Iwaniec, Urszula T.] Oregon State Univ, Ctr Healthy Aging Res, Corvallis, OR 97331 USA. [Branscum, Adam J.] Oregon State Univ, Sch Biol & Populat Hlth Sci, Corvallis, OR 97331 USA. [Menn, Scott A.] Oregon State Univ, Ctr Radiat, Corvallis, OR 97331 USA. [Taylor, James; Zhang, Ye; Wu, Honglu; Sibonga, Jean D.] NASA, Johnson Space Ctr, Houston, TX USA. [Zhang, Ye] Wyle Integrated Sci & Engn Grp, Houston, TX USA. RP Turner, RT (reprint author), Oregon State Univ, Sch Biol & Populat Hlth Sci, Skeletal Biol Lab, Corvallis, OR 97331 USA. EM Russell.Turner@oregonstate.edu FU NASA [NNX12AL24G]; National Institute of Health [AR 060913] FX This work was supported by the NASA grant number NNX12AL24G (to RT Turner) and by the National Institute of Health grant AR 060913 (to UT Iwaniec). NR 55 TC 9 Z9 9 U1 0 U2 8 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 8756-3282 EI 1873-2763 J9 BONE JI Bone PD NOV PY 2013 VL 57 IS 1 BP 164 EP 173 DI 10.1016/j.bone.2013.08.002 PG 10 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 235TC UT WOS:000325742600023 PM 23954507 ER PT J AU Acikmese, B Carson, JM Blackmore, L AF Acikmese, Behcet Carson, John M., III Blackmore, Lars TI Lossless Convexification of Nonconvex Control Bound and Pointing Constraints of the Soft Landing Optimal Control Problem SO IEEE TRANSACTIONS ON CONTROL SYSTEMS TECHNOLOGY LA English DT Article DE Convex optimization; convexification; interior point method algorithms; optimal control; planetary soft landing ID CONVEX-OPTIMIZATION; DESCENT GUIDANCE; POWERED-DESCENT; SEMIDEFINITE AB Planetary soft landing is one of the benchmark problems of optimal control theory and is gaining renewed interest due to the increased focus on the exploration of planets in the solar system, such as Mars. The soft landing problem with all relevant constraints can be posed as a finite-horizon optimal control problem with state and control constraints. The real-time generation of fuel-optimal paths to a prescribed location on a planet's surface is a challenging problem due to the constraints on the fuel, the control inputs, and the states. The main difficulty in solving this constrained problem is the existence of nonconvex constraints on the control input, which are due to a nonzero lower bound on the control input magnitude and a nonconvex constraint on its direction. This paper introduces a convexification of the control constraints that is proven to be lossless; i.e., an optimal solution of the soft landing problem can be obtained via solution of the proposed convex relaxation of the problem. The lossless convexification enables the use of interior point methods of convex optimization to obtain optimal solutions of the original nonconvex optimal control problem. C1 [Acikmese, Behcet] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA. [Carson, John M., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Blackmore, Lars] SpaceX Co, Hawthorne, CA 90250 USA. RP Acikmese, B (reprint author), Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA. EM behcet@austin.utexas.edu; jmcarson@jpl.nasa.gov; lars.blackmore@spacex.com FU National Aeronautics and Space Administration FX The authors would like to thank M. Ivanov and J. Casoliva of the Jet Propulsion Laboratory for their valuable comments, and S. Boyd, Y. Wang, and J. Mattingley of Stanford University for their insights on convexification and real-time convex optimization. This research was partially performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 29 TC 11 Z9 13 U1 0 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1063-6536 EI 1558-0865 J9 IEEE T CONTR SYST T JI IEEE Trans. Control Syst. Technol. PD NOV PY 2013 VL 21 IS 6 BP 2104 EP 2113 DI 10.1109/TCST.2012.2237346 PG 10 WC Automation & Control Systems; Engineering, Electrical & Electronic SC Automation & Control Systems; Engineering GA 240OG UT WOS:000326105800009 ER PT J AU Davies, TJ Wolkovich, EM Kraft, NJB Salamin, N Allen, JM Ault, TR Betancourt, JL Bolmgren, K Cleland, EE Cook, BI Crimmins, TM Mazer, SJ McCabe, GJ Pau, S Regetz, J Schwartz, MD Travers, SE AF Davies, T. Jonathan Wolkovich, Elizabeth M. Kraft, Nathan J. B. Salamin, Nicolas Allen, Jenica M. Ault, Toby R. Betancourt, Julio L. Bolmgren, Kjell Cleland, Elsa E. Cook, Benjamin I. Crimmins, Theresa M. Mazer, Susan J. McCabe, Gregory J. Pau, Stephanie Regetz, Jim Schwartz, Mark D. Travers, Steven E. TI Phylogenetic conservatism in plant phenology SO JOURNAL OF ECOLOGY LA English DT Article DE climate change; flowering times; phenology; phylogenetic conservatism; plant-climate interactions; plasticity; spring indices ID FLOWERING PHENOLOGY; CLIMATE-CHANGE; PHENOTYPIC PLASTICITY; SPRING PHENOLOGY; LIFE-HISTORY; NICHE CONSERVATISM; NATURAL-SELECTION; FUNCTIONAL TRAIT; NORTH-AMERICA; GLOBAL CHANGE AB Phenological events - defined points in the life cycle of a plant or animal - have been regarded as highly plastic traits, reflecting flexible responses to various environmental cues. The ability of a species to track, via shifts in phenological events, the abiotic environment through time might dictate its vulnerability to future climate change. Understanding the predictors and drivers of phenological change is therefore critical. Here, we evaluated evidence for phylogenetic conservatism - the tendency for closely related species to share similar ecological and biological attributes - in phenological traits across flowering plants. We aggregated published and unpublished data on timing of first flower and first leaf, encompassing 4000 species at 23 sites across the Northern Hemisphere. We reconstructed the phylogeny for the set of included species, first, using the software program Phylomatic, and second, from DNA data. We then quantified phylogenetic conservatism in plant phenology within and across sites. We show that more closely related species tend to flower and leaf at similar times. By contrasting mean flowering times within and across sites, however, we illustrate that it is not the time of year that is conserved, but rather the phenological responses to a common set of abiotic cues. Our findings suggest that species cannot be treated as statistically independent when modelling phenological responses.Synthesis. Closely related species tend to resemble each other in the timing of their life-history events, a likely product of evolutionarily conserved responses to environmental cues. The search for the underlying drivers of phenology must therefore account for species' shared evolutionary histories. C1 [Davies, T. Jonathan] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Wolkovich, Elizabeth M.] Univ British Columbia, Biodivers Res Ctr, Vancouver, BC V5Z 1M9, Canada. [Kraft, Nathan J. B.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Salamin, Nicolas] Univ Lausanne, Dept Ecol & Evolut, CH-1015 Lausanne, Switzerland. [Salamin, Nicolas] Swiss Inst Bioinformat, CH-1015 Lausanne, Switzerland. [Allen, Jenica M.] Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA. [Ault, Toby R.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Betancourt, Julio L.] US Geol Survey, Reston, VA 22092 USA. [Bolmgren, Kjell] Lund Univ, Lund, Sweden. [Bolmgren, Kjell] Swedish Univ Agr Sci, Swedish Natl Phenol Network, Lund, Sweden. [Cleland, Elsa E.] Univ Calif San Diego, Ecol Behav & Evolut Sect, San Diego, CA 92103 USA. [Cook, Benjamin I.] NASA Goddard Inst Space Studies, New York, NY USA. [Cook, Benjamin I.] Lamont Doherty Earth Observ, Palisades, NY USA. [Crimmins, Theresa M.] USA Natl Phenol Network, Tucson, AZ USA. [Mazer, Susan J.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. [McCabe, Gregory J.] US Geol Survey, Denver, CO 80225 USA. [Pau, Stephanie] Florida State Univ, Dept Geog, Tallahassee, FL 32306 USA. [Regetz, Jim] Natl Ctr Ecol Anal & Synth, Santa Barbara, CA USA. [Schwartz, Mark D.] Univ Wisconsin, Dept Geog, Milwaukee, WI 53201 USA. [Travers, Steven E.] N Dakota State Univ, Dept Biol Sci, Fargo, ND 58105 USA. RP Davies, TJ (reprint author), McGill Univ, Dept Biol, 1205 Doctor Penfield Ave, Montreal, PQ H3A 1B1, Canada. EM j.davies@mcgill.ca RI Cook, Benjamin/H-2265-2012; Kraft, Nathan/A-2817-2012; Bolmgren, Kjell/E-1459-2016 OI Kraft, Nathan/0000-0001-8867-7806; Bolmgren, Kjell/0000-0001-9552-9684 FU National Center for Ecological Analysis and Synthesis, a Center; NSF [EF-0553768]; University of California, Santa Barbara; State of California; National Science Foundation [IOS-0639794]; NSF's Postdoctoral Fellow program [DBI-0905806]; NSF LTER program (NSF Grant) [BSR 88-11906, DEB 9411976, DEB 0080529, DEB 0217774]; Department of Botany, Smithsonian National Museum of National History; NSF grant [DEB 0238331, 0922080]; Luquillo NSF DEB grants [9411973, 0080538, 0218039, 0620910, 0614659]; Konza Environmental Education Program (KEEP) FX This work was conducted as a part of the 'Forecasting Phenology' Working Group supported by the National Center for Ecological Analysis and Synthesis, a Center funded by NSF (Grant #EF-0553768), the University of California, Santa Barbara, and the State of California. Additional support was also provided by the USA - National Phenology Network (USA-NPN) and its Research Coordination Network (supported by National Science Foundation Grant IOS-0639794). Support for EMW for came from NSF's Postdoctoral Fellow program (Grant DBI-0905806). We thank B. McGill for his contribution to the working group. Special thanks to all data holder and curators, including (in no particular order) David Inouye and George Aldridge (Gothic), Paul Huth, Shanan Smiley and John Thompson (Mohonk Preserve), John O'Keefe (Harvard), Tim Sparks (Marsham), Richard Primack and Abe Miller-Rushing (Concord), Dan Herms (OPG and Herms data from Ohio and Michigan), Jess Zimmerman, Chris Nytch and Jimena Forero-Montana (Luquillo), K. Vanderbilt and K. Wetherill (Sevilleta), Joe Wright (BCI), Sylvia Orli, with special acknowledgement of the two main data contributors, Aaron Goldberg and the late John Wurdack (Washington, D. C.), A. H. Fitter with special acknowledgement of the late R. S. R. Fitter (Chinnor, UK) and to M. Lechowicz, who provided an electronic version of the data from the late T. Mikesell (Wauseon). Ethel Johansson kindly shared the data collected by her late husband, Gunnar Johansson.; Significant funding for the collection of some data was provided by the NSF LTER program (NSF Grant numbers BSR 88-11906, DEB 9411976, DEB 0080529 and DEB 0217774). Data collection for Washington D. C. was supported by A. Goldberg and J. Wurdack and is organized through the Department of Botany, Smithsonian National Museum of National History. Data from Gothic were supported by NSF grant DEB 0238331 and 0922080; data from Luquillo NSF DEB grants: #9411973, #0080538, #0218039, #0620910, #0614659, #0218039. Some data used in this publication were obtained by scientists of the Hubbard Brook Ecosystem Study. The Hubbard Brook Experimental Forest is operated and maintained by the Northeastern Research Station, US Department of Agriculture, Newtown Square, Pennsylvania. Data for Konza supported by Konza Environmental Education Program (KEEP). The SI models were developed using phenological data that now reside and are available through the National Phenology Database at the USA National Phenology Network. NR 76 TC 42 Z9 44 U1 10 U2 143 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-0477 EI 1365-2745 J9 J ECOL JI J. Ecol. PD NOV PY 2013 VL 101 IS 6 BP 1520 EP 1530 DI 10.1111/1365-2745.12154 PG 11 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 238XE UT WOS:000325984300015 ER PT J AU Villanueva, GL Magee-Sauer, K Mumma, MJ AF Villanueva, G. L. Magee-Sauer, K. Mumma, M. J. TI Modeling of nitrogen compounds in cometary atmospheres: Fluorescence models of ammonia (NH3), hydrogen cyanide (HCN), hydrogen isocyanide (HNC) and cyanoacetylene (HC3N) SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Planetary atmospheres; Nitrogen species; Comets; Fluorescence ID COMPUTED LINE LIST; O1 HALE-BOPP; SYNTHETIC SPECTRA; ISOTOPIC CO2; BAND SYSTEM; MOLECULES; TRANSMITTANCE; PLANETARY; HALLEY; WATER AB We developed full cascade fluorescence models for NH3, HCN and HNC, and a new band model for the nu(1) ro-vibrational band of HC3N. The models are based on ab-initio spectral databases containing millions of spectral lines and also include extremely precise spectral information contained in several high-resolution spectral databases. Using these new models we derive detailed cascade maps for these species, and obtain realistic fluorescence efficiencies applicable to high-resolution infrared spectra. The new models permit accurate synthesis of line-by-line spectra for a wide range of rotational temperatures. We validated the models by comparing simulated emissions of these nitrogen species with measured spectra of comet C/2007 W1 (Boattini) acquired with high-resolution infrared spectrometers at high altitude sites. The new models accurately describe the complex emission spectrum, providing distinct rotational temperatures and production rates at greatly improved accuracy compared with results derived from earlier fluorescence models. In addition, we made use of the completeness and scope of the new databases to investigate possible HCN <-> HNC radiative isomerization mechanisms, obtaining estimates of conversion efficiencies under typical cometary conditions. (C) 2013 Elsevier Ltd. All rights reserved. C1 [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. [Magee-Sauer, K.] Rowan Univ, Dept Phys & Astron, Glassboro, NJ USA. RP Villanueva, GL (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Mailstop 690-3, Greenbelt, MD 20771 USA. EM Geronimo.Villanueva@nasa.gov RI Magee-Sauer, Karen/K-6061-2015 OI Magee-Sauer, Karen/0000-0002-4979-9875 FU NASA's Planetary Atmospheres and Planetary Astronomy Programs [08-PATM08-0031, 08-PAST08-0033/34, 11-PAST11-0045]; NASA's Astrobiology Institute [NAI5/NNH08ZDA002C]; Planetary Astronomy RUI program of the National Science Foundation FX GLV and MJM acknowledge support from NASA's Planetary Atmospheres and Planetary Astronomy Programs (08-PATM08-0031 (PI: GLV), 08-PAST08-0033/34 (PI: MJM), 11-PAST11-0045 (PI: MJM)), NASA's Astrobiology Institute (NAI5/NNH08ZDA002C, PI: MJM). KMS was supported by the Planetary Astronomy RUI program of the National Science Foundation. NR 43 TC 8 Z9 8 U1 1 U2 23 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV PY 2013 VL 129 BP 158 EP 168 DI 10.1016/j.jqsrt.2013.06.010 PG 11 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 237BQ UT WOS:000325843600015 ER PT J AU El-Gabry, LA Thurman, DR Poinsatte, PE Heidmann, JD AF El-Gabry, Lamyaa A. Thurman, Douglas R. Poinsatte, Philip E. Heidmann, James D. TI Detailed Velocity and Turbulence Measurements in an Inclined Large-Scale Film Cooling Array SO JOURNAL OF TURBOMACHINERY-TRANSACTIONS OF THE ASME LA English DT Article DE film cooling; turbulence measurements; jet in crossflow; high blowing ID DENSITY RATIO; INJECTION; HOLES; JETS; FLOW; ROW AB A large-scale model of an inclined row of film cooling holes is used to obtain detailed surface and flow field measurements that will enable future computational fluid dynamics code development and validation. The model consists of three holes of 1.9-cm diameter that are spaced three hole diameters apart and inclined 30 deg from the surface. The length to diameter ratio of the coolant holes is about 18. Measurements include film effectiveness using IR thermography and near wall thermocouples, heat transfer using liquid crystal thermography, flow field temperatures using a thermocouple, and velocity and turbulence quantities using hotwire anemometry. Results are obtained for blowing ratios of up to 2 in order to capture severe conditions in which the jet is lifted. For purposes of comparison with prior art, measurements of the velocity and turbulence field along the jet centerline are made and compare favorably with two data sets in the open literature thereby verifying the test apparatus and methodology are able to replicate existing data sets. In addition, a computational fluid dynamics model using a two-equation turbulence model is developed, and the results for velocity, turbulent kinetic energy and turbulent dissipation rate are compared with experimentally derived quantities. C1 [El-Gabry, Lamyaa A.] Amer Univ Cairo, Dept Mech Engn, New Cairo 11835, Egypt. [Thurman, Douglas R.] Glenn Res Ctr, US Army Res Lab, Cleveland, OH 44135 USA. [Poinsatte, Philip E.; Heidmann, James D.] NASA, Glenn Res Ctr, Turbomachinery & Heat Transfer Branch, Cleveland, OH 44135 USA. RP El-Gabry, LA (reprint author), Amer Univ Cairo, Dept Mech Engn, New Cairo 11835, Egypt. EM lelgabry@aucegypt.edu FU NASA FX The research was carried out as part of the Subsonic Fixed Wing Project under NASA's Fundamental Aeronautics Program whose support is acknowledged. The authors would like to acknowledge the support of the NASA Glenn Faculty Fellowship program and the input of Dr. Khairul Zaman of NASA Glenn Research center on hotwire measurements. NR 19 TC 1 Z9 1 U1 0 U2 4 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 0889-504X EI 1528-8900 J9 J TURBOMACH JI J. Turbomach.-Trans. ASME PD NOV PY 2013 VL 135 IS 6 AR 061013 DI 10.1115/1.4023347 PG 11 WC Engineering, Mechanical SC Engineering GA 239KS UT WOS:000326023100013 ER PT J AU Feeley, KJ Hurtado, J Saatchi, S Silman, MR Clark, DB AF Feeley, Kenneth J. Hurtado, Johanna Saatchi, Sassan Silman, Miles R. Clark, David B. TI Compositional shifts in Costa Rican forests due to climate-driven species migrations SO GLOBAL CHANGE BIOLOGY LA English DT Article DE climate change; cloud forest; extinction; forest inventory plots; global warming; species migrations; thermal distributions ID ELEVATIONAL RANGE SHIFTS; MONTANE CLOUD FORESTS; FUTURE DISTRIBUTIONS; TROPICAL MOUNTAIN; EXTINCTION RISK; BIODIVERSITY; IMPACTS; PRECIPITATION; DEFORESTATION; VULNERABILITY AB Species are predicted to shift their distributions upslope or poleward in response to global warming. This prediction is supported by a growing number of studies documenting species migrations in temperate systems but remains poorly tested for tropical species, and especially for tropical plant species. We analyzed changes in tree species composition in a network of 10 annually censused 1-ha plots spanning an altitudinal gradient of 70-2800m elevation in Costa Rica. Specifically, we combined plot data with herbarium records (accessed through GBIF) to test if the plots' community temperature scores (CTS, average thermal mean of constituent species weighted by basal area) have increased over the past decade as is predicted by climate-driven species migrations. In addition, we quantified the contributions of stem growth, recruitment, and mortality to the observed patterns. Supporting our a priori hypothesis of upward species migrations, we found that there have been consistent directional shifts in the composition of the plots, such that the relative abundance of lowland species, and hence CTS, increased in 90% of plots. The rate of the observed compositional shifts corresponds to a mean thermal migration rate (TMR) of 0.0065 degrees Cyr(-1) (95% CI=0.0005-0.0132 degrees Cyr(-1)). While the overall TMR is slower than predicted based on concurrent regional warming of 0.0167 degrees Cyr(-1), migrations were on pace with warming in 4 of the 10 plots. The observed shifts in composition were driven primarily by mortality events (i.e., the disproportionate death of highland vs. lowland species), suggesting that individuals of many tropical tree species will not be able to tolerate future warming and thus their persistence in the face of climate change will depend on successful migrations. Unfortunately, in Costa Rica and elsewhere, land area inevitably decreases at higher elevations; hence, even species that are able to migrate successfully will face heightened risks of extinction. C1 [Feeley, Kenneth J.] Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA. [Feeley, Kenneth J.] Fairchild Trop Bot Garden, Coral Gables, FL 33156 USA. [Hurtado, Johanna] Org Trop Studies, La Selva Biol Stn, Puerto Viejo de Sarapiqui, Costa Rica. [Saatchi, Sassan] CALTECH, Jet Prop Lab, Los Angeles, CA 91011 USA. [Saatchi, Sassan] Univ Calif Los Angeles, Inst Environm, Los Angeles, CA 90095 USA. [Silman, Miles R.] Wake Forest Univ, Dept Biol, Winston Salem, NC 27109 USA. [Silman, Miles R.] Wake Forest Univ, Ctr Energy Environm & Sustainabil, Biodivers & Ecosyst Serv Grp, Winston Salem, NC 27109 USA. [Clark, David B.] Univ Missouri, Dept Biol, St Louis, MO 63121 USA. RP Feeley, KJ (reprint author), Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA. EM kjfeeley@gmail.com RI Feeley, Kenneth/A-7631-2009 FU Kushlan Tropical Science Institute at the Fairchild Tropical Botanic Gardens; NASA [TE08-0037, TE11-0100]; US National Science Foundation [DEB-1257655, DEB-1258112]; Tropical Ecology Assessment and Monitoring (TEAM) Network FX The census data used in this publication were provided by the Tropical Ecology Assessment and Monitoring (TEAM) Network, a collaboration between Conservation International, the Missouri Botanical Garden, the Smithsonian Institution, and the Wildlife Conservation Society, and partially funded by these institutions, the Gordon and Betty Moore Foundation, and other donors. Additional financial support for this study was provided by the Kushlan Tropical Science Institute at the Fairchild Tropical Botanic Gardens, NASA grants TE08-0037 and TE11-0100 to S. Saatchi, and the US National Science Foundation grants DEB-1257655 to K.J. Feeley and DEB-1258112 to M.R. Silman. Logistic support for field work in Braulio Carrillo National Park and La Selva was provided by the staff of the Organization for Tropical Studies' La Biological Station. We thank the Ministerio de Ambiente y Energia for permission to conduct research in Costa Rica. We also thank the Global Biodiversity Information Facility, and all contributing herbaria for making their data publicly available and facilitating studies of ecology and biogeography. This is contribution #252 of the Program in Tropical Biology at Florida International University. NR 48 TC 25 Z9 26 U1 9 U2 149 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1354-1013 EI 1365-2486 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD NOV PY 2013 VL 19 IS 11 BP 3472 EP 3480 DI 10.1111/gcb.12300 PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 233KL UT WOS:000325567100020 PM 23794172 ER PT J AU Turner, DP Jacobson, AR Ritts, WD Wang, WL Nemani, R AF Turner, David P. Jacobson, Andrew R. Ritts, William D. Wang, Weile L. Nemani, Ramakrishna TI A large proportion of North American net ecosystem production is offset by emissions from harvested products, river/stream evasion, and biomass burning SO GLOBAL CHANGE BIOLOGY LA English DT Article DE atmospheric inversion model; biomass burning; carbon flux; net ecosystem exchange; net ecosystem production; river evasion ID CONTERMINOUS UNITED-STATES; GROSS PRIMARY PRODUCTION; CARBON-DIOXIDE EXCHANGE; ATMOSPHERIC CO2; INTERANNUAL VARIABILITY; TERRESTRIAL GROSS; HIGH-RESOLUTION; DECADAL TRENDS; FLUX TOWER; STAND AGE AB Diagnostic carbon cycle models produce estimates of net ecosystem production (NEP, the balance of net primary production and heterotrophic respiration) by integrating information from (i) satellite-based observations of land surface vegetation characteristics; (ii) distributed meteorological data; and (iii) eddy covariance flux tower observations of net ecosystem exchange (NEE) (used in model parameterization). However, a full bottom-up accounting of NEE (the vertical carbon flux) that is suitable for integration with atmosphere-based inversion modeling also includes emissions from decomposition/respiration of harvested forest and agricultural products, CO2 evasion from streams and rivers, and biomass burning. Here, we produce a daily time step NEE for North America for the year 2004 that includes NEP as well as the additional emissions. This NEE product was run in the forward mode through the CarbonTracker inversion setup to evaluate its consistency with CO2 concentration observations. The year 2004 was climatologically favorable for NEP over North America and the continental total was estimated at 1730 +/- 370TgCyr(-1) (a carbon sink). Harvested product emissions (316 +/- 80TgCyr(-1)), river/stream evasion (158 +/- 50TgCyr(-1)), and fire emissions (142 +/- 45TgCyr(-1)) counteracted a large proportion (35%) of the NEP sink. Geographic areas with strong carbon sinks included Midwest US croplands, and forested regions of the Northeast, Southeast, and Pacific Northwest. The forward mode run with CarbonTracker produced good agreement between observed and simulated wintertime CO2 concentrations aggregated over eight measurement sites around North America, but overestimates of summertime concentrations that suggested an underestimation of summertime carbon uptake. As terrestrial NEP is the dominant offset to fossil fuel emission over North America, a good understanding of its spatial and temporal variation - as well as the fate of the carbon it sequesters is needed for a comprehensive view of the carbon cycle. C1 [Turner, David P.; Ritts, William D.] Oregon State Univ, Dept Forest Ecosyst & Soc, Corvallis, OR 97331 USA. [Jacobson, Andrew R.] Univ Colorado, Boulder, CO 80305 USA. [Jacobson, Andrew R.] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA. [Wang, Weile L.; Nemani, Ramakrishna] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Turner, DP (reprint author), Oregon State Univ, Dept Forest Ecosyst & Soc, Corvallis, OR 97331 USA. EM david.turner@oregonstate.edu FU NASA [NNX09AL51G] FX This research was supported by the NASA Terrestrial Ecology Program (NNX09AL51G). Data from the AmeriFlux and FluxNet networks, the Biogeochemical Dynamics Distributed Active Archive Center, and the Land Processes Distributed Active Archive Center were essential for its completion. M. Zhao (University of Maryland) generously provided the filled MODIS Collection 5 FPAR product. We thank Arlyn Andrews and Ed Dlugokencky (NOAA Earth System Research Laboratory) and Doug Worthy (Environment Canada) for coordination of the CO2 measurement networks. NASA provided use of the NEX computing facility at the NASA Ames Laboratory. NR 87 TC 6 Z9 6 U1 3 U2 64 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1354-1013 EI 1365-2486 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD NOV PY 2013 VL 19 IS 11 BP 3516 EP 3528 DI 10.1111/gcb.12313 PG 13 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 233KL UT WOS:000325567100024 PM 23824790 ER PT J AU Jahanshahi, MR Jazizadeh, F Masri, SF Becerik-Gerber, B AF Jahanshahi, Mohammad R. Jazizadeh, Farrokh Masri, Sami F. Becerik-Gerber, Burcin TI Unsupervised Approach for Autonomous Pavement-Defect Detection and Quantification Using an Inexpensive Depth Sensor SO JOURNAL OF COMPUTING IN CIVIL ENGINEERING LA English DT Article DE Pavement management; Defects; Probe instruments; Pavement-condition assessment; Defect detection; Defect quantification; Depth sensor ID CRACK DETECTION; DISTRESS DETECTION; CLASSIFICATION; RECOGNITION; SYSTEM AB Current pavement condition-assessment procedures are extensively time consuming and laborious; in addition, these approaches pose safety threats to the personnel involved in the process. In this study, a RGB-D sensor is used to detect and quantify defects in pavements. This sensor system consists of a RGB color image, and an infrared projector and a camera that act as a depth sensor. An approach, which does not need any training, is proposed to interpret the data sensed by this inexpensive sensor. This system has the potential to be used for autonomous cost-effective assessment of road-surface conditions. Various road conditions including patching, cracks, and potholes are autonomously detected and, most importantly, quantified, using the proposed approach. Several field experiments have been carried out to evaluate the capabilities, as well as the limitations of the proposed system. The global positioning system information is incorporated with the proposed system to localize the detected defects. This approach has the potential to be deployed as a supplementary sensor system in pavement surface-assessment vehicles and reduce the operation cost. (C) 2013 American Society of Civil Engineers. C1 [Jahanshahi, Mohammad R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Jazizadeh, Farrokh; Masri, Sami F.; Becerik-Gerber, Burcin] Univ So Calif, Viterbi Sch Engn, Sonny Astani Dept Civil & Environm Engn, Los Angeles, CA 90089 USA. RP Jahanshahi, MR (reprint author), CALTECH, Jet Prop Lab, M-S 198-235,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mohammad@caltech.edu; jazizade@usc.edu; masri@usc.edu; becerik@usc.edu RI Becerik-Gerber, Burcin/D-6897-2013; Jazizadeh, Farrokh/P-8822-2014 OI Becerik-Gerber, Burcin/0000-0001-8648-0989; Jazizadeh, Farrokh/0000-0002-0690-1307 FU National Science Foundation FX This study was supported in part by a grant from the National Science Foundation. NR 27 TC 9 Z9 9 U1 0 U2 20 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0887-3801 EI 1943-5487 J9 J COMPUT CIVIL ENG JI J. Comput. Civil. Eng. PD NOV 1 PY 2013 VL 27 IS 6 BP 743 EP 754 DI 10.1061/(ASCE)CP.1943-5487.0000245 PG 12 WC Computer Science, Interdisciplinary Applications; Engineering, Civil SC Computer Science; Engineering GA 234LR UT WOS:000325646200016 ER PT J AU Yang, F Noebe, RD Mills, MJ AF Yang, F. Noebe, R. D. Mills, M. J. TI Precipitates in a near-equiatomic (Ni plus Pt)-rich TiNiPt alloy SO SCRIPTA MATERIALIA LA English DT Article DE Shape memory alloys; Precipitation; Crystal structure; High-angle annular dark field ID TOTAL-ENERGY CALCULATIONS; SHAPE-MEMORY ALLOYS; WAVE BASIS-SET; ULTRASOFT PSEUDOPOTENTIALS; TRANSITION; SIMULATION; STEM AB Age-treating a 49.5Ti-29.5Ni-21Pt (at.%) high-temperature shape memory alloy introduces precipitates. At 500 degrees C, the P-L phase is stable up to 1000 h. At 600 degrees C, a transformation from the PL phase to Ti-2(Ni,Pt)(3) was observed. The Ti2(Ni,Pt)3 phase was shown to be the final stable precipitate phase in this alloy. Employing high-resolution scanning transmission electron microscopy, a model for the unit cell of the Ti-2(Ni,Pt)(3) phase was proposed. (C) 2013 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved. C1 [Yang, F.; Mills, M. J.] Ohio State Univ, Columbus, OH 43210 USA. [Noebe, R. D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Yang, F (reprint author), Ohio State Univ, 2041 Coll Rd, Columbus, OH 43210 USA. EM yang.1052@osu.edu RI Mills, Michael/I-6413-2013 FU US Department of Energy, Office of Basic Energy Sciences [DE-SC0001258]; NASA Fundamental Aeronautics Program, Aeronautical Sciences Project FX This work was supported by the US Department of Energy, Office of Basic Energy Sciences under Grant #DE-SC0001258 (for F.Y. and M.J.M.). R.D.N. acknowledges funding from the NASA Fundamental Aeronautics Program, Aeronautical Sciences Project, Dale Hopkins, API. NR 18 TC 1 Z9 1 U1 0 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-6462 J9 SCRIPTA MATER JI Scr. Mater. PD NOV PY 2013 VL 69 IS 10 BP 713 EP 715 DI 10.1016/j.scriptamat.2013.08.002 PG 3 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA 234SY UT WOS:000325665800003 ER PT J AU Tayon, WA Domack, MS Hoffman, EK Hales, SJ AF Tayon, Wesley A. Domack, Marcia S. Hoffman, Eric K. Hales, Stephen J. TI Texture Evolution within the Thermomechanically Affected Zone of an Al-Li Alloy 2195 Friction Stir Weld SO METALLURGICAL AND MATERIALS TRANSACTIONS A-PHYSICAL METALLURGY AND MATERIALS SCIENCE LA English DT Article ID GRAIN-STRUCTURE; MICROSTRUCTURAL EVOLUTION; ALUMINUM-ALLOY; MATERIAL FLOW AB Friction stir welding (FSW) of Al-Li alloy 2195 plate produces strong texture gradients. The microstructural characteristics evolve from the base plate, through the thermomechanically affected zone (TMAZ), to the weld nugget interface. In the current study, electron backscattered diffraction (EBSD) analyses were employed to quantify the spatial distribution of texture gradients associated with the evolution of texture within the TMAZ. The strong texture of the base plate enabled the texture evolution to be characterized as a function of location. Systematic partitioning of EBSD data relative to the degree of lattice rotation at each point accurately captured the crystallographic transitions across the advancing side TMAZ. Over a large section of this region, the texture evolves as a result of continuous rigid body rotations. The rigid body rotations were correlated with the complex material flow patterns commonly associated with the FSW process and prior observations of shear-related textures. Finally, a correlation between texture and fracture in a subscale tensile specimen is observed, where failure occurs within a visible band of low-Taylor factor grains. C1 [Tayon, Wesley A.; Domack, Marcia S.; Hoffman, Eric K.; Hales, Stephen J.] NASA, Adv Mat & Proc Branch, Langley Res Ctr, Hampton, VA 23681 USA. RP Tayon, WA (reprint author), NASA, Adv Mat & Proc Branch, Langley Res Ctr, Hampton, VA 23681 USA. EM wesley.a.tayon@nasa.gov NR 27 TC 3 Z9 3 U1 11 U2 48 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1073-5623 J9 METALL MATER TRANS A JI Metall. Mater. Trans. A-Phys. Metall. Mater. Sci. PD NOV PY 2013 VL 44A IS 11 BP 4906 EP 4913 DI 10.1007/s11661-013-1802-z PG 8 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 223QM UT WOS:000324822100008 ER PT J AU Brice, CA Hofmeister, WH AF Brice, Craig A. Hofmeister, William H. TI Determination of Bulk Residual Stresses in Electron Beam Additive-Manufactured Aluminum SO METALLURGICAL AND MATERIALS TRANSACTIONS A-PHYSICAL METALLURGY AND MATERIALS SCIENCE LA English DT Article ID FREEFORM FABRICATION; DEPOSITION PATTERNS; NEUTRON-DIFFRACTION; THERMAL-STRESSES; PREDICTION; PLATE; PARTS AB Additive-manufactured aluminum alloy deposits were analyzed using neutron diffraction to characterize the effect of intermediate stress relief anneal heat treatment on bulk residual stresses in the final part. Based on measured interplanar spacing, stresses were calculated at various locations along a single bead, stacked wall deposit. A comparison between an uninterrupted deposited wall and an interrupted, stress-relieved, and annealed deposited wall showed a measureable reduction in residual stress magnitude at the interface with a corresponding shift in stress character into the deposit. This shift changes the interface stresses from purely compressive to partially tensile. The residual stress profile varied along the length of the deposit, and the heat-treatment procedure reduced the overall magnitude of the stress at the interface by 10 through 25 MPa. These results are interpreted in terms of thermal gradients inherent to the process and compared with prior residual stress-characterization studies in additive-manufactured metallic structures. C1 [Brice, Craig A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Hofmeister, William H.] Univ Tennessee, Inst Space, Dept Mat Sci & Engn, Tullahoma, TN 37388 USA. RP Brice, CA (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM craig.a.brice@nasa.gov OI Hofmeister, William/0000-0002-4145-7061 FU U.S. Department of Energy, Office of Basic Energy Sciences FX This research performed at Oak Ridge National Laboratory's Spallation Neutron Source was sponsored by the U.S. Department of Energy, Office of Basic Energy Sciences. The authors would like to thank Dr. Ke An and Dr. Harley Skorpenske for their technical assistance in conducting the neutron diffraction experiments. The authors would also like to thank Mr. Richard Martin and Mr. Harold Claytor of NASA Langley Research Center for their assistance with the deposition trials and metallographic analysis. NR 21 TC 7 Z9 7 U1 8 U2 48 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1073-5623 J9 METALL MATER TRANS A JI Metall. Mater. Trans. A-Phys. Metall. Mater. Sci. PD NOV PY 2013 VL 44A IS 11 BP 5147 EP 5153 DI 10.1007/s11661-013-1847-z PG 7 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 223QM UT WOS:000324822100029 ER PT J AU Wang, L Eldridge, JI Guo, SM AF Wang, Li Eldridge, Jeffrey I. Guo, S. M. TI Thermal radiation properties of plasma-sprayed Gd2Zr2O7 thermal barrier coatings SO SCRIPTA MATERIALIA LA English DT Article DE Thermal barrier coating; Plasma spraying; Gd2Zr2O7; Optical absorption; Optical reflectivity ID ABSORPTION-COEFFICIENTS; TAILORED MICROSTRUCTURE; TURBINE APPLICATIONS; EB-PVD; CONDUCTIVITY; REFLECTANCE; ZIRCONIA; REFLECTIVITY; TEMPERATURES; SCATTERING AB The reflectance and transmittance spectra of plasma-sprayed Gd2Zr2O7 coatings were measured and the absorption and scattering coefficient as a function of wavelength were extracted using the four-flux model. Results showed that Gd2Zr2O7 is a high scattering, low absorption material at the wavelength <6 mu m, and the scattering coefficient decreases with the increase of wavelength. Compared with yttria-stabilized zirconia, Gd2Zr2O7 shows higher reflectance and lower transmittance in the wavelength range of 0.8-2.7 mu m, which is desirable in thermal barrier coating applications. (C) 2013 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved. C1 [Wang, Li; Guo, S. M.] Louisiana State Univ, Dept Mech & Ind Engn, Baton Rouge, LA 70803 USA. [Eldridge, Jeffrey I.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Guo, SM (reprint author), Louisiana State Univ, Dept Mech & Ind Engn, Baton Rouge, LA 70803 USA. EM sguo2@lsu.edu RI Wang, Li/E-9963-2014 OI Wang, Li/0000-0002-1876-3079 FU NASA [NNX09AP72A] FX This research is sponsored by NASA under Cooperative Agreement Number NNX09AP72A. NR 32 TC 14 Z9 15 U1 1 U2 38 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-6462 J9 SCRIPTA MATER JI Scr. Mater. PD NOV PY 2013 VL 69 IS 9 BP 674 EP 677 DI 10.1016/j.scriptamat.2013.07.026 PG 4 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA 228NW UT WOS:000325194500008 ER PT J AU Lacelle, D Davila, AF Fisher, D Pollard, WH DeWitt, R Heldmann, J Marinova, MM Mckay, CP AF Lacelle, Denis Davila, Alfonso F. Fisher, David Pollard, Wayne H. DeWitt, Regina Heldmann, Jennifer Marinova, Margarita M. Mckay, Christopher P. TI Excess ground ice of condensation-diffusion origin in University Valley, Dry Valleys of Antarctica: Evidence from isotope geochemistry and numerical modeling SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID REGENERATIVE-DOSE PROTOCOL; NORTHERN VICTORIA LAND; WATER-VAPOR ADSORPTION; MIOCENE GLACIER ICE; BEACON VALLEY; NORTHWEST-TERRITORIES; EAST ANTARCTICA; TAYLOR VALLEY; NEAR-SURFACE; PERMAFROST AB This study investigates the origin and age of ground ice in the uppermost 1 m of permafrost in University Valley, one of the upper valleys in the McMurdo Dry Valleys of Antarctica. In contrast to other regions in the MDV, mean daily air and soil temperatures at the coring sites are always below 0 degrees C, which allows for unique cryogenic processes to occur. In the two cores that were analyzed, excess ground ice was measured throughout, ranging between 23% and 85%. Isotope geochemical trends in the ice-rich permafrost indicate that the ground in Core 5 ( 65 cm long) and the uppermost 52 cm of Core 7 originated from condensation-diffusion of water vapor; whereas the ground ice between 57-90 cm in Core 7 originated from freezing of liquid water. Using numerical modeling, we show that the excess ground ice of condensation-diffusion origin formed by the long-term thermal contraction-expansion of the cryotic sediments, which allowed for the ice content to exceed pore-filling capacity. Absolute age estimates of the sandy-loam sediments based on Optically Stimulated Luminescence dating indicate that soils have been accreting at the site for at least the last 170 +/- 36 ka years, and this places an upper limit to the age of the ground ice. Absolute soil ages allowed us to link the change in ground ice origin in Core 7, which took place around 152 +/- 12 ka years, with shifts in climate conditions since marine isotope stage 5e interglacial period. Our findings offer a new process of ground ice emplacement in sediments in cold-dry environments and allow an alternative explanation regarding the enigmatic origin of excess ground ice identified by Mars Odyssey and Phoenix in the northern martian plain, which is that overfilled pore ice can form by vapor deposition and repeated thermal cycling without the presence of melt water. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Lacelle, Denis] Univ Ottawa, Dept Geog, Ottawa, ON K1N 6N5, Canada. [Davila, Alfonso F.] Carl Sagan Ctr Study Life Universe, SETI Inst, Mountain View, CA USA. [Fisher, David] Univ Ottawa, Dept Earth Sci, Ottawa, ON K1N 6N5, Canada. [Pollard, Wayne H.] McGill Univ, Dept Geog, Montreal, PQ, Canada. [DeWitt, Regina] E Carolina Univ, Dept Phys, Greenville, NC USA. [Heldmann, Jennifer; Marinova, Margarita M.; Mckay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [DeWitt, Regina] Oklahoma State Univ, Dept Phys, Stillwater, OK 74078 USA. RP Lacelle, D (reprint author), Univ Ottawa, Dept Geog, Ottawa, ON K1N 6N5, Canada. EM dlacelle@uottawa.ca RI Davila, Alfonso/A-2198-2013; OI Davila, Alfonso/0000-0002-0977-9909; DeWitt, Regina/0000-0003-2876-5489; Lacelle, Denis/0000-0002-6691-8717 FU NASA's ASTEP program FX This work was supported by NASA's ASTEP program and operated by the NSF Office of Polar Programs. We thank the two anonymous reviewers and the associate editor for their constructive comments on the manuscript. NR 74 TC 14 Z9 14 U1 1 U2 20 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD NOV 1 PY 2013 VL 120 BP 280 EP 297 DI 10.1016/j.gca.2013.06.032 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 223MH UT WOS:000324809000018 ER PT J AU Muller, IA Brunner, B Breuer, C Coleman, M Bach, W AF Mueller, Inigo A. Brunner, Benjamin Breuer, Christian Coleman, Max Bach, Wolfgang TI The oxygen isotope equilibrium fractionation between sulfite species and water SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID DISSIMILATORY SULFATE REDUCTION; SULFUR-DIOXIDE; ELEMENTAL SULFUR; BISULFITE ION; PHASE OXIDATION; DEEP BIOSPHERE; ACID-RAIN; EXCHANGE; BACTERIAL; DISPROPORTIONATION AB Sulfite is an important sulfoxy intermediate in oxidative and reductive sulfur cycling in the marine and terrestrial environment. Different aqueous sulfite species exist, such as dissolved sulfur dioxide (SO2), bisulfite (HSO3), pyrosulfite (S2O52) and sulfite sensu stricto (SO32-), whereas their relative abundance in solution depends on the concentration and the pH. Conversion of one species into another is rapid and involves in many cases incorporation of oxygen from, or release of oxygen to, water (e.g. SO2 + H2O <-> HSO3- + H+), resulting in rapid oxygen isotope exchange between sulfite species and water. Consequently, the oxygen isotope composition of sulfite is strongly influenced by the oxygen isotope composition of water. Since sulfate does not exchange oxygen isotopes with water under most earth surface conditions, it can preserve the sulfite oxygen isotope signature that it inherits via oxidative and reductive sulfur cycling. Therefore, interpretation of delta O-18(SO4)2- values strongly hinges on the oxygen isotope equilibrium fractionation between sulfite and water which is poorly constrained. This is in large part due to technical difficulties in extraction of sulfite from solution for oxygen isotope analysis. To overcome these challenges, anoxic isotope equilibration experiments were performed with dissolved sodium sulfite in solutions with distinct oxygen isotope signatures. Sulfite was precipitated using two different agents, barium chloride and silver nitrate. The experiments were performed at 22 degrees C and varying pH of 1.5, 6.3, 6.6, and 9.7 to investigate how changes in sulfite speciation affect the oxygen isotope equilibrium fractionation between sulfite and water. From the experiments at pH 1.5 where SO2 is the dominant sulfite species, a rough estimate of 37.0 parts per thousand was determined for the oxygen isotope equilibrium fractionation factor between aqueous SO2 and water (epsilon(EQ)(SO2) <-> H2O). The oxygen isotope equilibrium fractionation between the aqueous phases is much larger than the known oxygen isotope equilibrium fractionation between gaseous SO2 and water vapor, probably because of a stronger association with water molecules. At pH values of 6.3- 9.7 a more firm estimate for the oxygen isotope equilibrium fractionation between HSO3, SO32- and water (epsilon(-EQ)(SO32) <-> H2O) of 15.2 +/- 0.7 parts per thousand was obtained. Our results provide new insights into the oxygen isotope fractionation during reductive and oxidative sulfur cycling. They demonstrate that isotope exchange between sulfite and water during dissimilatory sulfate reduction (DSR) alone is too small to be responsible for the apparent oxygen isotope equilibrium fractionation between sulfate and water mediated by DSR. Our estimates also provide a basis for tracing and quantifying the transformation of sulfoxy intermediates during the oxidation of reduced sulfur compounds to sulfate. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Mueller, Inigo A.; Brunner, Benjamin] Max Planck Inst Marine Mikrobiol, Biogeochem Dept, D-28359 Bremen, Germany. [Mueller, Inigo A.; Breuer, Christian; Bach, Wolfgang] Univ Bremen, MARUM Ctr Marine Environm Sci, D-28359 Bremen, Germany. [Brunner, Benjamin] Aarhus Univ, Dept Biosci, Ctr Geomicrobiol, DK-8000 Aarhus C, Denmark. [Breuer, Christian; Bach, Wolfgang] Univ Bremen, Dept Geosci, D-28359 Bremen, Germany. [Coleman, Max] CALTECH, Jet Prop Lab, NASA, Planetary Surface Instruments Grp, Pasadena, CA 91109 USA. RP Muller, IA (reprint author), Max Planck Inst Marine Mikrobiol, Biogeochem Dept, Celsiusstr 1, D-28359 Bremen, Germany. EM imueller@mpi-bremen.de RI Bach, Wolfgang/D-3713-2017 OI Bach, Wolfgang/0000-0002-3099-7142 FU MARUM (Center for Marine Environmental Sciences); Max Planck Society; National Aeronautics and Space Administration (NASA); NASA Astrobiology Institute (NAI-WARC) FX The authors thank T.G. Ferdelman and M.M.M. Kuypers for supporting this study, T. Max for crucial help with the mass spectrometer and assistance in the laboratory. We thank S.M. Bernasconi for the isotopic analysis and support as well as A.V. Turchyn for inspiring discussions and valuable advice. This project would not have been possible without the financial support provided by MARUM (Center for Marine Environmental Sciences) and the Max Planck Society. We would like to acknowledge K.W. Mandernack, B.A. Wing, the anonymous reviewer and the associate editor E.A. Schauble for their detailed, insightful comments and suggestions that greatly helped to improve our manuscript. The contribution of M.C. was carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA), with support from the NASA Astrobiology Institute (NAI-WARC). NR 72 TC 8 Z9 8 U1 3 U2 54 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD NOV 1 PY 2013 VL 120 BP 562 EP 581 DI 10.1016/j.gca.2013.06.037 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 223MH UT WOS:000324809000033 ER PT J AU Stebner, AP Vogel, SC Noebe, RD Sisneros, TA Clausen, B Brown, DW Garg, A Brinson, LC AF Stebner, A. P. Vogel, S. C. Noebe, R. D. Sisneros, T. A. Clausen, B. Brown, D. W. Garg, A. Brinson, L. C. TI Micromechanical quantification of elastic, twinning, and slip strain partitioning exhibited by polycrystalline, monoclinic nickel-titanium during large uniaxial deformations measured via in-situ neutron diffraction SO JOURNAL OF THE MECHANICS AND PHYSICS OF SOLIDS LA English DT Article DE Shape memory alloy; Neutron diffraction; Twinning; Monoclinic; Plasticity ID SHAPE-MEMORY ALLOYS; CRYSTALLITE SIZE DISTRIBUTION; PERCENT-NI-ALLOY; ELECTRON-MICROSCOPY; CONSTITUTIVE MODEL; MARTENSITIC-TRANSFORMATION; TEXTURE ANALYSIS; SINGLE-CRYSTALS; B19 MARTENSITE; THIN-FILMS AB We draw upon existing knowledge of twinning and slip mechanics to develop a diffraction analysis model that allows for empirical quantification of individual deformation mechanisms to the macroscopic behaviors of low symmetry and phase transforming crystalline solids. These methods are applied in studying elasticity, accommodation twinning, deformation twinning, and slip through neutron diffraction data of tensile and compressive deformations of monoclinic NiTi to similar to 18% true strain. A deeper understanding of tension-compression asymmetry in NiTi is gained by connecting crystallographic calculations of polycrystalline twinning strains with in situ diffraction measurements. Our analyses culminate in empirical, micromechanical quantification of individual elastic, accommodation twinning, deformation twinning, and slip contributions to the total macroscopic stress-strain response of a monoclinic material subjected to large deformations. From these results, we find that 20-40% of the total plastic response at high strains is due to deformation twinning and 60-80% due to slip. 2013 Elsevier Ltd. All rights reserved. C1 [Stebner, A. P.; Brinson, L. C.] Northwestern Univ, Dept Mech Engn, Evanston, IL 60208 USA. [Vogel, S. C.; Sisneros, T. A.; Clausen, B.; Brown, D. W.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Noebe, R. D.; Garg, A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Brinson, L. C.] Northwestern Univ, Dept Mat Sci & Engn, Evanston, IL 60208 USA. RP Stebner, AP (reprint author), Colorado Sch Mines, Dept Mech Engn, Golden, CO 80401 USA. EM astebner@mines.edu RI Brinson, L. Catherine/B-6678-2009; Stebner, Aaron/A-7685-2015; Clausen, Bjorn/B-3618-2015; Brinson, L Catherine/B-1315-2013; OI Clausen, Bjorn/0000-0003-3906-846X; Brinson, L Catherine/0000-0003-2551-1563; Vogel, Sven C./0000-0003-2049-0361 FU Office of Basic Energy Sciences of the Department of Energy under DOE Contract [DE-AC52-06NA25396]; Toshio Mura Endowment, Predictive Science and Engineering Design Cluster at Northwestern (PSED); Initiative for Sustainability and Energy at Northwestern (ISEN); Army Research Office [W911 NF-12-1-0013/P00002]; NASA Fundamental Aeronautics Program; Aeronautical Sciences Project FX This work has benefited from the use of the Lujan Neutron Scattering Center at LANSCE, which is funded by the Office of Basic Energy Sciences of the Department of Energy under DOE Contract DE-AC52-06NA25396. A.S. acknowledges funding through fellowships from the Toshio Mura Endowment, Predictive Science and Engineering Design Cluster at Northwestern (PSED), Initiative for Sustainability and Energy at Northwestern (ISEN). A.S. and C.B. acknowledge the support of the Army Research Office, Grant # W911 NF-12-1-0013/P00002, and A.G. and R.D.N. acknowledge support from the NASA Fundamental Aeronautics Program, Aeronautical Sciences Project. G.B. Olson is thanked for pre-submission critique of this work. NR 81 TC 29 Z9 29 U1 4 U2 54 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-5096 EI 1873-4782 J9 J MECH PHYS SOLIDS JI J. Mech. Phys. Solids PD NOV PY 2013 VL 61 IS 11 BP 2302 EP 2330 DI 10.1016/j.jmps.2013.05.008 PG 29 WC Materials Science, Multidisciplinary; Mechanics; Physics, Condensed Matter SC Materials Science; Mechanics; Physics GA 223EK UT WOS:000324787300012 ER PT J AU Charles, JB Paloski, WH LeBlanc, A Watson, D AF Charles, John B. Paloski, William H. LeBlanc, Adrian Watson, David TI 18th IAA humans in space meeting, Houston SO ACTA ASTRONAUTICA LA English DT Editorial Material C1 [Charles, John B.] NASA, Human Res Program Off, Johnson Space Ctr, Houston, TX USA. [Paloski, William H.] Univ Houston, Dept Hlth & Human Performance, Houston, TX 77204 USA. [LeBlanc, Adrian] Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA. [Watson, David] Natl Space Biomed Res Inst, Houston, TX USA. RP Paloski, WH (reprint author), Univ Houston, Dept Hlth & Human Performance, Houston, TX 77204 USA. EM whpaloski@uh.edu NR 0 TC 0 Z9 0 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD NOV PY 2013 VL 92 IS 1 SI SI BP 1 EP 2 DI 10.1016/j.actaastro.2013.04.017 PG 2 WC Engineering, Aerospace SC Engineering GA 212VX UT WOS:000324012000001 ER PT J AU Arzeno, NM Stenger, MB Bloomberg, JJ Plats, SH AF Arzeno, Natalia M. Stenger, Michael B. Bloomberg, Jacob J. Plats, Steven H. TI Spaceflight-induced cardiovascular changes and recovery during NASA's Functional Task Test SO ACTA ASTRONAUTICA LA English DT Article; Proceedings Paper CT 18th Humans in Space (HIS) Symposium of the International-Academy-of-Astronautics (IAA) CY APR 11-15, 2011 CL Houston, TX SP Int Acad Astronaut DE Microgravity; Autonomic activity; Heart rate variability; Cardiovascular deconditioning ID HEART-RATE-VARIABILITY; SHORT-DURATION SPACEFLIGHT; ARTERIAL-PRESSURE; SPECTRAL-ANALYSIS; SPACE; HUMANS; RESPONSES; ORDER; TILT AB Microgravity-induced physiologic changes could impair a crewmember's performance upon return to a gravity environment. The Functional Task Test aims to correlate these physiologic alterations with changes in performance during mission-critical tasks. In this study, we evaluated spaceflight-induced cardiovascular changes during 11 functional tasks in 7 Shuttle astronauts before spaceflight, on landing day, and 1, 6, and 30 days after landing. Mean heart rate was examined during each task and autonomic activity was approximated by heart rate variability during the Recovery from Fall/Stand Test, a 2-min prone rest followed by a 3-min stand. Heart rate was increased on landing day during all of the tasks, and remained elevated 6 days after landing during 6 of the 11 tasks. Parasympathetic modulation was diminished and sympathovagal balance was increased on landing day. Additionally, during the stand test 6 days after landing, parasympathetic modulation remained suppressed and heart rate remained elevated compared to preflight levels. Heart rate and autonomic activity were not different from preflight levels 30 days after landing. We detected changes in heart rate and autonomic activity during a 3-min stand and a variety of functional tasks, where cardiovascular deconditioning was still evident 6 days after returning from short-duration spaceflight. The delayed recovery times for heart rate and parasympathetic modulation indicate the necessity of assessing functional performance after long-duration spaceflight to ensure crew health and safety. (C) 2012 IAA. Published by Elsevier Ltd. All rights reserved. C1 [Arzeno, Natalia M.; Stenger, Michael B.] Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA. [Bloomberg, Jacob J.; Plats, Steven H.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. RP Stenger, MB (reprint author), Wyle Sci Technol & Engn Grp, 1290 Hercules Dr, Houston, TX 77058 USA. EM natalia.m.arzeno@nasa.gov; michael.b.stenger@nasa.gov; jacob.j.bloomberg@nasa.gov; steven.platts-1@nasa.gov NR 20 TC 2 Z9 2 U1 2 U2 26 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 NOV PY 2013 VL 92 IS 1 SI SI BP 10 EP 14 DI 10.1016/j.actaastro.2012.05.023 PG 5 WC Engineering, Aerospace SC Engineering GA 212VX UT WOS:000324012000003 ER PT J AU Clement, G Wood, SJ AF Clement, Gilles Wood, Scott J. TI Motion perception during tilt and translation after space flight SO ACTA ASTRONAUTICA LA English DT Article; Proceedings Paper CT 18th Humans in Space (HIS) Symposium of the International-Academy-of-Astronautics (IAA) CY APR 11-15, 2011 CL Houston, TX SP Int Acad Astronaut DE Motion perception; Vestibular system; Microgravity-induced physiological effects; Weightlessness ID VERTICAL AXIS ROTATION; PROLONGED WEIGHTLESSNESS; LINEAR ACCELERATION; ROLL; SPACEFLIGHT; FREQUENCY; SICKNESS AB Preliminary results of an ongoing study examining the effects of space flight on astronauts' motion perception induced by independent tilt and translation motions are presented. This experiment used a sled and a variable radius centrifuge that translated the subjects forward-backward or laterally, and simultaneously tilted them in pitch or roll, respectively. Tests were performed on the ground prior to and immediately after landing. The astronauts were asked to report about their perceived motion in response to different combinations of body tilt and translation in darkness. Their ability to manually control their own orientation was also evaluated using a joystick with which they nulled out the perceived tilt while the sled and centrifuge were in motion. Preliminary results confirm that the magnitude of perceived tilt increased during static tilt in roll after space flight. A deterioration in the crewmember to control tilt using non-visual inertial cues was also observed post-flight. However, the use of a tactile prosthesis indicating the direction of down on the subject's trunk improved manual control performance both before and after space flight. (C) 2012 IAA. Published by Elsevier Ltd. All rights reserved. C1 [Clement, Gilles] Int Space Univ, F-67400 Illkirch Graffenstaden, France. [Wood, Scott J.] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA. [Wood, Scott J.] NASA, Neurosci Lab, Johnson Space Ctr, Houston, TX 77058 USA. RP Clement, G (reprint author), Int Space Univ, Parc Innovat,1 Rue Jean Domin Cassini, F-67400 Illkirch Graffenstaden, France. EM clement@isu.isunet.edu NR 15 TC 1 Z9 1 U1 0 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD NOV PY 2013 VL 92 IS 1 SI SI BP 48 EP 52 DI 10.1016/j.actaastro.2012.03.011 PG 5 WC Engineering, Aerospace SC Engineering GA 212VX UT WOS:000324012000008 ER PT J AU Adelstein, BD Kaiser, MK Beutter, BR McCann, RS Anderson, MR AF Adelstein, Bernard D. Kaiser, Mary K. Beutter, Brent R. McCann, Robert S. Anderson, Mark R. TI Display strobing: An effective countermeasure against visual blur from whole-body vibration SO ACTA ASTRONAUTICA LA English DT Article; Proceedings Paper CT 18th Humans in Space (HIS) Symposium of the International-Academy-of-Astronautics (IAA) CY APR 11-15, 2011 CL Houston, TX SP Int Acad Astronaut DE Vibration; Thrust oscillation; Readability; Visual blur; Strobe; Displays; Countermeasure AB Crews and equipment in aerospace vehicles, including spacecraft at launch, can be exposed to significant vibration. Prior to this study, we examined the ability of vibrating observers to read alphanumeric symbology on stationary (i.e., non-vibrating) flight-relevant display formats and noted performance degradation with increasing vibration amplitude and decreasing font size. Here we test the efficacy of a display strobing countermeasure for the reading decrements caused by the same 12-Hz whole-body vibration in the surge (chest-to-spine) direction applied in our prior studies. To produce the strobe countermeasure, we triggered the backlight of a stationary liquid crystal diode (LCD) display panel to flash in synchrony with the 12-Hz vibration of the observer's seat while experimentally varying both the strobe duty cycle and phase angle between the strobe onset and the vibration cycle zero-crossings. Strobing proved an effective countermeasure, restoring reading error rates during 0.7g (6.9 m/s(2) half-amplitude) whole-body vibration to levels indistinguishable from those achieved under the non-strobed (equivalent luminance) non-vibrating baseline condition and improving response times although not fully to the baseline. While we noted differences in the "preferred" phase angle of individual observers, on average, no overall effect of phase angle was detected. Likewise, no effect was seen for the two duty cycles and their respective equivalent luminance levels. Further studies are needed to determine the efficacy of strobing for multi-axis and multi-frequency vibration, and for displays with moving images. Published by Elsevier Ltd. on behalf of IAA. C1 [Adelstein, Bernard D.; Kaiser, Mary K.; Beutter, Brent R.; McCann, Robert S.; Anderson, Mark R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Anderson, Mark R.] Dell Serv Fed Govt, Washington, DC USA. RP Adelstein, BD (reprint author), NASA, Ames Res Ctr, Mail Stop 262-2, Moffett Field, CA 94035 USA. EM Bernard.D.Adelstein@nasa.gov NR 14 TC 1 Z9 1 U1 0 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD NOV PY 2013 VL 92 IS 1 SI SI BP 53 EP 64 DI 10.1016/j.actaastro.2012.07.003 PG 12 WC Engineering, Aerospace SC Engineering GA 212VX UT WOS:000324012000009 ER PT J AU McCabe, NP Androjna, C Hill, E Globus, RK Midura, RJ AF McCabe, N. Patrick Androjna, Caroline Hill, Esther Globus, Ruth K. Midura, Ronald J. TI Simulated microgravity alters the expression of key genes involved in fracture healing SO ACTA ASTRONAUTICA LA English DT Article; Proceedings Paper CT 18th Humans in Space (HIS) Symposium of the International-Academy-of-Astronautics (IAA) CY APR 11-15, 2011 CL Houston, TX SP Int Acad Astronaut DE Simulated microgravity; Fracture healing; Gene expression; Angiogenesis; Chondrogenesis; Osteogenesis ID ENDOTHELIAL GROWTH-FACTOR; ALKALINE-PHOSPHATASE; BONE SIALOPROTEIN; MESSENGER-RNA; DIFFERENTIATION; SPACEFLIGHT; CARTILAGE; REPAIR; CELL; OSTEOBLASTS AB Fracture healing in animal models has been shown to be altered in both ground based analogs of spaceflight and in those exposed to actual spaceflight. The molecular mechanisms behind altered fracture healing as a result of chronic exposure to microgravity remain to be elucidated. This study investigates temporal gene expression of multiple factors involved in secondary fracture healing, specifically those integral to the development of a soft tissue callus and the transition to that of hard tissue. Skeletally mature female rats were subjected to a 4 week period of simulated microgravity and then underwent a closed femoral fracture procedure. Thereafter, they were reintroduced to the microgravity and allowed to heal for a 1 or 2 week period. A synchronous group of weight bearing rats was used as a normal fracture healing control. Utilizing Real-Time quantitative PCR on mRNA from fracture callus tissue, we found significant reductions in the levels of transcripts associated with angiogenesis, chondrogenesis, and osteogenesis. These data suggest an altered fracture healing process in a simulated microgravity environment, and these alterations begin early in the healing process. These findings may provide mechanistic insight towards developing countermeasure protocols to mitigate these adaptations. (C) 2012 IAA. Published by Elsevier Ltd. All rights reserved. C1 [McCabe, N. Patrick; Androjna, Caroline; Midura, Ronald J.] Cleveland Clin, Lerner Res Inst, Dept Biomed Engn, Cleveland, OH 44195 USA. [Hill, Esther] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Globus, Ruth K.] NASA, Biosci Div, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Midura, RJ (reprint author), Cleveland Clin, Lerner Res Inst, Dept Biomed Engn ND20, 9500 Euclid Ave, Cleveland, OH 44195 USA. EM midurar@ccf.org NR 37 TC 1 Z9 1 U1 1 U2 17 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD NOV PY 2013 VL 92 IS 1 SI SI BP 65 EP 72 DI 10.1016/j.actaastro.2012.04.016 PG 8 WC Engineering, Aerospace SC Engineering GA 212VX UT WOS:000324012000010 ER PT J AU George, KA Rhone, J Chappell, LJ Cucinotta, FA AF George, Kerry A. Rhone, Jordan Chappell, Lori J. Cucinotta, Francis A. TI Cytogenetic biodosimetry using the blood lymphocytes of astronauts SO ACTA ASTRONAUTICA LA English DT Article; Proceedings Paper CT 18th Humans in Space (HIS) Symposium of the International-Academy-of-Astronautics (IAA) CY APR 11-15, 2011 CL Houston, TX SP Int Acad Astronaut DE Biodosimetry; Chromosomal aberrations; Space radiation; HZE nuclei ID CHROMOSOMAL-ABERRATIONS; SPACE EXPLORATION; RISK; DAMAGE; INTERPHASE; METAPHASE; DOSIMETRY; FLIGHTS; CANCER AB Cytogenetic analysis of peripheral blood lymphocytes is the most sensitive and reliable method currently available for in vivo assessment of the biological effects of exposure to radiation and provides the most informative measurement of radiation induced health risks. Data indicates that space missions of a few months or more can induce measureable increases in the yield of chromosome damage in the blood lymphocytes of astronauts that can be used to estimate an organ dose equivalent, and biodosimetry estimates lie within the range expected from physical dosimetry. Space biodosimetry poses some unique challenges compared to terrestrial biological assessments of radiation exposures, but data provides a direct measurement of space radiation damage, which takes into account individual radiosensitivity in the presence of confounding factors such as microgravity and other stress conditions. Moreover if chromosome damage persists in the blood for many years, results can be used for retrospective dose reconstruction. In contrast to physical measurements, which are external to body and require multiple devices to detect all radiation types all of which have poor sensitivity to neutrons, biodosimetry is internal and includes the effects of shielding provided by the body itself plus chromosome damage shows excellent sensitivity to protons, heavy ions, and neutrons. In addition, chromosome damage is reflective of cancer risk and biodosimetry values can therefore be used to validate and develop risk assessment models that can be used to characterize health risk incurred by crewmembers. The current paper presents a review of astronaut biodosimetry data, along with recently derived data on the relative cancer risk estimated using the quantitative approach derived from the European Study Group on Cytogenetic Biomarkers and Health database. (C) 2013 IAA. Published by Elsevier Ltd. All rights reserved. C1 [George, Kerry A.] Wyle Integrated Sci & Engn Grp, Houston, TX 77508 USA. [Rhone, Jordan] Univ Houston, Houston, TX USA. [Chappell, Lori J.] USRA, Div Life Sci, Houston, DC USA. [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP George, KA (reprint author), Wyle Integrated Sci & Engn Grp, 1290 Hercules Dr, Houston, TX 77508 USA. EM kerry.a.george@nasa.gov NR 25 TC 0 Z9 0 U1 2 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD NOV PY 2013 VL 92 IS 1 SI SI BP 97 EP 102 DI 10.1016/j.actaastro.2012.05.001 PG 6 WC Engineering, Aerospace SC Engineering GA 212VX UT WOS:000324012000014 ER PT J AU Steinberg, S Kundrot, C Charles, J AF Steinberg, Susan Kundrot, Craig Charles, John TI Human health and performance considerations for near earth asteroids (NEA) SO ACTA ASTRONAUTICA LA English DT Article; Proceedings Paper CT 18th Humans in Space (HIS) Symposium of the International-Academy-of-Astronautics (IAA) CY APR 11-15, 2011 CL Houston, TX SP Int Acad Astronaut DE Asteroid; Risk criticality; Destination; Distance; Duration; Design AB Humans are considered as a system in the design of any deep space exploration mission. The addition of many potential near asteroid (NEA) destinations to the existing multiple mission architecture for Lunar and Mars missions increases the complexity of human health and performance issues that are anticipated for exploration of space. We suggest that risks to human health and performance be analyzed in terms of the 4 major parameters related to multiple mission architecture: destination, duration, distance and vehicle design. Geological properties of the NEA will influence design of exploration tasks related to sample handling and containment, and extravehicular activity (EVA) capabilities including suit ports and tools. A robotic precursor mission that collects basic information on NEA surface properties would reduce uncertainty about these aspects of the mission as well as aid in mission architecture and exploration task design. Key mission parameters are strongly impacted by duration and distance. The most critical of these is deep-space radiation exposure without even the temporary shielding of a nearby large planetary body. The current space radiation permissible exposure limits (PEL) limits mission duration to 3-10 months depending on age, gender and stage of the solar cycle. Duration also impacts mission architectures including countermeasures for bone, muscle, and cardiovascular atrophy during continuous weightlessness; and behavioral and psychological issues resulting from isolation and confinement. Distance affects communications and limits abort and return options for a NEA mission. These factors are anticipated to have important effects on crew function and autonomous operations, as well as influence medical capability, supplies and training requirements of the crew. The design of a habitat volume that can maintain the physical and psychological health of the crew and support mission operations with limited intervention from earth will require an integrated research and development effort between NASA's Human Research Program (HRP), engineering and human factors groups. Packaging food to extend shelf life and waste management will be important components of vehicle subsystem design. (C) 2012 IAA. Published by Elsevier Ltd. All rights reserved. C1 [Steinberg, Susan] Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA. [Kundrot, Craig; Charles, John] NASA, JSC, Houston, TX 77058 USA. RP Steinberg, S (reprint author), Wyle Sci Technol & Engn Grp, 1290 Hercules, Houston, TX 77058 USA. EM susan.l.steinberg@nasa.gov; Craig.E.Kundrot@nasa.gov; john.b.charles@nasa.gov NR 5 TC 0 Z9 0 U1 1 U2 29 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD NOV PY 2013 VL 92 IS 1 SI SI BP 119 EP 124 DI 10.1016/j.actaastro.2012.05.026 PG 6 WC Engineering, Aerospace SC Engineering GA 212VX UT WOS:000324012000017 ER PT J AU Harstad, K Bellan, J AF Harstad, Kenneth Bellan, Josette TI Prediction of premixed, n-heptane and iso-octane unopposed jet flames using a reduced kinetic model based on constituents and light species SO COMBUSTION AND FLAME LA English DT Article DE Premixed laminar flame prediction using reduced kinetics ID MASS DIFFUSION-COEFFICIENTS; PRIMARY REFERENCE FUELS; HIGH-PRESSURE; SPEEDS AB A model of steady, quasi one-dimensional premixed laminar jet flame developing unopposed into a uniform flow has been formulated using a previously successful reduced chemical-kinetics model [10,11]. A detailed derivation of the steady quasi one-dimensional conservation equations revealed that it is only under very restrictive conditions - probably very difficult to achieve experimentally and the validity of which is not reported in detail in experimental studies - that the quasi one-dimensional concept is meaningful. The governing equations have been mathematically manipulated to be consistent with the framework of the reduced chemical-kinetics model which relied on constituents representing the heavy species, and on quasi-steady light species and unsteady light species. The flame model includes accurate transport property calculation for high-pressure conditions and a real-gas equation of state. Based on a found self-similarity [10,11] which deteriorates at increasingly rich conditions, the chemistry model consists of tables of kinetic rates, quasi-steady species molar fractions and the heavy species mean molar mass extracted from the LLNL model in the framework of the reduced kinetics. The progress variables are only the mass fractions of the unsteady light species and the temperature. The values of the dependent variables are specified at the inflow location and null gradients are specified at the outflow. Simulations were performed for both n-heptane and iso-octane air oxidation over a wide range of pressures and equivalence ratios. The limited documentation of experimental conditions not specifying the inflow velocity (or flux) made it impossible to use this data for detailed comparison. In the one case where the inflow velocity was available for a burner experiment, those conditions were adopted for the simulation and the configuration was changed to a constant-area jet to approach the burner configuration. Results from this simulation compared favorably with the data, considering the different configurations. Results from parametric studies not associated with experimental data showed that at stoichiometric conditions the flame temperature, flame velocity and strain rate are not sensitive to the pressure, although flames become increasingly thinner with increasing pressure and the yield of the unsteady light species is different. Computations conducted at 40 bar for various equivalence ratios and for velocities differing with the equivalence ratio showed that the maximum flame velocity, flame strain and flame temperature were obtained at stoichometric conditions. Finally, we discuss the limitations of utilizing a priori obtained reduced chemical-kinetic models in flames calculations. (C) 2013 The Combustion Institute. Published by Elsevier Inc. All rights reserved. C1 [Harstad, Kenneth; Bellan, Josette] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bellan, Josette] CALTECH, Mech & Civil Engn Deparmentt, Pasadena, CA 91125 USA. RP Bellan, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 125-109, Pasadena, CA 91109 USA. EM Josette.Bellan@jpl.nasa.gov FU Army Research Office FX This study was conducted at the California Institute of Technology, Jet Propulsion Laboratory (JPL), and was sponsored by the Army Research Office, with Dr. Ralph Anthenien as Program Manager. Computations were performed using the JPL Supercomputing facility. NR 27 TC 1 Z9 1 U1 2 U2 17 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0010-2180 J9 COMBUST FLAME JI Combust. Flame PD NOV PY 2013 VL 160 IS 11 BP 2404 EP 2421 DI 10.1016/j.combustflame.2013.06.005 PG 18 WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary; Engineering, Chemical; Engineering, Mechanical SC Thermodynamics; Energy & Fuels; Engineering GA 212TT UT WOS:000324006400011 ER PT J AU Nayagam, V AF Nayagam, Vedha TI Activation energy asymptotics for methanol droplet extinction in microgravity SO COMBUSTION AND FLAME LA English DT Article DE Methanol droplet combustion; Activation energy asymptotics; Extinction; Microgravity ID COMBUSTION; IGNITION; NUMBER AB An activation energy asymptotic theory for methanol droplet combustion in microgravity is presented by extending earlier models to account for time-dependent water dissolution or evaporation from the liquid droplet. The model predictions for droplet extinction diameter as a function of its initial diameter are shown to compare favorably with experimental results for methanol burning in air. (c) 2013 The Combustion Institute. Published by Elsevier Inc. All rights reserved. C1 NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. RP Nayagam, V (reprint author), NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. EM v.nayagam@grc.nasa.gov NR 19 TC 2 Z9 2 U1 1 U2 7 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0010-2180 J9 COMBUST FLAME JI Combust. Flame PD NOV PY 2013 VL 160 IS 11 BP 2638 EP 2640 DI 10.1016/j.combustflame.2013.05.011 PG 3 WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary; Engineering, Chemical; Engineering, Mechanical SC Thermodynamics; Energy & Fuels; Engineering GA 212TT UT WOS:000324006400031 ER PT J AU Douillard, B Nourani-Vatani, N Johnson-Roberson, M Pizarro, O Williams, S Roman, C Vaughn, I AF Douillard, B. Nourani-Vatani, N. Johnson-Roberson, M. Pizarro, O. Williams, S. Roman, C. Vaughn, I. TI Frequency-based underwater terrain segmentation SO AUTONOMOUS ROBOTS LA English DT Article DE Perception; Segmentation; Underwater; Scan registration; 3D processing; Structured light; Dense stereo ID IMAGE SEGMENTATION; RANGE IMAGE; REGISTRATION; VEHICLE; SONAR AB A method for segmenting three-dimensional data of underwater unstructured terrains is presented. The three-dimensional point clouds are converted to two-dimensional elevation maps and analyzed for segmentation in the frequency domain. The lower frequency components represent the slower varying undulations of the underlying ground. The cut-off frequency, below which the frequency components form the ground surface, is determined automatically using peak detection. The user can also specify a maximum admissible size of objects to drive the automatic detection of the cut-off frequency. The points above the estimated ground surface are clustered via standard proximity clustering to form object segments. The precision of the segmentation is compared against ground truth hand labelled data acquired by a stereo camera pair and a structured light sensor. It is also evaluated for registration error when the extracted segments are used for sub-map alignment. The proposed approach is compared to three point cloud based and two image based segmentation algorithms. The results show that the approach is applicable to a range of different terrains and is able to generate features useful for navigation. C1 [Douillard, B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nourani-Vatani, N.; Pizarro, O.; Williams, S.] Univ Sydney, Australian Ctr Field Robot, Sydney, NSW 2006, Australia. [Johnson-Roberson, M.] Univ Michigan, Dept Naval Architecture & Marine Engn, Ann Arbor, MI 48109 USA. [Roman, C.; Vaughn, I.] Univ Rhode Isl, Dept Ocean Engn, Narragansett, RI 02882 USA. RP Douillard, B (reprint author), CALTECH, Jet Prop Lab, M-S 198-235,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Bertrand.Douillard@jpl.nasa.gov; n.nourani-vatani@acfr.usyd.edu.au; mattjr@umich.edu; o.pizarro@acfr.usyd.edu.au; s.william@acfr.usyd.edu.au RI Nourani, Vahid/F-4051-2017; OI Williams, Stefan/0000-0001-9416-5639 FU Australian Research Council (ARC) [DP110101986]; Australian Government through the SIEF program; Australian Centre for Field Robotics at the University of Sydney FX This research was supported by the Australian Research Council (ARC) through the Discovery program (DP110101986), the Australian Government through the SIEF program, and by the Australian Centre for Field Robotics at the University of Sydney. The authors would like to thank Alastair Quadros, Peter Morton and Vsevolod Vlaskine for valuable help with software, as well as James P. Underwood, Mitch Bryson and Donald Danserau for useful discussions. NR 36 TC 1 Z9 1 U1 0 U2 33 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0929-5593 EI 1573-7527 J9 AUTON ROBOT JI Auton. Robot. PD NOV PY 2013 VL 35 IS 4 SI SI BP 255 EP 269 DI 10.1007/s10514-013-9353-0 PG 15 WC Computer Science, Artificial Intelligence; Robotics SC Computer Science; Robotics GA 208CV UT WOS:000323654900003 ER PT J AU Fisher, TC Carpenter, MH AF Fisher, Travis C. Carpenter, Mark H. TI High-order entropy stable finite difference schemes for nonlinear conservation laws: Finite domains SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE High-order finite difference methods; Conservation; Skew symmetric; Entropy conservation; Entropy stability; Navier-Stokes; SBP-SAT; WENO ID NAVIER-STOKES EQUATIONS; ESSENTIALLY NONOSCILLATORY SCHEMES; BOUNDARY-VALUE-PROBLEMS; PARTS OPERATORS; WENO SCHEMES; SYSTEMS; APPROXIMATIONS; ENERGY; THERMODYNAMICS; SIMULATIONS AB Nonlinear entropy stability is used to derive provably stable high-order finite difference operators including boundary closure stencils, for the compressible Navier-Stokes equations. A comparison technique is used to derive a new Entropy Stable Weighted Essentially Non-Oscillatory (SSWENO) finite difference method, appropriate for simulations of problems with shocks. Viscous terms are approximated using conservative, entropy stable, narrow-stencil finite difference operators. The efficacy of the new discrete operators is demonstrated using both smooth and discontinuous test cases. Published by Elsevier Inc. C1 [Fisher, Travis C.; Carpenter, Mark H.] NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA. [Fisher, Travis C.] Purdue Univ, Sch Mech Engn, W Lafayette, IN 47907 USA. RP Carpenter, MH (reprint author), NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA. EM tcfishe@sandia.gov; mark.h.carpenter@nasa.gov NR 48 TC 20 Z9 20 U1 2 U2 17 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9991 J9 J COMPUT PHYS JI J. Comput. Phys. PD NOV 1 PY 2013 VL 252 BP 518 EP 557 DI 10.1016/j.jcp.2013.06.014 PG 40 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 194KZ UT WOS:000322633500027 ER PT J AU Papadimitriou, VC McGillen, MR Smith, SC Jubb, AM Portmann, RW Hall, BD Fleming, EL Jackman, CH Burkholder, JB AF Papadimitriou, Vassileios C. McGillen, Max R. Smith, Shona C. Jubb, Aaron M. Portmann, Robert W. Hall, Bradley D. Fleming, Eric L. Jackman, Charles H. Burkholder, James B. TI 1,2-Dichlorohexafluoro-cyclobutane (1,2-c-C4F6Cl2, R-316c) a Potent Ozone Depleting Substance and Greenhouse Gas: Atmospheric Loss Processes, Lifetimes, and Ozone Depletion and Global Warming Potentials for the (E) and (Z) Stereoisomers SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID SPECTRUM TEMPERATURE-DEPENDENCE; STRATOSPHERIC OZONE; IMPACT; O(D-1); 1,2-DICHLOROHEXAFLUOROCYCLOBUTANE; CHEMISTRY; EXCHANGE; CLIMATE; YIELDS; MODEL AB The atmospheric processing of (E)- and (Z)-1,2-dichlorohexafluorocyclobutane (1,2-c-C4F6Cl2, R-316c) was examined in this work as the ozone depleting (ODP) and global warming (GWP) potentials of this proposed replacement compound are presently unknown. The predominant atmospheric loss processes and infrared absorption spectra of the R-316c isomers were measured to provide a basis to evaluate their atmospheric lifetimes and, thus, ODPs and GWPs. UV absorption spectra were measured between 184.95 to 230 nm at temperatures between 214 and 296 K and a parametrization for use in atmospheric modeling is presented. The Cl atom quantum yield in the 193 nm photolysis of R-316c was measured to be 1.90 +/- 0.27. Hexafluorocydobutene (c-C4F6) was determined to be a photolysis co-product with molar yields of 0.7 and 1.0 (+/-10%) for (E)- and (Z)-R-316c, respectively. The 296 K total rate coefficient for the O(D-1) + R-316c reaction, i.e., O(D-1) loss, was measured to be (1.56 +/- 0.11) X 10(-10) cm(3) molecule(-1)s(-1) and the reactive rate coefficient, i.e., R-316c loss, was measured to be (1.36 +/- 0.20) X 10(-10) cm(3) molecule(-1) s(-1) corresponding to a 88% reactive yield. Rate coefficient upper-limits for the OH and O-3 reaction with R-316c were determined to be <2.3 X 10(-17) and <2.0 x 10(-22) cm(3) molecule(-1) s(-1), respectively, at 296 K The quoted uncertainty limits are 2 sigma and include estimated systematic errors. Local and global annually averaged lifetimes for the (E)- and (Z)-R-316c isomers were calculated using a 2-D atmospheric model to be 74.6 +/- 3 and 114.1 +/- 10 years, respectively, where the estimated uncertainties are due solely to the uncertainty in the UV absorption spectra. Stratospheric photolysis is the predominant atmospheric loss process for both isomers with the O(D-1) reaction making a minor, similar to 2% for the (E) isomer and 7% for the (Z) isomer, contribution to the total atmospheric loss. Ozone depletion potentials for (E)- and (Z)-R-316c were calculated using the 2-D model to be 0.46 and 0.54, respectively. Infrared absorption spectra for (E)- and (Z)-R-316c were measured at 296 K and used to estimate their radiative efficiencies (REs) and GWPs; 100-year time-horizon GWPs of 4160 and 5400 were obtained for (E)- and (Z)-R-316c, respectively. Both isomers of R-316c are shown in this work to be long-lived ozone depleting substances and potent greenhouse gases. C1 [Papadimitriou, Vassileios C.; McGillen, Max R.; Smith, Shona C.; Jubb, Aaron M.; Portmann, Robert W.; Burkholder, James B.] NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO 80305 USA. [Papadimitriou, Vassileios C.; McGillen, Max R.; Smith, Shona C.; Jubb, Aaron M.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Papadimitriou, Vassileios C.] Univ Crete, Dept Chem, Lab Photochem & Chem Kinet, Iraklion 71003, Crete, Greece. [Hall, Bradley D.] NOAA, Earth Syst Res Lab, Global Monitoring Div, Boulder, CO 80305 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 20706 USA. RP Burkholder, JB (reprint author), NOAA, Earth Syst Res Lab, Div Chem Sci, 325 Broadway, Boulder, CO 80305 USA. EM James.B.Burkholder@noaa.gov RI McGillen, Max/G-5196-2011; Jubb, Aaron/G-4538-2013; Jackman, Charles/D-4699-2012; Burkholder, James/H-4914-2013; Portmann, Robert/C-4903-2009; Manager, CSD Publications/B-2789-2015; OI McGillen, Max/0000-0002-1623-5985; Jubb, Aaron/0000-0001-6875-1079; Portmann, Robert/0000-0002-0279-6087; Smith, Shona/0000-0001-7667-6216 FU NOAAs Climate Goal; NASAs Atmospheric Composition: Laboratory Studies and Modeling and Analysis Programs FX This work was supported in part by NOAAs Climate Goal and NASAs Atmospheric Composition: Laboratory Studies and Modeling and Analysis Programs. NR 32 TC 5 Z9 5 U1 0 U2 17 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 OCT 31 PY 2013 VL 117 IS 43 BP 11049 EP 11065 DI 10.1021/jp407823k PG 17 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 247HL UT WOS:000326608400007 PM 24079521 ER PT J AU Machacek, JR Anderson, EK Makochekanwa, C Buckman, SJ Sullivan, JP AF Machacek, J. R. Anderson, E. K. Makochekanwa, C. Buckman, S. J. Sullivan, J. P. TI Positron scattering from molecular hydrogen SO PHYSICAL REVIEW A LA English DT Article ID SCHWINGER MULTICHANNEL METHOD; LOW-ENERGY POSITRONS; CROSS-SECTIONS; ATOMS; IONIZATION; COLLISIONS; IMPACT; H-2; ANNIHILATION; GASES AB We present results for total and partial cross sections for positron scattering from H-2. The total scattering and positronium formation cross sections are reported between 0.5 and 200 eV. Total quasielastic and inelastic scattering cross sections are reported for energies between the positronium formation threshold and 50 eV, with quasielastic differential scattering cross sections reported at 1, 3, 5, 7, and 10 eV. Our results are compared with previous work, both experimental and theoretical, with particular attention paid to the region below the positronium formation threshold, where there are apparent discrepancies in previous work. A discussion of possible reasons for discrepancies between this and previous work is presented, including a focus on known systematic effects in the experimental results. C1 [Machacek, J. R.; Anderson, E. K.; Makochekanwa, C.; Buckman, S. J.; Sullivan, J. P.] Australian Natl Univ, Res Sch Phys & Engn, ARC Ctr Antimatter Matter Studies, Canberra, ACT 0200, Australia. [Buckman, S. J.] Univ Malaya, Inst Math Sci, Kuala Lumpur, Malaysia. RP Machacek, JR (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RI Sullivan, James/F-3040-2011; Buckman, Stephen/B-4750-2009; Machacek, Joshua/A-5316-2011 OI Sullivan, James/0000-0003-4489-4926; FU Australia Research Council (ARC) through its Centre of Excellence Program FX Funding for this work was provided by the Australia Research Council (ARC) through its Centre of Excellence Program. The authors also thank Steve Battisson and Ross Tranter for the excellent technical support provided during the course of this work. NR 33 TC 11 Z9 11 U1 2 U2 17 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD OCT 31 PY 2013 VL 88 IS 4 AR 042715 DI 10.1103/PhysRevA.88.042715 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 244LE UT WOS:000326389100008 ER PT J AU Fong, KC Wollman, EE Ravi, H Chen, W Clerk, AA Shaw, MD Leduc, HG Schwab, KC AF Fong, Kin Chung Wollman, Emma E. Ravi, Harish Chen, Wei Clerk, Aashish A. Shaw, M. D. Leduc, H. G. Schwab, K. C. TI Measurement of the Electronic Thermal Conductance Channels and Heat Capacity of Graphene at Low Temperature SO PHYSICAL REVIEW X LA English DT Article ID LORENZ NUMBER; SHOT-NOISE; QUANTUM AB The ability to transport energy is a fundamental property of the two-dimensional Dirac fermions in graphene. Electronic thermal transport in this system is relatively unexplored and is expected to show unique fundamental properties and to play an important role in future applications of graphene, including optoelectronics, plasmonics, and ultrasensitive bolometry. Here, we present measurements of bipolar thermal conductances due to electron diffusion and electron-phonon coupling and infer the electronic specific heat, with a minimum value of 10k(B) (10(-22) J/K) per square micron. We test the validity of the Wiedemann-Franz law and find that the Lorenz number equals 1.32 x (pi(2)/3)(k(B)/e)(2). The electron-phonon thermal conductance has a temperature power law T-2 at high doping levels, and the coupling parameter is consistent with recent theory, indicating its enhancement by impurity scattering. We demonstrate control of the thermal conductance by electrical gating and by suppressing the diffusion channel using NbTiN superconducting electrodes, which sets the stage for future graphene-based single-microwave photon detection. C1 [Fong, Kin Chung; Wollman, Emma E.; Ravi, Harish; Schwab, K. C.] CALTECH, Kavli Nanosci Inst, Pasadena, CA 91125 USA. [Chen, Wei; Clerk, Aashish A.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Shaw, M. D.; Leduc, H. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Schwab, KC (reprint author), CALTECH, Kavli Nanosci Inst, MC 128-95, Pasadena, CA 91125 USA. EM schwab@caltech.edu RI Clerk, Aashish/A-4008-2008; OI Clerk, Aashish/0000-0001-7297-9068; Wollman, Emma/0000-0002-5474-3745 FU FAME Center, one of six centers of STARnet; FAME Center, one of six centers of STARnet, a Semiconductor Research Corporation program; MARCO; DARPA; U.S. NSF [DMR-0804567]; Institute for Quantum Information and Matter, an NSF Physics Frontiers Center; Gordon and Betty Moore Foundation; Department of Energy Office of Science Graduate Fellowship Program (DOE SCGF) [DE-AC05-06OR23100] FX We acknowledge helpful conversations with P. Kim, J. Hone, E. Henriksen, and D. Nandi. This work was supported in part by (1) the FAME Center, one of six centers of STARnet, a Semiconductor Research Corporation program sponsored by MARCO and DARPA, (2) the U.S. NSF (DMR-0804567), (3) the Institute for Quantum Information and Matter, an NSF Physics Frontiers Center with the support of the Gordon and Betty Moore Foundation, and (4) the Department of Energy Office of Science Graduate Fellowship Program (DOE SCGF), made possible in part by the American Recovery and Reinvestment Act of 2009, administered by ORISE-ORAU under Contract No. DE-AC05-06OR23100. We are grateful to G. Rossman for the use of a Raman spectroscopy setup. Device fabrication was performed at the Kavli Nanoscience Institute (Caltech) and at the Micro Device Laboratory (NASA/JPL), and 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 50 TC 24 Z9 24 U1 7 U2 69 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2160-3308 J9 PHYS REV X JI Phys. Rev. X PD OCT 29 PY 2013 VL 3 IS 4 AR 041008 DI 10.1103/PhysRevX.3.041008 PG 7 WC Physics, Multidisciplinary SC Physics GA 250WJ UT WOS:000326886900001 ER PT J AU Rignot, E Mouginot, J Larsen, CF Gim, Y Kirchner, D AF Rignot, E. Mouginot, J. Larsen, C. F. Gim, Y. Kirchner, D. TI Low-frequency radar sounding of temperate ice masses in Southern Alaska SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID BLACK RAPIDS GLACIER; BERING GLACIER; LASER ALTIMETRY; HUBBARD GLACIER; SEA-LEVEL; USA; AIRBORNE; COLUMBIA; CANADA; SYSTEM AB We present the Warm Ice Sounding Explorer (WISE), a low-frequency (2.5 MHz) radar for the sounding of temperate ice. WISE deployment in southern Alaska in 2008 and 2012 provides comprehensive measurements of glacier thickness, reveals deep valleys beneath glaciers and the full extent of zones grounded below sea level. The east branch of Columbia Glacier is deeper that its main branch and remains below sea level 20 km farther inland. Ice is 1000 m deep on Tazlina Glacier. On Bering glacier, two sills separate three deep bed depressions (> 1200 m) that coincide with the dynamic balance lines during surges. The piedmont lobe of Malaspina Glacier and the lower reaches of Hubbard Glacier are entirely grounded below sea level 40 and 10 km, respectively, from their termini. Knowledge of ice thickness in these regions helps better understand their glacier dynamics, mass balance, and impact on sea level. C1 [Rignot, E.; Mouginot, J.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Rignot, E.; Gim, Y.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Larsen, C. F.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. [Kirchner, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. RP Rignot, E (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. EM erignot@uci.edu RI Mouginot, Jeremie/G-7045-2015; Rignot, Eric/A-4560-2014 OI Rignot, Eric/0000-0002-3366-0481 FU NASA [NNX11AC24G S03] FX The 2012 deployment was funded by NASA's Operation IceBridge grant NNX11AC24G S03. The work was performed at UCI, UI, UAF, and JPL under contracts with NASA's Cryospheric Science, Planetary Instrument Definition and Development (PIDDP) and Suborbital Programs. We dedicate this study to the memory of Dr. Ali Safaeinili, the creator of WISE, who passed away in 2009. NR 24 TC 12 Z9 12 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 OCT 28 PY 2013 VL 40 IS 20 BP 5399 EP 5405 DI 10.1002/2013GL057452 PG 7 WC Geosciences, Multidisciplinary SC Geology GA 301DY UT WOS:000330514200013 ER PT J AU Gierach, MM Messie, M Lee, T Karnauskas, KB Radenac, MH AF Gierach, Michelle M. Messie, Monique Lee, Tong Karnauskas, Kristopher B. Radenac, Marie-Helene TI Biophysical responses near equatorial islands in the Western Pacific Ocean during El Nino/La Nina transitions SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID GALAPAGOS-ISLANDS; COLD-TONGUE; ENSO; CHLOROPHYLL; CLIMATE; EVENTS; BLOOM AB The biological response in the western equatorial Pacific Ocean during El Nino/La Nina transitions and the underlying physical mechanisms were investigated. A chlorophyll a bloom was observed near the Gilbert Islands during the 2010 El Nino/La Nina transition, whereas no bloom was observed during the 2007 El Nino/La Nina transition. Compared to the previously observed bloom during the 1998 El Nino/La Nina transition, the 2010 bloom was weaker, lagged by 1-2 months, and was displaced eastward by similar to 200 km. Analysis suggested that the occurrence, magnitude, timing, and spatial pattern of the blooms were controlled by two factors: easterly winds in the western equatorial Pacific during the transition to La Nina and the associated island mass effect that enhanced vertical processes (upwelling and vertical mixing), and the preconditioning of the thermocline depth and barrier layer thickness by the preceding El Nino that regulated the efficiency of the vertical processes. Despite the similar strength of easterly winds in the western equatorial Pacific during the 1998 and 2010 transitions to La Nina, the 20092010 El Nino prompted a deeper thermocline and thicker barrier layer than the 1997-1998 El Nino that hampered the efficiency of the vertical processes in supplying nutrients from the thermocline to the euphotic zone, resulting in a weaker bloom. C1 [Gierach, Michelle M.; Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Messie, Monique] Monterey Bay Aquarium Res Inst, Moss Landing, CA USA. [Karnauskas, Kristopher B.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. [Radenac, Marie-Helene] Lab Etud Geophys & Oceanog Spatiales, Toulouse, France. RP Gierach, MM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 300-323, Pasadena, CA 91109 USA. EM michelle.gierach@jpl.nasa.gov RI Messie, Monique/K-2022-2012; OI Messie, Monique/0000-0002-4985-3413; Gierach, Michelle/0000-0002-8161-4121 FU NASA; NASA New Investigator Program in Earth Science; NSF [OCE 1031971] FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. M. M. G. was supported by the NASA New Investigator Program in Earth Science. K. B. K. was supported by NSF OCE 1031971. NR 24 TC 3 Z9 3 U1 1 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD OCT 28 PY 2013 VL 40 IS 20 BP 5473 EP 5479 DI 10.1002/2013GL057828 PG 7 WC Geosciences, Multidisciplinary SC Geology GA 301DY UT WOS:000330514200026 ER PT J AU Hansen, J Sato, M Russell, G Kharecha, P AF Hansen, James Sato, Makiko Russell, Gary Kharecha, Pushker TI Climate sensitivity, sea level and atmospheric carbon dioxide SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Article DE climate; climate sensitivity; palaeoclimate; sea level ID EOCENE THERMAL MAXIMUM; LAST INTERGLACIAL PERIOD; SOUTHWEST PACIFIC-OCEAN; GEOLOGICAL WATER CYCLE; HUMAN HEAT TOLERANCE; PAST 800,000 YEARS; METHANE HYDRATE; ANTARCTIC ICE; RUNAWAY GREENHOUSE; OXYGEN ISOTOPES AB Cenozoic temperature, sea level and CO2 covariations provide insights into climate sensitivity to external forcings and sea-level sensitivity to climate change. Climate sensitivity depends on the initial climate state, but potentially can be accurately inferred from precise palaeoclimate data. Pleistocene climate oscillations yield a fast-feedback climate sensitivity of 3 +/- 1 degrees C for a 4 W m(-2) CO2 forcing if Holocene warming relative to the Last Glacial Maximum (LGM) is used as calibration, but the error (uncertainty) is substantial and partly subjective because of poorly defined LGM global temperature and possible human influences in the Holocene. Glacial-to-interglacial climate change leading to the prior (Eemian) interglacial is less ambiguous and implies a sensitivity in the upper part of the above range, i.e. 3-4 degrees C for a 4 W m(-2) CO2 forcing. Slow feedbacks, especially change of ice sheet size and atmospheric CO2, amplify the total Earth system sensitivity by an amount that depends on the time scale considered. Ice sheet response time is poorly defined, but we show that the slow response and hysteresis in prevailing ice sheet models are exaggerated. We use a global model, simplified to essential processes, to investigate state dependence of climate sensitivity, finding an increased sensitivity towards warmer climates, as low cloud cover is diminished and increased water vapour elevates the tropopause. Burning all fossil fuels, we conclude, would make most of the planet uninhabitable by humans, thus calling into question strategies that emphasize adaptation to climate change. C1 [Hansen, James; Sato, Makiko; Kharecha, Pushker] Columbia Univ, Earth Inst, New York, NY 10027 USA. [Russell, Gary; Kharecha, Pushker] NASA, Goddard Inst Space Studies, New York, NY 10027 USA. RP Hansen, J (reprint author), Columbia Univ, Earth Inst, New York, NY 10027 USA. EM jimehansen@gmail.com NR 137 TC 42 Z9 42 U1 10 U2 79 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 OCT 28 PY 2013 VL 371 IS 2001 AR UNSP 20120294 DI 10.1098/rsta.2012.0294 PG 31 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 298GN UT WOS:000330312300002 PM 24043864 ER PT J AU Lin, GP Furst, JU Strekalov, DV Yu, N AF Lin, Guoping Fuerst, Josef U. Strekalov, Dmitry V. Yu, Nan TI Wide-range cyclic phase matching and second harmonic generation in whispering gallery resonators SO APPLIED PHYSICS LETTERS LA English DT Article ID CONTINUOUS-WAVE; MODES; LIGHT; BBO; EMISSION; CRYSTAL AB We report on a wide-range efficient method for optical second harmonic generation based on a whispering gallery mode resonator made from crystalline beta barium borate. In this single resonator, we were able to generate second harmonic fields for four different pump wavelengths ranging from the infrared (1557 nm) to the visible (634 nm) regime. The highest conversion efficiencies achieved in this whispering gallery mode resonator are as high as 4.6% (mW)(-1). This conversion process is based on type-I phase matching with continuously varying optical axis orientation in an xy-cut configuration of the resonator. In such a geometry, the second harmonic whispering gallery mode experiences an oscillatory modulation of the refractive index. This enables wide-range cyclic phase matching along the circumference of the disk resonator. (c) 2013 AIP Publishing LLC. C1 [Lin, Guoping; Fuerst, Josef U.; Strekalov, Dmitry V.; Yu, Nan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Fuerst, Josef U.] Univ Erlangen Nurnberg, Dept Phys, Erlangen, Germany. RP Lin, GP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM nan.yu@jpl.nasa.gov RI Lin, Guoping/I-3381-2015 OI Lin, Guoping/0000-0003-4007-1850 FU NASA; Max Planck Society FX This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. G. Lin acknowledges support from the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities (ORAU). J. U. Furst acknowledges financial support from the Max Planck Society and thanks Rosalin Hertrich for valuable comments. NR 32 TC 21 Z9 21 U1 2 U2 17 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD OCT 28 PY 2013 VL 103 IS 18 AR 181107 DI 10.1063/1.4827538 PG 4 WC Physics, Applied SC Physics GA 263NT UT WOS:000327816000051 ER PT J AU Alexander, SP Klekociuk, AR McDonald, AJ Pitts, MC AF Alexander, S. P. Klekociuk, A. R. McDonald, A. J. Pitts, M. C. TI Quantifying the role of orographic gravity waves on polar stratospheric cloud occurrence in the Antarctic and the Arctic SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article AB [1] The proportion of polar stratospheric clouds due to orographic gravity wave (OGW) forcing is quantified during four Antarctic (2007-2010) and four Arctic (2006/2007 to 2009/2010) winter seasons. OGW-active days are defined as those days above major polar mountain ranges which have wave-ice polar stratospheric clouds (PSCs), tropospheric wind conditions appropriate for orographic wave generation and propagation, and stratospheric temperatures below the frost point: 37% of Antarctic days and 12% of Arctic days are OGW-active. Regions downstream of these mountain ranges are defined using a forward-trajectory model which follows particle movement from ridge lines for 24 h periods. In both hemispheres in these mountain regions, more than 75% of H2O ice PSCs and around 50% of a high number density liquid-nitric acid trihydrate mixture class (Mix 2-enh) are attributed to OGW activity, with the balances due to non-orographic formation. For the whole Arctic (equatorward of 82 degrees), 25% of Mix 2-enh and 54% of H2O ice PSCs are attributed to OGWs, while for the whole Antarctic, 7% of Mix 2-enh and 13% of H2O ice PSCs are attributed to OGWs. For all types of PSC, 5% in the whole Antarctic and 12% in the whole Arctic are attributed to OGW forcing. While gravity waves play a role in PSC formation in the Antarctic, overall it is minor compared with other forcing sources. However, in the synoptically warmer Arctic, much larger proportions of PSCs are due to OGW activity. C1 [Alexander, S. P.; Klekociuk, A. R.] Australian Antarctic Div, 203 Channel Highway, Kingston, Tas 7050, Australia. [McDonald, A. J.] Univ Canterbury, Dept Phys & Astron, Christchurch, New Zealand. [Pitts, M. C.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Alexander, SP (reprint author), Australian Antarctic Div, 203 Channel Highway, Kingston, Tas 7050, Australia. EM alexander@aad.gov.au RI Klekociuk, Andrew/A-4498-2015; OI Klekociuk, Andrew/0000-0003-3335-0034; Alexander, Simon/0000-0001-6823-8857; McDonald, Adrian/0000-0002-1456-6254 FU Australian Antarctic program [737, 3140, 4012]; Antarctica New Zealand; Royal Society of New Zealand FX The CALIPSO CALIOP v3.01 Level 1B Profile data products were obtained through the NASA Langley Atmospheric Science Data Center (ASDC). The COSMIC version 2.0 dry temperature data were obtained from the COSMIC Data Analysis and Archive Center (CDAAC). Aura MLS data (v3.3) used in this study were acquired as part of the NASA's Earth-Sun System Division and archived and distributed by the Goddard Earth Sciences (GES) Data and Information Services Center (DISC) Distributed Active Archive Center (DAAC). This research was conducted for projects 737, 3140, and 4012 of the Australian Antarctic program and partially supported by Antarctica New Zealand. This work was partially supported by the Royal Society of New Zealand Marsden Fund project Evaluating the Impact of Excess Ionization on the Atmosphere. We thank the three anonymous reviewers for their constructive comments, which allowed us to improve an earlier version of the manuscript. NR 53 TC 8 Z9 8 U1 1 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 OCT 27 PY 2013 VL 118 IS 20 BP 11493 EP 11507 DI 10.1002/2013JD020122 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA V45WS UT WOS:000209847300002 ER PT J AU Wolfe, RE Lin, GQ Nishihama, M Tewari, KP Tilton, JC Isaacman, AR AF Wolfe, Robert E. Lin, Guoqing Nishihama, Masahiro Tewari, Krishna P. Tilton, James C. Isaacman, Alice R. TI Suomi NPP VIIRS prelaunch and on-orbit geometric calibration and characterization SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article AB [1] The Visible Infrared Imaging Radiometer Suite (VIIRS) sensor was launched 28 October 2011 on the Suomi National Polar-orbiting Partnership (SNPP) satellite. VIIRS has 22 spectral bands covering the spectrum between 0.412 mu m and 12.01 mu m, including 16 moderate resolution bands (M-bands) with a nominal spatial resolution of 750m at nadir, five imaging resolution bands (I-bands) with a nominal spatial resolution of 375m at nadir, and a day-night band (DNB) with a near-constant nominal 750 m spatial resolution throughout the scan. These bands are located in a visible and near-infrared focal plane assembly (FPA), a shortwave and midwave infrared FPA, and a long-wave infrared FPA. All bands, except the DNB, are coregistered for proper environmental data records retrievals. Observations from VIIRS instrument provide long-term measurements of biogeophysical variables for climate research and polar satellite data stream for the operational community's use in weather forecasting and disaster relief and other applications. Well Earth-located (geolocated) instrument data are important to retrieving accurate biogeophysical variables. This paper describes prelaunch pointing and alignment measurements, and the two sets of on-orbit correction of geolocation errors, the first of which corrected error from 1300m to within 75 m (20% I-band pixel size) and the second of which fine-tuned scan-angle dependent errors, bringing VIIRS geolocation products to high maturity in one and a half years of the SNPP VIIRS on-orbit operations. Prelaunch calibration and the on-orbit characterization of sensor spatial impulse responses and band-to-band coregistration are also described. C1 [Wolfe, Robert E.; Tilton, James C.] NASA, Goddard Space Flight Ctr, Greenbelt Rd, Greenbelt, MD 20771 USA. [Lin, Guoqing; Tewari, Krishna P.; Isaacman, Alice R.] Innovim, Greenbelt, MD USA. [Nishihama, Masahiro] Sigma Space Corp, Lanham, MD USA. RP Wolfe, RE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt Rd, Greenbelt, MD 20771 USA. EM Robert.E.Wolfe@nasa.gov RI Wolfe, Robert/E-1485-2012 OI Wolfe, Robert/0000-0002-0915-1855 FU SNPP SDS; SNPP Project Science Office; NOAA Center for Satellite Applications and Research (STAR) FX The authors acknowledge the sponsorship of this work by the SNPP SDS, the SNPP Project Science Office, and NOAA Center for Satellite Applications and Research (STAR), and the cooperation and assistance from many colleagues at The Aerospace Corporation, Raytheon Company, Northrop Grumman Aerospace Systems, the SNPP Land PEATE, the VIIRS Calibration Support Team (VCST) Radiometric Group, and the JPSS Program Office. NR 17 TC 31 Z9 31 U1 2 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 OCT 27 PY 2013 VL 118 IS 20 BP 11508 EP 11521 DI 10.1002/jgrd.50873 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA V45WS UT WOS:000209847300003 ER PT J AU Trail, M Tsimpidi, AP Liu, P Tsigaridis, K Hu, Y Nenes, A Stone, B Russell, AG AF Trail, M. Tsimpidi, A. P. Liu, P. Tsigaridis, K. Hu, Y. Nenes, A. Stone, B. Russell, A. G. TI Potential impact of land use change on future regional climate in the Southeastern US: Reforestation and crop land conversion SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article AB [1] The impact of future land use and land cover changes (LULCC) on regional and global climate is one of the most challenging aspects of understanding anthropogenic climate change. We study the impacts of LULCC on regional climate in the southeastern U.S. by downscaling the NASA Goddard Institute for Space Studies global climate model E to the regional scale using a spectral nudging technique with the Weather Research and Forecasting Model. Climate-relevant meteorological fields are compared for two southeastern U.S. LULCC scenarios to the current land use/cover for four seasons of the year 2050. In this work it is shown that reforestation of cropland in the southeastern U.S. tends to warm surface air by up to 0.5 K, while replacing forested land with cropland tends to cool the surface air by 0.5 K. Processes leading to this response are investigated and sensitivity analyses conducted. The sensitivity analysis shows that results are most sensitive to changes in albedo and the stomatal resistance. Evaporative cooling of croplands also plays an important role in regional climate. Implications of LULCC on air quality are discussed. Summertime warming associated with reforestation of croplands could increase the production of some secondary pollutants, while a higher boundary layer will decrease pollutant concentrations; wintertime warming may decrease emissions from biomass burning from wood stoves. C1 [Trail, M.; Tsimpidi, A. P.; Liu, P.; Hu, Y.; Russell, A. G.] Georgia Inst Technol, Sch Civil & Environm Engn, Atlanta, GA 30332 USA. [Tsigaridis, K.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Tsigaridis, K.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Nenes, A.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Nenes, A.] Georgia Inst Technol, Sch Chem & Biomol Engn, Atlanta, GA 30332 USA. [Stone, B.] Georgia Inst Technol, Sch City & Reg Planning, Atlanta, GA 30332 USA. RP Trail, M (reprint author), Georgia Inst Technol, Sch Civil & Environm Engn, Atlanta, GA 30332 USA. EM mcus2rail@gmail.com RI Hu, Yongtao/H-7543-2016 OI Hu, Yongtao/0000-0002-5161-0592 FU US EPA [EPA-G2008-STAR-J1]; NASA FX While this work was supported, in part, by grants from the US EPA (EPA-G2008-STAR-J1) and NASA, reference herein to any specific commercial products, process, or service by trade name, trademark, manufacturer, or otherwise, does not necessarily constitute or imply their endorsement or recommendation. NARR data were provided by the NOAA/OAR/ESRL PSD, Boulder, Colorado, USA, from their Web site at http://www.esrl.noaa.gov/psd/. The views and opinions expressed herein are those of the authors and do not necessarily state or reflect those of the United States Government. NR 51 TC 13 Z9 14 U1 0 U2 33 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 OCT 27 PY 2013 VL 118 IS 20 BP 11577 EP 11588 DI 10.1002/2013JD020356 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA V45WS UT WOS:000209847300008 ER PT J AU Cao, CY Xiong, J Blonski, S Liu, QH Uprety, S Shao, X Bai, Y Weng, FZ AF Cao, Changyong Xiong, Jack Blonski, Slawomir Liu, Quanhua Uprety, Sirish Shao, Xi Bai, Yan Weng, Fuzhong TI Suomi NPP VIIRS sensor data record verification, validation, and long-term performance monitoring SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article AB [1] The successful launch of the Suomi National Polar-orbiting Partnership Satellite on 28 October 2011 with the key instrument Visible Infrared Imaging Radiometer Suite signifies a new era of moderate-resolution imaging capabilities following the legacy of AVHRR and Moderate-Resolution Imaging Spectroradiometer (MODIS). After a year and half of calibration and validation, the Visible Infrared Imaging Radiometer Suite (VIIRS) instrument is performing very well. By early 2013, the sensor data records have achieved provisional maturity status and have been used in the routine production of more than 20 environmental data records by users worldwide. Based on comparisons with MODIS, the VIIRS reflective solar band radiometric uncertainties are now comparable in reflectance to that of MODIS Collection 6 equivalent bands (within 2%) although radiance differences could be larger for several bands, while an agreement on the order of 0.1 K has also been achieved for the thermal emissive bands, except for bands with significant spectral differences or certain bands at extreme temperatures (below 200 K or above 343 K). The degradation in the VIIRS rotating telescope assembly mirrors is gradually leveling off after reaching similar to 30% and thus far has limited impact on instrument performance and products. Environmental data record users are generally satisfied with the VIIRS data quality which meets the product requirements. While the specific technical details are documented in other papers in this special issue and in Cao et al. (2013a), this paper focuses on the major findings of VIIRS calibration and validation since launch, radiometric performance validation, and uncertainties, as well as lessons learned. C1 [Cao, Changyong; Weng, Fuzhong] NOAA, NESDIS, STAR, College Pk, MD USA. [Xiong, Jack] NASA GSFC, Greenbelt, MD USA. [Blonski, Slawomir; Liu, Quanhua; Shao, Xi] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Uprety, Sirish] Colorado State Univ, CIRA, Ft Collins, CO 80523 USA. [Bai, Yan] ERT Inc, College Pk, MD USA. RP Cao, CY (reprint author), 5825 Univ Res Ct,Suite 3250, College Pk, MD 20740 USA. EM Changyong.Cao@noaa.gov RI Weng, Fuzhong/F-5633-2010 OI Weng, Fuzhong/0000-0003-0150-2179 NR 33 TC 57 Z9 59 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD OCT 27 PY 2013 VL 118 IS 20 BP 11664 EP 11678 DI 10.1002/2013JD020418 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA V45WS UT WOS:000209847300015 ER PT J AU Bardeen, CG Gettelman, A Jensen, EJ Heymsfield, A Conley, AJ Delanoe, J Deng, M Toon, OB AF Bardeen, C. G. Gettelman, A. Jensen, E. J. Heymsfield, A. Conley, A. J. Delanoe, J. Deng, M. Toon, O. B. TI Improved cirrus simulations in a general circulation model using CARMA sectional microphysics SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article AB [1] We have developed a new cirrus model incorporating sectional ice microphysics from the Community Aerosol and Radiation Model for Atmospheres (CARMA) in the latest version of NCAR's Community Atmosphere Model (CAM5). Comparisons with DARDAR and 2C-ICE show that CAM5/CARMA improves cloud fraction, ice water content, and ice water path compared to the standard CAM5. Prognostic snow in CAM5/CARMA increases overall ice mass and results in a melting layer at similar to 4 km in the tropics that is largely absent in CAM5. Subgrid scale supersaturation following Wilson and Ballard (1999) improves ice mass and relative humidity. Increased middle and upper tropospheric condensate in CAM5/CARMA requires a reduction in low-level cloud for energy balance, resulting in a 3.1 W m(-2) improvement in shortwave cloud forcing and a 3.8 W m(-2) improvement in downwelling shortwave flux at the surface compared to CAM5 and Clouds and Earth's Radiant Energy Systems (CERES). Total and clear-sky longwave upwelling flux at the top are improved in CAM5/CARMA by 1.0 and 2.6 W m(-2), respectively. CAM has a 2-3K cold bias at the tropical tropopause mostly from the prescribed ozone file. Correction of the prescribed ozone or nudging the CAM5/CARMA model to GEOS5-DAS meteorology yields tropical tropopause temperatures and water vapor that agree with the Constellation Observing System for Meteorology, Ionosphere, and Climate (COSMIC) and the Microwave Limb Sounder (MLS). CAM5 relative humidity appears to be too large resulting in a +1.5 ppmv water vapor bias at the tropical tropopause when using GEOS5-DAS meteorology. In CAM5/CARMA, 75% of the cloud ice mass originates from ice particles detrained from convection compared to 25% from in situ nucleation. C1 [Bardeen, C. G.; Gettelman, A.; Heymsfield, A.; Conley, A. J.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. [Jensen, E. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Delanoe, J.] UVSQ CNRS, IPSL, LATMOS, Guyancourt, France. [Deng, M.] Univ Wyoming, Laramie, WY 82071 USA. [Toon, O. B.] Dept Atmospher & Ocean Sci, Boulder, CO USA. [Toon, O. B.] Lab Atmospher & Space Phys, Boulder, CO USA. RP Bardeen, CG (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. EM bardeenc@ucar.edu FU NCAR ASP Fellowship; NASA [NNX10AO53A, NNX09AK71G]; CNES (Centre National d'Etudes Spatiales); National Science Foundation; Office of Science (BER) of the U.S. Department of Energy FX Portions of this research were supported by an NCAR ASP Fellowship and NASA Grants NNX10AO53A (ATTREX) and NNX09AK71G (MAP). Julien Delanoe's research is partly funded by CNES (Centre National d'Etudes Spatiales). Thank you to the COSMIC, MLS, AIRS, CloudSat, and CALIPSO teams for making their data products available and for assistance in the use of those products. Thanks also to Jeffrey Taylor for making his gridded COSMIC data set available for this work. Computing 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 and by the Climate Simulation Laboratory at NCAR's Computational and Information Systems Laboratory (CISL), sponsored by the National Science Foundation and other agencies. We wish to thank the ICARE Data and Services Center for providing access to the DARDAR data used in this study. The CESM project is supported by the National Science Foundation and the Office of Science (BER) of the U.S. Department of Energy. NCAR is sponsored by the National Science Foundation. NR 69 TC 5 Z9 5 U1 1 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD OCT 27 PY 2013 VL 118 IS 20 BP 11679 EP 11697 DI 10.1002/2013JD020193 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA V45WS UT WOS:000209847300016 ER PT J AU Monteil, G Houweling, S Butz, A Guerlet, S Schepers, D Hasekamp, O Frankenberg, C Scheepmaker, R Aben, I Rockmann, T AF Monteil, Guillaume Houweling, Sander Butz, Andre Guerlet, Sandrine Schepers, Dinand Hasekamp, Otto Frankenberg, Christian Scheepmaker, Remco Aben, Ilse Rockmann, Thomas TI Comparison of CH4 inversions based on 15 months of GOSAT and SCIAMACHY observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article AB [1] Over the past decade the development of Scanning Imaging Absorption Spectrometer for Atmospheric Chartography (SCIAMACHY) retrievals has increased the interest in the use of satellite measurements for studying the global sources and sinks of methane. Meanwhile, measurements are becoming available from the more advanced Greenhouse Gases Observing Satellite (GOSAT). The aim of this study is to investigate the application of GOSAT retrievals to inverse modeling, for which we make use of the TM5-4DVAR inverse modeling framework. Inverse modeling calculations are performed using data from two different retrieval approaches: a full physics and a lightpath proxy ratio method. The performance of these inversions is analyzed in comparison with inversions using SCIAMACHY retrievals and measurements from the National Oceanic and Atmospheric Administration-Earth System Research Laboratory flask-sampling network. In addition, we compare the inversion results against independent surface, aircraft, and total-column measurements. Inversions with GOSAT data show good agreement with surface measurements, whereas for SCIAMACHY a similar performance can only be achieved after significant bias corrections. Some inconsistencies between surface and total-column methane remain in the Southern Hemisphere. However, comparisons with measurements from the Total Column Carbon Observing Network in situ Fourier transform spectrometer network indicate that those may be caused by systematic model errors rather than by shortcomings in the GOSAT retrievals. The global patterns of methane emissions derived from SCIAMACHY (with bias correction) and GOSAT retrievals are in remarkable agreement and allow an increased resolution of tropical emissions. The satellite inversions increase tropical methane emission by 30 to 60 Tg CH4/yr compared to initial a priori estimates, partly counterbalanced by reductions in emissions at midlatitudes to high latitudes. C1 [Monteil, Guillaume; Houweling, Sander; Rockmann, Thomas] Univ Utrecht, Inst Marine & Atmospher Res Utrecht, NL-3584 CC Utrecht, Netherlands. [Monteil, Guillaume; Houweling, Sander; Guerlet, Sandrine; Schepers, Dinand; Hasekamp, Otto; Scheepmaker, Remco; Aben, Ilse] SRON Netherlands Inst Space Res, Utrecht, Netherlands. [Butz, Andre] Karlsruhe Inst Technol, IMK ASF, Eggenstein Leopoldshafen, Germany. [Frankenberg, Christian] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Monteil, G (reprint author), Univ Utrecht, Inst Marine & Atmospher Res Utrecht, NL-3584 CC Utrecht, Netherlands. EM g.monteil@sron.nl RI Butz, Andre/A-7024-2013; Rockmann, Thomas/F-4479-2015; Frankenberg, Christian/A-2944-2013 OI Butz, Andre/0000-0003-0593-1608; Rockmann, Thomas/0000-0002-6688-8968; Frankenberg, Christian/0000-0002-0546-5857 FU Dutch NWO [865.07.007]; ESA's Climate Change Initiative on GHGs; European Commission [218793]; NWO [ALW-GO-AO/21]; Deutsche Forschungsgemeinschaft (DFG) [BU2599/1-1] FX This project was funded by the Dutch NWO under grant 865.07.007. Funding from ESA's Climate Change Initiative on GHGs (Sandrine Guerlet) and the European Commission's 7th framework program under grant agreement 218793 (Sandrine Guerlet and Remco Scheepmaker) is acknowledged. Dinand Schepers is supported by the gebruikersondersteuning ruimteonderzoek program of NWO through project ALW-GO-AO/21. Andre Butz has been supported by Deutsche Forschungsgemeinschaft (DFG) through the Emmy-Noether Programme (grant BU2599/1-1, RemoteC). We thank SURFsara (www.surfsara.nl) for the support in using the Dutch national super computer Huygens. We thank the data providers: Access to the GOSAT data was granted through the 2nd GOSAT research announcement jointly issued by JAVA, NIES, and MOE; surface observations from the NOAA/CMDL network were obtained from the website http://www.esrl.noaa.gov/gmd/dv/iadv; TCCON data were obtained from the TTCON DATA Archive, operated by the California Institute of Technology (http://tccon.ipac.caltech.edu); we thank Steven Wofsy (Harvard University) for providing the HIPPO data used in the paper and for his useful suggestions. NR 73 TC 22 Z9 23 U1 0 U2 24 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 OCT 27 PY 2013 VL 118 IS 20 BP 11807 EP 11823 DI 10.1002/2013JD019760 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA V45WS UT WOS:000209847300026 ER PT J AU Hegglin, MI Tegtmeier, S Anderson, J Froidevaux, L Fuller, R Funke, B Jones, A Lingenfelser, G Lumpe, J Pendlebury, D Remsberg, E Rozanov, A Toohey, M Urban, J von Clarmann, T Walker, KA Wang, R Weigel, K AF Hegglin, M. I. Tegtmeier, S. Anderson, J. Froidevaux, L. Fuller, R. Funke, B. Jones, A. Lingenfelser, G. Lumpe, J. Pendlebury, D. Remsberg, E. Rozanov, A. Toohey, M. Urban, J. von Clarmann, T. Walker, K. A. Wang, R. Weigel, K. TI SPARC Data Initiative: Comparison of water vapor climatologies from international satellite limb sounders SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TROPICAL TROPOPAUSE TEMPERATURES; STRATOSPHERIC WATER; UPPER TROPOSPHERE; TECHNICAL NOTE; BOARD ENVISAT; DATA SET; VALIDATION; RETRIEVAL; AEROSOL; UARS AB [1] Within the SPARC Data Initiative, the first comprehensive assessment of the quality of 13 water vapor products from 11 limb-viewing satellite instruments (LIMS, SAGE II, UARS-MLS, HALOE, POAM III, SMR, SAGE III, MIPAS, SCIAMACHY, ACE-FTS, and Aura-MLS) obtained within the time period 1978-2010 has been performed. Each instrument's water vapor profile measurements were compiled into monthly zonal mean time series on a common latitude-pressure grid. These time series serve as basis for the "climatological" validation approach used within the project. The evaluations include comparisons of monthly or annual zonal mean cross sections and seasonal cycles in the tropical and extratropical upper troposphere and lower stratosphere averaged over one or more years, comparisons of interannual variability, and a study of the time evolution of physical features in water vapor such as the tropical tape recorder and polar vortex dehydration. Our knowledge of the atmospheric mean state in water vapor is best in the lower and middle stratosphere of the tropics and midlatitudes, with a relative uncertainty of +/- 2-6% (as quantified by the standard deviation of the instruments' multiannual means). The uncertainty increases toward the polar regions (+/- 10-15%), the mesosphere (+/- 15%), and the upper troposphere/lower stratosphere below 100 hPa (+/- 30-50%), where sampling issues add uncertainty due to large gradients and high natural variability in water vapor. The minimum found in multiannual (1998-2008) mean water vapor in the tropical lower stratosphere is 3.5 ppmv (+/- 14%), with slightly larger uncertainties for monthly mean values. The frequently used HALOE water vapor data set shows consistently lower values than most other data sets throughout the atmosphere, with increasing deviations from the multi-instrument mean below 100 hPa in both the tropics and extratropics. The knowledge gained from these comparisons and regarding the quality of the individual data sets in different regions of the atmosphere will help to improve model-measurement comparisons (e.g., for diagnostics such as the tropical tape recorder or seasonal cycles), data merging activities, and studies of climate variability. C1 [Hegglin, M. I.] Univ Reading, Dept Meteorol, POB 243, Reading RG6 6BB, Berks, England. [Tegtmeier, S.; Toohey, M.] Helmholtz Ctr Ocean Res Kiel, GEOMAR, Kiel, Germany. [Anderson, J.] Hampton Univ, Dept Atmospher & Planetary Sci, Hampton, VA 23668 USA. [Froidevaux, L.; Fuller, R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Funke, B.] CSIC, Inst Astrofis Andalucia, Granada, Spain. [Jones, A.; Pendlebury, D.; Walker, K. A.] Univ Toronto, Dept Phys, Toronto, ON, Canada. [Lingenfelser, G.; Remsberg, E.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Lumpe, J.] Computat Phys Inc, Boulder, CO USA. [Rozanov, A.; Weigel, K.] Univ Bremen, Inst Environm Phys IUP, Bremen, Germany. [Urban, J.] Chalmers, Dept Earth & Space Sci, Gothenburg, Sweden. [von Clarmann, T.] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, Karlsruhe, Germany. [Wang, R.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. RP Hegglin, MI (reprint author), Univ Reading, Dept Meteorol, POB 243, Reading RG6 6BB, Berks, England. EM m.i.hegglin@reading.ac.uk RI Urban, Jo/F-9172-2010; Funke, Bernd/C-2162-2008; Toohey, Matthew/G-3129-2010; Hegglin, Michaela/D-7528-2017 OI Urban, Jo/0000-0001-7026-793X; Funke, Bernd/0000-0003-0462-4702; Toohey, Matthew/0000-0002-7070-405X; Hegglin, Michaela/0000-0003-2820-9044 FU International Space Science Institute in Bern (ISSI); WCRP; Toronto SPARC office; CSA; ESA; WGL project TransBrom; EU [FP7-ENV-2007-1-226224]; NASA; Canadian Foundation for Climate and Atmospheric Sciences; DFG Research Unit FOR 1095 "Stratospheric Change and its role for Climate Prediction (SHARP)" [GZ WE 3647/3-1]; Sweden (Swedish National SpaceBoard); Canada (CSA); France (Centre National d'tudes Spatiales); Finland (Tekes); National Oceanic and Atmospheric Administration's Educational Partnership Program Cooperative Remote Sensing Science and Technology Center (NOAA EPP CREST) FX The climatology comparisons presented in this study resulted from an activity within the World Climate Research Programme's (WCRP's) Stratospheric Processes and their Role in Climate project-the SPARC Data Initiative. We thank in particular the instrument teams and the various space agencies (CSA, ESA, NASA, and other national agencies) for providing their data and manpower. The SPARC Data Initiative thanks the International Space Science Institute in Bern (ISSI), which supported the activity through their ISSI International Team activity program, and the WCRP and the Toronto SPARC office for generous travel funds. M.I.H. thanks the CSA and ESA for supporting her work for the SPARC Data Initiative. The work from S.T. was funded from the WGL project TransBrom and the EU project SHIVA (FP7-ENV-2007-1-226224). Work at the Jet Propulsion Laboratory, California Institute of Technology, was performed under contract with NASA. The Atmospheric Chemistry Experiment (ACE), also known as SCISAT, is a Canadian-led mission mainly supported by the CSA. Development of the ACE-FTS climatologies was supported by grants from the Canadian Foundation for Climate and Atmospheric Sciences and the CSA. Work on the SCIAMACHY water vapor at the University of Bremen was supported by the DFG Research Unit FOR 1095 "Stratospheric Change and its role for Climate Prediction (SHARP)" (project GZ WE 3647/3-1). Odin is a Swedish-led satellite project funded jointly by Sweden (Swedish National SpaceBoard), Canada (CSA), France (Centre National d'tudes Spatiales), and Finland (Tekes), with support by the third party mission program of ESA. The work from Hampton University was partially funded under the National Oceanic and Atmospheric Administration's Educational Partnership Program Cooperative Remote Sensing Science and Technology Center (NOAA EPP CREST). NR 59 TC 31 Z9 31 U1 1 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 OCT 27 PY 2013 VL 118 IS 20 BP 11824 EP 11846 DI 10.1002/jgrd.50752 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA V45WS UT WOS:000209847300027 ER PT J AU Toohey, M Hegglin, MI Tegtmeier, S Anderson, J Anel, JA Bourassa, A Brohede, S Degenstein, D Froidevaux, L Fuller, R Funke, B Gille, J Jones, A Kasai, Y Kruger, K Kyrola, E Neu, JL Rozanov, A Smith, L Urban, J von Clarmann, T Walker, KA Wang, RHJ AF Toohey, M. Hegglin, M. I. Tegtmeier, S. Anderson, J. Anel, J. A. Bourassa, A. Brohede, S. Degenstein, D. Froidevaux, L. Fuller, R. Funke, B. Gille, J. Jones, A. Kasai, Y. Krueger, K. Kyrola, E. Neu, J. L. Rozanov, A. Smith, L. Urban, J. von Clarmann, T. Walker, K. A. Wang, R. H. J. TI Characterizing sampling biases in the trace gas climatologies of the SPARC Data Initiative SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article AB [1] Monthly zonal mean climatologies of atmospheric measurements from satellite instruments can have biases due to the nonuniform sampling of the atmosphere by the instruments. We characterize potential sampling biases in stratospheric trace gas climatologies of the Stratospheric Processes and Their Role in Climate (SPARC) Data Initiative using chemical fields from a chemistry climate model simulation and sampling patterns from 16 satellite-borne instruments. The exercise is performed for the long-lived stratospheric trace gases O-3 and H2O. Monthly sampling biases for O-3 exceed 10% for many instruments in the high-latitude stratosphere and in the upper troposphere/lower stratosphere, while annual mean sampling biases reach values of up to 20% in the same regions for some instruments. Sampling biases for H2O are generally smaller than for O-3, although still notable in the upper troposphere/lower stratosphere and Southern Hemisphere high latitudes. The most important mechanism leading to monthly sampling bias is nonuniform temporal sampling, i.e., the fact that for many instruments, monthly means are produced from measurements which span less than the full month in question. Similarly, annual mean sampling biases are well explained by nonuniformity in the month-to-month sampling by different instruments. Nonuniform sampling in latitude and longitude are shown to also lead to nonnegligible sampling biases, which are most relevant for climatologies which are otherwise free of biases due to nonuniform temporal sampling. C1 [Toohey, M.; Tegtmeier, S.] GEOMAR Helmholtz Ctr Ocean Res Kiel, Dusternbrooker Weg 20, D-24105 Kiel, Germany. [Hegglin, M. I.] Univ Reading, Dept Meteorol, Reading, Berks, England. [Anderson, J.] Hampton Univ, Atmospher Sci, Hampton, VA 23668 USA. [Anel, J. A.] Univ Oxford, Smith Sch Enterprise & Environm, Oxford, England. [Anel, J. A.] Univ Vigo, EPhysLab, Orense, Spain. [Bourassa, A.; Degenstein, D.] Univ Saskatchewan, Inst Space & Atmospher Studies, Saskatoon, SK, Canada. [Brohede, S.; Urban, J.] Chalmers, Dept Earth & Space Sci, Gothenburg, Sweden. [Froidevaux, L.; Fuller, R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Funke, B.] Inst Astrofis Andalucia, Granada, Spain. [Gille, J.; Smith, L.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Gille, J.] Univ Colorado Boulder, Ctr Limb Atmospher Sounding, Boulder, CO USA. [Jones, A.; Walker, K. A.] Univ Toronto, Dept Phys, Toronto, ON, Canada. [Kasai, Y.] Natl Inst Informat & Commun Technol, Koganei, Tokyo, Japan. [Kyrola, E.] Finnish Meteorol Inst, Helsinki, Finland. [Rozanov, A.] Univ Bremen, Inst Environm Phys IUP, Bremen, Germany. [von Clarmann, T.] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, Karlsruhe, Germany. [Wang, R. H. J.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. RP Toohey, M (reprint author), GEOMAR Helmholtz Ctr Ocean Res Kiel, Dusternbrooker Weg 20, D-24105 Kiel, Germany. EM mtoohey@geomar.de RI Urban, Jo/F-9172-2010; Funke, Bernd/C-2162-2008; Toohey, Matthew/G-3129-2010; Hegglin, Michaela/D-7528-2017 OI Urban, Jo/0000-0001-7026-793X; Funke, Bernd/0000-0003-0462-4702; Toohey, Matthew/0000-0002-7070-405X; Hegglin, Michaela/0000-0003-2820-9044 FU International Space Science Institute in Bern (ISSI); World Climate Research Programme; Toronto SPARC office; BMBF MIKLIP project ALARM [01LP1130B]; Canadian Space Agency (CSA); European Space Agency; WGL project TransBrom; EU [FP7-ENV-2007-1-226224]; National Oceanic and Atmospheric Administration's Educational Partnership Program Cooperative Remote Sensing Science and Technology Center (NOAA EPP CREST); National Aeronautics and Space Administration; CSA; Canadian Foundation for Climate and Atmospheric Sciences; Swedish National Space Board (SNSB); National Technology Agency of Finland (Tekes); Centre National d'Etudes Spatiales (CNES) in France; ESA; Academy of Finland [134325]; NASA's EOS Program in the U.S.; UK by NERC; Spanish MINECO [AYA2011-23552]; EC FEDER funds; German Aerospace Agency (DLR) [50EE1105]; DFG Research Unit FOR 1095 "Stratospheric Change and its role for Climate Prediction (SHARP)" [GZ WE 3647/3-1]; State of Bremen; University of Bremen FX The SPARC Data Initiative thanks the International Space Science Institute in Bern (ISSI) who supported the activity through their ISSI International Team activity program, and the World Climate Research Programme and the Toronto SPARC office for generous travel funds. The work by Matthew Toohey is supported by the BMBF MIKLIP project ALARM through the grant 01LP1130B. Michaela Hegglin thanks the Canadian Space Agency (CSA) and the European Space Agency for supporting her work for the SPARC Data Initiative. The work from Susann Tegtmeier was funded from the WGL project TransBrom and the EU project SHIVA (FP7-ENV-2007-1-226224). The work from Hampton University was partially funded under the National Oceanic and Atmospheric Administration's Educational Partnership Program Cooperative Remote Sensing Science and Technology Center (NOAA EPP CREST). Work at the Jet Propulsion Laboratory, California Institute of Technology, was performed under contract with the National Aeronautics and Space Administration. ACE is a Canadian-led mission mainly supported by the CSA. Development of the ACE-FTS climatologies was supported by grants from the Canadian Foundation for Climate and Atmospheric Sciences and the CSA. Odin is a Swedish-led satellite project funded jointly by the Swedish National Space Board (SNSB), the CSA, the National Technology Agency of Finland (Tekes), the Centre National d'Etudes Spatiales (CNES) in France, and the Third Party Mission program of ESA. The work of E. Kyrola was supported by the Academy of Finland through the project MIDAT (134325). Work on HIRDLS was supported by NASA's EOS Program in the U.S. and in the UK by NERC. IAA was supported by the Spanish MINECO under grant AYA2011-23552 and EC FEDER funds. The work of the University of Bremen team on SCIAMACHY climatologies was funded in part by the German Aerospace Agency (DLR) within the project SADOS (50EE1105), by the DFG Research Unit FOR 1095 "Stratospheric Change and its role for Climate Prediction (SHARP)" (project GZ WE 3647/3-1), and by the State and University of Bremen. WACCM simulations were performed in the Centro de Supercomputacion de Galicia under a Reto2009 Project, and the authors thank Rolando Garcia, who developed the WACCM model version used here, and Andrew Gettelman for guidance with the model. Finally, the authors thank Ted Shepherd, Peter Braesicke, and Karen Rosenlof for helpful feedback on early results from this work, and two anonymous reviewers who provided valuable comments on the submitted manuscript. NR 37 TC 21 Z9 21 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 OCT 27 PY 2013 VL 118 IS 20 BP 11847 EP 11862 DI 10.1002/jgrd.50874 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA V45WS UT WOS:000209847300028 ER PT J AU Saw, JHW Schatz, M Brown, MV Kunkel, DD Foster, JS Shick, H Christensen, S Hou, SB Wan, XH Donachie, SP AF Saw, Jimmy H. W. Schatz, Michael Brown, Mark V. Kunkel, Dennis D. Foster, Jamie S. Shick, Harry Christensen, Stephanie Hou, Shaobin Wan, Xuehua Donachie, Stuart P. TI Cultivation and Complete Genome Sequencing of Gloeobacter kilaueensis sp nov., from a Lava Cave in Kilauea Caldera, Hawai'i SO PLOS ONE LA English DT Article ID DNA-DNA HYBRIDIZATION; CAROTENOID BIOSYNTHESIS; OXYGENIC PHOTOSYNTHESIS; VANCOMYCIN RESISTANCE; PHYLOGENETIC ANALYSES; PHYTOENE DESATURASE; VIOLACEUS PCC-7421; SPECIES DEFINITION; LACKS THYLAKOIDS; CYANOBACTERIUM AB The ancestor of Gloeobacter violaceus PCC 7421(T) is believed to have diverged from that of all known cyanobacteria before the evolution of thylakoid membranes and plant plastids. The long and largely independent evolutionary history of G. violaceus presents an organism retaining ancestral features of early oxygenic photoautotrophs, and in whom cyanobacteria evolution can be investigated. No other Gloeobacter species has been described since the genus was established in 1974 (Rippka et al., Arch Microbiol 100:435). Gloeobacter affiliated ribosomal gene sequences have been reported in environmental DNA libraries, but only the type strain's genome has been sequenced. However, we report here the cultivation of a new Gloeobacter species, G. kilaueensis JS1(T), from an epilithic biofilm in a lava cave in Kilauea Caldera, Hawai'i. The strain's genome was sequenced from an enriched culture resembling a low-complexity metagenomic sample, using 9 kb paired-end 454 pyrosequences and 400 bp paired-end Illumina reads. The JS1(T) and G. violaceus PCC 7421(T) genomes have little gene synteny despite sharing 2842 orthologous genes; comparing the genomes shows they do not belong to the same species. Our results support establishing a new species to accommodate JS1(T), for which we propose the name Gloeobacter kilaueensis sp. nov. Strain JS1(T) has been deposited in the American Type Culture Collection (BAA-2537), the Scottish Marine Institute's Culture Collection of Algae and Protozoa (CCAP 1431/1), and the Belgian Coordinated Collections of Microorganisms (ULC0316). The G. kilaueensis holotype has been deposited in the Algal Collection of the US National Herbarium (US# 217948). The JS1(T) genome sequence has been deposited in GenBank under accession number CP003587. The G+C content of the genome is 60.54 mol%. The complete genome sequence of G. kilaueensis JS1(T) may further understanding of cyanobacteria evolution, and the shift from anoxygenic to oxygenic photosynthesis. C1 [Saw, Jimmy H. W.; Hou, Shaobin; Wan, Xuehua; Donachie, Stuart P.] Univ Hawaii Manoa, Dept Microbiol, Honolulu, HI 96822 USA. [Schatz, Michael] Cold Spring Harbor Lab, Cold Spring Harbor, NY 11724 USA. [Brown, Mark V.] Univ Hawaii, NASA Astrobiol Inst, Honolulu, HI 96822 USA. [Brown, Mark V.] Univ New S Wales, Sch Biotechnol & Biomol Sci, Sydney, NSW, Australia. [Kunkel, Dennis D.] Dennis Kunkel Microscopy Inc, Kailua, HI USA. [Foster, Jamie S.] Univ Florida, Space Life Sci Lab, Dept Microbiol & Cell Sci, Kennedy Space Ctr, Kennedy, FL USA. [Christensen, Stephanie] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Dept Oceanog, Honolulu, HI 96822 USA. [Hou, Shaobin; Wan, Xuehua] Univ Hawaii Manoa, Honolulu, HI 96822 USA. RP Donachie, SP (reprint author), Univ Hawaii Manoa, Dept Microbiol, Honolulu, HI 96822 USA. EM donachie@hawaii.edu RI Saw, Jimmy/A-9972-2009; Wan, Xuehua/D-5433-2016; OI Saw, Jimmy/0000-0001-8353-3854; Wan, Xuehua/0000-0002-6367-848X; Hou, Shaobin/0000-0003-3467-8242 FU College of Natural Sciences; EPSCoR REAP award through NSF [0554657]; Lewis and Clark Fund for Exploration and Field Research in Astrobiology FX Early investigations of the epilithic biofilm were supported by start-up funds to SPD from the Dean of the College of Natural Sciences, and by an EPSCoR REAP award to SPD, MVB, Gernot Presting and John M. Berestecky through NSF #0554657 IMUA 2: NSF Hawaii EPSCoR to James Gaines (PI), Kenneth Kaneshiro (Co-PI), and Donald Price (co-PI). Fieldwork was supported by a grant from The Lewis and Clark Fund for Exploration and Field Research in Astrobiology to JHWS. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 56 TC 17 Z9 19 U1 8 U2 43 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 OCT 23 PY 2013 VL 8 IS 10 AR e76376 DI 10.1371/journal.pone.0076376 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 239PE UT WOS:000326037000015 PM 24194836 ER PT J AU Ackermann, M Ajello, M Albert, A Allafort, A Baldini, L Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Bissaldi, E Bloom, ED Bonamente, E Bottacini, E Brandt, TJ Bregeon, J Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Casandjian, JM Cecchi, C Charles, E Chaves, RCG Chekhtman, A Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Cutini, S D'Ammando, F de Angelis, A de Palma, F Dermer, CD Digel, SW Di Venere, L Drell, PS Drlica-Wagner, A Essig, R Favuzzi, C Fegan, SJ Ferrara, EC Focke, WB Franckowiak, A Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Germani, S Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Gomez-Vargas, GA Grenier, IA Guiriec, S Gustafsson, M Hadasch, D Hayashida, M Hill, AB Horan, D Hou, X Hughes, RE Inoue, Y Izaguirre, E Jogler, T Kamae, T Knodlseder, J Kuss, M Lande, J Larsson, S Latronico, L Longo, F Loparco, F Lovellette, MN Lubrano, P Malyshev, D Mayer, M Mazziotta, MN McEnery, JE Michelson, PF Mitthumsiri, W Mizuno, T Moiseev, AA Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nakamori, T Nemmen, R Nuss, E Ohsugi, T Okumura, A Omodei, N Orienti, M Orlando, E Ormes, JF Paneque, D Perkins, JS Pesce-Rollins, M Piron, F Pivato, G Raino, S Rando, R Razzano, M Razzaque, S Reimer, A Reimer, O Romani, RW Sanchez-Conde, M Schulz, A Sgro, C Siegal-Gaskins, J Siskind, EJ Snyder, A Spandre, G Spinelli, P Suson, DJ Tajima, H Takahashi, H Thayer, JG Thayer, JB Tibaldo, L Tinivella, M Tosti, G Troja, E Uchiyama, Y Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Winer, BL Wood, KS Wood, M Yang, Z Zaharijas, G Zimmer, S AF Ackermann, M. Ajello, M. Albert, A. Allafort, A. Baldini, L. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Bissaldi, E. Bloom, E. D. Bonamente, E. Bottacini, E. Brandt, T. J. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Casandjian, J. M. Cecchi, C. Charles, E. Chaves, R. C. G. Chekhtman, A. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Cutini, S. D'Ammando, F. de Angelis, A. de Palma, F. Dermer, C. D. Digel, S. W. Di Venere, L. Drell, P. S. Drlica-Wagner, A. Essig, R. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Focke, W. B. Franckowiak, A. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Gomez-Vargas, G. A. Grenier, I. A. Guiriec, S. Gustafsson, M. Hadasch, D. Hayashida, M. Hill, A. B. Horan, D. Hou, X. Hughes, R. E. Inoue, Y. Izaguirre, E. Jogler, T. Kamae, T. Knoedlseder, J. Kuss, M. Lande, J. Larsson, S. Latronico, L. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Malyshev, D. Mayer, M. Mazziotta, M. N. McEnery, J. E. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nakamori, T. Nemmen, R. Nuss, E. Ohsugi, T. Okumura, A. Omodei, N. Orienti, M. Orlando, E. Ormes, J. F. Paneque, D. Perkins, J. S. Pesce-Rollins, M. Piron, F. Pivato, G. Raino, S. Rando, R. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Romani, R. W. Sanchez-Conde, M. Schulz, A. Sgro, C. Siegal-Gaskins, J. Siskind, E. J. Snyder, A. Spandre, G. Spinelli, P. Suson, D. J. Tajima, H. Takahashi, H. Thayer, J. G. Thayer, J. B. Tibaldo, L. Tinivella, M. Tosti, G. Troja, E. Uchiyama, Y. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Winer, B. L. Wood, K. S. Wood, M. Yang, Z. Zaharijas, G. Zimmer, S. TI Search for gamma-ray spectral lines with the Fermi Large Area Telescope and dark matter implications SO PHYSICAL REVIEW D LA English DT Article ID GALAXY AB Weakly interacting massive particles (WIMPs) are a theoretical class of particles that are excellent dark matter candidates. WIMP annihilation or decay may produce essentially monochromatic gamma rays detectable by the Fermi Large Area Telescope (LAT) against the astrophysical gamma-ray emission of the Galaxy. We have searched for spectral lines in the energy range 5-300 GeV using 3.7 years of data, reprocessed with updated instrument calibrations and an improved energy dispersion model compared to the previous Fermi-LAT Collaboration line searches. We searched in five regions selected to optimize sensitivity to different theoretically motivated dark matter density distributions. We did not find any globally significant lines in our a priori search regions and present 95% confidence limits for annihilation cross sections of self-conjugate WIMPs and decay lifetimes. Our most significant fit occurred at 133 GeV in our smallest search region and had a local significance of 3.3 standard deviations, which translates to a global significance of 1.5 standard deviations. We discuss potential systematic effects in this search, and examine the feature at 133 GeV in detail. We find that the use both of reprocessed data and of additional C1 [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Albert, A.; Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA. [Allafort, A.; Bechtol, K.; Bloom, E. D.; Bottacini, E.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Di Venere, L.; Drell, P. S.; Drlica-Wagner, A.; Essig, R.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Hill, A. B.; Inoue, Y.; Izaguirre, E.; Jogler, T.; Kamae, T.; Lande, J.; Malyshev, D.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Reimer, A.; Reimer, O.; Romani, R. W.; Sanchez-Conde, M.; Snyder, A.; Tajima, H.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, W W Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Allafort, A.; Bechtol, K.; Bloom, E. D.; Bottacini, E.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Di Venere, L.; Drell, P. S.; Drlica-Wagner, A.; Essig, R.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Hill, A. B.; Inoue, Y.; Izaguirre, E.; Jogler, T.; Kamae, T.; Lande, J.; Malyshev, D.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Reimer, A.; Reimer, O.; Romani, R. W.; Sanchez-Conde, M.; Snyder, A.; Tajima, H.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Baldini, L.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.] Ist Nazl Fis Nucl, I-56127 Pisa, Italy. [Barbiellini, G.; Longo, F.; Zaharijas, G.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Pivato, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Bissaldi, E.; Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Bissaldi, E.; Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perigue, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brandt, T. J.; Ferrara, E. C.; Guiriec, S.; McEnery, J. E.; Moiseev, A. A.; Nemmen, R.; Perkins, J. S.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] M Merlin Univ Politecn Bari, Dipartimento Fis, I-70126 Bari, Italy. [Brigida, 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. [Bruel, P.; Fegan, S. J.; Horan, D.] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France. [Caliandro, G. A.; Hadasch, D.] Inst Ciencies Espai, IEEE CSIC, Barcelona 08193, Spain. [Caraveo, P. A.] INAF, Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Casandjian, J. M.; Chaves, R. C. G.; Grenier, I. A.] Univ Paris Diderot, CEA IRFU CNRS, Lab AIM, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Chekhtman, A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Ciprini, S.; Cutini, S.; Gasparrini, D.] ASI, Sci Data Ctr, I-00044 Rome, Italy. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Rome, Italy. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univ & Particules Montpellier, F-34095 Montpellier, France. [Conrad, J.; Larsson, S.; Yang, Z.; Zimmer, S.] Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden. [Conrad, J.; Larsson, S.; Yang, Z.; Zimmer, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden. CNR, Ist Radioastron, INAF, I-40129 Bologna, Italy. [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.] Ist Nazl Fis Nucl, Grup Collegato Udine, Sez Trieste, I-33100 Udine, Italy. [Dermer, C. D.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Fukazawa, Y.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Gomez-Vargas, G. A.; Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Gomez-Vargas, G. A.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain. [Gomez-Vargas, G. A.] Univ Autonoma Madrid, Inst Fis Teor, IFT UAM CSIC, E-28049 Madrid, Spain. [Gustafsson, M.] Univ Libre Bruxelles, Serv Phys Theor, B-1050 Brussels, Belgium. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hou, X.] CEN Bordeaux Gradignan, Univ Bordeaux 1, IN2P3 CNRS, F-33175 Gradignan, France. [Knoedlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [Moiseev, A. A.; Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA. [Okumura, A.; Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Perkins, J. S.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. [Perkins, J. S.] Univ Maryland, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Razzano, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Razzano, M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Razzano, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Razzaque, S.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa. [Siegal-Gaskins, J.] CALTECH, Pasadena, CA 91125 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, New York, NY 11560 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 I- Roma, Italy. [Zaharijas, G.] Abdus Salaam Int Ctr Theoret Phys, I-34151 Trieste, Italy. RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. EM albert.143@osu.edu; elliott@slac.stanford.edu; echarles@slac.stanford.edu; winer@mps.ohio-state.edu RI Bissaldi, Elisabetta/K-7911-2016; Orlando, E/R-5594-2016; Rando, Riccardo/M-7179-2013; Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Funk, Stefan/B-7629-2015; Gomez-Vargas, German/C-7138-2015; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016; Di Venere, Leonardo/C-7619-2017; OI Bissaldi, Elisabetta/0000-0001-9935-8106; Reimer, Olaf/0000-0001-6953-1385; Morselli, Aldo/0000-0002-7704-9553; Funk, Stefan/0000-0002-2012-0080; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; Di Venere, Leonardo/0000-0003-0703-824X; Inoue, Yoshiyuki/0000-0002-7272-1136; De Angelis, Alessandro/0000-0002-3288-2517; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; Zaharijas, Gabrijela/0000-0001-8484-7791; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; Hill, Adam/0000-0003-3470-4834; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726 FU K. A. Wallenberg Foundation; Marie Curie IOF [275861] FX The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK), and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council, and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. We would also like to thank Christoph Weniger for providing the limit values used in Fig. 10. J. Conrad is a Royal Swedish Academy of Sciences Research Fellow, funded by a grant from the K. A. Wallenberg Foundation. A. B. Hill was funded by a Marie Curie IOF, FP7/2007-2013 under Grant No. 275861. E. Troja is a NASA Postdoctoral Program Fellow. NR 44 TC 109 Z9 109 U1 4 U2 13 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 OCT 22 PY 2013 VL 88 IS 8 AR 082002 DI 10.1103/PhysRevD.88.082002 PG 34 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 240OU UT WOS:000326107300001 ER PT J AU Santer, BD Painter, JF Bonfils, C Mears, CA Solomon, S Wigley, TML Gleckler, PJ Schmidt, GA Doutriaux, C Gillett, NP Taylor, KE Thorne, PW Wentz, FJ AF Santer, Benjamin D. Painter, Jeffrey F. Bonfils, Celine Mears, Carl A. Solomon, Susan Wigley, Tom M. L. Gleckler, Peter J. Schmidt, Gavin A. Doutriaux, Charles Gillett, Nathan P. Taylor, Karl E. Thorne, Peter W. Wentz, Frank J. TI Human and natural influences on the changing thermal structure of the atmosphere SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE climate change detection; climate modeling ID STRATOSPHERIC TEMPERATURE TRENDS; CLIMATE-CHANGE; ATTRIBUTION; SIMULATIONS; OZONE AB Since the late 1970s, satellite-based instruments have monitored global changes in atmospheric temperature. These measurements reveal multidecadal tropospheric warming and stratospheric cooling, punctuated by short-term volcanic signals of reverse sign. Similar long-and short-term temperature signals occur in model simulations driven by human-caused changes in atmospheric composition and natural variations in volcanic aerosols. Most previous comparisons of modeled and observed atmospheric temperature changes have used results from individual models and individual observational records. In contrast, we rely on a large multimodel archive and multiple observational datasets. We show that a human-caused latitude/altitude pattern of atmospheric temperature change can be identified with high statistical confidence in satellite data. Results are robust to current uncertainties in models and observations. Virtually all previous research in this area has attempted to discriminate an anthropogenic signal from internal variability. Here, we present evidence that a human-caused signal can also be identified relative to the larger "total" natural variability arising from sources internal to the climate system, solar irradiance changes, and volcanic forcing. Consistent signal identification occurs because both internal and total natural variability (as simulated by state-of-the-art models) cannot produce sustained global-scale tropospheric warming and stratospheric cooling. Our results provide clear evidence for a discernible human influence on the thermal structure of the atmosphere. C1 [Santer, Benjamin D.; Painter, Jeffrey F.; Bonfils, Celine; Gleckler, Peter J.; Doutriaux, Charles; Taylor, Karl E.] Lawrence Livermore Natl Lab, Program Climate Model Diag & Intercomparison, Livermore, CA 94550 USA. [Mears, Carl A.; Wentz, Frank J.] Remote Sensing Syst, Santa Rosa, CA 95401 USA. [Solomon, Susan] MIT, Cambridge, MA 02139 USA. [Wigley, Tom M. L.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Wigley, Tom M. L.] Univ Adelaide, Sch Earth & Environm Sci, Adelaide, SA 5005, Australia. [Schmidt, Gavin A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Gillett, Nathan P.] Environm Canada, Canadian Ctr Climate Modelling & Anal, Victoria, BC V8W 2Y2, Canada. [Thorne, Peter W.] Nansen Environm & Remote Sensing Ctr, N-5006 Bergen, Norway. RP Santer, BD (reprint author), Lawrence Livermore Natl Lab, Program Climate Model Diag & Intercomparison, Livermore, CA 94550 USA. EM santer1@llnl.gov RI Santer, Benjamin/F-9781-2011; Schmidt, Gavin/D-4427-2012; Taylor, Karl/F-7290-2011; Gleckler, Peter/H-4762-2012; Thorne, Peter/F-2225-2014 OI Schmidt, Gavin/0000-0002-2258-0486; Taylor, Karl/0000-0002-6491-2135; Gleckler, Peter/0000-0003-2816-6224; Thorne, Peter/0000-0003-0485-9798 FU DOE [DE-AC52-07NA27344]; DOE/Office of Biological and Environmental Research (OBER) Early Career Research Program Award [SCW1295]; DOE/OBER [DE-AC52-07NA27344] 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 (listed in SI Appendix, Table S1) for producing and making available their model output. For CMIP, the Department of Energy (DOE) Program for Climate Model Diagnosis and Intercomparison (PCMDI) provides coordinating support and led development of software infrastructure in partnership with the Global Organization for Earth System Science Portals. Helpful comments and advice were provided by Jim Boyle (PCMDI), Kerry Emanuel (Massachusetts Institute of Technology), and Mike MacCracken. At Lawrence Livermore National Laboratory, work by B. D. S., J.F.P., P.J.G., and K. E. T. was performed under the auspices of the DOE under Contract DE-AC52-07NA27344; C. B. was supported by the DOE/Office of Biological and Environmental Research (OBER) Early Career Research Program Award SCW1295; and C. D. was funded under DOE/OBER Contract DE-AC52-07NA27344. NR 36 TC 18 Z9 19 U1 8 U2 61 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 OCT 22 PY 2013 VL 110 IS 43 BP 17235 EP 17240 DI 10.1073/pnas.1305332110 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 238JU UT WOS:000325943300027 PM 24043789 ER PT J AU Bahadori, AA Sato, T Slaba, TC Shavers, MR Semones, EJ Van Baalen, M Bolch, WE AF Bahadori, Amir A. Sato, Tatsuhiko Slaba, Tony C. Shavers, Mark R. Semones, Edward J. Van Baalen, Mary Bolch, Wesley E. TI A comparative study of space radiation organ doses and associated cancer risks using PHITS and HZETRN SO PHYSICS IN MEDICINE AND BIOLOGY LA English DT Article ID ACCURATE UNIVERSAL PARAMETERIZATION; ABSORPTION CROSS-SECTIONS; TRANSPORT CODE SYSTEM; 95TH PERCENTILE MALE; FEMALE ASTRONAUTS; BENCHMARKING; PARTICLE; PHANTOMS; 50TH; 5TH AB NASA currently uses one-dimensional deterministic transport to generate values of the organ dose equivalent needed to calculate stochastic radiation risk following crew space exposures. In this study, organ absorbed doses and dose equivalents are calculated for 50th percentile male and female astronaut phantoms using both the NASA High Charge and Energy Transport Code to perform one-dimensional deterministic transport and the Particle and Heavy Ion Transport Code System to perform three-dimensional Monte Carlo transport. Two measures of radiation risk, effective dose and risk of exposure-induced death (REID) are calculated using the organ dose equivalents resulting from the two methods of radiation transport. For the space radiation environments and simplified shielding configurations considered, small differences (<8%) in the effective dose and REID are found. However, for the galactic cosmic ray (GCR) boundary condition, compensating errors are observed, indicating that comparisons between the integral measurements of complex radiation environments and code calculations can be misleading. Code-to-code benchmarks allow for the comparison of differential quantities, such as secondary particle differential fluence, to provide insight into differences observed in integral quantities for particular components of the GCR spectrum. C1 [Bahadori, Amir A.; Bolch, Wesley E.] Univ Florida, Gainesville, FL 32611 USA. [Bahadori, Amir A.; Semones, Edward J.; Van Baalen, Mary] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Sato, Tatsuhiko] Japan Atom Energy Agcy, Tokai, Ibaraki, Japan. [Slaba, Tony C.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Shavers, Mark R.] Wyle Integrated Sci & Engn, Houston, TX 77058 USA. RP Bahadori, AA (reprint author), Univ Florida, Gainesville, FL 32611 USA. EM amir.a.bahadori@nasa.gov RI Sato, Tatsuhiko/G-5964-2012 OI Sato, Tatsuhiko/0000-0001-9902-7083 FU NASA GSRP [NNX09AK14H]; NASA [NAS9-02078] FX The authors thank Dr Patrick O'Neill for providing the Badhwar-O'Neill 2010 GCR model. The authors would also like to thank Dr David Pawel at the US EPA for providing guidance on calculating REID using the EPA radiogenic cancer risk model. This work was supported by NASA GSRP grant NNX09AK14H and NASA Bioastronautics Contract NAS9-02078. NR 48 TC 2 Z9 2 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0031-9155 J9 PHYS MED BIOL JI Phys. Med. Biol. PD OCT 21 PY 2013 VL 58 IS 20 BP 7183 EP 7207 DI 10.1088/0031-9155/58/20/7183 PG 25 WC Engineering, Biomedical; Radiology, Nuclear Medicine & Medical Imaging SC Engineering; Radiology, Nuclear Medicine & Medical Imaging GA 228FY UT WOS:000325172500011 PM 24061091 ER PT J AU Abbas, MM LeClair, A Woodard, E Young, M Stanbro, M Flasar, FM Kunde, VG Achterberg, RK Bjoraker, G Brasunas, J Jennings, DE AF Abbas, M. M. LeClair, A. Woodard, E. Young, M. Stanbro, M. Flasar, F. M. Kunde, V. G. Achterberg, R. K. Bjoraker, G. Brasunas, J. Jennings, D. E. CA Cassini CIRS Team TI DISTRIBUTION OF CO2 IN SATURN'S ATMOSPHERE FROM CASSINI/CIRS INFRARED OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; interplanetary medium; planets and satellites: atmospheres; planets and satellites: composition ID GIANT PLANETS; ICE MIXTURES; SOLID CO; INTERSTELLAR ICES; TITANS ATMOSPHERE; SWS OBSERVATIONS; ISO OBSERVATIONS; BAND STRENGTHS; SPECTROMETER; H2O AB This paper focuses on the CO2 distribution in Saturn's atmosphere based on analysis of infrared spectral observations of Saturn made by the Composite Infrared Spectrometer aboard the Cassini spacecraft. The Cassini spacecraft was launched in 1997 October, inserted in Saturn's orbit in 2004 July, and has been successfully making infrared observations of Saturn, its rings, Titan, and other icy satellites during well-planned orbital tours. The infrared observations, made with a dual Fourier transform spectrometer in both nadir-and limb-viewing modes, cover spectral regions of 10-1400 cm(-1), with the option of variable apodized spectral resolutions from 0.53 to 15 cm(-1). An analysis of the observed spectra with well-developed radiative transfer models and spectral inversion techniques has the potential to provide knowledge of Saturn's thermal structure and composition with global distributions of a series of gases. In this paper, we present an analysis of a large observational data set for retrieval of Saturn's CO2 distribution utilizing spectral features of CO2 in the Q-branch of the nu(2) band, and discuss its possible relationship to the influx of interstellar dust grains. With limited spectral regions available for analysis, due to low densities of CO2 and interference from other gases, the retrieved CO2 profile is obtained as a function of a model photochemical profile, with the retrieved values at atmospheric pressures in the region of similar to 1-10 mbar levels. The retrieved CO2 profile is found to be in good agreement with the model profile based on Infrared Space Observatory measurements with mixing ratios of similar to 4.9 x 10(-10) at atmospheric pressures of similar to 1 mbar. C1 [Abbas, M. M.; LeClair, A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Woodard, E.; Young, M.; Stanbro, M.] Univ Alabama, Huntsville, AL 35899 USA. [Flasar, F. M.; Achterberg, R. K.; Bjoraker, G.; Brasunas, J.; Jennings, D. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kunde, V. G.] Univ Maryland, College Pk, MD 20742 USA. RP Abbas, MM (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM Mian.M.Abbas@nasa.gov; Andre.C.LeClair@nasa.gov; eaw0009@uah.edu; youngmm@uah.edu; mcs0001@uah.edu; f.m.flasar@nasa.gov; virgil.g.kunde@gsfc.nasa.gov RI Flasar, F Michael/C-8509-2012 NR 49 TC 0 Z9 0 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2013 VL 776 IS 2 AR 73 DI 10.1088/0004-637X/776/2/73 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 255CF UT WOS:000327216100010 ER PT J AU Archambault, S Arlen, T Aune, T Behera, B Beilicke, M Benbow, W Bird, R Bouvier, A Buckley, JH Bugaev, V Byrum, K Cesarini, A Ciupik, L Connolly, MP Cui, W Errando, M Falcone, A Federici, S Feng, Q Finley, JP Fortson, L Furniss, A Galante, N Gall, D Gillanders, GH Griffin, S Grube, J Gyuk, G Hanna, D Holder, J Hughes, G Humensky, TB Kaaret, P Kertzman, M Khassen, Y Kieda, D Krawczynski, H Krennrich, F Kumar, S Lang, MJ Madhavan, AS Maier, G Majumdar, P McArthur, S McCann, A Millis, J Moriarty, P Mukherjee, R de Bhroithe, AO Ong, RA Otte, AN Park, N Perkins, JS Pohl, M Popkow, A Prokoph, H Quinn, J Ragan, K Reyes, LC Reynolds, PT Richards, GT Roache, E Saxon, DB Sembroski, GH Smith, AW Staszak, D Telezhinsky, I Theiling, M Varlotta, A Vassiliev, VV Vincent, S Wakely, SP Weekes, TC Weinstein, A Welsing, R Williams, DA Zitzer, B Bottcher, M Fegan, SJ Fortin, P Halpern, JP Kovalev, YY Lister, ML Liu, J Pushkarev, AB Smith, PS AF Archambault, S. Arlen, T. Aune, T. Behera, B. Beilicke, M. Benbow, W. Bird, R. Bouvier, A. Buckley, J. H. Bugaev, V. Byrum, K. Cesarini, A. Ciupik, L. Connolly, M. P. Cui, W. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fortson, L. Furniss, A. Galante, N. Gall, D. Gillanders, G. H. Griffin, S. Grube, J. Gyuk, G. Hanna, D. Holder, J. Hughes, G. Humensky, T. B. Kaaret, P. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Kumar, S. Lang, M. J. Madhavan, A. S. Maier, G. Majumdar, P. McArthur, S. McCann, A. Millis, J. Moriarty, P. Mukherjee, R. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Park, N. Perkins, J. S. Pohl, M. Popkow, A. Prokoph, H. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Saxon, D. B. Sembroski, G. H. Smith, A. W. Staszak, D. Telezhinsky, I. Theiling, M. Varlotta, A. Vassiliev, V. V. Vincent, S. Wakely, S. P. Weekes, T. C. Weinstein, A. Welsing, R. Williams, D. A. Zitzer, B. Boettcher, M. Fegan, S. J. Fortin, P. Halpern, J. P. Kovalev, Y. Y. Lister, M. L. Liu, J. Pushkarev, A. B. Smith, P. S. CA VERITAS Collaboration TI DISCOVERY OF A NEW TeV GAMMA-RAY SOURCE: VER J0521+211 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: individual (VER J0521+211); gamma rays: galaxies ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; EXTRAGALACTIC BACKGROUND LIGHT; ALL-SKY SURVEY; HIGH-ENERGY EMISSION; MULTIWAVELENGTH OBSERVATIONS; SOURCE CATALOG; BL-LAC; LINEAR-POLARIZATION; DETECTED BLAZARS AB We report the detection of a new TeV gamma-ray source, VER J0521+211, based on observations made with the VERITAS imaging atmospheric Cherenkov Telescope Array. These observations were motivated by the discovery of a cluster of >30 GeV photons in the first year of Fermi Large Area Telescope observations. VER J0521+211 is relatively bright at TeV energies, with a mean photon flux of (1.93 +/- 0.13(stat) +/- 0.78(sys)) x 10(-11) cm(-2) s(-1) above 0.2 TeV during the period of the VERITAS observations. The source is strongly variable on a daily timescale across all wavebands, from optical to TeV, with a peak flux corresponding to similar to 0.3 times the steady Crab Nebula flux at TeV energies. Follow-up observations in the optical and X-ray bands classify the newly discovered TeV source as a BL Lac-type blazar with uncertain redshift, although recent measurements suggest z = 0.108. VER J0521+211 exhibits all the defining properties of blazars in radio, optical, X-ray, and gamma-ray wavelengths. C1 [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Staszak, D.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Arlen, T.; Aune, T.; Majumdar, P.; Ong, R. A.; Popkow, A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Behera, B.; Federici, S.; Hughes, G.; Krawczynski, H.; Maier, G.; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Vincent, S.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Beilicke, M.; Buckley, J. H.; Bugaev, V.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Galante, N.; Roache, E.; Weekes, T. C.; Fortin, P.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bird, R.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Byrum, K.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cesarini, A.; Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Errando, M.; Mukherjee, R.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Federici, S.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Fortson, L.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Gall, D.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Holder, J.; Kumar, S.; Saxon, D. B.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Holder, J.; Kumar, S.; Saxon, D. B.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Humensky, T. B.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Krennrich, F.; Madhavan, A. S.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Majumdar, P.] Saha Inst Nucl Phys, Kolkata 700064, India. [McArthur, S.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Dublin, Ireland. [Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Boettcher, M.] North West Univ, Ctr Space Res, ZA-2531 Potchefstroom, South Africa. [Fegan, S. J.] Ecole Polytech, CNRS, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Halpern, J. P.; Liu, J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Kovalev, Y. Y.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Kovalev, Y. Y.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Lister, M. L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Pushkarev, A. B.] Pulkovo Astron Observ, St Petersburg 196140, Russia. [Pushkarev, A. B.] Crimean Astrophys Observ, UA-98409 Nauchnyi, Crimea, Ukraine. [Smith, P. S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Archambault, S (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. EM errando@astro.columbia.edu; jholder@physics.udel.edu; sfegan@llr.in2p3.fr; fortin@veritas.sao.arizona.edu RI Kovalev, Yuri/J-5671-2013; Khassen, Yerbol/I-3806-2015; Pushkarev, Alexander/M-9997-2015; OI Errando, Manel/0000-0002-1853-863X; Lang, Mark/0000-0003-4641-4201; Bird, Ralph/0000-0002-4596-8563; Kovalev, Yuri/0000-0001-9303-3263; Khassen, Yerbol/0000-0002-7296-3100; Smith, Paul/0000-0002-5083-3663; Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610; Liu, Jia/0000-0001-8219-1995 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the UK; INAF in Italy; CNES in France; NASA [NNX10AP66G, NNX12AJ30G, NNX10AF89G]; Russian Foundation for Basic Research [11-02-00368, 12-02-33101]; Russian Academy of Sciences; Dynasty Foundation; South African Department of Science and Technology through the National Research Foundation under NRF SARChI Chair [64789]; NASA-Fermi [NNX08AV67G, 11-Fermi11-0019, NNX09AU10G] FX VERITAS is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748), and by STFC in the 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 support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council, and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged.; M. E. acknowledges support from the NASA grants NNX10AP66G and NNX12AJ30G. Y.Y.K. was supported in part by the Russian Foundation for Basic Research (projects 11-02-00368 and 12-02-33101), the basic research program "Active Processes in Galactic and Extragalactic Objects" of the Physical Sciences Division of the Russian Academy of Sciences, and the Dynasty Foundation. M. B. acknowledges support by the South African Department of Science and Technology through the National Research Foundation under NRF SARChI Chair grant No. 64789.; This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. 2009a). The MOJAVE project is supported under NASA-Fermi grants NNX08AV67G and 11-Fermi11-0019. The authors thank Julie Skinner for obtaining, as a target of opportunity, the first MDM spectrum of RGB J0521.8+2112 used in this paper, and Talvikki Hovatta for providing the OVRO radio data. Observations at Steward Observatory were supported by the NASA Fermi Guest Investigator Program grant NNX09AU10G. Finally, the authors thank the Swift team for accepting and carefully scheduling the target of opportunity observations of VER J0521+211 that were used in the paper and for support from the Swift Guest Investigator program, NASA grant NNX10AF89G. NR 93 TC 12 Z9 13 U1 0 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 OCT 20 PY 2013 VL 776 IS 2 AR 69 DI 10.1088/0004-637X/776/2/69 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 255CF UT WOS:000327216100006 ER PT J AU Bauschlicher, CW Ricca, A AF Bauschlicher, Charles W., Jr. Ricca, Alessandra TI THE INFRARED SPECTRA OF POLYCYCLIC AROMATIC HYDROCARBONS WITH SOME OR ALL HYDROGEN ATOMS REMOVED SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; infrared: ISM; ISM: lines and bands; ISM: molecules; line: identification; methods: numerical; molecular data ID ORTHO-BENZYNE; VIBRATIONAL FREQUENCIES; EMISSION; ENERGY; APPROXIMATION; SPECTROSCOPY; EXCHANGE; FEATURES AB The loss of one hydrogen from C96H24 does not significantly affect the infrared spectra of the neutral, cation, or anion. Excluding a very weak C-C stretching band at 5.1 mu m, the loss of two adjacent duo hydrogens does not significantly affect the spectra compared with the parent. Removing all of the hydrogen atoms significantly increases the intensity of the new C-C stretching band, and, for the cation, shifts it to a longer (5.2 mu m) wavelength. Observations show a feature near 5.25 mu m, which has been attributed to overtone and combination bands from polycyclic aromatic hydrocarbons (PAHs). This current work suggests that dehydrogenated PAHs might also contribute to this band, but its weakness implies that fully dehydrogenated cationic or dicationic species are very rare. C1 [Bauschlicher, Charles W., Jr.] NASA, Entry Syst & Technol Div, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ricca, Alessandra] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. RP Bauschlicher, CW (reprint author), NASA, Entry Syst & Technol Div, Ames Res Ctr, Mail Stop 230-3, Moffett Field, CA 94035 USA. EM Charles.W.Bauschlicher@nasa.gov; Alessandra.Ricca-1@nasa.gov FU NASA's Astrophysics Theory and Fundamental Physics (ATFP) [NNX09AD18G]; NASA's Laboratory Astrophysics "Carbon in the Galaxy" Consortium Grant [NNH10ZDA001N] FX A.R. thanks NASA's Astrophysics Theory and Fundamental Physics (ATFP) (NNX09AD18G) and Laboratory Astrophysics "Carbon in the Galaxy" Consortium Grant (NNH10ZDA001N) programs for their generous support of this work. NR 23 TC 8 Z9 8 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 OCT 20 PY 2013 VL 776 IS 2 AR 102 DI 10.1088/0004-637X/776/2/102 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 255CF UT WOS:000327216100039 ER PT J AU Dekany, R Roberts, J Burruss, R Bouchez, A Truong, T Baranec, C Guiwits, S Hale, D Angione, J Trinh, T Zolkower, J Shelton, JC Palmer, D Henning, J Croner, E Troy, M McKenna, D Tesch, J Hildebrandt, S Milburn, J AF Dekany, Richard Roberts, Jennifer Burruss, Rick Bouchez, Antonin Tuan Truong Baranec, Christoph Guiwits, Stephen Hale, David Angione, John Thang Trinh Zolkower, Jeffry Shelton, J. Christopher Palmer, Dean Henning, John Croner, Ernest Troy, Mitchell McKenna, Dan Tesch, Jonathan Hildebrandt, Sergi Milburn, Jennifer TI PALM-3000: EXOPLANET ADAPTIVE OPTICS FOR THE 5 m HALE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE atmospheric effects; instrumentation: adaptive optics; minor planets, asteroids: individual (Ganymede); planets and satellites: detection; techniques: high angular resolution; techniques: imaging spectroscopy ID WAVE-FRONT SENSOR; BROWN DWARF; MASKING INTERFEROMETRY; STELLAR MASS; HR 8799; SYSTEM; PLANET; COMPANION; RECONSTRUCTION; STAR AB We describe and report first results from PALM-3000, the second-generation astronomical adaptive optics (AO) facility for the 5.1 m Hale telescope at Palomar Observatory. PALM-3000 has been engineered for high-contrast imaging and emission spectroscopy of brown dwarfs and large planetary mass bodies at near-infrared wavelengths around bright stars, but also supports general natural guide star use to V approximate to 17. Using its unique 66 x 66 actuator deformable mirror, PALM-3000 has thus far demonstrated residual wavefront errors of 141 nm rms under similar to 1 '' seeing conditions. PALM-3000 can provide phase conjugation correction over a 6 ''.4 x 6 ''.4 working region at lambda = 2.2 mu m, or full electric field (amplitude and phase) correction over approximately one-half of this field. With optimized back-end instrumentation, PALM-3000 is designed to enable 10(-7) contrast at 1 '' angular separation, including post-observation speckle suppression processing. While continued optimization of the AO system is ongoing, we have already successfully commissioned five back-end instruments and begun a major exoplanet characterization survey, Project 1640. C1 [Dekany, Richard; Bouchez, Antonin; Baranec, Christoph; Hale, David; Zolkower, Jeffry; Henning, John; Croner, Ernest; McKenna, Dan; Hildebrandt, Sergi; Milburn, Jennifer] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA. [Roberts, Jennifer; Burruss, Rick; Tuan Truong; Guiwits, Stephen; Angione, John; Thang Trinh; Shelton, J. Christopher; Palmer, Dean; Troy, Mitchell; Tesch, Jonathan; Hildebrandt, Sergi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Dekany, R (reprint author), CALTECH, Caltech Opt Observ, 1200 East Calif Blvd,MC 11-17, Pasadena, CA 91125 USA. EM rgd@astro.caltech.edu FU National Science Foundation (NSF) [AST-0619922, AST-1007046]; Jet Propulsion Laboratory; Caltech Optical Observatories; NASA SBIR [NNG05CA21C] FX This work was performed with financial support of National Science Foundation (NSF) through awards AST-0619922 and AST-1007046, Jet Propulsion Laboratory, Caltech Optical Observatories, and the generous philanthropy of Ron and Glo Helin. Development of the Xinetics, Inc. The PALM-3000 HODM was funded by NASA SBIR award #NNG05CA21C. The successful deployment of PALM-3000 could not have been possible without the notable talent and dedication of the entire Palomar Observatory staff. We gratefully acknowledge the specific contributions from Dan McKenna, John Henning, Steve Kunsman, Kajsa Peffer, Jean Mueller, Kevin Rykowski, Carolyn Heffner, Steve Einer, Greg van Idsinga, Mike Doyle, and Bruce Baker in interfacing to the Hale Telescope and to obtaining the commissioning data described herein. NR 83 TC 39 Z9 39 U1 0 U2 11 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 OCT 20 PY 2013 VL 776 IS 2 AR 130 DI 10.1088/0004-637X/776/2/130 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 255CF UT WOS:000327216100067 ER PT J AU Feldmeier, JJ Hagen, A Ciardullo, R Gronwall, C Gawiser, E Guaita, L Hagen, LMZ Bond, NA Acquaviva, V Blanc, GA Orsi, A Kurczynski, P AF Feldmeier, John J. Hagen, Alex Ciardullo, Robin Gronwall, Caryl Gawiser, Eric Guaita, Lucia Hagen, Lea M. Z. Bond, Nicholas A. Acquaviva, Viviana Blanc, Guillermo A. Orsi, Alvaro Kurczynski, Peter TI SEARCHING FOR NEUTRAL HYDROGEN HALOS AROUND z similar to 2.1 AND z similar to 3.1 Ly alpha EMITTING GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: evolution; galaxies: halos; galaxies: high-redshift; galaxies: structure ID STAR-FORMING GALAXIES; DEEP FIELD-SOUTH; LYMAN BREAK GALAXIES; EMISSION-LINE GALAXIES; CCD SURFACE PHOTOMETRY; HIGH-REDSHIFT GALAXIES; FRAME ULTRAVIOLET-SPECTRA; DIFFUSE OPTICAL LIGHT; EARLY RELEASE SCIENCE; I. SURVEY DESIGN AB We search for evidence of diffuse Ly alpha emission from extended neutral hydrogen surrounding Ly alpha emitting galaxies (LAEs) using deep narrow-band images of the Extended Chandra Deep Field South. By stacking the profiles of 187 LAEs at z = 2.06, 241 LAEs at z = 3.10, and 179 LAEs at z = 3.12, and carefully performing low-surface brightness photometry, we obtain mean surface brightness maps that reach 9.9, 8.7, and 6.2 x 10(-19) erg cm(-2) s(-1) arcsec(-2) in the emission line. We undertake a thorough investigation of systematic uncertainties in our surface brightness measurements and find that our limits are 5-10 times larger than would be expected from Poisson background fluctuations; these uncertainties are often underestimated in the literature. At z similar to 3.1, we find evidence for extended halos with small-scale lengths of 5-8 kpc in some but not all of our sub-samples. We demonstrate that sub-samples of LAEs with low equivalent widths and brighter continuum magnitudes are more likely to possess such halos. At z similar to 2.1, we find no evidence of extended Ly alpha emission down to our detection limits. Through Monte-Carlo simulations, we also show that we would have detected large diffuse LAE halos if they were present in our data sets. We compare these findings to other measurements in the literature and discuss possible instrumental and astrophysical reasons for the discrepancies. C1 [Feldmeier, John J.] Youngstown State Univ, Dept Phys & Astron, Youngstown, OH 44555 USA. [Hagen, Alex; Ciardullo, Robin; Gronwall, Caryl; Hagen, Lea M. Z.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Hagen, Alex; Ciardullo, Robin; Gronwall, Caryl; Hagen, Lea M. Z.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Gawiser, Eric; Kurczynski, Peter] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Guaita, Lucia] Stockholm Univ, Dept Astron, Oskar Klein Cosmol Ctr, SE-10691 Stockholm, Sweden. [Bond, Nicholas A.] NASA, Goddard Space Flight Ctr, Cosmol Lab Code 665, Greenbelt, MD 20771 USA. [Acquaviva, Viviana] CUNY, New York City Coll Technol, Dept Phys, Brooklyn, NY 11201 USA. [Blanc, Guillermo A.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Orsi, Alvaro] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago, Chile. [Orsi, Alvaro] Pontificia Univ Catolica Chile, Ctr Astroingn, Santiago, Chile. RP Feldmeier, JJ (reprint author), Youngstown State Univ, Dept Phys & Astron, Youngstown, OH 44555 USA. EM jjfeldmeier@ysu.edu RI Blanc, Guillermo/I-5260-2016; OI Orsi, Alvaro/0000-0002-8359-7812; Feldmeier, John/0000-0003-2908-2620 FU NSF [AST 06-07416, AST 08-07570, AST 08-07873, AST 08-07885, AST 10-55919]; DOE [DE-GF02-08ER41560, DE-FG02-08ER41561]; Eberly College of Science; Office of the Senior Vice President for Research at the Pennsylvania State University FX This work was supported by NSF grants AST 06-07416, AST 08-07570, AST 08-07873, AST 08-07885, and AST 10-55919, and DOE grants DE-GF02-08ER41560 and DE-FG02-08ER41561. The Institute for Gravitation and the Cosmos is supported by the Eberly College of Science and the Office of the Senior Vice President for Research at the Pennsylvania State University. NR 116 TC 18 Z9 18 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 OCT 20 PY 2013 VL 776 IS 2 AR 75 DI 10.1088/0004-637X/776/2/75 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 255CF UT WOS:000327216100012 ER PT J AU Ko, YK Tylka, AJ Ng, CK Wang, YM Dietrich, WF AF Ko, Yuan-Kuen Tylka, Allan J. Ng, Chee K. Wang, Yi-Ming Dietrich, William F. TI SOURCE REGIONS OF THE INTERPLANETARY MAGNETIC FIELD AND VARIABILITY IN HEAVY-ION ELEMENTAL COMPOSITION IN GRADUAL SOLAR ENERGETIC PARTICLE EVENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; shock waves; solar wind; Sun: abundances; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: heliosphere; Sun: particle emission ID CORONAL MASS EJECTIONS; ADVANCED COMPOSITION EXPLORER; SOURCE SURFACE MODEL; FAST-WIND REGIONS; DRIVEN SHOCKS; ISOTOPE SPECTROMETER; CYCLE 23; SPECTRAL PROPERTIES; TEMPORAL EVOLUTION; HE-3-RICH EVENTS AB Gradual solar energetic particle (SEP) events are those in which ions are accelerated to their observed energies by interactions with a shock driven by a fast coronal mass ejection (CME). Previous studies have shown that much of the observed event-to-event variability can be understood in terms of shock speed and evolution in the shock-normal angle. However, an equally important factor, particularly for the elemental composition, is the origin of the suprathermal seed particles upon which the shock acts. To tackle this issue, we (1) use observed solar-wind speed, magnetograms, and the potential-field source-surface model to map the Sun-L1 interplanetary magnetic field (IMF) line back to its source region on the Sun at the time of the SEP observations and (2) then look for a correlation between SEP composition (as measured by Wind and Advanced Composition Explorer at similar to 2-30 MeV nucleon(-1)) and characteristics of the identified IMF source regions. The study is based on 24 SEP events, identified as a statistically significant increase in similar to 20 MeV protons and occurring in 1998 and 2003-2006, when the rate of newly emergent solar magnetic flux and CMEs was lower than in solar-maximum years, and the field-line tracing is therefore more likely to be successful. We find that the gradual SEP Fe/O is correlated with the field strength at the IMF source, with the largest enhancements occurring when the footpoint field is strong due to the nearby presence of an active region (AR). In these cases, other elemental ratios show a strong charge-to-mass (q/M) ordering (at least on average), similar to that found in impulsive events. Such results lead us to suggest that magnetic reconnection in footpoint regions near ARs bias the heavy-ion composition of suprathermal seed ions by processes qualitatively similar to those that produce larger heavy-ion enhancements in impulsive SEP events. To address potential technical concerns about our analysis, we also discuss efforts to exclude impulsive SEP events from our event sample. C1 [Ko, Yuan-Kuen; Wang, Yi-Ming] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Tylka, Allan J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ng, Chee K.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Dietrich, William F.] Praxis Inc, Alexandria, VA 22303 USA. RP Ko, YK (reprint author), Naval Res Lab, Div Space Sci, Code 7680, Washington, DC 20375 USA. EM yko@ssd5.nrl.navy.mil RI Tylka, Allan/G-9592-2014 NR 111 TC 5 Z9 5 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 OCT 20 PY 2013 VL 776 IS 2 AR 92 DI 10.1088/0004-637X/776/2/92 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 255CF UT WOS:000327216100029 ER PT J AU Kospal, A Moor, A Juhasz, A Abraham, P Apai, D Csengeri, T Grady, CA Henning, T Hughes, AM Kiss, C Pascucci, I Schmalzl, M AF Kospal, A. Moor, A. Juhasz, A. Abraham, P. Apai, D. Csengeri, T. Grady, C. A. Henning, Th. Hughes, A. M. Kiss, Cs. Pascucci, I. Schmalzl, M. TI ALMA OBSERVATIONS OF THE MOLECULAR GAS IN THE DEBRIS DISK OF THE 30 Myr OLD STAR HD 21997 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; stars: individual (HD 21997) ID A-TYPE STARS; PICTORIS CIRCUMSTELLAR DISK; SUN-LIKE STARS; ROTATIONAL VELOCITIES; EVOLUTION; SYSTEMS; COMETS; DUST; ORIGIN; RATIOS AB The 30 Myr old A3-type star HD 21997 is one of the two known debris dust disks having a measurable amount of cold molecular gas. With the goal of understanding the physical state, origin, and evolution of the gas in young debris disks, we obtained CO line observations with the Atacama Large Millimeter/submillimeter Array (ALMA). Here, we report on the detection of (CO)-C-12 and (CO)-C-13 in the J = 2-1 and J = 3-2 transitions and (CO)-O-18 in the J = 2-1 line. The gas exhibits a Keplerian velocity curve, one of the few direct measurements of Keplerian rotation in young debris disks. The measured CO brightness distribution could be reproduced by a simple star+disk system, whose parameters are r(in) < 26 AU, r(out) = 138 +/- 20 AU, M-* = 1.8(-0.2)(+0.5) M-circle dot, and i = 32 degrees.6 +/- 3 degrees.1. The total CO mass, as calculated from the optically thin (CO)-O-18 line, is about (4-8) x 10(-2) M-circle plus, while the CO line ratios suggest a radiation temperature on the order of 6-9 K. Comparing our results with those obtained for the dust component of the HD 21997 disk from ALMA continuum observations by Moor et al., we conclude that comparable amounts of CO gas and dust are present in the disk. Interestingly, the gas and dust in the HD 21997 system are not colocated, indicating a dust-free inner gas disk within 55 AU of the star. We explore two possible scenarios for the origin of the gas. A secondary origin, which involves gas production from colliding or active planetesimals, would require unreasonably high gas production rates and would not explain why the gas and dust are not colocated. We propose that HD 21997 is a hybrid system where secondary debris dust and primordial gas coexist. HD 21997, whose age exceeds both the model predictions for disk clearing and the ages of the oldest T Tauri-like or transitional gas disks in the literature, may be a key object linking the primordial and the debris phases of disk evolution. C1 [Kospal, A.] European Space Agcy, Estec, SRE SA, NL-2200 AG Noordwijk, Netherlands. [Moor, A.; Abraham, P.; Kiss, Cs.] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, H-1525 Budapest, Hungary. [Juhasz, A.; Schmalzl, M.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands. [Apai, D.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Apai, D.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Csengeri, T.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Grady, C. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Grady, C. A.] Eureka Sci, Oakland, CA 94602 USA. [Henning, Th.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Hughes, A. M.] Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA. [Pascucci, I.] Univ Arizona, Lunar & Planetary Lab, Dept Planetary Sci, Tucson, AZ 85721 USA. RP Kospal, A (reprint author), European Space Agcy, Estec, SRE SA, POB 299, NL-2200 AG Noordwijk, Netherlands. EM akospal@rssd.esa.int FU Hungarian Scientific Research Fund [OTKA-101393]; NASA; Bolyai Fellowship FX We thank the anonymous referee for useful comments that helped us to improve the manuscript. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00780.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This work was partly supported by the grant OTKA-101393 of the Hungarian Scientific Research Fund. This work is based in part on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. A. M. acknowledges the support of the Bolyai Fellowship. NR 42 TC 29 Z9 29 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 OCT 20 PY 2013 VL 776 IS 2 AR 77 DI 10.1088/0004-637X/776/2/77 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 255CF UT WOS:000327216100014 ER PT J AU Lemze, D Postman, M Genel, S Ford, HC Balestra, I Donahue, M Kelson, D Nonino, M Mercurio, A Biviano, A Rosati, P Umetsu, K Sand, D Koekemoer, A Meneghetti, M Melchior, P Newman, AB Bhatti, WA Voit, GM Medezinski, E Zitrin, A Zheng, W Broadhurst, T Bartelmann, M Benitez, N Bouwens, R Bradley, L Coe, D Graves, G Grillo, C Infante, L Jimenez-Teja, Y Jouvel, S Lahav, O Maoz, D Merten, J Molino, A Moustakas, J Moustakas, L Ogaz, S Scodeggio, M Seitz, S AF Lemze, Doron Postman, Marc Genel, Shy Ford, Holland C. Balestra, Italo Donahue, Megan Kelson, Daniel Nonino, Mario Mercurio, Amata Biviano, Andrea Rosati, Piero Umetsu, Keiichi Sand, David Koekemoer, Anton Meneghetti, Massimo Melchior, Peter Newman, Andrew B. Bhatti, Waqas A. Voit, G. Mark Medezinski, Elinor Zitrin, Adi Zheng, Wei Broadhurst, Tom Bartelmann, Matthias Benitez, Narciso Bouwens, Rychard Bradley, Larry Coe, Dan Graves, Genevieve Grillo, Claudio Infante, Leopoldo Jimenez-Teja, Yolanda Jouvel, Stephanie Lahav, Ofer Maoz, Dan Merten, Julian Molino, Alberto Moustakas, John Moustakas, Leonidas Ogaz, Sara Scodeggio, Marco Seitz, Stella TI THE CONTRIBUTION OF HALOS WITH DIFFERENT MASS RATIOS TO THE OVERALL GROWTH OF CLUSTER-SIZED HALOS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: clusters: individual (Abell 611, Abell 963, Abell 1423, Abell 2261, MACS J1206.2-0848, RX J2129.7+0005, CL 2130.4-0000); galaxies: kinematics and dynamics ID PROBE WMAP OBSERVATIONS; DARK-MATTER HALOES; DIGITAL SKY SURVEY; SCALE-INDEPENDENT METHOD; GALAXY CLUSTERS; VELOCITY ANISOTROPY; DENSITY PROFILES; DATA RELEASE; ACCELERATING UNIVERSE; MACS J1206.2-0847 AB We provide a new observational test for a key prediction of the Lambda CDM cosmological model: the contributions of mergers with different halo-to-main-cluster mass ratios to cluster-sized halo growth. We perform this test by dynamically analyzing 7 galaxy clusters, spanning the redshift range 0.13 < z(c) < 0.45 and caustic mass range 0.4-1.5 10(15) h(0.73)(-1) M-circle dot, with an average of 293 spectroscopically confirmed bound galaxies to each cluster. The large radial coverage (a few virial radii), which covers the whole infall region, with a high number of spectroscopically identified galaxies enables this new study. For each cluster, we identify bound galaxies. Out of these galaxies, we identify infalling and accreted halos and estimate their masses and their dynamical states. Using the estimated masses, we derive the contribution of different mass ratios to cluster-sized halo growth. For mass ratios between similar to 0.2 and 0.7, we find a similar to 1 sigma agreement with Lambda CDM expectations based on the Millennium simulations I and II. At low mass ratios, less than or similar to 0.2, our derived contribution is underestimated since the detection efficiency decreases at low masses, similar to 2 x 10(14) h(0.73)(-1) M-circle dot. At large mass ratios, greater than or similar to 0.7, we do not detect halos probably because our sample, which was chosen to be quite X-ray relaxed, is biased against large mass ratios. Therefore, at large mass ratios, the derived contribution is also underestimated. C1 [Lemze, Doron; Ford, Holland C.; Medezinski, Elinor; Zheng, Wei] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Postman, Marc; Koekemoer, Anton; Bradley, Larry; Coe, Dan; Ogaz, Sara] Space Telescope Sci Inst, Baltimore, MD 21208 USA. [Genel, Shy] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Balestra, Italo; Nonino, Mario; Biviano, Andrea] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy. [Balestra, Italo; Mercurio, Amata] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Donahue, Megan] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Kelson, Daniel; Voit, G. Mark] Carnegie Observ, Carnegie Inst Sci, Pasadena, CA USA. [Rosati, Piero] European So Observ, D-85748 Garching, Germany. [Umetsu, Keiichi] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Sand, David] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Meneghetti, Massimo] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Meneghetti, Massimo] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy. [Melchior, Peter] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Melchior, Peter] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Newman, Andrew B.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Bhatti, Waqas A.; Graves, Genevieve] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Zitrin, Adi; Bartelmann, Matthias] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, D-69120 Heidelberg, Germany. [Broadhurst, Tom] Univ Basque Country UPV EHU, Dept Theoret Phys, E-48080 Bilbao, Spain. [Broadhurst, Tom] Basque Fdn Sci, IKERBASQUE, E-48011 Bilbao, Spain. [Benitez, Narciso; Jimenez-Teja, Yolanda; Molino, Alberto] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Bouwens, Rychard] Leiden Univ, Leiden Observ, NL-2333 Leiden, Netherlands. [Graves, Genevieve] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Grillo, Claudio] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Infante, Leopoldo] Pontificia Univ Catolica Chile, Inst Astrophys, Santiago, Chile. [Infante, Leopoldo] Pontificia Univ Catolica Chile, Ctr Astroengn, Santiago, Chile. [Jouvel, Stephanie] Inst Cincies Espai IEE CSIC, E-08193 Bellaterra, Barcelona, Spain. [Lahav, Ofer] UCL, Dept Phys & Astron, London, England. [Maoz, Dan] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Merten, Julian; Moustakas, Leonidas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Moustakas, John] Siena Coll, Dept Phys & Astron, Loudonville, NY USA. [Scodeggio, Marco] INAF IASF Milano, I-20133 Milan, Italy. [Seitz, Stella] Univ Sternwarte Munchen, Inst Astron, D-81679 Munich, Germany. [Seitz, Stella] Univ Sternwarte Munchen, Inst Astrophys, D-81679 Munich, Germany. [Seitz, Stella] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany. RP Lemze, D (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA. RI Bartelmann, Matthias/A-5336-2014; Molino Benito, Alberto/F-5298-2014; Jimenez-Teja, Yolanda/D-5933-2011; Grillo, Claudio/E-6223-2015; Meneghetti, Massimo/O-8139-2015; OI Grillo, Claudio/0000-0002-5926-7143; Meneghetti, Massimo/0000-0003-1225-7084; Bhatti, Waqas/0000-0002-0628-0088; Nonino, Mario/0000-0001-6342-9662; Balestra, Italo/0000-0001-9660-894X; Scodeggio, Marco/0000-0002-2282-5850; Umetsu, Keiichi/0000-0002-7196-4822; Biviano, Andrea/0000-0002-0857-0732; Genel, Shy/0000-0002-3185-1540; Moustakas, Leonidas/0000-0003-3030-2360; Koekemoer, Anton/0000-0002-6610-2048; Benitez, Narciso/0000-0002-0403-7455; Voit, Gerard/0000-0002-3514-0383 FU NASA [HST-GO-12065.01-A]; PRIN INAF; ASI; Baden Wurttemberg Stiftung FX We thank Margaret J. Geller, Kenneth Rines, Michael Kurtz, and Antonaldo Diaferio for providing their redshift data for A611 and CL2130 and for providing the redshift data for A963, A2261, A1423, and RXJ2129 in advance of publication. We also thank them for many helpful discussions. In addition, we acknowledge very useful discussions with Ana Laura Serra, Dan Gifford, Mark Neyrinck, Yuval Birnboim, Eyal Neistein, and Maxim Markevitch. We thank the anonymous referee for useful comments. D. L. thanks Eran Ofek for his publicly available Matlab scripts. This research is supported in part by NASA grant HST-GO-12065.01-A. M. M. acknowledges support from PRIN INAF 2009 and ASI (agreement Euclid phase B2/C). A.Z. is supported by contract research "Internationale Spitzenforschung II/2-6" of the Baden Wurttemberg Stiftung. NR 102 TC 21 Z9 21 U1 1 U2 13 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 OCT 20 PY 2013 VL 776 IS 2 AR 91 DI 10.1088/0004-637X/776/2/91 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 255CF UT WOS:000327216100028 ER PT J AU Morales, FY Bryden, G Werner, MW Stapelfeldt, KR AF Morales, F. Y. Bryden, G. Werner, M. W. Stapelfeldt, K. R. TI HERSCHEL-RESOLVED OUTER BELTS OF TWO-BELT DEBRIS DISKS AROUND A-TYPE STARS: HD 70313, HD 71722, HD 159492, AND F-TYPE: HD 104860 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: planetary systems; planets and satellites: formation; stars: individual (HD 70313, HD 71722, HD 104860, HD 159492) ID SPITZER-SPACE-TELESCOPE; BETA-PICTORIS DISK; PLANETARY SYSTEMS; MASS STARS; HR 8799; DUST; FOMALHAUT; GRAINS; IMAGES; RING AB We present dual-band Herschel/Photodetector Array Camera and Spectrometer imaging for four stars whose spectral energy distributions (SEDs) suggest two-ring disk architectures that mirror that of the asteroid-Kuiper Belt geometry of our own solar system. The Herschel observations at 100 mu m spatially resolve the cold/outer-dust component for each star-disk system for the first time, finding evidence of planetesimals at >100 AU, i.e., a larger size than assumed from a simple blackbody fit to the SED. By breaking the degeneracy between the grain properties and the dust's radial location, the resolved images help constrain the dust grain-size distribution for each system. Three of the observed stars are A-type and one solar-type. On the basis of the combined Spitzer/IRS+MIPS (5-70 mu m), the Herschel/PACS (100 and 160 mu m) dataset, and under the assumption of idealized spherical grains, we find that the cold/outer belts of the three A-type stars are well fit with a mixed ice/rock composition rather than pure rocky grains, while the debris around the solar-type star is consistent with either rock or ice/rock grains. For the solar-type star HD 104860, we find that the minimum grain size is larger than expected from the threshold set by radiative blowout. The A-type stars HD 71722 and HD 159492, on the other hand, require minimum grain sizes that are smaller than blowout for inner-and outer-ring populations. In the absence of spectral features for ice, we find that the behavior of the continuum can help constrain the composition of the grains (of icy nature and not pure rocky material) given the Herschel-resolved locations of the cold/outer-dust belts. C1 [Morales, F. Y.; Bryden, G.; Werner, M. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Morales, F. Y.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA. [Stapelfeldt, K. R.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. RP Morales, FY (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Farisa@jpl.nasa.gov FU Jet Propulsion Laboratory, California Institute of Technology; National Aeronautics and Space Administration FX The research described in this publication was carried out with internal R&TD funding at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This publication makes use of data products from the Two Micron All Sky Survey (2MASS) and from the SIMBAD Web site. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This work is based (in part) on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This research is based (in part) on the PhD dissertation work of F. Morales for the Department of Physics and Astronomy, University of Southern California. NR 48 TC 22 Z9 22 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 OCT 20 PY 2013 VL 776 IS 2 AR 111 DI 10.1088/0004-637X/776/2/111 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 255CF UT WOS:000327216100048 ER PT J AU Tsai, CW Turner, JL Beck, SC Meier, DS Wright, SA AF Tsai, Chao-Wei Turner, Jean L. Beck, Sara C. Meier, David S. Wright, Shelley A. TI THE CIRCUMNUCLEAR STAR FORMATION ENVIRONMENT OF NGC 6946: Br gamma AND H-2 RESULTS FROM KECK INTEGRAL FIELD SPECTROSCOPY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 6946); galaxies: starburst; galaxies: star clusters: general; HII regions; infrared: galaxies; radio continuum: galaxies ID SPIRAL GALAXY NGC-6946; MOLECULAR-HYDROGEN EMISSION; STARBURST GALAXIES; NUCLEAR STARBURST; ANTENNAE GALAXIES; NEARBY GALAXIES; GALACTIC-CENTER; CENTRAL REGIONS; DISK GALAXIES; GAS-DYNAMICS AB We present a three-dimensional data cube of the K-band continuum and the Br gamma, H-2 S(0), and S(1) lines within the central 18 '' 5 x 5 x 13.'' 8 (520 pc x 390 pc) region of NGC 6946. Data were obtained using OSIRIS, a near-infrared Integral Field Spectrograph at Keck Observatory, with Laser Guide Star Adaptive Optics. The 0.'' 3 resolution allows us to investigate the stellar bulge and the forming star clusters in the nuclear region on 10 pc scales. We detect giant HII regions associated with massive young star clusters in the nuclear spiral/ring (R similar to 30 pc) and in the principal shocks along the nuclear bar. Comparisons of the Br gamma fluxes with Pa alpha line emission and radio continuum indicate A(K) similar to 3, A(V) similar to 25 for the nuclear star-forming regions. The most luminous HII regions are restricted to within 70 pc of the center, despite the presence of high gas columns at larger radii (R similar to 200 pc). H-2 emission is restricted to clouds within R similar to 60 pc of the center, resembling the distribution of HCN line emission. We propose that gas-assisted migration of the young star clusters is contributing to the buildup of the nuclear bar and nuclear star cluster (R < 30 pc) in this galaxy. C1 [Tsai, Chao-Wei] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Turner, Jean L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Beck, Sara C.] Tel Aviv Univ, Dept Phys & Astron, Ramat Aviv, Israel. [Meier, David S.] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA. [Meier, David S.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Wright, Shelley A.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON, Canada. RP Tsai, CW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Chao-Wei.Tsai@jpl.nasa.gov FU W. M. Keck Foundation FX The authors thank the anonymous referee for a very thorough and helpful review. C. W. T. acknowledges Tuan Do for his help with the OSIRIS observations. We are grateful to Steve Maciejewski and Bruce Elmegreen for discussions of these results at a TIARA conference. This work is based 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 NASA, and was made possible by the generous financial support of the W. M. Keck Foundation. The authors also 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. The 18 cm radio data reported in this paper are based on archived data made with MERLIN, a National Facility operated by the University of Manchester at Jodrell Bank Observatory on behalf of STFC. NR 74 TC 3 Z9 3 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 OCT 20 PY 2013 VL 776 IS 2 AR 70 DI 10.1088/0004-637X/776/2/70 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 255CF UT WOS:000327216100007 ER PT J AU Demory, BO de Wit, J Lewis, N Fortney, J Zsom, A Seager, S Knutson, H Heng, K Madhusudhan, N Gillon, M Barclay, T Desert, JM Parmentier, V Cowan, NB AF Demory, Brice-Olivier de Wit, Julien Lewis, Nikole Fortney, Jonathan Zsom, Andras Seager, Sara Knutson, Heather Heng, Kevin Madhusudhan, Nikku Gillon, Michael Barclay, Thomas Desert, Jean-Michel Parmentier, Vivien Cowan, Nicolas B. TI INFERENCE OF INHOMOGENEOUS CLOUDS IN AN EXOPLANET ATMOSPHERE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; stars: individual (Kepler-7); techniques: photometric ID TIDALLY LOCKED EXOPLANETS; EXTRASOLAR GIANT PLANETS; SPITZER-SPACE-TELESCOPE; HOT JUPITERS; HD 189733B; TRANSITING PLANETS; CIRCULATION; ALBEDO; MODELS; SIMULATIONS AB We present new visible and infrared observations of the hot Jupiter Kepler-7b to determine its atmospheric properties. Our analysis allows us to (1) refine Kepler-7b's relatively large geometric albedo of Ag = 0.35 +/- 0.02, (2) place upper limits on Kepler-7b thermal emission that remains undetected in both Spitzer bandpasses and (3) report a westward shift in the Kepler optical phase curve. We argue that Kepler-7b's visible flux cannot be due to thermal emission or Rayleigh scattering from H-2 molecules. We therefore conclude that high altitude, optically reflective clouds located west from the substellar point are present in its atmosphere. We find that a silicate-based cloud composition is a possible candidate. Kepler-7b exhibits several properties that may make it particularly amenable to cloud formation in its upper atmosphere. These include a hot deep atmosphere that avoids a cloud cold trap, very low surface gravity to suppress cloud sedimentation, and a planetary equilibrium temperature in a range that allows for silicate clouds to potentially form in the visible atmosphere probed by Kepler. Our analysis does not only present evidence of optically thick clouds on Kepler-7b but also yields the first map of clouds in an exoplanet atmosphere. C1 [Demory, Brice-Olivier; de Wit, Julien; Lewis, Nikole; Zsom, Andras; Seager, Sara] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Fortney, Jonathan] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Knutson, Heather; Desert, Jean-Michel] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Heng, Kevin] Univ Bern, Ctr Space & Habitabil, CH-3012 Bern, Switzerland. [Madhusudhan, Nikku] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Madhusudhan, Nikku] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Gillon, Michael] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege 1, Belgium. [Barclay, Thomas] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Parmentier, Vivien] Univ Nice Sophia Antipolis, CNRS, Lab JL Lagrange, UMR 7293, F-06304 Nice 4, France. [Cowan, Nicolas B.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. RP Demory, BO (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM demory@mit.edu OI Fortney, Jonathan/0000-0002-9843-4354; Demory, Brice-Olivier/0000-0002-9355-5165 FU NASA; German Science Foundation (DFG) [ZS107/2-1]; California Institute of Technology; NASA through the Sagan Fellowship Program; Belgian American Educational Foundation; Wallonie-Bruxelles International FX We thank G. Basri and both anonymous referees for helpful comments that improved the Letter. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the JPL, Caltech under a contract with NASA. A. Zsom was supported by the German Science Foundation (DFG) under grant ZS107/2-1. This work was performed in part under contract with the California Institute of Technology funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. J. de Wit acknowledges support from the Belgian American Educational Foundation and Wallonie-Bruxelles International. NR 41 TC 62 Z9 62 U1 2 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 20 PY 2013 VL 776 IS 2 AR L25 DI 10.1088/2041-8205/776/2/L25 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 232JO UT WOS:000325490200008 ER PT J AU Fragos, T Lehmer, BD Naoz, S Zezas, A Basu-Zych, A AF Fragos, T. Lehmer, B. D. Naoz, S. Zezas, A. Basu-Zych, A. TI ENERGY FEEDBACK FROM X-RAY BINARIES IN THE EARLY UNIVERSE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE dark ages, reionization, first stars; galaxies: high-redshift; galaxies: stellar content; stars: evolution; X-rays: binaries; X-rays: diffuse background ID REGULATED STAR-FORMATION; ACTIVE GALACTIC NUCLEI; LUMINOSITY FUNCTION; BLACK-HOLES; HIGH-REDSHIFT; GALAXIES; EVOLUTION; MASS; REIONIZATION; EMISSION AB X-ray photons, because of their long mean-free paths, can easily escape the galactic environments where they are produced, and interact at long distances with the intergalactic medium, potentially having a significant contribution to the heating and reionization of the early universe. The two most important sources of X-ray photons in the universe are active galactic nuclei (AGNs) and X-ray binaries (XRBs). In this Letter we use results from detailed, large scale population synthesis simulations to study the energy feedback of XRBs, from the first galaxies (z similar to 20) until today. We estimate that X-ray emission from XRBs dominates over AGN at z greater than or similar to 6-8. The shape of the spectral energy distribution of the emission from XRBs shows little change with redshift, in contrast to its normalization which evolves by similar to 4 orders ofmagnitude, primarily due to the evolution of the cosmic star-formation rate. However, the metallicity and the mean stellar age of a given XRB population affect significantly its X-ray output. Specifically, the X-ray luminosity from high-mass XRBs per unit of star-formation rate varies an order of magnitude going from solar metallicity to less than 10% solar, and the X-ray luminosity from low-mass XRBs per unit of stellar mass peaks at an age of similar to 300 Myr and then decreases gradually at later times, showing little variation for mean stellar ages greater than or similar to 3 Gyr. Finally, we provide analytical and tabulated prescriptions for the energy output of XRBs, that can be directly incorporated in cosmological simulations. C1 [Fragos, T.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fragos, T.; Naoz, S.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Lehmer, B. D.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Lehmer, B. D.; Basu-Zych, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zezas, A.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece. [Zezas, A.] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece. RP Fragos, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tfragos@cfa.harvard.edu RI Zezas, Andreas/C-7543-2011; Fragos, Tassos/A-3581-2016; OI Zezas, Andreas/0000-0001-8952-676X; Fragos, Tassos/0000-0003-1474-1523; Naoz, Smadar/0000-0002-9802-9279 FU CfA prize fellowship program; ITC prize fellowship program; NASA through an Einstein Postdoctoral Fellowship [PF2-130096] FX T.F. acknowledges support from the CfA and the ITC prize fellowship programs. S.N. is supported by NASA through an Einstein Postdoctoral Fellowship (contract PF2-130096). NR 41 TC 45 Z9 45 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 20 PY 2013 VL 776 IS 2 AR L31 DI 10.1088/2041-8205/776/2/L31 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 232JO UT WOS:000325490200014 ER PT J AU Henry, A Scarlata, C Dominguez, A Malkan, M Martin, CL Siana, B Atek, H Bedregal, AG Colbert, JW Rafelski, M Ross, N Teplitz, H Bunker, AJ Dressler, A Hathi, N Masters, D McCarthy, P Straughn, A AF Henry, Alaina Scarlata, Claudia Dominguez, Alberto Malkan, Matthew Martin, Crystal L. Siana, Brian Atek, Hakim Bedregal, Alejandro G. Colbert, James W. Rafelski, Marc Ross, Nathaniel Teplitz, Harry Bunker, Andrew J. Dressler, Alan Hathi, Nimish Masters, Daniel McCarthy, Patrick Straughn, Amber TI LOW MASSES AND HIGH REDSHIFTS: THE EVOLUTION OF THE MASS-METALLICITY RELATION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: abundances; galaxies: evolution ID STAR-FORMING GALAXIES; DEEP FIELD-SOUTH; OXYGEN ABUNDANCES; LENSED GALAXIES; SPECTROSCOPY; CONSTRAINTS; ORIGIN; Z-SIMILAR-TO-1.0-1.5; SEQUENCE; STELLAR AB We present the first robust measurement of the high redshift mass-metallicity (MZ) relation at 10(8) less than or similar to M/M-circle dot less than or similar to 10(10), obtained by stacking spectra of 83 emission-line galaxies with secure redshifts between 1.3 less than or similar to z less than or similar to 2.3. For these redshifts, infrared grism spectroscopy with the Hubble Space Telescope Wide Field Camera 3 is sensitive to the R-23 metallicity diagnostic: ([OII] lambda lambda 3726, 3729 + [OIII] lambda lambda 4959, 5007)/H beta. Using spectra stacked in four mass quartiles, we find a MZ relation that declines significantly with decreasing mass, extending from 12+log(O/H) = 8.8 at M = 10(9.8) M-circle dot, to 12+log(O/H)= 8.2 at M = 10(8.2)M(circle dot). After correcting for systematic offsets between metallicity indicators, we compare our MZ relation to measurements from the stacked spectra of galaxies with M greater than or similar to 10(9.5)M(circle dot) and z similar to 2.3. Within the statistical uncertainties, our MZ relation agrees with the z similar to 2.3 result, particularly since our somewhat higher metallicities (by around 0.1 dex) are qualitatively consistent with the lower mean redshift (z = 1.76) of our sample. For the masses probed by our data, the MZ relation shows a steep slope which is suggestive of feedback from energy-driven winds, and a cosmological downsizing evolution where high mass galaxies reach the local MZ relation at earlier times. In addition, we show that our sample falls on an extrapolation of the star-forming main sequence (the SFR-M-* relation) at this redshift. This result indicates that grism emission-line selected samples do not have preferentially high star formation rates (SFRs). Finally, we report no evidence for evolution of the mass-metallicity-SFR plane; our stack-averaged measurements show excellent agreement with the local relation. C1 [Henry, Alaina; Straughn, Amber] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Henry, Alaina; Martin, Crystal L.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Scarlata, Claudia; Bedregal, Alejandro G.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. [Dominguez, Alberto; Siana, Brian; Masters, Daniel] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Malkan, Matthew; Ross, Nathaniel] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Atek, Hakim] Ecole Polytech Fed Lausanne, Astrophys Lab, Observ Sauverny, CH-1290 Versoix, Switzerland. [Bedregal, Alejandro G.] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. [Colbert, James W.; Rafelski, Marc] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Teplitz, Harry] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Bunker, Andrew J.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Dressler, Alan; Hathi, Nimish; Masters, Daniel; McCarthy, Patrick] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. RP Henry, A (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 665, Greenbelt, MD 20771 USA. EM alaina.henry@nasa.gov RI Hathi, Nimish/J-7092-2014; OI Hathi, Nimish/0000-0001-6145-5090; Dominguez, Alberto/0000-0002-3433-4610 FU NASA; HST GO [11696, 12284, 12568] FX We acknowledge Dawn Erb, Kate Whitaker and Danielle Berg for helpful discussions. 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. A. H. also acknowledges support from HST GO 11696, 12284, and 12568. NR 45 TC 43 Z9 43 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 20 PY 2013 VL 776 IS 2 AR L27 DI 10.1088/2041-8205/776/2/L27 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 232JO UT WOS:000325490200010 ER PT J AU Meech, KJ Yang, B Kleyna, J Ansdell, M Chiang, HF Hainaut, O Vincent, JB Boehnhardt, H Fitzsimmons, A Rector, T Riesen, T Keane, JV Reipurth, B Hsieh, HH Michaud, P Milani, G Bryssinck, E Ligustri, R Trabatti, R Tozzi, GP Mottola, S Kuehrt, E Bhatt, B Sahu, D Lisse, C Denneau, L Jedicke, R Magnier, E Wainscoat, R AF Meech, Karen J. Yang, Bin Kleyna, Jan Ansdell, Megan Chiang, Hsin-Fang Hainaut, Olivier Vincent, Jean-Baptiste Boehnhardt, Hermann Fitzsimmons, Alan Rector, Travis Riesen, Timm Keane, Jacqueline V. Reipurth, Bo Hsieh, Henry H. Michaud, Peter Milani, Giannantonio Bryssinck, Erik Ligustri, Rolando Trabatti, Roberto Tozzi, Gian-Paolo Mottola, Stefano Kuehrt, Ekkehard Bhatt, Bhuwan Sahu, Devendra Lisse, Carey Denneau, Larry Jedicke, Robert Magnier, Eugene Wainscoat, Richard TI OUTGASSING BEHAVIOR OF C/2012 S1 (ISON) FROM 2011 SEPTEMBER TO 2013 JUNE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE comets: general; comets: individual (ISON) ID DIGITAL SKY SURVEY; COMET SCHWASSMANN-WACHMANN-1; HALE-BOPP; NUCLEUS; GEOLOGY; SYSTEM; SHAPE AB We report photometric observations for comet C/2012 S1 (ISON) obtained during the time period immediately after discovery (r = 6.28 AU) until it moved into solar conjunction in mid-2013 June using the UH2.2 m, and Gemini North 8 m telescopes on Mauna Kea, the Lowell 1.8 m in Flagstaff, the Calar Alto 1.2 m telescope in Spain, the VYSOS-5 telescopes on Mauna Loa Hawaii and data from the CARA network. Additional pre-discovery data from the Pan STARRS1 survey extends the light curve back to 2011 September 30 (r = 9.4 AU). The images showed a similar tail morphology due to small micron sized particles throughout 2013. Observations at submillimeter wavelengths using the James Clerk Maxwell Telescope on 15 nights between 2013 March 9 (r = 4.52 AU) and June 16 (r = 3.35 AU) were used to search for CO and HCN rotation lines. No gas was detected, with upper limits for CO ranging between 3.5-4.5 x 10(27) molecules s(-1). Combined with published water production rate estimates we have generated ice sublimation models consistent with the photometric light curve. The inbound light curve is likely controlled by sublimation of CO2. At these distances water is not a strong contributor to the outgassing. We also infer that there was a long slow outburst of activity beginning in late 2011 peaking in mid-2013 January (r similar to 5 AU) at which point the activity decreased again through 2013 June. We suggest that this outburst was driven by CO injecting large water ice grains into the coma. Observations as the comet came out of solar conjunction seem to confirm our models. C1 [Meech, Karen J.; Yang, Bin; Kleyna, Jan; Chiang, Hsin-Fang; Riesen, Timm; Keane, Jacqueline V.; Reipurth, Bo; Hsieh, Henry H.] NASA, Astrobiol Inst, Honolulu, HI 96822 USA. [Meech, Karen J.; Yang, Bin; Kleyna, Jan; Ansdell, Megan; Chiang, Hsin-Fang; Riesen, Timm; Keane, Jacqueline V.; Reipurth, Bo; Denneau, Larry; Jedicke, Robert; Magnier, Eugene; Wainscoat, Richard] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Hainaut, Olivier] European So Observ, Santiago 19001, Chile. [Vincent, Jean-Baptiste; Boehnhardt, Hermann] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Fitzsimmons, Alan] Queens Univ Belfast, Belfast BT7 1NN, Antrim, North Ireland. [Rector, Travis] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA. [Michaud, Peter] Northern Operat Ctr, Gemini Observ, Hilo, HI 96720 USA. [Milani, Giannantonio] Associaz Astronom Euganea, I-35131 Padua, Italy. [Bryssinck, Erik] BRIXIIS Observ, B-9150 Kruibeke, Belgium. [Ligustri, Rolando] Talmassons Observ CAST, I-33030 Talmassons, Italy. [Trabatti, Roberto] Staz Astronom Descartes, I-2013 Chignolo Po, Italy. [Tozzi, Gian-Paolo] INAF Osservatorio Astrofis Arcetri, I-40125 Florence, Italy. [Mottola, Stefano; Kuehrt, Ekkehard] Inst Planetary Res, DLR German Aerosp Ctr, D-12489 Berlin, Germany. [Bhatt, Bhuwan; Sahu, Devendra] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Lisse, Carey] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. IASF INAF, CARA Project, I-00133 Rome, Italy. RP Meech, KJ (reprint author), NASA, Astrobiol Inst, Honolulu, HI 96822 USA. EM meech@ifa.hawaii.edu RI Lisse, Carey/B-7772-2016 OI Lisse, Carey/0000-0002-9548-1526 FU NASA [NNX08AR22G, HF-51274.01, NAS 5-26555]; NSF [AST-123886, 1010059]; Univ. of MD; Eotvos Lorand Univ; NASA Astrobiology Institute [NNA08DA77A]; Space Telescope Science Institute FX Gemini is operated by AURA under a cooperative agreement with the NSF on behalf of the Gemini partnership. The James Clerk Maxell Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, and the National Research Council of Canada. Data were acquired using the PS1 System operated by the PS1 Science Consortium (PS1SC) and its member institutions. The Pan-STARRS1 Surveys (PS1) have been made possible by contributions from PS1SC member Institutions and NASA through Grant NNX08AR22G, the NSF under Grant No. AST-123886, the Univ. of MD, and Eotvos Lorand Univ. B.Y., T. R. and K.J.M. acknowledge support through the NASA Astrobiology Institute under Cooperative Agreement NNA08DA77A. H. H. H. is supported by NASA through Hubble Fellowship grant HF-51274.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy for NASA, under contract NAS 5-26555. J.K. and J.V.K. acknowledge support through NSF grant number 1010059. We also thank the following CARA observers for their contributions: Giovanni Sostero, Ernesto Guido, Nick Howes, Martino Nicolini, Herman Mikuz, Daniele Carosati, Jean Francois Soulier, Man-To Hui, Gianni Galli, Walter Borghini, Paolo Bacci and Diego Tirelli. NR 30 TC 12 Z9 12 U1 0 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 20 PY 2013 VL 776 IS 2 AR L20 DI 10.1088/2041-8205/776/2/L20 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 232JO UT WOS:000325490200003 ER PT J AU Singer, LP Cenko, SB Kasliwal, MM Perley, DA Ofek, EO Brown, DA Nugent, PE Kulkarni, SR Corsi, A Frail, DA Bellm, E Mulchaey, J Arcavi, I Barlow, T Bloom, JS Cao, Y Gehrels, N Horesh, A Masci, FJ McEnery, J Rau, A Surace, JA Yaron, O AF Singer, Leo P. Cenko, S. Bradley Kasliwal, Mansi M. Perley, Daniel A. Ofek, Eran O. Brown, Duncan A. Nugent, Peter E. Kulkarni, S. R. Corsi, Alessandra Frail, Dale A. Bellm, Eric Mulchaey, John Arcavi, Iair Barlow, Tom Bloom, Joshua S. Cao, Yi Gehrels, Neil Horesh, Assaf Masci, Frank J. McEnery, Julie Rau, Arne Surace, Jason A. Yaron, Ofer TI DISCOVERY AND REDSHIFT OF AN OPTICAL AFTERGLOW IN 71 deg(2): iPTF13bxl AND GRB 130702A SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma-ray burst: individual (GRB 130702A) ID GAMMA-RAY BURST; 28 FEBRUARY 1997; LIGHT CURVES; ERROR BOX; SUPERNOVA; SWIFT; REPOSITORY; TELESCOPE; SPECTRA; MISSION AB We report the discovery of the optical afterglow of the gamma-ray burst (GRB) 130702A, identified upon searching 71 deg(2) surrounding the Fermi Gamma-ray Burst Monitor (GBM) localization. Discovered and characterized by the intermediate Palomar Transient Factory, iPTF13bxl is the first afterglow discovered solely based on a GBM localization. Real-time image subtraction, machine learning, human vetting, and rapid response multi-wavelength follow-up enabled us to quickly narrow a list of 27,004 optical transient candidates to a single afterglow-like source. Detection of a new, fading X-ray source by Swift and a radio counterpart by CARMA and the Very Large Array confirmed the association between iPTF13bxl and GRB 130702A. Spectroscopy with the Magellan and Palomar 200 inch telescopes showed the afterglow to be at a redshift of z = 0.145, placing GRB 130702A among the lowest redshift GRBs detected to date. The prompt gamma-ray energy release and afterglow luminosity are intermediate between typical cosmological GRBs and nearby sub-luminous events such as GRB 980425 and GRB 060218. The bright afterglow and emerging supernova offer an opportunity for extensive panchromatic follow-up. Our discovery of iPTF13bxl demonstrates the first observational proof-of-principle for similar to 10 Fermi-iPTF localizations annually. Furthermore, it represents an important step toward overcoming the challenges inherent in uncovering faint optical counterparts to comparably localized gravitational wave events in the Advanced LIGO and Virgo era. C1 [Singer, Leo P.; Brown, Duncan A.] CALTECH, LIGO Lab, Pasadena, CA 91125 USA. [Cenko, S. Bradley; Gehrels, Neil; McEnery, Julie] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Kasliwal, Mansi M.; Mulchaey, John] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Perley, Daniel A.; Kulkarni, S. R.; Bellm, Eric; Barlow, Tom; Cao, Yi; Horesh, Assaf] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Ofek, Eran O.; Arcavi, Iair; Yaron, Ofer] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Brown, Duncan A.] Syracuse Univ, Dept Phys, Syracuse, NY 13244 USA. [Nugent, Peter E.; Bloom, Joshua S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Nugent, Peter E.; Bloom, Joshua S.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Corsi, Alessandra] George Washington Univ, Washington, DC 20052 USA. [Frail, Dale A.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Masci, Frank J.; Surace, Jason A.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Rau, Arne] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Singer, LP (reprint author), CALTECH, LIGO Lab, Pasadena, CA 91125 USA. EM lsinger@caltech.edu RI Horesh, Assaf/O-9873-2016; OI Horesh, Assaf/0000-0002-5936-1156; Singer, Leo/0000-0001-9898-5597 FU National Science Foundation [PHY-0847611]; NSF-CDI grant [0941742]; Carnegie-Princeton Fellowship; NASA through the Hubble Fellowship [HST-HF-51293.01, HST-HF-51296.01-A]; Space Telescope Science Institute; NASA [NAS 5-26555]; Israeli Ministry of Science; I-CORE Program; RCSA Cottrell Scholar award FX This research is supported by the National Science Foundation through a Graduate Research Fellowship for L. P. S., award PHY-0847611 for D. A. B., and NSF-CDI grant 0941742 for J.S.B. M. M. K. acknowledges generous support from the Carnegie-Princeton Fellowship. M. M. K. and D. A. P. are supported by NASA through the Hubble Fellowship grants HST-HF-51293.01 and HST-HF-51296.01-A, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. E.O.O. is the incumbent of the Arye Dissentshik career development chair and is supported by grants from the Israeli Ministry of Science and the I-CORE Program. D. A. B. is further supported by an RCSA Cottrell Scholar award. NR 39 TC 22 Z9 24 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 20 PY 2013 VL 776 IS 2 AR L34 DI 10.1088/2041-8205/776/2/L34 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 232JO UT WOS:000325490200017 ER PT J AU Graettinger, AH Ellis, MK Skilling, IP Reath, K Ramsey, MS Lee, RJ Hughes, CG McGarvie, DW AF Graettinger, A. H. Ellis, M. K. Skilling, I. P. Reath, K. Ramsey, M. S. Lee, R. J. Hughes, C. G. McGarvie, D. W. TI Remote sensing and geologic mapping of glaciovolcanic deposits in the region surrounding Askja (Dyngjufjoll) volcano, Iceland SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID TABLE MOUNTAINS; 1875 ERUPTION; DRY PHASES; FLOW; BEZYMIANNY; EVOLUTION; DYNAMICS; ASTER; FIELD; WET AB The surface geology of the Northern Volcanic Zone in Iceland is dominated by volcanic ridges, central volcanoes, shield volcanoes, and tuyas. The largest features are typically ice-confined (glaciovolcanic) in origin, and are overlain by voluminous Holocene (subaerial) lavas and glacial outwash deposits. The literature has focused heavily on prominent or very young features, neglecting small and older volcanic features. The purpose of this study is to demonstrate the application of remote-sensing mapping techniques to the glaciovolcanic environment in order to identify dominant lithologies and determine locations for textural, stratigraphic, and age studies. The deposits targeted in this study occur on and around Askja volcano, in central Iceland, including Pleistocene glaciovolcanic tuffs and subaerial pumice from the 1875 rhyolitic eruption of Askja. Data from the Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) were used in conjunction with previously published geologic and remote-sensing data sets and recent field work on glaciovolcanic deposits of Askja for validation. Remotely acquired data sets include aerial photographs and one ASTER scene obtained in August 2010. Visible and near-infrared (VNIR) and thermal infrared (TIR) classifications and linear deconvolution of the TIR emissivity data were performed using end-members derived from regions of interest and laboratory spectra. End-members were selected from samples of representative lithologic units within the field area, including glaciovolcanic deposits (pillow lavas, tuffs, etc.), historical deposits (1875 pumice, 1920s basaltic lavas), and Holocene basaltic lavas from Askja. The results demonstrate the potential for remote sensing-based ground cover mapping of areas of glaciovolcanic deposits relevant to palaeo-ice reconstructions in areas such as Iceland, Antarctica, and British Columbia. Remote sensing-based mapping will benefit glaciovolcanic studies, by determining the lithologic variability of these relatively inaccessible massifs and serving as an important springboard for the identification of future field sites in remote areas. C1 [Graettinger, A. H.; Ellis, M. K.; Reath, K.; Ramsey, M. S.; Lee, R. J.] Univ Pittsburgh, Dept Geol & Planetary Sci, Pittsburgh, PA 15260 USA. [Skilling, I. P.] Univ South Wales, Energy & Environm Res Inst, Pontypridd, M Glam, Wales. [Hughes, C. G.] JPL, Pasadena, CA USA. [McGarvie, D. W.] Open Univ, Dept Environm Earth & Ecosyst, Edinburgh, Midlothian, Scotland. RP Graettinger, AH (reprint author), SUNY Buffalo, Ctr Geohazard Studies, Buffalo, NY 14260 USA. EM agraettinger@gmail.com RI Reath, Kevin/B-2866-2017 OI Reath, Kevin/0000-0003-1843-8046 FU NSF FX Field work logistics were made possible by the Vatnajokull National Park Iceland, the University of Iceland, and a NSF grant to IPS. ASTER global DEM is a product of METI and NASA. The manuscript was improved by two anonymous reviewers. NR 35 TC 3 Z9 3 U1 5 U2 66 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0143-1161 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PD OCT 20 PY 2013 VL 34 IS 20 BP 7178 EP 7198 DI 10.1080/01431161.2013.817716 PG 21 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 196IL UT WOS:000322767600014 ER PT J AU Lee, JH Biging, GS Radke, JD Fisher, JB AF Lee, Jun-Hak Biging, Gregory S. Radke, John D. Fisher, Joshua B. TI An improved topographic mapping technique from airborne lidar: application in a forested hillside SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID SMALL-FOOTPRINT LIDAR; DIGITAL ELEVATION MODELS; LASER SCANNER DATA; ALTIMETRY DATA; TERRAIN; EXTRACTION; ALGORITHM; CANOPY; GENERATION; ACCURACY AB We developed a robust method to reconstruct a digital terrain model (DTM) by classifying raw light detection and ranging (lidar) points into ground and non-ground points with the help of the Progressive Terrain Fragmentation (PTF) method. PTF applies iterative steps for searching terrain points by approximating terrain surfaces using the triangulated irregular network (TIN) model constructed from ground return points. Instead of using absolute slope or offset distance, PTF uses orthogonal distance and relative angle between a triangular plane and a node. Due to this characteristic, PTF was able to classify raw lidar points into ground and non-ground points on a heterogeneous steep forested area with a small number of parameters. We tested this approach by using a lidar data set covering a part of the Angelo Coast Range Reserve on the South Fork of the Eel River in Mendocino County, California, USA. We used systematically positioned 16 reference plots to determine the optimal parameter that can be used to separate ground and non-ground points from raw lidar point clouds. We tested at different admissible hillslope angles (15 degrees to 20 degrees), and the minimum total error (1.6%) was acquired at the angle value of 18 degrees. Because classifying raw lidar points into ground and non-ground points is the basis for other types of analyses, we expect that our study will provide more accurate terrain approximation and contribute to improving the extraction of other forest biophysical parameters. C1 [Lee, Jun-Hak; Biging, Gregory S.] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Radke, John D.] Univ Calif Berkeley, Dept Landscape Architecture & Environm Planning, Berkeley, CA 94720 USA. [Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Lee, JH (reprint author), Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. EM jhlee@berkeley.edu OI Fisher, Joshua/0000-0003-4734-9085 FU National Aeronautics and Space Administration; W.S. Rosecrans Fellowship, Environmental Science, Policy, and Management, University of California, Berkeley FX We gratefully acknowledge the use of lidar data sets supplied by Dr William E. Dietrich and the National Center of Airborne Laser Mapping (NCALM). J.H. Lee was funded by the W.S. Rosecrans Fellowship, Environmental Science, Policy, and Management, University of California, Berkeley. Dr Joshua B. Fisher contributed to this paper through work in the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 53 TC 1 Z9 2 U1 3 U2 40 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0143-1161 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PD OCT 20 PY 2013 VL 34 IS 20 BP 7293 EP 7311 DI 10.1080/01431161.2013.817710 PG 19 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 196IL UT WOS:000322767600020 ER PT J AU Huber, D Carter, JA Barbieri, M Miglio, A Deck, KM Fabrycky, DC Montet, BT Buchhave, LA Chaplin, WJ Hekker, S Montalban, J Sanchis-Ojeda, R Basu, S Bedding, TR Campante, TL Christensen-Dalsgaard, J Elsworth, YP Stello, D Arentoft, T Ford, EB Gilliland, RL Handberg, R Howard, AW Isaacson, H Johnson, JA Karoff, C Kawaler, SD Kjeldsen, H Latham, DW Lund, MN Lundkvist, M Marcy, GW Metcalfe, TS Aguirre, VS Winn, JN AF Huber, Daniel Carter, Joshua A. Barbieri, Mauro Miglio, Andrea Deck, Katherine M. Fabrycky, Daniel C. Montet, Benjamin T. Buchhave, Lars A. Chaplin, William J. Hekker, Saskia Montalban, Josefina Sanchis-Ojeda, Roberto Basu, Sarbani Bedding, Timothy R. Campante, Tiago L. Christensen-Dalsgaard, Jorgen Elsworth, Yvonne P. Stello, Dennis Arentoft, Torben Ford, Eric B. Gilliland, Ronald L. Handberg, Rasmus Howard, Andrew W. Isaacson, Howard Johnson, John Asher Karoff, Christoffer Kawaler, Steven D. Kjeldsen, Hans Latham, David W. Lund, Mikkel N. Lundkvist, Mia Marcy, Geoffrey W. Metcalfe, Travis S. Aguirre, Victor Silva Winn, Joshua N. TI Stellar Spin-Orbit Misalignment in a Multiplanet System SO SCIENCE LA English DT Article ID RED-GIANT STARS; EXOPLANETARY SYSTEMS; PLANETARY SYSTEM; ROTATION AXIS; HOT STARS; ALIGNMENT; KEPLER; OBLIQUITIES; MODES; TRANSIT AB Stars hosting hot Jupiters are often observed to have high obliquities, whereas stars with multiple coplanar planets have been seen to have low obliquities. This has been interpreted as evidence that hot-Jupiter formation is linked to dynamical disruption, as opposed to planet migration through a protoplanetary disk. We used asteroseismology to measure a large obliquity for Kepler-56, a red giant star hosting two transiting coplanar planets. These observations show that spin-orbit misalignments are not confined to hot-Jupiter systems. Misalignments in a broader class of systems had been predicted as a consequence of torques from wide-orbiting companions, and indeed radial velocity measurements revealed a third companion in a wide orbit in the Kepler-56 system. C1 [Huber, Daniel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Carter, Joshua A.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barbieri, Mauro] Univ Padua, CISAS, I-35131 Padua, Italy. [Miglio, Andrea; Chaplin, William J.; Campante, Tiago L.; Elsworth, Yvonne P.; Handberg, Rasmus] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Miglio, Andrea; Chaplin, William J.; Bedding, Timothy R.; Campante, Tiago L.; Christensen-Dalsgaard, Jorgen; Elsworth, Yvonne P.; Stello, Dennis; Arentoft, Torben; Handberg, Rasmus; Karoff, Christoffer; Kjeldsen, Hans; Lund, Mikkel N.; Lundkvist, Mia; Metcalfe, Travis S.; Aguirre, Victor Silva] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Deck, Katherine M.; Sanchis-Ojeda, Roberto; Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Fabrycky, Daniel C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Montet, Benjamin T.; Johnson, John Asher] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Hekker, Saskia] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Montalban, Josefina] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Bedding, Timothy R.; Stello, Dennis] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Ford, Eric B.; Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32111 USA. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Isaacson, Howard; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Kawaler, Steven D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Metcalfe, Travis S.] Space Sci Inst, Boulder, CO 80301 USA. RP Huber, D (reprint author), NASA, Ames Res Ctr, MS 244-30, Moffett Field, CA 94035 USA. EM daniel.huber@nasa.gov RI Karoff, Christoffer/L-1007-2013; Basu, Sarbani/B-8015-2014; OI Kawaler, Steven/0000-0002-6536-6367; Fabrycky, Daniel/0000-0003-3750-0183; Karoff, Christoffer/0000-0003-2009-7965; Basu, Sarbani/0000-0002-6163-3472; Handberg, Rasmus/0000-0001-8725-4502; Montet, Benjamin/0000-0001-7516-8308; Barbieri, Mauro/0000-0001-8362-3462; Buchhave, Lars A./0000-0003-1605-5666; Bedding, Timothy/0000-0001-5943-1460; Metcalfe, Travis/0000-0003-4034-0416; Bedding, Tim/0000-0001-5222-4661; Lund, Mikkel Norup/0000-0001-9214-5642; Lundkvist, Mia Sloth/0000-0002-8661-2571 FU NASA's Science Mission Directorate; NASA; NSF [DGE1144469, AST-1105930]; Netherlands Organisation for Scientific Research; BELSPO for contract PRODEX COROT; NASA Kepler Participating Scientist program; David and Lucile Packard foundation; Alfred P. Sloan foundation; Danish National Research Foundation [DNRF106]; ASTERISK; European Research Council [267864] FX We gratefully acknowledge the entire Kepler team for making this paper possible. Funding for the Kepler Mission is provided by NASA's Science Mission Directorate. We thank E. Agol and D. Raggozine for helpful comments on the manuscript. Supported by an appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA (D. H.); a NSF Graduate Research Fellowship (K. M. D.); a NSF Graduate Research Fellowship under grant DGE1144469 (B. T. M.); the Netherlands Organisation for Scientific Research (S. H.); BELSPO for contract PRODEX COROT (J.M.); the NASA Kepler Participating Scientist program (R.S.-O., J.N.W., and E. B. F.); NSF grant AST-1105930 (S. B.); and the David and Lucile Packard and Alfred P. Sloan foundations (J.A.J.). J.A.C. is a Hubble Fellow of the Harvard-Smithsonian Center for Astrophysics. Funding for the Stellar Astrophysics Centre is provided by Danish National Research Foundation grant DNRF106. The research is supported by the ASTERISK (Asteroseismic Investigations with SONG and Kepler) project funded by the European Research Council (grant agreement 267864). NR 30 TC 89 Z9 89 U1 0 U2 9 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 OCT 18 PY 2013 VL 342 IS 6156 BP 331 EP 334 DI 10.1126/science.1242066 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 235XG UT WOS:000325755100036 PM 24136961 ER PT J AU Shannon, RM Ravi, V Coles, WA Hobbs, G Keith, MJ Manchester, RN Wyithe, JSB Bailes, M Bhat, NDR Burke-Spolaor, S Khoo, J Levin, Y Oslowski, S Sarkissian, JM van Straten, W Verbiest, JPW Wang, JB AF Shannon, R. M. Ravi, V. Coles, W. A. Hobbs, G. Keith, M. J. Manchester, R. N. Wyithe, J. S. B. Bailes, M. Bhat, N. D. R. Burke-Spolaor, S. Khoo, J. Levin, Y. Oslowski, S. Sarkissian, J. M. van Straten, W. Verbiest, J. P. W. Wang, J. -B. TI Gravitational-Wave Limits from Pulsar Timing Constrain Supermassive Black Hole Evolution SO SCIENCE LA English DT Article ID ACTIVE GALACTIC NUCLEI; BINARY EVOLUTION; GALAXIES; ARRAY; SIMULATION; COSMOLOGY; PACKAGE; TEMPO2; BAND AB The formation and growth processes of supermassive black holes (SMBHs) are not well constrained. SMBH population models, however, provide specific predictions for the properties of the gravitational-wave background (GWB) from binary SMBHs in merging galaxies throughout the universe. Using observations from the Parkes Pulsar Timing Array, we constrain the fractional GWB energy density (Omega(GW)) with 95% confidence to be Omega(GW)(H-0/73 kilometers per second per megaparsec)(2) < 1.3 x 10(-9) (where H-0 is the Hubble constant) at a frequency of 2.8 nanohertz, which is approximately a factor of 6 more stringent than previous limits. We compare our limit to models of the SMBH population and find inconsistencies at confidence levels between 46 and 91%. For example, the standard galaxy formation model implemented in the Millennium Simulation Project is inconsistent with our limit with 50% probability. C1 [Shannon, R. M.; Ravi, V.; Hobbs, G.; Keith, M. J.; Manchester, R. N.; Khoo, J.; Wang, J. -B.] Commonwealth Sci & Ind Res Org CSIRO Astron & Spa, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Ravi, V.; Wyithe, J. S. B.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Coles, W. A.] Univ Calif San Diego, Dept Elect & Comp Engn, La Jolla, CA 92093 USA. [Bailes, M.; Bhat, N. D. R.; Oslowski, S.; van Straten, W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Bhat, N. D. R.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Burke-Spolaor, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Khoo, J.] CSIRO Adv Sci Comp Informat Management & Technol, Clayton, Vic 3169, Australia. [Levin, Y.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Sarkissian, J. M.] CSIRO Astron & Space Sci, Parkes Observ, Parkes, NSW 2870, Australia. [Verbiest, J. P. W.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Wang, J. -B.] Chinese Acad Sci, Xinjiang Astron Observ, Urumqi 830011, Xinjiang, Peoples R China. RP Shannon, RM (reprint author), Commonwealth Sci & Ind Res Org CSIRO Astron & Spa, Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia. EM ryan.shannon@csiro.au; v.ravi@pgrad.unimelb.edu.au OI Wyithe, Stuart/0000-0001-7956-9758; Shannon, Ryan/0000-0002-7285-6348; van Straten, Willem/0000-0003-2519-7375; Oslowski, Stefan/0000-0003-0289-0732 FU Commonwealth of Australia for operation; R.N.M.'s Australian Research Council (ARC) Federation Fellowship [FF0348478]; CSIRO; ARC [DP0985272]; John Stocker Postgraduate Scholarship from the Science and Industry Endowment Fund; ARC QEII Fellowship [DP0878388]; Australian Research Council Laureate Fellowship; NASA; European Research Council (ERC) for the ERC Starting Grant Beacon [279202] FX We thank all of the observers, engineers, and Parkes observatory staff members who have assisted with the observations reported in this paper. We thank N. McConnell for providing and confirming some dynamical SMBH and bulge mass measurements, S. Mutch for discussions on the Millennium-based model, and X.-J. Zhu for comments on the manuscript. The Parkes radio telescope 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. The Millennium and Millennium-II Simulation databases used in this paper and the Web application providing online access to these databases were constructed as part of the activities of the German Astrophysical Virtual Observatory. The PPTA project was initiated with support from R.N.M.'s Australian Research Council (ARC) Federation Fellowship (no. FF0348478) and from the CSIRO under that fellowship program. The PPTA project has also received support from ARC Discovery Project grant no. DP0985272. V. R. is a recipient of a John Stocker Postgraduate Scholarship from the Science and Industry Endowment Fund, G. H. is the recipient of an ARC QEII Fellowship (no. DP0878388), and J.S.B.W. acknowledges an Australian Research Council Laureate Fellowship. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. J.P.W.V. acknowledges the financial support by the European Research Council (ERC) for the ERC Starting Grant Beacon under contract no. 279202. The authors declare no conflicts of interest. Data used in this analysis can be accessed via the Australia National Data Service (www.ands.org.au). NR 27 TC 73 Z9 74 U1 2 U2 19 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 OCT 18 PY 2013 VL 342 IS 6156 BP 334 EP 337 DI 10.1126/science.1238012 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 235XG UT WOS:000325755100037 PM 24136962 ER PT J AU Webster, CR Mahaffy, PR Atreya, SK Flesch, GJ Farley, KA AF Webster, Christopher R. Mahaffy, Paul R. Atreya, Sushil K. Flesch, Gregory J. Farley, Kenneth A. CA MSL Sci Team TI Low Upper Limit to Methane Abundance on Mars SO SCIENCE LA English DT Article ID MARTIAN DUST DEVILS; OXIDANT ENHANCEMENT; ATMOSPHERE; ORIGIN; LIFE; HABITABILITY; SEARCH; STORMS; AIR AB By analogy with Earth, methane in the Martian atmosphere is a potential signature of ongoing or past biological activity. During the past decade, Earth-based telescopic observations reported "plumes" of methane of tens of parts per billion by volume (ppbv), and those from Mars orbit showed localized patches, prompting speculation of sources from subsurface bacteria or nonbiological sources. From in situ measurements made with the Tunable Laser Spectrometer (TLS) on Curiosity using a distinctive spectral pattern specific to methane, we report no detection of atmospheric methane with a measured value of 0.18 +/- 0.67 ppbv corresponding to an upper limit of only 1.3 ppbv (95% confidence level), which reduces the probability of current methanogenic microbial activity on Mars and limits the recent contribution from extraplanetary and geologic sources. C1 [Webster, Christopher R.; Flesch, Gregory J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mahaffy, Paul R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Atreya, Sushil K.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Farley, Kenneth A.] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Webster, CR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM chris.r.webster@jpl.nasa.gov RI szopa, cyril/C-6865-2015; Martin-Torres, Francisco Javier/G-6329-2015; Blanco, Juan Jose/E-3627-2014; Harri, Ari-Matti/C-7142-2012; Zorzano, Maria-Paz/F-2184-2015; Dworkin, Jason/C-9417-2012; Hayes, Alexander/P-2024-2014; Zorzano, Maria-Paz/C-5784-2015; Gonzalez, Rafael/D-1748-2009; Lemmon, Mark/E-9983-2010; Frydenvang, Jens/D-4781-2013; Balic-Zunic, Tonci/A-6362-2013; de Pablo, Miguel Angel/J-6442-2014; Gomez-Elvira, Javier/K-5829-2014; Ramos, Miguel/K-2230-2014; Gomez, Felipe/L-7315-2014; Rodriguez-Manfredi, Jose/L-8001-2014 OI szopa, cyril/0000-0002-0090-4056; Martin-Torres, Francisco Javier/0000-0001-6479-2236; Blanco, Juan Jose/0000-0002-8666-0696; Harri, Ari-Matti/0000-0001-8541-2802; Zorzano, Maria-Paz/0000-0002-4492-9650; Dworkin, Jason/0000-0002-3961-8997; Muller, Jan-Peter/0000-0002-5077-3736; Hayes, Alexander/0000-0001-6397-2630; Zorzano, Maria-Paz/0000-0002-4492-9650; Lemmon, Mark/0000-0002-4504-5136; Frydenvang, Jens/0000-0001-9294-1227; Balic-Zunic, Tonci/0000-0003-1687-1233; de Pablo, Miguel Angel/0000-0002-4496-2741; Gomez-Elvira, Javier/0000-0002-9068-9846; Ramos, Miguel/0000-0003-3648-6818; Gomez, Felipe/0000-0001-9977-7060; Rodriguez-Manfredi, Jose/0000-0003-0461-9815 FU National Aeronautics and Space Administration (NASA) FX The research described here was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). Data described in the paper are further described in the supplementary materials and have been submitted to NASA's Planetary Data System under an arrangement with the Mars Science Laboratory project. NR 24 TC 38 Z9 41 U1 9 U2 108 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 OCT 18 PY 2013 VL 342 IS 6156 BP 355 EP 357 DI 10.1126/science.1242902 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 235XG UT WOS:000325755100043 PM 24051245 ER PT J AU Moffat-Griffin, T Jarvis, MJ Colwell, SR Kavanagh, AJ Manney, GL Daffer, WH AF Moffat-Griffin, T. Jarvis, M. J. Colwell, S. R. Kavanagh, A. J. Manney, G. L. Daffer, W. H. TI Seasonal variations in lower stratospheric gravity wave energy above the Falkland Islands SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MIDDLE-ATMOSPHERE; POLAR VORTEX; NUMERICAL SIMULATIONS; MACQUARIE ISLAND; CLIMATOLOGY; CIRCULATION; CONVECTION; ROTORS; MODELS C1 [Moffat-Griffin, T.; Jarvis, M. J.; Colwell, S. R.; Kavanagh, A. J.] British Antarctic Survey, Cambridge CB3 0ET, England. [Manney, G. L.] NorthWest Res Associates, Socorro, NM USA. [Daffer, W. H.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Moffat-Griffin, T (reprint author), British Antarctic Survey, Madingley Rd, Cambridge CB3 0ET, England. EM tmof@bas.ac.uk FU National Aeronautics and Space Administration FX We would like to thank the Met Office for their assistance and guidance in using the radiosonde data set and the BADC for making the data publically available. Thanks to NASA's Global Modelling and Assimilation Office for providing the MERRA reanalysis used in defining polar vortex diagnostics. NCEP Reanalysis data were provided by the NOAA/OAR/ESRL PSD, Boulder, Colorado, USA (http://www.esrl.noaa.gov/psd/). Work at the Jet Propulsion Laboratory, California Institute of Technology was done under contract with the National Aeronautics and Space Administration. NR 49 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 OCT 16 PY 2013 VL 118 IS 19 BP 10861 EP 10869 DI 10.1002/jgrd.50859 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 297PF UT WOS:000330266700013 ER PT J AU Wu, D Dong, XQ Xi, BK Feng, Z Kennedy, A Mullendore, G Gilmore, M Tao, WK AF Wu, Di Dong, Xiquan Xi, Baike Feng, Zhe Kennedy, Aaron Mullendore, Gretchen Gilmore, Matthew Tao, Wei-Kuo TI Impacts of microphysical scheme on convective and stratiform characteristics in two high precipitation squall line events SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID CLOUD-RESOLVING MODEL; NUMERICAL SIMULATIONS; PART I; BULK PARAMETERIZATION; TROPICAL CONVECTION; ISOLATED MICROBURST; SENSITIVITY; ICE; MESOSCALE; DYNAMICS C1 [Wu, Di; Dong, Xiquan; Xi, Baike; Feng, Zhe; Kennedy, Aaron; Mullendore, Gretchen; Gilmore, Matthew] Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58202 USA. [Wu, Di; Tao, Wei-Kuo] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Feng, Zhe] Pacific NW Natl Lab, Richland, WA 99352 USA. RP Dong, XQ (reprint author), Univ N Dakota, Dept Atmospher Sci, 4149 Univ Ave,Stop 9006, Grand Forks, ND 58202 USA. EM dong@aero.und.edu RI Feng, Zhe/D-9531-2013; Feng, Zhe/E-1877-2015; OI Feng, Zhe/0000-0002-7540-9017; Dong, Xiquan/0000-0002-3359-6117 FU U.S. Department of Energy Office of Energy Research, Office of Health and Environmental Research, Environmental Sciences Division; NOAA GOES-R project [NA11NES440004]; DOE ASR project [DE-SC0008468]; NASA EPSCoR CAN [NNX11AM15A]; DOE Atmospheric System Research (ASR) program FX Surface data and Oklahoma Mesonet precipitation were obtained from the Atmospheric Radiation Measurement Program sponsored by the U.S. Department of Energy Office of Energy Research, Office of Health and Environmental Research, Environmental Sciences Division. We are in debt to Song-You Hong from Yonsei University for providing reflectivity calculation algorithm based on WSM6 scheme. Comments from three anonymous reviewers improved the manuscript and are appreciated. We are also very grateful to Samson Hagos at PNNL for his constructive comments. This research was primarily supported by NOAA GOES-R project managed by Ingrid Guch and Mark DeMaria with award NA11NES440004 at the University of North Dakota. The University of North Dakota authors were also supported by DOE ASR project with award number DE-SC0008468, and NASA EPSCoR CAN under grant NNX11AM15A. The PNNL author is also supported by the DOE Atmospheric System Research (ASR) program. NR 50 TC 13 Z9 13 U1 1 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 OCT 16 PY 2013 VL 118 IS 19 BP 11119 EP 11135 DI 10.1002/jgrd.50798 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 297PF UT WOS:000330266700044 ER PT J AU Li, SS Garay, MJ Chen, LF Rees, E Liu, Y AF Li, Shenshen Garay, Michael J. Chen, Liangfu Rees, Erika Liu, Yang TI Comparison of GEOS-Chem aerosol optical depth with AERONET and MISR data over the contiguous United States SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MATTER COMPONENT CONCENTRATIONS; REMOTE-SENSING OBSERVATIONS; FIRE EMISSIONS; IMPROVED ALGORITHM; NORTH-AMERICA; MINERAL DUST; SATELLITE; THICKNESS; MODEL; RETRIEVALS C1 [Li, Shenshen; Chen, Liangfu] Chinese Acad Sci, Inst Remote Sensing & Digital Earth, State Key Lab Remote Sensing Sci, Beijing, Peoples R China. [Li, Shenshen; Rees, Erika; Liu, Yang] Emory Univ, Rollins Sch Publ Hlth, Atlanta, GA 30322 USA. [Garay, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Liu, Y (reprint author), Emory Univ, Rollins Sch Publ Hlth, 1518 Clifton Rd NE, Atlanta, GA 30322 USA. EM yang.liu@emory.edu RI Chem, GEOS/C-5595-2014 FU National Natural Science Foundation of China [41101400]; Strategic Priority Research Program of the Chinese Academy of Sciences [XDB05020100]; MISR science team at the Jet Propulsion Laboratory [1363692]; NASA Applied Science Program [NNX09AT52G, NNX11AI53G]; NASA; [41130528] FX This work was supported by the National Natural Science Foundation of China for Young Scholar (grant 41101400) and the Key Program (grant 41130528) and the Strategic Priority Research Program of the Chinese Academy of Sciences (grant XDB05020100). We thank the principal investigators (PI) and their staff for establishing and maintaining the AERONET sites used in this investigation. The work of Shenshen Li and Yang Liu is partially supported by the MISR science team at the Jet Propulsion Laboratory led by David Diner (subcontract 1363692) and by NASA Applied Science Program managed by John Haynes (agency grant NNX09AT52G and NNX11AI53G, grant PI: Y. Liu). Portions of this work were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. We acknowledge the technical support of Zhongting Wang and Meng Fan. NR 48 TC 7 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 OCT 16 PY 2013 VL 118 IS 19 BP 11228 EP 11241 DI 10.1002/jgrd.50867 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 297PF UT WOS:000330266700042 ER PT J AU Nedoluha, GE Gomez, RM Allen, DR Lambert, A Boone, C Stiller, G AF Nedoluha, Gerald E. Gomez, R. Michael Allen, Doug R. Lambert, Alyn Boone, Chris Stiller, Gabriele TI Variations in middle atmospheric water vapor from 2004 to 2013 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID STRATOSPHERIC WATER; TROPICAL TROPOPAUSE; TEMPERATURE; VALIDATION; CIRCULATION; MESOSPHERE; HUMIDITY; MIPAS; SPECTROMETER; PROFILES C1 [Nedoluha, Gerald E.; Gomez, R. Michael] Naval Res Lab, Washington, DC 20375 USA. [Allen, Doug R.; Lambert, Alyn] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Boone, Chris] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. [Stiller, Gabriele] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-76021 Karlsruhe, Germany. RP Nedoluha, GE (reprint author), Naval Res Lab, Washington, DC 20375 USA. EM nedoluha@nrl.navy.mil RI Stiller, Gabriele/A-7340-2013 OI Stiller, Gabriele/0000-0003-2883-6873 FU National Aeronautics and Space Administration; Canadian Space Agency; NASA under the Upper Atmosphere Research Program; Naval Research Laboratory FX We wish to thank S. McDermid, D. Walsh, and T. LeBlanc at Table Mountain and Mauna Loa for their technical assistance. Work at the Jet Propulsion Laboratory, California Institute of Technology, was carried out under a contract with the National Aeronautics and Space Administration. The provision of MIPAS level-1b data by ESA is gratefully acknowledged. Funding for the Atmospheric Chemistry Experiment comes primarily from the Canadian Space Agency. This project was funded by NASA under the Upper Atmosphere Research Program and by the Naval Research Laboratory. NR 38 TC 6 Z9 6 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD OCT 16 PY 2013 VL 118 IS 19 BP 11285 EP 11293 DI 10.1002/jgrd.50834 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 297PF UT WOS:000330266700043 ER PT J AU Fioletov, VE McLinden, CA Krotkov, N Yang, K Loyola, DG Valks, P Theys, N Van Roozendael, M Nowlan, CR Chance, K Liu, X Lee, C Martin, RV AF Fioletov, V. E. McLinden, C. A. Krotkov, N. Yang, K. Loyola, D. G. Valks, P. Theys, N. Van Roozendael, M. Nowlan, C. R. Chance, K. Liu, X. Lee, C. Martin, R. V. TI Application of OMI, SCIAMACHY, and GOME-2 satellite SO2 retrievals for detection of large emission sources SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OZONE MONITORING INSTRUMENT; SULFUR-DIOXIDE; AIR-POLLUTION; ATMOSPHERIC COMPOSITION; MISSION; MEXICO; CHINA; ECOSYSTEM; QUALITY; PLUMES C1 [Fioletov, V. E.; McLinden, C. A.] Environm Canada, Toronto, ON M3H 5T4, Canada. [Krotkov, N.; Yang, K.] NASA Goddard Space Flight Ctr, Lab Atmospher Chem & Dynam, Greenbelt, MD USA. [Yang, K.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Loyola, D. G.; Valks, P.] Deutsch Zentrum Luft & Raumfahrt, Wessling, Germany. [Theys, N.; Van Roozendael, M.] Belgian Inst Space Aeron BIRA IASB, Brussels, Belgium. [Nowlan, C. R.; Martin, R. V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Chance, K.; Liu, X.; Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lee, C.] Korea Meteorol Adm, Natl Inst Meteorol Res, Seoul, South Korea. RP Fioletov, VE (reprint author), Environm Canada, 4905 Dufferin St, Toronto, ON M3H 5T4, Canada. EM Vitali.Fioletov@ec.gc.ca RI Liu, Xiong/P-7186-2014; Martin, Randall/C-1205-2014; Krotkov, Nickolay/E-1541-2012; OI Liu, Xiong/0000-0003-2939-574X; Martin, Randall/0000-0003-2632-8402; Krotkov, Nickolay/0000-0001-6170-6750; Nowlan, Caroline/0000-0002-8718-9752; Fioletov, Vitali/0000-0002-2731-5956; Chance, Kelly/0000-0002-7339-7577 FU NASA Earth Science Division; O3M-SAF project; EUMETSAT; ESA within the TEMIS project; ESA within the SACS project; ESA within the GSE PROMOTE project; Advanced Research on Applied Meteorology of the Korea Meteorological Administration (KMA) FX We acknowledge the NASA Earth Science Division for funding of OMI SO2 product development and analysis. The Dutch-Finnish-built OMI instrument is part of the NASA EOS Aura satellite payload. The OMI project is managed by KNMI and the Netherlands Agency for Aerospace Programs (NIVR). The generation of the GOME-2 SO2 operational products has been funded by the O3M-SAF project with EUMETSAT and national contributions. The SCIAMACHY data product has been developed under ESA funding within the TEMIS, SACS, and GSE PROMOTE projects. The work of one of the coauthors (C.L.) was supported by the Advanced Research on Applied Meteorology of the Korea Meteorological Administration (KMA). NR 58 TC 40 Z9 42 U1 4 U2 36 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 OCT 16 PY 2013 VL 118 IS 19 BP 11399 EP 11418 DI 10.1002/jgrd.50826 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 297PF UT WOS:000330266700027 ER PT J AU Marsh, DR Janches, D Feng, WH Plane, JMC AF Marsh, Daniel R. Janches, Diego Feng, Wuhu Plane, John M. C. TI A global model of meteoric sodium SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MESOSPHERIC NA LAYER; LARGE-APERTURE RADARS; INPUT FUNCTION; UPPER-ATMOSPHERE; HIGH-POWER; 40-DEGREES-N; CLIMATOLOGY; TEMPERATURE; CHEMISTRY; DYNAMICS C1 [Marsh, Daniel R.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Janches, Diego] NASA, Space Weather Lab, GSFC, Greenbelt, MD USA. [Feng, Wuhu; Plane, John M. C.] Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England. RP Marsh, DR (reprint author), Natl Ctr Atmospher Res, Div Atmospher Chem, POB 3000, Boulder, CO 80307 USA. EM marsh@ucar.edu RI Janches, Diego/D-4674-2012; Marsh, Daniel/A-8406-2008; FENG, WUHU/B-8327-2008; Plane, John/C-7444-2015 OI Janches, Diego/0000-0001-8615-5166; Marsh, Daniel/0000-0001-6699-494X; FENG, WUHU/0000-0002-9907-9120; Plane, John/0000-0003-3648-6893 FU National Science Foundation; NSF [ATM-05311464, ATM-0525655, ATM-0634650, AST-0908118]; UK Natural Environment Research Council (NERC) [NE/G019487/1] FX The National Center for Atmospheric Research is operated by the University Corporation for Atmospheric Research under sponsorship of the National Science Foundation. The MIF was developed under NSF Grants ATM-05311464, ATM-0525655, ATM-0634650, and AST-0908118 to NorthWest Research Associates. We also acknowledge support by the UK Natural Environment Research Council (NERC grant NE/G019487/1). NR 45 TC 28 Z9 29 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 OCT 16 PY 2013 VL 118 IS 19 BP 11442 EP 11452 DI 10.1002/jgrd.50870 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 297PF UT WOS:000330266700056 ER PT J AU Verronen, PT Andersson, ME Rodger, CJ Clilverd, MA Wang, SH Turunen, E AF Verronen, Pekka T. Andersson, Monika E. Rodger, Craig J. Clilverd, Mark A. Wang, Shuhui Turunen, Esa TI Comparison of modeled and observed effects of radiation belt electron precipitation on mesospheric hydroxyl and ozone SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SOLAR PROTON EVENTS; MIDDLE ATMOSPHERE C1 [Verronen, Pekka T.; Andersson, Monika E.] Finnish Meteorol Inst, FI-00101 Helsinki, Finland. [Rodger, Craig J.] Univ Otago, Dept Phys, Dunedin, New Zealand. [Clilverd, Mark A.] British Antarctic Survey NERC, Cambridge, England. [Wang, Shuhui] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Turunen, Esa] Univ Oulu, Sodankyla Geophys Observ, Sodankyla, Finland. RP Verronen, PT (reprint author), Finnish Meteorol Inst, POB 503, FI-00101 Helsinki, Finland. EM pekka.verronen@fmi.fi RI Verronen, Pekka/G-6658-2014; Rodger, Craig/A-1501-2011 OI Verronen, Pekka/0000-0002-3479-9071; Rodger, Craig/0000-0002-6770-2707 FU Academy of Finland [136225, 140888]; New Zealand Marsden fund; National Aeronautics and Space Administration FX The work of P.T.V. and M.E.A was supported by the Academy of Finland through projects 136225 and 140888 (SPOC: Significance of Energetic Electron Precipitation to Odd Hydrogen, Ozone, and Climate). C.J.R. was supported by the New Zealand Marsden fund. Research at the Jet Propulsion Laboratory, California Institute of Technology is performed under contract with the National Aeronautics and Space Administration. NR 32 TC 5 Z9 5 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD OCT 16 PY 2013 VL 118 IS 19 BP 11419 EP 11428 DI 10.1002/jgrd.50845 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 297PF UT WOS:000330266700038 ER PT J AU Cucinotta, FA Kim, MHY Chappell, LJ Huff, JL AF Cucinotta, Francis A. Kim, Myung-Hee Y. Chappell, Lori J. Huff, Janice L. TI How Safe Is Safe Enough? Radiation Risk for a Human Mission to Mars SO PLOS ONE LA English DT Article ID CIRCULATORY DISEASE; IONIZING-RADIATION; SPACE EXPLORATION; EXPOSURE; CANCER; IRRADIATION; DEPENDENCE; PARTICLES; MORTALITY; MODEL AB Astronauts on a mission to Mars would be exposed for up to 3 years to galactic cosmic rays (GCR) - made up of high-energy protons and high charge (Z) and energy (E) (HZE) nuclei. GCR exposure rate increases about three times as spacecraft venture out of Earth orbit into deep space where protection of the Earth's magnetosphere and solid body are lost. NASA's radiation standard limits astronaut exposures to a 3% risk of exposure induced death (REID) at the upper 95% confidence interval (CI) of the risk estimate. Fatal cancer risk has been considered the dominant risk for GCR, however recent epidemiological analysis of radiation risks for circulatory diseases allow for predictions of REID for circulatory diseases to be included with cancer risk predictions for space missions. Using NASA's models of risks and uncertainties, we predicted that central estimates for radiation induced mortality and morbidity could exceed 5% and 10% with upper 95% CI near 10% and 20%, respectively for a Mars mission. Additional risks to the central nervous system (CNS) and qualitative differences in the biological effects of GCR compared to terrestrial radiation may significantly increase these estimates, and will require new knowledge to evaluate. C1 [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Space Radiat Program, Houston, TX 77058 USA. [Cucinotta, Francis A.] Univ Nevada, Dept Hlth Phys & Diagnost Sci, Las Vegas, NV 89154 USA. [Kim, Myung-Hee Y.; Chappell, Lori J.; Huff, Janice L.] Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA. RP Cucinotta, FA (reprint author), NASA, Lyndon B Johnson Space Ctr, Space Radiat Program, Houston, TX 77058 USA. EM francis.cucinotta@unlv.edu OI Kim, Myung-Hee/0000-0001-5575-6858 FU NASA Space Radiation Risk Project; University of Nevada Las Vegas FX This work was supported by the NASA Space Radiation Risk Project, and the University of Nevada Las Vegas. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 45 TC 31 Z9 32 U1 5 U2 15 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 OCT 16 PY 2013 VL 8 IS 10 AR e74988 DI 10.1371/journal.pone.0074988 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 239JR UT WOS:000326019400003 PM 24146746 ER PT J AU Gierach, MM Vazquez-Cuervo, J Lee, T Tsontos, VM AF Gierach, Michelle M. Vazquez-Cuervo, Jorge Lee, Tong Tsontos, Vardis M. TI Aquarius and SMOS detect effects of an extreme Mississippi River flooding event in the Gulf of Mexico SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE sea surface salinity; river discharge; Aquarius; SMOS; remote sensing; Gulf of Mexico ID WEST FLORIDA SHELF; WATERS; OCEAN; PLUME AB Sea surface salinity (SSS) measurements from the Aquarius/Satelite de Aplicaciones Cientificas (SAC)-D satellite and Soil Moisture and Ocean Salinity (SMOS) mission were used to document the freshening associated with the record 2011 Mississippi River flooding event in the Gulf of Mexico (GoM). Assessment of the salinity response was aided by additional satellite observations, including chlorophyll-a (chl-a) and ocean surface currents, and a passive tracer simulation. Low SSS values associated with the spreading of the river plume were observed 1-3months after peak river discharge which then receded and became unidentifiable from satellite observations 5months after maximum discharge. The seasonal wind pattern and general circulation of the GoM dramatically impacted the observed salinity response, transporting freshwater eastward along the Gulf coast and entraining low salinity waters into the open GoM. The observed salinity response from Aquarius was consistent with SMOS SSS, chl-a concentrations, and the passive tracer simulation in terms of the pathway and transit time of the river plume spreading. This study is the first successful application of satellite SSS to study salinity variation in marginal seas. C1 [Gierach, Michelle M.; Vazquez-Cuervo, Jorge; Lee, Tong; Tsontos, Vardis M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gierach, MM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 300-323, Pasadena, CA 91109 USA. EM michelle.gierach@jpl.nasa.gov OI Gierach, Michelle/0000-0002-8161-4121 FU NASA FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. We would like to acknowledge Ou Wang of JPL for assistance with the ECCO model tracer tool. The LOCEAN_v2013 Sea Surface Salinity maps have been produced by LOCEAN/IPSL (UMR CNRS/UPMC/IRD/MNHN) laboratory that participates to the Ocean Salinity Expertise Center (CECOS) of Centre Aval de Traitemenent des Donnees SMOS (CATDS). This product is distributed by the Ocean Salinity Expertise Center (CECOS) of the CNES-IFREMER Centre Aval de Traitemenent des Donnees SMOS (CATDS), at IFREMER, Plouzane (France). We would like to thank Jacqueline Boutin and an anonymous reviewer for all their helpful comments and suggestions. NR 19 TC 26 Z9 26 U1 2 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 OCT 16 PY 2013 VL 40 IS 19 BP 5188 EP 5193 DI 10.1002/grl.50995 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 243JB UT WOS:000326311600039 ER PT J AU Yuan, T Oreopoulos, L AF Yuan, Tianle Oreopoulos, Lazaros TI On the global character of overlap between low and high clouds SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE low cloud; cloud overlap; ice cloud; tropopause; cloud regimes ID OPTICAL-PROPERTIES; LAYER AB The global character of overlap between low and high clouds is examined using active satellite sensors. Low-cloud fraction has a strong land-ocean contrast with oceanic values double those over land. Major low-cloud regimes include not only the eastern ocean boundary stratocumulus and shallow cumulus but also those associated with cold air outbreaks downwind of wintertime continents and land stratus over particular geographic areas. Globally, about 30% of low clouds are overlapped by high clouds. The overlap rate exhibits strong spatial variability ranging from higher than 90% in the tropics to less than 5% in subsidence areas and is anticorrelated with subsidence rate and low-cloud fraction. The zonal mean of vertical separation between cloud layers is never smaller than 5 km and its zonal variation closely follows that of tropopause height, implying a tight connection with tropopause dynamics. Possible impacts of cloud overlap on low clouds are discussed. C1 [Yuan, Tianle; Oreopoulos, Lazaros] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD 20771 USA. [Yuan, Tianle] UMBC, Joint Ctr Environm Technol, Baltimore, MD USA. [Yuan, Tianle] UMBC, Dept Phys, Baltimore, MD USA. RP Yuan, T (reprint author), NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Bldg 33,Rm A306,Mail Code 613, Greenbelt, MD 20771 USA. EM tianle.yuan@nasa.gov RI Oreopoulos, Lazaros/E-5868-2012; Yuan, Tianle/D-3323-2011 OI Oreopoulos, Lazaros/0000-0001-6061-6905; FU NASA's CALIPSO-CloudSat; Radiation Science programs FX The authors acknowledge funding support from NASA's CALIPSO-CloudSat and Radiation Science programs. We also thank the reviewers for helpful comments and suggestions. NR 31 TC 8 Z9 8 U1 5 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 OCT 16 PY 2013 VL 40 IS 19 BP 5320 EP 5326 DI 10.1002/grl.50871 PG 7 WC Geosciences, Multidisciplinary SC Geology GA 243JB UT WOS:000326311600063 ER PT J AU Harding, LB Schultz, IR Goetz, GW Luckenbach, JA Young, G Goetz, FW Swanson, P AF Harding, Louisa B. Schultz, Irvin R. Goetz, Giles W. Luckenbach, J. Adam Young, Graham Goetz, Frederick W. Swanson, Penny TI High-throughput sequencing and pathway analysis reveal alteration of the pituitary transcriptome by 17 alpha-ethynylestradiol (EE2) in female coho salmon, Oncorhynchus kisutch SO AQUATIC TOXICOLOGY LA English DT Article DE Endocrine disruption; Fish reproduction; Pituitary; Gonadotropins; Circadian rhythm; Transcriptomics ID ZEBRAFISH DANIO-RERIO; FOLLICLE-STIMULATING-HORMONE; MINNOWS PIMEPHALES-PROMELAS; ENVIRONMENTAL ENDOCRINE DISRUPTERS; DIFFERENTIAL EXPRESSION ANALYSIS; GRAPHICAL SYSTEMS-MODEL; BETA-SUBUNIT GENE; GROWTH-FACTOR-I; RNA-SEQ DATA; RAINBOW-TROUT AB Considerable research has been done on the effects of endocrine disrupting chemicals (EDCs) on reproduction and gene expression in the brain, liver and gonads of teleost fish, but information on impacts to the pituitary gland are still limited despite its central role in regulating reproduction. The aim of this study was to further our understanding of the potential effects of natural and synthetic estrogens on the brain-pituitary-gonad axis in fish by determining the effects of 17 alpha-ethynylestradiol (EE2) on the pituitary transcriptome. We exposed sub-adult coho salmon (Oncorhynchus kisutch) to 0 or 12 ng EE2/L for up to 6 weeks and effects on the pituitary transcriptome of females were assessed using high-throughput Illumina (R) sequencing, RNA-Seq and pathway analysis. After 1 or 6 weeks, 218 and 670 contiguous sequences (contigs) respectively, were differentially expressed in pituitaries of EE2-exposed fish relative to control. Two of the most highly up- and down-regulated contigs were luteinizing hormone beta subunit (241-fold and 395-fold at 1 and 6 weeks, respectively) and follicle-stimulating hormone beta subunit (-3.4-fold at 6 weeks). Additional contigs related to gonadotropin synthesis and release were differentially expressed in EE2-exposed fish relative to controls. These included contigs involved in gonadotropin releasing hormone (GNRH) and transforming growth factor-beta signaling. There was an over-representation of significantly affected contigs in 33 and 18 canonical pathways at 1 and 6 weeks, respectively, including circadian rhythm signaling, calcium signaling, peroxisome proliferator-activated receptor (PPAR) signaling, PPAR alpha/retinoid x receptor alpha activation, and netrin signaling. Network analysis identified potential interactions between genes involved in circadian rhythm and GNRH signaling, suggesting possible effects of EE2 on timing of reproductive events. Published by Elsevier B.V. C1 [Harding, Louisa B.; Goetz, Giles W.; Young, Graham] Univ Washington, Sch Aquat & Fishery Sci, Seattle, WA 98195 USA. [Schultz, Irvin R.] Pacific NW Natl Lab, Marine Sci Lab, Battelle, Sequim, WA 98382 USA. [Luckenbach, J. Adam; Swanson, Penny] Natl Ocean & Atmospher Adm, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Seattle, WA 98112 USA. [Luckenbach, J. Adam; Young, Graham; Swanson, Penny] Washington State Univ, Ctr Reprod Biol, Pullman, WA 98164 USA. [Goetz, Frederick W.] Natl Ocean & Atmospher Adm, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Manchester Res Stn, Manchester, WA 98353 USA. RP Swanson, P (reprint author), Natl Ocean & Atmospher Adm, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2725 Montlake Blvd E, Seattle, WA 98112 USA. EM penny.swanson@noaa.gov FU Washington Sea Grant Project [RB-49]; Richard T. Whiteleather scholarship; Melvin Anderson Endowed Scholarship in Fisheries; Roy Jensen Research Fellowship; Lauren R. Donaldson Scholarship FX Funding for this project was provided by Washington Sea Grant Project RB-49 and scholarships to Louisa Harding from the Richard T. Whiteleather scholarship, the Melvin Anderson Endowed Scholarship in Fisheries, the Roy Jensen Research Fellowship, and the Lauren R. Donaldson Scholarship. The authors also wish to acknowledge Abby Tillotson, Jon Dickey, and Mollie Middleton for technical assistance with fish sampling and Dr. Josep Planas for valuable comments during the drafting of this manuscript. NR 107 TC 13 Z9 14 U1 7 U2 60 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0166-445X EI 1879-1514 J9 AQUAT TOXICOL JI Aquat. Toxicol. PD OCT 15 PY 2013 VL 142 BP 146 EP 163 DI 10.1016/j.aquatox.2013.07.020 PG 18 WC Marine & Freshwater Biology; Toxicology SC Marine & Freshwater Biology; Toxicology GA 267JM UT WOS:000328093900015 PM 24007788 ER PT J AU Ren, YX Huang, H Xie, GD Ahmed, N Yan, Y Erkmen, BI Chandrasekaran, N Lavery, MPJ Steinhoff, NK Tur, M Dolinar, S Neifeld, M Padgett, MJ Boyd, RW Shapiro, JH Willner, AE AF Ren, Yongxiong Huang, Hao Xie, Guodong Ahmed, Nisar Yan, Yan Erkmen, Baris I. Chandrasekaran, Nivedita Lavery, Martin P. J. Steinhoff, Nicholas K. Tur, Moshe Dolinar, Samuel Neifeld, Mark Padgett, Miles J. Boyd, Robert W. Shapiro, Jeffrey H. Willner, Alan E. TI Atmospheric turbulence effects on the performance of a free space optical link employing orbital angular momentum multiplexing SO OPTICS LETTERS LA English DT Article ID LIGHT; PROPAGATION; CHANNEL; STATES; BEAMS; WAVE AB We experimentally investigate the performance of an orbital angular momentum (OAM) multiplexed free space optical (FSO) communication link through emulated atmospheric turbulence. The turbulence effects on the crosstalk and system power penalty of the FSO link are characterized. The experimental results show that the power of the transmitted OAM mode will tend to spread uniformly onto the neighboring mode in medium-to-strong turbulence, resulting in severe crosstalk at the receiver. The power penalty is found to exceed 10 dB in a weak-to-medium turbulence condition due to the turbulence-induced crosstalk and power fluctuation of the received signal. (C) 2013 Optical Society of America C1 [Ren, Yongxiong; Huang, Hao; Xie, Guodong; Ahmed, Nisar; Yan, Yan; Willner, Alan E.] Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA. [Erkmen, Baris I.; Dolinar, Samuel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chandrasekaran, Nivedita; Shapiro, Jeffrey H.] MIT, Elect Res Lab, Cambridge, MA 02139 USA. [Lavery, Martin P. J.; Padgett, Miles J.] Univ Glasgow, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. [Steinhoff, Nicholas K.] Opt Sci Co, Anaheim, CA 92825 USA. [Tur, Moshe] Tel Aviv Univ, Sch Elect Engn, IL-69978 Tel Aviv, Israel. [Neifeld, Mark] Univ Arizona, Dept Elect & Comp Engn, Tucson, AZ 85721 USA. [Boyd, Robert W.] Univ Rochester, Inst Opt, Dept Phys & Astron, Rochester, NY 14627 USA. RP Ren, YX (reprint author), Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA. EM yongxior@usc.edu RI Padgett, Miles/B-7625-2008; Lavery, Martin/H-2265-2015 OI Padgett, Miles/0000-0001-6643-0618; FU DARPA under the InPho (Information in a Photon) program FX We acknowledge the support of DARPA under the InPho (Information in a Photon) program. NR 18 TC 52 Z9 55 U1 3 U2 39 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 EI 1539-4794 J9 OPT LETT JI Opt. Lett. PD OCT 15 PY 2013 VL 38 IS 20 BP 4062 EP 4065 DI 10.1364/OL.38.004062 PG 4 WC Optics SC Optics GA 246WD UT WOS:000326570300025 PM 24321923 ER PT J AU Dwivedi, P Gazda, DB Keelor, JD Limero, TF Wallace, WT Macatangay, AV Fernandez, FM AF Dwivedi, Prabha Gazda, Daniel B. Keelor, Joel D. Limero, Thomas F. Wallace, William T. Macatangay, Ariel V. Fernandez, Facundo M. TI Electro-Thermal Vaporization Direct Analysis in Real Time-Mass Spectrometry for Water Contaminant Analysis during Space Missions SO ANALYTICAL CHEMISTRY LA English DT Article ID SOLID-PHASE MICROEXTRACTION; ION-SOURCE; EMERGING CONTAMINANTS; ATMOSPHERIC-PRESSURE; IONIZATION SOURCE; CURRENT ISSUES; OPEN-AIR; DERIVATIZATION; ALDEHYDES; DRINKING AB The development of a direct analysis in real time-mass spectrometry (DART-MS) method and first prototype vaporizer for the detection of low molecular weight (similar to 30-100 Da) contaminants representative of those detected in water samples from the International Space Station is reported. A temperature-programmable, electro-thermal vaporizer (ETV) was designed, constructed, and evaluated as a sampling interface for DART-MS. The ETV facilitates analysis of water samples with minimum user intervention while maximizing analytical sensitivity and sample throughput. The integrated DART-ETV-MS methodology was evaluated in both positive and negative ion modes to (1) determine experimental conditions suitable for coupling DART with ETV as a sample inlet and ionization platform for time-of-flight MS, (2) to identify analyte response ions, (3) to determine the detection limit and dynamic range for target analyte measurement, and (4) to determine the reproducibility of measurements made with the method when using manual sample introduction into the vaporizer. Nitrogen was used as the DART working gas, and the target analytes chosen for the study were ethyl acetate, acetone, acetaldehyde, ethanol, ethylene glycol, dimethylsilanediol, formaldehyde, isopropanol, methanol, methylethyl ketone, methylsulfone, propylene glycol, and trimethylsilanol. C1 [Dwivedi, Prabha; Keelor, Joel D.; Fernandez, Facundo M.] Georgia Inst Technol, Sch Chem & Biochem, Atlanta, GA 30332 USA. [Gazda, Daniel B.; Limero, Thomas F.; Wallace, William T.] Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA. [Macatangay, Ariel V.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. RP Fernandez, FM (reprint author), Georgia Inst Technol, Sch Chem & Biochem, Atlanta, GA 30332 USA. EM facundo.fernandez@chemistry.gatech.edu FU NASA [NNX11AR50G] FX This work was supported by NASA Award Number NNX11AR50G to F.M.F.. NR 41 TC 10 Z9 10 U1 2 U2 41 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 OCT 15 PY 2013 VL 85 IS 20 BP 9898 EP 9906 DI 10.1021/ac402365k PG 9 WC Chemistry, Analytical SC Chemistry GA 240VU UT WOS:000326126600067 PM 24050110 ER PT J AU Choudhary, DP Gosain, S Gopalswamy, N Manoharan, PK Chandra, R Uddin, W Srivastava, AK Yashiro, S Joshi, NC Kayshap, P Dwivedi, VC Mahalakshmi, K Elamathi, E Norris, M Awasthi, AK Jain, R AF Choudhary, Debi Prasad Gosain, Sanjay Gopalswamy, Nat Manoharan, P. K. Chandra, R. Uddin, W. Srivastava, A. K. Yashiro, S. Joshi, N. C. Kayshap, P. Dwivedi, V. C. Mahalakshmi, K. Elamathi, E. Norris, Max Awasthi, A. K. Jain, R. TI Flux emergence, flux imbalance, magnetic free energy and solar flares SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Flux emergence; Flux imbalance; Magnetic free energy; Sunspot area; Solar flare ID CORONAL MASS EJECTION; ACTIVE REGIONS; EMERGING FLUX; QUIET SUN; FIELDS; INTENSITY AB Emergence of complex magnetic flux in the solar active regions lead to several observational effects such as a change in sunspot area and flux embalance in photospheric magnetograms. The flux emergence also results in twisted magnetic field lines that add to free energy content. The magnetic field configuration of these active regions relax to near potential-field configuration after energy release through solar flares and coronal mass ejections. In this paper, we study the relation of flare productivity of active regions with their evolution of magnetic flux emergence, flux imbalance and free energy content. We use the sunspot area and number for flux emergence study as they contain most of the concentrated magnetic flux in the active region. The magnetic flux imbalance and the free energy are estimated using the HMI/SDO magnetograms and Virial theorem method. We find that the active regions that undergo large changes in sunspot area are most flare productive. The active regions become flary when the free energy content exceeds 50% of the total energy. Although, the flary active regions show magnetic flux imbalance, it is hard to predict flare activity based on this parameter alone. (C) 2013 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Choudhary, Debi Prasad; Norris, Max] Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA. [Gosain, Sanjay] Natl Opt Astron Observ, Natl Solar Observ, Tucson, AZ 85726 USA. [Gopalswamy, Nat; Yashiro, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Awasthi, A. K.; Jain, R.] Phys Res Lab, Dept Space, Ahmadabad 380009, Gujarat, India. [Uddin, W.; Srivastava, A. K.; Joshi, N. C.; Kayshap, P.] Aryabhatta Res Inst Observat Sci ARIES, Naini Tal 263129, India. [Chandra, R.] Kumaun Univ, Dept Phys, Naini Tal 263002, India. [Manoharan, P. K.; Dwivedi, V. C.; Mahalakshmi, K.; Elamathi, E.] Tata Inst Fundamental Res, NCRA, Radio Astron Ctr, Udhagamandalam Ooty 643001, India. RP Choudhary, DP (reprint author), Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA. EM debiprasad.choudhary@csun.edu RI Awasthi, Arun/H-5596-2016 OI Awasthi, Arun/0000-0001-5313-1125 NR 48 TC 7 Z9 7 U1 0 U2 8 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 OCT 15 PY 2013 VL 52 IS 8 BP 1561 EP 1566 DI 10.1016/j.asr.2013.07.009 PG 6 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 233TJ UT WOS:000325592100014 ER PT J AU Bollengier, O Choukroun, M Grasset, O Le Menn, E Bellino, G Morizet, Y Bezacier, L Oancea, A Taffin, C Tobie, G AF Bollengier, Olivier Choukroun, Mathieu Grasset, Olivier Le Menn, Erwan Bellino, Guillaume Morizet, Yann Bezacier, Lucile Oancea, Adriana Taffin, Cecile Tobie, Gabriel TI Phase equilibria in the H2O-CO2 system between 250-330 K and 0-1.7 GPa: Stability of the CO2 hydrates and H2O-ice VI at CO2 saturation SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID DIOXIDE-WATER SYSTEM; HIGH-PRESSURE; CARBON-DIOXIDE; CLATHRATE HYDRATE; CH4-CO2-H2O SYSTEM; RAMAN-SPECTROSCOPY; AQUEOUS-SOLUTIONS; PVTX PROPERTIES; CO2-H2O SYSTEM; IMPROVED MODEL AB Although carbon dioxide is of interest in planetary science, few studies have been devoted so far to the H2O-CO2 system at pressures and temperatures relevant to planetary interiors, especially of the icy moons of the giant planets. In this study, new sapphire and diamond anvil cell experiments were conducted in this binary system to constrain the stability of the CO2 hydrates and H2O-ice VI at CO2 saturation in the 250-330 K and 0-1.7 GPa temperature and pressure ranges. Phases and equilibria were characterized by in situ Raman spectroscopy and optical monitoring. The equilibrium between the CO2 sI clathrate hydrate and the H2O-rich liquid phase was constrained over the entire pressure range of stability of the hydrate, up to 0.7-0.8 GPa, with results in agreement with previous studies at lower pressures. Above this pressure and below 1 GPa, our experiments confirmed the existence of the new CO2 high-pressure hydrate reported recently. Finally, the melting curve of the H2O-ice VI at CO2 saturation in the absence of CO2 hydrates was determined between 0.8 and 1.7 GPa. Using an available chemical potential model for H2O, a first assessment of the solubility of CO2 along the H2O-ice VI melting curve is given. Consistent with these new results and previous studies of the H2O-CO2 system, a P-T-X description of the binary system is proposed. The evolution with pressure of the Raman signatures of the two CO2 hydrates is detailed, and their stability is discussed in light of other clathrate hydrate-forming systems. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Bollengier, Olivier; Grasset, Olivier; Le Menn, Erwan; Bellino, Guillaume; Morizet, Yann; Bezacier, Lucile; Oancea, Adriana; Taffin, Cecile; Tobie, Gabriel] Univ Nantes, CNRS, Lab Planetol & Geodynam Nantes, UMR 6112, F-44322 Nantes 3, France. [Choukroun, Mathieu] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bollengier, O (reprint author), Univ Nantes, CNRS, Lab Planetol & Geodynam Nantes, UMR 6112, F-44322 Nantes 3, France. EM olivier.bollengier@univ-nantes.fr RI Choukroun, Mathieu/F-3146-2017 OI Choukroun, Mathieu/0000-0001-7447-9139 FU European Research Council under the European Community [259285]; PRES-UNAM; NASA FX The authors would like to thank the associate editor and the three reviewers for their insightful comments and suggestions that helped improve the manuscript significantly. The research leading to these results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013 Grant Agreement No. 259285). This work received funding from the PRES-UNAM. Part of this work was conducted at the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA. Support by the NASA Outer Planets Research Program and government sponsorship is acknowledged. NR 84 TC 16 Z9 16 U1 4 U2 72 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD OCT 15 PY 2013 VL 119 BP 322 EP 339 DI 10.1016/j.gca.2013.06.006 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 213EC UT WOS:000324036200021 ER PT J AU Macaulay, E Wehus, IK Eriksen, HK AF Macaulay, E. Wehus, I. K. Eriksen, H. K. TI Lower Growth Rate from Recent Redshift Space Distortion Measurements than Expected from Planck SO PHYSICAL REVIEW LETTERS LA English DT Article ID POWER SPECTRA; 2DF-SDSS LRG; QSO SURVEY; VELOCITIES; EXPANSION; GALAXIES; GRAVITY AB We perform a metastudy of recently published redshift space distortion (RSD) measurements of the cosmological growth rate, f(z)sigma(8)(z) . We analyze the latest results from the 6dFGS, BOSS, LRG, WiggleZ, and VIPERS galaxy redshift surveys, and compare the measurements to expectations from Planck. In this Letter we point out that the RSD measurements are consistently lower than the values expected from Planck, and the relative scatter between the RSD measurements is lower than expected. A full resolution of this issue may require a more robust treatment of nonlinear effects in RSD models, although the trend for a low sigma(8) agrees with recent constraints on sigma(8) and Omega(m) from Sunyaev-Zeldovich cluster counts identified in Planck. C1 [Macaulay, E.] Univ Sussex, Dept Phys & Astron, Falmer BN1 9QH, E Sussex, England. [Macaulay, E.; Wehus, I. K.] Univ Oxford, Oxford OX1 3RH, England. [Wehus, I. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Eriksen, H. K.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. RP Macaulay, E (reprint author), Univ Sussex, Dept Phys & Astron, Falmer BN1 9QH, E Sussex, England. EM edward.macaulay@astro.ox.ac.uk; i.k.wehus@fys.uio.no; h.k.k.eriksen@astro.uio.no FU ERC [StG2010-257080, 259505]; Leverhulme visiting professorship; BIPAC; STFC FX We thank the two anonymous referees for useful comments which have substantially improved this Letter, Jonathan Patterson for help with parallelization of the analysis code, Tessa Baker for help with the model parametrization, Erminia Calabrese for help with the Planck parameters for the growth rate, Lado Samushia for help with the growth rate models, Rita Tojeiro for help with the BOSS data, Chris Blake for useful suggestions and help with the WiggleZ data, and Pedro Ferreira for comments and discussions. This project was supported by an ERC Starting Grant No. StG2010-257080 and a Leverhulme visiting professorship for H. K. E. E. M. acknowledges support from the BIPAC and STFC. I. K. W. acknowledges support from ERC Grant No. 259505. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 31 TC 48 Z9 48 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD OCT 14 PY 2013 VL 111 IS 16 AR 161301 DI 10.1103/PhysRevLett.111.161301 PG 4 WC Physics, Multidisciplinary SC Physics GA 240TG UT WOS:000326119300005 PM 24182250 ER PT J AU Drouin, BJ Yu, SS Elliott, BM Crawford, TJ Miller, CE AF Drouin, Brian J. Yu, Shanshan Elliott, Ben M. Crawford, Timothy J. Miller, Charles E. TI High resolution spectral analysis of oxygen. III. Laboratory investigation of the airglow bands SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID ROTATIONAL RAMAN-SPECTRA; TRANSITION; O-16(2); O-2; O-2(B(1)SIGMA(+)(G); O-17O-18; SYSTEMS AB We report the first high spectral resolution laboratory measurements of simulated oxygen A-band night glow. Our static discharge system approximates the conditions of the mesospheric oxygen night glow - suggesting O(D-1) + O-2 (X-3 Sigma(-)(g)) -> O(P-3) + O-2 (b(1)Sigma(+)(g)) -> O-2 (X-3 Sigma(-)(g)) + h nu as the primary source of the emission. Additionally, use of the static cell has enabled us to collect spectra for all six molecular oxygen isotopologues using isotopically enriched samples. The (0,0), (0,1), and (1,1) b - X vibrational bands were observed for all six isotopologues. The (1,2) and (2,2) bands were also observed for O-16(2). The frequencies of the observed (0,1) transitions resolved discrepancies in Raman data for (OO)-O-16-O-17, O-17(2), and (OO)-O-17-O-18, enabling us to improve the vibrational parameterization of the ground electronic state global fit. Rotationally resolved intensities were determined for the (0,0), (0,1), and (1,1) bands. The experimental band intensity ratios I(0,0)/I(0,1) = 13.53(24); I(1,1)/I(1,0) = 11.9(65); I(0,0)/I(0,2) = 503(197); and I(1,1)/I(1,2) = 5.6(19) are in excellent agreement with the recent mesospheric remote sensing data and calculated Franck-Condon factors. (C) 2013 AIP Publishing LLC. C1 [Drouin, Brian J.; Yu, Shanshan; Elliott, Ben M.; Crawford, Timothy J.; Miller, Charles E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Drouin, BJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM brian.j.drouin@jpl.nasa.gov RI Yu, Shanshan/D-8733-2016; Sung, Keeyoon/I-6533-2015 FU Jet Propulsion Laboratory, California Institute of Technology, National Aeronautics and Space Administration (NASA) FX This paper presents research carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). Government sponsorship is acknowledged. NR 30 TC 4 Z9 4 U1 1 U2 26 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD OCT 14 PY 2013 VL 139 IS 14 AR 144301 DI 10.1063/1.4821759 PG 11 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 236FL UT WOS:000325780800020 PM 24116613 ER PT J AU Scaringi, S Groot, PJ Still, M AF Scaringi, S. Groot, P. J. Still, M. TI Kepler observations of the eclipsing cataclysmic variable KIS J192748.53+444724.5 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries: close; stars: individual: KIS J192748.53+444724.5; stars: individual: KIC 8625249 AB We present results from long-cadence Kepler observations covering 97.6 d of the newly discovered eclipsing cataclysmic variable KIS J192748.53+444724.5/KIC 8625249. We detect deep eclipses of the accretion disc by the donor star every 3.97 h. Additionally, the Kepler observations also cover a full outburst for this cataclysmic variable, making KIS J192748.53+444724.5 the second known eclipsing cataclysmic variable system in the Kepler field of view. We show how in quiescence a significant component associated with the hotspot is visible preceding the eclipse, and that this component is swamped by the brightness increase during the outburst, potentially associated with the accretion disc. Furthermore, we present evidence for accretion disc radius changes during the outburst by analysing the out-of-eclipse light levels and eclipse depth through each orbital cycle. We show how these parameters are linearly correlated in quiescence, and discuss how their evolution during the outburst suggests disc radius changes and/or radial temperature gradient variations in the disc. C1 [Scaringi, S.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Groot, P. J.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Still, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Still, M.] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA. RP Scaringi, S (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Louvain, Belgium. EM simone.scaringi@ster.kuleuven.be RI Groot, Paul/K-4391-2016; OI Groot, Paul/0000-0002-4488-726X; Scaringi, Simone/0000-0001-5387-7189 FU FWO Pegasus Marie Curie Fellowship programme FX This research has made use of NASA's Astrophysics Data System Bibliographic Services. SS acknowledges funding from the FWO Pegasus Marie Curie Fellowship programme. Additionally, SS acknowledges the use of the astronomy and astrophysics package for Matlab (Ofek, in preparation). NR 31 TC 3 Z9 3 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 OCT 11 PY 2013 VL 435 IS 1 BP L68 EP L72 DI 10.1093/mnrasl/slt099 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA V40MZ UT WOS:000209484000015 ER PT J AU Lin, B Ismail, S Harrison, FW Browell, EV Nehrir, AR Dobler, J Moore, B Refaat, T Kooi, SA AF Lin, Bing Ismail, Syed Harrison, F. Wallace Browell, Edward V. Nehrir, Amin R. Dobler, Jeremy Moore, Berrien Refaat, Tamer Kooi, Susan A. TI Modeling of intensity-modulated continuous-wave laser absorption spectrometer systems for atmospheric CO2 column measurements SO APPLIED OPTICS LA English DT Article ID MULTIPLE-SCATTERING; LIDAR MEASUREMENTS; CLOUD PROPERTIES; SATELLITE; TEMPERATURE; MISSION AB The focus of this study is to model and validate the performance of intensity-modulated continuous-wave (IM-CW) CO2 laser absorption spectrometer (LAS) systems and their CO2 column measurements from airborne and satellite platforms. The model accounts for all fundamental physics of the instruments and their related CO2 measurement environments, and the modeling results are presented statistically from simulation ensembles that include noise sources and uncertainties related to the LAS instruments and the measurement environments. The characteristics of simulated LAS systems are based on existing technologies and their implementation in existing systems. The modeled instruments are specifically assumed to be IM-CW LAS systems such as the Exelis' airborne multifunctional fiber laser lidar (MFLL) operating in the 1.57 mu m CO2 absorption band. Atmospheric effects due to variations in CO2, solar radiation, and thin clouds, are also included in the model. Model results are shown to agree well with LAS atmospheric CO2 measurement performance. For example, the relative bias errors of both MFLL simulated and measured CO2 differential optical depths were found to agree to within a few tenths of a percent when compared to the in situ observations from the flight of 3 August 2011 over Railroad Valley (RRV), Nevada, during the summer 2011 flight campaign. In addition, the horizontal variations in the model CO2 differential optical depths were also found to be consistent with those from MFLL measurements. In general, the modeled and measured signal-to-noise ratios (SNRs) of the CO2 column differential optical depths (tau(d)) agreed to within about 30%. Model simulations of a spaceborne IM-CW LAS system in a 390 km dawn/dusk orbit for CO2 column measurements showed that with a total of 42 W of transmitted power for one offline and two different sideline channels (placed at different locations on the side of the CO2 absorption line), the accuracy of the tau(d) measurements for surfaces similar to the playa of RRV, Nevada, will be better than 0.1% for 10 s averages. For other types of surfaces such as low-reflectivity snow and ice surfaces, the precision and bias errors will be within 0.23% and 0.1%, respectively. Including thin clouds with optical depths up to 1, the SNR of the td measurements with 0.1 s integration period for surfaces similar to the playa of RRV, Nevada, will be greater than 94 and 65 for sideline positions placed +3 and +10 pm, respectively, from the CO2 line center at 1571.112 nm. The CO2 column bias errors introduced by the thin clouds are <= 0.1% for cloud optical depth <= 0.4, but they could reach similar to 0.5% for more optically thick clouds with optical depths up to 1. When the cloud and surface altitudes and scattering amplitudes are obtained from matched filter analysis, the cloud bias errors can be further reduced. These results indicate that the IM-CW LAS instrument approach when implemented in a dawn/dusk orbit can make accurate CO2 column measurements from space with preferential weighting across the mid to lower troposphere in support of a future ASCENDS mission. (c) 2013 Optical Society of America C1 [Lin, Bing; Ismail, Syed; Harrison, F. Wallace; Nehrir, Amin R.] NASA Langley Res Ctr, Hampton, VA 23681 USA. [Dobler, Jeremy] Exelis Inc, Ft Wayne, IN 46818 USA. [Moore, Berrien] Univ Oklahoma, Norman, OK 73072 USA. [Refaat, Tamer] Old Dominion Univ, Norfolk, VA 23529 USA. [Kooi, Susan A.] 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; NASA Langley Research Center FX The authors express their appreciation to C. Hostetler, W. Edwards, M. Dijoseph, B. Meadows, J. Campbell, S. Chen, M. Vanek, Z. Liu, J. Dempsey, Y. Hu, W. Sun, and J. LaPan for their valuable comments and encouragement, and to D. McGregor, N. Blume, G. Mathew, and the entire LaRC/Exelis team for their strong support in instrument evaluation and data collection. This research was supported by the NASA ASCENDS Mission Study and NASA Langley Research Center. NR 39 TC 10 Z9 11 U1 0 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 OCT 10 PY 2013 VL 52 IS 29 BP 7062 EP 7077 DI 10.1364/AO.52.007062 PG 16 WC Optics SC Optics GA 236AE UT WOS:000325764900002 PM 24217721 ER PT J AU Nixon, CA Jennings, DE Bezard, B Vinatier, S Teanby, NA Sung, K Ansty, TM Irwin, PGJ Gorius, N Cottini, V Coustenis, A Flasar, FM AF Nixon, C. A. Jennings, D. E. Bezard, B. Vinatier, S. Teanby, N. A. Sung, K. Ansty, T. M. Irwin, P. G. J. Gorius, N. Cottini, V. Coustenis, A. Flasar, F. M. TI DETECTION OF PROPENE IN TITAN'S STRATOSPHERE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planets and satellites: atmospheres; planets and satellites: composition; planets and satellites: individual (Titan) ID FAR-INFRARED SPECTRA; MOLECULAR SPECTROSCOPIC DATABASE; CASSINI CIRS; COUPLING PHOTOCHEMISTRY; UPPER-ATMOSPHERE; HAZE FORMATION; WATER-VAPOR; MODEL; HC3N; HYDROCARBONS AB The Voyager 1 flyby of Titan in 1980 gave a first glimpse of the chemical complexity of Titan's atmosphere, detecting many new molecules with the infrared interferometer spectrometer (IRIS). These included propane (C3H8) and propyne (CH3C2H), while the intermediate-sized C3Hx hydrocarbon (C3H6) was curiously absent. Using spectra from the Composite Infrared Spectrometer on Cassini, we show the first positive detection of propene (C3H6) in Titan's stratosphere (5 sigma significance), finally filling the three-decade gap in the chemical sequence. We retrieve a vertical abundance profile from 100-250 km, that varies slowly with altitude from 2.0 +/- 0.8 ppbv at 125 km, to 4.6 +/- 1.5 ppbv at 200 km. The abundance of C3H6 is less than both C3H8 and CH3C2H, and we remark on an emerging paradigm in Titan's hydrocarbon abundances whereby alkanes > alkynes > alkenes within the C2Hx and C3Hx chemical families in the lower stratosphere. More generally, there appears to be much greater ubiquity and relative abundance of triple-bonded species than double-bonded, likely due to the greater resistance of triple bonds to photolysis and chemical attack. C1 [Nixon, C. A.; Flasar, F. M.] NASA Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. [Jennings, D. E.] NASA Goddard Space Flight Ctr, Detector Syst Branch, Greenbelt, MD 20771 USA. [Bezard, B.; Vinatier, S.; Coustenis, A.] Observ Paris, CNRS, LESIA, F-92195 Meudon, France. [Teanby, N. A.] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England. [Sung, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ansty, T. M.] Cornell Univ, Dept Space Sci, Ithaca, NY 14853 USA. [Irwin, P. G. J.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. [Gorius, N.] Catholic Univ Amer, IACS, Washington, DC 20064 USA. [Cottini, V.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Nixon, CA (reprint author), NASA Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012; Sung, Keeyoon/I-6533-2015; OI Nixon, Conor/0000-0001-9540-9121; Teanby, Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X FU NASA Cassini Mission; National Aeronautics and Space Administration; NASA; UK STFC; Leverhulme Trust; Centre National d'Etudes Spatiales (CNES) FX Our thanks to Linda Brown (JPL) and Steven Sharpe (PNNL) for providing us with molecular spectroscopic data for propane and propene: absorbances and line lists. C.A.N., D.E.J., N.G., T.M.A., and F.M.F. were supported by the NASA Cassini Mission. 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. V.C. was supported by the NASA Post-Doctoral Program. N.A.T. and P.G.J.I. received support for their portion of this work from the UK STFC, and NAT received additional support from the Leverhulme Trust. B.B., S.V., and A.C. were supported by the Centre National d'Etudes Spatiales (CNES). NR 44 TC 14 Z9 14 U1 2 U2 28 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 OCT 10 PY 2013 VL 776 IS 1 AR L14 DI 10.1088/2041-8205/776/1/L14 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 232JG UT WOS:000325489200001 ER PT J AU Currie, T Burrows, A Madhusudhan, N Fukagawa, M Girard, JH Dawson, R Murray-Clay, R Kenyon, S Kuchner, M Matsumura, S Jayawardhana, R Chambers, J Bromley, B AF Currie, Thayne Burrows, Adam Madhusudhan, Nikku Fukagawa, Misato Girard, Julien H. Dawson, Rebekah Murray-Clay, Ruth Kenyon, Scott Kuchner, Marc Matsumura, Soko Jayawardhana, Ray Chambers, John Bromley, Ben TI A COMBINED VERY LARGE TELESCOPE AND GEMINI STUDY OF THE ATMOSPHERE OF THE DIRECTLY IMAGED PLANET, beta PICTORIS b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: early-type; stars: individual (beta Pictoris) ID SPECTRAL IRRADIANCE CALIBRATION; CANDIDATE SUBSTELLAR COMPANION; FINDING CAMPAIGN DISCOVERY; EXTRASOLAR GIANT PLANETS; DIRECT-IMAGING DISCOVERY; YOUNG SOLAR ANALOG; ORBITING HR 8799; MU-M; UPPER SCORPIUS; BROWN DWARFS AB We analyze new/archival VLT/NaCo and Gemini/NICI high-contrast imaging of the young, self-luminous planet beta Pictoris b in seven near-to-mid IR photometric filters, using advanced image processing methods to achieve high signal-to-noise, high precision measurements. While beta Pic b's near-IR colors mimic those of a standard, cloudy early-to-mid L dwarf, it is overluminous in the mid-infrared compared to the field L/T dwarf sequence. Few substellar/planet-mass objects-i.e., kappa And b and 1RXJ 1609B-match beta Pic b's JHK(s)L' photometry and its 3.1 mu m and 5 mu m photometry are particularly difficult to reproduce. Atmosphere models adopting cloud prescriptions and large (similar to 60 mu m) dust grains fail to reproduce the beta Pic b spectrum. However, models incorporating thick clouds similar to those found for HR 8799 bcde, but also with small (a few microns) modal particle sizes, yield fits consistent with the data within the uncertainties. Assuming solar abundance models, thick clouds, and small dust particles (< a > = 4 mu m), we derive atmosphere parameters of log(g) = 3.8 +/- 0.2 and T-eff = 1575-1650 K, an inferred mass of 7(-3)(+4) M-J, and a luminosity of log(L/L-circle dot) similar to -3.80 +/- 0.02. The best-estimated planet radius, approximate to 1.65 +/- 0.06 R-J, is near the upper end of allowable planet radii for hot-start models given the host star's age and likely reflects challenges constructing accurate atmospheric models. Alternatively, these radii are comfortably consistent with hot-start model predictions if beta Pic b is younger than approximate to 7 Myr, consistent with a late formation well after its host star's birth similar to 12(-4)(+8) Myr ago. C1 [Currie, Thayne; Jayawardhana, Ray] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Madhusudhan, Nikku] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Fukagawa, Misato] Osaka Univ, Toyonaka, Osaka 5600043, Japan. [Girard, Julien H.] European So Observ, Santiago 19, Chile. [Dawson, Rebekah; Murray-Clay, Ruth; Kenyon, Scott] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kuchner, Marc] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Matsumura, Soko] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Chambers, John] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Bromley, Ben] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. RP Currie, T (reprint author), Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. FU McLean Postdoctoral Fellowship; NSF-GRFP [DGE-1144152] FX We thank Christian Thalmann, France Allard, and the anonymous referee for helpful comments and discussions and Michael Cushing for providing IRTF/SpeX and Subaru/IRCS spectra of field L dwarfs. We are grateful to the telescope staff at ESO Paranal Observatory and Gemini-South Cerro Pachon Observatory for support for our observations, all of which were obtained with "delegated visitor mode" or "eavesdropping mode." Finally, we thank Christian Marois for very detailed discussions on image processing techniques and extensive helpful suggestions that improved this manuscript. T. C. acknowledges support from a McLean Postdoctoral Fellowship. R. D. acknowledges NSF-GRFP grant DGE-1144152. NR 91 TC 38 Z9 38 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 OCT 10 PY 2013 VL 776 IS 1 AR 15 DI 10.1088/0004-637X/776/1/15 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 225UM UT WOS:000324989000015 ER PT J AU Hopkins, PF Christiansen, JL AF Hopkins, Philip F. Christiansen, Jessie L. TI TURBULENT DISKS ARE NEVER STABLE: FRAGMENTATION AND TURBULENCE-PROMOTED PLANET FORMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; hydrodynamics; instabilities; planets and satellites: formation; protoplanetary disks; turbulence ID SELF-GRAVITATING DISCS; MACH NUMBER RELATION; DENSITY PROBABILITY-DISTRIBUTION; FULLY-DEVELOPED TURBULENCE; INITIAL MASS FUNCTION; EXCURSION-SET MODEL; COOLING TIME-SCALE; PROTOPLANETARY DISKS; ISOTHERMAL TURBULENCE; INTERSTELLAR-MEDIUM AB A fundamental assumption in our understanding of disks is that when the Toomre Q >> 1, the disk is stable against fragmentation into self-gravitating objects (and so cannot form planets via direct collapse). But if disks are turbulent, this neglects a spectrum of stochastic density fluctuations that can produce rare, high-density mass concentrations. Here, we use a recently developed analytic framework to predict the statistics of these fluctuations, i.e., the rate of fragmentation and mass spectrum of fragments formed in a turbulent Keplerian disk. Turbulent disks are never completely stable: we calculate the (always finite) probability of forming self-gravitating structures via stochastic turbulent density fluctuations in such disks. Modest sub-sonic turbulence above Mach number M similar to 0.1 can produce a few stochastic fragmentation or "direct collapse" events over similar to Myr timescales, even if Q >> 1 and cooling is slow (t(cool) >> t(orbit)). In transsonic turbulence this extends to Q similar to 100. We derive the true Q-criterion needed to suppress such events, which scales exponentially with Mach number. We specify to turbulence driven by magneto-rotational instability, convection, or spiral waves and derive equivalent criteria in terms of Q and the cooling time. Cooling times greater than or similar to 50 t(dyn) may be required to completely suppress fragmentation. These gravo-turbulent events produce mass spectra peaked near similar to(Q M-disk/M-*)(2) M-disk (rocky-to-giant planet masses, increasing with distance from the star). We apply this to protoplanetary disk models and show that even minimum-mass solar nebulae could experience stochastic collapse events, provided a source of turbulence. C1 [Hopkins, Philip F.] CALTECH, TAPIR, Pasadena, CA 91125 USA. [Hopkins, Philip F.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Hopkins, Philip F.] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. [Christiansen, Jessie L.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP Hopkins, PF (reprint author), CALTECH, TAPIR, Mailcode 350-17, Pasadena, CA 91125 USA. EM phopkins@caltech.edu FU NASA [PF1-120083, NAS8-03060]; Chandra X-ray Observatory Center FX We thank Jim Stone, Eugene Chiang, and Eliot Quataert for insightful discussions that helped inspire this paper. Support for P. F. H. was provided by NASA through Einstein Postdoctoral Fellowship Award Number PF1-120083 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. NR 104 TC 12 Z9 12 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2013 VL 776 IS 1 AR 48 DI 10.1088/0004-637X/776/1/48 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 225UM UT WOS:000324989000048 ER PT J AU Howard, CD Sandell, G Vacca, WD Duchene, G Mathews, G Augereau, JC Barrado, D Dent, WRF Eiroa, C Grady, C Kamp, I Meeus, G Menard, F Pinte, C Podio, L Riviere-Marichalar, P Roberge, A Thi, WF Vicente, S Williams, JP AF Howard, Christian D. Sandell, Goeran Vacca, William D. Duchene, Gaspard Mathews, Geoffrey Augereau, Jean-Charles Barrado, David Dent, William R. F. Eiroa, Carlos Grady, Carol Kamp, Inga Meeus, Gwendolyn Menard, Francois Pinte, Christophe Podio, Linda Riviere-Marichalar, Pablo Roberge, Aki Thi, Wing-Fai Vicente, Silvia Williams, Jonathan P. TI HERSCHEL/PACS SURVEY OF PROTOPLANETARY DISKS IN TAURUS/AURIGA-OBSERVATIONS OF [O I] AND [C II], AND FAR-INFRARED CONTINUUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; protoplanetary disks; stars: pre-main sequence ID T-TAURI STARS; HUBBLE-SPACE-TELESCOPE; MAIN-SEQUENCE STARS; AURIGA MOLECULAR CLOUD; YOUNG CIRCUMSTELLAR DISKS; GG-TAURI; PLANET FORMATION; MAGNETOSPHERIC ACCRETION; ADAPTIVE OPTICS; LINE EMISSION AB The Herschel Space Observatory was used to observe similar to 120 pre-main-sequence stars in Taurus as part of the GASPS Open Time Key project. Photodetector Array Camera and Spectrometer was used to measure the continuum as well as several gas tracers such as [O I] 63 mu m, [O I] 145 mu m, [C II] 158 mu m, OH, H2O, and CO. The strongest line seen is [O I] at 63 mu m. We find a clear correlation between the strength of the [O I] 63 mu m line and the 63 mu m continuum for disk sources. In outflow sources, the line emission can be up to 20 times stronger than in disk sources, suggesting that the line emission is dominated by the outflow. The tight correlation seen for disk sources suggests that the emission arises from the inner disk (<50 AU) and lower surface layers of the disk where the gas and dust are coupled. The [OI] 63 mu m is fainter in transitional stars than in normal Class II disks. Simple spectral energy distribution models indicate that the dust responsible for the continuum emission is colder in these disks, leading to weaker line emission. [C II] 158 mu m emission is only detected in strong outflow sources. The observed line ratios of [O I] 63 mu m to [OI] 145 mu m are in the regime where we are insensitive to the gas-to-dust ratio, neither can we discriminate between shock or photodissociation region emission. We detect no Class III object in [O I] 63 mu m and only three in continuum, at least one of which is a candidate debris disk. C1 [Howard, Christian D.; Sandell, Goeran; Vacca, William D.] NASA, SOFIA USRA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Howard, Christian D.] Google, Mountain View, CA 94043 USA. [Duchene, Gaspard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Duchene, Gaspard; Augereau, Jean-Charles; Menard, Francois; Pinte, Christophe; Podio, Linda; Thi, Wing-Fai] UJF Grenoble 1, CNRS, INSU, Inst Planetol & Astrophys IPAG UMR 5274, F-38041 Grenoble, France. [Mathews, Geoffrey] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Mathews, Geoffrey; Williams, Jonathan P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Barrado, David; Riviere-Marichalar, Pablo] CSIC INTA, Dept Astrofis, Ctr Astrobiol, E-28691 Villanueva De La Canada, Spain. [Barrado, David] Ctr Astron Hispano Aleman, Calar Alto Observ, E-04004 Almeria, Spain. [Dent, William R. F.] ALMA SCO, Santiago, Chile. [Eiroa, Carlos; Meeus, Gwendolyn] Univ Autonoma Madrid, Fac Ciencias, Dep Fis Teor, E-28049 Madrid, Spain. [Grady, Carol; Roberge, Aki] NASA, Exoplanets & Stellar Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Grady, Carol] Eureka Sci, Oakland, CA 96002 USA. [Grady, Carol] NASA, Goddard Ctr Astrobiol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kamp, Inga; Vicente, Silvia] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Menard, Francois] CNRS France, UMI 3386, UMI FCA, Santiago, Chile. [Menard, Francois] U Chile PUC U Concept, Santiago, Chile. RP Howard, CD (reprint author), NASA, SOFIA USRA, Ames Res Ctr, MS 232-12,Bldg N232,Rm 146,Box 1, Moffett Field, CA 94035 USA. RI Roberge, Aki/D-2782-2012; Barrado Navascues, David/C-1439-2017 OI Roberge, Aki/0000-0002-2989-3725; Barrado Navascues, David/0000-0002-5971-9242 FU Milenium Nucleus [P10-022-F]; Chilean Government; EU [284405] FX This work made extensive use of the SIMBAD Database, operated at CDS, Strasbourg, France, and NASA's Astrophysics Data System Abstract Service. We thank Uma Gorti for stimulating discussions. We thank the referee for a very careful reading of the manuscript and for his/her constructive criticism. F. Menard acknowledges financial support from the Milenium Nucleus P10-022-F, funded by the Chilean Government, and by the EU FP7-2011 programme, under Grant Agreement 284405. NR 138 TC 24 Z9 24 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2013 VL 776 IS 1 AR 21 DI 10.1088/0004-637X/776/1/21 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 225UM UT WOS:000324989000021 ER PT J AU Kwon, RY Kramar, M Wang, TJ Ofman, L Davila, JM Chae, J Zhang, J AF Kwon, Ryun-Young Kramar, Maxim Wang, Tongjiang Ofman, Leon Davila, Joseph M. Chae, Jongchul Zhang, Jie TI GLOBAL CORONAL SEISMOLOGY IN THE EXTENDED SOLAR CORONA THROUGH FAST MAGNETOSONIC WAVES OBSERVED BY STEREO SECCHI COR1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic fields; Sun: corona; Sun: fundamental parameters; waves ID MAGNETIC-FIELD STRENGTH; EXTREME-ULTRAVIOLET WAVE; II RADIO-BURST; MASS-EJECTION; LOOP OSCILLATIONS; SHOCK-WAVES; EIT WAVE; ELECTRON-DENSITY; MORETON WAVE; EUV WAVE AB We present global coronal seismology for the first time, which allows us to determine inhomogeneous magnetic field strength in the extended corona. From the measurements of the propagation speed of a fast magnetosonic wave associated with a coronal mass ejection (CME) and the coronal background density distribution derived from the polarized radiances observed by the STEREO SECCHI COR1, we determined the magnetic field strengths along the trajectories of the wave at different heliocentric distances. We found that the results have an uncertainty less than 40%, and are consistent with values determined with a potential field model and reported in previous works. The characteristics of the coronal medium we found are that (1) the density, magnetic field strength, and plasma beta are lower in the coronal hole region than in streamers; (2) the magnetic field strength decreases slowly with height but the electron density decreases rapidly so that the local fast magnetosonic speed increases while plasma beta falls off with height; and (3) the variations of the local fast magnetosonic speed and plasma beta are dominated by variations in the electron density rather than the magnetic field strength. These results imply that Moreton and EIT waves are downward-reflected fast magnetosonic waves from the upper solar corona, rather than freely propagating fast magnetosonic waves in a certain atmospheric layer. In addition, the azimuthal components of CMEs and the driven waves may play an important role in various manifestations of shocks, such as type II radio bursts and solar energetic particle events. C1 [Kwon, Ryun-Young; Kramar, Maxim; Wang, Tongjiang; Ofman, Leon] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Kwon, Ryun-Young; Kramar, Maxim; Wang, Tongjiang; Ofman, Leon; Davila, Joseph M.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Kwon, Ryun-Young; Zhang, Jie] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA. [Chae, Jongchul] Seoul Natl Univ, Astron Program, Dept Phys & Astron, Seoul 151, South Korea. RP Kwon, RY (reprint author), Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, 620 Michigan Ave, Washington, DC 20064 USA. FU NASA [NNX10AN10G, NNX12AB34G, NNX11AO68G, NNG11PL10A] FX R.-Y.K. and L.O. acknowledge support by the NASA grant NNX10AN10G. L.O. acknowledges support by NASA grants NNX12AB34G and NNX11AO68G. The work of T. W. was supported by the NASA cooperative agreement NNG11PL10A to CUA and the NASA grant NNX12AB34G. NR 63 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 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2013 VL 776 IS 1 AR 55 DI 10.1088/0004-637X/776/1/55 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 225UM UT WOS:000324989000055 ER PT J AU Nielsen, EL Liu, MC Wahhaj, Z Biller, BA Hayward, TL Close, LM Males, JR Skemer, AJ Chun, M Ftaclas, C Alencar, SHP Artymowicz, P Boss, A Clarke, F Dal Pino, ED Gregorio-Hetem, J Hartung, M Ida, S Kuchner, M Lin, DNC Reid, IN Shkolnik, EL Tecza, M Thatte, N Toomey, DW AF Nielsen, Eric L. Liu, Michael C. Wahhaj, Zahed Biller, Beth A. Hayward, Thomas L. Close, Laird M. Males, Jared R. Skemer, Andrew J. Chun, Mark Ftaclas, Christ Alencar, Silvia H. P. Artymowicz, Pawel Boss, Alan Clarke, Fraser Dal Pino, Elisabete de Gouveia Gregorio-Hetem, Jane Hartung, Markus Ida, Shigeru Kuchner, Marc Lin, Douglas N. C. Reid, I. Neill Shkolnik, Evgenya L. Tecza, Matthias Thatte, Niranjan Toomey, Douglas W. TI THE GEMINI NICI PLANET-FINDING CAMPAIGN: THE FREQUENCY OF GIANT PLANETS AROUND YOUNG B AND A STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; instrumentation: adaptive optics; planetary systems; planets and satellites: detection; stars: individual (HIP 79797) ID INTERMEDIATE-MASS STARS; BROWN DWARF COMPANION; DUSTY DEBRIS DISKS; CIRCUMSTELLAR DISK; HR 8799; SOLAR NEIGHBORHOOD; BETA-PICTORIS; STELLAR MASS; SUBSTELLAR COMPANION; EVOLUTIONARY MODELS AB We have carried out high contrast imaging of 70 young, nearby B and A stars to search for brown dwarf and planetary companions as part of the Gemini NICI Planet-Finding Campaign. Our survey represents the largest, deepest survey for planets around high-mass stars (approximate to 1.5-2.5 M-circle dot) conducted to date and includes the planet hosts beta Pic and Fomalhaut. We obtained follow-up astrometry of all candidate companions within 400 AU projected separation for stars in uncrowded fields and identified new low-mass companions to HD 1160 and HIP 79797. We have found that the previously known young brown dwarf companion to HIP 79797 is itself a tight (3 AU) binary, composed of brown dwarfs with masses 58(-20)(+21) M-Jup and 55(-19)(+20) M-Jup, making this system one of the rare substellar binaries in orbit around a star. Considering the contrast limits of our NICI data and the fact that we did not detect any planets, we use high-fidelity Monte Carlo simulations to show that fewer than 20% of 2 M-circle dot stars can have giant planets greater than 4 M-Jup between 59 and 460 AU at 95% confidence, and fewer than 10% of these stars can have a planet more massive than 10 M-Jup between 38 and 650 AU. Overall, we find that large-separation giant planets are not common around B and A stars: fewer than 10% of B and A stars can have an analog to the HR 8799 b (7 M-Jup, 68 AU) planet at 95% confidence. We also describe a new Bayesian technique for determining the ages of field B and A stars from photometry and theoretical isochrones. Our method produces more plausible ages for high-mass stars than previous age-dating techniques, which tend to underestimate stellar ages and their uncertainties. C1 [Nielsen, Eric L.; Liu, Michael C.; Chun, Mark; Ftaclas, Christ] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Wahhaj, Zahed] European So Observ, Santiago 19, Chile. [Biller, Beth A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Hayward, Thomas L.; Hartung, Markus] AURA, Southern Operat Ctr, Gemini Observ, La Serena, Chile. [Close, Laird M.; Males, Jared R.; Skemer, Andrew J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Alencar, Silvia H. P.] Univ Fed Minas Gerais, ICEx, Dept Fis, BR-30270901 Belo Horizonte, MG, Brazil. [Artymowicz, Pawel] Univ Toronto Scarborough, Toronto, ON M1C 1A4, Canada. [Boss, Alan] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Clarke, Fraser; Tecza, Matthias; Thatte, Niranjan] Univ Oxford, Dept Astron, Oxford OX1 3RH, England. [Dal Pino, Elisabete de Gouveia; Gregorio-Hetem, Jane] Univ Sao Paulo, Dept Astron, IAG USP, BR-05508900 Sao Paulo, Brazil. [Ida, Shigeru] Tokyo Inst Technol, Meguro Ku, Tokyo 1528550, Japan. [Kuchner, Marc] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Lin, Douglas N. C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Reid, I. Neill] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Shkolnik, Evgenya L.] Lowell Observ, Flagstaff, AZ 86001 USA. [Toomey, Douglas W.] Mauna Kea Infrared LLC, Hilo, HI 96720 USA. RP Nielsen, EL (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. RI Ida, Shigeru/A-7840-2014; Gregorio-Hetem, Jane/A-5924-2013; Alencar, Silvia/C-2803-2013; de Gouveia Dal Pino, Elisabete/H-9560-2013; OI Ida, Shigeru/0000-0002-9676-3891; de Gouveia Dal Pino, Elisabete/0000-0001-8058-4752; Biller, Beth/0000-0003-4614-7035; Skemer, Andrew/0000-0001-6098-3924; Nielsen, Eric/0000-0001-6975-9056 FU Space Telescope Science Institute; NSF [AST-0713881, AST-0709484, AAG-1109114]; NASA [NNX11 AC31G]; National Aeronautics and Space Administration; National Science Foundation; U.S. Government [NAG W-2166]; [HST-HF-01204.01-A]; [NAS 5-26555] FX We thank Jessica Lu, Adam Kraus, Rolf Kudritzki, and Lisa Kewley for helpful discussions that greatly benefited this work. We thank the anonymous referee for the constructive suggestions that have improved this work. B. A. B. was supported by Hubble Fellowship grant HST-HF-01204.01-A awarded by the Space Telescope Science Institute, which is operated by AURA for NASA, under contract NAS 5-26555. This work was supported in part by NSF grants AST-0713881 and AST-0709484 awarded to M. Liu, NASA Origins grant NNX11 AC31G awarded to M. Liu, and NSF grant AAG-1109114 awarded to L. Close. The Gemini Observatory 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 Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil), and CONICET (Argentina). This research is based on observations made with the European Southern Observatory telescopes obtained from the ESO/ST-ECF Science Archive Facility. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This research has made use of the VizieR catalog access tool, CDS, Strasbourg, France. The Digitized Sky Survey was produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. NR 95 TC 70 Z9 70 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2013 VL 776 IS 1 AR 4 DI 10.1088/0004-637X/776/1/4 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 225UM UT WOS:000324989000004 ER PT J AU Perera, BBP McLaughlin, MA Cordes, JM Kerr, M Burnett, TH Harding, AK AF Perera, B. B. P. McLaughlin, M. A. Cordes, J. M. Kerr, M. Burnett, T. H. Harding, A. K. TI MODELING THE NON-RECYCLED FERMI GAMMA-RAY PULSAR POPULATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: general; stars: neutron ID LARGE-AREA TELESCOPE; OUTER-GAP MODEL; RADIO-EMISSION GEOMETRY; INITIAL SPIN PERIODS; EMPIRICAL-THEORY; MAGNETIC-FIELD; PROPER-MOTION; LIGHT CURVES; GALACTIC POPULATION; POWERED PULSARS AB We use Fermi Gamma-ray Space Telescope detections and upper limits on non-recycled pulsars obtained from the Large Area Telescope (LAT) to constrain how the gamma-ray luminosity L-gamma depends on the period P and the period derivative (P) over dot. We use a Bayesian analysis to calculate a best-fit luminosity law, or dependence of L-gamma on P and (P) over dot, including different methods for modeling the beaming factor. An outer gap (OG) magnetosphere geometry provides the best-fit model, which is L-gamma proportional to P-a (P) over dot(b) where a = 1.36 +/- 0.03 and b = 0.44 +/- 0.02, similar to but not identical to the commonly assumed L-gamma proportional to root(E) over dot proportional to P-1.5 (P) over dot(0.5). Given upper limits on gamma-ray fluxes of currently known radio pulsars and using the OG model, we find that about 92% of the radio-detected pulsars have gamma-ray beams that intersect our line of sight. By modeling the misalignment of radio and gamma-ray beams of these pulsars, we find an average gamma-ray beaming solid angle of about 3.7 pi for the OG model, assuming a uniform beam. Using LAT-measured diffuse fluxes, we place a 2 sigma upper limit on the average braking index and a 2 sigma lower limit on the average surface magnetic field strength of the pulsar population of 3.8 and 3.2 x 10(10) G, respectively. We then predict the number of non-recycled pulsars detectable by the LAT based on our population model. Using the 2 yr sensitivity, we find that the LAT is capable of detecting emission from about 380 non-recycled pulsars, including 150 currently identified radio pulsars. Using the expected 5 yr sensitivity, about 620 non-recycled pulsars are detectable, including about 220 currently identified radio pulsars. We note that these predictions significantly depend on our model assumptions. C1 [Perera, B. B. P.; McLaughlin, M. A.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. [Cordes, J. M.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Cordes, J. M.] Cornell Univ, NAIC, Ithaca, NY 14853 USA. [Kerr, M.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Kerr, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Burnett, T. H.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Harding, A. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Perera, BBP (reprint author), W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. FU Research Corporation; Fermi GI Program; NASA; National Aeronautics and Space Administration; Department of Energy in the United States; Commissariat a l'Energie Atomique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan; K. A. Wallenberg Foundation; Swedish Research Council; Swedish National Space Board in Sweden FX B.B.P.P. and M. A. M. are supported through the Research Corporation. M. A. M. gratefully acknowledges support from Oxford Astrophysics while on sabbatical leave. A. K. H. acknowledges support from the Fermi GI and NASA Astrophysics Theory Programs. Some of the results in this paper have been derived using the HEALPix (Gorski et al. 2005) package.; 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. NR 75 TC 5 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 OCT 10 PY 2013 VL 776 IS 1 AR 61 DI 10.1088/0004-637X/776/1/61 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 225UM UT WOS:000324989000061 ER PT J AU Pucci, S Poletto, G Sterling, AC Romoli, M AF Pucci, Stefano Poletto, Giannina Sterling, Alphonse C. Romoli, Marco TI PHYSICAL PARAMETERS OF STANDARD AND BLOWOUT JETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: flares; Sun: X-rays, gamma rays; techniques: spectroscopic ID X-RAY TELESCOPE; POLAR CORONAL HOLES; EXTREME-ULTRAVIOLET; BRIGHT POINTS; HINODE XRT; SOLAR-WIND; DICHOTOMY; DYNAMICS; MISSION; MASS AB The X-ray Telescope on board the Hinode mission revealed the occurrence, in polar coronal holes, of much more numerous jets than previously indicated by the Yohkoh/Soft X-ray Telescope. These plasma ejections can be of two types, depending on whether they fit the standard reconnection scenario for coronal jets or if they include a blowout-like eruption. In this work, we analyze two jets, one standard and one blowout, that have been observed by the Hinode and STEREO experiments. We aim to infer differences in the physical parameters that correspond to the different morphologies of the events. To this end, we adopt spectroscopic techniques and determine the profiles of the plasma temperature, density, and outflow speed versus time and position along the jets. The blowout jet has a higher outflow speed, a marginally higher temperature, and is rooted in a stronger magnetic field region than the standard event. Our data provide evidence for recursively occurring reconnection episodes within both the standard and the blowout jet, pointing either to bursty reconnection or to reconnection occurring at different locations over the jet lifetimes. We make a crude estimate of the energy budget of the two jets and show how energy is partitioned among different forms. Also, we show that the magnetic energy that feeds the blowout jet is a factor of 10 higher than the magnetic energy that fuels the standard event. C1 [Pucci, Stefano; Romoli, Marco] Univ Florence, Dept Phys & Astron, I-50121 Florence, Italy. [Poletto, Giannina] Arcetri Astrophys Observ, INAF, I-50125 Florence, Italy. [Sterling, Alphonse C.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. RP Pucci, S (reprint author), Univ Florence, Dept Phys & Astron, I-50121 Florence, Italy. EM stpucci@arcetri.astro.it RI Romoli, Marco/H-6859-2012 FU NASA's Office of Space Science through the Living With a Star Targeted Research & Technology Program; [ASI I/023/09/0] FX S.P. and G. P. acknowledge support from ASI I/023/09/0. A. C. S. was supported by funding from NASA's Office of Space Science through the Living With a Star Targeted Research & Technology Program. Hinode is a Japanese mission developed and launched by ISAS/JAXA, collaborating with NAOJ as a domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and NSC (Norway). We thank the anonymous referee for thorough analysis of our work, and helpful comments and valuable suggestions that lead to an improvement of our paper. NR 40 TC 16 Z9 16 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 OCT 10 PY 2013 VL 776 IS 1 AR 16 DI 10.1088/0004-637X/776/1/16 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 225UM UT WOS:000324989000016 ER PT J AU Ricca, A Bauschlicher, CW Allamandola, LJ AF Ricca, Alessandra Bauschlicher, Charles W., Jr. Allamandola, Louis J. TI THE INFRARED SPECTROSCOPY OF NEUTRAL POLYCYCLIC AROMATIC HYDROCARBON CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; infrared: general; methods: numerical; molecular data ID GAUSSIAN-BASIS SETS; EMISSION FEATURES; MOLECULES; GALAXIES; SPECTRUM; DUST; BANDS AB The mid-infrared spectra of neutral homogeneous polycyclic aromatic hydrocarbon (PAH) clusters have been computed using density functional theory including an empirical correction for dispersion. The C-H out-of-plane bending modes are redshifted for all the clusters considered in this work. The magnitude of the redshift and the peak broadening are dependent on PAH size, shape, and on the PAH arrangement in the cluster. C1 [Ricca, Alessandra] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Bauschlicher, Charles W., Jr.] NASA, Ames Res Ctr, Entry Syst & Technol Div, Moffett Field, CA 94035 USA. [Allamandola, Louis J.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Ricca, A (reprint author), SETI Inst, Carl Sagan Ctr, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA. EM Alessandra.Ricca-1@nasa.gov; Charles.W.Bauschlicher@nasa.gov FU NASA's Astrophysics Theory and Fundamental Physics (ATFP) program [NNX09AD18G]; NASA's Laboratory Astrophysics Program Roses Grant [NNH09ZDA001N]; "Carbon in the Galaxy" Consortium Grant [NNH10ZDA001N]; NASA Astrobiology program FX A.R. thanks NASA's Astrophysics Theory and Fundamental Physics (ATFP) (NNX09AD18G) program, NASA's Laboratory Astrophysics Program Roses Grant (NNH09ZDA001N), and the "Carbon in the Galaxy" Consortium Grant (NNH10ZDA001N) for generous support of this work. We also acknowledge support from NASA Astrobiology program. NR 37 TC 5 Z9 5 U1 1 U2 19 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2013 VL 776 IS 1 AR 31 DI 10.1088/0004-637X/776/1/31 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 225UM UT WOS:000324989000031 ER PT J AU Veilleux, S Melendez, M Sturm, E Gracia-Carpio, J Fischer, J Gonzalez-Alfonso, E Contursi, A Lutz, D Poglitsch, A Davies, R Genzel, R Tacconi, L de Jong, JA Sternberg, A Netzer, H Hailey-Dunsheath, S Verma, A Rupke, DSN Maiolino, R Teng, SH Polisensky, E AF Veilleux, S. Melendez, M. Sturm, E. Gracia-Carpio, J. Fischer, J. Gonzalez-Alfonso, E. Contursi, A. Lutz, D. Poglitsch, A. Davies, R. Genzel, R. Tacconi, L. de Jong, J. A. Sternberg, A. Netzer, H. Hailey-Dunsheath, S. Verma, A. Rupke, D. S. N. Maiolino, R. Teng, S. H. Polisensky, E. TI FAST MOLECULAR OUTFLOWS IN LUMINOUS GALAXY MERGERS: EVIDENCE FOR QUASAR FEEDBACK FROM HERSCHEL SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; ISM: jets and outflows; ISM: molecules; quasars: general ID ULTRALUMINOUS INFRARED GALAXIES; STAR-FORMING GALAXIES; SCALE GASEOUS OUTFLOWS; PALOMAR-GREEN QUASARS; BAND IMAGING SURVEY; II ESI SPECTRA; GALACTIC WINDS; BLACK-HOLES; DYNAMICAL PROPERTIES; INTERSTELLAR-MEDIUM AB We report the results from a systematic search for molecular (OH 119 mu m) outflows with Herschel/PACS in a sample of 43 nearby (z < 0.3) galaxy mergers, mostly ultraluminous infrared galaxies (ULIRGs) and QSOs. We find that the character of the OH feature (strength of the absorption relative to the emission) correlates with that of the 9.7 mu m silicate feature, a measure of obscuration in ULIRGs. Unambiguous evidence for molecular outflows, based on the detection of OH absorption profiles with median velocities more blueshifted than -50 km s(-1), is seen in 26 (70%) of the 37 OH-detected targets, suggesting a wide-angle (similar to 145 degrees) outflow geometry. Conversely, unambiguous evidence for molecular inflows, based on the detection of OH absorption profiles with median velocities more redshifted than +50 km s(-1), is seen in only four objects, suggesting a planar or filamentary geometry for the inflowing gas. Terminal outflow velocities of similar to-1000 km s(-1) are measured in several objects, but median outflow velocities are typically similar to-200 km s(-1). While the outflow velocities show no statistically significant dependence on the star formation rate, they are distinctly more blueshifted among systems with large active galactic nucleus (AGN) fractions and luminosities [log (L-AGN/L-circle dot) >= 11.8 +/- 0.3]. The quasars in these systems play a dominant role in driving the molecular outflows. However, the most AGN dominated systems, where OH is seen purely in emission, show relatively modest OH line widths, despite their large AGN luminosities, perhaps indicating that molecular outflows subside once the quasar has cleared a path through the obscuring material. C1 [Veilleux, S.; Melendez, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Veilleux, S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Veilleux, S.; Sturm, E.; Gracia-Carpio, J.; Contursi, A.; Lutz, D.; Poglitsch, A.; Davies, R.; Genzel, R.; Tacconi, L.; de Jong, J. A.] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany. [Fischer, J.; Polisensky, E.] Naval Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Gonzalez-Alfonso, E.] Univ Alcala de Henares, Dept Fis & Matemat, E-28871 Madrid, Spain. [Sternberg, A.; Netzer, H.] Tel Aviv Univ, Sackler Sch Phys & Astron, IL-69978 Ramat Aviv, Israel. [Hailey-Dunsheath, S.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Verma, A.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Rupke, D. S. N.] Rhodes Coll, Dept Phys, Memphis, TN 38112 USA. [Maiolino, R.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Maiolino, R.] Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Teng, S. H.] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Veilleux, S (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM veilleux@astro.umd.edu; marcio@astro.umd.edu FU NASA [1427277, 1454738, 1364043, 1435724, 1456609]; Alexander von Humboldt Foundation; Spanish Ministerio de Economia y Competitividad [AYA2010-21697-C05-0, FIS2012-39162-C06-01]; U.S. Office of Naval Research; National Aeronautics and Space Administration FX We thank the referee for suggesting changes that helped improve this paper. Support for this work was provided by NASA through Herschel contracts 1427277 and 1454738 (S. V. and M.M.) and contracts 1364043, 1435724, and 1456609 (J.F.). S. V. also acknowledges support from the Alexander von Humboldt Foundation for a "renewed visit" to Germany following up the original 2009 award, and thanks the host institution, MPE Garching, where a portion of this paper was written. E. G.-A. is a Research Associate at the Harvard-Smithsonian Center for Astrophysics, and thanks the support by the Spanish Ministerio de Economia y Competitividad under projects AYA2010-21697-C05-0 and FIS2012-39162-C06-01. Basic research in IR astronomy at the Naval Research Laboratory is funded by the U.S. Office of Naval Research. This research made use of PySpecKit, an open-source spectroscopic toolkit hosted at http://pyspeckit.bitbucket.org. This work has made use of NASA's Astrophysics Data System Abstract Service and 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 78 TC 107 Z9 107 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 OCT 10 PY 2013 VL 776 IS 1 AR 27 DI 10.1088/0004-637X/776/1/27 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 225UM UT WOS:000324989000027 ER PT J AU Wang, J Fischer, DA Barclay, T Boyajian, TS Crepp, JR Schwamb, ME Lintott, C Jek, KJ Smith, AM Parrish, M Schawinski, K Schmitt, JR Giguere, MJ Brewer, JM Lynn, S Simpson, R Hoekstra, AJ Jacobs, TL LaCourse, D Schwengeler, HM Chopin, M Herszkowicz, R AF Wang, Ji Fischer, Debra A. Barclay, Thomas Boyajian, Tabetha S. Crepp, Justin R. Schwamb, Megan E. Lintott, Chris Jek, Kian J. Smith, Arfon M. Parrish, Michael Schawinski, Kevin Schmitt, Joseph R. Giguere, Matthew J. Brewer, John M. Lynn, Stuart Simpson, Robert Hoekstra, Abe J. Jacobs, Thomas Lee LaCourse, Daryll Schwengeler, Hans Martin Chopin, Mike Herszkowicz, Rafal TI PLANET HUNTERS. V. A CONFIRMED JUPITER-SIZE PLANET IN THE HABITABLE ZONE AND 42 PLANET CANDIDATES FROM THE KEPLER ARCHIVE DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: detection; techniques: photometric; techniques: radial velocities; techniques: spectroscopic; surveys ID SOLAR-TYPE STARS; INPUT CATALOG; CHROMOSPHERIC ACTIVITY; LIGHT CURVES; II. ANALYSIS; DATA RELEASE; GALAXY ZOO; M-DWARF; KECK; EXOPLANETS AB We report the latest Planet Hunter results, including PH2 b, a Jupiter-size (R-PL = 10.12 +/- 0.56 R-circle plus) planet orbiting in the habitable zone of a solar-type star. PH2 b was elevated from candidate status when a series of false-positive tests yielded a 99.9% confidence level that transit events detected around the star KIC 12735740 had a planetary origin. Planet Hunter volunteers have also discovered 42 new planet candidates in the Kepler public archive data, of which 33 have at least 3 transits recorded. Most of these transit candidates have orbital periods longer than 100 days and 20 are potentially located in the habitable zones of their host stars. Nine candidates were detected with only two transit events and the prospective periods are longer than 400 days. The photometric models suggest that these objects have radii that range between those of Neptune and Jupiter. These detections nearly double the number of gas-giant planet candidates orbiting at habitable-zone distances. We conducted spectroscopic observations for nine of the brighter targets to improve the stellar parameters and we obtained adaptive optics imaging for four of the stars to search for blended background or foreground stars that could confuse our photometric modeling. We present an iterative analysis method to derive the stellar and planet properties and uncertainties by combining the available spectroscopic parameters, stellar evolution models, and transiting light curve parameters, weighted by the measurement errors. Planet Hunters is a citizen science project that crowd sources the assessment of NASA Kepler light curves. The discovery of these 43 planet candidates demonstrates the success of citizen scientists at identifying planet candidates, even in longer period orbits with only two or three transit events. C1 [Wang, Ji; Fischer, Debra A.; Boyajian, Tabetha S.; Schmitt, Joseph R.; Giguere, Matthew J.; Brewer, John M.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Barclay, Thomas] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Barclay, Thomas] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA. [Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Schwamb, Megan E.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Schwamb, Megan E.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Lintott, Chris; Smith, Arfon M.; Parrish, Michael; Lynn, Stuart] Adler Planetarium, Chicago, IL 60605 USA. [Schawinski, Kevin] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. RP Wang, J (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA. EM ji.wang@yale.edu OI Smith, Arfon/0000-0002-3957-2474; Schmitt, Joseph/0000-0003-1874-0552; Brewer, John/0000-0002-9873-1471; Schwamb, Megan/0000-0003-4365-1455; Schawinski, Kevin/0000-0001-5464-0888; Wang, Ji/0000-0002-4361-8885; Fischer, Debra/0000-0003-2221-0861 FU Yale University; NASA [10-OUTRCH.210-0001, ADAP12-0172, NAS5-26555]; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-100325]; American Philosophical Society; Swiss National Science Foundation [PP00P2_138979/1]; Leverhulme Trust; Alfred P. Sloan foundation; NASA JPL's PlanetQuest program; National Science Foundation [DRL-0941610]; National Aeronautics and Space Administration; NASA Science Mission directorate; NASA Office of Space Science [NNX09AF08G] FX D.F. acknowledges funding support for PlanetHunters.org from Yale University and support from the NASA Supplemental Outreach Award, 10-OUTRCH.210-0001, and the NASA ADAP12-0172. M. E. S. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-100325 and in part by an American Philosophical Society Grant. K. S. gratefully acknowledges support from Swiss National Science Foundation grant PP00P2_138979/1. The Zooniverse is supported by The Leverhulme Trust and by the Alfred P. Sloan foundation. Planet Hunters is supported in part by NASA JPL's PlanetQuest program. The Talk system used by Planet Hunters was built during work supported by the National Science Foundation under grant No. DRL-0941610. We gratefully acknowledge the dedication and achievements of the Kepler science team and all those who contributed to the success of the mission. We acknowledge use of public release data served by the NASA/IPAC/NExScI Star and Exoplanet Database, 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 paper includes data collected by the Kepler spacecraft and we gratefully acknowledge the entire Kepler mission team's efforts in obtaining and providing the light curves used in this analysis. Funding for the Kepler mission is provided by the NASA Science Mission directorate. The publicly released Kepler light curves were obtained from the Mikulski Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-Hubble Space Telescope data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. NR 66 TC 23 Z9 23 U1 1 U2 17 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2013 VL 776 IS 1 AR 10 DI 10.1088/0004-637X/776/1/10 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 225UM UT WOS:000324989000010 ER PT J AU Gilbert, HR Inglis, AR Mays, ML Ofman, L Thompson, BJ Young, CA AF Gilbert, H. R. Inglis, A. R. Mays, M. L. Ofman, L. Thompson, B. J. Young, C. A. TI ENERGY RELEASE FROM IMPACTING PROMINENCE MATERIAL FOLLOWING THE 2011 JUNE 7 ERUPTION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: corona; Sun: filaments, prominences; Sun: flares ID SEQUENTIAL CHROMOSPHERIC BRIGHTENINGS; GLOBAL EUV WAVE; ABSORPTION FEATURES; FILAMENT ERUPTION; ATOMIC DATABASE; MASS; SDO/AIA; SUN; INSTABILITIES; OSCILLATIONS AB Solar filaments exhibit a range of eruptive-like dynamic activity, ranging from the full or partial eruption of the filament mass and surrounding magnetic structure as a coronal mass ejection to a fully confined or failed eruption. On 2011 June 7, a dramatic partial eruption of a filament was observed by multiple instruments on board the Solar Dynamics Observatory (SDO) and Solar-Terrestrial Relations Observatory. One of the interesting aspects of this event is the response of the solar atmosphere as non-escaping material falls inward under the influence of gravity. The impact sites show clear evidence of brightening in the observed extreme ultraviolet wavelengths due to energy release. Two plausible physical mechanisms for explaining the brightening are considered: heating of the plasma due to the kinetic energy of impacting material compressing the plasma, or reconnection between the magnetic field of low-lying loops and the field carried by the impacting material. By analyzing the emission of the brightenings in several SDO/Atmospheric Imaging Assembly wavelengths, and comparing the kinetic energy of the impacting material (7.6 x 10(26)-5.8 x 10(27) erg) to the radiative energy (approximate to 1.9 x 10(25)-2.5 x 10(26) erg), we find the dominant mechanism of energy release involved in the observed brightening is plasma compression. C1 [Gilbert, H. R.; Inglis, A. R.; Mays, M. L.; Ofman, L.; Thompson, B. J.; Young, C. A.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Inglis, A. R.; Mays, M. L.; Ofman, L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Gilbert, HR (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA. RI Inglis, Andrew/D-7674-2012; Thompson, Barbara/C-9429-2012 FU NASA [NNX10AN10G, NNX12AB34G] FX L.O. acknowledges NASA grants NNX10AN10G and NNX12AB34G. The authors are grateful to the SDO/AIA science team for making available the data used in this study. We also thank Terry Kucera for insightful conversations regarding cross-sections. L.O. thanks Peter Israelevich for useful discussions. NR 36 TC 19 Z9 19 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 10 PY 2013 VL 776 IS 1 AR UNSP L12 DI 10.1088/2041-8205/776/1/L12 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 224TX UT WOS:000324913500012 ER PT J AU MacKay, RA Gabb, TP Nathal, MV AF MacKay, R. A. Gabb, T. P. Nathal, M. V. TI Microstructure-sensitive creep models for nickel-base superalloy single crystals SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article DE Nickel base superalloys; Single crystals; Creep; Gamma prime; Regression; Lattice mismatch ID HIGH-TEMPERATURE CREEP; DEFORMATION-BEHAVIOR; VOLUME FRACTION; CMSX-4; PARAMETERS; TANTALUM; TUNGSTEN; COBALT AB Microstructure-sensitive creep models have been developed for Ni-base superalloy single crystals. Creep rupture testing was conducted on fourteen single crystal alloys at two applied stress levels at each of two temperatures, 982 and 1093 degrees C. The variation in creep lives among the different alloys could be explained with regression models containing relatively few microstructural parameters. At 982 degrees C, gamma-gamma' lattice mismatch, gamma' volume fraction, and initial gamma' size were statistically significant in explaining the creep rupture lives. At 1093 degrees C, only lattice mismatch and gamma' volume fraction were significant. These models could explain from 84% to 94% of the variation in creep lives, depending on test condition. Longer creep lives were associated with alloys having more negative lattice mismatch, lower gamma' volume fractions, and finer gamma' sizes. The gamma-gamma' lattice mismatch exhibited the strongest influence of all the microstructural parameters at both temperatures. Although a majority of the alloys in this study were stable with respect to topologically close packed (TCP) phases, it appeared that up to similar to 2 vol% TCP phase did not affect the 1093 degrees C creep lives under applied stresses that produced lives of similar to 200-300 h. In contrast, TCP phase contents of similar to 2 vol% were detrimental at lower applied stresses where creep lives were longer. Published by Elsevier B.V. C1 [MacKay, R. A.; Gabb, T. P.; Nathal, M. V.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP MacKay, RA (reprint author), NASA, Glenn Res Ctr, 21000 Brookpark Rd, Cleveland, OH 44135 USA. EM Rebecca.A.MacKay@nasa.gov FU Fixed Wing project under NASA's Fundamental Aeronautics Program FX The authors wish to acknowledge Dr. Anita Garg of U. Toledo for performing SEM microscopy on the gamma-gamma' microstructures. This work was supported by the Fixed Wing project under NASA's Fundamental Aeronautics Program. NR 46 TC 6 Z9 6 U1 3 U2 34 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0921-5093 J9 MAT SCI ENG A-STRUCT JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process. PD OCT 10 PY 2013 VL 582 BP 397 EP 408 DI 10.1016/j.msea.2013.04.072 PG 12 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA 220EV UT WOS:000324566100053 ER PT J AU Moreno-Madrinan, MJ Fischer, AM AF Moreno-Madrinan, Max J. Fischer, Andrew M. TI Performance of the MODIS FLH algorithm in estuarine waters: a multi-year (2003-2010) analysis from Tampa Bay, Florida (USA) SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID INDUCED CHLOROPHYLL FLUORESCENCE; REMOTE-SENSING ALGORITHMS; NATURAL FLUORESCENCE; COASTAL WATERS; OCEAN COLOR; A FLUORESCENCE; QUANTUM YIELD; PHYTOPLANKTON; REFLECTANCE; PHOTOSYNTHESIS AB Although satellite technology promises great usefulness for the consistent monitoring of chlorophyll- concentration in estuarine and coastal waters, the complex optical properties commonly found in these types of waters seriously challenge the application of this technology. Blue-green ratio algorithms are susceptible to interference from water constituents, different from phytoplankton, which dominate the remote-sensing signal. Alternatively, modelling and laboratory studies have not shown a decisive position on the use of near-infrared (NIR) algorithms based on the sun-induced chlorophyll fluorescence signal. In an analysis of a multi-year (2003-2010) in situ monitoring data set from Tampa Bay, Florida (USA), as a case, this study assesses the relationship between the fluorescence line height (FLH) product from the Moderate Resolution Imaging Spectrometer (MODIS) and chlorophyll-alpha. C1 [Moreno-Madrinan, Max J.] Indiana Univ, Richard M Fairbanks Sch Publ Hlth, Dept Environm Hlth Sci, Indianapolis, IN 46202 USA. [Fischer, Andrew M.] Univ Tasmania, Australian Maritime Coll, Natl Ctr Marine Conservat & Resource Sustainabil, Launceston, Tas 7250, Australia. [Moreno-Madrinan, Max J.] NASA Postdoctoral Program, SERVIR, Huntsville, AL 35805 USA. [Moreno-Madrinan, Max J.] NASA, MSFC, Global Hydrol & Climate Ctr, Huntsville, AL 35805 USA. RP Fischer, AM (reprint author), Indiana Univ, Richard M Fairbanks Sch Publ Hlth, Dept Environm Hlth Sci, Indianapolis, IN 46202 USA. EM andy.fischer@utas.edu.au OI Fischer, Andrew/0000-0001-5284-6428 FU SERVIR/MSFC through NASA; Oak Ridge Associated Universities FX We express our great appreciation to the Environmental Protection Commission of Hillsborough County (EPCHC) for sharing Tampa Bay water quality data and particularly to Dr Rick Garrity, Mr Richard Boler, and Mr Joe Barron from EPCHC for their assistance. MODIS data collection and processing was made possible through the efforts of MODAPS services at the NASA GSFC. We also acknowledge the SeaDAS Development group at NASA GSFC for the use of the SeaDAS software to process the MODIS imagery. This research was partially funded by SERVIR/MSFC through the NASA Postdoctoral Program under contract with Oak Ridge Associated Universities. We would also like to express our gratitude to Dr Doug Rickman from NASA/MSFC along with unknown reviewers for examining the manuscript and providing valuable input. NR 68 TC 3 Z9 3 U1 1 U2 40 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND SN 0143-1161 EI 1366-5901 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PD OCT 10 PY 2013 VL 34 IS 19 BP 6467 EP 6483 DI 10.1080/01431161.2013.804227 PG 17 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 180QI UT WOS:000321609300001 ER PT J AU Davami, K Weathers, A Kheirabi, N Mortazavi, B Pettes, MT Shi, L Lee, JS Meyyappan, M AF Davami, Keivan Weathers, Annie Kheirabi, Nazli Mortazavi, Bohayra Pettes, Michael T. Shi, Li Lee, Jeong-Soo Meyyappan, M. TI Thermal conductivity of ZnTe nanowires SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID MOLECULAR-DYNAMICS SIMULATIONS; THERMOELECTRIC FIGURE; SEMICONDUCTOR NANOWIRES; SILICON NANOWIRES; RESISTANCE; TRANSPORT; MERIT; NANOSTRUCTURES AB The thermal conductivity of individual ZnTe nanowires (NWs) was measured using a suspended micro-bridge device with built-in resistance thermometers. A collection of NWs with different diameters were measured, and strong size-dependent thermal conductivity was observed in these NWs. Compared to bulk ZnTe, NWs with diameters of 280 and 107 nm showed approximately three and ten times reduction in thermal conductivity, respectively. Such a reduction can be attributed to phonon-surface scattering. The contact thermal resistance and the intrinsic thermal conductivities of the nanowires were obtained through a combination of experiments and molecular dynamic simulations. The obtained thermal conductivities agree well with theoretical predictions. (C) 2013 AIP Publishing LLC. C1 [Davami, Keivan; Kheirabi, Nazli; Lee, Jeong-Soo; Meyyappan, M.] Pohang Univ Sci & Technol POSTECH, Dept IT Convergence Engn, Pohang, South Korea. [Weathers, Annie; Pettes, Michael T.; Shi, Li] Univ Texas Austin, Dept Mech Engn, Austin, TX 78712 USA. [Mortazavi, Bohayra] Ctr Rech Publ Henri Tudor, Dept Adv Mat & Struct, L-4002 Esch Sur Alzette, Luxembourg. [Mortazavi, Bohayra] Univ Strasbourg, Inst Mecan Fluideset Solides, CNRS, F-67000 Strasbourg, France. [Shi, Li] Univ Texas Austin, Ctr Nano & Mol Sci & Technol, Texas Mat Inst, Austin, TX 78712 USA. [Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Meyyappan, M (reprint author), Pohang Univ Sci & Technol POSTECH, Dept IT Convergence Engn, Pohang, South Korea. EM m.meyyappan@nasa.gov RI Shi, Li/C-8123-2013; Pettes, Michael/D-3572-2012 OI Shi, Li/0000-0002-5401-6839; Pettes, Michael/0000-0001-6862-6841 FU World Class University program through the National Research Foundation of Korea; Ministry of Education, Science and Technology [R31-2008-000-10100-0]; Center for Advanced Soft Electronics under the Global Frontier Research Program of the Ministry of Education, Science and Technology, Korea [2011-0031638] FX This work was supported by the World Class University program through the National Research Foundation of Korea funded by the Ministry of Education, Science and Technology under Project No. R31-2008-000-10100-0. Moreover, the research was also partly supported by a grant (Code No. 2011-0031638) from the Center for Advanced Soft Electronics under the Global Frontier Research Program of the Ministry of Education, Science and Technology, Korea. Most of this work was done at UT Austin during Keivan Davami's visit and Professor Shi's group is acknowledged for hosting the visit. Bohayra Mortazavi greatly appreciates Dr. Toniazzo at CRP Henri-Tudor for providing computational facilities. NR 32 TC 8 Z9 8 U1 1 U2 31 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-8979 EI 1089-7550 J9 J APPL PHYS JI J. Appl. Phys. PD OCT 7 PY 2013 VL 114 IS 13 AR 134314 DI 10.1063/1.4824687 PG 7 WC Physics, Applied SC Physics GA 232JB UT WOS:000325488700049 ER PT J AU Bogucki, DJ Spiers, G AF Bogucki, D. J. Spiers, G. TI What percentage of the oceanic mixed layer is accessible to marine lidar? Global and the Gulf of Mexico prospective SO OPTICS EXPRESS LA English DT Article ID SEA-WATER; SCATTERING COEFFICIENT; BACKWARD DIRECTION; BEAM ATTENUATION; DEPTHS; MODEL AB The oceanic mixed layer is a nearly homogenous region of the upper ocean which, in principle, has a little or no variation in turbulence strength, temperature or density with depth. This layer mediates oceanic fluxes of gas, momentum and heat. Here, based on the chosen [1] marine Lidar system, we have carried out estimates of the depth penetration of the Lidar when compared to the local mixed layer depth. On average, we have found that at least 50% of the global oceanic mixed layer depth is accessible to the Lidar observations. When operating in a single scattering mode, which is more attenuating but more amenable to analysis, the modeled Lidar was found to access 0.4 of global mixed layer depth in half of the cases. The single scattering Lidar was found to access a large fraction of the equatorial mixed layer - a region very important when addressing global climatic issues. In a coastal environment such as the Gulf of Mexico the single scattering Lidar was found to penetrate upper half of the mixed layer, underscoring the potential for Lidar to address environmental issues there. (C) 2013 Optical Society of America C1 [Bogucki, D. J.] Texas A&M Univ, Dept Phys & Environm Sci, Corpus Christi, TX 78412 USA. [Spiers, G.] Jet Prop Lab, Pasadena, CA 91109 USA. RP Bogucki, DJ (reprint author), Texas A&M Univ, Dept Phys & Environm Sci, Corpus Christi, TX 78412 USA. EM darek.bogucki@tamucc.edu FU BP/The Gulf of Mexico Research Initiative; JPL/NASA FX Analyses and visualizations used in this paper were produced with the Giovanni online data system, developed and maintained by the NASA Goddard Earth Sciences (GES) Data and Information Services Center (DISC) [37]. This research was made possible in part by a grant from BP/The Gulf of Mexico Research Initiative, and in part by JPL/NASA funds. NR 36 TC 2 Z9 2 U1 1 U2 9 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 OCT 7 PY 2013 VL 21 IS 20 BP 23997 EP 24014 DI 10.1364/OE.21.023997 PG 18 WC Optics SC Optics GA 233EU UT WOS:000325549800095 PM 24104310 ER PT J AU Andersson, N Baker, J Belczynski, K Bernuzzi, S Berti, E Cadonati, L Cerda-Duran, P Clark, J Favata, M Finn, LS Fryer, C Giacomazzo, B Gonzalez, JA Hendry, M Heng, IS Hild, S Johnson-McDaniel, N Kalmus, P Klimenko, S Kobayashi, S Kokkotas, K Laguna, P Lehner, L Levin, J Liebling, S MacFadyen, A Mandel, I Marka, S Marka, Z Neilsen, D O'Brien, P Perna, R Read, J Reisswig, C Rodriguez, C Ruffert, M Schnetter, E Searle, A Shawhan, P Shoemaker, D Soderberg, A Sperhake, U Sutton, P Tanvir, N Was, M Whitcomb, S AF Andersson, Nils Baker, John Belczynski, Krzystof Bernuzzi, Sebastiano Berti, Emanuele Cadonati, Laura Cerda-Duran, Pablo Clark, James Favata, Marc Finn, Lee Samuel Fryer, Chris Giacomazzo, Bruno Antonio Gonzalez, Jose Hendry, Martin Heng, Ik Siong Hild, Stefan Johnson-McDaniel, Nathan Kalmus, Peter Klimenko, Sergei Kobayashi, Shiho Kokkotas, Kostas Laguna, Pablo Lehner, Luis Levin, Janna Liebling, Steve MacFadyen, Andrew Mandel, Ilya Marka, Szabolcs Marka, Zsuzsa Neilsen, David O'Brien, Paul Perna, Rosalba Read, Jocelyn Reisswig, Christian Rodriguez, Carl Ruffert, Max Schnetter, Erik Searle, Antony Shawhan, Peter Shoemaker, Deirdre Soderberg, Alicia Sperhake, Ulrich Sutton, Patrick Tanvir, Nial Was, Michal Whitcomb, Stan TI The transient gravitational-wave sky SO CLASSICAL AND QUANTUM GRAVITY LA English DT Review ID GAMMA-RAY BURSTS; CORE-COLLAPSE SUPERNOVAE; MASS BLACK-HOLES; DIFFERENTIALLY ROTATING STARS; ACCRETING NEUTRON-STARS; ARMED SPIRAL INSTABILITY; POLOIDAL MAGNETIC-FIELDS; BAR-MODE INSTABILITY; EARLY WARNING SYSTEM; SPIN-DOWN LIMIT AB Interferometric detectors will very soon give us an unprecedented view of the gravitational-wave sky, and in particular of the explosive and transient Universe. Now is the time to challenge our theoretical understanding of short-duration gravitational-wave signatures from cataclysmic events, their connection to more traditional electromagnetic and particle astrophysics, and the data analysis techniques that will make the observations a reality. This paper summarizes the state of the art, future science opportunities, and current challenges in understanding gravitational-wave transients. C1 [Andersson, Nils] Univ Southampton, Sch Math, Southampton SO17 1BJ, Hants, England. [Baker, John] NASA GSFC, Gravitat Phys Lab, Greenbelt, MD 20771 USA. [Belczynski, Krzystof] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland. [Belczynski, Krzystof] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA. [Bernuzzi, Sebastiano; Johnson-McDaniel, Nathan] Univ Jena, Inst Theoret Phys, D-07743 Jena, Germany. [Berti, Emanuele] Univ Mississippi, Dept Phys & Astron, University, MS 38677 USA. [Berti, Emanuele; Reisswig, Christian; Sperhake, Ulrich] CALTECH, Pasadena, CA 91125 USA. [Cadonati, Laura; Clark, James] Univ Massachusetts, Dept Phys, Amherst, MA 01003 USA. [Cerda-Duran, Pablo] Univ Valencia, Dept Astron & Astrofis, E-46100 Burjassot, Spain. [Favata, Marc] Montclair State Univ, Montclair, NJ 07043 USA. [Finn, Lee Samuel] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Finn, Lee Samuel] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Fryer, Chris] Los Alamos Natl Lab, CCS 2, Los Alamos, NM 87545 USA. [Giacomazzo, Bruno; Perna, Rosalba] Univ Colorado, JILA, Boulder, CO 80309 USA. [Giacomazzo, Bruno; Perna, Rosalba] NIST, Boulder, CO 80309 USA. [Antonio Gonzalez, Jose] Univ Michoacana, Inst Fis & Matemat, Morelia 58040, Michoacan, Mexico. [Hendry, Martin; Heng, Ik Siong] Univ Glasgow, Sch Phys & Astron, SUPA, Glasgow G12 8QQ, Lanark, Scotland. [Hild, Stefan] Univ Glasgow, Inst Gravitat Res, Glasgow G12 8QQ, Lanark, Scotland. [Kalmus, Peter; Searle, Antony; Whitcomb, Stan] CALTECH, LIGO Lab, Pasadena, CA 91125 USA. [Klimenko, Sergei] Univ Florida, Gainesville, FL 32611 USA. [Kobayashi, Shiho] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Kokkotas, Kostas] Univ Tubingen, IAAT, D-72076 Tubingen, Germany. [Laguna, Pablo; Shoemaker, Deirdre] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Lehner, Luis; Schnetter, Erik] Perimeter Inst Theoret Phys, Waterloo, ON, Canada. [Levin, Janna] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Liebling, Steve] Long Isl Univ, Brookville, NY 11548 USA. [MacFadyen, Andrew] New York Univ, Dept Phys, New York, NY 10003 USA. [Mandel, Ilya] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Marka, Szabolcs] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Marka, Zsuzsa] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Neilsen, David] Brigham Young Univ, Dept Phys & Astron, Provo, UT 84602 USA. [O'Brien, Paul; Tanvir, Nial] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Read, Jocelyn] Calif State Univ Fullerton, Dept Phys, Fullerton, CA 92831 USA. [Rodriguez, Carl] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Ruffert, Max] Univ Edinburgh, Sch Math, Edinburgh EH16 5JN, Midlothian, Scotland. [Ruffert, Max] Univ Edinburgh, Maxwell Inst, Edinburgh EH16 5JN, Midlothian, Scotland. [Schnetter, Erik] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. [Schnetter, Erik] Louisiana State Univ, Ctr Computat & Technol, Baton Rouge, LA 70803 USA. [Shawhan, Peter] Univ Maryland, College Pk, MD 20742 USA. [Soderberg, Alicia] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sperhake, Ulrich] Ctr Math Sci, DAMTP, Cambridge CB3 0WA, England. [Sperhake, Ulrich] CENTRA IST, Lisbon, Portugal. [Sutton, Patrick] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Was, Michal] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. RP Andersson, N (reprint author), Univ Southampton, Sch Math, Southampton SO17 1BJ, Hants, England. EM plaguna@gatech.edu RI Hild, Stefan/A-3864-2010; Kokkotas, Kostas/B-7878-2010; Cerda-Duran, Pablo/D-7857-2015; Finn, Lee Samuel/A-3452-2009; Neilsen, David/J-4862-2015; Berti, Emanuele/C-9331-2016; Giacomazzo, Bruno/I-8088-2012 OI Schnetter, Erik/0000-0002-4518-9017; Reisswig, Christian/0000-0001-6855-9351; MacFadyen, Andrew/0000-0002-0106-9013; Mandel, Ilya/0000-0002-6134-8946; Kokkotas, Kostas/0000-0001-6048-2919; Cerda-Duran, Pablo/0000-0003-4293-340X; Finn, Lee Samuel/0000-0002-3937-0688; Neilsen, David/0000-0002-6142-5542; Berti, Emanuele/0000-0003-0751-5130; Giacomazzo, Bruno/0000-0002-6947-4023 FU National Science Foundation [0946361, 1231548, PHY-0847182, PHY-1055103, PHY-0653550, PHY-0955773, PHY-0653462, CBET-0940924, PHY-0969857, 0903973, 1205864, PHY-0925345, PHY-0955825]; 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 Educacion y Ciencia; Conselleria d'Economia, Hisenda i Innovacio of the Govern de les Illes Balears; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; National Aeronautics and Space Administration; Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation; Alfred P Sloan Foundation; NSF [PHY11-25915, HRD 1242090, AST-1009396]; Columbia University in the City of New York; NASA [NNX09AV06A, NNX12AO67G]; German Science Foundation [SFB/TR7]; NSERC; Industry Canada; Province of Ontario through the Ministry of Research and Innovation; Spanish Ministerio de Educacion y Ciencia [AYA 2010-21097-C03-01]; Generalitat Valenciana [PROMETEO-2009-103]; ERC [CAMAP-259276]; US Department of Energy [W-7405-ENG-36] FX The 'Gravitational Wave Bursts' workshops in Chichen-Itza, Mexico (9-1 December 2009) and Tobermory, Scotland (29-31 May 2012) were supported by National Science Foundation grant numbers 0946361 and 1231548. The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory and 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. 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 Educacion y Ciencia, the Conselleria d'Economia, Hisenda i Innovacio of the Govern de les Illes Balears, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P Sloan Foundation. We thank the Kavli Institute for Theoretical Physics at UC-Santa Barbara, supported in part by NSF grant PHY11-25915, for hosting the workshop 'Chirps, Mergers and Explosions: The Final Moments of Coalescing Compact Binaries.' The Columbia Experimental Gravity group is grateful for the generous support from Columbia University in the City of New York and from the National Science Foundation under cooperative agreement PHY-0847182. E.B. is supported by National Science Foundation through CAREER Award Number PHY-1055103. KB acknowledges NASA grant number NNX09AV06A and NSF grant numbers HRD 1242090 awarded to the Center for Gravitational Wave Astronomy, UTB. SB and KK acknowledge support from the German Science Foundation SFB/TR7 'Gravitational Wave Astronomy.' LC acknowledges National Science Foundation grant numbers PHY-0653550 and PHY-0955773. LL was supported in part by an NSERC through discovery grant. Research at Perimeter Institute is supported through Industry Canada and by the Province of Ontario through the Ministry of Research and Innovation. PCD acknowledges Spanish Ministerio de Educacion y Ciencia grant number AYA 2010-21097-C03-01, Generalitat Valenciana grant number PROMETEO-2009-103 and ERC starting grant number CAMAP-259276. The work of CF is under the auspices of the US Department of Energy, and supported by its contract W-7405-ENG-36 to Los Alamos National Laboratory. LSF acknowledges National Science Foundation grant numbers PHY-0653462, CBET-0940924 and PHY-0969857. BG and RP acknowledge support from NSF grant number AST-1009396 and NASA grant number NNX12AO67G. PL acknowledges National Science Foundation grant numbers 0903973 and 1205864. DMS acknowledges National Science Foundation grant numbers PHY-0925345 and PHY-0955825. We wish to thank Christian Ott and Harald Pfeiffer for useful contributions to this review. NR 421 TC 24 Z9 24 U1 1 U2 22 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 OCT 7 PY 2013 VL 30 IS 19 AR 193002 DI 10.1088/0264-9381/30/19/193002 PG 45 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 223PW UT WOS:000324819900002 ER PT J AU Fortenberry, RC Huang, XC Crawford, TD Lee, TJ AF Fortenberry, Ryan C. Huang, Xinchuan Crawford, T. Daniel Lee, Timothy J. TI The 1 (3)A ' HCN and 1 (3)A ' HCO+ Vibrational Frequencies and Spectroscopic Constants from Quartic Force Fields SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID SHELL HARTREE-FOCK; COUPLED-CLUSTER THEORY; EXCITED-STATES; PERTURBATION-THEORY; HYDROGEN-CYANIDE; FUNDAMENTAL-BAND; WAVE-FUNCTIONS; BASIS-SETS; ENERGY; IONS AB Building on previous studies involving coupled cluster quartic force fields for the description of spectroscopic constants and vibrational frequencies of astronomically relevant molecules, this work applies the same techniques to the elucidation of such properties for the bent 1 (3)A' state of HCN and the isoelectronic 1 (3)A' HCO+. Core correlation is treated both by explicit means and as a correction. Each approach gives closely comparable spectroscopic constants and vibrational frequencies once more, indicating that the composite method is a viable and less costly alternative. We are providing fundamental vibrational frequencies for these systems where agreement with experiment in previous studies has been within 4 cm(-1) or better. Frequencies for the first overtones and combination bands as well as various spectroscopic constants are also reported. C1 [Fortenberry, Ryan C.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA. [Crawford, T. Daniel] Virginia Tech, Dept Chem, Blacksburg, VA 24061 USA. RP Fortenberry, RC (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Ryan.C.Fortenberry@nasa.gov; Timothy.J.Lee@nasa.gov RI Lee, Timothy/K-2838-2012; HUANG, XINCHUAN/A-3266-2013; Crawford, Thomas/A-9271-2017 OI Crawford, Thomas/0000-0002-7961-7016 FU National Science Foundation Multi-User Chemistry Research Instrumentation and Facility (CRIF:MU) [CHE-0741927]; NASA/SETI Institute Cooperative Agreement [NNX12AG96A]; NASA [10-APRA10-0167] FX The NASA Postdoctoral Program administered by Oak Ridge Associated Universities through a contract with NASA funded the work done by R.C.F. T.D.C. and R.C.F. acknowledge support from the National Science Foundation Multi-User Chemistry Research Instrumentation and Facility (CRIF:MU) award CHE-0741927, which provided the computational hardware utilized in this study. X.H. acknowledges funding from the NASA/SETI Institute Cooperative Agreement NNX12AG96A. NASA Grant 10-APRA10-0167 funded the work done by T.J.L. Drs. John C. Pearson and Shanshan Yu of the Jet Propulsion Laboratory deserve the authors' thanks for broaching the importance of this project and for engaging in beneficial discussions related to the work. The CheMVP program was utilized in the creation of the figures. T.J.L. thanks Professor Takeshi Oka for his encouragement and insight in the study of astrochemistry over much of the last 30 years. NR 61 TC 11 Z9 11 U1 0 U2 8 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 EI 1520-5215 J9 J PHYS CHEM A JI J. Phys. Chem. A PD OCT 3 PY 2013 VL 117 IS 39 BP 9324 EP 9330 DI 10.1021/jp309243s PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 243EV UT WOS:000326300600003 PM 23121098 ER PT J AU Sprague, MK Mertens, LA Widgren, HN Okumura, M Sander, SP McCoy, AB AF Sprague, Matthew K. Mertens, Laura A. Widgren, Heather N. Okumura, Mitchio Sander, Stanley P. McCoy, Anne B. TI Cavity Ringdown Spectroscopy of the Hydroxy-Methyl-Peroxy Radical SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID (A)OVER-TILDE-(X)OVER-TILDE ELECTRONIC-TRANSITION; GAS-PHASE REACTION; PHOTO-OXIDATION; GASEOUS FORMALDEHYDE; DOWN SPECTROSCOPY; FLASH-PHOTOLYSIS; CROSS-SECTIONS; MECHANISM; KINETICS; HO2 AB We report vibrational and electronic spectra of the hydroxy-methylperoxy radical (HOCH2OO center dot or HMP), which was formed as the primary product of the reaction of the hydroperoxy radical, HO2 center dot, and formaldehyde, HCHO. The vi vibrational (OH stretch) 'spectrum and the A <- X electronic spectrum of HMP were detected by infrared cavity ringdown spectroscopy (IR-CRDS), and assignments were verified with density functional calculations. The HMP radical was generated in reactions of HCHO with HO2 center dot. Free radical reactions were initiated by pulsed laser photolysis (PLP) of Cl-2 in the presence of HCHO and O-2 in a flow reactor at 300-330 Torr and 295 K. IR-CRDS spectra were measured in mid-IR and near-IR regions over the ranges 3525-3700 cm(-1) (nu(1)) and 7250-7800 cm(-1) (A <- X) respectively, at a delay time 100 mu s after, photolysis. The vi spectrum had an origin at 3622 cm(-1) and exhibited partially resolved P- and R-branch contours and a small Qbranch. At these short delay times, spectral interference frorn'HOOH and HCOOH was minimal and could be subtracted. From B3LYP/6-31+G(d,p) calculations, we found that the anharmonic vibrational frequency and band contour predicted for the lowest energy conformer; HMP-A, were in good agreement with the observed spectrum. In the near-IR, we observed four well spaced vibronic bands, each with partially resolved rotational contours. We assigned the apparent origin of the A <- X electronic spectrum of HMP at 7389 cm(-1) and two bands to the blue to a progression in rib', the lowest torsional mode of the A state (vis' = 171 cm(-1)). The band furthest to the red was assigned as a hot band in v(15)'', leading to a ground state torsional frequency of (v(15 '') = 122 cm(-1)). We simulated the spectrum using second order vibrational perturbation theory (VPT2) with B3LYP/6-31+G(d,p) calculations at the minimum energy geometries of the HMP-A conformer on the X and A states. The predictions of the electronic origin frequency, torsional frequencies, anharmonicities, and rotational band contours matched the observed spectrum. We investigated the torsional modes more explicitly by computing potential energy surfaces of HMP as a function of the two dihedral angles THoco and rooco. Wave functions and energy levels were calculated on the basis of this potential surface; these results were used to calculate the Franck Condon factors, which reproduced the vibronic band intensities in the observed electronic spectrum. The transitions that we observed all involved states with wave functions localized on the minimum energy conformer, HMP-A. Our calculations indicated that the observed near-IR spectrum was that of the lowest energy 5( state conformer HMP-A, but that this conformer is not the lowest energy conformer in the A state, which remains unobserved. We estimated that the energy of this lowest conformer (HMP-B) of the A state is E-0 HMP-B) approximate to 7200 cm(-1), on the basis of the energy difference E-0(HMP-B) - E-0(HMP-A) on the A state computed at the B3LYP/6-31+G(d,p) level. C1 [Sprague, Matthew K.; Mertens, Laura A.; Widgren, Heather N.; Okumura, Mitchio] CALTECH, Arthur Amos Noyes Lab Chem Phys, Pasadena, CA 91125 USA. [Sander, Stanley P.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. [McCoy, Anne B.] Ohio State Univ, Dept Chem & Biochem, Columbus, OH 43210 USA. RP Okumura, M (reprint author), CALTECH, Arthur Amos Noyes Lab Chem Phys, MC 127-72, Pasadena, CA 91125 USA. EM mo@its.caltech.edu; Stanley.P.Sander@jpl.nasa.gov; mccoy@chemistry.ohio-state.edu RI Okumura, Mitchio/I-3326-2013; OI Okumura, Mitchio/0000-0001-6874-1137; Sprague, Matthew/0000-0002-3526-7077 FU National Aeronautics and Space Administration (NASA) Upper Atmosphere Research Program [NNX09AE21G, NNX12AI01G]; National Science Foundation (NSF) [CHE-0957490, CHE-1213347]; NASA Tropospheric Chemistry Program; National Aeronautics and Space Administration (NASA); National Defense Science and Engineering Graduate Fellowship; NSF Graduate Fellowship; Caltech Student-Faculty Programs office FX Financial support was provided by the National Aeronautics and Space Administration (NASA) Upper Atmosphere Research Program (grants NNX09AE21G and NNX12AI01G), the National Science Foundation (NSF, Grant CHE-0957490 for experimental work at Caltech and Grant CHE-1213347 for computational work by ABM), and the NASA Tropospheric Chemistry Program. Part of this research was carried out by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). We acknowledge support of a National Defense Science and Engineering Graduate Fellowship for M.K.S., an NSF Graduate Fellowship for LAM., and the Caltech Student-Faculty Programs office for H.N.W. through the Summer Undergraduate Research Fellowship program. We thank Dr. Andrew Mollner, who performed the initial setup of the experiment and the formaldehyde sampling system, Dr. Ralph Page for vital technical assistance and optimization of the spectrometer optics, Michael Roy for machining support, and Richard Gerhart for glassware construction and repair. We acknowledge the inspiration provided by Takeshi Oka for this work. NR 52 TC 5 Z9 5 U1 1 U2 55 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 OCT 3 PY 2013 VL 117 IS 39 BP 10006 EP 10017 DI 10.1021/jp400390y PG 12 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 243EV UT WOS:000326300600081 PM 23641685 ER PT J AU Drouin, BJ AF Drouin, Brian J. TI Isotopic Spectra of the Hydroxyl Radical SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID BEAM ELECTRIC RESONANCE; ROTATIONAL SPECTRUM; LABORATORY MEASUREMENT; MICROWAVE-SPECTRUM; GROUND-STATE; OH; OD; SPECTROSCOPY; PARAMETERS; HYPERFINE AB Rotational spectra of OH and its isotopologues have been precisely measured using high efficiency terahertz (THz) sources. The measurements are compared with existing data and are useful for global modeling. For the first time, microwave measurements of the Lambda-doubling transitions of the (OH)-O-17 isotopologue are combined with THz data successfully. Precise rotational, fine-structure, and hyperfine structure parameters for the (OH)-O-17 isotopologue are reported. An isotopically independent Dunham model for all isotopologues of (2)Pi OH nu < 3 is presented. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Drouin, BJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM brian.j.drouin@jpl.nasa.gov FU National Aeronautics and Space Administration FX The author would like to thank the reviewers and Edward Cohen for their comments on the manuscript. This paper presents research carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 69 TC 6 Z9 6 U1 2 U2 17 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 EI 1520-5215 J9 J PHYS CHEM A JI J. Phys. Chem. A PD OCT 3 PY 2013 VL 117 IS 39 BP 10076 EP 10091 DI 10.1021/jp400923z PG 16 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 243EV UT WOS:000326300600089 PM 23634899 ER PT J AU Michalski, JR Bleacher, JE AF Michalski, Joseph R. Bleacher, Jacob E. TI Supervolcanoes within an ancient volcanic province in Arabia Terra, Mars SO NATURE LA English DT Article ID THERMOKARST LAKES; GEOLOGIC RECORD; THARSIS REGION; MERIDIANI; HISTORY; CRUST; DISPERSAL; LANDFORMS; OUTCROPS; SULFUR AB Several irregularly shaped craters located within Arabia Terra, Mars, represent a new type of highland volcanic construct and together constitute a previously unrecognized Martian igneous province. Similar to terrestrial supervolcanoes, these low-relief paterae possess a range of geomorphic features related to structural collapse, effusive volcanism and explosive eruptions. Extruded lavas contributed to the formation of enigmatic highland ridged plains in Arabia Terra. Outgassed sulphur and erupted fine-grained pyroclastics from these calderas probably fed the formation of altered, layered sedimentary rocks and fretted terrain found throughout the equatorial region. The discovery of a new type of volcanic construct in the Arabia volcanic province fundamentally changes the picture of ancient volcanism and climate evolution on Mars. Other eroded topographic basins in the ancient Martian highlands that have been dismissed as degraded impact craters should be reconsidered as possible volcanic constructs formed in an early phase of widespread, disseminated magmatism on Mars. C1 [Michalski, Joseph R.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Michalski, Joseph R.] Nat Hist Museum, Dept Earth Sci, London SW7 5BD, England. [Bleacher, Jacob E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Michalski, JR (reprint author), Planetary Sci Inst, Tucson, AZ 85719 USA. EM michalski@psi.edu RI Bleacher, Jacob/D-1051-2012 OI Bleacher, Jacob/0000-0002-8499-4828 FU NASA Mars Data Analysis programme FX We thank H. Frey, B. Hynek, S. Wright, J. Zimbelman and L. Tornabene for discussions that improved the quality of the manuscript. Funding was provided by the NASA Mars Data Analysis programme. NR 50 TC 18 Z9 18 U1 4 U2 34 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD OCT 3 PY 2013 VL 502 IS 7469 BP 47 EP + DI 10.1038/nature12482 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 227IM UT WOS:000325106000028 PM 24091975 ER PT J AU Lee, JSF Tezak, EP Berejikian, BA AF Lee, Jonathan S. F. Tezak, Eugene P. Berejikian, Barry A. TI Ontogenetic Changes in Dispersal and Habitat Use in Hatchery-Reared Lingcod SO REVIEWS IN FISHERIES SCIENCE LA English DT Article DE Ophiodon elongatus; stock enhancement; before-after-control-impact; release methods; movement ID STOCK ENHANCEMENT; OPHIODON-ELONGATUS; POPULATION-STRUCTURE; PUGET-SOUND; RELEASE; SIZE; WASHINGTON; PATTERNS; TRACKING; PROGRAMS AB Preliminary experiments that optimize release methods pave the way to larger-scale releases and proper evaluation methods. One evaluation method is before-after-control-impact, which requires that more animals remain at release areas (site fidelity to impact areas) than disperse to control areas. This study tested whether there are release methods that maximize fidelity to the release area and minimize dispersal to nearby areas, which might enable a before-after-control-impact experiment. Lingcod that were 17-months old at release showed greater fidelity to release areas (23% remaining one year after release) than lingcod that were 9- and 11-months old at release. None of the 17- and 21-month-old release groups were detected on more distant structured habitats 44 weeks after release, but 8% and 13% of lingcod from the 9- and 11-month-old release groups were detected at distant structured habitat. Thus, releasing 17-month-old lingcod maximized fidelity to the release area and minimized dispersal to other areas. Differences in fidelity and dispersal rates among release-age groups may reflect ontogenetic changes in dispersal and habitat use patterns that have also been reported for wild lingcod. These behavioral similarities with wild lingcod also suggest that hatchery lingcod have potential to interact and integrate with wild lingcod in nature. C1 [Lee, Jonathan S. F.; Tezak, Eugene P.; Berejikian, Barry A.] NOAA Fisheries, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Manchester Res Stn, Manchester, WA 98353 USA. RP Lee, JSF (reprint author), NOAA Fisheries, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Manchester Res Stn, POB 130, Manchester, WA 98353 USA. EM jon.lee@noaa.gov FU Puget Sound Recreational Fisheries Enhancement Program (PSRFE); Science Consortium for Ocean Replenishment (SCORE) FX The authors thank Terry Wright (Northwest Indian Fisheries Commission) and the dive teams led by Mike Racine (Washington SCUBA Alliance) and Ocean Eveningsong (WDFW) for egg collections, and Matt Cook and Jeff Atkins for rearing the lingcod. Rob Endicott, Megan Moore, Katy Doctor, and Jeff Atkins provided occasional assistance in the field. MeganMoore and Rob Endicott also provided helpful discussion on acoustic telemetry. Wayne Palsson and James Beam helped with preliminary habitat assessments near Itsami. The authors are grateful to the Puget Sound Recreational Fisheries Enhancement Program (PSRFE) and the Science Consortium for Ocean Replenishment (SCORE) for financial support. NR 34 TC 1 Z9 1 U1 2 U2 4 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 1064-1262 EI 1547-6553 J9 REV FISH SCI JI Rev. Fish. Sci. PD OCT 2 PY 2013 VL 21 IS 3-4 SI SI BP 267 EP 275 DI 10.1080/10641262.2013.799391 PG 9 WC Fisheries SC Fisheries GA 252NO UT WOS:000327013000006 ER PT J AU Sahraoui, F Robert, P Goldstein, ML Khotyaintsev, YV AF Sahraoui, F. Robert, P. Goldstein, M. L. Khotyaintsev, Yu V. TI Comment on "Evidence of a Cascade and Dissipation of Solar-Wind Turbulence at the Electron Gyroscale" Reply SO PHYSICAL REVIEW LETTERS LA English DT Editorial Material ID SCALES C1 [Sahraoui, F.; Robert, P.] Ecole Polytech, CNRS, Lab Phys Plasmas, F-91120 Palaiseau, France. [Goldstein, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Khotyaintsev, Yu V.] Swedish Inst Space Phys, SE-75121 Uppsala, Sweden. RP Sahraoui, F (reprint author), Ecole Polytech, CNRS, Lab Phys Plasmas, F-91120 Palaiseau, France. EM fouad.sahraoui@lpp.polytechnique.fr NR 13 TC 2 Z9 2 U1 0 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD OCT 2 PY 2013 VL 111 IS 14 AR 149002 DI 10.1103/PhysRevLett.111.149002 PG 2 WC Physics, Multidisciplinary SC Physics GA 230UW UT WOS:000325369600027 PM 24138276 ER PT J AU Beauchamp, VB Koontz, SM Suss, C Hawkins, C Kyde, KL Schnase, JL AF Beauchamp, Vanessa B. Koontz, Stephanie M. Suss, Christine Hawkins, Chad Kyde, Kerrie L. Schnase, John L. TI An introduction to Oplismenus undulatifolius (Ard.) Roem. & Schult. (wavyleaf basketgrass), a recent invader in Mid-Atlantic forest understories SO JOURNAL OF THE TORREY BOTANICAL SOCIETY LA English DT Article DE deciduous forest; Fagus grandifolia; introduced species; Maximum Entropy Modeling; Microstegium vimineum; niche ID MICROSTEGIUM-VIMINEUM POACEAE; TRIN. A.-CAMUS; REGIONAL ENVIRONMENTAL GRADIENTS; CANOPY DECIDUOUS FORESTS; EXOTIC PLANT INVASIONS; WHITE-TAILED DEER; HABITAT-SUITABILITY; UNITED-STATES; SPECIES DISTRIBUTIONS; HARDWOOD FOREST AB A critical aspect of early-stage invasive species management is determining the niche and assessing the impact of a new species. A multi-scale strategy to predict potential habitat and impacts at the ecosystem, community and species level presents a robust, efficient, and cost effective tool for invasive species management. Regional scale maximum entropy modeling and local scale field studies were used to characterize species-environment and species-species interactions of Oplismenus undulatifolius, a recent invader in Mid-Atlantic forest understories. Oplismenus undulatifolius was first discovered in the U. S. near Baltimore, Maryland in 1996 and is currently found in 13 counties in Maryland and Virginia. At the landscape scale the USDA estimates that 30 percent of the U. S. is suitable for the establishment of O. undulatifolius. Regional scale modeling indicated that 22% of the area modeled was suitable for O. undulatifolius, with 1% highly suitable. Local scale field studies indicated that O. undulatifolius thrives at low light levels (2-11 mols m(-2) day(-1)) across a wide range of litter depths (0-6 cm) and that light and litter depth are involved in dominance of O. undulatifolius over Microstegium vimineum. Interactions with Fagus grandifolia result in decreased O. undulatifolius cover and dominance, and areas of high O. undulatifolius cover typically have low species richness. Oplismenus undulatifolius has the ability to invade a far greater portion of the forest than M. vimineum, and more research on the community and ecosystem-level effects of this new invasive forest understory species is needed. C1 [Beauchamp, Vanessa B.; Koontz, Stephanie M.] Towson Univ, Dept Biol Sci, Towson, MD 21252 USA. [Suss, Christine; Hawkins, Chad] NASA, Goddard Space Flight Ctr, DEVELOP Internship Program, Greenbelt, MD 20771 USA. [Kyde, Kerrie L.] Wildlife & Heritage Serv, Maryland Dept Nat Resources, Gaithersburg, MD 20878 USA. [Schnase, John L.] NASA, Goddard Space Flight Ctr, Off Computat & Informat Sci & Technol, Greenbelt, MD 20771 USA. RP Beauchamp, VB (reprint author), Towson Univ, Dept Biol Sci, Towson, MD 21252 USA. EM vbeauchamp@towson.edu FU NASA's DEVELOP Internship Program; NASA's High-End Computing Program; Middle Patuxent Environmental Foundation; NSF Research Experience for Teachers (RET) program; Baltimore Excellence in STEM Teaching (BEST) Project at Towson University; Fisher College of Science and Mathematics; National Fish and Wildlife Foundation's Pulling Together Initiative FX Funding for this project was provided by NASA's DEVELOP Internship Program and NASA's High-End Computing Program, the Middle Patuxent Environmental Foundation, the NSF Research Experience for Teachers (RET) program, the Baltimore Excellence in STEM Teaching (BEST) Project at Towson University, the Fisher College of Science and Mathematics and the National Fish and Wildlife Foundation's Pulling Together Initiative. NR 129 TC 1 Z9 1 U1 2 U2 12 PU TORREY BOTANICAL SOC PI LAWRENCE PA 810 E 10TH ST, LAWRENCE, KS 66044 USA SN 1095-5674 EI 1940-0616 J9 J TORREY BOT SOC JI J. Torrey Bot. Soc. PD OCT PY 2013 VL 140 IS 4 BP 391 EP 413 DI 10.3159/TORREY-D-13-00033.1 PG 23 WC Plant Sciences SC Plant Sciences GA AM2CK UT WOS:000339656000002 ER PT J AU Blue, RS Hudson, JC Rieders, MF James, JT Stepaniak, PC AF Blue, Rebecca S. Hudson, Joseph C. Rieders, Michael F. James, John T. Stepaniak, Philip C. TI Medical Management of a Potentially Toxic Accidental Trialkylamine Ingestion During Spaceflight SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE iodine; water filtration; toxicity; spaceflight ID RAT AB Introduction: To reduce excessive iodine consumption by astronauts, the National Aeronautics and Space Administration (NASA) has developed various methods of removing residual iodine after iodine-based water purification aboard spacecraft. The Low Iodine Residual System (LIRS) was developed as an iodine removal system for use aboard the space shuttle. This is a case report of an accidental, potentially toxic ingestion by astronauts aboard a space shuttle mission following exposure to contaminated water from LIRS filtration and the medical response operations that followed. Case Report: Astronauts ingested significant levels of trialkylamines from water that had passed through gamma-irradiated, de-iodination resin in the LIRS hardware. Medical response operations included crew evaluations, consultations with toxicologists and systems experts, hardware testing, contaminant evaluation, and close crewmember follow-up. Discussion: Despite the significant ingestion there were no adverse clinical symptoms in any of the exposed astronauts; however, the case highlights a simple pitfall in the classification of hardware that ultimately lead to a potentially harmful toxic ingestion among the crewmembers, and the real-time response of medical personnel to ensure crew safety. C1 [Blue, Rebecca S.] Univ Texas Med Branch, Galveston, TX 77555 USA. [Hudson, Joseph C.] Lakenheath Royal AFB, Med Grp 48, Lakenheath, Suffolk, England. [Rieders, Michael F.] Natl Med Serv Inc, Willow Grove, PA USA. [James, John T.] NASA, Lyndon B Johnson Space Ctr, Biomed Res & Environm Sci Div, Houston, TX 77058 USA. [Stepaniak, Philip C.] NASA, Lyndon B Johnson Space Ctr, Med Operat Branch, Houston, TX 77058 USA. RP Blue, RS (reprint author), Univ Texas Med Branch, Dept Prevent Med, 301 Univ Blvd, Galveston, TX 77555 USA. EM rblue.md@gmail.com NR 11 TC 0 Z9 0 U1 0 U2 2 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 EI 1943-4448 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD OCT PY 2013 VL 84 IS 10 BP 1100 EP 1104 DI 10.3357/ASEM.3711.2013 PG 5 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA AD1LW UT WOS:000332996500015 PM 24261066 ER PT J AU Inman, JA Bathel, BF Johansen, CT Danehy, PM Jones, SB Gragg, JG Splinter, SC AF Inman, Jennifer A. Bathel, Brett F. Johansen, Craig T. Danehy, Paul M. Jones, Stephen B. Gragg, Jeffrey G. Splinter, Scott C. TI Nitric-Oxide Planar Laser-Induced Fluorescence Measurements in the Hypersonic Materials Environmental Test System SO AIAA JOURNAL LA English DT Article ID GAS-FLOWS; VELOCITY AB Planar laser-induced fluorescence of naturally occurring nitric oxide has been used to provide insight into baseline flow conditions of the Hypersonic Materials Environmental Test System 400 kW arc-heated wind tunnel at NASA Langley Research Center via radial and axial velocity measurements and instantaneous flow-visualization images. This represents both the first flow-tagging velocity measurements and the first application of nitric-oxide planar laser-induced fluorescence flow visualization in an arcjet facility. Results are presented at selected facility run conditions, including some in a simulated Earth atmosphere (75% nitrogen, 20% oxygen, 5% argon) and others in a simulated Martian atmosphere (71% carbon dioxide, 24% nitrogen, 5% argon) for specific bulk enthalpies ranging from 6.5 to 18.4 MJ/kg. Flow-visualization images reveal the presence of large-scale unsteady flow structures and indicate nitric-oxide fluorescence signal over more than 70% of the core flow for specific bulk enthalpies below about 11 MJ/kg but over less than 10% of the core flow for specific bulk enthalpies above about 16 MJ/kg. Axial velocimetry was performed using molecular tagging velocimetry. Axial velocities of about 3 km/s were measured along the centerline. Radial velocimetry was performed by scanning the wavelength of the narrowband laser and analyzing the resulting Doppler shift. Radial velocities of +/- 0.5 km/s were measured. C1 [Inman, Jennifer A.; Danehy, Paul M.; Jones, Stephen B.] NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23681 USA. [Bathel, Brett F.] Univ Virginia, Charlottesville, VA 22903 USA. [Bathel, Brett F.] NASA Grad Co Op, Hampton, VA USA. [Johansen, Craig T.] Natl Inst Aerosp, Dept Mech & Mfg Engn, Hampton, VA 23666 USA. [Gragg, Jeffrey G.] NASA, Langley Res Ctr, Structures Expt Branch, Hampton, VA 23681 USA. [Splinter, Scott C.] NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA. RP Inman, JA (reprint author), NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, MS 493, Hampton, VA 23681 USA. FU NASA's Fundamental Aeronautics Program, Hypersonics Project, Experimental Capabilities Discipline FX The authors wish to thank Amy Brewer for her help in running the arcjet facility as well as summer students Jeff Wheeler and Ethan Brewer for their contributions in acquiring the data presented in this paper. This work was funded in part by NASA's Fundamental Aeronautics Program, Hypersonics Project, Experimental Capabilities Discipline. NR 22 TC 2 Z9 2 U1 0 U2 4 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD OCT PY 2013 VL 51 IS 10 BP 2365 EP 2379 DI 10.2514/1.J052246 PG 15 WC Engineering, Aerospace SC Engineering GA AA8WK UT WOS:000331375500005 ER PT J AU Gray, J Moore, KT Hearn, TA Naylor, BA AF Gray, Justin Moore, Kenneth T. Hearn, Tristan A. Naylor, Bret A. TI Standard Platform for Benchmarking Multidisciplinary Design Analysis and Optimization Architectures SO AIAA JOURNAL LA English DT Article ID FRAMEWORK AB The multidisciplinary design analysis and optimization community has developed a multitude of algorithms and techniques, called architectures, for performing optimizations on complex engineering systems that involve coupling between multiple discipline analyses. These architectures seek to efficiently handle optimizations with computationally expensive analyses including multiple disciplines. A new testing procedure is proposed that can provide a quantitative and qualitative means of comparison among architectures. The proposed test procedure is implemented within the open-source framework, OpenMDAO, and comparative results are presented for five well-known architectures: multiple design feasible, individual design feasible, collaborative optimization, bilevel integrated systems synthesis, and bilevel integrated systems synthesis 2000. How using open-source software development methods can allow the multidisciplinary design analysis and optimization community to submit new problems and architectures to keep the test suite relevant is also demonstrated. C1 [Gray, Justin; Moore, Kenneth T.; Hearn, Tristan A.; Naylor, Bret A.] NASA, John H Glenn Res Ctr, Lewis Field, MDAO Branch, Cleveland, OH 44135 USA. RP Gray, J (reprint author), NASA, John H Glenn Res Ctr, Lewis Field, MDAO Branch, Mail Stop 5-11, Cleveland, OH 44135 USA. NR 45 TC 7 Z9 8 U1 0 U2 7 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 OCT PY 2013 VL 51 IS 10 BP 2380 EP 2394 DI 10.2514/1.J052160 PG 15 WC Engineering, Aerospace SC Engineering GA AA8WK UT WOS:000331375500006 ER PT J AU Wilson, J Schatzman, D Arad, E Seifert, A Shtendel, T AF Wilson, Jacob Schatzman, David Arad, Eran Seifert, Avraham Shtendel, Tom TI Suction and Pulsed-Blowing Flow Control Applied to an Axisymmetric Body SO AIAA JOURNAL LA English DT Article ID SIMULATION AB A flow-control study using steady suction and pulsed blowing in close proximity was conducted on an axisymmetric bluff body at length-based Reynolds numbers between 1.0 and 4.0 x 10(6). The study included a coupled incremental computational-fluid-dynamics and experimental approach. It began with computations of various model setup designs. Subsequently, flow-control experiments and computations were used to optimize steady suction alone. Finally, flow control was provided by a synchronized array of 28 suction and oscillatory blowing actuators, positioned slightly upstream of the baseline separation. Results show suction alone has a limited ability to delay separation and reduce drag on this geometry. Suction located far from the baseline separation is shown to actually increase drag. Addition of pulsed blowing enables separation delay to the trailing edge and drag to be nullified. Increased overall system efficiency, including estimated total actuator power invested, was found at low momentum input for optimally located steady suction and pulsed blowing. This was partially attributed to the particular geometry used because the active flow-control system shows a robust ability to delay separation. Not all measured trends were predicted by computation due to the complex nature of this configuration and the active flow-control system characteristics. C1 [Wilson, Jacob] NASA, Ames Res Ctr,Dev & Engn Command, US Army Aviat Dev Directorate AFDD Aviat & Missil, Dev & Engn Ctr Res,Aeroflightdynam Directorate, Moffett Field, CA 94035 USA. [Schatzman, David] Sci & Technol Corp, US Army Aviat Dev Directorate AFDD Aviat & Missil, Dev & Engn Command, Aeroflightdynam Directorate,Dev & Engn Ctr Res, Moffett Field, CA 94035 USA. [Arad, Eran] Rafael Ltd, Computat Fluid Dynam, Aeronaut Syst, IL-31021 Haifa, Israel. [Seifert, Avraham; Shtendel, Tom] Tel Aviv Univ, Sch Mech Engn, IL-69978 Tel Aviv, Israel. RP Wilson, J (reprint author), NASA, Ames Res Ctr,Dev & Engn Command, US Army Aviat Dev Directorate AFDD Aviat & Missil, Dev & Engn Ctr Res,Aeroflightdynam Directorate, Mail Stop 215-1, Moffett Field, CA 94035 USA. NR 31 TC 8 Z9 8 U1 0 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 OCT PY 2013 VL 51 IS 10 BP 2432 EP 2446 DI 10.2514/1.J052333 PG 15 WC Engineering, Aerospace SC Engineering GA AA8WK UT WOS:000331375500010 ER PT J AU Matthews, B Das, S Bhaduri, K Das, K Martin, R Oza, N AF Matthews, Bryan Das, Santanu Bhaduri, Kanishka Das, Kamalika Martin, Rodney Oza, Nikunj TI Discovering Anomalous Aviation Safety Events Using Scalable Data Mining Algorithms SO JOURNAL OF AEROSPACE INFORMATION SYSTEMS LA English DT Article ID OUTLIER DETECTION; DATA SETS; SUPPORT AB The worldwide civilian aviation system is one of the most complex dynamical systems created. Most modern commercial aircraft have onboard flight data recorders that record several hundred discrete and continuous parameters at approximately 1 Hz for the entire duration of the flight. These data contain information about the flight control systems, actuators, engines, landing gear, avionics, and pilot commands. In this paper, recent advances in the development of a novel knowledge discovery process consisting of a suite of data mining techniques for identifying precursors to aviation safety incidents are discussed. The data mining techniques include scalable multiple-kernel learning for large-scale distributed anomaly detection. A novel multivariate time-series search algorithm is used to search for signatures of discovered anomalies on massive datasets. The process can identify operationally significant events due to environmental, mechanical, and human factors issues in the high-dimensional flight operations quality assurance data. All discovered anomalies are validated by a team of independent domain experts. This novel automated knowledge discovery process is aimed at complementing the state-of-the-art human-generated exceedance-based analysis that fails to discover previously unknown aviation safety incidents. In this paper, the discovery pipeline, the methods used, and some of the significant anomalies detected on real-world commercial aviation data are discussed. C1 [Matthews, Bryan; Das, Santanu; Bhaduri, Kanishka; Das, Kamalika; Martin, Rodney; Oza, Nikunj] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Matthews, B (reprint author), Stinger Ghaffarian Technol Inc, Greenbelt, MD 20770 USA. FU NASA Aviation Safety Program's System-Wide Safety and Assurance Technologies Project FX This research is supported by the NASA Aviation Safety Program's System-Wide Safety and Assurance Technologies Project. We would like to thank Ashok Srivastava and John Stutz for their contributions and feedback. We would also like to thank Irv Statler, Bob Lawrence, Mike Feary, Immanuel Barshi, and the partner air carrier for providing data and expertise. NR 23 TC 6 Z9 8 U1 2 U2 20 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 1940-3151 EI 2327-3097 J9 J AEROSP INFORM SYST JI J. Aerosp. Inf. Syst. PD OCT PY 2013 VL 10 IS 10 BP 467 EP 475 DI 10.2514/1.I010080 PG 9 WC Engineering, Aerospace SC Engineering GA AB2GN UT WOS:000331611300003 ER PT J AU Jung, SN You, YH Lau, BH Johnson, W Lim, JW AF Jung, Sung N. You, Young H. Lau, Benton H. Johnson, Wayne Lim, Joon W. TI Evaluation of Rotor Structural and Aerodynamic Loads Using Measured Blade Properties SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY LA English DT Article ID VORTEX INTERACTION AIRLOADS; COMPREHENSIVE ANALYSIS; PREDICTION; CODE AB The structural properties of Higher Harmonic Aeroacoustic Rotor Test (HART I) blades have been measured using the original set of blades tested in the wind tunnel in 1994. A comprehensive rotor dynamics analysis is performed to address the effect of the measured blade properties on airloads, blade motions, and structural loads of the rotor. The measurements include bending and torsion stiffness, geometric offsets, and mass and inertia properties of the blade. The measured properties are correlated against the estimated values obtained by the manufacturer of the blades. The previously estimated blade properties showed consistently higher stiffnesses, up to 30% for the flap bending in the blade inboard root section. The measured offset between the center of gravity and the elastic axis is larger by about 5% chord length, as compared with the estimated value. A comprehensive rotor dynamics analysis is carried out using the measured blade property set for HART I rotor. A significant improvement in blade motions and structural loads is obtained with the measured blade properties. The location of the center of gravity and the elastic axis and their offset are shown to be the most influential factors for the improved correlation. C1 [Jung, Sung N.; You, Young H.] Konkuk Univ, Seoul, South Korea. [Lau, Benton H.; Johnson, Wayne] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Lim, Joon W.] NASA, Ames Res Ctr, Aeroflightdynam Directorate AMRDEC, Moffett Field, CA 94035 USA. RP Jung, SN (reprint author), Konkuk Univ, Seoul, South Korea. EM snjung@konkuk.ac.kr FU National Research Foundation of Korea; Korean government [NRF-2011-013-D00024]; Leading Foreign Research Institute Recruitment Program through the National Research Foundation of Korea; Ministry of Education, Science and technology [K2060100001]; HART I team; DLR; DNW; NASA; ONERA; AFDD FX This work was supported by the National Research Foundation of Korea grant funded by the Korean government (NRF-2011-013-D00024). This research was supported by Leading Foreign Research Institute Recruitment Program through the National Research Foundation of Korea funded by the Ministry of Education, Science and technology (K2060100001). The authors appreciate Berend van der Wall of DLR (German Aerospace Center) for providing HART I blades, and William Warmbrodt of NASA Ames and Thomas Maier of the U.S. Army Aeroflightdynamics Directorate (AFDD) for valuable comments on this work. The authors would like to acknowledge the support of the HART I team, including DLR, DNW, NASA, ONERA, and AFDD. The authors acknowledge Benton Lau, who began the blade property measurement but passed away before the completion of the task. NR 24 TC 1 Z9 1 U1 0 U2 0 PU AMER HELICOPTER SOC INC PI ALEXANDRIA PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA SN 0002-8711 EI 2161-6027 J9 J AM HELICOPTER SOC JI J. Am. Helicopter Soc. PD OCT PY 2013 VL 58 IS 4 AR 042004 DI 10.4050/JAHS.58.042004 PG 12 WC Engineering, Aerospace SC Engineering GA AB5MY UT WOS:000331834000004 ER PT J AU Theodore, CR Tischler, MB AF Theodore, Colin R. Tischler, Mark B. TI Development and Operation of an Automatic Rotor Trim Control System for the UH-60 Individual Blade Control Wind Tunnel Test SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY LA English DT Article ID HELICOPTER AB An automatic rotor trim control system was developed and used successfully during a wind tunnel test of a full-scale UH-60 rotor system with individual blade control (IBC) actuators. The trim control system allowed rotor trim to be set more quickly, precisely, and repeatably than in previous wind tunnel tests. This control system also allowed the rotor trim state to be maintained during transients and drift in wind tunnel flow and through changes in IBC actuation. The ability to maintain a consistent rotor trim state was key to quickly and accurately evaluating the effect of IBC on rotor performance, vibration, noise, and loads. This paper presents details of the design and implementation of the trim control system including the rotor system hardware, trim control requirements, and trim control hardware and software implementation. Results are presented showing the effect of IBC on rotor trim and dynamic response, a validation of the rotor dynamic simulation used to calculate the initial control gains and tuning of the control system, and the overall performance of the trim control system during the wind tunnel test. C1 [Theodore, Colin R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Tischler, Mark B.] US Army RDECOM, Aeroflightdynam Directorate AMRDEC, Moffett Field, CA USA. RP Theodore, CR (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM ctheodore@mail.arc.nasa.gov NR 11 TC 0 Z9 0 U1 2 U2 7 PU AMER HELICOPTER SOC INC PI ALEXANDRIA PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA SN 0002-8711 EI 2161-6027 J9 J AM HELICOPTER SOC JI J. Am. Helicopter Soc. PD OCT PY 2013 VL 58 IS 4 AR 042007 DI 10.4050/JAHS.58.042007 PG 13 WC Engineering, Aerospace SC Engineering GA AB5MY UT WOS:000331834000007 ER PT J AU Suess, M Greenhall, CA AF Suess, Matthias Greenhall, Charles A. TI Congruence of two Kalman filter composite clocks SO METROLOGIA LA English DT Article ID ADMITS MEASUREMENT NOISE; ENSEMBLE ALGORITHM; TIMESCALES AB This paper compares the estimation results of two composite clock algorithms based on Kalman filtering of measured clock differences: the original Jones-Tryon algorithm and Greenhall's covariance-reduction modification. The theory is carried out for a general clock model that includes the model introduced by Davis et al: the sum of the three-state linear model and a set of Markov processes used to approximate flicker-frequency noise. Since measurement noise is allowed, at each measurement time the corrected clock offsets (the difference between the clock offsets and their estimates) do not coincide but form a set of values, different for the two algorithms. The core result is that these two sets are congruent, that is, they differ by a common scalar shift. As a function of time the value of the shift behaves as a random walk. Moreover, the two Kalman filters have the same measurement residuals. Therefore, any detector algorithm that uses the measurement residuals is not impacted by the covariance reduction. The congruency holds for time-varying measurement matrices. Therefore, the result is applicable to the measurement setup of laboratories as well as that of a Global Navigation Satellite System with varying visibilities of satellite clocks at ground stations. These results are illustrated by a simulated ensemble of three caesium clocks and two active hydrogen masers, measured against one of the masers. C1 [Suess, Matthias] German Aerosp Ctr, Oberpfaffenhoffen, Germany. [Greenhall, Charles A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Suess, M (reprint author), German Aerosp Ctr, Muenchener Str 20, Oberpfaffenhoffen, Germany. EM Matthias.Suess@dlr.de; cgreenhall@onemain.com NR 17 TC 2 Z9 3 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0026-1394 EI 1681-7575 J9 METROLOGIA JI Metrologia PD OCT PY 2013 VL 50 IS 5 BP 499 EP 508 DI 10.1088/0026-1394/50/5/499 PG 10 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA AA1BN UT WOS:000330831400009 ER PT J AU Autsavapromporn, N Suzuki, M Funayama, T Usami, N Plante, I Yokota, Y Mutou, Y Ikeda, H Kobayashi, K Kobayashi, Y Uchihori, Y Hei, TK Azzam, EI Murakami, T AF Autsavapromporn, Narongchai Suzuki, Masao Funayama, Tomoo Usami, Noriko Plante, Ianik Yokota, Yuichiro Mutou, Yasuko Ikeda, Hiroko Kobayashi, Katsumi Kobayashi, Yasuhiko Uchihori, Yukio Hei, Tom K. Azzam, Edouard I. Murakami, Takeshi TI Gap Junction Communication and the Propagation of Bystander Effects Induced by Microbeam Irradiation in Human Fibroblast Cultures: The Impact of Radiation Quality SO RADIATION RESEARCH LA English DT Article ID MEDIATED INTERCELLULAR COMMUNICATION; MONTE-CARLO-SIMULATION; ION TRACK STRUCTURE; X-RAY MICROBEAM; GENOMIC INSTABILITY; IONIZING-RADIATION; MAMMALIAN-CELLS; ALPHA-PARTICLES; NONUNIFORM DISTRIBUTIONS; CARCINOMA-CELLS AB Understanding the mechanisms underlying the bystander effects of low doses/low fluences of low-or high-linear energy transfer (LET) radiation is relevant to radiotherapy and radiation protection. Here, we investigated the role of gap-junction intercellular communication (GJIC) in the propagation of stressful effects in confluent normal human fibroblast cultures wherein only 0.036-0.144% of cells in the population were traversed by primary radiation tracks. Confluent cells were exposed to graded doses from monochromatic 5.35 keV X ray (LET; 6 keV/mu m), 18.3 MeV/u carbon ion (LET similar to 103 keV/mu m), 13 MeV/u neon ion (LET; 380 keV/mu m) or 11.5 MeV/u argon ion (LET; 1,260 keV/lm) microbeams in the presence or absence of 18-alpha-glycyrrhetinic acid (AGA), an inhibitor of GJIC. After 4 h incubation at 37 degrees C, the cells were subcultured and assayed for micronucleus (MN) formation. Micronuclei were induced in a greater fraction of cells than expected based on the fraction of cells targeted by primary radiation, and the effect occurred in a dose-dependent manner with any of the radiation sources. Interestingly, MN formation for the heavy-ion microbeam irradiation in the absence of AGA was higher than in its presence at high mean absorbed doses. In contrast, there were no significant differences in cell cultures exposed to X-ray microbeam irradiation in presence or absence of AGA. This showed that the inhibition of GJIC depressed the enhancement of MN formation in bystander cells from cultures exposed to high-LET radiation but not low-LET radiation. Bystander cells recipient of growth medium harvested from 5.35 keV X-irradiated cultures experienced stress manifested in the form of excess micronucleus formation. Together, the results support the involvement of both junctional communication and secreted factor(s) in the propagation of radiation-induced stress to bystander cells. They highlight the important role of radiation quality and dose in the observed effects. (C) 2013 by Radiation Research Society C1 [Autsavapromporn, Narongchai; Suzuki, Masao; Murakami, Takeshi] Natl Inst Radiol Sci, Res Ctr Charged Particle Therapy, Chiba 2638555, Japan. [Funayama, Tomoo; Yokota, Yuichiro; Mutou, Yasuko; Ikeda, Hiroko; Kobayashi, Yasuhiko] Japan Atom Energy Agcy, Quantum Beam Sci Directorate, Med & Biotechnol Applicat Div, Microbeam Radiat Biol Grp, Takasaki, Gumma 3701292, Japan. [Usami, Noriko; Kobayashi, Katsumi] High Energy Accelerator Res Org, Photon Factory, Tsukuba, Ibaraki 3050801, Japan. [Plante, Ianik] Univ Space Res Assoc, NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Uchihori, Yukio] Natl Inst Radiol Sci, Res Dev & Support Ctr, Chiba 2638555, Japan. [Hei, Tom K.] Columbia Univ, Med Ctr, Ctr Radiol Res, New York, NY 10032 USA. [Azzam, Edouard I.] Rutgers State Univ, Dept Radiol, New Jersey Med Sch, Ctr Canc, Newark, NJ 07103 USA. RP Suzuki, M (reprint author), Natl Inst Radiol Sci, Res Ctr Charged Particle Therapy, Chiba 2638555, Japan. EM m_suzuki@nirs.go.jp FU JSPS KAKENHI [23-01513, 18310042, 24620014]; Japan Science and Technology Agency FX The authors acknowledge the excellent help from all the support personnel at TIARA, KEK and NIRS, especially Dr. Cuihua Liu, Ms. Yumiko Kaneko and Ms. Toshie Iizuka. This study was supported in part by JSPS KAKENHI Grant Number 23-01513, 18310042, 24620014 and the Quantum Beam Technology Program from the Japan Science and Technology Agency. NR 52 TC 14 Z9 16 U1 0 U2 15 PU RADIATION RESEARCH SOC PI LAWRENCE PA 810 E TENTH STREET, LAWRENCE, KS 66044 USA SN 0033-7587 EI 1938-5404 J9 RADIAT RES JI Radiat. Res. PD OCT PY 2013 VL 180 IS 4 BP 367 EP 375 DI 10.1667/RR3111.1 PG 9 WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology, Nuclear Medicine & Medical Imaging GA AA3KS UT WOS:000330991900005 PM 23987132 ER PT J AU Santanello, JA Kumar, SV Peters-Lidard, CD Harrison, K Zhou, SJ AF Santanello, Joseph A., Jr. Kumar, Sujay V. Peters-Lidard, Christa D. Harrison, Ken Zhou, Shujia TI Impact of Land Model Calibration on Coupled Land-Atmosphere Prediction SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID DATA ASSIMILATION SYSTEM; SOUTHERN GREAT-PLAINS; SURFACE MODEL; SOIL-MOISTURE; WARM-SEASON; HYDRAULIC-PROPERTIES; UNITED-STATES; WRF; PRECIPITATION; SIMULATIONS AB Land-atmosphere (LA) interactions play a critical role in determining the diurnal evolution of both planetary boundary layer (PBL) and land surface heat and moisture budgets, as well as controlling feedbacks with clouds and precipitation that lead to the persistence of dry and wet regimes. In this study, the authors examine the impact of improved specification of land surface states, anomalies, and fluxes on coupled Weather Research and Forecasting Model (WRF) forecasts during the summers of extreme dry (2006) and wet (2007) land surface conditions in the U.S. southern Great Plains. The improved land initialization and surface flux parameterizations are obtained through calibration of the Noah land surface model using the new optimization and uncertainty estimation subsystems in NASA's Land Information System (LIS-OPT/LIS-UE). The impact of the calibration on the 1) spinup of the land surface used as initial conditions and 2) the simulated heat and moisture states and fluxes of the coupled WRF simulations is then assessed. In addition, the sensitivity of this approach to the period of calibration (dry, wet, or average) is investigated. Results show that the offline calibration is successful in providing improved initial conditions and land surface physics for the coupled simulations and in turn leads to systematic improvements in land-PBL fluxes and near-surface temperature and humidity forecasts. Impacts are larger during dry regimes, but calibration during either primarily wet or dry periods leads to improvements in coupled simulations due to the reduction in land surface model bias. Overall, these results provide guidance on the questions of what, how, and when to calibrate land surface models for coupled model prediction. C1 [Santanello, Joseph A., Jr.; Kumar, Sujay V.; Peters-Lidard, Christa D.; Harrison, Ken] NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kumar, Sujay V.] Sci Applicat Int Corp, Mclean, VA 22102 USA. [Harrison, Ken] Univ Maryland, College Pk, MD 20742 USA. [Zhou, Shujia] Northrop Grumman Informat Syst, Chantilly, VA USA. [Zhou, Shujia] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Santanello, JA (reprint author), NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Code 617 Bldg 33,Rm G220, Greenbelt, MD 20771 USA. EM joseph.a.santanello@nasa.gov RI Santanello, Joseph/D-4438-2012; Kumar, Sujay/B-8142-2015; Peters-Lidard, Christa/E-1429-2012 OI Santanello, Joseph/0000-0002-0807-6590; Peters-Lidard, Christa/0000-0003-1255-2876 FU NASA; Earth Science Technology Office (ESTO) FX This work was supported by NASA's Advanced Information System Technology program (AIST) and the Earth Science Technology Office (ESTO). The NU-WRF team was also instrumental in providing support related to LIS-WRF coupling and a stable and updated version of the coupled system. The data for the MET analysis are from the Research Data Archive (RDA), which is maintained by the Computational and Information Systems Laboratory (CISL) at the National Center for Atmospheric Research (NCAR). The original data are available in dataset number ds337.0 (http://rda.ucar.edu/datasets/ds337.0). NR 69 TC 13 Z9 13 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 OCT PY 2013 VL 14 IS 5 BP 1373 EP 1400 DI 10.1175/JHM-D-12-0127.1 PG 28 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 301KX UT WOS:000330532300001 ER PT J AU Kidd, C Dawkins, E Huffman, G AF Kidd, Chris Dawkins, Erin Huffman, George TI Comparison of Precipitation Derived from the ECMWF Operational Forecast Model and Satellite Precipitation Datasets SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID DIURNAL CYCLE; TROPICAL RAINFALL; PASSIVE MICROWAVE; SEA-BREEZE; RADAR DATA; CONVECTION; TRMM; LAND; CLIMATOLOGY; RESOLUTION AB Precipitation is an important component of the climate system, and the accurate representation of the diurnal rainfall cycle is a key test of model performance. Although the modeling of precipitation in the cooler midlatitudes has improved, in the tropics substantial errors still occur. Precipitation from the operational ECMWF forecast model is compared with satellite-derived products from the Tropical Rainfall Measuring Mission (TRMM) Multisatellite Precipitation Analysis (TMPA) and TRMM Precipitation Radar (PR) to assess the mean annual and seasonal diurnal rainfall cycles. The analysis encompasses the global tropics and subtropics (40 degrees N-40 degrees S) over a 7-yr period from 2004 to 2011. The primary aim of the paper is to evaluate the ability of an operational numerical model and satellite products to retrieve subdaily rainfall. It was found that during the first half of the analysis period the ECMWF model overestimated precipitation by up to 15% in the tropics, although after the implementation of a new convective parameterization in November 2007 this bias fell to about 4%. The ECMWF model poorly represented the diurnal cycle, simulating rainfall too early compared to the TMPA and TRMM PR products; the model simulation of precipitation was particularly poor over Indonesia. In addition, the model did not appear to simulate mountain-slope breezes well or adequately capture many of the characteristics of mesoscale convective systems. The work highlights areas for further study to improve the representation of subgrid-scale processes in parameterization schemes and improvements in model resolution. In particular, the proper representation of subdaily precipitation in models is critical for hydrological modeling and flow forecasting. C1 [Kidd, Chris] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Kidd, Chris; Huffman, George] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dawkins, Erin] Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England. RP Kidd, C (reprint author), NASA Goddard Space Flight, Mail Code 612, Greenbelt, MD 20771 USA. EM chris.kidd@nasa.gov RI Huffman, George/F-4494-2014; Kidd, Christopher/H-9910-2014 OI Huffman, George/0000-0003-3858-8308; FU U.K. Natural Environment Research Council [NE/H525454/1] FX The authors acknowledge the support of the U.K. Natural Environment Research Council through their Master Training Grant (NE/H525454/1), which supported the second author. Thanks also go to the European Centre for Medium-Range Weather Forecasts for provision of their operational forecast precipitation product and to NASA's Precipitation Processing System for the TMPA and PR datasets. We would also like to thank the anonymous reviewers for their diligence in reviewing the manuscript. NR 57 TC 12 Z9 12 U1 0 U2 12 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD OCT PY 2013 VL 14 IS 5 BP 1463 EP 1482 DI 10.1175/JHM-D-12-0182.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 301KX UT WOS:000330532300005 ER PT J AU Cohen, HS Mulavara, AP Peters, BT Sangi-Haghpeykar, H Kung, DH Mosier, DR Bloomberg, JJ AF Cohen, Helen S. Mulavara, Ajitkumar P. Peters, Brian T. Sangi-Haghpeykar, Haleh Kung, Doris H. Mosier, Dennis R. Bloomberg, Jacob J. TI Sharpening the Tandem Walking Test for Screening Peripheral Neuropathy SO SOUTHERN MEDICAL JOURNAL LA English DT Article DE balance testing; clinical examination; neurology testing; sensitivity and specificity; tandem gait ID CLINICAL BALANCE TESTS; TRUNK SWAY MEASURES; DYNAMIC POSTUROGRAPHY; PHYSICAL CAPABILITY; POSTURAL STABILITY; AGE AB Objective: Few tests of functional motor behavior are useful for rapidly screening people for lower extremity peripheral neuropathy. The goal of this study was to improve the widely used tandem walking (TW) test. Methods: We tested "normal'' (control) adult and ambulatory patients with peripheral neuropathy (PN) with their eyes open and eyes closed while they performed TW on industrial carpeting in sock-covered feet. Each subject wore a torso-mounted inertial motion unit to measure kinematic data. The data of subjects with PN also were compared with historical data on patients with vestibular impairments. Results: The normal and PN groups differed significantly on TW and on the number of steps completed. PN and vestibular impairments data also differed significantly on both visual conditions. Kinematic data showed that patients with PN were more unstable than normal patients in the group. For the number of steps taken during the eyes open condition, receiver operating characteristic (ROC) values were only 0.81 and for the number of steps taken during the eyes closed condition, ROC values were 0.88. Although not optimal, this ROC value is better. Sensitivity and specificity at a cutoff of two steps were 0.81 and 0.92, respectively, and at a cutoff of three steps were 0.86 and 0.75, respectively. ROC values for kinematic data were <0.8, and when combined with the ROC value for the number of steps, the total ROC value did not improve appreciably. Conclusions: Although not ideal for screening patients who may have PN, counting the number of steps during TW is a quick and useful clinical test. TW is most sensitive to patients with PN when they are tested with eyes closed. C1 Baylor Coll Med, Bobby R Alford Dept Otolaryngol Head & Neck Surg, Dept Obstet & Gynecol, Houston, TX 77030 USA. Baylor Coll Med, Dept Neurol, Houston, TX 77030 USA. Univ Space Res Assoc, Wyle Sci Technol & Engn Grp, Houston, TX USA. NASA, Lyndon B Johnson Space Ctr, Neurosci Res Labs, Houston, TX 77058 USA. RP Cohen, HS (reprint author), Baylor Coll Med, Bobby R Alford Dept Otolaryngol Head & Neck Surg, One Baylor Plaza, Houston, TX 77030 USA. EM hcohen@bcm.edu FU National Institutes of Health [R01DC009031]; National Space Biomedical Research Institute through NASA [NCC 9-58] FX This study was supported by National Institutes of Health grant R01DC009031 (HSC) and grants from the National Space Biomedical Research Institute through NASA NCC 9-58. NR 22 TC 3 Z9 3 U1 1 U2 3 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA SN 0038-4348 EI 1541-8243 J9 SOUTH MED J JI South.Med.J. PD OCT PY 2013 VL 106 IS 10 BP 565 EP 569 DI 10.1097/SMJ.0000000000000009 PG 5 WC Medicine, General & Internal SC General & Internal Medicine GA 298UK UT WOS:000330349800005 PM 24096950 ER PT J AU Kozyra, JU Manchester, WB Escoubet, CP Lepri, ST Liemohn, MW Gonzalez, WD Thomsen, MW Tsurutani, BT AF Kozyra, J. U. Manchester, W. B. Escoubet, C. P. Lepri, S. T. Liemohn, M. W. Gonzalez, W. D. Thomsen, M. W. Tsurutani, B. T. TI Earth's collision with a solar filament on 21 January 2005: Overview SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE magnetic reconnection; magnetotail; plasma sheet; solar filament; coronal mass ejection ID CORONAL MASS EJECTION; 1-2 SEPTEMBER 1859; MAGNETIC CLOUDS; GEOSYNCHRONOUS ORBIT; GEOMAGNETIC STORMS; INTERPLANETARY CONDITIONS; AUGUST 4; WIND; ENERGY; PLASMA AB On 21 January 2005, one of the fastest interplanetary coronal mass ejections (ICME) of solar cycle 23, containing exceptionally dense plasma directly behind the sheath, hit the magnetosphere. We show from charge-state analysis that this material was a piece of the erupting solar filament and further, based on comparisons to the simulation of a fast CME, that the unusual location of the filament material was a consequence of three processes. As the ICME decelerated, the momentum of the dense filament material caused it to push through the flux rope toward the nose. Diverging nonradial flows in front of the filament moved magnetic flux to the sides of the ICME. At the same time, reconnection between the leading edge of the ICME and the sheath magnetic fields worked to peel away the outer layers of the flux rope creating a remnant flux rope and a trailing region of newly opened magnetic field lines. These processes combined to move the filament material into direct contact with the ICME sheath region. Within 1 h after impact and under northward interplanetary magnetic field (IMF) conditions, a cold dense plasma sheet formed within the magnetosphere from the filament material. Dense plasma sheet material continued to move through the magnetosphere for more than 6 h as the filament passed by the Earth. Densities were high enough to produce strong diamagnetic stretching of the magnetotail despite the northward IMF conditions and low levels of magnetic activity. The disruptions from the filament collision are linked to an array of unusual features throughout the magnetosphere, ionosphere, and atmosphere. These results raise questions about whether rare collisions with solar filaments may, under the right conditions, be a factor in producing even more extreme events. C1 [Kozyra, J. U.; Manchester, W. B.; Lepri, S. T.; Liemohn, M. W.] Univ Michigan, AOSS Dept, Ann Arbor, MI 48109 USA. [Escoubet, C. P.] ESA ESTEC, Noordwijk, Netherlands. [Gonzalez, W. D.] Natl Inst Space Res, Sao Jose Dos Campos, Brazil. [Thomsen, M. W.] Los Alamos Natl Lab, Los Alamos, NM USA. [Tsurutani, B. T.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Kozyra, JU (reprint author), Univ Michigan, AOSS Dept, 1414-A Space Res Bldg.,2455 Hayward St, Ann Arbor, MI 48109 USA. EM jukozyra@umich.edu RI Lepri, Susan/I-8611-2012; Liemohn, Michael/H-8703-2012; Manchester, Ward/I-9422-2012 OI Liemohn, Michael/0000-0002-7039-2631; FU NASA [NNX10AQ34C, NNH09AK621, NNH11AR241, NNX07AT186]; NSF [ATM-0903596]; University of Michigan FX The authors would like to acknowledge support for the research under NASA (NNX10AQ34C, NNH09AK621, NNH11AR241, and NNX07AT186) and NSF (ATM-0903596) grants. This work was partially supported by the University of Michigan. Portions of this research were performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Thanks to Ruth Skoug and Heather Elliott for providing reprocessed ACE solar wind parameters. NR 85 TC 7 Z9 7 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 OCT PY 2013 VL 118 IS 10 BP 5967 EP 5978 DI 10.1002/jgra.50567 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 296JH UT WOS:000330180600001 ER PT J AU Ofman, L Gedalin, M AF Ofman, L. Gedalin, M. TI Rippled quasi-perpendicular collisionless shocks: Local and global normals SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Shocks; Hybrid models; collisionless plasma; Heliosphere ID BOW SHOCK; MAGNETIC-FIELD; ION DISTRIBUTIONS; CLUSTER OBSERVATIONS; SELF-REFORMATION; MACH-NUMBER; MOTION; FRONT; NONSTATIONARITY; THERMALIZATION AB Proper determination of the shock normal is necessary for reliable determination of observed heliospheric shock parameters and comparison of observations with theory. The existing methods work sufficiently well for low and moderate Mach numbers one-dimensional stationary shocks. Higher-Mach-number shocks are no longer planar at the scales of the ion convective gyroradius or smaller. In rippled shock fronts, the local shock normal may differ substantially from the global normal. The former is determined by the local direction of the fastest variation of the magnetic field, while the latter is determined by the far upstream and far downstream plasma conditions. Here we use 2-D hybrid modeling of quasi-perpendicular collisionless shocks with moderate and high Mach numbers to quantify the difference between the directions of the two normals. We find that the angle between the local normal and the global normal may be as large as 40 degrees within the front of a rippled heliospheric shock. The coplanarity method of the shock normal determination is sensitive to the choice of the region for the magnetic field averaging. We also find that the usage of the sliding averaging region in the close vicinity of the shock transition provides satisfactory estimates of the global normal. C1 [Ofman, L.] CUA, Greenbelt, MD 20771 USA. [Ofman, L.] NASA GSFC, Greenbelt, MD 20771 USA. [Gedalin, M.] Ben Gurion Univ Negev, Dept Phys, IL-84105 Beer Sheva, Israel. RP Ofman, L (reprint author), CUA, Code 671, Greenbelt, MD 20771 USA. EM Leon.Ofman@nasa.gov FU NASA [NNX10AC56G] FX L.O. would like to acknowledge discussions with A. F. Vinas, and support by NASA grant NNX10AC56G. NR 44 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 OCT PY 2013 VL 118 IS 10 BP 5999 EP 6006 DI 10.1002/2013JA018780 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 296JH UT WOS:000330180600004 ER PT J AU Tenerani, A Le Contel, O Califano, F Robert, P Fontaine, D Cornilleau-Wehrlin, N Sauvaud, J-A AF Tenerani, A. Le Contel, O. Califano, F. Robert, P. Fontaine, D. Cornilleau-Wehrlin, N. Sauvaud, J. -A. TI Cluster observations of whistler waves correlated with ion-scale magnetic structures during the 17 August 2003 substorm event SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE plasma physics; magnetosphere; plasma waves ID MAGNETOSHEATH LION ROARS; INHOMOGENEOUS-PLASMA; GEOTAIL OBSERVATIONS; ELECTRIC-FIELD; RECONNECTION; MAGNETOSPHERE; MAGNETOTAIL; EFW AB We provide evidence of the simultaneous occurrence of large-amplitude, quasi-parallel whistler mode waves and ion-scale magnetic structures, which have been observed by the Cluster spacecraft in the plasma sheet at 17 Earth radii, during a substorm event. It is shown that the magnetic structures are characterized by both a magnetic field strength minimum and a density hump and that they propagate in a direction quasi-perpendicular to the average magnetic field. The observed whistler mode waves are efficiently ducted by the inhomogeneity associated with such ion-scale magnetic structures. The large amplitude of the confined whistler waves suggests that electron precipitations could be enhanced locally via strong pitch angle scattering. Furthermore, electron distribution functions indicate that a strong parallel heating of electrons occurs within these ion-scale structures. This study provides new insights on the possible multiscale coupling of plasma dynamics during the substorm expansion, on the basis of the whistler mode wave trapping by coherent ion-scale structures. C1 [Tenerani, A.; Le Contel, O.] UPMC, Ecole Polytech, CNRS, LPP, St Maur Des Fosses, France. [Tenerani, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Califano, F.] Univ Pisa, Dept Phys, I-56100 Pisa, Italy. [Robert, P.; Fontaine, D.; Cornilleau-Wehrlin, N.] Ecole Polytech, CNRS, LPP, F-91128 Palaiseau, France. [Cornilleau-Wehrlin, N.] LESIA, Observ Paris, Meudon, France. [Sauvaud, J. -A.] IRAP UPS, Toulouse, France. RP Tenerani, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM Anna.Tenerani@jpl.nasa.gov NR 39 TC 7 Z9 7 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 OCT PY 2013 VL 118 IS 10 BP 6072 EP 6089 DI 10.1002/jgra.50562 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 296JH UT WOS:000330180600010 ER PT J AU Pulkkinen, TI Partamies, N Kissinger, J McPherron, RL Glassmeier, KH Carlson, C AF Pulkkinen, T. I. Partamies, N. Kissinger, J. McPherron, R. L. Glassmeier, K. -H. Carlson, C. TI Plasma sheet magnetic fields and flows during steady magnetospheric convection events SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE steady convection; plasma sheet; inner magnetosphere ID SOLAR-WIND; SUBSTORM; DYNAMICS AB Inner magnetosphere magnetic field and plasma flow data are examined during 228 steady magnetospheric convection events. We find that the B-Z component of the magnetic field around geostationary orbit is weaker than during average conditions and the plasma flow speeds are higher than average in the dusk sector just beyond geostationary orbit. The steady magnetospheric convection periods include more enhanced earthward and tailward flow intervals than during average conditions. The steady convection period magnetic field is not steady: The near-geostationary nightside field grows increasingly taillike throughout the steady convection period. In the midtail, earthward flows are enhanced in a wide region around the midnight sector, which leads to enhanced magnetic flux transport toward the Earth during the steady convection periods. Compared to well-known characteristics during magnetospheric substorms, the inner tail evolution resembles that during the substorm growth phase, while the midtail flow characteristics during steady convection periods are similar to those found during substorm recovery phases. C1 [Pulkkinen, T. I.] Aalto Univ, Sch Elect Engn, Helsinki, Finland. [Partamies, N.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. [Kissinger, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McPherron, R. L.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. [Glassmeier, K. -H.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany. [Carlson, C.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Pulkkinen, TI (reprint author), Aalto Univ, Sch Elect Engn, POB 11000, Aalto 00076, Finland. EM tuija.pulkkinen@aalto.fi RI Partamies, Noora/G-3408-2014; Pulkkinen, Tuija/D-8403-2012 OI Partamies, Noora/0000-0003-2536-9341; Pulkkinen, Tuija/0000-0002-6317-381X FU German Ministerium fur Wirtschaft und Technologie; Deutsches Zentrum fur Luft- und Raumfahrt [50OC1102, 50OC1001] FX We thank the THEMIS team for making the data available in a readily accessible format. We thank the NSSDC for providing the solar wind and interplanetary field measurements and their work for propagating the disturbance fronts to the Earth orbit. T.P. thanks Minna Palmroth for useful discussions. The work by K.H.G. was financially supported by the German Ministerium fur Wirtschaft und Technologie and the Deutsches Zentrum fur Luft- und Raumfahrt under grants 50OC1102 and 50OC1001. NR 31 TC 3 Z9 3 U1 0 U2 11 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 OCT PY 2013 VL 118 IS 10 BP 6136 EP 6144 DI 10.1002/jgra.50574 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 296JH UT WOS:000330180600015 ER PT J AU Ream, JB Walker, RJ Ashour-Abdalla, M El-Alaoui, M Kivelson, MG Goldstein, ML AF Ream, J. B. Walker, R. J. Ashour-Abdalla, M. El-Alaoui, M. Kivelson, M. G. Goldstein, M. L. TI Generation of Pi2 pulsations by intermittent earthward propagating dipolarization fronts: An MHD case study SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE MHD simulation; magnetotail; substorm; Pi2 ID BURSTY BULK FLOWS; PLASMA SHEET; SUBSTORM ONSET; GEOTAIL OBSERVATIONS; PI-2 PULSATIONS; FLUX TUBES; MAGNETOTAIL; TAIL; MAGNETOSPHERE; CHALLENGE AB Using a global magnetohydrodynamic (MHD) simulation of the magnetosphere during a disturbed interval on 14 September 2004, we have investigated fluctuations in plasma properties of the magnetotail in the Pi2 range and their relationship to dipolarization fronts (DFs). Results from the MHD simulation indicate that this event is a very active interval with variable convection and disorder in the tail on a range of scales as small as approximate to 1 R-E. DFs are observed in the simulation at the leading edge of fast earthward flows that originate from reconnection regions that form between approximate to-15 and -30 R-E in the tail. Pi2 period fluctuations are identified in pressure, magnetic field, and velocity components inside -13 R(E)following each burst of DFs in the midnight sector. The fluctuations observed in the pressure appear to be generated by the successive DFs as they approach the interface between stretched tail field lines and dipolar field lines. Fluctuations in the velocity may be the result of interactions between successive DFs and are amplified directly following the passage of the DFs as they propagate earthward. Although the limited azimuthal extent of the pulsations near the plasma sheet, just inside of the braking region, makes it difficult to draw a direct comparison between the ground-based measurements and the pulsations at -6 R-E, the temporal evolution of the simulated DFs and Pi2 pulsations approximately reproduces the timing of the variations observed by satellites and ground-based instruments. Therefore, we have been able to use the global simulation to track the bursty flows, dipolarization fronts, and associated Pi2 period fluctuations throughout the entire magnetosphere in order to understand the sources of the changes measured in the near-Earth region. C1 [Ream, J. B.; Ashour-Abdalla, M.; El-Alaoui, M.; Kivelson, M. G.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Ream, J. B.; Walker, R. J.; Kivelson, M. G.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [Walker, R. J.] Natl Sci Fdn, Arlington, VA 22230 USA. [Ashour-Abdalla, M.; El-Alaoui, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Goldstein, M. L.] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA. RP Ream, JB (reprint author), Univ Calif Los Angeles, Dept Earth & Space Sci, 595 Charles Young Dr East,Box 951567, Los Angeles, CA 90095 USA. EM jodiebt@ucla.edu FU NASA Graduate Student Research Program through Goddard Space Flight Center [NNX10AM08H]; UCLA; Goddard Space Flight Center by an Interdisciplinary Science grant from the Magnetospheric Multiscale project (NASA grant at UCLA) [NNX08AO48G]; NASA [NNX10AQ47G]; National Science Foundation [OCI-1053575]; Individual Research and Development at the National Science Foundation; NASA grant UCB/NASA NAS [5-02099] FX This research was support by the NASA Graduate Student Research Program through Goddard Space Flight Center, grant NNX10AM08H. This research was also supported at UCLA and the Goddard Space Flight Center by an Interdisciplinary Science grant from the Magnetospheric Multiscale project (NASA grant NNX08AO48G at UCLA). M. El-Alaoui was supported by NASA grant NNX10AQ47G. Computational resources were provided by the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant OCI-1053575. R.J. Walker's contribution to this work was supported as Individual Research and Development while he was at the National Science Foundation. M.G. Kivelson was supported by NASA grant UCB/NASA NAS 5-02099. We acknowledge the experiment teams that acquired, processed, and provided the OMNI-included data, and J.H. King and N.E. Papitashvili of NASA/GSFC for creating the OMNI data set. Geotail magnetic field data were provided by T. Nagai, JAXA in Japan. Geotail and OMNI data were obtained through the Virtual Magnetospheric Observatory (VMO). We acknowledge C. Carr and the Double Star TC1 FGM instrument team, as well as ESA, Double Star, Center for Space Science and Applied Research, and the Chinese Academy of Sciences for Double Star data. We also acknowledge the World Data Center for Geomagnetism, Kyoto, and the Geomagnetic Network of China, for Pi2 and geomagnetic field data, and the SuperMAG network for Norolisk magnetometer data. We would also like to thank Krishan Khurana, Tung-Shin Hsu, and Robert J. Strangeway for helpful discussions concerning this research. NR 66 TC 2 Z9 2 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 OCT PY 2013 VL 118 IS 10 BP 6364 EP 6377 DI 10.1002/2013JA018734 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 296JH UT WOS:000330180600034 ER PT J AU Khazanov, GV Tel'nikhin, AA Kronberg, TK AF Khazanov, G. V. Tel'nikhin, A. A. Kronberg, T. K. TI Radiation belt electron dynamics driven by large-amplitude whistlers SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE RB electrons; oblique large-amplitude whistler waves; stochastic process; intermittent chaotic dynamics ID RELATIVISTIC ELECTRONS; GEOMAGNETIC STORMS; CHORUS; MAGNETOSPHERE; WAVES; FIELD AB Acceleration of radiation belt electrons driven by oblique large-amplitude whistler waves is studied. We show analytically and numerically that this is a stochastic process; the intensity of which depends on the wave power modified by Bessel functions. The type of this dependence is determined by the character of the nonlinear interaction due to coupling between action and phase. The results show that physically significant quantities have a relatively weak dependence on the wave power. C1 [Khazanov, G. V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tel'nikhin, A. A.; Kronberg, T. K.] Altai State Univ, Dept Phys & Technol, Barnaul 656099, Russia. RP Khazanov, GV (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM george.v.khazanov@nasa.gov RI feggans, john/F-5370-2012 FU NASA Van Allen Probes Project; NASA LWS Program FX Funding support for this study was provided by NASA Van Allen Probes (formerly known as the Radiation Belt Storm Probes (RBSP)) Project and the NASA LWS Program. G.K. also is grateful to Jenni Kissinger for her helpful comments. NR 30 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD OCT PY 2013 VL 118 IS 10 BP 6397 EP 6404 DI 10.1002/2013JA019122 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 296JH UT WOS:000330180600037 ER PT J AU Stephens, GK Sitnov, MI Kissinger, J Tsyganenko, NA McPherron, RL Korth, H Anderson, BJ AF Stephens, G. K. Sitnov, M. I. Kissinger, J. Tsyganenko, N. A. McPherron, R. L. Korth, H. Anderson, B. J. TI Empirical reconstruction of storm time steady magnetospheric convection events SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE steady magnetospheric convection; empirical geomagnetic field modeling; magnetotail convection crisis ID PLASMA PRESSURE DISTRIBUTION; FINITE-WIDTH MAGNETOTAIL; DAWN-DUSK ASYMMETRY; BURSTY BULK FLOWS; RING CURRENT; MAGNETIC-FIELD; EARTHS MAGNETOTAIL; SOLAR-WIND; INNER MAGNETOSPHERE; GEOMAGNETIC STORMS AB We investigate the storm-scale morphology of the magnetospheric magnetic field as well as underlying distributions of electric currents, equatorial plasma pressure, and entropy for four steady magnetospheric convection (SMC) events that occurred during the May 2000 and October 2011 magnetic storms. The analysis is made using the empirical geomagnetic field model TS07D, in which the structure of equatorial currents is not predefined and it is dictated by data. The model also combines the strengths of statistical and event-oriented approaches in mining data for the reconstruction of the magnetic field. The formation of a near-Earth minimum of the equatorial magnetic field in the midnight sector is inferred from data without ad hoc assumptions of a special current system postulated in earlier empirical reconstructions. In addition, a new SMC class is discovered where the minimum equatorial field is substantially larger and located closer to Earth. The magnetic field tailward of the minimum is also much larger, and the corresponding area of accumulated magnetic flux may occupy a very short tail region. The equatorial current and plasma pressure are found to be strongly enhanced far beyond geosynchronous orbit and in a broad local time interval covering the whole nightside region. This picture is consistent with independent recent statistical studies of the SMC pressure distributions, global MHD, and kinetic Rice Convection Model-Equilibrium (RCM-E) simulations. Distributions of the flux tube volume and entropy inferred from data reveal different mechanisms of the magnetotail convection crisis resolution for two classes of SMC events. C1 [Stephens, G. K.; Sitnov, M. I.; Korth, H.; Anderson, B. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Kissinger, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tsyganenko, N. A.] St Petersburg Univ, Dept Earth Phys, St Petersburg, Russia. [McPherron, R. L.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [McPherron, R. L.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. RP Stephens, GK (reprint author), JHU APL, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM Grant.Stephens@jhuapl.edu RI Tsyganenko, Nikolai/J-7377-2012; Sitnov, Mikhail/H-2316-2016 OI Tsyganenko, Nikolai/0000-0002-5938-1579; FU NSF [ATM0817333]; NASA [NNX10AT26G]; NSF Space [Weather-AGS-0720422]; [NASA-NNX07AG16G] FX The authors thank J. Yang, R. Wolf, F. Toffoletto, V. A. Sergeev, and V. G. Merkin for useful discussions. This work was supported by NSF grant ATM0817333 and NASA grant NNX10AT26G. J. Kissinger and R. L. McPherron would like to acknowledge support from NASA-NNX07AG16G and NSF Space Weather-AGS-0720422. NR 87 TC 7 Z9 7 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 OCT PY 2013 VL 118 IS 10 BP 6434 EP 6456 DI 10.1002/jgra.50592 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 296JH UT WOS:000330180600041 ER PT J AU Sundberg, T Boardsen, SA Slavin, JA Uritsky, VM Anderson, BJ Korth, H Gershman, DJ Raines, JM Zurbuchen, TH Solomon, SC AF Sundberg, Torbjoern Boardsen, Scott A. Slavin, James A. Uritsky, Vadim M. Anderson, Brian J. Korth, Haje Gershman, Daniel J. Raines, Jim M. Zurbuchen, Thomas H. Solomon, Sean C. TI Cyclic reformation of a quasi-parallel bow shock at Mercury: MESSENGER observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE bow shock; Mercury; MESSENGER ID AMPLITUDE MAGNETIC-STRUCTURES; PERPENDICULAR SHOCKS; COLLISIONLESS SHOCKS; FIELD OBSERVATIONS; STRUCTURES SLAMS; UPSTREAM; WAVES; IONS; MAGNETOSPHERE; INSTRUMENT AB We here document with magnetic field observations a passage of the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft through Mercury's magnetosphere under conditions of a quasi-parallel bow shock, i.e., when the direction of the upstream interplanetary magnetic field was within 45 degrees of the bow shock normal. The spacecraft's fast transition of the magnetosheath and the steady solar wind conditions during the period analyzed allow both spatial and temporal properties of the shock crossing to be investigated. The observations show that the shock reformation process can be nearly periodic under stable solar wind conditions. Throughout the 25-min-long observation period, the pulsation duration deviated by at most similar to 10% from the average 10 s period measured. This quasiperiodicity allows us to study all aspects of the shock reconfiguration, including ultra-low-frequency waves in the upstream region and large-amplitude magnetic structures observed in the vicinity of the magnetosheath-solar wind transition region and inside the magnetosheath. We also show that bow shock reformation can be a substantial source of wave activity in the magnetosphere, on this occasion having given rise to oscillations in the magnetic field with peak-to-peak amplitudes of 40-50 nT over large parts of the dayside magnetosphere. The clean and cyclic behavior observed throughout the magnetosphere, the magnetosheath, and the upstream region indicates that the subsolar region was primarily influenced by a cyclic reformation of the shock front, rather than by a spatial and temporal patchwork of short large-amplitude magnetic structures, as is generally the case at the terrestrial bow shock under quasi-parallel conditions. C1 [Sundberg, Torbjoern] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA. [Sundberg, Torbjoern; Boardsen, Scott A.; Uritsky, Vadim M.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD USA. [Sundberg, Torbjoern] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England. [Boardsen, Scott A.] Univ Maryland, Goddard Earth Sci & Technol Ctr, College Pk, MD 20742 USA. [Slavin, James A.; Gershman, Daniel J.; Raines, Jim M.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Uritsky, Vadim M.] Catholic Univ Amer, Washington, DC 20064 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 Sundberg, T (reprint author), Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England. EM torbjorn.sundberg@gmail.com RI Slavin, James/H-3170-2012 OI Slavin, James/0000-0002-9206-724X FU NASA Discovery Program [NAS5-97271, NASW-00002]; NASA Postdoctoral Program at the Goddard Space Flight Center through NASA; NASA Planetary Data Analysis Program [NNX10AU26G] FX 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. This research was also supported by the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA, and by the NASA Planetary Data Analysis Program grant NNX10AU26G. NR 38 TC 7 Z9 7 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 OCT PY 2013 VL 118 IS 10 BP 6457 EP 6464 DI 10.1002/jgra.50602 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 296JH UT WOS:000330180600042 ER PT J AU Moore, TE Chandler, MO Buzulukova, N Collinson, GA Kepko, EL Garcia-Sage, KS Henderson, MG Sitnov, MI AF Moore, T. E. Chandler, M. O. Buzulukova, N. Collinson, G. A. Kepko, E. L. Garcia-Sage, K. S. Henderson, M. G. Sitnov, M. I. TI "Snowplow" injection front effects SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE plasma; injection; front; substorm; plasmasphere; trough ID NEAR-EARTH MAGNETOTAIL; INNER MAGNETOSPHERE; ION ENERGIZATION; PLASMA SHEET; ART.; DYNAMICS; CLUSTER; EVENTS; MOTION; COLD AB As the Polar spacecraft apogee precessed through the magnetic equator in 2001, Polar encountered numerous substorm events in the region between geosynchronous orbit and 10 R-E geocentric distance; most of them in the plasma sheet boundary layers. Of these, a small number was recorded near the neutral sheet in the evening sector. Polar/Thermal Ion Dynamics Experiment provides a unique perspective on the lowest-energy ion plasma, showing that these events exhibited a damped wavelike character, initiated by a burst of radially outward flow transverse to the local magnetic field at similar to 80km/s. They then exhibit strongly damped cycles of inward/outward flow with a period of several minutes. After one or two cycles, they culminated in a hot plasma electron and ion injection, quite similar to those observed at geosynchronous orbit. Cold plasmaspheric plasmas comprise the outward flow cycles, while the inward flow cycles contain counterstreaming field-parallel polar wind-like flows. The observed wavelike structure, preceding the arrival of an earthward moving substorm injection front, suggests an outward displacement driven by the inward motion at local times closer to midnight, that is, a snowplow effect. The damped in/out flows are consistent with interchange oscillations driven by the arrival at the observed local time by an injection originating at greater radius and local time. C1 [Moore, T. E.; Buzulukova, N.; Collinson, G. A.; Kepko, E. L.; Garcia-Sage, K. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Chandler, M. O.] NASA, Marshall Space Flight Ctr, Huntsville, AL USA. [Buzulukova, N.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Henderson, M. G.] Los Alamos Natl Lab, Los Alamos, NM USA. [Sitnov, M. I.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Moore, TE (reprint author), NASA, Goddard Space Flight Ctr, Code 670, Greenbelt, MD 20771 USA. EM thomas.e.moore@nasa.gov RI Kepko, Larry/D-7747-2012; Sitnov, Mikhail/H-2316-2016; Henderson, Michael/A-3948-2011 OI Kepko, Larry/0000-0002-4911-8208; Henderson, Michael/0000-0003-4975-9029 FU Polar-Wind-Geotail (Global Geospace) Program; Goddard Heliophysics Science Division; Magnetospheric Multiscale Mission Project FX The authors acknowledge support from the Polar-Wind-Geotail (Global Geospace) Program, the Goddard Heliophysics Science Division, the Magnetospheric Multiscale Mission Project, and other sources. For the ground magnetometer data, we gratefully acknowledge the following: CARISMA, Ian Mann; CANMOS; The S-RAMP Database, K. Yumoto, and K. Shiokawa; SuperMAG, Jesper W. Gjerloev. NR 37 TC 4 Z9 4 U1 0 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 OCT PY 2013 VL 118 IS 10 BP 6478 EP 6488 DI 10.1002/jgra.50573 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 296JH UT WOS:000330180600044 ER PT J AU Li, X Schiller, Q Blum, L Califf, S Zhao, H Tu, W Turner, DL Gerhardt, D Palo, S Kanekal, S Baker, DN Fennell, J Blake, JB Looper, M Reeves, GD Spence, H AF Li, X. Schiller, Q. Blum, L. Califf, S. Zhao, H. Tu, W. Turner, D. L. Gerhardt, D. Palo, S. Kanekal, S. Baker, D. N. Fennell, J. Blake, J. B. Looper, M. Reeves, G. D. Spence, H. TI First results from CSSWE CubeSat: Characteristics of relativistic electrons in the near-Earth environment during the October 2012 magnetic storms SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE radiation belt electrons; CubeSat; Van Allen Probes; CSSWE ID RADIATION BELT ELECTRONS; SOLAR-WIND VELOCITY; GEOMAGNETIC STORMS; ULF OSCILLATIONS; WAVE POWER; ACCELERATION; MAGNETOSPHERE; ZONE; PRECIPITATION; ENHANCEMENTS AB Measurements from the Relativistic Electron and Proton Telescope integrated little experiment (REPTile) on board the Colorado Student Space Weather Experiment (CSSWE) CubeSat mission, which was launched into a highly inclined (65 degrees) low Earth orbit, are analyzed along with measurements from the Relativistic Electron and Proton Telescope (REPT) and the Magnetic Electron Ion Spectrometer (MagEIS) instruments aboard the Van Allen Probes, which are in a low inclination (10 degrees) geo-transfer-like orbit. Both REPT and MagEIS measure the full distribution of energetic electrons as they traverse the heart of the outer radiation belt. However, due to the small equatorial loss cone (only a few degrees), it is difficult for REPT and MagEIS to directly determine which electrons will precipitate into the atmosphere, a major radiation belt loss process. REPTile, a miniaturized version of REPT, measures the fraction of the total electron population that has small enough equatorial pitch angles to reach the altitude of CSSWE, 480km x 780km, thus measuring the precipitating population as well as the trapped and quasi-trapped populations. These newly available measurements provide an unprecedented opportunity to investigate the source, loss, and energization processes that are responsible for the dynamic behavior of outer radiation belt electrons. The focus of this paper will be on the characteristics of relativistic electrons measured by REPTile during the October 2012 storms; also included are long-term measurements from the Solar Anomalous and Magnetospheric Particle Explorer to put this study into context. C1 [Li, X.; Schiller, Q.; Blum, L.; Califf, S.; Zhao, H.; Baker, D. N.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA. [Li, X.; Schiller, Q.; Blum, L.; Califf, S.; Zhao, H.; Gerhardt, D.; Palo, S.] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80303 USA. [Tu, W.; Reeves, G. D.] ISR 1 Los Alamos Natl Lab, Los Alamos, NM USA. [Turner, D. L.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA. [Kanekal, S.] NASA GSFC, Greenbelt, MD USA. [Fennell, J.; Blake, J. B.; Looper, M.] Aerosp Corp, Dept Space Sci, Los Angeles, CA 90009 USA. [Spence, H.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. RP Li, X (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA. EM xinlin.li@lasp.colorado.edu RI Tu, Weichao/B-6507-2011; Reeves, Geoffrey/E-8101-2011; OI Tu, Weichao/0000-0003-4547-3269; Reeves, Geoffrey/0000-0002-7985-8098; Blum, Lauren/0000-0002-4797-5476; PALO, SCOTT/0000-0002-4729-4929; Spence, Harlan/0000-0002-2526-2205 FU NSF (CubeSat program) [AGSW 0940277]; NASA [NAS5-01072, NAS5-02099] FX We would like to thank Richard Selesnick and Mike Temerin for their helpful discussions. This work is mainly supported by NSF (CubeSat program) grant AGSW 0940277 and also NASA contract NAS5-01072 (Van Allen Probes mission) and NAS5-02099 (THEMIS mission). NR 54 TC 16 Z9 16 U1 2 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD OCT PY 2013 VL 118 IS 10 BP 6489 EP 6499 DI 10.1002/2013JA019342 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 296JH UT WOS:000330180600045 ER PT J AU Tierney, D Briggs, MS Fitzpatrick, G Chaplin, VL Foley, S McBreen, S Connaughton, V Xiong, S Byrne, D Carr, M Bhat, PN Fishman, GJ Greiner, J Kippen, RM Meegan, CA Paciesas, WS Preece, RD von Kienlin, A Wilson-Hodge, C AF Tierney, D. Briggs, M. S. Fitzpatrick, G. Chaplin, V. L. Foley, S. McBreen, S. Connaughton, V. Xiong, S. Byrne, D. Carr, M. Bhat, P. N. Fishman, G. J. Greiner, J. Kippen, R. M. Meegan, C. A. Paciesas, W. S. Preece, R. D. von Kienlin, A. Wilson-Hodge, C. TI Fluence distribution of terrestrial gamma ray flashes observed by the Fermi Gamma-ray Burst Monitor SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE tgf AB The observed ray fluence distribution of terrestrial gamma ray flashes (TGFs) detected by the Fermi Gamma-ray Burst Monitor (GBM) is altered by instrumental effects. We perform corrections for dead time, pulse pileup, and detection efficiency in a model-independent manner. A sample of 106 GBM TGFs is selected to include both TGFs that triggered GBM and weaker TGFs found using an off-line search. Detector dead time and pulse pileup lower the observed fluence of each TGF and the detection efficiency causes weaker TGFs to have a lower probability of detection than brighter TGFs. Monte Carlo simulations are performed in each case to correct for these effects. The corrected fluence distribution is well fit with a power law of index =-2.200.13. This is consistent with previous estimates using other techniques. Neither a high-fluence cutoff nor a low-fluence limit is found. The fluence distribution is also expressed in units of TGF h(-1) km(-2) versus photons cm(-2) per TGF. C1 [Tierney, D.; Fitzpatrick, G.; Foley, S.; McBreen, S.; Byrne, D.; Carr, M.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Briggs, M. S.; Chaplin, V. L.; Connaughton, V.; Xiong, S.; Bhat, P. N.; Preece, R. D.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Briggs, M. S.; Connaughton, V.; Preece, R. D.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Fishman, G. J.] Jacobs Engn Inc, Huntsville, AL USA. [Greiner, J.; von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM USA. [Meegan, C. A.; Paciesas, W. S.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA. [Wilson-Hodge, C.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. RP Tierney, D (reprint author), Univ Coll Dublin, Sch Phys, Stillorgan Rd, Dublin 4, Ireland. EM david.tierney@ucd.ie OI Preece, Robert/0000-0003-1626-7335 FU Science Foundation Ireland [09-RFP-AST-2400]; Irish Research Council; Irish Research Council for Science, Engineering and Technology; Marie Curie Actions; Programme for Research in Third Level Institutions (PRTLI); European Regional Development Fund FX D.T. acknowledges support from Science Foundation Ireland under grant 09-RFP-AST-2400. G.F. acknowledges the support of the Irish Research Council. S.F. acknowledges the support of the Irish Research Council for Science, Engineering and Technology, cofunded by Marie Curie Actions under FP7. D.B. acknowledges support from the Programme for Research in Third Level Institutions (PRTLI) Cycle 5 and from the European Regional Development Fund. We thank the anonymous reviewers for helpful suggestions during the refereeing process. NR 25 TC 8 Z9 8 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD OCT PY 2013 VL 118 IS 10 BP 6644 EP 6650 DI 10.1002/jgra.50580 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 296JH UT WOS:000330180600058 ER PT J AU Pillar, EA Guzman, MI Rodriguez, JM AF Pillar, Elizabeth A. Guzman, Marcelo I. Rodriguez, Jose M. TI Conversion of Iodide to Hypoiodous Acid and Iodine in Aqueous Microdroplets Exposed to Ozone SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID AIR/WATER INTERFACE; ARCTIC ATMOSPHERE; AEROSOL FORMATION; BOUNDARY-LAYER; SEA-SURFACE; WATER; KINETICS; DESTRUCTION; HYDROLYSIS; PARTICLES AB Halides are incorporated into aerosol sea spray, where they start the catalytic destruction of ozone (O-3) over the oceans and affect the global troposphere. Two intriguing environmental problems undergoing continuous research are (1) to understand how reactive gas phase molecular halogens are directly produced from inorganic halides exposed to O-3 and (2) to constrain the environmental factors that control this interfacial process. This paper presents a laboratory study of the reaction of. O-3 at variable iodide (I-) concentration (0.010-100 mu M) for solutions aerosolized at 25 degrees C, which reveal remarkable differences in the reaction intermediates and products expected in sea spray for low tropospheric [O-3]. The ultrafast oxidation of I- by O-3 at the air-water interface of microdroplets is evidenced by the appearance of hypoiodous acid (HIO), iodite (IO2-), iodate (IO3-), triiodide (I-3(-)), and molecular iodine (I-2). Mass spectrometry measurements reveal an enhancement (up to 28%) in the dissolution of gaseous O-3 at the gas-liquid interface when increasing the concentration of NaI or NaBr from 0.010 to 100 mu M. The production of iodine species such as HIO and I-2 from NaI aerosolized solutions exposed to 50 ppbv O-3 can occur at the air-water interface of sea spray, followed by their transfer to the gas-phase, where they contribute to the loss of tropospheric ozone. C1 [Pillar, Elizabeth A.; Guzman, Marcelo I.] Univ Kentucky, Dept Chem, Lexington, KY 40506 USA. [Rodriguez, Jose M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Guzman, MI (reprint author), Univ Kentucky, Dept Chem, Lexington, KY 40506 USA. EM marcelo.guzman@uky.edu RI Guzman, Marcelo/C-5966-2008; Rodriguez, Jose/G-3751-2013 OI Guzman, Marcelo/0000-0002-6730-7766; Rodriguez, Jose/0000-0002-1902-4649 FU NASA [NNX10AV39A]; NSF CAREER award [CHE-1255290] FX We thank research funding from NASA (NNX10AV39A) and NSF CAREER award (CHE-1255290). NR 64 TC 8 Z9 8 U1 1 U2 37 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 OCT 1 PY 2013 VL 47 IS 19 BP 10971 EP 10979 DI 10.1021/es401700h PG 9 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 295CT UT WOS:000330094900030 PM 23987087 ER PT J AU Li, JR Okin, GS Skiles, SM Painter, TH AF Li, Junran Okin, Gregory S. Skiles, S. McKenzie Painter, Thomas H. TI Relating variation of dust on snow to bare soil dynamics in the western United States SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE remote sensing; snow hydrology; desert dust; water resource management; vegetation dynamics ID CLIMATE; DEPOSITION; VEGETATION; DESERT; COVER; MONSOON; ASIA AB The deposition of desert dust to mountain snow directly impacts the hydrologic cycle and water resource management through the depression of snow albedo and acceleration of snowmelt. However, the key processes that control the variation of dust deposition to snow are poorly understood. Here we relate the bare soil exposure from the moderate resolution imaging spectroradiometer (MODIS) reflectance data for the period of 2002-2011, with dust loading in snow at downwind mountain sites in southern Colorado, the United States. We found that, for many pixels, remotely sensed fraction of bare soil in the dust-emitting area is significantly correlated with end-of-season dust concentrations in snow, and that the highest number of significantly correlated pixels in the dust-source area corresponds well with the period of peak dust deposition in the mountain snow (April-May). This analysis indicates that surface conditions in the dust-source area may provide first-order controls on emission of dust and deposition of that dust to the mountain snowcover. A preliminary analysis of precipitation records indicates that bare ground cover is strongly affected by prior rainfall in the months preceding the dust-emission season. C1 [Li, Junran] Univ Tulsa, Dept Geosci, Tulsa, OK 74104 USA. [Okin, Gregory S.; Skiles, S. McKenzie] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA. [Painter, Thomas H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Painter, Thomas H.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. RP Li, JR (reprint author), Univ Tulsa, Dept Geosci, Tulsa, OK 74104 USA. EM junran@utulsa.edu RI Painter, Thomas/B-7806-2016; OI Okin, Gregory/0000-0002-0484-3537 FU NASA [NNX10AO97G] FX This research was supported by NASA Grant NNX10AO97G. We greatly acknowledge Matt Zebrowski and Jida Wang for their assistance in data processing and remote sensing analysis. Part of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration. NR 36 TC 5 Z9 5 U1 1 U2 15 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-9326 J9 ENVIRON RES LETT JI Environ. Res. Lett. PD OCT-DEC PY 2013 VL 8 IS 4 AR 044054 DI 10.1088/1748-9326/8/4/044054 PG 8 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 288IJ UT WOS:000329604900061 ER PT J AU Yue, H Lay, T Schwartz, SY Rivera, L Protti, M Dixon, TH Owen, S Newman, AV AF Yue, Han Lay, Thorne Schwartz, Susan Y. Rivera, Luis Protti, Marino Dixon, Timothy H. Owen, Susan Newman, Andrew V. TI The 5 September 2012 Nicoya, Costa Rica M-w 7.6 earthquake rupture process from joint inversion of high-rate GPS, strong-motion, and teleseismic P wave data and its relationship to adjacent plate boundary interface properties SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE 2012 Costa Rica earthquake; Seismic; Geodetic joint inversion; Finite fault model; Hypocenter relocation ID SEISMOGENIC ZONE; TOHOKU EARTHQUAKE; CONVERGENT MARGIN; PENINSULA; MODELS; SEISMICITY; DEFORMATION; CONSTRAINTS; CATALOG AB On 5 September 2012, a large thrust earthquake (M-w 7.6) ruptured a densely instrumented seismic gap on the shallow-dipping plate boundary beneath the Nicoya Peninsula, Costa Rica. Ground motion recordings directly above the rupture zone provide a unique opportunity to study the detailed source process of a large shallow megathrust earthquake using very nearby land observations. Hypocenter relocation using local seismic network data indicates that the event initiated with small emergent seismic waves from a hypocenter 10 km offshore, 13 km deep on the megathrust. A joint finite-fault inversion using high-rate GPS, strong-motion ground velocity recordings, GPS static offsets, and teleseismic P waves reveals that the primary slip zone (slip>1 m) is located beneath the peninsula. The rupture propagated downdip from the hypocenter with a rupture velocity of 3.0 km/s. The primary slip zone extends 70 km along strike and 30 km along dip, with an average slip of 2 m. The associated static stress drop is 3 MPa. The seismic moment is 3.5 x 10(20) Nm, giving M-w=7.6. The coseismic large-slip patch directly overlaps an onshore interseismic locked region indicated by geodetic observations and extends downdip to the intersection with the upper plate Moho. At deeper depths, below the upper plate Moho, seismic tremor and low-frequency earthquakes have been observed. Most tremor locates in adjacent areas of the megathrust that have little coseismic slip; a region of prior slow slip deformation to the southeast also has no significant coseismic slip or aftershocks. An offshore locked patch indicated by geodetic observations does not appear to have experienced coseismic slip, and aftershocks do not overlap this region, allowing the potential for a comparable size rupture offshore in the future. C1 [Yue, Han; Lay, Thorne; Schwartz, Susan Y.] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Rivera, Luis] Univ Strasbourg, CNRS, Inst Phys Globe Strasbourg, Strasbourg, France. [Protti, Marino] Univ Nacl, Observ Vulcanol & Sismol Costa Rica, Heredia, Costa Rica. [Dixon, Timothy H.] Univ S Florida, Dept Geol, Tampa, FL 33620 USA. [Owen, Susan] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Newman, Andrew V.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. RP Yue, H (reprint author), Univ Calif Santa Cruz, Dept Earth & Planetary Sci, 1156 High St, Santa Cruz, CA 95064 USA. EM johnyuehan2003@gmail.com RI Newman, Andrew/E-7682-2012 OI Newman, Andrew/0000-0001-7414-1197 FU NSF [EAR-1245717, OCE-0841061, EAR-0842338] FX We made extensive use of the frequency-wavenumber integration code in the seismic wave simulation software made openly available by Robert Herrmann (http://www.eas.slu.edu/eqc/eqccps.html). We thank Victor Gonzalez for installing and operating the Nicoya seismic and CGPS networks, and Aaron Moya from LIS-UCR for providing the strong motion data. We thank two anonymous reviewers and the Associate Editor for their helpful reviews. This work made use of GMT and SAC software. The IRIS DMS data center was used to access the seismic data from Global Seismic Network and Federation of Digital Seismic Network stations. This work was supported by NSF grants EAR-1245717 (T. L.) and OCE-0841061 and EAR-0842338 (S.Y.S). We thank Jake Walter for providing the aftershock catalog. NR 49 TC 33 Z9 33 U1 4 U2 16 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 OCT PY 2013 VL 118 IS 10 BP 5453 EP 5466 DI 10.1002/jgrb.50379 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 292AV UT WOS:000329874900021 ER PT J AU Baird, RW Oleson, EM Barlow, J Ligon, AD Gorgone, AM Mahaffy, SD AF Baird, Robin W. Oleson, Erin M. Barlow, Jay Ligon, Allan D. Gorgone, Antoinette M. Mahaffy, Sabre D. TI Evidence of an Island-Associated Population of False Killer Whales (Pseudorca crassidens) in the Northwestern Hawaiian Islands SO PACIFIC SCIENCE LA English DT Article ID CYCLONIC EDDIES; MOVEMENTS; PATTERNS; WATERS AB Two populations of false killer whales, Pseudorca crassidens, are recognized from Hawaiian waters: the Hawaiian insular population, an island-associated population found around the main Hawaiian Islands; and the Hawai'i pelagic population, found in offshore waters. This species has not been previously documented near the Northwestern Hawaiian Islands. During a 2010 large-vessel survey throughout the Exclusive Economic Zone (EEZ) surrounding the Hawaiian Islands, false killer whales from 11 encounters were individually photo-identified, and photos were compared among encounters and with a catalog of false killer whales from the main Hawaiian Islands. Individuals from three of the encounters, all in the Northwestern Hawaiian Islands within the eastern part of the Papahanaumokuakea Marine National Monument, were the only ones documented that matched with false killer whales previously seen around the main Hawaiian Islands, and the matches were to individuals documented off Kaua'i in 2008 that were of unknown population membership. Two individuals from one of these three 2010 encounters were instrumented with satellite tags attached to dorsal fins, and their movements were documented over 4.6 and 52 days. Movements of the tagged individuals ranged from French Frigate Shoals to Middle Bank (between Nihoa and Ni'ihau) and included shallow nearshore waters and deep waters to 147 km from land. Combined, the photo-identification and satellite-tagging results suggest that there is a second island-associated population of this species in Hawai'i that primarily uses the Northwestern Hawaiian Islands, with a range that overlaps with that of the main Hawaiian Islands insular population. C1 [Baird, Robin W.; Mahaffy, Sabre D.] Cascadia Res Collect, Olympia, WA 98501 USA. [Oleson, Erin M.] NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96814 USA. [Barlow, Jay] NOAA, Southwest Fisheries Sci Ctr, Natl Marine Fisheries Serv, La Jolla, CA 92037 USA. [Gorgone, Antoinette M.] NOAA, Southwest Fisheries Sci Ctr, Natl Marine Fisheries Serv, Beaufort, NC 98250 USA. RP Baird, RW (reprint author), Cascadia Res Collect, 218 1-2 West 4th Ave, Olympia, WA 98501 USA. EM rwbaird@cascadiaresearch.org NR 15 TC 6 Z9 6 U1 0 U2 6 PU UNIV HAWAII PRESS PI HONOLULU PA 2840 KOLOWALU ST, HONOLULU, HI 96822 USA SN 0030-8870 EI 1534-6188 J9 PAC SCI JI Pac. Sci. PD OCT PY 2013 VL 67 IS 4 BP 513 EP 521 DI 10.2984/67.4.2 PG 9 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 283PU UT WOS:000329260300002 ER PT J AU Shibuya, T Tahata, M Ueno, Y Komiya, T Takai, K Yoshida, N Maruyama, S Russell, MJ AF Shibuya, Takazo Tahata, Miyuki Ueno, Yuichiro Komiya, Tsuyoshi Takai, Ken Yoshida, Naohiro Maruyama, Shigenori Russell, Michael J. TI Decrease of seawater CO2 concentration in the Late Archean: An implication from 2.6 Ga seafloor hydrothermal alteration SO PRECAMBRIAN RESEARCH LA English DT Article DE Archean; Carbon dioxide; Seawater; Hydrothermal alteration; Carbonation; Pilbara ID CARBON-DIOXIDE CONCENTRATIONS; BANDED IRON-FORMATION; BILLION YEARS AGO; DE-FUCA RIDGE; WESTERN-AUSTRALIA; OCEANIC-CRUST; GREENSTONE-BELT; PILBARA CRATON; PRECAMBRIAN CARBONATES; ISOTOPIC COMPOSITION AB Before continents attained a critical aerial dimension on the early Earth, hydrothermal carbonation of subseafloor crust is considered to have played the dominant role in fixing CO2 from the CO2-rich ocean. However, it is uncertain how and when the seawater CO2 level decreased and the strong carbonation of oceanic crust ceased. Here we report the depth profiles of the volume concentration and the carbon isotopes of calcites in the Late Archean/Paleoproterozoic volcanic rocks (Fortescue and Hamersley groups), exposed in the southwestern Pilbara Craton, Western Australia. The depth profiles indicate that 2.6 Ga seafloor hydrothermal carbonation is well preserved in the study area and that the CO2 content of subseafloor crust per seafloor unit area is estimated to be clearly lower than those in the Early and Middle Archean and similar to the Phanerozoic equivalents. This suggests that the CO2 concentration in seawater decreased from the Middle Archean to the Late Archean. This period broadly corresponds to the time of the first appearance of supercontinent on Earth. The amalgamation of continents has the potential to decrease seawater CO2 concentration due to the removal of platform carbonate to continental interior. Subsequent fragmentation of supercontinent likely cause the carbonate deposition around newly created continental shelves. It is therefore implied that seawater CO2 concentration in the early Earth was lowered by not only the hydrothermal carbonation of subseafloor crust but also through the formation and breakup of supercontinent in the Late Archean. (C) 2013 Elsevier B.V. All rights reserved. C1 [Shibuya, Takazo; Takai, Ken] Japan Agcy Marine Earth Sci & Technol JAMSTEC, Precambrian Ecosyst Lab, Yokosuka, Kanagawa 2370061, Japan. [Shibuya, Takazo; Takai, Ken] Japan Agcy Marine Earth Sci & Technol JAMSTEC, Submarine Hydrothermal Syst Res Grp, Yokosuka, Kanagawa 2370061, Japan. [Shibuya, Takazo; Russell, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tahata, Miyuki; Ueno, Yuichiro] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan. [Komiya, Tsuyoshi; Maruyama, Shigenori] Univ Tokyo, Dept Earth Sci & Astron, Meguro Ku, Tokyo 1538902, Japan. [Takai, Ken] Japan Agcy Marine Earth Sci & Technol JAMSTEC, Subsurface Geobiol Adv Res SUGAR Project, Yokosuka, Kanagawa 2370061, Japan. [Yoshida, Naohiro] Tokyo Inst Technol, Dept Environm Sci & Technol, Yokohama, Kanagawa 2268502, Japan. [Yoshida, Naohiro] Tokyo Inst Technol, Dept Environm Chem & Engn, Yokohama, Kanagawa 2268502, Japan. RP Shibuya, T (reprint author), Japan Agcy Marine Earth Sci & Technol JAMSTEC, Precambrian Ecosyst Lab, 2-15 Natsushima Cho, Yokosuka, Kanagawa 2370061, Japan. EM takazos@jamstec.go.jp RI Yamaichi, Takeshi/A-5595-2010; Ueno, Yuichiro/A-9959-2014; Yoshida, Naohiro/A-8335-2010; Komiya, Tsuyoshi/A-3704-2009 OI Ueno, Yuichiro/0000-0002-9095-4742; Yoshida, Naohiro/0000-0003-0454-3849; Komiya, Tsuyoshi/0000-0002-4000-0617 FU Ministry of Education, Culture, Sports, Science and Technology of Japan [15104008, 20840053, 22740333]; Mitsubishi Zaidan; NASA's Astrobiology Institute (Icy Worlds) FX We thank M. Terabayashi, K. Hirose, T. Kabashima, H. Ohta, G. Kimura and Y. Kato for assistance during field work. We are grateful to N. Sleep and an anonymous reviewer for their valuable comments, and R. Parrish for editorial handling and suggestions. This work was partly supported by grants from the Ministry of Education, Culture, Sports, Science and Technology of Japan (no. 15104008, 20840053 and 22740333) and by Mitsubishi Zaidan. MJR's research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration: Exobiology and Evolutionary Biology and supported by NASA's Astrobiology Institute (Icy Worlds). NR 50 TC 7 Z9 7 U1 4 U2 22 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0301-9268 EI 1872-7433 J9 PRECAMBRIAN RES JI Precambrian Res. PD OCT PY 2013 VL 236 BP 59 EP 64 DI 10.1016/j.precamres.2013.07.010 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 277GD UT WOS:000328806100005 ER PT J AU Khazanov, GV Sibeck, DG AF Khazanov, George V. Sibeck, David G. TI Restrictions on the quasi-linear description of electron-chorus interaction in the earth's magnetosphere SO RADIATION EFFECTS AND DEFECTS IN SOLIDS LA English DT Article DE magnetosphere; relativistic electrons; whistlers waves ID PITCH-ANGLE DIFFUSION; WHISTLER-MODE CHORUS; CHAOTIC MOTION; WAVE; PRECIPITATION AB The interaction of electrons with coherent chorus waves in the random phase approximation can be described as quasi-linear diffusion for waves with amplitudes below some limit. The limit is calculated for relativistic and non-relativistic electrons. For stronger waves, the friction force should be taken into account. C1 [Khazanov, George V.; Sibeck, David G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Khazanov, GV (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. EM george.v.khazanov@nasa.gov FU NASA Van Allen Probes; NASA LWS Program FX Funding support for this study was provided by NASA Van Allen Probes (formerly known as the Radiation Belt Storm Probes (RBSP)) Project, and the NASA LWS Program. We also are grateful to Dr Krivorutsky for helpful comments. NR 18 TC 0 Z9 0 U1 0 U2 0 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND SN 1042-0150 EI 1029-4953 J9 RADIAT EFF DEFECT S JI Radiat. Eff. Defects Solids PD OCT 1 PY 2013 VL 168 IS 10 SI SI BP 799 EP 804 DI 10.1080/10420150.2013.829841 PG 6 WC Nuclear Science & Technology; Physics, Fluids & Plasmas; Physics, Condensed Matter SC Nuclear Science & Technology; Physics GA 264HI UT WOS:000327867200006 ER PT J AU Sultana, M Herrero, F Khazanov, G AF Sultana, Mahmooda Herrero, Fred Khazanov, George TI Graphene chemical sensors for heliophysics applications SO RADIATION EFFECTS AND DEFECTS IN SOLIDS LA English DT Article DE graphene; chemical sensor; atomic oxygen; atomic oxygen ion; ionospheric plasma ID LARGE-AREA; OXIDE; PERFORMANCE; QUALITY; SHEETS; FILMS; GAS AB Graphene is a single layer of carbon atoms that offer a unique set of advantages as a chemical sensor due to a number of its inherent properties. Graphene has been explored as a gas sensor for a variety of gases, and molecular sensitivity has been demonstrated by measuring the change in electrical properties due to the adsorption of target species (Schedin, F.; Geim, A.K.; Morozov, S.V.; Hill, E.W.; Blake, P.; Katsnelson, M.I.; Novoselov, K.S. Nat. Mater2007,6, 652-655. doi:10.1038/nmat1967). In this paper, we discuss the development of an array of chemical sensors based on graphene and its relevance to plasma physics due to its sensitivity to radical species such as O+, H+ and the corresponding neutrals. We briefly discuss the great impact such sensors will have on a number of heliophysics applications such as ground-based manifestations of space weather. C1 [Sultana, Mahmooda; Khazanov, George] NASA, Detector Syst Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sultana, Mahmooda; Khazanov, George] NASA, Geospace Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Herrero, Fred] Space Syst Res Corp, Alexandria, VA 22314 USA. RP Sultana, M (reprint author), NASA, Detector Syst Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM mahmooda.sultana@nasa.gov RI feggans, john/F-5370-2012 NR 28 TC 0 Z9 0 U1 1 U2 8 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 1042-0150 EI 1029-4953 J9 RADIAT EFF DEFECT S JI Radiat. Eff. Defects Solids PD OCT 1 PY 2013 VL 168 IS 10 SI SI BP 805 EP 811 DI 10.1080/10420150.2013.831853 PG 7 WC Nuclear Science & Technology; Physics, Fluids & Plasmas; Physics, Condensed Matter SC Nuclear Science & Technology; Physics GA 264HI UT WOS:000327867200007 ER PT J AU Herrero, FA Khazanov, GV AF Herrero, Fred A. Khazanov, George V. TI A numerical study of the 30 degrees parallel plate analyzer for ionospheric electron spectroscopy SO RADIATION EFFECTS AND DEFECTS IN SOLIDS LA English DT Article DE charged-particle spectrometry; electron energy spectra; ionospheric electrons; parallel plate spectrograph ID ROCKET MEASUREMENT; ENERGY-SPECTRA; PHOTOELECTRONS; AIRGLOW AB A charged-particle spectrometer is described that uses a configuration of the 30 degrees parallel plate analyzer that differs from the previous one in that the entrance slit sits at the base plate while the exit slit is, as before, displaced to a point beneath the base plate. This approach preserves the second-order focusing previously found, yielding energy resolution of 0.01-0.3 eV for electrons in the energy range 1-30 eV. This is sufficient to address two identified problems in ionospheric electron energy distributions. In addition, the analyzer provides focusing of electron energies along a flat plane to operate as an energy spectrograph with a geometric factor of 10(-3) cm(2)-sr at an energy resolution Delta K/K=0.01; the performance required for very high resolution photoelectron spectroscopy in the ionospheric plasma. C1 [Herrero, Fred A.; Khazanov, George V.] NASA, Geospace Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Herrero, FA (reprint author), Space Syst Res Corp, Alexandria, VA USA. EM fherrero@thessrc.com RI feggans, john/F-5370-2012 FU NASA Goddard Office of the Chief Technologist under its Internal Research and Development Program at the NASA Goddard Space Flight Center, Greenbelt, Maryland FX This work was supported by the NASA Goddard Office of the Chief Technologist under its Internal Research and Development Program at the NASA Goddard Space Flight Center, Greenbelt, Maryland. NR 11 TC 0 Z9 0 U1 1 U2 3 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 1042-0150 EI 1029-4953 J9 RADIAT EFF DEFECT S JI Radiat. Eff. Defects Solids PD OCT 1 PY 2013 VL 168 IS 10 SI SI BP 812 EP 820 DI 10.1080/10420150.2013.831854 PG 9 WC Nuclear Science & Technology; Physics, Fluids & Plasmas; Physics, Condensed Matter SC Nuclear Science & Technology; Physics GA 264HI UT WOS:000327867200008 ER PT J AU Nicholas, A Finne, T Jones, H Herrero, F Vancil, B Aalami, D Galysh, I Mai, A Yen, J AF Nicholas, Andrew Finne, Ted Jones, Hollis Herrero, Fred Vancil, Bernie Aalami, Dean Galysh, Ivan Mai, Anthony Yen, James TI Wind Ion-drift Neutral Composition Suite cathode activation procedure and current-voltage characteristics SO RADIATION EFFECTS AND DEFECTS IN SOLIDS LA English DT Article DE ion source; laboratory plasmas; ionospheric plasma; ion-neutral coupling; thermosphere and ionosphere dynamics; neutral winds; ion-drifts; temperatures and densities AB The Wind Ion-drift Neutral Composition Suite (WINCS) uses three BaO thermionic cathodes in three ion sources for its neutral air measurements. The cathode activation procedure, obtained in laboratory measurements on a series of stock WINCS cathodes, ensures optimum cathode emission and life. The procedure begins by heating the cathode to 300-500 degrees C to evolve CO2 and other gaseous products of the binder and the BaCO3; then the cathode temperature is raised to above 900 degrees C for breakdown to BaO and sintering some of the Ba into the tungsten substrate; finally, activation begins by applying a small extraction voltage to the anode in front of the cathode. After activation, the cathode is ready to operate with any selected anode voltage. Electron emission of the WINCS cathodes easily exceeds 1 mA, and the fraction transmitted through the WINCS anodes exceeds 10% as required for WINCS. A maximum electron kinetic energy of about 90 eV was established as safe, also providing optimal ionization efficiency. C1 [Nicholas, Andrew; Finne, Ted; Galysh, Ivan; Mai, Anthony; Yen, James] Naval Res Lab, Washington, DC USA. [Jones, Hollis] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Herrero, Fred] Space Syst Res Corp, Alexandria, VA USA. [Vancil, Bernie] E Beam Corp, Beaverton, OR USA. [Aalami, Dean] Space Instruments, Irvine, CA USA. RP Herrero, F (reprint author), Space Syst Res Corp, Alexandria, VA USA. EM fherrero@thessrc.com FU Office of Naval Research FX The authors would like to thank the Office of Naval Research for support and the Department of Defense Space Test Program for providing the experiments with access to space. NR 6 TC 1 Z9 1 U1 0 U2 2 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 1042-0150 EI 1029-4953 J9 RADIAT EFF DEFECT S JI Radiat. Eff. Defects Solids PD OCT 1 PY 2013 VL 168 IS 10 SI SI BP 821 EP 832 DI 10.1080/10420150.2013.826217 PG 12 WC Nuclear Science & Technology; Physics, Fluids & Plasmas; Physics, Condensed Matter SC Nuclear Science & Technology; Physics GA 264HI UT WOS:000327867200009 ER PT J AU Herrero, F AF Herrero, Fred TI A gas kinetic method for investigations of the ionospheric plasma and the thermosphere SO RADIATION EFFECTS AND DEFECTS IN SOLIDS LA English DT Article DE ionospheric plasma; ion-neutral coupling; thermosphere and ionosphere dynamics; neutral winds; ion-drifts; temperatures and densities ID MIDNIGHT TEMPERATURE MAXIMUM; DYNAMICS EXPLORER; WINDS AB The gas kinetic method (GKM) obtains the Maxwellian velocity distributions of ionospheric plasma and thermospheric species (e.g. O (+), O (+)(2), O and N (2)) from in situ measurements of energy-angle distributions of the air stream entering an orbiting spectrometer. Referenced to the spectrometer ram axis, measurements based on the GKM yield the ion-drift or neutral wind vector (W) over right arrow, the ion or neutral temperature T, and ion or neutral number density n with sensitivities that may be implemented with present technologies for energy-angle spectrometers, i.e. the CubeSat WINCS spectrometers, designed to measure ion-drift and wind vectors together with ion and neutral temperatures, and composition. C1 [Herrero, Fred] NASA, Detector Syst Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Herrero, Fred] NASA, Geospace Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Herrero, F (reprint author), NASA, Detector Syst Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM fherrero@thessrc.com FU Office of the Chief Technologist; NASA-NOAA GOES project; NASA Goddard Space Flight Center, Greenbelt, MD FX This work was supported by the Office of the Chief Technologist and by summer assistantships from the NASA-NOAA GOES project and at the NASA Goddard Space Flight Center, Greenbelt, MD. The authors acknowledge an anonymous referee for noting the fast atomic oxygen possibility at high altitudes and other valuable comments. NR 14 TC 1 Z9 1 U1 0 U2 0 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 1042-0150 EI 1029-4953 J9 RADIAT EFF DEFECT S JI Radiat. Eff. Defects Solids PD OCT 1 PY 2013 VL 168 IS 10 SI SI BP 833 EP 846 DI 10.1080/10420150.2013.838243 PG 14 WC Nuclear Science & Technology; Physics, Fluids & Plasmas; Physics, Condensed Matter SC Nuclear Science & Technology; Physics GA 264HI UT WOS:000327867200010 ER PT J AU Eastman, JR Sangermano, F Machado, EA Rogan, J Anyamba, A AF Eastman, J. Ronald Sangermano, Florencia Machado, Elia A. Rogan, John Anyamba, Assaf TI Global Trends in Seasonality of Normalized Difference Vegetation Index (NDVI), 1982-2011 SO REMOTE SENSING LA English DT Article DE NDVI; GIMMS NDVI3g; Seasonal Trend Analysis; AVHRR; phenology ID IMAGE TIME-SERIES; CLIMATE-CHANGE; ARCTIC TUNDRA; SNOW COVER; ECOLOGICAL RESPONSES; ENVIRONMENTAL-CHANGE; SPRING PHENOLOGY; EUROPEAN FORESTS; SHRUB EXPANSION; SATELLITE DATA AB A 30-year series of global monthly Normalized Difference Vegetation Index (NDVI) imagery derived from the Global Inventory Modeling and Mapping Studies (GIMMS) NDVI3g archive was analyzed for the presence of trends in changing seasonality. Using the Seasonal Trend Analysis (STA) procedure, over half (56.30%) of land surfaces were found to exhibit significant trends. Almost half (46.10%) of the significant trends belonged to three classes of seasonal trends (or changes). Class 1 consisted of areas that experienced a uniform increase in NDVI throughout the year, and was primarily associated with forested areas, particularly broadleaf forests. Class 2 consisted of areas experiencing an increase in the amplitude of the annual seasonal signal whereby increases in NDVI in the green season were balanced by decreases in the brown season. These areas were found primarily in grassland and shrubland regions. Class 3 was found primarily in the Taiga and Tundra biomes and exhibited increases in the annual summer peak in NDVI. While no single attribution of cause could be determined for each of these classes, it was evident that they are primarily found in natural areas (as opposed to anthropogenic land cover conversions) and that they are consistent with climate-related ameliorations of growing conditions during the study period. C1 [Eastman, J. Ronald; Sangermano, Florencia] Clark Univ, Clark Labs, Worcester, MA 01610 USA. [Eastman, J. Ronald; Sangermano, Florencia; Rogan, John] Clark Univ, Grad Sch Geog, Worcester, MA 01610 USA. [Machado, Elia A.] CUNY Herbert H Lehman Coll, Dept Earth Environm & Geospatial Sci, Bronx, NY 10468 USA. [Anyamba, Assaf] NASA, GESTAR USRA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Anyamba, Assaf] NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Eastman, JR (reprint author), Clark Univ, Clark Labs, 950 Main St, Worcester, MA 01610 USA. EM reastman@clarku.edu; fsangermano@clarku.edu; elia.machado@lehman.cuny.edu; jrogan@clarku.edu; assaf.anyamba@nasa.gov NR 81 TC 46 Z9 48 U1 10 U2 76 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD OCT PY 2013 VL 5 IS 10 BP 4799 EP 4818 DI 10.3390/rs5104799 PG 20 WC Remote Sensing SC Remote Sensing GA 274OD UT WOS:000328614900004 ER PT J AU Peng, DL Jiang, ZY Huete, AR Ponce-Campos, GE Nguyen, U Luvall, JC AF Peng, Dailiang Jiang, Zhangyan Huete, Alfredo R. Ponce-Campos, Guillermo E. Uyen Nguyen Luvall, Jeffrey C. TI Response of Spectral Reflectances and Vegetation Indices on Varying Juniper Cone Densities SO REMOTE SENSING LA English DT Article DE juniper; hyperspectral; vegetation index; cones; ASD; phenology ID MODIS; BAND AB Juniper trees are widely distributed throughout the world and are common sources of allergies when microscopic pollen grains are transported by wind and inhaled. In this study, we investigated the spectral influences of pollen-discharging male juniper cones within a juniper canopy. This was done through a controlled outdoor experiment involving ASD FieldSpec Pro Spectroradiometer measurements over juniper canopies of varying cone densities. Broadband and narrowband spectral reflectance and vegetation index (VI) patterns were evaluated as to their sensitivity and their ability to discriminate the presence of cones. The overall aim of this research was to assess remotely sensed phenological capabilities to detect pollen-bearing juniper trees for public health applications. A general decrease in reflectance values with increasing juniper cone density was found, particularly in the Green (545-565 nm) and NIR (750-1,350 nm) regions. In contrast, reflectances in the shortwave-infrared (SWIR, 2,000 nm to 2,350 nm) region decreased from no cone presence to intermediate amounts (90 g/m(2)) and then increased from intermediate levels to the highest cone densities (200 g/m(2)). Reflectance patterns in the Red (620-700 nm) were more complex due to shifting contrast patterns in absorptance between cones and juniper foliage, where juniper foliage is more absorbing than cones only within the intense narrowband region of maximum chlorophyll absorption near 680 nm. Overall, narrowband reflectances were more sensitive to cone density changes than the equivalent MODIS broadbands. In all VIs analyzed, there were significant relationships with cone density levels, particularly with the narrowband versions and the two-band vegetation index (TBVI) based on Green and Red bands, a promising outcome for the use of phenocams in juniper phenology trait studies. These results indicate that spectral indices are sensitive to certain juniper phenologic traits that can potentially be used for juniper cone detection in support of public health applications. C1 [Peng, Dailiang] Chinese Acad Sci, Inst Remote Sensing & Digital Earth, Key Lab Digital Earth Sci, Beijing 100094, Peoples R China. [Jiang, Zhangyan; Uyen Nguyen] Univ Arizona, Dept Soil Water & Environm Sci, Tucson, AZ 85721 USA. [Huete, Alfredo R.] Univ Technol Sydney, Plant Funct Biol & Climate Change Cluster C3, Sydney, NSW 2007, Australia. [Ponce-Campos, Guillermo E.] USDA ARS Southwest Watershed Res, Tucson, AZ 85719 USA. [Ponce-Campos, Guillermo E.] Univ Arizona, Tucson, AZ 85721 USA. [Luvall, Jeffrey C.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35805 USA. RP Peng, DL (reprint author), Chinese Acad Sci, Inst Remote Sensing & Digital Earth, Key Lab Digital Earth Sci, Beijing 100094, Peoples R China. EM dlpeng@ceode.ac.cn; zyjiang2007@hotmail.com; alfredo.huete@uts.edu.au; geponce@gmail.com; nguyenthingocuyen@gmail.com; jluvall@nasa.gov RI Huete, Alfredo/C-1294-2008 OI Huete, Alfredo/0000-0003-2809-2376 FU National Natural Science Foundation of China [41201354]; NASA; National Basic Research Program of China [2009CB723902]; National High-tech R&D Program of China [2012AA12A301]; Chinese Academy of Sciences of Wenjiang Huang [Y24001101A] FX This study was funded by the National Natural Science Foundation of China No. 41201354, NASA Applications in Public Health grant (J. Luvall, P. I.), National Basic Research Program of China No. 2009CB723902, National High-tech R&D Program of China No: 2012AA12A301, and Hundred Talent Program of the Chinese Academy of Sciences of Wenjiang Huang No: Y24001101A. We also thank Bing Zhang from Key Laboratory of Digital Earth Science, Institute of Remote Sensing and Digital Earth, Chinese Academy of Sciences, for his help with several constructive comments. NR 27 TC 1 Z9 1 U1 0 U2 15 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD OCT PY 2013 VL 5 IS 10 BP 5330 EP 5345 DI 10.3390/rs5105330 PG 16 WC Remote Sensing SC Remote Sensing GA 274OD UT WOS:000328614900027 ER PT J AU Schumann, GJP Neal, JC Voisin, N Andreadis, KM Pappenberger, F Phanthuwongpakdee, N Hall, AC Bates, PD AF Schumann, G. J. -P. Neal, J. C. Voisin, N. Andreadis, K. M. Pappenberger, F. Phanthuwongpakdee, N. Hall, A. C. Bates, P. D. TI A first large-scale flood inundation forecasting model SO WATER RESOURCES RESEARCH LA English DT Article DE flood inundation forecasting; large scale; hydrodynamics ID ZAMBEZI RIVER-BASIN; PRECIPITATION PRODUCTS; WEATHER PREDICTION; SYSTEM; UNCERTAINTY; MOZAMBIQUE; DISCHARGE; LAND AB At present continental to global scale flood forecasting predicts at a point discharge, with little attention to detail and accuracy of local scale inundation predictions. Yet, inundation variables are of interest and all flood impacts are inherently local in nature. This paper proposes a large-scale flood inundation ensemble forecasting model that uses best available data and modeling approaches in data scarce areas. The model was built for the Lower Zambezi River to demonstrate current flood inundation forecasting capabilities in large data-scarce regions. ECMWF ensemble forecast (ENS) data were used to force the VIC (Variable Infiltration Capacity) hydrologic model, which simulated and routed daily flows to the input boundary locations of a 2-D hydrodynamic model. Efficient hydrodynamic modeling over large areas still requires model grid resolutions that are typically larger than the width of channels that play a key role in flood wave propagation. We therefore employed a novel subgrid channel scheme to describe the river network in detail while representing the floodplain at an appropriate scale. The modeling system was calibrated using channel water levels from satellite laser altimetry and then applied to predict the February 2007 Mozambique floods. Model evaluation showed that simulated flood edge cells were within a distance of between one and two model resolutions compared to an observed flood edge and inundation area agreement was on average 86%. Our study highlights that physically plausible parameter values and satisfactory performance can be achieved at spatial scales ranging from tens to several hundreds of thousands of km(2) and at model grid resolutions up to several km(2). C1 [Schumann, G. J. -P.; Neal, J. C.; Hall, A. C.; Bates, P. D.] Univ Bristol, Sch Geog Sci, Bristol, Avon, England. [Schumann, G. J. -P.; Andreadis, K. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Voisin, N.] Pacific NW Natl Lab, Richland, WA 99352 USA. [Pappenberger, F.] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England. [Pappenberger, F.] Hohai Univ, Coll Hydrol & Water Resources, Nanjing, Jiangsu, Peoples R China. [Phanthuwongpakdee, N.] Univ Bristol, Dept Civil Engn, Bristol, Avon, England. [Bates, P. D.] Univ Bristol, Cabot Inst, Bristol, Avon, England. RP Schumann, GJP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Guy.J.Schumann@jpl.nasa.gov RI Bates, Paul/C-8026-2012; Voisin, Nathalie/D-8845-2014; Neal, Jeffrey/C-8723-2009; Schumann, Guy/F-9760-2011; Pappenberger, Florian/A-2839-2009; OI Bates, Paul/0000-0001-9192-9963; Neal, Jeffrey/0000-0001-5793-9594; Pappenberger, Florian/0000-0003-1766-2898; Voisin, Nathalie/0000-0002-6848-449X FU Leverhulme Trust Research Project grant; NERC National Centre for Earth Observation (NCEO); Leverhulme Trust Early Career Fellowship scheme; KULTURisk; GLOWASIS; DEWFORA (EC-FP7) projects FX Part of this work was funded by a Leverhulme Trust Research Project grant and part of this work was also carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology, Pasadena, CA, USA under a contract with the National Aeronautics and Space Administration (NASA). G.J.-P.S.'s time at the University of Bristol was funded by a NERC National Centre for Earth Observation (NCEO) small grant and J.C.N. was funded by the Leverhulme Trust Early Career Fellowship scheme. F.P. was supported by the KULTURisk, GLOWASIS, and the DEWFORA (EC-FP7) projects. N.(K.)P.'s work formed part of his M.Sc. Degree awarded at the University of Bristol. NR 63 TC 25 Z9 25 U1 5 U2 47 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD OCT PY 2013 VL 49 IS 10 BP 6248 EP 6257 DI 10.1002/wrcr.20521 PG 10 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 258BI UT WOS:000327432500009 ER PT J AU Harvey, JW Bohlke, JK Voytek, MA Scott, D Tobias, CR AF Harvey, Judson W. Boehlke, J. K. Voytek, Mary A. Scott, Durelle Tobias, Craig R. TI Hyporheic zone denitrification: Controls on effective reaction depth and contribution to whole-stream mass balance SO WATER RESOURCES RESEARCH LA English DT Article DE hyporheic zone; groundwater-surface water interactions; denitrification; nitrogen cycling; biogeochemistry; surface water quality ID TRANSIENT STORAGE; FRESH-WATER; NONSORBING SOLUTES; NITROGEN DYNAMICS; MOUNTAIN STREAM; NITRATE UPTAKE; RICH STREAM; BED FORMS; ECOSYSTEMS; EXCHANGE AB Stream denitrification is thought to be enhanced by hyporheic transport but there is little direct evidence from the field. To investigate at a field site, we injected (NO3-)-N-15, Br (conservative tracer), and SF6 (gas exchange tracer) and compared measured whole-stream denitrification with in situ hyporheic denitrification in shallow and deeper flow paths of contrasting geomorphic units. Hyporheic denitrification accounted for between 1 and 200% of whole-stream denitrification. The reaction rate constant was positively related to hyporheic exchange rate (greater substrate delivery), concentrations of substrates DOC and nitrate, microbial denitrifier abundance (nirS), and measures of granular surface area and presence of anoxic microzones. The dimensionless product of the reaction rate constant and hyporheic residence time, (hzhz) define a Damkohler number, Da(den-hz) that was optimal in the subset of hyporheic flow paths where Da(den-hz) approximate to 1. Optimal conditions exclude inefficient deep pathways where substrates are used up and also exclude inefficient shallow pathways that require repeated hyporheic entries and exits to complete the reaction. The whole-stream reaction significance, R-s (dimensionless), was quantified by multiplying Da(den-hz) by the proportion of stream discharge passing through the hyporheic zone. Together these two dimensionless metrics, one flow-path scale and the other reach-scale, quantify the whole-stream significance of hyporheic denitrification. One consequence is that the effective zone of significant denitrification often differs from the full depth of the hyporheic zone, which is one reason why whole-stream denitrification rates have not previously been explained based on total hyporheic-zone metrics such as hyporheic-zone size or residence time. C1 [Harvey, Judson W.; Boehlke, J. K.] US Geol Survey, Reston, VA 20192 USA. [Voytek, Mary A.] NASA, Astrobiol Inst, Washington, DC 20546 USA. [Scott, Durelle] Virginia Polytech Inst & State Univ, Blacksburg, VA 24061 USA. [Tobias, Craig R.] Univ Connecticut, Dept Marine Sci, Groton, CT 06340 USA. RP Harvey, JW (reprint author), US Geol Survey, Water Resources Discipline, 12201 Sunrise Valley Dr,MS 430, Reston, VA 20192 USA. EM jwharvey@usgs.gov RI Harvey, Judson/L-2047-2013 OI Harvey, Judson/0000-0002-2654-9873 FU USGS HRD; NAWQA Programs; NSF [EAR-0810140, EAR-0814990]; U.S. Department of Agriculture Cooperative State Research, Education and Extension Service (National Research Initiative Competitive Grants Program in Watershed Processes and Water Resources) FX This project was funded by USGS HR&D and NAWQA Programs and by NSF Grants EAR-0810140 and EAR-0814990 and a grant from the U.S. Department of Agriculture Cooperative State Research, Education and Extension Service (National Research Initiative Competitive Grants Program in Watershed Processes and Water Resources). We thank Joel Detty, Mike Doughten, Janet Hannon, Julie Kirstein, Stan Mroczkowski, Jessica Newlin, and Eric Nemeth for assistance in the field and laboratory. Helpful comments on the manuscript were provided by Rich Alexander, Josh Koch, and two anonymous reviewers at WRR. Any use of trade, firm, or product names is for descriptive purposes only and does not imply endorsement by the U.S. Government. NR 77 TC 52 Z9 53 U1 10 U2 85 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD OCT PY 2013 VL 49 IS 10 BP 6298 EP 6316 DI 10.1002/wrcr.20492 PG 19 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 258BI UT WOS:000327432500013 ER PT J AU Guan, B Molotch, NP Waliser, DE Fetzer, EJ Neiman, PJ AF Guan, Bin Molotch, Noah P. Waliser, Duane E. Fetzer, Eric J. Neiman, Paul J. TI The 2010/2011 snow season in California's Sierra Nevada: Role of atmospheric rivers and modes of large-scale variability SO WATER RESOURCES RESEARCH LA English DT Article DE snow water equivalent; Sierra Nevada; atmospheric rivers; Arctic Oscillation; Pacific-North American teleconnection pattern; El Nino; Southern Oscillation ID RIO-GRANDE HEADWATERS; EXTREME PRECIPITATION; GEOPOTENTIAL HEIGHT; ARCTIC OSCILLATION; PACIFIC-OCEAN; WEST-COAST; SATELLITE; IMPACTS; TEMPERATURE; CONNECTION AB The anomalously snowy winter season of 2010/2011 in the Sierra Nevada is analyzed in terms of snow water equivalent (SWE) anomalies and the role of atmospheric rivers (ARs)narrow channels of enhanced meridional water vapor transport between the tropics and extratropics. Mean April 1 SWE was 0.44 m (56%) above normal averaged over 100 snow sensors. AR occurrence was anomalously high during the period, with 20 AR dates during the season and 14 in the month of December 2010, compared to the mean occurrence of nine dates per season. Fifteen out of the 20 AR dates were associated with the negative phases of the Arctic Oscillation (AO) and the Pacific-North American (PNA) teleconnection pattern. Analysis of all winter ARs in California during water years 1998-2011 indicates more ARs occur during the negative phase of AO and PNA, with the increase between positive and negative phases being approximate to 90% for AO, and approximate to 50% for PNA. The circulation pattern associated with concurrent negative phases of AO and PNA, characterized by cyclonic anomalies centered northwest of California, provides a favorable dynamical condition for ARs. The analysis suggests that the massive Sierra Nevada snowpack during the 2010/2011 winter season is primarily related to anomalously high frequency of ARs favored by the joint phasing of -AO and -PNA, and that a secondary contribution is from increased snow accumulation during these ARs favored by colder air temperatures associated with -AO, -PNA, and La Nina. C1 [Guan, Bin; Molotch, Noah P.; Waliser, Duane E.; Fetzer, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Guan, Bin] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. [Molotch, Noah P.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA. [Molotch, Noah P.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. [Neiman, Paul J.] NOAA, Earth Syst Res Lab, Div Phys Sci, Boulder, CO USA. RP Guan, B (reprint author), CALTECH, Jet Prop Lab, MS 233-300,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM bin.guan@jpl.nasa.gov RI Guan, Bin/F-6735-2010; Molotch, Noah/C-8576-2009 FU NASA [NNX08AH18G, NNXIIAK35A]; NSF [EAR1032295]; American Recovery and Reinvestment Act (ARRA) funds; Water Resources Area of the NASA Applied Sciences Program FX This research was supported by NASA grants NNX08AH18G and NNXIIAK35A, NSF grant EAR1032295, and by American Recovery and Reinvestment Act (ARRA) funds. Additional support was provided by the Water Resources Area of the NASA Applied Sciences Program. DEW's, EJF's, and BG's contribution, and part of NPM's contribution, to this study were carried out on behalf of the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 55 TC 27 Z9 27 U1 4 U2 31 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD OCT PY 2013 VL 49 IS 10 BP 6731 EP 6743 DI 10.1002/wrcr.20537 PG 13 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 258BI UT WOS:000327432500042 ER PT J AU Andreadis, KM Schumann, GJP Pavelsky, T AF Andreadis, Konstantinos M. Schumann, Guy J. -P. Pavelsky, Tamlin TI A simple global river bankfull width and depth database SO WATER RESOURCES RESEARCH LA English DT Article DE global rivers; hydraulic geometry ID HYDRAULIC GEOMETRY; DISCHARGE; CHANNEL; DIMENSIONS AB Hydraulic and hydrologic modeling has been moving to larger spatial scales with increased spatial resolution, and such models require a global database of river widths and depths to facilitate accurate river flow routing. Hydraulic geometry relationships have a long history in estimating river channel characteristics as a function of discharge. A simple near-global database of bankfull widths and depths (along with confidence intervals) was developed based on hydraulic geometry equations and the HydroSHEDS hydrography data set. The bankfull width estimates were evaluated with widths derived from Landsat imagery for reaches of nine major rivers, showing errors ranging from 8 to 62% (correlation of 0.88), although it was difficult to verify whether the satellite observations corresponded to bankfull conditions. Bankfull depth estimates were compared with in situ measurements at sites in the Ohio and Willamette rivers, producing a mean error of 24%. The uncertainties in the derivation approach and a number of caveats are identified, and ways to improve the database in the future are discussed. Despite these limitations, this is the first global database that can be used directly in hydraulic models or as a set of constraints in model calibration. C1 [Andreadis, Konstantinos M.; Schumann, Guy J. -P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Pavelsky, Tamlin] Univ N Carolina, Dept Geol Sci, Chapel Hill, NC USA. RP Andreadis, KM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM konstantinos.m.andreadis@jpl.nasa.gov RI Schumann, Guy/F-9760-2011 FU NASA New Investigator Program [NNX12AQ77G]; 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. Tamlin Pavelsky was funded by NASA New Investigator Program grant NNX12AQ77G. NR 26 TC 16 Z9 16 U1 3 U2 23 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD OCT PY 2013 VL 49 IS 10 BP 7164 EP 7168 DI 10.1002/wrcr.20440 PG 5 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 258BI UT WOS:000327432500078 ER PT J AU Lambin, EF Gibbs, HK Ferreira, L Grau, R Mayaux, P Meyfroidt, P Morton, DC Rudel, TK Gasparri, I Munger, J AF Lambin, E. F. Gibbs, H. K. Ferreira, L. Grau, R. Mayaux, P. Meyfroidt, P. Morton, D. C. Rudel, T. K. Gasparri, I. Munger, J. TI Estimating the world's potentially available cropland using a bottom-up approach SO GLOBAL ENVIRONMENTAL CHANGE-HUMAN AND POLICY DIMENSIONS LA English DT Article DE Agro-ecological zone; Land reserve; Land use; Land change; Agriculture; Food security; Degraded lands ID TROPICAL FORESTS; GLOBAL DISTRIBUTION; NORTHERN ARGENTINA; AGRICULTURAL LAND; AMAZON BASIN; TIME-SERIES; CONGO BASIN; DRY FORESTS; DEFORESTATION; CONSERVATION AB Previous estimates of the land area available for future cropland expansion relied on global-scale climate, soil and terrain data. They did not include a range of constraints and tradeoffs associated with land conversion. As a result, estimates of the global land reserve have been high. Here we adjust these estimates for the aforementioned constraints and tradeoffs. We define potentially available cropland as the moderately to highly productive land that could be used in the coming years for rainfed farming, with low to moderate capital investments, and that is not under intact mature forests, legally protected, or already intensively managed. This productive land is underutilized rather than unused as it has ecological or social functions. We also define potentially available cropland that accounts for trade-offs between gains in agricultural production and losses in ecosystem and social services from intensified agriculture, to include only the potentially available cropland that would entail low ecological and social costs with conversion to cropland. In contrast to previous studies, we adopt a "bottom-up" approach by analyzing detailed, fine scale observations with expert knowledge for six countries or regions that are often assumed to include most of potentially available cropland. We conclude first that there is substantially less potential additional cropland than is generally assumed once constraints and trade offs are taken into account, and secondly that converting land is always associated with significant social and ecological costs. Future expansion of agricultural production will encounter a complex landscape of competing demands and tradeoffs. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Lambin, E. F.; Meyfroidt, P.] Catholic Univ Louvain, Georges Lemaitre Ctr Earth & Climate Res, Earth & Life Inst, B-1348 Louvain, Belgium. [Lambin, E. F.] Stanford Univ, Sch Earth Sci, Stanford, CA 94305 USA. [Lambin, E. F.] Stanford Univ, Woods Inst, Stanford, CA 94305 USA. [Gibbs, H. K.; Munger, J.] Univ Wisconsin, Dept Geog, Madison, WI 53726 USA. [Gibbs, H. K.; Munger, J.] Univ Wisconsin, Nelson Inst Environm Studies, Madison, WI 53726 USA. [Ferreira, L.] Univ Fed Goias, Image Proc & GIS Lab, BR-74001970 Goiania, Go, Brazil. [Grau, R.; Gasparri, I.] Univ Nacl Tucuman, CONICET, Inst Ecol Reg, RA-4107 Yerba Buena, Tucuman, Argentina. [Mayaux, P.] Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-21027 Ispra, VA, Italy. [Meyfroidt, P.] FRS FNRS, Brussels, Belgium. [Morton, D. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rudel, T. K.] Rutgers State Univ, Dept Human Ecol, New Brunswick, NJ 08901 USA. [Rudel, T. K.] Rutgers State Univ, Dept Sociol, New Brunswick, NJ 08901 USA. RP Lambin, EF (reprint author), Catholic Univ Louvain, Georges Lemaitre Ctr Earth & Climate Res, Earth & Life Inst, Pl Louis Pasteur 3, B-1348 Louvain, Belgium. EM eric.lambin@uclouvain.be RI Ferreira, Laerte/H-4046-2014; Morton, Douglas/D-5044-2012; Meyfroidt, Patrick/G-7768-2012 OI Meyfroidt, Patrick/0000-0002-1047-9794 FU Francqui Foundation and Academia Belgica in Rome; NSF [CNHS 0709598, 0709645] FX This paper is based on a workshop funded by the Francqui Foundation and Academia Belgica in Rome. Their support is gratefully acknowledged. Matthew Clark and Mitchell Aide provided the land cover shape files generated by NSF Grant CNHS 0709598 and 0709645 for the analysis of Chaco. We are grateful to T. Searchinger and two anonymous reviewers for their critical comments that have contributed to improve this paper. All the inadequacies of this study remain our responsibility. NR 69 TC 69 Z9 69 U1 28 U2 84 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 OCT PY 2013 VL 23 IS 5 SI SI BP 892 EP 901 DI 10.1016/j.gloenvcha.2013.05.005 PG 10 WC Environmental Sciences; Environmental Studies; Geography SC Environmental Sciences & Ecology; Geography GA 268OC UT WOS:000328179400008 ER PT J AU Rapp, JF Draper, DS Mercer, CM AF Rapp, Jennifer F. Draper, David S. Mercer, Cameron M. TI Anhydrous liquid line of descent of Yamato-980459 and evolution of Martian parental magmas SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID PHYRIC SHERGOTTITE YAMATO-980459; HOSTED MELT INCLUSIONS; LARKMAN NUNATAK 06319; MULTICOMPONENT PYROXENES; NAKHLITE METEORITES; MINERAL CHEMISTRY; PHASE-RELATIONS; SNC METEORITES; UPPER-MANTLE; 50 KILOBARS AB We report the results of nominally anhydrous equilibrium and fractional crystallization experiments on a synthetic Yamato-980459 (Y98) bulk composition at 0.5GPa. These experiments allow us to test a suggested fractional crystallization model, calculated using MELTS by Symes etal. (), in which a Y98-like initial liquid yielded a magma closely resembling the bulk composition of QUE 94201. Although the two meteorites cannot be cogenetic owing to their age difference, they are thought to represent bona fide magmatic liquids rather than products of crystal accumulation, as are most Martian basaltic meteorites. Hence, understanding possible petrogenetic links between these types of liquids could be revealing about processes of melting and crystallization that formed the range of Martian basalts. We find that Y98 can, in fact, generate a residual liquid closely resembling QUE, but only after a very different crystallization process, and different degree of crystallization, than that modeled using MELTS. In addition, both the identity and sequence of crystallizing phases are very different between model and experiments. Our fractional crystallization experiments do not produce a QUE-like liquid, and the crystallizing phases are an even poorer match to the MELTS-calculated compositions than in the equilibrium runs. However, residual liquids from our experiments define a liquid line of descent that encompasses bulk compositions of parental melts calculated for several Martian basaltic meteorites, suggesting that the known Martian basaltic meteorites had their ultimate origin from the same or very similar source lithologies. These are, in turn, similar to source rocks modeled by previous studies as products of extensive crystallization of an initial Martian magma ocean. C1 [Rapp, Jennifer F.; Draper, David S.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Astromat Res Off, Houston, TX 77058 USA. [Rapp, Jennifer F.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Mercer, Cameron M.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. RP Rapp, JF (reprint author), NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Astromat Res Off, 2101 NASA Pkwy,Code KR111, Houston, TX 77058 USA. EM jennifer.f.rapp@nasa.gov OI Mercer, Cameron/0000-0003-0534-848X FU NASA [COS11-0052] FX We wish to thank J. Balta, G. J. Taylor, S. Symes, and the associate editor G. Benedix for their thoughtful and constructive reviews. This work was supported by NASA Cosmochemistry grant COS11-0052 to DSD. This is LPI contribution 1740. NR 72 TC 5 Z9 5 U1 0 U2 7 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 OCT PY 2013 VL 48 IS 10 BP 1780 EP 1799 DI 10.1111/maps.12197 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 268DY UT WOS:000328150100002 ER PT J AU Rietmeijer, FJM Nuth, JA Pun, A AF Rietmeijer, Frans J. M. Nuth, Joseph A. Pun, Aurora TI The formation of Mg,Fe-silicates by reactions between amorphous magnesiosilica smoke particles and metallic iron nanograins with implications for comet silicate origins SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID INTERPLANETARY DUST PARTICLE; HERBIG AE/BE STARS; MAGNESIUM-SILICATE; PHASE EQUILIBRIA; HALLEY DUST; 81P/WILD 2; CONDENSATION; GRAINS; EVOLUTION; CIRCUMSTELLAR AB This thermal annealing experiment at 1000K for up to 167h used a physical mixture of vapor phase-condensed magnesiosilica grains and metallic iron nanograins to test the hypothesis that a mixture of magnesiosilica grains and an Fe-source would lead to the formation of ferromagnesiosilica grains. This exploratory study found that coagulation and thermal annealing of amorphous magnesiosilica and metallic grains yielded ferromagnesiosilica grains with the Fe/(Fe+Mg) ratios in interplanetary dust particles. Furthermore, decomposition of brucite present in the condensed magnesiosilica grains was the source for water and the cause of different iron oxidation states, and the formation of amorphous Fe3+-ferrosilica, amorphous Fe3+-Mg, Fe-silicates, and magnesioferrite during thermal annealing. Fayalite and ferrosilite that formed from silica/FeO melts reacted with forsterite and enstatite to form Mg, Fe-silicates. The presence of iron in different oxidation states in extraterrestrial materials almost certainly requires active asteroid-like parent bodies. If so, the possible presence of trivalent Fe compounds in comet P/Halley suggests that Halley-type comets are a mixture of preserved presolar and processed solar nebula dust. The results from this thermal annealing experiment further suggest that the Fe-silicates detected in the impact-induced ejecta from comet 9P/Temple 1 might be of secondary origin and related to the impact experiment or to processing in a regolith. C1 [Rietmeijer, Frans J. M.; Pun, Aurora] 1 Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [Nuth, Joseph A.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. RP Rietmeijer, FJM (reprint author), 1 Univ New Mexico, Dept Earth & Planetary Sci, MSC3-2040, Albuquerque, NM 87131 USA. EM fransjmr@unm.edu FU NASA LARS Program [NNX11AC36G]; Exobiology program; NASA [NAGW-3646]; NNX10AK28G FX We are most grateful to George Flynn and Hugh Hill for their excellent reviews. FJMR was supported by grant NNX11AC36G through the NASA LARS Program and Cosmochemistry grant NNX10AK28G (PI: J.A. Nuth). JN also acknowledges support from the Exobiology program. Guofei Fu collected the data as partial fulfillment of his (unfinished) PhD thesis program at UNM where he was supported by NASA grant NAGW-3646. NR 66 TC 1 Z9 1 U1 1 U2 4 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 OCT PY 2013 VL 48 IS 10 BP 1823 EP 1840 DI 10.1111/maps.12194 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 268DY UT WOS:000328150100004 ER PT J AU Ade, PAR Aghanim, N Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Balbi, A Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Bernard, JP Bersanelli, M Bhatia, R Bikmaev, I Bobin, J Bohringer, H Bonaldi, A Bond, JR Borgani, S Borrill, J Bouchet, FR Bourdin, H Brown, ML Burenin, R Burigana, C Cabella, P Cardoso, JF Carvalho, P Castex, G Catalano, A Cayon, L Chamballu, A Chiang, LY Chon, G Christensen, PR Churazov, E Clements, DL Colafrancesco, S Colombi, S Colombo, LPL Comis, B Coulais, A Crill, BP Cuttaia, F Da Silva, A Dahle, H Danese, L Davis, RJ de Bernardis, P de Gasperis, G de Zotti, G Delabrouille, J Democles, J Desert, FX Diego, JM Dolag, K Dole, H Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Flores-Cacho, I Forni, O Fosalba, P Frailis, M Franceschi, E Frommert, M Galeotta, S Ganga, K Genova-Santos, RT Giard, M Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gregorio, A Gruppuso, A Hansen, FK Harrison, D Hempel, A Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hurier, G Jaffe, TR Jaffe, AH Jagemann, T Jones, WC Juvela, M Keihanen, E Khamitov, I Kisner, TS Kneissl, R Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Lawrence, CR Le Jeune, M Leonardi, R Liddle, A Lilje, PB Lopez-Caniego, M Luzzi, G Macias-Perez, JF Maino, D Mandolesi, N Maris, M Marleau, F Marshall, DJ Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Mazzotta, P Mei, S Melchiorri, A Melin, JB Mendes, L Mennella, A Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S Pajot, F Paoletti, D Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Piffaretti, R Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prunet, S Puget, JL Rachen, JP Reach, WT Rebolo, R Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Roman, M Rosset, C Rossetti, M Rubino-Martin, JA Rusholme, B Sandri, M Savini, G Scott, D Smoot, GF Starck, JL Sudiwala, R Sunyaev, R Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tuovinen, J Valenziano, L Van Tent, B Varis, J Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Welikala, N White, SDM White, M Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Balbi, A. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Bernard, J-P. Bersanelli, M. Bhatia, R. Bikmaev, I. Bobin, J. Boehringer, H. Bonaldi, A. Bond, J. R. Borgani, S. Borrill, J. Bouchet, F. R. Bourdin, H. Brown, M. L. Burenin, R. Burigana, C. Cabella, P. Cardoso, J. -F. Carvalho, P. Castex, G. Catalano, A. Cayon, L. Chamballu, A. Chiang, L. -Y Chon, G. Christensen, P. R. Churazov, E. Clements, D. L. Colafrancesco, S. Colombi, S. Colombo, L. P. L. Comis, B. Coulais, A. Crill, B. P. Cuttaia, F. Da Silva, A. Dahle, H. Danese, L. Davis, R. J. de Bernardis, P. de Gasperis, G. de Zotti, G. Delabrouille, J. Democles, J. Desert, F. -X. Diego, J. M. Dolag, K. Dole, H. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Flores-Cacho, I. Forni, O. Fosalba, P. Frailis, M. Franceschi, E. Frommert, M. Galeotta, S. Ganga, K. Genova-Santos, R. T. Giard, M. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gregorio, A. Gruppuso, A. Hansen, F. K. Harrison, D. Hempel, A. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hurier, G. Jaffe, T. R. Jaffe, A. H. Jagemann, T. Jones, W. C. Juvela, M. Keihanen, E. Khamitov, I. Kisner, T. S. Kneissl, R. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Lawrence, C. R. Le Jeune, M. Leonardi, R. Liddle, A. Lilje, P. B. Lopez-Caniego, M. Luzzi, G. Macias-Perez, J. F. Maino, D. Mandolesi, N. Maris, M. Marleau, F. Marshall, D. J. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Mazzotta, P. Mei, S. Melchiorri, A. Melin, J. -B. Mendes, L. Mennella, A. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Osborne, S. Pajot, F. Paoletti, D. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Piffaretti, R. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prunet, S. Puget, J. -L. Rachen, J. P. Reach, W. T. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Roman, M. Rosset, C. Rossetti, M. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Savini, G. Scott, D. Smoot, G. F. Starck, J. -L. Sudiwala, R. Sunyaev, R. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Tuovinen, J. Valenziano, L. Van Tent, B. Varis, J. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Welikala, N. White, S. D. M. White, M. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck intermediate results V. Pressure profiles of galaxy clusters from the Sunyaev-Zeldovich effect (vol 550, A131, 2013) SO ASTRONOMY & ASTROPHYSICS LA English DT Correction DE cosmology: observations; galaxies: clusters: general; galaxies: clusters: intracluster medium; submillimeter: general; X-rays: general; errata, addenda C1 [Bartlett, J. G.; Cardoso, J. -F.; Castex, G.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Le Jeune, M.; Patanchon, G.; Piat, M.; Remazeilles, M.; Roman, M.; Rosset, C.; Smoot, G. F.] Univ Paris Diderot, APC, CNRS IN2P3, CEA Irfu,Observ Paris,Sorbonne Paris Cite, F-75205 Paris 13, France. [Lahteenmaki, A.; Poutanen, T.] Aalto Univ Metsahovi Radio Observ, Kylmala 02540, Finland. [Bikmaev, I.] Acad Sci Tatarstan, Kazan 420111, Republic Of Tat, Russia. [Natoli, P.; Polenta, G.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, I-00044 Frascati, Italy. [Mandolesi, N.] Agenzia Spaziale Italiana, I-00198 Rome, Italy. [Ashdown, M.; Carvalho, P.; Hobson, M.; Lasenby, A.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Bhatia, R.; Kneissl, R.] Atacama Large Millimeter Submillimeter Array, ALMA Santiago Cent Off, Santiago, Chile. [Bond, J. R.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J-P.; Flores-Cacho, I.; Forni, O.; Giard, M.; Jaffe, T. R.; Marshall, D. J.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] IRAP, CNRS, F-31028 Toulouse 4, France. [Dore, O.; Hildebrandt, S. R.; Mei, S.; Rocha, G.] CALTECH, Pasadena, CA 91125 USA. [Dahle, H.; Lilje, P. B.] Univ Oslo, Ctr Math Applicat, N-0317 Oslo, Norway. [Da Silva, A.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Hernandez-Monteagudo, C.] CEFCA, Teruel 44001, Spain. [Borrill, J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Rebolo, R.] CSIC, Madrid, Spain. [Melin, J. -B.; Piffaretti, R.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. [Norgaard-Nielsen, H. U.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Frommert, M.; Kunz, M.] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland. [Atrio-Barandela, F.] Univ Salamanca, Fac Ciencias, Dept Fis Fundamental, E-37008 Salamanca, Spain. [Toffolatti, L.] Univ Oviedo, Dept Fis, Oviedo 3307, Spain. [Bikmaev, I.] Kazan Fed Univ, Dept Astron & Geodesy, Kazan 420008, Russia. [Rachen, J. P.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Colombo, L. P. L.; Pierpaoli, E.] Univ So Calif, Dana & David Dornsife Coll Letter Arts & Sci, Dept Phys & Astron, Los Angeles, CA 90089 USA. [Liddle, A.] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Juvela, M.; Keihanen, E.; Kurki-Suonio, H.; Poutanen, T.; Suur-Uski, A. -S.] Univ Helsinki, Dept Phys, Helsinki 00014, Finland. [Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Smoot, G. F.; White, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA. [Cayon, L.] Purdue Univ, Dept Stat, W Lafayette, IN 47907 USA. [Matarrese, S.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Nati, F.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Bersanelli, M.; Maino, D.; Mennella, A.; Rossetti, M.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy. [Borgani, S.; Gregorio, A.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Burigana, C.; Natoli, P.] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy. [Balbi, A.; Bourdin, H.; de Gasperis, G.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Cabella, P.] Univ Roma Tor Vergata, Dipartimento Matemat, I-00133 Rome, Italy. [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark. [Hempel, A.; Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain. [Kneissl, R.] ESO Vitacura, European So Observ, Santiago, Chile. [Dupac, X.; Jagemann, T.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain. [Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands. [Mei, S.] Observ Paris, GEPI, Sect Meudon, F-92195 Meudon, France. [Kurki-Suonio, H.; Lahteenmaki, A.; Poutanen, T.; Suur-Uski, A. -S.] Univ Helsinki, Helsinki Inst Phys, FIN-00014 Helsinki, Finland. 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H.; Mortlock, D.; Novikov, D.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, F-38042 Grenoble, France. [Dole, H.] Inst Univ France, F-75005 Paris, France. [Aghanim, N.; Aumont, J.; Dole, H.; Douspis, M.; Kunz, M.; Lagache, G.; Miville-Deschenes, M. -A.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Remazeilles, M.; Welikala, N.] Univ Paris 11, CNRS, UMR8617, Inst Astrophys Spatiale, F-91405 Orsay, France. [Benabed, K.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] Inst Astrophys Paris, CNRS UMR7095, F-75014 Paris, France. [Fosalba, P.] Fac Ciencies, CSIC IEEC, Inst Ciencies Espai, Bellaterra 08193, Spain. [Popa, L.] Inst Space Sci, Bucharest 077125, Romania. [Marleau, F.] Univ Innsbruck, Inst Astro & Particle Phys, A-6020 Innsbruck, Austria. [Chiang, L. -Y] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Efstathiou, G.; Harrison, D.; Sutton, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Dahle, H.; Eriksen, H. K.; Hansen, F. K.; Lilje, P. B.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Genova-Santos, R. T.; Hempel, A.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife 38200, Spain. [Barreiro, R. B.; Diego, J. M.; Gonzalez-Nuevo, J.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Toffolatti, L.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain. [Bartlett, J. G.; Colombo, L. P. L.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Lawrence, C. R.; Mitra, S.; Rocha, G.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Bonaldi, A.; Brown, M. L.; Davis, R. J.; Noviello, F.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Harrison, D.; Lasenby, A.; Sutton, D.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Henrot-Versille, S.; Luzzi, G.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, CNRS IN2P3, LAL, F-91898 Orsay, France. [Catalano, A.; Coulais, A.; Lamarre, J. -M.] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Arnaud, M.; Bobin, J.; Democles, J.; Piffaretti, R.; Pratt, G. W.; Starck, J. -L.] Univ Paris Diderot, CNRS, CEA DSM, IRFU,Serv Astrophys,Lab AIM,CEA Saclay, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS UMR 5141, Lab Traitement & Commun Informat, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France. [Catalano, A.; Comis, B.; Hurier, G.; Macias-Perez, J. F.; Perotto, L.; Renault, C.] Univ Grenoble 1, Lab Phys Subat & Cosmol, CNRS IN2P3, Inst Natl Polytech Grenoble, F-38026 St Martin Dheres, France. [Van Tent, B.] Univ Paris 11, Phys Theor Lab, F-91405 Orsay, France. [Van Tent, B.] CNRS, F-91405 Orsay, France. [Kisner, T. S.; Smoot, G. F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Churazov, E.; Dolag, K.; Doerl, U.; Ensslin, T. A.; Hernandez-Monteagudo, C.; Knoche, J.; Rachen, J. P.; Reinecke, M.; Riller, T.; Sunyaev, R.; White, S. D. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Boehringer, H.; Chon, G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Tuovinen, J.; Varis, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo 02044, Finland. [Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Crill, B. P.] CALTECH, Pasadena, CA 91125 USA. [Savini, G.] UCL, Opt Sci Lab, London, England. [Baccigalupi, C.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Ade, P. A. R.; Munshi, D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Burenin, R.] Space Res Inst IKI, Moscow 117997, Russia. [Churazov, E.; Sunyaev, R.] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Khamitov, I.] TUBITAK Natl Observ, TR-07058 Antalya, Turkey. [Benabed, K.; Bouchet, F. R.; Colombi, S.; Hivon, E.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UMR 7095, F-75014 Paris, France. [Mei, S.] Univ Paris 07, F-75205 Paris 13, France. [Banday, A. J.; Flores-Cacho, I.; Forni, O.; Giard, M.; Jaffe, T. R.; Marshall, D. J.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Dolag, K.] Univ Munich, Univ Observ, D-81679 Munich, Germany. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Pointecouteau, E (reprint author), Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. EM etienne.pointecouteau@irap.omp.eu RI Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Fosalba Vela, Pablo/I-5515-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Novikov, Dmitry/P-1807-2015; Bouchet, Francois/B-5202-2014; Lahteenmaki, Anne/L-5987-2013; Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Lopez-Caniego, Marcos/M-4695-2013; Bobin, Jerome/P-3729-2014; Battaner, Eduardo/P-7019-2014; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Churazov, Eugene/A-7783-2013; White, Martin/I-3880-2015; Gruppuso, Alessandro/N-5592-2015 OI Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; Bobin, Jerome/0000-0003-1457-7890; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; White, Martin/0000-0001-9912-5070; Gruppuso, Alessandro/0000-0001-9272-5292 NR 7 TC 1 Z9 1 U1 2 U2 22 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2013 VL 558 AR C2 DI 10.1051/0004-6361/201220040e PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000151 ER PT J AU Biviano, A Rosati, P Balestra, I Mercurio, A Girardi, M Nonino, M Grillo, C Scodeggio, M Lemze, D Kelson, D Umetsu, K Postman, M Zitrin, A Czoske, O Ettori, S Fritz, A Lombardi, M Maier, C Medezinski, E Mei, S Presotto, V Strazzullo, V Tozzi, P Ziegler, B Annunziatella, M Bartelmann, M Benitez, N Bradley, L Brescia, M Broadhurst, T Coe, D Demarco, R Donahue, M Ford, H Gobat, R Graves, G Koekemoer, A Kuchner, U Melchior, P Meneghetti, M Merten, J Moustakas, L Munari, E Regos, E Sartoris, B Seitz, S Zheng, W AF Biviano, A. Rosati, P. Balestra, I. Mercurio, A. Girardi, M. Nonino, M. Grillo, C. Scodeggio, M. Lemze, D. Kelson, D. Umetsu, K. Postman, M. Zitrin, A. Czoske, O. Ettori, S. Fritz, A. Lombardi, M. Maier, C. Medezinski, E. Mei, S. Presotto, V. Strazzullo, V. Tozzi, P. Ziegler, B. Annunziatella, M. Bartelmann, M. Benitez, N. Bradley, L. Brescia, M. Broadhurst, T. Coe, D. Demarco, R. Donahue, M. Ford, H. Gobat, R. Graves, G. Koekemoer, A. Kuchner, U. Melchior, P. Meneghetti, M. Merten, J. Moustakas, L. Munari, E. Regos, E. Sartoris, B. Seitz, S. Zheng, W. TI CLASH-VLT: The mass, velocity-anisotropy, and pseudo-phase-space density profiles of the z=0.44 galaxy cluster MACS J1206.2-0847 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: individual: MACS J1206-0847; galaxies: kinematics and dynamics; galaxies: evolution; dark matter ID DARK-MATTER HALOS; STRONG-LENSING ANALYSIS; REGION NEARBY SURVEY; DIGITAL SKY SURVEY; EQUATION-OF-STATE; X-RAY; COMA CLUSTER; RICH CLUSTERS; REDSHIFT SURVEY; INFALL REGION AB Aims: We constrain the mass, velocity-anisotropy, and pseudo-phase-space density profiles of the z = 0.44 CLASH cluster MACS J1206.2-0847, using the projected phase-space distribution of cluster galaxies in combination with gravitational lensing. Methods: We use an unprecedented data-set of similar or equal to 600 redshifts for cluster members, obtained as part of a VLT/VIMOS large program, to constrain the cluster mass profile over the radial range similar to 0-5 Mpc (0-2.5 virial radii) using the MAMPOSSt and Caustic methods. We then add external constraints from our previous gravitational lensing analysis. We invert the Jeans equation to obtain the velocity-anisotropy profiles of cluster members. With the mass-density and velocity-anisotropy profiles we then obtain the first determination of a cluster pseudo-phase-space density profile. Results: The kinematics and lensing determinations of the cluster mass profile are in excellent agreement. This is very well fitted by a NFW model with mass M-200 = (1.4 +/- 0.2) x 10(15) M-circle dot and concentration c(200) = 6 +/- 1, only slightly higher than theoretical expectations. Other mass profile models also provide acceptable fits to our data, of (slightly) lower (Burkert, Hernquist, and Softened Isothermal Sphere) or comparable (Einasto) quality than NFW. The velocity-anisotropy profiles of the passive and star- forming cluster members are similar, close to isotropic near the center and increasingly radial outside. Passive cluster members follow extremely well the theoretical expectations for the pseudo-phase-space density profile and the relation between the slope of the mass-density profile and the velocity anisotropy. Star-forming cluster members show marginal deviations from theoretical expectations. Conclusions: This is the most accurate determination of a cluster mass profile out to a radius of 5 Mpc, and the only determination of the velocity-anisotropy and pseudo-phase-space density profiles of both passive and star-forming galaxies for an individual cluster. These profiles provide constraints on the dynamical history of the cluster and its galaxies. Prospects for extending this analysis to a larger cluster sample are discussed. C1 [Biviano, A.; Balestra, I.; Girardi, M.; Nonino, M.; Annunziatella, M.; Munari, E.] INAF Osservatorio Astron Trieste, I-34131 Trieste, Italy. [Rosati, P.] ESO, D-85748 Garching, Germany. [Balestra, I.; Mercurio, A.; Brescia, M.] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy. [Girardi, M.; Presotto, V.; Annunziatella, M.; Munari, E.; Sartoris, B.] Univ Trieste, Dipartimento Fis, I-34143 Trieste, Italy. [Grillo, C.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Scodeggio, M.; Fritz, A.] INAF IASF Milano, I-20133 Milan, Italy. [Lemze, D.; Ford, H.; Zheng, W.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Kelson, D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Postman, M.; Bradley, L.; Coe, D.; Koekemoer, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Zitrin, A.; Bartelmann, M.] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, D-69120 Heidelberg, Germany. [Czoske, O.; Maier, C.; Ziegler, B.; Kuchner, U.] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Ettori, S.; Meneghetti, M.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Ettori, S.; Meneghetti, M.] INFN, Sez Bologna, I-40127 Bologna, Italy. [Lombardi, M.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy. [Medezinski, E.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Mei, S.] Observ Paris, GEPI, F-75014 Paris, France. [Mei, S.] Univ Paris 07, F-75205 Paris, France. [Strazzullo, V.] CEA Saclay, F-91191 Gif Sur Yvette, France. [Tozzi, P.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Benitez, N.] Inst Astrofis Andalucia CSIC, Granada 18008, Spain. [Broadhurst, T.] Univ Basque Country, Dept Theoret Phys, Bilbao 48080, Spain. [Demarco, R.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Gobat, R.] Univ Paris Diderot, Lab AIM Paris Saclay, CEA DSM CNRS, Irfu,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Graves, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Graves, G.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Melchior, P.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Merten, J.; Moustakas, L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Regos, E.] European Lab Particle Phys CERN, CH-1211 Geneva 23, Switzerland. [Seitz, S.] Univ Observ Munich, D-81679 Munich, Germany. [Seitz, S.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. RP Biviano, A (reprint author), INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34131 Trieste, Italy. EM biviano@oats.inaf.it RI Bartelmann, Matthias/A-5336-2014; Grillo, Claudio/E-6223-2015; Ettori, Stefano/N-5004-2015; Meneghetti, Massimo/O-8139-2015; OI Biviano, Andrea/0000-0002-0857-0732; LOMBARDI, MARCO/0000-0002-3336-4965; Moustakas, Leonidas/0000-0003-3030-2360; Koekemoer, Anton/0000-0002-6610-2048; Benitez, Narciso/0000-0002-0403-7455; Tozzi, Paolo/0000-0003-3096-9966; Umetsu, Keiichi/0000-0002-7196-4822; Grillo, Claudio/0000-0002-5926-7143; Ettori, Stefano/0000-0003-4117-8617; Meneghetti, Massimo/0000-0003-1225-7084; Nonino, Mario/0000-0001-6342-9662; Balestra, Italo/0000-0001-9660-894X; Scodeggio, Marco/0000-0002-2282-5850; Brescia, Massimo/0000-0001-9506-5680; Maier, Christian/0000-0001-6405-2182 FU BASAL Center for Astrophysics and Associated Technologies (CATA); FONDECYT [1130528]; PRIN INAF: "Architecture and Tomography of Galaxy Clusters" FX We wish to thank Colin Norman for originally suggesting one of us (AB) to determine the pseudo-phase-space density profiles. We also thank Stefano Borgani, Gary Mamon, Giuseppe Murante, Tommaso Treu, and the referee, Elmo Tempel, for useful suggestions and discussions, and Hans Bohringer for providing phase 2 information on his VIMOS programme (169.A-0595) also used in this study. This research is partly supported by the PRIN INAF 2010: "Architecture and Tomography of Galaxy Clusters". P.R. and I.B. acknowledge partial support by the DFG cluster of excellence Origin and Structure of the Universe (http://www.universe-cluster.de). R.D. gratefully acknowledges the support provided by the BASAL Center for Astrophysics and Associated Technologies (CATA), and by FONDECYT grant N. 1130528. NR 217 TC 42 Z9 42 U1 1 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2013 VL 558 AR A1 DI 10.1051/0004-6361/201321955 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000001 ER PT J AU Boley, PA Linz, H van Boekel, R Henning, T Feldt, M Kaper, L Leinert, C Muller, A Pascucci, I Robberto, M Stecklum, B Waters, LBFM Zinnecker, H AF Boley, Paul A. Linz, Hendrik van Boekel, Roy Henning, Thomas Feldt, Markus Kaper, Lex Leinert, Christoph Mueller, Andre Pascucci, Ilaria Robberto, Massimo Stecklum, Bringfried Waters, L. B. F. M. Zinnecker, Hans TI The VLTI/MIDI survey of massive young stellar objects Sounding the inner regions around intermediate- and high-mass young stars using mid-infrared interferometry SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE surveys; stars: massive; techniques: interferometric ID ULTRACOMPACT HII-REGIONS; HERBIG-AE/BE STARS; SOUTHERN GALACTIC PLANE; INTERSTELLAR SILICATE MINERALOGY; INFRARED IMAGING POLARIMETRY; DISTRIBUTED METHANOL MASERS; H II REGIONS; HIGH-RESOLUTION; MONOCEROS R2; ORION-NEBULA AB Context. Because of inherent difficulties involved in observations and numerical simulations of the formation of massive stars, an understanding of the early evolutionary phases of these objects remains elusive. In particular, observationally probing circumstellar material at distances less than or similar to 100 AU from the central star is exceedingly difficult, as such objects are rare (and thus, on average, far away) and typically deeply embedded. Long-baseline mid-infrared interferometry provides one way of obtaining the necessary spatial resolution at appropriate wavelengths for studying this class of objects; however, interpreting such observations is often difficult due to sparse spatial-frequency coverage. Aims. We aim to characterize the distribution and composition of circumstellar material around young massive stars and to investigate exactly which physical structures in these objects are probed by long-baseline mid-infrared interferometric observations. Methods. We used the two-telescope interferometric instrument MIDI of the Very Large Telescope Interferometer of the European Southern Observatory to observe a sample of 24 intermediate-and high-mass young stellar objects in the N band (8-13 mu m). We had successful fringe detections for 20 objects and present spectrally-resolved correlated fluxes and visibility levels for projected baselines of up to 128 m. We fit the visibilities with geometric models to derive the sizes of the emitting regions, as well as the orientation and elongation of the circumstellar material. Fourteen objects in the sample show the 10 mu m silicate feature in absorption in the total and correlated flux spectra. For 13 of these objects, we were able to fit the correlated flux spectra with a simple absorption model, allowing us to constrain the composition and absorptive properties of the circumstellar material. Results. Nearly all of the massive young stellar objects observed show significant deviations from spherical symmetry at mid-infrared wavelengths. In general, the mid-infrared emission can trace both disks and outflows, and in many cases it may be difficult to disentangle these components on the basis of interferometric data alone, because of the sparse spatial frequency coverage normally provided by current long-baseline interferometers. For the majority of the objects in this sample, the absorption occurs on spatial scales larger than those probed by MIDI. Finally, the physical extent of the mid-infrared emission around these sources is correlated with the total luminosity, albeit with significant scatter. Conclusions. Circumstellar material is ubiquitous at distances less than or similar to 100 AU around young massive stars. Long-baseline mid-infrared interferometry provides the resolving power necessary for observing this material directly. However, in particular for deeply-embedded sources, caution must be used when attempting to attribute mid-infrared emission to specific physical structures, such as a circumstellar disk or an outflow. C1 [Boley, Paul A.; Linz, Hendrik; van Boekel, Roy; Henning, Thomas; Feldt, Markus; Leinert, Christoph] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Boley, Paul A.] Max Planck Inst Radio Astron, D-53121 Bonn, Germany. [Kaper, Lex; Waters, L. B. F. M.] Astron Inst Anton Pannekoek, NL-1098 XE Amsterdam, Netherlands. [Mueller, Andre] European So Observ, Santiago 19, Chile. [Pascucci, Ilaria] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Robberto, Massimo] Space Telescope Sci Inst, Baltimore, MD 21212 USA. [Stecklum, Bringfried] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Waters, L. B. F. M.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Zinnecker, Hans] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. RP Boley, PA (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM boley@mpia.de NR 131 TC 13 Z9 13 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2013 VL 558 AR UNSP A24 DI 10.1051/0004-6361/201321539 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000024 ER PT J AU Hurier, G Macias-Perez, JF Hildebrandt, S AF Hurier, G. Macias-Perez, J. F. Hildebrandt, S. TI MILCA, a modified internal linear combination algorithm to extract astrophysical emissions from multifrequency sky maps SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: data analysis; techniques: image processing; cosmic background radiation ID MICROWAVE BACKGROUND OBSERVATIONS; PROBE WMAP OBSERVATIONS; COMPONENT SEPARATION; POWER SPECTRUM; CMB; FREQUENCIES; FOREGROUNDS; TEMPLATE; FASTICA; CATALOG AB This analysis of current cosmic microwave background (CMB) experiments is based on the interpretation of multifrequency sky maps in terms of different astrophysical components and it requires specifically tailored, component separation algorithms. In this context, internal linear combination (ILC) methods have been extensively used to extract the CMB emission from the WMAP multifrequency data. We present here a modified internal linear component algorithm (MILCA) that generalizes the ILC approach to the case of multiple astrophysical components for which the electromagnetic spectrum is known. In addition, MILCA corrects for the intrinsic noise bias in the standard ILC approach and extends it to a hybrid space-frequency representation of the data. It also allows us to use external templates to minimize the contribution of extra components but still using only a linear combination of the input data. We applied MILCA to simulations of the Planck satellite data at the frequency bands from 100 GHz to 857 GHz. We explore the possibility of reconstructing the Galactic molecular CO emission and the thermal Sunyaev-Zeldovich effect from the Planck maps. We conclude that MILCA is able to accurately estimate those emissions, and it has been successfully used for this purpose within the Planck collaboration. C1 [Hurier, G.; Macias-Perez, J. F.; Hildebrandt, S.] Univ Grenoble 1, Lab Phys Subatom & Cosmol, CNRS IN2P3, Inst Natl Polytech Grenoble, F-38026 Grenoble, France. [Hurier, G.] Univ Paris 11, CNRS UMR8617, Inst Astrophys Spatiale, F-91405 Orsay, France. [Hildebrandt, S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Hurier, G (reprint author), Univ Grenoble 1, Lab Phys Subatom & Cosmol, CNRS IN2P3, Inst Natl Polytech Grenoble, 53 Rue Martyrs, F-38026 Grenoble, France. EM ghurier@ias.u-psud.fr OI Hurier, Guillaume/0000-0002-1215-0706 NR 56 TC 28 Z9 28 U1 0 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2013 VL 558 AR A118 DI 10.1051/0004-6361/201321891 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000118 ER PT J AU Kuzmychov, O Berdyugina, SV AF Kuzmychov, O. Berdyugina, S. V. TI Paschen-Back effect in the CrH molecule and its application for magnetic field measurements on stars, brown dwarfs, and hot exoplanets SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE brown dwarfs; stars: magnetic field; stars: atmospheres; polarization; radiative transfer ID THEORETICAL SPECTRAL PATTERNS; ZEEMAN REGIME; STELLAR; SOLAR; ATMOSPHERES; DIAGNOSTICS; SYSTEM AB Aims. We investigated the Paschen-Back effect in the (0,0) band of the A(6)Sigma(+)-X-6 Sigma(+) system of the CrH molecule, and we examined its potential for estimating magnetic fields on stars and substellar objects, such as brown dwarfs and hot exoplanets. Methods. We carried out quantum mechanical calculations to obtain the energy level structure of the electronic-vibrational-rotational states considered both in the absence and in the presence of a magnetic field. Level mixing due to magnetic field perturbation (the Paschen-Back effect) was consistently taken into account. Then, we calculated frequencies and strengths of transitions between magnetic sublevels. Employing these results and solving numerically a set of the radiative transfer equations for polarized radiation, we calculated Stokes parameters for both the individual lines and the (0, 0) band depending on the strength and orientation of the magnetic field. Results. We demonstrate that magnetic splitting of the individual CrH lines shows a significant asymmetry due to the Paschen-Back effect already at 1 G field. This leads to a considerable signal in both circular and linear polarization, up to 30% at the magnetic field strength of >= 3 kG in early L dwarfs. The polarization does not cancel out completely even at very low spectral resolution and is seen as broad-band polarization of a few percent. Since the line asymmetry depends only on the magnetic field strength and not on the filling factor, CrH lines provide a very sensitive tool for direct measurement of the stellar magnetic fields on faint cool objects, such as brown dwarfs and hot Jupiters, observed with low spectral resolution. C1 [Kuzmychov, O.; Berdyugina, S. V.] Kiepenheuer Inst Sonnenphys, D-79104 Freiburg, Germany. [Berdyugina, S. V.] Univ Hawaii, NASA Astrobiol Inst, Honolulu, HI 96822 USA. RP Kuzmychov, O (reprint author), Kiepenheuer Inst Sonnenphys, Schoneckstr 6, D-79104 Freiburg, Germany. EM oleksii.kuzmychov@kis.uni-freiburg.de; sveta@kis.uni-freiburg.de FU Leibniz Association [SAW-2011-KIS-7]; ERC Advanced Grant HotMol; NASA Astrobiology Institute FX We are grateful to P. Bernath for his helpful advice on the calculation of the rotational structure of the CrH. We thank Ch. Helling and S. Witte for providing us with the Drift-Phoenix model atmospheres and the corresponding dust properties. This work was supported by the grant of the Leibniz Association SAW-2011-KIS-7, ERC Advanced Grant HotMol, and the NASA Astrobiology Institute. NR 26 TC 6 Z9 6 U1 0 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2013 VL 558 AR A120 DI 10.1051/0004-6361/201220041 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000120 ER PT J AU Magdis, GE Rigopoulou, D Helou, G Farrah, D Hurley, P Alonso-Herrero, A Bock, J Burgarella, D Chapman, S Charmandaris, V Cooray, A Dai, YS Dale, D Elbaz, D Feltre, A Hatziminaoglou, E Huang, JS Morrison, G Oliver, S Page, M Scott, D Shi, Y AF Magdis, G. E. Rigopoulou, D. Helou, G. Farrah, D. Hurley, P. Alonso-Herrero, A. Bock, J. Burgarella, D. Chapman, S. Charmandaris, V. Cooray, A. Dai, Y. Sophia Dale, D. Elbaz, D. Feltre, A. Hatziminaoglou, E. Huang, J. -S. Morrison, G. Oliver, S. Page, M. Scott, D. Shi, Y. TI Mid- to far-infrared properties of star-forming galaxies and active galactic nuclei SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: evolution; galaxies: active; galaxies: starburst; galaxies: star formation; infrared: galaxies ID SPITZER-SPACE-TELESCOPE; SPECTRAL ENERGY-DISTRIBUTIONS; POLYCYCLIC AROMATIC-HYDROCARBONS; NEED ULTRAVIOLET EXCITATION; PALOMAR-GREEN QUASARS; POWER-LAW GALAXIES; DEEP-FIELD-SOUTH; MIDINFRARED SPECTROSCOPY; INTERSTELLAR-MEDIUM; LUMINOUS GALAXIES AB We study the mid- to far-IR properties of a 24 mu m-selected flux-limited sample (S-24 > 5mJy) of 154 intermediate redshift (< z > similar to 0.15), infrared luminous galaxies, drawn from the 5 Milli-Jansky Unbiased Spitzer Extragalactic Survey. By combining existing mid-IR spectroscopy and new Herschel SPIRE submm photometry from the Herschel Multi-tiered Extragalactic Survey, we derived robust total infrared luminosity (L-IR) and dust mass (M-dust) estimates and infered the relative contribution of the AGN to the infrared energy budget of the sources. We found that the total (8-1000 mu m) infrared emission of galaxies with weak 6.2 mu m PAH emission (EW6.2 <= 0.2 mu m) is dominated by AGN activity, while for galaxies with EW6.2 > 0.2 mu m more than 50% of the L-IR arises from star formation. We also found that for galaxies detected in the 250-500 mu m Herschel bands an AGN has a statistically insignificant effect on the temperature of the cold dust and the far-IR colours of the host galaxy, which are primarily shaped by star formation activity. For star-forming galaxies we reveal an anti-correlation between the L-IR-to-rest-frame 8 mu m luminosity ratio, IR8 = L-IR/L-8 and the strength of PAH features. We found that this anti-correlation is primarily driven by variations in the PAHs emission, and not by variations in the 5-15 mu m mid-IR continuum emission. Using the [NeIII]/[NeII] line ratio as a tracer of the hardness of the radiation field, we confirm that galaxies with harder radiation fields tend to exhibit weaker PAH features, and found that they have higher IR8 values and higher dust-mass-weighted luminosities (L-IR/M-dust), the latter being a proxy for the dust temperature (T-d). We argue that these trends originate either from variations in the environment of the star-forming regions or are caused by variations in the age of the starburst. Finally, we provide scaling relations that will allow estimating L-IR, based on single-band observations with the mid-infrared instrument, on board the upcoming James Webb Space Telescope. C1 [Magdis, G. E.; Rigopoulou, D.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Rigopoulou, D.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. [Helou, G.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Farrah, D.] Virginia Polytech Inst & State Univ, Dept Phys, Blacksburg, VA 24061 USA. [Hurley, P.; Oliver, S.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Alonso-Herrero, A.] CSIC UC, Inst Fis Cantabria, Santander 39005, Spain. [Bock, J.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Burgarella, D.] Aix Marseille Univ, CNRS, LAM, F-13388 Marseille 13, France. [Chapman, S.] Dalhousie Univ, Halifax, NS B3H 4R2, Canada. [Charmandaris, V.] Univ Crete, Dept Phys, Iraklion 71003, Greece. [Charmandaris, V.] Univ Crete, ITCP, Iraklion 71003, Greece. [Charmandaris, V.] IESL Fdn Res & Technol Hellas, Iraklion 71110, Greece. [Charmandaris, V.] Observ Paris, F-75014 Paris, France. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Dai, Y. Sophia; Huang, J. -S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dale, D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Elbaz, D.] Univ Paris Diderot, CNRS, CEA,DSM,Irfu, Lab AIM Paris Saclay, F-19190 Gif Sur Yvette, France. [Feltre, A.] ESO, D-85748 Garching, Germany. [Feltre, A.; Hatziminaoglou, E.] Dipartimento Fis & Astron, I-35122 Padua, Italy. [Huang, J. -S.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Morrison, G.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Morrison, G.] Canada France Hawaii Telescope, Kamuela, HI 96743 USA. [Page, M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Scott, D.] Univ British Columbia, Dept Phys Astron, Vancouver, BC V6T 1Z1, Canada. [Shi, Y.] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. RP Magdis, GE (reprint author), Univ Oxford, Dept Phys, Keble Rd, Oxford OX1 3RH, England. EM georgios.magdis@astro.ox.ac.uk RI Charmandaris, Vassilis/A-7196-2008; Magdis, Georgios/C-7295-2014; Alonso-Herrero, Almudena/H-1426-2015; OI Charmandaris, Vassilis/0000-0002-2688-1956; Magdis, Georgios/0000-0002-4872-2294; Alonso-Herrero, Almudena/0000-0001-6794-2519; Scott, Douglas/0000-0002-6878-9840 FU John Fell Oxford University Press (OUP); University of Oxford; Universidad de Cantabria August G. Linares Programme; EU [PIRSES-GA-20120316788] FX GEM acknowledges support from the John Fell Oxford University Press (OUP) Research Fund and the University of Oxford. A.A.-H. acknowledges funding through the Universidad de Cantabria August G. Linares Programme. VC acknowledges partial support from the EU FP7 Grant PIRSES-GA-20120316788. This paper uses data from Herschel's photometer SPIRE. SPIRE has been developed by a consortium of institutes led by Cardiff University (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); and Caltech, JPL, NHSC, Univ. Colorado (USA). NR 95 TC 15 Z9 15 U1 0 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2013 VL 558 AR UNSP A136 DI 10.1051/0004-6361/201322226 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000136 ER PT J AU Oshagh, M Boue, G Figueira, P Santos, NC Haghighipour, N AF Oshagh, M. Boue, G. Figueira, P. Santos, N. C. Haghighipour, N. TI Probing the effect of gravitational microlensing on the measurements of the Rossiter-McLaughlin effect SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary systems; techniques: spectroscopic; gravitational lensing: micro; methods: numerical ID SPIN-ORBIT; SYSTEM; VELOCITY; PLANET AB In general, in the studies of transit light-curves and the Rossiter-McLaughlin (RM) effect, the contribution of the planet's gravitational microlensing is neglected. Theoretical studies, have, however shown that the planet's microlensing can affect the transit light-curve and in some extreme cases cause the transit depth to vanish. In this paper, we present the results of our quantitative analysis of the contribution of microlensing on the RM effect. Results indicate that for massive planets in long-period orbits, the planet's microlensing will have considerable contributions to the star's RV measurements. We present the details of our study, and discuss our analysis and results. C1 [Oshagh, M.; Figueira, P.; Santos, N. C.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Oshagh, M.; Santos, N. C.] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4169007 Oporto, Portugal. [Boue, G.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Haghighipour, N.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Haghighipour, N.] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA. [Haghighipour, N.] Univ Tubingen, Dept Computat Phys, Inst Astron & Astrophys, D-72076 Tubingen, Germany. RP Oshagh, M (reprint author), Univ Porto, Ctr Astrofis, Rua Estrelas, P-4150762 Oporto, Portugal. EM moshagh@astro.up.pt RI Santos, Nuno/E-9957-2011; Figueira, Pedro/J-4916-2013; OI Santos, Nuno/0000-0003-4422-2919; Figueira, Pedro/0000-0001-8504-283X; Oshagh, Mahmoudreza/0000-0002-0715-8789 NR 19 TC 3 Z9 3 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 OCT PY 2013 VL 558 AR A65 DI 10.1051/0004-6361/201322337 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000065 ER PT J AU Robitaille, TP Tollerud, EJ Greenfield, P Droettboom, M Bray, E Aldcroft, T Davis, M Ginsburg, A Price-Whelan, AM Kerzendorf, WE Conley, A Crighton, N Barbary, K Muna, D Ferguson, H Grollier, F Parikh, MM Nair, PH Guenther, HM Deil, C Woillez, J Conseil, S Kramer, R Turner, JEH Singer, L Fox, R Weaver, BA Zabalza, V Edwards, ZI Bostroem, KA Burke, DJ Casey, AR Crawford, SM Dencheva, N Ely, J Jenness, T Labrie, K Lim, PL Pierfederici, F Pontzen, A Ptak, A Refsdal, B Servillat, M Streicher, O AF Robitaille, Thomas P. Tollerud, Erik J. Greenfield, Perry Droettboom, Michael Bray, Erik Aldcroft, Tom Davis, Matt Ginsburg, Adam Price-Whelan, Adrian M. Kerzendorf, Wolfgang E. Conley, Alexander Crighton, Neil Barbary, Kyle Muna, Demitri Ferguson, Henry Grollier, Frederic Parikh, Madhura M. Nair, Prasanth H. Guenther, Hans M. Deil, Christoph Woillez, Julien Conseil, Simon Kramer, Roban Turner, James E. H. Singer, Leo Fox, Ryan Weaver, Benjamin A. Zabalza, Victor Edwards, Zachary I. Bostroem, K. Azalee Burke, D. J. Casey, Andrew R. Crawford, Steven M. Dencheva, Nadia Ely, Justin Jenness, Tim Labrie, Kathleen Lim, Pey Lian Pierfederici, Francesco Pontzen, Andrew Ptak, Andy Refsdal, Brian Servillat, Mathieu Streicher, Ole CA Astropy Collaboration TI Astropy: A community Python package for astronomy SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: data analysis; methods: miscellaneous; virtual observatory tools ID OBSERVATIONS COSMOLOGICAL INTERPRETATION; FITS; REPRESENTATIONS AB We present the first public version (v0.2) of the open- source and community- developed Python package, Astropy. This package provides core astronomy- related functionality to the community, including support for domain- specific file formats such as flexible image transport system (FITS) files, Virtual Observatory (VO) tables, and common ASCII table formats, unit and physical quantity conversions, physical constants specific to astronomy, celestial coordinate and time transformations, world coordinate system (WCS) support, generalized containers for representing gridded as well as tabular data, and a framework for cosmological transformations and conversions. Significant functionality is under active development, such as a model fitting framework, VO client and server tools, and aperture and point spread function (PSF) photometry tools. The core development team is actively making additions and enhancements to the current code base, and we encourage anyone interested to participate in the development of future Astropy versions. C1 [Robitaille, Thomas P.; Crighton, Neil] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Tollerud, Erik J.] Yale Univ, Dept Astron, New Haven, CT 06510 USA. [Greenfield, Perry; Droettboom, Michael; Bray, Erik; Davis, Matt; Ferguson, Henry; Bostroem, K. Azalee; Dencheva, Nadia; Ely, Justin; Lim, Pey Lian; Pierfederici, Francesco] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Aldcroft, Tom; Guenther, Hans M.; Burke, D. J.; Refsdal, Brian; Servillat, Mathieu] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ginsburg, Adam; Conley, Alexander] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Price-Whelan, Adrian M.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Kerzendorf, Wolfgang E.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Barbary, Kyle] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. [Muna, Demitri] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Parikh, Madhura M.] SV Natl Inst Technol, Surat 395007, India. [Deil, Christoph; Zabalza, Victor] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Woillez, Julien] European So Observ, D-85748 Garching, Germany. [Conseil, Simon] Univ Aix Marseille, OAMP, Lab Astrophys Marseille, F-13388 Marseille, France. [Conseil, Simon] CNRS, F-13388 Marseille, France. [Kramer, Roban] Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland. [Turner, James E. H.] Gemini Observ, La Serena, Chile. [Singer, Leo] CALTECH, LIGO Lab, Pasadena, CA 91125 USA. [Weaver, Benjamin A.] New York Univ, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Edwards, Zachary I.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Casey, Andrew R.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Weston, ACT 2611, Australia. [Crawford, Steven M.] SAAO, ZA-7925 Cape Town, South Africa. [Jenness, Tim] Joint Astron Ctr, Hilo, HI 96720 USA. [Jenness, Tim] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Labrie, Kathleen] Gemini Observ, Hilo, HI 96720 USA. [Pontzen, Andrew] Oxford Astrophys, Oxford OX1 3RH, England. [Pontzen, Andrew] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Ptak, Andy] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab Code 662, Greenbelt, MD 20771 USA. [Servillat, Mathieu] CEA Saclay, Lab AIM, F-91191 Gif Sur Yvette, France. [Streicher, Ole] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. RP Robitaille, TP (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM robitaille@mpia.de OI Burke, Douglas/0000-0003-4428-7835; Tollerud, Erik/0000-0002-9599-310X; Gunther, Hans Moritz/0000-0003-4243-2840; Jenness, Tim/0000-0001-5982-167X; Streicher, Ole/0000-0001-7751-1843; Ginsburg, Adam/0000-0001-6431-9633; Kerzendorf, Wolfgang/0000-0002-0479-7235; Casey, Andrew/0000-0003-0174-0564; Robitaille, Thomas/0000-0002-8642-1329 FU NASA [NAS8-39073] FX We thank the referee, Igor Chiligarian, for suggestions that helped improve this paper. We would like to thank the NumPy, SciPy (Jones et al. 2001), IPython and Matplolib communities for providing their packages which are invaluable to the development of Astropy. We thank the GitHub (h t t p : //www. github.com) team for providing us with an excellent free development platform. We also are grateful to Read the Docs (https : //readthedocs.org /), Shining Panda (https://www. shiningpanda-ci.com/), and Travis (htps://www.tavis-ci.org/) for providing free documentation hosting and testing respectively. Finally, we would like to thank all the a s t r o p y users that have provided feedback and submitted bug reports. The contribution by T. Aldcroft and D. Burke was funded by NASA contract NAS8-39073. The name resolution functionality shown in Fig. 4 makes use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 40 TC 274 Z9 274 U1 3 U2 16 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2013 VL 558 AR UNSP A33 DI 10.1051/0004-6361/201322068 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000033 ER PT J AU Wallstrom, SHJ Biscaro, C Salgado, F Black, JH Cherchneff, I Muller, S Berne, O Rho, J Tielens, AGGM AF Wallstrom, Sofia H. J. Biscaro, Chiara Salgado, Francisco Black, John H. Cherchneff, Isabelle Muller, Sebastien Berne, Olivier Rho, Jeonghee Tielens, Alexander G. G. M. TI CO rotational line emission from a dense knot in Cassiopeia A Evidence for active post-reverse-shock chemistry SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: supernova remnants; submillimeter: ISM; ISM: individual objects: Cassiopeia A ID SUPERNOVA 1987A; DUST; EJECTA; EXPLOSION; SN-1987A AB We report a Herschel* detection of high-J rotational CO lines from a dense knot in the supernova remnant Cas A. Based on a combined analysis of these rotational lines and previously observed ro-vibrational CO lines, we find the gas to be warm (two components at similar to 400 and 2000 K) and dense (10(6-7) cm(-3)), with a CO column density of similar to 5 x 10(17) cm(-2). This, along with the broad line widths (similar to 400 km s(-1)), suggests that the CO emission originates in the post-shock region of the reverse shock. As the passage of the reverse shock dissociates any existing molecules, the CO has most likely reformed in the past several years in the post-shock gas. The CO cooling time is similar to the CO formation time, therefore we discuss possible heating sources (UV photons from the shock front, X-rays, electron conduction) that may maintain the high column density of warm CO. C1 [Wallstrom, Sofia H. J.; Black, John H.] Chalmers, Dept Earth & Space Sci, S-43992 Onsala, Sweden. [Biscaro, Chiara; Cherchneff, Isabelle] Univ Basel, Dept Phys, CH-4056 Basel, Switzerland. [Salgado, Francisco; Tielens, Alexander G. G. M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Muller, Sebastien] Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden. [Berne, Olivier] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Berne, Olivier] CNRS, IRAP, F-31028 Toulouse 4, France. [Rho, Jeonghee] SETI Inst, Mountain View, CA 94043 USA. [Rho, Jeonghee] NASA, Ames Res Ctr, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. RP Wallstrom, SHJ (reprint author), Chalmers, Dept Earth & Space Sci, S-43992 Onsala, Sweden. EM sofia.wallstrom@chalmers.se OI Wallstrom, Sofia/0000-0001-8345-7097; /0000-0002-9931-1313 FU ESF EuroGENESIS programme through CoDustMas network FX S.W. and C.B. thank the ESF EuroGENESIS programme for financial support through the CoDustMas network. NR 34 TC 9 Z9 9 U1 0 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2013 VL 558 AR UNSP L2 DI 10.1051/0004-6361/201322576 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000153 ER PT J AU Yildiz, UA Acharyya, K Goldsmith, PF van Dishoeck, EF Melnick, G Snell, R Liseau, R Chen, JH Pagani, L Bergin, E Caselli, P Herbst, E Kristensen, LE Visser, R Lis, DC Gerin, M AF Yildiz, Umut A. Acharyya, Kinsuk Goldsmith, Paul F. van Dishoeck, Ewine F. Melnick, Gary Snell, Ronald Liseau, Rene Chen, Jo-Hsin Pagani, Laurent Bergin, Edwin Caselli, Paola Herbst, Eric Kristensen, Lars E. Visser, Ruud Lis, Dariusz C. Gerin, Maryvonne TI Deep observations of O-2 toward a low-mass protostar with Herschel-HIFI SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: formation; ISM: molecules; ISM: individual objects: NGC 1333 IRAS 4A ID DENSE INTERSTELLAR CLOUDS; STAR-FORMING REGIONS; WAVE-ASTRONOMY-SATELLITE; YOUNG STELLAR OBJECTS; NGC 1333; MOLECULAR-OXYGEN; DUST GRAINS; CHEMICAL HISTORY; WATER FORMATION; OPHIUCHI CLOUD AB Context. According to traditional gas-phase chemical models, O-2 should be abundant in molecular clouds, but until recently, attempts to detect interstellar O-2 line emission with ground-and space-based observatories have failed. Aims. Following the multi-line detections of O-2 with low abundances in the Orion and. Oph A molecular clouds with Herschel, it is important to investigate other environments, and we here quantify the O-2 abundance near a solar-mass protostar. Methods. Observations of molecular oxygen, O-2, at 487 GHz toward a deeply embedded low-mass Class 0 protostar, NGC 1333IRAS 4A, are presented, using the Heterodyne Instrument for the Far Infrared (HIFI) on the Herschel Space Observatory. Complementary data of the chemically related NO and CO molecules are obtained as well. The high spectral resolution data are analysed using radiative transfer models to infer column densities and abundances, and are tested directly against full gas-grain chemical models. Results. The deep HIFI spectrum fails to show O-2 at the velocity of the dense protostellar envelope, implying one of the lowest abundance upper limits of O-2/H-2 at = 6x 10-9 (3s). The O-2/CO abundance ratio is less than 0.005. However, a tentative (4.5s) detection of O-2 is seen at the velocity of the surrounding NGC 1333 molecular cloud, shifted by 1 km s-1 relative to the protostar. For the protostellar envelope, pure gas-phase models and gas-grain chemical models require a long pre-collapse phase (similar to 0.7-1 x 106 years), during which atomic and molecular oxygen are frozen out onto dust grains and fully converted to H2O, to avoid overproduction of O2 in the dense envelope. The same model also reproduces the limits on the chemically related NO molecule if hydrogenation of NO on the grains to more complex molecules such as NH2OH, found in recent laboratory experiments, is included. The tentative detection of O-2 in the surrounding cloud is consistent with a low-density PDR model with small changes in reaction rates. Conclusions. The low O-2 abundance in the collapsing envelope around a low-mass protostar suggests that the gas and ice entering protoplanetary disks is very poor in O-2. C1 [Yildiz, Umut A.; van Dishoeck, Ewine F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Acharyya, Kinsuk] SN Bose Natl Ctr Basic Sci, Kolkata 700098, Salt Lake, India. [Goldsmith, Paul F.; Chen, Jo-Hsin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [van Dishoeck, Ewine F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Melnick, Gary; Kristensen, Lars E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Snell, Ronald] Univ Massachusetts, Dept Astron, LGRT 619, Amherst, MA 01003 USA. [Liseau, Rene] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Pagani, Laurent] Observ Paris, LERMA, F-75014 Paris, France. [Pagani, Laurent] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Bergin, Edwin; Visser, Ruud] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Caselli, Paola] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Caselli, Paola] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Herbst, Eric] Univ Virginia, Dept Chem, Charlottesville, VA USA. [Herbst, Eric] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Herbst, Eric] Univ Virginia, Dept Phys, Charlottesville, VA 22901 USA. [Lis, Dariusz C.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Gerin, Maryvonne] Observ Paris, CNRS, UMR 8112, LRA,LERMA, F-75231 Paris 5, France. [Gerin, Maryvonne] Ecole Normale Super, F-75231 Paris 5, France. RP Yildiz, UA (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM yildiz@strw.leidenuniv.nl RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Goldsmith, Paul/H-3159-2016 OI Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; FU Netherlands Research School for Astronomy (NOVA); Spinoza grant; Netherlands Organisation for Scientific Research (NWO) [614.001.008]; European Community [238258, 291141]; NASA FX U. A. Y. and astrochemistry in Leiden are supported by the Netherlands Research School for Astronomy (NOVA), by a Spinoza grant and grant 614.001.008 from the Netherlands Organisation for Scientific Research (NWO), and by the European Community's Seventh Framework Programme FP7/2007-2013 under grant agreement 238258 (LASSIE) and 291141 (CHEMPLAN). This work was carried out in part at the Jet Propulsion Laboratory, which is operated by the California Institute of Technology under contract with NASA. The authors are grateful to many funding agencies and the HIFI-ICC staff, who has been contributing for the construction of Herschel and HIFI for many years. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiolog a (CSIC-INTA). Sweden: Chalmers University of Technology -MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University -Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, NASA/JPL, NHSC. NR 86 TC 24 Z9 25 U1 1 U2 17 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 OCT PY 2013 VL 558 AR A58 DI 10.1051/0004-6361/201321944 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000058 ER PT J AU Fraeman, AA Arvidson, RE Catalano, JG Grotzinger, JP Morris, RV Murchie, SL Stack, KM Humm, DC McGovern, JA Seelos, FP Seelos, KD Viviano, CE AF Fraeman, A. A. Arvidson, R. E. Catalano, J. G. Grotzinger, J. P. Morris, R. V. Murchie, S. L. Stack, K. M. Humm, D. C. McGovern, J. A. Seelos, F. P. Seelos, K. D. Viviano, C. E. TI A hematite-bearing layer in Gale Crater, Mars: Mapping and implications for past aqueous conditions SO GEOLOGY LA English DT Article ID IRON; STABILITY; OXIDATION; EVOLUTION; ORIGIN AB Oversampled Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) visible and near-infrared hyperspectral data over Mount Sharp in Gale Crater, Mars, were used to generate spatially sharpened maps of the location of red crystalline hematite within the uppermost stratum of an similar to 6.5-km-long ridge on the mound's northern flank. Finely layered strata underlie the ridge to the north and have dips consistent with the nearby Mount Sharp sedimentary sequence. Fe-Mg smectites are exposed in a valley to the south of the ridge. Emplacement of the hematite is hypothesized to result either from exposure of anoxic Fe2+-rich ground-water to an oxidizing environment, leading to precipitation of hematite or its precursors, or from in-place weathering of precursor silicate materials under oxidizing conditions. These hypotheses and implications for habitability will be testable with in situ measurements by the Mars rover Curiosity when it reaches Mount Sharp. C1 [Fraeman, A. A.; Arvidson, R. E.; Catalano, J. G.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Grotzinger, J. P.; Stack, K. M.] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. [Morris, R. V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Murchie, S. L.; Humm, D. C.; McGovern, J. A.; Seelos, F. P.; Seelos, K. D.; Viviano, C. E.] Johns Hopkins Appl Phys Lab, Laurel, MD 20723 USA. RP Fraeman, AA (reprint author), Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. RI Catalano, Jeffrey/A-8322-2013; Murchie, Scott/E-8030-2015; Viviano-Beck, Christina/F-3942-2015; Seelos, Kimberly/F-4647-2015; Humm, David/B-8825-2016; Seelos, Frank/C-7875-2016 OI Catalano, Jeffrey/0000-0001-9311-977X; Murchie, Scott/0000-0002-1616-8751; Viviano-Beck, Christina/0000-0003-1601-2105; Seelos, Kimberly/0000-0001-7236-0580; Humm, David/0000-0003-1520-261X; Seelos, Frank/0000-0001-9721-941X FU CRISM APL/JPL contract [104149]; National Science Foundation [DGE-1143954]; NASA Mars Fundamental Research Program [NNX11AH09G]; Mars Exploration Program FX We thank the CRISM Science Operations Center for their assistance in developing the along-track oversampled observations scheme. This manuscript was substantially improved by insightful reviews from E. Rampe, N. Tosca, S. Ruff, and one anonymous reviewer; we also thank S. McLennan and J. Hurowitz for comments on an early version. This work was supported by CRISM APL/JPL contract 104149, and Fraeman was funded by National Science Foundation Graduate Student Research Fellowship grant DGE-1143954. Catalano acknowledges financial support from the NASA Mars Fundamental Research Program (grant NNX11AH09G), and Morris acknowledges the support of the Mars Exploration Program. NR 20 TC 26 Z9 27 U1 2 U2 23 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 EI 1943-2682 J9 GEOLOGY JI Geology PD OCT PY 2013 VL 41 IS 10 BP 1103 EP 1106 DI 10.1130/G34613.1 PG 4 WC Geology SC Geology GA 257NJ UT WOS:000327391200016 ER PT J AU Vojinovic, Z Abebe, YA Ranasinghe, R Vacher, A Martens, P Mandl, DJ Frye, SW van Ettinger, E de Zeeuw, R AF Vojinovic, Z. Abebe, Y. A. Ranasinghe, R. Vacher, A. Martens, P. Mandl, D. J. Frye, S. W. van Ettinger, E. de Zeeuw, R. TI A machine learning approach for estimation of shallow water depths from optical satellite images and sonar measurements SO JOURNAL OF HYDROINFORMATICS LA English DT Article DE bathymetry; machine learning; remote sensing; satellite images; sonar measurements; support vector machine ID MULTISPECTRAL SCANNER DATA; RAW LIDAR DATA; LANDSAT MSS; REGULARIZATION; METHODOLOGY; LAKE AB There has been a rapid growth in the field of remote sensing and its various applications in the area of water management. Nowadays, there are several remote sensing techniques that can be used as a source to derive bathymetry data along coastal areas. The key techniques are: sonar (sound navigating and ranging), LiDAR (light detection and ranging) and high-resolution satellite images. The present paper describes a method which was developed and used to create a shallow water bathymetry data along the Dutch side of Sint Maarten Island by combining sonar measurements and satellite images in a nonlinear machine learning technique. The purpose of this work is to develop a bathymetry dataset that can be used to set up physically-based models for coastal flood modelling work. The nonlinear machine learning technique used in the work is a support vector machine (SVM) model. The sonar data were used as an output whereas image data were used as an input into the SVM model. The results were analysed for three depth ranges and the findings are promising. It remains to further verify the capacity of the new method on a dataset with higher resolution satellite imagery. C1 [Vojinovic, Z.; Abebe, Y. A.; Ranasinghe, R.] UNESCO IHE, Inst Water Educ, Delft, Netherlands. [Vacher, A.] UNDP, Hastings, Barbados. [Martens, P.] Brandweer, Sint Maarten, Dutch Caribbean, Netherlands. [Mandl, D. J.; Frye, S. W.] NASA, Goddard Space Flight Ctr Greenbelt, Greenbelt, MD 20771 USA. [van Ettinger, E.; de Zeeuw, R.] Delft Univ Technol, Shore Monitoring & Res, Delft, Netherlands. RP Vojinovic, Z (reprint author), UNESCO IHE, Inst Water Educ, Delft, Netherlands. EM Z.Vojinovic@unesco-ihe.org RI Ranasinghe, Roshanka/C-6711-2009; OI Ranasinghe, Roshanka/0000-0001-6234-2063 FU UNDP, Barbados FX The work presented in this paper is part of the R3i project, supported by UNDP, Barbados. The authors would like to express their gratitude to Mr Eddy Johnson, Manager Maritime Department-Chief Pilot Ports Authority N.V., Mr Louis Brown, Director VROMI and other officials from the Sint Maarten Government for providing their support throughout this project. We also acknowledge the contribution from the Royal Netherlands Navy for providing deeper bathymetry data. NR 41 TC 2 Z9 2 U1 2 U2 18 PU IWA PUBLISHING PI LONDON PA ALLIANCE HOUSE, 12 CAXTON ST, LONDON SW1H0QS, ENGLAND SN 1464-7141 EI 1465-1734 J9 J HYDROINFORM JI J. Hydroinform. PD OCT PY 2013 VL 15 IS 4 BP 1408 EP 1424 DI 10.2166/hydro.2013.234 PG 17 WC Computer Science, Interdisciplinary Applications; Engineering, Civil; Environmental Sciences; Water Resources SC Computer Science; Engineering; Environmental Sciences & Ecology; Water Resources GA 251BM UT WOS:000326902800024 ER PT J AU Ali, A Sittler, EC Chomay, D Rowe, BR Puzzarini, C AF Ali, A. Sittler, E. C., Jr. Chomay, D. Rowe, B. R. Puzzarini, C. TI Cyclopropenyl cation - the simplest Huckel's aromatic molecule - and its cyclic methyl derivatives in Titan's upper atmosphere SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Titan; Upper atmosphere; Carbocations; Organic chemistry; Molecular structures; Spectroscopic observations ID INFRARED-LASER SPECTROSCOPY; DIFFUSION MONTE-CARLO; RADIATIVE ASSOCIATION; MASS-SPECTROMETER; CARBONIUM-IONS; AB-INITIO; INTERSTELLAR CHEMISTRY; PROTONATED ACETYLENE; ELECTRONIC-STRUCTURE; WAVE SPECTRUM AB The recent measurements by Cassini Ion Neutral Mass Spectrometer (INMS) showed the presence of numerous carbocations and shed light on their composition in Titan's upper atmosphere. The present research identifies an important class of ion-molecule reactions proceeding via carbocation collision complexes, and its implications in the chemistry of Titan's thermosphere and ionosphere. An analysis (based on the kinetics and dynamics of the elementary chemical processes identified) of the Cassini measurements reveals the mechanism of formation of the three-membered Huckel aromatic rings-Cyclopropenyl cation and its cyclic methyl derivatives. For carbocations, a nonclassical three-carbon-center two-electron-bond structure is no longer a controversial topic in chemistry literature. Emphasis has been placed on a future coordinated effort of state-of-the-art laboratory experiments, quantum-chemical calculations, and astronomical ALMA and JWST observations including planetary in situ measurements at millimeter and submillimeter wavelengths to elucidate the structure, energetics and dynamics of the compositions of carbocations detected by Cassini cationic mass spectrometry. The carbocation chemistry in Titan's upper atmosphere has a possible bearing on the organic chemistry and aromaticity in the atmosphere of primitive earth. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Ali, A.; Sittler, E. C., Jr.; Chomay, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ali, A.; Chomay, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Rowe, B. R.] Univ Rennes 1, Equipe Astrochim Expt, Inst Phys Rennes, CNRS, F-35042 Rennes, France. [Puzzarini, C.] Univ Bologna, Dipartimento Chim Giacomo Ciamician, I-40126 Bologna, Italy. RP Ali, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM ashraf.ali@nasa.gov; cristina.puzzarini@unibo.it RI PUZZARINI, CRISTINA/E-4640-2015 OI PUZZARINI, CRISTINA/0000-0002-2395-8532 FU NASA Goddard Space Flight Center by the Cassini Plasma Spectrometer (CAPS) Project through NASA Jet Propulsion Laboratory [1243218]; Southwest Research Institute in San Antonio, Texas; Italian MIUR: PRIN FX This work was supported in part at NASA Goddard Space Flight Center by the Cassini Plasma Spectrometer (CAPS) Project through NASA Jet Propulsion Laboratory contract 1243218 with the Southwest Research Institute in San Antonio, Texas. C.P. gratefully acknowledges support from Italian MIUR: PRIN 2009 funds (Project: "Molecular Spectroscopy for Atmospherical and Astrochemical Research: Experiment, Theory and Applications"). A.A. thanks Dr. J. Hunter Waite for a critical reading of the manuscript and helpful discussions about the limitations of INMS measurements. We are grateful to both reviewers for a careful reading of the manuscript and for comments. One of the referees (anonymous) summarized the version of our paper. We appreciated his summary so much that we have decided to paraphrase his abstract, and this is included in the last section of the manuscript in a bulleted format. NR 86 TC 9 Z9 9 U1 0 U2 14 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD OCT PY 2013 VL 87 BP 96 EP 105 DI 10.1016/j.pss.2013.07.007 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263LM UT WOS:000327810100010 ER PT J AU Rinella, DJ Wipfli, MS Walker, CM Stricker, CA Heintz, RA AF Rinella, Daniel J. Wipfli, Mark S. Walker, Coowe M. Stricker, Craig A. Heintz, Ron A. TI Seasonal persistence of marine-derived nutrients in south-central Alaskan salmon streams SO ECOSPHERE LA English DT Article DE Alaska; aquatic macroinvertebrate; Dolly Varden (Salvelinus malma); fatty acid; horsetail (Equisetum fluviatile); Kenai Peninsula; marine-derived nutrients; seasonal persistence; stable isotopes ID RIPARIAN FOREST GROWTH; JUVENILE COHO SALMON; PACIFIC SALMON; SOCKEYE-SALMON; FRESH-WATER; SOUTHEASTERN ALASKA; COMMUNITY DYNAMICS; ONCORHYNCHUS SPP.; STABLE-ISOTOPES; SPAWNING SALMON AB Spawning salmon deliver annual pulses of marine-derived nutrients (MDN) to riverine ecosystems around the Pacific Rim leading to increased growth and condition in aquatic and riparian biota. The influence of pulsed resources may last for extended periods of time when recipient food webs have effective storage mechanisms yet few studies have tracked the seasonal persistence of MDN. With this as our goal we sampled stream water chemistry and selected stream and riparian biota spring through fall at 18 stations (in six watersheds) that vary widely in spawner abundance and at nine stations (in three watersheds) where salmon runs were blocked by waterfalls. We then developed regression models that related dissolved nutrient concentrations and biochemical measures of MDN assimilation to localized spawner density across these 27 stations. Stream water ammonium-N and orthophosphate-P concentrations increased with spawner density during the summer salmon runs but responses did not persist into the following fall. The effect of spawner density on delta N-15 in generalist macroinvertebrates and three independent MDN metrics (delta N-15 delta S-34 and omega 3:omega 6 fatty acids) in juvenile Dolly Varden (Salvelinus malma) was positive and similar during each season indicating that MDN levels in biota increased with spawner abundance and were maintained for at least nine months after inputs. Delta N-15 in a riparian plant horsetail (Equisetum fluviatile) and scraper macroinvertebrates did not vary with spawner density in any season suggesting a lack of MDN assimilation by these lower trophic levels. Our results demonstrate the ready assimilation of MDN by generalist consumers and the persistence of this pulsed subsidy in these organisms through the winter and into the next growing season. C1 [Rinella, Daniel J.] Univ Alaska Fairbanks, Dept Biol & Wildlife, Fairbanks, AK 99775 USA. [Rinella, Daniel J.] Univ Alaska Anchorage, Environm & Nat Resources Inst, Anchorage, AK 99508 USA. [Wipfli, Mark S.] Univ Alaska Fairbanks, Inst Arctic Biol, Alaska Cooperat Fish & Wildlife Res Unit, US Geol Survey, Fairbanks, AK 99775 USA. [Walker, Coowe M.] Kachemak Bay Natl Estuarine Res Reserve, Homer, AK 99603 USA. [Stricker, Craig A.] US Geol Survey, Ft Collins Sci Ctr, Denver, CO 80225 USA. [Heintz, Ron A.] Natl Marine Fisheries Serv, Auke Bay Labs, Juneau, AK 99801 USA. RP Rinella, DJ (reprint author), Univ Alaska Anchorage, Alaska Nat Heritage Program, Anchorage, AK 99508 USA. EM djrinella@alaska.edu FU Exxon Valdez Oil Spill Trustees Council FX This work was funded by the Gulf Ecosystem Monitoring program, Exxon Valdez Oil Spill Trustees Council. Steve Baird, Ori Badajos, Megan Murphy, and Matt Rogers gave invaluable help in the field. Cayce Gulbransen conducted the stable isotope analyses. Thanks to Matt Rinella, Brandt Meixell, and Jacek Maselko for input on statistical analyses and to Ted Otis, Nicky Szarzi, and David Westerman for help with ADF&G spawner counts. The U.S. Forest Service Forest Health and the Kachemak Bay Research Reserve provided laboratory and bunkhouse space in Cooper Landing and Homer, respectively. Thanks to Jeff Falke and two anonymous reviewers for constructive edits and comments. The use of any trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the U.S. Government. This work was conducted under the University of Alaska Fairbanks IACUC protocol number 06-04. NR 95 TC 12 Z9 12 U1 4 U2 42 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 2150-8925 J9 ECOSPHERE JI Ecosphere PD OCT PY 2013 VL 4 IS 10 AR UNSP 122 DI 10.1890/ES13-00112.1 PG 18 WC Ecology SC Environmental Sciences & Ecology GA 257JT UT WOS:000327380400005 ER PT J AU Sievers, JL Hlozek, RA Nolta, MR Acquaviva, V Addison, GE Ade, PAR Aguirre, P Amiri, M Appel, JW Barrientos, LF Battistelli, ES Battaglia, N Bond, JR Brown, B Burger, B Calabrese, E Chervenak, J Crichton, D Das, S Devlin, MJ Dicker, SR Doriese, WB Dunkley, J Dunner, R Essinger-Hileman, T Faber, D Fisher, RP Fowlera, JW Gallardo, P Gordon, MS Gralla, MB Hajian, A Halpern, M Hasselfield, M Hernandez-Monteagudo, C Hill, JC Hilton, GC Hilton, M Hincks, AD Holtz, D Huffenberger, KM Hughes, DH Hughes, JP Infante, L Irwin, KD Jacobson, DR Johnstone, B Juin, JB Kaul, M Klein, J Kosowsky, A Lau, JM Limon, M Lin, YT Louis, T Lupton, RH Marriage, TA Marsden, D Martocci, K Mauskopf, P McLaren, M Menanteau, F Moodley, K Moseley, H Netterfield, CB Niemack, MD Page, LA Page, WA Parker, L Partridge, B Plimpton, R Quintana, H Reese, ED Reid, B Rojas, F Sehgal, N Sherwin, BD Schmitt, BL Spergel, DN Staggs, ST Stryzak, O Swetz, DS Switzer, ER Thornton, R Trac, H Tucker, C Uehara, M Visnjic, K Warne, R Wilson, G Wollack, E Zhao, Y Zunckel, C AF Sievers, Jonathan L. Hlozek, Renee A. Nolta, Michael R. Acquaviva, Viviana Addison, Graeme E. Ade, Peter A. R. Aguirre, Paula Amiri, Mandana Appel, John William Barrientos, L. Felipe Battistelli, Elia S. Battaglia, Nick Bond, J. Richard Brown, Ben Burger, Bryce Calabrese, Erminia Chervenak, Jay Crichton, Devin Das, Sudeep Devlin, Mark J. Dicker, Simon R. Doriese, W. Bertrand Dunkley, Joanna Duenner, Rolando Essinger-Hileman, Thomas Faber, David Fisher, Ryan P. Fowlera, Joseph W. Gallardo, Patricio Gordon, Michael S. Gralla, Megan B. Hajian, Amir Halpern, Mark Hasselfield, Matthew Hernandez-Monteagudo, Carlos Hill, J. Colin Hilton, Gene C. Hilton, Matt Hincks, Adam D. Holtz, Dave Huffenberger, Kevin M. Hughes, David H. Hughes, John P. Infante, Leopoldo Irwin, Kent D. Jacobson, David R. Johnstone, Brittany Juin, Jean Baptiste Kaul, Madhuri Klein, Jeff Kosowsky, Arthur Lau, Judy M. Limon, Michele Lin, Yen-Ting Louis, Thibaut Lupton, Robert H. Marriage, Tobias A. Marsden, Danica Martocci, Krista Mauskopf, Phil McLaren, Michael Menanteau, Felipe Moodley, Kavilan Moseley, Harvey Netterfield, Calvin B. Niemack, Michael D. Page, Lyman A. Page, William A. Parker, Lucas Partridge, Bruce Plimpton, Reed Quintana, Hernan Reese, Erik D. Reid, Beth Rojas, Felipe Sehgal, Neelima Sherwin, Blake D. Schmitt, Benjamin L. Spergel, David N. Staggs, Suzanne T. Stryzak, Omelan Swetz, Daniel S. Switzer, Eric R. Thornton, Robert Trac, Hy Tucker, Carole Uehara, Masao Visnjic, Katerina Warne, Ryan Wilson, Grant Wollack, Ed Zhao, Yue Zunckel, Caroline CA Atacama Cosmology Telescope TI The Atacama Cosmology Telescope: cosmological parameters from three seasons of data SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE CMBR experiments; Sunyaev-Zeldovich effect; physics of the early universe; cosmological parameters from CMBR ID MICROWAVE-ANISOTROPY-PROBE; ANGULAR POWER SPECTRUM; SOUTH-POLE TELESCOPE; BARYON ACOUSTIC-OSCILLATIONS; SKY SURVEY DATA; HUBBLE CONSTANT; DARK ENERGY; INFLATIONARY UNIVERSE; WMAP OBSERVATIONS; BACKGROUND POLARIZATION AB We present constraints on cosmological and astrophysical parameters from highresolution microwave background maps at 148 GHz and 218 GHz made by the Atacama Cosmology Telescope (ACT) in three seasons of observations from 2008 to 2010. A model of primary cosmological and secondary foreground parameters is fit to the map power spectra and lensing deflection power spectrum, including contributions from both the thermal Sunyaev-Zeldovich (tSZ) effect and the kinematic Sunyaev-Zeldovich (kSZ) effect, Poisson and correlated anisotropy from unresolved infrared sources, radio sources, and the correlation between the tSZ effect and infrared sources. The power PO/27 of the thermal SZ power spectrum at 148 GHz is measured to be 3.4 1.4 1tK2 at = 3000, while the corresponding amplitude of the kinematic SZ power spectrum has a 95% confidence level upper limit of 8.6 1tK2. Combining ACT power spectra with the WMAP 7-year temperature and polarization power spectra, we find excellent consistency with the LCDM model. We constrain the number of effective relativistic degrees of freedom in the early universe to be Neff = 2.79 0.56, in agreement with the canonical value of Neff = 3.046 for three massless neutrinos. We constrain the sum of the neutrino masses to be Krn, < 0.39 eV at 95% confidence when combining ACT and WMAP 7-year data with BAO and Hubble constant measurements. We constrain the amount of primordial helium to be Yp = 0.225 0.034, and measure no variation in the fine structure constant a since recombination, with a/ao = 1.004 0.005. We also find no evidence for any running of the scalar spectral index, dnsld ln k = 0.004 0.012. C1 [Sievers, Jonathan L.; Appel, John William; Essinger-Hileman, Thomas; Faber, David; Fisher, Ryan P.; Fowlera, Joseph W.; Hajian, Amir; Hincks, Adam D.; Holtz, Dave; Lau, Judy M.; Limon, Michele; Marriage, Tobias A.; Martocci, Krista; Niemack, Michael D.; Page, Lyman A.; Page, William A.; Parker, Lucas; Partridge, Bruce; Reid, Beth; Sehgal, Neelima; Sherwin, Blake D.; Staggs, Suzanne T.; Stryzak, Omelan; Switzer, Eric R.; Uehara, Masao; Visnjic, Katerina; Zhao, Yue] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Sievers, Jonathan L.; Nolta, Michael R.; Battaglia, Nick; Bond, J. Richard; Hajian, Amir; Hincks, Adam D.; Switzer, Eric R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M55 3H8, Canada. [Hlozek, Renee A.; Gordon, Michael S.; Hajian, Amir; Hasselfield, Matthew; Hill, J. Colin; Lin, Yen-Ting; Lupton, Robert H.; Marriage, Tobias A.; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Acquaviva, Viviana] New York City Coll Technol, Brooklyn, NY 11201 USA. [Addison, Graeme E.; Amiri, Mandana; Battistelli, Elia S.; Burger, Bryce; Halpern, Mark; Hasselfield, Matthew] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. [Addison, Graeme E.; Calabrese, Erminia; Dunkley, Joanna; Louis, Thibaut] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Ade, Peter A. R.; Mauskopf, Phil; Tucker, Carole] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Aguirre, Paula; Barrientos, L. Felipe; Duenner, Rolando; Gallardo, Patricio; Infante, Leopoldo; Juin, Jean Baptiste; Quintana, Hernan; Rojas, Felipe] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile. [Battistelli, Elia S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [Battaglia, Nick; Trac, Hy] Carnegie Mellon Univ, Dept Astron, Pittsburgh, PA 15260 USA. [Brown, Ben; Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Chervenak, Jay; Moseley, Harvey; Wollack, Ed] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Crichton, Devin; Gralla, Megan B.; Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Das, Sudeep] Univ Calif Berkeley, LBL, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Das, Sudeep] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. [Devlin, Mark J.; Dicker, Simon R.; Jacobson, David R.; Kaul, Madhuri; Klein, Jeff; Limon, Michele; Marsden, Danica; McLaren, Michael; Plimpton, Reed; Reese, Erik D.; Schmitt, Benjamin L.; Swetz, Daniel S.; Thornton, Robert] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Doriese, W. Bertrand; Fowlera, Joseph W.; Hilton, Gene C.; Irwin, Kent D.; Niemack, Michael D.; Swetz, Daniel S.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Hernandez-Monteagudo, Carlos] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Hilton, Matt] Univ Nottingham, Sch Phys & Astron, Ctr Astron & Particle Theory, Nottingham NG7 2RD, England. [Hilton, Matt; Moodley, Kavilan; Warne, Ryan] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Huffenberger, Kevin M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA. [Hughes, David H.] INAOE, Puebla, Mexico. [Hughes, John P.; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Marsden, Danica] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Johnstone, Brittany; Thornton, Robert] West Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA. [Limon, Michele] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Lin, Yen-Ting] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan. [Lin, Yen-Ting] Acad Sinica, Inst Astron Sz Astrophys, Taipei 115, Taiwan. [Switzer, Eric R.] Kavli Inst Cosmol Phys, Lab Astrophys & Space Res, Chicago, IL 60637 USA. [Mauskopf, Phil] Arizona State Univ, Glendale, AZ 85306 USA. [Netterfield, Calvin B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. [Sehgal, Neelima] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Wilson, Grant] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Zunckel, Caroline] Univ KwaZulu Natal, Dept Chem & Phys, ZA-3209 Scottsville, South Africa. RP Sievers, JL (reprint author), Princeton Univ, Joseph Henry Labs Phys, Jadwin Hall, Princeton, NJ 08544 USA. EM renee.hlozek@gmail.com RI Trac, Hy/N-8838-2014; Wollack, Edward/D-4467-2012; OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451; Gordon, Michael/0000-0002-1913-2682; Limon, Michele/0000-0002-5900-2698; Huffenberger, Kevin/0000-0001-7109-0099; Menanteau, Felipe/0000-0002-1372-2534; Sievers, Jonathan/0000-0001-6903-5074; McLaren, Michael/0000-0003-1575-473X NR 195 TC 130 Z9 130 U1 2 U2 21 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD OCT PY 2013 IS 10 AR 060 DI 10.1088/1475-7516/2013/10/060 PG 48 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 252BN UT WOS:000326979500060 ER PT J AU Signorini, SR Mannino, A Najjar, RG Friedrichs, MAM Cai, WJ Salisbury, J Wang, ZA Thomas, H Shadwick, E AF Signorini, Sergio R. Mannino, Antonio Najjar, Raymond G., Jr. Friedrichs, Marjorie A. M. Cai, Wei-Jun Salisbury, Joe Wang, Zhaohui Aleck Thomas, Helmuth Shadwick, Elizabeth TI Surface ocean pCO(2) seasonality and sea-air CO2 flux estimates for the North American east coast SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE coastal carbon; sea-air CO2 fluxes; North American east coast ID CONTINENTAL-SHELF CARBON; MIDDLE ATLANTIC BIGHT; INORGANIC CARBON; UNITED-STATES; NEURAL-NETWORK; SCOTIAN SHELF; VARIABILITY; DIOXIDE; GULF; WATER AB Underway and in situ observations of surface ocean pCO(2), combined with satellite data, were used to develop pCO(2) regional algorithms to analyze the seasonal and interannual variability of surface ocean pCO(2) and sea-air CO2 flux for five physically and biologically distinct regions of the eastern North American continental shelf: the South Atlantic Bight (SAB), the Mid-Atlantic Bight (MAB), the Gulf of Maine (GoM), Nantucket Shoals and Georges Bank (NS+GB), and the Scotian Shelf (SS). Temperature and dissolved inorganic carbon variability are the most influential factors driving the seasonality of pCO(2). Estimates of the sea-air CO2 flux were derived from the available pCO(2) data, as well as from the pCO(2) reconstructed by the algorithm. Two different gas exchange parameterizations were used. The SS, GB+NS, MAB, and SAB regions are net sinks of atmospheric CO2 while the GoM is a weak source. The estimates vary depending on the use of surface ocean pCO(2) from the data or algorithm, as well as with the use of the two different gas exchange parameterizations. Most of the regional estimates are in general agreement with previous studies when the range of uncertainty and interannual variability are taken into account. According to the algorithm, the average annual uptake of atmospheric CO2 by eastern North American continental shelf waters is found to be between -3.4 and -5.4 Tg C yr(-1) (areal average of -0.7 to -1.0 mol CO2 m(-2) yr(-1)) over the period 2003-2010. C1 [Signorini, Sergio R.] Sci Applicat Int Corp, Washington, DC USA. [Mannino, Antonio] NASA, Goddard Space Flight Ctr, Ocean Ecol Lab, Greenbelt, MD 20771 USA. [Najjar, Raymond G., Jr.] The Pennsylvania, Dept Meteorol, University Pk, PA USA. [Friedrichs, Marjorie A. M.] Coll William & Mary, Virginia Inst Marine Sci, Gloucester Point, VA USA. [Cai, Wei-Jun] Univ Delaware, Sch Marine Sci & Policy, Newark, DE USA. [Salisbury, Joe] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Wang, Zhaohui Aleck] Woods Hole Oceanog Inst, Dept Marine Chem & Geochem, Woods Hole, MA 02543 USA. [Thomas, Helmuth] Univ Halifax, Dept Oceanog, Halifax, NS, Canada. [Shadwick, Elizabeth] Univ Tasmania, Antarctic Climate & Ecosyst Cooperat Res Ctr, Hobart, Tas, Australia. RP Signorini, SR (reprint author), NASA, Goddard Space Flight Ctr, Code 616-2,Bldg 28-Rm W168,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM sergio.signorini@nasa.gov RI Mannino, Antonio/I-3633-2014; Cai, Wei-Jun/C-1361-2013; OI Cai, Wei-Jun/0000-0003-3606-8325; Friedrichs, Marjorie/0000-0003-2828-7595 FU NASA Ocean Biology and Biogeochemistry program FX We wish to acknowledge the NASA Ocean Biology and Biogeochemistry program for providing funds for this project. We also want to acknowledge Daniel Tomaso for providing the compiled climatologic data sets for sea surface salinity and mixed layer depth, and Environment Canada for making available the wind data from Sable Island. NR 56 TC 22 Z9 22 U1 1 U2 21 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 OCT PY 2013 VL 118 IS 10 BP 5439 EP 5460 DI 10.1002/jgrc.20369 PG 22 WC Oceanography SC Oceanography GA 257JQ UT WOS:000327380100044 ER PT J AU Boisvert, LN Markus, T Vihma, T AF Boisvert, Linette N. Markus, Thorsten Vihma, Timo TI Moisture flux changes and trends for the entire Arctic in 2003-2011 derived from EOS Aqua data SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE moisture flux; Arctic sea ice; specific humidity; EOS Aqua; AIRS; AMSR-E ID PARAMETERIZING TURBULENT EXCHANGE; ATMOSPHERIC BOUNDARY-LAYER; SEA-ICE; PROFILE RELATIONSHIPS; GRADIENT RELATIONSHIPS; SURFACE-LAYER; TEMPERATURE; REANALYSES; CLOUD; SIMULATIONS AB The Arctic sea ice acts as a barrier between the ocean and lower atmosphere, reducing the exchange of heat and moisture. In recent years the ice pack has undergone many changes, in particular a rapid reduction in sea ice extent and compactness in summer and autumn. This, along with modeling studies, would cause one to believe that the moisture flux would be increasing. We estimate the daily moisture flux from 2003 to 2011 using geophysical data from multiple sensors onboard NASA's Aqua satellite, taking advantage of observations being collected at the same time and along the same track. Our findings show the moisture flux, averaged over the entire Arctic, has had large interannual variations, with smallest fluxes in 2010, 2003, and 2004, and largest ones in 2007, 2008, and 2005. Increases in air specific humidity tend to reduce the moisture flux, whereas the decrease in sea ice cover tends to increase the flux. Statistically significant seasonal decreasing trends are seen in December, January, and February because of the dominating effect of increase in 2 m air specific humidity increasing, reducing the surface-air specific humidity difference by -0.0547 kg/kg in the Kara/Barents Seas, E. Greenland Sea, and Baffin Bay regions where there is some open water year round. Our results also show that the contribution of the sea ice zone to the total moisture flux (from the open ocean and sea ice zone) has increased by 3.6% because the amount of open water within the sea ice zone has increased by 4.3%. C1 [Boisvert, Linette N.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Markus, Thorsten] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Vihma, Timo] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. RP Boisvert, LN (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. EM linette.n.boisvert@nasa.gov OI Boisvert, Linette/0000-0003-4778-4765 FU ACE academic support team; ESSIC [NNX12AD03A]; Academy of Finland via the CACSI project [259537] FX The authors thank the ACE academic support team for their support on this project. The work of Linette Boisvert was supported by ESSIC Cooperative Agreement NNX12AD03A, Task 624. The work of Timo Vihma was supported by the Academy of Finland via the CACSI project (contract 259537). The authors would also like to thank the suggestions and input from two anonymous reviewers. We thank Timo Palo, Erko Jakboson, and Jaak Jaagus from the University of Tartu, Estonia, for providing us with the Tara observations. NR 54 TC 13 Z9 13 U1 1 U2 10 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 OCT PY 2013 VL 118 IS 10 BP 5829 EP 5843 DI 10.1002/jgrc.20414 PG 15 WC Oceanography SC Oceanography GA 257JQ UT WOS:000327380100068 ER PT J AU Misa, WFXE Drazen, JC Kelley, CD Moriwake, VN AF Misa, William F. X. E. Drazen, Jeffrey C. Kelley, Christopher D. Moriwake, Virginia N. TI Establishing species-habitat associations for 4 eteline snappers with the use of a baited stereo-video camera system SO FISHERY BULLETIN LA English DT Article ID ESSENTIAL FISH HABITAT; JUVENILE PINK SNAPPER; PRISTIPOMOIDES-FILAMENTOSUS; UNDERWATER VIDEO; HAWAIIAN-ISLANDS; RELATIVE DENSITY; DEMERSAL FISH; REEF-FISH; CLASSIFICATION; ARCHIPELAGO AB With the use of a baited stereo-video camera system, this study semiquantitatively defined the habitat associations of 4 species of Lutjanidae: Opakapaka (Pristipomoides filamentosus), Kalekale (P. sieboldii), Onaga (Etelis coruscans), and Ehu (E. carbunculus). Fish abundance and length data from 6 locations in the main Hawaiian Islands were evaluated for species-specific and size-specific differences between regions and habitat types. Multibeam bathymetry and back-scatter were used to classify habitats into 4 types on the basis of substrate (hard or soft) and slope (high or low). Depth was a major influence on bottomfish distributions. Opakapaka occurred at depths shallower than the depths at which other species were observed, and this species showed an ontogenetic shift to deeper water with increasing size. Opakapaka and Ehu had an overall preference for hard substrate with low slope (hard-low), and Onaga was found over both hard-low and hard-high habitats. No significant habitat preferences were recorded for Kalekale. Opakapaka, Kalekale, and Onaga exhibited size-related shifts with habitat type. A move into hard-high environments with increasing size was evident for Opakapaka and Kalekale. Onaga was seen predominantly in hard-low habitats at smaller sizes and in either hard-low or hard-high at larger sizes. These ontogenetic habitat shifts could be driven by reproductive triggers because they roughly coincided with the length at sexual maturity of each species. However, further studies are required to determine causality. No ontogenetic shifts were seen for Ehu, but only a limited number of juveniles were observed. Regional variations in abundance and length were also found and could be related to fishing pressure or large-scale habitat features. C1 [Misa, William F. X. E.; Drazen, Jeffrey C.; Moriwake, Virginia N.] Univ Hawaii, Sch Ocean & Earth Sci & Technol, Dept Oceanog, Honolulu, HI 96822 USA. [Kelley, Christopher D.] Univ Hawaii, Sch Ocean & Earth Sci & Technol, Hawaii Undersea Res Lab, Honolulu, HI 96822 USA. RP Misa, WFXE (reprint author), NOAA, Fisheries Res & Monitoring Div, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2570 Dole St, Honolulu, HI 96822 USA. EM wfmisa@hawaii.edu RI Drazen, Jeffrey/C-1197-2013 OI Drazen, Jeffrey/0000-0001-9613-3833 FU State of Hawaii DLNR-DAR; Federal Aid in Sport Fish Restoration Program FX We would like to thank C. Moore, D. Sackett, and F. De Leo for input on statistical design and testing; C. Demarke, B. Alexander, J. Yeh, J. Friedman, and B. Schumacher for many hours of field operations and video analysis; D. Merritt, K. Wong, and the Coral Reef Ecosystem Division of the NOAA Pacific Islands Fisheries Science Center for giving us access to BotCam units; J. Ault, S. Smith, M. Parke, G. DiNardo, and J. Brodziak for assistance with the experimental design; and captains R. Cates (Wailoa) and G. Jones (Red Raven; Huki Pono). This project was funded by the State of Hawaii DLNR-DAR and in part by the Federal Aid in Sport Fish Restoration Program. NR 41 TC 5 Z9 5 U1 0 U2 15 PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE PI SEATTLE PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA SN 0090-0656 EI 1937-4518 J9 FISH B-NOAA JI Fish. Bull. PD OCT PY 2013 VL 111 IS 4 BP 293 EP 308 DI 10.7755/FB.111.4.1 PG 16 WC Fisheries SC Fisheries GA 251SZ UT WOS:000326952300001 ER PT J AU Drymon, JM Carassou, L Powers, SP Grace, M Dindo, J Dzwonkowski, B AF Drymon, J. Marcus Carassou, Laure Powers, Sean P. Grace, Mark Dindo, John Dzwonkowski, Brian TI Multiscale analysis of factors that affect the distribution of sharks throughout the northern Gulf of Mexico SO FISHERY BULLETIN LA English DT Article ID CO-INERTIA ANALYSIS; RHIZOPRIONODON-TERRAENOVAE; CARCHARHINUS-LIMBATUS; MARINE ECOSYSTEMS; TOP PREDATOR; HABITAT USE; GROWTH; BAY; PATTERNS; DECLINES AB Identification of the spatial scale at which marine communities are organized is critical to proper management, yet this is particularly difficult to determine for highly migratory species like sharks. We used shark catch data collected during 2006-09 from fishery-independent bottom-longline surveys, as well as biotic and abiotic explanatory data to identify the factors that affect the distribution of coastal sharks at 2 spatial scales in the northern Gulf of Mexico. Centered principal component analyses (PCAs) were used to visualize the patterns that characterize shark distributions at small (Alabama and Mississippi coast) and large (northern Gulf of Mexico) spatial scales. Environmental data on temperature, salinity, dissolved oxygen (DO), depth, fish and crustacean biomass, and chlorophyll-a (chl-a) concentration were analyzed with normed PCAs at both spatial scales. The relationships between values of shark catch per unit of effort (CPUE) and environmental factors were then analyzed at each scale with co-inertia analysis (COIA). Results from COIA indicated that the degree of agreement between the structure of the environmental and shark data sets was relatively higher at the small spatial scale than at the large one. CPUE of Blacktip Shark (Carcharhinus limbatus) was related positively with crustacean biomass at both spatial scales. Similarly, CPUE of Atlantic Sharpnose Shark (Rhizoprionodon terraenovae) was related positively with chl-a concentration and negatively with DO at both spatial scales. Conversely, distribution of Blacknose Shark (C. acronotus) displayed a contrasting relationship with depth at the 2 scales considered. Our results indicate that the factors influencing the distribution of sharks in the northern Gulf of Mexico are species specific but generally transcend the spatial boundaries used in our analyses. C1 [Drymon, J. Marcus; Powers, Sean P.] Univ S Alabama, Dept Marine Sci, Mobile, AL 36688 USA. [Drymon, J. Marcus; Powers, Sean P.; Dindo, John; Dzwonkowski, Brian] Dauphin Isl Sea Lab, Dauphin Isl, AL 36528 USA. [Carassou, Laure] Rhodes Univ, Dept Zool & Entomol, ZA-6140 Grahamstown, South Africa. [Grace, Mark] NOAA, Mississippi Labs, Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Pascagoula, MS 39567 USA. RP Drymon, JM (reprint author), Univ S Alabama, Dept Marine Sci, LSCB-25, Mobile, AL 36688 USA. EM mdrymon@disl.org RI Carassou, Laure/L-3425-2013; OI Dzwonkowski, Brian/0000-0002-2333-2185 FU Alabama Department of Conservation; Natural Resources, Marine Resources Division FX The authors wish to thank all members of the Fisheries Ecology Laboratory at Dauphin Island Sea Laboratory (DISL), as well as members of the NOAA Southeast Fisheries Science Center Mississippi Laboratories shark team for the countless hours they spent at sea collecting valuable data. Data from DISL's Fisheries Oceanography of Coastal Alabama research program, which is funded by the Alabama Department of Conservation and Natural Resources, Marine Resources Division, were used to provide ground truth for remotely sensed data from NASA's Sea-viewing Wide Field-of-view Sensor (SeaWifs) Project. We wish to thank T. Henwood and E. Hoffmayer from the National Marine Fisheries Service for constructive comments that improved this manuscript. NR 39 TC 6 Z9 6 U1 2 U2 32 PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE PI SEATTLE PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA SN 0090-0656 EI 1937-4518 J9 FISH B-NOAA JI Fish. Bull. PD OCT PY 2013 VL 111 IS 4 BP 370 EP 380 DI 10.7755/FB.111.4.6 PG 11 WC Fisheries SC Fisheries GA 251SZ UT WOS:000326952300006 ER PT J AU Glavin, DP Freissinet, C Miller, KE Eigenbrode, JL Brunner, AE Buch, A Sutter, B Archer, PD Atreya, SK Brinckerhoff, WB Cabane, M Coll, P Conrad, PG Coscia, D Dworkin, JP Franz, HB Grotzinger, JP Leshin, LA Martin, MG McKay, C Ming, DW Navarro-Gonzalez, R Pavlov, A Steele, A Summons, RE Szopa, C Teinturier, S Mahaffy, PR AF Glavin, Daniel P. Freissinet, Caroline Miller, Kristen E. Eigenbrode, Jennifer L. Brunner, Anna E. Buch, Arnaud Sutter, Brad Archer, P. Douglas, Jr. Atreya, Sushil K. Brinckerhoff, William B. Cabane, Michel Coll, Patrice Conrad, Pamela G. Coscia, David Dworkin, Jason P. Franz, Heather B. Grotzinger, John P. Leshin, Laurie A. Martin, Mildred G. McKay, Christopher Ming, Douglas W. Navarro-Gonzalez, Rafael Pavlov, Alexander Steele, Andrew Summons, Roger E. Szopa, Cyril Teinturier, Samuel Mahaffy, Paul R. TI Evidence for perchlorates and the origin of chlorinated hydrocarbons detected by SAM at the Rocknest aeolian deposit in Gale Crater SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars Science Laboratory; Sample Analysis at Mars; Rocknest soil; chlorohydrocarbons; perchlorates; MTBSTFA ID POLYCYCLIC AROMATIC-HYDROCARBONS; CHROMATOGRAPHY-MASS-SPECTROMETRY; ALLAN HILLS 84001; MARTIAN SOIL; ORGANIC-COMPOUNDS; THERMAL-DECOMPOSITION; MAGNESIUM PERCHLORATE; AMINO-ACIDS; BIOLOGICAL EXPERIMENTS; IONIZING-RADIATION AB A single scoop of the Rocknest aeolian deposit was sieved (<150 mu m), and four separate sample portions, each with a mass of similar to 50mg, were delivered to individual cups inside the Sample Analysis at Mars (SAM) instrument by the Mars Science Laboratory rover's sample acquisition system. The samples were analyzed separately by the SAM pyrolysis evolved gas and gas chromatograph mass spectrometer analysis modes. Several chlorinated hydrocarbons including chloromethane, dichloromethane, trichloromethane, a chloromethylpropene, and chlorobenzene were identified by SAM above background levels with abundances of similar to 0.01 to 2.3nmol. The evolution of the chloromethanes observed during pyrolysis is coincident with the increase in O-2 released from the Rocknest sample and the decomposition of a product of N-methyl-N-(tert-butyldimethylsilyl)-trifluoroacetamide (MTBSTFA), a chemical whose vapors were released from a derivatization cup inside SAM. The best candidate for the oxychlorine compounds in Rocknest is a hydrated calcium perchlorate (Ca(ClO4)(2)nH(2)O), based on the temperature release of O-2 that correlates with the release of the chlorinated hydrocarbons measured by SAM, although other chlorine-bearing phases are being considered. Laboratory analog experiments suggest that the reaction of Martian chlorine from perchlorate decomposition with terrestrial organic carbon from MTBSTFA during pyrolysis can explain the presence of three chloromethanes and a chloromethylpropene detected by SAM. Chlorobenzene may be attributed to reactions of Martian chlorine released during pyrolysis with terrestrial benzene or toluene derived from 2,6-diphenylphenylene oxide (Tenax) on the SAM hydrocarbon trap. At this time we do not have definitive evidence to support a nonterrestrial carbon source for these chlorinated hydrocarbons, nor do we exclude the possibility that future SAM analyses will reveal the presence of organic compounds native to the Martian regolith. C1 [Glavin, Daniel P.; Eigenbrode, Jennifer L.; Brunner, Anna E.; Brinckerhoff, William B.; Conrad, Pamela G.; Dworkin, Jason P.; Franz, Heather B.; Martin, Mildred G.; Pavlov, Alexander; Mahaffy, Paul R.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Freissinet, Caroline] NASA, NASA Postdoctoral Program, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Miller, Kristen E.; Summons, Roger E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. [Brunner, Anna E.] Univ Maryland, Dept Astron, Ctr Res & Explorat Space Sci & Technol, College Pk, MD 20742 USA. [Buch, Arnaud] Ecole Cent Paris, Lab Genie Proc & Mat, Chatenay Malabry, France. [Sutter, Brad] Jacobs Technol ESCG, Houston, TX USA. [Sutter, Brad; Archer, P. Douglas, Jr.; Ming, Douglas W.] NASA, Astromat Res & Explorat Sci Directorate, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Atreya, Sushil K.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Cabane, Michel; Coscia, David; Szopa, Cyril; Teinturier, Samuel] Univ Versailles St Quentin, Univ Paris 06, Atmospheres Lab, Paris, France. [Cabane, Michel; Coscia, David; Szopa, Cyril; Teinturier, Samuel] CNRS, Paris, France. [Coll, Patrice] Univ Paris 07, Univ Paris Est Creteil, Lab Interuniv Syst Atmospher, Creteil, France. [Coll, Patrice] Hop Henri Mondor, CNRS, F-94010 Creteil, France. [Franz, Heather B.] Univ Maryland Baltimore Cty, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21228 USA. [Grotzinger, John P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Leshin, Laurie A.] Rensselaer Polytech Inst, Dept Earth & Environm Sci, Troy, NY USA. [Leshin, Laurie A.] Rensselaer Polytech Inst, Sch Sci, Troy, NY USA. [Martin, Mildred G.] Catholic Univ Amer, Dept Chem, Washington, DC 20064 USA. [McKay, Christopher] NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA. [Navarro-Gonzalez, Rafael] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. [Steele, Andrew] Carnegie Inst Sci, Geophys Lab, Washington, DC USA. RP Glavin, DP (reprint author), NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Code 699, Greenbelt, MD 20771 USA. EM daniel.p.glavin@nasa.gov RI Glavin, Daniel/D-6194-2012; Gonzalez, Rafael/D-1748-2009; szopa, cyril/C-6865-2015; Dworkin, Jason/C-9417-2012 OI Glavin, Daniel/0000-0001-7779-7765; szopa, cyril/0000-0002-0090-4056; Dworkin, Jason/0000-0002-3961-8997 FU NASA ROSES MSL Participating Scientist Program; NASA Postdoctoral Program; NASA FX NASA provided support for the development of SAM. Data from these SAM experiments will be archived in the Planetary Data System (pds.nasa.gov) in 2013. Essential contributions to the successful operation of SAM on Mars and the acquisition of these data were provided by the SAM development, operations, and testbed teams. D. P. G., J.L.E., K. E. M., M. G. M., J.P.D., and R. E. S. acknowledge funding support from the NASA ROSES MSL Participating Scientist Program. C. F. and P. D. A. acknowledge support from the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. We thank M. Benna for providing input on the modeled pressure and flow conditions in SAM. We thank R. Quinn and an anonymous reviewer for helpful comments and appreciate valuable discussions with H. Steininger. NR 91 TC 74 Z9 75 U1 12 U2 75 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 OCT PY 2013 VL 118 IS 10 BP 1955 EP 1973 DI 10.1002/jgre.20144 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 252RJ UT WOS:000327026900001 ER PT J AU Buratti, BJ Dalba, PA Hicks, MD Reddy, V Sykes, MV McCord, TB O'Brien, DP Pieters, CM Prettyman, TH McFadden, LA Nathues, A Le Corre, L Marchi, S Raymond, C Russell, C AF Buratti, B. J. Dalba, P. A. Hicks, M. D. Reddy, V. Sykes, M. V. McCord, T. B. O'Brien, D. P. Pieters, C. M. Prettyman, T. H. McFadden, L. A. Nathues, Andreas Le Corre, Lucille Marchi, S. Raymond, Carol Russell, Chris TI Vesta, vestoids, and the HED meteorites: Interconnections and differences based on Dawn Framing Camera observations SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE asteroids; Vesta; HED; vestoids ID ASTEROID 4 VESTA; SURFACE-COMPOSITION; DARK MATERIAL; PARENT BODY; SPACE; HETEROGENEITY; EARTH; HOWARDITE; REGOLITH; EUCRITE AB The Framing Camera (FC) on the Dawn spacecraft provided the first view of 4 Vesta at sufficiently high spatial resolution to enable a detailed correlation of the asteroid's spectral properties with geologic features and with the vestoid (V-type) asteroids and the Howardite-Eucrite-Diogenite (HED) class of meteorites, both of which are believed to originate on Vesta. We combine a spectral analysis of the basin with visible and near-IR spectroscopy of vestoids and with archived data over the same spectral range for HED meteorites. The vestoids are only slightly more akin to the Rheasilvia basin than to Vesta as a whole, suggesting that the crustal material ejected is a well-mixed collection of eucritic and diogenitic materials. The basin itself is more diogenitic, implying Vesta is differentiated and the impact that created Rheasilvia uncovered a mineralogically distinct layer. The Rheasilvia basin exhibits a larger range in pyroxene band strengths than Vesta as a whole, further implying that the basin offers a view into a complex, differentiated protoplanet. The discrepancy between the spectral properties of the HED meteorites and Vesta, in particular the meteorites' deeper pyroxene absorption band and the redder color of the vestoids, can be explained by the abundance of smaller particles on Vesta and by the addition of low-albedo exogenous particles to its surface, which in turn are due to its larger gravity and longer exposure time to impact processing. Solar phase effects are slight and do not explain the spectral discrepancies between the HEDs, Vesta, and the vestoids. C1 [Buratti, B. J.; Dalba, P. A.; Hicks, M. D.; Raymond, Carol] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Reddy, V.; Sykes, M. V.; O'Brien, D. P.; Prettyman, T. H.] Planetary Sci Inst, Tucson, AZ USA. [McCord, T. B.] Bear Fight Inst, Winthrop, WA USA. [Pieters, C. M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [McFadden, L. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nathues, Andreas; Le Corre, Lucille] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany. [Marchi, S.] NASA, Lunar Sci Inst, Boulder, CO USA. [Russell, Chris] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. [Russell, Chris] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. RP Buratti, BJ (reprint author), CALTECH, JPL Jet Prop Lab, 4800 Oak Grove Dr 183-401, Pasadena, CA 91109 USA. EM bonnie.buratti@jpl.nasa.gov OI McFadden, Lucy/0000-0002-0537-9975; Reddy, Vishnu/0000-0002-7743-3491; Prettyman, Thomas/0000-0003-0072-2831; Le Corre, Lucille/0000-0003-0349-7932 FU Dawn Participating Scientist program; National Aeronautics and Space Administration FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology under contract to the National Aeronautics and Space Administration. We acknowledge support from the Dawn Participating Scientist program. This research utilizes spectra acquired by the NASA RELAB facility at Brown University. We thank Dr. Deborah Domingue and an anonymous referee for their detailed reviews. NR 44 TC 5 Z9 5 U1 0 U2 3 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 OCT PY 2013 VL 118 IS 10 BP 1991 EP 2003 DI 10.1002/jgre.20152 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 252RJ UT WOS:000327026900004 ER PT J AU Spudis, PD Bussey, DBJ Baloga, SM Cahill, JTS Glaze, LS Patterson, GW Raney, RK Thompson, TW Thomson, BJ Ustinov, EA AF Spudis, P. D. Bussey, D. B. J. Baloga, S. M. Cahill, J. T. S. Glaze, L. S. Patterson, G. W. Raney, R. K. Thompson, T. W. Thomson, B. J. Ustinov, E. A. TI Evidence for water ice on the moon: Results for anomalous polar craters from the LRO Mini-RF imaging radar SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Moon; poles; radar; ice; water ID LUNAR SOUTH-POLE; OUTER PLANET SATELLITES; COHERENT-BACKSCATTER; GALILEAN SATELLITES; HYDROGEN DEPOSITS; NORTH-POLE; CLEMENTINE; MERCURY; IMAGES; STABILITY AB The Mini-RF radar instrument on the Lunar Reconnaissance Orbiter spacecraft mapped both lunar poles in two different RF wavelengths (complete mapping at 12.6 cm S-band and partial mapping at 4.2 cm X-band) in two look directions, removing much of the ambiguity of previous Earth- and spacecraft-based radar mapping of the Moon's polar regions. The poles are typical highland terrain, showing expected values of radar cross section (albedo) and circular polarization ratio (CPR). Most fresh craters display high values of CPR in and outside the crater rim; the pattern of these CPR distributions is consistent with high levels of wavelength-scale surface roughness associated with the presence of block fields, impact melt flows, and fallback breccia. A different class of polar crater exhibits high CPR only in their interiors, interiors that are both permanently dark and very cold (less than 100 K). Application of scattering models developed previously suggests that these anomalously high-CPR deposits exhibit behavior consistent with the presence of water ice. If this interpretation is correct, then both poles may contain several hundred million tons of water in the form of relatively clean ice, all within the upper couple of meters of the lunar surface. The existence of significant water ice deposits enables both long-term human habitation of the Moon and the creation of a permanent cislunar space transportation system based upon the harvest and use of lunar propellant. C1 [Spudis, P. D.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Bussey, D. B. J.; Cahill, J. T. S.; Patterson, G. W.; Raney, R. K.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Baloga, S. M.] Proxemy Res, Laytonville, MD USA. [Glaze, L. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Thompson, T. W.; Ustinov, E. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Thomson, B. J.] Boston Univ, Ctr Remote Sensing, Boston, MA 02215 USA. RP Spudis, PD (reprint author), Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA. EM spudis@lpi.usra.edu RI Glaze, Lori/D-1314-2012; Ustinov, Eugene/D-1350-2015; Cahill, Joshua/I-3656-2012; Patterson, Gerald/E-7699-2015 OI Ustinov, Eugene/0000-0003-0227-4286; Cahill, Joshua/0000-0001-6874-5533; FU NASA Operations Mission Directorate; NASA NLSI Polar Science Team of The Johns Hopkins University Applied Physics Laboratory; LRO Science Team; National Aeronautics and Space Administration FX We thank the former NASA Operations Mission Directorate (Associate Administrator W. Readdy, R. Spearing, and J. Crusan) for initially funding the Mini-RF project and for critical support at several points in our long journey back to the Moon. This work was partly supported by the NASA NLSI Polar Science Team of The Johns Hopkins University Applied Physics Laboratory (Ben Bussey, PI) and by the LRO Science Team. Work carried out at the Jet Propulsion Laboratory, California Institute of Technology, (T. Thompson and E. Ustinov) was under a contract with the National Aeronautics and Space Administration. This work is Lunar and Planetary Institute Contribution Number 1751. NR 63 TC 23 Z9 26 U1 1 U2 15 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 OCT PY 2013 VL 118 IS 10 BP 2016 EP 2029 DI 10.1002/jgre.20156 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 252RJ UT WOS:000327026900006 ER PT J AU Heuer, AH Nakagawa, T Azar, MZ Hovis, PB Smialek, JL Gleeson, B Hine, NDM Guhl, H Lee, HS Tangney, P Foulkes, WMC Finnis, MW AF Heuer, A. H. Nakagawa, T. Azar, M. Z. Hovis, P. B. Smialek, J. L. Gleeson, B. Hine, N. D. M. Guhl, H. Lee, H. -S. Tangney, P. Foulkes, W. M. C. Finnis, M. W. TI On the growth of Al2O3 scales SO ACTA MATERIALIA LA English DT Article DE Oxidation; Alumina; Scales ID OXYGEN POTENTIAL GRADIENTS; HIGH-TEMPERATURE OXIDATION; ALUMINA SCALES; TRANSIENT OXIDATION; VACANCY INJECTION; GRAIN-BOUNDARIES; VOID FORMATION; OXIDE SCALE; TRANSPORT; ALLOYS AB Understanding the growth of Al2O3 scales requires knowledge of the details of the chemical reactions at the scale-gas and scale-metal interfaces, which in turn requires specifying how the creation/annihilation of 0 and Al vacancies occurs at these interfaces. The availability of the necessary electrons and holes to allow for such creation/annihilation is a crucial aspect of the scaling reaction. The electronic band structure of polycrystalline Al2O3 thus plays a decisive role in scale formation and is considered in detail, including the implications of a density functional theory (DFT) calculation of the band structure of a Sigma 7 {4 (5) over bar1 0} bicrystal boundary, for which the atomic structure of the boundary was known from an independent DFT energy-minimization calculation and comparisons with an atomic-resolution transmission electron micrograph of the same boundary. DFT calculations of the formation energy of 0 and Al vacancies in bulk Al(2)O(3)in various charge states as a function of the Fermi energy suggested that electronic conduction in Al2O3 scales most likely involves excitation of both electrons and holes, which are localized on singly charged 0 vacancies, V-o and doubly charged Al vacancies, VI, respectively. We also consider the variation of the Fermi level across the scale and bending ("tilting") of the conduction band minimum and valence band maximum due to the electric field developed during the scaling reaction. The band structure calculations suggest a new mechanism for the "reactive element" effect a consequence of segregation of Y, Hf, etc., to grain boundaries in Al2O3 scales, which results in improved oxidation resistance namely, that the effect is due to the modification of the near-band edge grain-boundary defect states rather than any blocking of diffusion pathways, as previously postulated. Secondly, Al2O3 scale formation is dominated by grain boundary as opposed to lattice diffusion, and there is unambiguous evidence for both 0 and Al countercurrent transport in Al2O3 scale-forming alloys. We postulate that such transport is mediated by migration of grain boundary disconnections containing charged jogs, rather than by jumping of isolated point defects in random high-angle grain boundaries. (C) 2013 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved. C1 [Heuer, A. H.; Nakagawa, T.; Azar, M. Z.; Hovis, P. B.] Case Western Reserve Univ, Dept Mat Sci & Engn, Cleveland, OH 44106 USA. [Smialek, J. L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Gleeson, B.] Univ Pittsburgh, Dept Mech Engn & Mat Sci, Pittsburgh, PA 15261 USA. [Heuer, A. H.; Hine, N. D. M.; Guhl, H.; Lee, H. -S.; Tangney, P.; Finnis, M. W.] Univ London Imperial Coll Sci Technol & Med, Dept Mat, London SW7 2AZ, England. [Hine, N. D. M.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Guhl, H.; Lee, H. -S.; Tangney, P.; Foulkes, W. M. C.; Finnis, M. W.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England. RP Heuer, AH (reprint author), Case Western Reserve Univ, Dept Mat Sci & Engn, Cleveland, OH 44106 USA. EM heuer@case.edu RI Hine, Nicholas/D-4109-2011; OI Hine, Nicholas/0000-0001-5613-3679; Foulkes, Matthew/0000-0001-8359-1122 FU Leverhulme Trust [F/07058/BS]; Office of Naval Research Global; EPSRC [EP/F067496]; Office of Science and Technology through EPSRC's High End Computing Programme FX The research at CWRU and the University of Pittsburgh was supported by the Office of Naval Research (ONR), Dr. David Shifler, Program Manager; while that at Imperial College, London was supported by The Leverhulme Trust Grant F/07058/BS and the Office of Naval Research Global. This work made use of facilities provided by the Imperial College London High Performance Computing Service. Via our membership of the UK's HPC Materials Chemistry Consortium, which is funded by the EPSRC (EP/F067496), this work also made use of the facilities of HECToR, the UK's national high-performance computing service, provided by UoE HPCx Ltd. at the University of Edinburgh, Cray Inc. and NAG Ltd., and funded by the Office of Science and Technology through EPSRC's High End Computing Programme. NR 49 TC 26 Z9 26 U1 8 U2 101 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 OCT PY 2013 VL 61 IS 18 BP 6670 EP 6683 DI 10.1016/j.actamat.2013.07.024 PG 14 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 241ZL UT WOS:000326207100003 ER PT J AU Zaretsky, EV Chiu, YP Tallian, TE AF Zaretsky, Erwin V. Chiu, Y. P. Tallian, T. E. TI Ceramic Bearings for Use in Gas Turbine Engines SO JOURNAL OF MATERIALS ENGINEERING AND PERFORMANCE LA English DT Article AB Three decades of research by U.S. industry and government laboratories have produced a vast array of data related to the use of ceramic rolling element bearings and bearing components for aircraft gas turbine engines. Materials such as alumina, silicon carbide, titanium carbide, silicon nitride, and a crystallized glass ceramic have been investigated. Rolling element endurance tests and analysis of full complement bearings have been performed. Materials and bearing design methods have continuously improved over the years. This paper reviews a wide range of data and analyses with emphasis on how early NASA contributions as well as more recent data can enable the engineer or metallurgist to determine just where ceramic bearings are most applicable for gas turbines. C1 [Zaretsky, Erwin V.] NASA, Lewis Res Ctr, Cleveland, OH 44135 USA. [Chiu, Y. P.] Torrington Co, Adv Technol Ctr, Torrington, CT 06790 USA. [Tallian, T. E.] Tallian Consulting Co, Newtown Sq, PA 19073 USA. RP Zaretsky, EV (reprint author), NASA, Lewis Res Ctr, Cleveland, OH 44135 USA. NR 3 TC 0 Z9 0 U1 2 U2 14 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 OCT PY 2013 VL 22 IS 10 BP 2830 EP 2846 DI 10.1007/s11665-013-0726-5 PG 17 WC Materials Science, Multidisciplinary SC Materials Science GA 245HW UT WOS:000326455600006 ER PT J AU Ziparo, F Popesso, P Biviano, A Finoguenov, A Wuyts, S Wilman, D Salvato, M Tanaka, M Ilbert, O Nandra, K Lutz, D Elbaz, D Dickinson, M Altieri, B Aussel, H Berta, S Cimatti, A Fadda, D Genzel, R Le Flo'ch, E Magnelli, B Nordon, R Poglitsch, A Pozzi, F Portal, MS Tacconi, L Bauer, FE Brandt, WN Cappelluti, N Cooper, MC Mulchaey, JS AF Ziparo, F. Popesso, P. Biviano, A. Finoguenov, A. Wuyts, S. Wilman, D. Salvato, M. Tanaka, M. Ilbert, O. Nandra, K. Lutz, D. Elbaz, D. Dickinson, M. Altieri, B. Aussel, H. Berta, S. Cimatti, A. Fadda, D. Genzel, R. Le Flo'ch, E. Magnelli, B. Nordon, R. Poglitsch, A. Pozzi, F. Sanchez Portal, M. Tacconi, L. Bauer, F. E. Brandt, W. N. Cappelluti, N. Cooper, M. C. Mulchaey, J. S. TI The lack of star formation gradients in galaxy groups up to z similar to 1.6 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: groups: general; galaxies: evolution; galaxies: stellar content; infrared: galaxies; X-rays: galaxies: clusters; galaxies: star formation ID DEEP FIELD-SOUTH; DIGITAL-SKY-SURVEY; INFRARED LUMINOSITY FUNCTIONS; FORMATION-DENSITY RELATION; HIGH-REDSHIFT GALAXIES; GOODS-MUSIC SAMPLE; YALE-CHILE MUSYC; X-RAY SOURCES; COSMOS FIELD; FORMATION HISTORY AB In the local Universe, galaxy properties show a strong dependence on environment. In cluster cores, early-type galaxies dominate, whereas star-forming galaxies are more and more common in the outskirts. At higher redshifts and in somewhat less dense environments (e.g. galaxy groups), the situation is less clear. One open issue is that of whether and how the star formation rate (SFR) of galaxies in groups depends on the distance from the centre of mass. To shed light on this topic, we have built a sample of X-ray selected galaxy groups at 0 < z < 1.6 in various blank fields [Extended Chandra Deep Field South (ECDFS), Cosmological Evolution Survey (COSMOS), Great Observatories Origin Deep Survey (GOODS)]. We use a sample of spectroscopically confirmed group members with stellar mass M-star > 10(10.3) M-circle dot in order to have a high spectroscopic completeness. As we use only spectroscopic redshifts, our results are not affected by uncertainties due to projection effects. We use several SFR indicators to link the star formation (SF) activity to the galaxy environment. Taking advantage of the extremely deep mid-infrared Spitzer MIPS and far-infrared Herschel(1) PACS observations, we have an accurate, broad-band measure of the SFR for the bulk of the star-forming galaxies. We use multi-wavelength Spectral Energy Distribution (SED) fitting techniques to estimate the stellar masses of all objects and the SFR of the MIPS and PACS undetected galaxies. We analyse the dependence of the SF activity, stellar mass and specific SFR on the group-centric distance, up to z similar to 1.6, for the first time. We do not find any correlation between the mean SFR and group-centric distance at any redshift. We do not observe any strong mass segregation either, in agreement with predictions from simulations. Our results suggest that either groups have a much smaller spread in accretion times with respect to the clusters and that the relaxation time is longer than the group crossing time. C1 [Ziparo, F.; Popesso, P.; Finoguenov, A.; Wuyts, S.; Wilman, D.; Salvato, M.; Nandra, K.; Lutz, D.; Berta, S.; Genzel, R.; Poglitsch, A.; Tacconi, L.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Ziparo, F.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Biviano, A.] INAF Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Finoguenov, A.] Univ Helsinki, Dept Phys, Helsinki 00014, Finland. [Finoguenov, A.; Cappelluti, N.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Tanaka, M.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Ilbert, O.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Elbaz, D.; Aussel, H.; Le Flo'ch, E.] Univ Paris Diderot, Lab AIM, CEA, DSM,CNRS,IFRU,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Dickinson, M.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Altieri, B.; Sanchez Portal, M.] ESA, European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain. [Cimatti, A.; Pozzi, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Fadda, D.] NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. [Magnelli, B.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Nordon, R.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Bauer, F. E.] Pontificia Univ Catllica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Cappelluti, N.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Cooper, M. C.] Univ Calif Irvine, Dept Phys & Astron, Ctr Galaxy Evolut, Irvine, CA 92697 USA. [Mulchaey, J. S.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. RP Ziparo, F (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. EM fziparo@star.sr.bham.ac.uk RI Brandt, William/N-2844-2015; OI Brandt, William/0000-0002-0167-2453; Altieri, Bruno/0000-0003-3936-0284 FU KAKENHI [23740144]; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT 1101024, ALMA-CONICYT 31100004, Anillo ACT1101]; Chandra X-ray Center [SAO SP1-12007B]; BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI (Italy); CICYT/MCYT (Spain); NASA; SDSS; Sloan Foundation; NSF; US Department of Energy; Japanese Monbukagakusho; Max-Planck Society; Higher Education Funding Council of England; SAO grant [SP112006B] FX MT gratefully acknowledges support by KAKENHI No. 23740144.; FEB acknowledges support from Basal-CATA (PFB-06/2007), CONICYT-Chile (under grants FONDECYT 1101024, ALMA-CONICYT 31100004 and Anillo ACT1101) and Chandra X-ray Center grant SAO SP1-12007B.; PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI (Italy) and CICYT/MCYT (Spain).; This research has made use of NASA's Astrophysics Data System, of NED, which is operated by JPL/Caltech, under contract with NASA, and of SDSS, which has been funded by the Sloan Foundation, NSF, the US Department of Energy, NASA, the Japanese Monbukagakusho, the Max-Planck Society and the Higher Education Funding Council of England. The SDSS is managed by the participating institutions (www.sdss.org/collaboration/credits.html).; This work has been partially supported by a SAO grant SP112006B grant to UMBC. NR 106 TC 22 Z9 22 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 OCT PY 2013 VL 434 IS 4 BP 3089 EP 3103 DI 10.1093/mnras/stt1222 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 229KK UT WOS:000325262300032 ER PT J AU Ibar, E Sobral, D Best, PN Ivison, RJ Smail, I Arumugam, V Berta, S Bethermin, M Bock, J Cava, A Conley, A Farrah, D Geach, J Ikarashi, S Kohno, K Le Floc'h, E Lutz, D Magdis, G Magnelli, B Marsden, G Oliver, SJ Page, MJ Pozzi, F Riguccini, L Schulz, B Seymour, N Smith, AJ Symeonidis, M Wang, L Wardlow, J Zemcov, M AF Ibar, E. Sobral, D. Best, P. N. Ivison, R. J. Smail, I. Arumugam, V. Berta, S. Bethermin, M. Bock, J. Cava, A. Conley, A. Farrah, D. Geach, J. Ikarashi, S. Kohno, K. Le Floc'h, E. Lutz, D. Magdis, G. Magnelli, B. Marsden, G. Oliver, S. J. Page, M. J. Pozzi, F. Riguccini, L. Schulz, B. Seymour, N. Smith, A. J. Symeonidis, M. Wang, L. Wardlow, J. Zemcov, M. TI Herschel reveals the obscured star formation in HiZELS H alpha emitters at z=1.47 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: high-redshift; galaxies: starburst; galaxies: star formation; galaxies: statistics; infrared: galaxies; submillimetre: galaxies ID SIMILAR-TO 1; SCIENCE DEMONSTRATION PHASE; FORMATION RATE INDICATORS; HUBBLE-SPACE-TELESCOPE; FORMATION RATE DENSITY; HIGH-REDSHIFT SURVEY; DIGITAL SKY SURVEY; FORMING GALAXIES; FORMATION RATES; COSMOS FIELD AB We describe the far-infrared (far-IR; rest-frame 8-1000-mu m) properties of a sample of 443 H alpha-selected star-forming galaxies in the Cosmic Evolution Survey (COSMOS) and Ultra Deep Survey (UDS) fields detected by the High-redshift Emission Line Survey (HiZELS) imaging survey. Sources are identified using narrow-band filters in combination with broad-band photometry to uniformly select H alpha (and [O ii] if available) emitters in a narrow redshift slice at z = 1.47 +/- 0.02. We use a stacking approach in Spitzer-MIPS mid-IR, Herschel-PACS/SPIRE far-IR [from the PACS Evolutionary Prove (PEP) and Herschel Multi-tiered Extragalactic Survey (HerMES)] and AzTEC mm-wave images to describe their typical far-IR properties. We find that HiZELS galaxies with observed H alpha luminosities of L(H alpha)(obs) approximate to 10(8.1-9.1) L-circle dot ( approximate to 10(41.7-42.7) erg s(-1)) have bolometric far-IR luminosities of typical luminous IR galaxies, L(8-1000 mu m) approximate to 10(-0.006)(11.41)(+0.04) L-circle dot. Combining the H alpha and far-IR luminosities, we derive median star formation rates (SFRs) of SFRH alpha, FIR = 32 +/- 5 M-circle dot yr(-1) and H alpha extinctions of A(H alpha) = 1.0 +/- 0.2 mag. Perhaps surprisingly, little difference is seen in typical HiZELS extinction levels compared to local star-forming galaxies. We confirm previous empirical stellar mass (M-*) to A(H alpha) relations and the little or no evolution up to z = 1.47. For HiZELS galaxies (or similar samples) we provide an empirical parametrization of the SFR as a function of rest-frame (u - z) colours and 3.6-mu m photometry - a useful proxy to aid in the absence of far-IR detections in high-z galaxies. We find that the observed H alpha luminosity is a dominant SFR tracer when rest-frame (u - z) colours are less than or similar to 0.9 mag or when Spitzer-3.6-mu m photometry is fainter than 22 mag (Vega) or when stellar masses are lower than 10(9.7) M-circle dot. We do not find any correlation between the [O ii]/H alpha and far-IR luminosity, suggesting that this emission line ratio does not trace the extinction of the most obscured star-forming regions, especially in massive galaxies where these dominate. The luminosity-limited HiZELS sample tends to lie above of the so-called main sequence for star-forming galaxies, especially at low stellar masses, indicating high star formation efficiencies in these galaxies. This work has implications for SFR indicators and suggests that obscured star formation is linked to the assembly of stellar mass, with deeper potential wells in massive galaxies providing dense, heavily obscured environments in which stars can form rapidly. C1 [Ibar, E.; Ivison, R. J.] Royal Observ, Sci & Technol Facil Council, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ibar, E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Sobral, D.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Best, P. N.; Ivison, R. J.; Arumugam, V.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Smail, I.; Wang, L.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Berta, S.; Lutz, D.; Magnelli, B.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Bethermin, M.; Le Floc'h, E.; Magdis, G.; Riguccini, L.] Univ Paris Diderot, CNRS, CEA DSM Irfu, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. [Bethermin, M.] Univ Paris 11, IAS, F-91405 Orsay, France. [Bethermin, M.] CNRS, UMR 8617, F-91405 Orsay, France. [Bock, J.; Schulz, B.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.; Riguccini, L.] Jet Prop Lab, Pasadena, CA 91109 USA. [Cava, A.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain. [Conley, A.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Farrah, D.; Oliver, S. J.; Smith, A. J.; Wang, L.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Geach, J.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Ikarashi, S.; Kohno, K.] Univ Tokyo, Inst Astron, Mitaka, Tokyo 1810015, Japan. [Kohno, K.] Univ Tokyo, Res Ctr Early Universe, Tokyo 1130033, Japan. [Marsden, G.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Page, M. J.; Seymour, N.; Symeonidis, M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Pozzi, F.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Schulz, B.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Seymour, N.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Wardlow, J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. RP Ibar, E (reprint author), Royal Observ, Sci & Technol Facil Council, UK Astron Technol Ctr, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. EM edoibar.puc@gmail.com RI Magdis, Georgios/C-7295-2014; Smail, Ian/M-5161-2013; Sobral, David/C-7919-2014; Wardlow, Julie/C-9903-2015; Ivison, R./G-4450-2011; Cava, Antonio/C-5274-2017 OI Seymour, Nicholas/0000-0003-3506-5536; Magdis, Georgios/0000-0002-4872-2294; Smail, Ian/0000-0003-3037-257X; Sobral, David/0000-0001-8823-4845; Wardlow, Julie/0000-0003-2376-8971; Ivison, R./0000-0001-5118-1313; Cava, Antonio/0000-0002-4821-1275 FU Netherland Organization for Scientific research (NWO) through a Veni fellowship; STFC; Leverhulme Fellowship; ERC Advanced Investigator programme DUSTYGAL; Royal Society/Wolfson Merit Award; ERC; ERC Advanced Investigator programme, COSMI-CISM; CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA); BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); CICYT/MCYT (Spain); NASA FX We thank the anonymous referee for the useful comments that helped improve this paper. EI agradece el financiamento de CONICYT/FONDECYT por el proyecto de postdoctorado No: 3130504. DS acknowledges financial support from the Netherland Organization for Scientific research (NWO) through a Veni fellowship. IS acknowledges support from STFC, a Leverhulme Fellowship, the ERC Advanced Investigator programme DUSTYGAL and a Royal Society/Wolfson Merit Award. RJI acknowledges support in the form of ERC Advanced Investigator programme, COSMI-CISM. The HiZELS data are based on observations obtained using both the Wide Field Camera on the 3.8-m United Kingdom Infrared Telescope (operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK) and Suprime-Cam on the 8.2-m Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. This research has made use of data from the HerMES project (http://hermes.sussex.ac.uk/). HerMES is a Herschel Key Programme utilizing Guaranteed Time from the SPIRE instrument team, ESAC scientists and a mission scientist. The data presented in this paper will be released through the HerMES database in Marseille, HeDaM (http://hedam.oamp.fr/HerMES). 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); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI (Italy) and CICYT/MCYT (Spain). This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. NR 95 TC 30 Z9 30 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 OCT PY 2013 VL 434 IS 4 BP 3218 EP 3235 DI 10.1093/mnras/stt1258 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 229KK UT WOS:000325262300042 ER PT J AU Huitson, CM Sing, DK Pont, F Fortney, JJ Burrows, AS Wilson, PA Ballester, GE Nikolov, N Gibson, NP Deming, D Aigrain, S Evans, TM Henry, GW des Etangs, AL Showman, AP Vidal-Madjar, A Zahnle, K AF Huitson, C. M. Sing, D. K. Pont, F. Fortney, J. J. Burrows, A. S. Wilson, P. A. Ballester, G. E. Nikolov, N. Gibson, N. P. Deming, D. Aigrain, S. Evans, T. M. Henry, G. W. des Etangs, A. Lecavelier Showman, A. P. Vidal-Madjar, A. Zahnle, K. TI An HST optical-to-near-IR transmission spectrum of the hot Jupiter WASP-19b: detection of atmospheric water and likely absence of TiO SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: spectroscopic; planets and satellites: atmospheres; planets and satellites: individual: WASP-19b; stars: individual: WASP-19; planetary systems ID HUBBLE-SPACE-TELESCOPE; GIANT PLANET ATMOSPHERES; MASS DWARF STARS; GROUND-BASED DETECTION; EXOPLANET HD 189733B; LIGHT-CURVE PROJECT; EXTRASOLAR PLANET; BROWN DWARFS; TRANSITING PLANET; C/O RATIO AB We measure the transmission spectrum of WASP-19b from three transits using low-resolution optical spectroscopy from the Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph (STIS). The STIS spectra cover a wavelength range of 0.29-1.03 mu m, with resolving power R = 500. The optical data are combined with archival near-infrared data from the HST Wide Field Camera 3 (WFC3) G141 grism, covering the wavelength range from 1.087 to 1.687 mu m, with resolving power R = 130. We reach signal-to-noise levels between 3000 and 11 000 in 0.1 mu m bins when measuring the transmission spectra from 0.53-1.687 mu m. WASP-19 is known to be a very active star, with the optical stellar flux varying by a few per cent over time. We correct the transit light curves for the effects of stellar activity using ground-based activity monitoring with the Cerro Tololo Inter-American Observatory. While we were not able to construct a transmission spectrum using the blue optical data because of the presence of large occulted starspots, we were able to use the spot crossings to help constrain the mean stellar spot temperature. To search for predicted features in the hot-Jupiter atmosphere, in addition to the transmission spectrum we also define spectral indices for differential radius (delta R-P/R-star) measurements to specifically search for the presence of TiO and alkali line features. Our measurements rule out TiO features predicted for a planet of WASP-19b's equilibrium temperature (2050 K) in the transmission spectrum at the 2.7-2.9 Sigma confidence level, depending on atmospheric model formalism. The WFC3 transmission spectrum shows strong absorption features due to the presence of H2O, which is detected at the 4 Sigma confidence level between 1.1 and 1.4 mu m. The transmission spectra results indicate that WASP-19b is a planet with no or low levels of TiO and without a high C/O ratio. The lack of observable TiO features are possibly due to rainout, breakdown from stellar activity or the presence of other absorbers in the optical. C1 [Huitson, C. M.; Sing, D. K.; Pont, F.; Wilson, P. A.; Nikolov, N.] Univ Exeter, Sch Phys, Astrophys Grp, Exeter EX4 4QL, Devon, England. [Fortney, J. J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Burrows, A. S.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Ballester, G. E.; Showman, A. P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Gibson, N. P.; Aigrain, S.; Evans, T. M.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Gibson, N. P.] European So Observ, D-85748 Garching, Germany. [Deming, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Henry, G. W.] Tennessee State Univ, Nashville, TN 37209 USA. [des Etangs, A. Lecavelier; Vidal-Madjar, A.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Zahnle, K.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Huitson, CM (reprint author), Univ Exeter, Sch Phys, Astrophys Grp, Stocker Rd, Exeter EX4 4QL, Devon, England. EM chuitson@astro.ex.ac.uk RI Nikolov, Nikolay/H-6183-2015; OI Nikolov, Nikolay/0000-0002-6500-3574; HUITSON, CATHERINE/0000-0002-4734-691X; Sing, David /0000-0001-6050-7645; Fortney, Jonathan/0000-0002-9843-4354; Gibson, Neale/0000-0002-9308-2353 FU National Science Foundation; STFC [ST/J001627/1]; NASA [HST-GO-12473] FX This work is based on observations with the NASA/ESA Hubble Space Telescope. This work makes use of data from the Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy, under contract with the National Science Foundation. We thank the anonymous referee for a thorough and thoughtful report. CMH and PAW acknowledge support from STFC. This research has made use of NASA's Astrophysics Data System, and components of the IDL astronomy library. The authors acknowledge support by NASA through grant HST-GO-12473. DKS and NN acknowledge support from STFC consolidated Grant ST/J001627/1. NR 80 TC 57 Z9 57 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 OCT PY 2013 VL 434 IS 4 BP 3252 EP 3274 DI 10.1093/mnras/stt1243 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 229KK UT WOS:000325262300045 ER PT J AU Iizumi, T Sakuma, H Yokozawa, M Luo, JJ Challinor, AJ Brown, ME Sakurai, G Yamagata, T AF Iizumi, Toshichika Sakuma, Hirofumi Yokozawa, Masayuki Luo, Jing-Jia Challinor, Andrew J. Brown, Molly E. Sakurai, Gen Yamagata, Toshio TI Prediction of seasonal climate-induced variations in global food production SO NATURE CLIMATE CHANGE LA English DT Article ID FORECASTS; AGRICULTURE; UNCERTAINTY; CHALLENGES; ADAPTATION AB Consumers, including the poor in many countries, are increasingly dependent on food imports(1) and are thus exposed to variations in yields, production and export prices in the major food-producing regions of the world. National governments and commercial entities are therefore paying increased attention to the cropping forecasts of important food-exporting countries as well as to their own domestic food production. Given the increased volatility of food markets and the rising incidence of climatic extremes affecting food production, food price spikes may increase in prevalence in future years(2-4). Here we present a global assessment of the reliability of crop failure hindcasts for major crops at two lead times derived by linking ensemble seasonal climatic forecasts with statistical crop models. We found that moderate-to-marked yield loss over a substantial percentage (26-33%) of the harvested area of these crops is reliably predictable if climatic forecasts are near perfect. However, only rice and wheat production are reliably predictable at three months before the harvest using within-season hindcasts. The reliabilities of estimates varied substantially by crop-rice and wheat yields were the most predictable, followed by soybean and maize. The reasons for variation in the reliability of the estimates included the differences in crop sensitivity to the climate and the technology used by the crop-producing regions. Our findings reveal that the use of seasonal climatic forecasts to predict crop failures will be useful for monitoring global food production and will encourage the adaptation of food systems to climatic extremes. C1 [Iizumi, Toshichika; Yokozawa, Masayuki; Sakurai, Gen] Natl Inst Agroenvironm Sci, Tsukuba, Ibaraki 3058604, Japan. [Sakuma, Hirofumi] JAMSTEC, Yokohama Inst Earth Sci, Res Inst Global Change, Yokohama, Kanagawa 2360001, Japan. [Sakuma, Hirofumi; Yamagata, Toshio] JAMSTEC, Yokohama Inst Earth Sci, Applicat Lab, Yokohama, Kanagawa 2360001, Japan. [Luo, Jing-Jia] Bur Meteorol, Ctr Australian Weather & Climate Res, Melbourne, Vic 3008, Australia. [Challinor, Andrew J.] Univ Leeds, Sch Earth & Environm, Inst Climate & Atmospher Sci, Leeds LS2 9JT, W Yorkshire, England. [Challinor, Andrew J.] Univ Copenhagen, Fac Sci, Dept Plant & Environm Sci, CGIAR ESSP Program Climate Change Agr & Food Secu, DK-1958 Frederiksberg, Denmark. [Brown, Molly E.] NASA, Biospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Iizumi, T (reprint author), Natl Inst Agroenvironm Sci, Tsukuba, Ibaraki 3058604, Japan. EM iizumit@affrc.go.jp RI Luo, Jing-Jia/B-2481-2008; Yamagata, Toshio/A-1807-2009; Brown, Molly/M-5146-2013; Yokozawa, Masayuki/O-2829-2014; Challinor, Andrew/C-4992-2008; Brown, Molly/E-2724-2010 OI Luo, Jing-Jia/0000-0003-2181-0638; Brown, Molly/0000-0001-7384-3314; Yokozawa, Masayuki/0000-0001-7053-2465; Challinor, Andrew/0000-0002-8551-6617; Brown, Molly/0000-0001-7384-3314 FU Japan Society for the Promotion of Science (JSPS) [23880030]; Ministry of the Environment, Japan [S-10-2] FX We thank R.C. Stone, P. McIntosh, H. Kanamaru and M. Otsuka for helpful comments on the earlier version of this manuscript. T.I. was supported by the Japan Society for the Promotion of Science (JSPS) Grant-in-Aid for Research Activity Start-up (23880030). T.I, M.Y. and G.S. were supported by the Environment Research and Technology Development Fund (S-10-2) of the Ministry of the Environment, Japan. The Science and Innovation Section of the British Embassy in Tokyo provided us with the opportunity to conduct this study through a UK-Japan workshop arrangement. NR 28 TC 26 Z9 26 U1 5 U2 58 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 OCT PY 2013 VL 3 IS 10 BP 904 EP 908 DI 10.1038/NCLIMATE1945 PG 5 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 249ZE UT WOS:000326818800017 ER PT J AU Strycker, PD Chanover, NJ Miller, C Hamilton, RT Hermalyn, B Suggs, RM Sussman, M AF Strycker, Paul D. Chanover, Nancy J. Miller, Charles Hamilton, Ryan T. Hermalyn, Brendan Suggs, Robert M. Sussman, Michael TI Characterization of the LCROSS impact plume from a ground-based imaging detection SO NATURE COMMUNICATIONS LA English DT Article ID LUNAR POLES; WATER ICE AB The Lunar CRater Observation and Sensing Satellite (LCROSS) mission was designed to search for evidence of water in a permanently shadowed region near the lunar south pole. An instrumented Shepherding Spacecraft followed a kinetic impactor and provided - from a nadir perspective - the only images of the debris plume. With independent observations of the visible debris plume from a more oblique view, the angles and velocities of the ejecta from this unique cratering experiment are better constrained. Here we report the first visible observations of the LCROSS ejecta plume from Earth, thereby ascertaining the morphology of the plume to contain a minimum of two separate components, placing limits on ejecta velocities at multiple angles, and permitting an independent estimate of the illuminated ejecta mass. Our mass estimate implies that the lunar volatile inventory in the Cabeus permanently shadowed region includes a water concentration of 6.3+/-1.6% by mass. C1 [Strycker, Paul D.] Univ Wisconsin Platteville, Dept Engn Phys, Platteville, WI 53818 USA. [Chanover, Nancy J.; Miller, Charles; Hamilton, Ryan T.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Hermalyn, Brendan] Univ Hawaii, Hawaii Space Flight Lab SOEST, Honolulu, HI 96822 USA. [Suggs, Robert M.] NASA Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Sussman, Michael] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Strycker, PD (reprint author), Univ Wisconsin Platteville, Dept Engn Phys, Platteville, WI 53818 USA. EM stryckerp@uwplatt.edu FU Universities Space Research Association [03450-32]; NASA [NNX08AF53A]; NASA through the NASA Astrobiology Institute under Office of Space Science [NNA09DA77A]; NASA Meteoroid Environment Office FX We thank L. Boucheron for critical discussions and T. McClanahan and E. Wright for the lunar renderings used for the validation of our PCA algorithms. This work was supported by contract number 03450-32 from the Universities Space Research Association and NASA grant number NNX08AF53A. B. Hermalyn was supported by NASA through the NASA Astrobiology Institute under Cooperative Agreement no. NNA09DA77A issued through the Office of Space Science. R. Suggs acknowledges partial support from the NASA Meteoroid Environment Office. NR 21 TC 2 Z9 2 U1 1 U2 4 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 OCT PY 2013 VL 4 AR UNSP 2620 DI 10.1038/ncomms3620 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 245OE UT WOS:000326472200009 PM 24135963 ER PT J AU Shebalin, JV AF Shebalin, John V. TI Global invariants in ideal magnetohydrodynamic turbulence SO PHYSICS OF PLASMAS LA English DT Article ID MEAN MAGNETIC-FIELD; BROKEN ERGODICITY; HOMOGENEOUS TURBULENCE; ISOTROPIC TURBULENCE; NUMERICAL-SIMULATION; ABSOLUTE EQUILIBRIUM; HELICITY; DYNAMO AB Magnetohydrodynamic (MHD) turbulence is an important though incompletely understood factor affecting the dynamics of many astrophysical, geophysical, and technological plasmas. As an approximation, viscosity and resistivity may be ignored, and ideal MHD turbulence may be investigated by statistical methods. Incompressibility is also assumed and finite Fourier series are used to represent the turbulent velocity and magnetic field. The resulting model dynamical system consists of a set of independent Fourier coefficients that form a canonical ensemble described by a Gaussian probability density function (PDF). This PDF is similar in form to that of Boltzmann, except that its argument may contain not just the energy multiplied by an inverse temperature, but also two other invariant integrals, the cross helicity and magnetic helicity, each multiplied by its own inverse temperature. However, the cross and magnetic helicities, as usually defined, are not invariant in the presence of overall rotation or a mean magnetic field, respectively. Although the generalized form of the magnetic helicity is known, a generalized cross helicity may also be found, by adding terms that are linear in the mean magnetic field and angular rotation vectors, respectively. These general forms are invariant even in the presence of overall rotation and a mean magnetic field. We derive these general forms, explore their properties, examine how they extend the statistical theory of ideal MHD turbulence, and discuss how our results may be affected by dissipation and forcing. C1 NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA. RP Shebalin, JV (reprint author), NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA. NR 36 TC 2 Z9 2 U1 0 U2 6 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD OCT PY 2013 VL 20 IS 10 AR 102305 DI 10.1063/1.4824009 PG 15 WC Physics, Fluids & Plasmas SC Physics GA 247TK UT WOS:000326644100046 ER PT J AU Clark, G Allegrini, F Randol, BM McComas, DJ Louarn, P AF Clark, G. Allegrini, F. Randol, B. M. McComas, D. J. Louarn, P. TI Response in electrostatic analyzers due to backscattered electrons: Case study analysis with the Juno Jovian Auroral Distribution Experiment-Electron instrument SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID PLASMA INSTRUMENT; SOLID TARGETS; SOLAR-WIND; ENERGY; PENETRATION; FLIGHT AB In this study, we introduce a model to characterize electron scattering in an electrostatic analyzer. We show that electrons between 0.5 and 30 keV scatter from internal surfaces to produce a response up to similar to 20% of the ideal, unscattered response. We compare our model results to laboratory data from the Jovian Auroral Distribution Experiment-Electron sensor onboard the NASA Juno mission. Our model reproduces the measured energy-angle response of the instrument well. Understanding and quantifying this scattering process is beneficial to the analysis of scientific data as well as future instrument optimization. (C) 2013 AIP Publishing LLC. C1 [Clark, G.; Allegrini, F.; McComas, D. J.] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX 78249 USA. [Clark, G.; Allegrini, F.; McComas, D. J.] SW Res Inst, Space Sci & Engn Div, San Antonio, TX 78238 USA. [Randol, B. M.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20071 USA. [Louarn, P.] Univ Toulouse 3, Inst Rech Astrophys & Planetol, F-31028 Toulouse, France. [Louarn, P.] CNRS, UMR5277, F-31028 Toulouse 4, France. RP Clark, G (reprint author), Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX 78249 USA. RI Clark, George/L-6433-2015 NR 33 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0034-6748 EI 1089-7623 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD OCT PY 2013 VL 84 IS 10 AR 105109 DI 10.1063/1.4824352 PG 9 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 247TS UT WOS:000326645300074 PM 24182165 ER PT J AU Zheng, YH Macneice, P Odstrcil, D Mays, ML Rastaetter, L Pulkkinen, A Taktakishvili, A Hesse, M Kuznetsova, MM Lee, H Chulaki, A AF Zheng, Yihua Macneice, Peter Odstrcil, Dusan Mays, M. L. Rastaetter, Lutz Pulkkinen, Antti Taktakishvili, Aleksandre Hesse, Michael Kuznetsova, M. Masha Lee, Hyesook Chulaki, Anna TI Forecasting propagation and evolution of CMEs in an operational setting: What has been learned SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE coronal mass ejection; forecasting; space weather ID CORONAL MASS EJECTIONS; ENERGETIC PARTICLE EVENTS; SOLAR-WIND; CONE MODEL; MAGNETIC RECONNECTION; MHD MODEL; ACCELERATION; DISTURBANCES; FLARES; SHOCKS AB One of the major types of solar eruption, coronal mass ejections (CMEs) not only impact space weather, but also can have significant societal consequences. CMEs cause intense geomagnetic storms and drive fast mode shocks that accelerate charged particles, potentially resulting in enhanced radiation levels both in ions and electrons. Human and technological assets in space can be endangered as a result. CMEs are also the major contributor to generating large amplitude Geomagnetically Induced Currents (GICs), which are a source of concern for power grid safety. Due to their space weather significance, forecasting the evolution and impacts of CMEs has become a much desired capability for space weather operations worldwide. Based on our operational experience at Space Weather Research Center at NASA Goddard Space Flight Center (http://swrc.gsfc.nasa.gov), we present here some of the insights gained about accurately predicting CME impacts, particularly in relation to space weather operations. These include: 1. The need to maximize information to get an accurate handle of three-dimensional (3-D) CME kinetic parameters and therefore improve CME forecast; 2. The potential use of CME simulation results for qualitative prediction of regions of space where solar energetic particles (SEPs) may be found; 3. The need to include all CMEs occurring within a similar to 24h period for a better representation of the CME interactions; 4. Various other important parameters in forecasting CME evolution in interplanetary space, with special emphasis on the CME propagation direction. It is noted that a future direction for our CME forecasting is to employ the ensemble modeling approach. C1 [Zheng, Yihua; Macneice, Peter; Odstrcil, Dusan; Mays, M. L.; Rastaetter, Lutz; Pulkkinen, Antti; Taktakishvili, Aleksandre; Hesse, Michael; Kuznetsova, M. Masha; Chulaki, Anna] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. [Odstrcil, Dusan] George Mason Univ, Fairfax, VA 22030 USA. [Mays, M. L.; Taktakishvili, Aleksandre] Catholic Univ Amer, NASA GSFC, Greenbelt, MD USA. [Lee, Hyesook] Korean Meteorol Adm, Seoul, South Korea. [Chulaki, Anna] Sigma Space Corp, Lanham, MD USA. RP Zheng, YH (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Code 674-0, Greenbelt, MD 20771 USA. EM Yihua.Zheng@nasa.gov RI feggans, john/F-5370-2012; Rastaetter, Lutz/D-4715-2012 OI Rastaetter, Lutz/0000-0002-7343-4147 NR 69 TC 14 Z9 14 U1 0 U2 13 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 OCT PY 2013 VL 11 IS 10 BP 557 EP 574 DI 10.1002/swe.20096 PG 18 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 251YL UT WOS:000326970600004 ER PT J AU Baker, DN Li, X Pulkkinen, A Ngwira, CM Mays, ML Galvin, AB Simunac, KDC AF Baker, D. N. Li, X. Pulkkinen, A. Ngwira, C. M. Mays, M. L. Galvin, A. B. Simunac, K. D. C. TI A major solar eruptive event in July 2012: Defining extreme space weather scenarios SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE extreme space weather; severe solar storm; worst case geomagnetic event ID 1-2 SEPTEMBER 1859; MAGNETIC STORM; AUGUST 1972; EARTH; MODEL; WIND; DST AB A key goal for space weather studies is to define severe and extreme conditions that might plausibly afflict human technology. On 23 July 2012, solar active region 1520 (similar to 141 degrees W heliographic longitude) gave rise to a powerful coronal mass ejection (CME) with an initial speed that was determined to be 2500500 km/s. The eruption was directed away from Earth toward 125 degrees W longitude. STEREO-A sensors detected the CME arrival only about 19 h later and made in situ measurements of the solar wind and interplanetary magnetic field. In this paper, we address the question of what would have happened if this powerful interplanetary event had been Earthward directed. Using a well-proven geomagnetic storm forecast model, we find that the 23-24 July event would certainly have produced a geomagnetic storm that was comparable to the largest events of the twentieth century (Dst=-500 nT). Using plausible assumptions about seasonal and time-of-day orientation of the Earth's magnetic dipole, the most extreme modeled value of storm-time disturbance would have been Dst=-1182 nT. This is considerably larger than estimates for the famous Carrington storm of 1859. This finding has far reaching implications because it demonstrates that extreme space weather conditions such as those during March of 1989 or September of 1859 can happen even during a modest solar activity cycle such as the one presently underway. We argue that this extreme event should immediately be employed by the space weather community to model severe space weather effects on technological systems such as the electric power grid. C1 [Baker, D. N.; Li, X.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA. [Pulkkinen, A.; Ngwira, C. M.; Mays, M. L.] NASA, Goddard Space Flight Ctr, Space Weather Res Ctr, Greenbelt, MD 20771 USA. [Ngwira, C. M.; Mays, M. L.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Galvin, A. B.; Simunac, K. D. C.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. RP Baker, DN (reprint author), Univ Colorado, Lab Atmospher & Space Phys, 3665 Discovery Dr, Boulder, CO 80303 USA. EM daniel.baker@lasp.colorado.edu FU NSF; Center for Integrated Space Weather Modeling (CISM) FX The authors appreciate useful suggestions by L.J. Lanzerotti, H.J. Singer, and R. L. McPherron. Thanks are also extended to G. Millward for modeling support. The authors are thankful for helpful discussions with M. Temerin in applying the TL06 model for this event. The authors also thank B.J. Thompson for useful discussions on the CME analysis. This work was supported by NSF grants including work supported by the Center for Integrated Space Weather Modeling (CISM). NR 30 TC 49 Z9 49 U1 1 U2 17 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 OCT PY 2013 VL 11 IS 10 BP 585 EP 591 DI 10.1002/swe.20097 PG 7 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 251YL UT WOS:000326970600006 ER PT J AU Mertens, CJ Meier, MM Brown, S Norman, RB Xu, XJ AF Mertens, Christopher J. Meier, Matthias M. Brown, Steven Norman, Ryan B. Xu, Xiaojing TI NAIRAS aircraft radiation model development, dose climatology, and initial validation SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE ionizing radiation; galactic cosmic rays; dosimetry ID GALACTIC COSMIC RAYS; EQUIVALENT PROPORTIONAL COUNTER; ADVANCED COMPOSITION EXPLORER; CONVERSION COEFFICIENTS; FLIGHT ATTENDANTS; SOLAR MODULATION; HELIOSPHERIC MODULATION; ADIABATIC DECELERATION; TISSUE-EQUIVALENT; SPACE EXPLORATION AB The Nowcast of Atmospheric Ionizing Radiation for Aviation Safety (NAIRAS) is a real-time, global, physics-based model used to assess radiation exposure to commercial aircrews and passengers. The model is a free-running physics-based model in the sense that there are no adjustment factors applied to nudge the model into agreement with measurements. The model predicts dosimetric quantities in the atmosphere from both galactic cosmic rays (GCR) and solar energetic particles, including the response of the geomagnetic field to interplanetary dynamical processes and its subsequent influence on atmospheric dose. The focus of this paper is on atmospheric GCR exposure during geomagnetically quiet conditions, with three main objectives. First, provide detailed descriptions of the NAIRAS GCR transport and dosimetry methodologies. Second, present a climatology of effective dose and ambient dose equivalent rates at typical commercial airline altitudes representative of solar cycle maximum and solar cycle minimum conditions and spanning the full range of geomagnetic cutoff rigidities. Third, conduct an initial validation of the NAIRAS model by comparing predictions of ambient dose equivalent rates with tabulated reference measurement data and recent aircraft radiation measurements taken in 2008 during the minimum between solar cycle 23 and solar cycle 24. By applying the criterion of the International Commission on Radiation Units and Measurements (ICRU) on acceptable levels of aircraft radiation dose uncertainty for ambient dose equivalent greater than or equal to an annual dose of 1 mSv, the NAIRAS model is within 25% of the measured data, which fall within the ICRU acceptable uncertainty limit of 30%. The NAIRAS model predictions of ambient dose equivalent rate are generally within 50% of the measured data for any single-point comparison. The largest differences occur at low latitudes and high cutoffs, where the radiation dose level is low. Nevertheless, analysis suggests that these single-point differences will be within 30% when a new deterministic pion-initiated electromagnetic cascade code is integrated into NAIRAS, an effort which is currently underway. C1 [Mertens, Christopher J.; Norman, Ryan B.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Meier, Matthias M.] DLR German Aerosp Ctr, Inst Aerosp Med Radiat Biol, Cologne, Germany. [Brown, Steven] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA. [Xu, Xiaojing] Sci Syst & Applicat Inc, Hampton, VA USA. RP Mertens, CJ (reprint author), NASA, Langley Res Ctr, Chem & Dynam Branch, Sci Directorate, 21 Langley Blvd,Mail Stop 401B, Hampton, VA 23681 USA. EM Christopher.J.Mertens@nasa.gov RI Norman, Ryan/D-5095-2017; OI Norman, Ryan/0000-0002-9103-7225; Meier, Matthias/0000-0003-0918-6473 FU National Aeronautics and Space Administration (NASA); North Carolina Space Grant Consortium FX This material is based upon work partially supported by the National Aeronautics and Space Administration (NASA) through Decision Support Through Earth Science Results and Living With A Star Targeted Research and Technology Programs under the Science Mission Directorate, the Human Research Program under the Human Exploration and Operations Mission Directorate, and the Advanced Radiation Protection Project under the Space Technology Mission Directorate's Game Changing Development Program. Mr. Brown contributed to this work under the NASA Langley Aerospace Research Summer Scholars (LARSS) Program and was partially supported by the North Carolina Space Grant Consortium. The authors would like to gratefully acknowledge the generous support with flight opportunities by the airline partners LTU Lufttransport-Unternehmen GmbH and Condor Flugdienst GmbH, which led to the flight data reported in section 3.3. Furthermore, the authors would like to express their gratitude to Captain Michael Nezel for his personal commitment in planning and performing the measuring flights reported in section 3.3. NR 98 TC 21 Z9 21 U1 0 U2 15 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 OCT PY 2013 VL 11 IS 10 BP 603 EP 635 DI 10.1002/swe.20100 PG 33 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 251YL UT WOS:000326970600008 ER PT J AU Yang, YG Zhou, ZQ AF Yang, Yaguang Zhou, Zhiqiang TI An analytic solution to Wahba's problem SO AEROSPACE SCIENCE AND TECHNOLOGY LA English DT Article DE Attitude estimation; Analytical solution; Spacecraft ID VECTOR OBSERVATIONS; ATTITUDE DETERMINATION AB All spacecraft attitude estimation methods are based on Wahba's optimization problem. This problem can be reduced to finding the largest eigenvalue and the corresponding eigenvector for Davenport's K-matrix. Several iterative algorithms, such as QUEST and FOMA, were proposed, aiming at reducing the computational cost. But their computational time is unpredictable because the iteration number is not fixed and the solution is not accurate in theory. Recently, an analytical solution, ESOQ was suggested. The advantages of analytical solutions are that their computational time is fixed and the solution should be accurate in theory if there is no numerical error. In this paper, we propose a different analytical solution to Wahba's problem. We use simple and easy to be verified examples to show that this method is numerically more stable than ESOQ potentially faster than QUEST and FOMA. We also use extensive simulation test to support this claim. Published by Elsevier Masson SAS. C1 [Yang, Yaguang] Res Off, NRC, Rockville, MD 20850 USA. [Zhou, Zhiqiang] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Yang, YG (reprint author), Res Off, NRC, 21 Church St, Rockville, MD 20850 USA. EM yaguang.yang@verizon.net; zhiqiang.zhou@nasa.gov NR 12 TC 4 Z9 4 U1 1 U2 3 PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS PA 23 RUE LINOIS, 75724 PARIS, FRANCE SN 1270-9638 EI 1626-3219 J9 AEROSP SCI TECHNOL JI Aerosp. Sci. Technol. PD OCT PY 2013 VL 30 IS 1 BP 46 EP 49 DI 10.1016/j.ast.2013.07.002 PG 4 WC Engineering, Aerospace SC Engineering GA 244BK UT WOS:000326361900006 ER PT J AU Kim, H Liou, MS AF Kim, Hyoungjin Liou, Meng-Sing TI Shape design optimization of embedded engine inlets for N2B hybrid wing-body configuration SO AEROSPACE SCIENCE AND TECHNOLOGY LA English DT Article DE Propulsion-airframe integration; Optimal shape design; Inlet distortion; Embedded engine ID UNSTRUCTURED ADJOINT METHOD; NAVIER-STOKES EQUATIONS; AERODYNAMIC DESIGN; TURBULENCE MODELS; MESHES; COMPUTATIONS; TRANSPORT; DUCT AB The N2B hybrid wing-body aircraft with embedded engines was conceptually designed to meet environmental and performance goals for the N + 2 generation transport set by the Subsonic Fixed Wing project of NASA Fundamental Aeronautics Program. In the present study, flow simulations are conducted around the N2B configuration by a Reynolds-averaged Navier-Stokes flow solver using unstructured meshes. Boundary conditions at fan faces and engine exhaust planes are provided by the Numerical Propulsion System Simulation (NPSS) thermodynamic engine cycle model. The flow simulations reveal challenging design issues arising from the integration of boundary-layer-ingestion offset inlets with the wing-body airframe. Adjoint-based optimal designs of the inlet shape are then carried out to minimize the airframe drag force and flow distortion at fan faces. Design surfaces are parameterized by Non-Uniform Rational B-Spline (NURBS), and the cowl lip geometry is modified by a spring analogy approach. By the drag minimization design, a massive flow separation on the cowl surfaces is almost removed, and the strength of a shock wave unintended in the original design is now remarkably reduced. For the distortion minimization design, the diffuser bottom and side walls are reshaped to minimize flow distortion at fan faces. This minimization results in a 12.5% reduction in distortion. (C) 2013 Elsevier Masson SAS. All rights reserved. C1 [Kim, Hyoungjin] Sci Applicat Int Corp, Cleveland, OH 44135 USA. [Liou, Meng-Sing] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Kim, H (reprint author), Sci Applicat Int Corp, Cleveland, OH 44135 USA. EM hyoungjinkim1@gmail.com FU NASA's Subsonic Fixed Wing Project of the Fundamental Aeronautics Program FX The authors are grateful for the support by the NASA's Subsonic Fixed Wing Project of the Fundamental Aeronautics Program. NR 39 TC 1 Z9 1 U1 1 U2 13 PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS PA 23 RUE LINOIS, 75724 PARIS, FRANCE SN 1270-9638 EI 1626-3219 J9 AEROSP SCI TECHNOL JI Aerosp. Sci. Technol. PD OCT PY 2013 VL 30 IS 1 BP 128 EP 149 DI 10.1016/j.ast.2013.07.011 PG 22 WC Engineering, Aerospace SC Engineering GA 244BK UT WOS:000326361900015 ER PT J AU Truong, KV Yeo, H Ormiston, RA AF Khiem-Van Truong Yeo, Hyeonsoo Ormiston, Robert A. TI Structural dynamics modeling of rectangular rotor blades SO AEROSPACE SCIENCE AND TECHNOLOGY LA English DT Article DE Helicopter rotor; Flexible blade structure; 1-D and 3-D structural modeling; Blade natural frequencies ID SECTIONAL ANALYSIS; COMPOSITE BEAMS AB This study investigates 1-D and 3-D methods for modeling helicopter rotor blade structural dynamics to better understand the accuracy of current structural modeling based on 1-D beam theory. Natural frequencies are calculated at various rotor angular speeds for a large variety of blades ranging from simple isotropic beams to a realistic composite blade. The blade shape is limited to rectangular planforms, but various lengths are considered. 1-D beam analysis is conducted using the RCAS rotorcraft comprehensive analysis with 2-D cross-sectional properties calculated from VASS. 3-D finite element analysis is based on the commercial code MSC/Marc. Accuracy of both 1-D and 3-D analyses have been assessed through analysis of discretization errors that originate from insufficiently refined meshing. There is very good agreement between 1-D and 3-D predictions for the eight lowest modes of a large variety of blades, when there is no coupling between modes of different nature (flap, torsion) induced by materials and when the blade length is greater than ten times chord. Effects of blade length for isotropic and composite beams with no coupling between modes are similarly predicted by 1-D and 3-D analyses, except for torsion frequency, where 1-D analysis closely follows classical beam theory. With the presence of flap-torsion coupling between modes, the two approaches differ on prediction of the torsion-dominant frequency and significantly on the flap-dominant frequency. (C) 2013 Elsevier Masson SAS. All rights reserved. C1 [Khiem-Van Truong] Off Natl Etud & Rech Aerosp, DADS, Chatillon, France. [Yeo, Hyeonsoo; Ormiston, Robert A.] US Army, Aviat Dev Directorate AFDD, Ames Res Ctr, Aviat & Missile Res Dev & Engn Ctr,Res Dev & Engn, Moffett Field, CA USA. RP Truong, KV (reprint author), Off Natl Etud & Rech Aerosp, DADS, Chatillon, France. EM khiem-van.truong@onera.fr; hyeonsoo.yeo@us.army.mil; robert.ormiston@us.army.mil OI TRUONG, Van Khiem/0000-0002-3236-0751 NR 30 TC 3 Z9 3 U1 1 U2 8 PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS PA 23 RUE LINOIS, 75724 PARIS, FRANCE SN 1270-9638 EI 1626-3219 J9 AEROSP SCI TECHNOL JI Aerosp. Sci. Technol. PD OCT PY 2013 VL 30 IS 1 BP 293 EP 305 DI 10.1016/j.ast.2013.08.014 PG 13 WC Engineering, Aerospace SC Engineering GA 244BK UT WOS:000326361900031 ER PT J AU Seddio, SM Jolliff, BL Korotev, RL Zeigler, RA AF Seddio, Stephen M. Jolliff, Bradley L. Korotev, Randy L. Zeigler, Ryan A. TI Petrology and geochemistry of lunar granite 12032,366-19 and implications for lunar granite petrogenesis SO AMERICAN MINERALOGIST LA English DT Article DE Granite; Moon; zirconolite; apatite; felsite; Apollo 12 ID SILICATE-LIQUID IMMISCIBILITY; ELECTRON-MICROPROBE ANALYSIS; RARE-EARTH; HANSTEEN-ALPHA; MOON; ABUNDANCES; CHEMISTRY; ROCKS; AGE; LUNAR-ROCK-12013 AB Apollo 12 sample 12032,366-19 is a 21.3 mg granite fragment that is distinct from any other lunar granite or felsite. It is composed of barian K-feldspar, quartz, sodic plagioclase, hedenbergite, fayalite, and ilmenite, with trace amounts of zirconolite, baddeleyite, apatite, and merrillite. The texture of 12032,366-19 is largely a micrographic intergrowth predominantly of K-feldspar and quartz and, to a lesser extent, plagioclase and quartz. Hedenbergite, fayalite, and ilmenite are present in minor but significant quantities-6.0, 3.1, and 1.7 wt%, respectively-and are scattered throughout the feldspar-quartz intergrowths. Trace amounts of Zr-bearing phases are found including zirconolite (0.6 wt%) and baddeleyite (0.04 wt%). Incompatible trace-element concentrations are high in 12032,366-19, particularly the high-field-strength elements, e.g., Zr, Sm, and Th (1500, 25, and 61 mu g/g, respectively). The chondrite-normalized, rare-earth-element concentrations form a "V-pattern" that is characteristic of other lunar granitic material. By modeling 12032,366-19 as a derivative from a KREEP-like parent melt, the composition and mineral assemblage can be obtained by extended fractional crystallization combined with separation of the low-density minerals plus trapped melt components prior to final solidification. However, this model cannot quantitatively account for the relatively sodic composition of the plagioclase (An(34-50)) and requires that the starting melt has Na2O of 1.2-1.4 wt%, which is higher than most KREEP compositions. Formation of this assemblage by silicate-liquid immiscibility is neither required nor indicated by petrogenetic modeling. C1 [Seddio, Stephen M.; Jolliff, Bradley L.; Korotev, Randy L.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Seddio, Stephen M.; Jolliff, Bradley L.; Korotev, Randy L.] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. [Zeigler, Ryan A.] NASA, Lyndon B Johnson Space Ctr, Astromat & Explorat Sci Directorate, Houston, TX 77058 USA. RP Seddio, SM (reprint author), Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. EM sseddio@levee.wustl.edu FU NASA [NNG04GG10G] FX We thank Paul Carpenter for his assistance with trace element analysis on the electron microprobe and insight into Zr-Ti phases. We thank Bob Dymek for his helpful insights and discussion especially regarding the ZrO2-SiO2 phase boundary. We thank Alian Wang and Weigang Kong for Raman spectroscopic measurements. We are grateful to G. Jeffrey Taylor and Malcolm J. Rutherford for their insightful reviews of this paper. This work was funded by NASA Grant NNG04GG10G (R.L.K.). NR 80 TC 15 Z9 15 U1 0 U2 18 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 OCT PY 2013 VL 98 IS 10 BP 1697 EP 1713 DI 10.2138/am.2013.4330 PG 17 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 243ZR UT WOS:000326357400007 ER PT J AU Siddon, EC Heintz, RA Mueter, FJ AF Siddon, Elizabeth C. Heintz, Ron A. Mueter, Franz J. TI Conceptual model of energy allocation in walleye pollock (Theragra chalcogramma) from age-0 to age-1 in the southeastern Bering Sea SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY LA English DT Article DE Walleye pollock (Theragra chalcogramma); Larval fish; Bering Sea; Bioenergetics; Energy allocation; Recruitment ID OSCILLATING CONTROL HYPOTHESIS; PRINCE-WILLIAM-SOUND; CLIMATE-CHANGE; SHELIKOF-STRAIT; VERTICAL-DISTRIBUTION; TEMPORAL VARIABILITY; WINTER MORTALITY; LIFE-HISTORY; ALASKA; SIZE AB Walleye pollock (Theragra chalcogramma) support the largest commercial fishery in the United States and are an ecologically important component of the southeastern Bering Sea (SEBS) pelagic ecosystem. Alternating climate states influence the survival of walleye pollock through bottom-up control of zooplankton communities and possible top-down control of predator abundance. Quantifying the seasonal progression and spatial trends in energy content of walleye pollock provides critical information for predicting overwinter survival and recruitment to age-1 because age-0 walleye pollock rely on energy reserves to survive their first winter. Age-0 and age-1 walleye pollock were collected in the SEBS from May to September 2008-2010. Energetic status was determined through quantification of energy density (Wig) and proximate composition (i.e., % lipid, % moisture) with variation in energy density primarily driven by variability in % lipid. Energy densities remained relatively low during the larval phase in spring, consistent with energy allocation to somatic growth and development. Lipid acquisition rates increased rapidly after transformation to the juvenile form (25-40 mm standard length), with energy allocation to lipid storage leading to higher energy densities in late summer. This transition in energy allocation strategies is a physiological manifestation of survival constraints associated with distinct ontogenetic stages; a strategy favoring growth to escape size-dependent predation appears limited to larval development while juvenile fish allocate proportionally more mass to lipid storage in late summer. We propose that the time after the end of larval development and before the onset of winter represents a short critical period for energy storage in age-0 walleye pollock, and that overwinter survival depends on accumulating sufficient stores the previous growing season and consequently may be an important determinant of recruitment success. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Siddon, Elizabeth C.; Mueter, Franz J.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Juneau, AK 99801 USA. [Heintz, Ron A.] Natl Ocean & Atmospher Adm, Ted Stevens Marine Res Inst, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK 99801 USA. RP Siddon, EC (reprint author), Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, 17101 Pt Lena Loop Rd, Juneau, AK 99801 USA. EM ecsiddon@alaska.edu FU North Pacific Research Board (NPRB) Bering Sea Integrated Ecosystem Research Program (BSIERP); NOAA's North Pacific Climate Regimes and Ecosystem Productivity Program (NPCREP); BEST-BSIERP Bering Sea Project [67] FX We thank the officers and crew of the NOAA ships Miller Freeman and Oscar Dyson, the USCG vessel Healy, and the R/Vs Knorr (WHOI) and Thompson (UW). Funding was provided through the North Pacific Research Board (NPRB) Bering Sea Integrated Ecosystem Research Program (BSIERP) and NOAA's North Pacific Climate Regimes and Ecosystem Productivity Program (NPCREP). NOAA's EcoFOCI, MACE, and BASIS programs kindly conducted additional sampling for this project. We thank Dr. Thomas Hurst, Dr. Matthew Wilson, and one anonymous reviewer for providing helpful comments that greatly improved the manuscript This research is NPRB publication #360 and BEST-BSIERP Bering Sea Project #67. Fig. 1 courtesy of Ross Parnell-Turner, University of Cambridge. Reference to trade names does not imply endorsement by the National Marine Fisheries Service (NMFS), NOAA. The findings and conclusions in the paper are those of the authors and do not necessarily represent the views of the NMFS, NOAA. NR 64 TC 24 Z9 25 U1 3 U2 26 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0645 EI 1879-0100 J9 DEEP-SEA RES PT II JI Deep-Sea Res. Part II-Top. Stud. Oceanogr. PD OCT 1 PY 2013 VL 94 BP 140 EP 149 DI 10.1016/j.dsr2.2012.12.007 PG 10 WC Oceanography SC Oceanography GA 244BH UT WOS:000326361600012 ER PT J AU Heintz, RA Siddon, EC Farley, EV Napp, JM AF Heintz, Ron A. Siddon, Elizabeth C. Farley, Edward V., Jr. Napp, Jeffrey M. TI Correlation between recruitment and fall condition of age-0 pollock (Theragra chalcogramma) from the eastern Bering Sea under varying climate conditions SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY LA English DT Article DE Pollock; Bering Sea; Recruitment; Climate change; Winter; Prey quality ID OSCILLATING CONTROL HYPOTHESIS; PRINCE-WILLIAM-SOUND; WALLEYE POLLOCK; WINTER MORTALITY; ECOSYSTEM; GROWTH; SIZE; SALMON; TEMPERATURE; ALASKA AB Fishery managers require an understanding of how climate influences recruitment if they are to separate the effects of fishing and climate on production. The southeastern Bering Sea offers opportunities to understand climate effects on recruitment because inter-annual oscillations in ice coverage set up warm or cold conditions for juvenile fish production. Depth-averaged temperature anomalies in the Bering Sea indicate the past nine years have included three warm (2003-2005), an average (2006), and five cold (2007-2011) years. We examined how these climatic states influenced the diet quality and condition (size, energy density and total energy) of young-of-the-year (YOY) pollock (Theragra chalcogramma) in fall. The implications of fall condition were further examined by relating condition prior to winter to the number of age-1 recruits-per-spawner the following summer (R/S). The percentage of lipid in pollock diets was threefold higher in cold years compared with warm years, but stomach fullness did not vary. Consequently, fish energy densities were 33% higher in cold years (P < 0.001) than in warm years. In contrast, neither fish size (P=0.666), nor total energy (P=0.197) varied with climatic condition. However, total energy was significantly (P=0.007) and positively correlated with R/S (R-2=0.736). We conclude that recruitment to age-1 in the southeastern Bering Sea is improved under environmental conditions that produce large, energy dense YOY pollock in fall. Published by Elsevier Ltd. C1 [Heintz, Ron A.; Farley, Edward V., Jr.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, Juneau, AK 99801 USA. [Siddon, Elizabeth C.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Juneau, AK 99801 USA. [Napp, Jeffrey M.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Seattle, WA 98115 USA. RP Heintz, RA (reprint author), NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, 17109 Pt Lena Loop Rd, Juneau, AK 99801 USA. EM ron.heintz@noaa.gov FU NSF [OPP-0327308] FX We thank all of the people involved in collecting and sorting the samples used in this study. This includes the crews of numerous vessels. In addition it includes numerous students that have helped to sort, prepare and process samples in the laboratory. Collection of summer 2004 prey samples was supported by NSF Grant OPP-0327308 (to G.L. Hunt, Jr.) and NOAA's North Pacific Climate Regimes and Ecosystem Productivity (NPCREP) research program. This research is contribution NPRB 414, BEST-BSIERP 93, and EcoFOCI-0797 to NOAA's NPCREP Program. References to trade names do not imply endorsement by the National Marine Fisheries Service, NOAA. The findings and conclusions in this paper are those of the authors and even though NOAA reviewed the work and paid our salaries the views here do not represent those of NMFS or NOAA. NR 38 TC 38 Z9 39 U1 5 U2 28 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0645 EI 1879-0100 J9 DEEP-SEA RES PT II JI Deep-Sea Res. Part II-Top. Stud. Oceanogr. PD OCT 1 PY 2013 VL 94 BP 150 EP 156 DI 10.1016/j.dsr2.2013.04.006 PG 7 WC Oceanography SC Oceanography GA 244BH UT WOS:000326361600013 ER PT J AU Copeman, LA Laurel, BJ Parrish, CC AF Copeman, Louise A. Laurel, Benjamin J. Parrish, Christopher C. TI Effect of temperature and tissue type on fatty acid signatures of two species of North Pacific juvenile gadids: A laboratory feeding study SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE Biomarker; Cod; Fatty acid; Juvenile; Pollock; Temperature ID COD GADUS-MORHUA; POLLOCK THERAGRA-CHALCOGRAMMA; FOOD-WEB; WALLEYE POLLOCK; ATLANTIC SALMON; LIPID-COMPOSITION; ESTIMATING DIETS; TROPHIC MARKERS; STABLE-ISOTOPE; FISH AB The utility of the fatty add biomarker (FAB) approach in fisheries ecology is limited by our understanding of how biotic and abiotic factors determine dietary markers in fish tissues. An 8-week laboratory experiment was conducted on two species of juvenile gadids (Pacific cod, Gadus macrocephalus and walleye Pollock, Theragra chalcogramma) reared at 3 degrees C or 9 degrees C and fed a diet enriched with either oils of marine origin or terrestrial plant origin. Non-linear models were fitted to investigate how tissue type and temperature mediated the proportion of FABs in fish. Across temperatures, fatty acid (FA) profiles were similar for both species of gadids. FAs also showed high temporal sensitivity across temperatures, and were evident in fish after only one week of feeding. Pacific cod held at 9 degrees C and fed a terrestrial plant oil (TPO) enriched diet had significantly higher C-18 polyunsaturated FAs (PUFAs) in their liver than cod held at 3 degrees C after one week, but this temperature effect diminished as tissues reached equilibrium with their diet C-18 PUFAs were significantly higher in liver than in muscle. Differential proportions of C-18 PUFAs among tissues provide temporal patterns that may help with disentangling the timing of offshore-inshore nursery migrations in juvenile fish. Calibration coefficients were determined to explain the relationship between FAs in the diet and FAs in fish tissues. These coefficients will support future development of quantitative estimates of diet in juvenile low-fat fish. (C) 2013 Elsevier B.V. All rights reserved. C1 [Copeman, Louise A.] Oregon State Univ, Hatfield Marine Sci Ctr, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA. [Copeman, Louise A.; Parrish, Christopher C.] Mem Univ Newfoundland, Dept Ocean Sci, St John, NF A1C 5S7, Canada. [Laurel, Benjamin J.] NOAA, Fisheries Behav Ecol Program, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. RP Copeman, LA (reprint author), Oregon State Univ, Hatfield Marine Sci Ctr, Cooperat Inst Marine Resources Studies, 2030 S Marine Sci Dr, Newport, OR 97365 USA. EM copemanl@onid.orst.edu; Ben.Laurel@noaa.gov; cparrish@mun.ca FU NOAA-AFSC Habitat and Ecosystem Process Research (HEPR) grant; Cooperative Institute for Marine Resources Studies, Oregon State University [NA17RJ1362]; NSERC FX Sample processing costs and salary for Louise Copeman were provided by a NOAA-AFSC Habitat and Ecosystem Process Research (HEPR) grant awarded to Benjamin Laurel, Clifford Ryer, Christopher Parrish, Allan Stoner, Brian Knoth and Dan Urban. Partial salary support to Louise Copeman was provided by a Cooperative Institute for Marine Resources Studies, Oregon State University grant (#NA17RJ1362). Salary support for Louise Copeman was also provided by a NSERC discovery grant awarded to Dr. C. Parrish. Many thanks to the technical staff in Dr. C. Parrish's lab (in particular Tara Hooper and Jeanette Wells), for processing lipid classes and FAs on extracted samples. Thanks also to Scott Haines, Paul Iseri and Michele Ottmar for providing assistance in the laboratory on juvenile feeding experiments. [RH] NR 52 TC 7 Z9 7 U1 3 U2 21 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 EI 1879-1697 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD OCT PY 2013 VL 448 BP 188 EP 196 DI 10.1016/j.jembe.2013.07.008 PG 9 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 245AE UT WOS:000326430500024 ER PT J AU Stephenson, JD Freeland, SJ AF Stephenson, James D. Freeland, Stephen J. TI Unearthing the Root of Amino Acid Similarity SO JOURNAL OF MOLECULAR EVOLUTION LA English DT Article DE Amino acids; Simplified alphabets; Similarity measures; Chemical properties; Protein structure ID SUBSTITUTION MATRICES; SEQUENCE ALIGNMENT; GLOBULAR-PROTEINS; ALPHABETS; FOLD; RECOGNITION; PREDICTION; RESIDUES; CLASSIFICATION; CONSERVATION AB Similarities and differences between amino acids define the rates at which they substitute for one another within protein sequences and the patterns by which these sequences form protein structures. However, there exist many ways to measure similarity, whether one considers the molecular attributes of individual amino acids, the roles that they play within proteins, or some nuanced contribution of each. One popular approach to representing these relationships is to divide the 20 amino acids of the standard genetic code into groups, thereby forming a simplified amino acid alphabet. Here, we develop a method to compare or combine different simplified alphabets, and apply it to 34 simplified alphabets from the scientific literature. We use this method to show that while different suggestions vary and agree in non-intuitive ways, they combine to reveal a consensus view of amino acid similarity that is clearly rooted in physico-chemistry. C1 [Stephenson, James D.; Freeland, Stephen J.] Univ Hawaii, NASA, Astrobiol Inst, Honolulu, HI 96822 USA. RP Stephenson, JD (reprint author), Univ Hawaii, NASA, Astrobiol Inst, Honolulu, HI 96822 USA. EM jds@ifa.hawaii.edu OI Stephenson, James/0000-0002-6427-5703 FU National Aeronautics and Space Administration through the NASA Astrobiology Institute through the Office of Space Science [NNA09DA77A] FX This material is based upon work supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement No. NNA09DA77A issued through the Office of Space Science. NR 51 TC 4 Z9 4 U1 1 U2 7 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2844 EI 1432-1432 J9 J MOL EVOL JI J. Mol. Evol. PD OCT PY 2013 VL 77 IS 4 SI SI BP 159 EP 169 DI 10.1007/s00239-013-9565-0 PG 11 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 245IG UT WOS:000326456600003 PM 23743923 ER PT J AU Li, F Choudhari, M Chang, CL White, J AF Li, Fei Choudhari, Meelan Chang, Chau-Lyan White, Jeffery TI Effects of injection on the instability of boundary layers over hypersonic configurations SO PHYSICS OF FLUIDS LA English DT Article ID TRANSITION; ROUGHNESS AB Computations are performed to study the boundary layer instability mechanisms pertaining to hypersonic vehicles with significant ablative effects. The process of laminar-turbulent transition over vehicles with ablative heat shields can be influenced by both the out-gassing associated with surface pyrolysis and the resulting modification of surface geometry including the formation of micro-roughness. To isolate the effects of out-gassing, this paper examines the stability of canonical boundary layer flows over smooth surfaces in the presence of gas injection into the boundary layer, with an emphasis on the case of massive injection that is relevant to previous laboratory experiments. For a slender cone, the effects of strong out-gassing on the predominantly second mode instability are found to be weakly stabilizing. This new, somewhat surprising result is confirmed by computations carried out on a flat plate boundary layer at high Mach numbers. In contrast, for a blunt capsule flow dominated by first mode instability, the effect of out-gassing is shown to be strongly destabilizing, consistent with the well-known behavior of subsonic boundary layers. (C) 2013 AIP Publishing LLC. C1 [Li, Fei; Choudhari, Meelan; Chang, Chau-Lyan; White, Jeffery] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Li, F (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM fei.li@nasa.gov RI Choudhari, Meelan/F-6080-2017 OI Choudhari, Meelan/0000-0001-9120-7362 NR 18 TC 1 Z9 1 U1 1 U2 8 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-6631 EI 1089-7666 J9 PHYS FLUIDS JI Phys. Fluids PD OCT PY 2013 VL 25 IS 10 AR 104107 DI 10.1063/1.4825038 PG 15 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 247TB UT WOS:000326642800035 ER PT J AU Bendek, EA Guyon, O Ammons, SM Belikov, R AF Bendek, Eduardo A. Guyon, Olivier Ammons, S. Mark Belikov, Ruslan TI Laboratory Demonstration of Astrometric Compensation Using a Diffractive Pupil SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE Astronomical Instrumentation ID TELESCOPE; PHOTOMETRY; SENSOR; PRECISION AB Astrometry is a promising exoplanet detection and characterization technique that can detect earth-size exoplanets if submicroarcsecond precision is achieved. However, instrumentation available today can only reach in the order of 10(2) microarcseconds, mainly limited by long-term dynamic distortions on wide-field observations. To overcome this problem, we propose the implementation of a diffractive pupil, which has an array of microscopic dots imprinted on the primary mirror coating. The dots create diffractive spikes on the focal plane that are used to calibrate image plane distortions that degrade the astrometric measurement precision. This astrometry technique can be utilized simultaneously with coronagraphy for exhaustive characterization of exoplanets (mass, spectra, orbit). We designed and built an astrometry laboratory to validate the diffractive pupil ability to calibrate distortions and stabilize wide-field astrometric measurements over time. We achieved a precision of 0.0123px, which represents 42% of the 0.0288px stability measured for this setup before the calibration. On sky units, this result is equivalent to 3.42xx10(-3)/D that corresponds to 150as for a 2.4m telescope at 500nm wavelength. Also, at large field angles the distortion error was reduced by a factor of 5 when the calibration was used, proving its effectiveness for large field of view. We present an astrometry error budget here to explain the source of the residual error observed when the diffractive pupil calibration is used. C1 [Bendek, Eduardo A.; Belikov, Ruslan] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Guyon, Olivier] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Guyon, Olivier] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Ammons, S. Mark] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. RP Bendek, EA (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. FU NASA [09-APRA09-0140]; Institute of International Education IIE; NASA; U.S. Department of Energy by the Lawrence Livermore National Laboratory [DE-AC52-07NA27344] FX This project is funded by NASA grant 09-APRA09-0140 program and it has been performed under the auspices of the following institutions: The Institute of International Education IIE with their Fulbright PhD Science and Technology program, the NASA Postdoctoral Program, and the U.S. Department of Energy by the Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. Also, we acknowledge the advice of the following people in different aspects of the project: Michael Shao, Stuart Shaklan, Robert Woodruff, Jim Burge, Roger Angel, Marie Levine, and Josh Eisner. NR 21 TC 1 Z9 1 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD OCT 1 PY 2013 VL 125 IS 932 BP 1212 EP 1225 DI 10.1086/673373 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 243PM UT WOS:000326329100005 ER PT J AU Colavita, MM Wizinowich, PL Akeson, RL Ragland, S Woillez, JM Millan-Gabet, R Serabyn, E Abajian, M Acton, DS Appleby, E Beletic, JW Beichman, CA Bell, J Berkey, BC Berlin, J Boden, AF Booth, AJ Boutell, R Chaffee, FH Chan, D Chin, J Chock, J Cohen, R Cooper, A Crawford, SL Creech-Eakman, MJ Dahl, W Eychaner, G Fanson, JL Felizardo, C Garcia-Gathright, JI Gathright, JT Hardy, G Henderson, H Herstein, JS Hess, M Hovland, EE Hrynevych, MA Johansson, E Johnson, RL Kelley, J Kendrick, R Koresko, CD Kurpis, P Mignant, D Lewis, HA Ligon, ER Lupton, W McBride, D Medeiros, DW Mennesson, BP Moore, JD Morrison, D Nance, C Neyman, C Niessner, A Paine, CG Palmer, DL Panteleeva, T Papin, M Parvin, B Reder, L Rudeen, A Saloga, T Sargent, A Shao, M Smith, B Smythe, RF Stomski, P Summers, KR Swain, MR Swanson, P Thompson, R Tsubota, K Tumminello, A Tyau, C van Belle, GT Vasisht, G Vause, J Vescelus, F Walker, J Wallace, JK Wehmeier, U Wetherell, E AF Colavita, M. M. Wizinowich, P. L. Akeson, R. L. Ragland, S. Woillez, J. M. Millan-Gabet, R. Serabyn, E. Abajian, M. Acton, D. S. Appleby, E. Beletic, J. W. Beichman, C. A. Bell, J. Berkey, B. C. Berlin, J. Boden, A. F. Booth, A. J. Boutell, R. Chaffee, F. H. Chan, D. Chin, J. Chock, J. Cohen, R. Cooper, A. Crawford, S. L. Creech-Eakman, M. J. Dahl, W. Eychaner, G. Fanson, J. L. Felizardo, C. Garcia-Gathright, J. I. Gathright, J. T. Hardy, G. Henderson, H. Herstein, J. S. Hess, M. Hovland, E. E. Hrynevych, M. A. Johansson, E. Johnson, R. L., Jr. Kelley, J. Kendrick, R. Koresko, C. D. Kurpis, P. Le Mignant, D. Lewis, H. A. Ligon, E. R. Lupton, W. McBride, D. Medeiros, D. W. Mennesson, B. P. Moore, J. D. Morrison, D. Nance, C. Neyman, C. Niessner, A. Paine, C. G. Palmer, D. L. Panteleeva, T. Papin, M. Parvin, B. Reder, L. Rudeen, A. Saloga, T. Sargent, A. Shao, M. Smith, B. Smythe, R. F. Stomski, P. Summers, K. R. Swain, M. R. Swanson, P. Thompson, R. Tsubota, K. Tumminello, A. Tyau, C. van Belle, G. T. Vasisht, G. Vause, J. Vescelus, F. Walker, J. Wallace, J. K. Wehmeier, U. Wetherell, E. TI The Keck Interferometer SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE Astronomical Instrumentation ID PALOMAR TESTBED INTERFEROMETER; NARROW-ANGLE ASTROMETRY; ADAPTIVE OPTICS SYSTEM; INFRARED INTERFEROMETRY; VISIBILITY ESTIMATORS; II TELESCOPE; WATER-VAPOR; NULLER; PERFORMANCE; PROGRESS AB The Keck Interferometer (KI) combined the two 10m W. M. Keck Observatory telescopes on Mauna Kea, Hawaii, as a long-baseline near- and mid-infrared interferometer. Funded by NASA, it operated from 2001 until 2012. KI used adaptive optics on the two Keck telescopes to correct the individual wavefronts, as well as active fringe tracking in all modes for path-length control, including the implementation of cophasing to provide long coherent integration times. KI implemented high sensitivity fringe-visibility measurements at H (1.6m), K (2.2m), and L (3.8m) bands, and nulling measurements at N band (10m), which were used to address a broad range of science topics. Supporting these capabilities was an extensive interferometer infrastructure and unique instrumentation, including some additional functionality added as part of the NSF-funded ASTRA program. This paper provides an overview of the instrument architecture and some of the key design and implementation decisions, as well as a description of all of the key elements and their configuration at the end of the project. The objective is to provide a view of KI as an integrated system, and to provide adequate technical detail to assess the implementation. Included is a discussion of the operational aspects of the system, as well as of the achieved system performance. Finally, details on V-2 calibration in the presence of detector nonlinearities as applied in the data pipeline are provided. C1 [Colavita, M. M.; Serabyn, E.; Berlin, J.; Booth, A. J.; Crawford, S. L.; Creech-Eakman, M. J.; Eychaner, G.; Fanson, J. L.; Garcia-Gathright, J. I.; Hardy, G.; Hovland, E. E.; Johnson, R. L., Jr.; Kelley, J.; Ligon, E. R.; Mennesson, B. P.; Moore, J. D.; Niessner, A.; Paine, C. G.; Palmer, D. L.; Parvin, B.; Reder, L.; Shao, M.; Smythe, R. F.; Swain, M. R.; Swanson, P.; Thompson, R.; Tumminello, A.; van Belle, G. T.; Vasisht, G.; Vescelus, F.; Wallace, J. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wizinowich, P. L.; Ragland, S.; Woillez, J. M.; Acton, D. S.; Appleby, E.; Beletic, J. W.; Bell, J.; Berkey, B. C.; Boutell, R.; Chaffee, F. H.; Chan, D.; Chin, J.; Chock, J.; Cohen, R.; Cooper, A.; Dahl, W.; Gathright, J. T.; Hess, M.; Hrynevych, M. A.; Johansson, E.; Kendrick, R.; Kurpis, P.; Le Mignant, D.; Lewis, H. A.; Lupton, W.; McBride, D.; Medeiros, D. W.; Morrison, D.; Nance, C.; Neyman, C.; Panteleeva, T.; Rudeen, A.; Saloga, T.; Smith, B.; Stomski, P.; Summers, K. R.; Tsubota, K.; Tyau, C.; Vause, J.; Walker, J.; Wehmeier, U.; Wetherell, E.] Calif Assoc Res Astron, WM Keck Observ, Kamuela, HI 96743 USA. [Akeson, R. L.; Millan-Gabet, R.; Abajian, M.; Beichman, C. A.; Boden, A. F.; Felizardo, C.; Henderson, H.; Herstein, J. S.; Koresko, C. D.; Papin, M.] CALTECH, NASA Exoplanet Sci Ctr, Pasadena, CA 91125 USA. RP Colavita, MM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU National Aeronautics and Space Administration (NASA); W. M. Keck Foundation; National Science Foundation [AST0619965]; NASA FX The Keck Interferometer was funded by the National Aeronautics and Space Administration (NASA). Observations 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. The ASTRA upgrade to KI was funded by the National Science Foundation under Grant No. AST0619965. Part of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology, and at the NASA Exoplanet Science Institute, California Institute of Technology, under contract with NASA. Thanks to the referee for helpful comments. NR 60 TC 7 Z9 7 U1 2 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD OCT 1 PY 2013 VL 125 IS 932 BP 1226 EP 1264 DI 10.1086/673475 PG 39 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 243PM UT WOS:000326329100006 ER PT J AU Wielicki, BA Young, DF Mlynczak, MG Thome, KJ Leroy, S Corliss, J Anderson, JG Ao, CO Bantges, R Best, F Bowman, K Brindley, H Butler, JJ Collins, W Dykema, JA Doelling, DR Feldman, DR Fox, N Huang, XL Holz, R Huang, Y Jin, Z Jennings, D Johnson, DG Jucks, K Kato, S Kirk-Davidoff, DB Knuteson, R Kopp, G Kratz, DP Liu, X Lukashin, C Mannucci, AJ Phojanamongkolkij, N Pilewskie, P Ramaswam, V Revercomb, YH Rice, J Roberts, Y Roithmayr, CM Rose, F Sandford, S Shirley, EL Smith, WL Soden, SB Speth, PW Sun, W Taylor, PC Tobin, D Xiong, X AF Wielicki, Bruce A. Young, D. F. Mlynczak, M. G. Thome, K. J. Leroy, S. Corliss, J. Anderson, J. G. Ao, C. O. Bantges, R. Best, F. Bowman, K. Brindley, H. Butler, J. J. Collins, W. Dykema, J. A. Doelling, D. R. Feldman, D. R. Fox, N. Huang, Xianglei Holz, R. Huang, Y. Jin, Z. Jennings, D. Johnson, D. G. Jucks, K. Kato, S. Kirk-Davidoff, D. B. Knuteson, R. Kopp, G. Kratz, D. P. Liu, X. Lukashin, C. Mannucci, A. J. Phojanamongkolkij, N. Pilewskie, P. Ramaswam, V. Revercomb, Y. H. Rice, J. Roberts, Y. Roithmayr, C. M. Rose, F. Sandford, S. Shirley, E. L. Smith, W. L. Soden, Sr. B. Speth, P. W. Sun, W. Taylor, P. C. Tobin, D. Xiong, X. TI Achieving Climate Change Absolute Accuracy in Orbit SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID OCEAN-ATMOSPHERE MODELS; INFRARED-SPECTRA; INTER-CALIBRATION; RADIANCE MEASUREMENTS; EARTHS ENERGY; SYSTEM; SPACE; INSTRUMENT; CLOUDS; FEEDBACKS AB The Climate Absolute Radiance and Refractivity Observatory (CLARREO) mission will provide a calibration laboratory in orbit for the purpose of accurately measuring and attributing climate change. CLARREO measurements establish new climate change benchmarks with high absolute radiometric accuracy and high statistical confidence across a wide range of essential climate variables. CLARREO's inherently high absolute accuracy will be verified and traceable on orbit to Systeme Internationale (SI) units. The benchmarks established by CLARREO will be critical for assessing changes in the Earth system and climate model predictive capabilities for decades into the future as society works to meet the challenge of optimizing strategies for mitigating and adapting to climate change. The CLARREO benchmarks are derived from measurements of the Earth's thermal infrared spectrum (5-50 m), the spectrum of solar radiation reflected by the Earth and its atmosphere (320-2300 nm), and radio occultation refractivity from which accurate temperature profiles are derived. The mission has the ability to provide new spectral fingerprints of climate change, as well as to provide the first orbiting radiometer with accuracy sufficient to serve as the reference transfer standard for other space sensors, in essence serving as a NIST [National Institute of Standards and Technology] in orbit. CLARREO will greatly improve the accuracy and relevance of a wide range of space-borne instruments for decadal climate change. Finally, CLARREO has developed new metrics and methods for determining the accuracy requirements of climate observations for a wide range of climate variables and uncertainty sources. These methods should be useful for improving our understanding of observing requirements for most climate change observations. C1 [Wielicki, Bruce A.; Young, D. F.; Mlynczak, M. G.; Corliss, J.; Doelling, D. R.; Johnson, D. G.; Kato, S.; Kratz, D. P.; Liu, X.; Lukashin, C.; Phojanamongkolkij, N.; Roithmayr, C. M.; Sandford, S.; Speth, P. W.; Taylor, P. C.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Thome, K. J.; Butler, J. J.; Jennings, D.; Xiong, X.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Leroy, S.; Anderson, J. G.; Dykema, J. A.] Harvard Univ, Cambridge, MA 02138 USA. [Ao, C. O.; Bowman, K.; Mannucci, A. J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Bantges, R.; Brindley, H.] Univ London Imperial Coll Sci Technol & Med, London, England. [Best, F.; Holz, R.; Knuteson, R.; Revercomb, Y. H.; Smith, W. L.; Tobin, D.] Univ Wisconsin Madison, Madison, WI USA. [Collins, W.; Feldman, D. R.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Fox, N.] Natl Phys Lab, London, England. [Huang, Xianglei] Univ Michigan, Ann Arbor, MI 48109 USA. [Huang, Y.] McGill Univ, Montreal, PQ, Canada. [Jin, Z.; Rose, F.; Sun, W.] Sci Syst Applicat, Hampton, VA USA. [Jucks, K.] NASA Headquarters, Washington, DC USA. [Kirk-Davidoff, D. B.] Univ Maryland, Greenbelt, MD USA. [Kopp, G.; Pilewskie, P.; Roberts, Y.] Univ Colorado Boulder, Boulder, CO USA. [Ramaswam, V.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. [Rice, J.; Shirley, E. L.] NIST, Gaithersburg, MD 20899 USA. [Soden, Sr. B.] Univ Miami, Miami, FL USA. RP Wielicki, BA (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. EM b.a.wielicki@nasa.gov RI Huang, Xianglei/G-6127-2011; Feldman, Daniel/N-8703-2013; Butler, James/D-4188-2013; Thome, Kurtis/D-7251-2012; Collins, William/J-3147-2014; Taylor, Patrick/D-8696-2015; Johnson, David/F-2376-2015; Huang, Yi/E-9479-2016; Richards, Amber/K-8203-2015; OI Huang, Xianglei/0000-0002-7129-614X; Feldman, Daniel/0000-0003-3365-5233; Collins, William/0000-0002-4463-9848; Taylor, Patrick/0000-0002-8098-8447; Johnson, David/0000-0003-4399-5653; Huang, Yi/0000-0002-5065-4198; Brindley, Helen/0000-0002-7859-9207; Rose, Fred G/0000-0003-0769-0772 FU Jet Propulsion Laboratory; California Institute of Technology; National Aeronautics and Space Administration FX We thank several reviewers for providing comments that significantly improved the clarity and presentation of 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. NR 64 TC 67 Z9 69 U1 5 U2 43 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 OCT PY 2013 VL 94 IS 10 BP 1519 EP 1539 DI 10.1175/BAMS-D-12-00149.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 241DO UT WOS:000326146800007 ER PT J AU Brown, AM Davis, RB DeHaye, MK AF Brown, Andrew M. Davis, R. Benjamin DeHaye, Michael K. TI Implementation of Speed Variation in the Structural Dynamic Assessment of Turbomachinery Flow Path Components SO JOURNAL OF ENGINEERING FOR GAS TURBINES AND POWER-TRANSACTIONS OF THE ASME LA English DT Article ID TIME-VARYING FREQUENCY AB During the design of turbomachinery flow path components, the assessment of possible structural resonant conditions is critical. Higher frequency modes of these structures are frequently found to be subject to resonance and, in these cases, design criteria require a forced response analysis of the structure with the assumption that the excitation speed exactly equals the resonant frequency. The design becomes problematic if the response analysis shows a violation of the high cycle fatigue (HCF) criteria. One possible solution is to perform a "finite-life" analysis, where Miner's rule is used to calculate the actual life in seconds in comparison to the required life. In this situation, it is beneficial to incorporate the fact that, for a variety of turbomachinery control reasons, the speed of the rotor does not actually dwell at a single value but instead dithers about a nominal mean speed and during the time that the excitation frequency is not equal to the resonant frequency, the damage accumulated by the structure is significantly diminished. Building on previous investigations into this process, we show that a steady-state assumption of the response is extremely accurate for this typical case, resulting in the ability to quickly account for speed variation in the finite-life analysis of a component which has previously had its peak dynamic stress at resonance calculated. A technique using a Monte Carlo simulation is also presented which can be used when specific speed time histories are not available. The implementation of these techniques can prove critical for successful turbo-pump design, since the improvement in life when speed variation is considered is shown to be greater than a factor of two. C1 [Brown, Andrew M.; Davis, R. Benjamin; DeHaye, Michael K.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Brown, AM (reprint author), NASA, Marshall Space Flight Ctr, Mail Code ER41, Huntsville, AL 35812 USA. EM andy.brown@nasa.gov; robert.b.davis@nasa.gov; michael.k.dehaye@nasa.gov OI Davis, R Benjamin /0000-0003-4478-302X NR 7 TC 0 Z9 0 U1 0 U2 5 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 0742-4795 EI 1528-8919 J9 J ENG GAS TURB POWER JI J. Eng. Gas. Turbines Power-Trans. ASME PD OCT PY 2013 VL 135 IS 10 AR 102503 DI 10.1115/1.4024960 PG 6 WC Engineering, Mechanical SC Engineering GA 241IH UT WOS:000326159400012 ER PT J AU Rowe, B Bacon, D Massey, R Heymans, C Haussler, B Taylor, A Rhodes, J Mellier, Y AF Rowe, Barnaby Bacon, David Massey, Richard Heymans, Catherine Haeussler, Boris Taylor, Andy Rhodes, Jason Mellier, Yannick TI Flexion measurement in simulations of Hubble Space Telescope data SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: weak; methods: data analysis; methods: observational; cosmology: observations ID POINT-SPREAD FUNCTION; WEAK-LENSING MEASUREMENTS; GALAXY SHAPE MEASUREMENT; IMAGE-ANALYSIS COMPETITION; ULTRA DEEP FIELD; COSMIC SHEAR; GRAVITATIONAL SHEAR; GREAT08 CHALLENGE; EVOLUTION SURVEY; POLAR SHAPELETS AB We present a simulation analysis of weak gravitational lensing flexion and shear measurement using shapelet decomposition, and identify differences between flexion and shear measurement noise in deep survey data. Taking models of galaxies from the Hubble Space Telescope Ultra Deep Field (HUDF) and applying a correction for the HUDF point spread function, we generate lensed simulations of deep, optical imaging data from Hubble's Advanced Camera for Surveys, with realistic galaxy morphologies. We find that flexion and shear estimates differ in our measurement pipeline: whereas intrinsic galaxy shape is typically the dominant contribution to noise in shear estimates, pixel noise due to finite photon counts and detector read noise is a major contributor to uncertainty in flexion estimates, across a broad range of galaxy signal-to-noise. This pixel noise also increases more rapidly as galaxy signal-to-noise decreases than is found for shear estimates. We provide simple power-law fitting functions for this behaviour, for both flexion and shear, allowing the effect to be properly accounted for in future forecasts for flexion measurement. Using the simulations, we also quantify the systematic biases of our shapelet flexion and shear measurement pipeline for deep Hubble data sets such as Galaxy Evolution from Morphology and SEDs, Space Telescope A901/902 Galaxy Evolution Survey or Cosmic Evolution Survey. Flexion measurement biases are found to be significant but consistent with previous studies. C1 [Rowe, Barnaby] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Rowe, Barnaby; Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rowe, Barnaby; Rhodes, Jason] CALTECH, Pasadena, CA 91106 USA. [Rowe, Barnaby; Mellier, Yannick] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Bacon, David] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 2EG, Hants, England. [Massey, Richard] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Heymans, Catherine; Taylor, Andy] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Haeussler, Boris] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. RP Rowe, B (reprint author), UCL, Dept Phys & Astron, Gower Pl, London WC1E 6BT, England. EM browe@star.ucl.ac.uk OI Rowe, Barnaby/0000-0002-7042-9174 FU European Research Council [240672, 240185]; Jet Propulsion Laboratory; National Science Foundation [PHY-1066293] FX The authors would like to thank Dave Goldberg for interesting discussions in the course of the work that led to this paper, and the anonymous referee for many helpful suggestions and improvements. BR and CH acknowledge support from the European Research Council in the form of a Starting Grant with numbers 240672 (BR) and 240185 (CH). JR and BR were supported by the Jet Propulsion Laboratory, which is run by California Institute of Technology under a contract for NASA. This work was supported in part by the National Science Foundation under Grant No. PHY-1066293 and the hospitality of the Aspen Center for Physics. NR 94 TC 11 Z9 11 U1 0 U2 3 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 OCT PY 2013 VL 435 IS 1 BP 822 EP 844 DI 10.1093/mnras/stt1353 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 236NL UT WOS:000325804300061 ER PT J AU Atwood, SA Reid, JS Kreidenweis, SM Cliff, SS Zhao, YJ Lin, NH Tsay, SC Chu, YC Westphal, DL AF Atwood, Samuel A. Reid, Jeffrey S. Kreidenweis, Sonia M. Cliff, Steven S. Zhao, Yongjing Lin, Neng-Huei Tsay, Si-Chee Chu, Yu-Chi Westphal, Douglas L. TI Size resolved measurements of springtime aerosol particles over the northern South China Sea SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Asian aerosol; Aerosol vertical distributions; Marine aerosol; Dust aerosol; Biomass burning aerosol ID LONG-RANGE TRANSPORT; 7-SEAS/DONGSHA EXPERIMENT; DUST; PRECIPITATION; RESOLUTION; POLLUTANTS; CLOUDS; MASS AB Large sources of aerosol particles and their precursors are ubiquitous in East Asia. Such sources are known to impact the South China Sea (henceforth SCS), a sometimes heavily polluted region that has been suggested as particularly vulnerable to climate change. To help elucidate springtime aerosol transport into the SCS, an intensive study was performed on the remote Dongsha (aka Pratas) Islands Atoll in spring 2010. As part of this deployment, a Davis Rotating-drum Uniform size-cut Monitor (DRUM) cascade impactor was deployed to collect size-resolved aerosol samples at the surface that were analyzed by X-ray fluorescence for concentrations of selected elements. HYSPLIT backtrajectories indicated that the transport of aerosol observed at the surface at Dongsha was occurring primarily from regions generally to the north and east. This observation was consistent with the apparent persistence of pollution and dust aerosol, along with sea salt, in the ground-based dataset. In contrast to the sea-level observations, modeled aerosol transport suggested that the westerly flow aloft (similar to 700 hPa) transported smoke-laden air toward the site from regions from the south and west. Measured aerosol optical depth at the site was highest during time periods of modeled heavy smoke loadings aloft. These periods did not coincide with elevated aerosol concentrations at the surface, although the model suggested sporadic mixing of this free-tropospheric aerosol to the surface over the SCS. A biomass burning signature was not clearly identified in the surface aerosol composition data, consistent with this aerosol type remaining primarily aloft and not mixing strongly to the surface during the study. Significant vertical wind shear in the region also supports the idea that different source regions lead to varying aerosol impacts in different vertical layers, and suggests the potential for considerable vertical inhomogeneity in the SCS aerosol environment. Published by Elsevier Ltd. C1 [Atwood, Samuel A.; Kreidenweis, Sonia M.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Reid, Jeffrey S.; Westphal, Douglas L.] Naval Res Lab, Marine Meteorol Div, Aerosol & Radiat Sect, Monterey, CA 93943 USA. [Lin, Neng-Huei] Natl Cent Univ, Dept Atmospher Sci, Chungli 32054, Taiwan. [Cliff, Steven S.; Zhao, Yongjing] Univ Calif Davis, Air Qual Res Ctr, Davis, CA 95616 USA. [Tsay, Si-Chee] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Chu, Yu-Chi] Taiwan Environm Protect Adm, Taipei, Taiwan. RP Reid, JS (reprint author), Naval Res Lab, Marine Meteorol Div, Aerosol & Radiat Sect, Grace Hopper Ave,Stop 2, Monterey, CA 93943 USA. EM satwood@atmos.colostate.edu; reidj@nrlmry.navy.mil; sonia@atmos.colostate.edu; sscliff@ucdavis.edu; yjzhao@ucdavis.edu; nhlin@cc.ncu.edu.tw; si-chee.tsay@nasa.gov; ycchu@epa.gov.tw; douglas.westphal@nrlmry.navy.mil RI Reid, Jeffrey/B-7633-2014; Tsay, Si-Chee/J-1147-2014; Kreidenweis, Sonia/E-5993-2011 OI Reid, Jeffrey/0000-0002-5147-7955; Kreidenweis, Sonia/0000-0002-2561-2914 FU NRL Base Research Program; Colorado State University Center for Geosciences/Atmospheric Research (CG/AR); Taiwanese Environmental Protection Administration; National Science Council; NASA Radiation Sciences Program FX This work was funded by the NRL Base Research Program and the Colorado State University Center for Geosciences/Atmospheric Research (CG/AR). The Dongsha field site, as part of the international 7SEAS activities, was funded by the Taiwanese Environmental Protection Administration and National Science Council, and by the NASA Radiation Sciences Program for the deployment of the COMMIT mobile laboratory. A portion of the analysis by Samuel Atwood was conducted as part of a Naval Research Enterprise Internship Program (NREIP). We are grateful for the support of the staff and students of the National Central University of Taiwan. We thank the NOAA Air Resources Laboratory for providing the HYSPLIT transport and dispersion model and the converted meteorological fields used in this publication. Finally, we would like to thank members of the Aerosol and Radiation Section for many useful conversations and help with data processing, including James Campbell, Cynthia Curtis, Walter Sessions, and Peng Xian-Lynch, as well as the ALS program including Kevin Perry. NR 41 TC 11 Z9 11 U1 3 U2 40 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 OCT PY 2013 VL 78 SI SI BP 134 EP 143 DI 10.1016/j.atmosenv.2012.11.024 PG 10 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 220RW UT WOS:000324605600012 ER PT J AU Materese, CK Nuevo, M Bera, PP Lee, TJ Sandford, SA AF Materese, Christopher K. Nuevo, Michel Bera, Partha P. Lee, Timothy J. Sandford, Scott A. TI Thymine and Other Prebiotic Molecules Produced from the Ultraviolet Photo-Irradiation of Pyrimidine in Simple Astrophysical Ice Analogs SO ASTROBIOLOGY LA English DT Article DE Pyrimidine; Nucleobases; Interstellar ices; Cometary ices; Molecular processes; Prebiotic chemistry ID POLYCYCLIC AROMATIC-HYDROCARBONS; MURCHISON METEORITE; HETEROCYCLIC-COMPOUNDS; DENSE CLOUDS; BUTYLDIMETHYLSILYL DERIVATIVES; EXTRATERRESTRIAL NUCLEOBASES; CARBONACEOUS METEORITES; INTERSTELLAR MATTER; ORGANIC RESIDUES; RADIATION-FIELD AB The informational subunits of RNA or DNA consist of substituted N-heterocyclic compounds that fall into two groups: those based on purine (C5H4N4) (adenine and guanine) and those based on pyrimidine (C4H4N2) (uracil, cytosine, and thymine). Although not yet detected in the interstellar medium, N-heterocycles, including the nucleobase uracil, have been reported in carbonaceous chondrites. Recent laboratory experiments and ab initio calculations have shown that the irradiation of pyrimidine in ices containing H2O, NH3, or both leads to the abiotic production of substituted pyrimidines, including the nucleobases uracil and cytosine. In this work, we studied the methylation and oxidation of pyrimidine in CH3OH:pyrimidine, H2O:CH3OH:pyrimidine, CH4:pyrimidine, and H2O:CH4:pyrimidine ices irradiated with UV photons under astrophysically relevant conditions. The nucleobase thymine was detected in the residues from some of the mixtures. Our results suggest that the abundance of abiotic thymine produced by ice photolysis and delivered to the early Earth may have been significantly lower than that of uracil. Insofar as the delivery of extraterrestrial molecules was important for early biological chemistry on early Earth, these results suggest that there was more uracil than thymine available for emergent life, a scenario consistent with the RNA world hypothesis. Key Words: PyrimidineNucleobasesInterstellar icesCometary icesMolecular processesPrebiotic chemistry. Astrobiology 13, 948-962. C1 [Materese, Christopher K.; Nuevo, Michel; Bera, Partha P.; Lee, Timothy J.; Sandford, Scott A.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Materese, Christopher K.; Nuevo, Michel] SETI Inst, Mountain View, CA USA. [Bera, Partha P.] Bay Area Environm Res Inst, Sonoma, CA USA. RP Sandford, SA (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. EM Scott.A.Sandford@nasa.gov RI Lee, Timothy/K-2838-2012; Bera, Partha /K-8677-2012 FU NASA grants from the NASA Astrobiology Institute; Origins of Solar Systems programs; NASA FX This work was supported by NASA grants from the NASA Astrobiology Institute and Origins of Solar Systems programs. C. K. M., M.N., and S. A. S. would like to acknowledge R. L. Walker (NASA Ames) for technical support. P. P. B. and T.J.L. would like to acknowledge financial support from NASA to investigate the formation and evolution of carbon-based material in the Universe. We would also like to thank two anonymous reviewers of this manuscript for useful comments and suggestions. NR 49 TC 14 Z9 14 U1 2 U2 30 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 OCT 1 PY 2013 VL 13 IS 10 BP 948 EP 962 DI 10.1089/ast.2013.1044 PG 15 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 237FS UT WOS:000325854600005 PM 24143868 ER PT J AU Smith, DJ AF Smith, David J. TI Microbes in the Upper Atmosphere and Unique Opportunities for Astrobiology Research SO ASTROBIOLOGY LA English DT Review DE Microbe; Aerobiology; Upper atmosphere; Stratosphere; Sampling ID SIMULATED MARTIAN CONDITIONS; EXPERIMENT PROTECT; ORGANIC-CARBON; PLANETARY PROTECTION; DIFFERENT ECOSYSTEMS; GLOBAL ATMOSPHERE; FUNGAL SPORES; NORTH-AMERICA; AIR SAMPLES; DOME FRANCE AB Microbial taxa from every major biological lineage have been detected in Earth's upper atmosphere. The goal of this review is to communicate (1) relevant astrobiology questions that can be addressed with upper atmosphere microbiology studies and (2) available sampling methods for collecting microbes at extreme altitudes. Precipitation, mountain stations, airplanes, balloons, rockets, and satellites are all feasible routes for conducting aerobiology research. However, more efficient air samplers are needed, and contamination is also a pervasive problem in the field. Measuring microbial signatures without false positives in the upper atmosphere might contribute to sterilization and bioburden reduction methods for proposed astrobiology missions. Intriguingly, environmental conditions in the upper atmosphere resemble the surface conditions of Mars (extreme cold, hypobaria, desiccation, and irradiation). Whether terrestrial microbes are active in the upper atmosphere is an area of intense research interest. If, in fact, microbial metabolism, growth, or replication is achievable independent of Earth's surface, then the search for habitable zones on other worlds should be broadened to include atmospheres (e.g., the high-altitude clouds of Venus). Furthermore, viable cells in the heavily irradiated upper atmosphere of Earth could help identify microbial genes or enzymes that bestow radiation resistance. Compelling astrobiology questions on the origin of life (if the atmosphere synthesized organic aerosols), evolution (if airborne transport influenced microbial mutation rates and speciation), and panspermia (outbound or inbound) are also testable in Earth's upper atmosphere. Key Words: MicrobeAerobiologyUpper atmosphereStratosphereSampling. Astrobiology 13, 981-990. C1 NASA, John F Kennedy Space Ctr, Surface Syst Off, Kennedy Space Ctr, FL 32899 USA. RP Smith, DJ (reprint author), NASA, John F Kennedy Space Ctr, Surface Syst Off, Mail Code NE S, Kennedy Space Ctr, FL 32899 USA. EM david.j.smith-3@nasa.gov NR 113 TC 9 Z9 9 U1 4 U2 75 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 OCT 1 PY 2013 VL 13 IS 10 BP 981 EP 990 DI 10.1089/ast.2013.1074 PG 10 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 237FS UT WOS:000325854600007 PM 24106911 ER PT J AU Abdo, AA Ajello, M Allafort, A Baldini, L Ballet, J Barbiellini, G Baring, MG Bastieri, D Belfiore, A Bellazzini, R Bhattacharyya, B Bissaldi, E Bloom, ED Bonamente, E Bottacini, E Brandt, TJ Bregeon, J Brigida, M Bruel, P Buehler, R Burgay, M Burnett, TH Busetto, G Buson, S Caliandro, GA Cameron, RA Camilo, F Caraveo, PA Casandjian, JM Cecchi, C Celik, O Charles, E Chaty, S Chaves, RCG Chekhtman, A Chen, AW Chiang, J Chiaro, G Ciprini, S Claus, R Cognard, I Cohen-Tanugi, J Cominsky, LR Conrad, J Cutini, S D'Ammando, F De Angelis, A DeCesar, ME De Luca, A Den Hartog, PR De Palma, F Dermer, CD Desvignes, G Digel, SW Di Venere, L Drell, PS Drlica-Wagner, A Dubois, R Dumora, D Espinoza, CM Falletti, L Favuzzi, C Ferrara, EC Focke, WB Franckowiak, A Freire, PCC Funk, S Fusco, P Gargano, F Gasparrini, D Germani, S Giglietto, N Giommi, P Giordano, F Giroletti, M Glanzman, T Godfrey, G Gotthelf, EV Grenier, IA Grondin, MH Grove, JE Guillemot, L Guiriec, S Hadasch, D Hanabata, Y Harding, AK Hayashida, M Hays, E Hessels, J Hewitt, J Hill, AB Horan, D Hou, X Hughes, RE Jackson, MS Janssen, GH Jogler, T Johannesson, G Johnson, RP Johnson, AS Johnson, TJ Johnson, WN Johnston, S Kamae, T Kataoka, J Keith, M Kerr, M Knodlseder, J Kramer, M Kuss, M Lande, J Larsson, S Latronico, L Lemoine-Goumard, M Longo, F Loparco, F Lovellette, MN Lubrano, P Lyne, AG Manchester, RN Marelli, M Massaro, F Mayer, M Mazziotta, MN McEnery, JE McLaughlin, MA Mehault, J Michelson, PF Mignani, RP Mitthumsiri, W Mizuno, T Moiseev, AA Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nakamori, T Nemmen, R Nuss, E Ohno, M Ohsugi, T Orienti, M Orlando, E Ormes, JF Paneque, D Panetta, JH Parent, D Perkins, JS Pesce-Rollins, M Pierbattista, M Piron, F Pivato, G Pletsch, HJ Porter, TA Possenti, A Raino, S Rando, R Ransom, SM Ray, PS Razzano, M Rea, N Reimer, A Reimer, O Renault, N Reposeur, T Ritz, S Romani, RW Roth, M Rousseau, R Roy, J Ruan, J Sartori, A Parkinson, PMS Scargle, JD Schulz, A Sgro, C Shannon, R Siskind, EJ Smith, DA Spandre, G Spinelli, P Stappers, BW Strong, AW Suson, DJ Takahashi, H Thayer, JG Thayer, JB Theureau, G Thompson, DJ Thorsett, SE Tibaldo, L Tibolla, O Tinivella, M Torres, DF Tosti, G Troja, E Uchiyama, Y Usher, TL Vandenbroucke, J Vasileiou, V Venter, C Vianello, G Vitale, V Wang, N Weltevrede, P Winer, BL Wolff, MT Wood, DL Wood, KS Wood, M Yang, Z AF Abdo, A. A. Ajello, M. Allafort, A. Baldini, L. Ballet, J. Barbiellini, G. Baring, M. G. Bastieri, D. Belfiore, A. Bellazzini, R. Bhattacharyya, B. Bissaldi, E. Bloom, E. D. Bonamente, E. Bottacini, E. Brandt, T. J. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Burgay, M. Burnett, T. H. Busetto, G. Buson, S. Caliandro, G. A. Cameron, R. A. Camilo, F. Caraveo, P. A. Casandjian, J. M. Cecchi, C. Celik, Oe . Charles, E. Chaty, S. Chaves, R. C. G. Chekhtman, A. Chen, A. W. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. Cognard, I. Cohen-Tanugi, J. Cominsky, L. R. Conrad, J. Cutini, S. D'Ammando, F. De Angelis, A. DeCesar, M. E. De Luca, A. Den Hartog, P. R. De Palma, F. Dermer, C. D. Desvignes, G. Digel, S. W. Di Venere, L. Drell, P. S. Drlica-Wagner, A. Dubois, R. Dumora, D. Espinoza, C. M. Falletti, L. Favuzzi, C. Ferrara, E. C. Focke, W. B. Franckowiak, A. Freire, P. C. C. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Germani, S. Giglietto, N. Giommi, P. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Gotthelf, E. V. Grenier, I. A. Grondin, M. -H. Grove, J. E. Guillemot, L. Guiriec, S. Hadasch, D. Hanabata, Y. Harding, A. K. Hayashida, M. Hays, E. Hessels, J. Hewitt, J. Hill, A. B. Horan, D. Hou, X. Hughes, R. E. Jackson, M. S. Janssen, G. H. Jogler, T. Johannesson, G. Johnson, R. P. Johnson, A. S. Johnson, T. J. Johnson, W. N. Johnston, S. Kamae, T. Kataoka, J. Keith, M. Kerr, M. Knoedlseder, J. Kramer, M. Kuss, M. Lande, J. Larsson, S. Latronico, L. Lemoine-Goumard, M. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Lyne, A. G. Manchester, R. N. Marelli, M. Massaro, F. Mayer, M. Mazziotta, M. N. McEnery, J. E. McLaughlin, M. A. Mehault, J. Michelson, P. F. Mignani, R. P. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nakamori, T. Nemmen, R. Nuss, E. Ohno, M. Ohsugi, T. Orienti, M. Orlando, E. Ormes, J. F. Paneque, D. Panetta, J. H. Parent, D. Perkins, J. S. Pesce-Rollins, M. Pierbattista, M. Piron, F. Pivato, G. Pletsch, H. J. Porter, T. A. Possenti, A. Raino, S. Rando, R. Ransom, S. M. Ray, P. S. Razzano, M. Rea, N. Reimer, A. Reimer, O. Renault, N. Reposeur, T. Ritz, S. Romani, R. W. Roth, M. Rousseau, R. Roy, J. Ruan, J. Sartori, A. Parkinson, P. M. Saz Scargle, J. D. Schulz, A. Sgro, C. Shannon, R. Siskind, E. J. Smith, D. A. Spandre, G. Spinelli, P. Stappers, B. W. Strong, A. W. Suson, D. J. Takahashi, H. Thayer, J. G. Thayer, J. B. Theureau, G. Thompson, D. J. Thorsett, S. E. Tibaldo, L. Tibolla, O. Tinivella, M. Torres, D. F. Tosti, G. Troja, E. Uchiyama, Y. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Venter, C. Vianello, G. Vitale, V. Wang, N. Weltevrede, P. Winer, B. L. Wolff, M. T. Wood, D. L. Wood, K. S. Wood, M. Yang, Z. TI THE SECOND FERMI LARGE AREA TELESCOPE CATALOG OF GAMMA-RAY PULSARS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; pulsars: general; stars: neutron ID WHITE-DWARF COMPANION; MIDDLE-AGED PULSAR; SUPERNOVA REMNANT G21.5-0.9; DEEP OPTICAL OBSERVATIONS; NANCAY RADIO TELESCOPE; PHOTON IMAGING CAMERA; MILLISECOND PULSARS; WIND NEBULA; LIGHT CURVES; CRAB PULSAR AB This catalog summarizes 117 high-confidence >= 0.1 GeV gamma-ray pulsar detections using three years of data acquired by the Large Area Telescope (LAT) on the Fermi satellite. Half are neutron stars discovered using LAT data through periodicity searches in gamma-ray and radio data around LAT unassociated source positions. The 117 pulsars are evenly divided into three groups: millisecond pulsars, young radio-loud pulsars, and young radio-quiet pulsars. We characterize the pulse profiles and energy spectra and derive luminosities when distance information exists. Spectral analysis of the off-peak phase intervals indicates probable pulsar wind nebula emission for four pulsars, and off-peak magnetospheric emission for several young and millisecond pulsars. We compare the gamma-ray properties with those in the radio, optical, and X-ray bands. We provide flux limits for pulsars with no observed gamma-ray emission, highlighting a small number of gamma-faint, radio-loud pulsars. The large, varied gamma-ray pulsar sample constrains emission models. Fermi's selection biases complement those of radio surveys, enhancing comparisons with predicted population distributions. C1 [Abdo, A. A.; Chekhtman, A.; Parent, D.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Allafort, A.; Bloom, E. D.; Bottacini, E.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Den Hartog, P. R.; Digel, S. W.; Di Venere, L.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Kamae, T.; Kerr, M.; Lande, J.; Massaro, F.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Allafort, A.; Bloom, E. D.; Bottacini, E.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Den Hartog, P. R.; Digel, S. W.; Di Venere, L.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Kamae, T.; Kerr, M.; Lande, J.; Massaro, F.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Baldini, L.] Univ Pisa, Ist Nazl Fis Nucl, Sezione Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Chaty, S.; Chaves, R. C. G.; Grenier, I. A.; Renault, N.] Univ Paris Diderot, CNRS, CEA IRFU, CEA Saclay,Lab AIM,Serv Astrophys, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sezione Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy. [Baring, M. G.] Rice Univ, Dept Phys & Astron, MS 108, Houston, TX 77251 USA. [Bastieri, D.; Busetto, G.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sezione Padova, I-35131 Padua, Italy. [Bastieri, D.; Busetto, G.; Buson, S.; Chiaro, G.; Pivato, G.; Rando, R.] Univ Padua, Dipartimento Fis Astron G Galilei, I-35131 Padua, Italy. [Belfiore, A.; Johnson, R. P.; Razzano, M.; Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Belfiore, A.; Johnson, R. P.; Razzano, M.; Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Belfiore, A.] Univ Pavia, I-27100 Pavia, Italy. [Belfiore, A.; Caraveo, P. A.; Chen, A. W.; Marelli, M.; Mignani, R. P.; Pierbattista, M.; Sartori, A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sezione Pisa, I-56127 Pisa, Italy. [Bhattacharyya, B.; Roy, J.] Natl Ctr Radio Astrophys, Tata Inst Fundamental Res, Pune 411007, Maharashtra, India. [Bissaldi, E.] Ist Nazl Fis Nucl, Sezione Trieste, I-34127 Trieste, Italy. [Bissaldi, E.] Univ Trieste, I-34127 Trieste, Italy. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sezione Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brandt, T. J.; Celik, Oe .; DeCesar, M. E.; Ferrara, E. C.; Guiriec, S.; Harding, A. K.; Hays, E.; Hewitt, J.; McEnery, J. E.; Nemmen, R.; Perkins, J. S.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Brigida, M.; De Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] M Merlin Univ Politecn Bari, Dipartimento Fis, I-70126 Bari, Italy. [Brigida, M.; De Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. 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[Celik, Oe .] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Ciprini, S.; Cutini, S.; Gasparrini, D.; Giommi, P.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Monte Porzio Catone, Italy. [Cognard, I.; Desvignes, G.; Theureau, G.] CNRS, LPCE, UMR 6115, F-45071 Orleans 02, France. [Cognard, I.; Desvignes, G.; Theureau, G.] CNRS, INSU, Stn radioastronomie Nancay, Observ Paris, F-18330 Nancay, France. [Cohen-Tanugi, J.; Desvignes, G.; Falletti, L.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univ & Particules Montpellier, Montpellier, France. [Cominsky, L. R.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA. [Conrad, J.; Larsson, S.; Yang, Z.] Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden. [Conrad, J.; Jackson, M. 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[Dumora, D.; Hou, X.; Lemoine-Goumard, M.; Mehault, J.; Reposeur, T.; Rousseau, R.; Smith, D. A.] Univ Bordeaux 1, CEN Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France. [Espinoza, C. M.; Janssen, G. H.; Kramer, M.; Lyne, A. G.; Stappers, B. W.; Weltevrede, P.] Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Manchester M13 9PL, Lancs, England. [Grondin, M. -H.; Knoedlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France. [Grondin, M. -H.; Knoedlseder, J.] Univ Toulouse, UPS, GAHEC, IRAP,OMP, Toulouse, France. [Hanabata, Y.; Ohno, M.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Hessels, J.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Hessels, J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hughes, R. E.; Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Dept Phys, Columbus, OH 43210 USA. [Jackson, M. S.] AlbaNova, Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Johnson, T. J.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Johnson, T. J.; Johnston, S.; Keith, M.; Manchester, R. N.; Shannon, R.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Latronico, L.] Ist Nazl Fis Nucl, Sezione Torino, I-10125 Turin, Italy. [McLaughlin, M. A.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. [Mignani, R. P.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Mignani, R. 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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. [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. [Thorsett, S. E.] Willamette Univ, Dept Phys, Salem, OR 97031 USA. [Tibolla, O.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [Torres, D. F.] ICREA, Barcelona, Spain. [Uchiyama, Y.] Rikkyo Univ, Toshima Ku, Tokyo 1718501, Japan. [Venter, C.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Wang, N.] NAOC, Urumqi Observ, Xinjiang 830011, Peoples R China. [Wood, D. L.] Praxis Inc, Alexandria, VA 22303 USA. RP Abdo, AA (reprint author), George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. EM ozlemceliktinmaz@gmail.com; hartog@stanford.edu; kerrm@stanford.edu; joshualande@gmail.com; smith@cenbg.in2p3.fr RI giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016; Bissaldi, Elisabetta/K-7911-2016; Massaro, Francesco/L-9102-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Di Venere, Leonardo/C-7619-2017; Venter, Christo/E-6884-2011; Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Funk, Stefan/B-7629-2015; Rea, Nanda/I-2853-2015; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; OI Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; 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; De Luca, Andrea/0000-0001-6739-687X; Giroletti, Marcello/0000-0002-8657-8852; Ransom, Scott/0000-0001-5799-9714; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; Bissaldi, Elisabetta/0000-0001-9935-8106; Massaro, Francesco/0000-0002-1704-9850; Torres, Diego/0000-0002-1522-9065; Di Venere, Leonardo/0000-0003-0703-824X; Thorsett, Stephen/0000-0002-2025-9613; giommi, paolo/0000-0002-2265-5003; Shannon, Ryan/0000-0002-7285-6348; Burgay, Marta/0000-0002-8265-4344; Caraveo, Patrizia/0000-0003-2478-8018; Venter, Christo/0000-0002-2666-4812; Reimer, Olaf/0000-0001-6953-1385; Morselli, Aldo/0000-0002-7704-9553; Funk, Stefan/0000-0002-2012-0080; Rea, Nanda/0000-0003-2177-6388; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726; Ray, Paul/0000-0002-5297-5278; Marelli, Martino/0000-0002-8017-0338 FU Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France FX The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the 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 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. The Green Bank Telescope is operated by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The Arecibo Observatory is part of the National Astronomy and Ionosphere Center (NAIC), a national research center operated by Cornell University under a cooperative agreement with the National Science Foundation. The Nancay Radio Observatory is operated by the Paris Observatory, associated with the French Centre National de la Recherche Scientifique (CNRS). The Lovell Telescope is owned and operated by the University of Manchester as part of the Jodrell Bank Centre for Astrophysics with support from the Science and Technology Facilities Council of the United Kingdom. TheWesterbork Synthesis Radio Telescope is operated by Netherlands Foundation for Radio Astronomy, ASTRON. This work made extensive use of the ATNF pulsar catalog (Manchester et al. 2005). NR 264 TC 237 Z9 237 U1 1 U2 30 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD OCT PY 2013 VL 208 IS 2 AR UNSP 17 DI 10.1088/0067-0049/208/2/17 PG 59 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 229OM UT WOS:000325276600004 ER PT J AU Bennett, CL Larson, D Weiland, JL Jarosik, N Hinshaw, G Odegard, N Smith, KM Hill, RS Gold, B Halpern, M Komatsu, E Nolta, MR Page, L Spergel, DN Wollack, E Dunkley, J Kogut, A Limon, M Meyer, SS Tucker, GS Wright, EL AF Bennett, C. L. Larson, D. Weiland, J. L. Jarosik, N. Hinshaw, G. Odegard, N. Smith, K. M. Hill, R. S. Gold, B. Halpern, M. Komatsu, E. Nolta, M. R. Page, L. Spergel, D. N. Wollack, E. Dunkley, J. Kogut, A. Limon, M. Meyer, S. S. Tucker, G. S. Wright, E. L. TI NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: FINAL MAPS AND RESULTS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmic background radiation; cosmology: observations; dark matter; early universe; instrumentation: detectors; space vehicles; space vehicles: instruments; telescopes ID NRAO PMN SURVEYS; OBSERVATIONS COSMOLOGICAL INTERPRETATION; GALACTIC FOREGROUND EMISSION; SYSTEMATIC-ERROR LIMITS; ANGULAR POWER SPECTRUM; POINT-SOURCE SEARCH; H-ALPHA EMISSION; SOURCE CATALOG; RADIOMETER CHARACTERIZATION; BACKGROUND ANISOTROPIES AB We present the final nine-year maps and basic results from the Wilkinson Microwave Anisotropy Probe (WMAP) mission. The full nine-year analysis of the time-ordered data provides updated characterizations and calibrations of the experiment. We also provide new nine-year full sky temperature maps that were processed to reduce the asymmetry of the effective beams. Temperature and polarization sky maps are examined to separate cosmic microwave background (CMB) anisotropy from foreground emission, and both types of signals are analyzed in detail. We provide new point source catalogs as well as new diffuse and point source foreground masks. An updated template-removal process is used for cosmological analysis; new foreground fits are performed, and new foreground reduced CMB maps are presented. We now implement an optimal C-1 weighting to compute the temperature angular power spectrum. The WMAP mission has resulted in a highly constrained Delta CDM cosmological model with precise and accurate parameters in agreement with a host of other cosmological measurements. When WMAP data are combined with finer scale CMB, baryon acoustic oscillation, and Hubble constant measurements, we find that big bang nucleosynthesis is well supported and there is no compelling evidence for a non-standard number of neutrino species (N-eff = 3.84 +/- 0.40). The model fit also implies that the age of the universe is t(0) = 13.772 +/- 0.059 Gyr, and the fit Hubble constant is H-0 = 69.32 +/- 0.80 km s(-1) Mpc(-1). Inflation is also supported: the fluctuations are adiabatic, with Gaussian random phases; the detection of a deviation of the scalar spectral index from unity, reported earlier by the WMAP team, now has high statistical significance (n(s) = 0.9608 +/- 0.0080); and the universe is close to flat/Euclidean (Omega(k) = -0.0027(-0.0038)(+0.0039)). Overall, the WMAP mission has resulted in a reduction of the cosmological parameter volume by a factor of 68,000 for the standard six-parameter Delta CDM model, based on CMB data alone. For a model including tensors, the allowed seven-parameter volume has been reduced by a factor 117,000. Other cosmological observations are in accord with the CMB predictions, and the combined data reduces the cosmological parameter volume even further. With no significant anomalies and an adequate goodness of fit, the inflationary flat Delta CDM model and its precise and accurate parameters rooted in WMAP data stands as the standard model of cosmology. C1 [Bennett, C. L.; Larson, D.; Weiland, J. L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Jarosik, N.; Page, L.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Hinshaw, G.; Halpern, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Odegard, N.; Hill, R. S.] ADNET Syst Inc, Lanham, MD 20706 USA. [Smith, K. M.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [Smith, K. M.; Spergel, D. N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Gold, B.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Komatsu, E.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Komatsu, E.; Spergel, D. N.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe, Kavli IPMU,WPI, Kashiwa, Chiba 2778583, Japan. [Komatsu, E.] Univ Texas Austin, Texas Cosmol Ctr, Austin, TX 78712 USA. [Komatsu, E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Nolta, M. R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Wollack, E.; Kogut, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dunkley, J.] Oxford Astrophys, Oxford OX1 3RH, England. [Limon, M.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Meyer, S. S.] Univ Chicago, KICP, Dept Astrophys, Chicago, IL 60637 USA. [Meyer, S. S.] Univ Chicago, KICP, Dept Phys, Chicago, IL 60637 USA. [Meyer, S. S.] Univ Chicago, EFI, Chicago, IL 60637 USA. [Tucker, G. S.] Brown Univ, Dept Phys, Providence, RI 02912 USA. [Wright, E. L.] UCLA Phys & Astron, Los Angeles, CA 90095 USA. RP Bennett, CL (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA. EM cbennett@jhu.edu RI Wollack, Edward/D-4467-2012; OI Wollack, Edward/0000-0002-7567-4451; Limon, Michele/0000-0002-5900-2698 FU Johns Hopkins University; Perimeter Institute by the Government of Canada through Industry Canada; Province of Ontario through the Ministry of Research Innovation; NASA [NNX08AL43G, NNX11AD25G]; NSF [AST-0807649, PHY-0758153]; Canada Foundation for Innovation under Compute Canada; Government of Ontario; Ontario Research Fund-Research Excellence; University of Toronto; NASA Headquarters FX C.L.B. was supported, in part, by the Johns Hopkins University. K. M. S. was supported at the Perimeter Institute by the Government of Canada through Industry Canada and by the Province of Ontario through the Ministry of Research & Innovation. E. K. was supported in part by NASA grants NNX08AL43G and NNX11AD25G and NSF grants AST-0807649 and PHY-0758153. We acknowledge use of the HEALPix (Gorski et al. 2005), CAMB (Lewis et al. 2000), and CMBFAST (Seljak & Zaldarriaga 1996) packages. Some computations were performed on the GPC supercomputer at the SciNet HPC Consortium. We thank SciNet, which is funded by the Canada Foundation for Innovation under the auspices of Compute Canada, the Government of Ontario, Ontario Research Fund-Research Excellence, and the University of Toronto. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by NASA Headquarters. NR 136 TC 715 Z9 718 U1 10 U2 52 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 OCT PY 2013 VL 208 IS 2 AR UNSP 20 DI 10.1088/0067-0049/208/2/20 PG 54 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 229OM UT WOS:000325276600007 ER PT J AU Goldstein, A Preece, RD Mallozzi, RS Briggs, MS Fishman, GJ Kouveliotou, C Paciesas, WS Burgess, JM AF Goldstein, Adam Preece, Robert D. Mallozzi, Robert S. Briggs, Michael S. Fishman, Gerald J. Kouveliotou, Chryssa Paciesas, William S. Burgess, J. Michael TI THE BATSE 5B GAMMA-RAY BURST SPECTRAL CATALOG SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE gamma-ray burst: general; methods: data analysis ID LARGE-AREA DETECTORS; PROMPT EMISSION; VARIABILITY; PEAK; SPECTROSCOPY; CALIBRATION; BEPPOSAX; MODEL; RATIO; TIME AB We present systematic spectral analyses of gamma-ray bursts (GRBs) detected with the Burst and Transient Source Experiment (BATSE) on board the Compton Gamma-Ray Observatory during its entire nine years of operation. This catalog contains two types of spectra extracted from 2145 GRBs, and fitted with five different spectral models resulting in a compendium of over 19,000 spectra. The models were selected based on their empirical importance to the spectral shape of many GRBs, and the analysis performed was devised to be as thorough and objective as possible. We describe in detail our procedures and criteria for the analyses, and present the bulk results in the form of parameter distributions. This catalog should be considered an official product from the BATSE Science Team, and the data files containing the complete results are available from the High-Energy Astrophysics Science Archive Research Center (HEASARC). C1 [Goldstein, Adam; Preece, Robert D.; Briggs, Michael S.; Burgess, J. Michael] Univ Alabama, Huntsville, AL 35899 USA. [Fishman, Gerald J.; Kouveliotou, Chryssa] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. [Paciesas, William S.] Univ Space Res Assoc, Huntsville, AL 35805 USA. RP Goldstein, A (reprint author), Univ Alabama, 320 Sparkman Dr, Huntsville, AL 35899 USA. OI Preece, Robert/0000-0003-1626-7335; Burgess, James/0000-0003-3345-9515 FU Graduate Student Researchers Program; NASA FX A.G. acknowledges the support of the Graduate Student Researchers Program funded by NASA. NR 46 TC 24 Z9 24 U1 1 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 OCT PY 2013 VL 208 IS 2 AR UNSP 21 DI 10.1088/0067-0049/208/2/21 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 229OM UT WOS:000325276600008 ER PT J AU Hinshaw, G Larson, D Komatsu, E Spergel, DN Bennett, CL Dunkley, J Nolta, MR Halpern, M Hill, RS Odegard, N Page, L Smith, KM Weiland, JL Gold, B Jarosik, N Kogut, A Limon, M Meyer, SS Tucker, GS Wollack, E Wright, EL AF Hinshaw, G. Larson, D. Komatsu, E. Spergel, D. N. Bennett, C. L. Dunkley, J. Nolta, M. R. Halpern, M. Hill, R. S. Odegard, N. Page, L. Smith, K. M. Weiland, J. L. Gold, B. Jarosik, N. Kogut, A. Limon, M. Meyer, S. S. Tucker, G. S. Wollack, E. Wright, E. L. TI NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL PARAMETER RESULTS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmic background radiation; cosmology: observations; dark matter; early universe; instrumentation: detectors; space vehicles; space vehicles: instruments; telescopes ID BARYON ACOUSTIC-OSCILLATIONS; SOUTH-POLE TELESCOPE; DIGITAL SKY SURVEY; SUPERNOVA LEGACY SURVEY; HUBBLE-SPACE-TELESCOPE; BACKGROUND POWER SPECTRUM; BRIGHTEST CLUSTER SAMPLE; MASSIVE GALAXY CLUSTERS; IA SUPERNOVAE; DARK ENERGY AB We present cosmological parameter constraints based on the final nine-year Wilkinson Microwave Anisotropy Probe (WMAP) data, in conjunction with a number of additional cosmological data sets. The WMAP data alone, and in combination, continue to be remarkably well fit by a six-parameter Delta CDM model. When WMAP data are combined with measurements of the high-l cosmic microwave background anisotropy, the baryon acoustic oscillation scale, and the Hubble constant, the matter and energy densities, Omega(b)h(2), Omega(c)h(2), and Omega(Lambda), are each determined to a precision of similar to 1.5%. The amplitude of the primordial spectrum is measured to within 3%, and there is now evidence for a tilt in the primordial spectrum at the 5 sigma level, confirming the first detection of tilt based on the five-year WMAP data. At the end of the WMAP mission, the nine-year data decrease the allowable volume of the six-dimensional Delta CDM parameter space by a factor of 68,000 relative to pre-WMAP measurements. We investigate a number of data combinations and show that their Delta CDM parameter fits are consistent. New limits on deviations from the six-parameter model are presented, for example: the fractional contribution of tensor modes is limited to r < 0.13 (95% CL); the spatial curvature parameter is limited to Omega(k) = -0.0027(-0.0038)(+0.0039); the summed mass of neutrinos is limited to Sigma m(nu) < 0.44 eV (95% CL); and the number of relativistic species is found to lie within N-eff = 3.84 +/- 0.40, when the full data are analyzed. The joint constraint on N-eff and the primordial helium abundance, Y-He, agrees with the prediction of standard big bang nucleosynthesis. We compare recent Planck measurements of the Sunyaev-Zel'dovich effect with our seven-year measurements, and show their mutual agreement. Our analysis of the polarization pattern around temperature extrema is updated. This confirms a fundamental prediction of the standard cosmological model and provides a striking illustration of acoustic oscillations and adiabatic initial conditions in the early universe. C1 [Hinshaw, G.; Halpern, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Larson, D.; Bennett, C. L.; Weiland, J. L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Komatsu, E.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Komatsu, E.; Spergel, D. N.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe, Kavli IPMU,WPI, Kashiwa, Chiba 2778583, Japan. [Komatsu, E.] Univ Texas Austin, Texas Cosmol Ctr, Austin, TX 78712 USA. [Komatsu, E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Spergel, D. N.; Smith, K. M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Dunkley, J.] Oxford Astrophys, Oxford OX1 3RH, England. [Nolta, M. R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Hill, R. S.; Odegard, N.] ADNET Syst Inc, Lanham, MD 20706 USA. [Page, L.; Jarosik, N.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Smith, K. M.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [Gold, B.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Kogut, A.; Wollack, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Limon, M.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Meyer, S. S.] Univ Chicago, KICP, Dept Astrophys, Chicago, IL 60637 USA. [Meyer, S. S.] Univ Chicago, KICP, Dept Phys, Chicago, IL 60637 USA. [Meyer, S. S.] Univ Chicago, EFI, Chicago, IL 60637 USA. [Tucker, G. S.] Brown Univ, Dept Phys, Providence, RI 02912 USA. [Wright, E. L.] UCLA Phys & Astron, Los Angeles, CA 90095 USA. RP Hinshaw, G (reprint author), Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. EM hinshaw@physics.ubc.ca RI Wollack, Edward/D-4467-2012; OI Wollack, Edward/0000-0002-7567-4451; Limon, Michele/0000-0002-5900-2698 FU Canadian Institute for Advanced Research; Johns Hopkins University; Perimeter Institute by the Government of Canada through Industry Canada; Province of Ontario through the Ministry of Research Innovation; NASA [NNX08AL43G, NNX11AD25G]; NSF [AST-0807649, PHY-0758153]; Canada Foundation for Innovation under Compute Canada; Government of Ontario; Ontario Research Fund-Research Excellence; University of Toronto; NASA Headquarters FX G.H. was supported, in part, by the Canadian Institute for Advanced Research. C. L. B. was supported, in part, by the Johns Hopkins University. K. M. S. was supported at the Perimeter Institute by the Government of Canada through Industry Canada and by the Province of Ontario through the Ministry of Research & Innovation. E. K. was supported in part by NASA grants NNX08AL43G and NNX11AD25G and NSF grants AST-0807649 and PHY-0758153. We acknowledge use of the HEALPix (Gorski et al. 2005), CAMB(Lewis et al. 2000), and CMBFAST (Seljak & Zaldarriaga 1996) packages. Some computations were performed on the GPC supercomputer at the SciNet HPC Consortium. We thank SciNet, which is funded by the Canada Foundation for Innovation under the auspices of Compute Canada, the Government of Ontario, Ontario Research Fund-Research Excellence, and the University of Toronto. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by NASA Headquarters. NR 200 TC 1606 Z9 1607 U1 10 U2 84 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 OCT PY 2013 VL 208 IS 2 AR UNSP 19 DI 10.1088/0067-0049/208/2/19 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 229OM UT WOS:000325276600006 ER PT J AU Mazeh, T Nachmani, G Holczer, T Fabrycky, DC Ford, EB Sanchis-Ojeda, R Sokol, G Rowe, JF Zucker, S Agol, E Carter, JA Lissauer, JJ Quintana, EV Ragozzine, D Steffen, JH Welsh, W AF Mazeh, Tsevi Nachmani, Gil Holczer, Tomer Fabrycky, Daniel C. Ford, Eric B. Sanchis-Ojeda, Roberto Sokol, Gil Rowe, Jason F. Zucker, Shay Agol, Eric Carter, Joshua A. Lissauer, Jack J. Quintana, Elisa V. Ragozzine, Darin Steffen, Jason H. Welsh, William TI TRANSIT TIMING OBSERVATIONS FROM KEPLER. VIII. CATALOG OF TRANSIT TIMING MEASUREMENTS OF THE FIRST TWELVE QUARTERS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE planetary systems; planets and satellites: detection; techniques: miscellaneous; techniques: photometric ID MULTIPLE-PLANET SYSTEMS; HOT-JUPITER; LIGHT CURVES; CONFIRMATION; CANDIDATES; MASS; ARCHITECTURE; PHOTOMETRY; OBLIQUITY; MODELS AB Following the works of Ford et al. and Steffen et al. we derived the transit timing of 1960 Kepler objects of interest (KOIs) using the pre-search data conditioning light curves of the first twelve quarters of the Kepler data. For 721 KOIs with large enough signal-to-noise ratios, we obtained also the duration and depth of each transit. The results are presented as a catalog for the community to use. We derived a few statistics of our results that could be used to indicate significant variations. Including systems found by previous works, we have found 130 KOIs that showed highly significant times of transit variations (TTVs) and 13 that had short-period TTV modulations with small amplitudes. We consider two effects that could cause apparent periodic TTV-the finite sampling of the observations and the interference with the stellar activity, stellar spots in particular. We briefly discuss some statistical aspects of our detected TTVs. We show that the TTV period is correlated with the orbital period of the planet and with the TTV amplitude. C1 [Mazeh, Tsevi; Nachmani, Gil; Holczer, Tomer; Sokol, Gil] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Fabrycky, Daniel C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Ford, Eric B.; Ragozzine, Darin] Univ Florida, Dept Astron, Gainesville, FL 32111 USA. [Sanchis-Ojeda, Roberto] MIT, Dept Phys, Cambridge, MA 02139 USA. [Sanchis-Ojeda, Roberto] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Rowe, Jason F.; Lissauer, Jack J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Zucker, Shay] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Dept Geophys Atmospher & Planetary Sci, IL-69978 Tel Aviv, Israel. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Carter, Joshua A.] Harvard Univ, Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Quintana, Elisa V.] SETI Inst, Mountain View, CA 94043 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Welsh, William] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. RP Mazeh, T (reprint author), Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. OI /0000-0002-0802-9145; /0000-0001-6545-639X; Fabrycky, Daniel/0000-0003-3750-0183 FU European Research Council under the EU [291352]; ISRAEL SCIENCE FOUNDATION [1423/11]; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G] FX We thank the referee for extremely valuable remarks and suggestions. The research leading to these results received funding from the European Research Council under the EU's Seventh Framework Programme (FP7/(2007-2013)/ERC Grant Agreement No. 291352) and from the ISRAEL SCIENCE FOUNDATION (grant No. 1423/11). All photometric data presented in this paper were obtained from the Mikulsky 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. NR 43 TC 57 Z9 57 U1 1 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 OCT PY 2013 VL 208 IS 2 AR UNSP 16 DI 10.1088/0067-0049/208/2/16 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 229OM UT WOS:000325276600003 ER PT J AU Meskhidze, N Petters, MD Tsigaridis, K Bates, T O'Dowd, C Reid, J Lewis, ER Gantt, B Anguelova, MD Bhave, PV Bird, J Callaghan, AH Ceburnis, D Chang, R Clarke, A de Leeuw, G Deane, G DeMott, PJ Elliot, S Facchini, MC Fairall, CW Hawkins, L Hu, YX Hudson, JG Johnson, MS Kaku, KC Keene, WC Kieber, DJ Long, MS Martensson, M Modini, RL Osburn, CL Prather, KA Pszenny, A Rinaldi, M Russell, LM Salter, M Sayer, AM Smirnov, A Suda, SR Toth, TD Worsnop, DR Wozniak, A Zorn, SR AF Meskhidze, Nicholas Petters, Markus D. Tsigaridis, Kostas Bates, Tim O'Dowd, Colin Reid, Jeff Lewis, Ernie R. Gantt, Brett Anguelova, Magdalena D. Bhave, Prakash V. Bird, James Callaghan, Adrian H. Ceburnis, Darius Chang, Rachel Clarke, Antony de Leeuw, Gerrit Deane, Grant DeMott, Paul J. Elliot, Scott Facchini, Maria Cristina Fairall, Chris W. Hawkins, Lelia Hu, Yongxiang Hudson, James G. Johnson, Matthew S. Kaku, Kathleen C. Keene, William C. Kieber, David J. Long, Michael S. Martensson, Monica Modini, Rob L. Osburn, Chris L. Prather, Kimberly A. Pszenny, Alex Rinaldi, Matteo Russell, Lynn M. Salter, Matthew Sayer, Andrew M. Smirnov, Alexander Suda, Sarah R. Toth, Travis D. Worsnop, Douglas R. Wozniak, Andrew Zorn, Soeren R. TI Production mechanisms, number concentration, size distribution, chemical composition, and optical properties of sea spray aerosols SO ATMOSPHERIC SCIENCE LETTERS LA English DT Article DE sea spray aerosol; source function; chemical composition; number concentration; optical properties C1 [Meskhidze, Nicholas; Petters, Markus D.; Gantt, Brett; Johnson, Matthew S.; Osburn, Chris L.; Suda, Sarah R.] N Carolina State Univ, Raleigh, NC 27695 USA. [Tsigaridis, Kostas] Columbia Univ, New York, NY USA. [Tsigaridis, Kostas] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Bates, Tim] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. [O'Dowd, Colin; Callaghan, Adrian H.; Ceburnis, Darius] Natl Univ Ireland, Galway, Ireland. [Reid, Jeff; Anguelova, Magdalena D.; Kaku, Kathleen C.] Naval Res Lab, Washington, DC USA. [Lewis, Ernie R.] Brookhaven Natl Lab, Upton, NY 11973 USA. [Bhave, Prakash V.] US EPA, Res Triangle Pk, NC USA. [Bird, James] Boston Univ, Boston, MA 02215 USA. [Callaghan, Adrian H.; Modini, Rob L.] Scripps Inst Oceanog, San Diego, CA USA. [Chang, Rachel; Long, Michael S.] Harvard Univ, Cambridge, MA 02138 USA. [Clarke, Antony] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [de Leeuw, Gerrit] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. [de Leeuw, Gerrit] Univ Helsinki, Deptartment Phys, Helsinki, Finland. [Deane, Grant; Prather, Kimberly A.; Russell, Lynn M.] Univ Calif San Diego, San Diego, CA 92103 USA. [DeMott, Paul J.] Colorado State Univ, Ft Collins, CO 80523 USA. [Elliot, Scott] Los Alamos Natl Lab, Los Alamos, NM USA. [Facchini, Maria Cristina; Rinaldi, Matteo] CNR, Inst Atmospher Sci & Climate, Bologna, Italy. [Fairall, Chris W.] NOAA, Earth Syst Res Lab, Boulder, CO USA. [Hawkins, Lelia] Harvey Mudd Coll, Claremont, CA 91711 USA. [Hu, Yongxiang] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Hudson, James G.] Univ Nevada, Desert Res Inst, Reno, NV 89506 USA. [Johnson, Matthew S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Keene, William C.] Univ Virginia, Charlottesville, VA USA. [Kieber, David J.] SUNY, New York, NY USA. [Martensson, Monica] Uppsala Univ, Uppsala, Sweden. [Pszenny, Alex] Univ New Hampshire, Durham, NH 03824 USA. [Salter, Matthew] Stockholm Univ, S-10691 Stockholm, Sweden. [Sayer, Andrew M.; Smirnov, Alexander] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sayer, Andrew M.] Univ Space Res Assoc, Columbia, MD USA. [Toth, Travis D.] Univ N Dakota, Grand Forks, ND 58201 USA. [Worsnop, Douglas R.] Aerodyne Res Inc, Billerica, MA USA. [Wozniak, Andrew] Old Dominion Univ, Norfolk, VA USA. RP Meskhidze, N (reprint author), N Carolina State Univ, Raleigh, NC 27695 USA. EM nmeskhidze@ncsu.edu RI Sayer, Andrew/H-2314-2012; Worsnop, Douglas/D-2817-2009; Modini, Rob/A-8451-2014; DeMott, Paul/C-4389-2011; Facchini, Maria Cristina/B-3369-2014; Reid, Jeffrey/B-7633-2014; Petters, Markus/D-2144-2009; O'Dowd , Colin/K-8904-2012; Hu, Yongxiang/K-4426-2012; Petters, Sarah/N-8450-2014; rinaldi, matteo/K-6083-2012; CHEMATMO Group, Isac/P-7180-2014; Gantt, Brett/G-2525-2013; FACCHINI, MARIA CRISTINA/O-1230-2015; Bates, Timothy/L-6080-2016; Prather, Kimberly/A-3892-2008; Smirnov, Alexander/C-2121-2009; OI Sayer, Andrew/0000-0001-9149-1789; Worsnop, Douglas/0000-0002-8928-8017; DeMott, Paul/0000-0002-3719-1889; Facchini, Maria Cristina/0000-0003-4833-9305; Reid, Jeffrey/0000-0002-5147-7955; Petters, Markus/0000-0002-4082-1693; O'Dowd , Colin/0000-0002-3068-2212; Petters, Sarah/0000-0002-4501-7127; rinaldi, matteo/0000-0001-6543-4000; Gantt, Brett/0000-0001-7217-2715; FACCHINI, MARIA CRISTINA/0000-0003-4833-9305; Prather, Kimberly/0000-0003-3048-9890; Smirnov, Alexander/0000-0002-8208-1304; Salter, Matthew/0000-0003-0645-3265; Ceburnis, Darius/0000-0003-0231-5324 FU National Science Foundation - NSF [AGS-1236957]; Department of Energy office of Biological and Environmental Research [DOE-DE-SC0007995]; National Oceanic and Atmospheric Administration - NOAA [Z763701]; National Aeronautics and Space Administration - NASA [NNX12AK27G]; Marine Meteorology and Atmospheric Effects Program at the Department of Defense Office of Naval Research (DOD-ONR); NSF [CHE-1038028]; Irish Research Council; Marie Curie actions under FP7; National Science Foundation Physical Oceanography Division [OCE-1155123] FX Funding for this workshop was provided by the National Science Foundation - NSF (AGS-1236957), the Department of Energy office of Biological and Environmental Research (DOE-DE-SC0007995), the National Oceanic and Atmospheric Administration - NOAA (Z763701), the National Aeronautics and Space Administration - NASA (NNX12AK27G), and the Marine Meteorology and Atmospheric Effects Program at the Department of Defense Office of Naval Research (DOD-ONR). D. Ceburnis acknowledges EPA Ireland fellowship grant for travel support. K. Prather and G. Deane were supported by NSF (CHE-1038028) grant. A. H. Callaghan would like to acknowledge financial support from the Irish Research Council and Marie Curie actions under FP7 and the National Science Foundation Physical Oceanography Division (Grant OCE-1155123). NR 5 TC 11 Z9 11 U1 4 U2 106 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1530-261X J9 ATMOS SCI LETT JI Atmos. Sci. Lett. PD OCT PY 2013 VL 14 IS 4 BP 207 EP 213 DI 10.1002/asl2.441 PG 7 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 239NV UT WOS:000326033400002 ER PT J AU Nelson, SM Fielding, EJ Zamora-Arroyo, F Flessa, K AF Nelson, Steven M. Fielding, Eric J. Zamora-Arroyo, Francisco Flessa, Karl TI Delta dynamics: Effects of a major earthquake, tides, and river flows on Cienega de Santa Clara and the Colorado River Delta, Mexico SO ECOLOGICAL ENGINEERING LA English DT Article DE Colorado River Delta; Channel change; Tidal inundation; Earthquake surface deformation ID GULF-OF-CALIFORNIA; NORTHERN BAJA-CALIFORNIA; MAYOR-CUCAPAH EARTHQUAKE; SOURCE MECHANISM; SALTON TROUGH; SONORA; FAULT AB The intertidal portion of Mexico's Colorado River Delta is a dynamic environment subject to complex interactions of tectonic, fluvial, and tidal forces at the head of the Gulf of California. We review the historical interactions of these forces, use sequential satellite images, overflights, ground observations, and interferometric synthetic aperture radar (InSAR) data to study the effects of the 2010 Mw 7.2 El Mayor-Cucapah Earthquake on changing patterns of tidal inundation within the Delta, and assess effects of these changes to the fluvial/hydrological regime of the Colorado River estuary and nearby Cienega de Santa Clara wetland. The objectives of this study are to highlight for environmental scientists, land managers, and ecological engineers the contribution of tectonic forces in shaping the intertidal Delta environment and to provide information on the effects of the 2010 earthquake which will be of practical value in planning and designing management measures and restoration projects for the estuary and Cienega. The Colorado River estuary is at present blocked by a tidal sand bar which restricts access by marine species to the upper estuary and obstructs the flow of fresh water into the lower estuary. Located 13 km east of the estuary, the Cienega is a 6000 ha wetland supported by agricultural drain water from Arizona and Mexico. South of the Cienega is the Santa Clara Slough, an unvegetated 26,000 ha basin subject to periodic inundation from the northern Gulf's high amplitude tides, which have historically reached the margins of the Cienega several times each year. The El Mayor-Cucapah earthquake ruptured the previously unknown Indiviso Fault which extends into the intertidal zone just west of the Cienega. The Cienega experienced only minor surface deformation having no direct effects to the wetland. Most of the significant ground movement and surface deformation occurred west of the Indiviso Fault adjacent to the estuary, where portions of the intertidal flats underwent extensive liquefaction, northward coseismic displacement and post-seismic subsidence. These surface deformations changed the pattern of tidal inundation, triggering development of a new system of natural tidal channels and creating conditions favorable for installation of projects to restore connectivity between the upper and lower estuary. The changed pattern of tidal inundation may also have contributed to an observed reduction in the occurrence of tidal flooding along the southwestern margin of the Cienega following the earthquake. (C) 2012 Elsevier B.V. All rights reserved. C1 [Fielding, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zamora-Arroyo, Francisco] Sonoran Inst, Tucson, AZ 85701 USA. [Flessa, Karl] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. RP Nelson, SM (reprint author), 6101 NE 102nd Ave Apt 5, Vancouver, WA 98662 USA. EM snelson@worldaccessnet.com RI Fielding, Eric/A-1288-2007 OI Fielding, Eric/0000-0002-6648-8067 FU NSF-Supported Research Coordination Network, Colorado River Delta; NASA Earth Surface and Interior focus area and performed at the Jet Propulsion Laboratory; California Institute of Technology, Pasadena, California FX The first, third and fourth authors thank the NSF-Supported Research Coordination Network, Colorado River Delta for their support. The first author thanks the Sonoran Institute for its support of field visits and overflights, Arnold Schoeck for assistance with field trip logistics, and Leigh Fall for assistance in preparing Aerial photographs and monitoring efforts were made possible by the contribution of flights by Lighthawk. ALOS PALSAR original data is copyright JAXA, METI and was provided through the US Government Research Consortium at the Alaska Satellite Facility. Envisat original data is copyright European Space Agency and provided through the WInSAR consortium. Part of this research was supported by the NASA Earth Surface and Interior focus area and performed at the Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California. NR 57 TC 12 Z9 12 U1 0 U2 16 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0925-8574 EI 1872-6992 J9 ECOL ENG JI Ecol. Eng. PD OCT PY 2013 VL 59 BP 144 EP 156 DI 10.1016/j.ecoleng.2012.09.004 PG 13 WC Ecology; Engineering, Environmental; Environmental Sciences SC Environmental Sciences & Ecology; Engineering GA 235VY UT WOS:000325750400015 ER PT J AU Hartley, TT Lorenzo, CF Trigeassou, JC Maamri, N AF Hartley, Tom T. Lorenzo, Carl F. Trigeassou, Jean-Claude Maamri, Nezha TI Equivalence of History-Function Based and Infinite-Dimensional-State Initializations for Fractional-Order Operators SO JOURNAL OF COMPUTATIONAL AND NONLINEAR DYNAMICS LA English DT Article DE fractional-order system; initialization; fractional integrator; infinite-dimensional state variable; fractional-order differential equation ID DIFFERENTIAL-EQUATIONS; INITIAL CONDITIONS; SYSTEMS; TRANSIENTS AB Proper initialization of fractional-order operators has been an ongoing problem, particularly in the application of Laplace transforms with correct initialization terms. In the last few years, a history-function-based initialization along with its corresponding Laplace transform has been presented. Alternatively, an infinite-dimensional state-space representation along with its corresponding Laplace transform has also been presented. The purpose of this paper is to demonstrate that these two approaches to the initialization problem for fractional-order operators are equivalent and that the associated Laplace transforms yield the correct initialization terms and can be used in the solution of fractional-order differential equations. C1 [Hartley, Tom T.] Univ Akron, Akron, OH 44325 USA. [Lorenzo, Carl F.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Trigeassou, Jean-Claude] Univ Bordeaux 1, F-33405 Talence, France. [Maamri, Nezha] LIAS ENSIP Univ Poitiers, F-86000 Poitiers, France. RP Hartley, TT (reprint author), Univ Akron, Akron, OH 44325 USA. EM thartley@uakron.edu; Carl.F.Lorenzo@nasa.gov; jean-claude.trigeassou@ims-bordeaux.fr; nezha.maamri@univ-poitiers.fr FU NASA Glenn Research Center FX The authors gratefully acknowledge the support of NASA Glenn Research Center. NR 55 TC 10 Z9 11 U1 0 U2 5 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 1555-1423 EI 1555-1415 J9 J COMPUT NONLIN DYN JI J. Comput. Nonlinear Dyn. PD OCT PY 2013 VL 8 IS 4 AR 041014 DI 10.1115/1.4023865 PG 7 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 239NK UT WOS:000326032300014 ER PT J AU Fang, M Hager, BH Kuang, WJ AF Fang, Ming Hager, Bradford H. Kuang, Weijia TI Degree One Loading by Pressure Variations at the CMB SO JOURNAL OF EARTH SCIENCE LA English DT Article ID EARTHS INNER-CORE; SECULAR VARIATION; GRAVITY-FIELD; FLUID CORE; SURFACE; DEFORMATION; OSCILLATIONS; MANTLE; OBLATENESS; SYSTEM AB Hemispherical asymmetry in core dynamics induces degree-1 pressure variations at the core mantle boundary (CMB), which in turn deforms the overlaying elastic mantle, at the same time keeps center of mass of the whole Earth stationary in space. We develop a systematic procedure to deal with the degree-1 CMB pressure loading. We find by direct calculation a surprisingly negative load Love number h(1)=-1.425 for vertical displacement. Further analysis indicates that the negative h(1)corresponds to thickening above the positive load that defies intuition that pressure inflation pushes overlaying material up and thins the enveloping shell. We also redefine the pressure load Love numbers in general to enable comparison between the surface mass load and the CM:13 pressure load for the whole spectrum of harmonic degrees. We find that the gravitational perturbations from the two kinds of loads at degrees n>1 are very similar in amplitude but opposite in sign. In particular, if the CMB pressure variation at degree 2 is at the level of similar to 1 hpa/yr (1 cm water height per year), it would perturb the variation of Earth's oblateness, known as the J(2), at the observed level. C1 [Fang, Ming; Hager, Bradford H.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Kuang, Weijia] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD USA. RP Fang, M (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. EM fang@chandler.mit.edu RI Kuang, Weijia/K-5141-2012 OI Kuang, Weijia/0000-0001-7786-6425 FU NASA [NNX09AK 70G] FX This study was supported in part by NASA (No. NNX09AK 70G). NR 37 TC 0 Z9 0 U1 1 U2 7 PU CHINA UNIV GEOSCIENCES PI WUHAN PA YUJIASHAN, WUHAN, PEOPLES R CHINA SN 1674-487X EI 1867-111X J9 J EARTH SCI-CHINA JI J. Earth Sci. PD OCT PY 2013 VL 24 IS 5 BP 736 EP 749 DI 10.1007/s12583-013-0367-5 PG 14 WC Geosciences, Multidisciplinary SC Geology GA 231VF UT WOS:000325445800008 ER PT J AU Rashki, A Kaskaoutis, DG Goudie, AS Kahn, RA AF Rashki, A. Kaskaoutis, D. G. Goudie, A. S. Kahn, R. A. TI Dryness of ephemeral lakes and consequences for dust activity: The case of the Hamoun drainage basin, southeastern Iran SO SCIENCE OF THE TOTAL ENVIRONMENT LA English DT Article DE Dry-bed lakes; Satellite imagery; Precipitation; Dust activity; Sistan; Iran ID AEROSOL PROPERTIES; SISTAN REGION; INDIAN-OCEAN; MIDDLE-EAST; STORMS; MODIS; LAND; VARIABILITY; INUNDATION; EMISSIONS AB This study examines the influence of changes in the water coverage in the Hamoun dry-bed lakes on visibility, dust outbreaks, aerosol loading and land-atmospheric fluxes over the region covering the period 1985-2005. The Hamoun basin, located on the southeastern Iran and western Afghanistan borders, has been recognized as one of the major dust source regions in south Asia and is covered by shallow, marshy lakes that are fed by the Helmand and Farahrood rivers. When the water in watersheds that support the lakes is drawn down for natural or human-induced reasons, the end result is a decrease in the water coverage in the basin, or even complete dryness as occurred in 2001. Then, strong seasonal winds, mainly in summer, blow fine sand and silt off the exposed lakebed, enhancing dust activity and aerosol loading over the region. Satellite (Landsat) and meteorological observations reveal that the water levels in the Hamoun lakes exhibit considerable inter-annual variability during the period 1985-2005 strongly related to anomalies in precipitation. This is the trigger for concurrent changes in the frequency of the dusty days, aerosol loading and deterioration of visibility over the region, as satellite (TOMS, MODIS, MISR) observations reveal. On the other hand, soil moisture and latent heat, obtained via model (GLDAS_noah-10) simulations are directly linked with water levels and precipitation over the region. The desiccation of the Hamoun lakes in certain years and the consequent increase in frequency and intensity of dust storms are serious concerns for the regional climate, ecosystems and human health. (C) 2013 Elsevier B.V. All rights reserved. C1 [Rashki, A.] Ferdowsi Univ Mashhad, Nat Resources & Environm Coll, Mashhad, Iran. [Kaskaoutis, D. G.] Shiv Nadar Univ, Sch Nat Sci, Dept Phys, Dadri 203207, India. [Goudie, A. S.] Univ Oxford, China Ctr, Oxford OX2 6HP, England. [Kahn, R. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kaskaoutis, DG (reprint author), Shiv Nadar Univ, Sch Nat Sci, Dept Phys, Dadri 203207, India. EM dimitriskask@hotmail.com RI Kahn, Ralph/D-5371-2012; OI Kahn, Ralph/0000-0002-5234-6359; Goudie, Andrew/0000-0002-5496-8207; Rashki, Alireza/0000-0003-0213-7097 FU NASA; EOS-MISR project FX The authors are grateful to the technical staff of the Zabol meteorological station for operating and maintaining the meteorological instruments. We greatly appreciate the UNDP (United Nations Development Program) report for the Hamoun drainage Basin. The NASA Giovanni visualization tool is acknowledged for providing data from MODIS, MISR and TOMS sensors as well as from GLDAS-noah-10 model. 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 79 TC 20 Z9 20 U1 2 U2 22 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0048-9697 EI 1879-1026 J9 SCI TOTAL ENVIRON JI Sci. Total Environ. PD OCT 1 PY 2013 VL 463 BP 552 EP 564 DI 10.1016/j.scitotenv.2013.06.045 PG 13 WC Environmental Sciences SC Environmental Sciences & Ecology GA 236WW UT WOS:000325831200063 PM 23831801 ER PT J AU Kiger, CJ Johnson, SW Hashemian, HM Hudson, EK AF Kiger, Chad J. Johnson, Steve W. Hashemian, H. M. Hudson, Edward K. TI Harnessing Wireless Data from the Containment of a Nuclear Power Plant SO IEEE INSTRUMENTATION & MEASUREMENT MAGAZINE LA English DT Article C1 [Kiger, Chad J.] AMS, Knoxville, TN 37923 USA. [Kiger, Chad J.; Johnson, Steve W.] US DOE, Washington, DC 20585 USA. [Johnson, Steve W.] Oak Ridge Natl Lab, Oak Ridge, TN 37831 USA. [Hashemian, H. M.] AMS Corp, Knoxville, TN 37923 USA. [Hudson, Edward K.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Kiger, CJ (reprint author), AMS, Knoxville, TN 37923 USA. FU Department of Energy [DE-NE0000378] FX The material herein is based upon work supported by the Department of Energy under Award Number DE-NE0000378. NR 7 TC 1 Z9 1 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1094-6969 EI 1941-0123 J9 IEEE INSTRU MEAS MAG JI IEEE Instrum. Meas. Mag. PD OCT PY 2013 VL 16 IS 5 BP 18 EP 23 PG 6 WC Engineering, Electrical & Electronic; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 234QP UT WOS:000325659300004 ER PT J AU Zhang, QY Middleton, EM Cheng, YB Landis, DR AF Zhang, Qingyuan Middleton, Elizabeth M. Cheng, Yen-Ben Landis, David R. TI Variations of Foliage Chlorophyll fAPAR and Foliage Non-Chlorophyll fAPAR (fAPAR(chl), fAPAR(non-chl)) at the Harvard Forest SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE fAPAR(chl); fAPAR(non-chl); fAPAR(canopy); terrestrial carbon cycle; vegetation photosynthesis ID LIGHT-USE EFFICIENCY; LEAF-AREA INDEX; PHOTOSYNTHETICALLY ACTIVE RADIATION; SURFACE PARAMETERIZATION SIB2; DECIDUOUS BROADLEAF FOREST; GROSS PRIMARY PRODUCTION; IN-SITU MEASUREMENTS; MODIS DATA; ECOSYSTEM PRODUCTION; CANOPY REFLECTANCE AB In the last three decades, substantial advancements have been made in understanding the global carbon cycle. Some of these advancements involve using the fraction of absorbed photosynthetically active radiation (fAPAR) by an entire canopy (fAPAR(canopy)) and/or the Normalized Difference Vegetation Index (NDVI) in modeling studies. In spite of these advancements, large uncertainties still remain. Zhang et al. (Remote Sens. Environ., 2005) [1] tried to mitigate some of these uncertainties with the concept of using fAPAR that is restricted to the foliage chlorophyll (fAPAR(chl)) instead of the entire canopy. In this current study, we calculated fAPAR(canopy), fAPAR(chl), and foliage non-chlorophyll fAPAR (fAPAR(non-chl)) for the Harvard Forest using a radiative transfer model and multi-temporal Earth Observing One (EO-1) Hyperion satellite images. The canopy-level proportions of foliar chlorophyll and non-chlorophyll absorption were determined at different seasons (spring, summer, autumn) in an effort to demonstrate temporal variations of three plant functional types: deciduous forest, coniferous forest, and grass. Comparisons were made for NDVI versus fAPAR and for the Enhanced Vegetation Index (EVI) versus fAPAR(chl). In addition, EO-1 Hyperion images were utilized to simulate these new fAPAR(canopy), fAPAR(chl), and fAPAR(non-chl) products at 60 m as prototypes for the proposed NASA HyspIRI satellite spectrometer. These products should prove useful for future terrestrial carbon cycle and ecosystem studies. C1 [Zhang, Qingyuan] Univ Space Res Assoc, Columbia, MD 21044 USA. [Zhang, Qingyuan; Middleton, Elizabeth M.; Cheng, Yen-Ben; Landis, David R.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Cheng, Yen-Ben] Earth Resources Technol, Laurel, MD 20707 USA. [Landis, David R.] Sigma Space Corp, Lanham, MD 20706 USA. RP Zhang, QY (reprint author), Univ Space Res Assoc, Columbia, MD 21044 USA. EM qyz72@yahoo.com FU NASA Headquarters FX This study was supported by two NASA Headquarters sponsored programs, the Earth Observing One (EO-1) Mission Science Office (Sponsor, Dr. Garik Gutman) and the HyspIRI science support project at the Goddard Space Flight Center (NASA/GSFC), through Mr. Woody Turner. Thanks to the JSTARS Associate Editor and the anonymous reviewers for their extremely helpful and constructive comments on the manuscript. Thanks also to Dr. J. William Munger, a Senior Research Fellow and the manager of the Harvard Forest tower. NR 63 TC 16 Z9 16 U1 1 U2 16 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD OCT PY 2013 VL 6 IS 5 SI SI BP 2254 EP 2264 DI 10.1109/JSTARS.2013.2275176 PG 11 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 235XW UT WOS:000325757300016 ER PT J AU Bryllert, T Drakinskiy, V Cooper, KB Stake, J AF Bryllert, Tomas Drakinskiy, Vladimir Cooper, Ken B. Stake, Jan TI Integrated 200-240-GHz FMCW Radar Transceiver Module SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES LA English DT Article DE Frequency modulated continuous wave (FMCW); imaging radar; millimeter wave; radar; Schottky diode; semiconductor membrane; transceiver ID POWER; GHZ; RECEIVER; BAND AB We present a 220-GHz homodyne transceiver module intended for frequency modulated continuous wave radar applications. The RF transceiver circuits are fabricated on 3-mu m-thick GaAs membranes, and consist of a Schottky diode based transmitter frequency doubler that simultaneously operates as a sub-harmonic down-converting mixer. Two circuits are used in a balanced configuration to improve the noise performance. The output power is > 3 dBm over a 40-GHz bandwidth (BW) centered at 220 GHz, and the receiver function is characterized by a typical mixer conversion loss of 16 dB. We present radar images at 4-m target distance with up to 60-dB dynamic range using a 30-mu s chirp time, and near-BW-limited range resolution. The module is intended for applications in high-resolution real-time 3-D radar imaging, and the unit is therefore designed so that it can be assembled into 1-D or 2-D arrays. C1 [Bryllert, Tomas; Drakinskiy, Vladimir; Stake, Jan] Chalmers, Terahertz & Millimetre Wave Lab, Dept Microtechnol & Nanosci, SE-41296 Gothenburg, Sweden. [Cooper, Ken B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bryllert, T (reprint author), Chalmers, Terahertz & Millimetre Wave Lab, Dept Microtechnol & Nanosci, SE-41296 Gothenburg, Sweden. EM bryllert@chalmers.se RI Stake, Jan/C-4383-2008 OI Stake, Jan/0000-0002-8204-7894 FU Swedish Civil Contingencies Agency, MSB; U.S. Department of Homeland Security, Science and Technology Directorate; Security Link; Swedish Government; National Aeronautics and Space Administration (NASA) FX This work was supported by the Swedish Civil Contingencies Agency, MSB, by the U.S. Department of Homeland Security, Science and Technology Directorate, and by Security Link, a Strategic Research Area for security and crisis management, funded by the Swedish Government. A portion of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). NR 16 TC 21 Z9 21 U1 1 U2 10 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9480 EI 1557-9670 J9 IEEE T MICROW THEORY JI IEEE Trans. Microw. Theory Tech. PD OCT PY 2013 VL 61 IS 10 BP 3808 EP 3815 DI 10.1109/TMTT.2013.2279359 PG 8 WC Engineering, Electrical & Electronic SC Engineering GA 236AC UT WOS:000325764600033 ER PT J AU Lam, CW Scully, RR Zhang, Y Renne, RA Hunter, RL McCluskey, RA Chen, BT Castranova, V Driscoll, KE Gardner, DE McClellan, RO Cooper, BL McKay, DS Marshall, L James, JT AF Lam, Chiu-wing Scully, Robert R. Zhang, Ye Renne, Roger A. Hunter, Robert L. McCluskey, Richard A. Chen, Bean T. Castranova, Vincent Driscoll, Kevin E. Gardner, Donald E. McClellan, Roger O. Cooper, Bonnie L. McKay, David S. Marshall, Linda James, John T. TI Toxicity of lunar dust assessed in inhalation-exposed rats SO INHALATION TOXICOLOGY LA English DT Article DE Lunar dust toxicity; lung lavage biomarkers; moon dust; nose-only exposure ID INTRATRACHEAL INSTILLATION; PULMONARY TOXICITY; SIMULATED LUNAR; MARTIAN DUSTS; CLEARANCE; PARTICLES; RETENTION; RESPONSES; TONER; RISK AB Humans will again set foot on the moon. The moon is covered by a layer of fine dust, which can pose a respiratory hazard. We investigated the pulmonary toxicity of lunar dust in rats exposed to 0, 2.1, 6.8, 20.8 and 60.6 mg/m(3) of respirable-size lunar dust for 4 weeks (6 h/day, 5 days/week); the aerosols in the nose-only exposure chambers were generated from a jet-mill ground preparation of a lunar soil collected during the Apollo 14 mission. After 4 weeks of exposure to air or lunar dust, groups of five rats were euthanized 1 day, 1 week, 4 weeks or 13 weeks after the last exposure for assessment of pulmonary toxicity. Biomarkers of toxicity assessed in bronchoalveolar fluids showed concentration-dependent changes; biomarkers that showed treatment effects were total cell and neutrophil counts, total protein concentrations and cellular enzymes (lactate dehydrogenase, glutamyl transferase and aspartate transaminase). No statistically significant differences in these biomarkers were detected between rats exposed to air and those exposed to the two low concentrations of lunar dust. Dose-dependent histopathology, including inflammation, septal thickening, fibrosis and granulomas, in the lung was observed at the two higher exposure concentrations. No lesions were detected in rats exposed to <= 6.8 mg/m(3). This 4-week exposure study in rats showed that 6.8 mg/m(3) was the highest no-observable-adverse-effect level (NOAEL). These results will be useful for assessing the health risk to humans of exposure to lunar dust, establishing human exposure limits and guiding the design of dust mitigation systems in lunar landers or habitats. C1 [Lam, Chiu-wing; Scully, Robert R.; James, John T.] NASA, Space Toxicol Off, Johnson Space Ctr, Houston, TX 77058 USA. [Lam, Chiu-wing; Scully, Robert R.; Zhang, Ye; Marshall, Linda] Wyle Sci Technol & Engn Grp, Houston, TX USA. [Lam, Chiu-wing; Hunter, Robert L.] Univ Texas Med Sch, Dept Pathol & Lab Med, Houston, TX USA. [Zhang, Ye] NASA, Bioanalyt Core Labs, Johnson Space Ctr, Houston, TX 77058 USA. [Renne, Roger A.] Roger Renne ToxPath Consulting Inc, Sumner, WA USA. [McCluskey, Richard A.] Naval Hosp Pensacola, Pensacola, FL USA. [Chen, Bean T.; Castranova, Vincent] NIOSH, Hlth Effects Lab Div, Morgantown, WV USA. [Driscoll, Kevin E.] PGT Healthcare, Geneva, Switzerland. [Gardner, Donald E.] Inhalat Toxicol Associates, Savannah, GA USA. [McClellan, Roger O.] Toxicol & Human Hlth Risk Anal, Albuquerque, NM USA. [Cooper, Bonnie L.; McKay, David S.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Cooper, Bonnie L.] Oceaneering Space Syst, Houston, TX USA. [Marshall, Linda] NASA, Clin Lab, Johnson Space Ctr, Houston, TX 77058 USA. RP Lam, CW (reprint author), NASA, Toxicol Lab, Biomed Res & Environm Sci Div, Wyle STE,Johnson Space Ctr SK Wyle 4, 2101 NASA Pkwy, Houston, TX 77058 USA. EM chiu-wing.lam-1@nasa.gov FU NASA Human Research Program FX This project was funded by the NASA Human Research Program. We gratefully acknowledge the Apollo Sample Curator for providing an Apollo 14 lunar regolith sample for this study. We thank the members of NASA-assembled Lunar Airborne Toxicity Assessment Group (LADTAG) and Non-Advocate Review Committee, for their advice on the lunar dust toxicity project, and L. Taylor and D. McKay for technical advice on mineralogy of lunar dust. Technical assistance from S. Bassett, S. Zalesak, S. Beck, C. Gonzalez, C. Garza, D. Martin, R. Miller, staffs of NASA JSC Clinical Laboratory and Histology Laboratory of the University Texas Medical Center (Houston) is also gratefully acknowledged. We also thank J. Krauhs and H. Garcia for editorial assistance. NR 40 TC 6 Z9 6 U1 2 U2 21 PU INFORMA HEALTHCARE PI LONDON PA TELEPHONE HOUSE, 69-77 PAUL STREET, LONDON EC2A 4LQ, ENGLAND SN 0895-8378 EI 1091-7691 J9 INHAL TOXICOL JI Inhal. Toxicol. PD OCT PY 2013 VL 25 IS 12 BP 661 EP 678 DI 10.3109/08958378.2013.833660 PG 18 WC Toxicology SC Toxicology GA 232WS UT WOS:000325525700002 PM 24102467 ER PT J AU Verma, S Kozon, T Ballinger, D Farrahi, A AF Verma, Savvy Kozon, Thomas Ballinger, Debbi Farrahi, Amir TI Functional Allocation of Roles Between Humans and Automation for a Pairing Tool Used for Simultaneous Approaches SO INTERNATIONAL JOURNAL OF AVIATION PSYCHOLOGY LA English DT Article AB Aircraft operations on parallel runways continue to motivate research into tools that can improve capacity safely by defining and automating procedures. However, there is no formal process or automation tool today to assist the air traffic controller with pairing aircraft for simultaneous approaches. To address this need, a controller-based aircraft pairing tool to assist controllers in pairing and aligning aircraft for simultaneous arrivals to parallel runways 750 ft apart was developed. Two simulation studies conducted at the National Aeronautics and Space Administration (NASA) Ames Research Center evaluated different stages of evolution of this tool. The respective roles of the controller and the automation tool were adjusted in the second experiment based on the results of the first experiment. Results indicate improvement on all dependent variables in the second study and suggest an implementation in a broader sense in light of the benefits provided by adaptable automation (Scerbo, 2001) where changes in the levels of automation are evoked by the user's actions. C1 [Verma, Savvy; Kozon, Thomas; Ballinger, Debbi; Farrahi, Amir] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Verma, S (reprint author), NASA, Ames Res Ctr, Aviat Syst Div, Mail Stop 210-9,POB 1, Moffett Field, CA 94035 USA. EM savita.a.verma@nasa.gov NR 19 TC 1 Z9 1 U1 1 U2 2 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1050-8414 EI 1532-7108 J9 INT J AVIAT PSYCHOL JI Int. J. Aviat. Psychol. PD OCT 1 PY 2013 VL 23 IS 4 BP 335 EP 367 DI 10.1080/10508414.2013.833764 PG 33 WC Psychology, Applied SC Psychology GA 234XN UT WOS:000325677700004 ER PT J AU Allan, SM Merritt, BJ Griffin, BF Hintze, PE Shulman, HS AF Allan, Shawn M. Merritt, Brandon J. Griffin, Brittany F. Hintze, Paul E. Shulman, Holly S. TI High-Temperature Microwave Dielectric Properties and Processing of JSC-1AC Lunar Simulant SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article DE Aerospace engineering; Moon; Microwaves; Synthetic materials; Temperature effects; Aerospace engineering; Moon; Microwaves; Synthetic materials ID SOIL AB Successful development of extraterrestrial microwave heating technologies depends on the study of the dielectric properties that control the microwave heating behavior of simulants and regoliths. Microwave heating may serve many lunar applications including heating the regolith for lunar surface dust stabilization, oxygen production, building materials, and mineral refinement. The dielectric properties (dielectric constant, epsilon, and loss factor, epsilon) of the lunar simulant, JSC-1AC, were measured at 2.45 GHz microwave frequency from room temperature to 1,100 degrees C. The dielectric loss tangent and half-power depth were calculated from the measured properties. The loss tangent increased from a low value of 0.02 at room temperature to a high value of 0.31 at 1,100 degrees C, indicating increased efficiency of microwave absorption at higher temperatures. The low temperature loss tangent indicated that relatively slow, low efficiency heating would be expected at room temperature. The microwave heating experiments confirmed weak heating related to absorption below 250 degrees C, and increasingly strong absorption above 250 degrees C, leading to rapid heating and melting or the so-called thermal runaway of JSC-1AC. Heating with microwaves as the only energy source produced a thermal runaway with wide variations in the JSC-1AC, such as fully molten glass, with unsintered loose particulate located millimeters away. The addition of a supplemental radiant heat source to the microwave mitigated the thermal runaway effect and produced uniform solid materials from the JSC-1A lunar simulant. The room temperature dielectric properties of JSC-1AC were measured and found to be comparable with the range of published lunar regolith properties, making JSC-1AC a reasonable starting point for microwave heating and computational modeling studies. C1 [Allan, Shawn M.; Shulman, Holly S.] Ceralink Inc, Troy, NY 12180 USA. [Merritt, Brandon J.] Alfred Univ, Alfred, NY 14802 USA. [Griffin, Brittany F.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA. [Hintze, Paul E.] NASA, Corros Technol Lab, Kennedy Space Ctr, FL 32899 USA. RP Allan, SM (reprint author), Ceralink Inc, 105 Jordan Rd, Troy, NY 12180 USA. EM shawn@ceralink.com; bjm4@alfred.edu; paul.e.hintze@nasa.gov; paul.e.hintze@nasa.gov; holly@ceralink.com OI Hintze, Paul/0000-0002-9962-2955 FU NYSERDA, the New York State Research and Development Authority FX The authors acknowledge Dr. Ron Hutcheon, of Microwave Properties North, Deep River, ON, Canada, for the dielectric measurements performed in this study. This work was partially supported by NYSERDA, the New York State Research and Development Authority. NR 29 TC 1 Z9 1 U1 0 U2 13 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0893-1321 EI 1943-5525 J9 J AEROSPACE ENG JI J. Aerosp. Eng. PD OCT 1 PY 2013 VL 26 IS 4 BP 874 EP 881 DI 10.1061/(ASCE)AS.1943-5525.0000179 PG 8 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA 218YP UT WOS:000324469100021 ER PT J AU Coats, S Smerdon, JE Seager, R Cook, BI Gonzalez-Rouco, JF AF Coats, Sloan Smerdon, Jason E. Seager, Richard Cook, Benjamin I. Gonzalez-Rouco, J. F. TI Megadroughts in Southwestern North America in ECHO-G Millennial Simulations and Their Comparison to Proxy Drought Reconstructions SO JOURNAL OF CLIMATE LA English DT Article DE North America; ENSO; Climate variability; Paleoclimate; Model evaluation; performance; Multidecadal variability ID 1000-YR CONTROL SIMULATION; COUPLED CLIMATE MODEL; SURFACE-TEMPERATURE; TROPICAL PACIFIC; INTERNAL VARIABILITY; LAST MILLENNIUM; DUST-BOWL; OSCILLATION; CALIFORNIA; SSTS AB Simulated hydroclimate variability in millennium-length forced transient and control simulations from the ECHAM and the global Hamburg Ocean Primitive Equation (ECHO-G) coupled atmosphere-ocean general circulation model (AOGCM) is analyzed and compared to 1000 years of reconstructed Palmer drought severity index (PDSI) variability from the North American Drought Atlas (NADA). The ability of the model to simulate megadroughts in the North American southwest is evaluated. (NASW: 25 degrees-42.5 degrees N, 125 degrees-105 degrees W). Megadroughts in the ECHO-G AOGCM are found to be similar in duration and magnitude to those estimated from the NADA. The droughts in the forced simulation are not, however, temporally synchronous with those in the paleoclimate record, nor are there significant differences between the drought features simulated in the forced and control runs. These results indicate that model-simulated megadroughts can result from internal variability of the modeled climate system rather than as a response to changes in exogenous forcings. Although the ECHO-G AOGCM is capable of simulating megadroughts through persistent La Nina-like conditions in the tropical Pacific, other mechanisms can produce similarly extreme NASW moisture anomalies in the model. In particular, the lack of low-frequency coherence between NASW soil moisture and simulated modes of climate variability like the El Nino-Southern Oscillation, Pacific decadal oscillation, and Atlantic multidecadal oscillation during identified drought periods suggests that stochastic atmospheric variability can contribute significantly to the occurrence of simulated megadroughts in the NASW. These findings indicate that either an expanded paradigm is needed to understand multidecadal hydroclimate variability in the NASW or AOGCMs may incorrectly simulate the strength and/or dynamics of the connection between NASW hydroclimate variability and the tropical Pacific. C1 [Coats, Sloan; Smerdon, Jason E.; Seager, Richard; Cook, Benjamin I.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Coats, Sloan] Columbia Univ, Dept Earth & Environm Sci, New York, NY USA. [Cook, Benjamin I.] NASA Goddard Inst Space Studies, New York, NY USA. [Gonzalez-Rouco, J. F.] Univ Complutense, Fac Ciencias Fis, Inst Geociencias UCM CSIC, E-28040 Madrid, Spain. RP Coats, S (reprint author), Lamont Doherty Earth Observ, 61 Route 9W, Palisades, NY 10964 USA. EM sjc2164@columbia.edu RI Smerdon, Jason/F-9952-2011; Cook, Benjamin/H-2265-2012; Gonzalez-Rouco, Jesus Fidel/B-1761-2012 OI Gonzalez-Rouco, Jesus Fidel/0000-0001-7090-6797 FU NOAA Award Global Decadal Hydroclimate Variability and Change [NA10OAR431037]; NSF [ATM09-02716]; NOAA [NA08-OAR4320912]; NSF Award North American Megadroughts: Atmosphere-Ocean Forcing and Landscape Response from the Medieval Period to the Near-Term Greenhouse Future [ATM-0902716]; [MMAMRM-200800050084028//200800050083542]; [MCIN-CGL2008-06558-C02-01]; [UCM/921407] FX SC, JES, and RS are supported by the NOAA Award Global Decadal Hydroclimate Variability and Change (NA10OAR431037). RS was also supported by NSF Award ATM09-02716 and NOAA Award NA08-OAR4320912. BIC was supported by the NSF Award North American Megadroughts: Atmosphere-Ocean Forcing and Landscape Response from the Medieval Period to the Near-Term Greenhouse Future (ATM-0902716). JFGR was supported by MMAMRM-200800050084028//200800050083542, MCIN-CGL2008-06558-C02-01, and UCM/921407. Cross-wavelet and wavelet coherence software was provided by A. Grinsted. NR 51 TC 24 Z9 24 U1 6 U2 33 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 OCT PY 2013 VL 26 IS 19 BP 7635 EP 7649 DI 10.1175/JCLI-D-12-00603.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 222TH UT WOS:000324753900020 ER PT J AU Tselioudis, G Rossow, W Zhang, YC Konsta, D AF Tselioudis, George Rossow, William Zhang, Yuanchong Konsta, Dimitra TI Global Weather States and Their Properties from Passive and Active Satellite Cloud Retrievals SO JOURNAL OF CLIMATE LA English DT Article DE Climate classification; regimes; Cloud radiative effects; Cloud retrieval; Satellite observations ID TROPICAL WESTERN PACIFIC; VERTICAL STRUCTURE; DECADAL VARIABILITY; STATISTICAL-MODEL; REGIMES; ISCCP; IDENTIFICATION; CONVECTION; PROFILES; BUDGET AB In this study, the authors apply a clustering algorithm to International Satellite Cloud Climatology Project (ISCCP) cloud optical thickness-cloud top pressure histograms in order to derive weather states (WSs) for the global domain. The cloud property distribution within each WS is examined and the geographical variability of each WS is mapped. Once the global WSs are derived, a combination of CloudSat and Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) vertical cloud structure retrievals is used to derive the vertical distribution of the cloud field within each WS. Finally, the dynamic environment and the radiative signature of the WSs are derived and their variability is examined. The cluster analysis produces a comprehensive description of global atmospheric conditions through the derivation of 11 WSs, each representing a distinct cloud structure characterized by the horizontal distribution of cloud optical depth and cloud top pressure. Matching those distinct WSs with cloud vertical profiles derived from CloudSat and CALIPSO retrievals shows that the ISCCP WSs exhibit unique distributions of vertical layering that correspond well to the horizontal structure of cloud properties. Matching the derived WSs with vertical velocity measurements shows a normal progression in dynamic regime when moving from the most convective to the least convective WS. Time trend analysis of the WSs shows a sharp increase of the fair-weather WS in the 1990s and a flattening of that increase in the 2000s. The fact that the fair-weather WS is the one with the lowest cloud radiative cooling capability implies that this behavior has contributed excess radiative warming to the global radiative budget during the 1990s. C1 [Tselioudis, George; Zhang, Yuanchong] Columbia Univ, NASA, GISS, New York, NY 10025 USA. [Tselioudis, George; Zhang, Yuanchong] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA. [Tselioudis, George; Konsta, Dimitra] Acad Athens, Res Ctr Atmospher Phys & Climatol, Athens, Greece. [Rossow, William] CUNY City Coll, NOAA, CREST, New York, NY 10031 USA. RP Tselioudis, G (reprint author), Columbia Univ, NASA, GISS, 2880 Broadway, New York, NY 10025 USA. EM gt9@columbia.edu RI Rossow, William/F-3138-2015; Konsta, Dimitra/O-5205-2015 FU NASA MAP program; NASA MEaSUREs program; NOAA CDR program; EU FP7 EUCLIPSE program FX The authors of this work would like to acknowledge support by the NASA MAP and MEaSUREs programs, the NOAA CDR program, and the EU FP7 EUCLIPSE program. NR 31 TC 23 Z9 23 U1 0 U2 15 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 OCT PY 2013 VL 26 IS 19 BP 7734 EP 7746 DI 10.1175/JCLI-D-13-00024.1 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 222TH UT WOS:000324753900027 ER PT J AU Goodwin, T McCarthy, M Osterrieder, N Kaufer, B Gilden, D Cohrs, R AF Goodwin, Thomas McCarthy, Maureen Osterrieder, Nikolaus Kaufer, Benedikt Gilden, Don Cohrs, Randall TI P3D Normal Human Neural Progenitor Tissue-Like Assemblies: A Model of Persistent VZV Infection SO JOURNAL OF NEUROVIROLOGY LA English DT Meeting Abstract CT 12th International Symposium on NeuroVirology CY OCT 29-NOV 02, 2013 CL Washington, DC C1 [Goodwin, Thomas; McCarthy, Maureen] NASA, Lyndon B Johnson Space Ctr, Dis Modeling Tissue Analogues Lab, Houston, TX 77058 USA. [Osterrieder, Nikolaus; Kaufer, Benedikt] Free Univ Berlin, Inst Virol, Berlin, Germany. [Gilden, Don; Cohrs, Randall] Univ Colorado, Sch Med, Dept Neurol, Boulder, CO 80309 USA. [Gilden, Don; Cohrs, Randall] Univ Colorado, Sch Med, Dept Microbiol, Boulder, CO 80309 USA. EM randall.cohrs@ucdenver.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1355-0284 EI 1538-2443 J9 J NEUROVIROL JI J. Neurovirol. PD OCT PY 2013 VL 19 SU 1 MA P71 BP S34 EP S34 PG 1 WC Neurosciences; Virology SC Neurosciences & Neurology; Virology GA 236EM UT WOS:000325777200072 ER PT J AU West, KL Sanchez, S Rotstein, D Robertson, KM Dennison, S Levine, G Davis, N Schofield, D Potter, CW Jensen, B AF West, Kristi L. Sanchez, Susan Rotstein, David Robertson, Kelly M. Dennison, Sophie Levine, Gregg Davis, Nicole Schofield, David Potter, Charles W. Jensen, Brenda TI A Longman's beaked whale (Indopacetus pacificus) strands in Maui, Hawaii, with first case of morbillivirus in the central Pacific SO MARINE MAMMAL SCIENCE LA English DT Article ID STENELLA-COERULEOALBA; COMMON DOLPHINS; SITE FIDELITY; INFECTION; OCEAN; DNA; WATERS C1 [West, Kristi L.] Hawaii Pacific Univ, Coll Nat & Computat Sci, Kaneohe, HI 96744 USA. [Sanchez, Susan] Univ Georgia, Dept Infect Dis, Coll Vet Med, Athens, GA 30602 USA. [Robertson, Kelly M.] NOAA, Protected Resources Div, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, La Jolla, CA 92037 USA. [Dennison, Sophie] Marine Mammal Radiol, San Francisco, CA 94107 USA. [Davis, Nicole; Schofield, David] Natl Marine Fisheries Serv, Pacific Isl Reg Off, Honolulu, HI 96814 USA. [Potter, Charles W.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. [Jensen, Brenda] Hawaii Pacific Univ, Coll Nat & Computat Sci, Kaneohe, HI 96744 USA. RP West, KL (reprint author), Hawaii Pacific Univ, Coll Nat & Computat Sci, 45-045 Kamehameha Highway, Kaneohe, HI 96744 USA. EM kwest@hpu.edu FU Prescott Grant Program FX We would like to thank Dera Look and Hawaii Stranding Response Network volunteers for their heroic efforts to recover this fresh specimen from Hana. We thank Dr. J. T. Saliki for his leadership, support and advice. We are also grateful to the staff of the Molecular Biology section of the Athens Veterinary Diagnostic lab for their dedication and assistance provided in the identification of this novel virus. We also thank Robin Baird for providing a preliminary species identification of the specimen. We are grateful to Whitney White, Susan Fertall White, and Robert Brownell. W. F. Perrin and Kerri Danil provided helpful comments that improved the manuscript. This work was funded by the Prescott Grant Program. NR 29 TC 15 Z9 15 U1 2 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0824-0469 EI 1748-7692 J9 MAR MAMMAL SCI JI Mar. Mamm. Sci. PD OCT PY 2013 VL 29 IS 4 BP 767 EP 776 DI 10.1111/j.1748-7692.2012.00616.x PG 10 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 232HF UT WOS:000325482800026 ER PT J AU Kirschke, S Bousquet, P Ciais, P Saunois, M Canadell, JG Dlugokencky, EJ Bergamaschi, P Bergmann, D Blake, DR Bruhwiler, L Cameron-Smith, P Castaldi, S Chevallier, F Feng, L Fraser, A Heimann, M Hodson, EL Houweling, S Josse, B Fraser, PJ Krummel, PB Lamarque, JF Langenfelds, RL Le Quere, C Naik, V O'Doherty, S Palmer, PI Pison, I Plummer, D Poulter, B Prinn, RG Rigby, M Ringeval, B Santini, M Schmidt, M Shindell, DT Simpson, IJ Spahni, R Steele, LP Strode, SA Sudo, K Szopa, S van der Werf, GR Voulgarakis, A van Weele, M Weiss, RF Williams, JE Zeng, G AF Kirschke, Stefanie Bousquet, Philippe Ciais, Philippe Saunois, Marielle Canadell, Josep G. Dlugokencky, Edward J. Bergamaschi, Peter Bergmann, Daniel Blake, Donald R. Bruhwiler, Lori Cameron-Smith, Philip Castaldi, Simona Chevallier, Frederic Feng, Liang Fraser, Annemarie Heimann, Martin Hodson, Elke L. Houweling, Sander Josse, Beatrice Fraser, Paul J. Krummel, Paul B. Lamarque, Jean-Francois Langenfelds, Ray L. Le Quere, Corinne Naik, Vaishali O'Doherty, Simon Palmer, Paul I. Pison, Isabelle Plummer, David Poulter, Benjamin Prinn, Ronald G. Rigby, Matt Ringeval, Bruno Santini, Monia Schmidt, Martina Shindell, Drew T. Simpson, Isobel J. Spahni, Renato Steele, L. Paul Strode, Sarah A. Sudo, Kengo Szopa, Sophie van der Werf, Guido R. Voulgarakis, Apostolos van Weele, Michiel Weiss, Ray F. Williams, Jason E. Zeng, Guang TI Three decades of global methane sources and sinks SO NATURE GEOSCIENCE LA English DT Review ID INTERCOMPARISON PROJECT ACCMIP; PAST 2 DECADES; ATMOSPHERIC METHANE; GROWTH-RATE; BIOGEOCHEMISTRY MODEL; TROPOSPHERIC METHANE; ISOTOPIC COMPOSITION; METHYL CHLOROFORM; CARBON-DIOXIDE; EMISSIONS AB Methane is an important greenhouse gas, responsible for about 20% of the warming induced by long-lived greenhouse gases since pre-industrial times. By reacting with hydroxyl radicals, methane reduces the oxidizing capacity of the atmosphere and generates ozone in the troposphere. Although most sources and sinks of methane have been identified, their relative contributions to atmospheric methane levels are highly uncertain. As such, the factors responsible for the observed stabilization of atmospheric methane levels in the early 2000s, and the renewed rise after 2006, remain unclear. Here, we construct decadal budgets for methane sources and sinks between 1980 and 2010, using a combination of atmospheric measurements and results from chemical transport models, ecosystem models, climate chemistry models and inventories of anthropogenic emissions. The resultant budgets suggest that data-driven approaches and ecosystem models overestimate total natural emissions. We build three contrasting emission scenarios - which differ in fossil fuel and microbial emissions - to explain the decadal variability in atmospheric methane levels detected, here and in previous studies, since 1985. Although uncertainties in emission trends do not allow definitive conclusions to be drawn, we show that the observed stabilization of methane levels between 1999 and 2006 can potentially be explained by decreasing-to-stable fossil fuel emissions, combined with stable-to-increasing microbial emissions. We show that a rise in natural wetland emissions and fossil fuel emissions probably accounts for the renewed increase in global methane levels after 2006, although the relative contribution of these two sources remains uncertain. C1 [Kirschke, Stefanie; Bousquet, Philippe; Ciais, Philippe; Saunois, Marielle; Chevallier, Frederic; Pison, Isabelle; Poulter, Benjamin; Schmidt, Martina; Szopa, Sophie] LSCE CEA UVSQ CNRS, F-91190 Gif Sur Yvette, France. [Canadell, Josep G.] CSIRO Marine & Atmospher Res, Global Carbon Project, Canberra, ACT 2601, Australia. [Dlugokencky, Edward J.; Bruhwiler, Lori] NOAA ESRL, Boulder, CO 80305 USA. [Bergamaschi, Peter] Joint Res Ctr, Inst Environm & Sustainabil, I-21027 Ispra, Va, Italy. [Bergmann, Daniel; Cameron-Smith, Philip] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. [Blake, Donald R.; Simpson, Isobel J.] Univ Calif Irvine, Irvine, CA 92697 USA. [Castaldi, Simona] Univ Naples 2, Dept Environm Sci, I-81100 Caserta, Italy. [Castaldi, Simona; Santini, Monia] Ctr Euro Mediterraneo Cambiamenti Climatici CMCC, I-73100 Lecce, Italy. [Feng, Liang; Fraser, Annemarie; Palmer, Paul I.] Univ Edinburgh, Sch Geosci, Edinburgh EH9 3JN, Midlothian, Scotland. [Heimann, Martin] Max Planck Inst Biogeochem, D-07701 Jena, Germany. [Hodson, Elke L.] Swiss Fed Res Inst WSL, CH-8903 Birmensdorf, Switzerland. [Houweling, Sander] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Houweling, Sander; Ringeval, Bruno] Inst Marine & Atmospher Res Utrecht, NL-3584 CA Utrecht, Netherlands. [Josse, Beatrice] CNRM GMGEC CARMA, Meteo France, F-31057 Toulouse, France. [Fraser, Paul J.; Krummel, Paul B.; Langenfelds, Ray L.; Steele, L. Paul] CSIRO Marine & Atmospher Res, Ctr Australian Weather & Climate Res, Aspendale, Vic 3195, Australia. [Lamarque, Jean-Francois] NCAR, Boulder, CO 80307 USA. [Le Quere, Corinne] Univ E Anglia, Tyndall Ctr Climate Change Res, Norwich NR4 7TJ, Norfolk, England. [Naik, Vaishali] NOAA, UCAR, Geophys Fluid Dynam Lab, Princeton, NJ 08540 USA. [O'Doherty, Simon] Univ Bristol, Bristol BS8 1TS, Avon, England. [Plummer, David] Environm Canada, Canadian Ctr Climate Modelling & Anal, Montreal, PQ H3A 1B9, Canada. [Prinn, Ronald G.] MIT, Cambridge, MA 02139 USA. [Rigby, Matt] Univ Bristol, Sch Chem, Bristol BS8 1TS, Avon, England. [Ringeval, Bruno] Univ Utrecht, IMAU, NL-3584 CC Utrecht, Netherlands. [Ringeval, Bruno] Vrije Univ Amsterdam, Dept Syst Ecol, NL-1081 HV Amsterdam, Netherlands. [Shindell, Drew T.; Voulgarakis, Apostolos] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Spahni, Renato] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Strode, Sarah A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Strode, Sarah A.] NASA, Univ Space Res Assoc, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sudo, Kengo] Nagoya Univ, Grad Sch Environm Studies, Chikusa Ku, Nagoya, Aichi 4648601, Japan. [van der Werf, Guido R.] Vrije Univ Amsterdam, Fac Earth & Life Sci, NL-1081 HV Amsterdam, Netherlands. [Voulgarakis, Apostolos] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England. [van Weele, Michiel; Williams, Jason E.] Royal Netherlands Meteorol Inst KNMI, NL-3730 AE De Bilt, Netherlands. [Weiss, Ray F.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Zeng, Guang] Natl Inst Water & Atmospher Res, Omakau 9352, Central Otago, New Zealand. RP Bousquet, P (reprint author), LSCE CEA UVSQ CNRS, F-91190 Gif Sur Yvette, France. EM Philippe.Bousquet@lsce.ipsl.fr RI Strode, Sarah/H-2248-2012; Chevallier, Frederic/E-9608-2016; Heimann, Martin/H-7807-2016; van der Werf, Guido/M-8260-2016; Castaldi, Simona/B-1699-2012; Le Quere, Corinne/C-2631-2017; Langenfelds, Raymond/B-5381-2012; Krummel, Paul/A-4293-2013; Fraser, Annemarie/D-3874-2012; Fraser, Paul/D-1755-2012; Rigby, Matthew/A-5555-2012; Szopa, Sophie/F-8984-2010; Shindell, Drew/D-4636-2012; Bergmann, Daniel/F-9801-2011; Naik, Vaishali/A-4938-2013; Lamarque, Jean-Francois/L-2313-2014; Palmer, Paul/F-7008-2010; Cameron-Smith, Philip/E-2468-2011; Canadell, Josep/E-9419-2010; Steele, Paul/B-3185-2009 OI Poulter, Benjamin/0000-0002-9493-8600; Strode, Sarah/0000-0002-8103-1663; Chevallier, Frederic/0000-0002-4327-3813; Heimann, Martin/0000-0001-6296-5113; van der Werf, Guido/0000-0001-9042-8630; Castaldi, Simona/0000-0003-3937-8169; Le Quere, Corinne/0000-0003-2319-0452; SANTINI, Monia/0000-0002-8041-8241; Ringeval, Bruno/0000-0001-8405-1304; Krummel, Paul/0000-0002-4884-3678; Rigby, Matthew/0000-0002-2020-9253; Szopa, Sophie/0000-0002-8641-1737; Bergmann, Daniel/0000-0003-4357-6301; Naik, Vaishali/0000-0002-2254-1700; Lamarque, Jean-Francois/0000-0002-4225-5074; Cameron-Smith, Philip/0000-0002-8802-8627; Canadell, Josep/0000-0002-8788-3218; Steele, Paul/0000-0002-8234-3730 FU UK NERC National Centre for Earth Observation; European Commission's 7th Framework Programme (FP7) [218793, 283080]; US DOE [DE-AC52-07NA27344, DE-AC02-05CH1123]; NOAA; Australian Climate Change Science Program; ERC [247349] FX This paper is the result of an international collaboration of scientists organized by the Global Carbon Project, a joint project of the Earth System Science Partnership. This work was supported by: the UK NERC National Centre for Earth Observation; the European Commission's 7th Framework Programme (FP7/2007-2013) projects MACC (grant agreement no. 218793) and GEOCARBON (grant agreement no. 283080); contract DE-AC52-07NA27344 with different parts supported by the US DOE IMPACTS and SciDAC Climate Consortium projects; computing resources of NERSC, which is supported by the US DOE under contract DE-AC02-05CH11231; NOAA flask data for CH3CCl3 (made available by S. Montzka); the Australian Climate Change Science Program, and ERC grant 247349. Simulations from LSCE were performed using HPC resources from DSM-CCRT and CCRT/CINES/IDRIS under the allocation 2012-t2012012201 made by GENCI (Grand Equipement National de Calcul Intensif). We thank the EDGAR group at JRC (Italy) and US-EPA for providing estimates of anthropogenic emissions. NR 91 TC 330 Z9 337 U1 63 U2 499 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD OCT PY 2013 VL 6 IS 10 BP 813 EP 823 DI 10.1038/NGEO1955 PG 11 WC Geosciences, Multidisciplinary SC Geology GA 225ZL UT WOS:000325003700010 ER PT J AU Yan, Y Yue, Y Huang, H Ren, YX Ahmed, N Tur, M Dolinar, S Willner, A AF Yan, Yan Yue, Yang Huang, Hao Ren, Yongxiong Ahmed, Nisar Tur, Moshe Dolinar, Samuel Willner, Alan TI Multicasting in a spatial division multiplexing system based on optical orbital angular momentum SO OPTICS LETTERS LA English DT Article AB We report multicasting data from a single orbital angular momentum (OAM) spatial channel onto multiple OAM channels of equally spaced OAM charge numbers. The designed sliced phase patterns for multicasting are loaded on the spatial light modulator. By optimizing the design of the phase pattern, the power of multicasted OAM channels can be equalized. We experimentally demonstrate multicasting five and seven OAM channels from a single-input OAM channel carrying a 100 Gbit/s quadrature phase-shift keying (QPSK) data stream. (C) 2013 Optical Society of America C1 [Yan, Yan; Yue, Yang; Huang, Hao; Ren, Yongxiong; Ahmed, Nisar; Willner, Alan] Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA. [Tur, Moshe] Tel Aviv Univ, Sch Elect Engn, IL-69978 Ramat Aviv, Israel. [Dolinar, Samuel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Yan, Y (reprint author), Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA. EM yanyan@usc.edu FU DARPA under the InPho program FX We acknowledge the support of DARPA under the InPho program. NR 12 TC 22 Z9 22 U1 1 U2 13 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 EI 1539-4794 J9 OPT LETT JI Opt. Lett. PD OCT 1 PY 2013 VL 38 IS 19 BP 3930 EP 3933 DI 10.1364/OL.38.003930 PG 4 WC Optics SC Optics GA 236MZ UT WOS:000325802800061 PM 24081091 ER PT J AU Beechie, T Imaki, H Greene, J Wade, A Wu, H Pess, G Roni, P Kimball, J Stanford, J Kiffney, P Mantua, N AF Beechie, T. Imaki, H. Greene, J. Wade, A. Wu, H. Pess, G. Roni, P. Kimball, J. Stanford, J. Kiffney, P. Mantua, N. TI RESTORING SALMON HABITAT FOR A CHANGING CLIMATE SO RIVER RESEARCH AND APPLICATIONS LA English DT Article DE restoration; climate change; decision support; adaptation; salmon habitat; stream flow; stream temperature ID COLUMBIA RIVER-BASIN; JUVENILE CHINOOK SALMON; WESTERN UNITED-STATES; LARGE WOODY DEBRIS; PACIFIC-NORTHWEST; STREAM TEMPERATURE; ECOLOGICAL PERSPECTIVE; EVOLUTIONARY HISTORY; ONCORHYNCHUS-MYKISS; HYPORHEIC EXCHANGE AB An important question for salmon restoration efforts in the western USA is How should habitat restoration plans be altered to accommodate climate change effects on stream flow and temperature?' We developed a decision support process for adapting salmon recovery plans that incorporates (1) local habitat factors limiting salmon recovery, (2) scenarios of climate change effects on stream flow and temperature, (3) the ability of restoration actions to ameliorate climate change effects, and (4) the ability of restoration actions to increase habitat diversity and salmon population resilience. To facilitate the use of this decision support framework, we mapped scenarios of future stream flow and temperature in the Pacific Northwest region and reviewed literature on habitat restoration actions to determine whether they ameliorate a climate change effect or increase life history diversity and salmon resilience. Under the climate change scenarios considered here, summer low flows decrease by 35-75% west of the Cascade Mountains, maximum monthly flows increase by 10-60% across most of the region, and stream temperatures increase between 2 and 6 degrees C by 2070-2099. On the basis of our literature review, we found that restoring floodplain connectivity, restoring stream flow regimes, and re-aggrading incised channels are most likely to ameliorate stream flow and temperature changes and increase habitat diversity and population resilience. By contrast, most restoration actions focused on in-stream rehabilitation are unlikely to ameliorate climate change effects. Finally, we illustrate how the decision support process can be used to evaluate whether climate change should alter the types or priority of restoration actions in a salmon habitat restoration plan. Copyright (c) 2012 John Wiley & Sons, Ltd. C1 [Beechie, T.; Imaki, H.; Greene, J.; Pess, G.; Roni, P.; Kiffney, P.] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Seattle, WA 98112 USA. [Wade, A.] Univ Calif Santa Barbara, Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93106 USA. [Wu, H.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Wu, H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kimball, J.; Stanford, J.] Univ Montana, Flathead Lake Biol Stn, Missoula, MT 59812 USA. [Mantua, N.] Univ Washington, Sch Aquat & Fishery Sci, Seattle, WA 98195 USA. RP Beechie, T (reprint author), NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, 2725 Montlake Blvd E, Seattle, WA 98112 USA. EM tim.beechie@noaa.gov RI Wu, Huan/K-1003-2013 OI Wu, Huan/0000-0003-2920-8860 FU Moore Foundation; National Marine Fisheries Service FX We thank the Moore Foundation and National Marine Fisheries Service for providing funding for this research. We also thank Sarah Morley for her insightful review of the manuscript. NR 103 TC 35 Z9 35 U1 8 U2 103 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1535-1459 EI 1535-1467 J9 RIVER RES APPL JI River Res. Appl. PD OCT PY 2013 VL 29 IS 8 BP 939 EP 960 DI 10.1002/rra.2590 PG 22 WC Environmental Sciences; Water Resources SC Environmental Sciences & Ecology; Water Resources GA 232DJ UT WOS:000325469700001 ER PT J AU Martin, AM Righter, K AF Martin, Audrey M. Righter, Kevin TI Melting of clinopyroxene plus magnesite in iron-bearing planetary mantles and implications for the Earth and Mars SO CONTRIBUTIONS TO MINERALOGY AND PETROLOGY LA English DT Article DE Magma; Redox; Carbonatite; Ultramafic lamprophyre; Kamafugite; Nakhlite; Experimental petrology ID ULTRAMAFIC LAMPROPHYRES; PHASE-RELATIONS; CARBONATE-RICH; EXPERIMENTAL CONSTRAINTS; LIQUID IMMISCIBILITY; DOLOMITE CARBONATITE; NAKHLITE METEORITES; THERMODYNAMIC DATA; MARTIAN METEORITE; DIAMOND FORMATION AB The assemblage clinopyroxene + magnesite was observed in Earth's high-pressure metamorphic samples, and its stability in subducting slabs was confirmed by experiments. Recent studies also suggested that the fO(2) variations observed in SNC meteorites can be explained by polybaric graphite-CO-CO2 equilibria in the Martian mantle. Although there is no direct evidence for the stability of the cpx + mc assemblage in Mars mantle, its high-pressure-high-temperature decomposition to cpx + fo + CO2 makes it a good analogue for the source of carbon metasomatism, in particular, to study nakhlites formation. Iron, which is present in the Earth's and Martian mantles, may, however, influence the speciation of carbon. We performed experiments on a clinopyroxene + magnesite assemblage at 1.8 and 3.0 GPa and temperatures corresponding to the Earth's and Martian mantles. The role of iron and of fO(2) was investigated by (1) replacing all or part of the magnesite by siderite FeCO3, (2) adding Fe-0 and (3) using graphite C capsules. A carbonate-silicate melt forms at both Earth and Mars conditions. Clinopyroxene and olivine are the main solid phases in the iron-free experiments. Fe2+ and Fe-0 decrease their melting temperatures and increase the silicate fraction in the melt. The produced carbonate-silicate melts may be involved in the formation of some carbon-rich lavas on Earth (e.g., carbonatites, ultramafic lamprophyres, or kamafugites). Our results may also be used to interpret ophiolite samples or inclusions. In particular, we show that wustite may form in equilibrium with carbonate-silicate melt in opx-(and silica-) poor regions of the mantle below 3 GPa. Our results also confirm the hypothesis of carbon metasomatism in the Martian nakhlites source. Immiscibility or reduction could explain the absence or rarity of C in Martian lavas. C1 [Martin, Audrey M.; Righter, Kevin] NASA Johnson Space Ctr, Mailcode KT, Houston, TX 77058 USA. 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 FU NASA Postdoctoral Program at the Johnson Space Center; National Science Foundation-Earth Sciences [EAR-1128799]; Department of Energy-Geosciences [DE-FG02-94ER14466]; U S Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-AC02-06CH11357] FX K. Pando and L. R. Danielson are gratefully acknowledged for their support on the experimental devices; A. Peslier, G. Robinson, and K. Ross for their help on the microscopes; L. Le for her assistance during Raman analyses; and S. Sutton and M. Newville for their support during XANES analyses. E. Medard is also acknowledged for his insightful comments. We thank three anonymous reviewers for their comments and Gordon Moore for his editorial work. 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, and by an RTOP to KR from the Mars Fundamental Research Program. Portions of this work were performed at GeoSoilEnviroCARS (Sector 13), Advanced Photon Source (APS), Argonne National Laboratory. GeoSoilEnviroCARS is supported by the National Science Foundation-Earth Sciences (EAR-1128799) and Department of Energy-Geosciences (DE-FG02-94ER14466). Use of the Advanced Photon Source was supported by the U S Department of Energy, Office of Science, Office of Basic Energy Sciences, under Contract no. DE-AC02-06CH11357. NR 121 TC 2 Z9 2 U1 1 U2 22 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0010-7999 EI 1432-0967 J9 CONTRIB MINERAL PETR JI Contrib. Mineral. Petrol. PD OCT PY 2013 VL 166 IS 4 BP 1067 EP 1098 DI 10.1007/s00410-013-0910-5 PG 32 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 220WK UT WOS:000324617600007 ER PT J AU Yates, EL Detweiler, AM Iraci, LT Bebout, BM McKay, CP Schiro, K Sheffner, EJ Kelley, CA Tadic, JM Loewenstein, M AF Yates, Emma L. Detweiler, Angela M. Iraci, Laura T. Bebout, Brad M. McKay, Christopher P. Schiro, Kathleen Sheffner, Edwin J. Kelley, Cheryl A. Tadic, Jovan M. Loewenstein, Max TI Assessing the role of alkaline soils on the carbon cycle at a playa site SO ENVIRONMENTAL EARTH SCIENCES LA English DT Article DE Semi-arid ecosystem; Playa; Alkaline soils; Carbon dioxide flux; Carbon cycle; Carbon dioxide adsorption ID NET ECOSYSTEM; CO2 FLUX; DIOXIDE; SEQUESTRATION; CALIBRATION; EXCHANGE; METHANE AB Alkaline soils occupy approximately 5 % of the Earth's land surface (7 million km), and this may increase due to the global trend towards increasing desertification, yet the extent to which these soils modulate carbon dynamics on regional and global scales is inadequately studied and poorly understood. Railroad Valley (RRV) playa (Nevada, USA) is a semi-arid playa with highly alkaline soils (pH > 10) and no vegetation. The extreme, alkaline environment and absence of vascular vegetation make RRV an ideal site to investigate the role of physiochemical processes of soil-atmosphere CO2 exchange. Both field and laboratory investigations were conducted. This work shows how the atmospheric CO2 mixing ratio decreases at nighttime at RRV playa to a value well below the average global background CO2 concentration. Laboratory investigations using soil samples collected at RRV playa confirmed that CO2 uptake by RRV playa soils occurs when temperatures are decreased. Both field and laboratory studies suggest that the alkaline RRV soil acts as a CO2 reservoir during colder periods, such as at nighttime. These results highlight the importance of investigating carbon dynamics in previously understudied environments. Given how little information is available on the CO2 flux in desert and semi-arid alkaline ecosystems lacking vegetation, our findings draw attention to these environments as becoming increasingly important for carbon fluxes on regional and global scales. C1 [Yates, Emma L.; Detweiler, Angela M.; Iraci, Laura T.; Bebout, Brad M.; McKay, Christopher P.; Sheffner, Edwin J.; Tadic, Jovan M.; Loewenstein, Max] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Detweiler, Angela M.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Schiro, Kathleen] Univ Calif Los Angeles, Dept Atmospher Sci, Los Angeles, CA 90095 USA. [Kelley, Cheryl A.] Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. RP Yates, EL (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM emma.l.yates@nasa.gov RI Kelley, Cheryl/K-9392-2015; Tadic, Jovan/P-3677-2016 FU NASA's Earth Science Division and Oak Ridge Associated Universities (ORAU) through the NASA Postdoctoral Program; NASA's Exobiology Program FX We specifically acknowledge the cooperation and efforts of the personnel involved in the Railroad Valley vicarious calibration experiment from the Atmospheric CO2 Observations from Space (ACOS) Team, Japan Aerospace Exploration Agency (JAXA), National Institute for Environmental Studies (NIES), Colorado State University (CSU) and particular thanks to G. Jacobson from Picarro Inc. We also thank the University of Arizona Remote Sensing Group for making the research facilities at Railroad Valley available, Prof. Craig Clements (San Jose State University) for additional instrumentation and Adrienne Frisbee for guidance. We acknowledge financial support from NASA's Earth Science Division and Oak Ridge Associated Universities (ORAU) through the NASA Postdoctoral Program (E.L.Y., J.M.T.). The participation of B. M. Bebout, C. A. Kelley and A. M. Detweiler was made possible by financial support from NASA's Exobiology Program. NR 31 TC 14 Z9 15 U1 1 U2 23 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1866-6280 J9 ENVIRON EARTH SCI JI Environ. Earth Sci. PD OCT PY 2013 VL 70 IS 3 BP 1047 EP 1056 DI 10.1007/s12665-012-2194-x PG 10 WC Environmental Sciences; Geosciences, Multidisciplinary; Water Resources SC Environmental Sciences & Ecology; Geology; Water Resources GA 216AJ UT WOS:000324252900006 ER PT J AU Golding, J Steer, CD Hibbeln, JR Emmett, PM Lowery, T Jones, R AF Golding, Jean Steer, Colin D. Hibbeln, Joseph R. Emmett, Pauline M. Lowery, Tony Jones, Robert TI Dietary Predictors of Maternal Prenatal Blood Mercury Levels in the ALSPAC Birth Cohort Study SO ENVIRONMENTAL HEALTH PERSPECTIVES LA English DT Article ID UK TOTAL DIET; METHYLMERCURY EXPOSURE; CHILD-DEVELOPMENT; FISH CONSUMPTION; REACTION CELL; ICP-MS; POPULATION; CADMIUM; FOOD; AGE AB BACKGROUND: Very high levels of prenatal maternal mercury have adverse effects on the developing fetal brain. It has been suggested that all possible sources of mercury should be avoided. However, although seafood is a known source of mercury, little is known about other dietary components that contribute to the overall levels of blood mercury. OBJECTIVE: Our goal was to quantify the contribution of components of maternal diet to prenatal blood mercury level. METHODS: Whole blood samples and information on diet and sociodemographic factors were collected from pregnant women (n = 4,484) enrolled in the Avon Longitudinal Study of Parents and Children (ALSPAC). The blood samples were assayed for total mercury using inductively coupled plasma dynamic reaction cell mass spectrometry. Linear regression was used to estimate the relative contributions of 103 dietary variables and 6 sociodemographic characteristics to whole blood total mercury levels (TBM; untransformed and log-transformed) based on R-2 values. RESULTS: We estimated that maternal diet accounted for 19.8% of the total variation in ln-TBM, with 44% of diet-associated variability (8.75% of the total variation) associated with seafood consumption (white fish, oily fish, and shellfish). Other dietary components positively associated with TBM included wine and herbal teas, and components with significant negative associations included white bread, meat pies or pasties, and french fries. CONCLUSIONS: Although seafood is a source of dietary mercury, seafood appeared to explain a relatively small proportion of the variation in TBM in our UK study population. Our findings require confirmation, but suggest that limiting seafood intake during pregnancy may have a limited impact on prenatal blood mercury levels. C1 [Golding, Jean; Steer, Colin D.; Emmett, Pauline M.] Univ Bristol, Ctr Child & Adolescent Hlth, Bristol, Avon, England. [Hibbeln, Joseph R.] NIAAA, NIH, US Dept HHS, Bethesda, MD USA. [Lowery, Tony] NOAA, Natl Marine Fisheries Serv, Natl Seafood Inspect Lab, Pascagoula, MS USA. [Jones, Robert] Ctr Dis Control & Prevent, Inorgan & Radiat Analyt Toxicol Branch, Atlanta, GA USA. RP Golding, J (reprint author), Sch Social & Community Med, Ctr Child & Adolescent Hlth, Oakfield House,Oakfield Rd, Bristol BS8 2BN, Avon, England. EM jean.golding@bristol.ac.uk OI Emmett, Pauline/0000-0003-1076-4779; Golding, Jean/0000-0003-2826-3307 FU National Oceanic and Atmospheric Administration (NOAA); Intramural Research Program of the National Institute on Alcohol Abuse and Alcoholism, National Institutes of Health (NIH) FX The UK Medical Research Council (MRC), the Wellcome Trust, and the University of Bristol currently provide core support for ALSPAC. The assays of the maternal blood samples were carried out at the Centers for Disease Control and Prevention with funding from the National Oceanic and Atmospheric Administration (NOAA), and the statistical analyses were carried out in Bristol with funding from NOAA and support from the Intramural Research Program of the National Institute on Alcohol Abuse and Alcoholism, National Institutes of Health (NIH). NR 45 TC 26 Z9 28 U1 3 U2 35 PU US DEPT HEALTH HUMAN SCIENCES PUBLIC HEALTH SCIENCE PI RES TRIANGLE PK PA NATL INST HEALTH, NATL INST ENVIRONMENTAL HEALTH SCIENCES, PO BOX 12233, RES TRIANGLE PK, NC 27709-2233 USA SN 0091-6765 J9 ENVIRON HEALTH PERSP JI Environ. Health Perspect. PD OCT PY 2013 VL 121 IS 10 BP 1214 EP 1218 DI 10.1289/ehp.1206115 PG 5 WC Environmental Sciences; Public, Environmental & Occupational Health; Toxicology SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Toxicology GA 227YU UT WOS:000325152400026 PM 23811414 ER PT J AU Chang, SK DiNardo, G Farley, J Brodziak, J Yuan, ZL AF Chang, Shui-Kai DiNardo, Gerard Farley, Jessica Brodziak, Jon Yuan, Zih-Lun TI Possible stock structure of dolphinfish (Coryphaena hippurus) in Taiwan coastal waters and globally based on reviews of growth parameters SO FISHERIES RESEARCH LA English DT Review DE Dolphinfish; Growth performance index; von Bertalanffy growth function; Simultaneous confidence region; Stock structure ID WESTERN CENTRAL ATLANTIC; EAST-CHINA SEA; NORTH-CAROLINA; REPRODUCTIVE-BIOLOGY; PACIFIC-OCEAN; AGE; FISH; POPULATION; GULF; MANAGEMENT AB Dolphinfish (Coryphaena hippurus) is used by many coastal countries. Sustaining harvest of this resource will require cooperation among fishing countries in each region, and determining population structure is paramount to ensuring effective management. Examining life-history parameters (such as growth rate) is a useful and relatively inexpensive method for identifying possible stock units, which can be subsequently confirmed by other methods. The purpose of this study is two-fold. First, we examine the two-stock assumption for Taiwanese dolphinfish and the reliability of estimated growth curves based on seasonally-stratified growth performance indices. The von Bertalanffy growth functions (VBGF) were firstly estimated from 2005 to 2009 length frequency sample data of eastern and southern coasts of Taiwan. New growth performance indices were then calculated from the log-transformed parameters of the VBGF and examined by a simultaneous confidence region (SCR) under the assumption of bivariate normal distribution. Second, we summarize VBGF parameter estimates from all regions worldwide and based on the growth parameters and performance indices, review the possible stock structures and the reliability of growth estimations for dolphinfish. The results support a single-stock hypothesis for dolphinfish in the Kuroshio Current off Taiwan with new estimated VBGF parameters of L-infinity = 149.4 cm and K = 0.72 year(-1). Some potentially biased estimates of dolphinfish growth parameters are identified in the worldwide VBGF dataset and are suggested for further investigations. Excluding these estimates, the results indicate at least a five-stock structure in the Pacific and the Atlantic oceans. (C) 2013 Elsevier B.V. All rights reserved. C1 [Chang, Shui-Kai; Yuan, Zih-Lun] Natl Sun Yat Sen Univ, Inst Marine Affairs, Kaohsiung 804, Taiwan. [DiNardo, Gerard; Brodziak, Jon] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96816 USA. [Farley, Jessica] CSIRO Marine & Atmospher Res, Hobart, Tas 7001, Australia. RP Chang, SK (reprint author), Natl Sun Yat Sen Univ, Inst Marine Affairs, 70 Lien Hai Rd, Kaohsiung 804, Taiwan. EM skchang@faculty.nsysu.edu.tw RI Farley, Jessica/E-4957-2014; OI Chang, Shui-Kai/0000-0003-2929-1510 FU NOAA [NFFR7400-11-04742, NFFR7400-12-03755]; Asia-Pacific Ocean Research Centre, National Sun Yat-sen University FX We appreciate the constructive comments made by Dr. Simon Hoyle of the Secretariat of the Pacific Community and Dr. Paige Eveson of the CSIRO Marine & Atmospheric Research on the manuscript. We also greatly appreciate the exhaustive comments and efforts made by the two anonymous reviewers. Financial support for the research was provided by NOAA contracts NFFR7400-11-04742 and NFFR7400-12-03755, and partially by the Asia-Pacific Ocean Research Centre, National Sun Yat-sen University. NR 57 TC 3 Z9 3 U1 2 U2 22 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-7836 J9 FISH RES JI Fish Res. PD OCT PY 2013 VL 147 BP 127 EP 136 DI 10.1016/j.fishres.2013.05.003 PG 10 WC Fisheries SC Fisheries GA 228MW UT WOS:000325191900014 ER PT J AU Hannan, KM Fogg, AQ Driggers, WB Hoffmayer, ER Ingram, GW Grace, MA AF Hannan, Kristin M. Fogg, Alex Q. Driggers, William B., III Hoffmayer, Eric R. Ingram, G. Walter, Jr. Grace, Mark A. TI Size selectivity and catch rates of two small coastal shark species caught on circle and J hooks in the northern Gulf of Mexico SO FISHERIES RESEARCH LA English DT Article DE Bottom longline; Carcharhinidae; Commercial fisheries; Elasmobranch ID PELAGIC LONGLINE FISHERY; EQUATORIAL ATLANTIC-OCEAN; MORTALITY; CONSERVATION; MANAGEMENT; BYCATCH; IMPACT; TARGET AB Experimental longline sets were conducted in the northern Gulf of Mexico to examine effects of similarly sized circle and J hooks on the catchability and size selectivity of Atlantic sharpnose (Rhizoprionodon terraenovae) and blacknose (Carcharhinus acronotus) sharks. Circle hooks caught relatively smaller fish but showed a higher catch per unit effort than J hooks for both species. Potential biasing factors such as spatiotemporal variability in longline deployment locations and differential bite-off rates between hook types were examined; however, neither source was found to be significant. As all gear components, with the exception of hook type, were constant, the difference in size selectivity and catchability between hook types was attributed to the narrower minimum width of the circle hooks, as has been suggested for other fishes. The results of this study demonstrate that when comparing similarly sized hook types, relatively small sharks are more susceptible to circle hooks than J hooks. This finding underlines the importance of understanding which segment of a population is most vulnerable to a specific hook type and size if mandating the use of a specific hook is considered as a management strategy. Published by Elsevier B.V. C1 [Hannan, Kristin M.; Fogg, Alex Q.; Driggers, William B., III; Hoffmayer, Eric R.; Ingram, G. Walter, Jr.; Grace, Mark A.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, Pascagoula, MS 39567 USA. RP Driggers, WB (reprint author), Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, PO Drawer 1207, Pascagoula, MS 39567 USA. EM william.driggers@noaa.gov NR 29 TC 4 Z9 5 U1 0 U2 23 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-7836 J9 FISH RES JI Fish Res. PD OCT PY 2013 VL 147 BP 145 EP 149 DI 10.1016/j.fishres.2013.05.005 PG 5 WC Fisheries SC Fisheries GA 228MW UT WOS:000325191900016 ER PT J AU DeBoer, DR Cruz-Pol, SL Davis, MM Gaier, T Feldman, P Judge, J Kellermann, KI Long, DG Magnani, L McKague, DS Pearson, TJ Rogers, AEE Reising, SC Taylor, G Thompson, AR AF DeBoer, David R. Cruz-Pol, Sandra L. Davis, Michael M. Gaier, Todd Feldman, Paul Judge, Jasmeet Kellermann, Kenneth I. Long, David G. Magnani, Loris McKague, Darren S. Pearson, Timothy J. Rogers, Alan E. E. Reising, Steven C. Taylor, Gregory Thompson, A. Richard TI Radio Frequencies: Policy and Management SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Radio astronomy; radio frequency interference; radio science; spectrum management AB The electromagnetic spectrum is a valued shared resource. Its scientific use allows us to learn about our universe, measure and monitor our planet, and communicate scientific data. The use of the spectrum is managed by national, regional, and global regulatory frameworks. There are increasing demands for new or extended allocations because of vast technological advances in the past few years. Understanding spectrum management is important in the successful planning and execution of missions and instruments, as well as in determining the potential source of radio frequency interference in existing data and instruments, and in working to ameliorate its impact. This paper provides a summary of this framework for radio scientists and engineers. C1 [DeBoer, David R.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Cruz-Pol, Sandra L.] Univ Puerto Rico, Mayaguez, PR 00682 USA. [Davis, Michael M.] SETI Inst, Mountain View, CA 94043 USA. [Davis, Michael M.] SETI Inst, Hat Creek, CA 94043 USA. [Gaier, Todd] Jet Propulson Lab, Pasadena, CA 91109 USA. [Feldman, Paul] FHH Law, Washington, DC 22209 USA. [Judge, Jasmeet] Univ Florida, Gainesville, FL 32611 USA. [Thompson, A. Richard] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Long, David G.] Brigham Young Univ, Provo, UT 84602 USA. [Magnani, Loris] Univ Georgia, Athens, GA 30602 USA. [McKague, Darren S.] Univ Michigan, Ann Arbor, MI 48109 USA. [Pearson, Timothy J.] CALTECH, Pasadena, CA 91125 USA. [Rogers, Alan E. E.] MIT, Cambridge, MA 02139 USA. [Reising, Steven C.] Colorado State Univ, Ft Collins, CO 80523 USA. [Taylor, Gregory] Univ New Mexico, Albuquerque, NM 87131 USA. RP DeBoer, DR (reprint author), Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. EM ddeboer@berkeley.edu; cruzpol@ece.uprm.edu; mdavis@seti.org; todd.c.gaier@jpl.nasa.gov; feldman@fhhlaw.com; jasmeet@ufl.edu; kellerm@nrao.edu; long@ee.byu.edu; loris@physast.uga.edu; dmckague@umich.edu; tjp@astro.caltech.edu; aeer@haystack.mit.edu; steven.reising@colostate.edu; gbtaylor@unm.edu; athompso@nrao.edu RI McKague, Darren/J-2590-2012; Long, David/K-4908-2015; Pearson, Timothy/N-2376-2015 OI McKague, Darren/0000-0003-0297-0388; Long, David/0000-0002-1852-3972; Pearson, Timothy/0000-0001-5213-6231 NR 12 TC 3 Z9 3 U1 2 U2 13 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD OCT PY 2013 VL 51 IS 10 SI SI BP 4918 EP 4927 DI 10.1109/TGRS.2013.2253471 PG 10 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 230XX UT WOS:000325377900002 ER PT J AU Bradley, D Morris, JM AF Bradley, Damon Morris, Joel M. TI On the Performance of Negentropy Approximations as Test Statistics for Detecting Sinusoidal RFI in Microwave Radiometers SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Entropy; information theory; interference; microwave radiometry ID RADIO-FREQUENCY INTERFERENCE AB Radio-frequency interference (RFI) is a persistent threat to Earth-observing microwave radiometers. A number of test statistics are used for radiometric RFI detection. This paper presents a new RFI detection method that uses the information theoretic quantity known as negentropy. In particular, we study six negentropy-based test statistics and compare their performance against kurtosis, Jarque-Bera, Anderson-Darling, and Shapiro-Wilk normality tests for specific RFI signal models. The Neyman-Pearson decision rule is used to develop receiver operating characteristic curves for each test statistic. We show that although negentropy can be used to detect RFI, it does not outperform kurtosis, except for the kurtosis blind-spot case. C1 [Bradley, Damon] NASA, Goddard Space Flight Ctr, Digital Signal Proc Technol Grp, Instrument Elect Dev Branch, Greenbelt, MD 20771 USA. [Bradley, Damon; Morris, Joel M.] Univ Maryland Baltimore Cty, Dept Comp Sci & Elect Engn, Baltimore, MD 21250 USA. RP Bradley, D (reprint author), NASA, Goddard Space Flight Ctr, Digital Signal Proc Technol Grp, Instrument Elect Dev Branch, Greenbelt, MD 20771 USA. NR 16 TC 5 Z9 5 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD OCT PY 2013 VL 51 IS 10 SI SI BP 4945 EP 4951 DI 10.1109/TGRS.2013.2266358 PG 7 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 230XX UT WOS:000325377900005 ER PT J AU Spencer, MW Chen, CW Ghaemi, H Chan, SF Belz, JE AF Spencer, Michael W. Chen, Curtis W. Ghaemi, Hirad Chan, Samuel F. Belz, John E. TI RFI Characterization and Mitigation for the SMAP Radar SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Earth remote sensing; L-band radar systems; radio frequency interference (RFI); Soil Moisture Active-Passive (SMAP) mission ID INSTRUMENT; MISSION AB The Soil Moisture Active-Passive (SMAP) mission will launch in late 2014 and will carry a combined L-band radiometer/radar instrument for the retrieval of global soil moisture and surface freeze-thaw state. Radio frequency interference (RFI) is a known challenge for Earth remote sensing in the L-band portion of the spectrum. This paper addresses efforts to characterize and mitigate RFI for the SMAP radar. A model for the RFI environment due to surface-based emitters is developed, and is shown to agree well with the observations of currently operating L-band radar systems. An analysis of the environment due to space-based emitters is also presented. Techniques to mitigate RFI in the radar band are described, and are shown to perform sufficiently well to meet the stringent SMAP measurement requirements. A companion paper addresses the different issues encountered with RFI in the radiometer band. C1 [Spencer, Michael W.; Chen, Curtis W.; Ghaemi, Hirad; Chan, Samuel F.; Belz, John E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Spencer, MW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM michael.w.spencer@jpl.nasa.gov; curtis.w.chen@jpl.nasa.gov; hirad.ghaemi@jpl.nasa.gov; samuel.f.chan@jpl.nasa.gov; john.e.belz@jpl.nasa.gov FU Jet Propulsion Laboratory, California Institute of Technology under National Aeronautics and Space Administration FX This work was supported by the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration. NR 11 TC 7 Z9 7 U1 0 U2 16 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD OCT PY 2013 VL 51 IS 10 SI SI BP 4973 EP 4982 DI 10.1109/TGRS.2013.2253472 PG 10 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 230XX UT WOS:000325377900008 ER PT J AU Walker, RT Holland, DM Parizek, BR Alley, RB Nowicki, SMJ Jenkins, A AF Walker, Ryan T. Holland, David M. Parizek, Byron R. Alley, Richard B. Nowicki, Sophie M. J. Jenkins, Adrian TI Efficient Flowline Simulations of Ice Shelf-Ocean Interactions: Sensitivity Studies with a Fully Coupled Model SO JOURNAL OF PHYSICAL OCEANOGRAPHY LA English DT Article DE Ice sheets; Ice shelves; Coupled models; Numerical analysis; modeling ID PINE ISLAND GLACIER; AUTONOMOUS UNDERWATER VEHICLE; THERMOHALINE CIRCULATION; GROUNDING LINE; TURBULENT HEAT; MASS-TRANSFER; WEDDELL SEA; BENEATH; ANTARCTICA; TEMPERATURE AB Thermodynamic flowline and plume models for the ice shelf-ocean system simplify the ice and ocean dynamics sufficiently to allow extensive exploration of parameters affecting ice-sheet stability while including key physical processes. Comparison between geophysically and laboratory-based treatments of ice-ocean interface thermodynamics shows reasonable agreement between calculated melt rates, except where steep basal slopes and relatively high ocean temperatures are present. Results are especially sensitive to the poorly known drag coefficient, highlighting the need for additional field experiments to constrain its value. These experiments also suggest that if the ice-ocean interface near the grounding line is steeper than some threshold, further steepening of the slope may drive higher entrainment that limits buoyancy, slowing the plume and reducing melting; if confirmed, this will provide a stabilizing feedback on ice sheets under some circumstances. C1 [Walker, Ryan T.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Walker, Ryan T.; Nowicki, Sophie M. J.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Holland, David M.] NYU, Courant Inst Math Sci, New York, NY USA. [Parizek, Byron R.] Penn State Univ, Du Bois, PA USA. [Alley, Richard B.] Penn State Univ, University Pk, PA 16802 USA. [Jenkins, Adrian] British Antarctic Survey, Nat Environm Res Council, Cambridge CB3 0ET, England. RP Walker, RT (reprint author), NASA, Goddard Space Flight Ctr, Code 615,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM ryan.t.walker@nasa.gov FU NASA [NNX10I04G, NNX12AD03A]; NSF [0909335, 0424589, ARC-0806393, ANT-0732869, ANT-1043395]; NYU Abu Dhabi [G1204] FX RTW, BRP, and RBA were supported by NASA through Grant NNX10I04G. RTW was also supported by NASA Grant NNX12AD03A to ESSIC. BRP and RBA were also supported by NSF through Grant 0909335 and through Grant 0424589 to the Center for Remote Sensing of Ice Sheets (CReSIS). DMH was supported by NSF through Grants ARC-0806393, ANT-0732869, and ANT-1043395, and by NYU Abu Dhabi Grant G1204. We thank the editor and two anonymous reviewers for their contributions to an improved final manuscript. NR 52 TC 4 Z9 4 U1 2 U2 18 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-3670 J9 J PHYS OCEANOGR JI J. Phys. Oceanogr. PD OCT PY 2013 VL 43 IS 10 BP 2200 EP 2210 DI 10.1175/JPO-D-13-037.1 PG 11 WC Oceanography SC Oceanography GA 232ZT UT WOS:000325534400011 ER PT J AU Christensen, MW Carrio, GG Stephens, GL Cotton, WR AF Christensen, Matthew W. Carrio, Gustavo G. Stephens, Graeme L. Cotton, William R. TI Radiative Impacts of Free-Tropospheric Clouds on the Properties of Marine Stratocumulus SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article DE Entrainment; Diurnal effects; Cirrus clouds; Cloud radiative effects; Satellite observations; Large eddy simulations ID SOUTHEAST PACIFIC STRATOCUMULUS; LARGE-EDDY SIMULATION; LIQUID WATER PATH; DIURNAL CYCLE; MIXED-LAYER; CLIMATE; VARIABILITY; FEEDBACKS; DRIZZLE; SYSTEM AB Observations from multiple satellites and large-eddy simulations (LESs) from the Regional Atmospheric Modeling System (RAMS) are used to determine the extent to which free-tropospheric clouds (FTCs) affect the properties of stratocumulus. Overlying FTCs decrease the cloud-top radiative cooling in stratocumulus by an amount that depends on the upper-cloud base altitude, cloud optical thickness, and abundance of moisture between the cloud layers. On average, FTCs increase the downward longwave radiative flux above stratocumulus clouds (at 3.5 km) by approximately 30 W m(-2). As a consequence, this forcing translates to a relative decrease in stratocumulus cooling rates by about 20%. Overall, the reduced cloud-top radiative cooling decreases the turbulent mixing, vertical development, and precipitation rate in stratocumulus clouds at night. During the day these effects are greatly reduced because the overlying clouds shade the stratocumulus from strong solar radiation, thus reducing the net radiative effect by the upper cloud. Differences in liquid water path are also observed in stratocumulus; however, the response is tied to the diurnal cycle and the time scale of interaction between the FTCs and the stratocumulus. Radiative effects by FTCs tend to be largest in the midlatitudes where the clouds overlying stratocumulus tend to be more frequent, lower, and thicker on average. In conclusion, changes in net radiation and moisture brought about by FTCs can significantly affect the dynamics of marine stratocumulus and these processes should be considered when evaluating cloud feedbacks in the climate system. C1 [Christensen, Matthew W.; Carrio, Gustavo G.; Cotton, William R.] Colorado State Univ, Ft Collins, CO 80523 USA. [Stephens, Graeme L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Christensen, MW (reprint author), CALTECH, Jet Prop Lab, 4800 Grove Dr, Pasadena, CA 91109 USA. EM matt.christensen@jpl.nasa.gov RI Christensen, Matthew/C-5733-2013 FU NASA [NNX07AR11G, NAS5-99237, NNX09AK02G] FX This work was funded by the NASA Grants NNX07AR11G, NAS5-99237, and NNX09AK02G. We thank Steven Saleeby for providing the microphysics code for RAMS and the technical support for running the model. The authors would also thank the three anonymous reviewers for their thoughtful input and suggestions in writing this manuscript. NR 32 TC 17 Z9 17 U1 1 U2 11 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 J9 J ATMOS SCI JI J. Atmos. Sci. PD OCT PY 2013 VL 70 IS 10 BP 3102 EP 3118 DI 10.1175/JAS-D-12-0287.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 227XB UT WOS:000325147900006 ER PT J AU Ganguly, R Lynch, RS Charlton, JC Eracleous, M Tripp, TM Palma, C Sembach, KR Misawa, T Masiero, JR Milutinovic, N Lackey, BD Jones, TM AF Ganguly, Rajib Lynch, Ryan S. Charlton, Jane C. Eracleous, Michael Tripp, Todd M. Palma, Christopher Sembach, Kenneth R. Misawa, Toru Masiero, Joseph R. Milutinovic, Nikola Lackey, Benjamin D. Jones, Therese M. TI A census of quasar-intrinsic absorption in the Hubble Space Telescope archive: systems from high-resolution echelle spectra SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; quasars: absorption lines; quasars: general ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; C-IV ABSORPTION; LINE KEY PROJECT; SOFT-X-RAY; ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; LY-ALPHA ABSORBERS; DRIVEN DISK WINDS; RADIO-LOUD QSOS; STELLAR OBJECTS AB We present a census of z(abs) less than or similar to 2 intrinsic (those showing partial coverage) and associated (z(abs) similar to z(em)) quasar absorption-line systems detected in the Hubble Space Telescope archive of Space Telescope Imaging Spectrograph echelle spectra. This work complements the Misawa et al. survey of 2 < z(em) < 4 quasars that selects systems using similar techniques. We confirm the existence of so-called strong N v intrinsic systems (where the equivalent width of H i Ly alpha is small compared to N v lambda 1238) presented in that work, but find no convincing cases of 'strong C iv' intrinsic systems at low redshift/luminosity. Moreover, we also report on the existence of 'strong O vi' systems. From a comparison of partial coverage results as a function of ion, we conclude that systems selected by the N v ion have the highest probability of being intrinsic. By contrast, the C iv and O vi ions are poor selectors. Of the 30 O vi systems tested, only two of the systems in the spectrum on 3C 351 show convincing evidence for partial coverage. However, there is an similar to 3 Sigma excess in the number of absorbers near the quasar redshift (vertical bar delta v vertical bar < 5000 km s(-1)) over absorbers at large redshift differences. In at least two cases, the associated O vi systems are known not to arise close to the accretion disc of the quasar. C1 [Ganguly, Rajib] Univ Michigan, Dept Comp Sci Engn & Phys, Flint, MI 48503 USA. [Lynch, Ryan S.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Charlton, Jane C.; Eracleous, Michael; Palma, Christopher] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Tripp, Todd M.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Sembach, Kenneth R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Misawa, Toru] Shinshu Univ, Sch Gen Educ, Nagano 3908621, Japan. [Masiero, Joseph R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Milutinovic, Nikola] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. [Lackey, Benjamin D.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Jones, Therese M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Ganguly, R (reprint author), Univ Michigan, Dept Comp Sci Engn & Phys, 213 Murchie Sci Bldg,303 East Keasley St, Flint, MI 48503 USA. EM ganguly@umflint.edu OI Masiero, Joseph/0000-0003-2638-720X FU NASA through Space Telescope Science Institute [HST-AR-10296.06-A]; NASA [NAS5-26555, NAG5-10817]; NSF [AST-0807993]; 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 FX The authors wish to thank Charles Danforth for useful discussions and the anonymous referee for a thoughtful review. RG acknowledges support provided under programme number HST-AR-10296.06-A by NASA through a grant from the Space Telescope Science Institute, which is operated by the Associated of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. This work was also supported by NASA grant NAG5-10817 and NSF grant AST-0807993.; 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. Funding for the Sloan Digital Sky Survey (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 (ARC) 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, the University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, the 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. NR 149 TC 7 Z9 7 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2013 VL 435 IS 2 BP 1233 EP 1264 DI 10.1093/mnras/stt1366 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 229KY UT WOS:000325264600025 ER PT J AU Datas, A Chubb, DL Veeraragavan, A AF Datas, A. Chubb, D. L. Veeraragavan, A. TI Steady state analysis of a storage integrated solar thermophotovoltaic (SISTPV) system SO SOLAR ENERGY LA English DT Article DE Solar energy; Thermal storage; Phase change material; Photovoltaics; Concentrating solar power; Solar thermophotovoltaics ID THERMAL-ENERGY STORAGE; PHASE-CHANGE MATERIAL; POWER-SYSTEM; EFFICIENCY; CONVERSION; MODEL; EMITTERS; CELLS AB This paper presents the theoretical analysis of a storage integrated solar thermophotovoltaic (SISTPV) system operating in steady state. These systems combine thermophotovoltaic (TPV) technology and high temperature thermal storage phase-change materials (PCM) in the same unit, providing a great potential in terms of efficiency, cost reduction and storage energy density. The main attraction in the proposed system is its simplicity and modularity compared to conventional Concentrated Solar Power (CSP) technologies. This is mainly due to the absence of moving parts. In this paper we analyze the use of Silicon as the phase change material (PCM). Silicon is an excellent candidate because of its high melting point (1680 K) and its very high latent heat of fusion of 1800 kJ/kg, which is about ten times greater than the conventional PCMs like molten salts. For a simple system configuration, we have demonstrated that overall conversion efficiencies up to similar to 35% are approachable. Although higher efficiencies are expected by incorporating more advanced devices like multijunction TPV cells, narrow band selective emitters or adopting near-field TPV configurations as well as by enhancing the convective/conductive heat transfer within the PCM. In this paper, we also discuss about the optimum system configurations and provide the general guidelines for designing these systems. Preliminary estimates of night time operations indicate it is possible to achieve over 10 h of operation with a relatively small quantity of Silicon. (c) 2013 Elsevier Ltd. All rights reserved. C1 [Datas, A.] Univ Politecn Madrid, Inst Energia Solar, E-28040 Madrid, Spain. [Chubb, D. L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Veeraragavan, A.] Univ Queensland, Sch Mech & Min Engn, Brisbane, Qld 4072, Australia. RP Datas, A (reprint author), Univ Politecn Madrid, Inst Energia Solar, E-28040 Madrid, Spain. EM a.datas@ies-def.upm.es RI Datas, Alejandro/M-2490-2014; OI Datas, Alejandro/0000-0001-5964-3818; Veeraragavan, Ananthanarayanan/0000-0001-6810-2204 NR 53 TC 15 Z9 15 U1 2 U2 29 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0038-092X J9 SOL ENERGY JI Sol. Energy PD OCT PY 2013 VL 96 BP 33 EP 45 DI 10.1016/j.solener.2013.07.002 PG 13 WC Energy & Fuels SC Energy & Fuels GA 225LA UT WOS:000324963200004 ER PT J AU Calhoun, DM Curran, SS Pulis, EE Provaznik, JM Franks, JS AF Calhoun, Dana M. Curran, Stephen S. Pulis, Eric E. Provaznik, Jennifer M. Franks, James S. TI Hirudinella ventricosa (Pallas, 1774) Baird, 1853 represents a species complex based on ribosomal DNA SO SYSTEMATIC PARASITOLOGY LA English DT Article ID MAXIMUM-LIKELIHOOD; STOMACH CONTENTS; BIOLOGICAL TAGS; ATLANTIC-OCEAN; TREMATODA; DIGENEA; PLATYHELMINTHES; HEMIUROIDEA; PARASITES; PACIFIC AB Digeneans in the genus Hirudinella de Blainville, 1828 (Hirudinellidae) from three species of pelagic fishes, Acanthocybium solandri (Cuvier), Makaira nigricans Lac,pSde and Thunnus albacares (Bonnaterre), and one benthic fish, Mulloidichthys martinicus (Cuvier), from the Gulf of Mexico are investigated using comparison of ribosomal DNA. Four species are identified based on molecular differences: Hirudinella ventricosa (Pallas, 1774) Baird, 1853 from A. solandri, Hirudinella ahi Yamaguti, 1970 from T. albacares, and two unidentified but distinct species of Hirudinella, herein referred to as Hirudinella sp. A (from both M. nigricans and M. martinicus) and Hirudinella sp. B from M. nigricans. Additionally, H. ahi, based tentatively on morphological identification, is reported from Thunnus thynnus (Linnaeus). This represents the first record of a hirudinellid from M. martinicus and the first record of H. ahi from T. thynnus. A phylogeny of some Hemiurata Skrjabin & Guschanskaja, 1954 using partial fragments of the 28S rDNA sequences is consistent with earlier phylogenies and the position of the Hirudinellidae Dollfus, 1932 is well-supported as a derived group most closely related to the Syncoeliidae Looss, 1899. C1 [Calhoun, Dana M.; Curran, Stephen S.; Pulis, Eric E.; Franks, James S.] Univ So Mississippi, Dept Coastal Sci, Ocean Springs, MS 39564 USA. [Provaznik, Jennifer M.] NOAA, Mississippi Labs, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr SEFSC, Pascagoula, MS 39567 USA. RP Calhoun, DM (reprint author), Univ So Mississippi, Dept Coastal Sci, 703 East Beach Dr, Ocean Springs, MS 39564 USA. EM dana.calhoun@colorado.edu OI Pulis, Eric/0000-0002-1695-7953 FU National Science Foundation [0529684]; RAPID [1055071]; USDC, NOAA [NA08NOS4730322]; Mississippi Department of Marine Resources [S-11-USM-GCRL, M10AF20151] FX We would like to thank Robin M. Overstreet for advice, and Lynnae C. Manuel, Jean Jovonvich Alvillar, and Janet Wright, for their assistance with DNA extractions (all from The University of Southern Mississippi, USM). We are also grateful to: Vasyl V. Tkach (University of North Dakota) for his great efforts in attempting to extract DNA from problematic worms; Kenneth Keene from the Southeast Fisheries Science Center Pelagic Observer Program in Miami, Florida, U.S.A. for facilitating collections; Bobby Carter, director of the Mississippi Gulf Coast Billfish Classic, and participating anglers; Bill Haffner, director of the Mobile Big Game Fishing Club, and participating anglers; Paul Grammer (USM), Sarah Ashworth (USM) and Michael Buchanan (Mississippi Department of Marine Resources) for facilitating collections. Two anonymous reviewers provided helpful suggestions for improving the manuscript. This material is based on work supported by the National Science Foundation under Grant No. 0529684, RAPID 1055071, as well as USDC, NOAA award no. NA08NOS4730322. The work was also supported by Mississippi Department of Marine Resources Sub-Grant S-11-USM-GCRL and USDI/MS DMR MSCIAP MS.R. 798 Award M10AF20151. NR 49 TC 8 Z9 9 U1 1 U2 6 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0165-5752 J9 SYST PARASITOL JI Syst. Parasitol. PD OCT PY 2013 VL 86 IS 2 BP 197 EP 208 DI 10.1007/s11230-013-9439-2 PG 12 WC Parasitology SC Parasitology GA 221FY UT WOS:000324644500008 PM 24048751 ER PT J AU Sheth, K Amis, T Gutierrez-Nolasco, S Sridhar, B Mulfinger, D AF Sheth, Kapil Amis, Thomas Gutierrez-Nolasco, Sebastian Sridhar, Banavar Mulfinger, Daniel TI Development of a Probabilistic Convective Weather Forecast Threshold Parameter for Flight-Routing Decisions SO WEATHER AND FORECASTING LA English DT Article DE Aircraft observations; Probability forecasts; models; distribution; Transportation meteorology AB This paper presents a method for determining a threshold value of probabilistic convective weather forecast data. By synchronizing air traffic data and an experimental probabilistic convective weather forecast product, it was observed that aircraft avoid areas of specific forecasted probability. Both intensity and echo top of the forecasted weather were synchronized with air traffic data to derive the probability threshold parameter. This value can be used by dispatchers for flight planning and by air traffic managers to reroute streams of aircraft around convective cells. The main contribution of this paper is to provide a method to compute the probability threshold parameters using a specific experimental probabilistic convective forecast product providing hourly guidance up to 6 h. Air traffic and weather data for a 4-month period during the summer of 2007 were used to compute the parameters for the continental United States. The results are shown for different altitudes, times of day, aircraft types, and airspace users. Threshold values for each of the 20 Air Route Traffic Control Centers were also computed. Additional details are presented for seven high-altitude sectors in the Fort Worth, Texas, center. For the analysis reported here, flight intent was not considered and no assessment of flight deviation was conducted since only aircraft tracks were used. C1 [Sheth, Kapil; Sridhar, Banavar; Mulfinger, Daniel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Amis, Thomas] Natl Weather Serv, Ft Worth, TX USA. [Gutierrez-Nolasco, Sebastian] Univ Calif Santa Cruz, Moffett Field, CA USA. RP Sheth, K (reprint author), NASA, Ames Res Ctr, MS 210-15, Moffett Field, CA 94035 USA. EM kapil.sheth@nasa.gov NR 29 TC 2 Z9 2 U1 0 U2 6 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0882-8156 J9 WEATHER FORECAST JI Weather Forecast. PD OCT PY 2013 VL 28 IS 5 BP 1175 EP 1187 DI 10.1175/WAF-D-12-00052.1 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 229MQ UT WOS:000325270500006 ER PT J AU Andersson, BG Piirola, V De Buizer, J Clemens, DP Uomoto, A Charcos-Llorens, M Geballe, TR Lazarian, A Hoang, T Vornanen, T AF Andersson, B-G Piirola, V. De Buizer, J. Clemens, D. P. Uomoto, A. Charcos-Llorens, M. Geballe, T. R. Lazarian, A. Hoang, T. Vornanen, T. TI EVIDENCE FOR H-2 FORMATION DRIVEN DUST GRAIN ALIGNMENT IN IC 63 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: individual objects (IC 63); ISM: magnetic fields; polarization ID POLARIZATION SURVEY GPIPS; INTERSTELLAR GRAINS; MOLECULAR-HYDROGEN; RADIATIVE TORQUES; INFRARED POLARIZATION; CHEMICAL-STRUCTURE; GALACTIC PLANE; POLARIMETRIC CALIBRATION; GAMMA CASSIOPEIAE; MAGNETIC-FIELD AB In the interstellar medium (ISM), molecular hydrogen is expected to form almost exclusively on the surfaces of dust grains. Due to that molecule's large formation energy (-4.5 eV), several dynamical effects are likely associated with the process, including the alignment of asymmetric dust grains with the ambient magnetic field. Such aligned dust grains are, in turn, believed to cause the broadband optical/infrared polarization observed in the ISM. Here, we present the first observational evidence for grain alignment driven by H-2 formation, by showing that the polarization of the light from stars behind the reflection nebula IC 63 appears to correlate with the intensity of H-2 fluorescence. While our results strongly suggest a role for "Purcell rockets" in grain alignment, additional observations are needed to conclusively confirm their role. By showing a direct connection between H-2 formation and a probe of the dust characteristics, these results also provide one of the first direct confirmations of the grain-surface formation of H-2. We compare our observations to ab initio modeling based on Radiative Torque Alignment (RAT) theory. C1 [Andersson, B-G; De Buizer, J.; Charcos-Llorens, M.] NASA, Ames Res Ctr, USRA, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Piirola, V.] Univ Turku, Finnish Ctr Astron ESO, FI-21500 Piikkio, Finland. [Clemens, D. P.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Uomoto, A.] Observ Carnegie Inst, Pasadena, CA 91101 USA. [Geballe, T. R.] Nothern Operat Ctr, Gemini Observ, Hilo, HI 96720 USA. [Lazarian, A.; Hoang, T.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Vornanen, T.] Univ Turku, Tuorla Observ, FI-21500 Piikkio, Finland. RP Andersson, BG (reprint author), NASA, Ames Res Ctr, USRA, SOFIA Sci Ctr, MS N211-3, Moffett Field, CA 94035 USA. EM bg@sofia.usra.edu FU NASA; NSF; W.M. Keck Foundation; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; NSF [AST-1109469, AST 06-07500, 09-07790]; Gemini Observatory FX This research was conducted also, in part, using the Mimir instrument, jointly developed at Boston University and Lowell Observatory and supported by NASA, NSF, and the W.M. Keck Foundation.; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England.; B-GA., M. C.-L., and A. L. acknowledge financial support from the NSF through grant AST-1109469. D. P. C. recognizes support from the NSF under AST 06-07500 and 09-07790. T.R.G.'s research is supported by the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., on behalf of the international Gemini partnership of Argentina, Australia, Brazil, Canada, Chile, the United Kingdom, and the United States of America. NR 98 TC 14 Z9 14 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2013 VL 775 IS 2 AR 84 DI 10.1088/0004-637X/775/2/84 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 222ME UT WOS:000324734400004 ER PT J AU Bodaghee, A Tomsick, JA Pottschmidt, K Rodriguez, J Wilms, J Pooley, GG AF Bodaghee, Arash Tomsick, John A. Pottschmidt, Katja Rodriguez, Jerome Wilms, Joern Pooley, Guy G. TI GAMMA-RAY OBSERVATIONS OF THE MICROQUASARS CYGNUS X-1, CYGNUS X-3, GRS 1915+105, AND GX 339-4 WITH THE FERMI LARGE AREA TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; gamma rays: stars; stars: neutron; X-rays: binaries; X-rays: individual (Cygnus X-3, Cygnus X-1, GRS 1915+105, GX 339-4) ID STOCHASTIC PARTICLE-ACCELERATION; GALACTIC BLACK-HOLES; X-RAY; ORBITAL MODULATION; RELATIVISTIC JET; RADIO-EMISSION; STELLAR WIND; ENERGY; BINARY; VARIABILITY AB Detecting gamma-rays from microquasars is a challenging but worthwhile endeavor for understanding particle acceleration and the jet mechanism and for constraining leptonic/hadronic emission models. We present results from a likelihood analysis on timescales of 1 day and 10 days of similar to 4 yr worth of gamma-ray observations (0.1-10 GeV) by Fermi-LAT of Cyg X-1, Cyg X-3, GRS 1915 + 105, and GX 339-4. Our analysis reproduced all but one of the previous gamma-ray outbursts of Cyg X-3 as reported with Fermi or AGILE, plus five new days on which Cyg X-3 is detected at a significance of similar to 5 sigma that are not reported in the literature. In addition, Cyg X-3 is significantly detected on 10 day timescales outside of known gamma-ray flaring epochs, which suggests that persistent gamma-ray emission from Cyg X-3 has been detected for the first time. For Cyg X-1 we find three low-significance excesses (similar to 3-4 sigma) on daily timescales that are contemporaneous with gamma-ray flares reported (also at low significance) by AGILE. Two other microquasars, GRS 1915+105 and GX 339-4, are not detected, and we derive 3 sigma upper limits of 2.3 x 10(-8) photons cm(-2) s(-1) and 1.6 x 10-8 photons cm(-2) s(-1), respectively, on the persistent flux in the 0.1-10 GeV range. These results enable us to define a list of the general conditions that are necessary for the detection of gamma-rays from microquasars. C1 [Bodaghee, Arash; Tomsick, John A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Pottschmidt, Katja] CRESST, Greenbelt, MD 20771 USA. [Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Pottschmidt, Katja] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Rodriguez, Jerome] Univ Paris Diderot, Lab AIM, CEA DSM IRFU SAp, CEA IRFU,CNRS INSU,Ctr Saclay, F-91191 Gif Sur Yvette, France. [Wilms, Joern] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, D-96049 Bamberg, Germany. [Pooley, Guy G.] Univ Cambridge, Mullard Radio Astron Observ, Cavendish Lab, Cambridge CB3 0HE, England. RP Bodaghee, A (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. EM bodaghee@ssl.berkeley.edu RI Wilms, Joern/C-8116-2013; OI Wilms, Joern/0000-0003-2065-5410; Rodriguez, Jerome/0000-0002-4151-4468 FU NASA [NNX10AP83G] FX The authors thank the anonymous referee, whose constructive criticism led to an improved manuscript. A. B. thanks Stephane Corbel, Robin H. D. Corbet, Victoria Grinberg, Michael McCullough, and Andrzej Zdziarski for useful discussions. A. B. and J.A.T. acknowledge partial support from NASA Fermi Guest Observer Award NNX10AP83G. 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, the SIMBAD database operated at CDS, Strasbourg, France, NASA's Astrophysics Data System Bibliographic Services, the Fermi Science Support Center, the Swift/BAT transient monitor results provided by the Swift/BAT team, and MAXI data provided by RIKEN, JAXA, and the MAXI team. NR 121 TC 17 Z9 17 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2013 VL 775 IS 2 AR 98 DI 10.1088/0004-637X/775/2/98 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 222ME UT WOS:000324734400018 ER PT J AU Line, MR Wolf, AS Zhang, X Knutson, H Kammer, JA Ellison, E Deroo, P Crisp, D Yung, YL AF Line, Michael R. Wolf, Aaron S. Zhang, Xi Knutson, Heather Kammer, Joshua A. Ellison, Elias Deroo, Pieter Crisp, Dave Yung, Yuk L. TI A SYSTEMATIC RETRIEVAL ANALYSIS OF SECONDARY ECLIPSE SPECTRA. I. A COMPARISON OF ATMOSPHERIC RETRIEVAL TECHNIQUES SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; methods: statistical; planets and satellites: atmospheres; radiative transfer ID HUBBLE-SPACE-TELESCOPE; MOLECULAR SPECTROSCOPIC DATABASE; COLLISION-INDUCED ABSORPTION; HD 209458B; TRANSMISSION SPECTROSCOPY; PLANETARY-ATMOSPHERES; THERMAL EMISSION; TEMPERATURE INVERSION; EXTRASOLAR PLANETS; DAYSIDE SPECTRUM AB Exoplanet atmosphere spectroscopy enables us to improve our understanding of exoplanets just as remote sensing in our own solar system has increased our understanding of the solar system bodies. The challenge is to quantitatively determine the range of temperatures and molecular abundances allowed by the data, which is often difficult given the low information content of most exoplanet spectra that commonly leads to degeneracies in the interpretation. A variety of spectral retrieval approaches have been applied to exoplanet spectra, but no previous investigations have sought to compare these approaches. We compare three different retrieval methods: optimal estimation, differential evolution Markov chain Monte Carlo, and bootstrap Monte Carlo on a synthetic water-dominated hot Jupiter. We discuss expectations of uncertainties in abundances and temperatures given current and potential future observations. In general, we find that the three approaches agree for high spectral resolution, high signal-to-noise data expected to come from potential future spaceborne missions, but disagree for low-resolution, low signal-to-noise spectra representative of current observations. We also compare the results from a parameterized temperature profile versus a full classical Level-by-Level approach and discriminate in which situations each of these approaches is applicable. Furthermore, we discuss the implications of our models for the inferred C-to-O ratios of exoplanetary atmospheres. Specifically, we show that in the observational limit of a few photometric points, the retrieved C/O is biased toward values near solar and near one simply due to the assumption of uninformative priors. C1 [Line, Michael R.; Wolf, Aaron S.; Zhang, Xi; Knutson, Heather; Kammer, Joshua A.; Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Ellison, Elias] Flintridge Preparatory Sch, La Canada Flintridge, CA 91011 USA. [Deroo, Pieter; Crisp, Dave] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Line, MR (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM mrl@gps.caltech.edu FU NAI Virtual Planetary Laboratory grant from the University of Washington; NASA [NNX09AB72G]; National Aeronautics and Space Administration FX We thank Jaimin Lee and Leigh Fletcher for their willingness to compare radiative transfer codes. We also thank John Johnson and Jonathan Fortney for useful conversations. We thank members of Yuk Yungs group for useful comments. This research was supported in part by an NAI Virtual Planetary Laboratory grant from the University of Washington to the Jet Propulsion Laboratory and California Institute of Technology. Part of the research described here was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Y.L.Y. was supported in part by NASA grant NNX09AB72G to the California Institute of Technology. NR 65 TC 49 Z9 49 U1 2 U2 20 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2013 VL 775 IS 2 AR 137 DI 10.1088/0004-637X/775/2/137 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 222ME UT WOS:000324734400057 ER PT J AU Walker, LM Butterfield, N Johnson, K Zucker, C Gallagher, S Konstantopoulos, I Zabludoff, A Hornschemeier, AE Tzanavaris, P Charlton, JC AF Walker, Lisa May Butterfield, Natalie Johnson, Kelsey Zucker, Catherine Gallagher, Sarah Konstantopoulos, Iraklis Zabludoff, Ann Hornschemeier, Ann E. Tzanavaris, Panayiotis Charlton, Jane C. TI THE OPTICAL GREEN VALLEY VERSUS MID-INFRARED CANYON IN COMPACT GROUPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: groups: general; galaxies: interactions; galaxies: photometry ID DIGITAL SKY SURVEY; COLOR-MAGNITUDE DIAGRAM; STAR-FORMATION; LUMINOSITY FUNCTION; NEARBY GALAXIES; DATA RELEASE; ULTRAVIOLET; ENVIRONMENT; EVOLUTION; EMISSION AB Compact groups of galaxies provide conditions similar to those experienced by galaxies in the earlier universe. Recent work on compact groups has led to the discovery of a dearth of mid-infrared transition galaxies (MIRTGs) in Infrared Array Camera (3.6-8.0 mu m) color space as well as at intermediate specific star formation rates. However, we find that in compact groups these MIRTGs have already transitioned to the optical ([g-r]) red sequence. We investigate the optical color-magnitude diagram (CMD) of 99 compact groups containing 348 galaxies and compare the optical CMD with mid-infrared (mid-IR) color space for compact group galaxies. Utilizing redshifts available from Sloan Digital Sky Survey, we identified new galaxy members for four groups. By combining optical and mid-IR data, we obtain information on both the dust and the stellar populations in compact group galaxies. We also compare with more isolated galaxies and galaxies in the Coma Cluster, which reveals that, similar to clusters, compact groups are dominated by optically red galaxies. While we find that compact group transition galaxies lie on the optical red sequence, LVL+SINGS mid-IR transition galaxies span the range of optical colors. The dearth of mid-IR transition galaxies in compact groups may be due to a lack of moderately star-forming low mass galaxies; the relative lack of these galaxies could be due to their relatively small gravitational potential wells. This makes them more susceptible to this dynamic environment, thus causing them to more easily lose gas or be accreted by larger members. C1 [Walker, Lisa May; Butterfield, Natalie; Johnson, Kelsey; Zucker, Catherine] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Gallagher, Sarah] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Konstantopoulos, Iraklis] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Zabludoff, Ann] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Zabludoff, Ann; Hornschemeier, Ann E.] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. [Charlton, Jane C.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Walker, LM (reprint author), Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. OI Konstantopoulos, Iraklis/0000-0003-2177-0146 FU Alfred P. Sloan Foundation; National Aeronautics and Space Administration; National Science Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; University of Chicago; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; University of Pittsburgh; Princeton University; United States Naval Observatory; University of Washington; Science and Industry Research Fund (Australia); NASA [ADAP-NNX10AD476, ADAP-NNX10AE88G]; David and Lucile Packard Foundation; NASA Postdoctoral Program Fellowship at NASA Goddard Space Flight Center; NASA FX Funding for the Sloan Digital Sky Survey (SDSS) has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the U.S. Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. The SDSS Web site is http://www.sdss.org/.; The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are The University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, University of Pittsburgh, Princeton University, the United States Naval Observatory, and the University of Washington.; We thank the referee for constructive comments that improved the paper. S. C. G. thanks the Natural Science and Engineering Research Council of Canada, and the Ontario Early Researcher Award Program. I. S. K. is the recipient of a John Stocker Research Fellowship from the Science and Industry Research Fund (Australia). A.I.Z. acknowledges support from NASA grants ADAP-NNX10AD476 and ADAP-NNX10AE88G. K.E.J. gratefully acknowledges support for this paper provided by the David and Lucile Packard Foundation through a Packard Fellowship. P. T. acknowledges support through a NASA Postdoctoral Program Fellowship at NASA Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 36 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 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2013 VL 775 IS 2 AR 129 DI 10.1088/0004-637X/775/2/129 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 222ME UT WOS:000324734400049 ER PT J AU Kishimoto, M Honig, SF Antonucci, R Millan-Gabet, R Barvainis, R Millour, F Kotani, T Tristram, KRW Weigelt, G AF Kishimoto, Makoto Hoenig, Sebastian F. Antonucci, Robert Millan-Gabet, Rafael Barvainis, Richard Millour, Florentin Kotani, Takayuki Tristram, Konrad R. W. Weigelt, Gerd TI EVIDENCE FOR A RECEDING DUST SUBLIMATION REGION AROUND A SUPERMASSIVE BLACK HOLE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: Seyfert; infrared: galaxies; techniques: interferometric ID ACTIVE GALACTIC NUCLEI; HOT DUST; NGC 4151; NGC-4151; VARIABILITY; SPECTRA; TORUS AB The near-IR emission in Type 1 active galactic nuclei (AGNs) is thought to be dominated by the thermal radiation from dust grains that are heated by the central engine in the UV/optical and are almost at the sublimation temperature. A brightening of the central source can thus further sublimate the innermost dust, leading to an increase in the radius of the near-IR emitting region. Such changes in radius have been indirectly probed by the measurements of the changes in the time lag between the near-IR and UV/optical light variation. Here we report direct evidence for such a receding sublimation region through the near-IR interferometry of the brightest Type 1 AGN in NGC 4151. The increase in radius follows a significant brightening of the central engine with a delay of at least a few years, which is thus the implied destruction timescale of the innermost dust distribution. Compiling historic flux variations and radius measurements, we also infer the reformation timescale for the inner dust distribution to be several years in this galactic nucleus. More specifically and quantitatively, we find that the radius at a given time seems to be correlated with a long-term average of the flux over the previous several (similar to 6) years, instead of the instantaneous flux. Finally, we also report measurements of three more Type 1 AGNs newly observed with the Keck interferometer, as well as the second epoch measurements for three other AGNs. C1 [Kishimoto, Makoto; Tristram, Konrad R. W.; Weigelt, Gerd] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Hoenig, Sebastian F.; Antonucci, Robert] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Hoenig, Sebastian F.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24118 Kiel, Germany. [Millan-Gabet, Rafael] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Barvainis, Richard] Natl Sci Fdn, Arlington, VA 22230 USA. [Millour, Florentin] Dept FIZEAU, Observ Cote d Azur, F-06304 Nice 4, France. [Kotani, Takayuki] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. RP Kishimoto, M (reprint author), Max Planck Inst Radioastron, Auf Hugel 69, D-53121 Bonn, Germany. EM mk@mpifr-bonn.mpg.de OI Tristram, Konrad/0000-0001-8281-5059; Hoenig, Sebastian/0000-0002-6353-1111 NR 12 TC 15 Z9 15 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2013 VL 775 IS 2 AR L36 DI 10.1088/2041-8205/775/2/L36 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 220ZP UT WOS:000324626700003 ER PT J AU Mayer, M Buehler, R Hays, E Cheung, CC Dutka, MS Grove, JE Kerr, M Ojha, R AF Mayer, M. Buehler, R. Hays, E. Cheung, C. C. Dutka, M. S. Grove, J. E. Kerr, M. Ojha, R. TI RAPID GAMMA-RAY FLUX VARIABILITY DURING THE 2013 MARCH CRAB NEBULA FLARE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma rays: stars; ISM: supernova remnants; pulsars: individual (Crab); radiation mechanisms: non-thermal ID PULSAR WIND NEBULAE; PARTICLE-ACCELERATION; MAGNETIC RECONNECTION; TERMINATION SHOCK; EMISSION; APRIL AB We report on a bright flare in the Crab Nebula detected by the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope. The period of significantly increased luminosity occurred in 2013 March and lasted for approximately two weeks. During this period, we observed flux variability on timescales of approximately 5 hr. The combined photon flux above 100 MeV from the pulsar and its nebula reached a peak value of (12.5 +/- 0.8) . 10(-6) cm(-2) s(-1) on 2013 March 6. This value exceeds the average flux by almost a factor of six and implies a similar to 20 times higher flux for the synchrotron component of the nebula alone. This is the second brightest flare observed from this source. Spectral and temporal analysis of the LAT data collected during the outburst reveal a rapidly varying synchrotron component of the Crab Nebula while the pulsar emission remains constant in time. C1 [Mayer, M.; Buehler, R.] Deutsch Elekt Synchrotron DESY, D-15738 Zeuthen, Germany. [Hays, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cheung, C. C.; Grove, J. E.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Dutka, M. S.; Ojha, R.] Catholic Univ Amer, Washington, DC 20064 USA. [Kerr, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Kerr, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Ojha, R.] ORAU NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Mayer, M (reprint author), Deutsch Elekt Synchrotron DESY, D-15738 Zeuthen, Germany. EM michael.mayer@desy.de; rolf.buehler@desy.de; elizabeth.a.hays@nasa.gov RI Hays, Elizabeth/D-3257-2012 FU NASA [NNH10ZDA001N, 41213]; NASA Postdoctoral Program at the Goddard Space Flight Center; NRL [NASADPRS-15633-Y]; Istituto Nazionale di Astrofisica in Italy; Centre National dEtudes Spatiales in France FX Elizabeth Hays and Rolf Buhler acknowledge generous support from the Fermi guest investigator program. This research was funded in part by NASA through Fermi Guest Investigator grant NNH10ZDA001N (proposal number 41213). 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. C.C.C. was supported at NRL by NASADPRS-15633-Y. The FermiLATCollaboration 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 dEtudes Spatiales in France. NR 29 TC 15 Z9 15 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2013 VL 775 IS 2 AR L37 DI 10.1088/2041-8205/775/2/L37 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 220ZP UT WOS:000324626700004 ER PT J AU Miller, JM Parker, ML Fuerst, F Bachetti, M Harrison, FA Barret, D Boggs, SE Chakrabarty, D Christensen, FE Craig, WW Fabian, AC Grefenstette, BW Hailey, CJ King, AL Stern, DK Tomsick, JA Walton, DJ Zhang, WW AF Miller, J. M. Parker, M. L. Fuerst, F. Bachetti, M. Harrison, F. A. Barret, D. Boggs, S. E. Chakrabarty, D. Christensen, F. E. Craig, W. W. Fabian, A. C. Grefenstette, B. W. Hailey, C. J. King, A. L. Stern, D. K. Tomsick, J. A. Walton, D. J. Zhang, W. W. TI NuSTAR SPECTROSCOPY OF GRS 1915+105: DISK REFLECTION, SPIN, AND CONNECTIONS TO JETS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; black hole physics; gravitation; relativistic processes; X-rays: binaries ID BLACK-HOLE SPIN; X-RAY BINARIES; ACCRETION DISK; GRS-1915+105; ENERGY; CONSTRAINTS; GRS1915+105; EXTRACTION; EMISSION; CORONAE AB We report on the results of spectral fits made to a NuSTAR observation of the black hole GRS 1915+105 in a "plateau" state. This state is of special interest because it is similar to the "low/hard" state seen in other black holes, especially in that compact, steady jets are launched in this phase. The 3-79 keV bandpass of NuSTAR, and its ability to obtain moderate-resolution spectra free from distortions such as photon pile-up, are extremely well suited to studies of disk reflection in X-ray binaries. In only 15 ks of net exposure, an extraordinarily sensitive spectrum of GRS 1915+105 was measured across the full bandpass. Ionized reflection from a disk around a rapidly spinning black hole is clearly required to fit the spectra; even hybrid Comptonization models including ionized reflection from a disk around a Schwarzschild black hole proved inadequate. A spin parameter of a = 0.98 +/- 0.01 (1 sigma statistical error) is measured via the best-fit model; low spins are ruled out at a high level of confidence. This result suggests that jets can be launched from a disk extending to the innermost stable circular orbit. A very steep inner disk emissivity profile is also measured, consistent with models of compact coronae above Kerr black holes. These results support an emerging association between the hard X-ray corona and the base of the relativistic jet. C1 [Miller, J. M.; King, A. L.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Parker, M. L.; Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. [Fuerst, F.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Bachetti, M.; Harrison, F. A.; Barret, D.; Grefenstette, B. W.] Univ Toulouse, UPS OMP, F-31400 Toulouse, France. [Bachetti, M.] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France. [Boggs, S. E.; Tomsick, J. A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Chakrabarty, D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Christensen, F. E.] Danish Tech Univ, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA USA. [Craig, W. W.; Hailey, C. J.] Columbia Univ, New York, NY 10027 USA. [Stern, D. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Miller, JM (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM jonmm@umich.edu RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337 FU NASA [NNG08FD60C] 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 NASA. J.M.M. thanks Sergei Trushkin for communicating radio results. NR 40 TC 39 Z9 39 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2013 VL 775 IS 2 AR L45 DI 10.1088/2041-8205/775/2/L45 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 220ZP UT WOS:000324626700012 ER PT J AU Moor, A Abraham, P Kospal, A Szabo, GM Apai, D Balog, Z Csengeri, T Grady, C Henning, T Juhasz, A Kiss, C Pascucci, I Szulagyi, J Vavrek, R AF Moor, A. Abraham, P. Kospal, A. Szabo, Gy. M. Apai, D. Balog, Z. Csengeri, T. Grady, C. Henning, Th. Juhasz, A. Kiss, Cs. Pascucci, I. Szulagyi, J. Vavrek, R. TI A RESOLVED DEBRIS DISK AROUND THE CANDIDATE PLANET-HOSTING STAR HD 95086 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; infrared: stars; stars: individual (HD 95086) ID MAIN-SEQUENCE STARS; CIRCLE-DOT STARS; SCORPIUS-CENTAURUS; HR 8799; HERSCHEL DATA; SPITZER MIPS; EVOLUTION; DUST; ASSOCIATION; PERFORMANCE AB Recently, a new planet candidate was discovered on direct images around the young (10-17 Myr) A-type star HD 95086. The strong infrared excess of the system indicates that, similar to HR8799, beta Pic, and Fomalhaut, the star harbors a circumstellar disk. Aiming to study the structure and gas content of the HD 95086 disk, and to investigate its possible interaction with the newly discovered planet, here we present new optical, infrared, and millimeter observations. We detected no CO emission, excluding the possibility of an evolved gaseous primordial disk. Simple blackbody modeling of the spectral energy distribution suggests the presence of two spatially separate dust belts at radial distances of 6 and 64 AU. Our resolved images obtained with the Herschel Space Observatory reveal a characteristic disk size of similar to 6 ''.0 x 5 ''.4 (540 x 490 AU) and disk inclination of similar to 25 degrees. Assuming the same inclination for the planet candidate's orbit, its reprojected radial distance from the star is 62 AU, very close to the blackbody radius of the outer cold dust ring. The structure of the planetary system at HD 95086 resembles the one around HR8799. Both systems harbor a warm inner dust belt and a broad colder outer disk and giant planet(s) between the two dusty regions. Modeling implies that the candidate planet can dynamically excite the motion of planetesimals even out to 270 AU via their secular perturbation if its orbital eccentricity is larger than about 0.4. Our analysis adds a new example to the three known systems where directly imaged planet(s) and debris disks coexist. C1 [Moor, A.; Abraham, P.; Szabo, Gy. M.; Kiss, Cs.] Hungarian Acad Sci, Konkoly Observ, Res Ctr Astron & Earth Sci, H-1525 Budapest, Hungary. [Kospal, A.] European Space Agcy ESA ESTEC SRE SA, NL-2200 AG Noordwijk, Netherlands. [Szabo, Gy. M.] ELTE Gothard Astrophys Observ, H-9700 Szombathely, Hungary. [Szabo, Gy. M.] Dept Expt Phys & Astron Observ, H-6720 Szeged, Hungary. [Apai, D.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Apai, D.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Balog, Z.; Henning, Th.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Csengeri, T.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Grady, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Grady, C.] Eureka Sci, Oakland, CA 94602 USA. [Juhasz, A.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands. [Szulagyi, J.] Univ Nice Sophia Antipolis, Observ Cote Azur, CNRS, UMR 7293, F-06108 Nice 2, France. [Vavrek, R.] ESA ESAC, Herschel Sci Ctr, Madrid 28691, Spain. RP Moor, A (reprint author), Hungarian Acad Sci, Konkoly Observ, Res Ctr Astron & Earth Sci, POB 67, H-1525 Budapest, Hungary. EM moor@konkoly.hu FU Hungarian OTKA [K101393, K104607]; European Space Agency (ESA) [PECS-98073]; Bolyai Research Fellowship of the Hungarian Academy of Sciences FX We thank our anonymous referee whose comments improved the manuscript. This project was supported by the Hungarian OTKA grants K101393 and K104607, the PECS-98073 program of the European Space Agency (ESA) and the Bolyai Research Fellowship of the Hungarian Academy of Sciences. NR 46 TC 16 Z9 16 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2013 VL 775 IS 2 AR L51 DI 10.1088/2041-8205/775/2/L51 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 220ZP UT WOS:000324626700018 ER PT J AU Lin, NH Tsay, SC Maring, HB Yen, MC Sheu, GR Wang, SH Chi, KH Chuang, MT Ou-Yang, CF Fu, JS Reid, JS Lee, CT Wang, LC Wang, JL Hsu, CN Sayer, AM Holben, BN Chu, YC Nguyen, XA Sopajaree, K Chen, SJ Cheng, MT Tsuang, BJ Tsai, CJ Peng, CM Schnell, RC Conway, T Chang, CT Lin, KS Tsai, YI Lee, WJ Chang, SC Liu, JJ Chiang, WL Huang, SJ Lin, TH Liu, GR AF Lin, Neng-Huei Tsay, Si-Chee Maring, Hal B. Yen, Ming-Cheng Sheu, Guey-Rong Wang, Sheng-Hsiang Chi, Kai Hsien Chuang, Ming-Tung Ou-Yang, Chang-Feng Fu, Joshua S. Reid, Jeffrey S. Lee, Chung-Te Wang, Lin-Chi Wang, Jia-Lin Hsu, Christina N. Sayer, Andrew M. Holben, Brent N. Chu, Yu-Chi Nguyen, Xuan Anh Sopajaree, Khajornsak Chen, Shui-Jen Cheng, Man-Ting Tsuang, Ben-Jei Tsai, Chuen-Jinn Peng, Chi-Ming Schnell, Russell C. Conway, Tom Chang, Chang-Tang Lin, Kuen-Song Tsai, Ying I. Lee, Wen-Jhy Chang, Shuenn-Chin Liu, Jyh-Jian Chiang, Wei-Li Huang, Shih-Jen Lin, Tang-Huang Liu, Gin-Rong TI An overview of regional experiments on biomass burning aerosols and related pollutants in Southeast Asia: From BASE-ASIA and the Dongsha Experiment to 7-SEAS SO ATMOSPHERIC ENVIRONMENT LA English DT Editorial Material DE Biomass burning; Aerosol; Air toxics; Southeast Asia; 7-SEAS; BASE-ASIA; Dongsha Experiment ID LONG-RANGE TRANSPORT; TRACE-P EXPERIMENT; OPTICAL-PROPERTIES; AIR-QUALITY; CHINA SEA; CHEMICAL-COMPOSITION; ATMOSPHERIC MERCURY; MARITIME CONTINENT; PCDD/F EMISSIONS; RICE STRAW AB By modulating the Earth-atmosphere energy, hydrological and biogeochemical cycles, and affecting regional-to-global weather and climate, biomass burning is recognized as one of the major factors affecting the global carbon cycle. However, few comprehensive and wide-ranging experiments have been conducted to characterize biomass-burning pollutants in Southeast Asia (SEA) or assess their regional impact on meteorology, the hydrological cycle, the radiative budget, or climate change. Recently, BASE-ASIA (Biomass-burning Aerosols in South-East Asia: Smoke Impact Assessment) and the 7-SEAS (7-South-East Asian Studies)/Dongsha Experiment were conducted during the spring seasons of 2006 and 2010 in northern SEA, respectively, to characterize the chemical, physical, and radiative properties of biomass-burning emissions near the source regions, and assess their effects. This paper provides an overview of results from these two campaigns and related studies collected in this special issue, entitled "Observation, modeling and impact studies of biomass burning and pollution in the SE Asian Environment". This volume includes 28 papers, which provide a synopsis of the experiments, regional weather/climate, chemical characterization of biomass-burning aerosols and related pollutants in source and sink regions, the spatial distribution of air toxics (atmospheric mercury and dioxins) in source and remote areas, a characterization of aerosol physical, optical, and radiative properties, as well as modeling and impact studies. These studies, taken together, provide the first relatively complete dataset of aerosol chemistry and physical observations conducted in the source/sink region in the northern SEA, with particular emphasis on the marine boundary layer and lower free troposphere (LFT). The data, analysis and modeling included in these papers advance our present knowledge of source characterization of biomass-burning pollutants near the source regions as well as the physical and chemical processes along transport pathways. In addition, we raise key questions to be addressed by a coming deployment during springtime 2013 in northern SEA, named 7-SEAS/BASELInE (Biomass-burning Aerosols & Stratocumulus Environment: Lifecycles and Interactions Experiment). This campaign will include a synergistic approach for further exploring many key atmospheric processes (e.g., complex aerosol-cloud interactions) and impacts of biomass burning on the surface-atmosphere energy budgets during the lifecycles of biomass-burning emissions. (c) 2013 The Authors. Published by Elsevier Ltd. All rights reserved. C1 [Lin, Neng-Huei; Yen, Ming-Cheng; Sheu, Guey-Rong; Wang, Sheng-Hsiang] Natl Cent Univ, Dept Atmospher Sci, Chungli 32054, Taiwan. [Tsay, Si-Chee; Hsu, Christina N.; Sayer, Andrew M.; Holben, Brent N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Maring, Hal B.] NASA Headquarters, Washington, DC USA. [Wang, Sheng-Hsiang] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Chi, Kai Hsien] Natl Yang Ming Univ, Inst Environm & Occupat Hlth Sci, Taipei 112, Taiwan. [Chuang, Ming-Tung; Lee, Chung-Te] Natl Cent Univ, Grad Inst Environm Engn, Chungli 32054, Taiwan. [Ou-Yang, Chang-Feng; Wang, Jia-Lin] Natl Cent Univ, Dept Chem, Chungli 32054, Taiwan. [Fu, Joshua S.] Univ Tennessee, Dept Civil & Environm Engn, Knoxville, TN USA. [Fu, Joshua S.] UTK ORNL, Ctr Interdisciplinary Res & Grad Educ, Knoxville, TN USA. [Reid, Jeffrey S.] Naval Res Lab, Monterey, CA USA. [Wang, Lin-Chi] Cheng Shiu Univ, Dept Chem & Mat Engn, Kaohsiung, Taiwan. [Wang, Lin-Chi] Cheng Shiu Univ, Super Micro Mass Res & Technol Ctr, Kaohsiung, Taiwan. [Sayer, Andrew M.] Univ Space Res Assoc, Columbia, MD 90034 USA. [Chu, Yu-Chi; Chang, Shuenn-Chin; Liu, Jyh-Jian; Chiang, Wei-Li] Taiwan Environm Protect Adm, Taipei, Taiwan. [Nguyen, Xuan Anh] Vietnam Acad Sci & Technol, Inst Geophys, Hanoi, Vietnam. [Sopajaree, Khajornsak] Chiang Mai Univ, Dept Environm Engn, Chiang Mai 50000, Thailand. [Chen, Shui-Jen] Natl Pingtung Univ Sci & Technol, Dept Environm Engn & Sci, Nei Pu, Pingtung, Taiwan. [Cheng, Man-Ting; Tsuang, Ben-Jei] Natl Chung Hsing Univ, Dept Environm Engn, Taichung 40227, Taiwan. [Tsai, Chuen-Jinn] Nation Chiao Tung Univ, Inst Environm Engn, Hsinchu, Taiwan. [Peng, Chi-Ming] WeatherRisk Explore Inc, Taipei, Taiwan. [Schnell, Russell C.; Conway, Tom] NOAA, ESRL, Global Monitoring Div, Boulder, CO USA. [Chang, Chang-Tang] Natl Ilan Univ, Dept Environm Engn, Yilan, Taiwan. [Lin, Kuen-Song] Yuan Ze Univ, Dept Chem Engn & Mat Sci, Chungli, Taiwan. [Tsai, Ying I.] Chia Nan Univ Pharm & Sci, Dept Environm Resources Management, Tainan, Taiwan. [Tsai, Ying I.] Chia Nan Univ Pharm & Sci, Dept Environm Engn & Sci, Tainan, Taiwan. [Lee, Wen-Jhy] Natl Cheng Kung Univ, Dept Environm Engn, Tainan 70101, Taiwan. [Huang, Shih-Jen] Natl Taiwan Ocean Univ, Dept Marine Environm Informat, Keelung, Taiwan. [Lin, Tang-Huang; Liu, Gin-Rong] Natl Cent Univ, Ctr Space & Remote Sensing Res, Chungli 32054, Taiwan. RP Lin, NH (reprint author), Natl Cent Univ, Dept Atmospher Sci, Chungli 32054, Taiwan. EM nhlin@cc.ncu.edu.tw RI Sayer, Andrew/H-2314-2012; Reid, Jeffrey/B-7633-2014; Tsay, Si-Chee/J-1147-2014; Wang, Lin-Chi/A-1397-2012; Wang, Sheng-Hsiang/F-4532-2010; Ou-Yang, Chang-Feng/R-2271-2016 OI Sayer, Andrew/0000-0001-9149-1789; Reid, Jeffrey/0000-0002-5147-7955; Wang, Lin-Chi/0000-0002-5126-1046; Wang, Sheng-Hsiang/0000-0001-9675-3135; Ou-Yang, Chang-Feng/0000-0002-8477-3013 NR 128 TC 59 Z9 60 U1 7 U2 112 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 OCT PY 2013 VL 78 SI SI BP 1 EP 19 DI 10.1016/j.atmosenv.2013.04.066 PG 19 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 220RW UT WOS:000324605600001 ER PT J AU Tsay, SC Hsu, NC Lau, WKM Li, C Gabriel, PM Ji, Q Holben, BN Welton, EJ Nguyen, AX Janjai, S Lin, NH Reid, JS Boonjawat, J Howell, SG Huebert, BJ Fu, JS Hansen, RA Sayer, AM Gautam, R Wang, SH Goodloe, CS Miko, LR Shu, PK Loftus, AM Huang, J Kim, JY Jeong, MJ Pantina, P AF Tsay, Si-Chee Hsu, N. Christina Lau, William K. -M. Li, Can Gabriel, Philip M. Ji, Qiang Holben, Brent N. Welton, E. Judd Nguyen, Anh X. Janjai, Serm Lin, Neng-Huei Reid, Jeffrey S. Boonjawat, Jariya Howell, Steven G. Huebert, Barry J. Fu, Joshua S. Hansen, Richard A. Sayer, Andrew M. Gautam, Ritesh Wang, Sheng-Hsiang Goodloe, Colby S. Miko, Laddawan R. Shu, Peter K. Loftus, Adrian M. Huang, Jingfeng Kim, Jin Young Jeong, Myeong-Jae Pantina, Peter TI From BASE-ASIA toward 7-SEAS: A satellite-surface perspective of boreal spring biomass-burning aerosols and clouds in Southeast Asia SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Biomass-burning; Aerosol; Cloud; Southeast Asia; BASE-ASIA; 7-SEAS ID ATMOSPHERIC BROWN CLOUDS; OPTICAL-PROPERTIES; HYDROLOGICAL CYCLE; FIRE EMISSIONS; SMOKE AEROSOLS; PART II; IMPACT; CLIMATE; PRECIPITATION; MICROPHYSICS AB In this paper, we present recent field studies conducted by NASA's SMART-COMMIT (and ACHIEVE, to be operated in 2013) mobile laboratories, jointly with distributed ground-based networks (e.g., AERONET, http://aeronet.gsfc.nasa.gov/ and MPLNET, http://mplnet.gsfc.nasa.gov/) and other contributing instruments over northern Southeast Asia. These three mobile laboratories, collectively called SMARTLabs (cf. http://smartlabs.gsfc.nasa.gov/, Surface-based Mobile Atmospheric Research & Testbed Laboratories) comprise a suite of surface remote sensing and in-situ instruments that are pivotal in providing high spectral and temporal measurements, complementing the collocated spatial observations from various Earth Observing System (EOS) satellites. A satellite-surface perspective and scientific findings, drawn from the BASE-ASIA (2006) field deployment as well as a series of ongoing 7-SEAS (2010-13) field activities over northern Southeast Asia are summarized, concerning (i) regional properties of aerosols from satellite and in-situ measurements, (ii) cloud properties from remote sensing and surface observations, (iii) vertical distribution of aerosols and clouds, and (iv) regional aerosol radiative effects and impact assessment. The aerosol burden over Southeast Asia in boreal spring, attributed to biomass burning, exhibits highly consistent spatial and temporal distribution patterns, with major variability arising from changes in the magnitude of the aerosol loading mediated by processes ranging from large-scale climate factors to diurnal meteorological events. Downwind from the source regions, the tightly coupled-aerosol cloud system provides a unique, natural laboratory for further exploring the micro- and macro-scale relationships of the complex interactions. The climatic significance is presented through large-scale anti-correlations between aerosol and precipitation anomalies, showing spatial and seasonal variability, but their precise cause-and-effect relationships remain an open-ended question. To facilitate an improved understanding of the regional aerosol radiative effects, which continue to be one of the largest uncertainties in climate forcing, a joint international effort is required and anticipated to commence in springtime 2013 in northern Southeast Asia. Published by Elsevier Ltd. C1 [Tsay, Si-Chee; Hsu, N. Christina; Lau, William K. -M.; Li, Can; Ji, Qiang; Holben, Brent N.; Welton, E. Judd; Hansen, Richard A.; Sayer, Andrew M.; Gautam, Ritesh; Goodloe, Colby S.; Miko, Laddawan R.; Shu, Peter K.; Pantina, Peter] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Li, Can; Ji, Qiang; Hansen, Richard A.; Huang, Jingfeng] Univ Maryland, College Pk, MD 20742 USA. [Gabriel, Philip M.] Colorado State Univ, Ft Collins, CO 80523 USA. [Nguyen, Anh X.] Vietnam Acad Sci & Technol, Hanoi, Vietnam. [Janjai, Serm] Silpakom Univ, Fac Sci, Dept Phys, Nakhon Pathom, Thailand. [Lin, Neng-Huei; Wang, Sheng-Hsiang] Natl Cent Univ, Hsinchu 300, Taiwan. [Reid, Jeffrey S.] Naval Res Lab, Monterey, CA USA. [Boonjawat, Jariya] Chulalongkorn Univ, Bangkok 10330, Thailand. [Howell, Steven G.; Huebert, Barry J.] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Fu, Joshua S.] Univ Tennessee, Knoxville, TN USA. [Sayer, Andrew M.; Gautam, Ritesh] Univ Space Res Assoc, Columbia, MD 90034 USA. [Loftus, Adrian M.] NASA, Goddard Space Flight Ctr, Postdoctoral Program, Greenbelt, MD 20771 USA. [Huang, Jingfeng] NOAA, NESDIS, Ctr Satellite Applicat & Res, College Pk, MD USA. [Kim, Jin Young] Korea Inst Sci & Technol, Seoul, South Korea. [Jeong, Myeong-Jae] Gangneung Wonju Natl Univ, Gaungneung, Gangwondo, South Korea. [Pantina, Peter] Sci Syst & Applications Inc, Lanham, MD USA. RP Tsay, SC (reprint author), NASA, Goddard Space Flight Ctr, Code 613, Greenbelt, MD 20771 USA. EM si-chee.tsay@nasa.gov RI Gautam, Ritesh/E-9776-2010; Sayer, Andrew/H-2314-2012; Reid, Jeffrey/B-7633-2014; Li, Can/F-6867-2011; Huang, Jingfeng/D-7336-2012; Loftus, Adrian/J-1148-2014; Tsay, Si-Chee/J-1147-2014; Lau, William /E-1510-2012; Wang, Sheng-Hsiang/F-4532-2010 OI Gautam, Ritesh/0000-0002-2177-9346; Sayer, Andrew/0000-0001-9149-1789; Reid, Jeffrey/0000-0002-5147-7955; Huang, Jingfeng/0000-0002-8779-2922; Lau, William /0000-0002-3587-3691; Wang, Sheng-Hsiang/0000-0001-9675-3135 FU NASA Interdisciplinary Studies (IDS) project, "Effects of biomass burning on Asian Monsoon water cycle and climate" FX The lead author thanks the continuous support of SMARTLabs deployments in Southeast Asia, as part of NASA Radiation Sciences Program managed by Dr. Hal B. Maring. Deployment of 7-SEAS/Son La IOP and data analysis are funded by NASA Interdisciplinary Studies (IDS) project, "Effects of biomass burning on Asian Monsoon water cycle and climate." We thank the NASA/EOS science teams of TOMS/OMI/SeaWiFS/MODIS/CALIPSO and AERONET/MPLNET for providing satellite and network data, respectively. The authors also gratefully acknowledge the team efforts led by J. Boonjawat (Southeast Asia START Regional Center at Chulalongkorn University, Thailand) and K. Bhuranapanon (Head of Phimai observatory and radar station, Bureau of Royal Rainmaking and Agricultural Aviation, Thailand) for supporting BASE-ASIA deployment, and by Anh X. Nguyen (Institute of Geophysics at Vietnam Academy of Science and Technology, Vietnam), S. Janjai (Department of Physics at Silpakorn University, Thailand), and N.-H. Lin (Department of Atmospheric Sciences at National Central University, Taiwan) in supporting 7-SEAS IOPs (2010-2012) over northern Southeast Asia. NR 84 TC 25 Z9 26 U1 1 U2 26 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD OCT PY 2013 VL 78 SI SI BP 20 EP 34 DI 10.1016/j.atmosenv.2012.12.013 PG 15 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 220RW UT WOS:000324605600002 ER PT J AU Gautam, R Hsu, NC Eck, TF Holben, BN Janjai, S Jantarach, T Tsay, SC Lau, WK AF Gautam, Ritesh Hsu, N. Christina Eck, Thomas F. Holben, Brent N. Janjai, Serm Jantarach, Treenuch Tsay, Si-Chee Lau, William K. TI Characterization of aerosols over the Indochina peninsula from satellite-surface observations during biomass burning pre-monsoon season SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Aerosol; Remote sensing; Southeast Asia; Biomass burning ID ENERGY SYSTEM CERES; DIURNAL VARIABILITY; HYDROLOGICAL CYCLE; TIBETAN PLATEAU; OPTICAL DEPTH; CLOUDS; ASIA; INSTRUMENT; ATMOSPHERE; THAILAND AB This paper presents characterization of aerosols over the Indochina peninsular regions of Southeast Asia during pre-monsoon season from satellite and ground-based radiometric observations. Our analysis focuses on the seasonal peak period in aerosol loading and biomass burning, prior to the onset of the Asian summer monsoon, as observed in the inter-annual variations of Aerosol Optical Depth (AOD) and fire count data from MODIS. Multi-year (2007-2011) analysis of spaceborne lidar measurements, from CALIOP, indicates presence of aerosols mostly within boundary layer, however extending to elevated altitudes to 4 km over northern regions of Indochina, encompassing Myanmar, northern Thailand and southern China. In addition, a strong gradient in aerosol loading and vertical distribution is observed from the relatively clean equatorial conditions to heavy smoke-laden northern regions (greater aerosol extinction and smaller depolarization ratio). Based on column-integrated ground-based measurements from four AERONET locations distributed over Thailand, the regional aerosol loading is found to be significantly absorbing with spectral single scattering albedo (SSA) below 0.91 +/- 0.02 in the 440-1020 nm range, with lowest seasonal mean SSA (most absorbing aerosol) over the northern location of Chiang Mai (SSA similar to 0.85) during pre-monsoon season. The smoke-laden aerosol loading is found to exhibit a significant diurnal pattern with higher AOD departures during early morning observations relative to late afternoon conditions (peak difference of more than 15% amplitude). Finally, satellite-based aerosol radiative impact is assessed using CERES shortwave Top-of-Atmosphere flux, in conjunction with MODIS AOD. Overall, a consistency in the aerosol-induced solar absorption characteristic is found among selected regions from ground-based sunphotometer-derived spectral SSA retrievals and satellite-based radiative forcing analysis. (c) 2012 Elsevier Ltd. All rights reserved. C1 [Gautam, Ritesh; Eck, Thomas F.] Univ Space Res Assoc, GESTAR, Columbia, MD 21044 USA. [Gautam, Ritesh; Hsu, N. Christina; Eck, Thomas F.; Holben, Brent N.; Tsay, Si-Chee; Lau, William K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Janjai, Serm; Jantarach, Treenuch] Silpakorn Univ, Nakhon Pathom 73000, Thailand. RP Gautam, R (reprint author), Univ Space Res Assoc, GESTAR, Columbia, MD 21044 USA. EM ritesh.gautam@nasa.gov RI Gautam, Ritesh/E-9776-2010; Tsay, Si-Chee/J-1147-2014 OI Gautam, Ritesh/0000-0002-2177-9346; FU NASA Radiation Sciences Program FX This work is supported by grant from the NASA Radiation Sciences Program, managed by Hal B. Maring. We thank the various science teams for provision of satellite data namely, CALIPSO, CERES and MODIS. The authors also gratefully acknowledge the efforts made by the AERONET team and site managers, including Jariya Boonjawat (Phimai) and Surasak Meesiri (Mukdahan), in maintaining the sites and making the data available online. We also thank Jingfeng Huang, Can Li, Zhaoyan Liu, Falguni Patadia for helpful discussions during preparation of the manuscript. Two anonymous reviewers are thanked for providing useful comments that helped improve an earlier version of the manuscript. NR 32 TC 30 Z9 30 U1 4 U2 28 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 OCT PY 2013 VL 78 SI SI BP 51 EP 59 DI 10.1016/j.atmosenv.2012.05.038 PG 9 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 220RW UT WOS:000324605600004 ER PT J AU Li, C Tsay, SC Hsu, NC Kim, JY Howell, SG Huebert, BJ Ji, Q Jeong, MJ Wang, SH Hansell, RA Bell, SW AF Li, Can Tsay, Si-Chee Hsu, N. Christina Kim, Jin Young Howell, Steven G. Huebert, Barry J. Ji, Qiang Jeong, Myeong-Jae Wang, Sheng-Hsiang Hansell, Richard A. Bell, Shaun W. TI Characteristics and composition of atmospheric aerosols in Phimai, central Thailand during BASE-ASIA SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Southeast Asia; Aerosols; Chemical composition; Microphysical properties; Optical properties ID SOUTHEAST-ASIA; AIR-QUALITY; RADIATIVE PROPERTIES; SIZE DISTRIBUTIONS; TROPOSPHERIC OZONE; NORTHERN VIETNAM; ELEMENTAL CARBON; ACE-ASIA; CHINA; PARTICLES AB Comprehensive measurements of atmospheric aerosols were made in Phimai, central Thailand (15.183 degrees N, 102.565 degrees E, elevation: 206 m) during the BASE-ASIA field experiment from late February to early May in 2006. The observed aerosol loading was sizable for this rural site (mean aerosol scattering: 108 +/- 64 Mm(-1); absorption: 15 +/- 8 Mm(-1); PM10 concentration: 33 +/- 17 mu g m(-3)), and dominated by submicron particles. Major aerosol compounds included carbonaceous (OC: 9.5 +/- 3.6 mu g m(-3); EC: 2.0 +/- 2.3 mu g m(-3)) and secondary species (SO42-: 6.4 +/- 3.7 mu g m(-3), NH4+: 2.2 +/- 1.3 mu g m(-3)). While the site was seldom under the direct influence of large forest fires to its north, agricultural fires were ubiquitous during the experiment, as suggested by the substantial concentration of K+ (0.56 +/- 0.33 mu g m(-3)). Besides biomass burning, aerosols in Phimai during the experiment were also strongly influenced by industrial and vehicular emissions from the Bangkok metropolitan region and long-range transport from southern China. High humidity played an important role in determining the aerosol composition and properties in the region. Sulfate was primarily formed via aqueous phase reactions, and hygroscopic growth could enhance the aerosol light scattering by up to 60%, at the typical morning RH level of 85%. The aerosol single scattering albedo demonstrated distinct diurnal variation, ranging from 0.86 +/- 0.04 in the evening to 0.92 +/- 0.02 in the morning. This experiment marks the first time such comprehensive characterization of aerosols was made for rural central Thailand. Our results indicate that aerosol pollution has developed into a regional problem for northern Indochina, and may become more severe as the region's population and economy continue to grow. (c) 2012 Elsevier Ltd. All rights reserved. C1 [Li, Can; Ji, Qiang; Hansell, Richard A.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Li, Can; Tsay, Si-Chee; Hsu, N. Christina; Kim, Jin Young; Ji, Qiang; Jeong, Myeong-Jae; Wang, Sheng-Hsiang; Hansell, Richard A.; Bell, Shaun W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kim, Jin Young] Korea Inst Sci & Technol, Natl Agenda Res Div, Seoul, South Korea. [Howell, Steven G.; Huebert, Barry J.] Univ Hawaii Manoa, Dept Oceanog, Honolulu, HI 96822 USA. [Jeong, Myeong-Jae] Gangneung Wonju Natl Univ, Dept Atmospher & Environm Sci, Kangnung 210702, Gangwon Do, South Korea. [Wang, Sheng-Hsiang] Natl Cent Univ, Dept Atmospher Sci, Jhongli, Taiwan. [Wang, Sheng-Hsiang] Oak Ridge Associated Univ, Oak Ridge, TN USA. [Bell, Shaun W.] Sci Syst & Applications Inc, Lanham, MD USA. RP Li, C (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 613-0, Greenbelt, MD 20771 USA. EM can.li@nasa.gov RI Li, Can/F-6867-2011; Tsay, Si-Chee/J-1147-2014; Hansell, Richard/J-2065-2014; Wang, Sheng-Hsiang/F-4532-2010 OI Wang, Sheng-Hsiang/0000-0001-9675-3135 FU NASA Radiation Sciences Program [NNG04GC59G]; Korea Institute of Science and Technology FX The BASE-ASIA project was supported by the NASA Radiation Sciences Program managed by Dr. Hal Maring. The UH group would like to acknowledge our funding agency (NASA Radiation Sciences Program, #NNG04GC59G). J.Y. Kim was supported by Korea Institute of Science and Technology. We also thank Jariya Boonjarwat, and the exceedingly helpful and generous staff of the Phimai facility. NR 54 TC 14 Z9 14 U1 0 U2 41 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 J9 ATMOS ENVIRON JI Atmos. Environ. PD OCT PY 2013 VL 78 SI SI BP 60 EP 71 DI 10.1016/j.atmosenv.2012.04.003 PG 12 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 220RW UT WOS:000324605600005 ER PT J AU Wang, SH Tsay, SC Lin, NH Chang, SC Li, C Welton, EJ Holben, BN Hsu, NC Lau, WKM Lolli, S Kuo, CC Chia, HP Chiu, CY Lin, CC Bell, SW Ji, Q Hansell, RA Sheu, GR Chi, KH Peng, CM AF Wang, Sheng-Hsiang Tsay, Si-Chee Lin, Neng-Huei Chang, Shuenn-Chin Li, Can Welton, Ellsworth J. Holben, Brent N. Hsu, N. Christina Lau, William K. M. Lolli, Simone Kuo, Chun-Chiang Chia, Hao-Ping Chiu, Chia-Yang Lin, Chia-Ching Bell, Shaun W. Ji, Qiang Hansell, Richard A. Sheu, Guey-Rong Chi, Kai-Hsien Peng, Chi-Ming TI Origin, transport, and vertical distribution of atmospheric pollutants over the northern South China Sea during the 7-SEAS/Dongsha Experiment SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Aerosols; Optical properties; Back trajectory; UV lidar; Biomass burning ID CHEMICAL-COMPOSITION; OPTICAL-PROPERTIES; RAMAN LIDAR; AEROSOL; DUST; POLLUTION; OUTFLOW; JAPAN; SMOKE; ASIA AB During the spring of 2010, comprehensive in situ measurements were made for the first time on a small atoll (Dongsha Island) in the northern South China Sea (SCS), a key region of the 7-SEAS (the Seven South East Asian Studies) program. This paper focuses on characterizing the source origins, transport processes, and vertical distributions of the Asian continental outflows over the region, using measurements including mass concentration, optical properties, hygroscopicity, and vertical distribution of the aerosol particles, as well as the trace gas composition. Cluster analysis of backward trajectories classified 52% of the air masses arriving at ground level of Dongsha Island as having a continental origin, mainly from northern China to the northern SCS, passing the coastal area and being confined in the marine boundary layer (0-0.5 km). Compared to aerosols of oceanic origin, the fine mode continental aerosols have a higher concentration, extinction coefficient, and single-scattering albedo at 550 nm (i.e., 19 vs. 14 mu g m(-3) in PM2.5; 77 vs. 59 Mm(-1) in beta(e); and 0.94 vs. 0.90 in omega, respectively). These aerosols have a higher hygroscopicity (f at 85% RH = 2.1) than those in the upwind inland regions, suggesting that the aerosols transported to the northern SCS were modified by the marine environment. In addition to the near-surface aerosol transport, a significant upper-layer (3-4 km) transport of biomass-burning aerosols was observed. Our results suggest that emissions from both China and Southeast Asia could have a significant impact on the aerosol loading and other aerosol properties over the SCS. Furthermore, the complex vertical distribution of aerosols-coinciding-with-clouds has implications for remote-sensing observations and aerosol-cloud-radiation interactions. (c) 2012 Elsevier Ltd. All rights reserved. C1 [Wang, Sheng-Hsiang; Lin, Neng-Huei; Chiu, Chia-Yang; Lin, Chia-Ching; Sheu, Guey-Rong; Peng, Chi-Ming] Natl Cent Univ, Dept Atmospher Sci, Chungli 32001, Taiwan. [Wang, Sheng-Hsiang; Tsay, Si-Chee; Li, Can; Welton, Ellsworth J.; Holben, Brent N.; Hsu, N. Christina; Lau, William K. M.; Lolli, Simone; Bell, Shaun W.; Ji, Qiang; Hansell, Richard A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Chang, Shuenn-Chin] Taiwan EPA, Taipei, Taiwan. [Li, Can; Ji, Qiang; Hansell, Richard A.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Lolli, Simone] Univ Maryland Baltimore Cty, JCET, Baltimore, MD 21228 USA. [Kuo, Chun-Chiang; Chia, Hao-Ping; Peng, Chi-Ming] Weatherrisk Inc, Taipei, Taiwan. [Bell, Shaun W.] Sci Syst & Applicat Inc, Lanham, MD USA. [Chi, Kai-Hsien] Natl Yang Ming Univ, Inst Environm & Occupat Hlth Sci, Taipei 112, Taiwan. RP Wang, SH (reprint author), Natl Cent Univ, Dept Atmospher Sci, Chungli 32001, Taiwan. EM shenghsiang.wang@gmail.com RI Li, Can/F-6867-2011; Tsay, Si-Chee/J-1147-2014; Hansell, Richard/J-2065-2014; Lau, William /E-1510-2012; Wang, Sheng-Hsiang/F-4532-2010 OI Lau, William /0000-0002-3587-3691; Wang, Sheng-Hsiang/0000-0001-9675-3135 FU National Science Council of Taiwan [99-2111-M-008-011, 100-2111-M-008-011, 101-2111-M-008-003]; Taiwan Environmental Protection Administration [EPA-99-FA11-03-A097, EPA-100-U1L1-02-101]; NASA Radiation Sciences Program FX This work was supported by the National Science Council of Taiwan under grants No. 99-2111-M-008-011, 100-2111-M-008-011, 101-2111-M-008-003, and by the Taiwan Environmental Protection Administration under contracts No. EPA-99-FA11-03-A097, EPA-100-U1L1-02-101 and also by the NASA Radiation Sciences Program managed by Dr. Hal Maring. The authors thank two anonymous reviewers for their useful comments and suggestions. NR 42 TC 11 Z9 12 U1 1 U2 49 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 OCT PY 2013 VL 78 SI SI BP 124 EP 133 DI 10.1016/j.atmosenv.2012.11.013 PG 10 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 220RW UT WOS:000324605600011 ER PT J AU Ou-Yang, CF Hsieh, HC Wang, SH Lin, NH Lee, CT Sheu, GR Wang, JL AF Ou-Yang, Chang-Feng Hsieh, Hsin-Cheng Wang, Sheng-Hsiang Lin, Neng-Huei Lee, Chung-Te Sheu, Guey-Rong Wang, Jia-Lin TI Influence of Asian continental outflow on the regional background ozone level in northern South China Sea SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Ozone; Continental outflow; 7SEAS; South China Sea ID LONG-RANGE TRANSPORT; SURFACE OZONE; AIR-QUALITY; ACID DEPOSITION; CARBON-MONOXIDE; HONG-KONG; TAIWAN; PACIFIC; DUST; POLLUTANTS AB Asian continental outflow is known to have very pronounced seasonality, which in turn can alter the trace gas contents of the Northern Hemisphere. In this study, field measurements were conducted during the spring of 2010, Dongsha, a small island situated between Taiwan and the Philippines, served as a remote site for monitoring surface ozone. Ozone was used as an effective indicator to distinguish between continental and marine air masses. Our measurements suggested that strong northeasterly winds arising from the winter Asian monsoon may have transported polluted air masses from the northern continent to locations as far south as Dongsha (latitude 20.70 degrees N), as indicated by elevated ozone levels of approximately 60 ppbv. In contrast, during periodic calm periods when the monsoon subsided low ozone levels of about 30 ppb were detected, which is typical for marine air masses. This outflow of polluted air masses from the Asian continent and Taiwan facilitated by the winter monsoon was also successfully simulated using the Pennsylvania State University/National Center for Atmospheric Research Mesoscale Model, version 5 (PSU/NCAR MM5) and the Taiwan Air Quality Model (TAQM). (c) 2012 Elsevier Ltd. All rights reserved. C1 [Ou-Yang, Chang-Feng; Hsieh, Hsin-Cheng; Wang, Jia-Lin] Natl Cent Univ, Dept Chem, Chungli 320, Taiwan. [Ou-Yang, Chang-Feng; Wang, Sheng-Hsiang; Lin, Neng-Huei; Sheu, Guey-Rong] Natl Cent Univ, Dept Atmospher Sci, Chungli 320, Taiwan. [Wang, Sheng-Hsiang] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Wang, Sheng-Hsiang] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lee, Chung-Te] Natl Cent Univ, Grad Inst Environm Engn, Chungli 320, Taiwan. RP Wang, JL (reprint author), Natl Cent Univ, Dept Chem, Chungli 320, Taiwan. EM cwang@cc.ncu.edu.tw RI Wang, Sheng-Hsiang/F-4532-2010; Ou-Yang, Chang-Feng/R-2271-2016 OI Wang, Sheng-Hsiang/0000-0001-9675-3135; Ou-Yang, Chang-Feng/0000-0002-8477-3013 FU Taiwan Environmental Protection Administration [EPA-98-U1L1-02-101, EPA-99-U1L1-02-101]; Taiwan National Science Council [NSC 98-2745-M-008-001-, NSC 99-2745-M-008-001-, NSC 98-2111-M-008-021-, NSC 99-2111-M-008-015-] FX This work was financially supported by the Taiwan Environmental Protection Administration under contracts: EPA-98-U1L1-02-101 and EPA-99-U1L1-02-101, and by Taiwan National Science Council under contracts: NSC 98-2745-M-008-001-, NSC 99-2745-M-008-001-, NSC 98-2111-M-008-021-, and NSC 99-2111-M-008-015-. The authors gratefully acknowledge the NOAA Air Resources Laboratory (ARL) for the provision of the HYSPLIT transport and dispersion model and/or READY website (http://www.arl.noaa.gov/ready.html) used in this publication. We also acknowledge the courtesy of the U.S. Geological Survey (USGS) for the provision of the Global Data Explorer used in this research. NR 36 TC 8 Z9 8 U1 0 U2 27 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 OCT PY 2013 VL 78 SI SI BP 144 EP 153 DI 10.1016/j.atmosenv.2012.07.040 PG 10 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 220RW UT WOS:000324605600013 ER PT J AU Bell, SW Hansell, RA Chow, JC Tsay, SC Hsu, NC Lin, NH Wang, SH Ji, Q Li, C Watson, JG Khlystov, A AF Bell, Shaun W. Hansell, Richard A. Chow, Judith C. Tsay, Si-Chee Hsu, N. Christina Lin, Neng-Huei Wang, Sheng-Hsiang Ji, Qiang Li, Can Watson, John G. Khlystov, Andrey TI Constraining aerosol optical models using ground-based, collocated particle size and mass measurements in variable air mass regimes during the 7-SEAS/Dongsha experiment SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Aerosols; Scattering; Absorption ID COMPLEX REFRACTIVE-INDEX; CHEMICAL-COMPOSITION; MINERAL-DUST; CLOSURE; DENSITY; CARBON; CALIBRATION; MOBILITY AB During the spring of 2010, NASA Goddard's COMMIT ground-based mobile laboratory was stationed on Dongsha Island off the southwest coast of Taiwan, in preparation for the upcoming 2012 7-SEAS field campaign. The measurement period offered a unique opportunity for conducting detailed investigations of the optical properties of aerosols associated with different air mass regimes including background maritime and those contaminated by anthropogenic air pollution and mineral dust. What appears to be the first time for this region, a shortwave optical closure experiment (lambda = 550 nm) for both scattering and absorption was attempted over a 12-day period during which aerosols exhibited the most change. Constraints to the optical model included combined SMPS and APS number concentration data for a continuum of fine and coarse-mode particle sizes up to PM2.5. We also take advantage of an IMPROVE chemical sampler to help constrain aerosol composition and mass partitioning of key elemental species including sea-salt, particulate organic matter, soil, non sea-salt sulfate, nitrate, and elemental carbon. Achieving full optical closure is hampered by limitations in accounting for the role of water vapor in the system, uncertainties in the instruments and the need for further knowledge in the source apportionment of the model's major chemical components. Nonetheless, our results demonstrate that the observed aerosol scattering and absorption for these diverse air masses are reasonably captured by the model, where peak aerosol events and transitions between key aerosols types are evident. Signatures of heavy polluted aerosol composed mostly of ammonium and non sea-salt sulfate mixed with some dust with transitions to background sea-salt conditions are apparent in the absorption data, which is particularly reassuring owing to the large variability in the imaginary component of the refractive indices. Consistency between the measured and modeled optical parameters serves as an important link for advancing remote sensing and climate research studies in dynamic aerosol-rich environments like Dongsha. (c) 2012 Elsevier Ltd. All rights reserved. C1 [Bell, Shaun W.] Sci Syst & Applicat Inc, Lanham, MD USA. [Bell, Shaun W.; Hansell, Richard A.; Tsay, Si-Chee; Hsu, N. Christina; Wang, Sheng-Hsiang; Ji, Qiang; Li, Can] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hansell, Richard A.; Wang, Sheng-Hsiang; Ji, Qiang; Li, Can] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Chow, Judith C.; Watson, John G.] Univ Nevada, Desert Res Inst, Div Atmospher Sci, Reno, NV 89506 USA. [Lin, Neng-Huei; Wang, Sheng-Hsiang] Natl Cent Univ, Dept Atmospher Sci, Jhongli, Taiwan. [Khlystov, Andrey] Duke Univ, Dept Civil & Environm Engn, Durham, NC 27706 USA. RP Hansell, RA (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. EM Richard.A.Hansell@nasa.gov RI Li, Can/F-6867-2011; Tsay, Si-Chee/J-1147-2014; Hansell, Richard/J-2065-2014; Khlystov, Andrey/C-6134-2009; Wang, Sheng-Hsiang/F-4532-2010 OI Khlystov, Andrey/0000-0001-9606-3919; Wang, Sheng-Hsiang/0000-0001-9675-3135 FU NASA Radiation Sciences Program FX This work was supported by the NASA Radiation Sciences Program managed by Dr. Hal B. Maring. We are grateful to Taiwan's Environmental Protection Administration for providing the necessary logistical support during the deployment of NASA's COMMIT laboratory at Dongsha. We would like to thank Dr. Chuck McDade of the University of California, Davis, for providing 50 IMPROVE cassettes, and Mr. Steve Kohl of DRI's Environmental Analysis Facility for coordinating field operation and conducting chemical analyses and data validation. Lastly, we express thanks to Dr. Mishchenko for making his Lorenz-Mie light scattering code available for public use and to the anonymous reviewers of this manuscript for their helpful and insightful comments. NR 52 TC 9 Z9 9 U1 0 U2 27 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 OCT PY 2013 VL 78 SI SI BP 163 EP 173 DI 10.1016/j.atmosenv.2012.06.057 PG 11 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 220RW UT WOS:000324605600015 ER PT J AU Yasunari, TJ Tan, Q Lau, KM Bonasoni, P Marinoni, A Laj, P Menegoz, M Takemura, T Chin, M AF Yasunari, Teppei J. Tan, Qian Lau, K. -M. Bonasoni, Paolo Marinoni, Angela Laj, Paolo Menegoz, Martin Takemura, Toshihiko Chin, Mian TI Estimated range of black carbon dry deposition and the related snow albedo reduction over Himalayan glaciers during dry pre-monsoon periods SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Biomass burning; Himalayas; Black carbon; Deposition; Snow melting ID AEROSOL OPTICAL-THICKNESS; SINGLE-SCATTERING ALBEDO; LIGHT-ABSORPTION; TIBETAN PLATEAU; MONSOON CLIMATE; SPECTRAL ALBEDO; MASS-BALANCE; MODEL; PARTICLES; PARAMETERIZATION AB One of the major factors attributed to the accelerated melting of Himalayan glaciers is the snow darkening effect of atmospheric black carbon (BC). The BC is the result of incomplete fossil fuel combustion from sources such as open biomass burning and wood burning cooking stoves. One of the key challenges in determining the darkening effect is the estimation uncertainty of BC deposition (BCD) rate on surface snow cover. Here we analyze the variation of BC dry deposition in seven different estimates based on different dry deposition methods which include different atmospheric forcings (observations and global model outputs) and different spatial resolutions. The seven simulations are used to estimate the uncertainty range of BC dry deposition over the southern Himalayas during pre-monsoon period (March-May) in 2006. Our results show BC dry deposition rates in a wide range of 270-4700 mu g m(-2) during the period. Two global models generate higher BC dry deposition rates due to modeled stronger surface wind and simplification of complicated sub-grid surface conditions in this region. Using ice surface roughness and observation-based meteorological data, we estimate a better range of BC dry deposition rate of 900-1300 mu g m(-2). Under dry and highly polluted conditions, aged snow and sulfate-coated BC are expected to possibly reduce visible albedo by 4.2-5.1%. Our results suggest that for estimating aerosol-induced snow darkening effects of Himalaya snowpacks using global and regional models, realistic physical representation of ice or snow surface roughness and surface wind speed are critical in reducing uncertainties on the estimate of BC deposition over snow surface. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Yasunari, Teppei J.; Tan, Qian; Lau, K. -M.; Chin, Mian] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Yasunari, Teppei J.; Tan, Qian] Univ Space Res Assoc, Goddard Earth Sci & Technol & Res, Columbia, MD USA. [Bonasoni, Paolo; Marinoni, Angela] CNR, Inst Atmospher Sci & Climate, I-40126 Bologna, Italy. [Bonasoni, Paolo] Ev K2 CNR Comm, Bergamo, Italy. [Laj, Paolo; Menegoz, Martin] Univ Grenoble 1, CNRS UMR5183, Lab Glaciol & Geophys Environm, F-38402 St Martin Dheres, France. [Takemura, Toshihiko] Kyushu Univ, Res Inst Appl Mech, Fukuoka 812, Japan. RP Yasunari, TJ (reprint author), Univ Space Res Assoc, Goddard Earth Sci & Technol & Res, Columbia, MD USA. EM teppei.j.yasunari@nasa.gov RI Takemura, Toshihiko/C-2822-2009; Chin, Mian/J-8354-2012; Kyushu, RIAM/F-4018-2015; Yasunari, Teppei/E-5374-2010; Bonasoni, Paolo/C-6338-2015; U-ID, Kyushu/C-5291-2016; Lau, William /E-1510-2012; OI Takemura, Toshihiko/0000-0002-2859-6067; Yasunari, Teppei/0000-0002-9896-9404; Bonasoni, Paolo/0000-0002-8812-5291; Lau, William /0000-0002-3587-3691; Menegoz, Martin/0000-0001-7098-9270 FU University of Maryland at Baltimore County (UMBC); University of Maryland at Baltimore County (NASA); University of Maryland at Baltimore County [NCC5-494]; NASA; [NNG11HP08] FX All the observed data in the atmosphere at NCO-P site were maintained by the framework of the Ev-K2-CNR "SHARE", UNEP "ABC" and PAPRIKA (ANR-EVK2CNR) projects. This research is conducted under the Joint Aerosol Monsoon Experiment (JAMEX). The first author was on a visiting fellowship to the Goddard Earth Science and Technology Center (GEST) at the University of Maryland at Baltimore County (UMBC, NASA Grant and Cooperative Agreement NCC5-494) and is currently on the fellowship to Goddard Earth Sciences Technology and Research (GESTAR), Universities Space Research Association (USRA, NASA Grant and Cooperative Agreement NNG11HP08). The MODIS data used in this paper were produced with the Giovanni online data system, developed and maintained by the NASA GES DISC. The authors gratefully acknowledge the NOAA Air Resources Laboratory (ARL) for the provision of the HYSPLIT transport and dispersion model and/or READY website (http://www.arl.noaa.gov/ready.php) used in this publication. We really appreciate Jan Angevine, at NASA Goddard Space Flight Center, for proofreading our paper. NR 51 TC 15 Z9 15 U1 4 U2 61 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 OCT PY 2013 VL 78 SI SI BP 259 EP 267 DI 10.1016/j.atmosenv.2012.03.031 PG 9 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 220RW UT WOS:000324605600025 ER PT J AU Huang, K Fu, JS Hsu, NC Gao, Y Dong, XY Tsay, SC Lam, YF AF Huang, Kan Fu, Joshua S. Hsu, N. Christina Gao, Yang Dong, Xinyi Tsay, Si-Chee Lam, Yun Fat TI Impact assessment of biomass burning on air quality in Southeast and East Asia during BASE-ASIA SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Biomass burning; Southeast Asia; CMAQ; Long-range transport; Aerosol chemical property; Aerosol optical property ID AEROSOL OPTICAL-PROPERTIES; SKY RADIANCE MEASUREMENTS; TRANSPORT; COMBUSTION; PARTICLES; ALGORITHM; SUPERSITE; EMISSIONS; PACIFIC; NETWORK AB A synergy of numerical simulation, ground-based measurement and satellite observation was applied to evaluate the impact of biomass burning originating from Southeast Asia (SE Asia) within the framework of NASA's 2006 Biomass burning Aerosols in Southeast Asia: Smoke Impact Assessment (BASE-ASIA). Biomass burning emissions in the spring of 2006 peaked in March-April when most intense biomass burning occurred in Myanmar, northern Thailand, Laos, and parts of Vietnam and Cambodia. Model performances were reasonably validated by comparing to both satellite and ground-based observations despite overestimation or underestimation occurring in specific regions due to high uncertainties of biomass burning emission. Chemical tracers of particulate K+, OC concentrations, and OC/EC ratios showed distinct regional characteristics, suggesting biomass burning and local emission dominated the aerosol chemistry. CMAQ modeled aerosol chemical components were underestimated at most circumstances and the converted AOD values from CMAQ were biased low at about a factor of 2, probably due to the underestimation of biomass emissions. Scenario simulation indicated that the impact of biomass burning to the downwind regions spread over a large area via the Asian spring monsoon, which included Southern China, South China Sea, and Taiwan Strait. Comparison of AERONET aerosol optical properties with simulation at multi-sites clearly demonstrated the biomass burning impact via long-range transport. In the source region, the contribution from biomass burning to AOD was estimated to be over 56%. While in the downwind regions, the contribution was still significant within the range of 26%-62%. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Huang, Kan; Fu, Joshua S.; Gao, Yang; Dong, Xinyi; Lam, Yun Fat] Univ Tennessee, Dept Civil & Environm Engn, Knoxville, TN 37996 USA. [Fu, Joshua S.] UTK ORNL Ctr Interdisciplinary Res & Grad Educ, Knoxville, TN USA. [Hsu, N. Christina; Tsay, Si-Chee] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Fu, JS (reprint author), Univ Tennessee, Dept Civil & Environm Engn, 59 Perkins Hall, Knoxville, TN 37996 USA. EM jsfu@utk.edu RI Tsay, Si-Chee/J-1147-2014; Huang, Kan/E-4824-2011; LAM, Yun Fat/K-7287-2015 OI LAM, Yun Fat/0000-0002-5917-0907 FU NASA GSFC [NNX09AG75G]; NASA Radiation Sciences Program FX We thank Thailand PCD, EANET, Taiwan EPA and AERONET for proving the measurement data. We thank Dr. Edward J. Hyer for providing FLAMBE biomass burning emission data. We thank NASA GSFC on funding support (grant no.: NNX09AG75G). Data products from SMART-COMMIT and Deep Blue groups of NASA GSFC are funded by the NASA Radiation Sciences Program, managed by Dr. Hal Maring. Hong Kong data was obtained from Hong Kong Environmental Protection Department. NR 33 TC 34 Z9 35 U1 6 U2 62 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 J9 ATMOS ENVIRON JI Atmos. Environ. PD OCT PY 2013 VL 78 SI SI BP 291 EP 302 DI 10.1016/j.atmosenv.2012.03.048 PG 12 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 220RW UT WOS:000324605600028 ER PT J AU Panicker, AS Park, SH Lee, DI Kim, DC Jung, WS Jang, SM Jeong, JH Kim, DS Yu, J Jeong, H AF Panicker, A. S. Park, Sung-Hwa Lee, Dong-In Kim, Dong-Chul Jung, Woon-Seon Jang, Sang-Min Jeong, Jong-Hoon Kim, Dong-Soon Yu, Jegyu Jeong, Harrison TI Observations of Black Carbon characteristics and radiative forcing over a Global Atmosphere Watch supersite in Korea SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Black carbon; Aerosol optical depth; Radiative forcing ID AEROSOL OPTICAL-PROPERTIES; URBAN-ENVIRONMENT; SOUTH-KOREA; PARTICLES; TRANSPORT; CLOUDS; SOOT AB This paper provides an account of observed variations in Black carbon (BC) mass concentrations and BC induced radiative forcing for the first time over a background Global Atmosphere Watch (GAW) site, Anmyeon in South Korea. BC concentrations were continuously measured over the site during January 2003-December 2004 periods using an Aethalometer. BC showed higher concentrations during 2003 in majority of the months (except in January, August and October). BC found to be showing higher concentrations in September 2003, with values reaching up to 3 mu g m(-3) over the site. It also showed higher peaks in May and December in 2003. BC values were found to be comparatively less during wet season (July-August; especially august), which could be associated with the rainout and washout associated with the Changma season (summer monsoon). Optical Properties of Aerosols and Clouds (OPAC) model in combination with a radiative transfer model (SBDART) were used to estimate aerosol radiative forcing separately for composite aerosols (total aerosols) and solely for BC aerosols using chemical composition data sets of Total Suspended Particulates (TSP) and BC. The atmospheric forcing for composite aerosols found to be +14.9 to +25.9 W m(-2) during spring, +13.4 to +20.4 W m(-2) in summer, +12.9 to +19.1 W m(-2) in autumn and +16 to +18.2 W m(-2) during winter, respectively. The respective BC atmospheric forcings were +8.1 to +11.8 W m(-2), +8.4 to +11.1 W m(-2), +8.7 to +11.4 W m(-2) and +8.8 to +11.7 W m(-2) during spring, summer, autumn and winter. The study suggests that BC induced atmospheric forcing can contribute up to 88% of total aerosol induced atmospheric warming. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Panicker, A. S.] Indian Inst Trop Meteorol, Pune 411008, Maharashtra, India. [Park, Sung-Hwa; Lee, Dong-In; Jung, Woon-Seon; Jang, Sang-Min; Jeong, Jong-Hoon] Pukyong Natl Univ, Dept Environm Atmospher Sci, Atmospher Environm Res Inst, Pusan, South Korea. [Kim, Dong-Chul] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Kim, Dong-Chul] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kim, Dong-Soon] Natl Res Inst Earth Sci & Disaster Prevent, Tsukuba, Ibaraki, Japan. [Yu, Jegyu; Jeong, Harrison] Korea Meteorol Adm, Korea Global Atmosphere Watch Ctr, Seoul, South Korea. RP Panicker, AS (reprint author), Indian Inst Trop Meteorol, Pune 411008, Maharashtra, India. EM abhilashpanicker@gmail.com; leedi@pknu.ac.kr RI Kim, Dongchul/H-2256-2012 OI Kim, Dongchul/0000-0002-5659-1394 FU National Research Foundation of Korea (NRF) through Korean Ministry of Education, Science & Technology (MEST) [2013-00037] FX A.S. Panicker acknowledges, Prof. B.N. Goswami, Director IITM and Dr. G. Beig for their encouragements. This work is supported by National Research Foundation of Korea (NRF) through a grant provided by the Korean Ministry of Education, Science & Technology (MEST) 2013 (No. 2013-00037). The aerosol chemical datasets maintained in Anmyendo GAW observatory used in this study is gratefully acknowledged. NR 33 TC 11 Z9 12 U1 3 U2 26 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD OCT PY 2013 VL 77 BP 98 EP 104 DI 10.1016/j.atmosenv.2013.04.020 PG 7 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 223YN UT WOS:000324848500009 ER PT J AU Streets, DG Canty, T Carmichael, GR de Foy, B Dickerson, RR Duncan, BN Edwards, DP Haynes, JA Henze, DK Houyoux, MR Jacobi, DJ Krotkov, NA Lamsal, LN Liu, Y Lu, ZF Martini, RV Pfister, GG Pinder, RW Salawitch, RJ Wechti, KJ AF Streets, David G. Canty, Timothy Carmichael, Gregory R. de Foy, Benjamin Dickerson, Russell R. Duncan, Bryan N. Edwards, David P. Haynes, John A. Henze, Daven K. Houyoux, Marc R. Jacobi, Daniel J. Krotkov, Nickolay A. Lamsal, Lok N. Liu, Yang Lu, Zifeng Martini, Randall V. Pfister, Gabriele G. Pinder, Robert W. Salawitch, Ross J. Wechti, Kevin J. TI Emissions estimation from satellite retrievals: A review of current capability SO ATMOSPHERIC ENVIRONMENT LA English DT Review DE Satellite retrievals; Emission inventories; Air quality management; Data assimilation; National Emission Inventory ID OZONE MONITORING INSTRUMENT; AEROSOL OPTICAL DEPTH; TROPOSPHERIC NITROGEN-DIOXIDE; EASTERN UNITED-STATES; GROUND-LEVEL PM2.5; IMAGING SPECTRORADIOMETER MODIS; ATMOSPHERIC INFRARED SOUNDER; NITRIC-OXIDE EMISSIONS; BIOMASS BURNING PLUMES; THERMAL POWER-PLANTS AB Since the mid-1990s a new generation of Earth-observing satellites has been able to detect tropospheric air pollution at increasingly high spatial and temporal resolution. Most primary emitted species can be measured by one or more of the instruments. This review article addresses the question of how well we can relate the satellite measurements to quantification of primary emissions and what advances are needed to improve the usability of the measurements by U.S. air quality managers. Built on a comprehensive literature review and comprising input by both satellite experts and emission inventory specialists, the review identifies several targets that seem promising: large point sources of NOx and SO2, species that are difficult to measure by other means (NH3 and CH4, for example), area sources that cannot easily be quantified by traditional bottom-up methods (such as unconventional oil and gas extraction, shipping, biomass burning, and biogenic sources), and the temporal variation of emissions (seasonal, diurnal, episodic). Techniques that enhance the usefulness of current retrievals (data assimilation, oversampling, multi-species retrievals, improved vertical profiles, etc.) are discussed. Finally, we point out the value of having new geostationary satellites like CEO-CAPE and TEMPO over North America that could provide measurements at high spatial (few km) and temporal (hourly) resolution. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Streets, David G.] Argonne Natl Lab, Decis & Informat Sci Div, Argonne, IL 60439 USA. [Canty, Timothy] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Carmichael, Gregory R.] Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA 52242 USA. [de Foy, Benjamin] St Louis Univ, Dept Earth & Atmospher Sci, St Louis, MO 63108 USA. [Duncan, Bryan N.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA. [Edwards, David P.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80301 USA. [Haynes, John A.] Natl Aeronaut & Space Adm, Div Earth Sci, Washington, DC 20546 USA. [Henze, Daven K.] Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA. [Houyoux, Marc R.] US EPA, Off Air Qual Planning & Stand, Res Triangle Pk, NC 27711 USA. [Jacobi, Daniel J.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Liu, Yang] Emory Clin, Dept Environm Hlth, Atlanta, GA 30322 USA. [Martini, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. [Pinder, Robert W.] US Environm Protect Agcy, Off Res & Dev, Res Triangle Pk, NC USA. RP Streets, DG (reprint author), Argonne Natl Lab, Decis & Informat Sci Div, 9700 S Cass Ave, Argonne, IL 60439 USA. EM dstreets@anl.gov RI Pinder, Robert/F-8252-2011; Lu, Zifeng/F-3266-2012; Canty, Timothy/F-2631-2010; de Foy, Benjamin/A-9902-2010; Salawitch, Ross/B-4605-2009; Krotkov, Nickolay/E-1541-2012; Dickerson, Russell/F-2857-2010; Duncan, Bryan/A-5962-2011 OI Streets, David/0000-0002-0223-1350; Pinder, Robert/0000-0001-6390-7126; Canty, Timothy/0000-0003-0618-056X; de Foy, Benjamin/0000-0003-4150-9922; Salawitch, Ross/0000-0001-8597-5832; Krotkov, Nickolay/0000-0001-6170-6750; Dickerson, Russell/0000-0003-0206-3083; FU NASA Air Quality Applied Sciences Team (AQAST); US Department of Energy [DE-AC02-06CH11357] FX Nine of the co-authors of this article (DGS, GRC, BdF, RRD, BND, DPE, DKH, DJJ, and YL) are members of the NASA Air Quality Applied Sciences Team (AQAST) and acknowledge funding support from this program. They wish to express their gratitude to the present (John Haynes) and former (Lawrence Friedl) NASA program managers. Argonne National Laboratory is operated by UChicago Argonne, LLC, under Contract No. DE-AC02-06CH11357 with the US Department of Energy. NR 311 TC 81 Z9 82 U1 14 U2 214 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 OCT PY 2013 VL 77 BP 1011 EP 1042 DI 10.1016/j.atmosenv.2013.05.051 PG 32 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 223YN UT WOS:000324848500107 ER PT J AU Garfinkel, CI Hurwitz, MM Waugh, DW Butler, AH AF Garfinkel, C. I. Hurwitz, M. M. Waugh, D. W. Butler, A. H. TI Are the teleconnections of Central Pacific and Eastern Pacific El Nio distinct in boreal wintertime? SO CLIMATE DYNAMICS LA English DT Article DE Central Pacific ENSO; Teleconnections; Stratospheric dynamics ID SEA-SURFACE TEMPERATURES; SOUTHERN-OSCILLATION; SEASONAL PREDICTION; WAVE-PROPAGATION; CLIMATE RESPONSE; NINO; STRATOSPHERE; VARIABILITY; PATTERNS; EVENTS AB A meteorological reanalysis dataset and experiments of the Goddard Earth Observing System Chemistry-Climate Model, Version 2 (GEOS V2 CCM) are used to study the boreal winter season teleconnections in the Pacific-North America region and in the stratosphere generated by Central Pacific and Eastern Pacific El Nio. In the reanalysis data, the sign of the North Pacific and stratospheric response to Central Pacific El Nio is sensitive to the composite size, the specific Central Pacific El Nio index used, and the month or seasonal average that is examined, highlighting the limitations of the short observational record. Long model integrations suggest that the response to the two types of El Nio are similar in both the extratropical troposphere and stratosphere. Namely, both Central Pacific and Eastern Pacific El Nio lead to a deepened North Pacific low and a weakened polar vortex, and the effects are stronger in late winter than in early winter. However, the long experiments do indicate some differences between the two types of El Nio events regarding the latitude of the North Pacific trough, the early winter polar stratospheric response, surface temperature and precipitation over North America, and globally averaged surface temperature. These differences are generally consistent with, though smaller than, those noted in previous studies. C1 [Garfinkel, C. I.; Waugh, D. W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21209 USA. [Hurwitz, M. M.] Morgan State Univ, NASA Goddard Earth Sci Technol & Res GESTAR, Baltimore, MD 21239 USA. [Hurwitz, M. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Butler, A. H.] NOAA, Climate Predict Ctr, NCEP, Camp Springs, MD USA. RP Garfinkel, CI (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21209 USA. EM cig4@jhu.edu RI Butler, Amy/K-6190-2012; garfinkel, chaim/H-6215-2012; Waugh, Darryn/K-3688-2016 OI Butler, Amy/0000-0002-3632-0925; garfinkel, chaim/0000-0001-7258-666X; Waugh, Darryn/0000-0001-7692-2798 FU NASA [NNX06AE70G]; NASA's ACMAP program FX This work was supported by the NASA grant number NNX06AE70G and NASA's ACMAP program. NR 60 TC 15 Z9 15 U1 1 U2 24 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 EI 1432-0894 J9 CLIM DYNAM JI Clim. Dyn. PD OCT PY 2013 VL 41 IS 7-8 BP 1835 EP 1852 DI 10.1007/s00382-012-1570-2 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 223NJ UT WOS:000324812200008 ER PT J AU Konishi, C Mudawar, I Hasan, MM AF Konishi, Christopher Mudawar, Issam Hasan, Mohammad M. TI Criteria for negating the influence of gravity on flow boiling critical heat flux with two-phase inlet conditions SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER LA English DT Article DE Flow boiling; Critical heat flux; Flow orientation; Microgravity ID WATER-FLOW; TRIGGER MECHANISM; VERTICAL SURFACES; CHF MECHANISM; SINGLE-PHASE; BODY FORCE; ORIENTATION; MODEL; TUBES; WALL AB This study explores the complex flow boiling CHF mechanisms encountered at different orientations relative to Earth's gravity when the fluid is supplied as a two-phase mixture. Using FC-72 as working fluid, different CHF regimes are identified for different orientations, mass velocities and inlet qualities. Low mass velocities are shown to produce the greatest sensitivity to orientation, while high mass velocities greatly reduce this influence, especially for high inlet qualities. It is also shown that the influence of orientation can be negated by simultaneously satisfying three separate criteria: overcoming the influence of gravity perpendicular to the heated wall, overcoming the influence of gravity parallel to the heated wall, and ensuring that the heated wall is sufficiently long to ensure liquid contact. These criteria are combined to determine the minimum mass velocity required to negate gravity effects in both terrestrial and space applications. Exceeding this minimum is of paramount importance to space systems since it enables the implementation of the vast body of published CHF data, correlations and models developed from terrestrial studies for design of thermal management systems for space applications. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Konishi, Christopher; Mudawar, Issam] Purdue Univ, Sch Mech Engn, Boiling & Phase Flow Lab 2, W Lafayette, IN 47907 USA. [Hasan, Mohammad M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Mudawar, I (reprint author), Purdue Univ, Sch Mech Engn, Boiling & Phase Flow Lab 2, 585 Purdue Mall, W Lafayette, IN 47907 USA. EM mudawar@ecn.purdue.edu FU National Aeronautics and Space Administration (NASA) [NNX13AC83G] FX The authors are grateful for the support of the National Aeronautics and Space Administration (NASA) under Grant no. NNX13AC83G. NR 46 TC 6 Z9 7 U1 1 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0017-9310 J9 INT J HEAT MASS TRAN JI Int. J. Heat Mass Transf. PD OCT PY 2013 VL 65 BP 203 EP 218 DI 10.1016/j.ijheatmasstransfer.2013.05.070 PG 16 WC Thermodynamics; Engineering, Mechanical; Mechanics SC Thermodynamics; Engineering; Mechanics GA 223XC UT WOS:000324844800021 ER PT J AU Shume, EB Rodrigues, FS de Paula, ER Batista, IS Butala, MD Galvan, DA AF Shume, E. B. Rodrigues, F. S. de Paula, E. R. Batista, I. S. Butala, M. D. Galvan, D. A. TI Day-time F region echoes observed by the Sao Luis radar SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Plasma irregularities; Electric fields; Conductivities; F region equatorial ionosphere; Radar observation ID EQUATORIAL SPREAD-F; IRREGULARITIES; JICAMARCA AB This brief report presents unique day-time F region coherent scatter echoes observed by the 30 MHz radar over Sao Luis in eastern Brazil. The radar observation was part of the July 2011 radar campaign designed to detect echoes from day-time F region irregularities. These rare day-time F region radar echoes, scattered from short wavelength plasma irregularities, have quasi patchy features. They are characterized by large upward Doppler velocities (similar to 100-200 m/s). They are very weak (by more than 10 dB) when compared to radar echoes observed over Sao Luis scattered from the night-time F plasma irregularities known as equatorial spread F. Simultaneous GPS vertical total electron content (TEC), and F-2 peak frequency (f(o)F(2)) and F-2 peak height (h(m)F(2)) estimated from ionosonde measurements over Sao Luis have provided additional evidence that the received day-time F region radar echoes were from genuine ionospheric scatterers. This report suggests physical explanations for the day-time radar echoes in terms of the generalized Rayleigh-Taylor instability mechanism operating on large magnetic declination (similar to 20 degrees westward) of the geomagnetic field geometry in Sao Luis, conductivity distribution in the winter southern hemisphere and summer northern hemisphere, and the resulting magnetic flux tube electric field configurations. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Shume, E. B.; Butala, M. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Rodrigues, F. S.] Univ Texas Dallas, WB Hanson Ctr Space Sci, Richardson, TX 75083 USA. [de Paula, E. R.; Batista, I. S.] Natl Inst Space Res, Sao Jose Dos Campos, Brazil. [Galvan, D. A.] RAND Corp, Santa Monica, CA USA. RP Shume, EB (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Esayas.B.Shume@jpl.nasa.gov RI Shume, Esayas/I-3354-2013; Batista, Inez/F-2899-2012; de Paula, Eurico/O-1709-2013; OI de Paula, Eurico/0000-0003-2756-3826; Shume, Esayas/0000-0002-4696-1283 FU National Aeronautics and Space Administration; AFOSR [FA9550-09-C-0205]; NASA; FAPESP [2007/08185-9, 99/00026-0, 04/01065-0] FX Portions of this research were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. E. B. Shume acknowledges the NPP program administered by Oak Ridge Associated Universities through a contract with NASA. AFOSR Project FA9550-09-C-0205 is acknowledged for making possible the upgrades in the Sao Luis radar data acquisition system that allowed the radar measurements. E. B. Shume acknowledges FAPESP project 2007/08185-9. The Sao Luis 30 MHz radar is partially supported by FAPESP grants 99/00026-0 and 04/01065-0. NR 20 TC 3 Z9 3 U1 0 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD OCT PY 2013 VL 103 SI SI BP 48 EP 55 DI 10.1016/j.jastp.2013.02.003 PG 8 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 225KZ UT WOS:000324963100008 ER PT J AU Huang, CY Roddy, PA Sutton, EK Stoneback, R Pfaff, RF Gentile, LC Delay, SH AF Huang, Cheryl Y. Roddy, Patrick A. Sutton, Eric K. Stoneback, Russell Pfaff, Robert F. Gentile, Louise C. Delay, Susan H. TI Ion-neutral coupling during deep solar minimum SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Equatorial ionosphere; Thermosphere; Nonmigrating tides; Plasma depletions ID LATENT-HEAT RELEASE; TIDES; DENSITY; CHAMP AB The equatorial ionosphere under conditions of deep solar minimum exhibits structuring due to tidal forces. Data from instruments carried by the Communication/Navigation Outage Forecasting System (C/NOFS) which was launched in April 2008 have been analyzed for the first 2 years following launch. The Planar Langmuir Probe (PLP), Ion Velocity Meter (IVM) and Vector Electric Field Investigation (VEFI) all detect periodic structures during the 2008-2010 period which appear to be tides. However when the tidal features detected by these instruments are compared, there are distinctive and significant differences between the observations. Tides in neutral densities measured by the Gravity Recovery and Climate Experiment (GRACE) satellite were also observed during June 2008. In addition, Broad Plasma Decreases (BPDs) appear as a deep absolute minimum in the plasma and neutral density tidal pattern. These are co-located with regions of large downward-directed ion meridional velocities and minima in the zonal drifts, all on the nightside. The region in which BPDs occur coincides with a peak in occurrence rate of dawn depletions in plasma density observed on the Defense Meterological Satellite Program (DMSP) spacecraft, as well as a minimum in radiance detected by UV imagers on the Thermosphere Ionosphere Mesosphere Energetics and Dynamics (TIMED) and IMAGE satellites. Published by Elsevier Ltd. C1 [Huang, Cheryl Y.; Roddy, Patrick A.; Sutton, Eric K.; Gentile, Louise C.] Air Force Res Lab, Space Vehicles Directorate, Kirtland AFB, NM 87116 USA. [Stoneback, Russell] Univ Texas Dallas, William B Hanson Ctr Space Sci, Richardson, TX 75083 USA. [Pfaff, Robert F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Delay, Susan H.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02167 USA. RP Huang, CY (reprint author), Air Force Res Lab, Space Vehicles Directorate, Kirtland AFB, NM 87116 USA. EM cheryl.huang@us.af.mil RI Sutton, Eric/A-1574-2016; OI Sutton, Eric/0000-0003-1424-7189; Stoneback, Russell/0000-0001-7216-4336 FU Air Force Research Laboratory; Department of Defense Space Test Program; National Aeronautics and Space Administration; Naval Research Laboratory; Aerospace Corporation; Air Force Office of Scientific Research [12RV120COR] FX The C/NOFS mission is supported by the Air Force Research Laboratory, the Department of Defense Space Test Program, the National Aeronautics and Space Administration, the Naval Research Laboratory, and the Aerospace Corporation. This research was supported by Air Force Office of Scientific Research Task 12RV120COR. We thank Dr. John Retterer for his assistance with VEFI data processing. NR 38 TC 3 Z9 3 U1 0 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD OCT PY 2013 VL 103 SI SI BP 138 EP 146 DI 10.1016/j.jastp.2012.11.009 PG 9 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 225KZ UT WOS:000324963100018 ER PT J AU Yizengaw, E Zesta, E Biouele, CM Moldwin, MB Boudouridis, A Damtie, B Mebrahtu, A Anad, F Pfaff, RF Hartinger, M AF Yizengaw, E. Zesta, E. Biouele, C. M. Moldwin, M. B. Boudouridis, A. Damtie, B. Mebrahtu, A. Anad, F. Pfaff, R. F. Hartinger, M. TI Observations of ULF wave related equatorial electrojet and density fluctuations SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE ULF waves; Pc5 pulsations; Equatorial electrodynamics; Electric field ID PRELIMINARY REVERSE IMPULSE; B DRIFT VELOCITIES; GRAVITY-WAVES; LOW LATITUDES; IONOSPHERE; FIELD; PROPAGATION; PULSATIONS; MAGNETOSPHERE; OSCILLATIONS AB We report on Pc5 wave related electric field and vertical drift velocity oscillations at the equator as observed by ground magnetometers for an extended period on 9 August 2008. We show that the magnetometer-estimated equatorial E x B drift oscillates with the same frequency as ULF Pc5 waves, creating significant ionospheric density fluctuations. We also show ionospheric density fluctuations during the period when we observed ULF wave activity. At the same time, we detect the ULF activity on the ground using ground-based magnetometer data from the African Meridian B-field Education and Research (AMBER) and the South American Meridional B-field Array (SAMBA). From space, we use magnetic field observations from the GOES 12 and the Communication/Navigation Outage and Forecast System (C/NOFS) satellites. Upstream solar wind conditions are provided by the ACE spacecraft. We find that the wave power observed on the ground also occurs in the upstream solar wind and in the magnetosphere. All these observations demonstrate that Pc5 waves with a likely driver in the solar wind can penetrate to the equatorial ionosphere and modulate the equatorial electrodynamics. While no direct drift measurements from equatorial radars exist for the 9 August 2008 event, we used JULIA 150 km radar drift velocities observed on 2 May 2010 and found similar fluctuations with the period of 5-8 min, as a means of an independent confirmation of our magnetometer derived drift dynamics. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Yizengaw, E.] Boston Coll, Inst Sci Res, Boston, MA 02467 USA. [Zesta, E.] AFRL, RVBXP, Kirtland AFB, NM USA. [Biouele, C. M.] Univ Yaounde I, Dept Phys, Yaounde, Cameroon. [Moldwin, M. B.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Boudouridis, A.] Space Sci Inst, Boulder, CO USA. [Damtie, B.] Bahir Dar Univ, Washera Geospace & Radar Sci Lab, Bahir Dar, Ethiopia. [Mebrahtu, A.] Mekelle Univ, Dept Phys, Mekelle, Ethiopia. [Anad, F.] Ctr Rech Astron Astrophys & Geophys, Algiers, Algeria. [Pfaff, R. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hartinger, M.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. RP Yizengaw, E (reprint author), Boston Coll, Inst Sci Res, Boston, MA 02467 USA. EM kassie@bc.edu RI Hartinger, Michael/H-9088-2012; Moldwin, Mark/F-8785-2011; Yizengaw, Endawoke/I-3471-2015 OI Hartinger, Michael/0000-0002-2643-2202; Moldwin, Mark/0000-0003-0954-1770; Yizengaw, Endawoke/0000-0001-5772-3355 FU NASA [NNX07AM22G, NNX09AR84G, NNX09AI62G]; NASA LWS [NNX10AQ53G, NNX11AP02G]; AFOSR YIP [FA9550-10-1-0096] FX This work was supported by NASA IHY and Geospace Science Programs (NNX07AM22G and NNX09AR84G), NASA LWS programs (NNX10AQ53G and NNX11AP02G), and AFOSR YIP Grant (FA9550-10-1-0096). MBM was partially support by a NASA Geospace Grant (NNX09AI62G). The geomagnetic indexes (Dst, Kp) and solar wind data are obtained from World Data Center. The authors are indebted to the ACE, GOES, THEMIS, and INTERMAGNET team for the data resources they made available to the public. We also thank Dr. James Weygand for the propagated solar wind data. NR 36 TC 3 Z9 3 U1 0 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD OCT PY 2013 VL 103 SI SI BP 157 EP 168 DI 10.1016/j.jastp.2013.03.015 PG 12 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 225KZ UT WOS:000324963100020 ER PT J AU Patterson, TA Wood, WG Andrews, RJ Slikker, W AF Patterson, Tucker A. Wood, W. Gibson Andrews, Russell J. Slikker, William, Jr. TI Preface SO MOLECULAR NEUROBIOLOGY LA English DT Editorial Material C1 [Patterson, Tucker A.; Slikker, William, Jr.] US FDA, Natl Ctr Toxicol Res, Jefferson, AR 72079 USA. [Wood, W. Gibson] Univ Minnesota, Sch Med, Dept Pharmacol, Geriatr Res Educ & Clin Ctr,VA Med Ctr, Minneapolis, MN 55455 USA. [Andrews, Russell J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Slikker, W (reprint author), US FDA, Natl Ctr Toxicol Res, 3900 NCTR Rd, Jefferson, AR 72079 USA. EM William.Slikker@fda.hhs.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU HUMANA PRESS INC PI TOTOWA PA 999 RIVERVIEW DRIVE SUITE 208, TOTOWA, NJ 07512 USA SN 0893-7648 J9 MOL NEUROBIOL JI Mol. Neurobiol. PD OCT PY 2013 VL 48 IS 2 BP 271 EP 273 DI 10.1007/s12035-013-8513-8 PG 3 WC Neurosciences SC Neurosciences & Neurology GA 221EN UT WOS:000324640600001 PM 23884619 ER PT J AU Zhang, DA Rand, E Marsh, M Andrews, RJ Lee, KH Meyyappan, M Koehne, JE AF Zhang, David A. Rand, Emily Marsh, Michael Andrews, Russell J. Lee, Kendall H. Meyyappan, M. Koehne, Jessica E. TI Carbon Nanofiber Electrode for Neurochemical Monitoring SO MOLECULAR NEUROBIOLOGY LA English DT Review DE Biosensor; Neurotransmitter; Carbon nanofiber; Nanoelectrode ID DEEP BRAIN-STIMULATION; NANOTUBE NANOELECTRODE ARRAYS; DOPAMINE; MICROELECTRODES; FABRICATION; INTERFACES; ACID AB The ability to rapidly detect neurotransmitter release has broad implications in the study of a variety of neurodegenerative diseases. Electrochemical detection methods using carbon nanofiber nanoelectrodes integrated into the Wireless Instantaneous Neurotransmitter Concentration Sensing System (WINCS) offer many important advantages including biocompatibility, selectivity, sensitivity, and rapid adsorption kinetics. Carbon nanofiber nanoelectrodes exhibit greater selectivity and sensitivity in the electrochemical detection of neurotransmitters compared to macroelectrodes and are able to resolve a ternary mixture of dopamine (DA), serotonin (5-HT), and ascorbic acid as well as to detect individual neurotransmitters in concentrations as low as 50 nM for DA and 100 nM for 5-HT using differential pulse voltammetry. Adsorption kinetics studies and isopropyl alcohol treatments modeled on previous studies on carbon fiber microelectrodes were conducted to investigate the analogous properties on carbon nanofiber electrodes using fast-scan cyclic voltammetry with WINCS and showed analogous results in carbon nanofiber electrodes compared with carbon fiber microelectrodes. C1 [Zhang, David A.; Rand, Emily; Andrews, Russell J.; Meyyappan, M.; Koehne, Jessica E.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. [Marsh, Michael; Lee, Kendall H.] Mayo Clin, Dept Bioengn, Rochester, MN 55905 USA. [Lee, Kendall H.] Mayo Clin, Dept Neurol Surg, Rochester, MN 55905 USA. RP Koehne, JE (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. EM Jessica.E.Koehne@nasa.gov FU National Institutes of Health [R01-NS75013] FX This work was supported in part by a grant from the National Institutes of Health (R01-NS75013) to Mayo Clinic. NR 27 TC 10 Z9 10 U1 10 U2 88 PU HUMANA PRESS INC PI TOTOWA PA 999 RIVERVIEW DRIVE SUITE 208, TOTOWA, NJ 07512 USA SN 0893-7648 J9 MOL NEUROBIOL JI Mol. Neurobiol. PD OCT PY 2013 VL 48 IS 2 BP 380 EP 385 DI 10.1007/s12035-013-8531-6 PG 6 WC Neurosciences SC Neurosciences & Neurology GA 221EN UT WOS:000324640600014 PM 23975638 ER PT J AU Jang, DC Meza, LR Greer, F Greer, JR AF Jang, Dongchan Meza, Lucas R. Greer, Frank Greer, Julia R. TI Fabrication and deformation of three-dimensional hollow ceramic nanostructures SO NATURE MATERIALS LA English DT Article ID TITANIUM NITRIDE; MECHANICAL-PROPERTIES; BRITTLE; SILICON; TRANSITION; NANOSCALE; FRACTURE AB Creating lightweight, mechanically robust materials has long been an engineering pursuit. Many siliceous skeleton species-such as diatoms, sea sponges and radiolarians-have remarkably high strengths when compared with man-made materials of the same composition, yet are able to remain lightweight and porous(1-7). It has been suggested that these properties arise from the hierarchical arrangement of different structural elements at their relevant length scales(8,9). Here, we report the fabrication of hollow ceramic scaffolds that mimic the length scales and hierarchy of biological materials. The constituent solids attain tensile strengths of 1.75 GPa without failure even after multiple deformation cycles, as revealed by in situ nanomechanical experiments and finite-element analysis. We discuss the high strength and lack of failure in terms of stress concentrators at surface imperfections and of local stresses within the microstructural landscape. Our findings suggest that the hierarchical design principles offered by hard biological organisms can be applied to create damage-tolerant lightweight engineering materials. C1 [Jang, Dongchan; Meza, Lucas R.; Greer, Julia R.] CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA. [Greer, Frank] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Greer, Julia R.] CALTECH, Kavli Nanosci Inst, Pasadena, CA 91125 USA. RP Greer, JR (reprint author), CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA. EM jrgreer@caltech.edu RI Jang, Dongchan/C-9510-2012 OI Jang, Dongchan/0000-0002-2814-9734 FU Dow-Resnick Innovation Fund at Caltech; DARPA's Materials with Controlled Microstructure and Architecture program; Army Research Office through the Institute for Collaborative Biotechnologies (ICB) at Caltech (ARO) [UCSB. ICB4b] FX The authors gratefully acknowledge the financial support from the Dow-Resnick Innovation Fund at Caltech, DARPA's Materials with Controlled Microstructure and Architecture program, and the Army Research Office through the Institute for Collaborative Biotechnologies (ICB) at Caltech (ARO Award number UCSB. ICB4b). Part of this work was carried out at the Jet Propulsion Laboratory under a contract with NASA. The authors acknowledge critical support and infrastructure provided by the Kavli Nanoscience Institute at Caltech. NR 33 TC 90 Z9 92 U1 21 U2 214 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1476-1122 J9 NAT MATER JI Nat. Mater. PD OCT PY 2013 VL 12 IS 10 BP 893 EP 898 DI 10.1038/NMAT3738 PG 6 WC Chemistry, Physical; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Materials Science; Physics GA 222MU UT WOS:000324736000014 PM 23995324 ER PT J AU Goldman, I Mohapatra, RN Nussinov, S Rosenbaum, D Teplitz, V AF Goldman, I. Mohapatra, R. N. Nussinov, S. Rosenbaum, D. Teplitz, V. TI Possible implications of asymmetric fermionic dark matter for neutron stars SO PHYSICS LETTERS B LA English DT Article ID MASSIVE PARTICLES; UNIVERSE; BARYON; NUMBER AB We consider the implications of fermionic asymmetric dark matter (ADM) for a "mixed neutron star" composed of ordinary baryons and dark fermions. We find examples, where for a certain range of dark fermion mass - when it is less than that of ordinary baryons - such systems can reach higher masses than the maximal values allowed for ordinary ("pure") neutron stars. This is shown both within a simplified, heuristic Newtonian analytic framework with non-interacting particles and via a general relativistic numerical calculation, under certain assumptions for the dark matter equation of state. Our work applies to various dark fermion models such as mirror matter models and to other models where the dark fermions have self-interactions. (C) 2013 Elsevier B.V. All rights reserved. C1 [Goldman, I.] Afeka Tel Aviv Acad Engn Coll, Dept Exact Sci, Tel Aviv, Israel. [Mohapatra, R. N.] Univ Maryland, Maryland Ctr Fundamental Phys, College Pk, MD 20742 USA. [Mohapatra, R. N.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Nussinov, S.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Nussinov, S.] Chapman Univ, Schmid Coll Sci, Orange, CA 92866 USA. [Rosenbaum, D.; Teplitz, V.] So Methodist Univ, Dept Phys, Dallas, TX 75275 USA. [Teplitz, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Mohapatra, RN (reprint author), Univ Maryland, Maryland Ctr Fundamental Phys, College Pk, MD 20742 USA. EM rmohapat@umd.edu OI Goldman, Itzhak/0000-0001-6200-7898 FU National Science Foundation [PHY-0968854] FX The work of R.N.M. is supported by National Science Foundation grant No. PHY-0968854. NR 44 TC 7 Z9 7 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0370-2693 EI 1873-2445 J9 PHYS LETT B JI Phys. Lett. B PD OCT PY 2013 VL 725 IS 4-5 BP 200 EP 207 DI 10.1016/j.physletb.2013.07.017 PG 8 WC Astronomy & Astrophysics; Physics, Nuclear; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 215PP UT WOS:000324223100004 ER PT J AU Benafan, O Notardonato, WU Meneghelli, BJ Vaidyanathan, R AF Benafan, O. Notardonato, W. U. Meneghelli, B. J. Vaidyanathan, R. TI Design and development of a shape memory alloy activated heat pipe-based thermal switch SO SMART MATERIALS AND STRUCTURES LA English DT Article ID NEUTRON-DIFFRACTION; IN-SITU; R-PHASE; TRANSFORMATION; BEHAVIOR; NITI; TEMPERATURES; DEFORMATION; TI50NI47FE3; RECOVERY AB This work reports on the design, fabrication and testing of a thermal switch wherein the open and closed states were actuated by shape memory alloy (SMA) elements while heat was transferred by a two-phase heat pipe. The motivation for such a switch comes from NASA's need for thermal management in advanced spaceport applications associated with future lunar and Mars missions. As the temperature can approximately vary between -233 and 127 degrees C during lunar day/night cycles, the switch was designed to reject heat from a cryogen tank into space during the night cycle while providing thermal isolation during the day cycle. A Ni47.1Ti49.6Fe3.3 (at.%) alloy that exhibited a reversible phase transformation between a trigonal R-phase and a cubic austenite phase was used as the sensing and actuating elements. Thermomechanical actuation, accomplished through an antagonistic spring system, resulted in strokes up to 7 mm against bias forces of up to 45 N. The actuation system was tested for more than thirty cycles, equivalent to one year of operation. The thermal performance, accomplished via a variable length, closed two-phase heat pipe, was evaluated, resulting in heat transfer rates of 13 W using pentane and 10 W using R-134a as working fluids. Experimental data were also compared to theoretical predictions where possible. Direct comparisons between different design approaches of SMA helical actuators, highlighting the effects of the helix angle, were carried out to give a layout of more accurate design methodologies. C1 [Benafan, O.; Vaidyanathan, R.] Univ Cent Florida, Adv Mat Proc & Anal Ctr, Mech Mat & Aerosp Engn Dept, Orlando, FL 32816 USA. [Notardonato, W. U.] NASA, Kennedy Space Ctr, Cryogen Test Lab, Kennedy Space Ctr, FL 32899 USA. [Meneghelli, B. J.] ASRC Aerosp Corp, Titusville, FL 32780 USA. RP Benafan, O (reprint author), NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. EM othmane.benafan@nasa.gov FU NASA KSC [NAS10-03006] FX Funding from NASA KSC Grant No. NAS10-03006 to UCF is gratefully acknowledged. The authors thank Mark D Velasco and Richard E Zotti for their contributions in machining parts and helpful suggestions. NR 45 TC 4 Z9 4 U1 3 U2 19 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0964-1726 J9 SMART MATER STRUCT JI Smart Mater. Struct. PD OCT PY 2013 VL 22 IS 10 SI SI AR 105017 DI 10.1088/0964-1726/22/10/105017 PG 17 WC Instruments & Instrumentation; Materials Science, Multidisciplinary SC Instruments & Instrumentation; Materials Science GA 221GD UT WOS:000324645000041 ER PT J AU He, JJ Guan, XF Peng, TS Liu, YM Saxena, A Celaya, J Goebel, K AF He, Jingjing Guan, Xuefei Peng, Tishun Liu, Yongming Saxena, Abhinav Celaya, Jose Goebel, Kai TI A multi-feature integration method for fatigue crack detection and crack length estimation in riveted lap joints using Lamb waves SO SMART MATERIALS AND STRUCTURES LA English DT Article ID PIEZOELECTRIC SENSOR/ACTUATOR NETWORK; WAFER ACTIVE SENSORS; DAMAGE IDENTIFICATION; PLATE; TRANSDUCERS; VALIDATION; GENERATION; SIGNALS AB This paper presents an experimental study of damage detection and quantification in riveted lap joints. Embedded lead zirconate titanate piezoelectric (PZT) ceramic wafer-type sensors are employed to perform in situ non-destructive evaluation (NDE) during fatigue cyclical loading. PZT wafers are used to monitor the wave reflection from the boundaries of the fatigue crack at the edge of bolt joints. The group velocity of the guided wave is calculated to select a proper time window in which the received signal contains the damage information. It is found that the fatigue crack lengths are correlated with three main features of the signal, i.e., correlation coefficient, amplitude change, and phase change. It was also observed that a single feature cannot be used to quantify the damage among different specimens since a considerable variability was observed in the response from different specimens. A multi-feature integration method based on a second-order multivariate regression analysis is proposed for the prediction of fatigue crack lengths using sensor measurements. The model parameters are obtained using training datasets from five specimens. The effectiveness of the proposed methodology is demonstrated using several lap joint specimens from different manufactures and under different loading conditions. C1 [He, Jingjing; Guan, Xuefei; Peng, Tishun; Liu, Yongming] Arizona State Univ, Sch Engn Matter Transport & Energy, Tempe, AZ 85281 USA. [Saxena, Abhinav; Celaya, Jose] NASA, Ames Res Ctr, SGT, Moffett Field, CA 94035 USA. [Goebel, Kai] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP He, JJ (reprint author), Arizona State Univ, Sch Engn Matter Transport & Energy, Tempe, AZ 85281 USA. EM yongming.liu@asu.edu FU NASA [NRANNX09AY54A] FX The research reported in this paper was supported by the NASA ARMD/AvSP IVHM and SSAT projects under NRANNX09AY54A. The support is gratefully acknowledged. The authors also thank the in-kind support for testing specimens and technical discussions with Dr Min Liao at NRC Canada and Mr Mike Venti of NASA Dryden Flight Research Center for providing and manufacturing additional test specimen. NR 39 TC 10 Z9 10 U1 1 U2 17 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0964-1726 J9 SMART MATER STRUCT JI Smart Mater. Struct. PD OCT PY 2013 VL 22 IS 10 SI SI AR 105007 DI 10.1088/0964-1726/22/10/105007 PG 12 WC Instruments & Instrumentation; Materials Science, Multidisciplinary SC Instruments & Instrumentation; Materials Science GA 221GD UT WOS:000324645000031 ER PT J AU O'Gorman, E Harper, GM Brown, A Drake, S Richards, AMS AF O'Gorman, Eamon Harper, Graham M. Brown, Alexander Drake, Stephen Richards, Anita M. S. TI MULTI-WAVELENGTH RADIO CONTINUUM EMISSION STUDIES OF DUST-FREE RED GIANTS SO ASTRONOMICAL JOURNAL LA English DT Article DE radio continuum: stars; stars: chromospheres; stars: individual (alpha Boo, alpha Tau); stars: late-type; stars: winds, outflows ID WAVE-DRIVEN WINDS; LATE-TYPE STARS; MAGNETIC-FIELD GEOMETRY; LUMINOUS COOL STARS; LOW-GRAVITY STARS; MASS-LOSS; STELLAR WINDS; ALFVEN WAVES; ZETA-AURIGAE; ALPHA-TAURI AB Multi-wavelength centimeter continuum observations of non-dusty, non-pulsating K spectral-type red giants directly sample their chromospheres and wind acceleration zones. Such stars are feeble emitters at these wavelengths, however, and previous observations have provided only a small number of modest signal-to-noise measurements slowly accumulated over three decades. We present multi-wavelength Karl G. Jansky Very Large Array thermal continuum observations of the wind acceleration zones of two dust-free red giants, Arcturus (alpha Boo: K2 III) and Aldebaran (alpha Tau: K5 III). Importantly, most of our observations of each star were carried out over just a few days, so that we obtained a snapshot of the different stellar atmospheric layers sampled at different wavelengths, independent of any long-term variability. We report the first detections at several wavelengths for each star including a detection at 10 cm (3.0 GHz: S band) for both stars and a 20 cm (1.5 GHz: L band) detection for alpha Boo. This is the first time single (non-binary) luminosity class III red giants have been detected at these continuum wavelengths. Our long-wavelength data sample the outer layers of alpha Boo's atmosphere where its wind velocity is approaching (or possibly has reached) its terminal value and the ionization balance is becoming frozen-in. For alpha Tau, however, our long-wavelength data are still sampling its inner atmosphere, where the wind is still accelerating probably due to its lower mass-loss rate. We compare our data with published semi-empirical models based on ultraviolet data, and the marked deviations highlight the need for new atmospheric models to be developed. Spectral indices are used to discuss the possible properties of the stellar atmospheres, and we find evidence for a rapidly cooling wind in the case of alpha Boo. Finally, we develop a simple analytical wind model for alpha Boo based on our new long-wavelength flux measurements. C1 [O'Gorman, Eamon; Harper, Graham M.] Univ Dublin Trinity Coll, Sch Phys, Dublin 2, Ireland. [Brown, Alexander] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Drake, Stephen] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Richards, Anita M. S.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. RP O'Gorman, E (reprint author), Univ Dublin Trinity Coll, Sch Phys, Dublin 2, Ireland. OI Richards, Anita/0000-0002-3880-2450 FU Science Foundation Ireland [SFI11/RFP.1/AST/3064]; Trinity College Dublin FX The data presented in this paper were obtained with the Karl G. Jansky Very Large Array (VLA), which is an instrument of the National Radio Astronomy Observatory (NRAO). The NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We wish to thank the NRAO helpdesk for their detailed responses to our CASA-related queries. We thank the referee for their careful reading of the manuscript and their valuable comments. This publication has emanated from research conducted with the financial support of Science Foundation Ireland under Grant Number SFI11/RFP.1/AST/3064, and a grant from Trinity College Dublin. NR 79 TC 4 Z9 4 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 2013 VL 146 IS 4 AR 98 DI 10.1088/0004-6256/146/4/98 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 218AL UT WOS:000324404800027 ER PT J AU Person, MJ Dunham, EW Bosh, AS Levine, SE Gulbis, AAS Zangari, AM Zuluaga, CA Pasachoff, JM Babcock, BA Pandey, S Amrhein, D Sallum, S Tholen, DJ Collins, P Bida, T Taylor, B Bright, L Wolf, J Meyer, A Pfueller, E Wiedemann, M Roeser, HP Lucas, R Kakkala, M Ciotti, J Plunkett, S Hiraoka, N Best, W Pilger, EJ Micheli, M Springmann, A Hicks, M Thackeray, B Emery, JP Tilleman, T Harris, H Sheppard, S Rapoport, S Ritchie, I Pearson, M Mattingly, A Brimacombe, J Gault, D Jones, R Nolthenius, R Broughton, J Barry, T AF Person, M. J. Dunham, E. W. Bosh, A. S. Levine, S. E. Gulbis, A. A. S. Zangari, A. M. Zuluaga, C. A. Pasachoff, J. M. Babcock, B. A. Pandey, S. Amrhein, D. Sallum, S. Tholen, D. J. Collins, P. Bida, T. Taylor, B. Bright, L. Wolf, J. Meyer, A. Pfueller, E. Wiedemann, M. Roeser, H. -P. Lucas, R. Kakkala, M. Ciotti, J. Plunkett, S. Hiraoka, N. Best, W. Pilger, E. J. Micheli, M. Springmann, A. Hicks, M. Thackeray, B. Emery, J. P. Tilleman, T. Harris, H. Sheppard, S. Rapoport, S. Ritchie, I. Pearson, M. Mattingly, A. Brimacombe, J. Gault, D. Jones, R. Nolthenius, R. Broughton, J. Barry, T. TI THE 2011 JUNE 23 STELLAR OCCULTATION BY PLUTO: AIRBORNE AND GROUND OBSERVATIONS SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; Kuiper belt objects: individual (Pluto); occultations; planets and satellites: atmospheres ID PLANETARY-ATMOSPHERES; THERMAL STRUCTURE; LIGHT CURVES; MODEL; INVERSION; DENSITY; METHANE; RADIUS; WAVES AB On 2011 June 23, stellar occultations by both Pluto (this work) and Charon (future analysis) were observed from numerous ground stations as well as the Stratospheric Observatory for Infrared Astronomy (SOFIA). This first airborne occultation observation since 1995 with the Kuiper Airborne Observatory resulted in the best occultation chords recorded for the event, in three visible wavelength bands. The data obtained from SOFIA are combined with chords obtained from the ground at the IRTF, the U. S. Naval Observatory Flagstaff Station, and Leeward Community College to give the detailed state of the Pluto-Charon system at the time of the event with a focus on Pluto's atmosphere. The data show a return to the distinct upper and lower atmospheric regions with a knee or kink in the light curve separating them as was observed in 1988, rather than the smoothly transitioning bowl-shaped light curves of recent years. The upper atmosphere is analyzed by fitting a model to all of the light curves, resulting in a half-light radius of 1288 +/- 1 km. The lower atmosphere is analyzed using two different methods to provide results under the differing assumptions of particulate haze and a strong thermal gradient as causes for the lower atmospheric diminution of flux. These results are compared with those from past occultations to provide a picture of Pluto's evolving atmosphere. Regardless of which lower atmospheric structure is assumed, results indicate that this part of the atmosphere evolves on short timescales with results changing the light curve structures between 1988 and 2006, and then reverting these changes in 2011 though at significantly higher pressures. Throughout these changes, the upper atmosphere remains remarkably stable in structure, again except for the overall pressure changes. No evidence of onset of atmospheric collapse predicted by frost migration models is seen, and the atmosphere appears to be remaining at a stable pressure level, suggesting it should persist at this full level through New Horizon's flyby in 2015. C1 [Person, M. J.; Bosh, A. S.; Levine, S. E.; Gulbis, A. A. S.; Zangari, A. M.; Zuluaga, C. A.; Sallum, S.; Springmann, A.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Dunham, E. W.; Levine, S. E.; Collins, P.; Bida, T.; Bright, L.] Lowell Observ, Flagstaff, AZ 86001 USA. [Gulbis, A. A. S.] S African Astron Observ, ZA-7935 Cape Town, South Africa. [Pasachoff, J. M.; Babcock, B. A.; Pandey, S.; Amrhein, D.; Lucas, R.] Williams Coll Hopkins Observ, Williamstown, MA USA. [Amrhein, D.] Wesleyan Univ, Middletown, CT USA. [Sallum, S.; Best, W.] Univ Arizona, Steward Observ, Tucson, AZ USA. [Tholen, D. J.; Micheli, M.] Univ Hawaii, Inst Astron, Manoa, HI USA. [Taylor, B.] Boston Univ, Boston, MA 02215 USA. [Wolf, J.; Pfueller, E.; Wiedemann, M.; Roeser, H. -P.] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany. [Wolf, J.; Meyer, A.; Pfueller, E.; Wiedemann, M.] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Kakkala, M.] Leeward Community Coll, Pearl City, HI USA. [Ciotti, J.; Plunkett, S.; Hiraoka, N.] Windward Community Coll, Kaneohe, HI USA. [Pilger, E. J.] Hawaii Geophys & Planetol, Honolulu, HI USA. [Hicks, M.; Thackeray, B.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Emery, J. P.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN USA. [Tilleman, T.; Harris, H.] US Naval Observ Flagstaff Stn, Flagstaff, AZ USA. [Sheppard, S.] Carnegie Inst Sci, Washington, DC USA. [Rapoport, S.] Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, Australia. [Ritchie, I.; Pearson, M.] EOS Space Syst, Sydney, NSW, Australia. [Mattingly, A.] IBM Corp, St Leonards, NSW, Australia. [Brimacombe, J.] James Cook Univ, Cairns, Qld, Australia. [Gault, D.] Int Occultat Timing Assoc, Sydney, NSW, Australia. [Nolthenius, R.] Cabrillo Observ, Aptos, CA USA. [Barry, T.] Univ Western Sydney, Penrith Observ, Sydney, NSW, Australia. RP Person, MJ (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. EM mjperson@mit.edu OI Springmann, Alessondra/0000-0001-6401-0126; Micheli, Marco/0000-0001-7895-8209 FU NASA [NNX10AB27G, NNX08AO50G, NNH11ZDA001N, NAS2-97001]; USRA grant [8500-98-003]; Deutsches SOFIA Institut (DSI) [50 OK 0901]; National Research Foundation of South Africa; Research Experiences for Undergraduates program of the National Science Foundation [AST-1005024] FX This work was supported in part by NASA Planetary Astronomy grants NNX10AB27G to MIT, NNX08AO50G and NNH11ZDA001N to Williams College, and USRA grant #8500-98-003 to Lowell Observatory.; This research is based in part on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). SOFIA is jointly operated by the Universities Space Research Association, Inc. (USRA) under NASA contract NAS2-97001 and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901 to the University of Stuttgart.; A. A. S. G. acknowledges funding from the National Research Foundation of South Africa. A. A. S. G. and J.P.E. were visiting astronomers at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. D. A. was a Keck Northeast Astronomy Consortium Summer Fellow, supported by the Research Experiences for Undergraduates program of the National Science Foundation under grant AST-1005024. NR 50 TC 14 Z9 14 U1 0 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 2013 VL 146 IS 4 AR 83 DI 10.1088/0004-6256/146/4/83 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 218AL UT WOS:000324404800012 ER PT J AU Petty, SM Neill, JD Jarrett, TH Blain, AW Farrah, DG Rich, RM Tsai, CW Benford, DJ Bridge, CR Lake, SE Masci, FJ Wright, EL AF Petty, S. M. Neill, J. D. Jarrett, T. H. Blain, A. W. Farrah, D. G. Rich, R. M. Tsai, C. -W. Benford, D. J. Bridge, C. R. Lake, S. E. Masci, F. J. Wright, E. L. TI UV-BRIGHT NEARBY EARLY-TYPE GALAXIES OBSERVED IN THE MID-INFRARED: EVIDENCE FOR A MULTI-STAGE FORMATION HISTORY BY WAY OF WISE AND GALEX IMAGING SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: formation; infrared: galaxies; ultraviolet: galaxies ID RECENT STAR-FORMATION; STANDARD STELLAR LIBRARY; INITIAL MASS FUNCTION; GIANT BRANCH STARS; TP-AGB MODELS; ELLIPTIC GALAXIES; SAURON PROJECT; EVOLUTIONARY SYNTHESIS; ULTRAVIOLET-RADIATION; DISK GALAXIES AB In the local universe, 10% of massive elliptical galaxies are observed to exhibit a peculiar property: a substantial excess of ultraviolet emission than what is expected from their old, red stellar populations. Several origins for this ultraviolet excess (UVX) have been proposed including a population of hot young stars and a population of old, blue horizontal branch or extended horizontal branch (BHB or EHB) stars that have undergone substantial mass loss from their outer atmospheres. We explore the radial distribution of UVX in a selection of 49 nearby E/S0-type galaxies by measuring their extended photometry in the UV through mid-infrared (mid-IR) with the Galaxy Evolution Explorer (GALEX), the Sloan Digital Sky Survey, and the Wide-field Infrared Survey Explorer (WISE). We compare UV/optical and UV/mid-IR colors with the Flexible Stellar Population Synthesis models, which allow for the inclusion of EHB stars. We find that combined WISE mid-IR and GALEX UV colors are more effective in distinguishing models than optical colors, and that the UV/mid-IR combination is sensitive to the EHB fraction. There are strong color gradients, with the outer radii bluer than the inner half-light radii by similar to 1 mag. This color difference is easily accounted for with an increase in the BHB fraction of 0.25 with radius. We estimated that the average ages for the inner and outer radii are 7.0 +/- 0.3 Gyr, and 6.2 +/- 0.2 Gyr, respectively, with the implication that the outer regions are likely to have formed similar to 1 Gyr after the inner regions. Additionally, we find that metallicity gradients are likely not a significant factor in the color difference. The separation of color between the inner and outer regions, which agrees with a specific stellar population difference (e. g., higher EHB populations), and the similar to 0.5-2 Gyr age difference suggests multi-stage formation. Our results are best explained by inside-out formation: rapid star formation within the core at early epochs (>4 Gyr ago) and at least one later stage starburst event coinciding with z similar to 1. C1 [Petty, S. M.; Farrah, D. G.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Petty, S. M.; Rich, R. M.; Lake, S. E.; Wright, E. L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Neill, J. D.; Bridge, C. R.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Jarrett, T. H.; Tsai, C. -W.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa. [Blain, A. W.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Benford, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Masci, F. J.] CALTECH, IPAC, Pasadena, CA 91125 USA. RP Petty, SM (reprint author), Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. RI Benford, Dominic/D-4760-2012 OI Benford, Dominic/0000-0002-9884-4206 FU National Aeronautics and Space Administration; NASA [NAS5-98034]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX We thank the anonymous referee for thorough comments that greatly improved this paper. We thank Marcio Catelan for discussions on evolved stellar populations, and D. Stern for numerous insights into the discussion of galaxy evolution. We also thank R. Assef for his feedback on the analysis and early development of this project. 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. The publication is based on observations made with the NASA Galaxy Evolution Explorer. GALEX is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. This publication makes use of data products from the Sloan Digital Sky Survey. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. 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 Web site is http://www.sdss.org/. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the NASA/IPAC 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 74 TC 5 Z9 5 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 2013 VL 146 IS 4 AR 77 DI 10.1088/0004-6256/146/4/77 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 218AL UT WOS:000324404800006 ER PT J AU Cochran, P Huntington, OH Pungowiyi, C Tom, S Chapin, FS Huntington, HP Maynard, NG Trainor, SF AF Cochran, Patricia Huntington, Orville H. Pungowiyi, Caleb Tom, Stanley Chapin, F. Stuart, III Huntington, Henry P. Maynard, Nancy G. Trainor, Sarah F. TI Indigenous frameworks for observing and responding to climate change in Alaska SO CLIMATIC CHANGE LA English DT Article ID INTERIOR ALASKA; RESPIRATORY-TRACT; VULNERABILITY; IMPACTS; ADAPTATION; KNOWLEDGE; WATER; COMMUNITIES; RESILIENCE; CANADA AB Despite a keen awareness of climate change, northern Indigenous Peoples have had limited participation in climate-change science due to limited access, power imbalances, and differences in worldview. A western science emphasis on facts and an indigenous emphasis on relationships to spiritual and biophysical components indicate important but distinct contributions that each knowledge system can make. Indigenous communities are experiencing widespread thawing of permafrost and coastal erosion exacerbated by loss of protective sea ice. These climate-induced changes threaten village infrastructure, water supplies, health, and safety. Climate-induced habitat changes associated with loss of sea ice and with landscape drying and extensive wildfires interact with northern development to bring both economic opportunities and environmental impacts. A multi-pronged approach to broadening indigenous participation in climate-change research should: 1) engage communities in designing climate-change solutions; 2) create an environment of mutual respect for multiple ways of knowing; 3) directly assist communities in achieving their adaptation goals; 4) promote partnerships that foster effective climate solutions from both western and indigenous perspectives; and 5) foster regional and international networking to share climate solutions. C1 [Cochran, Patricia] Alaska Native Sci Commiss, Anchorage, AK 99524 USA. [Huntington, Orville H.] Tanana Chiefs Conf, Wildlife & Pk, Fairbanks, AK 99701 USA. [Tom, Stanley] Newtok Village Council, Newtok, AK 99559 USA. [Chapin, F. Stuart, III] Univ Alaska Fairbanks, Inst Arctic Biol, Fairbanks, AK 99775 USA. [Maynard, Nancy G.] NASA, Cryospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Trainor, Sarah F.] Univ Alaska Fairbanks, Alaska Ctr Climate Assessment & Policy, Fairbanks, AK 99775 USA. RP Chapin, FS (reprint author), Univ Alaska Fairbanks, Inst Arctic Biol, Fairbanks, AK 99775 USA. EM terry.chapin@alaska.edu RI Brooks, Katya/J-4975-2014; OI Chapin III, F Stuart/0000-0002-2558-9910 NR 67 TC 21 Z9 21 U1 6 U2 72 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0165-0009 EI 1573-1480 J9 CLIMATIC CHANGE JI Clim. Change PD OCT PY 2013 VL 120 IS 3 SI SI BP 557 EP 567 DI 10.1007/s10584-013-0735-2 PG 11 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 216HB UT WOS:000324271700005 ER PT J AU Williams, LJ Campbell, MD Tsang, PCW Sulikowski, JA AF Williams, Laura Jay Campbell, Matthew D. Tsang, Paul C. W. Sulikowski, James A. TI Using estradiol and progesterone concentrations to assess individual variability in the reproductive cyclicity of captive female little skates, Leucoraja erinacea, from the western Gulf of Maine SO FISH PHYSIOLOGY AND BIOCHEMISTRY LA English DT Article DE Life history; Radioimmunoassay; Rajidae; Steroid hormones ID STEROID-HORMONES; SEXUAL-MATURITY; RAJA-ERINACEA; SERUM CONCENTRATIONS; SQUALUS-ACANTHIAS; EXTINCTION VULNERABILITY; VIVIPAROUS DOGFISH; AMBLYRAJA-RADIATA; ATLANTIC STINGRAY; GONAD DEVELOPMENT AB In the current study, plasma steroid hormones were used to assess the individual variability of Leucoraja erinacea over the course of 12 months, in hopes of further defining its reproductive cycle. No statistical differences in hormone concentrations were observed between the isolated and non-isolated female skates. Monthly E-2 concentrations ranged from 1,430 pg ml(-1) in August to 3,940 pg ml(-1) in March, indicating the presence of mature ovarian follicles and supporting the conclusions from previous studies that L. erinacea is capable of reproducing year-round. Concentrations of E-2 were significantly elevated or depressed during some months (February, March, June, July, August, and September) of the year, suggesting that reproductive activity may vary over the annual cycle. Even though monthly P-4 concentrations were highly variable, ranging from 82 pg ml(-1) in November to 816 pg ml(-1) in September, no significant reproductive peaks were observed. In addition, a persistently large variation in E-2 and P-4 concentrations, indicative of reproductive asynchrony within (mean CV 62 % and CV 69 %, respectively) and between (mean range CV 78 and 125 %, respectively) individual skates, was observed throughout the study. Collectively, the continually high E-2 concentrations and variability in both hormones observed in the current study are indicative of an oviparous species that reproduces actively throughout the year. However, the weekly sampling frequency revealed that plasma E-2 concentrations, not P-4, were more useful to assess reproductive status in asynchronous continuously breeding oviparous elasmobranchs. C1 [Williams, Laura Jay; Sulikowski, James A.] Univ New England, Ctr Marine Sci, Biddeford, ME 04005 USA. [Campbell, Matthew D.] Mississippi Labs, Natl Marine Fisheries Serv, Pascagoula, MS 39564 USA. [Tsang, Paul C. W.] Univ New Hampshire, Dept Cellular Mol & Biomed Sci, Durham, NH 03824 USA. RP Williams, LJ (reprint author), Univ New England, Ctr Marine Sci, 11 Hills Beach Rd, Biddeford, ME 04005 USA. EM laurajaywilliams@gmail.com OI Campbell, Matthew/0000-0002-0087-5291 FU University of New England's Graduate School and Marine Science Center FX We would like to thank captain J. Jurek of the F.V. "Mystique Lady" and Puggy Jr. of the F.V. "Lady Victoria'' for collection of the little skates and the University of New England's Graduate School and Marine Science Center for funding and use of the wet laboratory facilities. We would also like to extend our gratitude to K. Coutre, R. Knotek, C. Peterson, and A. Traverse-Taylor for assisting with the collection and processing of samples and Dr. David Koester for his thoughtful review of this manuscript. This manuscript represents MSC contribution number 48. NR 42 TC 2 Z9 2 U1 2 U2 14 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0920-1742 J9 FISH PHYSIOL BIOCHEM JI Fish Physiol. Biochem. PD OCT PY 2013 VL 39 IS 5 BP 1089 EP 1099 DI 10.1007/s10695-012-9766-2 PG 11 WC Biochemistry & Molecular Biology; Fisheries; Physiology SC Biochemistry & Molecular Biology; Fisheries; Physiology GA 217EL UT WOS:000324339500004 PM 23307173 ER PT J AU Kawai, J Jagota, S Kaneko, T Obayashi, Y Yoshimura, Y Khare, BN Deamer, DW McKay, CP Kobayashi, K AF Kawai, Jun Jagota, Seema Kaneko, Takeo Obayashi, Yumiko Yoshimura, Yoshitaka Khare, Bishun N. Deamer, David W. McKay, Christopher P. Kobayashi, Kensei TI Self-assembly of tholins in environments simulating Titan liquidospheres: implications for formation of primitive coacervates on Titan SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY LA English DT Article DE coacervates; liquidosphere; self-assembly; tholin; Titan ID INTERNAL STRUCTURE; MASS-SPECTROMETRY; ORGANIC-MATTER; AMINO-ACIDS; EARLY EARTH; ATMOSPHERE; SURFACE; HAZE; AEROSOLS; SYSTEM AB Titan, the largest satellite of Saturn, has a thick atmosphere containing nitrogen and methane. A variety of organic compounds have been detected in the atmosphere, most likely produced when atmospheric gases are exposed to ultraviolet light, electrons captured by the magnetosphere of Saturn and cosmic rays. The Cassini/Huygens probe showed that the average temperature on the surface of Titan is 93.7 K, with lakes of liquid ethane and methane. Sub-surface mixtures of liquid ammonia and water may also be present. We have synthesized complex organic compounds (tholins) by exposing a mixture of nitrogen and methane to plasma discharges, and investigated their interactions with several different liquids that simulate Titan's liquidosphere. We found that coacervates formed when tholins were extracted in non-polar solvents followed by exposure to aqueous ammonia solutions. The results suggest that coacervates can self-assemble in Titan's liquidosphere which have the potential to undergo further chemical evolution. Similar processes are likely to occur in the early evolution of habitable planets when tholin-like compounds undergo phase separation into microscopic structures dispersed in a suitable aqueous environment. C1 [Kawai, Jun; Kaneko, Takeo; Obayashi, Yumiko; Kobayashi, Kensei] Yokohama Natl Univ, Dept Chem & Biotechnol, Hodogaya Ku, Yokohama, Kanagawa 2408501, Japan. [Jagota, Seema; Khare, Bishun N.; McKay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Yoshimura, Yoshitaka] Tamagawa Univ, Dept Life Sci, Machida, Tokyo 1948600, Japan. [Deamer, David W.] Univ Calif Santa Cruz, Jack Baskin Sch Engn, Santa Cruz, CA 95064 USA. RP Kawai, J (reprint author), Yokohama Natl Univ, Dept Chem & Biotechnol, Hodogaya Ku, Yokohama, Kanagawa 2408501, Japan. EM kawai-jun-jy@ynu.ac.jp OI Kobayashi, Kensei/0000-0003-2951-1341; Kaneko, Takeo/0000-0002-8904-1030 NR 55 TC 3 Z9 3 U1 1 U2 22 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1473-5504 EI 1475-3006 J9 INT J ASTROBIOL JI Int. J. Astrobiol. PD OCT PY 2013 VL 12 IS 4 BP 282 EP 291 DI 10.1017/S1473550413000116 PG 10 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 220NH UT WOS:000324590800002 ER PT J AU Davila, AF Willson, D Coates, JD Mckay, CP AF Davila, Alfonso F. Willson, David Coates, John D. Mckay, Christopher P. TI Perchlorate on Mars: a chemical hazard and a resource for humans SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY LA English DT Article DE hazards; ISRU; Mars; oxygen; perchlorate (ClO4-) AB Perchlorate (ClO4-) is widespread in Martian soils at concentrations between 0.5 and 1%. At such concentrations, perchlorate could be an important source of oxygen, but it could also become a critical chemical hazard to astronauts. In this paper, we review the dual implications of ClO4- on Mars, and propose a biochemical approach for removal of perchlorate from Martian soil that would be energetically cheap, environmentally friendly and could be used to obtain oxygen both for human consumption and to fuel surface operations. C1 [Davila, Alfonso F.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Davila, Alfonso F.; Willson, David; Mckay, Christopher P.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Coates, John D.] Univ Calif Berkeley, Dept Plant & Microbial Biol, Berkeley, CA 94720 USA. RP Davila, AF (reprint author), SETI Inst, Carl Sagan Ctr, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA. EM adavila@seti.org RI Davila, Alfonso/A-2198-2013 OI Davila, Alfonso/0000-0002-0977-9909 NR 17 TC 15 Z9 15 U1 4 U2 28 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1473-5504 J9 INT J ASTROBIOL JI Int. J. Astrobiol. PD OCT PY 2013 VL 12 IS 4 BP 321 EP 325 DI 10.1017/S1473550413000189 PG 5 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 220NH UT WOS:000324590800007 ER PT J AU Baker, MR Gobush, KS Vynne, CH AF Baker, Matthew R. Gobush, Kathleen S. Vynne, Carly H. TI Review of factors influencing stress hormones in fish and wildlife SO JOURNAL FOR NATURE CONSERVATION LA English DT Review DE Corticosterone; Cortisol; Environmental disturbance; Glucocorticoids ID CONSERVATION PHYSIOLOGY; GLUCOCORTICOIDS; INDICATORS; MANAGEMENT; RESPONSES; ECOLOGY AB Conservation efforts to better understand how wildlife populations respond to environmental change and anthropogenic disturbance has led to a proliferation of research examining physiological indicators of stress response in wildlife. Glucocorticoid stress hormones (GCs), typically cortisol and corticosterone, are among the most frequently measured indicators of the vertebrate stress response. To review the current state of research on stress physiology of free-ranging animals and its application to conservation, we canvassed more than 1000 articles on GC measures in wildlife published since 1969. For 454 studies published since 1990, we assessed the most commonly analysed correlates and disturbances and conducted a meta-analysis on commonly studied species. We noted a prominent divide in the legacies of fish-related analyses and those of higher order vertebrates and the need and opportunity to transfer knowledge between fields. Fish studies most frequently measured physiological indicators, condition, and the relationship between stress and mortality, whereas other vertebrate studies most frequently measured reproduction, condition, and environmental correlates. Correlates that significantly influenced GC levels across all vertebrate groups and are thus important to control for in study design and analyses include density and dispersal of conspecifics, season, reproductive status, and social status. Consistent trends across commonly studied species included positive GC response to capture and handling, reduced GC response related to acclimation, and a lack of correlation between condition and baseline GC levels. Our synthesis within and across diverse taxonomic orders reveals substantial research coverage but a lack of depth in multivariate analyses and a disparity in how correlates are controlled. This paper provides a comprehensive assessment of correlates and disturbances that influence GC measures and, as such, has useful applications to assist conservation physiologists in study design, analysis, and interpretation. (C) 2013 Elsevier GmbH. All rights reserved. C1 [Baker, Matthew R.] NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Seattle, WA 98115 USA. [Gobush, Kathleen S.] NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96814 USA. [Vynne, Carly H.] Natl Fish & Wildlife Fdn, Washington, DC 20005 USA. RP Baker, MR (reprint author), NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 7600 Sand Point Way NE,Bldg 4, Seattle, WA 98115 USA. EM Matthew.Baker@noaa.gov; kathleen.gobush@noaa.gov; Carly.Vynne@nfwf.org NR 33 TC 25 Z9 25 U1 9 U2 130 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 1617-1381 J9 J NAT CONSERV JI J. Nat. Conserv. PD OCT PY 2013 VL 21 IS 5 BP 309 EP 318 DI 10.1016/j.jnc.2013.03.003 PG 10 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 213DO UT WOS:000324034700007 ER PT J AU Hilker, T Hall, FG Coops, NC Collatz, JG Black, TA Tucker, CJ Sellers, PJ Grant, N AF Hilker, Thomas Hall, Forrest G. Coops, Nicholas C. Collatz, James G. Black, T. Andrew Tucker, Compton J. Sellers, Piers J. Grant, Nicholas TI Remote sensing of transpiration and heat fluxes using multi-angle observations SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Multi-angle remote sensing AMSPEC; GPP; Transpiration; Ball-Berry relationship; Stomatal conductance ID LIGHT-USE EFFICIENCY; SURFACE-ENERGY BALANCE; WATER-VAPOR EXCHANGE; DOUGLAS-FIR FOREST; SATELLITE DATA; PARAMETERIZATION SIB2; STOMATAL CONDUCTANCE; MODEL FORMULATION; ATMOSPHERIC GCMS; BOUNDARY-LAYER AB Surface energy balance is a major determinant of land surface temperature and the Earth's climate. To date, there is no approach that can produce effective, physically consistent, global and multi-decadal energy-water flux data over land. Net radiation (R-n) can be quantified regionally using satellite retrievals of surface reflectance and thermal emittance with errors <10%. However, consistent, useful retrieval of latent heat flux (lambda E) from remote sensing is not yet possible. In theory, lambda E could be inferred as a residual of R-n, ground heat (G) and sensible heat (H) fluxes (R-n-H-G). However, large uncertainties in remote sensing of both H and G result in low accuracies for lambda E. Where vegetation is the dominant surface cover, lambda E is largely driven by transpiration of intercellular water through leaf stomata during the photosynthetic uptake of carbon. In these areas, satellite retrievals of photosynthesis (GPP) could be used to quantify transpiration rates through stomatal conductance. Here, we demonstrate how remote sensing of GPP could be applied to obtain lambda E from passive optical measurements of vegetation leaf reflectance related to the photosynthetic rate independent of knowledge of H, R-n and G. We validate the algorithm using five structurally and physiologically diverse eddy flux sites in western and central Canada. Results show that transpiration and H were accurately predicted from optical data and highly significant relationships were found between the energy budget obtained from eddy flux measurements and remote sensing (0.64 <= r(2) <= 0.85). We conclude that spaceborne estimates of GPP could significantly improve not only estimates of the carbon balance but also the energy balance over land. (c) 2013 Elsevier Inc. All rights reserved. C1 [Hilker, Thomas] Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA. [Hall, Forrest G.; Collatz, James G.; Tucker, Compton J.; Sellers, Piers J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Coops, Nicholas C.] Univ British Columbia, Fac Forest Resources Mgmt, Vancouver, BC V6T 1Z4, Canada. [Grant, Nicholas] Univ British Columbia, Fac Land & Food Syst, Vancouver, BC V6T 1Z4, Canada. RP Hilker, T (reprint author), Oregon State Univ, Coll Forestry, 231 Peavy Hall, Corvallis, OR 97331 USA. EM thomas.hilker@oregonstate.edu RI collatz, george/D-5381-2012; Coops, Nicholas/J-1543-2012 OI Coops, Nicholas/0000-0002-0151-9037 FU Canadian Carbon Program (Canadian Foundation for Climate and Atmospheric Science (CFCAS); Natural Sciences and Engineering Research Council of Canada (NSERC); BIOCAP; NSERC-Accelerator grant FX Thank you to Zoran Nesic, Dominic Lessard, Andrew Hum and Rick Ketler from UBC Faculty of Land and Food Systems (LFS) for their assistance in technical design, installation, and maintenance of Amspec and Amspec II. Mathew Brown is thanked for analyzing the EC data. The quality control for the climate data at SOA was done by Alan Barr. This research was partially funded by the Canadian Carbon Program (Canadian Foundation for Climate and Atmospheric Science (CFCAS), the Natural Sciences and Engineering Research Council of Canada (NSERC) and BIOCAP, and an NSERC-Accelerator grant to Coops. NR 58 TC 10 Z9 11 U1 2 U2 62 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD OCT PY 2013 VL 137 BP 31 EP 42 DI 10.1016/j.rse.2013.05.023 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 214SR UT WOS:000324156600004 ER PT J AU Tang, WQ Yueh, S Fore, A Neumann, G Hayashi, A Lagerloef, G AF Tang, Wenqing Yueh, Simon Fore, Alexander Neumann, Gregory Hayashi, Akiko Lagerloef, Gary TI The rain effect on Aquarius' L-band sea surface brightness temperature and radar backscatter SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Aquarius; L-band; Radiometer; Radar; Rain effect ID WESTERN EQUATORIAL PACIFIC; GENERATED RING-WAVES; WATER SURFACES; SCATTEROMETER MEASUREMENTS; DIELECTRIC-CONSTANT; OCEAN ALGORITHM; SALINITY; SCATTERING; RADIOMETER; CHALLENGE AB We analyze the surface emissivity and radar backscatter measured by the Aquarius L-band radiometer and scatterometer under rainy conditions. The residual signals due to rain are derived from measurements after accounting for roughness due to wind and flat surface emissivity. The wind roughness is accounted for by a geophysical model function (GMF) built using rain-free data. Using more than one year of Aquarius data collocated with SSMI/S, WindSAT rain rate and NCEP wind, our analysis reveals rain rate dependence in radar backscatter and surface emissivity, which become increasingly significant as the wind speed approaches zero and not significant above 15 m s(-1). The effect of rain on radar backscatter is dominated by raindrop splashing as indicated by the incidence angle dependence and polarization characteristics of the residuals. (c) 2013 Elsevier Inc. All rights reserved. C1 [Tang, Wenqing; Yueh, Simon; Fore, Alexander; Neumann, Gregory; Hayashi, Akiko] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lagerloef, Gary] Earth & Space Res, Seattle, WA USA. RP Tang, WQ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 300-323, Pasadena, CA 91109 USA. EM wenqing.tang@jpl.nasa.gov FU National Aeronautics and Space Administration FX The work 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 41 TC 22 Z9 22 U1 0 U2 21 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 OCT PY 2013 VL 137 BP 147 EP 157 DI 10.1016/j.rse.2013.06.016 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 214SR UT WOS:000324156600013 ER PT J AU Aurin, D Mannino, A Franz, B AF Aurin, Dirk Mannino, Antonio Franz, Bryan TI Spatially resolving ocean color and sediment dispersion in river plumes, coastal systems, and continental shelf waters SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Ocean color; Coastal oceanography; Satellite remote sensing; Spatial resolution; Atmospheric correction; Total suspended material ID AEROSOL OPTICAL-THICKNESS; TOTAL SUSPENDED MATTER; CHESAPEAKE BAY; ATMOSPHERIC CORRECTION; AMAZON RIVER; VARIABILITY; SEAWIFS; SEA; RETRIEVAL; ALGORITHM AB Satellite remote sensing of ocean color in dynamic coastal, inland, and nearshore waters is impeded by high variability in optical constituents, demands specialized atmospheric correction, and is limited by instrument sensitivity. To accurately detect dispersion of bio-optical properties, remote sensors require ample signal-to-noise ratio (SNR) to sense small variations in ocean color without saturating over bright pixels, an atmospheric correction that can accommodate significant water-leaving radiance in the near infrared (NIR), and spatial and temporal resolution that coincides with the scales of variability in the environment. Several current and historic space-borne sensors have met these requirements with success in the open ocean, but are not optimized for highly red-reflective and heterogeneous waters such as those found near river outflows or in the presence of sediment resuspension. Here we apply analytical approaches for determining optimal spatial resolution, dominant spatial scales of variability ("patches"), and proportions of patch variability that can be resolved from four river plumes around the world between 2008 and 2011. An offshore region in the Sargasso Sea is analyzed for comparison. A method is presented for processing Moderate Resolution Imaging Spectroradiometer (MODIS) Aqua and Terra imagery including cloud detection, stray light masking, faulty detector avoidance, and dynamic aerosol correction using short-wave- and near-infrared wavebands in extremely turbid regions which pose distinct optical and technical challenges. Results show that a pixel size of similar to 520 m or smaller is generally required to resolve spatial heterogeneity in ocean color and total suspended materials in river plumes. Optimal pixel size increases with distance from shore to similar to 630 m in nearshore regions, similar to 750 m on the continental shelf, and similar to 1350 m in the open ocean. Greater than 90% of the optical variability within plume regions is resolvable with 500 m resolution, and small, but significant, differences were found between peak and nadir river flow periods in terms of optimal resolution and resolvable proportion of variability. (c) 2013 Elsevier Inc. All rights reserved. C1 [Aurin, Dirk] NASA, Sci Syst & Applicat Inc, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Aurin, Dirk; Mannino, Antonio; Franz, Bryan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Aurin, D (reprint author), NASA, Sci Syst & Applicat Inc, Goddard Space Flight Ctr, Code 616,Bldg 22,Rm 248, Greenbelt, MD 20771 USA. EM dirk.a.aurin@nasa.gov RI Mannino, Antonio/I-3633-2014; Franz, Bryan/D-6284-2012 OI Franz, Bryan/0000-0003-0293-2082 FU NASA GEO-CAPE mission pre-formulation activity FX The authors wish to especially thank Michael Ondrusek at NOAA/NESDIS/STAR/SOCD for providing field measurements of TSM following T.S. Lee. Thanks also to Xiaoxiong Xiong and Amit Angal of the NASA MODIS Characterization Support Team (MCST), and to Gerhardt Meister of the NASA Ocean Biology Processing Group (OBPG) for providing detailed on-orbit characterization of detector-specific noise levels. Thanks to all those from OBPG and elsewhere who advised via the NASA Ocean Color forum, particularly Sean Bailey and Gerhard Meister. Funding was provided by the NASA GEO-CAPE mission pre-formulation activity. NR 38 TC 12 Z9 12 U1 1 U2 71 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 OCT PY 2013 VL 137 BP 212 EP 225 DI 10.1016/j.rse.2013.06.018 PG 14 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 214SR UT WOS:000324156600018 ER PT J AU Thompson, DR Juarez, MD Barker, CM Holeman, J Lundeen, S Mulligan, S Painter, TH Podest, E Seidel, FC Ustinov, E AF Thompson, David R. Juarez, Manuel de la Torre Barker, Christopher M. Holeman, Jodi Lundeen, Sarah Mulligan, Steve Painter, Thomas H. Podest, Erika Seidel, Felix C. Ustinov, Eugene TI Airborne imaging spectroscopy to monitor urban mosquito microhabitats SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Imaging spectroscopy; Disease vector control; West Nile virus; Green swimming pools; Matched filter detection; Urban environments ID WEST NILE VIRUS; SWIMMING POOLS; WATER; REFLECTANCE; CHLOROPHYLL; AVIRIS; RESOLUTION; FEATURES; IMAGERY; MODELS AB West Nile (WNV) is now established in the continental United States with new human cases occurring annually in most states. Mosquitoes in the genus Culex are the primary vectors and exploit urban stagnant water and swimming pools as larval habitats. Public health surveys to monitor unmaintained pools typically rely on visual inspections of aerial imagery. This work demonstrates automated analysis of airborne imaging spectroscopy to assist Culex monitoring campaigns. We analyze an overflight of Fresno County, CA by the Airborne Visible Infrared Imaging Spectrometer instrument (AVIRIS), and compare the spectral information with a concurrent ground survey of swimming pools. Matched filter detection strategies reliably detect pools against a cluttered urban background. We also evaluate remotely sensed spectral markers of ecosystem characteristics related to larval colonization. We find that commonly used chlorophyll signatures accurately predict the probability of pool colonization by Culex larvae. These results suggest that AVIRIS spectral data provide sufficient information to remotely identify pools at risk for Culex colonization. Published by Elsevier Inc. C1 [Thompson, David R.; Juarez, Manuel de la Torre; Lundeen, Sarah; Painter, Thomas H.; Podest, Erika; Seidel, Felix C.; Ustinov, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Barker, Christopher M.] Univ Calif Davis, Ctr Vectorborne Dis, Davis, CA 95616 USA. [Holeman, Jodi; Mulligan, Steve] Consolidated Mosquito Abatement Dist, Selma, CA USA. RP Juarez, MD (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM david.r.thompson@jpl.nasa.govemail; mtj@jpl.nasa.govemail; cmbarker@ucdavis.edu RI Ustinov, Eugene/D-1350-2015; Painter, Thomas/B-7806-2016; OI Ustinov, Eugene/0000-0003-0227-4286; Seidel, Felix/0000-0002-4282-2198 FU Jet Propulsion Laboratory Research and Technology Development Grant; CDC, Climate Change: Environmental Impact on Human Health [U01 EH000418]; Research and Policy for Infectious Disease Dynamics (RAPIDD) program of the Science and Technology Directorate, Department of Homeland Security; Fogarty International Center, National Institutes of Health; U.S. Government FX We thank Joao Teixeira, Robert Staehle, and Michael Gunson whose suggestions and support contributed significantly to this research. This work was supported by a Jet Propulsion Laboratory Research and Technology Development Grant. AVIRIS data is available courtesy NASA and the Jet Propulsion Laboratory. The Consolidated Mosquito Abatement District provided spatial data on swimming pool conditions. The aerial image in this article was provided courtesy Russ Parman and the Santa Clara County Vector Control District, and Robert Franklin of Aerial Services, a division of TeamBuilders, Inc. C. M. Barker is supported by grant U01 EH000418 from CDC, Climate Change: Environmental Impact on Human Health, and by the Research and Policy for Infectious Disease Dynamics (RAPIDD) program of the Science and Technology Directorate, Department of Homeland Security and Fogarty International Center, National Institutes of Health. Copyright 2013 California Institute of Technology. All Rights Reserved. U.S. Government support acknowledged. NR 35 TC 2 Z9 2 U1 1 U2 27 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD OCT PY 2013 VL 137 BP 226 EP 233 DI 10.1016/j.rse.2013.06.015 PG 8 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 214SR UT WOS:000324156600019 ER PT J AU Neigh, CSR Nelson, RF Ranson, KJ Margolis, HA Montesano, PM Sun, GQ Kharuk, V Naesset, E Wulder, MA Andersen, HE AF Neigh, Christopher S. R. Nelson, Ross F. Ranson, K. Jon Margolis, Hank A. Montesano, Paul M. Sun, Guoqing Kharuk, Viacheslav Naesset, Erik Wulder, Michael A. Andersen, Hans-Erik TI Taking stock of circumboreal forest carbon with ground measurements, airborne and spaceborne LiDAR SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE LiDAR; Biomass; Carbon; Boreal forest ID ICESAT GLAS DATA; LAND-COVER DATABASE; CENTRAL SIBERIA; CLIMATE-CHANGE; ABOVEGROUND BIOMASS; VEGETATION HEIGHT; RUSSIAN FORESTS; HEDMARK COUNTY; BOREAL; MODIS AB The boreal forest accounts for one-third of global forests, but remains largely inaccessible to ground-based measurements and monitoring. It contains large quantities of carbon in its vegetation and soils, and research suggests that it will be subject to increasingly severe climate-driven disturbance. We employ a suite of ground-, airborne- and space-based measurement techniques to derive the first satellite LiDAR-based estimates of aboveground carbon for the entire circumboreal forest biome. Incorporating these inventory techniques with uncertainty analysis, we estimate total aboveground carbon of 38 +/- 3.1 Pg. This boreal forest carbon is mostly concentrated from 50 to 55 degrees N in eastern Canada and from 55 to 60 degrees N in eastern Eurasia. Both of these regions are expected to warm >3 degrees C by 2100, and monitoring the effects of warming on these stocks is important to understanding its future carbon balance. Our maps establish a baseline for future quantification of circumboreal carbon and the described technique should provide a robust method for future monitoring of the spatial and temporal changes of the aboveground carbon content. Published by Elsevier Inc. C1 [Neigh, Christopher S. R.; Nelson, Ross F.; Ranson, K. Jon; Montesano, Paul M.; Sun, Guoqing] NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Margolis, Hank A.] Univ Laval, Ctr Etud Foret, Quebec City, PQ G1V 0A6, Canada. [Montesano, Paul M.] Sigma Space Corp, Lanham, MD 20705 USA. [Montesano, Paul M.; Sun, Guoqing] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Kharuk, Viacheslav] Russian Acad Sci, Sukachev Inst Forest, Krasnoyarsk 660036, Russia. [Naesset, Erik] Norwegian Univ Life Sci, Dept Ecol & Nat Resource Management, NO-1432 As, Norway. [Wulder, Michael A.] Nat Resources Canada, Pacific Forestry Ctr, Canadian Forest Serv, Victoria, BC V82Z 1M5, Canada. [Andersen, Hans-Erik] Univ Washington, US Forest Serv, Pacific NW Res Stn, Seattle, WA 98195 USA. RP Neigh, CSR (reprint author), NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Code 618, Greenbelt, MD 20771 USA. EM Christopher.S.Neigh@nasa.gov RI Neigh, Christopher/D-4700-2012; Ranson, Kenneth/G-2446-2012; Nelson, Ross/H-8266-2014; Wulder, Michael/J-5597-2016 OI Neigh, Christopher/0000-0002-5322-6340; Ranson, Kenneth/0000-0003-3806-7270; Wulder, Michael/0000-0002-6942-1896 FU NASA [NNH08ZDA001N-TE, NNH06ZDA001N-CARBON]; NSERC Discovery Grant FX This study was made possible by NASA's Terrestrial Ecology program under grants NNH08ZDA001N-TE and NNH06ZDA001N-CARBON. We also acknowledge the NSERC Discovery Grant to Hank Margolis for contributing partial support for the airborne data collection in Canada. We would like to thank three anonymous reviewers who improved the quality and content of this manuscript. We would also like to thank Sergi Im, Mukhtar Naurzbaev, Pasha Oskorbin, and Marsha Dvinskaya of the Sukachev Institute of Forest and Bruce Cook from the NASA Goddard Space Flight Center for help in collecting field measurements in Siberia. NR 75 TC 26 Z9 26 U1 2 U2 65 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD OCT PY 2013 VL 137 BP 274 EP 287 DI 10.1016/j.rse.2013.06.019 PG 14 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 214SR UT WOS:000324156600023 ER PT J AU Draper, C Reichle, R de Jeu, R Naeimi, V Parinussa, R Wagner, W AF Draper, Clara Reichle, Rolf de Jeu, Richard Naeimi, Vahid Parinussa, Robert Wagner, Wolfgang TI Estimating root mean square errors in remotely sensed soil moisture over continental scale domains SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Microwave soil moisture; Remotely sensed soil moisture validation; Triple colocation; Error propagation ID OPTICAL DEPTH RETRIEVAL; LAND-SURFACE MODELS; TRIPLE COLLOCATION; ERS SCATTEROMETER; DATA ASSIMILATION; VALIDATION; METHODOLOGY; CATCHMENT; NETWORKS; MISSION AB Root Mean Square Errors (RMSEs) in the soil moisture anomaly time series obtained from the Advanced Scatterometer (ASCAT) and the Advanced Microwave Scanning Radiometer (AMSR-E; using the Land Parameter Retrieval Model) are estimated over a continental scale domain centered on North America, using two methods: triple colocation (RMSETC) and error propagation through the soil moisture retrieval models (RMSEEP). In the absence of an established consensus for the climatology of soil moisture over large domains, presenting a RMSE in soil moisture units requires that it be specified relative to a selected reference data set. To avoid the complications that arise from the use of a reference, the RMSE is presented as a fraction of the local time series standard deviation (fRMSE). For both sensors, the fRMSE(TC) and fRMSE(EP) show similar spatial patterns of relatively high/low errors, and the mean fRMSE for each land cover class is consistent with expectations. Triple colocation is also shown to be surprisingly robust to representativity differences between the soil moisture data sets used, and it is believed to accurately estimate the fRMSE in the remotely sensed soil moisture anomaly time series. Comparing the ASCAT and AMSR-E fRMSE(TC) shows that in general both data sets have good skill over low to moderate vegetation cover. Additionally, they have similar accuracy even when considered by land cover class, although the AMSR-E fRMSEs show a stronger signal of the vegetation cover. (c) 2013 The Authors. Published by Elsevier Inc. All rights reserved. C1 [Draper, Clara; Reichle, Rolf] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Draper, Clara] Univ Space Res Assoc, GESTAR, Columbia, MD USA. [de Jeu, Richard; Parinussa, Robert] Vrije Univ Amsterdam, Fac Earth & Life Sci, Amsterdam, Netherlands. [Naeimi, Vahid] German Aerosp Ctr, German Remote Sensing Data Ctr, Wessling, Germany. [Naeimi, Vahid; Wagner, Wolfgang] Vienna Univ Technol, Dept Geodesy & Geoinformat, A-1040 Vienna, Austria. RP Draper, C (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA. EM clara.draper@nasa.gov RI Reichle, Rolf/E-1419-2012; Draper, Clara/P-6097-2016; OI Draper, Clara/0000-0002-8299-4939; Wagner, Wolfgang/0000-0001-7704-6857 FU NASA Soil Moisture Active Passive mission; NASA program on the Science of Terra and Aqua FX This research was supported by the NASA Soil Moisture Active Passive mission and by the NASA program on the Science of Terra and Aqua. Gabrielle De Lannoy and Qing Liu contributed through many helpful discussions. NR 41 TC 45 Z9 45 U1 4 U2 40 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD OCT PY 2013 VL 137 BP 288 EP 298 DI 10.1016/j.rse.2013.06.013 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 214SR UT WOS:000324156600024 ER PT J AU Mansour, NN Kosovichev, AG Komm, R Longcope, D Leibacher, JW AF Mansour, Nagi N. Kosovichev, Alexander G. Komm, Rudolf Longcope, Dana Leibacher, John W. TI Solar Dynamics and Magnetism from the Interior to the Atmosphere Preface SO SOLAR PHYSICS LA English DT Editorial Material C1 [Mansour, Nagi N.] NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA. [Kosovichev, Alexander G.] Stanford Univ, Stanford, CA 94305 USA. [Komm, Rudolf; Leibacher, John W.] Natl Opt Astron Observ, Natl Solar Observ, Tucson, AZ 85726 USA. [Longcope, Dana] Montana State Univ, Bozeman, MT 59717 USA. [Leibacher, John W.] Inst Astrophys Spatial, Orsay, France. RP Mansour, NN (reprint author), NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA. EM nagi.n.mansour@nasa.gov; sasha@sun.stanford.edu; rkomm@nso.edu; dana@solar.physics.montana.edu; john.leibacher@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD OCT PY 2013 VL 287 IS 1-2 BP 1 EP 7 DI 10.1007/s11207-013-0377-6 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 214FB UT WOS:000324115600001 ER PT J AU Duvall, TL Hanasoge, SM AF Duvall, T. L., Jr. Hanasoge, S. M. TI Subsurface Supergranular Vertical Flows as Measured Using Large Distance Separations in Time-Distance Helioseismology SO SOLAR PHYSICS LA English DT Article DE Helioseismology, observations; Helioseismology, direct modeling; Interior, convective zone; Supergranulation; Velocity fields, interior ID WAVE-LIKE PROPERTIES; SOLAR SUPERGRANULATION; LOCAL HELIOSEISMOLOGY; TRAVEL-TIMES; MODES; SENSITIVITY; SIMULATIONS; INTERIOR; KERNELS AB As large-distance rays (say, 10 -aEuro parts per thousand 24A degrees) approach the solar surface approximately vertically, travel times measured from surface pairs for these large separations are mostly sensitive to vertical flows, at least for shallow flows within a few Mm of the solar surface. All previous analyses of supergranulation have used smaller separations and have been hampered by the difficulty of separating the horizontal and vertical flow components. We find that the large-separation travel times associated with supergranulation cannot be studied using the standard phase-speed filters of time-distance helioseismology. These filters, whose use is based upon a refractive model of the perturbations, reduce the resultant travel-time signal by at least an order of magnitude at some distances. More effective filters are derived. Modeling suggests that the center-annulus travel-time difference [delta t (oi)] in the separation range Delta=10 -aEuro parts per thousand 24(a similar to) is insensitive to the horizontally diverging flow from the centers of the supergranules and should lead to a constant signal from the vertical flow. Our measurement of this quantity, 5.1 +/- 0.1 seconds, is constant over the distance range. This magnitude of the signal cannot be caused by the level of upflow at cell centers seen at the photosphere of 10 m s(-1) extended in depth. It requires the vertical flow to increase with depth. A simple Gaussian model of the increase with depth implies a peak upward flow of 240 m s(-1) at a depth of 2.3 Mm and a peak horizontal flow of 700 m s(-1) at a depth of 1.6 Mm. C1 [Duvall, T. L., Jr.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Hanasoge, S. M.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Hanasoge, S. M.] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. RP Duvall, TL (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. EM Thomas.L.Duvall@nasa.gov; hanasoge@mps.mpg.de FU NASA SDO; NASA SDO Science Center program [SCEX22011D]; NASA [NNX11AB63G] FX The data used here are courtesy of NASA/SDO and the HMI Science Team. We thank the HMI team members for their hard work. This work is supported by NASA SDO and the NASA SDO Science Center program through grant SCEX22011D awarded to NASA GSFC. S. M. H. acknowledges funding from NASA grant NNX11AB63G. NR 33 TC 12 Z9 12 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD OCT PY 2013 VL 287 IS 1-2 BP 71 EP 83 DI 10.1007/s11207-012-0010-0 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 214FB UT WOS:000324115600005 ER PT J AU Liu, Y Zhao, JW Schuck, PW AF Liu, Yang Zhao, Junwei Schuck, P. W. TI Horizontal Flows in the Photosphere and Subphotosphere of Two Active Regions SO SOLAR PHYSICS LA English DT Article DE Solar active regions, photosphere and subphotosphere; Solar active regions, flows ID LOCAL CORRELATION TRACKING; VECTOR MAGNETOGRAMS; MAGNETIC-FIELD; INDUCTION EQUATION; SOLAR ATMOSPHERE; VELOCITY-FIELD; FLUX ROPE; ENERGY; HMI; ALGORITHMS AB We compare horizontal flow fields in the photosphere and in the subphotosphere (a layer 0.5 Mm below the photosphere) in two solar active regions: AR 11084 and AR 11158. AR 11084 is a mature, simple active region without significant flaring activity, and AR 11158 is a multipolar, complex active region with magnetic flux emerging during the period studied. Flows in the photosphere are derived by applying the Differential Affine Velocity Estimator for Vector Magnetograms (DAVE4VM) on HMI-observed vector magnetic fields, and the subphotospheric flows are inferred by time-distance helioseismology using HMI-observed Dopplergrams. Similar flow patterns are found for both layers for AR 11084: inward flows in the sunspot umbra and outward flows surrounding the sunspot. The boundary between the inward and outward flows, which is slightly different in the photosphere and the subphotosphere, is within the sunspot penumbra. The area having inward flows in the subphotosphere is larger than that in the photosphere. For AR 11158, flows in these two layers show great similarities in some areas and significant differences in other areas. Both layers exhibit consistent outward flows in the areas surrounding sunspots. On the other hand, most well-documented flux-emergence-related flow features seen in the photosphere do not have counterparts in the subphotosphere. This implies that the horizontal flows caused by flux emergence do not extend deeply into the subsurface. C1 [Liu, Yang; Zhao, Junwei] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Schuck, P. W.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. RP Liu, Y (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. EM yliu@sun.stanford.edu RI Zhao, Junwei/A-1177-2007 FU NASA [NAS5-02139] FX The authors wish to thank the anonymous referee for the valuable comments and suggestions. This work was supported by NASA Contract NAS5-02139 (HMI) to Stanford University. The data are used courtesy of NASA/SDO and the HMI science team. SOHO is a project of international cooperation between ESA and NASA. NR 35 TC 22 Z9 22 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD OCT PY 2013 VL 287 IS 1-2 BP 279 EP 291 DI 10.1007/s11207-012-0089-3 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 214FB UT WOS:000324115600018 ER PT J AU Panasenco, O Martin, SF Velli, M Vourlidas, A AF Panasenco, Olga Martin, Sara F. Velli, Marco Vourlidas, Angelos TI Origins of Rolling, Twisting, and Non-radial Propagation of Eruptive Solar Events SO SOLAR PHYSICS LA English DT Article DE Coronal mass ejections, low coronal signatures; Coronal mass ejections, initiation and propagation; Magnetic fields, corona; Coronal holes, prominences, formation and evolution; Filaments ID CORONAL MASS EJECTIONS; FILAMENT CHANNELS; STEREOSCOPIC ANALYSIS; PROMINENCE; RECONSTRUCTION; SIMULATIONS; DEFLECTION; EXPANSION; CHIRALITY; FEATURES AB We demonstrate that major asymmetries in erupting filaments and CMEs, namely major twists and non-radial motions are typically related to the larger-scale ambient environment around eruptive events. Our analysis of prominence eruptions observed by the STEREO, SDO, and SOHO spacecraft shows that prominence spines retain, during the initial phases, the thin ribbon-like topology they had prior to the eruption. This topology allows bending, rolling, and twisting during the early phase of the eruption, but not before. The combined ascent and initial bending of the filament ribbon is non-radial in the same general direction as for the enveloping CME. However, the non-radial motion of the filament is greater than that of the CME. In considering the global magnetic environment around CMEs, as approximated by the Potential Field Source Surface (PFSS) model, we find that the non-radial propagation of both erupting filaments and associated CMEs is correlated with the presence of nearby coronal holes, which deflect the erupting plasma and embedded fields. In addition, CME and filament motions, respectively, are guided towards weaker field regions, namely null points existing at different heights in the overlying configuration. Due to the presence of the coronal hole, the large-scale forces acting on the CME may be asymmetric. We find that the CME propagates usually non-radially in the direction of least resistance, which is always away from the coronal hole. We demonstrate these results using both low- and high-latitude examples. C1 [Panasenco, Olga; Martin, Sara F.] Helio Res, La Crescenta, CA 91214 USA. [Velli, Marco] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Vourlidas, Angelos] Naval Res Lab, Div Space Sci, Washington, DC USA. RP Panasenco, O (reprint author), Helio Res, La Crescenta, CA 91214 USA. EM panasenco.olga@gmail.com RI Vourlidas, Angelos/C-8231-2009 OI Vourlidas, Angelos/0000-0002-8164-5948 FU NASA [NNX09AG27G, S-136361-Y]; National Aeronautics and Space Administration FX We are indebted to the SOHO, STEREO/SECCHI and SDO teams. O.P. and S. M. are supported in this research by the NASA grant NNX09AG27G. The work of M. V. was conducted at the Jet Propulsion Laboratory, California Institute of Technology under a contract from the National Aeronautics and Space Administration. A. V. is supported by NASA contract S-136361-Y to the Naval Research Laboratory. SOHO is a mission of international cooperation between ESA and NASA. The SECCHI data are produced by an international consortium of the NRL, LMSAL, and NASA GSFC (USA), RAL and Univ. Birmingham (UK), MPS (Germany), CSL (Belgium), IOTA and IAS (France). The AIA data used here are courtesy of SDO (NASA) and the AIA consortium. NR 48 TC 18 Z9 18 U1 0 U2 6 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD OCT PY 2013 VL 287 IS 1-2 BP 391 EP 413 DI 10.1007/s11207-012-0194-3 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 214FB UT WOS:000324115600024 ER EF